Evolution of Galaxies E
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1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
The Molecular Gas Reservoir of 6 Low-Metallicity Galaxies from the Herschel Dwarf Galaxy Survey a Ground-Based Follow-Up Survey of CO(1–0), CO(2–1), and CO(3–2)
A&A 564, A121 (2014) Astronomy DOI: 10.1051/0004-6361/201322096 & c ESO 2014 Astrophysics The molecular gas reservoir of 6 low-metallicity galaxies from the Herschel Dwarf Galaxy Survey A ground-based follow-up survey of CO(1–0), CO(2–1), and CO(3–2) D. Cormier1,S.C.Madden2, V. Lebouteiller2,S.Hony3, S. Aalto4, F. Costagliola4,5, A. Hughes3, A. Rémy-Ruyer2, N. Abel6, E. Bayet7, F. Bigiel1, J. M. Cannon8,R.J.Cumming9, M. Galametz10, F. Galliano2, S. Viti11,andR.Wu2 1 Institut für theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany e-mail: [email protected] 2 Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, Irfu/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France 3 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 4 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 5 Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008 Granada, Spain 6 University of Cincinnati, Clermont College, Batavia OH 45103, USA 7 Sub-Dept. of Astrophysics, Dept. of Physics at University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 8 Department of Physics & Astronomy, Macalester College, 1600 Grand Avenue, Saint Paul MN 55105, USA 9 Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden 10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 11 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK Received 17 June 2013 / Accepted 17 November 2013 ABSTRACT Context. -
Photometric and Spectroscopic Studies of Star-Forming Regions Within Wolf
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 2 October 2018 (MN LATEX style file v2.2) Photometric and spectroscopic studies of star-forming regions within Wolf-Rayet galaxies Chrisphin Karthick, M,1,2⋆ Angel´ R. L´opez-S´anchez,3,4 D. K. Sahu,5 B. B. Sanwal,1 Shuchi Bisht,6 1Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital-263 002, India 2Department of Astrophysics, Pondicherry University, Puducherry - 605 014, India 3Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 4Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia 5Indian Institute of Astrophysics(IIA), Bangalore-560 034, India 6Kumaun University, Nainital-263 001, India Received date: 20 Mar 2012; Accepted date: 28 Nov 2013 ABSTRACT We present a study of the properties of star-forming regions within a sample of 7 Wolf-Rayet (WR) galaxies. We analyze their morphologies, colours, star-formation rate (SFR), metallicities, and stellar populations combining broad-band and narrow- band photometry with low-resolution optical spectroscopy. The UBV RI observations were made through the 2m HCT (Himalayan Chandra Telescope) and 1m ARIES tele- scope. The spectroscopic data were obtained using the Hanle Faint Object Spectrograph Camera (HFOSC) mounted on the 2m HCT. The observed galaxies are NGC 1140, IRAS 07164+5301, NGC 3738, UM 311, NGC 6764, NGC 4861 and NGC 3003. The optical spectra have been used to search for the faint WR features, to confirm that the ionization of the gas is consequence of the massive stars, and to quantify the oxygen abundance of each galaxy using several and independent empirical calibrations. -
Classification of Galaxies Using Fractal Dimensions
UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. -
New Methods for Identifying Lyman Continuum Leakers and Reionization-Epoch Analogues
