Author name code: sauval ADS astronomy entries on 2022-09-14 author:"Sauval, A. Jacques" ------------------------------------------------------------------------ Title: The elemental composition of the Sun. III. The heavy elements Cu to Th Authors: Grevesse, Nicolas; Scott, Pat; Asplund, Martin; Sauval, A. Jacques Bibcode: 2015A&A...573A..27G Altcode: 2014arXiv1405.0288G We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data that we have employed.

Tables 1-3 are available in electronic form at http://www.aanda.org Title: The elemental composition of the Sun. II. The iron group elements Sc to Ni Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Bergemann, Maria; Sauval, A. Jacques Bibcode: 2015A&A...573A..26S Altcode: 2014arXiv1405.0287S We redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log ɛSc = 3.16 ± 0.04, log ɛTi = 4.93 ± 0.04, log ɛV = 3.89 ± 0.08, log ɛCr = 5.62 ± 0.04, log ɛMn = 5.42 ± 0.04, log ɛFe = 7.47 ± 0.04, log ɛCo = 4.93 ± 0.05 and log ɛNi = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data we employed.

Tables 1-3 are available in electronic form at http://www.aanda.org Title: The elemental composition of the Sun. I. The intermediate mass elements Na to Ca Authors: Scott, Pat; Grevesse, Nicolas; Asplund, Martin; Sauval, A. Jacques; Lind, Karin; Takeda, Yoichi; Collet, Remo; Trampedach, Regner; Hayek, Wolfgang Bibcode: 2015A&A...573A..25S Altcode: 2014arXiv1405.0279S The chemical composition of the Sun is an essential piece of reference data for astronomy, cosmology, astroparticle, space and geo-physics: elemental abundances of essentially all astronomical objects are referenced to the solar composition, and basically every process involving the Sun depends on its composition. This article, dealing with the intermediate-mass elements Na to Ca, is the first in a series describing the comprehensive re-determination of the solar composition. In this series we severely scrutinise all ingredients of the analysis across all elements, to obtain the most accurate, homogeneous and reliable results possible. We employ a highly realistic 3D hydrodynamic model of the solar photosphere, which has successfully passed an arsenal of observational diagnostics. For comparison, and to quantify remaining systematic errors, we repeat the analysis using three different 1D hydrostatic model atmospheres (marcs, miss and Holweger & Müller 1974, Sol. Phys., 39, 19) and a horizontally and temporally-averaged version of the 3D model (⟨ 3D ⟩). We account for departures from local thermodynamic equilibrium (LTE) wherever possible. We have scoured the literature for the best possible input data, carefully assessing transition probabilities, hyperfine splitting, partition functions and other data for inclusion in the analysis. We have put the lines we use through a very stringent quality check in terms of their observed profiles and atomic data, and discarded all that we suspect to be blended. Our final recommended 3D+NLTE abundances are: log ɛNa = 6.21 ± 0.04, log ɛMg = 7.59 ± 0.04, log ɛAl = 6.43 ± 0.04, log ɛSi = 7.51 ± 0.03, log ɛP = 5.41 ± 0.03, log ɛS = 7.13 ± 0.03, log ɛK = 5.04 ± 0.05 and log ɛCa = 6.32 ± 0.03. The uncertainties include both statistical and systematic errors. Our results are systematically smaller than most previous ones with the 1D semi-empirical Holweger & Müller model, whereas the ⟨ 3D ⟩ model returns abundances very similar to the full 3D calculations. This analysis provides a complete description and a slight update of the results presented in Asplund et al. (2009, ARA&A, 47, 481) for Na to Ca, and includes full details of all lines and input data used.

Tables 1-4 and Appendix A are available in electronic form at http://www.aanda.org Title: ``Old'' versus ``New'' Solar Chemical Composition Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 2013ASPC..479..481G Altcode: We follow the evolution since 1989 of element abundance determinations in the solar photosphere. We describe how the largely used high metallicity mixtures (Z = 0.02 to 0.017) of Anders & Grevesse (1989), Grevesse & Noels (1993) and Grevesse & Sauval (1998) have been obtained and explain why these mixtures should not be used anymore. They are to be replaced by the more recent mixture of Asplund et al. (2009) which results from the first comprehensive and homogeneous analysis for many decades. We describe the main characteristics of this work and discuss some impacts of this low Z (Z = 0.0134) mixture. We also comment on another recent analysis by Caffau et al. (2011) that leads to somewhat larger metal abundances. Title: The New Solar Chemical Composition — from Z = 0.02 to Z = 0.013 Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 2012ASPC..462...41G Altcode: We review the current status of our knowledge of the chemical composition of the sun and present a redetermination of the solar abundances of all available elements. These new results have recently been published by Asplund et al. (2009). The basic ingredients of this work, the main results and their implications are discussed. We show why the abundances of the main contributors to the metallicity have decreased and why the old high solar metallicity, Z ∼ 0.02, is definitely obsolete and should not be used anymore. We also show why other recent analyzes of the solar composition report solar metallicities somewhat larger than the one we recommend. Title: The chemical composition of the sun Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 2011CaJPh..89..327G Altcode: No abstract at ADS Title: The New Solar Composition and the Solar Metallicity Authors: Grevesse, Nicolas; Asplund, Martin; Sauval, A. Jacques; Scott, Pat Bibcode: 2011sswh.book...51G Altcode: No abstract at ADS Title: The chemical composition of the Sun Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 2010Ap&SS.328..179G Altcode: 2010Ap&SS.tmp...48G We present a redetermination of the solar abundances of all available elements. The new results have very recently been published by Asplund et al. (Annu. Rev. Astron. Astrophys. 47:481, 2009). The basic ingredients of this work, the main results and some of their implications are summarized hereafter. Title: The Chemical Composition of the Sun Authors: Asplund, Martin; Grevesse, Nicolas; Sauval, A. Jacques; Scott, Pat Bibcode: 2009ARA&A..47..481A Altcode: 2009arXiv0909.0948A The solar chemical composition is an important ingredient in our understanding of the formation, structure, and evolution of both the Sun and our Solar System. Furthermore, it is an essential reference standard against which the elemental contents of other astronomical objects are compared. In this review, we evaluate the current understanding of the solar photospheric composition. In particular, we present a redetermination of the abundances of nearly all available elements, using a realistic new three-dimensional (3D), time-dependent hydrodynamical model of the solar atmosphere. We have carefully considered the atomic input data and selection of spectral lines, and accounted for departures from local thermodynamic equilibrium (LTE) whenever possible. The end result is a comprehensive and homogeneous compilation of the solar elemental abundances. Particularly noteworthy findings are significantly lower abundances of C, N, O, and Ne compared to the widely used values of a decade ago. The new solar chemical composition is supported by a high degree of internal consistency between available abundance indicators, and by agreement with values obtained in the Solar Neighborhood and from the most pristine meteorites. There is, however, a stark conflict with standard models of the solar interior