Galaxy Groups and Clouds in the Local (Z~ 0.01) Universe
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Arxiv:1601.00329V3 [Astro-Ph.CO] 19 Aug 2016 Early Data
DES 2015-0085 FERMILAB-PUB-16-003-AE Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 22 August 2016 (MN LATEX style file v2.2) The Dark Energy Survey: more than dark energy - an overview Dark Energy Survey Collaboration: T. Abbott1, F. B. Abdalla2, J. Aleksic´47, S. Allam3, A. Amara4, D. Bacon6, E. Balbinot46, M. Banerji7;8, K. Bechtol56;57, A. Benoit-Levy´ 13;2;12, G. M. Bernstein10, E. Bertin12;13, J. Blazek14, C. Bonnett15, S. Bridle16, D. Brooks2, R. J. Brunner41;20, E. Buckley- Geer3, D. L. Burke11;17, G. B. Caminha51;52, D. Capozzi6, J. Carlsen6, A. Carnero-Rosell18;19, M. Carollo54, M. Carrasco-Kind20;21, J. Carretero9;47, F. J. Castander9, L. Clerkin2, T. Collett6, C. Conselice55, M. Crocce9, C. E. Cunha11, C. B. D’Andrea6, L. N. da Costa19;18, T. M. Davis49, S. Desai25;24, H. T. Diehl3, J. P. Dietrich25;24, S. Dodelson3;27;58, P. Doel2, A. Drlica-Wagner3, J. Estrada3, J. Etherington6, A. E. Evrard22;29, J. Fabbri2, D. A. Finley3, B. Flaugher3, R. J. Foley21;41, P. Fosalba9, J. Frieman27;3, J. Garc´ıa-Bellido43, E. Gaztanaga9, D. W. Gerdes22, T. Giannantonio8;7, D. A. Goldstein44;37, D. Gruen17;11, R. A. Gruendl20;21, P. Guarnieri6, G. Gutierrez3, W. Hartley4, K. Honscheid14;32, B. Jain10, D. J. James1, T. Jeltema53, S. Jouvel2, R. Kessler27;58, A. King49, D. Kirk2, R. Kron27, K. Kuehn33, N. Kuropatkin3, O. Lahav2;?, T. S. Li23, M. Lima19;35, H. Lin3, M. A. G. Maia19;18, M. Makler51, M. Manera2, C. Maraston6, J. L. -
XMM–Newton Observations of NGC 3268 in the Antlia Galaxy Cluster: Characterization of a Hidden Group of Galaxies at Z ≈ 0.41
MNRAS 00, 1 (2018) doi:10.1093/mnras/sty1401 Advance Access publication 2018 May 28 XMM–Newton observations of NGC 3268 in the Antlia Galaxy Cluster: characterization of a hidden group of galaxies at z ≈ 0.41 I. D. Gargiulo,1,4‹ F. Garc´ıa,2,3,4,5 J. A. Combi,2,3,4 J. P. Caso1,2,4 and L. P. Bassino1,2,4 1Instituto de Astrof´ısica de La Plata (CCT La Plata, CONICET, UNLP), Paseo del Bosque s/n, B1900FWA La Plata, Argentina 2Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina 3Instituto Argentino de Radioastronom´ıa (CCT-La Plata, CONICET; CICPBA), C.C. No. 5, 1894 Villa Elisa, Argentina 4Consejo Nacional de Investigaciones Cient´ıficas y Tecnicas,´ Rivadavia 1917, Ciudad Autonoma´ de Buenos Aires, C1033AAJ Buenos Aires, Argentina 5Laboratoire AIM (UMR 7158 CEA/DRF-CNRS-Universite´ Paris Diderot), Irfu/Departament´ d’Astrophysique, Centre de Saclay, F-91191 Gif-sur-Yvette, France Accepted 2018 May 25. Received 2018 May 25; in original form 2016 December 1 ABSTRACT We report on a detailed X-ray study of the extended emission of the intracluster medium (ICM) around NGC 3268 in the Antlia Cluster of galaxies, together with a characterization of an extended source in the field, namely a background cluster of galaxies at z ≈ 0.41, which was previously accounted as an X-ray point source. The spectral properties of the extended emission of the gas present in Antlia were studied using data from the XMM–Newton satellite, complemented with optical images of Cerro Tololo Inter-American Observatory (CTIO) Blanco telescope, to attain for associations of the optical sources with the X-ray emission. -
198 7Apj. . .312L. .11J the Astrophysical Journal, 312:L11-L15
