TAPAS, a web-based service of atmospheric transmission computation for astronomy^⋆

¹ LATMOS, University of Versailles Saint-Quentin, 11 boulevard d’Alembert, 78280 Guyancourt, France
e-mail: jean-loup.bertaux@latmos.ipsl.fr
² GEPI, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France
e-mail: rosine.lallement@obspm.fr
³ ACRI-ST, BP234, 260 route du Pin Montard, 06904 Sophia-Antipolis, France
⁴ IPSL, Institut Pierre-Simon Laplace, Place Jussieu, 75252 Paris, France

Received: 28 July 2013
Accepted: 3 February 2014

Abstract

Context. Spectra of astronomical targets acquired from ground-based instruments are affected by the atmospheric transmission.

Aims. The authors and their institutes are developing a web-based service, TAPAS (Transmissions Atmosphériques Personnalisées pour l’AStronomie, or Transmissions of the AtmosPhere for AStromomical data). This service, freely available, is developed and maintained within the atmospheric ETHER data center.

Methods. TAPAS computes the atmospheric transmission in the line-of-sight (LOS) to the target indicated by the user. The user files a request indicating the time, ground location, and either the equatorial coordinates of the target or the zenith angle of the LOS. The actual atmospheric profile (temperature, pressure, humidity, ozone content) at that time and place is retrieved from the ETHER atmospheric database (from a combination of ECMWF meteorological field and other information), and the atmospheric transmission is computed from LBLRTM software and HITRAN database for a number of gases: O₂, H₂O, O₃, CO₂, CH₄, N₂O, and Rayleigh extinction. The first purpose of TAPAS output is to allow identifying observed spectral features having an atmospheric or astrophysical origin. The returned transmission may also serve for characterizing the spectrometer on the wavelength scale and instrument line spectral function (ILSF) by comparing one observed spectrum of an atmospheric feature to the transmission. Finally, the top of atmosphere (TOA) spectrum may be obtained either by division of the observed spectrum by the computed transmission or other techniques developed on purpose. The obtention of transmissions for individual species allows more potentialities and better adjustments to the data.

Results. In this paper, we briefly describe the mechanism of computation of the atmospheric transmissions, and we show some results for O₂ and H₂O atmospheric absorption. The wavelength range is presently 500–2500 nm, but may be extended in the future.

Conclusions. It is hoped that this service will help many astronomers in their research. The user may also contribute to the general knowledge of the atmospheric transmission, if he/she finds systematic discrepancies between synthetic transmissions and the observed spectra. This has already happened in the recent past.