AST3 detector properties

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Manuel Gomez-Rodriguez* Jens Kober† Bernhard Schölkopf†

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Presentation transcript:

AST3 detector properties Ma Bin (NAOC) 2015.03.09 2015 AST3 meeting@HKU

OUTLINE 1 AST3 CCD 2 CCD test results 3 Nonlinear PTC 4 Current status

1 AST3 CCD STA 1600FT 10560 * 10560 pixels Pixel size 9μm -> 1” thermoelectric cooling (TEC)

Frame transfer -> FOV 4.3deg2 16 readout amplifiers Slow: 40s; fast 2.5s

2 CCD test results To check the overall performance Fridge: producing different environment temperatures down to −80C Light source: a LED lighting through several layers of white paper

Linearity Signal level .vs. Exposure time Full well capacity > 100,000 e−

Photon Transfer Curve (PTC) gain: e- -> analog-to-digital units (ADU) pairs of flat frames with various signal levels Variance: photon shot noise + readout noise σ2= N/g + σ2rd/g2 1/g is the slope of the variance-signal plot g ~ 1.64 e-/ADU

Readout Noise RMS of the overscan Slow: 4 e-; fast: 9-12 e- sky brightness (AST3-1 in 2012) 8e-/sec for 60sec exposure, photon shot noise 22 e- Fast mode is used for observation

Dark Current thermal electrons decreases by half as the temperature is lowered every 7.3C

Charge Transfer Eﬃciency CTE: the fraction of charges transferred from one pixel to the next during readout Extended Pixel Edge Response (EPER): excess charges found in the overscan

3 Nonlinear PTC Downing+06 reported this effect, and found it was caused by signal correlation between pixels Downing & Sinclaire (2013): charge diffusion due to the Coulomb force of stored charges (charge sharing) Antilogus+ 14: effective pixel boundaries shift; predicting brighter-fatter effect from PTC Downing & Sinclaire (2013)

We proposed a simple model, named charge sharing PSF, assuming charge sharing fraction as a function of signal level AST3 CCDs show significant signal correlation between a pixel and its neighbors: (0,±1)(0, ±2)(±1,±1) Deriving charge sharing PSF from PTC, then estimating the effect on real image

Profiles of stars (FWHM, elongation) depend on their brightness, biasing photometry and shape measurement.

4 Current status CCD#1 (engineering grade) on AST3#1 in 2012 In Jan 2015, 31th Chinese Antarctic Research Expedition (CHINARE) team deployed AST3#2 with CCD#2, and replaced CCD#1 with CCD#3 Realtime status is shown on website http://aag.bao.ac.cn/ast3-2/index.php

CCD temperature control Original TEC control makes t_CCD oscillate around setpoint with a amplitude of 4 degrees Prof. Ashley has done a great job to keep it much more stable (~0.2 degree) 2015.02.11 2015.02.16

The heat from CCD chip by TEC is not removed efficiently, so TEC cannot cool CCD very much T_CCD is about 10 degrees above ambient temperature Dark current level@-50C: 1.7e-/sec (CCD#1), 0.29e-/sec(CCD#2) sky brightness (AST3-1 in 2012) 8e-/sec Noise from dark current is expected to be insignificant

Thank you !