40 research outputs found
BATSE Soft Gamma-Ray Observations of GROJ0422+32
We report results of a comprehensive study of the soft gamma-ray (30 keV to
1.7 MeV) emission of GROJ0422+32 during its first known outburst in 1992. These
results were derived from the BATSE earth-occultation database with the JPL
data analysis package, EBOP (Enhanced BATSE Occultation Package). Results
presented here focus primarily on the long-term temporal and spectral
variability of the source emission associated with the outburst. The light
curves with 1-day resolution in six broad energy-bands show the high-energy
flux (>200 keV) led the low-energy flux (<200 keV) by ~5 days in reaching the
primary peak, but lagged the latter by ~7 days in starting the declining phase.
We confirm the "secondary maximum" of the low-energy (<200 keV) flux at TJD
8970-8981, ~120 days after the first maximum. Our data show that the "secondary
maximum" was also prominent in the 200-300 keV band, but became less pronounced
at higher energies. During this 200-day period, the spectrum evolved from a
power-law with photon index of 1.75 on TJD 8839, to a shape that can be
described by a Comptonized model or an exponential power law below 300 keV,
with a variable power-law tail above 300 keV. The spectrum remained roughly in
this two-component shape until ~9 November (TJD 8935) and then returned to the
initial power-law shape with an index of ~2 until the end of the period. The
correlation of the two spectral shapes with the high and low luminosities of
the soft gamma-ray emission is strongly reminiscent of that seen in Cygnus X-1.
We interpret these results in terms of the Advection Dominated Accretion Flow
(ADAF) model with possibly a "jet-like" region that persistently produced the
non-thermal power-law gamma rays observed throughout the event.Comment: 40 pages total, including 10 figures and 2 table
Gamma-Ray Spectra & Variability of the Crab Nebula Emission Observed by BATSE
We report ~ 600 days of BATSE earth-occultation observations of the total
gamma-ray (30 keV to 1.7 MeV) emission from the Crab nebula, between 1991 May
24 (TJD 8400) and 1994 October 2 (TJD 9627). Lightcurves from 35-100, 100-200,
200-300, 300-400, 400-700, and 700-1000 keV, show that positive fluxes were
detected by BATSE in each of these six energy bands at significances of
approximately 31, 20, 9.2, 4.5, 2.6, and 1.3 sigma respectively per day. We
also observed significant flux and spectral variations in the 35-300 keV energy
region, with time scales of days to weeks. The spectra below 300 keV, averaged
over typical CGRO viewing periods of 6-13 days, can be well described by a
broken power law with average indices of ~ 2.1 and ~ 2.4 varying around a
spectral break at ~ 100 keV. Above 300 keV, the long-term averaged spectra,
averaged over three 400 d periods (TJD 8400-8800, 8800-9200, and 9200-9628,
respectively) are well represented by the same power law with index of ~ 2.34
up to ~ 670 keV, plus a hard spectral component extending from ~ 670 keV to ~
1.7 MeV, with a spectral index of ~ 1.75. The latter component could be related
to a complex structure observed by COMPTEL in the 0.7-3 MeV range. Above 3 MeV,
the extrapolation of the power-law continuum determined by the low-energy BATSE
spectrum is consistent with fluxes measured by COMPTEL in the 3-25 MeV range,
and by EGRET from 30-50 MeV. We interpret these results as synchrotron emission
produced by the interaction of particles ejected from the pulsar with the field
in different dynamical regions of the nebula system, as observed recently by
HST, XMM-Newton, and Chandra.Comment: To be published in the November 20, 2003, Vol 598 issue of the
Astrophysical Journa
Novel design for an all-sky low-energy gamma-ray observatory (ALLEGRO)
We present a novel concept for a MIDEX satellite mission that allows all sky coverage for gamma-ray bursts and hard x-ray transients. The multiscale alternating shadow collimator (MASC) alone allows for arc minute positioning of 1 second bursts 3 times weaker than the BATSE sensitivity. Our scientific objectives include the ability: (a) to detect and monitor thousands of gamma-ray bursts (GRBs) and hard x- ray sources with sensitivity 3-10 times better than BATSE; (b) to solve the gamma-ray burst mystery; (c) to use gamma- ray bursts as probes of cosmological star formation and to measure cosmological parameters; (d) to understand the physics of the high energy radiation from AGNs and BLAZARs; (e) to study the physics of matter in the extreme around black holes and neutron stars; (f) to determine the pulsar birth rate and physical characteristics. The mission concept, MASC concept, and simulations are presented
Absolute Calibration and Characterization of the Multiband Imaging Photometer for Spitzer. II. 70 micron Imaging
The absolute calibration and characterization of the Multiband Imaging
Photometer for Spitzer (MIPS) 70 micron coarse- and fine-scale imaging modes
are presented based on over 2.5 years of observations. Accurate photometry
(especially for faint sources) requires two simple processing steps beyond the
standard data reduction to remove long-term detector transients. Point spread
function (PSF) fitting photometry is found to give more accurate flux densities
