OBSERVERTHE AUSTRALIAN ASTRONOMICAL OBSERVATORY NEWSLETTER NUMBER 120 AUGUST 2011 Multi-Object IFU comes to the AAT km/s H#009

km/s H#009

The 6dFGS Fundamental Plane Are you biased? Dragonfly flutters its wings DIRECTOR’S MESSAGE

Director’s message Matthew Colless

We are currently in the process of developing mode, particularly if refurbishment of the the opportunities to gain additional access the AAO Forward Look, a strategic plan that telescope and an upgrade to 6dF allow more to international facilities in which Australian will define the AAO’s goals for 2011-2015 and ambitious programs, such as the proposed astronomers have an interest. beyond. It is based on the goals and priorities TAIPAN galaxy survey. 6. Exploiting the improved facilities of the set out in the Australian Astronomy Decadal AAO’s new Sydney headquarters to energise Plan 2006-2015 and the recent Mid-Term Review 3. Managing the AAO’s evolving role at Siding and advertise the organisation. The move of of the Decadal Plan (see http://www.science. Spring Observatory in light of foreshadowed the AAO’s headquarters to new premises in org.au/natcoms/nc-astronomy/decadalplan. changes in ANU’s role and support. Over North Ryde, slated for the middle of next year, html). The AAO Advisory Committee endorsed the next five to ten years the ANU is likely represents a significant investment in the the Forward Look process at its inaugural to be scaling back its level of support for organisation by the Australian government. meeting in March, and initial consultations operations at Siding Spring Observatory (SSO). The new building will provide improved have already been held with the Advisory Appropriate evolution of the operations model office areas and better facilities for the Committee, the AAL Board, AAL’s Optical for SSO therefore needs to be considered, instrumentation program, allowing the AAO Telescopes Advisory Committee, the AAO including the possibility that the AAO might to efficiently assemble, integrate and test Users’ Committee, the Australian Time assume responsibility for SSO operations. In larger instruments for larger telescopes. Assignment Committee and AAO staff. that case the ANU would continue to own the site, but become one of several organisations Together with the solid funding outlook for the There are many challenges and opportunities with facilities at SSO that are supported by the Observatory, the new headquarters will provide for the AAO in the next few years, but the eight AAO. the AAO with the confidence and capacity to framing goals for the Forward Look are: make the changes needed to respond to the 4. Improving the AAO’s support model for changing astronomical environment and to 1. Maximising the research productivity and offshore telescopes where Australia is a undertake more ambitious instrument projects. impact of both the AAO itself and the users partner in an international consortium. This in turn will energise AAO staff and of its facilities. This is the fundamental goal At present the AAO’s focus is on operating advertise to the world that the AAO continues of the AAO, and sets the context in which all its onshore telescopes (AAT & UKST), but it to be a force in international astronomy. other issues are addressed. The AAO aims also supports Australian users of offshore to be a world-class astronomical institution, telescopes (Gemini & Magellan). As the focus 7. Recruiting and nurturing world-class providing excellent optical and infrared and investments shift to larger offshore staff. A research institution’s staff is its observing facilities and innovative telescope telescopes, the AAO must develop a plan for most important resource, so it is key to the instrumentation that enable Australian maximising outcomes from such facilities. AAO’s future that it continues to recruit and astronomers to do outstanding science (as This will involve some appropriate mix of nurture world-class astronomers, instrument evidenced by the articles on pages 6, 10, 11 organisational support (for time allocation scientists and engineers. This will be possible and 15 of this issue). committees, user committees and so on), if the AAO is recognised internationally as a user support (for preparation of proposals, powerhouse of astronomical research and 2. Determining the effective scientific remote observing capabilities, expert technology development, and if it provides lifetimes of the AAT and UKST, and assistance in data reduction and the like) facilities and opportunities that excite and developing appropriate and cost-effective and instrumentation