A Black Hole Nova Obscured by an Inner Disk Torus

Corral-Santana, J. M.; Casares, J.; Muñoz-Darias, T.; Rodríguez‐Gil, P.; Shahbaz, T.; Torres, M. A. P.; Zurita, C.; Tyndall, A. A.

doi:10.1126/science.1228222

Cited by 110 publications

(136 citation statements)

References 42 publications

Supporting

Mentioning

125

Contrasting

Order By: Relevance

“…Assuming a distance of 1.5 kpc (Rau et al 2011;Corral-Santana et al 2013) the corresponding X-ray luminosity would be 8.5 +5.5 −2.6 × 10 29 erg s −1 , which would make Swift J1357.2-0933 the faintest BH yet in quiescence (below the ∼ 3 × 10 30 erg s −1 luminosity of GS 2000+250, XTE J1650-500 and A0620-00; Gallo et al 2008;Garcia et al 2001, see Fig. 3).…”

Section: Discussionmentioning

confidence: 99%

“…Swift J1357.2-0933 is a BH LMXB in a estimated 2.8±0.3 hours orbit (Corral-Santana et al 2013). It was discovered in outburst on 2011 January 28 with Swift's Burst Alert Telescope (BAT; Barthelmy et al 2005;.…”

Section: Introductionmentioning

confidence: 99%

“…This makes Swift J1357.2-0933 a confirmed BH in a very faint X-ray binary; these are X-ray binaries that have L peak X < 10 36 erg s −1 (Wijnands et al 2006). Based on photometry of Archival Sloan Digital Sky Survey (SDSS) data (obtained prior to the outburst), it was suggested that Swift J1357.2-0933 has an M4 companion star and is located at a distance of D ∼1.5 kpc (Rau et al 2011;Corral-Santana et al 2013). However, Shahbaz et al (2013) found that the quiescent optical light is not dominated by the companion star and instead set a distance in the range D=0.5-6.3 kpc.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Swift J1357.2−0933: the faintest black hole?

Padilla¹,

Wijnands

Degenaar³

et al. 2014

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Swift J1357.2-0933 is a confirmed very faint black hole X-ray transient and has a short estimated orbital period of 2.8 hr. We observed Swift J1357.2-0933 for ∼50 ks with XMM-Newton in 2013 July during its quiescent state. The source is clearly detected at a 0.5-10 keV unabsorbed flux of ∼ 3 × 10 −15 erg cm −2 s −1 . If the source is located at a distance of 1.5 kpc (as suggested in the literature), this would imply a luminosity of ∼ 8 × 10 29 erg s −1 , making it the faintest detected quiescent black hole LMXB. This would also imply that there is no indication of a reversal in the quiescence Xray luminosity versus orbital period diagram down to 2.8 hr, as has been predicted theoretically and recently supported by the detection of the 2.4 hr orbital period black hole MAXI J1659-152 at a 0.5-10 keV X-ray luminosity of ∼ 1.2 × 10 31 erg s −1 . However, there is considerable uncertainty in the distance of Swift J1357.2-0933 and it may be as distant as 6.3 kpc. In this case, its quiescent luminosity would be L X ∼ 1.3 × 10 31 erg s −1 , i.e., similar to MAXI J1659-152 and hence it would support the existence of such a bifurcation period. We also detected the source in optical at r ′ ∼22.3 mag with the Liverpool telescope, simultaneously to our X-ray observation. The Xray/optical luminosity ratio of Swift J1357.2-0933 agrees with the expected value for a black hole at this range of quiescent X-ray luminosities.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Swift J1357.2−0933: the faintest black hole?

