1. AIA Presentation SDO Mission PDR
Alan Title
Principal Investigator
Lockheed Martin
James Lemen
Instrument Scientist
Lockheed Martin
Gary Kushner
Deputy Program Manager
Lockheed Martin

2. AIA Presentation Agenda
Science Investigation Overview Title 5 min
Program Overview Title 5 min
Driving Requirements (Instrument & S/C) Lemen min
Instrument Design & Status Lemen min
Reviews to Date and Planned in Near Term Kushner 5 min
Risks and Issues Kushner 5 min
Schedule, Future Activities, and Conclusions Kushner 5 min

3. AIA is a key component to understanding the Sun and how it drives space weather
AIA images the solar outer atmosphere; its science domain is shaded
HMI measures the surface magnetic fields and the flows that distribute it
EVE provides the variation of the spectral irradiance in the (E)UV

4. Overview of the AIA science investigation
Produce and deliver an instrument that provides new views of the solar corona
Obtain continuous observations of the entire solar corona visible in the EUV
Evaluate the observations to identify processes and discover phenomena
Analyze the observations with the aim of understanding space weather drivers
Infer the coupling mechanisms between various physical domains
Archive the data in an unrestricted web-accessible, easily-queried environment
Provide search tools and metadata to allow efficient retrieval of data by users
Provide access to the data archive and various summary structures
Deliver requested data and calibration techniques to interested users
Involve and stimulate all branches of the LWS research community
Accommodate space-weather community needs in product definition

5. AIA Scientific Objectives•
Energy Input, Storage and Release in
the Outer Solar Atmosphere
The Dynamics of the 3 -
D Corona
Coronal Heating and Irradiance
The Thermal Structure and Heating
Locations
Transients
The Sources of High Energy Radiation and
Particles
Connections to
Geospace
The Particle and Magnetic Field Output of
the Sun
Coronal Seismology
A New Diagnostic of Coronal Physics
A Multi
Thermal Image showing AIA resolution and FOV
A flare showing rapid oscillations in the surrounding loops.
QuickTime™ and a
DV - NTSC decompressor
are needed to see this picture.

6. AIA Level 1 Performance Requirements
FULL SUCCESS Performance Requirements
The AIA shall obtain full-disk images of the solar atmosphere with a field of view of at least 40 arc-minutes in at least eight wavelengths spanning the temperature range from 20,000 to 3 million Kelvin (K) with at least 1.2 arc-seconds resolution (two pixels) and a cadence of no less than one set of eight images every 10 seconds.
MINIMUM SUCCESS Performance Requirements
The AIA shall obtain full-disk images of the solar atmosphere with a field of view of at least 40 arc-minutes in one chromospheric wavelength and three coronal wavelengths spanning the temperature range from 20,000 to 3 million Kelvin (K) with at least 1.2 arc-seconds resolution (two pixels) and a cadence of no less than one set of four images every 10 seconds

7. Program Overview & Future
AIA Program began on 7 November 2003
Quickly confirmed original approaches: science, instrument, and organizations
Augmented HMI team to form LMSAL AIA & HMI & Joint teams
Got program off and rolling at SAO – major partner/subcontractor and time critical
Interface Working Meetings with Project took place immediately
November, January, February
No problems with accommodating AIA onto the S/C; just needs routine work
Conducted PDR-1 on 4 March
Requirements, early design, S/C interfaces and accommodations
Participating in Mission PDR this week
Will conduct PDR-2 in a month (14-15 April)
Preliminary Design classical review
Program moving rapidly and successfully
Enormous leverage from HMI
Extensive heritage from TRACE
Excellent established working relationships with SDO GSFC Project
AIA WILL BE IN-STEP WITH ALL OF SDO BY CONFIRMATION REVIEW

