TY - JOUR
T1 - THE NEXT GENERATION VIRGO CLUSTER SURVEY. IX. ESTIMATING THE EFFICIENCY OF GALAXY FORMATION ON THE LOWEST-MASS SCALES
AU - Grossauer, Jonathan
AU - Taylor, James E.
AU - Ferrarese, Laura
AU - MacArthur, Lauren A.
AU - Côté, Patrick
AU - Roediger, Joel
AU - Courteau, Stéphane
AU - Cuillandre, Jean Charles
AU - Duc, Pierre Alain
AU - Durrell, Patrick R.
AU - Gwyn, S. D.J.
AU - Jordán, Andrés
AU - Mei, Simona
AU - Peng, Eric W.
N1 - Publisher Copyright:
© 2015. The American Astronomical Society. All rights reserved.
PY - 2015/7/1
Y1 - 2015/7/1
N2 - The Next Generation Virgo Cluster Survey has recently determined the luminosity function of galaxies in the core of the Virgo cluster down to unprecedented magnitude and surface brightness limits. Comparing simulations of cluster formation to the derived central stellar mass function, we attempt to estimate the stellar-to-halo-mass ratio (SHMR) for dwarf galaxies, as it would have been before they fell into the cluster. This approach ignores several details and complications, e.g., the contribution of ongoing star formation to the present-day stellar mass of cluster members, and the effects of adiabatic contraction and/or violent feedback on the subhalo and cluster potentials. The final results are startlingly simple, however; we find that the trends in the SHMR determined previously for bright galaxies appear to extend down in a scale-invariant way to the faintest objects detected in the survey. These results extend measurements of the formation efficiency of field galaxies by two decades in halo mass or five decades in stellar mass, down to some of the least massive dwarf galaxies known, with stellar masses of ∼105 M⊙.
AB - The Next Generation Virgo Cluster Survey has recently determined the luminosity function of galaxies in the core of the Virgo cluster down to unprecedented magnitude and surface brightness limits. Comparing simulations of cluster formation to the derived central stellar mass function, we attempt to estimate the stellar-to-halo-mass ratio (SHMR) for dwarf galaxies, as it would have been before they fell into the cluster. This approach ignores several details and complications, e.g., the contribution of ongoing star formation to the present-day stellar mass of cluster members, and the effects of adiabatic contraction and/or violent feedback on the subhalo and cluster potentials. The final results are startlingly simple, however; we find that the trends in the SHMR determined previously for bright galaxies appear to extend down in a scale-invariant way to the faintest objects detected in the survey. These results extend measurements of the formation efficiency of field galaxies by two decades in halo mass or five decades in stellar mass, down to some of the least massive dwarf galaxies known, with stellar masses of ∼105 M⊙.
UR - http://www.scopus.com/inward/record.url?scp=84936753552&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/807/1/88
DO - 10.1088/0004-637X/807/1/88
M3 - Article
AN - SCOPUS:84936753552
SN - 0004-637X
VL - 807
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 88
ER -