Wallace 2011 Solar Flux Atlas

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A Solar Flux Atlas for the Visible

and Near Infrared.

L. Wallace and K. Hinkle,

National Optical Astronomy Observatory*,

W. C. Livingston and S. P. Davis,

National Solar Observatory*.

Introduction.

Kurucz, Furenlid, Brault and Testerman (1984) have already produced a solar flux atlas for the v

ble and near-infrared region using very high quality Brault NSO (National Solar Observatory)

(Fourier Transform Spectrometer) spectra (Davis, Abrams and Brault, 2001). We have produce

different version which we present here. Most importantly, it includes corrections for discrete terres

absorptions mostly due to H O and O This atlas also includes spectral plots with line identifica


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absorptions mostly due to H O and O This atlas also includes spectral plots with line identifica

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Correction for Telluric Lines.

The primary discrete terrestrial absorbers in this region, H2

O and O2

, are illustrated in Figur

Figure 1 is the telluric spectrum derived for the correction of the integrated sun spectra used here. T

weaker bands of H2O (Camy-Peyret et al. 1985) are also apparent in the atlas panels centered ab

19,800 cm1

(5050o

A). It is apparent from Figure 1 that telluric lines have a substantial effect on a l

part of the visible and near infrared spectrum. Note that in Fig. 1, of the observed spectrum was su

tuted for the derived telluric spectrum in telluric line centers when the derived ratio was excessi

noisy.

Our basic scheme for removing the telluric lines when working with center disk spectra is to r

two solar spectra at air masses differing by the order of unity, stretch the ratio to match the telluric l

of the spectrum with the smallest air mass, then divide by the stretched ratio. This only works becaus

the almost complete resolution of the features. The most prominent defects in the process are incre

noise. The S/N is lowest in the centers of strong lines and is reflected in the inability to get good co

tions in the centers of these lines.

We have used this approach with the archival integrated sun spectra but could not generally ob

satisfactory results, there being substantial differences in the Doppler shifts of the solar lines in the

spectra ratioed to obtain a transmission spectrum and much noise due to excessive stretching of the rof spectra differing only by small amounts in air mass. This lead us to the modified scheme of u

ratios of center disk spectra to obtain the transmission spectrum, and then applying that transmis


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lines are apparent, we plot the corrected flux spectrum in one panel and in a second, the telluric transm

sion spectrum used for the correction and the observed flux spectrum, the latter shifted down by

Where the telluric lines are not apparent, only the observed flux spectrum is given.

Table 2. Extent of Labeled Molecular Features.

Molecular Molecular Vibrational Frequency Wavelength

Label Transition Band Region (cm1

) Region (o

A)

CN Red CN Red A2-X

2 1-0 10,801-10,938 9140-9255

4-2 11,236-12,078 8277-8897

3-1 11,046-12,393 8067-9050

2-0 11,156-12,699 7873-8961

6-3 12,757-13,407 7457-7837

5-2 12,757-13,678 7309-7837

4-1 12,867-14,061 7110-7770

3-0 13,026-14,392 6946-7675

C2Swan C

2Swan A

3-X

3 0-1 17,740-18,320 5457-5636

0-0 19,361-20,526 4870-51641-1 19,516-20,045 4987-5123

1-0 21,109-21,587 4631-4736


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Identifications.

For the near infrared through 13,500 cm1

(7405oA) the identificalions were taken from Wall

Hinkle and Livingston (1993); for 13,500 to 28,000 cm1 (3570 to 7405oA) we used Wallace, Hinkle

Livingston (1998); and for 28,000 to 33,800 cm1

(2958 to 3570o

A) we used Hinkle, Wallace, Va

and Ayres (2005). We have also made considerable use of the older studies by Moore, Minnaert

Houtgast (1966) and Pierce and Breckinridge (1973).

Because of lack of space in the plots we have had to truncate the molecular labels to only

molecule and in most cases used an abbreviation for the transition, e.g., CN Red for CN Red A

X2 and dropped vibrational and rotational assignments completely. For clarification and guidance

have added Table 2 which gives frequency and wavelength limits on the bands included in the pThese limits only apply to the labeling and not to the inherent extent of the bands.

References to individual atoms and molecules, taken largely from our previous work, are as

lows.

H - Garcia and Mack (1965).

Li I - Brault and Muller (1975).

C I - Johansson (1966).

N I - Eriksson (1958) with Moore (1959).

O I - Eriksson and Isberg (1963b and 1967).


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Cr II - As with Cr I, we have used Kiess(1951) as the primary source, but replaced his line p

tions with calculated positions from the energy levels given by Sugar and Corliss (1985) which w

derived from unpublished line measurements by S. Johansson.

Mn I - Catalan, Meggers and Garcia-Riquelme (1964).

Mn II - Iglesias and Velasco (1964), as quoted by Kelly (1979), plus Phelps (1982).

Fe I - Primarily Nave et al. (1994a) augmented with Nave and Johansson (1993) and Nave e

(1994b), and extended with Russell and Moore (1944), Kiess, Rubin and Moore (1961)and Phelps (19

Here we have 4,906 lines labeled as Fe I.

Fe II - Dobbie (1938), Johansson (1978) and Moore (1972).

Co I - Pickering and Thorne (1996).

Co II - Pickering, Raasen, Uylings and Johansson (1998).

Ni I - Litzen, Brault and Thorne (1993) and Phelps (1982).

Ni II - Shenstone (1970).

Cu I - Shenstone (1948).

Zn I - Hetzler, Boreman and Burns (1935).

Ge I - Andrew and Meissner (1959).

Rb I - Johansson (1961).


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Nd II - Albertson, Harrison and McNally (1942) and Meggers, Corliss and Scribner (1975).

