Atomic and molecular data for optical stellar spectroscopy

Heiter, U.; Lind, Karin; Asplund, Martin; Barklem, P. S.; Bergemann, M.; Magrini, L.; Masseron, T.; Mikolaitis, Š.; Pickering, Juliet C.; Ruffoni, M. P.

doi:10.1088/0031-8949/90/5/054010

Cited by 155 publications

(164 citation statements)

References 27 publications

Supporting

Mentioning

161

Contrasting

Order By: Relevance

“…3.3.3 and 3.3.5, respectively), as described below. From the lines of the GES v4 line list (Heiter et al 2015b), we rejected all those lines whose flag related to the atomic data quality was "N" (meaning that the transition probabilities are expected to have low accuracy and that the usage of these lines is not recommended). However, we allowed for lines for which the synthesis profile in the Sun and Arcturus were Notes.…”

Section: Line Listmentioning

confidence: 99%

“…For details of such flags, see Heiter et al (2015b). In this article we focused on the ten α and iron-peak elements that have at least 12 spectral lines.…”

Section: Line Listmentioning

confidence: 99%

“…The atomic data were taken from the fourth version of the line list created for the Gaia-ESO survey (Heiter et al 2015b). Likewise, the atmospheric models are those employed by the analysis of the spectra in the Gaia-ESO survey.…”

Section: Atomic Data and Atmospheric Modelsmentioning

confidence: 99%

See 2 more Smart Citations

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

Jofré

Heiter

Soubiran

et al. 2015

A&A

137

View full text Add to dashboard Cite

Context. In the current era of large spectroscopic surveys of the Milky Way, reference stars for calibrating astrophysical parameters and chemical abundances are of paramount importance. Aims. We determine elemental abundances of Mg, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni for our predefined set of Gaia FGK benchmark stars. Methods. By analysing high-resolution spectra with a high signal-to-noise ratio taken from several archive datasets, we combined results of eight different methods to determine abundances on a line-by-line basis. We performed a detailed homogeneous analysis of the systematic uncertainties, such as differential versus absolute abundance analysis. We also assessed errors that are due to non-local thermal equilibrium and the stellar parameters in our final abundances. Results. Our results are provided by listing final abundances and the different sources of uncertainties, as well as line-by-line and method-by-method abundances. Conclusions. The atmospheric parameters of the Gaia FGK benchmark stars are already being widely used for calibration of several pipelines that are applied to different surveys. With the added reference abundances of ten elements, this set is very suitable for calibrating the chemical abundances obtained by these pipelines.

show abstract

Section: Line Listmentioning

confidence: 99%

“…For details of such flags, see Heiter et al (2015b). In this article we focused on the ten α and iron-peak elements that have at least 12 spectral lines.…”

Section: Line Listmentioning

confidence: 99%

See 1 more Smart Citation

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

Jofré

Heiter

Soubiran

et al. 2015

A&A

137

View full text Add to dashboard Cite

show abstract

“…The compilation of accurate atomic line lists for large scale homogeneous quality assessments and stellar surveys, such as BRASS, the European space agency Gaia survey (Gaia collaboration 2016), and abundances of the APOGEE/Kepler sample (Hawkins et al 2016), is an arduous task and requires robust merging of data from multiple sources (Heiter et al 2015). Given the far-reaching impact of large surveys any errors in line lists or uncertainties can easily propagate throughout the field and so it is of the utmost importance that line lists are built as accurately as possible.…”

Section: Introductionmentioning

confidence: 99%

The Belgian repository of fundamental atomic data and stellar spectra (BRASS)

Laverick

Lobel

Merle

et al. 2018

A&A

View full text Add to dashboard Cite

Context. Fundamental atomic parameters, such as oscillator strengths, play a key role in modelling and understanding the chemical composition of stars in the universe. Despite the significant work underway to produce these parameters for many astrophysically important ions, uncertainties in these parameters remain large and can propagate throughout the entire field of astronomy. Aims. The Belgian repository of fundamental atomic data and stellar spectra (BRASS) aims to provide the largest systematic and homogeneous quality assessment of atomic data to date in terms of wavelength, atomic and stellar parameter coverage. To prepare for it, we first compiled multiple literature occurrences of many individual atomic transitions, from several atomic databases of astrophysical interest, and assessed their agreement. In a second step synthetic spectra will be compared against extremely highquality observed spectra, for a large number of BAFGK spectral type stars, in order to critically evaluate the atomic data of a large number of important stellar lines. Methods. Several atomic repositories were searched and their data retrieved and formatted in a consistent manner. Data entries from all repositories were cross-matched against our initial BRASS atomic line list to find multiple occurrences of the same transition. Where possible we used a new non-parametric cross-match depending only on electronic configurations and total angular momentum values. We also checked for duplicate entries of the same physical transition, within each retrieved repository, using the non-parametric cross-match. Results. We report on the number of cross-matched transitions for each repository and compare their fundamental atomic parameters. We find differences in log(g f ) values of up to 2 dex or more. We also find and report that ∼2% of our line list and Vienna Atomic Line Database retrievals are composed of duplicate transitions. Finally we provide a number of examples of atomic spectral lines with different retrieved literature log(g f ) values, and discuss the impact of these uncertain log(g f ) values on quantitative spectroscopy. All cross-matched atomic data and duplicate transition pairs are available to download at brass.sdf.org.

show abstract

“…However, the quantity and quality of the existing data lies far from the current needs of the astronomical community, remaining the Achilles' heel of the field of Galactic archeology (Bigot & Thévenin 2006). Several attempts have been made to assemble comprehensive line lists with reliable atomic data (Heiter et al 2015b) that can be used as a standard input for the different local thermodynamic equilibrium (LTE) and non-LTE models used to determine chemical abundances.…”

Section: Introductionmentioning

confidence: 99%

Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

Belmonte

Pickering

Ruffoni

et al. 2017

ApJ

View full text Add to dashboard Cite

We report new experimental Fe I oscillator strengths obtained by combining measurements of branching fractions measured with a Fourier Transform spectrometer and time-resolved, laser-induced fluorescence lifetimes. This study covers the spectral region ranging from 213 to 1033 nm. A total of 120 experimental ( ) gf log -values coming from 15 odd-parity energy levels are provided, 22 of which have not been reported previously and 63 of which have values with lower uncertainty than the existing data. The radiative lifetimes for 60 upper energy levels are presented, 39 of which have no previous measurements.

show abstract

Atomic and molecular data for optical stellar spectroscopy

Cited by 155 publications

References 27 publications

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

The Belgian repository of fundamental atomic data and stellar spectra (BRASS)

Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

Contact Info

Product

Resources

About