J/ApJS/214/18 VII log(gf) values, and V abundance in HD 84937 (Wood+ 2014)
Improved V II log(gf) values, hyperfine structure constants, and abundance
determinations in the photospheres of the Sun and metal-poor star HD 84937.
Wood M.P., Lawler J.E., Den Hartog E.A., Sneden C., Cowan J.J.
<Astrophys. J. Suppl. Ser., 214, 18 (2014)>
=2014ApJS..214...18W 2014ApJS..214...18W
ADC_Keywords: Atomic physics ; Line Profiles ; Abundances
Keywords: atomic data; methods: laboratory: atomic; stars: abundances;
stars: individual: HD 84937; Sun: abundances
Abstract:
New experimental absolute atomic transition probabilities are reported
for 203 lines of V II. Branching fractions are measured from spectra
recorded using a Fourier transform spectrometer and an echelle
spectrometer. The branching fractions are normalized with radiative
lifetime measurements to determine the new transition probabilities.
Generally good agreement is found between this work and previously
reported V II transition probabilities. Two spectrometers, independent
radiometric calibration methods, and independent data analysis
routines enable a reduction in systematic uncertainties, in particular
those due to optical depth errors. In addition, new hyperfine
structure constants are measured for selected levels by least squares
fitting line profiles in the FTS spectra. The new V II data are
applied to high resolution visible and UV spectra of the Sun and
metal-poor star HD 84937 to determine new, more accurate V abundances.
Lines covering a range of wavelength and excitation potential are used
to search for non-LTE effects. Very good agreement is found between
our new solar photospheric V abundance, logε(V)=3.95 from
15 V II lines, and the solar-system meteoritic value. In HD 84937, we
derive [V/H]=-2.08 from 68 lines, leading to a value of [V/Fe]=0.24.
Description:
This V II transition probability study makes use of archived Fourier
transform spectrometer (FTS) data from the 1.0m FTS previously at the
National Solar Observatory (NSO) on Kitt Peak (13 FTS spectra were
recorded from 1979 Dec. 12 to 1986 July 30).
In addition to the 13 FTS spectra, 75 CCD frames of echelle
spectrometer spectra are also part of this V II transition probability
study. They were recorded from 2013 May 17 to 2014 May 14.
Objects:
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RA (ICRS) 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 54 203 Experimental atomic transition probabilities for
203 lines of VII from upper odd-parity levels
organized by increasing wavelength in air
table4.dat 53 21 New VII magnetic dipole hyperfine structure
constants from FTS spectra
table5.dat 54 1125 Hyperfine structure line component patterns for
67 lines of VII (ionized Vanadium)
table7.dat 29 68 Sixty-eight lines of ionized vanadium in HD 84937
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See also:
J/ApJS/211/20 : NiI transition probability measurements (Wood+, 2014)
J/ApJS/208/27 : Sun and HD 84937 TiII log(gf) and abundances (Wood+, 2013)
J/ApJS/207/20 : Parity-forbidden [Co II] and [VII] lines (Ruffoni+, 2013)
J/ApJS/207/13 : The spectrum and term analysis of VII (Thorne+, 2013)
J/ApJ/762/26 : Most metal-poor stars. II. Galactic halo stars (Yong+, 2013)
J/ApJS/194/35 : Atomic transition probabilities of Mn (Den Hartog+, 2011)
J/MNRAS/412/843 : SAGA extremely metal-poor stars (Suda+, 2011)
J/A+A/501/519 : Extremely metal-poor stars abundances (Bonifacio+, 2009)
J/AJ/137/272 : Space velocities orbits in the MW halo (Roederer+ 2009)
J/ApJS/182/80 : Rare earth abundances (Sneden+, 2009)
J/ApJ/681/1524 : Detailed abundances for 28 metal-poor stars (Lai+, 2008)
J/A+A/439/129 : HERES II. Spectroscopic analysis (Barklem+, 2005)
J/A+A/416/1117 : Abundances in the early Galaxy (Cayrel+, 2004)
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 lambda [2123.3/4600.2] Wavelength in air (Å) (1)
11- 19 F9.3 cm-1 E1 Upper level (2)
21 I1 --- J1 [0/6] Upper level J value (2)
23- 31 F9.3 cm-1 E0 Lower level (2)
33 I1 --- J0 [0/6] Lower level J value (2)
35- 41 F7.3 10+6/s A Transition probability
43- 48 F6.3 10+6/s e_A Total uncertainty in TranP
50- 54 F5.2 --- log.gf [-2.9/0.6] log(gf) (degeneracy times oscillator
strength)
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Note (1): Computed from energy levels using the standard index of air
from Peck & Reeder (1972JOSA...62..958P 1972JOSA...62..958P).
Note (2): From Thorne et al. (2013, Cat. J/ApJS/207/13).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Conf Assigned configuration (1)
15- 19 A5 --- Term Term (1)
21 I1 --- J [1/6] J value (1)
23 A1 --- P [eo] Parity (even or odd) (1)
26- 34 F9.3 cm-1 E [2605/47052] Level energy (1)
36- 40 F5.1 10-3/cm Ahf [-13.7/30.5] This work hyperfine structure
constant A
42- 44 F3.1 10-3/cm e_Ahf [1/3] Ahf uncertainty
46- 49 F4.1 10-3/cm Ahf1 [11.1/31.3]? Hyperfine structure constant A
from Arvidsson (2)
51- 53 F3.1 10-3/cm e_Ahf1 [0.2/5.7]? Ahf1 uncertainty (2)
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Note (1): Level energies and classifications are from Thorne et al. (2013,
Cat. J/ApJS/207/13).
Note (2): Arvidsson, 2003, master's thesis at Lund University, Lund, Sweden.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 F9.3 cm-1 sig [21901/37415] Center-of-Gravity wavenumber σ
11- 19 F9.4 0.1nm lambda [2672/4565] Center-of-Gravity air wavelength (Å)
21- 23 F3.1 --- F1 [0.5/9.5] Upper level F total angular momentum
25- 27 F3.1 --- F0 [0.5/8.5] Lower level F total angular momentum
29- 36 F8.5 cm-1 dsig Component offset wavenumber δσ (1)
38- 46 F9.6 0.1nm dlam Component offset wavelength δλ (1)
48- 54 F7.5 --- Str [0/1] Component strength normalized to sum to one
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Note (1): With respect to center-of-gravity wavenumber or wavelength.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lambda [2677/40235] Air wavelength (Å)
10- 14 F5.3 eV E0 [0.004/1.9] Lower level excitation energy
16- 20 F5.2 --- log(gf) [-1.7/0.6] Log of degeneracy times oscillator
strength
22- 25 F4.2 --- log(eps) [1.7/2.1] Log of abundance logε (H=12)
27- 29 A3 --- HFS [yes/no ] Hyperfine structure used in abundance
calculation?
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 13-Oct-2014