ING Instrumentation Working Group ================================= Minutes of the 4th meeting held Mon 23 October 2000 --------------------------------------------------- Location: Astrophysics Group Department of Physics University of Oxford, UK Time: 10.00 - 17.15 Present: Dr Richard G McMahon (Chair) (RGM) Dr Gavin B Dalton (GBD) Dr Vikram S Dhillon (VSD) Dr Simon F Green (SFG) Prof Konrad Kuijken (KK) Dr Ramon Garcia Lopez (RGL) Dr Nicholas A Walton (Secretary) (NAW) In Attendance: Dr Richard G Bingham (OSL/UCL) (RGB) Dr James R Lewis (CASU/IoA) (JRL) Dr Richard M Myers (Durham) (RMM) Papers: these were distributed at the meeting a. Agenda for 23 Oct 2000 meeting b. Action items outstanding from previous IWG's c. Draft minutes from the 5 May 2000 meeting d. Contribution from RGL comparing LIRIS, UIST, ISAAC iwg10-00-liris.ps These and the following overheads are available on the ING IWG WWW pages at http://zwolle.ing-slo.iac.es/IWG/Meetings/Internal e. View graphs from NAW over viewing current ING instrumentation (gzipped ps file) iwg10-00-naw.ps f. View graphs from RGB concerning the coronograph iwg10-00-coron.ps g. View graphs from RMM about NAOMI iwg10-00-naomi.ppt (powerpoint) h. View graphs from RMM about TEIFU iwg10-00-teifu.ppt (powerpoint) i. View graphs from JRL about pipeline data issues iwg10-00-pipe.ps Abbreviations and Glossary: 2dF The 2deg prime focus fibre fed multi-object spectrograph capability on the AAT AAT 3.9-m Anglo Australian Telescope ALFA The LGS AO system on the 3.6-m Calar Alto telescope AO Adaptive Optics CFHT 3.6-m Canada France Hawaii Telescope ELECTRA The Durham multi segment mirror AO system - this will form the heart of NAOMI ESO European Southern Observatory FOV Field of View LGS Laser Guide Star IFU Integral Field Unit INGB Isaac Newton Group Board INGRID a near IR 1kx1k camera for the WHT INT 2.5-m Isaac Newton Telescope LIRIS a near IR spectrograph being built by the IAC for the 4.2-m WHT NAOMI The optical/IR AO system for the WHT PSF The point spread function TAURUS The Fabry-Perot imaging spectrograph, mounted at the Cassegrain focus of the WHT TEIFU Thousand Element Integral Field Unit - an IFU to feed WYFFOS TTF TAURUS tunable filter (for low spectral resolution, wide field imaging) UES The WHT's Utrecht Echelle Spectrograph UKIRT 3.8-m UK Infra Red Telescope UltraDAS The ING's new Data Acquisition System VLT ESO's 4x8-m Very Large Telescope WHT 4.2-m William Herschel Telescope WYFFOS The WHT's Nasmyth mounted, fibre fed, spectrograph IWG materials on-line (p/w protected) at: http://zwolle.ing-slo.iac.es/IWG/Meetings/Internal/ INTRODUCTION 1. Introduction: welcome to Ramon Garcia Lopez who is standing in for Santiago Arribas (SAM). 1.1 RGM noted that RGB, JRL and RMM were in attendance to provide input into the discussions on Coronograph (RGB) and NAOMI (RMM) developments at the ING and Data Reduction Pipeline issues (JRL). MATTERS ARISING 2. NAW reported on the action points from the previous IWG meetings. 2.1 Matters arising from meeting of May 5 2000: 2.1.1 [IWG5-00/2.3] NAW reported that the availability on the ING web pages of engineering information of interest to observers and visiting astronomers was being continuously improved. Examples included detector information, and information concerning tracking performance of the telescopes etc. NAW stated, that after discussion with ING engineers, it was though appropriate to not place the complete detailed engineering information resources of the ING on-line. External users who might need this would be asked to contact with appropriate staff at the ING. This would ensure access to relevant information. The IWG AGREED with this policy. [ACTION: NAW - CLOSED] 2.1.2 [IWG5-00/2.4] NAW noted that announcements from the ING were distributed using the ING's own extensive email exploder and also via the ING Majordomo mailing list. There was no intention to make use of the PPARC Astronews mailing list, as this could cause confusion as to the origin of the news. Further, it would lead to many users receiving unwanted duplicates of messages. However, NAW reported that in future, short messages announcing new issues of the ING Newsletter would be circulated via Astronews. [ACTION: NAW - CLOSED] RGM noted that in the recent redesign of the ING WWW pages, that the item indicating how to subscribe/unsubscribe to the ING Majordomo mailing list was no longer prominently displayed on the ING home page. He felt it important that this information should be readily accessible. [IWG10-00/2.1.2 ACTION: NAW] Investigate how to better locate information about how to subscribe to the ING mailing list on the ING WWW pages. 