Joint Astronomy Centre Annual Report 2005/6

660 North A`ohoku Place Hilo, Hawaii 96720 USA Tel: +1 808 961 3756 Fax: +1 808 961 6516 Web: http://www.jach.hawaii.edu/ Introduction by the Director

Welcome to the JAC Annual Report for modern times. Over its eight-year lifetime, it accounted 2005/06. It follows the same format as for roughly 75% of all publications based on JCMT data, last year’s. The reporting period, how- and was, at one stage, ranked second only to the HST ever, has been adjusted to match the in terms of its impact on astronomy. One of its most financial year, rather than the calendar notable successes was the discovery of a large popula- year, to bring this report into synchronic- tion of massive, dust-enshrouded galaxies in the early ity with our programme reports to the Universe, a class of objects now known universally as two telescope Boards. The period has certainly been “SCUBA galaxies”. The retirement of SCUBA clearly eventful, with the JCMT in the midst of a transforma- marks the end of an era. tion to third-generation instrumentation, whilst at UKIRT, observations have commenced on a major and much- The JCMT is undergoing an extremely ambitious pro- anticipated science campaign. gramme of development in which the entire instrumentation suite is being replaced. The integration of ACSIS The UKIRT highlight of 2005/06 was undoubtedly the ob- into the JCMT’s new Observatory Control System contin- servation of the impact of the NASA Deep Impact probe ued throughout the reporting period. HARP, the world’s on comet Tempel-1. UKIRT was the first large telescope first array receiver for the 345-GHz band, was delivered to observe the direct light from the impact, and CGS4 to the telescope in November 2005, and commissioning echelle spectra obtained after impact show both fluores- is in progress. Development work also continued on our cent water lines and emission from icy dust grains. In collaboration with the SMA and the CSO to conduct a the longer term, however, UKIRT’s major achievement joint programme of submillimetre interferometry in the during the reporting period was the commissioning of its years before ALMA becomes operational; first fringes new wide-field camera, WFCAM, and the commence- were obtained in July, and first spectra in September. ment of the UKIRT Infrared Deep Sky Survey (UKIDSS). This seven-year programme will go three orders of The flagship of the development programme is clearly magnitude deeper than the 2MASS survey and will pro- SCUBA-2. The project was re-approved by PPARC vide the definitive near-infrared counterpart to the Sloan Council in February 2005 and is now fully funded. As Digital Sky Survey in the visible. The UKIDSS Early Data part of the JAC’s contribution towards the resourcing Release, a “taster” based on a very small fraction of the of SCUBA-2, the observing night was reduced in Janu- full survey, took place in February 2006 and is already a ary 2006 from 16 hours to 12. The instrument is being unique astronomical resource; the first full data release, developed at the UK ATC and it is currently scheduled scheduled for July 2006, will be a major and much-an- for delivery to the JCMT in late 2006. Because the size ticipated event. and weight of this novel instrument requires a completely new support infrastructure, the JCMT was closed The major event of the year at the JCMT was, undoubt- on 13 February 2006 for six months of engineering work. edly, the retirement, through ill health, of the SCUBA The observatory is currently a construction site, and the instrument. SCUBA was one of the most successful and scale of the work being undertaken is staggering; it is productive ground-based astronomical instruments of scheduled to come back on line in August 2006. ii In recognition of the potential of HARP and SCUBA-2 for large-area mapping, the JCMT Board approved, in July 2005, an ambitious set of legacy surveys for the JCMT. The survey programme was allocated 55% of the telescope time over Semesters 07A through 08B. In order to handle the high data rates of HARP and SCU- BA-2 and to ensure the legacy value of the surveys by providing uniform data processing, a new project called the JCMT Science Archive was approved and initiated in 2005. This is a collaboration between the JAC and the Canadian Astronomical Data Centre and is resourced from the JAC, by PPARC and from Canadian sources.

Finally, both JAC telescopes underwent strategic reviews during 2005. A panel led by Richard Ellis (CalTech) visited UKIRT in June, and a similar panel chaired by Martin Harwit (Cornell) visited the JCMT in September. Both panels were provided with comprehensive documentation describing telescope management, community demand, scientific productivity and future plans; they also visited the observatories and met with JAC staff at all levels. In both cases, the records of innovative instrumentation, novel observing modes and profound scientific impact over many years were very highly praised. The development plans for the two telescopes were also reviewed and the panels declared that JCMT and UKIRT would, consistent with the JAC’s mission statement, maintain their positions as the most advanced of their kind in the world.

Professor Gary Davis Director

JCMT (top) and UKIRT (bottom) on Mauna Kea in Hawai’i. Photos by Nik Szymanek.

iii Foreword by the UKIRT Board Chair

One important event for UKIRT this began its first large scale “campaign mode” science year was the international review of the project, the UKIRT Infrared Deep Sky Survey, UKIDSS. telescope and its operations by a panel Over the next two years UKIDSS will use 50% of the chaired by Prof. R. Ellis of CalTech. The observing time on UKIRT to carry out a set of five large panel reviewed a range of documenta- scale public survey projects. In February 2005, the first tion supplied by UKIRT, the Board and small subset of UKIDSS data was released to give the others, and visited the telescope in June community a sample of things to come. The first major 2005. Prof. Ellis delivered his panel’s report to the Board data release is scheduled for July 2006 and is eagerly in September. This report highlighted UKIRT’s achieve- anticipated. ments, its current status and operations and its overall science productivity. Perhaps most importantly, the To summarise this past year of UKIRT operations, as review panel recognised that UKIRT has an important described in this annual report, I add the UKIRT Board’s future role and recommended that a plan be developed wholehearted support, as expressed in the first line of for the telescope’s projected use and development. The the executive summary of the Ellis Panel report: “The Board would like to publicly thank Prof. Ellis and the panel considers UKIRT to be a remarkably efficient and members of his panel, Prof. S. Lilly, Prof. J. Graham, well-run observatory whose recent scientific output is Prof. J. Dunlop, Prof. H. Richer and Dr. P. Roche, for commendable.” their hard work in producing their review. Dr Gary Fuller The first step in developing a plan for UKIRT’s future University of Manchester direction was an open meeting in April 2005 in conjunc- UKIRT Board Chair tion with the National Astronomy Meeting in Birmingham. At this well-attended meeting, a wide range of exciting ideas about new scientific projects and new instruments were presented, demonstrating a very high level of interest in continued exploitation of UKIRT to produce world- leading science. As a result of this meeting and the recommendations of the Ellis panel, the Board is now setting up a process to solicit and review formal proposals for new observational and instrumental projects.

This annual report covers a period when the science operation of UKIRT has undergone a significant change. After its delivery and initial commissioning late last year, WFCAM started routine science observations, producing panoramic images with typically 0.6’’ seeing. With the start of science observations with WFCAM, UKIRT iv Foreword by the JCMT Board Chair

On behalf of the JCMT Board, I am very During the year, the Board re-emphasised the impor- pleased to welcome this annual report of tance of SCUBA-2 and identified it as the highest priority the JAC. The past year has been a peri- of the observatory. We are pleased that it is now fully od of great challenge and change for the resourced and look forward to its arrival at the telescope JCMT and its staff, culminating in the re- and to the acquisition of astronomical data. The sea- tirement of SCUBA and the DAS, and the change in observing capabilities that the new instru- receipt of HARP, a 16-pixel heterodyne ments will deliver led the Board to call for legacy survey array receiver for use at 345 GHz, and the new digital proposals in 2005. Seven proposals were received and correlator, ACSIS, together with the first fringes obtained externally refereed, with the result that all seven were with the eSMA. In addition, the JCMT was closed in approved by the Board and some 55% of observing time February 2006 to allow the necessary engineering work over four semesters was allocated to them. to be undertaken in readiness for the arrival of SCUBA-2 and to enable the observatory to move to 12-hour nights Overall, the Board is confident that, with the dedication, as part of its contribution to SCUBA-2 funding. experience and motivation of the JCMT staff, the talents of instrument builders and software engineers, coupled The new instruments will each improve the efficiency with the innate curiosity of visiting astronomers, the ‘new’ of previous instruments by one to three orders of JCMT will thrive. We look forward to many new and magnitude and will ensure a productive future for the unexpected discoveries in the hope that the JCMT will telescope. With this increase in sensitivity comes an be able to significantly advance our understanding of the increase in complexity, which has already put an addi- origins of planets, stars, galaxies and the Universe. tional level of demand on staff during the commissioning of ACSIS and HARP, in parallel with the new observatory We commend this report to you as a summary of work control system. The Board recognises that the commit- undertaken and the promise of even greater things to ment and dedication of staff at the JCMT has enabled come. much to be achieved in the past year. Professor Tom Millar In summer 2005, the work of the JCMT was reviewed Queen’s University Belfast by an international panel chaired by Professor Martin JCMT Board Chair Harwit (Cornell University). Their report identified the JCMT as the world’s leading submillimetre observatory and concluded that it would remain so for the foreseea- ble future, once SCUBA-2 comes online. The report was especially helpful in persuading PPARC that it should seek a suitable strategy for the facility, post-2009, with its partner agencies.

The Joint Astronomy Centre base facility in Hilo, Hawai’i. Contents

Introduction by the Director...... ii Foreword by the UKIRT Board Chair...... iv Foreword by the JCMT Board Chair...... v

Introduction to the Joint Astronomy Centre...... 1 UKIRT Science Highlights...... 3 UKIRT Operations and Instrumentation...... 9 JCMT Science Highlights...... 15 JCMT Operations and Instrumentation...... 19 JAC Technical Support...... 29 Administrative Group...... 30 Science Education and Public Outreach...... 31

Appendix:

Staff Organisation in 2005/6...... 32 Financial Statement, 2005–2006...... 34 Telescope Time Awards (UKIRT)...... 36 Telescope Time Awards (JCMT)...... 40 Refereed Publications in 2005/6 (UKIRT)...... 48 Refereed Publications in 2005/6 (JCMT)...... 50 Committee Membership as of 31 March 2006...... 53 Joint Astronomy Centre Seminars in 2005/6...... 54 Abbreviations and Acronyms...... 56 Some of the staff of the Joint Astronomy Centre, photographed in spring 2006 by Inge Heyer. Introduction to the Joint Astronomy Centre

Description manner on behalf of the funding agencies; and • to be responsive to the changing needs of the contrib- The JAC operates two telescopes at the summit of uting organisations. Mauna Kea on the island of Hawai’i: the United King- dom Infrared Telescope (UKIRT) and the James Clerk United Kingdom Infrared Telescope (UKIRT) Maxwell Telescope (JCMT). The altitude (roughly 4,200 m/14,000 ft) and the dryness make Mauna Kea the UKIRT is the world’s largest telescope dedicated exclu- premier site for ground-based astronomy in the northern sively to observations in the infrared region of the spec- hemisphere. trum. It is funded entirely by PPARC and is governed by a Board. Time is allocated by a UK-based TAG. UKIRT is The JAC is an Establishment of the Particle Physics and also a member of the Opticon Consortium, and partici- Astronomy Research Council (PPARC) of the United pates in the Opticon transnational access programme. Kingdom. PPARC provides funds to the JAC for UKIRT and for the UK share of the JCMT. The JAC also re- Primary mirror diameter: 3.8 m ceives contributions from the National Research Council First light: 1979 (NRC) of Canada and the Netherlands Organisation Wavelengths covered: 0.8 µm–30 µm for Scientific Research (NWO) towards operation of the JCMT. James Clerk Maxwell Telescope (JCMT) The JAC has a staff complement of roughly 60, com- The JCMT is the world’s largest single-dish telescope prised of a mixture of local and international staff. The operating in the submillimetre region of the spectrum. It workforce is divided into five groups: one operations is a partnership between the UK (55%), Canada (25%) group for each telescope, and three groups for common and the Netherlands (20%) and is governed by a tripar- support services (engineering, software, administration). tite Board. Time is allocated by the ITAC, supported by three national TAGs. The JCMT is also a member of the Mission RadioNet consortium and participates in the RadioNet transnational access programme. The Joint Astronomy Centre provides services and support: Primary mirror diameter: 15 m First light: 1987 • to enable visiting and staff astronomers to undertake Wavelengths covered: 200 µm–2 mm top-quality, front-line international-class research using the James Clerk Maxwell Telescope and the United Kingdom Infrared Telescope; • to develop these facilities in order to maintain their position as the most advanced of their kind in the world; • to operate them in the most cost-effective and efficient

UKIRT

UKIRT/WFCAM image (a fraction of a full tile), showing the W75N and DR21 star-forming regions in J, H, and H21-0S(1) molecular emission. Davis et. al., JAC

UKIRT

Science Highlights

Cassegrain Science Highlights Solar System Figure 1: CGS4 spectroscopy of Tempel-1 post-impact, showing continuum The undoubted highlight of 2005/06 was the observa- and water vapour lines in the cometary spectrum. tion of the impact of the NASA Deep Impact probe on comet Tempel-1. UKIRT was the first large telescope to observe the direct light from the impact (timings were issued from the summit, at the time, and these have since been amply confirmed), and CGS4 echelle spectra obtained both before and after impact were taken to detect fluorescent water lines and thermal emission from dust grains in the ejecta. This observation (PI Miller, UCL) was granted a number of half-nights bracketing the event itself.

UKIRT uses a visible camera to provide a guide signal, and the comet was sufficiently bright, even pre-impact, to guide on it directly. Variations in the resulting guide star signal proved very useful in determining physical Figure 2: Guide trace from the fast guider, showing the development of the parameters of interest after the impact. By estimating the light curve well after impact. velocity of the ejecta and knowing the maximum kinetic energy available from the impactor, it was possible to infer the mass of ejecta. In view of the predicted effect Extragalactic of the impact—putting 19GJ of energy into the production of 1028 water molecules at temperatures of order UKIRT data have long figured at the forefront of studies 1,000K—the observed wavelength region was chosen of galaxies, radio galaxies and quasars at a range of to maximise the detection of hot water lines. Analysis redshift. In 2005, Dunlop et al. carried out a study of the of the CGS4 echelle data has shown that the spectrum most massive galaxies (3CRR-class radio galaxies) at contains a large number of excited water lines, some high redshift. Deep K-band UFTI imaging was obtained of which were previously unknown in cometary spectra in the redshift range 1.5 < z < 2.5. The great depth of and, thus, highly likely to reflect the unique effect of the the imaging (obtained using 2–4 hours integration per impact event. object) combined with good image quality (FWHM<0.6”) to allow unambiguous determination of morphological parameters via two-dimensional modelling (Figure 3).

UKIRT

Preliminary results from this project, which was active in cent dark cloud, where currently accepted grain align- the queue throughout the Cassegrain time in Semester ment mechanisms should not function (Chrysostomou et 05A, indicate that the scale-lengths of powerful radio gal- al.; Figure 4).This result will place strong constraints on axies at z~2 are typically ~5kpc, a factor of two smaller models of grain alignment in dark, quiescent regions of than their counterparts at lower redshift. This suggests molecular clouds. that these systems experience significant dynamical evolution in the redshift interval 1.0< z<2.5.

