Revisiting the Low-Luminosity Galaxy Population of the NGC 5846 Group with SDSS
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Lawrence Berkeley National Laboratory Recent Work
Lawrence Berkeley National Laboratory Recent Work Title PTF12os and iPTF13bvn: Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 Permalink https://escholarship.org/uc/item/4535j05z Authors Fremling, C Sollerman, J Taddia, F et al. Publication Date 2016-09-01 DOI 10.1051/0004-6361/201628275 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Astronomy & Astrophysics manuscript no. ngc5806˙13bvn12os˙accepted c ESO 2016 June 10, 2016 PTF12os and iPTF13bvn: Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 C. Fremling1, J. Sollerman1, F. Taddia1, M. Ergon1, M. Fraser2, E. Karamehmetoglu1, S. Valenti3, A. Jerkstrand4, I. Arcavi3;5, F. Bufano6, N. Elias Rosa7, A. V. Filippenko8, D. Fox9, A. Gal-Yam5, D. A. Howell3;10, R. Kotak4, P. Mazzali11;12, D. Milisavljevic13, P. E. Nugent8;14, A. Nyholm1, E. Pian15;16, and S. Smartt4 1 Department of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, 10691 Stockholm, Sweden 2 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 3 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA 4 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK 5 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 6 INAF-Osservatorio Astrofisico di Catania, Via Santa Sofia, 78, 95123, Catania, Italy 7 INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 8 Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 9 Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA 10 Department of Physics, Broida Hall, University of California, Santa Barbara, CA 93106-9530, USA 11 Astrophysics Research Institute, Liverpool John Moores University, Liverpool L3 5RF, UK 12 Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. -
Stellar Tidal Streams As Cosmological Diagnostics: Comparing Data and Simulations at Low Galactic Scales
RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Author: Referees: Gustavo MORALES Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL Astronomisches Rechen-Institut Heidelberg Graduate School of Fundamental Physics Department of Physics and Astronomy 14th May, 2018 ii DISSERTATION submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of DOCTOR OF NATURAL SCIENCES Put forward by GUSTAVO MORALES born in Copiapo ORAL EXAMINATION ON JULY 26, 2018 iii Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Referees: Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL iv NOTE: Some parts of the written contents of this thesis have been adapted from a paper submitted as a co-authored scientific publication to the Astronomy & Astrophysics Journal: Morales et al. (2018). v NOTE: Some parts of this thesis have been adapted from a paper accepted for publi- cation in the Astronomy & Astrophysics Journal: Morales, G. et al. (2018). “Systematic search for tidal features around nearby galaxies: I. Enhanced SDSS imaging of the Local Volume". arXiv:1804.03330. DOI: 10.1051/0004-6361/201732271 vii Abstract In hierarchical models of galaxy formation, stellar tidal streams are expected around most galaxies. Although these features may provide useful diagnostics of the LCDM model, their observational properties remain poorly constrained. Statistical analysis of the counts and properties of such features is of interest for a direct comparison against results from numeri- cal simulations. In this work, we aim to study systematically the frequency of occurrence and other observational properties of tidal features around nearby galaxies. -
Lopsided Spiral Galaxies: Evidence for Gas Accretion
