Pulsar observations with the Effelsberg LOFAR station Masaya - - PowerPoint PPT Presentation

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Pulsar observations with the Effelsberg LOFAR station Masaya - - PowerPoint PPT Presentation

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Pulsar observations with the Effelsberg LOFAR station Masaya Kuniyoshi Max Planck Institute for Radio Astronomy on be half of MKSP/PWG Friday, June 7, 13 Who are you? ~2007 : Waseda University in Japan 2007~2009 : LWA in the U.S.

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SLIDE 1

Pulsar observations with the Effelsberg LOFAR station

Masaya Kuniyoshi

Max Planck Institute for Radio Astronomy

  • n be half of MKSP/PWG

Friday, June 7, 13

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SLIDE 2

Who are you?

  • ~2007 : Waseda University in Japan
  • 2007~2009 : LWA in the U.S.
  • 2009~Present : LOFAR in Germany

Friday, June 7, 13

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SLIDE 3

Who are you?

  • ~2007 : Waseda University in Japan
  • 2007~2009 : LWA in the U.S.
  • 2009~Present : LOFAR in Germany

Friday, June 7, 13

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SLIDE 4

Who are you?

  • 2007~2009 : LWA in the U.S.

Friday, June 7, 13

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SLIDE 5

Who are you?

  • 2007~2009 : LWA in the U.S.

VLA V L A VLA LWA

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SLIDE 6

Who are you?

  • 2009~Present : LOFAR in Germany

Friday, June 7, 13

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SLIDE 7

Who are you?

  • 2009~Present : LOFAR in Germany
Pulse number! Pulse phase!

Friday, June 7, 13

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SLIDE 8

Outline

  • Effelsberg LOFAR station
  • Pulsar Observations
  • Jones Matrix calibrations
  • Public Outreach

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SLIDE 9

The LOw Frequency ARray (LOFAR)

Friday, June 7, 13

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SLIDE 10

The LOw Frequency ARray (LOFAR)

  • A pathfinder to the SKA
  • Operation in the frequency from 10 to 240 MHz
  • An international telescope
  • Eight international stations and more down the road

Humbug in Germany, three stations in Poland.

Friday, June 7, 13

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SLIDE 11

The LOFAR stations

Friday, June 7, 13

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SLIDE 12

The LOFAR stations

Cosmic Magnetism Cosmic Rays Epoch of Reionization Extragalactic Surveys Solar Physics Transients

The core is heavily subscribed! Many projects only require short baselines, leaving the international LOFAR stations unused.

Friday, June 7, 13

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SLIDE 13

The LOFAR stations

Cosmic Magnetism Cosmic Rays Epoch of Reionization Extragalactic Surveys Solar Physics Transients The core is heavily subscribed! Many projects only require short baselines, leaving the international LOFAR stations unused.

Friday, June 7, 13

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SLIDE 14

The LOFAR stations

Cosmic Magnetism Cosmic Rays Epoch of Reionization Extragalactic Surveys Solar Physics Transients The core is heavily subscribed! Many projects only require short baselines, leaving the international LOFAR stations unused.

Friday, June 7, 13

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SLIDE 15

Effelsberg LOFAR Station (DE601)

The first LOFAR station outside the Netherlands

Friday, June 7, 13

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SLIDE 16

Stand-Alone mode

Beamforming Recording & Processing A pulsar profile

HBA tile LBA dipole HBA LBA

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SLIDE 17

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SLIDE 18

Pulsars

Courtesy: A.Noutsos (MPIfR)

  • Rapidly rotating highly

magnetized neutron stars

  • Weighing more than our Sun,

yet only 20 km in diameter, these incredibly dense objects produce radio beams that sweep the sky like a lighthouse.

  • Approximately 2000 have

been found.

  • pulsars are among the most

polarized of all known radio sources.

Friday, June 7, 13

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SLIDE 19

Pulsar Observations

Friday, June 7, 13

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SLIDE 20

Pulsar Observations

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SLIDE 21

Effelsberg

The circumpolar PSR B0329+54 track Effelsberg horizon surrounded by a valley

30 60

pulsar loccation

Friday, June 7, 13

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SLIDE 22

Station Stability Monitoring

A circumpolar PSR B0329 observation, day-long sequence

  • f hourly observations lasting a few minutes each

Friday, June 7, 13

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SLIDE 23

Station Stability Monitoring

A circumpolar PSR B0329 observation, day-long sequence

  • f hourly observations lasting a few minutes each

Friday, June 7, 13

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SLIDE 24

Station Stability Monitoring

Friday, June 7, 13

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SLIDE 25

Dispersion Measure (DM)

The quadratic frequency dependence of DM delay leaning to the right a little bit ?

− D× DM f 2

DM = ne dl

d

∫

D = e2 2πmec

n: electron number density D: dispersion constant e: charge of an electron m: mass of an electron

After removing dispersion which accounts for the correction with DM 26.833 (pulsar catalogue).

Friday, June 7, 13

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SLIDE 26

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SLIDE 27

DM Measurement with LOFAR

DM 26.76 (2013): LOFAR DM 26.83 (1986): Lovell

total linear circular linear total circular

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SLIDE 28

LOFAR's Applicability to High Precision Timing

  • In high-precision timing, the

biggest problem is variations in DM.

  • LOFAR works at lower

frequencies, which can make these measurements much more accurately and can measure DM variations at a much more precise level.

Measurements of interstellar dispersion to the pulsar J2145‐0750. Courtesy: J.Verbiest (MPIfR) The Universe is filled with a background of gravitational waves.

Friday, June 7, 13

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SLIDE 29
  • A mean value
  • A rich variety structure
  • A wealth of emission process
  • Time-variable plasma processes

create

Individual pulses

Pulse number! Pulse phase!

0.714 (s)

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SLIDE 30

Jones Matrix

  • Hamaker. J

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SLIDE 31

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SLIDE 32

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SLIDE 33

The first discovered pulsar CP1919

Jocelyn Bell & Antony Hewish

Nobel Prize in Physics in 1972

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SLIDE 34

Public Outreach

(brainwashing kids into SKA) circular! linear! total!

Our group has been involved in public outreach, organizing lectures at schools, where the general public was given a chance to perform pulsar observations with LOFAR. The young students were excited to see the profile of the first discovered pulsar CP1919, in 30 seconds of LOFAR data. 2013-01-27 Düsseldorf, Germany

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SLIDE 35

Thank you for your attention!

Friday, June 7, 13