ESP Data Products: Lev 1 and
Lev 0C
Leonid Didkovsky
USC Space Sciences Center
Overview
• ESP Lev 1 Data Product:
1. How the irradiance is calculated (both solar
and SURF)
2. Program components and structure
3. ESP Lev 1 Inputs/Outputs
4. Calibration parameters in-flight
5. Calibration updates(?)
6. Fits headers(?) and Lev 0C (TBD)
• ESP Lev 0C Data Product
• Things to do before SDO launch
• EVE Workshop’s Action items
Dec 8 2009
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LASP
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ESP Solar Irradiance Equation
Cef
∆G (T , V , TID )
)
⋅ (1 −
∆
t
∆t
E (λ , t ) =
− EOS
λ0 + ∆λ
⎛λ ⎞
R ( λ , α , β ) ⋅ ⎜ ⎟ ⋅ F ( λ ) dλ
∫
⎝ hc ⎠
λ0 − ∆λ
A⋅
f deg rad ( channel , t ) ⋅ f1 AU (t )
λ0 + ∆λ
∫ F (λ )dλ
λ0 − ∆λ
R (λ , α , β ) = S (λ , FOV ) * RBL − 9
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ESP Slit Functions and Responsivities
in the `solar’ FOV of ± 960 arc sec
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ESP SURF Irradiance Equations
InpIrrad (Ch ) =
CalcIrrad (Ch ) =
∑λ F (λ ) • ∆λ • I • h • c
A⋅λ
cnteff
A • ∑ F ( λ ) • ∆λ • I •
λ
Dec 8 2009
∑λ F (λ )
λ
hc
• Rλ
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− EOS
At the entrance slit
At the Ch’s output
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Results: Irradiance (calculated vs input)
• An Input irradiance
Input (BL2) and Calculated (ESP) Irradiance
IRRADIANCE, W/cm^2
1.00E-04
1.00E-05
I=0.296 mA BL2
I=0.296 mA ESP
1.00E-06
I=0.252 mA BL2
I=0.252 mA ESP
1.00E-07
1.00E-08
0
1
2
3
4
5
6
7
8
9
10
ESP CHANNELS
Dec 8 2009
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(W/cm2 ) was
determined from
BL2 flux for beam
energy of 380 MeV
and two beam
currents: 0.296 mA
(ESP calibration on
Feb 13, 2007 with 45° orienation) and
0.252 mA (ESP
calibration on Aug
30, 2007 with +45°
orientation). Then
the determined ESP
efficiencies and ESP
Equations were
used to calculate the
‘unknown’ Irradiance
based on channel’s
count rates. Ch5 is
mean QD channel.
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Components & Structure for ESPF
esp_level1.pro
Copy valid data from L0D
Read time range from HK file
Esp_level1, YYYYDOY, int_time,
status, show_data,
filter=filter, version=version
It checks for input parameters
and files, writes parameters
into a log file, returns status
Esp_subtract_dark
Esp_gain_temp_corr
Esp_gain_tid_corr
MB__L1_...fit
Esp_get_flux1
MA__L1_...fit
Esp_get_flux2
Convolution
Esp_get_irrad2
Esp_L1_....fit
Esp_L1_...log
Dec 8 2009
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LASP
Esp_get_irrad_corr
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Components & Structure for ESPR
espr_level1u.pro
Copy valid data from L0D
Subtract_dark
Espr_level1u, YYYYDOY,
status, show_data,
version=version
Rocket_spectrum.dat
Checks for input parameters,
Files, writes parameters into
log file, returns status
Gain_temp_corr
Cnt_eff
Gain_tid_corr
get_irrad12_convolved_slit
fAU , Atm_transm(λ, h)
Esp_rocket_L1_....fit
Esp_rocket_L1_...log
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get_irrad_corr
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ESPF Lev 1 Program Inputs/Outputs
Lev 0D
•
•
•
•
•
•
•
Ch3
Ch i
Flt
t
T
Vref
Valid
Dec 8 2009
L1 Program
•
•
•
•
•
•
•
•
•
•
f(1AU)
Chd(T)
Ch3(T)
Vis
∆G/ ∆t
R(λ,α,β)
f_degrad
A, h, c, λ
∆λ
Eos
MEGS L1
• MEGS-A
• MEGS-B
HK
• α,β-?
• Filter
ESP Lev 1:
FITS, LOG
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Calibration Parameters In-flight
Flight ESP calibration:
• Darks vs. T, t;
• References vs. T, t;
• Vis vs. t (should be corrected for AU distance);
• FOV map for a quiet Sun (± 0.25˚);
• FOV maps for active Sun: irradiance (absolute
and spectral) variability minus solar rotation(?)
• Cruciform;
• Aluminum Filters in the Filter-Wheel;
Dec 8 2009
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Calibr. Updates (Changes in the L1 programs)
• One-time (initial) updates after ESPF
engineering run;
• Weekly updates of ESPF parameters that
show a significant change(?)
