COMMISSIONS AND OF THE I A U
INFORMATION BULLETIN ON VARIABLE STARS
Nos
November July
EDITORS L SZABADOS K OLAH
TECHNICAL EDITOR A HOLL
TYPESETTING K ORI
ADMINISTRATION Zs KOVARI
EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT
E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG
M RODONO N N SAMUS J SMAK C STERKEN Chair
H BUDAPEST XI I Box HUNGARY
URL http www konkoly hu IBVS IBVS html
HU ISSN
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CONTENTS
C STERKEN A JONES B VOS I ZEGELAAR
A M van GENDEREN M de GROOT On the Cyclicity of the S Dor
Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: :
J BOROVICKA L SAROUNOVA The Period and Lightcurve of
NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::::
W LILLER A F JONES A New Very Long Period Variable Star in
Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::::::
E A KARITSKAYA V P GORANSKIJ Unusual Fading of V Cygni
Cyg X in Early November :::::::::::::::::::::::::::::::::::::::
K N GRANKIN M M ZAKIROV G C ARZUMANYANTS S Yu
MELNIKOV New Eclipsing Binary Star CoD in the Direction
of the Star Forming Region Oph ::::::::::::::::::::::::::::::::::::::::
F AGERER GSC a New Eclipsing Binary ::::::::::::::::::::
A LASALA GARCIA NSV a New Detached Eclipsing Binary
Star in Ophiuchus ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::
G ZAJTSEVA P PETROV I ILYIN R DUEMLER I TUOMINEN
RY Tauri at High Brightness ::::::::::::::::::::::::::::::::::::::::::::::
J GREINER M L HAZEN HV and the Sup ersoft X Ray
Source RX J :::::::::::::::::::::::::::::::::::::::::::::::::
E GARCIA MELENDO J M GOMEZ FORRELLAD NSV a New
Detached Eclipsing Binary Star in Canis Minor ::::::::::::::::::::::::::::
P L NEDIALKOV N A TIKHONOV R G KURTEV G R IVANOV
New Variables in the North Eastern Part of M ::::::::::::::::::::::::::
R M ROBB M D GLADDERS New Variables in the Field of
RE J ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::
Z I KADLA A N GERASHCHENKO Yu N MALAKHOVA Variable
Stars in the Globular Cluster M ::::::::::::::::::::::::::::::::::::::::
Z I KADLA A N GERASHCHENKO Yu N MALAKHOVA Variable
Stars in the Globular Cluster NGC :::::::::::::::::::::::::::::::::::
A S SHAROV On Novae and and Possible Nova in M
M A CERRUTI V Cen New Times of Minima and a Possible
Short Period Mo dulation ::::::::::::::::::::::::::::::::::::::::::::::::::
B A SKIFF A Revision of Dolidze s List of Probable Long Period
Variables of M Types ::::::::::::::::::::::::::::::::::::::::::::::::::
A N GERASHCHENKO Z I KADLA Yu N MALAKHOVA Variable
Stars in the Globular Cluster NGC :::::::::::::::::::::::::::::::::::
G CUTISPOTO M KURSTER I PAGANO M RODONO UBV RI
c
Photometry of the Rapidly Rotating K Type Star HD
Sp eedy Mic ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::
G V WILLIAMS NSV Minor Planet Suleika ::::::::::::::
L N BERDNIKOV D G TURNER Photo electric BVI Observations and
C
a New Classi cation for V Arae ::::::::::::::::::::::::::::::::::::::::
L N BERDNIKOV D G TURNER Photo electric BVI Observations and
C
a New Classi cation for the RS CVn Star GR Normae ::::::::::::::::::::
J M GOMEZ FORRELLAD E GARCIA MELENDO NSV a
Detached Eclipsing Binary Star in Orion ::::::::::::::::::::::::::::::::::
J VIDAL SAINZ J M GOMEZ FORRELLAD E GARCIA MELENDO
NSV is an Overcontact Binary System in Pisces :::::::::::::::::::::
J JUAN SAMSO J GUARRO FLO NSV a Possible Semiregular
Variable in Hercules ::::::::::::::::::::::::::::::::::::::::::::::::::: :::
F CAMPOS CUCARELLA J M GOMEZ FORRELLAD
E GARCIA MELENDO A New Beta Lyrae Variable SAO and Two
New Possible Irregular Stars BD and SAO ::::::::::::::::
J M GOMEZ FORRELLAD A GARRIGOS SANCHEZ NSV
a New Overcontact Eclipsing Binary System in Triangulum ::::::::::::::::
M MIKOLAJEWSKI T TOMOV D KOLEV Activity of T Coronae
Borealis in ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::
Yu A SHOKIN N N SAMUS Accurate Positions for Variables in a
Field Around BL Lac ::::::::::::::::::::::::::::::::::::::::::::::
K KRISCIUNAS R A CROWE A Search for Doradus Type Variables
in the Op en Cluster M ::::::::::::::::::::::::::::::::::::::::::::::::
B A SKIFF Identi cation of the Margoni Stagni Variables ::::::::::::::
T BERTHOLD F AGERER NSV is an Eclipsing Binary ::::::::::
B A SKIFF Identi cation of the Rosino Guzzi Variables in Sagitta ::::::
Yu N MALAKHOVA A N GERASHCHENKO Z I KADLA Variable
Stars in the Globular Cluster M ::::::::::::::::::::::::::::::::::::::::
T PRIBULLA D CHOCHOL P ROVITHIS H ROVITHIS LIVANIOU
Sudden Period Change in the Contact Binary AW UMa ::::::::::::::::::
E GARCIA MELENDO J M GOMEZ FORRELLAD
A GARRIGOS SANCHES Two Variable Stars in Auriga the New
Classical Cepheid NSV and the New Eclipsing Binary System
GSC ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::
L N BERDNIKOV D G TURNER Photo electric BVI Observations
c
New Elements and a New Classi cation for BZ Tuc ::::::::::::::::::::::::
L N BERDNIKOV O V VOZYAKOVA V V IGNATOVA Photo electric
BVR Observations for the UU Her Star EV Aurigae ::::::::::::::::::::::
c
T ROUNTHWAITE G HUDSON R HUDSON E BUDDING Optical
Photometry of CF Tuc Mid Through :::::::::::::::::::::::::::
N MASETTI C BARTOLINI A GUARNIERI A PICCIONI
A Susp ected Red Variable in the Error Box of GRB :::::::::::::::
B A SKIFF Identi cation of Variables Near NGC ::::::::::::::::::
C LLOYD N D JAMES T BERTHOLD G J KIRBY M J COLLINS
GSC a New Deeply Eclipsing Binary System in Delphinus ::::::
E PAUNZEN HD a New Variable Star ::::::::::::::::::::::::::
J WOITAS Detection of New Bright Variables Stars by the Tycho
Instrument of the Hipparcos Satellite ::::::::::::::::::::::::::::::::::::::
T N DOROKHOVA N I DOROKHOV Observations of Three Bo otis
Stars by Using Dual Channel Photometer :::::::::::::::::::::::::::::::::
A N GERASHCHENKO Z I KADLA Yu N MALAKHOVA Variable
Stars in the Globular Cluster NGC :::::::::::::::::::::::::::::::::::
A N GERASHCHENKO Z I KADLA Yu N MALAKHOVA Variable
Stars in the Globular Cluster NGC :::::::::::::::::::::::::::::::::::
B A SKIFF G V WILLIAMS Identi cation of Dahlmark Variables I :::
G V WILLIAMS B A SKIFF Identi cation of Dahlmark Variables II ::
B A SKIFF G V WILLIAMS Identi cation of Dahlmark Variables III
G V WILLIAMS B A SKIFF Identi cation of Dahlmark Variables IV
L SAROUNOVA M WOLF CCD Photometry of Eclipsing Binary AL
Ophiuchi ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::::
J MANFROID P RENSON M BURNET HR a Low Amplitude
Cepheid ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::::
S ENGIN K YUCE Photo electric Observations of X Persei ::::::::::::
L L CHINAROVA Orbital Period of the Eclipsing Variable V Cygni
L N BERDNIKOV D G TURNER Photo electric VI Observations and
c
New Elements for V Carinae HR :::::::::::::::::::::::::::::::
Yu MALAKHOVA A N GERASHCHENKO Z I KADLA Variable
Stars in the Globular Cluster NGC ::::::::::::::::::::::::::::::::::
L DAHLMARK New Variable Stars in the Northern Milky Way :::::::::
B A SKIFF Identi cations for Baade s variables in Sagitta and Cygnus ::
S M RUCINSKI On the Name Over Contact Binary Systems :::::::::
R K ZAMANOV V I ZAMANOVA UBV Observations of T CrB :::::::
Corrigenda ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::
S L KIM M Y CHUN W B LEE L DOYLE A Flare Event Detected
in the Eclipsing Binary CM Dra ::::::::::::::::::::::::::::::::::::::::::
H G REIMANN C FRIEDEMANN A New Susp ected Variable in Pisces
V P ZALINIAN H M TOVMASSIAN Detection of Fast Flares of
EV Lac In ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::
H M TOVMASSIAN E RECILLAS O CARDONA V P ZALINIAN
Observations of Flare Stars EV Lac V Mon and YZ CMi ::::::::::::::
S L KIM H SUNG S G LEE SA HD A New
Eclipsing Binary Among Landolt s Standard Stars :::::::::::::::::::::::::
J R PERCY A DESJARDINS M MARINOVA K LUEDEKE
M S SMITH R R THOMPSON J E WOOD Sorting Out W Bo otis
and its Comparison Stars :::::::::::::::::::::::::::::::::::::::::::::::::
W MOSCHNER E GARCIA MELENDO J M GOMEZ FORRELLAD
W KLEIKAMP Improved Ephemeris and New Observations of NSV
J M GOMEZ FORRELLAD E GARCIA MELENDO Photometric
Results on Three Hipparcos Variables The New Eclipsing Binary Systems
HD and HD and the Star HD :::::::::::::::::::::::
N Z ISMAILOV Photometric Obsrevation of T Tauri Type Stars
DI Cep T Tau V Tau GW Ori V Ori :::::::::::::::::::::::::::::
E V KAZAROVETS N N SAMUS The rd Name List of Variable
Stars ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::::
F AGERER J HUEBSCHER Photo electric Minima of Selected
Eclipsing Binaries and Maxima of Pulsating Stars :::::::::::::::::::::::::
is a New Binary Star ::::::::::::::::::::::::: M JANG GSC
R M ROBB The Eclipsing Binary Star MS ::::::::::::::::
H AK Discovery of an Eclipsing Binary Star in Auriga ::::::::::::::::::
J MANEK Improved Positions for Sonneb erg Variables Part :::::::::
B L NELLERMOE L E REITZLER Eclipse Observations of
AB Andromedae ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::
J MANEK Correct Position of MX Sagittae ::::::::::::::::::::::::::::::
V M IBRAHIMOVA M A IBRAHIMOV Fuor V Cyg Two Years
in Lo cal Minimum ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::
R WASATONIC E F GUINAN Aldebaran Discovery of Small
Amplitude Light Variations :::::::::::::::::::::::::::::::::::::::::::::::
P FRANK W KLEIKAMP W MOSCHNER New Elements of V
Aquilae ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::
T S METCALFE UBV Photometry of the W UMa Star BH Cas ::::::::
R KUSCHNIG E PAUNZEN W W WEISS HD a Pulsating
Candidate Bo otis Star :::::::::::::::::::::::::::::::::::::::::::::::::
M E SACHKOV Radial Velocity Curves and First Calculations of the
Radii for Four Double Mo de Cepheids ::::::::::::::::::::::::::::::::::::
S V ANTIPIN A New Double Mo de Cepheid in Scutum ::::::::::::::::
R M ROBB R GREIMEL The Eclipsing Binary RX J :::::
L N BERDNIKOV D G TURNER The First Photo electric Observations
for the Double Mo de Cepheid BD ::::::::::::::::::::::::::::::
L N BERDNIKOV D G TURNER Photo electric Observations for Two
Misclassi ed Variables AF Crucis and CG Sagittarii Are not Cepheids ::::
R NOVAK Revealing of a New SU UMa Type Variable Star Var
Coronae Borealis ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::
P M VEEN A M van GENDEREN J de JONG Two New Variable Stars
Near the Variable WR HD and the Constant WR
HD ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::
A ALKSNIS A S SHAROV Yu A SHOKIN N M ESTIGNEEVA More
Flares of HY Andromedae ::::::::::::::::::::::::::::::::::::::::::::::::
L V TOTH M KUN New Water Maser in L :::::::::::::::::::::::
Erratum ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::
R M ROBB R GREIMEL Optical Observations of the Star
RX J ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::
E A KOLOTILOV S J KENYON The Recent Optical Decline of
V Cyg ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::
A SKOPAL Photometric Peculiarities of CH Cyg during Its Recent
Quiescent Phase :::::::::::::::::::::::::::::::::::::::::::::::::
J KELEMEN Observation of the Optical Counterpart of the
GRB Source ::::::::::::::::::::::::::::::::::::::::::::::::::: :::
Corrigenda ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::
AIYING ZHOU Multip erio dicity of the Scuti Star BR Cancri ::::::::::
J MANEK Improved Positions for Sonneb erg Variables Part ::::::::::
N D MORGAN R WASATONIC E F GUINAN Near IR TiO Band
Photometry of Ori ::::::::::::::::::::::::::::::::::::::::::::
T A MAHLER R WASATONIC E F GUINAN Radius and Luminosity
Variations of Mira from Wing Near IR Photometry :::::::::::::::::::::::
AUTHOR INDEX
Agerer F Gro ot M de
Ak H Guarnieri A
Alksnis A Guarro Flo J
Antipin S V Guinan E F
Arzumanyants G C Hazen M L
Bartolini C Hudson G
Berdnikov L N Hudson R
Huebscher J
Beresky T Ibrahimov M A
Berthold T Ibrahimova V M
Borovi cka J Ignatova V V
Budding E Ilyin I
Burnet M Ismailov N Z
Camp os Cucarella F Ivanov G R
Cardona O James N D
Cerrutti M A Jang M
Chinarova L L Jones A F
Cho chol D Jong J de
Chun M Y Juan Samso J
Collins M J Kadla Z I
Crowe R A
Cutisp oto G Karitskaya E A
Dahlmark L Kazarovets E V
Desjardins A Kelemen J
Dorokhov N I Kenyon S J
Dorokhova T N Kim S L
Doyle L Kirby G J
Duemler R Kleikamp W
Engin S Kolev D
Evstigneeva N M Kolotilov E A
Frank P Krisciunas K
Friedemann C Kun M
Garcia Melendo E Kurtev R G
Kuschnig R
Garrigos Sanchez A K urster M
Genderen A M van Lasala Garcia A
Gerashchenko A N Lee W B
Liller W
Gladders M D Lloyd C
Gomez Forrellad J M Luedeke K
Mahler T A
Malakhova Yu N
Goranskij V P
Grankin K N M anek J
Greimel R Manfroid J
Greiner J Marinova M
Masetti N Wasatonic R
Melnikov S Yu Weiss W W
Metcalfe T S Williams G V
Mikola jewski M
Morgan N D Woitas J
Moschner W Wolf M
Nedialkov P L Woo d J E
Nellermo e B L Y uce K
Nov ak R Za jtseva G
Pagano I Zakirov M M
Paunzen E Zalinian V P
Percy J R Zamanov R K
Petrov P Zamanova V I
Piccioni A Zegelaar I
Pribulla J Zhou Aiying
Recillas E
Reimann H G
Reitzler L E
Renson P
Robb R M
Ro don o M
Rounthwaite T
Rovithis P
Rovithis Livaniou H
Rucinski S M
Sachkov M E
Samus N N
Sarounov a L
Sharov A S
Shokin Yu A
Ski B A
Skopal A
Smith M S
Sterken C
Sung H
Thompson R R
Tikhonov N A
Tomov T
T oth V
Tovmassian H M
Tuominen I
Turner D G
Veen P M
Vidal Sainz J
Vos B
Vozyakova O V
INDEX OF VARIABLES
The huge lists of variable stars published in the IBVS issues Nos
are not rep eated here
Star IBVS No Star IBVS No
V Pup NSV
AB And
MX Sge
HY
CG Sgr
V Aql
EW Sct
V Ara
BQ Ser
CO Aur
T Tau
EV
RY
W Bo o
V
BR Cnc
Alpha
BZ Tuc
YZ CMi
CF
AG Car
AW UMa
V
Antipin s Var in CrB
TU Cas
BH
BD
BD RE J
V Cen
BD
DI Cep
CoD
Omicron
GRB
T CrB
GSC
AF Cru
GSC
GSC
CH Cyg
GSC
V
HD
V
HD
V
HD
S Dor
HD
HD
CM Dra
HD
EV Lac
HD
GY
HD
V Mon
HD
HD
GR Nor
HD
AL Oph
HR
GW Ori
HV
V
IRAS
Alpha
LD
X Per
Star IBVS No Star IBVS No
MS HD
HD
NSV
HD
NSV
HD
NSV
HR
NSV
IRAS
NSV
LD LD
NSV
in M
NSV
MS
NSV
rd Name List
NSV
in Pisces
NSV
RE J
NSV
RX J
NSV
RX J
h m s 0 00
RE J BD
:
h m s 0 00
:
RX J
h m s 0 00
RX J
h m s 0 00
:
RX J
SAO
SAO
Variables in Clusters
in M
in M
in M
in NGC
in NGC
in NGC
in NGC
in NGC
Extragalactic Variables
in M
in M
New Variables
BD
BD
CoD
GRB
GSC
GSC
GSC
GSC
GSC
HD
HD
HD
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
November
HU ISSN
ON THE CYCLICITY OF THE S Dor PHASES IN AG CARINAE
AG Car HD is a most enigmatic LBV of the southern hemisphere Its light curve
displays episo des of fading and brightening with strongly variable amplitude In
the star was in one of its brightest maxima since the double maximum of and
is now again on its decline Figure displays the light curve since The dots are
visual estimates collected by one of us A J the op en circles that are connected by a full
line represent Walraven V data transformed to Johnson V taken from van Genderen et
al and Str omgren y data from the Long Term Photometry of Variables
LTPV pro ject at ESO Sterken for the data see Manfroid et al
and Sterken et al
Van Genderen et al discussed all available photometric data covering more than
one century and introduced the concept S Dor phase SD viz the phases of brightening
with a more or less regular pattern of recurrence In particular they introduce a new
nomenclature and distinguish normal S Dor phases sup erimp osed on a much slower
rhythm of brightening and fading for which they coin the term Very long term S Dor
phase VLT SD For more details we refer to their pap er
Figure Light curve of AG Car since are visual estimates are based on data from van
Genderen et al and on published LTPV data The continuous line connects all published
photo electric V data
1 Based on observations collected at the Europ ean Southern Observatory Chile
Figure Schematic light curve of AG Car since adapted from van Genderen et al
The solid line covers the observations the dotted line is the lower envelope of the continuous line and
illustrates how the authors think the underlying VLT SD phase could b e represented The numbered
maxima do not corresp ond to the cycle numbers as shown in Figure Note the double maximum
From on after JD the light curve shows a fairly uninterrupted sequence
of S Dor maxima Numbered in the van Genderen et al pap er this se
d d
quence of times of maximum yielded a p erio d of see Figure for a partial
repro duction of Figure of van Genderen et al Extrap olating the cycle numbering
d d
scheme to the past these authors re ned the p erio d to P The resulting
O C diagram did not show a random pattern but suggested a p ossible cyclic b ehaviour
on a time scale of ab out d or y for the time interval
Unfortunately diminishing opp ortunities for observing AG Car in the framework of
LTPV made a complete coverage of the double maximum imp ossible How
ever from a preliminary reduction of yet unreleased LTPV data collected in November
and December we could derive one additional time of maximum viz HJD
corresp onding to cycle E see Figure The visual light curve also suggests max
ima at JD and The photo electric maximum at E fully
con rms the one derived visually The rst of the new visual maxima was not taken to
corresp ond to the brightest estimate b ecause the real maximum likely o ccurs around the
middle of the corresp onding blo ck of data as is also illustrated by the di erence b etween
the brightest y measurement and the maximum of the tted curve in Figure The
maximum at E provisionally estimated at JD and bracketed in Table
of van Genderen et al in reality seemed to have o ccurred later that is around
JD Note that the estimation of the time of extremum during a sup ermaximum
maxima in Figure the double maxima in and in is particularly
di cult b ecause the star do es not have the time to fall back to its low state of light output
b efore the d cycle is completed
Figure LTPV y V photometry in the natural system Each data p oint represents one
di erential measurement The line represents the tted third degree p olynomial used to calculate the
time of maximum Note the asymmetric form with a descending branch that is much steep er than the
ascending branch a phenomenon that is typical for normal SD phases on the descending branch of the
VLT SD phase see also Figure
The new O C diagram is shown in Figure The two estimates of the time of
maximum corresp onding to E have b een agged by an arrow in Figure as well as
the last p oint in the diagram which ultimately may turn out to shift upward as suggested
in the gure The gure clearly con rms the cyclic pattern on a time scale of y as
suggested by van Genderen et al
Figure O C diagram for SD maxima cycle numbers of AG Car for the linear
d
ephemeris constructed with P van Genderen et al The at E is derived from
a sequence of photo electric measurements see Figure The op en circles at E are based on
new visual estimates The upp er vertical arrow indicates the corrected p osition of the E maximum
which was provisionally estimated on the basis of incomplete data by van Genderen et al The indicates the shift to b e exp ected when the current SD phase will have b een observed completely
The new visual and photo electric data collected after the conclusion of the study of
van Genderen et al allow us to con rm that the cyclic b ehaviour of the normal
S Dor phases of AG Car is maintained
This work was supp orted by a research grant from the Belgian Fund for Scienti c
Research NFWO The data have b een obtained during ESO time allo cation D
C STERKEN
University of Brussels VUB
Pleinlaan
B Brussels Belgium
A JONES
Carter Observatory
P O Box
Wellington New Zealand
B VOS
I ZEGELAAR
A M van GENDEREN
Leiden Observatory
Postbus
RA Leiden The Netherlands
M de GROOT
Armagh Observatory
College Hill
Armagh BT DG Northern Ireland
Belgian Fund for Scienti c Research NFWO
References
van Genderen A M Sterken C de Gro ot M A A in press
van Genderen A M Th e P S Augusteijn Th et al A AS
van Genderen A M Th e P S Heemskerk M et al A AS
Manfroid J Sterken C Bruch A et al A AS
Manfroid J Sterken C Cunow B et al A AS
Sterken C The Messenger
Sterken C in Precision Photometry D Kilkenny E Lastovica J Menzies Eds
South African Astronomical Observatory
Sterken C Manfroid J Anton K et al A AS
Sterken C Manfroid J Beele D et al A AS
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
THE PERIOD AND LIGHTCURVE OF NSV
h m s
The variability of NSV SVS UMa GSC
0 00
J was discovered by Parenago He classi ed the star as
an eclipsing binary and gave two times when the star was found near minimum light on
a photographic plate The star had b een then neglected for a long time except for an
inconclusive visual survey of Lo cher We started to observe NSV in with
an cm telescop e and a SBIG ST CCD camera The observations were continued in
with the same telescop e but b etter ST camera These early observations made
without a lter con rmed the type of variability and yielded four times of minima and a
preliminary p erio d
In we p erformed a regular photometry of NSV with a cm telescop e and
the ST camera Standard V Johnson and R Cousins photometric lters were used
The technical con guration of the telescop e normally used for other purp oses did not
allow to change the lters automatically Instead in some cases only one lter was used
in a particular night Typical exp osures were as long as seconds and the high
signal to noise ratio enabled the relative precision of one measurement of ab out
mag in R and mag in V lter to b e reached Altogether measurements in
was used as the comparison star R and in V have b een obtained GSC
and GSC as the check star The magnitudes were transformed to the absolute
scale using the standard stars according to Landolt and checked by the Guide
Star Catalog Due to the uncertainties in extinction low precision of photometric data
in the GSC and other instrumental e ects the absolute calibration is less certain and
a systematic shift as high as mag is p ossible We derived the magnitude of the
comparison and the check star as V V R and V V R
m
resp ectively The probable error of the color indices is The variable comparison
and check stars are identi ed in Figure
All times of primary minima are given in Table Using only our minima we derived
the following light elements
JD min E
hel
The O C residuals relative to these elements are also given in Table Parenago s two
minima show negative O C residuals probably larger than the error of observation
This suggests that the p erio d of the star was slightly longer in the past but the lack of
data prevents to draw a rm conclusion
1
The table of observational data in ASCI I format is available as the t txt le together with the electronic version of the Bulletin
0 0
Figure Identi cations chart of NSV The size of the eld is The
comparison star is denoted with A and the check star is C
Table The times of minima of NSV
JD f N w E O C source
hel
pg Parenago
pg
cm ST
cm ST
R cm ST
R
V
R
f lter N number of measurements w weight E ep o ch
Table The lightcurve parameters of NSV
M A A
max I II
V band
R band
M magnitude A amplitude mag
I I I primary and secondary minimum resp ectively
The mean lightcurve of NSV in the V and R lters is given in Figure It is
a typical lightcurve of an Algol type eclipsing binary The eclipses are partial and their
h
duration is i e of the p erio d No sign of asymmetry is present The magnitudes
are summarized in Table
-0.4
V -0.2
e ud it R gn 0.0 a m
e v ti a l 0.2 e
R NSV 4497
0.4
-0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2
Phase
Figure The mean lightcurve of NSV Relative V R magnitudes to the
comparison star A are given
J BOROVICKA
L SAROUNOVA
Astronomical Institute
Ond rejov Observatory
Czech Republic
e mail b orovic asu cas cz
lenka asu cas cz
References
Landolt A Astron J
Lo cher K B B S A G Bul l No
Parenago P Perem Zvezdy
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
A NEW VERY LONG PERIOD VARIABLE STAR IN NORMA
IAU Circular rep orted the p ossible photographic discovery on May of
a nova by W Liller and the same IAUC rep orted that the ob ject s existence had b een
con rmed by R H McNaught and D Overbeek and by D Baade and J Krautter The
last pair of observers obtained a sp ectrogram which showed several strong narrow Balmer
lines in emission plus Fe I I at nm but also strong molecular bands as in stars of
sp ectral type M M They go on to say that the ob ject may b e related to the class of
symbiotic stars although no trace of emission due to O I I I and nm and He I I
nm are seen McNaught noted that the star app eared clearly red and further
rep orted that a search of photographic charts back to shows its variation from
00
mag to fainter than B : He also gave a precise p osition Equinox
h m s 0 00
R A : Dec :
The variable app ears in the Hubble Guide Star Catalog its average p osition from two
GSC determinations is Equinox
h m s 0 00
R A : Dec :
The GSC magnitudes listed are and Duerb eck includes the star as
N Nor variable of late type p and provides a nding chart p
His curiosity aroused A F Jones b egan to make visual observations of the star while
Liller continued to take photographs of this region of the Southern Milky Way as a part of
his continuing PROBLICOM nova search program Later with the acquisition of a CCD
Liller started to follow the brightness changes of the star using a cm f Schmidt
camera and various lters
As of this writing eight maxima have b een observed and Figure shows the light curve
around the well observed maximum of as measured visually by Jones and with an
un ltered CCD by Liller The more than magnitude di erence in the p eak magnitudes
obviously results from the strong red and by inference infrared continuum rep orted in
IAUC by Baade and Krautter and the extended red and infrared sensitivity of the
CCD Esp ecially noteworthy are the pre maximum standstill clearly visible in the
CCD measurements and just barely detected by Jones and the much slower decrease
in brightness after maximum as measured with the CCD than visually mag compared
with mag during the rst days However the two times of o ccurrence of p eak
brightness agree very closely at JD
Combining all the observations available we arrive at a mean p erio d of days
years Times of maximum for the rest of this century are herewith predicted to b e
on or ab out Oct and May
The p erio d of the Norma variable is considerably longer than the days given by
Ho meister et al as the maximum of the p erio d distribution of all Mira variables indeed only Miras of are listed as having p erio ds longer than days However
Figure The light curve of the new variable in Norma showing Jones s visual magnitudes crosses and Liller s
non ltered CCD magnitudes closed circles The v s represent selected fainter than estimates Note the two
p ositive visual sightings near J D b oth were very close to the limit of detectability on those nights
the p erio d of the Norma variable is still far less than that of the day p erio d given
for BX Mon and listed as a symbiotic Mira variable Sp M ep F in the th edition
of the General Catalogue of Variable Stars Kholop ov et al
We intended to publish elsewhere all the observations which we have accumulated
meanwhile the numerical data can b e obtained by writing the rst author
WILLIAM LILLER
ALBERT F JONES
Instituto Isaac Newton
Carter Observatory
Casilla Correo
P O Box
Santiago Chile
Wellington N Z
References
Duerb eck H W A Reference Catalogue and Atlas of Galactic Novae Dordrecht
Reidel
Ho meister C Richter G and Wenzel W Variable Stars New York Springer
Verlag p
Kholop ov P N Samus N N Frolov M S Goranskij V P Gorynya N A Kazarovets
E V Kireeva N N Kukarkina N P Kuro chkin N E Medvedeva G I Perova
N B Rastorguev A S and Shugarov S Yu General Catalogue of Variable
Stars Vol th edition Moscow Nauka p
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
UNUSUAL FADING OF V CYGNI Cyg X
IN EARLY NOVEMBER
Monitoring of V Cyg an optical counterpart of the X ray source Cyg X and
known black hole candidate was carried out at Tien Shan astronomical observatory
Kazakhstan from Octob er to November The meter re ector and a four
h m s
channel WBVR photometer were used The A V type star HD
m
V was used as a comparison star in this observational set Its
magnitudes were taken from the Catalogue of WBVR Magnitudes of Northern Sky Bright
h m s
Stars Kornilov et al Two check stars selected by Lyutyi a
h m s
and c were measured regularly with
the variable star The diaphragm was always used for the visual binary a thus
we measured the combined brightness The star a was found to b e a small amplitude
m m
variable in the range of V with one of the two p ossible p erio ds P
d d
and P
6
V Cyg Cyg X
V
s
s
s
s
s
s
m
s s s s s
s s s s
s s s :
s
s s s
s s s s s s s
s s s s
s s s s s
ss s s
s s s s s
s s s s
s s s ss
s s s s s s s
s
s s s s
s s s
s s
s s s s s s s
s s s ss s s s s s s s
ss s s ss
s s ss s s ss s
s s s s ss s s s s
s ss s s s s s s s s
s s s s s s s s
s s s s s s s s s s s s s s s
s s s s s s s s s s sss s
ss s s s s
s s s s s s s s s s s
s s s s s s s s
s s s s s s
s s s s s sss
s s s s s s s s s ss
s s s s s s
s s s s s
s s s s ss s ss s ss
s s s s s
s s sss s
s s s s s s s
s s s s s
s s s s s
s s s
s
s s
s s
s s s s s s
s
s
s s
s s
s
s s
s
s
s
s
s
s
s
s
s
s
s s
s
s s
s
s
V
c
c
c
c c
c c c
c c
c
m
c
c c c
c cc :
c c c
c
c c
c c c
c c c c
c c c c c
c c c
c c c c c
c c c c c c
c c c c c c c c c
c c c c c
c c c c
c c c c c c c cc
c c c c c c c c
c c c c c c
c c c c c c
c c c c c c c c c c c
c c c c c c
c c c c c c cc c c c c c c c c c
c c c c c c c c c c
c c cc c c c cc c c c c c c c c c
c c c c c c c cc c cc c c c c c c c
c c c c c c c c c c c c c c
c c c c c c c c
c c c cc cc c c c c c c
c c c c c c c c
c c c c c c c c c c c
c c c c c c c cc c c c c c
c c c c c c
c c c c
c c c c c c
c c
c
cc c c c
c
c
c
c c
c c c
c
c
c
c
c
Control star c
-
JD
Figure Light curves of V Cyg and of the check star V are deviations of
observations from the mean ellipsoidal light curve
V Cyg normally shows ellipsoidal double wave variability with the p erio d of P
d m
and the total mean amplitude of V The accuracy of an individual measurement
m m
was in the range of But on November the star was found to b e fainter by
m m
V than the mean ellipsoidal wave level and its brightness b ecame lower by than
Min I Deep fading of V Cyg without colour variations was seen on JD
During this time the star demonstrated ellipsoidal variations with the former amplitude
in all the photometric bands Figure shows light deviations of V Cyg in V band
against the normal double wave level and the light curve of the check star c The OB
star light predominates in the radiation of this system The contribution of the accretion
m
disk into combined light was estimated by Bruevich et al to b e V This value
is approximately equal to the depth of the fading The dramatic change of the brightness
level may suggest a strong change of the accretion disk structure which has led to the
disapp earance of the optical radiation from the disk
It would b e very imp ortant to know the b ehaviour of the X ray radiation at this time
E A KARITSKAYA
V P GORANSKIJ
Institute for Astronomy
Sternberg Astronomical Institute
of Russian Academy of Sciences
Moscow University
Moscow Russia
Russia
karitsk sai msu su
goray sai msu su
References
Bruevich V V Kilyachkov N N Syunyaev R A Shevchenko V S Soviet Astron
Letters
Kornilov V G Volkov I M Zakharov A I et al Sternberg Astron Inst Trans
Lyutyi V M Variable Stars
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
NEW ECLIPSING BINARY STAR CoD IN THE DIRECTION
OF THE STAR FORMING REGION Oph
The members of the Upp er Scorpius region were observed by Eggen in an
extensive intermediate band and H photometry He detected the variability of CoD
m
SAO The star was changing its light from V August
m m
to V September In September the star had a brightness of R
m m m
and R I while the resp ective values were and and in July Herbig
see Struve and Straka determined the sp ectral type to b e A or A but found no
emission in The star is situated in the direction of the star forming region Oph
near the weak line T Tauri stars Rox and Rox
We present the results taken from a long term photometric monitoring program for
CoD made during three runs from August to July Our
UBVR observations were obtained at the Mt Maidanak Observatory Uzb ekistan us
ing m and m telescop es equipp ed with a pulse counting FEU photomultiplier
m
tub es The mean error of a observation is typically in V CoD was used
m m m m
as comparison star V U B B V and V R
A p erio dogram analysis of observations proved that CoD is a short p erio d
eclipsing binary star likely of W UMa type The ephemeris for the primary minimum is
d
Min I JDH E
The total number of observations are in U in B in V and in R We
detected moments of minima and they are listed in Table The light curves of the
binary are shown in Figure The main photometric characteristics are given in Table
Table
JDH E O C JDH E O C
d d
Table
Phase V U B B V V R
Max
MinI
MinI I
Figure Light curves in the U B V and R bands for CoD
The change in the colors of the variable is slight We note that the p osition of the
binary in the color color diagram do es not corresp ond to a sp ectrum A The comp onents
of the binary may b e F G stars Perhaps the binary is a foreground ob ject in the direction
of the star forming region Oph
One of us MMZ was supp orted by Fund for Fundamental Research of Republic Uzb ek
istan Contract
K N GRANKIN
M M ZAKIROV
G C ARZUMANYANTS
S Yu MELNIKOV
Astronomical Institute
Astronomical str Tashkent
Uzb ekistan CIS
e mail grankin silk glas ap c org
e mail mamnun astro gov us
References
Eggen O J Mon Not R Astr Soc
Struve O and Straka W C Publs Astr Soc Paci c
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
GSC A NEW ECLIPSING BINARY
BAV Mitteilungen Nr
In a photometric investigation in the eld of PX Cep one of the stars GSC
proved to b e variable A check of the GCVS and NSV catalogs did not reveal any previ
ously known variable at this p osition The Guide Star Catalog quotes GSC as a
m
non stellar ob ject p ossibly caused by a nearby star merging with the new variable
m
The brightness of GSC is given as :
Observations were p erformed in nights b etween June and November An
ST CCD camera without lters attached to a cm SC telescop e was used The primary
m m
and secondary minima have an amplitude of : and : resp ectively As the variable
always was measured together with its companion in the di erential ap erture photometry
the real amplitude of b oth minima may b e somewhat greater GSC served as
comparison star several other stars in the same eld were used to check its constancy
The time b etween rst and last contact is ab out hours a total eclipse could not b e
detected The individual measurements are sent via e mail on request Obviously the
brightness in maximum light is not constant This may result from interference with the
nearby companion If not GSC may b e of RS CVn type
A p erio d analysis program based on the algorithm of Schwarzenberg Czerny
together with the times of minimum light resulted in the preliminary ephemeris
d
Min I HJD : E
Figure Finding chart for GSC v the comparison star is c North is up
0 0
east to the left The eld is : :
Figure Di erential light curve of GSC drawn with the ephemeris derived in
this pap er
Table Times of CCD measured minima for GSC ep o chs and residuals
computed with resp ect to the ephemeris derived in this pap er
N JD hel W Ep o ch O C
F AGERER
Bundesdeutsche Arb eitsgemeinschaft
f urVer anderliche Sterne e V BAV
Munsterdamm
D Berlin Germany
E mail
agerer zweik t online de
Reference
Schwarzenberg Czerny A Monthly Notices R Astr Soc
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
NSV A NEW DETACHED
ECLIPSING BINARY STAR IN OPHIUCHUS
According to Kholop ov the variability of NSV BD BV
CSV GSC was announced by Strohmeier et al who indicated
m
that this ob ject underwent fast light changes b etween photographic magnitudes : and
m
: without sp ecifying the type of variability In the Guide Star Catalogue NSV
is a star with a photographic magnitude of This magnitude value was
determined from photographic plates taken with the U K SERC Schmidt Telescope using
a GG lter and a I I IaJ photographic emulsion The sp ectral information recorded in
the NSV catalogue indicates that the sp ectral type of NSV is A
To con rm its variability NSV was observed in the V band for nights from
June to September using a CCD camera attached to a m telescop e from
Zaragoza and Morata de Jalon Spain GSC and GSC were used as
comparison and check stars resp ectively Photometric reductions suggest that the check
star might b e slightly variable It is planned to monitor this ob ject in the near future to
check its variability Figure
Observations show that NSV is a detached eclipsing binary star with a p erio d
close to days see Figure The depth of the primary minimum in the V band is
m m
: : The secondary minimum is ab out magnitudes shallower Figure
The following ephemeris has b een computed
d
Min I HJD : E
Antonio LASALA GARCIA
Grup d Estudis Astronomics
Apartado
Barcelona
Spain
e mail alasala astro gea cesca es
References
Kholop ov P N editor New Catalogue of Susp ected Variable Stars Moscow
Strohmeier W Kipp enhahn R Geyer E KVB No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
RY TAURI AT HIGH BRIGHTNESS
m m
The T Tau star RY Tau has increased its brightness from V : to V : in the
p erio d from middle of Octob er to middle of November this year with no changes in U B
and B V Photometric monitoring of RY Tau is going on at the Crimean Lab oratory of
the Sternberg Astronomical Institute Russia with the cm telescop e and the photon
counting photometer The following is a subset of the photometric data from and
the recent observations in Octob er and November also plotted in Figure
JD V U B B V
Figure Light and colour variations of RY Tau
4 Relative intensity 3
2
1
0 -400 -200 0 200 400
Radial velocity
Figure Variations in H pro le the most intensive pro le is of December low
brightness of the star others are of November high brightness
1.10
1.05
1.00 Relative intensity 0.95
0.90
0.85
0.80
0.75
0.70 5430 5440 5450 5460 5470
Stellar wavelength
Figure Fragment of the photospheric absorption sp ectrum of RY Tau taken at
di erent brightness of the star the sp ectra are overplotted No di erence in line pro le or intensity is noticeable
High resolution echelle sp ectra of RY Tau were taken with the SOFIN sp ectrograph at
the m Nordic Optical Telescope La Palma Spain at low brightness of the star
Dec and at high brightness Nov Nov Nov Nov and Dec
The sp ectral range was nm the resolving p ower S N ratio In spite of
the large brightness di erence all the sp ectra show the same photospheric sp ectrum of a
late G star with the same line depths and line ratios and with the same veiling factor of
ab out The equivalent width of H emission has changed from nm to nm that
is the ux radiated in the line remains at ab out the same level as b efore the brightening
of the star see Figure The sp ectra taken at high brightness of RY Tau show the usual
night to night variations in emission line pro les of HI and CaI I sup erp osition of broad
emission with multiple variable absorption comp onents at radial velocities from to
km s No variations were found in photospheric absorption lines see Figure
Similar event of brightening of RY Tau by more than one magnitude with constant
colours was observed in Za jtseva et al Sov Astron Lett
G ZAJTSEVA
Sternberg Astronomical Institution
Russia
P PETROV
Crimean Astrophysical Observatory
Ukraine
I ILYIN
R DUEMLER
I TUOMINEN University of Oulu Finland
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
1
HV AND THE SUPERSOFT X RAY SOURCE RX J
The discovery of the sup ersoft X ray source RX J during the ROSAT rst
light observation Tr umper et al of the Large Magellanic Cloud LMC in June
has directed some attention to the optical variable HV b ecause its lo cation is
within the X ray error circle of RX J Tr umper et al Greiner et al
Later ROSAT observations improved the X ray p osition resulting in a larger o set
to HV Cowley et al Greiner et al a b However it also b ecame clear
that there are no exact co ordinates available no SIMBAD entry for HV To our
knowledge the only nding chart available for HV is the Large Magellanic Cloud atlas
by Ho dge Wright see Figure but unfortunately the scale is to o p o or and the
variable itself invisible While only a summary of the variability of HV is published
in form of table entries in Shapley Mohr based on the investigation of only
plates and Shapley McKibb en Nail the detailed notes of the Gap oschkins
C H Payne Gaposchkin and S Gap oschkin on the brightness estimates of HV on
plates taken b etween and of mainly the A series are unpublished
Given these facts we went back to the original plates and re identi ed HV From
the unpublished individual brightness estimates recently archived by D L Welch and elec
tronically available on http www physics mcmaster ca HCO we selected four plates
two with HV b eing brightest and two plates with it b eing in a faint state A com
parison of the brightest faintest plate pairs quickly revealed a clearly variable ob ject with
an amplitude consistent with the value of m mag Shapley McKibb en Nail
Our indep endent relative brightness estimates on nearly further plates are in
go o d agreement to those of the Gap oschkins and thus con rm the correctness of our
re identi cation The astrometry on plates showing HV in the bright state is over
plotted on a CCD frame taken in March small circle in Figure and demonstrates
00
that its p osition is within the X ray error circle of RX J
These ndings provided the motivation to determine the pattern of optical variability
of HV over the last six years during which RX J was found to gradually
decline in X ray intensity Greiner et al a b For this purp ose we investigated
ab out blue plates out of the plates blue red taken b etween Oct
and Jan within the EROS pro ject for the search of microlensing events of the
LMC Aub ourg et al Two di erent emulsions were used in the blue passband
with lter GG I IaO during and the emulsion I I IaF during Oct
While plates of b oth emulsion types are generally more sensitive than the Harvard
00
plates the I I IaF emulsion even provides a spatial resolution b elow thus reaching in
00
b est cases a quality comparable to the CCD image shown in Figure seeing of :
As a consequence in most cases several or even all of the at least ob jects within the
astrometric error circle of HV are resolved and detectable on these EROS pro ject
1 PARTLY BASED ON OBSERVATIONS WITH THE ESO M TELESCOPE AT LA SILLA CHILE MPI TIME
0 0
Figure A : : area around HV center repro duced from the Ho dge
Wright atlas of the LMC The variable is lo cated inside the triangle ab ove the
mark North is at the top and East to the left
00
Figure The X ray error radius large circle of RX J overplotted on a
min B image taken on March with the ESO m telescop e at La
Silla Chile The small circle denotes the b est t astrometric p osition of HV as
determined from plate A of the Harvard plate collection Numbers denote all
resolved ob jects within the X ray error circle large circle Greiner et al a
plates In addition to these plates we have investigated single plates taken for other
purp oses in and The surprising result of our analysis of all
the investigated plates was the fact that we did not nd any variable ob ject within or
around the astrometric p osition of HV
The non variability of any of these ob jects on the EROS Schmidt plates as opp osed to
the apparent variability on the Harvard plates can b e due to several reasons
The re identi cation of HV is wrong while the original measurements are of a
di erent ob ject We have carefully checked this p ossibility but can de nitely exclude
it There is no other star of the given brightness around the p osition marked on the
Ho dge Wright atlas and in addition the variability pattern found on the
plates coincides with that of the unpublished notes of the Gap oschkins
HV has ceased to be variable in the two decades b etween the last Harvard plates
and the rst EROS pro ject plates with the few other individual plates
it would b e even b efore Though this would b e a rare circumstance it cannot
b e excluded
HV is not intrinsically variable on the Harvard plates Instead the combination
of variable seeing and di erent limiting magnitudes of the plates result in a di erent
size of the image of the several overlapping ob jects and thus counterfeits a variability
This reasoning implies a clear prediction namely that HV app ears bright on
plates with b etter than average seeing and sensitivity so that ob jects and and
probably also contribute to the size of the merged image while on plates with bad
seeing and sensitivity only ob ject is imaged thus resulting in a considerably smaller
size on the plate A re investigation of the Harvard plates has indeed con rmed this
relation b etween the brightness of HV and the plate quality
We therefore conclude that though variations are seen at rst glance on the Harvard
plates a careful lo ok including a consideration of the e ects of di erent seeing di erent
fog level and limiting magnitude shows that variations of HV are marginal at b est
A hint of supp ort comes from the fact that the measurements on the unpublished notes
from the Gap oschkins were crossed out which usually means that they did not consider
the ob ject to b e variable in the end We would like to mention however that it is not
p ossible to exclude de nitely intrinsic optical variability of HV
Given the large amplitude of the X ray decline of RX J over the last six
years a factor of one is inclined to exp ect a correlated either p ositive or negative
variability of its optical emission The lack of any obvious optical variability of ob jects
through in Figure though somewhat uncertain for the faint ob jects through
suggests that none of these is the optical counterpart of RX J Sensitive
optical observations imaging and sp ectroscopy at sub arcsecond resolution are certainly
required to identify RX J
Acknowledgements JG is indebted to J Guib ert and E Lesquoy for kind hospital
ity at the Paris Observatory We are grateful to D Welch for detailed information on
the unpublished Gap oschkin material JG is supp orted by the Deutsche Agentur f ur
Raumfahrtangelegenheiten DARA GmbH under contract FKZ OR
JOCHEN GREINER
MARTHA L HAZEN
MPI f ur extraterrestrische Physik
Harvard College Observatory
Giessenbachstr
Garden Street
D Garching Germany
Cambridge MA
e mail jcg mp e garching mpg de
e mail mhazen cfa harvard edu
References
Aub ourg E Bareyre P Brehin S Gros M Lachieze Rey M Laurent B Lesquoy E
Magneville C Milszta jn A Moscoso L Queinnec F Rich J Spiro M Vigroux
L Zylb erach S Ansari R Cavalier F Moniez M Beaulieu J P Ferlet R Grison
Ph Vidal Madjar Guib ert J Moreau O Tajahmady F Maurice E Prevot L
Gry C Nat
Cowley A P Schmidtke P C Hutchings J B Crampton D McGrath T K ApJ
L
Greiner J Hasinger G Kahabka P A A L
Greiner J Schwarz R Hasinger G Orio M a A A
Greiner J Schwarz R Hasinger G Orio M b in Sup ersoft X ray Sources ed J
Greiner LNP p
Ho dge P W Wright F W Atlas of The Large Magellanic Cloud Smithonian
Press
Shapley H Mohr J Ann of Harvard Col l Obs No
Shapley H McKibb en Nail V Proc of Nat Acad of Sci No
Tr umper J Hasinger G Aschenbach B Br auningerH Briel U G Burkert W Fink H
Pfe ermann E Pietsch W Predehl P Schmitt J H M M Voges W Zimmermann
U Beuermann K Nat
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
NSV A NEW DETACHED ECLIPSING BINARY STAR
IN CANIS MINOR
Following the co op eration program b etween the Esteve Duran Observatory Foundation
and the Grup d Estudis Astronomics for the identi cation and study of p o orly observed
variable stars NSV WR CSV was monitored in the V band for
nights using a CCD camera from January to May Observations were carried
out with the m Cassegrain telescop e at Esteve Duran Observatory in Seva Spain
and the m telescop e at Mollet del Valles Observatory Spain GSC and
GSC were used as comparison and check stars resp ectively NSV could
b e unambiguously identi ed with GSC
In the NSV catalogue Kholop ov it is recorded that variability of NSV
was rst observed by Weber who rep orted that this star was a p ossible Cepheid
m m
with a photographic brightness variation from : to :
Our observations show that NSV is not a Cepheid but a detached eclipsing
binary star with a p erio d over days Phase curve indicates that primary and secondary
m m
minima are : and : deep partial o ccultations resp ectively Figure The following
ephemeris has b een derived
d
Min I HJD : E
Figure
To determine the magnitude and B V color index of NSV and its comparison
star these ob jects were also observed in the B and V bands using an Optec SSP A
photo electric photometer HR HR and HR were used as comparison
stars As a result it was obtained that NSV has a visual magnitude at maximum
light of and an observed color index of
Sp ectroscopic observations and multicolor photometry should b e p erformed in order
to obtain more accurate information ab out this new eclipsing binary star
E GARCIA MELENDO
J M GOMEZ FORRELLAD
Esteve Duran Observatory
Grup d Estudis Astronomics
El Montanya Seva
Apartado
SEVA
Barcelona
Barcelona
Spain
Spain
e mail jmgomez astro gea cesca es
e mail duranobs astro gea cesca es
References
Kholop ov P N editor New Catalogue of Susp ected Variable Stars Moscow
Weber R Do cumentation des Observateurs Circulaire No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
NEW VARIABLES IN THE NORTH EASTERN PART OF M
The north eastern part of M has b een p o orly studied for variable stars in contrast
to the south western one After the pioneering survey of Hubble which covered
0
the entire b o dy of the galaxy only elds each with a diameter of lo cated at the
di erent galacto centric distances along south western ma jor axis were studied for variable
stars in details Baade Swope Gap oschkin Only one new day
cepheid has b een added Ivanov in the north eastern part since Hubble s times
The main goal of this work is to lo ok for new variables in the north eastern part of
0 0
M We used plates B passband eld obtained at the m telescop e f
h m s
of SAO RAN Russia from until They are centered on
0
and This p osition was considered to include the larger part of the bulge
of M which is the most probable area for discovering of novae and study of all four
Hubble Sandage variables in Andromeda nebula The exp osure time was usually hours
A separate calibration curve was constructed for each of our plates We used
standard stars from the photo electric sequences of Humphreys et al and CCD
measurements of Massey et al The mean error of our calibration curves is ab out
m
: The stars were measured with a constant slit photometer
We selected new variable stars candidates within the investigated area blinking
pairs They were included in a list of known or susp ected variables together with
00
previously known variables within the same area Their co ordinates accurate to :
are given in Table The identi cation chart for these variables is given in Figure
Table Co ordinates of known and susp ected variables in the NE part of M
No Points Rem No Points Rem
h m s 0 00 h m s 0 00
V
V
nova
I V
V
V
V
V
V V
V V
V
VA
Figure
Table Photometry of stars No No and No
JD No No No
Figure Light curve of star No
Figure Light curve of star No
Figure Light curve of star No
Our measurements show that practically all the susp ected variables show measurable
m
change in brightness amplitudes greater than : but only for of them we can present
a list with more than p oints of observation A p erio d nding programme was applied
to obtain the appropriate p erio ds For three of these stars acceptable light curves were
found Photometry of these stars is presented in Table
Figures show computed light curves with obtained p erio ds Luminosities of these
variables coincide with the values predicted by the p erio d luminosity relation for the
cepheids in M The star No was classi ed from Hubble as an irregular
variable
The limiting magnitude of our plates prevents us from reaching the levels more p op
ulated by cepheids Most of the known and susp ected variables are found out of the
b oundaries of the OB asso ciations
This pro ject is supp orted by grants F and F with the National Science
Foundation Bulgaria
P L NEDIALKOV
R G KURTEV
