8Th October 2002
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
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 -
GMRT HI Observations of the Eridanus Group of Galaxies A. Omar
J. Astrophys. Astr. (2005) 26, 1–70 GMRT HI Observations of the Eridanus Group of Galaxies A. Omar∗1 & K. S. Dwarakanath2 Raman Research Institute, Sadashivanagar, Bangalore 560 080, India. 1e-mail: [email protected] 2e-mail: [email protected] Received 2004 August 23; accepted 2005 March 22 Abstract. The GMRT HI 21cm-line observations of galaxies in the Eri- danus group are presented. The Eridanus group, at a distance of ∼23 Mpc, is a loose group of ∼200 galaxies. The group extends to more than 10 Mpc in projection. The velocity dispersion of the galaxies in the group is ∼240 km s−1. The galaxies are clustered into different sub-groups. The overall population mix of the group is 30% (E + S0) and 70% (Sp + Irr). The observations of 57 Eridanus galaxies were carried out with the GMRT for ∼ 200 h. HI emission was detected from 31 galaxies. The channel rms of ∼ 1 mJy beam−1 was achieved for most of the image-cubes made with 4 h of data. The corresponding HI column density sensitivity (3σ)is ∼1 × 1020 cm−2 for a velocity-width of ∼ 13.4kms−1. The 3σ detection 7 −1 limit of HI mass is ∼1.2 × 10 M for a line-width of 50 km s . Total HI images, HI velocity fields, global HI line profiles, HI mass surface densi- ties, HI disk parameters and HI rotation curves are presented. The velocity fields are analysed separately for the approaching and the receding sides of the galaxies. These data will be used to study the HI and the radio con- tinuum properties, the Tully–Fisher relations, the dark matter halos, and the kinematical and HI lopsidedness in galaxies. -
Super-Massive Black Hole Scaling Relations and Peculiar Ringed Galaxies
SUPER-MASSIVE BLACK HOLE SCALING RELATIONS AND PECULIAR RINGED GALAXIES A DISSERTATION SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY BURCIN MUTLU IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY MARC S. SEIGAR June, 2017 c BURCIN MUTLU 2017 ALL RIGHTS RESERVED Acknowledgements There are several people who I would like to acknowledge for directly or indirectly contributing to this dissertation. First and foremost, I would like to acknowledge the guidance and support of my ad- visor, Marc S. Seigar. I am thankful to him for his continuous encouragement, patience, and kindness. I appreciate all his contributions of knowledge, expertise, and time, which were invaluable to my success in graduate school. He has set an example of excellence as a researcher, mentor, and role model. In addition, I would like to thank my dissertation committee, Liliya L. R. Williams, M. Claudia Scarlata, and Robert Lysak, for their insightful input, constructive criticism and direction during the course of this dissertation. I have crossed paths with many collaborators who have influenced and enhanced my research. Patrick Treuthardt has been a collaborator for most of the work during my dissertation. The addition of his scientific point of view has improved the quality of the work in this dissertation tremendously. Our discussions have always been stimulating and rewarding. I am thankful to him for mentoring me and being a dear friend to me. I would also like to thank Benjamin L. Davis for numerous helpful advice and inspiring discussions. He has directly involved with many aspects of Chapter 1. -
A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im. -
PDF (Accepted Manuscript)
Swinburne Research Bank http://researchbank.swinburne.edu.au Brough, Sarah; Forbes, Duncan A.; Kilborn, Virginia A.; Couch, Warrick. (2006). Southern GEMS groups I : dynamical properties. Monthly notices of the Royal Astronomical Society. 370, (3): 1223-1246. Available at: http://dx.doi.org/10.1111/j.1365-2966.2006.10542.x © 2006 The Royal Astronomical Society. This is the author’s version of the work. It is posted here with the permission of the publisher for your personal use. No further distribution is permitted. If your library has a subscription to this journal, you may also be able to access the published version via the library catalogue. The definitive version is available at www.interscience.wiley.com Mon. Not. R. Astron. Soc. 000, 1–20 (2005) Printed 5 February 2008 (MN LATEX style file v2.2) Southern GEMS Groups I: Dynamical Properties Sarah Brough1⋆, Duncan A. Forbes1, Virginia A. Kilborn1,2, Warrick Couch3 1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 1710, Australia 3School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia Accepted... Received...; in original form 2005 ABSTRACT Here we present an investigation of the properties of 16 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multi- wavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydro- gen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey (6dFGS) and NASA/IPAC Extra-galactic Database (NED). -