according to helioseismology, a discrepancy that has yet to find a satisfactory resolution. Title: Experimental and theoretical radiative decay rates for highly excited ruthenium atomic levels and the solar abundance of ruthenium Authors: Fivet, V.; Quinet, P.; Palmeri, P.; Biémont, É.; Asplund, M.; Grevesse, N.; Sauval, A. J.; Engström, L.; Lundberg, H.; Hartman, H.; Nilsson, H. Bibcode: 2009MNRAS.396.2124F Altcode: 2009MNRAS.tmp..738F The solar photospheric abundance of ruthenium is revised on the basis of a new set of oscillator strengths derived for RuI transitions with wavelengths in the spectral range 2250-4710 Å. The new abundance value (in the usual logarithmic scale where the solar hydrogen abundance is equal to 12.00), ARu = 1.72 +/- 0.10, is in agreement with the most recent meteoritic result, ARu = 1.76 +/- 0.03. The accuracy of the transition probabilities, obtained using a relativistic Hartree-Fock model including core-polarization effects, has been assessed by comparing the theoretical lifetimes with previous experimental results. A comparison is also made with new measurements performed in this work by the time-resolved laser-induced fluorescence spectroscopy for 10 highly excited odd-parity levels of RuI. Title: On the Solar Nickel and Oxygen Abundances Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Sauval, A. Jacques Bibcode: 2009ApJ...691L.119S Altcode: 2008arXiv0811.0815S Determinations of the solar oxygen content relying on the neutral forbidden transition at 630 nm depend upon the nickel abundance, due to a Ni I blend. Here, we rederive the solar nickel abundance, using the same ab initio three-dimensional hydrodynamic model of the solar photosphere employed in the recent revision of the abundances of C, N, O, and other elements. Using 17 weak, unblended lines of Ni I together with the most accurate atomic and observational data available, we find log epsilonNi = 6.17 ± 0.02(statistical) ± 0.05(systematic), a downward shift of 0.06-0.08 dex relative to previous abundances based on one-dimensional model atmospheres. We investigate the implications of the new nickel abundance for studies of the solar oxygen abundance based on the [O I] 630 nm line in the quiet Sun. Furthermore, we demonstrate that the oxygen abundance implied by the recent sunspot spectropolarimetric study of Centeno & Socas-Navarro needs to be revised downward from log epsilonO = 8.86 ± 0.07 to 8.71 ± 0.10. This revision is based on the new nickel abundance, the application of the best available gf value for the 630 nm forbidden oxygen line, and a more transparent treatment of CO formation. Determinations of the solar oxygen content relying on forbidden lines now appear to converge around log epsilonO = 8.7. Title: The Solar Chemical Composition Authors: Grevesse, N.; Asplund, M.; Sauval, A. J. Bibcode: 2007SSRv..130..105G Altcode: 2007SSRv..tmp..105G We present our current knowledge of the solar chemical composition based on the recent significant downward revision of the solar photospheric abundances of the most abundant metals. These new solar abundances result from the use of a 3D hydrodynamic model of the solar atmosphere instead of the classical 1D hydrostatic models, accounting for departures from LTE, and improved atomic and molecular data. With these abundances, the new solar metallicity, Z, decreases to Z=0.012, almost a factor of two lower than earlier widely used values. We compare our values with data from other sources and analyse a number of impacts of these new photospheric abundances. While resolving a number of longstanding problems, the new 3D-based solar photospheric composition also poses serious challenges for the standard solar model as judged by helioseismology. Title: The Solar Chemical Composition Authors: Grevesse, N.; Asplund, M.; Sauval, A. J. Bibcode: 2007coma.book..105G Altcode: We present our current knowledge of the solar chemical composition based on the recent significant downward revision of the solar photospheric abundances of the most abundant metals. These new solar abundances result from the use of a 3D hydrodynamic model of the solar atmosphere instead of the classical 1D hydrostatic models, accounting for departures from LTE, and improved atomic and molecular data. With these abundances, the new solar metallicity, Z, decreases to Z=0.012, almost a factor of two lower than earlier widely used values. We compare our values with data from other sources and analyse a number of impacts of these new photospheric abundances. While resolving a number of longstanding problems, the new 3D-based solar photospheric composition also poses serious challenges for the standard solar model as judged by helioseismology. Title: Line formation in solar granulation. VII. CO lines and the solar C and O isotopic abundances Authors: Scott, P. C.; Asplund, M.; Grevesse, N.; Sauval, A. J. Bibcode: 2006A&A...456..675S Altcode: 2006astro.ph..5116S CO spectral line formation in the Sun has long been a source of consternation for solar physicists, as have the elemental abundances it seems to imply. We modelled solar CO line formation using a realistic, ab initio, time-dependent 3D radiative-hydrodynamic model atmosphere. Results were compared with space-based observations from the ATMOS space shuttle experiment. We employed weak 12C16O, 13C16O and 12C18O lines from the fundamental (Δ v = 1) and first overtone (Δ v = 2) bands to determine the solar carbon abundance, as well as the 12C/13C and 16O/18O isotopic ratios. A weighted solar carbon abundance of logɛ_C=8.39 ± 0.05 was found. We note with satisfaction that the derived abundance is identical to our recent 3D determination based on C i, [C i], C2 and CH lines, increasing our confidence in the accuracy of both results. Identical calculations were carried out using 1D models, but only the 3D model was able to produce abundance agreement between different CO lines and the other atomic and molecular diagnostics. Solar 12C/13C and 16O/18O ratios were measured as 86.8+3.9-3.7 (δ13C = 30+46-44) and 479+29-28 (δ18O = 41+67-59), respectively. These values may require current theories of solar system formation, such as the CO self-shielding hypothesis, to be revised. Excellent agreement was seen between observed and predicted weak CO line shapes, without invoking micro- or macroturbulence. Agreement breaks down for the strongest CO lines however, which are formed in very high atmospheric layers. Whilst the line asymmetries (bisectors) were reasonably well reproduced, line strengths predicted on the basis of C and O abundances from other diagnostics were weaker than observed. The simplest explanation is that temperatures are overestimated in the highest layers of the 3D simulation. Thus, our analysis supports the presence of a COmosphere above the traditional photospheric temperature minimum, with an average temperature of less than 4000 K. This shortcoming of the 3D model atmosphere is not surprising, given that it was never intended to properly describe such high layers. Title: The new solar abundances - Part I: the observations Authors: Asplund, M.; Grevesse, N.; Sauval, A. J. Bibcode: 2006CoAst.147...76A Altcode: The new solar abundances have been derived from analyses of the photospheric spectrum. They result from the use of a 3D hydrodynamical model of the solar atmosphere instead of the classical 1D hydrostatic models, accounting for departures from LTE when possible and improved atomic and molecular data. The new solar abundances are lower than previously recommended values and the present solar metallicity, Z, and Z/X, decrease to Z = 0.0122 and Z/X = 0.0165 respectively, almost a