Structure and Kinematics of the Peculiar Galaxy NGC
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Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Torques and Angular Momentum: Counter-Rotation in Galaxies and Ring Galaxies
MNRAS 000, 000{000 (2016) Preprint 9 July 2018 Compiled using MNRAS LATEX style file v3.0 Torques and angular momentum: Counter-rotation in galaxies and ring galaxies N. G. Kantharia1? 1 National Centre for Radio Astrophysics, TIFR, Post Bag 3, Ganeshkhind, Pune-411007, India Last updated; in original form ABSTRACT We present an alternate origin scenario to explain the observed phenomena of (1) counter-rotation between different galaxy components and (2) the formation of ring galaxies. We suggest that these are direct consequences of the galaxy being acted upon by a torque which causes a change in its primordial spin angular momentum first observed as changes in the gas kinematics or distribution. We suggest that this torque is exerted by the gravitational force between nearby galaxies. This origin requires the presence of at least one companion galaxy in the vicinity - we find a companion galaxy within 750 kpc for 51/57 counter-rotating galaxies and literature indicates that all ring galaxies have a companion galaxy thus giving observable credence to this origin. Moreover in these 51 galaxies, we find a kinematic offset between stellar and gas heliocentric velocities > 50 kms−1 for several galaxies if the separation between the galaxies < 100 kpc. This, we suggest, indicates a change in the orbital angular momentum of the torqued galaxies. A major difference between the torque origin suggested here and the existing model of gas accretion/galaxy collision, generally used to explain the above two phenomena, is that the torque acts on the matter of the same galaxy whereas in the latter case gas, with different properties, is brought in from outside. -
Discovery of Counter-Rotating Gas in the Galaxies NGC 1596 and 3203 and the Incidence of Gas Counter-Rotation in S0 Galaxies
Mon. Not. R. Astron. Soc. 366, 182–188 (2006) doi:10.1111/j.1365-2966.2005.09840.x Discovery of counter-rotating gas in the galaxies NGC 1596 and 3203 and the incidence of gas counter-rotation in S0 galaxies M. Bureau1⋆ and A. Chung2⋆ 1Sub-Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH 2Department of Astronomy, Columbia University, New York, NY 10027, USA Accepted 2005 November 4. Received 2005 October 29; in original form 2005 July 26 ABSTRACT We have identified two new galaxies with gas counter-rotation (NGC 1596 and 3203) and have confirmed similar behaviour in another one (NGC 128), this using results from separate studies of the ionized-gas and stellar kinematics of a well-defined sample of 30 edge-on disc galaxies. Gas counter-rotators thus represent 10 ± 5 per cent of our sample, but the fraction climbs to 21 ± 11 per cent when only lenticular (S0) galaxies are considered and to 27 ± 13 per cent for S0 galaxies with detected ionized gas only. Those fractions are consistent with but slightly higher than previous studies. A compilation from well-defined studies of S0 galaxies in the literature yields fractions of 15 ± 4 and 23 ± 5 per cent, respectively. Although mainly based on circumstantial evidence, we argue that the counter-rotating gas originates primarily from minor mergers and tidally induced transfer of material from nearby objects. Assuming isotropic accretion, twice those fractions of objects must have undergone similar processes, underlining the importance of (minor) accretion for galaxy evolution. Applications of gas counter-rotators to barred galaxy dynamics are also discussed. -
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. -
Cold Gas in a Complete Sample of Group-Dominant Early-Type Galaxies?,?? E
