An X‐Ray and Optical Study of Matter Distribution in Clusters of Galaxies

Cirimele, G.; Nesci, R.; Trèvese, D.

doi:10.1086/303538

Cited by 43 publications

(58 citation statements)

References 31 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…All objects in their sample fall in the range M/L V = 100−150 h 50 M /L . Similar values were derived by Cirimele et al (1997) from a sample of 12 clusters in the temperature range from 2 to 10 keV…”

Section: Mass Versus Light As a Function Of Scalesupporting

confidence: 80%

Entropy scaling in galaxy clusters: Insights from anXMM-Newtonobservation of the poor cluster A1983

Pratt

Arnaud

2003

A&A

111

View full text Add to dashboard Cite

Abstract. An XMM-Newton observation of the cool (kT = 2.1 keV) cluster A1983, at z = 0.044, is presented. Gas density and temperature profiles are calculated over the radial range up to 500 h −1 50 kpc, corresponding to ∼0.35 r 200 . The outer regions of the surface brightness profile are well described with a β-model with β = 0.74, but the central regions require the introduction of a second component. The temperature profile is flat at the exterior with a slight dip towards the centre. The total mass profile, calculated from the temperature and density information assuming hydrostatic equilibrium, is consistent with an NFW profile, but with a low concentration parameter c = 3.75 ± 0.74, which may be due to the cluster not being totally relaxed. Published optical data are used to calculate the M/L B ratio profile and the overall iron mass over luminosity ratio. The M/L B ratio profile shows that, at large scale, light traces mass to a reasonable extent, and the M/L B ratio at 0.35r 200 is consistent with the trends with mass observed in the optical. The iron mass over luminosity ratio is about two times less than that observed for a cluster at 5 keV. The gas mass fraction rises rapidly in the central regions to level off quickly at ∼200 h −1 50 kpc; the value at 0.35 r 200 is ∼8%. The scaling properties of the emission measure profile are consistent with the empirical relation M gas ∝ T 1.94 ; use of the standard self-similar relation M gas ∝ T 1.5 results in a scaled profile that is a factor of about two too low as compared to the reference mean profile for hot clusters. Comparison of the entropy profile of this cool cluster with that of the hot cluster A1413 shows that the two profiles are extremely well scaled using the empirically determined relation S ∝ T 0.65 , suggesting that the slope of the S -T relation is shallower than expected in the standard self-similar model. The form of the two entropy profiles is remarkably similar, and there is no sign of a larger isentropic core in the cooler cluster. These data provide powerful agruments against preheating models. In turn, there is now increasing observational support for a trend of f gas with system mass, which may go some way towards explaining the observed scaling behaviour.

show abstract

Section: Mass Versus Light As a Function Of Scalesupporting

confidence: 80%

Entropy scaling in galaxy clusters: Insights from anXMM-Newtonobservation of the poor cluster A1983

Pratt

Arnaud

2003

A&A

111

View full text Add to dashboard Cite

show abstract

“…with somewhat lower values in the samples by Cirimele et al (1997);Finoguenov et al (2003) (though still growing with radius in the latter) and somewhat higher values in the sample by Roussel et al (2000). Whether the fraction of hot vs. cold baryons, that is the efficiency of galaxy formation, increases noticeably with cluster temperature and richness is on the other hand still a matter of debate (Bryan 2000;Balogh et al 2001;Lin et al 2003).…”

