ÐÏà¡±á>þÿ =?þÿÿÿ:;<ÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿì¥Á7 ø¿u'bjbjUU $b7|7|R+ ÿÿÿÿÿÿlöööö²²²Æ„—„—„—8¼—4ð—lÆxÐfhœhœ(œœ¦œgžgžgž[Ï]Ï]Ï]Ï]Ï]Ï]Ï$ÞÑ þÓvÏ±²gžEž"gžgžgžÏá¦ööœ¦œŸ2Ðá¦á¦á¦gžzö†œ²¦œ[Ïá¦gž[Ïá¦>á¦rß´T|6²Oµ¦œ\œ°AÚÕÍÀÆ¾“„—á¦3µOµHÐ0xÐAµtÔá¦tÔOµá¦ÆÆööööÙCELT Report No. 14 Design Team Quarterly Report No. 2 March 2001 Contents 1. Introduction 2. Summary 3. Budget 4. Schedule 5. Concerns 6. Task Descriptions 1. Introduction The University of California and the California Institute of Technology (partners in the W. M. Keck Observatory) are collaborating to build a 30-meter telescope (CELT), designed to be fully steerable and operate on the ground. With its Ritchey-Chretien optical design it will have a large, 20-arcminute, field of view; and with planned adaptive optics, it will produce diffraction-limited images for wavelengths as short as one micron. A year-long Conceptual Design Phase is described in CELT Report No. 9 "CELT Conceptual Design Plan", Jerry Nelson, Terry Mast, Gary Chanan, Richard Dekany (July 2000). The first quarter is reported in CELT Report #12 which describes many details of the Tasks. For efficiency we have not repeated them here; we mainly describe here the progress in the second quarter. Table 1 lists some aspects of the full CELT Observatory Project and organizes the thirty conceptual design phase tasks by aspect. Table 1. Tasks in context of full CELT program Observatory Requirements Task [ 1] Telescope Design Error Budgets Task [ 2] External Design Driver: Wind Task [ 3] Optical Design Task [ 4] Primary Mirror Tasks[ 5 -17] Auxiliary Optics Tasks[18-19] Telescope Structure Tasks[20-21] Adaptive Optics Modes of operation Task [22] Error budgets Task [23] Alternative Design Concepts Tasks[24] Conceptual Design Review Task [25] Preliminary Design Plan Task [26] CELT Working Groups Task [27] Conceptual Design Phase Management Task [28] CELT Website Management Task [29] Contingency Management Task [30] Table 2 gives the titles of the 30 conceptual design-phase tasks and serves as a table of contents. Table 2. Task List page [ 1] Observatory requirements 8 [ 2] Error budgets 9 [ 3] Analyze and model wind influence on telescope 10 [ 4] Complete the optical design 12 [ 5] Establish the segmentation geometry 13 [ 6] Establish the segment material 15 [ 7] Establish the segment fabrication vendor candidates 17 [ 8] Establish the segment fabrication cost 18 [ 9] Stressing fixture design, fabricate, and test 19 [10] Define the segment figure tests 20 [11] Design the segment passive support 22 [12] Develop algorithms to combine Displacement Sensor and Telescope-Control Wavefront Sensor (TCWS) readings 23 [13] Study the spatial frequency response of the primary mirror control 25 [14] Segment displacement sensors (design, fabricate, test) 26 [15] Design Telescope-Control Wavefront Sensor (TCWS) hardware 27 [16] Segment support actuators (design, select, test) 28 [17] Design camera required to determine desired sensor readings 30 [18] Define secondary mirror physical & performance parameters 31 [19] Develop algorithms for TCWS control of primary, secondary, & guiding 32 [20] Design the telescope structure 33 [21] Generate strawman designs of the bearings, drives, encoders 34 [22] Identify the candidate AO modes & define requirements for each 35 [23] Develop first order error budgets for AO components 35 [24] Develop conceptual AO system optical designs for each AO mode 35 [25] Prepare for Conceptual Design Review 36 [26] Write the Preliminary Design development plan 36 [27] Support the CELT Working Groups 37 [28] Manage the Conceptual Design phase program 37 [29] Manage the CELT Website 38 [30] Contingency Management 38 2. Summary Significant progress has been made on a number of key design issues during this quarter. We have complete or nearly complete reports addressing segment passive support, segment actuators, and segment interferometric testing. We also have excellent first drafts of the design requirements and the error budgets. We have hired consultants to work with us on the telescope structure, telescope bearings, drives, and encoders. We have also hired consultants to create an intial design of one of the candidate actuator types. Tools were created that calculate the CELT segment control matrix, analyze its spatial frequency content, and use it to understand error propagation based on the proposed displacement sensor design. A Reports and Technical Notes series document the design efforts, and a website provides access to these as well as information about CELT personnel and calendar activities. A full time engineer has been hired at UCO/Lick who will work on designing a prototype stressing fixture and a test facility for prototype sensors. He will also be available for future testing of candidate actuators and mechanical testing of segment surfaces. A technical staff member of UCO/Lick is working on CELT sensor design issues and prototypes. Significant progress was made this quarter on the issues listed below. Details about these issues and others are given in the Section 6. observatory requirements error budgets segment displacement sensors interferometric testing of segments segment passive support segment support actuators spatial frequency response of the primary mirror control 3. Budget TaskDESCRIPTIONBudgetQ1DecJanFebLiensTotalBalanceADMINISTRATION28Project Management20.012.81.22.80.116.928Travel20.09.90.81.62.314.6TOTAL ADMINISTRATION40.022.72.04.32.40.031.58.5OBSERVATORY3Wind influence on telescope60.00.10.00.127Working Groups Support50.00.029Website Management10.00.01Observatory Requirements10.07.10.10.17.225Conceptual Design Review15.00.00.10.1TOTAL OBSERVATORY145.07.10.20.10.10.07.4137.6OPTICS4Optical Design5.00.05Segmentation Geometry5.00.06Segment Material5.00.07Segment Fab vendor candidates20.00.09Stress fixture design, fab & test45.00.011Design segment passive support55.08.48.40.022.555.012Combine Displace /TCWS readings12.00.013Primary mirror control SFR19.00.014Segment Displace Sensors60.00.015TCSE hardware Design7.00.016Segment Support actuators 45.01.05.00.030.845.017Camera design14.00.024Conceptual AO system optical designs50.00.0TOTAL OPTICS342.023.89.413.40.053.3100.0242.0TELESCOPE20Telescope Structure Design65.035.010.010.020.065.021Prelim design bearings, drives, encoders30.030.030.0TOTAL TELESCOPE95.035.00.010.010.050.095.00.030MANAGEMENT CONTINGENCY128.0128.0TOTAL750.088.72.214.42.6103.3233.9516.1 4. Schedule Activity duration start end [ 1] Observatory Requirements255 d22-Sep-0024-Sep-01 Observatory Requirements Document51 w22-Sep-0024-Sep-01 Quarterly Review #10 d01-Dec-001-Dec-00 Quarterly Review #20 d06-Mar-016-Mar-01 Quarterly Review #30 d05-Jun-015-Jun-01 Quarterly Review #40 d11-Sep-0111-Sep-01[ 2] Error budgets255 d22-Sep-0024-Sep-01 Adaptive Optics on51 w22-Sep-0024-Sep-01 Adaptive Optics off51 w22-Sep-0024-Sep-01 Internal Review0 d15-Jan-0115-Jan-01 Detailed Review0 d01-Feb-011-Feb-01[ 3] Analyze and model wind influence on telescope125 d22-Sep-0026-Mar-01 Caracterize Free Winds at Sites25 w22-Sep-0026-Mar-01 Determine Wind Force on Dome25 w22-Sep-0026-Mar-01 Determine Wind Spectra Inside Dome25 w22-Sep-0026-Mar-01 Determine Wind Dynamics on Primary Mirror25 w22-Sep-0026-Mar-01[ 4] Complete the optical design255 d22-Sep-0024-Sep-01 Optical Design51 w22-Sep-0024-Sep-01 Initial Optical Design0 d22-Sep-0022-Sep-00 Revised Optical Design0 d02-Feb-012-Feb-01 Conceptual Stage Optical Design0 d11-Sep-0111-Sep-01[ 5] Establish the segmentation geometry51 w22-Sep-0024-Sep-01[ 6] Establish the segment material 51 w22-Sep-0024-Sep-01[ 7] Establish the segment fabrication vendor candidates51 w22-Sep-0024-Sep-01[ 8] Establish the segment fabrication cost51 w22-Sep-0024-Sep-01[ 9] Stressing fixture design, fabricate, and test127 d22-Sep-0028-Mar-01 Calculate Conceptual Design & Reqiurements14 w22-Sep-008-Jan-01 Design Stress Fixture4 w04-Jan-0131-Jan-01 Fabricate Stress Fixture4 w01-Feb-0128-Feb-01 Test Mirror Stress Fixture4 w01-Mar-0128-Mar-01[10] Define the segment fabrication figure tests255 d22-Sep-0024-Sep-01 Design an LVDT system4 w04-Jan-0131-Jan-01 Test LVDT System4 w01-Feb-0128-Feb-01 Develop Optical Test of Segment Figure51 w22-Sep-0024-Sep-01[11] Design the segment passive support236 d22-Sep-0028-Aug-01 write requirements236 d22-Sep-0028-Aug-01 write contract and award2 w22-Sep-005-Oct-00 segment support study21 w06-Oct-0012-Mar-01 Freeze Concept0 d14-Mar-0114-Mar-01 Fabricate Prototype8 w14-Mar-018-May-01 Test Protype16 w09-May-0128-Aug-01[12] Algorithms to combine Displacement & TCWS readings51 w22-Sep-0024-Sep-01[13] Study the spatial frequency response of the primary mirror control51 w22-Sep-0024-Sep-01[14] Segment displacement sensors (design, fabricate, test)159 d03-Jan-0113-Aug-01 