Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data

Melchior, P.; Gruen, D.; McClintock, Thomas; Varga, T. N.; Sheldon, E.; Rozo, Eduardo; Amara, Adam; Becker, M. R.; Benson, B. A.; Bermeo, A.; Bridle, Sarah; Clampitt, Joseph; Dietrich, J. P.; Hartley, W. G.; Hollowood, D. L.; Jain, Bhuvnesh; Jarvis, Mike; Jeltema, T.; Kacprzak, T.; MacCrann, N.; Rykoff, E. S.; Saro, A.; Suchyta, E.; Troxel, M. A.; Zuntz, Joe; Bonnett, C.; Plazas, A. A.; Abbott, T. M. C.; Abdalla, F. B.; Annis, J.; Benoit-Lévy, A.; Bernstein, G. M.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; Desai, S.; Eifler, T. F.; Flaugher, B.; Fosalba, P.; García-Bellido, J.; Gaztañaga, E.; Gerdes, D. W.; Gruendl, R. A.; Gschwend, J.; Gutiérrez, G.; Honscheid, K.; James, D. J.; Kirk, D.; Krause, E.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Martini, Paul; Menanteau, F.; Miller, Christopher J.; Miquel, R.; Mohr, J. J.; Nichol, R. C.; Ogando, R. L. C.; Romer, A. K.; Sánchez, E.; Scarpine, V.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Swanson, M. E. C.; Tarlè, G.; Thomas, Daniel; Walker, A. R.; Weller, J.; Zhang, Y.

doi:10.1093/mnras/stx1053

Cited by 124 publications

(187 citation statements)

References 118 publications

(168 reference statements)

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“…The best fit parameters are listed in Table 1. We obtain a halo mass M 200 = 2.06 +0.61 −0.41 × 10 14 M that is consistent with the halo mass fitting result in Miyatake et al (2016), as well as the halo mass estimated by mass-richness relation in Melchior et al (2017) and Shan et al (2017) . To compare our measurements with the three-dimensional (3D) N-body simulation results directly, we correct the C 200 with the 3D correction in Giocoli et al (2012):…”

Section: Resultssupporting

confidence: 88%

Do satellite galaxies trace matter in galaxy clusters?

Wang

Gao

et al. 2018

Monthly Notices of the Royal Astronomical Society

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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 ).

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Section: Resultssupporting

confidence: 88%

Do satellite galaxies trace matter in galaxy clusters?

Wang

Gao

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Umetsu et al (2016) quantified unaccounted sources of systematic errors in the CLASH weak-lensing measurements by considering the following effects: (1) dilution of the weaklensing signal by residual contamination from cluster members (2.4%±0.7%), (2) photo-z bias in the mean depth estimates (0.27%; Section 3.2), and (3) shear calibration uncertainty (5%; Section 3.3.2). These errors add up to 5.6% in quadrature, which is translated into the cluster mass uncertainty as 5.6%/Γ;7%, with Γ;0.75 the typical value of the logarithmic derivative of the weak-lensing signal with respect to cluster mass (Melchior et al 2017).…”

Section: Systematic Errorsmentioning

confidence: 99%

“…Gravitational lensing offers a direct probe of the cluster mass distribution through observations of weak shear lensing (e.g., Gruen et al 2014;von der Linden et al 2014;Hoekstra et al 2015;Melchior et al 2017;Sereno et al 2017a;Medezinski et al 2018), weak magnification lensing (e.g., Hildebrandt et al 2011;Umetsu et al 2011b;Coupon et al 2013;Chiu et al 2016;Tudorica et al 2017), strong gravitational lensing (e.g., Broadhurst et al 2005a;Zitrin et al 2013;Jauzac et al 2015;Cerny et al 2017;Diego et al 2018), and the combination of these effects (e.g., Umetsu et al 2011a;Coe et al 2012;Medezinski et al 2013;Umetsu et al 2015Umetsu et al , 2016. The critical advantage of gravitational lensing is its unique ability to map the mass distribution independently of assumptions about their physical or dynamical state.…”

