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9/15/19, 9:00 AM
Welcome Remarks -Director, IIA, Bengaluru
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9/15/19, 9:10 AM
"L&T's contribution to Mega Science Projects"-Ravi Kataria, Head Business Development & Marketing, Missiles & Aerospace Business, Larsen & Toubro Limited.
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9/15/19, 10:00 AM
“Square Kilometre Array”-Y. Gupta, Centre Director,NCRA
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9/15/19, 10:30 AM
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9/15/19, 11:45 AM
INTRODUCTION-
SPDC is a nonlinear instant optical process that converts one photon of higher energy (namely, a pump photon), into a pair of photons (namely, a signal photon, and an idler photon) of lower energy, in accordance with the law of conservation of energy and law of conservation of momentum. It is an important process in quantum optics, for the generation of entangled photon pairs,...
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9/15/19, 12:00 PM
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The Infrared Astronomy Group (IR group) of TIFR has been developing near-infrared (NIR) instruments for ground based Indian telescopes, far-infrared instruments for TIFR 100-cm balloon borne telescope and has recently developed space platforms via IRSIS & other projects. This
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talk will present an overview of NIR astronomical cameras developed by the IR group which have been... -
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Reducing power supply noise is one of the essential steps in order to implement precision and reliable instrumentation. However, commercial power supplies are usually insufficient for the purpose of astronomical instrumentation. They usually lack noise characterization over a range of frequencies and also over a range of applied load. In this regard, we have defined a method of estimating...
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9/15/19, 4:45 PM
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9/15/19, 5:00 PM
Challenges in Designing a Digital Spectrometer for Detection of Signals from CD/EoR, Girish B. S, RRI
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9/15/19, 5:15 PM
The Expanded GMRT (eGMRT) is a proposal to look at three expansions to the
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GMRT - increasing the field of view, increasing angular resolution and
improving the sensitivity to the extended radio emission. In this talk, we
would focus on increasing the field-of-view using Focal Plane Array (FPA)
and the ongoing development of the FPGA-based prototype FPA beamformer. A
prototype is being... -
9/15/19, 5:30 PM
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9/15/19, 9:45 PM
“Square Kilometre Array”-Y. Gupta, Director,NCRA
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9/16/19, 9:00 AM
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97. “The 3.6 m DOT electronics: Maintenance and future upgradation strategies”- Dr Kumar T. S. ARIES9/16/19, 2:30 PM
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105. “Developmental status of X-ray polarization sensitive mirrors”-Mr Panini Singam, IIA, Bengaluru9/16/19, 4:35 PM
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9/17/19, 6:00 AM
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We have developed a 21 cm receiver based on a horn antenna and RTL SDR, and successfully detected the 21 cm line emission from different directions. The design details and results will be presented in this poster.
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Modern FPGAs are revolutionizing the digital system designs with built-in analog to digital converters (RFSoC), floating point DSP processors and with high-level programming tools. We have planned to build a versatile digital receiver, namely the accelerated tile processor, by exploiting these FPGA features. We will present here the salients features of the digital processing architecture...
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Adaptive optics is an inevitable technology in any modern large ground-based telescope. It involves use of corrective optical elements within the telescope to compensate for the deleterious effects of the Earth's atmospheric turbulence on the image quality. Indian Institute of Astrophysics is deliberating on building a 2 m class large solar telescope (The National Large Solar Telescope) and a...
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LIGO (Laser Interferometer for Gravitational-Wave Observatory) is one of the technological marvel involving world's advanced technology. It has overcome many difficulties to achieve one of the finest scientific measurements ever taken precisely. Its extreme engineering can be divided into different domains including mechanical structures, optics, civil engineering, physics, geology,...
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SARAS is an ongoing experiment aiming to detect the redshifted global 21-cm signal expected from Cosmic Dawn (CD) and the Epoch of Reionization (EoR). Standard cosmological models predict the signal to be present in the redshift range z ~6-30 corresponding to a frequency range of 40-200 MHz, and as a spectral distortion of amplitude 20-200 mK to the cosmic microwave background. Design of a...
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Design considerations and challenges of integrating on-chip antennas in nanoscale CMOS technology at millimeter-wave (mm-wave) to achieve a compact front-end receiver for 5G communication systems. Solutions to overcome these challenges are offered and realized in digital 28-nm CMOS. A monolithic on-chip antenna is designed and optimized in the presence of rigorous metal density rules and other...
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ARIES 3.6 m optical telescope at Devasthal is enclosed in steel building with rotating dome. Dome comprises of upper rotating cylindrical steel structure and lower fixed dome support structure. Rotating dome being a fabricated structure of about 16.5m mean diameter involved lot of welding and a clearance of about 150 mm was kept between fixed dome structure outer wall and rotating dome outer...
