162 research outputs found
Absorption spectrum of the quasar HS1603+3820 I. Observations and data analysis
We present the analysis of multi-wavelength observations of bright quasar
HS1603+3820: the optical data taken with the MMT and Keck telescopes, and X-ray
data obtained with the Chandra X-ray Observatory. The optical spectra contain a
very large number of absorption lines from numerous heavy elements. We derived
X-ray properties of HS1603. The quasar has the optical-to-X-ray slope index
alpha_ox of 1.70, which is on the high end of the typical range for radio quiet
QSOs. We found 49 individual heavy element absorption clouds, which can be
grouped into eleven distinct systems. We determined column densities and
redshifts of the individual components. Absorbers from the associated system
which is likely spatially closest to the QSO show large CIV to HI column
density ratio, reaching ca.20.Comment: Accepted for publication in A&A, 17 pages, 11 figures, 5 table
Absorption spectra of Q 0000-263 and Q 1442+101
Studying the Lyman-alpha forest allows us to trace the cosmological distribution of matter through time, and may reveal insights into important questions such as the onset of galaxy formation. An equation for determining the number of Lyman-alpha absorption lines per redshift per rest equivalent in the Lyman-alpha forest is given. For a nonevolving population of clouds gamma = 1 for q(sub 0) = 0, and gamma = 0.5 for q(sub 0) = 0.5. A detailed study of the Lyman-alpha forests of Q 1442+101 at z(sub em) = 3.54 and Q 0000-263 at z(sub em) = 4.11
A Uniform Analysis of the Ly-alpha forest at z = 0 - 5: II. Measuring the mean intensity of the extragalactic ionizing background using the proximity effect
A homogeneous sample of 99 moderate resolution QSO spectra at z > 1.7 were
presented in Paper I, including 39 previously unpublished spectra from the
Multiple Mirror Telescope. The statistics of the Lyman alpha forest were
discussed. In this analysis, we demonstrate that a proximity effect is present
in the data, ie. there exists a significant (5.5) deficit of lines at
. Within 1.5 Mpc of the QSO emission redshift,
the significance does depend on QSO luminosity, in accordance with the theory
that this effect is caused by enhanced ionization of hydrogen in the vicinity
of the QSO from UV photons from the QSO itself. The photoionization model of
Bajtlik, Duncan, and Ostriker (1988) permits an estimate of the mean intensity
of the extragalactic background radiation at the Lyman limit. We compare the
results of this standard analysis with those obtained using a maximum
likelihood technique. The best fit value for is
7.0 x 10 ergs/s/cm/Hz/sr, over the redshift range
1.7 < z < 3.8, using QSO redshifts based on narrow emission lines. The best fit
value for the HI ionization rate is 1.9 x 10 s,
in good agreement with models of the background which incorporate QSOs only.
This large absorption line sample and these techniques for measuring the
background and understanding the systematics involved allow us to place what we
believe are are the firmest limits on the background at these redshifts.Comment: revised figures 13 and 14, and other minor corrections, 42 Latex
pages, 23 encapsulated Postscript figures, uses emulateapj.sty, To appear in
the Sept. 2000 ApJ
Strongly Variable z=1.48 FeII and MgII Absorption in the Spectra of z=4.05 GRB 060206
We report on the discovery of strongly variable FeII and MgII absorption
lines seen at z=1.48 in the spectra of the z=4.05 GRB 060206 obtained between
4.13 to 7.63 hours (observer frame) after the burst. In particular, the FeII
line equivalent width (EW) decayed rapidly from 1.72+-0.25 AA to 0.28+-0.21 AA,
only to increase to 0.96+-0.21 AA in a later date spectrum. The MgII doublet
shows even more complicated evolution: the weaker line of the doublet drops
from 2.05+-0.25 AA to 0.92+-0.32 AA, but then more than doubles to 2.47+-0.41
AA in later data. The ratio of the EWs for the MgII doublet is also variable,
being closer to 1:1 (saturated regime) when the lines are stronger and becoming
closer to 2:1 (unsaturated regime) when the lines are weaker, consistent with
expectations based on atomic physics. We have investigated and rejected the
possibility of any instrumental or atmospheric effects causing the observed
strong variations. Our discovery of clearly variable intervening FeII and MgII
lines lends very strong support to their scenario, in which the characteristic
size of intervening patches of MgII ``clouds'' is comparable to the GRB beam
size, i.e, about 10^16 cm. We discuss various implications of this discovery,
including the nature of the MgII absorbers, the physics of GRBs, and
measurements of chemical abundances from GRB and quasar absorption lines.Comment: 14 pages, 3 figures, 1 table; ApJ Letters, accepte
Chandra Detection of X-ray Absorption Associated with a Damped Lyman Alpha System
We have observed three quasars, PKS 1127-145, Q 1331+171 and Q0054+144, with
the ACIS-S aboard the Chandra X-ray Observatory, in order to measure soft X-ray
absorption associated with intervening 21-cm and damped Ly absorbers.
