The first outburst of the black-hole candidate MAXI J1836−194 observed by INTEGRAL,<i>Swift</i>, and RXTE

Ferrigno, C.; Bozzo, E.; Santo, M. Del; Capitanio, Fiamma

doi:10.1051/0004-6361/201118474

Cited by 39 publications

(51 citation statements)

References 18 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…5. The uncertainties on the rms of each observation was obtained from bootstrapping simulations with 1000 realizations (for a detailed description of the method see Ferrigno et al 2012). The source exhibited an rms < ∼ 10% in all XRT pointings and no particular trend is found when the rms is plotted as a function of the total source countrate (see Fig.…”

Section: Resultsmentioning

confidence: 99%

“…Radio emission at this state is no longer observed, most likely because of the suppression of the jet. The time variability of the source is also significantly different in the two states, being generally more pronounced in the LHS with rms values of up to ∼30% and characterized by the quasi-periodical oscillations (QPOs) in the HSS in combination with a strongly suppressed rms Capitanio et al 2009;Ferrigno et al 2012). …”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

INTEGRAL andSwiftobservations of the hard X-ray transient MAXI J1828-249

Filippova¹,

Bozzo²,

Ferrigno³

2014

A&A

Self Cite

View full text Add to dashboard Cite

In this paper we report on the observations performed with INTEGRAL and Swift of the first outburst detected from the hard X-ray transient MAXI J1828-249. During the first about two days of the outburst, the source was observed by MAXI to undergo a very rapid transition from a hard to a softer spectral state. While the hard state was not efficiently monitored because the transition occurred so rapidly, the evolution of the source outburst in the softer state was covered quasi-simultaneously in a broad energy range (0.6−150 keV) by the instruments on board INTEGRAL and Swift. During these observations, the spectra measured from the source displayed both a prominent thermal emission with temperature kT ∼ 0.7 keV and a power-law hard component with a photon index Γ ∼ 2.2 extending to 200 keV. The properties of the source in the X-ray domain are reminiscent of those displayed by black hole transients during the soft intermediate state, which supports the association of MAXI J1828-249 with this class of objects.

show abstract

Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

INTEGRAL andSwiftobservations of the hard X-ray transient MAXI J1828-249

Filippova¹,

Bozzo²,

Ferrigno³

2014

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…There were also optical+NIR observations collected with GROND (Rau et al 2011). All these observations were taken during a failed hard-to-soft state transition (Brocksopp et al 2004) that occurred between the beginning of September and the end of October (Ferrigno et al 2012). During this period, the source went into a hard-intermediate state (HIMS) but never reached the soft state and, instead, the outburst "failed" and went back to the hard state.…”

Section: Observationsmentioning

confidence: 99%

Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

Péault

Malzac

Coriat

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The black hole candidate MAXI J1836-194 was discovered in 2011 when it went into an outburst, and was the subject of numerous, quasi-simultaneous, multi-wavelength observations in the radio, infrared, optical and X-rays. In this paper, we model its multi-wavelength radio to optical spectral energy distributions (SEDs) with an internal shock jet model. The jet emission is modelled on five dates of the outburst, during which the source is in the hard and hard intermediate X-ray spectral states. The model assumes that fluctuations of the jet velocity are driven by the variability in the accretion flow which is traced by the observed X-ray timing properties of the source. While the global shape of the SED is well reproduced by this model for all the studied observations, the variations in bolometric flux and typical energies require at least two parameters to evolve during the outburst. Here we investigate variations of the jet power and mean Lorentz factor, which are both found to increase with the source luminosity. Our results are compatible with the evolution of the jet Lorentz factor reported in earlier studies of this source. However, due to the large degeneracy of the parameters of the ishem model, our proposed scenario is not unique.

show abstract

“…A few failed outbursts have been reported in H 1743−322 so far (Capitanio et al 2009;Chen et al 2010). In addition to this source, there are a few other BHXBs that underwent failed outbursts, like XTE J1550−564 and MAXI J1836−164 (Sturner & Shrader 2005;Ferrigno et al 2012). The 1-500 keV unabsorbed luminosity in Epoch 1 (calculated from the best-fit model) is estimated to be 6.1 × 10 37 D 2 8.5 erg s −1 .…”

Section: Failed Outburst In 2012 Octobermentioning

confidence: 99%

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

Shidatsu

Ueda

Yamada

et al. 2014

ApJ

View full text Add to dashboard Cite

We report on the results from Suzaku observations of the Galactic black hole X-ray binary H1743−322 in the low/hard state during its outburst in 2012 October. We appropriately take into account the effects of dust scattering to accurately analyze the X-ray spectra. The time-averaged spectra in the 1-200 keV band are dominated by a hard power-law component of a photon index of ≈1.6 with a high-energy cutoff at ≈60 keV, which is well described with the Comptonization of the disk emission by the hot corona. We estimate the inner disk radius from the multi-color disk component, and find that it is 1.3-2.3 times larger than the radius in the high/soft state. This suggests that the standard disk was not extended to the innermost stable circular orbit. A reflection component from the disk is detected with R = Ω/2π ≈ 0.6 (Ω is the solid angle). We also successfully estimate the stable disk component independent of the time-averaged spectral modeling by analyzing short-term spectral variability on a ∼1 s timescale. A weak low-frequency quasi-periodic oscillation at 0.1-0.2 Hz is detected, whose frequency is found to correlate with the X-ray luminosity and photon index. This result may be explained by the evolution of the disk truncation radius.

show abstract

The first outburst of the black-hole candidate MAXI J1836−194 observed by INTEGRAL,Swift, and RXTE

Cited by 39 publications

References 18 publications

INTEGRAL andSwiftobservations of the hard X-ray transient MAXI J1828-249

INTEGRAL andSwiftobservations of the hard X-ray transient MAXI J1828-249

Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

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

Contact Info

Product

Resources

About