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Introduction to and Introduction to and methods of SPACE-based methods of SPACE-based observational astronomyobservational astronomy
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
Armando Gil de Paz (Universidad Complutense de Madrid)
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SchemeScheme 1 st
MAGPOP School
(Budapest, Aug 23-25 2006) Current Space Observatories with GO/GI programs: (Guest Observer/Guest Investigator)
HST GALEX
SpitzerMAGPOP’s favorites!
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SchemeScheme 1 st
MAGPOP School
(Budapest, Aug 23-25 2006) Other current Space Observatories with GO/GI programs:
IntegralXMM-Newton
Chandra Akari (Astro-F)FUSE
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1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
Past/Present/
Future Space Observatorie
s:
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SchemeScheme 1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
HST
• Description of the Observatory
• Preparing a HST proposal:
• Constraints, APT, etc.
• Using Archival Data: MAST
Covering the basics: • Why observing from Space?
Today’s lecture
Image quality, low background,
transparency Costs & risks
VS.
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SchemeScheme 1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
GALEX
• Description of the Observatory
• Preparing a GALEX proposal
• Bright-star and background limitations
• Using Archival Data
Spitzer
• Description of the Observatory
• Preparing a Spitzer proposal: Using Spot
• Observing constraints, pipeline, & latents
• Using Archival Data: Using Leopard
tomorrow
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SchemeScheme 1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
• James Webb Space Telescope (JWST)
friday
• Using IUE, IRAS, ISO dataPast:
Future:
Space-based Astronomy Tools and Science:
• Use of Space-based data
• Synergy with ground-based data (e.g. HST-Keck/VLT, JWST-ALMA)
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Space Astronomy: Why? Space Astronomy: Why?
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
No atmosphere
• Better image quality (no atmospheric seeing) FWHMseeing ~-0.2 ; Diffraction limit = /D
UpsUps
Mauna Kea (average)
Antarctica (average)
Antarctica (best 25%)
Diff.Lim 2m Diff.Lim 8m
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Space Astronomy: Why? Space Astronomy: Why?
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
No atmosphere
• Better transparency & no cloudy nights
UpsUps
Antarctica
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Space Astronomy: Why? Space Astronomy: Why?
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
No atmosphere
• Less (scattered and thermal) background
UpsUps
Antarctica
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Space Astronomy: Why? Space Astronomy: Why?
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
Existence of Continuous Viewing Zones (CVZ)UpsUps
HST HDF observations in CVZ
• Longer lasting (& fixed) CVZ
• Lower thermal background from Earth
• No South Atlantic Anomaly passages
In high orbits (Earth-trailing, L2)
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Space Astronomy: Why?Space Astronomy: Why? 1 st
MAGPOP School
(Budapest, Aug 23-25 2006) DownsDowns Higher risks
• Not 100% launch and deploy successful rates (e.g. HETE, Abrixas, ASTRO-E, WIRE)
• Telescope & instruments never tested under exact working conditions (e.g. HST).
• Difficult to repair if something fails. Impossible for satellites in high orbits.
Limited lifetime
• Instrument consumables (cooling: NICMOS, ISO, Spitzer)
• Propellant (to compensate for atmospheric drag -Compton GRO- or angular momentum build up -JWST)
• Gyros (despite redundant systems).
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Space Astronomy: Why?Space Astronomy: Why? 1 st
MAGPOP School
(Budapest, Aug 23-25 2006) DownsDownsHigher costs
Source: Federation of American Scientists
• For both telescope & instruments plus launch cost.
• Example: All four VLTs cost ~1/7 HST.
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Space Astronomy: Why?Space Astronomy: Why? 1 st
MAGPOP School
(Budapest, Aug 23-25 2006) DownsDowns Higher rates of high-energy particles:
• Cosmic-rays events in HST detectors are several times higher than in the ground (1.5-3% ACS/WFC pixels affected in 1000s).
• This situation is worse in high orbits (5%-10% pixels expected to be affected in a JWST 1000s exposure) where there is no protection by the Van Allen belts.
