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Gemini South Explores a Young Planetary System Inside This Issue
• The Gemini Deep Deep Survey • Recent Science Highlights • Gemini Instrumentation Update • StarTeachers and Public Information & Outreach Update • Meet Gemini South’s Peter McEvoy • A Visit to the New Gemini South Base Facility
Interior of the Frederick C. Gillett Gemini Telescope (Gemini North) by moonlight. This 50-second exposure was obtained on February 9th, 2003 using the same equipment as the images on the inside front cover.
NsLtrCvr0603rev2 1 5/16/03, 4:55:16 PM STARS OVER WELCOME TO THE NEW GEMINI GEMINI NORTH SOUTHERN OPERATIONS CENTER
The star-trail image above is a “stack” of about 100 images 50-second exposure. A dark frame subtraction was also used from a new time-lapse movie of the early summer sky rising to reduce noise from the charge-coupled device (CCD) in over Gemini North. A final image was added that reveals the camera. the stars offset by about 20 minutes and shows the stars of the constellation of Scorpius (among others) over the The smaller images shown at the top are individual frames Gemini dome. Automobile tail-lights can be seen as well from the sequence obtained during the course of the night. as a red light that was used to highlight the dome. The The image at left shows the first glow from the early yellowish light on the right side of the dome is light from morning sunrise and the rising Milky Way. The image at the setting moon, and the light on the left side of the dome right reveals the final glow of evening twilight with the 10- is from the first glow of dawn. A Nikon D1X digital camera day old moon (not visible) still high in the sky illuminating was used with a AFNikkor 14mm lens (at f/2.8) for each the Gemini enclosure. Both images have the same technical specifications as the star-trail image.
Gemini Observatory Images
NsLtrCvr0603rev2 2 5/16/03, 4:55:26 PM Published twice annually in June and December. Distributed to staff, users, organizations and others involved in the Gemini Observatory. THROUGH A CRADLE OF DUST: GEMINI EXPLORES A YOUNG PLANETARY SYSTEM
Scott Fisher A team from the University of Florida and Gemini Observatory obtained this data with Gemini South in December 2001. Team members include: C. M. Telesco, N. Mariñas, R. S. Fisher, J. T. Radomski, R. K. Piña and T. L. Hayward. ntil recently, Beta Pictoris was a relatively bright (mv = 3.9) Ubut unremarkable star in the southern constellation Pictor. That all changed when the Infrared Astronomy Satellite (IRAS) observed it in 1984.
What IRAS discovered was that the star emitted much more infrared radiation than was expected for a normal main- sequence type-A star. This “excess” infrared emission was detected at all the wavelengths IRAS could observe: 12, 25, 60 and 100 microns. Moreover, the excess was strong. After calibration of the data, it was found that the source is at least an order of magnitude brighter than expected at mid- and far-infrared wavelengths (λ > 12 microns). The origin of the excess emission was attributed to emission from a disk of dust surrounding the star that was being heated by the star itself. This hypothesis was subsequently proven correct by the fi rst images of the disk taken soon after the IRAS observations. Figure 1: Beta Pictoris at 18 microns. Here we see emission from the star as the bright source in the center of the image In part due to its proximity to Earth with the disk extending to either side. Particularly interesting (and never seen before) is the small-scale structure in the (19.3 parsecs), the dust disk around Beta disk. The “S curve” shape seen in the lower right side of the disk is likely caused by one or more as-yet-unseen planets orbiting the central star. This kind of structure is akin to the “wake” of the planets as they shape the distribution of dust Pictoris is one of the few that is bright while circling deep within the disk itself. (See color image on cover.)
Gemini Newsletter #26 - June 2003 1
NsLtr0603txt-rev2 1 5/16/03, 4:56:27 PM enough and large enough in the sky to study in detail. Indeed, Beta Pictoris has become the archetypal proto-planetary disk source and has been studied intensely for the last 20 years at most wavelengths, from the ultraviolet to radio.
We have continued the study of this archetype by observing it at mid-infrared wavelengths (10 and 18 microns) with OSCIR on Gemini South. The data we present here are the highest resolution images of the disk ever made at these wavelengths. The southern declination (-51 degrees) of Beta Pictoris combined with the excellent image quality provided by OSCIR and Gemini South let us resolve structure in the disk to an unprecedented resolution of approximately (~) 0.5 arcseconds at 18 microns. These images of the disk are also among the deepest ever obtained in the mid-infrared. In particular, we have resolved the disk at the “short” wavelength of 10 microns to
the same extent as at 18 microns. This has Figure 2: Map of the optical depth of the dust in the Beta Pictoris disk. The optical depth is a measure of how dense important consequences on how we can the dust is along the line of site at a given point in the disk. The position of the central star is at the central cross. The use our data to study the disk, which we inner 40 astronomical units of the map are blocked due to contamination from silicate emission, which skews the discuss in the following paragraphs. calculation of the optical depth. The red lobes on either side of the disk (see color image on the cover) likely represent a “ring-like” structure in the disk that is related to the “S curve” seen in Figure 1. This is additional evidence for perturbation of the dust by planetary bodies within the disk. There is good reason to observe these disks contours are spaced logarithmically. Another exciting discovery in our data at mid-infrared wavelengths. Not only Photospheric emission from the central is the presence of what seems to be does the dust of the disk glow brightly star is seen as the bright white spot in the a ring-like structure within the disk. at these relatively long wavelengths, it center of the disk, and the disk itself is Evidenced by brighter clumps of emission is also only in this part of the spectrum seen as the elongation of the source to the seen symmetrically in both lobes of the that the contrast between the extremely northeast and southwest (north is up, and 18-micron image, these “rings” likely bright central star and the relatively faint east is to the left). trace regions of space where there is an emission from the dust is low enough that enhanced density of the dust due to the the disk is not overwhelmed by its stellar This image shows that we have strongly shrouded planets sculpting the disk from host as it is in the visible, and to a certain detected the emission from the disk to a within. extent, in the near-infrared. Because of diameter of greater than 200 astronomical this, we do not need to observe the source units. Perhaps the most striking features As we previously mentioned, a unique with a coronagraph that would block out of Figure 1 are the never before seen aspect of this data set is that we have the inner section of the disk, which is a small-scale structures detected in the detected emission from the disk at 10 very important consideration in this case approximate mid-plane of the disk. The microns to the same extent as at 18 since we are trying to study the disk as “S curve” shape seen in the southwest lobe microns. This is a signifi cant point since close to the central star as possible. (lower right) is particularly exciting since observing the disk at two mid-infrared it may be direct evidence for one or more wavelengths gives us the information In Figure 1, we show our 18-micron as-yet-unseen planetary companions we need to investigate the temperature, image of Beta Pictoris with contours of orbiting the star. Ongoing modeling of density and even the size of the dust constant-brightness overlaid. Presented the structure implies that this kind of grains that are emitting the radiation. with a 0.375-arcsecond Gaussian smooth structure is akin to the “wake” of the applied to the data, the lowest contour planet(s) as it travels through the disk In Figure 2, we show a map of the (edge of the color shading) traces three and redistributes the dust through its optical depth of the dust in the disk. This times the smoothed noise in the image gravitational infl uence. is essentially a measure of how dense the (3σ = 31 mJy/square arcsecond). The dust is along the line of sight at a given
2 Gemini Newsletter #26 - June 2003
NsLtr0603txt-rev2 2 5/16/03, 4:56:32 PM point in the disk. Only possible due to the high-quality data we have at two mid- infrared wavelengths, this map provides us a fi rst look at several previously unseen and exciting characteristics of the disk.
The central part of the image is masked out due to contamination of the optical depth map by emission from warm silicate grains in that region of the disk. On the broadest scale, we can see that the disk has a toroidal shape (think of a bagel turned on its side and cut in half; you can see the two lobes pointed toward us as the large green areas). The “doughnut” shape of the disk has been theorized for several years now and is not too surprising to see. However, the small-scale structures seen within the large lobes are entirely new. Analysis of these substructures has revealed that the densest part (the red areas on the cover color image) of the disk is likely related to the ring-like structure seen in the direct images. It is also interesting to note that the highest density region of the disk is spatially coincident with the “S Figure 3: Scan through the map shown in Figure 2. The scan runs through the peak in optical depth in the lower right curve”’ seen in Figure 1. and upper left (red spot on either side of the star). The lower values of optical depth in the center of the disk represent a central cleared region where there is little dust present. Similar in size to our Solar System, this inner hole seems to define the size of the Beta Pictoris planetary system and may be giving us our very first mid-infrared look at an exo-solar The line cut through the disk presented in “Kuiper belt.” Figure 3 reveals perhaps the most exciting discovery yet. The area of low optical Caught in the act of forming a planetary in mind, Gemini will be able to explore depth in the center of the disk represents system, Beta Pictoris and its disk give us a this (and other) circumstellar disks with a central cleared region that is essentially snapshot glimpse at what we believe the unprecedented resolution and sensitivity. devoid of dust. Since we expect the dust Solar System looked like approximately 5 Using front-line, large-aperture telescopes to spiral into the star under the force of billion years ago. With an estimated age like Gemini in the mid-infrared is the gravity in a relatively short period of time, of around 20 million years, the central star best way to see through the cradles of dust the fact that this cleared region exists is and disk are very young, so young in fact hiding these baby solar systems, which in the strongest evidence yet for planetary we believe that the star has only recently turn will let us extend the understanding companions. Namely, we believe it is the reached the main sequence. However, it is of the origin of our own Earth. presence of planets that are “sweeping up” in this early stage of evolution where the the dust as it falls toward the star that remnant material from the formation of keeps this region clear. Interestingly, the the star itself aggregates and coalesces into central cleared region is almost the exact bodies that will form, or have formed, into size of our own Solar System. Given the planets like those in the Solar System. much higher density of dust just outside this cleared region, we believe that what Probing the detailed structure of these we are seeing in this map is the fi rst mid- disks is exactly the kind of project for which infrared detection of an exo-solar Kuiper Gemini was intended. Designed from the belt. ground up with infrared-optimization
Gemini Newsletter #26 - June 2003 3
NsLtr0603txt-rev2 3 5/16/03, 4:56:33 PM THE GEMINI DEEP DEEP SURVEY: Status Report and Overview of the GMOS Nod-and-Shuffle Mode
The Gemini Deep Deep Survey Team R. G. Abraham (University of Toronto; Canadian Principal Investigator); K. Glazebrook (Johns Hopkins University; Co-U.S. Principal Investigator); P. McCarthy (Observatories of the Carnegie Institution of Washington; Co-US Principal Investigator); R. Carlberg (University of Toronto); H. W. Chen (Massachusetts Institute of Technology); D. Crampton (Herzberg Institute of Astrophysics, National Research Council [NRC] Canada); I. Hook (Oxford University); I. Jørgensen (Gemini Observatory) R. Marzke (San Francisco State University); R. Murowinski (Herzberg Institute of Astrophysics, NRC Canada); K. Roth (Gemini Observatory); S. Savaglio (Johns Hopkins University)
onventional spectroscopy of diffi cult to obtain. Telescope (Gemini North) on Mauna galaxies at redshifts of 1
4 Gemini Newsletter #26 - June 2003
NsLtr0603txt-rev2 4 5/16/03, 4:56:33 PM It is important to emphasize that in most ways N&S observing with GMOS is target Night sky emission lines the same as normal observing with the instrument. However, life is far simpler with N&S mode once the photons have A Nod distance on sky been collected because sky subtraction is reduced to a trivial operation e.g., a single Image Reduction and Analysis Facility Shuffl e distance on CCD (IRAF) command that subtracts the skies as an entire frame of data in one step B automatically. As will be described below, the added complexity of N&S comes at the initial mask design stage.
