Big BOSS Mapping the Universe Big BOSS designed

Big. BOSS Mapping the Universe Big. BOSS designed to measure dark energy from the BAO “standard ruler” 1. Spectroscopic survey of ~20 million Emission Line Galaxies at 0 < z < 1. 7 2. Spectroscopic survey of ~3. 5 million Luminous Red Galaxies at z < 1. 0 3. Spectroscopic survey of ~0. 6 million QSOs at 1. 0 < z < 3. 5 Definitive BAO experiment at 0 < z < 1. 5 20 X volume of BOSS

Mapping the Universe Our observable Universe Stage IV BAO Volume mapped by SDSS BAO Scale M. Blanton for SDSS Surface of last scattering • • M. Tegmark Volume to be mapped by SDSS-III (ca. 2015) BAO scale length provides a “standard ruler” whose measurement is limited by the survey volume, sampling, and redshift accuracy Robust against systematic errors, sub-percent accuracies possible

Instrument Kitt Peak 4 -m (Mayall) at Kitt Peak, Arizona, 5 year survey 5000 fiber positioners on 1 -m focal plane, f/4. 5 Corrector lenses 3° FOV SDSS-inspired: simple, high-throughput 5000 fibers 10 spectrographs X 3 channels each

Big. BOSS Science Reach

Based on BOSS • BOSS works! • The **preliminary** BOSS signal from 1500 deg 2 of the 10, 000 deg 2 footprint. On schedule to finish the full footprint in June 2014. Errors are as expected. • Do not redistribute (embargoed)!!! 5

Big. BOSS Science Reach DETF Figure of Merit [P]: Planck; [g. B]: galaxy BAO; [l. B]: Ly- BAO; [Rkmax]: redshift space distortion, for k < kmax ; [Akmax]: all galaxy information for k < kmax. Anticipated Big. BOSS-NORTH figures of merit when various combinations of measures are used to determine the parameters w 0 and wa of the dark energy equation of state, along with the error on w(z) at the best-measured point, wp, and the error on Wk. The coverage is 14 k square degrees with dn=dz as predicted for Big. BOSS. 6

Big. BOSS Science Reach Distance Scale Accuracy • Angular Distance • Big. BOSS N+S 7

Big. BOSS Science Reach Distance Scale Accuracy • Hubble Parameter • Big. BOSS N+S

Redshift Space Distortions • Big. BOSS N+S • Growth rate times the amplitude of the power spectrum • Predicted by an therefore a test of GR 9

Shot Noise Limit • n. P(z) distribution 10

Big. BOSS Budget & Schedule

KA 13: Dark Energy Projects (C) Scenario C • Big. BOSS – Stage IV Dark Energy ground-based project – Substantial immediate support for Big. BOSS R&D recommended by PASAG – Recommended in all PASAG scenarios – “Need for a robust 3 -probe measurement” • WL: DES HSC LSST • BAO: BOSS (1. 5 Mgal) Big. BOSS (20 Mgal) • SNe: – – Highly rated by Astro 2010 Responded to NOAO call for proposals for Mayall telescope use Accepted by NOAO Default NOAO plan operates Mayall 10+ years in flat budget scenario (priorities will be LSST and Big. BOSS in last 5 yrs). February 2011 OHEP LBNL Budget Briefing - Physics 12

PASAG/Astro 2010 “Big. BOSS is in the early planning stages, but presents a legitimate possibility of achieving a significant fraction of the BAO science goals for JDEM at <$100 M cost. Substantial immediate support is recommended for Big. BOSS R&D so that ground BAO possibilities are known for timely planning of a coherent ground-space dark energy effort. The ground astronomy agencies (NSF/NOAO) are essential partners in the Big. BOSS project and planning. Scenario A: . . ”DOE leadership in a large project would require eliminating support for the other 2 projects and a significant delay to push expenses into the following decade. Given the importance of the science, the need for a robust 3 -probe measurement, and the technological readiness of all projects, this is highly undesirable. The alternative is to fund Big. BOSS for the BAO probe and hope that one or both large projects approach astrophysical limits for the SN and WL probes through the support of other funding agencies with much-reduced DOE participation. 2010 Decadal Survey: “This survey received 29 proposals that would be eligible for competition, with an aggregate construction or fabrication cost of roughly $1. 2 billion. The Program Prioritization Panels recommended very highly a subset of these: Big. BOSS, …. [one of four listed in the $40 -$120 M range]. ”

KA 13: Dark Energy Projects (C) • Big. BOSS Strong international collaboration (35 institutions) Recent meeting 108 attendees, 90 talks – FNAL(Annis, Diehl, Kent, Flaugher), SLAC(Roodman, Reil), Brookhaven(Slosar) Brookhaven National Laboratory Ewha Womans University, Korea Fermi National Accelerator Laboratory French Participation Group APC, IAP- Paris; CPP, CPT, LAP Marseille; CEA, IRFU – Saclay Johns Hopkins University Lawrence Berkeley National Laboratory National Optical Astronomy Observatory New York University The Ohio State University Shanghai Astronomical Observatory SLAC National Accelerator Laboratory February 2011 Spanish Participation Group IAA, Granada; IAC, Tenerife; ICC, Barcelona; IFT, Madrid; U. Valencia UK Participation Group Durham, Edinburgh, UC London, Portsmouth University of California, Berkeley University of Kansas University of Michigan University of Pittsburgh University of Science and Technology of China University of California, Santa Cruz/Lick Observatory University of Utah Yale University OHEP LBNL Budget Briefing - Physics 14

