Stray Light Correction of the XRT Temperature Response Functions

(7, September, 2015 by Aki Takeda)
(11 Sep,2015 added ratio curves & estimation of open fraction.)
(16 Dec,2019 figures of telescope.)

1. Introduction.

What is the XRT temperature response functions?

2. XRT's effective area function.

[Effective Area] = [aperture] * [prefilter] * [mirror1] * [mirror2] * [filter1] * [filter2] * [ccdqe] * [contamination]
aperture=2.28 cm^2
filter1=1.0 (FW1=OPEN)
filter2=1.0 (FW2=OPEN)

Effective Area modified partially opened prefilter (without X-ray filters).

3. Modified response functions.

After multiplying the FW1 and FW2 responses, take convolution with the model solar spectra calculated based on Chianti version 7.1.3.
Here we assume the Open Fraction having the value of 0.45 and 0.95 (see Section 5 for derivation).

Open/Al-meshOpen/Ti-poly
Al-poly/OpenThin-Be/Open
Open/thick-AlOpen/thick-Be

4. Modification of the Filter Ratio.

Al-poly/Al-meshTi-poly/Al-mesh
thin-Be/Al-polythick-Be/thick-Al

5. Estimation of the "Open Fraction" of the prefilter.

G-band images taken with VLS(visible light shutter) Open or Close can be used to estimate the amount of stray light coming through the open area of the prefilter. VLI transmission from the Blue Book section 2.5.1.

Ratio of total image intensity :
[VLS_close]/[VLS_open]=0.446..
Ratio of total image intensity :
[VLS_close]/[VLS_open]=0.953..

6. Software to use the modified response functions.

Under development....