39 research outputs found
Optimizations of Pt/SiC and W/Si multilayers for the Nuclear Spectroscopic Telescope Array
The Nuclear Spectroscopic Telescope Array, NuSTAR, is a NASA funded Small Explorer Mission, SMEX, scheduled for launch in mid 2011. The spacecraft will fly two co-aligned conical approximation Wolter-I optics with a focal length of 10 meters. The mirrors will be deposited with Pt/SiC and W/Si multilayers to provide a broad band reflectivity from 6 keV up to 78.4 keV. To optimize the mirror coating we use a Figure of Merit procedure developed for gazing incidence optics, which averages the effective area over the energy range, and combines an energy weighting function with an angular weighting function to control the shape of the desired effective area. The NuSTAR multilayers are depth graded with a power-law, d_i = a/(b + i)^c, and we optimize over the total number of bi-layers, N, c, and the maximum bi-layer thickness, d_(max). The result is a 10 mirror group design optimized for a flat even energy response both on and off-axis
NuSTAR Observations of the Magnetar 1E 2259+586
We report on new broad band spectral and temporal observations of the
magnetar 1E 2259+586, which is located in the supernova remnant CTB 109. Our
data were obtained simultaneously with the Nuclear Spectroscopic Telescope
Array (NuSTAR) and Swift, and cover the energy range from 0.5-79 keV. We
present pulse profiles in various energy bands and compare them to previous
RXTE results. The NuSTAR data show pulsations above 20 keV for the first time
and we report evidence that one of the pulses in the double-peaked pulse
profile shifts position with energy. The pulsed fraction of the magnetar is
shown to increase strongly with energy. Our spectral analysis reveals that the
soft X-ray spectrum is well characterized by an absorbed double-blackbody or
blackbody plus power-law model in agreement with previous reports. Our new hard
X-ray data, however, suggests that an additional component, such as a
power-law, is needed to describe the NuSTAR and Swift spectrum. We also fit the
data with the recently developed coronal outflow model by Beloborodov for hard
X-ray emission from magnetars. The outflow from a ring on the magnetar surface
is statistically preferred over outflow from a polar cap.Comment: 37 pages, 9 figures, corresponding author, [email protected]
The Central X-Ray Point Source in Cassiopeia A
The spectacular first light observation by the Chandra X-Ray Observatory
revealed an X-ray point source near the center of the 300 yr old Cas A
supernova remnant. We present an analysis of the public X-ray spectral and
timing data. No coherent pulsations were detected in the Chandra/HRC data. The
3-sigma upper limit on the pulsed fraction is 20 ms. The
Chandra/ACIS spectrum of the point source may be fit with an ideal blackbody
(kT=0.5 keV), or with BB models modified by the presence of a NS atmosphere
(kT=0.25-0.35 keV), but the temperature is higher and the inferred emitting
area lower than expected for a 300 yr old NS according to standard cooling
models. The spectrum may also be fit with a power law model (photon index
2.8-3.6). Both the spectral properties and the timing limits of the point
source are inconsistent with a young Crab-like pulsar, but are quite similar to
the properties of the anomalous X-ray pulsars. The spectral parameters are also
very similar to those of the other radio-quiet X-ray point sources in the
supernova remnants Pup A, RCW 103, and PKS 1209-52. Current limits on an
optical counterpart for the Cas A point source rule out models that invoke
fallback accretion onto a compact object if fallback disk properties are
similar to those in quiescent low-mass X-ray binaries. However, the optical
limits are marginally consistent with plausible alternative assumptions for a
fallback disk. In this case, accreting NS models can explain the X-ray data,
but an accreting BH model is not promising.Comment: 17 pages including 2 figs. To appear in ApJ, Vol. 546 (Jan 10, 2001).