development (setting challenge the best young people in Australia operations models. World-class research scientific agendas and winning guaranteed and from overseas. CONTENTS requires an appropriate mix of facilities on time for the community). Together these 8. Maintaining good relations with the all scales. In the next 5 years the Decadal services must provide evident added value to SCIENCE HIGHLIGHTS Plan and Mid-Term Review recommend astronomy community by being responsive Australian users of these facilities. to changing needs and effective in delivering SAMI Commissioning – First Hexabundle Galaxy Spectra 4 that Australia increase its access to large optical facilities to at least the equivalent of 5. Planning the AAO’s next generation of services. The AAO’s success and strong Galaxy Parameter Variations Across and Through the 6dFGS Fundamental Plane 6 a 20% share in an 8-metre telescope. On a instruments for all these telescopes, and support in the Australian astronomical Dragonfly flutters its wings 7 ten-year timescale, Australian astronomers leveraging the best scientific opportunities community is founded upon its track record of responsiveness to community needs RAVE at half a million 10 aim for a 10% share in an ‘Extremely Large for Australian astronomers through Telescope’, an ambition currently realised by the instrumentation program. The AAO and effectiveness in providing competitive The Magellanic Quasars Survey 11 Australia’s participation in the 25-metre Giant has one of the world’s best astronomical facilities and services for researchers. Close The Integrated Photonic Spectrograph’s First Look at the Heart of the Scorpion 13 Magellan Telescope project. The effective instrumentation programs and is a leader in consultation with the community is essential to maintain this situation in future, and the AAO Using AAOmega to measure the age of the young open cluster IC2602 15 lifetimes of the AAT and UKST depend on wide-field multi-object spectrographs and their scientific competitiveness with respect robotic fibre positioners. The AAO also has Forward Look must therefore be consulted with, and owned by, the community if it is to achieve Making MANIFEST fibres for the Giant Magellan Telescope 19 to such facilities, which in turn depends on a unique and innovative instrument science its goals. A Voyage Through FOG 20 telescope capabilities, instrumentation suites, group developing new technologies such as levels of access, scientific agendas, and the OH-suppression fibres, hexabundles, starbug We plan to make a consultation draft of the OBSERVATORY NEWS operational funding available to support robots and integrated photonic spectrographs Forward Look available to the Australian Australia’s portfolio of optical telescopes. (see the articles on pages 4, 7 and 13 of astronomical community in early November, Are You Biased? 21 With the ongoing refurbishment program, this issue). These capabilities are already with the final version to be completed and AusGO Corner 24 new instruments such as HERMES, and exploited to keep the AAT competitive and made public by the end of the year. In order upgrades to the existing instrument suite, to leverage additional access to front-rank to ensure that the community has every The 2011 Southern Cross Astrophysics Conference 26 the AAT will remain scientifically competitive facilities by providing instruments. The latter opportunity to discuss the draft and provide Scientist Meets Parliament 27 for another decade while also remaining a approach will become increasingly important feedback, I will be visiting major centres valuable testbed for new instruments and for the AAO and Australian astronomers to hold town-hall meetings discussing the LOCAL NEWS technologies. Over this period, however, as the importance of Australia’s onshore Forward Look during November and early the AAO, which already supports Australian facilities declines relative to international December. The AAO’s Forward Look will be Epping News 28 access to Gemini and Magellan, will shift its offshore facilities. The next generation of critical to the successful evolution of the AAO Vale Tom Cragg 29 operational emphasis towards these larger AAO instruments needs to be matched to the as Australia’s national optical observatory over telescopes and GMT. In the meantime, the scientific lifetimes and operational models the next five to ten years, so I look forward to Letter from Coonabarabran 30 UKST can continue operating in user-pays of the AAT and UKST, and balanced with these discussions! SCIENCE HIGHLIGHTS SCIENCE HIGHLIGHTS