Figure 3: Left—Image of 3C068.2, Centre—residual image after subtraction of best-fitting 2D model, Right—radial profile of the radio galaxy and the best- fitting model. Stellar Astronomy

The end of Semester 05A saw the completion of an Figure 4: Top—absorption feature due to cold (< 10K) solid CO in the Taurus ambitious project (PI Peletier, Groningen), which pro- Dark Cloud. Bottom—polarization feature confirming (i) grain alignment and duced a large stellar spectroscopic atlas in the infrared. (ii) dichroic absorption. This project involved grism spectroscopic observations of very bright stars, and considerable observational com- UKIDSS Science Highlights promises were made to ensure linearity of the spectra. With an engineering schedule change coming late in the Introduction semester, a six-night summit status period was accorded to this project in the last week of the semester; the com- The UKIRT Infrared Deep Sky Survey (UKIDSS) is pleteness of the project owes much to this change. the key project for the Wide Field Camera (WFCAM). UKIDSS commenced operations in the early summer Interstellar of 2005, after a short period of “Science Verification” observations undertaken to confirm the appropriateness The first two months of Semester 06A were seriously of each of the survey modes. This survey represents affected by bad weather, but a notable highlight from the 80% of the UK’s UKIRT time allocation, when WFCAM is very start of the semester was the detection of polariza- in place on the telescope, and will, henceforth, amount tion in the absorption feature due to solid CO in a quies- to 50% of all UKIRT observing time. UKIDSS results will

UKIRT

figure strongly in future annual reports; the basis for the • discover Pop II brown dwarfs, if they exist survey is fully described here, with some representative • construct a galaxy catalogue at z=1 as large as the highlights from early data. SDSS catalogue • measure the growth of structure and bias from z=3 to UKIDSS comprises five separate projects, as detailed the present day in Table 1 and Figure 5, and coordinates their collective • determine the epoch of spheroid formation execution. Their successful commencement represents • clarify the relationship between quasars, ULIRGs, and a major scientific milestone for UKIRT. There are two galaxy formation wide-area “legacy” surveys, the LAS and GPS, one sur- • map the Milky Way through the dust, to several kpc vey focusing entirely on galactic star clusters (the GCS) • increase the number of known Young Stellar Objects and two extragalactic surveys of increasing depth and by an order of magnitude, including rare types, such as decreasing area (DXS, UDS). The main science goals of FU Orionis stars the individual surveys are detailed below, but the overall aim of UKIDSS is to provide an infrared survey of the sky of unprecedented depth and lasting legacy value, Table 1: The UKIDSS Surveys and an infrared counterpart to the Sloan Digital Sky Sur- Survey Area Filter K-band 2 vey at visible wavelengths. Full details are available on (deg ) Depth the UKIDSS web site (http://www.ukidss.org/). Large-Area Survey (LAS 27.3 YJHK 18.1 Galactic-Plane Survey (GPS) 14.9 JHK 17.7 UKIDSS was designed by a consortium of UK and (lat- Galactic-Clusters Survey (GCS) 7.0 ZYJHK 18.1 terly) ESO astronomers, who also undertake to carry out the required observing in conjunction with UKIRT staff Deep Extragalactic Survey (DXS) 2.4 JK 20.7 astronomers. The consortium is led by the UKIDSS PI, Ultra-Deep Survey (UDS) 0.8 JK 21.1 Prof. A. Lawrence (Edinburgh), and detailed organisation is carried out by Dr. S. Warren (Oxford). Data quality assurance is carried out in part by Dr. S. Dye (Cardiff). The UKIDSS design is fully described in Lawrence et al. (2006, MNRAS, submitted); summaries are given here and the reader is referred to Lawrence et al. for details. Science Goals

The key science aims of UKIDSS are to: • find the nearest and faintest sub-stellar objects • break the z=7 quasar barrier • determine the epoch of re-ionisation Figure 5: The UKIDSS fields on the sky. Diagram by S. Warren (see the • determine the substellar mass function UKIDSS website).

UKIRT

Data Releases Galactic-Plane Survey

Released after quality control and ingest into the The main goals of the Galactic Plane Survey (GPS) are

WFCAM science archive, UKIDSS data become im- to probe the IMF down to M=0.05Msun in star-formation mediately public to the ESO community and to a small regions within 2 kpc of the sun, to detect stars below the number of individual members of the Japanese commu- main sequence turn-off in the galactic bulge and to de- nity. 2005 saw the first major data taking in the UKIDSS tect luminous objects, such as OB stars and post-AGB programme, with some 10% of the total expected data stars across the whole galaxy. To do this, it will map half being taken (the whole of Semester 2005B was devoted of the Milky Way to within a latitude of 5 degrees and a to WFCAM operations). A small subset of the data taken K-band magnitude limit (5s) of 18.8. An example of the in 2005 was released in February 2006 as the UKIDSS diagnostic power of the GPS is shown in Figure 7. Early Data Release (EDR)—a taster of the data quality and a useful test of the science archive.

Figure 7: Extinction map of the M17 star-forming region. Photometric analysis by Hoare and from the UKIDSS GCS/GPS SV data. Extinctions up to Av=35 are sampled in this image, which has approximately 15 arcseconds resolution. Inset is the 2MASS three-colour image of the same region.

Large-Area Survey

Figure 6: The spiral galaxy M51, from 2005 UKIDSS data, compared with The Large-Area Survey (LAS) aims to map a large area some representative previous infrared imaging. Top left—image taken with 2 the first-generation UKIRT infrared imager (IRCAM). Top right—2MASS im- of the Northern Sky (4,000 deg ). When combined with age. Bottom—WFCAM/UKIDSS image at two different levels of detail. the SDSS, an atlas will be produced covering almost

UKIRT

an order of magnitude in wavelength, and within which DXS data in the Early Data Release include four fields spectroscopic data (from the SDSS) will already exist for at, or close to, full depth in J and K, plus shallower data a huge number of objects. The LAS reaches K magni- from flanking fields. tudes of 18.2 and includes a second epoch observation in the J-band to determine proper motions and, hence, Ultra-Deep Survey kinematic distances for nearby objects. The Ultra-Deep Survey (UDS) aims to allow detailed One of the key goals of the LAS is to detect extremely studies of the luminosity functions, clustering and high redshift (z=7) quasars and to distinguish them from spectral energy distributions of galaxies over a large, very low mass stars using the purpose-developed “Y” representative volume out to a redshift of 3, providing filter. From data within the Early Data Release, the esti- a complete census of the Universe at these epochs, mated rate of false positives for high-redshift objects is picking up galaxies which are abnormally red due to remarkably good at 20:1. Follow-up 4m iYJ imaging will dust extinction or old stellar populations. It will map refine the sample before undertaking spectroscopy. 0.77 square degrees to a 5s point-source sensitivity of J=24.8, H=23.8, K=22.8. Such depths are required to Deep Extragalactic Survey reach typical L* galaxies at z=3, and the survey area is two orders of magnitude larger than any previous survey The main goal of the Deep Extragalactic Survey (DXS) is at this depth. The UDS anticipates detecting more than to produce a photometric galaxy sample within a volume 10,000 galaxies at redshifts greater than 2. comparable to that of the Sloan Digital Sky Survey, selected in the rest-frame optical, but at a redshift of 1–2. Comparison with the present day will allow a direct test of the evolution of the galaxy population and determine how galaxies of different types (passive, star-forming, AGN) trace large-scale structure. The DXS aims to set tight constraints on cosmological simulation models with a field of view large enough to avoid cosmic variance. To achieve this, the DXS will map 35 square degrees of sky to a 5s point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The sample will also enable the selection of clusters of galaxies in this redshift range, where cosmological models predict numbers to be sensitive to the total mass density of the Universe. Figure 8: EDR data from the UDS/DXS SV phase, showing the detection of nearly 500 very red galaxies (J-K>2.3). With a magnitude limit of 16th magnitude in K, 2MASS (the previously largest infrared sky survey) samples only the left third of this figure.

UKIRT

Galactic-Clusters Survey

The Galactic-Clusters Survey (GCS) aims to address the crucial questions of the nature and universality of the initial mass function (IMF) below the brown-dwarf bound- ary. To do this, it will survey 10 large open star clusters and star-formation associations, covering a total of 1,067 square degrees. A first pass in the ZJHK filters will reach a depth of K=18.6, sufficient to reach 30 Jupiter masses in a typical cluster, and a second pass in K will permit the determination of proper motions for confirmation of cluster memberships.

Indications from the Early Data Release are good, with individual positional measurements accurate to ~10 milliarcseconds, and a likely proper motion precision of a few milliarcseconds per year over a five-year baseline.

UKIRT getting ready for a night’s observing. Photo by Douglas Pierce-Price.

Figure 9: Detection of substellar objects in the M17 field from the GCS/GPS SV data set.

UKIRT

Operations and Instrumentation

Telescope Usage of increased vulnerability to wind shake. A long-term solution to this issue awaits a concerted effort on servo 2005 began with the Wide-Field Camera (WFCAM) performance, scheduled in 2006. off the telescope for adjustments after the first phase of commissioning. Cassegrain operations continued The enclosure suffered some storm damage in the through to April 2005 when the second commissioning winter of 2004/5, and some deteriorating weatherproof- phase commenced. Semester 2005A, which would nor- ing allowed water into the dome. The latter problem was mally have run from the start of February, began in fact solved in engineering in 2005. A major failure occurred in mid-December 2004. in the shutter drive chain in March 2005. A temporary repair was effected quickly, but a complete cure required Table 1 summarizes the usage of UKIRT between Janu- closure of the telescope for two nights. ary 2005 and March 2006. The main feature of these statistics is the decreased fault rate compared to 2004, Emissivity despite the fact that more than half of the observing time was devoted to the new wide-field instrument. The chief contributor to emissivity changes over the period was variation in the silver-dielectric dichroic surface Table 1: Usage Statistics for UKIRT at the tertiary mirror. This was addressed in July 2005 Total Number of Nights 424.0 with the replacement of these reflectors using a simple Engineering and Commissioning Nights 33.9 gold patch dichroic. The slight (2–3 magnitude) degrada- tion in on-axis visible guiding performance is well worth Science Nights 390.1 the increased stability of the system emissivity. Science Nights Observed 62% Science Nights Lost to Faults 3% Instrumentation Science and Engineering Nights Lost to Weather 36% UIST

Telescope and Enclosure UIST remained the most-requested Cassegrain instrument, with an order of 50% of the Cassegrain proposal Telescope and Dome Control load in each semester. The instrument displayed a number of minor electronics problems, losing about The telescope had one or two major and long-term 3% of the UIST observing time. More major faults in- faults, including a once-off failure of its declination ampli- cluded a failed grism wheel, which removed 50% of the fier and persistent oscillations in the north. The underly- spectroscopic modes in February and March 2005; the ing optical system remains sound, capable of deliver- wheel was forced to an open position, and observing ing <0.3 arcsecond imaging on occasions when the continued on those projects, which could use the grisms atmosphere permits. Adjustments of servo parameters still available in the other wheel. This fault was cured in in 2005 largely removed the oscillations, at the expense

UKIRT

open-cryostat engineering during the April–July 2005 WFCAM WFCAM block. WFCAM commenced its second commissioning phase New direct-ruled IJ and JH grisms were delivered in April in April 2005, following a period off the telescope during 2005. The new IJ grism addresses a serious throughput which the focal plane assembly was shimmed to adjust problem found with the replicated grism originally deliv- its tilt with respect to the optical axis. Weather caused ered with UIST. The JH grism was procured to permit the loss of the majority of the five scheduled engineer- the same type of medium-resolution science already ing nights, and engineering was subsequently merged in practicable with the HK disperser. In practice, these two with scheduled observing, UKIDSS sky survey science grisms were found to be incapable of achieving a good verification and calibration observing. During the engi- focus; new, offset slits were procured from the UK ATC neering time, there were still approximately 6 mrad of tilt. and installed in December 2005, but results still were not In the absence of any immediately obvious explanation, perfect, and engineering is scheduled for the summer of the tilt was temporarily corrected by an adjustment to 2006 to address this issue. the attitude of the secondary mirror M2. Also, an inde- pendent adjustment of the external tilt shims beneath Also installed in spring 2005 was a new Wollaston prism, the cryostat was made. At this point, image quality was servicing the other grism wheel (including the L and reasonable (subarcsecond commonplace), and it was M band grisms). Spectropolarimetry is now available decided to press on with commissioning, UKIDSS Sci- across all UIST grisms, and because of the more logical ence Verification and scheduled observing runs. order of the dispersers, slit and Wollaston is much more stable and easily set up than was the case with CGS4. Commissioning time included major efforts on wavefront This makes spectropolarimetry amenable to full flexible sensing and tuning the primary active support. By late scheduling. April, operation was relatively routine, with bulk data flowing for UKIDSS SV and visiting observers work- In December 2005, a prototype coronagraphic imaging ing with the usual UKIRT support levels. Image quality polarimetry mask was installed in the UIST slit wheel. improved further into May, when cryostat tilt was final- Based on a spare imaging polarimetry mask modified ized, and the UKIDSS surveys were underway. When by attaching a piece of fine wire across one of the mask WFCAM came off the telescope in June, it was opened apertures, initial results obtained on bright (H~3-5 mag) up for a final attempt to cure the focal-plane tilt issue. post-AGB stars are very promising, as outlined in the Spring 2006 UKIRT Newsletter. A proper mask with 0.6 WFCAM went back on the telescope in August, with the and 1.2 arcsecond occulting wires is being procured and cryostat tilt shims set to zero tilt, and measurements should be available in Semester 2006B. confirmed that focal plane tilt shimming had been successful, with residual tilt at the 0.2 mrad level. This can be compensated for with an M2 tilt adjustment small enough to not measurably degrade image quality.

10 UKIRT

Wavefront sensing measurements were then taken with IRPOL two main results: (i) some residual spherical aberration was beyond the range of the primary mirror actuators Both imaging polarimetry and spectropolarimetry are to correct. (ii) astigmatism, coma and trefoil corrections now fully supported by the ORAC-DR pipeline. The were now very small, though sometimes detectable. The versatility of IRPOL, and the availability of the pipeline phase-diversity software used in UKIRT wavefront sens- support, are reflected in the continued popularity of ing is not able to differentiate reliably between coma and IRPOL at UKIRT—some 30% of proposals in Semester astigmatism at this level. As of October 2005, WFCAM 05A requested polarimetry. was regularly providing 0.6 arc-sec delivered image quality, and the UKIDSS surveys were well under way. The data-acquisition sequence recommended by Aitken Typically 160-200GB of data are acquired on a good- and Hough (2001, PASP, 113, 1300) was implemented weather night. Efforts to fully understand the wavefront for testing and used for the first time on PATT science and dynamic tilt effects and to reduce data-acquisition in February 2006. This change in the waveplate rotation overheads continued. sequence appears to be extremely successful in sup- pressing the “waveplate ripple,” which typically afflicts CGS4 waveplate spectropolarimetry. Figure 10 shows the polarization spectrum of the BN object in the 5-mm win- CGS4 performed well through the reporting period. dow, using the standard four-waveplate-position angles It was used with great success in the Deep Impact and the new, eight-position sequence. The success of observations reported elsewhere, in the continuing the method is obvious, and it is now the default IRPOL programme of monitoring of the evolution of Sakurai’s acquisition sequence. object and in the detection of metastable H3+ in the galactic centre (Geballe, McCall and Oka). CGS4’s fault rate remained exceptionally low, at a few tenths of a percent.

UFTI

UFTI remains popular, being used for more than one quarter of the science time in Semester 05A. The instrument performed well with a fault rate below 1%. Dur- ing August 2005 the shutter mechanism began to lose steps, and a small amount of time was lost to partially vignetted data.

Figure 10: Polarimetry Ripple Suppression.

