J/A+A/587/A136 Balmer break galaxies at z<1.5 star formation (Diaz Tello+, 2016)
Star formation activity in Balmer break galaxies at z < 1.5.
Diaz Tello J., Donzelli C., Padilla N., Akiyama M., Fujishiro N.,
Yoshikawa T., Hanami H.
<Astron. Astrophys., 587, A136-136 (2016)>
=2016A&A...587A.136D 2016A&A...587A.136D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Redshifts
Keywords: galaxies: evolution - galaxies: star formation -
galaxies: high-redshift - galaxies: active - galaxies: stellar content
Abstract:
We present a spectroscopic study of the properties of 64 Balmer break
galaxies that show signs of star formation. The studied sample of
star-forming galaxies spans a redshift range from 0.094 to 1.475 with
stellar masses in the range 108-1012M☉. The sample also
includes eight broad emission line galaxies with redshifts between
1.5<z<3.0. We derived star formation rates (SFRs) from emission line
luminosities and investigated the dependence of the SFR and specific
SFR (SSFR) on the stellar mass and color. Furthermore, we investigated
the evolution of these relations with the redshift. We found that the
SFR correlates with the stellar mass; our data is consistent with
previous results from other authors in that there is a break in the
correlation, which reveals the presence of massive galaxies with lower
SFR values (i.e., decreasing star formation). We also note an
anticorrelation for the SSFR with the stellar mass. Again in this
case, our data is also consistent with a break in the correlation,
revealing the presence of massive star-forming galaxies with lower
SSFR values, thereby increasing the anticorrelation. These results
might suggest a characteristic mass (M0) at which the red sequence
could mostly be assembled. In addition, at a given stellar mass,
high-redshift galaxies have on average higher SFR and SSFR values than
local galaxies. Finally, we explored whether a similar trend could be
observed with redshift in the SSFR-(u-B) color diagram, and we
hypothesize that a possible (u-B)0 break color may define a
characteristic color for the formation of the red sequence.
Description:
The galaxies presented in this article come from a sample constructed
to study star formation activity of massive galaxies in the redshift
range z=0.1-3.0 (Diaz Tello et al., 2013ApJ...771....7D 2013ApJ...771....7D; hereafter
D13). The chosen field, the SXDF (RA=02:18:00, DE=-05:00:00;
Furusawa et al., 2008, Cat. J/ApJS/176/1) has the advantage that deep
photometric data is available in the bands u, B, R, i, z (Subaru), J,
H, K (UKIRT), and in all MIR Spitzer bands. The parent sample was
selected using the λ3646 Balmer and λ4000 break features
as tracers of redshift, as described by Daddi et al.
(2004ApJ...617..746D 2004ApJ...617..746D), utilizing the BzK color-color diagram to select
star-forming galaxies in a particular redshift range. Furthermore, we
used two color-color diagrams to select star-forming galaxies in a
lower redshift range than the BzK diagram; these diagrams were
presented in Hanami et al. (2012PASJ...64...70H 2012PASJ...64...70H; uVi and uRJ diagrams).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 93 72 Spectroscopic sample obtained with IMACS and GMOS
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See also:
J/MNRAS/372/741 : SXDF 100µJy catalogue (Simpson+, 2006)
J/MNRAS/403/2063 : SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SXDF]
5- 19 A15 --- SXDF SXDF designation, HHMMSS.s+DDMMSS
21- 25 A5 --- Inst [IMACS GMOS] Instrument
27- 28 I2 h RAh Right ascension (J2000)
30- 31 I2 min RAm Right ascension (J2000)
33- 38 F6.3 s RAs Right ascension (J2000)
40 A1 --- DE- Declination sign (J2000)
41- 42 I2 deg DEd Declination (J2000)
44- 45 I2 arcmin DEm Declination (J2000)
47- 51 F5.2 arcsec DEs Declination (J2000)
53- 57 F5.3 --- zsp Spectroscopic redshift
59- 63 F5.2 mag umag ?=- Measured observer frame u-band photometry
in AB magnitudes
65- 68 F4.2 mag e_umag ?=- rms uncertainty on umag
70- 93 A24 --- Com Detection of a counterpart in X-ray, FIR,
and/or submillimeter
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-May-2016