Black Hole Mass Determination in the X-Ray Binary 4u 1630-47: Scaling of Spectral and Variability Characteristics

Seifina, Elena; Titarchuk, L.; Shaposhnikov, Nikolai

doi:10.1088/0004-637x/789/1/57

Cited by 53 publications

(70 citation statements)

References 88 publications

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“…Consequently, when using model C to fit Obs 1-4 we found that the Γ parameter artificially increases to values > 5 and therefore we decide to fix it to an acceptable value of 2.5. Seifina et al (2014) reported Γ values up to 3 by analyzing RXTE observations along multiple accretion states, although given that our Γ value obtained from the more physical model simpl is < 2.0 we have considered that Γ = 3.0 is a bit too large. On the other hand, the fit obtained using models C, D for Obs 7 tend to decrease N (H) to unrealistic values (i.e < 0.01 ×10 22 cm −2 ).…”

Section: Continuum Modelingmentioning

confidence: 99%

Chandrahigh-resolution spectra of 4U 1630-47: the disappearance of the wind

Gatuzz

Trigo²,

Miller-Jones

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the analysis of six Chandra X-ray high-resolution observations of the black hole low-mass X-ray binary 4U 1630-47 taken during its 2012-2013 outburst. Fe XXVI Kα, Kβ, Fe XXV Kα, Kβ and Ca XX Kα blueshifted absorption lines were identified in the first four observations, which correspond to soft accretion states. The remaining observations, associated to intermediate and possibly hard accretion states, do not show significant absorption features down to equivalent width of 1 eV for both Fe XXVI and Fe XXV. We inferred wind launching radii between 1.2 − 2.0 (10 12 cm/n)×10 11 cm and column densities N (H) > 10 23 cm −2 . In the first four observations we found that thermal pressure is likely to be the dominant launching mechanism for the wind, although such conclusions depend on the assumed density. We used the spectral energy distributions obtained from our continuum modeling to compute thermal stability curves for all observations using the xstar photoionization code. We found that the absence of lines in the transitional state cannot be attributed to an evolution of the plasma caused by thermal instabilities derived from the change in the continuum spectrum. In contrast, the disappearance of the wind could indicate an acceleration of the flow or that the plasma has been exhausted during the soft state.

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Section: Continuum Modelingmentioning

confidence: 99%

Chandrahigh-resolution spectra of 4U 1630-47: the disappearance of the wind

Gatuzz

Trigo²,

Miller-Jones

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…We computed the detectability in individual observations for each source in our sample and considered those suitable for a pulsar search, with > ( ) f min 50% p at the s 3 level. For the three brightest sources in the Norma survey, the timing properties are already presented elsewhere: (i) the quasi-periodic oscillations of the BH binary 4U1630-472 (NNR 1), extensively studied using the Rossi X-Ray Timing Explorer (Dieters et al 2000;Tomsick & Kaaret 2000;Seifina et al 2014); (ii) the HMXB pulsar IGRJ16393-4643 (NNR 2), with a period of 904 s, whose spin-up rate was determined from recent NuSTAR observations (B16); and (iii) the NuSTARdiscovered 206ms pulsar PSRJ1640−4631 (NNR 3), associated with the TeV source HESSJ1640−465 (G14; Archibald et al 2016).…”

