The UHURU catalog of X-ray souces.

Giacconi, R.; Murray, S. S.; Gursky, H.; Kellogg, E.; Schreier, E.; Tananbaum, H.

doi:10.1086/151790

Cited by 279 publications

(185 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: 66%

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: 66%

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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“…Further long-term broad-band X-ray behaviour 4U 0614+091 was discovered by UHURU with variable flux levels between about 15 and 70 mCrab (2−6 keV; Giacconi et al 1972). Other early measurements of the flux, besides those from UHURU, may be found in, e.g., Mason et al (1976), Swank et al (1978), Parsignault & Grindlay (1978), Markert et al (1979), and Warwick et al (1981).…”

Section: Asm Long-term Persistent Flux and Burst Recurrence Timesmentioning

confidence: 92%

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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“…The ONC was first detected in X-rays by the Uhuru satellite (Giacconi et al 1972). Subsequent imaging observations performed with the Einstein and ROSAT observatories (Ku & Chanan 1979;Gagné, Caillault, & Stauffer 1995) indicated that (1) ONC members are powerful X-ray emitters, with typical L X =L bol close to the saturation value, 10 À3 , observed for fast rotators on the main sequence; (2) no relation seems to hold between X-ray activity and stellar rotation; and (3) stars with circumstellar accretion disks may have lower levels of X-ray activity.…”

Section: Introductionmentioning

confidence: 99%

ChandraX‐Ray Observation of the Orion Nebula Cluster. I. Detection, Identification, and Determination of X‐Ray Luminosities

Flaccomio

Damiani

Micela

et al. 2003

ApJ

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In this first of two companion papers on the Orion Nebula Cluster (ONC), we present our analysis of a 63 ks Chandra HRC-I observation that yielded 742 X-ray detections within the 30 0 Â 30 0 field of view. To facilitate our interpretation of the X-ray image, here we collect a multiwavelength catalog of nearly 2900 known objects in the region by combining 17 different catalogs from the recent literature. We define two reference groups: an infrared sample, containing all objects detected in the K band, and an optical sample comprising low-extinction, well-characterized ONC members. We show for both samples that field object contamination is generally low. Our X-ray sources are primarily low-mass ONC members. The detection rate for optical sample stars increases monotonically with stellar mass from zero at the brown dwarf limit to $100% for the most massive stars but shows a pronounced dip between 2 and 10 M . We determine L X and L X =L bol for all stars in our optical sample and utilize this information in our companion paper to study correlations between X-ray activity and other stellar parameters.

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The UHURU catalog of X-ray souces.

Cited by 279 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

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

ChandraX‐Ray Observation of the Orion Nebula Cluster. I. Detection, Identification, and Determination of X‐Ray Luminosities

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