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Linking Dust Emission to Fundamental Properties in Galaxies: the Low-Metallicity Picture?
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. 709, 91191 Gif-sur-Yvette, France 3 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium 4 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics & Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 5 Laboratoire d’Astrophysique de Marseille – LAM, Université d’Aix-Marseille & CNRS, UMR 7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France 6 Department of Physics, University of Crete, 71003 Heraklion, Greece 7 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany 8 Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA 9 Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Mail H30, PO Box 218, Hawthorn VIC 3122, Australia 10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 11 Max-Planck für Extraterrestrische Physik, Giessenbachstr. 1, 85748 Garching-bei-München, Germany 12 European Southern Observatory, Karl-Schwarzschild-Str. -
Appendix A: the HRS+ Members
Appendix A: The HRS+ Members 207 Table A.1: The general properties of galaxies comprising the HRS+ sample. Each column contains: (1) the HRS+ identification 208 number; (2) an alternative name taken from either the New General Catalogue (NGC; Dreyer, 1888), the Catalogue of Galaxies and Clusters of Galaxies (CGCG; Zwicky et al., 1961), Uppsala General Catalogue (UGC; Nilson, 1973), the Virgo Cluster Catalogue (VCC; Binggeli et al., 1985), and the Index Catalogue (IC; Dreyer, 1908); (3) J2000 right ascension, from NED; (4) J2000 declination, from NED; (5) distance; (6) the morphological classification from NED; (7) total 2MASS K band magnitude −2 (Skrutskie et al., 2006); (8) the optical isophotal distance D25 (25 mag arcsec ); (9) the heliocentric radial velocity from NED; (10) the cluster or cloud membership; and (11) the galactic extinction Schlegel et al., 1998. ◦ ′ ′′ −1 HRS+ Alt.Name R.A.(hms) Dec.( ) D (Mpc) Type KStot D25 (′) V (km s ) Member AB (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) 1 CGCG 123-035 10 17 39.66 +22 48 35.9 15.7 Pec 11.59 1.00 1175 Leo Cl. 0.13 2 UGC 5588 10 20 57.13 +25 21 53.4 17.2 S? 11.03 0.52 1291 Leo Cl. 0.10 3 NGC 3226 10 23 27.01 +19 53 54.7 15.3 E2:pec;LINER;Sy3 8.57 3.16 1169 Leo Cl. 0.10 4 NGC 3227 10 23 30.58 +19 51 54.2 15.4 SAB(s)pec;Sy1.5 7.64 5.37 1148 Leo Cl. -
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. -
Arxiv:0907.4718V1 [Astro-Ph.GA] 27 Jul 2009 Nnab Aais Hi Ihlmnste ( Luminosities High Their Objects Point-Like Galaxies
Submitted to Astrophysical Journal A Preprint typeset using L TEX style emulateapj v. 04/03/99 ULTRALUMINOUS X-RAY SOURCE CORRELATIONS WITH STAR-FORMING REGIONS Douglas A. Swartz1 Allyn F. Tennant2, and Roberto Soria3 Submitted to Astrophysical Journal ABSTRACT Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u − g, g − r and r − i colors are used to determine whether Ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of H ii regions in M 81 and M 101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher’s linear discriminant analysis. It is found that 60% (49%) of ULXs in optically-bright environments are within regions blueward of their host galaxy’s H ii regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3σ above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, ∼<10 Myr, OB associations. However, none of the ULX environments have the morphology and optical brightness suggestive of a massive young super star cluster though several are in extended or crowded star-forming (blue) environments that may contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with estimated X-ray luminosities in excess of 3×1039 ergs s−1 are equally divided among the group of ULX environments redward of H ii regions and the group of optically faint regions. -
