855 research outputs found
Infrared spectroscopic diagnostics for Active Galactic Nuclei
Infrared spectroscopy in the mid- and far-infrared provides powerful
diagnostics for studying the emission regions in active galaxies. The large
variety of ionic fine structure lines can probe gas conditions in a variety of
physical conditions, from highly ionized gas excited by photons originated by
black hole accretion to gas photoionized by young stellar systems. The critical
density and the ionization potential of these transitions allow to fully cover
the density-ionization parameter space. Some examples of line ratios diagrams
using both mid-infrared and far-infrared ionic fine structure lines are
presented. The upcoming space observatory Herschel will be able to observe the
far-infrared spectra of large samples of local active galaxies. Based on the
observed near-to-far infrared emission line spectrum of the template galaxy
NGC1068, are presented the predictions for the line fluxes expected for
galaxies at high redshift. To observe spectroscopically large samples of
distant galaxies, we will have to wait fot the future space missions, like
SPICA and, ultimately, FIRI.Comment: Proc. of the Winter School "Astronomy in the submillimeter and far
infrared domains with the Herschel Space Observatory", Centre de Physique des
Houches 23 april - 04 may 200
How many active galaxies and QSOs will future Space Missions detect?
Averaged spectral energy distributions (SEDs) of active and starburst
galaxies from the 12 micron sample in the Local Universe and Quasars, from an
optically selected sample at a mean redshift =0.7, are built from
optical/near-IR/far-IR (IRAS & ISO) photometric observations. These SEDs are
then used to predict at various redshifts the number of Seyfert type 1 and type
2, starburst, normal galaxies, and quasars, that will be detected by future
Space Missions dedicated to far-infrared and submillimeter astronomy, like
SIRTF and Herschel. These predictions are then compared with the expected
capabilities and detection limits of future deep far-IR surveys. Possible ways
to identify AGN candidates on far-IR colour-colour plots for follow-up
observations are then explored.Comment: accepted in Ap
Spitzer spectra of Seyfert galaxies
The Spitzer IRS high resolution spectra of about 90 Seyfert galaxies from the
12um Galaxy Sample are presented and discussed. These represent about 70% of
the total complete sample of local Seyfert galaxies. The presence of starburst
components in these galaxies can be quantified by powerful mid-IR diagnostics
tools (i.e. 11.25um PAH feature equivalent width and the H_2 emission line
intensity) as well as the AGN dominance can be measured by specific fine
structure line ratios (e.g. [NeV]/[NeII], [NeV]/[SiII], etc.). The observed
line ratios are compared to the results of semianalytical models, which can be
used to compute the AGN and starburst contributions to the total luminosity of
the galaxies. The results are also discussed in the light of unification and
evolution models.Comment: to appear in the proceedings of "The Starburst-AGN Connection
Conference", Shanghai, China, 27 Oct - 1 Nov 2008, ASP Conference Serie
Seyfert Galaxies in the Local Universe: Analysis of Spitzer Spectra of a Complete Sample
The Spitzer high resolution spectra of 72 Seyfert galaxies from the 12m
Galaxy Sample are presented and discussed. The presence of starburst components
in these galaxies can be quantified by powerful mid-IR diagnostics tools (i.e.
11.25m PAH feature equivalent width and the H emission line
intensity), as well as the AGN dominance can be measured by specific fine
structure line ratios (e.g. [NeV]/[NeII], [NeV]/[SiII], etc.). The two types of
Seyfert galaxies do not show any statistical difference in our diagnostic
tools. However, the Seyfert 2's showing hidden Broad Line Regions in
spectro-polarimetric observations have on average an higher AGN dominance, a
weaker star formation component and a warmer [60 - 25] spectral index than
those without broad emission lines.Comment: Proceedings of the Conference "The central kiloparsec. Active
Galactic Nuclei and their hosts, 4-6 June 2008, Ierapetra, Crete, Greec
Emission Line Properties of Seyfert Galaxies in the 12 Micron Sample
We present spectroscopy of emission lines for 81 Seyfert 1 and 104 Seyfert 2
galaxies in the IRAS 12m galaxy sample. We analyzed the emission-line
luminosity functions, reddening, and other gas diagnostics. The narrow-line
regions (NLR) of Sy1 and 2 galaxies do not significantly differ from each other
in most of these diagnostics. Combining the H/H ratio with a new
reddening indicator-the [SII]6720/[OII]3727 ratio, we find the average
for Sy1s and for Sy2s. The NLR of Sy1
galaxies has only marginally higher ionization than the Sy2s. Our sample
includes 22 Sy1.9s and 1.8s. In their narrow lines, these low-luminosity
Seyferts are more similar to the Sy2s than the Sy1s. We construct a BPT
diagram, and include the Sy1.8s and 1.9s. They overlap the region occupied by
the Sy2s. The C IV equivalent width correlates more strongly with [O
III]/H than with UV luminosity. The Sy1 and Sy2 luminosity functions of
[OII]3727 and [OIII]5007 are indistinguishable. Unlike the LF's of Seyfert
galaxies measured by SDSS, ours are nearly flat at low L. The larger number of
faint Sloan "AGN" is attributable to their inclusion of weakly emitting LINERs
and H II+AGN "composite" nuclei, which do not meet our classification criteria
for Seyferts. An Appendix investigates which emission line luminosities provide
the most reliable measures of the total non-stellar luminosity. The hard X-ray
or near-ultraviolet continuum luminosity can be crudely predicted from either
the [O III]5007 luminosity, or the combination of [O III]+H, or [N
II]+H lines, with a scatter of times for the Sy1s and
times for the Sy2s. The latter two hybrid (NLR+BLR) indicators have
the advantage of predicting the same HX luminosity independent of Seyfert type.Comment: 70 pages, including 15 Figures and 10 Tables. Accepted for
publication in The Astrophysical Journa
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