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The Local Radio-Galaxy Population at 20
Mon. Not. R. Astron. Soc. 000, 1–?? (2013) Printed 2 December 2013 (MN LATEX style file v2.2) The local radio-galaxy population at 20GHz Elaine M. Sadler1⋆, Ronald D. Ekers2, Elizabeth K. Mahony3, Tom Mauch4,5, Tara Murphy1,6 1Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006, Australia 2Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia 3ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands 4Oxford Astrophysics, Department of Physics, Keble Road, Oxford OX1 3RH 5SKA Africa, 3rd Floor, The Park, Park Road, Pinelands, 7405, South Africa 6School of Information Technologies, The University of Sydney, NSW 2006, Australia Accepted 0000 December 08. Received 0000 December 08; in original form 0000 December 08 ABSTRACT We have made the first detailed study of the high-frequency radio-source population in the local universe, using a sample of 202 radio sources from the Australia Telescope 20GHz (AT20G) survey identified with galaxies from the 6dF Galaxy Survey (6dFGS). The AT20G- 6dFGS galaxies have a median redshift of z=0.058 and span a wide range in radio luminosity, allowing us to make the first measurement of the local radio luminosity function at 20GHz. Our sample includes some classical FR-1 and FR-2 radio galaxies, but most of the AT20G-6dFGS galaxies host compact (FR-0) radio AGN which appear lack extended radio emission even at lower frequencies. Most of these FR-0 sources show no evidence for rela- tivistic beaming, and the FR-0 class appears to be a mixed population which includes young Compact Steep-Spectrum (CSS) and Gigahertz-Peaked Spectrum (GPS) radio galaxies. -
V. Spatially-Resolved Stellar Angular Momentum, Velocity Dispersion, and Higher Moments of the 41 Most Massive Local Early-Type Galaxies
MNRAS 000,1{20 (2016) Preprint 9 September 2016 Compiled using MNRAS LATEX style file v3.0 The MASSIVE Survey - V. Spatially-Resolved Stellar Angular Momentum, Velocity Dispersion, and Higher Moments of the 41 Most Massive Local Early-Type Galaxies Melanie Veale,1;2 Chung-Pei Ma,1 Jens Thomas,3 Jenny E. Greene,4 Nicholas J. McConnell,5 Jonelle Walsh,6 Jennifer Ito,1 John P. Blakeslee,5 Ryan Janish2 1Department of Astronomy, University of California, Berkeley, CA 94720, USA 2Department of Physics, University of California, Berkeley, CA 94720, USA 3Max Plank-Institute for Extraterrestrial Physics, Giessenbachstr. 1, D-85741 Garching, Germany 4Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 5Dominion Astrophysical Observatory, NRC Herzberg Institute of Astrophysics, Victoria BC V9E2E7, Canada 6George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present spatially-resolved two-dimensional stellar kinematics for the 41 most mas- ∗ 11:8 sive early-type galaxies (MK . −25:7 mag, stellar mass M & 10 M ) of the volume-limited (D < 108 Mpc) MASSIVE survey. For each galaxy, we obtain high- quality spectra in the wavelength range of 3650 to 5850 A˚ from the 246-fiber Mitchell integral-field spectrograph (IFS) at McDonald Observatory, covering a 10700 × 10700 field of view (often reaching 2 to 3 effective radii). We measure the 2-D spatial distri- bution of each galaxy's angular momentum (λ and fast or slow rotator status), velocity dispersion (σ), and higher-order non-Gaussian velocity features (Gauss-Hermite mo- ments h3 to h6). -
Jet-Induced Star Formation in 3C 285 and Minkowski's Object⋆
A&A 574, A34 (2015) Astronomy DOI: 10.1051/0004-6361/201424932 & c ESO 2015 Astrophysics Jet-induced star formation in 3C 285 and Minkowski’s Object? Q. Salomé, P. Salomé, and F. Combes LERMA, Observatoire de Paris, CNRS UMR 8112, 61 avenue de l’Observatoire, 75014 Paris, France e-mail: [email protected] Received 5 September 2014 / Accepted 6 November 2014 ABSTRACT How efficiently star formation proceeds in galaxies is still an open question. Recent studies suggest that active galactic nucleus (AGN) can regulate the gas accretion and thus slow down star formation (negative feedback). However, evidence of AGN positive feedback has also been observed in a few radio galaxies (e.g. Centaurus A, Minkowski’s Object, 3C 285, and the higher redshift 4C 41.17). Here we present CO observations of 3C 285 and Minkowski’s Object, which are examples of jet-induced star formation. A spot (named 3C 285/09.6 in the present paper) aligned with the 3C 285 radio jet at a projected distance of ∼70 kpc from the galaxy centre shows star formation that is detected in optical emission. Minkowski’s Object is located along the jet of NGC 541 and also shows star formation. Knowing the distribution of molecular gas along the jets is a way to study the physical processes at play in the AGN interaction with the intergalactic medium. We observed CO lines in 3C 285, NGC 541, 3C 285/09.6, and Minkowski’s Object with the IRAM 30 m telescope. In the central galaxies, the spectra present a double-horn profile, typical of a rotation pattern, from which we are able to estimate the molecular gas density profile of the galaxy. -
