First result with PAF on a big single-dish radio telescope X. Deng, A. Chippendale, S. Johnston, G. Hobbs, D. George, R. Karuppusamy ASTRONOMY AND SPACE.

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Presentation transcript:

First result with PAF on a big single-dish radio telescope X. Deng, A. Chippendale, S. Johnston, G. Hobbs, D. George, R. Karuppusamy ASTRONOMY AND SPACE SCIENCE 7 July 2016, ASA meeting

Project background Phased Array Feed (PAF) was designed by CSIRO Astronomy and Space Science (CASS) for Australian Square Kilometre Array Pathfinder (ASKAP); Michael Kramer from Max Planck Institute for Radio Astronomy (MPIfR) bought it for FRB searching; CASS and MPIfR employed me to follow the project; To make the system working on single-dish telescope:  We installed the system at Parkes during Chinese new year;  CASS is updating PAF system (software);  MPIfR and Jodrell Bank is working on FRB searching and pulsar timing mode;  Curtin is working on spectral line mode; To install the system at Germany:  We will remove the system from Parkes at October ;  I will move to Germany with the system by the end of 2016;  We will install it at Effelsberg after that. Result from PAF on Parkes | Dr. Xinping Deng 2 |

System overview 5 | PAF: 600 MHz DRX: 600 MHz BMF: 384 MHz 9 GPU nodes PAF: 188 ports, 94 ports each polarization; DRX: digitize different ports individually; BMF: correlation for beam forming; BMF: form up to 36 beams; Result from PAF on Parkes | Dr. Xinping Deng BMF: 1 MHz frequency channel; BMF: 108 us sampling; GPU: beam formed data processing;

Passband 6 | Chippendale et al., ICEAA 2016 Band 1: GHz, CF GHz Band 2: GHz, CF GHz Band 3: GHz, CF GHz Result from PAF on Parkes | Dr. Xinping Deng

System temperature 7 | Chippendale et al., ICEAA 2016 System temperature is around 50 K in all frequencies It is significantly better than ASKAP (around 90 K) Efficiency is around 0.8 in all frequencies Temperature over efficiency is around 60 K in all frequencies Result from PAF on Parkes | Dr. Xinping Deng On and off source observation with Virgo A to get system temperature

End-to-end system temperature 8 | Astronomers are more interested in end-to-end system temperature; Not finished yet due to packets problem; Will do it again when we get a stable system; Do prove that beam forming works as expected; PSR J (Vela): 3x3 Square Footprint on 0.215° Pitch, S1400 = 1.1 Jy, 42 MHz, 10 minutes Beam 1 Beam 2 Beam 3 Beam 4 Beam 5 Beam 6 Beam 9 Beam 8 Beam 7 Result from PAF on Parkes | Dr. Xinping Deng

Boresight pulsar observing 9 | Vela: full bandwidth, 10 minutes Boresight beam tracking with full bandwidth; Good signal to noise ratio; Dispersion as expected; Result from PAF on Parkes | Dr. Xinping Deng

Boresight pulsar observing 10 | PSR J , polarization is not calibrated Boresight beam tracking with full bandwidth; Good signal to noise ratio; The effect of parallactic angle is observed in timing residual; Timing residuals dominated by “jitter” noise; Result from PAF on Parkes | Dr. Xinping Deng

Multiple pulsar observation 11 | Problem: PAF can not be rotated in Parkes focus cabin Can not rotate PAF to track outside pulsar; Outside pulsar drifts through beam; SNR changes significantly; Result from PAF on Parkes | Dr. Xinping Deng

Multiple pulsar observation 12 | Solution: track with different beams Form different beams to track outside pulsar; Make sure that no significant change in SNR; Result from PAF on Parkes | Dr. Xinping Deng

Spectral line 13 | H I gas in a young galaxy at z=0.44 Result from PAF on Parkes | Dr. Xinping Deng

Astronomy and Space Science X. Deng Experimental scientist Astronomy and Space Science A. Chippendale Research engineer ASTRONOMY AND SPACE SCIENCE Thank you Photo by John Sarkissian

Astronomy and Space Science S. Johnston Research Scientist Astronomy and Space Science George Hobbs Research Scientist Astronomy and Space Science D. George Research Engineer Max Plank Institute for Radio Astronomy Ramesh Karuppusamy Research Engineer ASTRONOMY AND SPACE SCIENCE