The Concentration-Mass relation from CLASH

Transcription

1 The Concentration-Mass relation from CLASH Snowcluster 2015 Snowbird March 16, 2015 Julian Merten Marie Curie Fellow University of Oxford

2 The CLASH One of three HST/MCT programs ~550 orbits Science Drivers To map the DM profile and substructure to unprecedented precision To detect SN 1a out to z ~ 2.5 To detect and analyse galaxies out to z > 7 To study the structure and evolution of galaxies in and behind the clusters

3 The CLASH One of three HST/MCT programs ~550 orbits Science Drivers To map the DM profile and substructure to unprecedented precision To detect SN 1a out to z ~ 2.5 To detect and analyse galaxies out to z > 7 To study the structure and evolution of galaxies in and behind the clusters

4 Collaborators (this work) Matthias Bartelmann / ITA Heidelberg Dan Coe / STScI Megan Donahue / MSU Anton Koekemoer / STScI Elinor Medezinski / JHU Peter Melchior / OSU Massimo Meneghetti / JPL & INAF Bologna Leonidas Moustakas / JPL Mario Nonino / INAF Trieste Marc Postman / STScI Keiichi Umtesu / ASIAA Adi Zitrin / Caltech

5 CLASH observations HST 524 orbits: 25 clusters, each imaged in 16 passbands. ( μm) ~20 orbits per cluster. CLASH observations are complete - Last HST images were taken July Chandra+XMM x-ray archival data +some new proposals (0.5 7 kev) Spitzer Space Telescope archival and new cycle 8 data (3.6, 4.5 μm) SZE observations (Bolocam, Mustang) to augment existing data (sub-mm) Subaru/Suprime-Cam wide-field imaging ( μm), mostly 5 at least 3 bands VLT, LBT, Magellan, MMT, Palomar Spectra

6 The dark matter density profile A(r) = A s r rs ( 1+ r rs )2 typical characterizations: r_2500 (SL, SZ) r_500 (X-ray) r_200 (WL) r_vir ( Theory ) M(r) =4πA s r 3 s c = r rs ln (1 + x) x = r r s x 1+x

7 The dark matter density profile A(r) = A s r rs ( 1+ r rs )2 typical characterizations: r_2500 (SL, SZ) r_500 (X-ray) r_200 (WL) r_vir ( Theory ) M(r) =4πA s r 3 s c = r rs Postman & CLASH 2012 ln (1 + x) x = r r s x 1+x

8 CLASH selection 0.2 < z < 0.9 Tx > 5 kev X - BCG separation < 20kpc Regular X-ray morphology Postman & CLASH 2012

9 CLASH selection 0.2 < z < 0.9 Tx > 5 kev X - BCG separation < 20kpc Regular X-ray morphology Postman & CLASH 2012

10 CLASH strong lensing Example: MACS J 1206 cyan: pre-clash green: post-clash Redshifts from literature + CLASH spec., or 16-band photo-zs Identifications for all CLASH clusters now Zitrin & CLASH 2014 Multiple image system identification using Zitrin 2009

11 CLASH Subaru weak lensing Umetsu KSB+ pipeline Medezinski CCselection Umetsu & CLASH 2012/14, Medezinski & CLASH 2014

12 CLASH HST weak lensing special ACS WL reductions single visit, detector frame CTI corrected by STScI RRG pipeline for shape measurement Background selection from 16-band photo-zs Medezinski & CLASH 2014, JM & CLASH 2014, Zitrin & CLASH 2014

13 Why all this?

14 Why all this?

15 CLASH reconstructions SaWLens implements WL and SL operates on adaptively refined grids (AMR) Subaru WL HST WL HST SL non-parametric method, this means that we make no assumptions on the lens mass profile JM et al. 2009

16 CLASH reconstructions SaWLens implements WL and SL operates on adaptively refined grids (AMR) Subaru WL HST WL HST SL non-parametric method, this means that we make no assumptions on the lens mass profile JM et al. 2009

17 CLASH reconstructions SaWLens implements WL and SL operates on adaptively refined grids (AMR) Subaru WL HST WL HST SL non-parametric method, this means that we make no assumptions on the lens mass profile JM et al. 2009

18 CLASH profiles JM & CLASH 2014 ( ) 11_fit_cov

19 CLASH profiles JM & CLASH 2014 ( ) 11_fit_cov

20 Test Facility: SkyLens with Massimo Meneghetti Realistic lensing scenario via raytracing HUDF through hydro simulations Treat output CCD images as real data and use your favourite pipeline Meneghetti, Rasia, JM et al 2010

21 Test Facility: SkyLens with Massimo Meneghetti Realistic lensing scenario via raytracing HUDF through hydro simulations Treat output CCD images as real data and use your favourite pipeline Meneghetti, Rasia, JM et al 2010

22 SaWLens Test: Sims 3 simulated clusters, 3 projections each Meneghetti, Rasia, JM 2010

23 SaWLens Test: Sims 3 simulated clusters, 3 projections each Meneghetti, Rasia, JM 2010

24 SaWLens Test: Sims 3 simulated clusters, 3 projections each Meneghetti, Rasia, JM 2010

25 SaWLens Test: Sims 3 simulated clusters, 3 projections each Meneghetti, Rasia, JM 2010

26 SaWLens Test: Lensed SNe MACS J news/heic1409/

27 SaWLens Test: Lensed SNe MACS J news/heic1409/

28 SaWLens Test: Lensed SNe RX J1532 Abell news/heic1409/

29 Lensed SNe We found 3 lensed supernovae behind CLASH clusters Two of them are of standardisable Type 1a + multi-colour light-curves: Car: 1.0 +/- 0.2 mag Did: 0.2 +/- 0.2 mag gravitational lensing: Car: / mag Did: / mag Patel, Iha, Rodney, Riess, JM et al see also: Nordin, Atek, Perlmutter et al. 2014

30 Lensed SNe We found 3 lensed supernovae behind CLASH clusters Lens Model Prediction Lens Model Prediction Two of them are of standardisable Type 1a + multi-colour light-curves: Car: 1.0 +/- 0.2 mag Did: 0.2 +/- 0.2 mag gravitational lensing: Car: / mag Did: / mag Patel, Iha, Rodney, Riess, JM et al see also: Nordin, Atek, Perlmutter et al. 2014

31 SNe+lensing continues Kelly et al. (2015) Science Rodney et al. (2015) in prep.

32 c-m and CLASH A = / (amplitude) B = / (redshift) C = / (mass) JM & CLASH 2014 ( ) Umetsu & CLASH 2014 ( )

33 c-m and CLASH A = / (amplitude) B = / (redshift) C = / (mass) Umetsu & CLASH 2014 JM & CLASH 2014 ( ) Umetsu & CLASH 2014 ( )

34 Literature comparison <c_obs/c_sim> 1.31 [ ] 1.16 [ ] JM & CLASH 2014 ( )

35 CLASH simulations MUSIC-2, 1500 re-simulated halos out of the 1 Gpc MultiDark box, 2x10^ x10^15 M_sol, 6 redshifts. Meneghetti & CLASH 2014 ( ) Full control over analysis technique and selection Analysis in 2D <-- --> X-ray selecting CLASH

36 Tailored comparison <c_obs/c_sim> 0.96 [ ] JM & CLASH 2014 ( )

37 Conclusions CLASH was in part designed to answer open questions regarding the density profile of clusters from observations CLASH combines lensing constraints in three different regimes to probe the full range of relevant scales CLASH and lensed Supernovae are a most recent way to understand the robustness of our models CLASH cluster mass profiles show good agreement with LCDM simulations once the selection function is controlled