SAMI Commissioning – First Hexabundle Galaxy Spectra Jon Lawrence (AAO), Scott Croom (University of Sydney), Amanda Bauer (AAO), Joss Bland-Hawthorn (University of Sydney), Sarah Brough (AAO), Julia Bryant (University of Sydney), Matthew Colless (AAO), Simon Ellis (AAO), Tony Farrell (AAO), Lisa Fogarty (University of Sydney), Michael Goodwin (AAO), Ron Heald (AAO), Anthony Horton (AAO), Andrew Hopkins (AAO), Heath Jones (Monash/AAO), Steve Lee (AAO), Geraint Lewis (University of Sydney), Stan Miziarski (AAO), Samuel Richards (AAO/University of Sydney), Max Spolaor (AAO)

Hexabundles are a recently developed simultaneously. If fed at a low enough technology (Bryant et al, 2011) that focal ratio, optics are not required in the Figure 2. Team member Sam Richards prepares for a long cold night in the triplet Figure 3. Schematic display of reconstructed hexabundle images based on offer the potential for integral-field fibre bundle, significantly simplifying top end. total integrated counts per hexabundle core for a field with 13 galaxies. Note spatially-resolved spectroscopy without alignment and assembly. Additionally, that hexabundles #6 and #2 were not functional during this observation. Galaxy positions were all centred within ~2 cores. the complexities inherent with existing each hexabundle IFU can be made much bulk-optic lenslet array, microlens array, smaller than its bulk- or micro-optics or image-slicing mirror techniques. counterpart – simplifying the positioner The hexabundle consists of a series of system design and allowing close packing multimode fibre cores (so far 7, 19, and of objects. 61 core devices have been demonstrated) that are lightly fused together over a The SAMI Instrument small (~20 mm) interaction length. With a view to providing the first on- Interstitial holes are filled with soft, low telescope demonstration of hexabundle refractive index glue. This geometry acts technology, the AAO and the University as a compact relatively high fill-factor of Sydney have collaborated on the integral-field unit (IFU)/image-slicer, development of the SAMI instrument for giving significant advantages for multi- the AAT. SAMI uses 13 x 61 core unfused object IFU systems that bridge the gap hexabundles that are mounted on a plug- Figure 1. The SAMI plug plate assembly unit mounted between large monolithic IFUs and plate at the 1 degree field-of-view triplet onto the Prime Focus Camera. The white “splice box” single-aperture multi-object systems. corrector top-end focus (Figure 1) on the connects the blue hexabundles and orange sky fibres from the brass plug-plate to the fibre bundle. Prime Focus Camera. At f/3.4 with 105 The Hexabundle Advantage μm core diameter fibres, each hexabundle The key benefits of integral-field samples a 14” field at 1.6” per fibre. At For acquisition and guiding we use a spectroscopy for extra-galactic science the output end, a total of 13 V-groove slit CCD camera mounted on a gantry above are that gas and stellar kinematics blocks are mounted at the AAOmega slit. the plug plate that views the central few over an entire galaxy can be measured Each slit block includes 63 fibres (all the arcmins of the field through a hole in the Figure 4. SAMI commissioning team galaxy-field celebrations. Figure 5. Velocity map produced from the first galaxy-field commissioning plate. The box is ~15” square. enabling the separation of dynamical fibres from 1 hexabundle and 2 fibres for plate. components, the measurement of sky subtraction). dynamical mass, the examination of A ribbonised fibre cable of length ~40m SAMI Commissioning the impact of winds and out flows, and joins the two instrument ends. Fibres the discovery of merging systems via The first commissioning run for the SAMI from this cable are glued into the positioned around several bright (m~6) Early in the morning on the first While some modifications to the dynamical disturbance. This information multi-object IFU instrument occurred V-grooves at the spectrograph slit. At the stars in the field. Fine adjustment was commissioning night, after alignment instrument are required, it appears is obtained in addition to parameters than from 1st-4th July 2011. After installing top end, the hexabundle fibres are each accomplished using fainter (m~14) stars and system checks using stellar field feasible to conduct dedicated science can be readily measured with single- the instrument, the initial step was to fusion spliced to the ribbon fibres inside coupled through the hexabundles and the plates were completed, a galaxy field surveys with SAMI in the near future. aperture spectroscopic instruments align the plug plate to the telescope a protective “splice box”, mounted on the AAOmega spectrograph. A near real-time plate was installed, and a 20 minute (e.g., star formation rates, gas phase optical axis. It was unsure prior to SAMI internal wall of the top-end barrel. data pipeline extracted the partially- galaxy observation was made (Figure 4). Acknowledgements metallicities, stellar ages, stellar commissioning whether the Prime reduced spectra from the detector Stacked images from subsequent nights metallicities, and black hole accretion Focus Camera that was originally We warmly thank all staff at the AAO Each hexabundle is mounted in a standard images and incorporated a schematic observing were used to construct velocity and extinction due to dust). built for commissioning of the AAT in for their support in developing and (SMA) screw-thread fibre connector. The display of reconstructed hexabundle fields for each of the target galaxies, see plug plates have a mating connector at the early 1970s and last used over a commissioning the SAMI instrument and Integral field spectroscopy has so far fields based on total integrated counts for example Figure 5. each object position. Two galaxy fields decade ago, would be well aligned to the the AAOmega spectrograph. almost exclusively been limited to per hexabundle core (Figure 3). Measured (i.e., 26 objects) are pre-drilled per plate telescope optical axis. This provided the single-object instruments, meaning centroids were used to derive precise Conclusions along with a set of 26 blank sky locations opportunity/necessity for an observer to References that it is time consuming to build large offsets for each bundle – allowing common to both galaxy fields. For the ride in the top end (Figure 2 and front The first commissioning run of the SAMI Bryant, J. et al, MNRAS, 2011, arXiv1104.0985 galaxy-samples. The key innovation of field rotation and telescope pointing proposed integration time of 2 hours per page), something also not seen at the instrument was extremely successful. the hexabundle-based approach is that it corrections. These data were also used to field this means that 3 plates (or 2 plate AAT for some years. This on-telescope experiment has becomes possible to build systems that derive corrections to the field distortion exchanges) are required each observing demonstrated the potential of hexabundle are capable of positioning a significant Initial coarse alignment of the plug plate coefficients that will be used for the next night. The down time between fields is technology for multi-object IFU science. number (i.e., tens to hundreds) of IFUs assembly was done by eye – using holes commissioning run. less than 30 minutes.

