The<i>Beppo</i>SAX WFC X-ray source catalogue

Verrecchia, F.; Zand, J. J. M. in ’t; Giommi, P.; Santolamazza, P.; Granata, S.; Schuurmans, Jaap; Antonelli, L. A.

doi:10.1051/0004-6361:20067040

Cited by 30 publications

(33 citation statements)

References 28 publications

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“…The total 2−10 keV soft X-ray luminosity in Arp220 is L Arp220 ∼ 7 × 10 40 erg s −1 (Iwasawa et al 2001(Iwasawa et al , 2011 corresponding to 225 × L GRS_1915+105 (Verrecchia et al 2007) and is therefore consistent with this total population size. Finally assuming a star-formation rate of 200 M yr −1 over a continuous burst lasting >10 Myr then at near solar metallicity Linden et al (2010) predict 2000 X-ray binaries brighter than GRS 1915+105 luminosity, more than enough to explain the required size of the parent population.…”

Section: Microblazarssupporting

confidence: 67%

Rapid variability of the compact radio sources in Arp220

Batejat¹,

Conway²,

Rushton³

et al. 2012

A&A

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Context. The two nuclei of the starburst galaxy Arp220 contain multiple compact radio sources previously identified as radio supernovae or supernova remnants. Aims. In order to search for an embedded radio AGN, or other possible exotic objects, we have carried out a programme of VLBI monitoring at 6 cm over three epochs each separated by four months. Methods. Combining the new data with existing data at 6 cm and 18 cm (spanning 4 and 12 years respectively) we are able to characterise source flux density variability on a range of timescales. Additionally we analyse the variability of sources in shape and position. Results. We detect rapid (<4 months) variability in three sources (W7, W26, and W29). These sources show possible superluminal motion (>4c) of jet-like features near rapidly varying almost stationary components. These enigmatic sources might be associated with an AGN or a highly beamed microquasar (i.e. microblazar). Other hypotheses include that the apparent variability is intrinsic and is produced by neutron star powered central components within a supernova remnant, by a sequence of several supernovae within super star clusters, or is extrinsic and is produced by Galactic interstellar scintillation of very compact non-varying objects. Conclusions. A microquasar/microblazar origin seems to be the best explanation for the nature of the variable sources in Arp220.

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Section: Microblazarssupporting

confidence: 67%

Rapid variability of the compact radio sources in Arp220

Batejat¹,

Conway²,

Rushton³

et al. 2012

A&A

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“…The BeppoSAX WFC instrument and its observing program are described by Jager et al (1997) and Verrecchia et al (2007), respectively. The WFCs were two identical coded mask instruments operating in the range 1.8-28 keV.…”

Section: Bepposax Wfcmentioning

confidence: 99%

ROSSI X-RAY TIMING EXPLORERANDBeppoSAXOBSERVATIONS OF THE TRANSIENT X-RAY PULSAR XTE J1859+083

Corbet

Zand

Levine

et al. 2009

ApJ

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We present observations of the 9.8 s X-ray pulsar XTE J1859+083 made with the All Sky Monitor (ASM) and Proportional Counter Array (PCA) on board the Rossi X-ray Timing Explorer, and the Wide Field Camera (WFC) on board BeppoSAX. The ASM data cover a 12 year time interval and show that an extended outburst occurred between approximately MJD 50,250 and 50,460 (1996 June 16 to 1997 January 12). The ASM data excluding this outburst interval suggest a possible modulation with a period of 60.65 ± 0.08 days. Eighteen sets of PCA observations were obtained over an approximately one month interval in 1999. The flux variability measured with the PCA appears consistent with the possible period found with the ASM. The PCA measurements of the pulse period showed it to decrease nonmonotonically and then to increase significantly. Doppler shifts due to orbital motion rather than accretion torques appear to be better able to explain the pulse period changes. Observations with the WFC during the extended outburst give a position that is consistent with a previously determined PCA error box, but which has a significantly smaller error. The transient nature of XTE J1859+083 and the length of its pulse period are consistent with it being a Be/neutron star binary. The possible 60.65 day orbital period would be of the expected length for a Be star system with a 9.8 s pulse period.

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“…Voges et al 1999;Bauer et al 2000;Ebisawa et al 2003;Verrecchia et al 2007;Mauch & Sadler 2007). It was classified as a Seyfert 1 by Maza et al (1994).…”

Section: Introductionmentioning

confidence: 99%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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Aims. We seek a comprehensive analysis of all the information provided by the XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810, CTS A08.12, and Mrk 110, including the UV range, to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra by taking advantage of the spectral range of these cameras. The high-resolution RGS spectra were analyzed to characterize the absorbing and emission line features that arise in the spectra of the sources. All these data, complemented by information in the UV, are analyzed jointly in order to achieve a consistent characterization of the observed features in each object. Results. The continuum emission of the sources can be characterized either by a combination of a power law and a black body for the weakest objects or by two power law components for the brightest ones. The continuum is not absorbed by neutral or ionized material in the line of sight to any of these sources. In all of them we have identified a narrow Fe-Kα line at 6.4 keV. In ESO 359-G19 we also find an Fexxvi line at about 7 keV. In the soft X-rays band, we identify only one Ovii line in the spectra of HE 1143-1810 and CTS A08.12, and two Ovii-Heα triplets and a narrow Oviii-Lyα emission line in Mrk 110. Conclusions. Not detecting warm material in the line of sight to the low state objects is due to intrinsically weaker or absent absorption in the line of sight and not to a low signal-to-noise ratio in the data. Besides this, the absence of clear emission lines cannot be fully attributed to dilution of those lines by a strong continuum.

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TheBeppoSAX WFC X-ray source catalogue

Cited by 30 publications

References 28 publications

Rapid variability of the compact radio sources in Arp220

Rapid variability of the compact radio sources in Arp220

ROSSI X-RAY TIMING EXPLORERANDBeppoSAXOBSERVATIONS OF THE TRANSIENT X-RAY PULSAR XTE J1859+083

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

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