DOCSLIB.ORG

E. O'sullivan1, K. Kolokythas2, JM Vrtilek1, L

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
E. O'sullivan1, K. Kolokythas2, JM Vrtilek1, L LGG 6 LGG 9 LGG 14 LGG 18 CLoGS: the complete NGC 193 NGC 315 local-volume groups sample NGC 128 NGC 410 1 2 1 1 E. O’Sullivan , K. Kolokythas , J.M. Vrtilek , L. David , NGC 407 G. Schellenberger1, M. Gitti3, S. Giacintucci4, A. Babul5, 6 1: Harvard-Smithsonian Center for Astrophysics, 2: North-West University, South Africa & S. Raychaudhury 3: Universitá di Bologna & INAF-Instituto di Radioastronomia, 4: Naval Research Laboratory, 5: University of Victoria, Canada, 6: IUCAA, India 5' 2' 5' 5' LGG 42 LGG 72 LGG 97 LGG 100 LGG 103 LGG 113 LGG 31 Background NGC 1407 Cluster Background Cluster NGC 1395 NGC 1550 NGC 777 NGC 1066 NGC 1453 NGC 677 NGC 1060 NGC 1400 5' 5' 5' 5' 5' 5' 5' LGG 12 LGG 23 LGG 27 LGG 58 LGG 61 LGG 158 LGG117 Galaxy groups in the local universe: CO survey O’Sullivan et al. (2015, 2018) A&ABackground 573, A111 and A&A 618, A126 results from a complete sample Group Background: Galaxy groups are arguably the most important environment for our understandingNGC 252 of galaxy evolution, AGN feedback,NGC and 524 the development of NGC 2563 NGC 584 NGC 924 the hot intra-group and intra-cluster medium. Most previous studies of groups NGC 940 NGC 1587 have either used optically-selected samples to examine galaxy populations, or X-ray selected samples (usually derived from the Rosat All-Sky Survey) to investigate gas properties. While these approaches have yielded important results, their selection methods mean they are subject to significant biases. 4' Optically-selected5' samples often include false groups, since at low masses 5' 4' 5' 5' 5' selection must be made using only a few galaxies. X-ray selection tends to LGG 167 LGG 66 LGG 78 LGG 80 LGG 126 LGG 138 LGG 185 produce samples dominated by cool-core systems with centrally-concentrated surface brightness, since these central peaks are most easily detected. Background Cluster Sample: We have created the Complete Local-Volume Groups Sample NGC 2768 (CLoGS), an optically-selected statistically-complete sample of 53 groups in the NGC 1106 NGC 1779 nearby Universe (D<80 Mpc), with complete coverage in the X-ray (Chandra NGC 1167 NGC 3078 and XMM-NewtonNGC), multi-frequency978 radio (GMRT 235 and 610 MHz) and, for the NGC 2292 dominant galaxies, CO (IRAM 30m and APEX). This combination of data allows Background us to examine the gas content of the groups, their dynamical state, and the role Cluster of AGN feedback in maintaining their thermal balance. 2' We5' select our sample from the Lyon5' Galaxy Group catalogue (LGG, Garcia5' 5' 5' 5' LGG 236 1993, A&AS 100, 47), choosingLGG 177 groups which have: LGG 205 LGG 232 LGG 255 LGG 262 LGG 278 • ≥ 4 member galaxies (excluding pairs & triples which may lack a common halo) All 53 group-dominant early-type galaxies have been observed in CO(2-1) • ≥ 1 early-type member (as spiral-only groups tend to be hot gas poor) and/or CO(1-0) using the IRAM 30m or APEX telescopes. We detect CO in 21 7 10 galaxies (~40%), with masses 1-610 x10 M¤. This detection rate is roughly • Optical luminosity LB > 3x10 L¤ for the brightest member Background double that of the general early-type population. Comparing radio luminosity to QSO • Declination > -30° (to ensure visibility from GMRT and VLA) NGC 4261 NGC 3665 molecular gas mass (see Figure above),NGC 3923 we find that while some of our galaxies We then expand andNGC 2911refine the galaxy membershipNGC 3325 using the LEDA galaxy NGC 3613 NGC 4008 catalogue, and exclude systems judged to be too rich (clusters) or too poor (too have properties consistent with star formation (the grey band), a large fraction are AGN dominated. However, the presence of CO is not clearly linked to radio few NGCgalaxies 2914 to characterize the population). power, or to the presence of hot gas. This suggests that while group-dominant For more details of sample selection and X-ray properties, see galaxies can build up a CO reservoir through cooling from the hot halo (as in O’Sullivan et al. (2017, MNRAS 472, 1482). galaxy clusters), many acquire it through gas-rich mergers. 