J/MNRAS/393/1467 Field early-type galaxies at 0.2<z<0.8 (Fritz+, 2009)
The evolution of field early-type galaxies in the FDF and WHDF.
Fritz A., Bohm A., Ziegler B.L.
<Mon. Not. R. Astron. Soc., 393, 1467-1492 (2009)>
=2009MNRAS.393.1467F 2009MNRAS.393.1467F
ADC_Keywords: Galaxies, photometry ; Photometry, UBVRI ; Velocity dispersion ;
Redshifts
Keywords: galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: formation - galaxies: kinematics and dynamics -
galaxies: stellar content - cosmology: observations
Abstract:
We explore the properties of 24 field early-type galaxies in the
redshift range 0.20<z<0.75 down to M_B≤-19.30 in a sample extracted
from the FORS Deep Field and the William Herschel Deep Field. Target
galaxies were selected on the basis of a combination of luminosity,
spectrophotometric type, morphology and photometric redshift or
broad-band colours. High signal-to-noise intermediate-resolution
spectroscopy has been acquired at the Very Large Telescope,
complemented by deep high-resolution imaging with the Advanced Camera
for Surveys onboard the HST and additional ground-based multi-band
photometry. All galaxy spectra were observed under sub-arcsecond
conditions and allow to derive accurate kinematics and stellar
population properties of the galaxies. To clarify the low level of
star formation detected in some galaxies, we identify the amount of
active galactic nuclei (AGN) activity in our sample using archive data
of Chandra and XMM-Newton X-ray surveys. None of the galaxies in our
sample were identified as secure AGN sources based on their X-ray
emission. The rest-frame B and K-band scaling relations of the
Faber-Jackson relation and the Fundamental Plane display a moderate
evolution for the field early-type galaxies. Lenticular (S0) galaxies
feature on average a stronger luminosity evolution and bluer
rest-frame colours which can be explained that they comprise more
diverse stellar populations compared to elliptical galaxies. The
evolution of the FP can be interpreted as an average change in the
dynamical (effective) mass-to-light ratio of our galaxies as
<Δlog(M/LB)/z≥-0.74±0.08. The M/L evolution of these field
galaxies suggests a continuous mass assembly of field early-type
galaxies during the last 5Gyr, that gets support by recent studies of
field galaxies up to z∼1. Independent evidence for recent star
formation activity is provided by spectroscopic (OII emission, Hdelta)
and photometric (rest-frame broad-band colors) diagnostics. Based on
the Hdelta absorption feature we detect a weak residual star formation
for galaxies that accounts for 5%-10% in the total stellar mass of
these galaxies. The co-evolution in the luminosity and mass of our
galaxies favours a downsizing formation process. We find some evidence
that our galaxies experienced a period of star formation quenching,
possible triggered by AGN activity that is in good agreement with
recent results on both observational and theoretical side.
Description:
Structural parameters, coordinates, redshifts, luminosities, colours,
dynamical masses, M/L ratios and velocity dispersions are presented
for a sample of 24 field early-type galaxies in the FORS Deep Field
and the William Herschel Deep Field. The galaxies cover the redshift
range 0.2<z<0.8. In addition, coordinates, redshifts, luminosities and
colours are presented for 15 identified cluster early-type galaxies at
z=0.335 in the FORS Deep Field.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table3.dat 49 15 Photometric data on 15 cluster early-type
galaxies in the FORS Deep Field
table5.dat 120 24 Photometric and kinematic data on 24 field
early-type galaxies in the FORS Deep Field
and the William Herschel Deep Field
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See also:
J/A+A/398/49 : UBgRIJKs photometry in the FORS Deep Field (Heidt+, 2003)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- FDF FORS Deep Field photometric catalogue number
6- 11 F6.4 --- z Spectroscopic redshift
13- 14 I2 h RAh Right ascension (J2000.0)
16- 17 I2 min RAm Right ascension (J2000.0)
19- 24 F6.3 s RAs Right ascension (J2000.0)
26 A1 --- DE- Declination sign (J2000.0)
27- 28 I2 deg DEd Declination (J2000.0)
30- 31 I2 arcmin DEm Declination (J2000.0)
33- 38 F6.3 arcsec DEs Declination (J2000.0)
40- 44 F5.2 mag Bmag Total apparent magnitude in Johnson B-band
46- 49 F4.2 mag B-I Rest-frame extinction-corrected B-I colour
index
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name FORS/WHDF Deep Field catalogue number (1)
11- 16 F6.4 --- z Spectroscopic redshift
18- 19 I2 h RAh Right ascension (J2000.0)
21- 22 I2 min RAm Right ascension (J2000.0)
24- 29 F6.3 s RAs Right ascension (J2000.0)
31 A1 --- DE- Declination sign (J2000.0)
32- 33 I2 deg DEd Declination (J2000.0)
35- 36 I2 arcmin DEm Declination (J2000.0)
38- 43 F6.3 arcsec DEs Declination (J2000.0)
45- 47 I3 km/s sigma Stellar velocity dispersion (2)
49- 50 I2 km/s e_sigma Error on stellar velocity dispersion
52- 54 I3 --- SNR Signal-to-noise ratio per Angstroem
in rest-frame (3)
56- 60 F5.2 mag Bmag ?=- Total apparent magnitude in Johnson
B-band
62- 66 F5.2 kpc logRe ?=- Log10 seeing corrected effective
radius (4)
68- 71 F4.2 kpc e_logRe ?=- Error on logRe
73- 76 F4.2 arcsec reff ?=- Seeing corrected effective radius
78- 82 F5.2 mag/arcsec2 ?=- Seeing corrected mean surface
brightness within reff in Johnson
B-band
84- 87 F4.2 mag/arcsec2 e_ ?=- Error on
89- 93 F5.2 solMass logMdyn ?=- Log10 dynamical mass
95- 98 F4.2 solMass e_logMdyn ?=- Error on logMdyn
100-103 F4.2 Sun logM/L ?=- Log10(M/L) in Johnson B-band (5)
105-109 F5.2 --- dlnM/L ?=- ΔLN(M/L) in Johnson B-band
111-114 F4.2 --- e_dlnM/L ?=- Error on Delta dlnM/L
116-120 F5.2 mag B-I Rest-frame extinction-corrected B-I
colour index
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Note (1): Nomenclature note:
WHDF NNNa identified as [FBZ2009] WHDF-NNNa in Simbad
Note (2): Velocity dispersions are not corrected for aperture effects.
Note (3): Signal-to-noise ratio per Angstroem in rest-frame.
One pixel is 1.6Å.
Note (4): Structural parameters were derived from 2-D surface brightness
profile fitting on HST/ACS images taking into account distortion and
PSF variation effects.
Note (5): The error on M/L ratio (in solar units) is the same as the error
on the dynamical mass Mdyn.
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Acknowledgements:
Alexander Fritz, afritz (at)gemini.edu
References:
Metcalfe et al., 2001MNRAS.323..795M 2001MNRAS.323..795M,
UBRI photometry in the William Herschel Deep Field
(End) Patricia Vannier [CDS] 30-Oct-2009