THE STELLAR-TO-HALO MASS RELATION FOR LOCAL GROUP GALAXIES

Journal Article · Thu Mar 20 00:00:00 EDT 2014 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/784/1/L14· OSTI ID:22365956

Brook, C. B.; Cintio, A. Di; Knebe, A.; Yepes, G. ^[1]; Gottlöber, S. ^[2]; Hoffman, Y. ^[3]

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1. Departamento de Física Teórica, Módulo C-15, Facultad de Ciencias, Universidad Autónoma de Madrid, E-28049, Madrid (Spain)
2. Leibniz Institute for Astrophysics Potsdam, An der Sternwarte 16, D-14482 Potsdam (Germany)
3. Racah Institute of Physics, Hebrew University Jerusalem, Jerusalem 91904 (Israel)

We contend that a single power-law halo mass distribution is appropriate for direct matching to the stellar masses of observed Local Group dwarf galaxies, allowing the determination of the slope of the stellar mass-halo mass relation for low-mass galaxies. Errors in halo masses are well defined as the Poisson noise of simulated Local Group realizations, which we determine using local volume simulations. For the stellar mass range 10{sup 7} M {sub ☉}

• OSTI ID: 22365956
• Journal Information: Astrophysical Journal Letters, Vol. 784, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COMPUTERIZED SIMULATION
GALAXIES
GALAXY CLUSTERS
MASS
MASS DISTRIBUTION
NOISE
NONLUMINOUS MATTER
STARS