GNOSIS: an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings

J. S. Lawrence, S. C. Ellis, J. Bland-Hawthorn, J. Bryant, S. Case, L. Gers, R. Haynes, A. Horton, S. Lee, S. Leon-Saval, H. Loehmannsroeben, S. Miziarski, J. Mladenoff, J. O'Byrne, W. Rambold, M. Roth, S. Smedley, C. Trinh

Research output: Chapter in Book/Report/Conference proceedingConference proceeding contributionResearch

Abstract

Astronomical near-infrared spectroscopy is made difficult by the extremely bright and variable night sky background. The night sky surface brightness is more than a thousand times brighter at 1.6m than at 0.4m. Furthermore the brightness of the sky changes by factors of 10% on time-scales of minutes. Background-subtraction is therefore frustrated by high Poisson noise from the extreme brightness, and by systematic noise from the variability. Between 1.0 and 1.8 m almost all of this background results from the rotational and vibrational de-excitiation of hydroxyl molecules located at 90 km in the atmosphere. The hydroxyl emission lines are intrinsically very bright, but very narrow. Between the OH lines the sky should be very dark; it is expected that the interline continuum is dominated by the zodiacal scattered light. Therefore selectively filtering the OH lines would enable deep near-infrared observations.

LanguageEnglish
Title of host publicationCLEO/Europe and EQEC 2011 Conference Digest
Place of PublicationPiscataway, N.J.
PublisherInstitute of Electrical and Electronics Engineers (IEEE)
Pages1-1
Number of pages1
ISBN (Electronic)9781457705328
ISBN (Print)9781457705335
DOIs
Publication statusPublished - 2011
EventCLEO/Europe and EQEC Conference - 2011 - Munich, Germany
Duration: 22 May 201126 May 2011

Other

OtherCLEO/Europe and EQEC Conference - 2011
CountryGermany
CityMunich
Period22/05/1126/05/11

Fingerprint

Infrared spectrographs
Astronomy
Fiber Bragg gratings
Luminance
Near infrared spectroscopy
Infrared radiation
Molecules

Cite this

Lawrence, J. S., Ellis, S. C., Bland-Hawthorn, J., Bryant, J., Case, S., Gers, L., ... Trinh, C. (2011). GNOSIS: an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings. In CLEO/Europe and EQEC 2011 Conference Digest (pp. 1-1). [5943684] Piscataway, N.J.: Institute of Electrical and Electronics Engineers (IEEE). https://doi.org/10.1109/CLEOE.2011.5943684
Lawrence, J. S. ; Ellis, S. C. ; Bland-Hawthorn, J. ; Bryant, J. ; Case, S. ; Gers, L. ; Haynes, R. ; Horton, A. ; Lee, S. ; Leon-Saval, S. ; Loehmannsroeben, H. ; Miziarski, S. ; Mladenoff, J. ; O'Byrne, J. ; Rambold, W. ; Roth, M. ; Smedley, S. ; Trinh, C. / GNOSIS : an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings. CLEO/Europe and EQEC 2011 Conference Digest. Piscataway, N.J. : Institute of Electrical and Electronics Engineers (IEEE), 2011. pp. 1-1
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title = "GNOSIS: an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings",
abstract = "Astronomical near-infrared spectroscopy is made difficult by the extremely bright and variable night sky background. The night sky surface brightness is more than a thousand times brighter at 1.6m than at 0.4m. Furthermore the brightness of the sky changes by factors of 10{\%} on time-scales of minutes. Background-subtraction is therefore frustrated by high Poisson noise from the extreme brightness, and by systematic noise from the variability. Between 1.0 and 1.8 m almost all of this background results from the rotational and vibrational de-excitiation of hydroxyl molecules located at 90 km in the atmosphere. The hydroxyl emission lines are intrinsically very bright, but very narrow. Between the OH lines the sky should be very dark; it is expected that the interline continuum is dominated by the zodiacal scattered light. Therefore selectively filtering the OH lines would enable deep near-infrared observations.",
author = "Lawrence, {J. S.} and Ellis, {S. C.} and J. Bland-Hawthorn and J. Bryant and S. Case and L. Gers and R. Haynes and A. Horton and S. Lee and S. Leon-Saval and H. Loehmannsroeben and S. Miziarski and J. Mladenoff and J. O'Byrne and W. Rambold and M. Roth and S. Smedley and C. Trinh",
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doi = "10.1109/CLEOE.2011.5943684",
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Lawrence, JS, Ellis, SC, Bland-Hawthorn, J, Bryant, J, Case, S, Gers, L, Haynes, R, Horton, A, Lee, S, Leon-Saval, S, Loehmannsroeben, H, Miziarski, S, Mladenoff, J, O'Byrne, J, Rambold, W, Roth, M, Smedley, S & Trinh, C 2011, GNOSIS: an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings. in CLEO/Europe and EQEC 2011 Conference Digest., 5943684, Institute of Electrical and Electronics Engineers (IEEE), Piscataway, N.J., pp. 1-1, CLEO/Europe and EQEC Conference - 2011, Munich, Germany, 22/05/11. https://doi.org/10.1109/CLEOE.2011.5943684

