ADC/CDS Standard Document for Catalog:/journal_tables/A+AS/113/71/
ADC/CDS Standard Document for Catalog:| 1. Use the ADC Data Viewer Suite to visualize the data. |
|
| 2. Get the data files via anonymous FTP. (See Note.) |
|
J/A+AS/113/71 Lines in the infrared solar spectrum (Ramsauer+, 1995)
================================================================================
Interesting lines in the infrared solar spectrum. II: Unblended lines between
1.0 and 1.8um
Ramsauer J., Solanki S.K., Biemont E.
<Astron. Astrophys. Suppl. Ser. 113, 71 (1995)>
=1995A&AS..113...71R (SIMBAD/NED BibCode)
================================================================================
ADC_Keywords: Sun; Spectra, infrared
Keywords: lines: profiles - lines: identification - atomic data - Sun: infrared
Description:
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.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1 146 339 Lines judged to be relatively unblended from
a visual examination between 1.00 and 1.34um
table2 39 101 Possible blends rejected as too weak
table3 146 353 Lines judged to be relatively unblended from
a visual examination in the H-band(1.49-1.80um)
table4 38 34 Possible blends rejected as too weak in H-band
table1-2.tex 80 1507 Plain TeX version of table1 and table2
table3-4.tex 80 1540 Plain TeX version of table3 and table4
papdef.tex 81 484 TeX definitions for tables and paper
paper.tex 79 584 The paper in plain TeX
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1, table3
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
2- 10 F9.3 0.1nm SolLam Solar wavelength of the lines (1)
12- 19 F8.3 cm-1 Vac []? Vaccum wavenumber
20 A1 --- n_Vac [*] See (2)
22- 24 A3 --- BlI1 Blending index derived from Delbouille et al.
(1981)
25- 26 A2 --- n_BlI1 [ab ] See (3)
28- 30 A3 --- BlI2 Blending index derived from Livingstone and
Wallace (1991) and Wallace et al. (1993)
32- 36 A5 --- Ion Ions and diatomic molecules identified as
sources of the solar spectral line
37 A1 --- n_Ion [ab] See (4)
39- 47 F9.3 0.1nm LabLam []? Laboratory wavelength of ions,
molecules
48 A1 --- n_LabLam [*] See (5)
49- 79 A31 --- 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).
80- 89 A10 --- r_Trans References for transition (6)
90 A1 --- n_Trans [*!abcde] See (7)
91- 95 F5.2 eV ExcPot []? Excitation potential of the lower
level of the transition
97-102 F6.3 --- gcalc []? Effective Lande factor calculated
from the listed transition
103 A1 --- n_gcalc [*a] See (8)
104-109 F6.3 --- gemp []? Effective Lande factor derived
empirically from laboratory measurements
110 A1 --- n_gemp [?] See (9)
112-116 F5.3 --- ChiPi []? Second order coefficient of the
{pi}-component of the expansion of a spectral
line according to its Zeeman moments
(Mathys and Stenflo 1987)
118-122 F5.3 --- ChiSigma []? Second order coefficient of the
{sigma}-component of the expansion of a
spectral line according to its Zeeman moments
(Mathys and Stenflo 1987)
124-129 F6.3 --- YSigma []? Third order coefficient of the
{sigma}-component of the expansion of a
spectral line according to its Zeeman moments
(Mathys and Stenflo 1987)
131-135 F5.3 0.1nm CalcLam []? Calculated wavelength
137-141 F5.2 --- log(gf) []? Logarithm of the statistically weighted
oscillator strength of the corresponding
atomic line from Kurucz (1991)
142 A1 --- n_log(gf) [abcd] See (10)
--------------------------------------------------------------------------------
Note (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.
Note (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.
Note (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)
Note (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
Note (5): When '*' for this line no laboratory wavelength is available in the
above references therefore the calculated wavelength has been written
instead
Note (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)
Note (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).
Note (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.
Note (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.
