266 research outputs found
The Continuum Slopes of Optically Selected QSOs
Quasi-simultaneous optical/near-IR photometry is presented for a sample of 37
luminous optically selected QSOs drawn from the Large Bright QSO Survey. Most
of the QSOs have decreased in brightness since discovery; this is expected in
flux-limited samples. The continuum shape of most of the QSOs can be
represented by a power-law of the form F(nu) = nu**-0.3, but a few have softer
(redder) continuum slopes.Comment: 14 pages, LaTeX, 2 postscript figures. Accepted for publication in
Publ. AS
A 12 μm ISOCAM survey of the ESO-Sculptor field
We present a detailed reduction of a mid-infrared 12 μm (LW10 filter) ISOCAM open time observation performed on the ESOSculptor
Survey field (Arnouts et al. 1997, A&AS, 124, 163). A complete catalogue of 142 sources (120 galaxies and 22 stars),
detected with high significance (equivalent to 5σ), is presented above an integrated flux density of 0.24 mJy. Star/galaxy separation
is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1 mJy and, below this flux density, the
incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of
the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the
field. For each star, the 12 μm flux density is derived by fitting optical colours from a multi-band χ^2 to stellar templates (BaSel-2.0)
and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange
et al. 2007, A&A, 475, 801) where the 12 μm faint galaxy counts are presented and analysed per galaxy type with the evolutionary
code PÉGASE.3
P\'egase.3: A code for modeling the UV-to-IR/submm spectral and chemical evolution of galaxies with dust
A code computing consistently the evolution of stars, gas and dust, as well
as the energy they radiate, is required to derive reliably the history of
galaxies by fitting synthetic SEDs to multiwavelength observations. The new
code P\'egase.3 described in this paper extends to the far-IR/submm the
UV-to-near-IR modeling provided by previous versions of P\'egase. It first
computes the properties of single stellar populations at various metallicities.
It then follows the evolution of the stellar light of a galaxy and the
abundances of the main metals in the ISM, assuming some scenario of mass
assembly and star formation. It simultaneously calculates the masses of the
various grain families, the optical depth of the galaxy and the attenuation of
the SED through the diffuse ISM in spiral and spheroidal galaxies, using grids
of radiative transfer precomputed with Monte Carlo simulations taking
scattering into account. The code determines the mean radiation field and the
temperature probability distribution of stochastically heated individual
grains. It then sums up their spectra to yield the overall emission by dust in
the diffuse ISM. The nebular emission of the galaxy is also computed, and a
simple modeling of the effects of dust on the SED of star-forming regions is
implemented. The main outputs are UV-to-submm SEDs of galaxies from their birth
up to 20 Gyr, colors, masses of galactic components, ISM abundances of metallic
elements and dust species, supernova rates. The temperatures and spectra of
individual grains are also available. The paper discusses several of these
outputs for a scenario representative of Milky Way-like spirals. P\'egase.3 is
fully documented and its Fortran 95 source files are public. The code should be
especially useful for cosmological simulations and to interpret future mid- and
far-IR data, whether obtained by JWST, LSST, Euclid or e-ELT.Comment: 15 pages. In press in A&A. Source files of the code available at
http://www.iap.fr/users/fioc/Pegase/Pegase.3/ (and
http://www.iap.fr/pegase/); documentation at arXiv:1902.0219
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