Multiwavelength Observations of the 2002 Outburst of GX 339−4: Two Patterns of X‐Ray–Optical/Near‐Infrared Behavior

Homan, J.; Buxton, M.; Markoff, Sera; Bailyn, Charles D.; Nespoli, E.; Belloni, T.

doi:10.1086/428722

Cited by 194 publications

(277 citation statements)

References 60 publications

Supporting

Mentioning

251

Contrasting

Order By: Relevance

“…Furthermore, radio observations show that the compact jet (at least for V404 Cyg) is maintained in quiescence (Gallo et al 2005). Even if the debate is still open regarding the contribution of the compact jet (Markoff & Nowak 2004;Homan et al 2005;Markoff et al 2006) at high energy, we can check if the jet model could explain the softening of X-ray spectra for BH in quiescence. To explain the X-ray spectra in the hard state, the electron energy distribution should have an energy index of the order of 2.2-2.4 .…”

Section: On the X-ray Emission Of Black Holes In Quiescencementioning

confidence: 93%

“…This may be related to continuous accretion in quiescence or possibly means that this could be the onset of the outburst that was detected by RXTE ASM about 90 days later (Swank 2004). Similarly, RXTE Proportional Counter Array ( PCA) detected the X-ray activity of GX 339À4 during its 2002 outburst at least 40 days before the initial ASM detection ( Homan et al 2005). This probably indicates that the Chandra observations at the lowest level are likely representative of the true quiescent phase of XTE J1550À564 and H1743À322.…”

Section: X-ray Luminosity In Quiescencementioning

confidence: 97%

See 1 more Smart Citation

On the Origin of Black Hole X‐Ray Emission in Quiescence:ChandraObservations of XTE J1550−564 and H1743−322

Corbel

Tomsick

Kaaret

2006

ApJ

112

View full text Add to dashboard Cite

We report the results of observations of the black hole binaries XTE J1550À564 and H1743À322 in their quiescent state using the Chandra X-Ray Observatory. Both sources are detected at their faintest level of X-ray emission ever observed with a 0.5-10 keV unabsorbed luminosity of 2 ; 10 32 (d /5 kpc) 2 ergs s À1 for XTE J1550À564 and 9 ; 10 31 (d /8 kpc) 2 ergs s À1 for H1743À322. These luminosities are in the upper range compared to the faintest levels observed in other black hole systems, possibly related to residual accretion for these sources with frequent outbursts. For XTE J1550À564, the Chandra observations also constrain the X-ray spectrum, as a fit with an absorbed powerlaw model yields a photon index of 2:25 AE 0:08, clearly indicating a softening of the X-ray spectrum at lower luminosities compared to the standard hard state. Similar softening at low luminosity is seen for several black hole transients with orbital periods less than 60 hr. Most of the current models of accreting black holes are able to reproduce such softening in quiescence. In contrast, we find that systems with orbital periods longer than 60 hr appear to have hard spectra in quiescence, and their behavior may be consistent with hardening in quiescence.

show abstract

Section: On the X-ray Emission Of Black Holes In Quiescencementioning

confidence: 93%

Section: X-ray Luminosity In Quiescencementioning

confidence: 97%

On the Origin of Black Hole X‐Ray Emission in Quiescence:ChandraObservations of XTE J1550−564 and H1743−322

Corbel

Tomsick

Kaaret

2006

ApJ

112

View full text Add to dashboard Cite

show abstract

“…Unfortunately, the ASM sensitivity level is well above the quiescent flux level, making it very likely that any extrapolation overestimates the delay. Besides, most of the sources detected by the ASM need to brighten significantly above quiescence to be detected (see, e.g., Homan et al 2005 for more details on this concern). Therefore, the true start of the X-ray outburst could be earlier than t X .…”

