82 research outputs found
Optical Identifications of Five INTEGRAL Hard X-ray Sources in the Galactic Plane Region
The results of optical identifications of five hard X-ray sources in the
Galactic plane region from the INTEGRAL all-sky survey are presented. The X-ray
data on one source (IGRJ20216+4359) are published for the first time. The
optical observations were performed with 1.5-m RTT-150 telescope (TUBITAK
National Observatory, Antalya, Turkey) and 6-m BTA telescope (Special
Astrophysical Observatory, Nizhny Arkhyz, Russia). A blazar, three Seyfert
galaxies, and a high-mass X-ray binary are among the identified sources.Comment: 7 pages, 10 figures, Astronomy Letters, v. 34, p. 65
Optical identification of hard X-ray source IGRJ18257-0707
We present the results of the optical identification of hard X-ray source
IGRJ18257-0707 trough the spectroscopic observations of its optical counterpart
with RTT150 telescope. Accurate position of the X-ray source, determined using
Chandra observations, allowed us to associate this source with the faint
optical object (m_R=~20.4), which shows broad H_\alpha emission line in its
optical spectrum. Therefore we conclude that the source IGRJ18257-0707 is a
type 1 Seyfert galaxy at redshift z=0.037.Comment: 4 pages, 3 figures, accepted for publication in Astronomy Letters,
the original text in Russian can be found at
http://hea.iki.rssi.ru/~rodion/pigrj18257-0707.pd
Optical Identification of Four Hard X-ray Sources from the Swift All-Sky Survey
We present the results of our optical identifications of four hard X-ray
sources from the Swift all-sky survey. We obtained optical spectra for each of
the program objects with the 6-m BTA telescope (Special Astrophysical
Observatory, Russian Academy of Sciences, Nizhnii Arkhyz), which allowed their
nature to be established. Two sources (SWIFT J2237.2+6324} and SWIFT
J2341.0+7645) are shown to belong to the class of cataclysmic variables
(suspected polars or intermediate polars). The measured emission line width
turns out to be fairly large (FWHM ~ 15-25 A), suggesting the presence of
extended, rapidly rotating (v~400-600 km/s) accretion disks in the systems.
Apart from line broadening, we have detected a change in the positions of the
line centroids for SWIFT J2341.0+7645, which is most likely attributable to the
orbital motion of the white dwarf in the binary system. The other two program
objects (SWIFT J0003.3+2737 and SWIFT J0113.8+2515) are extragalactic in
origin: the first is a Seyfert 2 galaxy and the second is a blazar at redshift
z=1.594. Apart from the optical spectra, we provide the X-ray spectra for all
sources in the 0.6-10 keV energy band obtained from XRT/Swift data.Comment: 9 pages, 6 figures, will be published in Astronomy Letters, 38, No.5,
pp.281-289 (2012
First hours of the GRB 030329 optical afterglow
We present the first results of the observations of the extremely bright
optical afterglow of gamma-ray burst (GRB) 030329 with the 1.5m Russian-Turkish
telescope RTT150 (TUBITAK National Observatory, Bakyrlytepe, Turkey). RTT150
was one of the first 1.5m-class telescopes pointed to the afterglow.
Observations were started approximately 6 hours after the burst. During the
first 5 hours of our observations the afterglow faded exactly as a power law
with index -1.19+-0.01 in each of the BVRI Bessel filters. After that, in all
BVRI filters simultaneously we observe a steepening of the power law light
curve. The power law decay index smoothly approaches the value ~= -1.9,
observed by other observatories later. This power law break occurs at t-t_0
=0.57 days and lasts for +-0.1 days. We observe no variability above the
gradual fading with the upper limits 10--1% on time scales 0.1--1000s. Spectral
flux distribution in four BVRI filters corresponds to the power law spectrum
with spectral index \alpha=0.66+-0.01. The change of the power law decay index
in the end of our observations can be interpreted as a signature of collimated
ultrarelativistic jet. The afterglow flux distribution in radio, optical and
x-rays is consistent with synchrotron spectrum. We continue our observations of
this unique object with RTT150.Comment: Astronomy Letters, Vol. 29, No. 9, p. 573; 6 pages, 5 figures;
pagination corrected; the original Russian version can be found at
http://hea.iki.rssi.ru/~br/030329/pfh030329.pd
Additional spectroscopic redshift measurements for galaxy clusters from the First Planck Catalogue
We present the results of spectroscopic redshift measurements for the galaxy
clusters from the first all-sky Planck catalogue of the Sunyaev-Zeldovich
sources, that have been mostly identified by means of the optical observations
performed previously by our team (Planck Collaboration, 2015a). The data on 13
galaxy clusters at redshifts from z=~0.2 to z=~0.8, including the improved
identification and redshift measurement for the cluster PSZ1 G141.73+14.22 at
z=0.828, are provided. The measurements were done using the data from
Russian-Turkish 1.5-m telescope (RTT-150), 2.2-m Calar Alto Observatory
telescope, and 6-m SAO RAS telescope (Bolshoy Teleskop Azimutalnyi, BTA).Comment: published in Astronomy Letter
Observing scattered X-ray radiation from gamma-ray bursts: a way to measure their collimation angles
There are observational facts and theoretical arguments for an origin of
gamma-ray bursts in molecular clouds in distant galaxies. If this is true, one
could detect a significant flux of GRB prompt and early afterglow X-ray
radiation scattered into our line of sight by the molecular and atomic matter
located within tens of parsecs of the GRB site long after the afterglow has
faded away. The scattered flux directly measures the typical density of the GRB
ambient medium. Furthemore, if the primary emission is beamed, the scattered
X-ray flux will be slowly decreasing for several months to years before falling
off rapidly. Therefore, it should be possible to estimate the collimation angle
of a burst from the light curve of its X-ray echo and a measured value of the
line-of-sight absorption column depth. It is shown that detection of such an
echo is for the brightest GRBs just within the reach of the Chandra and
XMM-Newton observatories.Comment: 6 pages, 2 figures. Accepted for publication in Astronomy and
Astrophysic
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