Turbulence in Hickson Compact Group NGC 7674
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Arxiv:1904.07129V1 [Astro-Ph.GA] 15 Apr 2019
Draft version April 16, 2019 Preprint typeset using LATEX style emulateapj v. 12/16/11 SPIRE SPECTROSCOPY OF EARLY TYPE GALAXIES Ryen Carl Lapham and Lisa M. Young Physics Department, New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801; [email protected], [email protected] Draft version April 16, 2019 ABSTRACT We present SPIRE spectroscopy for 9 early-type galaxies (ETGs) representing the most CO-rich and far-infrared (FIR) bright galaxies of the volume-limited Atlas3D sample. Our data include detections of mid to high J CO transitions (J=4-3 to J=13-12) and the [C I] (1-0) and (2-1) emission lines. CO spectral line energy distributions (SLEDs) for our ETGs indicate low gas excitation, barring NGC 1266. We use the [C I] emission lines to determine the excitation temperature of the neutral gas, as well as estimate the mass of molecular hydrogen. The masses agree well with masses derived from CO, making this technique very promising for high redshift galaxies. We do not find a trend between the [N II] 205 flux and the infrared luminosity, but we do find that the [N II] 205/CO(6-5) line ratio is correlated with the 60/100 µm Infrared Astronomical Satellite (IRAS) colors. Thus the [N II] 205/CO(6-5) ratio can be used to infer a dust temperature, and hence the intensity of the interstellar radiation field (ISRF). Photodissociation region (PDR) models show that use of [C I] and CO lines in addition to the typical [C II], [O I], and FIR fluxes drive the model solutions to higher densities and lower values of G0. -
1501.01010V1.Pdf
Draft version January 7, 2015 Preprint typeset using LATEX style emulateapj v. 5/2/11 JET-ISM INTERACTION IN THE RADIO GALAXY 3C293: JET-DRIVEN SHOCKS HEAT ISM TO POWER X-RAY AND MOLECULAR H2 EMISSION L. Lanz1, P. M. Ogle1, D. Evans2, P. N. Appleton3, P. Guillard4, B. Emonts5 Draft version January 7, 2015 ABSTRACT We present a 70ks Chandra observation of the radio galaxy 3C 293. This galaxy belongs to the class of molecular hydrogen emission galaxies (MOHEGs) that have very luminous emission from warm molecular hydrogen. In radio galaxies, the molecular gas appears to be heated by jet-driven shocks, but exactly how this mechanism works is still poorly understood. With Chandra, we observe X-ray emission from the jets within the host galaxy and along the 100 kpc radio jets. We model the X-ray spectra of the nucleus, the inner jets, and the X-ray features along the extended radio jets. Both the nucleus and the inner jets show evidence of 107 K shock-heated gas. The kinetic power of the jets is more than sufficient to heat the X-ray emitting gas within the host galaxy. The thermal X-ray and warm H2 luminosities of 3C 293 are similar, indicating similar masses of X-ray hot gas and warm molecular gas. This is consistent with a picture where both derive from a multiphase, shocked interstellar medium (ISM). We find that radio-loud MOHEGs that are not brightest cluster galaxies (BCGs), like 3C 293, typically have LH2 /LX ∼ 1 and MH2 /MX ∼ 1, whereas MOHEGs that are BCGs have LH2 /LX ∼ 0.01 and MH2 /MX ∼ 0.01. -
H {\Alpha} Imaging of Nearby Seyfert Host Galaxies
Draft version November 6, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES Rachel L. Theios1 and Matthew A. Malkan and Nathaniel R. Ross2 Department of Physics and Astronomy, University of California, Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA Draft version November 6, 2018 ABSTRACT We used narrowband (∆λ = 70 Å) interference filters with the CCD imaging camera on the Nickel 1.0 meter telescope at Lick Observatory to observe 31 nearby (z < 0:03) Seyfert galaxies in the 12 µm Active Galaxy Sample (Spinoglio & Malkan 1989). We obtained pure emission line images of each galaxy, which reach down to a flux limit of 7:3 10−15 erg cm−2 s−1 arcsec−2, and corrected these images for [N ii] emission and extinction. We separated× the Hα emission line from the “nucleus” (central 100–1000 pc) from that of the host galaxy. The extended Hα emission is expected to be powered by newly formed hot stars, and indeed correlates well with other indicators of current SFRs in these galaxies: 7.7 µm PAH, far infrared, and radio luminosity. Relative to what is expected from recent star formation, there is a 0.8 dex excess of radio emission in our Seyfert galaxies. The Hα luminosity we measured in the galaxy centers is dominated by the AGN, and is linearly correlated with hard X-ray luminosity. There is, however, an upward offset of 1 dex in this correlation for Seyfert 1s, because their nuclear Hα emission includes a strong additional contribution from the Broad Line Region. -
