A Thermal Wind Model for the X-Ray Outflow in GRO J1655-40

Netzer, H.

doi:10.1086/510067

Cited by 36 publications

(68 citation statements)

References 12 publications

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“…code ION (Netzer 2006) with an H-atom containing 40 levels, solar abundances, hydrogen density of 10 10 cm −3 , column density of 10 23 cm −2 and ionization parameter of 10 −1.5 . The exact shape is insensitive to the exact value of these parameters and the normalization is done by direct fits to the observations.…”

Section: Thin Disk Continuum Approachmentioning

confidence: 99%

Active galactic nuclei atz∼ 1.5 – II. Black hole mass estimation by means of broad emission lines

Mejía-Restrepo

Trakhtenbrot

Lira

et al. 2016

Mon. Not. R. Astron. Soc.

136

153

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This is the second in a series of papers aiming to test how the mass (M BH ), accretion rate (Ṁ ) and spin (a * ) of super massive black holes (SMBHs) determine the observed properties of type-I active galactic nuclei (AGN). Our project utilizes a sample of 39 unobscured AGN at z 1.55 observed by VLT/X-shooter, selected to map a large range in M BH and L/L Edd and covers the most prominent UV-optical (broad) emission lines, including Hα, Hβ, Mg II λ2798, and C IV λ1549. This paper focuses on single-epoch, "virial" M BH determinations from broad emission lines and examines the implications of different continuum modeling approaches in line width measurements. We find that using a local power-law continuum instead of a physically-motivated thin disk continuum leads to only slight underestimation of the FWHM of the lines and the associated M BH (FWHM). However, the line dispersion σ line and associated M BH (σ line ) are strongly affected by the continuum placement and provides less reliable mass estimates than FWHM-based methods. Our analysis shows that Hα, Hβ and Mg II can be safely used for virial M BH estimation. The C IV line, on the other hand, is not reliable in the majority of the cases, this may indicate that the gas emitting this line is not virialized. While Hα and Hβ show very similar line widths, the mean FWHM(Mg II) is about 30% narrower than FWHM(Hβ). We confirm several recent suggestions to improve the accuracy in C IV-based mass estimates, relying on other UV emission lines. Such improvements do not reduce the scatter between C IV-based and Balmer-line-based mass estimates.

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Section: Thin Disk Continuum Approachmentioning

confidence: 99%

Active galactic nuclei atz∼ 1.5 – II. Black hole mass estimation by means of broad emission lines

Mejía-Restrepo

Trakhtenbrot

Lira

et al. 2016

Mon. Not. R. Astron. Soc.

136

153

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“…From a detailed analysis of the absorption line profile, they detected multiple components in the wind, where a more ionized part was located at a smaller radius. After Miller et al (2006) first reported the Chandra/HETG result, the unusual wind in GRO J1655−40 has been revisited many times from both observational and theoretical points of view (Netzer 2006;Miller et al 2008;Kallman et al 2009;Luketic et al 2010;Neilsen & Homan 2012;Higginbottom & Proga 2015). Many previous studies were based on the assumption that the wind was optically thin and launched at a few percent of the Eddington luminosity, in constructing photoionized plasma models and performing hydrodynamic simulations.…”

Section: Where Is the Hidden Compton-thick Wind Located?mentioning

confidence: 99%

“…In 2005, a remarkable wind from GRO J1655−40 was detected with the Chandra High Energy Transmission Grating (HETG) (Miller et al 2006(Miller et al , 2008Netzer 2006). The observed spectrum exhibited a rich forest of blueshifted ionized absorption lines.…”

Section: Introductionmentioning

confidence: 99%

An Optically Thick Disk Wind in Gro J1655–40?

Shidatsu

Done

Ueda

2016

ApJ

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The 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-pro t 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 revisited the unusual wind in GRO J1655−40, detected with Chandra in 2005 April, using long-term Rossi X-ray Timing Explorer X-ray data and simultaneous optical/near-infrared photometric data. This wind is the most convincing case for magnetic driving in black hole binaries, as it has an inferred launch radius that is a factor of 10 smaller than the thermal wind prediction. However, the optical and near-infrared (OIR) fluxes monotonically increase around the Chandra observation, whereas the X-ray flux monotonically decreases from 10 days beforehand. Yet the optical and near-infrared fluxes are from the outer, irradiated disk, so for them to increase implies that the X-rays likewise increased. We applied a new irradiated disk model to the multi-wavelength spectral energy distributions. Fitting the OIR fluxes, we estimated the intrinsic luminosity at the Chandra epoch was  L 0.7 Edd , which is more than one order of magnitude larger than the observed X-ray luminosity. These results could be explained if a Compton-thick, almost completely ionized gas was present in the wind and strong scattering reduced the apparent X-ray luminosity. The effects of scattering in the wind should then be taken into account for discussion of the wind-driving mechanism. Radiation pressure and Compton heating may also contribute to powering the wind at this high luminosity.

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“…Most follow up studies have supported the magnetic origin of the wind (Neilsen & Homan 2012, and references therein). However, thermally-driven winds remain a possibility (Netzer 2006). …”

Section: Introductionmentioning

confidence: 99%

Wind, jet, hybrid corona and hard X-ray flares: multiwavelength evolution of GRO J1655−40 during the 2005 outburst rise

Kalemci¹,

Begelman²,

Maccarone³

et al. 2016

Mon. Not. R. Astron. Soc.

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We have investigated the complex multiwavelength evolution of GRO J1655−40 during the rise of its 2005 outburst. We detected two hard X-ray flares, the first one during the transition from the soft state to the ultra-soft state, and the second one in the ultra-soft state. The first X-ray flare coincided with an optically thin radio flare. We also observed a hint of increased radio emission during the second X-ray flare. To explain the hard flares without invoking a secondary emission component, we fit the entire data set with the eqpair model. This single, hybrid Comptonization model sufficiently fits the data even during the hard X-ray flares if we allow reflection fractions greater than unity. In this case, the hard X-ray flares correspond to a Comptonizing corona dominated by non-thermal electrons. The fits also require absorption features in the soft and ultra-soft state which are likely due to a wind. In this work we show that the wind and the optically thin radio flare co-exist. Finally, we have also investigated the radio to optical spectral energy distribution, tracking the radio spectral evolution through the quenching of the compact jet and rise of the optically thin flare, and interpreted all data using state transition models.

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A Thermal Wind Model for the X-Ray Outflow in GRO J1655-40

Cited by 36 publications

References 12 publications

Active galactic nuclei atz∼ 1.5 – II. Black hole mass estimation by means of broad emission lines

Active galactic nuclei atz∼ 1.5 – II. Black hole mass estimation by means of broad emission lines

An Optically Thick Disk Wind in Gro J1655–40?

Wind, jet, hybrid corona and hard X-ray flares: multiwavelength evolution of GRO J1655−40 during the 2005 outburst rise

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