Department of Astronomy
Department of Astronomy
So a University Bulgaria
So a University Bulgaria
N A TIKHONOV
G R IVANOV
SAO of the Russian Academy of Sci
Department of Astronomy
Nizhnij Arkhyz Russia
So a University Bulgaria
References
Baade W Swope H AJ
Baade W Swope H AJ
Gap oschkin S AJ
Hubble E ApJ
Humphreys R Sitko M Sitko A PASP
Ivanov G Ap SS
Massey P Armandro T Conti P AJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
NEW VARIABLES IN THE FIELD OF RE J
The sky was surveyed in the extreme ultraviolet EUV region of the sp ectrum by the
EUVE satellite Malina et al and the ROSAT satellite Pounds et al and
catalogs of the sources included RE J EUVE J BD
The star was one of the sub jects of an investigation by Je ries GSC
who concluded from sp ectral observations that it was a pair of nearly identical K dwarf
d
stars orbiting with a : p erio d
The automated m telescop e Cousins R lter and CCD camera of the Climen
haga Observatory of the University of Victoria Robb and Honkanen were used to
make photometric observations of RE J Using IRAF routines the frames were
de biased and at elded and the magnitudes were found from arc second ap erture
photometry after using the Gaussian centering option of the PHOT package
The eld of stars we observed is shown in Figure and their designations co ordinates
J and magnitudes from the Hubble Space Telescope Guide Star Catalog GSC
Jenkner et al and the R magnitudes are tabulated in Table The R di er
ences in magnitude are found from our data in the sense of the star minus GSC
m
The standard deviation of the di erences during a night ranged from : for a bright
m
star on a go o d night to : for the faint stars on p o or nights The R magnitude given
in the table is the mean of the thirteen nightly mean di erential magnitudes and the
standard deviations measure night to night variations The stars and
have large standard deviations and are variable from night to night Due to the small eld
of view extinction e ects were negligible and no corrections have b een made for them No
corrections have b een made to transform the R magnitude to a standard system
Photometric observations were made from February to March UT Bright
ness variations in RE J were evident b oth during a night and from night to night
A least squares t of a single sine wave to the data shows a deep minimum in at a
d
p erio d of : A p erio d nding routine based on that of Jurkevich found the b est
d
p erio d to b e : Two other p ossible p erio ds are rendered less likely by the sp ectral
d d
observations Je ries namely : which is a one cycle p er day alias and :
which is twice the adopted p erio d
So in agreement with Je ries the b est ephemeris from our data is
d d
HJD of Minima : : E
d d
: :
A plot of the di erential R magnitudes phased at this p erio d is shown in Figure
with di erent symbols for each of the di erent nights While the light curve do es show a
p ossible primary eclipse the lack of a corresp onding secondary eclipse leads us to b elieve
that this is not an eclipsing system a p ossibility suggested by Je ries We susp ect
1
IRAF is distributed by National Optical Astronomy Observatories which is op erated by the Asso ciation of Universities for Research in Astronomy Inc under contract to the National Science Foundation
Table Stars observed in the eld of RE J
GSC No RA Dec GSC R
J J Mag Mag
h m s 0 00
h m s 0 00
h m s 0 00
h m s 0 00
h m s 0 00
h m s 0 00
h m s 0 00
Figure Finder chart of the eld lab eled with the GSC numbers Jenkner et al
Figure Light curve of the di erential R data of RE J for
Table Di erential observations of GSC
HJD R HJD R HJD R HJD R
that one or b oth stars have large active regions on them causing the brightness variations
and the large EUV emission The light curve do es show shifts of a few hundredths of a
magnitude in mean level from night to night likely due to di erential rotation or active
region evolution and could b e studied by further photometric observations
As a p ossible comparison star GSC was monitored but was found to vary
from night to night The di erential R magnitudes are given in Table The star was
at maximum brightness on approximately HJD and decreased in brightness at
m
roughly : p er day during our observations
The star GSC was also found to vary in brightness during a night Using
a p erio d nding routine based on that of Jurkevich our b est estimate is
cycles p er day Using the metho d of Kwee and Van Woerden Helio centric Julian
dates of primary minimum were found to b e and and times of
secondary minimum were and The precision
d
of the minima determinations were nominally : but this do es not include an
allowance for the asymmetry of the minima In Figure the data are plotted as a function
of phase according to the ephemeris
d d
HJD of Minima : : E
d d
: :
Figure Light curve of the di erential R data of GSC for
To help classify the two serendipitously discovered variable stars color information
was sought Unfortunately only a V frame and an I frame were obtained under non
photometric conditions While not de nitive they are indicative of the type of stars As
suming RE J has the V I of a normal K V Je ries then GSC is
has the color of approximately an early K star an extremely late M star and GSC
Therefore GSC is likely a long p erio d or irregular variable and GSC is
most likely an ellipsoidal or eclipsing binary and not a Delta Scuti type star The shap e of
the light curve small amplitude and di erence in maxima are consistent with a W UMa
star seen with a small inclination
Further photometric and sp ectroscopic observations will b e valuable to con rm our
conclusions as to the reason for the variability of these stars
R M ROBB
M D GLADDERS
Climenhaga Observatory
Dept of Physics and Astronomy
University of Victoria
Victoria BC CANADA V W P
Internet robb uvastro phys uvic ca
Internet gladders astro utoronto ca
References
Je ries R D MNRAS
Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ
Jurkevich I Ap Sp Sci
Kwee K K and Van Woerden H Bull Astr Inst Neth
Malina R F et al AJ
Pounds K A et al MNRAS
Robb R M and Honkanen N N in A S P Conf Ser Automated Telescopes
for Photometry and Imaging ed Adelman Dukes and Adelman
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER M
NGC M l b is a variable rich Oo IA cluster The cluster is
classi ed as CC IX concentration class and according to Kukarkin has a radius
0
R The list of stars in the Third Catalogue of Variable stars Sawyer Hogg
contains RR Lyrae variables with known p erio ds with no p erio d determinations
non variables and one red variable V The four variables V V V V
0 0
detected at larger distances R all have a p ositive X co ordinate Periods
have b een determined for the rst three and hence there are known RR Lyr variables
0
with R A comparison of the p osition of the stars on the repro duced plates with
the accompanying lists of Shapley Shapley and Ritchie and Sawyer Hogg
indicates that the X co ordinates of V and V should have an opp osite sign
i e minus and plus corresp ondingly These errors have not b een corrected in catalogue
of Sawyer Hogg
During the past years no further search had b een made for variable stars in this
cluster and no p erio ds were determined for V V V V V V V V
V In order to check the variability of the stars with unknown p erio ds and
search for as yet undetected variables the metho d prop osed and applied for M Kadla
Gerashchenko was used It is based on an analysis of a color magnitude diagram
obtained from measurements of two plates or CCD taken simultaneously A variable
is thus at identical phase and the RR Lyrae stars are lo cated in a de nite strip By
indicating the p ossible variables the diagram considerably narrows down the number of
stars which need further investigation
We had at our disp osal a pair of the necessary CCD B V exp osures obtained with the
cm Dutch telescop e at La Silla Details on the observations metho ds of reduction are
0
given in the pap er by Bro cato et al The eld includes stars with R in
the variable star list Sawyer Hogg Photo electric standards obtained by Dickens
were used to transform the instrumental magnitudes The resulting V B V
m m
diagram Figure includes stars in the magnitude range V the
known variable stars b eing denoted by an asterisk
The p ositions of V V and V on the color magnitude diagram indicate that they
b elong to the GB Of the four stars V V V and V lo cated in the vicinity of
the RHB stars only V has a known p erio d V is listed as a non variable and the last
0
two are most probably RHB stars It was di cult to identify the variables with R
found by Sawyer Hogg The repro duced plate of the cluster do es not have the
necessary quality and no known variables are marked although according to the listed
co ordinates V is lo cated close to the known variable V
The co ordinates V and B V of the susp ected variable stars in the RR Lyr variability
strip are given in Table Their p ositions were determined using as a reference frame the
co ordinates system given in the catalogue of Sawyer Hogg
Figure The color magnitude diagram for the globular cluster NGC The known
RR Lyrae stars are denoted by asterisks the stars from Table S circles R
pluses
Table Positions and photometric data for susp ected variables S and for p ossible
variable stars lo cated at the intersection with the RHB R
N X Y V B V N X Y V B V
arcsec arcsec arcsec arcsec
S R
S R
S R
S R
S R
S R
S R
S
S
Figure Chart of the cluster The notations V S and R preceding the star number
refer to known and susp ected Table variables
Figure The central part of NGC The notation are the same as in Figure
As the observed RR Lyrae instability strip slightly intersects the RHB there is a p ossi
bility that some of the latter stars are variable The co ordinates V and B V of the stars
which should b e checked are listed in Table The maps of NGC with known and
susp ected variable stars are shown in Figure and Figure co ordinates are in pixels
00
pixel Almost all the susp ected variables are lo cated in the central part of cluster
Z I KADLA
A N GERASHCHENKO
Yu N MALAKHOVA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia
e mail kadla pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A A Ap
Dickens R J MNRAS
Kadla Z I Gerashchenko A N Isv Main A O of the Academy of Sci of USSR
Pulkovo
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Sawyer Hogg H Comm David Dunlap Obs No
Sawyer Hogg H Publ David Dunlap Obs No
Shapley H Mt Wilson Contr No ApJ
Shapley H Ritchie M Mt Wilson Contr No ApJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
December
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER NGC
NGC M C l b is a variable p o or Oo II cluster
I I VP With F e H it is one of several clusters which lie in the metallicity
interval where alongside with I I VP there co exist I VR Oo I variable rich clusters The
m
cluster has an absolute magnitude M concentration class CC V apparent
v
o
0 0
radius r Kukarkin and limiting radius r Kukarkin Kireeva
The cluster was rst searched for variable stars by Rosino In the investigated
area he discovered ve variable stars three of which are eld variables with a distance
0
r from the cluster center The other two variables designated V and V at
0 0
r and resp ectively were noted by Rosino as RR and at the time of publication
of the Third Catalogue of Variable Stars in Globular Clusters Sawyer Hogg were
the only known variables assumed to b e cluster members
A further search for variables was made by Liller In the investigated eld she
discovered variables including the ve previously detected by Rosino Three of the
0 0 0
variables found by Liller with r and are within the limiting radius of the
cluster The estimated p erio ds for four of them excluding V enabled their classi cation
as RR Lyrae variables However according to the mean magnitude two of the latter
0 0
V and V renamed Rosino V at r and were found to have low probability
0
membership thus limiting the distance of the three cluster variables at r In Liller s
table there is a misprint in the signs of the X co ordinates of V and V which should
b e and resp ectively
Details of the CCD observations obtained with the m Dutch telescop e at ESO La
Silla metho ds of reduction are given in the pap er by Bro cato et al The metho d
of a search for as yet undiscovered variables was the same as in the companion pap er
Kadla et al The V and B magnitudes of the measured stars are based on
m
photo electric standards Landolt within the magnitude intervals V
m m m m m
and B B V CMD was obtained using
for the mean V and B magnitudes from V and B consecutive exp osures the time
di erence b etween the mean V and B magnitudes b eing minutes
The stars in the instability strip of the resulting CMD diagram are shown in Figure
The available photometric data exp osures V and B p ermitted to con rm
the variability of nine stars including the aforementioned two known RR Lyr variables
discovered by Rosino and Liller Data for these variables numbered op en circles
and other stars in the instability strip are given in Table and Figure Six stars Nos
triangles are probably variables but need further con rmation and three Nos
m
V are probably eld variables There are three stars Nos
asterisks in the instability strip which did not show any sign of variability in our data If
0
the variable V without a determined p erio d at r found by Liller is included there
are at present ten known RR Lyrae stars b elonging to the cluster
0 0
Figure The CMD for stars in an area centered on the cluster Concerning
notation of stars in the instability strip see the text
Figure Chart of the cluster showing the p osition stars in Table
Table Photometric data for variables
N X Y V B V N X Y V B V
arcsec arcsec arcsec arcsec
Financial supp ort from Russian Fund for Basic Research is gratefully acknowledged
Z I KADLA
A N GERASHCHENKO
Yu N MALAKHOVA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia e mail kadla pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Kadla Z I Gerashchenko A N Malakhova Yu N IBVS No
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Kukarkin B V Kireeva N N Astr Zh English transl Soviet Astr
Landolt A U AJ
Liller M AJ
Rosino L Mem Soc Astron Ital No
Sawyer Hogg H Publ David Dunlap Obs No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
ON NOVAE AND AND POSSIBLE NOVA IN M
Using plates obtained with the cm Maksutov telescop e of the Sternberg Astronomical
Institute Crimean Lab oratory we studied two novae in M discovered by Della Valle et
al These novae were also indep endently found on our plates
The co ordinates of the novae are the following
h m s 0 00
Nova No
h m s 0 00
Nova No
The B magnitudes of the novae based on the photo electric sequence Sandage and
Johnson are given in the table
Nova Nova
J D B J D B
Nova was seen on plates of Della Valle et al According to our data the nova
was bright on J D and so on b ecome fainter but it was still seen for ab out two
months
Nova was seen on a single plate of Della Valle et al This nova is now con rmed
on our plates though on J D it was appreciably fainter than according to Della
Valle et al m pg
In connection with the search for novae in M it is necessary to mention the star
B Humphreys and Sandage It was bright in V and fainter
than V in The star is absent on all known to us published photographs
of M since Keeler It is not seen on any of our nearly plates with
B taken in and on the plate with B as a part of Yu N
lim lim
Efremov s program at the m Russian telescop e in
It seems that the star B is a nova and a search for it on plates taken in if
they exist should b e desirable
A S SHAROV
Sternberg Astronomical Institute
Universitetskij Prosp
Moscow Russia
References
Della Valle M Rosino L Bianchini A and Livio M Astron Astrophys
Humphreys R M and Sandage A Astrophys J Suppl Ser
Keeler J E Publ Lick Obs Plate
Sandage A and Johnson H L Astrophys J
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
V Cen NEW TIMES OF MINIMA
AND A POSSIBLE SHORT PERIOD MODULATION
We present new photo electric hereafter p e minima of the very short p erio d red W
m
type W UMa star V Cen GSC V ' : Sp T ' K Other available
minima are the photographic ones hereafter pg from the discoverer Ho meister
and the photo electric ones by G omez and Lapasset hereafter GL and by Gray
et al a b hereafter GWS History a nder chart light curves and preliminary
elements can b e found in GWS The rst p erio d study of V Cen was made by Woo d
and Forbes
The observations rep orted here were made in and at Cerro Tololo Inter
American Observatory in Chile with the Lowell telescop e refrigerated phototub es stan
dard UBVRI lters and photon counting techniques GSC and GSC
HD K CoD were used as comparison and check stars resp ectively
The derived minima are listed in the lower part of Table The two minima corresp ond
ing to the season were determined through the Sliding Integral s Algorithm Ghedini
hereafter SIA while the minimum was determined by extrap olation using the
tracing pap er metho d Szafraniec With these minima we have extended the p e
baseline of minima from ab out in GWS to cycles
We made a least squares weighted parab olic solution taking into account all available
minima to derive an improved ephemeris and a p ossible p erio d variation Standard devi
d d d
ations for the pg minima : : and : were estimated from a linear solution
with equal weights for the p e minima we used those published by GWS and those from
the output of SIA The standard deviations of the minimum were estimated visually
d d d
while those from GL were estimated as the pg ones : : and : b ecause they
are lacking in the publication We have taken extreme care to reconcile the pg with the
p e minima The parab olic solution is
d d d
Min I HJD : : E : E
d d d
: : : m e
Residuals from this solution are lab eled O C in Table Those lab eled O C are
the residuals from the linear solution As can b e seen comparing the linear and parab olic
residuals or from the term that takes into account the total variation of the p erio d
is only marginally detectable We might conclude that the system remained stable along
the revolutions cycles covered by the available observations The b ehavior of the
O C residuals is depicted in Figure
1 Op erated by AURA Inc under co op erative agreement with the NSF
Table Times of minima and residuals for V Cen
HJD sigma
Ref Min Band E O C O C
I pg
II pg
I pg
I pg
II pg
II pg
I pg
II pg
I pg
II pg
I pg
II pg
I pg
II pg
I pg
I pg
II pg
I pg
I pg
I pg
II pg
II pg
I pg
I pg
II pg
I pg
I pg
II pg
II pg
I pg
I pg
II pg
I pg
II pg
I pg
II pg
II pg
I pg
II pg
I pg
II pg
I pg
I pg
II pg
II pg
II pg
I pg
II pg
I pg
II pg
II pg
I pg
I pg
II pg
II pg
I pg
II pg
Table cont
HJD sigma
Ref Min Band E O C O C
I pg
II pg
II pg
I pg
I pg
II pg
II pg
I pg
II pg
I pg
II pg
I pg
II pg
I pg
I pg
II pg
II pg
II pg
I pg
I pg
II pg
I pg
I pg
II pg
II pg
I pg
I U
I B
I V
I U
I B
I V
II p e
II p e
II p e
I p e
I p e
I p e
II p e
II p e
II p e
II p e
II p e
II p e
II p e
II p e
II p e
I p e
I p e
II p e
II p e
I BVRI
I BVRI
I V
I R
I I
References Ho meister minima GL minima GWS minima minimum
Figure Behavior of the O C residuals for V Cen from Formula Hollow circles
stand for primary minima
As can b e seen in the p e residuals of Figure there app ears to b e a mo dulation of
d
semi amplitude of : and a p erio d of ab out years This might b e explained on one
hand by a third b o dy light time e ect Mayer On the other hand as noted in
GWS the O Connell e ect present in their light curves at phase is interchanged in
GL phase so some mechanism in particular related to magnetic activity in this
late type star might b e resp onsible for the p erio d mo dulation van t Veer Applegate
However due to the scanty material analyzed here new p e times of minima will
only give a conclusive answer ab out this p oint The author would like to thank the sta
and Director of CTIO for their hospitality
Miguel Angel CERRUTI
I A F E
CC Suc
Buenos Aires
Argentina
miguelan iafe uba ar
References
Applegate J H Astrophys J
Ghedini S Mem Soc astr Ital SIA
G omezM Lapasset E Inf Bul l Var Stars No GL
Gray J D Woissol S Samec R G a Inf Bul l Var Stars No GWS
Gray J D Woissol S Samec R G b Inf Bul l Var Stars No ERRATUM
Ho meister C Ver o Sonneberg Part
Mayer P Bul l Astron Inst Czechosl
Szafraniec R Acta Astron Serie c
van t Veer F Astron Astrophys
Woo d D B Forbes J E Astron J
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
A REVISION OF DOLIDZE S
LIST OF PROBABLE LONG PERIOD VARIABLES OF M TYPES
The following table constitutes a revision of the star list app earing in an obscure pap er
by Dolidze concerning sp ectral p eculiarities of M stars and the p ossibility of using
these to predict the type of variability I b ecame interested in using the list to get visible
light identi cations and sp ectral types for IRAS sources The original publication includes
a list of sp ectral types determined on red light ob jective prism plates for stars plus
seven supplemental stars Ab out half of these were known or susp ected variables but the
remaining probable variables app ear to have b een observed for the rst time at least
for sp ectral type
A large number of errors were found in the pap er so a complete revision seemed
necessary in order to make the IRAS identi cations In particular the p ositions supplied
0
by Dolidze are commonly in error by or more Luckily nder charts from ob jective
prism plates are shown for each star which were necessarily relied up on to identify them I
was able to match these with digitized sky survey images in all but two cases The revised
list provides precise p ositions for the remainder with identi cations from the IRAS and
Guide Star Catalogues where p ossible plus links with other names available through the
SIMBAD database For many of the known variables precise p ositions are provided for
the rst time among which are substantial corrections to the GCVS Kholop ov et al
The pro cedure was simply to compare Dolidze s nder charts against the digitized sky
survey using the Go ddard SkyView facility McGlynn et al Scollick and
0
SIMBAD The original charts cover square Matching star elds was usually unam
biguous I then did searches in SIMBAD around the p osition estimated from SkyView for
IRAS sources and other previously published names as well as GSC p ositions For stars
with large Dolidze p osition errors often the reverse pro cedure proved successful calling
up SkyView images centered on various IRAS sources near the nominal lo cation When
a GSC identi cation was made its p osition was adopted Positions for stars missing
from the GSC were taken most often from the U S Naval Observatory UJ or A
catalogues Monet et al Monet although in a few cases I derived them from
SkyView frames at large image scale
The table shows Dolidze s designation from his Tables and in the rst column
followed by the equinox p osition the co ded source of the p osition A A G
GSC P PPM S SkyView U U and IRAS and GSC numbers as available
The sp ectral types are from Dolidze b eing mean values if types were determined on more
than one plate The types were assigned usually only in o dd numbered increments M
M M etc but with many intermediate values e g M I have taken this to
mean the types are not highly accurate although comparison with other published values
suggests there are neither gross systematic errors nor much scatter in the types esp ecially
considering that all the stars are surely variable and observed at random phases
Table
D RA Dec s IRAS GSC sp ec Remarks
p G C
p G C
p G M S
p A M S S
p A C CGCS
p G M S
p U dM e
G M V Cas
U M V Cas
G M
G M
G M
G M SC V Cas
G M NSV
G M
G M BL Cas
G M AP Cet
G M R Per
G M AP Per
G M
G M
G M TX Tau
G M
G M see note
G M
G M S NSV
G M V Tau
G M
G M EE Aur
G M
G M
G M W Aur
G M V Ori
U M
A M AW Aur PEP
A M RU Aur
G M V Ori
G M AZ Tau
G M DT Ori
G M
A M see note
G M
G M
A M
G M V Gem
G M
G M T CMi
G M CLS
G M
G M BK Sco
A M
G M NSV
A M
U M see note
G M
G M UV Sco
G M
A M UZ Sco
G M
G M VW Sco
Table cont
D RA Dec s IRAS GSC sp ec Remarks
A M VY Sco
A M
G M NSV
G M Y Sco
A M see note
A M FK Sgr
G M EK Her see note
A M VV Sgr
G M BE Ser
A M
G M PS Her
G M FL Her
G M
A M
A M
G M FR Sct
G M
G M V Sgr
A M
G M
G M CZ Dra StM
G M T Ser
A M V Sgr
G M
G M BP Ser
G M BI Oph
A M S TY Oph see note
G M VW Sct
A M
G M
G M V Oph
G M V Oph
G M BK Oph
G M BR Ser
A M
G M
G M AN Lyr
G M
G M
A M V Lyr
U M
A M
U M
G M M e
G M V Cyg
G M M e IRC
G M
G M
U M IRC
A M
G M KZ Cyg
A M V Cyg
G M EN Vul
G M V Cyg
U M
U M V Cyg
G M
A M
G M
Table cont
D RA Dec s IRAS GSC sp ec Remarks
G M
G M
G M
G M UW Vul
G M
U M UX Cyg
G M V Cyg
G M
G M
G M LD
G M LD
G M
G M V Cyg
G M IRC
U M V Cyg see note
M see note
G M M
S M
U M V Cyg
G M IRC
G M
G M IRC
G M
G M V Cyg
G M
G M
G M V Cyg
G M
M see note
G M
U M
G M
A M
A M
G M GN Cep IRC
G M TT Cep
G M
G M
G M NSV
G M NV Lac
G M
G M
P M R Lac
G M LD
G M
G M
G M AL Cep
G M
G M NSV
G M
G M V Cas
U M
G M same as
G M IRC
G M same as
G M
G M CH Cep
P M V Cas
U M OQ Cep
Table cont
D RA Dec s IRAS GSC sp ec Remarks
U M V Cas
A M
U M
G M
U M NSV
U M
U M
G M
G M
G M DG Cas
G M V Cas
G M
S M
A M
A M Z Cas
G M RT Cas
U M IRC EM Cas
G M
G M
G M V Cas
Notes
CGCS however not a carb on star cf Bidelman
ID somewhat uncertain p osition is for brightest DSS image
s 0 00
ID somewhat uncertain alternate star NW has end gures :
Dolidze Dec error
also GSC
HD CGCS this is surely a carb on star Dolidze type wrong
chart identical to
can t identify on sky Dolidze p osition given
can t identify on sky Dolidze p osition given
For intermediate types and in taking averages I have adopted the notation of Houk see
for example Houk Cowley which uses a slash e g M to indicate uncertainty
rather than a truly intermediate sp ectral class Note several cases where Dolidze found
indications of carb on star or S type characteristics e g M S
The remarks and notes show additional identi cations from SIMBAD particularly
variable star names In several cases Dolidze has given incorrect variable star designa
tions which are herewith corrected
I appreciate the help of William P Bidelman in making a number of identi cations from
his bibliographic le Two on line facilities were indisp ensable for this work SIMBAD
maintained by the Centre de Donn ees Astronomique Strasb ourg France and SkyView
maintained by Keith Scollick of the Go ddard Space Flight Center This work was b egun
during a stay at the CDS Strasb ourg I gratefully acknowledge the assistance of the sta
there
Brian A SKIFF
Lowell Observatory
West Mars Hill Road
Flagsta AZ
USA
e mail bas lowell edu
References
Bidelman W P Publ Warner Swasey Obs
Dolidze M V Byul l Abastuman Astro z Obs
Houk N and Cowley A P University of Michigan Catalogue of Two Dimensional
Spectral Types for the HD Stars Univ of Michigan Ann Arb or
Kholop ov P N editor et al General Catalogue of Variable Stars th edition
Nauka Moscow
McGlynn T A White N E and Scollick K Bul l Amer Astr Soc
abstract
Monet D Canzian B and Henden A Bul l Amer Astr Soc ab
stract
Monet D G Bul l Amer Astr Soc abstract
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER NGC
NGC C l b is a cluster of intermediate metallicity
as it follows from its sp ectral class F Hesser Shawl although a wide range
of its values was quoted in the literature from Samus et al to
0
Bro cato et al It has the apparent radius r Kukarkin the tidal
0
radius r Webbink and the concentration class CC V
According to the data published in A Third Catalogue of Variable Stars in Globular
Clusters SHC Sawyer Hogg and later investigation by Fourcade et al
and Liller Richten altogether variables have b een discovered within the ap
parent radius of this cluster Ten of these stars are classi ed as RRAB and six as RRC
With Pab and Nc Nab the cluster is classi ed as OoI I variable po or I IVP
The observational material and the metho d of search for variable stars are the same
as in our previous pap ers Kadla et al a b CMD was obtained as in Kadla et
al b using the mean V and B magnitudes from several consecutive V and B
0 0 0
exp osures CMD for stars with R within the investigated area is shown
in Figure In the instability strip b esides of the ab ove variables there are stars
which may b e RR Lyr variables The data for the latter stars are given in Table Their
p ositions were determined using as the reference frame the co ordinates system given in
the catalogue of Sawyer Hogg Our photometric data exp osures V and
B p ermitted to con rm the variability of short p erio d variable stars and detect
variability for susp ected variables N and N from Table All variables known and
susp ected are shown in the cluster chart Figure
Figure The color magnitude diagram for the globular cluster NGC The known RR Lyrae
stars are denoted by susp ected ones by
Figure Chart of the cluster Variable stars are denoted by The notations V preceding the star
number refer to known variables
Table Positions and photometric data for susp ected variable stars
N X Y V B V N X Y V B V
arcsec arcsec arcsec arcsec
We are grateful to the Russian Foundation for Basic Research for nancial supp ort
A N GERASHCHENKO
Z I KADLA
Yu N MALAKHOVA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia e mail mal pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Fourcade C R Lab orde J R Puch A A Arias J C Peremennye Zvezdy Vari
able Stars in Russian
Hesser J E Shawl S J PASP
Kadla Z I Gerashchenko A N Malakhova Yu N a IBVS No
Kadla Z I Gerashchenko A N Malakhova Yu N b IBVS No
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Liller M H Lichten S M AJ
Sawyer Hogg H Publ David Dunlap Obs No
Samus N Ipatov A Smirnov O Kravtsov V Alcaino G Liller W Alvarado F
A AS
Webbink R F IAU Symp osium No eds by J Go o dman P Hut Reidel Dordrecht
CORRIGENDA
Correction to IBVS No In order to bring to accordance Table and Figure it is
necessary to interchange star s Nos and in Table and to attribute No to that one of two
stars with number in Figure that has co ordinates Xpixel and Ypixel Y Malakhova
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
UBV RI PHOTOMETRY OF THE RAPIDLY ROTATING
c
1
K TYPE STAR HD SPEEDY MIC
HD SAO CPD RE J was found to b e a
very strong EUV and X ray source during the ROSAT all sky survey with most of the
emission due to a very intense are event Bromage et al Matthews et al
K urster Optical sp ectroscopy has revealed that the star is single and shows Ca I I
H K emission a very strong Li I A line and a highly variable H pro le Bromage et
al Je ries From the vsin i value of km s and optical photometry
it was immediately clear that HD was an extremely fast rotator and it was indeed
nicknamed Speedy Mic Bromage et al So far HD is the most rapidly
rotating nearby single late type star known
A V band photometric study was presented by Anders et al which from a
total of observations over three nights in August September inferred photometric
p erio ds of and days They present the whole data set by using the day
p erio d that however pro duce a quite scattered light curve see Figure in Anders et
al They also computed a vsin i value of km s from the analysis of the
Li A and Ca A lines and estimated a K sp ectral type
In order to further investigate on the rotational p erio d of HD multicolor pho
tometric observations were carried out over the interval Octob er by using the
m ESO telescop e La Silla Chile equipp ed with a single channel photon counting
photometer a thermo electrically co oled R Hamamatzu photomultiplier and stan
dard ESO lters matching the UBV RI system Accurate di erential photometry was
c
obtained with resp ect to HD and SAO that were used as comparison and
check stars resp ectively The observations were corrected for atmospheric extinction and
transformed to the standard UBV RI system Details on the observations and reduc
c
tion pro cedures can b e found in Cutisp oto The typical error of our di erential
photometry is of the order of magnitudes We have also obtained the following V
magnitude and colors for the comparison and check stars
HD V B V U B V R V I
c c
SAO V B V U B V R V I
c c
The errors on these values are of the order of magnitudes
We have collected a total of UBV RI photometric observations of HD that
c
have b een analyzed according to the metho d presented by Scargle which is es
sentially a Fast Fourier Transform adapted for unequally spaced data The highest p eak
in the p erio dogram F corresp onds to a photometric p erio d of days i e
hours see Figure There is a second signi cant frequency F in the
p erio dogram that corresp onds to a p erio d of days
1 based on data collected at the Europ ean Southern Observatory La Silla Chile
0.02
F1 1b
0.015
1a significance level = 99.99% F2 2b 1c 0.01 2c
2a 2d 0.005 1d
0
2 4 6 8 10
Figure The p erio dogram obtained for HD The highest p eak F corresp onds to a day
p erio d the a b c and d p eaks are aliases of the F p erio d A second frequency F corresp onding to a day p erio d and its aliases a b c and d are also visible
9.25 V 9.30
9.35
9.40
9.45 0.50 U-B
0.55
0.60
0.90 B-V
0.95
1.00
0.50 V-R
0.55
0.60
1.05 V-I
1.10
1.15
0 0.5 1
Figure V band light curve and colors of HD obtained over the time interval Octob er
Phases are reckoned from the photometric ephemeris HJD E
The resulting V band light curve with a p eak to p eak amplitude of ab out mag
nitudes is shown in Figure along with color variations that app ear in phase with the
V band mo dulation Phases are reckoned from the photometric ephemeris
HJD E
The day p erio d pro duces a rather scattered light curve Our light curve folded
with the day p erio d has a smaller amplitude with resp ect to the Anders et al
data and presents a maximum and a minimum luminosity that are ab out and
magnitudes brighter resp ectively We also note that folding the Anders et al
data with our day p erio d a light curve much less scattered than the original one is
obtained
The B V and V R colors of HD are consistent with those of a K V star
c
while the U B and the V I app ears to o blue and to o red resp ectively for such a
c
classi cation These di erences could b e due to a very high activity level to the fact that
HD has not yet arrived on the main sequence or to b oth circumstances However
from the vsin i value computed by Anders et al and our new photometric p erio d
the minimum stellar radius falls in the range R thus supp orting the hypothesis
that HD is a pre main sequence star Anders et al
Acknowledgements Financial supp ort by the Italian Ministry for Universities and
Research MURST and the National Research Council Grupp o Nazionale di As
tronomia is gratefully acknowledged MK acknowledges supp ort by the Austrian Fond
zur F orderung der wissenschaftlichen Forschung under grant S AST
G CUTISPOTO
M KURSTER
I PAGANO
M RODONO
1
Osservatorio Astro sico di Catania v le A Doria I Catania Italy
e mail gcutisp oto alpha ct astro it
2
Institut f urAstronomie Universit atWien A Wien Austria
3
Max Planck Institut f urextraterrestrische Physik Giessenbachstrasse D
Garching Germany
4
Istituto di Astronomia Univ degli Studi v le A Doria I Catania Italy
References
Anders G J Je ries R D Kellett B J Coates D W MNRAS
Bromage G E Kellett B J Je ries R D et al in th Cambridge Workshop
on Cool Stars Stel lar Systems and the Sun M S Giampapa J A Bo okbinder
eds ASP Conf Ser Vol p
Cutisp oto G A AS
Je ries R D MNRAS
K urster M in Proceedings of the IAU Col loquium Flares and Flashes Son
neb erg December J Greiner H W Duerb eck R E Gershberg eds
Lecture Notes in Physics Series Springer Verlag Vol p
Matthews L Bromage G E Kellett B J et al MNRAS
Scargle J D ApJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
NSV MINOR PLANET SULEIKA
In the New Catalogue of Suspected Variable Stars Kholop ov et al it is suggested
that NSV is a minor planet An investigation by the current author shows that
NSV is the minor planet Suleika
The original rep ort of NSV is by Innes a who lo cated the ob ject numbered
in his list during a survey of variable stars near R Coronae Austrinae Innes
app ears only on a single minute plate taken by H E Woo d on Aug where it
is recorded as b eing magnitude Further details are given in Innes b where it
is stated that the sole image is a go o d stellar image It is here that the remark Is only
image found Minor pl app ears
An addendum to the initial rep ort remarks that a further plate a minute exp osure
by Woo d on Aug had b ecome available and that comparison of this plate and
the plate of Aug proved that three of the ob jects identi ed initially as variable stars
were actually minor planets Innes a made identi cations as follows Innes
Calliop e Metis and Tirza The rst two identi cations are
con rmed as correct but Innes is in reality Vala
Table Minor Planet Candidates Rep orted by Innes
Innes No R A Dec Equinox Ref MP No
h m s 0 00
Woo d
Innes a
Woo d
Woo d
Table J Co ordinates for Minor Planet Candidates
Innes No R A Dec MP No
h m s 0 00
Table Predicted Minor Planet Positions and V Magnitudes
MP No R A Dec V Innes No
h m s 0 00 m
The time of exp osure of the Aug plate was not given by Innes Woo d later
rep orted precise measurements of the three recognised minor planets from b oth the Aug
and plates rep eating the misidenti cation of as and giving the times of
mid exp osure as Aug UT and Aug UT
Table gives the original equinox measurements for the four Innes ob jects that are
minor planets Table lists the corresp onding J co ordinates Table lists the
predicted J minor planet co ordinates and visual magnitudes for Aug
UT
Gareth V WILLIAMS
Harvard Smithsonian Center for
Astrophysics
Garden Street
Cambridge MA
U S A
E mail gwilliams cfa harvard edu
References
Innes R T A a Union Obs Circ No
Innes R T A b Union Obs Circ No
Kholop ov P N et al New Catalogue of Suspected Variable Stars Moscow Nauka
Publishing House
Woo d H E Union Obs Circ No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
PHOTOELECTRIC BVI OBSERVATIONS AND A NEW CLASSIFICATION
C
FOR V ARAE
V Ara was included in our program of photo electric observations for Cepheids b ecause
it is classi ed in GCVS IV as a p ossible Cepheid We observed the star at CTIO during
the p erio d September November using the m re ector A total of BVI
c
measurements were obtained Table the accuracy of the individual data b eing near
m
in all lters
Our observations are plotted in Figure The data indicate a range of light variability
m m m
of in V in B V and in V I but the star cannot b e a Cepheid b ecause
c
rst changes in B V color are asynchronous with the changes in V which is atypical
of Cepheids and second it has a very large infrared excess It seems more likely that
V Ara is a semiregular variable
Table
JD V B V V I JD V B V V I
hel c hel c
V V804 Ara 13.0
13.4 B-V 1.5 1.7 V-I C 3.3 3.5
2450360 50380 JD
Figure
The research describ ed here was made p ossible in part by grants No and
No from the Russian Foundation of Basic Research to LNB and through
NSERC Canada to DGT The authors were Visiting Astronomers at Cerro Tololo Inter
American Observatory National Optical Astronomy Observatories which is op erated
by the Asso ciation of Universities for Research in Astronomy Inc AURA under co
op erative agreement with the National Science Foundation
L N BERDNIKOV
Sternberg Astronomical Institute
Universitetskij prosp
Moscow Russia
D G TURNER
Saint Mary s University
Halifax Nova Scotia B H C Canada
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
PHOTOELECTRIC BVI OBSERVATIONS
c
FOR THE RS CVn STAR GR NORMAE
GR Nor is classi ed in GCVS IV as a Cepheid CEP type with the elements
M axJ D E
hel
GR Nor was included in our program of photo electric observations for Cepheids b ecause
there are few published observations for the star and hence it is imp ossible to construct
a go o d light curve for it We observed the star at CTIO during the p erio d September
November using the m re ector A total of BVI measurements were obtained
c
m
Table the accuracy of the individual data b eing near for all lters
The observations are plotted in Figure a using the ab ove elements A comparison
of our observations with published data by Walraven et al Harris and
Diethelm Figures b d suggests that GR Nor cannot b e a Cepheid b ecause
the shap e of the light curve is not stable A search of the literature revealed that Lloyd
Evans had previously drawn attention to the sp ectroscopic p eculiarities of the
variable which suggest that it has characteristics of RS CVn variables
Table
JD V B V V I JD V B V V I
hel c hel c
The research describ ed here was made p ossible in part by grants No from the
Russian Foundation of Basic Research to LNB and through NSERC Canada to DGT The
authors were Visiting Astronomers at Cerro Tololo Inter American Observatory National
Optical Astronomy Observatories which is op erated by the Asso ciation of Universities for
Research in Astronomy Inc AURA under co op erative agreement with the National Science Foundation V a. JD 2450348-89 12.6 12.8 B-V 1.2 1.4 V-I C 1.5 1.7 0.0 0.5 1.0 V b. JD 2434567-979 12.3 12.5 B-V 1.2 1.4 0.0 0.5 1.0 V c. JD 2443694-4146 12.5
13.0
0.0 0.5 1.0 V d. JD 2445540-51 12.4 12.6 B-V 1.4 1.6
0.0 0.5 1.0 Phase
Figure
L N BERDNIKOV
Sternberg Astronomical Institute
Universitetskij prosp
Moscow Russia
D G TURNER
Saint Mary s University
Halifax Nova Scotia B H C
Canada
References
Diethelm R Astron Astrophys Suppl
Harris H C Ph D Thesis University of Washington Seattle
Lloyd Evans T Observatory
Walraven Th Muller A B Oosterho P Th B A N
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
NSV A DETACHED ECLIPSING BINARY STAR IN ORION
The variability of NSV HD GSC SVS CSV was
rst rep orted by Parenago In the NSV catalogue Kholop ov this ob ject is
recorded as an eclipsing binary star without sp ecifying type with a photographic variation
m m
range from : to : and sp ectral type G
NSV was observed for nights in the V band from Octob er to Febru
ary from Mollet Observatory Spain using a CCD camera and a m telescop e
GSC and GSC were used resp ectively as comparison and check stars
To determine the magnitude and B V color index of NSV and its comparison star
these ob jects were also observed in the B and V bands using a photo electric photometer
attached to the Cassegrain fo cus of the m telescop e at Esteve Duran Observatory As
comparison stars HR HR and HR were used
Observations showed that NSV is in fact a detached eclipsing binary star with
a p erio d over days Figure This ob ject has a V magnitude of at
m m m m
maximum light The amplitude also in V is : : for minimum I and : :
for minimum I I Phase curve suggests that the primary minimum with a duration of
hours is an annular transit It also shows that minimum II is centered at phase
which indicates eccentric orbits for the comp onents Nevertheless the long duration
of eclipses and continuous bad weather conditions during the observation p erio d did not
allow to con rm these preliminary results Figure
To check p ossible B V color index variations observations in the B and V bands
were also p erformed for nights from Octob er to January which sampled
the light curve at the primary and secondary minima and at maximum light These
m m
observations indicate that the B V color index has a value of : : with no
detectable variations b eyond data scatter
The following ephemeris was also derived
d
Min I HJD : E
Although observations are not go o d enough to t an accurate physical mo del for the
binary system they allowed to estimate the relative dimensions and luminosities of b oth
comp onents These estimates indicate that the secondary star might b e a K ob ject of
smaller size than the primary comp onent New sp ectroscopic and more photometric data
are needed to clarify the exact nature of this system
J M GOMEZ FORRELLAD
E GARCIA MELENDO
Grup d Estudis Astronomics
Esteve Duran Observatory
Apartado
El Montanya Seva
Barcelona
Seva Barcelona
Spain
Spain
e mail jmgomez astro gea cesca es
e mail duranobs astro gea cesca es
References
Kholop ov P N New Catalogue of Susp ected Variable Stars Moscow
Parenago P P PZ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
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January
HU ISSN
NSV IS AN OVERCONTACT BINARY SYSTEM IN PISCES
NSV HV CSV P GSC was announced as a p os
sible RR Lyrae type star by Shapley and Hughes According to Kholop ov
it varies from the to photographic magnitudes without giving other data ab out
its variability
In order to have more information ab out this star NSV was included in the
program of the Grup d Estudis Astronomics for the identi cation and characterization of
new variable stars The ob ject was observed for nights b etween Octob er and
December at Monegrillo Observatory Spain A CCD camera equipp ed with B
and V lters was used attached to the m telescop e BD GSC
and GSC were used as comparison and check stars resp ectively To have an
indication of its magnitude in the B and V bands the comparison star was also observed
with a photo electric photometer coupled to the Cassegrain fo cus of the m telescop e
at Esteve Duran Observatory
Figure
These observations allowed to determine that NSV is not an RR Lyrae but an
overcontact eclipsing binary star with an amplitude of magnitudes at Min I
m m m
in the V band of : : in B and magnitudes at Min II :
m
: in B At maximum light NSV is a magnitude ob ject in the V
m m
band : : in B Figure shows the phase curve of NSV in the V band
The following ephemeris has b een computed for the system
d
Min I HJD : E
E GARCIA MELENDO
J VIDAL SAINZ
Esteve Duran Observator
J M GOMEZ FORRELLAD
El Montanya Seva
Grup d Estudis Astronomics
Seva Barcelona
Apartado
Spain
Barcelona
e mail duranobs astro gea cesca es
Spain
e mail vidal astro gea cesca es
jmgomez astro gea cesca es
References
Kholop ov P N editor New Catalogue of Susp ected Variable Stars Moscow
Shapley H Hughes E M HA No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
NSV A POSSIBLE SEMIREGULAR VARIABLE IN HERCULES
NSV BD CSV BV GSC was announced as
a variable star by Strohmeier and Knigge who indicated that it presented rapid
variations b etween the and photographic magnitudes Its sp ectrum is K and
the Guide Star Catalog records this star with photovisual magnitude of
PAL V lter
The star was observed for nights in the V band b etween May and December
from Els Hostalets de Pierola Observatory Spain with a CCD camera attached
to a m telescop e Some observations with the m Schmidt Cassegrain telescop e at
Piera Observatory Spain were also carried out As comparison star GSC was
used
During the observation interval NSV varied with an amplitude of magni
tudes in V showing successive maxima and minima Figure An analysis of the data
suggests that it could b e a semiregular star with a cycle of ab out days Nevertheless
more observations are necessary to con rm this preliminary result
Figure
J JUAN SAMSO
J GUARRO FLO
Grup d Estudis Astronomics
Apartado
Barcelona
Spain
e mail gea astro gea cesca es
Reference
Strohmeier W Knigge R Bamberg Ver o No
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Number
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January
HU ISSN
A NEW BETA LYRAE VARIABLE SAO AND TWO NEW
POSSIBLE IRREGULAR STARS BD AND SAO
SAO HD PPM BD AGK GSC
with a sp ectral type A is one of the variables discovered with the TYCHO
instrument of the Europ ean satellite HIPPARCOS Its light variation was announced by
Makarov et al indicating that its raw magnitude uctuated b etween and
without giving any further information
From November SAO was visually monitored by one of us to obtain
more information ab out this ob ject These preliminary observations indicated that it
might b e a Beta Lyrae type eclipsing binary star with a p erio d close to days This
star was subsequently observed in the V band from July to December
using a CCD camera and a cm nder telescop e from Mollet del Valles Observatory
and Esteve Duran Observatory Spain As comparison stars SAO SAO
SAO and GSC were used Photometric observations were also p erformed
using a photo electric photometer attached to the Cassegrain fo cus of the m telescop e
at Esteve Duran Observatory
Our CCD observations show that SAO is a Beta Lyrae type eclipsing binary
star Its light curve Figure shows a conspicuous O Connell e ect O Connell
that amounts to m Max I I Max I magnitudes where Max II is the maximum
following secondary minimum According to photometric measurements SAO is a
magnitude ob ject at Max I In addition the star fades magnitudes at
primary minimum and at secondary minimum The following ephemeris was also
computed
d
HJD Min I : E
Figure
Figure
Figure
Photometric reductions also showed that the star BD PPM
AGK GSC with a sp ectral type M is also variable During
m
the observation p erio d BD underwent light changes in the V band b etween :
m
and : Figure Its light curve indicates that it is probably irregular although more
photometric observations should b e p erformed to ascertain its exact nature
Furthermore the star SAO HD PPM BD
AGK GSC with a V magnitude of and sp ectral type K was
used as a check star Photometric reduction suggests that this ob ject is slightly variable
with a maximum observed amplitude of magnitude Figure depicts the mean mag
nitude of SAO for every night and also the mean magnitude of SAO C
with resp ect to SAO C Variability of SAO is probably real and not due
to di erential color extinction the comparison star SAO is also a K sp ectral type
ob ject but shows no detectable light variations b eyond light curve scatter However more
photometric observations should b e p erformed to con rm the variability of SAO
F CAMPOS CUCARELLA
E GARCIA MELENDO
J M GOMEZ FORRELLAD
Esteve Duran Observatory
Grup d Estudis Astronomics
El Montanya Seva
Apartado
Seva Barcelona
Barcelona
Spain
Spain
e mail duranobs astro gea cesca es
e mail jmgomez astro gea cesca es
References
Makarov V Bastian U Ho eg E Grossmann V and Wicenec A IBVS No
O Connell D M K Riverview Pub
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
NSV A NEW OVERCONTACT ECLIPSING BINARY SYSTEM
IN TRIANGULUM
NSV Wr CSV GSC was announced as a p ossi
m
ble Cepheid by Weber with a photographic magnitude variation from : to
m
: without giving any further information To check it the star was included in the
program of the Grup d Estudis Astronomics for observing p o orly studied variables An
initial monitoring with the m telescop e at Mollet del Valles Observatory showed that
NSV is not a Cepheid but an overcontact eclipsing binary system It was then de
cided to follow this ob ject with the m telescop e at L Ametlla del Valles Observatory
Spain NSV was observed for nights b etween September and December
GSC and GSC were used as comparison and check stars resp ec
tively The Guide Star Catalog records GSC NSV with a photovisual
magnitude of PAL V lter Figure
Observations obtained in the V band with a CCD camera con rmed our preliminary
data in the sense that NSV is an overcontact eclipsing binary system with a p erio d
close to hours minutes Figure The amplitude of the light variation is
magnitude at minimum I which is a transit and magnitude at minimum I I
which is an o ccultation The following ephemeris has b een computed
d
Min I HJD : E
J M GOMEZ FORRELLAD
A GARRIGOS SANCHEZ
Grup d Estudis Astronomics
Apartado
Barcelona
Spain
e mail jmgomez astro gea cesca es
Reference
Weber R IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
ACTIVITY OF T CORONAE BOREALIS IN
T CrB is one of b est studied recurrent novae having undergone ma jor eruptions in
and At quiescence it is classi ed as a symbiotic binary with an M giant
co ol comp onent Kenyon and references therein The most uncertain parameters
of the system are the masses of b oth comp onents Most of the published orbital solutions
e g Kraft Kenyon Garcia prefer the hot comp onent less massive than
the M giant but larger than the Chandrasekhar limit This leads to mo dels with rapidly
increasing mass transfer onto a main sequence star as the reason of the nova like outbursts
e g Webbink Cannizzo Kenyon However the UV data e g Selvelli et al
and o ccasionally demonstrated ickering activity in the optical see Dobrzycka et
al and references therein are more easily interpreted if the giant has a white dwarf
