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CrI transition probabilities
Branching fraction measurements from Fourier transform spectra in conjunction with published radiative lifetimes are used to determine transition probabilities for 263 lines of... -
Photoionization of H in strong magnetic fields
A recently developed computational scheme, based on the complex-rotation method combined with a mixed Slater-Landau basis expansion, has been applied to calculations of... -
Eq. of State in Magnetic Neutron Stars
This catalog is based on the calculated equation of state in cold dense matter. Each table in the catalog lists bulk properties of Fe-56 in a magnetic field ranging from one... -
He-10830 triplet EW in young stars
Young exoplanets trace planetary evolution, in particular the atmospheric mass loss that is most dynamic in youth. However, the high activity level of young stars can mask or... -
O III recombination coefficients
We calculate effective recombination coefficients for the formation of the 5g-4f lines of O III in the intermediate coupling scheme. Photoionization data for the 5g levels... -
UMIST database. 1995
We report the release of a new version of the UMIST database for astrochemistry. The database contains the rate coefficients of 3864 gas-phase reactions important in... -
Sc II, Y II & Zr II Stark width
Here we present Stark widths for some astrophysically important ns-np transitions of Sc II, Y II and Zr II. Stark widths were calculated within the modified semiempirical... -
[Ni I] & [Ni II] transition probabilities
New radiative transition probabilities have been calculated for forbidden lines of astrophysical interest in Ni I and Ni II. The accuracy of the transition probability scales is... -
Polarization profiles of H lines
In this paper we provide extensive tables of the coefficients that are needed in the calculation of the second-order moments of the polarization profiles of hydrogen lines. We... -
Study of fine-structure constants
A statistical analysis of fine splitting of C IV, N V, O VI, Mg II, Al III and Si IV doublet absorption lines in quasar spectra is carried out in order to estimate a possible... -
Lines unaffected by polarization
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Solar beryllium abundance revisited
The present-day abundance of beryllium in the solar atmosphere provides clues about mixing mechanisms within stellar interiors. However, abundance determinations based on the... -
Line list for convective blueshift analysis
Stellar variability strongly impacts the search for low-mass exoplanets with radial velocity techniques. Two types of planet-free time series can be used to quantify this... -
M-star spectra FeH, CrH, and NiH line lists
Molecular bands of metal oxides and hydrides dominate the optical and near-infrared spectra of M dwarfs. High-resolution spectra of these bands have immense potential for... -
Effective collision strengths for Ni III
Recent JWST observations of the Type Ia supernova (SN Ia) 2021aefx in the nebular phase have paved the way for late-time studies covering the full optical to mid-infrared (MIR)... -
VPNEP. I. Initial data release
We embarked on a high-resolution optical spectroscopic survey of bright Transiting Exoplanet Survey Satellite (TESS) stars around the Northern Ecliptic Pole (NEP), dubbed the... -
2-hydroxyprop-2-enal millimetre-wave spectroscopy
Several sugar-like molecules have been found in the interstellar medium. The molecule studied in this work, 2-hydroxyprop- 2-enal, is among the candidates to be searched for, as... -
Metallicity trend and spread in GCs
The metallicity spread, or the metallicity trend along the evolutionary sequence of a globular cluster, is a rich source of information to help understand the cluster physics... -
Transitions of cysteamine analysis
Cysteamine (NH_2_CH_2_CH_2_SH), a molecule of potential astrobiological interest, has not yet been detected in the interstellar medium. Furthermore, the sulfur-substituted... -
Vanadium measurements for 135 M dwarfs
M-dwarf spectra are complex and notoriously difficult to model, posing challenges to understanding their photospheric properties and compositions in depth. Vanadium (V) is an...
