G.N. Rajasekhara Girish Kumar Beeharry Mauritius Radio Telescope The CALLISTO spectrograph in Mauritius.

Slides:



Advertisements
Similar presentations
T-3 Histograms. Histogram Basics A histogram is a special type of bar graph that measures the frequency of data Horizontal axis: represents values in.
Advertisements

The Cylinder Radio Telescope: Observing the CMB Paul A. Fleiner Ph 70 Popular Presentation May 10, 2011.
X-ray Emission due to Charge Exchange between Solar Wind and Earth Atmosphere on September Hironori Matsumoto (Kobayashi-Maskawa Institute, Nagoya.
EXAMPLE 1 Making a Frequency Table Science The numbers of named stars in a group of 34 constellations are listed below. Make a frequency table of the data.
Soobash Daiboo Arvind Nayak N Udaya Shankar Girish Kumar Beeharry Mauritius Radio Telescope Raman Research Institute The Southern Sky at MHz: Latest.
Page 1 18-OCT-2004 RHESSI Data Analysis Workshop RHESSI Reuven Ramaty High Energy Solar Spectroscopic Imager Use or disclosure of data contained on this.
The Green Bank Telescope a powerful instrument for enhancing ALMA science Unblocked Aperture Low sidelobes gives high dynamic range Resistance to Interference.
Solar radio observations in Belgium C. Marqué, F. Clette, J.-L. Dufond, A. Ergen, J. Magdalenic, B. Dabrowski Royal Observatory of Belgium 2 nd LOFAR Solar.
Technical improvements and possibilities to observe solar oscillations with the small Metsähovi radiotelescope Juha Kallunki Metsähovi.
CALLISTO Double - Heterodyne - Frequency Agile - Radio - Spectrometer EuroSETI Symposium Heppenheim March 26…28th 2004 Christian Monstein ETH Zürich Compound.
Temporal Variability of Gamma- Ray Lines from the X-Class Solar Flare of 2002 July 23 Albert Y. Shih 1,2, D. M. Smith 1, R. P. Lin 1,2, S. Krucker 1, R.
Solar corona observations at decameter wavelengths Artem Koval Institute of Radio Astronomy Kharkov, Ukraine.
4th LOFAR solar KSP meeting Potsdam4th LOFAR KSP meeting Potsdam 2010 November 8-9 4th LOFAR KSP meeting Potsdam 2010 November 8-9 NRH and LOFAR Scientific.
What’s Going on in Canada?
Rachel Klima (on behalf of the MASCS team) JHU/APL MASCS/VIRS Data Users’ Workshop LPSC 2014, The Woodlands, TX March 17,2014 MASCS Instrument & VIRS Calibration.
SOFIA — The Observatory open cavity (door not shown) TELESCOPE pressure bulkhead scientific instrument (1 of 7) Scientist work stations, telescope and.
Solar dynamic spectra C. Vocks and G. Mann 1. Spectrum of the quiet Sun: First results 2. How to obtain spectra: Beamformed data 3. Single station spectra.
Very Low Frequency Astronomy
Notebook Telescope 1m BPF AR 5000 BPF FFT LO 21cm (1.42 GHz) IF 1 ≈152 MHz 10.7 MHz H2-Converter PSU COM RS-232 L-Band (Neutral Hydrogen, 21 cm / 1421.
Assessment of RFI measurements for LOFAR Mark Bentum, Albert-Jan Boonstra, Rob Millenaar ASTRON, The Netherlands Telecommunication Engineering, University.
Dale E. Gary Professor, Physics, Center for Solar-Terrestrial Research New Jersey Institute of Technology 1 03/15/2012Preliminary Design Review.
Ionospheric-magnetospheric VLF Wave Propagation: RPI/IMAGE-HAARP Correlative Study RPI/IMAGE-HAARP Correlative Study V. Paznukhov, B. Reinisch, G. Sales,
2nd LOFAR KSP meeting Potsdam 2009 July Experience of NRH observations: which benefit for LOFAR KSP ? A. Kerdraon Observatoire de Paris - LESIA -
Solar observation modes: Commissioning and operational C. Vocks and G. Mann 1. Spectrometer and imaging modes 2. Commissioning proposals 3. Operational.
Creating Flash Movies for Pocket PC Presentation by: JOSE BARRIGA.
Polarization Surveys with the DRAO 26-m Telescope at 1.4 GHz Maik Wolleben, T. Landecker, O. Davison Dominion Radio Astrophysical Observatory W. Reich,
Hvar Observatory Faculty of Geodesy Kačićeva 26, Zagreb.
RHESSI and Radio Imaging Observations of Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD G. Trottet, Observatoire.