11 UKIRT

06A. Note that DXS SV time also included time for UDS This work amply confirmed UIST as an extremely stable verification. spectropolarimetry platform, and the new Wollaston, which extends its wavelength coverage out to the M Table 2: PATT Time Awarded by Instrument band, makes it unique on Mauna Kea. 05A 05B 06A Instrument # % # % # % Demand CGS4 7.1 18.2 N/A N/A 5.0 13.6 Semester 05A was a split-mode semester that ran from UFTI 5.6 14.3 N/A N/A 3.8 10.3 December 2004 through to the middle of August 2005. UIST 21.6 55.2 N/A N/A 16.8 45.5 The middle section of the semester (March–June) was WFCAM 4.8 12.3 9.0 100.0 11.3 30.6 the first WFCAM science-observing block, bracketed before and after by Cassegrain blocks in which CGS4, UFTI and UIST were offered. During this WFCAM pe- Table 3: PATT Time Awarded by Science Category riod, the majority of the time was devoted to the com- 05A 05B 06A mencement of the UKIDSS survey. Semester 05B was a Subject # % # % # % WFCAM-only semester, running from the end of August Extragal. 19. 48.7 6 66.7 15 37.5 2005 to mid-February 2006. Of this time 80% was allocated to UKIDSS observing after engineering, UH and Galactic 18 46.2 3 33.3 22 55.0 Japanese observing time was top-sliced. Semester 06A Solar Sys. 2 5.1 0 0.0 3 7.5 is a split-mode semester, featuring Cassegrain mode observing from February to April, and WFCAM from Table 4: UKIDSS Relative Time Allocations Per Survey May to July, again with 80% of UK time set aside for Science Verifi- 05A 05B UKIDSS operations. UKIRT PATT time continued to be cation oversubscribed by about a factor of two. The overall ratio Sub- Hours % Hours % Hours % of total number of nights requested to the number of survey nights allocated ranged between 1.9 and 2.4, with PATT WFCAM time oversubscribed by a factor of 2.9 in 06A. DXS 26.20 28.1 50.40 40.6 214.25 30.1 Oversubscription for PATT Cassegrain time remained GCS 11.35 12.2 17.30 13.9 97.39 13.7 comparable to semesters preceding the introduction of GPS 14.30 15.3 29.15 23.5 122.75 17.3 WFCAM. Tables 2 and 3 break down successful PATT- LAS 20.30 21.7 27.40 22.0 152.65 21.5 panel telescope allocations by science category and instrumentation. UDS 21.20 22.7 0.00 0.0 124.05 17.4

Table 4 indicates the time (in hours) spent on each UKIDSS Support UKIDSS sub-survey from 1 Jan 2005 to 31 March 2006. Note that the 06A WFCAM block did not begin until UKIDSS scheduling developed over the year, and the May 2006, so no UKIDSS statistics are presented for key requirements of contiguous coverage and uniform

12 UKIRT

depth are now reasonably and comfortably achieved in normal operations. A hybrid approach has been adopted in which the priority of individual MSBs is adjusted to foster contiguous sky coverage in real time, and the priority of whole survey projects (for example the Galactic Plane Survey, GPS) is adjusted to ensure completion, as needed. Progress is monitored, and priorities adjusted, twice weekly. Throughout the 2005 WFCAM blocks, some 30% of the UKIDSS observing was carried out by UKIRT staff astronomers.

UKIRT in the afternoon glow on Mauna Kea in Hawai’i. Photo by Nik Szymanek.

13 JCMT

The James Clerk Maxwell Telescope on Mauna Kea. Photo by Nik Szymanek.

14 JCMT

Science Highlights

Extra-Solar Systems and Star Formation entire cloud, but a more substantial fraction of the very highest extinction regions of the cloud (10% of the mass On their largest scales, molecular clouds do not collapse at Av > 10 mag). A quantitative argument for the mini- to form stars, and yet, on smaller scales, some sub-re- mum extinction for core formation can be found in Kirk gions do collapse. Understanding how the largest scales et al. 2006 (MNRAS, 360, 1506). In addition, the SCUBA of clouds are supported while allowing the formation cores are preferentially located offset from the peaks of of stars in sub-regions is an ongoing challenge. Us- the extinction, indicative of a triggered-star-formation ing data from the COMPLETE Survey (see http://www. scenario. Both of these results indicate the strong con- cfa.harvard.edu/COMPLETE, Ridge et al. 2006), Kirk, straints that can be placed on theories of cloud support Johnstone and Di Francesco (2006, ApJ, in press, as- and star formation by large surveys of molecular clouds. troph-0602089) studied the column-density structure of the Perseus molecular cloud to gain an understanding of Protoplanetary disks of gas and dust are the material these two processes, using data from SCUBA to meas- reservoirs for the planet-formation process. Information ure the small-scale column structure of the cloud, and about the properties and evolution of these disks can be from the 2MASS survey extinction data to measure the used to extrapolate forward in time to infer how planetary large-scale column density structure. systems are created. Submillimetre-wavelength thermal continuum emission originates in the cool midplane of these disks and traces the vast majority of the disk vol-

Figure 11: Thermal dust emission observations of the Perseus molecular cloud from SCUBA. The greyscale ranges from -0.2 to +0.2 Jy/bm. Overlaid are extinction contours (from 2MASS) at 3, 5, 7, and 9 mag.

Figure 11 shows the SCUBA observations overlaid with contours of the extinction data. The dense cores detected with SCUBA lie only in regions of high extinction (Av > 5). A similar result was found in the Ophiuchus molecular cloud, although the minimum extinction at which cores were found there was higher (Av ~10 mag; Figure 12: Andrews and Williams (2005), using SCUBA, found evidence of Johnstone et al. 2004). In Perseus, the SCUBA cores dust grain growth, “dust bunnies”, in young protoplanetary disks, such as the represent only a small fraction (1%) of the mass of the one depicted here (Image credit: NASA/JPL-Caltech/T. Pyle [SSC]).

15 JCMT

ume. Andrews and Williams (2005, ApJ, 631, 1134) have recently completed a deep multiwavelength photometry survey of ~150 protoplanetary disks in the Taurus-Au- riga star-formation region with the SCUBA camera. The survey was designed to exploit the stability and sensitivity of SCUBA to probe roughly five times deeper than previous millimetre-wavelength surveys and to provide a much more uniform completeness limit.

With such a large sample, the authors could determine typical values for the characteristic properties of protoplanetary disks. Most of the continuum emission at submillimetre wavelengths is optically thin, making the flux densities sensitive to the total mass in the disk. The inferred distribution of protoplanetary disk masses in the

Taurus-Auriga region has a median value of ~0.005 Msun and a large spread over three orders of magnitude. The spectral energy distribution (SED) of the submillimetre continuum emission from protoplanetary disks is well- described by a power law in frequency, with a median in- Figure 13: Histogram from Andrews and Williams (2005), showing (left panels) that the mass of the circumstellar disk decreases as the disk evolves (younger dex of ~2 between 350 μm and 1.3 mm. Measurements at top, older at bottom). The right panels show how the spectral index de- of the SED shape can be converted into estimates of creases as the disks evolve, implying the growth of dust grains. the sizes of the dust grains in the disks. The results from this SCUBA continuum survey indicate that β ~ 1, and galactic nuclei of an early phase corresponding to the therefore that solid particles have grown to at least a few main growth of the host galaxy and formation of the cen- millimetres in size. This represents growth of ~3 orders tral black hole. Using the observed flux with SCUBA, the of magnitude from the canonical maximum grain size, authors were able to derive a star-formation rate of ~600 compared to interstellar dust. Figure 13 shows distribu- Msun per year, and estimate the dust mass to be Mdust ~ tions of the disk mass and submillimeter spectral index 420 million solar masses. for various disk evolutionary states. Ultraluminous infrared galaxies (ULIRGs) represent a Cosmology and Extragalactic Astronomy truly remarkable class of object and are found both in the local and in the very distant Universe. With far infrared 11 12 In “Submillimetre detection of a high-redshift type 2 luminosities of LFIR > 10 -10 Lsun, these objects emit QSO” (MNRAS, 356, 1571), Mainieri et al. presented the a significant fraction of their total luminosity at infrared first detection (with SCUBA) of a z=3.660 quasar. This wavelengths. A consensus is forming on the origin of this extremely distant galaxy is an ideal candidate for active emission, with massive star-formation being the domi-

16 JCMT

atmospheric absorption severely limits the range of transitions that can be seen from ground-based telescopes for any given high redshift object; it is not uncommon for it to be possible to measure only a couple of molecular

Figure 14: (Left) Spitzer image of the field toward a high-redshift quasar, the most distant detected by SCUBA. The field is 11” across. The big dashed circle is the 5” radius from which the 850 μm flux from SCUBA can be origi- nated, while the smaller circle indicates the Chandra positional error. (Right) A zoom of the central part (5” across) from a VLT image, showing contours of X-ray emission. The large dashed circle is the SCUBA positional error. nant power source. A large fraction of the molecular gas in these objects is in a dense state. The interstellar medium is not just a scaled-up version of that seen in our own galaxy, but one more representative of conditions seen in regions of star formation. Isaak, Papadopoulos and van der Werf (2006, in preparation) have been using the suite of receivers at JCMT to build up a picture of the molecular gas in a sample of ULIRGs. Obtaining spectra has been a slow process, particularly at the highest frequencies, as extremely dry skies are needed. Recently, they reported the first detection of CO(6-5) and CO(4-3) emission from Mrk 231, a ULIRG. Isaak and her collaborators used RxW to obtain CO J=6- 5 and CO J=4-3 spectra from Mrk231 and RxB3 to make observations of the CO J=3-2 and HCN J=4-3 emission. Figure 15: (Top) High excitation CO line emission: CO(4-3) (bold) overlaid on CO(6-5), toward the ultraluminous infrared galaxy Mrk 231. (Bottom) CO(3-2) Their spectra are shown in Figure 15. Their results indi- (bold) and 10x HCN(4-3), both smoothed to a resolution of ~20 km/s. cate that the high-J transitions trace a dense-gas phase that is distinct from a more diffuse state traced by the lower-J transitions, indicating a large mass of very dense lines in objects at cosmological redshift. With the current gas. Their work has important implications not only to generation of radio, mm and sub-mm interferometers, studies of local galaxies, but also to the much more this means, more often than not, that these are the high- distant Universe. Restricted transmission arising from J CO lines. The line ratios, typically r65/r43, are unable

17 JCMT

to set constraints on the physical properties of the gas. This work on Mrk231 has shown that both low and high- J transitions are required, as well as at least one 13CO transition: the latter is critical in discriminating between a cold, dense, optically thick phase and a much warmer, less dense one.

Solar System Projects

On the night of July 3/4, 2005, a NASA satellite, Deep Impact, intercepted and collided with Comet P/Tempel 1. The entire ground-based science team of the Deep Impact Mission published a single paper in Science 310, 265 (“Deep Impact: Observations from a Worldwide Earth-based Campaign”) containing a summary of all data obtained by the group, including RxB data from the JCMT (unfortunately a non-detection). The paper was authored by Karen Meech, along with 208 co-authors, probably a record for a JCMT-related (if in very small part) publication. Although a disappointing result for the

JCMT, the observations nevertheless provided a limit on Figure 16: Moment of encounter of the Deep Impact satellite with Comet the gas production after the impact, helping to confirm P/Tempel 1. The JCMT was part of a large consortium of ground-based that the comet was very dusty and gas-poor. observatories monitoring this mission. Photo courtesy of NASA.

18 JCMT

Operations and Instrumentation

Operations hours of clear time were available for observing; of these 92% were spent observing allocated projects. This figure This section reports on JCMT operations from 1 Janu- rises to 95.5% if one adds the time observed outside ary 2005 until 13 February 2006, at which time the regular hours of operations, e.g., to carry out daytime JCMT was closed for six months of engineering work observations of comets and planets. in preparation for SCUBA-2. This has been an excit- Table 5: JCMT Allocations by Semester and Queue ing, but also difficult, time at the JCMT, and operations during the reporting period were quite challenging. On 05A 05B the one hand, two of the main instruments, SCUBA U.K. 42 47 and the DAS—one or the other of which is required for Netherlands 20 32 all observations—were both retired but caused a lot of frustration and required significant technical attention. Canada 33 29 On the other hand, two long-awaited major new instru- International 5 6 ments, ACSIS and HARP, were delivered and installed University of Hawaii 16 8 on the telescope. Total 116 123 Telescope Usage Weather Table 5 shows the allocated number of projects per observing queue for the observing Semesters 05A (Febru- The JCMT uses five weather grades, ‘1’ being the best, ary 2005–July 2005) and 05B (August 2005–February and Figure 17 shows the relative distribution of the 2006) to be approximately 120 science programmes per grades for each month. Usually, grade-1 weather is semester. In addition to these projects, there were about needed for SCUBA 450 mm and heterodyne 490/690 25 service projects. Not included in the numbers pre- GHz observations. sented are the Director’s discretionary time allocation of eight shifts per semester and engineering and commis- 2005 and early 2006 were interesting in terms of weath- sioning time (E&C: typically 25 shifts/semester). er. Close to 40% of the time was lost to bad weather (including snow and ice) during the first three months More than 200 visiting astronomers, including students, of 2005, but the weather remained better than average observed at the JCMT during Semesters 05A and 05B, throughout most of the rest of the period. In particular, typically for three to seven nights each. the summer months were much better than normal, with about 20% more time available to observing than nor- The nightly observing and the detailed accounting mal. In fact, the weather losses over the period through and progress of the individual science programmes February amounted to 18% compared to 26% over the are tracked by the Observation Management System. previous years. Figure 18 shows the amount of grade Detailed operations statistics and fault rates over the 1–3 weather in 2005/06 compared to the average of reporting period are presented below. A total of 5,137 1989-2003. Not included in the statistics above is March

19 JCMT

Operations Statistics

The Observation Management System, developed at the JAC to provide the logistical support for “dynamical scheduling” and “queue observing” at the JCMT and UKIRT, includes a detailed and comprehensive accounting of the use of the telescopes on a night-to- night basis. Figure 19 shows the operations statistics for the reporting period. A total of 6,340 schedulable hours were available over the reporting period, of which 1,120 (18%) were lost to weather and 83 to facility shutdowns in August and in October for HARP installation work. This left a total of 5,137 hours available for observing. Figure 17: Relative 225 GHz opacities per grade for each month. Of these, 4,054 hours (79%) were accounted towards allocated science programs, with the remaining time of 1,083 hours going to engineering and commissioning observations (678 hours), “other” time (41 hours), and faults (364 hours). One of the sources of “other” time is chauffeuring non-driving observers between HP and the telescope when weather conditions don’t allow for the telescope to be left observing unattended.

Figure 18: The normal amount of grade 1–3 weather in 2005 compared to the average of 1989–2003.

2006 during which time the JCMT was closed. However, unprecedented in history of the JCMT, that month had only 2 nights when the weather was grade-3 or better and 26 nights on which the telescope would have likely remained closed because of bad weather

Figure 19: Operations statistics for the JCMT in 2005.

20 JCMT

Not included in any of the statistics presented thus far in August resulted primarily from a crash of the main are the 314 hours observed in extended time, outside system disk in combination with a failure of its backup the normal operating hours of 05:30 pm to 09:30 am. mirror, both likely resulting from overheating problems. Together these add a significant 6.2% to the total time The overall rise of the fault level can be attributed to observed on projects. Throughout the year, the JCMT lingering problems with the DAS and the increased level operators volunteer the extended time, but some is of development and commissioning work throughout the scheduled daytime observing of comets and planets in- reporting period. volving the local science staff. In this case, about half the extended time was used in support of ACSIS and HARP Instrument Use commissioning in January and February 2006. The four main instruments of the JCMT (SCUBA, RxW, Fault Rate RxB, RxA) are permanently installed on the telescope and can be selected for observations by rotating the The JCMT fault rate is defined as the amount of clear tertiary mirror. Not all instruments require the same time lost to technical faults during the 16-hour nights weather conditions: the higher the observing frequency, the observatory is in operations. The average fault rate the lower the opacity (i.e. water vapor content) needs to for the reporting period of 6.3% represents an increase be. Figure 21 shows the instruments use per weather compared to 2004 and exceeds the operational target grade and indicates that the use is as expected for RxB, of 5%. Figure 20 shows the technical fault rate during RxA, and AzTEC, with RxB dominating the use of grade- each month. The spike in January is associated with 2 weather. SCUBA, which normally dominates grade water damage to the DAS, reported below. The increase 1+2, was hardly available for observing during 05A and

Figure 21: Instrument use per weather grade during Semesters 05A and 05B. SCUBA and RxW were available only part-time during 05A. AzTEC was Figure 20: The monthly JCMT fault rate for January 2005–March 2006. available during three months of 05B.

