PAU camera

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FOM 1/σ(w0) σ(wa) 1/σ(γ) 1/σ(w0) σ(wa)σ(γ)DES (MAG) 47 (109) 35 (48) 1.6 (5) x 10 3 DESpec (MAG) 116 (401) 77 (84) 9 (34) x 10 3 DESpec (MAG+RSD) 1430 (1736) 127 (141) 182 (245) x 10 3 <strong>PAU</strong>200 (MAG+RSD) 171 (195) 31 (33) 5 (6) x 10 3 Om - ODE - h - sig8 - Ob - w0 - wa - gamma - ns - b1- db1dz- b2- db2dz+Planck+ Stage-SN II (assume bias is known)FoM 5 8 25 17 200 DESpec/DES:Factor of 4 in Growth & 30 in DEfactor of 10 in joinned FoM
• Galaxy evolution<strong>PAU</strong> SurveyAlthough the survey is designed and optimized for DE,many other science topics could be addressed• Galactic astronomy• High redshift galaxies• Interstellar dust• Quasars and Lyα systems• Clusters• Stellar populations• Halo stars• Local group galaxies• Serendipitous discoveries• Weak gravitational lensing• Strong gravitational lensing
Page 1 and 2: Cosmology with AccuratePhotometric
Page 3 and 4: Survey requirements• The precisio
Page 5 and 6: The trickPAU survey• Use photomet
Page 7 and 8: Requirements on Redshift Precisions
Page 10 and 11: Lensing Magnification• Lensing ef
Page 12 and 13: PAU survey• The main goal of the
Page 14 and 15: The PAU CameraO. Ballester(2), L. C
Page 16 and 17: The PAU CameraTelescopio William He
Page 18 and 19: The PAU CameraTelescopio William He
Page 20 and 21: The PAU CameraCamara efficiency•F
Page 22 and 23: The PAU CameraDistribution22
Page 24 and 25: The PAU CameraFilters40 narrow band
Page 26 and 27: The PAU CameraFilter TraysNeed to b
Page 28 and 29: The PAU CameraElectronicsMonsoon a
Page 30 and 31: The PAU Camera30
Page 32: PAU survey• The PAU survey collab
Page 35: PAU survey• The PAU collaboration
Page 39: DES landscape• If and when LSST o

PAU camera

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