RECENT RESULTS FROM THE AUSTRALIAN SKA SITE Lister Staveley-Smith1,2,3

1.  International Centre for Radio Astronomy Research (ICRAR), University of Western Australia 2.  ARC Centre for All-sky Astrophysics (CAASTRO) 3.  Co-chair HI-Galaxy SKA science working group

0 Sec 1.

NAOC 2014 April 24

With funding from…

•  For discussions on: –  Intensity Mapping at Parkes, FAST, TianLai, SKA –  HI surveys on ASKAP and FAST –  Optical redshifts for HI stacking –  Flows and dark matter in the local Universe –  Australia-China collaboration

•  NAOC collaborators: –  Xuelei Chen, Di Li, Ming Zhu, JinLin Han, Xiang-Ping Wu –  And many others!

1

CAASTRO intensity mapping postdoc

Jonghwan Rhee

Outline

•  Australian SKA Pathfinder (ASKAP) –  HI surveys

–  Arecibo Ultra Deep Survey

–  Early results

•  Murchison Widefield Array (MWA) –  Description and science goals

–  GLEAM

•  Path to the SKA

2

Australian SKA Pathfinder (ASKAP)

•  Radio interferometer – 36 ×12-m dishes

•  CSIRO Phased Array Feed (PAF) technology: 36 beams

•  Frequency range 700 to 1800 MHz

•  Maximum baseline 6 km

•  First BETA six-antenna image in Apr 2014

•  ASKAP-12 early science in late-2015

3

Murchison Radio-astronomy Observatory (MRO)

Master Title 4

ASKAP MWA

ASKAP Science Survey Program

•  Wallaby: all-sky extragalactic HI survey

•  EMU: all-sky radio continuum survey

•  Also: Magnetism, Galactic Plane, Transients, VLBI,

Magellanic Clouds, deep HI survey, HI absorption

survey, pulsars

Master Title 5

Evolution of the star formation rate

Hopkins & Beacom (2006)

•  The rate at which stars in

galaxies are formed has declined

a factor of 10 in the last 7 billion

years (redshift 1 to 0).

6

Evolution of the cosmic gas density

•  However, the neutral gas supply

in galaxies seems not to have

declined.

•  Errors are high

•  Models are uncertain

Master Title 7

LMC

•  .

Stars & ionised gas (Smith; CTIO)

HI (Kim et al., Staveley-Smith et al.; ATCA/PKS)

•  . LMC/SMC optical (Mellinger)

LMC/SMC HI Parkes (Bruens)

ESO DG 28 Feb 2014 10

SKA HI pathfinders

ASKAP MeerKAT

ASKAP

•   36  x  12m  dishes  •   30  deg2  field  of  view  (via  PAF)  •   700-­‐1800  MHz  (300  MHz  instantaneous)  •   30  dishes  within  2km,  +6  within  6km  

FAST:

•  500m  dish  •  0.05  deg2  field  of  view  (1.4  GHz)  •  1050-­‐1450  MHz  (19  beams)  

 

 

WSRT-Apertif

MeerKAT :

•  64  x  13.5m  dishes  •  0.8  deg2  field  of  view  (1.4  GHz)  •  900-­‐1670  MHz  (2016)  

FAST

:

WSRT/Apertif:

•  12  x  25m  dishes  •  8  deg2  field  of  view  (1.4  GHz)  •  1000-­‐1700  MHz  (2016)  

HI Pathfinder Surveys

LADUMA (MeerKAT): - 10k galaxies, 1+ deg2, z<1.4, 5000 hours DINGO (ASKAP): - UDEEP: 50k gals, 60 deg2, 0.1<z<0.43 2500 hrs/

pointing - DEEP: 50k gals, 150 deg2, z<0.26, 500 hrs/pointing

DASH (APERTIF): - 25k galaxies, 40 deg2, 0.1<z<0.3 MED-DEEP (APERTIF): -  120k galaxies, 500 deg2, z<0.26

WALLABY (ASKAP) + WNSHS (APERTIF) + FAST: - 500k galaxies, all-sky, z<0.26

z = 1.4

z = 0

WALLABY

DINGO DEEP

DINGO UDEEP

LADUMA Small Area Deep

All-Sky Shallow

z=0.43

z=0.26

Master Title 12

Evolution of the HI mass function

Hoppmann, LSS et al. (2014)

13

z<0.06 z>0.06

AUDS

Cosmic Gas Density and AUDS results Hoppmann, LSS et al (2014)

14

First ASKAP extragalactic HI detection

15

Master Title 16

First ASKAP-BETA continuum image: 9 beams, 6 telescopes

Murchison Widefield Array (MWA)

•  Australia/NZ/India/US-funded radio interferometer

•  Radio-quiet SKA site

•  First operational SKA precursor (July 2013)

•  128 tiles (collecting area ~2750 m2 at 150 MHz)

•  Frequency range 80 to 300 MHz

•  Maximum baseline 3 km

•  Tingay et al. (2013)

Master Title 17

N.  Hurley-­‐Walker  (ICRAR/CurUn)  

1 beam per tile: 30 × 30 deg2 at 150 MHz

MWA – spatial tile layout •  Core:

–  ~50 tiles distributed uniformly within a 100 meter radius core

–  High surface brightness EOR sensitivity on ~1 degree scales

•  Mid-array:

