1 hubble space telescope cutaway. 2 hubble space telescope field of view wfc3 acs stis cos fgs
TRANSCRIPT
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Hubble Space Telescope Cutaway
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Hubble Space Telescope Field of View
• WFC3• ACS• STIS• COS• FGS
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HST: WFC3
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HST: WFC3
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HST: ACS
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HST: ACS
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HST: STIS
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HST: STIS
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Spitzer Space Telescope
• IRAC• IRS• MIPS
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Spitzer Space Telescope: IRAC
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Spitzer Space Telescope: IRS
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Spitzer Space Telescope: MIPS
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Chandra Space Telescope
• ACIS• HRC• Spectral modes
Advanced Charged Couple Imaging Spectrometer (ACIS): Ten CCD chips in 2 arrays provide imaging and spectroscopy; imaging resolution is 0.5 arcsec over the energy range 0.2 - 10 keV; sensitivity: 4x10-15 ergs/cm2/sec in 105 s
High Resolution Camera (HRC): Uses large field-of-view mircro-channel plates to make X-ray images: ang. resolution < 0.5 arcsec over field-of-view 31x31 arc0min; time resolution: 16 micro-sec sensitivity: 4x10-15 ergs/cm2/sec in 105 s
High Energy Transmission Grating (HETG): To be inserted into focused X-ray beam; provides spectral resolution of 60-1000 over energy range 0.4 - 10 keV
Low Energy Transmission Grating (LETG): To be inserted into focused X-ray beam; provides spectral resolution of 40-2000 over the energy range 0.09 - 3 keV
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Chandra Space Telescope: ACIS
• Chandra Advanced CCD Imaging Spectrometer (ACIS)
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Chandra Space Telescope: HRC
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Chandra Space Telescope: Spectroscopy
• High Resolution Spectrometers - HETGS and LETGS • These are transmision gratings
– low energy: 0.08 to 2 keV – high energy: 0.4 to 10 keV (high and medium resolution)
• Groove spacings are a few hundred nm.
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Gemini (North)
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Gemini (South)
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JWST
• NIRCAM
• NIRSPEC
• MIRI
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JWST: NIRCAM
• Nyquist-sampled imaging at 2 and 4 microns -- short wavelength sampling is 0.0317"/pixel and long wavelength sampling is 0.0648"/pixel
• 2.2'x4.4' FOV for one wavelength provided by two identical imaging modules, two wavelength regions are observable simultaneously via dichroic beam splitters.
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JWST: NIRSPEC
• 1-5 um; R=100, 1000, 3000
• 3.4x3.4 arcminute field
• Uses a MEMS shutter for the slit
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JWST: MIRI
• 5-27 micron, imager and medium resolution spectrograph (MRS)
• MIRI imager: broad and narrow-band imaging, phase-mask coronagraphy, Lyot coronagraphy, and prism low-resolution (R ~ 100) slit spectroscopy from 5 to 10 micron.
• MIRI will use a single 1024 x 1024 pixels Si:As sensor chip assembly. The imager will be diffraction limited at 7 microns with a pixel scale of ~0.11 arcsec and a field of view of 79 x 113 arcsec.
• MRS: simultaneous spectral and spatial data using four integral field units, implemented as four simultaneous fields of view, ranging from 3.7 x 3.7 arcsec to 7.7 x 7.7 arcsec with increasing wavelength, with pixel sizes ranging from 0.2 to 0.65 arcsec. The spectroscopy has a resolution of R~3000 over the 5-27 micron wavelength range. The spectrograph uses two 1024 x 1024 pixels Si:As sensor chip assemblies.
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JWST: MIRI MRS
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NIRSPEC/Keck Optical LayoutSide View
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NIRSPEC/Keck Optical LayoutTop View
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Large CCD Mosaics
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LSST Has a Big Camera
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LSST Has a Big Focal Plane
Guide Sensors (8 locations)
Wavefront Sensors (4 locations)
3.5 degree Field of View (634 mm diameter)
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History of Infrared Light Detection
• Herschel’s detection of IR from Sun in 1800
• Johnson’s IR photometry of stars (PbS) mid 60’s
• Neugebauer & Leighton: 2um Sky Survey (PbS), late 60’s
• Development of bolometer (Low) late 60’s
• Development of InSb (mainly military) early 70’s
• IRAS 1983
• Arrays (InSb, HgCdTe, Si:As IBCs) mid-80’s
• NICMOS, 2MASS, IRTF, UKIRT, KAO, common-user instruments, Gemini, etc.
• JWST and the search for cosmic origins
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Detector Size
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Applications
Imaging (single photon counting)
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Figures Courtesy of Don Hall (University of Hawaii)
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Fermi Gamma-ray Large Area Space Telescope (GLAST)
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GLAST LAT
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Gamma Ray Detection Airshowers
• It is possible to detect gamma rays by the presence of their by-products produced in Earth’s atmosphere.
