Virial masses of galactic haloes from galaxy–galaxy lensing: theoretical modelling and application to Sloan Digital Sky Survey data

By J. Guzik, Uros Seljak. 2002

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We present a theoretical analysis of galaxy–galaxy lensing in the context of halo models with cold dark matter motivated dark matter profiles. The model enables us to distinguish between the central galactic and non-central group/cluster contributions. We apply the model to the recent Sloan Digital Sky Survey (SDSS) measurements with known redshifts and luminosities of the lenses. This allows one to model accurately the mass distribution of a local galaxy population around and above L*. We find that the virial mass of an L* galaxy is M200= (5 − 10) × 1011h−1 M⊙ depending on the colour of the galaxy. This value varies significantly with galaxy morphology, with M* for late types being lower by a factor of 10 in u′, a factor of 7 in g′ and a factor of 2.5–3 in r′, i′ and z′ relative to early types. The fraction of non-central galaxies in groups and clusters is estimated to be below 10 per cent for late types and around 30 per cent for early types. Using the luminosity dependence of the signal, we find that for early types the virial halo mass M scales with luminosity as M∝L1.4±0.2 in red bands above L*. This shows that the virial mass-to-light ratio (M/L) is increasing with luminosity for galaxies above L*, as predicted by theoretical models. The virial mass-to-light ratio in the i′ band is 17 (45) h M⊙/L⊙ at L* for late (early) types. Combining this result with cosmological baryon fraction, one finds that 70 (25) per cent h−1ΥiΩm/12Ωb of baryons within r200 are converted to stars at L*, where Υi is the stellar mass-to-light ratio in the i′ band. This indicates that for both early- and late-type galaxies around L* a significant fraction of all the baryons in the halo is transformed into stars.

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

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Citations in the corpus

Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “Similar to the galaxy-galaxy autocorrelation function, the galaxy-matter cross correlation function can be accurately modeled using the halo model (Guzik & Seljak 2001, 2002; Mandelbaum et al. 2005; Yoo et al. 2006; Cacciato et al. 2009; Leauthaud et al. 2011, 2012; van Uitert et al. 2011).”
The Galaxy-Mass Correlation Function Measured from Weak Lensing in the Sloan Digital Sky Survey (2003, result): “Because C(R) depends on luminosity, the average of the subsamples could, in principle, differ from the mean estimated from the full sample, as suggested by Guzik & Seljak (2002) regarding the results of McKay et al. (2002).”
Systematic errors in weak lensing: application to SDSS galaxy-galaxy weak lensing (2005, background): “…of galaxy–galaxy weak lensing (Brainerd, Blandford & Smail 1996; Hudson et al. 1998; Fischer et al. 2000; McKay et al. 2001; Smith et al. 2001; Guzik & Seljak 2002; Hoekstra et al. 2003; Sheldon et al. 2004; Hoekstra, Yee & Gladders 2004; Seljak et al. 2005), the tangential shear distortion…”
Binary Quasars in the Sloan Digital Sky Survey: Evidence for Excess Clustering on Small Scales (2005, background): “Another complementary set of low-redshift observations that probe clustering on small scales (10 h 1 kpc to 1 h 1 Mpc) is the SDSS galaxy-galaxy lensing studies (Guzik & Seljak 2002; Sheldon et al. 2004), whichmeasure the galaxy–darkmatter crosscorrelation function.”
What Do Gravitational Lens Time Delays Measure? (2002, background): “…dynamical measurements (see, e.g., Rix et al. 1997; Romanowsky & Kochanek 1999; Gerhard et al. 2001; Treu & Koopmans 2002), weak lensing (see, e.g., Guzik & Seljak 2002), and X-ray measurements (see, e.g., Fabbiano 1989; Lowenstein & White 1999) all require mass distributions close to the dark…”
Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, methodology): “Moreover, from their analysis of SDSSgalaxies, Guzik & Seljak (2002) find thatL∗ galaxies have mass-to-light ratio Υ of order of 100 in theB band, again implying substantial dark matter, since the stellar contribution to the mass-to-light ratio is thought to be onlyΥ∗ ≃ 8 in the blue band (see e.g. ”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…al. 1998; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Yang et al. 2003; Scoccimarro et al. 2001; Cooray & Sheth 2002; Berlind & Weinberg 2002; Guzik & Seljak 2002; Zheng et al. 2005; Mandelbaum et al. 2006; van den Bosch et al. 2007) framework, to solve for the mapping between the stellar…”
Large‐scale bias and stochasticity of haloes and dark matter (2004, background): “We will show the results for a range of halo masses, which can be roughly thought as corresponding to galaxies with different luminosities since there is a tight relation between the halo mass and luminosity (McKay et al. 2001; Guzik & Seljak 2002; ?).”
The Local Group and Other Neighboring Galaxy Groups (2005, background): “Recently, Guzik & Seljak (2002) and Hoekstra et al. (2004) determined parameters of dark halos for field galaxies and members of loose groups from weak lensing in the Sloan DSS and in the Red-Sequence Cluster Survey.”
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, methodology): “Indeed, recently Guzik & Seljak (2002) and Yang et al. (2002) used the galaxy-galaxy weak lensing results of the SDSS (McKay et al. 2001) to constrain the virial masses of galaxies brighter than L∗ (see also McKay et al. 2002).”
The kinematic connection between galaxies and dark matter haloes (2010, methodology): “Seljak (2002) used the weak lensing virial mass-to-light ratios from Guzik & Seljak (2002) and the same method as used here to derive a Vopt/V200 ratio for L* galaxies.”
Observing the Dark Matter Density Profile of Isolated Galaxies (2003, background): “Moreover, the galaxy–mass correlation function can be affected by neighbors of the lens galaxy (e.g., Smith et al. 2001; Guzik & Seljak 2002).”
Stars beyond galaxies: the origin of extended luminous haloes around galaxies (2005, unknown): “It is unclear whether the mass of the halo of the Milky Way is unusually low compared with other spiral galaxies of similar luminosity, but galaxy-galaxy weak lensing data seem to favour halo masses of the order we find here for late-typeL∗ galaxies (see, e.g., Guzik & Seljak 2002).”
Galaxy Masses: A Review (2013, methodology): “The halo model was used by Guzik & Seljak (2002) and Mandelbaum et al. (2006b) to interpret the results from the SDSS and constrain the fraction of satellite galaxies.”