Section: Introductionmentioning

confidence: 99%

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Umetsu

Sereno

Tam

et al. 2018

ApJ

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We reconstruct the two-dimensional (2D) matter distributions in 20 high-mass galaxy clusters selected from the CLASH survey by using the new approach of performing a joint weak gravitational lensing analysis of 2D shear and azimuthally averaged magnification measurements. This combination allows for a complete analysis of the field, effectively breaking the mass-sheet degeneracy. In a Bayesian framework, we simultaneously constrain the mass profile and morphology of each individual cluster, assuming an elliptical Navarro-Frenk-White halo characterized by the mass, concentration, projected axis ratio, and position angle (PA) of the projected major axis. We find that spherical mass estimates of the clusters from azimuthally averaged weak-lensing measurements in previous work are in excellent agreement with our results from a full 2D analysis. Combining all 20 clusters in our sample, we detect the elliptical shape of weak-lensing halos at the 5σ significance level within a scale of 2 h Mpc 1 -. The median projected axis ratio is 0.67±0.07 at a virial mass of M M 15.2 2.8 10 vir 14 = ´ ( ) , which is in agreement with theoretical predictions from recent numerical simulations of the standard collisionless cold dark matter model. We also study misalignment statistics of the brightest cluster galaxy, X-ray, thermal Sunyaev-Zel'dovich effect, and strong-lensing morphologies with respect to the weak-lensing signal. Among the three baryonic tracers studied here, we find that the X-ray morphology is best aligned with the weak-lensing mass distribution, with a median misalignment angle of PA 21We also conduct a stacked quadrupole shear analysis of the 20 clusters assuming that the X-ray major axis is aligned with that of the projected mass distribution. This yields a consistent axis ratio of 0.67±0.10, suggesting again a tight alignment between the intracluster gas and dark matter.

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“…Many authors have argued that, when a limited number of filters are used in source selection by removing red-sequence galaxies, one of the important systematic errors is the contamination by faint blue cluster members (e.g., Broadhurst et al 2005;Okabe et al 2010;Applegate et al 2014;Melchior et al 2017). Recently, Medezinski et al (2017) suggested that the blue cluster member contamination is not only limited to the cluster central region, but also to outskirts and will thus impact determinations of both mass and concentration.…”

Section: Cluster Member Contaminationmentioning

confidence: 99%

First Weak-lensing Results from “See Change”: Quantifying Dark Matter in the Two z ≳ 1.5 High-redshift Galaxy Clusters SPT-CL J2040–4451 and IDCS J1426+3508

Jee

Perlmutter

et al. 2017

ApJ

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We present a weak-lensing study of SPT-CL J2040-4451 and IDCS J1426+3508 at z = 1.48 and 1.75, respectively. The two clusters were observed in our "See Change" program, a Hubble Space Telescope (HST) survey of 12 massive high-redshift clusters aimed at high-z supernova measurements and weak-lensing estimation of accurate cluster masses. We detect weak but significant galaxy shape distortions using infrared images from the Wide Field Camera 3 (WFC3), which has not yet been used for weak-lensing studies. Both clusters appear to possess relaxed morphology in projected mass distribution, and their mass centroids agree nicely with those defined by both the galaxy luminosity and X-ray emission. Using a Navarro-Frenk-White profile, for which we assume that the mass is tightly correlated with the concentration parameter, we determine the masses of SPT-CL J2040-4451 and IDCS J1426+3508 to be M 200 = 8.6+1.7 −1.4 × 10 14 M and 2.2 +1.1 −0.7 × 10 14 M , respectively. The weak-lensing mass of SPT-CL J2040-4451 shows that the cluster is clearly a rare object. Adopting the central value, the expected abundance of such a massive cluster at z 1.48 is only ∼0.07 in the parent 2500 sq. deg. survey. However, it is yet premature to claim that the presence of this cluster creates a serious tension with the current ΛCDM paradigm unless that tension will remain in future studies after marginalizing over many sources of uncertainties such as the accuracy of the mass function and the mass-concentration relation at the high mass end. The mass of IDCS J1426+3508 is in excellent agreement with our previous Advanced Camera for Surveys-based weak-lensing result while the much higher source density from our WFC3 imaging data makes the current statistical uncertainty ∼40% smaller.

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Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data

Cited by 124 publications

References 118 publications

Do satellite galaxies trace matter in galaxy clusters?

Do satellite galaxies trace matter in galaxy clusters?

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

First Weak-lensing Results from “See Change”: Quantifying Dark Matter in the Two z ≳ 1.5 High-redshift Galaxy Clusters SPT-CL J2040–4451 and IDCS J1426+3508

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