DOCSLIB.ORG

Stellar Mass Function in the Field

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Stellar Mass Function in the Field Professor David Carter (PI) Liverpool John Moores University UK Dr Habib G. Khosroshahi Liverpool John Moores University UK Mr Mustapha Mouhcine Liverpool John Moores University UK Ms Susan M. Percival Liverpool John Moores University UK Dr Harry C. Ferguson (USA PI) Space Telescope Science Institute USA/MD Dr Paul Goudfrooij Space Telescope Science Institute USA/MD Dr Terry Bridges Queen's University Canada Dr Thomas H. Puzia Dominion Astrophysical Observatory Canada Dr Carlos del Burgo Dublin Institute For Advanced Studies Ireland Dr Bryan Miller Gemini Observatory, Southern Operations Chile Dr Bianca Poggianti INAF - Osservatorio Astronomico di Padova Italy Dr Alfonso Aguerri Instituto de Astrofisica de Canarias Spain Dr Marc Balcells Instituto de Astrofisica de Canarias Spain Mr Derek Hammer Johns Hopkins University USA/MD Dr Reynier F. Peletier Kapteyn Astronomical Institute Netherlands Prof. Edwin Valentijn Kapteyn Astronomical Institute Netherlands Dr Gijs Verdoes Kleijn Kapteyn Astronomical Institute Netherlands Dr Peter Erwin Max-Planck-Insitute for Extraterrestrial Physics Germany Dr Ann Hornschemeier NASA Goddard Space Flight Center USA/MD Dr Yutaka Komiyama National Astronomical Observatory of Japan Japan Dr Masafumi Yagi National Astronomical Observatory of Japan Japan Dr Jennifer Lotz National Optical Astronomy Observatories, AURA USA/AZ National Radio Astronomy Observatory, Dr Neal A. Miller USA/VA and Johns Hopkins University Dr Eric W. Peng Peking University China Dr Dan Batcheldor Rochester Institute of Technology USA/NY Prof. David Merritt Rochester Institute of Technology USA/NY Dr Ronald O. Marzke San Francisco State University USA/CA Dr Alister W. Graham Swinburne University of Technology Australia Dr Helmut Jerjen The Australian National University Australia Dr Avon P. Huxor University of Bristol UK Prof. Steve Phillipps University of Bristol UK Mr James Price University of Bristol UK Prof. Bahram Mobasher University of California - Riverside USA/CA Dr Neil Trentham University of Cambridge UK Dr John Lucey University of Durham UK Prof. Ray M. Sharples University of Durham UK Dr Russell Smith University of Durham UK Dr Rafael Guzman University of Florida USA/FL Dr Carlos Hoyos University of Florida USA/FL Dr Kristin Chiboucas University of Hawaii USA/HI Dr R. Brent Tully University of Hawaii USA/HI Prof. Shardha Jogee University of Texas at Austin USA/TX Prof. Sadanori Okamura University of Tokyo, Department of Astronomy Japan Dr Jonathan Davies University of Wales, College of Cardiff UK Dr Michael J. Hudson University of Waterloo Canada HST/ACS Coma Cluster Treasury Survey Supporting Observations MMT Hectospec KPNO 4m Mosaic Keck DEIMOS/LRIS CFHT Megacam CFHT WIRCam UKIRT Subaru SuprimeCam Subaru MOIRCS XMM/EPIC GALEX Spitzer/IRAC VLA Why the Coma Cluster? Why the Coma Cluster? The ACS Fornax Cluster Survey Why the Coma Cluster? Local Coma Group The ACS Fornax Cluster Survey 12 13 14 15 Log Halo Mass (solar masses) Why the Coma Cluster? Local Coma Group The ACS Fornax Cluster Survey 12 13 14 15 Log Halo Mass (solar masses) Luminosity Functions: The Theoretical Problem Rees & Ostriker 1977 Schechter 1976 White & Rees 1978 Felten 1977 Davis et al. 1985 Huchra et al. 1982 White & Frenk 1991 Efstathiou, Ellis & Peterson 1988 CDM Halo Mass SpectrumSNe Mergers Photoionization tcool > t0 AGN Luminosity Functions: The Observational Problem Imaging Too much background contamination Luminosity Functions: The Observational Problem Imaging Too