Coma Berenices
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results Alice Shapley California Institute of Technology, Pasadena CA, 91125, USA G. Fabbiano Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 P. B. Eskridge Ohio State University, Dept. of Astronomy, 140 W 18th Ave, Columbus, OH 43210 ABSTRACT We have performed a multiparametric analysis of luminosity data for a sample of 234 normal spiral and irregular galaxies observed in X-rays with the Einstein Observatory. This sample is representative of S and Irr galaxies, with a good coverage of morphological types and absolute magnitudes. In addition to X-ray and optical data, we have compiled H-band magnitudes, IRAS near- and far-infrared, and 6cm radio continuum observations for the sample from the literature. We have also performed a careful compilation of distance estimates. We have explored the effect of morphology by dividing the sample into early (S0/a-Sab), intermediate (Sb-Sbc), and late-type (Sc-Irr) subsamples. The data were analysed with bivariate and multivariate survival analysis techniques that make full use of all the information available in both detections and limits. We find that most pairs of luminosities are correlated when considered individually, and this is not due to a distance bias. Different luminosity-luminosity correlations follow different power-law relations. Contrary to previous reports, the LX LB correlation follows a power-law with exponent − larger than 1. Both the significances of some correlations and their power-law relations are morphology dependent. -
Brightest Cluster Galaxies and Intracluster Light - Observations Magda Arnaboldi European Southern Observatory (Garching) O
Brightest cluster galaxies and intracluster light - Observations Magda Arnaboldi European Southern Observatory (Garching) O. Gerhard, L. Coccato, G. Ventimiglia, S. Okamura P. Das, M. Doherty, K. Freeman, E. Mc Neil, N. Yasuda, J.A.L. Aguerri, R. Ciardullo, K. Dolag, J.J. Feldmeier, G.H. Jacoby. M. Arnaboldi – BCGs and ICL: observations ESO, FVC+, 27 June - 01 July 2011 1 Outline 1. Brightest Cluster Galaxies and Intracluster light in clusters 2. Planetary nebulae as kinematical tracers 3. The Virgo cluster & M87 – The PNs’ VLOS and the projected phase space distribution – Dynamical status of the Virgo core – Large scale distribution of the ICL 4. The Hydra cluster & NGC 3311 – Observations : long-slit spectroscopy, MSIS, surface photometry – Debris from disrupted galaxies by the cluster potential 5. The Coma cluster core & the NGC 4874/NGC 4889 binary merger 6. Conclusions M. Arnaboldi – BCGs and ICL: observations ESO, FVC+, 27 June - 01 July 2011 2 1. ICL from deep photometry • Core of the Coma cluster: Photographic photometry Thuan & Kormendy 1977 • Abell 4010 (left, z=0.096) Abell 3888 (center, z=0.151) Deep CCD photometry Krick & Bernstein 2007 Abell 1914 (right) Feldmeier+2004 See also Melnick+’77, Bernstein ’95, Feldmeier+’04, Gonzalez+’05, Mihos+’05, Krick+’06 See contributions from J. Krick, J. Melnick, C. Rudick, S. Okamura M. Arnaboldi – BCGs and ICL: observations ESO, FVC+, 27 June - 01 July 2011 3 ICL properties in individual clusters • ICL surface brightness profile shape varies between clusters - Krick & Bernstein 2007 • Ellipticity generally increases with radius, position angle sometimes has sharp variations - Gonzalez + 2005 • Suggests ICL is dynamically young and separate from BCG PA (o) 50 0 -50 1 10 100 (kpc/h) 4 M. -
The Principal Axis of the Virgo Cluster