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Galaxy Parameter Variations Across and Through References Bernardi et al. 2003 AJ 125, 1866 the 6dFGS Fundamental Plane Djorgovski & Davis 1987 ApJ 313, 59 Dressler et al. 1987 ApJ 313, 42 Christina Magoulas (University of Melbourne), Christopher Springob (AAO), and the 6dFGS team Graves, Faber, & Schiavon 2009a ApJ 693, 486 http://www.aao.gov.au/local/www/6df/ Graves, Faber, & Schiavon 2009b ApJ 698, 1590 Jarrett, Chester, Cutri, Schneider, Skrutskie, & Huchra 2000 AJ 119, 2498 Jones et al. 2009 MNRAS 399, 683 La Barbera, de Carvalho, de la Rosa, Lopes, Kohl- From 2001 to 2006, the UK Schmidt 2009a), yet the statistical models and individually. We find that they occupy Moreira, & Capelato 2010 MNRAS 408, 1313 Telescope undertook an all-southern fitting techniques used to determine the the same FP, though there is some Magoulas et al., 2011, (in prep) sky spectroscopic survey, known as the plane have not evolved with the same segregation along the FP, such that spiral Figure 1: 6dFGSv galaxies plotted in (J-band) Figure 2: 6dFGSv galaxies binned in FP space, with Pahre, de Carvalho, Djorgovski 1998 AJ 116, 1591 Six-degree Field Galaxy Survey (6dFGS). level of detail. Many previous studies bulges are preferentially larger in size. ‘Fundamental Plane space’. Fundamental Plane redder colours corresponding to increasing values of space is the logarithmic parameter space determined each stellar population parameter. The colour bar on The final data release of 6dFGS redshifts used simplistic linear regression fitting However, this trend is likely an artifact Saglia, Colless, Burstein, Davies, McMahan, & by the three Fundamental Plane parameters, half- the right shows the log of stellar age in Gigayears. Wegner 2001 MNRAS 324, 389 took place in 2009 (Jones et al., 2009), techniques and model the distribution of our galaxy selection. We only include light radius R , velocity dispersion , and surface The size of each sphere scales with the logarithm of e Springob et al., 2011, MNRAS, (submitted) though we continue to make use of the of galaxies in FP space as a 2D plane spiral galaxies whose bulge is enclosed brightness Ie. The best-fit plane is shown in green. the number of galaxies in the bin σ survey’s spectra for extragalactic and with scatter. However, these fitting by the large 6dF fibre. Therefore the cosmological studies. methods fail to account for the censoring spiral bulges in our sample are more present in an observed FP sample likely to be galaxies that are larger The peculiar velocity subsample of and the measurement errors (and and/or nearby. In any case, we find no 6dFGS (6dFGSv) includes approximately their correlations) in each of the FP evidence of a large offset of the FP 10,000 early-type galaxies. With the parameters and so are susceptible to between morphological subsamples. goal of ultimately deriving the distances bias, limiting any interpretations drawn Including spiral bulges in our sample and peculiar velocities of each of these from their best-fit plane. Instead, we does not increase the total scatter of the galaxies, we make use of an important adopt a three-dimensional Gaussian Fundamental Plane. correlation for early-type galaxies, model for the FP distribution, whose the Fundamental Plane (FP). The FP best-fit parameters are determined Stellar Population Parameters is a three-dimensional relation in the Dragonfly flutters its wings using a maximum likelihood method (in and the Fundamental Plane logarithmic space of galaxy size, velocity a similar manner to Saglia et al., 2001). Nemanja Jovanovic (AAO/Macquarie University), Barnaby Norris (University of Sydney), Simon dispersion and surface brightness The most recent FP studies (La Barbera Our fitting method properly accounts for Gross (Macquarie University), Paul Stewart (University of Sydney), Ned Charles (University of (Djorgovski & Davis 1987; Dressler et al., et al., 2010, Graves et al., 2009b) have selection effects in the sample (due to Sydney), Peter G. Tuthill (University of Sydney), Sylvestre Lacour (Observatoire de Paris), Martin 1987). A redshift-independent distance focussed on analysing trends of the FP cuts in velocity dispersion and apparent Ams (Macquarie University), Jon Lawrence (AAO/Macquarie University), Graham D. Marshall to an early-type galaxy can be derived by with stellar population parameters in magnitude) and observational error (and (Macquaire University), Gordon Robertson (University of Sydney), Michael Ireland (AAO/ measuring its offset from the FP relation. order to understand how they contribute their correlations) in the FP parameters However, such an analysis requires us to to the scatter and tilt of the FP. We have Macquarie University), and Michael J. Withford (Macquarie University) (Magoulas et al., in prep). carefully consider how we fit the FP, and derived stellar population parameters how we account for selection effects. In In the J-Band, our tightest sample, the for 7132 of the galaxies in 6dFGSv, and this article, we describe how we fit the best-fit Fundamental Plane has a slope examined the variation of the stellar FP for this sample, and how we account and scatter that is consistent with other population parameters in FP space. We for the