Decimal Ra=2.9165857, Dec=-0.47393445

Total Page:16

File Type:pdf, Size:1020Kb

Decimal Ra=2.9165857, Dec=-0.47393445 Object name: SDSS J001139.98-002826.1 Source: galaxyzoo.org SDSS ID 587731185668325535 Position: decimal ra=2.9165857, dec=-0.47393445 Redshifts 0.057 red blob NW SDSS photometry ugriz 16.87 15.44 14.80 14.43 14.15 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587731185668325535 Other data: interacting SDSS Image Object name: SDSS J001558.24-001812.6 Source: galaxyzoo.org/year3a SDSS ID 588015508734214286 Position: decimal ra=3.99268881, dec=-0.3035158 Redshifts 0.0394 (W) 0.0397 (E) SDSS photometry ugriz 17.42 15.32 14.48 14.08 13.75 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015508734214286 Other data: NGC 0060; stripe82 8647474691409969299 interacting? SDSS Image Object name: SDSS J002025.78+004934.8 Source: galaxyzoo.org052408 SDSS ID 587731187279921175 Position: decimal ra=5.10744559, dec=0.82634628 Redshifts 0.016942 (SW) 0.018436 (NE, NED) SDSS photometry ugriz 16.14 14.58 13.73 13.30 13.03 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp? id=587731187279921175 Other data: NGC 78. Mkn 547 interacting? SDSS Image Object name: SDSS J002820.53-001304.3 Source: galaxyzoo.org/011608 SDSS ID 588015508735590537 Position: decimal ra=7.08554208, dec=-0.21786197 Redshifts 0.061 (E) SDSS photometry ugriz 16.85 15.19 14.41 13.99 13.78 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=588015508735590537 Other data: UGC 280; SDSS says object W is a galaxy too. SDSS Image Object name: NGC 191, SDSS J003859.43-090009.3 Source: galaxyzoo.org/KW SDSS ID 587727180601163792 Position: decimal ra=9.74766481, dec=-9.00261082 Redshifts 0.020 S SDSS photometry ugriz 15.85 13.84 12.97 12.53 12.23 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587727180601163792 Other data: interacting SDSS Image Object name: SDSS J003918.79+005330.9 Source: galaxyzoo.org/year3a SDSS ID 588015510347382868 Position: decimal ra=9.82830964, dec=0.89192003 Redshifts 0.0139 (S) 0.01419 (N, NED) SDSS photometry ugriz 17.10 15.79 18.13 15.25 14.92 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015510347382868 Other data: NGC 196/7; stripe82 tidal asymmetry interacting SDSS Image Object name:SDSS J004153.50-092943.9 Source: galaxyzoo.org/tmpthread SDSS ID 587727180064620552 Position: decimal ra=10.47293259, dec=-9.49553546 Redshifts 0.051 (middle of 3) SDSS photometry ugriz 20.39 18.37 17.46 16.96 16.52 SDSS explorer http://cas.sdss.org/dr6/en/tools/explore/obj.asp? id=587727180064620552 Other data: interacting SDSS Image Object name: SDSS J005555.93+003940.3 Source: galaxyzoo.org/thread SDSS ID 587731187283787895 Position: decimal ra=13.98308254, dec=0.66121656 Redshifts 0.067 (E) SDSS photometry ugriz 18.88 16.75 15.69 15.16 14.75 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587731187283787895 Other data: interacting SDSS Image Object name: SDSS J010006.52+000649.3 Source: galaxyzoo.org/year3a SDSS ID 588015509275934785 Position: decimal ra=15.02717513, dec=0.11369875 Redshifts SDSS photometry ugriz 18.85 16.90 15.84 15.39 14.99 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015509275934785 Other data: stripe82 8647474691951689768 where’s overlap? SDSS Image Object name: SDSS J010008.54+000615.7 Source: galaxyzoo.org/year3a SDSS ID 588015509275934803 Position: decimal ra=15.03558427, dec=0.10438068 Redshifts 0.1102 (E) SDSS photometry ugriz 20.03 18.07 17.04 16.60 16.26 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015509275934803 Other data: stripe 82 8647474691951690053; in field with above pair SDSS Image Object name: SDSS J011728.10+144215.8 