Oscillator Strengths for Ultraviolet Transitions in P ii: The Multiplet at 1308 Å

Brown, Michael S.; Alkhayat, Rabee B.; Irving, R. E.; Heidarian, Negar; Brown, Jeremy Bancroft; Federman, S. R.; Cheng, Song; Curtis, L. J.

doi:10.3847/1538-4357/aae688

Cited by 12 publications

(27 citation statements)

References 40 publications

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“…Schectman et al (2005) found contaminating lines from highly-ionized chlorine (Cl IV and V) in their THIA data on Cl II, too. The same situation was observed by Brown et al (2018) in their work on P II. Further measurements at 170 keV were produced on the Cl V line at 545.11 Å to establish its short lifetime.…”

Section: Methodssupporting

confidence: 83%

Lifetimes and Oscillator Strengths for Ultraviolet Transitions in Neutral Chlorine

Alkhayat

Irving

Federman

et al. 2019

ApJ

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We present lifetime measurements using beam-foil techniques for radiative transitions from the 3p 4 ( 1 S)4s 2 S 1/2 , 3p 4 ( 3 P )5s 2 P 1/2,3/2 , and 3p 4 ( 3 P )3d 2 F 5/2 levels in Cl I and the corresponding results of the oscillator strengths for transitions at 1004.68, 1079.88, 1090.73, and 1094.77Å, respectively. We compare our experimental results with available theoretical calculations and astronomical observations in an effort to resolve discrepancies among them.

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Section: Methodssupporting

confidence: 83%

Lifetimes and Oscillator Strengths for Ultraviolet Transitions in Neutral Chlorine

Alkhayat

Irving

Federman

et al. 2019

ApJ

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“…Jenkins (2009) adopted theoretical P ii f -values originally obtained by Hibbert (1988). However, more precise experimentallydetermined f -values for the important λ1152 and λ1301 transitions are now available (Federman et al 2007;Brown et al 2018). These new experimental results indicate that the P ii column densities obtained from the λ1152 and λ1301 transitions should be revised downward by 0.045 dex and 0.188 dex, respectively, in agreement with recent theoretical calculations (Tayal 2003;Froese Fischer et al 2006).…”

Section: Introductionsupporting

confidence: 68%

“…For our analysis of P ii column densities, we adopt the experimentally determined oscillator strength for the P ii λ1301 transition recently published by Brown et al (2018). Their f -value for P ii λ1301 indicates that a downward revision of 0.188 dex should be applied to column densities derived using the older Hibbert (1988) fvalue (which is the one recommended by Morton 2003).…”

Section: Phosphorus Column Densitiesmentioning

confidence: 99%

A Reexamination of Phosphorus and Chlorine Depletions in the Diffuse Interstellar Medium

Ritchey¹,

Brown²,

Federman³

et al. 2023

Preprint

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We present a comprehensive examination of interstellar P and Cl abundances based on an analysis of archival spectra acquired with the Space Telescope Imaging Spectrograph of the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer. Column densities of P ii, Cl i, and Cl ii are determined for a combined sample of 107 sight lines probing diffuse atomic and molecular gas in the local Galactic interstellar medium (ISM). We reevaluate the nearly linear relationship between the column densities of Cl i and H 2 , which arises from the rapid conversion of Cl + to Cl 0 in regions where H 2 is abundant. Using the observed total gas-phase P and Cl abundances, we derive depletion parameters for these elements, adopting the methodology of Jenkins. We find that both P and Cl are essentially undepleted along sight lines showing the lowest overall depletions. Increasingly severe depletions of P are seen along molecule-rich sight lines. In contrast, gas-phase Cl abundances show no systematic variation with molecular hydrogen fraction. However, enhanced Cl (and P) depletion rates are found for a subset of sight lines showing elevated levels of Cl ionization. An analysis of neutral chlorine fractions yields estimates for the amount of atomic hydrogen associated with the H 2 -bearing gas in each direction. These results indicate that the molecular fraction in the H 2 -bearing gas is at least 10% for all sight lines with log N (H 2 ) 18 and that the gas is essentially fully molecular at log N (H 2 ) ≈ 21.

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“…For absorp-tion lines of interest we constructed theoretical Voigt line profiles from initial estimates of v, N, and b, and allowed these parameters to vary until a minimum in χ 2 between profile and data was reached. Oscillator strengths for the lines were taken from Morton (2003), Kisielius et al (2014) (S II), Federman et al (2007) (P II λ1152), or Brown et al (2018) (P II λ1301). Theoretical line profiles were convolved with COS Line Spread Functions (LSFs) constructed by interpolating LSF tables 2 to the relevant wavelength.…”

Section: Line Identification and Profile Fittingmentioning

confidence: 99%

Absorption-line Abundances in the SMC-like Galaxy UGC 5282: Evidence of ISM Dilution from Inflows on Kiloparsec Scales*

Bowen

Tripp

Jenkins

et al. 2020

ApJ

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We present an HST Cosmic Origins Spectrograph (COS) spectrum of the QSO SDSS J095109.12+330745.8 (z em = 0.645) whose sightline passes through the SMC-like dwarf galaxy UGC 5282 (M B = −16.0, cz = 1577 km s −1 ), 1.2 kpc in projection from the central H II region of the galaxy. Damped Lyα (DLA) absorption is detected at the redshift of UGC 5282 with log [N(H I) cm −2 ] = 20.89 +0.12 −0.21 . Analysis of the accompanying S II, P II and O I metal lines yields a neutral gas metallicity, Z H I , of [S/H] [P/H] = −0.80 ± 0.24. The metallicity of ionized gas from the central H II region, Z H II , measured from its emission lines is [O/H]= −0.37 ± 0.10, a difference of +0.43 ± 0.26 from Z H I . This difference δ is consistent with that seen towards H II regions in other star-forming galaxies and supports the idea that ionized gas near star forming regions shows systematically higher metallicities than exist in the rest of a galaxy's neutral interstellar medium (ISM). The positive values of δ found in UGC 5282 (and the other star forming galaxies) is likely due to infalling low metallicity gas from the intergalactic medium that mixes with the galaxy's ISM on kpc scales. This model is also consistent with broad Lyα emission detected at the bottom of the DLA absorption, offset by ∼ 125 km s −1 from the absorption velocity. Models of galaxy evolution that attempt to replicate population characteristics, such as the mass-metallicity relation, may need to start with a galaxy metallicity represented by Z H I rather than that measured traditionally from Z H II .

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Oscillator Strengths for Ultraviolet Transitions in P ii: The Multiplet at 1308 Å

Cited by 12 publications

References 40 publications

Lifetimes and Oscillator Strengths for Ultraviolet Transitions in Neutral Chlorine

Lifetimes and Oscillator Strengths for Ultraviolet Transitions in Neutral Chlorine

A Reexamination of Phosphorus and Chlorine Depletions in the Diffuse Interstellar Medium

Absorption-line Abundances in the SMC-like Galaxy UGC 5282: Evidence of ISM Dilution from Inflows on Kiloparsec Scales*

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