subaruUM2010_murayama

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かずゆきえいさか
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1 SuMIRe/PFS 村山斉 (IPMU & Berkeley) Subaru Users 国立天文台

2 PFS HSC 5 PFS

3 (FIRST) HSC PFS weak lensing BAO dark energy PFS cf. white paper

4 UM UM PFS exciting

5 SAC HSC UM Eric Prieto (Marseille)

7 Astro 2010 Science Objectives Cosmic Dawn New Worlds Physics of the Universe Dark Energy Dark Matter Inflation Test GR

8 Large Scale Space Program - Prioritized 1. Wide Field InfraRed Survey Telescope (WFIRST) 2. Explorer Program Augmentation Dark Energy 3. Laser Interferometer Space Antenna (LISA) 4. International X-ray Observatory (IXO) Roger Blandford ASTRO 2010 roll-out New Worlds, New Horizons in Astronomy and Astrophysics 20

9 Large-scale Ground-based Program - Prioritized 1. Large Synoptic Survey Telescope (LSST) 2. Mid-Scale Innovations Program Dark Energy 3. Giant Segmented Mirror Telescope (GSMT) 4. Atmospheric Cerenkov Telescope Array (ACTA) Roger Blandford ASTRO 2010 roll-out New Worlds, New Horizons in Astronomy and Astrophysics 32

10 Physics of the Universe The properties of dark energy would be inferred from the measurement of both its effects on the expansion rate and its effects on the growth of structure (the pattern of galaxies and galaxy clusters in the universe). In doing so it should be possible to measure deviations from a cosmological constant larger than about a percent. Massively multiplexed spectrographs in intermediate-class and large-aperture ground-based telescopes would also play an important role.

11 Timeline WL BAO DES HSC SDSS/BOSS PFS LSST Euclid? WFIRST?

12 BOSS DES HSC WL PFS BAO PFS bias PFS+HSC (σ(w pivot )σ(w a )) 1

13 SuMIRe Subaru Measurement of Images and Redshifts 8.2 m, excellent seeing 0.6, 1.5 HyperSuprimeCam: weak lensing survey 0.9 B pixels, 3 ton 10 ~40, PrimeFocusSpectrograph: 2400 fibers, ~2000 sq. dg. >1M redshifts ~50, 16.5 SDSS 8.2m HSC PFS

WFMOS Wide-Field Multi-Object Spectrograph 2006/7: HSC 18 2007/5: WFMOS conceptual design study

15 WFMOS Wide-Field Multi-Object Spectrograph 2006/7: HSC /5: WFMOS conceptual design study 2009/1: Subaru Users Meeting WFMOS 2009/2: Team B design (PI: Richard Ellis) 2009/5: Gemini WFMOS HSC

16 SuMIRe /7 565 SuMIRe / , 2009/ ?

17 2010/3/29: /6/1: 2 : HSC 12 PFS 17 5 cf. WFMOS 58?

18 collaboration

19 PFS collaboration Latest News Blog Media Room Press Kits Fact Sheets Profiles John Hopkins? Current Past Future Proposed All

22 Jan 14: Subaru Users Meeting July 13: Subaru Advisory Committee July 20-21: first PFS collaboration meeting July 29: meeting with Caltech/JPL Aug NAOJ Aug 13: Astro 2010 rollout Sep 9-10: IPMU Oct 7-8: Caltech Oct 9: PFS collaboration meeting Dec 9: PFS NAOJ White paper 219 pages!

23 WFMOS

24 WFMOS

25 WFMOS : (5m x 3m) (2m x 2m)! Hamamatsu 4k!2k CCD moving parts static ( nm) Gemini

26 BAO minimum nm, R 3000 (4k x 4k) nm, R z~10

27 20000 OII Ly α (Å) PFS z

28 Fully depleted back-illuminated CCD Red sensitive! Hamamatsu Photonics! Quantum efficiency (sensitivity) Old Wave length nano meter Large format CCD 3cmx6cm 2048 pixels x 4096 pixels!

29 (%) (%)!"# #!!" $!!"!!## +!",!"!!## *!" +!"!!## minimum )!" (!" *!"!!## )!"!!## maximum '!" &!" (!"!!## '!"!!##,-." %!" $!" &!"!!## %!"!!## # $' - # # +$").# '!(/0# #########,$"'.# )&&/0# #########+*"*.#1$!)'/0 #!" $!"!!##,/0.!"!"!!## &*!# '!!# '&!# ')!# ',!# (%!# ((!# (+!# )$!# )'!# )*!# *!!# *&!# *)!# *,!# +%!# +(!# ++!# wavelength (nm)

30 fiber positioner JPL Cobra design 精度~10μのpointingを約30秒で

31 Jim Gunn

32 throughput

33 Eric Prieto (Marseille) blue arm red arm

34 (z=0 10) Lyman alpha forest QSO

35 UM UM PFS exciting

~0.5% ~ % 4.5% 22% 74% 0%

~0.5% ~ % 4.5% 22% 74% 0% IPMU UC Berkeley @IPMU 2011 7 29 ~0.5% ~0.1 1.5% 4.5% 22% 74% 0% ! " 1.5 1.0 0.5 Supernova Cosmology Project Kowalski, et al., Ap.J. (2008) SNe BAO Union 08 SN Ia compilation Flat CMB ( 70 ) 0.0 0.0 0.5