trends of other parameters within near-infrared Fundamental Planes (La bin the galaxies along the axes of the Since the first detection of exoplanets some interferometer but unlike interferometers within a photonic chip. The waveguides ‘FP space’. This process also allows us to Barbera et al., 2010; Pahre et al., 1998). three-dimensional Gaussian model, fit 20 years ago (Wolszczan et al, 1992), more before it, it takes a revolutionary remap the pupil of the telescope into a gain new insights about galaxy formation The FP slope in velocity dispersion, a, with the maximum likelihood method than 500 planets have been discovered to new approach to the design of such 1-D slit at the output, which is known as and evolution. is observed to be steeper (a ~ 1.5) in the discussed above, and compute median date (see http://exoplanet.eu). The majority instrumentation; it is based on integrated pupil remapping. The emanating beams near-infrared than is usually found in values of these bins of stellar age, [Fe/H], of planets found have been detected via photonic circuits (micro-optic chips), are recollimated with a second micro-lens Sample Selection and the optical (a ~ 1.2), which is consistent [Z/H], and [ /Fe]. We find clear trends two methods: high precision surveys of micro-mechanical mirrors and micro- array before being dispersed and focused Fundamental Plane Fitting with an old stellar population. Figure 1 in each of these parameters across and stellar radial velocity (Wright et al, 2007), optics as shown in Figure 1 (Tuthill et al, onto an InGaAs detector. α or transits in which the planet partially 2010). shows the distribution of galaxies in 6dF through the plane (Springob et al., 2011). This unique photonic based instrument 6dFGSv comprises 10,000 of the brightest occults the light from its host (Borucki et J-Band FP sample, in the space of the The light enters the instrument from offers many benefits including: galaxies with redshift z < 0.055 from From the perspective of using the FP as al, 2010). Both techniques are strongly Fundamental Plane parameters along the left of Figure 1 and is directed onto the main redshift survey of 6dFGS. a distance indicator, the most important biased towards finding planets with higher „„ Spatial filtering - the light with the best-fitting plane of the three a segmented mirror which is placed in The near-infrared target selection of of these trends is the trend of stellar age masses in tight orbits. For studying planets propagating within the single-mode dimensional Gaussian. the pupil plane of the telescope. This 6dFGS favours older, bulge-dominated in FP space. As Figure 2 shows, stellar that are further out there is strong interest waveguides has a simple planar mirror can be used to steer each segment galaxies, as these wavelengths are less age is seen to vary directly through the in so-called “direct detection” techniques, wavefront. As a result, all residual Morphology and the of the pupil in both tip and tilt and can sensitive to dust extinction than are plane. We find that selecting on age such as coronography or optical stellar phase aberration across each sub- Fundamental Plane be pistoned to alter the path length optical wavelengths. The 6dFGSv sample yields a modest reduction in the FP interferometry in which planetary light is aperture is rejected, resulting in a difference for each segment through combines 6dFGS velocity dispersion We have visually inspected our entire scatter, as galaxies younger than 3 Gyr isolated, negating the need for continuous mode-cleansed interferogram. the instrument. The light then passes measurements with photometric sample of galaxies to classify their occupy a plane with a scatter along the monitoring over one or more orbital through a beam reducing telescope „„ Simple, high precision optical parameters in the J,H and K near- morphological type, identifying any distance dimension of 31.5%, while those periods (>20 years). infrared passbands from the Two Micron disc-dominated galaxies that may older than 3 Gyr occupy a plane with which re-images the pupil onto a micro- path length matching – Routing of All Sky Survey (Jarrett et al., 2000). be contaminating our sample. We scatter 27.2%. In the coming months, With the aim of developing an instrument lens array such that there is a 1-to-1 waveguides within the chip can be have separated the sample into pure we will be calculating peculiar velocities that allows for high dynamic range correspondence between each element achieved with sub-micron precision Since the original formulation of the early-type galaxies (i.e., elliptical and for all 10,000 galaxies in 6dFGSv, and imaging for use in exoplanetary on each component, respectively. The allowing for extremely precise Fundamental Plane relation, the size lenticular) and spiral bulges. We have fit a accounting for these age trends to get science, the Dragonfly instrument was focused beams are then injected into an matching of optical path lengths. and quality of galaxy samples has more accurate distances. conceived. Dragonfly is an optical stellar array of optical waveguides embedded steadily increased (Bernardi et al., 2003; Fundamental Plane to each of these La Barbera et al., 2010; Graves et al., morphologically selected subsamples

