563 research outputs found
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
Far-infrared line spectra of active galaxies from the Herschel/PACS Spectrometer: the complete database
We present a coherent database of spectroscopic observations of far-IR
fine-structure lines from the Herschel/PACS archive for a sample of 170 local
AGN, plus a comparison sample of 20 starburst galaxies and 43 dwarf galaxies.
Published Spitzer/IRS and Herschel/SPIRE line fluxes are included to extend our
database to the full 10-600 spectral range. The observations are
compared to a set of CLOUDY photoionisation models to estimate the above
physical quantities through different diagnostic diagrams. We confirm the
presence of a stratification of gas density in the emission regions of the
galaxies, which increases with the ionisation potential of the emission lines.
The new [OIV]25.9/[OIII]88 vs [NeIII]15.6/[NeII]12.8 diagram is proposed as the best diagnostic to separate: AGN activity
from any kind of star formation; and low-metallicity dwarf galaxies from
starburst galaxies. Current stellar atmosphere models fail to reproduce the
observed [OIV]25.9/[OIII]88 ratios, which are much higher when
compared to the predicted values. Finally, the ([NeIII]15.6 +
[NeII]12.8)/([SIV]10.5 + [SIII]18.7) ratio is proposed as
a promising metallicity tracer to be used in obscured objects, where optical
lines fail to accurately measure the metallicity. The diagnostic power of mid-
to far-infrared spectroscopy shown here for local galaxies will be of crucial
importance to study galaxy evolution during the dust-obscured phase at the peak
of the star formation and black-hole accretion activity (). This
study will be addressed by future deep spectroscopic surveys with present and
forthcoming facilities such as JWST, ALMA, and SPICA.Comment: Accepted for publication in the ApJ
The physics of Galaxy Evolution with SPICA observations
The evolution of galaxies at Cosmic Noon (redshift 1<z<3) passed through a
dust-obscured phase, during which most stars formed and black holes in galactic
nuclei started to shine, which cannot be seen in the optical and UV, but it
needs rest frame mid-to-far IR spectroscopy to be unveiled. At these
frequencies, dust extinction is minimal and a variety of atomic and molecular
transitions, tracing most astrophysical domains, occur. The future IR space
telescope mission, SPICA, currently under evaluation for the 5th Medium Size
ESA Cosmic Vision Mission, fully redesigned with its 2.5 m mirror cooled down
to T < 8K will perform such observations. SPICA will provide for the first time
a 3-dimensional spectroscopic view of the hidden side of star formation and
black hole accretion in all environments, from voids to cluster cores over 90%
of cosmic time. Here we outline what SPICA will do in galaxy evolution studies.Comment: Contributed talk at the IAU Symp 359 Galaxy Evolution and Feedback
Across Different Environments, 2020 March 2-6, Bento Concalves, Brazil. arXiv
admin note: text overlap with arXiv:1911.1218
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