• Ground-based gamma ray telescopes actually detect Cherenkov radiation emitted by high energy particles produced through the interaction of the gamma rays and atmospheric particles.
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Caltech Submillimeter Observatory (CSO)
• CSO has a 10.4m primary dish.
• SHARCII has 350, 450, 850um passbands, 12x32, 2.6x1amin field.
• Dry nights lead to better sensitivity
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Stratospheric Observatory for Infrared Astronomy (SOFIA)
• SOFIA has 2.5m mirror.
• It has a variety of instruments (see below) covering optical to FIR.
• HAWK is being upgraded with new detectors and polarimeters.
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Herschel
• The Herschel telescope is a Cassegrain design with a 3.5m primary. The three scientific instruments are: – HIFI (Heterodyne Instrument for the
Far Infrared), a very high resolution heterodyne spectrometer
– PACS (Photodetector Array Camera and Spectrometer) - an imaging photometer and medium resolution grating spectrometer
– SPIRE (Spectral and Photometric Imaging Receiver) - an imaging photometer and an imaging Fourier transform spectrometer
• Covers 60-670 um.
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Planck
• The Planck telescope has an off-axis 1.5m primary. The scientific instruments are: – LFI (Low Frequency Instrument),
a High Electron Mobility Transistor based radio receiver.
– HFI (High Frequency Instrument), a bolometer based imaging array
• Covers 300um to 1.2cm.
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ALMA
• The Atacama Large Millimeter/submillimeter Array
• Covers 300um to a few cm
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Radio Telescope Components
• Reflector(s)
• Feed horn(s)
• Low-noise amplifier
• Filter
• Downconverter
• IF Amplifier
• Spectrometer
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Antenna Fundamentals
• An antenna is a device for converting electromagnetic radiation into electrical currents or vice-versa, depending on whether it is being used for receiving or for transmitting.
• In radio astronomy, antennas are used for receiving.
• The antenna receiver usually receives radiation from a dish, but it doesn’t have to.
• For instance, the Long Wavelength Array (LWA) that has ~104 dipoles. At a wavelength of 15m, the dipoles have ~106
m2 of effective collecting area, where collecting area goes as wavelength squared, divided by 4 pi.
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Very Large Array (VLA)
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VLA Main Features
• 27 radio antennas in a Y-shaped configuration
• fifty miles west of Socorro, New Mexico
• each antenna is 25 meters (82 feet) in diameter
• data from the antennas are combined electronically to give the resolution of an antenna 36km (22 miles) across
• sensitivity equal to that of a single dish 130 meters (422 feet) in diameter
• four configurations: – A array, with a maximum antenna separation of 36 km; – B array -- 10 km; – C array -- 3.6 km; and – D array -- 1 km.
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VLA Receivers
Receivers Available at the VLA
4 Band P Band L Band C Band X Band U Band K Band Q Band
Frequency (GHz) 0.073-0.0745 0.30-0.34 1.34-1.73 4.5-5.0 8.0-8.8 14.4-15.4 22-24 40-50
Wavelength (cm) 400 90 20 6 3.6 2 1.3 0.7
Primary beam (arcmin) 600 150 30 9 5.4 3 2 1
Highest resolution (arcsec) 24.0 6.0 1.4 0.4 0.24 0.14 0.08 0.05
System Temp 1000-10,000.K 150-180.K 37-75.K 44.K 34.K 110.K 50-190.K 90-140.K
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Very Long Baseline Array (VLBA)
• ten radio telescope antennas– 25 meters (82 feet) in diameter and weighing 240 tons– Mauna Kea to St. Croix in the U.S. Virgin Islands
• VLBA spans more than 5,000 miles, providing astronomers with the sharpest vision of any telescope on Earth or in space.
• efforts to reduce funding
• efforts to increase sensitivity (~6x)
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Chandra
Chandra in Earth orbit (artist’s conception)http://chandra.nasa.gov/
Originally AXAFAdvanced X-ray Astrophysics Facility
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Chandra Orbit
• Deployed from Columbia, 23 July 1999
• Elliptical orbit– Apogee = 86,487 miles (139,188 km) – Perigee = 5,999 miles (9,655 km)
• High above LEO Can’t be Serviced
• Period is 63 h, 28 m, 43 s– Out of Earth’s Shadow for Long Periods– Longer Observations
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Chandra Mirrors Assembled and Aligned by Kodak in Rochester
“Rings”
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Mirrors Integrated into spacecraft at
TRW (NGST), Redondo Beach, CA
(Note scale of telescope compared to workers)
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Chandra ACIS CCD Sensor