factor of two lower than earlier widely used values. We briefly discuss the new results for the most abundant elements, show why they are trustworthy and discuss some implications (see also Montalban et al. 2006, Part II). Title: The solar model problem resurrected Authors: Asplund, M.; Grevesse, N.; Guedel, M.; Sauval, A. J. Bibcode: 2005astro.ph.10377A Altcode: The new solar composition, when applied to compute a model of the Sun, leads to serious disagreement between the predictions of the model and the observations obtained by helioseismology. New measurements of the coronal Ne/O abundance ratio in nearby stars using X-ray spectra typically find high values of Ne/O=0.4 rather than 0.15 normally adopted for the Sun. Drake & Testa (2005) suggest that this high Ne/O ratio is appropriate also for the Sun, which would bring the solar models back in agreement with the helioseismological observations. Here we present arguments why the high Ne/O ratio is unlikely to be applicable to the Sun. Title: The Solar Chemical Composition Authors: Asplund, M.; Grevesse, N.; Sauval, A. J. Bibcode: 2005ASPC..336...25A Altcode: We review our current knowledge of the solar chemical composition as determined from photospheric absorption lines. In particular we describe the recent significant revisions of the solar abundances as a result of the application of a time-dependent, 3D hydrodynamical model of the solar atmosphere instead of 1D hydrostatic models. This has decreased the metal content in the solar convection zone by almost a factor of two compared with the widely used compilation by Anders & Grevesse (1989). While resolving a number of long-standings problems, the new 3D-based element abundances also pose serious challenges, most notably for helioseismology. Title: Line formation in solar granulation. IV. [O I], O I and OH lines and the photospheric O abundance Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto, C.; Kiselman, D. Bibcode: 2005A&A...435..339A Altcode: A&A, 417, 751-768 (2004), DOI:10.1051/0004-6361:20034328 Title: Line formation in solar granulation. VI. [C I], C I, CH and C2 lines and the photospheric C abundance Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto, C.; Blomme, R. Bibcode: 2005A&A...431..693A Altcode: 2004astro.ph.10681A The solar photospheric carbon abundance has been determined from [C I], C I, CH vibration-rotation, CH A-X electronic and C2 Swan electronic lines by means of a time-dependent, 3D, hydrodynamical model of the solar atmosphere. Departures from LTE have been considered for the C I lines. These turned out to be of increasing importance for stronger lines and are crucial to remove a trend in LTE abundances with the strengths of the lines. Very gratifying agreement is found among all the atomic and molecular abundance diagnostics in spite of their widely different line formation sensitivities. The mean value of the solar carbon abundance based on the four primary abundance indicators ([C I], C I, CH vibration-rotation, C2 Swan) is log ɛC = 8.39 ± 0.05, including our best estimate of possible systematic errors. Consistent results also come from the CH electronic lines, which we have relegated to a supporting role due to their sensitivity to the line broadening. The new 3D based solar C abundance is significantly lower than previously estimated in studies using 1D model atmospheres. Title: The New Solar Chemical Composition Authors: Grevesse, N.; Asplund, M.; Sauval, A. J. Bibcode: 2005EAS....17...21G Altcode: We present our current knowledge of the solar chemical composition based on the recent significant downward revision of the solar photospheric abundances of the most abundant metals very recently reviewed in detail by Asplund et al. (2005a). These new solar abundances result from the use of a 3D hydrodynamical model of the solar atmosphere instead of the classical 1D hydrostatic models, accounting for departures from LTE, and improved atomic and molecular data. With these abundances, the new solar metallicity, Z, and Z/X, decrease to Z = 0.012 and Z/X = 0.0165 respectively, almost a factor of 2 lower than earlier widely used values. While resolving a number of longstanding problems, the new 3D-based solar photospheric composition also poses serious challenges for the standard solar model. Title: Line formation in solar granulation. IV. [O I], O I and OH lines and the photospheric O abundance Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto, C.; Kiselman, D. Bibcode: 2004A&A...417..751A Altcode: 2003astro.ph.12290A The solar photospheric oxygen abundance has been determined from [O I], O I, OH vibration-rotation and OH pure rotation lines by means of a realistic time-dependent, 3D, hydrodynamical model of the solar atmosphere. In the case of the O I lines, 3D non-LTE calculations have been performed, revealing significant departures from LTE as a result of photon losses in the lines. We derive a solar oxygen abundance of log ɛO = 8.66 ± 0.05. All oxygen diagnostics yield highly consistent abundances, in sharp contrast with the results of classical 1D model atmospheres. This low value is in good agreement with measurements of the local interstellar medium and nearby B stars. This low abundance is also supported by the excellent correspondence between lines of very different line formation sensitivities, and between the observed and predicted line shapes and center-to-limb variations. Together with the corresponding down-ward revisions of the solar carbon, nitrogen and neon abundances, the resulting significant decrease in solar metal mass fraction to Z = 0.0126 can, however, potentially spoil the impressive agreement between predicted and observed sound speed in the solar interior determined from helioseismology. Title: ISO-SWS calibration and the accurate modelling of cool-star atmospheres. III. A0 to G2 stars Authors: Decin, L.; Vandenbussche, B.; Waelkens, K.; Eriksson, C.; Gustafsson, B.; Plez, B.; Sauval, A. J. Bibcode: 2003A&A...400..695D Altcode: 2002astro.ph..7636D Vega, Sirius, beta Leo, alpha Car and alpha Cen A belong to a sample of twenty stellar sources used for the calibration of the detectors of the Short-Wavelength Spectrometer on board the Infrared Space Observatory (ISO-SWS). While general problems with the calibration and with the theoretical modelling of these stars are reported in {Decin} et al. (\cite{Decin2000b}), each of these stars is discussed individually in this paper. As demonstrated in {Decin} et al. (\cite{Decin2000b}), it is not possible to deduce the effective temperature, the gravity and the chemical composition from the ISO-SWS spectra of these stars. But since ISO-SWS is absolutely calibrated, the angular diameter (thetad ) of these stellar sources can be deduced from their ISO-SWS spectra, which consequently yields the stellar radius (R), the gravity-inferred mass (Mg) and the luminosity (L) for these stars. For Vega, we obtained thetad = 3.35 +/- 0.20 mas, R = 2.79 +/- 0.17 Rsun, Mg = 2.54 +/- 1.21 Msun and L = 61 +/- 9 Lsun; for Sirius thetad = 6.17 +/- 0.38 mas, R = 1.75 +/- 0.11 Rsun, Mg = 2.22 +/- 1.06 Msun and L = 29 +/- 6 Lsun; for beta Leo thetad = 1.47 +/- 0.09 mas, R = 1.75 +/- 0.11 Rsun, Mg = 1.78 +/- 0.46 Msun and L = 15 +/- 2 Lsun; for alpha Car thetad = 7.22 +/- 0.42 mas, R = 74.39 +/- 5.76 Rsun, Mg = 12.80+24.95-6.35 Msun and L = 14573 +/- 2268 Lsun and for alpha Cen A thetad = 8.80 +/- 0.51 mas, R = 1.27 +/- 0.08 Rsun, Mg = 1.35 +/- 0.22 Msun and L = 1.7 +/- 0.2 Lsun. These deduced parameters are confronted with other published values and the goodness-of-fit between observed ISO-SWS data and the corresponding synthetic spectrum is discussed.

Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries France, Germany, The Netherlands and the UK) and with the participation of ISAS and NASA.}\fnmsep\thanks{Appendices A and B are only available in electronic form at http://www.edpsciences.org} Title: ISO-SWS calibration and the accurate modelling of cool-star atmospheres. IV. G9 to M2 stars Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Decin, G.; Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J. Bibcode: 2003A&A...400..709D Altcode: 2002astro.ph..7653D A detailed spectroscopic study of 11 giants with spectral type from G9 to M2 is presented. The 2.38-4.08 mu m wavelength-range of band 1 of ISO-SWS (Short-Wavelength Spectrometers on board of the Infrared Space Observatory) in which many different molecules - with their own dependence on each of the stellar parameters - are absorbing, enables us to estimate the effective temperature, the gravity, the microturbulence, the metallicity, the CNO-abundances, the 12C/13C-ratio and the angular diameter from the ISO-SWS data. Using the Hipparcos' parallax, the radius, luminosity and gravity-inferred mass are derived. The stellar parameters obtained are in good agreement with other published values, though also some discrepancies with values deduced by other authors are noted. For a few stars (delta Dra, xi Dra, alpha Tuc, H Sco and alpha Cet) some parameters - e.g. the CNO-abundances - are derived for the first time. By examining the correspondence between different ISO-SWS observations of the same object and between the ISO-SWS data and the corresponding synthetic spectrum, it is shown that the relative accuracy of ISO-SWS in band 1 (2.38-4.08 mu m) is better than 2% for these high-flux sources. The high level of correspondence between observations and theoretical predictions, together with a confrontation of the estimated Teff (ISO) value with Teff values derived from colours - which demonstrates the consistency between V-K, BCK, Teff and thetad derived from optical or IR data - proves that both the used MARCS models to derive the stellar quantities and the flux calibration of the ISO-SWS detectors have reached a high level of reliability.

Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries France, Germany, The Netherlands and the UK) and with the participation of ISAS and NASA.

Appendices A-D are only available in electronic form at http://www.edpsciences.org Title: ISO-SWS calibration and the accurate modelling of cool-star atmospheres. II. General results Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J.; Hinkle, K. Bibcode: 2003A&A...400..679D Altcode: 2002astro.ph..7621D The fine calibration of the ISO-SWS detectors (Infrared Space Observatory - Short Wavelength Spectrometer) has proven to be a delicate problem. We therefore present a detailed spectroscopic study in the 2.38-12 mu m wavelength range of a sample of 16 A0-M2 stars used for the calibration of ISO-SWS. By investigating the discrepancies between the ISO-SWS data of these sources, the theoretical predictions of their spectra, the high-resolution FTS-KP (Kitt Peak) spectrum of alpha Boo and the solar FTS-ATMOS (Atmospheric Trace Molecule Spectroscopy) spectrum, both calibration problems and problems in computing the theoretical models and the synthetic spectra are revealed. The underlying reasons for these problems are sought for and the impact on the further calibration of ISO-SWS and on the theoretical modelling is discussed extensively.

Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries France, Germany, The Netherlands and the UK) and with the participation of ISAS and NASA.

Appendix is only available in electronic form at http://www.edpsciences.org Title: The Composition of the solar photosphere Authors: Grevesse, N.; Sauval, A. J. Bibcode: 2002AdSpR..30....3G Altcode: The Sun is unique because chemical composition data can be derived from very different layers, from the center to the outermost coronal layers, using very different techniques like helioseismology, spectroscopy, particle collection techniques, … Differences in chemical composition are observed allowing to discover how the different solar layers evolve. The composition of the solar photosphere, which represents the composition of the outer convective zone, is the basic reference source of elemental abundances. We review the current status of our knowledge of the chemical composition of this layer and compare it with data from other solar sources as well as with meteoritic data. Title: ISO-SWS calibration and the accurate modelling of cool-star atmospheres. I. Method Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J.; Van Assche, W.; Vandenbussche, B. Bibcode: 2000A&A...364..137D Altcode: 2000astro.ph..8316D A detailed spectroscopic study of the ISO-SWS data of the red giant alpha Tau is presented, which enables not only the accurate determination of the stellar parameters of alpha Tau, but also serves as a critical review of the ISO-SWS calibration. This study is situated in a broader context of an iterative process in which both accurate observations of stellar templates and cool star atmosphere models are involved to improve the ISO-SWS calibration process as well as the theoretical modelling of stellar atmospheres. Therefore a sample of cool stars, covering the whole A0 - M8 spectral classification, has been observed in order to disentangle calibration problems and problems in generating the theoretical models and corresponding synthetic spectrum. By using stellar parameters found in the literature large discrepancies were seen between the ISO-SWS data and the generated synthetic spectrum of alpha Tau. A study of the influence of various stellar parameters on the theoretical models and synthetic spectra, in conjunction with the Kolmogorov-Smirnov test to evaluate objectively the goodness-of-fit, enables us to pin down the stellar parameters with a high accuracy: Teff = 3850 +/- 70 K, log g = 1.50 +/- 0.15, M = 2.3 +/- 0.8 Msun, z = -0.15 +/- 0.20 dex, xit = 1.7 +/- 0.3 km s-1, 12C/13C = 10 +/- 1, varepsilon (C) = 8.35 +/- 0.20 dex, varepsilon (N) = 8.35 +/- 0.25 dex, varepsilon (O) = 8.83 +/- 0.15 dex and thetad = 20.77 +/- 0.83 mas. These atmospheric parameters were then compared with the results provided by other authors using other methods and/or spectra. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA. Title: ISO Impact on Stellar Models and Viceversa Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J.; van Assche, W.; Vandenbussche, B. Bibcode: 2000ESASP.456..289D Altcode: 2000astro.ph..8362D; 2000ibp..conf..289D We present a detailed spectroscopic study of a sample of bright, mostly cool, stars observed with the Short-Wavelength Spectrometer (SWS) on board ISO, which enables the accurate determination of the stellar parameters of the cool giants, but also serves as a critical review of the ISO-SWS calibration. Title: Solar Abundances Authors: Grevesse, N.; Sauval, A. Bibcode: 2000eaa..bookE1979G Altcode: What is the Sun made of? This fundamental question only received an answer about 70 years ago. H N RUSSELL, whose name is associated with much pioneering research in astrophysics during the first half of this century as well as with a series of basic work in atomic spectroscopy, made the first quantitative analysis of the chemical composition of the SOLAR PHOTOSPHERE in 1929. Using eye estimates ... Title: Abundances of the Elements in the Sun Authors: Grevesse, N.; Sauval, A. J. Bibcode: 2000orel.conf..261G Altcode: No abstract at ADS Title: The solar abundance of iron and the photospheric model Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1999A&A...347..348G Altcode: Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the