8. LMSAL Combined HMI/AIA Organization
James Lemen
AIA Inst. Scientist
Alan Title
AIA Principal Investigator
& HMI-LMSAL Lead
Phil Scherrer
HMI Principal Investigator
Stanford University
Karel Schrijver
AIA Science Lead
Jake Wolfson
Technical Advisor
Frank Friedlaender
Resource Manager
Edward McFeaters
Mission Assurance
Larry Springer
Program Manager
Rock Bush
HMI Program Manager
Brock Carpenter
System Engineering
Ruth Mix
Configuration Mgmt.
Gary Kushner Wolfson (A)
AIA Deputy PM
Barbara Fischer
HMI Deputy PM
SAO Subsystems – Golub
System Engr. – Carpenter
Optics – Wülser
Mechanical – Chou
Thermal – Yanari
Integ. & Test – Levay
Guide Telescope – Wülser
System Engr. – Miles / Carpenter (A)
Optics – Rairden
Mechanical – Gradwohl
Thermal – Navarro
Integ. & Test – Levay
Drake
Software
Akin
Mechanisms
Lindgren
Electronics
Duncan
CCDs
Thomas
Camera Electronics
HMI & AIA
SOC Ops

9. LMSAL SDO Organizational Features
Single LMSAL SDO Program Manager
Co-ordinates efforts of AIA and HMI
Co-ordinates with Lead Engineers for common program elements
AIA builds on the HMI systems already in place
Electronics and software are the prime instrumental examples
Mission Assurance & Risk Management functions are the prime programmatic examples.
Single LMSAL SDO “Boss”
Alan Title is both the LMSAL Lead on HMI and the PI of AIA
Dedicated Deputy Program Mangers for AIA and HMI
Strong advocates of their programs
Treat the common elements groups almost like vendors
Dedicated Systems Engineers for AIA and HMI
Much of the AIA efforts for mission operations, data analysis, and EPO will be conducted by Stanford University as an extension to those efforts already in place for HMI.
The Smithsonian Astrophysical Observatory has a major role in the AIA program.

10. Driving Requirements Instrument Design and Status
James Lemen
Instrument Scientist

11. AIA Requirements Flow Down
AIA will address all 7 SDO science questions
AIA makes 1 of 5 required SDO science measurements (atmospheric images)
AIA will capture the initiation and progression of dynamic processes with necessary spatial resolution to infer connection to magnetic field and spectral coverage to infer the processes at multiple temperatures
LWS Goals
7 Science Questions
5 Science Measurement
Requirements
5 AIA Science Objectives
Level 1
AIA Instrument
Requirements
Level 3
Mission Requirements
(MRD)
Level 2
Requirements

12. Flowdown to AIA Observing Reqs.
The AIA instrument design and science investigation address all over-arching science questions (1…7) in the SDO Level-1 Requirements (August 2003) 1 2 3
What mechanisms drive the quasi-periodic
11-year cycle of solar activity?
How is active region magnetic flux synthesized, concentrated & dispersed across the solar surface?
How does magnetic reconnection on small scales reorganize the large-scale field topology and current systems?
How significant is it in heating the corona and accelerating the solar wind? 4 5 6 7
Where do the observed variations in the Sun’s total & spectral
irradiance arise, how do they relate to the magnetic activity cycle?
What magnetic field configurations lead to CMEs, filament eruptions
and flares which produce energetic particles and radiation?
Can the structure & dynamics of the solar wind near Earth be
determined from the magnetic field configuration & atmospheric
structure near the solar surface?
When will activity occur and is it possible to make accurate
and reliable forecasts of space weather and climate?
Requirement Spatial Temporal Thermal Intensity
Field of View
x= 1Mm
t continuity
logT T coverage
Accu-racy
Dynamic Range
Science theme
1) Energy Input
Storage & Release
1 4
2 5
3 6
Full Corona
~10 s
Full Disk
passage
~0.3
0.7-8 MK
(full corona) -
Large for simul-taneous obs. of
faint & bright structures
40’-46’
Dynamic Coronal Structure 7
2) Coronal Heating &
Irradiance 4 2 3 7
Active
Regions
<1 min,
a few sec in flares
Days
0.3 for
DEM inv. MK
(full corona)
10%
>1000
Thermal Structure &
Emission
3) Transients 4
2 5 3 7
Majority
of Disk
A few sec in flares
At least
days for
buildup
~0.3 for
T<5MK,
~0.6 for
T>5MK
5000 K - 20 MK -
>1000 in
quiescent
channels
Sources of Radiation
& Energetic Particles
4) Connections to
Geospace 4 5 6 7
Full Disk
+off-limb
~10 s
Continuous observing
~0.3
5000 K - 20 MK
10%
for thermal
struct.
Large to study
high coronal
field
Material & Magnetic
Field Output of the Sun 4 3
As short
as possible
Continuous
for
discovery
~0.5 to
limit LOS confusion
multi-T obs.
for thermal
evolution
10%
for density
5) Coronal Seismology
Active
Regions
>10
Access to new physics

