J/ApJS/208/27 Sun and HD 84937 TiII log(gf) and abundances (Wood+, 2013)
Improved Ti II log(gf) values and abundance determinations in the
photospheres of the Sun and metal-poor star HD 84937.
Wood M.P., Lawler J.E., Sneden C., Cowan J.J.
<Astrophys. J. Suppl. Ser., 208, 27 (2013)>
=2013ApJS..208...27W 2013ApJS..208...27W
ADC_Keywords: Atomic physics ; Abundances ; Stars, metal-deficient ; Sun
Keywords: atomic data - methods: laboratory: atomic - Sun: abundances -
stars: abundances - stars: individual: HD 84937
Abstract:
Atomic transition probability measurements for 364 lines of Ti II in
the UV through near-IR are reported. Branching fractions from data
recorded using a Fourier transform spectrometer (FTS) and a new
echelle spectrometer are combined with published radiative lifetimes
to determine these transition probabilities. The new results are in
generally good agreement with previously reported FTS measurements.
Use of the new echelle spectrometer, independent radiometric
calibration methods, and independent data analysis routines enables a
reduction of systematic errors and overall improvement in transition
probability accuracy over previous measurements. The new Ti II data
are applied to high-resolution visible and UV spectra of the Sun and
metal-poor star HD 84937 to derive new, more accurate Ti abundances.
Lines covering a range of wavelength and excitation potential are used
to search for non-LTE effects. The Ti abundances derived using Ti II
for these two stars match those derived using Ti I and support the
relative Ti/Fe abundance ratio versus metallicity seen in previous
studies.
Description:
The 14 1.0m FTS (Fourier transform spectrometer) spectra (1989 Feb 28
to 1992 Jul 29) used in this TiII branching fraction analysis are
available in the NSO electronic archives.
In addition to the 14 FTS spectra, 48 charge-coupled device (CCD)
frames of Ti HCD spectra (from 2011 Jul 27 to 2012 Feb 23), recorded
with the echelle spectrometer, are part of this TiII branching
fraction study. See section 3 for further details.
Objects:
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RA (2000) DE Designation(s)
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09 48 56.10 +13 44 39.3 HD 84937 = TYC 834-654-1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 71 364 Comparison of experimental branching fractions from
FTS data for 364 lines of TiII from upper
odd-parity levels organized by upper level
table4.dat 60 364 Experimental Atomic Transition Probabilities for
364 lines of TiII from upper odd-parity levels
organized by increasing wavelength in air
table5.dat 25 43 Solar Photospheric Titanium Abundances from
Individual TiII Lines
table6.dat 25 147 Titanium Abundances from Individual TiII Lines
in HD 84937
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See also:
III/193 : Chemical Abundances in Late-Type Stars (Thevenin, 1998)
J/A+A/554/A96 : Metal-poor star spectra of the LiI 670.8nm line (Lind+, 2013)
J/ApJS/199/8 : Interstellar column densities compilation (Gudennavar+, 2012)
J/MNRAS/404/1321 : TiII in Milky way and Magellanic clouds (Welty+, 2010)
J/MNRAS/396/1895 : MgI and sTiO index definitions (Cenarro+, 2009)
J/MNRAS/367/1478 : Interstellar NaI, TiII + CaIIK obs. (Hunter+, 2006)
J/A+A/404/187 : Equivalent widths for metal-poor stars (Gratton+, 2003)
J/ApJ/562/528 : Teff and log(g) of low-metallicity stars (Snider+, 2001)
J/A+AS/133/221 : Library of ELODIE spectra (F5-K7 stars) (Soubiran+ 1998)
J/A+AS/109/193 : IRON project VIII. Ti-like ions (Berrington, 1995)
J/AJ/90/2089 : Stars of very low metal abundance. I (Beers+, 1985)
http://nsokp.nso.edu/ : Kitt Peak NSO home page
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 F9.4 0.1nm lamAir [2325/9748] Wavelength in air; Angstroms (G1)
11- 19 F9.3 cm-1 E1 [29544/47626] Upper level (G2)
21- 23 F3.1 --- J1 [0.5/5.5] Upper level J value (G2)
25- 33 F9.3 cm-1 E0 [0/32333] Lower level (G2)
35- 37 F3.1 --- J0 [0.5/5.5] Lower level J value (G2)
39- 45 F7.5 --- BF-P01 [0.0003/0.95]? Branching fraction;
Pickering et al. 2001ApJS..132..403P 2001ApJS..132..403P
47- 48 I2 % e_BF-P01 [1/43]? Uncertainty in BF-P01
50- 57 F8.6 --- BF-B93 [4.8e-05/0.8]? Branching fraction;
Bizzarri et al. 1993A&A...273..707B 1993A&A...273..707B
59- 60 I2 % e_BF-B93 [1/57]? Uncertainty in BF-B93
62- 68 F7.5 --- BF [6e-05/1] Branching fraction; this experiment
70- 71 I2 % e_BF [0/20] Uncertainty in BF
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 0.1nm lamAir [2325/9748] Wavelength in air; Angstroms (G1)
11- 19 F9.3 cm-1 E1 [29544/47626] Upper level (G2)
21- 23 F3.1 --- J1 [0.5/5.5] Upper level J value (G2)
25- 33 F9.3 cm-1 E0 [0/32333] Lower level (G2)
35- 37 F3.1 --- J0 [0.5/5.5] Lower level J value (G2)
39- 46 F8.4 10+6/s A [0.015/198] Transition probability
48- 54 F7.4 10+6/s e_A [0.002/10] Total uncertainty in A
56- 60 F5.2 --- log(gf) [-3.4/0.6] Log of degeneracy times
oscillator strength
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Byte-by-byte Description of file: table[56].dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lamAir [2474/9433] Wavelength in air
10- 14 F5.3 eV E0 [0/3.2] Lower level energy
16- 20 F5.2 --- log(gf) [-3.4/0.5] Log of degeneracy times
oscillator strength
22- 25 F4.2 [---] log(eps) [2.8/5.1] Log of abundance (logε)
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Global notes:
Note (G1): Computed from energy levels using the standard index of air
from Peck & Reeder (1972JOSA...62..958P 1972JOSA...62..958P).
Note (G2): From Saloman (2012JPCRD..41a3101S 2012JPCRD..41a3101S).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 31-Oct-2013