INTEGRAL and<i>Swift</i>observations of the hard X-ray transient MAXI J1828-249

Filippova, E.V.; Bozzo, E.; Ferrigno, C.

doi:10.1051/0004-6361/201323337

Cited by 7 publications

(5 citation statements)

References 13 publications

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“…This is reminiscent of that of MAXI J1836−194, which exhibited an incomplete state transition and never reached the high/soft state. Considering all the above results, and presuming that the hysteresis is observed only after the source completed its hard-to-soft state transition, we infer that MAXI J1828−249 stayed in the soft intermediate state and did not reach the genuine high/soft state in the Suzaku observation, as also suggested by Filippova et al (2014). The observed properties of MAXI J1828−249, including the strong hard tail and relatively enhanced variability above ∼ 5 keV, are literally between those in the low/hard state and the high/soft state (table 3).…”

Section: Identification Of the Spectral Statesupporting

confidence: 60%

“…It is hence suggested that the source was evolving through the low/hard state toward the high/soft state, even though a transition to the genuine high/soft state was not clearly recognized. X-ray spectra obtained in this period were characterized with a strong multi-color disk blackbody component and a power-law tail with a photon index of ∼2, seen mainly below and above ∼10 keV, respectively (Filippova et al 2014;Grebenev et al 2016). Then, the flux gradually decreased for ∼100 days down to undetectable levels.…”

Section: Long-term X-ray Evolution In the Outburstmentioning

confidence: 90%

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X-ray and Optical Observations of the Black Hole Candidate MAXI J1828-249

Oda,

Shidatsu,

Nakahira

et al. 2019

Preprint

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We report results from X-ray and optical observations of the Galactic black hole candidate MAXI J1828−249, performed with Suzaku and the Kanata telescope around the X-ray flux peak in the 2013 outburst. The time-averaged X-ray spectrum covering 0.6-168 keV was approximately characterized by a strong multi-color disk blackbody component with an inner disk temperature of ∼0.6 keV, and a power-law tail with a photon index of ∼2.0. We detected an additional structure at 5-10 keV, which can be modelled neither with X-ray reflection on the disk, nor relativistic broadening of the disk emission. Instead, it was successfully reproduced with a Comptonization of disk photons by thermal electrons with a relatively low temperature ( < ∼ 10 keV). We infer that the source was in the intermediate state, considering its long-term trend in the hardness intensity diagram, the strength of the spectral power-law tail, and its variability properties. The low-temperature Comptonization component could be produced in a boundary region between the truncated standard disk and the hot inner flow, or a Comptonizing region that somehow developed above the disk surface. The multi-wavelength spectral energy distribution suggests that the optical and UV fluxes were dominated by irradiated outer disk emission.

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Section: Identification Of the Spectral Statesupporting

confidence: 60%

Section: Long-term X-ray Evolution In the Outburstmentioning

confidence: 90%

X-ray and Optical Observations of the Black Hole Candidate MAXI J1828-249

Oda,

Shidatsu,

Nakahira

et al. 2019

Preprint

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“…During the first two days of the outburst, the source was observed by MAXI to undergo a very rapid transition from a hard to a softer state [348], so that observations of the source in the LHS were limited because of the swiftness of the transition. The rest of the outburst (essentially the HSS) was covered by a joint observation campaign over a wide energy range from 0.6-150 keV by the instruments on Swift and INTEGRAL, although MAXI J1828−249 did not show significant spectral evolution [130], reaching, however, a peak luminosity L ≈ 10 38 ergs s −1 assuming a distance of 8 kpc.…”

Section: Maxi J1828−249mentioning

confidence: 99%

The INTEGRAL view on Black Hole X-ray Binaries

Motta,

Rodriguez,

Jourdain

et al. 2021

Preprint

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INTEGRAL is an ESA mission in fundamental astrophysics that was launched in October 2002. It has been in orbit for over 18 years, during which it has been observing the high-energy sky with a set of instruments specifically designed to probe the emission from hard X-ray and soft γ-ray sources. This paper is devoted to the subject of black hole binaries, which are among the most important sources that populate the high-energy sky. We present a review of the scientific literature based on INTEGRAL data, which has significantly advanced our knowledge in the field of relativistic astrophysics. We briefly summarise the state-of-the-art of the study of black hole binaries, with a particular focus on the topics closer to the INTEGRAL science. We then give an overview of the results obtained by INTEGRAL and by other observatories on a number of sources of importance in the field. Finally, we review the main results obtained over the past 18 years on all the black hole binaries that INTEGRAL has observed. We conclude with a summary of the main contributions of INTEGRAL to the field, and on the future perspectives.

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“…When fitting the broadband spectra, we added the cross-calibration constants between the three instruments to take into account the nonsimultaneity of the observations. A difference of the cross-calibration constants between the JEM-X and ISGRI/IBIS instruments is observed when working with the INTEGRAL data (see, e.g., Filippova et al 2014a).…”

Section: Integral Datamentioning

confidence: 99%

“…It is believed that during an outburst the system must pass from the low/hard to high/soft state and back, exhibiting the intermediate states and a characteristic "q" shape on the hardness-intensity diagram (Belloni and Motta 2016). However, many sources with black hole candidates exhibit the so-called failed outbursts, when the system does not reach the high/soft state (Ferrigno et al 2012(Ferrigno et al , 2014aDel Santo et al 2015; Mereminskiy et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Investigation of the Outburst Activity of the Black Hole Candidate GRS 1739-278

et al. 2019

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We have performed a joint spectral and timing analysis of the outburst of GRS 1739-278 in 2014 based on Swift and INTEGRAL data. We show that during this outburst the system exhibited both intermediate states: hard and soft. Peaks of quasi-periodic oscillations (QPOs) in the frequency range 0.1-5 Hz classified as type-C QPOs have been detected from the system. Using Swift/BAT data we show that after the 2014 outburst the system passed to the regime of mini-outburst activity: apart from the three mini-outbursts mentioned in the literature, we have detected four more mini-outbursts with a comparable (∼20 mCrab) flux in the hard energy band (15-50 keV). We have investigated the influence of the accretion history on the outburst characteristics: the dependence of the peak flux in the hard energy band in the low/hard state on the time interval between the current and previous peaks has been found (for the outbursts during which the system passed to the high/soft state).

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

Cited by 7 publications

References 13 publications

X-ray and Optical Observations of the Black Hole Candidate MAXI J1828-249

X-ray and Optical Observations of the Black Hole Candidate MAXI J1828-249

The INTEGRAL view on Black Hole X-ray Binaries

Investigation of the Outburst Activity of the Black Hole Candidate GRS 1739-278

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