Joint Astronomy Centre Annual Report 2006/7

660 North A`ohoku Place Hilo, Hawai`i 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 at the UK ATC. Through a combination of increased 2006/07. I am pleased to report that the sensitivity, a larger field of view and full sampling of the year has once again been a busy, pro- focal plane, SCUBA-2 will map the submillimetre sky up ductive and exciting one. to 1,000 times faster than SCUBA. Delivery is scheduled for Autumn 2007. In preparation for this revolutionary The JCMT is, by any objective measure, instrument, the JCMT was closed from mid-February to the world’s most productive submillimetre mid-August 2006 for major structural engineering work. telescope. A review of observatory productivity by Trim- A summary of this very successful project is provided in ble & Zaich (PASP, 118, 933, 2006) ranked the JCMT this report. first in the world amongst its competitors according to all three metrics they used (number of papers, number The JCMT is also preparing for a programme of sub- of citations, and number of citations per paper). This arcsecond astronomy in collaboration with the SMA and rewarding result is based heavily on the success of the the CSO. Tests of the integrated eSMA system have SCUBA instrument, which continues to dominate the progressed throughout 2006/07, and we envisage issu- scientific output of the observatory despite its retirement ing a call to the community for observing proposals with in 2005. this system before the end of 2007. RxW was upgraded during this reporting period for compatibility with the Building on this success, the JCMT is in the midst of eSMA, and will also provide enhanced sensitivity in two a profound transformation to its third-generation suite polarisations for single-dish JCMT users. of instruments. Driven by the scientific requirement for larger sample sizes, the new suite is optimised for Finally, the agreement between the three JCMT funding large-area mapping. I reported last year that the DAS agencies contains a break point in 2009. In order to fully had been replaced by ACSIS, our new multi-channel exploit the investment made in the new scientific capa- backend spectrometer. During this reporting period, bilities, which is on the order of US$40M, the agencies RxB3 was retired after many years of service and was are currently negotiating an extension of operations until replaced by HARP, the world’s first array receiver for the 2012. I expect the outcome to be announced in Autumn 345-GHz atmospheric window. HARP and ACSIS were 2007. both commissioned during 2006/07 and were released for community use in semester 07A. The HARP/ACSIS Turning now to UKIRT, the ambitious seven-year combination brings an unprecedented spectral imaging UKIDSS survey is now up and running at full speed. The capability to the JCMT, and some of the early science second full data release contained over a terabyte of results are compelling; the first megapixel image ever data, and some exciting science results have emerged. recorded in the submillimetre, for example, is presented Some of these are highlighted in this report, including, in this report. in particular, the coolest brown dwarf yet detected. The regime between planets and brown dwarfs is not well- The flagship of the JCMT’s transformation is SCUBA-2, explored, and this was one of the primary goals of the the successor to SCUBA, currently under development UKIDSS Large-Area Survey. ii The strategic review of UKIRT in 2005, chaired by Finally, in recognition of the work load and challenges Professor Richard Ellis of CalTech, recommended that at both telescopes, the JAC senior management was the future role of UKIRT, as an excellent 4-m-class re-organised in early 2007. Dr Antonio Chrysostomou telescope on a superb site, should be to concentrate on was recruited to the new position of Associate Director, “campaign-style” science. Accordingly, the Board issued JCMT, mirroring the position held by Dr Andy Adamson a call for campaign proposals in 2006, and a total of 21 for UKIRT. The organisation is now symmetrical be- proposals was received requesting more than nine years tween the two telescopes, allowing me to split my own of telescope time! This extremely high level of demand time more equitably between them than has been the demonstrates the very high regard in which UKIRT is case in the past. The new arrangements are working held by its user community. In the end, nine of these well and we are now fit for purpose to address the chal- proposals were awarded time, including renewals of the lenges of the future. five UKIDSS surveys. The Board also decided to alter the split of UK telescope time between campaign and PI Professor Gary Davis observing from 48%:52% to 64%:36%. Director

UKIRT continues to turn out science results using its entire range of capabilities, as described in this report. The observatory has always been characterised by a high level of user support and by an extremely efficient operation, and this continued through 2006/07: the operational fault rate of only 3% is exceptionally low in absolute terms but is typical of UKIRT.

PPARC Council decided, in May 2005, to reduce its financial commitment to UKIRT operations to roughly 50% of its current level by 2010 at the latest. This perturbation exceeds any internal savings that we could generate at the observatory, and we are therefore searching for new partners to participate in UKIRT’s future programme. UKIRT is unique amongst world-class observatories in being funded exclusively by one agency, so its conversion to an international telescope would bring it into line with the norm. I am optimistic that this challenge will be met and that UKIRT will continue to deliver world-leading science for many years to come.

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

iii Foreword by the UKIRT Board Chair

A number of important events have one being 6.7 in magnitude. As we now know, UKIRT, punctuated this year at UKIRT. These unlike some of the other telescopes on the mountain, include big data releases, big observing was relatively unscathed and, thanks to the efforts of programmes, a big earthquake and many the observatory staff, was back on the sky in two days. apparently small changes but with big Indeed, UKIRT could have been observing even sooner consequences. had the weather cooperated. Interestingly, the telescope was back in operation long before power was restored to During this year the first two data releases from UKIDSS some places on Oahu! were made. In terms of number of sources detected, the second UKIDSS data release, DR2, is now the larg- During my time on the UKIRT Board I have continu- est-ever infrared survey. The Board look forward to the ally been impressed with the reliability of UKIRT, as exploitation of these data by the community and the sub- measured, for example, by its very small loss of usable sequent UKIDSS data releases, which will provide even observing time due to technical faults. Furthermore, the more extensive views of the infrared universe. observatory staff are continually striving to improve this efficiency. To mention just two examples from this past In April, following a recommendation of the Ellis review year, the ETS Division have reduced the down time of of UKIRT in 2005, the Board issued a call for propos- the telescope during change-over between wide-field als for large observing campaigns or surveys. This call and Cassegrain modes to just two nights. This translates was intended to serve as the formal review of UKIDSS into saving hundreds of hours over the seven-year dura- after two years of operation, as well as to solicit new tion of UKIDSS. At the same time, work on the WFCAM proposals. For the November deadline, 21 propos- data acquisition system has saved two seconds per rea- als were received, with a range of compelling science dout. This amount may appear to be small, but with the cases. The size of this response and the total request short, five-second exposures often used, it represents for over nine years of observing time were very gratify- saving about a hundred nights of observing time over ing. It clearly demonstrates the community’s regard for the same seven-year time frame. This is an impressive UKIRT as a productive facility with a long term future. achievement, squeezing even more science out of each These proposals were reviewed by a set of international night’s observing. referees and then discussed at a special two-day Board meeting in February. The outcome of this meeting was So once again, I would like to congratulate the Director, that the Board reaffirmed its commitment to UKIDSS, Associate Director, and all the staff at UKIRT and at JAC adjusting the allocations and observing priorities of the on a highly successful and productive year and wish five UKIDSS sub-surveys and allocating time to four new them, and the telescope, well for the coming year. campaigns. Dr Gary Fuller In October, an ordinary night’s observing for me on University of Manchester Mauna Kea ended over breakfast when the Big Is- UKIRT Board Chair land was rocked by two major earthquakes, the first iv Foreword by the JCMT Board Chair

On behalf of the JCMT Board, I am very herein, are starting to flow. The legacy programme is pleased to welcome the JAC Annual Re- now underway through the Spectral Line Survey. port 2006/07 and commend it you. The Board has also been monitoring the progress of The past year has been one of transfor- SCUBA-2 and has been helped in this through the mation for the JCMT as it prepared itself Project Management Board, which holds monthly for the arrival of new hardware (the digital telecons with the ATC team in Edinburgh. As we are all autocorrelation spectrometer ACSIS, the 345-GHz array aware, the instrument is complex, with many ground- receiver HARP, and SCUBA-2, the new continuum cam- breaking technologies, so delays are not unexpected. era that will map the sky up to 1,000 times faster than Despite this, there have been several major achieve- the very successful SCUBA instrument), new software ments over the past year, and the Board is looking (the installation of the Observatory Control System and forward to SCUBA-2’s arrival at the telescope in Autumn the implementation of the JCMT Science Archive at 2007. The Harwit review identified a further high-prior- CADC) and new staff—in particular, the creation of the ity project, extended SMA (or eSMA) interferometry. post of Associate Director, JCMT, filled by Dr Antonio Progress has been made during the year, including the Chrysostomou. conversion of RxW, and a workshop held in Leiden in February 2007 to plan collaborative programmes which The necessary preparations resulted in the closure of will demonstrate the scientific capability of the eSMA. the telescope for several months, with six months in this reporting period being lost to science operations. Finally, the Board is anxious to see that agreement on This, and the commissioning of ACSIS and HARP, have the operation of the telescope post-May 2009 is reached meant that the past year has not been as full of science by the funding agencies. While there are sensitive and highlights, which help motivate observers and staff alike. difficult issues to be resolved, we sense a desire on all Yet there has been an unrelenting commitment, by the sides to build on the commitment each has made to the staff at the JCMT in particular, and at the JAC in general, JCMT for over 20 years and, with the promise of what is and by the instrument builders to deliver the infrastruc- essentially a new telescope and revolutionary science to ture and instruments that will ensure that the JCMT re- come, to plan for a productive future. We remain hopeful tains its position as the premier submillimetre telescope that agreement can be reached by the end of 2007. in the world. In closing, I would, on behalf of the Board, like to warmly The Board met twice during the year, in Leiden in May acknowledge the achievements of the JCMT staff over 2006 and in Hilo in November 2006, where it took the the past year and look forward with them to an exciting opportunity to witness the tremendous feat achieved and fulfilling year to come. by the engineering staff in preparing the telescope and infrastructure for the arrival of SCUBA-2. It was also able Professor Tom Millar to note some early science from HARP and is pleased Queen’s University Belfast that significant new results, some of which are reported JCMT Board Chair

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 JCMT SCUBA-2 Infrastructure Work...... 26 JAC Technical Support...... 31 Administration Division...... 32 Science Education and Public Outreach...... 33

Appendix:

Staff Organisation in 2006/7...... 34 Financial Statement, 2006–2007...... 36 Telescope Time Awards (UKIRT)...... 38 Telescope Time Awards (JCMT)...... 42 Refereed Publications in 2006/7 (JCMT)...... 48 Refereed Publications in 2006/7 (UKIRT)...... 50 Committee Membership as of 31 March 2007...... 53 Joint Astronomy Centre Seminars in 2006/7...... 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 • to be responsive to the changing needs of the contributing organisations. The JAC operates two telescopes on Mauna Kea on the island of Hawai`i: the United Kingdom Infrared Tele- United Kingdom Infrared Telescope (UKIRT) scope (UKIRT) and the James Clerk Maxwell Telescope (JCMT). The altitude (roughly 4,200 m/14,000 ft) and the UKIRT is the world’s largest telescope dedicated exclu- dryness make Mauna Kea the premier site for ground- sively to observations in the infrared region of the spec- based astronomy in the northern hemisphere. trum. It is funded entirely by STFC and is governed by a Board. Time is allocated by a UK-based TAG. UKIRT is The JAC is an Establishment of the Science and Tech- also a member of the OPTICON Consortium, and partici- nology Facilities Council (STFC) of the United Kingdom. pates in the OPTICON transnational access programme. STFC provides funds to the JAC for UKIRT and for the UK share of the JCMT. The JAC also receives contri- Primary mirror diameter: 3.8 m butions from the National Research Council (NRC) of First light: 1979 Canada and the Netherlands Organisation for Scientific Wavelengths covered: 0.8 µm–30 µm Research (NWO) towards operation of the JCMT. James Clerk Maxwell Telescope (JCMT) The JAC has a staff complement of roughly 60, com- prised of a mixture of local and international staff. The The JCMT is the world’s largest single-dish telescope workforce is divided into five divisions: one operations operating in the submillimetre region of the spectrum. It division for each telescope, and three divisions for com- is a partnership between the UK (55%), Canada (25%) mon support services (engineering, software, adminis- and the Netherlands (20%) and is governed by a tripar- tration). 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 manner on behalf of the funding agencies; and

UKIRT

Figure 1: H2 2.122 µm mosaic of Orion A by C.Davis (JAC) and collaborators. Positions of candidate Spitzer protostars are marked with circles. The areas outlined with a thick line have been mapped at 1300µm (Stanke et al., in preparation); areas marked with a thin line have been mapped at 850 µm (Nutter and Ward-Thompson 2007). Inset: the region to the north of M 43, with MAMBO 1300 µm contours overplotted. Major flows are numbered and marked with dashed arrows.

