Spectroscopic evidence for a low-mass black hole in SWIFT J1753.5−0127

Neustroev, V.; Veledina, Alexandra; Poutanen, Juri; Zharikov, S. V.; Tsygankov, Sergey S.; Sjoberg, George; Kajava, J. J. E.

doi:10.1093/mnras/stu1924

Cited by 47 publications

(66 citation statements)

References 73 publications

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“…The distance of Swift J1753.5-0127 is poorly constrained, but likely lies somewhere between 2.5−10 kpc (Cadolle Bel et al 2007;Zurita et al 2008). Recent optical observations suggest that the binary consists of a low-mass BH and a somewhat evolved 0.2 M companion star (Neustroev et al 2014). We adopt i = 40…”

Section: Swift J17535-0127mentioning

confidence: 99%

The origin of seed photons for Comptonization in the black hole binary Swift J1753.5–0127

Kajava

Veledina

Tsygankov

et al. 2016

A&A

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Aims. The black hole binary Swift J1753.5-0127 is providing a unique data set to study accretion flows. Various investigations of this system and of other black holes have not, however, led to an agreement on the accretion flow geometry or on the seed photon source for Comptonization during different stages of X-ray outbursts. We place constraints on these accretion flow properties by studying long-term spectral variations of this source. Methods. We performed phenomenological and self-consistent broad band spectral modeling of Swift J1753.5-0127 using quasisimultaneous archived data from INTEGRAL/ISGRI, Swift/UVOT/XRT/BAT, RXTE/PCA/HEXTE, and MAXI/GSC instruments. Results. We identify a critical flux limit, F ∼ 1.5 × 10 −8 erg cm −2 s −1 , and show that the spectral properties of Swift J1753.5-0127 are markedly different above and below this value. Above the limit, during the outburst peak, the hot medium seems to intercept roughly 50 percent of the disk emission. Below it, in the outburst tail, the contribution of the disk photons reduces significantly and the entire spectrum from the optical to X-rays can be produced by a synchrotron-self-Compton mechanism. The long-term variations in the hard X-ray spectra are caused by erratic changes of the electron temperatures in the hot medium. Thermal Comptonization models indicate unreasonably low hot medium optical depths during the short incursions into the soft state after 2010, suggesting that non-thermal electrons produce the Comptonized tail in this state. The soft X-ray excess, likely produced by the accretion disk, shows peculiarly stable temperatures for over an order of magnitude changes in flux. Conclusions. The long-term spectral trends of Swift J1753.5-0127 are likely set by variations of the truncation radius and a formation of a hot, quasi-spherical inner flow in the vicinity of the black hole. In the late outburst stages, at fluxes below the critical limit, the source of seed photons for Comptonization is not the thermal disk, but more likely they are produced by non-thermal synchrotron emission within the hot flow near the black hole. The stability of the soft excess temperature is, however, not consistent with this picture and further investigations are needed to understand its behavior.

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Section: Swift J17535-0127mentioning

confidence: 99%

The origin of seed photons for Comptonization in the black hole binary Swift J1753.5–0127

Kajava

Veledina

Tsygankov

et al. 2016

A&A

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“…Examples of the application of this technique to the real data are given in Neustroev (1998), Neustroev et al (2002Neustroev et al ( , 2014. References.…”

Section: Accretion Disc Parameters From Modelling Of the Emission-linmentioning

confidence: 99%

Voracious vortexes in cataclysmic variables

Neustroev

Zharikov

Borisov

2016

A&A

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We present multi-epoch, time-resolved optical spectroscopic observations of the dwarf nova HT Cas, which were obtained during 1986, 1992, 1995, and 2005 with the aim of studying the properties of emission structures in the system. We determined that the accretion disc radius, measured from the double-peaked emission-line profiles, is consistently large and lies within the range of 0.45-0.52a, where a is the binary separation. This is close to the tidal truncation radius r max = 0.52a. However, this result is not consistent with previous radius measurements. An extensive set of Doppler maps reveals a very complex emission structure of the accretion disc. Apart from a ring of disc emission, the tomograms display at least three areas of enhanced emission: the hot spot from the area of interaction between the gas stream and the disc, which is superposed on the elongated spiral structure, and the extended bright region on the leading side of the disc, which is opposite to the location of the hotspot. The position of the hotspot in all the emission lines is consistent with the trajectory of the gas stream. However, the peaks of emission are located in the range of distances 0.22-0.30a, which are much closer to the white dwarf than the disc edge. This suggests that the outer disc regions have a very low density, allowing the gas stream to flow almost freely before it starts to be seen as an emission source. We have found that the extended emission region on the leading side of the disc is always observed at the very edge of the large disc. Observations of other cataclysmic variables, which show a similar emission structure in their tomograms, confirm this conclusion. We propose that the leading side bright region is caused by irradiation of tidally thickened sectors of the outer disc, by the white dwarf and/or hot inner disc regions.

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“…BHC Swift J1753.5-0127 has a short orbital period of 3.2 ± 0.2 hrs (Zurita et al 2007). However Neustroev et al (2014) suggested the orbital period is 2.85 hrs. They also reported that the binary has a primary BH mass of less than 5 M ⊙ and companion as 0.17−0.25M ⊙ and disk inclination angle of > 40…”

Section: Introductionmentioning

confidence: 99%

Accretion Flow Properties of Swift J1753.5-0127 during Its 2005 Outburst

Debnath

Jana

Chakrabarti

et al. 2017

ApJ

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Galactic X-ray binary black hole candidate Swift J1753.5-0127 was discovered on June 30 2005 by Swift/BAT instrument. In this paper, we make detailed analysis of spectral and timing properties of its 2005 outburst using RXTE/PCA archival data. We study evolution of spectral properties of the source from spectral analysis with the additive table model fits file of the Chakrabarti-Titarchuk two-components advective flow (TCAF) solution. From spectral fit, we extract physical flow parameters, such as, Keplerian disk accretion rate, sub-Keplerian halo rate, shock location and shock compression ratio, etc. We also study the evolution of temporal properties, such as observation of low frequency quasi-periodic oscillations (QPOs), variation of X-ray intensity throughout the outburst. From the nature of the variation of QPOs, and accretion rate ratios (ARRs=ratio of halo to disk rates), we classify entire 2005 outburst into two harder (hard-intermediate and hard) spectral states. No signature of softer (soft-intermediate and soft) spectral states are seen. This may be because of significant halo rate throughout the outburst. This behavior is similar to a class of other short orbital period sources, such as, MAXI J1836-194, MAXI J1659-152 and XTE J1118+480. Here, we also estimate probable mass range of the source, to be in between 4.75M ⊙ to 5.90M ⊙ based on our spectral analysis.

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Spectroscopic evidence for a low-mass black hole in SWIFT J1753.5−0127

Cited by 47 publications

References 73 publications

The origin of seed photons for Comptonization in the black hole binary Swift J1753.5–0127

The origin of seed photons for Comptonization in the black hole binary Swift J1753.5–0127

Voracious vortexes in cataclysmic variables

Accretion Flow Properties of Swift J1753.5-0127 during Its 2005 Outburst

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