write requirements2 w03-Jan-0116-Jan-01 write contract4.25 w17-Jan-0115-Feb-01 Segment displacement sensor study25 w20-Feb-0113-Aug-01[15] Design Telescope-Control Wavefront Sensor (TCWS) hardware51 w22-Sep-0024-Sep-01[16] Segment support actuators (design, select, test)220 d22-Sep-006-Aug-01 write requirements220 d22-Sep-006-Aug-01 write contract and award2 w22-Sep-005-Oct-00 actuator study18 w06-Oct-0019-Feb-01 Lorell Study- Write contract and award19.6 w22-Sep-0015-Feb-01 Lorell Actuator Study24 w16-Feb-012-Aug-01 Accuire Test Acturators8 w20-Feb-0116-Apr-01 Develop Actuator Test Program6 w20-Feb-012-Apr-01 Test Actuators16 w17-Apr-016-Aug-01[17] Design camera required to determine desired sensor readings51 w22-Sep-0024-Sep-01[18] Define secondary & tertiary physical & performance parameters51 w21-Sep-0021-Sep-01[19] Algorithms for TCWS control of primary, secondary, & guiding 25 w01-Mar-0122-Aug-01[20] Design the telescope structure101 d22-Sep-0020-Feb-01 Write requirements and contract goals for SJM and award contract2 w22-Sep-005-Oct-00 Telescope structure study18.4 w05-Oct-0020-Feb-01[21] Generate strawman designs of the bearings, drives, encoders145 d04-Dec-003-Jul-01 Write Contract and Award4 w04-Dec-009-Jan-01 Phase 1 Bearings, Drives, and Encoders Study16 w10-Jan-011-May-01 Phase 2 Bearings, Drives, and Encoders Study9 w02-May-013-Jul-01[22] Identify the candidate AO modes & define requirements for each51 w22-Sep-0024-Sep-01[23] Develop first order error budgets for AO components51 w22-Sep-0024-Sep-01[24] Develop conceptual AO system optical designs for each AO mode51 w22-Sep-0024-Sep-01[25] Prepare for Conceptual Design Review5 w15-Aug-0118-Sep-01[26] Write the Preliminary Design development plan5 w15-Aug-0118-Sep-01[27] Support the CELT Working Groups51 w22-Sep-0024-Sep-01[28] Manage the Conceptual Design phase program255 d22-Sep-0024-Sep-01 Weekly Telecons and Team Meetings51 w22-Sep-0024-Sep-01 CELT Workshop Meeting0 d02-Feb-012-Feb-01[29] Manage the CELT Website51 w22-Sep-0024-Sep-01 A Gantt chart will be presented at the CELT Steering Committee meeting. 5. Concerns Although there has been important and significant progress, there are key issues that are unresolved and are required for many other parts of the study. Their timely resolution is critical. The effects of the wind are not yet adequately understood,, and the plan for completing this task is vague. The effect of wind may be a critical driver for the telescope, but this must be made quantitative. Hence completion of the telescope structural design is seriously hindered by the poor progress on understanding wind. It may be that the most acceptable telescope structures (acceptable due to wind) produce significant blockage of the primary. The likely scientific impact of this blockage needs to be carefully assessed. If it is viewed as a serious problem, and none of the current telescope structure designs are acceptable, then more radical departures in design may be necessary. This could drive the entire design study. Plausible costs for edge sensors, actuators, and segment fabrication are needed before we can reasonably optimize the segment size and the primary mirror focal length. We will also need the segment alignment error budget and secure knowledge about the mirror cell gravity deformations. Concerted effort needs to be applied here so we can freeze the optical design sooner, rather than later. Adaptive optics requires technologies not yet availabl,e and building designs around non-existent technology is risky. An adaptive secondary mirror may be extremely challenging, so its value must be carefully understood. If needed, it will influence the telescope structure design. Further, the optical design for MCAO may drive the telescope optical design. The auxiliary requirements of MCAO (number, launch locations, and power of lasers) may have a strong influence on the observatory design, and the requirements are unknown. Many tasks are either not started or barely begun, and our ability to complete the conceptual design study in 12 months is untested. The fact that many tasks are strongly inter-related and that some key ones are barely begun is a clear cause for concern about keeping to our schedule. 6. Task Descriptions For each task we briefly repeat from CELT Report No. 9 "California Extremely Large Telescope (CELT) Conceptual Design Plan", the description of the task. Then for each task we describe the progress made this quarter and the plans for the future. Task [ 1] Determine Observatory Requirements Description We will write the observatory requirements which will form the over riding document that dictates the design objectives. This will evolve with discussions with the working groups and with the Steering Committee. Inputs Working Group Reports Impact on Other Tasks Fundamental requirements for all tasks Progress this Quarter The first draft was written and carefully reviewed by the Steering Committee on 1 February 2001. A second draft has been issued based on comments from that meeting It has been distributed to the Steering committee for comment. Plan for Future The following open issues need to be resolved. • The value of a prime focus needs to be reviewed in light of very small FOV. • The short wavelength cutoff of the telescope needs to be reviewed in light of coating concerns. • The environmental conditions at sites other than Mauna Kea need to be included. • Sky coverage with laser beacons is not yet known. • What Strehl degradation vs FOV is required/possible? • Adaptive secondary specifications need review: number of degrees of freedom and f-ratio. Task [ 2] Error budgets Description Error budgets for image quality will be completed. These are being constructed for both observing modes; AO-on (in terms of rms wavefront error) and AO-off (in terms of 80% enclosed energy diameters). Objectives Construct global telescope error budgets and detailed error budgets for the segmented primary mirror. Also construct error budgets for image motion. Inputs Complete Task 4 Initial work on Tasks 5 and 10 Initial values of telescope optical design. Baseline design for primary mirror active control. Site environmental properties Impact on Other Tasks All other tasks will interact strongly with the error budgets. Candidate designs will define the budgeting and the budgeted errors will drive the designs. Progress this Quarter Initial draft error budgets for AO-on and AO-off modes have been written and are currently being refined with detailed calculations. The error budgets include both a global telescope budget and a detailed budget for the primary mirror. An important contribution to any adaptive optics error budget is the "fitting error" that describes the rms residual wavefront resulting from the limited ability of the deformable mirror to correct all spatial frequencies. Much has been studied and written about fitting errors. At the intersection of AO and a segmented primary, is the fitting error resulting from surface errors in the segments. We have nearly completed CELT Technical Note No. 1 that calculates the fitting error (as a function of deformable mirror actuator spacing) for random Zernike aberrations in an array of hexagonal segments. Substantial progress was made during this quarter on completing the error budgets. The required ray trace, rms wavefront, and AO fitting error calculation tools were completed. The methods and assumptions were reviewed in a two-hour review with the CELT Steering Committee. With the completion of these milestones we are now poised to rapidly complete the budgets. The calculation of the contribution of each term is described in terms of equations, so that the value can be readily revised when the telescope optical or primary mirror design parameters change. Plan for Future In the first half of the third quarter we will complete the Error Budgets, CELT Report No. 10, and the supporting documents. Task [ 3] Analyze and model wind influence on telescope Description Wind loads on the telescope will be studied. Loads during operations and survival loads on the dome will be addressed. During operations, there is the potential that wind loads directly on the top end of the telescope will cause the telescope to move and oscillate, causing image motion. In addition there is the possibility that wind loads on the primary itself will cause distortion of the primary mirror, occurring at frequencies higher than the bandwidth of the primary mirror active control system (ACS). Finally, wind loads on the dome itself may cause motion of the earth and hence the entire telescope on its pier. We expect to use a combination of analytic tools, computer simulation, wind tunnel testing, and scaling from other observatories to assess the size of the wind