Kinematics of AWM and MKW Poor Clusters

Koranyi, D.; Geller, Margaret J.

doi:10.1086/338096

Cited by 31 publications

(58 citation statements)

References 59 publications

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“…Bahcall & Comerford (2002) derive an analogous dependence of M =L B on X-ray temperature, which they attribute to differences in the ages of the stellar population for galaxies in groups of different mass. The decrease in the fraction of starforming galaxies with the mass or velocity dispersion of groups appeared to support the argument that the variation in M/L with mass was a population effect (see, e.g., Biviano et al 1997;Koranyi & Geller 2002;Balogh et al 2004).…”

Section: Introductionsupporting

confidence: 60%

“…For systems observed by Zabludoff & Mulchaey (1998) and Koranyi & Geller (2002) we search the 2MASS catalog to the radius listed in Table 1.…”

Section: The Group Catalog and Group Membershipmentioning

confidence: 99%

“…For redshifts from Mahdavi et al (1999, Zabludoff & Mulchaey (1998), and Koranyi & Geller (2002) we take the membership assignments given by these authors. We searched the NASA / IPAC Extragalactic Database (NED) 2 for additional members of each group.…”

Section: The Group Catalog and Group Membershipmentioning

confidence: 99%

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K-Band Properties of Well-Sampled Groups of Galaxies

et al. 2004

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We use a sample of 55 groups and six clusters of galaxies ranging in mass from 7 ; 10 11 to 1:5 ; 10 15 M to examine the correlation of the K s -band luminosity with mass discovered by Lin and coauthors in 2003. We use the Two-Micron All-Sky Survey catalog and published redshifts to construct complete magnitude-limited redshift surveys of the groups. From these surveys we explore the IR photometric properties of groups members, including their IR color distribution and luminosity function. Although we find no significant difference between the group K s luminosity function and the general field, there is a difference between the color distribution of luminous group members and their counterparts (generally background) in the field. There is a significant population of luminous galaxies with H À K s k 0:35, which are rarely, if ever, members of the groups in our sample. The most luminous galaxies that populate the groups have a very narrow range of IR color. Over the entire mass range covered by our sample, the K s luminosity increases with mass as L K s / M 0:64AE0:06 , implying that the mass-to-light ratio in the K s band increases with mass. The agreement between this result and earlier investigations of essentially nonoverlapping sets of systems shows that this window in galaxy formation and evolution is insensitive to the selection of the systems and to the details of the mass and luminosity computations.

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Section: Introductionsupporting

confidence: 60%

“…For systems observed by Zabludoff & Mulchaey (1998) and Koranyi & Geller (2002) we search the 2MASS catalog to the radius listed in Table 1.…”

Section: The Group Catalog and Group Membershipmentioning

confidence: 99%

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K-Band Properties of Well-Sampled Groups of Galaxies

et al. 2004

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“…We find that the source emission fills the entire field of view, contrary to the analysis in O'Sullivan et al (2005), which reported a ''soft excess'' described by a 0.6 keV bremsstrahlung component, probably the misinterpreted source. It is difficult to classify AWM 4 as a merging system, given its relaxed appearance both in the X-rays and in the optical (Koranyi & Geller 2002). Instead, the flat temperature profile likely reflects the influence of the powerful AGN, with radio lobes extending out from the central galaxy NGC 6051 along the minor axis of the galaxy to 100 kpc (e.g., Neumann et al 1994).…”

Section: Results For Individual Objectsmentioning

confidence: 99%

Probing the Dark Matter and Gas Fraction in Relaxed Galaxy Groups with X‐Ray Observations fromChandraandXMM‐Newton

Gastaldello

Buote

Humphrey

et al. 2007

ApJ

168

253

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We present radial mass profiles within $0:3r vir for 16 relaxed galaxy groups-poor clusters (kT range 1Y3 keV ) selected for optimal mass constraints from the Chandra and XMM-Newton data archives. After accounting for the mass of hot gas, the resulting mass profiles are described well by a two-component model consisting of dark matter, represented by an NFW model, and stars from the central galaxy. The stellar component is required only for eight systems, for which reasonable stellar mass-to-light ratios (M/L K ) are obtained, assuming a Kroupa IMF. Modifying the NFW dark matter halo by adiabatic contraction does not improve the fit and yields systematically lower M /L K . In contrast to previous results for massive clusters, we find that the NFW concentration parameter (c vir ) for groups decreases with increasing M vir and is inconsistent with no variation at the 3 level. The normalization and slope of the c vir -M vir relation are consistent with the standard ÃCDM cosmological model with 8 ¼ 0:9 (considering a 10% bias for early forming systems). The small intrinsic scatter measured about the c vir -M vir relation implies that the groups represent preferentially relaxed, early forming systems. The mean gas fraction ( f ¼ 0:05 AE 0:01) of the groups measured within an overdensity Á ¼ 2500 is lower than for hot, massive clusters, but the fractional scatter ( f /f ¼ 0:2) for groups is larger, implying a greater impact of feedback processes on groups, as expected.

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“…How to make them and what it does to the rest of the cluster are the most important issue, and the middle references on this sound a bit mutually contradictory. Koranyi & Geller (2002) conclude that the rest of a smallish cluster doesn't seem to know or care whether there is a cD at its center, while Matsushita et al (2002) conclude that M87 is fully integrated with the inner part of Virgo, at least in X-ray properties.…”

Section: ϫ4mentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

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Kinematics of AWM and MKW Poor Clusters

Cited by 31 publications

References 59 publications

K-Band Properties of Well-Sampled Groups of Galaxies

K-Band Properties of Well-Sampled Groups of Galaxies

Probing the Dark Matter and Gas Fraction in Relaxed Galaxy Groups with X‐Ray Observations fromChandraandXMM‐Newton

Astrophysics in 2002

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