292 citations · 7.2k across the 143 of their papers we have counts for
6 papers · 1 filter
Formation of S0 galaxies through mergers. Bulge-disc structural coupling resulting from major mergers
M. Querejeta, M. C. Eliche-Moral, T. Tapia +4
Observations reveal a strong structural coupling between bulge and disc in S0 galaxies, which seems difficult to explain if they have formed from supposedly catastrophic events suc…
The Spitzer Survey of Stellar Structure in Galaxies (SG): Precise Stellar Mass Distributions from Automated Dust Correction at 3.6 microns
M. Querejeta, S. E. Meidt, E. Schinnerer +26
The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 IRAC band has been exploited to this effect, but such mass estimates can be biased by…
Being WISE I: Validating Stellar Population Models and M/L ratios at 3.4 and 4.6 microns
Mark A. Norris, Sharon Meidt, Glenn Van de Ven +3
Using data from the WISE mission, we have measured near infra-red (NIR) photometry of a diverse sample of dust-free stellar systems (globular clusters, dwarf and giant early-type g…
Formation of S0 galaxies through mergers. V. Antitruncated stellar discs resulting from major mergers
Alejandro Borlaff, M. Carmen Eliche-Moral, Cristina Rodríguez-Pérez +6
Lenticular galaxies (S0s) are more likely to host antitruncated (Type-III) stellar discs than galaxies of later Hubble types. Major mergers are popularly considered too violent mec…
Evolution induced by dry minor mergers onto fast-rotator S0 galaxies
Trinidad Tapia, M. Carmen Eliche-Moral, Miguel Querejeta +9
We analysed collisionless N-body simulations of intermediate and minor dry mergers onto S0s to test whether these mergers can generate S0 galaxies with kinematics intermediate betw…
Reconstructing the stellar mass distributions of galaxies using S4G IRAC 3.6 and 4.5 micron images: II. The conversion from light to mass
Sharon E. Meidt, Eva Schinnerer, Glenn van de Ven +26
We present a new approach for estimating the 3.6 micron stellar mass-to-light ratio in terms of the [3.6]-[4.5] colors of old stellar populations. Our approach avoids several of th…