An optical to IR sky brightness model for the LSST

Peter Yoachim; Michael Coughlin; George Z. Angeli; Charles F. Claver; Andrew J. Connolly; Kem Cook; Scott Daniel; A. Ivezia; R. Lynne Jones; Catherine Petry; Michael Reuter; Christopher Stubbs; Bo Xin

doi:10.1117/12.2232947

An optical to IR sky brightness model for the LSST

Peter Yoachim, Michael Coughlin, George Z. Angeli, Charles F. Claver, Andrew J. Connolly, Kem Cook, Scott Daniel, A. Ivezia, R. Lynne Jones, Catherine Petry, Michael Reuter, Christopher Stubbs, Bo Xin

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

13 Scopus citations

Abstract

To optimize the observing strategy of a large survey such as the LSST, one needs an accurate model of the night sky emission spectrum across a range of atmospheric conditions and from the near-UV to the near-IR. We have used the ESO SkyCalc Sky Model Calculator^{1, 2} to construct a library of template spectra for the Chilean night sky. The ESO model includes emission from the upper and lower atmosphere, scattered starlight, scattered moonlight, and zodiacal light. We have then extended the ESO templates with an empirical fit to the twilight sky emission as measured by a Canon all-sky camera installed at the LSST site. With the ESO templates and our twilight model we can quickly interpolate to any arbitrary sky position and date and return the full sky spectrum or surface brightness magnitudes in the LSST filter system. Comparing our model to all-sky observations, we find typical residual RMS values of ±0.2-0.3 magnitudes per square arcsecond.

Original language	English (US)
Title of host publication	Observatory Operations
Subtitle of host publication	Strategies, Processes, and Systems VI
Editors	Alison B. Peck, Robert L. Seaman, Chris R. Benn
Publisher	SPIE
ISBN (Electronic)	9781510601994
DOIs	https://doi.org/10.1117/12.2232947
State	Published - 2016
Externally published	Yes
Event	Observatory Operations: Strategies, Processes, and Systems VI - Edinburgh, United Kingdom Duration: Jun 27 2016 → Jul 1 2016

Publication series

Name	Proceedings of SPIE - The International Society for Optical Engineering
Volume	9910
ISSN (Print)	0277-786X
ISSN (Electronic)	1996-756X

Conference

Conference	Observatory Operations: Strategies, Processes, and Systems VI
Country/Territory	United Kingdom
City	Edinburgh
Period	6/27/16 → 7/1/16

Bibliographical note

Publisher Copyright:
© 2016 SPIE.

Keywords

Astronomy Software
Python
Sky Emission

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Yoachim, P., Coughlin, M., Angeli, G. Z., Claver, C. F., Connolly, A. J., Cook, K., Daniel, S., Ivezia, A., Jones, R. L., Petry, C., Reuter, M., Stubbs, C., & Xin, B. (2016). An optical to IR sky brightness model for the LSST. In A. B. Peck, R. L. Seaman, & C. R. Benn (Eds.), Observatory Operations: Strategies, Processes, and Systems VI Article 99101A (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9910). SPIE. https://doi.org/10.1117/12.2232947

An optical to IR sky brightness model for the LSST. / Yoachim, Peter; Coughlin, Michael; Angeli, George Z. et al.
Observatory Operations: Strategies, Processes, and Systems VI. ed. / Alison B. Peck; Robert L. Seaman; Chris R. Benn. SPIE, 2016. 99101A (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9910).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Yoachim, P, Coughlin, M, Angeli, GZ, Claver, CF, Connolly, AJ, Cook, K, Daniel, S, Ivezia, A, Jones, RL, Petry, C, Reuter, M, Stubbs, C & Xin, B 2016, An optical to IR sky brightness model for the LSST. in AB Peck, RL Seaman & CR Benn (eds), Observatory Operations: Strategies, Processes, and Systems VI., 99101A, Proceedings of SPIE - The International Society for Optical Engineering, vol. 9910, SPIE, Observatory Operations: Strategies, Processes, and Systems VI, Edinburgh, United Kingdom, 6/27/16. https://doi.org/10.1117/12.2232947

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abstract = "To optimize the observing strategy of a large survey such as the LSST, one needs an accurate model of the night sky emission spectrum across a range of atmospheric conditions and from the near-UV to the near-IR. We have used the ESO SkyCalc Sky Model Calculator1, 2 to construct a library of template spectra for the Chilean night sky. The ESO model includes emission from the upper and lower atmosphere, scattered starlight, scattered moonlight, and zodiacal light. We have then extended the ESO templates with an empirical fit to the twilight sky emission as measured by a Canon all-sky camera installed at the LSST site. With the ESO templates and our twilight model we can quickly interpolate to any arbitrary sky position and date and return the full sky spectrum or surface brightness magnitudes in the LSST filter system. Comparing our model to all-sky observations, we find typical residual RMS values of ±0.2-0.3 magnitudes per square arcsecond.",

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AU - Daniel, Scott

AU - Ivezia, A.

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AU - Stubbs, Christopher

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AB - To optimize the observing strategy of a large survey such as the LSST, one needs an accurate model of the night sky emission spectrum across a range of atmospheric conditions and from the near-UV to the near-IR. We have used the ESO SkyCalc Sky Model Calculator1, 2 to construct a library of template spectra for the Chilean night sky. The ESO model includes emission from the upper and lower atmosphere, scattered starlight, scattered moonlight, and zodiacal light. We have then extended the ESO templates with an empirical fit to the twilight sky emission as measured by a Canon all-sky camera installed at the LSST site. With the ESO templates and our twilight model we can quickly interpolate to any arbitrary sky position and date and return the full sky spectrum or surface brightness magnitudes in the LSST filter system. Comparing our model to all-sky observations, we find typical residual RMS values of ±0.2-0.3 magnitudes per square arcsecond.

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An optical to IR sky brightness model for the LSST

Abstract

Publication series

Conference

Bibliographical note

Keywords

Access

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