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Science Highlights

PATT Science Highlights A Year of Stellar Astronomy

The year 2006 saw UKIRT used highly productively for observations of stellar systems and star formation regions, with a variety of projects taking particular advantage of the instrumental facilities and scheduling flexibility possible at UKIRT. Here we give three highlights of an exciting year. The Eruption of RS Ophiuchi

RS Ophiuchi is one of the most celebrated of recurrent novae, having undergone eruptions in at least 1898, 1933, 1958, 1967 and 1985. This system contains a Figure 2: UKIRT spectra taken soon after the outburst and just over a month later. Note the onset of high-ionisation line emission in the later spectrum . white dwarf close to the Chandrasekhar limit and a red giant, which has a substantial wind. When a nova temperature of 104K, suggesting ionisation of the wind of eruption occurs on the white dwarf, the ejected material, the giant star by the UV flash from the eruption. traveling at about two tenths of the speed of light, col- lides with the wind from the red giant, producing strong Million-degree coronal emission lines ([S VIII, IX and X-ray and non-thermal radio emission. It has been X], [Si VI and VII]) became more prominent, along with speculated that systems like RS Oph might be progeni- X-ray emission, when the wind was shocked—some tors of Type Ia supernovae. In many ways, observing 50 days after the eruption. Line profiles show that the an RS Oph eruption is like watching the evolution of a kinematics of the ejecta, the wind, and the interaction supernova in fast-forward mode. between them is complex. However, all the line profiles became narrower with time, due to the deceleration of The latest eruption, in February 2006, triggered an the ejected material as it ploughed into the giant wind. international multi-wavelength campaign led by Evans The UKIRT observations contribute to a huge dataset (Keele), using telescopes in space (Swift, Spitzer, accumulated by a large international collaboration; these Chandra, XMM, RXTE, HST) and on the ground. Very observations are continuing and are complemented by high-quality data were obtained with UKIRT within 12 data from Spitzer. days of the eruption. The early near-infrared spectra were dominated by hydrogen recombination lines (see Figure 2). Brackett and Pfund discontinuities indicate a

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Spectroscopic Monitoring of SS433 survey of molecular outflows across the entire Orion A Giant Molecular Cloud (see Figure 1 at the beginning of After 30 years of intensive study and more than 700 this UKIRT section). The data are being used to provide papers in the literature, we still do not know some basic statistical information on the frequency, brightness and information about the prototypical Galactic microqua- extent of molecular outflows across the region. Fifty new sar SS433, such as whether the compact object is a flows have quickly been discovered, bringing the grand black hole or a neutron star, and the nature and mass total in Orion A to almost 130. Images of some regions of the companion star. Identification of the companion taken seven years ago with smaller-format instruments has been a real conundrum, since the system shows are being combined with the WFCAM data to measure features consistent with a remarkable variety of stellar tangential velocities of knots and bow shocks in the types. It has been classified as anything from a normal more complex regions. main sequence star of a few solar masses to a very massive A-type supergiant or WR star. The mass of the The random scatter of flow directions in Orion A sug- compact object is similarly controversial. gests that after 10,000—100,000 years, large-scale magnetic fields have little influence on the orientation of To date spectroscopic data relevant to the companion accretion disks and their associated outflows. However, star and the accretion disc have been very limited, and the relatively modest number of flows also suggests that in spite of more than eight magnitudes of extinction the current epoch of star formation injects insufficient in the optical, little study has been done in the infra- turbulent energy to support the cloud against gravitation- red. Blundell (Oxford) and collaborators have set out al collapse; magnetic fields must also contribute to cloud to rectify this situation, taking advantage of the ability support. There is also tentative evidence that clustering of the UKIRT queue to obtain UIST long-slit near-IR may inhibit disk accretion, since the obvious abundance spectra every night throughout an entire orbital period of protostars does not translate into an abundance of (approximately 13 days) in August 2006. By comparing molecular outflows. the spectra taken before, during, and after the primary and secondary eclipses, they expect be able to decouple Together with Spitzer mid-infrared photometry and which spectral features arise from the companion star. IRAM/MAMBO 1,200µm continuum maps, these WFCAM observations give a complete picture of dynam- Star Formation with WFCAM ic star formation in Orion and will contribute to a better understanding of the influence of star formation and, The combination of WFCAM and UKIRT is proving particularly, of outflows on GMCs as a whole. extraordinarily powerful in a wide variety of fields of

study. The availability of the key narrow-band H2 1-0 S(1) filter makes it highly versatile in wide-field studies of star formation regions. Chris Davis (JAC) and collaborators have used UKIRT/WFCAM to perform the first

complete, homogeneous, wide-field H2 1-0 S(1) imaging

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community. The Early Data Release (EDR) reported last UKIDSS Science Highlights year has since been followed by Data Releases 1 and 2 (DR1, DR2). Table 1 shows statistics of the second data Introduction release, which, by definition, incorporates all prior data releases. Within DR2, catalogue rows alone consume The UKIRT Infrared Deep Sky Survey (UKIDSS) is the more than a terabyte of storage within the WFCAM Sci- key project for the Wide Field Camera (WFCAM). The ence Archive. survey was designed by a consortium of UK and (latter- ly) ESO and Japanese astronomers, who also undertake to carry out the required observing in conjunction with Table 1: UKIDSS Data Statistics at DR2 UKIRT staff astronomers. The UKIDSS Survey design Survey Multiframes1 Detections Filter K Depth is fully described in Lawrence et al. (2007, submitted to LAS 97000 30x106 YJHK 18.2 MNRAS); summaries are given here, and the reader is GPS 113500 604x106 JHK 18.1 referred to Lawrence et al. for details. GCS 54000 38x106 ZYJHK 18.2 6 The UKIDSS consortium devised and coordinates the DXS 150000 9x10 JK 19.2-21.1 collective execution of five survey projects. There are UDS 30000 192x103 JK 21.5 two wide-area “legacy” surveys—the Large Area (LAS) 1Multiframes contain fully-reduced images from all four WFCAM detectors. and Galactic Plane Surveys (GPS), one survey focusing entirely on galactic star clusters (the GCS) and two ex- Galactic-Plane Survey tragalactic surveys of increasing depth and decreasing area (Deep Extragalactic (DXS) and Ultra-Deep (UDS) The main goals of the Galactic Plane Survey are to Surveys). Full details are available on the UKIDSS web probe the initial mass function down to 0.05 solar site. By the end of the reporting period, UKIDSS was masses in star formation regions within 2 kpc of the Sun, within a month of the end of its first two years of data to detect stars below the main sequence turn off in the taking. Galactic bulge, and to detect luminous objects such as OB stars and post-AGB stars across the whole Galaxy. Data Releases In terms of catalogued sources, the GPS is an order of magnitude larger than any other UKIDSS survey. Com- Released after quality control and ingest into the bining UKIDSS GPS with other surveys can generate WFCAM science archive, pipeline-processed UKIDSS powerful diagnostics of stellar and star-formation proper- data become immediately public to the ESO commu- ties. Figure 3 shows the combination of UKIDSS GPS nity and to named individual members of the Japanese with Spitzer GLIMPSE data, demonstrating both the great depth of the GPS (probing visual extinctions up to http://www.ukidss.org/ 40m) and the ability of these data, combined with longer http://surveys.roe.ac.uk/wsa/ wavelengths, to provide powerful colour-colour diagnos- http://casu.ast.cam.ac.uk/surveys-projects/wfcam/ tics. In this example, in a six-arcminute field around the

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extinguished cluster G28.983-0.603, Spitzer data allow the first published LAS high-redshift QSO, with z>5.8 ~100 sources to be classified. The UKIDSS GPS data (Venemans et al. 2007, MNRAS 376, L76). increase the number of classified sources to 1,000. Figure 4 shows the detection image and a follow-up Gemini-South GNIRS spectrum of ULASJ0034-00 (Warren et al. 2007). This object holds the record for the coolest known brown dwarf, with an effective temperature of 650K as evidenced by the relative depths of methane and water bands in the follow-up spectrum. The LAS was only 5% complete at the time the discovery image was taken, suggesting that the survey goals

Figure 3: Combination of UKIDSS JHK data with Spitzer, demonstrating the diagnostic potential of the two data sets when isolating class I and II YSOs from field stars and Class III YSOs. The difference between UKIRT (K-band) and Spitzer (4.5mm) (y-axis) is plotted against visual extinction determined from J-H colour (x-axis).

Large-Area Survey

With an overall intent to provide an infrared complement to the Sloan Digital Sky Survey (SDSS), two of the key goals of the LAS are to detect both the closest substellar objects outside the Solar System and the highest- redshift quasars, through their abnormal colours in the Figure 4 (upper): ULAS J0034 (arrowed). Discovery imaging from the UKIDSS Large Area Survey. (lower): Spectrum of ULAS J0034 obtained LAS wavebands (Y, J, H, and K). The first major highlight using Gemini South, compared with other very cool brown dwarfs and model of the LAS—detection of the coolest-known isolated atmospheres. Warren et al. (2007, submitted to MNRAS) combine these data brown dwarf—is described below; 2006 also produced with observations in the mid-infrared from Spitzer.

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in the substellar regime will be realized in full over the Ultra-Deep Survey longer term. Despite a disappointing Winter 2006 observing season, Deep Extragalactic Survey in which the Mauna Kea seeing was rarely sufficient for observing in this survey, the UDS has already passed The main goal of the DXS is to produce a photometric a significant milestone, becoming the deepest near-IR galaxy sample within a volume comparable to that of survey over such a large area. It has continued to push the Sloan Digital Sky Survey, selected in the rest-frame deeper and to higher redshift, and is already a highly optical, but at a redshift of 1–2. Nearly 10 million sources productive source of significant science results. For ex- have so far been detected, and the maximum depth is ample, using UDS data, Foucaud et al. (2007, MNRAS slightly deeper than K=21 at DR2. 376, L20) produced the first measurement of clustering of J-K selected Distant Red Galaxies (DRGs), showing The first release of deep DXS fields occurred this year, that these must inhabit very massive dark matter halos; and new discoveries are being made. For example, and McLure et al. (2006, MNRAS 372, 357) discovered Swinbank et al. (2007, in press) analysed the first public- rare massive galaxies at z>5. released deep field (ELAIS N1, using the UKIDSS EDR) to identify candidate galaxy over-densities at z~1 across As an example of the type of statistical power which the a square degree, combining UKIRT JK data with Subaru increasing depth of the UDS will bring to high-redshift I band and Spitzer 3.6µm imaging. Many candidate science, Figure 5 shows the luminosity functions of structures emerge. Spectroscopic follow-up with Gemini/ red and blue galaxies as a function of redshift, based GMOS confirms five of these as true over-densities on many thousands of photometric redshifts deter- containing between five and 19 members each, tightly mined from UKIDSS UDS and Subaru BVRi’z’ imaging clustered at a redshift of 0.89+/-0.01, and covering (Cirasuolo et al., astro-ph/0609287). The apparent dis- an area on the sky 30Mpc on a side. The very narrow appearance of the classic bimodality in the red and blue redshift range of these over-dense regions indicates the luminosity functions beyond z=1.5 is a key result which presence of a supercluster in this field. Modelling allows should become better established as the UDS pushes to some inferences to be made as to the properties of the ever greater depth. structure, which appears to be similar to the well-studied Shapley and Hercules superclusters at lower redshift. The UDS is attracting a considerable body of multiwavelength data; nearly 300 hours of Spitzer time have The DR2 data release includes eight full WFCAM fields recently been awarded to cover the entire UDS field. in J and K, and four partial fields in K in the four DXS areas. Galactic-Clusters Survey

The Galactic Clusters Survey has proceeded extremely well, and results have been produced in most of the key regions studied. The UKIDSS GCS is finding hundreds

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of new brown dwarfs in a variety of Galactic cluster and candidate brown dwarf members are isolated on the star formation environments, some with masses as low basis of five-band UKIDSS photometry alone. GCS col- as 10 times that of Jupiter. The GCS is well on the way our-magnitude diagrams reveal more than 20 substellar towards an accurate measurement of the form of the multiple-system candidates out of 63 candidate brown substellar initial mass function and a determination of its dwarfs (Figure 6), yielding a binary frequency between universality (or otherwise) in the local part of the Milky 28 and 44% in the mass range between 0.075 and

Way. 0.030 M. This exceeds by a factor of three the binary fractions reported from high-resolution imaging surveys In a GCS highlight, Lodieu et al. (2007, arXiv 0706.2234) of field ultracool dwarfs and Pleiades brown dwarfs. A present results from 12 square degrees of the Pleiades. tentative photometric estimate of the mass ratios seems Over 340 high-probability proper motion members down to support the hypothesis that binary brown dwarfs tend to 0.03 solar masses are extracted, using a combination to reside in near equal-mass ratio systems. of UKIDSS photometry and proper motion measurements obtained by cross-correlating the GCS with data from 2MASS, the INT and CFHT. Additionally, 73 new

Figure 5: Changes in the red (circles) and blue (triangles) galaxy K-band Figure 6: Binary substellar objects seen above the single object sequence in luminosity functions with redshift, from study of 22,000 galaxies in the UDS the Pleiades, from UKIDSS GCS data. field by Cirasuolo et al.

UKIRT

Operations and Instrumentation

Telescope Usage May 2007, but no change was made to the semester layout. Throughout, the split between PATT, University of UKIRT operates a block schedule, with Cassegrain op- Hawai`i and Japanese time remained unchanged, with erations occupying some 40% of the time and wide-field the addition of some flexibility in the fraction of WFCAM survey operations taking up the remaining 60%. The time allocated to UH. Within the WFCAM blocks, 80% of Spring and Summer of 2006 were characterized by rela- the UK time continued to be allocated to UKIDSS, leav- tively short blocks and numerous instrument switches, ing 20% to be allocated by the TAG. as shown in Figure 7. UKIRT PATT time continued to be oversubscribed by 2006 about a factor of two in the two 2006 semesters. In Apr May Jun Jul Aug Sep Semesters 06A and B, Cassegrain time was oversub- CASS WIDEFIELD CASS scribed by factors of 1.9 and 1.8, respectively, and WFCAM time was oversubscribed by factors of 3.1 and 06A 06B 1.7, respectively. Tables 2 and 3 break down successful PATT allocations by instrumentation and science cat- 2006 2007 egory, respectively. Oct Nov Dec Jan Feb Mar CASS WIDEFIELD Table2: Projects Allocated UKIRT Time 06B 06A 06B Instrument Projects % Projects % Figure 7: Block schedule for UKIRT for the reporting period. Rows are: year, month, mode, and semester. CGS4 5 14 3.5 13 UFTI 3.8 10 2.5 10 Demand UIST 16.8 46 12 46 WFCAM 11.3 31 8 31 Within the reporting period, there have been two active semesters, as shown in Figure 7. The extension past Table 3: Time Awarded by Science Area the standard end of the semester at the end of Janu- ary was agreed with the UKIRT TAG as a way to pro- 06A 06B vide clarity in the proposal process for 06B, which was Subject Projects % Projects % advertised as an entirely WFCAM semester. The end Extraga- 11 32 9+1 c/o 29 of the semester was originally identified with the end of lactic the WFCAM block at the end of March, but after discus- Galactic 20 59 13+8 c/o 62 sion of the two-year plan completion rate with UKIDSS, Solar 3 9 2+1 c/o 9 it was clear that additional WFCAM nights would allow System UKIDSS to reach 2/3 of their expected completion; the resulting adjustment extended the WFCAM block to mid-

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Table 4: UKIDSS Outcomes The long WFCAM block which began in late October Sub-Sur- 06A 06B 2006 was enormously productive for most UKIDSS vey surveys, with the exception of the Ultra-Deep Survey Hours % Hours % (UDS); this project requires consistently good seeing DXS 74.75 23 28.5 5 (0.8 arcseconds or better), and the seeing across Mauna GCS 17.7 5 67.2 11 Kea was notoriously poor between November and De- GPS 124.8 38 101.5 17 cember 2006. LAS 107.35 33 355.5 58 Table 5 and Figures 8a and 8b summarize the usage UDS ------56.1 9 of UKIRT between April 2006 and March 2007. Nights closed for pre-planned engineering are not included in Table 4 indicates the time (in hours) spent on each the totals. The main feature of these statistics remains UKIDSS sub-survey from 1 Apr 2006 to 31 Mar 2007. the consistently low fault rate.

