MAESTRO Sun Scan Analysis Florian Nichitiu May 14, 2004.
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Transcript of MAESTRO Sun Scan Analysis Florian Nichitiu May 14, 2004.
MAESTRO Sun Scan Analysis
Florian NichitiuMay 14, 2004
After on-orbit commissioning of the spacecraft and instruments a series of on-orbit science-oriented activities have been undertaken. Sun Scanning (Open Loop): 21 Feb. 2004 High Sun Scanning (Closed Loop): 14 – 17 Apr. 2004The purpose of these activities is to: - extend and verify the results obtained during pre-launch lab-tests - to find the appropriate parameters for operational measurements. ***MAESTRO field of view characterization, UV and VIS slit position, using Sun Scan measurements.
On-orbit dispersion equations, absolute sensitivity using High Sun measurements
Closed Loop offset sun-pointing parameters using High Sun Scan measurements
Sun ScanSun tracker in Open Loop
0.04 0.06 0.08 0.10 0.12 0.14 0.16 0.18
-1.00
-0.98
-0.96
-0.94
-0.92
-0.90
-0.88
-0.86
-0.84
Delta(T)=35.5 sec
High Sun ( just before Sun Scan EL-az )
(NIR)Ximag=65.21(NIR)Yimag=60.29
CL_AZoffset=1250CL_ELoffset=450
EL
(M
ec)
AZ (Mec)0.36 0.38 0.40 0.42 0.44 0.46
-1.18
-1.16
-1.14
-1.12
-1.10
-1.08
-1.06
-1.04
Delta(T)=35.5 sec
(NIR)Ximag=65.23(NIR)Yimag=60.29
CL_AZoffset=1250CL_ELoffset=450
High Sun ( just before Sun Scan AZ only)
EL
(M
ec)
AZ (Mec)
S/C motion during High Sun
Sun tracker on Closed Loop
High Sun spectra
Sun tracker in Closed Loop
0 50 100 150 200 250
2500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000
Up to = 1078429778.014000
Unix Time=1078429553.394000
Pre
ad
Int S
pe
ctra
(U
V fr
om
pix
:50
1 to
10
00
)
Time (sec) from : 1129146353.394000
Int Table 23
Occultation
High Sun
Occultation
Bg. (dark current)
0 10 20 30 40 50 602500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000
SP
Inte
gra
l (U
V p
rere
ad
)
Relative Time
UVaz IntelPaz IntUVel IntUVelMaz Int High Sun
Sun Scanning (Open Loop)
0 50 100 150 200-2.5
-2.0
-1.5
-1.0
-0.5
0.0
0.5
1.0
1.5
2.0
2.5
3.0
-1.75-2.00
0.05-0.20
2.662.41
EL
EL-az
EL+az
OPT AZ during elevation Sun Scan
OP
T A
Z (
mra
d)
Relative Time
0 50 100 150 200-4.0
-3.5
-3.0
-2.5
-2.0
-1.5
-1.0
-0.5
0.0
-3.14
-2.67
Relative Time
OPT EL during AZ-Sun Scan
OP
T E
L (
mra
d)
Sun Scanning (Open Loop) : sun scan in azimuth (elevation) with elevation(azimuth) fixed
0 1 2 3 4 5 6 7 8 93.00
3.05
3.10
3.15
3.20
3.25
3.30
3.35
3.40
EL+azEL+az
ELEL
AZ AZEL-az EL-az
SP
IN
T (
10
^6)
NR of Sun Scan
UV1 UV2 HS
0 1 2 3 4 5 6 7 8 9-0.10
-0.09
-0.08
-0.07
-0.06
-0.05
-0.04
-0.03
-0.02
-0.01
0.00
0.01
EL+az
EL
AZ
EL-az AZEL-az
EL+az
EL
(Int(SS)-Int(HS))/Int(HS)
Y A
xis
Titl
e
X Axis Title
First Scan Second Scan
Maximum of spectrum integral during Sun Scan
-10 -5 0 5 10 152500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000AZ Solar Scan First ( EL=-2.67)
Y A
xis
Titl
e
OPT Az (mrad)
UVaz
0.2
0.4
0.6
0.8
1.0
1.2
1.4
Center: FTS T=+0.35 mrad MAESTRO T=-1.21 mrad
mct
-6 -4 -2 0 2 4 6
0.0
0.2
0.4
0.6
0.8
1.0
AZ=-0.21176
MAESTRO First Scan in EL
OPT EL
Inte
gra
l (N
orm
aliz
ed
)
Data: visElA_visModel: LimbDark Chi^2 = 0.00002R^2 = 0.99974 P1 1.00002 ±0.00169P2 1 ±0P3 4.60657 ±0.01586P4 -0.98823 ±0.00422P5 1.46745 ±0.02264
EL=-0.98823
