&lt;title&gt;In-orbit performance and calibration of the Rossi X-ray Timing Explorer (RXTE) Proportional Counter Array (PCA)&lt;/title&gt;

Jahoda, K.; Swank, J. H.; Giles, A. B.; Stark, M. J.; Strohmayer, Tod E.; Zhang, William W.; Morgan, E.

doi:10.1117/12.256034

Cited by 532 publications

(84 citation statements)

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“…The cyan line represents MJD 55963, the approximate time IGR J17091-3624 transitions from the soft to the hard state (Drave et al 2012). RXTE /PCA (Jahoda et al 1996) data are for the 2-16 keV energy band and taken from (Altamirano et al 2011a), Swift/BAT (Barthelmy 2000) data are for 15-50 keV, Swift/XRT (Burrows et al 2003) data are for 0.3-10 keV and INTEGRAL/ISGRI (Ubertini et al 2003) data are for 20-40 keV. Note that the data from Swift/XRT (Panel B) are shown with a logarithmic y-axis to better show the late time progression of the outburst.…”

Section: Rxtementioning

confidence: 99%

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An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

Court

Altamirano

Pereyra

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We performed an analysis of all RXTE observations of the Low Mass X-ray Binary and Black Hole Candidate IGR J17091-3624 during the 2011-2013 outburst of the source. By creating lightcurves, hardness-intensity diagrams and power density spectra of each observation, we have created a set of 9 variability 'classes' that phenomenologically describe the range of types of variability seen in this object. We compare our set of variability classes to those established by Belloni et al. (2000) to describe the similar behaviour of the LMXB GRS 1915+105, finding that some types of variability seen in IGR J17091-3624 are not represented in data of GRS 1915+105. We also use all available X-ray data of the 2011-2013 outburst of IGR J17091-3624 to analyse its longterm evolution, presenting the first detection of IGR J17091-3624 above 150 keV as well as noting the presence of 're-flares' during the latter stages of the outburst. Using our results we place new constraints on the mass and distance of the object, and find that it accretes at 33% of its Eddington limit. As such, we conclude that Eddingtonlimited accretion can no longer be considered a sufficient or necessary criterion for GRS 1915+105-like variability to occur in Low Mass X-Ray Binaries.

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Section: Rxtementioning

confidence: 99%

“…For our variability study, we focus on the data from the Proportional Counter Array (PCA, Jahoda et al 1996) aboard the Rossi X-Ray Riming Experiment (RXTE, Bradt et al 1993). We analysed all 2011 PCA observations of IGR J17091, corresponding to OBSIDs 96065-03, 96103-01 and 96420-01.…”

Section: Rxtementioning

confidence: 99%

An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

Court

Altamirano

Pereyra

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…In this study we have used all public pointed observations, with data from the Proportional Counter Array (PCA, Jahoda et al 1996). The PCA consists of five identical Proportional Counter Units (PCUs), and is sensitive in the 2-60 keV energy range.…”

Section: The Archival Datamentioning

confidence: 99%

Evolution of the 0.01–25 Hz power spectral components in Cygnus X-1

Axelsson¹,

Borgonovo²,

Larsson³

2005

A&A

112

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Abstract. Analyzing the archival data from the Rossi X-ray Timing Explorer (RXTE), we study the power density spectra (PDS) of Cygnus X-1 from 1996 to 2003 in the frequency range of 0.01-25 Hz. Using a model consisting of one or two Lorentzians and/or an exponentially cut-off power-law, we are able to achieve a good fit to the PDS during the observations. With our model we are also able to track the evolution of the Lorentzian components through all spectral states of the source. We confirm the relation between characteristic frequencies seen both in black hole candidate and neutron star sources, and show the changes in this relation during the transitional and soft states of the source. The connection between the Lorentzian components is investigated by analyzing similarities and differences in their behavior. We find that the spectral state of the source can be uniquely determined from the parameters of these components. The parameter correlations can all be described by continuous functions, which differ between components. We discuss our results in the context of relativistic precession model for the accretion disk, and show a remarkable agreement between the model prediction and the data in the hard state. We estimate a value for the specific angular momentum of a * = 0.49 (−0.57) in the case of prograde (retrograde) rotation and an estimate for the inner radius of 22 to 50 (25 to 55) gravitational radii. Additional assumptions are required to explain the soft state data, and attempting to invoke rotational reversal for state transitions shows that it is insufficient to explain the differences between the hard and soft state data.

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“…The PCA consists of an array of five collimated xenon/methane multi-anode proportional counter units (PCUs) operating in the 2−60 keV range, with a total effective area of approximately 6500 cm 2 and a field of view of ∼1 • FWHM (Jahoda et al 1996). Our 136 observations are of various lengths (see Table 1).…”

Section: Observationsmentioning

confidence: 99%

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Dib¹,

Kaspi²,

Gavriil³

2007

Isolated Neutron Stars: From the Surface to the Interior

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We report on 10 years of monitoring of the 8.7-s Anomalous X-ray Pulsar 4U 0142+61 using the Rossi X-Ray Timing Explorer (RXTE). This pulsar exhibited stable rotation from 2000 March until 2006 February: the RMS phase residual for a spin-down model which includes ν, ν, and ν is 2.3%. We report a possible phase-coherent timing solution valid over a 10-yr span extending back to March 1996. A glitch may have occured between 1998 and 2000, but is not required by the existing timing data. The pulse profile has been evolving since 2000. In particular, the dip of emission between its two peaks got shallower between 2002 and 2006, as if the profile were evolving back to its pre-2000 morphology, following an earlier event, which possibly also included the glitch suggested by the timing data. These profile variations are seen in the 2−4 keV band but not in 6−8 keV. We also detect a slow increase in the pulsed flux between 2002 May and 2004 December, such that it has risen by 36±3% over 2.6 years in the 2−10 keV band. The pulsed flux variability and the narrow-band pulse profile changes present interesting challenges to aspects of the magnetar model.

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<title>In-orbit performance and calibration of the Rossi X-ray Timing Explorer (RXTE) Proportional Counter Array (PCA)</title>

Cited by 532 publications

References 0 publications

An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

Evolution of the 0.01–25 Hz power spectral components in Cygnus X-1

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

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