Combining Strong and Weak Gravitational Lensing in Abell 1689

Limousin, M.; Richard, Johan; Jullo, Eric; Kneib, Jean-Paul; Fort, B.; Soucail, G.; Elíasdóttir, Árdís; Natarajan, Priyamvada; Ellis, Richard S.; Smail, Ian; Czoske, O.; Smith, Graham P.; Hudelot, P.; Bardeau, S.; Ebeling, H.; Egami, Eiichi; Knudsen, K. K.

doi:10.1086/521293

Cited by 318 publications

(579 citation statements)

References 69 publications

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“…We also note that photometric redshifts based on upto five photometric bands are becoming more common as a method for selecting background galaxies (Limousin et al 2007; Gavazzi et al 2009;Gruen et al 2013;Applegate et al 2014;McCleary, dell'Antonio & Huwe 2015;Melchior et al 2015). However photometric redshifts based on a small number of filters are problematic for galaxies with blue observed colours because their spectral energy distribution is relatively featureless.…”

Section: Introductionmentioning

confidence: 92%

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LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

Self Cite

153

179

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We present weak-lensing mass measurements of 50 X-ray luminous galaxy clusters at 0.15 z 0.3, based on uniform high quality observations with Suprime-Cam mounted on the 8.2-m Subaru telescope. We pay close attention to possible systematic biases, aiming to control them at the ∼ < 4 per cent level. The dominant source of systematic bias in weak-lensing measurements of the mass of individual galaxy clusters is contamination of background galaxy catalogues by faint cluster and foreground galaxies. We extend our conservative method for selecting background galaxies with (V − i ′ ) colours redder than the red sequence of cluster members to use a colour-cut that depends on cluster-centric radius. This allows us to define background galaxy samples that suffer 1 per cent contamination, and comprise 13 galaxies per square arcminute. Thanks to the purity of our background galaxy catalogue, the largest systematic that we identify in our analysis is a shape measurement bias of 3 per cent, that we measure using simulations that probe weak shears upto g = 0.3. Our individual cluster mass and concentration measurements are in excellent agreement with predictions of the mass-concentration relation. Equally, our stacked shear profile is in excellent agreement with the Navarro Frenk and White profile. Our new LoCuSS mass measurements are consistent with the CCCP and CLASH surveys, and in tension with the Weighing the Giants at ∼ 1 − 2σ significance. Overall, the consensus at z 0.3 that is emerging from these complementary surveys represents important progress for cluster mass calibration, and augurs well for cluster cosmology.

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Section: Introductionmentioning

confidence: 92%

“…Broadhurst et al 2005;Limousin et al 2007). It is therefore of prime importance to make a secure selection of background galaxies.…”

Section: Introductionmentioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

Self Cite

153

179

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“…A1689 (z = 0.183) has the largest Einstein radius of all massive lensing clusters, θ E ∼ 50 . Broadhurst et al (2005) and Limousin et al (2007) performed a strong lensing analysis using HST data and identified 115 images of 34 multiply lensed background galaxies in the redshift range 1 < z < 5.5 based on spectroscopic and photometric redshift estimates. A cluster mass model of AC114 (z = 0.312, θ E ∼ 30 ) and several strongly lensed sources, including a 5-image configuration at z = 3.347 were presented in Campusano et al (2001).…”

Section: Clusters As Gravitational Telescopesmentioning

confidence: 99%

Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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Aims. Powerful gravitational telescopes in the form of massive galaxy clusters can be used to enhance the light collecting power over a limited field of view by about an order of magnitude in flux. This effect is exploited here to increase the depth of a survey for lensed supernovae at near-IR wavelengths. Methods. We present a pilot supernova search programme conducted with the ISAAC camera at VLT. Lensed galaxies behind the massive clusters A1689, A1835, and AC114 were observed for a total of 20 h divided into 2, 3, and 4 epochs respectively, separated by approximately one month to a limiting magnitude J < ∼ 24 (Vega). Image subtractions including another 20 h worth of archival ISAAC/VLT data were used to search for transients with lightcurve properties consistent with redshifted supernovae, both in the new and reference data. Results. The feasibility of finding lensed supernovae in our survey was investigated using synthetic lightcurves of supernovae and several models of the volumetric type Ia and core-collapse supernova rates as a function of redshift. We also estimate the number of supernova discoveries expected from the inferred star-formation rate in the observed galaxies. The methods consistently predict a Poisson mean value for the expected number of supernovae in the survey of between N SN = 0.8 and 1.6 for all supernova types, evenly distributed between core collapse and type Ia supernovae. One transient object was found behind A1689, 0.5 from a galaxy with photometric redshift z gal = 0.6 ± 0.15. The lightcurve and colors of the transient are consistent with being a reddened type IIP supernova at z SN = 0.59. The lensing model predicts 1.4 mag of magnification at the location of the transient, without which this object would not have been detected in the near-IR ground-based search described in this paper (unlensed magnitude J ∼ 25). We perform a feasibility study of the potential for lensed supernovae discoveries with larger and deeper surveys and conclude that the use of gravitational telescopes is a very exciting path for new discoveries. For example, a monthly rolling supernova search of a single very massive cluster with the HAWK-I camera at VLT would yield > ∼ 10 lensed supernova lightcurves per year, where type Ia supernovae would constitute about half of the expected sample. Conclusions.

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“…In particular, dwarfs and low surface-brightness galaxies suggest a much shallower profile with a relatively flat slope (α ≥ −0.5 with ρ(r) ∼ r α ) (Palunas & Williams 2000;Salucci & Burkert 2000;de Blok et al 2001;Swaters et al 2003;Gentile et al 2004;Spekkens et al 2005;Goerdt et al 2006;Walter et al 2008;Oh et al 2011;Walker & Peñarrubia 2011). On the other extreme of the halo mass scale, galaxy clusters tend to have a central cusp, as evidenced by studies combining strong and weak lensing (e.g., Limousin et al 2007;Leonard et al 2007; Umetsu et al 2007), but shallower slopes than the NFW one can also be found within the inner ≈ 5 kpc (Sand et al 2004;Sand et al 2008;Newman et al 2009;Newman et al 2011;Newman et al 2013;Richtler et al 2011). Note that a recent study found a cusp slope over 5 − 350 kpc of α = −1.62, again from combined weak and strong lensing analysis of the complete CLASH cluster sample (Zitrin et al 2015).…”

Section: Introductionmentioning

confidence: 98%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

144

141

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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Combining Strong and Weak Gravitational Lensing in Abell 1689

Cited by 318 publications

References 69 publications

LoCuSS: weak-lensing mass calibration of galaxy clusters

LoCuSS: weak-lensing mass calibration of galaxy clusters

Near-IR search for lensed supernovae behind galaxy clusters

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

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