UKIDSS Support Table 5: Usage Statistics for UKIRT Total Number of Nights 354.0 JAC support and execution of the UKIDSS constituent Engineering and Commissioning Nights 15.3 surveys developed over the year, with two significant Science Nights 338.7 changes: firstly, a change in the method by which priority is set on the surveys and, secondly, by a reorganization Science Nights Lost to Faults 3% in the UKIRT science group, providing for the recruit- Science and Engineering Nights Lost to Weather 35% ment of a support scientist specifically responsible for progress monitoring and interaction with the individual survey heads.

UKIDSS observations fell into two blocks in the reporting period, as shown in Figure 7. The short May–July 2006 block, although quite heavily affected by instrument readout problems in the early stages, was highly productive for the Galactic Plane Survey (GPS), which essentially owned the entire second half of the night for most of the duration of the block. One major issue was apparent: RA-limited projects in the Large Area Survey (LAS) systematically failed to gain completion, largely due to the relatively high loading of PATT-sponsored and UH projects in May 2006. Figure 8a: UKIRT Operations Statistics 2006-7.

10 UKIRT

Gemini coating plant. Alternative plans are also being investigated, concentrating mainly on the secondary mirror.

Instrumentation

UIST

UIST remained the most-demanded instrument in the Cassegrain suite, requested in two thirds of all proposals for Cassegrain instrumentation in Semesters 06 A and B.

Figure 8b: UKIRT Technical Fault Rate 2006-7. Following successful testing reported last year, the Telescope and Enclosure prototype “stretched-wire” coronagraphic mask was replaced in late Spring with a properly engineered version, The telescope has, in general, performed well, with no and used successfully in the Autumn 2006 Cassegrain major faults and only one or two persistent minor issues schedule block. Spectral blocking arrangements for the being worked around. JH grism were completed, and grism spectroscopy is now fully supported from IJ through to M band. Systematic image quality variations were a feature of the first year of WFCAM operations, but concerted ef- Replacement of the EDICT array controller with an ARC forts on modelling and compensation, led by Tom Kerr model was agreed upon as a project during 2006. With a in 2006 and early 2007, have dramatically improved goal of allowing readout fast enough to permit full-array performance in this area. Work is in progress on addi- readout in the thermal infrared, this project was under- tional temperature sensors on the trusses which should taken jointly between the JAC and UK ATC throughout significantly improve on the current performance. the period of this report. Although initial on-sky tests of the controller in October were unsuccessful due to Emissivity electronics issues, the problem was identified quickly thereafter; at the time of writing, the controller has been Telescope emissivity remained in the 10–12% range, reading out perfectly and with much improved noise thanks to regular cleaning of the primary and dichroic performance over the EDICT system. Commissioning is tertiary mirrors. The telescope Board approved a multi- planned for the last week of May, and the outcome will part plan for emissivity reduction at its meeting in May be documented in the next report. 2006. Two key items in this programme are silver coating of the primary and secondary mirrors, and efforts to The other two Cassegrain instruments, CGS4 and achieve this have been focused on gaining access to the UFTI, split the remaining requests approximately equally.

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This was identified as necessary for the removal of direct One other major project has been the investigation of moon ghosts, which were a problem for UKIDSS obser- the UIST throughput, which remains below specification. vations in 2005 and 2006A. Internally to the cryostat, Optical tests were performed in January 2007, with the WFCAM hardware remains unchanged, apart from the cryostat open, employing calibrated sources and with installation of a narrow-band J filter for the high-redshift a photodetector situated at three points in the optical emission-line search of Smail et al., replacing the Brack- train. The results showed optical transmission somewhat ett-g filter, which was in relatively low demand. (10%) low, relative to the optical reference model, but still not sufficiently poor to produce the known shortfall. Upgrades to the computing hardware and software With suspicion focusing on the Aladdin III InSb array, the were a major feature of the reporting period. Upgrades detector was shipped to Raytheon (the manufacturers) to the data acquisition PC system—both software in for quantum efficiency testing. Results of this test have June 2006 and hardware and software between August recently been received and pose an additional conun- and November 2006—resulted in typically 30 minutes drum: the wavelength dependence of the measured QE more data being taken per night, a major change which does not match the manufacturer’s original reference will, for example, save 100 nights over the course of curve. Analysis of these results is ongoing at the time of the entire UKIDSS survey programme. Disk storage writing. arrangements were also upgraded in both the acquisition and the data reduction machines, resulting in fewer WFCAM storage failures, faster data access, and additional space, particularly in the acquisition side. Approximately The UKIRT wide-field imager, WFCAM, had an im- two weeks of raw data are now available for fast access mensely productive year, both for PI projects and for the at any given time. Finally, the data reduction machines UKIDSS Sky Survey, although the beginnings of both were themselves upgraded, and the resulting systems WFCAM schedule blocks in the reporting period were now cope ably with the incoming data rate in all but the characterised by readout problems, which elevated the most crowded Galactic-plane fields. fault rate for the instrument to greater than 10% in some weeks. In both cases, the causes of the faults were Work on the interaction between WFCAM and the isolated and removed, and in both cases, by the end of telescope has been taken to a satisfactory conclusion. the respective schedule block, the instrument was turn- The top end was made to largely eliminate tilts arising ing out significantly increased numbers of data frames internally in the camera, and the resulting linked, ac- per hour than it was at the start. Here we summarize the tive system now provides image quality limited only by changes made in WFCAM, first at the hardware level atmospheric seeing and the telescope focus model over and then on the computing side. the whole sky.

There was one change to the WFCAM hardware: the CGS4 design (at the UK ATC), fabrication (under contract) and subsequent installation of a tubular baffle at the bottom There were no changes in CGS4, either internally or of the autoguider focus lens barrel above the field lens. in external electronics and computing. The instrument

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has continued to perform very well, the only major faults higher than with normal linear polarimetry. Imaging and appearing to be communication hang-ups not related to spectro-polarimetry with UFTI and UIST are now routine. the instrument itself. We are considering two significant Source acquisition with UIST works identically to that upgrades: firstly, to replace the ALICE controller, and for normal imaging and spectroscopy, and robust DR secondly, to replace the VAX-based mechanism control recipes for all linear-polarimetry modes are in place. DR system. Both of these aging items have developed into recipes for circular polarimetry are being fine-tuned. operational risks. The first part of this work would be to upgrade ALICE to an ARC controller, which in principle could be achieved within FY07/08. While the cost is not insignificant, the UKIRT Board has recently endorsed this project in view of the risk mitigation that it represents.

UFTI

UFTI continued to provide a highly reliable near-infrared imaging capability and remains the instrument of choice for high-sensitivity JHK imaging over a 1.5 arcminute field of view. There has been only one change internal to the instrument, with the installation of a YMK (WFCAM Y) filter enabling WFCAM follow-up studies. Since the UFTI

2.248MK H2 narrow band filter receives very little use, and since this capability is also available in UIST, this filter was removed to make space for MKY .

IRPOL

Polarimetry at UKIRT is now perhaps more popular than it has ever been, with time being awarded to six programmes in 06A and eight (including three carried over) in 06B. Two of the 06B programmes involved the (U. Hertfordshire) circular polarimetry module. Data were ac- quired with both UIST (circular spectro-polarimetry) and UFTI. The circular polarimetry instrumentation worked very well with both instruments, set-up only taking about 30 minutes on the first night and less than 10 minutes on subsequent nights. Overheads were not significantly UKIRT in the afternoon on Mauna Kea in Hawai`i. Photo by Inge Heyer.

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The James Clerk Maxwell Telescope on Mauna Kea. Photo by Inge Heyer.

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Science Highlights

Solar System The group used HARP/ACSIS to obtain the first simul- taneous day and night measurements of the abundance

Although perhaps better known for its high-profile levels of the SO, SO2, ClO, and HDO molecules at an research in cosmology and star formation, the JCMT altitude of 70–100 km in the Venusian atmosphere. The continues to make important breakthroughs in provid- results show quite dramatic sulphur abundance vari- ing a better understanding of the nature of bodies in our ations of up to 50% on timescales as short as a day own Solar System. A good example of such research is (Figure 9). In addition, theory and all models indicate that on Venus, a programme led by Brad Sandor, Todd SO and SO2 (collectively SOX) react chemically with

Clancy, and Gerald Schieven (JAC). H2O. However, models do not agree as to the effect

of H2O on the ratio SO/SO2, or even whether H2O and

This project was scheduled on the JCMT contemporane- SOX are positively or negatively correlated. These high ously with observations by the Venus Express satellite in s/n spectra of HDO (i.e. deuterated water) with SO and orbit about Venus, as well as during a gravity-assist flyby SO2, together with future such data, will observationally of the Mercury Messenger mission. JCMT observations constrain and resolve these issues. complement those of the orbiter by providing data both day and night (Venus Express can do so for either day Because of the large angular size of Venus at Great- est Western Elongation, the group was able to obtain, through observations of the deep CO J=3-2 absorption feature, the first global wind maps of Venus at other than inferior conjunction and hence the first global wind maps including both dayside as well as nightside. Mapping winds over half or more of the Venusian diurnal cycle will be a new science objective in future proposals.

Star Formation The development of star formation theory hinges on observational evidence, and one of the best-established Figure 9: HARP/ACSIS provided the first spectra of SO absorption in the empirical facts in star formation is the stellar initial mass atmosphere of Venus, revealing abundance changes over the period of a week in January 2007. function (IMF), often referred to as the Salpeter function. Over the last decade, the core mass function (CMF) of or night) and altitude resolution through pressure-broad- pre-stellar cores (a gravitationally-bound body absent of ened lines (as opposed to total-column measurements star formation activity) was measured and found to mim- from the Express). When altitude-sensitive observations ic the Salpeter function for normal stars. The implication are possible with the Venus Express, then any overlap is that the mass spectrum of stars is pre-determined in in altitude provides an opportunity for mutual calibration the fragmentation and collapse of the giant molecular between the spacecraft and the observatory.

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cloud from which the stars form. Evidence to support this In a paper by Nutter and Ward Thompson (2007, idea for low-mass stars, however, remained incomplete. MNRAS, 374, 1413), the JCMT archive was mined for all observations of the Orion Molecular Cloud ever made with SCUBA. These data were re-reduced and combined to produce the deepest sub-millimetre map of the cloud yet obtained (see Figure 10), with 1-s noise levels 2–4 times better than any previously published for this region. Over 390 objects were detected in the final maps. Comparisons were made between those SCUBA sources and archive data from the Spitzer Space Telescope to eliminate contamination from protostellar objects. The resulting CMF is shown in Figure 10.

The CMF is seen to turn over at significantly higher

mass than the completeness limit (~0.3 M), the first time that this turnover has been detected. This shows that, as well as mimicking the IMF at the high mass end, the CMF also follows the shape of the IMF for low masses. If it is assumed that the CMF directly translates into an IMF (i.e. that one pre-stellar core produces one star), then the corresponding star formation efficiency estimated by Nutter and Ward Thompson is just 6%, compared to measured rates in Orion of ~30%. The implication is that the formation of multiple stars from single cloud cores is a normal and regular event.

Semester 06B saw the first science results emerge from HARP and ACSIS. These much-anticipated instruments are finally fulfilling their promise, with some excellent data and results presented in the Spring 2007 edition of the newsletter JCMT Spectrum. Of particular note was the first submillimetre mega-pixel image, a 6.25 square degrees 12CO raster map of the Rosette nebula (Figure Figure 10: SCUBA archive map (left) of Orion B North from Nutter and Ward- 11). The data were observed by Dent and collaborators Thompson. The stellar IMF is compared to the clump mass function in the as part of their award of guaranteed time for building Orion Molecular Cloud (right), showing, for the first time, the turnover at the low mass end. The vertical dashed line shows the completeness limit of the ACSIS. sample.

16 JCMT

us) does not seem to be associated with dark lanes. There is a copious amount of information present in this data set, which will take some time before it is fully analysed.

Cosmology

A special session on Galactic and extragalactic surveys using AzTEC was held at the January 2007 American Astronomical Society meeting in Seattle. These surveys took place when the AzTEC camera, a large-format array comprising 144 bolometers and ultimately bound for the LMT, was installed on the JCMT as a visiting instrument during semester 05B. AzTEC operated exclusively at 1.1 mm and spent about 600 hours on the sky in what was a very successful run. However, due to the complexities of the data acquisition and reduction, an extensive period of software coding was required after the observations were completed. Nevertheless, prelimi- nary results, which demonstrated the value and promise of the instrument, were presented at the AAS meeting.

Figure 11: The 12CO J=3-2 emission from the Rosette Nebula. The optical One of the projects was to observe the GOODS-N field image (David Malin, UKST) is shown in the inset, with its extent depicted by in order to search for, and detect, a population of high- the dashed lines. The HARP/ACSIS image itself is 2.5 degrees across. The image is made by combining three velocity channels: emission at 16–25 km/s redshift submillimetre galaxies (SMGs), first discov- is shown as red, emission at 11–16 km/s is shown as green, and emission at ered by SCUBA and sometimes referred to as SCUBA -1–11 km/s is shown as blue. galaxies. Their importance to cosmology emerged when For the first time, the whole ensemble of clouds around it was quickly realised that their submillimetre luminos- the central nebula can be studied in detail. In the optical ity implied that they must be massive and undergoing image, dark lanes and structures (so-called “cometary intense bouts of dust-enshrouded star formation. Given globules”) are present which are, in most cases, as- their high redshift, this makes them a unique tracer of sociated with blue-shifted CO gas. Closer inspection of structure and evolution in the early universe, providing the spectral information in the cube shows that these important constraints on formation models and a study structures are being accelerated away from the core and of the star formation history of the universe. towards us, most likely driven by the UV flux from the luminous central stars. In contrast to this, the red-shifted Several extragalactic projects were observed with Az- material (undergoing similar acceleration but away from TEC (including the whole of the SHADES region), but it

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was observations of the GOODS-N field that produced per, deep Spitzer images were used to find counterparts what is perhaps the deepest millimetre map yet made, to 60% of the SCUBA sample, providing the largest sam- with an rms noise level of 1-s ~1.0 mJy/beam (Figure ple of identified SCUBA galaxies. The spectral energy 12). This depth resulted in the detection of several faint distributions for these galaxies were used by Pope et sources whose numbers allow challenges to be made to al. to show that the SMGs peak at cooler temperatures galaxy evolution models. than local ULIRGs of the same luminosity. This peaking demonstrates the existence of strong selection effects Nine sources were detected above 5-s, of which five had in both the local and high-redshift universe and provides also been detected by SCUBA and have spectroscopic a warning that these effects will result in an incomplete redshifts. The brightest AzTEC source coincides with the census of the ULIRG populations. brightest of the submillimetre sources detected by SCU- BA in this field, the study of which has been reported this last year by Pope et al. (MNRAS, 370, 1185). In this pa-

Figure 12: The 1.1mm AzTEC image of the GOODS-N field. The image is 10 JCMT observing in the afternoon. Photo by Inge Heyer. x 16 arcminutes. There are nine sources circled, each with S/N > 5-s.

