Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Molinari, Sergio and Swinyard, Bruce M. and Bally, John and Barlow, Michael J. and Bernard, Jean P. and Martin, Peter G. and Moore, Toby J.T. and Noriega-Crespo, Alberto and Plume, René and Testi, Leonardo and Zavagno, Annie and Abergel, Alain and Ali, Babar and Anderson, Lynn D. and Ándré, P. and Baluteau, Jean P. and Battersby, Cara and Beltrán, Maria T. and Benedettini, Milena and Billot, Nicolas and Blommaert, Joris A.D.L. and Bontemps, Sylvain and Boulanger, François and van den Brand, Jan F.J. and Brunt, Christopher M. and Burton, Michael G. and Calzoletti, Luca and Carey, Sean J. and Caselli, Paola E.S. and Cesaroni, Riccardo and Cernicharo, José R. and Chakrabarti, Sukanya and Chrysostomou, Antonio C. and Cohen, Martin G. and Compiegne, Mathieu and De Bernardis, Paolo and De Gasperis, Giancarlo and Di Giorgio, Anna Maria and Elia, D. and Faustini, Fabiana and Flagey, N. and Fukui, Yasuo and Fuller, Gary A. and Ganga, Ken M. and Garcia-Lario, Pedro and Glenn, Jason and Goldsmith, Paul F. and Griffin, Matthew J. and Hoare, Matthew J. and Huang, Maohai and Ikhenaode, David and Joblin, Christine and Joncas, Gilles and Juvela, Mika and Kirk, Jason M. and Lagache, Guilaine and Li, Jin Zeng and Lim, Tanya L. and Lord, Steven D. and Marengo, Massimo and Marshall, Douglas J. and Masi, Silvia and Massi, Fabrizio and Matsuura, Makiko and Minier, Vincent and Miville-Deschênes, Marc Antoine and Montier, Ludovic A. and Morgan, L.K. and Motte, Frédérique and Mottram, Joseph C. and Müller, Thomas G. and Natoli, Paolo and Neves, J. and Olmi, Luca and Paladini, Roberta and Paradis, Delphine and Parsons, Harriet A.L. and Peretto, Nicolas and Pestalozzi, Michele R. and Pezzuto, Stefano and Piacentini, Francesco and Piazzo, Lorenzo and Polychroni, Danae and Pomarès, M. and Popescu, Cristina C. and Reach, William T. and Ristorcelli, Isabelle and Robitaille, J.F. and Robitaille, Thomas P. and Rodón, Javier A. and Roy, Arabindo and Royer, Pierre and Russeil, Delphine and Saraceno, Paolo and Sauvage, Marc André and Schilke, Peter and Schisano, Eugenio and Schneider, Nicola and Schuller, Frédéric and Schulz, Bernhard and Sibthorpe, Bruce and Smith, Howard A. and Smith, Michael D. and Spinoglio, Luigi and Stamatellos, Dimitris and Strafella, Francesco and Stringfellow, Guy S. and Sturm, Eckhard and Taylor, Russ S. and Thompson, M.A. and Traficante, Alessio and Tuffs, Richard J. and Umana, Grazia M. and Valenziano, Luca and Vavrek, Roland and Veneziani, Milena and Viti, Serena and Waelkens, C. and Ward-Thompson, Derek and White, Glenn J. and Wilcock, Lawrence A. and Wyrowski, Friedrich and Yorke, Harold W. and Zhang, Qizhou (2010) Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way. Astronomy & Astrophysics, 518 (8). 0-0. ISSN 0004-6361. (doi: (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

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We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l = 30° and l = 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV ∼ 1 is exceeded for the regions in the l = 59° field; a AV value between 5 and 10 is found for the l = 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm -2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

Item Type: Article
Uncontrolled keywords: Galaxy: general, ISM: clouds, ISM: structure, Stars: formation, Column density, Compact sources, Critical level, Galactic plane, Galaxy: general, HERSCHEL, ISM : clouds, ISM: structure, Large-scale converging, Milky ways, Numerical simulation, Physical parameters, Protostars, Reduction strategy, Stars: formation, Surface density, Clouds, Data reduction, Galaxies, Stars, Filaments (lamp)
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 10 Aug 2015 15:55 UTC
Last Modified: 11 Aug 2015 09:01 UTC
Resource URI: (The current URI for this page, for reference purposes)
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