Decadal Survey Town Hall Berkeley, 29 Nov BigBOSS

Transcription

1 Decadal Survey Town Hall Berkeley, 29 Nov 2010 BigBOSS David Schlegel, Lawrence Berkeley National Lab Astro2010 Town Hall, 29 Nov

2 Why map the sky? Earliest maps of the Universe were limited CfA2 galaxy redshift map (Geller & Huchra 1989) Correlation function What did we learn? Galaxy (~matter) fluctuations are ~Gaussian, scale-free Grav. growth explains CMB fluctuations galaxy Astro2010 Town Hall, 29 Nov

3 Why map the sky? Today s maps of the Universe SDSS galaxy redshift map Turn-over depends upon horizon size at matterradiation equality Sound horizon scale at recombination (BAO) Text Galaxy halo occupation of dark matter halos (HOD) Nonlinear growth Astro2010 Town Hall, 29 Nov

4 Dark Energy discovery in 1998 with supernovae Contradicted what we knew : lack of strong lenses said no acceleration Type Ia Supernovae Relative brightness fainter magnitude Perlmutter, Physics Today (2003) Supernova Cosmology Project High-Z Supernova Search Calan/Tololo 25 Supernova Survey Accelerating Universe with vacuum energy without vacuum energy 0 empty mass density 1 21 Decelerating Universe redshift Astro2010 Town Hall, 29 Nov 2010 Scale of the Universe 4 [relative to today's scale]

5 Dark Energy Task Force (DETF) report (June 2006) The Big 4 techniques: I. Baryon Acoustic Oscillations (BAO) Sound scale in distribution of galaxies: d A (z) and H(z). II. Clusters (CL) Spatial distribution of galaxy clusters: d A (z), H(z) Growth of structure III. Supernovae (SN) Flux and redshift of Type Ia SNe: d L (z). IV. Weak Lensing (WL) Distortion of background images due to grav. lensing: d A (z) NSF + DOE + NASA Growth of structure DETF defines progressive capabilities: Stage I: knowledge ca Stage II: running experiments BAO Stage III: near-term experiments, ie. SDSS-III/BOSS BAO Stage IV: BigBOSS Astro2010 Town Hall, 29 Nov

6 Dark Energy Task Force (DETF) report (June 2006) The Big 4 techniques: I. BAO d A (z) and H(z). II. Clusters (CL) d A (z), H(z) Growth III. Supernovae (SN) d L (z). IV. Weak Lensing (WL) d A (z) Growth These are the direct observables Each measurement is low S/N: ~1 for SN, ~0.01 for WL,... Ultimately limited by systematic errors of each technique Astro2010 Town Hall, 29 Nov

7 DOE does not fund astronomy DOE does fund non-accelerator physics Dark energy Dark matter Neutrinos Astro2010 are astronomy recommendations Astro2010 Town Hall, 29 Nov

8 NOAO > KPNO Home NOAO telescope call Nov 18, 2009 ReSTAR program implementation by NOAO Announcement of Opportunity for Large Science Programs Providing New Observing Capabilities for the Mayall 4m Telescope on Kitt Peak NOAO announces an opportunity to partner with NOAO and the National Science Foundation to pursue a large science program with the Mayall 4-meter telescope on Kitt Peak and to develop a major observing capability (instrument, software, and archival plans) for the Mayall 4-meter telescope of the Kitt Peak National Observatory for the purpose of enabling large, high impact science programs and improving the capabilities provided as part of the U.S. System of ground-based optical and near-ir telescopes. Projects that use a diverse range of observing requirements (e.g. time of year, lunar phase, etc.) are encouraged. The dual goals of the large science program, as discussed in a recent edition of NOAO Currents are to enable frontier science and to improve the U.S. system of ground-based ØIR facilities. Although there are no restrictions on the type or scale Astro2010 of Town instrument, Hall, NOAO 29 Nov encourages 2010 proposals that will build 8 on the Mayall telescope s strengths, utilizing its unique wide-field capabilities. NOAO has investigated potential

