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Introduction
Publications
Publications (131)
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 star formation rate of a system and interpret unresolved star clusters across the Universe. So far, there is littl...
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 star formation rate of a system and interpret unresolved star clusters across the universe. So far, there is littl...
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 luminosity, mass, column density and dust temperature of star-forming regions imaged by the ALMA-IMF large program. Hig...
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 . We aim to measure the luminosity, mass, column density and dust temperature of star-forming regions imaged by th...
We present N-PDFs of 29 Galactic regions obtained from Herschel imaging at high angular resolution, covering diffuse and quiescent clouds, and those showing low-, intermediate-, and high-mass star formation (SF), and characterize the cloud structure using the Delta-variance tool. The N-PDFs are double-log-normal at low column densities, and display...
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 decade in star formation research, many studies have targeted low- and high-mass star formation regions located at...
During the last decade in star formation research, many studies have targeted low- and high-mass star formation regions located at different distances, with different telescopes having specific angular resolution capabilities. We present a systematic investigation of the angular resolution effects, with special attention being paid to the derived m...
Context: The mass segregation of stellar clusters could be primordial rather than dynamical. Despite the abundance of studies of mass segregation for stellar clusters, those for stellar progenitors are still scarce, so the question concerning the origin and evolution of mass segregation is still open. Aims: Our goal is to characterize the structure...
Context. The mass segregation of stellar clusters could be primordial rather than dynamical. Despite the abundance of studies of mass segregation for stellar clusters, those for stellar progenitors are still scarce, so the question concerning the origin and evolution of mass segregation is still open.
Aims. Our goal is to characterize the structure...
The mass segregation of stellar clusters could be primordial rather than dynamical. Despite the abundance of studies of mass segregation for stellar clusters, those for stellar progenitors are still scarce, so the question on the origin and evolution of mass segregation is still open. Our goal is to characterize the structure of the NGC 2264 molecu...
We report the first map of large-scale (10 pc in length) emission of millimeter-wavelength hydrogen recombination lines (mm-RRLs) toward the giant H II region around the W43-Main young massive star cluster (YMC). Our mm-RRL data come from the IRAM 30 m telescope and are analyzed together with radio continuum and cm-RRL data from the Karl G. Jansky...
The mass growth of protostars is a central element to the determination of fundamental stellar population properties such as the initial mass function. Constraining the accretion history of individual protostars is therefore an important aspect of star formation research. The goal of the study presented here is to determine whether high-mass (proto...
The mass growth of protostars is a central element to the determination of fundamental stellar population properties such as the initial mass function. Constraining the accretion history of individual protostars is therefore an important aspect of star formation research. The goal of the study presented here is to determine whether high-mass (proto...
Aims. It has been proposed that the magnetic field, which is pervasive in the interstellar medium, plays an important role in the process of massive star formation. To better understand the impact of the magnetic field at the pre- and protostellar stages, high-angular resolution observations of polarized dust emission toward a large sample of massi...
It has been proposed that the magnetic field, pervasive in the ISM, plays an important role in the process of massive star formation. To better understand its impact at the pre and protostellar stages, high-angular resolution observations of polarized dust emission toward a large sample of massive dense cores are needed. To this end, we used the At...
This table presents the properties of each of 203 compact ArTeMiS sources identified in the images analysed in the paper. These sources have been identified across 5 fields: SDC326, SDC328, SDC340, SDC343, SDC345. \\\\(1 data file).
We present a detailed study of the Orion B molecular cloud complex ( d ~ 400 pc), which was imaged with the PACS and SPIRE photometric cameras at wavelengths from 70 to 500 μ m as part of the Herschel Gould Belt survey (HGBS). We release new high-resolution maps of column density and dust temperature for the whole complex, derived in the same consi...
We present a detailed study of the Orion B clouds (d~400 pc), imaged with the PACS/SPIRE cameras at 70-500 $\mu$m by the Herschel Gould Belt survey (HGBS). We release new high-res. maps of column density and dust temperature. In the filamentary sub-regions NGC2023/2024, NGC2068/2071, and L1622, 1768 starless dense cores were identified, ~28-45% of...
