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LYRA Tests and Selections. SCSL Meeting Bern 29 Nov - 01 Dec 2006. Contents. I. From Model to Configuration II. BESSY Campaigns a. Flux Linearity b. Stability, Drift c. LEDs, Dark Current d. Spectral Responsivity e. Homogeneity, Flatfield III. Summary.

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LYRA Tests and Selections

SCSL Meeting Bern 29 Nov - 01 Dec 2006


Contents

I. From Model to Configuration

II. BESSY Campaigns

a. Flux Linearity

b. Stability, Drift

c. LEDs, Dark Current

d. Spectral Responsivity

e. Homogeneity, Flatfield

III. Summary


I. From Model to Configuration

  • Choice of filters: Zirconium (150 nm, 300 nm), Aluminium, Lyman-alpha (N, XN, VN, and combinations thereof), Herzberg, …

  • Choice of detectors: MSMxx (diamond), PINxx (diamond), AXUVxx (silicon), …

  • Tested separately to find transmittance and responsivity

  • Simulated with TIMED-SEE solar spectra to find expected response values and purities

  • cf.http://lyra.oma.be/radiometric_model/radiometric_model.php

  • Example: “high” flux + “Herzberg” filter + “PIN” detector


Selected configurations
Selected configurations:

filter detector nominal FWHM measured

1-1 Ly XN + MSM12 121.5 +/- nm 116-126 nm

1-2 Herzberg + PIN10 200-220 nm 197-218 nm

1-3Aluminium + MSM11 17-80 nm (1)-2.4, 17-35 nm

1-4Zr (300nm) + AXUV20D 1-20 nm (1)-1.3, 6-15 nm

2-1 Ly XN + MSM21 121.5 +/- nm 116-126 nm

2-2 Herzberg + PIN11 200-220 nm 199-219 nm

2-3 Aluminium + MSM15 17-80 nm (1)-1.4, 17-27 nm

2-4 Zr (150nm) + MSM19 1-20 nm (1)-1.3, 6-12 nm

3-1 Ly N+XN + AXUV20A 121.5 +/- nm 116-126 nm

3-2 Herzberg + PIN12 200-220 nm 198-219 nm

3-3 Aluminium + AXUV20B 17-80 nm (1)-2.4, 17-35 nm

3-4 Zr (300nm) + AXUV20C 1-20 nm (1)-1.3, 6-15 nm


Consequence
Consequence:

  • All channels individual

  • No simple redundancy

  • Combined responsivities

  • New estimates for response and purity (cf. II d.)


Ii bessy campaigns
II. BESSY Campaigns

  • NI beamline (40 – 240 nm, 60 C) July 2005

    Doc. RP-ROB-LYR-0132-NI-July2005

  • GI beamline (1 – 30 nm, 60 C) July 2005

    Doc. RP-ROB-LYR-0132-GI-July2005

  • (Final) NI beamline (40 – 240 nm, 37 C) March 2006

    Doc. RP-ROB-LYR-0132-NI-March2006

  • (Final) GI beamline (1 – 30 nm, 37 C) March 2006

    Doc. RP-ROB-LYR-0132-GI-March2006


A flux linearity
a. Flux Linearity

  • Using different aperture stops, or

  • Varying exit slit of monochromator

  • Relation fitted (2006) with a function I=[c+]a*P^b

  • Results: almost linear, slightly sub/superlinear, sub/superlinear (qualitatively)

  • or: b~1, c~0 (quantitatively)


Results in detail
Results in detail:

NI 2006 GI 2005 NI 2006 GI 2006

(121.6 nm, 200 nm) (20 nm, 10 nm) (121.6 nm, 210 nm, 50 nm) (18 nm, 10 nm)

1-1 MSM slightly sublin. 0.99572

1-2 PIN slightly superlin. 1.00656

1-3 MSM 0.98565 1.1719, but c>0

1-4 AXUV 1.00155

2-1 MSM slightly sublin. 1.03661

2-2 PIN slightly superlin. 0.99483

2-3MSM superlinear 1.02234 0.97894

2-4MSM slightly superlin. 1.04009

3-1 AXUV almost linear 1.02434

3-2 PIN almost linear 0.99529

3-3 AXUV sublinear 0.00230 0.99253

3-4AXUV almost linear 1.00064


B stability drift
b. Stability, Drift

  • Shutter was opened and closed every 60 s, then every 600 s

  • Some additional longer tests were executed

  • BESSY 2005 campaigns (60 C) still to be analyzed in detail

  • LED values, dark current values and 44 C, 50 C temperature effects: see below

    Example:

    Channel 2-1 (Ly XN + MSM21) at BESSY NI 2006


Results 2006 in detail
Results (2006) in detail:

start drift stop

(“slow” ~min, “almost immediate” ~s) (“tail” ~min, “almost immediate” ~s)

