J/A+AS/113/71 J/A+AS/113/71 Lines in the infrared solar spectrum J Ramsauer S K Solanki E Biemont Astron. Astrophys. Suppl. Ser. 113 71 1995 1995A&AS..113...71R atomic data line: identification line: profiles Sun: infrared We 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.

SolLam Solar wavelength of the lines number=1 Whenever possible {lambda}_sun_ has been determined from the Delbouille et al. (1981) atlas. If the line is too strongly blended in their spectra, then we have obtained the wavelength from the Livingston and Wallace 1991 or Wallace et al. 1993 spectra. All values are only corrected for Doppler shift. 0.1nm Vac Vaccum wavenumber cm-1 n_Vac See number=2 When '*' the wavenumber of this line was taken from a purely solar component of the Livingstone and Wallace (1991) spectral atlas due to the too strong telluric blending of the line in the Delbouille et al. (1981) spectral atlas. --- BlI1 Blending index derived from Delbouille et al. (1981) --- n_BlI1 See number=3 When 'a': In the Delbouille et al. (1981) atlas these lines look less blended than the values given here, but according to the Wallace et al. (1993) and the Livingstone and Wallace (1991) atlases the lines are blended with a telluric line having almost the same wavelength, so that the blends show no readily visible effects. When 'b' line is blended according to Biemont et al. (1985a) --- BlI2 Blending index derived from Livingstone and Wallace (1991) and Wallace et al. (1993) --- Ion Ions and diatomic molecules identified as sources of the solar spectral line --- n_Ion See number=4 When 'a': according to the available log(gf) this identification is extremely unlikely. When 'b' : according to Biemont and Brault (1987a,b) this line is a blend of different hyperfine components --- LabLam Laboratory wavelength of ions, molecules 0.1nm n_LabLam See number=5 When '*' for this line no laboratory wavelength is available in the above references therefore the calculated wavelength has been written instead --- Trans Atomic 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). --- r_Trans References for transition number=6 For Table1: ---------------------------------- [1] Biemont (1976) [2] Biemont et al. (1985a) [3] Biemont et al. (1985b) [4] Biemont et al. (1986) [5] Biemont et al. (1994) [6] Biemont, Grevesse (1973) [7] Striganov, Sventitskii (1968) [8] Zaidel et al. (1970) [9] Swensson et al. (1970) [10] Kurucz (1991) [11] Kurucz, Peytremann (1975) [12] Livingston, Wallace (1991) [13] Wallace, Livingston (1991) [14] Martin, Zalubas (1983) [15] Reader et al. (1980) [16] Hall (1974) [17] Nave et al. (1994) ----------------------------------- For Table 3: ---------------------------------- [1] Biemont (1976) [2] Biemont et al. (1985a) [3] Biemont et al. (1985b) [4] Biemont et al. (1986) [5] Biemont, Brault (1987a) [6] Biemont, Brault (1987b) [7] Biemont, Grevesse (1973) [8] Hall (1974) [9] Litzen (1976) [10] Litzen, Verges (1976) [11] Johansson, Learner (1990). In accordance with this reference JK notation is used for the levels of the 3d6 4s 6D 4f configuration. [12] Kurucz (1991) [13] Kurucz, Peytremann (1975) [14] Livingston, Wallace (1991) [15] Wallace, Livingston (1991) [16] Martin, Zalubas (1979) [17] Nave, Johansson (1993) [18] Mohler (1955) [19] Nave et al. (1994) --- n_Trans See number=7 When '*' this transition involves a change in orbital angular momentum DL>1, making the identification uncertain. Such identifications are listed only where no other possible identification is known. ! When '!' the order of the multiple line identifications represents their probable contribution to the line (e.g. due to the huge equivalent width of the primary identification, the secondary (blend) probably provides only a very small contribution to the line). a When 'a' this transition involves a change in total spin DS>1 making the identification uncertain. Such identifications are listed only where no other possible identification is known. b When 'b' the sign of the Lande factor of Fe I 15611.151 A is opposite to that expected from the observed Stokes V profile, so that the identification is probably wrong. c When 'c' Ni I 16673.715 A and Ni I 16996.271 A : the laboratory wavelengths of both lines can be matched much better by the calculated wavelengths of the transitions identified by Biemont and Brault (1987b) if the 3d9 5p 1F3o level common to both lies at 48672.085+-0.015 cm-1 (instead of 48671.9 cm-1 listed in Corliss and Sugar, 1981) d When 'd' due to the large equivalent width of the primary identification, the secondary identification (blend) probably contributes only a very minute amount to the line. e When 'e' AlI 16750.614 A is blended with a telluric line of about the same wavelength and is also distorted by the large hyperfine splitting of the given transition (see Biemont and Brault 1987b). --- ExcPot Excitation potential of the lower level of the transition eV gcalc Effective Lande factor calculated from the listed transition --- n_gcalc See number=8 When '*' and 'a' for most transitions the LS coupling Lande factors of the upper and lower levels are used to determine g_eff_. For the levels of the 3d6 4s 6D 4f configuration g values have been taken from Johansson and Learner (1990). When 'a' according to Stokes profile calculations by Muglach and Solanki (1992) the g_eff_ values listed here are incompatible with the observed splittings of these lines. --- gemp Effective Lande factor derived empirically from laboratory measurements --- n_gemp See number=9 If only g_l_ or g_u_ is available from laboratory measurements, the missing atomic level Lande factor is assumed to be represented by its LS coupling value. --- ChiPi Second order coefficient of the {pi}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- ChiSigma Second order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- YSigma Third order coefficient of the {sigma}-component of the expansion of a spectral line according to its Zeeman moments (Mathys and Stenflo 1987) --- CalcLam Calculated wavelength 0.1nm log(gf) Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991) --- n_log(gf) See number=10 When 'a' the value was derived from Nave et al. (1994); 'b' from the compilation by Kurucz and Peytremann (1975); 'c' from Biemont et al. (1994); 'd' from Biemont, Grevesse (1973). --- SolLam Solar wavelength of the lines 0.1nm Ion Ions and diatomic molecules identified as sources of the solar spectral line --- LabLam Laboratory wavelength of ions and molecules 0.1nm n_LabLam See Note (5) in Table 1 and 3 --- ExcPot Excitation potential of the lower level of the transition eV log(gf) Logarithm of the statistically weighted oscillator strength of the corresponding atomic line from Kurucz (1991) --- n_log(gf) See Note (10) in Table 1 and 3 --- table1-2.texPlain TeX version of table1 and table2 table3-4.texPlain TeX version of table3 and table4 papdef.texTeX definitions for tables and paper paper.texThe paper in plain TeX Simona Mei CDS 1995May12 J_A+AS_113_71.xml