¼¼Çwªâðw¦¹Á¼ºëw£Àêëw ˆ†‰€ «ÆÊ¿Àäàww«¸ÂÀ ‰‡‡Œ†ˆ‰†‰Œ
¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. P.A. w R.A. Size Size Chart N a he ss d l Object Type Con. Mag. Class t NGC Description l AS o o sc e s r ( h m ) max min No. C a ( ' ) ( ) sc R AAS e r e M C T e B H H x x NGC 3511 GALXY CRT 11 03.4 -23 05 11 6 m 2.1 m 76 SBc vF,vL,mE 98 x x NGC 3513 GALXY CRT 11 03.8 -23 15 11.5 2.9 m 2.4 m 75 SBb vF,vL,mE 98 IC 2627 GALXY CRT 11 09.9 -23 44 12 2.6 m 2.1 m SBbc eF,L,R,stell N 98 NGC 3573 GALXY CEN 11 11.3 -36 53 12.3 3.6 m 1 m 4 Sa eF,S,R,glbM,3 st 11 f 98 NGC 3571 GALXY CRT 11 11.5 -18 17 12.1 3 m 0.9 m 94 SBa pF,pL,iF,bM 98 B,pL,E,vsmbMN,2 B st x NGC 3585 GALXY HYA 11 13.3 -26 45 9.9 5.2 m 3.1 m 107 Elliptical 98 tri NGC 3606 GALXY HYA 11 16.3 -33 50 12.4 1.5 m 1.4 m Elliptical eF,S,R,gbM 98 x x x NGC 3621 GALXY HYA 11 18.3 -32 49 9.7 12.4 m 5.7 m 159 SBcd cB,vL,E 160,am 4 st 98 NGC 3673 GALXY HYA 11 25.2 -26 44 11.5 3.7 m 2.4 m 70 SBb F,vL,gvlbM,*7 s 6' 98 PK 283+25.1 PLNNB HYA 11 26.7 -34 22 12.1 188 s 174 s 98 x NGC 3693 GALXY CRT 11 28.2 -13 12 13 3.4 m 0.7 m 85 Sb cF,S,E,gbM 98 NGC 3706 GALXY CEN 11 29.7 -36 24 11.3 3.1 m 1.8 m 78 E-SO pB,cS,R,psmbM 98 NGC 3717 GALXY HYA 11 31.5 -30 19 11.2 6.2 m 1 m 33 Sb pB,S,mE,*13 att 98 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. -
Balogh Et Star Wilman 2003; That 2004; 1998; Al
Mon. Not. R. Astron. Soc. 000, 1–16 (2005) Printed 15 October 2018 (MN LATEX style file v2.2) Eridanus - A Supergroup in the Local Universe? Sarah Brough1,⋆ Duncan A. Forbes1, Virginia A. Kilborn1,2, Warrick Couch3, Matthew Colless4 1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 1710, Australia 3School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia 4Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia Accepted... Received...; in original form 2005 ABSTRACT We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with 2MASS and HyperLEDA photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies. The overall structure is made up of three 13 individual groups that are likely to merge to form a cluster of mass ∼ 7 × 10 M⊙. We conclude that this structure is a supergroup. We also examine the colours, mor- phologies and luminosities of the galaxies in the region with respect to their local projected surface density. We find that the colours of the galaxies redden with in- creasing density, the median luminosities are brighter with increasing environmental density and the morphologies of the galaxies show a strong morphology-density rela- tion. The colours and luminosities of the galaxies in the supergroup are already similar to those of galaxies in clusters, however the supergroup contains more late-type galax- ies, consistent with its lower projected surface density. -
Inner Rings in Disc Galaxies: Dead Or Alive ,
A&A 555, L4 (2013) Astronomy DOI: 10.1051/0004-6361/201321983 & c ESO 2013 Astrophysics Letter to the Editor Inner rings in disc galaxies: dead or alive, S. Comerón1,2 1 University of Oulu, Astronomy Division, Department of Physics, PO Box 3000, 90014 Oulu, Finland e-mail: [email protected] 2 Finnish Centre of Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland Received 28 May 2013 / Accepted 17 June 2013 ABSTRACT In this Letter, I distinguish “passive” inner rings as those with no current star formation as distinct from “active” inner rings that have undergone recent star formation. I built a sample of nearby galaxies with inner rings observed in the near- and mid-infrared from the NIRS0S and the S4G surveys. I used archival far-ultraviolet (FUV) and Hα imaging of 319 galaxies to diagnose whether their inner rings are passive or active. I