The proportional counter array (PCA) instrument for the X-ray timing explorer satellite (XTE)

Gläßer, Cornelia; Odell, C.E.; Seufert, S.E.

doi:10.1109/23.322911

Cited by 23 publications

(22 citation statements)

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“…These correspond to time periods during which the source spectra appear quite stable, with very small or absent spectral variability as monitored on the time scale of a few SCWs. We searched simultaneous IBIS and PCA (Glasser et al 1994) data in the XTE public archive 2 , but unfortunately only for epoch 1 PCA standard products are available. No public PCA data are available for the epoch 2, 3 and 4 .…”

Section: Observations and Data Analysismentioning

confidence: 99%

RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITHINTEGRAL

Fiocchi¹,

Natalucci²,

Chenevez³

et al. 2009

ApJ

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We report on the results of INTEGRAL observations of the neutron star low mass X-ray binary SAX J1810.8-2609 during its latest active phase in August 2007. The current outburst is the first one since 1998 and the derived luminosity is 1.1 − 2.6 × 10 36 erg s −1 in the 20-100 keV energy range. This low outburst luminosity and the long-term time-average accretion rate of ∼ 5 × 10 −12 M ⊙ yr −1 suggest that SAX J1810.8-2609 is a faint soft X-ray transient. During the flux increase, spectra are consistent with a thermal Comptonization model with a temperature plasma of kT e ∼ 23-30 keV and an optical depth of τ ∼ 1.2-1.5, independent from luminosity of the system. This is a typical low hard spectral state for which the X-ray emission is attributed to the upscattering of soft seed photons by a hot, optically thin electron plasma. During the decay, spectra have a different shape, the high energy tail being compatible with a single power law. This confirm similar behavior observed by BeppoSAX during the previous outburst, with absence of visible cutoff in the hard X-ray spectrum. INTEGRAL/JEM-X instrument observed four X-ray bursts in Fall 2007. The first one has the highest peak flux (≈ 3.5 Crab in 3-25 keV) giving an upper limit to the distance of the source of about 5.7 kpc, for a L Edd ≈ 3.8 × 10 38 erg s −1 . The observed recurrence time of ∼1.2 days and the ratio of the total energy 1 INTEGRAL is an ESA project with instruments and science data center funded by ESA member states (especially the PI countries:

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Section: Observations and Data Analysismentioning

confidence: 99%

RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITHINTEGRAL

Fiocchi¹,

Natalucci²,

Chenevez³

et al. 2009

ApJ

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“…Each PCU contains three multianode detector layers with a mixture of xenon and methane gas, has a bandpass of 2-60 keV and a geometric collecting area of 1400 cm 2 . The energy resolution of each detector is 8% FWHM at 6.6 keV (Glasser, Odell, & Seufert 1994). PCA data were collected only from PCUs 0-2, since PCUs 3 and 4 were turned on for a smaller fraction of the on-source time due to breakdown.…”

Section: Rxtementioning

confidence: 99%

SimultaneousEUVE/ASCA/RXTEObservations of NGC 5548

Chiang¹,

Reynolds²,

Blaes³

et al. 2000

ApJ

142

179

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We present simultaneous observations by EUVE, ASCA, and RXTE of the type 1 Seyfert galaxy NGC 5548. These data indicate that variations in the EUV emission (at 0 2 keV) appear to lead similar modulations in higher energy (1 keV) X-rays by 10-30 ks. This is contrary to popular models which attribute the correlated variability of the EUV, UV and optical emission in type 1 Seyferts to reprocessing of higher energy radiation. This behavior instead suggests that the variability of the optical through EUV emission is an important driver for the variability of the harder X-rays which are likely produced by thermal Comptonization. We also investigate the spectral characteristics of the fluorescent iron K« line and Compton reflection emission. In contrast to prior measurements of these spectral features, we find that the iron K« line has a relatively small equivalent width (W K« 100 eV) and that the reflection component is consistent with a covering factor which is significantly less than unity (ª 2 0 4-0.5). Notably, although the 2-10 keV X-ray flux varies by ¦ 25% and the derived reflection fraction appears to be constant throughout our observations, the flux in the Fe K« line is also constant. This behavior is difficult to reconcile in the context of standard Compton reflection models.

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“…They are also equipped with a collimator providing the same field of view for all the PCUs (#1°). The five proportional counters give a total collecting area of #6500 cm 2 , an energy resolution of 18 per cent at 6 keV and a time resolution of 1 s. A detailed description of the Proportional Counter Array Instrument can be found in Glasser, Odell & Seufert (1994).…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

Timing properties of the X-ray pulsar EXO 2030+375 during an X-ray outburst

Reig

Coe

1998

Monthly Notices of the Royal Astronomical Society

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We present Rossi X‐ray Timing Explorer (RXTE) observations of the Be/X‐ray transient EXO 2030+375 during an outburst after a period of quiescence between 1993 August and 1996 April. When active, EXO 2030+375 is normally detected at each periastron passage of the neutron star. Our observations correspond to the third periastron passage after the source ‘turned on’ again. All outbursts after the quiescent period, including the one reported here, have been occurring at a much earlier binary phase than in the past. We discuss the possible mechanisms that may explain this shift in the onset of the outburst. Pulsations in the X‐ray radiation are detected throughout the entire run. The neutron star spun up during the outburst at a rate of −1.16×10−8 s s−1, but no variations in the shape of the pulse profile as a function of intensity were seen. A correlation between the hardness ratio and the intensity is observed at low energies (6–12/2–6 keV). By comparing the magnetospheric and corotation radii we argue that the neutron star spins at a rate close to the equilibrium period. Finally, we perform pulse‐phase spectroscopy and comment on changes seen as a function of spin phase.

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The proportional counter array (PCA) instrument for the X-ray timing explorer satellite (XTE)

Cited by 23 publications

References 0 publications

RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITHINTEGRAL

RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITHINTEGRAL

SimultaneousEUVE/ASCA/RXTEObservations of NGC 5548

Timing properties of the X-ray pulsar EXO 2030+375 during an X-ray outburst

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