companion Recently Miko lajewski et al suggested that T CrB may b elong to
the sub class propellers of symbiotic binaries in which a massive magnetic and rapidly
rotating white dwarf accretes matter from the M giant s wind
Photo electric observations were carried out using the one channel UBVRI photometer
m
with the cm telescop e at Toru n observatory The stars HD V U B
m m m m m
B V V R V I and HD V U B
m m m m
B V V R V I were used as the comparison and the
m
check resp ectively However the rst one seems to b e a low amplitude less than
d
variable UBVRI light curves covering more than one orbital p erio d P are shown
in Figure The o ccasional one to three hours searches for rapid variability are marked
in Figure as lled triangles for p ositive detection or op en ones for negative detection
m m m
During three nights we observed a ickering with amplitude and in U
and B resp ectively During the two remaining runs a p ossible amplitude was less than
m m
in b oth lters No ickering with an amplitude larger than was observed in the
VRI bands
Sp ectral observations of the H region were carried out with a CCD camera mounted
in the coud e spectrograph of the m telescop e at NAO Rozhen The resolution is A
and the S N ratio in the continuum around H The ep o chs of observations are
marked in Figure and the pro les are shown in Figure
Iijima noted that b etween dramatic nova like outbursts T CrB exhibits two
states a high one when the emission lines H I He I and the hot continuum are rela
tively strong and a low one when they almost disapp ear The last increase of Balmer
emission lines as well as the He I I app earance was noted by Iijima in April July
and over the ve last years T CrB seems to remain in a low state The Slovak photometric
campaign see Skopal et al and references therein for previous rep orts shows a very
low level of U and B brightness and it excludes the presence of a blue continuum dur
ing this p erio d Anupama and Prabhu rep orted measurements of H equivalent
widths that remain b elow A after the high state in when they were larger
than A H is also very weak in June Ivison et al
Figure T CrB UBVRI light curves in Estimations derived from ickering runs are marked by
open and l led triangles for negative and p ositive detection resp ectively The ep o chs of the H
observations are marked by arrows in the U light b ox The orbital phases from sp ectroscopic
conjunction M giant in front are taken from Kenyon Garcia
In the b eginning of April we observed a rapid increase in U light Figure by
m
ab out Simultaneously ickering variations with time scales from a few minutes to
m m
half an hour and amplitudes of ab out in U and in B app eared whereas three
weeks earlier they were not detected Afterwards the U magnitudes changed with an
m
amplitude up to and time scale months but until the end of our observations
m
remained at least ab ove the level of the low state in March The VRI light
curves exhibit only the well known e g Bailey ellipsoidal variations of the M
giant with two distinct minima at sp ectroscopic conjunctions The domination of the M
giant in VRI is con rmed by the lack of ickering variations in these wavelengths The B
magnitudes in Figure re ect b oth the rotation of the M giant and the hot comp onent activity
Figure T CrB H pro les in The equivalent width and orbital phase are written in each b ox
Until now there is no observational evidence that T CrB is an eclipsing binary Kenyon
and Garcia mentioned that the ellipsoidal variations suggest a large orbital incli
nation and that several minima in the emission line uxes and the total UV ux o ccurred
close to phase Our data seemingly do not supp ort this p oint of view Just after phase
Figure the U magnitudes are close to the maximal value which we observed over
the whole p erio d and pronounced ickering variability is present as well Nevertheless
m
b etween phases and a deep minimum is evidently visible in U light Moreover
we did not detect ickering variations during this minimum The minimum lo oks like
an eclipse of the hot comp onent by the M giant which almost lls its Ro che lob e On
the other hand it is very similar to the previous two minima o ccurring typically for
months variability Additionally the sp ectroscopic conjunctions phases in
Figure and the minima caused by the ellipsoidal variations of the M giant VRI curves
are in go o d agreement So the minimum in U signi cantly precedes the sp ectroscopic
conjunction in phase and this cannot b e interpreted as an eclipse
Our sp ectral data Figure cover more than p er cent of the orbital p erio d but
there are no indications that any emission comp onent of H re ects the orbital motion
However we tried to measure the radial velocity of each pro le s base after cutting
everything at the level ab ove the continuum The H base velocity do es not change
signi cantly and remains ab out km s blueshifted relative to the velocity The lack
of orbital motion in H suggests that the dimension of the region in which this emission
originates can b e comparable to the distance b etween stars and or that q M M
cool hot
The large amplitude K km s obtained by Kraft from velocities of
hot
the H emission on seven plates is probably casual Any new observations esp ecially
during the high activity phase are very needed
The equivalent width of H systematically decreases from A to A b etween April
and June Similar values of the equivalent widths were observed by Anupama and
Prabhu during the previous activity p erio d in These authors also rep orted
a very strange b ehaviour of H with pronounced p eaks of intensity at b oth sp ectroscopic
conjunctions Our observations obtained a few days b efore orbital phase do not show
such b ehaviour and the mentioned e ect can rather b e an artefact
Rising U and B brightness and H emission as well as ickering activity denote that
T CrB was in a high activity state in
Acknowledgments We are much indebted to students of Toru n University Karolina
Darowny Jakub Janowski Maciej Wojtkowski and Pawe l Reng for their assistance in
carrying out photometric observations This research was sp onsored by the Polish KBN
Grant No P and Bulgarian NFSR Grant No F
T TOMOV D KOLEV
M MIKO LAJEWSKI
NAO Rozhen
Centre for Astronomy
P O Box
Nicolaus Cop ernicus University
Smolyan Bulgaria
Gagarina Toru n
e mail rozhen tempus tu plovdiv bg Poland
e mail mamiko astro uni torun pl
References
Anupama G C Prabhu T P MNRAS
Bailey J J Brit Astron Assoc
Cannizzo J K Kenyon S J ApJ L
Dobrzycka D Kenyon S J Milone A A E AJ
Iijima T J Am Assoc Variable Star Obs
Ivison R J Bo de M F Meaburn J A AS
Kenyon S J The Symbiotic Stars Cambridge University Press Cambridge
Kenyon S J Garcia M R AJ
Kraft R P ApJ
Miko lajewski M Miko lajewska J Tomov T Compact Stars In Binaries eds J
van Paradijs et al Kluwer Dordrecht p
Selvelli P L Cassatella A Gilmozzi R ApJ
Skopal A Hric L Cho chol D et al Contr Astr Obs Skalnate Pleso
Webbink R F Nature
ERRATUM
In the original version Fig have b een erroneously inserted in place of Fig to o
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
ACCURATE POSITIONS FOR VARIABLES
IN A FIELD AROUND BL Lac
Photographs of the eld around BL Lac were taken with the AFR wide eld astro
graph D cm F cm : : eld at Mt Maidanak Uzb ekistan in
The observations used the metho d describ ed by Shokin which allows to attenuate
brightness of bright reference stars This reduces the in uence of the brightness equation
on p ositions of faint ob jects and makes it p ossible to determine their co ordinates in a
system very close to the fundamental one
Positions of individual stars were derived from measurements of up to plates Table
contains equatorial co ordinates ep o chs of observations and GSC numbers Lasker et al
for variable stars in a eld The rst column contains GCVS names or NSV
catalog numbers Asterisks mark stars whose p ositions are most accurate b etter than to
00 00 00
: for the ma jority of stars the p ositions are accurate to : : For four stars V
Cyg V Cyg V Cyg V Cyg the derived p ositions are least accurate to ab out
00
: b ecause we had to use three steps for reductions to the source catalog The Palomar
prints show V Cyg as two comp onents partially overlapping The co ordinates in Table refer to the eastern red comp onent its variability is evident from two Palomar O prints
N N
E E
GT Cyg EL Lac Figure
Table
Star Ep o ch GSC
: :
h m s 0 00
UZ Cyg : :
GT Cyg
MN Cyg
MU Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
V Cyg
RS Lac
RY Lac
BI Lac
BK Lac
BL Lac
BO Lac
DE Lac
DL Lac
EL Lac
ET Lac
FU Lac
GN Lac
KQ Lac
V Lac
V Lac
NSV
NSV
NSV
NSV
NSV
NSV
NSV
NSV
Table
Star PPM HIC
NSV
NSV
RT Lac
BG Lac
CM Lac
CS Lac
CX Lac
VZ Cyg
Table contains PPM catalog R oser and Bastian identi cations for eight bright
variable stars in the program eld three of them are also identi ed with the HIPPARCOS
input catalog We present nding charts earlier never published for GT Cyg and
EL Lac we have con rmed the variability of the corresp onding stars using plates taken
0 0
with the Sternberg Institute s cm astrographs in Crimea Each charts covers a
eld
We are grateful to Mr S Antipin and Dr V Goranskij for assistance This study
was partially supp orted by the Russian Foundation for Basic Research through grant No
The nding charts are based on the Digitized Sky Survey pro duced at the
Space Telescope Science Institute under U S Government grant NAG W
Yu A SHOKIN
N N SAMUS
Sternberg Astronomical Institute
Institute of Astronomy
Universitetskij Prosp
Pyatnitskaya Str
Moscow Russia
Moscow Russia
References
HIPPARCOS Input Catalogue Europ ean Space Agency ESA SP
Lasker B M Sturch C R McLean B J et al Astron J
R oser S and Bastian U PPM Star Catalogue Heidelb erg Astron Rechen Inst
Shokin Yu A Astron Tsirk No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
A SEARCH FOR DORADUS TYPE VARIABLES
IN THE OPEN CLUSTER M
The Doradus stars constitute a new class of low amplitude variable stars Krisciunas
Handler list known members and candidates These stars typically show bright
ness variations of several hundredths of a magnitude on time scales of to days
Dor stars typically have early F type sp ectra and are found on or just ab ove the main
sequence in the Hertzsprung Russell Diagram The most likely explanation for their vari
ability is that they are exhibiting non radial gravity mo de pulsations Aerts Krisciunas
Balona et al
Eggen and Krisciunas et al suggest that the Doradus phenomenon
is age related There is evidence that many of these stars are younger than Myr
Krisciunas et al searched for candidates in the Hyades age Myr and
found none The basic idea is that once photospheric convection sets in the gravity mode
pulsations no longer are observable Given the masses of these stars M their
main sequence phase must last ab out Gyr We are naturally interested to know what
fraction of their main sequence life is sp ent exhibiting pulsations
Our interest in M NGC is that it is a reasonably nearby op en cluster whose
age is estimated to b e Myr Ianna Schlemmer which is in b etween the age of
NGC with eight Dor stars and that of the Hyades Ianna Schlemmer
provide a nding chart plates co ordinates apparent magnitudes and B V colors for the
stars Their photometry however is derived from photographic plates and is accurate to
no b etter than mag
Given that early F stars listed in the Bright Star Catalogue have B V colors in the
range to and given the color excesses of the stars in M mag we selected
stars from Ianna and Schlemmer s list with B V With one exception UVa
all of our program stars have membership probabilities greater than We used
UVa as our principal comparison star and UVa as a check star These two stars
and of our program stars were observed photo electrically by Johnson Our
observing pro cedure was to do V band di erential photometry and observe the principal
comparison star after every third program star Transformation to the UBV system was
accomplished with di erential measures of the red blue pair BS and BS Hall
We observed at Mauna Kea with the University of Hawaii s m telescop e and an
Optec SSP photometer b elonging to the University of Hawaii at Hilo Our seven night
run b egan on September UT We lost three whole nights to clouds and one to
equipment problems but did manage to obtain some accurate photometry From obser
vations of the principal check star UVa and of our program stars that app eared
to b e constant UVa and we estimate that the accuracy of an
individual measurement was mmag Our faintest star UVa gave a lower signal
to noise ratio and a corresp ondingly larger internal error
Table Summary of di erential photometry of M stars The comparison star in all cases was UVa
V B V For each star we give the assigned UVa numbers of Ianna Schlemmer
the mean di erential V magnitude the internal error of a single di erential value i e the
standard deviation of the distribution not the mean error of the mean and the number of data p oints
UVa V mmag N
Our individual data amounting to di erential measurements can b e obtained
from IAU Commission as le E of unpublished photometry See Breger Jaschek
Dub ois for further information on that archive We give in Table a summary
of the photometry obtained The internal error of our nightly means in Table compared
to the di erential magnitudes derivable from Table of Ianna Schlemmer is
mag which we attribute to the fact that their data were derived from photographic
plates It is also revealed that the V magnitude adopted by Ianna Schlemmer is
systematically to o bright If we use as a reference the V band values for the stars
observed photo electrically by Johnson the mean internal error is mag
One should adopt Johnson s value of V for the comparison star UVa
Because the di erential magnitudes of our check star UVa and ve of our pro
gram stars were constant we have great con dence that our comparison star UVa is
constant Therefore any variations observed in the other program stars can b e attributed
to those stars Six of our eleven program stars showed evidence of low amplitude vari
ability and are deserving of further study UVa and showed evidence
of di ering nightly means while UVa and showed some evidence for
variations over the course of a single night While we do not yet have data su cient to
prove that any of these stars are bona de Doradus type variables one would want
enough to obtain a decent p ower sp ectrum we show b elow the light curve of the b est
Dor candidate in M UVa It is reminiscent of parts of other single site light curves
of Dor stars See for example Mantegazza Poretti Zerbi
If it is con rmed that one or more of the early F stars in M vary by several hundredths
of a magnitude on a time scale of to days we will then know for certain that the
Doradus phenomenon extends to an age of Myr in the lives of main sequence stars of
mass M
Acknowledgments We thank Ted Simon for drawing our attention to M We thank
Susanna Martin for useful discussions and for her clouded out attempts to observe these
same stars KK thanks the University of Hawaii for time on the m telescop e and
thanks the Joint Astronomy Centre for observing supp ort
Figure Di erential V band photometry of UVa vs UVa dots Data for the star UVa
vs UVa op en circles are also shown o set by an arbitrary amount
K KRISCIUNAS
R A CROWE
Astronomy Department
Dept of Physics and Astronomy
University of Washington
University of Hawaii at Hilo
Box
West Kawili Street
Seattle Washington
Hilo Hawaii
USA
USA
e mail kevin astro washington edu
email rcrowe maxwell uhh hawaii edu
References
Aerts C and Krisciunas K MNRAS
Balona L et al MNRAS
Breger M Jaschek C and Dub ois P IBVS No
Eggen O J IBVS No
Hall D S IAPPP Communic
Ianna P A and Schlemmer D M AJ
Johnson H L ApJ
Krisciunas K Crowe R A Luedeke K D and Rob erts M MNRAS
Krisciunas K and Handler G IBVS No
Mantegazza L Poretti E and Zerbi F M MNRAS
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
IDENTIFICATION OF THE MARGONI STAGNI VARIABLES
In a publication A search for new variable stars in the Milky Way eld at l
b R Margoni and R Stagni give nding charts light curves and elements for
new variable stars A follow up pap er Margoni et al contains additional
observations for the same stars Ab out three quarters of these are now named variables
I have gone through this list to determine precise p ositions for all the stars and have
made identi cations with the IRAS and GSC catalogues Positions were drawn mostly
from the GSC version or the U S Naval Observatory UJ and A catalogues
Monet et al Monet The deep USNO catalogues were of considerable value
in obtaining p ositions for the fainter stars Where a star do es not app ear in any of these
I have used the Go ddard SkyView facility Scollick to estimate p ositions accurate
00
to ab out from the digitized sky survey DSS with a co ordinate grid overlay
The table is largely self explanatory The source of each p osition is indicated in the
column s immediately following using the following co des
A A
G GSC
U UJ
S SkyView
P PPM one star only
Stars and have p ositions from the literature as noted in the remarks which I have
veri ed by comparing the Margoni Stagni charts against the DSS
The principal variable star names are given in the Other IDs column along with
names found in SIMBAD Notes on sp eci c stars are indicated by an asterisk in column
n and follow after the end of the table
Table The Margoni Stagni Variables
MS RA Dec s IRAS GSC n Other IDs
A
U V Cyg
U Hen
U
S V Cyg
S V Cyg
S V Cyg
G LHS
U
S V Cyg
G V Cyg
A
U V Cyg
G V Cyg
Table cont
MS RA Dec s IRAS GSC n Other IDs
G
G
S V Cyg
U V Cyg
EM VES
U V Cyg
U V Cyg
A V Cyg
G
G V Cyg
CGCS
S V Cyg
A V Cyg
U V Cyg
U V Cyg
U V Cyg
U not GSC
S V Cyg
not HD
G V Cyg
S V Cyg
CGCS
S V Cyg
U V Cyg
G
U
U V Cyg
G V Cyg
EM VES
S V Cyg
G V Cyg
S V Cyg
G
A V Cyg
A
G V Cyg
A V Cyg
G V Cyg
U V Cyg
U V Cyg
P AG
G V Cyg
A
U V Cyg
LD
Table cont
MS RA Dec s IRAS GSC n Other IDs
U
G DO
IRC
PCC
S V Cyg
G
U V Cyg
S V Cyg
U V Cyg
U
G V Cyg
U V Cyg
A
G V Cyg
G V Cyg
U V Cyg
U V Cyg
S V Cyg
G V Cyg
S V Cyg
G V Cyg
U V Cyg
S
S V Cyg
U V Cyg
U V Cyg
U V Cyg
A V Cyg
U V Cyg
S V Cyg
G V Cyg
U V Cyg
V Cyg
G V Cyg
S
G V Cyg
U
A V Cyg
U
U
A V Cyg
U
G V Cyg
U V Cyg
A V Cyg
Table cont
MS RA Dec s IRAS GSC n Other IDs
A V Cyg
G V Cyg
Notes
symbiotic star Carrasco et al
00 00
G p osition corrected for annual prop er motion of : :
the southeastern star of a close pair
Margoni Stagni chart slightly in error northwestern star of a close pair
the northwestern star of a close pair
the northern star of a close pair
p osition is for the northern brighter of two stars
the southern fainter of two stars
BD IRC The PPM assigns the BD name in error to the visually fainter
s 00
companion southwest at end gures :
VLA p osition from Lewis et al
not GSC
not NSV which is at U
western star of a merged pair
eastern of two stars
crowded p osition somewhat uncertain
on northwest side of GSC
AFGL p osition from Joyce et al
the southeastern of two stars
northeastern of two stars
I appreciate the help of William P Bidelman in reviewing this list for errors and
identi cations This work was greatly facilitated by the use of SIMBAD maintained
by the Centre de Donn ees Astronomiques Strasb ourg France SkyView maintained by
Keith Scollick at Go ddard Space Flight Center and the wonderful U S Naval Observatory
PMM catalogues which were prepared by Dave Monet and colleagues at USNO Flagsta
Brian A SKIFF
Lowell Observatory
West Mars Hill Road
Flagsta AZ
USA
e mail bas lowell edu
References
Carrasco L Costero R and Serrano A in IAU Symp D Flower ed p
Joyce R R et al Astrophys J L
Lewis B M Chengalur J N Schmelz J and Terzian Y Mon Not R Astron
Soc
Margoni R and Stagni R Astron Astrophys Suppl Ser
Margoni R Stagni R Munari U and Marton S Astron Astrophys Suppl
Ser
Monet D Canzian B and Henden A Bul l Amer Astr Soc ab
stract
Monet D G Bul l Amer Astr Soc abstract
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
NSV IS AN ECLIPSING BINARY
BAV Mitteilungen Nr
NSV GSC PPM SAO BD
HD A CSV Pr AG was announced
m
as a short p erio d variable by Ho meister with a brightness range b etween and
m
and a sp ectral type A Sandig found NSV Pr to b e constant
m
at : on photographic plates According to Tsesevich NSV is probably
not p erio dic and in no case short p erio dic
Because of their proximity NSV was included in a photometric investigation of
AV Hya Every third day NSV showed an ascending branch from a minimum Our
photo electric measurements on nights in and excluded that the p erio d is an
integer fraction of these days
The photo electric observations were made at the private observatory of one of us
F A with an automatic photo electric telescop e The photometer was equipp ed with
an unco oled EMI A tub e and Schott lters for B and V The moment of minimum
light of completely observed minima was calculated using the metho d of Kwee and van
Woerden for the others the minima times were derived from the descending or
ascending branches
SAO F served as comparison star and SAO F was used to check
m
its constancy The amplitude of the primary minimum is ab out : In the secondary
m
minimum the amplitude do es not exceed : in V and is even less in B The duration
b etween rst and last contact is ab out hours a total eclipse could not b e detected
The individual measurements are sent by e mail on request
The construction of a complete lightcurve was found to b e extremely di cult from one
lo cation for the di erence b etween the p erio d and three whole days sums up to almost
a whole day after a year The photo electric lightcurve is therefore incomplete To get
information ab out p erio d changes in the past and of those parts of the lightcurve which
could not b e observed one of us T B investigated the star on plates of the Sonneb erg
Sky Survey covering the interval from until Photographic magnitudes were
obtained with a photometer and refer to Harvard Groningen SA see Figure The
following comparison stars were used
m GSC
pg
m GSC
pg
GSC m pg
Figure Di erential photographic light curve of NSV drawn with the ephemeris
derived in this pap er
Figure Di erential photo electric light curve in V and B V of NSV drawn with
the ephemeris derived in this pap er
Figure O C diagram of NSV drawn with the ephemeris derived in this pap er
Obviously the p erio d has not b een constant in the examined interval Weighted least
squares ts provided the following set of linear ephemeris
From JD to JD
d
Min I HJD : E
From JD to JD
d
Min I HJD : E
Until now it has b een not p ossible to decide whether the p erio d changes o ccur in an
erratic p erio dic or secular way Further observations are needed
Table Times of minima for NSV ep o chs and residuals computed with resp ect to
the ephemeris
N JD hel W T Ep o ch O C Observer
P Berthold
P
P
P
P
P
P
P
P
P
V Agerer
B
V
B
B
V
V
B
V
V
B
P denotes photographic minima B and V are photo electrically observed those
marked got reduced weight W
We want to acknowledge the help by the management and sta of Sonneb erg Obser
vatory
T BERTHOLD
F AGERER
Bundesdeutsche Arb eitsgemeinschaft
f ur Ver anderliche Sterne e V BAV
Munsterdamm
D Berlin Germany
E mail
agerer zweik t online de
b erthold mtl t online de
References
Ho meister C Astr Nachrichten
Kwee K K van Woerden H Bul l Astron Inst Netherland
Sandig H U Astr Nachrichten
Tsesevich V P Var Stars
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
IDENTIFICATION OF THE ROSINO GUZZI VARIABLES IN SAGITTA
The list b elow gives accurate co ordinates and IRAS identi cations for all but one of
the red variable stars found by Rosino Guzzi on a series of infrared plates
These faint stars lie in very crowded Milky Way elds To determine accurate p ositions
each star was examined on the digitized sky survey using the Go ddard SkyView facility
Scollick The IRAS identi cations were found using SIMBAD A few of the stars
were bright enough to app ear in the GSC or the USNO UJ and A catalogues Monet
et al Monet these p ositions were adopted when available
The nder chart for the star numbered MX Sge do es not match the sky at the
p osition given by Rosino Guzzi I searched at the p ositions of nearby IRAS sources
m 0
and at various obvious places where a typo might b e involved etc all to
no avail MX Sge must b e considered lost for now The p osition for star PP Sge
was given in error by in Dec and is corrected b elow
The table lists equinox p ositions the source of the p osition A A G GSC
version S SkyView U UJ IRAS names sp ectral types from the source pa
p er they are for the time of maximum and variable star designations from the GCVS
Kholop ov et al The nal column contains additional remarks an asterisk indi
cates a note at the b ottom of the table
I appreciate the e orts of G erardJasniewicz l Observatoire de Strasb ourg to integrate
these stars into the SIMBAD database
Brian A SKIFF
Lowell Observatory
West Mars Hill Road
Flagsta AZ
USA
e mail bas lowell edu
References
Kholop ov P N editor et al General Catalogue of Variable Stars th edition
Nauka Moscow
Monet D Canzian B and Henden A Bul l Amer Astr Soc ab
stract
Monet D G Bul l Amer Astr Soc abstract
Rosino L and Guzzi L Astron Astrophys Suppl Ser
advanced Scollick K http skview gsfc nasa gov cgi bin v skyview
Table The Rosino Guzzi Variables
RG RA Dec s IRAS sp ec GCVS Remarks
A HV Sge
A M HW Sge
A M HX Sge
U M HY Sge
S M HZ Sge
G M I I Sge GSC
S M IK Sge
A IM Sge
S M IN Sge
A IO Sge
A M IP Sge
S M IR Sge
S M IQ Sge
A IS Sge
S IT Sge
S M IU Sge
A M IV Sge
S M IW Sge
S M IX Sge
S M IY Sge crowded
G M IZ Sge GSC
G M KK Sge GSC
S M KM Sge
S KL Sge
A M KN Sge
A M KO Sge
A M KP Sge
A M KQ Sge
A KR Sge
S M KS Sge
S M KT Sge
S M KU Sge
A KV Sge
S M KW Sge
S M KX Sge
S M KY Sge
S KZ Sge
S M LL Sge
S M LM Sge
A LN Sge
S V Aql
S M LO Sge
S M LP Sge
S LQ Sge
S M LR Sge
S M LS Sge
S M LT Sge
A M LU Sge
S M V Aql
S M LV Sge
S V Aql
S M LW Sge
S V Aql
A M LX Sge
S LZ Sge
Table The Rosin Guzzi Variables cont d
RG RA Dec s IRAS sp ec GCVS Remarks
A LY Sge
S MM Sge
A M MN Sge
S MO Sge
S MP Sge
S M MQ Sge
S M MR Sge
S MS Sge
S M MT Sge
S MU Sge
S M MV Sge
M MX Sge
A MW Sge
S M MY Sge
S M MZ Sge
G M NO Sge GSC
S M NN Sge
S NP Sge
A M NQ Sge
S NS Sge
S M NT Sge
S M NV Sge
S M NU Sge
S M NX Sge
A M NW Sge
S M NY Sge
S M NZ Sge
S M OO Sge
S M OP Sge
S M OQ Sge
S NZ Vul
S M OO Vul
A M OP Vul
S OQ Vul
S M OR Vul
S M OS Vul
S OT Vul
S OU Vul
S OR Sge
S OS Sge
S M OV Vul
S M OT Sge
G M OW Vul GSC
S M OU Sge
S M OX Vul
S M OV Sge
A OW Sge
A OY Vul
S M OX Sge
S OY Sge
S M OZ Sge
A PP Sge
S M OZ Vul
S M PQ Sge
S M PR Sge
Table The Rosino Guzzi Variables concluded
RG RA Dec s IRAS sp ec GCVS Remarks
S M PS Sge
A M PT Sge
S M PP Vul
S M PQ Vul
A M PV Sge
A M PU Sge
A M PW Sge
S PX Sge
S M PY Sge
S M IL Sge
S V Aql
S NR Sge
S PZ Sge
Notes
ID somewhat uncertain p osition is for the northwestern star of a merged pair
this is not the M dwarf G
south southeastern star of a pair
crowded p osition is for southwestern of two stars
western star of a merged pair
northern star of a pair
southeastern star of a pair
western of two stars
s 00
ID uncertain alternate candidate at end gures :
southwestern star of a trio
northern star of a merged pair
p osition is just within the error ellipse of IRAS
in the eld of cluster Palomar
chart do es not match the star eld at the nominal p osition
northeastern star of a merged pair
in the eld of cluster Palomar
northeastern star of two
ID uncertain p osition is for the southwestern star of a merged pair
GSC p osition slightly o set due to crowding
western of two stars
p osition is just outside the error ellipse of IRAS
northwestern of two stars
Rosino Guzzi Dec error
northwestern star of a pair
southwestern star of a pair
ID uncertain p osition is for the southmost star of a trio
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER M
NGC M C l b is a variable po or cluster It is
0
an intermediate metallicity cluster with concentration class IX apparent radius r
0
Kukarkin and tidal radius r Webbink
The only variable found in this cluster by Sawyer Hogg is a long p erio d Cepheid
Later Clement et al con rmed her result that it was a W Vir variable number
d d
in Table and discovered its p erio d to b e unstable ranging from to
0 0
In our investigation we study four elds with the common size of One may
nd details of the observations and data reduction in the pap er by Bro cato et al
Search for variable stars in the cluster was made in the same way as describ ed in our
previous pap er Kadla et al From V and B frames we selected for our
study B V pairs with the time interval b etween B and V exp osures shorter than
min There are two stars numbers and in Table in the instability strip of the colour
magnitude diagram Figure that can b e considered as RR Lyrae variable candidates
Unfortunately the duration of observations was insu cient to con rm the variability of
these stars Data for susp ected variables co ordinates V magnitudes and colour B V
are listed in Table
Figure The color magnitude diagram for the globular cluster M susp ected
variables are marked by circles
A nding chart for M susp ected variables are denoted by circles
Table Positions and photometric data for susp ected variables
N X Y V B V
pixels pixels
Yu N MALAKHOVA
A N GERASHCHENKO
Z I KADLA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia e mail mal pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Clement Ch M Hogg H S Lee A AJ No
Kadla Z I Gerashchenko A N Malakhova Yu N IBVS No
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Sawyer Hogg H Publ Domin Astroph Obs No
Webbink R F IAU Symp osium No eds by J Go o dman P Hut Reidel Dordrecht
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
SUDDEN PERIOD CHANGE IN THE CONTACT BINARY AW UMa
The orbital p erio d change of the contact binary AW UMa was rstly rep orted by
Woo dward et al Hrivnak considered it as a sudden decrease of the p erio d
from one constant p erio d days to another one days which
o ccurred around or as a continuous decrease Due to the lack of observations it was
imp ossible to decide which type of p erio d change o ccurred
Our UBV photo electric observations were carried out at the Star a Lesn a Observatory
SL in Skalnat e Pleso Observatory SP in and and Kryonerion
Station of the National Observatory of Athens K in and The telescop es
and their equipments are describ ed in Hric et al BD was used as the
comparison star U B V light curves of AW UMa based on the and data are
depicted in Figure Mid eclipse brightening was registered in the secondary minimum
Pribulla and Cho chol Derman et al and Bakos et al rep orted
pronounced light and colour variations of AW UMa in Our light curves show
that AW UMa is in a quiet phase now The times of minima and their standard errors
determined using Kwee and van Woerden s metho d are given in Table
Figure U B and V light curves obtained at Star a Lesn a Observatory in and
Phases were calculated using the ephemeris
Table Times of minima of AW UMa
JD Min Obs Filt JD Min Obs Filt
hel hel
I K BV II SL UBV
I K BV I SL UBV
I K BV II SL UBV
I K BV II SP UBVR
I SP V I SL UBV
II SL UBV II SL UBV
I SL UBV I SP UBV
II SL UBV II SL UBV
I SL UBV II SL B
I SL UBV II SL V
Figure The O C diagram
The times of minima given in Table together with the data published by Yim and
Jeong and M uyessero gluet al as well as the data compiled from literature
by Bakos et al and Demircan et al were used to study p erio d change The
O C residuals Figure were calculated using the ephemeris
d
Min I HJD E
As it is apparent from Figure the data could b e explained either by two sudden p erio d
changes which o ccurred in and or by a continuous p erio d change The linear
ephemeris b etween the two sudden p erio d changes is identical with ephemeris
The p erio d days determined by Hrivnak and our ephemeris
indicate a p erio d jump P P The minima after the second jump are
de ned by the following linear ephemeris
d
Min I HJD E
The corresp onding p erio d jump P P is smaller than the rst one
The data in Figure tted by a parab ola continuous p erio d change are represented by
the following ephemeris
d
Min I HJD E E
The sum of squares of the residuals for the three linear ts d is half of that
for the quadratic t d therefore the sudden p erio d change seems to b e more
probable than the continuous one
Acknowledgements This work was partly supp orted by a NATO grant No
and by a VEGA grant
T PRIBULLA
H ROVITHIS LIVANIOU
D CHOCHOL
Section of Astrophysics
Astronomical Institute
University of Athens
Slovak Academy of Sciences
GR Zografos
Tatransk a Lomnica
Greece
Slovakia
e mail elivan atlas uoa gr
e mail pribula auriga ta sk
P ROVITHIS
Astronomical Institute
The National Obs of Athens
P O Box
GR Athens
Greece
References
Bakos G A Hor ak T B Tremko J Bul l Astron Inst Czechosl
Demircan O Derman E M uyessero glu Z A A
Derman E Demircan O M uyessero glu Z IBVS No
Hric L Skopal A Urban Z Contrib Astron Obs Skalnat e Pleso
Hrivnak B J Astrophys Journal
Kwee K K van Woerden H Bul l Astron Inst Neth
M uyessero glu Z G urol B Selam S O IBVS No
Pribulla T Cho chol D In Proceedings of the conference Contemporary problems
of astronomy Odessa in press
Woo dward E J Ko ch R H Eisenhardt P R Astron Journal No
Yim J R Jeong J H J Astron Space Sci
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
January
HU ISSN
TWO VARIABLE STARS IN AURIGA THE NEW CLASSICAL
CEPHEID NSV AND THE NEW ECLIPSING BINARY
SYSTEM GSC
The variability of NSV CSV VB GSC was rst
announced by Horn d Arturo and Lacchini In the NSV catalogue Kholop ov
NSV is recorded as an RR Lyrae star with a photographic amplitude of
magnitudes During the autumn of a variable star search carried out with the m
telescop e at Mollet del Valles Observatory Spain revealed that this susp ected variable
had a p erio d to o long for an RR Lyrae star To study more thoroughly its nature it was
monitored in the V band with the m telescop e at Esteve Duran Observatory Spain
using a CCD camera Observations were also p erformed with the m telescop e at
L Ametlla del Valles Observatory NSV was observed for nights from Octob er
to December GSC was used as comparison star and GSC as
check star
Photometric data shows that NSV is not an RR Lyrae star but a classical
Cepheid with a p erio d close to days which can b e unambiguously identi ed with
GSC an ob ject with an average photovisual magnitude PAL V lter of
m m
according to the Guide Star Catalogue Its amplitude in the V band is of : :
The phase curve Figure presents an asymmetry factor M m P The following
ephemeris was computed
d
Max HJD : E
Figure
Figure
Brightness measurements obtained from archival plates would allow to improve the
ab ove given ephemeris and also study its light curve in the past In addition to this sp ec
troscopic and more photometric data would help to obtain additional relevant information
ab out this new pulsating star
CCD reductions yielded that the check star GSC lo cated ab out arc
seconds to the Southwest of NSV is also variable According to the Guide Star
Catalogue its photovisual magnitude PAL V lter is This ob ject is an eclipsing
m m
binary star with a p erio d close to days and has an amplitude of : : at
m m
primary minimum and : : at secondary minimum in the V band Phase curve
Figure presents higher disp ersion around primary minimum than around minimum
I I Simultaneous observations p erformed with two di erent telescop es showed that this is
due to cycle to cycle changes in the shap e of the light curve probably as a consequence
of some form of stellar activity Although data scatter do es not allow to compute the
physical parameters of this binary system a preliminary study suggests that the primary
comp onent is ab out times as massive as the secondary one Minimum I is a transit
whereas minimum I I is an o ccultation
Due to the unstable shap e of primary minimum ephemeris to predict times of minima
was derived for minimum I I
d
Min I I HJD : E
A list of minimum I I timings and O C residuals for the ab ove given ephemeris was
also obtained after using the Kwee and van Woerden s metho d These are given in Table
Table
HJD O C
J M GOMEZ FORRELLAD
E GARCIA MELENDO
A GARRIGOS SANCHEZ
Esteve Duran Observatory
Grup d Estudis Astronomics
El Montanya Seva
Apartado
Seva
Barcelona
Barcelona
Spain
Spain
e mail jmgomez astro gea cesca es
e mail duranobs astro gea cesca es
References
Horn d Arturo G Lacchini G B Bologna Pubbl No
Kholop ov P N editor New Catalogue of Susp ected Variable Stars Moscow
Kwee K K van Woerden H BAN
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
PHOTOELECTRIC BVI OBSERVATIONS NEW ELEMENTS
c
AND A NEW CLASSIFICATION FOR BZ Tuc
BZ Tuc HV was included in our program of photo electric observations for
Cepheids b ecause it is listed in GCVS IV as a classical Cepheid with the elements
M axJ D E
We observed the star at CTIO during September November using the m re ector
A total of BVI measurements were obtained Table the accuracy of the individual
c
m
data b eing near in all lters Our new observations are plotted as lled dots in
Figure while op en circles refer to our earlier observations Berdnikov Turner
The slight o set of the new observations from our earlier observations in Figure
suggests that our data do not satisfy the ab ove elements In order to re ne them we
analyzed all available published observations using Hertzsprung s metho d the derived
ep o chs of maxima listed in Table together with times of maxima from Leavitt
were introduced into a linear least squares solution to obtain the following improved
ephemeris
M axJ D E
Table
JD V B V V I JD V B V V I
c c
Table
M axJ D Uncertainty Filter E O C Number of Author
Observations
pg Leavitt
B Gascoigne Kron
V Gascoigne Kron
B Eggen
V van Genderen
V Eggen
B van Genderen
B Madore
V Madore
V Freedman at el
V Harris
B Caldwell Coulson
V Caldwell Coulson
V This pap er
B This pap er
V BZ Tuc P=127.6 11.6
12.3 B-V 0.8
1.3 V-I C 0.9 1.2
0.0 0.5 1.0 Phase
Figure The light curve of BZ Tuc established by our earlier observations Berdnikov
Turner op en circles and the observations of Table lled circles
O - C P BZ Tuc C = 2430242.8+127.447·E
0.1
0.0
0.1
2420000 30000 40000 JD
Figure The O C diagram for BZ Tuc For convenience the O C values are expressed
in fractions of the p erio d
V BZ Tuc P=127.4 11.6
12.4 B-V 0.8 1.2
0.0 0.5 1.0 V BZ Tuc P=127.4 11.6
12.3 B-V 0.9 1.3 0.0 0.5 1.0 V BZ Tuc P=127.4 11.6
12.4 B-V 0.9 1.3
0.0 0.5 1.0 Phase
Figure The light curve of BZ Tuc according to van Genderen top Caldwell
Coulson middle and Eggen b ottom
The new ephemeris was used to calculate the O C values listed in Table as well
as for plotting Figures and In b oth Table and Figure we have taken into account
that maxima in lter B precede those in V by days The data of Figure as well as
the observations of van Genderen Caldwell Coulson and Eggen
which are replotted in Figure a c for the new ephemeris indicate that the shap e of the
light curve of BZ Tuc varies slightly Moreover a shift in the times of maxima for B V
relative to those in V is evident Such variability in light curve shap e suggests that BZ
Tuc cannot b e a classical Cepheid Likewise it cannot b e a type I I Cepheid b ecause of its
very long p erio d Possibly BZ Tuc is an RV Tauri variable or alternatively a semiregular variable of the UU Herculis class
The research describ ed here was made p ossible in part by grants No
from the Russian Foundation of Basic Research to LNB and through NSERC Canada to
DGT The authors were Visiting Astronomers at Cerro Tololo Inter American Observa
tory National Optical Astronomy Observatories which is op erated by the Asso ciation of
Universities for Research in Astronomy Inc AURA under co op erative agreement with
the National Science Foundation
D G TURNER
L N BERDNIKOV
Saint Mary s University
Sternberg Astronomical Institute
Halifax Nova Scotia B H C
Universitetskij prosp
Canada
Moscow Russia
References
Berdnikov L N Turner D G Astron Letters
Caldwell J A R Coulson I M South Afr Astron Observ Circ No
Eggen O J Astrophys J Suppl
Freedman W L Grieve G R Madore B F Astrophys J Suppl
Gascoigne S C B Kron G E M N R A S
Harris H C Ph D Thesis University of Washington
Leavitt H C Ann Astron Observ Harvard Col lege
Madore B F Astrophys J Suppl
van Genderen A M Astron Astrophys Suppl
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
PHOTOELECTRIC BVR OBSERVATIONS
c
FOR THE UU Her STAR EV AURIGAE
EV Aur is classi ed in GCVS IV as a classical Cepheid with a p erio d of
days We observed this star photo electrically in for nights JD
and revealed no changes is brightness Berdnikov with this p erio d Schmidt et al
observed EV Aur with CCD and susp ected that EV Aur was an UU Her star with
the elements
Max JD E
hel
To examine these elements we observed the star at Mt Maidanak Observatory Uzb ek
istan in September using the m re ector A total of BVR measurements were
c
m
obtained the accuracy of the individual data b eing near in all lters These data
as well as the observations taken in are listed in Table and presented graphically
in Figure
In Figure our data dots are represented together with observations published by
Schmidt et al circles Both o set in phase and di erence in shap e of our light curve
with resp ect to data of Schmidt et al con rm their conclusion most likely EV Aur is
an UU Her star
The research describ ed here was made p ossible in part by grant No from
the Russian Foundation of Basic Research
Table
JD V B V V R JD V B V V R
hel c hel c
V EV Aur P=55 11.9
12.3 B-V 1.9 2.1 V-R C 1.9 2.1
0.0 0.5 1.0 Phase Figure
V EV Aur P=55 11.9
12.3 B-V 1.9 V-R 2.1 1.7 1.9
0.0 0.5 1.0 Phase
Figure
V V IGNATOVA
L N BERDNIKOV
Astronomical Institute
O V VOZYAKOVA
Astronomicheskaya ul
Sternberg Astronomical Institute
Tashkent Uzb ekistan
Universitetskij prosp
Moscow Russia
References
Berdnikov L N Astronomicheskij Circular No
Schmidt E G Chab J R Reiswig D E Astron J
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
OPTICAL PHOTOMETRY OF CF Tuc MID THROUGH
CF Tuc CABS is a relatively bright V RS CVn type binary Hearnshaw
and Oliver It consists of a G type Main Sequence dwarf orbiting in a d
p erio d Budding ep o ch HJD with a K subgiant The star app ears
in front of the southern end of the SMC and has received signi cant attention from
observers in Australasia Budding and Zeilik and refs cited therein
The scale of related photometric starsp ot maculation activity has varied from very
large tenths of mag cf Hall to apparently insigni cant mag Budding and
McLaughlin with many observers recording irregularities on the order of mag
Drake et al p ointed out appreciable X ray emission from CF Tuc It is listed
in the ROSAT EUV Bright Source Catalogue Pounds et al and K urster
rep orted a very large are observed by ROSAT It has also b een found to b e a reasonably
active radio source Slee et al and this has prompted e orts toward multiwave
length observational studies Gunn et al The present article attempts to put
together recent photometric information as a background to such multiwavelength stud
ies involving further observations at the Australia Telescope in June which covered
a complete orbital cycle of the binary
In Figure we show data which has b een collected from two sites in New Zealand from
mid up to the end of the year The earliest p oints observed from the Kotipu Place
Observatory s APT KPO cf Hudson et al may b e slightly brighter than the
later trend towards a low secondary minimum This is in the sense that later KPO data
combined with that from T Rounthwaite indicate that towards the end of there was
a reasonably coherent maculation wave centering at phase around This wave may
have previously b een at a higher phase and subsequently drifted down in longitude Such
e ects are frequently observed for RS CVn stars showing sp ot waves and the rate of this
drift for CF Tuc has b een found to b e typically of order deg p er year Budding and
Zeilik in keeping with what could b e exp ected from the trends studied by Henry et
al although appreciable variations in the apparent rates of sp ot drifts are found
in particular cases
Figure indicates that the maculation wave continued its downward migration into
decreasing somewhat in amplitude in the pro cess The overall rate of drift over the
whole of would then app ear to b e ab out deg and if the drift was uniform over
this p erio d then the phase of the main minimum should have b een ab out at the time
of the radio observations in Australia carried out at the end of June
1
CABS refers to the Catalogue of Strassmeier et al
V Mag
c
c
7.5
c
c
c
c
c
c
c
c
c c
c c
c c c
c
c
c c
c
c
7.55
c
c
c
c
c
c
c
c cc
c
7.6
c
c
c
c
c
7.65
c
7.7
.0 .1 .2 .3 .4 .5 .6 .7 .8 .9 .0
Phase
Figure V light curve of CF Tuc Aug Dec KPO Rounthwaite
V Mag
7.5
c
c
c
c
c
c
c
c
c
c
c
c
c
c
c
c
c
c
c
7.55
c
c
c
c
c
c
c
c
c
c
c
c
7.6
7.65
7.7
.0 .1 .2 .3 .4 .5 .6 .7 .8 .9 .0
Phase
Figure V light curve of CF Tuc Jul Dec KPO Rounthwaite
Data continue to b e assembled and checked as part of a wider programme of active
star studies More intensive and detailed analyses can b e exp ected in further stages of
this programme
T ROUNTHWAITE
G HUDSON
R HUDSON
E BUDDING
Auckland Observatory
Kotipu Place Observatory
Wellington New Zealand
References
Budding E Inf Bul l Var Stars No
Budding E McLaughlin E Astrophys Space Sci
Budding E Zeilik M Astrophys Space Sci
Drake S A Simon T Linsky J L Astrophys J Suppl Ser
Gunn A G Migenes V Doyle J G Sp encer R E Mathioudakis M Mon
Not Roy Astron Soc in press
Hall D S in Solar Phenomena in Stars and Stel lar Systems eds R M Bonnet
A K Dupree Reidel Dordrecht
Hearnshaw J B Oliver J P Inf Bul l Var Stars No
Henry W Eaton J A Hamer A Hall D S Astrophys J Suppl
Hudson G Hudson R and Budding E Proc IAU Col l Posters eds I S
Elliott and C J Butler Dublin Institute for Advanced Studies
K urster M Cool Stars Stel lar Systems and the Sun th Cambridge Workshop
ASP Conf Series
Pounds K et al authors MNRAS
Slee O B Nelson G J Stewart R T Wright A E Innis J L Ryan S G Vaughan
A E Mon Not Roy Astron Soc
Strassmeier K G Hall D S Fekel F C Scheck M Astron Astrophys Suppl
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
A SUSPECTED RED VARIABLE IN THE ERROR BOX OF GRB
GRB is a gamma ray burst detected by the satellite Bepp oSAX on January
Costa et al So on after the event we observed the eld of GRB
Guarnieri et al with the meter telescop e BFOSC of the Bologna University
and compared it to the Digitized Sky Survey DSS We noticed on the R frames the
clear presence of a star Figure which was barely visible on the DSS whose limiting
magnitude is R The star is also practically invisible on the Palomar Sky Survey
red plates and absent on the blue ones limiting magnitude for b oth From the
DSS we deduced the co ordinates of this ob ject
h m s
equinox
with a conservative error of for b oth values The star is inside the GRB error
b ox communicated by Hurley et al see also Figure No variable ob ject within
a circle of radius and centered on these co ordinates is mentioned in the SIMBAD
database
From frames in R band in B and in V resp ectively collected b etween Jan
and Jan we determined the magnitudes of the star by means of the DAOPHOT
II package Stetson and the ALLSTAR pro cedure implemented in MIDAS The
entire log of observations together with the Palomar data is rep orted in Table
Table Available magnitudes and color indices for the variable
JD B V R B V V R Source
Palomar plates
m BFOSC
m BFOSC
m BFOSC
The calibration has then b een p erformed with the use of the photometric standards
in the eld of PG Landolt The star on January was at
R thus showing a variation of more than a magnitude with resp ect to the
Palomar red plates April while on January the R magnitude was
On January its magnitude in the R band was found to b e During the
same night its V R color index was Unfortunately the ob ject was to o faint to
b e visible in the B band even with an exp osure time of minutes we can however give
an indicative B V color index of by comparing the V R of the star with those
of eld stars with known B V color indices These colors suggest that this ob ject is a
mid late K sp ectral type star dep ending on the luminosity class Lang All this
seems to indicate that this susp ected variable might b e a long p erio d red star
Figure The eld of the susp ected variable in the Johnson R band exp osure time
minutes observed on January The star is indicated by the ticks North is at top east is to
the left The northern part of GRB error b ox by Hurley et al is also rep orted
CORRADO BARTOLINI NICOLA MASETTI
ADRIANO GUARNIERI Dipartimento di Astronomia
ADALBERTO PICCIONI
Universit adi Padova
Dipartimento di Astronomia
vicolo dell Osservatorio
Universit adi Bologna
I Padua Italy
via Zamboni
I Bologna Italy
References
Costa E Feroci M Piro L et al IAU Circ No
Guarnieri A Bartolini C Piccioni A et al IAU Circ No
Hurley K Kouvelioutou C Fishman G Meegan C IAU Circ No
Landolt A U AJ
Lang K R Astrophysical Data Planets and Stars Springer Verlag New York
Stetson P B PASP
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
IDENTIFICATION OF VARIABLES NEAR NGC
A group of new and known variable stars in the eld of the emission nebula NGC
was studied by Rosino Bianchini and Martino In the source pap er approximate
p ositions sp ectral types and elements of variation were presented along with nder charts
for the thirty two new variables All but one of these are now named variables Although
the p ositions provided are generally accurate they are not precise For the fainter stars
esp ecially precise p ositions are required b oth for their recovery for further study at the
telescop e and for linkage within other surveys such as IRAS
The tables b elow give precise p ositions and identi cations for all the stars Table
matches the Rosino et al Table in showing the variables already known at the time of
publication The sources of the p ositions are co ded in column s as follows
A A Monet et al
G GSC version
P PPM
S SkyView
U UJ Monet et al
For stars not in any available catalogue I used the Go ddard SkyView facility Scollick
00
to estimate p ositions from the Digitized Sky Survey to using a co ordinate grid
overlay The p ositions for MO Cas and MP Cas which lie in the bright nebulous region
of NGC were given erroneously by Rosino At the request of G Williams
amateur observer D diCicco obtained CCD frames that allowed measurement of their
p ositions which are given here
The sp ectral types are copied directly from Rosino et al those in parentheses were
taken from the literature An asterisk in the nal column indicates a note at the b ottom
of the tables
Table
Name RA Dec s GSC sp ec n
CC Cep U G K
AS Cep G M
CR Cas G K sic
DP Cep G F
PV Cas P B V
GU Cep G M
V Cas P M e
CI Cep G M e
HQ Cep U
Table cont d
Name RA Dec s GSC sp ec n
OQ Cep U M
CY Cep A
MO Cas M
MP Cas M
CH Cas G F pIb
V Cas P M
DQ Cas G M
V Cas G M
PW Cas G F G
IS Cas G A
CY Cas G G G Ib
DR Cas G M
V Cas G
V Cas U
DS Cas G C
V Cas A M
RS Cas G F G Ib
Table containing Rosino et al s new variables is arranged in a similar way Because
the stars are somewhat fainter few of them app ear in the GSC IRAS identi cations are
shown instead following the p ositions
Table
No Name RA Dec s IRAS sp ec n
PZ Cep S
QQ Cep U
V Cep P
QR Cep A M
NSV A
QS Cep A M
QT Cep S M
QU Cep A M
QV Cep G
QW Cep U M
QX Cep A M
QY Cep A M
V Cas A M
V Cas U
V Cas U M e
V Cas S M
V Cas A M
V Cas A M
V Cas G M
V Cas A M e
V Cas S M
Table cont d
No Name RA Dec s IRAS sp ec n
V Cas U
V Cas A
V Cas G M
V Cas A M
V Cas S M
V Cas A M
V Cas A M
V Cas A M
V Cas U M
V Cas G M
V Cas G M
Notes
Table
CR Cas LS I I I GCVS sp ectral type in error cf Popper
CI Cep IRAS
m
OQ Cep S Rosino et al RA error
CY Cep ID veri ed with chart in Rosino
MO Cas p osition from CCD frames by diCicco
MP Cas p osition from CCD frames by diCicco
CH Cas large Rosino GCVS RA error ID veri ed with chart in Parenago Kukarkin
V Cas IRAS Case CGCS
DR Cas IRAS
V Cas S
V Cas large Rosino et al GCVS p osition error ID veri ed with chart in Ho meister
Table
V Cep HD
QT Cep southmost star in the nebulous patch BFS GM
QV Cep GSC
V Cas southern star of a merged pair on DSS
V Cas IRC
V Cas LRS CGCS
V Cas GSC
V Cas GSC IRAS C CGCS
V Cas GSC IRAS large Rosino et al p osition error
0
