371 research outputs found
XMM-Newton View of PKS 2155-304: Characterizing the X-ray Variability Properties with EPIC-PN
Starting from XMM-Newton EPIC-PN data, we present the X-ray variability
characteristics of PKS 2155-304 using a simple analysis of the excess variance,
\xs, and of the fractional rms variability amplitude, fvar. The scatter in \xs\
and \fvar, calculated using 500 s long segments of the light curves, is smaller
than the scatter expected for red noise variability. This alone does not imply
that the underlying process responsible for the variability of the source is
stationary, since the real changes of the individual variance estimates are
possibly smaller than the large scatters expected for a red noise process. In
fact the averaged \xs and \fvar, reducing the fluctuations of the individual
variances, chang e with time, indicating non-stationary variability. Moreover,
both the averaged \sqxs (absolute rms variability amplitude) and \fvar show
linear correlation with source flux but in an opposite sense: \sqxs correlates
with flux, but \fvar anti-correlates with flux. These correlations suggest that
the variability process of the source is strongly non-stationary as random
scatters of variances should not yield any correlation. \fvar spectra were
constructed to compare variability amplitudes in different energy bands. We
found that the fractional rms variability amplitude of the source, when
significant variability is observed, increases logarithmically with the photon
energy, indicating significant spectral variability. The point-to-point
variability amplitude may also track this trend, suggesting that the slopes of
the power spectral density of the source are energy-independent. Using the
normalized excess variance the black hole mass of \pks was estimated to be
about . This is compared and contrasted with the
estimates derived from measurements of the host galaxies.Comment: Accepted for publication in The Astrophysical Journa
Examining the Seyfert - Starburst Connection with Arcsecond Resolution Radio Continuum Observations
We compare the arcsecond-scale circumnuclear radio continuum properties
between five Seyfert and five starburst galaxies, concentrating on the search
for any structures that could imply a spatial or causal connection between the
nuclear activity and a circumnuclear starburst ring. No evidence is found in
the radio emission for a link between the triggering or feeding of nuclear
activity and the properties of circumnuclear star formation. Conversely, there
is no clear evidence of nuclear outflows or jets triggering activity in the
circumnuclear rings of star formation. Interestingly, the difference in the
angle between the apparent orientation of the most elongated radio emission and
the orientation of the major axis of the galaxy is on average larger in
Seyferts than in starburst galaxies, and Seyferts appear to have a larger
physical size scale of the circumnuclear radio continuum emission. The
concentration, asymmetry, and clumpiness parameters of radio continuum emission
in Seyferts and starbursts are comparable, as are the radial profiles of radio
continuum and near-infrared line emission. The circumnuclear star formation and
supernova rates do not depend on the level of nuclear activity. The radio
emission usually traces the near-infrared Br-gamma and H2 1-0 S(1) line
emission on large spatial scales, but locally their distributions are
different, most likely because of the effects of varying local magnetic fields
and dust absorption and scattering.Comment: 21 pages, 10 figures. Accepted for publication in the Astronomical
Journa
Morphology of the 12-micron Seyfert Galaxies: II. Optical and Near-Infrared Image Atlas
We present 263 optical and near-infrared (NIR) images for 42 Seyfert 1s and
48 Seyfert 2s, selected from the Extended 12-micron Galaxy Sample.
Elliptically-averaged profiles are derived from the images, and isophotal radii
and magnitudes are calculated from these. We also report virtual aperture
photometry, that judging from comparison with previous work, is accurate to
roughly 0.05mag in the optical, and 0.07mag in the NIR. Our B-band isophotal
magnitude and radii, obtained from ellipse fitting, are in good agreement with
those of RC3. When compared with the B band, V, I, J, and K isophotal diameters
show that the colors in the outer regions of Seyferts are consistent with the
colors of normal spirals. Differences in the integrated isophotal colors and
comparison with a simple model show that the active nucleus+bulge is stronger
and redder in the NIR than in the optical. Finally, roughly estimated Seyfert
disk surface brightnesses are significantly brighter in B and K than those in
normal spirals of similar morphological type.Comment: 17 pgs including figures; Table 2 is a separate file. Complete Figure
1 is available by contacting the authors. Accepted for publication in ApJ
Clinical findings in relation to mortality in non-tuberculous mycobacterial infections : patients with Mycobacterium avium complex have better survival than patients with other mycobacteria
We compared the clinical findings and survival in patients with Mycobacterium avium complex (MAC) and other non-tuberculous mycobacteria (NTM). A total of 167 adult non-human immunodeficiency virus (HIV) patients with at least one positive culture for NTM were included. Medical records were reviewed. The patients were categorised according to the 2007 American Thoracic Society (ATS) criteria. MAC comprised 59 % of all NTM findings. MAC patients were more often female (70 % vs. 34 %, p <0.001) and had less fatal underlying diseases (23 % vs. 47 %, p = 0.001) as compared to other NTM patients. Symptoms compatible with NTM infection had lasted for less than a year in 34 % of MAC patients but in 54 % of other NTM patients (p = 0.037). Pulmonary MAC patients had a significantly lower risk of death compared to pulmonary other NTM (hazard ratio [HR] 0.50, 95 % confidence interval [CI] 0.33-0.77, p = 0.002) or subgroup of other slowly growing NTM (HR 0.55, 95 % CI 0.31-0.99, p = 0.048) or as rapidly growing NTM (HR 0.47, 95 % CI 0.25-0.87, p = 0.02). The median survival time was 13.0 years (95 % CI 5.9-20.1) for pulmonary MAC but 4.6 years (95 % CI 3.4-5.9) for pulmonary other NTM. Serious underlying diseases (HR 3.21, 95 % CI 2.05-5.01, p <0.001) and age (HR 1.07, 95 % CI 1.04-1.09, p <0.001) were the significant predictors of mortality and female sex was a predictor of survival (HR 0.38, 95 % CI 0.24-0.59, p <0.001) in the multivariate analysis. Pulmonary MAC patients had better prognosis than pulmonary other NTM patients. The symptom onset suggests a fairly rapid disease course.Peer reviewe
HST Observations of the Serendipitous X-ray Companion to Mrk 273: Cluster at z=0.46?
