This dissertation has been microfilmed exactly as received 68—3067

SIMONSON, HI, Simon Christian, 1938- A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGA­ TION OF THE STELLAR ASSOCIATION CEPHEUS OB2. The Ohio State University, Ph.D., 1967 Astronomy

University Microfilms, Inc., Ann Arbor, Michigan A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGATION

OP THE STELLAR ASSOCIATION CEPHEUS OB2

DISSERTATION

Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University

By

Simon Christian Simonson, III, S.B., M.Sc,

The Ohio State University 1967

Approved fcy

Department of Astronomy MKNOWLEDGMEHTS

It is a pleasure to thank my adviser, Professor Arne

Slettebak, for his encouragement, guidance, and support in this investigation. Professor Phillip C. Keenan and Pro­ fessor Carlos Jaschek read the manuscript and provided much helpful advice and criticism. I am also indebted to them and to Professor Slettebak for many discussions about the spectral classification.

My wife, Jade, cheerfully endured the discomforts of a disrupted household, provided many useful ideas about computer programming, and also typed the manuscript and final copy in a most professional way. For all this and her loyal encouragement throughout the production of this thesis, I am grateful.

The Lowell Observatory generously provided six nights of their 21-inch telescope time and gave substantial sup­ port during my observing period with the 72-inch telescope.

I particularly thank Dr. John S. Hall, the director? Dr.

Peter B. Boyce, who made his integrating photometer avail­ able? Dr. K. Serkowski, who provided his gain calibration in advance of publication? and Mr. Erik H. Olsen.

ii Dr. Robert F. Garrison of the Mount Wilson and Paiomar

Observatories kindly showed me the ropes on the 72-inch telescope, and gave me many helpful suggestions about this investigation.

I gratefully acknowledge the support of the Ohio State

University Computer Center^ which contributed large amounts of free computer time for the data reduction.

This work was begun while I had the support of a Na­ tional Defense Education Act Fellowship and completed while

I held a National Aeronautics and Space Administration

Traineoship.

iii VITA

December 20, 1938 Born-Fergus Falls, Minnesota

I960* ...... S. B., Massachusetts Institute of Technology ^ Cambridge, Massachusetts

1960-1963. . . . Active duty, U. S. Wavy, Mare Island Naval Shipyard, Vallejo, California

1965...... M. Sc., The Ohio State University, Columbus, Ohio

PUBLICATIONS

"Photographic UBV Capabilities of the 16/24-inch Schottland Schmidt Telescope of Perkins Observatory." M.Sc. Thesis, The Ohio State University, June 1965, 52 pp.

FIELDS OF STUDY

Major Fields Astronomy

Studies in Stellar Spectra. Professors Arne E. Slettebak and Phillip C. Keenan

Studies in Stellar Systems. Professors Phillip C. Keenan? Carlos Jascheky and Walter 3. Mitchell, Jr.

Studies in Theoretical Astrophysics. Professors Arne E. Slettebak? George W. Collins, II? Eugene R. Capriotti? Walter K. Bonsack? and Stanley J. Czyzak

Studies in Radio Astronomy. Professors John D. Kraus and H. C. Ko

Minor Fields Physics

Studies in Quantum Mechanics and Atomic Structure. Pro­ fessors Jan Korringa, Clifford V. Heer, Hershel J. Hausman, and Charles H. Shaw

Studies in Mechanics and Plasma Physics. Professor Carl H. Nielsen

iv TABLE OF CONTENTS Page

ACKNOWLEDGMENTS ii

VTTA iv

LIST OF TABLES vii

LIST OF ILLUSTRATIONS ix

Chapter I. INTRODUCTION...... 1 Purpose of This Investigation. .... 2

Summary of Previous Work .«••••• 4 Discovery Spectroscopic and photometric observations The question of expansion The nuclear clusters Surveys and other observations Radio observations

II. SPECTRAL CLASSIFICATION...... 14

Slit Spectroscopy. •••••••••• 14 Selection of stars Observations Classification and results

Objective Prism Spectroscopy • • • • • 25 Observations Classification criteria Results

III. PHOTOMETRIC OBSERVATIONS...... 42

Photoelectric UBV Photometry • . • • • 42 observations Results

v TABLE OF CONTENTS— Continued

•Page

Chapter IIIContinued

Photographic Photometry...... 55 Observations Reduction of observations

IV. RESULTS AND CONCLUSIONS...... S3

Photometric Distances...... S3 Presentation of results Discussion of errors Star distribution

Clusters •••••••• ...... 117 NGC 7160 Trumpler 37 Possible new clusters

Motions...... 125 Radial velocities Proper motions

Radio Observations •••••••.•• 131

Conclusions. ••••• ...... 133 The structure of Cepheus OB2 Relation to galactic structure Suggestions for future work

L IS T OF REFERENCES...... 143

vi LIST OF TABLES

Table Page

1. MK Standards used in this Work. • • • • • 13

2. Results of Spectral Classification. . . . 20'

3. Schmidt Plates used for Spectral Classification. •••••••••••• 27

4. MK Standards Observed with the Schmidt Telescope ••••••.•••••••• 23

5. Comparison of Schmidt and MK Classification. •••••••••••• 34

6. Extinction and Instrumental Corroctions for Photoelectric Photometry. • • • • • 49

7. Results of Photoelectric Photometry . . . 52

3. Photometric Plates Taken with the 4-Inch Ross Camera, •••••••••• 56

9. Magnitude Reduction Coefficients. • • • • 60

10. Absorption and Distances from MK Classi­ fication and Photoelectric Photometry . 64

11. Absorption and Distances from Schmidt Classification and Photoelectric Photometry. ••••••••••••.. 67

12. Absorption and Distances from MK Classi­ fication and Photographic Photometry. • 68

13. Absorption and Distances from Schmidt Classification and Photographic Photometry. •••••••••••••• 69

14. Intrinsic Colors and Absolute Magnitudes. 106

15. Observed star Distribution. ••••••• 113

vii LIST OF TABLES— Continued

Table Page

16, 19 Cephei Cluster Members ...... 122

17* Members of Anonymous Cluster at 22^07m , +57°10*...... 123

18. Members of Cluster Near HD 210478 • • • • 124

19. Stellar Radial Velocities 126

viii LIST OF ILLUSTRATIONS

Figure Page

1. Comparison of MK and Schmidt Classi­ fication for Luminosity Classes V and IV...... 36

2. Natural Groups of the Schottland Schmidt Telescope ••••• ...... 39

3. Finding Chart for Eastern Cepheus 0B2 . . 99

4. Finding Chart for Western Cepheus 0B2 . . 100

5. Finding Chart for Tr 37...... 101

S. Finding Chart for Region of 19 Cephei and NGC 7160...... 102

7. V-Mv vs. Eg^y for Stars Observed in Cepheus ••.••••••••••... 104

S. Space Distribution of Stars in Tables 10, 11, and 12...... 110

9. Observed Star Distribution vs. Distance from the Sun...... 114

10. Observed Star Distribution vs. Distance from the Sun. ••••••••••••• 114 11. H-R Diagram for NGC 7160...... 117

12. H-R Diagram for Tr 3 7 ...... 120

13. Radial Velocity vs. Distance for Stars in Table 1 9 ...... 123

14. H-R Diagram for Stars Between 350 and 700 pc...... 134

ix LIST OF ILLUSTRATIONS— Continued

Figure Page

15. Appearance on the Sky of Group A. . • • . 136

16. Appearance on the Sky of Group B . 136

17. H-R Diagram for Stars Between 700 and 1000 p c ...... 137

x I . INTRODUCTION

The early-type star association designated Cepheus OB2 by the International Astronomical union (1964 Transactions,

12B. 34S) lies above the galactic equator in latitudes b H = 1° to 9° between longitudes I11 =* 94° to 106° (20^50m to 22h10^ +55° to +63° in equatorial coordinates), Cepheus

032 has previously been called Cepheus II by Ambartsumian

(1949b) and I Cephei by Morgan, Whitford, and Code (1953).

It is one of the nearer and richer associations. Morgan,

Whitford, and Code (1953) listed 21 probable members of absolute magnitude brighter than -3 and placed it at 720 parsecs (pc)? Markarian (1952) listed 26 probable members of early spectral type and placed it at 630 pc.

Markarian (1953) gave a summary description of Cepheus

032 s

In the area between £l2* * 98° to 105°, b11 = 1° to 9°3 one finds an aggregation of 0-B2 stars v/hich form the association Cepheus f0B2*], . . . The absorption of light is greater in the direc­ tion of the association than in the surrounding area. Seven members are class c and their appar­ ent magnitudes range from 5 to 6. The distance of the association is about 600 pcj its diameter is about 30 pc. Over 3/4 of this area is occu­ pied by the gaseous nebulae S86, IC 1396, S7, and S8. Two open clusters are presents Trump- ler (Tr) 37 and NGC 7160, and also many multi­ ple stars and star chains, such as ADS 15434, 14749, 14868, 15624, and 15601.

1 2

Markarian (1953) also presented a map of the distribution of all stars of types B2 and earlier for which corrected TT distance moduli could be obtained between 1 = 90° to 110° and b11 =-10° to +10°. Cepheus 032 appears as a concen­ tration of stars separated from the galactic field at a corrected distance modulus of about 3,9, It also appealed to Morgan, Whitford, and Code (1953) as a separate con­ centration.

Purpose of this Investigation

Because Cepheus 0B2 comprises many hot, bright, young stars and the interstellar material which some of them ionize ancl from which they are all thought to have been formed, it appears to be a good region in which to study the processes of star formation, Cepheus 0B2 is particu­ larly valuable because it is near the sun. Since it ex­ tends to fairly high galactic latitudes, there should be a good possibility of distinguishing stars of the associ­

ation from more distant stars in the galactic plane,

Nevertheless, despite its richness and nearness,

little is known about the stars fainter than absolute mag­

nitude -4 which may belong to the association (Blaauw

1964), although Shakhovskoi (1956) concluded from a stat­

istical study of catalogued Information that Cepheus 0B2

probably comprises about 150 stars of spectral types 0-B5

and about 1500 stars of spectral types B8-A1. There is 3 even a question whether all the bright stars which have been attributed to Cepheus 0B2 should be considered mem­ bers. Using information from catalogues, Shakhovskoi

(195S) found large dispersion in the photometric distances, and Kopylov (1S5Q) found four groups of early-type stars at distances of 460 to 1350 pc.

Among the OB associations and early-type clusters near the sun, Cepheus 032 stands out because of the lack of information available for it (Blaauw 1964). 3ven some of the brighter stars attributed to the association lack photometric distances. *Ihe distribution of fainter early-

type stars in the region has been largely unknown. In­

sufficient information has been available to answer the question of the physical reality of the association,

to determine its structure, to investigate its state of

motion, or to establish the distribution of stellar masses

and luminosities. The addition of photometric distances

for the bright stars, extension of iiK classification to

fainter stars, and the identification of possible fainter

members were required in order to answer these questions.

The right instruments for obtaining these data were

at hand at the Perkins Observatory in Delax^are, Ohio, and

at the Lowell Observatory in Flagstaff, Arizona. Spectro­

grams at a useful dispersion for MK classification could

bo obtained with the 72-inch Perkins reflector at the

Lowell Observatory and the 32-inch Schottland reflector at 4 the Perkins observatory. Photoelectric UBV observations could be made with tho 21-inch telescope at the Lowell observatory to obtain photometric distances for the stars with MK classifications and to establish a sequence of photometric standards for photographic photometry. The

16-inch Schottland Schmidt telescope at the Perkins Ob­ servatory is eq;uipped with an ultraviolet-transmitting prism which is particularly useful in the classification of early-type stars. The Schmidt telescope was not suit­ able for photographic photometry because of deviations of the photographic plates from the focal surface, but a

4-inch Ross camera with a wide field x?as available for this purpose.

Summary of Previous Work

Discovery

Struve (1927) first called attention to the group of hot stars now called Cepheus 0B2, picking it out on the basis of the information in the Henry Draper (I-ID) cata­ logue. Pannekoek (1929) found a distance of about 500 pc for this group, which he called Cepheus 1. When Ambart­

sumian (1949a) introduced the term stellar association to

indicate the importance of these groups of hot stars in

stellar formation and evolution, he called attention to

Cepheus OB2 (Ambartsumian 1949b), designating it Cepheus

II. Markarian continued Ambartsumian*s work and in a series of papers he discussed the relation of the nucleus cluster Tr 37 to the rest of the association (Markarian

1951), described the contents of the association (Mar­ karian 1952), and considered its state of motion, which he felt showed expansion (Markarian 1953), In their study of the space distribution of the blue giant stars, Morgan,

Whitford, and Code (1953) also called attention to Cepheus

0B2, which they listed as I Cephei, finding it to be a separate, large-scale clustering at a distance of about

720 pc.

Spectroscopic and Photometric observations

Morgan (Morgan, Whitford a.ncl Code 1953? Morgan, Code, and Whitford 1955) has provided the main body of two-dim­ ensional spectral classification for the stars in the region of Cepheus 0B2, His lists include about 30 stars, selected from the HD catalogue and its extension (HDE) and the finding list of Nassau and Morgan (1951),

Visual magnitudes and colors on the system were given for Morgan's stars lay Morgan, Code, and Whitford

(1955), extending the original catalogue of Stebbins,

Huffer, and :?hitford (1940), Hiltner (1956) measured the

UBV magnitudes and colors and the polarisation for about

20 of these stars, including nine of the stars on the orig­ inal list of Morgan, Whitford, and Code (1953), Four of the early-type stars in the region are standards of the UBV system (Johnson 1965). Mirzoyan (1955) measured ten stars of the association on the Barbier-Chalongo photomet­ ric system. Twenty-six of the stars on Markarian*s (1953) list were measured lay Grigorian (1957a) on his own three- color photoelectric system, which can he linearly related to the UBV system. Grigorian (1957b) also measured the polarization of 29 stars in the region.

The region of Cepheus 0B2 contains about 40 of the

571 3 stars whose spectroscopic absolute magnitudes were determined by Petrie and Lee (1966) from measurements of the equivalent widths of HY. Since Petrie included an estimate of the one-dimensional spectral type in this work, it amounts to two-dimensional classification. From the same plate material, G. A. H* Walker and s. M. Hodge

(1966) obtained the equivalent widths and half-widths of

He I W4338 and 4-471, estimated the rotational velocities from the central depths and widths of the lines, and measured the central depth of the interstellar absorption feature at \4430. Petrie and Lee (1966) gave photovisual magnitudes for their stars, and Walker and Hodge (1966) gave the color excesses in B-V,

Shakhovskoi (1956) has exhaustively treated the in­ formation in earlier catalogues. Except for the stars with MK classifications by Morgan, he had only one-dim­ ensional, objective prism classifications, mostly from the HO and HOE catalogues and the Bergedorf Spektral- Durchmus terung (Schwassmann and van Rhijn 1935). Shakhov- skoi took photoelectric color indices from Stebbins,

Kuffer, and Whitford (1940) where he could, but mostly he had to roly on photographic and photovisual magnitudes, largely from Berg and Stoynova (1937). He was only par­ tially successful in constructing a spectrum-lumino3ity diagram (also called Hertssprung-Russell, or H-R diagram), finding large dispersion in the photometric distances.

The question of expansion

Martarian (1953) was the first to investigate the motions of the stars in Cepheus 0B2. He selected stars according to their distance modulus corrected for absorp­ tion as given by Duke (1951) and coribined the proper mo­ tions from the General Catalogue (Boss 1937) with the radial velocities from Petrie and Pearce (1931). Data were available for IS stars. Markarian found that their motions could be interpreted as linear expansion at the rate of 8 lon/s? this implied an age for the association of 4.5 million years.

Artiukhina (1954) added AGK2 proper motions to the data compiled by Markarian, gaining an additional star, and confirmed the presence of expansion but stated that the stars expand from the two nuclear clusters, NGC 7160 and Tr 37. Later, Artiukhina (1956) added absolute proper motions of 44 0-B5 stars in the region of Cepheus 8

0B2 from positions given in meridian and photographic catalogues and reconfirmed expansion from two centers.

Several authors criticized the results of Markarian's and Artiukhina's investigations. Lebedinskil and Khoro- sheva (1956) showed that the expansion of Cepheus 0332, as well as several other associations, could be considered as the parallel motion of two groups of stars. In the case of Cepheus 0B2, Khorosheva (1956) found that Artiukhina's proper motions could be grouped in several ways to show expansion, lack of expansion, and even contraction. She proposed a grouping which gave five groups of stars with

a common proper motion in each group. Kopylov (1950) was

oven more critical of Artiukhina's results, particularly

since he found that the association broke doim into sep­

arate groups of stars at different distances. Kopylov

found that only one of IChorosheva*s (1956) groups consis­

ted of stars at the same distance, and concluded that the

motion of the stars in Cepheus 0B2 was far from simple.

On the other hand, Shteins and Abele (1958) attemp­

ted to refute Lebedinskii and IChorosheva (1956) and to

show that the space distribution of the stars, not consid­

ering the velocity distribution, is consistent with Am­

bartsumian's (1950) hypothesis of radial expansion from

a small prestellar body. 3y projecting Artiukhina1s

(1956) proper motions backward, they found that the max­

imum concentration occurred 2.0 million years ago. The stars at that time did not seem to occupy a much smaller volume of space than they do now, but Shteins and Abele thought that observational errors in the proper motions would account for this.

When discussing the proper motions, it must be kept in mind that errors of Ol'OOS in the annual proper motions that

Dieckvoss (1963) quotes for this zone in the Yale cata­ logue amount to 15 Itm/s at 500 pc. According to Scott

(1963), the errors for the General Catalogue (Boss 1937) are equally grreat and the errors in the FK3 are about 20 percent of this amount. It should also be noted that Van

Kerk (1959), when checking the expansion that had been found for the association Lacerta CB1, discovered that the motions for almost all the stars in this zone of the sky showed "expansion". The effect might result from this zone being in the zenith for most of the observatories contributing to the proper motion catalogues (Scott 1963).

The region of Cepheus studied here adjoins the region studied by Van Kerk.

The discussions of Artiukhina (1954, 1956), Khoro­ sheva (1956), and Kopylov (1953) also omitted to take into account the component of solar motion in this direction, which is about 12.5 km/s, directed upward and toward the galactic center at an angle of 34° to the galactic plane.

The component of galactic rotation in this direction is about -0^005 per year, or -24 Vzci/ b per kpc, which is 10 obtained from tho Oort formula

4.74 ^ B + A cos 2 1IX# using Schmidt's (1965) values of A -15 Jan/s per kpc and

B = -10 km/s per kpc.

The nuclear clusters

A general feature of OB associations is the presence of v/hat Ambartsumian (1949a) has called nuclei. These usually are open clusters whose brightest stars are of early type, often multiple o stars resembling the Trap- osium in Orion. The two clusters Tr 37, immersed in the large H II region IC 1396, and 1TGC 7160 are regarded as the nuclei of Cepheus 032 by Markarian (1952). They have bean the subject of several spectral and photometric investigations.

1TGC 7160 is a strongly condensed, 33-type cluster of fewer than 50 stars (Trumnler 1930). The principal work on I5IGC 7160 is the UBV photometry in the catalogue of gal­ actic star clusters by Hoag, Johnson, Iriarte, Mitchell,

Hallarn, and Sharpless (1960), which gives photoelectric measurements for 30 stars and photographic measurements

for an additional 99 stars. Johnson, Hoag, Iriarte, Mit­

chell, and liallam (1961) found a distance of 340 pc from

this woric. Hoag (1966) rediscussod the distance modulus

and found a distance of 870 pc. 11

Tr 37 is a rich, O-typo cluster which does not stand out much from the general field (Trumpler 1930)* It is involved In tho H II region IC 1396 which its central star,

HD 206267, ionises* IC 1396 Is well known for the "ele­ phant trunks" and dark "globules" which are prominent in it* The major work on Tr 37 is Kirillova*s (1953) investi­ gation, which employed photovisual and photographic mag­ nitudes obtained with a 20-cm Schmidt camera together with spectral types taken mostly from the HD and HDE. For 0 to

&5 stars the apparent photographic distance modulus was found to loo m-M« 11*1, corresponding to a distance of

603 pc* Dolidze and Vyasovov (1959) surveyed IC 1396 for

Ha emission stars with a 70-cm meniscus telescope and found 125 of them brighter than 16n .

Courtes (I960) measured the radial velocity of IC

1396 on four plates with a Fabry-Perot interferometer. Tho result was vr =-17,2db3.2 kra/s. For comparison, the radial velocity ©f HD 206267 is vr = -7.3 Jcm/s (Wilson 1953) and the velocity of the interstellar lines in IID 206267 is vr =s-13.3 km/s (Munch 1957).

Surveys and other observations

Surveys for emission-line stars have been made in the region of Cepheus 0B2, mostly in the lower part, by Blanco and FitzGerald (1964), Gonzalez and Gonzalez (1956), and i .organ and Bidelman (1946). References to earlier work by 12

Merrill and his associates are given by Gonzalez and Gon­

zales (1956). Host of the emission objects found have been

Be stars. A search for T Tauri stars would be desirable,

since they have been found in most of the nearby associa­

tions (Blaauw 1964), but none has been reported.

Martin (1964) applied Oilman*s (1927) method of abso­

lute magnitude determination to OB. stars in a region which

overlaps part of Cepheus 0B2.

Munch (1957) measured interstellar absorption lines

for five stars in tho association. v7hen reduced to the

local standard of rest, the interstellar lines had radial

velocities about half that of the stars, although the dif­

ferences in radial velocity between tho stars, the inter­

stellar calcium, and the interstellar neutral hydrogen

amounted to only about 3 to 5 km/s.

Radio observations

Dieter (1960) analyzed 21-cm hydrogen-line profiles

obtained by Muller and Westorhout (1957) and found a con­

centration of neutral hydrogen at the correct position of

Cepheus 0B2 and with tho same mean velocity as the stars.

If the velocity were interpreted as the velocity of galac­

tic rotation on either the Schmidt (1956) model or the

Weaver (1961) model, the distance of the hydrogen attrib­

uted to the association would be about 2.3 kpc instead of

0.7 kpc. 13

Radio continuum surveys of the Milky Way have detect­ ed IC 139G. A source in the correct position was listed as

FIB 22 in the catalogue of Brown and Hazard (1953)? the in- —26 ? tensity at 159 Mhz \*as 50 flux units (1 f.u. =10 w/m

per cycle per second), Wilson and Bolton (1960) identi­

fied their source CTB 105 with IC 1396? the flux density

at 960 Mhz was 210 f,u. and the size was 225x2°. Lynds r (1961) observed IC 1396 at 1400 Hhz with the 35-foot tele­

scope of tho National Radio Observatory, scanning in dec­

lination over a G°-square area. He found a rather weak,

extended source with a brightness distribution similar to

that of the optical emission. 'Hie flux density at 1400

Mhz was 116 f.u. Although the combination of his result

with that of Wilson and Bolton (1960) indicated a very

steep spectrum, Lynds felt that this conclusion was erron­

eous and was a result of the complex brightness distribu­

tion of the source and the galactic background to the

south. SPECTRAL CLASSIFICATION

Slit Spectroscopy

Selection of stars

In order to obtain photometric distances of suffic­ ient accuracy, MK classifications were desired for as many stars as possible that were thought to be members of the association. Stars were selected for observation with the

Yc spectrograph on the 72-inch Perlcins reflector according to the following criterias (1) stars listed as probable members of the association by Morgan, Whitford, and Code

(1953) or Markarian (1953)? (2) the brightest members of the clusters NGC 7160 and Tr 37? (3) stars within the boundaries of the association with HD types B and B1-B3 ?

(4) stars within the boundaries of the association with

HDE types B and BO. The selected stars were checked on

Schmidt objective prism plates to confirm the HD types, and the objective prism plates were also scanned for other stars of early type which might have escaped notice in the previous surveys. Magnitude limits appropriate to the

HD and HDE spectral types were established based on the apparent distance modulus V - Mv = 11 to 13 for the stars listed by Morgan, Whitford, and Code (1953). Thus, for

14 15

example, a faint BO star t*ould not be included because it

is likely to be too distant, and a bright B3 star would not be included because it is likely to be too near.

At the telescope it was found that observing time was

seriously limited because of interference between the spec­

trograph and the south pier when the telescope was pointed

toward Cepheus in the eastern sky. It also proved to be

impossible to guide the telescope when the hour angle ex­

ceeded 4*1 west because of interference between the guiding

telescope and the right ascension setting circle. Because

of these limitations insufficient time was available to

turn the spectrograph slit from east-west to other direc­

tions? consequently some double and multiple stars whose

companions fell on the slit had to be deleted. Neverthe­

less, all the stars on the list of Morgan, Whitford; and

Code (1953) and all the stars on Markarian*s (1952) list

except KD 210352 and SA1S-390 were observed.

Observations

Stars in Cepheus selected as described above and

early-type MK standards were observed during the nights of

2-12 September 1966 with the Yc spectrograph on the 72-

inch Perlcins Reflector of the Ohio State and Ohio Wesleyan

universities at the Lowell Observatory in Flagstaff, Ari­

zona. The Yc spectrograph has a Schmidt camera of 10-cm

focal length, and was used with a grating of 600 lines/mm 16 blazed in the blue in the second order to give a reciprocal dispersion of 80 l^mm. The slit width was adjusted to give

a resolution of about 2.2 A, or 28 microns on the plate.

The slit length was adjusted to give a spectrum width of

0.45 mm on the plate. Baked lla-O plates were used. The

plates were developed 12 minutes at 63°F in metolsulfite

(Morgan, Meinel, and Johnson 1954), a high-speed, fine-

grain, moderate-contrast developer.

For the brighter stars a neutral-density filter was

used to obtain a correct exposure, since screens for this

purpose were not available. The neutral-density filter

depressed the ultraviolet continuum but it permitted an

even exposure along the slit. To obtain a better calibra­

tion of the ultraviolet continuum, exposures of the bright

stars were also made lay using the slewing motion to widen

the spectra, even though the spectra were streaked because

of the telescope vibration.

Additional standard stars were found to be recxuired

besides those taken at Flagstaff. These were obtained

using the Meinel spectrograph on the 32-inch Schottland

reflector at the Perkins Observatory. The dispersion of

this instrument using a grating with 400 lines/ram blazed

for the blue in the second order is 86 H/mm. The slit

width and length were adjusted to be very close to -that used

with the Yc spectrograph. The plates and development were

the same. 17

Classification and results

A list of the MK standard stars is given in Table 1. .

Four categories of standards were useds (1) MK primary standards observed with the Yc spectrograph; (2) stars classified by Morgan on the MK system (Johnson and Morgan

1953) observed with the Yc spectrograph; (3) MK primary standards observed with the Meinel spectrograph; and (4) an

MK secondary standard taken with the Meinel spectrograph with a narrow, wide slit and developed in D-1S.

The stars were classified using direct, emulsion-to- emulsion comparison with the standards. On most of the standards, the iron comparison spectrum was only impressed on one side to make side-by-side viewing easier. The clas­ sifications were always made with reference to the primary standards, secondary standards being used to confirm the classification in the case of unusual conditions such as rapid rotation in the star in question or improper exposure of the plate.

The results of the spectral classification are listed in Table 2, along with the HD typos and the MK types as­ signed by Morgan (Morgan, Whitford, and Code 1953, and

Hiltner 1956). I am indebted to Dr. Phillip C. Keenan for aid in the classification of the M-type stars and to Dr.

Carlos Jaschok and Dr. Mercedes Jaschek for aid in the classification of HD 203095B. Classifications which are questionable for any reason arc followed by a colon and an explanation is provided in the notes.

TABLE 1

MK STANDARDS USED IN THIS WORK

Type Star Plate Notes Type Star Plate Notes

Category Is MIC primary standards— Yc spectrograms

OSf X Cep Ycl7Q9 1. B2III tp -4 Ori Ycl331 1. 1790 1033 1. 00 +40°501 1047 B2lb 9 Cep 1305 l.,2. osv 10 Lac 1311 1. B3V tj Aur 1377 1312 1373 09V 14 Cop 1033 2 a | 3 . 1873 1. G9.5Ib 19 Cep 130G 2. 1030 1. BOV v Ori 1914 4. B3Ia 55 Cyg 1065 1915 4. B5V v And 1776 5. BOV HD 207530 1770 2. 1834 1. BOV HD 20S103 1907 2. 1375 B0.5V c Per 1316 4. 1876 S. 1351 1. B5IV * Her 1339 7. 1852 1. 1SSS 4. BlIII o Per 1314 4. 1090 4. 1349 1. B5III 6 Per 1013 3. Bllb £ Per 1315 1. BGIb 13 Cep 1031 2. 1050 1. BOV a Del 1364 1. Blla * Cas 1775 B9III V Lvr 1319 1. 1731 1. A2la v Cep 1867 2. B2V 3 Sco C 1307 1063 1333 M21 a Cop 1069 1370 19

TABL3 1— Continued

Type Star Plate Notes Type Star Plate Notes

Category 2s MK secondary standards— Yc spectrograms

301b HD 20519S YC1782 2. B3V p-2 Cyg Ycl833 1906 BQV p Lib 1883 1. B0.5V p SCO A 1885 4. 1384 1. 1886 1. B9III 5-2 Cet 1777 BlV —1°935 1912 1794 1. 1913 1884 1. B2V -0°936 1336 B9la HR 1035 1910 1. B2V 8 Lac B 1810 1911 1. B3V i Her 1099 1900

Category 3s MK primary standards— Meinel spectrograms

07 S Mon M163 B2la X-2 Ori M195 09III i Ori 191 B3V n UMa 173 09. 5V a Ori 165 B3V v Ori 196 166 3311 t CMa 206 167 207 09.511 6 Ori A 190 B3la o-2 CMa 200 09.51a a Cam 132 201 BOV v Ori 183 202 B0III 1 Cara A 181 B5V ¥>-2 Aqr 175 BOIa e Ori 139 B5III t Ori 185 B0.5la k Ori 194 B5la X Aur 187 BlXb p Leo 171 B5la rj CMa 203 B2V 3 Cas 177 204 173 205 32V o Cas 130 B6V P Sex 172 B2IV y Peg 176 B6lVnn 23 Tau 210 9. B2III 12 Lac 174 B3III 27 Tau 209 B2III Y Ori 186 B8II Y CMa 203 B2II c CMa 197 B3Ib 53 Cas 179 193 B3Ia P Ori 133 199 134

Category 4 s MK secondary standard— Meinel spectrogram

B8III tt- 2 Cyg M 47 09V 10 Lac M 48 10. 20

NOTES TO TABLE 1

1. 2ria5 neutral density filter installed.

2. Probable member of Cepheus OB2 (Morgan, Whit ford, and Code 1953). 3. Double-line spectroscopic binary (Petrie 1966).

4. 2^5 neutral density filter installed? plate slightly light.

5. Slightly dark.

6. Light.

7 . S1 i ghtly dark • 0. 2^5 neutral density filter installed? plate slightly dark.