disturbances. Objectives We will estimate the static wind speed distribution inside the dome (near the top end of the telescope down to the primary mirror) relative to the outside wind speed. This will be used to calculate the static force on the telescope. This speed distribution will be determined by some combination of Measurements at Keck or other large telescope Computer modeling Wind or water tunnel measurements We will estimate the dynamic effects of wind on the telescope as well, including spatial and temporal coherence. Inputs • Wind statistics for each candidate site (probability distribution of wind speeds on clear nights) • Maximum 100 year wind speeds for each site (for survival study) • Elastic properties of the soil under the dome for each site. • Shape and cross section details of the top end of the telescope • Power spectrum of wind at the site Impact on Other Tasks This will influence the telescope design, and the dome design Status Wind forces on the telescope may cause image motion in excess of allowed values. This is a critical unresolved issue for the CELT design The central problem is to estimate the dynamic forces on the telescope that may cause the images to move. There are several approaches to becoming informed: 1. Simple calculations of “static” wind force on the telescope can be made, using some assumed wind attenuation inside the dome and appropriate drag coefficients and Reynolds numbers. Then, given an assumed telescope stiffness, image motion can be estimated There exists Gemini data with wind speeds at top of structure structure, along with external wind speed and orientation. Analysis of this data could be informative. Computer-based simulations of the wind power spectrum inside the dome might be made. Wind tunnel tests to estimate the wind power spectrum inside the dome might b e made Wind speeds and turbulent spectrum might be measured at Keck. Progress this Quarter We have been exploring different sources of wind information, from books to experts to wind data on Gemini. This education process is continuing, so no definitive conclusions are yet available. We have had preliminary discussions with Rose McCallan of LLNL concerning the likely effects of wind on structures. She recommends some combination of wind tunnel testing and computer simulations for reliable results. Efforts to explore the use of an environmental wind tunnel at UC Davis, operated by Bruce White, have led to the conclusion that this wind tunnel is not appropriate. We have made a preliminary examination of some of the Gemini wind tests (anemometers inside the dome of Gemini S). From this, our view is that wind speeds inside the dome at the top of the telescope will be reduced by about a factor of two from the outside air, with some dependence on the orientation of the dome slit with respect to the wind direction. Further, it appears that the wind speed near the primary mirror is reduced by roughly a factor of 10 relative to the outside wind speed. These results are compatible with those used in modeling Keck. The upper "tube" of CELT is likely to be composed of trusses, rather than simple tubular beams. Discussions with McCallan and the reading of wind references (Simiu and Scanlan Wind Effects on Structures) suggest that wind forces on these trusses can be estimated by standard methods (F = Cdrðv2A/2) and that cross talk between members of the truss will not significantly alter the result. For some of the telescope designs in progress we have estimated the static wind loads and possible resulting image motion. The results suggest that wind will be a significant issue, driving the telescope design, but also that acceptable solutions might be possible. Plan for Future We will examine the Gemini data more carefully to better assess the static and dynamic characteristics of wind inside the dome. We will work closely with McCallan to check our methodology and to assess which wind tunnel tests should be carried out and which computer modeling should be done. The power spectrum of the wind will be estimated through some combination of Gemini data, simulations, and wind tunnel tests. The likely forces on several telescope designs will be produced, and the likely resulting image motion will be estimated and fed back into the telescope structure design. Task [ 4] Complete the optical design Description We will produce an optical design for CELT that includes a mathematical description of the optical surfaces and locations. The design performance of the system will be produced, including image quality, field of view, focal surface curvature, pupil positions, and sensitivity to misalignment. Objectives We will produce a Ritchey-Chretien optical design giving a 20 arc minute field of view with 0.5 arc second image quality (100% enclosed energy). Initial and final f-ratios are critical parameters that will be set, after a trade off study. The compatibility with planned adaptive optics systems for CELT will be carefully assessed and maximized. The sizes of the secondary and tertiary will also be carefully explored to understand their values in the optical design and the tradeoffs against difficulty of fabrication. Focal plane locations will be determined, taking into account the space required for science instruments Inputs Requirements on FOV, plate scale, and instrument sizes from working groups Impact on Other Tasks The optical design parameters are fundamentally related to the optimization of the segment polishing, mainly though the primary mirror focal length. The requirements of AO are also key inputs to the optical design, through the final focal length, focus position, and possibly special requirements for the secondary mirror. The telescope structure is driven by the optical design. Status A conceptual design exists with an f/1.5 primary (k = 90 m) and a back focal distance of 15 m with a final f-ratio of f/15. This design is sufficiently complete for current purposes. Progress this Quarter An analysis of the potential for using the prime focus has been completed. A seeing limited FOV of 24 arcseconds is possible. Its value needs to be assessed. Plan for Future When we have additional information on component costs and alignment sensitivities we will make a trade study of the value of changing the primary focal length. Information from the working groups may also cause us to re-evaluate the final focal length and back focal distance. Task [ 5] Establish the segmentation geometry As expected, the descriptions for this task status, progress, and plan have not changed this quarter. For convenience they are repeated here from the Quarterly Report No. 1 Description We will establish the thickness and radius (and thus the number of segments) of each segment. This will involve a complex tradeoff of many issues including predicted effects of thermal and gravitational changes, segment material costs, segment fabrication costs, segment passive support system costs, segment active control costs, impact on adaptive optics, re-aluminizing costs, and handling costs. Inputs None required for about six months. Then for a review, and possible revision of the geometry, we will require initial telescope and primary mirror error budgets and initial cost estimates for segment fabrication. Cost estimates for segment fabrication and tests Impact on Other Tasks The definition of the segmentation is strongly inter-related to almost all other tasks. Progress this Quarter The segmentation geometry of the primary mirror is mainly defined by two parameters: the hexagonal segment sidelength (a) and the segment thickness (h). The selection of a segment size, and hence the number of segments, depends on a complex tradeoff of many costs. A larger segment size (radius = a, thickness = h) increases the amount of asphericity required in the surface figure (~a2), the gravity-induced deflections on a support, (~a4 / h2) , the weight for handling (~a2 h), and sensitivity to position errors in the array (~a2). A smaller segment size increases the number of active control actuators and sensors, the complexity of a control wavefront sensor, and the complexity of the alignment and control software. The selection of the segment thickness is also a complex compromise between costs. A larger thickness will require larger required forces for intentional deformation during fabrication, greater cost of the blank material, greater thermal inertia in the telescope, and a greater mass for the support structure (the telescope). A smaller thickness will require more support points to reduce deformations due to gravity. We have not yet gathered estimates of these costs and cost variations. This will be required to make final informed compromises. Based on our experience with the Keck telescopes, we have