.11J The Astrophysical Journal, 312:L11-L15,1987 January 1 .312L. © 1987. The American Astronomical Society. All rights reserved. Printed in U.S.A. 7ApJ. 198 INTERSTELLAR DUST IN SHAPLEY-AMES ELLIPTICAL GALAXIES M. Jura and D. W. Kim Department of Astronomy, University of California, Los Angeles AND G. R. Knapp and P. Guhathakurta Princeton University Observatory Received 1986 August 11; accepted 1986 September 30 ABSTRACT We have co-added the IRAS survey data at the positions of the brightest elliptical galaxies in the Revised Shapley-Ames Catalog to increase the sensitivity over that of the IRAS Point Source Catalog. More than half of 7 8 the galaxies (with Bj< \\ mag) are detected at 100 /xm with flux levels indicating, typically, 10 or 10 M0 of cold interstellar matter. The presence of cold gas in ellipticals thus appears to be the rule rather than the exception. Subject headings: galaxies: general — infrared: sources I. INTRODUCTION infrared emission from the elliptical galaxy in the line of sight. The traditional view of early-type galaxies is that they are Our criteria for a real detection are as follows: essentially free of interstellar matter. However, with advances 1. The optical position of the galaxy and the position of the in instrumental sensitivity, it has become possible to observe IRAS source agree to better than V. (The agreement is usually 21 cm emission (Knapp, Turner, and Cunniffe 1985; Wardle much better than T.) and Knapp 1986), optical dust patches (Sadler and Gerhard 2. The flux is at least 3 times the r.m.s. noise. -
Early-Type Galaxies in the Antlia Cluster: Catalogue and Isophotal Analysis
MNRAS 477, 1760–1771 (2018) doi:10.1093/mnras/sty611 Advance Access publication 2018 March 7 Early-type galaxies in the Antlia cluster: catalogue and isophotal analysis Juan P. Calderon,´ 1,2,3‹ Lilia P. Bassino,1,2,3 Sergio A. Cellone1,3,4 and Mat´ıas Gomez´ 5 1Consejo Nacional de Investigaciones Cient´ıficas y Tecnicas,´ Rivadavia 1917, Buenos Aires, Argentina 2Instituto de Astrof´ısica de La Plata (CCT La Plata - CONICET - UNLP), La Plata, Argentina 3Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina Downloaded from https://academic.oup.com/mnras/article-abstract/477/2/1760/4924514 by Universidad Andres Bello user on 28 May 2019 4Complejo Astronomico´ El Leoncito (CONICET - UNLP - UNC - UNSJ), San Juan, Argentina 5Departamento de Ciencias F´ısicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Santiago, Chile Accepted 2018 February 26. Received 2018 February 26; in original form 2017 December 14 ABSTRACT We present a statistical isophotal analysis of 138 early-type galaxies in the Antlia cluster, located at a distance of ∼ 35 Mpc. The observational material consists of CCD images of four 36 × 36 arcmin2 fields obtained with the MOSAIC II camera at the Blanco 4-m telescope at Cerro Tololo Interamerican Observatory. Our present work supersedes previous Antlia studies in the sense that the covered area is four times larger, the limiting magnitude is MB ∼−9.6 mag, and the surface photometry parameters of each galaxy are derived from Sersic´ model fits extrapolated to infinity. In a companion previous study we focused on the scaling relations obtained by means of surface photometry, and now we present the data, on which the previous paper is based, the parameters of the isophotal fits as well as an isophotal analysis. -
Chapter 1 Inventory of the Local Universe
Chapter 1 Inventory of the Local Universe 1 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE 1.1 The major types of galaxies: Hubble-Sandage system Hubble-Sandage Tuning Fork: Kormendy & Bender, ApJ 464, L119 (1996), revised for ellipticals. Other classification schemes: e.g. de Vaucouleurs (1959), van den Bergh (1960/66), Yerkes (Morgan, 1957 ff) 2 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE Primary classification criteria of commonly used Hubble-Sandage system: Bulge-to-disk ratio (S0/Sa: 5 to 0.3, Sb: 1 to 0.1, Sc/Irr: 0.2 to 0) Opening angle of spiral arms (Sa: 0 to 10, Sb: 5 to 20, Sc: 10 to 30 degrees) Bars Physical parameters varying along the Hubble-Sandage system: Stellar mass M increases from irregulars (108M ) to ellipticals (1012M ) Specific Angular Momentum J=M of baryons increases from ellipticals to spirals Mean age increases from irregulars through spirals to ellipticals (B-V increases from 0.3 