Tables of atomic spectral lines for the 10000 Å to 40000 Å region

Outred, M

doi:10.1063/1.555568

Cited by 39 publications

(7 citation statements)

References 3 publications

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“…Three heavy elements were found to be detectable in the APOGEE window, with identified lines from Ce II (8 lines), Nd II (10 lines), and Yb II (1 line). The initial identifications of these lines were facilitated by the compilation of heavy-element spectral lines in the wavelength range of λ10,000 − 40,000Å by Outred (1978). By and large, these lines are mostly weak and usually blended in R ∼ 22, 500 stellar spectra (although a few of the Ce II lines can be fairly strong in red giants); however, they can provide abundances in certain populations observed by APOGEE.…”

Section: Heavy Element Lines In Dr16mentioning

confidence: 99%

The APOGEE Data Release 16 Spectral Line List

et al. 2021

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Smith et al.The updated H-band spectral line list (from λ15,000 -17,000Å) adopted by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) for the SDSS IV Data Release 16 (DR16) is presented here. The APOGEE line list is a combination of atomic and molecular lines with data from laboratory, theoretical, and astrophysical sources. Oscillator strengths and damping constants are adjusted using high signal-tonoise, high-resolution spectra of the Sun and α Boo (Arcturus) as "standard stars". Updates to the DR16 line list, when compared to the previous DR14 version, are the inclusion of molecular H 2 O and FeH lines, as well as a much larger (by a factor of ∼4) atomic line list, which includes significantly more transitions with hyperfine splitting. More recent references and line lists for the crucial molecules CO and OH were used, as well as for C 2 and SiH. In contrast to DR14, DR16 contains measurable lines from the heavy neutron-capture elements cerium (as Ce II), neodymium (as Nd II), and ytterbium (as Yb II), as well as one line from rubidium (as Rb I), that may be detectable in a small fraction of APOGEE red giants.

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Section: Heavy Element Lines In Dr16mentioning

confidence: 99%

The APOGEE Data Release 16 Spectral Line List

et al. 2021

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“…The only obvious exception is the transition in 7 3 P − 4 3 S 1.7455 µm, which is very strong compared to model predictions of Smits (1996) even after subtraction of the expected contribution of [Fe II] 1.7454 µm. This feature may include a third unidentified line blended with He I and [Fe II], possibly C I at 1.7453 µm (Outred 1978). We do not expect fluorescent emission in H 2 7-5 Q(3) at 1.7463 µm to contribute significantly to this blend in the Orion bar or Orion S. In conclusion, it appears that the transitions in n 3 P − 2 3 S are optically thick in Hubble 12 and G45.12+0.13, while the effect is less extreme in Orion.…”

Section: Helium Linesmentioning

confidence: 99%

Near‐Infrared Spectroscopy of Photodissociation Regions: The Orion Bar and Orion S

Luhman

Engelbracht

Luhman

1998

ApJ

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We have obtained moderate-resolution (R ∼ 3000) spectra of the Orion bar and Orion S regions at J (1.25 µm), H (1.64 µm), and K (2.2 µm). Towards the bar, the observations reveal a large number of H 2 emission lines that, when compared to model predictions of Draine & Bertoldi (1996), are indicative of a high-density photodissociation region (PDR) (n H = 10 6 cm −3 , χ = 10 5 , T 0 = 1000 K) rather than shocked material. Behind the bar into the molecular cloud, the H 2 spectrum again matches well with that predicted for a dense PDR (n H = 10 6 cm −3 ) but with a lower temperature (T 0 = 500 K) and UV field strength (χ = 10 4 ). The H 2 spectrum and stratification of near-IR emission lines (O I, H I, [Fe II], [Fe III], H 2 ) near Orion S imply the presence of a dense PDR with an inclined geometry in this region as well (n H = 10 6 cm −3 , χ = 10 5 , T 0 = 1500 K). The extinction measurements towards the bar (A K ∼ 2.6) and Orion S (A K ∼ 2.1) H 2 emission regions are much larger than expected from either face-on (A K ∼ 0.1) or edge-on (A K ∼ 1) homogeneous PDRs, indicating that clumps may significantly affect the structure of the PDRs.In addition, we have observed the strongest ∼ 30 near-IR He I emission lines, many of which have not been detected previously. There is good agreement between most observed and theoretical He I line ratios, while a few transitions with upper levels of n 3 P (particularly 4 3 P − 3 3 S 1.2531 µm) are enhanced over strengths expected from collisional excitation. This effect is possibly due to opacity in the UV series n 3 P − 2 3 S. We also detect several near-IR [Fe II] and [Fe III] transitions with line ratios indicative of low densities (n e ∼ 10 3 -10 4 cm −3 ), whereas recent observations of optical [Fe II] emission imply the presence of high-density gas (n e ∼ 10 6 cm −3 ). These results are

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“…In order to sort out the lines of the gases, we have compared spectra of magnesium with spectra of aluminium and vanadium recorded in similar conditions. We have also checked for possible impurities using the infrared line list of Outred [16]. Except in a few cases for wide profiles or very weak lines for which the corresponding wavenumbers were obtained by interpolation, a special computer program has been used to obtain automatically the approximate wavenumbers of the lines.…”

Section: Introductionmentioning

confidence: 99%

The Infrared Spectrum of Magnesium (1800 < σ < 9000 cm^-1) and an Extension of the Term Systems of Mg I and Mg II

Biémont

Brault

1986

Phys. Scr.

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The spectrum of neutral and singly ionized magnesium produced by a hollow-cathode discharge has been observed by the Fourier transform spectroscopy technique between 1800 and 9000 cm-1. The observations reported here have allowed an extension of the term systems of Mg I and Mg II; more particularly, first observational evidence is reported for 3s ng 1,3G(n ⩽ 8) terms of Mg I and ni 2I(n ⩽ 10) terms of Mg II. The results are also used for refining the identification of magnesium lines in the solar photospheric spectrum.

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Tables of atomic spectral lines for the 10000 Å to 40000 Å region

Cited by 39 publications

References 3 publications

The APOGEE Data Release 16 Spectral Line List

The APOGEE Data Release 16 Spectral Line List

Near‐Infrared Spectroscopy of Photodissociation Regions: The Orion Bar and Orion S

The Infrared Spectrum of Magnesium (1800 < σ < 9000 cm^-1) and an Extension of the Term Systems of Mg I and Mg II

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Tables of atomic spectral lines for the 10000 Å to 40000 Å region

Cited by 39 publications

References 3 publications

The APOGEE Data Release 16 Spectral Line List

The APOGEE Data Release 16 Spectral Line List

Near‐Infrared Spectroscopy of Photodissociation Regions: The Orion Bar and Orion S

The Infrared Spectrum of Magnesium (1800 < σ < 9000 cm-1) and an Extension of the Term Systems of Mg I and Mg II

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The Infrared Spectrum of Magnesium (1800 < σ < 9000 cm^-1) and an Extension of the Term Systems of Mg I and Mg II