adopted for now a baseline segment design. During the conceptual design phase this will evolve to final values for the radius and thickness. In the meantime we have adopted a segment radius of a = 0.5 meters and a segment thickness of h = 45 millimeters. The resulting array contains 1080 segments. A central subset of 19 segments is deleted from the array since the light to them is blocked by the secondary mirror. This baseline array has an area = 702 m2. A discussion of some segment fabrication issues that affect the selection of segmentation geometry is given in CELT Report No. 5. "Primary Mirror Segment Fabrication for CELT", Terry S. Mast, Jerry E. Nelson, and Gary Sommargren, Proceedings of the SPIE, 4003, 2000 The current status is summarized in Quarterly Report No. 1, (CELT Report 12 Progress on this task relies on the completion of other tasks (7-9, 14,16) that are currently being actively addressed. Progress on the selection of a segmentation geometry is being made through work on other tasks. Definition of baseline designs for segment actuators (Task 16), segment sensors (Task 14), and segment support (Task 9) will allow estimates of these component costs. Definition of the segment fabrication techniques and vendor estimates (Tasks 7 to 10) will provide additional cost estimates. All of these costs are required for the selection of a final segmentation geometry. Plan for Future Work on all associated costs will continue. We do not expect to have the required cost estimates until the end of the third quarter. We also have the option of adjusting the positions of some peripheral segments to keep a closely circular periphery and at the same time to allow for convenient division of the array into subsets (full and partial “rafts” of 19 segments) for ease of handling. This adjustment, the inter-segment gap size, and the segment prism geometry are additional segmentation geometry issues that will be addressed. Work on all associated costs will continue. We do not expect to have the required cost estimates until the end of the third quarter. Task [ 6] Establish the segment material Description The choice of segment material is important since most interesting materials are very expensive. The method of creating the optical surface on the segments will influence the options for material. For segment polishing, one needs either a directly polishable material or one that can be effectively plated. Glassy materials such as Zerodur or ULE are well known, but expensive choices. Aluminum is another potentially less expensive option that needs to be explored. More exotic materials such as SiC should also be investigated. Objectives Based on collected material properties we will assess the likely impact on segment thickness and mass, resulting telescope mass, and passive segment support. All these will influence, and may strongly impact, the overall telescope cost. Inputs Information on the material properties of candidate materials including E,ðrð,ðað,ð k, internal stresses (needed for evaluating warping from cutting), availability, size limitations, long term stability, polishability, and cost. ESO reports on the evaluation of aluminum. Impact on Other Tasks Material choice is closely related to segment fabrication technique, methods of coating segments, segment passive support, telescope structural design. Progress this Quarter The baseline material for the segments is Zerodur. We met with a representative of Hextek Corporation. They are eager to work with us to assess the possibility of Hextek supplying the mirror blanks for CELT. They make light-weighted (hexagonal cell interior with back and front face sheets) blanks of fused Schott borosilicate glass. The clear advantages of these blanks are their reduced mass (possibly allowing a lighter weight telescope structure) and a shorter thermal time constant. A number of important issues need to be explored in detail together with Hextek technical personnel. These include: the susceptibility to quilting during stressing for stressed mirror polishing, quilting due to pressure and thermal effects during polishing, quilting and other surface deformations induced by temperature changes and thermal gradients during testing and operations, the consequences of cutting after stressed mirror polishing, a design for the segment support system (and its thermal and gravitational characteristics), a design for incorporating edge sensors (and its thermal and gravitational characteristics), and others. A second general option for using Hextek blanks uses Reactive Atom Plasma Processing to create the final figure in a hexagonal blank. This process uses a traveling "torch" emitting a plasma of chemical species to chemically erode the blank in a controlled and deterministic process. The amount of erosion is controlled by 1) the concentration of the eroding species (usually CF4), 2) the distance of the torch from the glass surface, and 3) the dwell time. This process allows a large and well-controlled amount of material to be removed from a surface in a deterministic manner and holds the promise of revolutionizing optical polishing. The initial development work was made at LLNL; and beginning in December, 2001, the development will move to the commercial sector. Use of this figuring technique would remove from concern some of the issues associated with the Hextek blanks. Use is this technique would allow the creation of the complete aspheric figure without the need for stressed mirror polishing. We have not explored this quarter, as we had planned, the potential for using aluminum blanks. Plan for Future During the third quarter, we will work with Hextek personnel to define the potential for using Hextek blanks. We will define quantitatively the issues associated with using aluminum blanks. The soon to be completed error budgets will allow us to make a quantitative assessment of the viability of these blank materials. Task [ 7] Establish the segment fabrication vendor candidates Description Based on an initial definition of segment requirements we will discuss with all potential vendors the desired segment characteristics that they would be able to provide at minimum cost. This will require concentrated personal interactions with teams from each candidate vendor. Segment design and fabrication methods will be modified to find a low cost solution to segment fabrication. Objectives Definition of potential segment fabrication vendors and characterization of each in a fixed set of categories including experience, infrastructure, depth, etc. Definition of a baseline fabrication scenario in enough detail to serve as a basis for a credible cost estimate. Inputs Documentation of planetary-stressed-mirror-polishing methods and fixtures. Documentation of an in-process test option, including test error budget Documentation of an interferometric test option, including test error budget Initial progress on Task 2 Error budgets, Task 4 Optical Design, Task 5 Establish the segmentation geometry , and Task 6 Establish the segment material. Impact on Other Tasks This is a prerequisite for Task 8. Status We assume that the segments will be polished by planetary stressed mirror polishing as described in CELT Report No. 5. "Primary Mirror Segment Fabrication for CELT", Suitable vendors are needed. Progress this Quarter We visited Rayleigh Optical in Tucson. They are extremely interested in making the CELt segments, and showed a good understanding of the task. Jeff Carr described a revolutionary technique for polishing optics using Reactive Atom Plasma Polishing (RAP). Clearly still in its nascent stages, it has the potential for revolutionizing polishing by predictable removal of up to 1g/min. Contact with other optical firms was not made Plan for Future We plan to make initial contact with the rest of the candidates in the 3nd quarter, a delay of 3 months from our previous plan Task [ 8] Establish the segment fabrication cost Description Based on Tasks 5, 6, 7, 9 we will be able to establish an accurate estimate for all the processes required for segment fabrication. Interactions with candidate vendors will allow us to fine tune the processes and to generate a plausible cost estimate. Costs will come from vendor discussions and opinions. Objectives Determine a reasonable cost estimate for segment fabrication Inputs Design information, extensive vendor discussions and cost estimates. Impact on Other Tasks May influence the size of segments if the cost is size sensitive. This in turn will influence many other tasks. Status Current plans assume roughly $30K/m2 based on earlier discussions with vendors. Their rough estimate was $15K/m2. Progress this Quarter No significant activity Plan for Future In the 3rd quarter we plan to discuss with vendors the