A. Rodríguez–Puebla,¹ V. Avila–Reese,¹ C. Firmani,^1,2 and P. Colín³

¹ Instituto de Astronomía, Universidad Nacional Autónoma de México, México.Apdo. Postal 70–264, 04510, Mexico, D.F., Mexico (apuebla@astroscu.unam.mx).

² Osservatorio Astronomico di Brera, via E.Bianchi 46, I–23807 Merate, Italy.

³ Centro de Radioastronomía y Astrofísica, UniversidadNacional Autónoma de Mexico, Apdo. Postal 72–3 (Xangari), Morelia, Michoacaán 58089, Mexico.

Received 2011 January 21
Accepted 2011 April 14

RESUMEN

Con la tecnica del empate de abundancias, las relaciones locales masa estelar y bariónica–masa de halo (M_s– M_h y M_b– M_h) para galaxias centrales azules y rojas (GAs y GRs) se infieren por separado. Se hace uso de las funciones de masa estelar galáctica observadas de GAs y GRs y las respectivas relaciones masa de gas–M_s. Las funciones de masa de halos asociados a las GAs y GRs centrales se toman de una descomposición adecuadamente obtenida de la función de halos distinguibles ACDM. Para M_h >_~ 10^11.5 Μ_Θ, la M_s de GRs tiende a ser mayor que la de GAs a una dada M_h, pero no más que un factor ~1.7. Para M_h >_~ 10^11.5 Μ_Θ, esta tendencia se invierte. Para GAs (GRs): (a) el máximo de f_s= M_s /M_h es 0.021+0.016 -0.009 (0.034 +0.026 -0.015) y se alcanza a log (M_h / Μ_Θ) = 12.0 (= 11.9); (b) f_s ∞M_h(f_s ∞M_h³) hacia el lado de bajas masas, mientras que en el otro extremo f_s ∞ M_h^–0'⁴ (f_s ∞ M_h^–0.6). Las f_b= M_b / M_h de GAs y GRs son cercanas para M_h >_~ 10^11.7 Μ_Θ, y alcanzan valores maximos de f_b = 0.028 +0.018 -0.011 y f_b = 0.034 +0.025 -0.014. Hacia masas menores la dependencia de f_b sobre M_h es mucho más empinada para GRs que para GAs. Discutimos las diferencias encontradas para las relaciones f_s–M_h y f_b– M_h entre GAs y GRs a la luz de inferencias semi–empíricas de evolución galáctica.

ABSTRACT

Using the abundance matching technique, we infer the local stellar and baryonic mass–halo mass ( M_s– M_h and M_b – M_h) relations separately for central blue and red galaxies (BGs and RGs). The observational inputs are the SDSS central BG and RG stellar mass functions and the measured gas mass–M_s relations. For halos associated to central BGs, the distinct ACDM halo mass function is used and set up to exclude: (i) the observed group/cluster mass function and (ii) halos with a central major merger at resdshifts z ≤ 0.8. For central RGs, the complement of this 5 mass function to the total one is used. At M_h > 10^11.5 Μ_Θ, the M_s of RGs tend to be higher than those of BGs for a given M_h, the difference not being larger than 1.7. At M_h < 10^11.5 Μ_Θ, this trend is inverted. For BGs (RGs): (a) the maximum value of f_s = M_s / M_h is 0.021+0.016 -0.009 (0.034 +0.026 -0.015)and it is attained at log(M_h/Μ_Θ) = 12.0 (= 11.9); (b) f_s ∞ M_h ( f_s ∞ M_h³) at the low–mass end while at the high–mass end, f_s ∞ M_h^–0.4 (f_s ∞ M_h^–06). The baryon mass fractions, f_b = M_b / M_h, of BGs and RGs reach maximum values of f_b = 0.028 +0.018 -0.011 y f_b = 0.034 +0.025 -0.014., respectively. At M_h < 10^11.3 Μ_Θ, the dependence of f_b on M_h is much steeper for RGs than for BGs. We discuss the differences found in the f_s – M_h and f_b – M_h relations between BGs and RGs in the light of semi–empirical galaxy evolution inferences.

Key Words: dark matter — galaxies: luminosity function, mass function.

DESCARGAR ARTÍCULO EN FORMATO PDF

We thank the referee for his/her useful comments and suggestions. We are grateful to Dr. S. More for sending us in electronic form the data plotted in Figure 8. A.R–P. Acknowledges a graduate student fellowship provided by Conacyt. We thank PAPIIT–Universidad Nacional Autónoma de México grant IN114509 and Conacyt grant 60354 for partial funding, as well as a bilateral DFG–Conacyt grant through which we got access to results from N–body numerical simulations performed by Dr. S. Gottloeber.

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