The Herschel Virgo Cluster Survey. XI. Environmental Effects On
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Near-Infrared Luminosity Relations and Dust Colors L
A&A 578, A47 (2015) Astronomy DOI: 10.1051/0004-6361/201525817 & c ESO 2015 Astrophysics Obscuration in active galactic nuclei: near-infrared luminosity relations and dust colors L. Burtscher1, G. Orban de Xivry1, R. I. Davies1, A. Janssen1, D. Lutz1, D. Rosario1, A. Contursi1, R. Genzel1, J. Graciá-Carpio1, M.-Y. Lin1, A. Schnorr-Müller1, A. Sternberg2, E. Sturm1, and L. Tacconi1 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Gießenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, 69978 Ramat Aviv, Israel Received 5 February 2015 / Accepted 5 April 2015 ABSTRACT We combine two approaches to isolate the AGN luminosity at near-IR wavelengths and relate the near-IR pure AGN luminosity to other tracers of the AGN. Using integral-field spectroscopic data of an archival sample of 51 local AGNs, we estimate the fraction of non-stellar light by comparing the nuclear equivalent width of the stellar 2.3 µm CO absorption feature with the intrinsic value for each galaxy. We compare this fraction to that derived from a spectral decomposition of the integrated light in the central arcsecond and find them to be consistent with each other. Using our estimates of the near-IR AGN light, we find a strong correlation with presumably isotropic AGN tracers. We show that a significant offset exists between type 1 and type 2 sources in the sense that type 1 MIR X sources are 7 (10) times brighter in the near-IR at log LAGN = 42.5 (log LAGN = 42.5). -
X-Ray Study of Extended Emission Around M86 Observed with Suzaku
Publ. Astron. Soc. Japan (2017) 00(0), 1–17 1 doi: 10.1093/pasj/xxx000 X-ray study of extended emission around M86 observed with Suzaku Ukyo HISHI, Ryuichi FUJIMOTO, Misato KOTAKE, Hiromasa ITO, Keigo TANAKA, Yu KAI, Yuya KINOSHITA Faculty of Mathematics and Physics, Kanazawa University, Kakuma-machi, Kanazawa, Ishikawa 920-1192 ∗E-mail: [email protected], [email protected] Received 2017 January 10; Accepted 2017 February 15 Abstract We analyzed the Suzaku data of M86 and its adjacent regions to study the extended emission around it. The M86 core, the plume, and the tail extending toward the northwest were clearly detected, as well as the extended halo around them. From the position angle ∼ 45◦ to ∼ 275◦, the surface brightness distribution of the core and the extended halo was represented relatively well with a single β-model of β ∼ 0.5 up to 15′–20′. The X-ray spectra of the core was represented with a two-temperature model of kT ∼ 0.9 keV and ∼ 0.6 keV. The temperatures of the core and the halo have a positive gradient in the center, and reach the maximum of kT ∼ 1.0 keV at r ∼ 7′, indicating that the halo gas is located in a larger scale potential structure than that of the galaxy. The temperatures of the plume and the tail were 0.86 ± 0.01 keV and 1.00 ± 0.01 keV. We succeeded in determining the abundances of α-element separately, for the core, the plume, the tail, and the halo for the first time. -
Downloading Rectification Matrices the first Step Will Be Downloading the Correct Rectification Matrix for Your Data Off of the OSIRIS Website
UNDERGRADUATE HONORS THESIS ADAPTIVE-OPTICS INTEGRAL-FIELD SPECTROSCOPY OF NGC 4388 Defended October 28, 2016 Skylar Shaver Thesis Advisor: Dr. Julie Comerford, Astronomy Honor Council Representative: Dr. Erica Ellingson, Astronomy Committee Members: Dr. Francisco Müller-Sánchez, Astrophysics Petger Schaberg, Writing Abstract Nature’s most powerful objects are well-fed supermassive black holes at the centers of galaxies known as active galactic nuclei (AGN). Weighing up to billions of times the mass of our sun, they are the most luminous sources in the Universe. The discovery of a number of black hole-galaxy relations has shown that the growth of supermassive black holes is closely related to the evolution of galaxies. This evidence has opened a new debate in which the fundamental questions concern the interactions between the central black hole and the interstellar medium within the host galaxy