contents of the RFQ. We expect to include a stressing jig design, analysis of its performance, a prototype, and results of experiments with it. In the 4th quarter we will initiate detailed discussions with vendors. Task [ 9] Stressing fixture design, prototype and test Description We will design, build, and test a full-scale prototype stressing fixture. We will apply it to an aluminum segment, and measure the response, repeatability, and temperature and vibration sensitivities. If discussions with vendors show that this demonstration will have no significant impact on the cost estimates, then we can postpone the prototype and test phases. Objectives All candidate vendors have no experience with Stressed Mirror Polishing in a planetary polishing facility. Thus, this is likely to be a high cost-risk process for both CELT and the vendors. A detailed demonstration of the process will allow the vendors to make a credible estimate of the fabrication costs. Experience suggests that without such a demonstration all vendors will be required to provide very high cost estimates. Impact on Other Tasks The design (and perhaps the fabrications and tests) on Task 8 Establish the segment fabrication cost Status Some initial concepts for stressing fixture design are given in CELT Report No. 1 " Giant Optical Devices" Jerry Nelson and Terry Mast (Proceedings of the Backaskog Workshop of Extremely Large Telescopes, Anderson, T. ed, pp1-11, June 1999, Lund University and ESO) and in CELT Report No. 5. "Primary Mirror Segment Fabrication for CELT" Terry S. Mast, Jerry E. Nelson, and Gary Sommargren, (Proceedings of the SPIE, 4003, 2000) Progress this Quarter No significant activity Plan for Future We expect to complete CELT Report No. 11 by April 2001. We have also started work toward building and testing a half-scale prototype of the stressing fixture. Our goal is to design and test this prototype in the first six months of 2001. A suitable glass blank is available for our use at the Lick optical laboratory. Local surface deformations near to the force/moment lever attachment points will be measured using the 6-inch diameter beam of the Lick phase-measuring Zygo interferometer. The full aperture can be measured for a nominal fee using the LLNL 20-inch diameter Zygo. The stressing fixture engineering design will begin now with the hiring of a mechanical engineer at UCO/Lick. The construction and testing of a prototype will follow. Task [10] Define the segment figure tests Description For mechanical measurement of segment surfaces we will build and test a system and use it to measure the performance of the prototype stress fixture of Task 9. For optical tests of segment surfaces we have defined three possible options. For each option we will make a detailed optical test design, calculate the sensitivity to variations in all possible degrees of freedom and temperature changes. These will be used to construct segment testing error budgets and, if needed, revise the test designs. These and discussions with vendors will be used to establish cost budgets for segment testing. Objectives Document the process of selecting baseline options for testing the segments. These must include detailed error budgets that be communicated candidate vendors Impact on Other Tasks Significant input to Task 8 Establish the segment fabrication cost. Progress this Quarter An initial study of interferometric testing options is given in CELT Report No. 5 "Primary Mirror Segment Fabrication for CELT," Terry S. Mast, Jerry E. Nelson, and Gary Sommargren, Proceedings of the SPIE, 4003, 2000. Since the outermost segment surface surface will contain about 20 microns of astigmatism, the fringe density is expected to be high. Three options for reducing the fringe density were considered in the above paper: A Uses computer generated holograms, B Uses the test configuration geometry of the final segment use, C Uses a tilted lens to create a canceling astigmatic wavefront. The group at Livermore (under the direction of Gary Sommargren) has pursued the design of this test. They have considerable experience using a point diffraction test to measure X-ray optics surfaces to a precision of about 1 nanometer. They have worked on a detailed study of using phase shifting diffraction interferometry (PSDI) test to measure the segment surfaces, and they have submitted a nearly complete draft describing their test design. The proposed test is simple conceptually and can be used to measure all segments in the CELT primary. Based on their experience with the PSDI at LLNL, they have concluded that, although the fringe density directly from the segments is high, it is still low enough to be used without reduction. The proposed test has the following elements. • Laser ( lð = 532 nm) " Fiber to provide the diffracting aperture " Polarization beam splitter sends beams to interferometer reference and to converging lens " Converging lens This lens is used to reduce the size of the test from about 90m to about 7m so the test can fit on a single optical table. The lens is placed about 5 meters from the end of the fiber. Depending on the segment under test to distance from the lens to the segment is varied from 75 to 2515 mm. It's position is accurately controlled using a distance measuring interferometer. There are options for the design of this lens; singlet with asphere surface, triplet with spherical surfaces, condensor/compensator lens combination, etc. A study of cost, performance, tolerances needs to be made before selecting a design. • Camera / Imaging Lens A four-element camera was designed to image the surface on the detector (magnification ~ 1/74) and to minimize shearing effects and distortion. • CCD detector A camera used at LLNL for this type of test uses a 1024 x 1024 CCD. With that CCD the fringe density in testing the CELT segments directly would be close to, but not above, the Nyquist frequency, If necessary, it is certainly feasible to acquire or build a camera with more pixels. Critical issues in the test are 1. Differential optical path errors due to non-common path of the measurement and reference wavefronts for an aspheric segment. 2. Distortion of the local mirror coordinate system in the detector plane. 3. Magnification calibration They have addressed these issues both in the design and in proposed calibration procedures that use additional fixtures. 1. spherical test mirror (radius nominally = 91 meters). 2. distortion calibration grid 3. magnification calibration mask The Livermore group has written software to simulate the test; including segment surfaces, coordinate systems, measurement configuration, etc. No progress was made this quarter (at UCSC), as we had hoped, on the design of a mechanical (surface contact) system for measuring the segment surfaces. We want to design, build, and test a prototype 2-dimensional array of probes to measure a prototype surface. Plan for Future The next step in the evaluation of this test will be a complete test error budget. The plan for creating this budget does not yet exist, and CELT and LLNL personnel need to collaborate on this plan. The LLNL simulation software could be used to calculate sensitivities required for the error budget. Task [11] Design the segment passive support Description We will design a passive support for the mirror segments, compatible with the active support system of three actuators and consistent with the thermal and gravitational disturbances. This must include supporting the segment against gravity in any orientation, while maintaining surface errors consistent with the error budget. Objectives For a specified segment size and material, we will devise a passive support system. This will include adequate axial support and lateral support. The segment deflections under gravity in any orientation will be calculated, and the design will produce adequately small deflections. The interfaces will be carefully described. This includes attachment to the segments and connection to the active control system actuators and mirror cell lateral support system as needed. The design will also include tolerancing of the support to ensure production is economical. The assembly process will also be addressed for feasibility. Thermal effects will be carefully investigated to ensure that performance is adequate, both for thermal effects between assembly and operations, and during operations. Durability of the system during segment installation, segment handling, segment exchanges, telescope lifetime, mirror cleaning, and mirror coating will be evaluated. Inputs Task 5 segment design, Task 6 mirror material, thermal characteristics of the site. Impact on Other Tasks segment fabrication, mirror coating, Progress this Quarter The conceptual design work for the passive