LOFAR Key Science Project Cosmic Magnetism in the Nearby Universe (MKSP)

LOFAR Key Science ProjectLOFAR Key Science Project

Cosmic MagnetismCosmic Magnetismin the Nearby Universein the Nearby Universe

(MKSP)(MKSP)

MKSP DocumentsMKSP Documents

Project Plan Project Plan (Science Case) (Science Case) – see MKSP Website– see MKSP Website

Project Description for LOFAR Book Project Description for LOFAR Book – submitted– submitted

MKSP Memo No. 1:MKSP Memo No. 1: Frequency Coverage AnalysisFrequency Coverage Analysis – by George Heald– by George Heald

MKSP Memo No. 2:MKSP Memo No. 2: Pulsar Studies of the Galactic Magnetic Field with LOFARPulsar Studies of the Galactic Magnetic Field with LOFAR - by Aris Noutsos- by Aris Noutsos

MKSP observation planMKSP observation plan

Galaxy surveyGalaxy survey (60 galaxies, 180-210 MHz, (60 galaxies, 180-210 MHz, 99h per galaxy,h per galaxy, together with Surveys KSPtogether with Surveys KSP))

Deep galaxy surveyDeep galaxy survey (10-20 galaxies, 120-180 MHz, (10-20 galaxies, 120-180 MHz, 100h per galaxy100h per galaxy))

Milky Way fieldsMilky Way fields: piggyback with deep extragalactic fields: piggyback with deep extragalactic fields

Radio galaxiesRadio galaxies (10 galaxies, 3 frequency bands, 5h per galaxy and band)(10 galaxies, 3 frequency bands, 5h per galaxy and band)

Stellar jetsStellar jets (5 objects, 120-180 MHz, 20h per object)(5 objects, 120-180 MHz, 20h per object)

LOFAR sensitivityLOFAR sensitivity(second revision)(second revision)

100h:100h:σσ ≈≈ 15 15 μμJyJy

J. AndersonJ. Anderson

LOFAR sensitivityLOFAR sensitivity(second revision)(second revision)

100h:100h:δΦδΦ ≈≈ 0.10.1 rad mrad m-2-2

for 75 for 75 μμJyJy sources sources

J. AndersonJ. Anderson

Observation timeObservation time

Total observation time needed for the deep fields:Total observation time needed for the deep fields: ≈ ≈ 1000-2000 h1000-2000 h

Total time for all national LOFAR consortia within the firstTotal time for all national LOFAR consortia within the first 5 years5 years (assuming 50% efficiency and 10 (assuming 50% efficiency and 10 →→ 64% open time): 64% open time): ≈ ≈ 14000 h14000 h

The MKSP needs The MKSP needs ≈ ≈ 10% of the available time !10% of the available time !

Some LOFAR PoliticsSome LOFAR Politics

Total observation time for GLOW in 5 years: 2600 hTotal observation time for GLOW in 5 years: 2600 h

The MKSP needs ≈60% of the time available for GLOWThe MKSP needs ≈60% of the time available for GLOW

5 German stations, wide interests: realistically only 20%5 German stations, wide interests: realistically only 20%

International support needed !International support needed !

New: 2 M€ Funding by DFGNew: 2 M€ Funding by DFGResearch network on observing magnetism with LOFAR:Research network on observing magnetism with LOFAR:

Magnetization of Interstellar and Intergalactic Media -Magnetization of Interstellar and Intergalactic Media -The Prospects of Low-Frequency Radio ObservationsThe Prospects of Low-Frequency Radio Observations

Speaker: Speaker: Uli Klein, Univ. BonnUli Klein, Univ. BonnVice Speaker:Vice Speaker: Rainer Beck, MPIfR Bonn Rainer Beck, MPIfR BonnFurther project leaders: Further project leaders: D. Bomans, M. Brüggen, R.-J. Dettmar, D. Bomans, M. Brüggen, R.-J. Dettmar, D. Elstner, T. Enßlin, M. Hoeft, Harald Lesch, W. ReichD. Elstner, T. Enßlin, M. Hoeft, Harald Lesch, W. Reich

Available positions: 11 PhD, 2 postdocs Available positions: 11 PhD, 2 postdocs (not yet filled)(not yet filled)