–  additional ~60 tiles distributed out to 750 meters

–  Excellent PSF

•  Outliers: –  16 tiles at a radius of ~1.5

km –  ~2.5 arcmin resolution at

150 MHz Tingay  et  al.  2013  

Epoch of

Reionization

MWA EoR Observations

Daniel  Jacobs  (ASU)  Stepped  tracking  

MWA proof-of-concept results

•  Trial power

spectrum upper

limits

•  MWA 32T prototype

•  Only ~2 hours per

band

Dillon,  Liu  et  al.  (arXiv:1304.4229)  

MWA sensitivity and proof-of-concept limits

Beardsley  et  al.  2013  Dillon  et  al.  2013    

Figure:  D.  Jacobs  (ASU)  

Solar, heliospheric,

ionospheric science

and space weather

Radio Movie of Sun

16  May,  2013  04:11:04  –  04:16:00  UT    ν0=153.905  MHz  Δν=640  kHz    Δt=1  second    Imaging  Dynamic  Range  ~1500       D.  Oberoi  (NCRA-­‐TIFR)  

GaLactic and

Extragalactic All-sky

MWA Survey (GLEAM)

GLEAM team

Master Title 29

GLEAM team

Master Title 30

GLEAM team

Master Title 31

CHIPASS    (Calabreda,  Staveley-­‐Smith  &  Barnes  2014)  

MWA  (McKinley  et  al.  2013)  MOON  for  scale  

GaLactic and Extragalactic All-sky MWA (GLEAM) survey

•  Meridian drift-scan survey

–  Stable primary beam; minimal rotational synthesis

•  7 declination settings

–  +19o, +2o, −13o, −27o, −40o, −55o, −72o

•  Full polarimetry

•  80 to 230 MHz

–  8.3 in continuous λ2 coverage

•  300 hrs on-sky

•  Night observations only

•  RFI-free

Master Title 33

MWA – spatial tile layout •  Core:

–  ~50 tiles distributed uniformly within a 100 meter radius core

–  High surface brightness EOR sensitivity on ~1 degree scales

•  Mid-array:

–  additional ~60 tiles distributed out to 750 meters

–  Excellent PSF

•  Outliers: –  16 tiles at a radius of ~1.5

km –  ~2.5 arcmin resolution at

150 MHz Tingay  et  al.  2013  

U-V coverage: 1-hr GLEAM drift scan

1 hour synthesis, full 30 MHz bandwidth

Master Title 36

GLEAM

George Heald

MWACS positional errors Hurley-Walker et al.

37  

GLEAM status (2014 Mar 17)

•  21 nights of observation in Aug, Nov 2013 and Mar 2014

–  Observations 75% complete

•  CASA pipeline operational:

–  40 TB uv data so far processed into 31,454 snapshots

–  CASA analysis 16% complete (of data in hand)

–  WSclean implemented (Offringa)

•  RTS pipeline under development:

–  Better primary beam parametrisation and mosaicing

–  Ionospheric and polarimetric calibration

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Observations (TB) CASA analysis (TB)

RTS analysis(TB)

TB

100%

GLEAM: key science areas

•  Magellanic Clouds, nearby galaxies

–  Old diffuse CR population

•  SNRs, PWN, cosmic rays

–  Diffuse Galactic objects

•  HII regions; recombination lines

–  Ionisation physics

•  Radio galaxies, clusters, cosmic web

–  CR acceleration; shock physics

•  Magnetism; Faraday tomography

–  Mageto-ionic properties of ISM

Master Title 39

Small Magellanic Cloud GLEAM survey data taken August 2013 (Hurley-Walker)

GLEAM (2 min) optical

Fornax A (McKinley)

Fornax A: 13 mins at 154 MHz (McKinley)

VLA

MOSAIC of Southern Galactic Plane (Kaplan)

Ø  Science commissioning data at three frequencies

A new Giant Radio Galaxy in the local Universe Johnston-Hollitt et al.

43  

600 kpc

Polarisation snakes (Lenc)

•  A 20×20 deg2 linear polarisation gradient map imaged using 200-230 MHz GLEAM data at high Galactic latitude.

•  The gradient map highlights turbulence in the local ISM.

•  It is the first to be made in these frequency bands.

•  Structures also appear to be resolved – not previous seen.

•  Reveals Mach number of turbulence

GLEAM pointing movie: 2013-B and 2014-A

45 David Kaplan

MWA Time Assignment

“ –  Guaranteed Time (GT)

•  60% of available observing time •  Allocated to proposals led by or

comprising mostly MWA Individual Members

–  Open Access Time (OA)

•  20% of available observing time •  Allocated to proposals not led by an

MWA Individual Member or comprising <50% MWA Individual Members

–  Director’s Discretionary Time (DDT)

•  20% of available observing time •  Test and commissioning of non-

standard observing modes and capabilities

–  2015-A deadline

•  October 2014

photo:  John  Goldsmith  

SKA Phase 1

SKA1-­‐low  SKA1-­‐survey  

Murchison Radio-astronomy Observatory (MRO)

Master Title 48

ASKAP MWA

MRO and SKA phase 1

Master Title 49

SKA1-survey (650-1670 MHz)

SKA1-low (50-350 MHz)

MRO

Summary

•  Arecibo Ultra Deep Survey (AUDS):

–  Accurate measure of low-redshift neutral gas density

•  ASKAP:

–  HI and continuum commissioning results!

•  MWA:

–  GLEAM observations and analysis underway

•  SKA:

–  SKA1-low and SKA1-survey (Australia) expected in 2023

–  SKA1-mid (RSA) also 2023

•  SKA HI-Galaxy, ASKAP, MWA collaborations welcome!