The Mass-to-Light Function of Virialized Systems and the Relationship between Their Optical and X-Ray Properties

By C. Marinoni, M. Hudson. 2001

143 citations recorded by the source corpus.

We compare the B-band luminosity function of virialized halos with the mass function predicted by the Press-Schechter theory in cold dark matter (CDM) cosmogonies. We find that all cosmological models fail to match our results if a constant mass-to-light ratio is assumed. In order for these models to match the faint end of the luminosity function, a mass-to-light ratio decreasing with luminosity as L-0.5 ± 0.06 is required. For a ΛCDM model, the mass-to-light function has a minimum of ~100 h in solar units in the B band, corresponding to ~25% of the baryons in the form of stars, and this minimum occurs close to the luminosity of an L* galaxy. At the high-mass end, the ΛCDM model requires a mass-to-light ratio increasing with luminosity as L+0.5 ± 0.26. This scaling behavior of the mass-to-light ratio seems to be in qualitative agreement with the predictions of semianalytical models of galaxy formation. In contrast, for the τCDM model, a constant mass-to-light ratio suffices to match the high-mass end. We also derive the halo occupation number, i.e., the number of galaxies brighter than L hosted in a virialized system. We find that the halo occupation number scales nonlinearly with the total mass of the system, Ngal(>L) ∝ ℳ0.55 ± 0.026 for the ΛCDM model. We find a break in the power-law slope of the X-ray-to-optical luminosity relation, independent of the cosmological model. This break occurs at a scale corresponding to poor groups. In the ΛCDM model, the poor-group mass is also the scale at which the mass-to-light ratio of virialized systems begins to increase. This correspondence suggests a physical link between star formation and the X-ray properties of halos, possibly due to preheating by supernovae or to efficient cooling of low-entropy gas into galaxies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2d7892f81023cb5790cf87469c84924f32191425