Arxiv:1801.08245V2 [Astro-Ph.GA] 14 Feb 2018
Draft version June 21, 2021 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE MASSIVE SURVEY IX: PHOTOMETRIC ANALYSIS OF 35 HIGH MASS EARLY-TYPE GALAXIES WITH HST WFC3/IR1 Charles F. Goullaud Department of Physics, University of California, Berkeley, CA, USA; [email protected] Joseph B. Jensen Utah Valley University, Orem, UT, USA John P. Blakeslee Herzberg Astrophysics, Victoria, BC, Canada Chung-Pei Ma Department of Astronomy, University of California, Berkeley, CA, USA Jenny E. Greene Princeton University, Princeton, NJ, USA Jens Thomas Max Planck-Institute for Extraterrestrial Physics, Garching, Germany. Draft version June 21, 2021 ABSTRACT We present near-infrared observations of 35 of the most massive early-type galaxies in the local universe. The observations were made using the infrared channel of the Hubble Space Telescope (HST ) Wide Field Camera 3 (WFC3) in the F110W (1.1 µm) filter. We measured surface brightness profiles and elliptical isophotal fit parameters from the nuclear regions out to a radius of ∼10 kpc in most cases. We find that 37% (13) of the galaxies in our sample have isophotal position angle rotations greater than 20◦ over the radial range imaged by WFC3/IR, which is often due to the presence of neighbors or multiple nuclei. Most galaxies in our sample are significantly rounder near the center than in the outer regions. This sample contains six fast rotators and 28 slow rotators. We find that all fast rotators are either disky or show no measurable deviation from purely elliptical isophotes. Among slow rotators, significantly disky and boxy galaxies occur with nearly equal frequency. -
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, -
Sardinia Radio Telescope Observations of Abell 194
University of Groningen Sardinia Radio Telescope observations of Abell 194. The intra-cluster magnetic field power spectrum Govoni, F.; Murgia, M.; Vacca, V.; Loi, F.; Girardi, M.; Gastaldello, F.; Giovannini, G.; Feretti, L.; Paladino, R.; Carretti, E. Published in: Astronomy and astrophysics DOI: 10.1051/0004-6361/201630349 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2017 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Govoni, F., Murgia, M., Vacca, V., Loi, F., Girardi, M., Gastaldello, F., Giovannini, G., Feretti, L., Paladino, R., Carretti, E., Concu, R., Melis, A., Poppi, S., Valente, G., Bernardi, G., Bonafede, A., Boschin, W., Brienza, M., Clarke, T. E., ... Vazza, F. (2017). Sardinia Radio Telescope observations of Abell 194. The intra-cluster magnetic field power spectrum. Astronomy and astrophysics, 603, [A122]. https://doi.org/10.1051/0004-6361/201630349 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. -
GALEX UV COLOR RELATIONS for NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R
The Astrophysical Journal Supplement Series, 173:597Y606, 2007 December # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALEX UV COLOR RELATIONS FOR NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R. Michael Rich,2 Sukyoung K. Yi,3 Young-Wook Lee,3 Alessandro Boselli,1 Armando Gil de Paz,4 Samuel Boissier,1 Ste´phane Charlot,5 Samir Salim,2 Luciana Bianchi,6 Tom A. Barlow,7 Karl Forster,7 Peter G. Friedman,7 Timothy M. Heckman,8 Barry F. Madore,9 D. Christopher Martin,7 Bruno Milliard,1 Patrick Morrissey,7 Susan G. Neff,10 David Schiminovich,11 Mark Seibert,7 Todd Small,7 Alex S. Szalay,8 Barry Y. Welsh,12 and Ted K. Wyder7 Received 2006 May 4; accepted 2006 July 20 ABSTRACT We use GALEX/optical photometry to construct color-color relationships for early-type galaxies sorted by mor- phological type. We have matched objects in the GALEX GR1 public release and the first IR1.1 internal release, with the RC3 early-type galaxies having a morphological type À5:5 T < À1:5, with mean error on T < 1:5 and mean error on (B À V )T < 0:05. After visual inspection of each match, we are left with 130 galaxies with reliable GALEX pipeline photometry in the far-UVand near-UV bands. This sample is divided into ellipticals (À5:5 T < À3:5) and lenticulars (À3:5 T < À1:5). After correction for Galactic extinction, the color-color diagrams FUV À NUV versus (B À V )Tc are plotted for the two subsamples. -
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 -
The Parkes Quarter-Jansky Flat-Spectrum Sample
