CFHT STRIPE82 SURVEY (CS82)

Transcription

1 CFHT STRIPE82 SURVEY (CS82) 160 degrees (130 effective) i=24.1, AB mag, 5σ, 2 aperture Seeing ~ 0.6 over full survey Pixel size : Alexie Leauthaud. Jean-Paul Kneib. Martin Makler. Ludovic van Waerbeke. + CS82 collboration

2 CS82 IN A NUTSHELL 171 Megacam pointing (1 sq. degree) Mostly between -40<RA<45-1<DEC<+1 30 min observations, 4x410 sec I-band depth ~ 23.5 for galaxies ~24 point sources Service mode : seeing < 0.8. Mean seeing 0.6 Lensing catalog = based on CFHTLS pipeline CS82 seeing SEEING Mag_auto MAG_AUTO

3 SCIENCE GOALS Weak lensing! Galaxy-galaxy lensing (e.g BOSS galaxies, z~0.55) Mass maps - cross-correlations (e.g. with CMB/ACT) Strong lensing Cluster science Galaxy sizes, morphology, BCGs + combinations with other wavelengths your cool idea here!

4 OUR SISTER PROJECT: VICS82 DEC S82m36p S82m39m S82m35p S82m38m S82m34p S82m37m S82m33p S82m32p S82m31p S82m30p S82m29p S82m28p S82m36m S82m35m S82m34m S82m33m S82m32m S82m31m S82m30m S82m27p S82m29m S82m28m S82m27m S82m26p S82m26m S82m25p S82m25m S82m24p W4m1m1 W4m1m2 W4m0m1 W4m0m2 W4p1m1 W4p1m2 W4p2m1 W4p2m2 S82m23p S82m24m S82m22p S82m23m S82m21p S82m22m S82m20p S82m21m S82m19p S82m18p S82m17p S82m16p S82m15p S82m14p S82m18m S82m17m S82m16m S82m15m S82m14m S82m13p S82m13m S82m12p S82m12m S82m11p S82m11m S82m10m S82m8p S82m9m S82m8m S82m7m S82m7p S82m6m S82m5p S82m4p S82m3p S82m5m S82m4m S82m3m S82m2m S82m2p S82m1m S82m1p S82m0p S82m0m RA CS82 DEC S82p0p S82p0m S82p1p S82p2p S82p3p S82p4p S82p5p S82p6p S82p7p S82p8p S82p9p S82p10p S82p11p S82p12p S82p13p S82p14p S82p15p S82p16p S82p17p S82p18p S82p19p S82p20p S82p21p S82p22p S82p1m S82p2m S82p3m S82p4m S82p5m S82p6m S82p7m S82p8m S82p9m S82p10m S82p11m S82p12m S82p13m S82p14m S82p15m S82p16m S82p17m S82p18m S82p19m S82p23p S82p24p S82p25p S82p26p S82p27p S82p28p S82p29p S82p30p S82p31p S82p32p S82p33p S82p34p S82p20m S82p21m S82p22m S82p23m S82p24m S82p25m S82p26m S82p27m S82p28m S82p29m S82p35p S82p36p S82p37p S82p38p S82p39p S82p30m S82p31m S82p32m S82p33m S82p34m S82p40p S82p35m S82p41p S82p42p S82p43p S82p36m S82p37m S82p38m S82p39m S82p44p S82p45p S82p46p S82p47p S82p48p S82p40m S82p41m S82p42m S82p43m RA VICS82 / J + K VISTA previous talk by Martin Makler WIRCAM

5 A FEW TASTY TIDBITS

6 SEXTRACTOR V.2 PROFILE FITTING +PSFEX 2D model fitting of stars and galaxies. de Vaucouleurs, Sersic, Exponential. + Improved star/galaxy classifier ( spread model ) Residuals: exponential profile CS82 Morphology Catalog Mores et al in prep, Charbonnier et al. in prep - 16 million objects - 4 profiles (de Vauc. Exp. Sersic. DeVauc+ exp) Eles x 4 profiles. 12h/profile/Ele Aldée Charbonnier. Bruno Moraes. Martin Makler. CS83 collab.

7 SEXTRACTOR V.2 PROFILE FITTING +PSFEX SDSS DR9 Galaxies with S/N > 5 & fracdev_i < 0.02 matching area of 14 sq. degrees Good agreement for MAG < Aldée Charbonnier. Bruno Moraes. Martin Makler. CS83 collab.

8 FORCED PHOTOMETRY ON STRIPE 82 SDSS DATA USING TRACTOR Model fixed from CS82 i-band image 0.6 seeing = truth Dustin Lang and CS82

9 FORCED PHOTOMETRY ON STRIPE 82 SDSS DATA USING TRACTOR Dustin Lang and CS82

10 FORCED PHOTOMETRY ON STRIPE 82 SDSS DATA USING TRACTOR Dustin Lang and CS82

11 FORCED PHOTOMETRY ON STRIPE 82 SDSS DATA USING TRACTOR Dustin Lang and CS82 Fits done on individual frames.

12 Various efforts to update the Annis et al co-adds (Linhua / Yusra / etc..). Can we compare the photometry from these different efforts? Depth? photoz s, cluster catalogs,... Topic for breakout session?