2.1.3 [IWG5-00/5.5.1] RGL attached a brief overview of the capabilities of LIRIS (WHT) compared with UIST (UKIRT) and ISAAC (VLT) (iwg10-00.liris.ps). The unique features of LIRIS were multi-object spectroscopy and a coronography option. It was noted that the slit width assumed for ISAAC (1 arcsec) might be somewhat pessimistic when calculating the exposure times. [ACTION: NAW/SAM - CLOSED] 2.1.4 [IWG5-00/5.5.2] NAW reported that no formal agreement had been reached by the ING and the IAC as to the status of LIRIS. Currently it is an 'own user' instrument. RGL commented that the IAC were keen to conclude negotiations with the hope that 'common user' status could be agreed. The IAC would be contacting Rene Rutten soon. [ACTION: NAW - ONGOING] 2.1.4.1 RGL gave a brief report on the construction status of LIRIS. Fabrication is complete 02/2001. The engineering detector is now being tested, the science detector will be delivered 01/2001. The first instrument cool down is foreseen for 04/2001. First commissioning will now take place on the WHT 12/2001 (c.f. [IWG5-00/5.5]) . The LIRIS team plan that commissioning will be complete by 06/2002 with first science use probably in Semester 2002B (from 08/2002). NAW asked whether LIRIS could be used with the GTC. [IWG10-00/2.1.2 ACTION: RGL] Report on use of LIRIS with GTC 2.1.4.2 RGL asked the IWG to indicate support for LIRIS. RGM noted that the LIRIS needed to viewed in the context of the current ING instrumentation programme and also against the IR instrumentation available, both on La Palma (e.g. at the TNG) and to the UK and NL communities elsewhere (e.g. Gemini and VLT). SFG thought that the ING should be careful not to duplicate instrumentation currently available at other UK facilities (e.g. UKIRT). VSD asked if the NL community saw a need for IR spectroscopy on a 4-m telescope. KK though that the MOS option would be of most interest, as to be available over wider fields with VLT+NIRMOS. GBD speculated that LIRIS+WHT could have a 4 year useful window from now before Gemini IR spectroscopy become established. Therefore the time-scales of deployment for LIRIS were important, delays to it could be critical. Summing up, RGM thought that the IWG could offer cautious support to LIRIS. However, it was considered necessary to re-visit this issue at the next IWG, comparing LIRIS with future 8-m and WHT instrumentation capabilities. [IWG10-00/2.1.4.2 ACTION: RGL/NAW] To overview LIRIS capabilities in the context of the ING instrumentation plan, and other relevant telescope capabilities. 2.1.5 [IWG 5-00/5.5.3] NAW reported that he had received information from SAM stating that the design of LIRIS was fixed such that it was unlikely that it could be feed from IR-TEIFU. RMM stated that this was probably correct, especially as LIRIS uses only a 1kx1k detector. [ACTION: SAM - CLOSED] [ http://www.iac.es/proyect/LIRIS ] 2.1.6 [IWG5-00/8.1.2] NAW reported that the old INT prime focus unit had been given to the Greek National Observatory. They had funded a ING technician to aid in it's installation. The ING would always be willing to listen to requests for it's old and decommissioned instrumentation. [ACTION: NAW - CLOSED] 2.1.7 [IWG5-00/8.2.4] NAW stated that he was generating comparisons of instrumental capabilities of ING's existing, in construction and proposed instrumentation. A draft would be made available before the next meeting. He also advised the IWG that existing capabilities were summarised at: www.ing.iac.es//Astronomy/instruments/instruments.html [ACTION: NAW - ONGOING] 2.1.8 [IWG5-00/3.1.4] NAW indicated that John Telting (ING's AF2 Project Scientist) will be contacting the AAO to exchange information concerning fibre manufacturing and testing procedures. [ACTION: NAW - CLOSED] 2.1.9 [IWG5-00/3.1.5] The science and technical inputs that were sent to RGB for his preliminary design work by the ING AF2 project scientist are located on the IWG WWW pages as iwg-10-00-2.1.9.ps. [ACTION: NAW - CLOSED] 2.1.10 [IWG5-00/3.1.6] NAW reported that the science requirements document for AF2/WYFFOS as a basis for decision making on future development in this area (especially for dIFUs and near-IR AF2 fibres) were currently being developed. [ACTION: NAW - ONGOING] 2.1.11 [IWG5-00/3.2.6] NAW indicated that the investigation of options for the development for IR-TEIFU were currently progressing. RMM discussed this further later in the meeting. [ACTION: NAW - ONGOING] 2.1.12 [IWG5-00/3.3.4] The IWG agreed that the Coronograph design with a 5 arcsec radius field of view was acceptable. [ACTION: IWG - CLOSED] 2.1.13 [IWG5-00/3.4.1] RGM indicated that both eh and NAW had received a full copy of the Chris Dainty lead JIF Laser Guide Star proposal. NAW would contact Chris Dainty, and if okay, would distribute copies of the executive summary to all IWG members and those persons who had written in support of the bid. [ACTION: NAW - ONGOING] [IWG5-00/11.1 ACTION: NAW/RGM] Confirmation of this meeting was done. [ACTION: NAW/RGM - CLOSED] 2.2 Matters arising from meeting of November 1 1999: 2.2.1 [IWG11-99/6] NAW reported that the complete manuscript had been reviewed by the New Astronomy Review editor and was now in the final publication stage. It was hoped that it would be in press before the end of the 2000. [ACTION: NAW - CLOSED] 2.2.2 [IWG11-99/10.2.1] The IWG was invited by NAW to comment on the WWW pages now available at http://zwolle.ing-slo.iac.es/IWG/ The passwords and user-names for the IWG internal pages had been distributed. RGM thought that the pages were clearly presented and looked forward to their continued expansion. The IWG AGREED that by default, any material submitted to NAW at IWG meetings would be made available on the IWG WWW pages in the password protected area. [ACTION: NAW - CLOSED] 2.2.3 [IWG11-99/10.2.2] NAW and RGM would aim to prepare an article for the next ING Bulletin giving an overview of current and proposed ING developments and enhancements to the community. [ACTION: NAW/RGM - ONGOING] 2.2.4 [IWG11-99/10.2.3] All approved IWG minutes are now available in the public areas of the IWG WWW pages. Draft minutes are located in the password protected area. [ACTION: NAW - CLOSED] 2.2.5 [IWG11-99/6] All the papers (in preprint form) presented at the ING Sheffield Conference (Apr 1999) have been placed on line at: http://zwolle.ing-slo.iac.es/IWG/Conf/sheffield.papers.html [ACTION: NAW - CLOSED] 2.3 Matters arising from meeting of April 6 1999 2.3.1 [IWG4-99/1.26] NAW and RMM reported that the status of UK access to Durham's TEIFU was still unclear. This was further discussed later in the meeting. More detailed negotiations between the ING and Durham are required. [ACTION: RGMR - ONGOING] 2.3.2 [IWG4-99/1.27] NAW discussed developments concerning the possibility of an AO feed to UES. This could occur in the context of the MOSAIC development. Removing FOS-II from under ISIS allows sufficient space for UES to be placed on the rotating floor under the Cassegrain focus. The fibre feed length from Nasymth is then quite short at ~10m. UES would be placed on rails to be moved into and out of position. Whilst in storage it would be located on a new roof near the door to the WHT control room. RGB thought that some UES components protruded into the current optical bench, this might need to be considered. RGL indicated that when using fibres to feed UES, their UV performance would need to be considered. He stated that he had recent data from a number of fibre manufacturers and would pass this to NAW. [IWG10-00/2.3.2 ACTION: RGL] provide information on fibre performance information to NAW. KK noted that moving UES avoided the question of whether it should be decommissioned or not. The IWG agreed that the next meeting should attempt to prioritise the WHT instrumentation suite. (see later action [IWG10-00/8.5] [ACTION: NAW - CLOSED] 2.4 The minutes of May 5 2000 (draft version dated 21 Oct 2000) were read and accepted. UPDATE ON CURRENT ING AO INSTRUMENTATION DEVELOPMENTS 3. The IWG received reports on the major AO initiatives currently in progress, funded or planned at the ING. NAOMI 3.1 RMM presented an extensive presentation concerning the recent NAOMI commissioning runs. He discussed current status and issues arising from the commissioning runs. (The overheads are available on the IWG WWW site as iwg10-00-naomi.ppt) 3.1.1 NAOMI is a high order AO system with a segmented mirror offering 228 degrees of freedom. Commissioning occurred on the WHT in August and September 2000. RMM noted that this had been ambitious schedule, with the ING pushing for the early deployment of NAOMI for scientific and operational reasons. 3.1.2 The performance of NAOMI was discussed. Diffraction limited images were obtained in K (~0.12 arcsec FWHM on the WHT). Short integration images were shown of the PN BD+30 3639. The spatial detail was comparable with images from the HST. 3.1.3 Of note was that the PSF across the full NAOMI INGRID field (~40 arcsec diameter) was stable - as measured from stars offset from the core of BD+30. 3.1.4 Hardware issues: before the commissioning the Zeiss fast steering mirror (FSM) failed, and hence the Aug/Sep runs utilised the spare, less functional, Durham FSM (this limited J band system performance). The Ziess FSM is expected to be repaired and ready for the Dec/Jan 2000/2001 science runs. A calibration lamp cover failed which is now being re-designed. 3.1.5 Software issues: the high level GUI for use by visiting observers to control NAOMI is still under development. RMM stated that he will be on La Palma from 24/11/2000 till after the Dec/Jan science runs to complete this package. He indicated that a small amount of sky time would be needed to test this - perhaps in mid December 2000. Some work was occurring at the UK ATC to fix EPICS control s/w problems which occasionally led to motor stalls. Logging of the seeing and WFS data did not occur during night time operation. Due to a memory leak this caused the guiding system to fail. This facility is being repaired for future runs. 3.1.6 Performance issues: the low light level modes not commissioned, e.g. 4x4 binning on the WFS. This reduces the delivered strehl ratio, but gives more light (1.5 mag) and allows fainter guide stars to be used. This mode is only of use in the H and K bands due to performance limitations, at J the loss in strehl is unacceptable. This mode was De-scoped from the Aug/Sep 2000 commissioning but will be reinstated in Dec 2000. RMM noted that instrumental throughputs needed to be obtained in good stable conditions, Insufficient data had been obtained so far on sky. There was so far insufficient data on system emissivity performance. This would be addressed in Dec 2000. 