Interplanetary Scintillation Observations of the Solar Wind Using SWIFT and Upgraded STEL Multi-station System M. Tokumaru, K. Fujiki, and T. Iju (STEL,
Lancaster University Department of Communication Systems Skymap at 38.2 MHz as Measured by IRIS Steve Marple.
Mileura Widefield Array – Low Frequency Demonstrator MHz * Currently in “Early Deployment” phase Goal: HI at redshift 6 to 17.
Effect of Geomagetic Activity on Cosmic Ray Muon Rate Mendon High School Regents Physics Honors Period 9 Class A group of Honors physics students plotted.
THE MURCHISON WIDEFIELD ARRAY: FROM COMMISSIONING TO OBSERVING D. Oberoi 1,2, I. H. Cairns 3, L. D. Matthews 2 and L. Benkevitch 2 on behalf of the MWA.
Girish Kumar Beeharry Mauritius Radio Telescope An African Low Frequency E-vlbi.
Academia Sinica National Taiwan University AMiBA System Performance Kai-yang Lin 1,2 and AMiBA Team 1,2,3 1 Institute of Astronomy and Astrophysics, Academia.
SH43A-16 The Green Bank Solar Radio Burst Spectrometer T. S. Bastian National Radio Astronomy Observatory 520 Edgemont.
Final Presentation By Matthew Lewis 17 th March 2006 “To Determine the Accuracy that GOES True Numbers can Reproduce the Full X-ray Spectrum of the Sun”
STEREO: Beyond 3D. Why the Sun? The sun provides energy for the development of life on our planet. Our orbit looks calm and peaceful, but there is nothing.
TYPE IV BURSTS AT FREQUENCIES MHz V.N. Melnik (1), H.O. Rucker (2), A.A. Konovalenko (1), E.P. Abranin (1), V.V. Dorovskyy(1), A. A. Stanislavskyy.
SRS Data Examples A brief overview of some types of radio emissions observed on the Solar Radio Spectrograph.
Notes 5.2Histograms A frequency table groups large amounts of data into intervals. The frequency is the number of times an item occurs within an interval.
2.1 Frequency distribution Histogram, Frequency Polygon.
Introduction to Radio Jove SSL 2006A Mel Blake. Project Summary 1.Construct a Receiver sensitive to 20MHz radiation 2.Construct an telescope to receive.
Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Observing Scripts Basic.
PR-2 Radar in Aguadilla Ricardo Ríos Olmo Advisor: Dr. José Colom.
Potential of a Low Frequency Array (LOFAR) for Ionospheric and Solar Observations ABSTRACT: The Low Frequency Array (LOFAR) is a proposed large radio telescope.
CODALEMA A Cosmic Ray Radio Detection Array ICRC 2007, 3-11 July Merida, Mexico CODALEMA A Cosmic Ray Radio Detection Array Didier Lebrun, LPSC Grenoble.
SOLAR RADIO PHYSICS RESEARCH IN INDONESIA
A Sample IHY 2007 Instrumentation Proposal J. Kasper, B. Thompson, N. Fox.
Ganghua Lin Huairou Solar Observating Station,NAO,CAS.
Solar Astronomy Space Science Lab 2008 Pisgah Astronomical Research Institute.
Global Structure of the Inner Solar Wind and it's Dynamic in the Solar Activity Cycle from IPS Observations with Multi-Beam Radio Telescope BSA LPI Chashei.
Yuki Takahashi Radio Interferometer Observatory Near the Lunar South Pole Yuki D. Takahashi (U. C. Berkeley) International Lunar Conference.
Telescopes B A Kagali. Galileo Moon through galileo tel.
Solar observations with single LOFAR stations C. Vocks 1. Introduction: Solar Radio radiation 2. Observations with single LOFAR stations 3. Spectrometer.
Station-4 MuID System: Status Ming X. Liu Los Alamos National Lab 1/7/091E906 Collaboration Meeting.
STCE Meeting – 06/06/2011 Summary of the « Radio Science Workshop » Hervé Lamy (BISA) Petra Van Lommel (STCE)
Radio Wave Propagation
ALL ABOUT THAT DATA UNIT 6 DATA. LAST PAGE OF BOOK: MEAN MEDIAN MODE RANGE FOLDABLE Mean.
Andreas Horneffer for the LOFAR-CR Team
Chengming Tan National Astronomical Observatories
SOFIA — The Observatory
Using a Radio Telescope
AAVS1 Calibration Aperture Array Design & Construction Consortium
Observing and Data Reduction
EVLA Project Peter Napier
MWA “burst mode”: Nov 2008 Solar 32 T Observations
Data Taking Plans for 32T and 128T
Antenna Analyzer EA4FRB
Antenna Analyzer EA4FRB
Presentation transcript:

G.N. Rajasekhara Girish Kumar Beeharry Mauritius Radio Telescope The CALLISTO spectrograph in Mauritius

Outline · First Antenna · Back end · Commissioning · First flare · Subsequent flares · Observations from other CALLISTOs · Future work

The First Antenna Broad band logarithmic periodic antenna at MRT site. The antenna was built out of standard aluminum profiles in the local workshop. Frequency range goes from 20 MHz up to 860 MHz in fixed vertical position Vertical tubes on both sides are made of PVC to mechanically support long, heavy dipoles..

The Back End The CALLISTO spectrometer is on the left side of the table (below ‘Toblerone Chocolate bar), power supplies just behind and monitor with keyboard and PC on the right.,

Commissioning (27.04,2009) X-axis shows time expressed in UT, Y-axis frequency in MHz and Z-axis denotes the stored digital value of the ADC(without any calibration). The frequency resolution is ~ 4 MHz and time resolution is 250 msec (4 sweeps Per second). Data is stored in 15 min FITS files

Quiet Sun: with background ( ) 45 MHz 860MHz 15 minute time interval (UT)

Quiet Sun: background subtracted ( ) 45 MHz 860MHz 15 minute time interval (UT)

Active sun having sunspots: with background ( ) 45 MHz 860MHz 15 minute time interval (UT)

Active sun having sunspots: with background subtraction ( ) 45 MHz 860MHz 15 minute time interval (UT)

Zoom in Active sun having sunspots: with bkgrnd subtraction ( ) 45 MHz 860MHz 15 minute time interval (UT)

“First light” flarZoom in Active sun having sunspots: with bkgrnd s092009)e ( 2009) Mauritius 45 MHz 860MHz 15 minute time interval (UT)

45 MHz 860MHz 15 minute time interval (UT) “First light”close up May 1 st 2009 Mauritius

Solar flare (6 th May 2009)Mauritius 45 MHz 860MHz 15 minute time interval (UT)

Solar flare (8 th May 2009) Mauritius 45 MHz 860MHz 15 minute time interval (UT)

Zoom in Solar flare (8 th May 2009) Mauritius 45 MHz 860MHz 15 minute time interval (UT)

Solar flare (8 th May 2009) other stations Bleien Humain

Solar flare (8 th May 2009) other stations Kasi Mauritius

Solar flare (8 th May 2009) other stations Ooty lin pol1: Lightning flash at 08:09:01.5 UT Ooty lin pol 2:Lightning flash at 08:09:04 UT

Zoom in Solar flare (24 th Sep 2009) Mauritius 45 MHz 860MHz 15 minute time interval (UT)

Future Work ­ Antenna array: improved gain & sky coverage ­ Calibration ­ Timing experiments - Software development Excellent first instrument for radio astronomy: Interested?