Lunar Radio Astronomy Explorer (LRX)
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1 Lunar Radio Astronomy Explorer (LRX) Opening the last unexplored wavelength window to the universe Heino Falcke LOFAR International Project Scientist Dept. Astronomy, ersity, Netherlands Foundation for Research in Astronomy (ASTRON) + Sebastian Jester MPIA Heidelberg
2 Basic Assumptions With the return to the Moon, a very-low frequency telescope is at the top of longterm science priorities around the world. Use first lander missions for prototyping and astronomical site-testing (if not EU then China ) Take ESA-NEXT study as first test case (boundary conditions) Develop demonstrator payload (TR6) consisting of 1-3 radio modules
3 Current Status at Long Wavelengths Extremely poor resolution, strong diffuse Galactic emission RAE-2 observations, Novaco & Brown 1978 T sys freq (MHz ) galactic synchrotron emission free-free absorption 4.7 MHz 1.31 MHz H. Falcke slide from G. Woan
4 Moon-Rotation Synthesis of Equatorial Strip Baseline Resolution 100m m 6 1km km 0.6
5 Maohai Huang, Astron. Obs. China
6 Galactic Background and local bubble With a couple of degree resolution we could perhaps see some holes in the ISM.
7 Observability Constraints Survey Resolution Maximum resolution and baseline are limited by interstellar and interplanetary scattering IPM scattering has not been measured well at low frequencies and could be a factor 15 smaller than given. 0.1 MHz is lowest useful frequency. MHz 30 MHz ~30 km H. Falcke Jester & Falcke (2007)
8 Observability Constraints Survey Sensitivity RMS sensitivity (1-sigma noise level) of an array of crossed dipoles (antenna effective area = 2 /4), for 5% fractional bandwidth and 24h observing time. Left axis gives the pointsource sensitivity. 1 1 MHz corresponds to 10 1 GHz ( -0.7 ) Right axis yields the surface brightness sensitivity in K for one resolution element after multiplying the given value by the square of the array's maximum baseline D, where D is measured in meters MHz 1 MHz N=100 H. Falcke Jester & Falcke (2007)
9 Jester & Falcke (2007) Observability Constraints Confusion Limit confusion limit maximum number of antennas EOR league km 100 µ MHz
10 HI in the dark ages The 21cm signal in the very early cosmoc is simply shaped by gravity, adiabatic cosmic expansion, and wellknown atomic physics and is not contaminated by complex astrophysical processes that affect the intergalactic medium at z < 30. Very rich data set Extremely difficult observation and calibration (req.: SNR>1,000,000:1) Needs perfect conditions & extensive prototyping H. Falcke Decoupling of CMB, gas, and spin temperatures Loeb & Zaldarriaga, Phys. Rev. Lett., 2004 Scott & Rees, MNRAS, 1990
11 HI in the dark ages 21 cm signal can in principle be detected in <1 year integration time at MHz. Problem is the unknown foreground contamination and spectral roughness Signal is only 10-6 of foreground! Feasibility needs to be studied by measuring spectral smoothness. H. Falcke Jester & Falcke (2008)
12 Ultra-High Energy Cosmic Rays & Neutrinos Astroparticle physics crown jewels: Ultra-high energy elementary particles with energies a Billion times higher than at CERN! They are rare and one needs a large detector volume Particles hitting the moon produce detectable radio Cherenkov emission. The moon is by far the largest particle detector available for astroparticle physics! Best data from radio obs. We need to understand the moon radio from neutrinos hitting the moon Gorham et al. (2000), Falcke & Gorham 2003, Scholten et al. (2006) Lunar array: Size: 3 Dipoles Time: ~ 1 year
13 Properties & Requirements Lower Frequencies: less SNR but higher isotropy of emission. 10 MHz only sees a few (but all) events per year at ev. 100 MHz will see 7 events per day at ev 10 MHz gives >1 cubic kilometer detector for neutrinos Also: Search for impulsive e.m. noise from meteorites and geological activities. Angular spread of emission 2.2 GHz 100 MHz Cherenkov angle
14 Philippe Zarka - Planetary science (Jupiter and Saturn magnetospheric radio emissions) is doable with 1-2 dipole antennas - Indeed we should concentrate below 10 MHz (perhaps a little more, up to 20? Dipoles of 2 x m should be a good compromise. - A 2-input receiver performing auto- and crosscorrelation of 2 antennas signals (thus measuring flux and partly polarization) in the range ~0-10 MHz could be a copy of the miniaturized receiver we (LESIA) build for BepiColombo/MMO. Typical resources are of order of 1 kg, 1 W.
15 Detectability from the Moon : all Jovian emissions + Saturn auroral emissions with C (N=1-10, 10 khz 1 sec) + Uranus & Neptune auroral emissions + Saturn & Uranus lightning (including LF cutoff) with C (N=10-100, 200 khz msec) C
16 Interest of (solar system) planetary radio emission studies : Long-term magnetospheric radio observations from a ~fixed vantage point (+ multi- correlations) Variabilities/periodicities (Planetary rotation period) magnetospheric dynamics Solar wind / Magnetosphere coupling Substorms? SW monitoring from 1 to 30 AU? Satellites / Magnetosphere coupling (Io, Titan ) Io volcanism + torus probing (radio em. + propag. effects) Magnetic anomalies + secular variations Uranus & Neptune radio emissions observed only once by Voyager 2!
17 Jean-Louis Bougeret Active/passive measurement of subsurface reflectivity With interferometer later do 3D subsurface imaging. Sources: Earth AKR radiation & Solar IP sources Rover pulls long wire
18 Martin Füllekrug Space qualified VLF instrument Bandwidth from DC to 40 khz weighs 100 g, consumes 1 W, can use any electrical antenna already mounted So far virtually no VLF measurements from satellites at moon distances of Earth. Active and passive experiments could target probing of plasmaspheric density reflections of VLF waves from the moon's surface particle beams in the solar wind transition radiation from cosmic rays
19 Lunar LOFAR with EADS Astrium 33 crossed dipoles 30 km baseline fibre links Local power supply
20 Lunar LOFAR Antenna Module
21 Requirements Matrix No. of Modules min max D channel t min t max Baseline pols Site processing Science [MHz] [MHz] [MHz] [khz] [months] [months] [km] Equatorial Strip imaging y y pole, shielded cross correlation autocorrelation & burst Dark ages foreground y pole, shielded excision Ultra-High Energy Cosmic rays y y y any pulse detection Planets y y y any (shielded) cc & ac Eartk AKR y y y near side ac Solar Wind y ac sub-surface sounding y y any active transmission ionospheric sounding y pole ac e.m.p. from meteorites y y y any pulse detection Transition Radiation from CRs y y y any pulse detection VLF y near side ac & cc; Earth station
22 Conclusions Quite a range of science issues can be tackled by ~2-3 antennas: Simple equatorial strip imaging (moon rotation synthesis) CR (and meteorite?) detection Limit on HI in Dark Ages and Galactic spectral shape/roughness Long-term planetary magnetospheric monitoring Plasma effects Many of these have a demonstrator component big step forward through interferometry. Ideal but unrealistic setup: 3 x MHz modules with direct conversion. Likely two 1-10 MHz modules: one with rover and one with lander (one of them more broad-band?).
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