13. Key AIA System Requirements
Level 1 and Level 2 Requirements Result in Key AIA System Requirements
Field of View (FOV) and Pixel Size 41 arcmin/0.6arcsec
Spatial Resolution arcsec2
Temperature Coverage 20K to 20M
Cadence 8 images in 10s
Dynamic Range 13-bit adc; image signal >1,000
Guide Telescope NEA = 1 arcsec; 10Hz update
Level 3 Requirements
Several Important Derived Requirements Flow from Level 3 Requirements
Filters, coatings, detector performance
Mechanisms and their performance
Image Stabilization System
Electronics and Software

14. Baseline Design AIA design meets the Level 1 and 2 Requirements
Four ST’s - 8 Science Channels
7 EUV Channels in a sequence of Fe lines and He 304Å
UV Channel with 1600Å, 1700Å, white light filters
Active secondaries for image stabilization (ISS)
Four GTs
Four 4096 x 4096 thinned, back-llluminated CCD’s
2.3 sec readout of Full CCD
Five mechanism types:
Filter Wheel
Shutter
Focus mechanism
Aperture door (one shot)
Aperture selector (in one telescope)
Flight electronics very similar to HMI
On-board data compression is square root binning and RICE

15. AIA Telescope Array Mounted on IM
Four nearly identical science telescopes
Each ST has a dedicated guide telescope to support its ISS
CEBs mount separately to the IM

16. AIA Telescope Assembly
A GT is mounted to each Science Telescope
CCD Radiator
Guide Telescope (GT)
Camera Electronics Box (CEB)
Proposed Configuration
CEB Radiator
Science Telescope (ST)
Aperture Door

17. AIA Science Telescope Optical Layout

18. Cross section: mechanism locations
Level 3 requirements have been flowed down to all mechanisms
Five mechanism types: all have design heritage
Aperture Door
Wavelength Selector
Shutter Assembly
Filterwheel Assembly
Focus Motor

19. AIA Field of View
Field of View: require observations to at least a pressure scale height (=0.1 Rsolar at Te=3 MK)
AIA: 41 arcmin = 1.3 P 46 arcmin = 2.0 P
(see dashed lines)
AIA will observe 96% of X-ray radiance (based on Yohkoh)
AIA will observe nearly all (~98%) emission that will be in EVE’s FOV
Estimated X-ray radiance at 3 MK as observed by Yohkoh/SXT as function of limb height.
Yohkoh/SXT 8 May 1992

20. Implementation of AIA FOV
AIA will have 41 arcmin FOV along detector axes
AIA will have 46 arcmin FOV along diagonal of detector
Corners of the FOV are vignetted by the filterwheel filters
Composite Trace Image
41 arcmin

21. Spatial Resolution
Telescope response must be adequate over the entire FOV
Criterion: spot size must fall within 1.2x1.2 arcsec2
e2v detector has 12 m pixel size (=0.6 arcsec)  focal length (4.125 m)
Two optical designs are being considered
Ritchey-Crétien: minimizes coma – results in symmetric PSF across FOV
Alternative: minimizes RMS spot size
Candidate Optical Prescription
Suncenter
Solar Limb
2 Pixels
Edge of Field
SDO_0011
24.00 µm
Each channel (half telescope) fits within 2×2 pixels

22. The Benefits of Resolution
EIT
TRACE vs. EIT, shown to
same scale.
AIA’s resolution is comparable
to TRACE.
TRACE
From Deluca et al (AIA00407)