A&A 618, A126 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833580 & c ESO 2018 Astrophysics Cold gas in a complete sample of group-dominant early-type galaxies?;?? E. O’Sullivan1, F. Combes2,3, P. Salomé2, L. P. David1, A. Babul4, J. M. Vrtilek1, J. Lim5,6, V. Olivares2, S. Raychaudhury7,8, and G. Schellenberger1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA e-mail: [email protected] 2 LERMA, Observatoire de Paris, CNRS, PSL Univ., Sorbonne Univ., 75014 Paris, France 3 Collège de France, 11 place Marcelin Berthelot, 75005 Paris, France 4 Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 2Y2, Canada 5 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong 6 Laboratory for Space Research, Faculty of Science, The University of Hong Kong, Pokfulam Road, Hong Kong 7 Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India 8 Department of Physics, Presidency University, 86/1 College Street, 700073 Kolkata, India Received 5 June 2018 / Accepted 23 July 2018 ABSTRACT We present IRAM 30 m and APEX telescope observations of CO(1-0) and CO(2-1) lines in 36 group-dominant early-type galaxies, completing our molecular gas survey of dominant galaxies in the Complete Local-volume Groups Sample. We detect CO emission 8 in 12 of the galaxies at >4σ significance, with molecular gas masses in the range ∼0:01−6 × 10 M , as well as CO in absorption in the non-dominant group member galaxy NGC 5354. In total 21 of the 53 CLoGS dominant galaxies are detected in CO and we −1 confirm our previous findings that they have low star formation rates (0.01–1 M yr ) but short depletion times (<1 Gyr) implying rapid replenishment of their gas reservoirs. -
Object Index
Object index 9C 99, 196. IC 9970, 424. A 85, 55,61. IC 4296, 424. A 545, 62. IC 4767, 9. A 559, 424. I Zw 18, 339. A 978, 54. A 1950, 424. Leo II, 168. A 1971, 54. Leo Triplet, 241. A 1419, 55. Local Group, 172, 330, 353, 379, 439, A 1515+2146, 10. 447. A 1847, 424. A 1927, 54. M 49, 142, 143. A 2029, 55. M 51, 7, 131, 270, 271, 296. A 2670, 61. M 67, 88. AM 2244-651, 409, 410. M 81, 7, 131, 132, 163, 241, 271. Andromeda, 144. M 82, 241,273. Arp 152, 223. M 89, 208. Arp 155, 223. M84, 196. Arp 157, 223. M 87, 27, 70, 71, 126, 142, 143, 151, Arp 220, 296. 192,193,196,201,205,381,403. M 92, 88. Carina, 164, 165, 166, 167, 169, 170, M 100, 7, 132. 171. M 101, 239, 240, 241, 242, 243, 247, Centaurus A, 27, 144, 146, 151. 248,273. w Cen, 172. M 104, 107. CGCG 157076, 460. Maffei II, 209. Coma Cluster, 18, 19, 21, 70. Magellanic Cloud, Large (LMC), 256,449. Magellanic Cloud, Small (SMC), 256,447, DDO 154, 163. 449. DDO 170, 163. Magellanic Clouds, 241, 251, 252, 273. Draco, 163, 164, 165, 166, 168, 169, 170, Magellanic galaxies, 94. 171,173. Magellanic stream, 273. Magellanic types, 18. E 294 -21 , 119. Malin 1, 8. E 406-90, 119. Milky Way, 85, 86, 87, 91, 92, 93, 94, 176, 241, 273, 278. F 568-6, 8. Mkn 948, 241. -
Appendix Appendix
Appendix Appendix Abbreviations Here general abbreviations, as used in the text, are explained. Excluded: galaxy classifica- tion (Table 1.2), catalog designations and names (Chapter 3), publications (see next Appendices), or directions (e.g., NW). AGN Active galactic nucleus BCD Blue compact dwarf (galaxy) BSO Blue stellar object CCD Charge coupled device CDM Cold dark matter DSS Digital Sky Survey fst Faintest star GA Great attractor GC Globular cluster GRB Gamma ray burst HII HII region HDF Hubble Deep Field HST Hubble Space Telescope LBV Luminous blue variable LF Luminosity function LG Local Group LPR Light pollution reduction (filter) LSB Low surface brightness (galaxy) OC Open cluster PN Planetary nebula POSS Palomar Observatory Sky Survey QSO Quasi stellar object (quasar) SC Star cloud SCT Schmidt-Cassegrain telescope SDSS Sloan Digital Sky Survey SSC Super star cluster UHC Ultra high contrast (filter) ULIRG Ultra luminous infrared galaxy WR Wolf-Rayet (galaxy) ZOA Zone of avoidance 230 General Literature Books on Galaxies and Related Subjects Appendix Binney, J., Merrifield, M., Galactic Astronomy, Princeton University Press, Princeton, NJ, 1998 Bok, B. J., Bok, P. F., The Milky Way, Harvard University Press, Cambridge, MA, 1981 Combes, F., Boisse, P., Mazure, A., Blanchard, A., Galaxies and Cosmology, Springer- Verlag, Heidelberg, 2002 Elmegreen, D. M., Galaxies and Galactic Structure, Prentice-Hall Inc., Upper Saddle River, NJ, 1998 Ferris, T., Galaxies, Stewart, Tabori & Chang Publ., New York, NY, 1982 Hodge, P. W., Galaxies, Harvard University Press, Cambridge, MA, 1986 Hubble, E. P., Realm of the Nebulae, Dover Publ., Mineola, NY, 1958 Jones, M., Lambourne, R. (eds), An Introduction to Galaxies and Cosmology, Cambridge University Press, Cambridge, 2004 Keel, C. -