VLBA Detection of Nuclear Compact Emission in the AGN-Driven Molecular Outflow Candidate NGC 1266
VLBA Detection of Nuclear Compact Emission in the AGN-Driven Molecular Outflow Candidate NGC 1266 Kristina Nyland New Mexico Tech 2012 New Mexico Symposium Outflows in Galaxies • Can help regulate star formation and SMBH growth • May be responsible for various empirical scaling relations in galaxies (e.g., Faber-Jackson relation) • Driving mechanisms: • Stellar feedback • Radiation pressure • Stellar winds (young O stars, AGB stars) • Supernovae • AGNs • Quasar mode (radiative) • Radio mode (mechanical/kinetic) Starburst-Driven Molecular Outflows M82 (Walter+02) Arp 220 (Sakamoto+09) • Prototypical SB galaxy • ULIRG • Interacting with M81 • merger remnant • Molecular gas entrained in • (But AGN may play a starburst wind see role, Rangwala+11) 8 7 • Moutflow = 3 x 10 Msun • Moutflow = 5 x 10 Msun • dM/dt = 30 Msun/year • dM/dt = 100 Msun/year • voutflow = 100 km/s • voutflow = 100 km/s HST HST AGN-Driven Molecular Outflows • Outflows of neutral/ionized gas relatively common in AGNs • Molecular outflows potentially powered by AGNs are rare • Much of the evidence is circumstantial • e.g., SDSS statistical analyses of timing of starbursts and AGN activity • Many candidates for direct evidence are high-redshift quasars • local candidates needed! AGN-Driven Molecular Outflows Mrk 231 (Feruglio+10) • Nearest quasar host • Interacting system 8 • Moutflow = 5.8 x 10 Msun • dM/dt = 100-700 Msun/yr • v = 700 km/s outflow Gemini NGC 1266: Local Candidate AGN- driven Molecular Outflow Host? • Morphology: S0 • Environment: Field – no evidence of recent major merger • Distance: 29.9 Mpc • MK = -22.93 DSS • σ* = 79 km/s 6 • MBH: ~3.2 x 10 Msun IRAM 30m CO Emission Figures from Alatalo et al. -
Hubble Space Telescope Images of Stephan's Quintet
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Hubble Space Telescope Images of Stephan's Quintet: Star Cluster Formation in a Compact Group Environment1;2 Sarah C. Gallagher, Jane C. Charlton3, Sally D. Hunsberger Department of Astronomy and Astrophysics The Pennsylvania State University University Park PA 16802 gallsc, charlton, [email protected] Dennis Zaritsky Steward Observatory University of Arizona Tucson, AZ 85721 [email protected] and Bradley C. Whitmore Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218 [email protected] ABSTRACT Analysis of Hubble Space Telescope/Wide Field Planetary Camera 2 images of Stephan’s Quintet, Hickson Compact Group 92, yielded 115 candidate star clusters (with V I<1:5). Unlike in merger remants, the cluster candidates in Stephan’s Quintet are not clustered in the inner− regions of the galaxies; they are spread over the debris and surrounding area. Specifically, these sources are located in the long sweeping tail and spiral arms of NGC 7319, in the tidal debris of NGC 7318B/A, and in the intragroup starburst region north of these galaxies. Analysis of the colors of the clusters indicate several distinct epochs of star formation that appear to trace the complex history of dynamical interactions in this compact group. Subject headings: galaxies: interactions | galaxies: individual (NGC 7318A, NGC 7318B, NGC 7319) | galaxies: star clusters | intergalactic medium 1. Introduction the central regions of mergers (Holtzman et al. 1992; Whitmore et al. 1993; Schweizer et al. 1996; Miller et al. The interactions of galaxies trigger bursts of star for- 1997; Whitmore et al. -
XXXI. Nuclear Radio Emission in Nearby Early-Type Galaxies