MNRAS 498, 164–180 (2020) doi:10.1093/mnras/staa2355 Advance Access publication 2020 August 14 New methods for identifying Lyman continuum leakers and reionization-epoch analogues Harley Katz,1‹ Dominika Durovˇ cˇ´ıkova´ ,2 Taysun Kimm ,3 Joki Rosdahl ,4 Jeremy Blaizot,4 Martin G. Haehnelt,5 Julien Devriendt,1 Adrianne Slyz,1 Richard Ellis6 and Nicolas Laporte 5,7 1Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK Downloaded from https://academic.oup.com/mnras/article/498/1/164/5892572 by University College London user on 19 January 2021 2New College, University of Oxford, Holywell Street, Oxford OX1 3BN, UK 3Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea 4Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France 5Kavli Institute for Cosmology and Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK 6Department of Physics and Astronomy, University College London, London WC1E 6BT, UK 7Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UK Accepted 2020 August 3. Received 2020 August 3; in original form 2020 May 3 ABSTRACT Identifying low-redshift galaxies that emit Lyman continuum radiation (LyC leakers) is one of the primary, indirect methods of studying galaxy formation in the epoch of reionization. However, not only has it proved challenging to identify such systems, it also remains uncertain whether the low-redshift LyC leakers are truly ‘analogues’ of the sources that reionized the Universe. Here, we use high-resolution cosmological radiation hydrodynamics simulations to examine whether simulated galaxies in the epoch of reionization share similar emission line properties to observed LyC leakers at z ∼ 3 and z ∼ 0. -
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. -
Core-Collapse Supernova Subtypes in Luminous Infrared Galaxies
Astronomy & Astrophysics manuscript no. aa ©ESO 2021 March 1, 2021 Core-collapse supernova subtypes in luminous infrared galaxies E. Kankare1, A. Efstathiou2, R. Kotak1, E. C. Kool3, T. Kangas4, D. O’Neill5, S. Mattila1, P. Väisänen6, 7, R. Ramphul6, 8, M. Mogotsi6, S. D. Ryder9, 10, S. Parker11, 12, T. Reynolds1, M. Fraser13, A. Pastorello14, E. Cappellaro14, P. A. Mazzali15, 16, P. Ochner17, 14, L. Tomasella14, M. Turatto14, J. Kotilainen18, 1, H. Kuncarayakti1, 18, M. A. Pérez-Torres19, 20, Z. Randriamanakoto6 , C. Romero-Cañizales21, M. Berton18, 22, R. Cartier23, T.-W. Chen3, L. Galbany24, M. Gromadzki25, C. Inserra26, K. Maguire27, S. Moran1, T. E. Müller-Bravo28, M. Nicholl29, 30, A. Reguitti13, 31, 32, and D. R. Young5 (Affiliations can be found after the references) March 1, 2021 ABSTRACT The fraction of core-collapse supernovae (CCSNe) occurring in the central regions of galaxies is not well-constrained at present. This is partly because large-scale transient surveys operate at optical wavelengths, making it challenging to detect transient sources that occur in regions suscep- tible to high extinction factors. Here we present the discovery and follow-up observations of two CCSNe that occurred in the luminous infrared galaxy (LIRG), NGC 3256. The first, SN 2018ec, was discovered using the ESO HAWK-I/GRAAL adaptive optics seeing enhancer, and was +0.3 classified as a Type Ic with a host galaxy extinction of AV = 2.1−0.1 mag. The second, AT 2018cux, was discovered during the course of follow-up observations of SN 2018ec, and is consistent with a sub-luminous Type IIP classification with an AV = 2.1 ± 0.4 mag of host extinction. -
Multi-Wavelength GOALS Observations of Star Formation and Active Galactic Nucleus Activity in the Luminous Infrared Galaxy IC
Draft version September 28, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 MULTI-WAVELENGTH GOALS OBSERVATIONS OF STAR FORMATION AND AGN ACTIVITY IN THE LUMINOUS INFRARED GALAXY IC 883 F. Modica1, T. Vavilkin1,2, A. S. Evans1,2,3,4,5, D.