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An Active Hydrogen Maser (AHM) unit was recently installed and upgraded the frequency standard of the Giant Metrewave Radio Telescope (GMRT) observatory. The ultra-low phase noise and stability characteristics of this AHM have facilitated the observatory to carry out Very Long Baseline Interferometry (VLBI) observations. The outputs from the AHM are used as a precision frequency reference for...
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The GROWTH (Global Relay of Observatories Watching Transients Happen) – India telescope at Hanle in Ladakh is India’s first effort towards a fully robotic telescope. It is also the first one dedicated for a rapid follow-up of transient events in the universe. Mounted in between the CCD camera and the output port of the GROWTH telescope is a filter wheel which houses 6 filters whose centers are...
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ABSTRACT
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The National Large Solar Telescope (NLST) is a proposed 2 m class telescope dedicated for making high resolution solar observations. A suitable site has been identified at Merak village, near Pangong Tso Lake in Jammu & Kashmir state, India.
It has been observed that installing a telescope near the lake produce good images during the day time observations. At the same time the... -
The National Large Solar Telescope (NLST) is proposed to be built in India which will be one of the most powerful telescopes to study the Sun. It will have a 2m size primary mirror. The primary mirror needs a removable cover to carryout two important functions: first one is to protect primary mirror from environmental conditions when the telescope is not in operation and second one is to...
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To cater the need of growing astronomical community of India, there is a proposal to realize a 10-12m size optical-NIR telescope, equipped with state of the art back-end instruments. With the current technology, it is not possible to realize a monolithic primary mirror required for such a large telescope. This necessitates use of smaller mirror segments aligned to act like a single mirror....
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The Solar ultraviolet imaging telescope (SUIT) onboard Aditya L1 is an upcoming space telescope to study the Sun in near UV (200nm - 400nm) range and will be placed in a halo orbit around Sun-Earth L1 point. The mechanical systems design of SUIT involved considering crucial factors of structural integrity to withstand launch loads, meeting temperature specifications within the payload,...
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The Thirty Meter Telescope (TMT) adopts a recently developed technology known as Stressed Mirror Polishing (SMP) for the polishing of its 492 glass blanks. In this process, first the meniscus type spherical shape glass blanks are converted in to the conjugate of desired aspheric shape by the application of forces around the edges using warping arms. This is followed by spherical polishing in...
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The 3.6 m optical telescope of ARIES is installed at Devasthal site for astronomical observations. Need for additional protection of telescope apart from that provided by its dome was felt to avoid any minute water leaks from dome roof, accumulation of dust on the mirrors and also to minimize effect of humidity on telescope during rainy season. A telescope cover structure has been designed to...
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We at TIFR, have initiated the development of a Multi-Object Infrared Spectrometer (MOIS) using a configurable multi-slit arrangement for a large aperture Indian optical/infrared telescope. In order to retain flexibility, avoid design and operational issues involved in using focal plane masks for multi-object spectroscopy we present here the first design concepts for the Configurable Slit...
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We have developed multilayer mirrors which can reflect X-rays are Brewster angle (~$45^o$) and hence are sensitive to X-ray polarization. We have fabricated several $W/B_4C$ multilayer mirrors using magnetron sputtering technique with different parameters, optimizing the performance and sensitivity at soft X-ray region (photon energy < 1 keV). We have developed a conceptual design for a...
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Dual polarized broadband dipole antenna feed with conical reflector for uGMRT
Hanumanth Rao B, Suresh Kumar S
GMRT Observatory, NCRA-TIFR, Post Bag 3, Ganeshkhind, Pune 411007, Maharashtra, India
(hanuman, skumar@gmrt.ncra.tifr.res.in )The Giant Metrewave Radio Telescope (GMRT) is an international facility for Radio Astronomy, operational since...
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Engineering challenges in realization of Visible Emission Line Coronagraph on-board Aditya L1
Nagabhushana S, Kamath P U, , Kathiravan S, Amit Kumar, Natarajan V, Pawan Kumar S Venkata Suresh Narra, Shalabh Misahra,Chavali Sumana, Varun kumar, Bhavana Hegde, Jagdev Singh, Raghavendra Prasad B
Indian Institute of Astrophysics, Bangalore
Visible Emission Line Coronagraph (VELC) on board...
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Now a days General Purpose GNU Linux Operating Systems employed in variety of applications from digital gadgets to avionics, flight navigation systems and nuclear power plant control applications. Monolithic kernel architecture of Linux OS makes it not suitable for safety and time critical applications. In such cases, to convert the GPOS into strict timing constraints, several approaches were...
