The Gas Imaging Spectrometer on Board ASCA

Ohashi, T.; Ebisawa, Ken; Fukazawa, Yasushi; Hiyoshi, Kenji; Horii, M.; Ikebe, Y.; Ikeda, Hitoshi; Inoue, Hajime; Ishida, M.; Ishisaki, Yoshitaka; Ishizuka, Toshio; Kamijo, S.; Kaneda, Hidehiro; Kohmura, Yoshiki; Makishima, Kazuo; Mihara, T.; Tashiro, M.; Murakami, T.; Shoumura, Riichirou; Tanaka, Yasuo; Ueda, Yoshihiro; Taguchi, Koji; Tsuru, Takeshi Go; Takeshima, T.

doi:10.1093/pasj/48.2.157

Cited by 257 publications

(129 citation statements)

References 5 publications

Supporting

Mentioning

129

Contrasting

Order By: Relevance

“…2). On both occasions, IGR J18410-0535 was outside the field of view (FOV) of the Solid-state Imaging Spectrometers (SIS, Burke et al 1993), but included in that of Gas Imaging Spectrometers (GIS, Ohashi et al 1996). The GISs were operated in the nominal PH mode with a time resolution of 62.5 ms for data taken in high bit-rate and 0.5 s for those taken in medium bit-rate.…”

Section: Asca Data Analysismentioning

confidence: 99%

XMM-Newtonobservations of IGR J18410-0535: the ingestion of a clump by a supergiant fast X-ray transient

Bozzo

Giunta

Cusumano

et al. 2011

A&A

View full text Add to dashboard Cite

Context. IGR J18410-0535 is a supergiant fast X-ray transients. This subclass of supergiant X-ray binaries typically undergoes fewhour-long outbursts reaching luminosities of 10 36 -10 37 erg s −1 , the occurrence of which has been ascribed to the combined effect of the intense magnetic field and rotation of the compact object hosted in them and/or the presence of dense structures ("clumps") in the wind of their supergiant companion. Aims. IGR J18410-0535 was observed for 45 ks by XMM-Newton as part of a program designed to study the quiescent emission of supergiant fast X-ray transients and clarify the origin of their peculiar X-ray variability. Methods. We carried out an in-depth spectral and timing analysis of these XMM-Newton data. Results. IGR J18410-0535 underwent a bright X-ray flare that started about 5 ks after the beginning of the observation and lasted for ∼15 ks. Thanks to the capabilities of the instruments on-board XMM-Newton, the whole event could be followed in great detail. The results of our analysis provide strong convincing evidence that the flare was produced by the accretion of matter from a massive clump onto the compact object hosted in this system. Conclusions. By assuming that the clump is spherical and moves at the same velocity as the homogeneous stellar wind, we estimate a mass and radius of M cl 1.4 × 10 22 g and R cl 8 × 10 11 cm. These are in qualitative agreement with values expected from theoretical calculations. We found no evidence of pulsations at ∼4.7 s after investigating coherent modulations in the range 3.5 ms-100 s. A reanalysis of the archival ASCA and Swift data of IGR J18410-0535, for which these pulsations were previously detected, revealed that they were likely to be due to a statistical fluctuation and an instrumental effect, respectively.

show abstract

Section: Asca Data Analysismentioning

confidence: 99%

XMM-Newtonobservations of IGR J18410-0535: the ingestion of a clump by a supergiant fast X-ray transient

Bozzo

Giunta

Cusumano

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…ASCA consists of four identical grazing-incident X-ray telescopes each equipped with an imaging spectrometer (Tanaka et al 1994). The focal plane detectors are two CCD cameras (known as the Solid-State Imaging Spectrometers, or SIS; Gendreau 1995) and two gas scintillation imaging proportional counters (Gas Imaging Spectrometer, or GIS; Ohashi et al 1996). The SIS detectors have superior energy resolution, whereas the GIS detectors provide a larger field of view.…”

Section: Ascamentioning

confidence: 99%

X-Ray Properties of Groups of Galaxies

Mulchaey

2000

Annu. Rev. Astron. Astrophys.

252

288

View full text Add to dashboard Cite

ROSAT observations indicate that approximately half of all nearby groups of galaxies contain spatially extended X-ray emission. The radial extent of the X-ray emission is typically 50-500 h −1 100 kpc or approximately 10-50% of the virial radius of the group. Diffuse X-ray emission is generally restricted to groups that contain at least one early-type galaxy. X-ray spectroscopy suggests the emission mechanism is most likely a combination of thermal bremsstrahlung and line emission. This interpretation requires that the entire volume of groups be filled with a hot, low-density gas known as the intragroup medium. ROSAT and ASCA observations indicate that the temperature of the diffuse gas in groups ranges from approximately 0.3 keV to 2 keV. Higher temperature groups tend to follow the correlations found for rich clusters between X-ray luminosity, temperature, and velocity dispersion. However, groups with temperatures below approximately 1 keV appear to fall off the cluster LX-T relationship (and possibly the LX-σ and σ-T cluster relationships, although evidence for these latter departures is at the present time not very strong.) Deviations from the cluster LX-T relationship are consistent with preheating of the intragroup medium by an early generation of stars and supernovae. There is now considerable evidence that most X-ray groups are real, physical systems and not chance superpositions or large-scale filaments viewed edge-on. Assuming the intragroup gas is in hydrostatic equilibrium, X-ray observations can be used to estimate the masses of individual systems. ROSAT observations indicate that the typical mass of an X-ray group is ∼ 10 13 h100−1

show abstract

“…Table 2 shows the log of the ASCA observations. Details concerning the instruments can be found in Burke et al (1991), Ohashi et al (1996), Makishima et al (1996), and Serlemitsos et al (1995), while Tanaka et al (1994) gives a general description of ASCA. The SIS data were obtained in the 1-CCD faint mode, and the GIS data were obtained in the normal PH mode.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

ASCA observations of massive medium-distant clusters of galaxies. II.

Matsumoto

Pierre²,

Tsuru

et al. 2001

A&A

View full text Add to dashboard Cite

Abstract.We have selected seven medium-distant clusters of galaxies (z ∼ 0.1-0.3) for multi-wavelength observations with the goal of investigating their dynamical state. Following Paper I (Pierre et al. 1999) which reported the ASCA results about two of them, we present here the analysis of the ASCA observations of the other five clusters; RX J1023.8-2715 (A 3444), RX J1031.6-2607, RX J1050.5-0236 (A 1111), RX J1203.2-2131 (A 1451), and RX J1314.5-2517. Except for RX J1031.6, whose X-ray emission turned out to be dominated by an AGN, the ASCA spectra are well fitted by a one-temperature thin thermal plasma model. We compare the temperatureluminosity relation of our clusters with that of nearby ones (z < 0.1). Two clusters, RX J1050.5 and RX J1023.8, show larger luminosities than the bulk of clusters at similar temperatures, which suggests the presence of a cooling flow. The temperature vs. iron-abundance relationship of our sample is consistent with that of nearby clusters.

show abstract

The Gas Imaging Spectrometer on Board ASCA

Cited by 257 publications

References 5 publications

XMM-Newtonobservations of IGR J18410-0535: the ingestion of a clump by a supergiant fast X-ray transient

XMM-Newtonobservations of IGR J18410-0535: the ingestion of a clump by a supergiant fast X-ray transient

X-Ray Properties of Groups of Galaxies

ASCA observations of massive medium-distant clusters of galaxies. II.

Contact Info

Product

Resources

About