1-1 MSM slowupwardtail

1-2 PIN almost immediate (almost) no almost immediate

1-3 MSM almost immediate, slowupwardtail, almost immediate

1-4 AXUV immediate no immediate

2-1 MSM slowupwardtail

2-2 PIN almost immediate (almost) no immediate

2-3 MSM slowupward almost immediate

2-4 MSM slowupward almost immediate

3-1 AXUV (almost) immediate (almost) no almost immediate

3-2 PIN almost immediate no immediate

3-3 AXUV (almost) immediate (almost) no (almost) immediate

3-4 AXUV immediate no almost immediate


C leds dark current
c. LEDs, Dark Current

visLED uvLED offset @37 C 44 C 50 C

1-1 MSM (0.005) (0.024) 0.001 0.010

1-2 PIN 0.004 0.014 0.000 -0.002

1-3 MSM (0.100) 0.000, -0.007 0.003 0.010

1-4 AXUV -0.004

2-1 MSM (0.012) (0.023) 0.001 0.009

2-2 PIN 0.015 -0.001 -0.002 -0.005

2-3 MSM ((0.016-0.136)) 0.000, -0.008 0.002 0.007

2-4 MSM -0.001

3-1 AXUV 0.000?0.000 0.002 0.008

3-2 PIN 0.006 -0.003 -0.005

3-3 AXUV (1.059) -0.001, -0.011 -0.003 -0.005

3-4 AXUV -0.014

All values in nA

(x) = varying around x, ((x-y)) = unstable from y to x, “negative” current values due to conversion


D spectral responsivity
d. Spectral Responsivity

  • Filters and detectors measured together (“channels” as configurated)

  • Relevant spectral range is tested, with special attention to range borders

  • V changed to A using appropriate gain resistor

  • Corrections for ring current applied

    Example: “high” solar flux simulated with measurements of channel 1-1 (Ly XN + MSM12) at BESSY NI 2006

  • How to estimate “correction factors”?

  • Consequences for data levels?


Expected signal and purity
Expected Signal and Purity

theorectical: “min” “high” measured: “min” “high”

1-1 MSM 0.139 nA (37%) 0.161 nA (44%) 0.240 nA(24%)0.267 nA(30%)

1-2 PIN 12.75 nA (86%) 12.77nA (86%) 12.57 nA (83%) 12.59 nA (83%)

1-3 MSM 0.120 nA (61%) 5.264 nA ( 3%) 0.086 nA (58%) 4.945 nA ( 3%)

1-4 AXUV 0.530 nA (99%) 15.37 nA (88%) 0.699 nA (100%) 19.09 nA (100%)

2-1 MSM 0.115 nA (39%) 0.135 nA (46%) 0.104 nA(21%)0.114 nA(26%)

2-2 PIN 13.80 nA (83%) 13.82 nA (83%) 13.75 nA (84%) 13.76 nA (84%)

2-3 MSM 0.127 nA (73%) 3.821 nA ( 6%) 0.074 nA (59%) 3.837 nA ( 3%)

2-4 MSM 0.111 nA (99%) 2.878 nA (100%) 0.094 nA (100%) 2.772 nA (100%)

3-1 AXUV 0.132 nA (46%) 0.156 nA (54%) 0.113 nA (81%) 0.148 nA (84%)

3-2 PIN 10.20 nA (85%) 10.22 nA (85%) 10.15 nA (83%) 10.16 nA (83%)

3-3 AXUV 1.072 nA (75%) 34.95 nA ( 6%) 1.090 nA (72%) 36.83 nA ( 5%)

3-4 AXUV 0.530 nA (99%) 15.37 nA (88%) 0.710 nA (100%) 19.31 nA (100%)


Calibration factor data levels
Calibration Factor, Data Levels

How to estimate the solar signal from the LYRA signal?

LYRA signal * purity / area / responsivity = solar signal

[A] [%] [m2] [A W-1] [W m-2]

\___________________/

calibration factor

Example: “max”, “high”, “min” flux + Channels 1-1, 1-2, 1-3, 1-4

  • Use constant factor, linear dependency on signal, knowledge about solar flux?

  • Change public data each time when calibration factor gets more realistic? Use different data levels?


E homogeneity flatfield
e. Homogeneity, Flatfield

Example: Channel 2-3 (detector diameter 4.2 mm)

What consequences will an off-pointing have?


Iii summary
III. Summary

Linearity Stability LEDs Signal, Purity

1-1 MSM + -- + -

1-2 PIN + + + ++

1-3MSM --- - +? --

1-4 AXUV + + ?? +++

2-1 MSM + - + -

2-2 PIN + + + ++

2-3MSM -- - -? --

2-4 MSM + - ?? +++

3-1AXUV + + - +

3-2 PIN + + +? ++

3-3 AXUV - + +? --

3-4 AXUV + + ?? +++


Recommendation
Recommendation

  • Head 2 should be nominal

  • Head 1 should be used once a week

  • Head 3 should be used once a month

    depending on the behaviour of LYRA (deterioration etc.)


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