Science with the Hyper Suprime-Cam (HSC) Survey

Transcription

1 Science with the Hyper Suprime-Cam (HSC) Survey Rachel Mandelbaum Survey webpage: Data release 1: 1

2 Subaru Telescope Prime-Focus Instrument Subaru summit of Mt. Mauna Kea (4200m), Big Island, Hawaii 2

3 Subaru Telescope: wide FoV & excellent image quality Fast, Wide, Deep & Sharp a cosmological survey needs these HST SuprimeCam image (M. Oguri) Galaxy cluster 3

4 Subaru Telescope: wide FoV & excellent image quality Hyper Suprime-Cam FoV: 1.5 degree diameter Fast, Wide, Deep & Sharp a cosmological survey needs these Galaxy cluster HST The current SuprimeCam image (M. Oguri) 4

5 HSC image of M31 5

6 HSC Image of M31 (HSC FoV=1.8 sq. degrees) 6

7 7

8 Parameters of HSC SSP Survey Wedding-cake-type survey Wide (1400 deg 2, i~26) Deep (28 deg 2, i~27) Ultradeep (3 deg 2, i=27.7) 8

9 Filters & Depth g r i z y N3 N8 N9 N10 W D UD For HSC-Deep and Ultra-Deep, a combination of broad- and narrow-band filters enables detection of Lyman-alpha emitters at z=2.2, 5.7, 6.6 and 7.3 9

10 HSC Survey started in March 2014 ~1.5 nights (S14A), ~12 nights (S14B), ~15 nights in S15A Now (mid-2017) ~50% of the survey s time has been allocated. Subaru HSC image (riz: ~2.5hrs) COSMOS HST (640 orbits: ~500hrs) a Reduced by HSC pipeline (Princeton, Kavli IPMU, NAOJ) 10

11 Exquisite image quality Camera will be presented in Miyazaki+17 in prep (from RM+17) 11

12 Gravitational lensing Strong lensing Sensitive to all matter along line of sight, including dark matter! 12

13 More generally Lensing predicted by Newton, with modified predictions by Einstein: Diagram from Narayan & Bartelmann (1997) Credit: Couch & Ellis / NASA 13

14 Weak lensing Very small deflection angles Coherent Does not require chance superposition like strong lensing Picture credit: LSST Science Book 14

15 Weak lensing Very small deflection angles Coherent Does Lensing not depends require on: chance superposition like Picture credit: LSST Science Book Enclosed mass Distance from that mass Lensing kernel : distances to lens and source strong lensing 14

16 Why should you care about weak lensing? Structure growth! Dark matter and dark energy! ESA/Planck Theory of gravity! Galaxy-dark matter connection! 15

17 So how does this work? Cosmic shear: weak lensing by large-scale structure Requires catalogs with: 1. Galaxy positions 2. Galaxy shear estimates And an estimate of dn/dz. 16

18 Another option: galaxy-galaxy or cluster-galaxy lensing Requires catalogs with: 1. Background galaxy positions, shear estimates, redshift estimates 2. A sample of foreground masses 17

19 Another option: galaxy-galaxy or cluster-galaxy lensing Projected mass Mass profiles of massive galaxies, including largescale structure (RM et al. 2013) Transverse(separation(R((Mpc/h)( 18

20 Weak lensing cosmological constraints: dark energy to z=1 Uncertainty in w(z) Redshift 19

21 Synergy between HSC and BOSS SDSS Subaru Suprime-Cam background gals halo (M>10^13Ms) CMASS gal (z=0.54) CMASS Credit: Masayuki Tanaka (IPMU) BOSS gals HSC data will add background galaxies as well as member galaxies around each BOSS galaxy Cross-correlation of BOSS with HSC galaxies (shapes and positions) over 1400 sq. degrees 20

22 Synergy between HSC and BOSS SDSS Subaru Suprime-Cam background gals background gals halo (M>10^13Ms) CMASS gal (z=0.54) CMASS Credit: Masayuki Tanaka (IPMU) BOSS gals HSC data will add background galaxies as well as member galaxies around each BOSS galaxy Cross-correlation of BOSS with HSC galaxies (shapes and positions) over 1400 sq. degrees 20

23 HSC data release in Feb 2017 Includes a wide range of image and catalog-level products, sky map,... ~100 deg 2 of data in all 5 bands to full depth Some deep-layer data released as well Some more data products in incremental releases as time goes on (e.g., early June, ) 21