A&A 438, 507–520 (2005) Astronomy DOI: 10.1051/0004-6361:20052631 & c ESO 2005 Astrophysics Lopsided spiral galaxies: evidence for gas accretion F. Bournaud1, F. Combes1,C.J.Jog2, and I. Puerari3 1 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France e-mail: [email protected] 2 Department of Physics, Indian Institute of Science, Bangalore 560012, India 3 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, Mexico Received 3 January 2005 / Accepted 15 March 2005 Abstract. We quantify the degree of lopsidedness for a sample of 149 galaxies observed in the near-infrared from the OSUBGS sample, and try to explain the physical origin of the observed disk lopsidedness. We confirm previous studies, but for a larger sample, that a large fraction of galaxies have significant lopsidedness in their stellar disks, measured as the Fourier amplitude of the m = 1 component normalised to the average or m = 0 component in the surface density. Late-type galaxies are found to be more lopsided, while the presence of m = 2 spiral arms and bars is correlated with disk lopsidedness. We also show that the m = 1 amplitude is uncorrelated with the presence of companions. Numerical simulations were carried out to study the generation of m = 1viadifferent processes: galaxy tidal encounters, galaxy mergers, and external gas accretion with subsequent star formation. These simulations show that galaxy interactions and mergers can trigger strong lopsidedness, but do not explain several independent statistical properties of observed galaxies. To explain all the observational results, it is required that a large fraction of lopsidedness results from cosmological accretion of gas on galactic disks, which can create strongly lopsided disks when this accretion is asymmetrical enough. -
Studying Late-Type Spiral Galaxies Using SDSS Pohlen, M.; Trujillo, I
University of Groningen The structure of galactic disks - Studying late-type spiral galaxies using SDSS Pohlen, M.; Trujillo, I. Published in: Astronomy & astrophysics DOI: 10.1051/0004-6361:20064883 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Final author's version (accepted by publisher, after peer review) Publication date: 2006 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Pohlen, M., & Trujillo, I. (2006). The structure of galactic disks - Studying late-type spiral galaxies using SDSS. Astronomy & astrophysics, 454(3), 759-U66. https://doi.org/10.1051/0004-6361:20064883 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 27-09-2021 Astronomy & Astrophysics manuscript no. SDSS May 5, 2006 (DOI: will be inserted by hand later) The structure of galactic disks Studying late-type spiral galaxies using SDSS M. Pohlen1,2 and I. -
1985Apjs ... 59 ...IW the Astrophysical Journal Supplement Series, 59:1-21,1985 September © 1985. the American Astronomical S
IW The Astrophysical Journal Supplement Series, 59:1-21,1985 September .... © 1985. The American Astronomical Society. All rights reserved. Printed in U.S.A. 59 ... A CATALOG OF STELLAR VELOCITY DISPERSIONS. I. 1985ApJS COMPILATION AND STANDARD GALAXIES Bradley C. Whitmore Space Telescope Science Institute Douglas B. McElroy Computer Sciences Corporation1 AND John L. Tonry California Institute of Technology Received 1984 October 23; accepted 1985 February 19 ABSTRACT A catalog of central stellar velocity dispersion measurements is presented, current through 1984 June. The catalog includes 1096 measurements of 725 galaxies. A set of 51 standard galaxies is defined which consists of galaxies with at least three reliable, concordant measurements. We suggest that future studies observe some of these standard galaxies in the course of their observations so that different studies can be normalized to the same system. We compare previous studies with the derived standards to determine relative accuracies and to compute scale factors where necessary. Subject headings: galaxies: internal motions I. INTRODUCTION be flattened by rotation. Results from Whitmore, Rubin, and The ability to make accurate measurements of stellar veloc- Ford (1984) conflict with the Kormendy and Illingworth con- ity dispersions has provided a major catalyst for the study of clusion. galactic structure and dynamics. Several important discoveries While most dispersion profiles are either flat or falling, have resulted from the use of this new tool. For example, a studies of cD galaxies at the center of rich clusters of galaxies correlation between the luminosity of an elliptical galaxy and have shown rising dispersion profiles (Dressier 1979; Carter the central stellar velocity dispersion was discovered by Faber et al 1981). -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
An Ultra Diffuse Galaxy in the NGC 5846 Group from the VEGAS Survey Duncan A