vis
30 40 50 60 702500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
Center: FTS T=48.57 sec MAESTRO T=48.57 sec
EL Solar Scan Second ( AZ=0.05)
Time (sec)
IntUVel
0.2
0.4
0.6
0.8
1.0
1.2
1.4 mct
Hestroffer Solar Limb Darkening. model:(Atron. Astrophys 333,338-342(1998))
-14 -12 -10 -8 -6 -4 -2 0 2 4 6
0.0
0.2
0.4
0.6
0.8
1.0
EL-az Solar Scan II
Nor
m In
t
OPTel (mrad)
UVint VISint
0.5 1.0 1.5 2.0 2.5 3.0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
Diff. in widths
(UofT test: 0.261 mrad)
EL-az Solar Scan II
0.26 mrad
OPTel (mrad)N
orm
Int
VISint UVint
UV=0.26 mrad
VIS
20 30 40 50 60 70 80 90 10085
80
75
70
65
60
55
50
45
[C]
[B]
[A]
NIR sunscan
ima
ge
r y
axi
s
imager x axis
-12 -10 -8 -6 -4 -2 0 2 4 6 8 102500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
[C]
[B]
[A]
Diff/Max=0.0125
-0.933
9.2 mrad
Solar Scan in elevation UV spectra
Co
un
ts
Optical EL (mrad)
EL #1 EL #2
Solar Scan in elevation 21 Feb. 2004
Solar Disk dimension
as expected:Solar disk radius = 4.6 mrad
45 50 55 60 65 70 75 80 85
30
40
50
60
70
80
NIR
ima
ge
r Y
NIR imager X
Edges: at Max Deriv. Edges: at 1/2Max DFLtest before flight
0 10 20 30 40 50 60
-100000
-80000
-60000
-40000
-20000
0
20000
40000
60000
80000
100000 Az scan IIAz scan I
Differentiate
Time
UVaz'
2500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000
UVaz
0 5 10 15 20 252500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000Az scan I
Int
Time
UVaz
30 35 40 45 50 55 602500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
3400000 Az scan II
Int
Time
UVaz
Using time as parameter Sun centroid in Imag coordinates
20 30 40 50 60 70 80 90 100 110
100
90
80
70
60
50
40
30NIR imager
de
tect
or
y a
xis
detector x axis
Slit VIS-spectrometer Slit UV-spectrometer Sun Scan in EL-az Sun Scan in AZ
20 30 40 50 60 70 80 90 100 110
100
90
80
70
60
50
40
30 NIR imager
detector x axis (pixels)
de
tect
or
y a
xis
(pix
els
)
NIRySS-VIS NIRySS-UV NIRyUVDFL NIRyVISDFL
Slit position on the NIR imager : - Sun Scan analysis - DFL: final test
125
120
115
110
105
100
95908580757065605550454035302520151050
125
120
115
110
105
100
95
90
85
80
75
70
65
60
55
50
45
40
35
30
25
20
15
10
5
0 20 40 60 80 100 120
120
100
80
60
40
20
0
detector x axis (pixels)
dete
ctor
y a
xis
(pix
els)
NIRy UV NIRy VIS
Slit position on the NIR imagerand Sun position during CL
250 300 350 400 450 500 550 600
5200
5400
5600
5800
6000
6200
6400
6600
6800
7000
Wavelength [nm]
Co
un
ts
Maestro UV SM20
300 350 400 450 500 550 6000.2
0.4
0.6
0.8
1.0
1.2
1.4
1.6
1.8
2.0
2.2
Wavelength [nm]
Solar Spectra 20 point AA Smoothing of SolarSp_B
Maestro spectra vs. Solar Spectra
300 320 340 360 380 400
-20
-10
0
10
20
30
Diff Maestro UV
Wavelength [nm]
-0.4
-0.2
0.0
0.2
0.4
0.6
0.8
Diff Solar Spectra
400 420 440 460 480 500-100
-50
0
50
100
150
Diff Maestro UV
Wavelength [nm]
-0.4
-0.2
0.0
0.2
0.4
0.6
Diff Solar Spectra
500 510 520 530 540 550 560 570-80
-60
-40
-20
0
20
40
60
Wavelength [nm]
Diff Maestro UV
-0.15
-0.10
-0.05
0.00
0.05
0.10
0.15
0.20
Diff Solar Spectra
Dispersion eq. For calculating wavelength (nm) from pixel number: Wavelength=-1.0261e-8*p^3-9.5161e-6*p^2+0.32629*p+254.98(From UofT Evaluation Test)
Difference between smoothing and Exp. spectra.