24 Quick snapshots of some results so far 22

25 arxiv: v1 [astro-ph.im] 3 May 2017 Characterization and Photometric Performance of the Hyper Suprime-Cam Software Pipeline Star PSF Magnitude Song Huang 1,2 Alexie Leauthaud 1,2, Ryoma Murata 2, 4, James Bosch 3, Paul Price 3, Robert Lupton 3, Rachel Mandelbaum 5, Claire Lackner 2, Steven Bickerton 2, Satoshi Miyazaki 6,7, Jean Coupon 8, Masayuki Tanaka 6 arxiv: Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA USA 2 Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo. 00, No.Institutes 0 for Advanced Study, the University of Tokyo (Kavli IPMU, 15 WPI), Kashiwa , Japan 3 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ Department of Physics, University of Tokyo, Tokyo , Japan 5 McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA 6 National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo , Japan 7 SOKENDAI (The Graduate University for Advanced Studies), Mitaka, Tokyo, , Japan 8 Department of Astronomy, University of Geneva, ch. d E cogia 16, 1290 Versoix, Switzerland (a) Note software pipeline is described in Bosch et al (2017, arxiv: ) song.huang@ipmu.jp Received hapril 2017i; Accepted h2017i Abstract The Subaru Strategic Program (SSP) is an ambitious multi-band survey using the Hyper Suprime-Cam (HSC) on the Subaru telescope. The Wide layer of the SSP is both wide and deep, reaching a detection limit of i 26.0 mag. At these depths, it is challenging to achieve accurate, unbiased, and consistent photometry across all five bands. The HSC data are reduced using a pipeline that builds on the prototype pipeline for the Large Synoptic Survey cmodel Magnitude Telescope. We have developed a Python-based, flexible framework to inject synthetic galaxies into real HSC images called SynPipe. Here we explain the design and implementation offig. 1. Illustration of the workflow of SynPipe. Gray boxes indicate required inputs at different stages. injects synthetic objects into single-frame images. Below the blue box, we show an HSC imag SynPipe and generate a sample of synthetic galaxies to examine the photometric performancesynpipe The positions of synthetic objects are highlighted with green circles. Red boxes depict the image coaddin On the of the HSC pipeline. For stars, we achieve 1% photometric precision at i 19.0 mag and 6%and multiband.py. At the bottom left, we show a coadd image which contains synthetic galaxies. Fig. 16. Relation between the log10 (Blendedness) parameter and the photometric accuracy f 23 tracts, patches, and visits. The red colored box corresponds to one tract which has an area of ab precision at i 25.0 in the i-band (corresponding to statistical scatters of 0.01 and 0.06 mag c and d). Left columns (a andasc) show the uncertainties PSF and/or cmodel magnitudes. Rig commonly known pointings ) with small rectanglesinrepresenting CCDs. patches are represented by Galaxy (c)

