Precision Cosmology with Subaru HSC and PFS ( after 10yrs efforts )

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1 Precision Cosmology with Subaru HSC and PFS ( after 10yrs efforts ) Masahiro Takada (Kavli IPMU) Chiaki Hikage (IPMU) Masamune Oguri (UTokyo/IPMU) arxiv: appeared TODAY!!

2 8.2m Subaru telescope Prime-Focus Instrument Subaru Telescope summit of Mt. Maunakea (4200m), Big Island, Hawaii

3 SuMIRe = Subaru Measurement of Images and Redshifts l Wide-field camera (Hyper Suprime-Cam: HSC): 1.5 deg. FoV l Wide-field multi-object spectrograph (Prime Focus Spectrograph: PFS): simultaneous spectroscopic observation Subaru (NAOJ) of 2400 objects over ~1.3 deg. FoV l Keep the Subaru Telescope a worldleading telescope in the TMT era l Precise images of 1B galaxies l Measure distances of ~4M galaxies l Do SDSS-like survey at z>1 HSC PFS

4 Subaru Telescope: wide FoV & excellent image quality Hyper Suprime-Cam FoV Fast, Wide, Deep & Sharp a cosmological survey needs these HST The current SprimeCam image (M. Oguri) Galaxy cluster ~50,000 galaxy images

5 HSC SDSS z~0.19 z~0.30 z~0.37 z~0.44 Huang et al

6 Subaru-300-nights HSC project ( ) International collaboration (Japan, Taiwan, Princeton U.)

7 HSC Survey Fields HSC-D R.A. HSC-W DEC Three survey layers HSC-D/UD Galactic Extinction E(B-V) Wide (i~26, grizy, 1400 deg 2 ) Deep (i~27, grizy+nbs, 28 deg 2 ) Ultra-D (i~28, grizy+nbs, 3.5 deg 2 )

8 Subaru HSC = superb image quality 6 fields (~140 sq. deg. in total) Dec [deg] HECTOMAP Dec [deg] VVDS RA [deg] RA [deg] 0.8 Dec [deg] 4 WIDE12H RA [deg] GAMA09H Dec [deg] GAMA15H Subaru HSC typically 0.6 seeing FWHM (spatial resolution) DES: ~0.9 RA [deg] XMM seeing [arcsec] Dec [deg] 2 Dec [deg] RA [deg] RA [deg]

9 HSC galaxy shape catalog Developed the pipeline for galaxy shape measurement Tested/validated the galaxy shape catalog with sophisticated image simulations ~10M galaxies (~20 gals/sq. arcmin., ~140 sq. deg.) Ready to use for weak lensing science

10 Weak gravitational lensing (shear) characterize the shape of every faint galaxy

11 Unprecedented wide and deep 3D DM map Oguri et al. 18 Largest 3D dark matter map one particular field (VVDS field)

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13 <latexit sha1_base64="sxdiv2dx4fmho27gqunljooudcu=">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</latexit> Cosmic shear cosmology Pros Can measure total matter power clustering Z C` = d W GL ( ) 2 2 Pm NL k = ` ; z( ) Cons All the systematic errors additively contribute the measurements ( g-g lensing) Challenges: Photo-z errors and baryonic physics HSC data are very deep compared to DES: precursor of LSST

14 Cosmic shear tomography Used photo-z s of each galaxy to have 4 tomographic bins Used the HSC-Wide depth data of COSMOS field for galaxies after the WL cut to calibrate the photo-z errors Test the results against the different photo-z catalogs Hikage, Oguri+ 18

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16 Hikage, Oguri+ 18 Blind analysis To avoid confirmation or human bias 3 catalogs: one is real, but other 2 catalogs are fake (no one knows which one is real Do not see the actual values of parameters in the parameter inference Do not compare with other results (such as Planck) Made various tests for more than 1 year Catalog 1 Catalog 2 Catalog 3

17 Hikage, Oguri+ 18 test, test, test... 17

18 After unblinding on 26 June Hikage, Oguri+ 18 HSC result consistent with other WL surveys HSC (140 deg 2 ) DES (4m, ~1300 deg 2 ) KiDS (2.65m, 400 deg 2 ) 18

19 After unblinding on 26 June Hikage, Oguri+ 18 HSC (140 deg 2 ) Planck CMB KiDS (400 deg 2 ) DES (~1300 deg 2 ) Tension? CMB (~400,000 yrs) and LSS probes (~8-14G yrs) are not consistent with each other for clumpiness of the Universe 19

20 <latexit sha1_base64="bscbnfojgvbxy1luzagjzdd9jh0=">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 <latexit sha1_base64="cl4qnw6gc3nlwcklxsflzvqmtxu=">aaacp3ichvhptxnbfh4solbrcl5mugxomoqhedodfe4elt4sp1qaunlmbl/rpluz6+y2owz4b/whohccxadxz/diirtr/gtjermvhny7rvep6nvszdffe983b2ac0fnrjhg9zo3fmbh7b3iqd3/6wcoz/oxclqp6xqwqg3ibqtsyik9pqsyq9qgegpk+49go011p8zt9mpek9hy8cgnplx2t2sqvmvpn/frdoy7scb3r0hg5eh6ya/hosj9upkndrs1mbtkgwnzpq9siuib06w9bm1/aiiikiewuikuxygb5uvwszvukky4cjkis5m+gas0iwiue+ecgiwbsgysiv10qgbaytwcjc4aryvieh5bjby+ricsks10eo7zahbga16lnlkld3sxj37dshkw8wgu8wy/4hr/gj1u9kswj7wxaszpuuticeft46/t/vt7pmbz+rfpnzzg0ozz1qrj3mgps HSC preferred universe Planck preferred universe simulated dark matter distribution in the Universe today 20