23. AIA Design for Temperature Coverage
AIA implementation makes use of multilayer coatings on normal incidence optics with filtering to achieve desired wavelength and bandpass
EUV wavelengths selected to observe corona at required temperatures
Selected lines of iron to minimize abundance effects
Four wavelengths have not been observed with TRACE or SOHO/EIT
Channel
Visible
1700Å
304Å
1600Å
171Å
193Å
211Å
335Å
94Å
133Å
†† -
12.7
4.7
6.0
7.0
16.5
0.9
4.4
Ion(s)
Continuum
He II
C IV+cont.
Fe IX
Fe XII, XXIV
Fe XIV
Fe XVI
Fe XVIII
Fe XX, XXIII
Region of Atmosphere*
Photosphere
Temperature minimum, photosphere
Chromosphere, transition region,
Transition region + upper photosphere
Quiet corona, upper transition region
Corona and hot flare plasma
Active-region corona
Flaring regions
Char. log(T)
3.7
5.0
5.8
6.1, 7.3
6.3
6.4
6.8
7.0, 7.2
AIA wavelength bands
*Absorption allows imaging of chromospheric material within the corona;
††FWHM, in Å
Fe XVIII
94 Å
Fe XX/XXIII
133 Å
1600Å?
Fe IX/X 171 Å
Fe XII 195 Å
Fe XIV 211 Å
C IV Å
He II 304 Å
Fe XVI 335 Å

24. Selection of Non Coronal Lines
UV channel will have three filters: White light, C IV 1550, UV Continuum
White light used for ground calibration
White light used for co-alignment with HMI and other ground-based instruments
UV filters are similar to TRACE bandpasses
Study waves and field going into the corona as well as particle beams and conducted thermal energy coming down
He II 304A
Observes the chromosphere
Monitor filaments
Key driver to chemistry of the Earth’s outermost atmospheric layers
EIT 304A
14 Sept 1999
Example of a prominence observed by SOHO/EIT. The upper chromosphere has a temperature of 60,000 K.

25. AIA Temperature Coverage
EUV Wavelength selection meets AIA science objectives
Dots are SOHO/CDS + Yohkoh data. Black curve is the recovered DEM using simulated AIA responses. The responses of the AIA channels are shown normalized to recovered DEM.

26. DEM Reconstruction Tests
Tests performed with simulated data – predicted AIA response functions show that multiple channels are necessary to constrain solution for DEM
Consistent with the fact that the solar atmosphere is emitting over a broad range of temperatures
With five channels, it is often possible to achieve solutions, but the quality of the recovered DEM improves with the number of temperature channels
4 channels
(131,175,193,211)
7 channels
(6 EUV+304)
From Deluca et al (AIA00407)

27. 10-s cadence achieved with 4 telescopes
Each telescope must maintain a 5-sec cadence
Looking at the AIA from the Sun
1600 C IV
1700 UV Cont.
4500 White Light
He II
Fe XIV
Fe XVI
304 94 UV
171
211
193
335
133
Fe XVIII
Fe IX
Fe XII/XXIV
Fe XX/XXIII +Y +Z
Instrument Module / Optical Bench

28. Dynamic Range AIA meets dynamic range requirements
Camera must be 13 bit design
AIA Science Objectives 2 and 3 require a dynamic range of >1,000
Camera design has 14 bit ADC
e2v CCD has low noise, high efficiency, adequate well dept (> 150,000 electrons)
335 A channel is the limiting case for EUV wavelengths: (12.398/335)/3.65*150,000=1521

29. GT Design Mechanically similar to STEREO/SECCHI
Same optical prescription as TRACE
Linear range is ±95 arcsec
Co-alignment to science telescope is ±20 arcsec
One will be ACS prime and the other will be redundant
All four are available to the ACS
Photo diodes and preamp circuits are redundant
No cross-strapping for ISS
Low and high gains enable ground testing with StimTel

30. SECCHI Guide Telescopes
AIA mechanical design is a copy of the STEREO/ SECCHI design
Optical prescription is same as TRACE
Preamp electronics are identical to SECCHI
1-Foot Ruler

31. Extensive Heritage with AIA Mechanisms
Triana/EPIC/XRT Shutter Mechanism
TRACE door
These mechanisms meet AIA requirements
SECCHI/EUVI active secondary
Solar-B Filterwheel mechanism