much background contamination 105 104 -2 3 deg 10 -1 102 N(r) mag 101 100 12 14 16 18 20 22 24 r Luminosity Functions: The Observational Problem Imaging Too much background contamination Popesso et al. 2006 Luminosity Functions: The Observational Problem Imaging Too much background contamination 100 ) r 10 N(M Coma (Secker et al. 1996) Virgo (Trentham & Hodgkin 2002) 1 -24 -22 -20 -18 -16 -14 -12 Mr Luminosity Functions: The Observational Problem Imaging Too much background contamination 100 Coma Jenkins et al. 2007 ) r 10 N(M Coma (Secker et al. 1996) Virgo (Trentham & Hodgkin 2002) 1 -24 -22 -20 -18 -16 -14 -12 Mr Luminosity Functions: The Observational Problem Imaging Spectroscopy Too much background contamination Not enough photons 100 Coma Jenkins et al. 2007 ) r 10 N(M Coma (Secker et al. 1996) Virgo (Trentham & Hodgkin 2002) 1 -24 -22 -20 -18 -16 -14 -12 Mr Luminosity Functions: The Observational Problem Imaging Spectroscopy Too much background contamination Not enough photons Christlein & 100 Coma Zabludoff 2003 JenkinsPopesso et al. et2007 al. 2006 ) r 10 N(M Coma (Secker et al. 1996) Virgo (Trentham & Hodgkin 2002) 1 -24 -22 -20 -18 -16 -14 -12 Mr An intermediate approach Surface brightness selection Tully et al. 2002 5 Dwarf/giant ratio increases with host 4 Coma halo mass 3 Virgo gal N 10 2 Log Ursa Major 1 Interpreted as evidence that global reionization 0 suppresses dwarf formation Local Goup in low-mass group halos -1 -24 -22 -20 -18 -16 -14 -12 Mr Surface Brightness Selection dE, dSph surface brightness -0.2 profiles from the literature -0.4 placed at Ursa Major and observed in 0.9” seeing -0.6 Better completeness Text intermediate surface-brightness -0.8 fail the criterion but are -1.0 straightforward to identify in other ways -1.2 the lowest surface-brightness -1.4 Inner Concentration Parameter galaxies are nearly always More efficient -1.6 members -20 -18 -16 -14 -12 -10 -8 Mr A Spectroscopic Survey of the Coma Cluster: From the Core to the Virial Radius 6259 spectra with MMT Hectospec 1392 members (524 newly detected) 300 1.5” fibers 5 minute configuration time Fabricant et al. 2005 RM, Ann Hornschemeier, Russell Smith Terry Bridges, Mike Hudson, Neal Miller, John Lucey 10 nights awarded through NOAO/TSIP N Hectospec Survey 2007-9 Faint end of the luminosity function to M* + 6.5 from the core to the E infall region Line index analysis of stellar populations to M* + 4.5 Detection and characterization of ultracompact dwarfs 3○ Coma Cluster Kinematics MMT 6000 Hectospec 4000 2000 new cluster members 0 -2000 -4000 cz - 6917 km/s (Colless & Dunn 1996) -6000 0 1 2 3 Projected distance from Coma X-ray center (Mpc) Coma Cluster Kinematics 6000 MMT Hectospec 4000 2000 0 new cluster members r > 18 -2000 -4000 cz - 6917 km/s (Colless & Dunn 1996) -6000 0 1 2 3 Projected distance from Coma X-ray center (Mpc) Coma Cluster Kinematics MMT 6000 Hectospec 4000 2000 new cluster members 0 r > 19.5 -2000 -4000 cz - 6917 km/s (Colless & Dunn 1996) -6000 0 1 2 3 Projected distance from Coma X-ray center (Mpc) Radial Distribution of Cluster Members Differential Cumulative 120 1500 100 80 1000 60 40 500 Number of galaxies Number of galaxies 20 0 0 0.0 0.5 1.0 1.5 2.0 2.5 3.0 0.0 0.5 1.0 1.5 2.0 2.5 3.0 Projected distance from cluster center (Mpc) Projected distance from cluster center (Mpc) Spectroscopically Confirmed Members: Core + Infall Regions 50 40 30 20 Number of galaxies per 0.15 mag 10 0 -22 -20 -18 -16 -14 Absolute Magnitude (r) Number of clean sources in Megacam i-band image 105 Photometric 104 Completeness 103 2 Number 10 101 selected by SDSS r-band 100 Petrosian magnitude 12 14 16 18 