Abstract Details
| Name: Susmita Barman Affiliation: School of Physics,University of Hyderabad Conference ID: ASI2018_1764 Title : A Photodissociation region in a massive star forming region of the Large Magellanic Cloud Authors and Co-Authors : Naslim Neelamkodan(School of Physics,University of Hyderabad,India) Franciska Kemper(Academia sinica Institute of Astronomy Astrophysics,Taipei,Taiwan) Oscar Morata(Academia Sinica Institute of Astronomy Astrophysics,Taipei,Taiwan) Suzanne Madden(CEA Saclay,Paris,France) Sacha Hony(University of Heidelberg,Germany) Frederic Galliano(CEA Saclay,Paris,France) Vianney Lebouteiller(CEA Saclay,Paris,France) Remy Indebetouw(National Radio Astronomical observatory,Charlottesville, USA) Karl Gordon (Space Telescope Science Institute, Baltimore, USA) Margaret Meixner (Space Telescope Science Institute, Baltimore, USA) Abstract Type : Poster Abstract Category : Extragalactic astronomy Abstract : Photodissociation regions (PDR) are formed in neutral hydrogen clouds where the incident Far Ultraviolet (FUV) radiation highly controls the evolution of dust and gas physical and chemical properties. In starforming regions, FUV radiation from young stars heats the PAHs and eject high energy photoelectrons. These photoelectrons then photodissociate the gas creating stratified layers of partially ionized, neutral and molecular gas. The resulting chemical structure is complex. Some atoms and molecules are highly enhanced in certain layers, while some other are depleted. In metal-poor environments, both gas and dust abundances vary relative to metal-rich environments due to the deficiency of heavy elemental abundances, which lowers the dust-to-gas ratio. Due to the diminished dust shielding, FUV radiation penetrates deeper into the molecular cloud and photodissociate most of the molecules including CO, except H2. The nearby Large Magellanic Cloud (LMC, metallicity Z=0.5 solar) galaxy is an excellent site to look for PDR structure and chemistry in the metal-poor environment due to its proximity. At a distance of 50 kpc, it allows us to resolve stars and ISM small-scale structures. A spectroscopic survey of selected extended sources in the LMC has been carried out as part of the SAGE-spectroscopic program (Kemper et al. 2010) using the Spitzer Spectroscopic capabilities. We present our preliminary work on the study of a spatially resolved edge-on PDR in the LMC using Spitzer and Herschel data. |