Single 600s-long HST ACS/WFC raw image
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Space Astronomy: SpecificsSpace Astronomy: Specifics
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
These These Ups and downsUps and downs determine the specifics of the determine the specifics of the analysis methods used in Space Astronomy:analysis methods used in Space Astronomy:
• High-spatial res. & Diff.Lim. images: PSF phot. (HST, Spitzer)
• Low background: Highly Poissonian statistics (HST & GALEX)
• High cosmic-rays rates: (HST CR-SPLIT)
• Count-rate, color, and position-dependent PSF (GALEX & MIPS)
• Multiple time constant response (MIPS 70 & 160um)
• Confusion limits (GALEX & MIPS)
Specifics of the instrumentation used in Space Specifics of the instrumentation used in Space Observatories exploring new windows (UV, FIR):Observatories exploring new windows (UV, FIR):
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Hubble Space TelescopeHubble Space Telescope
1 st
MAGPOP School
(Budapest, Aug 23-25 2006) • 2.5-m telescope in a low orbit (600 km) deployed in 1990.
• Current functioning instruments: ACS, NICMOS, WFPC2
• Replaced or non-functioning (“legacy”) instruments: FOC, FOS, GHRS, HST, WF/PC, STIS
• New service mission (SM4) has not yet been decided.
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HST InstrumentsHST Instruments
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
Imaging:Imaging:
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HST InstrumentsHST Instruments
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
Choosing the right imaging instrument:Choosing the right imaging instrument:
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HST InstrumentsHST Instruments
1 st
MAGPOP School
(Budapest, Aug 23-25 2006) Slitless spectroscopy: Slitless spectroscopy: (no long-slit spectroscopy since STIS failure in 2004)
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Proposing for HSTProposing for HST
1 st
MAGPOP School
(Budapest, Aug 23-25 2006) Feasibility:Feasibility:
Need for HST:Need for HST:
• Reasonable number of orbits (compared with the expected scientific return and number of people involved). Use ETC.
• The assumptions for determining the number of orbits are well justified and the overheads are properly accounted for.
• Also address: 2-gyros mode impact, parallel observations.
Flexibility:Flexibility:
• HST (and only HST) can address this particular science topic.
• Available in the MAST archive? If so, justify additional time.
• Long & frequent visibility windows and no unnecessary timing or orientation constraints.
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Proposing for HST: ConstraintsProposing for HST: Constraints
1 st
MAGPOP School
(Budapest, Aug 23-25 2006) • Orbit: 96 min long. Most objects partially occulted by the Earth (up to 44 min/orbit). CVZ within 24o the orbital poles.
(Note: CVZ should not be requested for background-limited broad-band imaging or observations with timing constraints, special orientation requirements, or ToO)
• SAA: Although precession cycle is 56 days (so objects can be in the CVZ for many days in a row), the SAA limits the longest continuous observation to 5-6 orbits.
• Pointing constraints: Within 60o of the Sun, 20o of the Earth and 9.5o of the Moon. Additional constraints for the ACS/SBC MAMA detector apply.
• Other constraints: Since Aug 2005, HST is observing in two-gyros mode.
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HST Phase I: APTHST Phase I: APT
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
First steps:First steps:
• Documentation: Call for Proposals, HST Primer, and relevant instrument (ACS, NICMOS, WFPC2) handbook.
• Get Scientific Justification LaTeX/Word/PDF template
• Software: Proposer Tool (APT) & Visualizer (VTT, Aladin)
(See APT training materials!)
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HST Phase I: APTHST Phase I: APT
1 st
MAGPOP School
(Budapest, Aug 23-25 2006)
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1 st
MAGPOP School
(Budapest, Aug 23-25 2006) • Images can be retrieved using starview and visualized using VTT (included in APT) or directly from MAST.
• Data formats (see the instruments data handbooks):
Multiextension FITS: Science, data quality and error arrays
• Extensions: RAW, FIT, CRJ, DRZ (ACS & STIS), _raw, _ima, _cal, _mos (NICMOS), _d0f, _c0f (WFPC2)
• WFPC2 associations: 15000 combined WFPC2 images created from associations of 50000 individual WFPC2 frames.
• Images are VO complaint.
HST archive: MASTHST archive: MAST