found that passive rings are found only in early-type disc galaxies (−3 ≤ T ≤ 2). In this range of stages, 21 ± 3% and 28 ± 5% of the rings are passive according to the FUV and Hα indicators, respectively. A ring that is passive according to the FUV is always passive according to Hα, but the reverse is not always true. Ring-lenses form 30–40% of passive rings, which is four times more than the fraction of ring-lenses found in active rings in the stage range −3 ≤ T ≤ 2. This is consistent with both a resonance and a manifold origin for the rings because both models predict purely stellar rings to be wider than their star-forming counterparts. -
Unveiling the Structure of Barred Galaxies at 3.6 Μm with the Spitzer Survey of Stellar Structure in Galaxies (S4G)
University of Louisville ThinkIR: The University of Louisville's Institutional Repository Faculty Scholarship 2-2014 Unveiling the structure of barred galaxies at 3.6 μm with the Spitzer Survey of Stellar Structure in Galaxies (S4G). I. Disk breaks. Taehyun Kim National Radio Astronomy Observatory Dimitri A. Gadotti European Southern Observatory Kartik Sheth National Radio Astronomy Observatory E. Athanassoula Aix Marseille Universite Albert Bosma Aix Marseille Universite See next page for additional authors Follow this and additional works at: https://ir.library.louisville.edu/faculty Part of the Astrophysics and Astronomy Commons Original Publication Information Kim, Taehyun, et al. "Unveiling the Structure of Barred Galaxies at 3.6 μm with the Spitzer Survey of Stellar Structure in Galaxies (S4G). I. Disk Breaks." 2014. The Astrophysical Journal 782(2): 19 pp. This Article is brought to you for free and open access by ThinkIR: The University of Louisville's Institutional Repository. It has been accepted for inclusion in Faculty Scholarship by an authorized administrator of ThinkIR: The University of Louisville's Institutional Repository. For more information, please contact [email protected]. Authors Taehyun Kim, Dimitri A. Gadotti, Kartik Sheth, E. Athanassoula, Albert Bosma, Myung Gyoon Lee, Barry F. Madore, Bruce G. Elmegreen, Johan H. Knapen, Dennis Zaritsky, Luis C. Ho, Sebastien Comeron, Benne W. Holwerda, Joannah L. Hinz, Juan Carlos Munoz-Mateos, Mauricio Cisternas, Santiago Erroz-Ferrer, Ron Buta, Eija Laurikainen, Heikki Salo, Jarkko Laine, Karin Menendez-Delmestre, Michael W. Regan, Bonita de Swardt, Armando Gil de Paz, Mark Seibert, and Trisha Mizusawa This article is available at ThinkIR: The University of Louisville's Institutional Repository: https://ir.library.louisville.edu/ faculty/203 The Astrophysical Journal, 782:64 (19pp), 2014 February 20 doi:10.1088/0004-637X/782/2/64 C 2014. -
Dave Mitsky's Monthly Celestial Calendar
Dave Mitsky’s Monthly Celestial Calendar January 2010 ( between 4:00 and 6:00 hours of right ascension ) One hundred and five binary and multiple stars for January: Omega Aurigae, 5 Aurigae, Struve 644, 14 Aurigae, Struve 698, Struve 718, 26 Aurigae, Struve 764, Struve 796, Struve 811, Theta Aurigae (Auriga); Struve 485, 1 Camelopardalis, Struve 587, Beta Camelopardalis, 11 & 12 Camelopardalis, Struve 638, Struve 677, 29 Camelopardalis, Struve 780 (Camelopardalis); h3628, Struve 560, Struve 570, Struve 571, Struve 576, 55 Eridani, Struve 596, Struve 631, Struve 636, 66 Eridani, Struve 649 (Eridanus); Kappa Leporis, South 473, South 476, h3750, h3752, h3759, Beta Leporis, Alpha Leporis, h3780, Lallande 1, h3788, Gamma Leporis (Lepus); Struve 627, Struve 630, Struve 652, Phi Orionis, Otto Struve 517, Beta Orionis (Rigel), Struve 664, Tau Orionis, Burnham 189, h697, Struve 701, Eta Orionis, h2268, 31 Orionis, 33 Orionis, Delta Orionis (Mintaka), Struve 734, Struve 747, Lambda Orionis, Theta-1 Orionis (the Trapezium), Theta-2 Orionis, Iota Orionis, Struve 750, Struve 754, Sigma Orionis, Zeta Orionis (Alnitak), Struve 790, 52 Orionis, Struve 816, 59 Orionis, 60 Orionis (Orion); Struve 476, Espin 878, Struve 521, Struve 533, 56 Persei, Struve 552, 57 Persei (Perseus); Struve 479, Otto Struve 70, Struve 495, Otto Struve 72, Struve 510, 47 Tauri, Struve 517, Struve 523, Phi Tauri, Burnham 87, Xi Tauri, 62 Tauri, Kappa & 67 Tauri, Struve 548, Otto Struve 84, Struve 562, 88 Tauri, Struve 572, Tau Tauri, Struve 598, Struve 623, Struve 645, Struve