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Operations and Instrumentation

Operations of the telescope after the engineering shutdown. A total of 76 proposals was received. The JCMT was closed in February 2006 for six months of engineering work in preparation for the arrival of SCU- Each of the national queues continues to be over- BA-2 and re-opened on schedule in mid-August 2006. subscribed, with the total oversubscription running at At this time, the facility entered a phase of functional approximately a factor of 3. In total, not counting person- checkout tests to the end of September 2006. Science nel visiting for instrument commissioning, 41 observers operations with RxA started once more in October 2006, visited the telescope to take part in astronomical obser- along with the commissioning of HARP/ACSIS. Due to vations. this, we report only on operations between October 2006 and March 2007. Table 6: Breakdown of JCMT Applications in Semester 06B by National Queue Queue Proposals Hours Hours Oversub- Hours Projects Received Requested Available scription Allocated Allocated This has been an extremely challenging period for the UK 25 784 363 2.2 5231 21 JCMT on many fronts, culminating in what is essentially 2 a new telescope and instrument suite. The DAS has CA 29 790 165 4.8 692 29 been replaced with ACSIS, while RxB has been retired NL 12 392 132 3.0 2832 10 and replaced by HARP. Working together with the SMA IN 9 248 n/a n/a 1453 6 and CSO, we are in the midst of commissioning the UH 1 112 72 1.5 112 1 eSMA to provide a submillimetre interferometer with Total 76 2326 732 3.2 1755 67 increased spatial resolution and twice the collecting area of the SMA. For this to happen, RxW was converted to 1 Includes time formally allocated (i.e., observer required a dual-polarisation receiver for the B- and D-bands. The to go to the telescope) plus fallback allocations (no ob- telescope has a new Observatory Control System, and server required at the telescope). we are now into our final preparations for the arrival of 2 Projects are ranked scientifically but not formally al- SCUBA-2. located on the schedule. Observers are invited to the telescope, based on the ranking of the proposal. Despite this intense activity during the reporting period, 3 Includes 32 hours of daytime observing. the science output from the observatory continues to be of the highest standard. Note that this table does not include time used for Engi- neering and Commissioning (E&C). Due to the intense Time Allocation ongoing commissioning throughout the semester, all of the Director’s Discretionary Time in Semester 06B (48 Table 6 shows a breakdown of the number of projects hours) was given to E&C. applied for and awarded time in each observing queue for semester 06B (1 October 2006 to 31 January 2007), foreshortened by two months due to the commissioning

19 JCMT

experienced. The summer and autumn months were particularly poor. There was no grade 1 weather available at all between June and November. Fortunately, the telescope was closed throughout most of this period and was being commissioned for the rest.

Figure 13: The distribution of 225 GHz opacities recorded throughout the t year (April 2006 to March 2007). Each value represents the average CSO measured each night between 9:00pm and 3:00am HST. Figure 14: The month-by-month weather record showing the of time spent (in %) in each weather grade during 2006–07 (left) compared with the historical Weather record (right).

The weather conditions at the JCMT are measured in In October, conditions were extremely poor, with over terms of the amount of precipitable water vapour to- 90% of the time in Grade 4 or worse! Somewhat wards the zenith, measured by the CSO radiometer. We fortunately, at this time, the observatory was coming t refer to this as the CSO tau ( CSO). The observing condi- out of functional check-out, and RxA, which can work tions are split into five so-called weather bands, with “1” in these relatively wet conditions, was the only facil- t t ( CSO < 0.05) the best and driest while “5” ( CSO > 0.2) ity instrument available. A marked improvement in the is the wettest. The weather conditions measured as a weather was seen in the following months just as our t function of CSO throughout 2006–07 are shown in Figure new spectral imaging system, HARP, became available 13. A comparison with the historical record can be seen (on a shared-risk basis) in November. During Decem- in Figure 14. ber and January, 60% of the time was spent in the best (Grade 1–2) weather bands, the dry conditions attribut- From Figures 13 and 14, it is clear that significant able to an El Niño, which was present over the Pacific amounts of the worst and best weather conditions were at that time.

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Operations Statistics an overshoot beyond 100% for the January statistics (all other overshoots are due to extended time). The Observatory Management System provides logis- tical support for managing the flexible queues at the All told, the average length of a JCMT night through- JCMT and UKIRT, and allows us to monitor and account out this period was 12.5 hours. The telescope was not for all the time that is used on the telescopes. For this closed at any point throughout this period (apart from the report, only those statistics recorded after the JCMT usual Christmas Eve closure). started science operations are considered. These are presented in Figure 15. Overall, 68% of telescope time was used for allocated science projects, while the time lost to weather amounts Overall, a total of 2,260 hours were available repre- to 24% of the total time; this includes any time in which senting 181 12-hour nights. In addition to this total, the observers may have persevered through poor condi- telescope was used for 57.7 hours of extended time tions. (where observations continue for usually no more than an hour beyond the usual 12-hour period) and 30.5 Fault Rate hours of daytime observing. Increased use of extended time in December, January, and March is mostly due to The fault rate on the JCMT is measured in terms of clear HARP and eSMA commissioning. Even though daytime time, i.e., all the time that the observatory is scheduled observing extends the observing time beyond 12 hours, to observe, minus any time lost to weather (Figure 16). in this instance, it needs to be recorded as Project time, In this way, this metric measures the impact that faults as it is time awarded by the ITAC and must be ac- have on our ability to deliver the science programme. counted for accordingly. This is partly the reason we see

Figure 16: The technical fault rate measured since February 2003.The red line shows the month-by-month fault rate, while the blue dashed line gives Figure 15: Performance statistics, presented as a fraction (%) of the time the running average over this period. The shaded region indicates the 6- available, since October 2006. month engineering shutdown between February and August 2006.

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For this reporting period, the technical fault rate (i.e., Instruments those which cannot be attributed to “human error”) ran at 6.4%. Instrument Use

There were just three instruments available during this reporting period: RxA, HARP, and RxWB. No continuum instrument was available. JCMT instruments are not efficient in all weather conditions, and this is illustrated in Figure 17. The B-band instruments (RxWB and HARP) dominate the driest weather conditions, whereas RxA, designed to work through wetter conditions at lower frequencies, dominates the usage in Grades 4–5.

The hours illustrated in Figure 17 do not include overheads (e.g., slewing to source, tuning receivers, etc.), nor E&C time, and therefore represent a fairly accurate record of how long the instruments are used for science in the different weather bands. The fact that RxA was Figure 17: The number of hours observed by each instrument as a function used in all weather bands (including Grade 1) does not of the weather grade. come as a surprise, given that, at times, it was the only instrument available. The rise in faults from January through to March, in many respects, reflects the observatory’s attempts to RxA recover from the shutdown period coupled to the ongoing commissioning of three instruments (HARP, ACSIS, Receiver A3 is a single-channel heterodyne receiver for and RxW), with RxA as the solitary backup to all of our the 230 GHz atmospheric window, the lowest-frequency operations. The majority of these faults was software- band in which the JCMT operates. The receiver per- related. This is not surprising, when one considers that formed very well during the reporting period, with only HARP, ACSIS, and the Telescope and Observatory Con- 1.85 hours of lost clear time attributed to it. trol Systems are all new and very complex systems on the telescope, running over 55 major tasks (with several RxW hundred minor tasks running simultaneously) on over 25 different computers connected throughout the network. Receiver W was originally developed in Cambridge as a single-polarisation receiver operating in the high-frequency windows at 470 GHz (C-band) and 690 GHz (D- band). In the winter of 2006, the JCMT Board endorsed a plan to convert the receiver to operate in the B- and D-

22 JCMT

bands to provide a dual-polarisation B-band receiver for HARP use with the eSMA. Funded in part via an NWO grant to Dr Ewine van Dishoeck, this work began in early Novem- The Heterodyne Array Receiver Programme (HARP) is ber with the installation of the new B-band and upgraded a 16-pixel heterodyne receiver built and developed in D-band blocks on the mixer plates. Although the cryostat Cambridge, UK, in collaboration with the UK ATC, HIA in was successfully cooled to operating temperature by Canada, and the JAC. On installation in November 2005, January, no LO power could be detected at 690 GHz two of the 16 pixels were found to be unresponsive and due to a faulty Gunn, which was subsequently sent back a third was damaged during commissioning. As such, for repairs. The new 345-GHz channel achieved first HARP was commissioned with 13 working receptors and light on 7 March 2007, and a number of observers used released for shared-risk observing in this state during RxWB while HARP was unavailable in March. most of semester 06B. In March 2007, one of the broken receptors was replaced by a spare, a faulty IF amplifier ACSIS to a second receptor was replaced, and the third receptor was replaced by a dummy block. HARP now has 15 The Auto-Correlation Spectrometer and Imaging System working receptors, and a replacement for the final recep- (ACSIS) took over from the DAS as the back-end for the tor, as well as a number of working spares, are being front-end receivers, with the re-opening of the telescope manufactured by Cambridge. in August 2006. ACSIS is a multi-channel correlator developed by the DRAO in Canada, in collaboration with HARP was used extensively when available, and the the UK ATC and the JAC. The complexity of the system scientific results were at times remarkable (see, for and its integration with the Observatory Control Sys- tem and instruments is great. Each of the OCS, ACSIS and HARP needed commissioning during the reporting period, and dependencies between them has, at times, hampered progress.

By the end of September, the ACSIS/OCS system had been largely commissioned, meaning that common-user observing with RxA could commence by 1st October, followed by commissioning of HARP. The performance of ACSIS has, in the main, been good, and observers are mostly happy. There remain a few outstanding issues, in particular with the software and observing recipes, and effort is being invested to resolve these.

Figure 18: WFCAM K-band image of the Orion nebula (left) compared to a HARP/ACSIS image (right) showing the distribution of CO gas over similar scales.

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example, Figure 18). One project in December collected Cardiff University, the Scottish Microelectronics Centre, more spectroscopic bytes of data, by itself and in one and a consortium of Canadian universities. Building on night, than all spectroscopy data ever collected by the the enormous success of SCUBA, SCUBA-2 will provide JCMT in its history! enhanced sensitivity over a much wider field of view with full (or nearly full) sampling of the focal plane. These Telescope and Facility enhancements will be achieved through a number of technical innovations, primary amongst which are the The biggest event to hit the telescope this past year was, development of transition-edge superconductor detec- arguably, the 6.7-magnitude earthquake of 15 October tion technology and a novel optical design which utilises 2006! It is astonishing to consider that the earthquake as much as possible of the JCMT’s field of view. The had little effect on the facility, although it took about two result of these innovations, in conjunction with novel weeks to determine that. The quality of the pointing on scanning and sampling techniques, is that SCUBA-2 October 23 was nominal. will be able to map large regions of the sky up to 1,000 times faster than SCUBA. This revolutionary instrument The issues of most concern with the telescope perform- will open up entirely new paradigms in submillimetre ance are its pointing and a secondary mirror unit (SMU) astronomy. vibration problem. Different to previous heterodyne instrumentation at the JCMT, HARP comes with an image The instrument is currently in its final verification phase rotator (the so-called K-mirror), which is used to keep the in the laboratory in Edinburgh. Although some difficult sky at a fixed orientation with respect to the array as the technical issues have arisen, this is only to be expected telescope tracks an object across the sky. The K-mirror in a high-risk, high-reward project involving the develop- introduces an additional six terms to the pointing model, ment of entirely new technologies. SCUBA-2 is currently and early results indicate that these may actually turn scheduled for delivery to the telescope in the Autumn of out to be quite small. Achieving an accurate and well-un- 2007. derstood pointing solution with HARP is a high priority. eSMA SMU vibrations, of order 2 arcseconds and audible from within the dome, have been reported since autumn The eSMA is a collaboration between the SMA, the 2006. The SMU is due to be serviced in 2007. JCMT and the CSO to form a single submillimetre interferometer with approximately twice the collecting area of Future Instruments the SMA, resulting in an increased sensitivity. The eSMA will operate part-time and in the 345-GHz window, tak- SCUBA-2 ing full advantage of Mauna Kea’s excellent observing conditions and prolonged periods of superb weather at SCUBA-2 is a new bolometric camera currently be- that frequency. ing developed at the UK ATC, in collaboration with the National Institute for Standards and Technology (USA),

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The three observatories have committed two nights per month to eSMA development, and, as a result of intense effort by all three groups, the system is gradually coming together. The objectives for 2007 are to establish the baselines, obtain fringes at 345-GHz, and complete a science demonstration project. A call will then be issued to the community for science proposals for the 42-night pilot programme agreed upon with the other observatories. In preparation for this opportunity, a highly-successful cross-community workshop was held in Leiden in February 2007.

Ancillary Instruments

The JCMT will also be taking delivery of three more instruments: ROVER, a heterodyne polarimeter which will operate with HARP, RxA, and RxW; POL-2, a continuum polarimeter which will operate in conjunction with SCUBA-2; and FTS-2, a Fourier transform spectrometer, which will also operate with SCUBA-2. ROVER was built at the UK ATC and has already been delivered to the JAC; the control and data reduction software are under development. The other two instruments are under development in Canadian university laboratories and are scheduled for delivery to the JCMT in 2008.

JCMT on the outside and the inside. Photos by Inge Heyer.