cluster V Cas GSC Rosino et al Dec error lo cated on north side of sparse
V Cas GSC
This work was facilitated by the use of SIMBAD maintained by the Centre de Donn ees
Astronomique Strasb ourg France I appreciate the e orts of G erardJasniewicz Univer
sit e de Montpellier to integrate these stars into the database The U S Naval Obser
vatory PMM catalogues which were prepared by Dave Monet and colleagues at USNO
Flagsta were an indisp ensable aid in identifying the fainter stars My thanks to Gareth
Williams for providing the p ositions for MO Cas and MP Cas
Brian A SKIFF
Lowell Observatory
West Mars Hill Road
Flagsta AZ
USA
e mail bas lowell edu
References
Ho meister C Astron Nach
Monet D Canzian B and Henden A Bul l Amer Astr Soc ab
stract see also http www usno navy mil pmm
Monet D et al USNO A V A Catalogue of Astrometric Standards Wash
ington DC see also http www usno navy mil pmm
Parenago P and Kukarkin B W Perem Zvezdy
Popper D E Astrophys J Suppl Ser
Rosino L Publ Obs Bologna No
Rosino L Publ Obs Bologna No
Rosino L Bianchini A and Martino D Astron Astrophys Suppl Ser
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced pl
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
GSC A NEW DEEPLY ECLIPSING BINARY SYSTEM
IN DELPHINUS
BAV Mitteilungen Nr
h m s
The magnitude star GSC has recently b een
found to b e variable on lms taken over the last years as part of the UK Nova Supernova
Patrol Programme Details of the discovery and early observations are given by Collins et
al Initial rep orts of the variation were circulated electronically Hurst a and
the star has also b een given the designation TAV J Hurst b On the survey
lms Ko dak Tech Pan the star was seen mostly at m but o ccasionally
pv
it faded b elow the limiting magnitude of suggesting an eclipsing binary with a
p erio d of near days Extensive visual observations con rmed the initial estimate of
the p erio d and further showed that the star faded b elow m The eclipse history of
v
the star has also b een followed on plates of the Sonneb erg and Hartha Observatories sky
patrols taken over the past years The plates are blue sensitive ORWO ZU Ko dak
a O like and the exp osures were typically mins The variable is visible throughout
the primary eclipse and yielded times of minimum These are collected with the other
photographic and visual times of minimum in Table A more complete discussion of
these observations will b e published elsewhere
Figure Light curve from the CCD observations with the mo del t overlaid The magnitude di erences
m
are relative to star D on the nding chart Figure GSC which is given as : in V
Figure Detail of primary minimum with the mo del t sup erimp osed
Figure O C diagram of the times of minima using the ephemeris given in the text The
photographic photovisual visual and CCD timings are plotted as lled circles op en circles lled
squares and an op en square resp ectively
Since discovery GSC has b een observed extensively with a Starlight Xpress
SX CCD and V lter on a cm Newtonian telescop e Exp osure times were sec
onds and the limiting magnitude is typically in V The comparison star used was
GSC V star D on the nding chart Figure and the check star used
was GSC V The mean V b etween the comparison and check star is
mag which is consistent with the GSC magnitudes The CCD observations
show that the star reaches V giving a primary eclipse of mag with a duration
of just over one day The secondary eclipse is not well de ned but it probably has a depth
of only mag
Table Times of minima
JD Cycle O C Source JD Cycle O C Source
pg pv
pg pv
pg pv
pg pg
pg pv
pg pg
pg pv
pg pv
pg pv
pg vis
pg vis
pg CCD
pg
Source pg Sonneb erg Hartha pv UK Nova Supernova Patrol vis Visual
The times of minimum have b een used to search for the p erio d which can b e determined
unambiguously The CCD observations around primary minimum have b een used to
derive E and the p erio d has b een determined from the visual and photographic times of
minimum The ephemeris
Min I HJD E
is used to plot the light curves in Figures and and O C diagram in Figure
Although the light curve is not complete the combination of very deep primary mini
mum and weak secondary minimum clearly suggest a high inclination Algol system The
light curve has b een mo delled using the Light co de Hill see also Hill et al
and it was initially assumed that the system contains a hot main sequence star and a larger
co ol companion The solution is largely indep endent of the initial conditions although the
temp eratures of the stars are p o orly constrained and this pro duces large uncertainties in
the absolute parameters of the system The ratio of the temp eratures of the comp onents
is with the secondary at K while the primary is probably in the range
K The secondary may b e lling its Ro che lob e for q and is only
slightly smaller than the Ro che radius for a wide range of mass ratios The radius of the
primary is only smaller than that of the secondary The inclination is
degrees which is on the cusp of totality It therefore seems most likely that the system
contains a mid B to mid A type primary and a G K subgiant secondary If the primary
is hot then the system may b e similar to AU Mon or if it is somewhat co oler VW Cyg
For all likely masses of the primary its radius is a factor of larger than would b e
exp ected for a main sequence star so this comp onent would also seem to b e evolved
This new variable is a relatively rare example of a long p erio d Algol with very deep
eclipses As it is rather brighter than most of the stars in this group it should b e a useful
ob ject for testing the evolutionary mo dels of these systems and should repay further study
It is a pleasure to acknowledge the management and sta of the Sonneb erg Observatory
for their help in accessing the Sky Patrol plates
Figure Finding chart for GSC taken from Collins et al The comparison is star D
South is up and the eld is arcmin square
G J KIRBY
C LLOYD
College Lane
Rutherford Appleton Lab oratory
Weymouth
Chilton Didcot
Dorset DT LP UK
OXON OX QX UK
compuserve com
cl ast star rl ac uk
M J COLLINS
N D JAMES
The Lawns
Tavistock Road
Everton
Chelmsford
Bedfordshire SG LB UK
Essex CM JL UK
compuserve com
ndj astro demon co uk
T BERTHOLD
Nr
D Nauhain
Germany
Berthold MTL t online de
References
Collins M J James N D Kirby G J Lloyd C The Astronomer
Hill G Pub DAO
Hill G Fisher W A Holmgren D A A
Hurst G M a ed TA e circ
Hurst G M b ed TA e circ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
HD A NEW VARIABLE STAR
The detection of variability in HD V CD SAO is re
p orted HD was used as one comparison star for the two Bo otis stars HD
and HD during our survey to detect pulsation within this group Both Bo otis
stars and the second comparison star HD turned out to b e constant with an
upp er limit of mmag in Str omgren b Paunzen et al Paunzen et al Obser
vations were p erformed at ESO during three nights see Table in Paunzen et al
A detailed description of the observation and reduction pro cedure can also b e found in
Paunzen et al
Variability in the brightness of HD is clearly evident in all three nights Figure
shows the di erential light curves of HD and HD for the rst night in
Str omgren v Furthermore the data for HD HD are presented to show
the go o d photometric quality of the night and to establish the variability for HD
Using the data of all three nights a time series analysis results in a p erio d of ab out
minutes and an amplitude of mmag in Str omgren v The high statistical signi cance
compared to the mean noise level proves the found p erio d Since Figure shows
that a semi regular or multiperio dic b ehaviour is evident these results are just rst
numerical estimations
In order to determine the nature of variability a search for informations in SIMBAD
was p erformed Houk classi ed this star as B V with a quality ag b est Unfor
tunately no photometric measurements in one of the common systems Geneva Johnson
or Str omgren were found making a calibration imp ossible Following this sp ectral type
a p ossible Scuti pulsation can b e excluded since the hot b order of the instability strip
ends at A Lo oking for other sources of variability among B type stars a p ossible mem
b ership in the Cephei group stars hotter than B with luminosity classes II to IV
and Be group emission line stars with shells p erio ds hours and amplitudes mag
e g Pleione Cas S Dor etc is very unlikely One may sp eculate that HD is
an unrecognized sp ectroscopic binary with a pulsating A type comp onent Also a false
classi cation by Houk cannot b e ruled out
In order to unambiguously establish the lo cation of HD in the Hertzsprung
Russell diagram and thus to determine the nature of variability photometric and sp ec
troscopic observations are very much needed The author therefore encourages further
observations as well as collab orations for solving the nature of HD
Acknowledgements This research was carried out within the working group Asteroseis
mology AMS with funding from the Fonds zur F orderungder wissenschaftlichen Forschung
pro ject S AST Use was made of the SIMBAD database op erated at CDS Stras
b ourg France
HD 193256 - HD 194170
HD 193084 - HD 193256 40 mmag (v)
0.65 0.70 0.75 0.80 0.85
HJD 2449560+
Figure The di erential light curves for HD HD and HD HD for the
rst night in Str omgren v
E PAUNZEN
Institut f ur Astronomie der
Universit atWien
T urkenschanzstr
A Wien
e mail paunzen astro ast univie ac at
References
Houk N University of Michigan Catalogue of Two Dimensional Spectral Types for
the HD Stars Volume I I I Astronomy Dept Univ Mich Ann Arb or Michigan
Paunzen E Weiss W W Kuschnig R IBVS No
Paunzen E Kuschnig R Handler G Gelbmann M Weiss W W A AS in press
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
February
HU ISSN
DETECTION OF NEW BRIGHT VARIABLE STARS
BY THE TYCHO INSTRUMENT OF THE HIPPARCOS SATELLITE
The Tycho exp eriment on b oard of the Hipparcos satellite has led to a photometric
catalogue that promises to improve our knowledge ab out variable stars greatly Mauder
H g For ab out one million stars up to B completeness up to mag
the brightness in two sp ectral bands Tycho V and Tycho B similar to Johnson V and
Johnson B is given at to moments which are spread over the four year lifetime
of the satellite
This database has great advantages against archived photoplates that are usually used
to search for new variable stars On the one hand the brightness is given in magnitudes
no further photometric reduction is necessary On the other hand the moments of obser
vations are almost completely indep endent of seasons and daytimes This is imp ortant
for variables having a p erio d of ab out one day or one year what makes them hardly
detectable by ground based observations
We have searched the Tycho Mean Photometric Catalogue TPMC and the Tycho
Photometric Observations Catalogue TPOC for new variable stars using merely two
criteria The rst one is that variability causes a scattering of the brightnesses at single
observations with resp ect to their median value Therefore the error of this median will
b e larger than one would exp ect for a constant star if the amplitude of the variability
is strong enough Grossmann private communication The other criterion do es only
a ect p erio dic variables Periodogram analysis Horne Baliunas has b een done
with the time series from the catalogue The height of maxima in the p erio dogram yields
a probability for a correct p erio d determination Scargle that is usually more than
for the stars presented here
This analysis is strongly a ected by the extremely uneven sampling The smallest time
interval b etween two single measurements is ab out one second but there can b e several
months without any observation of the star This leads to instabilities of maxima in the
p erio dogram We tried to overcome this problem by computing the p erio dogram over
di erent time intervals but this is only an improvement and not a complete solution
The measurement technique of Tycho causes another problem The presence of eld stars
in the neighborho o d of a program star and esp ecially an unknown multiplicity of the star
can simulate a variability that in fact do es not exist For these reasons we encourage
astronomers to observe the stars that are presented here This will lead to a b etter
con dence for the variability and esp ecially the p erio d determinations
The p erio dic lightcurves shown here were pro duced as follows The data were phased
with resp ect to the p erio d taken from the p erio dogram and then binned into equal
parts of the p erio d The gures show to cycles The reason for this binning is that single
observations may b e disturb ed and can lead to wrong conclusions if they are taken to o seriously
d
Figure Phased lightcurve P : of the star HD in V This may b e an eclipsing binary of
Lyr type
d
Figure Phased lightcurve P : of the star HD in V triangles and B squares Note
the variability of the colour index B V
d
Figure Phased lightcurve P : of the star HD in V triangles and B squares
Table Results on the new variables
No TICID Cross RA Dec Period Type
Identi cation days
h m s 0 00
HD : : RRc
HD L
HD
HD L
HD SR
HD EW
HD
HD EW
HD EB
HD SR
HD L
HD L
HD L
HD EB
HD
HD
HD L
HD
HD SR
HD L
HD SR
HD RRb
HD SR
HD RRa
HD
HD L
HD L
HD SR
HD EA
HD
HD L
HD EB
HD L
HD L
HD SR
HD L
HD
HD Cep
HD
HD
HD Cep
SAO L
CSI RRb
The TICID is the name of a star in the Tycho Catalogue The rst number gives the GSC region
the second one is a running number inside this region and the last one numbers comp onents of multiple
systems
Because the space is limited not all of the lightcurves can b e presented here They
are available on the IBVS ftp site ftp konkoly hu pub ibvs f
No is the serial number in Table
Acknowledgements I am thankful to Prof Horst Mauder T ubingen for giving me the
p ossibility to work with Tycho data Andreas Wicenec and Volkmar Grossmann help ed
me very much in doing my diploma thesis This research has made use of the SIMBAD
database op erated at CDS France
J WOITAS
Max Planck Institut f urAstronomie
D Heidelb erg
Germany
e mail woitas mpia hd mpg de
References
Horne J Baliunas S ApJ
Mauder H H g E A A
Scargle J ApJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
OBSERVATIONS OF THREE BOOTIS STARS
BY USING DUAL CHANNEL PHOTOMETER
A small group of Bo o stars attracts astrophysicists attention owing to their contro
versial evolutionary status These stars related apparently to a short lived evolutionary
phase are available for the development and control of the mo dern stellar atmosphere
theories Gray Corbally The discovery of the Bo o stars pulsations Weiss et
al gives the opp ortunity to apply the to ols of asteroseismology for their profound
investigation Observations of the variability of Bo o stars with di erent equipments
are widely presented in IBVS by the Vienna working group Asteroseismology AMS It
should b e noted that a high quality of sky seeing and instrumentation and long time
data series are needed for such observations b ecause the stars with relatively long p erio ds
from up to hours have very low amplitudes from mag to mag
During we have observed stars from the list of Gray Corbally by
using the dual channel photometer Dorokhov Dorokhova attached to the m
Ritchey Chretien telescop e situated in Central Asia at the Mt Dushak Erekdag station
of Odessa Astronomical Observatory
HD was observed in Str omgren v lter on two nights and Oct
and HD C HD C HD was observed in Johnson B lter on and
Nov in single channel by using star mo de see Breger Our observations
con rm nonvariability of b oth stars within the upp er limits which are higher by mag
than presented in the pap ers by Paunzen et al and by Kuschnig et al
Figure On the top panel light curves for HD and comparison star HD in Johnson s B
on the b ottom panel the VAR COM curves for two nights and Nov All the curves are
presented as residuals to the corresp onding night means The solid line is a least squares t of f and
1
f frequencies 2
Figure Fourier sp ectrum of b oth nights data The middle panel shows the same after removal for
f c d the lower panel the result of the prewhitening for f c d and f c d
1 1 2
HD was tested by Paunzen Handler in August They obtained
a p erio d of min and amplitude mmag in Str omgren b We observed HD
and a comparison star HD m mag A simultaneously in dual channel mo de
of the photometer on the nights and Nov The data were acquired as
continuous sec integrations in Johnson s B lter interrupted by the channel reductions
ab out one time p er hour
Then the counts of the comparison star in channel were reduced to the sensitivity level
of channel the data were corrected for coincidence counting losses the sky background
contribution and the atmospheric extinction and were binned to min integrations by
taking p oint averages Figure shows the light curves of HD and the comparison
star and the di erential data as residuals to the nightly means for each date In order to
decrease the di erential data noise level comparison star s observations were smo othed
by a rectangle lter with window size The solid line in Figure is a least squares t
of two frequencies which were revealed from subsequently prewhitened amplitude Fourier
sp ectrum of common series of data Figure The packaged program PERIOD Breger
was used for Fourier analysis Two p eaks at frequencies f c d P
1
hour A mag and f c d P min A mag could b e in uenced
2
by a c d aliasing The result needs in further control b ecause the variations of sky
transparency may a ect the such low amplitude light curves even in the case of dual
channel photometry Here we can only supp ose that HD as well as already known
HD Paunzen et al and Cyg Kusakin Mkrtichian is another
example of the multiperio dicity of Bo otis stars like that taking place in Scuti stars
T N DOROKHOVA
N I DOROKHOV
Astronomical Observatory
Odessa State University
Shevchenko Park Odessa Ukraine
References
Breger M Commun Asteroseismology
Breger M Commun Asteroseismology
Dorokhov N I Dorokhova T N Odessa Astronomical Publ
Gray R O Corbally C J AJ
Kusakin A V Mkrtichian D E IBVS No
Kuschnig R Gelbmann M Paunzen E Weiss W W IBVS No
Paunzen E Handler G Weiss W W North P IBVS No
Paunzen E Handler G IBVS No
Paunzen E Weiss W W Kuschnig R IBVS No
Weiss W W Paunzen E Kuschnig R Schneider H A A
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER NGC
NGC C l b according to its sp ectral class F
Hesser Shawl is a relatively high metallicity but p o orly studied cluster Goran
skii obtained an upp er part of the CMD and detected one RR Lyrae variable near
the cluster center At present the only CCD photometric study of this cluster was made
by Bro cato et al Our search for RR Lyrae variables was made on the base of
these CCD observations by the metho d describ ed in Kadla et al
0
The cluster has a small apparent angular radius r Kukarkin and a high
00
central concentration For this reason the CMD was obtained for stars with r
00
Figure In the instability strip there are two stars one is a known RR Lyr
variable V detected by Goranskii and the other is a susp ected RR Lyr star
Their p ositions are shown in the cluster chart Figure
Figure The color magnitude diagram for the globular cluster NGC The known
RR Lyrae star is denoted by susp ected
Figure Chart of the cluster Variable stars are denoted by
We are grateful to the Russian Foundation for Basic Research for nancial supp ort
A N GERASHCHENKO
Z I KADLA
YU N MALAKHOVA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia e mail mal pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Goranskii V P Soviet Astronomy
Hesser J E Shawl S J PASP
Kadla Z I Gerashchenko A N Malakhova Yu N IBVS
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub lishing House Nauka Moscow
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER NGC
The globular cluster NGC C l b has a low concen
tration CC XI I and relatively low metallicity Estimates of the latter range from
Bica Pastoriza to Frogel et al The integral sp ectral class F
Hesser Shawl favours the former value The cluster has an apparent radius
0 0
r Kukarkin and tidal radius r Webbink
In the rst two editions of Catalogue of Variable Stars in Globular Clusters Sawyer
with reference to a communication from H Shapley there are unpublished
and susp ected variables in the cluster However no data are given for these stars In
a search for variables Fourcade et al two type unknown were discovered at a
0
considerable distance from the cluster center r A further search Kaluzny
Krzeminski detected short p erio d SX Phe type variables and close binaries In
0
the present study the search for RR Lyr type variables was made in the area r using
the same V and B observations Bro cato et al in four overlapping elds with
consecutive exp osures and applying the same metho d of search for variable stars as in our
previous pap ers Kadla et al a b
Figure The color magnitude diagram for the globular cluster NGC The
susp ected RR Lyrae stars are denoted by
Figure Chart of the western part of the cluster Variable stars are denoted by
Table Positions and photometric data for susp ected variables stars
N X Y V B V
arcsec arcsec
A comparison of the CMDs for the four elds revealed that the absorption in the
southern part of the investigated area is less than in the northern part E B V
The resulting CMD corrected for di erential absorption is shown in Figure Data for
the four stars in the instability strip which are susp ected RR Lyr variables are given in
Table Their p ositions are determined using as a reference frame the co ordinate system
given in the pap er by Kaluzny Krzeminski and are shown in the nding chart
Figure V and B V values for V are corrected for di erential absorption The short
duration of the observations less than min in each color for each eld did not p ermit the con rmation of the variability of these stars
We are grateful to the Russian Foundation for Basic Research for nancial supp ort
A N GERASHCHENKO
Z I KADLA
Yu N MALAKHOVA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia
e mail mal pulkovo spb su
References
Bica C L D Pastoriza M G ApSS
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Fourcade C R Lab orde J R Albarraem J Atlas y Catalogo de estrellas
variables en cumulos globulares al sur de Cordoba
Frogel J A Cohen J G Persson S E ApJ
Hesser J E Shawl S J PASP
Kadla Z I Gerashchenko A N Malakhova Yu N a IBVS No
Kadla Z I Gerashchenko A N Malakhova Yu N b IBVS No
Kaluzny J Krzeminski W MNRAS
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Sawyer H Publ David Dunlap Obs No
Sawyer H Publ David Dunlap Obs No
Webbink R F IAU Symp osium No eds by J Go o dman P Hut Reidel Dordrecht
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
IDENTIFICATION OF DAHLMARK VARIABLES I
The amateur observer Lennart Dahlmark has published a useful series of IBVS notes
listing a number of candidate variable stars most of which were new Although adequate
charts and reliable semi accurate p ositions were supplied no other identi cations were
usually given If the stars are to b e recovered for further study and linkage within other
surveys IRAS etc then precise p ositions must b e determined to make identi cation
unambiguous within crowded galactic elds
Table gives precise p ositions and identi cations for the rst list of variables published
by Dahlmark The variable stars were identi ed indep endently by the two authors
Ski compared Dahlmark s charts against the Digitized Sky Survey DSS using the Go d
dard SkyView facility Scollick The identi cations were found within SIMBAD
for the GSC and in the U S Naval Observatory s UJ and A star catalogues Monet
et al Monet et al Williams compared Dahlmark s charts against the DSS
maintained as a service at the Center for Astrophysics by the Computation Facility Po
sitions are taken either from the GSC or preferably from the USNO A UA
catalogue For those ob jects not found in these catalogues p ositions were measured from
the DSS using comparison stars from the UA catalogue the r m s residuals of
00
the comparison stars were under :
Table Dahlmark Variables LD LD
Name RA Dec s IRAS GSC n Other ids
LD U
LD G
LD D
LD D
LD G
LD U
LD D
LD G
LD G
LD U
LD U
LD G V Cyg
LD U
LD U
LD U
LD G V Cyg
Table Dahlmark Variables LD LD cont
Name RA Dec s IRAS GSC n Other ids
LD U
LD G
LD U V Cyg
LD U
LD U
LD D
LD U
LD U V Cyg
LD G
LD U
LD G V Cyg
LD D
LD G V Cyg
LD G
LD U
LD G V Cyg
LD G
LD U
LD G
LD G V Cyg
LD D EM CGHA
LD U
LD U
LD U
LD G EM VES
LD G V Cyg
LD D
LD U
LD D V Cyg
LD G V Cyg
LD D
LD U
LD U V Cyg
LD G V Cyg
LD U
LD U V Cyg
LD G
LD U V Cyg
LD U
LD G V Cyg
LD U V Cyg
LD G CGCS
Notes
LD Not visible on POSS I O print and R on E print GSC plate taken when V
s 00
blended with companion star to N with p osition end gures : : D
LD SE of two stars
LD Not IRAS
LD The brighter of two stars on DSS
LD Sp ectral type M Dolidze
LD Sp ectral type M Dolidze
LD Sp ectral type M Dolidze
LD ID veri ed against chart in Bychkov b SW star of two
LD Very close pair blended in GSC Position given is for brighter on DSS NW comp onent
s 00
SE comp onent has end gures : : D
LD ID veri ed against chart in Bartunov
LD ID veri ed against chart in Bychkov a
The table lists the LD name followed by the J p osition and its source co ded in
the table and notes as follows U UA G GSC D measurement from DSS
using UA comparison stars The next two columns give IRAS p oint source and GSC
designations An asterisk in the next column indicates a note at the b ottom of the table
The nal column contains GCVS designations and other names from SIMBAD
The authors thank the following for their indisp ensable assistance in completing this
work SIMBAD maintained by the Centre de Donn eesAstronomique Strasb ourg France
and SkyView maintained by Keith Scollick at Go ddard Space Flight Center
Brian A SKIFF
Gareth V WILLIAMS
Lowell Observatory
Harvard Smithsonian Center
West Mars Hill Road
for Astrophysics
Flagsta AZ
Garden Street
U S A
Cambridge MA
e mail bas lowell edu
U S A
e mail gwilliams cfa harvard edu
References
Bartunov O S Astron Tsirk
Bychkov S M a Astron Tsirk
Bychkov S M b Astron Tsirk
Dahlmark L IBVS No
Dolidze M V Byul l Abastuman Astro z Obs
Monet D Canzian B and Henden A Bul l Amer Astr Soc
abstract see also http www usno navy mil pmm
Monet D G et al USNO A V U S Naval Observatory Washington DC
see also http www usno navy mil pmm
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced pl
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
IDENTIFICATION OF DAHLMARK VARIABLES II
This note is a continuation of a series Ski Williams listing accurate co or
dinates and identi cations for variable stars discovered by the amateur observer Lennart
Dahlmark This work is intended to assist in the recovery of these variable stars for
further study and linkage within other surveys
The metho ds used by the authors in their indep endent identi cation of the variable
stars are describ ed in the rst note of this series Ski Williams Table gives
precise p ositions and identi cations for the second list of variables published by Dahlmark
The table lists the LD name followed by the J p osition and its source co ded
in the table and notes as follows U UA G GSC D measurement from
DSS using UA comparison stars The next two columns give IRAS p oint source and
GSC designations An asterisk in the next column indicates a note at the b ottom of the
table The nal column contains GCVS designations and other names from SIMBAD
Table Dahlmark Variables LD LD
Name RA Dec s IRAS GSC n Other ids
LD U
LD D
LD U V Cas
LD G
LD U
LD U CGCS
LD G
LD U
LD G V Cas
LD G
LD D CGCS
LD U
LD U
LD G
LD D
LD U V Cas
LD U
LD G
LD G V Cas
LD D
LD G
LD U
LD G
Table cont
Name RA Dec s IRAS GSC n Other ids
LD D
LD D CGCS
LD G
LD G
LD G CGCS
LD G
LD G
LD G
LD U
LD D
LD U
LD G
LD D
LD G
LD G V Cas
LD G
LD G V Cas
Notes
LD Published declination in error by Corrected following corresp ondence with Dahlmark
LD Close pair Position given is for the brighter on the DSS comp onent Other comp onent
s 00
has end gures : :
LD Sp ectral type M Dolidze
LD Sp ectral type M Dolidze
LD Close pair Position given is for NE comp onent SW comp onent GSC has
s 0 00
end gures : : D
LD Sp ectral type M Dolidze
LD Sp ectral type M SC Dolidze
LD Pair blended in GSC Position given is for the brighter on the DSS comp onent
s 0 00
Other comp onent has end gures : : D
LD Not AV Cas cf remarks by Stephenson
LD Not a blue star as indicated by LD color
LD Pair blended in GSC Position given is for the brighter on the DSS comp onent
s 0 00
Other comp onent has end gures : : D
s 00
LD Very close pair Position given is S comp onent Other comp onent has end gures : : D
LD Sp ectral type M Rust
The authors thank the following for their indisp ensable assistance in completing this
work SIMBAD maintained by the Centre de Donn eesAstronomique Strasb ourg France
and SkyView maintained by Keith Scollick at Go ddard Space Flight Center
Brian A SKIFF
Gareth V WILLIAMS
Lowell Observatory
Harvard Smithsonian Center
West Mars Hill Road
for Astrophysics
Flagsta AZ
Garden Street
U S A
Cambridge MA
e mail bas lowell edu
U S A
e mail gwilliams cfa harvard edu
References
Dahlmark L IBVS No
Dolidze M V Byul l Abastuman Astro z Obs
Rust C F Astrophys J
Ski B A and Williams G V IBVS No
Stephenson C B IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
IDENTIFICATION OF DAHLMARK VARIABLES III
This note is a continuation of a series Ski Williams a Williams Ski
listing accurate co ordinates and identi cations for variable stars discovered by the
amateur observer Lennart Dahlmark This work is intended to assist in the recovery of
these variable stars for further study and linkage within other surveys
The metho ds used by the authors in their indep endent identi cation of the variable
stars are describ ed in the rst note of this series Ski Williams a Table gives
precise p ositions and identi cations for the third list of variables published by Dahlmark
The table lists the LD name followed by the J p osition and its source
co ded in the table and notes as follows U UA G GSC D measurement
from DSS using UA comparison stars The next two columns give IRAS p oint source
and GSC designations An asterisk in the next column indicates a note at the b ottom of
the table The nal column contains GCVS designations and other names from SIMBAD
Table Dahlmark Variables LD LD
Name RA Dec s IRAS GSC n Other ids
LD U V Lyr
LD U V Vul
LD G V Lyr
LD U V Lyr
LD G V Lyr
LD G V Lyr
LD D V Vul
LD U V Vul
LD G V Vul
LD U V Lyr
LD U V Lyr
LD U V Vul
LD G V Vul
LD U V Vul
LD G V Vul
LD U V Vul
LD D V Lyr
LD U V Vul
LD U V Lyr
LD G V Cyg
LD U V Vul
LD U V Cyg
Table cont
Name RA Dec s IRAS GSC n Other ids
LD G V Vul
LD U V Cyg
LD U V Cyg
LD U V Vul
LD D V Vul
LD G V Vul
LD U V Cyg
LD G V Cyg
LD D V Cyg
LD U V Cyg
LD G AI Vul
LD U V Cyg
LD U V Vul
LD D V Cyg
LD U V Cyg
LD U V Vul
LD U
LD U V Vul
LD U V Cyg
LD U V Vul
LD U V Vul
LD D V Vul
LD D V Vul
LD U V Vul
LD D V Cyg
LD U V Cyg
LD G V Cyg
LD D V Cyg
LD D V Cyg
LD G V Cyg
LD U V Vul
LD D V Cyg
LD U V Cyg
LD U V Vul
LD U V Cyg
LD U V Vul
LD U HX Vul
LD G V Vul
LD U V Vul
LD U V Vul
LD U V Cyg
LD U V Vul
LD U V Vul
Table cont
Name RA Dec s IRAS GSC n Other ids
LD U V Vul
LD D V Vul
LD U V Lyr
LD U V Vul
LD U V Vul
LD U V Cyg
LD D V Cyg
LD D V Cyg
LD U V Cyg
LD U V Cyg
LD D V Cyg
LD U V Vul
LD G V Cyg
LD D V Vul
LD U V Vul
Notes
LD IRC
LD CGCS
LD CGCS
LD CGCS Not EM VES Close trio blended in GSC Other comp onents
s 00 s 00
have end gures : : D and : : D
s 00
LD Pair GSC entry agged as nonstellar N comp onent has end gures : : U
s 00
LD CGCS Pair N comp onent has end gures : : D
LD CGCS
LD Identity con rmed by comparison with nder chart on MVS
s 00
LD Pair blended in GSC N comp onent has end gures : : D
s 00
LD Pair E comp onent has end gures : : D
The authors thank the following for their indisp ensable assistance in completing this
work SIMBAD maintained by the Centre de Donn eesAstronomique Strasb ourg France
and SkyView maintained by Keith Scollick at Go ddard Space Flight Center
Brian A SKIFF
Gareth V WILLIAMS
Lowell Observatory
Harvard Smithsonian Center
West Mars Hill Road
for Astrophysics
Flagsta AZ
Garden Street
U S A
Cambridge MA
e mail bas lowell edu
U S A
e mail gwilliams cfa harvard edu
References
Dahlmark L IBVS No
Dahlmark L J AAVSO
Ski B A and Williams G V IBVS No
Williams G V and Ski B A IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
March
HU ISSN
IDENTIFICATION OF DAHLMARK VARIABLES IV
This note is a continuation of a series Ski Williams a b Williams Ski
listing accurate co ordinates and identi cations for variable stars discovered by the
amateur observer Lennart Dahlmark This work is intended to assist in the recovery of
these variable stars for further study and linkage within other surveys
The metho ds used by the authors in their indep endent identi cation of the variable
stars are describ ed in the rst note of this series Ski Williams a Table gives
precise p ositions and identi cations for the fourth list of variables published by Dahlmark
The table lists the LD name followed by the J p osition and its source
co ded in the table and notes as follows U UA G GSC D measurement
from DSS using UA comparison stars The next two columns give IRAS p oint source
and GSC designations An asterisk in the next column indicates a note at the b ottom of
the table The nal column contains GCVS designations and other names from SIMBAD
Table Dahlmark Variables LD LD
Name RA Dec s IRAS GSC n Other ids
LD G V Cyg
LD U
LD U
LD U
LD U
LD G
LD G
LD D
LD U FBS L
LD G
LD U
LD U
LD U
LD U NSV
LD U
LD D
LD U
LD G
LD U
LD G
LD U
LD G
LD U HL Lac
Table cont
Name RA Dec s IRAS GSC n Other ids
LD G
LD G
LD U
LD D
LD G
LD G
LD G
LD D
LD U
LD U
LD U
LD U NSV
Notes
LD NE comp onent of very close pair blended in GSC SE comp onent has
s 00
end gures : : D
s 00
LD NE comp onent of pair SW comp onent has end gures : : D
LD Sp ectral type M Dolidze
LD Not FK Lac see Williams
LD Faint on POSS I red print R bright in GSC
LD SW comp onent of pair blended in GSC NE comp onent has end gures
s 00
: : D
LD SV R
The authors thank the following for their indisp ensable assistance in completing this
work SIMBAD maintained by the Centre de Donn eesAstronomique Strasb ourg France
and SkyView maintained by Keith Scollick at Go ddard Space Flight Center
Brian A SKIFF
Gareth V WILLIAMS
Lowell Observatory
Harvard Smithsonian Center
West Mars Hill Road
for Astrophysics
Flagsta AZ
Garden Street
U S A
Cambridge MA
e mail bas lowell edu
U S A
e mail gwilliams cfa harvard edu
References
Dahlmark L J AAVSO
Dahlmark L IBVS No
Dolidze M V Byul l Abastuman Astro z Obs
Ski B A and Williams G V a IBVS No
Ski B A and Williams G V b IBVS No
Williams G V IBVS No
Williams G V and Ski B A IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
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March
HU ISSN
CCD PHOTOMETRY OF ECLIPSING BINARY AL OPHIUCHI
h m s
The eclipsing binary AL Ophiuchi GSC
0 00
is a neglected rather faint binary near Oph Its V magnitude given
m
in the Guide Star Catalogue is Unfortunately this variable has not b een studied
photometrically for more than years and the light elements of this system are not given
in the GCVS
Variability of this star with amplitude mag was discovered photographically
by Reinmuth in Heidelb erg The sp ectral type of AL Oph was measured by Bond
and Ti t during their sp ectroscopic survey of some high latitude blue variables
They found a sp ectrum of G Meinunger concluded that AL Oph b elongs to
the W UMa type and the amplitude is to o small for the p erio d determination from the
older photographic measurements Recently the variability of AL Oph was examined on
the plates of the Odessa Observatory by V I Marsakova Andronov and several
weakenings were obtained This star was also measured by Paschke All previous
measurements lead to uncertain conclusions ab out its type and light elements
The present CCD photometry of AL Oph was carried out during nights in the
p erio d from June to November at the Ond rejov Observatory Czech Republic using
a cm re ecting telescop e with a CCD camera SBIG ST in the primary fo cus The
measurements were done using the standard Cousins R lter with exp osure time from to
s Two nearby stars GSC V mag and GSC V mag
on the same frame as AL Oph served as a comparison and check stars Figure Some
of the observations were done through thin clouds The CCD data were reduced using
software developed by P Pravec and M Velen Pravec et al No correction of
relative magnitudes was allowed for airmass due to the proximity of the comparison star
to the variable arcsec Deviations caused by di erential extinction in the broad band
lter for di erent colours of stars should not b e signi cant Due to preliminary p erio d
close to one sidereal day the primary minima were observable only b efore the end of
June On August we obtained a at secondary minimum and fortunately in
November LS observed a part of the descending branch to the primary minimum
The times of minimum and p erio d were determined using a new metho d of iterative
least squares p olynomial tting The metho d for a minimum determination was developed
esp ecially for pro cessing of precise lightcurves with partial coverage of b oth branches
This is a typical result of non automatical CCD observations when several ob jects are
followed and for a particular ob ject we obtain groups of consequent images separated by
large time intervals This metho d should provide also more reliable results in the case
when the number of p oints on each branch di ers We supp ose only the symmetry of the minimum
Figure Finding chart of AL Oph The comparison and check stars are also plotted
Table New times of minimum of AL Oph
JD Hel Error Min O C Ep o ch N
days type days
Pri
Pri
Sec
Similar way of solution double iteration connected with the least squares tting
can b e used for determination of light elements from several night observation We choose
a symmetrical feature on the lightcurve primary minimum estimate p erio d and basic
light minimum Then we t a low order p olynomial like in the case of simple minimum
determination Varying the p erio d we nd a minimum residual corresp onding to the b est
p erio d Using this metho d we can determine the precise value of p erio d in the case of
AL Oph where we have only two primary minima with low accuracy in a short time
interval see Table We derived the following linear light elements for the current use
d
Pri Min HJD E
Observed times of minima are presented in Table In this table N stands for the
number of observations used in the calculation of the minimum time the other symbols
are self explanatory Figure shows the comp osite di erential R light curve during the
summer The light amplitude in R colour for primary minimum according to our
measurement is A mag for secondary minimum we found A
mag The duration of b oth minima seems to b e ab out hours New measurements
of this system are necessary to improve the ab ove given elements
Figure Comp osite di erential R light curve of AL Oph obtained in
Acknowledgment This work has b een supp orted in part by the Grant Agency of
the Czech Republic grant No and by the ESO C EE Programme grant
No A This research has made use of the SIMBAD database op erated at CDS
Strasb ourg France
Lenka SAROUNOVA
Marek WOLF
Astronomical Institute
Astronomical Institute
Academy of Sciences
Charles University Prague
CZ Ond rejov
CZ Praha Sv edsk a
Czech Republic
Czech Republic
Internet lenka asu cas cz
Internet wolf mbox cesnet cz
References
Andronov I private communication
Bond H E Ti t W G PASP
Meinunger L Mitteilungen Ver Sterne
Paschke A private communication
Pravec P Hudec R Sold an J Sommer M Schenkl K H Experimental As
tronomy
Reinmuth K Astronomische Nachrichten
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Number
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March
HU ISSN
HR A LOW AMPLITUDE CEPHEID
h m s 0
HD HR V was chosen as
a comparison star for a study of photometric variations of some Ap stars the results of
which will b e published elsewhere The observations have b een made at La Silla ESO
during a three week run in August with the cm Swiss telescop e equipp ed with
the seven colour double b eam Geneva photometer Since HD was a comparison
star for our initial programme we could not use di erential measurements We had to
rely on absolute data Fortunately these are of high quality in the Geneva system at La
Silla
This bright star is neither in the GCVS nor in the NSVSC It is a standard of the
Geneva system and do es not app ear in Rufener Bartholdi s list of susp ected
variables Neither is it susp ected in variability in the Hipparcos Input Catalogue Turon
et al Hence we were somewhat surprised to nd HR to b e slightly variable
HD190422 P=3.150 t0=2 450 000.00
-0.2 0 0.2 0.4 0.6 0.8 1 1.2
Figure Lightcurves of HD in Geneva s UBV b ottom to top The phase on the horizontal
m
axis is computed with the origin JD Tick marks on the vertical axis are separated by
Renson s p erio d searching algorithm has b een applied to the measure
d d
ments obtained for this star The resulting p erio d is P Figure shows the
measured Geneva V B and U magnitudes plotted vs phases calculated with this value of
P and the time origin The total amplitude has b een estimated by tting a
m m m
smo oth analytical curve through the observations It is ab out and in
V B and U resp ectively All colours vary in phase with a rapid brightening followed by
a slower fading The maximum brightness is reached around phase and the minimum
at
The HD sp ectral type of the star is F which is in p erfect agreement with Johnson s
colour index B V An MK type F V has also b een published Buscombe
The asymmetric shap e of the variation the colour dep endence of the amplitude and
the synchronism of the light curves in all colours p oint toward HR b eing a low
amplitude cepheid On the other hand the luminosity class V disagrees with a cepheid
nature of the star
A con rmation of the origin of the variations would b e obtained by a radial velocity
analysis Because of the small amplitude a high accuracy is needed This is probably
di cult to achieve b ecause of the large value of v sin i km s
M BURNET J MANFROID
ESO
P RENSON
Correo
Institut d Astrophysique
Santiago Chile
Avenue de Cointe
B Li ege Belgium
References
Buscombe W MK Sp ectral Classi cations Third General Catalogue
Renson P A A
Renson P A A
Rufener F Bartholdi P A AS
Turon et al Hipparcos Input Catalogue ESA SP
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HU ISSN
PHOTOELECTRIC OBSERVATIONS OF X PERSEI
X Persei HD is the optical counterpart of X ray transient source U
The system consists of a neutron star secondary accreting from an O I I Ie primary via
stellar wind pro cesses To investigate whether the last fading phase of X Persei b eginning
in is going on we observed the system The present observations were made in John
son s UBV bands with the cm Maksutov telescop e of Ankara University Observatory
In the observations BD was used as comparison star while BD and
BD were chosen as the check stars The magnitude di erences b etween check
stars and comparison star were constant within probable errors of in V band The
individual di erential observations were corrected for atmospheric extinction and light
time e ect of Earth s motion and the V band di erential magnitude determinations were
transformed to the standard system
Since the end of th century X Persei has b een known to b e a variable on a long
time scale Ro che et al presented the most comprehensive optical light curve over
the p erio d During this p erio d the Be star has undergone two extended faint
non variable phases seen in and After this study Zamanov and
Zamanova have observed X Persei in the p erio d Their data are shown
as in the gures and are evaluated together with our data Their observations showed
the optical low state that b egan in the mid nished in the spring of After
this the star has entered the optical high state Our observations b etween see
Table indicate that the brightness of the system decreased again in and the star
was still in a low state during our last observations in Figure
Figure presents the V band light curve over the p erio d Our observations
shown as op en circles have completed the missing data in the vicinity of maximum after
the low state The magnitude at maximum obtained at the end of Octob er
is found of close to the values of the previous maxima Also the current low state is
similar to the previous ones V and only the minimum in is deep er
than others V If these minima are due to the loss of the Be star circumstellar
disk the current low phase must b e asso ciated with a new partial or complete disk loss
state
The B V and U B colour changes are shown in Figures and Although the
observed B V and U B colour index values show a large amount of scatter it is seen
that during the rapid brightening that followed the low state the B V colour
b ecame redder as exp ected At low state the observed U B index is b etween
and This value is consistent with a B star which has a colour excess
E B V given by Fabregat et al During the stage of high luminosity the
observed U B increased to ab out suggesting that the disk radiation contributes to the observed Balmer excess 6.1
6.2 o + o oo 6.3 + + 6.4 + o + ++ + +++ o+o 6.5 o 6.6 o o oo
V magnitude o o o o oo 6.7 o + + ++ + ++ ++ 6.8 + 6.9 48500 48900 49300 49700 50100 50500
HJD (2400000+)
Figure The long term V band light curve of X Persei
0 0.05 + ++ + + ++ 0.1 + + + 0.15 ++ o +++ oo oo 0.2 ++ +++ o oo o + o o
(B-V) 0.25 +++ o o 0.3 o o ooo 0.35 0.4 0.45 48500 48900 49300 49700 50100 50500
HJD (2400000+)
Figure The B V colour changes of X Persei over the past years
-0.9 o -0.85 oo o + oo oo + o o -0.8 + o ++++ o oo o + oo -0.75 + + o + ++++
(U-B) -0.7 ++ + + + ++ -0.65 + -0.6 -0.55 48500 48900 49300 49700 50100 50500
HJD (2400000+)
Figure The U B colour changes of X Persei over the past years
HJD V B V U B
Semanur ENGIN
Kutluay YUCE
Ankara University Observatory
Science Faculty Tando gan
Ankara TURKEY
References
Fabregat J Reglero V Co e M J et al A A
Ro che P Co e M J Fabregat J et al A A
Zamanov R K Zamanova V I Inf Bul l Var Stars No
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HU ISSN
ORBITAL PERIOD OF THE ECLIPSING VARIABLE
V CYGNI
V Cyg HBV was discovered by Wachmann who estimated the p erio d
d d
as n In the GCVS IV Kholop ov et al another p ossible p erio d is
listed We have measured the star on photographic plates of the Odessa Sky Patrol
by using the comparison stars published by Wachmann
For the p erio d search we have used moments of most prominent weakenings HJD
m m
Wachmann
m m
this pap er
We have used the fast algorithm and computer co de describ ed by Andronov
The test function used is the r m s deviation of from where is
the phase of decreased brightness The phase curves were plotted for most prominent
minima at the p erio dogram This visual control allowed us to choose the value of the
p ossible p erio d corresp onding to the th by p erio dogram value minimum The linear
ephemeris for the moments of minima is
M inH J D E
Besides visual analysis we have computed the slow p erio dograms corresp onding to
the metho ds of La er and Kinman and Deeming by using the computer co de
d
written by I L Andronov The optimal value of the p erio d was found to b e P
for b oth metho ds The accuracy estimate is b etter than days the value of the
p erio d shift for which the depth of the minimum at the p erio dogram decreases by
p er cent Naturally smaller error estimate was obtained for the p erio dogram using all
observations instead of moments of used in Eq
m
The light curve is shown in Figure Outside eclipse the r m s scatter equal to
m
is typical of photographic measurements Mean value is is in excellent agreement
m
with the value listed in GCVS The amplitudes of the rst and second harmonics
do not exceed and thus are not statistically signi cant The duration of the eclipse
is P
The scatter of photographic data may mask the secondary minimum at phase the
m m
depth of which do es not exceed As the depth of the primary minimum is
this may argue for a co oler secondary Another p ossibility is that the real p erio d is twice
larger than the value mentioned ab ove In this case the minima may b e of comparable
depths arguing for similar surface brightnesses of b oth stars From the present data we
cannot determine magnitudes at b oth minima with an accuracy needed to nd di erence
d
b etween them Comparing Wachmann s estimate n with the p erio d value
computed in this work one may easily nd that n There is no contradiction
as Wachmann had used dim magnitudes instead of true minima one of which
was marked as unsure Two sure minima were used to determine the p erio d and are in excellent agreement with the given elements
Figure Photographic light curve of V Cyg HBV computed according to the ephemeris
M inH J D E
Assuming the stars are of nearly spherical shap e from the EA classi cation one
may obtain the geometric inequality e g Tsessevich R R a sin
Additionally assuming that b oth stars ob ey the main sequence mass radius rela
tion R R R M M with R Allen one may easily obtain another
inequality
=
=
sin GM P
M M
R R
where is the phase of the rst contact i e half duration of the minimum Equality holds
for the inclination angle i For our data one may estimate M M M for
d d
P and M M M for the hypothesis of double p erio d P
To distinguish b etween these two p erio ds CCD or photo electric photometry in at least
two lters is needed
Acknowledgement The author is thankful to the referee for helpful comments
L L CHINAROVA
Astronomical Observatory
Odessa State University
T G Shevchenko Park
Ukraine Odessa
ro ot astro o dessa ua
References
Allen C W Astrophysical Quantities London Athlone Press
Andronov I L Kinem Fiz Nebesn Tel No
Andronov I L Odessa Astron Publ
Deeming T J M N R A S
Kholop ov P N et al General Catalogue of Variable Stars IV th Edit Moscow
Nauka Publ
La er J Kinman T D Ap J Suppl
Tsessevich V P Peremennye Zvezdy i ih Nabludenie in Russian Moscow Nauka
Wachmann A A Berged Abh No
COMMISSIONS AND OF THE IAU
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Number
Konkoly Observatory
Budap est
March
HU ISSN
PHOTOELECTRIC VI OBSERVATIONS
c
AND NEW ELEMENTS FOR V CARINAE HR
Arellano Ferro analyzed observations of V Car HD HR the
brightest member of sp ectral type A Ia O Turner see also references cited by
Arellano Ferro of the young cluster IC and found four p ossible p erio ds in
its p ower sp ectrum and days He noted that a p erio d of
days provided the b est match of his observations to those supplied by Madore
In an attempt to up date the ephemeris for the star we observed it at CTIO in
September November using the m re ector A total of VI measurements
c
m
were obtained the accuracy of the individual data b eing near in b oth lters The
observations are listed in Table
The mean magnitudes of Arellano Ferro s as well as Cousins observations
were coincidenced with our V band data in order to increase the sample available for a
p erio d search We derived the following elements
Max JD E
hel
Those elements are used in Figure for plotting the light curve in V where our
observations are identi ed by large circles and observations published by Arellano Ferro
and Cousins are denoted by small circles and dots resp ectively The shorter
p erio d found here app ears to b e supp orted by the rapid change in brightness of the star
detected over our observing season
Table
JD V V I JD V V I
hel c hel c
V V399 Car P=47.25 4.63
4.70
0.0 0.5 1.0 Phase
Figure
As a member of the cluster IC HR has an estimated luminosity of M
V
Turner placing it in the regime of the hypergiant stars It is of interest to
note that at the p erio d found here HR falls almost exactly on the p erio d luminosity
relation for pulsating B and A type sup ergiants published several years ago by Maeder
Rufener see also Burki
The research describ ed here was made p ossible in part by grants No and
No from the Russian Foundation of Basic Research to LNB and through
NSERC Canada to DGT The authors were Visiting Astronomers at Cerro Tololo Inter
