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FEB 08 TUNA: SUPPS, EX, ALTS

FEB 08 TUNA: SUPPS, EX, ALTS. Rate Sensor Units (“Gyros”). A RGA system consists of a Rate Sensor Unit (RSU) and an Electronic Control Unit (ECU): Three RSUs are attached to the Optical Telescope Assembly (OTA) and accessed through the Aft Shroud

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FEB 08 TUNA: SUPPS, EX, ALTS

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  1. FEB 08 TUNA: SUPPS, EX, ALTS

  2. Rate Sensor Units (“Gyros”) • A RGA system consists of a Rate Sensor Unit (RSU) and an Electronic Control Unit (ECU): • Three RSUs are attached to the Optical Telescope Assembly (OTA) and accessed through the Aft Shroud • Three ECUs are mounted in Support System Module (SSM) Bay 10 • Each RSU contains two Rate Sensors • Any combination of the six Rate Sensors can be used for HST attitude control • Three primary RSUs and one contingency RSU are manifested • One ECU is manifested as a contingency unit RSU Locations

  3. Design of ERS Program • Demonstrate new capabilities/verify performance • Wide-field UV/NIR imaging • Large filter complement • Grisms • Parallel imaging operations (WFC3 + ACS) • Provide baseline complementary data for GO proposals (no proprietary period) • Do not preclude large GO programs • First publications SM4 + 4-6 mo • Nominal 200 Orbits of Director’s Discretionary Time

  4. ERS Program: Themes Star Formation in Nearby Galaxies Leads: D. Calzetti and B. Whitmore Panchromatic Survey of Galaxies at Intermediate Redshifts (GOODS Field Survey) Leads: P. McCarthy and R. Windhorst

  5. WFC3 GOODS FIELD SURVEY Single 5’x10’ field8 WFC3 pointings5 filters + 1 grism ineach pointing2 add’l grisms in4 central pointingsNominal 2 orbits/filter+ ACS Parallels (4 filters)

  6. Intermediate Redshift ProgramScience Goals • Overall: galaxy assembly/origin of Hubble sequence at critical epoch z ~ 1-3 • Improved photo-z’s and spectrophoto-z’s from broader SED coverage (filters) and grism spectra (especially z ~ 1-2.5 and > 7) • SF rates z ~ 1-2 from well-sampled rest UV (filters) and Ly-Alpha/H-Alpha (UV/IR grisms) • Slope of the low-mass luminosity function (IR filters) • “UV-upturn” population in old systems z ~ 1 (UV filters)

  7. GOODS Field Survey: Depth AB_nu 25.0 29.0 WFC3 ACS WFC3

  8. Star Formation in Nearby Galaxies---Sample--- * * Two pointings

  9. Star Formation ProgramScience Goals • Star formation histories from multiband... • Aperture photometry • Pixel-by-pixel photometry • Resolved stars • Resolved star clusters • Environmental influences on cluster LF’s • ISM properties (ionization, shocks), SF feedback & regulation • Local Group clusters: VLM IMF and pre-MS accretion

  10. Star Formation Program: Filters Continuum: NUV, U, B, V, I, YJ, H Line: [O II], H-Beta, [O III], H-Alpha, [S II], P-Beta, H2O, [Fe II]

  11. NGC 2841 (Sb flocc) NGC 4150 (S0)

  12. Rapid star formers M82 (starburst) M83 (Sc) NGC 4214 (Irr)

  13. ALT, EX, ADDS

  14. AGN - Ty1 & XBONG 2.28p AGN - opt. faint Ultra Deep Field 1.216 AGN - Ty 1, unobs 0.665 AGN - XBONG 0.773 AGN - XBONG 1.82p AGN - opt. faint AGN - Optically faint 1.65p AGN - opt. faint 1.69p AGN - opt. faint Starbursts 0.456 Starburst 3.193 AGN - Ty 1, unobs 1.309 AGN - XBONG 4.29p AGN - opt. faint 0.438 Starburst 3.064 AGN - Ty 2 0.414 Starburst 1.53p AGN - opt. faint

  15. Prizkal et al. Astro-ph/0403458 Ly  at z = 5.5 Rhoads et al. 2004 Ultra Deep Field ERO z ~ 1 Ly at z = 5.5 1.69p AGN - opt. faint Malhotra et al. 2004 Galaxy z = 5.8 Galaxy z = 6.7 Galaxy z = 0.48

  16. Hubble Space Telescope

  17. Cosmic Origins Spectrograph COS installed in ORUC COS Fitcheck in the HFMS

  18. ACS Repair Development Grid Cutter 1G Development Card Extraction Tool Development

  19. Completed ACS Repair

  20. Ex, Alt, Supps

  21. Hubble is Powerful... • Because it’s large? NO. Only 100-in compared to 400-in on ground. Instead: • Because it’s in space without atmosphere to blur images or absorb or scatter light. • Because it was built to high precision to exploit its orbital environment. • Because it can be serviced to upgrade instruments and replace malfunctioning parts.

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