Source: galaxyzoo.org/thread SDSS ID 587724198816383056 Position: decimal ra=19.36712184, dec=14.70441657 Redshifts 0.043 (NW) SDSS photometry ugriz 17.28 15.83 15.07 14.66 14.30 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587724198816383056 Other data: interacting SDSS Image Object name:SDSS J013402.46-010432.7 Source: galaxyzoo.org/071408 SDSS ID 588015507669057650 Position: decimal ra=23.51025813, dec=-1.07576861 Redshifts : 0.01556 (NED) SDSS photometry ugriz 16.25 14.58 13.77 13.33 12.96 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp? id=588015507669057650 Other data: UGC 1120 too far apart SDSS Image Object name: SDSS J014724.52+140454.2 Source: galaxyzoo.org/thread SDSS ID 587724198819594346 Position: decimal ra=26.8521868, dec=14.08172444 Redshifts 0.421 (emission) 0.071 (absorption) SDSS photometry ugriz 19.33 17.47 16.54 16.11 15.77 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587724198819594346 Other data: redshifts are the wrong way around for absorption. B dz SDSS Image Object name:SDSS J020934.56+060546.5 Source: galaxyzoo.org/051309 SDSS ID 587744293894553676 Position: decimal ra=32.39402114, dec=6.09627678 Redshifts SDSS photometry ugriz 16.35 15.08 14.40 14.04 13.75 SDSS explorer http://cas.sdss.org/dr7/en/tools/explore/obj.asp? id=587744293894553676 Other data: interacting SDSS Image Object name: SDSS J021106.49-003921.3 Source: galaxyzoo.org/thread SDSS ID 588015508209991735 Position: decimal ra=32.77706747, dec=-0.6559434 Redshifts 0.019931 (E, NED) 0.019908 (W, NED) SDSS photometry ugriz 22.48 20.87 20.42 24.36 21.71 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp? id=588015508209991735 Other data: warped - interacting SDSS Image Object name: SDSS J021559.11+183224.2 Source: galaxyzoo.org/year3a SDSS ID 758881523725631607 Position: decimal ra=33.99632242, dec=18.54005704 Redshifts SDSS photometry ugriz 18.01 15.94 15.00 14.51 14.17 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=758881523725631607 Other data: interacting SDSS Image Object name: SDSS J021623.73+005416.3 Source: galaxyzoo.org/year3a SDSS ID 588015510358065294 Position: decimal ra=34.09889199, dec=0.90453477 Redshifts SDSS photometry ugriz 20.80 19.00 18.26 17.99 17.83 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015510358065294 Other data: stripe82 8647474693033754748 bg too small SDSS Image Object name: SDSS J022053.43+003324.3 Source: galaxyzoo.org/year3a SDSS ID 588015509821653051 Position: decimal ra=35.22263327, dec=0.55675572 Redshifts 0.02437 (W, NED) 0.05842 (E, NED) SDSS photometry ugriz 16.59 14.68 13.80 13.46 13.10 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015509821653051 Other data: UGC 1809, UM 420 (bg) asymmetric large dz SDSS Image Object name: SDSS J023143.18+005415.8 Source: galaxyzoo.org/year3a SDSS ID 588015510359703672 Position: decimal ra=37.92993908, dec=0.9043924 Redshifts 0.0210 (W) SDSS photometry ugriz 16.56 15.32 14.69 14.37 14.14 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015510359703672 Other data: stripe82 8647474693035458592 interacting SDSS Image Object name: SDSS J030503.86-010356.8 Source: galaxyzoo.org/year3a SDSS ID 588015507679019130 Position: decimal ra=46.2661165, dec=-1.06578496 Redshifts 0.1539 (SE) SDSS photometry ugriz 20.36 18.45 17.25 16.78 16.44 SDSS explorer http://cas.sdss.org/public/en/tools/explore/obj.asp? id=588015507679019130 Other data: stripe82 8647474690354709161 too far apart SDSS Image Object name: SDSS J030614.52-002039.7 Source: galaxyzoo.org/thread SDSS ID 588015508752891945 Position: decimal ra=46.56051024, dec=-0.34438157 Redshifts 0.029 (SE) 0.029 (NW) SDSS