2019 Gone Fishin’ – Observing List Notes
The Eldorado Star Party 2019 Telescope Observing Club by Bill Flanagan Houston Astronomical Society Purpose and Rules Welcome to the Annual ESP Telescope Club! The main purpose of this club is to give you an opportunity to observe some of the showpiece objects of the fall season under the pristine skies of Southwest Texas. We have also included a few items on the observing lists that may challenge you to observe some fainter and more obscure objects that present themselves at their very best under the dark skies of the Eldorado Star Party. The rules are simple; just observe the required number of objects listed while you are at the Eldorado Star Party to receive a club badge. Gone Fishin’ West Texas may be known for its dry climate and dry river beds, but in the fall after the sun goes down, the night skies over X-Bar Ranch provide an excellent opportunity to go fishing. Pisces (the Fish) and Pisces Austrinus (the Southern Fish) can be reeled in during most of the night. Delphinus (the Dolphin) is high in the sky just after sunset. The constellation Eridanus (the River) winds its way through the southern portion of the sky, and Cetus (the Sea Monster) can be seen dipping his front flippers into this magnificent winding river. So given this great fall opportunity, the Telescope Observing Club program for the 2019 Eldorado Star Party is “Gone Fishin’.” The program is a list of 27 objects located in the five above mentioned constellations. You only have to reel in 22 of the 27 objects on the list with a telescope to qualify for the Telescope Observing Club badge. -
HB-NGC Index
Object Name Constellation Type Dec RA Season HB Page IC 1 Pegasus Double star +27 43 00 08.4 Fall C-21 IC 2 Cetus Galaxy -12 49 00 11.0 Fall C-39, C-57 IC 3 Pisces Galaxy -00 25 00 12.1 Fall C-39 IC 4 Pegasus Galaxy +17 29 00 13.4 Fall C-21, C-39 IC 5 Cetus Galaxy -09 33 00 17.4 Fall C-39 IC 6 Pisces Galaxy -03 16 00 19.0 Fall C-39 IC 8 Pisces Galaxy -03 13 00 19.1 Fall C-39 IC 9 Cetus Galaxy -14 07 00 19.7 Fall C-39, C-57 IC 10 Cassiopeia Galaxy +59 18 00 20.4 Fall C-03 IC 12 Pisces Galaxy -02 39 00 20.3 Fall C-39 IC 13 Pisces Galaxy +07 42 00 20.4 Fall C-39 IC 16 Cetus Galaxy -13 05 00 27.9 Fall C-39, C-57 IC 17 Cetus Galaxy +02 39 00 28.5 Fall C-39 IC 18 Cetus Galaxy -11 34 00 28.6 Fall C-39, C-57 IC 19 Cetus Galaxy -11 38 00 28.7 Fall C-39, C-57 IC 20 Cetus Galaxy -13 00 00 28.5 Fall C-39, C-57 IC 21 Cetus Galaxy -00 10 00 29.2 Fall C-39 IC 22 Cetus Galaxy -09 03 00 29.6 Fall C-39 IC 24 Andromeda Open star cluster +30 51 00 31.2 Fall C-21 IC 25 Cetus Galaxy -00 24 00 31.2 Fall C-39 IC 29 Cetus Galaxy -02 11 00 34.2 Fall C-39 IC 30 Cetus Galaxy -02 05 00 34.3 Fall C-39 IC 31 Pisces Galaxy +12 17 00 34.4 Fall C-21, C-39 IC 32 Cetus Galaxy -02 08 00 35.0 Fall C-39 IC 33 Cetus Galaxy -02 08 00 35.1 Fall C-39 IC 34 Pisces Galaxy +09 08 00 35.6 Fall C-39 IC 35 Pisces Galaxy +10 21 00 37.7 Fall C-39, C-56 IC 37 Cetus Galaxy -15 23 00 38.5 Fall C-39, C-56, C-57, C-74 IC 38 Cetus Galaxy -15 26 00 38.6 Fall C-39, C-56, C-57, C-74 IC 40 Cetus Galaxy +02 26 00 39.5 Fall C-39, C-56 IC 42 Cetus Galaxy -15 26 00 41.1 Fall C-39, C-56, C-57, C-74 IC -
Revised Shapley Ames.Pdf
A REVISED SHAPLEY-AMES CATALOG OF BRIGHT GALAXIES The Las Canspanas ridge iii Chile during the last stages of construction of the dome for the du Pont 2.5-meter reflector. The du Pout instrument is at the north end of'thr long escarpment. The Swope 1-meter reflector is in the left foreground. Photu courtesy oi'R, J. Bruuito ; 1*<7*J-. A Revised Shapley-Ames Catalog of Bright Galaxies Containing Data on Magnitudes, Types, and Redshifts for Galaxies in the Original Harvard Survey, Updated to Summer 1980. Also Contains a Selection of Photographs Illustrating the Luminosity Classification and a List of Additional Galaxies that Satisfy the Magnitude Limit of the Original Catalog. Allan Sandage and G. A. Tammann CARNEGIE INSTITUTION OF WASHINGTON PUBLICATION 635 WASHINGTON, D.C. • 198 1 ISBN:0-87U79-<i52-:i Libran oi'CongrrssCatalog Card No. 80-6H146 (JompoMtion. Printing, and Binding by Mmden-Stinehour. Inr. ('<»p\ritiht C ]'M\, (Jariit'^it* Institution nf Washington ACKNOWLEDGMENTS We are indebted to Miss B. Flach and Mrs. R. C. Kraan- Korteweg for their help in compiling part of the data. We also owe special thanks to Basil Katem for his large effort in de- termining revised coordinates by measurement of National Geo- graphic-Palomar Sky Survey prints and Uppsala Schmidt plates for most of the listed galaxies, and to John Bedke for his skill in reproducing the photographs. We are especially grateful to R. J. Brucato for his important help in obtaining the most recent plates at Las Campanas. We greatly appreciate the help of several observers for provid- ing prepublication redshift data. -