The observing procedure for N&S is as follows: A–B 1) Calibration data (arcs/fl ats/standards/ etc.) are obtained in the normal way. It is not necessary to shuffl e these. In fact, it Figure 1: Schematic of nod-and-shuffl e for a single slit. When the telescope is in the “object” position, CCD area “A” may not even be necessary to use them to records a spectrum. The “sky” position records the nodded spectrum (in this case the telescope has been nodded a few arcseconds along the slit direction). The area “B” is non-illuminated by the mask and serves as a storage area for the fi rst order N&S as it makes bias and fl at “sky position.” The image difference subtracts the sky, and leaves a positive and negative object spectrum for subsequent fi eld corrections unnecessary. For higher extraction. order corrections, it may be necessary to shuffl e bias/dark frames. If biases and 2) The shutter is closed, and charge is required between telescope motion and darks are to be taken in N&S mode, then shuffl ed by +Y pixels. charge motion embodied by this sequence for bias frames the number of nod and is fully automated. Once initiated, it shuffl e cycles (described below) should be 3) The telescope is moved to a second is transparent to the observer at the the same as for the science observations. position (position B). telescope. All that is required to subtract For dark frames, all parameters should the sky from the spectrum is to subtract be identical to those for the science 4) The shutter is opened at position B, the sky portion of the CCD image observations. and the observation is continued. from the object portion of the CCD image (conveniently accomplished with 2) The fi eld should be acquired in the 5) The shutter is closed, and charge is the gnssky subtask in the Gemini IRAF normal way by centering the reference shuffl ed by -Y pixels. software distribution). At this point, the stars in their mask apertures. sky-subtracted spectrum can be extracted 6) The telescope is moved back to in the usual way with the usual tools. 3) Guide stars should be set up on probes, position A. As will be described below, some mask and their placement should bear in mind designs allow the object to be observed the nod vector. 7) The procedure is iterated until the at a different position on the slit, or on exposure is complete. The fi nal exposure a separate slit, while the telescope is at At this point several parameters must be set time is the product of the subintegration position B. In which case, a positive and before N&S observations can be initiated. time and the number of subintegrations. negative object spectrum results, and the These are: (i) the shuffl e distance, Y; (ii) two must be extracted separately (and the subintegration time; and (iii) the In addition to these steps, we have found the latter needs to be multiplied by -1 number of subintegrations. With the that (because of low-level charge traps before the two spectra added together can specifi cation of these parameters, the in the EEV detectors) the quality of maximize the signal-to-noise ratio). N&S observation can be initiated. The combined N&S spectra is enhanced by observing system proceeds by activating dithering the GMOS detector controller A trade-off between observing effi ciency the following nod-and-shuffl e sequence: translation stage and central wavelength and multiplexing lies at the heart of N&S, position slightly between long exposures. and this can make mask design quite 1) An observation is taken at a fi rst tricky. The optimal mask design depends position on the sky (position A) while The common case of nodding along a sensitively on target brightness and sky guiding. slit is shown schematically in Figure 1 density. For example, one may choose for a single slit. The close coordination to maximize multiplexing using many
Gemini Newsletter #26 - June 2003 5
NsLtr0603txt-rev2 5 5/16/03, 4:56:34 PM (a) (b) (c) is shuffl ed in one large shuffl e. In this case, 66% of the detector must be used for storage, which is larger than Case 1, but still less than standard MOS modes. This would be a good design for fi elds in which a compact distribution of objects is to be observed (such as a grouping of HII regions or emission-line knots in a single galaxy).
Case 3 (see Figure 2c): An intermediate Buffer storageShuffl e Buffer storage Buffer storage Shuffl e case. In many cases, a design such as this
Shuffl e is probably optimal in terms of packing density and minimization of storage overhead. Here the number of interfaces
Objects between object-sky regions in the mask
ed Spectra Slit Masks is reduced since these have to be greater than the instrumental PSF width.
Shuffl Sky For the GDDS, we chose to use a Case 1 mask design because our prime targets Figure 2: Illustration of masks with different shuffl e distances. The top row shows the input masks, and the bottom row (infrared-selected candidate 1 Case 1 (see Figure 2a): The shuffl e distance is small, and the sky image is recorded immediately below each object image. In this limit (for high densities), 50 percent of the detector is used for storage. The packing density is limited by the necessity to leave small gaps between the images to allow for the Point Spread Function (PSF) width. This case is perhaps the easiest to deal with as it requires no modifi cation to the mask- Figure 3: An image showing the “supercombined” GDDS 22h mask. Object spectra are sandwiched between positive and negative sky spectra on the mask. The inset shows a blow-up of a small region showing part of four spectra. These making software. One can design effective show positive and negative continua and emission lines. 6 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 6 5/16/03, 4:56:35 PM microshuffl ing mode of N&S allows us to observe 65 to 85 red-selected galaxies GDDS-01-1724 in each 5’x5’ GMOS fi eld. Two fi elds have been completed to date, and the two remaining fi elds are being observed in semester 2003A. z=0.994 I=21.7 Our sample is taken from the Las GDDS-01-1543 Campanas Infrared Survey (LCIR) and is K-band selected to a limit of K=20.8 that is nearly a magnitude deeper than the K20 survey (McCarthy, et al., z=1.131 I=23.7 2001; Chen, et al., 2001; Firth, et al., GDDS-01-1255 2001). Photometric redshifts from the 8-color LCIR imaging survey allow us to reject the z<1 foreground. The high- slit density afforded by N&S allows us to add additional I-band-selected and z=1.338 I=23.8 photo-z-fi ltered objects in regions of the fi eld devoid of suitable K-selected GDDS-15-2172 objects. A sky-subtracted GMOS frame showing how this sky density is translated to spectral coverage on the CCD frame is shown in Figure 3. This z=1.561 I=24.1 frame is the result of running a combined data frame through the Gemini IRAF GDDS-15-2264 package’s gnssky subtask, which is used to subtract a shifted copy of the image from itself, resulting in regions of clean- sky-subtracted slits sandwiched between z=1.671 I=24.3 light and dark bands that correspond to noise where the data has been subtracted out-of-phase. Figure 4: Montage of 100ks Gemini GMOS nod-and-shuffled spectra from the GDDS. Ground-based I-band images (in ~0.8 arcsecond seeing) are shown at right. Objects shown span a redshift range of 0.994 Gemini Newsletter #26 - June 2003 7 NsLtr0603txt-rev2 7 5/16/03, 4:56:36 PM the redshift and magnitude limit of the CFRS. This spectrum illustrates the spectacular signal-to-noise ratio achieved in 100ks with Gemini/GMOS for galaxies near the limits of the previous generation of surveys. Each of the four other representative spectra demonstrate our ability to determine absorption line redshifts squarely in the middle of the so- called redshift desert, and show canonical ultraviolet spectral features and the typical signal-to-noise achieved for fainter galaxies in our sample. GDDS-01-1543 (z=1.13) and GDDS-01-1255 (z=1.34) are well matched by a local early-type galaxy template (overlaid on the object spectra in the fi gure), while GDDS-15- 2172 (z=1.56) and GDDS-15-2264 (z=1.67) show narrow metallic absorption features characteristic of local starbursts and originating in the galaxies’ interstellar medium (ISM). The K-band-selected objects in Figure 4 that are red at rest visual wavelengths but which show blue rest-ultraviolet continua are particularly interesting. Figure 5 shows a composite spectrum obtained by combining individual spectra for 13 Figure 6: I-K color as a function of redshift for the GDDS + LDSS (Low-Dispersion Survey Spectrograph) such systems at 1.3 8 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 8 5/16/03, 4:56:37 PM RECENT SCIENTIFIC HIGHLIGHTS Jean-René Roy & Phil Puxley he year 2002 was the fi rst year and shuffl e,” this technique synchronizes Gemini North telescope. Although of abundance for referred papers a small shift in the telescope’s pointing no Jupiter-like planets have yet been Tbased on data from the Gemini on the sky with a precise shuffl ing of found, the exploration of several stars telescopes. Twenty-four papers (compared the images on a charge-coupled device has revealed a relatively high number of with two in 2001) were published in the (CCD) detector. This results in a brown-dwarf stars, which are a sort of main reference journals. The majority signifi cant increase in the signal-to-noise celestial hybrid between a giant planet of them were based on data obtained ratio of the data. Using this technique, and a small star. Brown dwarfs have with the visitor instruments OSCIR and Gemini astronomers have discovered that masses less than 7 percent that of the Hokupa‘a on the Frederick C. Gillett the apparent “redshift desert” of galaxies, Sun and 100 times that of giant planets Gemini Telescope (Gemini North), and which was thought to exist at an epoch of like Jupiter. A brown dwarf’s low mass four papers were from data obtained with about one-third to one-half the age of the doesn’t allow for nuclear fusion, but does the Gemini Multi-Object Spectrograph Universe, is actually well populated with allow for planetary characteristics such as on Gemini North (GMOS-N). The galaxies representing the various stages of atmospheric weather. fi rst paper from Gemini South based on evolution. More details are given in the data obtained with the high-resolution previous article (starting on page 4) in The study of low-mass stars by Laird Close spectrograph Phoenix was published this issue. and his collaborators at the University of in December 2002. The fi rst Near- Arizona has led to some surprising results. Infrared Imager (NIRI) paper appeared in Companionship in Low-Mass Stars This work comes the closest yet to a large March 2003, a study of host galaxies of z program on Gemini, as evidenced by approximately (~) 4.7 quasars. Finding large Jupiter-like planets around the amount of excellent data that were nearby stars has been the goal of several obtained, analyzed and published. Recently, a top highlight has been the programs using the University of Hawaii‘s implementation of the nod-and-shuffl e Hokupa‘a adaptive optics system on the Compared to their more massive cousins, technique on both low-mass stars of about GMOS North and one-tenth or less the South. An international mass of our Sun come team led by Bob in pairs more often Abraham (University and form much tighter of Toronto) and Karl orbiting systems. This Glazebrook (John unexpected fi nding Hopkins University) was disclosed by Laird in close collaboration Close, Melanie Freed, with Gemini staff has Nick Siegler and Beth provided Gemini with Biller of the University a unique and very of Arizona using the powerful technique, adaptive optics system which counters the Hokupa‘a on the fl uorescence of the night Gemini North telescope. sky that contaminates Their observations the far-red end of the also showed that optical spectrum. The many low-mass star result of this work is systems have brown- that Gemini can obtain dwarf companions much deeper spectra in Figure 1: Low-mass stars come more often in pairs and form tighter systems than their more massive cousins. (Figure 1). This this spectral region than The four images obtained with the adaptive optics system Hokupa‘a on Gemini North are part of a survey research indicates that done by Laird Close and his University of Arizona colleagues. The size of the arrows shows the angular has ever been possible distance in arcseconds between the two components, and the scale is comparable to the approximate distance the frequency of brown- before. Called “nod between our Sun and Jupiter or Saturn. (Gemini Observatory) dwarf companions Gemini Newsletter #26 - June 2003 9 NsLtr0603txt-rev2 9 5/16/03, 4:56:38 PM Figure 2: The tightest-orbiting brown-dwarf companion ever directly imaged was discovered around low-mass star LHS 2397a. The faint companion completes its orbit around the parent star every 20 years. The first image on the left is an image at visible wavelength obtained with the Hubble Space Telescope on April 12, 1997. The brown dwarf is seen as the very faint object at 9 o’clock and is very difficult to detect in this unenhanced image. The next three images were obtained using adaptive optics in the near-infrared wavelength (J, H, K band) on Gemini North about 5 years later (February 7, 2002). Figure 3: The binary low-mass star system LHS 2397a of meteorological features that show a (also shown in Figure 2) contains the closest brown- seasonal cycle. dwarf companion ever spotted (imaged) around a star. This system is located about 50 light-years away, and the companion orbits at a distance that is less than the Titan’s apparent angular diameter from distance of Jupiter from our Sun. The brown-dwarf Earth (~0.8 arcsecond) can be resolved