A. Men’shchikov
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View article: ALMA-IMF
ALMA-IMF Open
Context. The ALMA-IMF Large Program imaged 15 massive protoclusters down to a resolution of ~2 kau scales, identifying about 10 3 star-forming cores. The mass and luminosity of these cores, which are fundamental physical characteristics, a…
View article: Supplementary material of ALMA-IMF XVI (Motte et al. 2025)
Supplementary material of ALMA-IMF XVI (Motte et al. 2025) Open
Figure entitled "ALMA-IMF-XVI_FigureD3.png" displays the distribution of the mass-averaged dust temperature of prestellar cores located within luminosity peaks (orange histogram) and far away from them (green histogram), as indicated by th…
View article: ALMA-IMF
ALMA-IMF Open
The stellar initial mass function (IMF) is critical to our understanding of star formation and the effects of young stars on their environment. On large scales, it enables us to use tracers such as UV or Hα emission to estimate the star fo…
View article: ALMA-IMF XV: The core mass function in the high-mass star-formation regime
ALMA-IMF XV: The core mass function in the high-mass star-formation regime Open
The stellar initial mass function (IMF) is critical to our understanding of star formation and the effects of young stars on their environment. On large scales, it enables us to use tracers such as UV or Halpha emission to estimate the sta…
View article: ALMA-IMF XII: Point-process mapping of 15 massive protoclusters
ALMA-IMF XII: Point-process mapping of 15 massive protoclusters Open
A crucial aspect in addressing the challenge of measuring the core mass function, that is pivotal for comprehending the origin of the initial mass function, lies in constraining the temperatures of the cores. We aim to measure the luminosi…
View article: Probing the filamentary nature of star formation in the California giant molecular cloud
Probing the filamentary nature of star formation in the California giant molecular cloud Open
Context. Recent studies suggest that filamentary structures are representative of the initial conditions of star formation in molecular clouds and support a filament paradigm for star formation, potentially accounting for the origin of the…
View article: <i>Herschel</i> Gould Belt Survey in Taurus – II. A census of dense cores and filaments in the TMC1 region
<i>Herschel</i> Gould Belt Survey in Taurus – II. A census of dense cores and filaments in the TMC1 region Open
We present a catalogue of dense cores and filaments in a $3.8^\circ \times 2.4^\circ$ field around the TMC1 region of the Taurus molecular cloud. The catalogue was created using photometric data from the Herschel SPIRE and PACS instruments…
View article: Herschel Gould Belt Survey in Taurus. II: A census of dense cores and filaments in the TMC1 region
Herschel Gould Belt Survey in Taurus. II: A census of dense cores and filaments in the TMC1 region Open
We present a catalogue of dense cores and filaments in a $3.8^{\circ}\times2.4^{\circ}$ field around the TMC1 region of the Taurus Molecular Cloud. The catalogue was created using photometric data from the Herschel SPIRE and PACS instrumen…
View article: ALMA-IMF
ALMA-IMF Open
Context . A crucial aspect in addressing the challenge of measuring the core mass function (CMF), that is pivotal for comprehending the origin of the initial mass function (IMF), lies in constraining the temperatures of the cores. Aims . W…
View article: ALMA-IMF
ALMA-IMF Open
Context. One of the central questions in astrophysics is the origin of the initial mass function (IMF). It is intrinsically linked to the processes from which it originates, and hence its connection with the core mass function (CMF) must b…
View article: ALMA-IMF X -- The core population in the evolved W33-Main (G012.80) protocluster
ALMA-IMF X -- The core population in the evolved W33-Main (G012.80) protocluster Open
We aimed to measure the CMF in the evolved W33-Main star-forming protocluster to compare it with CMF recently obtained in other Galactic star-forming regions, including the ones included in the ALMA-IMF program. We used observations from t…
View article: Inaccuracies and biases of the Gaussian size deconvolution for extracted sources and filaments
Inaccuracies and biases of the Gaussian size deconvolution for extracted sources and filaments Open
A simple Gaussian size deconvolution method is routinely used to remove the blur of observed images caused by insufficient angular resolutions of existing telescopes, thereby to estimate the physical sizes of extracted sources and filament…
View article: Inaccuracies and biases of the Gaussian size deconvolution for extracted sources and filaments
Inaccuracies and biases of the Gaussian size deconvolution for extracted sources and filaments Open
A simple Gaussian size deconvolution method is routinely used to remove the blur of observed images caused by insufficient angular resolutions of existing telescopes, thereby to estimate the physical sizes of extracted sources and filament…
View article: Properties of the dense cores and filamentary structures in the Vela C molecular cloud
Properties of the dense cores and filamentary structures in the Vela C molecular cloud Open
The initial and boundary conditions of the Galactic star formation in molecular clouds are not well understood. In an effort to shed new light on this long-standing problem, we measured the properties of dense cores and filamentary structu…
View article: Properties of the dense cores and filamentary structures in the Vela C molecular cloud
Properties of the dense cores and filamentary structures in the Vela C molecular cloud Open