20 22 Petrosian magnitude (r) r < 20.5 Fraction of Megacam sources detected by SDSS 1.0 0.8 and SDSS r-band 0.6 0.4 3” fiber magnitude Completeness 0.2 r < 22.5 0.0 12 14 16 18 20 22 Petrosian magnitude (r) no color cut in 2007A 24 g-r < 1.2 in 2008A, 2009A 22 20 completeness determined using 18 deeper CFHT/Megacam imaging 16 3 arcsec aperture magnitude (r) 12 14 16 18 20 22 over 3x3 degree field obtained in Petrosian magnitude (r) 2008A Simulated SDSS photometry of local dEs/dSphs translated to 100Mpc Local Group Sculptor Group 26 M81 Group Cen A Virgo 24 22 Published Sersic fits 3" aperture magnitude (r) 20 Binggeli & Jerjen 1998 18 Jerjen, Freeman & Binggeli 2000 16 18 20 22 24 26 Caldwell et al. 1998 Total magnitude (r) Spectroscopic completeness Hectospec Core Hectospec NE fiber assignment in dense 1.0 1.0 regions dominates overall 0.8 0.8 completeness 0.6 0.6 0.4 0.4 Completeness Completeness 0.2 0.2 0.0 0.0 15 16 17 18 19 20 21 15 16 17 18 19 20 21 spectroscopic redshifts r-band Petrosian magnitude r-band Petrosian magnitude Hectospec W XMM Footprint (SW) obtained in all populated 1.0 1.0 magnitude/surface- 0.8 0.8 brightness bins to r=20.5 0.6 0.6 0.4 0.4 Completeness Completeness In fully observed regions, 0.2 0.2 80% complete at r=20 0.0 0.0 15 16 17 18 19 20 21 15 16 17 18 19 20 21 50% complete at r=20.5 r-band Petrosian magnitude r-band Petrosian magnitude Overall Luminosity Functions Hectospec Core Hectospec NE 100.0 100.0 Corrected for photometric and 10.0 10.0 spectroscopic incompleteness in 1.0 1.0 0.4 magnitude bins in Number per 0.4 mag bin Number per 0.4 mag bin Petrosian magnitude 0.1 0.1 12 14 16 18 20 12 14 16 18 20 and fiber magnitude r-band Petrosian magnitude r-band Petrosian magnitude Hectospec W XMM Footprint (SW) 100.0 100.0 10.0 10.0 1.0 1.0 Posterior probability Number per 0.4 mag bin Number per 0.4 mag bin 0.1 0.1 12 14 16 18 20 12 14 16 18 20 r-band Petrosian magnitude r-band Petrosian magnitude The faint-end upturn in Coma The Coma LF turns up at Mr ~ -16.5 Popesso et al.
Load more

Recommended publications
  • Mass Deficits, Stalling Radii, and the Merger Histories of Elliptical Galaxies David Merritt Rochester Institute of Technology
    Rochester Institute of Technology RIT Scholar Works Articles 5-22-2006 Mass Deficits, Stalling Radii, and the Merger Histories of Elliptical Galaxies David Merritt Rochester Institute of Technology Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation David Merritt 2006 ApJ 648 976 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. DRAFT VERSION FEBRUARY 5, 2008 Preprint typeset using LATEX style emulateapj v. 10/09/06 MASS DEFICITS, STALLING RADII, AND THE MERGER HISTORIES OF ELLIPTICAL GALAXIES DAVID MERRITT Department of Physics, Rochester Institute of Technology, Rochester, NY 14623 Draft version February 5, 2008 Abstract A binary supermassive black hole leaves an imprint on a galactic nucleus in the form of a “mass deficit,” a decrease in the mass of the nucleus due to ejection of stars by the binary. The magnitude of the mass deficit is in principle related to the galaxy’s merger history, but the relation has never been quantified. Here, high- accuracy N-body simulations are used to calibrate this relation. Mass deficits are shown to be Mde f ≈ 0.5M12, with M12 the total mass of the binary; the coefficient in this relation depends only weakly on M2/M1 or on the galaxy’s pre-existing density profile. Hence, after N mergers, Mde f ≈ 0.5N M• with M• the final (current) black hole mass. When compared with observed mass deficits, this result implies 1 ∼< N ∼< 3, in accord with hierarchical galaxy formation models.