MNRAS 458, 2221–2268 (2016) doi:10.1093/mnras/stw391 Advance Access publication 2016 February 24 The ATLAS3D Project – XXXI. Nuclear radio emission in nearby early-type galaxies Kristina Nyland,1,2‹ Lisa M. Young,3 Joan M. Wrobel,4 Marc Sarzi,5 Raffaella Morganti,2,6 Katherine Alatalo,7,8† Leo Blitz,9 Fred´ eric´ Bournaud,10 Martin Bureau,11 Michele Cappellari,11 Alison F. Crocker,12 Roger L. Davies,11 Timothy A. Davis,13 P. T. de Zeeuw,14,15 Pierre-Alain Duc,10 Eric Emsellem,14,16 Sadegh Khochfar,17 Davor Krajnovic,´ 18 Harald Kuntschner,14 Richard M. McDermid,19,20 Thorsten Naab,21 Tom Oosterloo,2,6 22 23 24 Nicholas Scott, Paolo Serra and Anne-Marie Weijmans Downloaded from Affiliations are listed at the end of the paper Accepted 2016 February 17. Received 2016 February 15; in original form 2015 July 3 http://mnras.oxfordjournals.org/ ABSTRACT We present the results of a high-resolution, 5 GHz, Karl G. Jansky Very Large Array study 3D of the nuclear radio emission in a representative subset of the ATLAS survey of early-type galaxies (ETGs). We find that 51 ± 4 per cent of the ETGs in our sample contain nuclear radio emission with luminosities as low as 1018 WHz−1. Most of the nuclear radio sources have compact (25–110 pc) morphologies, although ∼10 per cent display multicomponent core+jet or extended jet/lobe structures. Based on the radio continuum properties, as well as optical emission line diagnostics and the nuclear X-ray properties, we conclude that the at MPI Study of Societies on June 7, 2016 3D majority of the central 5 GHz sources detected in the ATLAS galaxies are associated with the presence of an active galactic nucleus (AGN). -
The Applicability of Far-Infrared Fine-Structure Lines As Star Formation
A&A 568, A62 (2014) Astronomy DOI: 10.1051/0004-6361/201322489 & c ESO 2014 Astrophysics The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types? Ilse De Looze1, Diane Cormier2, Vianney Lebouteiller3, Suzanne Madden3, Maarten Baes1, George J. Bendo4, Médéric Boquien5, Alessandro Boselli6, David L. Clements7, Luca Cortese8;9, Asantha Cooray10;11, Maud Galametz8, Frédéric Galliano3, Javier Graciá-Carpio12, Kate Isaak13, Oskar Ł. Karczewski14, Tara J. Parkin15, Eric W. Pellegrini16, Aurélie Rémy-Ruyer3, Luigi Spinoglio17, Matthew W. L. Smith18, and Eckhard Sturm12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium e-mail: [email protected] 2 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany 3 Laboratoire AIM, CEA, Université Paris VII, IRFU/Service d0Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France 4 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 5 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 6 Laboratoire d0Astrophysique de Marseille − LAM, Université Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille CEDEX 13, France 7 Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 8 European Southern Observatory, Karl -
The Low-Metallicity Picture A
Linking dust emission to fundamental properties in galaxies: the low-metallicity picture A. Rémy-Ruyer, S. C. Madden, F. Galliano, V. Lebouteiller, M. Baes, G. J. Bendo, A. Boselli, L. Ciesla, D. Cormier, A. Cooray, et al. To cite this version: A. Rémy-Ruyer, S. C. Madden, F. Galliano, V. Lebouteiller, M. Baes, et al.. Linking dust emission to fundamental properties in galaxies: the low-metallicity picture. Astronomy and Astrophysics - A&A, EDP Sciences, 2015, 582, pp.A121. 10.1051/0004-6361/201526067. cea-01383748 HAL Id: cea-01383748 https://hal-cea.archives-ouvertes.fr/cea-01383748 Submitted on 19 Oct 2016 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 582, A121 (2015) Astronomy DOI: 10.1051/0004-6361/201526067 & c ESO 2015 Astrophysics Linking dust emission to fundamental properties in galaxies: the low-metallicity picture? A. Rémy-Ruyer1;2, S. C. Madden2, F. Galliano2, V. Lebouteiller2, M. Baes3, G. J. Bendo4, A. Boselli5, L. Ciesla6, D. Cormier7, A. Cooray8, L. Cortese9, I. De Looze3;10, V. Doublier-Pritchard11, M. Galametz12, A. P. Jones1, O. Ł. Karczewski13, N. Lu14, and L. Spinoglio15 1 Institut d’Astrophysique Spatiale, CNRS, UMR 8617, 91405 Orsay, France e-mail: [email protected]; [email protected] 2 Laboratoire AIM, CEA/IRFU/Service d’Astrophysique, Université Paris Diderot, Bât. -
The Weak Fe Fluorescence Line and Long-Term X-Ray Evolution of The
MNRAS 467, 4606–4621 (2017) doi:10.1093/mnras/stx357 Advance Access publication 2017 February 13 The weak Fe fluorescence line and long-term X-ray evolution of the Compton-thick active galactic nucleus in NGC 7674 P. Gandhi,1,2‹ A. Annuar,2 G. B. Lansbury,2,3 D. Stern,4 D. M. Alexander,2 F. E. Bauer,5,6,7 S. Bianchi,8 S. E. Boggs,9 P. G. Boorman,1 W. N. Brandt,10,11,12 M. Brightman,13 F. E. Christensen,14 A. Comastri,15 W. W. Craig, 14,16 A. Del Moro,17 M. Elvis,18 M. Guainazzi,19,20 C. J. Hailey,21 F. A. Harrison,13 M. Koss,22 I. Lamperti,22 G. Malaguti,23 A. Masini,15,24 G. Matt,8 S. Puccetti,25,26 C. Ricci,5 E. Rivers,13 D. J. Walton3,4,13 and W. W. Zhang27 Affiliations are listed at the end of the paper Accepted 2017 February 8. Received 2017 February 7; in original form 2016 May 24 ABSTRACT We present NuSTAR X-ray observations of the active galactic nucleus (AGN) in NGC 7674. The source shows a flat X-ray spectrum, suggesting that it is obscured by Compton-thick gas columns. Based upon long-term flux dimming, previous work suggested the alternate possibility that the source is a recently switched-off AGN with the observed X-rays being the lagged echo from the torus. Our high-quality data show the source to be reflection-dominated in hard X-rays, but with a relatively weak neutral Fe Kα emission line (equivalent width [EW] of ≈ 0.4 keV) and a strong Fe XXVI ionized line (EW ≈ 0.2 keV). -
