Statistical properties of SZ and X-ray cluster detections

Pace, Francesco; Maturi, M.; Bartelmann, Matthias; Cappelluti, N.; Dolag, K.; Meneghetti, M.; Moscardini, L.

doi:10.1051/0004-6361:200809550

Cited by 13 publications

(20 citation statements)

References 54 publications

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“…Pace et al (2008) found that ACT could detect tSZ halos down to 6 × 10 13 h −1 M fairly independent of redshift, whereas we have found that these halos become hard to detect at higher redshifts. The analysis of Pace et al (2008) only included the CMB as a foreground, so it is conceivable that the inclusion of point source foregrounds would degrade their forecasts for low-mass halos at high redshift, as we have found to be the case in our analysis. We also note that the analysis of Malte Schäfer & Bartelmann (2007) found that PLANCK could detect halos of mass 6 × 10 13 M h −1 below z = 0.1 when they included the CMB and all galactic foregrounds.…”

Section: Discussioncontrasting

confidence: 54%

“…Prospects for detection of tSZ clusters have been studied previously in the case of PLANCK (Malte Schäfer & Bartelmann 2007;Melin et al 2006), ACT (Pace et al 2008;Sehgal et al 2007), and SPT (Melin et al 2006), but these studies have mainly focused on the statistics of tSZ detections above the mass completeness limit of the respective surveys. Pace et al (2008) found that ACT could detect tSZ halos down to 6 × 10 13 h −1 M fairly independent of redshift, whereas we have found that these halos become hard to detect at higher redshifts.…”

Section: Discussionmentioning

confidence: 99%

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Detection of Hot Gas in Galaxy Groups via the Thermal Sunyaev-Zel'dovich Effect

Moodley

Warne

Goheer

et al. 2009

ApJ

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Motivated by the observed shortfall of baryons in the local universe, we investigate the ability of highresolution cosmic microwave background (CMB) experiments to detect hot gas in the outer regions of nearby group halos. We construct hot gas models with the gas in hydrostatic equilibrium with the dark matter and described by a polytropic equation of state. We also consider models that add entropy to the gas in line with constraints from X-ray observations. We calculate the thermal Sunyaev-Zel'dovich (tSZ) signal in these halos and compare it to the anticipated sensitivities of forthcoming tSZ survey experiments such as Antenna Cosmology Telescope, PLANCK, and South Pole Telescope. Using a multifrequency Wiener filter we derive tSZ detectability limits as a function of halo mass and redshift in the presence of galactic and extragalactic foregrounds and the CMB. We find that group-sized halos with virial masses below 10 14 M can be detected at z 0.05 with the threshold mass dropping to (3-4) × 10 13 M at z 0.01. The tSZ distortion of nearby group-sized halos can thus be mapped out to the virial radius by these CMB experiments, beyond the sensitivity limits of X-ray observations. These measurements will provide a unique probe of hot gas in the outer regions of group halos, shedding insight into the local census of baryons and the injection of entropy into the intragroup medium from nongravitational feedback.

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Section: Discussioncontrasting

confidence: 54%

Section: Discussionmentioning

confidence: 99%

Detection of Hot Gas in Galaxy Groups via the Thermal Sunyaev-Zel'dovich Effect

Moodley

Warne

Goheer

et al. 2009

ApJ

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“…Our method belongs to the matched filters developed for cosmic microwave background (CMB) observations (e.g. Schäfer et al 2006; Pace et al 2008) which use at once all available bands to obtain a unique response. With this respect, the algorithm presented here is a special case where a single band is considered, but could be naturally extended to include the full available colour information.…”

Section: Optimal Filter For Galaxy Overdensitiesmentioning

confidence: 99%

Optimal filtering of optical and weak lensing data to search for galaxy clusters: application to the COSMOS field

Bellagamba¹,

Maturi²,

Hamana³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal‐to‐noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi‐band approach which could include not only additional optical bands but also observables with different nature such as X‐rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo‐z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3σ level including both optical and weak‐lensing information.

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“…Optimal Filtering is a general technique to extract and measure an expected signal in a data-set affected by a noisy background. In astronomy, it was originally applied to weak lensing detection of galaxy clusters by Maturi et al (2005) and Pace et al (2007), and to X-ray and SZ detections in Pace et al (2008). In Bellagamba et al (2011), it was shown that in case of photometric detections, if one assumes that the background is homogeneous, the Optimal Filter actually corresponds to a Matched Filter.…”

Section: Introductionmentioning

confidence: 99%

AMICO: optimized detection of galaxy clusters in photometric surveys

Bellagamba

Roncarelli

Maturi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present AMICO (Adaptive Matched Identifier of Clustered Objects), a new algorithm for the detection of galaxy clusters in photometric surveys. AMICO is based on the Optimal Filtering technique, which allows to maximise the signal-to-noise ratio of the clusters. In this work we focus on the new iterative approach to the extraction of cluster candidates from the map produced by the filter. In particular, we provide a definition of membership probability for the galaxies close to any cluster candidate, which allows us to remove its imprint from the map, allowing the detection of smaller structures. As demonstrated in our tests, this method allows the deblending of closeby and aligned structures in more than 50% of the cases for objects at radial distance equal to 0.5 × R 200 or redshift distance equal to 2 × σ z , being σ z the typical uncertainty of photometric redshifts. Running AMICO on mocks derived from N-body simulations and semi-analytical modelling of the galaxy evolution, we obtain a consistent massamplitude relation through the redshift range 0.3 < z < 1, with a logarithmic slope ∼ 0.55 and a logarithmic scatter ∼ 0.14. The fraction of false detections is steeply decreasing with S/N, and negligible at S/N > 5.

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Statistical properties of SZ and X-ray cluster detections

Cited by 13 publications

References 54 publications

Detection of Hot Gas in Galaxy Groups via the Thermal Sunyaev-Zel'dovich Effect

Detection of Hot Gas in Galaxy Groups via the Thermal Sunyaev-Zel'dovich Effect

Optimal filtering of optical and weak lensing data to search for galaxy clusters: application to the COSMOS field

AMICO: optimized detection of galaxy clusters in photometric surveys

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