A thorough study of the intriguing X-ray emission from the Cartwheel ring

Wolter, A.; Trinchieri, G.

doi:10.1051/0004-6361:20047110

Cited by 58 publications

(123 citation statements)

References 33 publications

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“…Only one of four bright emission line regions belonging to its southern spiral arm (Sulentic et al 2001) is detected (source #2), at a luminosity of ∼7 × 10 39 erg s −1 . While high, examples of luminosities such as this are now found in increasing number associated with star-forming regions (Zezas et al 1999;Roberts & Warwick 2000;Fabbiano et al 2001;Zezas & Fabbiano 2002;Wolter & Trinchieri 2004). Several models suggest that interaction/collisions could enhance the star formation activity in galaxies (e.g.…”

Section: X-ray Emission From Sq Member Galaxiesmentioning

confidence: 99%

Stephan's Quintet with XMM-Newton

Trinchieri¹,

Sulentic

Pietsch

et al. 2005

A&A

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100

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The prototype compact group known as Stephan's Quintet (SQ) was observed with XMM-Newton in order to complement the excellent resolution of Chandra with high sensitivity to extended emission. SQ is a dynamic environment whose main effect, at both X-ray and optical wavelengths, appears to be ISM stripping. This is manifested by: 1) secular evolution of morphological types towards earlier types and 2) growth of diffuse emission. Virtually all cold, warm, and hot gas in SQ is found outside of the member galaxies. XMM-Newton offers the opportunity to study the hot gas with unprecedented sensitivity. We find two main components: 1) extended high surface brightness emission from shocked gas associated with an ongoing collision and 2) even more extended and unrelaxed diffuse emission that follows the stripped stellar envelope of the group.

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Section: X-ray Emission From Sq Member Galaxiesmentioning

confidence: 99%

Stephan's Quintet with XMM-Newton

Trinchieri¹,

Sulentic

Pietsch

et al. 2005

A&A

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100

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“…As I've already noted, the two principal lines of thought are: (1) most ULXs are IMBHs; (2) most ULXs are luminous X-ray sources of 'normal' stellar origin and the IMBH explanation should be sought only for the ULXs with L bol > 10 41 erg s -1 (the M82 ULX, Matsumoto et al 2001; the NGC2276 ULX, Davis & Mushotzky 2004; the most luminous ULX in the Cartwheel galaxy, Gao et al 2003, Wolter & Trinchieri 2004; and the variable ULX in NGC7714, .…”

Section: Association With Qsosmentioning

confidence: 99%

X-ray Source Populations in Galaxies

Fabbiano

2003

Chin. J. Astron. Astrophys.

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Today's sensitive, high-resolution X-ray observations allow the study of populations of X-ray sources, in the luminosity range of Galactic X-ray binaries, in galaxies as distant as 20-30Mpc. The traditional astronomical tools of photometric diagrams and luminosity functions are now applied to these populations, providing a direct probe of the evolved binary component of different stellar populations. The study of the X-ray populations of E and S0 galaxies has revamped the debate on the formation and evolution of low-mass X-ray binaries (LMXBs) and on the role of globular clusters in these processes. While overall stellar mass drives the amount of X-ray binaries in old stellar populations, the amount of sources in star forming galaxies is related to the star formation rate. Short-lived, luminous, high mass binaries (HMXBs) dominate these young X-ray populations. The most luminous sources in these systems are the debated ULXs, which have been suggested to be ~100-1000 M  black holes, but could alternatively include a number of binaries with stellar mass black holes. Very soft sources have also been discovered in many galaxies and their nature is currently being debated. Observations of the deep X-ray sky, and comparison with deep optical surveys are providing the first evidence of the X-ray evolution of galaxies.

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“…For reference, the Eddington limit of a black hole accretor of $10 M is in the range $(1:5 3) ; 10 39 ergs s À1 , depending on the chemical composition of the accreted material. ULXs are especially prevalent in galaxies with starburst activity, including ones that have likely undergone a recent dynamical encounter (e.g., Fabbiano et al 2001;Wolter & Trinchieri 2004;Fabbiano & White 2006;Colbert & Miller 2006). Many, but not all, of the ULXs are identified with young star-forming regions (see, e.g., Fabbiano & White 2006).…”

Section: Introductionmentioning

confidence: 99%

Models of Ultraluminous X‐Ray Sources with Intermediate‐Mass Black Holes

Madhusudhan¹,

Justham²,

Nelson³

et al. 2006

ApJ

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We have computed models for ultraluminous X-ray sources (ULXs) consisting of a black hole accretor of intermediate mass (IMBH; e.g., $1000 M ) and a captured donor star. For each of four different sets of initial donor masses and orbital separations we computed 30,000 binary evolution models using a full Henyey stellar evolution code. To our knowledge, this is the first time that a population of X-ray binaries this large has been carried out with other than approximation methods, and it serves to demonstrate the feasibility of this approach to large-scale population studies of mass transfer binaries. In the present study, we find that in order to have a plausible efficiency for producing active ULX systems with IMBHs having luminosities k10 40 ergs s À1 , there are two basic requirements for the capture of companion/donor stars. First, the donor stars should be massive, i.e., k8 M . Second, the initial orbital separations after circularization should be close, i.e., P6-30 times the radius of the donor star when on the main sequence. Even under these optimistic conditions, we show that the production rate of IMBH-ULX systems may fall short of the observed values by factors of 10-100.

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A thorough study of the intriguing X-ray emission from the Cartwheel ring

Cited by 58 publications

References 33 publications

Stephan's Quintet with XMM-Newton

Stephan's Quintet with XMM-Newton

X-ray Source Populations in Galaxies

Models of Ultraluminous X‐Ray Sources with Intermediate‐Mass Black Holes

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