FAR-INFRARED PHOTOMETRY of a STATISTICAL SAMPLE of LATE-TYPE VIRGO CLUSTER GALAXIES1 Richard J
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The Flint River Observer
1 bachelorette status by becoming Mrs. Laura Feltman. THE Everyone in FRAC wishes Laura and Trent Feltman, her husband-to-be, years of happily wedded bliss. FLINT RIVER -Bill Warren * * * OBSERVER Last Month’s Meeting/Activities. We had 21 members – speaker Felix Luciano and Dwight NEWSLETTER OF THE FLINT Harness, Alfred McClure, Bill Warren, Carlos RIVER ASTRONOMY CLUB Flores, Ken Harris, Tom Moore, Kenneth & Rose Olson, Alan Rutter, Aaron Calhoun, Erik An Affiliate of the Astronomical League Erikson, Truman Boyle, Dan Pillatzki, Larry Higgins, Eva Schmidler, Dawn Chappell, John Vol. 21, No. 3 May, 2018 Felbinger, Sean Neckel, Steve Hollander and Officers: President, Dwight Harness (1770 Cindy Barton – at our April meeting. Felix’s Hollonville Rd., Brooks, Ga. 30205, 770-227-9321, impressive performance took us through the process [email protected]); Vice President, Bill he uses to convert captured photons of light into his Warren (1212 Everee Inn Rd., Griffin, Ga. 30224, amazing astrophotos that you see in the Observer. [email protected]); Secretary, Carlos Our non-photographers might not have understood Flores; Treasurer, Jeremy Milligan. everything he talked about, but we appreciate the Board of Directors: Larry Higgins; Aaron effort that goes into the making of an astrophoto. Calhoun; and Alan Rutter. It’s a lot of work, but to folks like Felix and Alan Facebook Coordinator: Laura Harness; Alcor: Pryor it’s a labor of love. Carlos Flores; Webmaster: Tom Moore; “Into each life some rain must fall,” sang Ella Program Coordinator/Newsletter Editor: Bill Firzgerald and the Ink Spots in 1944. For Warren; Observing Coordinator: Sean Neckel; astronomers, though, it doesn’t take rain to cancel NASA Contact: Felix Luciano. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
T He Cool Stellar P Opulations of E Arly-T Y Pe G
T h e C o ol S t e l l a r P o pu l a t io n s o f E a r l y -T y p e G a l a x ie s a n d t h e G a l a c t ic B ulge dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Mark Lee Houdashelt, 3|C $ J ) t + $ The Ohio State University 1995 Dissertation Committee: Approved by Prof. Jay A. Frogel Prof. Kristen Sellgren /J (J Advisor Prof. Donald M. Temdrup Department of Astronomy ONI Number: 9533992 UMI Microform 9533992 Copyright 1995, by UMI Company. All rights reserved. This microform edition is protected against unauthorized copying under Title 17, united States Code. UMI 300 North Zeeb Road Ann Arbor, MI 48103 To Mom and Tim ii A cknowledgements First and foremost, I would like to express my deepest appreciation to my mother, Darlene, and my brother, Tim, for their unwavering support before, during, and (hopefully) after my graduate studies. Without them, I would not have achieved as much as I have nor be as happy as I am. Thank you, Mom amd Tim, for all that you have done for me. Obviously, I am deeply indebted to my advisor, Jay Frogel, for his support (both financial and otherwise), his scientific expertise and his belief in my abilities. He suggested the initial dissertation project to me and helped me to redefine it along the way, always remaining positive and encouraging. -
Line-Of-Sight Velocity Distributions of Low-Luminosity Elliptical Galaxies
Mon. Not. R. Astron. Soc. 326, 473–489 (2001) Line-of-sight velocity distributions of low-luminosity elliptical galaxies C. Halliday,1P† Roger L. Davies,1 Harald Kuntschner,1 M. Birkinshaw,2 Ralf Bender,3 R. P. Saglia3 and Glenn Baggley1 1Department of Physics, University of Durham, Science Labs, South Road, Durham DH1 3LE 2H.H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL 3Universita¨ts-Sternwarte, Scheinerstr. 1, D-81679 Mu¨nchen, Germany Accepted 2001 March 7. Received 2000 December 21; in original form 2000 December 21 ABSTRACT The shape of the line-of-sight velocity distribution (LOSVD) is measured for a sample of 14 elliptical galaxies, predominantly low-luminosity ellipticals. The sample is dominated by galaxies in the Virgo cluster but also contains ellipticals in nearby groups and low-density environments. The parametrization of the LOSVD given by Gerhard and van der Marel & Franx is adopted, which measures the asymmetrical and symmetrical deviations of the LOSVD from a Gaussian by the amplitudes h3 and h4 of the Gauss–Hermite series. Rotation, velocity dispersion, h3 and h4 are determined as a function of radius for both major and minor axes. Non-Gaussian LOSVDs are found for all galaxies along the major axes. Deviations from a Gaussian LOSVD along the minor axis are of much lower amplitude if present at all. Central decreases in velocity dispersion are found for three galaxies. Two galaxies have kinematically decoupled cores: NGC 4458 and the well-known case of NGC 3608. Key words: galaxies: elliptical and lenticular, cD – galaxies: formation – galaxies: kinematics and dynamics. -
