85 research outputs found
Role of Gut Microbiota-Immunity Axis in Patients Undergoing Surgery for Colorectal Cancer: Focus on Short and Long-Term Outcomes
The formerly X-ray reflection-dominated Seyfert~2 galaxy NGC6300
In this paper, a BeppoSAX observation of the bright Seyfert 2 galaxy NGC6300
is presented. The rapidly variable emission from the active nucleus is seen
through a Compton-thin (NH ~ 3x10^23 atomoms/cm/cm) absorber. A
Compton-reflection component with an unusually high reflection fraction (R ~
4.2), and the comparison with a reflection-dominated spectrum measured by RXTE
two and half years earlier suggest that NGC6300 belongs to the class of
"transient" AGN, undergoing long and repeated periods of low-activity. The
spectral transition provides support to the idea that Compton-thick and
Compton-thin X-ray absorbers in Seyfert 2 galaxies are decoupled, the former
being most likely associated with the "torus", whereas the latter is probably
located at much larger distances.Comment: 5 Latex pages, 5 figures, To appear in Monthly Notices of the Royal
Astronomical Society (Letters
Enhanced Star Formation in Narrow Line Seyfert 1 AGN revealed by Spitzer
We present new low resolution Spitzer mid-infrared spectroscopy of a sample
of 20 ROSAT selected local Narrow Line Seyfert 1 galaxies (NLS1s). We detect
strong AGN continuum in all and clear PAH emission in 70% of the sources. The
6.2 micron PAH luminosity spans three orders of magnitudes, from ~10^(39) erg/s
to ~10^(42) erg/s providing strong evidence for intense ongoing star formation
in the circumnuclear regions of these sources. Using the IRS/Spitzer archive we
gather a large number of additional NLS1s and their broad line counterparts
(BLS1s) and constructed NLS1 and BLS1 sub-samples to compare them in various
ways. The comparison shows a clear separation according to FWHM(H_beta) such
that objects with narrower broad H_beta lines are the strongest PAH emitters.
We test this division in various ways trying to remove biases due to luminosity
and aperture size. Specifically, we find that star formation activity around
NLS1 AGN is larger than around BLS1 of the same AGN luminosity. The above
result seems to hold over the entire range of distance and luminosity. Moreover
the star formation rate is higher in low black hole mass and high L/L_Edd
systems indicating that black hole growth and star formation are occurring
simultaneously.Comment: 30 pages, 11 figures, 4 tables. Now accepted in MNRA
Testing current synthesis models of the X-ray background
We present synthesis models of the X-ray background where the available X-ray
observational constraints are used to derive information on the AGN population
properties. We show the need for luminous X-ray absorbed AGNs, the QSO2s, in
reproducing the 2-10 keV source counts at relatively bright fluxes. We compare
a model where the evolution of absorbed AGNs is faster than that of unabsorbed
ones, with a standard model where absorbed and unabsorbed AGNs evolve at the
same rate. It is found that an increase by a factor of ~2 from z=0 to z~1.3 in
the ratio between absorbed and unabsorbed AGNs would provide a significant
improvement in the data description. Finally, we make predictions on the AGNs
to be observed in deep X-ray surveys which contain information on the AGN space
density at high redshift.Comment: 11 pages with 8 figures, A&A accepte
Chandra unveils a binary Active Galactic Nucleus in Mrk463
We analyse Chandra, XMM-Newton and HST data of the double-nucleus
Ultraluminous Infrared Galaxy (ULIRG), Mrk463. The Chandra detection of two
luminous ( and
erg cm s), unresolved nuclei in Mrk~463
indicates that this galaxy hosts a binary AGN, with a projected separation of
kpc ( arcsec). While the East nucleus was already
known to be a Seyfert 2 (and this is further confirmed by our Chandra detection
of a neutral iron line), this is the first unambiguous evidence in favour of
the AGN nature of the West nucleus. Mrk463 is therefore the clearest case so
far for a binary AGN, after NGC6240.Comment: 7 pages, 7 figures, accepted for publication in MNRA
Local Supermassive Black Holes, Relics of Active Galactic Nuclei and the X-ray Background
We quantify the importance of mass accretion during AGN phases in the growth
of supermassive black holes (BH) by comparing the mass function of black holes
in the local universe with that expected from AGN relics, which are black holes