Minor revisions per referee. Pulsation limits revised in light of HRC wiring
problem. Typos correcte
NuSTAR on-ground calibration: I. Imaging quality
The Nuclear Spectroscopic Telescope Array (NuSTAR) launched in June 2012 carries the first focusing hard Xray (5 - 80 keV) telescope to orbit. The on-ground calibration was performed at the RaMCaF facility at Nevis, Columbia University. During the assembly of the telescopes, mechanical surface metrology provided surface maps of the reflecting surfaces. Several flight coated mirrors were brought to BNL for scattering measurements. The information from both sources is fed to a raytracing code that is tested against the on-ground calibration data. The code is subsequently used for predicting the imaging properties for X-ray sources at infinite distance
NuSTAR ground calibration: The Rainwater Memorial Calibration Facility (RaMCaF)
The Nuclear Spectroscopic Telescope Array (NuSTAR) is a NASA Small Explorer mission that will carry the first focusing hard X-ray (5-80 keV ) telescope to orbit. The ground calibration of the three flight optics was carried out at the Rainwater Memorial Calibration Facility (RaMCaF) built for this purpose. In this article we present the facility and its use for the ground calibration of the three optics
NuSTAR Hard X-ray Survey of the Galactic Center Region I: Hard X-ray Morphology and Spectroscopy of the Diffuse Emission
We present the first sub-arcminute images of the Galactic Center above 10
keV, obtained with NuSTAR. NuSTAR resolves the hard X-ray source IGR
J17456-2901 into non-thermal X-ray filaments, molecular clouds, point sources
and a previously unknown central component of hard X-ray emission (CHXE).
NuSTAR detects four non-thermal X-ray filaments, extending the detection of
their power-law spectra with - up to ~50 keV. A
morphological and spectral study of the filaments suggests that their origin
may be heterogeneous, where previous studies suggested a common origin in young
pulsar wind nebulae (PWNe). NuSTAR detects non-thermal X-ray continuum emission
spatially correlated with the 6.4 keV Fe K fluorescence line emission
associated with two Sgr A molecular clouds: MC1 and the Bridge. Broad-band
X-ray spectral analysis with a Monte-Carlo based X-ray reflection model
self-consistently determined their intrinsic column density (
cm), primary X-ray spectra (power-laws with ) and set a
lower limit of the X-ray luminosity of Sgr A* flare illuminating the Sgr A
clouds to erg s. Above ~20 keV, hard
X-ray emission in the central 10 pc region around Sgr A* consists of the
candidate PWN G359.95-0.04 and the CHXE, possibly resulting from an unresolved
population of massive CVs with white dwarf masses . Spectral energy distribution analysis suggests that G359.95-0.04 is
likely the hard X-ray counterpart of the ultra-high gamma-ray source HESS
J1745-290, strongly favoring a leptonic origin of the GC TeV emission.Comment: 27 pages. Accepted for publication in the Astrophysical Journa
A broadband x-ray study of the Geminga pulsar with NuSTAR and XMM-Newton
We report on the first hard X-ray detection of the Geminga pulsar above 10
keV using a 150 ks observation with the NuSTAR observatory. The double-peaked
pulse profile of non-thermal emission seen in the soft X-ray band persists at
higher energies. Broadband phase-integrated spectra over the 0.2-20 keV band
with NuSTAR and archival XMM-Newton data do not fit to a conventional
two-component model of a blackbody plus power-law, but instead exhibit spectral
hardening above ~5 keV. We find two spectral models fit the data well: (1) a
blackbody (kT1 ~ 42 eV) with a broken power-law (Gamma1 ~ 2.0, Gamma2 ~ 1.4 and
Ebreak ~ 3.4 keV), and (2) two blackbody components (kT1 ~ 44 eV and kT2 ~ 195
eV) with a power-law component (Gamma ~ 1.7). In both cases, the extrapolation
of the Rayleigh-Jeans tail of the thermal component is consistent with the UV
data, while the non-thermal component overpredicts the near-infrared data,
requiring a spectral flattening at E ~ 0.01 - 1 keV. While strong phase
variation of the power-law index is present below ~5 keV, our phase-resolved
spectroscopy with NuSTAR indicates that another hard non-thermal component with
Gamma ~ 1.3 emerges above ~5 keV. The spectral hardening in non-thermal X-ray
emission as well as spectral flattening between the optical and X-ray bands
argue against the conjecture that a single power-law may account for
multi-wavelength non-thermal spectra of middle-aged pulsars.Comment: Accepted to Ap
CAST constraints on the axion-electron coupling
In non-hadronic axion models, which have a tree-level axion-electron interaction, the Sun produces a strong axion flux by bremsstrahlung, Compton scattering, and axiorecombination, the "BCA processes." Based on a new calculation of this flux, including for the first time axio-recombination, we derive limits on the axion-electron Yukawa coupling gae and axion-photon interaction strength ga using the CAST phase-I data (vacuum phase). For ma <~ 10 meV/c2 we find ga gae < 8.1 × 10−23 GeV−1 at 95% CL. We stress that a next-generation axion helioscope such as the proposed IAXO could push this sensitivity into a range beyond stellar energy-loss limits and test the hypothesis that white-dwarf cooling is dominated by axion emission