1,509 research outputs found
Using BATSE to measure gamma-ray burst polarization
We describe a technique for measuring the polarization of hard x-rays from γ-ray bursts based on the angular distribution of that portion of the flux which is scattered off the top of the Earth’s atmosphere. The scattering cross section depends not only on the scatter angle itself, but on the orientation of the scatter angle with respect to the incident polarization vector. Consequently, the distribution of the observed albedo flux will depend on the direction and the polarization properties (i.e., the level of polarization and polarization angle) of the source. Although the BATSE design (with its large field-of-view for each detector) is not optimized for albedo polarimetry, we have nonetheless investigated the feasibility of this technique using BATSE data
Monitoring Cen X-3 with BATSE
The eight uncollimated BATSE Large Area Detectors (LAD's) provide the ability to monitor pulsed hard x ray sources on a nearly continuous basis. Using data from the LAD's, the pulse timing and pulsed flux of the 4.8 second period binary x ray pulsar Centaurus X-3 was analyzed over a two month period. The methods and initial results of this analysis, which includes both data folded onboard GRO and 1.024 second resolution discriminator rates folded on the ground, are presented
Chandra localization of XTE J1906+090 and discovery of its optical and infrared counterparts
We present the Chandra identification and localization of the transient X-ray source XTE J1906+090 and the discovery of its optical and infrared counterparts. Our analysis of archival Chandra ACIS-I observations of the field found the source approximately 8 away from the position determined earlier with the RXTE PCA. We have confirmed the source identification with timing analysis of the X-ray data, which detected the source spin period of 89.6 s. The best Chandra position for the source is R.A. = 19h04m47491, decl. = +09024140. Subsequently, we performed optical observations of the field around the new location and discovered a coincident optical source with R-band magnitude of 18.7. A search in the Two Micron All Sky Survey catalog revealed an infrared point source with J = 15.2, H = 14.2, and K = 13.5, whose location is also coincident with our Chandra and optical positions. Our results add fresh evidence for a Be/X-ray transient nature for XTE J1906+090
Observations of Accreting Pulsars
We discuss recent observations of accreting binary pulsars with the all-sky BATSE instrument on the Compton Gamma Ray Observatory. BATSE has detected and studied nearly half of the known accreting pulsar systems. Continuous timing studies over a two-year period have yielded accurate orbital parameters for 9 of these systems, as well as new insights into long-term accretion torque histories
Recent Outbursts from the Transient X-Ray Pulsar Cep X-4 (GS 2138+56)
We report on X-ray observations of the 66 s period transient X-ray pulsar Cep
X-4 (GS 2138+56) with the Burst and Transient Source Experiment (BATSE) on the
Compton Gamma-Ray Observatory (CGRO) and with the Rossi X-ray Timing Explorer
(RXTE). Two outbursts from Cep X-4 were observed with BATSE in 1993 June-July
and 1997 July. Pulse frequencies of 15.0941 +/- 0.0002 mHz on 1993 June 25 (MJD
49,163) and 15.0882 +/- 0.0002 mHz on 1997 July 12 (MJD 50,641) were each
measured from 2 day spans of BATSE data near each outburst's peak. Cep X-4
showed an average spin down rate of (-4.14 +/- 0.08)*10^(-14) Hz/s between the
1993 and 1997 outbursts. After BATSE could no longer detect Cep X-4, public
observations were performed on 1997 July 18 & 25 with the Proportional Counter
Array (PCA) on RXTE. A pulse frequency of 15.088 +/- 0.004 mHz was measured
from observations on 1997 July 18 (MJD 50,647). Significant aperiodic noise,
with an rms variance of ~18% in the frequency range 0.01-1.0 Hz was observed on
both days. Energy and intensity dependent pulse shape variations were also seen
in these data. Recently published optical observations associate Cep X-4 with a
Be companion star. If all 4 outbursts observed from Cep X-4 are assumed to
occur at the same orbital phase, we find that the orbital period is between 23
days and 147.3 days.Comment: 19 pages (LaTeX) including 9 figures. Accepted for publication in the
Astrophysical Journa
Variable Spin-down in the Soft Gamma Repeater SGR 1900+14 and Correlations with Burst Activity
We have analyzed Rossi X-ray Timing Explorer Proportional Counter Array
observations of the pulsed emission from SGR 1900+14 during September 1996,
June - October 1998, and early 1999. Using these measurements and results
reported elsewhere, we construct a period history of this source for 2.5 years.