photometry ugriz 17.13 16.00 15.30 14.96 14.73 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=588015508752891945 Other data: interacting SDSS Image Object name: SDSS J031320.80-071952.5 Source: galaxyzoo.org/thread SDSS ID 587724241229512856 Position: decimal ra=48.33667378, dec=-7.33125029 Redshifts 0.116 (E) SDSS photometry ugriz 19.61 17.80 16.87 16.37 15.95 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp?id=587724241229512856 Other data: interacting SDSS Image Object name:SDSS J032454.54+010609.1 Source: galaxyzoo.org/040210 SDSS ID 8647475122537955651 DR7: 587731514230571158 Position: decimal ra=51.22727924, dec=1.10254994 Redshifts 0.0303 SDSS photometry ugriz 17.74 16.85 16.55 16.33 16.16 SDSS explorer http://cas.sdss.org/stripe82/en/tools/explore/obj.asp? id=8647475122537955651 Other data: SDSS: red blotch NW is galaxy; Zoo2 image N at top too small SDSS82 Image Object name:SDSS J033440.48-070838.0 Source: galaxyzoo.org/thread SDSS ID 587724240694935697 Position: decimal ra=53.66869035, dec=-7.14391344 Redshifts 0.038 (NW) SDSS photometry ugriz 17.84 16.49 15.74 15.33 15.00 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp? id=587724240694935697 Other data: interacting SDSS Image Object name: SDSS J035424.20+003938.3 Source: galaxyzoo.org/040210 SDSS ID 587731513696977042 Stripe82: 8658182045944905874 Position: decimal ra=58.60085004, dec=0.66065494 Redshifts SDSS photometry ugriz 20.98 18.75 17.51 16.84 16.32 SDSS explorer http://cas.sdss.org/dr7/en/tools/explore/obj.asp? id=587731513696977042 Other data: stripe82. Tides? interacting SDSS Image Object name:SDSS J063612.48+825808.9 Source: galaxyzoo.org/122108 SDSS ID 758882630213763298 Position: decimal ra=99.05200041, dec=82.96916195 Redshifts 0.014223 (NED) SDSS photometry ugriz 16.55 14.07 13.06 12.59 12.22 SDSS explorer http://cas.sdss.org/astro/en/tools/explore/obj.asp? id=758882630213763298 Other data: IC 442 B E in foreground? SDSS Image Object name:SDSS J074901.11+381046.5 Source: galaxyzoo.org/062709 SDSS ID 588007004156592494 Position: decimal ra=117.25463618, dec=38.1796 Redshifts SDSS photometry ugriz
Recommended publications
  • Clusters of Galaxies…
    Budapest University, MTA-Eötvös François Mernier …and the surprisesoftheir spectacularhotatmospheres Clusters ofgalaxies… K complex ) ⇤ Fe ) α [email protected] - Wallon Super - Wallon [email protected] Fe XXVI (Ly (/ Fe XXIV) L complex ) ) (incl. Ne) α α ) Fe ) ) α ) α α ) ) ) ) α ⇥ ) ) ) α α α α α α Si XIV (Ly Mg XII (Ly Ni XXVII / XXVIII Fe XXV (He S XVI (Ly O VIII (Ly Si XIII (He S XV (He Ca XIX (He Ca XX (Ly Fe XXV (He Cr XXIII (He Ar XVII (He Ar XVIII (Ly Mn XXIV (He Ca XIX / XX Yo u are h ere ! 1 km = 103 m Yo u are h ere ! (somewhere behind…) 107 m Yo u are h ere ! (and this is the Moon) 109 m ≃3.3 light seconds Yo u are h ere ! 1012 m ≃55.5 light minutes 1013 m 1014 m Yo u are h ere ! ≃4 light days 1013 m Yo u are h ere ! 1014 m 1017 m ≃10.6 light years 1021 m Yo u are h ere ! ≃106 000 light years 1 million ly Yo u are h ere ! The Local Group Andromeda (M31) 1 million ly Yo u are h ere ! The Local Group Triangulum (M33) 1 million ly Yo u are h ere ! The Local Group 10 millions ly The Virgo Supercluster Virgo cluster 10 millions ly The Virgo Supercluster M87 Virgo cluster 10 millions ly The Virgo Supercluster 2dFGRS Survey The large scale structure of the universe Abell 2199 (429 000 000 light years) Abell 2029 (1.1 billion light years) Abell 2029 (1.1 billion light years) Abell 1689 Abell 1689 (2.2 billion light years) Les amas de galaxies 53 Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”…
    [Show full text]
  • Guide Du Ciel Profond