3.1.7 The throughput to the Wave Front Sensor (WFS-AO) where up to a magnitude shortfall (could be less as the prediction depends on the natural seeing, which was not good at this time) was noted was the main area of concern. Areas for improving this include: - commissioning the low light level modes (gains > 1.5 mag), - re-alluminise the tertiary mirror (currently at 82%) - remove the glass windows in the derotator - replace the 830nm cutoff dichroic with one at ~1um (~20% gain) [IWG10-00/3.1.7 ACTION: NAW] To report these areas of improvement to ING NAOMI engineering and scientific staff (RGT and CRB) RMM stated that the effective limiting WFS guide star that could be used during the Aug/Sep 2000 commissioning run was V ~13 mag (c.f. the V ~14 mag expected). In discussing the tertiary coating, RGB noted that, at a recent visit to REOSC in France, he was shown over-coated silver surfaces which suffered very little reflectivity loss with time. KK inquired why some of the images shown appeared to have asymmetric PSF's. RMM noted that these were initial images, and after system tuning, the PSF's were symmetric. RMM did note however that there was evidence for some very low level ghosting when an out of field bright guide star was being used, this was to be investigated. 3.1.8 Telescope performance issues: RMM stated that it was vital that the telescope was operating optimally, especially when implementing AO systems in the visible wavebands. He noted that the ING (especially Chris Benn, Kevin Dee and Cliev Jackman) had made great progress in reducing the glitches seen in the WHT tracking. The current main oscillation is a saw tooth one only affecting the Nasymth focus. 3.1.9 Integration with INGRID: NAW noted that the commissioning of NAOMI had employed INGRID as the science detector, this running the new IR-UltraDAS system - new ING developed instrumentation and control systems recently successfully deployed on the WHT. RMM stated that the NAOMI team had received excellent support from ING staff in this area. VSD asked about the effect of the surface irregularities found on the INGRID filter set (see [IWG5/00-5.1]). NAW reported that after visual inspection, and testing, the effect on the AO wavefront was found to be negligible. 3.1.9 Development issues: RMM highlighted two important developments. - as part of the OASIS project (see [3.2]) the optical science port is being redesigned to become the universal science (IR + optical) science port. The core of this will be a range of dichroics enabling a light of interest to be diverted to the science instrumentation, with the rest being transmitted to the WFS. This opens the possibility to improve on the amount of light to the WFS (see [3.1.7] - NAOMI's turbulence conjugation upgrade path could be implemented. This opens the possibility to obtain guide stars over an increased (x2) field. This is of maximum importance if the is no LGS available. It could be implemented quickly (in 2001). VSD thought that this would be an important development to pursue. [IWG10-00/3.1.9 ACTION: RGM/IWG] The IWG AGREED to recommend re-scoping NAOMI to include the turbulence conjugation upgrade path. RGM to pass this recommendation to Rene Rutten. 3.1.10 Other issues: RGM inquired as to the new performance measures that would be needed with NAOMI, and whether visiting astronomers would be able to tell the state of the instrument. KK assumed that the ING would develop and maintain performance indicators for NAOMI as for their other instrumentation. VSD was concerned as to how the hand over of NAOMI to the ING was proceeding. RMM indicated that progress was good, the ING had already successfully dismantled and re-assembled NAOMI. The high level control GUI s/w was being developed partly by ING s/w engineers. The main area to clarify was long term support of the WFS/AO correction real time s/w. [IWG10-00/3.1.10A ACTION: NAW] To report the IWG's concern that the proper implementation of the handover of NAOMI to the ING was vital and to report back to the next IWG. RGM stated that a comprehensive user guide for AO users is required before next Mar 2001 telescope application deadline. This will help in increasing the usage of NAOMI. [IWG10-00/3.1.10B ACTION: NAW] To stress that the delivery of full documentation is needed. 