support is complete. Steve Gunnels did an excellent job and created a passive support system (axial & lateral) that is acceptable. He made a study of fabrication and assembly sensitivities that will be used to create the fabrication and assembly error budget. He also calculated the basic deformations required to predict the capability of a Keck style warping harness. He studied the segment deformations due to wind loads. The deformations will be quite small compared to rigid body motions on the elastic passive support system, as expected. He completed a detailed cost estimate for the cost of designing, building, and mounting on the segments the passive support system. The estimated cost per segment is $1100, quite a bit lower than our goal of $2000/segment. Steve calculated the natural deformation frequencies a segment on 3 actuators. The lowest frequency is ~ 350Hz. Plan for Future A plan for additional studies and prototype construction and testing needs to be established. Task [12] Develop algorithms to combine Displacement Sensor and Telescope-Control Wavefront Sensor (TCWS) readings Initial work on this task were described in Quarterly Report No.1. No additional activity has taken place this quarter. Task [13] Study the spatial frequency response of the primary mirror control Quarterly Report No.1 (CELT Report No 12) describes the progress made on matrix inversion time and condition number by Gary Chanan. This work was extended this quarter to include the specific character of the proposed CELT displacement sensors. The error multipliers for the first 30 singular value decomposition normal modes are listed below, and the first 50 modes are plotted in the figure below. These lower SVD modes correspond closely to Zernike deformations of the full primary mirror. The error multiplier is the ratio of the rms wavefront error to the rms sensor noise. M ºð Srms / sðs Chanan defines a dimensionless parameter, að s , to describe the ratio of the focus mode sensitivity to normal mode sensitivity and it depends on the details of the sensor design. ð ð ð ð ðaðs ðºð b2/(12 t g) where b is sense capacitor size, t = the radius of the actuator triangle, g = the sensor gap For a baseline segment / capacitor design (t = 255 mm, g = 2 mm) Gary considered three examples for aðs and calculated the following multipliers, M. The first mode corresponds to focus mode, or a Z20 deformation of the primary. This mode depends strongly on the assumed sensor geometry, and the multipliers for this mode are confirmed with a simple geometric derivation. ð ð ð ð ðaðs = 0.05 0.1 0.15 ð ð ð ð ð ðb ð ð= 17.5 mm 24.7 mm 30.3 mm ð ð ð ð ðLeff ð= 19.1 mm 38.1 mm 57.3 mm SVD mode M M M 1 24.656 12.694 8.764 2 8.774 8.198 7.541 3 8.774 8.198 7.541 4 3.908 3.656 3.360 5 3.761 3.531 3.252 6 3.287 3.014 2.685 7 3.287 3.014 2.685 8 2.296 2.145 1.964 9 2.296 2.145 1.964 10 1.780 1.657 1.500 11 1.780 1.657 1.500 12 1.551 1.444 1.317 13 1.550 1.444 1.317 14 1.550 1.442 1.305 15 1.149 1.067 0.972 16 1.117 1.051 0.963 17 1.094 1.020 0.930 18 1.045 0.986 0.906 19 1.032 0.964 0.876 20 1.032 0.964 0.876 21 0.851 0.792 0.722 22 0.851 0.792 0.722 23 0.780 0.732 0.670 24 0.780 0.732 0.670 25 0.744 0.697 0.634 26 0.744 0.697 0.634 27 0.665 0.618 0.563 28 0.665 0.618 0.563 29 0.623 0.585 0.535 30 0.572 0.541 0.499 rms of all 3240 modes 29.3 19.5 16.1 rms without mode #1 15.8 14.8 13.5 The figure below shows the multipliers for the first 50 modes. These multipliers for the rms surface error and similar multipliers for the rms image blur will be used in the creation of the error budgets. Task [14] Segment Displacement Sensors (design, prototype, test) Description This a potentially very expensive and complex item for CELT. About 6000 displacement sensors are required for segment stabilization. We will create an in-house design and also complete a thorough survey of commercially available devices. If no commercially suitable devices are available and affordable, we will prototype and test the in-house design. Objectives Complete a thorough survey of commercially available devices Create an in-house design. If no commercially suitable devices are available and affordable, prototype and test the in-house design Status Initial Sensors design concepts are given in CELT Report No. 6 "Segmented Mirror Control System Hardware for CELT", Terry S. Mast and Jerry E. Nelson (Proceedings of the SPIE, 4003, 2000). Progress this Quarter We have begun a program to understand the sources of the larger than expected noise in the Keck sensors. We have also outlined a three-stage program for the coming two quarters for prototyping and testing prototype displacement sensor designs. Kirk Gilmore made an initial trip to Keck Obsrevatory to learn about their existing sensor/actuator test stand in Waimea. Kirk will return (with Gary Chanan) to Keck to test for RF pickup in sensors at the summit in late March. Kirk has visited LBL and discussed the Keck sensors with Bob Minor. He acquired srawings of sensor and test electronics. For prototypes we will cut Zerodur blocks, coat them with gold to form the required capacitors, ground planes, and traces; construct or assemble electronics; design and construct a test stand; and test prototype sensors. All this will be carried out in the UCO/Lick shops and clean room. We are currently designing the initial capacitor layout and designing the test stand. A mechanical engineer at UCO/Lick is working on the design of a facility to make controlled moves of a prototype sensor in three degrees of freedom in step sizes of order 5 nm. We are also completing the theoretical sensor design with calculations of sensitivities to motions in all degrees of freedom and gravity and temperature sensitivities. Plan for Future We will pursue the above program for prototype sensors and plan to complete most of this program by the end of the fourth quarter. It is likely we will be able to borrow from Keck and LBNL much of the required electronics and software for the prototype testing, and that will greatly expedite this program. In addition, Bob Minor may be available to participate directly in the some the design and prototype activity. Task [15] Design Telescope-Control Wavefront Sensor (TCWS) hardware Description It will be highly desirable for CELT to have a Gemini- or VLT-style Telescope-Control Wavefront Sensor (TCWS) for monitoring the lowest ten to thirty spatial frequency modes of the primary mirror. The baseline assumption is that the TCWS will be a Shack-Hartmann-type camera in which the primary mirror is re-imaged onto a lenslet array, producing an array of stellar subimages (containing wavefront gradient information) on a CCD. The current task will determine the conceptual design parameters of the TCWS. Progress this Quarter Our initial effort on this task is to learn about wavefront sensors being used on large telescopes. Schoeck and Chanan researched the wavefront sensor for the Gemini telescopes. "The Gemini active optics wavefront sensors - guidelines for the CELT telescope-control wavefront sensor" (Schoeck and Chanan, October 2000), CELT Technical Note No 2. Plan for Future We plan to make a similar study of the VLT wavefront sensor and write a note describing the design issues and candidates designs for the TCWS. Task [16] Segment support actuators (design, select, test) Description The segment support actuators are potentially very expensive and complex. About 3300 segment actuators are required. We will make a thorough survey of the availability and cost of commercial actuators. We will design a lever-actuator system in order to expand the range of applicable commercial actuators. Every effort will be made to define the actuator requirements to minimize the costs: acquisition, fabrication, and maintenance. Robustness of candidate actuators will be tested, since the active control system has zero redundancy for actuator failure. Objectives Develop or acquire an adequate displacement sensor Status Quarterly Report No.,1 described the actuator requirements and gave many details of the survey by Alan Schier (The Pilot Group, 3130 Foothill Blvd., Unit 1, La Crescenta, CA 91214, (818)790-7481). At the end of this quarter, Alan submitted a substantial and detailed final report summarizing his survey of many types of actuators and many vendors. After collecting the data and comparing a very large range of potential candidates, he identified six candidates that are likely to meet the CELT requirements and meet a cost goal of less than $2000. Progress this Quarter We give a very abbreviated description here; mostly for identification purposes. Alan's report gives many details and thoughts about what we might do in the future to pursue these candidates Two of these (#1 and #3) use a motion reducer to provide the small resolution (< 4 nm) using commercial actuators. 