TY - JOUR
T1 - Early-type galaxies in the sloan digital sky survey. III. The fundamental plane
AU - Bernardi, Mariangela
AU - Sheth, Ravi K.
AU - Annis, James
AU - Burles, Scott
AU - Eisenstein, Daniel J.
AU - Finkbeiner, Douglas P.
AU - Hogg, David W.
AU - Lupton, Robert H.
AU - Schlegel, David J.
AU - SubbaRao, Mark
AU - Bahcall, Neta A.
AU - Blakeslee, John P.
AU - Brinkmann, J.
AU - Castander, Francisco
AU - Connolly, Andrew J.
AU - Csabai, István
AU - Doi, Mamoru
AU - Fukugita, Masataka
AU - Frieman, Joshua
AU - Heckman, Timothy
AU - Hennessy, Gregory S.
AU - Ivezić, Željko
AU - Knapp, G. R.
AU - Lamb, Don Q.
AU - McKay, Timothy
AU - Munn, Jeffrey A.
AU - Nichol, Robert
AU - Okamura, Sadanori
AU - Schneider, Donald P.
AU - Thakar, Aniruddha R.
AU - York, Donald G.
PY - 2003/4
Y1 - 2003/4
N2 - A magnitude-limited sample of nearly 9000 early-type galaxies in the redshift range 0.01 ≤ z ≤ 0.3 was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The fundamental plane relation in this sample is Ro ∝ σ 1.49±0.05 Io-0.75±0.01 in the r* band, It is approximately the same in the g*, i*, and z* bands. Relative to the population at the median redshift in the sample, galaxies at lower and higher redshifts have evolved only a little. If the fundamental plane is used to quantify this evolution, then the apparent magnitude limit can masquerade as evolution; once this selection effect has been accounted for, the evolution is consistent with that of a passively evolving population that formed the bulk of its stars about 9 Gyr ago. One of the principal advantages of the SDSS sample over previous samples is that the galaxies in it lie in environments ranging from isolation in the field to the dense cores of clusters. The fundamental plane shows that galaxies in dense regions are slightly different from galaxies in less dense regions.
AB - A magnitude-limited sample of nearly 9000 early-type galaxies in the redshift range 0.01 ≤ z ≤ 0.3 was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The fundamental plane relation in this sample is Ro ∝ σ 1.49±0.05 Io-0.75±0.01 in the r* band, It is approximately the same in the g*, i*, and z* bands. Relative to the population at the median redshift in the sample, galaxies at lower and higher redshifts have evolved only a little. If the fundamental plane is used to quantify this evolution, then the apparent magnitude limit can masquerade as evolution; once this selection effect has been accounted for, the evolution is consistent with that of a passively evolving population that formed the bulk of its stars about 9 Gyr ago. One of the principal advantages of the SDSS sample over previous samples is that the galaxies in it lie in environments ranging from isolation in the field to the dense cores of clusters. The fundamental plane shows that galaxies in dense regions are slightly different from galaxies in less dense regions.
KW - Galaxies: elliptical and lenticular, cD
KW - Galaxies: evolution
KW - Galaxies: fundamental parameters
KW - Galaxies: photometry
KW - Galaxies: stellar content
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U2 - 10.1086/367794
DO - 10.1086/367794
M3 - Article
AN - SCOPUS:0043233567
SN - 0004-6256
VL - 125
SP - 1866
EP - 1881
JO - Astronomical Journal
JF - Astronomical Journal
IS - 4 1768
ER -