Competition between shocks and entropy floor: Unifying groups and clusters of galaxies

Santos, S. Dos; Doré, O.

doi:10.1051/0004-6361:20011750

Cited by 40 publications

(49 citation statements)

References 56 publications

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“…This behaviour becomes even more noticeable for verylow temperature (kT < 1 keV) systems (Helsdon & Ponman 2000a;Mulchaey 2000;Xue & Wu 2000) where the departures from the self-similar scaling laws traced for galaxy clusters have been explained by models of pre-heating of the gas before it falls into the group (Cavaliere et al 1997;Ponman et al 1999;Balogh et al 1999;Dos Santos & Doré 2002).…”

Section: Introductionmentioning

confidence: 94%

The detection of diffuse emission in HCG 16 with XMM-Newton

Belsole¹,

Sauvageot²,

Ponman³

et al. 2003

A&A

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Abstract.We report results obtained from analysis of the XMM-Newton observation of the compact group of galaxies HCG 16. It is a peculiar system composed of 7 spirals, 6 of which are active, and its nature as a bound system has been much debated. The EPIC camera observations give new insights into the X-ray parameters describing the physical status of the group. We detect diffuse X-ray emission with a rather elliptical morphology which extends to at least a radius of 135 h −1 50 kpc from the group centre. The spectrum within this region is well modelled by a thermal plasma with a temperature of 0.49 ± 0.17 keV, and a non-zero metallicity. We measure a bolometric X-ray luminosity of 9.6×10 40 h −2 50 erg s −1 which may be only a small fraction of the total luminosity because of the limit in spatial detection arising from the high background level. Despite its low temperature and luminosity, HCG 16 obeys the L X − T relation obtained for brighter galaxy groups even if it lies in a very extreme position. The properties of the diffuse emission confirm the bound nature of HCG 16 even if the gas trapped in the potential well may not yet be virialized. This reopens the debate about the real nature of spiral-dominated galaxy groups, and on their role in a more general cosmological context.

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Section: Introductionmentioning

confidence: 94%

The detection of diffuse emission in HCG 16 with XMM-Newton

Belsole¹,

Sauvageot²,

Ponman³

et al. 2003

A&A

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“…Recent work has explored the SZ-mass relation using numerical simulations (e.g., Oh & Benson 2003;da Silva et al 2004;Motl et al 2005;Nagai 2005) and analytical approximations (e.g., Dos Santos & Doré 2001;Reid & Spergel 2006;Roychowdhury et al 2005;Ostriker et al 2005). Numerical models find that the SZ-mass relation is expected to be very tight, implying that cluster masses can be directly read out from the SZ observations once the SZ-mass relation has been calibrated.…”