The initial and boundary conditions of the Galactic star formation in molecular clouds are not well understood. In an effort to shed new light on this long-standing problem, we measured properties of dense cores and filamentary structures …
View article: IC 5146 Dark Streamer: The First Reliable Candidate of Edge Collapse, Hub-filament Systems, and Intertwined Sub-filaments
IC 5146 Dark Streamer: The First Reliable Candidate of Edge Collapse, Hub-filament Systems, and Intertwined Sub-filaments Open
The paper presents an analysis of multiwavelength data of a nearby star-forming site, the IC 5146 dark streamer ( d ∼ 600 pc), which has been treated as a single and long filament, fl . Two hub-filament systems (HFSs) are known to exist to…
View article: ALMA-IMF
ALMA-IMF Open
Context. Among the most central open questions regarding the initial mass function (IMF) of stars is the impact of environment on the shape of the core mass function (CMF) and thus potentially on the IMF. Aims. The ALMA-IMF Large Program a…
View article: ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst
ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst Open
Among the most central open questions regarding the initial mass function (IMF) of stars is the impact of environment on the shape of the core mass function (CMF) and thus potentially on the IMF. The ALMA-IMF Large Program aims to investig…
View article: ALMA-IMF
ALMA-IMF Open
Aims. The processes that determine the stellar initial mass function (IMF) and its origin are critical unsolved problems, with profound implications for many areas of astrophysics. The W43-MM2&MM3 mini-starburst ridge hosts a rich young pr…
View article: Velocity structure of the 50 pc long NGC 6334 filamentary cloud
Velocity structure of the 50 pc long NGC 6334 filamentary cloud Open
Context. The interstellar medium is observed to be organized in filamentary structures, and in neutral (H I ) and ionized (H II ) bubbles. The expanding nature of these bubbles shapes the surrounding medium and possibly plays a role in the…
View article: ALMA-IMF. III. Investigating the origin of stellar masses: top-heavy core mass function in the W43-MM2&MM3 mini-starburst
ALMA-IMF. III. Investigating the origin of stellar masses: top-heavy core mass function in the W43-MM2&MM3 mini-starburst Open
International audience
View article: Filament coalescence and hub structure in Mon R2
Filament coalescence and hub structure in Mon R2 Open
There is growing evidence of the role of hub-filament systems (HFS) in the formation of stars from low to high masses. As of today, however, the detailed structures of these systems are still not well described. Here we study the Mon R2 st…
View article: ALMA-IMF
ALMA-IMF Open
Aims. Thanks to the high angular resolution, sensitivity, image fidelity, and frequency coverage of ALMA, we aim to improve our understanding of star formation. One of the breakthroughs expected from ALMA, which is the basis of our Cycle 5…
View article: ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results Open
The ALMA-IMF Large Program imaged a total noncontiguous area of 53pc2, covering 15 extreme, nearby protoclusters of the Milky Way. They were selected to span relevant early protocluster evolutionary stages. Our 1.3mm and 3mm observations p…
View article: Filament coalescence and hub structure in MonR2: Implications to massive star and cluster formation
Filament coalescence and hub structure in MonR2: Implications to massive star and cluster formation Open
Here we study the MonR2 star forming region, which has a rich network of filaments joining in a star cluster forming hub, aiming at understanding the hub structure and to examine the mass fraction residing in the hub and in the filaments, …
View article: ALMA-IMF
ALMA-IMF Open
We present the first data release of the ALMA-IMF Large Program, which covers the 12m-array continuum calibration and imaging. The ALMA-IMF Large Program is a survey of fifteen dense molecular cloud regions spanning a range of evolutionary…
View article: Multicomponent, multiwavelength benchmarks for source- and filament-extraction methods
Multicomponent, multiwavelength benchmarks for source- and filament-extraction methods Open
Modern multiwavelength observations of star-forming regions that reveal complex, highly structured molecular clouds require adequate extraction methods that provide both complete detection of the structures and their accurate measurements.…
View article: Multicomponent, multiwavelength benchmarks for source- and filament-extraction methods
Multicomponent, multiwavelength benchmarks for source- and filament-extraction methods Open
Modern multiwavelength observations of star-forming regions that reveal highly structured molecular clouds require adequate extraction methods that provide both detection of the structures and their accurate measurements. The omnipresence …
View article: Strong dependence of the physical properties of cores on spatial resolution in observations and simulations
Strong dependence of the physical properties of cores on spatial resolution in observations and simulations Open
The angular resolution of a telescope is the primary observational parameter, along with the detector sensitivity in defining the quality of the observed images and of the subsequent scientific exploitation of the data. During the last dec…
View article: Multiscale, multiwavelength extraction of sources and filaments using separation of the structural components:<i>getsf</i>
Multiscale, multiwavelength extraction of sources and filaments using separation of the structural components:<i>getsf</i> Open
High-quality astronomical images delivered by modern ground-based and space observatories demand adequate, reliable software for their analysis and accurate extraction of sources, filaments, and other structures, containing massive amounts…