339 research outputs found
Panton-Valentine Leucocidin-Positive Staphylococcus Aureus Gonarthritis in a Healthy Adult Leads To Fulminant Sepsis with Multiple Metastatic Soft Tissue Infection and Necessity of Extracorporeal Membrane Oxygenation
Background: Infections with Panton-Valentine leucocidin (PVL) positive Staphylococcus aureus ( S. aureus ) are often complicated by necrotizing pneumonia, myositis and osteomyelitis. Case Description: We describe a 50 years old, previously healthy male which presented a severe infection with PVL-positive, methicillin- susceptible S. aureus (MSSA) in his left knee after returning from China. He developed a fulminant sepsis with necrotizing pneumonia, acute respiratory distress syndrome (ARDS), acute renal failure and multiple soft tissue abscesses. Extra-corporeal membrane oxygenation (ECMO) was needed for five days. The patient recovered after multiple surgical interventions and long-term antibiotic treatment and eventually returned to work five months after initial admission. Conclusion: While most staphylococcal skin and soft tissue infections (SSTI) show a favorable outcome, SSTI caused by PVL- positive bacteria can lead to fulminant and fatal disease manifestations. Immunocompetent individuals are equally affected as immunocompromised ones. Early suspicion, surgical intervention with debridement and drainage of abscess formations are of key importance in concert with appropriate antibiotic therapy without delay. Imaging should be done to identify clinically silent foci
Exploratory Chandra Observations of the Three Highest Redshift Quasars Known
We report on exploratory Chandra observations of the three highest redshift
quasars known (z = 5.82, 5.99, and 6.28), all found in the Sloan Digital Sky
Survey. These data, combined with a previous XMM-Newton observation of a z =
5.74 quasar, form a complete set of color-selected, z > 5.7 quasars. X-ray
emission is detected from all of the quasars at levels that indicate that the
X-ray to optical flux ratios of z ~ 6 optically selected quasars are similar to
those of lower redshift quasars. The observations demonstrate that it will be
feasible to obtain quality X-ray spectra of z ~ 6 quasars with current and
future X-ray missions.Comment: 15 pages, ApJL, in press; small revisions to address referee Comment
The Evolution of Quasar CIV and SiIV Broad Absorption Lines Over Multi-Year Time Scales
We investigate the variability of CIV 1549A broad absorption line (BAL)
troughs over rest-frame time scales of up to ~7 yr in 14 quasars at redshifts
z>2.1. For 9 sources at sufficiently high redshift, we also compare CIV and
SiIV 1400A absorption variation. We compare shorter- and longer-term
variability using spectra from up to four different epochs per source and find
complex patterns of variation in the sample overall. The scatter in the change
of absorption equivalent width (EW), Delta EW, increases with the time between
observations. BALs do not, in general, strengthen or weaken monotonically, and
variation observed over shorter (<months) time scales is not predictive of
multi-year variation. We find no evidence for asymmetry in the distribution of
Delta EW that would indicate that BALs form and decay on different time scales,
and we constrain the typical BAL lifetime to be >~30 yr. The BAL absorption for
one source, LBQS 0022+0150, has weakened and may now be classified as a
mini-BAL. Another source, 1235+1453, shows evidence of variable, blue continuum
emission that is relatively unabsorbed by the BAL outflow. CIV and SiIV BAL
shape changes are related in at least some sources. Given their high
velocities, BAL outflows apparently traverse large spatial regions and may
interact with parsec-scale structures such as an obscuring torus. Assuming BAL
outflows are launched from a rotating accretion disk, notable azimuthal
symmetry is required in the outflow to explain the relatively small changes
observed in velocity structure over times up to 7 yr
Microvessel stenosis, enlarged perivascular spaces, and fibrinogen deposition are associated with ischemic periventricular white matter hyperintensities
Periventricular white matter hyperintensities (pvWMH) are neuroimaging abnormalities surrounding the lateral ventricles that are apparent on magnetic resonance imaging (MRI). They are associated with age, neurodegenerative disease, and cerebrovascular risk factors. While pvWMH ultimately represent a loss of white matter structural integrity, the pathological causes are heterogeneous in nature, and currently, cannot be distinguished using neuroimaging alone. pvWMH could occur because of a combination of small vessel disease (SVD), ependymal loss, blood–brain barrier dysfunction, and microgliosis. In this study we aimed to characterize microvascular stenosis, fibrinogen extravasation, and microgliosis within pvWMH with and without imaging evidence of periventricular infarction. Using postmortem neuroimaging of human brains (n = 20), we identified pvWMH with and without periventricular infarcts (PVI). We performed histological analysis of microvessel stenosis, perivascular spaces, microgliosis, and immunohistochemistry against fibrinogen as a measure of serum protein extravasation. Herein, we report distinctions between pvWMH with and without periventricular infarcts based on associations with microvessel stenosis, enlarged perivascular spaces, and fibrinogen IHC. Microvessel stenosis was significantly associated with PVI and with cellular deposition of fibrinogen in the white matter. The presence of fibrinogen was associated with PVI and increased number of microglia. These findings suggest that neuroimaging-based detection of infarction within pvWMH may help distinguish more severe lesions, associated with underlying microvascular disease and BBB dysfunction, from milder pvWMH that are a highly frequent finding on MRI
Probing the Origins of the CIV and Fe Kalpha Baldwin Effect
We use UV/optical and X-ray observations of 272 radio-quiet Type 1 AGNs and
quasars to investigate the CIV Baldwin Effect (BEff). The UV/optical spectra
are drawn from the Hubble Space Telescope, International Ultraviolet Explorer
and Sloan Digital Sky Survey archives. The X-ray spectra are from the Chandra
and XMM-Newton archives. We apply correlation and partial-correlation analyses
to the equivalent widths, continuum monochromatic luminosities, and alpha_ox,
which characterizes the relative X-ray to UV brightness. The equivalent width
of the CIV 1549 emission line is correlated with both alpha_ox and luminosity.
