INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS
The physical mechanisms that induce the transformation of a certain mass of gas in new stars are far from being well understood. Infrared bubbles associated with H ii regions have been considered to be good samples for investigating triggered star formation. In this paper we report on the investigat...
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n1_p_Liu |
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todo:paper_0004637X_v818_n1_p_Liu2023-10-03T14:02:39Z INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS Liu, H.-L. Li, J.-Z. Wu, Y. Yuan, J.-H. Liu, T. Dubner, G. Paron, S. Ortega, M.E. Molinari, S. Huang, M. Zavagno, A. Samal, M.R. Huang, Y.-F. Zhang, S.-J. H II regions ISM: bubbles ISM: individual objects (N4) stars: formation stars: massive The physical mechanisms that induce the transformation of a certain mass of gas in new stars are far from being well understood. Infrared bubbles associated with H ii regions have been considered to be good samples for investigating triggered star formation. In this paper we report on the investigation of the dust properties of the infrared bubble N4 around the H ii region G11.898+0.747, analyzing its interaction with its surroundings and star formation histories therein, with the aim of determining the possibility of star formation triggered by the expansion of the bubble. Using Herschel PACS and SPIRE images with a wide wavelength coverage, we reveal the dust properties over the entire bubble. Meanwhile, we are able to identify six dust clumps surrounding the bubble, with a mean size of 0.50 pc, temperature of about 22 K, mean column density of 1.7 10 22 cm -2 , mean volume density of about 4.4 × 10 4 cm -3 , and a mean mass of 320 M ȯ . In addition, from PAH emission seen at 8 μm, free-free emission detected at 20 cm, and a probability density function in special regions, we could identify clear signatures of the influence of the H ii region on the surroundings. There are hints of star formation, though further investigation is required to demonstrate that N4 is the triggering source. © 2016. The American Astronomical Society. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n1_p_Liu |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
H II regions ISM: bubbles ISM: individual objects (N4) stars: formation stars: massive |
| spellingShingle |
H II regions ISM: bubbles ISM: individual objects (N4) stars: formation stars: massive Liu, H.-L. Li, J.-Z. Wu, Y. Yuan, J.-H. Liu, T. Dubner, G. Paron, S. Ortega, M.E. Molinari, S. Huang, M. Zavagno, A. Samal, M.R. Huang, Y.-F. Zhang, S.-J. INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| topic_facet |
H II regions ISM: bubbles ISM: individual objects (N4) stars: formation stars: massive |
| description |
The physical mechanisms that induce the transformation of a certain mass of gas in new stars are far from being well understood. Infrared bubbles associated with H ii regions have been considered to be good samples for investigating triggered star formation. In this paper we report on the investigation of the dust properties of the infrared bubble N4 around the H ii region G11.898+0.747, analyzing its interaction with its surroundings and star formation histories therein, with the aim of determining the possibility of star formation triggered by the expansion of the bubble. Using Herschel PACS and SPIRE images with a wide wavelength coverage, we reveal the dust properties over the entire bubble. Meanwhile, we are able to identify six dust clumps surrounding the bubble, with a mean size of 0.50 pc, temperature of about 22 K, mean column density of 1.7 10 22 cm -2 , mean volume density of about 4.4 × 10 4 cm -3 , and a mean mass of 320 M ȯ . In addition, from PAH emission seen at 8 μm, free-free emission detected at 20 cm, and a probability density function in special regions, we could identify clear signatures of the influence of the H ii region on the surroundings. There are hints of star formation, though further investigation is required to demonstrate that N4 is the triggering source. © 2016. The American Astronomical Society. All rights reserved. |
| format |
JOUR |
| author |
Liu, H.-L. Li, J.-Z. Wu, Y. Yuan, J.-H. Liu, T. Dubner, G. Paron, S. Ortega, M.E. Molinari, S. Huang, M. Zavagno, A. Samal, M.R. Huang, Y.-F. Zhang, S.-J. |
| author_facet |
Liu, H.-L. Li, J.-Z. Wu, Y. Yuan, J.-H. Liu, T. Dubner, G. Paron, S. Ortega, M.E. Molinari, S. Huang, M. Zavagno, A. Samal, M.R. Huang, Y.-F. Zhang, S.-J. |
| author_sort |
Liu, H.-L. |
| title |
INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| title_short |
INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| title_full |
INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| title_fullStr |
INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| title_full_unstemmed |
INTERACTIONS OF THE INFRARED BUBBLE N4 WITH ITS SURROUNDINGS |
| title_sort |
interactions of the infrared bubble n4 with its surroundings |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n1_p_Liu |
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1807324578593112064 |