Context. High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest of these systems, making it an excellent target for case studies.
Aims. We investigate the morphology, stability and dynamical properties of the Mon R2 hub-filament system.
Method...
High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2, harbors one of the closest such systems, making it an excellent target for case studies. We investigate the morphology, stability and dynamical properties of the hub-filament system on basis of 13CO and C18O observations obtained with the IRAM-30m telescope a...
Fluxes and information for the 23 massive dense cores (MDCs) found in NGC 6357. Information for 155 reliable sources. \\\\(4 data files).
Context. Molecular filaments have received special attention recently thanks to new observational results on their properties. In particular, our early analysis of filament properties from Herschel imaging data in three nearby molecular clouds revealed a narrow distribution of median inner widths centered at a characteristic value of about 0.1 pc....
[Abridged] Molecular filaments have received special attention recently, thanks to new observational results on their properties. In particular, our early analysis of filament properties revealed a narrow distribution of median widths centered at a value of about 0.1 pc. Here, we extend and complement our initial study with the analysis of the fila...
Understanding the processes that determine the stellar Initial Mass Function (IMF) is a critical unsolved problem, with profound implications for many areas of astrophysics. In molecular clouds, stars are formed in cores, gas condensations which are sufficiently dense that gravitational collapse converts a large fraction of their mass into a star o...
We report the first map of large-scale (10 pc in length) emission of millimeter-wavelength hydrogen recombination lines (mm-RRLs) toward the giant H ii region around the W43-Main young massive star cluster (YMC). Our mm-RRL data come from the IRAM 30 m telescope and are analyzed together with radio continuum and cm-RRL data from the Karl G. Jansky...
The characterization of dust properties in the interstellar medium (ISM) is key for star formation. Mass estimates are crucial to determine gravitational collapse conditions for the birth of new stellar objects in molecular clouds. However, most of these estimates rely on dust models that need further observational constraints from clouds to preste...
Aims. To constrain models of high-mass star formation, the Herschel -HOBYS key program aims at discovering massive dense cores (MDCs) able to host the high-mass analogs of low-mass prestellar cores, which have been searched for over the past decade. We here focus on NGC 6334, one of the best-studied HOBYS molecular cloud complexes.
Methods. We used...
The scaling relations and star formation laws for molecular cloud complexes (MCCs) in the Milky Way are investigated. MCCs are mostly large (R > 50 pc), massive (~106 ) gravitationally unbound cloud structures. We compare their masses , mass surface densities , radii R, velocity dispersions σ, star formation rates (SFRs), and SFR densities with tho...
Herschel has shown that filamentary structures are ubiquitous in star-forming regions, in particular in nearby molecular clouds associated with Gould's Belt. High dynamic range far-infrared imaging of the Musca cloud with SPIRE and PACS reveals at least two types of filamentary structures: (1) the main ∼10-pc scale high column-density linear filame...
Diffuse Galactic light (DGL) has been observed in the optical since the 1930s. We propose that, when observed in the optical with deep imaging surveys, it can be used as a tracer of the turbulent cascade in the diffuse interstellar medium, down to scales of about 1 arcsec. Here we present a power spectrum analysis of the dust column density of a di...
To link the physical and star formation properties of structures ranging from Giant Molecular Clouds (GMCs), to Molecular Cloud Complexes (MCCs), and to Galaxies, we compare the mutual relations between their masses $M$, mass surface densities $\Sigma_{M_{\rm gas}}$, radii $R$, velocity dispersions $\sigma$, star formation rates $SFR$, and SFR dens...
The radiative feedback of massive stars on molecular clouds creates pillars, globules and other features at the interface between the HII region and molecular cloud. We present here Herschel observations between 70 and 500 micron of the immediate environment of the Cygnus OB2 association, performed within the HOBYS program. All structures were dete...
The surroundings of HII regions can have a profound influence on their development, morphology, and evolution. This paper explores the effect of the environment on H II regions in the MonR2 molecular cloud. We aim to investigate the density structure of envelopes surrounding HII regions and to determine their collapse and ionisation expansion ages....