9. Secondary standard 10. Taken using narrow, long slit? developed in D-19. Used for comparison with tr-2 Cyg.

TABLE 2

RESULTS OP SPECTRAL CLASSIFICATION

Yc Spectral Type HD/BD Plate Remarks No. SCS HDWWM

1S0895 1767 BlVe B BlV Note 1., 2. 1763 Bl sVse Wide slit 19S308 1773 B2V B3 199661 1773 B3V B3 200G57 1302 B3III B2 33III Note 2. 202214 1303 30 V B2 BOV ADS 14749? note 2. 203025 1730 B2V(e) B3 B2III(o) ADS 14332? notes 2., 3. 203330 1373 31 sV + Mleplb ICO Note 4. 203374 1731 BOVnne B0p BOlVpe ADS 14363? 1304 BOVnne notes 2., 5. 204116 1325 BlVep B0 BlVe Notes 2., 6. 21

TABLE 2— Continued

Yc Spectral Type HD/BD Plate Remarks No. SCS HD WWM

204150 1771 B2V B3 Note 7. 204327 1840 BOV B BOV Note 2. 1903 BOV 205139 1326 Bill BO Bill Note 2. 205948 1977 B2V B5 206257 1797 05(f) 0e5 06 ADS 15184? 1801 06(f) notes 2 ., 0. 20G267C 1738 BOV Note 9. 1903 BOV 20S267D 1300 BOV 1909 BO sV Note 10. 206327 1772 B2V Oe5 Note 7. 20S773 1323 BlsVsnne 30p BOVspe Notes 2., 11. 1366 B1sVsnne 207017 1343 B2V B Note 12. 207193 1327 09.511(oe) B2 0911(111) Notes 2., 13. 207303 1844 31 Vn B2 B0.5V Note 7. 209751 1773 B2V B8 Note 7. 203095A 1345 BGV B2 ADS 15405 203095B 1346 AOp Si-Sr star? note 14. 203106 1351 B3V B2 203135A 1362 B2V B2 ADS 15417 2031G5B 1363 B3V 203213 1329 B1III-II Bl 31111s NGC 7160-1? notes 2., 15. 203266 1392 BlV B2 200392 1330 BlVn B3 BlIVs EM Cep ? NGC 7160-2? notes 2., 16. 203440 1341 BlV NGC 7160-3 203761 1393 B3V B2 203316 1371 B2?pe + Map W Cep? note 1372 M2epla 17. 203905 1303 BlV “ B3 BlVp? Note 2. 209339 1332 BOIV BO BOIV BS Cats binaryi note 2. 209454 1774 E2V B3 Note 7. 209744 1307 BlV B5 BlV ADS 15601? note 2. 239531 1901 B2V B 239613 1822 B2Ve BO Note 7., 13. 239626 1396 BOV BO Note 7. 239671 1902 B2V BO 22

TABLE 2— Continued

YC Spectral Type HD/BD Plate Remarks NO. SCS HO WWM

239710 1733 B3V B2 239712 1324 B2Vnne B2 Notes 7., 19. 239724 1734 B1III B2 Note 20. 239725 1736 B2V B8 239727 1796 A2Ia 35 Note 21. 239729 1737 BOV B3 239743 1394 B2V B 239753 1823 B2Vn(e) B0 B2IIIsnn Notes 7., 22, 239767 1904 B0.5V B B0.5pV s AI Cep, eclips­ ing binary. +61°2213 1342 B3V + B5V NGC 7160-4? note 23. 1393 B3V + B5 Note 24. 1905 B3V + B5V Note 25. +61°2214 1053 B3V NGC 7160-6. +61°2215 1059 B3V NGC 7160-5. +G1°2218 1357 B3sV NGC 7.160-7? slightly out of focus. 1897 B3V Note 26. 1 NOTES TO TABLE 2

1. H{3 has fairly broad emission on wide, weak absorp­ tion? Hy alasorption line appears weak (filled in)? H6 is slightly weak. N.b.s neither Morgan (Morgan, Whitford, and Code 1953) nor Potrie (Petrie and Lee 1966) mention emission, although the star is listed as B2e in Merrill and Burwell (1933).

2. ProbaTole member of Copheus 0B2 (Morgan, Whitford, and Code 1953).

3. Hp is weak (slightly filled in) with possible weak, sharp emission in the center? Hy is slightly weak. Spectroscopic binary with range 123 Ion/s (Adams, Joy, and Sanford 1924).

4. Spectral typo of the B star was estimated from the appearance of the H linos. The other criteria were affected by the M star* The spectral type of the M star was Teased on comparison with m- Cephei (M2Ia). The TiO bands wore not quite so strong, implying slightly earlier type. The luminosity was estimated from ratios among- 23

NOTES TO TABLE 2— Continued

Pe XX437S, 4383, and 4389. Emission appears at about X4240. See Note 1., Table 10, regarding confirmation of the type of the B star from U3V photometry.

5. Absorption lines are very broad. Sharp emission lines are superposed on the H absorption lines s strong at H(3; moderate at Hy, weak at H6, H«, and HO? very weak at HS. Emission is also suspected at about \4600.

S. Hp has broad, very weal: absorption (filled in) with trace of central eraisoion? Ey is broad, slightly weak, with possible emission displaced toward tlie red. Although the other lines indicate type BlV, Si X4129 is enhanced, appearing more as in types 33V-B5V.

7. Probable member of Cepheus 0B2 (Markarian 1953).

8. Absorption lines are fairly broad. Slight emis­ sion appears at the red edge of He II X4636 (more marked on Yc 1797), and also at about XX4550 and 4630, Spectro­ scopic binary of period 1*36 days

9. Lines are fairly broad.

10. Although the general appearance indicates BOV, on plate Yc 1909 some BlV characteristics are seen.

11. Absorption linos are extremely broad and diffuse. Emission lines appear superimposed on the H absorption linoss Hp strong, broad, and double, with violet com­ ponent stronger? Hy double, both components of equal strength? H6 and He very weak, narrox*, single.

12. Broad lines.

13. Classified 09III by Johnson (1965). The spectral type was based on the ratios He I X4471/He II X4541 and He II 14200/He I X4337, which appear to be the same as in 6 Ori A (09.511) and 19 Cep (09.51b), Peculiar emission appears at about X4960.

14. Si-Sr stars Si II X4129 is stronger than Ca II K, Si XX3056, 3853 and Sr X4077 arc present, Mg II X4431 is very weak, Fe X4233 is present. The H lines are only mod­ erately strong and resemble those in class III.

15. Luminosity class II assigned from ratios He I X4337/0 II XX441S, 4565, 4652, and 4656, but the ratio N II X3995/Hc I X4009 indicates class III. 24

NOTES TO TABLE 2— Continued

IS. Eclipsing binary of 20h period (Lynds 1959); W UMa system.

17. All K lines are seen in emission with a narrow absorption core characteristic of a shell. As a result, the emission lines appear double, with a stronger violet component. The absorption features arc all blended with the M star, but no Si IV X4089 is seen, indicating a type later than BO, and other lines indicate a type earlier than B5. The M star resembles t* Cep. Strong emission occurs at about XX4220-4230.

18. The absorption linos are moderately broad. The H lines appear in emissions H0 has narrow, strong emis­ sion on absorption core; Hy has narrow, moderately strong emission; H« , I-IO, and K9 show very weak emission. Other weak emission occurs at XX4010, 3975, 4305, 4550, and 4590.

19. The absorption lines are very broad. Emission lines occur at Hp, weak, narrow; Hy, very weak, narrow; H6, trace,

20. Appears to be slightly brighter than o Per (Bl III) with respect to Si III XX4552, 4565, and 4650.

21. Resembles v Cep almost exactly, except that Ca II H and K are very slightly stronger.

22. Absorption lines are broad. Hp is weak (par­ tially filled in) with trace of emission in the center. Hy is asymmetrical with slight amission displaced toward tho red appearing in the core. TThile the ratio He I X4121/X4144may indicate class III, there is no trace of Si ill X4552; the H lines are not useful as luminosity criteria because of omission.

23. Lines of the two stars are not completely sep­ arated. The relative velocity is about 235 Icm/s, jwith tho B3V star approaching.

24. Relative velocity close to 0.

25. Lines of the twp stars are well separated. The relative velocity is about 210 km/s, with the B3V star approaching. 26. Sharp lines. The Ho lines appear weak. The star appears excessively blue in the aolor-magnitude diagram of NGC 7160 (Hoag et al 1961), 25

Objective Prism Spectroscopy

Observations Objective prism plates were taken with the 40/S0-cm f/2.7 Schottland Schmidt telescope at the Perkins Observa­ tory. The telescope is equipped with a 4° objective prism of ultraviolet-transmitting glass giving a dispersion of approximately 1000 &/mm at Hy. The short-wavelength trans­ mission cutoff occurs at about 3400 &. A spectrum-widen­ ing mechanism is installed that advances the plateholder in increments of 5 microns at regular intervals that can be varied from 0.5 sec to 5 min.

For these observations the telescope was modified to take glass plates instead of the original films. The use of glass plates was felt to have several advantages, such as convenience in processing, handling, and storage. How­ ever, because of the short focal length of 110 cm, which is also the radius of curvature of the focal surface, it was impossible to make the plates conform exactly to the focal surface when held by the edges. About half of the

5-inch square area was in satisfactory focus for spectra.

The deviations, however, were too extreme to permit photo­ graphic photometry with the Schmidt telescope.

Because of the probability of breakage, which averaged about ten percent with plates of 0.040-inch thickness and about one percent with plates of 0.030-inch thickness, a 26 protective cover glass was placed just in front of the . plate to prevent damage to the mirror. Tho cover glass was made by removing the emulsion from a thin photographic plate. It was found to have negligible effect on either tho image quality or the transmittance.

Because of tho restricted sise of the region of good

focus, five plates were required to achieve satisfactory

coverage of the entire Cepheus 0B2 association. Exposures

of 1 minute, 5 minutes, and 30 minutes were made with the

spectra widened 0.25 mm. An additional set of plates was

exposed for 30 minutes with tho spectra widened only 0.1 mra. The plates were developed 12 minutes at 70°F in metol-

sulfitc. A list of the plates used for classification in

Cepheus is given in Table 3.

Classification criteria

For tho purposes of calibrating the classification, observations were made of standard stars of the MK system.

The brighter standards could not obtained with tho

Schmidt telescope because it was found to bo impossible

to obtain satisfactory exposures of less than 5 seconds.

This imposed a magnitude limit of a7x>ut 3 = 3. The alter­

natives of stopping down the telescope aperture or using

neutral-density filters wore rejected on the ground that

thmeasures would change the appearance of the spectra.

Who primes.; MK standards were unobtainable, fainter stars 27

TABLE 3

SCHMIDT PLATES USED FOR SPECTRAL CLASSIFICATION

Date Plate Center No. Ercp. Seeing Remarks (1966) (1900)

46 12 Oct 21h16m + 6191 30^ 2 Good definition. 47 12 Oct 21 50 61.1 30 3 Small region of good definition. 49 12 Oct 21 17 57,1 30 3 Good definition. 51 7 Nov 22 01 53.2 30 3 Good definition. 52 7 NOV 22 02 60.7 25 3 One side of each spectrum blurred by clouds. 53 13 Nov 20 59 55.2 30 Jo 54 13 Nov 21 09 53.5 30 3 57 14 Nov 21 40 57.2 30 2 53 14 Nov 21 40 57.2 30 2-3 0.1 mm widening. 59 14 Nov 21 54 62.0 30 2 0.1 mm widening. GO ld- Nov 21 16 61.1 30 2-1 0.1 mm widening. 61 14 Nov 20 59 55.2 30 1 0.1 mm widening. 62 14 Nov 22 01 53.2 30 1 0.1 mm widening. 54 16 Nov 21 16 57.1 30 0-1 0.1 ran widening; fair. 32 16 Dec 21 16 51.7 5/1 1-2 Good definition. 03 15 Dec 21 41 56.3 5/1 1-2 16 Dec 21 54 61.3 5/1 1-2 35 16 Dec 21 16 56.3 5/1 1-2 — - 36 IS Dec 20 59 54.3 5/1 1-2 37 16 Dec 20 01 50.2 5/1 1-2 that hacl been classifiGcl by Morgan on the MK system were substituted. The primary ancl secondary standards are listed in Table 4.

Inspection of tho spectra of the MIC standards revealed the following temperature and luminosity criteria which could be seen in the objective prism plates for the stars of lower luminosity* 23

TABLE 4

MK STANDARDS OBSERVED WITH T‘IE SCHMIDT TELESCOPE

Type Star Plato Notes Type Star i'late Notes

Category Is MK standards ol^sorved with Schmidt telescope

06 HD 46223 65 B2Ia HD 14143 33 05 HD 45150 66 B3Ia HD 14134 39 06 IiD 40099 66 B5III 6 Por 34 03V HD 47123 66 B5Ia 13267 09 OOVn KD 45056 66 B6V IS Tau OS 03 +40°501 65 BGIII 17 Tau 39 00.5 KD 46149 66 B6Ia HD 15497 39 03 V HD 46202 66 B7IV 16 Tau 53 HD 46366 ■ 56 B7III 20 Tau OS 09.5 V a ori 96 1. tj Tau 39 09.511 6 cri 36 1. B3V 13 Tau 63 09.51b IS Cep 34 1. 21 Tau 63 BOV x> Ori 33 B3III 27 Tau 03 HD 46101 66 B3Ib 13 Tau 33 BOIa € Ori 92 1. BOIa HD 14542 39 30.5 V NGC2244-3 66 B9V HR 1133 33 B2Ib HD 13341 39 HD 133S6 39 9 Cap

Category 2s MK secondary standards

BOIV HD 47417 66 2. B2IV 22 Ori 35 3. BOIII HD 47032 66 2. v j Ori 92 3. HD 47302 66 2. B3V 29 Per 34 3. B0.5V HD 47360 66 2. HR 1032 94 3. o HD 47367 66 2. B3III w Ori 92 O • LlV HD 46434 66 2. B5V 31 Per 94 ^ • o 23 Ori 95 3. 34 Per 94 • 25 Ori 95 3. B5IV 32 Ori 91 3. J-'.LIb HD 47240 66 2. B5III 6 Per 94 3. 29

NOTES TO TABLE 4

1. Ovorertposcd.

2. Soectral typos from Morgan, Code, and Whitford (2.955).

3. Spectral t\r^es hy Morgan in Slettebak and Howard (1955).

Typo C.— G stars show extremely weak hydrogen linos,

H6, K «, and H3 being strongest. Ho \\4541 and 4471 are sometimes faintly soen in tho earlier types. Pour lines also appear at about the position of the Balmcr lirait. In the region of NGC 2244, stars of class 04, 05, and 06 have definitely weaker H lines than those of class 03Vn, 03.5,

03V, and 09V. Thus two groups of ecurlv and late o-type stars can be distinguished. The later 0-typo stars have weaker lines than BOV.

Type BO.— BOV stars have very weak K lines compared with BlV, although they are stronger than in 08V-09V. The

Balmer jump is only very slightly apparent. He X402S is very weak. In certain cases, such as in the members of

NGC 2244, the Ca II K lines can be seen and He is stronger than the other H lines. This docs not seem to be so in

Orion. BOIII stars (e.g., HD 473032) have weaker H lines than BOV and look like the late 0 types. BOIV stars (e.g.,

HD 47417) look like BOV.

Type Bl.— The Balr.ior jump is very slight but apparent in BlV and tho strength of the H lines is intermediate 30 between those in BO and B2. He X4026 is about half as strong as H6 or H«, Type B2.— The H lines are slightly stronger than in Bl, and tho Balmer jump is more noticeable. The ultraviolet continuum is stronger than in B3. Ho \4026 is at maximum strength relative to tho H lines. B2III (42 Ori) is not significantly different from B2V.

Typo B 3 . ~ In B3V stars Ho X4026 is well-defined, al­ though it is slightly woo]'or relative to the I-I linos than in B2. Ho \4144 is slightly visible, \4471 is apparent.

The Balmer jump is less than at B5V, but stronger than at

B2. B3IIIe (« Ori) lacks the strengthening of the ultra­ violet continuum seen in later class III stars although tho

Balmer discontinuity loo3:s weaker than class V. It has very weak H linos with no HP and weal; Hy. Typo B5.— In class B5V, the Balmer gradient is steeper

tha.ii s.t B3 but more gradual than at 36. He XX4471 and 4026 can lie made out more clearly than in B6V. The strengthening

of the Balmer continuum is apparent s.t B5III (6 Per) and the

K lines arc weal:. Tho 35o star p Per can be distinguished

by the absence of HP and tho weakness of Hy relative to the higher members of the Balmer series.

Typo B6.— At BS, Ho XX4471 and 4026 can lie seen faintly.

Tho amount of tho Balraer jump is less than at BG but it can­

not be easily distinguished from 37. The B6III stars can be 31 separated from the B6V by the strengthening of the Balmer continuum, Typo 37.— The B7III stars have a somewhat steeper

Balmer gradient than BOIII (e.g., comparing i) Tau and 20 Tau with 27 Tau, although *1 Tau seems to have more of a Balmer

jump than 20 Tau).

Ty?x) BO.— BGV stars have noticeably weaker H lines than

AOV and no other linos arc visible except possibly in pecu­

liar stars. Glass III shows the Balmer continuum, lout this

can also be seen occasionally in class V, although to a

lesser extent (e.g., comparing 27 Tau, BOIII, with HR 1172,

BOV, in tho Pleiades). In the a Per cluster, the BOIII

stars have slightly weaker lines than BOIV. Under the best

conditions, the MK criterion that Ca II K=Si \4128 can be

employed.

Typo BS«— The H linos are not quite so strong as in AO,

but stronger than in BOV. Ca II K may occasionally be vis­

ible, as in HR 1103 in the Pleiades.

Typo AO.— AO stars have very strong' lines, and

Ca II K is marginally visible. Class III shows the typical

strengthening of the Balmer continuum.

Later A types.— Although standards wore not taken spe­

cifically, comparison among standard stars which appear on

plates taken for other purposes suggests that it should be

possible to distinguish several A-typo subgroups along the main sequence lay the relative strength of Ca II K and tho 32

H linos together with tho strength of the Balmer gradient.

However* ono may he misled by peculiarities (Bidolman 1966).

A small number of standard stars of high luminosity

were observed. The following temperature and luminosity

criteria were apparent in their spectras

Tyoo OS.511.— (6 Ori (overexposed)) The blends at

HY* K6* He \4026, He, HG, and possibly Ca II K are very

woalc but visible. Typo BOIa.--(Based on € Ori, overexposed) The blend

at H6 is the only lino visible.

Type 30.51b.— The blend at H6 is fairly strong, tho

blond at HY is very weak, and those are the only lines

visible.

Type Bllb.— (HD 47240) There are no H linos except

for weaIz suggestions of tho blends at H6 and HY. The typo

is not easily distinguished from early 0.

Type B2Ib.— (9 Cep and 10 Per) No lines are visible

except faint blend near H6. There is a slight suggestion

of the Balmer discontinuity. Type B5Ia.— (5 Per) The Balmer jump is evident and I-I

lines are faintly visible.

Types 301b.— (13 Cep) The Balmer jump is somewhat

more pronounced than at B5la. He, H8, and H9 are the only

visible lines.

Tyne AQIb.— (13 Mon) The Balmer jump is fairly strong-

and the I-I linos are evident. 33

Typo A2Ib»— (9 Por) TIio Balmer jump is pronounced.

He, Ca II K, and H3 are clearly visible.

Type A2Ia.— (v Cop) 'The general appearance is like

A2Ib with a broad, faint feature at H6.

In order to see how well tho classification could actually be carried out, no MK standards or other stars with MK types in the region of Cepheus 0B2 except 13 Cop and v cep were included among tho stars regarded as Schmidt standards. After tho entire classification was complete, these stars were identified and the Schmidt classifications were compared with the MK types. The results are given in

Table 5. The source of the MIC classification in Table 5

is indicated by S for Simonson (the present work), K for

Keenan, M for Morgan, and MK for MIC standard. The star

number refers to Table 13, and the number of Schmidt

classifications is given in the column labelled "n".

Tlie nomenclature for tho Schmidt classification is

related to the MIC system. Since luminosity criteria wore

observable, it was felt desirable to use a system of desig­

nating the luminosity classes which would resemble the MK

designation, but since all the MIC classes could not be dis­

tinguished, an identical system was avoided. Tie MK

classes la, lb, and II were designated i, class III was

designated iii, and classes IV and V were designated v.

Tie spectral, typos remain the same, although 10 subtypes

were not always assigned. In particular, B4 is absent. TABLE 5

COMPARISON OF SCHMIDT AND MK CLASSIFICATION

HD/BDMK Source Schmidt n Notes

199300 B2V S Blv 3 199661 B3V S B3v 3 202214 BOV S,M BOv 3 203333 BlV+MlepIl: s ,k Comp B+M 3 203374 BOVnne s CB 2 204116 BlVep S BOvs 4 Out of focus or overexpos ed. 204150 B2V s BOv o 204027 BOV S,M OB 6 Strong H6. 205139 Bill S,M OBs 3 Overexposed. 205196 BOlb MK 30i 5 Absorption at H6 and ^4650. 205940 B2V s Blv 4 206165 B2I b MK OBs 2 Overexpos od. 206103 BOV MK BOvs 2 Slightly out of focus. 2062.67 06f+2BOV S Mult 0 3 206327 B2V s Blv 3 205773 Bl sVsniio s OB 4 207017 32 V s Blv 5 207190 09.511 s OB 4 207260 A2Ia MK Ai 3 Overexposed. 207300 BlVn s 03 4 207530 BOV MIC OBs 6 Out of focus or overexposed. 207951 B2V s Blv 3 200095 BOV+AOp s B5vs 2 Overexposed. 200106 B3V s Blv 3 200105 B2V+B3V s BOv 3 200218 B1III-XI s BOiii 3 200392 BlVn s BOs 1 Overexposed. 200440 BlV s Blv 1 200761 B3V s B3v 3 203016 B2?+M2Ia s Comp 2 W Cep. 203905 BlV s BOv 4 209339 BOIV S,M BOv 2 209454 09V MK BOv 2 209744 BlV 3,14 BOv 5 Wealc, sharp II lines. 209975 09.51b MIC OB 2 Very faint, high- order I-I lines. 210339 OGf MIC OBs 2 Overexposed. 209145 BlV M BOv 6 35

TABLE 5— Continued

HD/BD MK Source Schmidt n Notes

209296 B1V M BOv 2 Out of focus or overexposed. 210473 B1V M OB 3 211330 B0.5V M CD 1 Double. 211371 A2lb M 7ii 5 239531 B2V S B2vs 3 Confused. 239610 B2Vo S B2(e) 3 239626 BOV s BOv 6 239671 B2V s Blv 4 239710 B3V s B2v 5 233712 B2Vnne s Blv ,1 239724 BlIII s 09V 4 233725 B2V s Blv 5 239727 A2la s Ai 4 239729 BOV s BOv O 239743 B2V s B2v 6 233758 B2Vn(e) s BOv 5 239757 B0.5V S,M OB 5 239023 B5Ia M OB 5 239336 B9Iab M Ai 3 +54°2623 B1IV M OB 1 +54°2623 Bill M OB 1 +54°267S Blsnne(V) M OB 1 Faint. +5602626 Bo.5III M BOvs 1 Faint. +57°2465 B0.5n(V) M CB 2 +60O2300 B2III M BOv A +5102213 B3V+B5V S B3v 2 +610 2214 B3V s B3v 1 +6102215 B3V b?f t B2v 2 +6102213 B3V s B2v 2 An BlIII M OB o

The results of the Schmidt classification and the

MIC classification are compared graphically in Figure 1 for luminosity classes IV and V. If the two classifica­ tions gave the same types, the points would all fall along the diagonal. Many points are below the diagonal, indicat­ ing that errors in the Schmidt classification tend to 36

B3 ooo

32 oo oo

Bl oo 888

SCHMIDT TYPE

BO 080 ooo

09

03 OOO BO 0.5 1OS 2 3 me TYPE

FIGURE 1

COMPARISON OF MIC AND SCHMIDT CLASSIFICATION FOR LUMINOSITY CLASSES V AND IV result in the assignment of earlier types. It is easy to understand why this should he so. The visibility of the

lines and the Balmer break, which are the only spectral features available for classification, is marginal at host. Any deterioration in the quality of the image caused by, for example, poor seeing or improper focus, tends to obscure these features. Tlie spectrum then appears more

lilce that of a star of earlier type, that is, with weaker 37 lines and less evident Balmer break. The same result may occur if the star has an unusual spectrum. In many cases, emission lines or rapid axial rotation cause tho star to be given an earlier type or to be put in the OB category as having a featureless spectrum.

From the comparison with the standard stars, an esti­ mate can be made of the "natural groups" of the Schottland

Schmidt telescope. Natural groups as described by Morgan

(1S51) include spectral types which cannot loe distinguished from each other on spectrograms of given quality.

Tlie natural groups of tho Schottland Schmidt tele­ scope are not as large as one might expect from the dis­ persion because of the extent of the transmission into the ultraviolet, which allows more features to be taken into account. This is a particular advantage in the early- type stars, which have such featureless spectra in compari­ son with the later types. In particular, there is no con­ fusion between early F-tvpe stars and middle B-type stars which have almost the same hydrogen line strength and almost the same gradient in the blue region. The strength of the ultraviolet continuum and the strength of the Ca II

N line afford easy distinction.

Important things to consider in judging the qual­ ity of the spectra on which to base the natural groups

Include tho dispersion of the spectrograph, the optical quality of the telescope, the characteristics of the 38 emulsion and the development process, and the seeing con­ ditions, The optical quality of the Schottland Schmidt telescope is considered excellent. The optics were refig­ ured in 1961 for hluo light, and v/hen properly collimated the image size is smaller than tho diffusion length in tho emulsion. There is some dependence of the focal length on wavelength, although the effect is small. Of greater concern is the deviation of the glass plates from the focal surface. This can be compensated b y talcing exposures at different focus setting or by talcing overlapping plates,

Tho first method was used in talcing standard stars? the second method was used with less success for the Cepheus

032 plates.

Tlie seeing was of importance only when it was very bad. There was no distinction between good and average seeing for exposures longer than about 30 seconds, and very little for exposures longer than 10 seconds. 'Hie seeing was judged lay the extent to which the image wandered in tho S-inch guide telescope. This subjective judgment could be soon and studied more objectively on exposures of bright stars when the telescope was moved very fast.

The spectral lines became irregular and the spectrum was streaked because of the rapid variations in refraction.

The plates in every case wore developed in metolsul- fite, which gave a significant improvement over D-19. Not only was the graininess much less with metolsulfite, but 39 tho increased latitude meant that a wider range of magni­ tudes could he satisfactorily e:cposed in a given exposure length, and in addition the emulsion was 25 percent faster.

It might he expected that the wide latitude of metolsulfite would result in some loss of visibility in the spectral

features because of lack of contrast, but the fine grain

apparently offsets this by making detail visible on a

smaller scale. For plates in good focus but otherwise of average

quality, the natural groups of the Schottland Schmidt

telescope are as displayed in Figure 2, The most luminous

------1------'*■ t .... . I I 1 1 mm 1 L J II 1 Lumi­ 1 1 OB nosity l III 1 I Class 1 1 1 i IV 1 1 I 1 1 1 1 1 l V 1 1 1 i i i i _ i 1 t i i 04 5 6 7 0 9 BO 1 2 3 5 6 7 0 9 AO 1 2 Spectral Type

FIGURE 2

NATURAL GROUPS OF THE SCHOTTLAND SCHMIDT TELESCOPE stars fall into the natural group of OB stars. As dis­ cussed above, this classification will also be applied to a few stars of later type or lower luminosity whose spec­ tral features are obliterated by rapid axial rotation,

omission, or unresolved duplicity. In some cases, it may be possible to separate subgroups from the OB classifica­

tion. For example, the early 0-tvpe stars of MK types

04-07 may sometimes be distinguished toy He \4451, and the

BOIa and Ito stars have strong- blends of H6 and HY with lines

of OIII, Ni III, and Si III.

Among the later typos it seems ’possible to distin­

guish three luminosity classes. 'Flic stars of highest lu­

minosity have an almost featureless spectrum except for a

very sharp Balmer discontinuity. The stars of MK lumino­

sity class III have a steeper gradient at the Balmer limit

than classes IV and V and the other linos are somewhat

weaker. The pise of the Balmer discontinuity distin­

guishes them from stars of earlier type. The temperature characteristics in the B typo stars

are mainly the amount of the Balmer toreal- and the strength

of the hydrogen and helium lines. It is difficult to dis­

tinguish a BlV star from a B2V star, but those seem quite

different from BOV on the ono hand and B3V on the other.

Similarly, it is difficult to distinguish B3V stars from

B5 stars but easy to distinguish those from BOV. The dif­

ference between BGV and B7V is hard to establish. Hie 41 types B8V, BSV, and AOV arc differentiated mainly by the relative strengths of the H lines and possibly by the com­ parison of Si X4123 with Ca II K, although this may loo in­ validated 7y y interstellar Ca II.

Results

Hie Schmidt plates were surveyed for all stars of typo BC and earlier, and all OB and A-typo supergiants.

The results of the spectral classification of the Schmidt plates are presentod in Tables 11 and 13, Chapter IV, along with the photographic photometry results. III. PHOTOMETRIC OBSERVATIONS

Photoelectric UBV Photometry

Observations

UBV observations were made vrith the Lowell Observatory

21-inch Cassograin reflector on the nights of 14-18 Septem­ ber 19SS. The U, B, and V filters were, respectively, 2rnm

Corning 9363, 5 rara Corning 5030 + 2 mm Schott GG13, and 3.6 mm

Corning 3334. An unrefrigernted EMI 6256S photomultiplier was used, operated at 1500 v. According to Jorzvkiewics and Serkowski (1966, "... the ... tube has a rod cutoff similar to that of the tube with which Johnson defined the

UBV system ([Johnson and Morgan, 19533)." The signal was amplified by a General Radio typo 1230-A DC amplifier and

integrated for 10 seconds on the Lowell Observatory inte­

grating photometer. The diaphragm diameter was 24" of arc except during a few brief periods when the size was in­ creased to 33" on account of excessive telescope vibration

in the wind.

The output from the integrating photometer consists of a punched paper tape and a printed tape on which it was

possible to write remarks at the time of observation. The

data in the paper tape were punched onto cards using the

42 1G20 data processing system. These data were then edited malting use of the remarks on the printed tape.

For each star, the sequence of observations was V, B,

U for the star? dark current? U, B, V for sky background?

darlc current? radium if the gain was low enough? V, B, U

for the star. In the case of standard stars, each obser­

vation in the sequence was made twice. The gain was kept

the some for all observations on each star, and the inte­

gration interval was kept at 10 seconds. In order to re­

duce the statistical fluctuations an integration count of

at least 10^ was required for all star readings. If this

was not achieved in 10 seconds, the observation was re­

peated instead of lengthening the integration time.

The photometer output contained the following informa­

tions time of observation in seconds from an arbitrary or­

igin? the star identification? the integration time? a num­

ber identifying the kind of observation, such as star B,

sky B, etc.? the gain setting? and the intensity integral.

In addition to the photometer data, a card was included

giving the coordinates of the star and the UBV values if

the star wore a standard. The precession was calculated

to obtain the coordinates of the star at the epoch of ob­

servation and from this and the time of observation the

moan air mass was computed, using the approximation formula

given by Hardie (1S62), p. 130, equations 2a and 2b. 44

The reduction of the observations for a single star in a single color proceeded according to the following equations

m ss -2.5 log10[l(star) - I (shy)] + gain, where ra is the magnitude on the instrumental system,

I(star) and I(sky) are the means of the integrals of the star and sky observations respectively.

The value for tho gain was taken from the calibration of Jersykiewicz and Serkowski (1966). A check was made of their calibration, using the radium source for the smaller values of the gain and tying it in with the larger values by observing a faint star at the zenith. Insufficient ob­ servations wore made to constitute a satisfactory calibra­ tion by themselves, but application of the Student t-test as a test for consistency of the chock observations with tho published calibration gave a probability of loss than

1 percent for inconsistency.

Tho following standard stars were observed: UBV pri­ mary standards 10 Lac, HR 3832, tj CrB, t Her, a Ari, and

HR 075? X Cep, 9 Cep, and BS 3327 from tho list of Johnson

(1065)? v And from the list of Johnson and Harris (1954)? and 3 Cyg A and B from the list of Johnson and Morgan

(1953).

Determination pf the extinction coefficients and tho instrumental corrections was accomplished entirely from the observations of the standard stars for each night 45 separately. The procedure followed that given by Hardie

(1962), except that all quantities were solved simulta­ neously. The equations were the followings (U-B) = F(U-B)»(u-b)-[l-E2(U-B)«x]

- F(U-B)-Ei(U-B)-X +Z(U-B) (la)

(B-V) = F(B-V)*(b-v)*[l-E2(B-V)-X] -F(B-V)*Ex(3-V)-X + Z(B-V) (lb)

V = v - E 0 ‘X. + F(V)« (3-V) +Z(V) , (lc) where the capital U, B, and V refer to the standard system

and the lower case u, b, and v refer to the instrumental

system? F is the instrumental correction factor? Eq , E^,

and E2 are respectively the primary, first-order, and

second-order extinction coefficients? X is the air mass?

and Z is the zero-point instrumental correction.

The solution of the color equations for the instrumen­

tal corrections and the extinction coefficients was done in

two steps, as recommended by Hardie (1962) and Serkowski

(1961). First, values for the instrumental factors were

assumeds F(U-B) = F(B-V) = 1.00 and Z(U-B) * Z(B-V) = 0,

Then the equations were solved for E^ and E2 according to

the principle of least squares as follows s

N N N E X + Z C1 e2 88 L [

N v N E ci E2 * L Ci£(c± -C i/F+Z/F)/X±'] , lr £ a C l | E l + 1=1 I 1=1 (2b) where are the individual color observations on the in­ strumental system, are the standard colors, and N is the total number of observations. The values for E^ and E2 from the above equation were used in the following set of equations to determine F and

Zs N NZ + i N ' - £ ! Cl (3a)

(1 ^ 1 2 + ( i a i 2 lp = i t " 1 " 1 ' (3b) where A^ = c-^ (1 - E2X ^ ) - EiXi •

The calculated values of F and Z were again substi­

tuted in equations (2a) and (2b) to obtain new values for

E2 and Ei* The iteration x^as continued until the differ­

ence between successive iterations was less than the esti­

mated root mean square (rms) error in the solutions. As

it turned out, the iteration condition was satisfied on

the first iteration. The estimated errors in the color equations were cal­

culated by the following formulas based on the principle

of least squaress

1) rms error in the solutions

k Erms 47

2) errors in the coefficients s

E(Z> = [ j ^ * i 2/D ] * Ban,

B(F) = [ f ^/D]^Brins .

