LX-SFR relation in star-forming galaxies

Gilfanov, M.; Grimm, H.-J.; Sunyaev, R.

doi:10.1111/j.1365-2966.2004.07450.x

Cited by 164 publications

(188 citation statements)

References 13 publications

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“…In particular, high-mass X-ray binaries (HMXBs) are considered to be the dominant source for the X-ray emission above 2 keV. A good correlation between the 2-10 keV luminosity and the star formation rate have been found for nearby star forming galaxies (Ranalli et al 2003;Grimm et al 2003;Gilfanov et al 2004) as well as for late type galaxies at higher redshift (Lehmer et al 2008). The galacticscale emission nebulae, traced by Hα and the soft X-ray emission in local starburst galaxies like M 82, suggested that these extended nebulae are produced by the shock heated interstellar medium, swept up by a starburst-driven outflow (see e.g., Notes.…”

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

152

271

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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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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

152

271

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“…Correlations between X-ray and radio luminosities of star forming galaxies, and between the X-ray and FIR ones, are well established for the local universe and have been tested for objects up to z ∼ 1 RCS03;Gilfanov et al 2004a;Persic & Rephaeli 2007). Both the radio and FIR luminosity are tracers of the star formation rate (SFR).…”

Section: The X-ray/radio Flux Ratiomentioning

confidence: 99%

“…The X-ray domain has also been recognized as a SF tracer in non-active galaxies (hereafter just "galaxies") thanks to a number of works highlighting the presence of X-ray vs. radio/infrared correlations (David et al 1992;Grimm et al 2003;Ranalli et al 2003, hereafter RCS03;Gilfanov et al 2004a). Strong absorption (i.e.…”

Section: Introductionmentioning

confidence: 99%

X-ray properties of radio-selected star forming galaxies in theChandra-COSMOS survey

Ranalli

Comastri

Zamorani

et al. 2012

A&A

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X-ray surveys contain sizable numbers of star forming galaxies, beyond the AGN which usually make the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multiwavelength properties. We aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. We build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolčić et al. (2008, ApJS, 177, 14) according to their optical colours and observed with Chandra. A similarly selected control sample of AGN is also used for comparison. We review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolčić et al. is such that ∼30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star forming galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, tough it is likely explained by a bias arising from the radio selection. Finally, we discuss the X-ray number counts of star forming galaxies from the VLA-and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra deep fields. The classification scheme proposed here may find application in future works and surveys.

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“…Some of these stars will be HMXB secondaries: Indeed several studies of late-type galaxies have established strong correlations between galaxy-wide X-ray luminosity and total SFR (e.g., Bauer et al 2002;Grimm et al 2003;Ranalli et al 2003;Gilfanov et al 2004a;Persic et al 2004;Hornschemeier et al 2005;Persic & Rephaeli 2007;Lehmer et al 2008Lehmer et al , 2010Mineo et al 2012). On the other hand, in quiescent (morphologically elliptical/S0) galaxies, longer-lived (1 Gyr) low-mass stars trace the total stellar mass accumulated over a galaxy's lifetime.…”

Section: Introductionmentioning

confidence: 99%

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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We obtain total galaxy X-ray luminosities, L X , originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of our galaxies, we find that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, we find that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the ±1σ scatter of the Mineo et al. L X -star formation rate (SFR) correlation or have higher L X than predicted by this correlation for their SFR. We discuss how these "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies are consistent with the Boroson et al. L X -stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low-or high-mass XRBs, we use appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L X values. We find that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L X values can be observed due to strong XRB variability.

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LX-SFR relation in star-forming galaxies

Cited by 164 publications

References 13 publications

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

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

X-ray properties of radio-selected star forming galaxies in theChandra-COSMOS survey

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

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