3.1.11 Scheduling issues were addressed. VSD noted that NAOMI, and AO systems in general, deliver optimum gains when the natural seeing conditions are median or better. Scheduling issues therefore become important, classical PATT type scheduling of AO programmes would not be effective. RGM suggested a possible model involving scheduling AO programmes in blocks, leaving a few nights free for contingency. The AO programmes would be carried out during this block during median or better seeing. During poorer conditions simple backup programmes with other instrumentation (e.g. ISIS) would be carried out in queue mode. The IWG AGREED that a more detailed model or range of models should be developed and resource implications considered. [IWG10-00/3.1.11 ACTION: RGM/NAW] Recommend to Rene Rutten that models for scheduling AO programmes be developed and a discussion initiated by the time allocations panels (PATT, NLTAC, CAT). [ NAOMI @ http://www.ing.iac.es/~crb/wht/ao.html ] [ INGRID @ http://www.ing.iac.es/IR/INGRID ] OASIS 3.2 OASIS: NAW informed the IWG that the NL's NWO/GBE have approved the Dfl 720K funding bid (PI: Thijs van der Hulst) to bring OASIS to the WHT. 3.2.1 In the coming year, the ING will redesign the optical science port of NAOMI such that it becomes a universal IR/optical science port. A selection of dichroics will enable a range of light to be diverted to the science instrumentation. 3.2.2 Initial design work is underway with the expectation that OASIS will be operational on the WHT in ~2 years. AO CORONOGRAPH 3.3 RGB gave a brief update on the current design for the AO Coronograph (with input from the PI: Peter Doel). (Overheads are available at iwg10-00-coron.ps) The design incorporates a compact unit with the possibility of a range of occulting disks and a rotating Lyot stop (matched to the WHT's primary support vanes). [IWG10-00/3.3 ACTION: NAW] Pass RGB information on which wavebands will be required for the science port. 3.3.1 RGB presented a preliminary design for a ADC, which is required for OASIS required for oasis. This would be located before the Coronograph unit. [IWG10-00/3.3.1 ACTION: NAW] Discuss with ING staff the ADC options. MOSIAC 3.4 NAW and RMM reported that a design study is now in progress in Durham. The SPIE paper is in press in Proc SPIE 4008. LASER GUIDE STAR SUMMARY 3.5 RMM presented a brief summary of the LGS proposals for deployment on the WHT. Two types are currently being proposed, complimentary to each other. (Overheads at iwg10-00-naomi.ppt) 3.5.1 The Rayleigh beacon uses Rayleigh backscatter from molecules (and at the higher altitudes Mie scattering from the Saharan dust) in the atmosphere up to an altitude of ~20km. Time gating is employed to tune the height of the beacon. An AO system using a Rayleigh beacon can not correct turbulence from altitudes above this out to ~90km. Hence partial AO corrections are achievable. However, the advantages are that the angle over which the corrections are valid is greater and the cost of the laser lower than for a Na LGS. La Palma has been shown to often have a dominant low level turbulent layer, so the Rayleigh system will often correct a significant fraction of atmospheric turbulence degradations. 3.5.2 MOSAIC has been proposed to exploit the Rayleigh beacon, giving partial AO corrected images (~0.2 arcsec in R) over ~5 arcmin fields. 3.5.3 The Durham PATT rolling grant includes funding to purchase a demonstrate a Raleigh beacon system. In Mar 2001 a test beacon with a mono-static launch and range gate system will be deployed on the WHT. Phase B studies in July 2001 will include integration with an AO system (based on the Durham ELECTRA spare system) and perhaps TEIFU to characterise on/off-axis performance. 3.5.4 The Sodium laser guide star system relies on sodium resonance backscatter from Na atoms in the atmosphere at ~90km. A JIF bid (PI: Chris Dainty) was submitted to implement a system at the WHT (UKP ~3.9M). A funding decision would be know towards the end of 2000. VSD wondered what action would be needed if the JIF bid failed? RGM indicated that the IWG AGREED that the LGS system was of vital importance to the success of both the ING and UK AO strategy. The IWG would fully support any necessary bid for LGS funding. RMM noted that if the JIF bid was unsuccessful, a bid to PPARC would need to be submitted in Spring 2001. This might mean that less effort would be available to fully complete the LGS Preparatory study report to ING. RGL indicated that Jesus Jimenez Fuensalida was leading the IAC LGS activities. [IWG10-00/3.5.4A ACTION: NAW/RGM] Communicate to RGMR the IWG's support for the LGS system for the WHT [IWG10-00/3.5.4B ACTION: NAW] Contact the IAC LGS team 3.5.3 RMM reported that the LGS preparatory study would be completed by 12/2000. This study showed that there were large seasonal and nightly variations in the Na layer above La Palma. It indicated the minimum power LGS system that would be required for an operational AO system (~20W) - this being used for the LGS JIF bid request. [LGS Prep study @ http://op.ph.ic.ac.uk/jkt_lgs/ 3.5.4 NAW mentioned the upcoming meeting at IC, London, UK on Mon 18 Dec 2000 (provisional date). Individuals active in the UK AO programme, and a number of colleagues from other institutes with AO interests on La Palma had been invited. The purpose of the meeting would be to: - highlight the developments currently occurring on the WHT - map out a medium term path for a Multi Conjugate AO (MCAO) system based on the WHT - use this as a technological and