For PKS 1127-145, we detect absorption which, if associated with an intervening
z_{abs}=0.312 absorber, implies a metallicity of 23% solar. If the absorption
is not at z_{abs}=0.312, then the metallicity is still constrained to be less
than 23% solar. The advantage of the X-ray measurement is that the derived
metallicity is insensitive to ionization, inclusion of an atom in a molecule,
or depletion onto grains. The X-ray absorption is mostly due to oxygen, and is
consistent with the oxygen abundance of 30% solar derived from optical nebular
emission lines in a foreground galaxy at the redshift of the absorber.
For Q1331+171 and Q 0054+144, only upper limits were obtained, although the
exposure times were intentionally short, since for these two objects we were
interested primarily in measuring flux levels to plan for future observations.
The imaging results are presented in a companion paper.Comment: 23 pages, 6 figures, accepted for publication in the Astrophysical
Journa
The VMC Survey - VI. Quasars behind the Magellanic system
The number and spatial distribution of confirmed quasi-stellar objects (QSOs)
behind the Magellanic system is limited. This undermines their use as
astrometric reference objects for different types of studies. We have searched
for criteria to identify candidate QSOs using observations from the VISTA
survey of the Magellanic Clouds system (VMC) that provides photometry in the
YJKs bands and 12 epochs in the Ks band. The (Y-J) versus (J-Ks) diagram has
been used to distinguish QSO candidates from Milky Way stars and stars of the
Magellanic Clouds. Then, the slope of variation in the Ks band has been used to
identify a sample of high confidence candidates. These criteria were developed
based on the properties of 117 known QSOs presently observed by the VMC survey.
VMC YJKs magnitudes and Ks light-curves of known QSOs behind the Magellanic
system are presented. About 75% of them show a slope of variation in Ks>10^-4
mag/day and the shape of the light-curve is in general irregular and without
any clear periodicity. The number of QSO candidates found in tiles including
the South Ecliptic Pole and the 30 Doradus regions is 22 and 26, respectively,
with a ~20% contamination by young stellar objects, planetary nebulae, stars
and normal galaxies. By extrapolating the number of QSO candidates to the
entire VMC survey area we expect to find about 1200 QSOs behind the LMC, 400
behind the SMC, 200 behind the Bridge and 30 behind the Stream areas, but not
all will be suitable for astrometry. Further, the Ks band light-curves can help
support investigations of the mechanism responsible for the variations.Comment: 17 pages, 15 figures, replaced with accepted version by Astronomy &
Astrophysic
Discovery of four X-ray quasars behind the Large Magellanic Cloud
We present the discovery of four X-ray quasars (z_em = 0.26, 0.53, 0.61,
1.63) located behind the Large Magellanic Cloud; three of them are located
behind the bar of the LMC. The quasars were identified via spectroscopy of
optical counterparts to X-ray sources found serendipitously by the Chandra
X-ray Observatory satellite. All four quasars have archival VI photometry from
the OGLE-II project; one of them was found by OGLE to be variable. We present
the properties of the quasars and discuss their possible applications.Comment: AASTeX, 8 pages, 1 ps figure, accepted for publication in
Ap.J.Letter
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