Radio Transients with Apertif Joeri van Leeuwen
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1 Radio Transients with Apertif Joeri van Leeuwen
2 [ movie at alert.eu.org ]
3 Apertif Phased Array Feeds 1.4 GHz, 300 MHz bandwidth, T sys = 70K
4 Apertif WSRT: Increased field of view 8.7 sq. deg. instantaneously
5 Apertif Status and timeline Dishes: all 12 retrofitted
6 Apertif Status and timeline Frontend PAFs: all in place
7 Apertif Status and timeline Frontend Cabling and Electronics: all in place
8 Apertif Status and timeline Correlator/Beamformer Electronics: all in place
9 Apertif Status and timeline Correlator/Beamformer Firmware & Software: in place, being commissioned now, 2016Q3 (Roy Smits, Emily Petroff, Yogesh Maan, Klim Mikhailov, Samayra Straal, Leon Oostrum,..)
10 Apertif Status and timeline Survey team: formed, buy-in continues to be possible, for data access before public release 10
11 Apertif Status and timeline Survey definition (5yr) : agreed and published, Imagining surveys commence 1 Jan 2017, time-domain (dedic. + comm.) starts 1 March 2017 Imaging (shallow + medium-deep) Time-domain dedicated (ALERT)
12 Science Overview What is the fundamental physics of space-time and matter? Where does our understanding of general relativity break down? How is matter accreted and expelled in strong gravity? How do black holes influence galaxy formation? Discover and characterize cosmological radio bursts, supernovae, neutron stars, and black holes.
13 Science Supernovae and Gamma-Ray Bursts Paragi et al. (2010)
14 Science Neutron Stars After Demorest et al. (2010)
15 Science Cosmological radio bursts Fast Radio Bursts (FRBs) at cosmological distances 2007 Parkes Lorimer burst 2013 Arecibo burst Spitler et al. (2014, 2016)
16 Science Cosmological radio bursts The origin of the bursts remains unexplained. Coalescing compact objects? X-ray afterglows Connected to the unexplained slow radio transients? Radio afterglows Supernova related? Optical, host galaxies Naked explosions? Consistent absence of galaxies Detect, localize, characterize
17 The ALERT survey Apertif: 8.7 deg 2 field, 20 frames/ms Westerbork Apertif
18 The ALERT survey LOFAR: resolution and sensitivity, at low frequency see Coenen, van Leeuwen et al. 2014
19 The problem and the opportunity
20 The solution: a real-time hybrid FPGA-GPU transient machine 2.1 Tbps > 150 Gbps 25 TMAC/s 150 Gbps -> 3.0 Tbps -> 0.2 Gbps 500 TFLOPS
![The solution: a real-time hybrid FPGA-GPU transient machine 16 Uniboard (128 Altera Stratix IV) [ 450 TABs, dedicated ] 5 Uniboard 2 (20 Altera Arria10) [](/docs-images/90/101589605/images/21-5.jpg "250 TABs, 24/7 ] 40 Servers 640 CPU Cores 160 GPUs (NVIDIA/AMD) 1 PFLOP (Top 250) 1 PB disk 10 TB RAM 50 Gbps to the world 6 Racks 50 kw (Air+Water")
21 The solution: a real-time hybrid FPGA-GPU transient machine 16 Uniboard (128 Altera Stratix IV) [ 450 TABs, dedicated ] 5 Uniboard 2 (20 Altera Arria10) [ 250 TABs, 24/7 ] 40 Servers 640 CPU Cores 160 GPUs (NVIDIA/AMD) 1 PFLOP (Top 250) 1 PB disk 10 TB RAM 50 Gbps to the world 6 Racks 50 kw (Air+Water cooled)
22 The solution: a real-time hybrid FPGA-GPU transient machine 16 Uniboard (128 Altera Stratix IV) 5 Uniboard 2 (20 Altera Arria10) 40 Servers 640 CPU Cores 160 GPUs (NVIDIA/AMD) 1 PFLOP (Top 250) 1 PB disk 10 TB RAM 50 Gbps to the world 6 Racks 50 kw (Air+Water cooled)
23 Fast transients: the ALERT survey after Coenen, van Leeuwen et al. 2014
24 Fast transients: The ALERT survey compared
25 Fast transients: The ALERT survey follow-up Radio, x-ray, gravitational-wave & optical follow-up Interpretation & modelling Host and progenitor associations, expected rates Electron density and distribution along lines of sight Coherent & afterglow emission, acceleration, densities
26 Slow transients: The Apertif Medium Deep Seven 12-hr repeats at 15 μjy/beam each, over 450 sq. deg. When emphasizing 3-month cadence, the peak timescale at 1.4 GHz for the afterglows for GRBs and TDEs: after Carbone et al. 2016
27 Conclusions Apertif on WSRT will offer a combination that is unique in the world, of wide-field detection and high-precision radio characterization. Through blind and triggered searches for fast and slower transient radio emission we intend to understand how dense matter behaves under extreme gravity.
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