BigBOSS: Scientific Prospects & Current Status

Juhan KimKIAS

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BigBOSS will enlarge redshift-space maps to 21 million objects10X larger than SDSS + SDSS-II + BOSSNecessary for Stage IV dark energy from BAO, RSD

4 million LRGs

16 million ELGs

0.6 million QSOs

BigBOSS Science Reach

DOE, NSF define Stages for ground-based Dark Energy Surveys

BAO: baryonic Acoustic Oscillation

Stage I: first detection by SDSS-IStage II: SDSS-I, II, Wiggle ZStage III: 3x better than Stage II: BOSS, HETDEXStage IV: 10x better than Stage II: BigBOSS

BigBOSS Timeline

Apr 2009 – BigBOSS white paper submitted to decadal surveyJun 2009 – BigBOSS RFP response to Astro2010 Decadal Survey submitted and

committee oral presentationJul 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 ProgramsMar 2010 – Letter of Intent Submitted to NOAOSep 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

TimelineOct 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 meetingSep 2011 – Third BigBOSS collaboration meeting held in conjunction with a

BigBOSS community workshopDec 2011 – BigBOSS DOE R&D Review. Received a strong endorsement in the

review reportSep 2012 – Mission need of MS-DESI (Mid-scale Dark Energy Spectroscopic

Instrument) signed by DOE Office of Science for Mayall and BlancoOct 2012 – Fourth BigBOSS collaboration meeting (Paris)Dec 2012 – Gordon & Betty Moore Foundation awards $2.1 M grant to BigBOSSMar 2013 – Fifth BigBOSS collaboration meeting (Shanghai)

Astro2010 Decadal Survey

Three major science objectivesCosmic Dawn: Searching for the First Stars, Galaxies, and BHsNew World: Seeking Nearby, Habitable PlanetsPhysics of the Universe: Understanding Scientific Principles

Space Projects , Ground ProjectsWFIRST, Explorer programs, LISA, IXOLSST, GSMT, ACTA

BigBOSS White Paper (arXiv:0904.0468)

BigBOSS White Paper (arXiv:0904.0468)

18 pagesDOE-NSF Stage IV ground-based DE experiment4000(5000)-fiber by automated positioning R=5000 spectroscopic on 3-deg FOV 0.2<z<3.5, LRG, emission line G, QSOsReuses 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 aperture30% of all nights, 1 hour per exposure (1000sec/exposure), 5M targets/year6 (5) year observational period at KPNO + 4 year followup for southern hemisphere at CITO after DESIn 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 degreesInstrument development in 2011-2014 (R&D: 2011-2013, )

A proposal to NOAO for the BigBOSS(Oct. 2010)

One-order of improvement in volume and size over the BOSSELB: OII line at 3727 ang.LRG: Balmer break at 4000 ang.

Target selection: Palomar Transient Factory (PTF), PanSTARRS-I, WISELRG: 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<1.7Factor 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-z QSOs, bright lensed galaxies, low metallicity stars, very cool white dwarfs

16 US institutions + China, France, Korea, Spain and UKHardware + software: LBNL,Operation & management: NOAO+Kitt PeakConstruction of instrument: 2013-2016First light in 2016 + start of survey operation in 2017

Dec. 2011 DOE R&D Review

Organizing Chart (DOE review)

BigBOSS Scheduletoday

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 starsKinematics of stars in open clusters and moving groupsMapping the ionizing structure and kinematics of IGM

Key Sciences details-IBAO 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/dlnaf ≅Ωm

ϒ

ϒ=6/11 for GRϒ≠6/11 for modified gravity or varying eos of DE

Galaxy-lensing cross-correlationBAO in Ly-a forests (cross correlation between qso forests)

Key Sciences details-II

Neutrino propertiesContribution of neutrino to PS

Additional radiation change of time of ϒ & matter equalityFree-streaming scale suppressing small-scale power by a few %

2σ detection of sum of the neutrino massesCurrent limits: <0.3eVσ(Σmν) = 0.024 eV

Constraints on the inflation modelsRunning spectral index?Primordial non-Gaussianity: expected σ(fnl) ~ 5

Community Sciences80% of fibers for core sciences, a few % for calibration, and remains for the synchronous science targets4-6 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 SurveyDeep, Mag-limited sub-survey far below L*Galaxy cluster (R: 70km/second)Brightest High-z galaxyGalaxy environments, central+satellites clustering

AGNQuasar LF, time evolution at z between 2.2 and 3.5Dual super massive BH (double peak & narrow emission line)

Summary of BigBOSS Sciences

Summary of BigBOSS Sciences

Instruments

Mayall 4m telescope diagram

Instrument (A Proposal to NOAO in Dec. 2010)

Fiber spacing: 145 arcsec ~ 2.5 arc minTen three-arm spectrographs & 4kx4k CCDs for each arm

Fiber actuator at the prime focus

BigBOSS Survey overview500 nights for 5 yearsFiber 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

Redshift distributions of targets

Survey Operation Plan2550 ELG + 800LRG + 640QSO + 1000 for sky, calibration stars, ancillary targets130 calendar nights/year5 tiles for each position

1 tile for QSO selection (QSO intensive tile)4 tiles for ELG, LRG, QSO

Survey Maps (1-4 year)

BigBOSS 한국과학자 그룹 - Korean Participation Group

1. 국가단위연구그룹 (SDSS KPG 와 같은 형태 ) 으로 가입 . 2013. 3.

2. 유료회원 ( 시니어 멤버 ; 학생 + 연구원 , 미공개 데이터 사용 ) 과일반회원 ( 모든 연구자 ; 공개 데이터 사용 ) 로 구성

3. 시니어 멤버양종만 , 안창림 , 박일흥 , 김찬주 ( 이화여대 )박창범 , 김주한 ( 고등과학원 )박병곤 , 이준협 ( 천문연구원 ) [more]

4. 일반 회원박명구 ( 경북대 ), 최윤영 ( 경희대 ), 박찬경 , 임명신 ( 서울대 ), 안홍배 ( 부산대 ), 조정연 ( 충남대 )……….이석천 , C. Sabiu, 김영래 , 황정선 , B. L’Huillier, 홍성욱 , B. Cervantes-Sodi (고등과학원 )

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.

Conclusion

BigBOSS: Stage IV ground-based Dark Energy surveyKey-sciences (80% of fibers)+ community science (20% of fibers)Feasibility of technologies:

2010-2012: WBS2 (R&D)2013- : WBS32017- : first light?