companion is the fainter object at about the 7 o’clock from the ground only with advanced position in this image. The system, found by Melanie Freed and her team at the University of Arizona, used techniques such as adaptive optics. The adaptive optics on the Gemini North telescope to obtain opacity of Titan’s stratospheric haze this data. (Gemini Observatory) decreases sharply with wavelengths across the visible into the infrared. There are narrow spectral windows in the near- infrared between methane bands through looser systems, while allowing tighter which it is possible to probe Titan’s to very-low-mass stars can be up to 20 systems to survive. Understanding the surface and lower atmosphere. times that of Sun-like stars. This comes mechanism that forms tight-orbiting low- as a surprise since there is a distinct lack mass stars may also throw light on why Henry Roe at the University of California, of brown-dwarf companion detections such a wide variety of planetary system Berkeley and his collaborators used at small separations from Sun-like confi gurations exists, many of which have adaptive optics on the Gemini North stars. From giant planets searches, it is giant planets with masses and properties and Keck II telescopes to study the estimated that only about 0.5 percent approaching those of brown dwarfs. tropospheric haze and the discrete clouds of stars have brown-dwarf companions of Titan, and to probe its surface (Figure within 3 astronomical units. This paucity The Arizona team also imaged the 4). Their observations have revealed that of brown dwarfs in normal stars has been tightest-known brown-dwarf-star pair the southern hemisphere shows more cloud referred to as the “brown-dwarf desert.” around the low-mass star LHS 2397a. activity than the northern one (Figure Located at about 50 light-years from our 5). Since no tropospheric brightening The very-low-mass binaries are tight Sun, this binary system represents the fi rst is seen in the far northern latitudes of and also tend to have companions that clear example of a brown-dwarf orbiting Titan, it is suggested that the south polar are nearly equal in mass. While there is within 4 astronomical units of its parent haze and clouds are of a seasonal origin. a dearth of wide systems, the absence of star — this is less than the orbital distance During the Titan summer (as is currently a brown-dwarf desert in tight, low-mass between Jupiter and the Sun (Figures 2 the case in it’s northern hemisphere in pairs has profound implications on how and 3). April 2003), the haze bank is depleted we think low-mass binaries might form of high concentration of molecules, such and evolve. Watching the Clouds and Probing the as C2H4, C4N2, CH3CN and C3H8, Icy Highlands of Titan and cloud activity ceases, especially near It is theorized that “gravitational kicks” Titan’s north pole (Figure 5). During eject preferentially low-mass stars through Saturn’s moon Titan, the second-largest Titan’s long winter (~8 Earth years long), interaction with other stars in stellar moon of the Solar System, is surrounded lack of sunlight drives the chemistry of clusters where stars are born. If the stars by a thick atmosphere of molecular the lower polar stratosphere towards an are pairs or multiple systems, this kicking nitrogen with a few percent methane. extremely different equilibrium relative process selectively unbinds wider and This atmosphere appears to host a variety to the sunlit stratosphere. This increases 10 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 10 5/16/03, 4:56:39 PM Figure 4: Hokupa‘a/Gemini images of Titan 1 The adaptive optics images have revealed obtained with Gemini North using a filter probing the surface of Titan on December 7–9, 2001. Image that the short-wavelength infrared A corresponds to the surface of the moon, and B probes emission from IRS-8 is largely in the form Relative Intensity its mid-stratosphere. Images C and D show the lower of a spectacular bow-shock surrounding troposphere. The bright feature at the southern pole a central star (Figure 7). The dust in (C and D) is the so-called bright continent. This may be an icy highland surrounded by seas or lakes of the bow-shock is heated and radiates hydrocarbons. The true nature of Titan’s surface and because it is compressed. It also absorbs the composition of the dark and bright areas remain ultraviolet radiation from IRS-8 itself unknown. and from the ambient Galactic Center energetic radiation fi eld. 0 The interstellar bow-shock is produced by a massive star, embedded in a dense wind envelope, moving at supersonic 1. Relative Intensity speeds e.g., tens or hundreds of kilometers/second, into the surrounding 0.5 gas/dust of the interstellar medium. The phenomenon is not unlike the bows 0 created by ships or other crafts moving 1. Relative Intensity in water (except that the water does not compress). With its apex at about 0.03 light-years (or 1,000 times the Earth-Sun 0. distance) from the central star, the IRS- 8 bow-shock is about 100 times smaller -0.6 than all other known bow-shocks formed Figure 5: Keck II adaptive optics images of the clouds on Titan during December 18–21, 2001. A special filter by speeding stars. probing the troposphere was employed. Cloud activity in the south of the moon increased from December 18 (A, E) to December 21 (C, G) and (D, H). The bottom row of images is the result of a wavelet transform of the images. The reason for this compactness is the the concentration of the above molecules, environment very dynamic and a source high density of the gas and dust through a process that favors condensation and of weird phenomena. There are also which IRS-8 is moving. Independent cloud formation (happening now in the several bright and compact objects infrared and radio observations indicate southern hemisphere of Titan). The whose nature, morphology and origin are that the density of the gas/dust is 100 cloud activity that we now see at Titan’s unclear. Most of these objects are hidden to 1,000 times higher than the average south pole will cease when another Titan from ultraviolet and optical observations interstellar density in the Milky Way. southern spring occurs in 2026. because of the high dust content along IRS-8 may actually be colliding with the line of sight to the Galactic Center. the “Northern Arm” of our Galaxy, a Meanwhile, the Cassini spacecraft due However, infrared detectors and adaptive region of high-density molecular gas that to arrive at Titan next year will be able optics allow us to peak right through to has been mapped by infrared and radio to look for these southern polar clouds. the very nucleus of our Galaxy. observations. If the mission remains active for more that 4-5 years, it will monitor the start IRS-8, a strong emitter at infrared The second reason for the bow-shock’s of spring cloud activity at Titan’s north wavelengths, has long been one of the tightness is the high velocity of the star. pole. mystery objects in the central stellar If the stellar wind properties of IRS-8 are cluster at the Galactic Center. François normal, the bow-shock geometry and size Speeding Massive Star Plows Through Rigaut, Tom Geballe and Jean-René Roy require a space velocity of approximately Interstellar Dust and Gas Near the from the Gemini Observatory, and Bruce 150 kilometers/second, which is not Galactic Center Draine of Princeton University have unusual for objects within a few light- analyzed the exquisite Galactic Center years of a supermassive black hole like Located 25,000 light-years from the images obtained with the University IRS-8. Using the axis of the bow-shock to Sun in the direction of the constellation of Hawaii’s adaptive optics camera give the direction of motion, IRS-8 could of Sagittarius, the nucleus of the Milky Hokupa‘a-QUIRC on the Gemini North have been in the vicinity of the nucleus Way is host to numerous high-energy telescope in order to study the source about 10,000 years ago. It is possible that phenomena including a supermassive IRS-8. The object is located about 4 IRS-8 was fl ung out of the central cluster black hole estimated to weigh in at light-years north of the Galactic Center of stars by gravitational interactions at the some 3 million times the mass of our (Figures 6 and 7). time. Sun, which makes our galaxy’s nucleus Gemini Newsletter #26 - June 2003 11 NsLtr0603txt-rev2 11 5/16/03, 4:56:40 PM arise from either thermal emission from the dust grains or synchrotron emission. The OSCIR observations show that the IRS-8 mid-infrared emission of NGC 4151 is compact but resolved. It extends ~3.5 arcseconds, or 200 parsecs across at a position angle that matches the narrow line region as observed in [OIII]5007 by the Hubble Space Telescope (Figure 8). The most likely explanation for the extended mid-infrared emission is dust in the narrow line region heated by the central engine that is likely powered by a black hole. The authors fi nd no extended emission associated with the proposed torus and are able to place an upper limit on its mid-infrared size of < 35 parsecs. Exploring Wolf-Rayet Stars in the Local Group Starburst Galaxy IC 10 Getting spectra of individual stars in nearby galaxies is something that has been done with 4-meter-class telescopes for some time. However, when the science Figure 6: Gemini/Hokupa‘a adaptive optics image of the Galactic Center region made of a composite of three images goals require high spectral resolution or obtained in the infrared bands J, H and K’. very high signal-to-noise ratios, the use of an 8-meter telescope becomes essential. the Galactic Center conference held in Principal Investigators Paul Crowthers Kona, HI in November 2002, and their of the University College London and paper was published in the proceedings of Laurent Drissen of Université Laval and the conference. Gemini sponsored and led this extremely successful conference. Probing the Heated Dust in the AGN of NGC 4151 with OSCIR James Radomski of the Figure 7: Smaller field J-H-K’ color composite (from Figure 6 image) of IRS-8 and its bow-shock. University of Florida and his collaborators used Gemini North/OSCIR The very center of our Milky Way to observe the nuclear contains a number of objects with region of NGC 4151 at characteristics similar to IRS-8 that are 10.8 and 18.2 microns. also the result of shock-heating or shock- NGC 4151 is one of the compression of dust. IRS-8 is the most nearest (13.2 megaparsecs) conspicuous member of this class of and best studied active fast-moving massive stars in the Galactic galactic nuclei (AGN). Center and emphasizes the violent nature It hosts a highly variable Figure 8: Contours of filter band N and IWW18 emission (after point-spread-function subtraction) overlaid on the Hubble Space Telescope of the Galactic Center environment continuum and line [OIII]5007 ionization region in (a) and (b). Images (c) and (d) show the associated with its massive black hole. emission source. The mid- same N and IWW18 emission overlaid on the radio jet observed at 18 infrared emission of NGC centimeters by Pedlar, et al. (1998) Rigaut, et al., Presented their results at 4151 has been suggested to 12 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 12 5/16/03, 4:56:40 PM Exploring Host Galaxies of z ~ 4.7 Quasars with NIRI Using NIRI, John Hutchings of the Herzberg Institute of Astrophysics/ National Research Council imaged fi ve redshift z ~ 4.7 quasar with NIRI using 2- micron broad- and narrowband imaging with Gemini North. The [OII]3727 nebular emission lines, which trace regions of high star-formation rate, are shifted into the near-infrared red that are close to 2 microns for these quasars. The [OII] emission is spatially resolved in all fi ve quasars. Hutchings shows that the quasars tend to be located in one centrally located unresolved body within a network of knots and fi laments that extend to several arcseconds. Line emission is localized in small regions within the host galaxy where star formation must be very active. He suggests that we may be seeing host galaxies that are in the early stages of assembly, and notes that luminous Figure 9: Shows the trend of WC/WN ratio for Local Group and Sculptor Group spiral and irregular galaxies versus oxygen content, which is a good indicator of the overcontent in heavier elements. The new Gemini data show how the quasars at z ~ 4.7 are found inside the position of IC 10 on this diagram is brought down closer to the general trend. most luminous galaxies (Figure 10) with a probable evolution of the galaxy stellar their collaborators employed GMOS-N to 0.6. The authors re-emphasize that populations along the K-z relationship. to obtain high signal-to-noise spectra of IC 10 hosts a substantial population of 28 Wolf-Rayet candidates in the nearby WR stars (where confi rmed, WC stars galaxy IC 10 in order to ascertain the outnumber WN stars). They predict that ratio of the WC/WN galaxies, which deeper studies will make IC 10 consistent should normally be <<1 in a galaxy with with the expected metallicity trend, a metallicity as low as one-fourth that of thereby, removing the need to call upon a our Sun. The galaxy, located at about 0.7 skewed Initial Mass Function in IC 10. +/- 1 megaparsecs, is remarkable for its very high star-formation rate. While all other Local Group galaxies show a clear trend of decreasing WC/WN with lower metallicity, previous works had inferred an abnormally high ratio of 2.0. The effect of a relatively higher number of WC stars is thought to arise from the deeper depletion of the stellar upper layers when metallicity is high. Winds are more powerful and mass loss reveals deeper layers down to the carbon core of the stars. From the GMOS-N spectra (and