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NGC 1333-SE DCO+ and H13CO+ datacubes
Electron fraction and cosmic-ray ionization rates in star-forming regions are important quantities in astrochemical modeling and are critical to the degree of coupling between... -
Molecular gas in AFGL 2298
We investigated the molecular environment of AFGL 2298, an obscured Galactic Luminous blue variable (LBV) star which hosts a highly structured circumstellar environment with... -
HL Tau SO2 14(0-14)-13(1,13) datacube
Planet-forming disks are not isolated systems. Their interaction with the surrounding medium affects their mass budget and chemical content. In the context of the ALMA-DOT... -
HCN and CN emission in Serpens Main region
Ultraviolet radiation (UV) influences the physics and chemistry of star-forming regions, but its properties and significance in the immediate surroundings of low-mass protostars... -
xCOLD GASS and xGASS. Metallicity gradients
The xGASS and xCOLD GASS surveys have measured the atomic (HI) and molecular gas (H_2_) content of a large and representative sample of nearby galaxies (redshift range of... -
Laboratory spectroscopy of isotopic c-H2C3O
Cyclopropenone was first detected in the cold and less dense envelope of the giant molecular cloud Sagittarius B2(N). It was found later in several cold dark clouds and it may... -
IRAS 04302+2247 CO, CS, CN, H2CO, CH3OH maps
The chemical composition of planets is inherited from that of the natal protoplanetary disk at the time of planet formation. Increasing observational evidence suggests that... -
Oxygen-rich AGB IRAM spectra
We aim to determine the abundances of SiO, CS, SiS, SO, and SO_2_ in a large sample of oxygen-rich asymptotic giant branch (AGB) envelopes covering a wide range of mass loss... -
Molecular Superbubbles in nearby galaxies
Star formation and stellar feedback are interlinked processes that redistribute energy, turbulence, and material throughout galaxies. Because young and massive stars form in... -
Molecular clouds from NOEMA CO(1-0) obs. in M82
We present a 154 pointing IRAM NOEMA mosaic of the CO(1-0) line emission in and around the nearby starburst galaxy M82. The observations, complemented by zero-spacing... -
Molecular ISM in nearby star-forming galaxies
We compare the observed turbulent pressure in molecular gas, P_turb_, to the required pressure for the interstellar gas to stay in equilibrium in the gravitational potential of... -
Splatalogue CASA LineTAP
This is a rendering of the CASA Offline Splatalogue_ in a draft LineTAP, mainly intended to enable verification of the standard. This is not recommended for production yet. In... -
VERTICO: the Virgo EnviRonment Traced In CO survey
We present the Virgo Environment Traced in CO (VERTICO) survey, a new effort to map ^12^CO(2-1), ^13^CO(2-1), and C^18^O(2-1) in 51 Virgo Cluster galaxies with the Atacama... -
Line lists for X^1^{Sigma}^+^ AlF and AlCl
Vibration-rotation line lists for AlF, Al^35^Cl, and Al^37^Cl have been prepared in their ground electronic states (X^1^{Sigma}^+^). Experimental rotational and ro-vibrational... -
Line lists for X^1^{Sigma}^+^ LiF and LiCl
Vibration-rotation line lists for ^6^LiF, ^7^LiF, ^6^Li^35^Cl, ^6^Li^37^Cl, ^7^Li^35^Cl, and ^7^Li^37^Cl in the X^1^{Sigma}^+^ ground states have been prepared. The... -
Improved A^3^{Pi}-X^3^{Sigma}^-^ transitions of OH+
Molecular ions are key reaction intermediates in the interstellar medium. OH+ plays a central role in the formation of more complex chemical species and for estimating the... -
Transition frequencies of ethanimine (CH_3_CHNH)
Ethanimine, a possible precursor of amino acids, is considered an important prebiotic molecule and thus may play important roles in the formation of biological building blocks... -
M51 ISM structures from the CO maps of PAWS
We compare the structure of molecular gas at 40pc resolution to the ability of gas to form stars across the disk of the spiral galaxy M51. We break the PdBI Arcsecond Whirlpool... -
History independent tracers
Molecular line emission is a powerful probe of the physical conditions of astrophysical objects but can be complex to model and it is often unclear which transitions would be...
