Photometric precision of a Si:As impurity band conduction mid-infrared detector and application to transit spectroscopy
| Autor: | Robert E. McMurray, Thomas L. Roellig, Kimberly Ennico, Taro Matsuo, Roy R. Johnson, Thomas P. Greene |
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| Rok vydání: | 2019 |
| Předmět: |
010504 meteorology & atmospheric sciences
FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Noise (electronics) Optics Spitzer Space Telescope 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Transit (astronomy) Spectral resolution 010303 astronomy & astrophysics Spectrograph Instrumentation and Methods for Astrophysics (astro-ph.IM) Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences Physics Earth and Planetary Astrophysics (astro-ph.EP) business.industry Detector Shot noise Astrophysics::Instrumentation and Methods for Astrophysics Astronomy and Astrophysics Exoplanet Space and Planetary Science Astrophysics::Earth and Planetary Astrophysics Astrophysics - Instrumentation and Methods for Astrophysics business Astrophysics - Earth and Planetary Astrophysics |
| DOI: | 10.48550/arxiv.1909.04769 |
| Popis: | Transit spectroscopy is the most promising path toward characterizing nearby terrestrial planets at mid-infrared wavelengths in the next 20 years. The Spitzer Space telescope has achieved moderately good mid-infrared photometric precision in observations of transiting planets, but the intrinsic photometric stability of mid-IR detectors themselves has not been reported in the scientific or technical literature. Here, we evaluated the photometric precision of a JWST MIRI prototype mid-infrared Si:As impurity band conduction detector, using time-series data taken under flood illumination. These measurements of photometric precision were conducted over periods of 10 hours, representative of the time required to observe an exoplanet transit. After selecting multiple sub-regions with a size of 10x10 pixels and compensating for a gain change caused by our warm detector control electronics for the selected sub-regions, we found that the photometric precision was limited to 26.3ppm at high co-added signal levels due to a gain variation caused by our warm detector control electronics. The photometric precision was improved up to 12.8ppm after correcting for the gain drift. We also translated the photometric precision to the expected spectro-photometric precision, assuming that an optimized densified pupil spectrograph is used in transit observations. We found that the spectro-photometric precision of an optimized densified pupil spectrograph when used in transit observations is expected to be improved by the square root of the number of pixels per a spectral resolution element. At the high co-added signal levels, the total noise could be reduced down to 7ppm, which was larger by a factor of 1.3 than the ideal performance that was limited by the Poisson noise and readout noise. The systematic noise hidden behind the simulated transit spectroscopy was 1.7ppm. Comment: 16 pages, 10 figures and 2 tables, it has been accepted by PASP |
| Databáze: | OpenAIRE |
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