1.3m Telescope Current Status and Future Up gradation Plans
Mukeshkumar Jaiswar 1, TS Kumar 1 and Shobhit Yadav 1
1 ARIES, Manora Peak, Nainital-263001
Corresponding Author(s): mukesh@aries.res.in, kumar@aries.res.in
Abstract: 1.3m DFM Telescope has been installed at ARIES Devasthal site in the year 2010. It is more than 10 Years old telescope most of its component has been...
Abstract
With the advanced technology in electrical/electronic (EE) systems and its applications in the field of Astronomy and Space Sciences, the functionality of EE systems and instruments in an intended/unintended Electromagnetic (EM) environment is crucial. This is ensured by conducting EMI (Electromagnetic Interference) and EMC (Electromagnetic Compatibility) testing. In a product...
The coming decade in astronomy focuses on large wide field imaging and spectroscopic surveys. At present, no wide field imaging or multi-object spectroscopic facilities extend to the UV region, which represents an important window into a wide variety of astrophysical problems. Combining a large focal area with a simple and efficient optical design, the Indian Spectroscopic and Imaging Space...
The Thirty Meter Telescope (TMT) is a joint venture of scientific institutions in Canada, China, India, Japan and the US to build a 30-m diameter optical–infra-red telescope. As part of India's contribution, the India-TMT Coordination Centre (ITCC) is developing various sub-systems needed for the telescope in collaboration with Indian industrial partners. The TMT will be a Ritchey-Chrétien...
The Wide Field Optical Spectrometer (WFOS) is an instrument under development for the first-light operation of the Thirty Meter Telescope (TMT), which will provide high throughput across the entire wavelength range of 310-1000 nm, including the extreme blue and red wavelengths. In order to achieve that, the design has a two-channel spectrograph layout, a red and a blue channel. Each channel...
Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES) is an infrared instrument for Keck-II, being built by a consortium including UC Santa Cruz, UC Irvine, UCLA, the Indian Institute for Astrophysics, Keck Observatory, and Caltech. SCALES will have an Integral Field Spectrograph (IFS) to characterize the planetary atmosphere and a high-contrast Imaging Channel to detect...
The FUV (900-1800 Å) is the richest part of the spectrum in terms of emission lines – O VI (1032/1038 Å) and C IV (1548/1550 Å) from hot gas, C III (977 Å) and N III (1750 Å) from warm gas, and the Lyman and Werner bands of molecular hydrogen from cold gas. We are building a spectrograph (TINI) to map the extended objects observed by UVIT in the emission lines of atoms and molecules. The...
Dome Automation of ARIES Schmidt Telescope
Shobhit Yadava 1, TS Kumar 1
1 Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital-263001, India
Corresponding Author(s): shobhit@aries.res.in, kumar@aries.res.in
Abstract: Schmidt telescope dome comprises of rotating steel structure with shutter and presently operating in manual mode. We describe here the...
Cross-correlation of two-dimensional digital images is fundamental to solar adaptive optics computations. It can be used in a simple tip-tilt correction system as well as in correlating sub-aperture images of a Shack-Hartmann wave-front sensor. While the software-based optimized cross-correlations may be sufficient when a small number of sub-apertures are used, hardware-accelerated (FPGA)...
Polarimeters are useful devices that help understand the polarization state of electromagnetic radiation. As such, they find applications in astronomy, medicine, crystallography, ellipsometry, remote sensing, and so on. Over the past few decades, IIA has built several polarimeters for astronomical observations. Continuing this activity, we have developed a full-stokes polarimeter that can be...
Radio Interferometry refers to the process of combining signals from multiple antennas to form an image of the radio source in the sky. Radio-astronomical signal processing using array telescopes is computationally challenging and poses strict performance and energy-efficiency requirements. The GMRT is one of the largest arrays with many antennas working in the metre wavelength. The ongoing...