5' 5' 5' 5' 5' 5' 5' LGG 310 LGG 276 LGG 329 LGG 341 LGG 345 LGG 351 LGG 314 Radio properties X-ray properties Kolokythas et al. (2018, 2019) MNRAS, 481, 1550 and MNRAS, 489, 2488 Group detection fraction: Of our 53 systems, 41 NGC 4697 ESO 507-25 • 26 (~50%) have a full group-scale X-ray halo (>65 kpc extent, LX>10 erg/s) NGC 4169 NGC 4956 NGC 5061 NGC 5084 40 41 NGC 5153 • 16 (~30%) have a galaxy-scale halo (LX=10 -10 erg/s) NGC 4175 • the remainder have only point-source emission in the dominant galaxy. Of the group-scale halos, ~1/3 are dynamically active, showing signs of ongoing mergers or sloshing (indicating a recent minor merger or tidal encounter). Roughly 65% have cool cores, a higher fraction than in clusters (~50%). Unlike 4' 5' 5' 5' clusters, many of 4'the merging groups retain their cool4' cores. The temperature 5' LGG 338 13 LGG 350 LGG 421 range ofLGG our 457 systems is ~0.4-1.5 keV, equivalentLGG 463 to masses of ~0.5-5 x10 M¤. New groups Background One goal of our sample was to search for new groups, previously undetected in Cluster the X-ray. Of our 26 systems with a full-scale intra-group medium (IGM), 12 were NGC 5044 NGCidentified 7252 as X-ray bright groups NGCfor the7377 first time, of which 8 were undetected NGC 6658 in the Rosat All-Sky Survey (RASS). Examples include: LGG 402 / NGC 5982 41 (bottom row) a faint (LX=3x10 erg/s), cool (0.59 keV) group which lacks a cool NGC 5127 core; LGG 72 / NGC 1060 (above left) a train-wreck merger with a 100 kpc arc of stripped gas linking the two cores; and LGG 398 / NGC 5903 (bottom row) in Our GMRT 235 and 610 MHz observations (~4hrs/target, rms ~0.1mJy/bm which a combination of galaxy interactions and a powerful AGN outburst seem to @610 MHz, ~0.6mJy/bm @ 235 MHz) are well suited to identifying AGN over a have disrupted the5' group core (see O’Sullivan et al. 2018 MNRAS, 473, 5248 for 5' wide range of scales and ages. For the5' group-dominant ellipticals we find:5' 5' more details). In each case, the lack of a relaxed cool core with a strong surface LGG 360 LGG 363 brightness peak probably explains the RASS non-detection. • 46/53 (87%) are detected in our GMRT data (or the NVSS or FIRST surveys) • 13 host jet sources (implying a duty cycle ~1/3) Future plans • 28 host point-like sources NGC 5350 We are currently working on several aspects of the sample, including: • 5 host diffuse sources (e.g., LGGs 31, 117, 185, 310). The origin of emission • MUSE observations of 17 dominant galaxies, providing information on stellar NGC 5354 in these sources is unclear (star formation? disrupted jets? radio phoenices?) NGC 5322 populations and cooling from the hot gas halo. NGC 5353 • Collecting interferometric observations of our CO-detected systems (via 11 of the 13 galaxies with jet sources reside in systems with group-scale NOEMA and ALMA/ACA) to map the gas and understand its origin. X-ray halos and cool cores. The plot above shows cavity enthalpy vs. cooling • Detailed studies of particularly interesting individual systems, e.g., the time (P vs L ) for 5 of our richest groups. Three fall on the relation, with cav cool asymmetric radio source in LGG 113 / NGC 1550. cooling and heating in balance, but two (LGGs 9 and 278) have P =50xL , cav cool • Expanding the sample to include southern and spiral-dominated groups. suggesting that these AGN may be dramatically over-heating their groups. 5' 5' LGG 370 LGG 376 LGG 383 LGG 393 LGG 398 LGG 402 LGG 473 NGC 5846 NGC 7626 NGC 5903 NGC 5982 NGC 7619 NGC 5444 NGC 5490 NGC 5629 NGC 5985 NGC 5898 5' 5' 5' 5' 5' 5' 5' CLoGS gallery: Each panel shows an adaptively smoothed 0.5-2 keV image of a CLoGS group, with an 2.5’x2.5’ optical (DSS or SDSS) image of the dominant early-type galaxy inset. For radio-detected systems, GMRT 610 or 235 MHz contours are overlaid. http://www.sr.bham.ac.uk/~ejos/CLoGS.html.