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A prototype Dragonfly instrument was taken to the Anglo-Australian Telescope (AAT) and tested on the 20th and 21st of May, 2011. The entire instrument was installed in the UCLES pre-slit Coude room (Figure 3). The instrument was aligned to be co- linear with the injection beam to UCLES such that the UCLES slit viewing camera could be used for telescope pointing and tracking. For the on-telescope tests, an 8 waveguide pupil remapping photonic chip was used which reformatted the light into a plane of equally spaced waveguides. In order to eliminate the redundancy induced by having equally spaced waveguides, certain guides were switched off, in order to simulate a non-redundant array Figure 1: Schematic diagram of the Dragonfly instrument. Orange circles indicate the segments used on each optical component. Red arrows depict the direction of of guides as shown in Figure 2(c). This propagation of the stellar signal through the instrument, arriving from the telescope at the left. arrangement of waveguides was used as it allowed us to simulate 6 baselines simultaneously (i.e. 6 sets of fringes are overlapped on the detector at once). „„ Compact and robust – An entire to optical waveguides makes it slits have light injected into them, it photonic chip encoding advanced possible to fill the entire pupil is possible to choose the separation Within 30 minutes after first injecting Figure 3: Nem aligning Dragonfly in the Coude room. processing capability will only plane with waveguides, allowing a between slits and hence frequency light from the scope, we had star light measure several centimetres in significant increase in sensitivity. of fringes that are generated on the on the detector. This in itself is an size, and is thus a compact, robust detector as shown in Figure 2. It’s accomplishment as the AAT does not have „„ Cross-dispersed integral field unit – device highly resilient to errors not only possible to select a single adaptive optics, making coupling into Pupil remapping into a linear pattern induced by thermal or mechanical set of fringes corresponding to a single-mode waveguides very difficult. permits the orthogonal ordinate of anisotropies. single baseline of the instrument Further, in order to avoid blurring of a 2‑D array detector to be utilized to as depicted in Figure 2(a) and (b), the fringes as a result of atmospheric „„ Non-redundant beam combination record spectral data. but it is also possible to turn on a fluctuations, we had to integrate at times – The input pupil geometry can „„ Waveguide coupling optimization – By combination of waveguides such that commensurate with the atmospheric be arbitrarily remapped into any positioning the segmented mirror multiple sets of fringes with various coherence time (~10 ms) which meant we output configuration. Therefore and the injection micro-lens array fringe frequencies are superimposed had very low signals on a high read-noise beam recombination schemes at the pupil plane of the telescope, it on the detector simultaneously, as laboratory grade detector. can be configured to eliminate any is possible to use the tip/tilt feature depicted in Figure 2(c). By measuring redundancy noise. On the second night, we pointed the of the segmented mirror to carefully the phase associated with multiple telescope at Antares as it is one of the „„ Full utilization of the available optimise the coupling into the 10 μm fringe frequencies/baselines/ brightest objects in the sky in the H-band telescope pupil – In contrast to optical waveguides. spatial frequencies, it is possible to (-3.5mag) and after stacking frames for aperture masking interferometry calculate a “closure phase”, which The principle of the interferometer is that several hours we managed to demonstrate where very few holes are used in a is a measurable used to eventually the output of each waveguide acts like that we could detect all 6 baselines of the plate to achieve non-redundancy, reconstruct an image of the stellar Figure 4: Power spectrum of the fringes detected by the system. Vertical axis is the wavelength a slit. By choosing which waveguides/ interferometer. Figure 4 shows the spatial the remapping capability inherent target. decreasing from ~1.75 to 1 μm as you move up the axis. Horizontal axis shows the spatial frequency frequency/baseline separation plot as a components of the interferogram. The lower band of dots is in the H-band and 6 can clearly be seen. function of wavelength. The white lines show the predicted position of the spatial frequencies/baselines for the system. This was a fantastic proof-of-concept demonstration and over the next 6 months we will be refining Dragonfly ready to go to a larger scope with an adaptive optics system, where we hope to begin doing science with it. One day, Dragonfly may help astronomers hunt for and study faint exoplanets which will give us a better understanding of planetary and solar system evolution, but for now it’s just a lot of fun.