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was retired in July. Although requested by relatively few cantly affected the schedule of the engineering staff dur- projects, RxW was used extensively and successfully ing this critical period. The Board therefore endorsed a throughout the spring requiring mostly grade-1 and good recommendation to decommission SCUBA in July 2005. grade-2 weather, but was unavailable during Semester SCUBA was one of the most successful and produc- 05B. AzTEC saw almost continuous use during Novem- tive ground-based astronomical instruments of modern ber and December. times: it accounted, over its 8-year lifetime, for roughly 75% of all publications based on JCMT data, and was, at Instruments one stage, ranked second only to the HST in terms of its impact on astronomy. One of its most notable successes Submillimetre Common-User Bolometer Array was the discovery of a large population of massive, (SCUBA) dust-enshrouded galaxies in the early Universe, a class of objects now known universally as “SCUBA galaxies”. SCUBA is the JCMT’s revolutionary submillimetre contin- The retirement of SCUBA marks the end of an era at the uum-array receiver with a 2.3 arc-minute diameter field JCMT. of view, able to observe simultaneously at 850 µm and 450 µm. The instrument developed a cyclic cryogenic Receiver W (RxW) problem in the autumn of 2004. The most likely cause of the problem was helium leaking into the inner vacuum Receiver W, developed at MRAO in Cambridge, is used chamber and then condensing, causing a thermal short. to observe high-frequency spectral lines at the JCMT, This caused SCUBA to slightly warm up, the helium to operating in two atmospheric windows at 430–500 GHz evaporate and to be pumped out, and the instrument to (C band) and 630–710 GHz (D band). The receiver was cool down again. SCUBA was usable, albeit with some very successfully used in the spring of 2005 but suffered sensitivity variation, on 2 nights of the 3-day cycle. With from a cryogenic problem in the summer of 2005. The support from the UK ATC, the lower indium seal was re- cold head started to create a large amount of vibration placed in February 2005. This was considered the most while still keeping the receiver cold. The extra vibration likely place for a helium leak. The replacement changed is the likely reason for subsequent wiring problems in the period to 5 days, but the cycling was still present. the cryostat. Lack of effort due to the commissioning of Further, SCUBA’s dilution fridge developed blockages ACSIS and HARP, as well as the start of the SCUBA-2 after the repair. The reason for the blockage was almost infrastructure work, delayed repairs until 2006, at the certaintly air leaking into the warm part of the gas-han- earliest. During the winter 2005/06, a proposal to convert dling system. Attempts to find and fix the air leak were RxW to a B/D-band receiver for use with the eSMA was unsuccessful. A company with experience in repairing developed and endorsed by the Board. Oxford dilution fridges was contacted to lead further repairs. However, the timescales were such that the Receiver B (RxB) repairs would be finished only 3 months before SCUBA was to be removed from the telescope, in any case, to Receiver B3 is a dual-channel heterodyne receiver for make way for SCUBA-2, and also would have signifi- the 345 GHz atmospheric window (B band), built mainly

22 JCMT

at the National Research Council’s Herzberg Institute of water damage caused intermittent problems throughout Astrophysics. RxB is the workhorse heterodyne receiver the remainder of 2005 and early 2006. operating in the prime observing window of the JCMT. The reliability during 2005 and first quarter 2006 has New Instruments been extremely good, with no significant faults. Receiver B3 will be decommissioned after the commissioning of ACSIS/OCS HARP in the fall of 2006. The Auto-Correlation Spectrometer and Imaging System Receiver A (RxA) (ACSIS) is a multi-channel correlator developed at the Dominion Radio Astrophysical Observatory in Pentic- Receiver A3 is a single-channel heterodyne receiver for ton, Canada, in collaboration with the JAC and the UK the 230 GHz atmospheric window (A band), the low- ATC. The ACSIS correlator has now replaced the old est-frequency operating band for the JCMT. Receiver DAS correlator. The commissioning of ACSIS, together A3 operated reliably during 2005, with minor cryogenic with the new Observatory Control System (OCS), has problems as well as some problems due to the very old been a major challenge. It was not possible to commis- microcomputer. It is running a CP/M operating system, sion ACSIS and the OCS independently, since ACSIS booting from a single-sided single-density 5¼” floppy, requires the new OCS, while the DAS is incompatible which had to be replaced. Replacement components with it. ACSIS was delivered in December of 2004 and have to be found on E-Bay and similar places, since installed in January 2005. they are no longer available through regular commercial channels. Throughout the year, upgrades to the OCS were being implemented in support of the commissioning of Digital Autocorrelation Spectrometer (DAS) ACSIS. In fact, the old, mostly VMS-based OCS was completely replaced with a new Linux-based system that The DAS, built by NFRA in the Netherlands, is the ven- runs on a distributed network of computers. The new erable spectrometer backend for use with heterodyne system replaced all of the software that coordinates and receivers. The DAS was decommissioned and removed controls JCMT observations, except for the telescope in February 2006. The new digital correlator, ACSIS, will control system itself. It consists of more than 50 major replace the DAS. Commissioned in 1992, the DAS has tasks running on over 25 different computers. Similarly, been the longest-running major instrument on the JCMT. new control hardware and software for the Secondary The DAS suffered severe problems after a water leak- Mirror Unit (SMU) were put in place. The SMU, one of age in January 2005. The water caused corrosion on the the most sophisticated of its kind in the world, is critical correlator boards, requiring a major effort to clean and to the operations of the JCMT in that it can chop rapidly restore the spectrometer to service. This exhausted the (typically 8 Hz) between an object and the background last supplies of spare boards and components, many of sky nearby, as well as execute complex patterns on the which can no longer be obtained. Lingering effects of the sky to fill in complete images using sparse receivers, or do both simultaneously.

23 JCMT

The ACSIS laboratory acceptance tests were repeated calibration system. Repair of the three dead pixels and at the telescope with good results. A few faulty boards calibration system is scheduled for September 2006. and units were found and replaced with spares. Further, After further tests and connection to the JCMT comput- it was noted that the cooling for the correlator rack would ers and network, HARP was ready for commissioning in not be sufficient during daytime in the summer, thereby January 2006. Some of the initial commissioning results requiring modifications. The subsequent integration into are already quite spectacular (Figure 24), and reveal the the JCMT system was slow and revealed a large number power of the HARP/ACSIS combination as the world’s of new problems, which are currently being worked on first spectral imager in the 345-GHz atmospheric win- while the JCMT is closed; ACSIS will be released for use dow. An ACSIS/HARP integration period and further with RxA & RxB in late September. commissioning of the receiver will follow the HARP repairs in September.

Figure 22: ACSIS at the JCMT in its environmentally stable enclosure. Figure 23: The newly installed HARP receiver (blue) on JCMT. HARP Telescope and Facility The Heterodyne Array Receiver Programme (HARP) is a 16-pixel heterodyne receiver developed at the Mullard No major faults occurred with the telescope or carousel Radio Astronomy Observatory in Cambridge, UK, in during 2005. The introduction of new software for the collaboration with the JAC, HIA and the UK ATC. HARP SMU and TMU, needed for ACSIS, HARP and SCUBA- was delivered to the JCMT in November 2005. The 2, has lost time due to unintended differences in opera- installation went smoothly, and first light was obtained tion. The surface, as measured with RxH3, was main- December 13th. However, three of the 16 pixels in tained at an accuracy of about 25 µm. HARP were dead, and there were problems with the

24 JCMT

Figure 24: Early commissioning CO(3-2) raster map of Orion obtained with HARP and ACSIS (North is to the right). This image is about three times the size of the full moon, and the total cube has ~170,000 individual spectra covering several spectral lines The observation took about 1.5 hours.

Water Vapour Monitor and Phase Monitor THUMPER, built by Cardiff University, is a seven- element bolometer array operating in the 200-mm The Water Vapour Monitor (WVM) worked without prob- atmospheric window. Observing at this wavelength lems and is used as the prime instrument for measuring requires exceptionally dry and rare weather conditions. the atmospheric opacity when the telescope is observ- THUMPER was installed on the JCMT in March and ing. The phase monitor was removed in 2004, and the April of 2005 and observations were undertaken during SMA is still working on getting new site permission for Director’s Discretionary Time. The major planets were the instrument. To reduce environmental impact one dish detected and imaged in spite of poor weather. will likely be placed on the JCMT carport roof and one on the SMA control building. The Redshift (Z) and Early Universe Spectrometer (ZEUS) was installed on the JCMT in April 2005. The Visitor Instruments ZEUS run was not successful due to bad weather and several instrumental problems. Three visitor instruments were used at the JCMT in 2005 and early 2006. These were THUMPER, ZEUS and From November 2005 through January 2006, AzTEC AzTEC. was brought to the JCMT as a visiting instrument. AzTEC is a 144-element bolometer array camera de-

25 JCMT

veloped at the University of Massachusetts for use in being fabricated, and the instrument is scheduled for the 1.1-mm atmospheric window. A total of 16 scientific delivery to the JCMT in late 2006. programmes, some initially intended for SCUBA, were successfully carried out, not in the least owing to the Because the size and weight of this novel instrument dedicated and enthusiastic support by the visiting Az- requires a completely new support infrastructure, the TEC team members. AzTEC filled a vital hiatus in JCMT JCMT was closed on 13 February for six months of continuum observing between SCUBA and SCUBA-2 engineering work. The project has several components: and produced some impressive results. a new gallery is being built above the control room to accommodate the SCUBA-2 support services; the re- Future Instruments ceiver cabin is being renovated in order to accommodate SCUBA-2 optics, including a new tertiary mirror; the car- SCUBA-2 ousel floor is being reinforced, and a transport system is being installed for handling the SCUBA-2 cryostat; the SCUBA-2 is a new bolometric camera currently be- Nasmyth platform structure, which supported SCUBA, ing developed at the UK ATC in collaboration with the is being replaced with a new mounting frame; and the National Institute for Standards and Technology (USA), computer room is being renovated, including removal Cardiff University, the Scottish Microelectronics Centre, of the DAS and installation of the ACSIS computers. and a consortium of Canadian universities. Building on The scale of the work being undertaken is staggering, the enormous success of SCUBA, SCUBA-2 will provide and the observatory is currently a construction site; it is enhanced sensitivity over a much wider field of view with scheduled to come back on line in August 2006. full (or nearly full) sampling of the focal plane. These en- hancements will be achieved through a number of technical innovations, primary amongst which are the development of transition-edge superconductor detection technology and a novel optical design which utilises as much as possible of the JCMT’s field of view. The result of these innovations, in conjunction with novel scanning and sampling techniques, is that SCUBA-2 will be able to map large regions of the sky up to 1,000 times faster than SCUBA. This revolutionary instrument will open up entirely new paradigms in sub-mm astronomy.

The project was re-approved by PPARC Council in February 2005 and is now fully funded. As part of the JAC’s contribution towards the resourcing of SCUBA-2, the observing night was reduced in January 2006 from 16 hours to 12. The science-grade arrays are currently Figure 25: SCUBA-2 infrastructure work at the JCMT.

26 JCMT

The eSMA equipment was installed in a dedicated bay in the JCMT cabin during June and first fringes between the SMA and JCMT were obtained at 267 GHz on July 12, 2005. After an upgrade of SMA’s tuning software, first spectra at 230 GHz were successfully observed in early October. The eSMA interface equipment for the CSO was delivered in September, and first fringes with the whole eSMA were obtained on October 31. A number of basic operations of the eSMA have been checked out successfully, and the baselines were refined to millimetre Figure 26: First fringes between the SMA and JCMT (Antenna 8). The fringes accuracy. After the JCMT is re-commissioned in Septem- start wrapping, due to a still imprecisely determined baseline between the JCMT and SMA antennas. ber 2006, we plan to continue with phase stability and imaging tests and the switchover to 345 GHz. A one- eSMA year pilot programme will follow this.

The eSMA is a collaboration between the SMA, the Starting in late 2006, the SMA will add 400-GHz receiv- JCMT, and the CSO to join into a single sub-mm inter- ers to the frequency line-up. These receivers overlap ferometer array with approximately twice the collecting with their 300 GHz receivers over most of the 345 GHz area of the SMA resulting in an increased sensitivity. The window but observe the orthogonal polarization. For the eSMA will operate part-time and in the 345 GHz sub-mm eSMA to take advantage of this dual-polarization ca- window, taking full advantage of Mauna Kea’s excellent pability the 460 GHz channel of RxW will be converted observing conditions and prolonged periods of superb to 345 GHz. Development of new 345-GHz mixers and weather at that frequency. The first initiatives for the a re-design of the optics has started at MRAO. The eSMA started in 1996, well before the completion of the new mixers are based on the HARP mixers and should SMA itself, and the special fibre-optics connections were provide the JCMT with a superb dual-polarization single- installed several years ago. Following the commission- pixel 345 GHz receiver. We plan to reinstall a converted ing and the start of operations of the SMA, the practical and upgraded RxW in the autumn of 2006, and, once in implementation of the enhanced interferometer has now place, it will become the primary receiver for observing begun. In May 2005 the JCMT took delivery of the inter- with the eSMA interferometer. The eSMA effort at the face equipment, built by the Smithsonian Astrophysical JCMT has been, in part, supported by a special NWO-M Observatory, consisting of a SMA-style antenna compu- grant from the Netherlands Organization for Scientific ter and LO and IF signal processing units. These enable Research. the JCMT receivers to tune to the modulated LO signal originating from the SMA and to ship the resulting IF signal back to the SMA correlator.

27 UKIRT/WFCAM image of the centre of the Milky Way galaxy, in the K-band filter. Preliminary reduction of data taken in engineering time at the start of the spring 2006 WFCAM block. A subset of a full WFCAM tile is shown. P. Hirst, JAC.