than aperture photometry. Based on the PSF fitting photometry, the calibration
factor shows no strong trend with flux density, background, spectral type,
exposure time, or time since anneals. The coarse-scale calibration sample
includes observations of stars with flux densities from 22 mJy to 17 Jy, on
backgrounds from 4 to 26 MJy sr^-1, and with spectral types from B to M. The
coarse-scale calibration is 702 +/- 35 MJy sr^-1 MIPS70^-1 (5% uncertainty) and
is based on measurements of 66 stars. The instrumental units of the MIPS 70
micron coarse- and fine-scale imaging modes are called MIPS70 and MIPS70F,
respectively. The photometric repeatability is calculated to be 4.5% from two
stars measured during every MIPS campaign and includes variations on all time
scales probed. The preliminary fine-scale calibration factor is 2894 +/- 294
MJy sr^-1 MIPS70F^-1 (10% uncertainty) based on 10 stars. The uncertainty in
the coarse- and fine-scale calibration factors are dominated by the 4.5%
photometric repeatability and the small sample size, respectively. The 5-sigma,
500 s sensitivity of the coarse-scale observations is 6-8 mJy. This work shows
that the MIPS 70 micron array produces accurate, well calibrated photometry and
validates the MIPS 70 micron operating strategy, especially the use of frequent
stimulator flashes to track the changing responsivities of the Ge:Ga detectors.Comment: 19 pages, PASP, in pres
Novel design for an all-sky low-energy gamma-ray observatory (ALLEGRO)
We present a novel concept for a MIDEX satellite mission that allows all sky coverage for gamma-ray bursts and hard x-ray transients. The multiscale alternating shadow collimator (MASC) alone allows for arc minute positioning of 1 second bursts 3 times weaker than the BATSE sensitivity. Our scientific objectives include the ability: (a) to detect and monitor thousands of gamma-ray bursts (GRBs) and hard x- ray sources with sensitivity 3-10 times better than BATSE; (b) to solve the gamma-ray burst mystery; (c) to use gamma- ray bursts as probes of cosmological star formation and to measure cosmological parameters; (d) to understand the physics of the high energy radiation from AGNs and BLAZARs; (e) to study the physics of matter in the extreme around black holes and neutron stars; (f) to determine the pulsar birth rate and physical characteristics. The mission concept, MASC concept, and simulations are presented
Absolute Calibration and Characterization of the Multiband Imaging Photometer for Spitzer. I. The Stellar Calibrator Sample and the 24 ÎŒm Calibration
We present the stellar calibrator sample and the conversion from instrumental to physical units for the 24 ÎŒm channel of the Multiband Imaging Photometer for Spitzer (MIPS). The primary calibrators are A stars, and the calibration factor based on those stars is MJy sr^â1 (DN s^â1)^â1, with a nominal uncertainty of 2%. We discuss the data reduction procedures required to attain this accuracy; without these procedures, the calibration factor obtained using the automated pipeline at the Spitzer Science Center is lower. We extend this work to predict 24 ÎŒm flux densities for a sample of 238 stars that covers a larger range of flux densities and spectral types. We present a total of 348 measurements of 141 stars at 24 ÎŒm. This sample covers a factor of 460 in 24 ÎŒm flux density, from 8.6 mJy up to 4.0 Jy. We show that the calibration is linear over that range with respect to target flux and background level. The calibration is based on observations made using 3 s exposures; a preliminary analysis shows that the calibration factor may be 1% and 2% lower for 10 and 30 s exposures, respectively. We also demonstrate that the calibration is very stable: over the course of the mission, repeated measurements of our routine calibrator, HD 159330, show a rms scatter of only 0.4%. Finally, we show that the point-spread function (PSF) is well measured and allows us to calibrate extended sources accurately; Infrared Astronomy Satellite (IRAS) and MIPS measurements of a sample of nearby galaxies are identical within the uncertainties
Towards screening Barrettâs Oesophagus: current guidelines, imaging modalities and future developments
Barrettâs oesophagus is the only known precursor to oesophageal adenocarcinoma (OAC). Although guidelines on the screening and surveillance exist in Barrettâs oesophagus, the current strategies are inadequate. Oesophagogastroduodenoscopy (OGD) is the gold standard method in screening for Barrettâs oesophagus. This invasive method is expensive with associated risks negating its use as a current screening tool for Barrettâs oesophagus. This review explores current definitions, epidemiology, biomarkers, surveillance, and screening in Barrettâs oesophagus. Imaging modalities applicable to this condition are discussed, in addition to future developments. There is an urgent need for an alternative non-invasive method of screening and/or surveillance which could be highly beneficial towards reducing waiting times, alleviating patient fears and reducing future costs in current healthcare services. Vibrational spectroscopy has been shown to be promising in categorising Barrettâs oesophagus through to high-grade dysplasia (HGD) and OAC. These techniques need further validation through multicentre trials