Where D is the determinant

N N ° = * & * 1 " (i?!Ai) *

The solution for the coefficients in equation (lc) for V was obtained by the straightforward application of the principle of least squares. It will facilitate the discussion if the system of equations is presented in ma­ trix forms

Ca](p) = IV} where £ a ] is the matrix of coefficients of the equations

N N - E x± f (B-V)i 1=1 1:1

N N N C a ] = " i=lI * i i=l 1=1

N N L (B-V)i £ Xi (B-V)i J ^ B - V ) , 2 i=l JL —*J,

3 is the column matrix of the desired quantities z(v)

E0 {*} - F(V) 48 and ( y ) is the column matrix

2 (V-V)± i=l N r Xitv-vji I*} =

N

The solution was performed by Cramer*s rules

„ _ iSsJ Pic - | a f where ja^J is the determinant of the array formed by re~ placing the Jcth column of £ a 3 by ^ Y } ? and | a| is the de­ terminant of £ a 3• The estimated rms error in the solution was calculated from the formulas

= [< I E (V-Vli2 - r i—1 3c=l The errors in the coefficients were estimated by the for­ mulas

E(&jc) = [Cw ,/|al3^ Erms • where Cj,j, is the cofactor of ajcjc in the array C a 3» The coefficients and their estimated errors for the four nights of observations are given in Table 6. 49

TABLE 6

EXTINCTION AND INSTRUMENTAL CORRECTIONS FOR PHOTOELECTRIC PHOTOMETRY

Part A. Extinction Coefficients

Sept £ 0 (V) e 2 (b -v ) e 2 (b -v ) EX (U-B) e 2 (u -b )

14 .1291.055 .1371.003 -.1211.005 .0621.011 .0631.016

16 .0901.021 .1751.007 -.1231.010 .1271.013 .0601.015

17 .1361.016 .1531.005 -.1261.007 .1311.010 .0641.010

13 .1231.019 .1551.005 —.1221.006 .1241.012 .0701.012

Part B. Instrumental Correction Factors

Sept F(V) F(B-V)F(U-B)

14 .0191.011 1.00031.0045 1.0001.020

16 .0121.013 0.99421.0119 1.0121.021

17 -.0051.010 0.99711.0072 1.0081.014

13 -.0021.011 0.99931.0072 1.0061.017

Part C • Zero Corrections ..

Sept Z(V) Z(B-V) Z(U-B)

14 .0961.062 .00011.0029 -.0031.014

16 .0601.032 .00201.0035 -.0141.017

17 .1461.024 .00161.0055 -.0081.012

18 .1151.028 -.00101.0055 -.0091.015 50

The propagation of errors in the final magnitudes and colors was calculated by the principle of least squares un­ der the assumption that the errors were all small and inde­ pendent, The equation giving the propagation of errors in a function f of J independent variables x j is s

8f \ 2 o S.C = 32C (4) j=l 8x. j where Sf is the standard deviation in the measured function and the sx^ are the standard deviations in the independent variables. The standard deviations in the coefficients have been discussed above. The standard deviations in the measured quantities were all estimated according to the formula

n -*2 sx - rsi (n-1) where x is the mean of the n measurements. The measured quantities were the intensity integral for the sky and star observations and the air mass.

The errors in the instrumental magnitudes were esti­ mated according to equation (4)s

2,5 logjQe m = (sstar + ssky ) + sgain > 1 s tarӣ sky)_ where sgain is the standard deviation of the gain, estimated

at 0,002 from the data of Jerzykiewicz and Serkowski (195S). 51

The errors in the colors were estimated from the equation

(4) as

s (m1-m2 ) 88 + sm2^ , v/here m^ and m2 are the magnitudes involved.

All the estimated errors in the measured quantities

and the coefficients were combined according to equation

(4), in which the function f was taken to represent equa­

tions (1).

Results

The results of the photoelectric photometry are given

in Table 7, together with a summary of the spectral classi­

fication. Where available, photoelectric UBV observations

by other observers, mostly by Hiltner (1956), are included

for comparison.

As a check of systematic differences between the ob­

served UBV colors and magnitudes and those of Johnson and

Hiltner, the differences between them were examined. For

the 11 stars measured in common with Hiltner, excluding the

variable HDE 2397S7 and the emission-line star HD 198895

and adjusting Hiltner*s measurement of HD 200857 by 2.5 mag, the differences in the sense Simonson-Hiltner were s

A V a +0.002 ± 0.000

A (B-V) * +0.016 ± 0.0003

A (U-B) a -0.003 db 0.003 . 52

TABLE 7

RESULTS OP PHOTOELECTRIC PHOTOMETRY

HD/BD V B-V IT-B V B-V U-B Notes

198895 3.09±. 04 0.63±.02 -0.40±.03 8.30 .56 -.31 1. 199308 7.50±.03 0•16±.01 -0.65±.02 199661 6.22±.03 -0.17±.01 -0.74±.02 200857 7.13±.04 0.57±.02 -0.26±.Q2 9.66 .56 -.23 2. 202214 5.64±.04 0.13d:.01 — 0.78±»03 5.63 .11 -.77 1. 203025 6.41±.07 0.21±.01 -0.50±.03 203338 5.66±.04 1.47±.04 0 . 07± . 06 203374 6.67±.04 0.32±.02 —0.76±.03 204116 7•94±•04 0.51±.03 -0.29±.03 204150 5.71±.04 0.03±.02 — 0.79±*03 204827 7 . 94± « 04 0.G2±.03 -0.11±.03 7.95 .81 -.15 1. 205139 5.51±.04 0.13db.02 -0.74±.03 205196 7.39*.03 O.Sli.Ol — 0.47i.02 7.45 .57 -.45 1. 205510 0.48±.03 0.33±.01 —0,41±.02 205943 8.65±-.03 0.27±.01 —0.58±.02 206135 4.74 .30 -.53 3. 206133 7 . 43± . 03 0.15±,01 — 0.78db.02 7.40 .14 -.79 1. 205267 5.SS±.05 0.21±.10 — 0.6 Id:. 10 4. 206267C 8.04*.09 0.29±.10 -0.73±.08 4. 20S267D 3.03±.04 0.16±.02 — 0.69±.03 206327 9,19±.03 0.20±.01 -0.57±.02 205482 7.42±.04 0.43±.02 0.07±.02 206773 6.90±.04 0.21±.02 -0.73*.03 6.91 .21 -.32 1. 206923 8.23db.08 0.14±.02 0.12d:.03 206936 4.03±.04 2.40dt.03 2.41±.05 5. 207017 8. 58± . 03 0.22±.01 -0.43±.02 207198 5.94 .31 -.64 3. 207260 4.29 .51 .12 3. 207303 7.49±.03 0.26±.01 -0.55±.02 207533 7.31±.03 0.36±.01 -0.64±.02 7.31 .33 -.64 207951 G,13±.03 0.16±.01 -0.57±.02 208095 5.71±.03 —0.12±,01 ~0.46±*02 2080953 6,S3±«04 —0.02i.05 —0.23±.06 203106 7.56±.03 0.15±.01 -0.52±.02 208135 7.3S±.04 0.13±.02 ~0.54±.03 20G185B S. 208218 6 *69±.05 0.23±.02 —0.45±.03 6.69 .24 -.57 7. 208266 G.12±.04 0.28±.02 -0.52±.02 200392 7,07±,05 0.26±.03 —0.50±.04 7.04 .26 -.56 3. 208440 7 . 95± • 04 0.03±.01 — 0,67±.03 7.90 .07 -.73 7. 208501 5.79±.03 0.76±.01 -0.04i.02 5.79 .74 -.02 1. 200316 4.95^.04 1.37±.03 0.43d:. 03 + + + + + COtOCOCOCOCOtOCOCOCUCOCOCOtOCOlOCUlOiUCOIOtOrotOtOIO rorocococococococo m OiO yi W U W (jJ W LO W U U W W tJ LJ U W U Ul W td CO w w w u 10 u WWHOOOOOO 3 H H HH ffi 4^j«j~j^j'<4>jcnJ Gl 01 ^ OJ W CO CO to H CO 00 C3 03 *0 i!^ CO H CD CD 03 W 03 cn w o td CO CO COCO Ul CD CO CO CO «0 CO O CO CO OJ CO CO Ul :> to CJ »D OJ H 1 d Ul CO d C3 I> CJ1 H CO c n i!^ H i!^ CD C7I t ) H M H M *J CO cn .?s>oj CO P H H H H H O CD CO CD 03O co CDO CO cD C3 CD CDO C 3CO CD CD 03 Ul d Ul CO**1C3 dCD CO 03CD CO CD CD CD GO CO CO -O • ••••••••••■•••••••••••••••••••••• • ••••• |?5> O w CO O to(> CD to CO to cn *>J O i£*C-* *J wH* J-* cn HOWOOO cnCO OJ OJ O H CO COCO i!^ CO CO CO O 03 CO O OJ CD CO d CO CO M CO Ul H* to OJ 01 Ul cn i?s» (31 OJ CO >£. d 03 CO CD CO U1 -J *o OJ HUHOCIO tf- K- H- K- H- H- hh H- H- K- K- H- K- H- H- H- H- K- H- H- H- H- H- H- H- H- If H- H- H- H- H- If H- H- H- H- H- H* H- • ••«•••••••••••••••••••••••••••••• • ••••• oooooooooooooooooooooooooooooooooo o o o o o o OJ £> ijs. ,N, ,ji> CO i!^ OJ OJ i!i> OJ i>. iO. OJ OJ OJ d OJ OJ £> tD> (>• iP* i> OJ CO CO OJ OJ CO CO OJ TABLE oooooooooooooooooooooooooooooooj -*o o o o o o o o • •••••••••••••!•••••••••••••••»•** «••••• (Jjj_>i_»[V-)l_icrl 0^cniD»cn->Jtoi-, 03toIri.uiojcooj.^rotocococnojiOt!^ojcni-1i-ji^HWOHOH a CD 00 03 CJ CO *0 .> .Fs» I-* -J CO S-* CO d CO CO CD CD 00 Ul {-* CO CO CO {-» {-» CO vj {-» O |> CD CD CD H*I H- H- H- If H- If H- If H- H- II- H- H- H- H- H- If If H- H- K- H- H- If If If If H- B- H- H- H- fr H- H- H- H- H- H- H- <

• ••••••••••••«•••••••••••••••••*•* • • • • • 1

oooooooooooooooooooooooooooooooooo o o o o o o Continued — HI-i|-*COJ-*l-ii>COHi^COI-,HCOH(-*C7i|-,COI-,Cnf-,f-,t!l»f-,f-,H'tOCOCOfOIOCOH HWHHHH I I I I I I I I I I I I I I ( I I I i I I I I I I II I I I I I I OOOOOOOOOOOOOOOOOOOOOOOOOOOOOOOHOO o o o o o o • •••••••&•••••••••••••••••••••••*• • ••••• c o : ! ^1'i.cocjoi-‘ OCJOOJcncnH-*uii-, t-, cni'^iii«cot>cn^cnojcoi>Cjocnt's»ocncoCO d CO d CO *J CD CJ1 ^ CD CD C3 03 C3 Cn CO CO d Ul Ul CO i> 01 CD 03 h> J-» 00 CO •> 03 >J O OJ CO JD CD cn co cn i>. ¥ If H- H- H- H- If B- If If If If If If H- H- If If If H- If H- If H- If H- If If !f If H- H- If H- H- H- H- If If H- H- a »••••••••••••••••••••••**••••••••• • ••••• oooooooooooooooooooooooooooooooooo o o o o o o UIOJCOCOCOCO'JCJ£Oi!i.COCOCOCOtOrOi>COOOCO(i^COCOCOCOCOCOOJCjJCOOJCOCOCO CO CO to CO CO CO H O CD CD 03 CO CD C3 CO CO 03 03 CO C3 CD *0 Ul Ul cn • • • • • • • • • • •• • % • • • • O w 03 CO CO Ul *0 CD CJ Ul CO cn cn CO CO O H co H* OJ i\J cn o cn co *> CJ 03 O o C3 • • c • • • • • H H t O H «o to CO o o ¥ Ul 03 CO o cn <>• co CD < I I I I I I I I • • • • • • « • ¥ .5* 1> OJ i£. CO Ul •O CO -o a cD CD OJ d Ul OJ <> OJ

H H 9 <1 -O «o -o CO H CO CD CD CO CD o co CD CD U) H I-1 • • • • • • • • s Ul i i • i to OJ NOTES TO TA3LE 7

1. UBV photometry by Hiltnor (1956).

2. UBV photometry by Hiltner (1956)? his V measure­ ment is in error by 2.5 mag.

3. UBV standard.

4. Affected by clouds.

5• Semi-regular variable. 6. Unresolved. 7. Members of NGC 7160. Photometry by Johnson in Hoag et al (1961).

8. Same as 7 f eclipsing binary of W Uma typo with 20 hour period (Lynds 1959 []Ap. J., 130, 603]]).

9. Magnitudes from Petrie and Lee (1966), adjusted by -0.1 mag to put them on the V system from the Pv system.

10. Same as 9? double-line binary.

11. Number 6-27 in catalogue of Kirillova (1953).

12. Same as 1? eclipsing binary AI Cep.

For the si:-: stars in NGC 7160 measured in common with John­ son, excluding the eclipsing binary HD 203392, the differ­ ences in the sense Simonson-Johnson weres

A V = +0.047 ± 0.002 A(B-V) a -0.001 ± 0.003

A(U-B) = +0.063 ± 0.010 .

■Tliis comparison shows that the photoelectric photom­ etry is on the UBV system to a very good approximation. It is felt that the comparison with Hiltner is more represen­ tative than that with Johnson even though Johnson's measure­ 55 ments should loo exactly on tho standard system* The reason is that tho measurements of NGC 7150 were made within a few minutes at a large hour angle at the end of the last night of observing whereas the observations compared with Hiltner were spread throughout the observing period.

Photographic Photometry

Observations Magnitudes and colors for the stars classified on the

Schmidt plates were obtained by photographic photometry on

the BV system. Because of the difficulty in making glass platos conform to the focal surface of the Schmidt tele­

scope, the 4-inch f/7 Ross camera attached to the 32-inch

Schottland reflector was used.

The observations were made on the BV system for two

reasons. First of all, because of the difference in the

size of the Balmer discontinuity between giants and dwarfs

in the later B types, it is necessary to exclude the region

to the violet of about 13300 from the blue photometric band.

Otherwise, as Johnson (1952) has shown, the transformation

between the instrumental system and the standard UBV system

will not only be nonlinear but multivalued. Secondly, the

UBV system was chosen in preference to other systems because

of the large number of stars observed in the UBV system

which are available in the survey region for use as stan­

dards. The U band was excluded because of low transmission 56 of the Ross triplet. Little loss was felt to result from this, since the measurements were intended only for indica­ tions of distance and reddening.

The following combinations of plates and filters were useds V=IIa-D+2 mm Schott GG14, B=IIa-0+2 mm Schott GG 13.

The filters were 5 inches square and were mounted in con­ tact with the emulsion. In order to cover the entire region of the association, two plates in each color were required. The plates which were selected for photometry are listed in Table 8. All plates were developed the equivalent of 4 - h minutes in D-1S

at 68°F.

TABLE 8

PHOTOMETRIC PLATES TAKEN WITH THE 4-INCH ROSS CAMERA

No. Plate Center H.A. Date Color (1950) Exp. Mid-exp.

5 17 Aug 65 B 21h 39m + 5925 21 rnin 2W 3Sm

8 18 Aug 66 V 21 13 +53.5 30 min 2E12m

9 13 Aug 66 V 21 39 +59.5 30 min 1E17”

12 13 Aug 66 B 21 13 +58.5 30 min 2W 55m

The magnitudes were measured with a Cuffey iris Astro-

photometer (Cuffey 1S56) manufactured by Astromechanics,

Inc., of Austin, Texas. Because of the small size of the

images, the instrument was modified lay the substitution of 57 an objective of shorter focal length to focus the image of the iris on the plate. This had two advantages. First of all, the iris image was made as small as the smallest stel­ lar images on the plate, This reduced the fluctuations caused by the background plate graininess which otherwise make up a large fraction of the signal. Secondly, the scale of the iris readings was effectively expanded by a factor of about 4, which increased the precision by the same amount.

Reduction of observations The reduction of the As tropho tome ter measurements was accomplished by a program written in OMNITAB (Hilsenrath et al, 1SSS), which is a computer program for statistical and numerical analysis. In addition to a collection of in­ put and output subroutines which includes a provision for plotting graphs, and manipulative and mathematical subrou­ tines, OMNITAB includes two major statistical subroutines.

One of these is an orthonormalisation program for perform­

ing least-squares fitting of polynomials or any other func­

tion set. This program was used to obtain a relation be­

tween the iris readings, Q, and the magnitudes, m, of the

following forms m = a + bQ + cQ2 + dQ3 + eX + f Y + gR + hR2 + 1QR + j (B - V) , where X, Y, and R are the coordinates of the star measured

from the center of the plate. Tha form of tho reduction equation was chosen for the following reasons s the first four terms talce into account the curvature of the magnitude-iris reading reduction. This is a function of the construction of the iris photometer and the response of the emulsion. The terms in X and Y correct for any tilt of the plate, which seemed from visual inspec­ tion to be present. The terms in R, , and QR are included to account for the off-axis vignetting and aberrations.

These have a complicated effect? not only is the light reaching tho emulsion diminished as the image is displaced from tho axis, but also the image is transformed from a cir­ cular shape to that of a cross. Because of the unknown re­ lation between this change in image structure and the corre­ sponding responses of tho emulsion and tho iris photometer, terms were included which would allow for change in observed magnitude with radius, some curvature in the change, and an effect on the iris measurement with radius. The term in

B - V was included for conversion to the standard system and to allow for extinction effects. No other extinction term, such as one depending on air mass, was included because all the standards wore observed simultaneously with the program stars.

For each plate, if any coefficient had a value less than its standard deviation, the term was deleted from the function set and a new solution obtained. The term in B - V was found to bo insignificant in every instance. This 59 indicates only that the instrumental system can be linearly related to the BV system within tho limits of the observa­ tional errors over the range of observed B - V. The extreme limits of this range were -0.17 and 1.G7, but values wore well distributed only between about 0.0 and 1.0. This was considered adequate because all program stars were of early type and were expected to bo moderately reddened.

Errors in the calibration curve may arise if there is a systematic difference in color with magnitude or plate position, or a correlation between magnitude and plate po­ sition. Plots of those relations revealed no such effects.

Furthermore, the deviations of the observed points from the calculated calibration curves showed no systematic effects as functions of color, magnitude, or radius.

The coefficients for each plate and their standard deviations are listed in Table 9.

The photometer readings had a tendency to drift during tho course of the measurements, apparently because of me­ chanical vibration from the chopper motor which gradually shifted the position of the mirror that deflects the iris beam onto the photomultiplier. The drift was corrected in the iris readings by measuring a standard star in a stan­ dard way every half hour. The time to the nearest minute of each measurement was recorded, and a least-squarcs fit was made to the standard iris readings, Q std/ as a second- 60

TABLE 9

MAGNITUDE REDUCTION COEFFICIENTS

TERM Plato 5 Plate 8

Constant 14 .254:0 .14 13 .454:0.25

Q (2 .3344:0 . 044 )xlO**2 (1.225±0.044)xl0“4 a2 (2.31±0.29)xl0“5 a3 (1.21±0.2S ):cl0”9 R —0.14±0.11 0.274:0.19

R2 0.044±0.035 -0,094±0.041

QR (5.1±2.0)5Cl0“4

No. Stds 79 70

Std. Dg v . 0.134- 0.157

TERM Plate 9 Plate 12

Constant 12.34±0.21 12.834:0.21

Q (1.634:0.14 JstlO"*3 (2.02±0.16)xlO“2 a2 (1.93±0.53)xl0“5 (1.92±0.46)2d0“5 a3 (3.04±0.60)2d0"3 (1.21±0.44)2c10“3 X -0.0264:0.010 0.14±0.14

Y —0.015±0.019 -0.041±0.016

R 0 . 224:0.16 0.474:0.12

R2 ~ 0 .041± 0.043 —0.126±0.030

QR (9.54=3.3 )xl0*"4 (4.2±1.3)xl0“4

No. Stds 73 51

Std. Dev. 0.147 0.091 61 degree polynomial in the times

°sta(t=°> = a + bt + ct2 Qsta

Occasionally the mirror was adjusted and the time was reset to zero for a new series of standard readings and a new correction curve. The estimated internal standard deviations in the indi­ vidual star measurements were calculated from the following formula based on equation (4)s sri as [sa2 + Q2Sk2 + a2SQ2 + Q4sc2 + 4c2Q 2sq2 + Q6s<32

+ 9d2Q4s g2 + X2se2 + e2sx2 + Y2Sf2 + f2sy2 + R2sg2

+ g2 S j + R 4 s ^ 2 + 41i ^ r 2 s ^ 2 + q 2 r 2 s _^2

. 2 /-2 2 r>2„ 2\-i'i + i (R S q + Q S j j )J , where sa , sv,# etc* are the standard deviations in the sub­ scripted quantities•

The standard deviations i n tho coefficients were calcu­ lated by the OMNITAB program. Standard deviations in the measured quantities wore estimated in the following ways s

The standard deviation in X and Y was estimated to be less than 0.10 inch, because the star positions were measured with a ruler graduated in tenths of an inch on contact prints of the plates. R was calculated from X and Y, so its standard deviation is estimated to be ~\f2 (0 .1 0 ). The standard deviation in Q was harder to estimate. The iris readings consisted of two measurements of the star image followed by one of the plate background. All these measure- monts contain tho experimental error in balancing the iris beam against the comparison beam. In addition, the star measurements contain errors in centering the star image in the iris imago. Hie measurements of the star images and the plate background contain errors due to the random var­ iation of the plate graininess and the bacJcground fog.

(Hie effect of field errors, that is, the errors which are a systematic effect of position on tho plate, are assumed to be accounted for by the reduction equation.) For a 2 sample of 200 measurements, the variance, Sq , in the star measurements was found to be 1.71. If this is taken to be the same in the background readings, the total variance in the iris readings is about 3.5. In order to be more cer­ tain of having a large enough estimate of this number, the value of 10 was adopted.

The results of the photographic photometry are given

in Table 13, Chapter IV. RESULTS AND CONCLUSIONS

Photometric Distances

Presentation of results

Tables 10, 11, 12, and 13 give the color excesses,

Eb_v » absorption, Ay.? corrected distance moduli, V-Ay-Mv ? and photometric distances, r, in parsecs for the observed

stars. The results of different combinations of photo­ metry and spectral classification are given in the tables

as follows? Table 10 gives the results of MK classification

and photoelectric photometry. Table 11 gives the results

of Schmidt classification and photoelectric photometry? the

spectral types, color excesses, etc. found by applying the

Q-method (Johnson 1958) are also presented. Table 12 gives

the results of MK classification and photographic photo­ metry. Table 13 gives the results of Schmidt classifica­

tion and photographic photometry. While the MK classifi­

cations and the photoelectric photometry have been present­

ed in earlier tables, the Schmidt classifications and pho­

tographic photometry in Tables 11, 12, and 13 appear here

for the first time. Finding charts for the stars listed in

Tables 10, 11, 12, and 13 are given in Figures 3, 4, 5, and 6 . 63 64

TABLE 10

ABSORPTION AND DISTANCES FROM MK CLASSIFICATION AND PHOTOELECTRIC PHOTOMETRY

No. HD/BD Sp. T y p e V EB-V A=3E V-A-Mv r Notes 1 193895 BlVe 8.09 0.94 2.82 8.0 400 2 199303 B2V 7.50 0.40 1.20 8.2 440 3 199661 B3V 6.22 0.03 0.09 7.6 330 4 200857 B3III 7.13 0.77 2.31 3.8 580 5 202214 BOV 5.64 0.43 1.29 7.3 360 6 203025 B2V(e) 6.41 0.45 1.35 7.0 250 7 203338 BlsV + Mleplb 5.66 0.4 1.2 9.2 690 1. a 203374 BOVnne 6.67 0.62 1.36 8.3 460 9 204116 BlVep 7.94 0.75 2.25 8.3 460 2. 10 204150 B2V 7.71 0.27 0.81 8.8 580 2. 11 204827 BOV 7.94 1.12 3.36 8.0 400 2. 12 205139 Bill 5.51 0.37 1.11 9.4 760 13 205196 BOIb 7.39 0.85 2.55 10.6 1320 14 205948 B2V 3.65 0.51 1.53 9.0 660 3. 15 206165 B2lb 4.74 0.47 1.41 9.0 630 16 206183 BOV 7.43 0.45 1.35 9.5 800 3. 17 206267 06(f) 5.86 0.53 1.59 9.6 830 3. 13 206267C BOV 3.04 0.59 1.77 9.7 870 3. 19 206267D BOV 3.03 0.46 1.38 10.1 1050 3. 20 206327 B2V 9.19 0.44 1.32 9.8 960 21 206773 BlsVsnne 6.90 0.5 1.5 8.2 440 3. 22 206936 M2la 4.03 0.5 1 .5 •5.5 300 4. 23 207017 B2V 8.58 0.46 1.33 9.1 660 2. 24 207193 09.511 5.94 0.62 1.86 9.8 910 25 207260 A2la 4.29 0.46 1.33 10.4 1200 26 207303 BlVn 7.49 0.52 1.56 8.6 520 27 207538 BOV 7.31 0.66 1.93 8.8 580 28 207951 B2V 0.13 0.40 1.20 8.9 600 29 208106 B3V 7.56 0.35 1.05 3.0 400 2. 30 208135 B2V + B3V 7.38 0.37 1.11 8.3 460 2.,5. 31 208218 BlIII— II 6.69 0.49 1.47 9.9 950 6. 32 203266 BlV 3.12 0.54 1.62 9.1 660 33 203392 BlVn 7.07 0.5 1.5 3.9 600 7. 34 208440 BlV 7.95 0.34 1.01 9.6 330 8. 35 208501 B3Ib 5.79 0.78 2.34 9.1 660 36 208316 B2?pe + M2epla 4.95 0.4 1.2 10.8 1440 9. 37 208905 BlV 6.99 0.37 1.11 8.6 520 38 209339 BOIV 6.66 0.39 1.17 9.9 960 39 209454 B2V 7.76 0.43 1.29 3.4 480 40 209481 09V 5.51 0.39 1.17 S.l 660 41 209744 BlV 6.73 0.50 1.50 7.9 330 65

TABLE 10— Continued i HD/BD Sp. Type V EB-V A=3E V-A-Mv r Notes 42 209975 09.51b 5.11 0.37 1.11 10.0 1000 43 210339 06 f 5.04 0.56 1.63 3.6 520 44 239531 B2V 7.93 0.65 1.95 7.9 330 45 239613 B2Ve 8.45 0.76 2.23 8.1 420 46 239626 BOV 9.29 0.67 2.01 10.3 1440 47 239712 B2Vnne 3.65 0.67 2.01 8.5 500 2. ,3. 43 239724 B1III 9.14 0.65 1.95 12.4 3000 49 239725 B2V 9.15 0.52 1.56 9.5 800 3. 50 239729 BOV 3.35 0.68 2.04 9.3 910 3. 51 239743 B2V 9.01 0.35 2.55 8.4 430 52 239753 B2Vn(e) 9.53 0.51 1.55 9.9 960 53 239767 B0.5V 9.21 0.99 2.97 10.1 1050 3*11. 54 +61°2213 B3V + B5V 9.03 0.33 1.14 10.0 1000 12. 55 +61°2214 B3V 9.90 0.43 1.29 10.1 1050 13. 56 +61°2215 B3V 9.39 0.39 1.17 9.7 370 14. 57 +61°2213 B3V 10.03 0.34 1.02 10.6 1320 15.

NOTES TO TABLE 10

1. Adopted absolute magnitude Mv = -4•7, intrinsic B-V = +1.1, and intrinsic U-B = -0.3 from combining values for B1V in Table 14 with Mv = -4.5 for the M star from Kee­ nan (1963) and Intrinsic B-V = +1.3 and U-B = +2.1 for the M star from Johnson (1965). The excess in B-V appears rea­ sonable in comparison with neighboring stars. The excess in U-B is +0.4, whereas it should be 0.7Eb » v = 0.3. Con­ sidering the uncertainties, this is close agreement and tends to confirm the type of the B star.

2. Variable radial velocity according to Petrie and Pearce (1962).

3. Member or possible member of Tr 37.

4. Semi-rogular variable? adopted intrinsic B-V =1.9; adopted absolute magnitude lb. = -7.0 from Johnson (1965) and Keenan (1963). Johnson*s (1965) data g i v e a distance mod­ ulus of 9.7.

5. Visual binary unresolved in photometer? adopted Mv = -2.0, intrinsic B-V =-0.24.

6. NGC 7160-1? intrinsic color and absolute magni­ tude taken for class III. 66

NOTES TO TABLE 10— Continued

7. NGC 7160-2? eclipsing, contact binary? adopted absolute magnitude for two B1V stars =-3.5.

8. NGC 7160-3.

9. W Cephei. Adopted absolute magnitude Mv = -7. Because of the peculiarities of the system; the color esc- cess was taken as the mean of that of other stars in the same directions HD 208185, 209339, and 209975.

10. Double-line binary (Petrie 1961)? adopted Mv =-4.8.

11. Eclipsing binary? adopted Mv = -3.9 for two B0.5V stars.

12. NGC 7160-4? double-line binary? adopted intrinsic B-V = -0.20, adopted absolute magnitude Mv =-2.1.

13. NGC 7160-6.

14. NGC 7150-5.

15. NGC 7160-7. 67

TABLE 11

ABSORPTION AND DISTANCES FROM SCHMIDT CLASSIFICATION AND PHOTOELECTRIC PHOTOMETRY

No. HD Sp. Type V EB-V A=3E V-A-Mv r Notes

Part A. Spectral types from Schmidt classification.

53 206482 Blv 7.42 0.69 2.07 3.0 400 59 239595 B3v 3.37 0.37 1.11 8.3 460 60 239644 B2v 9.33 0.65 1.95 9.4 760 61 239649 Blv 9.32 0.47 1.41 10.6 1320 62 239675 B3v 9.16 0.52 1.56 9.1 660 63 239676 Blv 9.06 0.30 2.40 9.4 760 1. 64 239631 Blv 9.34 0.55 1.65 10.3 1150 65 239633 B2v 9.32 0.55 1.65 9.6 330 2. 66 239689 BOv 8.33 0.51 1.53 10.8 1440 3. 67 239693 B3v 9.54 0.45 1.35 9.6 830 68 239732 B2v 3.75 0.83 2.49 3.2 440 69 239733 Blv 10.13 0.72 2.16 10.6 1320 70 239742 Blv 9.42 0.43 1.44 10.6 1320 71 239743 Blv 3.75 0.45 1.35 10.1 1050 3. 72 239772 B2v 10.23 0.70 2.34 9.3 920 73 239789 BOv 9.23 0.74 2.22 10.6 1320 74 239312 B3v 9.96 0.77 2.31 9.2 700 75 239023 Blv 10.49 0.39 2.67 10.5 1250

Part B. Spectral types and color excesses from Q-method.

53 206432 B3V 7.42 0.51 1.53 6.0 160 4. 59 239595 B1.5V 3.37 0.41 1.23 9.9 950 60 239644 B2V 9.33 0.64 1.92 9.4 760 61 239649 BlV 9.32 0.42 1.26 9.8 920 62 239675 B5V 9.16 0.48 1.44 3.9 600 63 239676 BlV 9.06 0.30 2.40 9.4 760 64 239601 B0V- 9.34 0.57 1.71 10.2 1100 65 239633 B2.5V 9.32 0.53 1.59 9.4 760 66 239639 B1V 8.83 0.43 1.44 10.1 1050 67 239693 B3V 9.54 0.45 1.35 9.7 870 68 239732 B7V 3.75 0.69 2.07 7.0 250 5. 69 239733 BOV 10.13 0.53 1.59 8.6 520 5. 70 239742 B1.5V 9.42 0.46 1.33 10.3 1150 71 239743 B0.5V 3.75 0.46 1.33 10.5 1250 72 239772 B6V 10.23 0.68 2.04 9.0 630 5. 73 239789 B2V 9.28 0.67 2.01 9.2 690 74 239812 B7V 9.96 0.68 2.04 8.4 430 5. 75 239328 BOV 10.49 0.73 2.19 8.4 430 5. 63

NOTES TO TABLE 11

1. Two spectra visible, spectroscopic binary according to Petrie and Pearce (1962).

2. Member or possible member of Tr 37.

3. Possible variable radial velocity (Petrie and Pearce 1S62).

4. The type from the Q-method is probably correct.

5. The type from the Schmidt classification is prob­ ably correct. The stars may have been misidentified in the photoelectric photometry.

