IUCAA Bulletin 2016
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Probing the Universe at Low Radio Frequencies Using the GMRT
The GMRT : a look at the Past, Present and Future Yashwant Gupta & Govind Swarup National Centre for Radio Astrophysics Pune India URSI GASS Montreal 2017 The GMRT : a look at the Past, Present and Future Yashwant Gupta & Govind Swarup National Centre for Radio Astrophysics Pune India URSI GASS Montreal 2017 Overview of today’s talk . Part I : the GMRT -- a historical perspective . Part II : the GMRT -- current status . Part III : future -- the upgraded GMRT Some history . It is the early 1980s… the VLA has recently become operational . Radio astronomy has shifted from the low frequencies, where it was born, to higher frequencies (cm and higher wavelengths) -- obvious reasons . Note, however, techniques like self-cal have been shown to work . In India, the radio astronomy group at the Tata Institute, under the leadership of Govind Swarup, is looking for the next big challenge… They have already : . Built the Ooty Radio Telescope in the late 1960s – still operational & producing international quality results (in fact, currently being upgraded with new receiver system!) . Built the Ooty Synthesis Radio Telescope (1980s) – short-lived but valuable learnings . Built up considerable experience in low frequencies (metre wavelengths) Birth of the GMRT . Motivation : bridge the gap in radio astronomy facilities at low frequencies and address science problems best studied at metre wavelengths . First concept : 1984 (started with large cylinders); evolved to 34 dishes of 45 metres by 1986 . Project cleared and funding secured by 1987 . Construction started : 1990; first antenna erected : 1992 . First light observations : 1997 – 1998 . Released for world-wide use : 2002 The GMRT : turning it ON Jan 1997 : First fringes with the prototype GMRT correlator Dec 1998 : first light pulsar observation with the GMRT Dedication of the GMRT The Giant Metrewave Radio Telescope was dedicated to the World Scientific Community by the Chairman of TIFR Council, Shri Ratan Tata. -
Prime Minister Dr Manmohan Singh Gives Away
ISSN 0409-7467 VOL 59 NO 1 15 JANUARY 2009 Prime Minister Dr Manmohan Singh gives away Shanti Swarup Bhatnagar Prizes for 2007 & 2008, CSIR Diamond Jubilee Technology Award for 2007 and CSIR Award for S&T Innovation for Rural Development for 2007 & 2008 Seen on the dais at the CSIR Award Presentation Function: Prime Minister Dr Manmohan Singh (centre), Minister for Science & Technology and Earth Sciences and Vice President, CSIR, Shri Kapil Sibal (left ) and Director General, CSIR, Prof. Samir K. Brahmachari Prime Minister of India and President, CSIR, Dr Manmohan Singh, gave away Shanti Swarup Bhatnagar Prizes for 2007 & 2008. CSIR Diamond Jubilee Technology Award for 2007 and CSIR Award for S&T Innovation for Rural Development for 2007 & 2008, at a glittering function held on 20 December 2008 in the Dr D.S. Kothari Auditorium, DRDO Bhawan, New Delhi. Attended by a galaxy of S&T personnel, the function was presided over by Shri Kapil Sibal, Minister for Science & Technology and Earth Sciences and Vice President, CSIR. Prof Samir K. Brahmachari, Director General, CSIR, proposed a vote of thanks. We bring in this issue, speeches of Dr Manmohan Singh, Shri Kapil Sibal and Prof. Brahmachari on the occasion along with the citations of the prize-winners. 15 JANUARY 2009 1 CSIR Award Function Speech of Prime Minister Dr Manmohan Singh am very pleased to be here in laboratories.” Iyour midst today to give away the It is this energy and this Shanti Swarup Bhatnagar Prizes for enthusiasm of our scientists that we the years 2007 & 2008. I honour and celebrate each year on congratulate each one of the award such events. -
00224Notice 10212019.Pdf