References Borucki, W. J. et al, 2010, Science, 327, 977 Figure 2: (a) and (b) depict the power spectra and fringe patterns (insets) associated with 2 pairs of waveguides with different separations. (c) Shows the power spectrum and the corresponding fringe pattern when light was injected into a combination of 4 waveguides. The dots represent the waveguides. Yellow – light injected, blue – light Tuthill, P. et al, 2010, Proc SPIE, 7734, 51 decoupled. The various baselines achieved with each combination of waveguides is displayed below each set of dots. Wolszczan, A. et al, 1992, Nature, 355, 145 Wright, J. T. et al, 2007, ApJ, 657, 533 Figure 5: The Dragonfly team celebrating their fringe victory.

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RAVE at half a million The Magellanic Quasars Survey Fred Watson [AAO] and the RAVE collaboration Szymon Kozlowski (Warsaw University Observatory), Christopher S. Kochanek (Ohio State University)

Back in June 2005, Coonabarabran laid demands extensive The variability of quasars has provided Unfortunately, while the SDSS Stripe controlled with a few ancillary cuts, as on a sparkling winter weekend when calibration and many clues about the nature of active 82 quasar sample was the largest and we explored in Kozlowski & Kochanek the AAO hosted RAVE’s seventh annual associated modelling, galactic nuclei (AGN), but recent best available, the light curves are not (2009). Second, we can use the variability collaboration meeting. Now, the town and this has involved developments are leading to a revolution very good -- too few epochs and an parameters for the SDSS quasars to has put on a repeat performance, with scientists at several in quantitatively analyzing variability. effective duration too short to well- identify sources varying like quasars. Here the thirteenth meeting being held in other institutions, Variability time scales led to some of the constrain the variability parameters of the contamination comes from irregularly June 2011, again with AAO sponsorship. including ANU, first crude constraints on the sizes of individual quasars. There are, however, varying massive stars, but most of the Between these two gatherings, RAVErs Johns Hopkins and AGN at all wavelengths. However, since quasars with extremely well-sampled quasar parameter range differs from that met in Ljubljana, Strasbourg, Baltimore, the University of few quasars were well monitored, studies light curves – any quasars lying in the of the stars, as we showed in Kozlowski Padua and Groningen. Who says Ljubljana. Other focused on the statistical variability of fields monitored by the microlensing et al. (2010). In both cases, you can Coonabarabran can’t mix it with the big centres involved large numbers of sparsely monitored surveys of the define selection criteria that produce league? in the project are quasars as a function of time scale. The high purities at the price of reduced www.rave-survey.iap.de/rave Magellanic Clouds and the Galactic l’Observatoire largest analyses used tens of thousands completeness. The 2005 meeting was held on the eve of Galactocentric projection showing data from bulge. The OGLE survey, for example, astrophysique de of SDSS quasars, finding that quasar RAVE taking over all available time on the the current RAVE internal catalogue (approx. currently contains 15-year-long When you go to plan your AAOmega Strasbourg, the Open University, and 420,000 stars), colour-coded for radial velocity in variability increases towards shorter UK Schmidt Telescope on a continuing continuously growing light curves observation, however, you realize you the universities of Cambridge, Central the range -50 km/s (blue) to +50 km/s (red). The optical wavelengths, lower luminosities user-pays basis. The project had been with ~1000 epochs for about 50 should simply forget about purity and aim Lancashire, Groningen, Heidelberg, reflex solar motion is hard to miss. [Credit: RAVE; and, probably, lower black hole masses running in pilot mode for two years, background image (c) 2000 Axel Mellinger.] million sources Oxford, Sydney and Victoria. (e.g., Van den Berk et al. 2004, de Vries and had already more than doubled the in the Magellanic et al. 2005). Detailed studies of individual number of previously measured stellar RAVE spectra cover the calcium triplet Clouds. For a serious quasars showed that they get bluer as radial velocities. By 2011, that number region, and include stars with 8

