Download Instruments

Spring semester, 2011.
Giant Telescope Science
2011, April, 26
Presentator :
Ham Ji-Beom
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Introduction & History
Instruments
Key Science
How to use
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Orbit Height : 559 km (Near Earth Circular orbit)
Orbit Period : 96 ~ 97 minutes
Diameter : 2.4m
Focal Length : 57.6m
Wavelength : Optical, NIR, UV
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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
Name
Wavelength
Year
Orbiting Solar
Observatory(OSO) (1-7)
UV, X-ray, gamma ray
1962-1975, Delta rocket
Orbiting (OAO) (1,2,B,3)
High quality UV images
1966-1972
OSO4
OAO1
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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.
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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
FOC
The Faint Object Camera
FOS
The Faint Object Spectrogra
ph
GHRS
The Goddard High Resolutio
n Spectrograph
HSP
The High Speed Photometer
WF/PC-1
Wide Field Planetary Camera
1
WFPC2
The Wide Field Planetary Ca
mera 2
Current HST Instruments
ACS
Advanced Camera for Surve
ys
COS
Cosmic Origins Spectrograp
h
FGS
The Fine Guidance Sensors
NICMOS
Near Infrared Camera and M
ulti Object Spectrometer
STIS
Space Telescope Imaging Sp
ectrograph
WFC3
Wide Field Camera 3
Service
Mission
Work
Space Shuttle
Year
SM1
WFPC2, COSTAR
Endeavor, STS-61
1993
SM2
STIS, NICMOS
Discovery, STS-82
1997
SM3A
FGS, Replace computer
Discovery, STS-103
1999
SM3B
ACS
Columbia, STS-109
2002
SM4
WFC3, COS
Fix ACS&STIS
2009
Atlantis, STS-125
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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 0.8-2.5 microns.
Each camera has 20 filter positions on a single
filter wheel.
Advanced Camera for Survey
 Pixel based CTE(Charge
transfer efficiency
correction) =>
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Wide Field Channel (WFC), with a field of view of
202x202 square arcsec covering the range from 3500
Å to 11000 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 11000 Å and a plate-scale of 0.027 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 0.032
arcsec/pixel.
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Wide Field Camera 3
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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: 0.16-0.41 e-/hour/pixel
Readnoise: 3.1 eFull Well: 75,000 - 80,000 eGain: 1.52 - 1.56 e-/ADU
Instrument Throughput: UVIS filters
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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: 0.011 (mode) 0.015 (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 filters
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Space Telescope Imaging Spectrograph
CCD: 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: Cs2Te 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.
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(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.
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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.
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Anyone can apply on telescope.
The ratio of time requested to time available
(the oversubscription ratio) typically ranges
between 6 and 9.
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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.
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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
http://www.nasa.gov/hubble/
http://hubble.nasa.gov/
http://hubblesite.org/
http://www.spacetelescope.org/