A Cryogenic PAF for Parkes

Transcription

1 A Cryogenic PAF for Parkes PAF Workshop 2017 Jimi Green Parkes Senior System Scientist, CASS Group Leader 16 th November 2017 CSIRO ASTRONOMY AND SPACE SCIENCE

2 Acknowledgements Matthew Bailes Ramesh Bhat Justin Bray Aaron Chippendale John Conway Joanne Dawson John Dickey Alex Dunning Ron Ekers Doug Hayman Clancy James Simon Johnston Evan Keane Michael Kramer J.P. Macquart Naomi McClure-Griffiths Ray Norris Bo Peng Maria Rioja Elaine Sadler Ryan Shannon Lister Staveley-Smith Tasso Tzioumis Nina Wang Laura Wolz Parkes Cryo-PAF Jimi Green

3 Overview The Parkes radio telescope (in a slide) Phased Array Feeds with Parkes The Cryo-PAF Proposal Drivers Specifications Benefits 3 Parkes Cryo-PAF Jimi Green

4 Parkes Radio Telescope (in a slide) 64 m radio telescope (f/d 0.41), ~380 km west of Sydney, ~20 km north from town of Parkes, owned and operated by CSIRO Three years to design and two years to build - officially opened on 31 October 1961 Operating for more than 55 years Continual upgrades & evolution have been key (new surfaces, new focus cabin, new receivers e.g. multibeam, backend systems) Multitude of scientific discovery Other activities - space craft tracking ( The Dish ) 4 Parkes Cryo-PAF Jimi Green

5 Parkes Radio Telescope Current capabilities 700 MHz to ~25GHz across 8 receivers Including 13-beam multibeam system Spectral and temporal back end capabilities For single-beam time domain (events < 1s) and spectrometry ( DFB4 ) For single-beam time domain and new limited piggyback spectrometry ( CASPSR ) For multi-beam (13 beams) time domain and spectrometry ( HIPSR/BPSR ) Real-time Fast Radio Burst detection For Very Long Baseline Interferometry, VLBI ( DAS & Mk-V ) 5 Parkes Cryo-PAF Jimi Green

6 Phased Array Feeds with Parkes Tests of PAF designs on site (cover of book!) Max Planck Institute (MPIfR) Phased Array Feed - Repurposed ASKAP feed ( MKII ) commissioned on Parkes in 2016 (~10 months on dish) Chippendale et al timed 3 Pulsars simultaneously Deng et al spectral line observations - very flat and stable bandpass Reynolds et al m antenna monitoring Vela pulsar ( MKI PAF), including detecting glitch Sarkissian et al Parkes Cryo-PAF Jimi Green

7 Science Drivers Transients Fast Radio Bursts (FRBs) Parkes role: First FRB discovered with Parkes (Lorimer et al. 2007) Major search campaigns, e.g. SUPERB real-time detection project >=21 of >=26 to date discovered with Parkes (e.g. Thornton et al., 2013), detection rate ~5 per year Competition: CHIME (Northern Hemisphere, predicted detection rate ~ 1 per day, localisation few arcmin in 1D) ; MeerKAT (expects 12 localised FRBs over a 5 year survey) ; Molonglo-UTMOST (~4 detected to date); ASKAP flys-eye (~10 detected to date) ; Caltech 10-m dish system Want: study of their origin and of the baryonic content of the Universe Have: mature data reduction & FRB detection pipeline, Southern Hemisphere Need: increased field of view, localisationability, accurate intensity 7 Parkes Cryo-PAF Jimi Green

8 Science Drivers Pulsars Parkes role: Detection machine >1500, ~2/3 of all Credit: MPIfR Ch. Ng. Competition: Meerkat existing Northern hemisphere single dishes, FAST (SKA ~20,000 detections) Want: more, more, more (timing sources, exotic systems) - explore fundamental physics, including matter equations of state, theories of gravity & gravitational wave regime at long wavelengths. Have: Improving GPU based backends (greater range of dispersion measures) Need: low Tsys (<=MB Tsys), increased field of view, wider bandwidth 8 Parkes Cryo-PAF Jimi Green

9 Science Drivers Hydrogen over cosmic time Parkes role: Multibeam studies: HI Parkes All Sky Survey (HIPASS), Galactic All Sky Survey (GASS), component of SGPS surveyed own Galaxy, Magellanic clouds, 1000s of nearby Galaxies, pushing further in redshift Competition: Low-z CHIME, Tian-Li, GBT-HIM, HIRAX, SKA-MID (+ high-z LOFAR, MWA, HERA, PAPER, SKA-LOW ) ASKAP, APERTIF, SKA Want: Detect & accurately quantify neutral gas content of galaxies & the cosmic web across ½ age of the Universe through intensity mapping (power spectrum and cross-correlation with optical redshift surveys, Chang et al. 2010) Have: ARC centres of Excellence CAASTRO -> ASTRO 3D, developed body of knowledge and theoretical experience (e.g. Wolz et al., 2016). Need: increased field of view, increased bandwidth, flatter baselines 9 Parkes Cryo-PAF Jimi Green