Load more

Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • NASA's Goddard Space Flight Center Laboratory for High Energy
    1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U.
    [Show full text]
  • Multicolor Surface Photometry of Lenticular Galaxies
    The Astronomical Journal, 129:630–646, 2005 February # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. MULTICOLOR SURFACE PHOTOMETRY OF LENTICULAR GALAXIES. I. THE DATA Sudhanshu Barway School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Y. D. Mayya Instituto Nacional de Astrofisı´ca, O´ ptica y Electro´nica, Apdo. Postal 51 y 216, Luis Enrique Erro 1, 72000 Tonantzintla, Pue., Mexico; [email protected] Ajit K. Kembhavi Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411007, India; [email protected] and S. K. Pandey1 School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Receivedv 2003 Auggust 13; accepted 2004 October 20 ABSTRACT We present multicolor surface and aperture photometry in the B, V, R,andK0 bands for a sample of 34 lenticular galaxies from the Uppsala General Catalogue. From surface photometric analysis, we obtain radial profiles of surface brightness, colors, ellipticity, position angle, and the Fourier coefficients that describe the departure of isophotal shapes from a purely elliptical form; we find the presence of dust lanes, patches, and ringlike structure in several galaxies in the sample. We obtain total integrated magnitudes and colors and find that these are in good agreement with the values from the Third Reference Catalogue. Isophotal colors are correlated with each other, following the sequence expected for early-type galaxies. The color gradients in lenticular galaxies are more negative than the corresponding gradients in elliptical galaxies. There is a good correlation between BÀVand BÀR color gradients, and the mean gradients in the BÀV, BÀR,andVÀK0 colors are À0:13 Æ 0:06, À0:18 Æ 0:06, and À0:25 Æ 0:11 mag dexÀ1 in radius, respectively.
    [Show full text]
  • Download This Article in PDF Format
    A&A 562, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201321493 & c ESO 2014 Astrophysics Li depletion in solar analogues with exoplanets Extending the sample, E. Delgado Mena1,G.Israelian2,3, J. I. González Hernández2,3,S.G.Sousa1,2,4, A. Mortier1,4,N.C.Santos1,4, V. Zh. Adibekyan1, J. Fernandes5, R. Rebolo2,3,6,S.Udry7, and M. Mayor7 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica de Canarias, C/ Via Lactea s/n, 38200 La Laguna, Tenerife, Spain 3 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, 4169-007 Porto, Portugal 5 CGUC, Department of Mathematics and Astronomical Observatory, University of Coimbra, 3049 Coimbra, Portugal 6 Consejo Superior de Investigaciones Científicas, CSIC, Spain 7 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland Received 18 March 2013 / Accepted 25 November 2013 ABSTRACT Aims. We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. Methods. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600–5900 K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs. Results. We confirm significant differences in the Li distribution of solar twins (Teff = T ± 80 K, log g = log g ± 0.2and[Fe/H] = [Fe/H] ±0.2): the full sample of planet host stars (22) shows Li average values lower than “single” stars with no detected planets (60).