TABLE 12

ABSORPTION AND DISTANCES PROM MIC CLASSIFICATION AND PHOTOGRAPHIC PHOTOMETRY

No. HD Sp. Type V e b -v A=3E V-A-Mv r Notes

76 203761 B3V 9.0 0.33 1.14 S.4 750 77 239671 B2V 9.2 0.45 1.35 9.7 870 73 239710 B3V 10.1 0.55 1.65 9.9 950 1. 79 239727 A2xa 9.3 1.00 3.00 13.8 5700

NOTES TO TABLE 12

1. Member or possible member of Tr 37. TABLE 13

RESULTS OF SCHMIDT CLASSIFICATION AND PHOTOGRAPHIC PHOTOMETRY > CO 1 il m NO. RA (1900) DEC LI I B 11 SP . V S.D., S.D. > V-A-M R NOTES

80 20 44.1 56 56 94.6 8.7 B5V 10.2 0.6 0.3 0.8 1.4 10.0 1000 81 20 45.5 60 32 97.5 10.9 B3 9.5 0.6 -0.0 0.8 0.6 10.4 1200 82 20 45.6 57 57 95.5 9.2 B 1V 7.0 0.6 1.4 0.9 5.0 4.7 80 1 83 20 46.1 55 26 93.6 7.6 B2V 9.1 0.7 0.5 0.9 2 . 2 8.8 570 84 20 46.1 55 7 93.3 7.3 B8V 8.0 0.7 -0.0 1.1 0.3 7.8 360 85 20 46.6 55 31 93.7 7.6 B2V 9.7 0.7 0.3 0.8 1.6 10.0 990 86 20 46.8 55 45 93.9 7.7 B5V 10.9 0.6 -0. 1 0.8 0.2 11.9 2420 87 20 48.0 56 33 94.6 8.1 B5V 8.7 0.6 0.3 0.8 1.4 8.5 500 88 20 48.9 56 20 94.5 7.8 B5V 7.3 0.6 -0.0 1.1 0.5 8.0 400 89 20 49.2 54 34 93.2 6.7 B8V 7.4 0.7 0.4 1.1 1.5 6.0 160 90 20 49.9 56 35 94.8 7.9 B 1V 9.5 0.5 0.4 0.7 2.0 10.2 1100 91 20 50.2 57 31 95.6 8.5 B3V 10.0 0.5 0.1 0.7 0.9 10.6 1310 92 20 50.6 56 42 95.0 7.9 B5 10.1 0.5 0.2 0.7 1.1 10.2 1100 2 93 20 51.0 56 6 94.6 7.5 B5V 7.4 0.6 -0.0 1.1 0.5 8.1 420 94 20 51.2 60 28 97.9 10.3 B3 9.3 0.5 0.6 0.7 2.4 8.4 470 95 20 51.4 58 43 96.6 9.1 B5V 8.4 0.5 0.4 0.8 1.7 7.9 380 3 96 20 51.6 56 37 95.0 7.7 B5V 10.5 0.3 0.2 0.5 1.1 10.6 1330 2 97 20 51.6 54 40 93.5 6.5 B9V 10.1 0.6 0.3 0.8 1.1 8.8 580 98 20 51.8 55 53 94.5 7.2 B8V 9.2 0.6 0.3 0.8 1.2 8.1 420 99 20 52.2 57 30 95.7 8.3 B9V 9.6 0.5 -0.0 0.7 0.2 9.2 690 100 20 52.4 57 23 95.7 8. 1 B9V 9.4 0.5 0.3 0.7 1.1 8.1 420 3 101 20 53.4 56 26 95.0 7.4 B9V 8.7 0.5 -0.0 0.8 0.2 8.3 460 102 20 54.7 54 35 93.8 6.1 B9V 10.3 0.6 0.6 0.8 2.0 8.1 420 103 20 54.9 56 28 95.2 7.3 B2V 7.8 0.5 0.7 0.9 2.8 6.9 230 104 20 55.1 59 5 97.2 9.0 B9V 9.5 0.4 0.1 0.7 0.5 8.8 580 105 20 55.4 58 19 96.6 8.5 B5V 7.6 0.5 0.3 0.9 1.4 7.4 300 106 20 55.6 59 17 97.4 9. 1 B8V 9.4 0.5 0.3 0.7 1.2 8.3 460 107 20 55.8 58 20 96.7 8.4 B8V 7.9 0.5 0.1 0.9 0.6 7.4 300 4 108 20 56.1 55 41 94.7 6.7 B5V 10.6 0.5 0.2 0.6 1.1 10.7 1390 TABLE 13— CONTINUED

NO. RA 11900) DEC LI I B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

109 20 56.2 54 45 94.0 6.0 B9V 9.5 0.6 0.2 0.8 0.8 8.5 500 110 20 56.5 55 9 94.3 6.2 B9V 8.4 0.5 -0. 1 0.9 -0.1 8.3 460 111 20 57.0 58 41 97.0 8.6 B5V 9.3 0.4 0.2 0.6 1.1 9.4 760 3 112 20 57.8 55 2 94.4 6.0 B8V 10.3 0.5 0.3 0.7 1.2 9.2 700 113 20 57.8 55 2 94.4 6.0 B5V 9.7 0.5 0.5 0.7 2.0 8.9 600 114 20 57.9 57 32 96.3 7.7 B3V 11.1 0.4 0.1 0.5 0.9 11.7 2180 5 115 20 58.6 56 17 95.4 6.8 B 1 11.4 0.4 -0. 1 0.6 0.5 13.6 5290 6 116 20 58.7 54 50 94.3 5.8 B5V 10.0 0.5 0.2 0.7 1.1 10.1 1050 117 20 58.8 58 7 96.8 8.0 B8V 8.1 0.4 0.4 0.8 1.5 6.7 220 118 20 59.3 60 7 98.3 9.3 B8V 11.0 0.4 -0.0 0.6 0.3 10.8 1460 119 20 59.4 55 46 95.1 6.4 B8II I 8.4 0.5 2.5 0.6 7.8 2.1 20 120 20 59.6 59 39 98.0 8.9 B9V 10.8 0.4 -0.1 0.5 -0.1 10.7 1390 121 20 59.7 61 35 99.5 10.2 B8V 9.0 0.6 0.5 0.8 1.8 7.3 290 122 21 0.1 57 16 96.3 7.3 B8V 7.1 0.5 -0. 1 1.1 -q.o 7.2 270 123 21 0.2 54 23 94.1 5.3 B5V 10.0 0.6 0.3 0.7 1.4 9.8 920 124 21 0.2 56 36 95.8 6.8 B5V 6.7 0.5 -0.2 1.4 -0.1 8.0 400 125 21 0.2 56 10 95.5 6. 5 B8III 6.1 0.5 -0.3 1.7 -0.6 8.2 440 126 21 0.4 60 25 98.6 9.4 B8V 9.5 0.4 0.4 0.6 1.5 8.1 420 127 21 0.9 57 27 96.5 7.3 B8V 8.8 0.4 0.3 0.7 1.2 7.7 350 128 21 1.1 54 49 94.5 5.5 B3V 10.0 0.5 0.5 0.7 2.1 9.4 750 129 21 1.5 54 25 94.3 5.2 B8V 10.3 0.5 0.5 0.7 1.8 8.6 530 130 21 1.7 63 28 101.1 11.3 B8V 8.1 0.7 0.3 1.0 1.2 7.0 250 131 21 1.7 58 55 97.6 8.3 B5V 9.7 0.4 0.3 0.6 1.4 9.5 800 3 132 21 2.2 56 56 96.2 6.9 B9V 9.5 0.4 0.2 0.6 0.8 8.5 500 133 21 2.6 58 34 97.5 7.9 B5 10.4 0.4 -0.1 0.5 0.2 11.4 1920 3 134 21 2.7 58 2 97.1 7.6 B9V 7.8 0.4 0.6 0.8 2.0 5.6 130 13 5 21 2.9 60 40 99.0 9.3 B 5 10.0 0.6 0.3 0.8 1.4 9.8 920 3 136 21 3.0 55 54 95.5 6. 1 B8V 8.4 0.5 0.2 0.8 0.9 7.6 330 137 21 3.0 61 22 99.6 9.8 B8V 8.4 0.9 0.2 1.1 0.9 7.6 330 138 21 3.2 55 47 95.5 6. 0 B8V 8.1 0.5 -0. 1 0.9 -0.0 8.2 440 7 139 21 3.4 61 39 99.8 10.0 B8V 7.8 1.0 0.2 1.3 0.9 7.0 250 TABLE 13— CONTINUED

NO. 0) DEC LI I BI I SP. V S.D. B-V S.D. A=3E

140 55 5 95.0 5.5 B8V 10.8 0.5 0.1 0.6 0.6 141 58 26 97.5 7.7 B8V 10.7 0.4 -0.2 0.5 -0.3 142 59 11 98.1 8.2 B3V 10.1 0.6 0.4 0.7 1.8 143 58 57 97.9 8.0 B8V 7.6 1.0 0.3 1.2 1.2 144 56 59 96.5 6.7 B5V 12.0 0.3 -0.9 0.5 -2.2 145 55 56 95.7 5.9 B3V 9.9 0.4 0.6 0.6 2.4 146 56 48 96.4 6.5 B5V 11.2 0.3 -0.0 0.5 0.5 147 57 55 97.2 7.2 B9V 11.1 0.5 0.1 0.7 0.5 148 55 16 95.3 5.4 B8V 9.9 0. 5 0.1 0.6 0.6 149 54 49 95.0 5.1 B8V 9.7 0.5 0. 1 0.7 0.6 150 56 23 96.1 6. 1 B8V 11.5 0.4 -0.1 0.5 -0.0 151 58 8 97.4 7.3 B8V 9.9 0.6 0.4 0.8 1.5 152 55 16 95.4 5.3 B5V 10.2 0.4 0.4 0.6 1.7 153 59 1 98.1 7.9 B8V 10.8 0.5 -1. 1 0.7 -3.0 154 56 0 95.9 5.8 B9V 10.1 0.4 -0.0 0.6 0.2 155 62 23 100.6 10.2 B8V 8.6 0.9 0.1 I .1 0.6 156 59 23 98.4 8. 1 B9V 10.6 0.5 0.5 0.6 1.7 157 58 38 97.9 7.6 B5V 11.0 0.5 0.3 0.6 1.4 158 55 13 95.5 5.2 B9V 8.0 1.0 0.3 1.3 1.1 159 57 23 97.0 6.7 B8V 10.4 0.6 0.4 0.7 1.5 160 54 32 95.0 4.7 B8V 8.8 0.5 0. 1 0.8 0.6 161 56 39 96.5 6.1 B8V 10.0 0.7 0. 1 0.8 0.6 162 57 16 97.0 6.5 B9V 8.8 0.8 0.1 1.0 0.5 16 3 59 5 98.3 7.8 B9V 9.5 0.6 0.4 0.8 1.4 164 61 26 100.0 9.4 B5V 11.3 0. 5 0.5 0.6 2.0 165 55 30 95.7 5.3 B 1 11.0 0.7 1. 1 0.8 4.1 166 55 55 96.1 5.5 B3V 10.1 0.7 0.7 0.8 2.7 167 59 43 98.9 8.1 B1V 9.4 0. 7 0.4 0.8 2.0 168 55 42 96.0 5.3 BOV 10.1 0.7 1.0 0.8 3.9 169 54 51 95.4 4.7 83 V 8.6 0.9 -0.5 1.2 -0.9 170 54 46 95.3 4.7 B8V 8.7 0.9 0.2 1.1 0.9 TABLE 13— CONTINUEO

NO. >) DEC LI I B I I SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

171 55 51 96.1 5.4 BIV 8.5 0.9 0.4 1.1 2.0 9.2 690 172 63 37 101.7 10.8 BOV 8.5 0.6 0. 8 0.9 3.3 8.7 540 173 57 7 97.0 6.3 B1V 8.1 0.9 -0.2 1.2 0.2 10.6 1330 10 174 57 34 97.3 6.6 B5V 11.0 0.5 0.2 0.6 1.1 11.1 1670 175 60 18 99.3 8. 5 B8V 11.0 0.5 0. 1 0.6 0.6 10.5 1270 176 56 44 96.8 6.0 B9V 10.5 0.6 0.6 0.7 2.0 8.3 460 177 56 13 96.4 5.6 B2V 9.3 0.7 0.4 0.9 1.9 9.3 710 11 178 57 5 97. 1 6.2 B5V 11.0 0.5 0.6 0.6 2.3 9.9 960 4 179 59 54 99.1 8.2 B5 10.1 0.5 0.4 0.6 1.7 9.6 830 12 180 58 25 98.0 7. 1 B1V 9.0 0.7 0.2 0.9 1.4 10.3 1150 181 58 25 98.0 7.1 B1V 10.3 0.5 -1.9 0.8 -4.9 17.9 38370 4,13 182 55 27 95.9 5.0 B8V 8.5 0.9 0.4 1.1 1.5 7.1 260 4 183 63 23 101.7 10.6 B5V 8.6 0.6 -0.2 1.0 -0.1 9.9 960 184 55 58 96.3 5.4 B8V 10.5 0.6 0.4 0.8 1.5 9.1 660 185 59 5 98.5 7.5 B8V 11.3 0.4 -0.2 0.5 -0.3 11.7 2210 4 186 60 11 99.4 8.3 B8V 10.8 0.5 0.4 0.6 1.5 9.4 760 187 55 4 95.7 4. 7 B8V 10. 1 0.7 0.9 0.9,, 3.0 7.2 270 188 55 59 96.3 5.4 B5V 10.7 0.6 0.4 0.7 1.7 10.2 1100 189 58 37 98.2 7.2 B9V 10.7 0.5 0.4 0.6 1.4 9.1 660 3 190 60 4 99.3 8.2 B5V 10.1 0.5 0.3 0.6 1.4 9.9 960 191 62 22 101.0 9.8 B8V 8.9 0.8 0.5 0.9 1.8 7.2 270 192 57 55 97.8 6.7 B3V 10.2 0.5 0.3 0.7 1.5 10.2 1090 193 61 5 100.1 8.9 B5V 11 .0 0.5 0.4 0.6 1.7 10.5 1270 14 194 57 15 97.3 6.2 B 5 10.6 0.5 0.5 0.6 2.0 9.8 920 3 195 57 48 97.7 6.5 B9V 7.5 1.1 0.1 1.3 0.5 6.8 230 196 61 43 100.6 9.3 B8V 11.0 0.5 0.4 0.6 1.5 9.6 840 197 58 45 98.4 7.2 B5V 10.4 0.4 0.6 0.5 2.3 9.3 730 198 56 57 97.2 5.9 B8V 10.7 0.5 0.3 0.7 1.2 9.6 840 199 58 1 97.9 6.7 B5V 10.6 0.5 0.4 0.6 1.7 10.1 1050 200 57 46 97.7 6.5 B8V 10.0 0.6 0. 1 0.7 0.6 9.5 800 -J 201 58 4 98.0 6.7 B3V 10.5 0.5 0.5 0.6 2.1 9.9 950 to TABLE 13— CONTINUED

* < CO LU > CD II NO. RA (1900) DEC L11 B11 SP. V S.D. l S.D. V-A-MR NOTES

202 21 12.4 57 37 97.7 6.3 B9V 10.8 0.5 0.4 0.6 1.4 9.2 690 203 21 12.4 56 11 96.6 5.3 B3V 10.7 0.6 0.8 0.7 3.0 9.2 690 204 21 12.5 55 46 96.4 5.0 B3V 10.3 0.6 0. 5 0.8 2.1 9.7 870 20 5 21 12.6 55 37 96.3 4.9 B9V 9.5 0.7 0.5 0.9 1.7 7.6 330 206 21 12.6 61 58 100.8 9.4 B8V 9.5 0.7 0.5 0.9 1.8 7.8 360 207 21 12.9 58 17 98.2 6.8 B9V 10.9 0.4 0.5 0.5 1.7 9.0 630 208 21 13.2 59 7 98.8 7.3 B5 11 .1 0.4 0.1 0.5 0.8 11.5 2010 15 209 21 13.5 60 56 100.1 8.6 B8V 10.4 0.5 0.2 0.6 0.9 9.6 840 210 21 13.6 57 37 97.8 6.2 B9V 10.5 0.5 0.4 0.6 1.4 8.9 600 211 21 13.6 58 45 98.6 7.0 B8V 10.9 0.4 0.5 0.5 1.8 9.2 700 212 21 13.8 56 56 97.3 5.7 B9V 9.7 0.6 0.2 0.7 0.8 8.7 550 213 21 14.0 57 49 98.0 6.3 B8V 9.3 0.7 0. 1 0.8 0.6 8.8 580 214 21 14.0 56 46 97.2 5.6 B3V 10.5 0.5 0.4 0.6 1.8 10.2 1090 215 21 14.6 54 33 95.7 3.9 B5V 10.4 0.5 0.2 0.6 1.1 10.5 1270 216 21 14.7 63 30 102.1 10.3 B5V 6.5 0.7 -0.3 1.5 -0.4 8.1 420 217 21 14.8 59 30 99.2 7.5 B9V 10.1 0.5 0.4 0.6 1.4 8.5 500 218 21 14.9 54 17 95.6 3.7 B2V 9.7 0.5 0.3 0.7 1.6 10.0 990 219 21 15.0 58 41 98.7 6.9 B5V 10.4 0.5 0.4 0.6 1.7 9.9 96 0 220 21 15.2 56 15 97.0 5.1 B5V 8.0 1.0 -0.5 1.2 -1.0 10.2 1100 221 21 15.4 56 8 96.9 5.0 B8V 10.0 0.6 0.2 0.7 0.9 9.2 700 222 21 15.6 57 27 97.9 5.9 B8V 10.4 0.5 0.3 0.6 1.2 9.3 730 223 21 15.6 56 50 97.4 5.5 B9V 8.8 0.8 -0. 0 0.9 0.2 8.4 480 224 21 15.7 59 37 99.4 7.5 BOV 10.5 0.5 0.4 0.6 2.1 11.9 2390 225 21 15.8 54 46 96.0 4.0 B9V •8.3 0.9 0.4 1. 1 1.4 6.7 220 226 21 15.9 59 56 99.6 7.7 B8V 10.9 0.4 0. 1 0.5 0.6 10.4 1210 227 21 16.0 60 11 99.8 7.8 B5V 11.2 0.4 0.4 0.5 1.7 10.7 1390 228 21 16.2 54 34 95.9 3.8 B9V 8.7 0.5 0.3 0.8 1.1 7.4 300 229 21 16.2 59 0 99.0 7.0 B9V 11.2 0.4 0.5 0.5 1.7 9.3 730 230 21 16.2 54 5 95.6 3.5 B8V 9.0 0.6 0.4 0.8 1.5 7.6 330 231 21 16.4 58 26 98.6 6.6 B1V 8.1 0.9 0.3 1.1 1.7 9.1 660 16 23 2 21 16.4 56 43 97.4 5.3 B5 10.9 0.5 0.6 0.6 2.3 9.8 920 2 TABLE 13— CONTINUED 1 NO. L11 811 SP. V S.D. CD < S.D. A=3E V-A-M R NOTES

233 99.3 7.2 B8V 10.3 0.5 0.5 0.5 1.8 8.6 530 234 98.7 6. 5 B8V 7.8 1.0 0.3 1.2 1.2 6.7 220 235 100.1 7.9 B5V 10.4 0.5 0.4 0.5 1.7 9.9 960 3 236 99.4 7.2 BOV 10.8 0.4 -0. 1 0.5 0.6 13.7 5490 3 237 97.7 5.4 B3V 10.5 0.5 0.5 0.6 2.1 9.9 950 3 23 8 102.3 10.0 B5V 8.0 0.6 -0.0 1.0 0.5 8.7 550 239 100.9 8.6 BOV 10.0 0.5 -0. 1 0.7 0.6 12.9 3800 240 100.3 8.0 B8V 9.8 0.5 0.2 0.7 0.9 9.0 630 241 102.5 10. 2 B2V 7.9 0.6 0.2 1.0 1.3 8.5 490 242 99.8 7.5 B5V 9.6 0.6 -0.7 0.7 -1.6 12.4 3040 4 243 96.5 4.0 B8V 9.7 0.7 0.4 0.8 1.5 8.3 460 244 99.9 7.5 B2V 10.2 0.5 0 . 1 0.6 1.0 11.1 1640 245 97.7 5.2 B3 11.0 0.5 0.7 0.6 2.7 9.8 910 2 246 101.0 8.5 B5V 11.1 0.4 -0.0 0.5 0.5 11.8 2310 247 100.1 7.6 B8V 8.8 0.7 0.3 0.8 1.2 7.7 350 248 97.2 4.6 B8V 7.8 1.0 -0.0 1.2 0.3 7.6 330 249 99.8 7.3 B8V 10.0 0.5 -0.4 0.6 -0.9 11.0 1600 4 250 99.2 6.6 B8V 11.7 0.3 0.4 0.4 1.5 10.3 1160 251 100.2 7. 7 B8V 11 .4 0.4 0.4 0.4 1.5 10.0 1010 252 99.2 6.5 B5V 11.0 0.4 0.5 0.5 2.0 10.2 1100 253 96.5 3.7 B2V 9.2 0.8 0.3 0.9 1.6 9.5 780 254 101.1 8.5 B2V 9.5 0.6 0.2 0.7 1.3 10.1 1030 255 101.4 8.8 B8V 9.9 0.6 0.4 0.7 1.5 8.5 500 256 101.2 8.6 B8V 12.0 0.4 -0.8 0.5 -2. 1 14.2 7010 257 100.1 7. 5 B8V 11.6 0.3 0.2 0.4 0.9 10.8 1460 25 8 100.0 7.3 B3V 10.5 0.4 0 . 1 0.5 0.9 11.1 1650 259 97.6 4.8 B3V 10.6 0.5 0.6 0.6 2.4 9.7 870 3 260 99.6 6.8 B9V 11.4 0.3 0.8 0.4 2.6 8.6 520 4 261 101.5 8.7 B8V 10.4 0.5 0.3 0.6 1.2 9.3 730 262 96.7 3.8 B2V 8.7 0.8 0.5 1.0 2.2 8.4 470 263 99.1 6.2 B5V 10.9 0.4 0.4 0.5 1.7 10.4 1210 TABLE 13— CONTINUED

NO. 3) DEC LI I BII SP. V S.D. B-V S.D. A=3E V-A-MR NOTES

264 58 30 99. 1 6.2 B5V 9.5 0.6 0.7 0.7 2.6 8.1 420 265 60 6 100.2 7.4 B8V 10.8 0.4 0. 1 0.5 0.6 10.3 1160 4 266 59 15 99.6 6.7 B5V 10.7 0.4 0.5 0.5 2.0 9.9 960 26 7 54 28 96.3 3.3 B2V 10.7 0.5 0.3 0.6 1.6 11.0 1570 3 268 59 14 99.6 6.7 B9V 11.0 0.4 0.6 0.4 2.0 8.8 580 269 62 9 101.6 8. 8 B8V 10.7 0.5 0.3 0.6 1.2 9.6 840 270 59 45 100.0 7.1 B8V 10.4 0.4 0.3 0.5 1.2 9.3 730 271 55 13 96.8 3.8 B8V 10.1 0.6 1.5 0.7 4.8 5.4 120 272 62 30 101.9 9.0 B8V 7.5 1. 1 0.3 1.3 1.2 6.4 190 273 54 47 96.6 3.5 B5V 8.1 1.0 0.1 1.2 0.8 8.5 500 274 59 57 100.1 7.2 B8V 11.4 0.3 0.3 0.4 1.2 10.3 1160 275 59 58 100.1 7. 2 B5V 10.8 0.4 0.2 0.5 1.1 10.9 1520 276 57 38 98.6 5.5 B8V 9.5 0.6 -0. 1 0.7 -0.0 9.6 840 277 59 7 99.6 6.5 B9V 9.3 0.6 0.3 0.7 1.1 8.0 400 278 55 52 97.4 4.2 B 1V 8.9 0.8 0.4 0.9 2.0 9.6 830 17 279 60 49 100.8 7.8 B5V 11.0 0.4 0.4 0.5 1.7 10.5 1270 14 280 60 49 100.8 7.8 BOV 8.8 0.7 0.2 0.9 1.5 10.8 1440 281 55 37 97.2 4.0 B8V 8.2 0.9 -0.3 1.1 -0.6 8.9 610 282 60 28 100.6 7.5 B8V 11.3 0.4 0.5 0.4 1.8 9.6 840 283 63 55 103.0 10. 0 B9V 10.7 0.5 0.6 0.7 2.0 8.5 500 6 284 62 15 101.8 8.8 B8V 9.6 0.6 0.4 0.7 1.5 8.2 440 4 285 60 10 100.4 7.2 BIV 10.3 0.4 0.6 0.5 2.6 10.4 1210 286 60 35 100.7 7.5 B8V 11.6 0.3 0.2 0.4 0.9 10.8 1460 287 60 17 100.5 7.3 B8V 10.9 0.4 0.7 0.4 2.4 8.6 530 4 288 59 52 100.2 7. 0 B8V 11.2 0.3 0.3 0.4 1.2 10.1 1060 289 58 16 99.1 5.8 B2V 10.6 0.4 0.8 0.5 3.1 9.4 750 290 57 44 98.8 5.4 B8V 7.7 1.0 0.1 1.2 0.6 7.2 270 291 59 35 100.1 6.8 B2V 9.8 0.5 0.2 0.6 1.3 10.4 1190 292 61 4 101.1 7.9 B8I II 9.3 0.6 -0.3 0.8 -0.6 11 .4 1930 4 293 59 47 100.2 6.9 B8V 11.2 0.3 0.3 0.4 1.2 10.1 1060 294 59 40 100.1 6.8 B1V 9.7 0.5 0.2 0.6 1.4 11 .0 1590 TA8LE 13— CONTINUED ii > m NO* LI I 811 SP. V S.D. B-V S.D. Ul V-A-M R NOTES

295 100.0 6.6 B5V 10.2 0.4 0.4 0.5 1.7 9.7 870 18 296 100.9 7.6 B8V 10.9 0.4 0.3 0.5 1.2 9.8 920 297 97.5 3.9 B5V 9.6 0.6 0.4 0.8 1.7 9.1 660 298 99.5 6.0 B 1V 9.9 0.5 0.4 0.6 2.0 10.6 1330 299 98.6 5.1 B5V 10.7 0.4 0.3 0.5 1.4 10.5 1270 300 103.2 9.9 B8V 10.5 0.5 0.5 0.7 1.8 8.8 580 301 102.2 8.9 B8V 8.5 0.8 1.3 0.9 4.2 4.4 70 302 96.8 3.0 B8V 10.6 0.5 0.3 0.6 1.2 9.5 800 303 100.9 7.5 B8V 9.6 0.5 0. 1 0.6 0.6 9.1 660 304 98.1 4.4 B5V 10.8 0.4 0.6 0.5 2.3 9.7 870 305 100.7 7.3 B2V 10.4 0.4 -0.1 0.5 0.4 11.9 2370 306 99.9 6.4 B5V 10.6 0.4 0.3 0.5 1.4 10.4 1210 307 99.9 6.3 B5V 9.7 0.5 0.3 0.6 1.4 9.5 800 19 308 97.5 3.8 B8V 9.6 0.6 0.2 0.8 0.9 8.8 580 309 97.6 3.8 B3V 10.4 0.5 0.6 0.6 2.4 9.5 790 310 101. i 7.6 B5V 10.9 0.4 0.4 0.5 1.7 10.4 1210 311 97.6 3.8 BIV 9.2 0.7 0.4 0.8 2.0 9.9 960 20,21 312 99.2 5.5 B9V 10.6 0.4 0.4 0.5 1.4 9.0 630 313 98.2 4.4 B8V 10.2 0.5 0.7 0.6 2.4 7.9 380 20 314 99.7 6.0 B9V 10.2 0.4 0.2 0.5 0.8 9.2 690 315 99.1 5.3 B5V 10.3 0.4 0.2 0.5 1.1 10.4 1210 316 100.9 7.1 B8V 11.0 0.3 0. 1 0.4 0.6 10.5 1270 4 317 99.6 5.8 B8V 10.3 0.4 0.3 0.5 1.2 9.2 700 318 100.4 6.6 B5V 10.5 0.4 0.3 0.5 1.4 10.3 1150 14 319 97.2 3.0 B5V 6.6 1.3 -0.2 1.8 -0. 1 7.9 380 320 96.8 2.6 83 10.9 0.5 1.0 0.6 3.6 8.8 570 321 99.0 4.9 B8V 10.4 0.4 0.4 0.5 1.5 9.0 630 20 322 101.5 7.7 B8V 9.0 0.7 0.5 0.8 1.8 7.3 290 323 100.6 6.7 BOV 7.3 1.2 0.5 1.3 2.4 8.4 470 22 324 100.5 6.5 B9V 11.3 0.3 0.6 0.4 2.0 9.1 660 2 32 5 99.7 5.6 BOV 10.0 0.5 0.8 0.5 3.3 10.2 1090 TABLE 13— CONTINUED

NO. )) DEC LI I B I I SP. V S.D. B-V S.D. A=3E V-A-M R NOTE

326 54 56 97.3 3.0 B5V 10.4 0.6 0.6 0.7 2.3 9.3 730 327 57 19 98.9 4.7 B1V 9.5 0.6 -0.0 0.7 0.8 11.4 1920 20, 328 59 59 100.7 6.7 B3V 9.2 0.6 0.6 0.7 2.4 8.3 450 24 329 57 18 98.9 4.7 B3V 10.1 0.5 0.4 0.6 1.8 9.8 910 20 330 57 46 99.2 5.1 B7V 9.2 0.6 0.2 0.7 1.0 8.7 550 20 331 59 37 100.5 6.4 B3V 10.7 0.4 0.5 0.4 2.1 10.1 1040 332 54 59 97.4 3.0 B5V 10.9 0.5 0.5 0.7 2.0 10.1 1050 333 57 14 98.9 4.7 B5V 10.7 0.4 0.4 0.5 1.7 10.2 1100 20 334 61 24 101.7 7.7 B1V 7.6 1.1 0.4 1.2 2.0 8.3 460 33 5 61 22 101.7 7.7 B8V 8.2 0.9 0.5 1.0 1.8 6.5 200 336 55 56 98.0 3.7 B3V 10.6 0.5 0.5 0.6 2.1 10.0 990 337 57 49 99.3 5.1 B8V 9.0 0.7 0. 1 0.8 0.6 8.5 500 20 338 59 16 100.3 6. 1 B1V 9.8 0.5 0.5 0.6 2.3 10.2 1100 339 59 51 100.7 6.6 B5V 11.0 0.3 0.3 0.4 1 .4 10.8 1450 340 54 53 97.3 2.9 B8V 10.5 0.6 0.5 0.7 1.8 8. 8 580 341 56 10 98.2 3.8 B5V 10.4 0.5 0. 6 0.6 2.3 9.3 730 20 342 59 54 100.7 6.6 B 1V 8.8 0.7 0.7 0.8 2.9 8.6 520 343 60 22 101.0 6.9 B2V 9.7 0.5 0.2 0.6 1.3 10.3 1130 344 56 47 98.6 4.3 B5V 11.1 0.4 0.5 0.5 2.0 10.3 1150 20 345 57 32 99.1 4.9 B 1V 10.2 0.4 0.2 0.5 1.4 11.5 2010 20 346 54 43 97.3 2.7 B8V 10.6 0.5 0.5 0.6 1.8 8.9 610 347 56 26 98.4 4.0 B5V 9.3 0.6 0.1 0.7 0.8 9.7 870 20 348 54 31 97.2 2.6 B5V 11.3 0.5 0.2 0.6 1.1 11.4 1920 349 61 1 101.5 7.4 B5V 10.9 0.4 0.4 0.4 1.7 10.4 1210 350 54 40 97.3 2.6 B5 10.9 0.5 0.7 0.7 2.6 9.5 800 351 56 12 98.3 3.8 B8V 10.4 0.5 0. 7 0.6 2.4 8.1 420 20 352 59 4 100.3 5.9 B1V 8.1 0.9 0.4 1.0 2.0 8.8 580 353 61 33 102.0 7.7 B8V 9.8 0.5 0.3 0.6 1.2 8.7 550 354 58 11 99.8 5.1 B8V 8.0 0.9 0.2 1.1 0.9 7.2 270 355 56 30 98.7 3.9 B5V 9.4 0.6 0.8 0.7 2.9 7.7 340 20 356 59 51 100.9 6.4 B9V 10.8 0.3 0.5 0.4 1.7 8.9 600 TABLE 13— CONTINUED ii NO. RA 11900) DEC LI I B 11 SP. V S.D. B-V S.D. > m V-A-M R NOTES