32. Significant Progress on Mechanism Design
Aperture selector used for 193Å/211Å telescope
Uses brushless DC motor
Position change requires 1 sec
Heritage from STEREO/SECCHI
Aperture Selector Design
Focus mechanism is based on the TRACE design
Provides 800 m movement of secondary mirror
Lever driven by brushless DC motor
Focus Mech Design (Trace)

33. AIA Block Diagram

34. AIA Electronics Boxes AIA Electronics Box (AEB)
Basic layout similar to HMI
Connectors will be on the long side
Connectors shown are notional
AIA Camera Electronics Box (CEB)
Identical to HMI
Mounts to IM behind science telescope focal plane assembly

35. Spacecraft Resources – Mass & Power
Allocation = 130 kg
Current Estimate: Harness (6kg) + AEB (27kg) + AOP (87kg) = 120 kg
Margin = 7.7 % (S/C holds >/= 20% margin above allocation)
AVERAGE POWER
Allocation = 135 W
Current Estimate = 108 W (avg. of imaging and readout power)
Margin = 20 % (S/C holds >/= 20% margin above allocation)
Resource estimates to be reviewed for PDR-2 to assure appropriate PDR-level margins are maintained at the Spacecraft level.

36. Program Status and Accomplishments
Gary Kushner
Deputy Program Manager

37. AIA on Track for Successful PDR in April (1 of 4)
Undefinitized letter of contract, November 2003
Definitized contract, February 2004
AIA and SAO making significant progress on design and interfaces
Letter of subcontract to SAO on November
Conferring weekly on designs and interfaces
Holding bi weekly contamination control working group discussions
Developed initial Telescope Assembly Alignment and Installation Plan
Long-Lead Items identified and well understood
Mirror blanks on order
Two life-test filterwheels on order
Life-test chamber and GSE designed; GSE under procurement
Coating Vendors under contract to start development-phase work
Front-filter test program initiated in February

38. AIA on Track for Successful PDR in April (2 of 4)
In a very short period of time, AIA has released a large amount of program documentation to PDR level.
HMI/AIA PAIP (Released)
Contamination Control Plan (Draft)
Risk Management Plan (Draft)
WBS Dictionary (In release)
Instrument Performance Document (Draft)
AIA Software Requirements Document (Draft)
AIA Software Management Plan (In Release)
HMI/AIA Program Management Plan (In Release)
HMI/AIA Configuration Management Plan (Released)
AIA Performance Verification Plan (Draft)
HMI/AIA SOC Ground System Plan (Draft)
Education and Public Outreach Plan (Draft)
Initial AIA Program Schedule

39. AIA on Track for Successful PDR in April (3 of 4)
AIA-Spacecraft ICD progress
Participated in January Interface Working Group to initiate AIA ICD
HMI Spacecraft ICD used as basis for first draft of AIA ICD, leveraging commonality
Received first draft of ICD on 1 March 2004, in review
Important trades initiated and discussed with Project
Project concurred on increase from 2 to 4 guide telescopes
Project reviewing data rate increase (58 to 67Mbs); currently at CCB
AIA reviewing CEB mounting Science Telescope to Instrument Module with Project
Design effort on track to support PDR in April 2004
Aggressive internal and peer review schedules (see following list)
Team in place with distributed responsibilities
EEE Parts Control Board Held at LMSAL on February 24, 2004
Successful meeting with 337 line items boarded, 301 approved (89%)
Materials and Process Board Held at LMSAL on February 25, 2004
Successful meeting with all materials (to-date) reviewed. Processes at next board.

40. AIA on Track for Successful PDR in April (4 of 4)
AIA Technical Reviews
Internal reviews
Focal Plane Assembly
Telescope Assembly and optical alignments
Secondary Spider Assembly
GT mounting legs
Focus Mechanism
Program Reviews
PDR-1, accommodations and requirements, March 4
AIA Technical Reviews Planned for March
Internal
Software
Electronics
Thermal
Peer Reviews
GT March 16
FPA March 17
Spider March 18
Telescope Assembly March 25
Thermal March 25
Mechanisms March 26
Electronics March 31
Software March 30
Program Reviews
AIA ICD WG March
PDR-2 April
CDR Jan 2005