There is a shift in Wavelength ~ 3.43 nm
400 420 440 460 480 500-0.6
-0.4
-0.2
0.0
0.2
0.4
0.6
Wavelength [nm]
A Solar Spectra
-150
-100
-50
0
50
100
150
Diff Maestro UV
400 420 440 460 480 500-0.6
-0.4
-0.2
0.0
0.2
0.4
0.6
Wavelength [nm]
A Solar Spectra
-150
-100
-50
0
50
100
150
Diff Maestro UV
Data from: “Solar Flux Atlas…NSO/Kitt Peak : ftp://ftp.noao.edu/fts
0 200 400 600 800 1000 12005.0
5.5
6.0
6.5
7.0
7.5
Average of 37 spectra
Average of 39 spectra
UV High Sun Spectra
Co
un
ts *
10
00
Pixel #
SP DK
540 560 580 600 620 640 660 680 700 720-100
-50
0
50
100
150
Pixel #
DiffMAE
-0.10
-0.05
0.00
0.05
0.10
0.15
DiffUVcor
UV spectra from Sun Scan 21 Feb 2004UV spectra from High Sun 14 Apr 2005
MAESTRO spectra ‘Stability’
500 550 600 650 700 750-0.6
-0.4
-0.2
0.0
0.2
0.4
0.6
Pixel #
DiffSol
-150
-100
-50
0
50
100
150
DiffMAE
0 200 400 600 800 1000 1200-0.05
0.00
0.05
0.10
0.15
0.20
0.25
0.30
0.35
Solar(ATLAS1) / MAEuv
Pol(3)
Pol(6)
So
lar(
AT
LA
S1)
/ M
AE
uv
Pixel #
New dispersion equation for wavelength Pixel (UV spectra):
WL=-1.0261e-8*p^3-9.5161e-6*p^2+0.32629*p+251.55
P=-747.50757+2.85456*WL+7.20263e-4*WL^2-1.45118E-6*WL^3+1.88693E-9*WL^4
‘correction’ of UV spectra for each pixel: From counts to micro-watts per square centimeter per nanometerData at each ~0.05 nm averaged for ~0.3 nm ( as UV Maestro at ~ 400 nm)
500 550 600 650 700 750
-0.6
-0.4
-0.2
0.0
0.2
0.4
0.6
Diff for Solar Spectra
Pixel #
-200
-150
-100
-50
0
50
100
150
200UV
Diff MAE
150 200 250 300 350-0.25
-0.20
-0.15
-0.10
-0.05
0.00
0.05
0.10
0.15
0.20
0.25
0.30
0.35
VIS
Pixel #
Diff for Solar Spectra
-40
-20
0
20
40
60
Diff MAE
L(VIS)=-2.1254e-8*p^3-8.6224e-6*p^2+0.52626*p+514.23Correct Lambda=L(VIS)-6.08 nmP(Vis)=-932.00736+1.7112*L+4.47888e-4*L^2-5.78258e-7*L^3+3.41003e-10*L^4
L(UV)=-1.0261e-8*P^3-9.5161e-6*P^2+0.32629*P+254.98Correct Lambda=L(UV)-3.43 nmP(UV)=-748.06497+2.85457*L+7.20675e-4*L^2-1.453e-6*L^3+1.88785e9*L^4
0 200 400 600 800 1000 1200
-100
0
100
200
300
400
500
Pixel #
VISmae
0.6
0.8
1.0
1.2
1.4
1.6
1.8
2.0
SM20v
0 200 400 600 800 1000 1200
-50
0
50
100
150
200
250
300
350 VIS
Se
nsi
tivity
(F
rom
Uo
fT L
ab
Te
st)
Se
nsi
tivity
(F
rom
So
lar
Sp
ect
ra)
Pixel #
MAEonSOLvis
0.00E+000
1.00E+008
2.00E+008
3.00E+008
4.00E+008
5.00E+008
6.00E+008
7.00E+008
UofT test
MAESTRO VIS spectrometer absolute sensitivity
Units: (counts/s)/(Wm^-2nm^-1)
0 200 400 600 800 1000 1200-500
0
500
1000
1500
2000
Pixel #
UVmae
0
2
SM20uv
200 400 600 800 1000-200
0
200
400
600
800
1000
Se
nsi
tivity
(F
rom
Uo
fT L
ab
Te
st)
Se
nsi
tivity
(F
rom
So
lar
Sp
ect
ra)
Pixel #
MAEonSolUV
0.00E+000
2.00E+008
4.00E+008
6.00E+008
8.00E+008
1.00E+009
1.20E+009
1.40E+009
1.60E+009UV UofT test
MAESTRO UV spectrometer absolute sensitivity
Units: (counts/s)/(Wm^-2nm^-1)
MAESTRO HIGH SUN scan
45 measurements with different sun tracker pointing positionsUsing Closed Loop offsets in azimuth and elevation (including the Standard CL offsets to the center of the High Sun : CL_AZ=1250; CL_EL=450)
CL_AZ=1750
CL_AZ= 750
CL_EL= -50 CL_EL=950
20 30 40 50 60 70 80 90 100 110
