J/A+AS/113/71ivo://CDS.VizieR/J/A+AS/113/71CDSRAMSAUER J.SOLANKI S.K.BIEMONT E.1997-12-09T17:54:16Z1997-12-09T18:54:08ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-suninfrared-astronomyspectroscopyWe list 603 spectral lines between 1.0, 1.8um that are judged to be relatively unblended from a visual inspection of spectra of the quiet sun. Much of the atomic data of relevance to studies of solar and stellar magnetism, convection and atmospheric structure are also provided. Particular attention is paid to blending by telluric lines. We determine the level of blending both in the presence and the absence of telluric lines. We also describe how telluric blends may be removed from spectra with high spectral resolution.1995A&AS..113...71Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/113/71CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/113/71https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/113/71http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/113/71https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/113/71https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/113/71http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/113/71GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/A+AS/113/71/table1Lines judged to be relatively unblended from a visual examination between 1.00 and 1.34umn_Vac[*] See (2)meta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSolLamSolar wavelength of the lines (1)0.1nmem.wldoubleVac[]? Vaccum wavenumbercm**-1phys.energy;phys.atmol.transitiondoubleBlI1Blending index derived from Delbouille et al. (1981)spect.indexcharn_BlI1[ab ] See (3)meta.notecharBlI2Blending index derived from Livingstone and Wallace (1991) and Wallace et al. (1993)spect.indexcharIonIons and diatomic molecules identified as sources of the solar spectral linephys.atmol.ionizationcharn_Ion[ab] See (4)meta.notecharLabLam[]? Laboratory wavelength of ions, molecules0.1nmem.wl;phys.atmol.transitiondoublen_LabLam[*] See (5)meta.notecharTransAtomic or molecular transition. The notation of the terms in the identified transitions follows the National Bureau of Standards (NBS) compilations of atomic energy levels, Kurucz (1991) and Nave et al. (1994).meta.id;phys.atmol.transitioncharr_TransReferences for transition (6)meta.refcharn_Trans[*!abcde] See (7)meta.notecharExcPot[]? Excitation potential of the lower level of the transitioneVphys.energy;phys.atmol.excitationfloatgcalc[]? Effective Lande factor calculated from the listed transitionphys.atmol.wOscStrengthfloatn_gcalc[*a] See (8)meta.notechargemp[]? Effective Lande factor derived empirically from laboratory measurementsphys.atmol.wOscStrengthfloatn_gemp[?] See (9)meta.notecharChiPi[]? Second order coefficient of the {pi}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)spect.line.broad.ZeemanfloatChiSigma[]? Second order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)spect.line.broad.ZeemanfloatYSigma[]? Third order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)stat.fit.paramfloatCalcLam[]? Calculated wavelength0.1nmem.wlfloatlog(gf)[]? Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991)phys.atmol.wOscStrengthfloatn_log(gf)[abcd] See (10)meta.notecharJ/A+AS/113/71/table2Possible blends rejected as too weakrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSolLamSolar wavelength of the lines0.1nmem.wldoubleIonIons and diatomic molecules identified as sources of the solar spectral linephys.atmol.ionizationcharLabLamLaboratory wavelength of ions and molecules0.1nmem.wl;phys.atmol.transitiondoublen_LabLam[*] See Note (5) in Table 1 and 3meta.notecharExcPotExcitation potential of the lower level of the transitioneVphys.energy;phys.atmol.excitationfloatlog(gf)Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991)phys.atmol.wOscStrengthfloatn_log(gf)[b] See Note (10) in Table 1 and 3meta.notecharJ/A+AS/113/71/table3Lines judged to be relatively unblended from a visual examination in the H-band(1.49-1.80um)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSolLamSolar wavelength of the lines (1)0.1nmem.wldoubleVac[]? Vaccum wavenumbercm**-1phys.energy;phys.atmol.transitiondoublen_Vac[*] See (2)meta.notecharBlI1Blending index derived from Delbouille et al. (1981)spect.indexcharn_BlI1[ab ] See (3)meta.notecharBlI2Blending index derived from Livingstone and Wallace (1991) and Wallace et al. (1993)spect.indexcharIonIons and diatomic molecules identified as sources of the solar spectral linephys.atmol.ionizationcharn_Ion[ab] See (4)meta.notecharLabLam[]? Laboratory wavelength of ions, molecules0.1nmem.wl;phys.atmol.transitiondoublen_LabLam[*] See (5)meta.notecharTransAtomic or molecular transition. The notation of the terms in the identified transitions follows the National Bureau of Standards (NBS) compilations of atomic energy levels, Kurucz (1991) and Nave et al. (1994).meta.id;phys.atmol.transitioncharr_TransReferences for transition (6)meta.refcharn_Trans[*!abcde] See (7)meta.notecharExcPot[]? Excitation potential of the lower level of the transitioneVphys.energy;phys.atmol.excitationfloatgcalc[]? Effective Lande factor calculated from the listed transitionphys.atmol.wOscStrengthfloatn_gcalc[*a] See (8)meta.notechargemp[]? Effective Lande factor derived empirically from laboratory measurementsphys.atmol.wOscStrengthfloatn_gemp[?] See (9)meta.notecharChiPi[]? Second order coefficient of the {pi}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)spect.line.broad.ZeemanfloatChiSigma[]? Second order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)spect.line.broad.ZeemanfloatYSigma[]? Third order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987)stat.fit.paramfloatCalcLam[]? Calculated wavelength0.1nmem.wlfloatlog(gf)[]? Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991)phys.atmol.wOscStrengthfloatn_log(gf)[abcd] See (10)meta.notecharJ/A+AS/113/71/table4Possible blends rejected as too weak in H-bandrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSolLamSolar wavelength of the lines0.1nmem.wldoubleIonIons and diatomic molecules identified as sources of the solar spectral linephys.atmol.ionizationcharLabLamLaboratory wavelength of ions and molecules0.1nmem.wl;phys.atmol.transitiondoublen_LabLam[*] See Note (5) in Table 1 and 3meta.notecharExcPotExcitation potential of the lower level of the transitioneVphys.energy;phys.atmol.excitationfloatlog(gf)Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991)phys.atmol.wOscStrengthfloatn_log(gf)[b] See Note (10) in Table 1 and 3meta.notechar