357 21 30.4 54 54 97.6 2.7 B8V 8.7 0.8 0. 1 1.0 0.6 8.2 440 358 21 30.7 58 5 99.8 5.0 B8V 10.5 0.4 0. 1 0.5 0.6 10.0 1010 20 359 21 30.8 57 11 99.2 4.3 B1V 9.9 0.5 0.4 0.6 2.0 10.6 1330 20 360 21 31.0 60 2 101.1 6.4 BIV 8.5 0.8 0.5 0.9 2.3 8.9 600 361 21 31.0 57 43 99.5 4.7 B3V 7.7 1.0 0.5 1.2 2.1 7.1 260 4,20,2 362 21 31 .1 57 52 99.7 4.8 B5V 11.1 0.3 0.7 0.4 2.6 9.7 870 20 363 21 31.1 60 41 101.5 6.9 B8V 9.9 0.5 0.4 0.6 1.5 8.5 500 364 21 31.2 63 49 103.7 9.3 B6V 7.5 0.6 0. 1 1.1 0.7 7.6 320 365 21 31.3 56 47 99.0 4.0 B8V 9.4 0.6 0.2 0.7 0.9 8.6 530 4,20 366 21 31.4 62 54 103.1 8.6 B3V 10.1 0.5 0.7 0.6 2.7 8.9 600 36 7 21 31.4 60 17 101.3 6.6 B2V 10.1 0.4 0.2 0.5 1.3 10.7 1360 368 21 31.5 56 54 99.1 4.1 B8V 10.6 0.4 0.3 0.5 1.2 9.5 800 20 369 21 31.6 59 0 100.5 5.6 B1V 9.4 0.6 0.8 0.6 3.2 8.9 600 370 21 31.6 55 17 98.0 2. 8 B8V 9.8 0.6 0.5 0.7 1.8 8.1 420 371 21 31.6 58 32 100.2 5.3 B8V 8.1 0.9 0.3 1.0 1.2 7.0 250 372 21 31.7 54 39 97.6 2.3 B8V 9.1 0.5 0.2 0.8 0.9 8.3 460 373 21 31.9 58 10 99.9 5.0 B IV 10.0 0.5 0.6 0.5 2.6 10.1 1050 20 374 21 32.0 54 35 97.6 2.3 B2V 9.2 0.7 0.2 0.9 1.3 9.8 900 375 21 32.0 57 0 99.2 4.1 B5V 10.1 0.4 0.4 0.5 1.7 9.6 8 30 4,20 376 21 32.1 58 59 100.5 5.6 B1V 10.8 0.3 0.7 0.4 2.9 10.6 1330 377 21 32.3 57 46 99.7 4.6 B9V 10.9 0.3 0. 1 0.4 0.5 10.2 1100 20 378 21 32.4 54 56 97.9 2.5 B3V 10.5 0.5 0.6 0.7 2.4 9.6 830 379 21 32.4 57 16 99.4 4.2 B3V 10.3 0.4 0.6 0.5 2.4 9.4 750 20 380 21 32.4 61 47 102.4 7.6 BOV 8.4 0.8 0.3 0.9 1.8 10.1 1040 381 21 32.5 60 13 101.4 6.5 B2V 10.3 0.4 0.4 0.5 1.9 10.3 1130 3 382 21 32.5 58 16 100.1 5.0 B2V 10.0 0.5 0.4 0.5 1.9 10.0 990 383 21 32.6 54 54 97.9 2.5 B8V 10.7 0.5 0.8 0.6 2.7 8.1 420 384 21 32.7 57 2 99.3 4. 1 B2V 10.1 0.5 0.5 0.6 2.2 9.8 900 20 385 21 32.8 55 1 98.0 2.5 B8V 10.2 0.6 0.5 0.7 1.8 8.5 500 386 21 33.0 56 59 99.3 4.0 BOV 8.3 0.8 0.3 1.0 1.8 10.0 990 20 387 21 33.0 55 23 98.2 2.8 B5V 9.3 0. 7 0.2 0.8 1.1 9.4 760 4 TABLE 13— CONTINUED

NO. RA 11900) DEC L11 B I I SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

388 21 33.0 59 50 101.2 6. 1 B1 10.8 0.3 0.8 0.4 3.2 10.3 1150 3 389 21 33.1 56 55 99.2 3.9 B3V 10.3 0.4 0.9 0.5 3.3 8.5 500 12,20 390 21 33.3 56 52 99.2 3.9 B2V 10.8 0.4 0.1 0.5 1.0 11.7 2160 20 391 21 33.4 '60 25 101.6 6.5 B5V 9.9 0.5 0.6 0.6 2.3 8.8 580 392 21 33.5 61 55 102.6 7.7 B2V 9.9 0.5 0.7 0.6 2.8 9.0 620 393 21 33.7 57 33 99.7 4.4 88 V 11.3 0.3 -0.6 0.4 -1.5 12.9 3850 20,26 394 21 33.8 58 30 100.4 5.1 B1V 10.5 0.4 0.7 0.4 2.9 10.3 1150 395 21 33.9 57 1 99.4 3.9 B2 V 9.5 0.6 0.2 0.7 1.3 10.1 1030 20 396 21 34.1 61 31 102.4 7.3 BIV 9.3 0.6 0.6 0.7 2.6 9.4 760 397 21 34.2 58 53 100.7 5.3 B5V 10.6 0.3 0.7 0.4 2.6 9.2 690 398 21 34.3 54 7 97.5 1.7 B5V 8.0 0.6 -0.2 1.1 -0.1 9.3 730 399 21 34.5 56 57 99.4 3.8 B8V 10.2 0.4 0.5 0.5 1.8 8.5 500 20 400 21 34.6 62 12 102.9 7.8 B3V 10.9 0.4 0. 1 0.5 0.9 11.5 1990 401 21 34.6 63 29 103.7 8.7 B3V 9.1 0.7 0.2 0.9 1.2 9.4 750 40 2 21 34.8 58 17 100.3 4.8 B8V 7.6 1.1 0.3 1.2 1.2 6.5 200 403 21 34.8 57 5 99.5 3.9- BIV 8.4 0.8 0.3 1.0 1.7 9.4 760 20 404 21 34.9 56 23 99. 1 3.4 B8V 9.3 0.6 0.2 0.7 0.9 8.5 500 20 405 21 35.0 56 30 99.2 3.4 B2V 9.8 0.5 0.5 0.6 2.2 9.5 780 20 406 21 35.2 63 24 103.7 8.6 B2V 10.1 0.6 -0.0 0.7 0.7 11 .3 1800 407 21 35.3 58 41 100.6 5. 1 B1V 9.8 0.5 0.6 0.6 2.6 9.9 960 408 21 35.3 57 8 99.6 3.9 BOV 11.2 0.3 0.7 0.4 3. 0 11 .7 2180 2,20 409 21 35.4 57 2 99.6 3.8 B5V 10.8 0.4 0.2 0.5 1.1 10.9 1520 20 410 21 35.6 56 41 99.3 3.5 B5V 10.5 0.4 0.3 0.5 1.4 10.3 1150 20 411 21 35.6 63 2 103.5 8.3 B8V 10.1 0.5 1.2 0.6 3.9 6.3 180 412 21 35.6 61 5 102.2 6.9 B9V 9.7 0.5 0.4 0.6 1 .4 8.1 420 413 21 35.7 57 18 99.8 4.0 B9V 9.6 0.5 0.6 0.6 2.0 7.4 300 20 414 21 35.7 61 53 102.8 7.5 B2V 10.5 0.4 0.5 0.5 2.2 10.2 1080 415 21 35.8 61 33 102.5 7.2 B2V 10.6 0.4 1.7 0.5 5.8 6.7 210 4 416 21 36.0 55 17 98.5 2.4 B5V 8.1 0.9 -0.1 1.1 0.2 9.1 660 417 21 36.0 61 26 102.5 7.1 B5V 10.5 0.4 0.4 0.5 1.7 10.0 1000 418 21 36.1 54 43 98.1 2.0 B5 10.9 0.5 0.7 0.7 2.6 9.5 800 2 TABLE 13— CONTINUED

NO. L11 B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

419 98.1 1.9 B8V 9.4 0.7 0.5 0.8 1.8 7.7 350 420 98.3 2.1 BOV 10.2 0.6 0.8 0.7 3.3 10.4 1200 421 104.2 9.0 B5 8.9 0.6 0.3 0.9 1.4 8.7 550 15 422 99.8 3.9 B2V 10.2 0.4 0.5 0.5 2.2 9.9 940 20 423 99.8 3.9 B8V 11 .0 0.4 0.3 0.4 1.2 9.9 960 20 424 99.5 3.5 B5V 11.6 0.3 0.4 0.4 1.7 11.1 1670 20 425 101.1 5.3 OB 10.4 0.4 0.3 0.5 1.9 14.5 8090 15 426 99.1 3.0 B8V 8.9 0.7 0.3 0.8 1.2 7.8 360 20 427 99.8 3.8 B5V 11.3 0.3 0.6 0.4 2.3 10.2 1100 20 428 102.8 7.3 B3V 10.6 0.4 0.5 0.5 2.1 10.0 990 429 99.7 3.7 B3V 10.6 0.4 0.7 0.5 2.7 9.4 750 4,20 430 99.8 3.8 B3V 10.6 0.4 0.2 0.5 1.2 10.9 1510 4,20 431 100.2 4.3 BOV 9.5 0.5 -0.4 0.7 -0.3 13.3 4570 4,20 432 101.8 6.2 BOV 9.9 0.5 0.5 0.5 2.4 11.0 1580 433 98. 1 1.8 B8V 10.1 0.6 0.5 0.7 1.8 8.4 480 434 99.6 3.5 B8V 11.3 0.4 0.7 0.4 2.4 9.0 630 20 43 5 102.9 7.4 B5V 11.4 0.4 0.2 0.5 1.1 11.5 2010 436 98.4 2. 1 OB 10.7 0.5 0.9 0.6 3.7 13.0 4050 437 99.7 3.7 B2V 10.9 0.4 0.9 0.4 3.4 9.4 750 20 43 8 102.9 7.3 B3V 10.7 0.4 0.5 0.5 2.1 10.1 1040 439 100. 1 4.0 B 1V 9.6 0.5 0.4 0.6 2.0 10.3 1150 20 440 99.7 3.5 B3V 10.9 0.4 0.3 0.5 1.5 10.9 1510 20 441 99.9 3.8 BOV 12.2 0.3 0.7 0.3 3.0 12.7 3460 442 99.7 3.6 B3V 10.5 0.4 0.6 0.5 2.4 9.6 830 20 443 99.8 3.6 B2V 10.2 0.4 0.4 0.5 1.9 10.2 1080 20 444 100.2 4.2 B 1V 10 .0 0.5 0.4 0.5 2.0 10.7 1390 20 445 103.9 8.4 B8V 11 .2 0.5 0.2 0.6 0.9 10.4 1210 446 102.8 7. 1 B3V 9.8 0.5 0.3 0.6 1.5 9.8 910 447 98.2 1.7 B8V 9.1 0.6 0.6 0.8 2.1 7.1 260 44 8 100.0 3.8 B1V 9.9 0.5 0.2 0.6 1.4 11.2 1750 20 449 100.0 3.7 B5V 10.5 0.4 0.4 0.5 1.7 10.0 1000 20 TABLE 13— CONTINUED > CD NO. RA (1900) DEC L11 B11 SP. V S.D. 1 S.D. A=3E V-A-M R NOTES

450 21 38.6 62 28 103.4 7.7 B3V 9.7 0.6 0.5 0.7 2.1 9.1 660 451 21 38.6 62 41 103.5 7.8 B8V 10.5 0.5 0.6 0.6 2.1 8.5 500 452 21 38.7 57 45 100.4 4. 1 B5V 10.1 0.4 0.5 0.5 2.0 9.3 730 4 453 21 38.7 56 22 99.5 3.0 B3V 10.0 0.5 0.4 0.6 1.8 9.7 870 20 454 21 38.7 56 53 99.8 3.4 B3V 10.9 0.4 0.3 0.5 1.5 10.9 1510 3,20 455 21 38.8 61 47 103.0 7.2 B8V 9.5 0.6 0.5 0.7 1.8 7.8 360 456 21 38.8 60 28 102.1 6.1 B3 10.5 0.4 0.4 0.4 1.8 10.2 1090 12 457 21 38.9 62 26 103.4 7.6 B9V 9.3 0.6 0. 1 0.8 0.5 8.6 520 458 21 39.0 58 2 100.6 4. 3 B1V 8.7 0.7 0. 1 0.9 1.1 10.3 1150 20 459 21 39.0 62 38 103.5 7.8 B5V 11.2 0.4 0.4 0.5 1.7 10.7 1390 460 21 39.2 57 5 100.0 3.5 B5V 12.1 0.3 0.1 0.4 0.8 12.5 3190 4,20 461 21 39.2 57 31 100.3 3.8 B9V 10.7 0.4 0.6 0.4 2 . 0 8.5 500 20 462 21 39.3 55 10 98.8 2.0 B9V 11.1 0.5 1.2 0.6 3.8 7.1 260 463 21 39.3 59 40 101.6 5.5 B5V 11.0 0.3 0.4 0.4 1.7 10.5 1270 3 464 21 39.4 58 13 100.7 4.4 B1V 10.7 0.3 0.5 0.4 2.3 11 .1 1670 3,4;20 465 21 39.4 60 30 102.2 6.1 B5V 10.3 0.4 0.2 0.5 1.1 10.4 1210 466 21 39.5 57 22 100.2 3.7 B3 10.3 0.4 0.7 0.5 2.7 9.1 660 20 467 21 39.5 62 50 103.7 7.9 B2V 9.9 0. 5 0. 3 0.7 1.6 10.2 1080 468 21 39.6 57 46 100.5 4.0 B IV 9.8 0.5 0.4 0.6 2.0 10.5 1270 20 469 21 39.7 60 52 102.5 6.4 B8V 11 .3 0.3 -0.1 0.4 -0.0 11.4 1930 4 470 21 40.0 57 17 100.2 3.6 B3V 10.1 0.4 0.4 0.5 1.8 9.8 910 20 471 21 40.1 55 1 98.8 1.8 B2V 8.3 0.9 -0.0 1.1 0.7 9.5 780 472 21 40.1 61 22 102.8 6.7 B8V 10.0 0.5 0.4 0.6 1.5 8.6 530 473 21 40.1 61 56 103.2 7.2 B5V 10.4 0.4 0.4 0.5 1.7 9.9 960 474 21 40.3 58 23 100.9 4.4 BOV 10.2 0.4 0.2 0.5 1.5 12.2 2750 475 21 40.5 56 32 99.8 3.0 BOV 8.9 0.7 0.1 0.8 1 . 2 11.2 1730 28 476 21 40.5 54 56 98.8 1.7 B5V 10.3 0.6 0.6 0.7 2.3 9.2 690 477 21 40.9 57 20 100.3 3.6 B8V 9.9 0.5 0.3 0.6 1 . 2 8.8 580 20 478 21 40.9 57 43 100.6 3.9 B5V 10.7 0.4 0.7 0.4 2.6 9.3 730 20 479 21 40.9 61 15 102.8 6.6 B8V 10.0 0.5 0.5 0.6 1.8 8.3 460 480 21 41.0 57 30 100.4 3.7 B5V 10.5 0.4 0.3 0.5 1.4 10.3 1150 TABLE 13— CONTINUED

NO. RA C1900) DEC L11 B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

481 21 41.1 55 5 98.9 1.8 B2 10.7 0.5 0.6 0.6 2.5 10.1 1030 29 482 21 41.1 56 57 100.1 3.2 B5V 10.5 0.4 0.6 0.5 2.3 9.4 760 483 21 41.3 55 5 98.9 1.8 B1V 9.4 0.7 0.4 0.8 2.0 10.1 1050 484 21 41.3 57 15 100.3 3.5 B8V 9.0 0.7 0.3 0.8 1.2 7.9 380 20 485 21 41.3 58 30 101.1 4.4 B5V 10.3 0.4 0.4 0.5 1.7 9.8 920 486 21 41.4 55 20 99.1 2.0 B5V 10.0 0.6 0.5 0.7 2.0 9.2 690 48 7 21 41.4 54 42 98.7 1.5 B5V 9.1 0.6 0.3 0.9 1.4 8.9 600 488 21 41.6 55 16 99.1 1.9 B8V 9.8 0.6 0.6 0.7 2.1 7.8 360 489 21 41.6 57 37 100.6 3. 7 B5V 10.9 0.3 0.3 0.4 1.4 10.7 1390 20 490 21 41.7 57 41 100.6 3.8 B8V 9.4 0.6 0.1 0.7 0.6 8.9 610 20 491 21 41.7 62 13 103.5 7.3 B3V 10.5 0.4 0.5 0.5 2.1 9.9 950 492 21 41.8 56 19 99.8 2.7 B2V 11.0 0.4 0.5 0.5 2.2 10.7 1360 20 49 3 21 41.9 58 52 101.4 4.7 B5V 10.9 0.3 0.5 0.4 2.0 10.1 1050 494 21 42.1 61 9 102.9 6.4 B9V 11.0 0.3 0.6 0.4 2.0 8.8 580 495 21 42.3 61 32 103.1 6.7 B8V 11 .0 0.4 0.2 0.4 0.9 10.2 1110 496 21 42.4 56 13 99.8 2.6 B5V 11.0 0.4 0.4 0.5 1.7 10.5 1270 20 497 21 42.5 55 26 99.3 1.9 B8V 10.1 0.5 0.4 0.6 1.5 8.7 550 498 21 42.6 61 10 102.9 6.4 B9V 11.3 0.3 -0.7 0.4 -1.9 13.0 4010 499 21 42.8 61 28 103.1 6.6 B8V 10.9 0.4 0.2 0.4 0.9 10.1 1060 4 500 21 42.9 59 5 101.6 4.7 B5V 9.6 0.5 0.1 0.6 0.8 10.0 1000 501 21 43.1 60 42 102.7 6.0 B3V 9.5 0.6 0.6 0.6 2.4 8.6 520 502 21 43.3 55 5 99.2 1.6 OB 10.3 0.6 0.4 0.7 2.2 14.1 6720 4 503 21 43.3 57 20 100.6 3.4 B 1V 8.8 0.7 0.1 0.8 1.1 10.4 1210 4,15,20 504 21 43.3 60 45 102.7 6.0 B5V 10.5 0.4 0.6 0.5 2.3 9.4 760 505 21 43.3 55 4 99.2 1.6 B8V 10.5 0.5 0.5 0.7 1.8 8.8 580 506 21 43.4 54 36 98.9 1.2 B2V 10.7 0.6 0.5 0.8 2.2 10.4 1190 507 21 43.7 56 50 100.3 2.9 B5V 10.3 0.4 0. 1 0.5 0.8 10.7 1390 20 508 21 43.8 62 2 103.6 7.0 B9V 9.8 0.5 0.1 0.6 0.5 9.1 660 509 21 44.0 55 6 99.2 1.5 B5V 10.5 0.5 0.6 0.6 2.3 9.4 760 510 21 44.0 61 49 103.5 6.8 B5V 11.3 0.4 0.2 0.4 1.1 11.4 1920 511 21 44.0 61 12 103.1 6.3 B2V 10.1 0.5 0. 1 0.6 1.0 11.0 1570 TABLE 13— CONTINUED

NO. RA (1900) DEC LI I B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

512 21 44.0 63 18 104.4 7.9 B5V 11 .4 0.5 0.3 0.6 1.4 11.2 1750 513 21 44.2 61 21 103.2 6.4 B5V 9.2 0.6 -0.0 0.7 0.5 9.9 960 514 21 44.2 59 14 101.9 4. 8 B1V 10.5 0.4 0.3 0.4 1.7 11.5 2010 2,4 515 21 44.6 58 34 101.5 4.2 B5V 10.9 0.3 0.2 0.4 1.1 11 .0 1590 516 21 44.6 55 4 99.3 1.5 OB 10.9 0.5 0.1 0.6 1.3 15.6 13420 517 21 44.7 61 22 103.2 6.4 B5V 11.4 0.3 0.1 0.4 0.8 11.8 2310 518 21 44.8 62 7 103.7 7.0 B3V 10.7 0.4 0.2 0.5 1.2 11.0 1580 519 21 44.9 56 43 100.4 2.7 B3 10.0 0.5 0. 5 0.6 2.1 9.4 750 4,15,2C 520 21 45.0 58 30 101.5 4. 1 B2V 10.2 0.4 -0.0 0.5 0.7 11.4 1880 30 521 21 45.1 57 56 101.1 3.7 B3V 10.0 0.5 -0.0 0.6 0.6 10.9 1510 522 21 45.2 57 26 100.8 3.3 B9V 10.5 0.4 0.6 0.5 2.0 8.3 460 20 523 21 45.2 57 26 100.8 3.3 B9V 10.4 0.4 0.8 0.5 2.6 7.6 330 20 524 21 45.2 58 I 101.2 3.7 B5V 11.2 0.3 0.4 0.4 1.7 10.7 1390 525 21 45.3 58 48 101.7 4.3 B5V 10.2 0.4 0.3 0.5 1.4 10.0 1000 526 21 45.4 57 30 100.9 3.3 B8V 8.2 0.9 0.2 1.0 0.9 7.4 300 527 21 45.4 57 24 100.8 3. 2 B5 V 8.2 0.9 0.2 1.0 1.1 8.3 460 20 528 21 45.5 55 0 99.3 1.3 OB 11.3 0.5 -0.0 0.6 1.0 16.3 18530 529 21 45.5 55 40 99.8 1.9 OB 10.3 0.5 0.9 0.6 3.7 12.6 3370 530 21 45.6 55 10 99.5 1.5 B2 11.0 0.5 0.6 0.6 2.5 10.4 1190 531 21 45.6 56 20 100.2 2.4 B3V 11.4 0.4 0.3 0.5 1.5 11.4 1900 20 532 21 45.7 62 2 103.8 6. 8 B5V 9.8 0.5 0.2 0.6 1.1 9.9 960 533 21 45.8 59 19 102.1 4.7 B3V 10.9 0.3 0.4 0.4 1.8 10.6 1310 534 21 45.9 54 26 99.0 0.9 BOV 10.1 0.7 0. 1 0.9 1.2 12.4 3010 535 21 46.6 58 32 101.7 4.0 B3V 10.8 0.3 0.2 0.4 1.2 11.1 1650 536 21 46.7 57 46 101.2 3.4 B3V 10.5 0.4 0.4 0.5 1.8 10.2 1090 537 21 47. 1 61 35 103.6 6.4 B9V 11.1 0.4 0. 3 0.4 1.1 9.8 920 538 21 47.1 61 7 103.3 6.0 B8V 10.8 0.4 0.4 0.4 1.5 9.4 760 539 21 47.2 56 38 100.6 2.5 B2V 10.5 0.4 0.5 0.5 2.2 10.2 1080 540 21 47.4 58 37 101.8 4.0 B1 11.6 0.3 0. 1 0.3 1.1 13.2 4400 6 541 21 47.6 58 53 102.0 4.2 B5V 10.2 0.4 1.4 0.5 4.7 6.7 220 6 542 21 47.8 59 40 102.5 4.8 B2V 10.5 0.4 0.4 0.4 1.9 10.5 1240 TABLE 13— CONTINUED

NO* RA <1900) DEC L11 BII SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

543 21 47.8 54 45 99.4 0.9 B 3 9.3 0.7 1.0 0.8 3.6 7.2 270 31 544 21 48.0 61 2 103.3 5.9 B8V 10.7 0.4 0.3 0.5 1.2 9.6 840 545 21 48.1 55 53 100.2 1.8 OB 9.5 0.6 0.3 0.7 1.9 13.6 5340 4 546 21 48.3 63 32 104.9 7.8 B2V 8.2 0.9 0.2 1.1 1.3 8.8 570 547 21 48.4 57 7 101.0 2.8 B8V 8.6 0.7 -0.0 0.9 0.3 8.4 480 548 21 48.5 59 23 102.4 4.5 B5V 10.7 0.3 0.1 0.4 0.8 11.1 1670 549 21 48.7 58 47 102.0 4.1 B8V 10.9 0.3 0.4 0.4 1.5 9.5 800 550 21 48.8 58 45 102.0 4.0 B8V 10.2 0.4 0. 1 0.5 0.6 9.7 880 551 21 48.8 62 32 104.4 7.0 B5V 11.3 0.4 0.1 0.5 0.8 11.7 2200 552 21 48.9 61 14 103.6 6. 0 B9V 10.4 0.4 0.5 0.5 1.7 8.5 500 553 21 48.9 57 30 101.3 3.0 B5V 10.1 0.5 0.2 0.6 1.1 10.2 1100 554 21 49.0 62 58 104.7 7.3 B9V 11.0 0.5 0.4 0.6 1.4 9.4 760 555 21 49.1 62 30 104.4 6.9 B5V 10.5 0. 5 -0.0 0.6 0.5 11.2 1750 556 21 49.2 56 29 100.7 2.2 B IV 10.5 0.5 0.5 0.5 2.3 10.9 1520 557 21 49.3 58 50 102.1 4.0 B8V 11 .0 0.3 -0.0 0.4 0.3 10.8 1460 55 8 21 49.3 59 2 102.2 4.2 B5V 11.1 0.3 0.1 0.4 0. 8 11.5 2010 559 21 49.4 59 25 102.5 4. 5 B8V 7.8 1.0 0.2 1.2 0.9 7.0 250 560 21 49.4 55 52 100.3 1.7 Bl 10.9 0.5 1.0 0.6 3.8 9.8 920 6 561 21 49.6 63 1 104.7 7.3 B3V 10.1 0.5 -0.0 0.7 0.6 11.0 1580 562 21 49.6 58 22 101.9 3.6 B2V 10.4 0*4 0.3 0.5 1.6 10.7 1360 563 21 49.6 61 53 104.0 6.4 B3V 9.3 0.6 -0.0 0.8 0.6 10.2 1090 564 21 49.7 54 32 99.5 0.6 B5V 7.4 0.7 0. 1 1.3 0.8 7.8 360 3 565 21 49.8 63 47 105.2 7.9 B5 10.7 0.6 0.4 0.7 1.7 10.2 1100 3 566 21 49.9 60 40 103.3 5.4 B8V 8.9 0.7 0.2 0.8 0.9 8.1 420 567 21 50.0 58 38 102.1 3.8 B9V 9.4 0.6 0.3 0.7 1.1 8.1 420 568 21 50.0 54 30 99.6 0.5 B5V 9.5 0.7 0.9 0.9 3.2 7.5 310 569 21 50.2 62 39 104.6 7.0 B8V 11.3 0.4 0.4 0.5 1.5 9.9 960 570 21 50.2 58 54 102.3 4.0 B5V 10.0 0.4 0. 1 0.5 0.8 10.4 1210 32 571 21 50.2 58 46 102.2 3.9 B2V 9.9 0.5 0.4 0.5 1.9 9.9 940 572 21 50.3 59 34 102.7 4. 5 B2V 10.6 0.4 0.5 0.4 2.2 10.3 1130 573 21 50.4 57 25 101.4 2.8 B3V 11.4 0.3 0.5 0.4 2.1 10.8 1440 TABLE 13— CONTINUED

NO. L11 BIT SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

574 99.8 0.8 BOV 9.7 0.6 0.9 0.8 3.6 9.6 830 575 104.6 7.0 B8V 10.5 0.5 0.3 0.6 1.2 9.4 760 576 99.6 0.4 B5V 10.0 0.7 0.5 0.9 2.0 9.2 690 577 104.2 6.4 B8V 11.2 0.4 0.4 0.5 1.5 9.8 920 578 104.2 6.4 B5V 12.0 0.4 0.6 0.4 2.3 10.9 1520 579 101.8 3.2 B3V 10.5 0.4 0.5 0.5 2.1 9.9 950 580 104.1 6.2 B5 12.0 0.3 0.3 0.4 1.4 11.8 2310 2 581 104.3 6.5 B9V 12.2 0.4 0.6 0.4 2.0 10.0 1000 582 104.5 6. 8 B5V 10.7 0.5 0. 1 0.6 0.8 11.1 1670 583 104.5 6.7 B9V 10.8 0.4 0.2 0.6 0.8 9.8 920 584 101.0 2.2 B8V 10.0 0.5 0.3 0.6 1.2 8.9 610 585 104.4 6.6 B9V 11 .6 0.4 -0. 1 0.5 -0. 1 11.5 2010 4 586 104.1 6.2 B9V 11.7 0.4 0.3 0.4 1. 1 10.4 1210 587 103.3 5.2 B3V 10.0 0.5 0.3 0.5 1.5 10.0 990 588 102.5 4.0 BIV 10.5 0.4 0.2 0.5 1.4 11.8 2310 589 103.8 5.8 B9V 10.9 0.4 -0.1 0.5 -0.1 10.8 1450 590 104.1 6.2 B8V 11 .7 0.4 0.5 0.4 1.8 10.0 1010 591 104.1 6.1 B3V 10.9 0.4 0.8 0.5 3.0 9.4 750 592 103.1 4.8 B3V 11.3 0.3 0.2 0.4 1.2 11.6 2080 593 103.2 4.9 B8V 11.2 0.3 -0.5 0.4 -1.2 12.5 3200 4 594 102.0 3.3 B8V 8.5 0.8 0. 1 0.9 0.6 8.0 400 33 595 103.4 5.1 B5V 10.8 0.4 0.4 0.4 1.7 10.3 1150 596 100.3 1.1 B5 11.8 0.5 -0.9 0.6 -2.2 15.2 11060 3 597 102.7 4. 1 B2V 11 .0 0.3 0.4 0.4 1.9 11.0 1570 598 104.0 5.8 B5V 11.1 0.4 0.5 0.5 2.0 10.3 1150 34 599 102.9 4.3 BOV 7.9 1.0 0.4 1.1 2.1 9.3 720 600 105.0 7.2 B8V 9.5 0.6 0. 1 0.8 0.6 9.0 630 601 104.6 6.6 B3V 10.0 0. 5 -0. 1 0.6 0.3 11.2 1730 602 102.5 3.7 BOV 8.0 0.9 0.4 1.1 2.1 9.4 750 35 603 101.5 2.5 B3V 11.0 0.4 0.3 0.5 1.5 11.0 1580 604 103.3 4.8 B8V 10.2 0.4 0.7 0.5 2.4 7.9 380 TABLE 13— CONTINUED

