Juhan Kim KIAS

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 2

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

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

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)

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

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

) + 2M ( 0.6M

) QSOs at 1.8

) In total, 50( 20 )M galaxies over 24,000 ( 14,000 ) square degrees Instrument development in 2011-2014 ( R&D: 2011-2013 , )

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

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-z QSOs, 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

today

Measure the expansion rate of the universe and growth of structures to sub-percent accuracies between 0

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

BAO in PS: d A accuracy in d (z), H(z) Expecting percent level of A (z), H(z) for various z  EOS of DE RSD: f = dlnD/dlna f ≅ Ω m ϒ 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)

Neutrino properties

Contribution of neutrino to PS Additional radiation  equality change of time of ϒ & matter Free-streaming scale  a few % suppressing small-scale power by 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

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)

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

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

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

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 ) 과 일반회원 ( 모든 연구자 ; 공개 데이터 사용 ) 로 구성 3. 시니어 멤버 양종만 , 안창림 박창범 , 김주한 박병곤 , 이준협 , 박일흥 , 김찬주 ( 이화여대 ) ( 고등과학원 ) ( 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 )

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

from SJTU to Ramada after the meeting.

(SJTU). It is located in a Shanghai suburb. We will have shuttles in the morning from Ramada to SJTU and 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.

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?