GNOSIS : an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings. / Lawrence, J. S.; Ellis, S. C.; Bland-Hawthorn, J.; Bryant, J.; Case, S.; Gers, L.; Haynes, R.; Horton, A.; Lee, S.; Leon-Saval, S.; Loehmannsroeben, H.; Miziarski, S.; Mladenoff, J.; O'Byrne, J.; Rambold, W.; Roth, M.; Smedley, S.; Trinh, C.

CLEO/Europe and EQEC 2011 Conference Digest. Piscataway, N.J. : Institute of Electrical and Electronics Engineers (IEEE), 2011. p. 1-1 5943684.

Research output: Chapter in Book/Report/Conference proceedingConference proceeding contributionResearch

TY - GEN

T1 - GNOSIS

T2 - an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings

AU - Lawrence,J. S.

AU - Ellis,S. C.

AU - Bland-Hawthorn,J.

AU - Bryant,J.

AU - Case,S.

AU - Gers,L.

AU - Haynes,R.

AU - Horton,A.

AU - Lee,S.

AU - Leon-Saval,S.

AU - Loehmannsroeben,H.

AU - Miziarski,S.

AU - Mladenoff,J.

AU - O'Byrne,J.

AU - Rambold,W.

AU - Roth,M.

AU - Smedley,S.

AU - Trinh,C.

PY - 2011

Y1 - 2011

N2 - Astronomical near-infrared spectroscopy is made difficult by the extremely bright and variable night sky background. The night sky surface brightness is more than a thousand times brighter at 1.6m than at 0.4m. Furthermore the brightness of the sky changes by factors of 10% on time-scales of minutes. Background-subtraction is therefore frustrated by high Poisson noise from the extreme brightness, and by systematic noise from the variability. Between 1.0 and 1.8 m almost all of this background results from the rotational and vibrational de-excitiation of hydroxyl molecules located at 90 km in the atmosphere. The hydroxyl emission lines are intrinsically very bright, but very narrow. Between the OH lines the sky should be very dark; it is expected that the interline continuum is dominated by the zodiacal scattered light. Therefore selectively filtering the OH lines would enable deep near-infrared observations.

AB - Astronomical near-infrared spectroscopy is made difficult by the extremely bright and variable night sky background. The night sky surface brightness is more than a thousand times brighter at 1.6m than at 0.4m. Furthermore the brightness of the sky changes by factors of 10% on time-scales of minutes. Background-subtraction is therefore frustrated by high Poisson noise from the extreme brightness, and by systematic noise from the variability. Between 1.0 and 1.8 m almost all of this background results from the rotational and vibrational de-excitiation of hydroxyl molecules located at 90 km in the atmosphere. The hydroxyl emission lines are intrinsically very bright, but very narrow. Between the OH lines the sky should be very dark; it is expected that the interline continuum is dominated by the zodiacal scattered light. Therefore selectively filtering the OH lines would enable deep near-infrared observations.

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U2 - 10.1109/CLEOE.2011.5943684

DO - 10.1109/CLEOE.2011.5943684

M3 - Conference proceeding contribution

SN - 9781457705335

SP - 1

EP - 1

BT - CLEO/Europe and EQEC 2011 Conference Digest

PB - Institute of Electrical and Electronics Engineers (IEEE)

CY - Piscataway, N.J.

ER -

Lawrence JS, Ellis SC, Bland-Hawthorn J, Bryant J, Case S, Gers L et al. GNOSIS: an OH suppressing near-infrared spectrograph for astronomy using fibre Bragg gratings. In CLEO/Europe and EQEC 2011 Conference Digest. Piscataway, N.J.: Institute of Electrical and Electronics Engineers (IEEE). 2011. p. 1-1. 5943684 https://doi.org/10.1109/CLEOE.2011.5943684