Yogesh Wadadekar
Associate Professor - G
Email: yogesh [at] ncra.tifr.res.in
Phone: +91 - 20 - 25719238
Extn: 9238
Office: F215
National Centre for Radio Astrophysics
Tata Institute of Fundamental Research
Savitribai Phule Pune University Campus,
Pune 411 007
Maharashtra, INDIA
Tata Institute of Fundamental Research
Savitribai Phule Pune University Campus,
Pune 411 007
Maharashtra, INDIA
Main Research Areas: Galaxy formation and evolution; radio properties of AGN and normal galaxies; High redshift radio galaxies; machine learning methods; SKA Telescope monitoring and control system architecture.
Biography:
Yogesh Wadadekar did his B. Tech. (Metallurgical Engg.) from IIT-Bombay. In 1994, he joined IUCAA for his Ph.D. In 2000, he finished his Ph.d. on the optical and radio properties of faint radio sources. He then went to the Institut d'Astrophysique de Paris as a postdoctoral fellow in 2001 and later moved to the Space Telescope Science Institute in Baltimore, USA in 2003. During 2006-07, he worked at the Dept. of Astrophysical Sciences, Princeton University, as the Astronomical Software Scientist for the Sloan Digital Sky Survey. Yogesh joined the National Centre for Radio Astrophysics in October 2007 and is now an Associate Professor.Research description:
Galaxy formation and evolution:
How galaxies form and evolve over the whole of cosmic history is a broad and active area of current research in astrophysics. The detailed physics is very complicated due to the complex interactions between stars, dust, gas and dark matter. Over the decades, detailed analytic and numerical modeling has made a number of predictions that can be tested with observations. I use data, mainly from large surveys in the ultraviolet, optical, infrared and radio bands to observationally test some of the predictions of galaxy evolution models. An area of specific interest is the evolution of the bulge component of disk galaxies.
How galaxies form and evolve over the whole of cosmic history is a broad and active area of current research in astrophysics. The detailed physics is very complicated due to the complex interactions between stars, dust, gas and dark matter. Over the decades, detailed analytic and numerical modeling has made a number of predictions that can be tested with observations. I use data, mainly from large surveys in the ultraviolet, optical, infrared and radio bands to observationally test some of the predictions of galaxy evolution models. An area of specific interest is the evolution of the bulge component of disk galaxies.
Radio properties of AGN and normal galaxies:
Most of the bright radio sources in the sky are Active Galactic Nuclei - supermassive black holes at the centres of galaxies that are driving radio jets which interact with the surrounding medium to produce radio lobes. Understanding the phenomonology of these sources has been a long standing research interest, and I have used both large area surveys with the VLA as well as deeper, smaller area surveys with the GMRT to characterise and understand these sources.
Most of the bright radio sources in the sky are Active Galactic Nuclei - supermassive black holes at the centres of galaxies that are driving radio jets which interact with the surrounding medium to produce radio lobes. Understanding the phenomonology of these sources has been a long standing research interest, and I have used both large area surveys with the VLA as well as deeper, smaller area surveys with the GMRT to characterise and understand these sources.
SKA Telescope design
The Square Kilometer Array telescope went through its detailed design phase from 2013-18. NCRA led the design work in an important area- the control and monitoring system for the SKA. I worked as the Project Scientist for a 7-nation consortium that worked on the engineering design of this system. After the successful completion of the criticial design review of our system in 2018, I have been working as a product owner for Scrum teams at NCRA working on various prototype implementations of the system we have designed.
The Square Kilometer Array telescope went through its detailed design phase from 2013-18. NCRA led the design work in an important area- the control and monitoring system for the SKA. I worked as the Project Scientist for a 7-nation consortium that worked on the engineering design of this system. After the successful completion of the criticial design review of our system in 2018, I have been working as a product owner for Scrum teams at NCRA working on various prototype implementations of the system we have designed.
Selected publications:
1. Connecting galaxy structure and star formation: the role of environment in formation of S0 galaxies (Mishra, Wadadekar & Barway 2019, MNRAS, 487, 5572) 2. Outlying Hα emitters in SDSS IV MaNGA (Bait, Wadadekar & Barway 2019, MNRAS, 485, 428) 3. Why are classical bulges more common in S0 galaxies than in spiral galaxies? (Mishra, Wadadekar & Barway 2018, MNRAS, 478, 351) 4. On the interdependence of galaxy morphology, star formation and environment in massive galaxies in the nearby Universe (Bait, Barway & Wadadekar 2017, MNRAS, 471, 2687) 5. On the nature of infrared-faint radio sources in the Subaru X-ray Deep and Very Large Array-VIMOS VLT Deep Survey fields (Singh, Wadadekar et al 2017, MNRAS, 470, 4956) 6. J021659-044920: a relic giant radio galaxy at z ~ 1.3 (Tamhane, Wadadekar et al 2015, MNRAS, 453, 2438) 7. Radio-Far Infrared correlation in blue cloud galaxies with 0 < z < 1.2 (Basu, Wadadekar et al 2015, ApJ, 803, 51) 8. Luminosity-dependent star formation history of S0 galaxies: evidence from GALEX-SDSS-2MASS-WISE colours (Barway, Wadadekar et al. 2013, MNRAS, 432, 430) 9. Near-infrared bulge-disc correlations of lenticular galaxies (Barway, Wadadekar et al. 2009, MNRAS, 39, 1991) 10. Faint U-Band Dropouts in the WFPC2 Parallels of the Hubble Ultra Deep Field (Wadadekar et al. 2006, AJ, 132, 1023) 11. The WFPC2 Archival Pure Parallels Project (Wadadekar et al. 2006, PASP, 118, 450) 12. Estimating Photometric Redshifts Using Support Vector Machines (Wadadekar 2005, PASP, 117, 79)
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