BigBOSS : Scientific Prospects & Current Status

1. BigBOSS: Scientific Prospects & Current Status Juhan Kim KIAS

2. BigBOSS Science Reach BigBOSS will enlarge redshift-space maps to 21 million objects 10X larger than SDSS + SDSS-II + BOSS Necessary for Stage IV dark energy from BAO, RSD 0.6 million QSOs 16 million ELGs 4 million LRGs 2

3. DOE, NSF define Stages for ground-based Dark Energy Surveys BAO: baryonic Acoustic Oscillation Stage I: first detection by SDSS-I Stage II: SDSS-I, II, Wiggle Z Stage III: 3x better than Stage II: BOSS, HETDEX Stage IV: 10x better than Stage II: BigBOSS

4. BigBOSS Timeline Apr 2009 – BigBOSS white paper submitted to decadal survey Jun 2009 – BigBOSS RFP response to Astro2010 Decadal Survey submitted and committee oral presentation Jul 2009 – BigBOSS presentation to the Particle Astrophysics Scientific Assessment Group (PASAG) Oct 2009 – The Particle Astrophysics Scientific Assessment Group (a subpanel of the NSF/DOE HEPAP Federal Advisory Committee) states: “Substantial immediate support is recommended for BigBOSS R&D” Nov 2009 – First BigBOSS collaboration meeting (LBNL) Dec 2009 – NOAO Call for proposals for Large Science Programs Mar 2010 – Letter of Intent Submitted to NOAO Sep 2010 – Astro2010 Decadal Survey Panel Report on Optical and Infrared Astronomy from the Ground identifies massively multiplexed spectroscopy as an essential capability Sep 2010 – Astro2010 Decadal Survey NWNH report calls BigBOSS a “compelling” medium-scale project. “The Program Prioritization Panels recommended very highly a subset of these…” where BigBOSS is 1 of the 4 such recommendations in the $40M to $120M range

5. Timeline Oct 2010 – The full 280 page BigBOSS proposal was submitted by a large international team that is led by the Lawrence Berkeley National Laboratory and includes 16 US institutions as well as international partners Nov 2010 – NOAO convenes external non-advocate review (Schmidt committee ) of BigBOSS Dec 2010 – Strong scientific endorsement of BigBOSS from the Schmidt committee. Endorses collaboration between NOAO and BigBOSS to bring BigBOSS to fruition Feb 2011 – Second BigBOSS collaboration meeting Sep 2011 – Third BigBOSS collaboration meeting held in conjunction with a BigBOSS community workshop Dec 2011 – BigBOSS DOE R&D Review. Received a strong endorsement in the review report Sep 2012 – Mission need of MS-DESI (Mid-scale Dark Energy Spectroscopic Instrument) signed by DOE Office of Science for Mayall and Blanco Oct 2012 – Fourth BigBOSS collaboration meeting (Paris) Dec 2012 – Gordon & Betty Moore Foundation awards $2.1 M grant to BigBOSS Mar 2013 – Fifth BigBOSS collaboration meeting (Shanghai)

6. Astro2010 Decadal Survey • Three major science objectives • Cosmic Dawn: Searching for the First Stars, Galaxies, and BHs • New World: Seeking Nearby, Habitable Planets • Physics of the Universe: Understanding Scientific Principles • Space Projects , Ground Projects • WFIRST, Explorer programs, LISA, IXO • LSST, GSMT, ACTA

7. BigBOSS White Paper (arXiv:0904.0468)

8. BigBOSS White Paper (arXiv:0904.0468) • 18 pages • DOE-NSF Stage IV ground-based DE experiment • 4000(5000)-fiber by automated positioning R=5000 spectroscopic on 3-deg FOV • 0.2<z<3.5, LRG, emission line G, QSOs • Reuses BOSS spectrograph & pipeline designs(NYU) • 4m Mayall telescope at KPNO (3degree diameter) • 10 spectrographs covering 340-1130(1060)nm, R=2300-6100 (3000-4800) • OII emissions to z=2 with 4m aperture • 30% of all nights, 1 hour per exposure(1000sec/exposure), 5M targets/year • 6 (5)year observational period at KPNO + 4 year followup for southern hemisphere at CITO after DES • In north, 30(20)M galaxies over 14,000 square degrees at 0.2<z<2(1.7) + 2M (0.6M) QSOs at 1.8<z<3.5(2.2<z<3.5) • In total, 50(20)M galaxies over 24,000 (14,000) square degrees • Instrument development in 2011-2014 (R&D: 2011-2013, )

9. A proposal to NOAO for the BigBOSS(Oct. 2010) • One-order of improvement in volume and size over the BOSS • ELB: OII line at 3727 ang. • LRG: Balmer break at 4000 ang. • Target selection: Palomar Transient Factory (PTF), PanSTARRS-I, WISE • LRG: 10,000 deg^2 (BOSS) + 4,000 deg^2 (additional) • QSO: first pass (targets: 250/deg^2 for 0<z<3.5) + 1 day break + subsequent passes (targets: 50/deg^2 for 2.2<z<3.5) • BOA scale accuracies: 0.4% for 0.5<z<1 & 0.6% for 1<z<1.7 • Factor of 6 improvement over Stage III BOA experiments • 10-20% of fibers will be used for synchronous sciences (5-10 M spectra) • Rare objects: high-zQSOs, bright lensed galaxies, low metallicity stars, very cool white dwarfs • 16 US institutions + China, France, Korea, Spain and UK • Hardware + software: LBNL, • Operation & management: NOAO+Kitt Peak • Construction of instrument: 2013-2016 • First light in 2016 + start of survey operation in 2017

