Hydro-geomorphic characteristics of the Indian (Peninsular) catchments: Based on morphometric correlation with hydro-sedimentary data

In terms of hydro-geomorphic characteristics, catchments in Peninsular India remained mostly unexplored except a few regional and local works that deal with tectonic, structural and paleo-climatic control on geomorphology. Catchment scale morphometric analyses deliver insights into dynamics, erosion capacity, probability of flood occurrence, lithological and structural control, and genetic response to the tectonics. The present study aimed to comprehend hydro-geomorphic characteristics of 12 major catchments in Peninsular India through GIS-based morphometric analysis. A total of 25 morphometric parameters were computed and several statistical analyses performed in establishing inter-correlation and classification of Indian rivers. Most of the rivers in Peninsular India were found 7th to 9th order catchments. Almost all basins showed a moderate relief ratio, hypsometric integral, ruggedness etc. Cauvery, Baitarni, and Brahmani showed exceptionally steeper gradient, high relief ratio, LS factor, and ruggedness index, which indicated higher erosion potential. Correlation among landscape variables revealed moderate scale dependency of few relief factors. Baitarni, Brahmani and Narmada showed higher hypsometric integral. A strong positive association between hypsometric integral and sediment yield suggested critically high erosion potential in catchments with high integral values. The present study provides some generic insights into the hydro-geomorphic characteristics with dissimilarity in lithology in Peninsular Indian catchments as a whole.     

A Cosmic Microscope to Probe the Universe from Present to Cosmic Dawn:Dual-element Lowfrequency Space VLBI Observatory

A space-based Very Long Baseline Interferometry (VLBI) program, named as the Cosmic Microscope, is proposed to involve dual VLBI telescopes in the space working together with giant ground-based telescopes (e.g., Square Kilometre Array, FAST, Arecibo) to image the low radio frequency Universe with the purpose of unraveling the compact structure of cosmic constituents including supermassive black holes and binaries, pulsars, astronomical masers and the underlying source, and exoplanets amongst others. The operational frequency bands are 30, 74, 330 and 1670 MHz, supporting broad science areas. The mission plans to launch two 30-m-diameter radio telescopes into 2 000 km×90 000 km elliptical orbits. The two telescopes can work in flexibly diverse modes. (i) Space-ground VLBI. The maximum space-ground baseline length is about 100 000 km; it provides a high-dynamic-range imaging capacity with unprecedented high resolutions at low frequencies (0.3 mas at 1.67 GHz and 20 mas at 30 MHz) enabling studies of exoplanets and supermassive black hole binaries (which emit nanoHz gravitational waves). (ii) Space-space single-baseline VLBI. This unique baseline enables the detection of flaring hydroxyl masers, and more precise position measurement of pulsars and radio transients at mas level. (iii) Single dish mode, where each telescope can be used to monitor transient bursts and rapidly trigger follow-up VLBI observations. The large space telescope will also contribute in measuring and constraining the total angular power spectrum from the Epoch of Reionization. In short, the Cosmic Microscope offers astronomers the opportunity to conduct novel, frontier science.