analyses of Fe i lines and, to a lesser extent, of Fe ii lines. Based on a set of 65 solar Fe i lines, with accurate transition probabilities as well as new accurate damping constants, we construct a new empirical photospheric model. We succeed to reconcile abundance results obtained from low and high excitation Fe i lines as well as from Fe ii lines and derive a solar photospheric abundance of iron, A_Fe = 7.50 +/- 0.05, which perfectly agrees with the meteoritic value. A detailed version of Table~2 is available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or at the ORB via anonymous ftp to ftpserver.oma.be/pub/astro/jacques. Title: VizieR Online Data Catalog: Solar abundance of iron (Grevesse+, 1999) Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1999yCat..33470348G Altcode: Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the analyses of Fe I lines and, to a lesser extent, of Fe II lines. Based on a set of 65 solar Fe I lines, with accurate transition probabilities as well as new accurate damping constants, we construct a new empirical photospheric model. We succeed to reconcile abundance results obtained from low and high excitation Fe I lines as well as from Fe II lines and derive a solar photospheric abundance of iron, AFe=7.50+/-0.05, which perfectly agrees with the meteoritic value. (1 data file). Title: Standard Solar Composition Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1998SSRv...85..161G Altcode: We review the current status of our knowledge of the chemical composition of the Sun, essentially derived from the analysis of the solar photospheric spectrum. The comparison of solar and meteoritic abundances confirms that there is a very good agreement between the two sets of abundances. They are used to construct a Standard Abundance Distribution. Title: Standard Solar Composition Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1998sce..conf..161G Altcode: No abstract at ADS Title: Standard Abundances Authors: Grevesse, N.; Noels, A.; Sauval, A. J. Bibcode: 1996ASPC...99..117G Altcode: 1996coab.proc..117G No abstract at ADS Title: A new analysis of the OH radical spectrum from solar infrared observations. Authors: Melen, F.; Sauval, A. J.; Grevesse, N.; Farmer, C. B.; Servais, Ch.; Delbouille, L.; Roland, G. Bibcode: 1995JMoSp.174..490M Altcode: The solar spectrum offered the opportunity to discover OH lines with high rotational quantum numbers, which do not appear on laboratory spectra. On solar absorption spectra, the authors have identified about 580 lines, among which about 400 were observed for the first time. They belong to pure rotational transitions in the ground state (υ = 0→3; Jmax″= 48.5), as well as to the (1-0), (2-1), and (3-2) vibration-rotation bands (Jmax″= 32.5). Previous pure rotation, vibration-rotation, and Λ-doubling data sets related to the υ = 0 up to 3 levels were fitted simultaneously together with this new set of data, in order to obtain a very complete and accurate set of molecular constants for the X2Π ground state. Title: High excitation Rydberg levels of Fe I from the ATMOS solar spectrum at 2.5 and 7 μm. Authors: Schoenfeld, W. G.; Chang, E. S.; Geller, M.; Johansson, S.; Nave, G.; Sauval, A. J.; Grevesse, N. Bibcode: 1995A&A...301..593S Altcode: The quadrupole-polarization theory has been applied to the 3d^6^4s(^6^D)4f and 5g subconfigurations of Fe I by a parametric fit, and the fitted parameters are used to predict levels in the 6g and 6h subconfigurations. Using the predicted values, we have computed the 4f-6g and 5g-6h transition arrays and made identifications in the ATMOS infrared solar spectrum. The newly identified 6g and 6h levels, based on ATMOS wavenumbers, are combined with the 5g levels and found to agree with the theoretical values with a root mean-squared-deviation of 0.042cm^-1^. Our approach yields a polarizability of 28.07 a_o_^3^and a quadrupole moment of 0.4360+/-0.0010ea_o_^2^for Fe II, as well as an improved ionization potential of 63737.700+/-0.010cm^-1^ for Fe I. Title: Charles FIEVEZ; 13 Years of Spectroscopy at the Observatoire Royal de Bruxelles (1877-1890) Authors: Sauval, A. J. Bibcode: 1995ASPC...81....3S Altcode: 1995lahr.conf....3S No abstract at ADS Title: A New Analysis of the OH Radical Spectrum from Solar Infrared Observations Authors: Melen, F.; Grevesse, N.; Delbouille, L.; Roland, G.; Servais, C.; Sauval, A. J.; Farmer, C. B. Bibcode: 1995ASPC...81..320M Altcode: 1995lahr.conf..320M No abstract at ADS Title: Workshop on Laboratory and Astronomical High Resolution Spectra : held in Brussels, Belgium 29 August-2 September 1994 in honour of the 150th birthday of Charles Vievez (1844-1890), the pioneer of astronomical spectroscopy in Belgium Authors: Sauval, A. J.; Blomme, R.; Grevesse, N. Bibcode: 1995ASPC...81.....S Altcode: 1995lahr.conf.....S No abstract at ADS Title: Atomic and Molecular Data in Solar Photospheric Spectroscopy Authors: Grevesse, N.; Noels, A.; Sauval, A. J. Bibcode: 1995ASPC...81...74G Altcode: 1995lahr.conf...74G No abstract at ADS Title: Statement Authors: Sauval, A. J.; Blomme, R.; Grevasse, N. Bibcode: 1995ASPC...81..627S Altcode: 1995lahr.conf..627S No abstract at ADS Title: Analysis of the 3d 64 s( 6D)4f--5g Supermultiplet of Fe i in Laboratory and Solar Infrared Spectra Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.; Grevesse, N.; Schoenfeld, W. G.; Change, E. S.; Farmer, C. B. Bibcode: 1994ApJ...429..419J Altcode: 1994astro.ph..4050J The combined laboratory and solar analysis of the highly-excited subconfigurations 4f and 5g of Fe I has allowed us to classify 87 lines of the 4f-5g supermultiplet in the spectral region 2545-2585 cm-1. The level structure of these JK-coupled configurations is predicted by semiempirical calculations and the quadrupolic approximation. Semiempirical gf-values have been calculated and are compared to gf values derived from the solar spectrum. The solar analysis has shown that these lines, which should be much less sensitive than lower excitation lines to departures from LTE and to temperature uncertainties, lead to a solar abundance of iron which is consistent with the meteoritic value (A_Fe = 7.51). Title: The Sun as a Laboratory Source for IR Molecular Spectroscopy Authors: Sauval, A. J.; Grevesse, N. Bibcode: 1994IAUS..154..549S Altcode: No abstract at ADS Title: Analysis of Very High Excitation Fe I Lines (4f - 5g) in the Solar Infrared Spectrum Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.; Grevesse, N. Bibcode: 1994IAUS..154..543J Altcode: No abstract at ADS Title: Molecules in the Sun and Molecular Data Authors: Grevesse, Nicolas; Sauval, A. Jacques Bibcode: 1994LNP...428..196G Altcode: 1994mse..conf..196G; 1994IAUCo.146..196G No abstract at ADS Title: Solar Abundances of C; N; O Authors: Grevesse, N.; Sauval, A. J.; Blomme, R. Bibcode: 1994IAUS..154..539G Altcode: No abstract at ADS Title: Line Shifts Asymmetries in the IR Solar Spectrum Authors: Blomme, R.; Sauval, A. J.; Grevesse, N. Bibcode: 1994IAUS..154..533B Altcode: No abstract at ADS Title: Data for the CN red System from solar lines Authors: Sauval, A. J.; Blomme, R.; Grevesse, N. Bibcode: 1994msep.conf..107S Altcode: 1994IAUCo.146P.107S No abstract at ADS Title: A revision of the solar abundance of dysprosium Authors: Grevesse, N.; Noels, A.; Sauval, A. J. Bibcode: 1993A&A...271..587G Altcode: The solar abundance of dysprosium is reevaluated from a new analysis of solar Dy II lines for which new accurate gf-values have recently been measured by Kusz (1992). The new result, ADy = 1.14±0.08, is in pretty good agreement with the meteoritic value. Title: On the accuracy of CO line positions for high resolution IR stellar spectroscopy