grown entirely with mass accretion during AGN phases. The local BH mass
function (BHMF) is estimated by applying the well-known correlations between BH
mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and
velocity functions. The density of BH's in the local universe is 4.6 (-1.4;
+1.9) (h/0.7)^2 10^5 Msun Mpc^-3. The relic BHMF is derived from the continuity
equation with the only assumption that AGN activity is due to accretion onto
massive BH's and that merging is not important. We find that the relic BHMF at
z=0 is generated mainly at z<3. Moreover, the BH growth is anti-hierarchical in
the sense that smaller BH's (MBH< 10^7 Msun) grow at lower redshifts (z<1) with
respect to more massive one's (z~1-3). Unlike previous work, we find that the
BHMF of AGN relics is perfectly consistent with the local BHMF indicating the
local BH's were mainly grown during AGN activity. This agreement is obtained
while satisfying, at the same time, the constraints imposed from the X-ray
background. The comparison with the local BHMF also suggests that the merging
process is not important in shaping the relic BHMF, at least at low redshifts
(z<3). Our analysis thus suggests the following scenario: local black holes
grew during AGN phases in which accreting matter was converted into radiation
with efficiencies epsilon = 0.04-0.16 and emitted at a fraction lambda =
0.1-1.7 of the Eddington luminosity. The average total lifetime of these active
phases ranges from ~4.5 10^8 yr for MBH
10^9 Msun. (abridged)Comment: 19 pages, 18 figures, MNRAS in press, minor changes following
referee's comment
The host galaxy/AGN connection. Brightness profiles of early-type galaxies hosting Seyfert nuclei
[ABRIDGED] We recently presented evidence of a connection between the
brightness profiles of nearby early-type galaxies and the properties of the AGN
they host. The radio loudness of the AGN appears to be univocally related to
the host's brightness profile: radio-loud nuclei are only hosted by ``core''
galaxies while radio-quiet AGN are only found in ``power-law'' galaxies. We
extend our analysis here to a sample of 42 nearby (V < 7000 km/s) Seyfert
galaxies hosted by early-type galaxies. We used the available HST images to
study their brightness profiles. Having excluded complex and highly nucleated
galaxies, in the remaining 16 objects the brightness profiles can be
successfully modeled with a Nuker law with a steep nuclear cusp characteristic
of ``power-law'' galaxies (with logarithmic slope 0.51 - 1.07). This result is
what is expected for these radio-quiet AGN based on our previous findings, thus
extending the validity of the connection between brightness profile and radio
loudness to AGN of a far higher luminosity. We explored the robustness of this
result against a different choice of the analytic form for the brightness
profiles, using a Sersic law. In no object could we find evidence of a central
light deficit with respect to a pure Sersic model, the defining feature of
``core'' galaxies in this modeling framework. We conclude that, regardless of
the modeling strategy, the dichotomy of AGN radio loudness can be univocally
related to the host's brightness profile. Our general results can be re-phrased
as ``radio-loud nuclei are hosted by core galaxies, while radio-quiet AGN are
found in non-core galaxies''.Comment: Accepted for publication in A&
Detecting quasars at very high redshift with next generation X-ray telescopes
The next generation of X-ray telescopes have the potential to detect faint
quasars at very high redshift and probe the early growth of massive black holes
(BHs). We present modelling of the evolution of the optical and X-ray AGN
luminosity function at 2 < z < 6 based on a CDM merger-driven model for the
triggering of nuclear activity combined with a variety of fading laws. We
extrapolate the merger-driven models to z > 6 for a range of BH growth
scenarios. We predict significant numbers of sources at z ~ 6 with fluxes just
an order of magnitude below the current detection limits and thus detectable
with XEUS and Constellation-X, relatively independently of the fading law
chosen. The predicted number of sources at even higher redshift depends
sensitively on the early growth history of BHs. For passive evolution models in
which BHs grow constantly at their Eddington limit, detectable BHs may be rare
