2,139 research outputs found
[O III] Equivalent Width and Orientation Effects in Quasars
The flux of the [OIII] line is considered to be a good indicator of the
bolometric emission of quasars. The observed continuum emission from the
accretion disc should instead be strongly dependent on the inclination angle
theta between the disc axis and the line of sight. Based on this, the
equivalent width (EW) of [OIII] should provide a direct measure of theta. Here
we analyze the distribution of EW([OIII]) in a sample of ~6,000 SDSS quasars,
and find that it can be accurately reproduced assuming a relatively small
intrinsic scatter and a random distribution of inclination angles. This result
has several implications: 1) it is a direct proof of the disc-like emission of
the optical continuum of quasars; 2) the value of EW([OIII]) can be used as a
proxy of the inclination, to correct the measured continuum emission and then
estimate the bolometric luminosity of quasars; 3) the presence of almost
edge-on discs among broad line quasars implies that the accretion disc is not
aligned with the circumnuclear absorber, and/or that the covering fraction of
the latter is rather small. Finally, we show that a similar analysis of EW
distributions of broad lines (Hbeta, Mg II, C IV) provides no evidence of
inclination effects, suggesting a disc-like geometry of the broad emission line
region.Comment: 8 pages, 5 figures. Accepted for publication in MNRA
Mid-Infrared line diagnostics of Active Galaxies -- A spectroscopic AGN survey with ISO-SWS
We present medium resolution (R approx. 1500) ISO-SWS 2.4--45 micron spectra
of a sample of 29 galaxies with active nuclei. This data set is rich in fine
structure emission lines tracing the narrow line regions and (circum-)nuclear
star formation regions, and it provides a coherent spectroscopic reference for
future extragalactic studies in the mid-infrared. We use the data set to
briefly discuss the physical conditions in the narrow line regions (density,
temperature, excitation, line profiles) and to test for possible differences
between AGN sub-types. Our main focus is on new tools for determining the
propertibes of dusty galaxies and on the AGN-starburst connection. We present
mid-IR line ratio diagrams which can be used to identify composite (starburst +
AGN) sources and to distinguish between emission excited by active nuclei and
emission from (circum-nuclear) star forming regions. For instance, line ratios
of high to low excitation lines like [O IV]25.9um/[Ne II]12.8um, that have been
used to probe for AGNs in dusty objects, can be examined in more detail and
with better statistics now. In addition, we present two-dimensional diagnostic
diagrams that are fully analogous to classical optical diagnostic diagrams, but
better suited for objects with high extinction. Finally, we discuss
correlations of mid-infrared line fluxes to the mid- and far-infrared
continuum. We compare these relations to similar relations in starburst
galaxies in order to examine the contribution of AGNs to the bolometric
luminosities of their host galaxies. The spectra are available in electronic
form from the authors.Comment: 24 pages, 23 figures, 5 tables. Accepted for A&
Black-Hole Mass and Growth Rate at High Redshift
We present new H and K bands spectroscopy of 15 high luminosity active
galactic nuclei (AGNs) at redshifts 2.3-3.4 obtained on Gemini South. We
combined the data with spectra of additional 29 high-luminosity sources to
obtain a sample with 10^{45.2}<\lambda L_{\lambda}(5100A)<10^{47.3} ergs/sec
and black hole (BH) mass range, using reverberation mapping relationships based
on the H_beta method, of 10^{8.8}-10^{10.7} M_sun. We do not find a correlation
of L/L_Edd with M_BH but find a correlation with \lambda L_{\lambda}(5100A)
which might be due to selection effects. The L/L_Edd distribution is broad and
covers the range ~0.07-1.6, similar to what is observed in lower redshift,
lower luminosity AGNs. We suggest that this consistently measured and
calibrated sample gives the best representation of L/L_Edd at those redshifts
and note potential discrepancies with recent theoretical and observational
studies. The lower accretion rates are not in accord with growth scenarios for
BHs at such redshifts and the growth times of many of the sources are longer
than the age of the universe at the corresponding epochs. This suggests earlier
episodes of faster growth at z>~3 for those sources. The use of the C IV method
gives considerably different results and a larger scatter; this method seems to
be a poor M_BH and L/L_Edd estimator at very high luminosity.Comment: 8 pages (emulateapj), 4 figures. Accepted for publication in Ap
Analyzing X-ray variability by State Space Models
In recent years, autoregressive models have had a profound impact on the
description of astronomical time series as the observation of a stochastic
process. These methods have advantages compared with common Fourier techniques
concerning their inherent stationarity and physical background. If
autoregressive models are used, however, it has to be taken into account that
real data always contain observational noise often obscuring the intrinsic time
series of the object. We apply the technique of a Linear State Space Model
which explicitly models the noise of astronomical data and allows to estimate
the hidden autoregressive process. As an example, we have analysed a sample of
Active Galactic Nuclei (AGN) observed with EXOSAT and found evidence for a
relationship between the relaxation timescale and the spectral hardness.Comment: 4 pages, Latex, uses Kluwer Style file crckapb.cls To appear in Proc.