and can be addressed by studying two crucial processes: feeding and feedback. Due to the nature of AGN, high spatial resolution observations are needed to study their properties in detail. We have acquired near infrared Keck/OSIRIS adaptive optics-assisted integral field spectroscopy data on 40 nearby AGN as part of a large program aimed at studying the relevant physical processes associated with AGN phenomenon. This program is called the Keck/OSIRIS nearby AGN survey (KONA). We present here the analysis of the spatial distribution and two-dimensional kinematics of the molecular and ionized gas in NGC 4388. This nearly edge-on galaxy harbors an active nucleus and exhibits signs of the feeding and feedback processes. NGC 4388 is located in the heart of the Virgo cluster and thus is subject to possible interactions with the intra-cluster medium and other galaxies. -
The Herschel⋆ Virgo Cluster Survey
A&A 545, A75 (2012) Astronomy DOI: 10.1051/0004-6361/201219689 & c ESO 2012 ! Astrophysics The Herschel! Virgo Cluster Survey XI. Environmental effects on molecular gas and dust in spiral disks!! C. Pappalardo1,S.Bianchi1,E.Corbelli1,C.Giovanardi1,L.Hunt1,G.J.Bendo6,A.Boselli4,L.Cortese5, L. Magrini1,S.Zibetti1,S.diSeregoAlighieri1,J.Davies2,M.Baes3,L.Ciesla4,M.Clemens7,I.DeLooze3,J.Fritz3, M. Grossi8,M.Pohlen2,M.W.L.Smith2,J.Verstappen3,andC.Vlahakis9 1 Osservatorio Astrofisico di Arcetri – INAF, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: [email protected] 2 Department of Physics and Astronomy, Cardiff University, The Parade, Cardiff,CF243AA,UK 3 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium 4 Laboratoire d’Astrophysique de Marseille – LAM, Université d’Aix-Marseille & CNRS, UMR 7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France 5 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Munchen, Germany 6 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, University of Manchester, Manchester, M13 9PL, UK 7 Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 8 CAAUL, Observatorio Astronomico de Lisboa, Universidade de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal 9 Joint ALMA Office, Alonso de Cordova 3107, Vitacura, Santiago, Chile / European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile Received 25 May 2012 / Accepted 10 July 2012 ABSTRACT Aims. We investigate the dust-to-gas mass ratio and the environmental effects on the various components of the interstellar medium for a spatially resolved sample of Virgo spirals. -
IRAC Near-Infrared Features in the Outer Parts of S4G Galaxies
Mon. Not. R. Astron. Soc. 000, 1{26 (2014) Printed 15 June 2018 (MN LATEX style file v2.2) Spitzer/IRAC Near-Infrared Features in the Outer Parts of S4G Galaxies Seppo Laine,1? Johan H. Knapen,2;3 Juan{Carlos Mu~noz{Mateos,4:5 Taehyun Kim,4;5;6;7 S´ebastienComer´on,8;9 Marie Martig,10 Benne W. Holwerda,11 E. Athanassoula,12 Albert Bosma,12 Peter H. Johansson,13 Santiago Erroz{Ferrer,2;3 Dimitri A. Gadotti,5 Armando Gil de Paz,14 Joannah Hinz,15 Jarkko Laine,8;9 Eija Laurikainen,8;9 Kar´ınMen´endez{Delmestre,16 Trisha Mizusawa,4;17 Michael W. Regan,18 Heikki Salo,8 Kartik Sheth,4;1;19 Mark Seibert,7 Ronald J. Buta,20 Mauricio Cisternas,2;3 Bruce G. Elmegreen,21 Debra M. Elmegreen,22 Luis C. Ho,23;7 Barry F. Madore7 and Dennis Zaritsky24 1Spitzer Science Center - Caltech, MS 314-6, Pasadena, CA 91125, USA 2Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain 3Departamento de Astrof´ısica, Universidad de La Laguna, 38206 La Laguna, Spain 4National Radio Astronomy Observatory/NAASC, Charlottesville, 520 Edgemont Road, VA 22903, USA 5European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 6Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea 7The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA 8Division of Astronomy, Department of Physics, University of Oulu, P.O. Box 3000, 90014 Oulu, Finland 9Finnish Centre of Astronomy with ESO (FINCA), University of Turku, V¨ais¨al¨antie20, FIN-21500 Piikki¨o 10Max-Planck Institut f¨urAstronomie, K¨onigstuhl17 D-69117 Heidelberg, Germany 11Leiden Observatory, Leiden University, P.O. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
