Документ взят из кэша поисковой машины. Адрес оригинального документа : http://site2010.sai.msu.ru/static/doc/ATokovinin_site2010.pdf Дата изменения: Mon Oct 18 12:28:22 2010 Дата индексирования: Mon Oct 1 20:09:52 2012 Кодировка: Поисковые слова: solar corona

Surface-layer turbulence measurements with lunar scintillometer Idea of the method
Hardware & software Campaigns & results New horizons

Andrei Tokovinin NOAO/CTIO
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Turbulence measurement from scintillation of extended sources
Moon's angular diameter =0.5 deg Correlated scintillation for b > z


z=10m b=0.1m z=100m b=1m z=10km b=100m

BI(b) = W(b,z) Cn2(z)dz

Weighting functions zW(z) for b=0...0.4m and d=1cm
2

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The principle

I/ ~104

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2010 MNRAS, 404, 1186

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Restoration of turbulence profile
Cn2 is nonlocal by definition. No "thin layers"! Fit covariance BI(b) to a smooth function Cn2(z) using W(b,z) Use 5 "pivot points", powerlaw segments Calculate seeing etc. from the model Old method: linear combination of data turbulence integrals in "layers"

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Example (1)

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Example (2)

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Pros and cons
Simple instrument Absolute calibration Solid theory (no
saturation, achromatic)

Does not measure high turbulence Sensitive to outer scale Wind bias NonKolmogorov?

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J.Beckers: SHABAR (ATST site campaign)

Various implementations

P.Hickson: lunar SHABAR (CTIO, Arctic & Mauna Kea) CTIO: lunar scintillometer, LuSci (several prototypes) ESO: several LuSci instruments Las Campanas: MooSci

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The CTIO instrument

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Instrument control software
Remote observing "Cold start" possible Correct pointing by webcam Automatic acquisition Periodic sky meas.

Software written by E.Bustos, for Windows
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What can go wrong? Pointing!

Flux vs. time plots
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Data processing (IDL)
Filter the data for each night Calculate covariances .cov file Calculate W(b,z) and fit OTP .tp file Use the OTP to compute SL seeing etc.
The code is available at http://www.ctio.noao.edu/~atokovin/profiler/code2.tar.gz
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Paranal: October 14, 2008

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Instrument comparison (ESO)

LuSci1

LuSci2

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Cerro Tololo, March 2009
Hickson's 12channel scintillometer (UBC) CTIO LuSci (LC) ESO LuSci3 (L3) MASSDIMM site monitor

UBC Mar 14/15

LC Mar 14/15

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Scintillometer comparison
log(Cn2): av. <0.12 rms 0.2 +30% Cn

2

Can SLODAR measure 1015 m2/3 ??
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Comparison with SLSLODAR
Turbulence integral JSL =Cn2(h) dh, in 1013 m1/3 limits (hmin,h
max

)

Paranal, 2009 (J. Osborn, A. Berdja) Osborn et al. 2010, MNRAS
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Comparison with microthermals

Penyon, Nov. 26, 2009, h=10m (J. Sebag)
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Comparison with DIMMMASS
Paranal Feb. 2009 Tololo Mar 2009

Penyon Nov 2009

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Where is the surface-layer turbulence?
Total seeing (DIMM) Free atm. (MASS) Surface layer (LuSci)

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Average profiles in the SL

Cn2(h) 1015 (h/30m)

1

J(6,500) = 1.3 (0.37")
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SL thickness and strength are meaningless without (hmin,hmax) SL integral is dominated by h
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Is the SL turbulence really weak?
Paranal, 1998: J(3,21)=0.4 (microthermal), no
difference between GSM (2m) and DIMM (6m)

Paranal, SLSLODAR: J(6,65)=0.6 Racine (2005): J(6,100)=0.5 Lunar scintillometers at Paranal, Tololo, Penyon, Mauna Kea: J(6,200) ~ 0.5
Turbulence integral JSL(hmin,hmax) in 1013 m DIMMMASS: JSL = 2...3 typically
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1/3


Can a DIMM be wrong?...
Northern wind

Els et al. 2009, PASP, 121, 922

... yes, sometimes!
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JGL(CTIO DIMM)/JGL(TMT DIMM)
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The "SL discrepancy"
The assumption that all site monitors have zero local turbulence is questionable. We do not know how strong Jloc is. DIMMs give an upper limit on seeing, it can in fact be better! Local turbulence is detected in all telescopes by SCIDARs, SLODARs, etc. It matters under good seeing only
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Site seeing depends on the elevation of the site monitor (cf. R. Racine) Systematic bias by local turbulence A modeldependent concept (real distortions are not stationary, the Kolmogorov model is approximate; gravity waves?) Telescopes have internal seeing, too (1990s: ~2" now: 0.5" or 0"?)

Elusiveness of "site seeing"

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Maidanak, 1975

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A typical situation?

Seeing 0.84"/0.62" with/without Jloc
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A new exciting challenge
If JSL=0.5 (0.2" seeing), can telescopes get images that good? A new round of dome/mirror environment study and optimization? Active optics widefield GLAO?
IMAKA (Chun et al. 2010): CFHT, 1o FoV, NGS Sitetesting and telescope optimization is not over yet!
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Acknowledgement
This presentation makes use of data obtained by many people at many sites. Thanks for sharing the data and for the collaboration!
CTIO ­ E. Bustos, A. Berdja ESO ­ M. Sarazin, G. Lombardi UBC ­ P. Hickson U. Durham ­ R. Wilson, J. Osborn LSST ­ J. Sebaq LCO ­ J. ThomasOsip http://www.ctio.noao.edu/~atokovin/papers/sl.pdf
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