Wide Field Astronomy from Space Steven Beckwith Space Telescope Science Institute January 9, 2002

1/9/20022 Limits: Space advantages:  Low B  Small  over FOV  PSF stability  Photometric stability  Full sky coverage  24 hr operation Ground advantages  Large area telescopes  Upgradable detectors (increase/repair FOV)  High survey speed at BLIP S/N = t 1/2 A  h F (F +  B ) 1/2 1/2 ( ) D = 6.5 m  = 0.3 ” D = 2 m  = /D

1/9/20023 ACS Survey Workshop Motivation: Motivation:  To determine the potential for new surveys with ACS  To identify areas for teaming on large initiatives Discussion findings: Discussion findings:  Obvious synergism between galaxy formation, AGN evolution, weak lensing, and cosmology (SN Ia) in need for a ~1  ° HDF-like survey  Recognition of multiple science potential of deep and wide surveys with HST March 2001

1/9/20024 GOODs Legacy & Treasury Programs Observations Observations  300 arcmin 2 in two fields: HDF-N, CDF-S  SIRTF: µm (IRAC+MIPS), 600 hours  HST: 4 bands, 500 orbits ACS, near HDF depth  Chandra: 2x10 6 sec imaging; XMM: ~5x10 5 sec imaging NorthSouth Science Science  Evolution of galaxies, 1 < z < 6  SN Ia detection via scheduling  AGN morphologies  Potential upgrades: wider fields for AGN, weak-lensing, DEEP fields

1/9/20025 All sky surveys Space advantages:  Low B  Small  over large FOV  PSF stability  Photometric stability  Full sky coverage  24 hr operation Ground advantages Ground advantages  Large area telescopes  Upgradable detectors (large FOV)  High survey speed at BLIP

1/9/20026 Ideal limiting magnitudes Space-survey science: Earth-crossing asteroids (sens.) Earth-crossing asteroids (sens.) Kuiper-belt objects (sens.,  ) Kuiper-belt objects (sens.,  ) Transient sources Transient sources  Supernovae (e.g. SN Ia) (sens.)  Micro-lensing sources (# stars) Dwarf stars: white, brown (sens.) Dwarf stars: white, brown (sens.) Quantify weak lensing in distant galaxies (small , stable PSF) Quantify weak lensing in distant galaxies (small , stable PSF) Parallaxes of faint stars (sens.) Parallaxes of faint stars (sens.) Rare objects (survey to R ~ 27 m ) Rare objects (survey to R ~ 27 m ) Eclipses of exo-planets (photometric stability) Eclipses of exo-planets (photometric stability) High z SN DMT 8.4m

1/9/  t (days) I (mag) z = 1.7 z = 1.4 z = 1.0 SN Ia Detection rate WFPC2: 2 orbit ACS: 2 orbit LSST 4 

1/9/20028 SN 1998ff A. Riess, F. Boffi & SNaZ Team ”

1/9/20029 HD b: Exoplanet eclipse 3 hours Ingress EclipseEgress 1σ ~ 2x x10 -4 Kepler selected as Discovery-class Mission courtesy Brown et al. (2001)

1/9/ Has a metallicity (abundance of elements heavier than helium) about one third that of the sun HST/WFPC2 DSS Globular Cluster 47 Tucanae Contains about 10 6 stars, at ~11 Gyr courtesy R. Gilliland et al. (2001)

1/9/ NEO Hazard courtesy DMT consortium

1/9/ Cumulative Distribution of NEAs 300m 4,000 – 77,000 Follow-up problem ? courtesy DMT consortium

1/9/ Planned surveys with spacecraft Galaxy, AGN evolution Galaxy, AGN evolution  HST/ACS, NGST Supernovae,  Supernovae,   HST/ACS+NICMOS, SNAP Eclipsing extra-solar planetary systems Eclipsing extra-solar planetary systems  Kepler Astrometric surveys Astrometric surveys  Hipparcos, SIM, GAIA  ~ /D B ~ Zodiacal light FOV ~ optics limit