The ionization potential of neutral iron, Fe I, by multistep laser spectroscopy

Worden, Earl F.; Comaskey, B.; Densberger, J.; Christensen, J. J.; McAfee, John M.; Paisner, J. A.; Conway, John G.

doi:10.1364/josab.1.000314

Cited by 21 publications

(7 citation statements)

References 5 publications

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“…The ionization energy determined for FeC is less than that of atomic iron ͑7.9024 eV͒ 24 by 1310Ϯ726 cm Ϫ1 . This indicates that the ground state of FeC is very nearly as strongly bound as the ground state of the cationic species.…”

Section: B Bond Strength Of Fecmentioning

confidence: 78%

Optical spectroscopy of jet-cooled FeC between 12 000 and 18 100 cm−1

Brugh

Morse

1997

The Journal of Chemical Physics

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Iron monocarbide has been investigated between 12 000 and 18 100 cm Ϫ1 in a supersonic expansion by resonant two-photon ionization spectroscopy. Six new electronic states have been identified for which origins relative to the ground state have been determined. Three of these possess ⍀Јϭ3, one possesses ⍀Јϭ4, and two possess ⍀Јϭ2. The ⍀Јϭ3 state with an origin near 13 168 cm Ϫ1 is likely a 3 ⌬ 3 state and has been assigned as the analog of the ͓14.0͔ 2 ⌺ ϩ ←X 2 ⌺ ϩ charge transfer transition in CoC. The ⍀Јϭ4 state is most likely a 3 ⌽ 4 state. Additionally, seven bands with ⍀Јϭ2 have been observed that have proven impossible to systematically group by electronic state. Because every transition rotationally resolved in this study possesses a lower state with ⍀ϭ3, the ground state has been confirmed as arising from an ⍀ϭ3 state that is most likely the ⍀ϭ3 spin orbit component of a 3 ⌬ i term derived from a 1␦ 3 9 1 configuration. The ionization energy ͑IE͒ of FeC has been determined as 7.74Ϯ0.09 eV by varying the wavelength of the ionization photon. When combined with the known IE of Fe and the bond energy of FeC ϩ , the bond energy of FeC is calculated to be 3.9Ϯ0.3 eV. Presentation of the results is accompanied by an analysis of the bonding in FeC from a molecular orbital standpoint.

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Section: B Bond Strength Of Fecmentioning

confidence: 78%

Optical spectroscopy of jet-cooled FeC between 12 000 and 18 100 cm−1

Brugh

Morse

1997

The Journal of Chemical Physics

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“…On the other hand, we observe two-components in the [Fe ii] profile at the locations of the radio hot spots. The [Fe ii] traces even lower ionization gas than Paβ as the ion Fe ii is formed in partially ionized regions, having an ionization potential of only 7.9 eV (Worden et al 1984), while the Paβ line originates from a fully ionized region (e.g. Riffel et al 2013a).…”

Section: Discussionmentioning

confidence: 99%

An Outflow Perpendicular to the Radio Jet in the Seyfert Nucleus of NGC 5929

Riffel

Storchi‐Bergmann

Riffel

2013

ApJ

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We report the observation of an outflow perpendicular to the radio jet in near-infrared integral field spectra of the inner 250 pc of the Seyfert 2 galaxy NGC 5929. The observations were obtained with the Gemini Near infrared Integral Field Spectrograph at a spatial resolution of ∼20 pc and spectral resolution R≈ 5300 and reveal a region ∼ 50 pc wide crossing the nucleus and extending by ∼ 300 pc perpendicularly to the known radio jet in this galaxy. Along this structure -which we call SE-NW strip -the emission-line profiles show two velocity components, one blueshifted and the other redshifted by −150km s −1 and 150km s −1 , respectively, relative to the systemic velocity. We interpret these two components as due to an outflow perpendicular to the radio jet, what is supported by low frequency radio emission observed along the same region. We attribute this feature to the interaction of ambient gas with an "equatorial outflow" predicted in recent accretion disk and torus wind models. Perpendicularly to the SE-NW strip, thus approximately along the radio jet, single component profiles show blueshifts of ≈ −150km s −1 to the north-east and similar redshifts to the south-west, which can be attributed to gas counter-rotating relative to the stellar kinematics. More double-peaked profiles are observed in association with the two radio hot-spots, attributed to interaction of the radio jet with surrounding gas.

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“…In Barbosa et al (2014), we use a "lemniscata" geometry (similar to that of an hourglass) to model the [Fe ii] kinematics (outflow), showing that it reproduces better the flux distributions in channel maps than a bicone. We attribute the larger extent and "broader" flux distribution to the fact that the ion Fe ii is also formed in partially ionized regions, as Fe i has an ionization potential of only 7.9 eV (Worden et al 1984). Thus, [Fe ii] emission can be observed beyond the fully ionized regions, in locations where there is no more H + or O ++ but may still be outflows.…”

Section: Ionized and Molecular Gas Distributionsmentioning

confidence: 93%

Feeding versus feedback in NGC 1068 probed with Gemini NIFS – I. Excitation

Riffel

Vale

Storchi‐Bergmann

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present emission-line flux distributions and ratios for the inner ≈ 200 pc of the narrow-line region of the Seyfert 2 galaxy NGC 1068, using observations obtained with the Gemini Near-infrared Integral Field Spectrograph (NIFS) in the J, H and K bands at a spatial resolution of ≈ 10 pc and spectral resolution of ≈ 5300. The molecular gas emission -traced by the K-band H 2 emission lines -outlines an offcentered circumnuclear ring with a radius of ≈ 100 pc showing thermal excitation. The ionized gas emission lines show flux distributions mostly outlining the previously known [O iii]λ5007 ionization bicone. But while the flux distributions in the H i and He ii emission lines are very similar to that observed in [O iii], the flux distribution in the [Fe ii] emission lines is more extended and broader than a cone close to the nucleus, showing a "double bowl" or 'hourglass" structure". This difference is attributed to the fact that the [Fe ii] emission, besides coming from the fully ionized region, comes also from the more extended partially ionized regions, in gas excited mainly by X-rays from the active galactic nucleus. A contribution to the [Fe ii] emission from shocks along the bicone axis to NE and SW of the nucleus is also supported by the enhancement of the [Fe ii](1.2570 µm)/[P ii](1.1885 µm) and [Fe ii](1.2570 µm)/Paβ emission-line ratios at these locations and is attributed to the interaction of the radio jet with the NLR. The mass of ionized gas in the inner 200 pc of NGC 1068 is M H II ≈ 2.2 × 10 4 M , while the mass of the H 2 emitting gas is only M H2 ≈ 29 M . Taking into account the dominant contribution of the cold molecular gas, we obtain an estimate of the total molecular gas mass of M cold ≈ 2 × 10 7 M .

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The ionization potential of neutral iron, Fe I, by multistep laser spectroscopy

Cited by 21 publications

References 5 publications

Optical spectroscopy of jet-cooled FeC between 12 000 and 18 100 cm−1

Optical spectroscopy of jet-cooled FeC between 12 000 and 18 100 cm−1

An Outflow Perpendicular to the Radio Jet in the Seyfert Nucleus of NGC 5929

Feeding versus feedback in NGC 1068 probed with Gemini NIFS – I. Excitation

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