• Responsivity updates(?) after NIST
calibration;
• Degradation updates(?) after SR flights;
• VIS and Gain (TID) updates as needed;
• Emergency updates as needed;
Dec 8 2009
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Components & Structure for Lev 0C
esp_level0c.pro
Copy valid data from L0D
ESPF_Subtract_dark
Esp_level0c, YYYYDOY,
status, show_data,
version=version
ESP_L1_YYYYDOY-1
ESP_L1_YYYYDOY-2
Checks for input parameters,
Files, writes parameters into
log file, returns status
Dec 8 2009
Gain_temp_corr
Cnt_eff
Gain_tid_corr
`Irri’ = eff_cnti / coefi
coef1 = 5.6*105
coef2 = 5.0*106
coef4 = 3.7*105
coef5 = 3.7*105 (2008105)
coef6 = 3.7*105
coef7 = 3.7*105
coef8 = 4.0*107
coef9 = 1.9*106
EVE Data Products Workshop,
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Esp_L0c_....fit
Esp_L0c_...log
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An Example for 2008105: Lev 0C
Dec 8 2009
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Things to do before the SDO Launch
1. Model ESP Lev 1 process for one full day based
on all input parameters required for a normal
(flight) operation; Determine whether the ESP
Lev 1 process should be waiting for MEGS-A,B
Lev 1 files or it is activated after the MEGS files
are ready.
2. Model daily (weekly) calibration runs with
extracting required data and updating the Lev 1
programs (a manual process or an automated
process with a visual checks).
3. Update ESP Lev 1 program to include in the fits
headers mean coefficients (ci = eff.cnti / Irri)
Dec 8 2009
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A Comparison of ESPR and MEGS
Dec 8 2009
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Backup slides
(Action Items)
Dec 8 2009
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EVE Workshop –October 7-9, 2008 – Action Items
• Action Item #1: What is the long-term
precision (stability) estimates for EVE
irradiance results? Eparvier for MEGS /
Didkovsky for ESP
Dec 8 2009
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Factors that Affect the Stability
(Degradation Correction)
•
•
•
•
SOHO/CELIAS/SEM
Model of solar variability
Model of atm. absorption
Model of spectral transfer
Stability and accuracy of
SURF calibration
• Dark (background)
• Cover ON/OFF
Dec 8 2009
•
•
•
•
SDO/EVE/ESP
No: Real-time MEGS
Yes
Yes or No
Yes, but better alignment
with QDs
• No, ESPR has a Vis Flt.
• No, ESPR is calibr. w ON
EVE Data Products Workshop,
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Factors that Affect the Stability
Dec 8 2009
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Factors that Affect the Stability
•
•
•
•
SEM
Model of solar variability
Model of atm. absorption
Model of spectral transfer
Stability and accuracy of
SURF calibration
• Dark (background)
• Cover ON/OFF
• About 6% (13 Years)
Dec 8 2009
•
•
•
•
ESP
No: Real-time MEGS
Yes
Yes or No
Yes, but better alignment
with QDs
• No, ESPR has a Vis Flt.
• No, ESPR is calibr. w ON
• About 3%
EVE Data Products Workshop,
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EVE Workshop –October 7-9, 2008 – Action
Items
• Action Item #2: Consider updating rocket
ESP optics before first SDO calibration
rocket flight. Replace rocket ESP grating
with more efficient grating now? Replace
rocket ESP diode #2 as not working well?
Organize telecon to decide. Didkovsky /
Wieman: Done
Dec 8 2009
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EVE Workshop –October 7-9, 2008 – Action
Items
• Action Item #18: Are there really EUV flares
without significant X-ray increase?
ESP will provide the answer. Why? How?
For example, could the SEM EUV flare
indications really be SEP effect instead of
solar flare? Where’s the data? Chamberlin /
Viereck
Easy to separate. SEM data are at USC
website
Dec 8 2009
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An Example of SEM 1st Order (Ch1) Data for 2003/10/28 event
Oct 28, 2003 SEM and GOES 10
2500
SEM Ch1, cnt/s
2000
1500
1000
RMw = (7 – 27) * 15s
EUV
0
10
Dec 8 2009
~100 protons = 2000cnt/s
SEPs
500
12
14
16
18
Time UT, h
20
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Correction for SEP: EVE/ESP
Difference in Proton response between selected ESP science
channels and Ch 3 (dark) detector for flare (based on GOES
"between flare" fluxes)
1.2
Difference (.25sec counts)
1
0.8
0.6
0.4
Ch9-Ch3
Ch1-Ch3
0.2
0
30
35
40
45
50
-0.2
Proton Incident Energy (MeV)
55
60
Correction for SEP:
EVE/ESP
Difference in Proton response between selected ESP science
channels and Ch 3 (dark) for an extreme solar flare (based on GOES
Nov 2, 2003 peak fluxes)
12
Difference (.25sec counts)
10
Ch9-Ch3
Ch1-Ch3
8
6
4
2
0
30
35
40
45
50
55
60
-2
Proton Incident Energy (MeV)
Solution: use science channel (with a blank filter in place) instead of
dark channel. A special program of observations related to extreme solar flares
EVE Workshop –October 7-9, 2008 – Action
Items
• 29A: Distribute the most recent SEM data
product. Judge / USC
Done in Dec 2008.
Dec 8 2009
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