A third-generation Adoptive optics instrument named SCALES, Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy, is being planned for commissioned on the W. M. Keck Observatory in near future. It has an integral field spectrograph (IFS) and a diffraction-limited infrared imaging channel to discover and spectrally characterize the directly imaged exoplanets. The imaging channel is...
The Spectroscopic Investigation of Nebular Gas (SING) payload is a near ultraviolet (NUV) imaging spectrograph, which is designed to operate in the wavelength range from 1400 Å to 2700 Å, with a spectral resolution of ~2 Å at 2200 Å. This spectrograph is designed to map the astrophysical spectrum at moderate spatial and spectral resolution in the NUV from a stable Chinese modular space...
Will discuss about various antenna design concepts used for GMRT upgrade.
The antenna aperture efficiency is a recurrence of illumination efficiency (or taper efficiency) and spillover efficiency and phase efficiency. The illumination efficiency depends on the taper of the feed and spillover depends on after taper how the radiation pattern falls and also the back lobes. Similarly, the ground temperature mostly depends on spillover temperature. The objective of this...
Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES) is a thermal infrared instrument for Keck-II to be built at W. M. Keck Observatory. Functionally, the instrument layout is divided into three parts, i.e., Fore-optics, IFS module, and Imaging Channel. The Imager filter wheel Mechanism is a part of the Imaging channel.
The Imager Filter Wheel Mechanism is a...
A real-time Radio Frequency Interference (RFI) filtering system has been commissioned and released for the Upgraded GMRT (uGMRT) users. Over the last couple of years, there has been a significant increase in the usage of the system. The system helps filter broadband powerline RFI, a dominant source of interference at frequencies below 800 MHz. This system is the first to be implemented in a...
A 32-input, 32 MHz bandwidth, 5-beam, aperture array beamformer has been designed and implemented as part of the Expanded GMRT (eGMRT) proposal. This prototype beamformer development was a precursor to a wideband beamformer (300 MHz bandwidth) which is currently being designed. We present the basic architecture and the optimizations to implement these prototype correlator and beamformer...
Sample - Stratospheric Altitude Microbiology Probe For Life Existence - A Balloon Borne Payload System To For Cosmic Dust Collection In The Stratosphere
Authors:
1. Rashi Srivastava, Central University of Karnataka
2. Dr. Margarita Safonova, Indian Institute of Astrophysics
3. Dr. Binukumar G. Nair, Indian Institute of Astrophysics
4. Bharat Chandra P, Indian Institute of...
The Upcoming side port imager for 3.6m telescope is having a subsystems of Main structure, filter wheel, turret camera mount etc. the filter wheel in side port instrument is measuring Ø600mm and carrying 16 filters different sizes arranged in outer periphery of wheel and perpendicular to disk. the turret Camera mount is design to stare a different camera in same instruments. the Poster is...
The Wide Field Optical Spectrometer (WFOS) is an instrument under development for the first-light operation of the Thirty Meter Telescope (TMT), which will provide high throughput across the entire wavelength range of 310-1000 nm, including the extreme blue and red wavelengths. WFOS is positioned on the Nasmyth platform of TMT and measures ~6m x 6m x 6m in size. The total mass is around 40...
High-Resolution Optical Spectrograph (HROS) is one of the proposed second-generation seeing limited instruments on the Nasmyth platform of the Thirty Meter Telescope (TMT). It is a workhorse instrument for TMT in the wavelength band from UV to Near Infrared. We present a conceptual design of a high-resolution optical spectrograph for TMT. The design uses strategies of successful spectrographs...
G/Tsys is define the ratio of gain (K/Jy) and the system temperature. The system temperature (Tsys) depends on ground temperature, sky temperature, and receiver temperature. Receiver temperature primarily depends on the noise of the low noise amplifier (LNA). The objective of this work is to design a three-stage LNA in the L band (1 GHz-1.7 GHz) with a noise temperature of less than 40 K and...