a few spectra from the Canada-France- Hawaii Telescope), the authors deduced a ratio of WC/WN ~1.5 (Figure 9). They also provide evidence that the number of WN stars is underestimated, Figure 10: K-z plot for radio galaxies, with the best estimated value for the quasi-stellar object and show that the ratio is probably closer host (open circles on the plot) from the Gemini NIRI observations. The lines sketch in passive evolution models for 1.0 and 0.1 Gyr starbursts at z = 20. Gemini Newsletter #26 - June 2003 13 NsLtr0603txt-rev2 13 5/16/03, 4:56:41 PM GEMINI INSTRUMENTATION PROGRAM UPDATE Doug Simons he past few months have Figure 2 shows the second image marked the beginning of ever recorded with the instrument, Ta period of intense activity a 20-second integration on a within the instrument program, as southern globular cluster called long-awaited instruments arrived Hodge 11. The GMOS-S at both sites, enabling signifi cant commissioning team went on that new avenues for research on the night to demonstrate fast tip/tilt Frederick C. Gillett Gemini guiding, closed-loop focus control Telescope (Gemini North) and and active optics corrections on the Gemini South. A total of six facility- telescope using the GMOS-S on- class instruments are scheduled instrument wavefront sensor. to arrive in a one year period. It is doubtful that such a large These remarkable achievements “wave” of new instrumentation certainly did not occur accidentally. will arrive at Gemini ever again, They are the result of painstaking and coordinating the arrival, work on the part of the builders Figure 1: GMOS-S on the up-looking instrument port is shown with its integration, commissioning and commissioning team in the foreground. of GMOS-S, the commissioning release of each instrument, while team and the hard work in Hawai‘i maintaining regular science operations, Figure 1 shows GMOS-S on the up- commissioning GMOS-N, so that lessons will be a challenge. In the meantime, looking port just before engineering fi rst learned with the fi rst instrument could the Gemini Multi-Object Spectograph light. On its fi rst integration, GMOS-S be used to make GMOS-S as “plug- on Gemini North (GMOS-N) and our recorded images with a full-width at half- ’n-play” as possible. Since engineering Near-Infrared Imager (NIRI) remain in maximum (FWHM) of 0.9 arcsecond fi rst light, GMOS-S has completed operation at Gemini North with only and an alignment error with respect to the most of its baseline commissioning tasks minor planned upgrades in the near Cassegrain rotator of only 1 arcsecond. (imaging and single-slit and multi-slit future, e.g., more gratings for GMOS- spectroscopy). A second integral fi eld N and testing of new higher unit (IFU) is being fabricated for resolution grisms in NIRI for use GMOS-S at the University of in adaptive optics spectroscopy. Durham UK, and the atmospheric We are also beginning to formulate dispersion compensators are plans for the next generation of being completed at the Herzberg instruments developed for Gemini Institute of Astrophysics (HIA) that will no doubt help defi ne the for both instruments, meaning scientifi c frontiers in ground-based additional modes will eventually astronomy through approximately be commissioned in the months 2010. ahead. GMOS South (GMOS-S) Michelle The fi rst facility instrument About a week after GMOS-S to arrive at Gemini South was collected its fi rst photons in Chile, GMOS-S, the clone of its highly Michelle experienced fi rst light successful counterpart in Hawai‘i. in Hawai‘i on Gemini North. GMOS-S had its engineering fi rst This followed a successful science light on 18 January 2003, and like campaign on the United Kingdom GMOS-N impressed everyone Figure 2: This 20-second R-band integration of Hodge 11 was the second Infrared Telescope (UKIRT) image recorded with GMOS-S during commissioning. with its on-sky performance. and was the starting point of a 14 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 14 5/16/03, 4:56:44 PM year-long deployment on Gemini along with methods for dealing North for this shared instrument. with acquisition and residual Prior to its arrival, a new science noncommon path aberrations. grade detector was installed in Work was also conducted to Michelle, and the instrument measure Altair’s throughput (~89 was reconfi gured in its “Gemini percent) during these runs. After mode,” which includes new fore these runs Altair was removed from optics and a frame to mount its the telescope, and modifi cations thermal electronics enclosures. were made to its wavefront sensor, Michelle experienced two runs in which we expect to enable more early 2003 on Gemini North, both stable performance under a broad of which were dedicated primarily range of seeing conditions and to working out engineering further reduce non-common path interface issues, verifying basic errors. Commissioning for Altair instrument focus and alignment Figure 3: Altair on Gemini North’s instrument support structure side port. will continue in semesters 2003A with respect to the telescope, and working on fast tip-tilt guiding while Altair Commissioning Update also chopping—something that is unique to Gemini among 8-to-10-meter-class As this issue of the newsletter neared completion, the third Altair commissioning run took place from April 15 to 22. After three months of rework at HIA and Gemini, this run has been very successful. telescopes. Michelle is currently back at One by one, the major functionalities of the system, including the interaction features with the telescope UKIRT, and the Gemini fore-optics were control system and the data acquisition sequencer, were successfully debugged, tested and character- sent back to Edinburgh, Scottland where ized. Altair is now able to (i) receive signals from the instrument On-Instrument WaveFront Sensor engineers at the Astronomy Technology (OIWFS) and use them to compensate for slow drift of image centering and defocus due to fl exures; (ii) offl oad at a slow rate the quasi-static shape of the deformable mirror to the telescope primary mirror; Centre are adjusting its internal optics to (iii) offl oad the centering tip-tilt and defocus errors to M2; and (iv) optimize several of the system oper- align them with respect to the telescope’s ating parameters in real time such as modal gains and WaveFront Sensor (WFS) centroid gain. pupil. We expect these modifi cations to be completed in time for more Michelle Altair is well integrated both with the Telescope Control System (TCS) and the Telescope Control Console (TCC). The telescope operator may now start and stop adaptive optics corrections from its TCC commissioning observations in June, control screens. in support of releasing Michelle for use by the Gemini community in Semester After dealing with system functionalities, the main thrust of the team’s effort during the last nights of 2003B. testing shifted toward performance evaluation and improvements. Things are taking shape on this front. Images of full width at half maximum (FWHM) were obtained from 59 to 85 milliarcseconds (mas) on the vast majority of objects observed. This is slightly short of the ultimate diffraction limit (42 milliarc- Altair seconds in H and 57 milliarcseconds in K), but the main culprits have been identifi ed. We have specifi c plans for improving these areas to reach our diffraction limited goals. Gemini’s fi rst facility adaptive optics The team was generally very pleased with the behavior of the system. The rework at HIA and Gemini (AO) system, built by Herzberg Institute in the past three months – including the refi tting of a new lenslet array, work on the NIRI OIWFS gim- of Astrophysics, arrived in October 2002, bal mechanisms and several software improvement and fi xes – has brought considerable improvements and was used twice on the Gemini North in the stability and overall performance of Altair. Following these successes, we are more confi dent than telescope later that year during extensive ever that the Gemini facility AO system will be fully competitive with its most serious competitors (e.g. commissioning runs. The fi rst attempt to NAOS). close the AO loop with Altair resulted in During the next two commissioning runs in May and July, we expect to concentrate on the remaining an image recorded by NIRI with a strehl problems and gray areas, including: of approximately (~) 25% at H, with the highest strehl achieved during the 1. A relatively strong vibration occurs somewhere in the system, varying from 5 to 35 milliarcseconds per axis. Investigations show that this comes from within Altair and most probably from the common fi rst commissioning runs of ~55% at K. path. The main suspect is the tip-tilt mirror, which could vibrate due to an electrical coupling with As expected, integrating Altair’s control an external source. This prevents Altair from reaching the ultimate diffraction limit. We have been rou- system into the Gemini North control tinely achieving 60-65 milliarcseconds at H and K wavelengths. system was a major task due to the 2. Although calibration of the static aberrations dependency vs. fl exure was carried out successfully with complexity of operating the AO system, the Altair internal calibration source, we measured large static aberrations on the sky. We are working telescope and instrument in a coordinated on identifying the source of these aberrations. One possible cause is from spatial aliasing of high-order manner. These complexities include aberrations on the order of a few tens of nanometers rms from the telescope. correctly opening and closing various 3. Regarding the isoplanatic angle, the offl oading of the Altair deformable mirror static shape to M1 guide loops while dither patterns on the has done a lot to improve the performance off-axis. We are fully aware of the importance of this issue. sky are executed. Additionally, various To address this, we regularly observed stellar fi elds during the run. The data are being analyzed and a offsets must be delivered to M1 and M2 database has been established which will help us characterize the anisoplanatism. Gemini Newsletter #26 - June 2003 15 NsLtr0603txt-rev2 15 5/16/03, 4:56:45 PM to prevent resource collisions with other the acceptance test team, T-ReCS was instruments being built there (see GSAOI shipped to Chile where the University reference on page 17), the replacement of Florida team will lead its reassembly NIFS is actually being contracted out to and work closely with the Gemini South Auspace Limited, a commercial aerospace engineering team to fully integrate T- company in Canberra, Australia, which ReCS into the various optical, mechanical already has a close working relationship and control system environments in with the team at Mt. Stromlo. Under which it must operate. We look forward the current plan, we expect NIFS to be to T-ReCS experiencing fi rst light commissioned on Gemini North in 2005, in June. At that point, an aggressive soon after the laser mode of Altair has been commissioning campaign will be used to commissioned. This will be key to the use make it available during Semester 2003B of NIFS since we expect the laser-guide- for shared-risk use. star mode of Altair to enable observations of many more targets compared to relying bHROS on natural adaptive optics guide stars. The other acceptance team (referenced in Figure 4: The badly damaged remains of NIFS are shown in this photo. The vacuum jacket was burned through and interior components gutted during the fire. and 2003B, with the latter semester including the fi rst science use of Altair via system-verifi cation observations. The data from these observations will be released to the community soon after they are acquired. NIFS As has been widely reported, Mt. Stromlo suffered devastating bush fi res in January 2003, which destroyed the Near-Infrared Integral Field Spectrograph (NIFS) being built there. This tragic fi re actually happened at the exact same time that we were celebrating the outstanding engineering fi rst-light results of GMOS- S making for a bitter-sweet moment in the brief history of Gemini’s instrument Figure 5: The University of Florida’s T-ReCS team is shown surrounding the instrument just prior to its program. Figure 4 shows the burned hulk shipment to Chile. that remains of the instrument that was the previous section) went to London to partially vaporized from the intense heat T-ReCS perform fi nal pre-ship acceptance tests on of the fi re. Prior to the fi re, NIFS was on Gemini’s new fi ber-fed, bench-mounted track for a mid-2003 delivery to Hawai‘i Soon after January’s engineering fi rst-light High-Resolution Spectrograph (bHROS) where it was planned to be used with activities commenced for new northern in mid-February. Built by the University Altair to provide a key new AO-based and southern instruments, Gemini College London, this is Gemini’s only integral fi eld spectroscopy capability at sent teams to two more instrument non-Cassegrain-mounted instrument. Gemini North. development sites to conduct fi nal pre- ship acceptance testing in mid-February. With a spectral resolution of 150,000, it represents a fairly unique facility on large Luckily, all of the NIFS design drawings One team was sent to Gainesville, FL, telescopes. bHROS reached the summit and several critical components, including where Gemini’s facility Thermal-Region of Cerro Pachón during the fi rst week the HAWAII-2 science detector, were Camera Spectograph (T-ReCS) was in April where it will be assembled and spared. Since the time of the fi re, thanks rigorously tested over a ~10-day period to aligned in the pier lab, an area that has to the fortitude of the NIFS team, a plan verify that key performance