Funding: VW acknowledges funding from the ERC (starting grant SEDmorph, PI. Wild)We analyze stellar age indicators (Dn4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with M∗≥1010M⊙ at z∼0.7 drawn from DR2 of the LEGA-C survey. Interpreting index variations in terms of equivalent single stellar population age, we find that the median stellar population is younger for larger galaxies at fixed stellar mass. The effect is significant, yet small; the ages of the larger and the smaller subsets differ by only<500 Myr, much less than the age variation among individual galaxies (∼1.5 Gyr). At the same time, quiescent galaxies with the strongest Hδ absorption —those experienced recent and rapid quenching events — tend to be smaller than the aver...
We use reconstructed star-formation histories (SFHs) of quiescent galaxies at z = 0.6 − 1 in the LEG...
Observations have shown that the star-formation activity and the morphology of galaxies are closely ...
One key problem in astrophysics is understanding how and why galaxies switch off their star formatio...
We analyze the stellar age indicators (D(n)4000 and EW(H delta)) and sizes of 467 quiescent galaxies...
We analyze the stellar age indicators (D n 4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with...
We analyze stellar age indicators (Dn4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with M∗≥10...
We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorptio...
We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorptio...
We present star formation histories (SFHs) for a sample of 104 massive (stellar mass M > 10^10 M_⊙) ...
Although there has been much progress in understanding how galaxies evolve, we still do not understa...
© 2016 The Authors. One key problem in astrophysics is understanding how and why galaxies switch off...
We analyze the stellar populations of a sample of 62 massive (log Mstar/Msun > 10.7) galaxies in the...
Deep surveys have allowed us to precisely chart the evolution of galaxies from billions of years ago...
In this paper, we investigate the relationship between star formation and structure, using a mass-co...
We investigate the stellar populations for a sample of 24 quiescent galaxies at 1.5 < z < 2.5 using ...
We use reconstructed star-formation histories (SFHs) of quiescent galaxies at z = 0.6 − 1 in the LEG...
Observations have shown that the star-formation activity and the morphology of galaxies are closely ...
One key problem in astrophysics is understanding how and why galaxies switch off their star formatio...
We analyze the stellar age indicators (D(n)4000 and EW(H delta)) and sizes of 467 quiescent galaxies...
We analyze the stellar age indicators (D n 4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with...
We analyze stellar age indicators (Dn4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with M∗≥10...
We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorptio...
We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorptio...
We present star formation histories (SFHs) for a sample of 104 massive (stellar mass M > 10^10 M_⊙) ...
Although there has been much progress in understanding how galaxies evolve, we still do not understa...
© 2016 The Authors. One key problem in astrophysics is understanding how and why galaxies switch off...
We analyze the stellar populations of a sample of 62 massive (log Mstar/Msun > 10.7) galaxies in the...
Deep surveys have allowed us to precisely chart the evolution of galaxies from billions of years ago...
In this paper, we investigate the relationship between star formation and structure, using a mass-co...
We investigate the stellar populations for a sample of 24 quiescent galaxies at 1.5 < z < 2.5 using ...
We use reconstructed star-formation histories (SFHs) of quiescent galaxies at z = 0.6 − 1 in the LEG...
Observations have shown that the star-formation activity and the morphology of galaxies are closely ...
One key problem in astrophysics is understanding how and why galaxies switch off their star formatio...