    [Show full text]
  • Curriculum Vitae Thomas Matheson
    Curriculum Vitae Thomas Matheson Address: NSF's National Optical-Infrared Astronomy Research Laboratory Community Science and Data Center 950 North Cherry Avenue Tucson, AZ 85719, USA Telephone: (520) 318{8517 Fax: (520) 318{8360 e-mail: [email protected] WWW: http://www.noao.edu/noao/staff/matheson/ Education: University of California, Berkeley, Berkeley, CA Department of Astronomy Ph.D. received June 2000 M.A. received June 1992 PhD Thesis Topic: The Spectral Characteristics of Stripped-Envelope Supernovae Thesis Advisor: Professor Alexei V. Filippenko Harvard University, Cambridge, MA Department of Astronomy & Astrophysics and Physics A.B. magna cum laude, received June 1989 Senior Thesis Topic: Transients in the Solar Transition Region Thesis Advisor: Professor Robert W. Noyes Employment: NSF's National Optical-Infrared Astronomy Research Laboratory (The Former National Optical Astronomy Observatory) Community Science and Data Center Head of Time-Domain Services 2017 { present Astronomer 2018 { present Associate Astronomer 2009 { 2018 (Tenure, 2011) Assistant Astronomer 2004 { 2009 Harvard-Smithsonian Center for Astrophysics Optical and Infrared Division Post-doctoral fellow 2000 { 2004 University of California, Berkeley Department of Astronomy Research Assistant 1991 { 2000 Harvard-Smithsonian Center for Astrophysics Solar and Stellar Physics Division Research Assistant 1989 { 1990 Thomas Matheson|Curriculum Vitae Teaching: Harvard University, Department of Astronomy, Teaching Assistant 2001, 2003 University of California, Berkeley,
    [Show full text]
  • The Cheshire Cat Gravitational Lens: the Formation of a Massive Fossil Group
    THE UNIVERSITY OF ALABAMA University Libraries The Cheshire Cat Gravitational Lens: The Formation of a Massive Fossil Group Jimmy A. Irwin – University of Alabama et al. Deposited 09/10/2018 Citation of published version: Irwin, J., et al. (2015): The Cheshire Cat Gravitational Lens: The Formation of a Massive Fossil Group. The Astrophysical Journal, 806(2). http://dx.doi.org/10.1088/0004- 637X/806/2/268 © 2015. The American Astronomical Society. All rights reserved. The Astrophysical Journal, 806:268 (14pp), 2015 June 20 doi:10.1088/0004-637X/806/2/268 © 2015. The American Astronomical Society. All rights reserved. THE CHESHIRE CAT GRAVITATIONAL LENS: THE FORMATION OF A MASSIVE FOSSIL GROUP Jimmy A. Irwin1, Renato Dupke1,2,3,4, Eleazar R. Carrasco5, W. Peter Maksym1, Lucas Johnson1, and Raymond E. White III1 1 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487, USA; [email protected] 2 Department of Astronomy, University of Michigan, 500 Church St., Ann Arbor, MI 48109, USA 3 Observatório Nacional, Rua Gal. José Cristino 77, São Cristóvão, CEP20921-400 Rio de Janeiro RJ, Brazil 4 Eureka Scientific Inc., 2452 Delmer St. Suite 100, Oakland, CA 94602, USA 5 Gemini Observatory/AURA, Southern Operations Center, AURA, Casilla 603, La Serena, Chile Received 2014 July 4; accepted 2015 April 28; published 2015 June 23 ABSTRACT The Cheshire Cat is a relatively poor group of galaxies dominated by two luminous elliptical galaxies surrounded by at least four arcs from gravitationally lensed background galaxies that give the system a humorous appearance. Our combined optical/X-ray study of this system reveals that it is experiencing a line of sight merger between two groups with a roughly equal mass ratio with a relative velocity of ∼1350 km s−1.