to 1.0, mass-to-light M=LB ratio increases from about 2 to 10) Mean stellar density of spheroids increases with decreasing spheroid luminosity Mean surface brightness of disks increases with luminosity cold gas content increases along Hubble sequence (fraction of baryonic mass: 0 in E/S0, 0.1 to 0.3 in Sa to Sc, up to 0.9 in Irr) hot gas content only significant in massive E (few percent of baryonic mass) 3 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE Examples for Normal Galaxies: Elliptical (E) Galaxies: The ellipticals M 84 (right) and M 86 (middle) in the Virgo cluster (NOAO). -
Disk Mass and Disk Heating in the Spiral Galaxy NGC 3223?
A&A 576, A57 (2015) Astronomy DOI: 10.1051/0004-6361/201425279 & c ESO 2015 Astrophysics Disk mass and disk heating in the spiral galaxy NGC 3223? G. Gentile1;2, C. Tydtgat1;3, M. Baes1, G. De Geyter1, M. Koleva1, G. W. Angus2, W. J. G. de Blok4;5;6, W. Saftly1, and S. Viaene1 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, 9000 Gent, Belgium e-mail: [email protected] 2 Department of Physics and Astrophysics, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium 3 Department of Solid State Sciences, Krijgslaan 281, 9000 Gent, Belgium 4 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands 5 Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa 6 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands Received 5 November 2014 / Accepted 11 February 2015 ABSTRACT We present the stellar and gaseous kinematics of an Sb galaxy, NGC 3223, with the aim of determining the vertical and radial stellar velocity dispersion as a function of radius, which can help to constrain disk heating theories. Together with the observed NIR photometry, the vertical velocity dispersion is also used to determine the stellar mass-to-light (M=L) ratio, typically one of the largest uncertainties when deriving the dark matter distribution from the observed rotation curve. We find a vertical-to-radial velocity dispersion ratio of σz/σR = 1:21 ± 0:14, significantly higher than expectations from known correlations, and a weakly-constrained Ks-band stellar M=L ratio in the range 0.5–1.7, which is at the high end of (but consistent with) the predictions of stellar population synthesis models. -
WALLABY Pre-Pilot Survey: Two Dark Clouds in the Vicinity of NGC 1395
University of Texas Rio Grande Valley ScholarWorks @ UTRGV Physics and Astronomy Faculty Publications and Presentations College of Sciences 2021 WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395 O. I. Wong University of Western Australia A. R. H. Stevens B. Q. For University of Western Australia Tobias Westmeier M. Dixon See next page for additional authors Follow this and additional works at: https://scholarworks.utrgv.edu/pa_fac Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation O I Wong, A R H Stevens, B-Q For, T Westmeier, M Dixon, S-H Oh, G I G Józsa, T N Reynolds, K Lee-Waddell, J Román, L Verdes-Montenegro, H M Courtois, D Pomarède, C Murugeshan, M T Whiting, K Bekki, F Bigiel, A Bosma, B Catinella, H Dénes, A Elagali, B W Holwerda, P Kamphuis, V A Kilborn, D Kleiner, B S Koribalski, F Lelli, J P Madrid, K B W McQuinn, A Popping, J Rhee, S Roychowdhury, T C Scott, C Sengupta, K Spekkens, L Staveley-Smith, B P Wakker, WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395, Monthly Notices of the Royal Astronomical Society, 2021;, stab2262, https://doi.org/10.1093/ mnras/stab2262 This Article is brought to you for free and open access by the College of Sciences at ScholarWorks @ UTRGV. It has been accepted for inclusion in Physics and Astronomy Faculty Publications and Presentations by an authorized administrator of ScholarWorks @ UTRGV. For more information, please contact [email protected], [email protected]. -
III. Characteristics of Group Central Radio Galaxies in the Local Universe