41. AIA Risk Assessment (1 of 2)
Camera Electronics Development – Medium
Covered by HMI
CCD Development – Medium
Contamination – Medium
Description
AIA is an EUV instrument and is sensitive to contamination
Performance of instrument can be degraded
Mitigation
Pervasive contamination control program with extensive experience with Trace and similar programs
Flowdown of requirements to component levels
Continuous monitoring and sampling program

42. AIA Risk Assessment (2 of 2)
EUV Coated Optics – Low
Description
If the optics coating vendor has difficulty delivering the coated optics, this could result in cost increases for the program
Mitigation
Parallel path coating development.
Start development early in program
Front Filters – Low
AIA uses thin aluminum and zirconium filters.
If the protection measures are not adequate to protect the filters from the acoustic environment, the program schedule will be delayed while the filter protection is redesigned.
Early program development of filter frame and testing in acoustic environment
Structural model testing of filter frames and flight like filters.

43. AIA Summary Schedule

44. AIA Schedule Notes
Due to the late start, AIA’s challenge is to meet the SDO instrument delivery need date.
The schedule shows delivery on 15 February 2007; two months later than the desired delivery in December 2006
The schedule includes 4 Months of program contingency.
We are working on options to improve the delivery
Critical path goes through the telescope structure at SAO
The EUV optics are currently 5 months off the critical path
CCD Detectors & CCD Camera Electronics 4 Months off the Critical Path
Important Milestones
AIA PDR & 15 April 2004
AIA CDR 13 January 2005
Final CCD deliveries 15 September 2005
Final Camera deliveries 22 December 2005
Last Telescope Delivery from SAO to LMSAL 25 April 2006
AIA Acceptance Testing Starts 2 August 2006

45. Near Term Focus on PDR and CDR
Conduct peer reviews of all major subsystems by PDR-2, April
Perform Radiation Ray Trace analysis on PDR design ~July 2004
Start Structural Model development June 2004
Majority of Structural Model tests completed prior to CDR.
Mechanisms life testing will start Oct 2004, some components already on order
Contamination modeling and release of Contamination Plan prior to CDR
SAO performing proof-of-concept acoustic tests of front filters

46. Conclusions
AIA design is rapidly approaching PDR level and will be in step with SDO program by Confirmation Review
AIA building on HMI design effort in many areas, from the focal plane to Level 1 Data Products
Mechanisms
CCDs
Cameras
Electronics
Data Pipeline
Software
LMSAL and SAO teams bring significant heritage and expertise
AIA has aggressive, but achievable, schedule for achieving PDR and CDR activities
LMSAL and SAO working closely on telescope and interface designs
Mission is well understood
Team is in place and ready for the challenge

47. Backups

48. AIA Technical Development Program
Two Technical Development paths:
1. CCDs
Incremental development of FPP format
E2v has already produced non-flight functioning devices
Development program underway:
First images obtained Early February
Demonstration Model Delivered to LMSAL April ’04
Demonstration Model Evaluation April – June ’04
2. Front Filters
Most filters well understood with Trace heritage
Zirconium filters have sounding rocket experience only
Prototype filter test program underway with planned acoustic testing
All other technologies have significant heritage and team experience

49. CCD Camera Systems CCD Camera Systems are key elements of HMI & AIA
Were to be provided by UK Co-investigators
Now being procured from UK suppliers under subcontracts (same suppliers)
HMI and AIA use identical cameras
CCD – 4096 x 4096, 12 micron pixels
Extension of devices that are being used on Solar-B FPP (2048 x 4096 pixels)
HMI and AIA use identical CCDs except AIA CCDs are back-side thinned
e2v has already produced functioning non-flight devices
e2v is the best supplier in the world for such devices
CEB – 8 Mpixels/sec via 2 Mpixels/sec from 4 ports simultaneously
Extension of SECCHI/STEREO cameras by RAL
Design modifications are quite mature with rescopes being imposed early to maintain schedule
High visibility and cooperative approach to obtaining the CCD Camera Systems
Working group established that includes GSFC experts
Weekly telecons
Three meetings in the UK and two in the US
Established demonstration programs at both RAL and e2v early in the mission
Confidence is high for obtaining both CCDs and Camera Electronics on schedule