Start: June 2010Start: June 2010

Funding: 3+ yearsFunding: 3+ years

Kickoff workshop: October 2010Kickoff workshop: October 2010

DFG Research UnitDFG Research Unit

RM SynthesisRM SynthesisRM synthesis works on observed Q,U cubes in wavelength toRM synthesis works on observed Q,U cubes in wavelength toproduce a cube of the complex Faraday dispersion functionproduce a cube of the complex Faraday dispersion function(pol. amplitude and intrinsic angle)(pol. amplitude and intrinsic angle) in Faraday depth in Faraday depth ΦΦ::

QQ UU

FFrr

FFii

RM SynthesisRM Synthesisλλ22 λλ22

ΦΦ ΦΦ

RM SynthesisRM Synthesis

RM Synthesis pipeline:RM Synthesis pipeline: Under construction, ready until start of MSSSUnder construction, ready until start of MSSS (Th. Riller, MPA Garching)(Th. Riller, MPA Garching)

Offline tools (RM Synthesis++):Offline tools (RM Synthesis++): Wiener Filter Wiener Filter (S. Duscha, Th. Riller & Th. Enßlin, MPA Garching),(S. Duscha, Th. Riller & Th. Enßlin, MPA Garching), Wavelet RM SynthesisWavelet RM Synthesis (R. Stepanov & P. Frick, ICMM Perm) (R. Stepanov & P. Frick, ICMM Perm)

Wavelet-basedWavelet-basedRM Synthesis (1)RM Synthesis (1)

Frick et al. 2010Frick et al. 2010

Perfect observation: complete wavelength rangePerfect observation: complete wavelength range

Wavelet-basedWavelet-basedRM Synthesis (2)RM Synthesis (2)

Frick et al. 2010Frick et al. 2010

385 – 500 MHz385 – 500 MHzGaussian component hardly visibleGaussian component hardly visible

Wavelet-basedWavelet-basedRM Synthesis (3)RM Synthesis (3)

Frick et al. 2010Frick et al. 2010

120 – 500 MHz120 – 500 MHzGaussian component not visible with classical RM Synthesis,Gaussian component not visible with classical RM Synthesis,

box component visible as two hornsbox component visible as two horns

PlansPlans Commissioning observations Commissioning observations (2010):(2010): Develop and test software for pol calibration,Develop and test software for pol calibration, RM Synthesis and source finding, …RM Synthesis and source finding, … (see next talk by James)(see next talk by James)

Million Source Shallow SurveyMillion Source Shallow Survey ( (MSSS, MSSS, 2010):2010): find polarization calibratorsfind polarization calibrators

Magnetism Early Experiment ExplorationMagnetism Early Experiment Exploration ( (MEEEMEEE, 2011):, 2011): Calibration techniques, extended sources, deep test fieldsCalibration techniques, extended sources, deep test fields

ASKAPASKAP(Australian SKA Pathfinder)(Australian SKA Pathfinder)

ASKAPASKAP: : 36 antennas of 12m diameter, max. baseline 6km,36 antennas of 12m diameter, max. baseline 6km,frequency range 0.7 -1.8 GHzfrequency range 0.7 -1.8 GHz

POSSUMPOSSUM: : POlarization Survey of the Universe´s MagnetismPOlarization Survey of the Universe´s Magnetism All-sky polarized continuum at 1.4 GHzAll-sky polarized continuum at 1.4 GHz Rotation measures for Rotation measures for ≈ ≈ 1.5 million sources (1.5 million sources (≈ ≈ 50 RMs/deg50 RMs/deg22)) Recognize large-scale fields in Milky Way, nearby galaxies and clustersRecognize large-scale fields in Milky Way, nearby galaxies and clusters

MeerKATMeerKATMeerQUITTENS:MeerQUITTENS:MeerKAT QU Investigation To Trace Extragalactic Nonthermal SourcesMeerKAT QU Investigation To Trace Extragalactic Nonthermal Sources

Deep imaging of synchrotron pol & RM grid of nearby spiral Deep imaging of synchrotron pol & RM grid of nearby spiral and dwarf galaxies, galaxy groups and clustersand dwarf galaxies, galaxy groups and clusters

900-1750 MHz and 8-10 GHz900-1750 MHz and 8-10 GHz Ideal complement to LOFARIdeal complement to LOFAR