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The Dynamical State of the Coma Cluster with XMM-Newton?
A&A 400, 811–821 (2003) Astronomy DOI: 10.1051/0004-6361:20021911 & c ESO 2003 Astrophysics The dynamical state of the Coma cluster with XMM-Newton? D. M. Neumann1,D.H.Lumb2,G.W.Pratt1, and U. G. Briel3 1 CEA/DSM/DAPNIA Saclay, Service d’Astrophysique, L’Orme des Merisiers, Bˆat. 709, 91191 Gif-sur-Yvette, France 2 Science Payloads Technology Division, Research and Science Support Dept., ESTEC, Postbus 299 Keplerlaan 1, 2200AG Noordwijk, The Netherlands 3 Max-Planck Institut f¨ur extraterrestrische Physik, Giessenbachstr., 85740 Garching, Germany Received 19 June 2002 / Accepted 13 December 2002 Abstract. We present in this paper a substructure and spectroimaging study of the Coma cluster of galaxies based on XMM- Newton data. XMM-Newton performed a mosaic of observations of Coma to ensure a large coverage of the cluster. We add the different pointings together and fit elliptical beta-models to the data. We subtract the cluster models from the data and look for residuals, which can be interpreted as substructure. We find several significant structures: the well-known subgroup connected to NGC 4839 in the South-West of the cluster, and another substructure located between NGC 4839 and the centre of the Coma cluster. Constructing a hardness ratio image, which can be used as a temperature map, we see that in front of this new structure the temperature is significantly increased (higher or equal 10 keV). We interpret this temperature enhancement as the result of heating as this structure falls onto the Coma cluster. We furthermore reconfirm the filament-like structure South-East of the cluster centre. -
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. -
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. -
The Coma Cluster in Relation to Its Environs
THE COMA CLUSTER IN RELATION TO ITS ENVIRONS Michael J. Westa Saint Mary’s University Department of Astronomy & Physics Halifax, Nova Scotia B3H 3C3, Canada E-mail: [email protected] Clusters of galaxies are often embedded in larger-scale superclusters with dimen- sions of tens or perhaps even hundreds of Mpc. Observational and theoretical evidence suggest an important connection between cluster properties and their surroundings, with cluster formation being driven primarily by the infall of mate- rial along large-scale filaments. Nowhere is this connection more obvious than the Coma cluster. 1 Historical Background The Coma cluster’s surroundings have been discussed in the astronomical liter- ature for nearly as long as the cluster itself. William Herschel (1785) discovered what he called “the nebulous stratum of Coma Berenices” and remarked that “I have fully ascertained the existence and direction of this stratum for more than 30 degrees of a great circle and found it to be almost every where equally rich in fine nebulae.” Coma’s sprawling galaxy distribution was also evident in Max Wolf’s (1902) catalogue of nebulae in and around Coma (see Figure 1). Shapley’s (1934) observations led him to conclude that “A general inspection of the region within several degrees of the Coma cluster suggests that the cluster is part of, or is associated with, an extensive metagalactic cloud...” Shane & Wirtanen (1954), on the other hand, argued that the Coma cluster is a single isolated entity which blends into the background at a projected distance of ∼ 2◦ (2.5 h−1 Mpc) from its centre. -
NASA-CR-2044 I Elei Aental Abundances in the Intracluster Gas and the Hot Galactic Coronae in Cluster A194 .-..VJ//-I<- ,I, N
.-..VJ//-i<- ,i, NASA-CR-2044_I Elei_aental Abundances in the Intracluster Gas and the Hot Galactic Coronae in Cluster A194 ,. - ? 4 NASA Grant NAG5-2611 Performance Report For the Period 15 June 1996 through 14 June 1997 Principal Investigator Dr. William R. Forman May 1997 Prepared for: National Aeronautics and Space Administration Goddard Space Flight Center Greenbelt, Maryland 20771 , Smithsonian Institution Astrophysical Observatory Cambridge, Massachusetts 02138 The Smithsonian Astrophysical Observatory is a member of the Halwatd-Smithsonian Center for Astrophysics The NASA Technical Oflicez for this grant is Dr. Nicholas E. White, NASA, Goddard Space Flight Center, Mail_op 662.0, Greenbelt, MD 20771. 1 Report for NAG5-2611 We have completed the analysis of observations of the Coma cluster and are continuing analysis of A1367 both of which are shown to be merging clusters. Also, we are analyzing observations of the Centaurus cluster which we see as a merger based in both its temperature and surface brightness distributions. 2 Coma Cluster Revisited Our results on the Coma cluster have been published in the Astrophysical Journal (1997 ApJ, 474, 7; see attached). We performed a wavelet transform analysis of the ROSAT PSPC images of the Coma cluster. On small scales, less than about 1 arc minute the wavelet analysis shows substructure dominated by two extended sources surrounding the two brightest cluster galaxies NGC 4874 and NGC 4889. On slightly larger scales, about 2 arc minutes, the wavelet analysis reveals a filament of X-ray emission originating near the cluster center, curving to the south and east for about 25 arc minutes in the direction of the galaxy NGC 4911, and ending near the galaxy NGC 4921. -
