Using an absorption cell, we measured the Doppler shifts of the interstellar hydrogen resonance glow to show the direction of the neutral hydrogen flow as it enters the inner heliosphere. The neutral hydrogen flow is found to be deflected relative to the helium flow by about 4 degrees . The most likely explanation of this deflection is a distortion of the heliosphere under the action of an ambient interstellar magnetic field. In this case, the helium flow vector and the hydrogen flow vector constrain the direction of the magnetic field and act as an interstellar magnetic compass.

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: O 2 , H 2 O, O 3 , CO 2 , CH 4 , N 2 O, 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 O 2 and H 2 O 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.

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