scientific milestone towards a MCAO system on an eventual ELT (25-m + telescope) VSD stressed that the IWG should balance near term ING instrumentation issues with these more ambitious MCAO plans. GBD and others noted that the case for development of AO instrumentation and the LGS system was strengthened if viewed in the context of a longer term framework (especially one of strategic importance for UK astronomy). Therefore the MCAO discussions were relevant. [IWG10-00/3.5.4 ACTION: NAW] To invite and distribute agenda of this Dec 2000 AO meeting to the IWG and Pat Roche (Gemini Project Scientist). EU MARIE CURIE AO FELLOWSHIPS 3.5 NAW reported that the EU have funded 60 staff months of effort, via the Marie Curie Fellowship programme. This will provide expert AO support. The IWG was asked to bring these posts to the attention of suitable candidates. The closing date is 31 Oct 2000. [ AAS ad @ http://www.aas.org/JobRegister/no11449.html ] TEIFU, WYFFOS AND WIDE FIELD MULTIOBJECT SPECTROSCOPY 4. NAW led the session on developments concerning WYFFOS, AF2 and TEIFU. 4.1 RMM presented overheads prepared by Jeremy Allington Smith (JAS) (TEIFU PI). (iwg10-00-teifu.ppt) 4.1.1 In comparison with OASIS, TEIFU can format a larger spectral range. However, realistically, TEIFU's excellence would be if upgraded to IR-TEIFU operating in the J+H bands. OASIS provides no capability about 1um. In discussion, it was noted that the minimum size detector of use with IR-TEIFU was a 2kx2k array. NAW noted that such a detector (a new Rockwell device perhaps with a sensitivity cut at ~1.9um) would also be of benefit for imaging and IR-WYFFOS purposes. There was some concern that H band performance with warm optics might be compromised. GBD noted that Subaru's OHS spectrograph performance was a lot worse than expected in H. Also, CIRSI was now designed to be operated at ~-40C. It was AGREED that a full estimation of IR-TEIFU at H was required before a case could be made for a new detector investment for it. [IWG10-00/4.1.1A ACTION: NAW] To contact JAS to confirm H band IR-TEIFU performance. [IWG10-00/4.1.1B ACTION: NAW/RGM] To investigate a test system using INGRID to characterise H band performance. 4.1.2 In the short term (~2-3 years) TEIFU could provide IFU spectroscopy in the optical with NAOMI. In a discussion, the IWG agreed that if TEIFU were offered in the optical, it should be in the simplest mode, with the two 500 fibre blocks formatted as one unit. RMM Indicated that this would make the instrument one with no moving parts, and therefore much easier to offer as a common user instrument. The IWG AGREED that the necessary changes to the TEIFU fore-optics should be implemented to allow it to be used with NAOMI. RMS indicated that Durham should be in a position to commission TEIFU with NAOMI Q1 2001. He anticipated that TEIFU would operate in a de-scoped fashion, with only the option of deploying the two 504 bundles as a 1008 element single IFU. [IWG10-00/4.1.2 ACTION: NAW] Communicate the decision that no split block capability with TEIFU is required to JAS at Durham. 4.2 NAW reported that the AF2 small fibre project was progressing well. Fabrication would be complete by Mar 2001 and commissioning would take place in Q2/3 20001. 4.2.1 In discussion NAW indicated that active autoguiding may be implemented with the new small fibre unit. At present, only manual autoguiding is possible - the semi-coherent bundles view a number of fidicual stars. The ING is investigating a coherent bundle to be placed by the AF2 robot at a guide star in the AF2 field. The coherent bundle will feed a standard ING autoguider head located at the PF and provide X-Y errors to the TCS. Rotation error correction will still be done manually by means of the semi-coherent guide bundles. 4.3 The WYFFOS upgrade project involving a redesign of the camera is proceeding. NAW commented that RGB has been involved in preliminary design work. The favoured design is currently one with a focal length of ~290mm, which enables the full 4kx4k EEV 2 chip CCD camera (~60mm x 60mm) to be imaged. This has the advantage that ~5-600 fibres can be imaged onto the detector from the WHT prime focus. 4.3.1 RGB noted that he would require the exact dimensions of the CCD detectors and their location within the cryostat. Also, as focus depends on waveband, the proposed waveband of operation was required in the generation of further designs. [IWG10-00/4.3.1 ACTION: NAW] provide RGB with final CCD and waveband parameters. 4.3.2 NAW reported that the ING, at this stage is not proposing to implement the IR upgrade to WYFFOS. Further modeling is needed as to throughputs to feedback into possible science cases. However, in making the final camera upgrade design, RGB is being asked to highlight areas where IR performance might be compromised. The intention is to allow the possibility of a near IR upgrade path at some point. RGB noted that a new IR optimised collimator would also be required, the current one has poor optical performance above ~1.1um. RGB has a low cost design for such a collimator. 