American Observatory National Optical Astronomy Observatories which is op erated
by the Asso ciation of Universities for Research in Astronomy Inc AURA under co
op erative agreement with the National Science Foundation
L N BERDNIKOV
Sternberg Astronomical Institute
Universitetskij prosp
Moscow Russia
D G TURNER
Saint Mary s University
Halifax Nova Scotia B H C
Canada
References
Arellano Ferro A P A S P
Burki G Astron Astrophys
Cousins A W J Roy Obs Bul l No E
Madore B F unpublished
Maeder A Rufener F IAU Symp No
Turner D G Astron J
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Number
Konkoly Observatory
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March
HU ISSN
VARIABLE STARS IN THE GLOBULAR CLUSTER NGC
M NGC C is lo cated close to the galactic center l b
This rather metal rich cluster Fe H Zinn West b elongs to the
0
concentration class CC IV its apparent radius is r Kukarkin and the tidal
0
radius Webbink M is rich in variables variables were discovered in
the cluster Sawyer Hogg p erio ds are de ned for of these stars Twelve of
them are classi ed as RRc and as RRab variables Values of P N N con rm the
ab c ab
classi cation of the cluster as OoI variable rich one
Table Positions and photometric data for susp ected variables
N X Y V B N X Y V B
SH SH SH SH
arcsec arcsec arcsec arcsec
Figure The color magnitude diagram for the globular cluster NGC corrected for di erent
reddening the known RR Lyrae stars are denoted by circles susp ected variables are marked by squares
Figure Finding chart for NGC The known RR Lyrae stars are denoted by circles and by their number from the catalog of SH susp ected variables are marked by squares
This study is based on CCD observations Bro cato et al We used the same
metho d of search for RR Lyrae variables as Kadla et al In the investigation area
0 0
there are known variables The identi cation of V and V was made
using co ordinates of SH catalog only They were not marked on Plate of Van Agt and
Oosterho since the stars are situated in the crowded central part of the cluster
Variables V V and V are brighter than the other variables In order to eliminate
errors due to crowding of the central part of the cluster we have not considered the region
0
of the cluster center r
The di erential reddening across the cluster eld Van Agt and Oosterho causes
an additional di culty for the investigation of this cluster
The colour magnitude diagram after correction for di erential reddening is shown in
Figure Apart from known variables there are stars in the instability strip
All data for susp ected variable stars are given in Table The co ordinates of stars in
arcseconds in the system of SH s catalog and the maxima of magnitude variations B
and V during our observations are listed in columns of Table In Figure and in
the nding chart Figure the known and susp ected variables are marked by circles and
squares corresp ondingly
Because of its p osition in Figure we supp ose that V is a red giant The stars V
V and V seem to b e eld variables
We are grateful to the Russian Foundation for Basic Research for nancial supp ort
Yu N MALAKHOVA
A N GERASHCHENKO
Z I KADLA
Central Astronomical Observatory of
the Russian Academy of Sciences at
Pulkovo Saint Petersburg
Russia e mail mal pulkovo spb su
References
Bro cato E Buonanno R Malakhova Yu Piersimoni A M A A
Kadla Z I Gerashchenko A N Malakhova Yu N IBVS No
Kukarkin B V The General Catalogue of Globular Clusters of our Galaxies Pub
lishing House Nauka Moscow
Sawyer Hogg H Publ David Dunlap Obs No SH
Van Agt S Oosterho P Th Leiden Ann
Webbink R F IAU Symp osium No eds by J Go o dman P Hut Reidel
Dordrecht
Zinn R West M J ApJSS
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
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March
HU ISSN
NEW VARIABLE STARS IN THE NORTHERN MILKY WAY
h m
The following is an evaluation of a area centered at
in my series of Milky Way elds Four elds have b een previously describ ed Dahlmark
Nineteen plate pairs Ko dak aD GG and aO were exp osed b etween
and and forty four were exp osed on Ko dak TechPan GG lter in the
years to Ten plate pairs were examined using a blink comparator as well as
four stereo comparators in the metho d describ ed by Dahlmark Magnitudes
for the comparison stars were taken from the Guide Star Catalogue GSC
In this eld variables were found of which app ear to b e new Table shows p o
sitions and identi cations The co ordinates were extracted from either the GSC source
co de G the U S Naval Observatory A catalogue co de A or using the Go ddard
SkyView facility co de S Scollick The lightcurves are based on magnitude esti
mates for each star From them the magnitude range colour index provisional variability
type ep o ch of maximum and p erio d have b een determined These are collected in Table
An asterisk next to the star name indicates a note at the b ottom of the table
The nding charts are based on mm Schmidt camera photographs taken
when the variable stars were at maximum light
Table Positions and identi cations LD
Name RA Dec s GSC IRAS Remarks
LD A
LD A
LD A
LD A
LD A
LD A
LD A StRS
LD A
LD A
LD A
LD A
LD A
LD A
LD A
LD A
LD A
LD A
LD G
LD A see note
LD A
LD A
LD A
Table Positions and identi cations LD cont d
Name RA Dec s GSC IRAS Remarks
LD A
LD G
LD A
LD A
LD G
LD A
LD G
LD A CGCS
LD S
LD A CGCS
LD A
LD A
LD A
LD A
LD A
LD S CGCS
LD A
LD A
LD A
LD A CGCS
LD A P
LD A
LD A
LD A
LD A
LD A
LD A GY Lac
LD A
LD A
LD A
LD A
LD A
LD A
LD S
LD G
LD A see note
LD A CGCS
LD S see note
LD A
LD A
LD A see note
Notes to Table
LD CGCS also Cl Berkeley SSWZ from Saurer et al
from plates on ve nights and CCD frames on two nights they nd
< V < B V
LD V Cas GCVS p osition error ID veri ed on MVS no
LD sp ectral type M Dolidze
LD IRC TASV J Collins
Figure
Figure
Table Elements of variation LD
Name max min mb mv type ep o ch p erio d
mv JD days
LD SRa
LD M
LD > SRa
LD SRa
LD SRa
LD SRa
LD SRa
LD > Lb
LD > L
LD > SRa
LD Lb
LD > SRb
LD SRb
LD Lb
LD > M
LD > > M
LD > M
LD M
LD > Lb
LD M
LD SRa
LD M
LD M
LD > SRb
LD > M
LD SRa
LD Lb
LD > Lb
LD > Lb
LD SRb
LD M
LD > M
LD > M
LD > M
LD > SRa
LD > Lb
LD L
LD > > M
LD > M
LD L
LD Lb
LD SRb
LD > M
LD > M
LD > M
LD M
Table Elements of variation LD cont d
Name max min mb mv type ep o ch p erio d
mv JD days
LD M
LD > > M
LD > L
LD M
LD > SR
LD > M
LD > > SR
LD > M
LD > M
LD > L
LD SR
LD > SR
LD M
LD M
Notes to Table
d
LD p erio d variable
d d d
LD p erio d decreasing
d
LD p erio d unstable
d
LD p erio d variable
d d d
LD p erio d decreasing
d d d
LD p erio d decreasing
d d
d d d
LD p erio d increasing
I would like to thank Brian Ski Lowell Observatory for helping me nd accurate
p ositions and the identi cations of my stars from various catalogues
Lennart DAHLMARK
Montlaux
F St Etienne les Orgues
France
References
Collins M The Astronomer
Dahlmark L IBVS No
Dahlmark L IBVS No
Dahlmark L IBVS No
Dahlmark L IBVS No
Dolidze M V Byul l Abastuman Astro z Obs
Saurer W Seeb erger R Weinberger R and Ziener R Astron J
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced pl
COMMISSIONS AND OF THE IAU
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Number
Konkoly Observatory
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March
HU ISSN
IDENTIFICATIONS FOR BAADE S VARIABLES
IN SAGITTA AND CYGNUS
The tables b elow show identi cations and precise p ositions for a group of variables
found by Walter Baade during his Bergedorfer days The stars rep orted in this
survey are of some historical interest b ecause it was as a result of this work that Baade
conceived ideas that led to his later recognition of the two stellar p opulations among
Galactic stars cf Osterbro ck
The pap er is one of the few variable star surveys where precise p ositions are supplied
for equinox so checks and identi cations were easy to make in mo dern catalogues
I examined each star on the digitized sky survey using the Go ddard SkyView facility
00
Scollick Baade s original p ositions in his Table are very go o d all less than
00
from FK system p ositions and often within In the Cygnus eld Table they are
00
somewhat less go o d but still within ab out : In either case making identi cations on
the sky is unambiguous despite the absence of nder charts Follow up lightcurves and
photometry of comparison stars with nding charts for several of Baade s short p erio d
variables can b e found in Henden and Schmidt Seth
The stars are listed in the same order as in Baade s tables The rst column shows
the provisional Kiel designation used in the Astronomische Nachrichten Baade did
not give all of these Next comes the prop er variable star name taken directly from the
machine readable version of volume of the GCVS available from the Strasb ourg CDS
ftp service N B the mix of O s and Q s among the names in Table Since few of the
stars app ear in the GSC I have by preference extracted p ositions from the U S Naval
Observatory UJ star catalogue Monet et al a or the more comprehensive A
catalogue Monet et al b The few remaining p ositions were taken directly from
00
Baade or estimated to using SkyView The source of the p osition is co ded as follows
A A B Baade S SkyView U UJ
Table Baade s variables in Sagitta
Provis desig Name RA Dec s GSC IRAS n
AN SZ Sge U
AN NSV U
AN NSV U
AN EI Sge U
AN NSV U
AN NSV U
AN FX Sge U
AN TX Sge U
AN NSV U
AN TU Sge U
AN NSV U
AN Y Sge U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
Table Baade s variables in Sagitta cont d
Provis desig Name RA Dec s GSC IRAS n
AN NSV U
AN NSV U
AN NSV U
AN RR Sge U
AN NSV U
AN DO Vul B
AN SY Sge U
AN RX Sge U
AN DW Sge U
AN RS Sge U
AN NSV A
AN NSV U
AN Z Sge U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN TW Sge A
AN NSV U
AN AP Sge U
AN DP Vul U
AN NSV A
AN NSV U
AN NSV U
AN NSV U
AN U
AN NSV A
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV B
AN NSV U
AN VW Sge U
AN NSV U
AN NSV U
AN NSV B
AN NSV U
AN RW Sge U
AN VV Sge U
AN TT Sge U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN NSV U
AN SX Sge A
Notes to Table
SY Sge HD LS I I
DO Vul no star on DSS precisely at Baade s p osition The Downes Shara dwarf nova
s 00
atlas identi es this as the northwestern star of a faint pair at p osition end gures :
The identi cation is uncertain however since there have b een no outbursts rep orted in
the mo dern literature
NSV BSNS
AN NGC V Cl NGC ZDA
00
NSV equal pair on DSS resolved in UJ Baade s p osition is close to the mean of
the two which was adopted
NSV evidently the southwestern star of a merged pair on DSS The p osition from Baade
00
given by Richter Greiner is in error by they identify the northeastern star
of the pair as the variable
NSV excellent IRAS p osition match but the color is relatively blue
Table Baade s variables in Cygnus
Provis desig Name RA Dec s GSC IRAS n
AN PU Cyg U
AN QZ Cyg U
AN QX Cyg U
AN PR Cyg U
AN OV Cyg U
AN OP Cyg U
AN PT Cyg A
AN V Cyg U
AN V Cyg A
AN OY Cyg U
AN FZ Cyg U
AN V Cyg A
AN GK Cyg U
AN NQ Cyg A
AN QQ Cyg U
AN V Cyg U
AN GM Cyg U
AN V Cyg U
AN GL Cyg U
AN QW Cyg U
AN OZ Cyg A
AN NV Cyg U
AN NS Cyg U
AN NSV U
AN NW Cyg B
AN NY Cyg U
AN PV Cyg U
AN OT Cyg U
AN OW Cyg U
AN NSV U
AN QU Cyg A
AN V Cyg A
AN OQ Cyg U
AN QT Cyg U
AN V Cyg U
AN NSV U
AN PZ Cyg U
AN PY Cyg U
AN QR Cyg U
AN CV Cyg U
AN QS Cyg U
AN OU Cyg U
Table Baade s variables in Cygnus cont d
Provis desig Name RA Dec s GSC IRAS n
AN OX Cyg U
AN QY Cyg U
AN NX Cyg U
AN PS Cyg U
AN OS Cyg U
AN V Cyg U
AN NSV U
AN PW Cyg U
AN NT Cyg B
AN PP Cyg A
AN NN Cyg U
AN OO Cyg U
AN PQ Cyg U
AN V Cyg U
AN NSV U
AN NR Cyg U
AN V Cyg U
AN V Cyg U
AN NO Cyg U
AN NP Cyg U
AN QV Cyg U
AN NZ Cyg U
AN NU Cyg U
AN OR Cyg U
AN PX Cyg U
Note to Table
QZ Cyg BD
I used SIMBAD to lo ok for the GSC and IRAS identi cations Additional remarks are
indicated by an asterisk and given following the tables
I am grateful to G erardJasniewicz Universit ede Montpellier who p ointed out several
typos in an early version of this list Taichi Kato Kyoto University provided comments
on DO Vul
Brian A SKIFF
Lowell Observatory
West Mars Hill Road
Flagsta AZ
USA
e mail bas lowell edu
References
Baade W Astron Nach
Downes R A and Shara M M Publ Astron Soc Pac
Henden A A Astron J
Monet D G et al a USNO UJ U S Naval Observatory Washington DC see
also http www usno navy mil pmm
Monet D G et al b USNO A V U S Naval Observatory Washington DC
see also http www usno navy mil pmm
Osterbro ck D E Journ Hist Astron
Richter G A and Greiner J IBVS No
Schmidt E G and Seth R Astron J
Scollick K http skview gsfc nasa gov cgi bin v skyview advanced pl
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HU ISSN
ON THE NAME OVER CONTACT BINARY SYSTEMS
During the recent years a new name of a group of binary stars seems to have app eared
These are over contact binaries The name is clear and p ersuasive in its content Since
contact binary stars exists the new name implies existence of binary stars that are in
b etter or more contact than ordinary contact systems In this note I would like to
express the opinion that the name is currently b eing used incorrectly and that it should
b e reserved for p ossible cases of genuine over ow of the outer critical equip otential surface
The name in question has b een surfacing from time to time in the literature but has
b een particularly frequently used recently in the IBVS A brief lo ok at the titles starting
with the issue number and continued to the most recent available number shows
that it has b een used in ve instances issues numbers In
all these cases normal contact binaries of the W UMa type are describ ed Not a single
case indicated over ow through the external Lagrangian p oint L arguably a reason to
2
call a system an over contact one
The basic groups of close binary stars have b een discussed and de ned by Kopal
in his monumental b o ok They have b een divided into detached semi detached and
contact systems according to the relation to the critical equip otentials passing through the
inner critical p oint L These p otentials known also as Ro che lob es although invisible
1
and not material act as lips dividing the connected vessels cf Pringle Fig The
group of contact binaries was de ned clearly by Kopal Sec VI I as systems lling
the common envelope encompassing b oth stars The observationally de ned group of
W UMa type eclipsing binaries was equated there with the theoretical concept of contact
binaries i e binaries whose surfaces are describ ed by p otentials intermediate b etween
those that pass through the critical Lagrangian p oints L and L
1 2
The meaning of the contact systems has gained a real solid basis after the two seminal
pap ers by Lucy a b who showed that single structures with two mass centres
can exist and can pro duce light curves exactly as those of the W UMa type Since then
a large b o dy of literature on contact binary stars has app eared The name of W UMa
type systems has attained the status of an op erational de nition of contact binaries with
orbital p erio ds shorter than one day which consist mostly of solar type stars whereas the
name of early type contact binaries is used for rare systems with orbital p erio ds longer
than one day
Apparently the new name originated through the incorrect application of the name
contact to describ e the relation of a star to its equip otential surface Thus the phrase
to b e in contact has b een sometimes used to describ e that the surface of a star is in
contact with the particular critical equipotential corresp ondingly the comp onent lling
its Ro che lob e would b e then called a contact comp onent This usage is illustrative
but carries a danger that it may lead to misunderstanding the equip otential is not a solid
surface in space and there is nothing to b e in contact with Whereas stars in a binary
system can b e in contact a single star cannot really b e in contact with a non material surface
The new name of over contact seems to have originated through a logical step further
to describ e the cases when the stellar surfaces are lo cated outside the inner critical or
Ro che lob e surfaces Here I would like to argue that in such situations the star
either slightly over lls its critical equip otential and then is part of a semi detached
system or forms a structure describ ed by a common equip otential e ectively making it
to b e in contact with the other comp onent
I prop ose that the name contact binary b e used to describ e systems which ll the
common equip otentials and form single b o dies with two mass centres and that the name
over contact b e reserved for so far undetected cases of genuine over ow of the contact
con gurations Such may exist probably brie y but their discovery would b e of immense
imp ortance for our understanding of the the angular momentum loss evolution which for
many close binaries carries them through the successive stages of detached semi detached
contact binary systems and then at the end through a brief stage of over contact to
single stars In light of this more rigorous de nition a claim that we know over contact
systems is certainly an over statement
I would like to thank Hilmar Duerb eck and Carla Maceroni for supp orting me with
the idea of publishing this note
S M RUCINSKI
David Dunlap Observatory
P O Box Richmond Hill
Ontario Canada L C Y
e mail rucinski astro utoronto ca
References
Kopal Z Close Binary Stars Chapman Hall Ltd
Lucy L B a ApJ
Lucy L B b ApJ
Pringle J E in Interacting Binary Stars eds J E Pringle R A Wade Cam
bridge Univ Press p
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HU ISSN
UBV OBSERVATIONS OF T CrB
T Coronae Borealis is a sp ectroscopic binary with a p erio d of days containing
an M giant and a hotter companion The star has exp erienced two outbursts with an
amplitude of ab out mag in and and is classi ed as a recurrent nova as well
as a symbiotic star The ultraviolet observations and the b ehaviour of the star during
the outbursts p oint to the hotter comp onent is an white dwarf with a mass close to the
Chandrasekhar limit Selvelli Cassatella and Gilmozzi in spite of the existence of
some doubts that it can b e a main sequence star e g Kenyon and Garcia The M
giant lls the Ro che lob e and the main part of the accretion is realized through the L
UBV observations of the recurrent nova T CrB were carried out with a single channel
photon counting photometer mounted at the m telescop e of the National Astronomical
m m
Observatory Rozhen The comparison star was HD V B V
m
U B The data was pro cessed using the APRN software Kirov et al
The accuracy is b etter than mag Our observations are summarized in Table
The long term photometry in the U band is presented in Figure The triangles
indicate our data the circles denote the data from Hric et al and
Skopal et al the crosses denote the data of Mikola jewski et al
From Figure it is visible that since TCrB has exp erienced three small outbursts
with an amplitude of mag in the U band and p eaks at JD JD and
JD The typical time b etween these mini outbursts is of ab out days Since
the star has shown a considerable increase in the U brightness It is interesting to
note that UV ux observations of Selvelli Cassatella and Gilmozzi over the p erio d
do not show similar b ehaviour They had observed only two minima in and
In the V band as well as in the IR see Yudin and Munari and references therein
TCrB shows a double wave light curve as a result of the ellipsoidal shap e of the M giant
In Figure the V data are shown using the ephemeris of Kenyon and Garcia
The dots refer to the data obtained b efore Lines et al Ra jkova and Antov
and Bruch The other symbols are the same as in Figure A Fourier
analysis of the data using a three term truncated Fourier series yields
V cos cos cos
sin sin sin
where is the orbital phase This t is also plotted in Figure Although the data spread
over years a distinction b etween the observations obtained in di erent ep o chs is not
visible This p oints to the fact that the V light curve has not changed in its main features
over the last years
Figure U band light curve of T CrB
Figure Phase plot of the V data according to
the orbital ephemeris of Kenyon and Garcia
Most of the radiation ux in the U is emitted from the hotter comp onent The el
lipsoidal variations are suggestive of a large orbital inclination but an eclipse cannot b e
detected in the UV ux Selvelli et al We also fail to detect eclipse in the U band
The U magnitudes of TCrB do not show correlation with the orbital p erio d It is worth
noting that the eccentricity of the system is practically zero Kenyon and Garcia
so the lack of connection with the orbital p erio d is not surprising
We ascrib e the variability in the U band to the accretion disk and or the b oundary
layer b etween the disk and the white dwarf In our opinion the most likely reason for the
observed variability is the changes in the mass transfer rate and or in the structure of the accretion disk
Table Photometric observations of T CrB
JD V B V U B JD V B V U B
This work was supp orted by NSF F
R K ZAMANOV
NAO Rozhen POB
Smoljan Bulgaria
e mail rozhen tu plovdiv bg
V I ZAMANOVA
Planetarium POB
Smoljan Bulgaria
References
Bruch A IBVS No
Bruch A A A
Kenyon S J Garcia M R AJ
Kirov N K Antov A P Genkov V V Compt rend Acad bulg Sci
No
Lines H C Lines R D McFaul T G AJ
Mikola jewski M Tomov T Kolev D IBVS No
Hric L Skopal A Urban Z et al Contr Astr Obs Skalnat e Pleso
Hric L Skopal A Urban Z et al Contr Astr Obs Skalnat e Pleso
Hric L Skopal A Cho chol D et al Contr Astr Obs Skalnat e Pleso
Ra jkova D Antov A IBVS No
Selvelli P L Cassatella A Gilmozzi R ApJ
Skopal A Hric L Urban Z et al Contr Astr Obs Skalnat e Pleso
Skopal A Hric L Cho chol D et al Contr Astr Obs Skalnat e Pleso
Yudin B Munari U A A
CORRIGENDA
In the No issue of the IBVS Figure is erroneously the rep etition of Figure The correct
version of Figure is as follows
Figure T CrB H pro les in The equivalent width and orbital phase are written in each b ox
The hardcopy of IBVS No has b een distributed in an incomplete form the last three
references page are missing The references cut o the end of the pap er are as follows
Krisciunas K Crowe R A Luedeke K D and Rob erts M MNRAS
Krisciunas K and Handler G IBVS No
Mantegazza L Poretti E and Zerbi F M MNRAS
a
The electronically accessible versions b oth L T X and PostScript contain the complete pap er
E
The Editors
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
A FLARE EVENT DETECTED IN THE ECLIPSING BINARY CM Dra
d
CM Dra is an eclipsing binary with the p erio d of : and the inclination angle
of : Lacy It is a very interesting ob ject by two facts First it has b een
currently known as a main sequence eclipsing double lined sp ectroscopic binary with the
lowest mass M and M Metcalfe et al Therefore it o ers an excellent
opp ortunity to test the structure and evolution mo del of very low mass stars Metcalfe et
al Chabrier Bara e Second a planetary o ccultation with a p erio d ab out
d
or a submultiple of it was rep orted in this eclipsing binary system Guinan
Martin and Deeg
In this pap er we present the detection of a are event from the BVI di erential pho
tometry p erforming as a part of the TEP Transits of Extrasolar Planets international
collab oration Martin et al Time series CCD photometry of CM Dra has b een
carried out for eight nights from January to March Table The observations
were made with a TEK CCD camera attached to the m telescop e at Bohyunsan
0
Optical Astronomy Observatory BOAO The eld of view on the CCD image is :
0
: at the f Cassegrain fo cus of the telescop e The exp osure times were sec sec
and sec for B V and I lters resp ectively
The prepro cessing of CCD images including the overscan correction the trimming of
unreliable subsection the bias correction and the at eld correction was made with the
IRAF CCDRED package We adopted simple ap erture photometry to obtain instrumen
tal magnitudes using the IRAF DAOPHOT package Massey Davis and applied
the classical two star di erential photometry to get di erential magnitudes Two compar
m m m m
ison stars V : B V : for C V : B V : for C from our observation
near CM Dra were monitored to check the light variability of CM Dra Figure The
detailed analysis of light variations Figure for CM Dra will b e given in elsewhere Kim
et al
Table Observation Log
Obs Date Start H J D Obs Time Airmass Phase Seeing
h 00
Jan : :
Feb
Mar
Figure Finding chart of CM Dra Two comparison stars are denoted as C and C
Peculiar light variations of CM Dra were observed on February J D
m m
from phase to The brightness increased up to ab out : in B and : in V
relative to the normal out of eclipse value This is unlikely to b e due to the atmospheric
di erential extinction b ecause the di erences in the airmass among three stars are neg
m m
ligible and their color di erences B V : and B V : are not
V C C C
so large Considering the brightness change within short time scale of hours and the
strong amplitude dep endence on colors it might b e a are as commonly detected in the
late type dwarfs dMe for CM Dra
An ultraviolet are of CM Dra was initially observed by Eggen Sandage on
m m
June Its brightness increased by : in U and U B color changed from :
m
to : on short time scale min during the increase of light after mid eclipse By
carrying out the BVRI high sp eed photometry and di erential I photometry to detect
are events of CM Dra Lacy found only a single are on May From
this he estimated the are rate ab out less than p er hour which is much to o low in
contrast to that of classical Pop I are stars with similar luminosity ares hour
Lacy et al He suggested that biased on the abnormally low are rate and the high
space velocity of km sec CM Dra might b e an evolved system Pop I I comp osition
Metcalfe et al also detected a single are event from the sp ectra of CM Dra In six
exp osures started from J D the emission lines of the primary were observed
to b e very strong
-1.0
B
-0.5
V
0.0
I
0.5
1.0
B
V 0.5 0.0 0.5 1.0
Phase
Figure Light variations of CM Dra A are event was observed on Feb from
m m
phase to The brightness increased by : in B and : in V
Table Flare events of CM Dra
Date J D Phase Duration Characteristics Flare rate Ref
h m
June eclipse : : increased in U
m
: increased in I hour
strong emission lines hour
m m
: : increased in B V hour
Ref Eggen Sandage Lacy Metcalfe et al This pap er
The characteristics of four are events which have b een detected in CM Dra are listed
in Table The ultraviolet ares of CM Dra might o ccur in any orbital phase The
brightness during a are event abruptly increased and decreased on very short time scale
of a few minutes two p oints of B at the phase of in Figure Then its intensity
decreased slowly continuing for hours Flare rate estimated in this pap er is
ares p er hour which is consistent with the other data This low are rate supp orts
Lacy s suggestion that CM Dra might b e a Population I I star
S L KIM M Y CHUN W B LEE
L DOYLE
Korea Astronomy Observatory
SETI Institute
Taejon
NASA Ames Research Center
Korea
Mo ett Field California
e mail slkim seeru b oao re kr
USA
References
Chabrier G Bara e I ApJ L
Eggen O J Sandage A ApJ
Guinan E IAUC No
Kim H I Kim S L Chun M Y Lee W B in preparation
Lacy C H ApJ
Lacy C H Mo ett T J Evans D S ApJS
Martin E L Deeg J IAUC No
Massey P Davis L E A User s Guide to Stel lar CCD photometry with IRAF
Metcalfe T S Mathieu R D Latham D W Torres G ApJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
A NEW SUSPECTED VARIABLE IN PISCES
We rep ort here of the nding of few brightenings of a star in the neighbourho o d of
the irregular variable RZ Piscium We b ecame aware of this b ehaviour during brightness
estimates of RZ Psc on sky patrol plates of the plate stacks of the Harvard College
Observatory Cambridge MA U S A
The presumed new variable was visible on only few plates Normally the magnitude of
the ob ject in question was b elow the limiting magnitude of the sky patrol plates
Figure Identi cation map for the presumed variable Y in the neighbourho o d of RZ Psc RZ
Comparison stars are marked to o Their B magnitudes are listed in Table The map covers an area of
North is on the top and east to the left The map is based on a B plate obtained by R Ziener
KSO Tautenburg
Plate aws can b e practically excluded as an explanation for the sp oradically app earing
ob ject since we found at the exact p osition of it a faint star on a CCD image taken with the
cm telescop e of the Gro schwabhausen GSH observing station of the Jena University
Observatory Indep endently we identi ed the star on prints of the Palomar Observatory
Sky Survey as well as on Schmidt plates in the plate archive of the Karl Schwarzschild
Observatory KSO Tautenburg
Table B magnitudes of the comparison stars
Comparison B Comparison B
star mag star mag
a
b
c
d
f
x
Table Brightnesses of star Y
Julian Date Brightness Remarks
mag
Harvard Obs B
Harvard Obs B
Harvard Obs B
Harvard Obs B
KSO Tautenburg B
KSO Tautenburg V
KSO Tautenburg R
KSO Tautenburg B
GSH CCD B
The identi cation map Figure covers only a part of that map for RZ Psc published
by Friedemann et al In the map presented here the ob ject in question RZ Psc
and the comparison stars are marked Their B magnitudes have b een derived on the
blue CCD images obtained by us using photometric standard stars measured by Pugach
and Kovalchuk and Wenzel The relevant photometric data are compiled
in Table The mean r m s error amounts to mag
The data of the few discovered brightenings are collected in Table The estimated
photometric uncertainties amount to m mag
Additional information have b een obtained by measuring the brightness of the star on
B V and R plates of the KSO For this aim we used for the comparison stars B and R
magnitudes from the USNO SA catalogue by Monet et al and V from the Guide
Star Catalog From the three KSO plates obtained at JD we derived
B V and R magnitudes amounting to and resp ectively Combination of
the B V and R data results in a colour index B V mag and V R mag
These values corresp ond to an unreddened star of sp ectral type F to F
Taking the brightenings found see Table as representative the amplitude of the light
variation amounts to m mag The amplitude derived from the few existing
B
photometric data and the distribution of the brightenings over the time are compatible
with the assumption that the variable probably b elongs to the class of U Geminorum stars
Acknowledgement The authors are indebted to Dr I Shapiro Director of the Har
vard College Observatory for the p ermission for using the plate collection and Dr Martha
Hazen Curator of the plate Collection for her kind supp ort and hospitality during their
stay Furthermore the authors thank Dr R Ziener from the KSO Thueringer Lan
dessternwarte Tautenburg for making the Schmidt plates available to them and Dr S
Klose for scanning these plates The work was partially supp orted by the Deutsche
Forschungsgemeinschaft Grant Fr
H G REIMANN
C FRIEDEMANN
Astrophysikalisches Institut und
Unversit ats Sternwarte Jena
Schillerg a chen
Jena Germany
e mail rei astro uni jena de
References
Friedemann C G urtler J Reimann H G A A
Guide Star Catalog Asso ciation of Universities for Research in Astronomy Inc
Monet D Bird A Canzian B Harris H Reid N Rho des A Sell S Ables H
Dahn C Guetter H Henden A Leggett S Levison H Luginbuhl C Martini
J Monet A Pier J Riep e B Stone R Vrba F Walker R USNO
SA edited by U S Naval Observatory Washington DC
Pugach A F Kovalchuk G U Perem Zvesdy
Wenzel W Private communication
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
DETECTION OF FAST FLARES OF EV Lac IN
Spiky type very short ares of a duration less than sec of some are stars have
b een detected Zalinian Tovmassian Tovmassian Zalinian by observations
made with the two channel U and B fast photometer of the Byurakan Astrophysical
Observatory Zalinian Tovmassian Fast ares of a total duration of a few seconds
or less have b een found also by Tsvetkov et al and Shvartsman et al
In the present contribution we rep ort on the results of the monitoring of EV Lac that
was carried out with the cm telescop e of the Byurakan Observatory in with
somewhat mo di ed mo de of observations In the present observations the monitoring was
done as b efore with sec integration time but counts in U and B were recorded with
an integration time of sec until the current count in U jump ed ab ove the mean value
of the preceding hundred counts by Then the signal in b oth channels was recorded
with sec integration time Hence the fast spiky type ares were recorded with sec
integration time whilst the relatively slowly rising usual ares were recorded with sec
integration time After each min the star was moved out from the diaphragm and
the sky background was recorded for sec In these observations b oth comp onents of
the double fell in the diaphragm of the photometer As usually in the case of observations
of are stars the U and B magnitudes were determined by the ratio I I where I is the
0 0
intensity of the star in its quiescent state Since observations were done simultaneously
in U and B we measured also U B values for the star during the are
Observations were done during hours Twelve ares were detected The total dura
tion of half of them is less than sec In consecutive columns of the Table the following
data on the detected ares are presented date of observation UT at the maximum of the
are designation of separate maximums s for relatively slow ares U and B mag
nitudes of the are U B color of the star at the are maximum rising time tr of the are
in seconds and total duration of the are In deducing the parameters of the detected
ares we accepted the following photometric data for EV Lac AB V B V
U B Mo et The U amplitudes and U B colors of ares were estimated
by using the light curves of ares smo othed by medians
Light curves of some ares are shown in Figures In Figure a the light curve
integrated in sec is shown The record of the short are that o ccurred after the main
one is shown in Figure b with an integration time of sec
We would like to draw attention that very short spiky ares of a total duration less
than sec seem mainly to o ccur shortly after the longer lasting ares
Figure Figure
Figure a Figure b
Table Data on ares of EV Lac
Date UT max Peaks U B U B t Duration
r
h m sec
Aug s m
a s
Aug s
Aug s
Aug s
Aug s m
Aug a s
b s
Aug s m
a s
Sep a s
b s
Not certain
VPZ is grateful to CONACYT for nancial supp ort by the Pro ject P E
during the reduction of observational data
V P ZALINIAN
Byurakan Astrophysical
Observatory of the Armenian
National Academy of Sciences
H M TOVMASSIAN
Instituto Nacional Astrophysica
Optica y Electronica
Puebla
Mexico
References
Mo et T J ApJ Suppl
Shvartsman V F Beskin G M Gershberg P E Neizvestni S I Plakhotenkova V L
Pustilnik L A Izv Crimean AO
Tovmassian H M Zalinian V P Astro zika
Tsvetkov M K Antov A P Tsvetkova A G Comm Konkoly Obs Hung Acad
Sci No
Zalinian V P Tovmassian H M IBVS No
Zalinian V P Tovmassian H M Contr Byurakan Obs
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
OBSERVATIONS OF FLARE STARS EV Lac V Mon AND YZ CMi
Observations of some are stars made with the cm telescop e of the Byurakan As
trophysical Observatory by using the two channel U and B fast photometer Zalinian
Tovmassian with sec integration time allowed to detect very short ares of a
duration of a few tenths of a second with rising times of sec or p erhaps less Zalinian
Tovmassian Tovmassian Zalinian Short ares of an order of a few seconds
were detected also by Tsvetkov et al and Shvartsman et al
In this communication we present the results of observations of are stars EV Lac V
Mon and YZ CMi made with the two channel photometer of the Byurakan Observatory
Observations were made with the m telescop e of the IA UNAM in Tonantzintla in
November and December and with the m telescop e of the INAOE in Cananea
in December and January Mexico Two photomultipliers EMI AQ were
used in the photometer
Dep ending on the size of the telescop e and on the observing conditions night sky
brightness brightness of the Mo on di erent integration times of and sec
have b een used In each min the sky background was recorded for sec
During the monitoring the obtained information has b een recorded in the memory of a
PC
The U and B magnitudes of the observed stars during the are were determined by
comparison with their corresp onding values in the quiescent state In this run just the
aring comp onent of the double star EV Lac was observed The observations lasted during
hours with the m telescop e and hours with the m telescop e V Mon
was observed during hours with the m telescop e and hours min with the m
telescop e YZ CMi was observed during hours only with the m telescop e Nine
ares of EV Lac and ve ares of V Mon were detected in these observations No
are of YZ CMi was detected Sometimes the ares are comp osite and short spiky ares
are observed over or immediately after the main relatively slow are
The data on the observed ares of EV Lac is summarized in Table and that of
the V Mon in Table For deducing the parameters of the observed ares it was
accepted that U and B magnitudes of the aring comp onent of EV Lac are equal to
m m
: and : resp ectively Alekseev Gershberg and that of V Mon are
m m
equal to : and : Shvartsman et al In consecutive columns of b oth Tables
the following information is given the date of observation UT at the maximum of are
the designation of separate p eaks observed during one are U and B magnitudes of
the are U B color of the star at the are maximum the rising time of the are t
r
the full duration of the are the integration time of observation and the telescop e with
which the observation was made For determining the parameters of ares the smo othed
by medians light curves of ares were used
Table Data on ares of EV Lac
Date UT max Peaks U B U B t Duration Tel
r
h m sec sec sec m
Nov
Nov
Nov
Nov a
b
Dec a
b
Jan slow
spike < <
Not certain
Figure Figure
Table Data on ares of V Mon
Date UT max Peaks U B U B t Duration Tel
r
h m sec sec sec m
Jan
Jan
Jan a
b
Jan
The small pre are Figure is not considered
Figure Figure
Light curves of some ares are shown in Figures The spiky type short ares of a
duration less than sec observed simultaneously in U and B are very remarkable Figures
Such spiky ares were also detected in previous observations with the two channel
fast photometer Tovmassian Zalinian Zalinian Tovmassian A chance
coincidence of two noise spikes on two indep endent records in U and B with values of
counts exceeding may take place once in hours Thus the observed spikes
are real ares Shvartsman et al stated that they have not detected ares with
duration less than sec though on the light curves demonstrated by them there are
some very short spikes similar to ares detected by us We may suggest that Shvartsman
et al assumed that such spikes registered at only one waveband were only noise and
for this reason were not considered by them as real ares The existence of such ares
put certain constrains on the theories of the origin of stellar ares
The authors acknowledge the Institute of Astronomy of the UNAM for use of their
facilities at the m telescop e in Tonantzintla to carry out the rep orted observations
VPZ is grateful to CONACYT for nancial supp ort by the Pro ject PE
H M TOVMASSIAN
Elsa RECILLAS
O CARDONA
Instituto Nacional Astrophysica
Optica y Electronica
Puebla Mexico
V P ZALINIAN
Byurakan Astrophysical Observatory
of the Armenian National Academy
of Sciences
References
Alekseev Yu Gershberg R E Astro zika
Shvartsman V F Beskin G M Gershberg P E Neizvestni S I Plakhotenkova V L
Pustilnik L A Izv Crimean AO
Tovmassian H M Zalinian V P Astro zika
Tsvetkov M K Antov A P Tsvetkova A G Comm Konkoly Obs Hung Acad
Sci No
Zalinian V P Tovmassian H M Contr Byurakan Obs
Zalinian V P Tovmassian H M IBVS No
Zalinian V P Tovmassian H M IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
SA HD A NEW ECLIPSING BINARY
AMONG LANDOLT S STANDARD STARS
We present observational results of a newly discovered eclipsing binary SA
h m s 0 00
HD RA DEC A It is one of well
observed stars in the Landolt s standard star list b eing widely used in the
UBVRI photometry for examples Menzies et al and Richer et al
During the observing runs at Siding Spring Observatory SSO from November
to March abnormal data p oints of SA were detected on February
m
HJD for the rst time The brightness decreased by in the B V I
magnitudes relative to that of the other standard stars see Figure upp er panel The
00 0 0
eld of view of SSO telescop e f with SITe CCD is and
covers the whole area of SA which contains many well observed standard stars
We carried out time series CCD observations of SA over four nights from March
to at the Bohyunsan Optical Astronomy Observatory BOAO in order to
detect its light variability These observations were done with a TEK CCD camera
0 0
attached to the BOAO m telescop e The eld of view in the CCD image is
at the f Cassegrain fo cus of the telescop e Three comparison stars SA and
see Table were monitored to check the light variability of SA Figure
The CCD prepro cessings such as bias subtraction and at elding were made with
the IRAF CCDRED package We adopted simple ap erture photometry to obtain instru
mental magnitudes using the IRAF DAOPHOT package Massey Davis and
transformed to the standard system as follows
B V b v a a X a B V a B V X
where B V and b v are standard and instrumental magnitudes and X is the airmass
Four co e cients of a a a and a are zero level primary extinction color and secondary
extinction term resp ectively We then obtained di erential magnitudes of SA which
are plotted in Figure and listed in Table B and V in the sense Var C I in the
sense of Var C
Table Photometric prop erties of observed stars Landolt
ID Star Name V B V U B
our s
Var SA
C SA
C SA
C SA
0 0
Figure A CCD frame of SA observed in the BOAO Three
comparison stars SA and are denoted by their number
Figure Light variations of SA observed at SSO upp er panel and BOAO lower
m
panel It is noted that the brightness of SA decreased by ab out in B and V
m
near HJD and by in B near HJD
Table Di erential magnitudes of SA
HJD B HJD B HJD B HJD V HJD I
Table cont
HJD B HJD B HJD B HJD V
Light variations of SA were clearly detected on one night HJD
Its brightness started decreasing at HJD then reached minimum near HJD
and then slightly increased again Figure The light curves are similar to
that of an Algol type eclipsing binary Ho meister et al Its binary nature can
b e also deduced from the SSO data which showed a similar brightness decrease of ab out
m
in all lters B V and I
Light variations of SA have not b een rep orted b efore Kholop ov et al
The UBVRI photometry p erformed by Landolt for nights data p oints did
not show any p eculiarity of SA and gave very low mean errors of magnitudes and
colors for example V However our observations suggest that it is
a detached eclipsing binary with a minimum brightness near HJD and an
m
amplitude of at least in the blue band
S L KIM
H SUNG
S G LEE
Korea Astronomy Observatory
Taejon Korea
e mail slkim seeru b oao re kr
Visiting Fellow MSSSO
Australian National University Australia
References
Ho meister C Richter G Wenzel W in Variable stars p
Kholop ov P N Samus N N Frolov M S Goranskij V P Gorynya N A Kireeva
N N Kukarkina N P Kuro chkin N E Medvedeva G I Perova N B Shugarov
S Yu General Catalogue of Variable Stars th Edition Moscow Nauka
Publishing House
Landolt A U AJ
Landolt A U AJ
Massey P Davis L E A User s Guide to Stel lar CCD photometry with IRAF
Menzies J W Marang F Laing J D Coulson I M Engelbrecht C A MNRAS
Richer H B Pritchet C J Crabtree D R ApJ
ERRATUM
In the printed version the a liation for author S G LEE was erroneously given as
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
SORTING OUT W BOOTIS AND ITS COMPARISON STARS
W Bo otis HR HD V SpT M I I I is a bright example of a
small amplitude red variable Percy Desjardins recently rep orted that W Bo o
had changed p erio d in ab out from days to days and suggested that W Bo o
had switched pulsation mo de Unfortunately the check star HD used in the
di erential photometry app eared to b e slightly variable A second check star HR
HD was adopted but it to o app eared to b e slightly variable We therefore decided
to observe all three stars in relative to the original comparison star and a new check
star We rep ort the results here
The comparison star was HR HD V B V SpT G V
and the new check star was HR HD V B V SpT K Five
observers Beresky Luedeke Smith Thompson Woo d carried out the measurements
as part of the American Asso ciation of Variable Star Observers AAVSO photo electric
photometry program Landis et al The observations were made and reduced as
describ ed there and in Percy Desjardins
We have a total of V observations of W Bo o and its comparison and new check star
observations of HD and observations of HR The standard deviation of
the new check comparison magnitudes is which is the exp ected error of the
observations esp ecially considering that they were made by ve di erent observers These
stars therefore app ear to b e constant The of the HR comparison magnitudes
is which suggests that this star is also constant
The of the HD comparison magnitudes is which suggests that this
star may b e slightly variable It is also p ossible that the larger scatter is due to the
faintness V of the star The p ower sp ectrum of the previous observations of this
star Percy Desjardins showed a p eak at cycle day but this p eak do es not
app ear in the p ower sp ectrum of the present observations nor do es it pro duce a reasonable
phase diagram There are several p eaks in the p ower sp ectrum of the present observations
none of which is very conspicuous The star is K I I I type so the variability if real could
b e due to star sp ots Hatzes Co chran have recently rep orted short term radial
velocity variations in K giants which they attribute to pulsation
The light curve of W Bo o Figure is very interesting The cycle count p erio d
is days very similar to the p erio d of W Bo o b efore but it is strongly mo du
lated and there is some evidence for long term variations The light curve can b e well
represented as the sup erp osition of two p erio ds and days Periods of and
days were found by Percy Desjardins and interpreted as adjacent radial mo des
The new and day p erio ds were determined indep endently of the previously known
p erio ds The mo de switching in W Bo o is rather similar to that recently rep orted in RR
UMi by Lloyd West This star switched b etween p erio ds of and days with
strong mo dulation of the amplitude
Figure The V light curve of W Bo o relative to the comparison star HR The time axis is
JD Note the mo dulation in the amplitude of the pulsation the light curve can b e
represented as the sup erp osition of and day p erio ds
Acknowledgements A Desjardins and M Marinova were participants in the University
of Toronto Mentorship Program which enables outstanding senior high school students
to take part in research pro jects at the university JRP acknowledges a research grant
from NSERC Canada and thanks the AAVSO for the infrastructure within which this
pro ject was carried out
KENNETH LUEDEKE
JOHN R PERCY
Giddings Avenue NE
ADRIEN DESJARDINS
Albuquerque NM USA
MARGARITA MARINOVA
Department of Astronomy and
MICHAEL S SMITH
Erindale College
N Table Mountain Rd
University of Toronto
Tucson AZ USA
Mississauga Ontario
RAYMOND R THOMPSON
Canada L L C
Welton Street
e mail jp ercy erin utoronto ca
Maple Ontario
TED BERESKY
Canada L A R
S Virginia Avenue
JAMES E WOOD
Spring eld MO USA
David Court
Bakers eld CA USA
References
Hatzes A P Co chran W D in Co ol Stars Stellar Systems and the Sun ed R
Pallavicini A K Dupree ASP Conf Ser
Landis H J Mattei J A Percy J R IBVS No
Lloyd C West K W IBVS No
Percy J R Desjardins A PASP
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
IMPROVED EPHEMERIS AND NEW OBSERVATIONS OF NSV
NSV S CSV GSC was originally announced as a vari
able star by Ho meister Additional observations carried out by Guarro Flo et al
showed that NSV is in fact a W UMa type eclipsing binary system The
following preliminary ephemeris was given
d
Min I HJD : E
To improve the ab ove ephemeris and its light curve NSV was observed in in
tegral light and in the B and V bands during several nights from December to
January using the m Ritchey Chretien telescop e Moschner and the m
SC telescop e Kleikamp equipp ed with ST cameras at private observatories in Ger
many and the m telescop e at l Ametlla del Valles Observatory in Spain equipp ed
with a Starlight Xpress CCD camera GSC and GSC were used as
comparison and check stars resp ectively
From the new set of data a list of minima were derived using the Kwee and van Woerden
metho d These new minima showed that the preliminary p erio d given by Guarro
Flo et al was an alias one After p erforming a least squares linear t on the minima the
following improved ephemeris was found
d
Min I HJD : E
Table
HJD Ep o ch Minimum Filter O C Observer
II no
II no
I no
II no
I no
II V
I V
II V
II V
I V
II B
II B
II B
I B
I no
I B
I B
II no
II no
I no
I no
Observer Moschner Garrigos Kleikamp
Figure Figure
Table summarizes minima timings and O C residuals according to the new ephemeris
After computing the improved ephemeris to obtain a history of the p erio d b ehaviour
of NSV the variable was investigated Moschner on plates taken with the
m astrograph at Sonneb erg Observatory The variable was found to b e at minimum light
on plates covering the interval from January until January
Analysis of the timings suggests that the p erio d of NSV has remained fairly
constant from JD until now The observational gap b etween JD and
JD do es not allow to ascertain whether the p erio d b efore JD was di erent
from the present one Figure shows O C residuals calculated against the new ephemeris
The typical error of photographic measurements is days whereas that of the CCD
measurements is days Before JD it is not p ossible to unambiguously
assign an ep o ch number For this reason Figure shows residuals for the two closest
computed ep o chs to the observed photographic minima b efore JD which are
represented by op en b oxes and crosses Solid circles represent residuals after JD
Table lists photographic minima b efore JD and gives the key to Figure Table
lists photographic minima after JD
Table
HJD Ep o ch Ep o ch O C O C
Op en b oxes Crosses Op en b oxes Crosses
Table
HJD Ep o ch O C
Also observations allowed to obtain a new light curve in the B and V bands To
obtain the B and V magnitudes of the light curve of NSV the comparison star
GSC was standardized using an OPTEC SSP A photo electric photometer
attached to the Cassegrain fo cus of the m telescop e at Esteve Duran Observatory
Spain Results indicate that NSV is an ob ject with a V magnitude of
at maximum I maximum I is the maximum following the primary minimum and
m m
an average B V color index of : : Figure depicts B V and B V phase
curves Table summarizes amplitudes of the primary and secondary minima and maxi
mum light levels in the B and V bands Systematic di erences app earing around Max I
might b e due to observational uncertainties
Table
Max magnitude Min I amplitude Min I I amplitude
m m m
B Band : : :
m m m
V Band : : :
Josep M GOMEZ FORRELLAD
Wolfgang MOSCHNER
Grup d Estudis Astronomics
Timmerschlade
Apartado
D Lennestadt
Barcelona
Germany
Spain
e mail wolfgang moschner t online de
e mal jmgomez astro gea cesca es
Enrique GARCIA MELENDO
Wilhelm KLEIKAMP
Esteve Duran Observatory
Hulsstr
El Montanya Seva
Marl
Seva
Germany
Barcelona
e mal wilhelm kleikamp t online de
Spain
e mail duranobs astro gea cesca es
References
Guarro Flo J Gomez Forrellad J M Garcia Melendo E Vidal Sainz J IBVS
No
Ho meister C Astronomische Abhand lungen Erganzungshefte zu den Astronomis
chen Nachrichten No
Kwee K K van Woerden H BAN
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
PHOTOMETRIC RESULTS ON THREE HIPPARCOS VARIABLES
THE NEW ECLIPSING BINARY SYSTEMS HD AND
HD AND THE STAR HD
An analysis of the photometric data from the Tycho Mean Photometric Catalogue and
the Tycho Photometric Observations Catalogue p erformed by Woitas yielded a list
of new bright variables Several b oreal stars of this list were included in the program
