The Herschel view of massive star formation in G035.39-00.33: dense and cold filament of W48 undergoing a mini-starburst

Nguyên Luong, Q., Motte, F., Hennemann, M., Hill, T., Rygl, K. L. J., Schneider, N., Bontemps, S., Men'shchikov, A., André, Ph., Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Anderson, L. D., Arzoumanian, D., Deharveng, L., Didelon, P., Di Francesco, J., Griffin, Matthew Joseph ORCID: https://orcid.org/0000-0002-0033-177X, Kirk, Jason M., Könyves, V., Martin, P. G., Maury, A., Minier, V., Molinari, S., Pestalozzi, M., Pezzuto, S., Reid, M., Roussel, H., Sauvage, M., Schuller, F., Testi, L., Ward-Thompson, Derek ORCID: https://orcid.org/0000-0003-1140-2761, White, G. J. and Zavagno, A. 2011. The Herschel view of massive star formation in G035.39-00.33: dense and cold filament of W48 undergoing a mini-starburst. Astronomy and Astrophysics 535 , A76. 10.1051/0004-6361/201117831

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Abstract

The filament IRDC G035.39–00.33 in the W48 molecular complex is one of the darkest infrared clouds observed by Spitzer. It has been observed by the PACS (70 and 160 μm) and SPIRE (250, 350, and 500 μm) cameras of the Herschel Space Observatory as part of the W48 molecular cloud complex in the framework of the HOBYS key programme. The observations reveal a sample of 28 compact sources (deconvolved FWHM sizes < 0.3 pc) complete down to ~5 M⊙ in G035.39–00.33 and its surroundings. Among them, 13 compact sources are massive dense cores with masses >20 M⊙. The cloud characteristics we derive from the analysis of their spectral energy distributions are masses of 20−50 M⊙, sizes of 0.1–0.2 pc, and average densities of 2−20 × 105 cm-3, which make these massive dense cores excellent candidates to form intermediate- to high-mass stars. Most of the massive dense cores are located inside the G035.39–00.33 ridge and host IR-quiet high-mass protostars. The large number of protostars found in this filament suggests that we are witnessing a mini-burst of star formation with an efficiency of ~15% and a rate density of ~40 M⊙ yr-1kpc-2 within ~8 pc2, a large area covering the full ridge. Part of the extended SiO emission observed towards G035.39–00.33 is not associated with obvious protostars and may originate from low-velocity shocks within converging flows, as advocated by previous studies.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	ISM: clouds / stars: formation / submillimeter: ISM / stars: protostars / ISM: individual objects: G035.39-00.33 / ISM: individual objects: W48
Additional Information:	11 pp. Pdf uploaded in accordance with publisher's policy at http://www.sherpa.ac.uk/romeo/issn/0004-6361/ (accessed 16/04/2014)
Publisher:	EDP Sciences
ISSN:	0004-6361
Date of First Compliant Deposit:	30 March 2016
Last Modified:	04 May 2023 13:25
URI:	https://orca.cardiff.ac.uk/id/eprint/24790

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