An X-ray catalog and atlas of galaxies

Fabbiano, G.; Kim, D. W.; Trinchieri, G.

doi:10.1086/191675

Cited by 392 publications

(470 citation statements)

References 1 publication

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“…The X-ray source in LAR5 appears slightly elongated in a direction perpendicular to the galaxy major axis, as seen in several nearby starburst galaxies (e.g. Fabbiano et al 1992, Dahlem et al 1998). However, this elongation may also be due to the degradation of the Chandra PSF at the offaxis-angle of this source (6 arcmin).…”

Section: X-ray Versus Optical Imagingmentioning

confidence: 66%

Spectroscopic identification of ten faint hard X-ray sources discovered by Chandra

et al. 2000

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Section: X-ray Versus Optical Imagingmentioning

confidence: 66%

Spectroscopic identification of ten faint hard X-ray sources discovered by Chandra

et al. 2000

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“…The most stringent cases (on-axis) place a limit of 2A on the radius of the [ X-rayÈemitting region, which, at z \ 0.5, corresponds to a poorly constraining limit of D15 kpc (starbursts have typical dimensions of kpc, e.g., Heckman, Armus, & [2 Miley 1990). However, this hypothesis appears to be rather unlikely because the X-ray luminosities associated with the detected X-ray sources would be a factor of D10È100 times larger than usually observed in nearby starburst and normal galaxies (Fabbiano, Kim, & Trinchieri 1992 ;David, Jones, & Forman 1992). Moreover, there is no suggestion in the literature for a signiÐcant number of starbursts in distant clustersÈnot any more prevalent than in the Ðeld (e.g., Balogh et al 1999).…”

Section: Powerful Starburst Galaxies Associated With the Clusters ?mentioning

confidence: 90%

BeppoSAXObservations of the Maser Seyfert 2 Galaxy ESO 103‐G35

Wilkes

Mathur

Fiore³

et al. 2001

ApJ

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We present results from a Chandra X-Ray Observatory study of the Ðeld X-ray source populations in four di †erent observations : two high-redshift (z D 0.5) clusters of galaxies 3C 295 and RX J003033.2]261819 ; and two noncluster Ðelds with similar exposure time. Surprisingly, the 0.5È2 keV source surface densities (D900È1200 sources deg~2 at a Ñux limit of 1.5 ] 10~15 ergs cm~2 s~1) measured in an D8@ ] 8@ area surrounding each cluster exceed by a factor of D2 the value expected on the basis of the ROSAT and Chandra log N-log S, with a signiÐcance of D2 p each, or D3.5 p when the two Ðelds are combined (i.e., a probability to be a statistical Ñuctuation of \1% and \0.04%, respectively). The same analysis performed on the noncluster Ðelds and on the outer chips of the cluster Ðelds does not show evidence of such an excess. In both cluster Ðelds, the summed 0.5È10 keV spectrum of the detected objects is well Ðtted by a power law with ! D 1.7 similar to active galactic nuclei (AGNs) and shows no sign of intrinsic absorption. The few (D10 of 35) optical identiÐcations available to date conÐrm that most of them are, as expected, AGNs, but the number of redshifts available is too small to allow conclusions on their nature. We discuss possible interpretations of the overdensity in terms of a statistical variation of cosmic background sources ; a concentration of AGNs and/or powerful starburst galaxies associated with the clusters ; and gravitational lensing of background QSOs by the galaxy clusters. All explanations, however, are difficult to reconcile with the large number of excess sources detected. Deeper X-ray observations and more redshifts measurements are clearly required to settle the issue.

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“…All nonactive spiral galaxies which met the NH criterion and have an X-ray ux greater than 45 10 13 erg cm 2 s 1 are included in the sample (see Table 2). The values of X-ray ux (0.2 4.0 KeV) are taken from Fabbiano, Kim & Trinchieri (1992). Note that, unlike IRAS, Einstein did not carry out a complete sky survey, so the X-ray sample is not complete in any sense.…”

Section: X-ray Brightnessmentioning

confidence: 99%

“…Devereux & Eales 1989) where D is the distance in Mpc and S60 m and S100 m, the IRAS 60 and 100 m uxes (in Janskys), are taken from Soifer et al (1989), and supplemented for the nearby, l o w-IRAS ux cases, from Rice et al (1988). The values of (0.2 4.0 keV) X-ray luminosity are taken from Fabbiano et al (1992), and scaled to the Tully (1988) distances.…”

Section: Multiwavelength Luminositiesmentioning

confidence: 99%

“…The EUV points are upper limits for bolometric ux escaping from the galaxy, i.e models A1 (open symbols) and A3 ( lled symbols) for T = 5 10 5 K. A line is drawn at the level of L SN (calculated as in section 3.4) as it is not known in what region of the spectrum this energy appears. Comparison between X-ray and supernovaluminosities for all members of the sample for which X-ray luminosities (Fabbiano et al 1992) are available. Circles denote normal galaxies and stars denote starbursts.…”

Section: Supernova Luminositiesmentioning

confidence: 99%

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EUV emission from normal galaxies

1995

Monthly Notices of the Royal Astronomical Society

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Using data from the ROSAT Wide Field Camera all-sky survey, w e h a v e established upper limits to the extreme ultraviolet (EUV) ux from a sample of 30 bright, nearby, non-active spiral galaxies. These galaxies were chosen to be those most likely to be detected in the EUV on the basis of (i) low i n terstellar absorption within our own galaxy, (ii) brightness in other wavebands, (iii) high star formation activity, and (iv) proximity. The derived EUV upper limits are restrictive, and establish that the EUV ux escaping from galaxies does not contribute a major component of their bolometric luminosity, and in particular that it is very unlikely to be the sink for the energy injected into the interstellar medium by supernova explosions, as had been suggested following the failure to detect this power in the X-ray band.

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An X-ray catalog and atlas of galaxies

Cited by 392 publications

References 1 publication

Spectroscopic identification of ten faint hard X-ray sources discovered by Chandra

Spectroscopic identification of ten faint hard X-ray sources discovered by Chandra

BeppoSAXObservations of the Maser Seyfert 2 Galaxy ESO 103‐G35

EUV emission from normal galaxies

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