Note (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).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2 table4
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
2- 10 F9.3 0.1nm SolLam Solar wavelength of the lines
12- 16 A5 --- Ion Ions and diatomic molecules identified
as sources of the solar spectral line
18- 26 F9.3 0.1nm LabLam Laboratory wavelength of ions and molecules
27 A1 --- n_LabLam [*] See Note (5) in Table 1 and 3
28- 32 F5.2 eV ExcPot Excitation potential of the lower level
of the transition
34- 38 F5.2 --- log(gf) Logarithm of the statistically weighted
oscillator strength of the corresponding
atomic line from Kurucz (1991)
39 A1 --- n_log(gf) [b] See Note (10) in Table 1 and 3
--------------------------------------------------------------------------------
References:
Biemont E. 1976, Astron. Astrophys. Suppl. Ser. 26, 89;
Biemont E., Brault J.W. 1987a, Physica Scr. 34, 751;
Biemont E., Brault J.W. 1987b, Physica Scr. 35, 286;
Biemont E., Brault J.W., Delbouille L., Roland G. 1985a,
Astron. Astrophys. Suppl. Ser 61, 107;
Biemont E., Brault J.W., Delbouille L., Roland G. 1985b,
Astron. Astrophys. Suppl. Ser 61, 185;
Biemont E., Brault J.W., Delbouille L., Roland G. 1986,
Astron. Astrophys. Suppl. Ser 65, 21;
Biemont E., Grevesse N. 1973, Atomic Data Nuclear Data Tables 12, 217;
Biemont E., Martin F., Quinet P., Zeippen C.J. 1994,
Astron. Astrophys 283, 339
Corliss C., Sugar J. 1981, Phys. Chem. Ref. Data 10, 197;
Delbouille L., Roland G., Brault J.W., Testerman L. 1981, Photometric Atlas
of the Solar Spectrum from 1850 to 10000 cm-1, NOAO, Tucson, Az;
Hall D.N.B. 1974, An Atlas of Infrared Spectra of the Solar Photosphere and
of Sunspot Umbrae, Kitt Peak National Observatory, Contribution No. 556,
Tucson, Az;
Johansson S., Learner R.C.M. 1990, Astrophys. J. 354, 755;
Kurucz R.L. 1991, Magnetic tape with atomic data;
Kurucz R.L., Peytremann E. 1975, Smiths. Astrophys. Obs. Spec. Report 362;
Litzen U. 1976, Physica Scr. 14, 165;
Litzen U., Verges J. 1976, Physica Scr. 13, 240;
Livingston W., Wallace L. 1991, An Atlas of the Solar Spectrum in the
Infrared (1.1 to 5.4 {mu}m), Techn. Rep. #91-001, National Solar Obs.,
Tucson, Az;
Martin W.C., Zalubas R. 1979, J. Phys. Chem. Ref. Data 8, 817;
Martin W.C., Zalubas R. 1983, J. Phys. Chem. Ref. Data 12, 323;
Mathys G. 1989, Fundam. Cosmic Phys. Vol. 13, No. 3, 143;
Mohler O.C. 1955, A Table of Solar Spectrum Wave Lengths: 11984 A to
25578 A, The University of Michigan Press, Ann Arbor;
Muglach K., Solanki S.K., 1992, Astron. Astrophys. 263, 301
Nave G., Johansson S. 1993 Astron. Astrophys. Suppl. Ser. 102, 269;
Nave G. et al. 1994 Astrophys. J. Suppl. Ser. 94, 221;
Reader J., Corliss C., Wiese W.L., Martin W.C. 1980, NSRDS-NBS 68:
Wavelengths, transition probabilities for atoms, atomic ions;
Solanki S.K., Biemont E., Muerset U., 1990, Astron. Astrophys.
Suppl. Ser. 83, 307 (Paper I)
Striganov A.R., Sventitskii N.S. 1968, Tables of spectral lines of
neutral, ionized atoms, IFI/Plenum;
Swensson J.W., Benedict W.S., Delbouille L., Roland G. 1970, The Solar
Spectrum from {lambda} 7498 to {lambda} 12016. Memoires de la Societe
Royale des Sciences de Liege, Special Volume No. 5;
Wallace L., Livingston W. 1991, An Atlas of a Dark Sunspot Umbral
Spectrum from 1970 to 8640 cm-1 (1.16 to 5.1 {mu}m, Techn. Rep. # 92-001,
National Solar Obs., Tucson, Az;
Wallace L., Hinkle H, Livingston W. 1993, An Atlas of the Photospheric
Spectrum from 8900 to 13600 cm-1 (7350 to 11230A), National Solar Obs.,
Techn. Rep.# 93-001, Tucson, Az;
Zaidel A.N., Prokofev V.K., Raiskii S.M., Slavnyi V.A., Shreider E.Ya.
1970, Tables of spectral lines, IFI/Plenum.
* NSRDS-NBS: National Standard Reference Data Series - National Bureau of
Standards.
================================================================================
(End) Simona Mei [CDS] 12-May-1995