STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1

By S.Giodini, D. Pierini, A. Finoguenov, G. Pratt, H. Boehringer, A. Leauthaud, L. Guzzo, H. Aussel, M. Bolzonella, P. Capak and 38 more. 2009

238 citations recorded by the source corpus.

We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 ⩽ z ⩽ 1 are selected from the COSMOS 2 deg2 survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R 500. The total sample of 118 groups and clusters with z ⩽ 1 spans a range in M 500 of ∼1013–1015 M ☉. We find that the stellar mass fraction associated with galaxies at R 500 decreases with increasing total mass as M −0.37 ± 0.04 500, independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f stars+gas 500 = f stars 500 + f gas 500) is found to increase by ∼25%, when M 500 increases from 〈M〉 = 5 × 1013 M ☉ to 〈M〉 = 7 × 1014 M ☉. After consideration of a plausible contribution due to intracluster light (11%–22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3σ for groups of 〈M〉 = 5 × 1013 M ☉. The discrepancy decreases toward higher total masses, such that it is 1σ at 〈M〉 = 7 × 1014 M ☉. We discuss this result in terms of nongravitational processes such as feedback and filamentary heating.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/679df2018e24d0abea4d8454b2b912a148e166a2

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

ANCIENT LIGHT FROM YOUNG COSMIC CITIES: PHYSICAL AND OBSERVATIONAL SIGNATURES OF GALAXY PROTO-CLUSTERS (2013, background): “…ICM on scales of about 1 Mpc. Galaxy kinematics and gravitational lensing studies show that cluster galaxies are embedded in a massive halo of dark matter with mass of& 1014 M⊙, which weighs about five times more than its baryonic contents (Gonzalez et al. 2007; Giodini et al. 2009; Andreon 2010).”
MASSIVE HALOS IN MILLENNIUM GAS SIMULATIONS: MULTIVARIATE SCALING RELATIONS (2009, background): “We note that Arnaud data agree with other observational determinations at high mass (Vikhlinin 2006; Giodini et al. 2009), while the Sun et al. (2009) data extend to lower mass, ∼ 1013 h−1 M⊙.”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “At R 500 , the measurement of f gas for massive clusters presented by Pratt et al. (2009) ( see also Giodini et al. 2009, for massive clusters with (4–10) × 10 14 M ⊙ ) is lower by a factor 1.3 with respect to our estimate (although compatible within ± 2 σ ). re-ported We can also compare our…”
What drives the growth of black holes (2011, background): “Observations show that the LX– TX relation is remarkably steep at the low-temperature end, suggesting that small to moderate-mass groups have lower baryon fractions in the centers of their darkmatter halos than higher-mass systems (e.g., Sun et al., 2009; Giodini et al., 2009).”
Lyα blobs as an observational signature of cold accretion streams into galaxies (2009, methodology): “The assumed gas mass fraction fgas = 0.08 is in good agreement with the value derived for groups of galaxies at z < 1 (e.g. Giodini et al. 2009).”
The VISTA deep extragalactic observations (VIDEO) survey (2012, background): “Within 0 < z < 1, clusters of galaxies appear to undergo little in the way of strong evolution, either in their gas-phase properties or in the properties of the more massive galaxies within them (e.g. Rosati, Borgani & Norman 2002; Collins et al. 2009; Giodini et al. 2009).”
Simulating galaxy formation with the IllustrisTNG model (2017, unknown): “…Illustris 1011 1012 1013 Total Halo Mass [ < r500c ] [ M sun ] 0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2 G as F ra ct io n [< r 50 0c ] Giodini et al. 2009 Lovisari et al. 2015 + b / + m L25n128 fiducial TNG L25n256 fiducial TNG L25n512 fiducial TNG L25n128 fiducial Illustris L25n256…”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, background): “…systems, the mass of hot, X-ray emitting gas far exceeds that in colder gas and stars (e.g. Lin & Mohr 2004; Gonzalez, Zaritsky, & Zabludoff 2007; Giodini et al. 2009; Dai et al. 2010; Leauthaud et al. 2012; Behroozi et al. 2013), and the gas mass fraction, fgas, is expected to approximately…”
THE BARYON CONTENT OF COSMIC STRUCTURES (2009, methodology): “The cluster data (Giodini et al. 2009) are referenced to ∆ = 500, so for H0 = 72 kms −1 Mpc−1 (Freedman et al. 2001), M500 = (204552 km −3 s3 M−1⊙ )V 3 500.”
Theoretical Challenges in Galaxy Formation (2016, background): “…systems are usually embedded in hot (> 105K) X-ray emitting gas comprising a significant fraction of the total baryonic mass (e.g. Anderson et al. 2015, Dai et al. 2010, Giodini et al. 2009, Kravtsov & Borgani 2012, Mulchaey 2000, Renzini & Andreon 2014, Sun et al. 2009, Vikhlinin et al. 2006).”
GALAXY CLUSTER BARYON FRACTIONS REVISITED (2013, methodology): “We list the projected and deprojected stellar mass relations in Table 4.”
Observational probes of cosmic acceleration (2012, background): “Some X-ray studies suggest a depletion of baryonic mass (stars + hot gas) relative to the universal Ωb/Ωm ratio by 20− 30% within the ∆ = 500ρc radius, with systematically larger depletion in less massive clusters (e.g., Giodini et al., 2009).”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, background): “However, recent results suggestthat there is still a∼ 3σ deficit of baryons with respect to that measured by WMAP on galaxy group scales (Giodini et al. 2009), implying that both coolingandheating must contribute to changing the thermodynamic properties of the ICM.”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, background): “For the two ends of the cluster mass range considered above, the best-fit relations of Giodini et al. (2009) then give Mgas/M∗,0 of about 7 and 11, respectively.”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, result): “As for the behaviour of the mass fraction in stars, we show in Figure 6 the comparison between our simulations and observational results from Gonzalez et al. (2007), who also included in thestellar budget the contribution from diffuse intra-cluster star (see also Giodini et al. 2009).”
First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies (2017, background): “…discrepancies, but are of substantial importance, for example, for the theoretical interpretation of abundance matching constraints at the cluster scale (Giodini et al. 2009; Andreon 2012; Budzynski et al. 2012; Gonzalez et al. 2013; Kravtsov et al. 2014; Andreon 2015; Chiu et al. 2016).”