Juhan Kim KIAS

2 2 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 4 million LRGs 16 million ELGs 0.6 million QSOs

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<z<3.5, LRG, emission line G, QSOs Reuses BOSS spectrograph & pipeline designs (NYU) 4m Mayall telescope at KPNO (3degree diameter) 10 spectrographs covering (1060)nm, R= ( ) 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 (R&D: , )

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-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: First light in start of survey operation in 2017

today

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

BAO in PS: d A (z), H(z) Expecting percent level of accuracy in d A (z), H(z) for various z EOS of DE RSD: f = dlnD/dlna f Ω m ϒ ϒ=6/11 for GR ϒ6/11 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 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) = 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 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 - Korean Participation Group 1. (SDSS KPG ) ( ; +, ) ( ; ) 3.,,, ( ), ( ), ( ) [more] 4. ( ), ( ),, ( ), ( ), ( )………., C. Sabiu,,, B. LHuillier,, B. Cervantes-Sodi ( )

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.

BigBOSS: Stage IV ground-based Dark Energy survey Key-sciences (80% of fibers)+ community science (20% of fibers) Feasibility of technologies: : WBS2 (R&D) : WBS : first light?