456

789:

Updates on PFS;<9:

Hitoshi Murayama (IPMU & Berkeley)
PFS workshop, NAOJ, Dec 9, 2010

imaging

proposedimaging

imaging

imaging + spectroscopy

imaging•••

CMBImages and Redshifts
1. imaging with 0.9B-pixels 3t
CCD camera from 2011
2. spectroscopy with ≈2000
BOSS
objects >2015
best measurements of dark
Panenergy params in this decade Starrs
DES
3D map of dark matter to ACT
observe structure formation
same telescope for both2008
2009
imaging and spectroscopy
2010
2011
like SDSS but 8.2m!
2011

2013

Figures of merit• Major study of dark energy• Subaru Measurement ofimaging + spectroscopy

SuMIRespectroscopy

SubaruSuMIRe

Subaru Measurement of Images and Redshifts• July 2009: Japanese LDP••••••

government announced
economic stimulus package
FIRST program announced,¥270B for 30 researchers
tried to save both HSC andmulti-object spectrograph
Sep 5, 2009: HM selected
Sep 16, 2009: new DPJ
government slashed ¥270B
to ¥100B
Jan 14: Subaru Users Mtg
long wait for the final wordfunding• Mar 29, 2010: ¥3.2B•••

awarded to HM
Jun 1, 2010: ¥0.2B“boost” awardedagency decision:
HSC ¥1.2B
PFS ¥1.7B
overhead ¥0.5B
cf. WFMOS ¥5.8B•••

Updates• Apr 13: meeting with Miyama• May 4: meeting with Marseille• July 13: Subaru Advisory Committee• July 20-21: first PFS collaboration meeting• July 29: meeting with Caltech/JPL• Aug 19-20: GOPIRA meeting @ NAOJ
• Aug 13: Astro 2010 rollout

How do we fit it in?
• Three basic strategies• find free labor• contribution from international partners• cost reduction• Princeton is interested in going beyond 1μ,but neither within WFMOS scope nor
current discussion; requires more funds
Aug 19-20: GOPIRA meeting @ NAOJWFMOS design• “big beam” spectrograph, 3 x (5m x 3m)!
• Subaru people don’t like this• 6k×3k CCD from LBNL/JPL• better use Hamamatsu 4k×4k• many moving parts to switch High & Low R• better have a static design
Aug 19-20: GOPIRA meeting @ NAOJ

technical specs• BAO• correlate distance from BAOto redshift ➔ dark energy• targets selected with HSC• go beyond BOSS: z≈0.6–1.6• most efficient (least exposure):
OII emission 372.7, 373.0 nm• need 600-1000nm, R≈3000• measure w down to 3%~500 fibers x 5• 4k×4kAugCCDs,
19-20: GOPIRA meeting @ NAOJ

Figure 1: Fractional errors in measuring the angular diameter distance and the Hubble
each redshift slices for the different BAO surveys, SDSS, BOSS and PFS. For the PFS s
survey parameters given in Table 3. Note that the expected accuracies of distancesensitive to the bias parameters or number densities of target galaxies we assumed.

tend to be brighter in redder bands than in i band. Therefore a more careful study for
the PFS survey needs to be done assuming the deep, multi-color data sets available fr

additional science• BAO• also reach z≈3 with Lyα• need blue: 400–600 nm• weak lensing tomography• HSC weak lensing survey with photo-z• with real z, can do tomography• 3D map of dark matter• observe structure evolution w/o bias
Aug 19-20: GOPIRA meeting @ NAOJ

other science?
• galactic archaeology based on dynamics• 393.5 (K), 397.0 (H), R~3000?
• 850.0, 854.4, 866.5 (CaII), R~5000?
• Galaxy evolution with primordial HeII 164?
• EoR with Lyα emitters?
• AGN with OIII 500.7?
• SNe?
• minimize cost, maximize science!
Aug 19-20: GOPIRA meeting @ NAOJ

brainstorming
Ouchi (ICRR)

Aug 19-20: GOPIRA meeting @ NAOJ

Conclusions• now likely that we can complete HSC• spectrograph still uncertain but possible• detailed specs will depend on funds
available• need lots of negotiations/discussions• next week visit UK, Marseille, JPL• Princeton and Brazil in September
Aug 19-20: GOPIRA meeting @ NAOJ

