67 research outputs found
Determining X-Ray Source Intensity and Confidence Bounds in Crowded Fields
We present a rigorous description of the general problem of aperture
photometry in high energy astrophysics photon-count images, in which the
statistical noise model is Poisson, not Gaussian. We compute the full posterior
probability density function for the expected source intensity for various
cases of interest, including the important cases in which both source and
background apertures contain contributions from the source, and when multiple
source apertures partially overlap. A Bayesian approach offers the advantages
that it allows one to (a) include explicit prior information on source
intensities, (b) propagate posterior distributions as priors for future
observations, and (c) use Poisson likelihoods, making the treatment valid in
the low counts regime. Elements of this approach have been implemented in the
Chandra Source Catalog.Comment: 32 pages, 12 figures. Fixed typos and incorrect statement at end of
4.2.3. Results unchange
Detection of x ray sources in PROS
The problem of detecting discrete sources in x-ray images has much in common with the problem of automatic source detection at other wavelengths. In all cases, one searches for positive brightness enhancements exceeding a certain threshold, which appear consistent with what one expects for a point source, in the presence of a (possibly) spatially variable background. Multidimensional point spread functions (e.g., dependent on detector position and photon energy) are also common. At the same time, the problem in x-ray astronomy has some unique aspects. For example, for typical x-ray exposures in current or recent observatories, the number of available pixels far exceeds the number of actual x-ray events, so Poisson, rather than Gaussian statistics apply. Further, extended cosmic x-ray sources are common, and one often desires to detect point sources in the vicinity or even within bright, diffuse x-ray emission. Finally, support structures in x-ray detectors often cast sharp shadows in x-ray images making it necessary to detect sources in a region of rapidly varying exposure. We have developed a source detection package within the IRAF/PROS environment which attempts to deal with some of the problems of x-ray source detection. We have patterned our package after the successful Einstein Observatory x-ray source detection programs. However, we have attempted to improve the flexibility and accessibility of the functions and to provide a graphical front-end for the user. Our philosophy has been to use standard IRAF tasks whenever possible for image manipulation and to separate general functions from mission-specific ones. We will report on the current status of the package and discuss future developments, including simulation tasks, to allow the user to assess detection efficiency and source significance, tasks to determine source intensity, and alternative detection algorithms
Dwarf Galaxies of the Local Group
XMM-Newton and Chandra have ushered in a new era for the study of dwarf
galaxies in the Local Group. We provide an overview of the opportunities,
challenges, and some early results. The large number of background sources
relative to galaxy sources is a major theme. Despite this challenge, the
identification of counterparts has been possible, providing hints that the same
mechanisms producing X-ray sources in larger galaxies are active in dwarf
galaxies. A supersoft X-ray source within 2" of the supermassive black hole in
M32 may be a remnant of the tidal disruption of a giant, although other
explanations cannot be ruled out.Comment: 6 pages, 4 figures, proceedings for 2004 IAU symposiu
The Discovery of a Spatially-Resolved Supernova Remnant in M31 with Chandra
Chandra observations of M31 allow the first spatially resolved X-ray image of
a supernova remnant (SNR) in an external spiral galaxy. CXOM31 J004327.7+411829
is a slightly elongated ring-shaped object with a diameter of ~11'' (42 pc). In
addition, the X-ray image hints that the chemical composition of the SNR is
spatial dependent. The X-ray spectrum of the SNR can be well fitted with a
Raymond-Smith model or a non-equilibrium ionization model. Depending on the
spectral model, the 0.3-7 keV luminosity is between 3.2x10^36 erg/s and
4.5x10^37 erg/s. The age of the SNR is estimated to be 3210-22300 years and the
number density of ambient gas is ~0.003-0.3 cm^-3. This suggests that the local
interstellar medium around the SNR is low.Comment: 5 pages, 3 figures; accepted for publication in ApJ
Chandra and Hubble Study of a New Transient X-ray Source in M31
We present X-ray and optical observations of a new transient X-ray source in
M31 first detected 23-May-2004 at R.A.=00:43:09.940 +/- 0.65'',
Dec.=41:23:32.49 +/- 0.66''. The X-ray lightcurve shows two peaks separated by
several months, reminiscent of many Galactic X-ray novae. The location and
X-ray spectrum of the source suggest it is a low mass X-ray binary (LMXB).
Follow-up HST ACS observations of the location both during and after the
outburst provide a high-confidence detection of variability for one star within
the X-ray position error ellipse. This star has B ~ 1 mag, and there is
only a ~1% chance of finding such a variable in the error ellipse. We consider
this star a good candidate for the optical counterpart of the X-ray source. The
luminosity of this candidate provides a prediction for the orbital period of
the system of 2.3 days.Comment: 17 pages, 3 figures, 4 tables, accepted for publication in Ap
Supersoft X-ray Sources in M31: I. A Chandra Survey and an Extension to Quasisoft Sources
We report on very soft X-ray sources (VSSs) in M31. In a survey which was
most sensitive to soft sources in four 8'x8' regions covered by Chandra's
ACIS-S S3 CCD, we find 33 VSSs that appear to belong to M31. Fifteen VSSs have
spectral characteristics mirroring the supersoft X-ray sources studied in the
Magellanic Cloud and Milky Way ( eV); we therefore call
these ``classical'' supersoft sources, or simply supersoft sources (SSSs).
Eighteen VSSs may either have small (< 10%) hard components, or slightly higher
effective temperatures (but still < 350 eV). We refer to these VSSs as
quasisoft sources (QSSs). While hot white dwarf models may apply to SSSs, the
effective temperatures of QSSs are too high, unless, e.g., the radiation
emanates from only a small portion of surface. Two of the SSSs were first
detected and identified as such through ROSAT observations. One SSS and one QSS
may be identified with symbiotics, and 2 SSSs with supernova remnants. Both
SSSs and QSSs in the disk are found near star-forming regions, possibly
indicating that they are young. VSSs in the outer disk and halo are likely to
be old systems; in these regions, there are more QSSs than SSSs, which is
opposite to what is found in fields closer to the galaxy center. The largest
density of bright VSSs is in the bulge; some of the bulge sources are close
enough to the nucleus to be remnants of the tidal disruption of a giant by the
massive central black hole. By using Chandra data in combination with ROSAT and
XMM observations, we find most VSSs to be highly variable, fading from or
brightening toward detectability on time scales of months. There is evidence
for VSSs with low luminosities ( erg s).Comment: 14 pages, 4 figures. Accepted for publication in ApJ. Classification
of supersoft and quasisoft sources is clarifie
A Soft X-ray Transient in the M31 Bulge
We have examined a probable soft X-ray transient source in the M31 bulge at
R.A.=0:42:41.814 +/- 0.08", Dec. = 41:16:35.86 +/- 0.07". On the three
occasions we observed the source, its spectrum was soft (kT_{in} ~1 keV). The
brightest detection of the source was 2004 July 17 with a 0.3-7 keV luminosity
of ~5 X 10^{37} erg/s. The only previous detection of the source was in 1979 by
the Einstein observatory. The multiple detections over 25 years suggest the
duty cycle of the source is in the range 0.02-0.06. Coordinated HST/ACS imaging
before, during, and after the outburst revealed no variable optical source
within the position errors of the X-ray source. The optical data place a firm
upper limit on the brightness of the counterpart of the X-ray outburst of
B>24.7, suggesting the binary has a period <5.2 days. The X-ray spectrum and
lack of bright stars at the source location indicate the source was a soft
transient event occurring in a low-mass X-ray binary, making this source a good
black hole candidate in M31.Comment: 18 pages, 4 tables, 3 figures, accepted for publication in Ap
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