Fig 5 - uploaded by Pierre Didelon
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Radial intensity profiles of the central UCH ii region showing the measurements done at 70 μ m (blue points) and 160 μ m (green points) taking advantage of the PACS highest resolution, compared with the 3-band temperature ( T 3B ) and the 4-band temperature ( T 4B ) data given by the black arrow. The
Source publication
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....
Contexts in source publication
Context 1
... the (small) central UCH ii region, the radial profiles of the T 3B and T 4B temperatures are shown in Fig. 4. The flux pro- files obtained from the 70 µm and 160 µm images with 6 and 12 resolutions are shown in Fig. 5. These four different esti- mators display similar radial shapes for the H ii region and give consistent size values: R H ii 0.09, 0.08, 0.09, and 0.09 pc for 70 µm, 160 µm, T 3B , and T 4B respectively. Similarly concordant measurements are found for the fully-resolved northern H ii re- gion in the T 4B and T 3B maps: R H ii (0.85 ± ...
Context 2
... value is between the typical size of Keplerian disks sur- rounding low-mass pre-main sequence T Tauri stars (∼0. 5) show that when r c R H ii , the value of r c does not have much influence on the expansion time of the ionised bubble. ...
Context 3
... -The size of ionised regions is estimated by the heating of big grains (Fig. 2a) and small grains excitation through their 70 µm flux (Fig. 5), in the close surrounding of H ii regions, prob- ably within the PDR. It ranges from ∼0.1 pc for Compact and UCH ii regions to ∼0.8 pc for the most classical Extended H ii re- ...
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Citations
... Such systems are particularly prominent in massive star-forming regions (e.g. MonR2: Didelon et al. 2015;Pokhrel et al. 2016;SDC335: Peretto et al. 2013), but also exist in clouds forming mostly (or only) low-to intermediate-mass stars (e.g. B59: Peretto et al. 2012;L1688: Ladjelate et al. 2020. ...
Molecular clouds are a fundamental ingredient of galaxies: they are the channels that transform the diffuse gas into stars. The detailed process of how they do it is not completely understood. We review the current knowledge of molecular clouds and their substructure from scales \sim1~\mbox{kpc} down to the filament and core scale. We first review the mechanisms of cloud formation from the warm diffuse interstellar medium down to the cold and dense molecular clouds, the process of molecule formation and the role of the thermal and gravitational instabilities. We also discuss the main physical mechanisms through which clouds gather their mass, and note that all of them may have a role at various stages of the process. In order to understand the dynamics of clouds we then give a critical review of the widely used virial theorem, and its relation to the measurable properties of molecular clouds. Since these properties are the tools we have for understanding the dynamical state of clouds, we critically analyse them. We finally discuss the ubiquitous filamentary structure of molecular clouds and its connection to prestellar cores and star formation.
... Such systems are particularly prominent in massive star-forming regions (e.g. MonR2: Didelon et al., 2015;Pokhrel et al., 2016;SDC335: Peretto et al., 2013), but also exist in clouds forming mostly (or only) low-to intermediate-mass stars (e.g. B59: Peretto et al., 2012;L1688: Ladjelate et al., 2020. ...
Molecular clouds are a fundamental ingredient of galaxies: they are the channels that transform the diffuse gas into stars. The detailed process of how they do it is not completely understood. We review the current knowledge of molecular clouds and their substructure from scales 1~kpc down to the filament and core scale. We first review the mechanisms of cloud formation from the warm diffuse interstellar medium down to the cold and dense molecular clouds, the process of molecule formation and the role of the thermal and gravitational instabilities. We also discuss the main physical mechanisms through which clouds gather their mass, and note that all of them may have a role at various stages of the process. In order to understand the dynamics of clouds we then give a critical review of the widely used virial theorem, and its relation to the measurable properties of molecular clouds. Since these properties are the tools we have for understanding the dynamical state of clouds, we critically analyse them. We finally discuss the ubiquitous filamentary structure of molecular clouds and its connection to prestellar cores and star formation.
