The 1997 spectroscopic GEISA databank

Jacquinet-Husson, N.; Arie, E.; Ballard, J.; Barbe, A.; Bjoraker, G. L.; Bonnet, B.; Brown, Linda R.; Camy‐Peyret, C.; Champion, Jean‐Paul; Chédin, A.; Chursin, A.A.; Clerbaux, Cathy; Duxbury, G.; Flaud, J.-M.; Fourrié, Nadia; Fayt, André; Graner, G.; Gamache, Robert R.; Goldman, A.; Golovko, V. F.; Guelachvili, G.; Hartmann, Jean‐Michel; Hilico, J. C.; Hillman, J. J.; Lefèvre, Georges; Lellouch, E.; Михайленко, С.Н.; Naumenko, O. V.; Nemtchinov, V.; Newnham, David; Nikitin, A.V.; Orphal, J.; Perrin, A.; Reuter, Dennis C.; Rinsland, C. P.; Rosenmann, L.; Rothman, Laurence S.; Scott, N. A.; Selby, John E.; Sinit︠s︡a, L. N.; Sirota, J. Marcos; Smith, Alice M.; Smith, Kevin M.; Tyuterev, Vladimir G.; Tipping, R. H.; Urban, Štěpán; Varanasi, P.; Weber, Mark

doi:10.1016/s0022-4073(98)00111-3

Cited by 245 publications

(89 citation statements)

References 127 publications

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“…the GEISA 5 database (Jacquinet-Husson et al 1999) and we measured their radial velocity in our program stars. The resulting zeropoint corrections, based on 200-250 telluric lines, amount to generally no more than ±1 km s −1 with typical errors in the mean of about 0.5 km s −1 , approximately five times larger than those in the radial velocity measurements.…”

Section: Radial Velocitiesmentioning

confidence: 99%

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Pancino

Carrera

Rossetti

et al. 2010

A&A

196

206

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Context. The present number of Galactic Open Clusters that have high resolution abundance determinations, not only of [Fe/H], but also of other key elements, is largely insufficient to enable a clear modeling of the Galactic Disk chemical evolution. Aims. To increase the number of Galactic Open Clusters with high quality measurements. Methods. We obtained high resolution (R∼30 000), high quality (S/N∼50-100 per pixel), echelle spectra with the fiber spectrograph FOCES, at Calar Alto, Spain, for three red clump stars in each of five Open Clusters. We used the classical Equivalent Width analysis method to obtain accurate abundances of sixteen elements: Al,

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Section: Radial Velocitiesmentioning

confidence: 99%

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Pancino

Carrera

Rossetti

et al. 2010

A&A

196

206

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“…We considered a BC density of 1 g cm −3 , and the refractive index for BC is taken to be m = 1.75-0.45i. Refractive indices for ice are taken from the GEISA database (Jacquinet-Husson et al, 1999). The corresponding mass absorption cross section (MAC) of BC resulting from these assumptions of size distribution, density, and refractive index reaches a value of 7.6 m 2 g −1 at 545 nm (mid-visible, see the MAC definition of Bergrstrom, 2006, andBoucher, 2011).…”

Section: Model Descriptionmentioning

confidence: 99%

Boreal and temperate snow cover variations induced by black carbon emissions in the middle of the 21st century