Binocular Challenges
This page intentionally left blank Cosmic Challenge Listing more than 500 sky targets, both near and far, in 187 challenges, this observing guide will test novice astronomers and advanced veterans alike. Its unique mix of Solar System and deep-sky targets will have observers hunting for the Apollo lunar landing sites, searching for satellites orbiting the outermost planets, and exploring hundreds of star clusters, nebulae, distant galaxies, and quasars. Each target object is accompanied by a rating indicating how difficult the object is to find, an in-depth visual description, an illustration showing how the object realistically looks, and a detailed finder chart to help you find each challenge quickly and effectively. The guide introduces objects often overlooked in other observing guides and features targets visible in a variety of conditions, from the inner city to the dark countryside. Challenges are provided for viewing by the naked eye, through binoculars, to the largest backyard telescopes. Philip S. Harrington is the author of eight previous books for the amateur astronomer, including Touring the Universe through Binoculars, Star Ware, and Star Watch. He is also a contributing editor for Astronomy magazine, where he has authored the magazine’s monthly “Binocular Universe” column and “Phil Harrington’s Challenge Objects,” a quarterly online column on Astronomy.com. He is an Adjunct Professor at Dowling College and Suffolk County Community College, New York, where he teaches courses in stellar and planetary astronomy. Cosmic Challenge The Ultimate Observing List for Amateurs PHILIP S. HARRINGTON CAMBRIDGE UNIVERSITY PRESS Cambridge, New York, Melbourne, Madrid, Cape Town, Singapore, Sao˜ Paulo, Delhi, Dubai, Tokyo, Mexico City Cambridge University Press The Edinburgh Building, Cambridge CB2 8RU, UK Published in the United States of America by Cambridge University Press, New York www.cambridge.org Information on this title: www.cambridge.org/9780521899369 C P. -
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 -
Statistical Analysis of Bound Companions in the Coma Cluster Martin Mendelin and Bruno Binggeli
A&A 604, A96 (2017) Astronomy DOI: 10.1051/0004-6361/201730567 & c ESO 2017 Astrophysics Statistical analysis of bound companions in the Coma cluster Martin Mendelin and Bruno Binggeli Department of Physics, Basel University, Klingelbergstrasse 82, 4056 Basel, Switzerland e-mail: [email protected]; [email protected] Received 6 February 2017 / Accepted 12 April 2017 ABSTRACT Aims. The rich and nearby Coma cluster of galaxies is known to have substructure. We aim to create a more detailed picture of this substructure by searching directly for bound companions around individual giant members. Methods. We have used two catalogs of Coma galaxies, one covering the cluster core for a detailed morphological analysis, another covering the outskirts. The separation limit between possible companions (secondaries) and giants (primaries) is chosen as MB = −19 and MR = −20, respectively for the two catalogs. We have created pseudo-clusters by shuffling positions or velocities of the primaries and search for significant over-densities of possible companions around giants by comparison with the data. This method was devel- oped and applied first to the Virgo cluster. In a second approach we introduced a modified nearest neighbor analysis using several interaction parameters for all galaxies. Results. We find evidence for some excesses due to possible companions for both catalogs. Satellites are typically found among the faintest dwarfs (MB < −16) around high-luminosity primaries. The most significant excesses are found around very luminous late-type giants (spirals) in the outskirts, which is expected in an infall scenario of cluster evolution. A rough estimate for an upper limit of bound galaxies within Coma is ∼2−4%, to be compared with ∼7% for Virgo. -
QUANTITATIVE MORPHOLOGY of GALAXIES in the CORE of the COMA CLUSTER Carlos M
