The <i>INTEGRAL</i> Science Data Centre (ISDC)

Courvoisier, T. J. L.; Walter, R.; Beckmann, V.; Dean, A. J.; Dubath, P.; Hudec, R.; Kretschmar, P.; Mereghetti, S.; Montmerle, T.; Mowlavï, N.; Paltani, S.; Martinez, A. Preite; Produit, N.; Staubert, R.; Strong, A. W.; Swings, Jean-Pierre; Westergaard, N. J.; White, N. E.; Winkler, Christoph; Zdziarski, A. A.

doi:10.1051/0004-6361:20031172

Cited by 393 publications

(357 citation statements)

References 15 publications

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“…27) as input source catalog. We processed the ISGRI and JEM-X data using the latest available Off-line Scientific Analysis software (OSA; see Courvoisier et al 2003), v. 7.0. The description of the algorithms used in the ISGRI and JEM-X scientific analyses can be found in Goldwurm et al (2003) and Westergaard et al (2003), respectively.…”

Section: Integral Ibis/isgri and Jem-xmentioning

confidence: 99%

What ignites on the neutron star of 4U 0614+091?

Kuulkers¹,

Zand

Atteia

et al. 2010

A&A

103

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The low-mass X-ray binary 4U 0614+091 is a source of sporadic thermonuclear (type I) X-ray bursts. We find bursts with a wide variety of characteristics in serendipitous wide-field X-ray observations by the WATCH on EURECA, the ASM on RXTE, the WFCs on BeppoSAX, the FREGATE on HETE-2, the IBIS/ISGRI on INTEGRAL, and the BAT on Swift, as well as pointed observations with the PCA and HEXTE on RXTE. Most of the bursts are bright, i.e., they reach a peak flux of about 15 Crab, but a few are weak and only reach a peak flux below a Crab. One of the bursts shows a very strong photospheric radius-expansion phase. This allows us to evaluate the distance to the source, which we estimate to be 3.2 kpc. The burst durations vary generally from about 10 s to 5 min. However, after one of the intermediate-duration bursts, a faint tail is seen to at least about 2.4 h after the start of the burst. One very long burst was observed, which lasted for several hours. This superburst candidate was followed by a normal type-I burst only 19 days later. This is, to our knowledge, the shortest burst-quench time among the superbursters. The observation of a superburst in this system is difficult to reconcile if the system is accreting at about 1% of the Eddington limit. We describe the burst properties in relation to the persistent emission. No strong correlations are apparent, except that the intermediate-duration bursts occurred when 4U 0614+091's persistent emission was lowest and calm, and when bursts were infrequent (on average roughly one every month to 3 months). The average burst rate increased significantly after this period. The maximum average burst recurrence rate is about once every week to 2 weeks. The burst behaviour may be partly understood if there is at least an appreciable amount of helium present in the accreted material from the donor star. If the system is an ultra-compact X-ray binary with a CO white-dwarf donor, as has been suggested, this is unexpected. If the bursts are powered by helium, we find that the energy production per accumulated mass is about 2.5 times less than expected for pure helium matter.

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Section: Integral Ibis/isgri and Jem-xmentioning

confidence: 99%

What ignites on the neutron star of 4U 0614+091?

Kuulkers¹,

Zand

Atteia

et al. 2010

A&A

103

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“…We achieved a serendipitous detection of PKS 2149-306 using the INTEGRAL public archive data; the source was in the IBIS (Ubertini et al 2003) (Courvoisier et al 2003). The imaging analysis of IBIS/ISGRI data (Goldwurm et al 2003) provided a source detection of signal-to-noise ratio S /N = 4 in the 20−100 keV energy band with exposure of 366 ks.…”

Section: Integralmentioning

confidence: 99%

The changing look of PKS 2149-306

Bianchin¹,

Foschini²,

Ghisellini

et al. 2009

A&A

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Aims. We study the blazar nature of the high-redshift Flat-Spectrum Radio Quasar PKS 2149-306 (z = 2.345) by investigating its long-term behavior. Methods. We analyzed all publicly available optical-to-X-ray observations performed by XMM-Newton, Swift, and INTEGRAL. Results. PKS 2149-306 is one of four blazars at z > 2 that have been observed in the hard-X-ray regime with both the BAT and ISGRI instruments. Observations acquired almost 1 year apart in the 60−300 keV energy band in the object rest frame, exhibit no noticeable change in spectral slope associated with a flux variation of more than a factor of two. Swift data appear to show a roll-off below ∼1 keV, which becomes increasingly evident during a ∼3-day time-frame, that can be explained as the natural spectral break caused by the Inverse Compton onset. The broad-band spectra allow us to identify two different states. The SED modeling suggests that they can be interpreted by only a change in the bulk Lorentz factor of the jet.

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“…Among the 14 Seyfert 1 galaxies of our sample, several objects have in fact intermediate Seyfert types. NGC 1386, NGC 2992, NGC 5033 are Seyfert 1.9 but their X-ray spectra do not show significant absorption (Dadina 2008;Terashima et al 1999). NGC 3227 and NGC 4151 are Seyfert 1.5 with complex and variable absorption (Gondoin et al 2003;Zdziarski et al 2002).…”

Section: Source Samplementioning

confidence: 95%

“…The ISGRI data were reduced using the INTEGRAL Offline Scientific Analysis software 2 version 7.0 publicly released by the INTEGRAL Science Data Centre (Courvoisier et al 2003). Individual sky images for each pointing have been produced in a broad energy band of 18-80 keV.…”

Section: Integral Data and Analysismentioning

confidence: 99%

The hard X-ray view of bright infrared galaxies

Walter

Cabral

2009

A&A

Self Cite

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Aims. The synthesis of the cosmic X-ray background (CXB) requires a large population of Compton-thick active galactic nuclei that have not been detected so far. We probe whether bright infrared galaxies could harbor a population of Compton-thick nuclei and if they could contribute significantly. Methods. We analyzed 112 Ms of INTEGRAL observations obtained on 613 galaxies from the IRAS Revised Bright Galaxy Sample. We derived the average hard X-ray (18-80 keV) emission of Seyfert and various non Seyfert galaxy subsamples to estimate their relative contribution to the locally emitted CXB. Results. The Seyfert 1 & 2 are detected at hard X-rays. None of the other galaxy subsamples were detected. ULIRGs are at least 5 times under-luminous at hard X-rays when compared to Seyferts. The upper limit obtained for the average non Seyfert galaxies is as low as 7 × 10 −13 erg s −1 cm −2 . On average, these galaxies do not contain active nuclei brighter than 10 41 erg s −1 at hard X-rays. The total hard X-ray flux detected from the sample is 4.9 × 10 −9 erg s −1 cm −2 (about 1% of the CXB), and 64% of this originates in absorbed active nuclei. Local non-Seyfert galaxies contribute for less than 7% and do not harbor the Compton-thick nuclei assumed to synthesize the locally emitted CXB.

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The INTEGRAL Science Data Centre (ISDC)

Cited by 393 publications

References 15 publications

What ignites on the neutron star of 4U 0614+091?

What ignites on the neutron star of 4U 0614+091?

The changing look of PKS 2149-306

The hard X-ray view of bright infrared galaxies

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