beyond z ~ 10 even with Generation-X. However, in the more probable scenario
that BH growth at z > 6 can be described by passive evolution with a small duty
cycle, or by our merger driven accretion model, then we predict that XEUS and
Generation-X will detect significant numbers of black holes out to z ~ 10 and
perhaps beyond.Comment: 18 pages, 11 Figures. Version accepted to MNRAS; extra data plotted,
XEUS and Con-X sensitivities corrected and predictions amended accordingl
The physics of galactic winds driven by active galactic nuclei
Active galactic nuclei (AGN) drive fast winds in the interstellar medium of
their host galaxies. It is commonly assumed that the high ambient densities and
intense radiation fields in galactic nuclei imply short cooling times, thus
making the outflows momentum-conserving. We show that cooling of high-velocity,
shocked winds in AGN is in fact inefficient in a wide range of circumstances,
including conditions relevant to ultra-luminous infrared galaxies (ULIRGs),
resulting in energy-conserving outflows. We further show that fast
energy-conserving outflows can tolerate a large amount of mixing with cooler
gas before radiative losses become important. For winds with initial velocity
v_in>~10,000 km s^-1, as observed in ultra-violet and X-ray absorption, the
shocked wind develops a two-temperature structure. While most of the thermal
pressure support is provided by the protons, the cooling processes operate
directly only on the electrons. This significantly slows down inverse Compton
cooling, while free free cooling is negligible. Slower winds with v_in~1,000 km
s^-1, such as may be driven by radiation pressure on dust, can also experience
energy-conserving phases but under more restrictive conditions. During the
energy-conserving phase, the momentum flux of an outflow is boosted by a factor
~v_in/2v_s by work done by the hot post-shock gas, where v_s is the velocity of
the swept-up material. Energy-conserving outflows driven by fast AGN winds
(v_in~0.1c) may therefore explain the momentum fluxes Pdot>>L_AGN/c of
galaxy-scale outflows recently measured in luminous quasars and ULIRGs. Shocked
wind bubbles expanding normal to galactic disks may also explain the
large-scale bipolar structures observed in some systems, including around the
Galactic Center, and can produce significant radio, X-ray, and gamma-ray
emission. [Abridged]Comment: 20 pages, 8 figures. MNRAS, in pres
A physical model for the origin of the diffuse cosmic infrared background
We present a physical model for origin of the cosmic diffuse infrared
background (CDIRB). By utilizing the observed stellar mass function and its
evolution as input to a semi-empirical model of galaxy formation, we isolate
the physics driving diffuse IR emission. The model includes contributions from
three primary sources of IR emission: steady-state star formation owing to
isolated disk galaxies, interaction-driven bursts of star formation owing to
close encounters and mergers, and obscured active galactic nuclei (AGN). We
find that most of the CDIRB is produced by equal contributions from objects at
z=0.5-1 and z>1, as suggested by recent observations. Of those sources, the
vast majority of the emission originates in systems with low to moderate IR
luminosities (L_{IR}<10^{12} $L_sun); the most luminous objects contribute
significant flux only at high-redshifts (z>2). All star formation in ongoing
mergers accounts for <10% of the total at all wavelengths and redshifts, while
emission directly attributable to the interaction-driven burst itself accounts
for <5%. We furthermore find that obscured AGN contribute <1-2% of the CDIRB at
all wavelengths and redshifts, with a strong upper limit of less than 4% of the
total emission. Finally, since electron-positron pair production interactions
with the CDIRB represent the primary source of opacity to very high energy
(VHE: E_\gamma > 1 TeV) \gamma-rays, the model provides predictions for the
optical depth of the Universe to the most energetic photons. We find that these
predictions agree with observations of high-energy cutoffs at TeV energies in
nearby blazars, and suggest that while the Universe is extremely optically
thick at >10 TeV, the next generation of VHE \gamma-ray telescopes can
reasonably expect detections from out to 50-150 Mpc.Comment: 14 pages, 13 figures, submitted to MNRA
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