NO. RA (1900) DEC LI I B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

605 21 53.2 62 55 105.0 7.0 B5V 10.0 0.6 0.2 0.7 1.1 10.1 1050 606 21 53.2 62 55 105.0 7.0 B5V 10.3 0.5 0.3 0.6 1.4 10.1 1050 607 21 53.3 62 7 104.5 6.3 B8V 10.2 0.5 0.3 0.6 1.2 9.1 660 608 21 53.3 62 5 104.5 6.3 B5V 9.8 0.6 0. 1 0.7 0.8 10.2 1100 609 21 53.4 62 24 104.7 6.6 BOV 7.4 1.1 0.3 1.3 1.8 9.1 660 610 21 53.7 59 58 103.3 4.6 B3V 10.9 0.4 0.7 0.4 2.7 9.7 870 611 21 53.9 62 3 104.5 6.3 B9V 11.5 0.4 0.3 0.5 1.1 10.2 1100 612 21 54.0 55 5 100.4 0.7 B9V 10.3 0.6 0.5 0.7 1.7 8.4 480 613 21 54.0 57 29 101.8 2.6 B5V 10.6 0.4 0.5 0.5 2.0 9.8 920 614 21 54.2 62 20 104.7 6.5 B5V 9.9 0.5 0.2 0.6 l.l 10.0 1000 615 21 54.2 62 13 104.7 6.4 B5V 9.7 0.6 0.4 0.7 1.7 9.2 690 616 21 54.2 59 57 103.3 4. 5 B5V 10.9 0.3 0.3 0.4 1.4 10.7 1390 617 21 54.3 59 50 103.2 4.4 B IV 11.1 0.3 0.3 0.4 1.7 12.1 2650 618 21 54.4 63 37 105.5 7.5 B5V 11.8 0.5 -0.0 0.6 0.5 12.5 3190 619 21 54.4 62 47 105.0 6.8 B3V 9.0 0.7 0.2 0.9 1.2 9.3 720 620 21 54.4 61 58 104.5 6.1 B3V 10.2 0.5 0.2 0.6 1.2 10.5 1250 621 21 54.4 63 16 105.3 7.2 B2V 10.3 0.6 0.2 0.7 1.3 10.9 1490 622 21 54.5 58 50 102.7 3.6 B5V 10.2 0.5 0. 3 0.6 1.4 10.0 1000 623 21 54.6 57 52 102.1 2.8 B5V 9.0 0.7 0.2 0.8 1.1 9.1 660 624 21 54.6 58 49 102.7 3.6 B8V 10.7 0.4 0.4 0.4 1.5 9.3 730 625 21 54.7 63 45 105.6 7.6 B5V 11.0 0.6 0. 1 0.6 0.8 11.4 1920 4 626 21 54.8 59 4 102.8 3.8 B5V 10.1 0.4 0.5 0.5 2.0 9.3 730 627 21 55.0 56 40 101.4 1.8 B5V 11 .0 0.4 0.5 0.5 2.0 10.2 1100 628 21 55.0 61 46 104.5 5.9 B8V 11.2 0.4 0.2 0.5 0.9 10.4 1210 629 21 55.1 57 46 102.1 2.7 BIV 10.6 0.4 0.5 0.5 2.3 11.0 1590 63 0 21 55.3 54 33 100.2 0. 1 B8 10.2 0.6 0.5 0.8 1.8 8.5 500 3 631 21 55.3 60 55 104.0 5.2 B9V 11.3 0.4 0.4 0.4 1.4 9.7 870 632 21 55.3 61 7 104.1 5.4 B3V 10.3 0.4 0.3 0.5 1.5 10.3 1140 633 21 55.4 55 41 100.9 1.0 □ B 10.5 0.5 0.9 0.6 3.7 12.8 3690 634 21 55.5 63 30 105.6 7.3 B8V 10.9 0.5 0.2 0.7 0.9 10.1 1060 635 21 55.6 63 31 105.6 7.3 BOV 11 .0 0.5 -0.3 0.7 -0.0 14.5 7940 TABLE 13— CONTINUED

NO. L11 B11 SP. V S.D. B-V S.D. A=3E V-A-M RNOTES

636 104.2 5.5 B8V 9.4 0.6 0.5 0.7 1.8 7.7 350 4 637 102.7 3.4 B5V 10.1 0.4 0.3 0.5 1.4 9.9 960 638 101.0 1.0 B5V 8.9 0.7 0.5 0.9 2.0 8.1 420 639 105.2 6.7 B8V 8.6 0.8 -0.0 1.0 0.3 8.4 480 640 105.6 7.3 B2V 8.6 0.8 0.5 1.0 2.2 8.3 450 641 105.7 7.4 BOV 9.8 0.7 0.1 0.8 1.2 12.1 2630 4 642 103.2 4.0 B2V 9.8 0.5 0.5 0.6 2.2 9.5 780 643 104.2 5.4 B5V 6.9 1.2 0.5 1.4 2.0 6.1 160 644 101.1 1.1 B5V 9.7 0.6 0.5 0.7 2.0 8.9 600 645 105.6 7.2 B8V 10.8 0.5 1.1 0.7 3.6 7.3 290 646 103.6 4.5 B3V 10.4 0.4 -0.0 0.5 0.6 11.3 1810 647 105.6 7. 2 B5V 11.1 0.5 0.3 0.7 1.4 10.9 1520 648 100.4 0.1 B5V 10.1 0.7 1.5 0.8 5.0 6.3 180 649 105.4 6.9 B1V 9.6 0.6 -0.0 0.8 0.8 11.5 2010 650 103.0 3.5 B 1V 9.8 0.5 -0.0 0.6 0.8 11.7 2200 36 651 101.8 2.0 B3V 9.3 0.6 0.3 0.7 1.5 9.3 720 652 101.9 2.1 B3V 6.9 1.2 -0.1 1.5 0.3 8.1 410 653 104.1 5.1 B5V 11.2 0.4 -0.0 0.4 0.5 11.9 2420 654 104.7 5.9 B9V 10.6 0.4 0.4 0.5 1.4 9.0 630 655 102.4 2.7 B1V 11.0 0.4 0.5 0.5 2.3 11.4 1920 656 104.0 4.9 B9V 8.7 0.7 0.4 0.9 1.4 7.1 260 657 103.1 3.7 B8V 10.3 0.4 0.1 0.5 0.6 9.8 920 658 104.7 5.8 88V 9.9 0.5 0.3 0.6 1.2 8.8 580 659 101.7 1.7 85V 9.9 0.5 0.1 0.7 0.8 10.3 1150 4 660 103.8 4.5 B5V 9.6 0.5 0.3 0.6 1.4 9.4 760 4 661 103.8 4.5 B5V 11.2 0.3 0.3 0.4 1.4 11.0 1590 2 662 101.8 1.9 B8V 10.7 0.4 0.3 0.5 1.2 9.6 840 663 105.3 6.6 B9V 11.7 0.4 0. 1 0.5 0.5 11.0 1590 664 103.3 3.8 B2V 10.4 0.4 0.2 0.5 1.3 11.0 1570 665 101.4 1.3 B5I 11 8.6 0.8 0.2 0.9 1.1 10.9 1520 666 105.2 6.3 B5V 9.8 0.6 -0.0 0.7 0.5 10.5 1270 TABLE 13— CONTINUED 1 CD NO. RA 11900) DEC LI I BII SP. V S.D. < S.D. A=3E V-A-MRNOTES

667 21 57.8 54 30 100.5 -0.1 881 11 7.9 1.0 0.5 1.2 1.8 7.6 330 668 21 57.8 54 37 100.5 -0.0 B IV 9.6 0.7 0.2 0.9 1.4 10.9 1520 669 21 57.8 55 3 100.8 0.3 B3V 9.4 0.7 0.2 0.9 1.2 9.7 870 670 21 57.9 61 11 104.4 5.3 B8V 11 .4 0.4 0.2 0.5 0.9 10.6 1330 671 21 57.9 61 17 104.5 5.4 B8V 10.9 0.4 0.5 0.5 1.8 9.2 700 672 21 58.0 60 16 103.9 4.5 B5V 11.3 0.3 -0.0 0.4 0.5 12.0 2530 673 21 58.2 57 1 102.0 1.9 B5V 11 .0 0.4 0.3 0.5 1.4 10.8 1450 674 21 58.2 61 35 104.7 5.6 B8V 10.7 0.4 0.3 0.5 1.2 9.6 840 675 21 58.3 62 47 105.4 6. 5 B8V 11.6 0.5 0.3 0.6 1.2 10.5 1270 676 21 58.3 63 1 105.5 6.7 B3V 10.5 0.5 -0. 2 0.7 -0.0 12.0 2510 4 677 21 58.6 56 56 102.0 1.8 B3V 10.7 0.4 0.4 0.5 1.8 10.4 1200 678 21 58.6 60 5 103.8 4.3 B2V 9.1 0.7 0.3 0.8 1.6 9.4 750 679 21 58.6 60 17 103.9 4.5 B5 11.3 0.3 0.3 0.4 1.4 11.1 1670 2 680 21 58.8 56 19 101.6 1.3 B8V 9.7 0.6 0.4 0.7 1.5 8.3 460 681 21 58.8 57 27 102.3 2.2 B5V 10.1 0.5 1.1 0.6 3.8 7.5 310 682 21 58.8 61 38 104.8 5.6 B9V 10.4 0.5 0.3 0.6 1 . 1 9.1 660 4 683 21 58.9 62 13 105.1 6.0 B3V 10.2 0.5 -0.3 0.7 -0.3 12.0 2510 684 21 59.0 56 23 101.7 1.3 B8V 10.8 0.5 0.2 0.6 0.9 10.0 1010 685 21 59.0 61 17 104.6 5.3 B8V 10.7 0.4 0.2 0.5 0.9 9.9 960 686 21 59.1 61 12 104.5 5.2 B9V 11.5 0.4 0.3 0.5 1. 1 10.2 1100 687 21 59.2 61 48 104.9 5.7 B5V 11.0 0.4 0.2 0.5 1.1 11. 1 1670 688 21 59.2 62 12 105.1 6.0 B8V 11.6 0.4 0. 1 0.5 0.6 11.1 1680 689 21 59.3 61 47 104.9 5.7 B3V 10.5 0.5 0.2 0.6 1.2 10.8 1440 690 21 59.4 59 52 103.8 4.1 B5V 11.2 0.4 0. 1 0.4 0.8 11.6 2100 4 691 21 59.4 60 36 104.2 4.7 B5V 7.9 0.9 -0.0 1.1 0.5 8.6 520 692 21 59.4 62 29 105.3 6.2 B6V 11.0 0.5 -0. 1 0.6 0 . 1 11.7 2160 693 21 59.5 55 31 101.2 0.6 Bl 10.2 0.6 0.6 0.7 2.6 10.3 1150 3 694 21 59.5 57 32 102.4 2.2 B3 7.7 1.0 0.2 1.2 1.2 8.0 390 37 695 21 59.5 63 28 105.9 7.0 B3V 10.3 0.6 0.4 0.7 1.8 10.0 990 696 21 59.5 57 29 102.4 2.2 B5 6.0 1.5 -0.6 2.2 -1.3 8.5 500 38 697 21 59.6 62 14 105.2 6.0 B9V 11.9 0.4 -0.0 0.5 0.2 11.5 2010 TABLE 13— CONTINUED

NO. LI I BII SP. V S.D. B-V S.D. A=3E V-A-M

698 104.4 4.9 B5V 10.1 0. 5 0.7 0.6 2.6 8.7 699 105.1 5.9 85V 9.9 0.6 -0.0 0.7 0.5 10.6 700 103.3 3.4 B8V 10.6 0.4 0.3 0.5 1.2 9.5 701 104. 1 4.4 B5V 11 .1 0.4 0.2 0.5 1.1 11 .2 702 105.5 6.4 B9V 11 .6 0.5 0.2 0.6 0.8 10.6 703 101.3 0.4 B3V 7.6 1.0 -0.0 1.3 0.6 8.5 704 104.6 5.0 B8V 10.8 0.4 0.4 0.5 1.5 9.4 705 105.0 5.7 B3V 10.6 0.5 0. 1 0.6 0.9 11.2 706 105.7 6.7 B3V 9.6 0.7 0.1 0.8 0.9 10.2 707 102.0 1.4 B9V 9.4 0.6 0.4 0.8 1.4 7.8 708 101.8 1.1 B9V 9.6 0.6 0.5 0.7 1.7 7.7 709 105.7 6.6 B5V 8.9 0.8 0. 1 0.9 0.8 9.3 710 101.9 1.2 B3 10.9 0.5 0.2 0.6 1.2 11.2 711 104.0 4.2 B8V 11.5 0.3 -0.1 0.4 -0.0 11 .6 712 105.7 6.6 B2V 9.6 0.7 0.1 0.8 1.0 10.5 713 105.8 6.7 B8V 9.2 0.7 0.1 0.9 0.6 8.7 714 101.4 0.5 B 1V 10.1 0.6 0.2 0.7 1.4 11.4 715 103.8 3.9 B8V 9.2 0.6 0.5 0.7 1.8 7.5 716 105.1 5.6 B8V 11.6 0.4 0.2 0.5 0.9 10.8 717 103.7 3.7 OB 11.1 0.4 0.5 0.5 2.5 14.6 718 103.8 3.8 B9V 10.0 0.5 0.3 0.6 1.1 8.7 719 104.6 4.8 B8V 10.8 0.4 0.3 0.5 1.2 9.7 720 105.0 5.4 B9V 9.7 0.6 0.4 0.7 1.4 8.1 721 105.1 5.5 B2V 10.8 0.5 0.6 0.6 2.5 10.2 722 105.1 5. 5 B8V 10.9 0.5 -0.9 0.6 -2.4 13.4 723 105.3 5.8 B8V 11.5 0.4 0.3 0.5 1.2 10.4 724 102.3 1.6 B8V 10.4 0.5 0.5 0.6 1.8 8.7 725 102.3 1.6 B2V 9.1 0.7 0.3 0.8 1.6 9.4 726 104.1 4.1 B5V 8.2 0.9 0.3 1.0 1.4 8.0 727 105.2 5.6 B2V 8.6 0.8 0.2 0.9 1.3 9.2 728 102.6 2.0 B8V 9.7 0.6 0.3 0.7 1.2 8.6 TABLE 13— CONTINUED

NO. RA (1900) DEC L11 BII SP. V S.D. B-V S.D. A=3E V-A-MRNOTES

72 9 22 1.4 59 22 103.7 3. 5 B5V 7.0 1.2 -0.1 1.5 0.2 8.0 400 14 730 22 1.4 62 59 105.8 6.5 B8V 11.4 0.5 0.1 0.6 0.6 10.9 1530 731 22 1.5 59 21 103.7 3.5 B8V 7.8 1.0 0. 1 1.2 0.6 7.3 290 732 22 1.5 61 31 104.9 5.3 B8V 8.8 0.7 0.4 0.9 1.5 7.4 300 4 733 22 1.5 61 47 105.1 5.5 B8V 11.3 0.4 0.9 0.5 3.0 8.4 480 734 22 1.6 59 35 103.8 3. 7 B8V 9.6 0.5 0.4 0.6 1.5 8.2 440 735 22 1.6 59 25 103.7 3.6 B8V 8.1 0.9 0.2 1.0 0.9 7.3 290 736 22 1.6 58 17 103.1 2.6 B5V 7.7 1.0 -0.1 1.2 0.2 8.7 550 737 22 1.6 61 43 105.1 5.4 B9V 11.4 0.4 -0.5 0.5 -1.3 12.5 3190 738 22 1.8 57 30 102.7 2.0 B 1 10.5 0.4 -0.3 0.6 -0.1 13.3 4610 739 22 1.8 61 17 104.8 5.1 B8V 9.8 0.5 0. 1 0.7 0.6 9.3 730 740 22 1.8 62 55 105.8 6.4 B9V 11.6 0.5 0.6 0.6 2.0 9.4 760 741 22 2.0 62 32 105.6 6.1 B8V 11.0 0.5 -0.0 0.6 0.3 10.8 1460 742 22 2.0 56 45 102.3 1.4 B8V 10.5 0.5 2.4 0.6 7.5 3.1 40 743 22 2.0 62 48 105.7 6.3 B8V 10.3 0.6 0.2 0.7 0.9 9.5 800 744 22 2.0 62 37 105.6 6.2 B2V 8.7 0.8 1.0 0.9 3.7 6.9 230 40 745 22 2.0 61 44 105.1 5.4 B9V 10.7 0.5 0.9 0.6 2.9 7.6 330 4 746 22 2.1 59 13 103.7 3.4 B8V 8.9 0.7 -0.2 0.8 -0.3 9.3 730 4 747 22 2.2 60 40 104.5 4.5 B5V 10.3 0.5 0.1 0.6 0.8 10.7 1390 4 748 22 2.2 56 18 102.0 1.0 B8V 9.9 0.6 -0.1 0.7 -0.0 10.0 1010 749 22 2.3 61 50 105.2 5.5 B3V 10.4 0.5 0.5 0.6 2.1 9.8 910 750 22 2.4 61 55 105.3 5.6 B5V 11.2 0.5 0.4 0.6 1.7 10.7 1390 751 22 2.4 59 5 103.6 3.2 B9V 10.7 0.4 0.4 0.5 1.4 9.1 660 752 22 2.4 60 30 104.4 4.4 B3V 11.1 0.4 0.3 0.5 1.5 11.1 1650 753 22 2.4 60 52 104.7 4.7 B5V 11 .3 0.4 1.1 0.5 3.8 8.7 550 754 22 2.4 62 19 105.5 5.9 B3V 11.1 0.5 -0.0 0.6 0.6 12 .0 2510 755 22 2.5 56 55 102.4 1.5 85 V 10.1 0.5 0.6 0.6 2.3 9.0 630 756 22 2.5 60 41 104.6 4.5 B8V 11.3 0.4 0.4 0.5 1.5 9.9 960 757 22 2.5 61 48 105.2 5.5 B IV 8.6 0.8 0.7 0.9 2.9 8.4 480 758 22 2.6 58 13 103.2 2.5 B8V 10.7 0.4 0.5 0.5 1.8 9.0 630 1 759 22 2.6 60 19 104.4 4.2 B5V 11.3 0.4 0.2 0.5 1.1 11 .4 1920 < TABLE 13— CONTINUED

NO. 0) DEC L11 B11 SP. V S.D. S-V S.D. A=3E

760 56 56 102.4 1.5 B5V 9.9 0.6 0.4 0.7 1.7 761 59 5 103.7 3.2 B9V 9.7 0.5 0.2 0.7 0.8 762 61 41 105.2 5.3 B8V 10.4 0.5 0.2 0.6 0.9 763 61 26 105.0 5.1 B8V 10.9 0.4 0. 1 0.5 0.6 764 57 17 102.6 1.7 B9V 11.0 0.4 0.3 0.5 1.1 765 62 20 105.6 5.9 B5V 11.5 0.5 0.2 0.6 1.1 766 59 32 104.0 3.6 B8V 10.9 0.4 0.8 0.5 2.7 767 59 8 103.7 3.2 B8V 9.8 0.5 0.1 0.6 0.6 768 62 7 105.4 5.7 B8V 11.2 0.4 0.2 0.6 0.9 769 63 28 106.2 6.8 BOV 11.2 0.6 0.2 0.7 1.5 770 57 26 102.8 1.8 B8V 9.4 0.6 0. 1 0.7 0.6 771 57 49 103.0 2.1 B8V 9.3 0.6 0. 1 0.8 0.6 77 2 60 17 104.4 4.2 B3V 10.5 0.4 0. 1 0.5 0.9 773 61 52 105.3 5.5 B5V 10.8 0.5 0.3 0.6 1.4 774 62 52 105.9 6.3 B9V 10.7 0.5 0.3 0.7 1.1 775 56 54 102.5 1.4 B2V 10.0 0.6 -0.0 0.7 0.7 776 57 57 103.1 2.2 B9V 10.5 0.5 0.2 0.6 0.8 777 63 30 106.3 6.8 □ B 8.1 1.0 0.3 1.1 1.9 778 55 50 101.9 0.5 B5V 6.7 1.3 -0. 2 1.7 -0.1 779 62 5 105.5 5.6 B5V 10.4 0.5 0. 1 0.7 0.8 780 63 11 106.1 6.5 B8V 10.2 0.6 0.3 0.7 1.2 781 58 52 103.7 3.0 B8V 9.5 0.6 0.2 0.7 0.9 782 61 25 105.1 5.1 B3V 11.0 0.4 -0. 1 0.6 0.3 783 62 26 105.7 5.9 B9V 10.0 0.6 0.3 0.7 1.1 784 56 41 102.4 1.2 B5V 9.1 0.7 -0.3 0.9 -0.4 785 61 7 105.0 4.8 B5V 10.9 0.4 0.1 0.6 0.8 786 60 9 104.4 4.0 B8V 8.7 0.7 0.2 0.9 0.9 787 56 55 102.6 1.3 OB 10.8 0.5 0.2 0.6 1.6 788 58 13 103.4 2.4 B9V 10.9 0.4 0.4 0.5 1.4 789 60 40 104.7 4.4 B5V 10.8 0.4 0.2 0.5 1.1 790 57 22 102.9 1.7 B3V 10.0 0.5 0.1 0.7 0.9 TABLE 13— CONTINUED

NO. RA C1900) DEC L11 B11 SP. V S.D. B-V S.D. A=3E V-A-M R NOTES

791 22 4.4 58 7 103.3 2.3 B5V 10.8 0.4 0.2 0.5 1.1 10.9 1520 792 22 4.4 59 35 104.1 3.5 B8V 11 .3 0.4 0.6 0.5 2.1 9.3 730 793 22 4.4 60 10 104.5 4.0 B2V 10.4 0.5 0.1 0.6 1.0 11.3 1800 794 22 4.5 57 37 103.0 1.9 B9V 10.4 0.5 0.5 0.6 1.7 8.5 500 79 5 22 4.6 55 50 102.0 0.4 B 1V 9.9 0.6 0.4 0.8 2.0 10.6 1330 796 22 4.6 55 50 102.0 0.4 B 1 10.4 0.6 0.9 0.7 3.5 9.6 830 2 797 22 4.7 63 40 106.5 6.8 B2V 9.2 0.8 -0.0 0.9 0.7 10.4 1190 798 22 4.8 60 37 104.8 4.3 B3V 8.5 0.8 -0.1 1.0 0.3 9.7 870 42 799 22 5.0 63 37 106.5 6.8 B9V 10.1 0.7 0.2 0.8 0.8 9.1 660 800 22 5.0 63 4 106.2 6.3 B5V 10.1 0.6 -0.0 0.8 0.5 10.8 1450 43 801 22 5.0 60 32 104.7 4.2 B3V 9.6 0.6 -0.4 0.7 -0.6 11.7 2180 44 802 22 5.1 57 25 103.0 1.7 OB 10.5 0.5 1.0 0.6 4.0 12.5 3220 803 22 5.1 57 42 103.1 1.9 B3V 10.7 0.5 0.3 0.6 1.5 10.7 1380 804 22 5.1 60 31 104.7 4.2 B 1V 9.5 0.6 0.3 0.7 1.7 10.5 1270 44 805 22 5.2 62 16 105.7 5.7 B9V 7.6 1.0 0.3 1.2 1.1 6.3 180 4,45 806 22 5.2 61 3 105.1 4.7 B3V 10.1 0.5 0.3 0.6 1.5 10.1 1040 807 22 5.3 57 0 102.8 1.3 OB 10.4 0.5 0.9 0.6 3.7 12.7 3530 808 22 5.3 60 40 104.8 4.3 B2V 10.3 0.5 -0.1 0.6 0.4 11.8 2260 809 22 5.3 57 30 103.0 1.7 B8V 10.2 0.5 0.3 0.6 1.2 9.1 660 810 22 5.4 60 34 104.8 4.2 B8V 11.5 0.4 0.6 0.5 2.1 9.5 800 811 22 5.4 60 25 104.7 4. 1 B2V 9.2 0.6 0.1 0.8 1.0 10.1 1030 812 22 5.5 60 37 104.8 4.3 B8V 8.2 0.9 0.1 1.1 0.6 7.7 350 4 813 22 5.6 59 59 104.5 3.7 BIV 10.8 0.4 0.3 0.5 1.7 11.8 2310 814 22 5.8 62 53 106.1 6.1 B8V 11.0 0.5 -0.0 0.7 0.3 10.8 1460 815 22 5.8 58 47 103.8 2.7 B8V 6.2 1.4 0. 1 1.8 0.6 5.7 130 7 816 22 5.8 61 14 105.2 4.8 B1V 9.4 0.6 -0.0 0.8 0.8 11.3 1830 817 22 5.8 63 40 106.6 6.8 B1V 9.0 0.8 0.2 1.0 1.4 10.3 1150 818 22 6.0 60 40 104.9 4.3 B5V 11.4 0.4 0.9 0.5 3.2 9.4 760 2 819 22 6.0 56 19 102.5 0.7 B2V 9.6 0.7 0.4 0.8 1.9 9.6 820 820 22 6.1 60 39 104.9 4.3 B5V 11.7 0.4 0.1 0.5 0.8 12.1 2650 2 , 821 22 6.1 62 50 106.1 6.1 B8V 11.3 0.5 0.3 0.7 1.2 10.2 1110 »< TABLE 13— CONTINUED

NO. 0) DEC L11 B11 SP. V S.D. B-V S.D. A=3E V-A-MR NOTES

822 58 37 103.8 2.6 B1V 10.4 0.5 0.4 0.6 2.0 11.1 1670 823 60 27 104.8 4. 1 B8V 11.4 0.4 0.3 0.5 1.2 10.3 1160 824 56 53 102.8 1. 1 B5V 11.4 0.5 0.4 0.6 1.7 10.9 1520 825 59 43 104.4 3.5 BO 10.4 0.5 0.7 0.6 3.0 10.9 1510 5 826 60 40 104.9 4.3 B5V 12.0 0.4 -0.0 0.5 0.5 12.7 3490 2 827 61 42 105.5 5. 1 B8V 8.6 0.8 0. 1 1.0 0.6 8.1 420 828 57 21 103.1 1.5 DB 10.7 0.5 0.8 0.6 3.4 13.3 4650 829 56 54 102.8 1.1 B5V 10.2 0.5 0.4 0.7 1.7 9.7 870 830 57 32 103.2 1.7 B8V 9.7 0.6 0.3 0.7 1.2 8.6 530 831 61 7 105.2 4.6 B5V 11.4 0.4 0.2 0.5 1.1 11.5 2010 832 57 2 102.9 1.2 B5V 11.3 0.5 -0.9 0.6 -2.2 14.7 8790 4 833 57 2 102.9 1.2 B5V 11.2 0.5 -0.7 0.6 -1.6 14.0 6360 4 834 57 2 102.9 1.2 B5V 10.6 0.5 0.6 0.6 2.3 9.5 800 835 57 2 102.9 1.2 B3V 9.9 0.6 0.4 0.7 1.8 9.6 830 836 63 5 106.3 6.2 B1V 10.5 0.6 0.2 0.7 1.4 11.8 2310 837 59 46 104.5 3.5 B5 10.9 0.4 -0.1 0.5 0.2 11.9 2420 2 838 57 34 103.2 1.7 B9V 9. 1 0.7 0.3 0.8 1.1 7.8 360 839 57 5 103.0 1.3 B5V 10.7 0.5 0.3 0.6 1.4 10.5 1270 4 840 56 38 102.7 0.9 OB 11.3 0.5 0.7 0.6 3.1 14.2 7040 841 58 36 103.8 2.5 B5 10.0 0.5 0. 1 0.6 0.8 10.4 1210 1 842 60 30 104.9 4.1 B8V 9.1 0.7 1.0 0.8 3.3 5.9 150 4 843 56 58 102.9 1.2 B5V 10.0 0.6 0.6 0.7 2.3 8.9 600 844 57 0 102.9 1.2 B8V 10.4 0.5 0.6 0.6 2.1 8.4 480 845 61 26 105.4 4.9 B8V 9.1 0.7 -0.1 0.9 -0.0 9.2 700 846 60 37 105.0 4.2 B5V 11.4 0.4 0. 1 0.5 0.8 11.8 2310 2 847 62 44 106.2 5.9 B3V 10.4 0.6 0.7 0.7 2.7 9.2 690 848 60 56 105.2 4.4 B1V 9.8 0.6 -0.1 0.7 0.5 12.0 2530 849 62 10 105.8 5.5 B3V 9.8 0.6 0.3 0.8 1.5 9.8 910 850 56 53 102.9 1.1 B3V 9.4 0.7 0.2 0.8 1.2 9.7 870 851 61 9 105.3 4.6 B3V 11.2 0.4 0.2 0.6 1.2 11.5 1990 852 59 27 104.4 3.2 B8V 10.5 0.5 0.2 0.6 0.9 9.7 880 TABLE 13— CONTINUED

NO. RA (1900) DEC L 11 B11 SP. V S.D. B-V S.D. A=3E V-A-MRNOTES

853 22 7.3 59 27 104.4 3.2 B8V 9.9 0.5 -0.0 0.6 0.3 9.7 880 854 22 7.4 56 17 102.6 0.6 B3V 10.5 0.6 0.4 0.7 1.8 10.2 1090 855 22 7.4 56 56 103.0 1.1 B8V 10.7 0.5 0.5 0.6 1.8 9.0 630 856 22 7.4 58 59 104.1 2.8 B5V 11.2 0.4 0.4 0.5 1.7 10.7 1390 857 22 7.5 57 38 103.4 1.7 OB 10.1 0.5 1.1 0.6 4.3 11.8 2330 858 22 7.6 58 37 103.9 2.5 B 1 10.8 0.5 0.6 0.6 2.6 10.9 1520 859 22 7.7 62 59 106.4 6.1 B9V 10.4 0.6 0.6 0.7 2.0 8.2 440 860 22 7.7 63 4 106.4 6.2 B2V 8.8 0.8 0.2 1.0 1.3 9.4 750 861 22 7.8 59 10 104.3 2.9 B3V 10.5 0.5 0. 5 0.6 2.1 9.9 950 862 22 7.8 57 9 103.1 1.2 B5V 10.4 0.5 0.5 0.7 2.0 9.6 830 863 22 8.1 56 26 102.8 0.6 B5V 9.9 0.6 0.5 0.8 2.0 9.1 660 864 22 8.5 57 36 103.5 1.6 B8V 10.6 0.5 0.3 0.6 1.2 9.5 800 865 22 8.5 60 39 105.2 4.1 B5V 10.3 0.5 0. 1 0.7 0.8 10.7 1390 4 866 22 8.5 61 8 105.4 4.5 B1V 8.3 0.9 0.2 1.0 1.4 9.6 830 86 7 22 8.6 60 45 105.2 4.2 B 1V 9.4 0.6 0.3 0.8 1.7 10.4 1210 868 22 8.6 62 44 106.3 5.8 Bl 10.3 0.6 1.1 0.7 4.1 8.9 600 3 869 22 8.7 60 15 104.9 3.7 B3V 10.9 0.5 0.3 0.6 1.5 10.9 1510 870 22 8.8 59 49 104.7 3.4 B3V 9.9 0.6 0. 1 0.7 0.9 10.5 1250 871 22 8.9 60 41 105.2 4.1 B2V 10.5 0.5 -0.4 0.7 -0.5 12.9 3760 4 872 22 8.9 56 22 102.8 0.5 B3V 10.7 0.6 1.6 0.7 5.4 6.8 220 873 22 9.1 62 54 106.5 5.9 OB 7.1 1.2 1.0 1.4 4.0 9.1 670 4,46 874 22 9.2 60 49 105.3 4.2 B 1V 10.9 0.5 0.3 0.6 1.7 11.9 2420 3 875 22 9.2 60 49 105.3 4.2 B3V 10.7 0.5 0.8 0.6 3.0 9.2 690, 876 22 9.2 56 46 103.1 0.8 BO 10.1 0.6 1.3 0.7 4.8 8.8 570 4 877 22 9.2 59 59 104.9 3.5 B8V 9.3 0.6 0.2 0.8 0.9 8.5 500' 878 22 9.3 56 45 103.1 0.8 BO 11.0 0.5 0.8 0.6 3.3 11.2 1730 879 22 9.4 59 7 104.4 2.8 Bl ,10.6 0.5 0.5 0.6 2.3 11.0 1590 880 22 9.4 60 52 105.4 4.2 B3V 10.3 0.5 0.2 0.7 1.2 10.6 1310 2 881 22 9.6 58 40 104.2 2.4 B8V 10.0 0.6 0.2 0.7 0.9 9.2 700 882 22 9.7 56 46 103.1 0.8 B3I 9.0 0.7 1.4 0.8 4.6 10.2 1100 4 883 22 9.8 62 15 106.2 5.3 Bl 9.3 0.7 0.2 0.8 1.4 10.6 1330 3 TABLE 13— CONTINUED