1. Conventional Lever (Motorized Micrometer and Flexured Lever) Proposed by: CSEM (Swiss Center of Electro-Mechanics) Description: Off-the-shelf motorized micrometer drives a conventional lever (with a flexural pivot). Micrometer (Physik Instrumente M-230.25) screw and nut driven by a gearhead and DC motor. A control loop around a motor mounted encoder ð ð ð ðÞð minimum commanded move at micrometer tip of 50 nm. Outstanding issues: cost, backlash, life 2. High Resolution Micrometer Proposed by: Diamond Motion Description: Motorized micrometer with high ratio internal gearhead. Stepper motor, micrometer screw, gearhead (> 10,000 : 1) Pushes against a ruby pad (since micrometer rotates) Outstanding issues: power, backlash, windup, life, reliability 3. Elastic Lever Proposed by: The Pilot Group Description: .Relatively coarse actuator with position feedback drives a flexural motion reducer through a cable drive. Motion reducer: 2 beams at 90 degrees; 1st converts motion at one end to a moment at the other, 2nd converts the moment to a small motion at the same end (other end is fixed) Outstanding issues: detailed design not made, mass, cost, life 4. Voice-Coil Actuator Proposed by: Blue Line Engineering Description: Voice coil actuator with position feedback around the output. Diaphragm flexures to support the output shaft, Eddy-current sensor provides resolution over full range. Force is off-loaded using air pressure and small control valves. Outstanding issues: need to air pressure, sensitivity of position sensor to pressure, 5. Magnetostrictive Inchworm Proposed by: Etrema Products Description: Inchworm using magneto-strictive materials and a lever mechanism to reduce the output. Outstanding issues: design not made, transient motions created by application and release of brake, power 6. High- Capacity Inchworm Proposed by: Greg Carman Description: Piezo electric inchworm with grooved brake pads to achieve desired axial load capacity. Outstanding issues: Uncertainty in when grooves are aligned for braking. Transient motions induced by application and release of brake. cost Plan for Future We are holding a CELT actuator workshop on March 8 in Santa Cruz where the above and other candidate actuators will be discussed. At this writing we expect about a dozen attendees including Alan. We will select two or three candidates to pursue; fund their further development, and acquire prototypes for testing. Task [17] Design camera required to determine desired sensor readings At the Keck telescopes, the desired sensor readings are determined by a Shack-Hartmann camera, known as the Phasing Camera System (PCS). In addition to this task, which can alternatively be thought of as aligning the segments in piston and tip/tilt, PCS can also zoom in on individual segments (or groups of seven segments) to determine the segment surface figures which are needed for warping harness adjustments. Although there exist other techniques which can in principle accomplish these tasks (e.g. curvature sensing, the Gerchberg- Saxton algorithm, phase diversity), PCS has the distinct virtue that it has been successfully proved on a large segmented telescope. While we are investigating some alternative techniques in the context of CELT alignment issues, here we explore the issues involved in scaling up Keck PCS to a CELT PCS. In Quarterly Report No.1 we reported some initial considerations of 1) Tip/Tilt Alignment, 2) Phasing, 3) and Segment Figure Measurements. No further progress was made on this task this quarter. Additional Telescope Design Activities CELT Diffraction Point Spread Functions In the last quarter we wrote code to evaluate the diffraction consequences (in mono-chromatic light) of various CELT segmentation geometries, segment alignment and figure errors, and secondary mirror support structures. The code supports: o segment piston errors o segment tip/tilt errors o segment second order wavefront errors o global focus errors o rudimentary secondary support structures o seeing (in the long term exposure limit only) To allow better image plane resolution we have now extended the FFT array from 1K x 1K to 8K by 8K. Task [18] Define secondary and tertiary physical & performance parameters Description The secondary mirror or mirrors is a fundamental part of the telescope design. We will assess the need for multiple secondaries, and what their desired optical properties are. We will assess the impact of secondary size on science performance. We will study the tertiary mirror requirements. We will also investigate field rotation issues and conceptual design options for addressing them. Objectives We will produce optical designs for two secondaries, one rigid for optical and near IR applications, a second one for an adaptive secondary. Surface and alignment specifications will be produced, and a weight estimate for each, including the entire support system. A cost estimate will be produced. Inputs The secondaries are fundamentally related to the primary and final f-ratios, as well as the location of the final focus. The design of the AO systems is also closely related. Size, location, weight, position tolerances will drive the structural design of the telescope. Progress this Quarter As a result of the review of the requirements, the secondary has been changed to deliver unvignetted images over a 20 arcminute FOV. This increases the size of the secondary from 3.64m to 3.87m. There is continuing interest in having an adaptive secondary that is interchangeable with the f/15 secondary. This is likely a 1-meter class mirror with roughly 500 actuators. No further details are available. Plan for Future In the next quarter we will generate a strawman support and contact Raytheon (who is fabricating the SOAR primary) for technical comments and a cost estimate. Task [19] Develop Algorithms for TCWS control of primary, secondary, & guiding Description The Telescope Control Wavefront Sensor (TCWS) will provide information required for the active control of each primary-mirror segment’s tip, tilt, and piston degrees of freedom. It will also provide low bandwidth information about the primary mirror as a whole, position and orientation of the secondary mirror, and the telescope guiding. We expect that a TCWS will be located at each instrument or each focus. Objectives The equations describing all the optical consequences of these degrees of freedom will be derived. The interaction of the degrees of freedom and the expected bandwidths for their control will be described. A baseline control algorithm and process will be created. The possible interaction of this control with the adaptive optics control system will be studied. Inputs Telescope optical design Impact on Other Tasks Possible impact on the design of the TCWS. Schedule This will begin once the telescope optical design is selected and be completed after the requirements for the TCWS have been defined. Status As planned, this task is yet to begin. Progress this Quarter None. Work on this task continues to be postponed until the error budgets (Task 2) are completed. (Completion of Task 2 planned for mid April.) Plan for Future Toward the end of the third quarter we will describe analytically the optical consequences of errors in all six degrees of freedom of the primary, secondary and tertiary. The telescope error budget (Task 2) will be used to set tolerances on all these degrees of freedom, as well as the required control bandwidths. Requirements will be derived for the Telescope Wavefront Sensor measurements for global control. Task [20] Design the Telescope Structure Description We will produce a conceptual design of the telescope that satisfies the constraints of primary mirror and final f-ratio. The location of foci, size of science instruments, support of segments, handling of segments, support and handling of the secondary, rapid exchange of the secondary, cleaning of the mirrors, repair of key active components including replacement of actuators will also be considered in the design. Methods for periodically CO2 cleaning the mirror will be described. A method for aligning the segments in all 6 degrees of freedom will be addressed. Objectives Produce a design that is compatible with all the physical and geometric constraints. The stiffness and natural frequencies will be determined, particularly the lowest modes that influence image location and quality. The possible effects of wind loads will be included in the design choices. The design will be compatible with plausible drive, bearing, and encoder systems. The support and exchange of secondary mirrors will be described. Progress this Quarter Steve Medwadowski is working on the design of the mirror cell and cradle