    Guide du ciel profond Olivier PETIT 8 mai 2004 2 Introduction hjjdfhgf ghjfghfd fg hdfjgdf gfdhfdk dfkgfd fghfkg fdkg fhdkg fkg kfghfhk Table des mati`eres I Objets par constellation 21 1 Androm`ede (And) Andromeda 23 1.1 Messier 31 (La grande Galaxie d'Androm`ede) . 25 1.2 Messier 32 . 27 1.3 Messier 110 . 29 1.4 NGC 404 . 31 1.5 NGC 752 . 33 1.6 NGC 891 . 35 1.7 NGC 7640 . 37 1.8 NGC 7662 (La boule de neige bleue) . 39 2 La Machine pneumatique (Ant) Antlia 41 2.1 NGC 2997 . 43 3 le Verseau (Aqr) Aquarius 45 3.1 Messier 2 . 47 3.2 Messier 72 . 49 3.3 Messier 73 . 51 3.4 NGC 7009 (La n¶ebuleuse Saturne) . 53 3.5 NGC 7293 (La n¶ebuleuse de l'h¶elice) . 56 3.6 NGC 7492 . 58 3.7 NGC 7606 . 60 3.8 Cederblad 211 (N¶ebuleuse de R Aquarii) . 62 4 l'Aigle (Aql) Aquila 63 4.1 NGC 6709 . 65 4.2 NGC 6741 . 67 4.3 NGC 6751 (La n¶ebuleuse de l’œil flou) . 69 4.4 NGC 6760 . 71 4.5 NGC 6781 (Le nid de l'Aigle ) . 73 TABLE DES MATIERES` 5 4.6 NGC 6790 . 75 4.7 NGC 6804 . 77 4.8 Barnard 142-143 (La tani`ere noire) . 79 5 le B¶elier (Ari) Aries 81 5.1 NGC 772 . 83 6 le Cocher (Aur) Auriga 85 6.1 Messier 36 . 87 6.2 Messier 37 . 89 6.3 Messier 38 .
    [Show full text]
  • HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land
    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land 1 Executive Summary • There are now 420 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 27 November, nineteen published papers in 2020 • HET papers have 29363 citations – Average of 70, median of 39 citations per paper – H-number of 90 – 81 papers have ≥ 100 citations; 175 have ≥ 50 cites • Wide angle surveys account for 26% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 47% of the papers and 47% of the citations, respectively. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 420 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2020 a total of fifteen HET papers appeared; nineteen have been published to date in 2020. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time.
    [Show full text]
  • Tracking Star Formation in Dwarf Cluster Galaxies Cody Millard Rude
    University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2015 Tracking Star Formation In Dwarf Cluster Galaxies Cody Millard Rude Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Rude, Cody Millard, "Tracking Star Formation In Dwarf Cluster Galaxies" (2015). Theses and Dissertations. 1829. https://commons.und.edu/theses/1829 This Dissertation is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. TRACKING STAR FORMATION IN DWARF CLUSTER GALAXIES by Cody Millard Rude Bachelor of Science, University of University of Minnesota Duluth, 2009 A Dissertation Submitted to the Graduate Faculty of the University of North Dakota in partial fulfillment of the requirements for the degree of Doctor of Philosophy Grand Forks, North Dakota August 2015 PERMISSION Title Tracking Star Formation in Dwarf Cluster Galaxies Department Physics and Astrophysics Degree Doctor of Philosophy In presenting this dissertation in partial fulfillment of the requirements for a graduate degree from the University of North Dakota, I agree that the library of this University shall make it freely available for inspection. I further agree that permission for extensive copying for scholarly purposes may be granted by the professor who supervised my dissertation work or, in their absence, by the chairperson of the department or the dean of the School of Graduate Studies. It is understood that any copying or publication or other use of this dissertation or part thereof for financial gain shall not be allowed without my written permission.