Authors: Sauval, A. J.; Farrenq, R.; Guelachvili, G.; Grevesse, N.; Farmer, C. B.; Norton, R. H. Bibcode: 1992A&A...265..355S Altcode: The paper demonstrates the high accuracy of line positions derived from improved sets of Dunham coefficients for the four more abundant isotopic species of carbon monoxide - (C-12)(O-16), (C-13)(O-16), (C-12)(O-18), and (C-12)(O-17) - which are present in the sun and in cool stellar atmospheres. These new spectroscopic constants make it possible to predict very accurate positions of CO lines at any J-values, especially at very high rotational excitation (up to J around 135). Earlier proposed identifications of CO lines at large J-values are checked, and some incorrect identifications in sunspot spectra are found. The present accurate line positions are also compared with predictions from other available sets of molecular constants. It is concluded that the present improved sets of molecular constants are the most appropriate to all problems of high-resolution stellar and solar spectroscopy at any J- and v-values, particularly for synthetic spectra of cool stars. Title: Photospheric abundances. Authors: Grevesse, Nicolas; Noels, A.; Sauval, A. J. Bibcode: 1992ESASP.348..305G Altcode: 1992cscl.work..305G The authors review the photospheric abundances of the chemical elements which are observed in the coronal spectrum, in the solar wind and in solar energetic particle events. Title: Molecular Data from Solar Spectroscopy Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1992RMxAA..23...71G Altcode: We show through a few examples how the analysis of molecular transitions present in the solar visible and infrared spectrum can be used to refine our knowledge of the molecular constants and to test the accuracy of available molecular data like transition probabilities and dissociation energies for a few diatomic molecules. Key words: ATOMIC PROCESSES - MOLECULAR PROCESSES - SUN: ATMOSPHERE - SUN: SPECTRA Title: Improved Dunham coefficients for CO from infrared solar lines of high rotational excitation Authors: Farrenq, R.; Guelachvili, G.; Sauval, A. J.; Grevesse, N.; Farmer, C. B. Bibcode: 1991JMoSp.149..375F Altcode: About 4500 unblended CO lines have been selected and their wavenumbers accurately measured on high resolution solar spectra obtained from space with the ATMOS Fourier transform spectrometer. Half of these lines are of high rotational excitation energy and have never been observed before in the laboratory. Line positions of the fundamental bands of 12C16O have been measured up to J = 133, those of 13C16O and of 12C18O up to J = 103 and 91, respectively. The first overtone bands of 12C16O have been measured up to J = 110. These new solar CO wavenumbers, with an additional selected set of about 14 000 accurate laboratory measurements, have been simultaneously fitted to the Dunham expression utilizing 10 recently published relations between isotopically invariant parameters Uij. The present set of coefficients reproduces all accurate laboratory positions and our solar measurements of high rotational excitation with a standard deviation of about 10-5 cm-1 (300kHz). This new set is particularly recommended for all high resolution studies of infrared laboratory and stellar spectra showing CO lines of high J-values.

It is with deep sorrow that we report the demise of R. H. Norton on March 22, 1991. His participation in this research was much appreciated. Title: First identification of pure rotation lines of NH in the infrared solar spectrum Authors: Geller, M.; Farmer, C. B.; Norton, R. H.; Sauval, A. J.; Grevesse, N. Bibcode: 1991A&A...249..550G Altcode: Pure rotation lines of NH of the v = 0 level and v = 1 level are detected in high-resolution solar spectra obtained from the Atmospheric Trace Molecule Spectroscopy (ATMOS) experimental observations. It is pointed out that the identification of the lines is favored by the typical appearance of the triplet lines of nearly equal intensities. The observed equivalent widths of these triplet lines are compared with predicted intensities, and it is observed that these widths are systematically larger than the predicted values. It is noted that because these very faint lines are observed in a region where the signal is very low, a systematic error in the measurements of the equivalent widths cannot be ruled out; therefore, the disagreement between the observed and predicted intensities is not considered to be real. Title: Vibration-rotation bands of CH in the solar infrared spectrum and the solar carbon abundance Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck, E. F.; Farmer, C. B.; Norton, R. H. Bibcode: 1991A&A...242..488G Altcode: High resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29-May 6, 1985) have made it possible to identify and measure a large number of lines of the vibration-rotation fundamental bands of the X2 Pi state of CH. From about 100 lines of the 1-0, 2-1, and 3-2 bands and adopting theoretical transition probabilities, a solar carbon abundance of 8.60 + or - 0.05 is derived. This value is compared with new results inferred from other carbon abundance indicators. The final recommended solar abundance of carbon is 8.60 + or - 0.05. Title: The infrared solar spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1991STIN...9413502G Altcode: The spectrum of the quiet Sun at wavelengths larger than about 1 micrometer (or wavenumbers shorter than 10,000/cm) are described. The main characteristics of studying the solar spectrum in the infrared region are summarized. The new high resolution low noise solar spectra obtained by the Atmospheric Trace Molecule Spectroscopy (ATMOS) Fourier transform spectrometer experiment on board the Space Shuttle are considered. Atomic and molecular spectroscopy/line identification are discussed. Solar observations in the infrared are summarized. Recent analyses have led to a better understanding of the heterogeneous structure of the solar outer layers: thermal bifurcation between the cool photosphere and the hot flux tube chromosphere, convective motions in the photosphere, oscillations in the photosphere and chromosphere, magnetic fields and shapes of the flux tubes, etc. Title: The Infrared Solar Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1991isrs.conf..215G Altcode: No abstract at ADS Title: Identification of solar vibration-rotation lines of NH and the solar nitrogen abundance Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck, E. F.; Farmer, C. B.; Norton, R. H. Bibcode: 1990A&A...232..225G Altcode: High resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29 - May 6, 1985) made it possible to detect for the first time vibration-rotation lines of NH from the X3 Sigma(-) state near 3 microns. Using recent theoretical results for the transition probabilities of 23 selected measured lines of the 1-0 and 2-1 bands, a solar abundance of nitrogen of 8.06 + or - 0.07 is derived. This value is compared with the result derived from N I lines and agrees with the abundance obtained from the 3s-3p, 3p-3d and 3s-prime - 3p-prime transitions, A(N) = 8.00 + or - 0.09. The final recommended solar abundance of nitrogen is A(N) = 8.00 + or - 0.05. Title: A new analysis of the vibration-rotation spectrum of CH from solar spectra Authors: Melen, F.; Grevesse, N.; Sauval, A. J.; Farmer, C. B.; Norton, R. H.; Bredohl, H.; Dubois, I. Bibcode: 1989JMoSp.134..305M Altcode: In the solar spectrum, CH vibration-rotation lines are excited to higher vibrational and much higher rotational quantum numbers than in any laboratory source. We have observed, for the first time, a very large number of new lines (1-0 and 2-1 up to J = 34.5, 3-2 up to J = 31.5, and even 4-3, never