The Principal Axis of the Virgo Cluster Michael J. West Department of Physics & Astronomy, University of Hawaii at Hilo, Hilo, HI 96720 and John P. Blakeslee1 Department of Physics, University of Durham, Durham, DH1 3LE, England [email protected] ABSTRACT Using accurate distances to individual Virgo cluster galaxies obtained by the method of Sur- face Brightness Fluctuations, we show that Virgo’s brightest ellipticals have a remarkably collinear arrangement in three dimensions. This axis, which is inclined by ∼ 10 − 15◦ from the line of sight, can be traced to even larger scales where it appears to join a filamentary bridge of galaxies connecting Virgo to the rich cluster Abell 1367. The orientations of individual Virgo ellipticals also show some tendency to be aligned with the cluster axis, as does the jet of the supergiant elliptical M87. These results suggest that the formation of the Virgo cluster, and its brightest member galaxies, have been driven by infall of material along the Virgo-A1367 filament. Subject headings: galaxies: clusters: individual (Virgo), galaxies: formation, cosmology: large-scale structure of universe 1. Introduction Virgo dwarf elliptical galaxies also appears some- what elongated in this direction (Binggeli 1999), The Virgo cluster, at a distance of approxi- as does the distribution of hot X-ray emitting in- h−1 mately 15 Mpc, is the nearest richly-populated tracluster gas (B¨ohringer et al. 1994; Schindler, cluster of galaxies and, consequently, one of the Binggeli & B¨ohringer 1999). However, without best studied. A number of authors have pointed accurate distances to individual galaxies, it is im- arXiv:astro-ph/0008470v1 30 Aug 2000 out that Virgo’s brightest elliptical galaxies have possible to say for certain whether Virgo’s appar- a remarkably linear arrangement, along a pro- ◦ ent principal axis is a genuine three-dimensional jected position angle of roughly 110 (measured structure, or merely an illusory chance alignment North through East). -
THE GLOBULAR CLUSTER SYSTEM of the COMA CD GALAXY NGC 4874 from HUBBLE SPACE TELESCOPE ACS and WFC3/IR IMAGING* Hyejeon Cho1, John P
The Astrophysical Journal, 822:95 (23pp), 2016 May 10 doi:10.3847/0004-637X/822/2/95 © 2016. The American Astronomical Society. All rights reserved. THE GLOBULAR CLUSTER SYSTEM OF THE COMA CD GALAXY NGC 4874 FROM HUBBLE SPACE TELESCOPE ACS AND WFC3/IR IMAGING* Hyejeon Cho1, John P. Blakeslee2, Ana L. Chies-Santos3,4, M. James Jee1, Joseph B. Jensen5, Eric W. Peng6,7, and Young-Wook Lee1 1 Department of Astronomy and Center for Galaxy Evolution Research, Yonsei University, Seoul 03722, Korea; [email protected], [email protected] 2 NRC Herzberg Astronomy & Astrophysics, Victoria, BC V9E 2E7, Canada; [email protected] 3 Departamento de Astronomia, Instituto de Física, UFRGS, Porto Alegre, R.S. 91501-970, Brazil 4 Departamento de Astronomia, IAGCA, Universidade de São Paulo, 05508-900 São Paulo, SP, Brazil 5 Department of Physics, Utah Valley University, Orem, Utah 84058, USA 6 Department of Astronomy, Peking University, Beijing 100871, China 7 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China Received 2016 January 31; accepted 2016 April 4; published 2016 May 11 ABSTRACT We present new Hubble Space Telescope (HST) optical and near-infrared (NIR) photometry of the rich globular cluster (GC) system NGC 4874, the cD galaxy in the core of the Coma cluster (Abell 1656). NGC 4874 was observed with the HST Advanced Camera for Surveys in the F475W (g475) and F814W (I814) passbands and with the Wide Field Camera3 IR Channel in F160W (H160). The GCs in this field exhibit a bimodal optical color distribution with more than half of the GCs falling on the red side at g475−I814>1. -
Curriculum Vitae John P
