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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
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:
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
See also: J/A+A/398/49 : UBgRIJKs photometry in the FORS Deep Field (Heidt+, 2003) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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 <mue> ?=- Seeing corrected mean surface brightness within reff in Johnson B-band 84- 87 F4.2 mag/arcsec2 e_<mue> ?=- Error on <mue> 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
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.
Acknowledgements: Alexander Fritz, afritz (at)gemini.edu References: Metcalfe et al., 2001MNRAS.323..795M, UBRI photometry in the William Herschel Deep Field
(End) Patricia Vannier [CDS] 30-Oct-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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