Sm II - King (1935) and Albertson (1936).

Eu II - King (1939) and Moore (1972).

Gd II - King (1943).

Dy II - King, Conway, Worden and Moore (1970).

Tm I and II - Meggers, Corliss and Scribner (1975).

Yb I and II - Meggers and Corliss (1966).

Lu II - Meggers and Scribner (1937).

Hf II and W I - Meggers, Corliss and Scribner (1975).

Os I, Ir I, Pt I and Au I - Moore (1972).

MgH (A2-x

2) - Balfour and Cartwright (1976).

C2Swan (d

3-a

3) - Prasad and Bernath (1994) and Phillips and Davis (1968).

CH (A2-X

2) - Zachwieja (1995), Bernath et al. (1991), Kiess and Broida (1956) and

(1941).

CH (B2-X2) - Kepa et al. (1996), Bernath et al. (1991), and Gero (1941).

CH (C2-X

2) - Heimer (1932) and Moore amd Broida (1959).

2 2


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Berkeley and Los Angeles, 1963.

Dobbie, J. C., The Spectrum of Fe II, Ann. Solar Phys. Obs., Cambridge, 5,1-58, 1938.

Edlen, B., The Refractive Index of Air, Metrologia, 2,71-80, 1966.

Edlen, B., and P. Risberg, The Spectrum of Singly-Ionized Calcium, Ca II, Ark. Fys., 10,553-566, 19

Engleman, R., Jr., The v=0 and +1 Sequence Bands of the CN Violet System Observed During

Flash Photolysis of BrCN, J. Molec. Spectr., 49,106-116, 1974.

Eriksson, K. B. S., Revised Energy Levels for the Neutral Nitrogen Atom, Ark. Fys., 13,429-438, 195

Eriksson, K. B. S., and H. B. S. Isberg, The Spectrum of Atomic Aluminum, Al I, Ark. Fys., 23,527-

1963a.

Eriksson, K. B. S., and H. B. S. Isberg, O I Quintet and Triplet Terms Below the Ionization Limit,

Fys., 24,549-558, 1963b.

Forsberg, P., The Spectrum and Term System of Neutral Titanium, Ti I, Phys. Scr., 44,446-476, 1991

Garcia, J. D., and J. E. Mack, Energy Level and Line Tables for One-Electron Atomic Spectra, J.

Soc. Amer., 55,654-685, 1965.

Gero, L. Vervollstandigung der Analyse der CH-Banden, Zeit. Phys., 118,27-36, 1941.

Heimer, T., Untersuchung uber die Kohlenwasserstoffbande 3143, Zeit. Phys., 78,771-780, 1932.

Hetzler, C. W., R. W. Boreman, and K. Burns, The Spectrum of the Zinc Arc in Vacuum, Phys. Rev.

656-659, 1935.Hinkle, H., L. Wallace, J. Valenti and T. Ayres, Ultraviolet Atlas of the Arcturus Spectrum, 1150-380

Astronomical Society of the Pacific, San Francisco, 2005.


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I,Astrophys. J. Suppl., 94,221-459, 1994a.

Nave, G., S. Johansson, O. Axner, P. Ljungberg, Y. Malmsten, and B. Baschek, Analysis of

3d64s(6D)6d Subconfiguration of Fe I by Laser-Induced Ionization and Emission Spectroscopy,

sica Scripta, 49,581-587, 1994b.

Nilsson, A. E., S. Johansson, and R. L. Kurucz, The Spectrum of Singly Ionized Yttrium, Y II, Phy

Scripta, 44,226-257, 1991.

Phelps, F. M., III, MIT Wavelength Tables, Vol. 2, Wavelengths by Element, The MIT Press,1982.

Phillips, J. G., and S. P. Davis, The Swan System of the C2

Molecule and the Spectrum of the H

Molecule,U. of California Press, Berkeley and Los Angeles, 1968.

Pierce, A. K., and J. B. Breckinridge, The Kitt Peak Table of Photographic Wavelengths, Kitt P

National Observatory, 1973.

Pickering, J. C., and A. P. Thorne, The Spectrum and Term Analysis of Co I, Astrophys. J. Suppl.,

761-809, 1996.

Pickering, J. C., A. J. J. Raasen, P. H. M. Uylings and S. Johansson, The Spectrum and Term Analys

Co II, Astrophys. J. Suppl., 117,261-311, 1998.

Prasad, C. V. V., P. F. Bernath, C. Frum, and R. Engleman, Jr., Fourier Transform Jet Emission Spect

copy of the B2

+-X

2

+Transition of CN, J. Molec. Spectr., 151,459-473, 1992.

Prasad, C. V. V., and P. F. Bernath, Fourier Transform Spectroscopy of the Swan (d3

g-a3

u) Systemthe Jet-Cooled C

2Molecule, Astrophys. J., 426,812-821, 1994.

Radziemshi, L. J., and K. L. Andrew, Arc Spectrum of Silicon, J. Opt. Soc. Amer., 55,474-491, 1965


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Wallace, L., K. Hinkle and W. Livingston, An Atlas of the Spectrum of the Solar Photosphere f

13,500 to 28,000 cm1

(3570 to 7405o

A),National Solar Observatory Tech. Report #98-001, 199

Zachwieja, M., New Investigations of the (A2-X2) Band System in the CH Radical and a New Re

tion of the Vibration-Rotation Spectrum of CH from Atmos Spectra, J. Molec. Spectros., 170,

309, 1995.

N. S. O. Technical Report #11-001

Published 2011, by

National Solar Observatory,

P. O. Box 26732, Tucson AZ 85726


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Wallace 2011 Solar Flux Atlas

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