District-Gorakhpur, College Name-MADAN MOHAN MALAVIYA UNIVERSITY OF TECHNOLOGY, GORAKHPUR, Postmatric 2019-20 (Fresh) ALL Application For Session 2019-20 as on 18- 10-2019 Serial No.Registration No Name Father Name Date Of Birth Caste Course Course Branch YearType Student TypeClaim FeesStatus 1 580380501901323 AASHISH KUMAR MISHRA RAVI PRAKASH MISHRA 21/01/2001 GEN B.TECH/B.E.Bachelor of Technology (Electrical1 Regular EngineeringD/s 80900 ) Forwd 2 580380501901096 AASTHA SHUKLA RANG NATH SHUKLA 12/04/1999 GEN M.SC M.Sc. in Mathematics and1 ComputingRegular D/s 41900 Forwd 3 580380501901048 AAYUSH SRIVASTAV JAI SHANKAR LAL SRIVASTAV 14/12/1999 GEN B.TECH/B.E.Bachelor of Technology (Electrical1 Regular EngineeringD/s 80900 ) Forwd 4 580380501900555 ABHAY RAJ SINGH SURYA PRATAP SINGH 02/04/2000 GEN B.TECH/B.E.Bachelor of Technology (Mechanical1 Regular Engineering)Host 25900 Forwd 5 580380501900038 ABHIJEET KUMAR SINGH RAJEEV RANJAN SINGH 01/03/1998 GEN B.TECH/B.E.Bachelor of Technology (Computer3 Regular ScienceHost &80900 Engineering)Forwd 6 580380501900942 ABHINAV PRAKASH PANDEY GIRISH CHANDRA PANDEY 27/07/2000 GEN B.TECH/B.E.Bachelor of Technology (Electrical1 Regular EngineeringHost 25900 ) Forwd 7 580380501900314 ABHINAY SINGH UDAY PRATAP SINGH 25/08/1997 GEN MCA Master in Computer Applications1 Regular D/s 55900 Forwd 8 580380501901425 ABHISHEK MISHRA GYANENDRA DHAR MISHRA 10/10/1998 GEN B.TECH/B.E.Bachelor of Technology (Electranics2 Regular &D/s Communication)90000 Forwd 9 580380501900571 ABHISHEK PANDEY RAKESH PANDEY 29/01/2001 -
Details of Shareholders Whose Shares Are Liable to Be Transfer to Iepf Sr.No Fol Dpid Clid Name 1 Y000004 Yusufali Alibhaikarimj
DETAILS OF SHAREHOLDERS WHOSE SHARES ARE LIABLE TO BE TRANSFER TO IEPF SR.NO FOL DPID CLID NAME 1 Y000004 YUSUFALI ALIBHAIKARIMJEE JAWANJEE 2 M003118 MONICA DILAWARI 3 V003054 V CHANDRA SHEKHAR 4 K003086 KISHAN LAL JANGID 5 D003051 DIPTI P PATEL 6 N003058 NILA A PATEL 7 L003009 LACHMANDAS RAMCHAND 8 R003170 RASIKBHAI K SAVJANI 9 G003039 GITA ASHWIN BANKER 10 H003036 HATIM ARIAAR 11 B003056 BHAVANA KAPASI 12 R003173 RAVI D SAWANT 13 M003083 M A NARAYANAN 14 V003075 VIJAY MALLYA 15 N003055 NAYEEMUDDIN SYED 16 M003088 MAHABALAPPA NANDIHALLI SHANMUKHA 17 A003090 ABDUL AZEEZ 18 K003066 K JEGATHEESAN 19 A003126 ASOKAN KUNJURAMAN 20 0010146 JAGAN NATH PAL 21 0010188 PARTH KHAKHAR 22 0010953 SHIKAR CHAND JAIN 23 A000295 AVTAR SINGH 24 A005583 ARVINDBHAI ISHWAR BHAI PATEL 25 G003898 GUNVANTRAI C MEHTA 26 J000382 JEET SINGH 27 J004092 JAI PARKASH 28 M003185 M P SRIDHARAN 29 M003986 M.V.S. SURYANARAYANA 30 N003999 NAND LAL DHAWAN 31 P003628 PRADNYA PRAKASH PAI 32 P004247 PATEL NANDLAL JAGJIVANDAS 33 R003427 RAJENDRA SINGH NEGI 34 T003414 TRIPTI GUPTA 35 U003427 URMILA GOEL 36 0010970 KIRAN VIJAY JAIPURIA 37 A000311 ANANG UDAYA SINGH DEO 38 A003013 AMARJEET SINGH KAMBOJ 39 A003020 AMRIT PAL MITTAL 40 A003028 ANIL KUMAR CHOPRA 41 A003046 ARUN KR SULTANIA 42 A003066 ASHOK KUMAR GUPTA 43 A003983 ANIL GOYAL 44 A004030 A RAJA BABU 45 A004113 A T THOMAS 46 A004564 A. RAJA BABU 47 A004666 ANIL KUMAR LUKKAD 48 A004677 ASHA DEVI 49 A004915 ASHOK GUPTA 50 A005458 ANURAG JAIN 51 A005468 AGA REDDY VANTERU 52 B000031 BHAIRULAL GULABCHAND 53 B000049 BALMUKAND AGARWAL -
Ap-Rasc 2019)
2019 URSI Asia-Pacific Radio Science Conference (AP-RASC 2019) New Delhi, India 9-15 March 2019 Pages 1-730 IEEE Catalog Number: CFP19E09-POD ISBN: 978-1-5386-8551-8 1/2 Copyright © 2019, International Union of Radio Science All Rights Reserved *** This is a print representation of what appears in the IEEE Digital Library. Some format issues inherent in the e-media version may also appear in this print version. IEEE Catalog Number: CFP19E09-POD ISBN (Print-On-Demand): 978-1-5386-8551-8 ISBN (Online): 978-90-825987-5-9 Additional Copies of This Publication Are Available From: Curran Associates, Inc 57 Morehouse Lane Red Hook, NY 12571 USA Phone: (845) 758-0400 Fax: (845) 758-2633 E-mail: [email protected] Web: www.proceedings.com TABLE OF CONTENTS SPECTRUM MONITOR SYSTEM AT QTT SITE.......................................................................................................................................1 Qi Liu ; Yue Wang ; Ye Liu ; Na Wang ; Feng Liu ; Hao Yan ; Yang Wang RFI PREDICTION FOR QTT RESTRICTED AREA..................................................................................................................................5 Ye Liu ; Qi Liu ; Yang Wang ; Yue Wang PRECISE CLOCK COMPARISON BY MEANS OF SOFTWARE-DEFINED RADIO RECEIVER...................................................9 Yi-Jiun Huang ; Huang-Tien Lin GENERALIZED PROBABILITY DENSITY FUNCTION FOR INTERMODULATION DISTORTION COMPONENTS GENERATED BY POWER AMPLIFIER......................................................................................................................10 -
