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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.

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Presentation on theme: "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."— Presentation transcript:

1 Juhan Kim KIAS

2 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

3 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 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 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 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

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10 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 { "@context": "http://schema.org", "@type": "ImageObject", "contentUrl": "http://images.slideplayer.com/5/1513210/slides/slide_10.jpg", "name": "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

11 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 { "@context": "http://schema.org", "@type": "ImageObject", "contentUrl": "http://images.slideplayer.com/5/1513210/slides/slide_11.jpg", "name": "One-order of improvement in volume and size over the BOSS ELB: OII line at 3727 ang.", "description": "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

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15 Measure the expansion rate of the universe and growth of structures to sub-percent accuracies between 0 { "@context": "http://schema.org", "@type": "ImageObject", "contentUrl": "http://images.slideplayer.com/5/1513210/slides/slide_15.jpg", "name": "Measure the expansion rate of the universe and growth of structures to sub-percent accuracies between 0

16 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)

17 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

18 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)

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

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25 500 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

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27 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

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29 BigBOSS - Korean Participation Group 1. (SDSS KPG ). 2013. 3. 2. ( ; +, ) ( ; ) 3.,,, ( ), ( ), ( ) [more] 4. ( ), ( ),, ( ), ( ), ( )………., C. Sabiu,,, B. LHuillier,, B. Cervantes-Sodi ( )

30 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.

31 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?


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