structure, and its support of the upper tube. This is proving to be a complex and difficult task. A tripod, a tetrapod, and a Keck-like top end are being analyzed. One problem is that the “natural” center of mass is below that of the proposed elevation axis at 4 meters. The natural center of gravity is 1-2 meters below this. In additional bending of the tripod/tetrapod legs is also adversely affecting the motion of secondary (horizon pointing). This may require additional cable stiffeners, and these are not yet designed. Tuning of the cradle has reduced the total mass very significantly. It is now approximately 500 tons. Results of his analysis are expected early in the third quarter. Plan for Future When we receive Steve's report we will list the major concerns. Then, based on money and time limitations, we will decide when to proceed with additional design work. Task [21] Generate strawman designs of the bearings, drives, encoders Description A conceptual design of the telescope elevation and azimuth bearings, the elevation and azimuth drives, and the elevation and azimuth encoders will be generated. Attention will be given to meeting the requirements, and providing a cost effective design. Design alternates will also be given, so options are understood. Objectives We will develop suitable designs for all 6 systems and describe their performance. The influence of wind will be given. Alternative designs will be sketched, to provide a start for a more detailed evaluation later in the project. Inputs The telescope structure will define the design requirements. Progress this Quarter A contract with Vertex/RSI is signed, and they are about to start work on the conceptual design of the telescope bearing, encoders, and drives.. Task [22] Identify the candidate AO modes and define requirements for each mode Description Based on the science requirements and potential technologies, systematically identify a set of candidate AO modes. Define the system-level requirements for each mode. Progress Quarterly Report No. 1 describes many of the issues in this task. The progress during this quarter is not reported yet. Task [23] Develop first order error budgets for adaptive optics (AO) modes Description Enumerate, evaluate, and balance error budget terms for the wavefront control performance of CELT. This includes participation in Task 1 error budgets for the entire observatory. Describe error budgets in terms traceable to component-level specification (i.e. rms nm of wavefront error). Progress Quarterly Report No. 1 describes many of the issues in this task. The progress during this quarter is not reported yet. Task [24] Develop conceptual AO system optical designs for each AO mode Description Develop a conceptual optical design for each AO mode for CELT. Objectives Identify key optical technology drivers, as well as any drivers in the telescope structural or configurational design (i.e., number or type of foci and secondary mirrors). Identify potential vendors and/or partners. Evaluate the state-of-the-art of AO component fabrication. Estimate the scope of any technology development programs necessary to realize the conceptual designs and estimate its cost. Provide alternatives for different cost points and describe the technical tradeoffs between these alternatives in terms of error budgets. Progress Quarterly Report No. 1 describes many of the issues in this task. The progress during this quarter is not reported yet. Task [25] Prepare for Conceptual Design Review Description All results of this phase will be collected and presented at a Conceptual Design Review (CoDR). At this review, the conceptual design of the telescope, AO, and instrument subsystems should be presented, as well as an update on site selection. A key component of the review will be to understand the level of effort necessary for the Preliminary Design phase, which will address many details not addressed by the Conceptual Design phase. Inputs All results from this phase Schedule This task will not begin until close to the end of this phase and will not be completed until after the Conceptual Design Review. Progress this Quarter None Plan for Future This work will be begun in the last quarter Task [26] Write the Preliminary Design development plan. Description We wish to develop the plan for the next phase of work, the preliminary design phase. This will consist of a description of the key tasks, the method for carrying them out, the likely budget and the schedule. Tasks will include more detailed descriptions than the conceptual design, resolution of issued raised in the conceptual design review, progress on key issues that were not undertaken in the conceptual design. Schedule This task will not begin until the final month of this phase. Task [27] Support the CELT Working Groups Description The CELT working groups need some funds to operate; travel to meetings, small studies, etc. This task provides those funds. Other Participants CELT working groups, including Steering Committee, Telescope, Science, Instruments, Adaptive optics, Site Progress this Quarter Working group activities are generally being reported separately. The Telescope and AO progress is included in this document. A substantial report (6 March 2001) by the Instrument Working Group is attached as a separate file. Task [28] Manage the Conceptual Design phase program Description The management of the phase 1 Development program will be begin with the definition of detailed tasks, schedules and milestones. These schedules and milestones will be regularly tracked during the program and updated in response to changing requirements and to changes in the cost-risk assessments. We will also define cost codes corresponding to all aspects of the program and track them against the approved budgets. When required, consultants and suppliers will be contracted for portions of the program. Budget and schedule summaries will be produced quarterly. Objectives Manage the conceptual design to a successful conclusion. This means a sound design will be developed, budget will be met, and schedule will be met. Also, preparation for the next phase will be completed. Progress this Quarter We currently have three contracts with consultants for work on CELT. Paragon Engineering (Steve Gunnels) has been contracted to carry out the conceptual study of the primary mirror segment support. The Pilot Group (Alan Schier) was contracted to carry out the conceptual study of the primary mirror actuators, and Steve Medwadowski was contracted to carry out a study of the telescope structure. We expect these studies to be completed in the early part of 2001. Plan for Future We are planning to contract at least three additional studies in the next few months; a conceptual study of bearing, encoders and drives; a conceptual study of segment displacement sensors; and a conceptual study of one particular type of primary mirror actuator. These contracts will likely be let by the end of the year or early next year. Task [29] Manage the CELT Website Description The CELT website is both a description of the project to the world and an internal communications tool. Objectives We will upgrade and maintain the CELT website, so that it announces all project activities, provides an archive for reports describing the results of all tasks, and educates the public about the nature and status of the project. Status The CELT web pages are hosted at www.ucolick.org/~CELT and there are links to the site at The Caltech astronomy site www.astro.caltech.edu/ and a major existing telescopes site www.seds.org/billa/bigeyes.html Progress this Quarter We have completely revised the organization and appearance of the website. It now includes the general categories of Institutions, Working Groups, Individuals, Calendar, Reports and Notes, and Presentations; as well as some artist concept renderings of the telescope. The Reports and Notes category contain the full text of CELT reports and technical notes. The Presentations category contains, when available, presentations made at internal meetings. This site is providing both an internal record and a description to the world of the CELT personnel, activities, and progress. Plan for Future The website will be updated regularly as additional reports, technical notes, and presentations are created. If resources are available, we will add a section giving the scientific and technical motivation for CELT that is specifically directed to the public at large. Task [30] Contingency management Status $128K is being held as contingency Progress this Quarter The contingency has not changed, but it seems likely that we will need to allocate some additional resources for actuator work and for telescope design work. 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