NO. RA (1900) DEC L11 Bl I SP. V S.O. B-V S.D. A=3E V-A-MR NOTES

884 22 9.9 62 8 106.1 5.2 B9V 8.5 0.8 0.1 1.0 0.5 7.8 360 885 22 10.0 56 15 102.9 0.3 B9V 9.0 0.8 0.7 0.9 2.3 6.5 200 886 22 10.2 62 44 106.5 5.7 B5I II 6.3 1.4 0.1 1.8 0.8 8.9 600 3 887 22 10.4 62 2 106.1 5.1 B3V 9.0 0.8 -0.0 0.9 0.6 9.9 950 888 22 10.6 57 10 103.4 1.0 B9V 8.2 0.9 0. 1 1.1 0.5 7.5 310 889 22 10.6 57 33 103.7 1.4 B9V 10.3 0.6 0.4 0.7 1.4 8.7 550 890 22 10.9 57 56 103.9 1.7 OB 11.3 0.5 0.4 0.6 2.2 15.1 10660 891 22 10.9 57 27 103.6 1.3 B8V 10.2 0.6 0.3 0.7 1.2 9.1 660 892 22 11.0 57 49 103.8 1.6 OB 10.3 0.6 -1.0 0.7 -2.0 18.3 46550 893 22 11.2 60 16 105.2 3.6 BOV 9.7 0.6 0.5 0.7 2.4 10.8 1440 894 22 11.4 5 9 20 104.7 2.8 B8V 9.6 0.6 0.2 0.7 0.9 8.8 580 895 22 11.6 61 15 105.8 4.4 BOV 8.2 0.9 0. 1 1.1 1.2 10.5 1250 896 22 11.7 56 10 103.0 0.1 BO 10.9 0.6 0.2 0.7 1.5 12.9 3800 4 897 22 11.9 56 23 103.2 0.3 B5V 9.0 0.8 0.1 0.9 0.8 9.4 760 898 22 12.0 55 19 102.6 -0.6 B3V 7.4 1.1 0.2 1.4 1.2 7.7 340 3 899 22 12.3 62 26 106.5 5.3 BO 8.7 0.8 0.1 1.0 1.2 11 .0 1580 15 900 22 12.6 55 7 102.6 -0.8 OB 9.9 0.8 0.8 0.9 3.4 12.5 3220 47 901 22 13.1 55 1 102.6 -0.9 OB 9.8 0.8 1.9 1.0 6.7 9.1 670 4 90 2 22 13.2 58 9 104.3 1.7 BIV 9.8 0.6 0. 3 0.8 1.7 10.8 1450 90 3 22 13.4 58 32 104.5 2.0 B5V 8.4 0.8 -0.2 1.1 -0.1 9.7 870 904 22 13.4 60 25 105.5 3.6 B3V 8.8 0.8 0.4 0.9 1.8 8.5 500 4 90 5 22 13.5 57 50 104. 1 1.4 B9V 9.1 0.7 -0.0 0.9 0.2 8.7 550 906 22 13.7 56 43 103.6 0.4 B2V 9.4 0.7 0.8 0.9 3.1 8.2 430 907 22 14.0 56 41 103.6 0.4 B5V 10.9 0.6 0.4 0.7 1.7 10.4 1210 90 8 22 14.2 56 46 103.7 0.4 B5V 10.9 0.6 0.6 0.7 2.3 9.8 920 909 22 14.5 60 10 105.5 3.3 B2V 9.7 0.6 0.3 0.8 1.6 10.0 990 910 22 14.7 62 47 106.9 5.5 OB 6.4 1.4 1.1 1.6 4.3 8.1 420 1 911 22 14.8 57 2 103.9 0.6 BO 11 .0 0.6 0.3 0.7 1.8 12.7 3460 912 22 14.8 58 15 104.5 1.7 B5V 10.7 0.6 0.3 0.7 1.4 10.5 1270 913 22 14.9 56 38 103.7 0.3 B2V 10.5 0.6 0.2 0.8 1.3 11.1 1640 914 22 15.1 55 25 103.0 -0.8 OB 10.1 0. 8 0.9 0.9 3.7 12.4 3070 2 TABLE 13— CONTINUED

NO. RA (1900) DEC L 11 Bl I SP. V S.D. B-V S.D. A=3E V-A-MR NOTES

915 22 15.4 55 52 103.3 -0.4 Bl 9.6 0.8 0.5 0.9 2.3 10.0 1000 3 916 22 15.6 57 13 104.1 0.7 B5V 9.6 0.7 0.4 0.8 1.7 9.1 660 917 22 15.9 56 30 103.7 0.1 BOV 10.0 0.7 0.4 0.8 2.1 11.4 1900 918 22 16.0 60 31 105.8 3.5 B8V 9.5 0.7 0.1 0.8 0.6 9.0 630 919 22 16.0 58 30 104.8 1.8 BOV 8.9 0.8 0.6 0.9 2.7 9.7 870 920 22 17.3 59 39 105.5 2.7 BOV 8.6 0.8 -0.0 1.0 0.9 11.2 1730

iO O* 97

NOTES TO TABLE 13

1. Double•

2. Classification uncertain? faint image.

3. Classification uncertain? slightly out of focus.

4. Magnitude and color uncertain? measurement influ- ced by neighboring star image or plate defect.

5. Spectrum appears reddened.

6. Classification uncertain? slightly faint image .

7. Double? two B3v stars.

3. Possible emission at \4050.

9. HDE 239506.

10. HD 202107.

11. HDE 239601. 12. Classification uncertain? confused with neighbor

13. HDE 239605? double with No. 180.

14. He X4026 appears unusually strong.

15. Classification uncertain? image out of focus.

16. HD 203266.

17. HDE 239652.

18. HDE 239668.

19. HDE 239673.

20. Member or possible member of Tr 37.

21. HDE 239671. 22. HD 204964. 23. HDE 239683. 24. HDE 239692. to U1 • HD 205510. 93

NOTES TO TABLE 13— Continued

26. HDE 239710.

27. HDE 239733.

23. HDE 239745.

29. Possibly B2c.

30. HDE 239772.

31. BD +54°2629.

32. HDE 239737.

33. HD 203453.

34. Possibly B5ve.

35. HD 207372.

36. HDE 239820. 37. Classification uncertain? confused with HD 209431.

38. HD 209431.

39. Strong Si \4128.

40. Possibly composite.

41. Possibly type 08.

42. Double? HD 210352.

43. Possibly B5e.

44. Double? companion has type 33v.

45. Possibly B5iii.

46. Type 09.

47. Type Of. 99 641-.: __ .. : ' -wto/ ;.**. ^ . b y '&% i 7* *fr%L to6 600 « ^ 4 1 1 ^ * r>«’3L'?Js$ Sf; 4 fi7 . ' 3(^1

4 6 7 - . * ° ™*'-/ #» ^

f *•■ fii ^37^207306^^■537 3Hy2cr73 • r r*&44i f-206k>S

09 (‘ < & ■ > I BM in aj^ew * o e * 2 7 ~ . flO#.‘ S 7 ! 64 6 - 2 ^ i-vm* aaevotsj

; ■207l&0-r»v \J*3 « * r 4 & ■ > » 360 ' ‘ VI* *V •^*^5* & ‘ ■ # & ^ '■■■ • 5W + 60 ' <465

2 X 0 3 9 . ~ « S ~9t9 ‘'903 0^ W I- * jx 'T." 7TI I «4» ^ a ^n'sS<^ r*®' & £ 7 6 V.- .• «*| . . ,»r^ ^ p»73a 991 . :'*L> a . ^ s£| ; ,**- 563fc» ^ •__ L. . ^ rrt, ■a% 9 3 6*fi 9° * \ t flsr \ *A -r . '_■I ■ *'~* .. / «2 55 309w ■ . s__^■ "• • •! 4® .35# “ *■ ~ ? * x% si 35* \ * L

« ® v. ; 5 ^ 3 '23S7/Jr:' ■ .« < % % * # • ['*37 In,1379 ■ > ■■■.:' ••-: Tr37i,W^« 3 7 .&T ./iw m -j „• •'/«' 627 •a®’! . . .-3wv»r . .FtemtE-5 j. s £ b 2S9KT^ 239&i -- w •5® ’ ■•*••. ‘ 360 I ■ 5p ■■'. 2 1 * - 3 0 ” ■•. -^v - 416 T ' jLdiei- 3 6 5 A3» N\ T|"+55" w ->><3 «'^ -^-v-■• • 447 , /3aJ T -5J6 Sff... . . >• '*'*-• • 3*9 ■42t.~ 364\ FIGURE 3

FINDING CHART FOR EASTERN CEPHEUS 0B2 , 3 ^ ^ J?* W * * 1 9 0 - ‘T * •

******6 2 ? .. ^***- S™*2* - 1 Of, 1 5 3 'jger'#S ist \ ^TbixZ^ ^aK * m 3 z*>. i 9 r*t ^ ; X s X A & J S I laM '^9«27 P* ■ • \2» >>/ • W '2Q5S« >' 9^, 5 S O * * ; J Mrt * > • • 33- \ ^ . ^ --- . '■** 2 & •

- 2 0 0 1 9 6 ,2 5 7 2 ‘, Z J9S"!7S

* t f • •;. 2^609 .^3 W 3^; ^22£> ■ i 3(51/ ' Z7S9UH 216 ' 2 W '205 t e a ^ •43X> 3 f:3^ 9 Z ^ 7 0 ’ ' r-ZO, ** **6 :,23990l •N2fl/

P? 156 ,S2 'HO

'.’• ,^K> 2 0 4 li& y. ' 2Z* V^JPy.^302 373 228/ ■<'2/5’

••" ••'• ~2W 3 0 " „ i _ *?5 ; • W ••••• " i ,

FIGURE 4

FINDING CHART FOR WESTERN CEPHEUS 0B2 101

• • r %

T * / • •— 4 6 6 4 3 9 • * • 3 9 3

4 7 0

461 . 4 2 2 4 4 9 •-"44£ • • *• , - f e ^ 4 S .

• 427-.. ;

• • • • § ' ' • •. 2 3 9 7 3 2 • •

•- ' * * * : 2 ^ 2 *•• T f064*2'43T-"42* 2^403 * 460 ■ • ««*- •• • 442-. * \ •.• 4 4 0 " * •. * * *586 454-* * ' .*239724^ . 4 ‘ * 389'-*. 2 3 9 7 2 ? - ^ .' ‘ • o W • 434^* • . * 4 2 4 — •* •

* * . •' •— 4/0 •

; - • .• * * « • • 2 0 6 / 8 3 23972S-^p •' *

FIGURE 5

FINDING CHART FOR TR 37 6/4^, ‘ ‘ •• ' 2 C 0 2 I 8 O ) L •

< > o 7 x

..^99 set 9 .

'779 • . .‘ . * " . / 2 0 5 6 , 3 . ' 7 2 7 • / * ' # • 7f3 • .-752 r/, -7<25 . ' * . .-L?A * ' ' S 9 o / ' $ d o . ® ;• see 749 *'• '' •v:4’87- ' C ‘f* - '• ^ ^ 7 3 3 i 689 . 658. 7 5 7 . ’" 5 9 ! ’ / *74^5 . 762 . 'V- . • . 7 2 0 . *~!~6 8 2 # • • • 763 >*s . 7 ? 2 ) 732 t 589 . . 739 . ^ f 5 ■ 67/

#

FIGURE 6

FINDING CHART FOR REGION OF 19 CEPHEI AND NGC 7160 103

Discussion of errors

The color excesses were computed using the calibration of the intrinsic colors of the early-type stars by Johnson

(19S5)• The absorption was calculated using 3.0 for the ratio, R, of the absolute absorption in V, A^, to the color excess in B-V, (Sharpless 1963).

The standard value of 3.0 was used in preference to the anomalous value of 5.4 which Johnson (1965) adopts in the same region of Cepheus. The reasons for this are the followings Johnson based his use of the value 5.4 on two observational results— the variation of the absorption across the association Cepheus 0B3 (III Cephoi) and UBV and infrared photometry of y. Cephei (M2Ia). Cepheus CBS is a small, compact association heavily involved in emission nebulosity and dust. While anomalous extinction may exist in this small region, it is difficult to see why the region of Cepheus 0B2 should differ from the general galactic field. As to the observations of |i Cephei, a highly lum­ inous, semi-regular variable, the extension to the infra­ red of the photoelectric observations presupposes knowledge of the intrinsic infrared colors, which Johnson obtained by 2 taking the mean of a Scorpii and 6 Lyrae. The results, instead of showing a variation in the reddening law, may indicate features in the spectrum of p Cephei. Further­ more, ji Cephei is seen at the edge of the H II region IC 104 1396, which may influence the infrared observations ancl the corrections for slcv background, or possibly even intro­ duce local anomalous reddening. As a check on the redden­ ing law, the V-Mv observations of the Cepheus stars were plotted as a function of in Figure 7. Little evidence can be seen for a significant deviation from R=3? most of the scatter comes from the dispersion in the distances.

o (0.03) O _

9 -

10

11

R=3 12

13

14 0.4 0 . 6 0.8 1.0 1.20.2

FIGURE 7

V-Mv VERSUS Eb _v FOR STARS

OBSERVED IN CEPHEUS 105

The absolute magnitudes for the early-type stars of classes V, IV, and III were taken from the calibration given by Weaver and Ebert (1964), Their calibration was used in preference to those of Keenan (1953), Blaauw

(1963), or Johnson and Iriarte (1958). Underhill (1966a) has criticized the latter calibration on the grounds that it is based on an unproven assumption that certain early- type stars are members of various clusters whose distance moduli are uncertain by amounts of a magnitude or more.

To some extent, the same criticism regarding cluster mem­ bership may be applied to Weaver and Ebert’s calibration, but their distance moduli for the 35 clusters that they used are expected to be substantially better. For lumi­ nosity classes la, lb, and II, Weaver and Ebert state that their data give no improvement over the earlier calibra­ tions? in fact, they find higher luminosity for class lb than for la. Therefore, for these luminosity classes the calibration of Blaauw (1963) was used? it is essentially that of Johnson and Iriarte (1958). The absolute mag­ nitudes and intrinsic colors that were used in this work are given in Table 14.

The errors in the calculation of the distance moduli and the distances can be discussed with the aid of equation

(4). The distance modulus,p , is given by

P = V - Ay - My = V — R Eg_y — My

= V - 3 (B-V) + 3(B—V)c - My. 10S

TABLE 14

INTRINSIC COLORS AND ABSOLUTE MAGNITUDES

MK T y p e V IV III II lb la

Part A. Intrinsic colors.

os -0.32 -0.32 -0.32 -0.32 -0.32 -0.32 09 -0.31 *-0.31 -0.31 -0.31 -0.29 -0.29 09.5 -0.30 -0.30 -0.30 -0.30 -0.27 -0.27 BO -0.30 -0.30 -0.30 -0.29 -0.24 -0.24 BO.5 -0.28 -0.23 -0.28 -0.27 -0.22 —0.22 Bl -0.2S -0.26 -0.26 -0.24 -0.19 -0.19 S2 -0.24 -0.24 -0.24 -0.22 -0.17 -0.17 B3 -0.20 -0.20 -0.20 -0.13 -0.13 -0.13 B5 -0.16 -0.16 -0.16 -0.14 -0.09 -0.09 BS -0.14 -0.14 -0.14 -0.13 -0.07 : -0.07 B7 -0.12 -0.12 -0.12 -0.12 —0.05 -0.05 B8 -0.09 -0.09 -0.09 -0.07 -0.02 —0 . 02 B9 -o.os -0.06 -0.06 -0.04 0.00 0.00 A2 ----- —— mmmm mmmmmm ----- +0.05 +0.05

Part B. Absolute magnitudes.

OS -5.1 09 -4.0 -5.0 -6.4 -6.0 -6.1 -6.2 09.5 -3.0 -4.7 -6.1 -5.9 — 6...0 -6.2 BO -3.5 -4.4 -5.3 -5.4 -5.8 -6.2 BO.5 -3.2 -4.1 -5.5 -5.5 -5.8 -6.4 Bl -2.7 -3.0 -5.2 -5.0 -5.7 -6.6 B2 -1.9 -3.1 -4.6 -4.3 -5.7 -6.8 B3 -1.5 -2.5 -4.0 -4.6 -5.7 -6.8 B5 -1.2 -1.9 -3.4 -4.4 -5.7 -7.0 BS -0.3 -1.4 -2.7 ---- -5.7 -7.1 B7 -0.5 -1.0 -2.1 -4.0 -5.6 -7.1 B3 -0.1 -0.5 -1.5 --- - -5.6 -7.1 B9 +0.2 -0.1 -0.9 -3.8 -5.5 -7.1 A2 —— ————— -2.9 -5.0 -7.5

The standard deviation; sp/ is then

sp = [s§, + 9£f^B_v j + S^(B-v)o + E®-Vs| + s®]5. (6)

The standard deviations, s, of the various terns were esti- 107 matecl in the following ways for the photoelectric and photo­ graphic photometry and the MK and Schmidt classifications.

The value of 0.3 was talcen for sR from Sharpiess

(1963). The standard deviations in the measured colors and magnitudes from the photoelectric photometry were talcen to be 0.05 magnitude? even if they were twice as large the re­ sult would not change significantly. The standard deviation in the intrinsic colors was implicitly assumed by Weaver and

Ebert (1964) to be about 0.03 magnitude, and that has been accepted here.

It is difficult to assess the uncertainty in the ab­ solute magnitude calibration of the early MIC types. Along the main sequence, the difference in absolute magnitude be­ tween one classification subdivision and the next may amount

to 0.5 magnitude. For a given spectral type, the differ­

ence between one luminosity class and the next may exceed

1.0 magnitude. In the early types, there seems to be an

almost continuous gradation from one luminosity class to

another, and of course there is a continuous gradation in

spectral type. Furthermore, there is some evidence (cf.

Underhill 1966a, 1956b) that the ratios of line strengths

used in the MK classification of 0 stars and luminous B

stars may reflect a parameter in addition to luminosity and

temperature, namely, the state of motion in the atmosphere.

Weaver and Ebert (1964) estimate the absolute magnitude

error in their calibration with respect to the zero-age 108 main sequence is 0.1 to 0.2 magnitude, The larger value is adopted in view of the intrinsic uncertainties.

Substituting- the values adopted for the standard dev­ iations of the various terms into equation (6), the stan­ dard deviation in the distance modulus is estimated as

S p = [0.0025 + 0.0225 + 0.0030 + 0.09e|_v +0.0400J3 = [0.073 + 0.1 E ^ ] * 3.

For a color excess of about 0.5 magnitude, sp is about

0.3 magnitude. For a color excess of about 1 magnitude,

Sp is about 0.4 magnitude. The corresponding error in the distance, r, is given by

sr = (1 +P/5) 10p/5 sp, since

r = 10(1+P/5).

For r = 1000 pc, p = 10, and sr * 300 sp . Considering that Sp = 0.3 to 0.4, the uncertainty in the distance is about 10 to 15 percent at about 1 lepc.

For the Schmidt classification, the error in the abso­ lute magnitude is, of course, larger. One Schmidt classifi­ cation subdivision corresponds to about two MK subdivisions, as indicated by the comparison in Table 5. The slope of the M v , Sp curve is about 0.5 magnitude per MK subdivision, so if an error of ± 1 MK subdivision is made, then the error in Mv becomes

sM (Schmidt) = [s^(MK) + (0.5)ss| (Schmidt)]^*

= [0.04 + 0.25]'^ a 0.54. 10S

Substituting this value in equation (6),

sp = (0.32 + 0.1 E §_V P .

For the distance moduli in Table 11, the errors are thus about 0.6 to 0.7 for color excesses of .5 to 1, and the distance error is about 20 to 25 percent at 1 kpc.

For the photographic photometry, the results of the distance calculations are very insecure. As seen in Table

13, the calculated values of Sy are about 0.3 to 0.6 or more, and the values of Sg_y are 0.3 to 0.3 or more. If the value of 0.4 is talcen for the typical standard dev­

iation in the magnitude of a ninth to tenth magnitude

star, then 0.6 is approximately the standard deviation in

the color. Inserting these into equation (6), we have

sp s (0.16 + 3.27 +0.01 + 0.1 E§_v + 0.2S)^

= (3.73 + 0.1 E§_V P = 1.3.

The corresponding- distance error at 1 kpc is 50 percent.

Star distribution

The photometric distances in Tables 10, 11, and 12

are plotted in Figure 3. The stars with MK types and

photoelectric photometry are shown lay larger filled circles

than those with the less precise measurements. The stars

of luminosity classes la, lb, and II are shown lay larger

open circles, and the BOV and 09V stars are shown by the

largest filled circles. (D -105° NGC ISO-met 7/60 39© Cl isfltr- (ft - Gal. • Z ~ Q 42 • 75 3 0 3 9 2.8 2232, t © 52 25 tn • y * - 100° © 33 f Sun 07 4 1 3 *■ - a4 ’eo 77 — Long.

- 95° RMS Distance Errors: ^5 kgc 1 kpc

10'

GROUP A' GROUP B X Ga1, • 61 3 6 — 5 ° fQCesp •69 • 200 400 600 800 1000 1200 1400 r (pc) 9 class JT, Tables ltS~!2 Q Classes CSr-TT 9 class Table. K> (T) Composite % O OSYSrBOV X D Ctass nr Q C luster

FIGURE 8

SPACE DISTRIBUTION OF STARS IN TABLES 10, 11, AND 12 Ill

Figure 0 reveals considerable spread in the distances of the stars considered by various authors to be members of the association. This is a familiar result of photo­ metric observations of associations (see, for example, the

discussion by Petrie and Stromgren in Eg-gen and Herbig

[1964]). In this investigation, the dispersion in the

photometric distances resulting from error in the luminos­

ity calibration has been somov/hat reduced by the use of

Weaver and Ebert*s (1964) improved calibration for the

lower luminosity classes. The luminous giants and supcr-

giants are on a separate system, and the two calibrations may not be consistent with each other. Future changes in

the calibrations may shift the two groups of luminous and

main sequence stars with respect to each other, but sub­

stantial alterations in the relative positions of the stars

in each group are not expected.

Photometric errors cannot account for the dispersion

in distances revealed in Figure S. iis the preceding dis­

cussion hcis attempted to show, uncertainties in the lumi­

nosity calibration, the MK classification, and the photo­

electric photometry result in a standard deviation of only

about 15 percent at 1 kpc. Because of the range in color

excesses, the use of R s 5 . 4 instead of R = 3 for the ratio

of absolute to selective absorption gives even greater

dispersion in the distances. 112

An attempt was made to account for the effects of duplicity in the cases where the stars are known to he spectroscopic binaries. The maximum effect in the distance modulus for undetected binaries is about 2.5 log 2 =0.8 for two components of equal brightness. If one of the components is fainter and redder, the net effect on the distance modulus would be less. On the other hand, if the system is significantly evolved, as many close binaries are, it is expected that this would be reflected in the spectral classification.

From the above arguments the dispersion in distance must 1x5 accepted as real. Figure 0, however, does not include all the stars in the region lout represents a selec­ tion made according to the criteria listed in Chapter II.

In order to obtain a picture of the total star distribution, the results of the Schmidt survey and photographic photo­ metry must be used. The survey covered the area of about

100 square dagreos enclosed by a curve drawn about 1 degree outside the boundary of the bright stars assigned to the association.

In view of the uncertainties in the photometric dis­ tances, it was felt to be more meaningful to group the data together. The photometric distances in Tables 10 through 13 were divided into intervals of 200 pc. It was necessary to include the photoelectric measurements along with the photographic measurements because the photoelectric 113 measurements were used for the standards in the photographic reduction. ‘The spectral classifications were divided up according to the natural groups of the Schottland Schmidt telescope (Figure 2)s OB (including stars of classes I and

II) and BO, Bl and B2, B3 to B6, B7 to BS. The numbers appearing in each spectral group at each distance interval were divided by the volume of the interval to obtain an observed star density. These densities are g-iven in Table

15 and Figures 9 and 10.

TABLE 15

OBSERVED STAR DISTRIBUTION

OB-BO B1-B2 B3-B6 B7-B9 r Vol. No. Dens, No, Dens, No. Dens, No. Dens, (10~5 (hpc) d o - 5 (10-5 (10^ pc3 ) pc”3 ) PC ) pc"0 ) pc-0)

0-0.2 0.00 0 0 1 12.5 3 37.5 17 212.5 0.2-0.4 0.57 1 1.0 9 15.0 21 35.1 69 121.0 0.4-0.6 1.54 6 3.9 26 16.9 34 27.9 92 60.9 0.6-0.a 3.00 0 2.7 20 9.3 53 29.7 67 22.4 0.0-1.0 4.95 16 3.2 22 4.5 63 12.5 40 7.0 1.0-1.2 *7/ • ou O o . oO 1.1 31 4.2- 54 7.3 21 2.9 1.2-1.4 10.3 0 0.0 22 2.2 35 3.4 6 0.6 1.4-1.6 13.7 12 0.8 10 0.8 26 1.9 12 0.9

Expected dens. 0.7 2.5 12.0 00.0

Also given in Table 15 and shown in Figures 9 and 10

are the expected numberr which would be observed if there were a uniform distribution of such objects around the sun.

These values were taken from the compilation of Allen (1963), 114

OB-BO B1-B2 B3-B6 30 B7-B9 Star Density 20 v - 6 .-3

10 Expected

r (kpc) FIGURE 9 OBSERVED STAR DENSITY VS. DISTANCE FROM THE SUN

OB-BO B1-B2 100 B3-BS B7-B9 Star Density

10 L _ - Expected L _

0.2 0.4 0 . 6 0.8 1.0 1.2 1.4 1.60 r (kpc) FIGURE 10 OBSERVED STAR DENSITY VS. DISTANCE FROM THE SUN (LOGARITHMIC DENSITY COORDINATE) 115 divided into type and luminosity according to the natural groups and the MK luminosity calibration in Table 14, For the earliest types this compilation may loe misleading since the area around the sun has a nonuniform distribution of these stars. They are found almost entirely in the spi­ ral arms which they define, and it is across such a spiral arm that we are looking. Nevertheless, this is the only comparison available. The numbers of stars on which the observed densities are based is small, particularly for the early-type stars and for later-type stars in the distance intervals far from the sun. The statistical fluctuations which may be expected range from as much as 50 percent in the cases just mentioned

to about 10 percent.

Despite these uncertainties, Figures 9 and 10 show

that the density of OB stars and stars of types earlier than

B3 significantly increases across the spiral arm from about

300 pc to 1200 pc. Almost all of the OB and B0 stars in

the figures have MK types and photoelectric photometry?

this is also true of roost of the B1-B2 stars closer than

GOO pc. For B1-B2 stars farther away, the diagram shows a

lower concentration than that which actually occurs because

the Schmidt classification tends to assign earlier types,

and this results in larger distance moduli. In addition to

this effect, interstellar absorption reduces the apparent

density of these stars at the larger distances. 115

The plot of observed densities for the stars in groups

B3-BG and B7-B9 shows strong effects of absorption and the low intrinsic brightness of these stars. If the absorp­ tion wore uniform and amounted to 2 magnitudes in V per kiloparsec, then beyond GOO pc one would expect to see no more BO stars and beyond 1000 pc no more B5 stars brighter than the survey limit of about B = 11.5. -actually, the ab­ sorption is irregular in this direction, and a logarithmic decrease is seen almost from the beginning for B7-BS stars and from GOO pc on for B3-BG stars.

It is interesting to note, although it may not be statistically significant, that an increase of 20 to 30 3 stars per 10 pc above the logarithmic decrease occurs in the B7-B9 stars across the spiral arm, and that the ob­ served distribution even near the sun is higher than the expected value in this direction. However, the main feature of the plot of B7-B9 stars is that it shows little concen­ tration toward the spiral a m . This is to be expected from considering that the ago of these stars allows considerable diffusion from their point of origin, even if that point is in a spiral arm.

In Figures 8, 9, and 10, two concentrations of early- type and luminous stars are seen. One, denoted Group A, is centered at 500 pc, and the other, denoted Group B, is centered at 900 pc. The significance of these groups is examined in the Conclusions section. 117

Clusters

NGC 7160

The H-R diagram for NGC 7160 is given in Figure 11.

o 1 o 2

ZAMS for V-Av-Mv ss 9.6 o4

o 11

10 o MK types 16 o Schmidt types 19 o % 17 11 Star numbers from Hoag et al (1961) 12 BO B1 B2 B3 B5 B6 B7 B8 B9 AO

FIGURE 11

H-R DIAGRAM FOR NGC 7160

The seven brightest stars have MK types? the others have

objective prism classification. in order to have con­

sistent photometry, Johnson*s measurements in Hoag et al

(1961) were used for all the stars. 1 1 8

The distance to NGC 7160 was found by Johnson et al

(1961) to he 340 pc. No evidence for a different distance could be seen in the combination of MIC classification of

the seven brightest stars with the photometry. Of the seven

stars, one is evolved, one is a W UMa binary system, one is

a double-line binary, one shows some evidence of peculiarity,

and one spectrogram was inferior. That leaves only two nor­ mal stars with good spectra, and the mean distance from

these was 350 pc.

If this distance is accepted, and if the assignment of

stars to the cluster by Hoag et al (1961) is accepted, then

the following conclusions can be drawn regarding some of the

members. Star No. 1, HD 203218, was classified BlIII-II in

this work, BlIIIs by Morgan (1953). If the intrinsic color

B-v = -0.26 can be accepted, and using R = 3, then the abso­

lute magnitude is Mv =-4.4, which corresponds more to class

IV-III. Star No. 2, HD 203392, was classified BlVn here and

BlIVs by Morgan (1953). It was found by Lynds (1959) to be

an eclipsing binary of extremely short period 20*1. He

thought the system was composed of two B2 stars in contact.

With the same assumptions as for star No. 1, the absolute

magnitude for two components of equal brightness is Mv =

-3.3, which would correspond approximately to B1IV by

Weaver and Ebert's (1954) calibration. 119

Star No. 4, BD +61°2213, was found to be a double­

line spectroscopic binary from three spectrograms. It was observed three times because the first spectrogram seemed

to have poor definition (a result of the two sets of lines), and the second was interrupted by clouds. The Julian dates

of the observations and observed velocity differences in

the sense brighter - fainter were 2439375.73, -235 km/sy

2439379.86, 0 km/s? 2439380.71, -210 km/s. The velocity

of the system cannot be completely determined, but it ap­

pears to be about -30 km/s. Many periods for the orbit

are possible from these data, but periods longer than about

5 days seem to be excluded. On the other hand, extremely

short periods can be ruled out because the axial rotational

velocity of the primary, which seems to be a normal B3V

star, seems to be only slightly greater than rj Aurigae,

which has been estimated by Slettebak and Howard (1955)

as v sin i =125 km/s. In view of the fairly large ob­

served velocity differences, the lino of sight probably

is close to the orbital plane. It may therefore be possi­

ble to observe eclipses in this system. Spectroscopy with

higher resolution can provide accurate spectral classifi­

cations because the lines become well separated and the

brightness difference is not great. The combination of

these circumstances might make it possible to add another

point to the mass-luminosity diagram. 120

Star No. 7, BD +61°2213, appears excessively blue in the color-magnitude diagram (Hoag et al 1961). It has sharp lines, and the He lines may be slightly weak, but not enough to warrant calling it peculiar.

Trumoler 37 The H-R diagram for Tr 37 is shown in Figure 12. The

o MK type+p.e. UBV o Schmidt type+p.e. UBV • Schmidt type+p.g. BV

ZAMS for V-Av-Mv = 9.64

10

11 OS 08BO 31 B2 B3 B5 BS B7 B8 B9 Spectral Type

FIGURE 12

H-R DIAGRAM FOR TR 37

distance modulus of 9.64±0.11, corresponding to 350 pc, was

found from the following stars with MK types and good photo­

metry s HD 205943| 206183; 20S267A, G, and D? HDE 239710?

239725/ and 239729. Weaver and Ebert*s (1964) main sequence 121 has been drawn in for this distance modulus. The stars in

the diagram are noted as members or possible members of Tr

37 in Tables 10, 11, 12, and 13? they include stars of early

type within a radius of 1.5 from HD 206267, which is the

area covered Joy IC 1396. As is expected from, the discussion in Chapter II, the

points obtained from the objective prism classification

fall generally below the main sequence curve drawn for the

stars with MK types. The classification errors resulting

from any defects in the images or peculiarities in the spec­

tra tend to favor earlier types. An apparent exception is

seen in the types B8 and B9? these stars, however, are

mostly foreground objects.

The two distant stars, HDE 239727 and 239724, are seen

right through the center of IC 1396. EDS 239724 appears to

be in the Perseus arm at 3 kpc? HDS 239727 appears to be at

5.7 kpc, but its distance modulus is uncertain because it

is based on photographic photometry. Star No. 441, BOv,

also apparently belongs in the Perseus arm with these stars.

At that distance, these stars are 200 pc above the galactic

plane.

Possible new clusters

As Blaauw (1964) has pointod out, small clusters of

recent origin are found in the nearly associations Orion

OBI and Perseus 0B2, and more small clusters may be expec- 122 ted to be found in the more distant associations such as

Ceplieus 0B2. Several groups of stars wore noticed during the classification of the Schmidt plates that warrant dis­ cussion and further investigation, although they may not be exactly the type of cluster that Blaauw had in mind.

The name of "spectroscopic cluster" has been suggested for such groups,

One such cluster is centered around 19 Cephei, HD

209975, The members are listed in Table 16, In addition

TABLE 16

19 CEPHEI CLUSTER MEMBERS

NO. Sp. V V-A-M No. Sp. VV-A-M

687 B5v 11.0 11.2 733 B3v 11.3 3.3 689 B3v 10.5 10.7 737 B9v 11.4 12.7 716 B3v 11.6 10.8 745 B9v 10.7 7.3 721 B2v 10.3 10.3 749 B3v 10.4 9.3 7215 B3v 9.8 9.5 750 B5v 11.2 10.7 722 B8v 10.9 13.5 757 Blv 3.7 3.5 727 B2v 3.6 9.3 773 B5v 10.3 10.7

to the 09.51b supergiant, there are one Blv star, two B2v stars, three B3v stars, and several B5v and B8v stars.