Estimating the Vacuum Energy Density E
Estimating the Vacuum Energy Density E. Margan Estimating the Vacuum Energy Density - an Overview of Possible Scenarios Erik Margan Experimental Particle Physics Department, “Jožef Stefan” Institute, Ljubljana, Slovenia 1. Introduction There are several different indications that the vacuum energy density should be non-zero, each indication being based either on laboratory experiments or on astronomical observations. These include the Planck’s radiation law, the spontaneous emission of a photon by a particle in an excited state, the Casimir’s effect, the van der Waals’ bonds, the Lamb’s shift, the Davies–Unruh’s effect, the measurements of the apparent luminosity against the spectral red shift of supernovae type Ia, and more. However, attempts to find the way to measure or to calculate the value of the vacuum energy density have all either failed or produced results incompatible with observations or other confirmed theoretical results. Some of those results are theoretically implausible because of certain unrealistic assumptions on which the calculation model is based. And some theoretical results are in conflict with observations, the conflict itself being caused by certain questionable hypotheses on which the theory is based. And the best experimental evidence (the Casimir’s effect) is based on the measurement of the difference of energy density within and outside of the measuring apparatus, thus preventing in principle any numerical assessment of the actual energy density. This article presents an overview of the most important estimation methods. - 1 - Estimating the Vacuum Energy Density E. Margan - 2 - Estimating the Vacuum Energy Density E. Margan 2. Planck’s Theoretical Vacuum Energy Density The energy density of the quantum vacuum fluctuations has been estimated shortly after Max Planck (1900-1901) [1] published his findings of the spectral distribution of the ideal thermodynamic black body radiation and its dependence on the temperature of the radiating black body. -
The Upgraded GMRT : Opening New Windows
The upgraded GMRT : Opening new windows Yashwant Gupta National Centre for Radio Astrophysics Pune India PHISC meeting NCRA Pune 6 Feb 2017 Plan of today's presentation . The upgraded GMRT (uGMRT) – goals & plans . Developments & current status of different aspects of the uGMRT . Status of (phased) release of the uGMRT to the user community The existing GMRT : An Overview . 30 dishes, 45 m diameter each . 12 dishes in a central 1 km x 1 km region (central square) . remaining along 3 arms of Y-shaped array . baselines : ~ 200 m (shortest); ~ 30 km (longest) . Frequency range : . 130-170 MHz . 225-245 MHz . 300-360 MHz . 580-660 MHz . 1000-1450 MHz . max instantaneous BW = 32 MHz . Effective collecting area (2-3% of SKA) : . 30,000 sq m at lower frequencies . 20,000 sq m at highest frequencies . Supports 2 modes of operation : . Interferometry, aperture synthesis . Array mode (incoherent & coherent) The existing GMRT : An Overview . 30 dishes, 45 m diameter each . 12 dishes in a central 1 km x 1 km region (central square) . remaining along 3 arms of Y-shaped array . baselines : ~ 200 m (shortest); ~ 30 km (longest) . Frequency range : . 130-170 MHz . 225-245 MHz . 300-360 MHz 1 km x . 580-660 MHz 1 km . 1000-1450 MHz . max instantaneous BW = 32 MHz 14 . Effective collecting area (2-3% of SKA) : km . 30,000 sq m at lower frequencies . 20,000 sq m at highest frequencies . Supports 2 modes of operation : . Interferometry, aperture synthesis . Array mode (incoherent & coherent) Dedication of the GMRT The Giant Metrewave Radio Telescope was dedicated to the World Scientific Community by the Chairman of TIFR Council, Shri Ratan Tata. -
Concept Note Indo-South African Flagship Programme in Astronomy