We find that by regressing l_UV with EW(CIV) and alpha_ox, we can obtain
tighter correlations than by regressing l_UV with only EW(CIV). Both
correlation and regression analyses imply that l_UV is not the only factor
controlling the changes of EW(CIV); alpha_ox (or, equivalently, the soft X-ray
emission) plays a fundamental role in the formation and variation of CIV.
Variability contributes at least 60% of the scatter of the EW(CIV)-l_UV
relation and at least 75% of the scatter of the of the EW(CIV)-alpha_ox
relation.
In our sample, narrow Fe Kalpha 6.4 keV emission lines are detected in 50
objects. Although narrow Fe Kalpha exhibits a BEff similar to that of CIV, its
equivalent width has almost no dependence on either alpha_ox or EW(CIV). This
suggests that the majority of narrow Fe Kalpha emission is unlikely to be
produced in the broad emission-line region. We do find suggestive correlations
between the emission-line luminosities of CIV and Fe Kalpha, which could be
potentially used to estimate the detectability of the Fe Kalpha line of quasars
from rest-frame UV spectroscopic observations
High-Redshift SDSS Quasars with Weak Emission Lines
We identify a sample of 74 high-redshift quasars (z>3) with weak emission
lines from the Fifth Data Release of the Sloan Digital Sky Survey and present
infrared, optical, and radio observations of a subsample of four objects at
z>4. These weak emission-line quasars (WLQs) constitute a prominent tail of the
Lya+NV equivalent width distribution, and we compare them to quasars with more
typical emission-line properties and to low-redshift active galactic nuclei
with weak/absent emission lines, namely BL Lac objects. We find that WLQs
exhibit hot (T~1000 K) thermal dust emission and have rest-frame 0.1-5 micron
spectral energy distributions that are quite similar to those of normal
quasars. The variability, polarization, and radio properties of WLQs are also
different from those of BL Lacs, making continuum boosting by a relativistic
jet an unlikely physical interpretation. The most probable scenario for WLQs
involves broad-line region properties that are physically distinct from those
of normal quasars.Comment: Updated to match version published in ApJ. 20 pages, 12 figure
AGN accretion disks as spatially resolved by polarimetry
A crucial difficulty in understanding the nature of the putative accretion
disk in AGNs is that some of its key intrinsic spectral signatures cannot be
observed directly. The strong emissions from the broad-line region (BLR) and
the obscuring torus, which are generally yet to be spatially resolved,
essentially 'bury' such signatures. Here we argue that we can actually isolate
the disk emission spectrum by using optical and near-infrared polarization of
quasars and uncover the important spectral signatures. In these quasars, the
polarization is considered to originate from electron scattering interior to
the BLR, so that the polarized flux shows the disk spectrum with all the
emissions from the BLR and torus eliminated. The polarized flux observations
have now revealed a Balmer edge feature in absorption and a blue near-infrared
spectral shape consistent with a specific and robust theoretical prediction.