May 2013 BRAS Newsletter
www.brastro.org May 2013 What's in this issue: PRESIDENT'S MESSAGE .............................................................................................................................. 2 NOTES FROM THE VICE PRESIDENT ........................................................................................................... 3 MESSAGE FROM THE HRPO ...................................................................................................................... 4 OBSERVING NOTES ..................................................................................................................................... 5 DEEP SKY OBJECTS ................................................................................................................................... 6 MAY ASTRONOMICAL EVENTS .................................................................................................................... 7 TREASURER’S NOTES ................................................................................................................................. 8 PREVIOUS MEETING MINUTES .................................................................................................................... 9 IMPORTANT NOTE: This month's meeting will be held on Saturday, May 18th at LIGO. PRESIDENT'S MESSAGE Hi Everyone, April was quite a busy month and the busiest day was International Astronomy Day. As you may have heard, we had the highest attendance at our Astronomy Day festivities at the HRPO ever. Approximately 770 people attended this year -
Arxiv:Astro-Ph/0305472 V1 23 May 2003
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) An Hα survey aiming at the detection of extraplanar diffuse ionized gas in halos of edge–on spiral galaxies ? II. The Hα survey atlas and catalog J. Rossa ??1,2 and R.–J. Dettmar1 1 Astronomisches Institut, Ruhr–Universit¨at Bochum, D–44780 Bochum, Germany e-mail: [email protected], [email protected] 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. (present address) Received 14 February 2003 / Accepted 6 May 2003 Abstract. In this second paper on the investigation of extraplanar diffuse ionized gas in nearby edge–on spiral galaxies we present the actual results of the individual galaxies of our Hα imaging survey. A grand total of 74 galaxies have been studied, including the 9 galaxies of a recently studied sub–sample (Rossa & Dettmar 2000). 40.5% of all studied galaxies reveal extraplanar diffuse ionized gas, whereas in 59.5% of the survey galaxies no extraplanar diffuse ionized gas could be detected. The average distances of this extended emission above the galactic midplane range from 1–2 kpc, while individual filaments in a few galaxies reach distances of up to |z| ∼ 6 kpc. In several cases a pervasive layer of ionized gas was detected, similar to the Reynolds layer in our Milky Way, while other galaxies reveal only extended emission locally. The morphology of the diffuse ionized gas is discussed for each galaxy and is compared with observations of other important ISM constituents in the context of the disk–halo connection, in those cases where published results were available. -
Overview on Spectral Line Source Finding and Visualisation
CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2012, 29, 359–370 http://dx.doi.org/10.1071/AS12030 Overview on Spectral Line Source Finding and Visualisation B. S. Koribalski CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia Email: [email protected] Abstract: Here I will outline successes and challenges for finding spectral line sources in large data cubes that are dominated by noise. This is a 3D challenge as the sources we wish to catalog are spread over several spatial pixels and spectral channels. While 2D searches can be applied, e.g. channel by channel, optimal searches take into account the 3-dimensional nature of the sources. In this overview I will focus on HI 21-cm spectral line source detection in extragalactic surveys, in particular HIPASS, the HI Parkes All-Sky Survey and WALLABY, the ASKAP HI All-Sky Survey. I use the original HIPASS data to highlight the diversity of spectral signatures of galaxies and gaseous clouds, both in emission and absorption. Among others, I report the À1 discovery of a 680 km s wide HI absorption trough in the megamaser galaxy NGC 5793. Issues such as source confusion and baseline ripples, typically encountered in single-dish HI surveys, are much reduced in interferometric HI surveys. Several large HI emission and absorption surveys are planned for the Australian Square Kilometre Array Pathfinder (ASKAP): here we focus on WALLABY, the 21-cm survey of the sky (d , þ308; z , 0.26) which will take about one year of observing time with ASKAP. -