Section: X-ray Variabilitymentioning

confidence: 99%

The NuSTAR Hard X-Ray Survey of the Norma Arm Region

Fornasini

Tomsick

Hong

et al. 2017

ApJS

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Citation for published item:pornsiniD prnes wF nd omsikD tohn eF nd rongD teu nd qotthelfD iri F nd fuerD prnz nd houiD prid nd ternD hniel nd fodgheeD ersh nd ghiuD tengEvun nd glvelD w¤ % nd gorrlEntnD tes¡ us nd rileyD ghrles tF nd urivonosD omn eF nd woriD uy nd elexnderD hvid wF nd frretD hidier nd foggsD teven iF nd ghristensenD pinn iF nd grigD illim F nd porsterD url nd qiommiD olo nd qrefenstetteD frin F nd rrrisonD pion eF nd rornstrupD elln nd uitguhiD ko nd uoglinD tF iF nd wdsenD uristin uF nd woD eter rF nd wiyskD riroms nd erriD wtteo nd ivovro'D wihel tF nd uettiD imonett nd nD ikrm nd estergrdD xiels tF nd hngD illim F @PHIUA 9he xue hrd Ery survey of the xorm rm regionF9D estrophysil journl supplement seriesFD PPW @PAF pF QQF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present a catalog of hard X-ray sources in a square-degree region surveyed by the Nuclear Spectroscopic Telescope Array (NuSTAR) in the direction of the Norma spiral arm. This survey has a total exposure time of 1.7 Ms, and the typical and maximum exposure depths are 50 ks and 1 Ms, respectively. In the area of deepest coverage, sensitivity limits of 5×10 −14 and 4×10 −14 ergs −1 cm −2 in the 3-10 and 10-20keV bands, respectively, are reached. Twenty-eight sources are firmly detected, and 10 are detected with low significance; 8 of the 38 sources are expected to be active galactic nuclei. The three brightest sources were previously identified as a low-mass X-ray binary, high-mass X-ray binary, and pulsar wind nebula. Based on their X-ray properties and multiwavelength counterparts, we identify the likely nature of the other sources as two colliding wind binaries, three pulsar wind nebulae, a black hole binary, and a plurality of cataclysmic variables (CVs). The CV candidates in the Norma region have plasma temperatures of ≈10-20keV, consistent with the Galactic ridge X-ray emission spectrum but lower than the temperatures of CVs near the Galactic center. This temperature difference may indicate that the Norma region has a lower fraction of intermediate polars relative to other types of CVs compared to the Galactic center. The NuSTAR logN-logS distribution in the 10-20keV band is consistent with the distribution measured by Chandra at 2-10keV if the average source spectrum is assumed to be a thermal model with kT≈15 keV, as observed for the CV candidates.

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“…Tomsick et al (1998) estimated a mass of 3 M for the BH in 4U 1630−47, based on the assumption that the maximum flux observed during outbursts (Parmar et al 1995) corresponded to the Eddington luminosity at a distance of 10 kpc. However, Seifina et al (2014) have recently estimated a mass of 10 M , based on scaling techniques and taking as reference sources GRO J1655−40, H 1743−322 and XTE J1550−564. We find that the wind in 4U 1630−47 can be launched via a thermal mechanism even if the mass of the BH is larger than 3 M .…”

Section: Wind Launching Mechanismmentioning

confidence: 99%

XMM-Newtonobservations reveal the disappearance of the wind in 4U 1630−47

Trigo¹,

Migliari

Miller-Jones

et al. 2014

A&A

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We report on XMM-Newton observations of the black hole X-ray binary 4U 1630−47 during its 2012−2013 outburst. The first five observations monitor the source as its luminosity increases across the high−soft state of accretion. In the sixth observation the source has made a transition to an "anomalous" state, characterised by a significant contribution of electron scattering. A thermally/radiatively driven disc wind is present in the first four observations, which becomes more photoionised as the luminosity increases with time. In the fifth observation, the wind is not observed any more as a consequence of strong photoionisation and the low sensitivity of this observation. This overall trend is then consistent with a fully ionised wind causing the electron scattering characteristic of the anomalous state in the sixth observation. A broad iron emission line co-exists with the absorption features from the wind in the first four observations but is not visible in the last two observations. We find that the changes in the state of the wind as measured from modelling the absorption features with a self-consistent warm absorber model are correlated to the changes in the broad iron line. When the latter is modelled with a reflection component we find that the reflection fraction decreases as the illumination increases. We propose that the changes in both the absorption and broad emission lines are caused by the increasing luminosity and temperature of the accretion disc along the soft state. Such changes ultimately enable the transition to a state where the wind is fully ionised and consequently Comptonisation plays a significant role.

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Black Hole Mass Determination in the X-Ray Binary 4u 1630-47: Scaling of Spectral and Variability Characteristics

Cited by 53 publications

References 88 publications

Chandrahigh-resolution spectra of 4U 1630-47: the disappearance of the wind

Chandrahigh-resolution spectra of 4U 1630-47: the disappearance of the wind

The NuSTAR Hard X-Ray Survey of the Norma Arm Region

XMM-Newtonobservations reveal the disappearance of the wind in 4U 1630−47

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