seen before, up to J = 24.5) on solar spectra obtained from space, with the ATMOS-SL3 instrument. A total of 558 lines have been used to derive new accurate molecular constants for the X2Π ground state of CH. Title: Concentrations of hydrogen chloride and hydrogen fluoride measured during the MAP/GLOBUS campaign of September 1983 Authors: Zander, R.; Roland, G.; Delbouille, L.; Sauval, A. J.; Marché, P.; Karcher, F.; Amoudei, M.; Dufour, B. Bibcode: 1987P&SS...35..665Z Altcode: Within the context of the MAP/GLOBUS campaign of September 1983, several trace species have been observed by absorption spectroscopy at the two ground stations of the Jungfraujoch, Switzerland (3580 m altitude) and the Observatoire de Haute-Provence, France (1905 m altitude). The results obtained for HCl and for HF, expressed in terms of mean integrated columns above these sites are: Jungfraujoch: (2.1 ± 0.2) E15 mol cm -2 HCl (4.8 ± 0.2) E14 mol cm -2 HF Haute-Provence: (2.6 ± 0.2) E15 mol cm -2 HCl. Taking into account the difference in the altitude of the two stations, the reported HC1 results are in agreement to within their respective uncertainties. The integrated column density of HCl and HF above 11 km altitude, deduced from airplane observations on 9 September 1983, are: (1.65 ± 0.25) E15 mol cm -2 HCl above 11 km (3.7 ± 1.7) E14 mol cm -2 HF above 10 km supporting satisfactorily the ground measurements. Title: Diatomic molecules in the solar infrared spectrum from ATMOS-SL3 highresolution observations. Authors: Grevesse, Nicolas; Sauval, A. J.; Farmer, C. B.; Norton, R. H. Bibcode: 1987LIACo..27..111G Altcode: 1987oahp.proc..111G The ATMOS Fourier Transform Spectrometer has observed, for the first time, the solar infrared spectrum, from 2 to 16 microns, free of any telluric absorption. A very large number of molecular lines are present on these high quality spectra: vibration-rotation lines of CO (Delta-v = 1 and 2; including the isotopic species C-13, O-18 and O-17), CH, NH, OH and pure rotation lines of OH. The analysis of these lines will allow to derive accurate values for the solar abundances of C, N and O and the isotopic ratios C-13/C-12, O-18/O-16, and O-17/O-16, to test the photospheric model from high to deep layers, to test the electric dipole moment functions of the different molecules and to derive much better molecular constants for CH. Title: Identification of vibration-rotation lines of CH in the solar infrared spectrum Authors: Sauval, A. J.; Grevesse, N. Bibcode: 1985AExpr...1..153S Altcode: Transitions of the fundamental band of CH have recently been measured with very high accuracy by Lubic and Amano (1984). The lines are shown to be present in the solar infrared spectrum (2580 - 2940 cm-1). The role these lines could play in solar and stellar spectroscopy is discussed. Title: The Interest of Simultaneous Spectral and Spatial High Resolution Spectroscopy in the Infrared Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J. Bibcode: 1985LNP...233..108D Altcode: 1985hrsp.proc..108D Up to the present, small scale structures on the sun have mostly been studied through observations made in the visible and ultraviolet. After having recalled some of the main advantages of infrared observations, the authors give a few samples of high spectral resolution/low noise solar spectra now routinely obtained in this spectral range by using Fourier transform spectrometers. The authors then show that such high spectral resolution spectra could be obtained in short period of time and for small scale solar structures, using a LEST type collector. Title: The interest of simultaneous spectral and spatial high resolution spectroscopy in the infrared. Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J. Bibcode: 1985CoORB..80.....D Altcode: After having recalled some of the main advantages of infrared observations, the authors give a few samples of high spectral resolution/low noise solar spectra now routinely obtained in this spectral range by using Fourier transform spectrometers. They then show that such high resolution spectra could be obtained in a short period of time and for small-scale solar structures, using a LEST type collector. Title: An analysis of vibration-rotation lines of OH in the solar infrared spectrum Authors: Grevesse, N.; Sauval, A. J.; van Dishoeck, E. F. Bibcode: 1984A&A...141...10G Altcode: High resolution solar spectra have permitted the measurement with great accuracy of equivalent widths of vibration-rotation lines of OH in the X2Pi state near 3-micron wavelength. Using recent theoretical results for the transition probabilities, a solar oxygen abundance of (8.93 + or - 0.02) is derived which is in perfect agreement with the abundance deduced from the OH pure rotation lines. The solar abundance of oxygen is therefore A(O) = 8.92 + or - 0.035, as inferred from the analysis of 43 vibration-rotation lines and 81 pure rotation lines of the OH molecule. It is confirmed that the dipole moment function of Werner, Rosmus and Reinsch (1983) together with the Holweger-Mueller (1974) solar atmosphere model are to be preferred in the analysis of the data. Title: A set of partition functions and equilibrium constants for 300 diatomic molecules of astrophysical interest Authors: Sauval, A. J.; Tatum, J. B. Bibcode: 1984ApJS...56..193S Altcode: Polynomial developments for partition functions and equilibrium constants of 300 diatomic molecules and of relevant atoms are given for a temperature range from 1000 to 9000K. All molecular spectroscopic data, with a few exceptions, are derived from the book by Huber and Herzberg in order to lead to a homogeneous set of data. Title: The pure rotation spectrum of OH and the solar oxygen abundance Authors: Sauval, A. J.; Grevesse, N.; Zander, R.; Brault, J. W.; Stokes, G. M. Bibcode: 1984ApJ...282..330S Altcode: High-resolution low-noise spectroscopic observations of the sun obtained in the 10.6-13-micron range using the Fourier-transform spectrometer at Kitt Peak National Observatory are reported. About 100 pure rotation lines of the X 2Pi electronic state of OH with v = 0, 1, 2, and 3 are identified and characterized. The data are presented in tables and graphs and used to calculate the solar O abundance as 8.91 + or - 0.01 (in agreement with Lambert, 1978). Agreement is also found with the electric-dipole-moment function of Werner et al. (1983) and the photospheric model of Holweger and Mueller (1974). Title: Molecules in red-giant stars. I - Column densities in models for K and M stars Authors: Johnson, H. R.; Sauval, A. J. Bibcode: 1982A&AS...49...77J Altcode: Weighted column densities have been calculated for neutral atoms and ions of most elements and for many molecules in 6 selected model atmospheres of red-giant stars (2500 ≤ Teff ≤ 4000 K) with solar composition. These comprise the most abundant molecules from a total of about 1600 compounds analyzed. This calculation provides a guide for identification of new molecular bands in cool stellar spectra and for laboratory analysis of those molecules of stellar interest which are as yet not studied spectroscopically. Title: Infrared bands of C2 in the solar photospheric spectrum Authors: Brault, J. W.; Testerman, L.; Grevesse, N.; Sauval, A. J.; Delbouille, L.; Roland, G. Bibcode: 1982A&A...108..201B Altcode: Lines of the C2 Phillips system have been successfully searched for on new tracings of high resolution solar spectra. From a rather large number of lines of the (0,0), (1,0), and (0, 1) bands, we derive empirical values for the band oscillator strengths: f00 = 1.41 10-3, f10 = 1.38 10-3, and f01 = 1.12 10-3. These solar f-values are discussed in section 3.1 and compared with recent laboratory data.