Expected Intermediate-Mass Black Holes in the Virgo Cluster – II. Late-Type Galaxies
MNRAS 484, 814–831 (2019) doi:10.1093/mnras/sty3068 Advance Access publication 2018 December 21 Expected intermediate-mass black holes in the Virgo cluster – II. Late-type galaxies Alister W. Graham ,1‹ Roberto Soria2,3,4 and Benjamin L. Davis 1 1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2College of Astronomy and Space Sciences, University of the Chinese Academy of Sciences, Beijing 100049, China Downloaded from https://academic.oup.com/mnras/article-abstract/484/1/814/5256645 by Swinburne Library user on 08 April 2019 3International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, WA 6845, Australia 4Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, Sydney, NSW 2006, Australia Accepted 2018 November 2. Received 2018 October 30; in original form 2018 August 10 ABSTRACT The Chandra X-ray Observatory’s Cycle 18 Large Program titled ‘Spiral galaxies of the Virgo Cluster’ will image 52 galaxies with the ACIS-S detector. Combined with archival data for an additional 22 galaxies, this will represent the complete sample of 74 spiral galaxies in the Virgo cluster with star formation rates 0.3 M yr−1. Many of these galaxies are expected to have an active nucleus, signalling the presence of a central black hole. In preparation for this survey, we predict the central black hole masses using the latest black hole scaling relations based on the spiral arm pitch angle φ, velocity dispersion σ , and total stellar mass M∗,galaxy. 2 5 With a focus on intermediate-mass black holes (IMBHs; 10 < Mbh/M < 10 ), we highlight 3 4 NGC 4713 and NGC 4178, both with Mbh ≈ 10 –10 (an estimate that is further supported in NGC 4178 by its nuclear star cluster mass). -
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 Star Formation History of NGC 4388 Combined Spectral and Photometric Analysis
The Star Formation History of NGC 4388 Combined spectral and photometric analysis Ciro Pappalardo (Observatoire de Strasbourg) Ariane Lançon - Bernd Vollmer (Observatoire de Strasbourg) Samuel Boissier (Laboratoire d’Astrophysique de Marseille) Pierre Ocvirk (Astrophysikalisches Institut Potsdam) Virgo distance D ~ 17 Mpc NGC 4388 d ~ 400 kpc Chung et al. 09 NGC 4388 HI emission (WSRT, Oosterloo & van Gorkom 05) H-alpha on optical (SUBARU, Yoshida et al. 02) RAM PRESSURE STRIPPING The galaxy is moving in the hot intracluster medium Roediger QuickTime™ et un décompresseur GIF sont requis pour visionner cette image. Vollmer & Huchtmeier, 03 RAM PRESSURE STRIPPING The galaxy is moving in the hot intracluster medium Vollmer (2009) Stripping age ~ 120 Myr Goal & Outline Gas has left the disk Star Formation STOPS STRIPPING AGE = time elapsed since the halt of star formation 1. Optical spectroscopy and Photom. data of NGC 4388 2. Non parametric inversion tool to reconstruct SFH 3. Parametric method to refine the results DATA Inner = typical star forming disk Outer = post starburst galaxy without emission line NON PARAMETRIC METHOD Inner region SFH = flat MET = Sun Outer region SFH drop ~ 300 Myr Parametric Results Spec Photo Both Source of Errors in parametric method 1. Choice of star formation history model : ~ 5/10 Myr 2. Extinction law : ~ 10 Myr 3. Metallicity value : ~ 10 Myr 4. Monte Carlo simulations : ~ 30 Myr Conclusions 1. For NGC 4388 the non parametric method recover a flat star formation history. 2. The metallicity of NGC 4388 is solar with a small radial gradient. 3. The non parametric method cannot provide precise stripping ages.