Concept Note Indo-South African Flagship Programme in Astronomy Preamble: The Indo-South Africa Flagship Workshop meetings took place at the Indian Institute of Astrophysics, Bangalore on 15th-16th September 2014, and at the Inter-University Centre for Astronomy and Astrophysics, Pune on 19th September, 2014 and were sanctioned by the Departments of Science and Technology of both countries. A list of participants is included in the appendix. 1. Introduction India and South Africa share common aspirations for scientific and technological development, and for the growth of human capital resources. The countries are members of the BRICS consortium, and have a current bi-lateral agreement to foster joint progress. Their shared goals are particularly apparent in the area of astronomy and astrophysics. Indo-African astronomy cooperation began with projects in radio astronomy in Nigeria and Mauritius in the 1980s, and the optical Nainital-Cape Survey, started in 1997. The Inter-University Centre for Astronomy and Astrophysics (IUCAA) joined SALT in 2007, and the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research (NCRA) has recently joined the SKA. Astronomy captures the imagination of people everywhere, and touches a fundamental human desire to understand the universe that surrounds us and our place in it. It provides an ideal way to attract young learners into scientific and technical studies, developing the human capacity for the knowledge-based economy of the future. Its appeal transcends boundaries of class and race and speaks to all members of our societies. The goal of the Indo-South African Flagship Programme in Astronomy is to exploit these basic strengths for the mutual betterment of our peoples. -
Kipac Annual Report 2017
KIPAC ANNUAL REPORT 2017 KAVLI INSTITUTE FOR PARTICLE ASTROPHYSICS AND COSMOLOGY Contents 2 10 LZ Director 11 3 Deputy Maria Elena Directors Monzani 4 12 BICEP Array SuperCDMS 5 13 Zeeshan Noah Ahmed Kurinisky 6 14 COMAP Athena 7 15 Dongwoo Dan Wilkins Chung Adam Mantz 8 16 LSST Camera Young scientists 9 20 Margaux Lopez Solar eclipse Unless otherwise specified, all photographs credit of KIPAC. 22 Research 28 highlights Blinding it for science 22 EM counterparts 29 to gravity waves An X-ray view into black holes 23 30 Hidden knots of Examining where dark matter planets form 24 32 KIPAC together 34 Publications Galaxy dynamics and dark matter 36 KIPAC members 25 37 Awards, fellowships and doctorates H0LiCOW 38 KIPAC visitors and speakers 26 39 KIPAC alumni Simulating jets 40 Research update: DM Radio 27 South Pole 41 On the cover Telescope Pardon our (cosmic) dust We’re in the midst of exciting times here at the Kavli Institute for Particle Astro- physics and Cosmology. We’ve always managed to stay productive, with contri- butions big and small to a plethora of projects like the Fermi Gamma-ray Space Telescope, the Dark Energy Survey, the Nuclear Spectroscopic Telescope Array, the Gemini Planet Imager and many, many more—not to mention theory and data analysis, simulations, and research with publicly available data. We have no shortage of scientific topics to keep us occupied. But we are currently hard at work building a variety of new experimental instru- ments, and preparing to reap the benefits of some very long-range planning that will keep KIPAC scientists busy studying our universe in almost every wavelength and during almost every major epoch of the evolution of the universe, into the late 2020s and beyond. -
Dr. Bharat Ratra
Baylor University and CASPER present: Dr. Bharat Ratra Professor of Cosmology and Astroparticle Physics, Kansas State University Dark Matter, Dark Energy, Einstein's Cosmological Constant, and the Accelerating Universe Abstract: Dark energy is the leading candidate for the mechanism that is responsible for causing the cosmological expansion to accelerate. Dr. Ratra wilI describe the astronomical data which persuaded cosmologists that (as yet undetected) dark energy and dark matter are by far the main components of the energy budget of the universe at the present time. He will review how these observations have led to the development of a quantitative "standard" model of cosmology that describes the evolution of the universe from an early epoch of inflation to the complex hierarchy of structure seen today. He will also discuss the basic physics, and the history of ideas, on which this model is based. Dr. Ratra joined Kansas State University in 1996 as an assistant professor of physics. He was a postdoctoral fellow at Princeton University, the California Institute of Technology and the Massachusetts Institute of Technology. He earned a doctorate in physics from Stanford University and a master's degree from the Indian Institute of Technology in New Delhi. He works in the areas of cosmology and astroparticle physics. He researches the structure and evolution of the universe. Two of his current principal interests are developing models for the large-scale matter and radiation distributions in the universe and testing these models by comparing predictions to observational data. In 1988, Dr. Ratra and Jim Peebles proposed the first dynamical dark energy model. -