Curriculum Vitae John P. Blakeslee National Research Council of Canada Phone: 1-250-363-8103 Herzberg Astronomy & Astrophysics Programs Fax: 1-250-363-0045 5071 West Saanich Road Cell: 1-250-858-1357 Victoria, B.C. V9E 2E7 Email: [email protected] Canada Citizenship: USA Education 1997 Ph.D., Physics, Massachusetts Institute of Technology (supervisor: Prof. John Tonry) 1991 B. A., Physics, University of Chicago (Honors; supervisor: Prof. Donald York) Employment History 2007 – present Astronomer, Senior Research Officer NRC Herzberg Institute of Astrophysics 2008 – present Adjunct Associate Professor Department of Physics, University of Victoria 2008 – 2013 Adjunct Professor Washington State University 2005 – 2007 Assistant Professor of Physics Washington State University 2004 – 2005 Research Scientist Johns Hopkins University 2000 – 2004 Associate Research Scientist Johns Hopkins University 1999 – 2000 Postdoctoral Research Associate University of Durham, U.K. 1996 – 1999 Fairchild Postdoctoral Scholar California Institute of Technology Fellowships and Awards 2004 Ernest F. Fullam Award for Innovative Research in Astronomy, Dudley Observatory 2003 NASA Certificate for contributions to the success of HST Servicing Mission 3B 1996 – 1999 Sherman M. Fairchild Postdoctoral Fellowship in Astronomy, Caltech Professional Service 2016 – present Canadian Large Synoptic Survey Telescope (LSST) Consortium, Co-PI 2014 – present Chair, NOAO Time Allocation Committee (TAC) Extragalactic Panel 2008 – present National Representative, Gemini International -
University of Groningen the Galaxy Population in the Coma Cluster Beijersbergen, Marco
University of Groningen The galaxy population in the Coma cluster Beijersbergen, Marco 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 Publisher's PDF, also known as Version of record Publication date: 2003 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Beijersbergen, M. (2003). The galaxy population in the Coma cluster. s.n. 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). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. 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: 07-10-2021 4 A Catalogue of Galaxies in the Coma Cluster Morphologies, Luminosity Functions and Cluster Dynamics M. Beijersbergen & J. M. van der Hulst ABSTRACT — We present a new multi-color catalogue of 583 spectroscopically confirmed members of the Coma cluster based on a deep wide field survey covering 5.2 deg2. -
The Herschel Sprint PHOTO ILLUSTRATION: PATRICIA GILLIS-COPPOLA, HERSCHEL IMAGE: WIKIMEDIA S&T
The Herschel Sprint PHOTO ILLUSTRATION: PATRICIA GILLIS-COPPOLA, HERSCHEL IMAGE: WIKIMEDIA S&T 34 April 2015 sky & telescope William Herschel’s Extraordinary Night of DiscoveryMark Bratton Recreating the legendary sweep of April 11, 1785 There’s little doubt that William Herschel was the most clearly with his instruments. As we will see, he did make signifi cant astronomer of the 18th century. His accom- occasional errors in interpretation, despite the superior plishments included the discovery of Uranus, infrared optics; for instance, he thought that the planetary nebula radiation, and four planetary satellites, as well as the M57 was a ring of stars. compilation of two extensive catalogues of double and The other factor contributing to Herschel’s interest multiple stars. His most lasting achievement, however, was the success of his sister, Caroline, in her study of the was his exhaustive search for undiscovered star clusters sky. He had built her a small telescope, encouraging her and nebulae, a key component in his quest to understand to search for double stars and comets. She located Messier what he called “the construction of the heavens.” In Her- objects and more, occasionally fi nding star clusters and schel’s time, astronomers were concerned principally with nebulae that had escaped the French astronomer’s eye. the study of solar system objects. The search for clusters Over the course of a year of observing, she discovered and nebulae was, up to that point, a haphazard aff air, with about a dozen star clusters and galaxies, occasionally not- a total of only 138 recorded by all the observers in history. -
