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UV and Infrared Astronomy

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UV and Infrared Astronomy Why Put a Telescope In Space? • Access to light that does not penetrate the atmosphere • No seeing. A telescope can reach the diffraction limit: 1.22 l/D radians Astronomy in Space. I. UV Astronomy Ultraviolet Astronomy 912-3650 Å (Lyman Limit to Balmer jump) • Continuua of hot stars (spectral types O,B,A) • H I Lyman lines (1-n transitions) • Resonance lines of Li-like ions C IV, N V, O VI • H2 Lyman and Werner bands Normal incidence optics • Special UV-reflective coatings The Far Ultraviolet 912 to 1150 Å • Defined by Lyman limit, MgF cutoff at 1150 Å • LiF + Al reflects longward of 1050 Å • SiC reflects at shorter wavelengths The Astronomy Quarterly, Vol. 7, pp. 131-142, 1990 0364-9229f90 $3.00+.00 Printed in the USA. All rights reserved. Copyright (c) 1990 Pergamon Press plc ASTRONOMICAL ADVANTAGES History OFAN • 9/1/1946: Lyman Spitzer EXTRA-TERRESTRIAL OBSERVATORY proposed a Space Telescope in LYMAN SPITZER, Jr. ’ a Report to project Rand This study points out, in a very preliminary way, the results that might be expected from astronomical measurements made with a satellite • 1966: Spitzer (Princeton) vehicle. The discussion is divided into three parts, corresponding to three different assumptions concerning the amount of instrumentation provided. chairs NASA Ad Hoc In the first section it is assumed that no telescope is provided; in the second a 10-&h reflector is assumed; in the third section some of the results Committee on the "Scientific obtainable with a large reflecting telescope, many feet in diameter, and revolving about the earth above the terrestrial atmosphere, are briefly Uses of the Large Space sketched. Telescope” It should be emphasized that this is only a preliminary survey of the scientific advantages that astronomy might gain from such a development. The many practical problems, which of course require a • 1972: OAO-3 (Copernicus) detailed solution before such a satellite might become possible, are not considered, although some partial mention is made of certain problems of launched. 0.8m mirror. purely astronomical instrumentation. The discussion of the astronomical results is not intended to be complete, and covers only certain salient Obtained spectra (900-3150Å) features. While a more exhaustive analysis would alter some of the details of the present study, it would probably not change the chief conclusion -- of 551 objects that such a scientific tool, if practically feasible, could revolutionize ’ The report re-printed here appeared as Appendix V of a larger document prepared for the Project RAND of the Douglas Aircraft Co., on 1 September 1946. At that time, Prof. Spitzer was on the astronomy faculty of Yale University; he has been affiliated with the Princeton University Observatory since 1947. 131 International Ultraviolet Explorer • Launched 1978; Decommissioned 1996 • Geosynchronous orbit; real-time operations • 0.45m mirror • 4 redundant cameras • 1150-2000Å • 1850-3300Å • Resolutions: 0.2, 6Å • Vidicon detector The Hubble Space Telescope • 1971: NASA Large Space Telescope Steering Group • Proposes 3m mirror • Estimated cost $300-500M • 1975: Congress rejects LST • NASA descoped to 2.4m Space Telescope • Estimated cost $200M • Bahcall and Spitzer lobby Congress • 1975: NASA Issues Call for proposals for the Space Telescope • 1977: Congress authorizes ST for 1983 launch • 1981: Mirror completed • 1984: OTC completed • 1985: S/C assembled • 1986: STS Challenger explodes • 4/24/90: Hubble Space Telescope placed on orbit The Hubble Space Telescope Concept • A large diffraction-limited UV/optical telescope above the atmosphere • 2.4m Ritchey-Chretien; f/24 • range: 1100Å to 3 µm • plate scale: 3.58 arcsec/mm • FWHM at 5000Å: 0.043 arcsec • Encircled Energy at 5000Å: 87% within 0.1 arcsec • Serviceable by astronauts • Instruments can be replaced and upgraded • Gyros, batteries, computer, memory