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Citations in the corpus

Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field (2014, methodology): “More sophisticated models have been proposed, such as the halomodel of Marinoni & Hudson (2002), and recently an iterative prescription to reconstruct the density field from the c© 0000 RAS, MNRAS 000, 000–000 distribution of halos (Wang et al. 2009).”
Cosmic evolution of quasar clustering: implications for the host haloes (2004, background): “…abundance and clustering properties of galaxies at both low (Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Marinoni & Hudson 2002; Magliocchetti & Porciani 2003; van den Bosch, Mo & Yang 2003; Yang, Mo & van den Bosch 2003; Zehavi et al. 2004) and high…”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, background): “…objects certainly impact the strongly inverse total mass dependence of the total stellar mass fraction found by Gonzalez et al. (2007). crete a large fraction of their galaxies (with a low stellar mass fraction, of the order of 0.01) from the field (White & Frenk 1991; Marinoni & Hudson 2002).”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, methodology): “The fundamental assumption of the abundance matching method (Marinoni & Hudson 2002; Vale & Ostriker 2004; also see Behroozi et al. 2010 for a review) is thatMb is a monotonically increasing function of Mh.”
Accurate masses for dispersion-supported galaxies (2009, background): “However, Willman et al. (2004) demonstrated with a simulation that using the intracluster stars as tracers of cluster mass is accurate to ∼ 10%. c© 0000 RAS, MNRAS 000, 000–000 White & Rees 1978; Marinoni & Hudson 2002; Yang et al. 2003; Conroy & Wechsler 2009; Moster et al. 2010).”
A halo-based galaxy group finder: calibration and application to the 2dFGRS (2004, background): “…et al. 2001; White 2001; Jing, Börner & Suto 2002; Bullock, Wechsler & Somerville 2002; Berlind & Weinberg 2002; Scranton 2002; Kang et al. 2002; Marinoni & Hudson 2002; Zheng et al. 2002; Magliocchetti & Porciani 2003; Kochanek et al. 2003; Yan, Madgwick& White 2003; Yan, White & Coil 2004).”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “This is because the observed luminosity function of galaxies has a dramatically different shape from the predicted mass function of DM halos (e.g., White & Rees 1978; White & Frenk 1991; Marinoni & Hudson 2002; Yang et al. 2003; Moster et al. 2010).”
The Luminosity and Color Dependence of the Galaxy Correlation Function (2004, background): “For example, the group multiplicity function will pin down the high-mass end of hN iM (Peacock & Smith 2000; Marinoni & Hudson 2002; Kochanek et al. 2003), allowing us to explore more flexible parameterizations of the low-occupancy regime when fitting wp(rp).”
Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, methodology): “…Two recent works suggest thatΥB has a non-monotonic variation with mass (or luminosity), with a minimum value around 80–100 for luminositiesLB ≈ 109−11 L⊙ (Marinoni & Hudson 2002; Yang et al. 2003), both studies predicting ΥB ≃ 100 h70 for LB = LB,∗ = 1.88 × 1010L⊙ (Mamon & Łokas 2005).”
Towards a concordant model of halo occupation statistics (2006, background): “…that the average mass-to-light ratio of clusters continues to increase with mass (Adami et al. 1998; Bahcall & Comerford 2002; Girardi et al. 2002; Marinoni & Hudson 2002; Lin, Mohr & Stanford 2003, 2004; Ramella et al. 2004; Rines et al. 2004; Vale & Ostriker 2004, 2006; Popesso et al. 2005).”
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, background): “…clustering statistics of the galaxy distribution (e.g., Jing, Mo & Börner 1998; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; White 2001; Jing, Börner & Suto 2002; Berlind & Weinberg 2002; Bullock, Wechsler & Somerville 2002; Scranton 2002; Kang et al. 2002; Marinoni & Hudson 2002).”
A 2.5 per cent measurement of the growth rate from small-scale redshift space clustering of SDSS-III CMASS galaxies (2014, methodology): “In the subhalo abundance matching (‘SHAM’) formalism, the maximum circular velocity at accretion is often used (Marinoni & Hudson 2002; Conroy, Wechsler & Kravtsov 2006; Vale & Ostriker 2006).”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, background): “…mass function and a GLF or GSMF demonstrates that, in order to explain the GSMF shape, the fraction of baryonic mass converted to stars increases with mass to a peak before decreasing (Marinoni & Hudson 2002; Shankar et al. 2006; BGD08; Conroy & Wechsler 2009; Guo et al. 2010; Moster et al. 2010).”
Associations of Dwarf Galaxies (2006, background): “The shallow faint end slope of observed luminosity functions of galaxies compared with the halo mass function has indicated a paucity of light at low masses (Marinoni & Hudson 2002; van den Bosch et al. 2003, 2005).”
Galaxy Groups Within 3500 km s−1 (2017, background): “However, if so, the mass-to-light ratios will be large, an anticipated condition from comparisons of the galaxy luminosity function and theoretically anticipated halo mass function (Marinoni & Hudson 2002; van den Bosch et al. 2003).”
Linking halo mass to galaxy luminosity (2004, background): “…by comparing the group luminosity function with the halo mass function, they obtain the luminosity associated with each halo (Peacock & Smith 2000; Marinoni & Hudson 2002) and also develop ways to estimate the number of galaxies hosted in a halo, thus coming back partly to the P(N|M) estimate of…”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, background): “For dark matter to stellar mass ratios typical of massive ellipticals (see, e.g., Marinoni & Hudson 2002; McKay et al. 2002), the dark matter haloes in which the sub-millimeter galaxies reside have masses of > 1013 M⊙.”
The Halo Occupation Distribution and the Physics of Galaxy Formation (2002, background): “…and galaxy-galaxy lensing, have been taken by Jing, Mo, & Börner (1998), Peacock & Smith (2000), Scoccimarro et al. (2001), Guzik & Seljak (2002), Marinoni & Hudson (2002), Yang, Mo, & van den Bosch (2003), van den Bosch, Yang, & Mo (2003), Zehavi et al. (2003), and Magliocchetti & Porciani…”
Galaxy Groups in the SDSS DR4. II. Halo Occupation Statistics (2007, background): “…1998, 2002; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Bullock et al. 2002; Scranton 2002; Kang et al. 2002; Marinoni & Hudson 2002; Zheng et al. 2002, 2005; Magliocchetti & Porciani 2003; Berlind et al. 2003; Zehavi et al. 2004, 2005; Tinker et al. 2005).”