Long Baseline Array Chris Phillips LBA Lead Scientist 5 September 2018 CSIRO ASTRONOMY & SPACE SCIENCE

Long Baseline Array Chris Phillips LBA Lead Scientist 5 September 2018 CSIRO ASTRONOMY & SPACE SCIENCE

The Long Baseline Array (LBA) Operated as a National Facility by CSIRO Astronomy & Space Science, in close cooperation with the University of Tasmania, Hartebeesthoek Radio Observatory and Auckland University of Technology Core elements: ATCA (5x22m), Mopra (22m), Parkes (64m), Ceduna (30m), Hobart (26m) + Tidbinbilla (70m & 34m), Warkworth (12m & 30m), Hartebeesthoek (26m & 15m), ASKAP (12m), AuScope (3x12m), plus ad-hoc arrangements with Korea and China. Typically ~25 days observing each year in ~4 sessions Plus RadioAstron survey and imaging experiments, some EVN/global experiments

EAVW 2018 LBA Phillips

Baseline lengths in km Pa At Mp Ho Cd Hh Yg Ke Ak Ww Ti Pa 0 322 207 1089 1361 9665 3128 2610 3091 2425 274 At 322 0 114 1396 1508 9847 3266 2493 3202 2409 566 Mp 207 114 0 1286 1448 9783 3213 2530 3159 2411 458 Ho 1089 1396 1286 0 1702 9167 3211 3431 3273 2415 832 Cd 1361 1508 1448 1702 0 8944 1792 1937 1756 3718 1455 Hh 9665 9847 9783 9167 8944 0 7848 9504 8019 10480 9589 Yg 3128 3266 3213 3211 1792 7848 0 2360 290 5362 3196 Ke 2610 2493 2530 3431 1937 9504 2360 0 2102 4752 2849 Ak 3091 3202 3159 3273 1756 8019 290 2102 0 5360 3184 Ww 2425 2409 2411 2415 3718 10480 5362 4752 5360 0 2301 Ti 274 566 458 832 1455 9589 3196 2849 3184 2301 0

The Long Baseline Array (LBA) Regular observations in 20, 13, 6, 3, 1cm bands 1.4-25 GHz Not all telescopes support all bands ATCA, Mopra 7 & 3mm, Tid 7mm Disk-based recorders (with most data later streamed to the correlator), evlbi available on subset of the array LBADR, Mk5b and flexbuf recorders Max bit-rate 1Gbps Data correlated on DiFX software correlator at Pawsey supercomputing facility Deller et al. 2007, PASP, 119, 318 (DiFX) Deller et al. 2011, PASP, 123, 275 (DiFX-2)

Locations & SEFDs (in Jy) of LBA elements Lat. Long. 20cm 13cm 6cm 3cm 1.5cm 9mm ATCA 5x22m 150 E 30 S 40 40 36 39 106 180 ASKAP 1x12m 117 E 26 S 6000 -- -- 3500 -- -- Ceduna 30m 134 E 32 S 1500 400 450 600 2500 -- Hobart 26m 147 E 43 S 450 650 650 560 1800 -- Hart 26m 28 E 26 S 200 210 290 340 1320 -- Mopra 22m 149 E 31 S 340 530 350 430 675 900 Parkes 64m 148 E 33 S 40 30 110 43 810 -- Tid 70m 149 E 35 S 23 16 -- 25 60 -- Tid 34m 149 E 35 S -- 165 -- 90 -- 180 Warkworth 12m 175 E 37 S 7000 3500 -- 3500 -- -- Warkworth 30m 175 E 37 S -- -- 650 1000 -- --

LBA Science in a year Measuring accurate position, velocity and distance (via parallax) to objects in our own Galaxy Figure 1: Left 22 GHz water maser emission in G 339.884 for our absolute proper motion measurements. The spectrum the inset showing an expanded view at high velocities includin of 8.6 GHz radio (Ellingsen et al. 1996) and 10 µm mid infr maser emission in G 339.884 1.259. Methanol masers (filled ci Forster & Caswell 1989) and OH masers (squares Caswel possible bipolar mass loss events. The diagonal line indicates proper motion and magnetic field measurements. Young massive stars, evolved stars, pulsars, gamma ray sources, black holes Accurately measure the structure and rotation of our own Galaxy Figure 2: The 3 D kinematics of the 6.7 GHz methanol (left) and (Sanna et al. 2010). The cones represent the direction and unce It is clear that both varieties trace distinctive structures and ar are concentrated towards the central region of G 23.01 0.41 i the plane, while the methanol masers trace a ring with proper EAVW 2018 LBA Phillips motion measurements is that the maser spot evolution will be u reference. T his will eliminate any biased analysis of the maser using an arbitrary reference point located within the source. T

LBA Science in a year (cont) Study the jets of Galactic and extra galactic black holes Study molecular disc around Circinus galaxy using water molecules Long term monitoring of radio jets from gamma ray loud AGN Detection of radio emission towards recent gravitational wave EAVW 2018 LBA Phillips

LBA Science in a year (cont) Improve the international radio reference frame (ICRF) Determine if SMBH candidate is binary source Detect radio emission from 90 Jupiter mass brown dwarf star Systematically compare optical and radio positions of galaxies ure 3: Left: Position uncertainties from prior LCS observations (blue point s) and new v561 obserons (gr een point s) after accounting for systematic errors; Right: an an example of a preliminary ge of EAVW a 2018 source LBA observed Phillips in v561a that has never been imaged before. The jet direction is reliably rmined.

Current Developments - ASKAP

Current Developments Parkes Ultrawideband receivers 700-4000 MHz Rx installed May 2018 22 K Tsys across band 4 GHz-26 GHz planned, not funded Focus cabin digitizers 12 bit quantization GPU based backend Single backend for all modes Adaptive RFI mitigation Investigation new calibration Pseudo random noise, picosecond pulse

Current Status: Pulsar Fold Mode Courtesy of W. van Straten EAVW 2018 LBA Phillips 12

Current Developments (cont) Parkes cryo-paf funding proposal to be submitted 36 beam backend limited by digital backend 20K Tsys better than current 13 beam multi-beam ATCA GPU backend planning 8 GHz bandwidth Demonstrated viability at GPUhackathon ASKAP tied array beam? PAF VLBI already demonstrated User Parkes-ASKAP experiment in December

International Collaborations? Investigating formally joining global VLBI experiments Single proposal requirement Software correlation and disk base recording make array interoperability much easier Should be be doing more Asia-LBA observing? Asian telescopes as part of LBA experiments LBA antenna as part of EAVN? Logistics are not trivial: Data transport (firewalls) Backend/receiver compatibility Educate observers on availability

Thank you CASS/ATNF Chris Phillips LBA Lead Scientist t +61 2 9372 4808 E Chris.Phillips@csiro.au w www.atnf.csiro.au CSIRO ASTRONOMY & SPACE SCIENCE

CODIF CSIRO Oversampled Data Interchange Format Extension to VDIF Based on VDIF2 proposal by Alan Whitney Used with CSIRO PAF at Bonn and Jodrell Added CODIF support to DIFX Used with ASKAP CRAFT project to localize FRBs