all replaceable (and upgradable) • Minimize moving parts and expendables 4/24/90 HST Computer DF-224 • 1.25 MHz • 80386 processor + 80387 math co-processor • Upgraded to 25 MHz 80406 processor in 1999 Original Instruments • FOC – Faint Object Camera (UV + optical) • GHRS – Goddard High Resolution Spectrograph (UV) • HSP – High Speed Photometer (UV and optical) • FOS – Faint Objects Spectrograph (UV and optical) • WFPC – Wide Field and Planetary Camera (UV + optical) • FGS – Fine Guidance Sensors. Primarily to hold S/C steady, but could also do precision astrometry First Light Images Spherical Aberration What Went Wrong? Mirror polishing Perkin-Elmer Corp. Danbury CT What Went Wrong. I. It is easy to test a mirror for deviations from sphericity • Perkin-Elmer designed a Reflective Null Corrector (RNC) to “correct” the mirror shape to appear spherical • The position of the field lens was set by a rod positioned by laser interferometry • The end of the rod was polished, and held in place by an anodized (black) flange. • A simpler inverse null corrector (INC) was used to test the RNC. • The INC showed the RNC had spherical aberration. What Went Wrong. II. The INC result was dismissed because it was less accurate than the RNC The mirror was polished to 8 nm RMS (0.014 waVes at 632.8 nm) - better than specifications Nobody noticed that: • The black anodized coating had been scratched – the laser was reflecting off the flange rather than the end of the rod. The field lens was 1.3mm off • It too longer than expected to grind the mirror • More glass was removed than expected The Difference Between Accuracy and Precision • HST has most precisely ground and polished mirror ever made for Astronomy • It is the wrong shape. • Fortunately, spherical aberration is easily correctible – at a cost of $40-$50M Servicing Missions SM 1 December 1993 • Replaced HSP with CoSTAR • Space Telescope Axial Replacement • Pairs of corrective optics for GHRS, FOS • Replaced WFPC with WFPC2 • Internal optics correct for primary mirror • Replaced Gyros, Solar Panels Post Co-STAR Imaging Servicing Missions SM 2 February 1997 • Replaced GHRS with STIS (UV/optical spectrograph) • Replaced FOC with NICMOS (Near IR imager) • Installed solid-state memory • Refurbished FGS • Replaced Gyros, Solar Panels Servicing Missions SM 3a February 1997 • Installed new computer (486 chip) • Refurbished FGS Replaced Gyros, Solar Panels SM 3b March 2002 • Replaced CoSTAR with ACS – Advanced Camera for Surveys • Installed cryocooler for NICMOS • Replaced Gyros, Solar Panels, batteries Servicing Missions SM 4 May 2009 • Replaced WFPC2 with WFC3 • Repaired STIS, ACS • Replaced FGS Replaced Gyros, Solar Panels, Batteries Added new thermal blankets Added soft capture mechanism for de-orbit Hubble Today (SM4: 2009) Hubble Today The HST Focal Plane HST Capabilities Spectroscopic • STIS: • MAMA: 1140 - 3180Å; R = 500 - 114,000 • CCD: 1640 - 10400Å; R = 530 – 10,300 • COS: • FUV: 900 - 2150Å; R = 1500 – 20,000 • NUV: 1700 - 3200Å; R = 2100 – 24,000 Imaging • ACS: • SBC: 0.03” pixels; 30x34” field; 1150-1700Å • WFC: 0.05” pixels; 202x202” field; 3500-11,000Å • WFC3: • UVIS: 0.04” pixels; 162x162” field; 2000-10,000Å • IR: 0.13”pixels (HgCsTe); 136x123” field; 8000-17,000Å • STIS: • MAMA: 0.025” pixels; 25x25” field; 1150-2000Å • CCD: 0.05”pixels; 52x52” field; 2000-10,300Å What’s Next? Astronomy in Space. II. IR Astronomy Atmospheric Transmission Source: Yoshii et al., SPIE2010 Near-IR Astronomy Science: • Photospheres of cool stars • Thermal emission from dust Optics: • Normal incidence Detectors: • Bolometers • Solid state devices with small work functions • HgCdTe (0.6 – 5 µm); InSb (5 -28 µm) Observing Techniques Sky is bright • Use chopping or nodding • The median of N(>2) images is the sky • Subtract the sky, then shift and add. Near-IR Telescopes • IRTF 3m Mauna Kea • Sofia 2.5m airborne • IRAS • Spitzer Space Telescope Future Missions • JWST • WFIRST (?).
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