Transition probabilities and electronic transition moments of the A 2Σ+–X 2Π and D 2Σ+–X 2Π systems of nitric oxide

Luque, Jorge; Crosley, David R.

doi:10.1063/1.480064

Cited by 205 publications

(217 citation statements)

References 66 publications

Supporting

Mentioning

209

Contrasting

Order By: Relevance

“…For the CN-blue, NH, and OH-blue systems, the line lists by Kurucz (1993) were adopted, as implemented in Castilho et al (1999). For the CH blue systems, the LIFBASE program of Luque & Crosley (1999) was used. The OH vibration-rotation line list is the one implemented in Meléndez et al (2001).…”

Section: Molecular Line Opacitiesmentioning

confidence: 99%

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

Coelho¹,

Barbuy²,

Meléndez³

et al. 2005

A&A

401

498

View full text Add to dashboard Cite

Libraries of stellar spectra are fundamental tools for the study of stellar populations, and both empirical and synthetic libraries have been used for this purpose. In this paper, a new library of high resolution synthetic spectra is presented, ranging from the near-ultraviolet (300 nm) to the near-infrared (1.8 µm). The library spans all the stellar types that are relevant to the integrated light of old and intermediate-age stellar populations in the involved spectral region (spectral types F through M and all luminosity classes). The grid was computed for metallicities ranging from [Fe/H] = -2.5 to +0.5, including both solar and α-enhanced ([α/Fe] = 0.4) chemical compositions. The synthetic spectra are a good match to observations of stars throughout the stellar parameter space encompassed by the library and over the whole spectral region covered by the computations.

show abstract

Section: Molecular Line Opacitiesmentioning

confidence: 99%

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

Coelho¹,

Barbuy²,

Meléndez³

et al. 2005

A&A

401

498

View full text Add to dashboard Cite

show abstract

“…For each element X, Col. 2 gives the mean abundance log (X) = log N X /N H + 12, Col. 3 the number of lines measured, Col. 4 the standard deviation of the results, and Cols. 5 and 6 [X/H] and [X/Fe], respectively (where program of Luque & Crosley (1999) was used to compute line positions and g f -values. Excitation energies and isotopic shifts were taken from the line list of Jörgensen et al (1996), as LIFBASE only provides line positions for 12 CH.…”

Section: Carbon and Nitrogenmentioning

confidence: 99%

First Stars II. Elemental abundances in the extremely metal-poor star CS 22949–037

Depagne¹,

Hill²,

Spite³

et al. 2002

A&A

170

179

View full text Add to dashboard Cite

Abstract. CS 22949-037 is one of the most metal-poor giants known ([Fe/H] ≈ −4.0), and it exhibits large overabundances of carbon and nitrogen (Norris et al.). Using VLT-UVES spectra of unprecedented quality, regarding resolution and S /N ratio, covering a wide wavelength range (from λ = 350 to 900 nm), we have determined abundances for 21 elements in this star over a wide range of atomic mass. The major new discovery is an exceptionally large oxygen enhancement, [O/Fe] , we discuss the pairinstability supernovae. Such very massive objects indeed produce large amounts of oxygen, and have been found to be possible sources of primary nitrogen. However, the predicted odd/even effect is too large, and the predicted Zn abundance much too low. Other scenarios are also discussed. In particular, the yields of a recent model (Z35Z) from Heger and Woosley are shown to be in fair agreement with the observations. The only discrepant prediction is the very low abundance of nitrogen, possibly curable by taking into account other effects such as rotationally induced mixing. Alternatively, the absence of lithium in our star, and the values of the isotopic ratios 12 C/ 13 C and 13 C/ 14 N close to the equilibrium value of the CN cycle, suggest that the CNO abundances now observed might have been altered by nuclear processing in the star itself. A 30-40 M supernova, with fallback, seems the most likely progenitor for CS 22949-037. Article published by EDP Sciences and available at

show abstract

“…The assignment of the spectral peaks is based on the LIFBASE database. 34 The P 1 (1) and Q 1 (1) (and Q 21 (1)) transitions originating from the J ′′ = 3/2 rotational ground state and P 1 (2) (and P 21 (2)) and Q 1 (2) (and Q 21 (2)) of the first rotational excited J ′′ = 5/2 are clearly resolved. Since our dye laser has a bandwidth of about 0.1 cm -1 , the lines Q 1 (1) and Q 21 (1), P 1 (2) and P 21 (2), and Q 1 (2) and Q 21 (2) are overlapped and not resolvable.…”

Section: Rotational State Populationsmentioning

confidence: 96%

Cold and intense OH radical beam sources

Ploenes¹,

Haas

Zhang

et al. 2016

Review of Scientific Instruments

View full text Add to dashboard Cite

We present the design and performance of two supersonic radical beam sources: a conventional pinhole-discharge source and a dielectric barrier discharge (DBD) source, both based on the Nijmegen pulsed valve. Both designs have been characterized by discharging water molecules seeded in the rare gases Ar, Kr, or Xe. The resulting OH radicals have been detected by laser-induced fluorescence. The measured OH densities are (3.0 ± 0.6) × 10 11 cm -3 and (1.0 ± 0.5) × 10 11 cm -3 for the pinholedischarge and DBD sources, respectively. The beam profiles for both radical sources show a relative longitudinal velocity spread of about 10%. The absolute rotational ground state population of the OH beam generated from the pinhole-discharge source has been determined to be more than 98%. The DBD source even produces a rotationally colder OH beam with a population of the ground state exceeding 99%. For the DBD source, addition of O 2 molecules to the gas mixture increases the OH beam density by a factor of about 2.5, improves the DBD valve stability, and allows to tune the mean velocity of the radical beam. Published by AIP Publishing. [http://dx

show abstract

Transition probabilities and electronic transition moments of the A 2Σ+–X 2Π and D 2Σ+–X 2Π systems of nitric oxide

Cited by 205 publications

References 66 publications

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

First Stars II. Elemental abundances in the extremely metal-poor star CS 22949–037

Cold and intense OH radical beam sources

Contact Info

Product

Resources

About