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Euclid Mission: baseline and options Ref: Euclid RB Laureijs et al arXiv:1110.3193 15,000 deg 2 40 deg 2 In ~6 years Shapes + Photo-z <strong>of</strong> n = 1.5 x10 9 galaxies z <strong>of</strong> n=5x10 7 galaxies Weak Lensing Photo-z BAO Euclid slides from Yannick Mellier
The VIS instrument Courtesy: S. Pottinger, R. Cole, M. Cropper and the VIS team (wide band channel)
Page 1 and 2: Optical/NIR Imaging Surveys Josh Fr
Page 3 and 4: 3 Brief Survey of New Imaging Surve
Page 5 and 6: 5 Dark Energy • What is the physi
Page 7 and 8: 7 • Clusters are proxies for mass
Page 9 and 10: Cosmic Shear Tomography
Page 11 and 12: 11 Galaxy angular power spectrum in
Page 13 and 14: 13 Photometric SN Cosmology • Hub
Page 16 and 17: 16 The Dark Energy Survey • Surve
Page 18 and 19: 18 DECam CCDs • 62 2kx4k fully de
Page 20 and 21: DECam First Light September 12, 201
Page 23 and 24: High Redshift Cluster Discovered by
Page 25 and 26: DECam composite image of deep SN fi
Page 27 and 28: Science Verification: fewx100 sq de
Page 29 and 30: R. Mandelbaum Picture credit: S. Mi
Page 31 and 32: Seeing variation across FOV 104 Sci
Page 33 and 34: Takada R. Mandelbaum 33
Page 36 and 37: Summary of High Level Requirements
Page 38 and 39: The telescope mount has been optimi
Page 40 and 41: Recent Progress: M1/M3
Page 44 and 45: The NISP Instrument Courtesy: T. Ma
Page 46 and 47: Photometric redshifts with Euclid M
Page 48 and 49: Astrophysics Focused Telescope Asse
Page 50 and 51: AFTA Instruments Wide-‐Field In
Page 52 and 53: AFTA is a more capable dark energy
Page 54 and 55: AFTA and Euclid have complementary
Page 56: AFTA will have the sensiAvity and t

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