    [Show full text]
  • Unveiling the Composition of Radio Plasma Bubbles in Galaxy Clusters with the Sunyaev-Zel’Dovich Effect
    A&A 430, 799–810 (2005) Astronomy DOI: 10.1051/0004-6361:20041576 & c ESO 2005 Astrophysics Unveiling the composition of radio plasma bubbles in galaxy clusters with the Sunyaev-Zel’dovich effect C. Pfrommer1,T.A.Enßlin1, and C. L. Sarazin2 1 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, PO Box 1317, 85741 Garching, Germany e-mail: [email protected] 2 Department of Astronomy, University of Virginia, PO Box 3818, Charlottesville, VA 22903-0818, USA Received 2 July 2004 / Accepted 23 August 2004 Abstract. The Chandra X-ray Observatory is finding a large number of cavities in the X-ray emitting intra-cluster medium which often coincide with the lobes of the central radio galaxy. We propose high-resolution Sunyaev-Zel’dovich (SZ) observa- tions to infer the still unknown dynamically dominant component of the radio plasma bubbles. This work calculates the thermal and relativistic SZ emission of different compositions of these plasma bubbles while simultaneously allowing for the cluster’s kinetic SZ effect. As examples, we present simulations of an Atacama Large Millimeter Array (ALMA) observation and of a Green Bank Telescope (GBT) observation of the cores of the Perseus cluster and Abell 2052. We predict a 5σ detection of the southern radio bubble of Perseus in a few hours with the GBT and ALMA while assuming a relativistic electron population within the bubble. In Abell 2052, a similar detection would require a few tens of hours with either telescope, the longer ex- posures mainly being the result of the higher redshift and the lower central temperature of this cluster.
    [Show full text]
  • The Galaxy Luminosity Function of the Abell 496 Cluster and Its Spatial Variations
    A&A 479, 335–346 (2008) Astronomy DOI: 10.1051/0004-6361:20077723 & c ESO 2008 Astrophysics The galaxy luminosity function of the Abell 496 cluster and its spatial variations G. Boué1,C.Adami2,F.Durret1,3,G.A.Mamon1,4, and V. Cayatte5 1 Institut d’Astrophysique de Paris (UMR 7095: CNRS & Université Pierre et Marie Curie), 98bis Bd Arago, 75014 Paris, France e-mail: [email protected] 2 LAM, Traverse du Siphon, 13012 Marseille, France 3 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France 4 Observatoire de Paris, GEPI (UMR 8111: CNRS & Université Denis Diderot), 61 Av. de l’Observatoire, 75014 Paris, France 5 Observatoire de Paris, section Meudon, LUTH, CNRS-UMR 8102, Université Paris 7, 5 Pl. Janssen, 92195 Meudon, France Received 26 April 2007 / Accepted 27 November 2007 ABSTRACT Context. The faint end slopes of galaxy luminosity functions (LFs) in clusters of galaxies have been observed in some cases to vary with clustercentric distance and should be influenced by the physical processes (mergers, tides) affecting cluster galaxies. However, there is a wide disagreement on the values of the faint end LF slopes, ranging from −1to−2.3 in the magnitude range −18 < Mr < −14. Aims. We investigate the LF in the very relaxed cluster Abell 496. Methods. Our analysis is based on deep images obtained at CFHT with MegaPrime/MegaCam in four bands (u∗gri) covering a 1 × 1deg2 region, which is centred on the cluster Abell 496 and extends to near its virial radius. The LFs are estimated by statistically subtracting a reference field taken as the mean of the 4 Deep fields of the CFHTLS survey.
    [Show full text]
  • Unraveling the Properties of the Brightest Cluster Galaxies Using Multi-Wavelength Data
    Introduction Sample and data Measurements Results Summary Unraveling the properties of the brightest cluster galaxies using multi-wavelength data Ilani Loubser [email protected] Ilani Loubser Unraveling the properties of the brightest cluster galaxies Introduction Sample and data Measurements Results Summary Introduction Ilani Loubser Unraveling the properties of the brightest cluster galaxies Introduction Sample and data Measurements Results Summary Introduction Perseus (NGC1275) Ilani Loubser Unraveling the properties of the brightest cluster galaxies Introduction Sample and data Measurements Results Summary Introduction Nearby BCGs exhibit diverse morphologies, stellar populations, and star formation histories { important for understanding: Mass build-up and evolution of BCGs and host clusters Explain the physical mechanisms behind heating and cooling cycle in cool-core clusters Ilani Loubser Unraveling the properties of the brightest cluster galaxies Introduction Sample and data Measurements Results Summary Sample Sample 14 MENeaCS (0:05 < z < 0:15) Gemini GMOS & CFHT MegaCam 18 CCCP (0:15 < z < 0:30) Gemini GMOS & CFHT MegaCam 4 CLASH (z ∼ 0:35) SALT RSS & HST 36 BCGs between 0:05 < z < 0:35 Ilani Loubser Unraveling the properties of the brightest cluster galaxies Introduction Sample and data Measurements Results Summary Sample Optical spectra Imaging X-ray/Cluster redshift stellar light profiles offset from X-ray peak rotation core size and inner slope centroid shift variance central vel dispersion isophote and core shapes halo mass vel dispersion slopes stellar circular vel profiles cluster vel dispersion young populations and ages colour gradients central entropy age/metallicity gradients multiple nuclei cooling time stellar M/L ratios brightness ellipticity Hoekstra et al.