A&A 386, 97–113 (2002) Astronomy DOI: 10.1051/0004-6361:20020119 & c ESO 2002 Astrophysics The Parkes quarter-Jansky flat-spectrum sample I. Sample selection and source identifications? C. A. Jackson1,J.V.Wall2,P.A.Shaver3,K.I.Kellermann4,I.M.Hook2, and M. R. S. Hawkins5 1 Research School of Astronomy & Astrophysics, The Australian National University, Mount Stromlo Observatory, Canberra, Australia 2 Department of Astrophysics, University of Oxford, Nuclear and Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei M¨unchen, Germany 4 National Radio Astronomy Observatory, Edgemont Road, Charlottesville, VA 22903-2475, USA 5 Royal Observatory, Blackford Hill, Edinburgh EH3 9HJ, UK Received 7 November 2001 / Accepted 22 January 2002 Abstract. We present a new sample of quarter-Jansky flat-spectrum radio sources selected to search for high- redshift quasars and to study the evolution of the flat-spectrum quasar population. The sample comprises 878 radio 5GHz ≥− ∝ α sources selected from the Parkes catalogues with spectral indices α2.7GHz 0.4 where Sν ν .Thesample covers all right ascensions and the declination range from −80◦. 0to+2◦. 5, excluding low galactic latitudes (| b |< 10◦) and the Magellanic Cloud regions. We have obtained improved radio source positions, firstly to reconfirm the majority of the existing identifications, and secondly, using digitized sky-survey data and deep B, Gunn-i and Gunn-z CCD-imaging, to find optical identifications for 223 previously-unidentified sources. We present the final catalogue of 878 flat-spectrum sources: 827 are compact radio sources identified with galaxies, quasars and BL Lac objects, 38 have either extended radio structure or are identified with Galactic objects (PN, HII or non-compact radio source), 4 are obscured by Galactic stars, and 9 (1 per cent of the total sample) remain unidentified. -
Arxiv:2010.08565V1 [Astro-Ph.GA] 16 Oct 2020
MNRAS 000,1–18 (2020) Preprint 20 October 2020 Compiled using MNRAS LATEX style file v3.0 WISDOM project - VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas Mark D. Smith,1★ Martin Bureau,1,2 Timothy A. Davis,3 Michele Cappellari,1 Lijie Liu,1 Kyoko Onishi,4,5,6 Satoru Iguchi,5,6 Eve V. North,3 and Marc Sarzi7 1Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK 2Yonsei Frontier Lab and Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea 3School of Physics & Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, UK 4Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Ehime, 790-8577, Japan 5Department of Astronomical Science, SOKENDAI (The Graduate University of Advanced Studies), Mitaka, Tokyo 181-8588, Japan 6National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Tokyo, 181-8588, Japan 7Armagh Observatory and Planetarium, College Hill, Armagh, BT61 DG, UK Accepted 2020 October 15. Received 2020 October 5; in original form 2020 February 11 ABSTRACT Empirical correlations between the masses of supermassive black holes (SMBHs) and properties of their host galaxies are well-established. Among these is the correlation with the flat rotation velocity of each galaxy measured either at a large radius in its rotation curve or via a spatially-integrated emission line width. We propose here the use of the de-projected integrated CO emission line width as an alternative tracer of this rotation velocity, that has already been shown useful for the Tully- Fisher (luminosity-rotation velocity) relation. -
V. Spatially Resolved Stellar Angular Momentum, Velocity Dispersion, and Higher Moments of the 41 Most Massive Local Early-Type Galaxies
MNRAS 464, 356–384 (2017) doi:10.1093/mnras/stw2330 Advance Access publication 2016 September 14 The MASSIVE Survey – V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies 1,2‹ 1‹ 3 4 Melanie Veale, Chung-Pei Ma, Jens Thomas, Jenny E. Greene, Downloaded from https://academic.oup.com/mnras/article-abstract/464/1/356/2194689 by Princeton University user on 27 August 2019 Nicholas J. McConnell,5 Jonelle Walsh,6 Jennifer Ito,1 John P. Blakeslee5 andRyanJanish2 1Department of Astronomy, University of California, Berkeley, CA 94720, USA 2Department of Physics, University of California, Berkeley, CA 94720, USA 3Max Plank-Institute for Extraterrestrial Physics, Giessenbachstr. 1, D-85741 Garching, Germany 4Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 5Dominion Astrophysical Observatory, NRC Herzberg Institute of Astrophysics, Victoria, BC V9E2E7, Canada 6George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA Accepted 2016 September 13. Received 2016 September 9; in original form 2016 July 18 ABSTRACT We present spatially resolved two-dimensional stellar kinematics for the 41 most massive ∗ 11.8 early-type galaxies (ETGs; MK −25.7 mag, stellar mass M 10 M)ofthevolume- limited (D < 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650–5850 Å from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec × 107 arcsec field of view (often reaching 2 to 3 effective radii).