X-ray Binaries in the Milky Way and Other Galaxies

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

doi:10.1088/1009-9271/3/s1/257

Cited by 14 publications

(10 citation statements)

References 102 publications

(138 reference statements)

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“…On the other hand, we detected no emission above 2 keV in Source 2. The luminosity extrapolated from the fit in the energy range 2 -10 keV is L x = 1.7 +1.3 −1.2 × 10 40 erg s −1 ; this is consistent with the value expected from the observed SFR (5 +1 −2 × 10 40 erg s −1 ), however, the predicted Xray luminosity derived using the scaling relation of Grimm et al 2003 refers to the luminosity of the galaxy as a whole; instead, the X-ray luminosity quoted for Source 2 was derived from a region including no more than about 50% of the galaxy mass (this is approximately the mass ratio between the boxy-bulge and the tadpole body highlighted in the sdss u-band image, Fig.1). It might be an indication that a weak AGN is present in Source 2.…”

Section: Nuclear Activitysupporting

confidence: 85%

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Characterization of a candidate dual AGN

Lena

Panizo-Espinar

Jonker

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present Chandra and optical observations of a candidate dual AGN discovered serendipitously while searching for recoiling black holes via a cross-correlation between the serendipitous XMM source catalog (2XMMi) and SDSS-DR7 galaxies with a separation no larger than ten times the sum of their Petrosian radii. The system has a stellar mass ratio M 1 /M 2 ≈ 0.7. One of the galaxies (Source 1) shows clear evidence for AGN activity in the form of hard X-ray emission and optical emission-line diagnostics typical of AGN ionisation. The nucleus of the other galaxy (Source 2) has a soft X-ray spectrum, bluer colours, and optical emission line ratios dominated by stellar photoionisation with a "composite" signature, which might indicate the presence of a weak AGN. When plotted on a diagram with X-ray luminosity vs [OIII] luminosity both nuclei fall within the locus defined by local Seyfert galaxies. From the optical spectrum we estimate the electron densities finding n 1 < 27 e − cm −3 and n 2 ≈ 200 e − cm −3 . From a 2D decomposition of the surface brightness distribution we infer that both galaxies host rotationally supported bulges (Sersic index < 1). While the active nature of Source 1 can be established with confidence, whether the nucleus of Source 2 is active remains a matter of debate. Evidence that a faint AGN might reside in its nucleus is, however, tantalising.

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Section: Nuclear Activitysupporting

confidence: 85%

“…of high-mass X-ray binaries to the X-ray luminosity. We used the relation derived by Grimm et al 2003:…”

Section: Star-formation Ratesmentioning

confidence: 99%

Characterization of a candidate dual AGN

Lena

Panizo-Espinar

Jonker

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Secondly, ULXs are most commonly associated with star-forming galaxies (Swartz et al 2011) or even young elliptical galaxies with recent star formation events rather than old elliptical ones with no star formation (Kim & Fabbiano 2004. This is consistent with ULXs belonging to a high-luminosity extrapolation of the X-ray binary population whose abundances correlate with the star formation rate (SFR) and the stellar mass (M * ) of their host galaxies (Gilfanov 2004;Grimm et al 2003;Mineo et al 2012). And finally, but perhaps most importantly, the direct observation of regular pulsations in some ULXs unmistakably points towards accretion onto a NS in binary systems.…”

Section: Introductionsupporting

confidence: 62%

An expanded ultraluminous X-ray source catalogue

Bernadich

Schwope

Kovlakas

et al. 2022

A&A

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Context. Ultraluminous X-ray sources (L X ×10 39 erg s −1 , ULXs) are excellent probes for extreme accretion physics, star formation history in galaxies, and intermediate-mass black holes searches. As the sample size of X-ray data from modern observatories such as XMM-Newton and Chandra increases, producing extensive catalogues of ULXs and studying their collective properties has become both a possibility and a priority. Aims. Our aim is to build a clean updated ULX catalogue based on one of the most recent XMM-Newton X-ray serendipitous survey data releases, 4XMM-DR9, and the most recent and exhaustive catalogue of nearby galaxies, HECATE. We performed a preliminary population study to test if the properties of the expanded XMM-Newton ULX population are consistent with previous findings. Methods. We performed positional cross-matches between XMM-Newton sources and HECATE objects to identify host galaxies, and we used distance and luminosity arguments to identify ULX candidates. We flagged interlopers by finding known counterparts in external catalogues and databases such as Gaia DR2, SSDS, Pan-STARRS1, the NASA/IPAC Extragalactic Database, and SIMBAD. Source, galaxy and variability parameters from 4XMM-DR9, HECATE, and 4XMM-DR9s were used to study the spectral, abundance, and variability properties of the ULX sample. Results. We identify 779 ULX candidates, 94 of which hold L X 5 × 10 40 erg s −1 . Spiral galaxies are more likely to host ULXs. For early spiral galaxies the number of ULX candidates per star-forming rate is consistent with previous studies, while a significant ULX population in elliptical and lenticular galaxies also exists. Candidates hosted by late-type galaxies tend to present harder spectra and to undergo more extreme inter-observation variability than those hosted by early-type galaxies. Approximately 30 candidates with L X > 10 41 erg s −1 are also identified, constituting the most interesting candidates for intermediate-mass black hole searches. Conclusions. We have built the largest ULX catalogue to date. Our results on the spectral and abundance properties of ULXs confirm the findings made by previous studies based on XMM-Newton and Chandra data, while our population-scale study on variability properties is unprecedented. Our study, however, provides limited insight into the properties of the brightest ULX candidates due to the small sample size. The expected growth of X-ray catalogues and potential future follow-ups will aid in drawing a clearer picture.

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“…These effects may even allow violations of the Eddington limit by a factor as large as 100 (Begelman 2002(Begelman , 2006) so our super-Eddington model may remain conservative. On the other hand, NS accretors seem to remain within twice the Eddington rate (Levine et al 1991(Levine et al , 1993Grimm et al 2003a). This approximation has subsequently been employed in several theoretical models of luminous X-ray binary formation (Rappaport et al 2005;Fragos et al 2008), and we adopt this assumption throughout.…”

Section: Simulation Code and Modelsmentioning

confidence: 98%

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

Linden

Kalogera

Sepinsky

et al. 2010

ApJ

175

227

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We investigate the characteristics of young (<20 Myr) and bright (L X > 1 × 10 36 erg s −1 ) high-mass X-ray binaries (HMXBs) and find the population to be strongly metallicity dependent. We separate the model populations among two distinct formation pathways: (1) systems undergoing active Roche lobe overflow (RLO) and (2) wind accretion systems with donors in the (super)giant stage, which we find to dominate the HMXB population. We find metallicity to primarily affect the number of systems which move through each formation pathway, rather than the observable parameters of systems which move through each individual pathway. We discuss the most important model parameters affecting the HMXB population at both low and high metallicities. Using these results, we show that (1) the population of ultra-luminous X-ray sources can be consistently described by very bright HMXBs which undergo stable RLO with mild super-Eddington accretion and (2) the HMXB population of the bright starburst galaxy NGC 1569 is likely dominated by one extremely metal-poor starburst cluster.

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X-ray Binaries in the Milky Way and Other Galaxies

Cited by 14 publications

References 102 publications

Characterization of a candidate dual AGN

Characterization of a candidate dual AGN

An expanded ultraluminous X-ray source catalogue

The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

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