Cold Gas in a Complete Sample of Group-Dominant Early-Type Galaxies ? E
Astronomy & Astrophysics manuscript no. CO_CLoGS2_astroph_v2 © ESO 2018 September 18, 2018 Cold gas in a complete sample of group-dominant early-type galaxies ? E. O’Sullivan1, F. Combes2;3, P. Salomé2, L. P. David1, A. Babul4, J. M. Vrtilek1, J. Lim5;6, V. Olivares2, S. Raychaudhury7;8, and G. Schellenberger1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA e-mail: [email protected] 2 LERMA, Observatoire de Paris, CNRS, PSL Univ., Sorbonne Univ., 75014 Paris, France 3 Collège de France, 11 place Marcelin Berthelot, 75005 Paris, France 4 Department of Physics and Astronomy, University of Victoria, Victoria, BC, V8W 2Y2, Canada 5 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong 6 Laboratory for Space Research, Faculty of Science, The University of Hong Kong, Pokfulam Road, Hong Kong 7 Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India 8 Department of Physics, Presidency University, 86/1 College Street, 700073 Kolkata, India Received 5 June 2018 / Accepted 23 July 2018 ABSTRACT We present IRAM 30m and APEX telescope observations of CO(1-0) and CO(2-1) lines in 36 group-dominant early-type galaxies, completing our molecular gas survey of dominant galaxies in the Complete Local-volume Groups Sample. We detect CO emission in 8 12 of the galaxies at >4σ significance, with molecular gas masses in the range ∼0.01-6×10 M , as well as CO in absorption in the non-dominant group member galaxy NGC 5354. In total 21 of the 53 CLoGS dominant galaxies are detected in CO and we confirm −1 our previous findings that they have low star formation rates (0.01-1M yr ) but short depletion times (<1 Gyr) implying rapid replenishment of their gas reservoirs. -
Structure and Kinematics of the Peculiar Galaxy NGC 128?
ASTRONOMY & ASTROPHYSICS FEBRUARY I 1999, PAGE 437 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 134, 437–451 (1999) Structure and kinematics of the peculiar galaxy NGC 128? M. D’Onofrio1, M. Capaccioli2,3, P. Merluzzi2,S.Zaggia2, and J. Boulesteix4 1 Dipartimento di Astronomia, Universit`a di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 2 Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131 Napoli, Italy 3 Dipartimento di Scienze Fisiche, Universit`a di Napoli, Mostra d’Oltremare, Padiglione 19, I-80125 Napoli, Italy 4 Observatoire de Marseille, 2 place Le Verrier, F-13248 Marseille Cedex 04, France Received February 13; accepted August 31, 1998 Abstract. This is a multiband photometric and spectro- 1. Introduction scopic study of the peculiar S0 galaxy NGC 128. We present results from broad (B and R) and narrow (Hα) The connection between the boxy/peanut morphology of band optical CCD photometry, near (NIR) and far (FIR) galactic bulges and the presence of a bar is difficult to infrared observations, long slit spectroscopy, and Fabry- prove observationally. The main difficulty comes from the Perot interferometry (CIGALE). fact that the peculiar morphology can be seen only in The peculiar peanut shape morphology of the galaxy almost edge-on systems. is observed both at optical and near-infrared wavelengths. Photometric evidences of a bar in boxy/peanut galax- The stellar disk is thick and distorted (arc-bended), with a ies have been found only in a few cases, e.g. the barred color asymmetry along the major axis due to the presence galaxy NGC 4442 at intermediate inclination (Bettoni of a large amount of dust, estimated through NIR and FIR & Galletta 1994), the edge-on S0 galaxy NGC 1381 (de 6 data of ∼ 610 M , in the region of interaction with the Carvalho & da Costa 1987), NGC 5170 (Dettmar companion galaxy NGC 127.