-C. Kim2,3, J. M. Mazzarella6, K. Iwasawa7, A. Petric8, J. H. Howell8, J. A. Surace8, L. Armus8, H. W. W. Spoon9, D. B. Sanders10, A. Wong3, & J. E. Barnes10 Draft version September 28, 2018 ABSTRACT New optical Hubble Space Telescope (HST), Spitzer Space Telescope, GALEX, and Chandra observa- tions of the single-nucleus, luminous infrared galaxy (LIRG) merger IC 883 are presented. The galaxy is a member of the Great Observatories All-sky LIRG Survey (GOALS), and is of particular interest for a detailed examination of a luminous late-stage merger due to the richness of the optically-visible star clusters and the extended nature of the nuclear X-ray, mid-IR, CO and radio emission. In the HST ACS images, the galaxy is shown to contain 156 optically visible star clusters distributed throughout the nuclear regions and tidal tails of the merger, with a majority of visible clusters residing in an arc ∼ 3{7 kpc from the position of the mid-infrared core of the galaxy. The luminosity functions of the clusters have an αF435W ∼ −2:17 ± 0:22 and αF814W ∼ −2:01 ± 0:21, compared with V-band derived values measured for the well-studied LIRG NGC 34 and the Antennae Galaxy of α ∼ −1:7 ± 0:1 and −2:13 ± 0:07, respectively. -
A Kinematic Study of the Irregular Dwarf Galaxy NGC 4861 Using HI
Astronomy & Astrophysics manuscript no. 11766.bw c ESO 2021 September 10, 2021 A kinematic study of the irregular dwarf galaxy NGC 4861 using H i and Hα observations J. van Eymeren1;2;3, M. Marcelin4, B. S. Koribalski3, R.-J. Dettmar2, D. J. Bomans2, J.-L. Gach4, and P. Balard4 1 Jodrell Bank Centre for Astrophysics, School of Physics & Astronomy, The University of Manchester, Alan Turing Building, Oxford Road, Manchester, M13 9PL, UK e-mail: [email protected] 2 Astronomisches Institut der Ruhr-Universitat¨ Bochum, Universitatsstraße¨ 150, 44780 Bochum, Germany 3 Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 1710, Australia 4 Laboratoire d’Astrophysique de Marseille, OAMP, Universite´ Aix-Marseille & CNRS, 38 rue Fred´ eric´ Joliot-Curie, 13013 Marseille, France Accepted 20 July 2009 ABSTRACT Context. Outflows powered by the injection of kinetic energy from massive stars can strongly affect the chemical evolution of galaxies, in particular of dwarf galaxies, as their lower gravitational potentials enhance the chance of a galactic wind. Aims. We therefore performed a detailed kinematic analysis of the neutral and ionised gas components in the nearby star-forming irregular dwarf galaxy NGC 4861. Similar to a recently published study of NGC 2366, we want to make predictions about the fate of the gas and to discuss some general issues about this galaxy. Methods. Fabry-Perot interferometric data centred on the Hα line were obtained with the 1.93m telescope at the Observatoire de Haute-Provence. They were complemented by H i synthesis data from the VLA. We performed a Gaussian decomposition of both the Hα and the H i emission lines in order to search for multiple components indicating outflowing gas. -
Arxiv:Astro-Ph/0401239V1 13 Jan 2004
Paper status: Accepted to the ApJ Missing Massive Stars in Starbursts: Stellar Temperature Diagnostics and the IMF J. R. Rigby and G. H. Rieke Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721 [email protected], [email protected] ABSTRACT Determining the properties of starbursts requires spectral diagnostics of their ultraviolet ra- diation fields, to test whether very massive stars are present. We test several such diagnostics, using new models of line ratio behavior combining Cloudy, Starburst99 and up-to-date spectral atlases (Pauldrach et al. 2001; Hillier & Miller 1998). For six galaxies we obtain new measure- ments of Hei 1.7 µm/Br10, a difficult to measure but physically simple (and therefore reliable) diagnostic. We obtain new measurements of Hei 2.06 µm/Brγ in five galaxies. We find that Hei 2.06 µm/Brγ and [Oiii]/Hβ are generally unreliable diagnostics in starbursts. The het- eronuclear and homonuclear mid–infrared line ratios (notably [Neiii] 15.6 µm / [Neii] 12.8 µm) consistently agree with each other and with Hei 1.7 µm/Br10; this argues that the mid–infrared line ratios are reliable diagnostics of spectral hardness. In a sample of 27 starbursts, [Neiii]/[Neii] is significantly lower than model predictions for a Salpeter IMF extending to 100 M⊙. Plausi- ble model alterations strengthen this conclusion. By contrast, the low–mass and low–metallicity galaxies II Zw 40 and NGC 5253 show relatively high neon line ratios, compatible with a Salpeter slope extending to at least ∼ 40–60 M⊙. One solution for the low neon line ratios in the high– metallicity starbursts would be that they are deficient in & 40 M⊙ stars compared to a Salpeter IMF. -