For the Ballik-Ramsay system, only a few unblended solar lines have been available, from which we deduced 0.6 10-3 ≪ f00 ≪ 1.2 10-3. Title: Molecular Data Needed in Stellar Spectroscopy Studies Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1980LIACo..21..289G Altcode: 1980smsl.conf..289G No abstract at ADS Title: Theoretical molecular abundances in cool stellar models Authors: Johnson, H. R.; Sauval, A. J. Bibcode: 1980LIACo..21..201J Altcode: 1980smsl.conf..201J No abstract at ADS Title: A search for faint molecular lines in the solar photospheric spectrum Authors: Sauval, A. J.; Biemont, E.; Grevesse, N.; Zander, R. Bibcode: 1980LIACo..21..235S Altcode: 1980smsl.conf..235S No abstract at ADS Title: Predicted presence and tentative identification of new molecules in the pure S star R Cyg. Authors: Sauval, A. J. Bibcode: 1978A&A....62..295S Altcode: A new approach to the problem of the identification of molecular features observed in the spectra of pure S stars has been attempted. From calculations of the chemical equilibrium in cool stellar models, including a very large number of compounds, a first selection has been made among molecules which ought to be present in S stars. On the basis of these predictions, a search has been made for bands of these new compounds in spectrograms of R Cyg recently obtained by Wyckoff and Wehinger. The presence of some new molecules, such as HfO and TaO, in this pure S star is proposed, but the lack of complete laboratory data and the existence of numerous blends in the stellar spectrum render very difficult any definite identification. Title: Conditions d'observation des Comètes périodiques Encke et Grigg-Skjellerup en 1977 Authors: Debehogne, H.; Sauval, A. J. Bibcode: 1976C&T....92..333D Altcode: No abstract at ADS Title: Influence of Uncertainties of Molecular Data upon the Determination of Abundances in Cool Stars Authors: Sauval, A. J. Bibcode: 1976IAUS...72...21S Altcode: No abstract at ADS Title: The CO fundamental bands in the solar spectrum. Authors: Muller, C.; Sauval, A. J. Bibcode: 1975A&A....39..445M Altcode: The result of a study of CO lines in the delta v equals 1 bands in the solar disk spectrum is presented. Recently, the photospheric spectrum has been recorded using a balloon-borne spectrometer from 40 km altitude. From a comparison between the observed and synthetic solar spectra, an agreement is shown using the best available solar and molecular data. Results are discussed and compared with other investigations in order to explain an apparent discrepancy between previous results. Title: The CO fundamental bands in the solar spectrum Authors: Muller, C.; Sauval, A. J. Bibcode: 1975STIN...7530990M Altcode: The results of a study of CO lines in the * delta v equals 1 bands in the solar disk spectrum are presented. The photospheric spectrum is recorded using a balloon-borne spectrometer from 40 km altitude. From a comparison between the observed and synthetic solar spectra are compared. An agreement is shown using the best available solar and molecular data. Results are discussed and compared with other investigations and explain an apparent discrepancy among previous results. Title: K. R. Lang - Astrophysical Formulae Authors: Sauval, A. J. Bibcode: 1975C&T....91..320S Altcode: No abstract at ADS Title: A Study of Molecular Lines in the Solar Photospheric Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1973A&A....27...29G Altcode: Summary. We have analysed the behaviour of lines of C2, CH, CN, MgH, NH and OH in the solar photospheric spectrum. Recently observed profiles of these lines have been measured and compared with profiles computed using recent solar and molecular data. The main results of this comparison are (I) there is good agreement between observed and calculated profiles for most of the molecular bands; (11) but large disagreements appear in the case of CN and MgH; these discrepancies cannot be explained satisfactorily, although different possible suggestions are investigated. In the Appendix, a review of the different experimental band oscillator strengths is presented and mean laboratory values are proposed. Key words: solar spectrum - molecular lines - molecular oscillator strengths Title: A Search for CH+ in the Solar Photospheric Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1971A&A....14..477G Altcode: We present the results of a search for lines of CH+ (A1H - X1 + transition) in the solar photospheric spectrum. We conclude that if CH+ is present, the equivalent widths of the most intense lines cannot exceed 2 mA. An empirical solar !00-value is derived and compared with a laboratory value and other available astrophysical values. Some possible reasons are given for explaining the large discrepancy between laboratory and astrophysical !00-values - Key words: solar spectrum - molecules - oscillator strengths Title: Oscillator strengths for SiH and SiH+ deduced from the solar spectrum. Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1971JQSRT..11...65G Altcode: No abstract at ADS Title: Identification of SiH~ in the Solar Photospheric Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 1970A&A.....9..232G Altcode: We present the first convincing identification of a molecular ion in a stellar atmosphere: the absorption band spectrum of SiH+ (transition A 1H - X i +) in the solar photospheric spectrum. Values of the band oscillator strengths have been deduced for two bands: too = 0.0005 and !oi = 0.0004. Title: Identification of SiH Lines in the Solar Disk Spectrum Authors: Sauval, A. J. Bibcode: 1969SoPh...10..319S Altcode: A new investigation of the presence of SiH lines in the solar disk spectrum has been performed. It may be concluded that molecular absorption lines of SiH are present in the disk spectrum with maximum equivalent widths of about 2 mÅ. A value of the oscillator strength of SiH has been derived (f00 = 0.0008 ± 0.0004). Title: The solar continuum from 900 to 130 000 Å and the photospheric temperature model Authors: Sauval, A. Bibcode: 1968SoPh....3...89S Altcode: In order to obtain a better agreement between observed and computed values of the solar intensity, an improved temperature distribution is deduced for the range 0.02<τ0< 10. The intensity observations here considered refer to the wavelength region between λ 1980 and λ 129 500, and the center-limb variations generally go down to cosθ = 0.1. The improved model, given in Figure 4 and Table II, differs rather little from the Utrecht 1964 model, used here as a reference. Title: Le projet West Ford Authors: Sauval, A. Bibcode: 1963C&T....79...12S Altcode: No abstract at ADS