Virial Masses and the Baryon Fraction in Galaxies

By H. Hoekstra, H. Hoekstra, B. Hsieh, H. Yee, Huan Lin, M. Gladders. 2005

133 citations recorded by the source corpus.

We have measured the weak-lensing signal as a function of rest-frame B-, V-, and R-band luminosity for a sample of "isolated" galaxies. These results are based on four-band photometry from the Red-Sequence Cluster Survey, enabling us to determine photometric redshifts for a large number of galaxies. We select a secure sample of lenses with photometric redshifts 0.2 < z < 0.4 and study the relation between the virial mass and baryonic contents. In addition, we discuss the implications of the derived photometric redshift distribution for published cosmic shear studies. The virial masses are derived from a fit to the observed lensing signal. For a galaxy with a fiducial luminosity of 1010 h-2 LB,☉, we obtain a mass Mvir = 9.9 × 1011 M☉. The virial mass as a function of luminosity is consistent with a power law ∝L1.5, with similar slopes for the three filters considered here. These findings are in excellent agreement with results from the Sloan Digital Sky Survey and semianalytic models of galaxy formation. We measure the fraction of mass in stars and the baryon fraction in galaxies by comparing the virial mass-to-light ratio to predicted stellar mass-to-light ratios. We find that star formation is inefficient in converting baryons into stars, with late-type galaxies converting ~33% and early-type galaxies converting only ~14% of baryons into stars. Our results imply that the progenitors of early-type galaxies must have low stellar mass fractions, suggestive of a high formation redshift.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/cd544d904c68f0808bb3753b5f5d44b1542c1b19

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Citations in the corpus

CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, background): “Since Hoekstra et al. (2005) find that different choices for that relation yield similar curves, we choose not to iterate further.”
THE BARYON CONTENT OF COSMIC STRUCTURES (2009, background): “Gravitational lensing (Hoekstra et al. 2005; Gavazzi et al. 2007) provides important constraints on the total mass, but the conversion to the equivalent circular velocity is sensitive to the assumed model.”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, methodology): “This is supported by observations, as, e.g., Hoekstra et al. (2005) find from stellar population analysis that elliptical galaxies must have formed much of their stellar mass around the time of the elliptical-producing event.”
The baryonic assembly of dark matter haloes (2011, background): “For most galaxy-sized haloes, however, the detected baryons represent such a small fraction of the DM mass (e.g. Hoekstra et al. 2005; McGaugh 2005), and the halo cooling times should be sufficiently short, that it is unlikely that all the missing baryons are simply undetected.”
Galaxy halo masses and satellite fractions from galaxy–galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies (2005, methodology): “Next, when accounting for luminosity evolution, difference in passbands, and different definitions of mass, Hoekstra et al. (2005) find that their masses are about 25 per cent higher than those from Guzik & Seljak (2002) when comparing against the g-band results, but still statistically consistent.”
The Hubble Flow around the Centaurus A/M83 Galaxy Complex (2006, background): “Hoekstra et al. (2005) detected such a signal by measuring the orientation of the major axes of background galaxies around single ‘‘lens galaxies’’ with photometric redshifts z ¼ 0:2Y0:4.”
The kinematic connection between galaxies and dark matter haloes (2010, background): “…the liter- ⋆ dutton@uvic.ca † CITA National Fellow ature has focused on the relation between halo mass and galaxy luminosity or stellar mass (e.g. Yang et al. 2003; Kravtsov et al. 2004; van den Bosch et al. 2004; Hoekstra et al. 2005; Mandelbaum et al. 2006; Conroy et al. 2007; More et al. 2009).”
Observational probes of cosmic acceleration (2012, background): “Therefore, in the decade of the 2000s the leading galaxy-galaxy lensing surveys became the 92 deg2 Red-Sequence Cluster Survey (RCS; Hoekstra et al. 2004, 2005; Kleinheinrich et al. 2006) and eventually the 104 deg2 SDSS (references below).”
Galaxy Masses: A Review (2013, methodology): “Such a selection, which requires (photometric) redshift information, was used in Hoekstra et al. (2005) to study the relation between the virial mass and the luminosity.”
The Sloan Lens ACS Survey. IV. The Mass Density Profile of Early-Type Galaxies out to 100 Effective Radii (2007, methodology): “…have typically relied on very large sample of galaxies (Brainerd et al. 1996; Griffiths et al. 1996; Wilson et al. 2001; Guzik & Seljak 2002; Hoekstra et al. 2004, 2005; Kleinheinrich et al. 2006) or recently in the SDSS survey (Sheldon et al. 2004; Mandelbaum et al. 2006, hereafter S04 and…”
The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts (2009, methodology): “…of the relationship between the baryonic content and the dark matter content of galaxies, using the cross-correlation between background galaxy shapes and foreground galaxy positions (e.g., Hoekstra et al. 2005; Heymans et al. 2006a; Mandelbaum et al. 2006c), known as galaxy-galaxy lensing.”
Dynamical friction and galaxy merging time-scales (2007, background): “5⋆ , which is appropriate for massive galaxies in groups and clusters (Guzik & Seljak 2002; Hoekstra et al. 2005; Mandelbaum et al. 2006).”
The Sloan Lens ACS Survey. VI. Discovery and Analysis of a Double Einstein Ring (2008, background): “Another piece of information comes from weak lensing results at intermediate redshift (0.2 < z < 0.4) by Hoekstra et al. (2005), who found that galaxies with magnitude V − 5 log h ≃ −19 have virial masses Mvir ≃ 1.50+0.99−0.64 × 1011 h−170 M⊙ which also corresponds to log(2Vmax) = 2.20± 0.09, in…”
A constant dark matter halo surface density in galaxies (2009, methodology): “…let us notice that it provides a fit marginally sufficient for the shear data, but less satisfactory than the Burkert profile especially around the most luminous objects (MB = −21.4) (Figure A1; see also Figure 6 of Hoekstra et al. 2005) we found Mvir = 4.2 × 10 12 where we found a reduced χ2 of 2.”