Optimization of the WFC3 Cold Stop Mask

Details Optimization of the WFC3 Cold Stop Mask Optimization of the WFC3 Cold Stop Mask

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001wfc..rept...16g&link_type=abstract

Instrument Science Report WFC3 2001-016, 12 pages

Computer Science

Hubble Space Telescope, Hst, Space Telescope Science Institute, Wide Field Camera 3, Wfc3

Scientific paper

We have modeled the contribution by the OTA and the instrument assembly to the WFC3 IR channel internal background in order to identify the optimal design of the cold stop mask. We have found that the contribution of the secondary mirror spiders and primary mirror hold-down pads are negligible for any value of the detector wavelength cut-off. The background coming from the hole in the primary mirror, which is reflected into the optical path by the secondary mirror, can also be neglected if the detector has a cut-off at ~1.75 μm or less. However, this contribution to the background is highly uncertain, because the temperatures of the various components within the hole are not well constrained. In any case, it becomes the dominant component if the detector's cut-off is at 1.9 μm. The background from the primary hole may also be a function of the aft-shroud temperature, and could increase after the installation of ACS and the NICMOS cryo-coolers. We recommend a minimal cold stop mask that, while ensuring good alignement, should not include spiders and pads. Compared to the current design by BATC, the optimized cold stop mask will increase the IR channel throughput by ~7 % without causing any significant increase in the instrument background.

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