These results critically verify the long-standing picture of an optically thick
and locally heated disk in AGNs.Comment: Proceedings for "The Universe under the Microscope" (AHAR 2008), held
in Bad Honnef (Germany) in April 2008, to be published in Journal of Physics:
Conference Series by Institute of Physics Publishing, R. Schoedel, A. Eckart,
S. Pfalzner, and E. Ros (eds.
Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Quasar Sample
We describe the algorithm for selecting quasar candidates for optical
spectroscopy in the Sloan Digital Sky Survey. Quasar candidates are selected
via their non-stellar colors in "ugriz" broad-band photometry, and by matching
unresolved sources to the FIRST radio catalogs. The automated algorithm is
sensitive to quasars at all redshifts lower than z=5.8. Extended sources are
also targeted as low-redshift quasar candidates in order to investigate the
evolution of Active Galactic Nuclei (AGN) at the faint end of the luminosity
function. Nearly 95% of previously known quasars are recovered (based on 1540
quasars in 446 square degrees). The overall completeness, estimated from
simulated quasars, is expected to be over 90%, whereas the overall efficiency
(quasars:quasar candidates) is better than 65%. The selection algorithm targets
ultraviolet excess quasars to i^*=19.1 and higher-redshift (z>3) quasars to
i^*=20.2, yielding approximately 18 candidates per square degree. In addition
to selecting ``normal'' quasars, the design of the algorithm makes it sensitive
to atypical AGN such as Broad Absorption Line quasars and heavily reddened
quasars.Comment: 62 pages, 15 figures (8 color), 8 tables. Accepted by AJ. For a
version with higher quality color figures, see
http://archive.stsci.edu/sdss/quasartarget/RichardsGT_qsotarget.preprint.p
The Ensemble Photometric Variability of ~25000 Quasars in the Sloan Digital Sky Survey
Using a sample of over 25000 spectroscopically confirmed quasars from the
Sloan Digital Sky Survey, we show how quasar variability in the rest frame
optical/UV regime depends upon rest frame time lag, luminosity, rest
wavelength, redshift, the presence of radio and X-ray emission, and the
presence of broad absorption line systems. The time dependence of variability
(the structure function) is well-fit by a single power law on timescales from
days to years. There is an anti-correlation of variability amplitude with rest
wavelength, and quasars are systematically bluer when brighter at all
redshifts. There is a strong anti-correlation of variability with quasar
luminosity. There is also a significant positive correlation of variability
amplitude with redshift, indicating evolution of the quasar population or the
variability mechanism. We parameterize all of these relationships. Quasars with
RASS X-ray detections are significantly more variable (at optical/UV
wavelengths) than those without, and radio loud quasars are marginally more
variable than their radio weak counterparts. We find no significant difference
in the variability of quasars with and without broad absorption line troughs.
Models involving multiple discrete events or gravitational microlensing are
unlikely by themselves to account for the data. So-called accretion disk
instability models are promising, but more quantitative predictions are needed.Comment: 41 pages, 21 figures, AASTeX, Accepted for publication in Ap
The Sloan Digital Sky Survey Quasar Catalog V. Seventh Data Release
We present the fifth edition of the Sloan Digital Sky Survey (SDSS) Quasar
Catalog, which is based upon the SDSS Seventh Data Release. The catalog, which
contains 105,783 spectroscopically confirmed quasars, represents the conclusion
of the SDSS-I and SDSS-II quasar survey. The catalog consists of the SDSS
objects that have luminosities larger than M_i = -22.0 (in a cosmology with H_0
= 70 km/s/Mpc Omega_M = 0.3, and Omega_Lambda = 0.7) have at least one emission
line with FWHM larger than 1000 km/s or have interesting/complex absorption
features, are fainter than i > 15.0 and have highly reliable redshifts. The
catalog covers an area of 9380 deg^2. The quasar redshifts range from 0.065 to
5.46, with a median value of 1.49; the catalog includes 1248 quasars at
redshifts greater than four, of which 56 are at redshifts greater than five.
The catalog contains 9210 quasars with i < 18; slightly over half of the
entries have i< 19. For each object the catalog presents positions accurate to
better than 0.1" rms per coordinate, five-band (ugriz) CCD-based photometry
with typical accuracy of 0.03 mag, and information on the morphology and
selection method. The catalog also contains radio, near-infrared, and X-ray
emission properties of the quasars, when available, from other large-area
surveys. The calibrated digital spectra cover the wavelength region 3800-9200
Ang. at a spectral resolution R = 2000 the spectra can be retrieved from the
SDSS public database using the information provided in the catalog. Over 96% of
the objects in the catalog were discovered by the SDSS. We also include a
supplemental list of an additional 207 quasars with SDSS spectra whose archive
photometric information is incomplete.Comment: Accepted, to appear in AJ, 7 figures, electronic version of Table 2
is available, see
http://www.sdss.org/dr7/products/value_added/qsocat_dr7.htm
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