KA 13: Dark Energy Projects (C) Big. BOSS MI&E Cost (CD-1 to CD-4) = $43 M US + $33 M Foreign $43 M US Cost if all DOE: Request FY 12 Request FY 13 Request FY 14 Request FY 15 Request FY 16 Request FY 17 Request FY 18 $2 M $4 M $9 M $11 M $10 M $9 M $4+1 Or, $28 M DOE (MI&E): if cost is offset by US private funds (universities and foundation), and NSF Request FY 12 Request FY 13 Request FY 14 Request FY 15 Request FY 16 Request FY 17 Request FY 18 $2 M $4 M $6 M $6 M $3+1 NOAO response to NSF portfolio review 15

Suggested Plan • Request for FY 11 for pre-conceptual design [SWF: $1. 9 M, M&S: $0. 2 M] — • Request for FY 12 transitions to conceptual design [SWF: $3. 5 M, M&S: $0. 5 M] — — — • Key R&D: optical concept, fiber system, spectrograph, cost reduction Key R&D: reduce technical risk, value engineering, conceptual design CD-0 by 12/2011 allows us to pursue foreign, private, NSF funding CD-0 would be contingent on NOAO compliant plan for Telescope Request for FY 13 transitions to preliminary design [$6+M] — CD-1 would be contingent on other funding sources, NSF senior review and approval by NSF 16

Big. BOSS-DES Schedule Comparison DES (actual) Big. BOSS SAGENAP/PASAG (rec R&D) Apr. 2004 June 2009 NOAO Proposal July 2004 Oct. 2010 NOAO Review Sept. 2004 Nov. 2010 CD-0 Nov. 2005 ? Dec. 2011 ? CDR May 2007 ? June 2013 ? PDR Jan. 2008 ? Feb. 2014 ? MOU between NOAO & FNAL May 2008 ? June 2014 ? First Light ? 2011 ? ? 2017 ?

Big. BOSS Budget Offset items/common-fund, major ( >$1 M) acquisitions: – – Corrector glass blanks Spectrograph glass blanks, optical components Hexapod Fibers Potential Funding — — — NSF + NSFC (China) GBMF, Sloan, Keck, Research Corp. Private university. BOSS model required participating institutions to provide $900 K in better financial times.

Budget Breakdown 19

Summary • “Stage-IV” dark energy experiment from the ground – “BAO spectrograph” optimized for redshift-finding • 0 < z < 1. 0 Luminous Red Galaxies • 0 < z < 1. 7 Emission-line galaxies 50 million in 10 years • 1 < z < 2 QSOs • 2 < z < 3. 5 QSO Ly. A forest • Neutrino Mass – Should be able to make a 2 -sigma detection of the sum of neutrino masses – Could rule out inverted mass hierarchy • Requires only 4 -m telescope time - North: Kitt Peak (4 m) South: CTIO (4 m)

Big. BOSS Instrument

Instrument: Telescope If we don’t do this, someone else will! 4 -m class telescopes: KPNO 4 -m 3 -deg possible CTIO 4 -m CFHT 3. 6 -m Calar Alto 3. 5 -m ARC 3. 5 -m (Apache Point) WIYN 3. 5 -m (Kitt Peak) Discovery Channel 4. 2 -m WHT 4. 2 -m ESO 3. 6 -m SOAR 4. 2 -m UKIRT 3. 8 -m Galileo 3. 58 -m ESO NNT 3. 58 -m VISTA 4 -m 2 -deg exists AAT 3. 9 -m

Instrument: Telescope Kitt Peak 4 -m (Mayall) at Kitt Peak, Arizona 5000 fiber positioners, 0. 9 m focal plane Corrector Lens + ADC Fiber positioning Camera Fiber run (bare fibers) 10 spectrographs Design by Mike Sholl, SSL

Instrument: Fiber positioners x 5000 Collaboration with USTC in Hefei, China Experience building 4000 LAMOST fiber positioners 2 rotation axes, 25. 4 mm center-to-center spacing Light from one galaxy enters fiber here 24

Instrument: Spectrograph Collaboration with France “QSO Lyα channel” 3400 -5400 Å at R~3000 e 2 v CCDs “supernova/QSO channel” 5000 -8000 Å at R~3000 LBL CCDs “galaxy channel” 7600 -10, 600 Å at R~4200 LBL “Extreme Silicon” • 10 3 -arm spectrographs cover 3400 -10600Å at medium resolution • Spectrograph design effort led by Eric Prieto, LAM, France • Mechanical / cryogenic systems development led by Stephan Aune, CEA, France

Instrument: LBNL Detectors • Current design calls for 20 LBNL fully-depleted CCDs resulting from high yield CCD development effort (LDRD funded and led by Natalie Roe) • Red spectro channel will use “extreme” 500 m thick silicon CCDs for improved red sensitivity [OII] @ z=1. 7 4 k x 4 k flat-packaged CCD for BOSS

Targets: Collaboration w/ SN Factory Palomar Transient Factory Big. BOSS uses existing imaging surveys to identify galaxy targets. g+r imaging (3 hours exposure) i-band from PTF, Pan. STARRS-1