J. Kainulainen
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View article: Dust extinction map of the Galactic plane based on the UKIDSS survey data
Dust extinction map of the Galactic plane based on the UKIDSS survey data Open
Dust plays a critical role in the study of the interstellar medium. Extinction maps derived from optical surveys often fail to capture regions with high column density due to the limited photometric depth in optical wavelengths. To address…
View article: The width of Herschel filaments varies with distance (Corrigendum)
The width of Herschel filaments varies with distance (Corrigendum) Open
Corrigendum to "The width of Herschel filaments varies with distance."
View article: Volume densities and star formation in nearby molecular clouds
Volume densities and star formation in nearby molecular clouds Open
Context . Volume density is a key physical quantity that controls the evolution of the interstellar medium (ISM) and star formation, but it cannot be accessed directly by observations of molecular clouds. Aims . Our aim is to estimate the …
View article: Emergence of high-mass stars in complex fiber networks (EMERGE)
Emergence of high-mass stars in complex fiber networks (EMERGE) Open
Context . Identified as parsec-size, gas clumps at the junction of multiple filaments, hub-filament systems (HFS) play a crucial role during the formation of young clusters and high-mass stars. These HFS still appear to be detached from mo…
View article: On volume density and star formation in nearby molecular clouds
On volume density and star formation in nearby molecular clouds Open
Volume density is a key physical quantity controlling the evolution of the interstellar medium (ISM) and star formation, but it cannot be accessed directly by observations of molecular clouds. We aim at estimating the volume density distri…
View article: Emergence of high-mass stars in complex fiber networks (EMERGE) V. From filaments to spheroids: the origin of the hub-filament systems
Emergence of high-mass stars in complex fiber networks (EMERGE) V. From filaments to spheroids: the origin of the hub-filament systems Open
Identified as parsec-size, gas clumps at the junction of multiple filaments, hub-filament systems (HFS) play a crucial role during the formation of young clusters and high-mass stars. These HFS appear nevertheless to be detached from most …
View article: The associations between mathematical skills, cognitive performance, and language background in elementary school children. a two-year follow-up study
The associations between mathematical skills, cognitive performance, and language background in elementary school children. a two-year follow-up study Open
View article: Deep learning denoising by dimension reduction: Application to the ORION-B line cubes
Deep learning denoising by dimension reduction: Application to the ORION-B line cubes Open
Context. The availability of large bandwidth receivers for millimeter radio telescopes allows for the acquisition of position-position-frequency data cubes over a wide field of view and a broad frequency coverage. These cubes contain a lot…
View article: Mixture of noises and sampling of non-log-concave posterior distributions
Mixture of noises and sampling of non-log-concave posterior distributions Open
This work considers a challenging radio-astronomyinverse problem of physical parameter inference from multispec-tral observations. The forward model underlying this problem isa computationally expensive numerical simulation. In addition,th…
View article: The width of Herschel filaments varies with distance
The width of Herschel filaments varies with distance Open
Context. Filamentary structures in nearby molecular clouds have been found to exhibit a characteristic width of 0.1 pc, as observed in dust emission. Understanding the origin of this universal width has become a topic of central importance…
View article: Gas kinematics around filamentary structures in the Orion B cloud
Gas kinematics around filamentary structures in the Orion B cloud Open
Context. Understanding the initial properties of star-forming material and how they affect the star formation process is key. From an observational point of view, the feedback from young high-mass stars on future star formation properties …
View article: Gas kinematics around filamentary structures in the Orion B cloud
Gas kinematics around filamentary structures in the Orion B cloud Open
Understanding the initial properties of star-forming material and how they affect the star formation process is key. From an observational point of view, the feedback from young high-mass stars on future star formation properties is still …
View article: Dust extinction map of the Galactic plane based on the VVV survey data
Dust extinction map of the Galactic plane based on the VVV survey data Open
Dust extinction is one of the most reliable tracers of the gas distribution in the Milky Way. The near-infrared (NIR) Vista Variables in the Vía Láctea (VVV) survey enables extinction mapping based on stellar photometry over a large area i…
View article: Bird’s eye view of molecular clouds in the Milky Way
Bird’s eye view of molecular clouds in the Milky Way Open
Context . The kinematics of molecular gas are crucial for setting the stage for star formation. One key question related to the kinematic properties of gas is how they depend on the spatial scale. Aims . We aim to describe the CO spectra, …
View article: Mélange de bruits et échantillonnage de posterior non log-concave
Mélange de bruits et échantillonnage de posterior non log-concave Open
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View article: The width of <i>Herschel</i> filaments varies with distance <i>(Corrigendum)</i>
The width of <i>Herschel</i> filaments varies with distance <i>(Corrigendum)</i> Open
