MSV-2035 Astronomy Document - Inside Design - FINAL - FINAL

Astronomy & Astrophysics 46 spectra. The numerical code developed by Indian astronomers will provide an accurate analysis and interpretation of the observed spectra and hence probe the exoplanetary atmosphere. Indian astronomers were part of an international campaign to study the transit signals due to planets around the ultra cool dwarf TRAPPIST-1 (2MASS J23062928-0502285). The extensive observations indicated the star to be hosting multiple planets. The transit of its planets is expected to give rise to significant asymmetry and produce phase- dependent polarisation. Adopting the known stellar and planetary physical parameters and employing a self- consistent cloudy atmosphere model of the M8 dwarf star, the transit polarisation profiles and the expected amount of polarisation of Trappist-1 during the transit phase of each individual planet, as well as that during the simultaneous transit of two planets, were presented and shown to be within the detection limit of a few existing facilities. 4.1.8 Galaxy Formation andEvolution Formation and evolution of galaxies is intimately connected with star formation and feedback processes that regulate star formation in galaxies, formation and growth of super-massive black holes, and the physical state of the intergalactic medium as it exchanges matter and radiation with galaxies through a variety of processes. Formation of the first generation of stars and galaxies also leads to ionisation of the intergalactic medium and this is an epoch of special interest to astronomers. India has a large community of astronomers working on the epoch of reionisation and the intergalactic medium. Using available observations of distant quasars, galaxies and cosmic microwave background radiation, they have placed stringent constraints on the epoch of reionisation and the nature of ionising sources. This field will have a major boost in the SKAera with the observations of H I 21-cm signal from the epoch of reionisation. India also has a large pool of astronomers working on various aspects of IGM studies who are playing a very important role in mapping the redshift evolution of atomic and molecular content of the universe through radio and optical spectroscopy. Important contributions include: (i) IGM and CGM observations using both optical and 21- cm H I spectroscopy; (ii) detection of H I, C II, CO and mm emission from distant galaxies; (iii) understanding the properties and evolution of radio galaxies and quasars; (iv) studies of low frequency radio emission and X-rays from high redshift galaxy clusters and groups; (v) most accurate measurements of clustering properties and thermal evolution of the IGM and; (vi) mapping of meta-galactic radiation field that imprints the galaxy evolution and interveningmaterial through radiative transport efforts in the Universe. The dynamics of stars and gas in galaxies, as well as use of information about orbits of gas, stars and satellite galaxies to uncover the shape and structure of the dark matter halos of galaxies is an area where several key results have been published by Indian astronomers. Computational work on evolution of features like bars in galaxies and the impact of Key ideas on galaxy evolution have been proposed, in particular, during the late stages of evolution of galaxies wherein star formation slows down and sometimes comes to an abrupt end. Important theoretical contributions have been made in the modelling of CGM gas, galactic winds that populates CGM and IGM, analytical and numerical modelling of IGM including various feed back processes. The role of feedback from star formation andAGN activity on gas content in galaxy halos has been studied using simulations. Some models of dark matter allow for decay of dark matter particles into other particles. In such models it is possible for some of the energy to be released as photons. This leads to observable effects and Indian scientists have confronted such models with observations to put strong constraints on parameters of thesemodels. MEGA SCIENCE VISION-2035