X-ray spectral components of starburst galaxies

Peršić, M.; Rephaeli, Yoel

doi:10.1051/0004-6361:20011679

Cited by 95 publications

(137 citation statements)

References 113 publications

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“…However, the equivalent width of the Fe-K complex arising from HMXBs, either observed directly in HMXBs (typically EW ∼ 0.3 keV: see White et al 1983) or inferred for galaxies with X-ray emission dominated by HMXBs (Persic & Rephaeli 2002), is not consistent with the huge value observed here. The flat hard continuum and the prominent Fe-Kα emission line, may alternatively suggest that IRAS 19254-7245 hosts a Compton-thick AGN (e.g.…”

Section: Spectral Analysiscontrasting

confidence: 92%

XMM-Newtonobservations of ULIRGs: A Compton-thick AGN in IRAS 19254–7245

Braito

Franceschini

Ceca

et al. 2003

A&A

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Abstract. We present the XMM-Newton observation of the merging system IRAS 19254-7245, also known as The Superantennae, whose southern nucleus is classified as a Seyfert 2 galaxy. The XMM-Newton data have allowed us to perform a detailed X-ray imaging and spectral analysis of this system. We clearly detect, for the first time in this system, a strong (EW ∼ 1.4 keV) Fe emission line at 6.49 ± 0.1 keV (rest-frame). The X-ray spectrum requires a soft thermal component (kT ∼ 0.9 keV; L 0.5−2 ∼ 4 × 10 41 erg s −1 ), likely associated with the starburst, and a hard power-law continuum above 2 keV (observed L 2−10 ∼ 4 × 10 42 erg s −1 ). We confirm the flatness of this latter component, already noted in previous ASCA data. This flatness, together with the detection of the strong Fe-Kα line and other broad band indicators, suggest the presence of a Compton-thick AGN with intrinsic luminosity > ∼ 10 44 erg s −1 . We show that a Compton-thick model can perfectly reproduce the X-ray spectral properties of this object.

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Section: Spectral Analysiscontrasting

confidence: 92%

XMM-Newtonobservations of ULIRGs: A Compton-thick AGN in IRAS 19254–7245

Braito

Franceschini

Ceca

et al. 2003

A&A

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“…In a starburst, there are various sources of X-ray emission (e.g., Persic & Rephaeli 2002) whose origin can be traced back to massive stars. Individual supernovae and their remnants, stellar-wind heated ISM in star clusters, and X-ray binaries can all be X-ray sources.…”

Section: Discussionmentioning

confidence: 99%

C-GOALS:Chandraobservations of a complete sample of luminous infrared galaxies from the IRAS Revised Bright Galaxy Survey

Iwasawa

Sanders²,

Teng

et al. 2011

A&A

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We present X-ray data for a complete sample of 44 luminous infrared galaxies (LIRGs), obtained with the Chandra X-ray Observatory. These are the X-ray observations of the high luminosity portion of the Great Observatory All-sky LIRG Survey (GOALS), which includes the most luminous infrared selected galaxies, log (L ir /L ) ≥ 11.73, in the local universe, z ≤ 0.088. X-rays were detected from 43 out of 44 objects, and their arcsec-resolution images, spectra, and radial brightness distributions are presented. With a selection by hard X-ray colour and the 6.4 keV iron line, AGN are found in 37% of the objects, with higher luminosity sources more likely to contain an AGN. These AGN also tend to be found in late-stage mergers. The AGN fraction would increase to 48% if objects with [Ne v]λ14.3 μm detection are included. Double AGN are clearly detected only in NGC 6240 among 24 double/triple systems. Other AGN are found either in single nucleus objects or in one of the double nuclei at similar rates. Objects without conventional X-ray signatures of AGN appear to be hard X-ray quiet, relative to the X-ray to far-IR correlation for starburst galaxies, as discussed elsewhere. Most objects also show extended soft X-ray emission, which is likely related to an outflow from the nuclear region, with a metal abundance pattern suggesting enrichment by core collapse supernovae, as expected for a starburst.

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“…Based on the flux ratio of the Ar xviii Ka line to the Fe He-like line (which should be produced inside the same hot scattering medium) observed in Circinus, in Arp 299 we would expect an Fe He-like line with EW ∼ 400 eV, 13 It should be recalled that Fe-Ka emission is also typical of high-mass Xray binaries (HMXBs) spectra (White, Swank, & Holt 1983). However, its EW, either observed directly in HMXBs (typically EW ∼ 0.3 keV; see White et al 1983) or inferred for galaxies with X-ray emission dominated by HMXBs (Persic & Rephaeli 2002), is inconsistent with the large value observed here (if the emission must be completely accounted for by HMXBs). a value consistent (within a factor of 2) with the derived 90% upper limit.…”

Section: Introductionmentioning

confidence: 92%