and interface been substantially refurbished over the was forwarded to Gemini and was recently requirements were met. After a few weeks past year to accommodate the singular approved to build NIFS again. In order of rework to deal with items identifi ed by 16 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 16 5/16/03, 4:56:46 PM that such a large recently awarded to the Research School cryogenic instrument of Astronomy and Astrophysics at the experiences during Australian National University with Peter its development McGregor as the Principal Investigator. phase. GNIRS is This instrument is scheduled for delivery now fully assembled in 2005 and is intended for use as both the including all of its commissioning camera and primary 1-to- optics (except for the 2.5-micron science imager for Gemini’s IFU being fabricated southern adaptive optics system. It is by the University unique in both its simplicity (single-plate of Durham, scale) and complexity in that it will be the UK), science and fi rst Gemini instrument to use a mosaic wavefront sensor of 2,0482 infrared detectors in its focal detector systems, plane. These HAWAII-2RG detectors are Figure 6: GNIRS is shown fully integrated in a horizontal position on the new NOAO mechanisms, being made for Gemini under a separate flexure rig facility in Tucson, AZ. electronics and contract with Rockwell Scientifi c. control system. needs of a high-resolution spectrograph. GNIRS commissioning is planned to A laser guidestar (LGS) upgrade to the Though the instrument is scheduled begin in 2003B. Whether it is used Altair adaptive optics system is planned to be integrated in the pier lab during as a single-slit spectrometer, across- for the fourth quarter of 2004. The the second quarter of 2003, its fi ber- dispersed spectrometer or an integral solid state, sum frequency laser system fore optics will not be fully integrated fi eld spectrometer, we expect GNIRS to is now under development at Coherent into GMOS, which will be used as its be popular within our community and Technologies, Inc., in Lafayette, CO acquisition system, until sometime in to become an important research tool for following a kickoff meeting held in Hilo 2004. This is due to the aforementioned viewing programs that encompass nearby in January of this year. The laser launch fl ood of instruments that are now being star-formation regions to distant galaxies. telescope contract at Electro-Optical delivered to Gemini South, the need Systems Technology (EOST) in Tucson, to maintain at least 70 percent science Ongoing Instrument Program AZ, also passed its critical design review time for our community starting in during January, and the critical design Semester 2004A, the sequence in which Gemini’s instrument program has a review for the internal work on the beam instruments are arriving and the scientifi c vigorous development component that transfer optics system was held in March. priorities assigned to facility instruments will be used to maintain a steady stream Work on the Safe Aircraft Localization (and their various modes) by the Gemini of state-of-the-art instrumentation at and Satellite Acquisition System (SALSA) Science Committee. While we remain both telescopes beyond those previously safety systems is also progressing. excited about integrating bHROS at mentioned. The newest instrument to be Gemini South in 2003, commissioning started up is the Gemini South Adaptive Design and development work for the will not commence until next year. Optics Imager (GSAOI), which was Gemini South adaptive optics system and its multi-conjugate adaptive GNIRS optics (MCAO) capability is now well underway (see Figure The fourth in the sequence of 7). Work on a contract for the instruments arriving in Chile optical bench, natural guide this year will be the Gemini -star wavefront sensors, and Near-Infrared Spectrograph electronics enclosures began at (GNIRS) built by the National EOST last November. The Optical Astronomy Observatory realtime controller subsystem (NOAO). Figure 6 shows is under development at the GNIRS being rigorously tested Optical Sciences Company on the fl exure rig facilities at (tOSC) in Anaheim, CA where NOAO. GNIRS has gone a preliminary design review through several cold tests in was successfully completed in Tucson, AZ since mid-2002. February of this year. Two We are making progress each prototype deformable mirrors time with resolving the usual Figure 7: The optical path of the Gemini MCAO system currently under development with 37 actuators and the 5 types of problems and challenges by Gemini staff. millimeter interactuator spacing Gemini Newsletter #26 - June 2003 17 NsLtr0603txt-rev2 17 5/16/03, 4:56:46 PM required for the GSAO design are in which is being built by the University of to procure instrumentation out through fabrication at Xinetics in Cambridge, Florida and is scheduled to arrive in Chile 2010. Forecasting scientifi c frontiers MA with test results expected by June. in the second semester of 2005. Likewise, is always a challenge. Nonetheless, Two conceptual design studies for the Hokupa‘a-85, which is a visitor adaptive having community input into the basic MCAO laser- guide-star wavefront sensor optics system under development at the capabilities of Gemini’s next generation at HIA and tOSC were completed in University of Hawaii, is scheduled for of instruments is crucial as we fi nd the April, and the request for proposals for completion in mid-2003. It will be used common threads among the myriad the laser system is planned for later this at Gemini South until NICI arrives of possible science missions identifi ed year. The overall program schedule calls that will provide the same narrow-fi eld through these workshops. From there, we for the delivery of the major subsystems to adaptive optics imaging as Hokupa‘a-85. hope to craft widely capable instruments Gemini in mid-2005 followed by system that will carry us into the next decade. integration leading to fi rst light and Finally, the next generation of Gemini commissioning in the fi rst half of 2006. instruments will be broadly defi ned in Once again, it is truly a remarkable and the near future through a network of exciting time in Gemini’s instrument Other facility-class instruments national, and ultimately international, program, with an unprecedented “wave” under development include NICI, science workshops attended by Gemini’s of new facility-class instruments arriving which is Gemini’s fi rst Near-Infrared broad family of users. These workshops now at both telescopes, and we are Coronagraphic Imager, and is scheduled are intended to distill the scientifi c taking the fi rst steps in defi ning our next- for deployment in Chile in early 2005. ambitions of our community into basic generation instruments. Also under development is Flamingos-2, design guidelines that should be used PIO REPORT Peter Michaud he past few months have signed with Akira Design to produce a 60 been a very productive to 90-second animation showing the Tperiod of growth for operation of the planned Gemini the Gemini Public Information Laser Guidestar System (LGS). and Outreach (PIO). This is the same company that produced the much- acclaimed The new Gemini Virtual Tour- Gemini Telescopes and adaptive Image/Animation Gallery optics animations (on the new CD- CD-ROM is now updated ROM), and we anticipate a great and available for distribution. product. Preliminary draft cuts We have just duplicated 10,000 look extremely promising, and we copies of this CD-ROM for use in anticipate this animation to be ready Gemini outreach programming, and for distribution by late 2003. Watch the disc is available upon request for for details about the LGS animation educational use (to obtain additional on the Gemini website and in the next copies, contact [email protected]). narrations issue of this newsletter. Most copies of this issue of the Gemini with a music Newsletter were shipped with the new background, several Many readers have probably already Virtual Tour as well. Please take a look new “science modules” that highlight noticed that the Gemini website has at the copy provided (it runs on either specifi c Gemini science fi ndings, become more dynamic over the past Macintosh or Windows platforms). The increased content from Gemini South 6 months. We are now changing the tour is still late in the development stage, and more staff profi les. The CD-ROM homepage headline every 2 weeks to and we appreciate any comments or also contains a wide selection of the latest keep content fresh and timely. This is a suggestions for improvement or content images and animations, including the very coordinated effort between the Gemini enhancement. popular adaptive optics animation, which Science Team and the PIO staff, and we is located at the end of both the Gemini think it has been extremely successful. We are also developing several additional North and South telescope animations. However, one can never rest on laurels. enhancements including partner-country The website’s horizons are still expanding. language translations, professional Regarding animations, a contract has been As this newsletter goes to press, the 18 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 18 5/16/03, 4:56:47 PM Gemini web redesign team headed up by makes the StarLab equipment, Learning the PIO staff, along with the Science and Technologies in Cambridge, MA, offered Networking staff, have developed a beta to donate a second complete StarLab to version of the new Gemini homepage, the Gemini Outreach offi ce in La Serena a sample of which is shown in Figure for expanded programming to local 1. We expect this new look to go schools. This exciting development will public early in the second half of 2003, allow Gemini to provide a new level of so keep your browser pointed at http: programming to local schools and will //www.gemini.edu. complement the existing partnership with CTIO and RedLaser. One of the most visible and exciting PIO projects of the past 6 months has been the “Adventures Along the Spectrum,” a hugely successful StarTeachers Exchange dynamic and interactive science program program. StarTeachers is a teacher for students, is another new initiative that exchange program that allows three is proving to be extremely successful. It teachers from each Gemini community was a development of local outreach (Hilo and La Serena) to travel to the programming in schools to augment other’s community for a period of 2 weeks. another new educational program about During the exchange, the teachers teach in Figure 1: A design concept for the new Gemini homepage. observatory careers. Both of these the host classroom while using Gemini’s programs have been made possible by networking technologies to concomitantly more program information and images interns provided by the NASA-funded teach their classes “back home.” see http://www.gemini.edu/project/ program “New Opportunities Through announcements/press/2003-1.html. Minority Initiatives in Space Science” In late March and early April, the three (NOMISS) at the University of Hawaii at StarTeachers from Hawai‘i traveled to The StarLab portable planetarium Hilo. See http://hubble.uhh.hawaii.edu/ Chile. As Hawai‘i teacher Alicia Hui said, continues to fuel the growth of other NOMISS/background.htm for more “Out of 100 points, this experience was ongoing outreach programs. StarLab is information. a 200!” During the exchange, teachers proving to be a valuable educational tool used Gemini’s internet technologies and a real hit with educators in both A key milestone has also been reached in to send back images, live and recorded Hawai‘i and Chile. A new initiative in the Gemini PIO effort with the hiring of video, and even used a digital white board Hawai‘i began with the training of about full-time Press Offi cer/Writer Jennifer so their students at both Gemini base 25 local teachers who can now borrow Anderson Akingkubedaggs. Jennifer’s facilities could interact in this exciting the StarLab equipment for lessons and offi ce is located at the Gemini offi ces in global classroom created by Gemini. multiple-day programming in their Hilo, and she will serve as the primary In the end, everyone learned a great schools. This has been the primary mode contact for local and international media deal about cultural, technological and of operation in Chile with the joint StarLab as well as become the main conduit for the scientifi c exchanges. Preparations are program between Gemini, CTIO and Gemini PIO Liaison Network. Hiring the now underway for the Chilean teachers RedLaser. Recently, to visit Hawai‘i in October 2003. For the company that Figure 3: The three Hawai‘i StarTeachers are joined by their counterparts and Gemini outreach staff in Chile during a visit to Cerro Pachón and Cerro Tololo in late March. From left to right: Antonieta Garcia (Gemini Staff), Viviana Calderón Tolmo (Chilean Figure 2: Students from StarTeacher Kristen Luning’s class at Keaau High School interact StarTeacher), Kristen Luning (Hawai‘i StarTeacher), Jenny Opazo González (Chilean live with students in Chile using a digital whiteboard during a videoconference lesson from StarTeacher), Alicia Hui (Hawai‘i StarTeacher), Janice Harvey (Gemini Staff), Carmen the Gemini base facilities in Hawai‘i and Chile. Luz Briones Castillo (Chilean StarTeacher), Chrisine Copes (Hawai‘i StarTeacher). Gemini Newsletter #26 - June 2003 19 NsLtr0603txt-rev2 19 5/16/03, 4:56:48 PM Press Offi cer completes the staffi ng portion of the 5-year PIO expansion effort. Now PIO will concentrate its efforts for the next 2.5 years on expanding, developing and evaluating PIO programming. Visitors to the Gemini base facility in Hilo will notice