for the identi cation and characterization of new variable stars carried out by the Grup
d Estudis Astronomics and the Esteve Duran Observatory The rst ob jects monitored
were HD HD and HD
HD SAO PPM BD AGK GSC
was observed in the V band for nights from to March using a CCD
camera and a cm refracting telescop e at Esteve Duran Observatory HD was
used as comparison star and HD HD and GSC as check stars
m
HD has an average photovisual magnitude of : and F sp ectral type According
to Woitas this ob ject is an RR Lyr variable with a day p erio d Observations show
that HD is not an RR Lyr star but an eclipsing binary system with a p erio d of
days Figure The light curve indicates that b oth minima are almost equally deep the
m
amplitude b eing : in V There was ambiguity in the selection of the primary minimum
so it was arbitrarily assigned to the b est observed minimum Additional photometric
observations should b e p erformed to clarify this p oint The following ephemeris was
computed
d
Min I HJD : E
Table gives a list of minimum timings and O C residuals
Table
HJD Ep o ch Minimum O C
d
II :
I
I
I
A preliminary analysis suggests that the mass ratio of the comp onents in this binary
system is close to the minima are due to partial o ccultations and than the ll out
factor f is bigger that
HD SAO PPM BD AGK GSC
was observed in the V band for nights from March to April
at Mollet del Valles Observatory using also a CCD camera and a cm refractor It is
Figure Figure
m
an ob ject with an average photovisual magnitude of : and A sp ectral type HD
and HD were used as comparison and check stars resp ectively HD was
classi ed as an RR Lyrae Woitas with a day p erio d CCD observations show
that this variable is not an RR Lyrae star but an eclipsing binary star with a p erio d
over day Figure Photometric data indicate that the primary minimum has an
m
amplitude of magnitude and the depth of the secondary minimum is : The
m
phase curve also displays an O Connell e ect O Connell amounting to m :
m Max I I Max I where Max I follows the primary minimum The following
ephemeris was computed
d
Min I HJD : E
HD SAO BD PPM AGK
GSC is a star of magnitude photovisual and G sp ectral type which
according to Woitas is a classical Cepheid variable with a p erio d of days This
ob ject was observed in the V band for hours during six consecutive nights from
to March with a CCD camera using the m telescop e at Mollet del Valles
Observatory BD was used as comparison star and GSC as check
star Observations show that HD remained constant during the six nights within
magnitudes Correct identi cation with HD has b een checked If this star
is variable photometric results indicate that it is not a Cepheid
E GARCIA MELENDO
J M GOMEZ FORRELLAD
Esteve Duran Observatory
Grup d Estudis Astronomics
El Montanya Seva
Apartado
Seva Barcelona
Barcelona
Spain
Spain
e mail duranobs astro gea cesca es
e mail jmgomez astro gea cesca es
References
O Connell D M K Riverview Pub
Woitas J IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
PHOTOMETRIC OBSERVATION OF T TAURI TYPE STARS
DI Cep T Tau V Tau GW Ori V Ori
Most of the pre main sequence stars as well as T Tauri type stars are characterized by
some kind of variability of their brightness In the UBV photometric system magnitudes
of these stars change by up to mag on a time scale of hours to years e g App enzeller
and Mundt Herbst et al
Photometric observations over the past years showed that sometimes regular some
times erratic b ehaviour casts some light on the pro cesses taking place in these ob jects and
on their interaction with the environment On the analysis of more than entries
on young stars Herbst et al prop osed that there were three groups of light
variations related to the sp ectra of these stars Application of mo dern Fourier analysis
metho ds now allows to reveal p erio dic comp onents of light variability for some of these
ob jects This prop erty of the T Tauri stars can b e explained by rotational mo dulation
for a star with an asymmetric distribution of sp ots on its surface e g Vrba et al
Shevchenko et al However a more detailed study of these ob jects needs a large
quantity of observational data on individual stars during a long time interval
Our WBVR observations of the T Tauri type stars DI Cep T Tau V Tau GW Ori
and V Ori were carried out in autumn with the single channel photon counting
photometer attached to the cm telescop e at the Crimean lab oratory of Sternberg
Astronomical Institute Moscow Observations were done by di erential photometry
All stars were measured together with two comparison stars and background light was
measured at least twice in each band For transformation to the standard system we
observed standard stars of luminosity classes IV V and late sp ectral types from the list
of Kornilov et al Rms errors of the di erential photometry are ab out
mag for BVR bands and mag for the W band In this note we rep ort on the results
of observations for ve ob jects The results are presented in the table
Application of the W photometric band Straizys for CTTSs has some ad
vantages compared to the U band thus the W band has lower transmission at larger
wavelengths decreasing the in uence of the Balmer jump which is essential for stars with
emission line sp ectra On the other hand the W band reduces the red leak while the
U band has a considerable red leak Our measurements in the W band showed little
di erence compared to U band measurements of other authors see e g Herbst et al
Table WBVR observations of T Tauri stars
JD V W B B V V R JD V W B B V V R
T Tau GW Ori
DI Cep
V Tau V Ori
Fortunately a long sequence of clear nights on Octob er allowed me to get continuous
measurements of some program stars In the table we presented Julian Dates W B V
and R measurements
Photometric monitoring of T Tauri type stars by di erent authors has revealed p erio dic
variations in some stars with p erio ds b etween and days Our data allow us to monitor
variability of the program stars continuously for days Moreover our measurements
show light variability of some stars within a night
Figure
Figure
In Figures and as an example we present p ortions of light curves resp ectively of
DI Cep and T Tau in all photometric bands Figure shows that on JD DI
m m
Cep increased its brightness by in W and B and by in V and R bands Thus
we see photometric activity of DI Cep during that night Other program stars showed no
m
marked photometric activity V
So continuous photometric monitoring has not revealed evident p erio dic mo dulation of
m
brightness for program stars We observed variability in WBVR bands within V
for all stars and a higher photometric activity for DI Cep
N Z ISMAILOV
Sternberg Astronomical Institute
Universitetskij Prosp
Moscow Russia
References
App enzeller I Mundt R Astron Astrophys Rev
Herbst W Herbst D K Grossman E J Weinstein D Astron J
Kornilov V G Volkov M I Zakharov A I et al Trudi GAISH LXI I I
Shevchenko V S Grankin K N Ibragimov M A et al IBVS No
Straizys V Multicolor Stellar Photometry Mokslas Vilnius
Vrba F J Rydgren A E Chugainov P F et al Astron J
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
THE rd NAME LIST OF VARIABLE STARS
The present rd Name List of Variable Stars compiled basically in the manner rst
introduced in the th Name List IBVS No contains all data necessary
for identi cation of new variables nally designated in The total number of
designated variable stars not counting designated non existing stars or stars subsequently
identi ed with earlier designated variables has now reached In the nearest future
we are going to present two sp ecial Name Lists containing variables discovered by the
HIPPARCOS mission and in the frame of the OGLE pro ject
The rd Name List consists of two tables Table contains the list of new variables
arranged in the order of their right ascensions It gives the ordinal number and the des
ignation of each variable its equatorial co ordinates for the equinox note that we
have changed the standard accuracy For all stars but two we present right ascensions
s 00
to and declinations to The co ordinates were found in the literature taken from
p ositional catalogues including GSC or determined by the authors Sometimes the ac
curacy may actually b e ab out seconds of arc For V and V Cas we could not
improve the published rough co ordinates b ecause nding charts are not available the
range of variability sometimes the column Min gives in parentheses the amplitude
of light variation and the system of magnitudes used the symbols Rc Ic desig
nate magnitudes in Cousins s RI system the symbols y b u mean Str omgren s
y b u magnitudes g designates magnitudes in the system of Thuan and Gunn T
stands for broad band Tycho magnitudes formed from B and V measurements r are
red magnitudes not tied to a particular system the type of variability according to the
classi cation system describ ed in the forewords to the rst three volumes of the th GCVS
edition with the additions introduced in the th Name List IBVS No in
the th Name List IBVS No and in the nd Name List IBVS No
two references to the list of pap ers which follows Table the rst reference is to the
investigation of the star the second one indicates the pap er containing a nding chart or
the corresp onding Durchmusterung BD CoD or CPD containing the variable or the
Hubble Space Telescope Guide Star Catalog GSC if the star can b e found using it
In a small number of cases the value of the variability amplitude column Min
in parentheses could not b e expressed in the same system of magnitudes as the star s
brightness in such cases we indicate the photometric band for the amplitude separately
Table contains the list of variables arranged in the order of their variable star names
within constellations After the designation of a variable its ordinal number from Ta
ble is given as well as identi cations with several ma jor catalogues and identi cations
necessary to nd this star in the pap ers with the rst or indep endent announcement of
the discovery of its variability References to such pap ers are given in square brackets af
ter the corresp onding identi cation The name of the discoverer accompanies the reference
only in the case of its b eing di erent from the name of the author s of the pap er referred
to For the stars having NSV catalogue numbers the references to discovery pap ers
already taken into account in the NSV catalogue are not always given After the identi
cations some minimal remarks are given if necessary
Several new corrections to earlier Name Lists have b een found necessary Thus in
the Name List No IBVS No V Oph is actually V Oph this was
not revealed b ecause of the then adopted co ordinates for V Oph b eing seriously in
error The same applies to V Lyr Name List No IBVS No actually the star
is identical with BI Lyr
Co ordinates for several stars in the Name Lists Nos op cit IBVS No
IBVS No are for di erent reasons in error The table b elow contains a list of
these stars with corrected co ordinates
No Star
: :
h m s 0
V Sco
V Sco
V Sco
V Sco
V Oph
AO Lyn
V Cyg
V Mon
V Sgr
The following signi cant identi cations are to b e added to the Name Lists Nos
and PZ And BD V Aql HD K Leo Gliese
V Ori AFGL V Sgr NSV V Sgr NSV V Sgr
NSV
Several more corrections to Name List No V Cyg should have the variability
range to P type SR V Oph the magnitudes quoted are in the V band
V Pup NSV not
Note that the corrected version of the past Name Lists in the form of a combined
Name List Nos is available as a zip le from Sternberg Astronomical Institute
ftp neptun sai msu su cd pub groups cluster gcvs
Thanks are due to S V Antipin O V Durlevich M S Frolov N N Kireeva and E N
Pastukhova for their help during the preparation of the present Name List and to all
members of the GCVS team who prepared information for the variable star data base
This study was supp orted in part by Russian Foundation for Basic Research through
grant
E V KAZAROVETS
N N SAMUS
Institute of Astronomy
of Russian Academy of Sciences
Pyatnitskaya Str
Moscow Russia
Table
No Name R A Decl Max Min Type Ref
h m s o m m
AY Scl J EA GSC
V Cas V M
V Cas V M
V Cas V M
LN Peg V RS BD
BI Psc B UV
QR And V NL
QS And V EW
V Cas B XM
V Cas V FU
V Cas g E
V Cas g E
V Cas g E
V Cas g E
V Cas g E
V Cas g E
V Cas g RRC
V Cas g E
V Cas g E
BK Psc V RS
QT And Rc V BY UV BD
BL Psc U NL
V Cas P SR
BG Phe V BE
AZ Scl V BE CoD
V Cas V M
alpha Scl u V SXARI CoD
V Cas V M
sigma Scl u V ACV CoD
V Cas V NB
QU And V RS BD
V Cas V M
BM Psc V EW
QV And U ACV BD
QW And V EW GSC
BN Psc V EW
BW Cet B V ACVO BD
BB Scl V E CoD
BO Psc V BY GSC
QX And V EW
XY Tri V RRAB
XZ Tri V RRAB
QY And P SRA
ER Eri U UV CPD
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Per V BE BD
YY Tri K M
V Per V IA BD
V Cas I M
XZ Ari V EW GSC
BX Cet V BY
V Cas I L
YY Ari J SR GSC
BY Cet V RS BD
VW For P AM
YZ Ari J M
BZ Cet V BY BD
V Cas P M
V Per V DSCTC BD
CC Cet H R GSC
CD Cet V BY
V Per V BY
V Per V BY GSC
V Per V BY GSC
V Per V BY
ES Eri V RS GSC
V Per V BY
V Per V BY GSC
V Per V BY
V Per V BY
V Per V BY
V Per V BY
V Per V BY
V Per V BY
V Per V BY GSC
V Per V BY GSC
VX For V UG
V Per V BY
CE Cam V ACYG BD
CL Oct V ZZ
ET Eri J SRB GSC
V Per V BY
V Per V BY GSC
VY For V XM
V Per V BY GSC
CF Cam P DCEP GSC
V Per V BY
V Per V BY
V Tau V RS BD
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Per V BY GSC
V Tau J M
V Tau V RS
V Per V BY
EU Eri T SRC CoD
V Tau V BY
V Tau V RRAB
V Tau U UV
CG Cam B RCB GSC
V Tau P UV
V Tau V BY
V Tau V BY
V Tau U UV
V Tau V BY UV
V Tau V EW
CH Cam V ZZ
EV Eri J SRB GSC
V Per V LB
V Tau V EA BD
V Tau V BY
V Tau V BY
V Tau V BY
V Tau V INB
TW Ret J RV
V Tau V ELL BD
V Per V LBV BD
CI Cam B ZAND GSC
TX Ret B DSCTC CPD
V Tau P M
V Tau P UV
TY Ret J SR GSC
V Tau V BY
V Tau V BY
V Tau V BY
V Per V BY
V Tau P UV
V Tau P UV
V Tau P UV
V Tau P UV
V Tau P UV
V Tau V RS BD
V Tau P UV
V Tau V EW
V Tau P UV
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
EW Eri J INT
V Tau P UV
V Tau V BY
V Tau V DSCTC BD
V Tau P UV
TZ Ret B RRAB
V Tau P UV
EX Eri b V DSCTC CoD
EY Eri J M
RS Cae V XM
V Aur V EW BD
CK Cam V DCEP BD
EZ Eri V RS BD
UU Col B XM
CL Cam V RS BD
V Ori V XM E
UU Pic P NL
UV Col J M GSC
UV Pic V BY CoD
V Tau V BY BD
UW Col J M
V Ori U UVN
UX Col V RS CoD
V Ori u BY UV
UW Pic V XM
V Ori U UVN
V Ori Ic BY
V Ori Ic FU
V Ori Ic BY
V Ori Ic BY
V Ori Ic INS
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori V INT
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Ori Ic BY
V Ori Ic BY
V Ori Ic BY
V Ori Ic IN
V Ori Ic BY
V Ori V UVN
V Ori Ic FU
V Ori Ic BY
V Ori Ic FU
V Ori Ic BY
V Ori Ic BY
V Ori Ic INS
V Ori Ic IN
V Ori Ic BY
V Ori Ic BY
V Ori Ic FU
V Ori Ic BY
V Ori Ic BY
V Ori Ic INS
V Ori Ic BY
V Ori Ic BY
UX Pic J M GSC
UY Pic V RS
V Ori V BY
V Ori Rc V EW
V Ori u INT
khi Ori V RS BD
V Aur V RS BD
V Aur V EB
V Aur V XM
UY Col V DSCT CoD
V Ori V RS BD
V Ori u V ACV
HY CMa V E RS BD
V Ori V RS BD
V Aur V EA BD
V Ori V BY BD
AH Men V NL
V Car B DSCTC CoD
V Mon J M
V Mon V EW
V Mon u U LBV BD
PR Gem V EW
HZ CMa y ELL CoD
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
II CMa V EW
IK CMa V EW
CM Cam V FKCOM BD
PS Gem V SRD BD
IL CMa V E LBV CoD
IM CMa b ELL
IN CMa V NL
BL Lyn V BY
BM Lyn V RS E BD
V Car B UG
V Pup y B ZZ
BM CMi V IS
V Mon B RRAB
PT Gem V RRAB
V Pup B DSCTC BD
EW UMa V IS
BN Lyn V SRD BD
FI Cnc V FKCOM BD
FK Cnc V BY BD
WX Pyx V XM
WY Pyx V M
MN Vel T SRA CoD
BO Lyn B DSCT GSC
FL Cnc V DSCTC BD
EX UMa V RRAB
FM Cnc V RRAB
MO Vel B V ACVO CoD
WZ Pyx Rc M
XX Pyx B V DSCTC CoD
EY UMa P RRAB
FN Cnc V RRAB
BP Lyn B E NL
MP Vel V DSCTC CoD
MM Hya B UG
MQ Vel K M
EZ UMa V SRD BD
MR Vel V XI
MN Hya Ic XM EA
DX Leo V BY BD
FF UMa V RS BD
AK Ant b V DSCTC BD
MS Vel T SRA CoD
MT Vel B DSCTC CoD
MU Vel K M
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
DY Leo V RS BD
V Car B V ACVO CPD
DZ Leo V RRC
TU Sex B EW
FG UMa V RS BD
MV Vel V BE CPD
SY LMi V RRAB
V Car B V ELL
V Car B V BE
V Car B BCEP
SZ LMi V RRAB
V Car B V ELL
FH UMa V AM
EE Leo V BY
TT LMi V RRC
V Car V DCEP
V Car V DSCTC
MW Vel T SRB CoD
FI UMa b V DSCTC BD
FK UMa V RS BD
TV Crt V RS CoD
CN Cam B RRAB BD
V Cen U CPD
EF Leo V RRAB
IQ Vir V DSCTC BD
TW Crv V R GSC
IQ Com V RRAB
CO Cru V DSCTC CPD
CP Cru V NA
CO Cam V ELL BD
GV Mus Ic EW
GW Mus Ic EW
GX Mus Ic EW
GY Mus Ic EW
GZ Mus Ic EW
HH Mus Ic EA
HI Mus Ic EB
HK Mus Ic EW
HL Mus Ic EW
HM Mus Ic EW
HN Mus Ic EA
HO Mus Ic EW
HP Mus Ic EB
HQ Mus Ic EB
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
HR Mus Ic EA
HS Mus Ic EB
HT Mus Ic EA
HU Mus Ic EW
HV Mus Ic EW
HW Mus Ic EA
HX Mus Ic EW
HY Mus Ic EW
HZ Mus Ic EW
II Mus Ic EW
IK Mus Ic EW
IL Mus Ic EW
IM Mus Ic EA D
IN Mus Ic EA
IO Mus Ic EW
IP Mus Ic EA
IQ Mus Ic EA
IR Mus Ic EW
IS Mus Ic EW
IT Mus Ic EW
IU Mus Ic EW
IR Vir V EW
IV Mus Ic EB
IW Mus Ic EW
IX Mus Ic EW
IY Mus Ic EB
IZ Mus Ic EW
KK Mus Ic EA
KL Mus Ic EW
V Cen V ZZA
KM Mus Ic EB
V Cen B RRAB
IR Com P UG E
MO Hya v V DSCTC CoD
CQ Cru B V E
CR Cru B V E
CS Cru B V E
CT Cru B V BCEP
CU Cru B V E
CV Cru B V BCEP E
CW Cru B V BE
CX Cru B V BCEP E
CY Cru B V BCEP E
CZ Cru B V BCEP
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
BQ CVn V RS BD
V Cen V NA
DL Cha P SRB
IS Vir V RS BD
IS Com V RRC GSC
BR CVn V SRB BD
V Cen V ELL
KN Mus B ZZO
IT Com V RS BD
V Cen P NL
V Cen P NL
V Cen V EA ACV CoD
IT Vir V ELL BD
V Cen K ZAND
BX Cir V PVTEL
IU Vir V ZZA
V Cen Ic SR
IV Vir V ELL BD
CY Boo V SRB BD
V Cen V E AM
MP Hya B DSCTC CoD
CZ Boo V RRAB
HN Lib V BY BD
V Cen V DSCTC CPD
BY Cir V N
DD Boo V RRC
BZ Cir V NL
DE Boo V RS BD
DF Boo V RRAB GSC
EU Dra V SRD BD
NY Ser V UGSU
CC Cir V WR
UZ CrB V RRAB
DG Boo B RRAB
HO Lib V BY BD
HP Lib V ZZB GSC
V Nor V PVTEL CoD
HQ Lib V ELL BD
VV CrB P SRB GSC
lambd Lib V ELL BD
V Sco T IA BD
HR Lib b V DSCTC BD
IN Lup V DSCTC CoD
IO Lup b V DSCTC CoD
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
VW CrB B UG
VX CrB B RRAB
EV Dra V RS BD
VY CrB B RRAB
V Her V EW BD
V Sco V ACV CoD
VZ CrB B RRAB
WW CrB B RRAB
EW Dra V BY
WX CrB B RRAB
WY CrB B RRAB
WZ CrB B RRAB
XX CrB V EW GSC
V Her B RRC
V Oph U UVN
V Oph U UVN
V Her B UG
V Her B CWA
V Nor B DSCTC
V Nor B DSCTC
V Nor B DSCTC
V Sco V ACV CoD
V Her V RS BD
V Sco U UV
V Sco U UV
V Her B RRAB
V Oph V BY
V Her B EB
V Sco U UV
V Her V UG
V Her B RRAB
V Her B RRAB
V Ara V M
V Her B RRAB
V Her B RRAB
V Her B EB
V Her B RRAB
V Oph U INA CoD
V Her B EA
V Her V EW
V Her B RRAB
V Her B RRAB
V Her V RRAB
V Her B EW
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Sco B BCEP
V Sco V XND E
V Sco V EA
V Her B RRC
V Her B RRAB
V Her V RRC GSC
V Her B EA
V Her B LB
V Her B RRAB
V Her B RRAB
V Oph J M
V Her B EA
V Her B RRAB
V Her B RRAB
V Her B EA
V Her V DSCT BD
V Her P EB
V Ara V BE CPD
V Her V RRAB
V Sco V WR CoD
V Her V RRAB
V Her V RRC GSC
V Oph R M
V Her V EB BD
V Oph V ZZ
V Oph R M
V Her V SXPHE
V Oph V RRAB
V Sco V ELL CoD
V Oph V NA
V Sco V PVTEL CoD
V Her V RRAB
V Her V RRAB
V Oph V DSCTC BD
V Oph V ELL BD
V Her V RRC
V Oph V BY
V Oph V BY GSC
V Oph V BY
V Oph V BY
V Oph V ELL BD
V Oph V BY
V Oph V BY
V Oph V ELL BD
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Oph V ELL BD
V Oph V BY
V Oph V BY
V Oph V ELL BD
V Oph B RRAB
V Sco J M
V Her V EW GSC
V Sgr V
V Oph B EA
V Sgr K M
V CrA H M
V Sgr J M
V Sgr J M
V Sgr V UG
V Sgr J M
V Oph B RRAB
V Sgr J SRA
V Sgr K M
V Oph B RRAB
V Oph B EB
V Oph B M
V Her V XM
V Oph B RRAB
V Oph B UG
V Oph B RRAB
V Oph B SRB
V Oph P CWA
V Oph B ISB
V Her V BY BD
EX Dra B UG E GSC
V Oph B SRA
V Oph B LB
V Sgr B RRAB
V Sgr B RRAB
V Her P BE
V Sgr B RRC
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRC
V Sgr B RRAB
V Sgr B RRAB
V Sgr B RRC
V Her U SRD
V Her V RRAB
V Oph B M
V Oph B M
V Oph B SRA
V Oph B RRAB
V Sgr P CEP
EY Dra V BY
V Oph B RRAB
V Sgr P N
V Pav b V DSCTC CPD
V CrA V DSCTC CoD
V Sct B BE GSC
NZ Ser U INA
V Oph K M
OO Ser K FU
V Sgr V NB
V Sgr B RRAB
V Sgr B RRAB
V Sgr B LB
V Sgr B RRAB
V Sgr B E
V CrA V EW
V CrA V EW
V CrA V EW
V CrA V EW
V Her V BY BD
V Lyr V RRAB
V Lyr V RRAB
V Pav V AM
V Lyr V EW GSC
V Lyr V EW
V Sct V BE BD
V Lyr V EW
V Lyr V RRAB
V Sgr V NC
V CrA V INB
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V CrA K INB
V Sgr V RRAB
V Aql V NA
V Sgr V EW
V Lyr V RS BD
V Lyr P EA
V Aql B EA BD
V Aql U SRD BD
V Sge V DSCTC BD
V Vul r SR
V Aql V BY BD
V Lyr V EW
V Lyr V EW
V Lyr V EA
V Lyr V UG
V Lyr V EA
V Lyr V EW
V Lyr V EW
V Lyr V EA RS
V Lyr V EW
V Lyr V EW
V Aql U SDOR BD
V Aql V EA RS
V Lyr V NL
V Lyr V EA
V Lyr V EW
V Lyr V EW
V Sgr V BY BD
V Vul V LBV BD
V Sgr V ELL BD
V Vul B WR
V Aql v ACVO BD
V Sgr B V ACVO CoD
V Aql V XM E
V Aql K M
V Sge K M
V Vul V ELL BD
V Vul V SR
QT Tel J SR GSC
V Pav P NL
V Cyg U BE GSC
V Pav P AM
QU Tel V ZZB
AX Cap V UG
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Vul V DSCTC
V Vul V DSCTC
EZ Dra P M
V Pav J M
V Vul v V DSCTC BD
V Sgr V EA
CM Oct J M
V Cyg B SR
V Cyg V SRB
V Cyg V EA
AY Cap J SR GSC
V Cyg V SRB
V Cyg B LB
V Cyg V SRA
V Cyg V SRB
V Cyg V SRB
LW Del V RRAB
V Cyg V SRB
V Cyg V SRB
HX Aqr V E GSC
V Cyg B LB
V Cyg B SRB
BO Mic V BY CoD
V Cyg U UVN
V Cyg B LB
V Pav J M
V Cyg P UVN
LX Del V RRAB
V Cyg V M
V Cyg V SRB
V Cyg V SRB
V Cyg U UVN
V Cyg U UVN
AZ Cap V BY UV
V Cyg U UVN
V Cyg V EW
V Cyg U UVN
BP Mic H M
V Cyg U UVN
V Cyg B LB
V Cyg V LB
V Cyg V LB
V Cyg V LB
LY Del V EA
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
V Cyg U UVN
V Vul V EW GSC
V Cyg B SR
V Cyg B LB
BQ Mic J M
V Cyg V SR
V Cyg R LB
V Cyg R UV
V Cyg B LB
V Cyg B LB
V Cyg B SR
V Cyg B LB
V Cyg V LB
V Vul V RRC
iota Cap V BY BD
V Vul V RRC
V Cyg R LB
V Cyg V NL
BR Mic V BCEP CoD
V Cyg B LB
CH Gru B NL
HY Aqr H M GSC
BB Cap V BY
V Cep P ISA
LO Peg V BY
V Cyg V LB
V Cyg P M
HZ Aqr V RS BD
CI Gru B UG
V Cyg B LB
LP Peg V EW
LQ Peg B NL
V Cep B INB
V Cep B INT
V Cyg V LB
V Cep r INT
LR Peg V RRAB
V Cep P ISA
LS Peg V UG
V Cyg V RS BD
V Cyg V SRD
LT Peg V RRAB
LU Peg V RRAB
LV Peg J M GSC
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
LW Peg V RRAB
LX Peg V EW GSC
V Cep P CWB
V Lac R LB
LY Peg V EB
V Lac V M
V Lac V M
LZ Peg V RRAB
II Aqr P NL
V Lac V NL
V Lac V SR
V Lac V BY UV BD
MM Peg V EW
V Lac V SR
IK Aqr P NL
V Lac V M
UV PsA B DSCTC CoD
V Lac V M
MN Peg P M GSC
V Lac V M
UW PsA B DSCTC CoD
MO Peg V RRAB
V Lac V M
MP Peg J M GSC
V Lac V M
V Lac V M
MQ Peg V EW GSC
V Lac V M
V Lac V SRA
IL Aqr V BY BD
MR Peg J M GSC
MS Peg V NL
QZ And V SR
V And V M
V And V M
MT Peg U BY BD
MU Peg V RRAB
MV Peg J M
MW Peg P SR
BI Ind V RS CPD
CP Tuc I XM
V Cas V RS BD
V And V SRD
V Cep V INT GSC
Table continued
No Name R A Decl Max Min Type Ref
h m s o m m
MX Peg V EW
BP Psc J IT GSC
CK Gru J M GSC
V And V M
MY Peg V RRAB
V And V M
V And v V DSCTC BD
BQ Psc V SXPHE
BR Psc V BY
BS Psc V BY BD
MZ Peg V RRAB
V Cas V E
V Cas V EW
V Cas V EA
V Cas V EW
V Cas V EB
V Cas V EB
V Cas V DSCTC
V Cas V EW
V Cas V EW
V Cas V EW
BT Psc B IB BD
BU Psc B IB BD
Table
QR And RX J GSC
QS And No
QT And BD RE RE J GSC
QU And HD G BD SAO IRAS
LTT G HIC GSC
QV And HR HD B BD SAO GSC
QW And GSC
QX And Hein NGC GSC
QY And No SVS GSC 6 LM And No
QZ And LD
V And LD IRAS GSC
V And LD GSC
V And LD IRAS GSC
V And LD IRAS
V And LD IRAS Prager Ross var CSV
NSV
V And And HR HD A BD SAO
NSV GSC
AK Ant HD A CoD CPD SAO
GSC
0
HX Aqr Comparison star for AE Aqr P A GSC
HY Aqr IRAS GSC
Table continued
HZ Aqr BD LDS A G LTT EUVE
J NSV GSC
II Aqr V
IK Aqr Var PHL CSV NSV
IL Aqr BD Gliese G LHS LFT
Ross GSC
V Aql Nova Aql Takamizawa
V Aql HD G BD SAO SVS
CSV NSV GSC
V Aql HD G BD SAO IRAS
AFGL HIP GSC
V Aql HD Ma BD Gliese A G
LHS LFT Ross GSC
V Aql BD IRAS MWC He
LS I I GSC
V Aql E GSC
V Aql Aql HR HD A BD SAO
GSC
V Aql RX J RX J
V Aql IRAS
h m s
V Ara IRAS
V Ara CoD CPD SAO IRAS
He Wray NSV GSC
XZ Ari No GSC
YY Ari IRAS GSC H O OH maser
YZ Ari IRAS AFGL
V Aur HD F BD SAO HIP
GSC
V Aur HR HD G BD SAO IRAS
HIC GSC
V Aur Wr CSV NSV GSC
V Aur RX J RX J GSC
V Aur HD A p BD SAO HIP
GSC
CY Bo o Vir HR HD Ma BD SAO
IRC IRAS HIP NSV
GSC
CZ Bo o No
DD Bo o HV CSV NSV GSC
DE Bo o HR HD K BD SAO IRAS
Gliese LFT LTT HIC
NSV GSC
DF Bo o No HV CSV NSV GSC
DG Bo o BV CSV NSV GSC
RS Cae RX J
CE Cam HR HD A p BD SAO
IRC IRAS HIP GSC
CF Cam V SVS GSC
CG Cam IRAS GSC
CH Cam PNN of NGC PK IRAS
CI Cam MWC LS V IRAS GSC
CK Cam HD G BD SAO IRAS
HIP GSC
CL Cam HD G BD SAO IRAS
HIC GSC
CM Cam HD G BD SAO IRAS HIC E GSC
Table continued
CN Cam BD SAO BV CSV NSV
GSC
CO Cam HR HD A BD SAO
IRAS HIP GSC
FI Cnc HD G BD SAO IRAS
HIC GSC
FK Cnc HD G BD SAO E
HIC GSC
FL Cnc HD A BD SAO GSC
FM Cnc No
FN Cnc No
BQ CVn HD K BD SAO HIC
GSC
BR CVn HD Mb BD SAO IRC
AFGL IRAS HIP GSC
HY CMa BD SAO RE J GSC
HZ CMa HR HD B CoD CPD
SAO IDS S A IRAS MWC
He HIP GSC
II CMa var Probable non member of the op en cluster Be
IK CMa var Probable member of the op en cluster Be
IL CMa HR HD B CoD CPD
SAO HIP GSC
IM CMa Star NGC CPD
IN CMa RE EUVE J EXOSAT
BM CMi Anon CMi GSC
AX Cap New CV
AY Cap IRAS GSC
AZ Cap EUVE J BD GSC
BB Cap Gliese G LHS LTT NSV GSC
Cap iota Cap Cap HR HD K BD
SAO IRC IRAS HIC GSC
V Car HD A CoD CPD SAO
GSC
V Car RX J GSC
V Car HD F CoD CPD SAO
GSC
V Car No NGC
V Car No NGC GSC
V Car No NGC CPD GSC
V Car No NGC
V Car No NGC GSC
V Car No NGC
V Cas LD No IRAS
V Cas LD IRAS
V Cas LD IRAS
V Cas RX J
V Cas RNO B IRAS
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas C V Gal NGC NGC V Foreground ob ject
Table continued
V Cas C V Gal NGC NGC V Foreground ob ject
V Cas TAV IRAS GSC
V Cas LD IRAS
V Cas LD IRAS CCS GSC Not AV
Cas
V Cas Nova Cas Yamamoto
V Cas LD GSC
V Cas M
V Cas M
V Cas Prager IRAS CSV NSV
GSC
V Cas BD SAO HIP GSC
V Cas GSC
V Cas No GSC In NGC eld
V Cas No In NGC eld
V Cas No In NGC eld
V Cas No In NGC eld
V Cas No In NGC eld
V Cas No NGC
V Cas No In NGC eld
V Cas No In NGC eld
V Cas No In NGC eld
V Cen HD G CoD CPD SAO
IRAS HIP GSC Close binary
eccentric system with a low mass unseen secondary and a p ost AGB primary
Long term variations plus p erio dic variability
V Cen BPM L WD Gliese LHS
LTT GSC
V Cen V In the globular cluster Ru a background ob ject
V Cen Nova Cen Lil ler
V Cen LSS GSC
V Cen V
V Cen V
V Cen HD A CoD CPD SAO
GSC
V Cen Star B IRAS Not HD
V Cen IRAS
V Cen EUVE J candidate Prager HV CSV
NSV
V Cen HD F CoD CPD SAO
GSC
V Cep No NSV
V Cep LkH HBC NSV GSC In the
cometary nebula IC A
V Cep No GSC
V Cep RNO S Illuminati ng star of the nebula RNO in NGC
m
Brightened at least by in SI I A FWHM A b etween
and
V Cep No NSV
V Cep No NSV GSC
V Cep BD IRAS AS HBC GSC
BW Cet HD A BD SAO GSC
BX Cet Gliese B G LHS LFT LTT GSC
BY Cet BD SAO EXOSAT EXO
GSC
BZ Cet HD G BD SAO E HIC GSC
Table continued
CC Cet PG WD GSC
CD Cet Gliese G LHS GSC
DL Cha S IRAS CSV NSV GSC
BX Cir LSS GSC
BY Cir Nova Cir Lil ler
BZ Cir E CIR
CC Cir HD O WR LSS He GSC
UU Col RX J
UV Col IRAS HV Prager CSV
NSV GSC
UW Col IRAS
UX Col CoD CPD EXOSAT EXO
GSC
UY Col HD F CoD CPD SAO
GSC
IQ Com No
IR Com S RX J
IS Com No GSC
IT Com HD K BD SAO IRAS
HIC GSC
V CrA IRAS Not V Sco
V CrA HD A CoD CPD
SAO GSC
V CrA CV in Sgr control eld
V CrA CV in Sgr control eld
V CrA CV in Sgr control eld
V CrA CV in Sgr control eld
V CrA CoD HBC VSS Wa CrA Kn Anon
GlPe i GSC
V CrA HH IRS Herbig Haro ob ject in CrA IR source asso ciated
with the HH ob ject
UZ CrB No
VV CrB S IRAS GSC
VW CrB Var
VX CrB Var GSC
VY CrB Var GSC
VZ CrB Var
WW CrB Var GSC
WX CrB Var GSC
WY CrB Var
WZ CrB Var
XX CrB No GSC
TW Crv EC GSC
TV Crt HD K CoD CPD SAO
ADS IRAS Gliese AB HIP
GSC
CO Cru HD F CoD CPD SAO
GSC
CP Cru Probable Nova Cru
CQ Cru No I NGC GSC
CR Cru No I NGC GSC
CS Cru CPD No IV NGC NGC
He Wray GSC
CT Cru CPD No I I I NGC LSS
GSC
CU Cru No I I NGC
CV Cru CPD No I NGC GSC
Table continued
CW Cru CPD No I I I NGC NGC
He GSC
CX Cru CPD No I I NGC GSC
CY Cru CPD No I I I NGC LSS HIP
GSC
CZ Cru CPD No I I NGC LSS GSC
V Cyg MWC He LS I I IRAS GSC
V Cyg CCS IRAS GSC
V Cyg BC
V Cyg HD F BD SAO Hoag NGC
Sanders Zug Ti t HIP GSC
V Cyg CCS IRAS GSC
V Cyg CCS GSC
V Cyg CCS IRAS GSC
V Cyg CCS IRAS GSC
V Cyg BC IRAS
V Cyg CCS IRAS GSC
V Cyg BC GSC
V Cyg CCS IRAS GSC
V Cyg CCS GSC
V Cyg Ton in Cyg T
V Cyg CCS IRAS GSC
V Cyg B in the NGC region
V Cyg LD GSC
V Cyg CCS
V Cyg CCS IRAS SVS
V Cyg Ton in Cyg T
V Cyg Ton in Cyg T
V Cyg Ton in Cyg T
V Cyg Anon Cyg GSC
V Cyg Ton in Cyg T
V Cyg Ton in Cyg T
V Cyg CCS GSC
V Cyg CCS CSV NSV
V Cyg BC IRAS
V Cyg CCS
V Cyg Ton in Cyg T
V Cyg CCS GSC
V Cyg CCS GSC
V Cyg BC IRAS SVS GSC
V Cyg CCS
V Cyg New variable star in Cepheus region GSC
V Cyg CCS
V Cyg CCS IRAS SVS GSC
V Cyg BC GSC
V Cyg CCS GSC
V Cyg CCS IRAS SVS
V Cyg BC IRAS SVS GSC
V Cyg RX J
V Cyg CCS IRAS SVS
V Cyg CCS IRAS SVS GSC
V Cyg LD V IRAS
V Cyg CCS IRAS GSC
V Cyg CCS LD IRAS SVS GSC
V Cyg HD K BD SAO IRAS HIC GSC
Table continued
V Cyg LD
LW Del Prager SVS CSV NSV GSC
LX Del HV CSV NSV GSC
LY Del TAV GSC
EU Dra HD G BD SAO HIP
GSC
EV Dra HD G BD SAO RE
HIC GSC
EW Dra Gliese B G LHS GSC Gliese A
NSV
EX Dra HS Barwig et al C ob ject KUV
MS GSC
EY Dra RE EUVE J GSC
EZ Dra Prager IRAS CSV NSV
GSC
ER Eri CoD CPD He PDS GSC
ES Eri E GSC
ET Eri IRAS Stephenson GSC
EU Eri HD K CoD CPD SAO
IRAS HIP GSC
EV Eri IRAS GSC
EW Eri L A HBC IRAS GSC
EX Eri HR HD A CoD CPD
SAO GSC
EY Eri IRAS
EZ Eri BD E GSC
VW For V
VX For Probable Dwarf Nova in Fornax Susp ected var near TU For
VY For EXOSAT EXO FOR
PR Gem No
PS Gem HD A BD SAO HIP
GSC
PT Gem No
CH Gru V
CI Gru V GRU
CK Gru Prager HV IRAS AFGL
CSV NSV GSC
V Her BD BV CSV NSV GSC
V Her Var GSC
V Her Var
V Her Var GSC
V Her HD K BD SAO GSC
V Her Var GSC
V Her Var GSC
V Her PG HER
V Her Var
V Her Var
V Her Var GSC
V Her Var
V Her Var GSC
V Her Var
V Her Var GSC
V Her BV CSV NSV GSC
V Her Var
V Her Var
V Her No
Table continued
V Her Var GSC
V Her Var GSC
V Her Var GSC
V Her No GSC
V Her Var GSC
V Her Var IRAS GSC
V Her Var
V Her Var
V Her Var GSC
V Her Var
V Her Var
V Her Var GSC
V Her HD F BD SAO HIC
GSC
V Her BD SAO Prager CSV
NSV GSC
V Her No
V Her No
V Her No GSC
V Her BD SAO DHK GSC
V Her No
V Her No
V Her No
V Her No
V Her No GSC
V Her WGA J
00
V Her ADS C BD C AC AB V
Her
V Her HD A BD SAO IRAS
GSC
V Her IRAS GSC
V Her No
V Her HD G BD SAO RE
HIC GSC
MM Hya PG HYA GSC
MN Hya RX J
MO Hya HR HD A CoD CPD
SAO GSC
MP Hya HD A CoD CPD
SAO GSC
BI Ind HD K CoD CPD GSC
V Lac HD Na S CCS IRAS NSV
HIP GSC
V Lac LD IRAS
V Lac LD IRAS
V Lac LD IRAS
V Lac LD IRAS
V Lac BD SAO RE EUVE
J GSC
V Lac LD S NSV
V Lac LD IRAS
V Lac LD
V Lac LD IRAS GSC
V Lac LD
V Lac LD IRAS GSC
V Lac LD IRAS
V Lac LD IRAS GSC
V Lac LD IRAS
Table continued
DX Leo HD K BD SAO IRAS
Gliese A HIC GSC
DY Leo HD F BD SAO HIC
GSC
DZ Leo No
EE Leo Gliese G LHS LFT Wolf GSC
EF Leo No
SY LMi No
SZ LMi No
TT LMi No
HN Lib BD Gliese LHS LTT NSV
GSC
HO Lib BD Gliese G LHS LTT
Wolf NSV GSC
HP Lib EC GSC
HQ Lib BD EC GSC
HR Lib HR HD A BD SAO
GSC
Lib lambda Lib Lib HR HD B BD
CPD SAO IRAS GSC
IN Lup HD F CoD CPD
SAO GSC
IO Lup HD F CoD CPD
SAO GSC
BL Lyn Gliese B G LTT Ross B NSV
GSC Gliese A VV Lyn
BM Lyn HD K BD SAO IRAS
S CSV NSV HIC GSC
BN Lyn Lyn HR HD K BD SAO
IRC IRAS NSV GSC
BO Lyn No in the RR eld GSC
BP Lyn PG KUV LYN GSC
V Lyr No
V Lyr No
V Lyr No GSC
V Lyr No
V Lyr No
V Lyr No
V Lyr HD K BD SAO RE
G HIC GSC
V Lyr S
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
V Lyr B NGC
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC B
V Lyr V NGC
V Lyr V NGC
V Lyr V NGC
AH Men H H MEN GSC
Table continued
BO Mic HD K CoD CPD
SAO RE J HIP Sp eedy Mic
GSC
BP Mic IRAS
BQ Mic IRAS AFGL
BR Mic HD B CoD CPD
SAO GSC
V Mon IRAS AFGL
V Mon S CSV NSV GSC
V Mon HR HD B BD SAO
HIP GSC
V Mon S CSV NSV GSC
GV Mus V Cr eld
GW Mus V Cr eld
GX Mus V Cr
GY Mus V Cr
GZ Mus V Cr
HH Mus V Cr eld
HI Mus V Cr eld
HK Mus V Cr eld
HL Mus V Cr
HM Mus V Cr
HN Mus V Cr
HO Mus V Cr
HP Mus V Cr eld
HQ Mus V Cr
HR Mus V Cr
HS Mus V Cr eld
HT Mus V Cr eld
HU Mus V Cr
HV Mus V Cr
HW Mus V Cr eld
HX Mus V Cr eld
HY Mus V Cr eld
HZ Mus V Cr
II Mus V Cr
IK Mus V Cr
IL Mus V Cr
IM Mus V Cr eld
IN Mus V Cr eld
IO Mus V Cr
IP Mus V Cr
IQ Mus V Cr S NSV
IR Mus V Cr
IS Mus V Cr eld
IT Mus V Cr eld
IU Mus V Cr eld
IV Mus V Cr eld
IW Mus V Cr
IX Mus V Cr eld
IY Mus V Cr
IZ Mus V Cr eld
KK Mus V Cr eld
KL Mus V Cr
KM Mus V Cr
KN Mus PNN of NGC HD Neb PK He
IRAS NSV GSC
V Nor CoD CPD GSC
V Nor IFA star NGC GSC
Table continued
V Nor IFA star NGC GSC
V Nor IFA star NGC GSC
CL Oct RE J GSC
CM Oct IRAS
V Oph Ton in the Oph region
V Oph Ton in the Oph region
V Oph BD Gliese G LHS LTT
NSV GSC GSC
V Oph HD A CoD CPD
SAO IRAS MWC GSC
V Oph IRAS
V Oph CoD IRC AFGL IRAS
CCS No GSC
V Oph CoD PNN of NGC PK IRAS
V Oph IRC AFGL IRAS No NSV
V Oph HV CSV NSV GSC
V Oph Nova Oph Akihiko Tago
V Oph HD A BD SAO Kop IC
GSC
V Oph HD B BD SAO Kop
IC GSC
V Oph P IC S IC GSC
V Oph P IC GSC
V Oph P IC S IC
V Oph P IC V No IC GSC
V Oph HD B BD SAO Kop IC
GSC
V Oph P IC
V Oph P IC V No IC GSC
V Oph HD B BD SAO Kop IC
GSC
V Oph HD B BD SAO ADS
Kop IC GSC
V Oph P IC V No IC GSC
V Oph P IC S IC GSC
V Oph HD B BD SAO Kop IC
GSC
V Oph Var
V Oph Var
V Oph Var
V Oph Var
V Oph Var GSC
V Oph Var GSC
V Oph Var
V Oph Var
V Oph Var
V Oph Var GSC
V Oph S NSV GSC
V Oph Var IRAS GSC
V Oph Var IRAS GSC
V Oph Var IRAS GSC
V Oph Var IRAS GSC
V Oph Var IRAS
V Oph Var IRAS GSC
V Oph Var
V Oph Var GSC
V Oph IRAS
Table continued
V Ori RJ RX J RX J
V Ori T Tof
V Ori San HRC TSN RE J NSV
GSC
V Ori Ton GSC
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW HBC EXOSAT EXO
GSC
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW Zinner CSV NSV
V Ori JW
V Ori JW
V Ori JW
V Ori JW CSV NSV
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW
V Ori JW CSV NSV
V Ori JW E CSV NSV
V Ori JW
V Ori JW
V Ori JW
m
V Ori JW NW Ic
V Ori JW
V Ori JW
m
V Ori JW NW Ic
V Ori JW
V Ori JW
m
V Ori JW N Ic Co ordinates need con rmation
V Ori JW
V Ori JW E CSV NSV
V Ori Gliese G LHS Ross GSC
V Ori GSC
V Ori No GSC
V Ori HD K BD RE J GSC
V Ori Star NGC GSC
V Ori HR HD G BD SAO
IRAS Gliese GSC
V Ori HD G BD SAO RE J
HIP GSC
Ori khi Ori HR HD F BD SAO IRC IRAS Gliese AB GSC
Table continued
V Pav HR HD A CoD CPD
SAO GSC
V Pav RE J RE RE J
V Pav V
V Pav V V Drissen V b
V Pav S IRAS CSV NSV
V Pav IRAS
LN Peg BD SAO G E HIC
GSC
LO Peg BD G RE EUVE
HIP GSC
LP Peg No
LQ Peg PG PEG GSC
LR Peg No
LS Peg Prager Stephenson H PEG CSV
NSV GSC
LT Peg No
LU Peg No
LV Peg IRAS GSC
LW Peg No
LX Peg No GSC
LY Peg WT GSC
LZ Peg No
MM Peg No
MN Peg J Takamizawa GSC
MO Peg No
MP Peg IRAS GSC
MQ Peg No GSC
MR Peg IRAS GSC
MS Peg GD EG WD KUV GSC
MT Peg HD G BD SAO GSC
MU Peg No
MV Peg IRAS
MW Peg BD DHK GSC
MX Peg No
MY Peg No
MZ Peg No
V Per BD SAO B Oo h Per GSC
V Per HD B BD SAO Oo h Per
HIP GSC
V Per HR HD A BD SAO GSC
V Per HE Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per HE Per GSC
V Per HE Per GSC
V Per AP Per
V Per AP Per GSC
V Per AP Per GSC
Table continued
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per AP Per GSC
V Per CCS SVS IRAS GSC
V Per HR HD B BD SAO GSC
V Per Gliese G LHS Ross GSC
BG Phe CoD CPD SAO B JL
HIP GSC
UU Pic V
UV Pic CoD EXOSAT EXO
GSC
UW Pic RE RE J RX J
UX Pic IRAS RAFGL S GSC
UY Pic HD G CoD CPD SAO
IRAS RE RE J GSC
GSC
BI Psc GB B GBS
BK Psc BD LHS RE RE J
GSC
BL Psc BD RE RE J GSC
BM Psc No
BN Psc No
BO Psc LDS A EXOSAT EXO GSC
BP Psc IRAS Stephenson H PDS GSC
BQ Psc SX Phe type var
BR Psc BD SAO IRAS Gliese
G LHS LFT LTT Laland NSV
GSC
BS Psc BD E GSC
BT Psc HD F BD SAO GSC
BU Psc HD A BD SAO GSC
GSC
UV PsA HD F CoD CPD
SAO GSC
UW PsA HD F CoD CPD
SAO GSC
V Pup PNN of NGC PK He IRAS
V Pup HD A BD CPD SAO
GSC
WX Pyx E PYX
WY Pyx PC IRAS CSS NSV GSC
WZ Pyx ELHS IRAS
XX Pyx CoD CPD GSC
TW Ret IRAS
TX Ret HD F CoD CPD SAO
GSC
TY Ret IRAS GSC
TZ Ret R Probable non member of the Reticulum system might b e a distant member of the LMC
Table continued
V Sge HD F BD SAO GSC
V Sge IRAS
m
V Sgr Sakurai s ob ject Sakurai Novalike star in Sgr on ESO SRC
J plate of May Brightened considerably by early then
continued brightening b ecoming gradually redder A hint to oscillations in
late The central star of an old planetary nebula A candidate nal
helium ash ob ject Resembles FG Sge but shows more rapid development
V Sgr IRAS
V Sgr IRAS
V Sgr IRAS
V Sgr Liller s Nova candidate Possible Nova Sgr
V Sgr IRAS
V Sgr IRAS
V Sgr IRAS
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr Rosino F NGC eld NSV
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr Rosino F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr Rosino F NGC eld
V Sgr Rosino F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr Rosino F NGC eld
V Sgr F NGC eld
V Sgr No
V Sgr Nova Sgr Sakurai
V Sgr Nova Sgr No Sakurai
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr F NGC eld
V Sgr Peculiar var in Sgr Wakuda
V Sgr SV in Sgr Galaxy Foreground star
V Sgr SV in Sgr Galaxy Non member of the Sgr Galaxy
V Sgr HD G BD SAO GSC
V Sgr HD B BD SAO HIP
GSC
V Sgr HD F CoD CPD
GSC
V Sgr HD G CoD CPD SAO
GSC
V Sco HD A BD CPD SAO
IRAS BV NSV GSC
V Sco HR HD A CoD CPD
SAO IDS S A GSC
V Sco HD B CoD CPD
SAO GSC
V Sco Ton NSV
Table continued
V Sco Ton in the Oph region
V Sco Ton in the Oph region
V Sco CPD Seggewiss NGC Braes GSC
V Sco X ray Nova Sco GRO J
V Sco CPD Seggewiss NGC Braes NSV
GSC
V Sco HD Oa CoD CPD SAO
WR He LSS GSC
V Sco HR HD Oe CoD CPD
SAO IDS S LSS Eggen NGC
Prager CSV NSV HIP GSC
V Sco HD B CoD CPD
SAO IRAS He LSS Wray
GSC
V Sco IRAS
AY Scl IRAS GSC
AZ Scl CoD SB GSC
BB Scl HD G CoD CPD SAO
IRAS Gliese ABC RE J NSV
HIP GSC
Scl alpha Scl HR HD B CoD
CPD SAO IRAS NSV GSC
Scl sigma Scl HR HD A CoD
CPD SAO GSC
V Sct MWC IRAS GSC
V Sct HD B p BD SAO MWC
LS IV GSC
NY Ser PG SER HV CSV NSV
NZ Ser MWC AFGL IRAS GSC
OO Ser DEOS Ser
TU Sex V in Sex dSph Galaxy Non member of the galaxy
V Tau HD G BD SAO HIC
GSC
V Tau IRAS
V Tau HI I Pleiades Zinner CSV NSV GSC
V Tau BD SAO F HI I Pleiades Zinner
CSV NSV GSC
V Tau No
V Tau K Pleiades TCSN Plf
V Tau Plf NSV
V Tau HI I Pleiades Zinner CSV NSV GSC
V Tau HI I Pleiades Zinner CSV NSV GSC
V Tau Flare star in the Pleiades region Pels GSC
V Tau RE J RE GSC
V Tau No
V Tau HD G BD SAO DHK
GSC
V Tau LkCa JH HBC GSC
V Tau Anon Anon near LkCa HBC GSC
V Tau LkCa GSC
V Tau LkCa HBC GSC
V Tau Tau HR HD F BD SAO
VB VA Hyades CSV NSV GSC
Table continued
V Tau DHK IRAS GSC
V Tau B GSC
V Tau VA Hyades GH Leiden GSC
V Tau LkCa GSC
V Tau VA Hyades GH GSC
V Tau B
V Tau B GSC
V Tau B
V Tau B GSC
V Tau B GSC
V Tau BD Wa Tau TAP HBC GSC
V Tau B
V Tau HV CSV NSV GSC
V Tau B
V Tau B GSC
V Tau LkCa HBC GSC
V Tau HR HD F BD SAO VB
Hyades NSV GSC
V Tau B GSC
V Tau B GSC
V Tau Tau HR HD G BD SAO
IDS N A IRAS Gliese HIP
GSC
QT Tel IRAS GSC
QU Tel EC GSC
XY Tri No
XZ Tri No
YY Tri IRAS
CP Tuc AX J AS
EW UMa BD GSC
EX UMa BV CSV NSV GSC
EY UMa GR
EZ UMa HR HD K BD SAO
IRC AFGL IRAS HIC GSC
FF UMa HD G BD SAO RE HIC
GSC
FG UMa HD K BD SAO IRAS
HIC GSC
FH UMa WGA J
FI UMa HR HD A BD SAO
GSC
FK UMa BD HIC GSC
MN Vel HD Ma CoD CPD SAO
IRAS CSV NSV GSC
MO Vel HD A CoD CPD SAO
GSC
MP Vel HD F CoD CPD SAO
GSC
MQ Vel IRAS
MR Vel RX J
MS Vel HD Ma CoD CPD SAO
IRAS HIP GSC
MT Vel HD F CoD CPD SAO
HIP GSC
MU Vel IRAS
MV Vel I Vel HR HD B p CoD
CPD SAO MWC GSC
Table continued
MW Vel HD Mc CoD CPD ISS
IRAS GSC
IQ Vir HR HD A BD SAO
GSC
IR Vir HV CSV NSV GSC
IS Vir HD K BD SAO H HIC
CSV NSV GSC
IT Vir HD Map BD SAO IRAS
HIP GSC
IU Vir EC
IV Vir BD GSC
V Vul CCS IRAS TASV GSC
V Vul Vul HR HD B BD SAO
EUVE J HIP CSV NSV
GSC
V Vul Rob erts WR GSC
V Vul HR HD B BD SAO
HIP NSV GSC
V Vul LD
V Vul Star NGC GSC
V Vul BD Star NGC GSC
V Vul HD A BD SAO HIP
GSC
V Vul No GSC
V Vul No
V Vul No
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M L Hazen AJ No
L Rosino Asiago Contr No
L Plaut AsAp Suppl No
IAU Circ No
IAU Circ No
M L Hazen AJ No
D Ho eit IBVS No
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J C Thomas I Pachoulakis IBVS No
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J Manfroid P Renson AsAp No
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Yu K Bergner V P Kozlov A A Krivtsov A S Miroshnichenko R V Yudin N Yu Yutanov
K G Dzhakusheva K S Kuratov D B Mukanov Astro zika No
R W Goodrich ApJ Suppl No
K W Hodapp J L Hora J T Rayner A J Pickles E F Ladd ApJ No
M Mateo P Fisher W Krzeminski AJ No
E Hertzsprung Leiden Ann part A
N D Melikian I Jankovics J Kelemen IBVS No
G Haro E Chavira G Gonz alez Ton Bol No
E S Parsamian Burakan so obshch No
J Kelemen IAU Symp No
F van Leeuwen P Alphenaar J Brand AsAp Suppl No
R D Je ries M R Burleigh R M Robb AsAp No L
D H Kaiser M E Baldwin J Gunn D Terrell Ch Stephan B Hakes IBVS No
K N Grankin IBVS No
G H Herbig F J Vrba A E Rydgren AJ No
J Bouvier E Covino O Kovo E L Mart n J M Matthews L Terranegra S C Beck AsAp No
K Krisciunas R A Crowe K D Luedeke M Roberts MN No
A S Hojaev IBVS No
General Catalogue of Variable Stars Team archive
H L Giclas R Burnham Jr N G Thomas Lowell Bull No
A S Hojaev IBVS No
J M Gomez Forrellad E Garcia Melendo IBVS No
C Koen D O Donoghue R S Stobie D Kilkenny R Ashley MN No
D Buckley SAAO Newsletter No
J Vandenbroere IBVS No
K Locher BBSAG Bull No
G Romano IBVS No
K P Singh P Szkody P Barrett N E White E Fierce A Silber D W Hoard P J Hakala V Piirola
K Sohl ApJ No L
R L Schutt AJ No
P Martinez IBVS No
C Motch G Hasinger W Pietsch AsAp No
J M Gomez Forrellad E Garcia Melendo IBVS No
A Jorissen O Hennen M Mayor A Bruch C Sterken AsAp No
R S Stobie D O Donoghue R Ashley C Koen A Chen D Kilkenny MN No L
M Niehues A Bruch H W Duerbeck ESO Messenger No
E Rudolf MVS H
M Col lins The Astronomer No
D P Hube G C L Aikman PASP No
I I Antokhin A M Cherepashchuk T R Irsmambetova S Yu Shugarov IBVS No
J M Benk o ApSS No
L Dahlmark IBVS No
J H Pena R Peniche S H Diaz Martinez IBVS No
F Haberl J R Thorstensen C Motch A Schwarzenberg Czerny M Pakul l A Shambrook W Pietsch
AsAp No
D G Turner G R Grieve W Herbst W E Harris AJ No
R S Stobie P N Okeke D A H Buckley D O Donoghue MN No L
G A Richter J Greiner ApSS Library
J Dachs D Kaiser AsAp Suppl No
G A Bakos BAC No
C Waelkens H van Winckel E Bogaert N R Trams AsAp No
B J Hrivnak Sun Kwok K M Volk ApJ No
S Messina E F Guinan IBVS No
J R Stau er L W Hartmann ApJ Suppl No
E H Olsen AsAp Suppl No
F Rufener AsAp Suppl No
V G Kornilov I M Volkov A I Zakharov V S Kozyreva L N Kornilova A M Krutjakov A V Krylov
A V Kusakin S E Leontiev A V Mironov V G Moshkalev T M Pogrosheva V N Sementsov
Kh F Khaliul lin Sternberg Inst Trudy
D Kilkenny D C B Whittet J K Davies A Evans M F Bode E I Robson R M Ban eld SAAO
Circ No
M M Zakirov Tashkent Tsirk No
A W J Cousins SAAO Circ No
C Ho meister AN Nr
P M Garnavich P Szkody R M Robb D R Zurek D W Hoard ApJ No L
E A Kolotilov Astron Zh Russia No
A J Delgado A J Alfaro J C Garc a Pelayo R Garrido AJ No
M Rodon o G Cutispoto S Messina AsAp No
J Bouvier AsAp Suppl No
K Tamikazawa VSNET Alert No
IAU Circ No
A U Landolt IAU Circ No
K N Grankin IBVS No
K N Grankin IBVS No
H C Thomas K Reinsch IAU Circ No
F Rufener P Bartholdi AsAp Suppl No
D J Axon D A Al len J Bailey J H Hough M J Ward R F Jameson MN No
ERRATUM
Dr G Williams has revealed a misprint in the rd Name List of newly designated variable stars IBVS
No In the introductory part when listing mistakes in the earlier Name Lists V Pup was claimed to
b e NSV The correct cross identi cation is however V Pup NSV N N SAMUS COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 4472
Konkoly Observatory Budapest 29 April 1997 HU ISSN 0374 – 0676
PHOTOELECTRIC MINIMA OF SELECTED ECLIPSING BINARIES AND MAXIMA OF PULSATING STARS
(BAV Mitteilungen No. 99)
In this 33rd compilation of BAV results, photoelectric observations obtained in the years 1996 and 1997 are presented on 93 variable stars giving 151 minima and maxima. All times of minima and maxima are heliocentric. The errors are tabulated in column “±”. The values in column O−C are determined without incorporation of nonlinear terms. The references are given in the section “remarks”. All information about photometers and filters are specified in the column “Rem”. The observations were made at private observatories. The photoelectric measurements and all the lightcurves with evaluations can be obtained from the office of the BAV for inspection. Table 1. Eclipsing binaries
Variable Min JD 24.. +/− Ph Obs O–C GCVS Rem
LO And 50422.2818 .0004 LB AG −0.0811 GCVS85 2) 50422.2820 .0007 LV AG −0.0809 GCVS85 2) ST Aqr 50394.2435 L KI −0.0228 GCVS85 1) CX Aqr 50369.3328 L KI −0.0008 GCVS85 1) V346 Aql 50343.3329 L KI −0.0053 GCVS85 1) V417 Aql 50303.4155 L KI −0.0415 BAVR9) 1) 50315.4511 .0003 LB AG −0.0411 s BAVR9) 2) 50315.4517 .0005 LV AG −0.0405 s BAVR9) 2) V609 Aql 50299.4307 L KI −0.0225 GCVS85 1) V724 Aql 50301.3793 L KI −0.0037 s BAVM57 1) AP Aur 50096.4104 L MS +0.0033 s BAVM67 1) CG Aur 50100.3663 L MS +0.0277 s GCVS85 1) GX Aur 50098.3305 L MS −0.0123 s BAVM69 1) 50158.3524 L MS −0.0111 BAVM69 1) IU Aur 50381.4989 .0005 LV AG −0.0013 s GCVS85 2) 50381.4998 .0009 LB AG −0.0004 s GCVS85 2) NSV2733Aur 50096.2680 L MS 1) 50101.5474 LMS 1) 50151.3335 LMS 1) TY Boo 50150.4382 L MS −0.0052 BAVM68 1) VW Boo 50086.6593 L MS −0.0229 BAVR8) 1) 50204.4183 L KI −0.0219 BAVR8) 1) AC Boo 50190.4053 L QU −0.0458 s GCVS85 5) 50193.4020 L QU −0.0448 GCVS85 5) FF Cnc 50115.3770 L FR −0.0336 BAVM65 1) 50123.3163 L FR −0.0331 BAVM65 1) 50140.5146 L FR −0.0357 BAVM65 1) 50152.4265 L FR −0.0321 BAVM65 1) 50156.3948 L FR −0.0333 BAVM65 1) 50158.3724 L FR −0.0404 s BAVM65 1) 50162.3462 L FR −0.0360 s BAVM65 1) 2 Table 1 (cont.)
Variable Min JD 24.. +/− Ph Obs O–C GCVS Rem
YY CMi 50157.3659 L KI +0.0123 GCVS85 1) AK CMi 50153.3079 .0003 LB AG −0.0128 GCVS85 2) 50153.3088 .0009 LV AG −0.0119 GCVS85 2) AV CMi 50152.3325 L KI +0.0011 GCVS85 1) V359 Cas 50344.5852 .0003 L AG +0.1426 GCVS85 1) U Cep 50203.394 L PTT +0.080 GCVS85 4) CW Cep 50300.5001 .0008 LB AG +0.0193 s GCVS85 2) 50300.5013 .0006 LV AG +0.0205 s GCVS85 2) SS Com50199.4782 L KI +0.0339 BAVR9) 1) CC Com 50188.4183 L KI −0.0086 s GCVS85 1) NSV6177Com 50187.4258 L MS +0.0106 s BAVM88 1) 50249.4683 L FR MS +0.0012 BAVM88 1) V370 Cyg 50153.6335 L MS −0.0115 GCVS85 1) V700 Cyg 50246.4825 .0003 L AG −0.0228 GCVS85 1) V961 Cyg 50152.6104 L MS −0.0617 GCVS85 1) 50153.6298 L MS −0.0612 s GCVS85 1) EX Del 50291.3807 L KI −0.0416 GCVS85 1) EF Dra 50301.5180 .0006 LV AG +0.0085 s BAVM63 2) 50301.5194 .0007 LB AG +0.0099 s BAVM63 2) TT Her 50249.4870 L KI +0.0267 GCVS85 1) AK Her 50248.4941 L KI +0.0041 GCVS85 1) HS Her 50281.500: .002 LB AG +0.807 GCVS85 2) 50281.500: .002 LV AG +0.807 GCVS85 2) 50304.426: .002 LB AG +0.809 GCVS85 2) 50304.427: .002 LV AG +0.810 GCVS85 2) 50313.4287 .0003 LV AG −0.0132 GCVS85 2) 50313.4293 .0003 LB AG −0.0126 GCVS85 2) DHK40 Her 50251.5088 .0003 LB AG 2) 50251.5090 .0004LVAG 2) 50291.4891 .0014LVAG 2) 50291.4924 .0011LBAG 2) NSV7457Her 50144.3803 L MS 1) 50144.5898 LMS 1) 50151.5038 LMS 1) FG Hya 50156.3407 L KI −0.0410 s GCVS85 1) CO Lac 50248.4857 .0007 LV AG +0.0097 s GCVS85 2) 50248.4860 .0004 LB AG +0.0100 s GCVS85 2) UV Leo 50190.4029 L KI +0.0166 GCVS85 1) XY Leo 50173.4305 L KI −0.0313 GCVS85 1) 50180.3974 L KI −0.0247 s GCVS85 1) XZ Leo 50175.3742 L KI +0.0213 GCVS85 1) AP Leo 50178.3981 L KI −0.0266 GCVS85 1) RT LMi 50154.3495 L MS −0.0009 s GCVS85 1) V404 Lyr 50158.5502 L MS −0.0648 GCVS85 1) 50248.4586 .0001 L AG −0.0627 GCVS85 1) BO Mon 50154.268: L KI −0.059 GCVS85 1) V449 Oph 50251.5146 L KI +0.0327 GCVS85 1) V508 Oph 50250.4693 L KI +0.0095 s GCVS85 1) V566 Oph 50252.4837 L KI +0.0417 GCVS85 1) V839 Oph 50284.4612 L KI −0.0846 s GCVS85 1) V1016 Ori 50080.494 L PTT +0.067 GCVS85 4) ZZ Peg 49934.4658 L MSR +0.1310 GCVS87 1) V482 Per 50106.2985 L MS +0.0346 BAVM68 1) CU Sge 50283.4426 L KI +0.0150 GCVS87 1) CW Sge 50279.4305 .0017 LB AG −0.0898 s GCVS87 2) 50279.4346 .0017 LV AG −0.0857 s GCVS87 2) 3 Table 1 (cont.)
Variable Min JD 24.. +/− Ph Obs O–C GCVS Rem
RS Sct 50286.4524 L KI +0.0032 GCVS87 1) DK Sct 50287.4765 L KI +0.0311 GCVS87 1) CU Tau 49710.2821 L MS −0.0758 GCVS87 1) 49710.4866 L MS −0.0774 s GCVS87 1) 49721.4198 L MS −0.0680 GCVS87 1) 49722.2436 L MS −0.0687 GCVS87 1) 49722.4498 L MS −0.0686 s GCVS87 1) 49723.2743 .0003 L AG −0.0685 s GCVS87 1) 50114.3675 .0003 L AG +0.0340 GCVS87 1) 50115.3979 .0003 L AG +0.0338 s GCVS87 1) HU Tau 50043.392 L QU +0.008 GCVS87 5) TX UMa50141.4465 L KRW +0.1221 GCVS87 5) TY UMa50192.5267 L FR −0.0594 s GCVS87 1) 50193.5905 L FR −0.0592 s GCVS87 1) 50194.4775 L FR −0.0586 GCVS87 1) 50195.3645 L FR −0.0579 s GCVS87 1) 50195.5409 L FR −0.0588 GCVS87 1) UY UMa50142.4061 L MS +0.0563 s GCVS87 1) 50142.5929 L MS +0.0551 GCVS87 1) 50152.3668 L MS +0.0526 GCVS87 1) 50192.4160 L MS +0.0561 s GCVS87 1)
Table 2. Pulsating Stars
Variable Max JD 24.. +/− Ph Obs O–C GCVS Rem
OV And 50115.2449 L BK −0.0038 MVS11,133 5) XX Boo 50249.4483 L BK +0.0196 GCVS85 5) CM Boo 50195.3938 L QU −0.0342 BAVM75 5) CS Boo 50088.6621 L MS −0.0041 IBVS2855 1) NSV6836Boo50175.5082 L MS 1) NSV7020Boo50190.4655 L MS 1) 50200.5584 LMS 1) HD32456Cam 50150.5520 LB GB +0.0089 BAVM84 7) 50150.5600 LV GB +0.0169 BAVM84 7) AQ Cnc 50186.4045 L BK −0.0474 GCVS85 5) RZ CVn 50152.4306 L KRW −0.2543 GCVS85 5) ST CVn 50153.500 L PS −0.061 GCVS85 3)red AD CMi 50153.3664 L KI +0.0072 GCVS85 1) RV CrB 50153.4574 L MS +0.0011 GCVS85 1) V798 Cyg 50314.4909 L BK −0.0680 GCVS85 5) GI Gem50081.5076 L BK +0.0685 GCVS85 5) 50153.4273 L BK +0.0661 GCVS85 5) BD Her 50282.5358 L KI +0.0857 GCVS85 1) 50300.5499 L BK +0.0913 GCVS85 5) DL Her 50247.4852 L KI +0.0217 GCVS85 1) LS Her 50252.5143 L BK +0.0122 GCVS85 5) V418 Her 50301.4673 L BK +0.0354 GCVS85 5) ET Hya 50151.4937 L BK +0.1043 GCVS85 5) DE Lac 50313.5138 L BK +0.0187 GCVS85 5) RR Leo 50170.4459 L QU +0.0229 GCVS85 5) 50194.4204 L QU +0.0206 GCVS85 5) ST Leo 50166.585 L PS −0.010 GCVS85 3) 50192.3934 L KI −0.0131 GCVS85 1) SZ Leo 50224.4201 L BK +0.2455 GCVS85 5) AA Leo 50166.465 L PS −0.055 GCVS85 3) 4 Table 2 (cont.)
Variable Max JD 24.. +/− Ph Obs O–C GCVS Rem
AX Leo 50189.4212 L BK −0.0187 GCVS85 5) BX Leo 50188.4399 L BK +0.0186 GCVS85 5) Y LMi 50146.3529 L BK +0.0548 GCVS85 5) 50170.4954 L BK +0.0716 GCVS85 5) 50190.4066 L BK +0.0529 GCVS85 5) EH Lib 50283.3665 L SG +0.0018 GCVS85 6) RW Lyn 50175.3572 L BK +0.0132 BAVM75 5) EX Lyr 50303.5011 L BK +0.0664 GCVS85 5) V462 Lyr 50287.5089 L BK +0.0616 GCVS85 5) V567 Oph 50286.5046 L BK +0.0624 GCVS85 5) FU Vir 50170.5380 L MS +0.1865 GCVS87 1) 50193.5098 L MS +0.1839 GCVS87 1) 50200.4203 L MS +0.2021 GCVS87 1)
Remarks:
AG Agerer, F. Tiefenbach MS Moschner, W. Lennestadt BK Birkner, C. Hagen MSR Moschner, J. Lennestadt PS Paschke, A. Rueti CH FR Frank, P. Velden PTT Petter, Dr.G. Dresden GB Groebel, R. Eckental QU Quester, W. Esslingen KI Kleikamp, W. Marl SG Sterzinger, Dr.P. Wien A KRW Krawietz, A. Hartha : = uncertain s = secondary minimum L = photoelectric observation - without filter LB = asabove-filter:B LV = as above - filter: V red = reducedresults 1) = photometer CCD 375x242 uncoated - without filter 2) = photometer EMI 9781A - filter: V=GG495,1mm; B=BG12,1mm+GG385,2mm 3) = photometer Cryocam 89A - without filter 4) = photometer TC-211 - without filter 5) = photometer ST-7 - without filter 6) = photometer SSP5 7) = photometer 1P21 - filter: V=GG14,2mm; B=BG12,1mm+GG13,2mm BAVM nn = BAV Mitteilungen No. nn BAVM 57 = BAV Mitteilungen No. 57 = IBVS No. 3555 BAVM 63 = BAV Mitteilungen No. 63 = IBVS No. 3811 BAVM 65 = BAV Mitteilungen No. 65 = IBVS No. 3859 BAVM 67 = BAV Mitteilungen No. 67 = IBVS No. 3942 BAVM 84 = BAV Mitteilungen No. 84 = IBVS No. 4306 BAVM 88 = BAV Mitteilungen No. 88 = IBVS No. 4386 BAVR 8) = BAV Rundbrief 32,122 ff BAVR 9) = BAV Rundbrief 33,152 ff GCVS nn = General Catalogue of Variable Stars, 4th ed. 19
Franz AGERER Joachim HUEBSCHER Bundesdeutsche Arbeitsgemeinschaft f¨ur Ver¨anderliche Sterne e.V. (BAV) Munsterdamm 90, D-12169 Berlin Germany Erratum (from IBVS 6048) TY UMa & 50192.5267 FR & has to be deleted \\ TY UMa & 50193.5905 FR & has to be deleted \\ TY UMa & 50194.4775 FR & has to be deleted \\ TY UMa & 50195.3645 FR & has to be deleted \\ TY UMa & 50195.5409 FR & has to be deleted \\
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
GSC IS A NEW BINARY STAR
CCD images taken at the Bohyunsan Optical Astronomy Observatory BOAO with
the m telescop e and at the Kyung Hee Astronomy Observatory KHAO with the
m telescop e on Jan Mar show that the star GSC V
h m s 0 00
lo cated at R A Decl equinox varies in magnitude
From the preliminary analysis of the light curve I derive the p erio d of day with