The cluster can be seen in Figure 6, Its dimensions are about the same as those of NGC 7160, but the number of stars is smaller and their concentration toward the center is less. The mean corrected distance modulus of the clus­ ter is 10,0±0,3, the same as that of 19 Cephei. 123

An apparent cluster was also noticed near the galac­ tic plane at l11 =103°, bX I =l°3. Its possible members are listed in Table 17.

TABLE 17

MEMBERS OP ANONYMOUS CLUSTER AT 22h 07m , +57°10'

■ . . No. Sp. VV-A-M No. Sp. V V-A-M

324 B5v 11.4 10.3 S39 B5v 10.7 10.5 329 B5v 10.2 9.9 343 B5v 10.0 3.7 332 B5v 11.2 14.3 s 844 B3v 10.5 3.5 333 B5v 11.2 14.0 s 850 B3v 9.4 9.6 834 B5v 10.5 9.6 355 B3v 10.7 9.0 835 B5v S.9 9.5

Of this group, 832, 833, 834, and 835 make an espec­

ially striking configuration. Otherwise, on direct photo­

graphs the group would entirely escape notice, particularly

when compared to such a concentrated cluster as NGC 7235,

less than half a degree away. On the objective prism plates,

however, the entire group stands out as a small concentra­

tion of stars that all have almost the same magnitude and

spectral type. The corrected distance modulus of this clus­

ter is 9.S ± 0.24, which puts it at the same distance as NGC

7150 and Tr 37. Another apparent cluster appears around HD 210478,

B1V. The members are listed in Table 18. 124

TABLE 13

MEMBERS OP CLUSTER NEAR HD 21047S

No. . Sp. V V-A-M No. Sp. V V-A-M

739 B5v 10.3 10.8 811 B2v 9.2 10.2 793 B2v 10.4 11.3 313 B5vs 11.4 9.4 793 B3v 3.5 10.5 820 . B5vs 11.7 12.2 301 B3v 9.6 11.7 323 B3v 11.4 10.3 804 Blv 9.5 10.3 326 B5vs 12.0 12.9 308 B2v 10.3 11.9 846 B5vs 11.4 11.8

This is a more dispersed grouping than that around

19 Cephei, and there are several foreground stars that give

it a misleading appearance on direct photographs. The cluster is shown in Figure 3. The little group of the pairs 801 and 804 is quite striking and looks very much

like a physical association. The corrected distance mod­

ulus of the cluster is 11.1±0.3. Using Hiltner*s (1956)

data, the true distance modulus of HD 210478 is 9.0, and

it therefore appears to 1x2 a foreground object.

Several stars are seen around HD 202214, BOV, in the

center of the H II region number 129 in Sharpless*s (1959)

catalogue. The group includes HDE 239595, B3v, and pos­

sibly 167, Blv. There is also a grouping of fainter stars

right around HD 202214, but their spectral types could not

be determined. The H II region itself is notable for the

evident interaction with gas concentrated toward the galac- 125 tic plane. Prom the photometric distance of 400 pc to HD

202214, the H II region has a diameter of about 10 pc.

It has the appearance of a shell, and it is considerably brighter and thicker and closer to the exciting star on the side toward the galactic plane. On the opposite side, the shell is very faint and extends farther from HD 202214.

The appearance suggests that the shell of gas was heated by the BOV star and expanded, sweeping up neutral gas in its path and slowing down on the side tov/ard the galactic plane# and dispersed freely upward on the other side.

Motions

Radial velocities

Fifty-five of the stars with photometric distances in

Tables 10, 11, and 12 also have published radial velocities, cither in the General Catalogue (Wilson 1953) or in the list of Petrie and Pearce (1962). These values are summarized in Table 19, where the source is indicated by a W for Wil­ son and a P for Petrie and Pearce, and they are plotted in

Figure 13.

In order to properly interpret the radial velocities, a correction must be made for the solar motion and the gal­ actic rotation. From the analysis by Delhaye (19S5), the solar motion relative to the local standard of rest is

16.5 km/s in the direction I1 1 »53°, b1 1 =25°. The compo­ nent of this motion in the direction l1 1 =100°, b1 1 »5°, is 126

TABLE 19

STELLAR RADIAL VELOCITIES

No. HD/BD vr Stcl. Dev. Qual. Source Notes 1 193395 -23 ±- 4.2 P 2 199303 -23 ± 0.5 P 3 199661 -19 c W 4 200357 -14 c W 5 202214 -16.2 b w 6 203025 -17.2 b w 7 203333 -2 0 . 6 b w 3 203374 - 7 c w 9 204116 -23 ± 9.1 c P,W l.,2 . 1 0 204150 -24 ±10.7 cl P,W 1.(3. 1 1 204327 + 2 0 ± 7.3 p 1 . 1 2 205139 -14.5 b w 13 205196 -14 c w 14 205943 -19 ± 0.7 p 15 206165 -13.2 b w 16 206133 - 4 G w 17 206267 - 7.8 a w 2 0 206327 -30 c w 2 1 206773 - 2 2 c w 2 2 206936 +19.3 a w 23 207017 -32 ±20.3 p 1 . 24 207198 -18.4 b w 25 207260 -20.3 b w 26 207303 - 2 1 ± 3.0 C P,W 4. 27 207533 -14.6 b w 23 207951 + 3 e w 29 203106 - 1 ±10.3 e P,W 1. / 5. 30 203135 - 2 2 ± 6 . 0 G P.W l.,6 . 31 203218 -21.3 b w 32 208266 - 1 2 -1 2 . 6 p 33 203392 -25.7 b w 7. 34 208440 -14 d w 35 203501 -15 c V7 36 203816 -13.7 a w 37 203905 - 2 0 c w 33 209339 -2 0 . 2 b w 39 209454 -17 c w 40 209481 - 1 1 c w S. 41 209744 -17.4 b w 42 209975 -1 2 . 8 a w 43 210339 -74 c w 44 239581 -17 ± 3.5 p 45 239618 ■■ oO ± 3.7 p 127 TABLE 19— -Continued

No. HD/BD vr Std. Dev. Qual. Source Notes 46 239626 -19 d W 47 239712 -25 ±15.1 P 1 . 50 239729 - 6 ± 4.3 P 51 239743 - 1 0 ± 2.3 P 52 239758 + 1 1 QW 54 +61°2213 -25 d W S. 55 +61°2215 -34 d W 59 239595 - 1 1 ± 5.3 P 63 239676 T. O ± 1.5 P 1 0 . 65 239689 -15 ± 4.1 P 1 1 . 71 239748 - 2 0 ± 1 . 6 P 76 239671 -IS ± 5.1 P

NOTES TO TABLE 19

1. Variable radial velocity according to Potrie and Pearco (19G2).

2. Moan of -23 (W) and -34 (P).

3. Moan of -37 (W) and -11 (P).

4. Moan of -23 (W) and -13 (P).

5* Weighted moan of -24 (W, weight 1) and +3 (P, weight 5), weighted lay the number of measurements.

6 . Weighted mean of -IS (W t weight 1) and -24 (P# weight 5), weighted by the number of measurements.

7. Eclipsing binary.

0. Double-line binary (Petrie 19G5). '

9. Double-line binary.

10. Soctroscopic binary (Petrie and Pearce 1962).

11. Variable radial velocity? (Petrie and Pearce 1962). +20 & l l (322 Std. I IDev. +10 6 6oO 5 2 D C B A O Q & 3 vr Quality km/s

Velocity 29 of Galactic Rotation Tr 37 NGC 7160

*3 6^0 Q 7 ^ <*> o 2 4 -20 * o 3 6'26 3 7 O . °7/ q < $ O/o

Q 0 2 5 'S ? t?4) lt») f * * Q l O -30 X 200 400 600 800 1000 1200 r ^J.400

FIGURE 13 128

RADIAL VELOCITY VS. DISTANCE FOR STARS IN TABLE 19 12S 10.2 Ion/s. Since the region is close to the sun, the velocity of galactic rotation can he computed from the

Oort formula

v = A r sin 2 l11.

The value of 15 lem/s for A has been adopted lay Schmidt

(1965). The line representing the correction for solar motion and galactic rotation has been plotted in Figure

13. A point on this lino represents a star which is talc­ ing part in the galactic rotation with no other motion.

There are several sources of error in the points that are plotted in Figure 13. The errors in position have al­ ready been discussed. The errors in the observed veloci­

ties may result from errors in measurement or variation in

the radial velocities of the stars. Peatrie (1963) found

that about half of the stars of the spectral types repre­

sented in the figure show variation due to their binary

nature. Some of these have been detected, as noted in the

table. Stars in the General Catalogue are noted, as bina­

ries only in the cases where orbits have been calculated.

The weights of the observed velocities, or qualities, were

assigned by Wilson on the basis of the dispersion in the

observed velocities and the number of observations. These

weights are reflected in the figure by the size of the cir­

cles representing the points.

As pointed out by Petrie (1963), there are several

sources of systematic error in the radial velocities of the 130

B stars in the General Catalogue. In the first place, there are differences amounting to 3 to 5 Ian/s between the observatories contributing radial velocities. No correc­ tion for this was applied by Wilson for the B stars. Sec­ ondly, there appears to be a systematic error in reducing the B-star velocities to an absolute system. The bright

B stars seem to require a correction of about -3 Icro/s.

This would remove most of the so-called K-term, which is an apparent general velocity of recession of about 5 km/s observed for the brightest B stars. Neither of these cor­ rections have been applied to the points in Figure 13, how­ ever, because only a few of the stars represented there are in the category of bright stars. A final correction should be considered— the gravitational redshift. This is equal to 0.634 (M/M®)/(R/R«) Jon/s, or about 1 Icra/s for the most massive stars shown here. This can be neglected in compari­ son with the other errors.

Proper motions

The addition of photometric distances has an important effect on the proper motions that Artiulchina (1954, 1956) compiled for 61 stars in the region of Cepheus 0B2, because it allows correcting the proper motions for the solar mo­ tion. The combination of the reflex of the solar motion and the galactic rotation results in a vector of almost con­ stant magnitude that only changes from 020030 per year to 131

Oi'0035 per year between 400 pc and 1400 pc, but whose direction changes by more than 70° from almost perpendicu­ lar to the g-alactic plane at 400 pc to almost in the plane at 1400 pc, When this resultant is subtracted from the ob­ served proper motions to remove the effects of galactic rotation and solar motion, the pattern of expansion claimed by Artiukhina (1956) tends to disappear, and the proper mo­ tions more often than not are reduced to a magnitude smaller than their standard deviations,

•Hie subgroups of stars with common proper motion that

IChorosheva (1955) selected from Artiukhina * s (1956) proper motions are found to lie generally composed of stars at vari­ ous distances. Consequently, not only is the significance of the subgroups lost, but also because of the galactic rotation and solar motion the proper motions become un­ aligned, This extends Kopylov’s (1953) criticism based on 19 stars with photometric distances to 49 stars with photometric distances from MIC classification and photo­ electric photometry.

Radio Observations

The Ohio State University 260-foot radio telescope was used to survey the zone between declinations +55° and

+60° in July, 1966, The survey was conducted for objects

located at high galactic latitudes, and the sensitivity was high. Consequently, when the telescope beam entered 132 low galactic latitudes, the recordings on the multi-chan­ nel hydrogen-line receiver frequently went off scale. Ad­ justments of the zero points wore often made, but some­ times the intensity exceeded the amount which the adjust­ ments could accomodate. Even when they were effective, the base line was often lost. For this reason, observations made in one part of the region of Cepheus 0B2 cannot be com­ pared with those in adjacent parts, even at the same decli­ nation. Nevertheless, some general observations can be made.

Substantial amount of hydrogen are seen in the region of

Cepheus 0B2, with radial velocities corresponding to those of the stars in this direction. There is more neutral hydrogen above the galactic plane than below the galactic plane. Lindblad*s (19S5) results show the same feature, which is peculiar to the region of Cepheus 0B2. It was also reported lay Dieter (19G0). The beam size of the Ohio

State University radio telescope is 10* lay 40*, and because of this high resolution, it can be seen that the distri­ bution of neutral hydrogen is far from uniform. This is not surprising since the spiral a m has considerable thicJcness, and one would expect to encounter discrete clouds of hydrogen. With one exception, discussed below, no cor­ respondence was apparent between the optical features and the radio features. At tlio position of IC 1396, a concentration of neutral hydrogen was seen with the same radial velocity as found by

Courtes (-19G0) for the ionised gas. The H I concentration was somewhat larger than the dimensions of the H II region, and the intensity was higher at the outer edges. This sug­ gests the possibility of a shell of neutral hydrogen sur­ rounding the ionized region. Unfortunately, useful obser­ vations were made only at a declination of +57° and were off scale at +56° and +58°, so this possibility cannot be fully examined. If such a shell exists, it has considerable vari­ ations in the distribution of gas. This would be in accord­ ance with the optical and radio continuum appearance of IC

139G (Lynds 1961).

Conclusions

The structure of Cepheus 0B2

The stars assigned to Cepheus OB2 by Morgan, Whitford,

and Code (1953) and Marharian (1953) are distributed over a

considerable distance across the Cygnus-Carina spiral arm.

It is not possible to regard all these stars as one physical

group. Tiro concentrations, however, may be present, as

pointed out above at the end of the Photometric Distances

section and as indicated in Figure 3.

The nearer concentration. Group A, contains four BOV

stars, HD 202214 at the center of the H II region Sharp-

less 129, HD 203374, HD 204327, and HD 207533. The 06f 134 star X Cephei that appears here cannot be regarded as origi­ nating here? its radial velocity of -74 km/s makes it a

"runaway star" from somewhere in Group B. In an interval of 1 0 ^ years from the time it received that velocity, it would have moved about 500 pc from its point of origin, which might have been in the region of NGC 7150 or possibly

Cepheus 0B3. Judging from Artiukhina's (195S) proper mo­ tions, \ Cephei did not originate in IC 1396, Other lum­ inous stars in Group A are HD 200057, B3III? HD 203330,

BlsV+MlepIb; HD 206165, B2lb? and HD 200501, B3Ib. The

H-R diagram of the stars in Group A is given in Figure 14.

A -

5 - V-Ay

6 -

7 - 88

06 08 • 09 B0 Bl B2 - B3 B5 BO Spectral Type

FIGURE 14

H-R DIAGRAM FOR STARS BETWEEN 350 AND 700 PC

Since the V magnitudes were corrected for absorption, the

H-R diagram represents the same information as Figure 8 . 135 The more distant concentration, Group B, contains the clusters Tr 37, in the H II region IC 1396; and NGC 7160, which v/ere regarded by Markarian and Ambartsumian as nu­ clei of Cepheus 0B2, Two additional small clusters in this region were revealed by the Schmidt survey* the cluster around 19 Cephei; whose earliest member; aside from the su­ pergiant; is Blv; and the cluster at 22*107m , +57°10', whose earliest member is B3v, Tr 37 and NGC 7160 contain many stars of early type. The other luminous stars in the region are HD 2C5139, Bill; HD 207193, 09,511; HD 209339, B0IV;

HD 209481, 09V; and HD 209975 (19 Cephei), 09.51b. The

M2Ia supergiant (j Cephei appears to be in this region, but its radial velocity of +19,3 km/s indicates that it origi­ nated elsewhere in the Galaxy. It is conceivable that \>

Cephei also belongs in Group B, If its absolute magnitude were -7 instead of -7,5, its photometric distance would be

950 pc. The H-R diagram for Group B is given in Figure 17,

The appearance on the sky of Groups A and B is shown in

Figures 15 and 16,

Group B has most of the characteristics of the OB associations in the solar neighborhood (cf. Blaauw £1964]),

The projected dimensions are about 110 by 95 pc. The depth is about 300 pc; which may be exaggerated by errors in the photometric distances. The more dispersed parts of the group are more evolved than the concentrated clusters.

The cluster NGC 716o; which appears quite devoid of inter- 136

9 ° i i r n r ~ ] ------1 1------1------1------1------r

8° £3 JS /O0 .30 * O 4 5 7 ° • 0 2 6 0 6 2 0 6 ® 2 © 6° 63 0 (J)7 II 03/ * 2 9 37 *7/ • « * 5° • • 0 3 2 % Z 7 % 7 4 68 4° 2/0 i • BT-TZ- '58 * 4 / # O-BOY 3° o r-n ©43 Comp. 2° (D J .1 . I J L J L 104® 102® 100® 98® 96®1II94<

FIGURE 15

APPEARANCE ON THE SKY OF GROUP A

8® r T 24 7® - 7 6 O' .20 NGC 0 / 2 O 7/60 • 6 3 6 ® > 3 8 19 Cep 5® Clustek. 67 -65 JI •• 4® 1396 ffl-TT 3® • •53 % 0 - BO i-n 2 ® A n o n . o CLUSrEK ^ n . o Cluster 1 ® l— L_T_ _L JL J_ 104° 1 0 2 6 TOO® 98® 96 ® ^ i i 94 ®

FIGURE 16

APPEARANCE ON THE SKY OF GROUP B 137

10 OG 09 BO B1 B2 B3 B5 BS AO A2 Spectral Type

FIGURE 17

H-R DIAGRAM OF STARS BETWEEN 700 AND 1000 PC stellar matter, is more evolved than the cluster Tr 37, which contains the trapezium system HD 206267 and is im­ mersed in the extensive, evolved, H II region, IC 1396.

The 06f star \ Cephei appears to he a runaway star from this region. The integrated absolute magnitude of the group is about -9 and the mass of stars earlier than B3V is in excess of 103. If the term OB association is to be re­ stricted to physical groupings of stars close together in space, which does not now seem to bo the case (cf. Kopylov

[19533), then it is suggested that the name Cepheus OB2 bo reserved for the stars in Group B at 900 pc. Some of the characteristics of an OB association are also shown by Group A. Three of the four BO stars are ap­ parently within 50 pc of each other, and one of them, HD

202214, is at the center of a shell-lil:e H II region and seems to be surrounded by several fainter stars. The to­ tal mass of this system around HD 202214 is less by several orders of magnitude than that in IC 139S, whoso mass of luminous gas was found to be 5300 solar masses by Gersch- berg and Motile (1950). There might be some justification for calling the stars in Group A an OB association, but it is probably more correct to regard it as a typical section of a spiral arm. The plot of radial velocities against photometric dis­ tance in Figure 13 shows that the stars in Group A have very close to the same radial velocity. The exceptions, such as HD 204027, are stars with poorly determined or vari­ able velocity. Figure 13 shows some indication for expan­ sion of Group A. The stars that are on the near side of the group have velocities more negative with respect to the velocity of galactic rotation than the stars on the far side. That is, the stars that aro nearer are approaching the sun; the stars that are more more distant are receding.

This tendency is slight, however, and in view of the uncer­ tainties in both the photometric distances and the radial velocities, the evidence for expansion is very insecure. It seems more correct to regard the distribution in the radial 139 velocity versus distance diagram as the result of the form­ ation of the stars in different locations with various velo­ cities .

In both Group A, and Group B, there is a tendency for the luminous, evolved stars to appear more distant than the main sequence stars. Aside from the good possibility that

this is the actual distribution, it may be a result of in­ consistency between the luminosity calibrations for the main sequence and evolved stars, or it may be a result of

the inherent uncertainties in the calibration. Referring

to Figure 13, it can be seen that the radial velocities for

the luminous stars give no indication that their present

distribution results from expansion from any common origin.

Too little is known about the stars more distant than

1 1 0 0 pc to tell if any grouping which should-be considered

an OB association occurs there. Between 1200 and 1400 pc

are found v Cephei, A2la? HD 205196, BOIb? HDS 239626,

BOV?, and HDE 239789, BOv. W Cephei may also be in this

region, although its distance modulus is particularly un­

certain. Its radial velocity, however, is in perfect agree­

ment with the assigned distance of 1440 pc. Both W Cephei

and HDE 239626 appear to be 200 pc above the galactic plane.

The distance modulus of HDE is confirmed by the application

of the Q-method (Johnson 1950).

The structure of Cepheus 0B2 that is described here is

similar in many respects to that found by Kopylov (1958). 140

Using photometric distances obtained from catalogued infor­ mation, he found four groups of starss Group A, at 4S0 pc, contained 3 stars? Group B, at 650 pc, contained 0 stars?

Group C, at 950 pc, contained 10 stars? and Group D, at

1350 pc, contained 4 stars. With the addition of more stars, the groups have become less well defined, and it seems preferable to regard Kopylov*& Groups A and B as a single group. Considering the errors in the photometric distances, the division between groups is arbitrary in any case. Star formation in the region covered by the survey

seems to have occurred first at a distance of about 1 0 0 0

pc, where we now see the dispersed group of evolved stars.

It has occurred most recently in the vicinity of IC 1396, where it has probably come to an end because of the evident

turbulence created by the energy flux from HD 206267. A

small amount of star formation may still occur here, how­

ever, because several extremely opaque “globules", which

actually have irregular shapes, are seen projected against

the luminous gas. If their densities are sufficiently

high, they may still be contracting to form stars.

Relation to cralactic structure

The stars in the region of Cepheus 0B2 are in the par­

tially-developed “fin" that starts to rise into positive

latitudes from the Cygnus-Carina arm. (The branch or fin that extends into negative latitudes is much better defined by the associations Cygnus 0B4, Lacerta OBI, Perseus 0B2, and Orion OBI (Sharpiess 1965) y the lower branch is nearer the sun.) This feature is not only shown in the stars and in the H II regions (Sharpless 1965), but also in the radio observations of the neutral hydrogen (Lindblad 1965).

Group B at 900 pc, Which displays so many features of an OB association, is centered about 50 pc above the galactic plane. Previously, Cepheus OB2 has been considered to be at a distance of 0.72 kpcy at that distance its position in the galactic plane was midway between the nearer and far­ ther branches of the Cygnus-Carina arm (cf Sharpless [19653#

Figure 1). A distance of 900 pc places it definitely in the farther branch, where it would seem to belong by virtue of its height above the galactic plane.

Kopylov (195S) has noted that the subgroups into which he divided Cepheus 0B2 tend to line up with subgroups of nearby associations to form long lanes of bright stars dis­ posed at rather large angles to the center line of the spi­ ral arm. Similar features are seen in external galaxies.

The nearer part of what has here been called Group A may be combined in this manner with part of Cepheus 033, Lacerta

OBI, Cygnus 0B4, and Cygnus 0B7. 142

Suggestions for future vrorlc

In future investigations, the conditions in the region of Group B between 700 pc and 1200 pc would seem to provide the most rewarding subject for study. This investigation has indicated the presence of a shell of neutral hydrogen surrounding IC 1396. The area should be surveyed more com­ pletely at 1420 Mhz with higher velocity resolution. The requirements on angular resolution are not greatt the H II region is 3° in diameter. It would be worth while to com­ bine hydrogen-line radio observations with Lynds's (1961) continuum results to obtain the total mass of hydrogen in the region. In combination with MK types and photoelectric photometry of fainter stars which have been pointed out as possible members of Tr 37, new information could be obtained about the initial mass distribution and the conditions for star formation.

Observations of the new cluster which is centered around

19 Cephei would be valuable if it turned out to be possible to relate the supergiant to the cluster through their mo­ tions. As this study has more than indicated, any improve­ ment in the calibration of the luminous stars will benefit investigations of galactic structure. LIST OF REFERENCES

Adams, W. S., Joy, A. I-I., and Sanford, R. F. 1924, Publ. Astron. Soc. Pacific 36, 138.

Allen, C. W. 1963, Astrophvsical Quantities (Londons Ath- lone Press)• Ambartsumian, V*. A. 1949a, Astron. J. USSR 26,, 3? 1951, Abhandl. Sovrjetischen Astron., Ser. l t 33. ------. 1949b, Dokl. Alcad. Nauk USSR 6 8 , 21.

------. 1950, Abhandl• Akad. Wiss. Berlin Klasse Math. Naturwiss. 1950, Nr. 2, 10.

Artiukhina, N. M. 1954, Astron. J. USSR 31, 264? Astron. Nev?s letter No. 02, 13.

■. 1956, Publ. Sternberg Astron. Inst. 27, 203? As­ tron. Nev;sletter No. 36, 27.

Berg, M. D., and Stoynova, K. T. 1937, Publ. Pulkova Obs. 51.

Bidolman, W. P. 1966, in Vistas in Astronomy, A* Beer and K. Aa. Strand, Eds. (Oxfords Pergammon Press), Vol. 0, p. 53.

Blaauw, A. 1963, in Basic Astronomical Data, K. Aa. Strand, Ed. (Chicago? University of Chicago Press), p. 383.

------• 1964, in Annual Review of Astronomy and Astrophy­ sics, L, Goldberg, Ed. (Palo Altos Annual Reviews, Inc.), Vol. 2, p. 213.

Blanco, V. M,, and FitzGerald, M. P. 1964, Publ. Astron. Soc. Pacific 76, 438.

Boss, B. 1937, General Catalogue of 33,342 Stars for the Epoch 1950 (Washingtons Carnegie Institution of Wash­ ington ).

Brown, R. Kanbury, and Hazard, C. 1953, Monthly Notices Roy. Astron. Soc. 113, 121.

143 144

Courtes, G. 1960, Ann. d^Astrophys. 23., 115? Publ. Obs. Haute-Provence 5_, No. 9,

Cuffey, J. 1956, Sky and Telescope 15, 258.

Delhaye, J. 1965, in Galactic Structurei A. Blaauw and M. Schmidt, Eds. (Chicagos University of Chicago Pieoe), p. 61. Dieckvoss, W. 1963, in Basic Astronomical Data. K. Aa. Strand, Ed. (Chicagos University of Chicago Press), p. 40. Dieter, N. H. 1960, Astrophys. J. 132. 49.

Dolidze, M. V., and Vyasovov, V. V. 1959, Abastumani Bull. 24, 3. Duke, D. 1951, Astrophys. J. 113, 100.

Eggen, 0. J., and Herbig, G. H. 1964, Roy. Obs. Bull. No. 82.

Gerschberg, R. E., and Metik, L. P. 1960, Comm. Astrophys. Obs. Crimea 24, 143.

Gonzalez, G., and Gonzalez, G. 1956, Bull. Tonantzintla y Tacubaya No. 15. Grigorian, K. A. 1957a, Comm. Biurakan Obs. No. 22, p. 34.

------. 1957b, ibid., p. 49. Hardie, R. H. 1962, in Astronomical Techniques, W. A. Hiltner, Ed. (Chicagos University of Chicago Press), P. 178. Hilsenrath, J., Ziegler, G. C., Messina, C. G., Walsh, P. J., and Herbold, R. J. 1966, OMNITAB. A Computer Pro­ gram for Statistical and Numerical A n a l y s i s (Washing­ tons U. S. Government Printing Office)? National Bu­ reau of Standards Handbook 101.

Hiltner, W. A. 1956, Astrophys. J. Suppl. Ser. 2, 389.

Hoag, A. A. 1966, in Vistas in Astronomy. A. Beer and K. Aa. Strand, Eds. (Oxfords Pergammon Press), Vol. 8 , p. 139. 145 Hoag, A. A., Johnson, H. L., Iriarte, B., Mitchell, R. I., Hallam, K. L., and Sharpless, S. 1961, Publ. U. S. Naval Obs. 17, 349.

Jerzykiewicz, M., and Serkowski, K. 1966, Lowell Obs. Bull. 6 , 295.

Johnson, H. L. 1952, Astrophys. J. 116, 272.

------. 1958, Lowell Obs. Bull. 4, 3. ------. 1965, Astrophys. J. 141, 923.

Johnson, H. L., and Harris, D. L. 1954, Astrophys. j. 120, 196. Johnson, H. L., Hoag, A. A., Iriarte, B., Mitchell, R. I., and Hallam, K. L. 1961, Lowell Obs. Bull. 5, 133.

Johnson, H. L., and Iriarte, B. 1958, Lowell Obs. Bull. 4, 47.

Johnson, H. L., and Morgan, W. W. 1953, Astrophys. J. 117, 313.

Keenan, P. C. 1963, in Basic Astronomical Data, K. Aa. Strand, Ed. (Chicagos University of Chicago Press), p. 70.

Khorosheva, 0. V. 1956, Astron. J. USSR 33., 880.

Kirillova, T. S. 1958, Publ. Sternberg Astron. Inst. 29; 178; Astron. Newsletter No. 100, p. 13.

Kopylov, I. M. 1958 Sov. Astron. AJ 2 t 359.

Lebedinskii, A. I., and Khorosheva, O. V. 1956, Astron. J. USSR 32, 54.

Lindblad, P. O. 1965, Bull. Astron. Inst. Netherlands Suppl. 1, 77.

Lynds, C. R. 1959, Astrophys. J. 130, 603.

------• 1961, Publ. Nat. Radio Astron. Obs. 2# '43.

Markarian, a E. 1951, C o m . Biurakan Obs. No. 9, p. 33. 146

Markarian, B. E. 1952, Dokl. Akad. Naulc Armenian SSR 15. 11.

------. 1953, Comm. Biurakan Obs. No. 11, p. 3.

Martin, N. 1964, J. Observateurs 47. 125.

Merrill, P. W., and Burwell, C. G. 1933, Astrophys. J. 78. 87.

Mirzoyan, L. V. 195!* Comm. Biurakan Obs. No. 16, p. 41.

Morgan, W. W. 1951, Publ. Univ. of Michigan Obs. 10. 33.

Morgan, W. W., and Bidelman, W. P. 1946, Astrophys. J. 103. 378.

Morgan, W. W., Code, A. D., and Whitford, A. E. 1955, As­ trophys. J. Suppl. Ser. 2 t 41.

Morgan, W. W., Meinel, A. B., and Johnson, H. M. 1954, Astrophys. J. 120. 506.

Morgan, W. W. , Whitford, A. E., and Code, A. D. 1953, As­ trophys. J. 118. 313.

Muller, C« A., and Westerhout, G. 1957, Bull. Astron. Inst. Netherlands 13, 151.

Munch, G. 1957, Astrophys. J. 125. 42.

Nassau, J. J., and Morgan, W. W. 1951, Astrophys. J. 113. 141.

6 hman, Y. 1927, Medd. Astron. Obs. Uppsala, No. 33.

Pannekoek, A. 1929, Publ. Astron. Inst. Amsterdam, No. 2.

Petrie, R. M. 1952, Publ. Dorn. Astrophys. Obs. 12. 111.

Petrie, R. M., and Lee, E. K. 1966 Publ. Dortu Astrophys. Obs. 12. 435.

Petrie, R. M., and Pearce, J. A. 1931, Publ. Dom. Astro­ phys. Obs. 5, 2.

------. 1962, ibid., 12, 1.

Scott, F. P. 1963, in Basic Astronomical Data. K. Aa. strand, Ed. (Chicagog University of Chicago Press), p. 1 1 . 147

Schmidt, M. 1956, Bull. Astron. Inst. Netherlands 13, 15.

1965, in Galactic Structure, A. Blaauw and M. Schmidt, Eds. (Chicago? University of Chicago Press), p. 513. Schwassmann, A., and van Rhijn, P. J. 1935, Bergedorfer S pole t r al-Durchmus terung 1, 190.

Serkowski, K. 1961, Lowell Obs. Bull. J5, 157.

Sharpless, S. 1959, Astrophys. J. Suppl. Ser. 4, 257.

------. 1965, in Galactic Structure. A. Blaauw and M. Schmidt, Eds. (Chicago? University of Chicago Press), p. 131.

Shakhovskoi, N. M. 1956, Publ. Sternberg Astron. Inst. 27, 165? Astron. Newsletter No. 8 6 , 26.

Shteins, K. A., and Abele, M. K. _ 1958, Sov. Astron. AJ 2 t 70.

Slettebak, A. E., and Howard, R. F. 1955, Astrophys. J. 121, 102. Stebbins, J., Huffer, C. M., and Whitford, A. 3. 1940, Astrophys. J. 91. 20.

Struve, 0. 1927, Astron. Nach. 231. 17.

Trumpler, R. J. 1930, Lick Obs. Bull. 14, 158.

Underhill, A. B. 1966a, The Early Type Stars (Dordrecht, Holland? D. Reidel Publishing Co.)

------1966b, in Vistas in Astronomy. A. Beer and K. Aa. Strand, Eds. (Oxfords Pergammon Press), Vol. 8 , p. 41.

Van Herk, G. 1959, Astronom. J. 64, 348.

Walkor, G. A. H., and Hodge, S. M. 1966 Publ. Dorn. Astro­ phys. Obs. 12, 401.

Weaver, H. F. 1961, Publ. Astron. Soc. Pac. 73, 38*

Weaver, H., and Ebert, A. 1964, Publ. Astron. Soc. Pac* 76, 148

Wilson, R. E. 1953, General Catalogue of Stellar Radial Velocities (Washingtons Carnegie Institution of Washington). Wilson, R. W., and Bolton, J. G. 1960, Publ. Astron. Soc, Pac. 72, 331.

I