Identifications of Four<i>INTEGRAL</i>Sources in the Galactic Plane via<i>Chandra</i>Localizations

Tomsick, John A.; Chaty, S.; Rodríguez, J.; Foschini, L.; Walter, R.; Kaaret, Philip

doi:10.1086/505595

Cited by 65 publications

(104 citation statements)

References 42 publications

(58 reference statements)

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“…The fast flaring activity detected from this source with INTEGRAL led Sguera et al (2006b) to associate this source with the SFXT class (see also Morris et al, 2009a). A Chandra observation performed in the direction of the source permitted to identify the supergiant companion and provide further support to this association (Tomsick et al, 2006a;Rahoui et al, 2008a).…”

Section: Discussionmentioning

confidence: 76%

“…The horizontal red line is the Galactic equator. 2009, 2012b; Tomsick et al, 2006aTomsick et al, , 2008Tomsick et al, , 2009aRahoui et al, 2008a;Burenin et al, 2008;Chaty et al, 2008;Lutovinov et al, 2012b;Karasev et al, 2012).…”

Section: Hard X-ray Sources and Their Identificationmentioning

confidence: 99%

“…It was soon understood that all SFXT systems were hosting a compact object accreting from the wind of a massive companion, typically a super-giant O-B star (Tomsick et al, 2006aChaty et al, 2008;Masetti et al, 2008b;Negueruela et al, 2008b;Tomsick, 2009;Tomsick et al, 2009b;Bodaghee et al, 2012a). SFXTs were thus classified as a subclass of windaccreting super-giant X-ray binaries.…”

Section: Super-giant Fast X-ray Transientsmentioning

confidence: 99%

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High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

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230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: Discussionmentioning

confidence: 76%

Section: Hard X-ray Sources and Their Identificationmentioning

confidence: 99%

Section: Super-giant Fast X-ray Transientsmentioning

confidence: 99%

See 1 more Smart Citation

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

Self Cite

230

234

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“…A first step is to provide an ∼arcsec position with soft X-ray telescopes such as XMM-Newton (Rodriguez et al 2003Bodaghee et al 2006) Chandra (Tomsick et al 2006(Tomsick et al , 2009, and also Swift (Rodriguez et al , 2009b. We then search for counterparts at a position consistent with the refined X-ray position of a given source.…”

Section: Introductionmentioning

confidence: 99%

Swiftfollow-up observations of 13 INTEGRAL sources

Rodríguez¹,

Tomsick

Bodaghee

2010

A&A

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The various IBIS/ISGRI catalogues contain a large population of hard X-ray sources whose nature is still unknown. Even if the >20 keV positional uncertainty provided by ISGRI is unprecedented, it is still too large to pinpoint the counterpart at other wavelengths, which is the only secure way of obtaining a source identification. We continue the work of trying to reveal the nature of these hard X-ray sources, starting with analysis of X-ray data collected via focusing X-ray telescopes, in order to obtain arcsec accurate X-ray positions. We can then identify counterparts at infrared and optical wavelengths and try to unveil the nature of the sources. We analysed data from observations of 13 INTEGRAL sources made with the Swift satellite. The X-ray images obtained by the X-Ray Telescope instrument allowed us to find possible counterparts to the IGR sources with a positional accuracy of a few arcsec. We then browsed the online catalogues (e.g., NED, SIMBAD, 2MASS, 2MASX, USNO B1.0) to search for counterparts at other wavelengths. We also made use of the X-ray spectral parameters in trying to identify the nature of those objects. For the 13 objects, we found possible counterparts at X-ray energies and identified the IR/optical and/or UV counterparts as seen with Swift/UVOT. We also discuss the likelihood of association of the X-ray and INTEGRAL source in each case. We confirm the previously proposed classification of IGR J02524-0829 (Sey 2 AGN), J08023-6954 (RS CVn star), and J11457-1827 (Sey 1 AGN). For 7 of these sources we give the first identification of their nature: IGR J02086-1742, J12060+3818, J12070+2535, J13042-1020, and J13412+3022 are AGN, and J14488-5942 is a probable X-ray binary. For J03184-0014, although we question the association of the IGR and Swift sources, we classify the latter as an AGN. We suggest that IGR J15283-4443 is a Galactic source, but we cannot classify the source further. Finally, we question the association of IGR J11457-1827 and J23130+8608 with the X-ray sources we found, and go on to question the genuineness of the former IGR source.

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“…Even when extinction is high and the distance large a near-infrared (K-band) image will reveal a bright counterpart if the source is a high-mass X-ray binary (e.g. Walter et al 2003, Tomsick et al 2006. Finally, often excess extinction over the Galactic interstellar value is found, implying that the extinction is intrinsic to the source.…”

Section: Identificationmentioning

confidence: 99%

Faint Galactic X-ray Binaries

Jonker¹,

Torres²,

Steeghs³

et al. 2008

AIP Conference Proceedings

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Abstract.We present a short overview of the properties of faint Galactic X-ray binaries. We place emphasis on current classification scenarios. One of the important parameters for the faint sources is their intrinsic luminosity. In the case of low-mass X-ray binaries it has recently been realised that besides a phase of radius expansion, the duration of type I X-ray bursts can be used as a primer for the source luminosity in some cases. Further, we show that a very low equivalent width of hydrogen and helium emission lines in the optical spectrum alone is not a tell-tale sign for an ultra-compact system. Finally, we list and discuss some unusual sources that could be X-ray binaries.

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Identifications of FourINTEGRALSources in the Galactic Plane viaChandraLocalizations

Abstract: Hard X-ray imaging of the Galactic plane by the INTEGRAL satellite is uncovering large numbers of 20

Cited by 65 publications

References 42 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Swiftfollow-up observations of 13 INTEGRAL sources

Faint Galactic X-ray Binaries

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