ENERGY CONDITIONS and SCALAR FIELD COSMOLOGY by SHAWN WESTMORELAND B.S., University of Texas, Austin, 2001 M.A., University of T
CORE Metadata, citation and similar papers at core.ac.uk Provided by K-State Research Exchange ENERGY CONDITIONS AND SCALAR FIELD COSMOLOGY by SHAWN WESTMORELAND B.S., University of Texas, Austin, 2001 M.A., University of Texas, Austin, 2004 Ph.D., Kansas State University, Manhattan, 2010 A REPORT submitted in partial fulfillment of the requirements for the degree MASTER OF SCIENCE Department of Physics College of Arts and Sciences KANSAS STATE UNIVERSITY Manhattan, Kansas 2013 Approved by: Major Professor Bharat Ratra Copyright Shawn Westmoreland 2013 Abstract In this report, we discuss the four standard energy conditions of General Relativity (null, weak, dominant, and strong) and investigate their cosmological consequences. We note that these energy conditions can be compatible with cosmic acceleration provided that a repulsive cosmological constant exists and the acceleration stays within certain bounds. Scalar fields and dark energy, and their relationships to the energy conditions, are also discussed. Special attention is paid to the 1988 Ratra-Peebles scalar field model, which is notable in that it provides a physical self-consistent framework for the phenomenology of dark energy. Appendix B, which is part of joint-research with Anatoly Pavlov, Khaled Saaidi, and Bharat Ratra, reports on the existence of the Ratra-Peebles scalar field tracker solution in a curvature-dominated universe, and discusses the problem of investigating the evolution of long-wavelength inhomogeneities in this solution while taking into account the gravitational back-reaction (in the linear perturbative approximation). Table of Contents List of Figures vi Acknowledgements vii Dedication viii 1 Energy conditions in classical General Relativity1 1.1 Introduction . -
Supernova Ia Constraints on a Time-Variable Cosmological
THE ASTROPHYSICAL JOURNAL, 532:109È117, 2000 March 20 ( 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A. SUPERNOVA Ia CONSTRAINTS ON A TIME-VARIABLE COSMOLOGICAL ““ CONSTANT ÏÏ SILVIU PODARIU AND BHARAT RATRA Department of Physics, Kansas State University, Manhattan, KS 66506 Received 1999 September 2; accepted 1999 November 3 ABSTRACT The energy density of a scalar Ðeld / with potential V (/) P /~a, a[0, behaves like a time-variable cosmological constant that could contribute signiÐcantly to the present energy density. Predictions of this spatially Ñat model are compared to recent Type Ia supernova apparent magnitude versus redshift data. A large region of model parameter space is consistent with current observations. (These constraints are based on the exact scalar Ðeld model equations of motion, not on the widely used time-independent equation of state Ñuid approximation equations of motion.) We examine the consequences of also incorporating constraints from recent measurements of the Hubble parameter and the age of the uni- verse in the constant and time-variable cosmological constant models. We also study the e†ect of using a noninformative prior for the density parameter. Subject headings: cosmology: observations È large-scale structure of universe È supernovae: general 1. INTRODUCTION 4. The need for mild antibiasing to accommodate the excessive intermediate- and small-scale power predicted in Current observations are more consistent with lower- the COBE DMRÈnormalized Ñat constant-" CDM model density cosmogonies dominated by cold dark matter with a scale-invariant spectrum (see, e.g., Cole et al. 1997). (CDM). For recent discussions see, e.g., Ratra et al.