28 JAC Technical Support

The Software and Computing Services, and Engineering remodelling of the JCMT computer room, networking and and Technical Services Divisions provide specialist sup- computer communications systems. port to both telescopes. Major project work is highlighted in previous sections dedicated to UKIRT and JCMT instru- The Engineering and Technical Services (ETS) Division mentation. provides routine maintenance, operational improvements and project support to both JCMT and UKIRT, as well as to The Software and Computing Services (SCS) Division is the JAC Hilo sea level facility. The group includes engineers made up of three groups: the Scientific Computing Group, and technicians with skills in the mechanical, electrical and the Instrument and Telescope Software Group and the electronic, cryogenic, vacuum and instrument disciplines. Computer Systems Group. SCS’s main role is to support all of the software that runs at both telescopes, as well as The past 12 months have been a particularly busy year the software provided to users for observation planning and for the ETS Division. Key activities have included the final scientific analysis. Much of the time spent by this group in- adjustment of the WFCAM detector focus, integration of volves tracking down faults reported by the telescopes and HARP and, most significantly, preparations for the arrival of facilitating and coordinating the solutions to them. SCUBA-2. Work on HARP and SCUBA-2 duties occupied the majority of the teams’ time and required careful plan- This year the Scientific Computing Group designed and ning and co-ordination of many different activities. This started development of the JCMT Science Archive. They culminated in the shutdown of JCMT in February 2006 to also put considerable time into the design and development allow the SCUBA-2 infrastructure work to be undertaken. of the SCUBA-2 Data Reduction Pipeline and the WFCAM The scale of the infrastructure work is beyond anything Data Reduction Pipeline. The group is also managing the attempted previously by the ETS and required augmenting transfer of responsibility for the Starlink software and up- the workforce with agency staff. The work is scheduled to grades to the Observational Tool (OT) software. complete in August 2006. In addition to these specific activities, the ETS team have The Instrument and Telescope Software (ITS) Group has continued to deliver the necessary levels of service to keep been mainly focussed on JCMT as three major systems UKIRT and JCMT operational including several WFCAM/ were being commissioned there: ACSIS, the OCS and Cass cluster changeovers for UKIRT, and the “nurse-maid- HARP. Included in this work was an upgrade to the JCMT ing” of both the DAS and SCUBA at the JCMT. Ultimately, secondary mirror unit (SMU), which replaced all of its digital the battle to keep SCUBA operational was lost, and with a control hardware and software. Additionally, this group great sense of disappointment the instrument was retired in planned the changes to the UKIRT OCS to accept UIST 2005. with a new array controller. Finally, turnover of staff in the Division has been relatively The Computer Systems Group is constantly upgrading the low across the period of this report, but a notable departure IT systems at the JAC. They recently changed the Sun Mi- was that of Neal Masuda, who had worked at the JAC for crosystems-based file servers over to Linux-based servers. more than 18 years. He will be missed, and we wish him They also planned and implemented a total overhaul and well.

29 Administrative Division

The JAC Administration Division provides a Human Re- security system and an overhaul of the JAC library. The sources service and Financial Management environment former has provided secure access to the building and that are both responsive and proactive to the needs of the improved out-of-hours security. The latter was a signifi- JAC and its staff. In addition, the Division takes the lead cant project, largely conducted in-house, which required role in satisfying the corporate and accountability require- the weeding of hundreds of journals, the re-cataloguing of ments set by the JAC’s parent organisation, the Particle some 1,044 books and the elimination of a termite problem Physics and Astronomy Research Council (PPARC) based discovered in one of the bookshelves! The library re- in the United Kingdom. opened formally in February 2006 and provides a comprehensive reference library for both the JAC and neighbour- ing observatory staff. A key project in 2005/06 was the introduction of a new, corporate (i.e., PPARC-wide) accounting and finance system. And, finally, our collaboration with the University of Vic- While a key feature of the new system is to improve and toria, British Columbia, continued to go from strength-to- streamline corporate reporting requirements, early con- strength, with two students completing work placements in cerns existed about the ability of the system to meet local autumn 2005 and spring 2006. In addition another student, information needs. The JAC finance team made important from Quebec’s Universite de Sherbrooke, spent four contributions to the testing of the system and, by the end of months at the JAC under sponsorship from the Canadian the financial year, confidence had increased significantly. It Research Council’s Women in Engineering and Science has been a difficult transition, but the system is now begin- programme. ning to meet JAC needs and, importantly, the end-of-year accounts were completed using the new system.

The emerging HR challenge in 2005/06 has been the retention of staff. Having released a number of individu- als under restructuring proposals agreed to in 2003, the continued uncertainty around the long-term futures of the telescopes has proved unsettling for the remaining staff. As a result, there has been a higher than normal interest in vacancies with other organisations. The HR team has continued to work with the Research Corporation of the University of Hawai’i (RCUH), who provide the majority of our staff, to maintain our competitiveness in the job market. This has included the development of career progression tables for functional groups and the examination of pay- ment of performance-related bonus awards.

Two further projects overseen by the Administration Divi- sion in the past year were the installation of a new building Anna Lucas re-opens the JAC library.

30 Science Education and Public Outreach

Science education and public outreach continues to be Tempel 1, which were the first detections of this event by an important part of JAC activities with an audience that any observatory. This event was the topic of several press extends from the local community in Hawai’i to the wider events in Hilo and the UK, in which JAC staff participated. public and science community across the globe. With The UKIRT WFCAM Orion First Light image was the “As- increasing emphasis on the need to improve scientific study tronomy Picture of the Day” on 6 January 2005. WFCAM in schools, it is ever more necessary for science institu- was also featured in an article written by staff for the UK tions to provide inspiration and tools for science education, “Astronomy Now” magazine. UKIRT’s 25th Anniversary was as well as educate the voting public on scientific issues, featured in the Winter 2005 issue of “Frontiers.” enabling them to participate in public debate and make The `Imiloa Astronomy Education Center of Hawaii (for- informed decisions. merly the Mauna Kea Astronomy Education Center) in Hilo opened in February 2006. It includes a number of exhibits JAC staff took part in a number of public events dur- featuring UKIRT and JCMT science results and profiles ing 2005 and the first quarter of 2006. In May 2005, JAC some JAC staff members. JAC continues to be part of the participated in the annual AstroDay at the Prince Kuhio Mauna Kea Observatories Outreach Committee (MKOOC). Plaza—the largest shopping mall on the island—setting up This committee, consisting of outreach officers from all the a booth with educational activities and handouts. This event observatories on the Big Island and `Imiloa, discusses and was the premier public astronomy event of the year and coordinates local outreach efforts. Larger projects included featured attendance by the local mayor, many public school the renovation of the Mauna Kea Visitor Information Station groups, all observatories, and many other local institutions. at Hale Pohaku. More than 15,000 people attended this event. Other events Outreach officer Douglas Pierce-Price left the JAC in Oc- included public talks at the Mauna Kea Visitor Information tober of 2005, and Inge Heyer joined as the new outreach Station as part of the “Universe Today” series and partici- officer in March 2006. pation in the regular “AstroTalk” forum at the University of Hawai’i at Hilo.

In January 2006, the JAC welcomed the BBC’s “Sky at Night” team and the filming of a programme entitled “On Top of the World.” The programme, which aired in the UK in February 2006, showcased science undertaken primarily at the JCMT and UKIRT, and included interviews with a number of staff.

UKIRT and JCMT science results were featured in a number of media articles, both in print and on the web. Main topics capturing the media’s interest were the Ex- tended Groth Strip galaxy survey, stellar disks and planetary system formation. A press release was issued on UKIRT’s observations of the Deep Impact mission to Comet JAC staff take part in AstroDay 2005.

31 Appendix

Staff Organisation in 2005/6

JAC HAWAII

Gary Davis Director JAC

Remo Tilanus Per Friberg Andy Adamson Craig Walther Simon Craig Stuart Putland (from 02/06) Head of JCMT Head of JCMT Associate Director Head of Software & (from 03/05) Wendy Light (to 03/06) Operations Instrumentation UKIRT Computing Services Chief Engineer Head of Administration

UKIRT Software & Computing Engineering & Technical JCMT Administration Outreach Services Services Timothy Carroll Vicki Barnard (to 06/05) Christine Campbell Inge Heyer (from 03/06) Christopher Davis Bradley Cavanagh Ken Brown Harold Butner (to 02/06) (from 09/05) Douglas PiercePrice Lucas Fuhrman Kynan Delorey Timothy Chuter Iain Coulson Velvet GonsalvesNases (to 09/05) Paul Hirst Shaun DeWitt (to 06/05) Tomas Chylek Jeff Cox (to 12/05) Sharlene Hamamoto Jonathan Kemp (50%) Frossie Economou Vernon DeMattos Donna DeLorm Ian Midson Thomas Kerr David Fuselier Marjorie Dougherty James Hoge Sally Nicol (to 10/05) Sandy Leggett Sam Hart (from 01/06) Mark Horita Jonathan Kemp (50%) Susan O'Neal Anna Lucas Maren HauschildtPurves Lenwood Jack Jamie Leech (50%) Felisa Teramoto Mark Rawlings Timothy Jenness James Kaulukukui Ed Lundin (to 12/05) (Vacancy) (from 04/05) Russell Kackley John Kuroda Gerald Schieven Watson Varricattu Jamie Leech (50%) Neal Masuda (to 03/06) Benjamin Warrington (to 11/05) Firmin Oliveira Robert Oliveira Jan Wouterloot Thor Wold Matt Rippa (to 03/06) John Pascual Ming Zhu Henry Stilmack Alan Rosario (03/05 to 10/05) Edward Sison 32 Erik Starman Jay Tsutsumi (Vacancy x2) Appendix

JAC HAWAII

Gary Davis Director JAC

Financial Statement 2005–2006

The financial statement below refers to the financial year from 1 April 2005 to 31 March 2006. The JAC is funded via the UK’s Science Budget through the Particle Physics and Astronomy Research Council (PPARC) with contributions towards the JCMT from the Canadian National Research Council (NRC) and the Netherlands Organisation for Scientific Research (NWO).

Operational costs US $ (000s) Capital costs US $ (000s) Expenditure Expenditure JCMT¹ Running costs 1,632.8 JCMT New instrumentation 3,291.4 Observing costs 494.2 Total 3,291.4 Maintenance 873.5 Astronomical Research 92.3 Income Development 1,003.7 JCMT PPARC (UK) 3,92.9 Total 4,096.5 NRC (CA) 82.5 UKIRT Running costs 1,602.2 NWO (NL) 116.0 Observing costs 568.0 Total 3,291.4 Maintenance 673.5 Astronomical Research 149.3 Development 24.5 Total 3,017.5 Income JCMT PPARC (UK) 2,393.8 NRC (CA) 1,008.4 NWO (NL) 694.3 Total 4,096.5 UKIRT PPARC (UK) 3,017.5 Total 3,017.5 ¹ Excludes the cost of 4.8 staff members seconded to the JAC by the partner countries.

34 Appendix

35 Appendix

Telescope Time Awards (UKIRT)

UKIRT Allocations, Semester 2005A (UK PATT) PI Title of Investigation Hours Summit Status* Banerjee Exploring the Circumstellar Environment of the Nova-Like Variable V4332 Sgr 4 Bower Galaxy Formation through the Cosmic Microscope - A Spatially Resolved Study 18 Bower Watching Clusters Grow: Mapping the Cosmic Web around High-Redshift Clusters 30 Brocksopp Trigger and Outburst Mechanisms of X-ray Transients 5 Brookes High Redshift Evolution of Radio Sources Using Improved Photometric Redshifts 29 Chapman Restframe Optical Emission-Line Maps of a New Sample of Confirmed High-z Spitzer... 42 yes Crawford Investigating the Excitation of the Emission-Line Gas in the Perseus Cluster 40 yes Dunlop Deep K-band Imaging of the Most Massive Galaxies at z ~ 2 30 Evans IR Observations of SIRTF ToO Novae 10 Evans The Infrared Evolution of V838 Mon 20 Fasano WFCAM Imaging of WINGS Galaxy Clusters 40 Froebrich Star Formation in IC1396W—The NIR View 17 Gledhill Near-IR Morphology of Magnetised Post-AGB Stars 21 yes Irwin A WFCAM Near-Infrared Survey of Local Group Galaxies 12 Jarvis AGN Feedback Processes in Massive Galaxy Formation 30 Kotak CO in Type Ic/IIn Supernovae and the Origin of Dust in the Early Universe 8 Kumar The Nature of Ring Shaped Proto-Clusters and the Formation of Small Clusters 13 yes Lowe Using H2 to Investigate the Onset of Fast Winds in Post-AGB Stars 27.7 yes Lumsden Near-Infrared Spectroscopy of Massive YSO Candidates 20 Miller Deep Impact on Comet Tempel-1 12 yes Oka Studies of Hot and Diffuse Gas near the Galactic Center Using Metastable H3+ 30 Oliveira L’-band Observations of Young Low-Mass Stars and Brown Dwarfs Near Sigma Ori 40 yes Peletier Opening up Unexplored Areas—Creating a Large Stellar Library in the NIR 50 Peletier The Formation of Spiral Bulges 30 Pinfield Turbulent Weather Phenomena in Ultracool Dwarf Atmospheres: Time Resolved NIR.. 26 Rawlings The AMI+WFCAM Survey of Distant Clusters 45 Rigby The Space-Density of High Redshift FRI Radio Galaxies, Part 2 15 Sarre Evolution of 3.3 um UIR Bands in Extended Objects 8 Simpson AGN Feedback and the Formation of Giant Ellipticals 30 Stallard The Characteristics of Saturn’s Auroral Atmosphere: Cassini Support Observation 15 yes

36 Appendix

UKIRT Allocations, Semester 2005A (UK PATT) PI Title of Investigation Hours Summit Status* Tanvir Rapid IR Follow-up of GRBs: Searching for Dark and Distant Afterglows 35 Van Loon Monitoring AGB Variables in M33: Star-Formation History, Chemical Enrichment.. 13 Verhoelst Probing the Upper Atmosphere of Cool Carbon Stars 2 Wilman Mapping the Hot Molecular Hydrogen in Cooling Flow Cores 27 yes

* Summit status: In the UKIRT flexing model, the observer at the summit observes their own project if (and only if) its weather requirements are met and there is time remaining on it. Otherwise they observe projects from the OMP queue. Thus summit status can be important and the TAG generally allocates it to top-ranked projects or those with very stringent weather requirements.

UKIRT Allocations, Semester 2005A (UH) PI Title of Investigation Hours Summit Status* Connelly UKIRT L’ Imaging Survey for Binary Young Stellar Objects 1.5 Cowie SMA Observations of the SCUBA Deep Field Sources 4 Dundon Spectroscopy of Comet-Asteroid Transition Objects 4* Hodapp Wide-Field Survey of Molecular Hydrogen in Star-Forming Regions 2* McGrath Characterization of the Luminosity Function for mJy Radio Sources 1x0.5*** McGrath Formation and Abundance of Galaxies with Old Stellar Populations at High z 2x0.5*** Rizzi Near Infrared Observations of Dwarf Galaxies in the Local Group 2x0.5 Sanders Hawai’i Imaging (UV/NIR/mm) of the HST-ACS Cosmos 2 Degree Treasury Field 5x0.5** Sanders K’-band Imaging of Luminous Infrared Galaxies in the IRAS RBGS Sample 7.5*

* Allocated time in the extensions of the semester (December 2004, August 2005) ** Allocation was 10x0.5 nights, but this was not possible to schedule. *** Flexed with engineering early in the April WFCAM block.

37 Appendix

UKIRT Allocations, Semester 2005A (Japan) PI Title of Investigation Hours Summit Status* Fujiyoshi Revealing the Magnetic Structure in a Circumstellar Envelope 1 Kodama Watching Clusters Grow: Mapping the Cosmic Web Around High Redshift Clusters 1 Motohara Probe the Assembly of Galaxies and Large Scale Structure in z~4 Universe 2 Nakajima IMFs in the M17 Massive Star-Forming Region 2 Pyo [FEII] l1.644mm Survey for Embedded Low-Mass YSOs in TMC (II) 1

UKIRT Allocations, Semester 2005B (UK PATT) PI Title of Investigation Hours Summit Status* Bower Watching Clusters Grow: Mapping the Cosmic Web around High-Redshift Clusters 33 Fasano WFCAM Imaging of WINGS Galaxy Clusters 40 Gunn The Evolution of the Sub-mJy Radio Population: WFCAM Imaging of a GMRT Deep... 44 Irwin A WFCAM Near-Infrared Survey of Local Group Galaxies 25 Jameson Constraining the Mass Function of the Pleiades into the “Planetary’’ Regime 40 Littlefair A Search for Pulsating, Young Brown Dwarfs 44 Lucey An Optical-NIR Study of Galaxy Bulges and Disks in Nearby Rich Clusters 6 Smail A WFCAM Survey of Star-Forming Galaxies at z=2.2 in the UKIDSS UDS and COSMOS 18 Van Loon Monitoring Red Giant Variables in M33: Star-Formation History, Chemical... 15

UKIRT Allocations, Semester 2005B (UH) PI Title of Investigation Hours Summit Status* Cowie Large-Scale Structure and Correlation Functions of AGN at z<3 4 Hodapp Jet Morphology and Excitation in NGC1333 1 Hodapp The Frequency of FU Orionis Events in M33 1 Kakazu A Wide-Field Optical Survey for High-Redshift Quasars 1.6* McGrath Origins of the Earliest Massive Galaxies 2+7 Reipurth A Wide-Field Molecular Hydrogen Survey in Perseus 2 Sanders Hawaii NIR/mm Imaging of the HST-ACS COSMOS 2-Deg2 Treasury Field 3

* indicates projects allocated time after the initial UH TAG meeting.

