P. André

Paul Scherrer Institute

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T. Montmerle

Institut d'Astrophysique de Paris

F. Motte

Institut de Planétologie et d'Astrophysique de Grenoble

A. Abergel

Institut d'Astrophysique Spatiale

P. Persi

National Institute for Astrophysics

Sylvain Bontemps

Laboratoire d'Astrophysique de Bordeaux

G. Olofsson

AlbaNova

M. Casali

Macquarie University

M. Pérault

Laboratoire de Physique de l'ENS

J.‐L. Puget

Institut d'Astrophysique Spatiale

D. Ward–Thompson

University of Central Lancashire

Cooperative Institutions

Centre National de la Recherche Scientifique

Université Paris Cité

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

CEA Paris-Saclay

Astrophysique, Instrumentation et Modélisation

Université Paris-Saclay

Délégation Paris 7

Max Planck Society

Institut de Planétologie et d'Astrophysique de Grenoble

National Institute for Astrophysics

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Submillimetre and Infrared Observations of Prestellar Cores

American Astronomical Society Meeting Abstracts #202 (2003)

J. M. Kirk D. Ward–Thompson P. André

Cosmic infrared background

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Citations (1)

Dust observations of the initial conditions of star formation

P. André A. Bacmann F. Motte D. Ward–Thompson

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VizieR Online Data Catalog: 4 molecular clouds SPIRE 250um maps (Schneider+, 2015)

HAL (Le Centre pour la Communication Scientifique Directe) (2015)

N. Schneider V. Ossenkopf T. Csengeri Ralf S. Klessen Christoph Federrath

Spire (mollusc)

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TheHerschelview of the on-going star formation in the Vela-C molecular cloud

Astronomy and Astrophysics (2012)

T. Giannini D. Elia D. Lorenzetti S. Molinari F. Motte

As part of the Herschel guaranteed time key program 'HOBYS', we present the photometric survey of the star forming region Vela-C, one of the nearest sites of low-to-high-mass star formation in the Galactic plane. Vela-C has been observed with PACS and SPIRE in parallel mode between 70 um and 500 um over an area of about 3 square degrees. A photometric catalogue has been extracted from the detections in each band, using a threshold of 5 sigma over the local background. Out of this catalogue we have selected a robust sub-sample of 268 sources, of which 75% are cloud clumps and 25% are cores. Their Spectral Energy Distributions (SEDs) have been fitted with a modified black body function. We classify 48 sources as protostellar and 218 as starless. For two further sources, we do not provide a secure classification, but suggest they are Class 0 protostars. From SED fitting we have derived key physical parameters. Protostellar sources are in general warmer and more compact than starless sources. Both these evidences can be ascribed to the presence of an internal source(s) of moderate heating, which also causes a temperature gradient and hence a more peaked intensity distribution. Moreover, the reduced dimensions of protostellar sources may indicate that they will not fragment further. A virial analysis of the starless sources gives an upper limit of 90% for the sources gravitationally bound and therefore prestellar. We fit a power law N(logM) prop M^-1.1 to the linear portion of the mass distribution of prestellar sources. This is in between that typical of CO clumps and those of cores in nearby star-forming regions. We interpret this as a result of the inhomogeneity of our sample, which is composed of comparable fractions of clumps and cores.

Vela

Galactic plane

Spire (mollusc)

Mass distribution

Solar mass

Star (game theory)

10.1051/0004-6361/201117811

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High-time-resolution chemical composition and source apportionment of PM2.5 in northern Chinese cities: implications for policy

Zenodo (CERN European Organization for Nuclear Research) (2023)

Yong Zhang Tian Jie Lu Qi Manousakas Loannis Manousos Han Yue-mei

Three real-time measurement campaigns were conducted in Xi’an, Shijiazhuang, and Beijing to investigate the chemical characteristics and source contributions of PM_2.5 and explore the formation progress of heavy pollution for policy implications. Chemeical components of PM_2.5 including OA, NO₃^-, SO₄^2-, NH₄⁺, Cl-, BC, and elements were monitored by Q-ACSM, AE33, and Xact, respectively. The results show that chemical compositions of PM_2.5in the three cities are all dominated by organic aerosol (OA) and nitrate (NO₃^-). And results of source apportionment analyzed by the hybrid environmental receptor model (HERM) show that the secondary nitrate plus sulfate contributed higher to PM_2.5 compared to other primary sources. Morevoer, the potential formation mechanisms of secondary aerosol in three cities were further explored by establishing the correlations between secondary nitrate plus sulfate and aerosol liquid water content (ALWC), and O_x (O₃ + NO₂). The results show that photochemical oxidation and aqueous-phase reaction were two important pathways of secondary aerosol fromation. Additionally, this study compared the changes in chemical composition and source contributions of PM_2.5 in past decades, and suggested that not only the activities of clean energy replacements for the rural household is urgently enhanced to reduce the primary source emissions in northern China, but also collaborative control ozone and particulate matter need to be contiouslty promoted to weaken the atmosphere oxidation capacity for reducing secondary aerosol formation.

Apportionment

10.5281/zenodo.7336744

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VizieR Online Data Catalog: NGC 2264 clumps column densities (Nony+, 2021)

VizieR Online Data Catalog (2020)

T. Nony Jean‐François Robitaille F. Motte M. González Isabelle Joncour

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Star Formation as Revealed by Herschel

P. André V. Könyves D. Arzoumanian P. Palmeirim N. Peretto

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The evolution of very small dust particles in molecular clouds observed with ISOCAM

EAS Publications Series (2002)

A. Abergel J.-P. Bernard F. Boulanger D. Cesarsky A. P. Jones

We present ISOCAM observations (5-18 μm) of illuminated surfaces of molecular clouds. The emission properties of the transiently heated small particles, which dominate the emission observed by ISOCAM, are analysed in relation with the spatial structure of the material. Striking spatial variations of the infrared colour (5-8.5 μm/12-18 μm) are detected. Spectroscopic observations show that they are due to variations of the intensity of the aromatic features (especially at 7.7 μm) relatively to the continuum emission increasing towards long wavelengths. Compared to the intensity of the continuum emission, the intensity of the aromatic features are significantly fainter at the illuminated surfaces of dense structures than in low density regions surrounding these dense structures. This effect could be the signature of photo-chemical evolution, size segregation due to grain dynamics in uni-directional radiation fields, or abundance variations of very small particles.

Intensity

10.1051/eas:2002062

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T Tauri star magnetism: is the classical dynamo at work?

T. Montmerle P. André S. Casanova Eric D. Feigelson

Magnetism

Star (game theory)

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A study of the cold cores population in the Perseus star-forming regions.