26 Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0 The first-year shear catalog of the Subaru Hyper Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0 Suprime-Cam SSP Survey Normalized Number 10 1 arxiv: Fig. 9. The effective (weighted) galaxy number density as a function of seeing in eac spacing of 0.5 arcmin on the tangent-projected sky using Gaussian smoothing with density as a function of seeing in each field, while the black points with errorbars s survey. Normalized Number 1 Rachel Mandelbaum, Hironao Miyatake2,3, Takashi Hamana4, Masamune 80 HECTOMAP PSF stars non-psf stars 5,6, Oguri, Melanie Simet7,2, Robert Armstrong, James Bosch, Ryoma GAMA09H Murata3,6, Franc ois Lanusse1, Alexie Leauthaud, Surhud WIDE12H, Jean Coupon GAMA15H More, Masahiro Takada, Satoshi Miyazaki, Joshua S. 30 Speagle, XMM 4 8 3,9 50 Masato Shirasaki, Cristo bal Sifo n, Song VVDS Huang, Atsushi J. 25 Nishizawa1240, Elinor Medezinski8, Yuki Okura13,14, Nobuhiro Okabe15,16, Nicole Czakon, Ryuichi Takahashi18, Will Coulton19, Chiaki Hikage3, Yutaka Komiyama4,20, Robert H. Lupton8, Michael A. Strauss8, Masayuki Tanaka4 and Yousuke Utsumi16 17 PSF shape residual correlation function 5 Residual Fractional Size Correlation fδσ McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 0 Pittsburgh, PA015213, USA fδσ fδσ Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 3 Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, 10 4 Tokyo Institutes for Advanced Study, The University Tokyo, Chiba , Japan w/ BFofcorrection PSF stars National Astronomical Observatory of Japan, Mitaka, , Japan w/o BF Tokyo correction non-psf stars 5 Research Center for the Early Universe, University of Tokyo, Tokyo , Japan Department of Physics, University of Tokyo, Tokyo , Japan 7 University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USA 8 Department of Astrophysical Sciences, 4 Ivy Lane, Princeton University, Princeton, NJ Department of Astronomy and Astrophysics, University of California, Santa 10 5 Cruz, 1156 High Street, Santa 0.01 Cruz, CA USA 10 Department of Astronomy, University of Geneva, ch. d E cogia 16, 1290 Versoix, Switzerland 11 Harvard University, 60 Garden St, Cambridge, MA Institute for Advanced Research, Nagoya University, Furocho Chikusa-ku, Nagoya, , Japan RIKEN Nishina Center, 2-1 Hirosawa, Wako, ipsf Saitama , Japan θ [deg] 14 RIKEN-BNL Research Center, Department of Physics, Brookhaven National Laboratory, Bldg. NY, 11792, USA size residual of the PSF star sample in each field. The size is defined by the determinant radius. The gray shaded Fig. 510, 6. TopUpton, left: Distribution of the fractional 15 Department of Physical Science, Hiroshima University, Kagamiyama, regions indicate the requirements on the mean residual for the first-year HSC survey data. The vertical dashed lines show the median of the fractional size residual of each field; Hiroshima the results are highly consistent across fields. Top right: Same as the top left, but for non-psf stars. Bottom left: Solid lines are median Higashi-Hiroshima, , Japan 16 Fig. 9. The effective galaxy as are a function of seeing in each fie and bootstrap error of residual size of Center, the PSF stars after brighter-fatter correction, as a (weighted) function of the i-band PSFnumber magnitude. density Dashed lines without Hiroshima Astrophysical Science Hiroshima University, Higashi-Hiroshima, brighter-fatter correction, as calculated using the first 61.5 nights of data through November 2015 (hence the observed area is different from what went into Kagamiyama 1-3-1, , Japan spacing of 0.5 arcmin on the tangent-projected sky using Gaussian smoothing 24 with σ the solid lines). The gray shaded regions indicates the requirements on the mean residual for the first-year HSC survey data. Bottom right: The correlation 17 Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box , Taipei 10617, Empirical constraints on PSF modeling errors and the importance of brighter/fatter corrections. density asanda dashed function of seeing each field, stars, while the black function of the fractional size residuals as a function of separation θ. Solid lines show results forin PSF and non-psf respectively. points with errorbars show

27 Two- and three-dimensional wide-field weak lensing mass maps from the Hyper Suprime-Cam Subaru Strategic Program S16A data Masamune OGURI 1,2,3,SatoshiMIYAZAKI 4,5,ChiakiHIKAGE 3, Rachel MANDELBAUM 6,YousukeUTSUMI 7,HironaoMIYATAKE 8,3, Masahiro TAKADA 3,RobertARMSTRONG 9,JamesBOSCH 9, Yutaka KOMIYAMA 4,5,AlexieLEAUTHAUD 10,SurhudMORE 3, Atsushi J. NISHIZAWA 11 and Nobuhiro OKABE 7,12,13 arxiv: Dec (J2000) Dec (J2000) Total mass from lensing RA (J2000) RA (J2000) Stellar mass of LRGs Publications of the Astronomical Society of Japan, (2014),Vol.00,No.0 Fig Test of systematic effects in weak lensing mass maps from crosscorrelations of mass maps with various quantities that are potentially a source 1.6of systematics (see also Vikram et al. 2015). We show results for smoothing 0.8 sizes of both θ s Mass map =4 (filled circles) and16 (filled squares). For comparison, 0.0 the rightmost points show the cross correlation coefficientsbe- tween weak lensingsystematics and galaxy mass maps presented Figure tests 9,whichrepresents the physical cross correlation rather than the systematic test. Errors are estimated from 50 mock samples of the weak lensing shear catalog, which include cosmic variance (see Appendix 1) between E- andb-mode mass maps and PSF parameters. We construct star mass maps κ star E and κ star B which use star ellipticities e star 1 and e star 2 to construct weak lensing mass maps with the same method as described in Section 3.1. The star catalog used for this analysis is same as the one used for various systematics tests in Mandelbaum et al. (2017). For this purpose, we use both the original star ellipticities e star i as well as star ellipticities after the PSF correction is applied, i.e., e star,cor i = e star i e 25 PSF i. We also create maps of star ellipticities e 1 and e 2 themselves. b m c c sm P sy th v 4 4 W w su to d l m th κ w is Σ w re

