Zcosmos 10k-bright spectroscopic sample – research database – university of groningen

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Aims. 7 data recovery suite key We present the analysis of the U – V rest-frame color distribution and some spectral features as a function of mass and environment for a sample of early-type galaxies up to z = 1 extracted from the zCOSMOS spectroscopic survey. Data recovery linux This analysis is used to place constraints on the relative importance of these two properties in controlling galaxy evolution.


Methods. Database modeling tools We used the zCOSMOS 10k-bright sample, limited to the AB magnitude range 15 <I <22.5, from which we extracted two different subsamples of early-type galaxies. G info database search The first sample (“red galaxies”) was selected using a photometric classification (2098 galaxies), while in the second case (“ETGs”) we combined morphological, photometric, and spectroscopic properties to obtain a more reliable sample of elliptical, red, passive, early-type galaxies (981 galaxies). Database administrator salary The analysis is performed at fixed mass to search for any dependence of the color distribution on environment, and at fixed environment to search for any mass dependence.

Results. Database triggers In agreement with the low redshift results of the SDSS, we find that the color distribution of red galaxies is not strongly dependent on environment for all mass bins, exhibiting only a weak trend such that galaxies in overdense regions (log(10)(1 + delta) similar to 1.2) are redder than galaxies in underdense regions (log(10)(1 + delta) similar to 0.1), with a difference of = 0.027 +/- 0.008 mag. Data recovery recuva On the other hand, the dependence on mass is far more significant, and we find that the average colors of massive galaxies (log(10)(M/M(circle dot)) similar to 10.8) are redder by = 0.093 +/- 0.007 mag than low-mass galaxies (log(10)(M/M(circle dot)) similar to 10) throughout the entire redshift range. Data recovery texas We study the color-mass (U -V)(rest) alpha S(M) . Database resume log(10)(M/M circle dot) relation, finding a mean slope <S (M)> = 0.12 +/- 0.005, while the color-environment (U -V)(rest) alpha S(delta) . Data recovery external hard drive mac log(10)(1 + delta) relation is flatter, with a slope always smaller than S(delta) approximate to 0.04.

The spectral analysis that we perform on our ETGs sample is in good agreement with our photometric results: we study the 4000 angstrom break and the equivalent width of the H delta Balmer line, finding for D4000 a dependence on mass ( = 0.11 +/- 0.02 between log10(M/M(circle dot)) similar to 10.2 and log(10)(M/M(circle dot)) similar to 10.8), and a much weaker dependence on environment (<D4000 > = 0.05 +/- 0.02 between high and low environment quartiles). Database management systems The same is true for the equivalent width of Hd, for which we measure a difference of Delta EW(0)(H(delta)) = 0.28 +/- 0.08 angstrom across the same mass range and no significant dependence on environment. 7 data recovery review By analyzing the lookback time of early-type galaxies, we support the possibility of a downsizing scenario, in which massive galaxies with a stronger D4000 and an almost constant equivalent width of H delta formed their mass at higher redshift than lower mass ones.

We also conclude that the main driver of galaxy evolution is the galaxy mass, the environment playing a subdominant role.

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Aims. Mode s database We present the analysis of the U – V rest-frame color distribution and some spectral features as a function of mass and environment for a sample of early-type galaxies up to z = 1 extracted from the zCOSMOS spectroscopic survey. Windows 8 data recovery This analysis is used to place constraints on the relative importance of these two properties in controlling galaxy evolution.

Methods. Java 8 database We used the zCOSMOS 10k-bright sample, limited to the AB magnitude range 15 <I <22.5, from which we extracted two different subsamples of early-type galaxies. Database tools The first sample (“red galaxies”) was selected using a photometric classification (2098 galaxies), while in the second case (“ETGs”) we combined morphological, photometric, and spectroscopic properties to obtain a more reliable sample of elliptical, red, passive, early-type galaxies (981 galaxies). Drupal 7 database api The analysis is performed at fixed mass to search for any dependence of the color distribution on environment, and at fixed environment to search for any mass dependence.

Results. Raid 6 data recovery In agreement with the low redshift results of the SDSS, we find that the color distribution of red galaxies is not strongly dependent on environment for all mass bins, exhibiting only a weak trend such that galaxies in overdense regions (log(10)(1 + delta) similar to 1.2) are redder than galaxies in underdense regions (log(10)(1 + delta) similar to 0.1), with a difference of = 0.027 +/- 0.008 mag. Database architecture On the other hand, the dependence on mass is far more significant, and we find that the average colors of massive galaxies (log(10)(M/M(circle dot)) similar to 10.8) are redder by = 0.093 +/- 0.007 mag than low-mass galaxies (log(10)(M/M(circle dot)) similar to 10) throughout the entire redshift range. Iphone 4 data recovery software We study the color-mass (U -V)(rest) alpha S(M) . Database java log(10)(M/M circle dot) relation, finding a mean slope <S (M)> = 0.12 +/- 0.005, while the color-environment (U -V)(rest) alpha S(delta) . Data recovery android log(10)(1 + delta) relation is flatter, with a slope always smaller than S(delta) approximate to 0.04.

The spectral analysis that we perform on our ETGs sample is in good agreement with our photometric results: we study the 4000 angstrom break and the equivalent width of the H delta Balmer line, finding for D4000 a dependence on mass ( = 0.11 +/- 0.02 between log10(M/M(circle dot)) similar to 10.2 and log(10)(M/M(circle dot)) similar to 10.8), and a much weaker dependence on environment (<D4000 > = 0.05 +/- 0.02 between high and low environment quartiles). C database tutorial The same is true for the equivalent width of Hd, for which we measure a difference of Delta EW(0)(H(delta)) = 0.28 +/- 0.08 angstrom across the same mass range and no significant dependence on environment. Data recovery services cost By analyzing the lookback time of early-type galaxies, we support the possibility of a downsizing scenario, in which massive galaxies with a stronger D4000 and an almost constant equivalent width of H delta formed their mass at higher redshift than lower mass ones.

We also conclude that the main driver of galaxy evolution is the galaxy mass, the environment playing a subdominant role.

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