Near-Infrared Properties of Galaxy Clusters: Luminosity as a Binding Mass Predictor and the State of Cluster Baryons

By Yen-Ting Lin, Joseph J. Mohr, S. Stanford. 2003

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We explore the near-infrared properties of galaxies within 27 galaxy clusters using data from the Two Micron All Sky Survey (2MASS). For a subsample of 13 clusters with available X-ray imaging data, we examine the properties of both the galaxies and the intracluster medium. We show that the K-band luminosity is correlated with cluster mass, providing a binding mass estimate accurate to 45%. The mass-to-light ratio in our ensemble increases by a factor of ~2 over the cluster mass range (1014-1015 M☉). We examine the total baryon fraction, showing that it is an increasing function of cluster mass. Using the mass-to-light ratio of massive clusters, we find that ΩM = 0.19 ± 0.03; using the total baryon fraction we find that ΩM = 0.28 ± 0.03, in good agreement with recent cosmic microwave background (CMB) anisotropy constraints. Differences between these two estimates suggest that the K-band mass-to-light ratio in massive clusters may be lower than that in the universe by as much as ~30%. We examine the stellar mass fraction, the intracluster medium (ICM) mass to stellar mass ratio, and the cluster iron mass fraction. The stellar mass fraction decreases by a factor of 1.8 from low- to high-mass clusters, and the ICM to stellar mass ratio increases from 5.9 to 10.4 over the same mass range. Together, these measurements suggest a decrease of star formation efficiency with increasing cluster mass and provide constraints on models of the thermodynamic history of the intracluster medium. The cluster iron mass to total mass ratio is constant and high, suggesting that some efficient and uniform enrichment process may have taken place before the bulk of stars in cluster galaxies formed.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/63e859eb46891af2e05d3f7b16523e31c0ba9f43

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Citations in the corpus

A Fitting Formula for the Merger Timescale of Galaxies in Hierarchical Clustering (2007, result): “This ratio is in reasonable agreement with the observed values of galaxy groups(Gonzalez et al. 2007; Lin et al. 2003).”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, background): “The observed anti-correlation in the relative dependencies of gas and stars with total mass implies that there is more mass locked in stars in systems which contain less gas (Lin et al. 2003; Gonzalez et al. 2007; Giodini et al. 2009).”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, methodology): “Contrary to Lin et al. (2003), who argued for Mgas/M∗,0 that is independent of total cluster mass, Gonzalez et al. (2007) find that Mgas/M∗,0 rises monotonically with cluster mass, from a value of about 5 for low-mass clusters to about 15 for the most-massive systems.”
GALAXY CLUSTERS IDENTIFIED FROM THE SDSS DR6 AND THEIR PROPERTIES (2009, background): “In general, theM/L is also described by a power law,M/L ∝ Lτ , with τ in the range 0.2– 0.4 (Bahcall & Comerford 2002; Girardi et al. 2002; Lin et al. 2003; Rines et al. 2004; Popesso et al. 2005).”
THE BLANCO COSMOLOGY SURVEY: DATA ACQUISITION, PROCESSING, CALIBRATION, QUALITY DIAGNOSTICS, AND DATA RELEASE (2012, background): “Interesting studies of the galaxy properties and their evolution within clusters include studies of the blue fraction and the halo occupation distribution (e.g. Butcher & Oemler 1984; Lin et al. 2003; Lin & Mohr 2004; Lin et al. 2006; Hansen et al. 2009; Zenteno et al. 2011).”
GALAXY CLUSTER BARYON FRACTIONS REVISITED (2013, methodology): “In particular, we consider results from Lin et al. (2003, 2012), Giodini et al. (2009), Andreon (2010), Laganá et al. (2011), Zhang et al. (2011), and Leauthaud et al. (2012).”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “However, the vast majority of the attempts to estimate the baryon mass fraction in nearby clusters have reported smaller values than expected (Ettori 2003; Lin et al. 2003; Biviano & Salucci 2006; McCarthy et al. 2007).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, background): “Lin et al. (2003) gave: M∗,500 = 7.30 × 10 11M⊙(TX/1keV) 1.169 (adjusted to our cosmology) from the 2MASS data of nearby groups and clusters, which includes the stellar mass in cluster galaxies.”
Jet-regulated cooling catastrophe (2010, methodology): “Their stellar fraction is the best fit of their data combined with data from Lin et al. (2003).”