Physical Conditions of the Molecular Gas in Metal-Poor Galaxies? L
A&A 606, A99 (2017) Astronomy DOI: 10.1051/0004-6361/201731000 & c ESO 2017 Astrophysics Physical conditions of the molecular gas in metal-poor galaxies? L. K. Hunt1, A. Weiß2, C. Henkel2; 3, F. Combes4, S. García-Burillo5, V. Casasola1, P. Caselli6, A. Lundgren9, R. Maiolino7, K. M. Menten2, and L. Testi1; 8 1 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy e-mail: [email protected] 2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 3 Astronomy Department, King Abdulaziz University, PO Box 80203, Jeddah, Saudia Arabia 4 Observatoire de Paris, LERMA, Collège de France, CNRS, PSL, Sorbonne University UPMC, 75014 Paris, France 5 Observatorio Astronómico Nacional (OAN)-Observatorio de Madrid, Alfonso XII, 3, 28014 Madrid, Spain 6 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany 7 Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK 8 ESO, Karl Schwarzschild str. 2, 85748 Garching bei München, Germany 9 Vittja 64, 74793 Alunda, Sweden Received 18 April 2017 / Accepted 8 August 2017 ABSTRACT Studying the molecular component of the interstellar medium (ISM) in metal-poor galaxies has been challenging because of the faint- ness of carbon monoxide emission, the most common proxy of H2. Here we present new detections of molecular gas at low metal- licities, and assess the physical conditions in the gas through various CO transitions for 8 galaxies. For one, NGC 1140 (Z=Z ∼ 0.3), two detections of 13CO isotopologues and atomic carbon, [Ci](1–0) and an upper limit for HCN(1–0) are also reported. -
An Atlas of Calcium Triplet Spectra of Active Galaxies 3
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 December 2018 (MN LATEX style file v2.2) An atlas of Calcium triplet spectra of active galaxies A. Garcia-Rissmann1⋆, L. R. Vega1,2†, N. V. Asari1‡, R. Cid Fernandes1§, H. Schmitt3,4¶, R. M. Gonz´alez Delgado5k, T. Storchi-Bergmann6⋆⋆ 1 Depto. de F´ısica - CFM - Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil 2 Observatorio Astron´omico de C´ordoba, Laprida 854, 5000, C´ordoba, Argentina 3 Remote Sensing Division, Code 7210, Naval Research Laboratory, 4555 Overlook Avenue, SW, Washington, DC 20375 4 Interferometric Inc., 14120 Parke Long Court, 103, Chantilly, VA20151 5 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), P.O. Box 3004, 18080 Granada, Spain 6 Instituto de F´ısica, Universidade Federal do Rio Grande do Sul, C.P. 15001, 91501-970, Porto Alegre, RS, Brazil 1 December 2018 ABSTRACT We present a spectroscopic atlas of active galactic nuclei covering the region around the λλ8498, 8542, 8662 Calcium triplet (CaT). The sample comprises 78 ob- jects, divided into 43 Seyfert 2s, 26 Seyfert 1s, 3 Starburst and 6 normal galaxies. The spectra pertain to the inner ∼ 300 pc in radius, and thus sample the central kine- matics and stellar populations of active galaxies. The data are used to measure stellar velocity dispersions (σ⋆) both with cross-correlation and direct fitting methods. These measurements are found to be in good agreement with each-other and with those in previous studies for objects in common. The CaT equivalent width is also measured. -
Molecules As Tracers of Galaxy Evolution: an EMIR Survey
Astronomy & Astrophysics manuscript no. costagliola˙evol c ESO 2018 February 8, 2018 Molecules as tracers of galaxy evolution: an EMIR survey I. Presentation of the data and first results F. Costagliola1,⋆, S. Aalto1,⋆⋆, M. I. Rodriguez2, S. Muller1, H. W. W. Spoon3, S. Mart´ın4, M. A. Per´ez-Torres2, A. Alberdi2, J. E. Lindberg1,5, F. Batejat1, E. J¨utte6, P. van der Werf7,8, and F. Lahuis7,9 1 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, SE-439 92 Onsala, Sweden, e-mail: [email protected] 2 Instituto de Astrof´ısica de Andaluc´ıa (IAA-CSIC), PO Box 3004, E-18080 Granada, Spain 3 Cornell University, Astronomy Department, Ithaca, NY 14853, USA 4 European Southern Observarory, Alonso de C´ordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile 5 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 København K, Denmark 6 Astronomisches Institut Ruhr-Universitaet Bochum, Universitaetsstr. 