38 Appendix

UKIRT Allocations, Semester 2005B (Japan) PI Title of Investigation Hours Summit Status* Goto Infrared Photometry of Distant Galaxy Cluster CL0910+5422 at z=1.1 1 Kodama Watching Clusters Grow: Mapping the Cosmic Web Around High-Redshift Clusters 2 Takata Scale of a Protocluster Traced by Massive Red Galaxies 1

UKIRT just after sunset on Mauna Kea in Hawai’i. Photo by Nik Szymanek.

39 Appendix

Telescope Time Awards (JCMT)

JCMT Allocations, Semester 05A (United Kingdom) PI Title of Investigation Hours Barnard V ToO SCUBA Observations of Gamma-ray Burst Afterglows in the Swift Era 24 Chrysostomou A Magnetic Fields in High Mass Protostellar Objects 16 Chrysostomou A Submillimetre Polarimetry of SgrA* and the Central Few pc of the Galaxy 28 Coulson I Sub-mm Observations of Comet Tempel 1: The Deep Impact Experiment 47 Crutcher R A Complete Description of the Magnetic Field in W3OH 8 Curran R Hydrostatic Facades of Turbulent Cores 8 Dunlop J The SCUBA/BLAST Wide-Field Extragalactic Survey 240 Edge A CO(2-1) and CO(3-2 ) in Cygnus-A—Feeding the Monster? 5 Evans A Monitoring CO Emission from Sakurai’s Object (V4334 Sgr) 2 Evans A Sub-mm Photometry of Sakurai’s Object 2 Fabbri J Neutral Carbon Observations of Three Low-Metallicity HII Galaxies 20 Fuller G Mapping High Mass Infall Candidates 31 Gao Y Dust, Gas, and Starbursts along a Merger Sequence: Completion 28 Greaves J Debris around Sun-like Stars 10 Greaves J Exploring a New Population of Debris Disks 20 Hughes D Identifying New Primary Flux-Calibrators at Sub-mm Wavelengths for BLAST, SOFIA... 16 Hughes D The Protocluster Environment of High-redshift Radio Galaxies 24 Iono D Imaging the 1.1mm Dust Continuum in the Antennae Galaxy 8 Kramer C The Dust Grain Opacity at Sub-mm Wavelengths 24 Mack K SCUBA Observations of the CORALZ Sample: The Dust Contents in Nearby Young Radio... 16 Millar T Mapping CO, 13CO and C18O in Edge Cloud 2 (EC2) 22 Millar T Multi-species Mapping of IRAS 16293-2422—A Chemical Clock—Continued 24 Nandra K The Link between Sub-mm Galaxies and the Most Active Lyman Break Galaxies 16 Nikola T ZEUS Observations of ULIG Galaxies: Energy Sources, Starburst Histories, and the [CII]... 16 Page M Measuring the Far Infrared Output of X-ray Bright, Intermediate Redshift Type-2 QSOs 16 Papadopoulos P Tracing Metal-rich H2 Mass in Exteme Environments 8 Rawlings J Initial Conditions of Star Formation: Molecular Tracers in L134 24 Rawlings J A Test of Surface Hydrogenation and Desorption in Molecular Clouds 32 Redman M The Two Classes of Starless Cores 24 Rigodopoulou D A New Class of Dusty Lyman Break Galaxies: The Missing Link 12 Rigodopoulou D Are Galaxy Spheroids and Massive Black Holes Co-eval? 24 Rowan-Robinson M The Sub-mm Properties of z>1 Starbursts & AGN Selected in the Mid-Infrared 16

40 Appendix

JCMT Allocations, Semester 05A (United Kingdom) PI Title of Investigation Hours Smail I Tracing the Formation of Elliptical Galaxies in Large Scale Structures at z=2-4 42 Stacey G [CII] Emission from High z Galaxies: Characterizing the Starbursts 16 Stevens J The Clustered Formation of Massive Galaxies 40 Takagi T Unveiling the Star-Formation Activity in a Proto-Cluster Region at z~5 16 Viti S From Proto- to Evolved PN: Using CO+ to Probe the Evolution of PNe 24 Wakelam V Sulphur Chemistry and Hot Corinos 35 Weinberger R Unravelling Some of the Nearest Knots: SCUBA Archaeology of a Nearby Fossil Bipolar... 24 Zijlstra A Dusty Disks and Magnetic Fields in Planetary Nebulae 8 Wilson G 1100um Imaging of the Spitzer FLS Verification Strip 32 Zijlstra A Dusty Disks and Magnetic Fields in Planetary Nebulae 8

JCMT Allocations, Semester 05A (Canada) PI Title of Investigation Hours Borys C The Radio-FIR Correlation at High-z: 450mm Photometry of Sources in GOODS-N 28 Brooks S 12CO 3-2 Emission Line Observations of BIMA SONG Galaxies 40 Butner H Dust Properties of Comets: Sub-mm Observations 16 Butner H Sub-mm Observations of Comet Tempel 1: the Deep Impact Experiment 21 Butner H Tracing H2CO in Low-Mass Protostar Environments 16 De Buizer J Search for SiO Outflows from Young Massive Stars with Linearly Distributed Methanol Masers 18 Fich M Characterizing the Gas in the Bipolar Outflow NGC 2264 G 32 Fiege J Origins of the Filamentary Trunks of the Eagle Nebula 25 Jayawardhana R Probing the Evolution and Physical Properties of Brown Dwarf Disks 40 Johnstone D Polarimetry of a Star-Formation Chain in Taurus 37 Kalas K SCUBA Observations of a Nearby Debris Disk at Age 1 Gyr 10.4 Kirk H COMPLETE-ing the SCUBA-Mapping of the Ophiuchus Molecular Cloud 45 Klaasen P A Study of Remnant Outflows from High Mass Protostellar Objects 23 Knee L Molecular Outflows in the R Coronae Australis Region 44 Leeuw L Kinematics, Structure, Origin and Evolution of Dense Gas in the Centre of Centaurus A 24 Leeuw L Polarised Sub-mm Emission in the Nucleus and Circumnuclear ~2.3kpc Diameter of Cen A 12 Matthews B A Survey for Debris Disks across Spectral Types to the Substellar Threshold 24 Matthews H A 850mm SCUBA Survey of the Galactic Plane 16 Matthews H Oort Cloud Comets: A Long-Term Target-of-Opportunity Program 48

41 Appendix

JCMT Allocations, Semester 05A (Canada) PI Title of Investigation Hours Matthews H Temporal and Latitudinal Dispersal of Trace Species in the Jovian Stratosphere 36 Muehle S Tracing the Properties of the Molecular Gas in the Metal-poor Starburst Galaxy NGC 1569 48 Plume R Deuterated Water in Cold Molecular Clouds 36 Plume R Electron Abundances and Magnetic Support in a Quiescent Protstellar Core in Ophiuchus 58.2 Poidevin A Multi-scale Analysis of Magnetic Fields in Filamentary Molecular Structures in Orion 43 Redman R Cores, Disks and Protostars in the G79.27+0.34 Infrared-dark Cloud 41 Redman R Protostellar Outflows and Gas Temperatures in IRDC Cores Identified by SCUBA and... 48 Sajina A The Nature of Spitzer-Selected Galaxies at z~1-2 32 Schieven G L1340: Bridging the Gap between Low and High Mass Star Formation 13 Schieven G ToO SCUBA Observations of Gamma-ray Burst Afterglows in the Swift Era 16 Scott D A Uniform SCUBA Survey of the Spitzer GOODS-North Field 64 Wu Y Characteristics of High Mass Sourceless Cores 30 Yee H Excess of Sub-mm Sources in High-Redshift Galaxy Clusters 40

JCMT Allocations, Semester 05A (Netherlands) PI Title of Investigation Hours Augereau J Disks around Pre-Main Sequence Stars 43 Baes M The Interstellar Dust and Dark Matter Content of Elliptical Galaxies 36 Bisshop S Testing Grain-Surface Astrochemistry 72 Ceccarelli C Is Cold H2 a Major Constituent of the Dark Matter? 41 Decin L Submillimeter Observations of Normal K/M Giants: Probing the Temperature Distribution... 11.6 Dominik C HDO in Young Protostellar Disks 16 Frieswijk W Gas Properties of Infrared Dark Clouds 33 Frieswijk W Temperature and Density Structure of Outer Galaxy Infrared Dark Clouds 18 Israel F J=3-2 13CO Absorption Line in Cen A 15 Israel F The Nature of the ON-1 Star-Forming Region 14 Israel F ZEUS Investigations of the Barred Spiral Galaxy M83: Feeding the Nuclear Starburst 32 Rottgering H SCUBA Observations of BzK Starbursts at z=2: Early-type Galaxies in Formation? 25 Shipman R The Temperature and Density Structure of Infrared Dark Clouds 22 Stuwe J Sub-mm Observations of Comet Tempel 1: The Deep Impact Experiment 17 Tielens A Unbiased Spectral Survey of the Low-Mass Protostar IRAS16293-2422 45 Tilanus R ToO SCUBA Observations of Gamma-ray Burst Afterglows in the Swift Era 16

42 Appendix

JCMT Allocations, Semester 05A (Netherlands) PI Title of Investigation Hours van Dishoeck E The Environment of Young Stellar Objects in Lupus Observed with Spitzer 52 Waters R Discs around Binary Post-AGB Stars 28 Webb T Making MUSYC with SCUBA: A Sub-mm Study of Distant Red Galaxies 64 Wijers R Sub-mm Photometry of Two Extreme GRB Host Galaxies 8

JCMT Allocations, Semester 05A (International) PI Title of Investigation Hours Abada-Simon M Coordinated Observations of Non-Thermal Flares from AE Aquarii 16 Gras-Velazquez A Probing the Missing Link between Weak-Line and Classical T Tauri Stars 20 Hill T Probing the Very Earliest Stages of Massive Star Formation 16 Mack K Dust in Radio-loud Broad Absorption Line Quasars 4 Sandell G Probing the Physical Conditions of the Youngest High-mass Star ever Found 29

JCMT Allocations, Semester 05A (University of Hawai’i) PI Title of Investigation Hours Andrews S Passive Disks and the Transition from Dust to Planetesimals 48 Botticelli S The Density Structure of the Inner Envelope of IRAS16293 from H2CO Emission 8 Botticelli S Single Dish Survey of Complex Organic Molecules in Massive Hot Cores 8 Brogan C JCMT Observations of Spitzer Filamentary Dark Clouds 16 Cowie L An Intensive Survey of the Hubble Deep Field North 32 Henry P Do Massive Galaxy Bulges and Black Holes Form Together? 32 Hodapp K Star-Formation in IC 1396 W 16 Liu M Masses of Disks around Young Brown Dwarfs 32 Meech K The Deep Impact Mission 56 Stanke T Submillimetre CO Imaging of Protostellar CO Jets—Paving the Way! 32 Williams J Measuring the Masses of Planetary (Debris) Disks 16

JCMT Allocations, Semester 05B (United Kingdom) PI Title of Investigation hours Allsop J An Unbiased Search for Outflows in the W3 Giant Molecular Cloud 48 Bell T From Proto- to Evolved PN: Using CO+ to Probe the Evolution of PNe 36

43 Appendix

JCMT Allocations, Semester 05B (United Kingdom) PI Title of Investigation hours Bonnell I Testing Cluster Star-Formation Simulations: The Case of Orion B 24 Bontemps S Probing the Warm, Inner Envelope Regions along the Evolution Line of Massive Protostars 18 Buckle J Depletion and Evolution in Prestellar Cores 65 Buckle J Momentum Transfer through Molecular Outflows Driven by Slow-Precessing Protostellar Jets 60 Dent W T Tauri stars in Taurus: A Magnitude-Limited Survey 60 Dent W The Gas Mass of the Disc around HD169142 16 Dunlop J (AzTEC) The SCUBA/BLAST Wide-Field Extragalactic Survey 200 Edge A CO(2-1) in Cygnus-A—A Challenge for ACSIS 5 Emprechtinger M Gas-Phase Depletion in the Eastern Core of IC5146 30 Evans A C2H in Sakurai’s Object 6 Evans A Monitoring CO Emission from Sakurai’s Object (V4334 Sgr) 6 Fuller G CO Depletion towards HMPOs 40 Fuller G Imaging Important Transitions in the 230GHz Band towards the SLS Targets 46 Fuller G Probing the Chemical Content of AFGL 2591 70 Fuller G The Outflows from High Mass Infall Candidates 21 Greaves J Confirming the Gas Disk around Brown Dwarf 2MASS 1207-3932 20 Greaves J Mapping Gas Flows in AB Aurigae’s Extended Disk 16 Hatchell J (AzTEC) Is there an Av Cutoff for Star-Formation 12 Hatchell J Depletion in Perseus Star-Forming Clusters 56 Herpin F S-bearing Molecules in High Mass Protostellar Objects 30 Hughes D (AzTEC) Large-scale Structures and the Protocluster Environment of a High-Redshift Radio... 48 Isaak K CO J=6-5 Emission in ULIRGs: Establishing the Properties of the Dense and Warm Gas 35 Jimenez-Serra I Physical Conditions and Chemistry along the Evolution of Shocks in the Young L1448-mm... 32 Lintott C A First Investigation of Sulphur Chemistry in M82 24 Marscher A Probing Blazar Jets through Multiwaveband Polarization Variability 48 Martin S The Physical Conditions and the Chemistry in the Nucleus of the Starburst Galaxy NGC253 27 Martin-Pintado J The Physical Conditions in the Nucleus of ARP220 42 Moore T (AzTEC) Core Formation in Contrasting Molecular-cloud Environments 30 Nisini B Probing the Excitation of EHV Protostellar Jets through CO Multifrequency Observations 28 Papadopoulos P A mm/Sub-mm CO, HCN Line Survey of Luminous IR Galaxies 20 Papadopoulos P CI emission in Ultra Luminous Infrared Galaxies 54 Pestalozzi M Studying the Environment of New Methanol Masers 24

44 Appendix

JCMT Allocations, Semester 05B (United Kingdom) PI Title of Investigation hours Redman M Searching for Wriggles in the Snake Nebula, Barnard 72 35 Richer J Probing Early-Stage Low-Mass Star Formation with Sub-mm Line Emission 38 Roberts H A Search for ND in L1544 and L694-2 33 Roberts H A Survey of OCS in High- and Low-Mass Protostellar Envelopes 35 Smail I (AzTEC) A Panoramic AzTEC/Spitzer/HST Survey for Obscured Activity in Clusters at z~0.5 30 Thompson M A Search for Infall Toward High-Mass Precluster Cores 88 Verma A [CII]158 in a Young Universe: A Search in a UV-Luminous z=6.17 Lyman-Break Galaxy 34 Verma A A CO Line Survey of Hyperluminous Infrared Galaxies 28 Wakelam V Sulphur Chemistry and Hot Corinos 8.5