We report the novel detection of complex high-column density tails in the
probability distribution functions (PDFs) for three high-mass star-forming
regions (CepOB3, MonR2, NGC6334), obtained from dust emission observed with
Herschel. The low column density range can be fit with a lognormal
distribution. A first power-law tail starts above an extin...
We present and discuss the results of the Herschel Gould Belt survey (HGBS) observations in an ∼11 deg2 area of the Aquila molecular cloud complex at d ∼ 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from 70 μm to 500 μm. Using the multi-scale, multi-wavelength source extraction algorithm getsources, we identify a comp...
We present and discuss the results of the Herschel Gould Belt survey
observations in a ~11 deg^2 area of the Aquila molecular cloud complex at d~260
pc, imaged with the SPIRE/PACS cameras from 70 to 500 micron. We identify a
complete sample of starless dense cores and embedded protostars in this region,
and analyze their global properties and spati...
The surroundings of HII regions can have a profound influence on their
development, morphology, and evolution. This paper explores the effect of the
environment on H II regions in the MonR2 molecular cloud. We aim to investigate
the density structure of envelopes surrounding HII regions and to determine
their collapse and ionisation expansion ages....
This work aims at improving the current understanding of the interaction
between H ii regions and turbulent molecular clouds. We propose a new method to
determine the age of a large sample of OB associations by investigating the
development of their associated H ii regions in the surrounding turbulent
medium. Using analytical solutions, one-dimensi...
The Chamaeleon molecular cloud complex is one of the nearest star-forming
sites encompassing three molecular clouds with a different star-formation
history, from quiescent (Cha III) to actively forming stars (Cha II), and
reaching the end of star-formation (Cha I). To charactize its large-scale
structure, we derived column density and temperature m...
Numerical simulations have explored the possibility to form molecular clouds
through either a quasi-static, self-gravitating mechanism or the collision of
gas streams or lower-density clouds. They also quantitatively predict the
distribution of matter at the transition from atomic to molecular gases. We aim
to observationally test these models by s...
We present the results of Herschel HOBYS (Herschel imaging survey of OB Young Stellar objects) photometric mapping combined with Berkeley Illinois Maryland Association (BIMA)
observations and additional archival data, and perform an in-depth study of the evolutionary phases of the star-forming clumps
in W 48A and their surroundings. Age estimates f...
Ionization feedback should impact the probability distribution function (PDF)
of the column density around the ionized gas. We aim to quantify this effect
and discuss its potential link to the Core and Initial Mass Function (CMF/IMF).
We used in a systematic way Herschel column density maps of several regions
observed within the HOBYS key program:...
Pillars and globules are present in many high-mass star-forming regions, such
as the Eagle nebula (M16) and the Rosette molecular cloud, and understanding
their origin will help characterize triggered star formation. The formation
mechanisms of these structures are still being debated. Recent numerical
simulations have shown how pillars can arise f...
Aims. Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods....
A key parameter to the description of all star formation processes is the density structure of the gas. In this Letter, we make use of probability distribution functions (PDFs) of Herschel column density maps of Orion B, Aquila, and Polaris, obtained with the Herschel Gould Belt survey (HGBS). We aim to understand which physical processes influence...
Context. Ionising stars reshape their original molecular cloud and
impact star formation, leading to spectacular morphologies such as
bipolar nebulae around H ii regions. Molecular clouds are structured in
filaments where stars principally form, as revealed by the Herschel
space observatory. The prominent southern hemisphere H ii region, RCW
36, is...
We present APEX/P-ArT\'eMiS 450\mu m continuum observations of RCW 36 and the
adjacent ridge, a high-mass high-column density filamentary structure at the
centre of the Vela C molecular cloud. These observations, at higher resolution
than Herschel's SPIRE camera, reveal clear fragmentation of the central
star-forming ridge. Combined with PACS far-i...