View article: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Three-dimensional Shape Explains Star Formation Mystery of California and Orion A Open
The new Gaia data release (EDR3) with improved astrometry has opened a new era in studying our Milky Way in fine detail. We use Gaia EDR3 astrometry together with 2MASS and WISE photometry to study two of the most massive molecular clouds …
View article: 3D shape explains star formation mystery of California and Orion A
3D shape explains star formation mystery of California and Orion A Open
The new Gaia data release (EDR3) with improved astrometry has opened a new era in studying our Milky Way in fine detail. We use Gaia EDR3 astrometry together with 2MASS and WISE photometry to study two of the most massive molecular clouds …
View article: Initial Conditions for Star Formation: A Physical Description of the Filamentary ISM
Initial Conditions for Star Formation: A Physical Description of the Filamentary ISM Open
The interstellar medium contains filamentary structure over a wide range of scales. Understanding the role of this structure, both as a conduit of gas across the scales and a diagnostic tool of local physics, is a major focus of star forma…
View article: The effect of viewing angle on the Kennicutt-Schmidt relation of the local molecular clouds
The effect of viewing angle on the Kennicutt-Schmidt relation of the local molecular clouds Open
The Gaia data give us an unprecedented view to the three-dimensional (3D) structure of molecular clouds in the solar neighbourhood. We study how the projected areas and masses of clouds, and consequently the Kennicutt-Schmidt (KS) relation…
View article: The width of <i>Herschel</i> filaments varies with distance
The width of <i>Herschel</i> filaments varies with distance Open
Context. Filamentary structures in nearby molecular clouds have been found to exhibit a characteristic width of 0.1 pc, as observed in dust emission. Understanding the origin of this universal width has become a topic of central importance…
View article: Revealing which Combinations of Molecular Lines are Sensitive to the Gas Physical Parameters of Molecular Clouds
Revealing which Combinations of Molecular Lines are Sensitive to the Gas Physical Parameters of Molecular Clouds Open
Atoms and molecules have long been thought to be versatile tracers of the cold neutral gas in the universe, from high-redshift galaxies to star forming regions and proto-planetary disks, because their internal degrees of freedom bear the s…
View article: Learning from model grids: Tracers of the ionization fraction in the ISM
Learning from model grids: Tracers of the ionization fraction in the ISM Open
The ionization fraction in neutral interstellar clouds is a key physical parameter controlling multiple physical and chemical processes, and varying by orders of magnitude from the UV irradiated surface of the cloud to its cosmic-ray domin…
View article: The width of Herschel filaments varies with distance
The width of Herschel filaments varies with distance Open
Context: Filamentary structures in nearby molecular clouds have been found to exhibit a characteristic width of 0.1 pc, as observed in dust emission. Understanding the origin of this universal width has become a topic of central importance…
View article: SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc
SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc Open
By combining two surveys covering a large fraction of the molecular material in the Galactic disc, we investigate the role spiral arms play in the star formation process. We have matched clumps identified by APEX Telescope Large Area Surve…
View article: The SEDIGISM survey: molecular clouds in the inner Galaxy
The SEDIGISM survey: molecular clouds in the inner Galaxy Open
We use the 13CO (2–1) emission from the SEDIGISM (Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium) high-resolution spectral-line survey of the inner Galaxy, to extract the molecular cloud population with a lar…
View article: The SEDIGISM survey: First Data Release and overview of the Galactic structure
The SEDIGISM survey: First Data Release and overview of the Galactic structure Open
The SEDIGISM (Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium) survey used the APEX telescope to map 84 deg2 of the Galactic plane between ℓ = −60° and +31° in several molecular transitions, including 13CO (2 –…
View article: Tracers of the ionization fraction in dense and translucent gas
Tracers of the ionization fraction in dense and translucent gas Open
Context. The ionization fraction in the neutral interstellar medium (ISM) plays a key role in the physics and chemistry of the ISM, from controlling the coupling of the gas to the magnetic field to allowing fast ion-neutral reactions that …
View article: Tracers of the ionization fraction in dense and translucent gas: I. Automated exploitation of massive astrochemical model grids
Tracers of the ionization fraction in dense and translucent gas: I. Automated exploitation of massive astrochemical model grids Open
The ionization fraction plays a key role in the physics and chemistry of the neutral interstellar medium, from controlling the coupling of the gas to the magnetic field to allowing fast ion-neutral reactions that drive interstellar chemist…
View article: C<sup>18</sup>O,<sup>13</sup>CO, and<sup>12</sup>CO abundances and excitation temperatures in the Orion B molecular cloud
C<sup>18</sup>O,<sup>13</sup>CO, and<sup>12</sup>CO abundances and excitation temperatures in the Orion B molecular cloud Open
Context. CO isotopologue transitions are routinely observed in molecular clouds for the purpose of probing the column density of the gas and the elemental ratios of carbon and oxygen, in addition to tracing the kinematics of the environmen…