Observing the sky with MeerKAT
Kurt van der HeydenOn behalf of:
MeerKAT & Deep Continuum team
What is MeerKAT?
• Countries shortlisted to host the SKA: South Africa and Australia
• Both countries are building Pathfinders
• South Africa’s Pathfinder is called MeerKAT and will be located in the Karoo desert
Candidate South African SKA site (along with some locals)
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MeerKAT Overview• Most sensitive centimetre wavelength instrument in
the southern hemisphere• MeerKAT will be used in remote observing mode• Fast dedicated fiber link from Karoo to Cape Town
completed by mid 2010• MeerKAT Operations and Science Centre in Cape
Town (Site selection underway)
Amsterdam
Rome
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Karoo Site
Karoo Astronomy Reserve
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• Close cooperation with broadcast and telecom operators during drafting of the Act
• Protects radio and optical astronomy
• Minister has broad powers
Karoo Astronomy Reserve
System Properties
Roll out schedule
KAT
Meer KAT
MeerKAT
Phases
• central Gaussian core:
• dispersion 300 m, max baseline ~1 km
• Gaussian outer component:
• dispersion 2.5 km, max baseline ~8 km
• Both components random 2D distribution
Array Configuration
Reference design :
1 km
8 km diameter
5 km diameter1 km
shortest baseline 20mlongest baseline of central
array 8 km
Poi
nt s
ourc
e se
nsiti
vity Sensitivities other telescopes
according to their exposure calculators
MeerKAT
Col
umn
dens
ity s
ensi
tivity
Sensitivities other telescopesaccording to their exposure
calculators
MeerKAT
courtesy E. de Blok
PSF plots for δ = −30o; major-axis cross section denoted by solid line, minor axis-section denoted by dotted line
courtesy B. Frank
PSF (dec = -30)
t=8h, δ=-30°
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weighted uv distribution
-100
-100
100
arcsec
30-30
-30
30
arcsec
-8 km 8 km
8 km
-8 km
-2 km
-2 km
-2 km 2 km
weighted beam
Weights & Beams
courtesy B. Frank
Sensitivity
• Low column density HI associated with the Cosmic Web and galaxy environments
• Ultra-deep narrow-field HI survey out to z=1.4 using gravitational lens amplification
• High spatial dynamic range HI imaging of 1000 galaxies
• Ultra-deep narrow-field continuum surveys down to micro-jansky detection limits
• Mapping magnetic fields in clusters
• All-sky continuum survey at 600 MHz
• Pulsar timing and monitoring
• SNR detection and GRB follow-up
• OH mega-masers and Zeeman splitting
• Galactic gas dynamics and magnetic fields
MeerKAT Science: L & S Band
MeerKAT Science: X & Ku-band
• All-sky (??) continuum survey at 8 GHz• Detection of CO lines at high redshift (z>6)• Mapping of S-Z clusters• Transients sources in the Galactic centre
• Observing time split between the Key Projects (~75%) and “normal” proposals (~25%)
• Call for Key Project proposals : deadline 15 March 2010
• Open access
• Key Project teams expected to contribute to pipelines, simulations etc
• SA SKA will support Key Projects in SA with postdocs, students
Call for Proposals
Tier-1: 1000 square degrees to 5µJy rms ; possible fields VISTA-VIKING and KIDS fields. large-scale structure of the Universe at z ~1; Possibly combine UV data with EMU. Time estimate: 1250 hours
Tier-2: 35 square degrees to 1µJy (rms); possible fields Elais-S1 (0037-43), XMMLSS (0218-05), ECDFS (0332-27) and COSMOS (1000+02). sensitive to starbursts of 100 M yr−1 at z ~4 and SCUBA-type galaxies with > 500 M yr−1 up to z > 7. Time estimate: 1050 hours
Tier-3: A single pointing to 0.1µJy (rms), possibly over Chandra-Deep-Field South - push the telescope to its limit and studies of star-formation and AGN activity to levels
Continuum ProposalCo-Pi’s K. vd Heyden & M. Jarvis
• To trace the evolution of strongly star-forming galaxies from z~6 to the present day, and quiescent star forming systems from z=1-2, using a wavelength unbiased by dust or molecular emission.• To trace the evolution of super-massive black holes throughout the history of the Universe, and understand their relationship to star-formation.• assess the AGN mechanical feedback and environmental impact on the intergalactic medium• To explore an uncharted region of observational parameter space
Some key Science goals
• Identify rare or specific populations (through techniques involving radio spectral index measurement?)
