GLEAM science from the first year of observations. Paul Hancock + the GLEAM TEAM
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1 GLEAM science from the first year of observations Paul Hancock + the GLEAM TEAM
2 The Martin Bell (CSIRO) Joe Callingham (USyd) K. S. Dwarakanath (RRI) Bi-Qing For (ICRAR/UWA) Tom Franzen (ICRAR/Curtin) Bryan Gaensler (USyd/Toronto) Paul Hancock (ICRAR/Curtin) Luke Hindson (VUW) Natasha Hurley-Walker (ICRAR/Curtin) Carole Jackson (ICRAR/Curtin) Melanie Johnston-Hollitt (VUW) Team Anna Kapinska (ICRAR/UWA) Emil Lenc (USyd) Ben McKinley (UMelb) John Morgan (ICRAR/Curtin) Andre Offringa (ASTRON) Pietro Procopio (UMelb) Lister Staveley-Smith (ICRAR/UWA) Randall Wayth (ICRAR/Curtin) Chen Wu (ICRAR/UWA) Cathie Zheng (VUW)
3 The MWA recall Randall s talk from yesterday or read 2013PASA T x Correlator = The MWA
4 MWA (u,v) coverage Snapshot, full bandwidth Snapshot, monochromatic Snapshot imaging!
5 Imaging strategy Snapshot imaging! In a 2-minute snapshot, MWA is close to coplanar Small w-terms can be fixed with appropriate imager We re using WSClean (Offringa et al, 2014) which includes our current best beam model Mosaic via image-plane co-addition after correcting for bulk ionospheric shifts and primary beam
6 GLEAM survey strategy Meridian drift scans as 2-minute snapshots, cycling through frequencies 7 DEC bands: 18.6, 1.6, -13.0, -26.7, -40.2, -55.0, Bands have significant overlap to allow primary beam response to be interpolated over the whole meridian 5 freq bands covering MHz, in MHz chunks Can be divided into 20x ~8 MHz sub bands
7 GLEAM Year 1 Obs 12 h 6h 0h 18 h 12 h GLEAM 1.3 Mar 2014 GLEAM 1.2 Nov 2013 GLEAM 1.1 Aug 2013 GLEAM 1.4 Jun 2014
8 GLEAM vs the world Wide bandwidth, moderate resolution, sensitive, all southern sky survey, with good low surface brightness sensitivity.
9 More details 2015PASA W
10 GLEAM near-term products Survey description paper 2015PASA W Polarised compact source catalogue: 2016 (Lenc) Southern Galactic plane map: 2016 (Hindson) Extragalactic ( b > 10) compact source catalogue (Stokes I): 2016 (HurleyWalker) Raw data are coming out of proprietary period Collaborate with a GLEAM-Team-er for some help
11 22 new SNRs in strip from GLON 345 to 255 New SNR 3-colour images from Luke Hindson (Victoria University of Wellington) in prep
12 The Radio Sky a-la GLEAM Unparalleled in freq coverage, FoV, surface brightness, cadence Credit: Natasha H-W
13 The Radio Sky a-la GLEAM What is all this wispy stuff? Credit: Natasha H-W
14 The Radio Sky a-la GLEAM What is all this wispy stuff? Credit: Natasha H-W
15 The Radio Sky a-la GLEAM What is all this wispy stuff? Credit: Natasha H-W
16 The Radio Sky a-la GLEAM This is all real emission!
17 GLEAM Extragalactic source catalogue Hurley-Walker et al. in prep Full analysis of GLEAM year 1 data focus on compact sources Using WSClean (Offringa) Using Aegean (Hancock, incl lots of special mods) With bulk ionosphere corrections (Morgan) With primary beam corrections (Callingham, Kapinska) Challenges: bright sources primary beam ionosphere changing effective PSF
18 Source finding - Aegean Aegean Find sources Characterise sources Sources can be gaussians or blobs BANE Characterise background Characterise noise Do it right Do it fast MIMAS Describe regions Combine regions Mask images Constrain Aegean Write MOC files
19 Catalog Strategy Wideband reference image MHz Create reference catalog from a deep, wideband, reference image For each narrow band image do a fit with priors from the reference catalog 8MHz narrow band Images (x20) Catalog contains all sources from deep image fluxes from each sub band for each source ZERO false cross ids Poster - The GLEAM survey: Images to Catalogs
20 SED for every source!
21 MRC Old Model + New data = See Jo Callingham s talk after lunch today
22 MRC Old Model + New data = New Model
23 GLEAM a legacy dataset for the MWA Coming soon to a VO-server near you!
24 GLEAM: One survey to rule them all Radio galaxies & AGN Your science here. Ask us how. Diffuse Galaxy & B field LMC/SMC SNRs & HII regions Galaxy clusters
25 2 GLEAM future Year 2 Twice the observing time vs year 1. Increased/different (u,v) coverage Alternate between HA +1 and HA -1 every ~6 weeks Same 7 DEC bands: +18.6, +1.6, -13.0, -26.7, -40.2, -55.0, Same 5 freq ranges covering MHz Improved frequency resolution: 10 khz Decreased time resolution: 2s (vs 0.5s)
26 Sensitivity vs LST (meridian) 154 MHz
27 GLEAM meridian beams Half-power contours 88 MHz XX (east-west) dipoles YY (north-south) dipoles 154 MHz
28 Ratio of XX / YY peak flux at Dec=+2 2nd order beam corrections (XX/YY) Hurley-Walker et al. in prep
29 2nd order beam corrections (XX/YY) Ratio XX/YY -> Old Beam Model Measured Predicted New Beam Model Declination ->
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