25 JCMT

SCUBA-2 Infrastructure Work at the JCMT

Introduction beam into as narrow a space envelope as possible. The delivered optical prescription is not suitable for SCUBA- Like most telescopes, the JCMT was designed for 2, and the beam is subsequently re-imaged twice before specific instrumentation envisaged during its design and reaching the detector focal plane. Including the tertiary construction. This necessarily limited perspective was mirror, nine mirrors are required to achieve the perform- driven by cost and by likely technological developments ance. These are all mounted to a high level of precision, over the expected lifetime of the telescope. Longev- with the last three cold inside the cryostat. ity and technology, however, have long outstripped the original payload capacity. To cope with the increasing The Modifications complexity and, in particular, the exceptional demands on the telescope from SCUBA-2, the Infrastructure A new gallery was required above the control room Project was developed. to site the support equipment for SCUBA-2, including closed-cycle cooling equipment, dilution refrigerator The SCUBA-2 Infrastructure Project is the largest gas handling system, and all electronics other than engineering project ever undertaken at the JCMT. The the array controllers. This gallery was installed prior to work was carried out by the Engineering and Technical the shutdown (Figure 19) and was made ready for the Services (ETS) Division of the JAC. The telescope was installation of power supplies and coolers as part of the closed for six months, beginning on 13th February, so shutdown work. that the work could be completed without interruption. This period represents an invisible investment in the scientific promise of SCUBA-2 of another £1M by the three JCMT funding agencies.

Telescope Infrastructure Challenges

SCUBA-2 represents a fundamental change in instrumentation, both in physical terms and in optical require- ments. The cryostat weighs ~4 tonnes and is a ~3m x 2m x 1.5m box housing the two focal planes and re-imaging optics, and the only location in which it can be mounted is well outside the main optical path. This requires the antenna light path to be bent and shaped to allow the beam to exit through a small aperture in the elevation bearing. This difficult feat is further exacerbat- ed by the instrument’s field of view, which is the largest ever accommodated at the JCMT. To achieve this, a set of optics is mounted in the receiver cabin to squeeze the Figure 19: Inspecting the beams for the new SCUBA-2 gallery.

26 JCMT

The receiver cabin houses a new Tertiary Mirror Unit The computer room housed the now-obsolete Digital and a set of relay optics to reduce the SCUBA-2 input Autocorrelation Spectrometer (DAS) and the space was beam to a size that can pass unvignetted through the left required for both HARP and SCUBA-2 data storage. A elevation bearing. To house these “cabin mirrors”, signifi- major refurbishment of this area was undertaken during cant redevelopment of the receiver cabin was required. the shutdown (Figure 20). This includes relocation of existing equipment, cleaning up of the cable runs and modification of the cabin bay SCUBA-2 requires a mounting frame to support the next to the bearing to accommodate the mirrors. instrument and the re-imaging “Nasmyth mirrors.” This structure was designed and fabricated by contractors The left-hand Nasmyth platform that had previously and installed by ETS staff towards the end of the shut- been enhanced to service the original SCUBA instru- down. ment and allowed access to the receiver cabin has been virtually eliminated to mount the re-imaging optics and The mass of SCUBA-2 is too large to be supported on the instrument itself. Work during the shutdown included the antenna and carousel floor by conventional means. removal of the existing platform and rebuilding of the As a result, a significant part of the project was to pro- receiver cabin access walkway. A further part of this vide dedicated handling equipment to install and remove work is extending the mezzanine platform below to allow the instrument. The size of the instrument dictates the access to SCUBA-2 when installed. location of this handling equipment and required modifications to the antenna azimuth axis limits to allow the

Figure 20: Refurbishment of the computer room. Figure 21: Lifting the cryostat mounting frame into the JCMT building.

27 JCMT

antenna to rotate into a previously prohibited zone to Scheduling the Work allow the rails to match up. The carousel floor required strengthening and the installation of a rail system and The normal work pattern for the ETS staff is to com- handling cart to manipulate SCUBA-2 (Figure 25). mute from Hilo to the observatory each day, allowing a six-hour working day on site. The infrastructure project, The cryostat mounting frame and the handling cart con- however, required a much more demanding schedule. tracts both slipped to the stage at which they could have Ideally, full-time residence at Hale Pohaku (the astrono- jeopardised the completion of the shutdown. Contractor mers’ residence at 9,000 feet, Figure 23), giving a 12- visits, frequent phone calls, and general harassment of hour working day at the observatory, would meet these shippers resulted in the equipment arriving just in time demands. Physical work at altitude is arduous, however, for installation. The frame arrived two weeks before and the ambitious schedule had to be balanced by con- the end of the shutdown (Figures 21 and 22). Despite cerns for the long-term well-being of the staff. the anxiety over schedule and concerns about the size of equipment, the installation proceeded amazingly This balance was achieved through a shift pattern, with smoothly. With the completion of this job, the shutdown half of the crew being resident at Hale Pohaku one week was officially over and the keys handed back to the and half commuting, then alternating roles in the fol- operations staff, who had the difficult task of re-commis- lowing week. This, we felt, was much more sustainable sioning the systems. over the six-month shutdown and less likely to result in burn-out at the end of the work. Even with this work pat-

Figure 22: Installing the cryostat mounting frame onto JCMT. Figure 23: Hale Pohaku and the Visitors Center at 9,000 feet.

28 JCMT

tern, it was a daunting schedule, and commitment by the Conclusion staff was necessary before it could be considered viable. Fundamental to achieving this commitment was a full The SCUBA-2 Infrastructure Project was the largest and open discussion of the issues and potential solu- engineering project ever undertaken by the JAC. After tions, together with an understanding of the importance 18 months of planning, it was a success in virtually every of SCUBA-2 to the future of the JCMT. respect: the work was completed on schedule and within budget, and without any safety incidents. This success is The JAC is justifiably proud of its safety record, and directly attributable to the ETS staff at the JAC, without throughout the work, every effort was made to ensure whose dedication and commitment this would not have safe working conditions. Starting with the early planning been possible. We now look forward to the scientific of hazardous operations, through daily safety briefings promise of SCUBA-2. (Figure 24) and weekly safety audits, we strived to cre- ate a safety-conscious culture. We were delighted that, despite the industrial work environment and the difficult conditions, there were no safety incidents during the entire project.

Figure 24: Daily safety and work briefings. Figure 25: Installing rail tracks for the cryostat handling cart.

29 UKIRT/WFCAM image of the Sombrero Galaxy.

30 JAC Technical Support

Software and Computing Services development at the University of British Columbia), Sam Hart worked on developing the SCUBA-2 Observing Tool Much of the Software and Computing Services Division (OT), and Frossie Economou led the design effort for the work this year was influenced by the JCMT engineer- JCMT Science Archive. ing shutdown and the subsequent functional checkout of the telescope and final commissioning of the ACSIS Several staff changes occurred in the SCS Division correlator and the HARP receiver. This work involved this year: Jamie Leech left in June 2006, and Kynan a complete reconstruction and upgrade of the JCMT Delorey left in February 2007. Walther Zwart arrived in computer room, a complete rework of the communica- November 2006 to provide much-needed support for the tion paths around JCMT, needed fixes to the ACSIS glish/AIPS++ portions of the ACSIS software. real-time data reduction software, switching the JCMT data reduction pipeline over to use Starlink software, Engineering and Technical Services commissioning of multi-subsystem modes in ACSIS, final commissioning of the translator, recommission- The past 12 months have again been a busy period for ing RxW as a B- and D-band receiver, eSMA work, and the ETS Division. Key activities have included overhaul- planning and implementing the data archive with CADC. ing the HARP focal plane and preparing for the arrival of This work consumed much of the time of the following SCUBA-2. The shutdown of JCMT in February 2006 to staff: Tim Jenness, Frossie Economou, Brad Cavanagh, allow the SCUBA-2 infrastructure work to be undertaken Russell Kackley, Firmin Oliveria, Henry Stilmack, Craig continued into this reporting year, and was completed on Walther and Walther Zwart. schedule in August 2006. A summary of these activities in included elsewhere in this report. While all this was going on, Maren Purves modified all of the UIST software for compatibility with the new ARC In addition to these specific activities the ETS team has array controller. The new Starlink-based WFCAM data continued to deliver the necessary levels of service to reduction summit pipeline (mostly developed by Brad keep UKIRT and JCMT operational, including several Cavanagh) was used for the first time at UKIRT and is WFCAM/Cassegrain instrument changeovers for UKIRT. proving to be dependable and useful. Henry Stilmack and David Fuselier upgraded all nine of the WFCAM Turnover of staff in the Division has been relatively low (and now UIST) computers at UKIRT, providing for faster across the period of this report, but a notable departure throughput on the acquisition side, as well as a faster was that of Tomas Chylek, our mechanical engineer who data reduction pipeline. has moved to the Discovery Channel Telescope project in Flagstaff, AZ. He will be missed, and we wish him well In addition to all this work, preparations for SCUBA-2’s for the future. The major hit on project work with Tomas’ arrival at JCMT continued. Russell Kackley and Craig departure was that of the hardware required to silver Walther worked on the needed SCUBA-2 changes to coat the UKIRT primary in the Gemini coating tank. A the OCS, Tim Jenness continued working as technical solution for coverage of the mechanical design activities lead on the SCUBA-2 data reduction pipeline (under is being developed.

31 Administration Division

The year started at a brisk pace for the Administration by its new recruits over the past year. The recruitment Division, which encompasses the Human Resources process itself has also been reviewed and re-structured, (HR), Financial Management, and Outreach functions resulting in more focused and informative application of the JAC. In April, the UK Research Councils’ Internal forms that have greatly aided the selection procedure. Audit Service (RCIAS) conducted an audit of the JAC “to provide assurance on the management, financial and The Finance Team has also had a busy year as the new operational systems and internal controls to safeguard finance system (introduced in 2006) has bedded in. Ini- against waste, irregularity or fraud.” A large part of the tial concerns about the inability of the system to meet the audit focused on the controls that we operate to ensure JAC’s needs quickly dissipated, and a suite of reports that the funding we receive is used effectively and ac- has been developed and made available to Budget Man- counted for in accordance with the appropriate govern- agers to support the in-year monitoring and forecasting ance rules. The two-week audit resulted in a “Substan- of expenditure. In January, the team also supported an tial Assurance” rating (equivalent to an “A” in academic exercise to revalue the plant and machinery assets at parlance), which means that we have a sound system the JAC. This exercise is required every five years by of internal control, with only a few recommendations for the UK accounting regulations, and it is reassuring to improvement. By the end of March, all but two of the rec- record that all the assets could be found and valued! ommended improvements had been implemented (the remaining two being associated with activities to support And, finally, the Research Corporation of the Univer- SCUBA-2’s arrival later in 2007). sity of Hawai`i (RCUH), which employs the majority of the JAC staff, held their annual Outstanding Employee Elsewhere, the HR team’s focus has continued to be on of the Year Award in February. RCUH supports 300 maintaining a service, and terms and conditions of serv- projects employing some 2,700 staff, and the JAC was ice, that encourage staff to remain at the JAC. In Octo- very proud to learn that Vernon De Mattos, JAC Facil- ber, we introduced a new performance award scheme, ity Maintenance Manager, was placed runner-up in this which recognises individual and team efforts that go prestigious event (see Figure 26). beyond what might be expected normally. Fittingly, the first commendation was a team award to the Engineer- ing and Technical Services staff for their work on the SCUBA-2 Infrastructure Project (detailed elsewhere in this report). Since then nine more individual awards have been made.

In the 12 months covered by this report, staff turnover was relatively low with only eight staff leaving the organisation. In those instances where recruitment was necessary, the job advertisements attracted good-quality applicants, and the JAC has been very well served Figure 26: Vernon De Mattos placing runner-up at the RCUH Awards.

32 Science Education and Public Outreach

Science education and public outreach activities contin- As part of a new Hawaiì internship programme, JAC ued to increase during the year. JAC staff participated hosted a student intern this year, who worked with mem- in a number of school career and science fairs, provid- bers of the computing group on a web-based database. ing speakers, judges and prizes. As a result of higher This student will continue her studies in a related field at visibility during these larger education events, teacher the University of Hawaiì at Manoa. requests have been more frequent, and JAC staff visited schools all over the Big Island. A particularly important The JAC outreach officer attended two conferences, event was the “Journey through the Universe” week, a focusing on networking with outreach and press offic- U.S. national programme that selected Hilo as one of 10 ers from other astronomical institutions, exchanging sites in the country. Throughout one week in January, ideas and tools for education and press activities. JAC staff from the Mauna Kea observatories visited schools continues to be part of the Mauna Kea Observatories in the area, providing hands-on astronomy education. A Outreach Committee (MKOOC), where the outreach number of follow-up events aimed specifically at teach- officers from all the observatories on the Big Island and ers have taken place, with participation from JAC staff ‘Imiloa discuss and coordinate local outreach efforts. (Figure 27). JAC science and engineering activities were featured Another major public event was the annual AstroDay at several times in a variety of media, including the local the Prince Kuhio Plaza, the largest shopping mall on the newspaper and the PPARC “Frontiers” magazine. To island. JAC staff set up a booth with educational activi- further increase the visibility of JAC activities locally and ties and handouts. This event was attended by public at specific events, color brochures were created high- school groups, all observatories, and many other local lighting JAC science results for distribution at ‘Imiloa and groups. Over 15,000 people attended the event. Other the Mauna Kea Visitor Information Station. larger events were the Math-Science Conference for 7th Grade Girls, and the Onizuka Science Day, both held at the University of Hawaiì at Hilo.

JAC staff continued to provide speakers for the public talks at the Mauna Kea Visitor Information Station as part of the “Universe Today” series and the regular “As- troTalk” forum at the University of Hawai`i at Hilo. Speak- ers were featured several times in the new ‘Imiloa As- tronomy Education Center’s monthly “The Sky Tonight” series, where scientists from the observatories provide regular updates on their research. JAC staff have further provided support for ‘Imiloa for a variety of educational events, as well as contributing to the “Astronomy Picture of the Day.” Figure 27: Andy Adamson teaches class during Journey through the Universe.