mag in R variation in primary and mag in R variation in secondary minimum
and GSC as the comparisons It is considered as an Algol using GSC
type eclipsing binary star The light curve shown is the combined data of Jan
and Feb using GSC as a comparison The average B V colour
m
index of this new variable is out of minima
0.50
0.75
1.00
1.25 DEL MAG.
1.50
1.75
2.00 0.0 0.2 0.4 0.6 0.8 1.0
PHASE
Figure Light curve of the new variable R lter data
Minhwan JANG
Dept of Astronomy and Space Science
Kyung Hee University Yongin Kyungki Do Korea
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
April
HU ISSN
THE ECLIPSING BINARY STAR MS
The sky was surveyed in the X ray region of the sp ectrum by the Einstein satellite and
the Extended Medium Sensitivity Survey Sto cke et al included MS
with the brightness given as in V and the sp ectral type as F V This star is also listed
in the Hubble Telescope Guide Star Catalog GSC Jenkner et al as GSC
The automated m telescop e Cousins R lter and CCD camera of the Climenhaga
Observatory of the University of Victoria was used to make these photometric observations
Robb et al The frames had the bias subtracted and were at elded in the usual
manner using IRAF The magnitudes were found from ap erture photometry using the
package PHOT The x y pixel co ordinates of each star for photometry were found from
insp ection of a few frames and were used as starting p oints for the Gaussian centering
option which precisely centered the arc second ap erture on each star for each frame
and the check star The primary comparison star used was SAO GSC
The precision of the photometry can b e estimated from the standard was GSC
deviation of the di erences in R magnitude for these two stars for each night This
standard deviation varies from on a clear night to on a p o or night Night to
night variations can b e estimated from the mean and standard deviation of the nightly
mean R magnitude di erences b etween the comparison and check stars The overall mean
is : and the standard deviation of a night ab out this mean is : The uncertainty
in a measurement b etween the comparison and variable star is usually smaller b ecause
the check star was fainter Due to the small eld of view rst order extinction e ects were
negligible and no corrections have b een made for them Nor have corrections b een made
for the colour di erence b etween the stars to transform it to a standard system
Photometric observations were b egun April continued on fteen more nights in
the spring of one night in and one night in Variations of brightness
from night to night were so on obvious and the few long nights showed that the p erio d of
the variation must b e more than a few hours A sine curve was t to various p erio ds and
reveals a minimum average chi squared at an inverse p erio d of : : days as seen
in Figure This is half the orbital p erio d and other minima in the gure corresp ond to
aliases and multiples of the real p erio d Times of minimum light have b een found from
the metho d of Kwee and Van Woerden to b e
and which yield a p erio d of
HJD of Primary Minimum E
where the uncertainties in the nal digit are given in brackets These uncertainties have
b een underestimated b ecause no allowance has b een made for the asymmetry in the
1
IRAF is distributed by National Optical Astronomy Observatories which is op erated by the Asso ciation of Universities for Research in Astronomy Inc under contract to the National Science Foundation
minima A plot of the di erential R magnitudes phased at this p erio d is shown in Figure
for the data from ab ove and b elow Di erent runs are plotted with di erent
symbols so that brightness variations from night to night can b e seen The data
have b een shifted up magnitudes but the apparent di erence b etween mean curves
is ab out magnitudes indicating that most of the light curve has shifted fainter
ab out magnitudes from to The b ottom of primary minimum was at an
intermediate level in and
0.0015
0.0013
0.0011 Chi-Sqr
0.0009
0.0007 0.2 0.7 1.2 1.7 2.2 2.7
Inverse Period in Days
Figure Chi squared t to a single sine curve for various p erio ds
Figure The light curve in R for ab ove and b elow
2.10
2.12 R Magnitude 2.14
2.16 9832.70 9832.80 9832.90
Julian Date - 2440000
Figure Di erential R magnitudes for Julian Date showing a are
Observations on the Julian Date are plotted in Figure A large are o ccured
at approximately UT and lasted until UT with an amplitude of magnitudes
The p eak p ower of the are is of the same order of magnitude as that of the active star
RE Robb which is one of the largest ever seen
1.00 Flux
0.90
0.00 0.25 0.50
Phase
Figure Di erential R magnitudes with example mo del
The light curve mo delling program Binmaker Bradstreet was used to make
a light curve which approximates the data as seen in Figure The parameters used are
temp eratures of K and K and relative p olar radii of and for the
hot and co ol star resp ectively The mass ratio was assumed to b e and the inclination
was One sp ot was used which had a co latitude of longitude of radius of
and a temp erature factor of All other inputs were set at values appropriate for these temp eratures
Figure Scale mo del of the system at phase
A scale mo del of the system at phase is shown in Figure again pro duced by
Binmaker Bradstreet The sizes and shap es of the stars are approximately
correct for a F V primary and a K V secondary star The size and longitude of the sp ot
are well constrained but the latitude of the sp ot is arbitrary A b etter t can b e obtained
by adding more sp ots but with less con dence in their prop erties
MS is an eclipsing binary star with active regions on its surface causing
brightness variations ares and X ray emission from an active corona Further observa
tions will b e interesting to increase the precision of the p erio d in order to lo ok for mass
transfer and magnetic braking
R M ROBB
Climenhaga Observatory
of the Dept of Physics and Astronomy
University of Victoria
Victoria BC CANADA V W P
Internet robb uvic ca
References
Bradstreet D H Binary Maker User Manual Contact Software Norristown
PA USA
Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ
Kwee K K and Van Woerden H Bul l Astr Inst Neth
Robb R M and Honkanen N N in A S P Conf Ser Automated Telescopes
for Photometry and Imaging ed Adelman Dukes and Adelman
Robb R M IBVS No
Sto cke J T Morris S L Gioia I M Maccacaro T Schild R Wolter A Fleming
T A and Henry J P ApJ Sup
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
DISCOVERY OF AN ECLIPSING BINARY STAR IN AURIGA
New photo electric observations of BD HD SAO have shown
that it is an Algol type eclipsing binary star with a p erio d slightly longer than either or
days
A check of the GCVS s up dated version ftp cdsarc u strasbg fr cats I I B cata
log Z and the recent volumes of the Information Bulletin on Variable Stars did not reveal
any previously known variable at the p osition of BD
BD with a sp ectral type B was observed as the check star during the obser
vations of early type eclipsing binary TT Aur Observations were p erformed in nights
b etween February and on April at the National Observatory by using
a SSP A photometer attached to a m Cassegrain telescop e
The reduced U B and V di erential observations of the check star BD
with resp ect to the comparison star BD show that BD is a detached
eclipsing binary see Figure The constancy of the comparison star to TT Aur was
shown b efore cf Wachmann Only the descending branch of two eclipse minima
were observed The observations with large scatter at the shoulder of the eclipse minimum
were made at very large zenith distance The following preliminary ephemeris has b een
computed for the future observations
d
MinI HJD : E
or
d
MinI HJD : E
This work was supp orted by The Scienti c and Technical Research Council of Turkey
The data have b een obtained during the test p erio d of m telescop e of the National
Observatory of Turkey http astroa physics metu edu tr tug home html I thank to
Osman Demircan for the encouragement and help at di erent stages of this work to
Fevzi Cetinand Cahit Ye silyaprak for their help in observations and Umit K z lo gluand
Ilhami Ye gingilfor their technical supp ort at the Observatory
Hasan AK
Ankara University Observatory
Science Faculty Tando gan
Ankara TURKEY
ak astro science ankara edu tr
Reference
Wachmann A A A AS
1.0 1.2 • •• • • • • • • • •• • • • 1.4 • •••• ••••• ••• 1.6 •••• 1.8 •• • B 2.0 •
∆ • 2.2 2.4 To=50488.57 2.6 P=2.02 • 2.8 3.0 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 1.1 1.2 phase
1.0 1.2 • •• • •• •• •• • •• • • 1.4 • •• •• •••• • • • • 1.6 •••••• 1.8 •• • B 2.0 •
∆ • 2.2 2.4 2.6 P=1.01 • 2.8 3.0 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 1.1 1.2
phase
Figure The light curve of BD
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
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May
HU ISSN
IMPROVED POSITIONS FOR SONNEBERG VARIABLES PART
The Sonneb erg Observatory is well known in the world for its large plate archive and
also for its contribution to the variable stars research eld with almost variables dis
covered there However most of these stars have had only approximate p ositions rep orted
so the follow up observations and cross referencing to other catalogues is sometimes dif
cult Because many Sonneb erg variables are lo cated on the elds of the PICA pro ject
one indep endent part of the pro ject is to determine more precise co ordinates for these
stars This pap er is the rst one devoted to the p osition improvements for Sonneb erg
variables
My work on the PICA pro ject signi cantly sp eed up after the USNO A catalogue
Monet et al was kindly supplied by D G Monet The identi cation pro cedure
now used is as follows the A catalogue is visualized on computer screen by means
of a sp ecial program written by the author and then compared with the published
chart When any problem app ears then Digitized Sky Survey DSS provided by STScI
is used in conjunction with Cotton s Fitsview utility which is also used
for p osition determination of ob jects present on DSS but not included in A catalogue
When no ob ject is found neither in A nor in DSS then the co ordinates are either
estimated according to the p osition marked on chart or preferably measured from direct
CCD images or plate scans
Table gives precise p ositions for ob jects having published nding charts in MVS
North on these charts is on the top with exceptions marked directly on
individual charts However there are deviations from this rule and these are noted in
remarks Comments from original pap er of Ho meister were used when p ossible
The source of the p osition is co ded as follows A A C CCD D DSS Fitsview
00
E estimate P plate scan Positions should b e precise to for A C P co de and
00
to for D co de The p ossible error for E co de is noted in remarks Identi cation with
GSC is given where p ossible No other identi cations were searched for As on the charts
is not every time given nal designation it was not known at the time when charts were
published provisional designation is given in the table to o The di erences resulting
from a comparison with the p ositions given in GCVS in the sense new GC V S are also
shown where is given is seconds of time and is given in minutes of arc
Table
Prov desig Name RA Dec GSC s Remark
AT Tau A : :
AW Tau A : :
AY Tau A : :
CG Tau D : :
BB Tau A : :
BC Tau A : :
BD Tau A : :
CN Tau A : :
CO Tau A : :
Table continued
Prov desig Name RA Dec GSC s Remark
BF Tau A : :
BO Aur A : :
BF Gem A : :
DP Gem A : :
BR Aur A : :
BB Aur A : :
BT Aur A : :
BS Aur A : :
BH Gem A : :
BV Aur A : :
CQ Mon A : :
CE Mon A : :
DI Mon A : :
BU Mon A : :
CG Mon A : :
DL Mon A : :
CL Mon A : :
BP Mon A : :
DS Mon A : :
V Mon A : :
DX Mon A : :
DZ Mon A : :
EH Mon A : :
EI Mon A : :
EK Mon A : :
EM Mon A : :
EX Mon A : :
BQ Mon A : :
EZ Mon A : :
FF Mon A : :
BR Mon A : :
FI Mon A : :
BW Mon A : :
FK Mon A : :
FP Mon A : :
FR Mon A : :
DZ CMa A : :
DR CMa A : :
DS CMa A : :
HN Pup A : :
KP Mon A : :
EE Pup A : :
FV Pup A : :
FX Pup A : :
HO Pup A : :
NSV A : :
BF Pup A : :
FZ Pup A : :
GH Pup A : :
GK Pup A : :
GN Pup A : :
GO Pup A : :
GQ Pup A : :
EG Her A : :
NR Her A : :
LW Her A : :
FS Her A : :
LY Her A : :
EH Her A : :
EI Her A : :
Table continued
Prov desig Name RA Dec GSC s Remark
EK Her A : :
LZ Her A : :
EL Her A : :
EN Her A : :
EO Her A : :
FT Her A : :
EP Her A : :
ER Her A : :
ES Her A : :
EU Her A : :
FW Her A : :
EV Her A : :
MN Her A : :
EW Her A : :
EY Her A : :
EZ Her A : :
FF Her A : :
FY Her A : :
FH Her A : :
FI Her A : :
Ross CG Her A : :
V Oph A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
NSV A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
NSV A : :
V Oph A : :
SV Oph A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
Table continued
Prov desig Name RA Dec GSC s Remark
V Oph A : :
V Oph A : :
V Oph A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
AX Ser A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
AY Ser A : :
V Oph A : :
Remarks
Two entries for the same star in A The p osition given in the table is an average
CG Tau mean p osition of a close double not known which comp onent varies
FK Mon north on the b ottom
BF Pup not sure northernmost in a small triangle
m
GH Pup GCVS p osition in error by
GN Pup southern comp onent of a double star the northern one is GSC at a distance of
00
ab out
EG Her north to the right side
00
EL Her nearby GSC represents another ob ject ab out to east On DSS it seems that
these two ob jects are connected with some nebulosity There also exist GSC which
is probably EL Her in maximum and blended with its eastern neighbour
FF Her north on the b ottom
FY Her north to the right side not left
V Oph and NSV two indep endent charts in one frame Should b e vertically divided into
two square frames
The author would like to thank D G Monet for providing the USNO A catalogue
Jan MANEK
Stef anikObservatory
Pet r n
Praha
Czech Republic
e mail jmanek mbox vol cz
References
Cotton W D Fitsview v
see also http www cv nrao edu bcotton fitsview html
Ho meister C Astron Nachr
Mitteilungen uber Ver anderliche Sterne No
Monet D G et al USNO A V U S Naval Observatory Washington DC
see also http www usno navy mil pmm
STScI http stdatu stsci edu dss
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
ECLIPSE OBSERVATIONS OF AB ANDROMEDAE
h m s 0 00
AB Andromedae G G V R J is a frequently
observed close eclipsing binary This system is on the AAVSO list of eclipsing binaries
Baldwin and Samolyk The AAVSO bulletin rep orts eclipse minimum observations
made b etween the dates JD and An O C plot of the AAVSO
observations shows the published p erio d of days is decreasing with time
The present note describ es CCD photometry of AB And from the University of Iowa
Automated Telescope Facility lo cated in Iowa City Iowa The system consists of an cm
00
refractor a Sp ectrasource HPC CCD camera format binned pixels p er
pixel and a Johnson R band lter We used the nearby Guide Star Catalog GSC
h m s 0 00 h m s 0 00
stars GSC GSC
h m s 0 00
GSC J as check stars and the nearby star GSC
h m s 0 00
J as the comparison star A second exp o
sure of a eld containing AB And as well as the check and comparison stars was rep eated
every two minutes for three hours Di erential ap erture photometry was p erformed by an
automated pro cedure after aligning all images to a common stellar reference No air mass
or color corrections were applied The AB And system was observed during the nights of
Octob er UT and July UT Light curves were pro duced by plotting the
data obtained on these nights These plots are shown in Figure
Figure Two light curves for AB And from the nights of Octob er and July The
primary minimum of Octob er has b een sup erimp osed over the secondary minimum of July The abscissa is correct for Octob er
Figure A sample folded light curve The MHJD of minima has b een set to zero and the absolute
value of the MHJD has b een plotted The data shown is for Octob er UT
We observed a primary minimum at Helio centric Julian Date
HJD and a secondary minimum at HJD The errors in the minima
were found by folding the light curves i e setting the HJD at the time of minimum
to zero and plotting the di erential magnitude versus the absolute value of the mo di ed
HJD to pro duce a folded light curve for each night As our original curves were almost
p erfectly symmetric any shift in the minimum HJD greater than HJD caused
noticeable discrepancies b etween the two halves A folded light curve is shown in Figure
The O C measurements available from the AAVSO compilation clearly show that the
linear ephemeris published in the AAVSO bulletin
JD E
min
where JD is the time of primary minima is not precise any longer Demircan et
min
al has shown that a sinusoidal function provides a satisfactory t to the O C
residuals from a linear ephemeris
JD JD E A cos E T P
min s s s
where JD is the reference ep o ch A is the semi amplitude in days T is the p erio d
s s
in orbital cycles and P is the minimum time in units of E Numerical values of the
s
parameters are listed in the table
Figure O C graph of the historical data of Demircan et al along with the minima rep orted in
this note The data has b een tted with Demircan s ephemeris and the ephemeris rep orted in this note
Our times of minima do not agree with this ephemeris They are consistent with a
phase shift of days with resp ect to Demircan et al s ephemeris We have solved for
a new p erio dic ephemeris that ts b oth his historical data and our data The table b elow
shows our revisions to Demircan s ephemeris The change in JD is due to a residual
o set required to b est t all data p oints
Reference JD A T P
s s s
Demircan et al
Nellermo e and Reitzler this note
Figure is a plot of Demircan s data along with the minima rep orted in this note
tted with the revised ephemeris equation The t has a ro ot mean square uncertainty
of days
This sinusoidal trend in the O C plot suggests the presence of a third b o dy with
a p erio d of approximately years Demircan et al suggest a similar result with a
third b o dy p erio d of years
The authors would like to thank Leslie Simon Sauerbrei Britt Scharringhausen and
Professors Lawrence A Molnar and Steven R Spangler for their help with this note
Interested parties can obtain the raw photometric data from the authors at the follow
ing e mail address atfproj astro physics uiowa edu
This research has b een supp orted by the Iowa Space Grant Consortium and the Na
tional Science Foundation
B L NELLERMOE
L E REITZLER
Van Allen Observatory
Dept Physics and Astronomy
University of Iowa
Iowa City IA
USA
References
Baldwin M and Samolyk G AAVSO Observed Minima Timings of Eclipsing
Binaries No
Demircan O et al Mon Not R Astron Soc
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
CORRECT POSITION OF MX SAGITTAE
During my work on PICA project Precise Identi cation and Co ordinate Adjustment
of ab out variables on stars in the eld of U Sge I found in that MX Sge
cannot b e lo cated at its nominal p osition Ski had also noticed this fact but he
was unable to nd its correct lo cation As nding chart was published by Rosino and
Guzzi I was successful after some e ort and found that the p osition rep orted by
Rosino and Guzzi for their star MX Sge exhibits quite large error in declination
print error
Precise p osition was extracted from Digitized Sky Survey provided by STScI
used in conjunction with Cotton s Fitsview utility b ecause the star is not in the
USNO A catalogue The correct p osition is as follows
h m s 0 00
RA : Decl :
This large declination error has also one imp ortant consequence MX Sge is actually
situated in Aquila similarly to WX Eri which is in Taurus despite its name
Jan MANEK
Stef anikObservatory
Pet r n
Praha
Czech Republic
e mail jmanek mbox vol cz
References
Cotton W D Fitsview v
see also http www cv nrao edu bcotton fitsview html
Monet D G et al USNO A V U S Naval Observatory Washington DC
see also http www usno navy mil pmm
Rosino L and Guzzi L Astron Astrophys Suppl Ser
Ski B IBVS No
STScI http stdatu stsci edu dss
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
FUOR V Cyg TWO YEARS IN LOCAL MINIMUM
The star V Cyg b elongs to a small number group of eruptive FU Orionis variables
or Fuors Herbig Hartmann et al Since p eak light in the light curve
of the Fuor V Cyg exhibits most remarkable and dynamic changes in comparison
with more quiescent b ehavior in p ost outburst stage of two other b est studied Fuors FU
Ori and V Cyg Over the p erio d V Cyg had declined by ab out of
mag in B Figure In contrast FU Ori and V Cyg have a much slower declining
rates Throughout p ost outburst states b oth FU Ori and V Cyg have faded by
and mag in B resp ectively Moreover in V Cyg
had suddenly dimmed by mag in B Ibrahimov Note that the drop in
magnitude of V Cyg is similar to the one of V Cyg In the observations
of V Cyg were continued at Mt Maydanak observatory These observations have
b een obtained using the same equipment as describ ed in Ibrahimov These new
observations are combined with existing ones and used to construct the gures Figure
shows historical pg B light curve of the Fuor based on all available data which have b een
compiled by the authors and joined with Mt Maydanak database Figure shows a more
detailed V light curve of the Fuor based on our own observations in Figure
shows the brightness and color variations of the Fuor in based only on Mt
Maydanak observations
The gures allow to conclude that the Fuor still remains in lo cal minimum The
observations of Figure show that the star has no visible trend neither to
increase nor to following decrease its brightness Besides Figures and indicate the
presence of a gradual increase in the amplitude of light variations from V in
to V in The similar increases in the amplitudes of light variations are observed
in U B and R to o Since mid eighties to the amplitudes have increased from to
in U from to in B and from to mag in R
The evolution of the colors of the Fuor in is most interesting Figure
Despite the continuation of smo othed large scale fading till the colors had practically
constant values in cf the Table in Ibrahimov During the next ve
years the light curve shows a slight b owl shaped increase in the brightness This
increasing light is accompanied by monotonic decrease of the average value of the U B
color from to mag At the same time the other two colors did not change
Thus b oth colors have remained practically constant during B V
and V R mag During the light curve of the star exhibited saw tooth
variations These variations are out of phase with similar saw tooth color variations i e
redder colors corresp ond to higher brightness and vice versa The drop in magnitude of V Cyg has led to common reddening by mag of all three colors of the star
Figure Historical pg B light curve of V Cyg in
Figure Detail V light curve of V Cyg in
Figure Brightness and color variations of V Cyg in
Now it can b e de ned that during the decade since mid eighties to the general
changes of the colors are ab out of mag for U B and ab out of mag for b oth B V
and V R
Thus we conclude that the new active phase of photometric changes of the Fuor
V Cyg b egan in The detected increase in the amplitude of light variations
since remarkable b ehavior of the colors and the drop in magnitude of V
Cyg provide strong supp ort to the conclusion The mentioned changes except the
drop in magnitude of V Cyg have no analogies in the photometric b ehavior of the
other Fuors New observations of the Fuor in this active and interesting state are very
imp ortant and useful
V M IBRAHIMOVA
M A IBRAHIMOV
Astronomical Institute
Astronomical str Tashkent
Uzb ekistan
valery astro gov uz
References
Herbig G H Astrophys J
Hartmann L W Kenyon S J Hartigan P in Protostars and Planets I I I eds E H
Levy and J Lunine Tucson Univ Arizona Press p
Ibrahimov M A IBVS No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
ALDEBARAN DISCOVERY OF SMALL AMPLITUDE
LIGHT VARIATIONS
Aldebaran Alpha Tau HD is one of the nearest and brightest red giant
stars It is a standard sp ectroscopic star with a sp ectral type of K I I I its average visual
magnitude is ab out mag with mean values of B V and U B
Aldebaran has a relatively well determined parallax of arcseconds that
should improve after the Hipparcos parallax is published The star also has relatively
high space motions with resp ect to the sun indicating that it is an old evolved disk star
Because of its brightness and accessibility from b oth ground based and orbiting obser
vatories it has b een a favorite target of numerous studies It is listed in the Bright Star
Catalog Ho eit and SIMBAD as a variable star and Petit classi es it as
an Lb type irregular star In the literature the visual magnitude range is from V
to most of these visual magnitude measurements are from surveys It should b e
noted that rep orted variability for bright stars such as Aldebaran can sometimes have
systematic errors due to saturation e ects of the detectors and the lack of nearby appro
priate comparison and check stars Hence some of the early visual magnitude values of
Aldebaran should b e treated with caution
The only concerted photometric study of Aldebaran was done by Krisciunas He
obtained V band photometry over observing seasons and
However the photometry was conducted only to nights p er season and a total of
only nights of data were obtained Krisciunas found no indication of variability of
greater than magnitude and rep orted Aldebaran to b e essentially constant within
the precision of his measurements He found mean values of hVi
magnitude and hB Vi magnitude The study of Krisciunas do es not
supp ort the relatively large light variations rep orted in the survey data but there
is not su cient coverage or precision to discern low amplitude brightness changes To
understand and b etter quantify the photometric b ehavior of Aldebaran we underto ok a
more intensive program of di erential photometry of this famous bright star
In August Aldebaran was added to the program of photometry of co ol giants
and sup ergiants b eing carried out by us at Wasatonic Observatory and Villanova Uni
versity Observatory The photometry rep orted here was conducted from August to
March at the Wasatonic Observatory Allentown Pennsylvania on nights using
an unco oled Optec photometer attached to a cm Schmidt Cassegrain telescop e The
detector employed was a silicon PIN photo dio de Di erential photometry was conducted
primarily with the V band but on several nights the star was also observed with the Wing
near IR three lter intermediate band system to measure TiO Wing The charac
teristics of the Wing three color system are given in Table The TiO index is calculated
according to Wing from
TiO Index A B B C
Table The Wing lter system
Filter Region Central Bandpass Measurements
Measured Wavelength FWHM
A TiO Band A A TiO Index
B IR Continuum A A B C Color Index
C IR Continuum A A B C Color Index
Table Photometric data
JD Visual magnitude
where A B and C are standardized magnitudes measured with these lters A near IR
color index is also formed from these observations and is useful for determining the
temp erature of co ol stars This color index is de ned as
IR Color Index B C
where B and C are the magnitudes measured at A and A resp ectively which
are regions clear of molecular absorption
The comparison star was Tau HD V B V G I I I which is
itself a wing IR standard star and the check star used was Tau HD V
B V G I I Ia Three ten second integrations were made for each observation
using the usual sky comparison variable comparison sky sequence Atmospheric extinc
tion and conversion to helio centric Julian Day number was done during data reduction
Corrections for the V band observations to the standard UBV system was also done IR
magnitudes were standardized using magnitude values supplied by Wing
Nightly and weekly means were computed from the V data and these are plotted
against helio centric Julian Day in Figure and tabulated in Table As can b e seen the
light variations observed over the month p erio d are relatively small Systematic trends
in the data and spline ts were applied to see if any regularities in the light variations
could b e found As shown in Figure Aldebaran app ears to vary on a time scale of ab out
days the full light variation is magnitude To check this p erio d analytically
Figure Aldebaran visual light curve calendar dates are mid month The sine curve shown was
generated using a day p erio d and varying semiamplitude
Figure Aldebaran DFT note p eak intensity at frequency p erio d days
Figure TiO index sp ectral type calibration indicating Aldebaran as an M star
the observations were sub jected to a formal p erio d search using a Discrete Fourier Trans
form DFT of Sinnot Figure shows the results of the DFT a p eak frequency
of days was found corresp onding to an approximate day p erio d This p e
rio d is close to the photometric p erio d found by insp ection A sine curve of decreasing
m m
semi amplitude from : to : was generated using the day p erio d This t
is shown in Figure The agreement with the observations is reasonably go o d
It is not certain if this p erio d is stable with time and if there are any long term changes
in brightness The mean brightness observed by us of hVi magnitude is in go o d
agreement with the hVi found earlier by Krisciunas this indicates that the star do es not
have signi cant long term brightness changes over the time scale of at least several years
Based on the apparent observed p erio d and varying amplitude it app ears that Alde
baran has photometric characteristics similar to the so called Small Amplitude Red Vari
ables SARVs SARVs are M giants which pulsate with small light amplitudes and have
p erio ds of up to days and visual amplitudes of up to magnitudes Percy If
so classi ed Aldebaran would have the smallest observed amplitude of this class of stars
Although we did not attempt to obtain light curves using the Wing IR lters we did
observe the star on four nights with this lter set From these observations we determined
the TiO index and the near IR color index to b e and
magnitude resp ectively From over co ol standard stars observed with the Wing lters
Wing a TiO index vs sp ectral type was calibrated for K and M type stars Part of
this calibration is seen in Figure where Aldebaran s TiO index indicates it is of sp ectral
type M I I I which is not the usual K III value asso ciated with this star Additionally
the U B and B V colors are more suitable for a M I I I star rather than a K I I I star
More observations using the Wing lters are needed to further quantify the sp ectral
type of Aldebaran and also to search for outer atmospheric TiO variations Continued
photometry is also planned to ascertain p erio d stability and amplitude changes
The authors wish to thank Dr Emilia Belserene for her assistance in translating the
DFT program from BASIC to FORTRAN We also than Dr Rob ert Wing for providing
standard star IR data For this research we utilized the SIMBAD database op erated by
CDS Strasb ourg France This work was supp orted in part by NSF grant AST
which we gratefully acknowledge
Rick WASATONIC
Edward F GUINAN
Dept of Astronomy and Astrophysics
Villanova University
Villanova PA
References
Ho eit D Yale Bright Star Catalog th Edition Yale University Observatory
Krisciunas K Inf Bul l Var Stars No
Percy J PASP
Petit M Variable Stars John Wiley Sons Ltd
Sinnot R W Sky and Telescope Vol No p
Wing R F Sp ectral Classi cation and Color Temperatures For Bright Stars
In The Range K M Astronomy Dept Ohio State University
Wing R F Standard Stars for Eight Color Photometry Dudley Obs Rep ort
A G Davis Philip ed
Wing R F Journal of the American Association of Variable Star Observers
Vol No p
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
May
HU ISSN
NEW ELEMENTS OF V AQUILAE
BAV Mitteilungen Nr
V Aql Aql GSC was discovered by Ho meister on
photographic plates of the Sonneb erg Observatory He classi ed the star as an Algol type
m m
variable in the range b etween : and :
First investigation of this variable was p erformed by Rohlfs She published
minima times for plates with weak images a photographic normal light curve and rst
elements
d
Min I HJD : : E
m m
The range of brightness is given as : : phot From her measurements she
h
derived a time of constant light in the minimum of : With these data V Aql is
listed in the fourth edition of the GCVS Kholop ov et al
Popper and Woo d p ointed out that V Aql is of sp ecial interest b ecause
d
of its for an Algol type variable extreme short p erio d of : Popper gives for the
primary comp onent a radius of : R sp ectral class F and the radial velocities from
two sp ectrograms Based on the p erio d given by Rohlfs Brancewicz and Dworak
published additional geometrical and physical parameters
Almost years later we put V Aql on our observing program The CCD ob
servations were made with SBIG ST cameras without lters attached to a cm RC
telescop e with f mm WM a cm SC telescop e with f mm WK and a
cm Aero Ektar astrograph with f mm PF The integration times were sec
onds at the RC SC telescopes and seconds at the astrograph Our CCD observations
cover years GSC served as the comparison star and several other stars in the
same eld were used to check its constancy In our instrumental system Aero Ektar the
m m
amplitude of variability is : for the primary minima and : for the secondary min
ima A constant phase in minimum light could not b e detected All our CCD measured
times of minimum light were calculated with the Kwee and van Woerden metho d
A thorough study of our measurements showed that the p erio d given in the GCVS is a
spurious one with the relation
P P d
GCVS sid
Using only CCD measured minima a weighted least squares t led to the new ephemeris
d
Min I HJD : E
:
One of us WM investigated the variable on ab out photographic plates of the
m astrographs of the Sonneb erg Observatory additional times of minimum light of
V Aql could b e found The plates taken b etween JD and JD were of
rst quality The scatter of the results is therefore small The gap b etween JD
and JD could not b e closed due to a lack of useful plates from that time Using
all available minima a weighted least squares t led to the new ephemeris
d
Min I HJD : : E
Figure Di erential light curve of V Aql Aero Ektar mm drawn with the
new ephemeris
Figure O C diagram for V Aql using the new ephemeris dots and the
ephemeris dashes represent CCD measured minima and 2 minima on
photographic plates
Table Observed times of minima for V Aql ep o chs and residuals computed with
resp ect to the linear ephemeris derived in this pap er
JD hel W T Ep o ch O C Lit JD hel W T Ep o ch O C Lit
P P
P P
P P
P P
P P
P P
P P
P P
P P
P P
P P
P P
P E
P E
P E
E P
P E
P E
E P
P E
E P
E P
P E
E P
P denotes photographic minima and E CCD observed minima
Those marked with got reduced weight
E Rohlfs VSS W Moschner this pap er P Frank this pap er
P Frank W Moschner this pap er W Kleikamp this pap er
We want to acknowledge the help and assistance by the management and sta of
Sonneb erg Observatory esp ecially of Dr Peter Kroll in using the library and plate archive
P FRANK
W KLEIKAMP
W MOSCHNER
Bundesdeutsche Arb eitsgemeinschaft
f ur Ver anderliche Sterne e V
BAV
Munsterdamm
D Berlin Germany
E mail
wilhelm kleikamp t online de
wolfgang moschner t online de frank velden t online de
References
Brancewicz H K Dworak T Z Acta Astronomica
Ho meister C Erg AN
Kholop ov P N et al General Catalogue of Variable Stars th Edition Nauka
Moscow
Kwee K K van Woerden H Bul l Astr Inst Netherlands
Popper D M Publ Astron Soc Pac
Rohlfs E Ver o entlichungen der Sternwarte zu Sonneberg No
Woo d et al Flower Reprint No
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May
HU ISSN
UBV PHOTOMETRY OF THE W UMa STAR BH Cas
The eclipsing binary BH Cassiop eiae was re established as a W UMa type star by
Metcalfe Observations in the V band were obtained in and at the
Steward Observatory m telescop e using the kBig CCD Photo electric observations in
the U and B bands were obtained in at the McDonald Observatory m telescop e
The extinction corrected normalized data are shown in Figure
Figure UBV observations of BH Cas phased with the ephemeris given in this pap er
Times of minimum light were derived from quadratic ts to the minima included in
the B and V band data see Table and the following ephemeris was determined
d
Min I HJD E
Table Observed times of minimum light for BH Cas
Type HJD of Min Ep o ch Type HJD of Min Ep o ch
II I
I II
II I
I II
II I
I II
Times derived from B band data
Sp ectroscopic observations to b e obtained from McDonald Observatory will allow the
absolute masses and radii of the two comp onents to b e determined Further constraints
would b e p ossible with the addition of R and I band light curves where BH Cas is brighter
m m Collab oration with observers at longitudes much di erent than
R I
h m
McDonald Observatory L ' on the sp ectroscopic observations is most welcome
w
T S METCALFE
Department of Astronomy
University of Texas
Austin Texas USA
e mail travis astro as utexas edu
Reference
Metcalfe T S IBVS No
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HD A PULSATING CANDIDATE BOOTIS STAR
The candidate Bo otis star HD was observed during ve nights with the mo d
ular photometer at the m telescop e observer R Kuschnig op erated by the South
African Astronomical Observatory SAAO The characteristics of these nonmagnetic
metal de cient Population I A to F type dwarfs are describ ed in more detail by Paunzen
et al The journal of observations and the chosen comparison stars are listed
in Table The light curve shown in Fig reveals the photometric variability of the
program star with resp ect to b oth comparison stars The applied standard time series
analysis Wei to the high quality data results in the amplitude sp ectrum and sp ec
tral window shown in Figure The highest signal detection app ears at the frequency
1
of d Hz which refers to a p erio d of min and the p eak to p eak amplitude
is ab out mmag in Str omgren v These values are typical compared to previous results
obtained by our survey for pulsating Bo otis stars Paunzen Handler
In order to establish the membership of HD to the Bo otis group an intermedi
ate resolution sp ectrum A pixel was obtained in the night of observer
E Paunzen with the Cassegrain sp ectrograph of the m telescop e at Ita juba Brazil
0.04 0.02 C1 (HD103017) 0.00 -0.02 -0.04 0.04 0.02 HD102541 0.00 -0.02 -0.04 0.04 0.02 C2 (HD103051) mag (v) residual to mean 0.00 -0.02 -0.04 9740.55 9740.60
JD 2440000+
Figure Light curve of HD and b oth comparison stars for the rst night in
Str omgren v 0.020 0.018 0.016 0.014 0.012 0.010
0.008 -40 -20 0 20 40 0.006 Semi-amplitude (v) 0.004 0.002 0.000
0 20 40 60 80 100 120 140
Frequency [d-1]
Figure Amplitude sp ectrum and sp ectral window for the merged di erential data of
all ve nights HD HD in Str omgren v
Table Journal of observations for the program and comparison stars
Star Durchm JD hours m Sp ec
V
HD CD Bo o
HD CD F IV V
HD CD F V
Houk classi ed HD as A I I I I I The Str omgen colours b y
m c Gray Olsen on the other hand indicate that
1 1
this star is actually a metal de cient dwarf Using the calibrations of Crawford and
Napiwotzki et al we derive T K log g typical for luminos
ef f
ity class V m and M The discrepancy b etween the luminosity
0 B ol
classi cation given in the Michigan catalogue and a reclassi cation with higher resolu
tion sp ectra is a common fact for Bo otis stars Gray We classify HD
based on the sp ectrum showed in Figure as kA hA mA V LB please note that the
Mg I I line is normal for A and not remarkably weak
Many similarities of HD to the pulsating P min Bo otis star HD
obs
are obvious Paunzen et al This star was also classi ed as A I I I I I but turned
out to b e a metal de cient dwarf Both stars are almost at the same place in the H R
diagram resulting in a comparable pulsation b ehaviour observed p erio d and amplitude
The observed p erio d for HD is very close to the theoretical radial fundamental
mo de P min derived by the PLC relation taken from Stellingwerf making
th
this star to an interesting target for an international multisite campaign
1.0
0.8
0.6 Intensity 0.4
0.2
4000 4200 4400 4600 4800
Wavelength [A]
Figure Intermediate resolution A pixel sp ectrum of HD
Acknowledgement This research was carried out within the working group Asteroseismo
logy AMS with funding from the Fonds zur F orderung der wissenschaftlichen Forschung
pro ject S AST We are indebted to the scienti c committees of LNA CNPq MCT
and SAAO for granting observing time This research has made use of the Simbad
database op erated at CDS Strasb ourg France
R KUSCHNIG
E PAUNZEN
W W WEISS
Institut f ur Astronomie der
Universit atWien
T urkenschanzstr
A Wien
e mail paunzen astro ast univie ac at
References
Crawford D L AJ
Gray R O in Precision Photometry Davis Philip A G Upgren A R Janes
K A eds p
Gray R O Olsen H H A AS
Houk N University of Michigan Catalogue of Two Dimensional Spectral Types for
the HD Stars Volume II Astronomy Dept Univ Mich Ann Arb or Michigan
Napiwotzki R Sch onberner D Wenske V A A
Paunzen E Weiss W W North P IBVS No
Paunzen E Handler G IBVS No
Paunzen E Weiss W W Heiter U North P A AS
Stellingwerf R ApJ
Wei W Time Series Analysis Addison Wesley Publishing Company
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RADIAL VELOCITY CURVES AND FIRST CALCULATIONS
OF THE RADI I FOR FOUR DOUBLE MODE CEPHEIDS
Double mo de Cepheids form a sp eci c group of Cepheids which includes a limited
number of stars The light and radial velocity curves of these stars show double mo de
variations whereas ordinary Cepheids show only one p erio d The ratio of p erio ds is almost
the same for most of these stars and is close to in agreement with the theoretical
ratio of p erio ds of the rst overtone P to fundamental tone P For CO Aur unlike other
stars this ratio is close to one can imagine based on the theory of stellar pulsations
that this star pulsates b oth in the second and rst overtone mo des
Berdnikov used a large number of original photo electric observations of
double mo de Cepheids to decomp ose their light and color curves into two oscillations
Since we have carried out systematic measurements of radial velocities of northern
Cepheids with a correlation sp ectrometer designed and made by Tokovinin Most
part of these observations were included in our two catalogues Gorynya et al
These data combined with our unpublished observations allowed us to derive
separate radial velocity curves for two oscillations in ve photometrically well studied
Cepheids V Sct EW Sct BQ Ser TU Cas CO Aur
Note that clear separation of radial velocity curves into two oscillations was made
p ossible by long sets of observations resulting in go o d coverage of radial velocity curves
Figures show the decomp osed radial velocity curves for each mo de
We used these curves to estimate the radii of the four double mo de Cepheids using
Balona s metho d which is a mo di cation of the well known Baade Wesselink
technique Wesselink We were forced to simplify our analysis b ecause the number
of radial velocity observations is much less than that of photometric measurements and
radial velocities alone do not p ermit us to nd the relation b etween the amplitudes and
phases of the two mo des found earlier in photometric data Berdnikov We
therefore assumed that the two oscillations are indep endent of each other
In this case the main least squares equation can b e written as
V A B V lg R r r C
where V and B V are current magnitude and colour R mean Cepheid radius
in R and A and C the constants to b e found The total pulsational radius variation
r r r can b e found by direct integration of radial velocity curves for two mo des
Z Z
r pP R V d pP R V d
r r
We use two color indices B V and V R as the e ective temp erature indicators
Table gives the Cepheid radii and their formal errors
10 First overtone +. +. +. +.. +. + +. . ++ 5 ... +. + + . + +. ..+. + +. +. + + 0 + ..+. . + . . + + .. +. . . -5 + + +. CO Aur +.. Vr(1), km/s +. ++. + +. . -10 +. . . + + -15 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Phase
Second overtone 5 + + . .. +.+. +. + +.. + . . . . + + . + + . .. + . + 0 + . + . + ++ + . + CO Aur .. +
Vr(2), km/s + +. . + + + .+. .+. + + ...... +. +. + + + + -5 + 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Phase Figure
Fundamental mode 20 ++ +... . .+.. . + +. ++ + .. + +.. + . + ++. .+. + + 10 ...+ + .+. +.+.+. + + . + . . +. + +... + 0 +. + . . +.+. ++.. . + + . + +.. + + +.+.. + . -10 . . +. +. + + TU Cas Vr(0), km/s + +.. . +.. +. +. -20 +
-30 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Phase First overtone 10 + + +. . . . + + . . .+ + + +. . +. . 5 .+.+. ++ + .+. . .. + . + +. ++ .. + + + ++..+. 0 . . + + +.. . + .++.. + . + + . +. + + + + -5 +. + + .+.. . +.. . + ++.. +.. . . + . . +. ..+. . ..+ + TU Cas Vr(1), km/s + + + + + -10 +
-15 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Phase Figure
Fundamental mode 20
+ 10 + + ++ + + + . . +...... +. ..+. .+.+. +....+...... +.. . +.. + + +++ + ++ + . + ..+..+. +.+. ++ + ++ ++ ++..+. + +. +... ++ + ... + ++.. +..+. + ..+ 0 + . +. +...... + + +. +++ ... . .+. .+..+ ++ + + .+.. + + .+. .+.+.+.++++ + + ...+.. + + +..+. + + .+. +.+. ..+... . . + EW Sct ++ . Vr(0), km/s ++ + + -10 + + +
-20 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Phase First overtone 10 + + + + + + . .+...... +.+. . . . + ++++ . +. . + + + + ... + + +.... + .. +.. .. . + 5 . + ++++. . +. + . + +.+. + .. +.. . + +.... .+ ++ + +... ++++ . ... . ++ + 0 ++ + + . . + + .+. + + + . + .... +.. + +++...... + EW Sct Vr(1), km/s +.. ++ + + . . ++ + + . .. + + .. . + ++ -5 ++.+.. . + +.. +...+ + .. . +. +.. +. . + + + + + + + + -10 + 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Phase Figure
15 Fundamental mode + + 10 + + +. + + + + ...... +. . . . + + .. + +. + .. 5 + . + + . . .. + +. + + + + + ...+.. . + .+. + ++ . + .... 0 + ... + . ++ V367 Sct + Vr(0), km/s + ...... + + . + ++ + + + +. . -5 + + ... + + .+. + .+...... + + + + -10 + 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Phase
10 First overtone + + ++ + + + ...... +.. + + ..+. + .+.. . + + 5 . +. .. + + + + + . . . . . + + + . + + + . + ... + 0 + .. + .. .. + ++ + . . . + .. . + + + . . .. . V367 Sct + + Vr(1), km/s . + + . + . . + + + -5 .... +. . .+. . + + + + + + +++ + -10 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Phase Figure
Fundamental mode 10 + + + + + + + 5 + ...... +.. . .. ++ + . . + + + .. + .. . ++ + . + + ++ + + . + + + + . . + + . + + . + 0 ...+. .. . + ++ .... . +. + + ++ +...... + + + ...... + + + + + + . . . +... +.... + ++ ++ + + + BQ Ser + + Vr(0), km/s + + + -5 + + + + + -10 + 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Phase
20 First overtone
+ + 10 + . .+. .. . . +.+. + . . + + . . + + . . + + .. + +. ++ + + + . ++ + + + .+...... +..+. . + . 0 + . . +. . . +. ++ + + .. + +.... ++ + .. + . . ++ ++ + . + + ++ +.+. + + + ...... + ++ +.+. BQ Ser Vr(1), km/s ...... +.. .. . -10 + + + + + + + + -20 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
Phase
Figure
Table
Star P P R R R R
B V R V R R
d d
EW Sct
BQ Ser
TU Cas
CO Aur
Radial velocity data for the faintest star V Sct cannot b e used for calculations
b ecause of large observational errors
We derived the following p erio d radius relations for the four double mo de Cepheids
assuming that CO Aur oscillates in the rst and second overtones
lg R lg P for B V
lg R lg P for V R
These relations agree well with that for single mo de Cepheids Rip epi et al
Sachkov et al we consider this agreement to b e a justi cation of our technique
applied to the double mo de Cepheids
The author is grateful to Drs A S Rastorgouev N A Gorynya and N N Samus for
helpful discussions
This work was partially supp orted by the Russian Foundation for Basic Research
through grant
M E SACHKOV
Institute of Astronomy of Russian
Acad Sci
Pyatnitskaya Str
Moscow Russia
e mail sachkov sai msu su
msachkov ra inasan ac ru
References
Balona L A M N R A S
Berdnikov L N Sov Astron Lett No
Berdnikov L N Sov Astron Lett No
Gorynya N A Irsmambetova T R Rastorgouev A S and Samus N N Sov
Astron Lett No
Gorynya N A Samus N N Rastorgouev A S and Sachkov M E Astronomy
Letters
Rip epi V Barone F Milano L and Russo G Astron and Astrophys
Sachkov M E Rastorgouev A S Gorynya N A and Samus N N Astron and
Astrophys in preparation
Tokovinin A A Soviet Astronomy
Wesselink A J Bul l Astr Inst Netherland
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A NEW DOUBLE MODE CEPHEID IN SCUTUM
h m s 0 00
The variability of BD GSC
J l b was discovered on Moscow collection plates taken with the
cm astrograph in Crimea
The new variable was estimated by eye in B band on plates for the interval
m m
JD The variability range is B band magnitudes of com
parison stars Table were measured photo electrically by L N Berdnikov private com
munication
Table Comparison Stars
GSC B
h m s 0 00 m
h m s 0 00 m
The results of the frequency analysis are presented in Figure The step in frequency
is ab out c d We can see the existence of two frequencies in the sp ectrum f and
f and their day aliases The second group of frequences f and day aliases is more
clearly seen in Figure b where f is whitened
Figure The p ower sp ectra
Figure The phased light curves a fundamental mo de b rst overtone mo de c
fundamental mo de where rst overtone has b een whitened d rst overtone where
fundamental mo de has b een whitened
The p eaks in the sp ectrum at frequencies f and f are almost equal But to have a
reasonable decision we should consider the frequency f as real In this case the p erio ds
and the p erio d ratio P P f f are typical for double mo de Cepheids The
shap es of the phased light curves constructed with the p erio ds P and P Fig cd
are in agreement with the CEP B type to o The rst overtone phased light curve has a
sinusoidal shap e M m
So we classify BD as a new Cepheid pulsating in two radial mo des with the
light elements
d
JD E fundamental mo de and
max
d
JD E rst overtone mo de
max
d
The error of p erio d determinations is
m m
Average amplitudes in B band are A and A It is necessary to
mention that among Galaxy s double mo de Cepheids the only one AX Vel has the am
plitude of an rst overtone mo de exceeding that of the fundamental mo de BD
is the second known double mo de Cepheid with the same p eculiarity But this is not a
rare phenomenon Among b eat Cepheids that pulsate in fundamental and rst over
tone mo des discovered by MACHO Pro ject in LMC show the strongest p eak in the
p ower sp ectrum at the rst overtone Alco ck et al
The author would like to thank Dr N N Samus for his help and attention to this
investigation to express gratitude to Dr L N Berdnikov for photo electric observations
of the comparison stars and for useful discussion and to Drs S Yu Shugarov and
V P Goranskij for software used in this work This study was partially supp orted by the
Russian Foundation for Basic Research through grants Nos and
S V ANTIPIN
Sternberg Astronomical Institute
Universitetskij Prosp
Moscow Russia
E mail antip sai msu su
Reference
Alco ck C Allsman R A Axelro d T S et al AJ
COMMISSIONS AND OF THE IAU
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Number
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HU ISSN
THE ECLIPSING BINARY RX J
The sky was surveyed in the X ray region of the sp ectrum by the ROSAT satellite Vo
ges et al and catalogs of the sources included RX J GSC
Jenkner et al A literature search using SIMBAD shows that the star has a
large prop er motion measured Giclas et al to b e an in right ascension and
an in declination The star was one of the ob jects found in a survey by Beers et
al who concluded from ob jective prism sp ectral observations that it was a faint
star displaying mo derate CaI I H K emission
The automated m telescop e Cousins R lter and CCD camera of the Climenhaga
Observatory of the University of Victoria Robb and Honkanen were used to make
photometric observations of RX J Using IRAF routines the frames were
de biased and at elded and the magnitudes were found from arc second ap erture
photometry after using the Gaussian centering option of the PHOT package
1 3 h 2 7 m 2 0 s 1 3 h 2 7 m 1 3 h 2 6 m 4 0 s
+ 4 5 o 3 8 ’ 881
601 618 626 + 4 5 o 3 4 ’ 771 780
+ 4 5 o 3 0 ’
1 3 h 2 7 m 2 0 s 1 3 h 2 7 m 1 3 h 2 6 m 4 0 s
Figure Finder chart of the eld lab elled with the GSC numbers Jenkner et al
The eld of stars is shown in Figure and their designations co ordinates J
and magnitudes from the Hubble Space Telescope Guide Star Catalog GSC Jenkner
et al and the R magnitudes are tabulated in Table The R di erences in
To magnitude are found from our data in the sense of the star minus GSC
lo ok for brightness variations during a night the standard deviation of the di erential
m
magnitudes for each star during a night were calculated and ranged from for a
m
for the faint stars on p o or nights To measure night bright star on a go o d night to
to night variations a run mean of the seven nightly averages was calculated and is shown
1
IRAF is distributed by National Optical Astronomy Observatories which is op erated by the Asso ciation of Universities for Research in Astronomy Inc under contract to the National Science Foundation
Table Stars observed in the eld of RX J
GSC No RA Dec GSC R V V R
C
J J Mag Mag
h m s
variable
h m s
h m s
h m s
h m s
h m s
as R in Table We consider GSC to b e the only signi cantly variable star
Due to the small eld of view extinction e ects were negligible and no corrections have
b een made for them No corrections have b een made to transform the R magnitude to a
standard system
Brightness variations in RX J were evident during a night A least squares
d
t of a single sine wave to all the the data shows a deep minimum in at a p erio d of
but a plot of the light curve shows unequal maxima which led us to double the p erio d
An eclipse was also apparent with ingress and egress not resolved On three o ccasions
the observations were terminated by clouds or dawn during the eclipse but we could
clearly see the ingress of the primary minimum seven times and the Helio centric Julian
Dates were and
with an uncertainty of ab out days A t to these times corrected to mid
eclipse gives the ephemeris
d d
HJD of Minima E
GSC R magnitudes phased at this A plot of the di erential GSC
p erio d is shown in Figure for our two b est nights Clearly there is a di erence of ab out
m
after the rst maximum but no di erence in the second maximum Most of the
other nights agreed with the data marked with symbols
Figure R band light curve of RX for HJD and
To help classify the variable star V and R frames were obtained under photometric
conditions along with observations of the nearby bright standard star HR Mo ett
and Barnes The V band brightness and V R colors are listed in Table for the
C
three brightest stars However great caution should b e exercised in using these data since
they are derived from only one standard star and its V R was transformed from the
Johnson system to the Cousins system using Taylor s equations While certainly
not de nitive these colors con rm that RX J is a late type approximately
M V star Cousins A dwarf star of this color would b e exp ected to have an
absolute magnitude of approximately V Allen so from our apparent magnitude
we nd the distance to b e ab out parsecs Combined with the prop er motion we nd
a large tangential velocity of km sec Observations were continued in the V and R
m m
lters through the eclipse and the depths were measured to b e in R and
m m
in V
Since no p oints were observed on the descending or ascending branches of any primary
minimum we observed with no lter and decreased the exp osure time to seconds for
a rep etition rate of seconds Still no p oints were seen on the descending branch and
only one p ossibly on the ascending branch The duration of the primary minimum was
d
so the ratio of the radii of the two stars must b e less than All other eclipses were consistent with this duration
1.00 Flux
0.00 0.25 0.50
Phase
Figure R band light curve p oints with example mo del line of M V and white dwarf
From the color information and the duration of the eclipse we can surmise that the
primary star is a M V and the secondary star is a white dwarf Assuming and
solar masses and and solar radii for the primary and secondary stars resp ec
r d
tively Allen we nd from our p erio d and Kepler s Law the relative radii of
and The temp erature of the co ol star was assumed to b e K and from the
depths of the minimum the temp erature of the white dwarf was estimated but needed to
b e adjusted to K Using these radii masses and temp eratures a mo del light curve
was made with Binmaker Bradstreet and is shown in Figure The inclina
tion was adjusted to to t the data however assuming di erent masses and radii would
require an inclination di erent by a few degrees To mo del the asymmetry in the maxima
one sp ot was used which had a co latitude of longitude of a radius of and
a temp erature factor of All other inputs were set at values appropriate for these
temp eratures The co ol star is well inside its Ro che lob e and it is not likely we will see
much evidence of mass transfer
The star RX J is therefore one of a small group of stars very similar to
the famous eclipsing binary V Tau Both stars have white dwarf secondary stars and
late type primary stars with evidence of starsp ots from asymmetrical and changing light
curves and X Ray emission Further photometric observations with a larger telescop e
will b e valuable to measure the relative radius the color and thus the temp erature of the
white dwarf star Sp ectroscopic observations will b e imp ortant to get a go o d sp ectral
class for the late type dwarf and radial velocities will measure the scale of the system and
the masses The space velocity is also of interest since the tangential velocity implies that
the star may b elong to Pop I I RG would like to thank the Austrian Ministry of Science
for nancial supp ort
R M ROBB
R GREIMEL
Climenhaga Observatory
Dept of Physics and Astronomy
University of Victoria
Victoria BC CANADA V W P
Internet robb uvic ca
References
Allen C W Astrophysical Quantities the Athlone Press University of London
London UK
Beers T C Bestman W and Wilhelm R AJ
Bradstreet D H Binary Maker Usermanual Contact Software Norristown PA
USA
Cousins A W SAAO Circ
Giclas H L Burnham R Jr Thomas N G Lowell Obs Bul l No
Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ
Mo ett T J and Barnes T G I I I PASP
Robb R M and Honkanen N N in A S P Conf Ser Automated Telescopes
for Photometry and Imaging ed Adelman Dukes and Adelman
Taylor B J ApJS
Voges W Aschenbach B Boller T Braeuninger H Briel U Burkert W Dennerl
D Englhauser J Grub er R Hab erl F Hartner G Hasinger G Kuerster M
Pfe ermann E Pietsch W Predehl P Rosso C Schmitt J H M M Truemper
M and Zimmermann H U A A preprint
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THE FIRST PHOTOELECTRIC OBSERVATIONS
FOR THE DOUBLE MODE CEPHEID BD
Antipin recently analyzed photographic archival plates at the Sternberg As
tronomical Institute in Moscow and found that the star BD is a double mo de
Cepheid with the elements
fundamental Max JD E
hel
rst overtone Max JD E
hel
We observed the Cepheid photo electrically at the South African Astronomical Observa
tory in April May using the cm re ector A total of V RI measurements
c
m
were obtained Table the accuracy of the individual data b eing near in all
lters The elements cited ab ove are used in Figures a and b for plotting our new
observations
Table
JD V V R V I JD V V R V I
hel c c hel c c
V a) P=4.841 9.5
10.0 V-R C 0.7 0.9 V-I C 1.4 1.6 0.0 0.5 1.0 V b) P=3.385 9.5
10.0 V-R C 0.7 0.9 V-I C 1.4 1.6
0.0 0.5 1.0 Phase
Figure
The research describ ed here was supp orted in part by the Russian Foundation of Ba
sic Research and the State Science and Technology Program Astronomy to LNB and
through NSERC Canada to DGT We would also like to express our gratitude to the
administration of the SAAO for their allo cation of a large blo ck of observing time
L N BERDNIKOV
Sternberg Astronomical Institute
Universitetskij prosp
Moscow Russia
D G TURNER
Saint Mary s University
Halifax Nova Scotia B H C
Canada
Reference
Antipin S V I B V S No
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PHOTOELECTRIC OBSERVATIONS FOR TWO MISCLASSIFIED
VARIABLES AF CRUCIS AND CG SAGITTARII ARE NOT CEPHEIDS
The present note addresses the status of two stars that are identi ed as Cepheid vari
ables in the fourth edition of the General Catalogue of Variable Stars AF Crucis and CG
Sagittarii
Grayzeck a found the star AF Cru to b e a Cepheid variable with the elements
Max JD E
hel
Its V magnitude was found to vary in brightness b etween and Grayzeck b
However the shap e of its light curve is very asymmetric which is unusual for a classical
Cepheid of that p erio d
Gerasimovic found CG Sgr discovered previously by Bailey to b e a
long p erio d Cepheid variable with the elements
Max JD E
In order to examine the light curves of b oth stars in greater detail we observed them
photo electrically at the South African Astronomical Observatory in April May using
the cm telescop e A total of VR measurements were obtained for AF Cru Table
c
and a total of V RI measurements were obtained for CG Sgr Table the
c
m
accuracy of the individual data b eing near in all lters
It is readily seen that our observations for CF Cru do not satisfy the elements given
by Grayzeck and that the star app ears not to b e varying A search of the literature
revealed that AF Cru was discovered by Uitterdijk as an eclipsing variable with
the elements
Min JD E
hel
p
Figure illustrates that our observations do not and a short eclipse duration of D
con ict with Uitterdijk s elements Our data suggest that AF Cru is indeed an eclipsing
variable although we have no measurements near the times of eclipses
Regarding Grayzeck s b observations they do not satisfy Uitterdijk s elements
Our attempts to nd a new p erio d using b oth the present and Grayzeck s observations
were unsuccessful
During the observing run for CG Sgr it was found that the star s brightness varied on a
time scale of hours not days in direct con ict with the elements of Gerasimovic Although
the light amplitude is comparable to that of certain RR Lyrae and Scuti variables the
time scale of variability app ears to b e to o small for an ob ject of the RR Lyrae class It
app ears that CG Sgr may b e a Sct star Our attempts to nd new elements for it were unsuccessful
V AF Cru P=1.895 9.7 9.9 V-R C 0.6 0.8
0.0 0.5 1.0 Phase
Figure
Table VR observations of AF Cru
c
JD V V R JD V V R
hel c hel c
Table VR observations of CG Sgr
c
JD V V R V I JD V V R V I
hel c c hel c c
The research describ ed here was supp orted in part by the Russian Foundation of Ba
sic Research and the State Science and Technology Program Astronomy to LNB and
through NSERC Canada to DGT We would also like to express our gratitude to the
administration of the SAAO for their allo cation of a large blo ck of observing time
D G TURNER
L N BERDNIKOV
Saint Mary s University
Sternberg Astronomical Institute
Halifax Nova Scotia B H C
Universitetskij prosp
Canada
Moscow Russia
References
Bailey S Harvard Bul letin No
Gerasimovic B Harvard Bul letin No
Grayzeck E J a Astron J
Grayzeck E J b Astron J
