The Dynamical Evolution of Stellar Black Holes in Globular Clusters

Dec 8, 2014 - Way-like GCs and address the question of retention of BHs in clusters and ..... (IMF) of Kroupa (2001), which is a broken power-law of t...

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Dec 8, 2014 - Department of Electrical Engineering and Computer Science, Northwestern University, Evanston,. IL, USA .... The answers to these questions can help to constrain the initial populations of BHs and BH kicks, ... N ∼ 105 due to the poor

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Nov 28, 2012 - star clusters, it is still unclear how many of those will be retained upon formation, and how many will be ejected through subsequent dynamical interactions. No such black holes have been found in any Milky ... BHs have already been fo

Jan 14, 2013 - e-mail: [email protected] 2 Gemini Observatory, Northern Operations Center, 670 N. ... velocity dispersion of its host galaxy (e.g.. Ferrarese & Merritt 2000; Gebhardt et al. 2000a; Gültekin et al. ... dates for hosting an intermediat

Nov 20, 2016 - The idea of black holes which might be situated at the centers of globular clusters has been seriously ... call & Ostriker 1975, Silk & Arons 1975, Newell, Da Costa &. Grindlay 1976). Ground based studies on ... epoch have to lead to t

e-mail: [email protected] Summary. Recent images taken ... shown here that a large fraction of the individual star clusters merge within a few tens to a hundred Myr. Bound stellar ..... The softening length is 1.5 pc in the units used here

Aug 17, 2007 - erties of their hosting galaxy have been deduced (see. Ferrarese & Ford ...... eds, Resolved Stellar Populations, ASP Conf. Se- ries, in press.

Oct 7, 2009 - 2NASA Goddard Space Flight Center, Exploration of the Universe Division, Code 667,. Greenbelt, MD 20771, USA ... stars have also been thought to have all been born at the same instant, from a cloud ... latter having been known since muc

(MN LATEX style file v1.4). Dynamical ... if the initial scale length of the GCs system is about twice as large as the effective radius of NGC ... Forbes 2002). In the case of cD and central cluster galax- ies a variety of processes may have contribu

Feb 1, 2008 - ties in excess of ~ 1039 erg s−1 (e.g., Fabbiano 1989; Fab- biano, Schweizer, & Mackie 1997; Colbert & ..... A hard binary is defined to have an orbital binding energy greater than the kinetic energy of a typical field star. As- .....

Oct 2, 2012 - 4School of Physics and Astronomy, University of Southampton, Highfield SO17 IBJ, UK. 5International ..... Supplementary Information is linked to the online version of the paper at .... do not account for the lack

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Jun 6, 2007 - curves that account for the performance of the system from optics to electronics, thereby allowing accurate ... horizontal branch model files and outlines the use of computer codes distributed with the models. 2. .... almost universal c

Jun 13, 2014 - Globular clusters have long been regarded as near-perfect laboratories for studies of stellar physics and stellar dynamics. Some reasons (and complications) are: • they are isolated in space (but not all clusters are found in galacti

Mar 28, 2012 - 5 University of Utah, Salt Lake City, UT 84112. 6 Department of Physics, University of Alberta, 4-183 CCIS,. Edmonton, AB, T6G 2E1, Canada from the ... ray binaries AC 211 and M15 X-2 (Johnston et al. 1991;. Miller-Jones et al. 2011) a

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May 11, 2016 - Miller & Hamilton. 2002), and they are approximately the same age as their host galaxy, suggesting that the IMBHs required for the growth of SMBHs in the early Universe might have ... (2003) in their analysis of the kinematic profile o

Jun 3, 2013 - ... 85748 Garching, Germany; [email protected] .... From the IFU data, a velocity dispersion profile was ob- ... duction and retention of stellar remnants (with retention fractions ... blue (IMBH, slope of β = 0.75) lines a

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these young stars in the immediate vicinity of the SBH poses a problem known as the youth .... Here we only explain in detail the additions to our code for this paper. ... For our models, tcoll within this radius is ∼ 104 yr, i.e., all stars restri

Jan 27, 2015 - email: [email protected] email: [email protected] 2 Sapienza-Universitá di Roma, P.le A. Moro 5, I-00165 Rome, Italy. 3 Universitá di Tor Vergata, Via O. Raimondo 18, I-00173 Rome, Italy. Abstract. Almost all galaxies along

Oct 20, 2009 - with sufficient BH-retention is likely to have at least one BH- pair that can merge within the cluster within a time-span of a few Gyr. Each of these clusters also typically eject a few. BH binaries that can merge within a Hubble time.

shows a Hβ –[MgFe] diagram for the two globulars W3 and W6 (data points), from which [Z]=0.00 ± 0.08 for W3 and ..... of GCs formed at various epochs after the Big Bang are plotted as a function of redshift z for the currently .... 1998, AJ, 115,