A&A 626, A66 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935499 & c ESO 2019 Astrophysics An ultra diffuse galaxy in the NGC 5846 group from the VEGAS survey Duncan A. Forbes1, Jonah Gannon1, Warrick J. Couch1, Enrichetta Iodice2, Marilena Spavone2, Michele Cantiello3, Nicola Napolitano4, and Pietro Schipani2 1 Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia e-mail: [email protected] 2 INAF-Astronomical Observatory of Capodimonte, Salita Moiariello 16, 80131 Naples, Italy 3 INAF Astronomical Observatory of Abruzzo, Via Maggini snc, 64100 Teramo, Italy 4 School of Physics and Astronomy, Sun Yat-sen University Zhuhai Campus, 2 Daxue Road, Tangjia, Zhuhai, Guangdong 519082, PR China Received 19 March 2019 / Accepted 10 May 2019 ABSTRACT Context. Many ultra diffuse galaxies (UDGs) have now been identified in clusters of galaxies. However, the number of nearby UDGs suitable for detailed follow-up remain rare. Aims. Our aim is to begin to identify UDGs in the environments of nearby bright early-type galaxies from the VEGAS survey. Methods. Here we use a deep g band image of the NGC 5846 group, taken as part of the VEGAS survey, to search for UDGs. Results. We found one object with properties of a UDG if it associated with the NGC 5846 group, which seems likely. The galaxy, 8 we name NGC 5846_UDG1, has an absolute magnitude of Mg = −14.2, corresponding to a stellar mass of ∼10 M . It also reveals a system of compact sources which are likely globular clusters. Based on the number of globular clusters detected we estimate a halo 10 mass that is greater than 8 × 10 M for UDG1. -
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact Information: Department of Physics & Astronomy San
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact information: Department of Physics & Astronomy +1-408-924-5225 (office) San Jose´ State University +1-409-924-2917 (FAX) One Washington Square [email protected] San Jose, CA 95192 U.S.A. http://www.sjsu.edu/people/aaron.romanowsky/ University of California Observatories +1-831-459-3840 (office) 1156 High Street +1-831-426-3115 (FAX) Santa Cruz, CA 95064 [email protected] U.S.A. http://www.ucolick.org/%7Eromanow/ Main research interests: galaxy formation and dynamics – dark matter – star clusters Education: Ph.D. Astronomy, Harvard University Nov. 1999 supervisor: Christopher Kochanek, “The Structure and Dynamics of Galaxies” M.A. Astronomy, Harvard University June 1996 B.S. Physics with High Honors, June 1994 College of Creative Studies, University of California, Santa Barbara Employment: Professor, Department of Physics & Astronomy, Aug. 2020 – present San Jose´ State University Associate Professor, Department of Physics & Astronomy, Aug. 2016 – Aug. 2020 San Jose´ State University Assistant Professor, Department of Physics & Astronomy, Aug. 2012 – Aug. 2016 San Jose´ State University Research Associate, University of California Observatories, Santa Cruz Oct. 2012 – present Associate Specialist, University of California Observatories, Santa Cruz July 2007 – Sep. 2012 Researcher in Astronomy, Department of Physics, Oct. 2004 – June 2007 University of Concepcion´ Visiting Adjunct Professor, Faculty of Astronomical and May 2005 Geophysical Sciences, National University of La Plata Postdoctoral Research Fellow, School of Physics and Astronomy, June 2002 – Oct. 2004 University of Nottingham Postdoctoral Fellow, Kapteyn Astronomical Institute, Oct. 1999 – May 2002 Rijksuniversiteit Groningen Research Fellow, Harvard-Smithsonian Center for Astrophysics June 1994 – Oct. -
X-Ray Nature of the LINER Nuclear Sources O
A&A 460, 45–57 (2006) Astronomy DOI: 10.1051/0004-6361:20054756 & c ESO 2006 Astrophysics X-ray nature of the LINER nuclear sources O. González-Martín1, J. Masegosa1, I. Márquez1,M.A.Guerrero1, and D. Dultzin-Hacyan2 1 Instituto de Astrofísica de Andalucía, CSIC, Apartado Postal 3004, 18080 Granada, Spain e-mail: [email protected] 2 Instituto de Astronomía, UNAM, Apartado Postal 70-264, 04510 México D.F., México Received 22 December 2005 / Accepted 17 May 2006 ABSTRACT We report the results from a homogeneous analysis of the X-ray (Chandra ACIS) data available for a sample of 51 LINER galaxies selected from the catalogue by Carrillo et al. (1999, Rev. Mex. Astron. Astrofis., 35, 187) and representative of the population of bright LINER sources. The nuclear X-ray morphology has been