33 Appendix

Staff Organisation in 2006/7

JAC HAWAII

Gary Davis Director JAC

Antonio Chrysostomou Andy Adamson Craig Walther Simon Craig Stuart Putland Associate Director Associate Director Head of Software & JCMT UKIRT Computing Services Chief Engineer Head of Administration (from 01/07)

Engineering & Technical JCMT UKIRT Software & Computing Administration Services Outreach Services Dan Bintley Tim Carroll Christine Campbell Ken Brown Inge Heyer Iain Coulson Chris Davis Brad Cavanagh Candee Corwin (50%) Tim Chuter Donna DeLorm Lucas Fuhrman Kyran Delorey (to 02/07) (from 03/07) Tomas Chylek (to 03/07) Jessica Dempsey Paul Hirst (to 09/06) Frossie Economou Velvet GonsalvesNases Vernon DeMattos (from 03/07) Jonathan Kemp (50%) David Fuselier Sharlene Hamamoto Marjorie Dougherty Per Friberg Tom Kerr Sam Hart Ian Midson Mark Horita Jim Hoge Sandy Leggett (to 07/06) Maren HauschildtPurves Susan O'Neal Lenwood Jack Jonathan Kemp (50%) Anna Lucas (75%) Tim Jenness Felisa Teramoto James Kaulukukui Jamie Leech (to 06/06) Mark Rawlings Russell Kackley John Kuroda Gerald Schieven Luca Rizzi (from 03/07) Firmin Oliveira Neal Oliveira Remo Tilanus Watson Varricattu Henry Stilmack John Pascual Ben Warrington (from 07/06) Walther Zwart Edward Sison Jan Wouterloot Thor Wold (from 11/06) Erik Starman Ming Zhu Jay Tsutsumi (vacancy) (Vacancy x2)

34 Appendix

JAC HAWAII

Gary Davis Director JAC

35 Appendix

Financial Statement 2006–2007

The financial statement below refers to the financial year from 1 April 2006 to 31 March 2007. The JAC is funded via the UK’s Science Budget through the Science and Technology Facilities Council (STFC) 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 1,483.5 JCMT New instrumentation 422.3 Observing costs 348.2 Total 422.3 Maintenance 677.4 Astronomical Research 51.4 Income Development 1,437.4 JCMT STFC (UK) 325.8 Total 3,998.0 NRC (CA) 62.5 UKIRT Running costs 1,466.6 NWO (NL) 34.0 Observing costs 560.5 Total 422.3 Maintenance 693.3 Astronomical Research 235.0 Development 110.9 Total 3,066.3 Income JCMT STFC (UK) 2,253.0 NRC (CA) 1,021.0 NWO (NL) 724.0 Total 3,998.0 UKIRT STFC (UK) 3,066.3 Total 3,066.3 ¹ Excludes the cost of 4.8 staff members directly recruited by partner countries.

36 Appendix

37 Appendix

Telescope Time Awards (UKIRT)

UKIRT Allocations, Semester 2006A (UK PATT) PI Title of Investigation Hours Blundell Sub-orbital-period resolution spectroscopy of SS 433 in the near-IR 12 Brocksopp Trigger and outburst mechanisms of X-ray transients 5 Buchanan The origin of thermally re-radiated emission in Seyfert galaxies 30 Chrysostomou Do cold grains align in dark molecular clouds? 8 Davis Integral-field and Echelle spectroscopy of jets from massive young stars 25 Evans The infrared evolution of V838 Mon 70* Fasano WFCAM Imaging of WINGS galaxy clusters 10 Fender Testing magnetic jet formation in black hole X-ray binaries 20 Ferguson Probing the outer regions of the Milky Way disk: A WFCAM study of the northern Galactic warp 22 Geballe High resolution 3-micron spectroscopy of molecules and haze in Jupiter and Saturn 20 Geballe Infrared spectroscopy of formaldehyde and methanol in hot cores 10

Gledhill IFU imaging of H2 in fast winds from hot post-AGB stars 15 Gledhill Imaging the circumstellar dust shells around hot post-AGB stars 20 Gledhill Near-IR imaging polarimetry of the Red Rectangle 6 Gosling Brackett-gamma survey of the Galactic Centre to identify accretion signatures 4 Hewett Imaging of dusty Ca II-selected damped Lyman-alpha systems at z~1 40 Hodgkin,Pinfield A UKIRT WFCAM search for transits around M stars 100b Jameson The ages of field L and T dwarfs 8 Jarvis AGN feedback processes in massive galaxy formation 30 Lucey A optical-NIR study of galaxy bulges and disks in nearby rich clusters 10 Lumsden Pilot project to study spectr. evolutionary seq. in deeply embedded massive protostars/YSOs 30 McHardy Evolution of sub-mJy radio population: WFCAM imaging a GMRT/Spitzer/X-ray Deep Survey Area 20 Miller Deep Impact mission support through observations of comet 73P/Schwassmann-Wachmann 3 15 Nisini Mapping the excitation of dense gas in the beams of young star jets 18 + Oka Study of the central molecular zone of the Galaxy using H3 and CO 12 Romanowsky Photometry of globular clusters and galaxy light in the Virgo Cluster 13 Scholz Variability of young stars and brown dwarfs in IC1396W 21 Smail A WFCAM survey of star-forming galaxies at z=1-9 in the COSMOS and UKIDSS UDS fields 55* Smartt NIR imaging of late-type galaxies to identify progenitors of future core-collapse supernovae 10 Swinbank Tracking black hole growth from sub-mm galaxies to QSOs 50 Tanvir Rapid IR follow-up of GRBs: searching for dark and distant afterglows 70*

38 Appendix

UKIRT Allocations, Semester 2006A (UK PATT) PI Title of Investigation Hours Teanby Mapping variations in Saturn’s atmospheric circulation with arsine and germane 15 Vink K-band line polarimetry on massive Young Stellar Objects 23 Warren Follow-up YJ imaging of UKIDSS LAS candidate z>6 quasars 12 Zapatero Near-infrared imaging polarimetry of young and field cool dwarfs 15

* Some of the allocation carries forward into subsequent semesters. b The project was scheduled as poor-weather backup in UKIDSS time.

UKIRT Allocations, Semester 2006A (UH) PI Title of Investigation Nights Granet Near-IR cluster survey 4

Reipurth A Wide-Field H2 survey 3 Sanders Hawaii UV/NIR imaging of the HST-ACS COSMOS 2-deg-square Treasury Field 7x0.4

Stanke An unbiased survey for protostellar H2 jets in the Rho-Oph molecular cloud 7x0.6 Takamiya The intergalactic component of the Virgo Cluster of Galaxies 4 Yang Near-infrared observations of Jovian Trojan asteroids 4

UKIRT Allocations, Semester 2006A (Japan) PI Title of Investigation Nights Inada The SDSS gravitationally lensed quasar survey 1 Ishihara Planetary-mass YSOs in the Ophiuchus dark cloud 2 Matsuoka Probing physical properties of broad-line regions in AGN with OI lines 1 Tanaka A search for high-z clusters at z > 1 2

39 Appendix

UKIRT Allocations, Semester 2006B (UK PATT) PI Title of Investigation Hours Caratti o Garatti NIR investigation of Class 0 jets as a probe of protostellar evolution 30 Chrysostomou Circular polarized imaging of the intermediate-mass star formation region NGC 2071 30 Clarke Near infrared spectroscopy of massive YSO candidates 40 Curran Spectroastrometry: A new way of establishing disc rotation? 5 Davis Calibrating the collimated jets in DR21/W75N 26 Dunlop The evolution of high-redshift quasar host galaxies 40* Edge The evolution of brightest cluster galaxies in the most massive clusters 20 Evans The aftermath of the 2006 eruption of the recurrent nova RS Oph 16* Fasano WFCAM imaging of WINGS galaxy clusters 14 Ferguson Probing the outer regions of the Milky Way disk: A WFCAM study of the southern warp region 16 Gledhill Near-IR imaging polarimetry of the Red Rectangle 6 Harries A near-IR polarimetric survey of the Taurus/Auriga star forming region 43 Irwin A WFCAM near-infrared survey of Local Group galaxies 25 Irwin Mapping cloud variations in Uranus’ atmosphere 8 Jarvis AGN feedback processes in massive galaxy formation 30 Juvela High-resolution mapping of interstellar clouds with near-infrared scattered light: TMC-1 40 Kendall Confirmation methane imaging of UKIDSS/LAS brown dwarf candidates from Early Data Release 18 Kishimoto The quasar big blue bump under hot dust emission 10 Lucey An optical-NIR study of galaxy bulges and disks in nearby rich clusters 4 Lumsden Pilot project to study spectr. evolutionary seq. in deeply embedded massive protostars/YSOs 25 McHardy Evolution of sub-mJy radio population: WFCAM imaging a GMRT/Spitzer/X-ray Deep Survey Area 14 Smail A WFCAM survey of star-forming galaxies at z=1-9 in the COSMOS and UKIDSS UDS fields 81 Trafton Response of Uranus’ thermosph./ionosph. to solar variability approaching solar minimum/equinox 42 van Loon Monitoring red giant variables in M33: star form. history, chemical enrichment, galactic structure 33* Vink Magnetic fields in Herbig Be stars and massive YSOs 15 Warren Follow-up J imaging of UKIDSS LAS candidate z>6 quasars: Finding a one in a million target 5

* Some of the allocation carries forward into subsequent semesters. Ten 2006A Cassegrain projects, totalling 119 hours, were carried forward into 06B due to very poor weather in the Spring of 2006.

40 Appendix

UKIRT Allocations, Semester 2006B (UH) PI Title of Investigation Nights Cowie The evolution of X-ray selected AGN 5 Liu Mining the Next-Generation IR Sky Survey 4 Reipurth Infrared monitoring of the Orion Nebula cluster 3 Rizzi The TGRB in the near infrared as a precise distance indicator 2 Sanders Hawaii NIR imaging of the HST-ACS COSMOS 2-deg-square Treasury Field 3 Walawender Near-IR imaging of shocks in Eastern Perseus 2 Yang Near-infrared and optical observation of Jovian Trojans 3

UKIRT Allocations, Semester 2006B (Japan) PI Title of Investigation Nights Inada The SDSS quasar lens search 1 Motohara Probe the assembly of galaxies and large scale structure in the high-z Universe 2 Takami A survey for fundamental CO emission towards pre-main sequence stars 1 Takata Scale of a proto cluster traced by massive red galaxies 1

UKIRT on Mauna Kea in Hawai`i. Photo by Inge Heyer.

41 Appendix

Telescope Time Awards (JCMT)

The following tables show the allocations for telescope time by the United Kingdom, Netherlands, International, Canadian, and University of Hawai`i queues for semesters 06B (1 October 2006 – 28 February 2007) and 07A (1 March – 31 July 2007). Since the telescope is generally queue-scheduled, the total time “allocated” by each queue is usually much larger than the total time available. Instead, for most queues, projects are simply ranked by scientific priority, and the PIs of the highest-ranked projects are invited to the telescope to observe their own and other projects, depending on the weather, scientific priority, and source availability. In each table, WB stands for the “weather band,” i.e.,WB 1 is extremely dry weather, WB 2 is very dry, WB 3 is dry, WB 4 is wet, and WB 5 is very wet weather. (“Dry” and “wet” refer to the amount of water vapour in the atmosphere, rather than the presence of precipitation, which, of course, requires the telescope to close.)

JCMT Allocations, Semester 06B (United Kingdom) PI Title of Investigation WB Hours Ceccarelli C A new method to probe cold baryonic matter around galaxies 2 16 Coulson I The D/H ratio in Jupiter-family comets 1,2,3 24 Dent W T Tauri gas discs in Taurus: completing a magnitude-limited survey 3 24 Edge A CO(2-1) in Cygnus-A—A challenge for ACSIS 3 5 Fuller G A spectral line survey of star-forming regions between 361 and 373 GHz 1,2 47 Fuller G Deuterium as a probe of depletion around HMPOs 3 20 Gomez H Molecular gas towards Kepler’s supernova remnant 3,4 22 Hatchell J Do pre/protostellar lifetimes depend on mass? 3 36 Jimenez-Serra I Measuring the electron density enhancement expected in C-shocks 2,3 20 Martin-Pintado J The physical conditions in the nuclei of ARP220 2,3 27 Moore T A HARP-B 13CO 3-2 pilot survey for the JCMT Plane Survey (JPS) project 2,3 45 Nisini B Probing the excitation of EHV protostellar jets through CO multifrequency observ. 1,3 17 Peretto N Studying the kinematics of filamentary Spitzer infrared dark clouds 3 60 Peretto N Tracing large-scale coherent collapse in the NGC2264-C protocluster 3,4 8 Pestalozzi M Studying the environment of new methanol masers 3,4 24 Salome P Mapping the CO(3-2) emission around NGC1275 2 12 Thi W-F Physical and chemical structure of circumstellar disks 3 24 Thi W-F Disk and outflow around a young brown dwarf 3 7 Thomas H Mapping depletion around HMPOs 3,4 48 Verma A A CO line survey of hyperluminous infrared galaxies 3,4 28 Viti S A statistical determination of clumpiness ahead of Herbig-Haro objects 3 9

42 Appendix

JCMT Allocations, Semester 06B (Canada) PI Title of Investigation WB Hours Azimlu M The effect of HII regions on star formation 5 50 Caselli P Probing the chemical evolution of the early universe 1 35 Di Francesco J H2D+ observations of starless cores 1 48 Di Francesco J A CO (2-1) line search for disks around brown dwarfs 4,5 54 Feldman P Search for SiO toward strong sources of extended red emission (ERE) 5 12 Klaassen P The dynamics of high mass star forming regions: JCMT followup 3 30 Klaassen P The dynamics of high mass star forming regions: SMA followup 4 8 Knee L Protostellar collapse around halo HII regions 3,5 38 Matthews B Kinematics and electron abundance of the rotating core of Barnard 1c 1,3 35 Matthews H Oort Cloud comets: A one-year target-of-opportunity program 3 60 Matthews H The molecular component of dusty Galactic regions 3 24

Muehle S H2CO as a tracer of the properties of the dense molecular gas in M82 1 50 Olmi L Spectral line follow up of Galactic plane starforming regions surveyed by BLAST 3 26 Plume R The formation of molecular clouds 3 24 Plume R A spectral line survey of star-forming regions between 361 and 373 GHz 2 24 Redman R Low-speed outflows from protostars in the IRDC G79.27+0.38 3,4 12 Schieven G Sequential star formation in L1340: Search for molecular outflows 3,4 100 Stankovic M PDR structure of the molecular gas in the Sgr A* environment 3,4 23 Wu Y Characteristics of high mass starless cores 3,4 39