A Catalogue of 1180 Galaxies in the Direction of the Virgo Cluster's Core
ASTRONOMY & ASTROPHYSICS FEBRUARY I 1998, PAGE 367 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 127, 367-395 (1998) The “Virgo photometry catalogue”; a catalogue of 1180 galaxies in the direction of the Virgo Cluster’s core C.K. Young1,2 and M.J. Currie3 1Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China 2Department of Physics, University of Oxford, Nuclear and Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK 3Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK Received February 25; accepted May 22, 1997 Abstract. We present a new catalogue of galaxies in merged images; our segmentation software being able to the direction of the Virgo Cluster’s core: the Virgo cope with the vast majority of image mergers. Photometry Catalogue (VPC)1. This catalogue contains 1180 galaxies (including background objects) within a 23 Key words: galaxies: clusters: individual: Virgo — square-degree area of the sky centred on R.A.1950.0 = catalogues — galaxies: fundamental parameters — h m ◦ 0 12 26 and dec.1950.0 =13 08 . The VPC galaxy sample galaxies: photometry comprises of non-stellar objects brighter than BJ25 =19.0; the completeness limits being BJ25 ≈ 18.5 for the northern half of the survey area and BJ25 ≈ 18.0 for the southern half. Independently-calibrated photographic surface pho- 1. Introduction tometry is presented for over 1000 galaxies in the U, BJ The Virgo Cluster, being the dominant nearby clus- and RC bands. Parameters listed for catalogued galax- ter of galaxies, has long attracted much attention. ies include: equatorial coordinates, morphological types, It is irregular and exhibits significant substructure. -
University of Southampton Research Repository Eprints Soton
University of Southampton Research Repository ePrints Soton Copyright © and Moral Rights for this thesis are retained by the author and/or other copyright owners. A copy can be downloaded for personal non-commercial research or study, without prior permission or charge. This thesis cannot be reproduced or quoted extensively from without first obtaining permission in writing from the copyright holder/s. The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the copyright holders. When referring to this work, full bibliographic details including the author, title, awarding institution and date of the thesis must be given e.g. AUTHOR (year of submission) "Full thesis title", University of Southampton, name of the University School or Department, PhD Thesis, pagination http://eprints.soton.ac.uk UNIVERSITY OF SOUTHAMPTON The Long-Term X-ray, UV and Optical Variability of Active Galactic Nuclei by Samuel Dominic Connolly Thesis for the degree of Doctor of Philosophy in the FACULTY OF PHYSICAL SCIENCES AND ENGINEERING Department of Physics & Astronomy June 2016 UNIVERSITY OF SOUTHAMPTON ABSTRACT FACULTY OF PHYSICAL SCIENCES AND ENGINEERING Department of Physics & Astronomy Doctor of Philosophy THE LONG-TERM X-RAY, UV AND OPTICAL VARIABILITY OF ACTIVE GALACTIC NUCLEI by Samuel Dominic Connolly The variability of emission from active galactic nuclei (AGN), both intrinsic, due to changes in the emitting regions, and extrinsic, due to absorption and scattering from material near to the black hole, can reveal a wealth of information about their geometry and accretion behaviour. In this thesis, I use analysis of the spectral variability of the X- ray, UV/optical emission from AGN to probe the properties of the material surrounding supermassive black holes at their centres. -
The SLUGGS Survey: a Catalog of Over 4000 Globular Cluster Radial Velocities in 27 Nearby Early-Type Galaxies