Annual Report Astronomy Australia Limited
2011 / 12 Annual Report Astronomy Australia Limited Vision Astronomers in Australia will have access to the best astronomical research infrastructure. Mission AAL will achieve its vision by: 1. Engaging with Australian astronomers to advance the national research infrastructure priorities of the Australian astronomy decadal plan. 2. Advising the Australian Government on future investments in national astronomical research infrastructure. 3. Managing investments in national astronomical research infrastructure as required. Principles 1. Access to major astronomical research infrastructure should be available to any Australian-based astronomer purely on scientific merit. 2. The concept of national astronomical research infrastructure includes Australian participation in international facilities. 3. The AAO and CSIRO are empowered by the Australian Government to provide a component of the national astronomical research infrastructure and there is no need for AAL to directly manage investments to upgrade or operate the AAT and ATNF. Front cover image Gemini Legacy image of the complex planetary nebula Sh2-71 as imaged by the Gemini Multi-Object Spectrograph on Gemini North on Mauna Kea in Hawai‘i. A research team, led by Australian astronomers David Frew and Quentin Parker (Macquarie University, Sydney) are studying the dimmer, bluer star to understand its nature. The long-assumed central star is the brightest star near the centre, but the much dimmer and bluer star (just to the right and down a little) might be the parent of this beautiful object. The image is composed of three narrow- band images, and each is assigned a colour as follows: H-alpha (orange), HeII (blue) and [OIII] (cyan). Image credit: Gemini Observatory/AURA Background image Dipoles on one “tile” of the Murchison Widefield Array; one of the first telescopes with no moving parts. -
The HI Chronicles of LITTLE THINGS BCDS III: Gas Clouds in and Around
November 12, 2018 Preprint typeset using LATEX style AASTeX6 v. 1.0 THE H I CHRONICLES OF LITTLE THINGS BCDS III: GAS CLOUDS IN AND AROUND MRK 178, VII ZW 403, AND NGC 3738 Trisha Ashley1 Department of Physics, Florida International University 11200 SW 8th Street, CP 204, Miami, FL 33199 Caroline E. Simpson Department of Physics, Florida International University 11200 SW 8th Street, CP 204, Miami, FL 33199 Bruce G. Elmegreen IBM T. J. Watson Research Center, 1101 Kitchawan Road, Yorktown Heights, New York 10598 Megan Johnson CSIRO Astronomy & Space Science P.O. Box 76, Epping, NSW 1710 Australia Nau Raj Pokhrel Department of Physics, Florida International University 11200 SW 8th Street, CP 204, Miami, FL 33199 1Current Address: NASA Ames Research Center, Moffett Field, CA, 94035 ABSTRACT In most blue compact dwarf (BCD) galaxies, it remains unclear what triggers their bursts of star formation. We study the H I of three relatively isolated BCDs, Mrk 178, VII Zw 403, and NGC 3738, in detail to look for signatures of star formation triggers, such as gas cloud consumption, dwarf-dwarf mergers, and interactions with companions. High angular and velocity resolution atomic hydrogen (H I) data from the Very Large Array (VLA) dwarf galaxy H I survey, Local Irregulars That Trace Luminosity Extremes, The H I Nearby Galaxy Survey (LITTLE THINGS), allows us to study the detailed kinematics and morphologies of the BCDs in H I. We also present high sensitivity H I maps from the NRAO Green Bank Telescope (GBT) of each BCD to search their surrounding regions for extended tenuous emission or companions.