    [Show full text]
  • Active Galactic Nucleus Feedback in Clusters of Galaxies
    Active galactic nucleus feedback in clusters of galaxies Elizabeth L. Blantona,1, T. E. Clarkeb, Craig L. Sarazinc, Scott W. Randalld, and Brian R. McNamarad,e aInstitute for Astrophysical Research and Astronomy Department, Boston University, 725 Commonwealth Avenue, Boston, MA 02215; bNaval Research Laboratory, 455 Overlook Avenue SW, Washington, DC 20375; cDepartment of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325; dHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; eDepartment of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 2G1, Canada; and Perimeter Institute for Theoretical Physics, 31 Caroline Street, North Waterloo, Ontario N2L 2Y5, Canada Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved February 22, 2010 (received for review December 3, 2009) Observations made during the last ten years with the Chandra there is little cooling. This is seen in the temperature profiles as X-ray Observatory have shed much light on the cooling gas in well as high resolution spectroscopy. An important early result the centers of clusters of galaxies and the role of active galactic from XMM-Newton high resolution spectra from cooling flows nucleus (AGN) heating. Cooling of the hot intracluster medium was that the emission lines from cool gas were not present at in cluster centers can feed the supermassive black holes found the expected levels, and the spectra were well-fitted by a cooling in the nuclei of the dominant cluster galaxies leading to AGN out- flow model with a low temperature cutoff (7, 8). This cutoff is bursts which can reheat the gas, suppressing cooling and large typically one-half to one-third of the average cluster temperature, amounts of star formation.
    [Show full text]
  • Ω Cen 127 M96 = NGC 3377 116 582
    INDEX OF OBJECTS Palomar 3 95 Palomar 4 95 Palomar 5 95 CLUSTERS OF GALAXIES Palomar 14 95 85 203 Abell Palomar 15 95 Abell 262 203 47 Tue 155 Abell 1060 203 Abell 1367 181 GALAXIES Abell 1795 189. 203 A0136-080 5, 315 Abell 2029 203 AM2020-5050 315 Abell 2199 203 Arp 220 432 Abell 2256 169-170 Abell 2319 203 Carina 145-147, 158-159, 247-249 Abell 2626 203 Cygnus A 208 AWM 4 167. 169 DDO 127 139, 141-142, 147-148, 152 AWM 7 169. 208 DDO 154 141 Cancer 59 Draco 5, 144-147, 149, 153-155, Canes-Venatici/Ursa Major complex 157-159, 247-249 115 ESO 415-G26 315 Centaurus 110, 168 ESO 474-G20 314 Coma 1, 15, 87, 97, 101, 112, 115, Fornax 5, 144-147, 158-159, 249, 165, 169, 181, 186-187, 283, 351 403, 408 Galaxy, The (Milky Way) 2, 16-20, DC1842-63 59-60 23-25, 33, 36, 39-41, 43-44, 46- Hercules 59 47, 49-50, 87-88, 95, 111, 119, Hickson 88 51-52 122, 127-130, 136, 197, 207, Local Group 43, 50, 100, 115, 250, 213, 237, 248-250, 289, 294-295, 253, 322, 331, 350, 362, 402, 297-298, 301, 322, 327, 331, 435, 439, 539, 541 356, 391, 397-398, 407, 411-413, MKW 4 169 433. 436, 473, 494, 496, 499, MKW 9 169 519, 525, 530-531, 535-536, 540, M96 Group 116 542, 551, 553, 555, 557 Pegasus I 59, 167 Hickson 88a 51-52 Perseus 15, 105, 186, 189, 197, IC 724 59 206-207, 313 IC 2233 416, 418 Sculptor Group 132 Magellanic Clouds 408 Virgo 97-104, 107-108, 110, 115, M31 49-50, 86-87, 127-128, 146, 162, 168, 175, 203, 216, 248, 249-250, 275, 297, 331, 334, 257, 322, 332, 350.