    [Show full text]
  • Central Massive Objects: the Stellar Nuclei – Black Hole Connection
    Astronomical News Report on the ESO Workshop Central Massive Objects: The Stellar Nuclei – Black Hole Connection held at ESO Garching, Germany, 22–25 June 2010 Nadine Neumayer1 Eric Emsellem1 1 ESO An overview of the ESO workshop on black holes and nuclear star clusters is presented. The meeting reviewed the status of our observational and the- oretical understanding of central mas- sive objects, as well as the search for intermediate mass black holes in globu- lar clusters. There will be no published proceedings, but presentations are available at http://www.eso.org/sci/ meetings/cmo2010/program.html. This workshop brought together a broad international audience in the combined fields of galaxy nuclei, nuclear star clus­ ters and supermassive black holes, to confront state­of­the art observations with cutting­edge models. Around a hundred participants from Europe, North and South America, as well as East Asia and Figure 1. Workshop participants assembled outside made up of several populations of stars. Australia gathered for a three­day meet­ ESO Headquarters in Garching. The existence of very young O and WR ing held at ESO Headquarters in Garching, stars in the central few arcseconds Germany (see Figure 1). The sessions around the black hole is puzzling. The were of very high quality, with many very – Are intermediate mass black holes currently favoured solution to this paradox lively, interesting and fruitful discussions. formed in nuclear clusters/globular of youth is in situ star formation in infalling All talks can be found online on the web clusters? gas clouds. This view is also supported page of the workshop1.
    [Show full text]
  • Accretion Onto a Quintessence Contaminated Rotating Black Hole : Violating the Lower Limit for Eta Over S Arxiv:1911.08304V2 [G
    Accretion onto a Quintessence Contaminated Rotating Black Hole : Violating the Lower Limit for Eta over s Ritabrata Biswas 1 Promila Biswas 3 Parthajit Roy 2∗ 1;3 Department of Mathematics, The University of Burdwan Golapbag Academic Complex, City:Burdwan-713104, Dist: Purba Bardhaman, State: West Bengal, India 1e-mail: [email protected] 3e-mail: [email protected] 2Department of Computer Science, The University of Burdwan City:Burdwan-713104, Dist: Purba Bardhaman, State: West Bengal, India e-mail: [email protected] ∗ Abstract Viscous accretion flow around a rotating supermassive black hole sitting in a quintessence tub is studied in this article. To introduce such a dark energy contaminated black hole's gravitational force, a new pseudo-Newtonian potential is used. This pseudo-Newtonian force can be calculated if we know the distance from the black hole's center, spin of the black hole and equation of state of the quintessence inside which the black hole is considered to lie. This force helps us to avoid complicated nonlinearity of general relativistic field equations. Transonic, viscous, continuous and Keplerian flow is assumed to take place. Fluid speed, sonic speed profile and specific angular momentum to Keplerian angular momentum ratio are found out for different values of spin parameter and arXiv:1911.08304v2 [gr-qc] 2 Mar 2021 quintessence parameter. Density variation is built and tallied with observations. Shear viscosity to entropy density ratio is constructed for our model and a comparison with theoretical lower limit is done. Keywords: Accretion Disc, Viscosity, Quintessence, Supermassive Black Holes, Shear Viscosity to entropy ratio PACS: 97.10.Gz; 51.20.+d; 51.30.+i; 95.36.+x; 97.60.25 1 Introduction Since 1998, despite the propositions of different conceptual models, we were not really able to construct a hundred percent correct theoretical support to the observations of late time cosmic acceleration.
