Atomic Data Assessment with PyNeb: Radiative and Electron Impact Excitation Rates for [Fe ii] and [Fe iii]

Mendoza, C.; Méndez-Delgado, J. E.; Bautista, M. A.; García‐Rojas, J.; Morisset, C.

doi:10.3390/atoms11040063

Cited by 6 publications

(3 citation statements)

References 63 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Fe III and Fe II are of high interest in astrophysics (see below), as has very recently been discussed by expert practitioners of spectral modeling and emission line analysis [154]. I agree with the uncertainty assessment of transition rate and level lifetime prediction, which is discussed there with many more examples than would be appropriate in the present text.…”

Section: Ar-like Fe IXsupporting

confidence: 77%

“…This is important for the prediction of branching fractions, which are of interest in astrophysical studies. The Stockholm Fe II lifetimes are quoted with uncertainties from 3% to about 14%, which is the same order of magnitude as the assessed prediction uncertainty in the study by Mendoza et al [154] mentioned above. A major uncertainty, in particular for very long lifetimes, is the correction for ion loss during storage in the ring.…”

Section: Mn-like Fe IIsupporting

confidence: 60%

See 1 more Smart Citation

Atomic Lifetimes of Astrophysical Interest in Ions of Fe

Träbert

2023

Atoms

View full text Add to dashboard Cite

Multiple charged ions of iron dominate the EUV spectrum of the solar corona. For the interpretation of such spectra, data on both the atomic structure and the transition rate are essential, most of which are provided by theory and computation. The wavelengths of observed spectra are used to test the predicted energy level structure, while the line intensities depend on level lifetimes and branch fractions. A number of electric dipole and higher-order transition rates have been measured over the years in the laboratory, mostly by beam-foil spectroscopy, at heavy-ion storage rings, and at various ion traps. In this paper, the state of the knowledge base on level lifetimes in all ions of Fe is assessed, and the problems of further progress are outlined.

show abstract

Section: Ar-like Fe IXsupporting

confidence: 77%

Section: Mn-like Fe IIsupporting

confidence: 60%

Atomic Lifetimes of Astrophysical Interest in Ions of Fe

Träbert

2023

Atoms

View full text Add to dashboard Cite

show abstract

“…[Fe II]λ4360 and [Fe II]λ4288 arise from the same atomic upper level, and their relative intensities are independent of the physical conditions of the gas and depend solely on the atomic transition probabilities. Because I(λ4360)/I(λ4288) = 0.73 (Mendoza et al 2023)…”

Section: Measurement Of Auroral-line Emissionmentioning

confidence: 99%

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

Rickards Vaught,

Sandstrom,

Belfiore

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

H ii region electron temperatures are a critical ingredient in metallicity determinations, and recent observations have revealed systematic variations in the temperatures measured using different ions. We present electron temperatures (T e ) measured using the optical auroral lines ([N ii]λ5756, [O ii]λ λ7320, 7330, [S ii]λ λ4069, 4076, [O iii]λ4363, and [S iii]λ6312) for a sample of H ii regions in seven nearby galaxies. We use observations from the Physics at High Angular resolution in Nearby Galaxies survey (PHANGS) obtained with integral field spectrographs on Keck (Keck Cosmic Web Imager) and the Very Large Telescope (Multi-Unit Spectroscopic Explorer). We compare the different T e measurements with H ii region and ISM environmental properties such as electron density, ionization parameter, molecular gas velocity dispersion, and stellar association/cluster mass and age obtained from PHANGS. We find that the temperatures from [O ii] and [S ii] are likely overestimated due to the presence of electron density inhomogeneities in H ii regions. We measure high [O iii] temperatures in a subset of regions with high molecular gas velocity dispersion and low ionization parameter, which may be explained by the presence of low-velocity shocks. In agreement with previous studies, the T e–T e between [N ii] and [S iii] temperatures have the lowest observed scatter and follow predictions from photoionization modeling, which suggests that these tracers reflect H ii region temperatures across the various ionization zones better than [O ii], [S ii], and [O iii].

show abstract

Discovery of ~2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy

Li,

Kreckel,

Sarbadhicary

et al. 2024

A&A

View full text Add to dashboard Cite

Supernova feedback injects energy and turbulence into the interstellar medium (ISM) in galaxies, influences the process of star formation, and is essential to understanding the formation and evolution of galaxies. In this paper we present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants (SNRs) exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS--MUSE project, we identified SNRs in 19 nearby galaxies at sim 100 pc scales. We used five different optical diagnostics: (1) line ratio maps of S ii /Halpha ; (2) line ratio maps of O i /Halpha ; (3) velocity dispersion map of the gas; and (4) and (5) two line ratio diagnostic diagrams from Baldwin, Phillips Terlevich (BPT) diagrams to identify and distinguish SNRs from other nebulae. Given that our SNRs are seen in projection against H ii regions and diffuse ionized gas, in our line ratio maps we used a novel technique to search for objects with S ii /Halpha or O i /Halpha in excess of what is expected at fixed Halpha surface brightness within photoionized gas. In total, we identified 2,233 objects using at least one of our diagnostics, and defined a subsample of 1,166 high-confidence SNRs that were detected with at least two diagnostics. The line ratios of these SNRs agree well with the MAPPINGS shock models and we validate our technique using the well-studied nearby galaxy M83, where all the SNRs we found are also identified in literature catalogs, and we recovered 51<!PCT!> of the known SNRs. The remaining 1,067 objects in our sample were detected with only one diagnostic, and we classified them as SNR candidates. We find that sim 35<!PCT!> of all our objects overlap with the boundaries of H ii regions from literature catalogs, highlighting the importance of using indicators beyond line intensity morphology to select SNRs We find that the O i /Halpha line ratio is responsible for selecting the most objects (1,368; 61<!PCT!>); however, only half are classified as SNRs, demonstrating how the use of multiple diagnostics is key to increasing our sample size and improving our confidence in our SNR classifications.

show abstract

Atomic Data Assessment with PyNeb: Radiative and Electron Impact Excitation Rates for [Fe ii] and [Fe iii]

Cited by 6 publications

References 63 publications

Atomic Lifetimes of Astrophysical Interest in Ions of Fe

Atomic Lifetimes of Astrophysical Interest in Ions of Fe

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

Discovery of ~2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy

Contact Info

Product

Resources

About