classified by their nuclear compactness in the hard band (4.5– 8.0 keV) into 2 categories: active galactic nuclei (AGN) candidates (with a clearly identified unresolved nuclear source) and starburst (SB) candidates (without a clear nuclear source). Sixty percent of the total sample are classified as AGNs, with a median luminosity 40 −1 of LX(2−10 keV) = 2.5 × 10 erg s , which is an order of magnitude higher than for SB-like nuclei. The spectral fitting allows us to conclude that most of the objects need a non-negligible power-law contribution. When no spectral fitting can be performed (data with a low signal-to-noise ratio), the color–color diagrams allow us to roughly estimate physical parameters, such as column density, temperature of the thermal model, or spectral index for a power-law, and therefore to better constrain the origin of the X-ray emission. -
Spectroscopic Study of MATLAS-2019 with MUSE: an Ultra-Diffuse Galaxy with an Excess of Old Globular Clusters?,?? Oliver Müller1, Francine R
Spectroscopic study of MATLAS-2019 with MUSE An ultra-diffuse galaxy with an excess of old globular clusters Muller, Oliver; Marleau, Francine R.; Duc, Pierre-Alain; Habas, Rebecca; Fensch, Jeremy; Emsellem, Eric; Poulain, Melina; Lim, Sungsoon; Agnello, Adriano; Durrell, Patrick; Paudel, Sanjaya; Sanchez-Janssen, Ruben; van der Burg, Remco F. J. Published in: Astronomy & Astrophysics DOI: 10.1051/0004-6361/202038351 Publication date: 2020 Document version Publisher's PDF, also known as Version of record Document license: CC BY-NC Citation for published version (APA): Muller, O., Marleau, F. R., Duc, P-A., Habas, R., Fensch, J., Emsellem, E., Poulain, M., Lim, S., Agnello, A., Durrell, P., Paudel, S., Sanchez-Janssen, R., & van der Burg, R. F. J. (2020). Spectroscopic study of MATLAS- 2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters. Astronomy & Astrophysics, 640, [A106]. https://doi.org/10.1051/0004-6361/202038351 Download date: 30. sep.. 2021 A&A 640, A106 (2020) Astronomy https://doi.org/10.1051/0004-6361/202038351 & c O. Müller et al. 2020 Astrophysics Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters?,?? Oliver Müller1, Francine R. Marleau2, Pierre-Alain Duc1, Rebecca Habas1, Jérémy Fensch3, Eric Emsellem3,4, Mélina Poulain2, Sungsoon Lim5, Adriano Agnello6, Patrick Durrell7, Sanjaya Paudel8, Rubén Sánchez-Janssen9, and Remco F. J. van der Burg4 1 Observatoire Astronomique de Strasbourg (ObAS), Universite de Strasbourg – CNRS, UMR 7550, Strasbourg, France e-mail: [email protected] 2 Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstraße 25/8, Innsbruck 6020, Austria 3 Univ. -
Astronomy Astrophysics
A&A 455, 453–459 (2006) Astronomy DOI: 10.1051/0004-6361:20054212 & c ESO 2006 Astrophysics The globular cluster system of NGC 5846 revisited: colours, sizes and X-ray counterparts A. L. Chies-Santos1,M.G.Pastoriza1,B.X.Santiago1, and D. A. Forbes2 1 Departamento de Astronomia, Instituto de Física, UFRGS. Av. Bento Gonçalves 9500, Porto Alegre, RS, Brazil e-mail: [email protected] 2 Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia Received 15 September 2005 / Accepted 21 April 2006 ABSTRACT Context. NGC 5846 is a giant elliptical galaxy with a previously well studied globular cluster system (GCS), known to have a bimodal colour distribution with a remarkably high red fraction. Aims. Here we revisit the central galaxy regions searching for new globular cluster (GC) candidates, and measure magnitudes, colours and sizes for them. We also search for their X-ray counterparts. Methods. We use archival Hubble Space Telescope WFPC2 images, from which we modelled and subtracted the host light distribution to increase the available sample of GCs. We performed photometry on the central objects, and measured sizes and coordinates for the entire GC system known in this galaxy. Results. We detect two dozen previously unknown GC candidates in the central regions. Reliable sizes are obtained for about 60 GCs; their typical effective radii are in the range 3−5 pc. The largest clusters are located in the central regions. We find 7 X-ray counterparts to GCs, most of them in the central region. They are among the most luminous X-ray sources in NGC 5846. -
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.