The Astronomical Journal, 153:114 (10pp), 2017 March https://doi.org/10.3847/1538-3881/153/3/114 © 2017. The American Astronomical Society. All rights reserved. The SLUGGS Survey: A Catalog of Over 4000 Globular Cluster Radial Velocities in 27 Nearby Early-type Galaxies Duncan A. Forbes1, Adebusola Alabi1, Jean P. Brodie2, Aaron J. Romanowsky2,3, Jay Strader4, Caroline Foster5, Christopher Usher6, Lee Spitler5,7, Sabine Bellstedt1, Nicola Pastorello1,8, Alexa Villaume2, Asher Wasserman2, and Vincenzo Pota9 1 Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia; [email protected] 2 University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA 3 Department of Physics and Astronomy, San José State University, One Washington Square, San Jose, CA 95192, USA 4 Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA 5 Australian Astronomical Observatory, P.O. Box 915, North Ryde, NSW 1670, Australia 6 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK 7 Macquarie Research Centre for Astronomy, Astrophysics & Astrophotonics, Macquarie University, Sydney, NSW 2109, Australia 8 Deakin Software and Technology Innovation Laboratory, Deakin University, Burwood, VIC 3125, Australia 9 INAF—Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16, I-80131 Napoli, Italy Received 2016 November 16; revised 2017 January 8; accepted 2017 January 9; published 2017 February 17 Abstract Here, we present positions and radial velocities for over 4000 globular clusters (GCs) in 27 nearby early-type galaxies from the SLUGGS survey. The SLUGGS survey is designed to be representative of elliptical and < / < lenticular galaxies in the stellar mass range 10 log M* Me 11.7. -
A Strong Dichotomy in S0 Disk Profiles Between the Virgo Cluster
To appear in ApJ Letters Preprint typeset using LATEX style emulateapj v. 11/10/09 A STRONG DICHOTOMY IN S0 DISK PROFILES BETWEEN THE VIRGO CLUSTER AND THE FIELD Peter Erwin Max-Planck-Institut f¨urextraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany Universit¨ats-Sternwarte M¨unchen, Scheinerstrasse 1, D-81679 M¨unchen, Germany and Leonel Gutierrez´ 1,2, John E. Beckman2,3 Instituto de Astrof´ısicade Canarias, C/ Via L´acteas/n, 38200 La Laguna, Tenerife, Spain To appear in ApJ Letters ABSTRACT We report evidence for a striking difference between S0 galaxies in the local field and in the Virgo Cluster. While field S0 galaxies have disks whose surface-brightness profiles are roughly equally divided between the three main types (Types I, II, and III: single-exponential, truncated, and antitruncated), Virgo S0s appear to be entirely lacking in disk truncations. More specifically, the fraction of trunca- +7 +4 tions in S0 galaxies with MB < −17 is 28−6% for the field, versus 0−0% for the Virgo Cluster galaxies; the difference is significant at the 99.7% level. The discrepancy is made up almost entirely by Type I profiles, which are almost twice as frequent in the Virgo Cluster as they are in the field. This suggests that S0 formation may be driven by different processes in cluster and field environ- ments, and that outer-disk effects can be useful tests of S0 formation models. Subject headings: galaxies: structure | galaxies: elliptical and lenticular, cD | galaxies: evolution | galaxies: clusters: general 1. INTRODUCTION ferences in S0 galaxies as a function of environment, dif- One of the most interesting unresolved questions in the ferences which could be used to test S0 formation models. -
DSO List V2 Current
7000 DSO List (sorted by name) 7000 DSO List (sorted by name) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs Dist SAC NOTES M 1 NGC 1952 SN Rem TAU 8.4 11 8' 05 34.5 +22 01 135 6.3k Crab Nebula; filaments;pulsar 16m;3C144 M 2 NGC 7089 Glob CL AQR 6.5 11 11.7' 21 33.5 -00 49 255 II 36k Lord Rosse-Dark area near core;* mags 13... M 3 NGC 5272 Glob CL CVN 6.3 11 18.6' 13 42.2 +28 23 110 VI 31k Lord Rosse-sev dark marks within 5' of center M 4 NGC 6121 Glob CL SCO 5.4 12 26.3' 16 23.6 -26 32 336 IX 7k Look for central bar structure M 5 NGC 5904 Glob CL SER 5.7 11 19.9' 15 18.6 +02 05 244 V 23k st mags 11...;superb cluster M 6 NGC 6405 Opn CL SCO 4.2 10 20' 17 40.3 -32 15 377 III 2 p 80 6.2 2k Butterfly cluster;51 members to 10.5 mag incl var* BM Sco M 7 NGC 6475 Opn CL SCO 3.3 12 80' 17 53.9 -34 48 377 II 2 r 80 5.6 1k 80 members to 10th mag; Ptolemy's cluster M 8 NGC 6523 CL+Neb SGR 5 13 45' 18 03.7 -24 23 339 E 6.5k Lagoon Nebula;NGC 6530 invl;dark lane crosses M 9 NGC 6333 Glob CL OPH 7.9 11 5.5' 17 19.2 -18 31 337 VIII 26k Dark neb B64 prominent to west M 10 NGC 6254 Glob CL OPH 6.6 12 12.2' 16 57.1 -04 06 247 VII 13k Lord Rosse reported dark lane in cluster M 11 NGC 6705 Opn CL SCT 5.8 9 14' 18 51.1 -06 16 295 I 2 r 500 8 6k 500 stars to 14th mag;Wild duck cluster M 12 NGC 6218 Glob CL OPH 6.1 12 14.5' 16 47.2 -01 57 246 IX 18k Somewhat loose structure M 13 NGC 6205 Glob CL HER 5.8 12 23.2' 16 41.7 +36 28 114 V 22k Hercules cluster;Messier said nebula, no stars M 14 NGC 6402 Glob CL OPH 7.6 12 6.7' 17 37.6 -03 15 248 VIII 27k Many vF stars 14.. -
