Next-generation X-ray cluster surveys

Slack, N. W.; Ponman, T. J.

doi:10.1093/mnras/stt2280

Cited by 3 publications

(6 citation statements)

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“…This relation, which has a self-similar expectation of L X ∝ T 2 for systems with temperatures above ∼3 keV, and a flatter slope at lower temperatures (L X ∝ T; Balogh, Babul & Patton 1999) where line emission is significant, has been shown to be significantly steeper, especially in the group regime (e.g. Helsdon & Ponman 2000;Osmond & Ponman 2004;Pratt et al 2009;Slack & Ponman 2014), with slopes of 3 to 4. This similarity breaking is attributed to feedback processes that inject entropy into the gas halo (e.g.…”

Section: X -T Specmentioning

confidence: 61%

“…2, we show our group sample overplotted on the L-T group data from the GEMS sample of Osmond & Ponman (2004). Also shown is the L-T relation (for groups only) found by Slack & Ponman (2014) using a compilation of several group and cluster studies spanning nearly two orders of magnitude in temperature:…”

Section: X -T Specmentioning

confidence: 99%

“…Overlaid are groups from theOsmond & Ponman (2004) sample (black points). The solid line represents the L-T relation ofSlack & Ponman (2014). We show the L-T relation of our sample, modified from theSlack & Ponman (2014) relation by re-fitting the normalization only, excluding the undetected groups 100053 and 200099, as the dashed line.…”

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confidence: 99%

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Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

Pearson

Ponman

Norberg

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Section: X -T Specmentioning

confidence: 61%

Section: X -T Specmentioning

confidence: 99%

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Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

Pearson

Ponman

Norberg

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The resulting values of M500 were then used to predict r500 radii, assuming a mean density 500 times the critical density of the Universe at the group's redshift, and the X-ray temperatures for each potential target group using the masstemperature relation of Sun et al (2009). These temperatures were then used to estimate X-ray luminosities using the LX − T relation derived by Slack & Ponman (2014) for archival data. As we are interested in high entropy groups, we would expect these groups to be underluminous relative to the typical group population.…”

Section: Group Samplementioning

confidence: 99%

Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

Pearson,

Ponman,

Norberg

et al. 2017

Preprint

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Observations with the Chandra X-ray Observatory are used to examine the hot gas properties within a sample of 10 galaxy groups selected from the Galaxy And Mass Assembly survey's optical friends-of-friends group catalogue. Our groups have been screened to eliminate spurious and unrelaxed systems, and the effectiveness of this procedure is demonstrated by the detection of intergalactic hot gas in 80 per cent of our sample. However we find that 9 of the 10 are X-ray underluminous by a mean factor ∼ 4 compared to typical X-ray selected samples. Consistent with this, the majority of our groups have gas fractions which are lower and gas entropies somewhat higher than those seen in typical X-ray selected samples. Two groups, which have high 2σ lower limits on their gas entropy, are candidates for the population of high entropy groups predicted by some AGN feedback models.

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“…We searched all fields for sources using a source searching algorithm based on the Voronoi tessellation algorithm implemented in CIAO. All detected sources were tested for extension using a Bayesian extension test developed by Slack & Ponman (2014) which checks for a significant difference in fit statistic between a point source model and a beta model blurred with the point spread function. Our final candidate list includes only extended sources with at least 100 counts in the soft band (0.5-2.0 keV).…”

Section: Sample Selection and Data Reductionmentioning

confidence: 99%

The Chandra Deep Group Survey – cool core evolution in groups and clusters of galaxies

Pascut

Ponman

2015

Monthly Notices of the Royal Astronomical Society

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We report the results of a study which assembles deep observations with the ACIS-I instrument on the Chandra Observatory to study the evolution in the core properties of a sample of galaxy groups and clusters out to redshifts z ≈ 1.3. A search for extended objects within these fields yields a total of 62 systems for which redshifts are available, and we added a further 24 non-X-ray-selected clusters, to investigate the impact of selection effects and improve our statistics at high redshift. Six different estimators of cool core strength are applied to these data: the entropy (K) and cooling time (t cool ) within the cluster core, the cooling time as a fraction of the age of the Universe (t cool /t Uni ), and three estimators based on the cuspiness of the X-ray surface brightness profile. A variety of statistical tests are used to quantify evolutionary trends in these cool core indicators. In agreement with some previous studies, we find that there is significant evolution in t cool /t Uni , but little evolution in t cool , suggesting that gas is accumulating within the core, but that the cooling time deep in the core is controlled by AGN feedback. We show that this result extends down to the group regime and appears to be robust against a variety of selection biases (detection bias, archival biases and biases due to the presence of central X-ray AGN) which we consider. Recent results (Semler et al. 2012;McDonald et al. 2013) based on samples of clusters selected by the Sunyaev-Zeldovich (SZ) effect, with Chandra follow-up, demonstrate that CC clusters do exist at redshifts greater than 0.5. Moreover, McDonald et al. (2013) found that there is no evolution in central cooling time out to redshifts ∼ 1. There are also studies on individual clusters, although not very numerous, which show that there are strong cool cores at high redshift. The WARPS cluster studied by Santos et al. (2012) is a CC cluster at redshift 1.03. Another interesting system is 3C188, studied by Siemiginowska et al. (2010), which is a strong CC system at z=1.03 with a powerful radio AGN at its centre. Signs of cooling at the centre of the cluster surrounding the z = 1.04 powerful quasar PKS1229-021 have also been reported by Russell et al. (2012).While most of these evolutionary studies have concentrated on rich clusters, and show a reduction in the incidence of strong CCs at

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Next-generation X-ray cluster surveys

Cited by 3 publications

References 48 publications

Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups

The Chandra Deep Group Survey – cool core evolution in groups and clusters of galaxies

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