    [Show full text]
  • The Star Clusters Young & Old Newsletter
    SCYON The Star Clusters Young & Old Newsletter edited by Holger Baumgardt, Ernst Paunzen and Pavel Kroupa SCYON can be found at URL: http://astro.u-strasbg.fr/scyon SCYONIssueNo.31 11December2006 EDITORIAL Here is the 31st issue of the SCYON newsletter. The current issue contains 35 abstracts, an an- nouncement for a new, parallel N-body code and announcements for conferences in Italy, Germany and Armenia. It also contains job advertisements for postdoctoral and tenure track positions from Rochester Institute of Technology. We wish everybody a merry holiday season and a happy new year 2007 and thank those who sent us their contributions. Holger Baumgardt, Ernst Paunzen and Pavel Kroupa ................................................... ................................................. CONTENTS Editorial .......................................... ...............................................1 SCYON policy ........................................ ...........................................2 Mirror sites ........................................ ..............................................2 Abstract from/submitted to REFEREED JOURNALS ........... ................................3 1. Star Forming Regions ............................... ........................................3 2. Embedded Clusters................................. .........................................7 3. Galactic Center Clusters........................... ..........................................9 4. Galactic Open Clusters............................. ........................................10
    [Show full text]
  • Galactic Nuclei
    Relativity, torque and spin PROFESSOR DAVID MERRITT DAVID PROFESSOR Professor David Merritt explains his interest in astrophysics and the focus of his current research. Describing the improvements made to the computational algorithms, he highlights the importance of taking into account the effects of relativity in these calculations sometimes reveal modes of behaviour that can be inefficient when applied to galactic are strikingly simple yet totally unexpected. nuclei, because motion is dominated by the presence of the SBH. A star or stellar remnant Your current project focuses on the dynamical will complete millions of orbits around evolution of dense clusters of stars and the SBH before coming close enough to stellar remnants around supermassive black another star to be perturbed, but it is those holes (SBHs) at the centre of galaxies. Why is perturbations that are driving the collective this important? evolution. The computer code needs to follow the unperturbed orbit about the SBH with A star like the Sun would be tidally torn apart extremely high precision: otherwise the effects if it came sufficiently close to an SBH. Partly of the small perturbations will be swamped by because of tidal effects, the only objects numerical errors. that we expect to find very near an SBH are ‘compact remnants’: neutron stars and Why is it important to take into account stellar-mass black holes, the dense leftovers the effects of relativity when simulating the from the evolution of massive stars. These evolution of nuclear star clusters? remnants can interact through ‘gravitational encounters’: close passages that exchange One insight that comes from my group’s research energy and gradually change orbits.
    [Show full text]
  • Extracting the Gravitational Recoil from Black Hole Merger Signals
    Extracting the Gravitational Recoil from Black Hole Merger Signals Vijay Varma,1, ∗ Maximiliano Isi,2, † and Sylvia Biscoveanu2, ‡ 1TAPIR 350-17, California Institute of Technology, 1200 E California Boulevard, Pasadena, CA 91125, USA 2LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA (Dated: March 11, 2020) Gravitational waves carry energy, angular momentum, and linear momentum. In generic binary black hole mergers, the loss of linear momentum imparts a recoil velocity, or a “kick”, to the remnant black hole. We exploit recent advances in gravitational waveform and remnant black hole modeling to extract information about the kick from the gravitational wave signal. Kick measurements such as these are astrophysically valuable, enabling independent constraints on the rate of second-generation mergers. Further, we show that kicks must be factored into future ringdown tests of general relativity with third-generation gravitational wave detectors to avoid systematic biases. We find that, although little information can be gained about the kick for existing gravitational wave events, interesting measurements will soon become possible as detectors improve. We show that, once LIGO and Virgo reach their design sensitivities, we will reliably extract the kick velocity for generically precessing binaries—including the so-called superkicks, reaching up to 5000 km/s. Introduction.— As existing gravitational wave (GW) de- galactic centers. The remnant BH can be significantly tectors, Advanced LIGO [1] and Virgo [2], approach their displaced or ejected [31, 32], impacting the galaxy’s evo- design sensitivities, they continue to open up unprece- lution [33–35], and event rates [36] for the future LISA dented avenues for studying the astrophysics of black mission [37].
    [Show full text]
  • Arxiv:0909.1318V2 [Astro-Ph.GA] 2 Jun 2010 ∼ Hs Tr Aemse F10 Par- 1991 of Al
    DRAFT VERSION NOVEMBER 11, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 THE DISTRIBUTION OF STARS AND STELLAR REMNANTS AT THE GALACTIC CENTER DAVID MERRITT Department of Physics and Center for Computational Relativity and Gravitation, Rochester Institute of Technology, Rochester, NY 14623, USA Draft version November 11, 2018 Abstract Motivated by recent observations that suggest a low density of old stars around the Milky Way supermassive black hole, models for the nuclear star cluster are considered that have not yet reached a steady state under the influence of gravitational encounters. A core of initial radius 1 1.5 pc evolves to a size of approximately 0.5 pc after 10 Gyr, roughly the size of the observed core. The ab−sence of a Bahcall-Wolf cusp is naturally explained in these models, without the need for fine-tuning or implausible initial conditions. In the absence of a cusp, the time for a 10M black hole to spiral in to the Galactic center from an initial distance of 5 pc can be much greater than 10 Gyr.⊙ Assuming that the stellar black holes had the same phase-space distribution initially as the stars, their density after 5 10 Gyr is predicted to rise very steeply going into the stellar core, but could remain substantially below the densities− inferred from steady-state models that include a steep density cusp in the stars. Possible mechanisms for the creation of the parsec-scale initial core include destruction of stars on centrophilic orbits in a pre-existing triaxial nucleus, inhibited star formation near the supermassive black hole, or ejection of stars by a massive binary.