    [Show full text]
  • Ellipticals in the CPG and in the Sample of Sramek (1975) 44
    RADIO AND OPTICAL PROPERTIES OF DOUBLE GALAXIES Item Type text; Dissertation-Reproduction (electronic) Authors Stocke, John T. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 27/09/2021 19:19:08 Link to Item http://hdl.handle.net/10150/289608 INFORMATION TO USERS This material was produced from a microfilm copy of the original document. While the most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the original submitted. The following explanation of techniques is provided to help you understand markings or patterns which may appear on this reproduction. 1. The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting thru an image and duplicating adjacent pages to insure you complete continuity. 2. When an image on the film is obliterated with a large round black mark, it is an indication that the photographer suspected that the copy may have moved during exposure and thus cause a blurred image. You will find a good image of the page in the adjacent frame. 3. When a map, drawing or chart, etc., was part of the material being photographed the photographer followed a definite method in "sectioning" the material.
    [Show full text]
  • 1978Apj. . .226. .559B the Astrophysical Journal, 226:559-565, 1978 December 1 © 1978. the American Astronomical Society. All R
    .559B .226. The Astrophysical Journal, 226:559-565, 1978 December 1 . © 1978. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1978ApJ. THE EVOLUTION OF GALAXIES IN CLUSTERS. II. THE GALAXY CONTENT OF NEARBY CLUSTERS Harvey Butcher Kitt Peak National Observatory* AND Augustus Oemler, Jr. Yale University Observatory Received 1978 May 4; accepted 1978 June 6 ABSTRACT We have studied the structure and galaxy content of most nearby rich clusters of galaxies, using new data as well as those already in the literature. Devising a simple numerical indicator of the central concentration of clusters, we find it to be strongly correlated with the spiral galaxy content of the clusters. Only the least-concentrated clusters show an appreciable content of spiral galaxies, in strong contrast to the distant clusters described in our previous paper. //' we are observing nearby clusters at every stage of dynamical evolution, these results strongly support the hypothesis of an efficient stripping mechanism in collapsed clusters. Subject headings: galaxies: clusters of — galaxies: evolution — galaxies: structure I. INTRODUCTION mine the galaxy content of these same clusters, and in It has been known for many years (Abell 1965; § IV we discuss the significance of our findings. Oemler 1974) that the structure of clusters of galaxies is correlated with their galaxy content. Irregular, II. CLUSTER STRUCTURE formless clusters have a galaxy population similar to that of the “field,” while regular, centrally concen- We wish to demonstrate that the galaxy content of a trated clusters contain, in their cores, only elliptical cluster depends on whether the cluster is irregular and and SO galaxies.
    [Show full text]
  • Determination of the Dark Matter Profile of Abell 2199 from Integrated Starlight
    Accepted for Publication in the Astrophysical Journal A Preprint typeset using L TEX style emulateapj v. 14/09/00 DETERMINATION OF THE DARK MATTER PROFILE OF ABELL 2199 FROM INTEGRATED STARLIGHT1 Daniel D. Kelson2,3, Ann I. Zabludoff4, K.A. Williams5, S.C. Trager6,7, J.S. Mulchaey6, and Michael Bolte5 Accepted for Publication in the Astrophysical Journal ABSTRACT We have obtained deep, long-slit spectroscopy along the major axis of NGC 6166, the cD galaxy in the cluster Abell 2199, in order to measure the kinematics of intracluster starlight at large radii. The velocity dispersion initially decreases from the central value of 300 kms−1, to 200 kms−1 within a few −1 −1 −1 kpc, and then steadily rises to 660 kms at a radius of 60 kpc (H0=75 kms Mpc ,Ωm=0.3, ΩΛ=0.7), −1 nearly reaching the velocity dispersion of the cluster (σA2199 = 775 50 kms ). These data suggest that the stars in the halo of the cD trace the potential of the cluster± and that the kinematics of these intracluster stars can be used to constrain the mass profile of the cluster. In addition, we find evidence for systematic rotation (V/σ 0.3) in the intracluster stars beyond 20 kpc. Such rotation is not seen in the kinematics of the cluster≈ members. The surface brightness and velocity dispersion profiles can be fit using a single component mass model only by making unphysical assumptions about the level of anisotropy for both the stars in the cD galaxy and for the kinematics of the galaxies in the cluster.
    [Show full text]