et al. 2013

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Abstract. We used a coupled climate-chemistry model to quantify the impacts of aerosols on snow cover north of 30 • N both for the present-day and for the middle of the 21st century. Black carbon (BC) deposition over continents induces a reduction in the mean number of days with snow at the surface (MNDWS) that ranges from 0 to 10 days over large areas of Eurasia and Northern America for the presentday relative to the pre-industrial period. This is mainly due to BC deposition during the spring, a period of the year when the remaining of snow accumulated during the winter is exposed to both strong solar radiation and a large amount of aerosol deposition induced themselves by a high level of transport of particles from polluted areas. North of 30 • N, this deposition flux represents 222 Gg BC month −1 on average from April to June in our simulation. A large reduction in BC emissions is expected in the future in all of the Representative Concentration Pathway (RCP) scenarios. In particular, considering the RCP8.5 in our simulation leads to a decrease in the spring BC deposition down to 110 Gg month −1 in the 2050s. However, despite the reduction of the aerosol impact on snow, the MNDWS is strongly reduced by 2050, with a decrease ranging from 10 to 100 days from presentday values over large parts of the Northern Hemisphere. This reduction is essentially due to temperature increase, which is quite strong in the RCP8.5 scenario in the absence of climate mitigation policies. Moreover, the projected sea-ice retreat in the next decades will open new routes for shipping in the Arctic. However, a large increase in shipping emissions in the Arctic by the mid-21st century does not lead to significant changes of BC deposition over snow-covered areas in our simulation. Therefore, the MNDWS is clearly not affected through snow darkening effects associated with these Arctic ship emissions. In an experiment without nudging toward atmospheric reanalyses, we simulated however some changes of the MNDWS considering such aerosol ship emissions. These changes are generally not statistically significant in boreal continents, except in Quebec and in the West Siberian plains, where they range between −5 and −10 days. They are induced both by radiative forcings of the aerosols when they are in the snow and in the atmosphere, and by all the atmospheric feedbacks. These experiments do not take into account the feedbacks induced by the interactions between ocean and atmosphere as they were conducted with prescribed sea surface temperatures. Climate change by the mid-21st century could also cause biomass burning activity (forest fires) to become more intense and occur earlier in the season. In an idealised scenario in which forest fires are 50 % stronger and occur 2 weeks earlier and later than at present, we simulated an increase in spring BC deposition of 21 Gg BC month −1 over continents located north of 30 • N. This BC deposition does not impact directly the snow cover through snow darkening effects. However, in an experiment considering ...

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“…The Rayleigh-scattering cross sections of O 2 are calculated following Sneep & Ubachs (2005) using refractive indices from Bates (1984). We retrieved the UV/visible photoabsorption cross section of O 3 at 293 K and 1 bar from the GEISA 1997 data base (Jacquinet-Husson et al 1999). We recall here that we are not doing a fit of our data but just compute altitude signatures related to a "standard" Earth atmospheric model.…”

Section: Model Calculationmentioning

confidence: 99%

The Earth as an extrasolar transiting planet

Vidal‐Madjar

Arnold

Ehrenreich

et al. 2010

A&A

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Context. An important goal within the quest for detecting an Earth-like extrasolar planet, will be to identify atmospheric gaseous bio-signatures. Aims. Observations of the light transmitted through the Earth's atmosphere, as for an extrasolar planet, will be the first important step for future comparisons. We have completed observations of the Earth during a lunar eclipse, a unique situation similar to that of a transiting planet. We aim at showing what species could be detected in its atmosphere at optical wavelengths, where a lot of photons are available in the masked stellar light. Methods. We present observations of the 2008 August 16 Moon eclipse performed with the SOPHIE spectrograph at the Observatoire de Haute-Provence (France). Locating the spectrograph's fibers in the penumbra of the eclipse, the Moon irradiance is then a mix of direct, unabsorbed Sun light and solar light that has passed through the Earth's atmosphere. This mixture essentially reproduces what is recorded during the transit of an extrasolar planet. Results. We report here the clear detection of several Earth atmospheric compounds in the transmission spectra, such as ozone, molecular oxygen, and neutral sodium as well as molecular nitrogen and oxygen through the Rayleigh signature. Moreover, we present a method that allows us to derive the thickness of the atmosphere versus the wavelength for penumbra eclipse observations. We quantitatively evaluate the altitude at which the atmosphere becomes transparent for important species like molecular oxygen and ozone, two species thought to be tightly linked to the presence of life. Conclusions. The molecular detections presented here are an encouraging first attempt, necessary to better prepare for the future of extremely-large telescopes and transiting Earth-like planets. Instruments like SOPHIE will be mandatory when characterizing the atmospheres of transiting Earth-like planets from the ground and searching for bio-marker signatures.

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The 1997 spectroscopic GEISA databank

Cited by 245 publications

References 127 publications

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Boreal and temperate snow cover variations induced by black carbon emissions in the middle of the 21st century

The Earth as an extrasolar transiting planet

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