    [Show full text]
  • Dynamics of the Globular Cluster System Associated with M87 (Ngc 4486)
    View metadata,Preprint citation typeset and using similar LAT EpapersX style at emulateapj core.ac.uk brought to you by CORE provided by CERN Document Server DYNAMICS OF THE GLOBULAR CLUSTER SYSTEM ASSOCIATED WITH M87 (NGC 4486). II. ANALYSIS Patrick Cot^ e´1;2;3;4,DeanE.McLaughlin4;5;6, David A. Hanes4;7;8;14, Terry J. Bridges4;8;9;10, Doug Geisler11;12;13, David Merritt2, James E. Hesser14, Gretchen L.H. Harris15, Myung Gyoon Lee16 Accepted for Publication in the Astrophysical Journal 1California Institute of Technology, Mail Stop 105-24, Pasadena, CA 91125, USA 2Department of Physics and Astronomy, Rutgers University, New Brunswick, NJ 08854, USA 3Sherman M. Fairchild Fellow 4Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique of France, and the University of Hawaii. 5Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA 6Hubble Fellow 7Department of Physics, Queen’s University, Kingston, ON K7L 3N6, Canada 8Anglo-Australian Observatory, P.O. Box 296, Epping, NSW, 1710, Australia 9Royal Greenwich Observatory, Madingley Road, Cambridge, CB3 0EZ, UK 10Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK 11Grupo de Astronom´ıa Dpto. de F´ısica, Universidad de Concepci´on, Casilla 160-C, Concepci´on, Chile 12Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by AURA, Inc., under cooperative agreement with the National Science Foundation. 13Visiting Astronomer,
    [Show full text]
  • Consequences of Triaxiality for Gravitational Wave Recoil of Black Holes Alessandro Vicari Universita Di Roma La Sapienza
    Rochester Institute of Technology RIT Scholar Works Articles 6-20-2007 Consequences of Triaxiality for Gravitational Wave Recoil of Black Holes Alessandro Vicari Universita di Roma La Sapienza Roberto Capuzzo-Dolcetta Universita di Roma La Sapienza David Merritt Rochester Institute of Technology Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation Alessandro Vicari et al 2007 ApJ 662 797 https://doi.org/10.1086/518116 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Consequences of Triaxiality for Gravitational Wave Recoil of black holes Alessandro Vicari,1 Roberto Capuzzo-Dolcetta,1 David Merritt2 ABSTRACT Coalescing binary black holes experience a “kick” due to anisotropic emission of gravitational waves with an amplitude as great as 200 km s−1. We examine ∼ the orbital evolution of black holes that have been kicked from the centers of triaxial galaxies. Time scales for orbital decay are generally longer in triaxial galaxies than in equivalent spherical galaxies, since a kicked black hole does not return directly through the dense center where the dynamical friction force is highest. We evaluate this effect by constructing self-consistent triaxial models and integrating the trajectories of massive particles after they are ejected from the center; the dynamical friction force is computed directly from the velocity dispersion tensor of the self-consistent model. We find return times that are several times longer than in a spherical galaxy with the same radial density profile, particularly in galaxy models with dense centers, implying a substantially greater probability of finding an off-center black hole.