9 BigBOSS proposal submitted Oct 1, 2010 A Proposal to NOAO for the BigBOSS Experiment at Kitt Peak National Observatory October 1, 2010 D. Schlegel p, F. Abdalla z, C. Ahn g, C. Allende-Prieto j, J. Annis h, E. Aubourg a, M. Azzaro i, C. Baltay ii, C. Baugh f,c.bebek p,s.becerril i, M. Blanton s, A. Bolton gg, B. Bromley gg, R. Cahn p, P.-H. Carton c, Y. Chu ff, M. Cortês p,x, K. Dawson gg, A. Dey r, H. T. Diehl h,p.doel z, A. Ealet d,j.edelstein x,d.eppelle c,s.escoffier d, A. Evrard cc, L. Faccioli p,x,c.frenk f,m.geha ii,d.gerdes cc, P. Gondolo gg, A. Gonzolez-Arroyo m, B. Grossan x, T. Heckman n, H. Heetderks x, S. Ho p, K. Honscheid u, D. Huterer cc, O. Ilbert o, I. Ivans gg,p.jelinsky x, Y. Jing v,s.kent h,d.kieda gg,c.kim g,j.-p.kneib o, X. Kong ff, A. Kosowsky dd, K. Krishnan g, O. Lahav z, M. Lampton x, S. LeBohec gg, V. Le Brun o, M. Levi p, H. Lim g, E. Linder g,x, W. Lorenzon cc, Ch. Magneville c, R. Malina o, C. Marinoni e, V. Martinez t,s.majewski hh, P. McDonald p,t.mckay cc, J. McMahon cc, B. Menard n, J. Miralda-Escude l, M. Modjaz s, N. Mostek p,x, J. Newman dd, R. Nichol ee, P. Nugent p,x,k.olsen r, N. Padmanabhan ii, I. Park g, J. Peacock aa, W. Percival ee, S. Perlmutter p,x, C. Peroux o, P. Petitjean k, F. Prada i,e.prieto o, J. Prochaska y,k.reil w, C. Rockosi y, N. Roe p, E. Rollinde k, A. Roodman w, N. Ross p,g.rudnick bb, V. Ruhlmann-Kleider c,c.schimd o,m.schubnell cc, R. Scoccimaro s, U. Seljak g,p,x, H. Seo x, M. Sholl x, R. Shulte-Ladbeck dd, A. Slosar b, G. Smoot g,p,x, W. Springer gg, A. Stril p, A. Szalay n, C. Tao d, G. Tarlé cc, E. Taylor x, A. Tilquin d,j.tinker s, J. Wang ff, T. Wang ff, B. A. Weaver s,d.weinberg u,m.white p,x, M. Wood-Vasey dd, J. Yang g, Ch. Yèche c, N. Zakamska n, A. Zentner dd, C. Zhai ff, P. Zhang v a Astrophysique, Particules et Cosmologie Laboratoire (APC), Paris b Brookhaven National Laboratory c CEA/IRFU, Saclay d Centre de Physique des Particules de Marseille e Centre de Physique Theorique, Université de Marseille f Durham University g Ewha Womans University, Korea h Fermi National Accelerator Laboratory Astro2010 Town Hall, 29 Nov

10 BigBOSS proposal submitted Oct 1, 2010 The proposal contains: Construct BigBOSS instrument: 3 deg diameter FOV prime focus corrector 5000 fiber positioner 10x3 spectrographs, ,600 Ang Conduct BigBOSS Key Project 500 nights at Mayall 4-m 14,000 deg 2 survey 50,000,000 spectra 20,000,000 galaxy redshifts 600,000 QSO spectra Astro2010 Town Hall, 29 Nov

11 BigBOSS Science Goals BAO z=0 3.5 near cosmic-variance limit RSD (redshift-space distortions) z=0 3.5 Neutrino masses Galaxy density map for weak lensing Detect non-gaussianity Astro2010 Town Hall, 29 Nov

12 BigBOSS Science Goals BAO z=0 3.5 near cosmic-variance limit RSD (redshift space distortions) z=0 3.5 Neutrino masses Galaxy density map for weak lensing Detect non-gaussianity BigBOSS Design Philosophy Optimize for z s only Simple design high throughput Full-sky Much more capable w/ public-access time Astro2010 Town Hall, 29 Nov

13 BigBOSS Stage IV BigBOSS designed to measures dark energy from the BAO standard ruler 1. Spectroscopic survey of ~20 million galaxies at 0 < z < Spectroscopic survey of ~600k QSOs at 2.2 < z < 3.5 Definitive BAO experiment at 0 < z < 1.5 Inflation probe exceeding reach of Planck satellite Galaxies 10X volume of BOSS More linear modes; full power not yet explored QSOs Astro2010 Town Hall, 29 Nov

14 Instrument: Telescope Kitt Peak 4-m (Mayall) at Kitt Peak, Arizona today Astro2010 Town Hall, 29 Nov

15 5000 fiber positioners on 1-m focal plane, f/4.5 Corrector lenses 3 FOV Instrument: Telescope Kitt Peak 4-m (Mayall) at Kitt Peak, Arizona in 6 years SDSS-inspired: simple, high-throughput 5000 fibers 10 spectrographs X 3 channels each Astro2010 Town Hall, 29 Nov

16 Instrument: Telescope New family of optical designs discovered for 3-deg field on Mayall telescope; Cassegrain designs - Mike Sholl Prime focus designs - Ming Liang 1-m focal plane at f/4.5 Physical space for fibers: 5x larger than DES, 2.8x HyperSuprime Astro2010 Town Hall, 29 Nov

17 Instrument: Telescope optics Only a handful of 4-m telescopes suitable to a wide-field survey KPNO 4-m CTIO 4-m CFHT 3.6-m Calar Alto 3.5-m ARC 3.5-m (Apache Point) WIYN 3.5-m (Kitt Peak) Discovery Channel 4.2-m WHT 4.2-m ESO 3.6-m SOAR 4.2-m UKIRT 3.8-m Galileo 3.58-m ESO NNT 3.58-m VISTA 4-m AAT 3.9-m 3-deg possible National treasures! 2-deg exists Astro2010 Town Hall, 29 Nov

18 Targets: Easy target survey Luminous Red Galaxies (LRGs): - Selected to z<1 - Efficient BAO tracers due to large bias Emission-line galaxies: Selected 0.7<z<1.7 at source density of dn/(dz deg 2 )=2000 Redshifts from [O II], [O III] emission lines, R~5000 QSOs: - Target all of them! - 3-D density map from Ly-alpha forest z>2.2 Astro2010 Town Hall, 29 Nov

19 BigBOSS timeline Apr 2009 White paper Nov 2009 DOE Particle Astrophysics Science Advisory Group (PASAG) BigBOSS is in the early planning stages, but presents a legitimate possibility of achieving a significant fraction of the BAO science goals for JDEM at <$100M cost. Substantial immediate support is recommended for BigBOSS R&D so that ground BAO possibilities are known for timely planning of a coherent ground-space dark energy effort. Nov 2009 NOAO call Large Science Programs Providing New Observing Capabilities for the Mayall 4m Telescope on Kitt Peak Aug 2010 Astro2010 Decadal Survey BigBOSS highly recommended as 1 of 4 Projects Thought Compelling for the Mid-Scale Innovations Program in the cost range $US million. Oct 2010 Telescope proposal 19

20 BigBOSS timeline Full-sky BAO survey possible by moving instrument south after Kitt Peak 4-m (Northern hemisphere) BigBOSS instrument deployable between sister telescopes Enables massive spectroscopic follow-up for LSST Cerro Tololo 4-m (Southern hemisphere) 20