STAR-FORMATION ACTIVITY IN THE NEIGHBORHOOD OF W-R 1503-160L STAR IN THE MID-INFRARED BUBBLE N46

• Published in: The Astrophysical journal 2016-07, Vol.826 (1), p.27-27, Article 27
• Main Authors: Dewangan, L. K., Baug, T., Ojha, D. K., Janardhan, P., Ninan, J. P., Luna, A., Zinchenko, I.
• Format: Article
• Language: English
• Subjects: A stars; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BUBBLES; CARBON; CARBON MONOXIDE; Condensation; COSMIC DUST; dust, extinction; FEEDBACK; HYDROGEN; INTERMEDIATE INFRARED RADIATION; ISM: clouds; ISM: individual objects (N46); LUMINOSITY; MASERS; METHANOL; POLARIZATION; regions; STAR EVOLUTION; Star formation; STARS; stars: formation; stars: pre-main sequence; Stellar age; STELLAR WINDS; TEMPERATURE RANGE; WAVELENGTHS; Wolf-Rayet stars
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/0004-637X/826/1/27

ABSTRACT In order to investigate star-formation (SF) processes in extreme environments, we have carried out a multi-wavelength analysis of the mid-infrared bubble N46, which hosts a WN7 Wolf-Rayet (W-R) star. We have used 13CO line data to trace an expanding shell surrounding the W-R star containing about five condensations within the molecular cloud associated with the bubble. The W-R star is associated with a powerful stellar wind having a mechanical luminosity of ∼4 × 1037 erg s−1. A deviation of the H-band starlight mean polarization angles around the bubble has also been traced, indicating the impact of stellar wind on the surroundings. The Herschel temperature map shows a temperature range of ∼18-24 K toward the five molecular condensations. The photometric analysis reveals that these condensations are associated with the identified clusters of young stellar objects, revealing ongoing SF process. The densest among these five condensations (peak N(H2) ∼9.2 × 1022 cm−2 and AV ∼ 98 mag) is associated with a 6.7 GHz methanol maser, an infrared dark cloud, and the CO outflow, tracing active massive SF within it. At least five compact radio sources (CRSs) are physically linked with the edges of the bubble, and each of them is consistent with the radio spectral class of a B0V-B0.5V-type star. The ages of the individual infrared counterparts of three CRSs (∼1-2 Myr) and a typical age of WN7 W-R star (∼4 Myr) indicate that the SF activities around the bubble are influenced by the feedback of the W-R star.