The Astrophysical Journal, 602:664–677, 2004 February 20 A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. QUANTITATIVE MORPHOLOGY OF GALAXIES IN THE CORE OF THE COMA CLUSTER Carlos M. Gutie´rrez, Ignacio Trujillo,1 and Jose A. L. Aguerri Instituto de Astrofı´sica de Canarias, E-38205, La Laguna, Tenerife, Spain Alister W. Graham Department of Astronomy, University of Florida, Gainesville, FL 32611 and Nicola Caon Instituto de Astrofı´sica de Canarias, E-38205, La Laguna, Tenerife, Spain Received 2003 July 26; accepted 2003 October 17 ABSTRACT We present a quantitative morphological analysis of 187 galaxies in a region covering the central 0.28 deg2 of the Coma Cluster. Structural parameters from the best-fitting Se´rsic r1=n bulge plus, where appropriate, expo- nential disk model, are tabulated here. This sample is complete down to a magnitude of R ¼ 17 mag. By examining the recent compilation by Edwards et al. of galaxy redshifts in the direction of Coma, we find that 163 of the 187 galaxies are Coma Cluster members and that the rest are foreground and background objects. For the Coma Cluster members, we have studied differences in the structural and kinematic properties between early- and late-type galaxies and between the dwarf and giant galaxies. Analysis of the elliptical galaxies reveals correlations among the structural parameters similar to those previously found in the Virgo and Fornax Clusters. Comparing the structural properties of the Coma Cluster disk galaxies with disk galaxies in the field, we find evidence for an environmental dependence: the scale lengths of the disk galaxies in Coma are 30% smaller. -
Galaxy Clusters Observations
Galaxy cluster observations: structure and dynamics of the intracluster medium Jeremy Sanders Max Planck Institute for Extraterrestrial Physics (MPE) K. Dennerl, H. R. Russell, C. Pinto, A. C. Fabian, S. A. Walker, J. ZuHone, D. Eckert, T. Tamura, F. Hofmann Clusters on large scales r 500 r 200 3r200 rvir Nelsen+14 Reiprich+13 Outer parts of clusters should be The turbulence in the intracluster increasingly disturbed/turbulent medium (ICM), the main baryonic cluster due to merging subclumps component, should increase with radius Perseus cluster: XMM EPIC-MOS mosaic Asymmetries likely caused by sloshing of gas in potential well due to perturbation, see e.g. Churazov+00, Simionescu+12 Detailed view of outer cold front in Perseus: Walker+18 (talk in meeting) Edges known as “Cold fronts” (Markevitch+07) 1 degree (1.3 Mpc) Perseus cluster: XMM EPIC-MOS mosaic Asymmetries likely caused by sloshing of gas in potential well due to perturbation, see e.g. Churazov+00, Simionescu+12 Detailed view of outer cold front in Perseus: Walker+18 (talk in meeting) Edges known as “Cold fronts” (Markevitch+07) ZuHone+18 simulation of different sightlines showing bulk motions 1 degree (1.3 Mpc) AGN feedback in clusters from J. Hlavacek-Larrondo (review in Fabian 2012) Many clusters show short cooling times in their cores – would rapidly cool if emitted energy not replaced Feedback is seen in the form of cavities generated by AGN jets in most clusters with short cooling times (e.g. Panagoulia+14) Energetically, AGN can prevent cooling in majority of objects over -
1977Apj. . .213. .327A the Astrophysical Journal, 213:327-344
.327A .213. The Astrophysical Journal, 213:327-344, 1977 April 15 . © 1977. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1977ApJ. THE LUMINOSITY FUNCTION AND STRUCTURE OF THE COMA CLUSTER G. O. Abell Department of Astronomy, University of California, Los Angeles Received 1976 August 6 ABSTRACT The luminosity function of the galaxies in the Coma cluster is determined by a procedure of extrafocal photographic photometry. The logarithmic integrated luminosity function rises sharply with increasing magnitude through the interval mv = 11.6 to 14.5, and then slowly for greater magnitudes to the limit mv = 19.4. The data suggest a moderate increase in the slope of the function for magnitudes fainter than mv = 17.5. The cluster is found, in projection, to be ellipsoidal in shape, centered at (1950) a = 12h56IP9; 0 5 = +28 14'. To the limit mv = 18.3 the cluster is estimated to have 1525 member galaxies. The brighter galaxies in the inner part of the cluster have a distribution resembling that of the iso- thermal polytrope, but there is no marked segregation of bright and faint galaxies, as would be required for complete statistical equilibrium. The luminosity of the cluster is estimated at 2 x 1013 L©. The mass-to-light ratio (in solar units) is found probably not to exceed 122. Subject headings: galaxies : clusters of—galaxies: photometry I. INTRODUCTION II. OBSERVATIONS The first important discussion of the galaxian a) Photometric Procedure luminosity function was by Hubble (1926), who Galaxian magnitudes are obtained here by a investigated the absolute magnitudes of 134 late method of extrafocal photographic photometry spirals and 11 irregular galaxies (most of which are described by Abell and Mihalas (1966).