Integration time

In astronomy, integration time or exposure time is the duration for which photons from a source are collected.[1] A longer integration time means that m

In astronomy, integration time or exposure time is the duration for which photons from a source are collected.[1] A longer integration time means that more photons are collected in total.[2] It is analogous to the term shutter speed in photography;[1] however, astronomical observations generally require a much longer integration time than traditional photography, and the total integration time may be segmented into multiple different observations. Higher integration time results in a higher signal-to-noise ratio for an observation.[1][3][4] Integration time is particularly relevant in radio astronomy, where the signal may be much smaller than the background noise for a short observation.[5]

Integration time can also refer to the duration of time for which the photons for each pixel of an image are collected in the case of radio telescopes and charge-coupled devices, which only collect information for one pixel at a time.[5][3]

Integration time can be a challenge for astronomers trying to collect data. Often times, getting an adequate signal-to-noise ratio or level of precision in a measurement can take up to tens of thousands of hours.[6] Additionally, a long integration time can smooth out signals that vary with time and result in loss of information, particularly in contexts where a changing signal may be relevant, such as in the detection of exoplanets.[7] For some types of cameras, such as EMCCDs, increasing integration time may not necessarily lead to a higher signal-to-noise ratio.[8]

References

  1. ^ a b c "Integration time". Archived from the original on 2026-02-09. Retrieved 2026-06-28.
  2. ^ "Integration time". Photonics Spectra. Archived from the original on 2024-06-14. Retrieved 2026-06-28.
  3. ^ a b "CCD Noise Sources and Signal-to-Noise Ratio". Evident Scientific. Archived from the original on 2026-03-16. Retrieved 2026-06-28.
  4. ^ Liu, Chao; Jones, Michael E.; Taylor, Angela C. (2021). "Characterizing the performance of high-speed data converters for RFSoC-based radio astronomy receivers". Monthly Notices of the Royal Astronomical Society. 501 (4): 5096–5104. arXiv:2011.05691. doi:10.1093/mnras/staa3895.
  5. ^ a b "Introduction to Radio Astronomy" (PDF). Society of Amateur Radio Astronomers. Archived (PDF) from the original on 2024-10-07. Retrieved 2026-06-28.
  6. ^ Mondal, Rajesh; Barkana, Rennan (2023). "Prospects for precision cosmology with the 21 cm signal from the dark ages". Nature Astronomy. 7 (9): 1025–1030. doi:10.1038/s41550-023-02057-y.
  7. ^ Morello, Giuseppe; Dyrek, Achrène; Changeat, Quentin (2022). "Is binning always sinning? The impact of time-averaging for exoplanet phase curves". Monthly Notices of the Royal Astronomical Society. 517 (2): 2151–2164. arXiv:2210.14194. doi:10.1093/mnras/stac2828.
  8. ^ Daigle, Olivier; Djazovski, Oleg; Dupuis, Jean; Doyon, René; Artigau, Étienne (2014). "Astronomical imaging with EMCCDs using long exposures". In Holland, Andrew D.; Beletic, James (eds.). High Energy, Optical, and Infrared Detectors for Astronomy VI. Vol. 9154. pp. 91540D. doi:10.1117/12.2056617.

Content Disclaimer

Informasi ini disarikan dari Wikipedia dan disajikan kembali untuk tujuan edukasi. Konten tersedia di bawah lisensi CC BY-SA 3.0. Kami tidak bertanggung jawab atas ketidakakuratan data yang bersumber dari kontribusi publik tersebut.

  1. The information displayed on this website is sourced in part or in whole from Wikipedia and has been adapted for the purpose of restating it. We strive to provide accurate and relevant information, however:
  2. There is no guarantee of absolute accuracy. Wikipedia is an open, collaborative project that can be edited by anyone, so information is subject to change.
  3. It is not intended to constitute professional advice. The content displayed is for informational and educational purposes only. For important decisions (e.g., medical, legal, or financial), please consult a professional.
  4. Content copyright. Wikipedia is licensed under the Creative Commons Attribution-ShareAlike License (CC BY-SA). This means that content may be reused with appropriate attribution and shared under a similar license.
  5. Responsible use. Any risk arising from the use of information from this website is entirely the responsibility of the user.