The Infrared Surface Brightness Fluctuation Distances to the Hydra
The Infrared Surface Brightness Fluctuation Distances to the Hydra and Coma Clusters 1 Joseph B. Jensen John L. Tonry and Gerard A. Luppino Institute for Astronomy, UniversityofHawaii 2680 Woodlawn Drive, Honolulu, HI 96822 e-mail: [email protected], [email protected], [email protected] ABSTRACT We present IR surface brightness uctuation (SBF) distance measurements to NGC 4889 in the Coma cluster and to NGC 3309 and NGC 3311 in the Hydra cluster. We explicitly corrected for the contributions to the uctuations from globular clusters, background galaxies, and residual background variance. We measured a distance of 85 10 Mp c to NGC 4889 and a distance of 46 5 Mp c to the Hydra cluster. 1 1 Adopting recession velo cities of 7186 428 km s for Coma and 4054 296 km s 1 1 for Hydra gives a mean Hubble constantofH =87 11km s Mp c . Corrections 0 for residual variances were a signi cant fraction of the SBF signal measured, and, if underestimated, would bias our measurementtowards smaller distances and larger values of H . Both NICMOS on the Hubble Space Telescop e and large-ap erture 0 ground-based telescop es with new IR detectors will make accurate SBF distance measurements p ossible to 100 Mp c and b eyond. Subject headings: distance scale | galaxies: clusters: individual (Hydra, Coma) | galaxies: individual (NGC 3309, NGC 3311, NGC 4889) | galaxies: distances and redshifts 1. Intro duction Measuring accurate and reliable distances is a critical part of the quest to measure the Hubble constant H .Until recently, di erenttechniques for estimating extragalactic distances 0 1 Currently with the Gemini 8-m Telescop es Pro ject, 180 Kino ole St. -
Structural Parameters of Compact Stellar Systems
Structural Parameters of Compact Stellar Systems Juan Pablo Madrid Presented in fulfillment of the requirements of the degree of Doctor of Philosophy May 2013 Faculty of Information and Communication Technology Swinburne University Abstract The objective of this thesis is to establish the observational properties and structural parameters of compact stellar systems that are brighter or larger than the “standard” globular cluster. We consider a standard globular cluster to be fainter than M 11 V ∼ − mag and to have an effective radius of 3 pc. We perform simulations to further un- ∼ derstand observations and the relations between fundamental parameters of dense stellar systems. With the aim of establishing the photometric and structural properties of Ultra- Compact Dwarfs (UCDs) and extended star clusters we first analyzed deep F475W (Sloan g) and F814W (I) Hubble Space Telescope images obtained with the Advanced Camera for Surveys. We fitted the light profiles of 5000 point-like sources in the vicinity of NGC ∼ 4874 — one of the two central dominant galaxies of the Coma cluster. Also, NGC 4874 has one of the largest globular cluster systems in the nearby universe. We found that 52 objects have effective radii between 10 and 66 pc, in the range spanned by extended star ∼ clusters and UCDs. Of these 52 compact objects, 25 are brighter than M 11 mag, V ∼ − a magnitude conventionally thought to separate UCDs and globular clusters. We have discovered both a red and a blue subpopulation of Ultra-Compact Dwarf (UCD) galaxy candidates in the Coma galaxy cluster. Searching for UCDs in an environment different to galaxy clusters we found eleven Ultra-Compact Dwarf and 39 extended star cluster candidates associated with the fossil group NGC 1132. -
Radio Investigations of Clusters of Galaxies