    [Show full text]
  • Sky & Telescope
    Eclipse from the See Sirius B: The Nearest Spot the Other EDGE OF SPACE p. 66 WHITE DWARF p. 30 BLUE PLANETS p. 50 THE ESSENTIAL GUIDE TO ASTRONOMY What Put the Bang in the Big Bang p. 22 Telescope Alignment Made Easy p. 64 Explore the Nearby Milky Way p. 32 How to Draw the Moon p. 54 OCTOBER 2013 Cosmic Gold Rush Racing to fi nd exploding stars p. 16 Visit SkyandTelescope.com Download Our Free SkyWeek App FC Oct2013_J.indd 1 8/2/13 2:47 PM “I can’t say when I’ve ever enjoyed owning anything more than my Tele Vue products.” — R.C, TX Tele Vue-76 Why Are Tele Vue Products So Good? Because We Aim to Please! For over 30-years we’ve created eyepieces and telescopes focusing on a singular target; deliver a cus- tomer experience “...even better than you imagined.” Eyepieces with wider, sharper fields of view so you see more at any power, Rich-field refractors with APO performance so you can enjoy Andromeda as well as Jupiter in all their splendor. Tele Vue products complement each other to pro- vide an observing experience as exquisite in performance as it is enjoyable and effortless. And how do we score with our valued customers? Judging by superlatives like: “in- credible, truly amazing, awesome, fantastic, beautiful, work of art, exceeded expectations by a mile, best quality available, WOW, outstanding, uncom- NP101 f/5.4 APO refractor promised, perfect, gorgeous” etc., BULLSEYE! See these superlatives in with 110° Ethos-SX eye- piece shown on their original warranty card context at TeleVue.com/comments.
    [Show full text]
  • 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.
    [Show full text]
  • 2019 Publication Year 2020-12-18T10:21:10Z
    Publication Year 2019 Acceptance in OA@INAF 2020-12-18T10:21:10Z Title Chandra Early-type Galaxy Atlas Authors þÿKim, Dong-Woo; Anderson, Craig; Burke, Douglas; D Abrusco, Raffaele; Fabbiano, Giuseppina; et al. DOI 10.3847/1538-4365/ab0ca4 Handle http://hdl.handle.net/20.500.12386/28989 Journal THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES Number 241 The Astrophysical Journal Supplement Series, 241:36 (32pp), 2019 April https://doi.org/10.3847/1538-4365/ab0ca4 © 2019. The American Astronomical Society. Chandra Early-type Galaxy Atlas Dong-Woo Kim1 , Craig Anderson1, Douglas Burke1 , Raffaele D’Abrusco1 , Giuseppina Fabbiano1 , Antonella Fruscione1, Jennifer Lauer1, Michael McCollough1 , Douglas Morgan1, Amy Mossman1, Ewan O’Sullivan1 , Alessandro Paggi1 , Saeqa Vrtilek1, and Ginevra Trinchieri2 1 Center for Astrophysics|Harvard & Smithsonian 60 Garden Street, Cambridge, MA 02138, USA 2 INAF-Osservatorio Astronomico di Brera, Via Brera 28, I-20121 Milan, Italy Received 2018 November 30; revised 2019 February 25; accepted 2019 March 3; published 2019 April 16 Abstract The hot interstellar medium (ISM) in early-type galaxies (ETGs) plays a crucial role in understanding their formation and evolution. The structural features of the hot gas identified by Chandra observations point to key evolutionary mechanisms, (e.g., active galactic nuclei, AGN, and stellar feedback, merging history). In our Chandra Galaxy Atlas (CGA) project, taking full advantage of the Chandra capabilities, we systematically analyzed the archival Chandra data of 70 ETGs and produced uniform data products for the hot gas properties. The primary data products are spatially resolved 2D spectral maps of the hot gas from individual galaxies. We emphasize that new features can be identified in the spectral maps that are not readily visible in the surface brightness maps.
    [Show full text]
  • 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.
    [Show full text]