Spring semester, Giant Telescope Science Presentator : Ham Ji-Beom 2011, April, 26

 Introduction & History  Instruments  Key Science  How to use

 Orbit Height : 559 km (Near Earth Circular orbit)  Orbit Period : 96 ~ 97 minutes  Diameter : 2.4m  Focal Length : 57.6m  Wavelength : Optical, NIR, UV

 In 1946, Lyman Spitzer wrote a paper “Astronomical advantages of extraterrastrial observatories”.  He explained two advantages, - Angular resolution - Different wavelength that is absorbed by Earth atmosphere

NameWavelengthYear Orbiting Solar Observatory(OSO) (1-7) UV, X-ray, gamma ray , Delta rocket Orbiting (OAO) (1,2,B,3)High quality UV images OSO4 OAO1

 Continuing success of the OAO program encouraged the LST(Large Space Telescope) should be major goal.  However, the funding issues led to reduction in the scale of project. - proposed mirror diameter reduced 3m to 2.4m - more compact and effective configuration.

 This telescope was planned to launch at 1986 Oct, however, because of the Challenge space shuttle disaster launch date was delayed.  Finally it was allowed to launch at 1990, April 24 on the Discovery space shuttle  US Total expenditure estimated at between $4.5 and $6 billion.

Former Generation Instruments FOCThe Faint Object Camera FOSThe Faint Object Spectrogra ph GHRSThe Goddard High Resolutio n Spectrograph HSPThe High Speed Photometer WF/PC-1Wide Field Planetary Camera 1 WFPC2The Wide Field Planetary Ca mera 2

Current HST Instruments ACSAdvanced Camera for Surve ys COSCosmic Origins Spectrograp h FGSThe Fine Guidance Sensors NICMOSNear Infrared Camera and M ulti Object Spectrometer STISSpace Telescope Imaging Sp ectrograph WFC3Wide Field Camera 3

Service Mission WorkSpace ShuttleYear SM1WFPC2, COSTAREndeavor, STS SM2STIS, NICMOSDiscovery, STS SM3AFGS, Replace computerDiscovery, STS SM3BACSColumbia, STS SM4WFC3, COS Fix ACS&STISAtlantis, STS

 Near Infrared Camera and Multi-Object Spectrometer  NICMOS employs three low-noise, high QE, 256x256 pixel HgCdTe arrays.  The NICMOS instrument is equipped with filters ranging from microns.  Each camera has 20 filter positions on a single filter wheel.

 Advanced Camera for Survey  Pixel based CTE(Charge transfer efficiency correction) =>

 Wide Field Channel (WFC), with a field of view of 202x202 square arcsec covering the range from 3500 Å to Å and a plate-scale of 0.05 arcsec/pixel;  High Resolution Channel (HRC), with a field of view of 29x26 square arcsec covering the range from 1700 Å to Å and a plate-scale of arcsec/pixel;  Solar Blind Channel (SBC), with a field of view of 34.6x30.5 arcsec field of view, spanning the range from 1150 Å to 1700 Å and a plate-scale of arcsec/pixel.

 Wide Field Camera 3

 UVIS  Components: 2x2Kx4K thinned, backside illuminated, UV optimized e2v CCDs  Wavelength Range: 200 to 1000mn  Total Field of View: 162 x 162 arcsec (rhomboidal)  Pixel format: 2 butted 2051x4096, 35-pixel gap.  Pixel Size: 15 microns  Plate Scale: 0.04 arcsec/pixel  Nominal Operating Temperature: -83C  Dark Current: e-/hour/pixel  Readnoise: 3.1 e-  Full Well: 75, ,000 e-  Gain: e-/ADU  Instrument Throughput: UVIS filtersUVIS filters  IR  Components: 1Kx1K Teledyne HgCdTe FPA, MBE grown, substrate removed  Wavelength Range: 900 to 1700 nm  Total Field of View: 123 x 136 arcsec (rectangular)  Pixel format: 1024x1024 (1014x1014 active)  Pixel Size: 18 microns  Plate Scale: 0.13 arcsec/pixel  Nominal Operating Temperature: 145 K  Dark Current: (mode) (median) e- /sec/pix  Readnoise: 21 e- (CDS) 15.5 e- (16-read linear fit)  Full Well: 93,000 e- (95% linearity)  Gain: 2.5 e-/ADU  Instrument Throughput: IR filtersIR filters

 Space Telescope Imaging Spectrograph CCDCCD: Scientific Image Technologies (SITe) CCD with ~0.05 arcsecond square pixels, covering a nominal 52 x 52 arcsecond square field of view (FOV), operating from ~2000 to 10,300 Å. NUV-MAMA: Cs 2 Te Multi-Anode Microchannel Array (MAMA) detector with ~0.024 arcsecond square pixels, and a nominal 25 x 25 arcsecond square field of view (FOV), operating in the near ultraviolet from 1600 to 3100 Å. FUV-MAMA: Solar-blind CsI MAMA with ~0.024 arcsec-pixels, and a nominal 25 x 25 arcsecond square FOV, operating in the far ultraviolet from 1150 to 1700 Å. NUV-MAMA FUV-MAMA

 (1) Study of the nearby intergalactic medium using quasar absorption lines to determine the properties of the intergalactic medium and the gaseous content of galaxies and groups of galaxies  (2) Medium deep survey using the Wide Field Camera to take data whenever one of the other instruments was being used  (3) Project to determine the Hubble Constant within ten percent by reducing the errors, both external and internal, in the calibration of the distance scale.

 Over 9000 papers based on Hubble data are reviewed.  about one-third of all astronomy papers have no citations, while only 2% of papers based on Hubble data have no citations.

 Anyone can apply on telescope.  The ratio of time requested to time available (the oversubscription ratio) typically ranges between 6 and 9.

 General observer - most common and covering routine observation  Snapshot observer – 45 minutes or less  Target of Opportunity – Transient event  DD(Direct’s discretionary) - 10% of telescope time  And in the first four cycles of telescope time, observations carried out by amateur astronomers.

 Proposal I Phase I proposals contain a scientific justification and abbreviated technical specifications for review by the Telescope Allocation Committee  Proposal II Phase II proposals provide many more technical details for programs recommended by the TAC and approved by the STScI Director