• • RADIO INVESTIGATIONS OF CLUSTERS OF GALAXIES a study of radio luminosity functions, wide-angle head-tailed radio galaxies and cluster radio haloes with the Westerbork Synthesis Radio Telescope proefschrift ter verkrijging van degraad van Doctor in de Wiskunde en Natuurwetenschappen aan de Rijksuniversiteit te Leiden, op gezag van de Rector Magnificus Or. D.J. Kuenen, hoogleraar in de Faculteit der Wiskunde en Natuurwetenschappen, volgens besluit van het College van Dekanen te verdedigen op woensdag 20 december 1978 teklokke 15.15 uur door Edwin Auguste Valentijn geboren te Voorburg in 1952 Sterrewacht Leiden 1978 elve/labor vincit - Leiden Promotor: Prof. Dr. H. van der Laan aan Josephine aan mijn ouders Cover: Some radio contours (1415 MHz) of the extended radio galaxies NGC6034, NGC6061 and 1B00+1SW2 superimposed to a smoothed galaxy distribution (number of galaxies per unit area, taken from Shane) of the Hercules Superoluster. The 90 % confidence error boxes of the Ariel VandUHURU observations of the X-ray source A1600+16 are also included. In the region of overlap of these two error boxes the position of a oD galaxy is indicated. The combined picture suggests inter-galactic material pervading the whole superaluster. CONTENTS CHAPTER 1 GENERAL INTRODUCTION AND SUMMARY 9 PART 1 OBSERVATIONS OF THE COI1A CLUSTER AT 610 MHZ 15 CHAPTER 2 COMA CLUSTER GALAXIES 17 Observation of the Coma Cluster at 610 MHz (Paper III, with W.J. Jaffe and G.C. Perola) I Introduction 17 II Observations 18 III Data Reduction 18 IV Radio Source Parameters 19 V Optical Data 20 VI The Radio Luminosity Function of the Coma Cluster Galaxies 21 a) LF of the (E+SO) Galaxies 23 b) LF of the (S+I) Galaxies 25 c) Radial Dependence of the LF 26 VII Other Properties of the Detected Cluster Galaxies 26 a) Spectral Indexes b) Emission Lines VIII The Central Radio Sources 27 a) 5C4.85 = NGC4874 27 b) 5C4.8I - NGC4869 28 c) Coma C 29 CHAPTER 3 RADIO SOURCES IN COMA NOT IDENTIFIED WITH CLUSTER GALAXIES 31 Radio Data and Identifications (Paper IV, with G.C. -
SAC's 110 Best of the NGC
SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog. -
Globular Cluster Systems in Brightest Cluster Galaxies
GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY Item Type Article Authors Harris, William E.; Ciccone, Stephanie M.; Eadie, Gwendolyn M.; Gnedin, Oleg Y.; Geisler, D.; Rothberg, B.; Bailin, Jeremy Citation GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY 2017, 835 (1):101 The Astrophysical Journal DOI 10.3847/1538-4357/835/1/101 Publisher IOP PUBLISHING LTD Journal The Astrophysical Journal Rights © 2017. The American Astronomical Society. All rights reserved. Download date 04/10/2021 03:48:29 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/622870 The Astrophysical Journal, 835:101 (21pp), 2017 January 20 doi:10.3847/1538-4357/835/1/101 © 2017. The American Astronomical Society. All rights reserved. GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY William E. Harris1, Stephanie M. Ciccone1, Gwendolyn M. Eadie1, Oleg Y. Gnedin2, Douglas Geisler3, Barry Rothberg4, and Jeremy Bailin5 1 Department of Physics & Astronomy, McMaster University, Hamilton, ON, Canada; [email protected], [email protected], [email protected] 2 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; [email protected] 3 Departamento de Astronomiá, Universidad de Concepción, Casilla 160-C, Concepción, Chile; [email protected] 4 LBT Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA; [email protected] 5 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA; [email protected] Received 2016 September 13; revised 2016 November 7; accepted 2016 November 21; published 2017 January 20 ABSTRACT We present new deep photometry of the rich globular cluster (GC) systems around the Brightest Cluster Galaxies UGC 9799 (Abell 2052) and UGC 10143 (Abell 2147),obtainedwiththeHubble Space Telescope (HST) ACS and WFC3 cameras.