150, 44780 Bochum, Germany 7 Leiden Observatory, Leiden University, NL-2300 RA, Leiden, The Netherlands 8 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, United Kingdom 9 SRON Netherlands Institute for Space Research, P.O. Box 800, NL-9700 AV, Groningen, The Netherlands ABSTRACT Aims. We investigate the molecular gas properties of a sample of 23 galaxies in order to find and test chemical signatures of galaxy evolution and to compare them to IR evolutionary tracers. Methods. Observation at 3 mm wavelengths were obtained with the EMIR broadband receiver, mounted on the IRAM 30 m telescope on Pico Veleta, Spain. -
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 -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
The JCMT Nearby Galaxies Legacy Survey VIII. CO Data and the LCO(3
The LCO(3−2)–LF IR correlation in the SINGS sample 1 The JCMT Nearby Galaxies Legacy Survey VIII. CO data and the LCO(3−2)–LF IR correlation in the SINGS sample C. D. Wilson1, B. E. Warren1,2, F. P. Israel3, S. Serjeant4, D. Attewell1, G. J. Bendo5, H. M. Butner6, P. Chanial7, D. L. Clements8, J. Golding1, V. Heesen9 J. Irwin10, J. Leech11, H. E. Matthews12, S. M¨uhle13, A. M. J. Mortier14, G. Petitpas15, J. R. S´anchez-Gallego16,17, E. Sinukoff1, K. Shorten1, B. K. Tan11, R. P. J. Tilanus18,19, A. Usero20, M. Vaccari21,43, T. Wiegert22, M. Zhu23, D. M. Alexander24, P. Alexander25,26, M. Azimlu27,15, P. Barmby27, C. Borys28, R. Brar10, C. Bridge28, E. Brinks9, S. Brooks1, K. Coppin29, S. Cˆot´e30, P. Cˆot´e30, S. Courteau10, J. Davies31, S. Eales31, M. Fich32, M. Hudson32, D. H. Hughes33, R. J. Ivison34,35, J. H. Knapen16,17, M. Page8, T. J. Parkin1, A. Pope36, D. Rigopoulou11,37, E. Rosolowsky38, E. R. Seaquist39, K. Spekkens40, N. Tanvir9, J. M. van der Hulst41, P. van der Werf3, C. Vlahakis42, T. M. Webb29, B. Weferling18, G. J. White4,37 1Department of Physics & Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada 2 International Centre for Radio Astronomy Research, M468, University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia 3Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 4Department of Physics & Astronomy, The Open University, Milton Keynes MK7 6AA, United Kingdom 5 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom 6Department of Physics and Astronomy, James Madison University, MSC 4502 - 901 Carrier Drive, Harrisonburg, VA 22807, U.S.A. -
CIRPASS Near-Infrared Integral-Field Spectroscopy of Massive Star Clusters in the Starburst Galaxy NGC 1140
This is a repository copy of CIRPASS near-infrared integral-field spectroscopy of massive star clusters in the starburst galaxy NGC 1140. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/144873/ Version: Published Version Article: de Grijs, R., Smith, L.J., Bunker, A. et al. (6 more authors) (2004) CIRPASS near-infrared integral-field spectroscopy of massive star clusters in the starburst galaxy NGC 1140. Monthly Notices of the Royal Astronomical Society, 352 (1). pp. 263-276. ISSN 0035-8711 https://doi.org/10.1111/j.1365-2966.2004.07932.x This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2004 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version. This is indicated by the licence information on the White Rose Research Online record for the item. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ Mon. Not. R. Astron. Soc. 352, 263–276 (2004) doi:10.1111/j.1365-2966.2004.07932.x CIRPASS near-infrared integral-field spectroscopy of massive star clusters in the starburst galaxy NGC 1140 R.