4.3.3 RGB cautioned that lead times for the optical components needed for the WYFFOS camera could be upto 9 months due to pressures on suppliers. However, NAW considered that the long camera should be in use by Semester 2002A 4.3.4 The IWG noted the complexities involved in the upgrade path's for WYFFOS, AF2, TEIFU, IR-TEIFU, IR-AF2. They indicated that the constraints and options should be presented at the next IWG. [IWG10-00/4.3.4 ACTION: NAW] to summarise the WYFFOS area developments to include options and trade-offs for WYFFOS, the long camera, (IR)-AF2, (IR)-TEIFU. This should be made available on the IWG WWW pages before the next IWG meeting. 4.3.5 GBD highlighted the current AF2 configure s/w. He noted that this is not optimum. Better s/w would be needed if more fibres were to be implemented. He suggested that Tony Farrell at the AAO be contacted concerning the AAO's 2dF configuration s/w. [IWG10-00/4.3.5 ACTION: NAW] Contact the AAO concerning 2dF configure s/w. PIPELINE DATA PROCESSING AND ARCHIVING 5. In the context of new Government initiatives for the provision of e-science, pipeline processing and archiving issues are becoming more important. RGM thought that only Observatories that provided high quality data products would be able to add value to National Virtual Observatories in the future. 5.1 Jim Lewis (CASU) reported on developments in support of data reduction and archiving at the ING. (IWG10-00-pipe.ps) 5.1.1 JRL highlighted the WFC data pipeline. This currently is able to linearise the data and correct for bias, flat field, and perform a astrometric solution (to ~1 arcsec absolute) 5.1.2 A second stage of the pipeline (developed by Mike Irwin) performs a more precise astrometric fit (good to the limit of the APM catalogues used as reference - so ~0.5 arcsec absolute, ~<0.1 arcsec relative). De-fringing is applied to R, I, Z data and object catalogues are generated. Integration of this and photometric solutions is in progress. 5.1.3 JRL indicated that the pipeline to handle INGRID IR data is well advanced and will be deployed at the ING in Jan 2001. 5.2 JRL mentioned that the 1996 vintage pipelines for ISIS and IDS could be updated. For WYFFOS GBD suggested investigating the use of the AAO 2dF pipeline. He noted that many programmes now use this to process their 2dF spectra data in near real-time. 5.2.1 The IWG AGREED that flux calibration of spectral data should NOT be part of the pipeline. 5.3 The main problems in developing an introducing the pipeline s/w were noted by JRL as: - poorly understood detectors (e.g. variations in linearity) - poorly defined header items - lack of observing protocols (e.g. sky flats etc.) - poorly defined user expectation (e.g. what does reduced mean?) VSD asked if some calibrations should be required from observers. There was general agreement that the twilight period should be optimally used for obtaining calibration data. Time not needed by the scheduled observers for their calibrations, should be used for more general calibrations (e.g. when imaging, flat fields in as many filters as possible - U band at start of twilight etc.) RGM stressed that the calibration data should be of high quality. For instance, special blank sky areas were required for the WFC. Wide slit standard star observations should be acquired if possible during twilight for ISIS, IDS. [IWG10-00/5.3 ACTION: RGM/JRL/NAW] to propose a minimal calibration plan needed for imaging and spectroscopic data pipelines 5.3 NAW stated that the ING have recently initiated the operation of the WFC pipeline. Also, it is being used in 'quick look' mode to give observers access to reduced data after ~4 mins. This makes use of library calibration frames (bias, flats etc). KK asked whether photometry was yet available. RGM indicated that it was planned that observations of standard Landolt photometric fields would lead to photometric solutions being automatically available. SFG noted that the stability of dome flats could be used to control instrument stability on a night-by-night basis. 5.4 NAW reported that the ING has funded an 8 node Beowulf cluster, named 'Gigawulf'. This will be deployed by Jan 2001 and will provide the processing the power to handle the pipeline data reduction and quick look demands of the ING. 5.5 JRL mentioned that the interface to the ING archive was been improved to enable easier association of calibration data with science data. 5.6 RGM gave a brief overview of the new government e-science initiative. As part of this UKP 30M (over 3 years) had been provided to PPARC, of which UKP 25M would go to HEP. About UKP 3M would go to astronomy. A consortium of IoA/ROE/Leicester/RAL had submitted a document to PPARC indicating how this might be used to support the development of the tools needed by a 'virtual Observatory' RGM had been in contact with Rene Rutten. The ING and IoA/CASU saw that the development of the ING data systems would provide a valuable reduced data set to form a nucleus in such future activities. THE DEVELOPMENT OF THE JKT TO SUPPORT NEO ACTIVITIES 6. NAW informed the IWG that the UK Government DTI sponsored study of Near Earth Objects has recommended a use for the JKT. (iwg10-00-neo.pdf) [ NEO report @ http://www.nearearthobjects.co.uk/ ] 6.1 SFG stated that he had been a key advisor to this report team. The would be used for determining the orbits of newly discovered NEO's and also to characterise their chemistry through multi-band photometry. This might involve a set of ~8 specialist filters. 