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Galactic Radioemission – Galactic Radioemission – a problem for precision cosmology ?a problem for precision cosmology ?
Absolute Temperatures at Short CM-Waves with
a Lunar Radio Telescope
Wolfgang Reich
Max-Planck-Institut für Radioastronomie
Bonn
Bremen 22./23.3.2005
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Summary and ConclusionSummary and Conclusion
Scientific needs:Scientific needs: absolutely calibrated sky surveys absolutely calibrated sky surveys in I and PI between ~5-15 GHz in I and PI between ~5-15 GHz
Technical needs:Technical needs: 10m/15m meridian telescope 10m/15m meridian telescope operating at 3-5 frequenciesoperating at 3-5 frequencies
Location:Location: backside of the moon close to backside of the moon close to equator (+/- ~5° latitude) equator (+/- ~5° latitude)
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Absolutely Calibrated Absolutely Calibrated All-Sky Radio Continuum All-Sky Radio Continuum
SurveysSurveys
408 MHz408 MHzHaslam et al. Haslam et al.
HPBW = 51’, HPBW = 51’, T = 2K T = 2K
1420 MHz1420 MHzReich et al. Reich et al.
HPBW = 35’, HPBW = 35’, T= 50mK T= 50mK
Spectral Index ßSpectral Index ß 408 MHz / 1420 MHz 408 MHz / 1420 MHz
= 2.4 (blue) – 3.0 (red) = 2.4 (blue) – 3.0 (red)Reich et al.Reich et al.
ß
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Galactic emissionGalactic emission
mixture of synchrotron ß = 2.4…3.2 mixture of synchrotron ß = 2.4…3.2 + thermal emission ß = 2.1 + thermal emission ß = 2.1
anomalous dust: 10 GHz – 30 GHz ?anomalous dust: 10 GHz – 30 GHz ? component separation difficult component separation difficult absolutely calibrated surveys at absolutely calibrated surveys at
several frequencies neededseveral frequencies needed extrapolation to CMB-Frequencies extrapolation to CMB-Frequencies
uncertainuncertain
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Absolute Calibration Sequence for Absolute Calibration Sequence for Total IntensitiesTotal Intensities
Absolute skyhorn measurements Absolute skyhorn measurements ~10°/15° angular resolution~10°/15° angular resolution
calibration of medium angular calibration of medium angular resolution all-sky surveysresolution all-sky surveys
calibration of high resolution maps calibration of high resolution maps e.g. Galactic plane surveyse.g. Galactic plane surveys
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Absolute „3K“ Absolute „3K“ MeasurementsMeasurements
largely uncertain largely uncertain below below λλ ~ 1cm ~ 1cm
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Available surveys
anomalous dust
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+212 µK
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1.41 GHz Dwingeloo polarization surveyBrouw & Spoelstra, 1976
absolutely calibrated
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Anticorrelation of I/ PI with Galactic latitude
(Reich et al. 1990, Duncan et al. 1999)
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24° x 9° section centered at l , b = 162°,0°
1.4 GHz Effelsberg Medium Latitude Survey (EMLS)
I
PI
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Absolute Polarization Calibration: Absolute Polarization Calibration: „A Must„A Must“ for Galactic Emission“ for Galactic Emission
Vector additionVector addition for polarisation for polarisation scalar addition for total intensityscalar addition for total intensity
PI = (UPI = (U22 + Q + Q22))1/2 1/2 measuredmeasured ΦΦ = 0.5 atan (U/Q) = 0.5 atan (U/Q) PIPIabsolute absolute = ((U+U= ((U+Uoffoff))22 +(Q+Q +(Q+Qoffoff))22))1/21/2
ΦΦ = 0.5 atan (U = 0.5 atan (U+U+Uoffoff))/(Q/(Q+Q+Qoffoff))
U/Q may be positive or negativeU/Q may be positive or negative
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Rotation Measure: RM [rad/m2] RM = 0.81 ne [cm-3] B||[G] L[pc], [rad] = RM 2 [m]
ForegroundForeground
BackgroundBackground
Faraday Screen
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High latitude field with dominating large scale emission. 20% of pixel exceed 3xr.m.s.-noise FS fraction.
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Angle statistics for G109+73
relative Effelsberg angles: mean -9.8°, rms 47°
absolute Eff.+DRAO angles:mean -36.5°, rms 7°
need for RM determination
Field reversal at high latitudes ?
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5 GHz RX for large scale polarization mapping at the Urumqi (China)
25m telescope(same 9.4‘ beam as 1.4 GHz EMLS)
MPIfR 5 GHz RX
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5 GHz Urumqi observations of W1 (NGC7822)
PI towards W1 (on relative level)
Distance = 850 pc
Observed PI =
PIFG– (PIFG + PIBG)
small Faraday effects in the ISM at 5 GHz
I
PI
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Green Bank 300-ft10m/15m telescope
3-5 RX out of 5–15 GHz band El-range ~180°backside of the Moon close to equator (+/- ~5° latitude)duration > 2 years ?
Green Bank 300ft
IAR 30m
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The End
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26-m telescope at DRAO/Canada: absolute polarization measurements
> -30° at 1.4 GHz first phase done (undersampled)
Thesis Maik Wolleben (2005)
30-m telescope at Villa Elisa/Argentina
I + PI survey at 1.4 GHz
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Selected surveys