Two kinds of stellar collapse

Katz, J. I.

doi:10.1038/253698a0

Cited by 214 publications

(160 citation statements)

References 10 publications

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“…It had been recognized since the early days of X-ray astronomy that GCs are highly efficient in producing low-mass X-ray binaries ( LMXBs;Clark 1975;Katz 1975). Thanks to the excellent imaging capabilities of Chandra and HST, tremendous progress has been made in recent years on the connection between LMXBs and GCs in external galaxies as distant as $30 Mpc.…”

Section: Extragalactic Globular Clustersmentioning

confidence: 99%

The ACS Fornax Cluster Survey. I. Introduction to the Survey and Data Reduction Procedures

Jordán¹,

Blakeslee²,

Côté³

et al. 2007

ASTROPHYS J SUPPL S

151

146

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The Fornax Cluster is a conspicuous cluster of galaxies in the southern hemisphere and the second largest collection of early-type galaxies within P20 Mpc after the Virgo Cluster. In this paper, we present a brief introduction to the ACS Fornax Cluster Survey-a program to image, in the F475W (g 475 ) and F850LP (z 850 ) bandpasses, 43 earlytype galaxies in Fornax using the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. Combined with a companion survey of Virgo, the ACS Virgo Cluster Survey, this represents the most comprehensive imaging survey to date of early-type galaxies in cluster environments in terms of depth, spatial resolution, sample size, and homogeneity. We describe the selection of the program galaxies, their basic properties, and the main science objectives of the survey, which include the measurement of luminosities, colors, and structural parameters for globular clusters associated with these galaxies, an analysis of their isophotal properties and surface brightness profiles, and an accurate calibration of the surface brightness fluctuation distance indicator. Finally, we discuss the data reduction procedures adopted for the survey.

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Section: Extragalactic Globular Clustersmentioning

confidence: 99%

The ACS Fornax Cluster Survey. I. Introduction to the Survey and Data Reduction Procedures

Jordán¹,

Blakeslee²,

Côté³

et al. 2007

ASTROPHYS J SUPPL S

151

146

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“…Suggestions have been made (Clark 1975;Katz 1975;Verbunt & Hut 1987) that dense stellar environments and, in particular, globular clusters are very efficient in producing LMXBs. The hypothesis was put forward that most, if not all, of the systems were formed as the result of dynamical interactions in clusters and then released from the clusters to populate the field (e.g., Grindlay 1984;White, Sarazin, & Kulkarni 2002).…”

Section: Predicted Number Of Systems In the Galactic Fieldmentioning

confidence: 99%

Galactic Populations of Ultracompact Binaries

Belczyński

Taam

2004

ApJ

110

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Recent RXTE and Chandra discoveries of low-mass X-ray binaries with ultrashort orbital periods have initiated theoretical work on the origins of these peculiar systems. Using the StarTrack population synthesis code, we analyze the formation and evolution of X-ray ultracompact binaries (UCBs) in the Galactic field. The relative number of UCBs with a neutron star or a black hole accretor populating our Galaxy is predicted. Our results demonstrate that standard evolutionary scenarios involving primordial binaries can be sufficient to produce the UCBs in the Galactic field without requiring additional processes associated with the dense stellar environments in the cores of globular clusters. In contrast to previous studies, we find that the majority of the immediate progenitors of these systems consist of a hydrogen-exhausted donor with an ONeMg white dwarf. The evolution of these systems leads to the accretion-induced collapse of the white dwarf to a neutron star, which can play an important role in the formation of a majority of Galactic UCBs. We predict that with an increase in the number of X-rayactive UCBs hosting neutron stars by an order of magnitude, a system with a black hole accretor may be found.

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“…In the Milky Way, it was realized soon after the discovery of X-ray emission from a handful of Galactic globular clusters (GCs; Giacconi et al 1974;Forman et al 1978) that the number of X-ray sources per unit mass is several hundred times higher in GCs than in the halo field ( Katz 1975;Clark 1975). The population of X-ray point sources associated with GCs was later found to be a mixture of dim (L X P 10 34:5 ergs s À1 ) and bright (10 36 ergs s À1 P L X P 10 38 ergs s À1 ) sources ( Hertz & Grindlay 1983).…”

Section: Introductionmentioning

confidence: 99%

The ACS Virgo Cluster Survey. III.ChandraandHubble Space TelescopeObservations of Low‐Mass X‐Ray Binaries and Globular Clusters in M87

Jordán

Côté

Ferrarese

et al. 2004

ApJ

131

150

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The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries ( LMXBs) in M87, the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images-with a total exposure time of 154 ks-are the deepest X-ray observations yet obtained of M87. We identify 174 X-ray point sources, of which $150 are likely LMXBs. This LMXB catalog is combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST ) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in our catalog, f X ¼ 3:6% AE 0:5% contain an LMXB. Dividing the globular cluster sample by metallicity, we find that the metal-rich clusters are 3 AE 1 times more likely to harbor an LMXB than their metalpoor counterparts. In agreement with previous findings for other galaxies based on smaller LMXB samples, we find the efficiency of LMXB formation to scale with both cluster metallicity Z and luminosity, in the sense that brighter, more metal-rich clusters are more likely to contain an LMXB. For the first time, however, we are able to demonstrate that the probability p X that a given cluster will contain an LMXB depends sensitively on the dynamical properties of the host cluster. Specifically, we use the HST images to measure the half-light radius, concentration index, and central density 0 for each globular and define a parameter À, which is related to the tidal capture and binary-neutron star exchange rate. Our preferred form for p X is then p X / À À0:42AE0:11 0 (Z=Z ) 0:33AE0:1 . We argue that if the form of p X is determined by dynamical processes, then the observed metallicity dependence is a consequence of an increased number of neutron stars per unit mass in metal-rich globular clusters. Finally, we present a critical examination of the LMXB luminosity function in M87 and reexamine the published LMXB luminosity functions for M49 and NGC 4697. We find no compelling evidence for a break in the luminosity distribution of resolved X-ray point sources in any of these galaxies. Instead, the LMXB luminosity function in all three galaxies is well described by a power law with an upper cutoff at L X $10 39 ergs s À1 .

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Two kinds of stellar collapse

Cited by 214 publications

References 10 publications

The ACS Fornax Cluster Survey. I. Introduction to the Survey and Data Reduction Procedures

The ACS Fornax Cluster Survey. I. Introduction to the Survey and Data Reduction Procedures

Galactic Populations of Ultracompact Binaries

The ACS Virgo Cluster Survey. III.ChandraandHubble Space TelescopeObservations of Low‐Mass X‐Ray Binaries and Globular Clusters in M87

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