JCMT Allocations, Semester 06B (Netherlands) PI Title of Investigation WB Hours Beaupuits J XDR diagnostic for NGC 1068 3,4 20 Decin L Molecular emission spectra probing the complex chemistry of AGB-star winds 3 52 Dominik C Gas masses and dust-to-gas ratio in protoplanetary disks 2 21 Helmich F A spectral line survey of star-forming regions between 361 and 373 GHz 2 5 Israel F CO isotopic ratios in active and merger galaxy nuclei 3 30 Tilanus R HARP-B CO(3-2) raster maps of M33, M83, and M51 2,3 72 van der Tak F H2D+ observations of starless cores 1 24 van Kenpen T Chemical/physical characteristics of envelopes and outflows of low-mass protostars 3 20 Wouterloot J Hot molecular outflows in globules? 1,4 15 Wouterloot J WB89-436/7: A study of a GMC in the far outer galaxy 3,4 24

43 Appendix

JCMT Allocations, Semester 06B (International) PI Title of Investigation WB Hours Cavalie T CO in the stratosphere of Saturn 1,2 17 Clancy R Contemporaneous observation of the Venus atmosphere with JCMT and Venus Express 2,3 32 Li D Blue and red velocity shifted components in L1544—molecular bullet or cloudlets? 3,4 24 Ramstedt S The mass loss and chemistry of S-type AGB stars 3 34 Sakai N Probing phys. conditions of early stage protostellar evol. w/complex organic molecules 3 12 Tsai C-W CO(3-2) investigation of luminous infrared merging galaxies 2,3 26

JCMT Allocations, Semester 06B (University of Hawai`i) PI Title of Investigation WB Hours Stanke T A CO 3-2 survey of Orion jets and outflows 1,2,3 112

JCMT Allocations, Semester 07A (United Kingdom) PI Title of Investigation WB Hours Bayet E Survey of sulfur-bearing species in starbursts: Stepping stone from Milky Way to high z 3,4 72 Davis C Mapping dynamic star formation across DR21/W75 3 36 Edge A CO(2-1) in Cygnus-A—A challenge for ACSIS 3 5 Emprechtinger M Probing the ortho to para ratio of H2D+ 1 8 Evans N The intracluster medium of M51 4,5 24 Evans N A submm survey of born-again giants 4,5 45 Fuller G The properties of the outflows from HMPOs 3 38 Fuller G A spectral line survey of star-forming regions between 361 and 373 GHz 1,2 36 Gomez H Molecular gas and dust towards Kepler’s supernova remnant 3,4 35 Greaves J Molecules from below the surface of Enceladus 2,3 24 Greaves J Do low-mass cores form planetary mass objects? 1,2 6 Lintott C CO diagnostics of jet/SNR interplay in SS433/W50: fossil interaction or jet excavation? 3,4 12 Lumsden S Outflows from young massive stars 2,3 36 Moore T A CO 3-2 survey of a portion of the inner Galactic plane 3 48 Pagani L Deuterated hydronium in L183 (L134N) 1 24 Patience J Search for molecular gas in transition disks around A & B stars in upper Sco OB Assoc. 2,3 34 Richer J Probing outflow dynamics and chemistry with HARP 3 24

44 Appendix

JCMT Allocations, Semester 07A (United Kingdom) PI Title of Investigation WB Hours Roberts H Comp. of distrib. of deuterated molec. in dense gas surround. low/high mass protostars 2 36 Thompson M Uncovering the relationship between methanol masers and molecular outflows 2,3 48 Tideswell D Molecular tracers of super star clusters 2,3 12 Tothill N Physical conditions of the outer layers of dense cores 4 12 Usero A Radiation feedback of starbursts on molecular ISM: HCO+/HOC+/CO+ network in M82 2,3 36 Verma A [CII]158um in a young Universe: A search in a UV luminous z=6.17 Lyman break galaxy 2 36 Whyatt W A statistical determination of clumpiness ahead of Herbig-Haro objects 3,4 6

JCMT Allocations, Semester 07A (Canada) PI Title of Investigation WB Hours Azimlu M The effect of HII regions on star formation 5 49 Bacmann A The abundance of H2H+ and gas temperature in the inner parts of pre-stellar cores 1 17 Caselli P Probing the chemical evolution of the early Universe 1 35 di Francesco J H2D+ observations of starless cores 1 24 Feldman P Search for SiO toward strong sources of extended red emission (ERE) 4,5 12 Friesen R H2D+ mapping in Oph B2: Probing deuteration chemistry in clustered star forming env. 1 48 Gibb A Probing molecular core mass function and the search for infall and outflows in M17-N 2 34 Jorgensen J Characterizing the strong deuteration in star forming regions 2,4 34 Klaassen P The dynamics of high mass star forming regions: JCMT Followup 3 30 Matthews B Kinematics and electron abundance of the rotating core of Barnard 1c 1 12 Matthews B Kinematics and electron abundance of the rotating core of Barnard 1c 3 23 Matthews H Modelling the upper atmosphere of Titan using molecular trace species 2 12 Matthews H The molecular component of dusty Galactic regions near l=44 degrees 3 24 Matthews H Following changes in the Jovian stratosphere 3 36 13 McCutcheon W Map. NGC 6334 in CO 3-2, CO 3-2, C18O 3-2, H2CO 5(23)-4(22), H2CO 5(05)-4(04) 2,3 24 Plume R Electron abundances & magnetic support in quiescent prototstellar core in Ophiuchus 3,4 41 Plume R A spectral line survey of star-forming regions between 361 and 373GHz 2 32 Rudolph A A search for circumstellar disks 3,4 6 Schieven G Sequential star formation in L1340B: Search for molecular outflows 3,4 10 Schneider N A CO 3-2 survey of the unexplored W48 molecular cloud complex 3 55 Seaquist E Methanol in the molecular clouds surrounding Sgr A* 2 37 Stankovic M PDR structure of the molecular gas in the Sgr A* environment 2 23

45 Appendix

JCMT Allocations, Semester 07A (Canada) PI Title of Investigation WB Hours Warren B Star formation & molecular gas in extended HI envel. of nearby gas-dominated galaxies 3 21 Wilson C Mapping molecular gas in (ultra)luminous infrared galaxies 3 24 Zhu M Characteristics of high mass starless cores 4 32

JCMT Allocations, Semester 07A (Netherlands) PI Title of Investigation WB Hours Baan W Diagnostics of the nuclear ISM of SBN and AGN 3,4 96 Benz A Internal or external irradiation of the S140 molecular cloud: UV versus X-rays 2,3 28 Bottinelli S Chemistry of disks surround. massive protostellar objects: complex organ. molecules 3,4 42 Bruderer S FUV and X-ray sensitive molecules in the water chemical network 1 31 Crapsi A Characterizing the gas content among the Serpens YSO clusters 2 17 Crapsi A Searching for massive pre-stellar cores through observations of N2H+ and N2D+ 2,3 20 Helmich F A spectral line survey of star-forming regions between 361 and 373GHz 2 32 Hill T Do all massive cores form stars? 3 72 Israel F Physics of the ISM in NGC 891 1,2,3,4 58 Israel F CO isotopic ratios in active and merger galaxy nuclei 3 40 Manthey E The warm gas in the advanced mergers NGC 4194 and NGC 4441 3 56 Monje R Complex chemistry in LIRG NGC4418: A deeply buried AGN or nascent starburst? 2 27 Perez-Beaupuit J An assessment of the nuclear power source in Seyferts: A chemical approach 2 40 Schneider N Study of photon dominated region (PDR) interface in the Rosette molecular cloud 2 24 Torstensson K Where methanol masers spring 2 24 van der TakF Search for extragalactic H3O+ 2 20 van Kempen T The physical characteristics of the envelopes and outflows of low-mass protostars 3,4 70 vanderWerf P A JCMT+IRAM mm/submm CO, HCO+, HCN line survey of luminous IRAS galaxies 1,2 88 Wouterloot J A survey of formaldehyde in the far outer Galaxy 4 25

JCMT Allocations, Semester 07A (International) PI Title of Investigation WB Hours Ceccarelli C A survey of D2H+ toward heavily depleted starless cores 1 Puravankara M Circumstellar disks and outflows from an optically visible, nearby, young massive star 3,4 Ramstedt S The mass loss and chemistry of S-type AGB stars 2,3,4 Sandor B Contemporaneous obs. of Venus atmosph. with JCMT, Venus Express & MESSENGER 2,3

46 Appendix

JCMT Allocations, Semester 07A (University of Hawai`i) PI Title of Investigation WB Hours Aspin C Outflows and natal reservoirs associated with FUor-like objects 1,2,3 12 Swift J Pre-stellar cores in infrared dark clouds 1,2 48 Williams J HARP mapping of the Elephant Trunk Nebula 1,2,3 40 Williams J Warm gas in protostellar disks 1 24

The JCMT dish under the Gortex membrane. Photo by Inge Heyer.

47 Appendix

Refereed Publications in 2006/7 (JCMT)

Belloche, Hennebelle, André, Strongly induced collapse in the Class 0 protostar NGC 1333 IRAS 4A, A&A, 453, 145 Bendo et al., The spectral energy distribution of dust emission in the edge-on spiral galaxy NGC 4631 as seen with Spitzer and the James Clerk Maxwell Telescope, ApJ, 652, 283 Bendo et al., Spitzer and JCMT observations of the active galactic nucleus in the Sombrero Galaxy (NGC 4594)”, ApJ, 645, 134 Birkmann, Krause, Lemke, Very cold and massive cores near ISOSS J18364-0221: Implications for the initial conditions of high- mass star formation, ApJ, 637, 380 Blake et al., On the cross-correlation of submm sources and optically selected galaxies”, MNRAS, 368, 732 Cartwright et al., Methods for analysing structure in molecular clouds, MNRAS, 369, 1411 Codella et al., Inside the large globule CB205: YSOs feeding multiple outflows, A&A, 457, 891 Coppin et al., The SCUBA half-degree extragalactic survey II. Submillimetre maps, catalogue and number counts, MNRAS, 372, 1621 Cullen, Alexander, Clemens, Gas in early-type galaxies: Cross-fuelling in late-type-early-type pairs?, MNRAS, 366, 49 de Ruyter et al., Keplerian discs around post-AGB stars: A common phenomenon?, A&A, 448, 641 Dye et al., An Investigation of the submillimeter background radiation using SCUBA and Spitzer, ApJ, 644, 769 Economou et al., Time-sensitive astronomy in non-robotic telescopes, AN, 327, 788 Fontani et al., Searching for massive pre-stellar cores through observations of N2H+ and N2D+, A&A, 460, 709 Gomez et al., Submillimetre emission from Eta Carinae, MNRAS, 372, 1133 Greaves, Space debris and planet detection, Astronomy & Geophysics, 47, 21 Hill et al., Millimetre continuum observations of southern massive star formation regions II. SCUBA observations of cold cores and the dust grain emissivity index, MNRAS, 368, 1223 Israel, Tilanus, Baas, CI and CO in the center of M 51, A&A, 445, 907 Ivison, Searching for a gigamaser in APM 08279+5255, and other short stories, MNRAS, 370, 495 Johnstone, Bally, Large-Area Mapping at 850mm. V. Analysis of the clump distribution in the Orion A south molecular cloud, ApJ, 653 383 Johnstone et al., Large Area Mapping at 850mm. IV. Analysis of the clump distribution in the Orion A south molecular cloud, ApJ, 639, 259 Jørgensen et al., The effect of a strong external radiation field on protostellar envelopes in Orion, A&A, 449, 609 Kirk, Johnstone, Di Francesco, The large and small scale structures of dust in the star-forming Perseus molecular cloud, ApJ, 646, 1009 Kirk, Ward-Thompson, Crutcher, SCUBA polarization observations of the magnetic fields in the pre-stellar cores L1498 and L1517B, MNRAS, 369, 1445 Klaassen et al., The possibly remnant massive outflow in G5.89-0.39. I. Observations and initial magnetohydrodynamic simula- tions, ApJ, 648, 1079 Knudsen et al., An ultradeep submillimetre map: Beneath the SCUBA confusion limit with lensing and robust source extraction, MNRAS, 368, 487 Lahuis et al., Hot organic molecules toward a young low-mass star: A look at inner disk chemistry, ApJ 636, 145

48 Appendix

Lestrade et al., Search for cold debris disks around M-dwarfs, A&A, 460, 733 Looney et al., Colliding clouds: The star formation trigger of the stellar cluster around BD +40 4124, ApJ, 642, 330 Moriarty-Schieven et al., Multigenerational star formation in L1551, ApJ, 645, 357 Nutter, Ward-Thompson, André, A SCUBA survey of L1689—The dog that didn’t bark, MNRAS, 368, 1833 Pope et al., The Hubble Deep Field-North SCUBA Super-map IV. Characterizing submillimetre galaxies using deep Spitzer imaging, MNRAS, 370, 1185 Poulton, Greaves, Cameron, Detecting a rotation in the Eta Eridani debris disc, MNRAS, 372, 53 Priddey et al., Millimetric properties of gamma-ray burst host galaxies, MNRAS, 369, 1189 Redman, Keto, Rawlings, Oscillations in the stable starless core Barnard 68, MNRAS, 370, L1 Reid, Wilson, High-mass star formation II. The mass function of submillimeter clumps in M17, ApJ, 644, 990 Reid, Wilson, High-mass star formation III. The functional form of the submillimeter clump mass function, ApJ, 650, 970 Ridge et al., The complete survey of star forming regions: Phase I data, AJ, 131, 2921 Sajina, The infrared spectral energy distributions of star-forming galaxies, Ph.D. Thesis, 2006, The University of British Columbia (Canada) Schöier, Olofsson, Lundgren, SiO in C-rich circumstellar envelopes of AGB stars: Effects of non-LTE chemistry and grain orption, A&A, 454, 247 Scott, Dunlop, Serjeant, A combined re-analysis of existing blank-field SCUBA surveys: Comparative 850mm source lists, combined number counts, and evidence for strong clustering of the bright submillimetre galaxy population on arcminute scales, MNRAS, 370, 1057 Seaquist, Lee, Moriarty-Schieven, A high-resolution map of 12CO J = 6-5 emission in the starburst galaxy M82, ApJ, 638, 148 Stanke, et al., An unbiased search for the signatures of protostars in the rho Ophiuchi molecular cloud II. Millimetre continuum observations, A&A, 447, 609 Tej et al., A multiwavelength study of the massive star-forming region IRAS 06055+2039 (RAFGL 5179), A&A, 452, 203 Teyssier et al., CO line emission from circumstellar envelopes, A&A, 450, 167 Thompson et al., A SCUBA imaging survey of ultracompact HII regions: The environments of massive star formation, A&A, 453, 1003 Türler et al., A historic jet-emission minimum reveals hidden spectral features in 3C 273, A&A, 451, L1 Vallée, Fiege, A cool filament crossing the warm protostar DR 21(OH): Geometry, kinematics, magnetic vectors, and pressure balance, ApJ, 636, 332 van der Tak et al., The chemistry of water in the envelopes and disks and outflows around young high-mass stars, A&A, 447, 1011 Vig et al., Infrared and radio study of star forming regions associated with IRAS 19111+1048 and IRAS 19110+1045, ApJ, 637, 400 Walawender et al., Multiple outflows and protostars near IC 348 and the Flying Ghost Nebula, AJ, 132, 467 Wang, Cowie, Barger, NIR analysis of the submillimeter background, ApJ, 647, 74 Ward-Thompson et al., SCUBA observations of the Horsehead nebula—What did the horse swallow?, MNRAS, 369, 1201 Williams, Andrews, The dust properties of eight debris disk candidates as determined by submillimeter photometry, ApJ 653, 1480 Young et al., Submillimeter Common-User Bolometer Array mapping of Spitzer C2d small clouds and cores, AJ, 132, 1998

