Pulsar Data analysis Desh, Anish RRI MWA Meeting Canberra, January 19-23 2009.

Slides:



Advertisements
Similar presentations
Ben Barsdell Matthew Bailes Christopher Fluke David Barnes.
Advertisements

Low-Frequency Pulsar Surveys and Supercomputing Matthew Bailes.
7/26/12W. Majid1 Crab Giant Pulses W. Majid *, S. Ellingson (PI), C. Garcia-Miro, T. Kuiper, J. Lazio, S. Lowe, C. Naudet, D. Thompson, K. Wagstaff * Jet.
Preliminary results of giant pulse investigations from Crab pulsar with Radioastron. Rudnitskiy A.G., Popov M.V., Soglasnov V.A. 12 th EVN SYMPOSIUM Cagliari,
The Highest Time-Resolution Measurements in Radio Astronomy: The Crab Pulsar Giant Pulses Tim Hankins New Mexico Tech and NRAO, Socorro, NM Extreme Astrophysics.
Zhen Yan, Zhi-Qiang Shen, Xin-Ji Wu On behalf of the Shanghai 65m Radio Telescope Team.
Pulsars with LWA1 Paul S. Ray and Sean Cutchin Naval Research Laboratory 2012 July 26 Basic research in radio astronomy at NRL is supported by NRL/ONR.
A young pulsar with a long radio trail emerging from SNR G F. Camilo, C.-Y. NG et al. arxiv : v1.
Discovery (?) for new population of isolated neutron star “ Transient radio bursts from rotating neutron star ” M.A. McLaughlin et al., Nat. Feb. 16, 2006.
1 A Grating Spectrograph for the LCLS Philip Heimann Advanced Light Source Observe the spontaneous radiation spectrum of the individual undulators Observe.
Search for Radio Emissions… 6/30/2015E-LOFAR SEARCH FOR RADIO EMISSIONS FROM EXTRASOLAR PLANETS.
New observations of three AXPs at low radio frequencies Daria Teplykh & V.M. Malofeev, A.E. Rodin, S.V. Logvinenko. Pushchino Radio Astronomy Observatory.
Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Digital Signal Processing.
Detection of Giant pulses from pulsar PSR B Smirnova T.V. Pushchino Radio Astronomy Observatory of ASC FIAN Pushchino Radio Astronomy.
Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)
Long-term monitoring of RRAT J HU HuiDong Urumqi Observatory, NAOC July 27, 2009 Rotating Radio Transients Observation.
Solar observation modes: Commissioning and operational C. Vocks and G. Mann 1. Spectrometer and imaging modes 2. Commissioning proposals 3. Operational.
Mean pulse profiles and spectra at the low frequencies Malov O.I., Malofeev V.M. Malov O.I., Malofeev V.M. Pushchino Radio Astronomy Observatory.
10 January 2006AAS EVLA Town Hall Meeting1 The EVLA: A North American Partnership The EVLA Project on the Web
FULLY DIFFERENTIAL OPAMP Eduardo Picatoste Calorimeter Electronics Upgrade Meeting.
5 Jan 2004, Boulder CO URSI The Current Status of the Green Bank Telescope.
Design and performance of fast transient detectors Cathryn Trott, Nathan Clarke, J-P Macquart ICRAR Curtin University.
Making MOPRA go! Lucyna Kedziora-Chudczer Friend of the telescope (UNSW)
21 cm Reionization Forecast and Search at GMRT
Finding Fast Pulsars Today andTomorrow Pulsar Timing Array - A Nanohertz Gravitational Wave Telescope July 21-23, 2005 Jason Hessels McGill University.
Single Pulse Investigations at the Decameter Range O.M. Ulyanov 1, V.V. Zakharenko 1, V.S. Nikolaenko 1, A. Deshpande 2, M.V. Popov 3, V.A. Soglasnov 3,
Real-time Acquisition and Processing of Data from the GMRT Pulsar Back- ends Ramchandra M. Dabade (VNIT, Nagpur) Guided By, Yashwant Gupta.
ETA Data Processing Steve Ellingson Low Frequency Software Workshop – Chicago – Aug 10, 2008.
Pulsar surveys at Arecibo and Green Bank David Champion Gravity Wave Meeting, Marsfield, Dec 2007.
Radio Emissions of Magnetars & Observations at Nanshan Xinjiang Astronomical Observatory Yuan Jianping, Wang Na, Liu Zhiyong Outline  Introduction of.
Murchison Widefield Array (MWA) : Design and Status Divya Oberoi, Lenoid Benkevitch MIT Haystack Observatory doberoi, On behalf.
RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing,
GSB : A real-time Software back-end for the GMRT Jayanta Roy National Centre for Radio Astrophysics Pune, India 12 th December 2008 Collaborators.
Aristeidis Noutsos University of Manchester. Pulsar Polarization Pulsar radiation is elliptically polarised with a high degree of linear polarization.
Ramesh Bhat Centre for Astrophysics & Supercomputing Swinburne University of Technology Time Domain Astronomy Meeting, Marsfield, 24 October 2011 Searching.
Aristeidis Noutsos University of Manchester. The LOFAR Ionosphere See Ger’s talk, in Hamburg last year. Variations of ~3 rad m –2 were observed in the.
Pulsar tools in DiFX Adam Deller ASTRON 6th DiFX workshop, CSIRO ATNF, Sydney AUS.
Low frequency observation of both pulsar wind and magnetodipole radiation from switch on-off pulsars Ya.N. Istomin P.N. Lebedev Physical Institute, Moscow,
Rick Perley 2 Nov 2001 EVLA Correlator Conceptual Design Review 1 Science Drivers for the EVLA Correlator Rick Perley EVLA Project Scientist 2 Nov 2001.
Coherent Dedispersion Pulsar Timing Machines Matthew Bailes + Swinburne, Caltech, ATNF, CASPER.
Interstellar turbulent plasma spectrum from multi-frequency pulsar observations Smirnova T. V. Pushchino Radio Astronomy Observatory Astro Space Center.
Radio Sounding of the Near-Sun Plasma Using Polarized Pulsar Pulses I.V.Chashei, T.V.Smirnova, V.I.Shishov Pushchino Radio Astronomy Obsertvatory, Astrospace.
Low Frequency Array (LOFAR): The French LOFAR Super Station Helmut O. Rucker Commission for Astronomy Austrian Academy of Sciences ÖAW, Vienna, Dec 14.
First Exploration of MWA Deep Field Point Source Population C. Williams - PhD Thesis J. Hewitt – reporting some analysis.
Longitudinal HOM power estimations for pulsed beams.rev W. Weingarten 31 May 20101SPL Cavity WG Meeting.
Yan Zhou, Anthony Colombo, David Grimes, Robert Field Cooperative effects in a dense Rydberg gas.
V f λ.
Damien Parent – Moriond, February PSR J , PSR J , and their cousins -- young & noisy gamma ray pulsars Damien Parent on behalf of.
Measurement of Electron Density Profile and Fluctuations on HSX C. Deng, D.L. Brower, W.X. Ding Electrical Engineering Department University of California,
Polarized Radio Emission within Pulsar Magnetosphere & Pulsar Observation with JMS 66m PengFei Wang PengFei Wang ( 王鹏飞 )NAOC
Chapter 6 Tutorial 6.
Camp Sentinel II Radar System [4] -Installed outside US Army Camp in Vietnam in Antenna Dimensions: 3.5 m diameter x 1 m tall antenna. -2 kW.
p no Bhaswati Bhattacharyya On behalf of GHRSS team
FRB Backend First Light
Sergei A. Trushkin , Sergei N. Fabrika, Peter G. Tsybulev
Searching FRB with Jiamusi-66m Radio Telescope
MWA “burst mode”: Nov 2008 Solar 32 T Observations
V f λ.
LOFAR Beam Formed (BF) Data & Pipeline Overview September 9, 2010
الفصل 1: الحركة الدورانية Rotational Motion
Pulsar and Transient Science with the 12m Antenna
The High Time Resolution Universe Survey Backend
What we will do today: Carry out calculations involving the relationship between speed, wavelength and frequency for waves.
GBT Status: Current Observing Capabilities
RM 2 7 +RM 2 4 RM 7 3 +RM 1 6 RM 5 2 +RM 2 4 RM 1 3 +RM5 2.
Observations of pulsar microstructure with the GMRT
Amateur Pulsar Detection With EME Equipment
Polarization Properties of an Eclipsing Pulsar
Calculate the missing information below.
Presentation transcript:

Pulsar Data analysis Desh, Anish RRI MWA Meeting Canberra, January

Pulsar Data analysis Desh, Anish RRI MWA Meeting Canberra, January

Pulsars Observed: B and B Data Taken on 18 Nov 2008 in the transit mode Length of data analysed ~ 600 S for each of the pulsars (~ 400 Pulses of B0834 and 200 Pulses of B ) Total BW of observation ~ 1.2 MHz (fre Chs used ~256) Data Analysis Mode: Preliminary results available for incoherent addition Data Analysis in coherent dedispersion mode in progress

B data

NAME B DM = F0 = P0 = S400= 89 S1400=4 W50 =23.9 W10 =33.9 SPINDX= -2.7 RM =23.6 DM: Dispersion measure (cm -3 pc) F0: Barycentric rotation frequency (Hz)F1: P0: Barycentric period of the pulsar (s) S400: Mean flux density at 400 MHz (mJy) S1400: Mean flux density at 1400 MHz(mJy) W50: Width of pulse at 50% of peak (ms). W10: Width of pulse at 10% (ms). SPINDX: Measured spectral index RM: Rotation measure (rad m -2 ) Numbers of Pulses Folded: ~ 400; Resolution BW used: 4.8 KHz

NAME B DM =2.958 F0 = P0 = S400= 400 S1400= 84 W50 =9.5 W10 =20.6 SPINDX =-1.7 RM =-0.66 DM: Dispersion measure (cm -3 pc) F0: Barycentric rotation frequency (Hz)F1: P0: Barycentric period of the pulsar (s) S400: Mean flux density at 400 MHz (mJy) S1400: Mean flux density at 1400 MHz(mJy) W50: Width of pulse at 50% of peak (ms). W10: Width of pulse at 10% (ms). SPINDX: Measured spectral index RM: Rotation measure (rad m -2 )

Data taken on: 18 Nov 2008 BW=1.6 MHz Int time = 5 min No data lost to RFI Self-cal