100
90
80
70
60
50
40
30NIR imager
dete
ctor
y a
xis
detector x axis
Slit VIS-spectrometer Slit UV-spectrometer Sun Scan in EL-az Sun Scan in AZ
0 100000 200000 300000 400000 500000 6000005100000
5150000
5200000
5250000
5300000
5350000
5400000
5450000
5500000
VIS High Sun Scan
To
t N
r o
f co
un
ts
Seconds 0 100000 200000 300000 400000 500000 600000
2500000
2600000
2700000
2800000
2900000
3000000
3100000
3200000
3300000
UV High Sun Scan
Seconds
To
t N
r o
f co
un
ts
Spectrum integral during High Sun Scan
Bg. ( spectrum integral for pointing ‘out of Sun’
0 100000 200000 300000 400000 500000 600000
3180000
3200000
3220000
3240000
3260000
UV High Sun
(~0.75 %)
(EL=450; AZ=1250)
(EL=450; AZ=1750)
Tot
_Nr_
Cou
nts
Seconds
0 100000 200000 300000 400000 500000-0.002
-0.001
0.000
0.001
0.002
0.003
0.004
Average val=3.23937E6
(Tot
_Nr_
of_c
ount
s-A
vera
ge)/
Ave
rage
Seconds
High Sun "Standard"A 2.57296E6 523.06589B 1.11479E-4 0.00154
0 200000 400000-4
-3
-2
-1
0
1
(From 14/04/2004)
MA
E_
TH
M_
SP
EC
_T
OP
(C
)
Seconds
TempTop
3234000
3236000
3238000
3240000
3242000
3244000
3246000
3248000
3250000
High Sun "Standard"
0 100000 200000 300000 400000 5000005468000
5470000
5472000
5474000
5476000
5478000
5480000
5482000
Seconds
To
t N
r o
f co
un
ts
To
t N
r o
f co
un
ts
Standard High Sun VIS
3234000
3236000
3238000
3240000
3242000
3244000
3246000
3248000
3250000
UV
0 100000 200000 300000 400000 500000 600000
-0.002
-0.001
0.000
0.001
0.002
0.003
0.004
0.005
(Tot
_Nr_
of_c
ount
s-A
vera
ge)/
Ave
rage
Seconds
Off Sun (Bg)Aerage = 2.57299E6
0 100000 200000 300000 400000 500000 600000
-0.002
-0.001
0.000
0.001
0.002
0.003
0.004
0.005
(Tot
_Nr_
of_c
ount
s-A
vera
ge)/
Ave
rage
Seconds
BG HS
Bg. High Sun
350000 400000 450000 500000 5500003180000
3190000
3200000
3210000
3220000
3230000
3240000
3250000
3260000
UV High Sun Scan
Seconds
"Standard" HS
To
t Nr
of
cou
nts
UV
300000 350000 400000 450000 500000 5500003180000
3190000
3200000
3210000
3220000
3230000
3240000
3250000
3260000
Tot
Nr
of c
ount
s
High Sun Scan
Seconds
UV
5460000
5462000
5464000
5466000
5468000
5470000
5472000
5474000
VIS
600 800 1000 1200 1400 1600 18003180000
3190000
3200000
3210000
3220000
3230000
3240000
3250000
3260000
"Standard" HS
UV High Sun Scan
To
t Nr
of c
ou
nts
Closed Loop AZ
UV
-200 0 200 400 600 800 1000800
1000
1200
1400
1600
1800
2000
2200
2400
xel
yaz
3.06178016e+000+4.82389927e-005 xel-...-008 yaz2
2D fit ( polynomial second degree in CL_AZ and CL_EL)
Conclusions:
From Sun Scan we find a good agreement:-For VIS and UV slit position and dimension with pre flight test.
-Corrections for VIS and UV : -New dispersion equation (pixel wave length) . -New spectrometer absolute sensitivity.
From High Sun Scan we confirm the appropriate Closed Loop Offsets parametersand we propose a new set of these parameters which can improve the quality of measurements. CL_AZ_offset = 1750 ( max) CL_EL_offset = 355
Acknowledgements:
James Drummond
Tom McElroy
Denis Dufour
Caroline Nowlan
Kathleen Gilbert
Sean D McLeod
Jay Kar
Jason Zou
Clive Midwinter