In infrared astronomy, the H band refers to an atmospheric transmission window centred on 1.65 micrometres with a Full width at half maximum of 0.35 micrometres[1] (in the near-infrared).
Save for a limited amount of absorption by water vapor, Earth's atmosphere is highly translucent at the wavelengths covered by the H band.[2] The window is also notably less likely to be contaminated by infrared excess than other bands.[3]
The band is useful for a range of infrared observations including the imaging of sunspots, spectroscopic investigation of late-type stars, and imaging planetary phenomena such as extraterrestrial vortices or volcanic activity in the solar system.[4] In addition stellar atmospheres are highly transparent in the H band and stellar light in the window originates from deeper in the stellar atmosphere than any other band. It also includes within it access to several sets of spectral lines including for carbon monoxide and cyanide.[5]
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References
- ^ Ian McClean, Electronic Imaging in Astronomy, Second Edition, Springer, 2008.
- ^ "Infrared Astronomy Optical Filters". www.andovercorp.com. Retrieved 2023-04-08.
- ^ Hanson, M. M.; Rieke, G. H.; Luhman, K. L. (October 1998). "Near-infrared H-band features in late O and B stars". Astronomical Journal. 116 (4): 1915–1921. Bibcode:1998AJ....116.1915H. doi:10.1086/300556. ISSN 0004-6256.
- ^ "InGaAs Cameras for Ground-Based NIR-II/SWIR Astronomy". Teledyne Princeton Instruments. Retrieved 2023-04-08.
- ^ Wing, Robert; Jørgensen, Uffe (December 2003). "Stellar Spectra in the H Band". The Journal of the American Association of Variable Star Observers. 31 (2): 110–120. Bibcode:2003JAVSO..31..110W.
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This page was last edited on 16 September 2023, at 23:22