128 research outputs found
Hard X-ray Properties of the Merging Cluster Abell 3667 as Observed with Suzaku
Wide-band Suzaku data on the merging cluster Abell 3667 were examined for
hard X-ray emission in excess to the known thermal component. Suzaku detected
X-ray signals in the wide energy band from 0.5 to 40 keV. The hard X-ray (> 10
keV) flux observed by the HXD around the cluster center cannot be explained by
a simple extension of the thermal emission with average temperature of ~7 keV.
The emission is most likely an emission from a very hot (kT > 13.2 keV) thermal
component around the cluster center, produced via a strong heating process in
the merger. In the north-west radio relic, no signature of non-thermal emission
was observed. Using the HXD, the overall upper-limit flux within a 34'x34'
field-of-view around the relic is derived to be 5.3e-12 erg s-1 cm-2 in the
10-40 keV band, after subtracting the ICM contribution estimated using the XIS
or the XMM-Newton spectra. Directly on the relic region, the upper limit is
further tightened by the XIS data to be less than 7.3e-13 erg s-1 cm-2, when
converted into the 10--40 keV band. The latter value suggest that the average
magnetic field within the relic is higher than 1.6 uG. The non-thermal pressure
due to magnetic fields and relativistic electrons may be as large as ~20% of
the thermal pressure in the region.Comment: 18 pages, 13 figures, to be appeared in PASJ 200
Pushing the limits of the NuSTAR detectors
NuSTAR (the Nuclear Spectroscopic Telescope ARray) is a NASA Small Explorer (SMEX) mission launched in June of 2012. Since its launch, NuSTAR has been the preeminent instrument for spectroscopic analysis of the hard X-ray sky over the 3-80 keV bandpass. The low energy side of the bandpass is limited by the absorption along the photon path as well as by the ability of the pixels to trigger on incident photons. The on-board calibration source does not have a low-energy line that we can use to calibrate this part of the response, so instead we use the "nearest-neighbor" readout in the NuSTAR detector architecture to calibrate the individual pixel thresholds for all 8 flight detectors on both focal plane modules (FPMs). These threshold measurements feed back into the quantum efficiency of the detectors at low (<5 keV) energies and, once well-calibrated, may allow the use of NuSTAR data below the current 3 keV limit
Ground calibration of the spatial response and quantum efficiency of the CdZnTe hard x-ray detectors for NuSTAR
Pixelated Cadmium Zinc Telluride (CdZnTe) detectors are currently flying on the Nuclear Spectroscopic Telescope ARray (NuSTAR) NASA Astrophysics Small Explorer. While the pixel pitch of the detectors is ≈ 605 μm, we can leverage the detector readout architecture to determine the interaction location of an individual photon to much higher spatial accuracy. The sub-pixel spatial location allows us to finely oversample the point spread function of the optics and reduces imaging artifacts due to pixelation. In this paper we demonstrate how the sub-pixel information is obtained, how the detectors were calibrated, and provide ground verification of the quantum efficiency of our Monte Carlo model of the detector response
Inflight performance and calibration of the NuSTAR CdZnTe pixel detectors
The Nuclear Spectroscopic Telescope Array (NuSTAR) satellite is a NASA Small Explorer mission designed to operate the first focusing high-energy X-ray (3-79 keV) telescope in orbit. Since the launch in June 2012, all the NuSTAR components have been working normally. The focal plane module is equipped with an 155Eu radioactive source to irradiate the CdZnTe pixel detectors for independent calibration separately from optics. The inflight spectral calibration of the CdZnTe detectors is performed with the onboard 155Eu source. The derived detector performance agrees well with ground-measured data. The in-orbit detector background rate is stable and the lowest among past high-energy X-ray instruments
Locating the most energetic electrons in Cassiopeia A
We present deep (2.4 Ms) observations of the Cassiopeia A supernova
remnant with {\it NuSTAR}, which operates in the 3--79 keV bandpass and is the
first instrument capable of spatially resolving the remnant above 15 keV. We
find that the emission is not entirely dominated by the forward shock nor by a
smooth "bright ring" at the reverse shock. Instead we find that the 15 keV
emission is dominated by knots near the center of the remnant and dimmer
filaments near the remnant's outer rim. These regions are fit with unbroken
power-laws in the 15--50 keV bandpass, though the central knots have a steeper
() spectrum than the outer filaments ().
We argue this difference implies that the central knots are located in the 3-D
interior of the remnant rather than at the outer rim of the remnant and seen in
the center due to projection effects. The morphology of 15 keV emission does
not follow that of the radio emission nor that of the low energy (12 keV)
X-rays, leaving the origin of the 15 keV emission as an open mystery. Even
at the forward shock front we find less steepening of the spectrum than
expected from an exponentially cut off electron distribution with a single
cutoff energy. Finally, we find that the GeV emission is not associated with
the bright features in the {\it NuSTAR} band while the TeV emission may be,
suggesting that both hadronic and leptonic emission mechanisms may be at work.Comment: 12 pages, 11 figures, accepted for publication in Ap
Suzaku observation of the metallicity distribution in the intracluster medium of the Fornax cluster
The metallicity distribution in the Fornax cluster was studied with the XIS
instrument onboard the Suzaku satellite. K-shell lines of O and Mg were
resolved clearly, and the abundances of O, Mg, Si, S and Fe were measured with
good accuracy. The region within a 4' radius of NGC 1399 shows approximately
solar abundances of Fe, Si and S, while the O/Fe and Mg/Fe abundance ratios are
about 0.4--0.5 and 0.7 in solar units. In the outer region spanning radii
between 6' and 23', the Fe and Si abundances drop to 0.4--0.5 solar and show no
significant gradient within this region. The abundance ratios, O/Fe and Mg/Fe,
are consistent with those in the central region. We also measured the Fe
abundance around NGC 1404 to be approximately solar, and the O, Ne and Mg
abundances to be 0.5--0.7 times the Fe level. The significant relative
enhancement of Fe within 130 kpc of NGC 1399 and in NGC 1404 indicates an
origin in SN Ia, in contrast to the species O, Ne, and Mg which reflect the
stellar metallicity. The mass-to-light ratios for O and Fe within 130 kpc of
NGC 1399 are over an order of magnitude lower than those in rich clusters,
reflecting the metal enrichment history of this poor cluster.Comment: 13 pages, accepted to PAS
Spectral calibration and modeling of the NuSTAR CdZnTe pixel detectors
The Nuclear Spectroscopic Telescope Array (NuSTAR) will be the first space
mission to focus in the hard X-ray (5-80 keV) band. The NuSTAR instrument
carries two co-aligned grazing incidence hard X-ray telescopes. Each NuSTAR
focal plane consists of four 2 mm CdZnTe hybrid pixel detectors, each with an
active collecting area of 2 cm x 2 cm. Each hybrid consists of a 32 x 32 array
of 605 micron pixels, read out with the Caltech custom low-noise NuCIT ASIC. In
order to characterize the spectral response of each pixel to the degree
required to meet the science calibration requirements, we have developed a
model based on Geant4 together with the Shockley-Ramo theorem customized to the
NuSTAR hybrid design. This model combines a Monte Carlo of the X-ray
interactions with subsequent charge transport within the detector. The
combination of this model and calibration data taken using radioactive sources
of Co-57, Eu-155 and Am-241 enables us to determine electron and hole
mobility-lifetime products for each pixel, and to compare actual to ideal
performance expected for defect-free material.Comment: 11 pages, 10 figures, to appear in Proceedings of the SPIE Conference
8145: UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XVI
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