On the 1 μm system of iron hydride

Balfour, Walter J.; Lindgren, B.; O'Connor, Seamus

doi:10.1016/0009-2614(83)80501-6

Cited by 12 publications

(6 citation statements)

References 4 publications

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“…The first laboratory spectrum of FeH was produced by Kleman & Åkerlind (1957, unpublished), but the rotational structure of the line spectrum was not analyzed. Balfour, Lindgren & O'Connor (1983) showed that the WFB was associated to a 4 ∆ − 4 ∆ transition. Phillips et al (1987) carried out a rotational analysis of the WFB, identifying seven vibrational bands and determining rotational and vibrational constants and spin splittings.…”

Section: Introductionmentioning

confidence: 99%

The FeH Wing‐Ford Band in Spectra of M Stars

Schiavon

Barbuy

Singh

1997

ApJ

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We study the FeH Wing-Ford band at λλ 9850 -10200Å by means of the fit of synthetic spectra to the observations of M stars, employing recent model atmospheres. On the basis of the spectrum synthesis, we analyze the dependence of the band upon atmospheric parameters.FeH lines are a very sensitive surface gravity indicator, being stronger in dwarfs. They are also sensitive to metallicity (Allard & Hauschildt 1995). The blending with CN lines, which are stronger in giants, does not affect the response of the Wing-Ford band to surface gravity at low resolution (or high velocity dispersions) because CN lines, which are spread all along the spectrum, are smeared out at convolutions of FWHM > ∼ 3Å. We conclude that the Wing-Ford band is a suitable dwarf/giant indicator for the study of composite stellar populations.

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Section: Introductionmentioning

confidence: 99%

The FeH Wing‐Ford Band in Spectra of M Stars

Schiavon

Barbuy

Singh

1997

ApJ

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“…A refined test dubbed the method of wavelength-coincidence statistics (WCS) has been applied by Cowley and colleagues to various problems of line identification in stellar spectra. The method was introduced by Hartoog, Cowley, and Cowley (1973) to test the controversial identification of promethium in the Ap star HR 465 (Aller and Cowley 1970). In the method of WCS, the stellar line list is searched for coincidences with a laboratory line list for the species of interest.…”

Section: B Some Guidelinesmentioning

confidence: 99%

On the identification of molecules in the cool carbon stars

Lambert¹

1988

PASP

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“…Rotational analysis at that time was hindered by the lack of obvious regularity and high sample temperatures. However, in 1983 Balfour et al made the breakthrough which has been the basis for all following work; a rotational analysis of the 988 nm system of the deuteride as a 4 ⌬ -4 ⌬ transition 8 which enabled a detailed analysis of the corresponding system in the emission spectrum of FeH. 9 The development of a new low-temperature production method of FeH by Beaton et al 10 provided the means to unlock the visible spectrum of this radical.…”

Section: Introductionmentioning

confidence: 99%

Complete characterization of the a 6Δ state of the FeH radical

Wilson¹,

Cook²,

Brown³

2001

The Journal of Chemical Physics

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The electronic spectrum of the fluoroborane free radical. II. Analysis of laser-induced fluorescence and single vibronic level emission spectra The electronic spectrum of the fluoroborane free radical. I. Theoretical calculation of the vibronic energy levels of the ground and first excited electronic states Rotational analysis and assignment of the green band system of FeH to the e6Π-a6Δ transitionThe electronic spectrum of the FeH radical at near ambient ͑ϳ450 K͒ temperature has been re-investigated at high resolution. More than 150 lines have been assigned by the use of LIF and dispersed LIF techniques. Dispersed fluorescence experiments in the green region have shown surprisingly strong ⌬⍀ϭ0, ϩ1, ϩ2... transitions in the e 6 ⌸ -a 6 ⌬ system, for which the case ͑a͒ selection rule is ⌬⍀ϭϪ1. The analysis of ⌬⍀ϭ0 and Ϫ1 sub-bands in this system has given term values in the previously unseen ⍀ϭ1/2 and Ϫ1/2 components of a 6 ⌬ (vϭ0), e 6 ⌸ Ϫ1/2 (vϭ0) and a 6 ⌬ 1/2 (vϭ1). The a 6 ⌬ state is now experimentally confirmed as a state of sextet nature and is only the second sextet state of FeH to be seen in all spin-orbit components ͑the other is c 6 ⌺ ϩ ͒. The a 6 ⌬ state is not well-described by a single state effective Hamiltonian; the best fit to this model gives a standard deviation of around 125 times the experimental error. In addition, term values have been determined for a set of levels whose term value origin lies at 3175 cm Ϫ1 above the ground state. These have been tentatively assigned to the vϭ0 level of the C 4 ⌽ 9/2 component and are hypothesised to be the cause of the known perturbation to the a 6 ⌬ 9/2 (vϭ1) level.

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On the 1 μm system of iron hydride

Cited by 12 publications

References 4 publications

The FeH Wing‐Ford Band in Spectra of M Stars

The FeH Wing‐Ford Band in Spectra of M Stars

On the identification of molecules in the cool carbon stars

Complete characterization of the a 6Δ state of the FeH radical

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