| Name: | Sarita Vig |
| Affiliation: | Indian Institute of Space science and Technology (IIST) |
| Conference ID : | ASI2024_7 |
| Title : | Understanding the cloud structure and kinematics towards the star forming complex G12.79+0.43 |
| Authors : | Arun Seshadri (1), Sarita Vig (1), Veena V. S. (2) |
| Authors Affiliation: | (1) Indian Institute of Space science and Technology (IIST), Thiruvananthapuram 695547, Kerala
(2) Max-Planck Institute of Radio Astronomy, Bonn 53121, Germany |
| Mode of Presentation: | Poster |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | We present a multi-wavelength investigation of the region spanning 24’ x 24’ about the object RCW 155. The optical image towards this region shows nebulae towards the west, east and south, also seen as bright emission in mid-infrared Spitzer images. The far-infrared emission mapped using Herschel images show filamentary structures towards the centre, as well as emission in the periphery. Column density and dust temperature maps have been generated by pixel-by-pixel fitting of the modified blackbody function to the far-infrared spectral energy distribution. The column density is seen to be lying within the range 6.5 x 10^(19) - 7.3 x 10^(22) cm^(-2), while the dust temperature is seen to be within 15 – 28 K. Two IRAS objects 18092-1742 and 18090-1732 lie to the south and north repectively, towards which the infrared emission is seen to peak. We present and analyse the 13CO and C18O spectra, obtained from SEDIGISM survey data towards the region. The presence of two components suggests that there might be two clouds along the line of sight. Radio interferometry observations were carried out for the region from GMRT in band-4, and show nebulous emission towards the central region. In addition, we observe radio emission from the HII regions associated with the IRAS sources. We attempt to understand the star formation scenario by assimilating all these results and interpret this in terms of triggered star formation. |
