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Advancements in Wide-Field Astronomy from Space: Insights by Steven Beckwith

This document details the advantages and methodologies of wide-field astronomy conducted from space, highlighting key aspects such as low background noise, photometric stability, and the ability to cover the full sky operating 24 hours. It discusses notable science objectives including the evolution of galaxies, supernova detection, and the study of transient sources. The interplay between space telescope capabilities (HST, SIRTF, Chandra, XMM) and scientific breakthroughs illustrates the profound impact of space-based observations on our understanding of the universe.

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Advancements in Wide-Field Astronomy from Space: Insights by Steven Beckwith

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

  2. Fn (Fn + DW Bn)1/2 A Dn hn ) ( 1/2 t1/2 S/N = Limits: • Space advantages: • Low Bn • Small DW 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 D = 6.5 m q = 0.3” D = 2 m q = l/D

  3. GOODs Legacy & Treasury Programs • Observations • 300 arcmin2 in two fields: HDF-N, CDF-S • SIRTF: 3.6-24 µm (IRAC+MIPS), 600 hours • HST: 4 bands, 500 orbits ACS, near HDF depth • Chandra: 2x106 sec imaging; XMM: ~5x105 sec imaging • Science • Evolution of galaxies, 1 < z < 6 • SN Ia detection via scheduling • AGN morphologies • Potential upgrades: wider fields for AGN, weak-lensing, DEEP fields North South

  4. All sky surveys • Space advantages: • Low Bn • Small DW over large FOV • PSF stability • Photometric stability • Full sky coverage • 24 hr operation • Ground advantages • Large area telescopes • Upgradable detectors (large FOV) • High survey speed at BLIP

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

  6. SN Ia Detection rate 23 z = 1.0 24 LSST 4p 25 z = 1.4 I (mag) WFPC2: 2 orbit 26 z = 1.7 ACS: 2 orbit 27 28 -40 0 40 80 120 Dt (days)

  7. ” 0.080 SN 1998ff A. Riess, F. Boffi & SNaZ Team

  8. Ingress Eclipse Egress HD 209458b: Exoplanet eclipse courtesy Brown et al. (2001) 3 hours 5x10-4 1σ ~ 2x10-4 Kepler selected as Discovery-class Mission

  9. Globular Cluster 47 Tucanae courtesy R. Gilliland et al. (2001) • Contains about 106 stars, at ~11 Gyr HST/WFPC2 • Has a metallicity (abundance of elements heavier than helium) about one third that of the sun DSS

  10. courtesy DMT consortium http://dmtelescope.org/science.html NEO Hazard

  11. Cumulative Distribution of NEAs courtesy DMT consortium http://dmtelescope.org/science.html Follow-up problem ? 4,000 – 77,000 300m

  12. Planned surveys with spacecraft • Galaxy, AGN evolution • HST/ACS, NGST • Supernovae, L • HST/ACS+NICMOS, SNAP • Eclipsing extra-solar planetary systems • Kepler • Astrometric surveys • Hipparcos, SIM, GAIA DW ~ l/D Bn ~ Zodiacal light FOV ~ optics limit

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