10 Science Drivers high-energy particle detection Parkes role: most sensitive experiment to date to detect high-energy particles, via Cerenkov radio pulse, used the Parkes 21 cm multibeam receiver, which was able to see 1/3 of the useful area of the moon (Bray et al. 2015) Competition: CROME (previously), SKA, LOFAR, AuScope FAST with a PAF (VLA, WSRT previously) Want: to know the nature & origin of ultra-high-energy particles ( one of the biggest mysteries of modern astrophysics ) Have: previous experience, sensitivity, backend options Need: increased field of view: see the entirety of the moon. 10 Parkes Cryo-PAF Jimi Green

11 Science Drivers ASKAP with Parkes PAF VLBI complement EMU survey will detect about 70 million radio sources. Separate Active Galactic Nuclei (AGN) vs star-forming galaxies, through singlebaseline Very Long Baseline interferometer (e.g. Norris & Kesteven, 2012, Middelberg et al. (2013 polarisation studies of the AGN, imaging of OH megamasers, and classification of pulsars and radio stars FLASH survey will detect Hi absorption in 1000 radio-loud AGN at z = (Allison et al., 2015). detect neutral gas outflows, associated with AGN feedback via < 1-percent optical depth sensitivity (achieved with very good spectral baseline and realtime RFI mitigation) localise position, measure size & kinematics of HI absorbers 11 Parkes Cryo-PAF Jimi Green

12 Science Drivers ASKAP single dish & VLBI complement GASKAP survey will observe HI and OH in the Milky Way over an area of 13,000 sq. degs (Dickey et al., 2013). Zero-spacing data to probe large spatial scales that ASKAP is insensitive to ultra-high sensitivity OH survey of entire Southern sky, probing new physical environments SKA1-mid/Parkes baseline astrometry towards a sample of 100 OH-maser sources would allow the internal angular rotations of the Magellanic Clouds to be modelled (proper motion to 10 micro-arc seconds yr 1 ( 2 km/s) accuracy Astrometry of pulsars is often beneficial in providing direct measurements of their distances independent of single dish timing data. 12 Parkes Cryo-PAF Jimi Green

13 Specifications Cryo-PAF Tests and Targets Cryogenically cooled Rocket Phased Array Feed (third generation CSIRO PAF designed by Alex Dunning & co) Prototype on dish testing (plus aperture tests) May very encouraging for purpose built version 700 MHz 2 GHz 3 x MB field of view (~4.5 deg) sub-20 K Tsys 13 Parkes Cryo-PAF Jimi Green

14 Specifications Cryo-PAF Targets System Temperature/Efficiency MPIPAF Parkes mul+beam (T/η) Cryogenic rocket PAF (est) Cryogenic rocket PAF (est.) MPIPAF Parkes mul+beam 14 Parkes Cryo-PAF Jimi Green

15 Improvement Summary Headlines Significant improvement in six key areas: 1. an improved receiver noise; 2. a wider field of view; 3. Nyquist sampling of the focal plane; 4. a wide front-end bandwidth; 5. greater aperture efficiency; 6. reduced baseline ripple. Together = 10 to 30-fold increase in survey speed 15 Parkes Cryo-PAF Jimi Green

16 Improvement Summary Science Impact FRBs: FRB detection by almost a factor of 3 (14±4 per year), arcmin localisation and accurate intensities PULSARS: 3 greater than the current system field of view, uniform sensitivity, larger bandwidth and 10 better localisation accuracy -> several hundred new detections HYDROGEN: 4x multibeam bandwidth, 3x field of view, extremely flat baselines, cost effective approach ASKAP: VLBI follow-up and zero-baseline spacing information HIGH-ENERGY PARTICLES: whole moon / entire limb field of view (plus potential for atmospheric via surrounding detectors) 16 Parkes Cryo-PAF Jimi Green

17 Benefits Search for Extra Terrestrial Intelligence: Breakthrough Listen Background 5-year programme, multi-year investment for telescope time Officially began observing October/November 2016 Observing blocks each day, stepping in time (Local Sidereal Time) through the week Dedicated backend managed by University of California, Berkeley, simultaneous use of GPU backend Mal Smith Gains Faster Galactic plane survey, more effective/efficient transient/fast Radio Burst simultaneous searches 17 Parkes Cryo-PAF Jimi Green

18 Benefits Education & Outreach Background programme Pulsar focused, secondary-level education programme with real-time access to, and control of, Parkes Telescope ~1500 high school students to date, ~130 schools, sessions across Australia, plus Canada, China, England, Japan, South Africa & Wales Undergraduate/postgraduate extension to the programme Observing with Parkes, Training and Introduction, Module for University STEM: OPTIMUS developed through CSIRO s ON PRIME Extending/varying science to include other aspects, STEM focus Gains Opportunity for students to learnt about PAF technology Broader science potential 18 Parkes Cryo-PAF Jimi Green

19 Summary Cryo-PAF natural evolution for prolific multibeam system Science drivers overlap with all the major SKA science goals including pulsars, transients, HI Plus always the unknown! Competitive design outlined and prototyped Exploring funding opportunities (cryo-paf a very cost effective approach to experiments) 19 Parkes Cryo-PAF Jimi Green

20 Credit: Wayne England Thank you CSIRO Astronomy and Space Science Jimi Green Parkes Senior System Scientist, CASS Group Leader t e james.green@csiro.au w CSIRO ASTRONOMY AND SPACE SCIENCE