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Abstract:
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To keep in pace with the emerging trends in scientific research and cater to the need of growing Indian astronomical community, a need is strongly felt for realising an 8-10 meter size optical telescope in India. Construction of such a large optical telescope size is possible only when the primary mirror is made of large number of small mirror segments. In segmented mirror... -
Radio Telescope Operating at Low Frequency suffer from various commercial transmission outside the observing ban. Low Noise Amplifier being the first device to receive the Radio signals easily get saturated due to the out of band transmission and become impossible to carry out useful Radio Astronomical observation. In addition to saturation the out of band Interfering signals produce in band...
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Giant Meterwave Radio Telescope (G.M.R.T) back-end system is installed in three different
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locations correlator room, new receiver room and Active Hydrogen Maser (A.H.M.) room there
are many critical electronics components whose electronics circuits are susceptible to variations
in environmental parameters such as temperature, humidity and supply voltage etc. Hence a
real time 24/7 monitoring... -
Optical imaging has been the driving force of astrophysical research, historically driven by the ground based telescopes, which still drives the ground based astronomy, with the recent surveys like the SDSS, PANSTARRS as well as the upcoming LSST. IR and UV wavelengths obtained from space are complimentary to the ground facilities. With the upcoming JSWT to compliment the IR wavelength range...
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Traditionally 1420 MHz line emission is used to study the Doppler Spectrum of the 21-cm hyper fine line of interstellar atomic hydrogen.This radiation comes from the transition between the two levels of the hydrogen 1s ground state, slightly split by the interaction between the electron spin and the nuclear spin. We have modified the old dish antenna and the receiver system to study the...
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Nanosatellites based experiments are having an exponential growth in recent times. These satellites use miniaturised components that consumes less power. Attitude control of Nanosatellites depends upon various sensors such as sun sensor, nadir sensor, inertial measurement unit and others. All these sensors need to be qualified/characterised before the actual flight. Academic institutions and...
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The proposed India's National Large Optical Telescope and the Mauna Kea Spectroscopic Explorer are optically designed to have nearly identical hyperbolic primary of 60 segments of size 1.44m, delivering a circumscribed 11.25 meter aperture. In order to get the best image quality, all the segments in the primary mirror need to be aligned in the telescope for a monolithic profile. Any...
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Cosmic Dawn to Epoch of reioniztion is a period which began in the history of universe, with the formation of stars for the first time and ended in transforming completely the neutral state of hydrogen to ionized state. Thermal history of the universe during this era is currently poorly understood. The 21cm line of neutral hydrogen is considered as a power tool to probe this era to gain better...
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In general a majority of optical system used conventional spherical surfaces as it is easy to make and characterize. Though advantages of using non-conventional surfaces such as aspheric, freeform are being well known since primitive era of geometric optics. The recent progress in high precision engineering technology continuously demanding these surfaces in order to meet stringent optical...
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A NUV (1800-3000 Å) spectrograph has been designed to investigate the diffuse nebulae and other extended sources. The spectrograph has been designed to fit into a 6U form factor (350 × 240 × 150 mm) Cubesat and will be launched into a low-earth orbit (LEO). Optical design, optimization, and tolerancing have been completed. Designs of mounting elements are in progress; stringent volume...
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Modern Engineering Trends in Astronomy – 2019
Sunday 15 September 2019 - Tuesday 17 September 2019, BengaluruAuthors : Mr. Irappa M. Halagali, irappa@gmrt.ncra.tifr.res.in , Mr. Ajith Kumar B. , ajit@ncra.tifr.res.in , and
Prof. Yashwant Gupta, ygupta@ncra.tifr.res.inAbstract for Poster :
“Heat and Power Management of new era Electronic Systems”
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Abstract for META2019
Poster Title : Prototype for raw voltage recording in the backend system of the upgraded GMRT
Author list : Shelton Gnanaraj, Mekhala Muley, Harshavardhan Reddy Suda, Sandeep Chaudhari, Sanjay Kudale, Irappa Halagalli, B. Ajith Kumar, Yashwant Gupta.
Go to contribution pageThe GMRT Wideband Backend (GWB) combines the Baseband signals of all antennas and gives out the visibilities in each... -
Giant Meterwave Radio Telescope (GMRT) is an array telescope of 30 antennas each of 45 meter in diameter located at Khodad, Pune. The upgraded GMRT have a seamless coverage over the frequency band ( 120 MHz – 1450 MHz ) with high dynamic radio receivers. The Radio frequency interference to a radio telescope is a permanent threat and needs continuous monitoring and mitigation to protect the...
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Low frequency radio telescope observations suffer from time varying interference from the neighborhood. We plan to extract radio spectrum features through a statistical analysis and develop machine learning techniques to make predictions about available good-band regions for an observation schedule. We consider routine monitoring of signals across a broadband and use noise characteristic...