a new exhibit in the main lobby (see Figure 4). It incorporates twin LCD display screens that dissolve dozens of images from Gemini with short captions in any language. The images are updated nightly from a webserver so each day the images can refl ect the latest information and fi ndings from the Gemini telescopes. Figure 4: Gemini’s new Press Officer, Jennifer Anderson Akingkubedaggs, with the new digital We anticipate that the National Science display in the lobby of the Gemini Southern Operations Center. Foundation will be installing this system at their headquarters in Arlington, VA in Gemini Collaborates with the Virtual Museum of Canada the next few months. A similar system will be installed in the lobby of the Gemini In our ongoing effort to leverage the education and outreach resources developed by Gemini, we have been Southern Operations Center during the working with the Canadian Heritage Information Network (CHIN) to provide content, visuals, anima- second half of this year. Any partner who tions and interactive elements from the Gemini Virtual Tour for a new virtual exhibit on astronomy at would like to install a similar system at the Virtual Museum of Canada (VMC). their facilities may do so by contacting By participating in this project we join other participants in Canada, Australia and Hawai‘i to share the PIO Offi ce to obtain a copy of the a wide variety of high-quality online materials that range from the latest scientifi c discoveries and tech- software and specs on recommended niques to the rich cultural and historical connections between people around the globe and the sky. Since hardware. its inauguration in 2001, the VMC has served more than 5 million visitors with over 20 million pages viewed. It is expected that this new virtual exhibit will continue to broaden both the VMC and Gemini audiences while expanding the public’s access and understanding of astronomy and the part that observa- Finally, the Gemini PIO Offi ce will tories like Gemini play in our exploration of the cosmos. be hosting two meetings this summer. Following the International Astronomical Another benefi t that this collaboration has already delivered to Gemini was a one-month Young Canada Works International internship that brought a young Canadian Graphic Artist, Sonja Wermann, from Union (IAU) meeting in Australia (where the Manitoba Museum to the Gemini Offi ces in Hilo. While Sonja was here in February of 2003, she we will also present a teacher workshop did extensive photography of Gemini and other observatories on Mauna Kea, including the production of on Gemini educational programs at the several new QuickTimeVR® movies that will be incorporated into the Gemini Virtual Tour materials. Powerhouse Museum on July 26th), For more information on the Virtual Museum of Canada, please visit: www.virtualmuseum.ca the second annual Gemini PIO Liaison Meeting will be held in Hilo on July Other VMC Astronomy Virtual Exhibit Participants Include: 30–August 1. We are anticipating at least one representative from each Gemini Australian Museums & Galleries Online, Australia Centre of the Universe, Canada partner, and expect to resolve many issues Glenbow Museum, Canada related to the interactions between our Manitoba Museum, Canada Press Offi ce in Hilo and the Gemini Mauna Kea Astronomy Education Center, Hawai‘i partnership. Immediately after that, on National Research Council of Canada August 4–6th, we will host the 3rd annual Planétarium de Montréal, Canada State-of-the-Art Telescope Education Consortium (STARTEC) meeting. STARTEC consists of representatives from most major state-of-the-art telescopes, and each of these meetings will include tours of Gemini and several of the telescopes on Mauna Kea. Learn more about STARTEC at http://www.startec- intl.org/ 20 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 20 5/16/03, 4:56:49 PM PROFILE: PETER MCEVOY Jennifer Anderson Akingkubedaggs hile hitchhiking from Madrid resources strategy for a multinational and Argentina meet. Pete says that he was to Alicante, Pete McEvoy telecommunications company. Pete’s pleased that, although drenched and Wlistened to his sister chat career prior to joining Gemini required confused by it all, Tom seemed to really fl uently in Spanish with the driver of him to travel extensively. Among his enjoy the experience. the beer truck in which they were riding. favorite destinations are Chile - his chosen Pete and his sister had negotiated a deal home - South Africa, northeast Brazil and After a transfer for traveling together on holiday in Spain Colombia. Not one to fear a challenge, with a previous - she would show him Spain, where she Pete has gone parachuting, bungee employer sent was at university, and he would show her jumping, microlyte fl ying and whitewater Pete to Santiago, how to hitchhike. During that fateful trip, rafting. He described one whitewater- Chile, from his unable to converse, Pete decided to learn rafting trip near Victoria Falls, Africa, base in the UK, Spanish. during which he nearly drowned. “One he joked with portion of the river,” he explains, “looked friends that at Upon his return to London, Pete like a toilet bowl fl ushing.” He fell from Peter McEvoy stands in front least a doubling of the new Gemini South Base began purchasing copies of “El País,” the raft and despite a life preserver and Facility. of his salary the Spanish newspaper, from a local helmet, he found himself trapped at the would be required newsstand. Each week, he sat down at bottom of the Zambezi River, and slipped to convince him to leave. “With so many a local Spanish café, armed with just a into unconsciousness. His body surfaced clear morning skies over Santiago, it is Spanish-English dictionary and a simple 100 yards downstream. After regaining possible to really enjoy the spectacle of book of Spanish grammar and learned the consciousness, he became violently ill. the sun ‘rising’ over the steep mountains. basics of the language by translating “El Then, astonishingly, he grabbed an oar You realize that you have another day to País” articles about sports, art and news. and immediately started rowing again. play with,” he says. Now that he lives in It was a word-by-word advance. As an “Every day is an absolute privilege,” he La Serena with his family, Pete is unsure interesting level 2 course, Pete translated says while refl ecting on the impact of the if even a doubling of his salary would the lyrics of songs by Julio Iglesias and experience. convince him to return to Santiago, Los Panchos. These budding Spanish despite La Serena’s frequent foggy language skills and his formal university Pete and his wife, Heleny Zafi ropulos mornings. The people, the surroundings studies formed the bridge between Pete’s Themistocleus, who is Chilean of Greek and the wonderful environment for his past and his future. parentage, have created a family life that family have a tremendous value for him. has taught Pete about love and helped Born near Leeds in Northern England, to mend wounds caused by his mother’s Pete confesses to a certain sense of Pete grew up with a brother and two passing early in his life. Pete and Heleny’s awe at the amount of talent around younger sisters. At the tender age of 13, son, Thomas Dimitri (“Tom”), is 4, and him at Gemini South, adding that Pete’s life was changed forever when his their daughter, Pauline Zoiche (“Lula”), just experiencing the commitment mother died. While his father worked is 2. Both have recently learned to swim, to always improve the operation is a to support their family, he accepted and the family enjoys spending time great motivating factor and one of the responsibility early and became almost together at the beach in La Serena and at reasons he loves being there. He looks a second “Dad” as well as a brother. He the AURA’s recinto pool. Pete refers to forward to the opportunity to introduce played soccer and rugby in his youth, his favorite book, “The Art of Loving,” practical improvements in the quality of captained his university’s rugby team by Eric Fromm as inspirational and a administrative services at Gemini South. and remains a devoted sports enthusiast. contribution to his family life. Getting home to his family in the evening After graduating with honors from Brunel rather than spending it at his computer is University, Pete continued his studies When asked about ongoing participation also a very high priority. He summarizes there culminating in a Master’s degree in in adventure sports, Pete’s wife has his vision in simple terms, “Gemini Industrial Relations and Labor Law. fi rmly ruled, “anything dangerous is now South Administration must come to be banned.” Pete has not given up hope, recognized as a center of professionalism Living in London gave way to exciting however, and even persuaded Heleny to with a clear focus on making a valuable career opportunities, overseas travel and allow him to take Tom, as a 2-year-old, contribution to the achievement of goals adventure sports. He spent the fi rst half of for a trip under the massive Foz de Iguazu in all work groups. We must function like his career working as a manager in human falls, where the borders of Brazil, Paraguay clockwork.” Gemini Newsletter #26 - June 2003 21 NsLtr0603txt-rev2 21 5/16/03, 4:56:51 PM PARTNER OFFICE REPORTS UNITED STATES Taft Armandroff emini support in the United ReCS passed the first portion of its In December, the GNIRS team carried States (U.S.) has been the preshipment acceptance testing. Gemini out its second cycle of GNIRS cold Gresponsibility of the U.S. Gemini and NGSC personnel traveled to testing. The cold cycle was performed Program (USGP). The National Optical Gainesville, FL and ran tests to determine with an engineering-grade array installed Astronomy Observatory (NOAO) is whether T-ReCS could meet its optical in GNIRS. During the cold test, the the home of the U.S. National Gemini performance requirements. The image instrument reached the desired operating Office. NOAO has reorganized USGP quality achieved in T-ReCS was found temperature. All motors and mechanisms into the NOAO Gemini Science Center to be outstanding and passed all such performed within specification including (NGSC). Our change in name from the performance requirements. Gemini, the on-instrument wavefront sensor construction-era designation of USGP to NGSC and Florida personnel carried out provided by the University of Hawaii the NGSC is intended to clearly express the remaining electronic, mechanical and Institute for Astronomy. Spectra our science emphasis and our association software acceptance tests in February. were obtained with the detector and with NOAO. After a few additional adjustments and the instrument was controlled by the fixes, T-ReCS was judged to have achieved complete GNIRS software suite. Based NGSC saw an enthusiastic response from all of the preshipment performance on the results of this testing, a series of the U.S. community to the Gemini Call adjustments were made to the instrument, for Proposals for 2003B. On Gemini and the science-grade detector was North for 2003B, 60 proposals were installed. The instrument was also tested received: 28 for the Gemini Multi-Object for weight and center of gravity and Spectrograph - North (GMOS-N), 21 for achieved these requirements. the Near-Infrared Imager (NIRI) and 13 for Michelle. Fifty-two U.S. proposals In March, another cycle of GNIRS cold were received for Gemini South: 18 testing was carried out. With the science- for T-ReCS, 17 for GMOS South, 15 grade infrared array installed, detailed for Phoenix and 2 for the Acquisition T-ReCS being lowered into shipping crate in Florida for tests of the spectroscopic performance Camera. In total, 107 U.S. Gemini shipment to Gemini South. in various modes were performed. The proposals sought 215 nights on the two requirements by late March. Then, results of these tests are encouraging. In Gemini telescopes. T-ReCS was packed for shipment to addition, flexure testing was performed Gemini South. As of this writing in early using the NOAO Flexure Test Facility, NGSC organized a booth for the April, T-ReCS has been shipped to Cerro and these results are also encouraging. January American Astronomical Society Pachón and will soon begin integration meeting held in Seattle, WA. The with the Gemini control systems and then As of early April, GNIRS is being warmed NGSC booth featured displays on undergo final acceptance testing. up for some additional adjustments. how to propose for Gemini observing Once these are complete, the GNIRS opportunities, brochures on available GNIRS team will begin another cold cycle that Gemini instruments and tutorials on is designed to test compliance with all preparing Phase II programs. Numerous The Gemini Near-Infrared Spectrograph instrument-performance requirements. community members visited the NGSC (GNIRS) is an infrared spectrograph for booth. the Gemini South telescope that will operate from 1 to 5 microns and will T-ReCS offer several features: two plate scales; a range of dispersions; and long-slit, cross- T-ReCS, the Thermal-Region Camera dispersed and integral-field modes. The Spectrograph, is a mid-infrared imager project is being carried out at NOAO and spectrograph, for the Gemini South in Tucson under the leadership of Neil telescope that was developed at the Gaughan (Project Manager), Jay Elias University of Florida by Charlie Telesco (Project Scientist) and Dick Joyce (Co- GNIRS is shown fully integrated on the new NOAO and his team. In late November, T- Project Scientist). flexure rig facility in Tucson. 