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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 198428.0, MPI für Astronomie / Publikationen_mpia
Star forming rates between z = 0.25 and z =
1.2 from the CADIS emission line survey
Authors:Hippelein, H.; Maier, C.; Meisenheimer, K.; Wolf, C.; Fried, J. W.; von Kuhlmann, B.; Kümmel, M.; Phleps, S.; Röser, H.-J.
Date of Publication (YYYY-MM-DD):2003
Title of Journal:Astronomy and Astrophysics
Journal Abbrev.:Astronomy and Astrophysics
Volume:402
Start Page:65
End Page:78
Sequence Number of Article:2003A&A...402...65H
Review Status:not specified
Audience:Experts Only
Abstract / Description:The emission line survey within the Calar Alto
Deep Imaging Survey (CADIS) detects emission
line galaxies by a scan with an imaging
Fabry-Perot interferometer. It covers 5 fields of
gt; 100 sq arcmin each in three wavelengths
windows centered on lambda =~ 700, 820, and
920 nm, and reaches to a typical limiting line
flux of 3 x 10-20 W m-2.
This is the deepest emission line survey
covering a field of several 100 sq arcmin .
Galaxies between z = 0.25 and z = 1.4 are
detected by prominent emission lines (from
H alpha; to [O II]372.7) falling into the FP
scans. Additional observations with a dozen
medium band filters allow to establish the line
identification and thus the redshift of the
galaxies to better than sigma z =
0.001. On the basis of a total of more than 400
emission line galaxies detected in H alpha;
(92 galaxies), [O III]500.7 (124 galaxies), or [O
II]372.7 (222 galaxies) we measure the
instantaneous star formation rate (SFR) in the
range 0.24 lt; z lt; 1.21. With this purely
emission line selected sample we are able to
reach much fainter emission line galaxies than
previous, continuum-selected samples. Thus
completeness corrections are much less
important. Although the relative [O III] emission
line strength depends on excitation and
metallicity and shows strong variation, the mean
line ratios yield SFR[O III] values consistent
with the SFR evolution. Our results
substantiates the indications from previous
studies (based on small galaxy samples) that the
SFR decreases by a factor of ~ 20 between z =
1.2 and today. In fact, for a Omegam = 0.3, Omega_ lambda = 0.7 cosmology, we find an
exponential decline dot rhoSFR ~ exp
(-tlookback/ 2.6 Gyr). This decrease
of the SFR with time follows an exponential law
which is compatible with the decreasing galaxy
merger rate as expected from model calculations.
The inferred SF density is in perfect agreement
with that deduced from the FIR emission of
optically selected galaxies which is explained
by a large overlap between both populations. We
show that self-consistent extinction corrections
of both our emission lines and the UV continua
lead to consistent results for the SF density.
Free Keywords:stars: formation; galaxies: general;
; galaxies: high-redshift; galaxies: luminosity
; function
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
External Affiliations:K ouml;nigstuhl 17, 69117 Heidelberg, Germany),
AB(Max-Planck-Institut f uuml;r Astronomie,
K ouml;nigstuhl 17, 69117 Heidelberg, Germany),
AC(Max-Planck-Institut f uuml;r Astronomie,
K ouml;nigstuhl 17, 69117 Heidelberg, Germany),
AD(Max-Planck-Institut f uuml;r Astronomie,
K ouml;nigstuhl 17, 69117 Heidelberg, Germany;
Department of Physics, Denys Wilkinson Bldg.,
University of Oxford, Keble Road, Oxford, OX1
3RH, UK), AE(Max-Planck-Institut f uuml;r
Astronomie, K ouml;nigstuhl 17, 69117
Heidelberg, Germany), AF(Max-Planck-Institut
f uuml;r Astronomie, K ouml;nigstuhl 17, 69117
Heidelberg, Germany), AG(Max-Planck-Institut
f uuml;r Astronomie, K ouml;nigstuhl 17, 69117
Heidelberg, Germany), AH(Max-Planck-Institut
f uuml;r Astronomie, K ouml;nigstuhl 17, 69117
Heidelberg, Germany), AI(Max-Planck-Institut
f uuml;r Astronomie, K ouml;nigstuhl 17, 69117
Heidelberg, Germany)
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi... [ID No:1]
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