G. Hamon - Academia.edu (original) (raw)
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Jet Propulsion Laboratory, California Institute of Technology
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Papers by G. Hamon
Astronomy and Astrophysics, 2009
Aims. Expanding HII regions and propagating shocks are common in the environment of young high-ma... more Aims. Expanding HII regions and propagating shocks are common in the environment of young high-mass star-forming complexes. They can compress a pre-existing molecular cloud and trigger the formation of dense cores. We investigate whether these phenomena can explain the formation of high-mass protostars within an infrared dark cloud located at the position of G327.3-0.6 in the Galactic plane, in between two large infrared bubbles and two HII regions. Methods. The region of G327.3-0.6 was imaged at 450 µm with the CEA P-ArTéMiS bolometer array on the Atacama Pathfinder EXperiment telescope in Chile. APEX/LABOCA and APEX-2A, and Spitzer/IRAC and MIPS archives data were used in this study. Results. Ten massive cores were detected in the P-ArTéMiS image, embedded within the infrared dark cloud seen in absorption at both 8 and 24 µm. Their luminosities and masses indicate that they form high-mass stars. The kinematical study of the region suggests that the infrared bubbles expand toward the infrared dark cloud.
Astronomy and Astrophysics, 2008
Aims. In an effort to make progress in the current debate on the earliest phases of massive star ... more Aims. In an effort to make progress in the current debate on the earliest phases of massive star formation, we took a census of Class 0-like protostellar dense cores in the NGC 3576 region, one of the nearest and most luminous embedded sites of high-mass star formation in the Galaxy. Methods. We used the P-ArTéMiS bolometer camera on the APEX telescope to produce the first 450 μm dust continuum map of the filamentary dense clump associated with NGC 3576. Results. Combining our 450 μm observations with existing data at other wavelengths, we identified seven massive protostellar sources along the NGC 3576 filament and placed them in the M env -L bol evolutionary diagram for protostars. Conclusions. Comparison with theoretical evolutionary tracks suggests that these seven protostellar sources will evolve into massive stars with masses M ∼ 15-50 M . Four sources are classified as candidate high-mass Class 0 objects, two sources as massive Class I objects, and one source appears to be at an intermediate stage.
Astronomy and Astrophysics, 2009
Aims. Expanding HII regions and propagating shocks are common in the environment of young high-ma... more Aims. Expanding HII regions and propagating shocks are common in the environment of young high-mass star-forming complexes. They can compress a pre-existing molecular cloud and trigger the formation of dense cores. We investigate whether these phenomena can explain the formation of high-mass protostars within an infrared dark cloud located at the position of G327.3-0.6 in the Galactic plane, in between two large infrared bubbles and two HII regions. Methods. The region of G327.3-0.6 was imaged at 450 µm with the CEA P-ArTéMiS bolometer array on the Atacama Pathfinder EXperiment telescope in Chile. APEX/LABOCA and APEX-2A, and Spitzer/IRAC and MIPS archives data were used in this study. Results. Ten massive cores were detected in the P-ArTéMiS image, embedded within the infrared dark cloud seen in absorption at both 8 and 24 µm. Their luminosities and masses indicate that they form high-mass stars. The kinematical study of the region suggests that the infrared bubbles expand toward the infrared dark cloud.
Astronomy and Astrophysics, 2008
Aims. In an effort to make progress in the current debate on the earliest phases of massive star ... more Aims. In an effort to make progress in the current debate on the earliest phases of massive star formation, we took a census of Class 0-like protostellar dense cores in the NGC 3576 region, one of the nearest and most luminous embedded sites of high-mass star formation in the Galaxy. Methods. We used the P-ArTéMiS bolometer camera on the APEX telescope to produce the first 450 μm dust continuum map of the filamentary dense clump associated with NGC 3576. Results. Combining our 450 μm observations with existing data at other wavelengths, we identified seven massive protostellar sources along the NGC 3576 filament and placed them in the M env -L bol evolutionary diagram for protostars. Conclusions. Comparison with theoretical evolutionary tracks suggests that these seven protostellar sources will evolve into massive stars with masses M ∼ 15-50 M . Four sources are classified as candidate high-mass Class 0 objects, two sources as massive Class I objects, and one source appears to be at an intermediate stage.