• Explore and develop techniques for extracting the maximum information from deep and potentially confused radio images.
Additional Science goals
AGN & Blackholes: Michael Brown, Anton Koekemoer, Somak Raychaudhury, Encarni Romero, Philip Best, Garret Cotter, Raffaella Morganti, Isabella Prandoni, Andrew Hopkins, Catherine Cress, Martin Hardcastle, Edo Ibar, Matt Jarvis
Galaxy Clusters: Marcus Brüggen, Somak Raychaudhury, Ian Smail, Jim Geach, Malcolm Bremer, Anna Scaife, Anton Koekemoer, Catherine Cress, Ilani Loubser, Martin Hardcastle, Nadeem Oozeer, Matt Jarvis
SF & SFH: Sung(eun) Kim, Stuart Lumsden, Philip Best, Isabella Prandoni, Andrew Hopkins,CatherineCress, Rob Ivison, Anton Koekemoer, Anna Scaife, Matt Jarvis
Galaxy Evolution: Loretta Dunne, Malcolm Bremer, Benne Holwerda, Chris Conselice, Ilani Loubser, Chris Pearson, Ian Smail, Anton Koekemoer, Jim Geach, Andrew Hopkins, Michael Brown, Rob Ivison, Edo Ibar, Matt Jarvis
High z Radio Galaxies: Girish Beeharry, Huub Rottgering, Philip Best, Anton Koekemoer, Chris Conselice, Catherine Cress, Rob Ivison, Hans-Rainer Kloeckner, Edo Ibar, Matt Jarvis
Cosmology: Girish Beeharry, Mathew Smith, David Bacon, Yabebal Tadesse, Roy Maartens, FilipeAbdalla, Marco Regis, Renee Hlozek, Catherine Cress, Matt Jarvis
The Polarized Sky: Richard Battye, Ian Browne, Neal Jackson
Transients: Patrick Woudt, Michael Bietenholz
Science Teams
Commissioning: Marcus Brueggen, Martin Hardcastle, Nadeem Oozeer, Rob Beswick, Viral Parekh, Deb Shepherd, Glenn White
Skills transfer and development: Bruce Bassett, Catherine Cress, Garret Cotter, Girish Beeharry, Renee Kraan-Korteweg, Matt Jarvis, Isabella Prandoni, Roy Marten, Matt Smith, Yabebal, Renee Hlozek, Nadeem Oozeer, Michael Garrett
Software, pipeline and simulations: Jose Afonso, Marcus Brüggen, Richard Willman, Nic Walton, Mike Irwin, Eduardo Gonzalez-Solares, Anna Scaife, Hans-Rainer Kloeckner, Anton Koekemoer, Yabebal Tadesse, Catherine Cress, Mark Lacy, Rob Ivison, Rob Beswick, Glenn White, Filipe Abdalla, Anthony Smith, Seb Oliver, Bradley Frank, Rob Ivison, Edo Ibar, Anna Scaife. Viral Parekh, Ian Stewart, Steve Rawlings
Survey strategy and field selection: Matt Jarvis, Michael Brown, Mattia Vaccari, Steve Maddox, Jose Afonso, DimitraRigopoulou, Rob Ivison, Anton Koekemoer, Isabella Prandoni
MeerKAT-EMU-APERTIF-Lofar collaboration: Ray Norris, Roy Booth, Huub Rottgering, Matt Jarvis, Anton Koekemoer, Glenn White, Philip Best, Andrew Hopkins
Salt & other wavelength collaboration: Encarni Romero, Alexei Knaizev, Benne Holwerda, Anton Koekemoer, Loretta Dunne, Nic Walton, Mike Irwin, Eduardo Gonzalez-Solares, Glenn White, Seb Oliver, Chris Pearson, Matt Jarvis, Petri Vaissanen, Kurt van der Heyden, Nicola Loaring
Multi-wavelength synergies: Manda Banerji, Stephen Serjeant, Mattia Vaccari, Michael Brown, Nicholas Seymour, Anton Koekemoer, Loretta Dunne, Girish Beeharry, Nic Walton, Mike Irwin, Eduardo Gonzalez-Solares, Mathew Smith, DimitraRigopoulou, Ilani Loubser, Chris Conselice, Philip Best, Anthony Smith, Michael Garrett, Kristen Coppin, Seb Oliver, RaffaellaMorganti, Isabella Prandoni, Andrew Hopkins, Rob Ivison, Chris Pearson, Anna Scaife, Matt Jarvis
Data Archive & VO: Nic Walton, Ian Stewart, Encarni Romero, Mark Lacy
Technical Teams
MeerKAT
Sensitivities
Borrowed from
Norris et al
MeerKAT ASKAP
Unexplored territory
????