Uitterdijk J B A N
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
REVEALING OF A NEW SU UMa TYPE VARIABLE STAR
VAR CORONAE BOREALIS
Var Coronae Borealis was discovered and designated by Antipin He classi ed
this star as a dwarf nova U Geminorum type with a photographic range of <
magnitudes Several outbursts were observed Two types of them were found di ering
by duration The longer outbursts with a duration of days or more and the shorter
ones lasting ab out days This b ehavior is very common to the SU Ursae Ma joris
subtype of cataclysmic variables These variable stars are characterized by the presence
of small amplitude semi p erio dic mo dulations in the light curve called sup erhumps
Even though CCD photometry was made by M Iida Nagamo Japan in and T
Vanmunster Landen Belgium no sup erhumps were detected
During the last sup eroutburst in May the CCD photometry at Nicholas Cop erni
cus Observatory and Planetarium in Brno Czech Republic was p erformed on night May
We used SBIG s CCD camera ST placed in primary fo cus of cm Newtonian
telescop e f mm For automatic reduction ap erture photometry package MuniPhot
by Filip Hro ch Masaryk University Brno using some author s routines which is based
on the well known DaoPhot I I New generation Stetson was used
mag
r
r
r
r
r
r
r
r
r
r
r
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r r
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r
r
V C r
r r r r
r
r r r
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r
r r
r
r
r
r
r
r
r
r
JD
Figure Light curve with three sup erhump maxima V C is di erence b etween variable and
comparison star 1
The observing run started on JD and ended on JD Total num
b er of exp osures was two of them were omitted from the list b eacuse of clouds
The star was near to mag in R band Kron Cousins lter Each exp osure lasted
seconds All images were pro cessed by standard dark frame and at eld corrections
The standard deviation of magnitude of variable star was : mag The star
GSC close to Var CrB p osition was used as a comparison
In the light curve Figure three sup erhump maxima were de nitely detected Using
Phase Disp ersion Minimization Stellingwerf analyzing routines written by Taichi
Kato Kyoto University Japan we obtain value of sup erhump p erio d as P
SH
day This result is well within the range of sup erhump p erio ds of usual SU
UMa stars which lies b elow the lower limit of the p erio d gap Osaki of cataclysmic
variables which is aproximately from hours to hours
Indep endent CCD photometry p erformed during the same night by Vanmunster
has con rmed our results So there are go o d reasons to classify variable star Var CrB
as an UGSU U Geminorum SU UMa sub class dwarf nova with a range of variability
h m s 0 00
< mag P and co ordinates : and
Acknowledgements The author would like to thank Taichi Kato and his group for
valuable comments literature supp ort and providing information to all administrators
of VSNET Variable Stars Network home page for their work to Tonny Vanmunster
for notifying ab out the outburst and indep endent observation of sup erhumps con rming
our results Jan Hollan and Zden ek Mikul a sek for valuable comments and manuscript
editing the Masaryk University for Internet access The author is grateful to Filip Hro ch
for ap erture photometry software supp ort
Rudolf NOVAK
N Cop ernicus Observatory
and Planetarium
Krav hora
Brno Czech Republic
Internet rudolfn physics muni cz
References
Antipin S V IBVS No
Kato T Nogami D Baba H http www kusastro kyoto u ac jp vsnet
Osaki Y PASP
Stellingwerf R F ApJ
Stetson P B PASP
Vanmunster T private communications and vsnet alert
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
TWO NEW VARIABLE STARS NEAR THE VARIABLE WR HD
AND THE CONSTANT WR HD
During our search for variability among Wolf Rayet WR stars on a timescale of
minutes to days we discovered two variable stars in the eld of view of WR HD
WN van der Hucht et al and of WR HD WN The variability of
WR will b e rep orted elsewhere Veen et al while WR app eared to b e stable
The observations were obtained using the Dutch cm telescop e at ESO La Silla
Chile equipp ed with a CCD camera ESO and a Bessel B lter ESO The
observations were p erformed during two consecutive nights in December and three
nights in January On each of these nights CCD images were obtained for to
hours continuously which resulted in a rate of ab out one frame p er two minutes
Ten stars in the eld were picked to see whether they were suitable as comparison
stars Because of di erent p ointings not all stars were recorded in each night Figure
displays a CCD image of the region around WR star in which the p osition of the
stars and are indicated During the analysis star turned out to
b e variable itself Stars and varied in brightness probably b ecause of di erential at
mospheric extinction Therefore the di erential magnitudes as presented in Figure are
computed with resp ect to the total ux of the stars and Figure displays the
eld of WR Observations in the night of January showed star k to b e vari
i GSC and j showed marginal photometric able Stars d GSC
variability Therefore the di erential magnitudes were calculated with resp ect to stars
b GSC c e f g and h GSC We notice that the stars near
WR are not listed in the Guide Star Catalogue GSC Lasker et al Russell et
al and Jenkner et al probably b ecause of light contamination by the ring
nebula NGC around WR
Table lists the co ordinates of the WR ob jects and of the variable stars The mean
magnitudes dB are determined with resp ect either to WR or to WR since they are
B
the only stars in the eld for which the B magnitude is known Mo at et al and
J
m
Denoyelle resp ectively However WR itself is variable at a level of Veen
et al The stars near WR have also b een investigated by Mo at et al
from photographic plates That program was not intended to detect p ossible variability
Column of Table lists the Johnson B magnitude that they determined
Table Particulars of the variable stars around WR and WR The numbers and letters in the rst
column corresp ond to those in Figures and The p ositions are determined from the CCD frames
relative to the WR star
number name RA Dec dB B variability
B J
m m m
WR
m m
m m
a WR
m m
k
Figure left CCD image of WR star Star and are variable They are listed in Table
0 0
East is to the left and north is up The size of the eld is ab out : x : Finding charts with a larger
eld can b e found in van der Hucht et al
Figure right CCD image of WR star a Star k showed a clear variability
Figure The lightcurves of star near WR
Figure Light variations of star k near WR at Because of a di erent p ointing star k was
not observed at other dates As a comparison the other diagrams show from left to right the constant light curves of a brighter an equally bright and a fainter star in the eld
Figure shows the impressive light variations of star near WR It shows a range
m
not less than each night Our very tentative opinion is that star is a Lyrae
or W UMa type eclipsing binary In the nights in December we may have observed the
ingress to the deep minimum and days later we observed a less steep ingress p ossibly
m
to the secondary minimum half a p erio d later Note the di erence of in the height
of the two pairs of maxima We suggest that cycles elapsed b etween the observations
in December and January The p erio d would then b e P day
Figure displays the lightcurve of star k near WR together with light curves of a
few comparison stars at the same date to illustrate the quality of the data A cyclicity
is suggested amounting to somewhat more than one hour The increase of scatter of the
data p oints in the course of the night is attributed to increasing cirrus
Both of these ob jects need further photometric and sp ectroscopic investigation to de
termine the type of variability and their astrophysical characteristics
Acknowledgements We thank Jos de Bruyne for p erforming the observations The dif
ferential photometrical measurements have b een determined using the DAPHOT package
developed by JdJ This research has made use of the Guide Star Catalog pro duced by the
Space Telescope Science Institute
P M VEEN
J de JONG
A M van GENDEREN
Astr Inst Anton Pannekoek
Leiden Observatory
University of Amsterdam
PO b ox
Kruislaan
RA Leiden The Netherlands
SJ Amsterdam
email veen strw leidenuniv nl
The Netherlands
References
Denoyelle J A AS
van der Hucht K A Conti P S Lundstr om I Stenholm B Sp Sc Rev
Jenkner H Lasker B M Sturch C R et al AJ
Lasker B M Sturch C R McLean B J et al AJ
Mo at A F J Fitzgerald M P Jackson P D A AS
Russell J L Lasker B M McLean B J et al AJ
Veen P M van Genderen A M van der Hucht A A in preparation
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
MORE FLARES OF HY ANDROMEDAE
The are star HY And was found by Sharov and Alksnis on two plates taken on
September with the cm Schmidt telescop e of the Radioastrophysical Obser
vatory and with the cm Maksutov telescop e of the Sternberg Astronomical Institute
Crimean Lab oratory
We insp ected ab out and plates obtained during with the Schmidt
and the Maksutov telescop e resp ectively
On b est plates taken with the Schmidt telescop e HY And was identi ed and its
brightness in quiescent state was estimated in the range B with the average
value B The scatter can b e attributed to the random error of estimates near the
limiting magnitude of the plates used
The variable in quiescent state is not seen on plates taken with the Maksutov telescop e
limiting magnitude B
Three more ares of HY And were found Data on all of them including slightly
revised data for the rst one are listed in Table
Table
Date JD B
Sep
Sep
Nov
Jul
For light estimates of HY And magnitudes of comparison stars based on photo electric
sequences for Nova Arp and for the Field IV of M Baade and Swope
were used Equatorial co ordinates from the Schmidt plate taken on JD and
magnitudes of six comparison stars are given in Table
The p osition of HY And was measured on the same plate and on lm copies made from
h m s
glass copies of POSS O and E plates The co ordinates of HY And are
0 00
for the mean ep o ch
Table
No B
h m s 0 00 m
The available plates with the images of HY And do not however provide reliable
prop er motion of the star
Positions of comparison stars given in Table might b e useful for future e orts to
determine the prop er motion of HY And
This study was supp orted in part by the Russian Foundation for Basic Research
through grant
A S SHAROV
A ALKSNIS
Yu A SHOKIN
Radioastrophysical Observatory
N M EVSTIGNEEVA
Latvian Academy of Sciences
Sternberg Astronomical Institute
Akademijas laukums
Universitetskii prosp ect
Riga LV Latvia
Moscow Russia
References
Arp H C Astron J
Baade W Swope H H Astron J
Sharov A S Alksnis A K Astron Tsirk No
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
NEW WATER MASER IN L
We rep ort the results of a water maser search carried out with the E elsb erg m
telescop e on Feb and in the direction of two IRAS sources in the L Lynds
dark cloud A Jy emission was detected towards IRAS
We observed the ! GHz transition of H O with a b eamwidth of
00
during the night of Feb from to UTC A liquid He co oled
maser receiver was used with system temp erature in the zenith of ab out K We used
the standard channel auto correlator with bandwidths of MHz and MHz
This corresp onds to and kms resolution and and kms velocity coverage
resp ectively We observed in the p osition switching mo de with minutes integration time
on b oth the OFF and ON p ositions and minutes ON and OFF for the high resolution
sp ectra NGC was used for ux calibration We adopted Jy for its ux density
at GHz frequency corresp onding to K brightness temp erature see Baars et al
The measured ux was NTU noise tub e unit with go o d p ointing
The IRAS p oint sources IRAS and IRAS were observed on
Feb th b etween and UTC and IRAS was reobserved on Feb
th at UTC
IRAS H O maser emission was detected towards IRAS The
sp ectrum obtained with MHZ bandwidth min integration time RMS noise
Jy is shown in Figure
h m
Figure The H O ! sp ectrum of IRAS histogram measured on Feb at
UTC with the E elsb erg radiotelescop e The central part of the sp ectrum is presented as there were no other
lines detected in the velocity range kms kms Gaussian t to the blue shifted side is overlaid thin
line A redshifted excess of of the total line area is seen
There is a clear detection of an S Jy line with total line area of W Jykms
It app ears at a velocity of kms which is redshifted by ab out kms relative to
the rest velocity of the NH cloud core H which is v NH cor e kms see
LSR
T oth Walmsley There is no indication for other lines i e S p eaks in the
velocity range kms kms
The corresp onding total luminosity of the maser sp ot upp er limit assuming isotropic
radiation is
L L
H O
if we adopt p c for the distance of L as derived by Kun and Prusti their
value has an uncertainty of p c This distance value is in agreement with Bal azs
unpublished result b eing p c The uncertainty of the luminosity value is
which comes from the uncertainty in the distance
The detected line is slightly asymmetric with a red shifted wing contributing approx
imately p ercent to the total line area In Figure the observed line is shown his
togram with the Gaussian t overlaid thin line which was tted masking out the km s
km s velocity range
We note that the line may also b e tted with two Gaussian comp onents with the
following parameters velocities of kms and kms FWHM
of kms and kms correction for instrumental broadening is
negligible with kms channelwidth a p eak ux of Jy and Jy rms Jy
and line area of Jykms and Jykms resp ectively
The far infrared FIR colour indices of IRAS are log F F
log F F and log F F JISWG Its total IRAS ux was cal
culated according to Emerson i e F F m F m
IRAS
F m F m Wm F IRAS
IRAS
distance
FIR luminosity assuming isotropic Wm which corresp onds to L
pc
FIR radiation
FIR colors of b oth IRAS and IRAS are similar to those of
other maser sources found in Cepheus by Wouterloot and Walmsley
Previous water maser observations of IRAS were unsuccessful according
to
Felli et al F Jy in Feb
T oth Walmsley F Jy in Oct
Claussen et al F Jy regularly observed from Dec to Oct
Three HH ob jects were found in asso ciation with IRAS by Eiroa et al
Near infrared K band observations of the p oint source by Ho dapp indicated a
cluster of p oint sources there the reddest one among them is p ossibly driving a CO
out ow Sato et al asso ciated with the IRAS p oint source
IRAS is one of the faintest IRAS p oint sources with detected water maser
emission see e g Wilking et al and its water maser ux is relatively high as
compared to the other known examples The L L empirical
H O FIR
relation of Felli et al predicts L L
H O
The maser emission may originate in the sho cked clumps near the driving source of the
out ow Interferometric observations of this source with the aim at determining a precise
p osition would help further interpretation
IRAS showed no water maser emission during our observations with a de
tection limit of Jy times the T in the velocity interval kms v
RMS LSR
kms Water maser emission of IRAS was rst detected by Wilking et
al in Jan From Claussen et al see their Fig and from the
detection by T oth Walmsley in Oct we may assume the maser source can
b e seen at least once in a quasi p erio d of months
This research was partly supp orted by the Hungarian State Research Found OTKA
F and T and the German Hungarian Technological and Scienti c Co op
eration Pro ject Nr
M aria KUN
L Viktor TOTH
Konkoly Observatory
Lor and E otv os University
of the Hungarian Academy
Budap est Ludovika t er
of Sciences
H Hungary
P O Box
and
H Budap est XI I
Max Planck Institut f ur Astronomie
Hungary
K onigstuhl
D Heidelb erg Germany
References
Baars J W M Genzel R Pauliny Toth I I K Witzel A A A
Claussen M J Wilking B A Benson P J Wootten A Myers P C Terebey S
ApJS
Eiroa C Torrelles J M Miranda L F Anglada G Estalella R A AS
Emerson J P in A K Dupree and M T V T Lago eds Formation and
Evolution of Low Mass Stars Kluwer Dordrecht p
Felli M Palagi F Tofani G A A
Ho dapp K W ApJS
Joint IRAS Science Working Group JISWG IRAS Faint Source Survey
Kun M Prusti T A A
Lynds B T ApJS
Sato F Mizuno A Nagahama T Onishi T Yonekura Y Fukui Y ApJ
T oth L V Walmsley C M IBVS No
T oth L V Walmsley C M A A
Wilking B A Claussen M J Benson P J Myers P C Terebey S and Wootten A
ApJ L
Wouterloot J G A Walmsley C M A A
ERRATUM
Dr G Williams has revealed a misprint in the rd Name List of newly designated
variable stars IBVS No In the introductory part when listing mistakes in the ear
lier Name Lists V Pup was claimed to b e NSV The correct cross identi cation
is however V Pup NSV N N SAMUS
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
OPTICAL OBSERVATIONS OF THE STAR RX J
The sky was surveyed in the X ray region of the sp ectrum by the ROSAT satellite Vo
ges et al and catalogs of the sources included RX J GSC
Jenkner et al
The automated m telescop e Cousins R lter and CCD camera of the Climenhaga
Observatory of the University of Victoria Robb and Honkanen were used to make
photometric observations of RX J Using IRAF routines the frames were
de biased and at elded and the magnitudes were found from arc second ap erture
photometry after using the Gaussian centering option of the PHOT package
1 2 h 4 0 m 2 0 s 1 2 h 4 0 m 1 2 h 3 9 m 4 0 s
+ 5 5 o 1 6 ’ 519 + 5 5 o 1 4 ’ 683
650 + 5 5 o 1 2 ’ 548 317
1 2 h 4 0 m 2 0 s 1 2 h 4 0 m 1 2 h 3 9 m 4 0 s
Figure Finder chart of the eld lab eled with the GSC numbers Jenkner et al
The eld of stars is shown in Figure and their designations co ordinates J and
magnitudes from the Hubble Space Telescope Guide Star Catalog GSC Jenkner et al
are given in Table To lo ok for brightness variations during a night the standard
deviation of the di erential magnitudes for each star during a night were calculated and
m m
ranged from for a bright star on a go o d night to for the faint stars on p o or
nights To measure night to night variations a run mean of the fourteen nightly averages
was calculated and is shown in Table as R in the sense the star minus GSC
We consider GSC to b e the only signi cantly variable star Due to the small eld
of view extinction e ects were negligible and no corrections have b een made for them No
corrections have b een made to transform the R magnitude to a standard system
1
IRAF is distributed by National Optical Astronomy Observatories which is op erated by the Asso ciation of Universities for Research in Astronomy Inc under contract to the National Science Foundation
Table Stars observed in the eld of RX J
GSC No RA Dec GSC R V R I
C
J J Mag Mag
h m s o
variable
h m s o
h m s o
h m s o
h m s o
0.020
0.015
0.010 Chi Squared
0.005
0.000 0.00 0.10 0.20 0.30 0.40 0.50
Cycles Per Day
Figure Period search of the nightly means of RX
Figure R band light curve of RX J for
Brightness variations in RX J were barely detectable during a night but
were obvious from night to night A sine curve was t to the nightly means and the for
various p erio ds is shown graphically in Figure The b est t was found for a frequency
m
of cycles p er day and semi amplitude of This gives the ephemeris
d d
HJD of Maxima E
where the uncertainty in the nal digit is given in brackets A plot of the nightly mean
di erential GSC R magnitudes phased at this p erio d is shown in
Figure with di erent symbols for each of the di erent nights
To help classify the variable star B V R and I frames were obtained under photomet
ric conditions JD along with observations of the nearby bright standard stars
HR HR HR and HR Mo ett and Barnes The V magnitudes
and R I colors are listed in Table for the three brightest stars The random errors
C
m
for these data are ab out However great caution should b e exercised in using these
data since they are derived from only a few standard stars and their R I was trans
formed from the Johnson system to the Cousins system using the equations of Taylor
While certainly not de nitive these colors con rm that RX J is a
late type approximately K star Cousins From the admittedly p o orly deter
m m
mined B V of RX J is more likely a dwarf and not a giant star
m
Assuming an absolute magnitude of Allen we nd a distance of approximately
parsecs
From the shap e and amplitude of the light curve and the length of the p erio d we
would exp ect that this is a single K V star with sp ots and X rays pro duced by an active
corona It is p ossible that this star is a giant with sp ots or with a close companion either
heating one hemisphere or causing a tidal distortion To eliminate this p ossibility further
photometric observations are useful to lo ok for variations in color or in the height of the
maxima Sp ectral observations would b e helpful to determine the sp ectral type to lo ok
for Ca H K emission to determine v sin i and to lo ok for radial velocity variations
RG would like to thank the Austrian Ministry of Science for nancial supp ort
R M ROBB
R GREIMEL
Climenhaga Observatory
Dept of Physics and Astronomy
University of Victoria
Victoria BC CANADA V W P
Internet robb uvic ca
References
Allen C W Astrophysical Quantities the Athlone Press University of London
London UK
Cousins A W SAAO Circ
Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ
Mo ett T J and Barnes T G I I I PASP
Robb R M and Honkanen N N in A S P Conf Ser Automated Telescopes
for Photometry and Imaging ed Adelman Dukes and Adelman
Taylor B J ApJS
Voges W Aschenbach B Boller T Braeuninger H Briel U Burkert W Dennerl
D Englhauser J Grub er R Hab erl F Hartner G Hasinger G Kuerster M
Pfe ermann E Pietsch W Predehl P Rosso C Schmitt J H M M Truemper
M and Zimmermann H U A A preprint
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
June
HU ISSN
THE RECENT OPTICAL DECLINE OF V Cyg
The pre main sequence star V Cyg was discovered as the second FU Orionis vari
able in Herbig The star brightened by mag in less than one year and
reached B in see Figure The optical sp ectrum also changed signi cantly
evolving from a T Tauri like sp ectrum into an A type sup ergiant with P Cyg type emis
sion lines The star also developed large near infrared and near ultraviolet excesses over
the sp ectral energy distribution exp ected for a normal sup ergiant The large broadening
1
of optical absorption lines further indicated signi cant rotation in excess of km s
at m
Following the eruption the brightness and sp ectrum continued to evolve The sp ectrum
co oled from an A type to an F type to a G type sup ergiant in roughly a decade The
optical brightness declined by nearly a factor of ten during this time and then leveled o
at B The system also declined at all other wavelengths The magnitude of the
decline decreased monotonically from mag at m to mag at m Kenyon
Hartmann interpreted this evolution in terms of a changing color temp erature of a
central accretion disc surrounding a low mass pre main sequence star Larger declines at
wavelengths exceeding m followed the overall decline in b olometric luminosity of the
optical source This radiation is optical light absorb ed and reradiated by a surrounding
dust cloud see Kenyon Hartmann
During the past decade we have acquired UBV photometry of V Cyg to follow
the continuing decline of this interesting system We acquired these data with the cm
Zeiss re ector at the Crimean Lab oratory of the Sternberg State Astronomical Institute
00
see Kolotilov Kenyon et al Most observations were made through a
00
ap erture a ap erture was used on nights of p o or seeing We reduced the data using
Landolt s star N as the comparison and star N as the control The probable
errors are mag in V and mag in B V
Figures show our B light curves The complete light curve in Figure illustrates
the mag irregular variability prior to the eruption the mag rise itself a roughly
1
yr decline mag yr a nearly yr p erio d of constant brightness and the recent
relatively rapid decline of nearly mag see also Kenyon Hartmann and references
therein The optical source varies irregularly mag on time scales of days to
weeks throughout the optical decline The amplitude of these irregular variations increases
towards blue wavelengths and may reach mag at U Kolotilov Kopatskaya
Figure shows the recent activity on an expanded scale The system declined mag
in months recovered by mag in yr and then faded by mag in the
past year The B V color increased by B V mag as the optical brightness
declined The B V color changed very little during the increase in B brightness during
Year compare Figures and
In addition to the obvious decline the B light curve contains a wave like uctuation
with a p erio d of yr and an amplitude of mag This variation was not visible
shortly after maximum and has developed in the past decade The variation maintained
its coherence through approximately one cycle during the recent mag decline Future
data will yield b etter estimates for the p erio d and amplitude of this variation
The recent evolution of the light curve with a total decline of mag in nearly
yr resembles the rapid fading of V Cyg in the s Kenyon et al The
evolution of V Cyg was comparable in magnitude but slightly faster with a decline
of mag in slightly less than one year The change in the B V color was identical in
b oth systems Neither system showed much sp ectroscopic evolution during the decline
b oth continued to show G type absorption features at minimum light
The simplest explanation for the optical minimum in V Cyg is a dust condensation
event in the out owing wind from the inner accretion disc Kenyon et al showed
that the decline of V Cyg can b e explained with this interpretation In V Cyg
the reddening of the B V color is consistent with a mag decline in B brightness for a
standard extinction law Mathis The lack of signi cant changes on optical sp ectra
of V Cyg suggests an external event rather than a sudden co oling of the central
source caused the brightness decline
Future optical photometry will provide a test of this simple picture The brightness of
V Cyg recovered from the mag decline in several years We exp ect a similar time
scale for recovery in V Cyg once it has reached a de nite minimum
10 V1057 Cyg
12
14 B Magnitude
16
-10 0 10 20 30
Time (Years)
Figure Historical B light curve of V Cyg
13
14 B Magnitude
15
20 22 24 26 28 30
Time (Years)
Figure Recent B light curve of V Cyg
1.5
2.0 B-V
2.5
20 22 24 26 28 30
Time (Years)
Figure Recent B V evolution of V Cyg
S J KENYON
E A KOLOTILOV
Smithsonian Astrophysical Obs
Crimean Lab oratory
Garden Street
Sternberg State Astronomical Inst
Cambridge MA USA
p o Nauchny Crimea
e mail skenyon cfa harvard edu
e mail kolotilov sai crimea ua
References
Herbig G H ApJ
Kenyon S J Hartmann L ApJ
Kenyon S J Kolotilov E A Hartmann L W PASP
Kolotilov E A Pis ma Astr Zh
Kopatskaya E N Astro z
Landolt A U PASP
Mathis J S ARA A
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
PHOTOMETRIC PECULIARITIES OF CH Cyg DURING ITS RECENT
QUIESCENT PHASE
CH Cyg is a p eculiar symbiotic star A high level of variability in all the observed
parameters makes it very di cult to understand A single star mo del had b een accepted
by some authors until the s when a regular variation in radial velocities of ab out
days was revealed and the binary nature for CH Cyg was suggested Yamashita and
Maehara However explanation of the total hot comp onent luminosity during the
maximum in such a wide binary app eared to b e a crucial problem Skopal
tried to solve this problem by assuming an asynchronous rotation of the giant star in the
long p erio d binary to get a larger mass transfer via the L p oint On the other hand
Mikola jewski and Mikola jewska suggested a long term accumulation of the wind
material around a rapidly rotating magnetic white dwarf b efore its nal accretion at a
high rate A new track in the investigation of the nature of CH Cyg was set by Hinkle
et al who suggested a triple star mo del in which an unseen G K dwarf on the
long year p erio d orbit revolves the inner binary the symbiotic pair as the short
day p erio d comp onent Skopal et al a supp orted the triple star mo del giving
however two main mo di cations of the previous suggestion They showed that CH Cyg
is the system with a very high inclination of b oth the orbits and instead of the unseen
G K dwarf there is another giant star in the system on the long p erio d orbit Also
multifrequency observations from ultraviolet to the radio mm wave region carried out
during the recent active phase revealed that outbursts can arise from accretion
of material from the giant comp onent onto its companion in the symbiotic pair of the
triple CH Cyg system Skopal et al b In this contribution we present the recent
development in its UBVR light curves
CH Cyg has b een regularly monitored at the Skalnat ePleso SP and Star aLesn a SL
observatories The observations have b een made in the standard Johnson system using
a one channel photo electric photometer installed in the Cassegrain fo cus of the m
re ectors The stars HD V B V U B V R and
SAO m m sp ectrum F were used as the comparison and the check
v pg
stars resp ectively
Our new UBVR photometric observations are introduced in Table and plotted in
right panels of Figure together with those published previously in the literature They
cover a p erio d of the CH Cyg return to quiescence from its recent active phase
Here we p oint two p eculiarities which developed during this p erio d i a sudden drop in
the U brightness by mag at ab out JD marked in Figure by a bar and
ii ab out mag deep and days broad minimum centered around JD
August and pronounced more in V and R
Table New photometric observations of CH Cyg
JD U B V R Date Obs
SP
SL
SL
SL
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SP
SL
SP
SL
SL
SP
SP
SP
SL
SL
SP
SP
SP
SP
SP
SP
SP
The rst event is probably caused by cessation of the mass accretion onto the active
star in the system indicating thus the end of the recent active phase After
this b etween approximately JD and JD the color indices did not di er
from those of a typical late type giant which supp orts the ab ove mentioned idea A rival
interpretation a dust condensation in the circumstellar envelope of CH Cyg should
b e tested by the infrared radio observations which however are not available at present time
Figure Right recent UBVR photometry of CH Cyg covering its return to quiescence
The end of the active phase is marked by a bar The eclipse in the symbiotic pair of the
triple star system is marked by e Left a part of the light curve during the previous
quiescent phase It displays variations in V similar to those recently observed
The second phenomenon the deep minimum is characterized by a change in the
U B index to Prior to this minimum the M giant s day pulsations were seen
well in the V R light curves A similar b ehaviour was recorded during the previous
quiescent phase see left panels of Figure during which a series of day pulses
of the giant star was also ended by a more pronounced minimum in the V band around
JD May Here we note that only the giant star in the symbiotic pair of
the triple CH Cyg system is resp onsible for the observed day variations Skopal in
preparation In addition sp ectroscopic observations made during these two minima in
and show a similar change in the co ol continuum a signi cant smo othing
of the TiO bands cf Figure of Bo de et al and Figure of Mikola jewski et al
According to these observations and a detailed discussion on the minimum by
Taranova and Yudin we can generally see the nature of the deep minimum in the
giant s intrinsic variability rather than in a new dust creation However multifrequency
observations are strongly needed to understand b etter the real nature of such the minima
in the light curve of CH Cyg
Acknowledgments This work has b een supp orted through the Alexander von Humboldt
foundation and the Slovak Academy of Sciences Grant No
A SKOPAL
Dr Remeis Sternwarte Bamberg
Astronomisches Institut der
Universit atErlangen N urnberg
Sternwartstr
D Bamberg
Germany
Astronomical Institute
Slovak Academy of Sciences
Tatransk a Lomnica
Slovakia
e mail astrskop auriga ta sk
References
Bo de M F Rob erts J A Ivison R J Meaburn J Skopal A MNRAS
Hinkle K H Fekel F C Johnson D S Scharlach W W G AJ
Mikola jewski M Mikola jewska J In J Mikola jewska et al eds IAU Coll
The Symbiotic Phenomenon Kluwer Acad Publ p
Mikola jewski M Tomov T Kolev D Leedj arvL IBVS No
Skopal A Contr Astron Obs Skalnat e Pleso
Skopal A Bo de M F Lloyd H M Tamura S a A A L
Skopal A Bo de M F Bryce M et al b MNRAS
Taranova O G Yudin B F A A
Yamashita Y Maehara H PASJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
OBSERVATION OF THE OPTICAL COUNTERPART OF
THE GRB SOURCE
With the aid of the cm Schmidt telescop e of the Konkoly Observatory we
obtained CCD images of the gamma ray source which was detected by the Bepp oSAX
Gamma Ray Burst Monitor on May UT We used a Photometrics AT
CCD camera having a x pixel KAF MCI I coated CCD chip displaying
a arcminute x arcminute area of the sky with an angular resolution of nearly
arcsecond pixel The images were taken on the nights May frames each
minutes exp time and May June frames each minutes exp time
In order to reduce the background noise and to reach as faint limiting magnitude as
p ossible we coadded the frames taken on one particular night Figure and Figure
Filters were not used for the imaging Based on the sp ectral sensitivity distribution of the
chip the brightness values represent close to R magnitudes To estimate the brightness
of the optical counterpart of the GRB we compared its intensity to the nearby
star arcsec north R Schaefer et al marked as c in Figures and
During our observations we made p ositive identi cation of the source on the night
May and a negative one on the night May June which means that
we could not identify any visible ob ject in the previous p osition of the optical counterpart
imaged two weeks b efore Because the limiting magnitude of our coadded frame was
magnitude we conclude that the ob ject has faded b elow this brightness level
The light curve based on the data listed in Table is shown in Figure
Figure CCD image of the optical counterpart of the GRB Date of the exp osure for the coadded image is May J D
Figure CCD image of the optical counterpart of the GRB Date of the exp osure for the
coadded image is Jun J D
19
20
21 R magnitude 22
23
24 575 580 585 590 595 600 605
JD + 2450000
Figure R lightcurve of the optical counterpart of the GRB based on the brightness data
published in the IAU Circulars see References The x represents the brightness estimation made at the Konkoly Observatory
Table Brightness data of the GRB in the R band
Date UT J D m R err source
May
Galama et al
Schaefer et al
Castro Tirado et al
Gunn r Djorgovski et al a
Gunn r Djorgovski et al b
Kopylov et al
Castro Tirado et al
Schaefer et al
Galama et al
Gunn r Djorgovski et al b
Gunn r Djorgovski et al a
Kopylov et al
Mignoli et al
Castro Tirado et al
Kopylov et al
Galama et al
Schaefer et al
Gunn r Djorgovski et al b
Gunn r Djorgovski et al a
Kopylov et al
Castro Tirado et al
Gro ot et al
Gunn r Djorgovski et al b
Garcia et al
Kopylov et al
Gunn r Djorgovski et al c
Kopylov et al
Chevalier et al
present pap er
Jun present pap er upp er limit
J anos KELEMEN
Konkoly Observatory
H Budap est Box
References
Castro Tirado A J et al IAU Circular No
Chevalier C et al IAU Circular No
Djorgovski S G et al a IAU Circular No
Djorgovski S G et al b IAU Circular No
Djorgovski S G et al c IAU Circular No
Galama T J et al IAU Circular No
Garcia M et al IAU Circular No
Gro ot P J et al IAU Circular No
Kopylov A I et al IAU Circular No
Mignoli M et al IAU Circular No
Schaefer B et al IAU Circular No
CORRIGENDA
Correction to IBVS No In order to bring to accordance Table and Figure it is
necessary to interchange star s Nos and in Table and to attribute No to that one of two
stars with number in Figure that has co ordinates Xpixel and Ypixel
Y Malakhova
The eclipsing binary nature of NSV see IBVS No was discovered earlier by J
Vandenbroere IBVS No see also Diethelm s note published in IBVS No The Editors
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
MULTIPERIODICITY OF THE SCUTI STAR BR CANCRI
BR Cancri HD SAO also known as KW in Praesep e cluster was
discovered as a Scuti star by Breger on the basis of several hour long observations
It pulsates with a p erio d of days The author found no more data available in
the literature For checking its variability observations covering a total of ten nights were
secured b etween February and March The observations were carried out by
using a three channel high sp eed photometer P A attached to a cm re ector of Xin
glong Station of Beijing Astronomical Observatory China The photometer is esp ecially
used in WET the Whole Earth Telescope network Nather et al The comparison
h m s 0 00
star RA D ec V used was chosen carefully No
variation was found in its brightness Furthermore the constancy of comparison star
h m s 0 00
was indep endently insp ected with another star RA D ec
V in one night The data were acquired as continuous s exp osures through
Johnson s V lter The data were corrected for the sky background contribution and the
atmospheric extinction In order to analyze pulsational frequencies all the measurements
were binned into s integrations by taking p oint averages and the times of measure
ments of BR Cnc were converted into HJD This way datap oints were obtained The
characteristics of the light curve of BR Cnc is shown schematically in Figure according
to the high time resolution photo electric photometry The brightness variation app ears
to b e multi perio dic
After the application of consecutive prewhitening pro cedure and frequency analysis
at least frequencies were resolved through a standard Fourier program Period Breger
Figure displays the preliminary p ower sp ectra of three apparently exhibited
Figure One of the typical high time resolution V light curves of BR Cnc observed on February
Exp osure time of each p oint is s
Figure The sp ectral window in top panel and p ower sp ectra of three suggested frequencies of
BR Cnc The fundamental frequency c d is displayed in the second panel the third and fourth
panels corresp ond to and c d resp ectively Note that di erent ordinates were used for
5
the DATA P f ordinate go es up to mag from the origin for DATA P f ordinate
1 2
6 6
go es from to for DATA P f the p eak value is just p ower of mag the b ottom
3
panel shows the p ower of the residuals of the tting with frequencies ab ove Abscissa in cycles day
frequencies f f and f cycles day with a standard error
of The p eaks at frequencies f and f could b e in uenced by a c d aliasing
which can b e seen from the sp ectral window In view of the relatively short coverage the
pulsational nature of this low amplitude Sct star deserves further investigation
I would like to thank Dr Li Zhiping for valuable suggestion which greatly inspired
me in the analysis of the observational data This research was granted by the National
Science Foundation of China
Aiying ZHOU
Beijing Astronomical Observatory
Chinese Academy of Sciences
Beijing P R China
Internet aiying bao bao ac cn
References
Breger M A A
Breger M Comm Asteroseismology Vienna Austrian Academy of Sciences
Nather R E Winget D E Clemens J C Hansen C J Hine B P ApJ
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
IMPROVED POSITIONS FOR SONNEBERG VARIABLES
PART
This pap er is the second one devoted to the p osition improvements for Sonneb erg
variables with more details given in M anek
Table gives precise p ositions for ob jects having published nding charts in MVS
North on these charts is on the top with exceptions marked directly on indi
vidual charts However there are deviations from this rule and these are noted in remarks
Comments from original pap ers of Ho meister were used when p ossible The
source of the p osition is co ded as follows A A C CCD D DSS Fitsview
00
E estimate P plate scan Positions should b e precise to for A C P co de and
00
to for D co de The p ossible error for E co de is noted in remarks Identi cation
with GSC is given where p ossible No other identi cations were searched for As the nal
designation do es not app ear on the charts it was not known at the time when charts
were published provisional designation is given in the table to o The di erences result
ing from a comparison with the p ositions given in GCVS in the sense new GC V S are
also shown where is given in seconds of time and is given in minutes of arc
Table
Prov desig Name RA Dec GSC s Remark
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Oph A : :
AZ Ser A : :
BB Ser A : :
V Oph A : :
V Oph A : :
V Oph A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
LT Aql A : :
V Aql A : :
UY Sge A : :
Table continued
Prov desig Name RA Dec GSC s Remark
CE Del A : :
CG Del A : :
WW Del A : :
XX Del A : :
AA Del A : :
AD Del A : :
AE Del A : :
SY Del A : :
BL Del A : :
DG Del A : :
DF Del A : :
AL Del A : :
DK Del A : :
BO Del A : :
AP Del A : :
TU Del A : :
DS Del A : :
DT Del A : :
BQ Del A : :
DU Del A : :
AU Del A : :
AW Del A : :
EE Del A : :
AZ Del A : :
BS Del A : :
BV Del A : :
V Oph A : :
NSV A : :
NSV A : :
NSV A : :
NSV A : :
NSV A : :
NSV A : :
V Oph A : :
V Oph A : :
NSV A : :
NSV A : :
V Oph A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
NSV A : :
V Oph A : :
V Oph A : :
V Oph A : :
NSV A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
Table continued
Prov desig Name RA Dec GSC s Remark
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A
V Aql A : :
EG Aql A : :
V Aql A : :
V Aql A : :
NSV A : :
QW Aql A : :
GZ Aql A : :
V Aql A : :
V Aql A : :
Ross QX Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
NSV A : :
V Aql A : :
NSV A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql D : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
V Aql A : :
Ross V Aql A : :
Table continued
Prov desig Name RA Dec GSC s Remark
V Aql A : :
V Aql A : :
UX Sge A : :
BZ Del A : :
CF Del A : :
BE Del A : :
VY Del A : :
CN Del A : :
CP Del A : :
WY Del A : :
CR Del A : :
CV Del A : :
AH Del A : :
AM Del A : :
AO Del A : :
DN Del A : :
DO Del A : :
AQ Del A : :
AS Del A : :
DV Del A : :
DW Del A : :
EF Del A : :
BT Del A : :
EH Del A : :
BR Cep A : :
BT Cep A : :
CH Cep A : :
CK Cep A : :
NSV A : :
Remarks
Two entries for the same star in A The p osition given in the table is an average
Slightly uncertain identi cation
BV Del unlab eled circle on chart for BS Del
V Oph Two GSC numbers and for one star Northern comp onent of a double
h m s 0 00
star the southern one having p osition : :
V Aql north on the b ottom
UX Sge mean p osition of a close double not known which comp onent varies
The author would like to thank D G Monet for providing the USNO A catalogue
Jan MANEK
Stef anikObservatory
Pet r n
Praha
Czech Republic
e mail jmanek mbox vol cz
References
Cotton W D Fitsview v
see also http www cv nrao edu bcotton fitsview html
Ho meister C Astron Nachr
Ho meister C Astron Nachr
M anek J IBSV No
Mitteilungen uber Ver anderliche Sterne No
Monet D G et al USNO A V U S Naval Observatory Washington DC
see also http www usno navy mil pmm
STScI http stdatu stsci edu dss
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
NEAR IR TiO BAND PHOTOMETRY OF Ori
Orionis Betelgeuse HD M Iab is the brightest star in the infrared sky It is
also one of the closest with the recent Hipparcos Survey revising its distance determination
to p c Wing The star s relative proximity coupled with its semi regular
variability and advanced evolutionary age has made it an attractive target for a number
of studies For example Guinan et al have rep orted an overall photometric
variability of mag over the last decade while Dupree et al have found a
yr p erio dic mo dulation of mag in blue wavelengths that stretches back to
Gilliland and Dupree have used direct imaging techniques with HST to uncover a
substantially extended chromosphere in the sup ergiant as well as a large bright sp ot that
app ears hotter than the surrounding chromosphere by at least K Dyck et al
have even used m interferometric techniques to obtain an angular diameter for Ori
of mas This corresp onds to a radius of R
Despite these studies Ori remains an enigmatic ob ject There is still some question
as to the prop er mass loss mechanism that can form the star s extensive circumstellar
envelope Dupree et al Furthermore the p erio d of pulsations may not b e constant
with time There is also evidence of p erio d doubling and p erio d tripling in the star s
visible ux Smith that hints at the star s internal complexities Optical wavelength
observations of Ori have continued up to the present by Krisciunas Luedeke
and at Villanova University by Guinan since but have shed little light on
these stellar riddles To understand and b etter quantify the b ehavior of Ori we decided
to undertake a more extensive program of di erential photometry of this famous star
From September to April Ori was observed at the Wasatonic Observatory
Allentown Penn as part of the ongoing program b etween the Wasatonic and Villanova
Observatories to study co ol giants and sup ergiants The photometry rep orted here was
conducted on a total of nights using an unco oled Optec photometer attached to a cm
Schmidt Cassegrain telescop e The detector employed was a silicon PIN photo dio de The
2
comparison star was Ori V B V K I I I and the check star was
Ori V B V B I I I Di erential photometry was conducted using the
standard sequence of sky comp var comp sky check comp sky in b oth the V band and
Wing near IR three lter system to measure TiO Wing
Wing s photometric system is characterized by observations in three separate band
passes denoted by A B and C Table lists the central wavelengths and bandwidths of
these three lters These lters were chosen to measure the three basic prop erties of co ol
stars their infrared magnitude their color and their temp erature as measured by the
strength of their TiO absorption band Filter A is sensitive to the TiO nm
bandhead while lters B and C are essentially clear of strong absorptions In order to
extract an unreddened measure of the strength of the TiO band Wing has devised
a reddening free TiO index as A B B C
Figure The V band and near IR observations of Ori The top panel shows Ori s
V band light curve over the observation p erio d The star s IR color index and C magnitude light
curves are shown in panels and resp ectively The b ottom panel is a plot of TiO indices as de ned
by Wing s three color lter system Note the inverse correlation b etween TiO strength and brightness of the star
Figure Results for Ori for the observation p erio d The top panel shows the star s
luminosity The middle panel shows Ori s temp erature as derived from TiO indices The b ottom panel
depicts Ori s radius over time based on a symmetric global pulsation mo del
1
Table Wing s Three Color Near IR Filter Set
Filter Region Measured Central Wavelength Bandpass FWHM
nm nm
A TiO Band
B Continuum
C Continuum
1
Taken from Wing
where A B and C are the magnitudes in those resp ective lters The quantity B C
is de ned as the star s near IR color index Wasatonic has provided a calibration
system based on standard stars Wing that relates TiO strength to a star s tem
p erature The result is an inverse correlation b etween temp erature and TiO index for K
to M stars shown b elow
T emp K TiO Index
Table Wasatonic Observatory Filter A B C Data for Ori
Sep Apr
JD A B C JD A B C
It should b e noted that this relationship fails outside the sp eci ed sp ectral classes since
TiO band strengths are insensitive to temp erature changes outside of the K to M range
The b olometric magnitude m of the star can also b e approximated using the Wing
bol
system Filter C is an accurate measure of an M star s near infrared continuum and
covers their wavelengths of p eak intensity Furthermore it is known that near infrared
continuum p oints of Mira variables are very similar to their b olometric light curves in
terms of shap e phase and amplitude Lo ckwoo d Wing Wing Hence the
magnitude of lter C is a go o d representation of the star s apparent b olometric magnitude
Using b olometric corrections from Novotny we compared the apparent m and
bol
C magnitudes of stars with comparable temp eratures to Orionis A total of eight
M I I I Wing standard stars Wing were used in the comparison Since b olometric
corrections are nearly identical for M giants and sup ergiants Novotny we found
that for b oth classes of stars
m C
bol
where C represents the magnitude of the C lter This magnitude correction has a
standard deviation of The luminosity of the star can then b e calculated from
its m by the usual means
bol
The data collected at the Wasatonic Observatory is listed in Table Observations were
conducted in b oth V band and Wing s three color lter system with light curves shown
in Figure The rst panel shows a plot of Ori s V band light curve Ori dropp ed
mag in V band brightness over the observation p erio d The maximum brightness
of mag is ab out the brightest the star ever achieves Guinan Light curves
of the star s near IR color index and C magnitude are shown in the second and
third panels resp ectively The small scale uctuations in the data app ear to b e physical
variations and are not observational scatter TiO indices were then calculated using the
Wing system describ ed ab ove and are shown in the b ottom panel of Figure Note the
general anti correlation b etween TiO band strengths and the brightness of the star
Figure summarizes our results based on the near IR data The top panel shows
Ori s luminosity the middle panel its e ective temp erature and b ottom panel its e ective
radius over our observation p erio d The left axis of the gure shows relative changes with
resp ect to the mean while the right axis shows absolute values As shown in the top
panel Ori s luminosity systematically dropp ed approximately with resp ect to the
mean over our observation stretch This was accompanied by a systematic drop in
e ective temp erature during the same time interval Based on our TiO data Ori
showed an average e ective surface temp erature of K The maximum and minimum
temp eratures were K and K corresp onding to TiO indices of and
resp ectively These temp erature values agree well with the interferometric estimated
surface temp erature of K by Dyck et al
It is still uncertain whether the luminosity changes shown in the top panel of Figure
are due to uniform global pulsations of the star or the growth and decay of lo cal
hot sp ots on the surface Goldb erg concludes from radial velocity data that the
visual brightness variations are probably not global in nature However Dupree et al
assert that the regularity of Ori s variability argues against the erratic random
variability asso ciated with the emergence of convective cells Under the assumption that
the luminosity variations are global in nature the e ective radius of Ori was computed
for each observation The result is shown in the b ottom panel of Figure
Ori exhibited an average e ective radius of R with changes of less than
ab ove and b elow the mean radius over the observation p erio d This value compares with
past interferometric radius determinations For instance Dyck et al used m
observations to obtain an angular diameter of mas corresp onding to a radius of
R and Balega et al have used A observations to obtain an angular diameter
of mas corresp onding to a radius of R This pap er s result however represents
the rst ndings of Ori s radius using intermediate infrared observations and the new
Hipparcos distance
Curiously there app ears to b e no systematic change in Ori s e ective radius to match
the trends discussed ab ove for Ori s luminosity and temp erature This might indicate
that global pulsations are not alone resp onsible for Ori s brightness variations Instead
the growth and decay of lo cal blobs and hot sp ots may contribute to Ori s variability in
a non trivial way More near IR and radial velocity data is needed b efore any p ermanent
conclusion can b e reached It should also b e noted that our absolute luminosity and radius
values critically dep end on the empirically derived transformation b etween the C
lter and b olometric magnitude Further observations of M I and I I I stars using Wing s
near IR lter system would improve the reliability of this transformation Observations
of Ori at the Villanova and Wasatonic Observatories will continue in b oth V band and
near IR wavelengths
The authors thank Rob ert Wing for his assistance For this research we utilized the
SIMBAD database op erated by CDS Strasb ourg France This work was supp orted in
part by NSF grants AST to Villanova University and AST to the Four
College Consortium which we gratefully acknowledge
Nicholas D MORGAN
Rick WASATONIC
Edward F GUINAN
Dept of Astronomy and Astrophysics
Villanova University Villanova PA
References
Balega Y Blazit A Bonneau D Ko echlin L Foy R Lab eyrie A A A
Dupree A K Baliunas S L Guinan E F Hartmann L Nassiop oulos G E
Sonneb orn G ApJ L
Dyck H M Benson J A van Belle G T Ridgway S T AJ
Gilliland R L Dupree A K ApJ L
Goldb erg L PASP
Guinan E F Deeney B Miller K IAUC No
Guinan E F unpublished
Krisciunas K Luedeke K D IBVS No
Lo ckwoo d G W Wing R F ApJ
Novotny E Introduction to Stel lar Interiors Oxford University Press p
Smith M A BAAS
Wasatonic R unpublished
Wing R F in Spectral Classi cation and Color Temperatures for Bright Stars
in the Range K M Astronomy Dept Ohio State University
Wing R F in The Study of Variable Stars Using Smal l Telescopes ed J R Percy
Cambridge University Press Cambridge England p
Wing R F JAAVSO
Wing R F private communication
COMMISSIONS AND OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number
Konkoly Observatory
Budap est
July
HU ISSN
RADIUS AND LUMINOSITY VARIATIONS OF MIRA
FROM WING NEAR IR PHOTOMETRY
Mira omicron Ceti AB is the prototype of a class of pulsating red asymptotic giants
that undergo large typically to mag in V brightness variations with p erio ds of
a few hundred days Mira itself is more complex as it is a binary system comp osed of
the luminous M I I Ie star o Ceti Mira A HD and a hot accreting comp onent
00
distant Mira B AAVSO visual estimates of Mira A have shown its brightness to
vary typically b etween rd and th magnitude over a p erio d P d Recently Mira s
parallax has b een re determined by Hipparcos to b e r p c van Leeuwen et al
As one of the nearest Mira variables its brightness has made it a favorite ob ject
for sp ectroscopic photometric and interferometric measurements
Of particular interest to the study of Mira and Mira variables in general are obser
vations obtained in the infrared Among the co olest of all stars their maximum energies
lie in the near infrared and typical Miras are magnitudes brighter in this region
than they are in the optical Also there are fewer molecular absorption features in the
infrared than at optical wavelengths As discussed by Wing the interpretation of
standard UBVRI optical photometry of Miras and other co ol variables is compromised
chie y by the presence of strong TiO molecular features that fall within these bandpasses
for stars with sp ectral types of M or later For these reasons Wing has developed
a simple near infrared photometric system for use with red stars including Miras This
photometric system uses three intermediate band lters that have b een carefully chosen
to have bandpasses that include a temp erature dep endent TiO molecular band and two
in the near IR that are essentially free of strong absorption features except in the co olest
of stars
The rst lter designated by Wing as A is centered around one of the strongest isolated
TiO bands and has a central wavelength of nm TiO was chosen b ecause it
is an excellent temp erature indicator in co ol stars and it has b een known for a long time
that visual maximum corresp onds to the time of highest temp erature and weakest TiO
band strength in Miras Pettit Nicholson Filter B with a central wavelength of
nm is placed in a region essentially clear of strong absorptions except in the co olest
of stars Both A and B have bandpasses of nm Filter C is also lo cated at a region
essentially free of absorption but at a much longer wavelength centered at nm where
it provides a measurement of the infrared apparent magnitude Its bandpass is larger at nm which comp ensates for the usual decreased detector sensitivity at this wavelength
Figure V light curve of Mira covering half of its pulsation p erio d
Figure Light curves of Mira s TiO Index B C Index and C mag
Figure Luminosity e ective temp erature and radius of Mira The prop erties were estimated using
the near IR B C Color Index to obtain an e ective temp erature and the transformed C as
mag
an approximation of m bol
As discussed by Wing lter C can also b e used as a short cut to measuring the
star s total energy output as the light curves of Mira variables measured at near infrared
continuum p oints are similar to b olometric light curves in shap e amplitude and phasing
Lo ckwoo d Wing Wing Filters B and C are used together to obtain a
color index de ned by
near IR Color Index B C
Because this color index measures the slop e of the continuum and is a ected little by
sp ectral lines and bands it is primarily an indicator of temp erature Finally a TiO index
can b e obtained by using the magnitudes of all three lters in the formula
TiO Index A B B C
With this metho d the continuum level is extrap olated to the TiO wavelength band and
the observed magnitude at this band is compared to the magnitude the star would have
if no TiO band were present The numerical co e cient is determined by the spacing of
the lters in wavelength The TiO Index is the measure of the relative strength of the
TiO bandhead near nm and as de ned the index b ecomes numerically larger as the
TiO absorption increases
Starting in photometric observations of Mira covering half of its pulsation p erio d
from light maximum to past light minimum have b een carried out by Wasatonic using
the Wing near infrared ABC bands just describ ed as well the V band With a cm
Schmidt Cassegrain SCT coupled to an unco oled Optec photometer the photometry
was carried out relative to nearby and check stars following the usual observing sequence
of sky comp var comp sky check comp sky The comparison star was HD V
B V G I I I and HD V B V K V was the
primary check star In addition several Wing standard stars ranging from M to M were
observed most nights and their TiO and B C indices were obtained The photometric
observations of Mira are provided in Table
Table Photometric data
JD V A B C
Figure shows the visual band light curve Phasing was done using a t of JD
max
and a p erio d of days Quirrenbach et al
Using the formula previously describ ed the TiO index was calculated for each obser
vation Figure shows the TiO Index B C Index and the C light curve versus phase
mag
From the data it can b e seen that the b olometric magnitude which is computed from
C see b elow reaches its faintest value near Mira s minimum phase at P
mag
As would b e exp ected the B C color index also reaches its greatest value at this phase
indicating the lowest temp erature The TiO index b ecomes unreliable as a temp erature
indicator at Mira s minimum b ecause the continuum regions of the sp ectrum b ecome con
taminated by lines of VO and other molecular sp ecies at T K Wing This
ef f
is noted in Figure as the TiO index is nearly constant from phases P
To test the accuracy of using the C as an approximation of the apparent
mag
b olometric magnitude m a calibration was carried out using a large number of Wing
bol
standard stars whose C or comparable I are given by Wing
mag mag
and whose V magnitudes and sp ectral type are known Wing By calculating m
bol
for each of these stars by the standard formula
m V BC
bol mag
and comparing the results to the given C it was found that the C was
mag mag
fainter by an average di erence of mag with a standard deviation of mag
Therefore this di erence was added to each C lter reading to obtain a go o d estimate of
the apparent b olometric magnitude The b olometric correction BC values were obtained
from Novotny
Using this adjusted value of m and the distance to Mira the absolute b olometric
bol
magnitudes M were calculated for each observation phase Mira s luminosity was then
bol
calculated relative to the sun s and is shown in the upp er panel of Figure
An estimate of Mira s temp erature at each observation phase was determined by apply
ing a set of standard stars whose e ective temp eratures are known and whose B C color
indices were obtained by Wasatonic The middle panel of Figure shows the variations
of Mira s temp erature with phase
With estimates of b oth Mira s luminosity and temp erature at each observation phase
a radius can b e determined from the standard formula
2 4
L R T
The b ottom panel of Figure shows Mira s radius versus phase Large scale radius changes
from an R R AU to an R R AU can b e seen in the plot
min max
To place Mira s size in b etter p ersp ective if the star were placed at the center of our
solar system it would extend from just b eyond the orbit of Mars AU to half way
the distance of Jupiter AU The following table summarizes the extremes of the
prop erties of Mira found during the ep o ch
Table Mira s Estimated Prop erties
V B C Index T Sp ec Type L L R R Radius AU
mag ef f
4
M I I I
3
M I I I
This work represents the rst time the radius of Mira has b een estimated using its
prop er distance and intermediate band near infrared photometric techniques The values
obtained for the radius compare well with previous interferometric measurements such
as those of Lab eyrie et al who found a radius of R at nm at light
maximum Phase Also the mean radius of R recently rep orted by van
Leeuwen et al is in excellent agreement with our mean radius of R However
interferometric observations at nm by Karovska et al when corrected for
Mira s recently determined distance yield an average radius of R at nearly light
maximum Phase Again it should b e noted that our estimates of radius and
luminosity are based up on a transformation of the C to m Relative changes
mag bol
obtained for the radius of Mira however are not dep endent on this approximation and
should b e of particular interest Further near IR observations of Mira over its entire
pulsation p erio d and the results of radius estimates will b e rep orted in the future
The authors wish to thank Rob ert Wing and the SIMBAD database for their assis
tance in this work This research is supp orted by NSF grants AST to Villanova
University and AST to the Four College Consortium
Todd A MAHLER
Rick WASATONIC
Edward F GUINAN
Dept of Astronomy and Astrophysics
Villanova University Villanova
PA
References
Karovska M Nisenson P Papaliolios C Boyle R P ApJ L
Lab eyrie A Ko echlin L Bonneau D Blazit A Foy R ApJ L
Lo ckwoo d G W Wing R F ApJ
Novotny E Introduction to Stel lar Interiors Oxford University Press p
Pettit E Nicholson S B ApJ
Quirrenbach A Mozurkewich D Armstrong J T Johnston K J Colavita M M
Shao M A A L
van Leeuwen F Feast M W Whitelo ck P A Yudin B MNRAS in press
Wing R F in Spectral Classi cation and Color Temperatures for Bright Stars
in the Range K M Astronomy Dept Ohio State University
Wing R F in The Study of Variable Stars Using Smal l Telescopes ed J R Percy
Cambridge University Press Cambridge England p
Wing R F JAAVSO