Need community input• Subaru Future Instrumentation Workshop• Sep 9 & 10, 2010 @ IPMU
• science scope, spectrograph specs• minimize cost, maximize science!
• hoping for community endorsement atJanuary Subaru Users MeetingAug 19-20: GOPIRA meeting @ NAOJ

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

Large Scale Space Program - Prioritized

1. Wide Field InfraRed Survey Telescope (WFIRST)

Dark Energy
2. Explorer Program Augmentation
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Large-scale Ground-based
Program - PrioritizedDark

1. Large Synoptic Survey Telescope (LSST)
2. Mid-Scale Innovations Program

Energy3. 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

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 ofgalaxies and galaxy clusters in the universe). In
doing so it should be possible to measuredeviations from a cosmological constant larger
than about a percent. Massively multiplexed
spectrographs in intermediate-class and largeaperture ground-based telescopes would also
play an important role.

Updates• Aug 23: meeting with UK group inEdinburgh• Aug 25: meeting with Olivier Le Fèvre(LAM)• Aug 27: video/phone meeting with Brazil• Oct 14, 15:Visit to ASIAA, Taipei• Oct 25-29: SDSS III/BOSS meeting @ IPMU
• potential interest from John-Hopkins• steering committee formed + Kobayashi• regular telecon with Subaru Observatory

Updates• Sep 9, 10: Subaru instrumentation WS@IPMU, discussed science case for PFS• Oct 7, 8: DENET workshop @Caltech• Oct 8: PFS steering committee meeting• Oct 9: PFS collaboration meeting @Caltech

Aim of this meeting• listen to Brazil proposal to join the collab.
• management plan from Hiroshi Karoji• decide path(s) on spectrograph design• additional science beyond BAO• How to obtain endorsement from Subaru

community
minimum cost, maximum science!
Oct 9: PFS collaboration meeting @ Caltech

a simple observation• multi-object wide-field spectroscopy on••••8m-scale telescope would be unique in theworld
exploit investments in HSC
main advantage over 2-4m: high-z galaxies!
HSC & PFS = SDSS × (8.2/2.5)2!
to capitalize on it, aim for a versatile
instrument

a simple comparison• SDSS/BOSS• z<0.6, 1.3M galaxies• 380-920nm, R=1800-2200• simply scale by 8.2/2.5 on lumi distance• z<1.6• 600-1500nm• In addition, blue makes Lyα possible

+,-./012.3456789:;<=>?!"#!
transmission probability
through the corrector lens coating
#!!"

+!"

minimum*!")!"

maximum:;<1B8!

(!"'!":;<,-."
&!"

%!"

$!"

#!"

@A,/0.!
!"
!""!

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wavelength (nm)))""!

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specs• minimal• 600-1000nm, R≈3000• one arm (4k x 4k)• best galaxy survey in the foreseeable future• 400-1300nm, R≈2000-5000• three arms
• OII covers z=0–2.5• Lyα covers z=2.2–10• continuous survey to very high z!

PFS collaboration

Latest NewsBlog
Media RoomPress Kits
Fact Sheets
ProfilesCurrent
Past
FutureProposedAllfiber positioner• fiber positioner basedon JPL cobra design• 2400 fibers

WFMOS

The IR Channel
1.

!

!

acquiring resources• Caltech: NSF proposal• JPL: internal funding• Princeton: NSF proposal• Brazil: two proposals• Marseille: internal resources

Lots of science• BAO, weak lensing tomography, redshift
space distortion, neutrino mass

• galaxy formation, evolution, assembly• QSO• Epoch of reionization• galactic archaeology based on dynamics

Conclusion• PFS design evolved to a much moreversatile instrument• absolutely unique in the world!
• hear about possible science with this
instrument from white-paper study• need constructive criticism to each other• make the best case to Users Meeting

Timeline
2021

2020

2019

2018

2017

2016

2015

2014

2013

2012

BAO

2011

2010
WLDES
HSC
SDSS/BOSSPFSLSSTEuclid?
WFIRST?