Continuum Surveys - Complimentarity
EMU + MeerKAT:• Combine UV data for 1000 sq deg (5 uJy) ??
LOFAR + MeerKAT (+ Apertif?):• Some overlap around equatorial region, ~20-30 deg??
MeerKAT + EMU + LOFAR (Apertif?)Data analysis (interferometry techniques etc)Software – data simulation, modeling, source confusion algorithms,
source identification & paramertirasationOptimisation of commensal observations Data storage, Joint source catalogues/databasesInterchange/sharing of expertise (staff, PDR, students) & resources?
• In 2005 the South African SKA Project initiated a targeted “Youth into Science and Engineering Programme” to develop highly skilled young scientists and engineers.
• The programme offers comprehensive bursaries to students in engineering, mathematics, physics and astronomy at undergraduate and postgraduate level.
• To date supported: >80 postgraduate students, 11 postdocs, 40 undergraduate students
• 5 SKA Research Chairs awarded (3 Science, 2 Technical) -funding for 15-year positions to build additional SKA-related research groups
Human Capacity
• THINGS: ~500 h
• VLA B, C and D on 34 galaxies
• per galaxy:
• 7.5h in B
• 2.5h in C
• 1.5h in D
• How does MeerKAT compare
MeerKAT THINGS(De Blok et al)
• Detailed maps of nearby galaxies can be obtained in same time and ~same sensitvity as VLA-B array observation, but with the C & D short baselines (and more) included
MeerKAT “Super” THINGS
Since the HI signal is weak, we use independent measurements of galaxy z before stacking:
• STEP 1: extract spectra using known positions and z (optical spectra)
• STEP 2: Using known z values, shift all lines to common channel
• STEP 3: Co-add spectra
Deep HI Survey(S-L. Blyth & B. Holwerda)
S1: 3 month, single pointing S3: 1 year, single pointing
Quick Comparison at z=0.4
ThunderKAT
MeerKAT Transients Key Science ProjectCo-PIs: Patrick Woudt (UCT) & Rob Fender (Southampton)
Astrophysics of accretion-induced relativistic outflows
Radio transients: - microquasars- complete census of LMXBs in the Galactic Bulge (population synthesis)- cataclysmic variables as jet sources- Extragalactic transients (ULXs)- Gamma-ray bursts- (obscured) radio SNe
ThunderKAT
The Hunt for Dynamic and Explosive Radio Transientswith MeerKAT
Global transient network of SKA precursors/pathfinders
Complementary approach: - Survey of the Galactic Bulge (census of faint LMXBs) and local Volume Galaxies- Monitoring of known sources- Commensal transient detection in other MeerKAT surveys- Target of Opportunity follow-up (MeerKAT, LOFAR, ASKAP)
MeerKAT/ThunderKAT
LOFAR/Transients KSP
ASKAP/VAST
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Dish Fabrication Facility
KAT-7 dish mould assembly
25At Karoo site
KAT-7 dish mould
Resin infusion
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Steel backing structure
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Completed reflector
30mould ~0.5mm rms: ~15 GHz
First KAT-7 antenna
July 2009
Then there were five
3 weeks ago
Is it real or is it cardboard?
Rob & Patrick (Feb 2010)
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