We find significant deviations from a steady spin-down trend during quiescence
and the burst active interval. Burst and Transient Source Experiment
observations of the burst emission are presented and correlations between the
burst activity and spin-down rate of SGR 1900+14 are discussed. We find an 80
day interval during the summer of 1998 when the average spin-down rate is
larger than the rate elsewhere by a factor ~ 2.3. This enhanced spin-down may
be the result of a discontinuous spin-down event or ``braking glitch'' at the
time of the giant flare on 27 August 1998. Furthermore, we find a large
discrepancy between the pulsar period and average spin-down rate in X-rays as
compared to radio observations for December 1998 and January 1999.Comment: 6 pages, 2 figures, submitted to ApJ Letter
On the Correlation of Torque and Luminosity in GX 1+4
Over five years of daily hard X-ray (>20 keV) monitoring of the 2-min
accretion-powered pulsar GX 1+4 with the Compton Gamma Ray Observatory/BATSE
large-area detectors has found nearly continuous rapid spin-down, interrupted
by a bright 200-d spin-up episode. During spin-down, the torque becomes more
negative as the luminosity increases (assuming that the 20-60 keV pulsed flux
traces bolometric luminosity), the opposite of what is predicted by standard
accretion torque theory. No changes in the shape of the 20-100 keV pulsed
energy spectrum were detected, so that a very drastic change in the spectrum
below 20 keV or the pulsed fraction would be required to make the 20-60 keV
pulsed flux a poor luminosity tracer. These are the first observations which
flatly contradict standard magnetic disk accretion theory, and they may have
important implications for understanding the spin evolution of X-ray binaries,
cataclysmic variables, and protostars. We briefly discuss the possibility that
GX 1+4 may be accreting from a retrograde disk during spin-down, as previously
suggested.Comment: 10 pages including 3 PS figures. To appear in ApJ Letter
On the nature of the ultraluminous X-ray transient in Cen~A (NGC 5128)
We combine 9 ROSAT, 9 Chandra, and 2 XMM-Newton observations of the Cen~A
galaxy to obtain the X-ray light curve of 1RXH J132519.8-430312 (=CXOU
J132519.9430317) spanning 1990 to 2003. The source reached a peak 0.1-2.4
keV flux F_X>10^{-12} ergs cm^{-2} s^{-1} during a 10~day span in 1995 July.
The inferred peak isotropic luminosity of the source therefore exceeded 3
10^{39} ergs s^{-1}, which places the source in the class of ultra-luminous
X-ray sources. Coherent pulsations at 13.264 Hz are detected during a second
bright episode (F_X >3 times 10^{-13} ergs cm^{-2} s^{-1}) in 1999 December.
The source is detected and varies significantly within three additional
observations but is below the detection threshold in 7 observations. The X-ray
spectrum in 1999 December is best described as a cut-off power law or a
disk-blackbody (multi-colored disk). We also detect an optical source, m_F555W
~ 24.1 mag, within the Chandra error circle of 1RXH J132519.8-430312 in HST
images taken 195~days before the nearest X-ray observation. The optical
brightness of this source is consistent with a late O or early B star at the
distance of Cen A. If the optical source is the counterpart, then the X-ray and
optical behavior of 1RXH J132519.8-430312 are similar to the transient Be/X-ray
pulsar A 0538-66.Comment: 7 pages, 8 figures. ApJ (accepted
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