22 Gemini Newsletter #26 - June 2003 Gemini Newsletter #26 - June 2003 23 Then, once Gemini agrees that all of the Instrument Update article in this issue.) U.S. Gemini Fellowships provide GNIRS preshipment performance tests South American students and educators have been successfully completed, GNIRS Other Activities from Argentina, Brazil and Chile will be shipped to Gemini South. The with opportunities to study, conduct project schedule indicates that 99 percent U.S. involvement continues in the independent research, work and teach in of the work toward GNIRS preshipment Gemini next-generation instrumentation the U.S. at universities and similar research acceptance has been completed. planning process. NGSC will hold institutions of their choice. The recipient a community workshop on “Future of the U.S. Gemini Fellowship for the NICI Instrumentation for the Gemini 8-Meter 2003-2004 cycle is Katia Cunha, PHD, Telescopes: U.S. Perspective in 2003” in currently at the Observatorio Nacional The Near-Infrared Coronagraphic Imager the Phoenix, AZ vicinity on May 30-31 in Rio de Janeiro, Brazil. Dr. Cunha (NICI) will provide a 1–5 micron dual- in order to discuss future Gemini science will take her U.S. Gemini Fellowship to beam coronagraphic imaging capability and instrumentation opportunities. A the University of Texas at El Paso. Her on the Gemini South telescope. Mauna subset of the participants in this meeting research plan addresses the chemical Kea Infrared (MKIR) in Hilo is building will represent the U.S. at the international evolution of Local Group galaxies via NICI under the leadership of Doug Gemini instrumentation-planning high-resolution infrared spectroscopy. Toomey. The NICI cryostat components meeting in Aspen, CO in late June. Cunha plans to use the Gemini South are undergoing fabrication as are the telescope and NOAO’s high-resolution NICI optical elements. In addition, NGSC hosted a meeting of the Gemini infrared spectrograph Phoenix in her development of the array controller Operations Working Group in Tucson, research. The U.S. Gemini Fellowship for the two NICI ALADDIN arrays is AZ on February 10, 2003. The working is carried out as a partnership between progressing well. Overall, 50 percent group had a productive meeting, with the AURA and NGSC, with funding from of the work to NICI fi nal acceptance by added feature of a tour of GNIRS and the the National Science Foundation, and Gemini, which is planned for December NOAO Flexure Test Facility. provides research support for up to 2 2004, has been completed. (See also the years. UNITED KINGDOM Isobel Hook ery signifi cant progress has been verifi cation has now begun, and the spectrograph (bHROS), was shipped made over the last 6 months on instrument will be offered for community from University College London to Vall the major U.K. instruments. use in Semester 2003B. The integral fi eld Gemini South in late March. Over the Since the last newsletter, two of these unit for GMOS-S is under construction next couple of months, bHROS will (GMOS South and Michelle) have had at the University of Durham and is due be assembled in the pier lab at Gemini engineering fi rst light on the Gemini to be shipped to Gemini South later this South where it will ultimately be fed light telescopes. A third instrument (bHROS) summer. through a fi ber feed from the GMOS-S has been delivered to Gemini South. Two mask plane. The fi bers themselves are others (GMOS North and CIRPASS) are Meanwhile on Gemini North, Michelle currently being worked on at La Palma in regular science use in Semester 2003A. (built at UKATC) also had fi rst light on Observatory and will be shipped to the Gemini in January. Initial tests uncovered U.K. where the bHROS relay optics will GMOS-S (built jointly by the UK a telescope problem with guiding while be attached and tested before shipment Astronomy Technology Centre chopping, but this and other telescope to Chile. The mechanical support for [UKATC] in Edinburgh, U.K., and the interface issues that will also affect T- the fi ber mechanism has been designed Herzberg Institute of Astrophysics in ReCS are now being addressed as high- and is being manufactured in the U.K. Victoria, Canada) was the fi rst facility priority engineering tasks. The sensitivity for shipment to Chile in mid-May. instrument to be installed on Gemini of Michelle is as expected, image quality Integration of bHROS in Chile is due to South and had engineering fi rst light in is good (0.4 arcseconds, full-width at be completed in mid-June, but telescope January. Since then, commissioning has half-maximum at 11.6 microns) and the time for on-sky commissioning has yet to progressed at great speed. The one faulty instrument is on track for community use be scheduled. charge-coupled device was replaced in as an imager late in Semester 2003A. April, giving a fully operational array of As the number of facility instruments and three EEV detectors. GMOS-S system The fi ber-fed high-resolution bench the available science time on the telescopes Gemini Newsletter #26 - June 2003 23 NsLtr0603txt-rev2 23 5/16/03, 4:56:53 PM increase, the U.K. Gemini support group on the Space Infrared Telescope Facility for 2003B remained high: 38 proposals is also expanding. Dimitra Rigopoulou deep fi eld surveys that include the Hubble for Gemini North and 22 for Gemini joined the group in February and is Deep Field South and the Chandra Deep South. This compares to 42 and 16 responsible for U.K. user support of T- Field South. respectively in 2003A. However, the ReCS as well as taking over from Alistair number of hours requested per proposal Glasse for user support of Michelle. Prior Semester 2003A was the fi rst semester has increased particularly for Gemini to joining Gemini, Dimitra was a Junior that the national offi ces were responsible South. The oversubscription rates appear Science Staff member at the Max Planck for receiving and checking Phase II fi les to have remained approximately constant Institute for Extraterrestrial Physics (MPE) from successful applicants and forwarding despite a more than 50-percent increase in in Munich. Before that, she worked as a the fi les to Gemini for inclusion in the available time on Gemini South. postdoctoral research assistant at MPE and queue. This process went reasonably well, as a European Union Fellow at Imperial although it is clear that the community is Finally, preparations continue for the College in London. Her research interests still coming to grips with the Observing Aspen 2003 workshop in Colorado. In include studies of ultraluminous infrared Tool software! January, a meeting was held to begin galaxies, in particular, investigating their discussing the U.K.’s requirements, nature (the starburst-active galactic nuclei In April, we held a tutorial on the use of and there have been further discussions connection) and evolution (ellipticals the Gemini Observing Tool for Phase II organized along the scientifi c themes of the in formation). She is also studying preparation. This took place during the Aspen meeting. Ten U.K. representatives the nature of the sources responsible National Astronomy Meeting in Dublin. will attend the Aspen workshop in June. for the cosmic infrared-submillimeter background, and she is a co-investigator The number of U.K. proposals received CANADA Dennis Crabtree anadian astronomers are busy for Semester 2003B on Gemini. The largest number of proposals is for Gemini preparing for the Gemini distribution of the proposals is shown in Multi-Object Spectrograph, with 70 CInstrumentation Workshop that the following two tables. The fi rst table percent of these requests for Gemini will be held in Aspen, CO at the end of shows the number of proposals, and the North. June. Canada has established a parallel second shows the distribution of time process to the Gemini international one. requested. The contract for the development of Science teams in each of four “themes” the Gemini Science Archive is now are investigating signed, and work is the most interesting proceeding. National Gemini science Research Council- from a Canadian Herzberg Institute perspective for of Astrophysics and the period 2007– Gemini staff held 2012. We will a very successful have a workshop “kickoff” meeting in in Montréal on late March in Hilo. May 4th and 5th The development where the work of phase is expected the teams will be to take about 1 presented, discussed, year. Negotiations and science cases are now underway drafted. The timing Canadian proposal totals for Gemini Semester 2003B. The top table indicates number of proposals. The bottom on an operations of the meeting allows table shows distribution of time requested. contract. The plan for further work and is to begin operating fi nalization of the science cases before the The number of proposals is encouraging, a very simple archive this summer and Aspen workshop. but with the average proposal request at to incrementally add functionality as the just over 13 hours, the oversubscription development process moves forward. Canada received a total of 35 proposals rate is somewhat low. As expected, the 24 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 24 5/16/03, 4:56:54 PM AUSTRALIA Warrick Couch riting this issue’s contribution thus, maintaining its importance within and most of the lenses — all survived the is made easy with the Australia as a research center and national fi re. Another key aspect is that all the Wabundance of news, but is icon well underway. Central to these fabrication will be out-sourced, through made diffi cult in having to report the plans is getting its Gemini instrument a subcontract to the Canberra-based terrible events that have affected the construction program back on track, aerospace company Auspace Limited Australian astronomy community, and not just in recovering from the loss of (which has worked closely with the more broadly, Gemini in the last 6 NIFS, but also ensuring that the building RSAA for many years and has already months. of the Gemini South Adaptive Optics been involved in the NIFS project). Imager (GSAOI) — the contract that Importantly, this will allow the RSAA On what has become known as “Black was awarded to the RSAA at the end of team to concentrate on GSAOI. Saturday” (January 18, 2003), a massive 2002 — is delivered to Gemini in a timely bush fi re swept up the slopes of Mt. manner. Fortunately, NIFS was covered by Stromlo, and destroyed much of the ANU insurance, although by a policy observatory at its summit. All of the Within a month of the fi re, Peter that will pay the RSAA only to build a telescopes were damaged beyond repair, McGregor and his team had a recovery replacement. Hence, the rebuild will allow including the 74–inch and Gemini to recover its investment 50–inch telescopes, the latter in NIFS and, provided it is done receiving worldwide recognition in a 2-year timeframe, will provide for its role in the MACHO an instrument that is still very (Massive Compact Halo competitive scientifi cally. Objects) experiment and about to commence an all-southern- As such, the RSAA has now sky digital survey. Many other received approval from Gemini’s buildings were lost, including director to proceed with this the heritage-listed administration plan. Meanwhile, the design and building (which housed the Image of Mt. Stromlo Observatory circa 1955 construction of GSAOI continues design offi ce and library), the almost uninterrupted, thanks to mechanical and electronic workshops, plan for NIFS in place, which involved temporary offi ce and workshop facilities and astronomers’/students’ houses. The building a clone by the end of 2004, being made available on the ANU campus bad news for Gemini was that its Near- and making it available to the Gemini and at the nearby Australian Defence Infrared Integral Field Spectrograph community by mid-2005. While clearly Force Academy. (NIFS), which was within 6 months of an ambitious plan, the recovery process being completed and delivered to Gemini is aided enormously by the fact that key Despite these events, Australia has North, was undergoing its third cool- NIFS components — such as the designs continued to actively prepare for the down within the workshops, and was and drawings, the HAWAII-2 science second Gemini Future Instrumentation totally destroyed by the extreme heat and detector, the pupil and fi eld mirror arrays, Workshop, in Aspen, CO. This has been building collapse. While the damage organized and structured around the to property was immense, we can same four science theme areas that be thankful that no observatory are the focus for Aspen. For each of personnel were injured or lost their these areas a local “Group Chair” has lives. been appointed, whose brief has been to canvas the members of our Gemini In the face of this calamity, the community as to what their scientifi c Research School of Astronomy needs and visions are in the post-2006 and Astrophysics (RSAA) staff era and, accordingly, develop science and the Australian National cases (with associated instrument University (ANU) have responded Rear view of the administration building and remnants of the 50 inch requirements) that they will take to magnifi cently, with plans for telescope on Mt. Stromlo after the January fire. and present at Aspen. Our Group rebuilding the observatory, and Photo courtesy of Matthew Colless, RSAA, ANU. Chairs are: Tim Bedding, Stuart Gemini Newsletter #26 - June 2003 25 NsLtr0603txt-rev2 25 5/16/03, 4:56:56 PM Ryder, Brad Gibson and Brian Boyle. To received for 2003A returning us to the Finally, Gemini will have a strong carry out this consultation process, they levels experienced in the 2002 semesters. presence at the upcoming International have organized a series of mini-workshops There was also much stronger demand Astronomical Union (IAU) General and