Padilla¹,

Wijnands

Degenaar³

et al. 2014

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…There are a few (black hole) LMXBs that did not show H-emission lines in their optical outburst spectra at some epochs, but have measured orbital periods of P orb 90 min: e.g., Swift J1357.2-0933 (Torres et al 2011), and Swift J1753.5-0127, (Jonker et al 2008). Nevertheless, their orbits are relatively small: P orb =2.8 and 2.85 or 3.2 hr, respectively (Zurita et al 2008;Corral-Santana et al 2013;Neustroev et al 2014). This may suggests a possible link between a short orbital period and the absence of H-emission lines.…”

Section: On the Size Of The Binary Orbitmentioning

confidence: 99%

Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

Degenaar

Altamirano

Parker

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

ABSTRACT1RXS J180408.9-342058 is a transient neutron star low-mass X-ray binary that exhibited a bright accretion outburst in 2015. We present NuSTAR, Swift, and Chandra observations obtained around the peak brightness of this outburst. The source was in a soft X-ray spectral state and displayed an X-ray luminosity of L X ≃(2 − 3) × 10 37 (D/5.8 kpc) 2 erg s −1 (0.5-10 keV). The NuSTAR data reveal a broad Fe-K emission line that we model as relativistically broadened reflection to constrain the accretion geometry. We found that the accretion disk is viewed at an inclination of i≃27 • -35 • and extended close to the neutron star, down to R in ≃5-7.5 gravitational radii (≃11-17 km). This inner disk radius suggests that the neutron star magnetic field strength is B 2×10 8 G. We find a narrow absorption line in the Chandra/HEG data at an energy of ≃7.64 keV with a significance of ≃4.8σ. This feature could correspond to blue-shifted Fe XXVI and arise from an accretion disk wind, which would imply an outflow velocity of v out ≃0.086c (≃25 800 km s −1 ). However, this would be extreme for an X-ray binary and it is unclear if a disk wind should be visible at the low inclination angle that we infer from our reflection analysis. Finally, we discuss how the X-ray and optical properties of 1RXS J180408.9-342058 are consistent with a relatively small (P orb 3 hr) binary orbit.

show abstract

“…In those sources, which are likely seen close to edge on, a geometrically thick accretion flow found close to the central supermassive BH is thought to screen the emission from the central part of the system, dramatically reducing the X-ray luminosity. Flared disks are also the most commonly used explanation for obscuration in X-ray binaries seen at high inclinations (see White & Holt 1982and, in particular, Revnivtsev et al 2002 for the case of V4641 Sgr, Fabrika 2004 for SS 433 andCorral-Santana et al 2013 for Swift J1357.2-0933). In both the AGN and BH X-ray binary populations, a large fraction of faint (obscured), high-inclination sources seems to be missed by current X-ray surveys (e.g., Ballantyne et al 2006, Severgnini et al 2011and Corral-Santana et al 2013.…”

Section: Introductionmentioning

confidence: 99%

The black hole binary V404 Cygni: a highly accreting obscured AGN analogue

Motta

Kajava

Sánchez–Fernández

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Typical black hole binaries in outburst show spectral states and transitions, characterized by a clear connection between the inflow onto the black hole and outflows from its vicinity. The transient stellar mass black hole binary V404 Cyg apparently does not fit in this picture. Its outbursts are characterized by intense flares and intermittent plateau and low-luminosity states, with a dynamical intensity range of several orders of magnitude on time-scales of hours. During the 2015 June-July X-ray outburst a joint Swift and INTEGRAL observing campaign captured V404 Cyg in one of these plateau states. The simultaneous Swift/XRT and INTE-GRAL /JEM-X/ISGRI spectrum is reminiscent of that of obscured/absorbed AGN. It can be modelled as a Comptonization spectrum, heavily absorbed by a partial covering, high-column density material (N H ≈ 1 − 3 × 10 24 cm −2 ), and a dominant reprocessed component, including a narrow Iron-Kα line. Such spectral distribution can be produced by a geometrically thick accretion flow able to launch a clumpy outflow, likely responsible for both the high intrinsic absorption and the intense reprocessed emission observed. Similarly to what happens in certain obscured AGN, the low-flux states might not be (solely) related to a decrease in the intrinsic luminosity, but could instead be caused by an almost complete obscuration of the inner accretion flow.

show abstract

A Black Hole Nova Obscured by an Inner Disk Torus

Cited by 110 publications

References 42 publications

Swift J1357.2−0933: the faintest black hole?

Swift J1357.2−0933: the faintest black hole?

Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

The black hole binary V404 Cygni: a highly accreting obscured AGN analogue

Contact Info

Product

Resources

About