21 PFS collaboration 21

22 PFS will populate 2394 individual fibers for simultaneous spectroscopy over this hexagonal field. ~1.5 deg

23 23

24 PFS Specifications Number of fibers 2400 Field of view 1.3 deg (hexagonal-diameter of circumscribed circle) Fiber diameter 1.13 diameter at center 1.03 at the edge Spectrograph Blue Red NIR Wavelength range [nm] ( ) Central resolving power ~2350 ~2900 (~5000) ~4200 Detector type CCD CCD HgCdTe Share WFC with HSC 4 spectrographs for 600 fibers each λ= nm with 3 arms ( nm for DESI) Fiber density: 2200/sq. degs ( ~140 for 2.5m BOSS; ~600 for 4m DESI) The medium resolution mode (R~5000) for the red arm is also available

25 <latexit sha1_base64="gkj4qys+2wrxjh6e7w1qm9vhl7k=">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</latexit> <latexit sha1_base64="gtb7g3u6uxnswunvrw63spvdq/a=">aaacj3ichvfnt9taeh24hyl5sukfqzeiikocyrq7uriqvextbw58psarfnlmsvc4a9d2iowip9bbtz1woljvof4arq249a/0we9apvkjcwfgtirgamxqd2ffzjt9o+senoxiotm+7dhj/oeng0p68mjo2hjm6ct7yg+grqi4vuehg44dcu8quyll7imnibr2w/heurp7lomvt0qysv+txe1abdxsupi70rvjhmqz2aoj6lj1xedlh6hdntnxysjm781brl6vcrv9i1ll5miykxwsfcflblhrtm <latexit sha1_base64="kyxeyane6vow6jlj+lqx846h/ou=">aaacvhichvg7tgjbfd2sl1wfrfymnkscssixgx+viy0ldxesjgr3gxddsrvzxuiq+ao0fhzwmhhj/awb sha1_base64="mwymqccyqvwqamjvxmt8pvx/q0a=">aaaci3ichvfntxrbeh0modigljw0xjysipgwqsuxahdijngtazyveozseobatcnsz9azu8ky2t/ah8de sha1_base64="o2ycdcn3iv0ingl/0wc4lxchmhq=">aaaci3ichvhnbtnaep5q/orb0scjiovvqhxiye1mixiuifuitqhtsfuprqk1u0lxddzm7uqkvl6gl1ak sha1_base64="jbrsskerxj9jhimiaiyw3h6syco=">aaaclnichvhnbtnaep5q/lrz05reqfwsoilewzqyrk24uieqnfdaefqprqk1u0lxddzm7urkrbxaxwak sha1_base64="obkunyq/op4vpdagg8dhwfk1iv0=">aaaclnichvhnbtnaep5q/lrz05reqfwsoilewzqyrk24uieqnfdaefqprqk1u0lxddzm7urkrbxaxwak Power of 8.2m Subaru Subaru allows a detection of [OII] emission lines even with 15min exposure Expected S/N of [OII] line f [OII] = erg cm 2 s <z<2.4 Blue Red NIR S N 5 TBD Redshift of [OII] emitters 25

26 For continuum Power of 8.2m Subaru 1 hour exposure Limiting mag. with S/N=5 26

27 Scientific drivers: Three Pillars All science cases are based on a spectroscopic follow-up of objects taken from the HSC imaging data Cosmology (~100 nights): 1400 sq. degrees ~4M redshifts of emission-line galaxies BAO and RSD at each of 6 redshift bins over 0.8<z<2.4 Cosmology with the joint experiment of WL and galaxy clustering (HSC/PFS) Galaxy Evolution (~100 nights): ~15 deg 2 A unique sample of galaxies (~0.5M) up to z~2, with the aid of the NIR arm Dense sampling of faint galaxies (also many pairs of foreground/background gals) Studying cosmic reionization with a sample of LAEs, LBGs and QSOs Galactic Archaeology (~100 nights): Milky Way/M31/dSphs ~1M star spectra for measuring their radial velocities Use the 6D phase-space structure, in combination with GAIA in order to study the origin of Milky Way (also use the M31 survey) Use a medium-resolution-mode survey of ~0.1M stars to study the chemodynamical evolution of stars in Milky Way

28 Takada et al. arxiv:

29 summary Achieved precision cosmology with Subaru Hyper Suprime-Cam (HSC) data! Determined S 8 (clumpiness of the Universe) to a 3.6% accuracy Still based on ~10% of the full dataset (a factor of 4 more data already taken) The full HSC data can make a rigorous test of ΛCDM model or could discover a new physics Prime Focus Spectrograph well underway Simultaneous spectroscopic observation of 2400 objects Envision we will start the large survey program from 2021 (spectroscopic follow-up of HSC stars/galaxies) 29