The fourth UHURU catalog of X-ray sources.

Forman, W.; Jones, C.; Cominsky, L.; Julien, P.; Murray, S. S.; Peters, George H.; Tananbaum, H.; Giacconi, R.

doi:10.1086/190561

Cited by 428 publications

(269 citation statements)

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“…This AXP was discovered by the Uhuru X-ray observatory in the early seventies (Giacconi et al 1972;Forman et al 1978). The spin period of 8.7 s was found by Israel et al (1994).…”

Section: Introductionmentioning

confidence: 68%

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

Hartog

Kuiper

Hermsen

et al. 2007

Astrophys Space Sci

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For the first time a quasi-simultaneous multiwavelength campaign has been performed on an Anomalous X-ray Pulsar from the radio to the hard X-ray band. 4U 0142+61 was an INTEGRAL target for 1 Ms in July 2005. During these observations it was also observed in the X-ray band with Swift and RXTE, in the optical and NIR with Gemini North and in the radio with the WSRT. In this paper we present the source-energy distribution. The spectral results obtained in the individual wave bands do not connect smoothly; apparently components of different origin contribute to the total spectrum. Remarkable is that the INTEGRAL hard X-ray spectrum (power-law index 0.79 ± 0.10) is now measured up to an energy of ∼230 keV with no indication of a spectral break. Extrapolation of the INTEGRAL power-law spectrum to lower energies passes orders of magnitude underneath the NIR and optical fluxes,

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“…This AXP was discovered by the Uhuru X-ray observatory in the early seventies (Giacconi et al 1972;Forman et al 1978). The spin period of 8.7 s was found by Israel et al (1994).…”

Section: Introductionmentioning

confidence: 68%

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

Hartog

Kuiper

Hermsen

et al. 2007

Astrophys Space Sci

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“…4U 0115+63 was discovered by the UHURU observatory in the early 1970s by Giacconi et al (1972);Forman et al (1978). During the SAS-3 observations in 1978, Cominsky et al (1978) found a pulsation period of 3.61 sec.…”

Section: Discussionmentioning

confidence: 98%

“…4U 1909+07 is a persistent X-ray pulsar discovered by the UHURU observatory (Forman et al, 1978) (also known as X 1908+075). An orbital periodicity of 4.4 days has been found in the RXTE/ASM data (Wen et al, 2000).…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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“…Several X-ray cluster samples have been constructed from previous X-ray missions and have been used for a variety of astrophysical studies (e.g. Romer et al 1994;Forman et al 1978;Scharf et al 1997;Vikhlinin et al 1998;Böhringer et al 2000Böhringer et al , 2004Borgani et al 2001;Burenin et al 2007). The current generation of X-ray satellites, XMM-Newton, Chandra, and Suzaku, provided follow-up observations of individual clusters that allowed a precise determination of their spatially resolved spectra (e.g.…”

Section: Introductionmentioning

confidence: 99%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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Aims. We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). We present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (L X − T ) relation. Methods. The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data we derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. Results. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03−0.70 (median z = 0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. For each cluster, the catalogue also provides the X-ray bolometric luminosity and the cluster mass at R 500 based on scaling relations and the position of the likely brightest cluster galaxy (BCG). The updated L X − T relation of the current sample with X-ray spectroscopic parameters is presented. We found the slope of the L X − T relation to be consistent with published ones. We see no evidence for evolution in the slope and intrinsic scatter of the L X − T relation with redshift when excluding the low-luminosity groups.

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The fourth UHURU catalog of X-ray sources.

Cited by 428 publications

References 0 publications

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

High-mass X-ray binaries in the Milky Way

The 2XMMi/SDSS Galaxy Cluster Survey

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