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G/Tsys defines the sensitivity of a radio telescope and is an important figure of merit. It is important to know the overall antenna efficiency and system noise temperature of the telescope in order to calculate the G/Tsys. In order to calculate the G/Tsys for uGMRT bands, a Software was developed in-house at GMRT-NCRA, named as RASCAL (Reflective Antenna Sensitivity CALculator).
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This paper... -
T100 is a TIFR 100 cm balloon borne telescope which is used for the FIR observation with the Japanese Fabry Perot Spectrometer (FPS) as a focal plane instrument. FPS is tuned to the [CII] line at ~158 micron to study Galactic star forming regions. T100 along with FPS is being flown regularly from TIFR Balloon Facility, Hyderabad. The FPS consists of two Fabry Perot Interferometer, one with...
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Authors: Shri. Sandeep Chaudhari, Shri. Prakash Hande, Mrs. Sweta Gupta, Shri. Navnath Shinde, Shri. Abhijeet Dhende, Shri. S. Harshavardhan Reddy, Shri. Ajay Vishwakarma, Shri. Ajith Kumar, Prof. Yashwant Gupta
The signal flow chain of a typical radio telescope receiver consists of various sub-systems viz. feeds, front-end electronics, signal conditioning circuits, signal transportation to...
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RFoF technology enables a path for low loss signal transmission over longer distances, carry huge bandwidth of data, and is also immune to electrical noise. The paper discusses the technology, design, and methods for implementing it for phased array antennas application. The RFoF backplane is very much compact and suitable for phased array antennas, these replace the need for bulky RF cables,...
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The Indian SWAN (Sky Watch Array Network) initiative aims to significantly enhance Indian observing capabilities in radio, and importantly, also to sustainably build & nurture future generations of talented radio astronomers in India to take up the challenges and lead in exciting research in astronomy. The SWAN focus is to design, develop and use a wide-band interferometric array of antenna...
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TMT is a ground-based optical/infrared telescope. The telescope utilizes a Ritchey-Chrétien optical design with 30-meter hyperboloid f/1 primary mirror. As it is difficult to make a monolithic mirror of such dimension the primary mirror is subdivided into 492 hexagonal segments each having a diameter of 1.44 meter from edge to edge. The primary mirror is having 6-fold symmetry and hence they...
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Abstract:
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To keep in pace with the emerging trends in scientific research and cater to the need of growing Indian astronomical community, a need is strongly felt for realising an 8-10 meter class optical telescope in India. Construction of such a large size optical telescope is possible only when the primary mirror is made of large number of small mirror segments. In segmented mirror... -
1.04M aperture optical telescope named as Sampurnanand has been installed as the one of the main observing facility in optical domain at, Aryabhatta Research Institute of Observational Sciences Manora Peak, Nainital. The 104-cm, f/13 telescope produce a field of around 45 arcmin with corrector at the cassegrain end. the total research output of the 104cm Sampurnanand Telescope reaches nearly...
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The Expanded GMRT (eGMRT) is a proposal to look at three expansions to the
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GMRT - increasing the field of view, increasing angular resolution and
improving the sensitivity to the extended radio emission. In this talk, we
would focus on the testing of multi-element, multi-beam beamformer using
the
144-element Focal Plane Array (FPA) procured from ASTRON.
The preliminary tests for the beamformer... -
We describe here the electronics aspects of the 3.6 m Devasthal Optical Telescope (DOT) and discuss the strategic approach adopted by the ARIES electronics engineering team for maintaining and upgrading the telescope. The construction of the 3.6 m DOT was completed at the AMOS Factory in Belgium in the year 2012 and the telescope was partially disassembled into its sub-systems and transported...
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Abstract: Reliability means the probability of the system to perform a required function without failure under stated conditions for a stated period of time. Reliability study is essential for electronic systems. Hence, this study is applicable to a radio telescope receiver. Giant Metrewave Radio Telescope’s (GMRT) receiver system consists front end (FE), antenna base receiver (ABR),...
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Broadband Radio Frequency Interference (RFI) is one of the main reasons for corruption of astronomical data observed using the Upgraded GMRT (uGMRT) at frequencies below 700 MHz. A real-time RFI excision system, operating on Nyquist-sampled digital time-series per antenna and polarization, has been implemented as part of the GMRT Wideband Backend (GWB). The system, implemented on FPGA,...
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Authors: Shri. Sandeep Chaudhari, Mrs. Mekhala Muley, Mrs. Sweta Gupta, Shri. Irappa Halagali, Shri. Navnath Shinde, Shri. Abhijeet Dhende, Shri. Ajith Kumar, Prof. Bhalchandra Joshi, Prof. Jayaram Chengalur, Prof. Yashwant Gupta
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The single dish telescope is a basic building element of radio astronomy that can be used for trying new concepts like FPA (Focal Plane Array), Pulsar & VLBI... -
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