Where are the stars?

Details Where are the stars? Where are the stars?

2004-12-02

arxiv.org/abs/astro-ph/0412049v1

Mon.Not.Roy.Astron.Soc. 362 (2005) 1233-1246

Astronomy and Astrophysics

Astrophysics

15 pages, 14 figures (1 colour), submitted to MNRAS

Scientific paper

10.1111/j.1365-2966.2005.09384.x

The 2dFGRS is used in conjunction with the 2MASSXSC to study the near-IR light and stellar mass content of the local Universe. Mock galaxy catalogues, constructed from cosmological N-body simulations and semi-analytical galaxy formation models, are used to gauge the accuracy with which quantities can be recovered. The mean luminosity densities of the Universe are found to be rho_J=(3.57+/-0.11)*10^8 h Lsol/Mpc^3 and rho_KS=(7.04+/-0.23)*10^8 h Lsol/Mpc^3 (statistical uncertainty). Using the 2PIGG catalogue, the group dynamical mass-to-light ratio in the K_S band is found to increase by a factor of ~3 when going from groups with total bJ-band luminosities of 3*10^10 h^-2 Lsol to rich clusters, which have typical values of Upsilon_K~80 h Upsilon_sol. Taking into account the bias introduced by uncertainties in estimating galaxy stellar masses from luminosities, a value of Omega_* h=(0.99+/-0.03)*10^-3 is measured, assuming that a Kennicutt stellar IMF is applicable to all galaxies. The 2PIGGs are then used to study the distribution of the stellar content of the local Universe. The three main conclusions are: (1) a slowly rising stellar M/L_KS is found with the clusters having the largest value of ~0.6 Upsilon_sol, (2) in contrast, the fraction of mass in stars decreases with increasing group size, reaching ~5*10^-3 h for the rich clusters, and (3) in answer to the question posed in the title, most stellar mass is contained in Local Group-sized objects (M~2*10^12 h^-1 Msol) with only ~2% in clusters with M>5*10^14 h^-1 Msol.

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