Stellar and Total Baryon Mass Fractions in Groups and Clusters Since Redshift 1*

Giodini, S.; Pierini, D.; Finoguenov, A.; Pratt, G. W.; Böehringer, H.; Leauthaud, Alexie; Guzzo, L.; Aussel, H.; Bolzonella, M.; Capak, P.; Elvis, M.; Hasinger, G.; Ilbert, O.; Kartaltepe, Jeyhan S.; Koekemoer, Anton M.; Lilly, S. J.; Massey, Richard; McCracken, H. J.; Rhodes, Jason; Salvato, M.; Sanders, D. B.; Scoville, N. Z.; Sasaki, S.; Smolčić, Vernesa; Taniguchi, Yuki; Thompson, D. J.

doi:10.1088/0004-637x/703/1/982

Cited by 298 publications

(479 citation statements)

References 82 publications

(121 reference statements)

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“…Baryonic evolution is potentially a thornier issue. Some X-ray studies suggest a depletion of baryonic mass (stars + hot gas) relative to the universal Ω b /Ω m ratio by 20 − 30% within the ∆ = 500ρ c radius, with systematically larger depletion in less massive clusters (e.g., Giodini et al, 2009). …”

Section: Theoretical Systematicsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: Theoretical Systematicsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…The M tot − Lop relations have power law slopes close to unity, but not quite so, as most studies indicate an increase of the mass-to-light ratio M/Lop with cluster mass. This is a direct consequence of the variation of the fraction of stars in galaxies (Lin et al 2003;Giodini et al 2009), suggesting that the efficiency of star formation or galaxy evolution processes depend on the total mass. We note that these same processes may also affect the ICM properties in low mass systems.…”

Section: Optical Scaling Relationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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Well-calibrated scaling relations between the observable properties and the total masses of clusters of galaxies are important for understanding the physical processes that give rise to these relations. They are also a critical ingredient for studies that aim to constrain cosmological parameters using galaxy clusters. For this reason much effort has been spent during the last decade to better understand and interpret relations of the properties of the intra-cluster medium. Improved X-ray data have expanded the mass range down to galaxy groups, whereas SZ surveys have openened a new observational window on the intracluster medium. In addition, continued progress in the performance of cosmological simulations has allowed a better understanding of the physical processes and selection effects affecting the observed scaling relations. Here we review the recent literature on various scaling relations, focussing on the latest observational measurements and the progress in our understanding of the deviations from self similarity.

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“…Baryon (top panel), hot gas (middle) and star (bottom) fractions versus halo mass for the four physics models at z = 0. In all panels, the solid black curve is the best-fitting observed relation from the COSMOS survey (Giodini et al 2009). We additionally show observed gas fractions from XMM-Newton data (Arnaud, Pointecouteau & Pratt 2007;Croston et al 2008) in the middle panel and the best-fitting relation between star fraction and halo mass from SDSS data (Budzynski et al 2014) in the lower panel.…”

Section: Baryon Gas and Star Fractionsmentioning

confidence: 99%

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Pike

Kay

Newton

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present results from a new set of 30 cosmological simulations of galaxy clusters, including the effects of radiative cooling, star formation, supernova feedback, black hole growth and AGN feedback. We first demonstrate that our AGN model is capable of reproducing the observed cluster pressure profile at redshift, z 0, once the AGN heating temperature of the targeted particles is made to scale with the final virial temperature of the halo. This allows the ejected gas to reach larger radii in highermass clusters than would be possible had a fixed heating temperature been used. Such a model also successfully reduces the star formation rate in brightest cluster galaxies and broadly reproduces a number of other observational properties at low redshift, including baryon, gas and star fractions; entropy profiles outside the core; and the Xray luminosity-mass relation. Our results are consistent with the notion that the excess entropy is generated via selective removal of the densest material through radiative cooling; supernova and AGN feedback largely serve as regulation mechanisms, moving heated gas out of galaxies and away from cluster cores. However, our simulations fail to address a number of serious issues; for example, they are incapable of reproducing the shape and diversity of the observed entropy profiles within the core region. We also show that the stellar and black hole masses are sensitive to numerical resolution, particularly the gravitational softening length; a smaller value leads to more efficient black hole growth at early times and a smaller central galaxy.

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Stellar and Total Baryon Mass Fractions in Groups and Clusters Since Redshift 1*

Cited by 298 publications

References 82 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Scaling Relations for Galaxy Clusters: Properties and Evolution

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

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