JCMT Allocations, Semester 05B (Canada) PI Title of Investigation hours Butner H Massive Star Migration, or Formation, at the Galactic Centre? 15 Caselli P Probing the Chemical Evolution of the Early Universe 35.1 Chapin E (AzTEC) An AzTEC 1.1 mm Confusion-Limited Map of GOODS-N 90 Cote S CO in the Dwarf Irregular Galaxy WLM 36 Di Francesco J A CO (2-1) Line Search for Disks around Brown Dwarfs 38 Fich M The Effect of HII Regions on Star Formation 61 Fong D Imaging the Extended Structure in the PN NGC 7027 11.3 Jorgensen J Dynamics of Low-Mass Protostars Observed at High Angular Resolution with the JCMT+SMA 32 KertonC (AzTEC) Observing the Earliest Stages of Massive Star Formation with AzTEC 26 Klaasen P Possible Remnant Outflows from High-Mass Protostellar Objects—Part II 27 Knee L A Cluster of Outflows in Corona Australis 44 Lefloch B SiO Emission in Protostellar Outflow Shock Regions 28 Li D Blue and Red Velocity-Shifted Components in L1544—Molecular Bullet or Cloudlets? 34 Matthews H Oort Cloud Comets: A Long-term Target-of-Opportunity Program 48 Matthews H The Molecular Component of Dust Galactic Regions 38.3 Mohanty S (AzTEC) Dusty Disks around Young Brown Dwarfs: Probing Substellar Origins with AzTEC 32 MuehleS CI Emission as a Molecular Gas Mass Tracer in Luminous Infrared Galaxies 70 Pineda J Neutrall Atomic Carbon in NGC 1569 25 Poidevin A Multi-scale Analysis of Magnetic Fields in Filamentary Molecular Structures in Orion 42 Schieven G A 12CO Mapping Survey of a Young Cluster in LDN 1188 8

45 Appendix

JCMT Allocations, Semester 05B (Canada) PI Title of Investigation hours Schieven G L1340B: Sequential Star Formation Triggered by Intermediate-mass Stars? 38 Stankovic M Preparatory Observations for a Multi-line Survey of the Sgr A* Region 8 Swift J The Importance of Magnetic Fields in a Newly Discovered Pre-protostellar Core 40 Terebey S Cloud Cores around Young Substellar Objects from the Spitzer Taurus Survey 36 Vallee J Rotating Sources—Testing Magnetic Models 50 Vallee J Zeeman Sources—Testing Magnetic Models 5 Wilson C Mapping Warm Gas in Ultra-luminous Infrared Galaxies in High Angular Resolution 21 Zhu M Methanol Emission from Massive Starless Cores 10

JCMT Allocations, Semester 05B (Netherlands) PI Title of Investigation hours Baes M A Deep Survey of Molecular and Atomic Gas in an Optically Selected Sample of Elliptical... 56 Bisschop S Testing Grain Chemistry 52 Caux E HDO in Proto-planetary Disks 26 Ceccarelli C Is Cold H2 a Major Constituent of the Dark Matter? 100 Dominik C HD2+ Observations of Proto-planetary Disks 20 Fridlund M The Interface between the Molecular Outflow and Disk in L1551 15 Helmich F 230-GHz Imaging of the SLS Targets 25 Helmich F Probing the Chemical Content of AFGL 2591 57 Hogerheijde M Dynamics of a Newly Discovered Young Stellar Object with a Prominent Jet 40 Hogerheijde M Molecular Gas Content of Three Newly Discovered Young Stellar Clusters in Serpens 53 Israel F J=3-2 13CO/12CO Observations of Active Galaxy Centers 38 Israel F Neutral Carbon and XDR/PDR Conditions in Galaxy... 26 Israel F Physics of Molecular Gas in Dwarf Galaxies 17 Israel F Physics of the ISM in NGC 891 59 Jakob H The Small Scale Structure of the PDR around DR21 15 Jorgensen J Low-mass Protostellar Outflows and Hot Cores Observed at High Angular Resolution with... 23 Knudsen K (AzTEC) Tracing the Formation of Cluster Ellipticals 24 Kramer C CI/CO Emission and Metallicity in M101 18 Kramer C The Chemistry of Photon-dominated Regions in the Normal Galaxy NGC278 31 Steuber P UV and X-ray Probes of Deeply Embedded Protostars 24 Thi W-F CI Emission from Circumstellar Disks 50

46 Appendix

JCMT Allocations, Semester 05B (Netherlands) PI Title of Investigation hours Tielens A HDO Abundance in the Envelope of Solar-mass Protostars 13 van der Werf P An HCN/CO Line Survey of Luminous IR Galaxies 145 van Dishoeck E Characterizing the Environment of Low-mass Protostars Observed by Spitzer 99 Wall W (AzTEC) Mm-Continuum Maps of Cold Dust in Nearby Spiral Galaxies—More 24 Wouterloot J Comparison of the Gas-to-Dust Ratio in Inner- and Far-outer Galaxy Star-forming Regions 32 Wouterloot J Hot Molecular Outflows in Globules? 21 Wouterloot J Spectroscopic Study of the Outer Galaxy Star-forming Region IRAS20406+4555 30

JCMT Allocations, Semester 05B (International) PI Title of Investigation hours Aalto S Abnormally Bright HNC in Luminous Mergers—Chemistry or Excitation? 14.5 Braine J (AzTEC) The Extent of Dust Emission and Molecular Gas in Spiral Galaxies 36 Brand J C18O/C17O ratios across the Galaxy 23 Clancy T Chemistry and Dynamics of the Mars and Venus Atmospheres 16 Humphreys E Do Sub-mm Water Masers Exist in Active Galactic Nuclei? 23 Loinard L (AzTEC) A Complete Map of M31 at 1.1 mm with AzTEC 24

47 Appendix

Refereed Publications in 2005/6 (UKIRT)

Alvarez and Hoare, A Search for Shock-Excited Optical Emission from the Outflows of Massive Young Stellar Objects, A&A, 440, 569, IRCAM Balogh et al., Near-infrared Imaging of 222 nearby Hδ-strong galaxies from the Sloan Digital Sky Survey, MNRAS, 360, 587, UFTI Brough et al., Environmental Dependence of the Structure of Brightest Cluster Galaxies, MNRAS, 364, 1354, IRCAM Bergeron et al., On the Interpretation of High-Velocity White Dwarfs as Members of the Galactic Halo, ApJ, 625, 838, UFTI Buschermohle et al., An Extended Search for Circularly Polarized Infrared Radiation from the OMC-1 Region of Orion, ApJ, 624, 821, UFTI+POL Chapelle et al., Crossing into the Substellar Regime in Praesepe, MNRAS, 361, 1323, UFTI Conselice et al., Evolution of the Near-Infrared Tully-Fisher Relation: Constraints on the Relationship between the Stellar and Total Masses of Disk Galaxies since z ~1, ApJ, 628, 160, UFTI Cool et al., Lifting the Iron Curtain: Toward an Understanding of the Iron Stars XX Oph and AS 325, PASP, 117, 462, UIST Cotter, Simpson and Bolton, Vigorous Star Formation in a Bulge-Dominated Extremely Red Object at z= 1.34, MNRAS, 360, 685, UFTI Cruikshank et al., A Spectroscopic Study of the Surfaces of Saturn’s Large Satellites, Icarus, 175, 268, CGS4 Davis et al., Near-Infrared Echelle Spectroscopy of Proto-Planetary Nebulae: Probing the Fast Wind in H2, MNRAS, 360, 104, CGS4 Fernandez, Jewitt and Sheppard, Albedos of Asteroids in Comet-Like Orbits, AJ, 130, 308, MICHELLE Figer et al., Massive Stars in the SGR 1806-20 Cluster, APJ, 622 L49, UIST Fridman et al., The Orientation Parameters and Rotation Curves of 15 Spiral Galaxies, A&A, 430, 67, UFTI? Geballe et al., Infrared Spectroscopy of U Equulei’s Warm Circumstellar Gas, ApJ, 624, 983, CGS4, UIST Gledhill, Axisymmetry in Protoplanetary Nebulae—II. A Near-Infrared Imaging Polarimetric Survey, MNRAS, 356, 883, IRCAM Goto et al., Search for H3+ in HD141569A, ApJ, 629, 865, CGS4 Hatch, Fabian and Johnstone, Detections of Molecular Hydrogen in the Outer Filaments of NGC 1275, MNRAS, 358, 765, CGS4 Hodapp et al., An S-shaped Outflow from IRAS 03256+3055 in NGC 1333, AJ, 129, 1580, UFTI Ivison et al., Rest-frame Optical and Far-Infrared Observations of Extremely Bright Lyman-Break Galaxy Candidates at z~2.5, MNRAS, 362, 535, UFTI, UIST James et al., The Hα Galaxy Survey, A&A, 429, 851, UFTI Jones et al., Carbon Monoxide inLow-Mass Dwarf Stars, MNRAS, 358, 105, CGS4 Kafka et al., A Multiwavelength Study of Am Herculis During the 2002–2004 Low States, AJ, 130, 2852, UIST Kim and Geballe, The 2.9-4 Micron Spectrum of Saturn: Clouds and CH4, PH3, and NH3, Icarus, 179, 449, CGS4 Kishimoto, Antonucci, Blaes; The Dust-Eliminated Shape of Quasar Spectra in the Near-Infrared: a Hidden Part of the Big Blue Bump, MNRAS, 364, 640, CGS4 + POL Kurosawa, Harries and Symington, Time-Series Paschenβ Spectroscopy of SU Aurigae, MNRAS, 358, 671, CGS4 Lee et al., High Resolution Observations of the Near-Infrared Emission from NGC 6822 Hubble V MNRAS, 361, 1273, CGS4

48 Appendix

Meech et al., Deep Impact: Observations from a Worldwide Earth-Based Campaign, Science, 310, 265, CGS4, Guider Misawa et al., Near-Infrared Search for C IV Absorption Counterparts Along the Line-of-Sights to Pair Quasars, AJ, 131, 34, UFTI Mugrauer et al., Four New Wide Binaries Among Exoplanet Host Stars, A&A, 440, 1051, UFTI O’Connell et al., The Near-Infrared Excitation of the HH 211 Protostellar Outflow, A&A, 431, 223, UFTI Oka et al., Hot and Diffuse Clouds near the Galactic Center Probed by Metastable H3+, ApJ, 632, 882, CGS4 Oliveira et al., Circumstellar Discs Around Solar Mass Stars in NGC 6611, MNRAS, 358, L21, UIST Oudmaijer, Drew, Vink; Near-Infrared Line Spectropolarimetry of Hot Massive Stars, MNRAS, 364, 725, CGS4 + POL Robberto et al., The Orion Nebula in the Mid-Infrared, AJ, 129, 1534, MAX Rushton et al., Infall and SiO emission in V838 Mon, MNRAS, 359, 624, CGS4 Rushton et al., Spectral Evolution of V838 Monocerotis in the Optical and Near-Infrared in Early 2002, MNRAS, 360, 1281, CGS4 Seigar et al., Dust-Penetrated Arm Classes: Insights from Rising and Falling Rotation Curves, MNRAS, 359, 1065, UFTI Snellen, High-Precision K-Band Photometry of the Secondary Eclipse of HD209458, MNRAS, 363, 211, UIST Sridharan, Williams and Fuller, Direct Detection of a (Proto)Binary-Disk System in IRAS 20126+4104, ApJ, 631, L73, UFTI, IRCAM Swinbank et al., Optical and Near-Infrared Integral Field Spectroscopy of the SCUBA Galaxy N2 850.4, MNRAS, 359, 401, UIST IFU Varricatt, Davis and Adamson, Multi-Epoch Infrared Photometric Study of the Star-Forming Region G173.58+2.45, MNRAS, 359, 2, UFTI, UIST Watanabe et al. TRISPEC: A Simultaneous Optical and Near-Infrared Imager, Spectrograph, and Polarimeter, PASP, 117, 870, TRISPEC Wilman, Edge and Johnstone The Nature of the Molecular Gas System in the Core of NGC 1275, MNRAS, 359, 755, UIST IFU Wolters et al., Optical and Thermal Infrared Observations of Six Near-Earth Asteroids in 2002, Icarus, 175, 92, MICHELLE Yusef-Zadeh, Biretta and Geballe, HST and UKIRT Observations of the Center of the Trifid Nebula: Evidence for the Photoevap- oration of a Proplyd and a Protostellar Condensation, AJ, 130, 1171, UIST

49 Appendix

Refereed Publications in 2005/6 (JCMT)

Almaini et al., Correlations Between Bright Submillimetre Sources and Low-Redshift Galaxies, MNRAS, 358, 875 Andrews and Williams, Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective, ApJ, 631, 1134 Bradford et al., Warm Molecular Gas Traced with CO J = 7-6 in the Galaxy’s Central 2 Parsecs: Dynamical Heating of the Circum- nuclear Disk, ApJ, 623, 866 Ceccarelli et al., Discovery of Deuterated Water in a Young Protoplanetary Disk, ApJ, 631, L81 Chapman et al., A Redshift Survey of the Submillimeter Galaxy Population, ApJ, 622, 772 Clements et al., Cold Dust in (Some) High-z Supernova Host Galaxies, MNRAS, 363, 229 Coppin et al., An 850 Micron SCUBA Map of the Groth Strip and Reliable Source Extration, MNRAS, 357, 1022 Dasyra et al., Is the Galactic Submillimeter Dust Emissivity Underestimated?, A&A, 437, 447 Dent, Greaves, and Coulson, CO Emission from Discs Around Isolated HAeBe and Vega-Excess Stars, MNRAS, 359, 663 de Ruyter et al., Strong Dust Processing in Circumstellar Discs Around 6 RV Tauri Stars: Are Dusty RV Tauri Stars All Binaries?, A&A, 435, 161 Doi, Kameno, and Inoue, Radio Spectra of the Low-Luminosity Active Galactic Nucleus NGC 266 at Centimetre-to-Submillimetre Wavelengths, MNRAS, 360, 119 Doi et al., A High-Frequency Radio Survey of Low-Luminosity Active Galactic Nuclei, MNRAS, 363, 692 Doty et al., Constraining the Structure of the Non-Spherical Pre-Protostellar Core L1544, MNRAS, 359, 228 Evans et al., Molecular Gas and Nuclear Activity in Radio Galaxies Detected by IRAS, ApJS, 159, 197 Eyres et al., Six Months of Mass Outflow and Inclined Rings in the Ejecta of V1494Aql, MNRAS, 358, 1019 Friesen et al., Fourier Transform Spectroscopy of the Submillimetre Continuum Emission from Hot Molecular Cores, MNRAS, 361, 460 Fuller, Williams, and Sridharan, The Circumstellar Environment of High Mass Protostellar Objects, A&A, 442, 949 Galliano et al., ISM Properties in Low-Metallicity Environments. III. The Spectral Energy Distributions of II Zw 40, He 2-10, and NGC 1140, A&A, 434, 867 Garland et al., The Nature of Nearby Counterparts to Intermediate-Redshift Luminous Compact Blue Galaxies, II. CO Observations, ApJ, 624, 714 Geach et al., A Submillimetre Survey of Lyman Alpha Haloes in the SA22 Protocluster at z=3.1, MNRAS, 363, 1398 Greaves et al., Structure in the Epsilon Eridani Debris Disk, ApJ., 619, L187 Greaves, Disks Around Stars and the Growth of Planetary Systems, Science, 307, 68 Greaves, Submillimetre Observations of Low-Mass Cloud Cores: Forming Tiny Objects in situ, AN, 326, 1044 Greaves, Molecular Gas in Irradiated Protoplanetary Discs, MNRAS, 364, L47 Grimes, Rawlings, and Willott, Implications for Unified Schemes from Submillimetre and Far-Infrared Follow-up of Radio-Selected Samples, MNRAS, 359, 1345 Gutermuth et al., The Initial Configuration of Young Stellar Clusters: A K-Band Number Counts Analysis of the Surface Density of Stars, ApJ, 632, 397 Hatchell et al., Star Formation in Perseus: Clusters, Filaments and the Conditions for Star Formation, A&A, 440, 151 Hodapp et al., An S-shaped Outflow from IRAS 03256+3055 in NGC 1333, AJ, 129, 1580 Holwerda et al., The Opacity of Spiral Galaxy Disks. V. Dust Opacity, HI Distributions and Sub-mm Emission, A&A, 444, 101