28 HSC Double source plane (DSP) lens serendipitously discovered in HSC Survey inner reddish arc and counter2 Collett et al. S1 Very rare double sourceimage plane(s1) systems 2 GRAVITATIONAL LENSING AND DOUBLE SOURCE SYSTEMS outer blue Einstein ring with Mass causes the deflection of light and so can act as a grav source 1 source 2 lens plane central knot (S2) tational lens, producing a set of images where the time dela plane plane observer Strong lensing Double source plane lenses 2 More et al. crolensing (e.g., Morgan et al. 2008; Motta et al. 2012). Quasar microlensing also enables us to directly measure the fraction of mass in stars in the foreground lens at the position of the quasar images. This provides crucial inds1 formation to measure the stellar initial mass function of Dls2 lensing galaxies (e.g., Oguri et al. 2014; Schechter et al. 2014; Jime nez-vicente et al. 2015). Furthermore, source Lens Source 1 Observer reconstruction of lensed quasars andsource their 2host gives a difunction is stationary. a strong lens system withinafilters sourc rect view on the co-evolution of quasars and host galaxies Figure 4. From leftfor to right, NIR VIKING imaging up to z 4 (e.g., Peng et al. 2002; Rusu et al. 2016). lying directly on the optical axis this produces an Einstei Systematic searches for lensed quasars have success- W1 and W2. The brighter pair of lensed images are close t Einstein radius is sensitive to the angular diamete fully found over hundreds of lens systems, in thering. radio The W1 and W2 imaging show emission from the lens galaxy al (e.g. Myers et al. 2003; Browne et al. 2003), in thedistances optibetween observer, lens and source. In the case of cal (e.g. Oguri et al. 2006; Inada et al. 2012; More et al. catalogs. North is up and East is left. The bar shows a scale o thin lens in an otherwise homogeneous universe the Einstei 2016)source as wellplane as other Figure 1. Sketch of a double lensmulti-wavelength system. For a regimes (e.g. radius Jackson et al. 2012). On galaxy scales, lensed quasars Double source plane (DSP) lens is given by singular isothermal sphere, are thetypically dimensionless number η is the or doubly imaged ( doubles ) quadruply! serendipitously discovered in HSC product of Dls1 and Ds2 (both in red) divided by the product of imaged ( quads ). Most of the lensed quasar systems 4GM (θe ) Dls are doubles. For example, a sample θe = (1 Dls2 and Ds1 (both in blue).discovered to datesurvey c2 Dol Dos of thirteen lensed quasars recently discovered by More - Sloan innerdigital reddish and counteret al. (2016) from the Skyarc Survey-III are where θe is the Einstein radius, M (θe ) is the projected mas all doubles. Nonetheless,image quads with their two additional (S1) images provide additional astrophysical information on the Einstein radius, and the Dij are the angular d within blue Einstein with the foreground lens- andouter the background source.ring Findameter distances between observer (o),1 lens (l) and sourc ing more quad quasar lenses is thus of tremendous value central knot (S2) 2010; Weinberg et al. 2012), but taking the ratio of the14 Fig. 1. Color (gri) composite of HSC J showing the (s). In this we assume toanbe SingularconIsothe to the community given the small number of currently fourwork blue lensed images (A, all B, Clenses and D) in Einstein-cross two Einstein radii in a known double source system allows us figuration. Apart from the central lensing galaxy (G), a companion quads. mal Spheres a C) spherically symmetric mass di Spectroscopic redshifts galaxy w independently galaxy(siss), (G1, closewith to image is probably contributing to lensing. In this of paper, report theconstant. discovery of from the quad to Lens constrain thewehubble 00 on the side. North is up and East is left. The image is 10 The density of an SIS profile is given by: lens HSC J (henceforth to as Magellan/FIRE datareferred tribution. This independent constraint not only teach us Suprime-Cam about HSC will J ) from the Hyper (HSC) zhelp =improve LENS σv 2 the nature of dark energy, but also Survey. Thewill HSC survey is a Subaru Strategic Program The lens system, HSC J , was recently disρ(r) =during the2.visual inspection of (2 zinstalled (SSP) usingparameters the newly HSC (Miyazaki et al. covered serendipitously S1 constraints on other cosmological by= 1.30 providing 2πGr 2012) instrument on- thez Subaru 8.2-m telescope. The data from the HSC Wide (internal data release = 1.99 S2example complimentary probes with a prior on w. For the survey consists of three layers (wide, deep, ultradeep), sq. deg., S15A). HSC been J of the SIS 2mass170distributions have shownconsists to approximat layer First known DSP lens with both main lens galaxy (G) with four lensed images (A, B, C where the wide is expected to cover 1400 deg WMAP7 constraints on h (the reduced Hubble constant) Tanaka, Wong, AM et al. in2016 the observational data configuration well (e.g. (see Koopmans al and D) in a cross Fig. 1). A et second grizy -bands down to aredshifts depth of rspectroscopically 26. The HSC source are h = ± data (Komatsu et al. 2011) for a flat 26 (G1) located very close image C, lensing is probably a al. 2010) and allow forto simple forecast are processed with hscpipe, which is derivedauger from et galaxy confirmed the main lensangle galaxyand G and is likely to perturb the at LSST pipeline (Ivezic ΛCDM model with w fixed 1,software whilst allowing w et to al. be2008; Axelrod since the satellite lensingofdeflection magnification have an Ds2 Dls1 Eye of Horusredshifts from Spectroscopic Magellan/FIRE data zlens = zs1 = 1.30 S2 S1 zs2 = 1.99 Double source plane (DSP) lenses First known DSP lens with both The Eye of Horus Quadruply lensed AGN! et al two sources at distinct redshifts being lensed by source redshifts spectroscopically (Tanaka, Wong, A. (More et al 2016) the same galaxy confirmed More et alonly 2016) - rarer than ordinary lenses, a handful known zqso=3.8 (e.g., Gavazzi+2008, Tu+2009) Gavazzi et al. 2008