Section: The Problem Of Dilutionmentioning

confidence: 66%

Chemical evolution of the intra-cluster medium

Moretti¹,

Portinari²,

Chiosi³

2003

A&A

View full text Add to dashboard Cite

Abstract. The high metallicity of the intra-cluster medium (ICM) is generally interpreted on the basis of the galactic wind scenario for elliptical galaxies. In this framework, we develop a toy model to follow the chemical evolution of the ICM, formulated in analogy to chemical models for individual galaxies. The model computes the galaxy formation history (GFH) of cluster galaxies, connecting the final luminosity function (LF) to the corresponding metal enrichment history of the ICM. The observed LF can be reproduced with a smooth, Madau-plot like GFH peaking at z ∼ 1−2, plus a "burst" of formation of dwarf galaxies at high redshift. The model is used to test the response of the predicted metal content and abundance evolution of the ICM to varying input galactic models. The chemical enrichment is computed from "galactic yields" based on models of elliptical galaxies with a variable initial mass function (IMF), favouring the formation of massive stars at high redshift and/or in more massive galaxies. For a given final galactic luminosity, these model ellipticals eject into the ICM a larger quantity of gas and of metals than do standard models based on the Salpeter IMF. However, a scenario in which the IMF varies with redshift as a consequence of the effect of the cosmic background temperature on the Jeans mass scale appears to be too mild to account for the observed metal production in clusters. The high iron-massto-luminosity-ratio of the ICM can be reproduced only by assuming a more dramatic variation of the typical stellar mass, in line with other recent findings. The mass in the wind-ejected gas is predicted to exceed the mass in galaxies by a factor of 1.5-2 and to constitute roughly half of the intra-cluster gas.

show abstract

“…Carlberg et al 1997;van der Marel et al 2000;Biviano & Girardi 2003) or based on the other methods (e.g. Cirimele et al 1997;Parker et al 2005;Sereno et al 2010). …”

Section: Discussionmentioning

confidence: 99%

“…Observationally, there are lots of controversies in the literature on whether satellite galaxies unbiasedly trace the underlying mass distribution in galaxy clusters/groups. Some studies conclude that the satellite (luminosity) distribution traces the mass distribution (Tyson & Fischer 1995;Squires et al 1996;Fischer & Tyson 1997;Cirimele et al 1997;Carlberg et al 1997;van der Marel et al 2000;Rines et al 2001;Tustin et al 2001;Biviano & Girardi 2003;Lokas & Mamon 2003;Kneib et al 2003;Biviano & Girardi 2003;Parker et al 2005;Popesso et al 2007;Sheldon et al 2009;Wojtak & Lokas 2010;Sereno et al 2010;Bahcall & Kulier 2014); whiles some studies suggest that the spatial distribution of satellites (luminosity) are less concentrated than that of matter (Rines et al 2000;Lin et al 2004;Hansen et al 2005;Nagai & Kravtsov 2005;Yang et al 2005;Budzynski et al 2012); still some claim luminosity distribution are actually more concentrated (Koranyi et al 1998;Carlberg et al 2001). …”

Section: Introductionmentioning

confidence: 99%

Do satellite galaxies trace matter in galaxy clusters?

Wang

Gao

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The spatial distribution of satellite galaxies encodes rich information of the structure and assembly history of galaxy clusters. In this paper, we select a redMaPPer cluster sample in SDSS Stripe 82 region with 0.1 ≤ z ≤ 0.33, 20 < λ < 100 and P cen > 0.7. Using the high-quality weak lensing data from CS82 Survey, we constrain the mass profile of this sample. Then we compare directly the mass density profile with the satellite number density profile. We find that the total mass and number density profiles have the same shape, both well fitted by an NFW profile. The scale radii agree with each other within 1σ error (r s,gal = 0.34 +0.04 −0.03 Mpc vs r s = 0.37 +0.15 −0.10 Mpc ).

show abstract

An X‐Ray and Optical Study of Matter Distribution in Clusters of Galaxies

Cited by 43 publications

References 31 publications

Entropy scaling in galaxy clusters: Insights from anXMM-Newtonobservation of the poor cluster A1983

Entropy scaling in galaxy clusters: Insights from anXMM-Newtonobservation of the poor cluster A1983

Chemical evolution of the intra-cluster medium

Do satellite galaxies trace matter in galaxy clusters?

Contact Info

Product

Resources

About