On the association of the ultraluminous X-ray sources in the Antennae galaxies with young stellar clusters★

Poutanen, Juri; Fabrika, S.; Valeev, A. F.; Sholukhova, O.; Greiner, J.

doi:10.1093/mnras/stt487

Cited by 65 publications

(67 citation statements)

References 54 publications

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“…These results are in agreement with studies of the XLF of starforming galaxies (e.g., Grimm et al 2003;Mineo et al 2012) and of the location of ULXs in stellar clusters (e.g., Poutanen et al 2013), which conclude that ULXs are a high-luminosity end of the XRB population harboring most possibly stellarmass BHs rather than IMBHs.…”

Section: Discussionsupporting

confidence: 90%

Revealing the Nature of the Ulx and X-Ray Population of the Spiral Galaxy NGC 4088

Mezcua

Fabbiano

Gladstone

et al. 2014

ApJ

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We present the first Chandra and Swift X-ray study of the spiral galaxy NGC 4088 and its ultraluminous X-ray source (ULX N4088-X1). We also report very long baseline interferometry (VLBI) observations at 1.6 and 5 GHz performed quasi-simultaneously with the Swift and Chandra observations, respectively. Fifteen X-ray sources are detected by Chandra within the D25 ellipse of NGC 4088, from which we derive the X-ray luminosity function (XLF) of this galaxy. We find the XLF is very similar to those of star-forming galaxies and estimate a star-formation rate of 4.5 M yr −1 . The Chandra detection of the ULX yields its most accurate X-ray position, which is spatially coincident with compact radio emission at 1.6 GHz. The ULX Chandra X-ray luminosity, L 0.2−10.0keV = 3.4 × 10 39 erg s −1 , indicates that N4088-X1 could be located at the high-luminosity end of the high-mass X-ray binary (HMXB) population of NGC 4088. The estimates of the black hole mass and ratio of radio to X-ray luminosity of N4088-X1 rule out a supermassive black hole nature. The Swift X-ray spectrum of N4088-X1 is best described by a thermal Comptonization model and presents a statistically significant high-energy cut-off. We conclude that N4088-X1 is most likely a stellar remnant black hole in a HMXB, probably fed by Roche lobe overflow, residing in a super-Eddington ultraluminous state. The 1.6 GHz VLBI source is consistent with radio emission from possible ballistic jet ejections in this state.

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Section: Discussionsupporting

confidence: 90%

Revealing the Nature of the Ulx and X-Ray Population of the Spiral Galaxy NGC 4088

Mezcua

Fabbiano

Gladstone

et al. 2014

ApJ

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“…Observations of the optical counterparts revealed that some of the ULXs are associated with young star clusters or star forming regions (Soria et al 2005;Kaaret 2005;Abolmasov et al 2007b;Grise et al 2008Grise et al , 2011Grise et al , 2012Avdan et al 2016a,b). These findings have been supported by identifying point like counterparts of ULXs with blue colors which indicative of early type, OB stars (Liu et al 2004;Grise et al 2005;Soria et al 2005;Roberts et al 2008;Poutanen et al 2013). These blue colors are consistent with emission from an irradiated accretion disk, however, it is noticed that the observed blue color may be partly due to contamination by the X-ray irradiation of the accretion disk and/or the companion star facing the X-ray source (Patruno & Zampieri 2010;Grise et al 2012;Jonker et al 2012;Vinokurov et al 2018).…”

Section: Introductionmentioning

confidence: 84%

“…Therefore, they are good candidates to examine the population properties of ULXs. Poutanen et al (2013) had extensively examined the significant associations between ULXs and stellar clusters in Antennae galaxies. Using HST and VLT data supplemented with theoretical stellar isochrones, they estimated the ages of these clusters as < 6 Myr.…”

Section: Introductionmentioning

confidence: 99%

Optical Counterparts of ULXs and Their Host Environments in NGC 4490/4485

Avdan

Akyüz

Винокуров

et al. 2019

ApJ

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We report the identification of the possible optical counterparts of five out of seven Ultraluminous X-ray Sources (ULXs) in NGC 4490/4485 galaxy pair. Using archival Hubble Space Telescope (HST) imaging data, we identified a single optical candidate for two ULXs (X-4 and X-7) and multiple optical candidates for the other three ULXs (X-2, X-3 and X-6) within ∼ 0. 2 error radius at the 90% confidence level. Of the two remaining ULXs, X-1 has no HST imaging data and photometry could not be performed due to the position of X-5 in NGC4490. Absolute magnitudes (M V ) of the optical candidates lie between −5.7 and −3.8. Color-Magnitude Diagrams (CMDs) have been used to investigate the properties of counterparts and their environments. The locations of the counterparts of X-2, X-4, and X-6 suggest possible association with nearby group of stars while others have no association with a star cluster or group of stars. For comparison purposes, we analyzed previously unused three archival XMM-Newton observations. The long-term X-ray light curves of the sources (except transient X-7) show variability by a factor of three in a time scale more than a decade. The use of disk blackbody model for the mass of the compact objects indicates that these objects might have masses most likely in the range 10−15 M .

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“…In this case, they should stay within the clusters. It has been found [26] that all brightest X-ray sources in Antennae galaxies are located nearby to very young stellar clusters with an age less than 5 Myrs. It was concluded that the sources were ejected in the process of formation of stellar clusters in the dynamical few-body encounters.…”

Section: Pos(apcs2016)046mentioning

confidence: 99%

Ultraluminous X-ray sources. Optical data.

Fabrika¹

2018

Proceedings of Accretion Processes in Cosmic Sources — PoS(APCS2016)

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The origin of Ultraluminous X-ray Sources (ULXs) in external galaxies whose X-ray luminosities exceed those of the brightest black holes in our Galaxy by hundreds and thousands of times is mysterious. The most popular models for the ULXs involve either intermediate mass black holes (IMBHs) or stellar-mass black holes accreting at super-Eddington rates. Here we review the ULX properties. Their X-ray spectra indicate a presence of hot winds in their accretion disks supposing the supercritical accretion. In recent years, new surprising results were discovered in X-ray data, ULX-pulsars and high-velocity outflows up to 0.2 c. They are also in accordance with the superEddington accretion. However, the strongest evidences come from optical spectroscopy. The spectra of the ULX counterparts are very similar to that of SS433, the only known supercritical accretor in our Galaxy. The spectra are apparently of WNL type (late nitrogen Wolf-Rayet stars) or LBV (luminous blue variables) in their hot state, which are very scarce stellar objects. We find that the spectra do not originate from WNL/LBV type donors but from very hot winds from the accretion disks, which have similar physical conditions as the stellar winds from these stars. The results suggest that bona-fide ULXs must constitute a homogeneous class of objects, which most likely have supercritical accretion disks.

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On the association of the ultraluminous X-ray sources in the Antennae galaxies with young stellar clusters★

Cited by 65 publications

References 54 publications

Revealing the Nature of the Ulx and X-Ray Population of the Spiral Galaxy NGC 4088

Revealing the Nature of the Ulx and X-Ray Population of the Spiral Galaxy NGC 4088

Optical Counterparts of ULXs and Their Host Environments in NGC 4490/4485

Ultraluminous X-ray sources. Optical data.

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