SPECTRAL AND TIMING PROPERTIES OF THE BLACK HOLE X-RAY BINARY H1743–322 IN THE LOW/HARD STATE STUDIED WITH<i>SUZAKU</i>

Shidatsu, M.; Ueda, Yoshihiro; Yamada, S.; Done, Chris; Hori, T.; Yamaoka, K.; Kubota, Aya; Nagayama, Takahiro; Moritani, Yuki

doi:10.1088/0004-637x/789/2/100

Cited by 37 publications

(39 citation statements)

References 87 publications

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“…The temperature (∼0.2 keV) and the normalization (> 10 3 ) of the disc component, which contributes less than 10 per cent to the 0.5-10 keV flux, are fully consistent with values reported for BHs in the hard state (e.g. Reis et al 2010;Armas Padilla et al 2014;Shidatsu et al 2014;Plant et al 2015). NS systems accreting at low luminosities generally display hotter blackbody temperatures (kT bb > ∼ 0.3 keV) and lower normalizations (< 10 3 ), with this component typically contributing at the ∼20-50 per cent level (Degenaar et al 2017;Sharma et al 2018;Di Salvo et al 2015).…”

Section: Discussionsupporting

confidence: 87%

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

Padilla

Muñoz-Darias

Sánchez-Sierras

et al. 2019

Monthly Notices of the Royal Astronomical Society

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MAXI J1813-095 is an X-ray transient discovered during an outburst in 2018. We report on X-ray and optical observations obtained during this event, which indicate that the source is a new low-mass X-ray binary. The outburst lasted ∼70 d and peaked at L X (0.5-10keV)∼ 7.6 × 10 36 erg s −1 , assuming a distance of 8 kpc. Swift/XRT follow-up covering the whole activity period shows that the X-ray emission was always dominated by a hard power-law component with a photon index in the range of 1.4-1.7. These values are consistent with MAXI J1813-095 being in the hard state, in agreement with the ∼30 per cent fractional root-mean-square amplitude of the fast variability (0.1-50 Hz) inferred from the only XMM-Newton observation available. The X-ray spectra are well described by a Comptonization emission component plus a soft, thermal component (kT ∼0.2 keV), which barely contributes to the total flux ( 8 per cent). The Comptonization y-parameter (∼1.5), together with the low temperature and small contribution of the soft component supports a black hole accretor. We also performed optical spectroscopy using the VLT and GTC telescopes during outburst and quiescence, respectively. In both cases the spectrum lack emission lines typical of X-ray binaries in outburst. Instead, we detect the Ca ii triplet and Hα in absorption. The absence of velocity shifts between the two epochs, as well as the evolution of the Hα equivalent width, strongly suggest that the optical emission is dominated by an interloper, likely a G-K star. This favours a distance 3 kpc for the X-ray transient.

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Section: Discussionsupporting

confidence: 87%

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

Padilla

Muñoz-Darias

Sánchez-Sierras

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…It correlates with the NuSTAR flux and the photon index ( Fig. 7), similar to many other BH and neutron star binary systems (see, e.g., Sobczak et al 2000;Revnivtsev et al 2001;Vignarca et al 2003;Titarchuk & Fiorito 2004;Ibragimov et al 2005;Gilfanov 2010;Shidatsu et al 2014;Fürst et al 2016b;Mereminskiy et al 2018). The QPO amplitude remained stable during the first half of the observation, and started to grow in the second part.…”

Section: Power Spectrumsupporting

confidence: 81%

Studying temporal variability of GRS 1739–278 during the 2014 outburst

Mereminskiy

Семена

Bykov

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We report a discovery of low-frequency quasi periodic oscillation at 0.3-0.7 Hz in the power spectra of the accreting black hole GRS 1739-278 in the hard-intermediate state during its 2014 outburst based on the NuSTAR and Swift/XRT data. The QPO frequency strongly evolved with the source flux during the NuSTAR observation. The source spectrum became softer with rising QPO frequency and simultaneous increasing of the power-law index and decreasing of the cut-off energy. In the power spectrum, a prominent harmonic is clearly seen together with the main QPO peak. The fluxes in the soft and the hard X-ray bands are coherent, however, the coherence drops for the energy bands separated by larger gaps. The phase-lags are generally positive (hard) in the 0.1-3 Hz frequency range, and negative below 0.1 Hz. The accretion disc inner radius estimated with the relativistic reflection spectral model appears to be R in < 7.3R g . In the framework of the relativistic precession model, in order to satisfy the constraints from the observed QPO frequency and the accretion disc truncation radius, a massive black hole with M BH ≈ 100M is required.

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“…We cannot rule out, however, the possibility that the soft component seen on March 25 was not the direct standard disk emission but a Comptonized emission produced around the inner edge of the standard disk, as discussed (Chiang et al 2010;Yamada et al 2013b;Shidatsu et al 2014). If this is the case, the direct disk component was below the energy range of the XRT, and the standard disk was further truncated, with a lower inner disk temperature than what we estimated above.…”

Section: Implications In Long-and Short-term X-ray Variationsmentioning

confidence: 84%

X-Ray, Optical, and Near-infrared Monitoring of the New X-Ray Transient MAXI J1820+070 in the Low/Hard State

Shidatsu

Nakahira

Yamada

et al. 2018

ApJ

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We report X-ray, optical, and near-infrared monitoring of the new X-ray transient MAXI J1820+070 discovered with MAXI on 2018 March 11. Its X-ray intensity reached ∼ 2 Crab in 2-20 keV at the end of March, and then gradually decreased until the middle of June. In this period, the X-ray spectrum was described by Comptonization of the disk emission, with a photon index of ∼1.5 and an electron temperature of ∼50 keV, which is consistent with a black hole X-ray binary in the low/hard state. The electron temperature and the photon index were slightly decreased and increased with increasing flux, respectively. The source showed significant X-ray flux variation on timescales of seconds. This shortterm variation was found to be associated with changes in the spectral shape, and the photon index became slightly harder at higher fluxes. This suggests that the variation was produced by a change in the properties of the hot electron cloud responsible for the strong Comptonization. Modeling a multi-wavelength SED around the X-ray flux peak at the end of March, covering the near-infrared to X-ray bands, we found that the optical and near-infrared fluxes were likely contributed substantially by the jet emission. Before this outburst, the source was never detected in the X-ray band with MAXI (with a 3σ upper limit of ∼0.2 mCrab in 4-10 keV, obtained from the 7-year data in 2009-2016), whereas weak optical and infrared activity was found at their flux levels ∼3 orders of magnitude lower than the peak fluxes in the outburst.

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SPECTRAL AND TIMING PROPERTIES OF THE BLACK HOLE X-RAY BINARY H1743–322 IN THE LOW/HARD STATE STUDIED WITHSUZAKU

Cited by 37 publications

References 87 publications

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

Studying temporal variability of GRS 1739–278 during the 2014 outburst

X-Ray, Optical, and Near-infrared Monitoring of the New X-Ray Transient MAXI J1820+070 in the Low/Hard State

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