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J/ApJS/229/23 New FeI level energies from stellar spectra. II. (Peterson+, 2017)

New Fe I level energies and line identifications from stellar spectra. II. Initial results from new ultraviolet spectra of metal-poor stars. Peterson R.C., Kurucz R.L., Ayres T.R. <Astrophys. J. Suppl. Ser., 229, 23-23 (2017)> =2017ApJS..229...23P (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Spectra, ultraviolet Keywords: atomic data; line: identification; methods: laboratory: atomic; techniques: spectroscopic; ultraviolet: stars Abstract: The Fe I spectrum is critical to many areas of astrophysics, yet many of the high-lying levels remain uncharacterized. To remedy this deficiency, Peterson & Kurucz (2015, J/ApJS/216/1) identified Fe I lines in archival ultraviolet and optical spectra of metal-poor stars, whose warm temperatures favor moderate Fe I excitation. Sixty-five new levels were recovered, with 1500 detectable lines, including several bound levels in the ionization continuum of Fe I. Here, we extend the previous work by identifying 59 additional levels, with 1400 detectable lines, by incorporating new high-resolution UV spectra of warm metal-poor stars recently obtained by the Hubble Space Telescope Imaging Spectrograph. We provide gf values for these transitions, both computed as well as adjusted to fit the stellar spectra. We also expand our spectral calculations to the infrared, confirming three levels by matching high-quality spectra of the Sun and two cool stars in the H-band. The predicted gf values suggest that an additional 3700 Fe I lines should be detectable in existing solar infrared spectra. Extending the empirical line identification work to the infrared would help confirm additional Fe I levels, as would new high-resolution UV spectra of metal-poor turnoff stars below 1900Å. Description: All of the new space-based UV spectra were obtained at a two-pixel resolution of 110000 with the E230H echelle grating of the Space Telescope Imaging Spectrograph (STIS) on HST, under program GO-14161 (R. Peterson, PI). See section 2 for further explanations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 45 59 New Fe I levels and energies table3.dat 96 10404 Newly classified lines of Fe I
See also: J/ApJS/216/1 : New FeI level energies from stellar spectra (Peterson+, 2015) J/A+A/547/A108 : Comparative modelling of cool giants spectra (Lebzelter+, 2012) J/A+A/520/A57 : New FeII energy levels from stellar spectra (Castelli+, 2010) J/A+AS/102/269 : Lab. and solar highly-excited levels of Fe I (Nave+ 1993) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1 A1 --- P e=even or o=odd levels 3- 22 A20 --- ExL Expanded label 24- 34 A11 --- Label Label 36 I1 --- J [0/7] Level J 38- 45 F8.2 cm-1 E [53591.5/67246.4] Energy
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 F9.4 nm lamAir [157.7/5997] Wavelength in air; vacuum below 200nm 11- 16 F6.3 [-] log(gf) [-10/0.7] Log of calculated oscillator strength times statistical weight of lower level 18 A1 --- l_dgf Upper limit on dgf if line not detected 19- 22 F4.1 --- dgf [-1.8/0.8]? If present, log(gf) which best matches observed spectra is log(gf) - dgf 26- 34 F9.3 cm-1 E.e [0/67717] Even level energy 37- 39 F3.1 --- J.e [0/7] Even level J 41- 50 A10 --- Label.e Even level label 54- 62 F9.3 cm-1 E.o [19350.8/65590.6] Odd level energy 65- 67 F3.1 --- J.o [0/8] Odd level J 69- 78 A10 --- Label.o Odd level label 81- 84 F4.2 [-] Gam.R [6.7/9.1] Log radiative damping constant 86- 90 F5.2 [cm-3] Gam.S [-6.1/-2.3] Log Stark damping constant/electron density 92- 96 F5.2 [cm-3] Gam.W [-7.8/-6.7] Log van der Waals damping constant/hydrogen density
History: From electronic version of the journal References: Peterson & Kurucz. Paper I 2015ApJS..216....1P Cat. J/ApJS/216/1
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 14-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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