The SLUGGS Survey: a Catalog of Over 4000 Globular Cluster Radial Velocities in 27 Nearby Early-Type Galaxies
The Astronomical Journal, 153:114 (10pp), 2017 March https://doi.org/10.3847/1538-3881/153/3/114 © 2017. The American Astronomical Society. All rights reserved. The SLUGGS Survey: A Catalog of Over 4000 Globular Cluster Radial Velocities in 27 Nearby Early-type Galaxies Duncan A. Forbes1, Adebusola Alabi1, Jean P. Brodie2, Aaron J. Romanowsky2,3, Jay Strader4, Caroline Foster5, Christopher Usher6, Lee Spitler5,7, Sabine Bellstedt1, Nicola Pastorello1,8, Alexa Villaume2, Asher Wasserman2, and Vincenzo Pota9 1 Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia; [email protected] 2 University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA 3 Department of Physics and Astronomy, San José State University, One Washington Square, San Jose, CA 95192, USA 4 Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA 5 Australian Astronomical Observatory, P.O. Box 915, North Ryde, NSW 1670, Australia 6 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK 7 Macquarie Research Centre for Astronomy, Astrophysics & Astrophotonics, Macquarie University, Sydney, NSW 2109, Australia 8 Deakin Software and Technology Innovation Laboratory, Deakin University, Burwood, VIC 3125, Australia 9 INAF—Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16, I-80131 Napoli, Italy Received 2016 November 16; revised 2017 January 8; accepted 2017 January 9; published 2017 February 17 Abstract Here, we present positions and radial velocities for over 4000 globular clusters (GCs) in 27 nearby early-type galaxies from the SLUGGS survey. The SLUGGS survey is designed to be representative of elliptical and < / < lenticular galaxies in the stellar mass range 10 log M* Me 11.7. -
Publications of the Astronomical Society of Australia Volume 18, 2001 © Astronomical Society of Australia 2001
Publishing Publications of the Astronomical Society of Australia Volume 18, 2001 © Astronomical Society of Australia 2001 An international journal of astronomy and astrophysics For editorial enquiries and manuscripts, please contact: The Editor, PASA, ATNF, CSIRO, PO Box 76, Epping, NSW 1710, Australia Telephone: +61 2 9372 4590 Fax: +61 2 9372 4310 Email: [email protected] For general enquiries and subscriptions, please contact: CSIRO Publishing PO Box 1139 (150 Oxford St) Collingwood, Vic. 3066, Australia Telephone: +61 3 9662 7666 Fax: +61 3 9662 7555 Email: [email protected] Published by CSIRO Publishing for the Astronomical Society of Australia www.publish.csiro.au/journals/pasa Downloaded from https://www.cambridge.org/core. IP address: 170.106.35.76, on 26 Sep 2021 at 20:11:13, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1071/AS01029 Publ. Astron. Soc. Aust., 2001, 18, 121–128 Total Magnitudes of Virgo Galaxies. I. Construction of a Self-Consistent Reference Dataset Spanning 8th to 18th Magnitude Christopher Ke-shih Young Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Xuhui District, Shanghai 200030, China [email protected] National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China Department of Astrophysics and Optics, School of Physics, University of New South Wales, Sydney 2052, Australia [email protected] Received 2000 May 3, accepted 2001 June 1 Abstract: The main objectives of this series of papers are: (1) to demonstrate the existence of serious mutual disagreements between established total (and other integrated) magnitude scales for Virgo galaxies; (2) to attempt to quantify both the systematic and random errors present within these magnitude scales; (3) to investigate the origins of any large error uncovered; and thereby (4) to encourage the general adoption of rigorous total-magnitude measurement procedures by the astronomical community.