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Radio Astronomy Activities at RRI. N. Udaya Shankar RRI. Indo-SA Astronomy Workshop 7 August 2012. The economically important Silk Road (red) and spice trade routes (blue). Pepper: MWA Precursor SKA EOI in SKA Low Science Case for SKA MID Evolution of HI in the universe. SALT.

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radio astronomy activities at rri

Radio Astronomy Activities at RRI

N. Udaya Shankar

RRI

Indo-SA Astronomy Workshop

7 August 2012

slide3

Pepper:

MWA Precursor SKA

EOI in SKA Low

Science Case for SKA MID

Evolution of HI in the universe.

SALT

a a group
A&A group

Theoretical astrophysics (5)

Observational astronomy to (7)

Builders: specialized instruments .

  • Collaborations: Many body interactions

Lead to joint pursuit of problems in

Theory, Observations, Specialized instruments

  • world-wide collaborations.
slide5
Present Focus:Low Frequency Radio Astronomy.Frequencies Below: 1.4 GHz.Developing interest in the freq range: 2 to 4 GHz.
slide6

Evolution of HI atom in the universe

  • a. HI mass fluctuations using ORT;
  • 327 MHz, z=3.3
  • b. EoR : I. Statistical Detection
  • Our participation in MWA
  • 80-300 MHz, z=4-16
  • ii. Global Signal Detection
  • In-house Projects
  • 87.5 – 175 MHz, z= 4-8
  • c. ERA : Epoch of Recombination array
  • 2 – 4 GHz, z=1000
  • 2.Transients and Pulsars, MWA and ORT
slide7

2.Transients and Pulsars,

MWA and ORT

3. Halos and Relics in Galaxy Clusters GMRT and MWA

50 MHz system for GMRT

4. Multi-frequency observations of Compact objects ,

X-ray polarimeter.

2 murchison wide field array mwa
2. Murchison Wide Field Array (MWA)

MWA is a low-frequency imaging radio interferometer facility being built in the radio-quiet area of Western Australia

this is one exciting project
This is one exciting project …
  • Scientifically rich
    • EOR, Solar, Transients, Pulsars, RRLs, etc.
  • Technologically innovative
    • Leading the way in multiple simultaneous areas
    • Trailblazing!
  • Excellent partnership
    • Common goals + motivations
    • Abundance of talent and energy
  • Enormous growth potential
    • Inexpensive hardware, Moore’s law
    • LFD/xNTD synergy, path to SKA
    • Opportunities abound, for Australian, Indian, US, and Global community

MWA-LFD Kick-Off June 2006

slide10

MWA

Murchison

physical layout

Cluster (50-100m diam.)

Array (~1.5km diam.)

Antenna tile (~4m diam.)

tile

node

clusters

Tile beamformer

Fiber out

Coax out

Central Processing

Physical Layout
slide13
A digital receiver for MWA has been developed and built in the Radio Astronomy laboratory at RRI.
  • RRI digital receivers operate between 80 and 300 MHz and are based on state-of-the-art Virtex-5 FPGA chips
  • The receivers operate at 655 MHz sampling, include poly-phase digital filters and fiber optic links.
mwa digital receiver
MWA Digital Receiver

Each receiver receives outputs from 8 tiles , digitize them, do 512 CH PFB and send them through fiber links after serializing.

rri contribution
RRI contribution
  • Development of

i) A/D and Filter Bank (ADFB) Architecture

ii) Firmware for ADFB board

  • Development of

i) Backplane and

ii) Clock for 32 T digital receiver

  • Development of

i) Hardware and firmware architecture for AGFO

ii) Design of Board and firmware development

  • Development of Imaging Algorithms: Nithya’s Talk
current status
Current status
  • Actively involving in system testing under integrated environment
  • Planning to mass produce 16 digital receivers for 128 tiles by mid 2012
  • Development of hardware and firmware to combine in the digital receiver the outputs of all 8 tiles to form one beam and use the entire bandwidth available
receiver is a 2 element interferometer w ith a space beam splitter
Receiver is a 2 element interferometer with a space beam splitter
  • Freq. range : 87.5 – 175 MHz

The screen is made resistive to ensure required phase diff. between transmitted and reflected signals exists and has equal transmission and reflected signals

receiver system for eor detection
Receiver system for EoR detection
  • Frequency Independent Antennas installed over absorber tiles
  • Well matched receivers with low noise figure
  • a digital receiver consisting of a high speed digitizers and a spectro-correlator
current status1
Current Status
  • The Zero space interferometer has been completely characterized for all its properties and data acquired are being analyzed.

Next Phase:

Take it to a radio quite zone

Australia

South Africa

5 x ray polarimeter
5. X-Ray Polarimeter
  • X-ray polarimeter based on the principle of Thomson scattering is being developed at the Raman Research Institute (RRI)
  • The experiment has been proposed to the Indian Space Research Organization for a small satellite mission.
scientific objective
Scientific Objective
  • Polarisation measurement gives insight about
    • The strength and the distribution of magnetic field in X-ray sources
    • Geometric anisotropies in the source
    • The nature of the accelerator responsible for energizing the electrons taking part in radiation and scattering.
  • The instrument is suitable for X-ray polarisation measurement of hard X-ray sources like
    • accretion powered pulsars,
    • black hole candidates in low-hard states etc.
instrument specifications
Instrument Specifications
  • Energy band covered – 5-30keV
  • Detectors – Proportional counters
  • Photon collection area ~ 1018 cm2
  • Field of view - 33 degree with 0.5 degree flat response
current status2

Current Status

The development of a Thomson polarimeter including

proportional counter detectors,

associated front-end electronics,

event processing logic,

data acquisition system, and

test and calibration system

have been completed successfully.

Engineering Model is being developed

For more details contact : bpaul@rri.res.in

sub mm telescope

Sub-mm telescope

New Optics design has been developed for constructing large sub-millimeter radio telescope economically.

Balasubramanyam, R, 2004, MNRAS, 354, 1189

current status3
Current Status
  • At present a 3m Submillimeter-wave telescope prototype (3mSTeP) is being built
  • The mechanical structure, design and optimization are completed
  • Work on 8 GHz wide band spectrometer is under progress.
  • For more details: contact : ramesh@rri.res.in
slide29

Studies of galaxy populations in merging galaxy clusters using SALT and GMRT.

  • Radio monitoring of transient X-ray sources, disk-jet connection.
  • 3. Optical reprocessing of X-rays, simultaneous observations with ASTROSAT and SALT.
  • 4. NIR-studies (in continuum and shocked molecular hydrogen @ 2.1/2.2 um) of chosen southern massive star forming regions.
  • 5. Observing for Global EoR signal detection in SKA site in SA.
slide35

Hierarchical Interference mitigation.

  • Imaging with a non-coplanar array.
  • Imaging two steradinas of the sky.
  • Human Resource Development:
  • 8 Ph.D. students
  • 1 MS student
  • Several student projects
major projects undertaken by rri
Major projects undertaken by RRI
  • Aperture Array for Low Frequency Radio astronomy
  • Development of Digital receivers for The Murchison Wide Field Array (MWA)
  • Multiband receiver system at Green Bank Telescope
  • Zero Spacing Interferometer to detect Cosmological Re-ionization Signatures
  • Development of an X-ray polarimeterfor small satellite mission
  • Upgradation of Ooty Radio Telescope
  • Development of a 3m Submillimeterwave telescope Prototype(3mSTeP)