6.2 Most of the NEO's of interest would be small and therefore nearby when discovered. These would likely have high proper motions, limiting on object exposure times. Thus the use of the UltraDAS on the JKT was important. 6.3 In discussion SFG indicated that a significant fraction of the JKT time (>= 50%) could be devoted to the photometry of NEO's. 6.4 NAW stated that he had organised an internal ING discussion where a number of proposals had been suggested to enable the JKT to carry out it's envisaged NEO role. Importantly this would involve making it an automatic telescope, and improving it's imaging quality. The IWG AGREED that a proposal should be developed to adapt the JKT to carry out a NEO role, assuming ~50% of it's use would be devoted to this area. The IWG thought that any bid should involve running costs for the NEO work, but noted that these would be minimised if the capital investment to automate the telescope was provided. [IWG10-00/6.4 ACTION: NAW/SFG] Develop case for JKT NEO role. 6.5 NAW indicated that there might be a role for the IC tip-tilt system to provide images of ~0.4 arcsec in the visible over reasonable fields. [IWG10-00/6.5 ACTION: NAW/VSD] Develop case for JKT tip-tilt system. [ JKT Tip tilt @ http://op.ph.ic.ac.uk/tt/tip_tilt.html ] IWG COMMITTEE MEMBERSHIP 7. RGM led a brief discussion on the rotation of IWG committee membership. The term of membership was nominally three years. 7.1 It was AGREED that RGM would suggest a plan for rotation. This would probably involve inviting 2-3 new members to the next Spring 2001 IWG, to overlap for one meeting with the existing members. At the following meeting they would then be replace 2-3 old members, and at the same time the meeting would add 2-3 more new members to overlap with the last 2-3 old IWG members. By Spring 2002 the committee membership would have rotated. [IWG 10-00/7.1 ACTION: RGM] To agree with Rene Rutten procedure for rotation of committee. 7.2 The IWG AGREED, having confirmed with the Director, ING, that Ramon Garcia Lopez was now the new Spanish representative on the IWG for a three year term. DUTCH INSTRUMENTATION ISSUES 8. KK provided a brief overview of NL instrumentation developments. 8.1 KK asked, following on from a NL user request, as to whether a spectroscopy option could be re-instated at the JKT. The IWG considered this to be unlikely. 8.2 KK noted that the development of OASIS for deployment on the WHT had recently been funded by NWO, and that the PI was Thijs van der Hulst (Groningen). 8.3 The Planetary Nebulae Spectrograph, for which KK is PI, would be commissioning on the WHT in Semester 2001A. [ PN spectrograph @ http://www.aao.gov.au/local/www/pns/pns.html ] 8.4 In a short discussion concerning the access to commissioning time when deploying new instrumentation, the IWG strongly SUPPORTED the notion that REALISTIC and JUSTIFIED commissioning time should awarded. This would facilitate the full characterisation of new instrumentation, having a beneficial impact on its ability to deliver science. 8.5 KK suggested that the next meeting of the IWG should re-address the instrumentation suite at the WHT, to identify which capabilities were or would soon be, uncompetitive. [IWG 10-00/8.5 ACTION: NAW] Include Instrumentation rationalisation as a Spring 2001 IWG agenda item. SPANISH INSTRUMENTATION ISSUES 9. RGL noted that the main thrust of current activity in Spain was in the provision of instrumentation for the GTC. He noted that issues concerning LIRIS had been discussed earlier in this meeting. [ GTC @ http://www.gtc.iac.es ] ANY OTHER BUSINESS 10. Any Other Business was discussed. 10.1 RGM noted that it would be useful for the breakdown of instrument request and usage to be available on the IWG WWW pages. [IWG10-00/10.1 ACTION: NAW] Place instrument usage data on-line 10.2 In a closing discussion the IWG noted that La Palma is a good site for future ELT's. The IWG believes that, in the context of the possible future of the UK within ESO, the ING could play a very important role, especially in the area of AO and LGS systems. 10.3 The date of the next meeting is to be arranged. However it should be before the next INGB meeting that will occur May 2001. Location is likely to be either Groningen or The Canary Islands. [IWG10-00/10.3 ACTION: NAW/RGM] Confirm and advise date of next IWG meeting. 10.4 RGM and NAW thanked Richard Bingham, Jim Lewis and Richard Myers for attending the meeting. 10.5 The meeting closed at 17.15 Nicholas A Walton accepted: 22 Mar 2001 (IWG secretary) (orig) : 25 Oct 2000