MNRAS 489, 2488–2504 (2019) doi:10.1093/mnras/stz2082 Advance Access publication 2019 July 30 The complete local volume groups sample – III. Characteristics of group central radio galaxies in the Local Universe Konstantinos Kolokythas,1‹ Ewan O’Sullivan ,2 Huib Intema ,3,4 Somak Raychaudhury ,1,5,6 Arif Babul,7,8 Simona Giacintucci9 and Myriam Gitti10,11 1Inter-University Centre for Astronomy and Astrophysics, Pune University Campus, Ganeshkhind, Pune, Maharashtra 411007, India 2Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 3International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia 4 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, the Netherlands Downloaded from https://academic.oup.com/mnras/article/489/2/2488/5541074 by guest on 23 September 2021 5School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK 6Department of Physics, Presidency University, 86/1 College Street, Kolkata 700073, India 7Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1, Canada 8Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland 9Naval Research Laboratory, 4555 Overlook Avenue SW, Code 7213, Washington, DC 20375, USA 10Dipartimento di Fisica e Astronomia, Universita´ di Bologna, via Gobetti 93/2, 40129 Bologna, Italy 11INAF, Istituto di Radioastronomia di Bologna, via Gobetti 101, 40129 Bologna, Italy Accepted 2019 July 22. Received 2019 July 17; in original form 2019 May 31 ABSTRACT Using new 610 and 235 MHz observations from the giant metrewave radio telescope (GMRT) in combination with archival GMRT and very large array (VLA) survey data, we present the radio properties of the dominant early-type galaxies in the low-richness subsample of the complete local-volume groups sample (CLoGS; 27 galaxy groups) and provide results for the radio properties of the full CLoGS sample for the first time. -
Cold Gas, Star Formation, and Substructure in the Nearby Antlia Cluster
University of Groningen KAT-7 science verification Hess, Kelley M.; Jarrett, T. H.; Carignan, Claude; Passmoor, Sean S.; Goedhart, Sharmila Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1093/mnras/stv1372 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: 2015 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Hess, K. M., Jarrett, T. H., Carignan, C., Passmoor, S. S., & Goedhart, S. (2015). KAT-7 science verification: Cold gas, star formation, and substructure in the nearby Antlia Cluster. Monthly Notices of the Royal Astronomical Society, 452(2), 1617-1636. https://doi.org/10.1093/mnras/stv1372 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. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. -
Dark Energy and Extending the Geodesic Equations of Motion: Connecting the Galactic and Cosmological Length Scales
General Relativity and Gravitation (2011) DOI 10.1007/s10714-010-1043-z RESEARCHARTICLE A. D. Speliotopoulos Dark energy and extending the geodesic equations of motion: connecting the galactic and cosmological length scales Received: 23 May 2010 / Accepted: 16 June 2010 c The Author(s) 2010 Abstract Recently, an extension of the geodesic equations of motion using the Dark Energy length scale was proposed. Here, we apply this extension to analyz- ing the motion of test particles at the galactic scale and longer. A cosmological check of the extension is made using the observed rotational velocity curves and core sizes of 1,393 spiral galaxies. We derive the density profile of a model galaxy using this extension, and with it, we calculate σ8 to be 0.73±0.12; this is within +0.049 experimental error of the WMAP value of 0.761−0.048. We then calculate R200 to be 206±53 kpc, which is in reasonable agreement with observations. Keywords Dark energy, Galactic density profile, Density fluctuations, Extensions of the geodesic equations of motion, Galactic rotation curves 1 Introduction In a previous paper [1], we constructed an extension of the geodesic equations of motion (GEOM). This construction is possible because with the discovery of +0.82 −30 3 Dark Energy, ΛDE = (7.21−0.84) × 10 g/cm [2; 3; 4], there is now a length 1/2 scale, λDE = c/(ΛDEG) , associated with the universe. As this length scale is also not associated with the mass of any known particle, this extension does not violate various statements of the equivalence principle. -