Section: An Optical Precursor To the X-ray Outburst?mentioning

confidence: 99%

The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480

Zurita

Torres

Steeghs

et al. 2006

ApJ

View full text Add to dashboard Cite

We present optical and infrared monitoring of the 2005 outburst of the halo black hole X-ray transient XTE J1118+480. We measured a total outburst amplitude of $5:7 AE 0:1 mag in the R band and $5 mag in the infrared J, H, and K s bands. The hardness ratio HR2 (5 12 keV : 3 5 keV ) from the RXTE ASM data is 1:53 AE 0:02 at the peak of the outburst, indicating a hard spectrum. Both the shape of the light curve and the ratio L X (1 10 keV)/L opt resemble the minioutbursts observed in GRO J0422+32 and XTE J1859+226. During early decline, we find a 0.02 mag amplitude variation consistent with a superhump modulation, like the one observed during the 2000 outburst. Similarly, XTE J1118+480 displayed a double-humped ellipsoidal modulation distorted by a superhump wave when settled into a near-quiescence level, suggesting that the disk expanded to the 3:1 resonance radius after outburst, where it remained until early quiescence. The system reached quiescence at R ¼ 19:02 AE 0:03, about 3 months after the onset of the outburst. The optical rise preceded the X-ray rise by at most 4 days. The spectral energy distributions (SEDs) at the different epochs during outburst are all quasi-power laws with F / increasing toward the blue. At the peak of the outburst, we derived ¼ 0:49 AE 0:04 for the optical data alone and ¼ 0:1 AE 0:1 when fitting solely the infrared. This difference between the optical and the infrared SEDs suggests that the infrared is dominated by a different component (a jet?), whereas the optical is presumably showing the disk evolution.

show abstract

“…For instance, Homan et al (2005) find that the infrared emission in the stellarmass black hole GX 339-4 may be jet-based synchrotron radiation. In the stellar-mass black hole XTE J1118+ 480, Hynes et al (2006) find that even the UVemission may be partially due to synchrotron emission.…”

Section: Introductionmentioning

confidence: 99%

SwiftObservations of the Cooling Accretion Disk of XTE J1817−330

Rykoff

Miller

Steeghs

et al. 2007

ApJ

139

181

View full text Add to dashboard Cite

The black hole candidate X-ray transient XTE J1817À330 was observed by the Swift satellite over 160 days of its 2006 outburst with the XRT and UVOT instruments. At the start of the observations, the XRT spectra show that the 0.6Y10 keV emission is dominated by an optically thick, geometrically thin accretion disk with an inner disk temperature of $0.8 keV, indicating that the source was in a high /soft state during the initial outburst phase. We tracked the source through its decline into the low/ hard state with the accretion disk cooling to $0.2 keV and the inner disk radius consistent with the innermost stable circular orbit at all times. Furthermore, the X-ray luminosity roughly follows L X / T 4 during the decline, consistent with a geometrically stable blackbody. These results are the strongest evidence yet obtained that accretion disks do not automatically recede after a state transition, down to accretion rates as low as 0:001L Edd . Meanwhile, the near-UV flux does not track the X-ray disk flux and is well in excess of what is predicted if the near-UVemission is from viscous dissipation in the outer disk. The strong correlation between the hard X-ray flux and the near-UV flux, which scale as L 0:5 X , indicate that reprocessed emission is most likely the dominate contribution to the near-UV flux. We discuss our results in the context of accretion disks and the overall accretion flow geometry in accreting black holes.

show abstract

Multiwavelength Observations of the 2002 Outburst of GX 339−4: Two Patterns of X‐Ray–Optical/Near‐Infrared Behavior

Cited by 194 publications

References 60 publications

On the Origin of Black Hole X‐Ray Emission in Quiescence:ChandraObservations of XTE J1550−564 and H1743−322

On the Origin of Black Hole X‐Ray Emission in Quiescence:ChandraObservations of XTE J1550−564 and H1743−322

The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480

SwiftObservations of the Cooling Accretion Disk of XTE J1817−330

Contact Info

Product

Resources

About