29 Source Selection for Cluster Weak Lensing Measurements in the Hyper Suprime-Cam Survey Elinor Medezinski 1,MasamuneOguri 2,3,4,AtsushiJ.Nishizawa 5, Joshua S. Speagle 6,HironaoMiyatake 2,7,KeiichiUmetsu 8,Alexie Leauthaud 9,RyomaMurata 2,4,RachelMandelbaum 10,Cristóbal Sifón 1, Michael A. Strauss 1,SongHuang 2,9,MelanieSimet 7,11,Nobuhiro Okabe 12,13,MasayukiTanaka 14 and Yutaka Komiyama 14,15 arxiv: Robust source selection for lensing measurements by optically-selected cluster samples (very high S/N) Transverse(separation(R((Mpc/h)( 27

30 Advertisement of ongoing work 28

31 Cosmic shear tomography (cross-correlations of shear in redshift slices) Power at wavenumber l Part of our blinding scheme for cosmology analysis To appear in Hikage et al (in prep); Total S/N exceeds 20 29

32 Lensing of SDSS-III BOSS CMASS galaxies 10 2 z [0.43, 0.55] z [0.55, 0.70] Σ (hm /pc 2 ) Projected mass R Σrp (M Mpc/pc 2 ) Measurement courtesy of Surhud More (No amplitudes shown due to use of blinded analysis method; random vertical offset applied) R (h 1 Mpc) R (h 1 Mpc) Transverse(separation(R((Mpc/h)( 30

33 Validating weak lensing analysis with simulations How you define your input galaxy sample matters! Simulations can reproduce observed galaxy properties if we include contributions from neighboring objects (instead of just isolated galaxies) Apparent size compared to PSF Mandelbaum et al (in prep) 31

34 Looking forward it s turtles galaxies all the way down 32

35 Looking forward Blending is a major challenge for deep future surveys like LSST, and will affect all aspects of the analysis (photometric redshifts, shear, ). We need to confront this problem and its impact on cosmological analysis. 33

36 Summary The HSC survey had its first data release You should download and play with our beautiful data! Check out hscmap Lots of science is being done! Keep an eye on arxiv We are learning valuable lessons for the era of precision cosmology. Feel free to me any questions: 34