An abuttable CCD imager for visible and X-ray focal plane arrays

Burke, Barry E.; Mountain, R. W.; Harrison, David C.; Bautz, M. W.; Doty, J.; Ricker, G.; Daniels, Peter J. L.

doi:10.1109/16.78381

Cited by 153 publications

(71 citation statements)

References 12 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

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

show abstract

“…While the nuclear X-ray luminosity is well constrained in the low-N H range, it is not constrained at N 1 H m Ϫ2 because of the limited bandpass of ROSAT. The ASCA observation of NGC 1316 was made on 1994 January 11 for 35 ks, with the Gas Imaging Spectrometer (GIS; Ohashi et al 1996 in the normal PH mode and the Solid-State Imaging Spectrometer (SIS; Burke et al 1991) in the 2-CCD faint mode. These data were already used in Paper I to detect the inverse Compton X-rays.…”

Section: ϫ16mentioning

confidence: 99%

The Declined Activity in the Nucleus of NGC 1316

Iyomoto

Makishima

Tashiro

et al. 1998

The Astrophysical Journal

View full text Add to dashboard Cite

NGC 1316 (Fornax A) is a radio galaxy with prototypical double lobes, where the magnetic field intensity is accurately measured via the inverse Compton technique. The radio-emitting electrons in the lobes are inferred to have a synchrotron lifetime of ∼0.1 Gyr. Considering the lobe energetics, we estimate the past nuclear X-ray luminosity of NGC 1316 to be at least ∼ W ( ergs s Ϫ1 ). Thus, the nucleus was rather active at 34 41 4 # 10 4 # 10 least 0.1 Gyr ago. In contrast, we confirmed with ASCA and ROSAT that the nucleus of NGC 1316 is very faint in X-rays at present, with the 2-10 keV luminosity of any active galactic nucleus-like hard component being less than W ( ergs s Ϫ1 ), even assuming a nuclear obscuration up to ∼10 28 m Ϫ2 (10 24 cm Ϫ2 ).33 40 2 # 10 2 # 10 This is at least an order of magnitude lower than the estimated past activity, indicating that the nucleus is presently very inactive. From these two results, we conclude that the nucleus of NGC 1316 has become dormant during the last 0.1 Gyr. This suggests the possible abundance of "dormant" quasars in nearby galaxies.

show abstract

“…The minimum cutoff rigidity is 6 GeV/c. The minimum elevation angle is 10 and 5 degree respectively for the Solid-state Imaging Spectrometer (hereafter SIS; Burke et al 1991;Yamashita et al 1997) and the Gas Imaging Spectrometer (GIS; Ohashi et al 1996;Makishima et al 1996). The minimum angle between the target and the illuminated Earth's limb is 20 degree for the SIS.…”

Section: Asca Observations and Multiband Resultsmentioning

confidence: 99%

ASCA observations of blazars and multiband analysis

Takahashi¹,

Kubo²,

Madejski³

et al. 1997

AIP Conference Proceedings

View full text Add to dashboard Cite

We present data for 18 blazars observed with the X-ray satellite ASCA, half of which were also observed contemporaneously with the EGRET instrument onboard Compton Gamma-ray Observatory as parts of multi-wavelength campaigns. The observations show a clear difference in the spectra between three subclasses of blazars, namely the High-energy peaked BL Lac objects (HBLs), Low-energy peaked BL Lac objects (LBLs), and quasar-hosted blazars (QHBs). The ASCA X-ray spectra of HBLs are the softest, with the power law energy index α ∼ 1 − 2, and they form the highest observable energy tail of the low energy (LE, synchrotron) component. The X-ray spectra of the QHBs are the hardest (α ∼ 0.6) and are consistent with the lowest observable energy end of the high energy (HE, Compton) component. For LBLs, the X-ray spectra are intermediate. We find that the radiation process responsible for the HE peak for HBLs can be explained solely by Doppler-boosted Synchrotron-Self-Compton (SSC) emission, with the Doppler factor δ consistent with the VLBI and/or γ-ray variability data. For many QHBs, on the other hand, the γ-rays cannot be solely due to the SSC mechanism unless δ is significantly in excess of that inferred from VLBI data. We consider an alternative scenario consistent with the measured values of δ, where the SSC component is still present in QHBs and it dominates in the X-ray band, but it is below the observed γ-ray spectrum. With an assumption that the peak of the SSC emission is on the extrapolation of the X-ray spectrum, and adopting δ of 10, we infer the magnetic field B to be 0.1 -1 Gauss, and Lorentz factors γ b of electrons radiating at the peak of the νF (ν) spectrum of ∼ 10 3 for QHBs; this is much lower than γ b ∼ 10 5 for HBLs, even though the values of B are comparable in the two sub-classes. This difference of γ b is most likely due to the large photon density expected in QHBs (e.g. from thermal components visible in these objects) as compared with that of HBLs; Compton upscattering of these photons may well provide the observed GeV flux.

show abstract

An abuttable CCD imager for visible and X-ray focal plane arrays

Cited by 153 publications

References 12 publications

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

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

The Declined Activity in the Nucleus of NGC 1316

ASCA observations of blazars and multiband analysis

Contact Info

Product

Resources

About