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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

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