drift scanning (time-delay integration) -...
TRANSCRIPT
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Drift Scanning (Time-Delay Integration)
David RabinowitzYale University Center for Astronomy and Astrophysics
2005 Michelson Summer Workshop, Caltech
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I. What is drift scanning- how a CCD reads out- drift scanning- pros and cons of drift scanning- drift scanning at high declinations
II. Drift scanning telescopes and cameras- Spacewatch, Sloan, Palomar Quest- world’s largest CCD cameras
III. The Palomar Quest camera- design- sample images
IV. Astrometry with Palomar-Quest drift scans- method- precision- limits on precision
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I. What is drift scanning ?
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How a CCD reads out
horizontal shift register
parallel shift
(1)Parallel shift all rows down one row(2) Shift out last row through horizontal register(3) repeat
output amplifier
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What is drift scanning ?
Point & Shoot:telescope tracking(1) open shutter(2) close shutter(3) readout CCD
Drift Scanning:-telescope stationary-shutter stays open-readout continuous
image is stationary in focal plane
-image drifts in focal plane-CCD rows shifted to match drift rate
parallel shift direction
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RA
Sample Drift Scan
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Why drift scan ?
(1) most efficient way to use a CCD camera
(2) consistent astrometry over widest possible field
(3) astrometric solution is linear in pixel coordinates
(4) precision unaffected by telescope tracking error
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Why not to drift scan ?
(1) difficult to drift scan far from equator
(2) scanning introduces some distortion to PSF
(3) images must be read and written at the same time
(4) variable sky conditions record spatially
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fast
slow
two problems at high declinations
(1) curvature of star paths(2) variation in drift rate across CCD
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two different solutions
smaller, alignableCCDs
great circle tracking
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II. Drift scanning telescopes and cameras
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Drift scanning telescopes
0.9-m Spacewatch Telescope, Kitt Peak1989 to 2003(www.spacewatch.org)
2.5-m Sloan Digital Sky Survey Telescope, Apache Point1999 to present(www.sdss.org)
1.2-m Oschin Schmidt/Palomar-Quest camera, Palomar2003 to present(www.yale.edu/quest)
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Spacewatch Telescope
optics: Newtonianaperture: 0.9mfocal ratio: f/5.34pixel scale: 1.05”pixels: 1 x [2048x2048]coverage: 0.3 deg2
first telescope to automate discovery of asteroids
first drift-scan survey telescope
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Sloan Survey Telescope
optics: Ritchey-Chrétienaperture: 2.5 mfocal ratio: f/5.0pixel scale: 0.44”pixels: 30x[2048x2048]coverage: 1.6 deg2
First multi-color driftscancamera
scans on great circles
requires choreographed changes in RA, DEC tracking rates and image rotation
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Palomar Quest Telescope
optics: Schmidtaperture: 1.3 mfocal ratio: f/2.5pixel scale: 0.88”pixels: 112x[600x2400]coverage: 9.6 deg2
first wide-field survey for variable objects
covers 500 deg2 per night in 4 colors
multiple coverage each year of Dec range -22.5 to +22.5
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World’s Largest CCD Cameras
Palomar-Quest112 600x2400
Sloan30 2048x2048
Megacam36 2048x4612
SuprimeCam10 2048x4096
19 cm
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World's Largest CCD Cameras
0
2
4
6
8
10
12
0 2 4 6 8 10
Telescope Aperture (m)
Fiel
d of
Vie
w (s
q. d
eg.) Quest
Sloan
MegaCam SuprimeCam
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Survey Power = QE*FOV*AP2
0
2
4
6
8
10
12
14
16
0 2 4 6 8 10
Telescope Aperture
Surv
ey P
ower
Quest
Sloan
Megacam
SuprimeCam
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III. The Palomar Quest camera
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Russel Porter drawing of the 48” Oschin Schmidt at Palomar
72” mirror
Focal Surface
48” Corrector
The 48” Oschin Schmidt at Palomar
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Palomar/Quest Camera
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star track
star trail
Nor
th <
----
----
----
----
----
----
--->
Sou
th
West <----- -------> East
25.0 cm
19.3 cm
Drift-scanning
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Palomar Quest CCD
- thinned, back-illuminated -fabricated for Yale by Sarnoff Corporation- 2400 x 600 pixels (RA x Dec) -optimal for scanning at |Dec| < 25°
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Color Photometry
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Orion Nebula Driftscan: BRI-composite, 140-sec exposure
Palomar Quest
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M90, Virgo cluster: BRI-composite
Palomar Quest
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III. Astrometry with Palomar-Quest drift scans
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drift scan astrometry
y
x
right ascension = A1y + C1
declination = A2x + C2
right ascension = A’1y + B’1x +C’1
declination = A’2x + B’2y + C’2
of-date reference coordinates catalog coordinate system
RA
Dec
RA
Dec DecDec
frame 1 frame 2 frame 3
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Palomar Quest astrometry
(1) find objects, measure their centers (pixel coords x,y)
(2) Precess catalog from J2000 to of-date reference frame
(3) match objects to catalog (triangle match)
(4) find transformation from x,y to of-date ra,dec
(5) Calculate of-date ra,dec for each object
(6) Precess objects positions from of-date to J2000
(7) Find transformation from x,y to J2000 ra,dec
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Distribution of RA and Dec pixel scales Single drift scan at Dec = 13.5°
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RA and Dec residuals vs RA
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RA and Dec residuals vs Dec
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Distribution of RA and Dec residuals
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Precision of scan to scan registration
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Conclusions
(1) hardware is complicated
(2) astrometry is easy
(3) millions of stars routinely catalogued over wide area to precision of reference catalog (~0.5”).
(4) Absolute precision limited to ~0.1” for Palomar Quest
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