<i>K</i>-Band Properties of Well-Sampled Groups of Galaxies

Ramella, M.; Boschin, W.; Geller, Margaret J.; Mahdavi, Andisheh; Rines, Kenneth J.

doi:10.1086/424862

Cited by 39 publications

(68 citation statements)

References 85 publications

(224 reference statements)

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“…There are multiple studies of the dependence of the total stellar luminosity of cluster galaxies on cluster mass. In the K band, find that for the galaxies alone (excluding the BCG) L / M with ¼ 0:82 AE 0:05 ( ¼ 0:82 AE 0:04) within r 500 (r 200 ), and Ramella et al (2004) find ¼ 0:74 AE 0:06 within r 200 . A least-squares fit to our I-band data for the cluster galaxies yields ¼ 0:71 AE 0:07 within r 500 , which is consistent with these results and most other published values (Girardi et al [2000] and Rines et al [2004], but see Kochanek et al [2003] for an exception).…”

Section: Behavior Versus M 500mentioning

confidence: 93%

A Census of Baryons in Galaxy Clusters and Groups

Gonzalez

Zaritsky

Zabludoff

2007

ApJ

374

556

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We determine the contribution of stars in galaxies, intracluster stars, and the intracluster medium to the total baryon budget in nearby galaxy clusters and groups. We find that the baryon mass fraction ( f b b / m ) within r 500 is constant for systems with M 500 between 6 ; 10 13 and 1 ; 10 15 M . Although f b is lower than the WMAP value, the shortfall is on the order of both the observational systematic uncertainties and the depletion of baryons within r 500 that is predicted by simulations. The data therefore provide no compelling evidence for undetected baryonic components, particularly any that would be expected to vary in importance with cluster mass. A unique feature of the current analysis is direct inclusion of the contribution of intracluster light (ICL) in the baryon budget. With the addition of the ICL to the stellar mass in galaxies, the increase in X-ray gas mass fraction with increasing total mass is entirely accounted for by a decrease in the total stellar mass fraction, supporting the argument that the behavior of both the stellar and X-ray gas components is dominated by a decrease in star formation efficiency in more massive environments. Within just the stellar component, the fraction of the total stellar luminosity in the central, giant brightest cluster galaxy (BCG) and ICL (hereafter the BCG +ICL component) decreases as velocity dispersion ( ) increases for systems with 145 km s À1 1026 km s À1 , suggesting that the BCG+ICL component, and in particular the dominant ICL component, grows less efficiently in higher mass environments. The degree to which this behavior arises from our sample selection, which favored systems with central, giant elliptical galaxies, remains unclear. A more robust result is the identification of low-mass groups with large BCG +ICL components, demonstrating that the creation of ''intracluster'' stars does not require a massive cluster environment. Within r 500 and r 200 , the BCG +ICL contributes on average 40% and 33% of the total stellar light, respectively, for the clusters and groups in our sample. Because these fractions are functions of both enclosed radius and system mass, care should be exercised when comparing these values with other studies and simulations.

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Section: Behavior Versus M 500mentioning

confidence: 93%

A Census of Baryons in Galaxy Clusters and Groups

Gonzalez

Zaritsky

Zabludoff

2007

ApJ

374

556

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“…Lin et al 2003Ramella et al 2004;Muzzin et al 2007). There are many advantages of using L K instead of stellar mass: it is relatively A&A 592, A9 (2016) inexpensive compared to multiwavelength observations; it is not affected very much by extinction or recent star formation (Cowie et al 1994); and k-corrections are small and almost independent of galaxy type (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The Two Micron All-Sky Survey (2MASS; Jarrett et al 2000) offers a complete infrared map of the sky, which enables the study of large sample of galaxies, groups, and clusters (e.g. Lin et al 2003Kochanek et al 2001;Ramella et al 2004). The K-band luminosity-mass (L K − M) relation for local systems revealed a slope of 0.6 with system masses measured via dynamical analysis (Ramella et al 2004) or inferred from X-ray scaling relations ).…”

Section: Introductionmentioning

confidence: 99%

“…Lin et al 2003Kochanek et al 2001;Ramella et al 2004). The K-band luminosity-mass (L K − M) relation for local systems revealed a slope of 0.6 with system masses measured via dynamical analysis (Ramella et al 2004) or inferred from X-ray scaling relations ). Muzzin et al (2007) have explored the L K − M for massive clusters in a wide redshift range (0.17 < z < 0.54), finding consistent results with other work in the local Universe.…”

Section: Introductionmentioning

confidence: 99%

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The XXL Survey

Ziparo

Smith

Mulroy

et al. 2016

A&A

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Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, L K,500 − M 500,WL , for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M 500,WL = 3.5 × 10 13 M . This allows us to investigate whether the slope of the L K − M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M 500,WL = 0.35−12.10 × 10 14 M , at 0 < z < 0.6. The K-band luminosity scales as log 10 (L K,500 /10 12 L ) ∝ β log 10 (M 500,WL /10 14 M ) with β = 0.85 +0.35 −0.27 and an intrinsic scatter of σ ln L K |M = 0.37 +0.19 −0.17 . Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05 +0.16 −0.14 and an intrinsic scatter of 0.14 +0.09 −0.07 . The flattening in the L K − M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies.

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“…This approach is often applied to large redshift surveys as a useful and relatively straightforward mass estimator (e.g. Eke et al 2004;Ramella et al 2004;Robotham et al 2011). This estimator requires that group membership be well-established, with limited contamination from foreground and background galaxies, though robust estimators of group velocity dispersion, such as the gapper estimator (Beers, Flynn & Gebhardt 1990), help to reduce the impact of outliers in the galaxy velocity distribution.…”

Section: Introductionmentioning

confidence: 99%