IRAC Instrument Handbook - IRSA - California Institute of Technology
IRAC Instrument Handbook - IRSA - California Institute of Technology
IRAC Instrument Handbook - IRSA - California Institute of Technology
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The linearization solution to the above quadratic model is:<br />
where<br />
2n+<br />
w n<br />
α ⎡⎛<br />
2<br />
L = ⎢⎜<br />
∑ i − ∑i<br />
2<br />
n(<br />
w + n)<br />
⎣⎝<br />
n+<br />
w+<br />
1 1<br />
<strong>IRAC</strong> <strong>Instrument</strong> <strong>Handbook</strong><br />
−1<br />
+ 1−<br />
4LαDN<br />
obs<br />
DN = (5.17)<br />
2Lα<br />
2<br />
⎞ t ⎤<br />
d<br />
⎟ − 2(<br />
1−<br />
) n(<br />
n + w)<br />
⎥ , (5.18)<br />
⎠ tc<br />
⎦<br />
A<br />
and α = , n is the Fowler number, and w is the wait period. The above expression for L is the<br />
2<br />
m<br />
correction required to account for multi-sampling. This is required because the multi-sampling results in<br />
the apparent time spent integrating not actually being equal to the real time spent collecting photons. Note<br />
that td is the time between the reset and the 1st readout <strong>of</strong> the pixel. For channel 3, we use a cubic<br />
linearization model:<br />
For the cubic model, the solution is derived via a numerical inversion.<br />
5.1.14 BGMODEL (zodiacal background estimation)<br />
DNobs = Ckt 3 + Akt 2 + kmt (5.19)<br />
For this module, a spacecraft-centric model <strong>of</strong> the celestial background was developed. For each image,<br />
the zodiacal background will be estimated (a constant for the entire frame) based on the pointing and time<br />
that the data were taken. This value is written to the header keyword ZODY_EST in units <strong>of</strong> MJy/sr. The<br />
zodiacal background is also estimated for the subtracted skydark (see next module) and placed in the<br />
header keyword SKYDRKZB.<br />
5.1.15 Dark Subtraction II: SKYDARKSUB (sky “delta-dark” subtraction)<br />
This module, the second part <strong>of</strong> dark subtraction, strongly resembles traditional ground-based data<br />
reduction techniques for infrared data. Since <strong>IRAC</strong> did not use the photon-shutter for its dark<br />
measurement, a pre-selected region <strong>of</strong> low zodiacal background in the north ecliptic cap is observed in<br />
order to create a “skydark". At least twice during each campaign a library <strong>of</strong> skydarks <strong>of</strong> all Fowler<br />
numbers and frame times were observed, reduced, and created by the calibration pipeline. The skydarks<br />
have had the appropriate labdark subtracted in their DARKCAL pipeline and are therefore a “delta-dark.”<br />
Pipeline Processing 83 Level 1 (BCD) Pipeline