meetings across all the astronomical for Gemini South time, a result of Assembly in Sydney, Australia in July institutions within Australia. The input GMOS South being offered for the fi rst with both the Gemini Observatory and from these meetings is now being collated time. The overall subscription factor for the Australian National Gemini Offi ce and merged into a “science driver” Gemini North was 2.1 with six proposals having exhibits alongside each other. document for each group. In early May, requesting time on GMOS North, two on This will provide a good opportunity to we will hold our second community-wide NIRI and two on Michelle. For Gemini publicize both national and international “Pre-Aspen” workshop, where the science South, the overall subscription factor was Gemini activities to the large number of cases for each group will be presented, 2.4 with eight proposals requesting time astronomers who will attend the IAU as discussed, and fi nal input received before on GMOS-S, one on Phoenix and one well as to the Sydney public. We hope they are taken to Aspen. on T-ReCS. Of note was the number that there will be good turnout at the of “hedged” proposals involving the use IAU from astronomers throughout the The Semester 2003B proposal deadline of either GMOS-N and/or GMOS-S as Gemini partnership, and we look forward has just passed. Pleasingly, the number well as Michelle and/or T-ReCS for their to seeing you in Sydney in July! of proposals received (20) represented programs. a factor of 2 increase on the number BRAZIL Max Faúndez-Abans e have successfully provided We are glad to announce that Kátia to intensify the PIO activities in Brazil the Brazilian Gemini Cunha, Ph.D. from Ministério da Ciência through press releases based on Brazilian Wcommunity our fi rst National e Tecnologia/Observatório Nacional has investigators and Gemini results as well as Gemini Offi ce (NGO) instrument been granted the U.S. Gemini Fellowship through increasing the number of Gemini support. It has been a good opportunity at the University of Texas at El Paso for highlights presented at talks and public to tighten the contact with other Gemini the 2003–2004 cycle. The Brazilian visitations. scientists and technicians, and we have NGO wishes to thank all the members gained experience. Our service has had a of the Gemini Fellowship Committee The LNA operates the Pico dos Dias good reception by the users, which assures and the members of the National Science Observatory (OPD) where a public us that we have done a good job. Foundation, Association of Universities visitation program for schools is carried for Research in Astronomy, Inc. and the out by the NGO staff astronomers. As for the proposals for Semester 2003B, a National Optical Astronomy Observatory About 1,400 students per year visit the total of 38.87 hours at Gemini North have involved in the process for the kind OPD and learn about the observatory, been requested representing a pressure assistance during the selection, and for astronomy, instrumentation, Gemini and factor of 1.77. For Gemini South, 88.39 this great career opportunity for Dr. SOAR (SOuthern Astrophysical Research hours have been requested with a pressure Cunha. Telescope). factor of 4.42. There has been a clear rise in the number of proposals submitted by The Brazilian NGO, Laboratório Senior citizens are also one of our target the Brazilian community in comparison Nacional de Astrofísica (LNA), intends groups for our outreach effort. They are to the last semesters e.g., 21 proposals willing to learn about modern technology in 2003B compared with 18 in Semester and the latest achievements of science and, 2002B. as such, they are amazed by the Gemini Observatory and the kind of science that The Brazilian NGO is working together is done with the twin telescopes. with Gemini to develop the staff training program that supports the instruments in We have used Gemini as an example of the Phase II process. We expect to have international cooperation, national effort our fi rst experiences with the instruments and state-of-the-art technology. The at the telescopes during the second Half of the senior citizens group (65-–87 years old) visiting the LNA has worked closely with ECONTI, semester of 2003. OPD/LNA to learn about observatories in general and about a senior citizens center based in Itajubá, Gemini. Minas Gerais (see picture). 26 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 26 5/16/03, 4:56:58 PM CHILE Luis Campusano & Sebastián López ONICYT, as a national host to Only three proposals (two for CIRPASS, hours in total, which corresponds to a Gemini, continued to receive and one for Phoenix) were received more healthy subscription factor of 2.4 . Cproposals for the use of its for Semester 2003A. The number of Gemini South telescope time through requested hours was 83, yielding a formal Semester 2003A was the fi rst semester the partnership. This refl ects the new subscription factor of 1.3, which is still where National Offi ces played an active modality of Chile participation in the rather small. role in supporting Phase II. Several issues partnership, which better serves the were identifi ed in this fi rst trial, which Chilean astronomical community and We have continued to use the Phase I will help us to prepare Chilean-specifi c the Gemini Observatory. A fund to Tool (PIT) with no complaints reported guidelines for the upcoming Phase II. invest in the development of astronomy and submissions via e-mail. No major For example, it will allow us to optimize and closely related sciences within Chile problems were identifi ed during the the NGO-PI (National Gemini Offi ce- is under consideration. The current feasibility reviews of the proposals, which Principal Investigator) interaction and access to 8-meter-class telescopes that is an indication that a suffi cient amount identify the different levels of queries we Chilean astronomers have is indeed of information is being provided in the may receive. very large in comparison to the other Gemini web pages. We expect far more partner astronomical communities. Thus, proposals in 2003B now that GMOS The PPARC Gemini studentship 2003, Gemini South with its instrumentation is being offered. The review committee available for Chilean students and has to compete with the Very Large should have more work and discussion administered in Chile by the Fundación Telescope and Magellan telescopes to this time. The deadline for receipt of Andes, had a strong competition this get the attention and interest of our 2003B proposals was again set to mid- year. It was awarded to Antonio Hales, privileged astronomers. Fortunately, April (14th), about 2 weeks later than a B.Sc. graduate in Astronomy from the both the formation of human resources deadlines of other observatories in Chile. University of Chile, who was accepted at departments and the increase of The latest news for 2003B is that ten the University College London (UCL) researchers in Chilean institutes are now proposals were received (seven for GMOS to study for a Ph.D. in Astronomy. We in an expansive period. and three for T-ReCS) asking for 205 wish Antonio a very successful research experience at UCL and a happy return to Chile in a few years’ time. Gemini Newsletter #26 - June 2003 27 NsLtr0603txt-rev2 27 5/16/03, 4:56:59 PM THE GEMINI SOUTHERN OPERATIONS CENTER Peter McEvoy emini Observatory passed a major videoconferencing facilities were base-level visitor and staff interaction to milestone in its development appropriately considered. All were in the telescope during observing runs. Gduring the fi rst weekend of place extremely quickly with minimal March, when months of construction disruption after the physical move. In March 2003, the new building hosted and logistical work terminated in the the Gemini Oversight Committee, and successful move of all staff and equipment A skeleton team of Gemini South staff Gemini Board members experienced the at Gemini South from temporary working plus several very welcome volunteers building for themselves when they met in quarters to the new Southern Operations were directly involved in the removal of La Serena in May. Center, located at the AURA Recinto in furniture, offi ce equipment and related La Serena, Chile. Dominating the landscape at the AURA Recinto, the The initial clearing of the site impressive building has for the building took nearly many Chilean touches in 17 months. The bulk of the its design, including facades construction work began of beautiful local stone in January 2002. Gemini with a copper roof (Chile contracted with three is the world’s number companies – Oda-McCarty one producer of copper). Architects, who designed Regrettably, while many the Hilo facility, the Andes offi ce windows overlook Group, a prestigious Chilean the city of La Serena and architectural fi rm, and the Pacifi c Ocean, few staff Rencoret Limited, a major members have the time to local builder – to work appreciate their view across together on the project with the facility’s landscaped a small Gemini construction gardens. There are no taskforce led by Paul Gillett complaints, however. After and Paul Collins. Their work The front entrance of the Gemini South Base Facility showing the locally quarried stone facade the years spent in temporary provided Gemini South staff and Chilean copper roof. See additional images of this new facility on the opposite page. offi ce space loaned from with very comfortable offi ce CTIO and in the old Casa and laboratory space. The remarkable materials from the “Casa Verde” and their Verde, all are enjoying the spaciousness, dedication of all involved to safe working subsequent placing in the new building quiet and working comforts available in standards resulted in no days lost due during long days over the weekend of the new Southern Operations Center. to accidents during the approximately March 1–2, 2003. 100,000 construction hours required to The move itself was a tremendous example build the facility. This record compares Costing US$2.3 million, the two-story of planning and team coordination at very favorably against both Chilean and building’s 17,668 square feet (1,642 a very detailed level, and the building U.S. standards. m2) provides offi ce and conference room stands as a symbol of Gemini’s progress. space for 60 staff and visitors. Shared with As one staff member commented during Detailed plans for the move were its neighbors CTIO and SOAR, the 42- the fi rst week of the building’s occupancy, developed to cover more than 70 seat lecture theater and major instrument “It is now very much up to us at Gemini distinct work packages, and have ensured laboratory are important additions to the South to make sure we perform top- that issues such as safety, network, AURA infrastructure in La Serena. The class work here to justify the wonderful power, telephony, air conditioning, Operations Room is designed, in a similar infrastructure, which has been put in offi ce furniture and equipment, and fashion to Gemini North, to facilitate place for us, not to just work with, but to enjoy.” 28 Gemini Newsletter #26 - June 2003 NsLtr0603txt-rev2 28 5/16/03, 4:56:59 PM STARS OVER WELCOME TO THE NEW GEMINI GEMINI NORTH SOUTHERN OPERATIONS CENTER The star-trail image above is a “stack” of about 100 images 50-second exposure. A dark frame subtraction was also used from a new time-lapse movie of the early summer sky rising to reduce noise from the charge-coupled device (CCD) in over Gemini North. A final image was added that reveals the camera. the stars offset by about 20 minutes and shows the stars of the constellation of Scorpius (among others) over the The smaller images shown at the top are individual frames Gemini dome. Automobile tail-lights can be seen as well from the sequence obtained during the course of the night. as a red light that was used to highlight the dome. The The image at left shows the first glow from the early yellowish light on the right side of the dome is light from morning sunrise and the rising Milky Way. The image at the setting moon, and the light on the left side of the dome right reveals the final glow of evening twilight with the 10- is from the first glow of dawn. A Nikon D1X digital camera day old moon (not visible) still high in the sky illuminating was used with a AFNikkor 14mm lens (at f/2.8) for each the Gemini enclosure. Both images have the same technical specifications as the star-trail image. Gemini Observatory Images NsLtrCvr0603rev2 2 5/16/03, 4:55:26 PM THE GEMINI OBSERVATORY is an international partnership managed by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation. Gemini Observatory Gemini Observatory Northern Operations Center Southern Operations Center 670 North A‘ohoku Place c/o AURA, Casilla 603 Hilo, Hawai‘i 96720, USA La Serena, Chile Phone 1-808-974-2500 / Fax: 1-808-935-9235 Phone 011-5651-205-600 / Fax: 011-5651-205-650 Gemini Observatory - Tucson Offi ce 950 N. Cherry Ave., P.O. Box 26732 Tucson, Arizona 85762-6732, USA Phone: 1-520-318-8545 / Fax: 1-520-318-8590 e-mail: [email protected] http://www.gemini.edu UNITED STATES • UNITED KINGDOM • CANADA • CHILE • AUSTRALIA • ARGENTINA • BRAZIL Gemini South Explores a Young Planetary System Inside This Issue • The Gemini Deep Deep Survey • Recent Science Highlights • Gemini Instrumentation Update • StarTeachers and Public Information & Outreach Update • Meet Gemini South’s Peter McEvoy • A Visit to the New Gemini South Base Facility Interior of the Frederick C. Gillett Gemini Telescope (Gemini North) by moonlight. This 50-second exposure was obtained on February 9th, 2003 using the same equipment as the images on the inside front cover. NsLtrCvr0603rev2 1 5/16/03, 4:55:16 PM