With its unprecedented spatial resolution and high sensitivity in the
far-infrared to submillimetre regime, {Herschel} is revolutionizing our
understanding of star formation. The HOBYS key program is an {Herschel}
mapping survey dedicated to the formation of OB-type stars (Motte,
Zavagno, Bontemps et al. 2010; see {http://hobys-herschel.cea.fr}. HO...
We present first results from the Herschel Gould Belt survey for the
B211/L1495 region in the Taurus molecular cloud. Thanks to their high
sensitivity and dynamic range, the Herschel images reveal the structure of the
dense, star-forming filament B211 with unprecedented detail, along with the
presence of striations perpendicular to the filament and...
In order to characterise the cloud structures responsible for the formation
of high-mass stars, we present Herschel observations of the DR21 environment.
Maps of the column density and dust temperature unveil the structure of the
DR21 ridge and several connected filaments. The ridge has column densities
larger than 1e23/cm^2 over a region of 2.3 pc...
We present Herschel images from the HOBYS key program of the Eagle Nebula (M 16) in the far-infrared and sub-millimetre, using the PACS and SPIRE cameras at 70 mu m, 160 mu m, 250 mu m, 350 mu m, 500 mu m. M 16, home to the Pillars of Creation, is largely under the influence of the nearby NGC 6611 high-mass star cluster. The Herschel images reveal...
We present Herschel images from the HOBYS key program of the Eagle Nebula
(M16) in the far-infrared and sub-millimetre, using the PACS and SPIRE cameras
at 70{\mu}m, 160{\mu}m, 250{\mu}m, 350{\mu}m, 500{\mu}m. M16, home to the
Pillars of Creation, is largely under the influence of the nearby NGC6611
high-mass star cluster. The Herschel images revea...
We present a multi-scale, multi-wavelength source extraction algorithm called
getsources. Although it has been designed primarily for use in the far-infrared
surveys of Galactic star-forming regions with Herschel, the method can be
applied to many other astronomical images. Instead of the traditional approach
of extracting sources in the observed i...
For many years feedback processes generated by OB-stars in molecular clouds,
including expanding ionization fronts, stellar winds, or UV-radiation, have
been proposed to trigger subsequent star formation. However, hydrodynamic
models including radiation and gravity show that UV-illumination has little or
no impact on the global dynamical evolution...
A growing body of evidence indicates that the formation of filaments in
interstellar clouds is a key component of the star formation process. In this
paper, we present new Herschel PACS and SPIRE observations of the B59 and Stem
regions in the Pipe Nebula complex, revealing a rich, organized network of
filaments. The asymmetric column density profi...
Herschel observations of molecular clouds reveal the presence of
complex filamentary structures which are shown to be the main sites of
core and protostar formation (André et al. 2010). Understanding
the properties of these filaments is a first step toward establishing
a broader scenario of star formation in the Galaxy. Thanks to their
unprecedente...
The Herschel Space Observatory provides a unique opportunity to improve
our global understanding of the earliest phases of star formation. I
will present an overview of the first results from the Gould Belt
survey, one of the largest key projects with Herschel. The immediate
objective of this imaging survey of nearby clouds is to obtain complete
s...
With its unprecedented spatial resolution and high sensitivity, Herschel
is revolutionising our understanding of high mass star formation and the
interstellar medium (ISM). In particular, Herschel is unveiling the
filamentary structure and molecular cloud constituents of the ISM where
star formation takes place. The Herschel Imaging Survey of OB Yo...
We present recent results from the Herschel HOBYS guaranteed time key program
of the Vela C andW48 star-forming complexes. We examine the column density
distribution in Vela C, in particular focusing on the cloud structure using
probability distribution functions, and characterise the star formation
efficiency in W48.
The filament IRDC G035.39--00.33 in the W48 molecular complex is one of the
darkest infrared clouds observed by \textit{Spitzer}. It has been observed by
the PACS (70 and 160\,$\micron$) and SPIRE (250, 350, and 500\,$\micron$)
cameras of the \textit{Herschel} Space Observatory as part of the W48 molecular
cloud complex in the framework of the HOBY...