    [Show full text]
  • J CQG BK 0214 Highlights-A4-5.Indd
    Classical and Quantum Gravity Highlights of 2012–2013 ISSN 0264-9381 It is my pleasure to present this year’s Classical and Quantum Gravity (CQG) Highlights. The Classicaland Editorial Board has chosen these articles as a selection of the highest quality work published QuantumGravity in CQG in the last year. Congratulations to all the featured authors on their excellent work! Volume 30 Number 24 21 December 2013 An exciting recent development on the journal is the introduction of CQG+. This is a companion An international journal of gravitational physics, cosmology, geometry and field theory website that makes CQG’s high-quality content accessible to all of the gravitational Focus issue Astrophysical black holes Guest Editors: D Merritt and L Rezzolla physics community in a more informal setting. Among other features, the website includes commentaries on recent articles written by authors and referees. You can follow CQG+ at cqgplus.com. We were very happy to see this year’s IOP Gravitational Physics Group’s Thesis Prize, iopscience.org/cqg sponsored by CQG, awarded to Anna Heffernan for her work on the self-force problem in gravitational physics. Anna completed her thesis at University College Dublin under the supervision of Professor Adrian Ottewill. IMPACT FACTOR With CQG’s impact factor at an all-time high of 3.562 there has never been a * better time to publish in the journal. I invite you to submit your next paper to 3.562 CQG and I hope to see it featured on CQG+. *As listed in the 2012 ISI Journal Citation Reports® Clifford M Will Editor-in-Chief Black holes A note on instabilities of extremal black holes under scalar perturbations from afar Black hole uniqueness theorems in TOPICAL Stefanos Aretakis REVIEW higher dimensional spacetimes 2013 Class.
    [Show full text]
  • The ACS Virgo Cluster Survey. IV. Data Reduction Procedures For
    Rochester Institute of Technology RIT Scholar Works Articles 2005 The CA S Virgo Cluster Survey. IV. Data Reduction Procedures for Surface Brightness Fluctuation Measurements with the Advanced Camera for Surveys Simona Mei The Johns Hopkins University John P. Blakeslee The Johns Hopkins University John L. Tonry University of Hawaii, Honolulu Andrés Jordán Rutgers University Eric W. Peng Rutgers University See next page for additional authors Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation Simona Mei et al 2005 ApJS 156 113 https://doi.org/10.1086/426544 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Authors Simona Mei, John P. Blakeslee, John L. Tonry, Andrés Jordán, Eric W. Peng, Patrick Côté, Laura Ferrarese, David Merritt, Miloš Milosavljević, and Michael J. West This article is available at RIT Scholar Works: http://scholarworks.rit.edu/article/1169 The ACS Virgo Cluster Survey IV: Data Reduction Procedures for Surface Brightness Fluctuation Measurements with the Advanced Camera for Surveys Simona Mei1, John P. Blakeslee1, John L. Tonry2, Andr´es Jord´an3,4,5, Eric W. Peng3, Patrick Cˆot´e3, Laura Ferrarese3, David Merritt6, MiloˇsMilosavljevi´c 7,8, and Michael J. West9 ABSTRACT The Advanced Camera for Surveys (ACS) Virgo Cluster Survey is a large program to image 100 early-type Virgo galaxies using the F475W and F850LP bandpasses of the Wide Field Channel of the ACS instrument on the Hubble Space Telescope (HST).
    [Show full text]
  • An ACS Treasury Survey of the Coma Cluster of Galaxies
    239 Hubble Space Telescope Cycle 15 GO Proposal An ACS Treasury Survey of the Coma cluster of galaxies Principal Investigator: Prof. David Carter Institution: Liverpool John Moores University Electronic Mail: [email protected] Scientific Category: UNRESOLVED STELLAR POPULATIONS Scientific Keywords: CLUSTERS OF GALAXIES, DWARF GALAXIES, GALAXY FORMATION AND EVOLUTION, GALAXY MORPHOLOGY AND STRUCTURE, SURVEY Instruments: ACS Proprietary Period: 0 Treasury: Yes Orbit Request Prime Parallel Cycle 15 164 0 Abstract We propose to use the unique spatial resolution of HST and ACS to construct a Treasury imaging survey of the core and infall region of the richest local cluster, Coma. We will observe samples of thousands of galaxies down to magnitude B=27.3 with the aim of studying in detail the dwarf galaxy population which, according to hierarchical models of galaxy formation, are the earliest galaxies to form in the universe. Our initial scientific objectives are: 1) A study of the structure of the dwarf galaxies, including scaling laws, nuclear structure and morphology, to compare with hierarchical and evolutionary models of their formation. 2) A study of the stellar populations from colors and color gradients, and how the internal chemical evolution of galaxies is affected by interaction with the cluster gaseous and galaxy environment. 3) To determine the effect of the cluster environment upon morphological features, disks, bulges and bars, by comparing these structure in the Coma sample with field galaxy samples. 4) Identification of dwarf galaxy samples for further study with the new generation of multi-object and integral- field spectrographs on 8-10 metre class telescopes such as Keck, Subaru, Gemini, and GTC.
    [Show full text]