Population of the Galactic X-ray binaries and eRosita

Doroshenko, V.; Ducci, L.; Santangelo, A.; Sasaki, M.

doi:10.1051/0004-6361/201423766

Cited by 21 publications

(20 citation statements)

References 15 publications

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“…A preliminary attempt to find pulsating ULXs (other than M82 X-2) in XMM-Newton archival data (Doroshenko et al 2014) found none, but more sensitive surveys will follow. Our attention has turned to IC10 X-1 as a NS candidate because of its modest (for a ULX) luminosity (LX 1.2 × 10 38 erg s −1 ) and its phase-shifted RV curve (Laycock et al 2015).…”

Section: Discussionmentioning

confidence: 96%

Revisiting the dynamical case for a massive black hole in IC10 X-1

Laycock

Maccarone

Christodoulou

2015

Monthly Notices of the Royal Astronomical Society: Letters

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The relative phasing of the X-ray eclipse ephemeris and optical radial velocity (RV) curve for the X-ray binary IC10 X-1 suggests the He[λ4686] emission-line originates in a shadowed sector of the stellar wind that avoids ionization by X-rays from the compact object. The line attains maximum blueshift when the wind is directly toward us at mid X-ray eclipse, as is also seen in Cygnus X-3. If the RV curve is unrelated to stellar motion, evidence for a massive black hole evaporates because the mass function of the binary is unknown. The reported X-ray luminosity, spectrum, slow QPO, and broad eclipses caused by absorption/scattering in the WR wind are all consistent with either a low-stellar-mass BH or a NS. For a NS, the centre of mass lies inside the WR envelope whose motion is then far below the observed 370 km/s RV amplitude, while the velocity of the compact object is as high as 600 km/s. The resulting 0.4% doppler variation of X-ray spectral lines could be confirmed by missions in development. These arguments also apply to other putative BH binaries whose RV and eclipse curves are not yet phase-connected. Theories of BH formation and predicted rates of gravitational wave sources may need revision.

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Section: Discussionmentioning

confidence: 96%

Revisiting the dynamical case for a massive black hole in IC10 X-1

Laycock

Maccarone

Christodoulou

2015

Monthly Notices of the Royal Astronomical Society: Letters

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“…However, the break at 2 × 10 37 erg s −1 was inconsistent with the single power-law slope from soft X-ray surveys. Doroshenko et al (2014) completed a robust analysis of Galactic LMXB and HMXB XLFs using the INTEGRAL catalog of Krivonos et al (2012). A novel method was used to create XLFs that did not require distance measurements for any of the sources.…”

Section: Hard X-ray Luminosity Functionsmentioning

confidence: 99%

Black Holes and Neutron Stars in Nearby Galaxies: Insights from NuSTAR

Vulic

Hornschemeier

Wik

et al. 2018

ApJ

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Nearby galaxy surveys have long classified X-ray binaries (XRBs) by the mass category of their donor stars (high-mass and low-mass). The NuSTAR observatory, which provides imaging data at E > 10 keV, has enabled the classification of extragalactic XRBs by their compact object type: neutron star (NS) or black hole (BH). We analyzed NuSTAR/Chandra/XMM-Newton observations from a NuSTAR-selected sample of 12 galaxies within 5 Mpc having stellar masses (M ⋆ ) 10 7−11 M ⊙ and star formation rates (SFR) ≈ 0.01 − 15 M ⊙ yr −1 . We detect 128 NuSTAR sources to a sensitivity of ≈ 10 38 erg s −1 . Using NuSTAR color-intensity and color-color diagrams we classify 43 of these sources as candidate NS and 47 as candidate BH. We further subdivide BH by accretion states (soft, intermediate, and hard) and NS by weak (Z/Atoll) and strong (accreting pulsar) magnetic field. Using 8 normal (Milky Way-type) galaxies in the sample, we confirm the relation between SFR and galaxy X-ray point source luminosity in the 4 − 25 and 12 − 25 keV energy bands. We also constrain galaxy X-ray point source luminosity using the relation L X = αM ⋆ + βSFR, finding agreement with previous work. The XLF of all sources in the 4 − 25 and 12 − 25 keV energy bands matches with the α = 1.6 slope for high-mass XRBs. We find that NS XLFs suggest a decline beginning at the Eddington limit for a 1.4 M ⊙ NS, whereas the BH fraction shows an approximate monotonic increase in the 4 − 25 and 12 − 25 keV energy bands. We calculate the overall ratio of BH to NS to be ≈ 1 for 4 − 25 keV and ≈ 2 for 12 − 25 keV.

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“…This part of the work is based on the novel method of modelling XRB populations of Doroshenko et al (2014).…”

Section: Calculationsmentioning

confidence: 99%

“…We assumed that SFXTs have the same spatial distribution as classical HMXBs (Grimm et al 2002;Coleiro & Chaty 2013;Doroshenko et al 2014) and the same flaring properties as the sample of known SFXTs, which have been investigated recently by P14. Based on the assumed spatial distribution, we assigned a random position within the Milky Way for each simulated source and calculated the survey exposure in the respective direction.…”

Section: Integralmentioning

confidence: 99%

Expected number of supergiant fast X-ray transients in the Milky Way

Ducci

Doroshenko

Romano

et al. 2014

A&A

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In the past fifteen years a new generation of X-ray satellites led to the discovery of a subclass of high-mass X-ray binaries (HMXBs) with supergiant companions and a peculiar transient behaviour: supergiant fast X-ray transients (SFXTs). We calculate the expected number of Galactic SFXTs for the first time, using two different statistical approaches and two sets of data based on Swift and INTEGRAL surveys, with the aim to determine how common the SFXT phenomenon really is. We find that the expected number of SFXTs in the Galaxy is ≈37, which shows that SFXTs constitute a large portion of X-ray binaries with supergiant companions in the Galaxy. We compare our estimate with the expected number of Galactic HMXBs predicted from observations and evolutionary models and discuss the implications for the nature of SFXTs.

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Population of the Galactic X-ray binaries and eRosita

Cited by 21 publications

References 15 publications

Revisiting the dynamical case for a massive black hole in IC10 X-1

Revisiting the dynamical case for a massive black hole in IC10 X-1

Black Holes and Neutron Stars in Nearby Galaxies: Insights from NuSTAR

Expected number of supergiant fast X-ray transients in the Milky Way

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