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KiDS 1433 CO spectra
Brightest cluster galaxies (BCGs) at the centers of clusters are among the most massive galaxies in the Universe. Their star formation history and stellar mass assembly are... -
Orion B molecular cloud CO and HCO datacubes
Recent Herschel observations of nearby molecular clouds have shown that filamentary structures are ubiquitous and that most prestellar cores form in dense filaments. Probing the... -
VERTICO III. Virgo cluster galaxies
In this Virgo Environment Traced in CO (VERTICO) science paper, we aim to study how the star formation process depends on the galactic environment and gravitational interactions... -
CO in the ALMA Radio-source Catalogue (ARC)
To evaluate the role of radio activity in galaxy evolution, we designed a large archival CO survey of radio galaxies (RGs) to determine their molecular gas masses at different... -
3 KiDS cluster galaxies at z~0.4 CO spectra
Brightest Cluster Galaxies (BCGs) are typically massive ellipticals at the centers of clusters. They are believed to experience strong environmental processing, and their mass... -
ALMA data cubes for OH/IR stars
OH/IR stars are examples of late stellar evolution on the asymptotic giant branch (AGB), and they are, as such, important objects to study. They are also excellent probes of... -
LkH{alpha} 330 SPHERE/VLT and ALMA images
Planets that are forming around young stars are expected to leave clear imprints in the distribution of the gas and dust of their parental protoplanetary disks. In this paper,... -
FEEDBACK from the NGC7538 HII region
The interaction of expanding HII regions with their environmental cloud is one of the central questions driving the SOFIA legacy program FEEDBACK. We want to understand the... -
Self-absorption in RCW 120
Revealing the 3D dynamics of HII region bubbles and their associated molecular clouds and HI envelopes is important for developing an understanding of the longstanding problem... -
Post-common-envelope PN and mol. mass
Most planetary nebulae (PNe) show beautiful, axisymmetric morphologies despite their progenitor stars being essentially spherical. Close binarity is widely invoked to help eject... -
Q1700-MD94 CI(1-0) datacube with NOEMA
We use a combination of new NOrthern Extended Millimeter Array (NOEMA) observations of the pair of [CI] transitions, the CO(7-6) line, and the dust continuum, in addition to... -
Virgo Filaments. I. CO and HI data
It is now well established that galaxies have different morphology, gas content and star formation rate in dense environments like galaxy clusters. The impact of environmental... -
G305 Giant Molecular Cloud II. Clump properties
G305 star-forming complex was observed in the 3-2 lines of 12 & 13CO to investigate the effect of feedback from the central OB stars on the complex. The region was... -
OGHReS 12CO(2-1) data cubes
Filaments are a ubiquitous morphological feature of the molecular interstellar medium and are identified as sites of star formation. In recent years, more than 100 large-scale... -
Galactic CO maps
Carbon monoxide (CO) is the best tracer of Galactic molecular hydrogen H_2_. Its lowest rotational emission lines are in the radio regime, and thanks to Galactic rotation,... -
HD 142527 disk 13CO and C18O images
Vortices are one of the most promising mechanisms to locally concentrate millimeter dust grains and allow the formation of planetesimals through gravitational collapse. The... -
Protoplanetary nebulae and young PN CO spectra
Fast outflows and their interaction with slow shells (generally known as the fossil circumstellar envelope of asymptotic giant branch stars) play an important role in the... -
4 post-AGB stars datacubes
There is a class of binary post-AGB stars with a remarkable near-infrared excess that are surrounded by Keplerian or quasi-Keplerian disks and extended outflows composed of gas... -
12CO(2-1) datacubes of 3 IR sources
The Lupus star-forming complex includes some of the closest low-mass star-forming regions, and together they house objects that span evolutionary stages from pre-stellar to... -
J1717-3342 and J1744-3116 CO spectra
The chemistry of the diffuse interstellar medium is driven by the combined influences of cosmic rays, ultraviolet (UV) radiation, and turbulence. Previously detected at the...