10. Dec. 2011 DOE R&D Review

11. Organizing Chart (DOE review)

12. BigBOSS Schedule today

13. Key Science Goals • Measure the expansion rate of the universe and growth of structures to sub-percent accuracies between 0<z<3.5 • Neutrino mass, inflationary models, modified gravity • Kinematic/chemical properties of MW stars • Kinematics of stars in open clusters and moving groups • Mapping the ionizing structure and kinematics of IGM

14. Key Sciences details-I • BAO in PS: dA(z), H(z) • Expecting percent level of accuracy in dA(z), H(z) for various z EOS of DE • RSD: f = dlnD/dlna • f≅Ωmϒ • ϒ=6/11 for GR • ϒ≠6/11 for modified gravity or varying eos of DE • Galaxy-lensing cross-correlation • BAO in Ly-a forests (cross correlation between qso forests)

15. Key Sciences details-II • Neutrino properties • Contribution of neutrino to PS • Additional radiation  change of time of ϒ & matter equality • Free-streaming scale  suppressing small-scale power by a few % • 2σ detection of sum of the neutrino masses • Current limits: <0.3eV • σ(Σmν) = 0.024 eV • Constraints on the inflation models • Running spectral index? • Primordial non-Gaussianity: expected σ(fnl) ~ 5

16. Community Sciences • 80% of fibers for core sciences, a few % for calibration, and remains for the synchronous science targets • 4-6 Calibration fields (30-40deg^2): densely sampled with deep spectroscopy ( ex. M31, Sagittarius stream, ND-WFS, COSMOS, SXDF, UDS up to i=22.0 – 22.5) • Galaxy: • Blind Spectroscopic Survey • Deep, Mag-limited sub-survey far below L* • Galaxy cluster (R: 70km/second) • Brightest High-z galaxy • Galaxy environments, central+satellites clustering • AGN • Quasar LF, time evolution at z between 2.2 and 3.5 • Dual super massive BH (double peak & narrow emission line)

17. Summary of BigBOSS Sciences

18. Summary of BigBOSS Sciences

19. Instruments

20. Mayall 4m telescope diagram

21. Instrument (A Proposal to NOAO in Dec. 2010) • Fiber spacing: 145 arcsec ~ 2.5 arc min • Ten three-arm spectrographs & 4kx4k CCDs for each arm

22. Fiber actuator at the prime focus

23. BigBOSS Survey overview • 500 nights for 5 years • Fiber allocation (1000 sec. exposure) • ELS: 0.64 (16.6min) • LRG: 0.2 (33.2min) • QSO: 0.14 (83min) Fiber allocation: fraction of fibers for the observation Fiber completeness: fibers/potential candidates Target selection efficiency: real objects/potential targets

24. Redshift distributions of targets

25. Survey Operation Plan • 2550 ELG + 800LRG + 640QSO + 1000 for sky, calibration stars, ancillary targets • 130 calendar nights/year • 5 tiles for each position • 1 tile for QSO selection (QSO intensive tile) • 4 tiles for ELG, LRG, QSO

26. Survey Maps (1-4 year)

27. BigBOSS한국과학자 그룹 - Korean Participation Group 1. 국가단위연구그룹 (SDSS KPG와 같은 형태)으로 가입. 2013. 3. 2. 유료회원(시니어 멤버; 학생+연구원, 미공개 데이터 사용)과 일반회원(모든 연구자; 공개 데이터 사용)로 구성 3. 시니어 멤버 양종만, 안창림, 박일흥, 김찬주 (이화여대) 박창범, 김주한 (고등과학원) 박병곤, 이준협 (천문연구원) [more] 4. 일반 회원 박명구(경북대), 최윤영(경희대), 박찬경, 임명신(서울대), 안홍배(부산대), 조정연(충남대)………. 이석천, C. Sabiu, 김영래, 황정선, B. L’Huillier, 홍성욱, B. Cervantes-Sodi (고등과학원)

28. Next BigBOSS Collaboration Meeting From Pengjie: • Date: March 27-29, 2013 • Hotel: Ramada hotel, Xujiahui district, Shanghai. Ramada conveniently locates at Shanghai downtown.  SJTU has a nice deal with Ramada and the discount rate is ~ 80 $/day. • Meeting: Minhang campus, Shanghai Jiaotong University (SJTU). It is located in a Shanghai suburb. We will have shuttles in the morning from Ramada to SJTU and from SJTU to Ramada after the meeting. • Registration fee: 1000 RMB (~160$)  to cover banquet,  lunch, coffee break, and other costs (e.g. shuttle/meeting rooms). • We plan to have a cruise banquet at the landmark HuangPu river.

29. Conclusion • BigBOSS: Stage IV ground-based Dark Energy survey • Key-sciences (80% of fibers)+ community science (20% of fibers) • Feasibility of technologies: • 2010-2012: WBS2 (R&D) • 2013- : WBS3 • 2017- : first light?