We have used HST I-band images to identify Mrk 273X, the very unusual
high-redshift X-ray-luminous Seyfert 2 galaxy found by ROSAT in the same
field-of-view as Mrk 273. We have measured the photometric properties of Mrk
273X and have also analyzed the luminosity distribution of the faint galaxy
population seen in the HST image. The luminosity of the galaxy and the
properties of the surrounding environment suggest that Mrk 273X is the
brightest galaxy in a relatively poor cluster at a redshift near 0.46. Its
off-center location in the cluster and the presence of other galaxy groupings
in the HST image may indicate that this is a dynamically young cluster on the
verge of merging with its neighboring clusters. We find that Mrk 273X is a
bright featureless elliptical galaxy with no evidence for a disk. It follows
the de Vaucouleurs (r^{1/4}) surface brightness law very well over a range of 8
magnitudes. Though the surface brightness profile does not appear to be
dominated by the AGN, the galaxy has very blue colors that do appear to be
produced by the AGN. Mrk 273X is most similar to the IC 5063 class of active
galaxies --- a hybrid Sy 2 / powerful radio galaxy.Comment: Accepted for publication in the Astrophysical Journal. 8 pages,
including 4 postscript figures. Uses emulateapj.sty and psfig.sty. Higher
quality version of Figure 1 is available at
http://rings.gsfc.nasa.gov/~borne/fig1-markgals.gi
Inner Size of a Dust Torus in the Seyfert 1 Galaxy NGC 4151
The most intense monitoring observations yet made were carried out on the
Seyfert 1 galaxy NGC 4151 in the optical and near-infrared wave-bands. A lag
from the optical light curve to the near-infrared light curve was measured. The
lag-time between the V and K light curves at the flux minimum in 2001 was
precisely 48+2-3 days, as determined by a cross-correlation analysis. The
correlation between the optical luminosity of an active galactic nucleus (AGN)
and the lag-time between the UV/optical and the near-infrared light curves is
presented for NGC 4151 in combination with previous lag-time measurements of
NGC 4151 and other AGNs in the literature. This correlation is interpreted as
thermal dust reverberation in an AGN, where the near-infrared emission from an
AGN is expected to be the thermal re-radiation from hot dust surrounding the
central engine at a radius where the temperature equals to that of the dust
sublimation temperature. We find that the inner radius of the dust torus in NGC
4151 is 0.04 pc corresponding to the measured lag-time, well outside
the broad line region (BLR) determined by other reverberation studies of the
emission lines.Comment: Accepted for publication in ApJ Letters, 13 pages, 3 figures;
Corrected typo
Obscuration in the Host Galaxies of Soft X-ray Selected Seyferts
We define a new sample of 96 low-redshift (z<0.1), soft X-ray selected
Seyferts from the catalog of the Einstein Slew Survey (Elvis etal. 1992,
Plummer et al. 1994). We probe the geometry and column depth of obscuring
material in the host-galaxy disks using galaxian axial ratios determined mainly
from the Digitized Sky Survey. The distribution of host-galaxy axial ratios
clearly shows a bias against edge-on spirals, confirming the existence of a
geometrically thick layer of obscuring material in the host-galaxy planes. Soft
X-ray selection recovers some of the edge-on objects missed in UV and visible
surveys but still results in 30% incompleteness for Type 1's. We speculate that
thick rings of obscuring material like the ones we infer for these Seyferts
might be commonly present in early type spirals, sitting at the Inner Lindblad
Resonances of the nonaxisymmetric potentials of the host galaxies.Comment: 14 pages including 2 tables and 3 eps figures, aas2pp4.sty, to appear
in Ap
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