50 Appendix

Hrivnak and Bieging, CO J = 2-1 and 4-3 Observations of Proto-planetary Nebulae: Time-variable Mass Loss, ApJ, 624, 331 Humphreys et al., First Detection of Millimeter/Submillimeter Extragalactic H2O Maser Emission, ApJ, 634, L133 Hunt, Bianchi, and Maiolino, The Optical-to-Radio Spectral Energy Distributions of Low-Metallicity Blue Compact Dwarf Galaxies, A&A, 434, 849 Israel, Molecular Gas in Compact Galaxies, A&A, 438, 855 Israel, CO, 13CO, and [CI] in Galaxy Centers, Ap&SS, 295, 155 Ivison et al., Rest-Frame Optical and Far-Infrared Observations of Extremely Bright Lyman-Break Galaxy Candidates at z~ 2.5, MN- RAS, 362, 535 Jorgensen, Schoier, and van Dishoeck, H2CO and CH3OH Abundances in the Envelopes Around Low-Mass Protostars, A&A, 437, 501 Jorstad et al., Polarimetric Observations Of 15 Active Galactic Nuclei At High Frequencies: Jet Kinematics From Bimonthly Monitoring With The Very Long Baseline Array, AJ, 130, 1418 Justtanont et al., W Hya Through the Eye of Odin, A&A, 439, 627 Kirk, Ward-Thompson, and Andre, The Initial Conditions of Isolated Star Formation, VI. SCUBA Mapping of Pre-Stellar Cores, MN- RAS, 360, 1506 Klein et al., A Millimeter Continuum Survey for Massive Protoclusters in the Outer Galaxy, ApJS, 161, 361 Knudsen et al., Submillimeter Observations of Distant Red Galaxies: Uncovering the 1 mJy 850 um Population, ApJ, 632, L9 Kramer et al., Photon Dominated Regions in the Spiral Arms of M83 and M51, A&A, 441, 961 Lindfors, Valtaoja, and Türler, SSC Mechanism in the Gamma-Ray Blazar 3C 279, A&A, 440, 845 Mainieri et al., Submillimetre Detection of a High-Redshift Type 2 QSO, MNRAS, 356, 1571 Maret et al., CH3OH Abundance in Low Mass Protostars, A&A, 442, 527 Marten et al., Improved Constraints on Neptune’s Atmosphere from Submillimetre-Wavelength Observations, A&A, 429, 1097 Massi et al., Outflows and Jets from Low Mass Protostars in Bok Globules: the Case of CB230, Mem. S.A. It., 76, 400 Matsuura et al., The Dark Lane of the Planetary Nebula NGC 6302, MNRAS, 359, 383 Meech et al., Deep Impact: Observations from a Worldwide Earth-based Campaign, Science, 310, 265 Meijerink et al., A Submillimeter Exponential Disk in M51: Evidence for an Extended Cold Dust Disk, A&A, 430, 427 Minier et al., Star-Forming Protoclusters Associated with Methanol Masers, A&A, 429, 945 Mortier et al., The SCUBA Half-Degree Extragalactic Survey, I. Survey Movitation, Design, and Data Processing, MNRAS, 363, 563 Najita and Williams, An 850 um Survey for Dust around Solar-Mass Stars, ApJ, 635, 625 Nutter, Ward-Thompson, and André, The Pre-Stellar and Protostellar Population of R Coronae Australis, MNRAS, 357, 975 Ormel et al., The Modelling of Infrared Dark Cloud Cores, A&A, 439, 613 Papadopoulos, A Search for CI J=2-1 Emission in IRAS F10214+4724, ApJ, 623, 763 Parise et al., HDO Abundance in the Envelope of the Solar-Type Protostar IRAS 16293-2422, A&A, 431, 547 Pontoppidan et al., Ices in the Edge-on Disk CRBR 2422.8-3423: Spitzer Spectroscopy and Monte Carlo Radiative Transfer Modeling, ApJ, 622, 463 Pope et al., The Hubble Deep Field North SCUBA Super-Map, III. Optical and Near-Infrared Properties of Submillimetre Galaxies, MNRAS, 358, 149

51 Appendix

Rathborne et al., Massive Protostars in the Infrared Dark Cloud MSXDC G034.43+00.24, ApJ, 630, L181 Reid, and Wilson, High-Mass Star Formation, I. The Mass Distribution of Submillimeter Clumps in NGC 7538, ApJ, 625, 891 Sandell, Goss, and Wright, Protostars and Outflows in the NGC 7538 IRS 9 Cloud Core, ApJ, 621, 839 Sandor and Clancy, Water Vapor Variations in the Venus Mesosphere from Microwave Spectra, Icarus, 177, 129 Sawicki and Webb, A SCUBA Map in the Spitzer First Look Survey: Source Catalog and Number Counts, ApJ, 618, L67 Schnee and Goodman, Density and Temperature Structure of TMC-1C from 450 and 850 Micron Maps, ApJ, 624, 254 Serjeant and Harrison, The Local Submillimetre Luminosity Functions and Predictions from Spitzer to Herschel, MNRAS, 356, 192 Schöier, Lindqvist, and Olofsson, Properties of Detached Shells Around Carbon Stars: Evidence of Interacting Winds, A&A, 436, 633 Shirley et al., Modeling the Physical Structure of the Low-Density Pre-Protostellar Core Lynds 1498, ApJ, 632, 982 Smith et al., SCUBA Sub-Millimetre Observations of Gamma-Ray Bursts, IV. GRB 021004, 021211, 030115, 030226, 041006, A&A, 439, 987 Smith et al., SCUBA Sub-Millimeter Observations of Gamma-Ray Bursts, III. GRB 030329: The Brightest Sub-Millimeter Afterglow to Date, A&A, 439, 981 Stäuber et al., X-ray Chemistry in the Envelopes Around Young Stellar Objects, A&A, 440, 949 Stevens, Amure, and Gear, Dust in Spiral Galaxies: Global Properties, MNRAS, 357, 361 Stevens et al., Submillimetre Photometry of X-ray Absorbed Quasi-Stellar Objects: Their Formation and Evolutionary Status, MNRAS, 360, 610 van Kampen et al., The Extragalactic Submillimetre Population: Predictions for the SCUBA Half-Degree Extragalactic Survey (SHADES), MNRAS, 359, 469 Vallée and Fiege, A Cool Magnetized Shell Wrapped Around the Hot HII region S106: Geometry, Kinematics, Magnetic Vectors, and Pressure Balance, ApJ, 627, 263 Vlahakis, Dunne, and Eales, The SCUBA Local Universe Galaxy Survey, III. Dust along the Hubble Sequence, MNRAS, 364, 1253 Walawender et al., Multiple Outflows and Protostars in Barnard 1, AJ, 130, 1795 Ward-Thompson et al., First Ground-Based 200-um Observing with THUMPER on JCMT—Sky Characterization and Planet Maps, MNRAS, 364, 843 Ward-Thompson, Hartmann, and Nutter, Turbulence in Class 0 and I Protostellar Envelopes, MNRAS, 357, 687 Webb et al., Submillimeter Imaging of RCS J022434-0002.5: Intense Activity in a High-Redshift Cluster?, ApJ, 631, 187 Weferling, Millimetre and Submillimetre Tau Relations, MNRAS, 362, 263 Williams, Fuller, and Sridharan, The Circumstellar Environments of High-Mass Protostellar Objects, A&A, 434, 257 Wilson and Batrla, An Alternate Estimate of the Mass of Dust in Cassiopeia A, A&A, 430, 561 Wouterloot, Brand, and Henkel, The Interstellar C18O/C17O Ratio in the Solar Neighborhood: The Rho Ophiuchus Cloud, A&A, 430, 549 Wu et al., The Discovery of a Massive SCUBA Core with both Inflow and Outflow Motions, ApJ, 628, L57 Wyatt et al., Submillimeter Images of a Dusty Kuiper Belt around Nu Corvi, ApJ, 620, 492 Zemcov, Halpern, and Pierpaoli, An Analysis of Optical Pick-up in SCUBA Data, MNRAS, 359, 447

52 Appendix

Committee Membership as at 31 March 2006

James Clerk Maxwell Telescope Board United Kingdom Infrared Telescope Board

Professor T Millar (Queen’s University of Belfast) Chair Dr G Fuller (University of Manchester) Chair Dr G Fahlman (National Research Council) Dr S Berry (PPARC) Professor G Joncas (Universite Laval, Canada) Dr K Blundell (University of Oxford) Dr T Moore (Liverpool John Moores University) Dr A Edge (Durham University) Dr J Richer (University of Cambridge) Dr R Joseph (Institute for Astronomy, University of Dr R Stark (NWO/GBE, Netherlands) Hawai’i) Dr P van der Werf (Leiden Observatory) Dr P Lucas (University of Hertfordshire) Dr C Vincent (PPARC) Dr N Tanvir (University of Hertfordshire) Dr J Williams (Institute for Astronomy, University of Dr D Telfer (PPARC) Secretary Hawai’i) Dr D Telfer (PPARC) Secretary UKIRT TAG Community Representatives Dr A Edge (Durham University) Chair Dr G Cotter (University of Oxford) Dr A Chrysostomou (University of Hertfordshire) Dr R de Grijs (University of Sheffield) Dr F Helmich (SRON, The Netherlands) Dr H Jones (University of Hertfordshire) Professor D Scott (University of British Columbia) Dr S Littlefair (University of Exeter) Dr J Oliveira (Keele University) JCMT ITAC Dr M Rawlings (Joint Astronomy Centre, Hawai’i) Secre- tary Dr H Matthews (NRC) Chair Dr J Stevens (University of Edinburgh) Dr J Hatchell (Exeter) Dr M Franx (Leiden Observatory) Dr G H Schieven (Joint Astronomy Centre, Hawai’i) Secretary

53 Appendix

Joint Astronomy Centre Seminars in 2005/6

Date Title of Seminar Speaker Affiliation 1 February Studying the Martian Atmosphere with Ground-based Telescopes Jeremy Bailey Australian Centre for Astrobiology 18 February An Update on SCUBA-2 Wayne Holland UKATC, Edinburgh 16 March The Infrared of Starforming Galaxies Anna Sajina UBC, Physics & Astronomy 6 April Ground-based Cassini Support with Infrared Observations of Saturn’s Tom Stallard UCL, London Aurora 19 April Subaru’s FMOS facility: Design, Capabilities and Opportunities Gavin Dalton Oxford University 11 May Examining the Evolutionary Sequence of Massive Star Formation: A Tracey Hill University of Precursor to the Methanol Maser? New South Wales 24 May Galaxy Clustering in the 2dF Galaxy Redshift Survey Will Percival Edinburgh 27 May The Global Star-Formation Law and Dense Molecular Gas in Galaxies Yu Gao Purple Mountain Observatory 21 June Two Adjacent Gigantic (~9 degree) IRAS Filaments of Bipolar Ronald Weinberger University of Morphology: Shock Fronts, Fossil Jets or Superpositions? Innsbruck 1 July Deep Impact at the JCMT Harold Butner JAC 1 July The BT2 High Accuracy Synthetic Water Line List—A Useful Tool for Robert Barbar University Astronomers College London 19 July Chemical Complexity in Galaxies: The NGC 253 Line Survey Sergio Martin IRAM, Spain 17 August LOFAR, a New Radio Telescope to Study the Distant Universe Mark Bentum ASTRON, Dwingeloo, The Netherlands 30 August A Circumstellar Disc Traced by Methanol Masers in a High-Mass Star- Michele Pestalozzi University of forming Region Hertfordshire, UK

54 Appendix

Date Title of Seminar Speaker Affiliation 15 November Staff Presentations to the JCMT Board Iain Coulson, JAC Harold Butner, Gerald Schieven, Jan Wooterloot 16 November The Thirty Meter Telescope Project (hosted by Gemini) Phil Daly, Bob NOAO Marshall 17 November Staff Presentations to the UKIRT Board Andy Adamson, JAC Watson Varricatt, Chris Davis 1 December Test-Driving HARP Russell Redman NRC-HIA, Canada 5 December The UKIRT Infrared Deep Sky Survey (hosted by Subaru) Andy Lawrence Edinburgh, UK 14 December On the Optical Properties of 6634 IRAS-SDSS Galaxies Tomotsugu Goto Japan Aerospace Exploration Agency 14 December The Near-Infrared Extinction Law in the Rho Ophiuchi, Chamaeleon Takahiro Naoi Japan and Coalsack Dark Clouds Aerospace Exploration Agency 16 December Filling the Gap Between Stars and Planets: The Formation History of Tim Kendall University of Galactic Brown Dwarfs Hertfordshire, UK 9 January The AzTEC Sub-mm Camera at JCMT: Results from the Past Two Grant Wilson University of Months Massachusetts 23 January Mapping Chemistry and Dynamics of the Venus and Mars Brad Sandor Space Science Atmospheres Institute, Boulder 3 February The Square Kilometre Array Site Spectrum Monitoring Rob Millenaar ASTRON, The Netherlands

55 Appendix

Abbreviations and Acronyms

ACSIS Auto-Correlation Spectrometer and Imaging System CGS4 Cooled Grating Spectrometer 4 DAS Digital Autocorrelation Spectrometer eSMA Extended Submillimeter Array ETS Engineering and Technical Services FTS Fourier Transform Spectrometer HARP Heterodyne Array Receiver Programme HIA Herzberg Institute of Astrophysics ITAC International Time Allocation Committee JAC Joint Astronomy Centre JCMT James Clerk Maxwell Telescope JIVE Joint Institute for VLBI in Europe MRAO Mullard Radio Astronomy Observatory Michelle Mid-Infrared Echelle Spectrograph NFRA Netherlands Foundation for Research in Astronomy NOVA Netherlands Research School for Astronomy NRC National Research Council (Canada) NWO Netherlands Organisation for Scientific Research OCS Observatory Control System OMP Observation Management Project ORAC-DR Observatory Reduction and Acquisition Control — Data Reduction PATT Panel for the Allocation of Telescope Time PPARC Particle Physics and Astronomy Research Council (UK) RCUH Research Corporation of the University of Hawai’i ROVER Roving Polarimeter SCS Software and Computing Services SCUBA Submillimetre Common-User Bolometer Array TAG Time Allocation Group UFTI UKIRT Fast-Track Imager UIST UKIRT Imager Spectrometer UK ATC UK Astronomy Technology Centre UKIDSS UKIRT Infrared Deep Sky Survey UKIRT United Kingdom Infrared Telescope WFCAM Wide Field Camera WVM Water Vapour Monitor

Design and Typesetting by Douglas Pierce-Price and Inge Heyer