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The dust properties and physical conditions of the interstellar medium in the LMC massive star-forming complex N11

M. Galametz 1 S. Hony 2 M. Albrecht 3 F. Galliano 4 D. Cormier Vianney Lebouteiller 4 M. Y. Lee S. C. Madden 5 A. Bolatto 6 C. Bot 7 A. Hughes F. Israel 8 M. Meixner J. M. Oliviera D. Paradis 9 E. Pellegrini 10 J. Roman-Duval M. Rubio M. Sewiło Y. Fukui 11 A. Kawamura 12 T. Onishi M. Oliviera
1 CAM - University of Cambridge [UK]
2 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
3 Leibniz-Institut für Kristallzüchtung
4 AIM (UMR_7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
5 DAPNIA - Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée
6 Department of Astronomy [College Park]
7 OAS - Observatoire astronomique de Strasbourg
8 Leiden Observatory [Leiden]
9 Météo-France [Paris]
10 ILL - Institut Laue-Langevin
11 Department of Astrophysics [Nagoya]
12 Institute of Environmental Systems (SUIKO)
Abstract : We combine Spitzer and Herschel data of the star-forming region N11 in the Large Magellanic Cloud (LMC) to produce detailed maps of the dust properties in the complex and study their variations with the interstellar-medium conditions. We also compare Atacama Pathfinder EXperiment/Large APEX Bolometer Camera (APEX/LABOCA) 870 μm observations with our model predictions in order to decompose the 870 μm emission into dust and non-dust [free-free emission and CO(3-2) line] contributions. We find that in N11, the 870 μm can be fully accounted for by these three components. The dust surface density map of N11 is combined with H I and CO observations to study local variations in the gas-to-dust mass ratios. Our analysis leads to values lower than those expected from the LMC low-metallicity as well as to a decrease of the gas-to-dust mass ratio with the dust surface density. We explore potential hypotheses that could explain the low `observed' gas-to-dust mass ratios (variations in the XCO factor, presence of CO-dark gas or of optically thick H I or variations in the dust abundance in the dense regions). We finally decompose the local spectral energy distributions (SEDs) using a principal component analysis (I.e. with no a priori assumption on the dust composition in the complex). Our results lead to a promising decomposition of the local SEDs in various dust components (hot, warm, cold) coherent with that expected for the region. Further analysis on a larger sample of galaxies will follow in order to understand how unique this decomposition is or how it evolves from one environment to another.
Keywords : infrared: ISM submillimetre: ISM Magellanic Clouds galaxies: ISM ISM: general galaxies: dwarf
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Journal articles
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https://hal.archives-ouvertes.fr/hal-02105260
Contributor : Vianney Lebouteiller Connect in order to contact the contributor
Submitted on : Wednesday, January 12, 2022 - 8:53:59 AM
Last modification on : Wednesday, January 12, 2022 - 8:54:04 AM

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CEA | UNIV-PARIS | SITE-ALSACE | CEA-DRF | CEA-UPSAY | IRFU-AIM | DSM-IRFU | CNRS | UNIV-PARIS7 | METEO | INSU | UP-SCIENCES

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M. Galametz, S. Hony, M. Albrecht, F. Galliano, D. Cormier, et al.. The dust properties and physical conditions of the interstellar medium in the LMC massive star-forming complex N11. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2015, 456 (2), pp.1767-1790. ⟨10.1093/mnras/stv2773⟩. ⟨hal-02105260⟩

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