49 Appendix

Refereed Publications in 2006/7 (UKIRT)

Ashok et al., Near-infrared and optical studies of the fast nova V4643 Sgr (Nova Sagittarii 2001), MNRAS, 368, 592. CGS4 Berger et al., Spectroscopy of GRB 050505 at z = 4.275: A log N(H I) = 22.1 DLA host galaxy and the nature of the progenitor, ApJ 642, 979. WFCAM Override Blay et al., Multiwavelength monitoring of BD +53 2790, the optical counterpart to 4U 2206+54, A&A 446, 1095 CGS4. UKT9 Brookes et al., CENSORS: A combined EIS-NVSS survey of radio sources II. Infrared imaging and the K-z relation, MNRAS, 366, 1265. UFTI Burgasser et al., A unified near-infrared spectral classification scheme for T dwarfs, ApJ, 637, 1067. CGS4 Chiar et al., Spectropolarimetry of the 3.4mm feature in the diffuse ISM toward the Galactic Center quintuplet cluster ApJ, 651, 268. CGS4+IRPOL Chiu et al., Seventy-one new L and T dwarfs from the Sloan Digital Sky Survey, AJ 131, 2722. CGS4, UFTI, UIST Service Christopher and Smail, A catalogue of potential adaptive optics survey fields from the UKIRT archive, MNRAS 365, 439. UFTI Archive Clarke et al., Evidence for variable outflows in the young stellar object V645 Cygni, A&A 457, 183. UIST, UFTI, Michelle Crowther et al., An ultraviolet to mid-infrared study of the physical and wind properties of HD 164270 (WC9) and comparison to BD +30 3639 ([WC9]), ApJ, 636, 1033. CGS4 Cruz et al., The 6C** sample of steep-spectrum radio sources: I. Radio data, near-infrared imaging and optical spectroscopy, MNRAS, 373, 1531. UFTI, UIST Davies et al., Near-infrared spectra of 12 Near-Earth Objects, Icarus, 186, 111. CGS4 Dye et al., The UKIRT Infrared Deep Sky Survey Early Data Release, MNRAS 372, 1227. WFCAM Elias-Rosa et al., Anomalous extinction behaviour towards the Type Ia SN 2003cg, MNRAS, 369, 1880. UIST Ellis et al., The colour-magnitude relations of ClJ1226.9+3332, a massive cluster of galaxies at z = 0.89, MNRAS, 368, 769. UFTI Gal-Yam et al., A novel explosive process is required for the gamma-ray burst GRB 060614, Nature 444, 1053. Override Gandhi et al., 4C +39.29—extended emission around a powerful Type 2 quasar, MNRAS 369, 1566. UFTI Geballe et al., The interstellar medium of IRAS 08572+3915 NW: H3+ and warm high velocity CO, ApJ, 644, 907. CGS4 Gorlova et al., On the CO near-infrared band and the line-splitting phenomenon in the yellow hypergiant Rho Cassiopeiae, ApJ, 651, 1130. CGS4 Service data Goto, Discovery of a new high-redshift QSO at z = 5.96 with the Subaru Telescope, MNRAS, 371, 769. UFTI Hales et al., Near-infrared imaging polarimetry of dusty young stars, MNRAS, 365, 1348. UIST+POL Hewett et al., The UKIRT Infrared Deep Sky Survey ZYJHK photometric system: Passbands and synthetic colours, MNRAS 367, 454. WFCAM Howell et al., Mass determination and detection of the onset of chromospheric activity for the substellar object in EF Eridani. ApJ, 652, 709.UFTI Service Hurkett et al., GRB 050505: a high-redshift burst discovered by Swift, MNRAS 368, 1101. WFCAM Override Imanishi et al., Infrared 3-4 micron spectroscopic investigations of a large sample of nearby ultraluminous infrared galaxies, ApJ 637, 114. CGS4

50 Appendix

Inskip, et al.,Deviations from passive evolution—star formation and the ultraviolet excess in z~1 radio galaxies, MNRAS, 367, 693. UFTI Service data Inskip, et al., Deep spectroscopy of 9C J1503+4528: A very young compact steep spectrum radio source at z=0.521. MNRAS, 370, 1585. UFTI Jakobsson et al., A mean redshift of 2.8 for Swift gamma-ray bursts, A&A, 447, 897. UFTI Override Justtanont et al., Near-infrared observations of water-ice in OH/IR stars, A&A, 450, 1051. CGS4 Khosroshahi et al., The central elliptical galaxy in fossil groups and formation of brightest cluster galaxies, MNRAS, 372, L68. UIST Khosroshahi et al., A fossil galaxy cluster: An X-ray and optical study of RX J1416.4+2315, MNRAS, 369, 1211. UIST Kundurthy et al., Mid-IR observations of T Tauri stars: Probing the star-disk connection in rotational evolution, AJ, 132, 2469. Max Leggett et al., JHK observations of faint standard stars in the Mauna Kea Observatories near-infrared photometric system, MN- RAS 373, 781. UFTI Levan et al., The first Swift X-ray flash: The faint afterglow of XRF 050215B, ApJ, 648, 1132. UFTI Override Lodieu et al., New members in the Upper Scorpius association from the UKIRT Infrared Deep Sky Survey Early Data Release, MNRAS, 373, 95. WFCAM Lynch et al., Early infrared spectral development of V1187 Scorpii (Nova Scorpii 2004 No. 2), ApJ 638, 987. CGS4, UIST Mason et al., Spatially-resolved mid-infrared spectroscopy of NGC 1068: The nature and distribution of the nuclear material, ApJ 640, 612. CGS4 McLure et al., The discovery of a significant sample of massive galaxies at redshifts 5 < z < 6 in the UKIDSS Ultra Deep Survey Early Data Release, MNRAS 372, 357. WFCAM Melin et al., Variability in the H3+ emission of Saturn: Consequences for ionisation rates and temperature, Icarus, 186, 234. CGS4 Migliari et al., Spitzer reveals infrared optically thin synchrotron emission from the compact jet of the neutron star X-ray binary 4U 0614+091, ApJ, 643, L41. UFTI Service Misawa et al., Near-infrared search for CIV absorption counterparts along the lines of sight to pair quasars, AJ, 131, 34. UFTI Mugrauer et al., HD 3651 B: The first directly imaged brown dwarf companion of an exoplanet host star, MNRAS, 373, L31. UFTI Oates et al., Anatomy of a dark burst and the afterglow of GRB 060108 MNRAS, 372, 327. WFCAM Override data Oliveira et al., Circumstellar discs in the young Sigma Orionis cluster, MNRAS, 369, 272. UIST Pavlenko et al., Spectral energy distribution for GJ406, A&A, 447, 709. CGS4 Price et al., Cosmological implications of the very high redshift GRB 050904, ApJ, 645, 851. UFTI Ravikumar et al., Photometric scaling relations for bulges of galaxies. A&A, 446, 827. IRCAM3 Reid et al., 2MASS J22521073-1730134: A resolved L/T binary at 14 parsecs, ApJ, 639, 1114. CGS4 Rothberg and Joseph, A survey of merger remnants II The emerging kinematic and photometric correlations, AJ, 131, 185. UIST Saumon et al., Ammonia as a tracer of chemical equilibrium in the T7.5 Dwarf Gliese 570D, ApJ, 647, 552. CGS4

51 Appendix

Simpson et al., Extremely red objects in the UKIDSS Ultra Deep Survey Early Data Release, MNRAS, 373, L21. WFCAM Stockton et al., Extremely red objects in two quasar fields at z ~1.4, ApJ, 650, 706. UFTI Swinbank et al., Galaxies under the cosmic microscope: Resolved spectroscopy and new constraints on the z=1 Tully-Fisher relation, MNRAS, 368, 1631. UIST Swinbank et al., The link between submillimetre galaxies and luminous ellipticals: near-infrared IFU spectroscopy of submillimetre galaxies, MNRAS, 371, 465. UIST Tafalla et al., Star formation in the vicinity of the IC 348 cluster, A&A, 456, 179. UIST Commissioning Taubenberger et al., SN 2004aw: Confirming diversity of Type Ic supernovae, MNRAS, 371, 1459. UIST Target of Opportunity Tej et al., A multiwavelength study of the massive star forming region IRAS 06055+2039 (RAFGL 5179), A&A, 452, 203. UFTI Service data

Todd and Ramsay Howat, Imaging and integral-field spectroscopy of shocked H2 around G25.65+1.05, MNRAS, 367, 238. CGS4, UFTI, UIST commissioning Topalovic et al., Diamonds and polycyclic aromatic hydrocarbons in the circumstellar environment of the Herbig Ae/Be star Elias 1, MNRAS, 372, 1299. UIST van Breukelen et al., Galaxy clusters at 0.6 < z < 1.4 in the UKIDSS Ultra Deep Survey Early Data Release, MNRAS, 373, L26. WFCAM Varricatt and Ashok, WR 143: A Wolf-Rayet binary, MNRAS, 365, 1365. UIST, CGS4 Service Watson et al., A logNHI = 22.6 damped Lyα absorber in a dark Gamma-Ray Burst: The environment of GRB 050401, ApJ, 652, 1011. WFCAM

UKIRT in beautiful weather on Mauna Kea in Hawai`i. Photo by Inge Heyer.

52 Appendix

Committee Membership as at 31 March 2007

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 A. Edge (Durham University) Dr T. Moore (Liverpool John Moores University) Dr R. Joseph (University of Hawai’i) Dr J. Richer (University of Cambridge) Dr P. Lucas (University of Hertfordshire) Dr R. Stark (NWO/GBE, Netherlands) Dr P. Sarre (University of Nottingham) Dr P. van der Werf (Leiden Observatory) Dr N. Tanvir (University of Leicester) Dr C. Vincent (PPARC) Dr D. Telfer (PPARC) Secretary Dr J. Williams (University of Hawai’i) Dr D. Telfer (PPARC) Secretary UKIRT TAG Community Representatives Dr A. Edge (Durham University) Chair Dr G. Cotter (University of Oxford) Dr J. Stevens (University of Hertfordshire) Dr P. Lucas (University of Hertfordshire) Dr F. Helmich (SRON, The Netherlands) Dr A. Ferguson (University of Edinburgh) 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) Technical Secretary Dr H. Matthews (NRC) Chair Dr J. Stevens (University of Hertfordshire) Dr J. Hatchell (University of Exeter) Dr F. van der Tak (SRON, The Netherlands) Dr G. Schieven (Joint Astronomy Centre) Technical Secretary

53 Appendix

Joint Astronomy Centre Seminars in 2006/7

Date Title of Seminar Speaker Affiliation 19 April The BT2 water line list reveals interesting changes in the Deep Impact Bob Barber University spectrum College London 3 May New results on the rotating accretion disk surrounding the young high- Goran Sandell SOFIA/USRA mass star NGC 7538S 18 May Globular cluster populations in early-type galaxies Maren Hempel Michigan State University 13 June James Clerk Maxwell: The Man who Changed Everything Gerald Schieven JAC 23 June SCUBA-2 project update Wayne Holland UKATC, Edinburgh 7 July Large scale extinction mapping Dirk Froebrich Dublin Institute for Advanced Studies 20 September CASSIS, a software package to speed up the scientific analysis of Emmanuel Caux CESR, spectral data Toulouse, France 2 October High-mass star formation in DR21/W75 - the big picture courtesy of Chris Davis JAC WFCAM, SPITZER and SCUBA 4 October Outflow and Accretion in Massive Star Forming Regions Pamela Classen McMaster University 6 November First Results from the UKIDSS Ultra-Deep Survey Omar Almaini University of Nottingham, UK 8 November Studying the disks in young stellar objects with mm interferometry Dave Lommen Leiden Observatory, The Netherlands 17 November The Early Phases of Star Formation Di Li JPL/Caltech, Pasadena 28 November Staff Presentations to the JCMT Board Gerald Schieven, JAC Ming Zhu, Simon Craig, Tim Jenness 28 November The ‘Imiloa Astronomy Center of Hawai`i Peter Giles ‘Imiloa Astronomy Center, Hilo

54 Appendix

Date Title of Seminar Speaker Affiliation 30 November Staff Presentations to the UKIRT Board Tim Jenness, JAC Watson Varricattu, Andy Adamson 8 January Star Formation in Perseus Jenny Hatchell Exeter, UK

9 March CONDOR—A new chance to investigate deuterium chemistry Martin University of Emprechtinger Koeln, Germany

JCMT awaiting another night’s observing. Photo by Inge Heyer.

55 Appendix

Abbreviations and Acronyms

ACSIS Auto-Correlation Spectrometer and Imaging System CGS4 Cooled Grating Spectrometer 4 CSO CalTech Submillimeter Observatory DAS Digital Autocorrelation Spectrometer DRAO Dominion Radio Astrophysical Observatory (Canada) 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 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 PI Principal Investigator 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 SCUBA-2 Submillimetre Common-User Bolometer Array 2 SMA (Harvard Smithsonian) Submillimeter Array STFC Science & Technology Facilities Council (UK) 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