IRAM Annual Report 2012
IRAM IRAM Annual Report 2012 Institut de Radioastronomie Millimétrique 30-meter diameter telescope, Pico Veleta 6 x 15-meter interferometer, Plateau de Bure The Institut de Radioastronomie Millimétrique (IRAM) is a multi-national scientific institute covering all aspects of radio astronomy at millimeter wavelengths: the operation of two high-altitude observatories – a 30-meter diameter telescope on Pico Veleta in the Sierra Nevada (southern Spain), and an interferometer of six 15 meter diameter telescopes on the Plateau de Bure in the French Alps – the development of telescopes and instrumentation, radio astronomical observations and their interpretation. IRAM was founded in 1979 by two national research organizations: the CNRS and the Max-Planck-Gesellschaft – the Spanish Instituto Geográfico IRAM Addresses: Nacional, initially an associate member, became a full member in 1990. Institut de Radioastronomie The technical and scientific staff of IRAM develops instrumentation and Millimétrique 300 rue de la piscine, software for the specific needs of millimeter radioastronomy and for the Saint-Martin d’Hères benefit of the astronomical community. IRAM’s laboratories also supply F-38406 France Tel: +33 [0]4 76 82 49 00 devices to several European partners, including for the ALMA project. Fax: +33 [0]4 76 51 59 38 [email protected] www.iram.fr IRAM’s scientists conduct forefront research in several domains of astrophysics, from nearby star-forming regions to objects at cosmological Observatoire du Plateau de Bure distances. Saint-Etienne-en-Dévoluy -
Existence and Importance of Magnetic Fields in Tight Pairs and Groups of Galaxies 15 3 Summary of the Published Articles 17 3.1
EXISTENCEANDIMPORTANCEOFMAGNETICFIELDSIN TIGHTPAIRSANDGROUPSOFGALAXIES błazej˙ nikiel-wroczynski´ A PhD thesis written under the supervision of Professor Marek Urbanik and co-supervision of Doctor Marek Jamrozy Astronomical Observatory Faculty of Physics, Astronomy and Applied Computer Science Jagiellonian University June 2015 Błazej˙ Nikiel-Wroczy´nski: Existence and importance of magnetic fields in tight pairs and groups of galaxies, © June 2015 supervisors: Prof. dr hab. Marek Urbanik Dr Marek Jamrozy alma mater: Jagiellonian University, Faculty of Physics, Astronomy and Applied Computer Science Dedication This work is dedicated to Rugia for being (probably unknowingly) an Earth-based analogue of the MHD dynamo, that amplified my determination to collect all the presented articles into one thesis, transferring the kinetic energy of my turbulent movements into a genuinely regular (not just anisotropic), scientific dissertation. ABSTRACT This dissertation is an attempt to investigate the existence and role of the intergalactic magnetic fields in compact groups and tight pairs of galaxies. Radio emission from several, well known objects of these types is analysed and properties of the discovered intergalactic mag- netised structures are discussed. Together, these results are used to show that wherever found, intergalactic magnetic fields play impor- tant role in the galactic dynamics and evolution. Non-thermal, in- tergalactic radio emission, which signifies existence of the magnetic fields, can be used as a very sensitive tracer of interactions and gas flows. Unusual magnetised objects and structures can be found in the intergalactic space, and their studies open a possibility to discover more about the cosmic magnetism itself. v PUBLICATIONS This dissertation has been written as a summary of the scientific ac- tivities previously reported in these articles: • Nikiel-Wroczy ´nski,B., Jamrozy, M., Soida, M., Urbanik, M., Multiwavelength study of the radio emission from a tight galaxy pair Arp 143, 2014, MNRAS, 444, 1729 • Nikiel-Wroczy ´nski,B., Soida, M., Bomans, D. -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea