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The Dark Energy Survey (DES)

The Dark Energy Survey (DES). Sarah Bridle, UCL On behalf of the DES Collaboration. The Dark Energy Survey. Blanco 4-meter at CTIO. Study Dark Energy using 4 complementary techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations

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The Dark Energy Survey (DES)

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  1. The Dark Energy Survey (DES) Sarah Bridle, UCL On behalf of the DES Collaboration

  2. The Dark Energy Survey Blanco 4-meter at CTIO • Study Dark Energy using 4 complementary techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae • Two multi-band surveys 5000 deg2g, r, i, z 40 deg2 repeat (SNe) • Build new 3 deg2 camera and data management system Survey 2010-2015 (525 nights) Response to NOAO AO 300,000,000 photometric redshifts

  3. The Dark Energy Survey Blanco 4-meter at CTIO • Study Dark Energy using 4 complementary techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae • Two multi-band surveys 5000 deg2g, r, i, z 40 deg2 repeat (SNe) • Build new 3 deg2 camera and data management system Survey 2010-2015 (525 nights) Response to NOAO AO 300,000,000 photometric redshifts

  4. The DES Collaboration Fermilab: J. Annis, H. T. Diehl, S. Dodelson, J. Estrada, B. Flaugher, J. Frieman, S. Kent, H. Lin, P. Limon, K. W. Merritt, J. Peoples, V. Scarpine, A. Stebbins, C. Stoughton, D. Tucker, W. Wester University of Illinois at Urbana-Champaign: C. Beldica, R. Brunner, I. Karliner, J. Mohr, R. Plante, P. Ricker, M. Selen, J. Thaler University of Chicago:J. Carlstrom, S. Dodelson, J. Frieman, M. Gladders, W. Hu, S. Kent, R. Kessler, E. Sheldon, R. Wechsler Lawrence Berkeley National Lab: N. Roe, C. Bebek, M. Levi, S. Perlmutter University of Michigan: R. Bernstein, B. Bigelow, M. Campbell, D. Gerdes, A. Evrard, W. Lorenzon, T. McKay, M. Schubnell, G. Tarle, M. Tecchio NOAO/CTIO: T. Abbott, C. Miller, C. Smith, N. Suntzeff, A. Walker CSIC/Institut d'Estudis Espacials de Catalunya (Barcelona):F. Castander, P. Fosalba, E. Gaztañaga, J. Miralda-Escude Institut de Fisica d'Altes Energies (Barcelona):E. Fernández, M. Martínez CIEMAT (Madrid): C. Mana, M. Molla, E. Sanchez, J. Garcia-Bellido University College London: O. Lahav, D. Brooks, P. Doel, M. Barlow, S. Bridle, S. Viti, J. Weller University of Cambridge:G. Efstathiou, R. McMahon, W. Sutherland University of Edinburgh:J. Peacock University of Portsmouth: R. Crittenden, R. Nichol, R. Maartnes, W. Percival University of Sussex: A. Liddle, K. Romer plus postdocs and students

  5. The Dark Energy Survey UK Consortium (I) PPARC funding: O. Lahav (PI), P. Doel, M. Barlow, S. Bridle, S. Viti, J. Weller (UCL), R. Nichol (Portsmouth), G. Efstathiou, R. McMahon, W. Sutherland (Cambridge) J. Peacock (Edinburgh) Submitted a proposal to PPARC requesting £ 1.7M for the DES optical design. In March 2006, PPARC Council announced that it “will seek participation in DES”. PPARC already approved £220K for current R&D. (II) SRIF3 funding: R. Nichol, R. Crittenden, R. Maartens, W. Percival (ICG Portsmouth) K. Romer, A. Liddle (Sussex) Funding the optical glass blanks for the UCL DES optical work These scientists will work together through the UK DES Consortium. Other DES proposals are under consideration by US and Spanish funding agencies.

  6. The Dark Energy Survey Camera: DECam DECam will replace the prime focus cage 4m Blanco telescope

  7. Expected performance of DECAM, Blanco, and CTIO site

  8. DeCamOptical Lay Out C1 C2 C3 C4 C5 978mm Filter 1870mm

  9. i zenith 0

  10. DES and VISTA synergy DES (griz) DES+VISTA(JK) VISTA J (<21) and K (<19) would improve photo-z by a factor of 2 for z>1 F. Abdalla, M. Banerji, OL, H. Lin, et al.

  11. DES Forecasts: Power of Multiple Techniques w(z) =w0+wa(1–a) 68% CL Assumptions: Clusters: 8=0.75, zmax=1.5, WL mass calibration BAO:lmax=300 WL:lmax=1000 (no bispectrum) Statistical+photo-z systematic errors only Spatial curvature, galaxy bias marginalized, Planck CMB prior Factor 4.6 improvement over Stage II DETF Figure of Merit: inverse area of ellipse

  12. DES Forecast Constraints DETF FoM • DES+Stage II combined = Factor 4.6 improvement over Stage II combined • Consistent with DETF range for Stage III DES-like project • Large uncertainties in systematics remain, but FoM is robust to uncertainties in any one probe, and we haven’t made use of all the information

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