13 REDMAPPER CLUSTER CATALOG random nice looking cluster RedMaPPer: Red sequence Matched-filter Probabilistic Percolation algorithm (Rykoff et al. 2013, Rozo et al. 2013) ( Eli s talk on Tuesday...) Photometric redshift accuracy for the clusters is +/ for z<0.3 and +/ for z> cluster with richness>20 and z < 0.7 high redshift extension to SDSS Eli Rykoff, Eduardo Rozo, and CS82

14 REDMAPPER CLUSTER CATALOG 100 SkyNet BCG Wcen Mean red galaxy position ΔΣ [[M M O pc -2 ] 10 Mis-centering R [ Mpc ] R [Mpc] Lensing signal for Stripe 82 clusters RedMapper improved centroids

15 CLUSTER VISUALIZATION TOOL Developed to inspect BCGs. But could be useful for other projects? Talk with us if you might be interested!! Could be adpated Anupreeta More, Eli Rykoff, Eduardo Rozo, and CS82

16 CENTERS OF DM HALOS Hoshino et al. in prep Hanako Hoshino, Claire Lackner, Chiaki Hikage, Rachel Mandelbaum Eli Rykoff, Eduardo Rozo Are central galaxies in clusters always the brightest LRG / BOSS Low-z member? 20 % of time answer is NO. RedMaPPer cluster is better. Empirically derived HOD Figure 1. for LRGs and BOSS Low-z sample? Ask Hanako Hoshino! Best-fit model parameters Measurement M180b c 180b qcen RMBCG qcen LBCG qcen BLRG Roff RMBCG Roff LBCG Roff BLRG [10 14 M /h] [per cent] [per cent] [per cent] [Mpc/h] [Mpc/h] [Mpc/h] χ 2 min

17 STRONG LENSING Strong lenses in CS82 Strong lensing candidates found by Arcfinder (More et al. 2012) and subsequent visual inspection by multiple volunteers Strong lens candidates found by Arcfinder (More et al. 2012) and Final sample being compiled now... subsequent visual inspection by multiple volunteers Measuring stellar masses and lens masses to give dark Measuring stellar masses and lens masses to give Dark Matter fraction matter fraction Anupreeta More, Gabriel Caminha,! Anna Niemiec, Martin Makler and CS82 collaboration Anupreeta More, Gabriel Caminha, Anna Niemiec, Martin Makler and CS82

18 ANGULAR CLUSTERING by Johan Comparat Angular clustering down to i<23 (fainter than this, inhomogeneities in survey start to matter) Above i>23 : depth of survey varies from tile to tile Θ> 0.2 deg w(θ) is highly covariant (geometry of Stripe) Small scales : w(θ) down to 0.002/0.004 deg Also : angular clustering of emission line galaxies (ELGs). Tracers for eboss and DESI. Comparat et al See talk by Jean-Paul

19 WEAK LENSING OF BOSS GALAXIES R x w p (r p ) [Mpc/h] [ M O pc -2 ] % 20% R [Mpc] R [Mpc/h] Most massive galaxies at z=0.5, log(m*) > % measurement of wp 20% measurement of ΔΣ (weak lensing) But also need to understand completeness... Leauthaud et al. in prep

20 sis steps outlined in the previous section. Figure 3 shows the results of this calculation. The recovered convergence power spectrum is shown in red, while the input convergence power spectrum is shown in black. The analysis pipeline accurately recovers the input power spectrum, within measured errors. With Sudeep Das, Blake Sherwin, CS82 and ACT collaborations V. RESULTS A. The CMB Lensing - Galaxy Lensing Cross Power Spectrum The cross power spectrum of the ACT CMB lensing and CS82 galaxy lensing convergence maps is shown in Fig. 4. bars for both spectra are computed from Monte Carlo estimates, as before. SHEAR X CMB CROSS-CORRELATIONS VI. Hand, AL et al CONCLUSIONS B. Null Tests We verify our pipeline and measured cross power spectrum with a series of null tests. We use 480 Monte Carlo realizations of simulated CMB lensing maps (containing signal and realistic noise), and compute the cross power spectrum of the true CS82 convergence field with these realizations. The mean of these spectra is shown in the top panel of Fig. 5 and as expected, the result is consistent with null, with a (slightly high) 2 = 10.0 for 5 degrees of freedom for a null fit. We also compute the mean cross power spectrum between the true ACT convergence field and 500 realizations of randomized shear maps (described in Section III). Shown in the center panel of Fig. 5, this mean correlation is also consistent with zero, with First detection of CMB x galaxy lensing cross-correlation! 3σ FIG. 4. The CMB lensing - galaxy lensing convergence cross power spectrum (red points), measured using ACT and CS82 data. Error bars are computed using Monte Carlo methods (see text), and the significance of the detection of the cross power spectrum is 3.1. Adjacent data points are 10% anticorrelated. The solid black line is the expected power spectrum assuming the best-fit Planck + WP + highl + BAO cosmological model. ACT Kappa map Galaxy Kappa map from CS82 (Stripe 82)

21 AND MORE... Li R et al Satellite halo masses Shan H.Y et al Mass maps & peak statistics Comparat et al Bias of color-selected BAO tracers See Jean-Paul s Talk

22 CS degrees to i<23.5 Seeing ~ 0.6 over full survey Galaxy 170 degrees morphology to i<23.5 / shear Seeing ~ 0.6 over full survey