of Astronomical Time Series, Tel Aviv, 199
Vogt-Koyanagi-Harada syndrome - current perspectives
Vogt-Koyanagi-Harada syndrome is a cause of noninfectious panuveitis, leading to significant vision loss in many patients. It is an autoimmune disease occurring in genetically susceptible individuals and clinically presents as bilateral panuveitis with serous retinal detachments and hyperemic, swollen optic discs, which are associated with neurological and auditory manifestations. Early diagnosis and prompt and adequate treatment with immunosuppressive agents (corticosteroids and other immunosuppressive drugs) may halt disease progression and prevent recurrences and vision loss. This review summarizes the current knowledge on the variable clinical aspects of this disease, highlighting diagnostic and treatment strategies
On the Signatures of Gravitational Redshift: The Onset of Relativistic Emission Lines
Aims. We quantify the effect of gravitational redshift on emission lines to
explore the transition region from the Newtonian to the Einsteinian regime.
With the emitting region closer to the Kerr black hole, lines are successively
subjected to a stronger gravitationally induced shift and distortion. Simulated
lines are compared to broad, optical emission lines observed in Mrk 110.
Methods. We simulate relativistic emission line profiles by using Kerr ray
tracing techniques. Emitting regions are assumed to be thin equatorial rings in
stationary Keplerian rotation. The emission lines are characterised by a
generalized Doppler factor or redshift associated with the line core. Results.
With decreasing distance from the black hole, the gravitational redshift starts
to smoothly deviate from the Newtonian Doppler factor: Shifts of the line cores
reveal an effect at levels of 0.0015 to 60% at gravitational radii ranging from
10^{5} to 2. This corresponds to fully relativistic Doppler factors of 0.999985
to 0.4048. The intrinsic line shape distortion by strong gravity i.e. very
asymmetric lines occur at radii smaller than roughly ten gravitational radii.
Conclusions. Due to the asymptotical flatness of black hole space-time, GR
effects are ubiquitous and their onset can be tested observationally with
sufficient spectral resolution. With a resolving power of ~100000, yielding a
resolution of ~0.1 Angstroems for optical and near-infrared broad emission
lines like H\beta, HeII and Pa\alpha, the gravitational redshift can be probed
out to approximately 75000 gravitational radii. [abridged]Comment: 9 pages, 9 figures, accepted for publication in A&
A Single Intrinsic Luminosity Function for Both Type-I and Type-II Active Galactic Nuclei
The luminous electromagnetic emission from distant active galactic nuclei
(AGNs) including quasars is believed to be powered by accretion onto
super-massive black holes (SMBHs). In the standard unification model for AGNs a
dusty torus covers a significant portion of the viewing angles to the accretion
disk and the BH. The system is classified as a type-I AGN if the accretion disk
is viewed through the opening part; otherwise it is called a type-II AGN.
Therefore the ratio of type-II to type-I AGNs serves as a sensitive probe to
the unification model. A surprising discovery made from several large sky
coverage and/or deep AGN surveys has found a significant anti-correlation
between the type-II fraction and the observed X-ray luminosity between 2-10
keV. This suggests two different luminosity functions for the two types of
AGNs, thus challenging the AGN unification model. However this observed
anti-correlation is a natural consequence of the AGN unification model with
only one intrinsic luminosity function if the inclination angle effects of the
X-ray emitting accretion disk are taken into account. Thus the AGN unification
model survived another critical test.Comment: 10 pages, 2 figures, submitted on 2004 Oct. 20 and accepted on 2004
Dec. 1 for publication in ApJ Letter
XMM-Newton RGS observation of the warm absorber in Mrk 279
The Seyfert 1 galaxy Mrk 279 was observed by XMM-Newton in November 2005 in
three consecutive orbits, showing significant short-scale variability (average
soft band variation in flux ~20%). The source is known to host a two-component
warm absorber with distinct ionisation states from a previous Chandra
observation. We aim to study the warm absorber in Mrk 279 and investigate any
possible response to the short-term variations of the ionising flux, and to
assess whether it has varied on a long-term time scale with respect to the
Chandra observation. We find no significant changes in the warm absorber on
neither short time scales (~2 days) nor at longer time scales (two and a half
years), as the variations in the ionic column densities of the most relevant
elements are below the 90% confidence level. The variations could still be
present but are statistically undetected given the signal-to-noise ratio of the
data. Starting from reasonable standard assumptions we estimate the location of
the absorbing gas, which is likely to be associated with the putative dusty
torus rather than with the Broad Line Region if the outflowing gas is moving at
the escape velocity or larger.Comment: 10 pages, 9 figures, 6 tables. Accepted for publication in Astronomy
& Astrophysic
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