Section: Sz Cluster Scaling Relationsmentioning

confidence: 99%

LSST Science Book, Version 2.0

Abell¹,

Burke²,

Hamuy³

et al. 2009

542

650

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Prepared by the LSST Science Collaborations, with contributions from the LSST Project. PrefaceMajor advances in our understanding of the Universe over the history of astronomy have often arisen from dramatic improvements in our ability to observe the sky to greater depth, in previously unexplored wavebands, with higher precision, or with improved spatial, spectral, or temporal resolution. Aided by rapid progress in information technology, current sky surveys are again changing the way we view and study the Universe, and the next-generation instruments, and the surveys that will be made with them, will maintain this revolutionary progress. Substantial progress in the important scientific problems of the next decade (determining the nature of dark energy and dark matter, studying the evolution of galaxies and the structure of our own Milky Way, opening up the time domain to discover faint variable objects, and mapping both the inner and outer Solar System) all require wide-field repeated deep imaging of the sky in optical bands.The wide-fast-deep science requirement leads to a single wide-field telescope and camera which can repeatedly survey the sky with deep short exposures. The Large Synoptic Survey Telescope (LSST), a dedicated telecope with an effective aperture of 6.7 meters and a field of view of 9.6 deg 2 , will make major contributions to all these scientific areas and more. It will carry out a survey of 20,000 deg 2 of the sky in six broad photometric bands, imaging each region of sky roughly 2000 times (1000 pairs of back-to-back 15-sec exposures) over a ten-year survey lifetime.The LSST project will deliver fully calibrated survey data to the United States scientific community and the public with no proprietary period. Near real-time alerts for transients will also be provided worldwide. A goal is worldwide participation in all data products. The survey will enable comprehensive exploration of the Solar System beyond the Kuiper Belt, new understanding of the structure of our Galaxy and that of the Local Group, and vast opportunities in cosmology and galaxy evolution using data for billions of distant galaxies. Since many of these science programs will involve the use of the world's largest non-proprietary database, a key goal is maximizing the usability of the data. Experience with previous surveys is that often their most exciting scientific results were unanticipated at the time that the survey was designed; we fully expect this to be the case for the LSST as well.The purpose of this Science Book is to examine and document in detail science goals, opportunities, and capabilities that will be provided by the LSST. The book addresses key questions that will be confronted by the LSST survey, and it poses new questions to be addressed by future study. It contains previously available material (including a number of White Papers submitted to the ASTRO2010 Decadal Survey) as well as new results from a year-long campaign of study and evaluation. This book does not attempt to be complete; there are many ...

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“…Cavaliere et al (1999) developed a model in which hierarchical clustering and thus in-fall from substructures was taken into account. Tozzi & Norman (2001) and Dos Santos & Doré (2002) looked at the effects of an initial background entropy level and shock heating. More recent models based on simulations integrate galaxy feedback and radiative cooling Kay 2004;Muanwong et al 2002).…”

Section: Entropy In the Cluster Centersmentioning

confidence: 99%

Tracing the X-ray emitting intra-cluster medium of clusters of galaxies beyondr$\mathsf{_{200}}$

Neumann

2005

A&A

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Abstract. We present in this paper a study of a sample of 14 nearby clusters of galaxies (0.06 < z < 0.1) observed with the ROSAT/PSPC. We only select clusters with low galactic absorption (nH ≤ 6 × 10 20 cm −2 ) in order to trace the hot X-ray emitting intra-cluster medium (ICM) out to large radii. We convert the X-ray surface brightness profiles of the clusters into emission measure profiles scaled to the classical scaling relations based on the spherical collapse model. We sort the clusters into different temperature bins and stack the scaled emission measure (ScEM) profiles of clusters belonging to the same bin together. This method enhances the statistics of the profiles -especially in outer regions. The stacked profiles allow us to observe a signal out to radii r > r 200 . In the center (r < 0.4r 200 ) we find that the ScEM profiles deviate from predicted scaling laws. Hotter clusters have systematically a higher ScEM than cooler clusters. This result is in very good agreement with current studies on the L X − T relation and the entropy-temperature relation (S ∝ T 0.65 ) found recently. At radii r > 0.4r 200 we find that the ScEM profiles agree well within the error bars, suggesting self-similarity. Fitting beta-models to the overall ScEM profiles, we find for the different subsamples r c = 0.15−0.18r 200 and β = 0.8, which is higher than the canonical value of β = 2/3 often found. The beta-model is generally a better representation for hotter than for cooler clusters. We see indications for continuous steepening of the profiles with increasing radius: at radii r > 0.8r 200 the profiles are systematically below the beta-model curve with β = 0.8. We discuss our results with respect to the observed X-ray luminosity L X − T relation, the gas mass M gas − T relation and the total mass M − T relation. We also address implications on the origin of the observed S − T relation. Furthermore, we discuss the observed steepness of the X-ray profiles, which falls off more rapidly than predicted from the NFW-profile for cold dark matter halos.

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Competition between shocks and entropy floor: Unifying groups and clusters of galaxies

Cited by 40 publications

References 56 publications

The detection of diffuse emission in HCG 16 with XMM-Newton

The detection of diffuse emission in HCG 16 with XMM-Newton

LSST Science Book, Version 2.0

Tracing the X-ray emitting intra-cluster medium of clusters of galaxies beyondr$\mathsf{_{200}}$

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