Gravitational Potential and X-Ray Luminosities of Early-Type Galaxies Observed with XMM-Newton and Chandra
A&A 501, 157–169 (2009) Astronomy DOI: 10.1051/0004-6361/200810978 & c ESO 2009 Astrophysics Gravitational potential and X-ray luminosities of early-type galaxies observed with XMM-Newton and Chandra R. Nagino and K. Matsushita Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, 162-8601 Tokyo, Japan e-mail: [email protected]; [email protected] Received 17 September 2008 / Accepted 25 March 2009 ABSTRACT Aims. We study the dark matter content in early-type galaxies and investigate whether X-ray luminosities of early-type galaxies are determined by the surrounding gravitational potential. Methods. We derived gravitational mass profiles of 22 early-type galaxies observed with XMM-Newton and Chandra. Results. Sixteen galaxies show constant or decreasing radial temperature profiles, and their X-ray luminosities are consistent with kinematical energy input from stellar mass loss. The temperature profiles of the other 6 galaxies increase with radius, and their X-ray luminosities are significantly higher. The integrated mass-to-light ratio of each galaxy is constant at that of stars within 0.5–1 re,and increases with radius, where re is the effective radius of a galaxy. The scatter of the central mass-to-light ratio of galaxies was less in K-band light. At 3 re, the integrated mass-to-light ratios of galaxies with flat or decreasing temperature profiles are twice the value at 0.5 re, where the stellar mass dominates, and at 6 re, these increase to three times the value at 0.5 re. Conclusions. This feature should reflect common dark and stellar mass distributions in early-type galaxies: within 3 re, the mass of dark matter is similar to the stellar mass, while within 6 re, the former is larger than the latter by a factor of two. -
ALABAMA University Libraries
THE UNIVERSITY OF ALABAMA University Libraries O VI In Elliptical Galaxies: Indicators of Cooling Flows Joel N. Bregman – University of Michigan Eric D. Miller – MIT Alex E. Athey – Carnegie Institution of Washington Jimmy A. Irwin – University of Michigan Deposited 09/13/2018 Citation of published version: Bregman, J., Miller, E., Athey, A., Irwin, J. (2005): O VI In Elliptical Galaxies: Indicators of Cooling Flows The Astrophysical Journal, 635(2). DOI: 10.1086/497421 © 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. The Astrophysical Journal, 635:1031–1043, 2005 December 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. O vi IN ELLIPTICAL GALAXIES: INDICATORS OF COOLING FLOWS Joel N. Bregman Department of Astronomy, University of Michigan, Ann Arbor, MI 48109; [email protected] Eric D. Miller Kavli Institute for Astrophysics and Space Science, MIT, Cambridge, MA 02139; [email protected] Alex E. Athey The Observatories, Carnegie Institution of Washington, Pasadena, CA 91101; [email protected] and Jimmy A. Irwin Department of Astronomy, University of Michigan, Ann Arbor, MI 48109; [email protected] Received 2005 April 25; accepted 2005 August 23 ABSTRACT Early-type galaxies often contain a hot X-ray–emitting interstellar medium [(3 8) ; 106 K] with an apparent radiative cooling time much less than a Hubble time. If unopposed by a heating mechanism, the gas will radiatively 4 À1 cool to temperatures P10 K at a rate proportional to LX /TX , typically 0.03–1 M yr . We can test whether gas is cooling through the 3 ; 105 K range by observing the O vi doublet, whose luminosity is proportional to the cooling rate.