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The Integrated Photonic Spectrograph’s First Look at the Heart of the Scorpion Nick Cvetojevic (Macquarie University), Nemanja Jovanovic (Macquarie University/AAO), Joss Bland-Hawthorn (University of Sydney), Roger Haynes (Astrophysics Institute Potsdam), Mick Withford (Macquarie University), and Jon Lawrence (AAO/Macquarie University) to X-ray sources in the fields only comes contaminating stellar sources, mostly physics. They supply a dense network of to about 80 sources per square degree previously unidentified B(e) stars, YSOs reference points for improving the proper At around 2am on a cold, clear night in mid index, into a series of waveguides with a „„ mass production: by relying on compared to an expectation of roughly and PNe. The contamination and failure motion measurements, particularly May, light from the star Antares ended its constantly increasing length increment. mature lithographic fabrication 25 quasars per square degree with I<21 rates are high, but this was expected. since the motions of the Clouds are six hundred year journey by bouncing off The output of these grating waveguides techniques developed principally by mag. Since there is no point in leaving a We estimate that completing the current presently limited by the need to map out the AAT’s mirror and into an integrated interferes within a second free-propagation the telecommunication industry we fibre empty, you should just do everything, OGLE-III LMC and SMC fields would the internal motions of the Clouds. The photonic spectrograph, the first of its zone producing wavelength dispersion, and can ensure that instrument costs including objects starting to be a little yield a total of ~700 quasars, and that an brighter quasars can also be used for kind in the world. The first successful is focused on the output face as a spectrum are not completely overwhelmed faint for the planned observation times. additional 3600 quasars can be identified absorption line studies of the interstellar detection of a stellar spectrum by our (Figure 1b ). by technology development and In this “no fibre left behind” approach, in the OGLE-IV fields, ignoring any medium, where we have already photonic spectrograph, accompanied by demonstration costs. Furthermore, Four key factors outline the potential contamination is a feature, not a bug, and potential gains from obtaining the longer, identified 10 new quasars brighter than the popping of champagne bottles, was as the primary expense in AWG advantages of an integrated photonic it will identify many peculiar LMC sources planned integrations. While the samples I<18 mag. a major achievement for astrophotonic chip fabrication is the up-front approach over the traditional spectrograph as a by-product. would still be smaller than the ~9000 technology as well as bolstering the tooling cost, it becomes practical SDSS quasars we considered in MacLeod References: design, in particular for multi-object So far we have observed 4 AAOmega AAO’s prominence in new and innovative (if not preferable) to fabricate large et al. (2010), the longer and more densely spectroscopy: fields in the LMC and 1 in the SMC out of de Vries et al. 2005, AJ, 129, 615 instrumentation for astronomy. quantities; sampled OGLE light curves should let Giveon et al. 1999, MNRAS, 306, 637 „„ miniaturisation: the entire spectrograph 17 planned, mostly while fighting cyclone The power of astrophotonics to expand the „„ modularisation: by breaking the us examine the physical correlations of unit, including collimating and focusing Yasi and with only one field completed to Kozlowski & Kochanek 2009, ApJ, 701, 508 capabilities of astronomical instruments system into low-cost modular the variability parameters with a higher optics and the disperser, is contained the planned depth. In 5 hours on sky, we Kozlowski et al. 2010, ApJ, 708, 927 by exploiting photonic technologies has components, low-maintenance, accuracy, making it easier to determine in a single, silica chip a few centimetres observed 1100 candidates, finding 174 Kozlowski et al. 2011a, ApJS, 194, 22 been recently illustrated by a number readily-expandable instruments can the intrinsic parameter distributions wide and a few millimetres thick. With new quasars, quadrupling (doubling) the Kozlowski et al. 2010b, arXiv:1106.3110 of demonstration devices (see Bland- be constructed with a large number and their correlations with the physical such a significant reduction in size, number known behind the LMC (SMC). The MacLeod et al. 2010, ApJ, 721, 1014 Hawthorn & Kern 2009). The Integrated of elements. properties of the quasars. very large multiplexing capacity (e.g., quasar samples are roughly 80% complete Peterson 1993, PASP, 105, 247 Photonic Spectrograph (IPS), essentially more than a hundred thousand spatial The IPS was initially demonstrated for I<19.2 mag, and the completeness then These quasars have additional uses Van den Berk et al. 2004, ApJ, 601, 692 a complete spectrograph on a single elements) becomes feasible; on-sky at the AAT with an observation drops. There are a comparable number of beyond studies of quasar variability photonic chip, is one such device (Figure of the emission spectrum of OH from 1a). While several alternative technologies „„ integration: with all the components of the atmosphere (Cvetojevic et al. 2009). for miniature astronomical spectrographs a classic spectrograph integrated on a For that initial test, the IPS device was have been proposed (e.g., Watson 1996, single chip, we diminish the impact of not interfaced to the telescope but was Bland-Hawthorn & Horton 2006), we problems such as alignment, stability simply collecting the light directly from have concentrated on the planar arrayed- and flexure which often add complexity the sky. The next logical step was to build waveguide grating (AWG). In an AWG to instrument design. Moreover, it an instrument that can successfully take spectrometer (Smit & Van Dam 1996), light permits exciting new possibilities for the light from the AAT and observe a is coupled from an input fibre, through a space-based or high temperature- spectrum from an astronomical source. free-propagation zone of constant refractive fluctuating applications.

(a) (b)

Figure 2: The spectra of ten of the 145 new LMC AGNs from Kozlowski et al. (2010b). The spectra have been flattened, smoothed and scaled, and emission lines from the ISM of the LMC have been suppressed. Figure 1. Photograph of a single AWG chip in the IPS prototype (a). This device accepts input light from optical fibres and outputs a spectrum on its output polished face (b).

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Using AAOmega to measure the age of the young open cluster IC2602 Paul Dobbie (AAO), Nicolas Lodieu (IAC) and Rob Sharp (ANU)

On the 19th of May, we interfaced a new Open clusters consist of co-eval with greater overshoot leading to larger which is necessary to determine the IPS prototype with the AAT using an IFU populations of stars residing at similar cluster age estimates. Thus a method of location of the LDB, is extremely which fed a multimode fibre (a fibre with heliocentric distances, that have formed determining ages which is independent challenging. Indeed, despite the youth a 50 micron core) and in turn a photonic from molecular gas clouds with near of assumptions about the physics of the and proximity of IC2602, no low mass lantern. This is the same interface as uniform chemical compositions. The stellar core boundary is to be preferred. stellar or substellar members have been used by the GNOSIS OH-suppression common properties of their members reported prior to this study. Fortunately, We are fortunate that such a technique instrument. The photonic lantern acts as render them excellent targets for the difficulties above can be mitigated has been successfully demonstrated a multimode-to-single mode converter, addressing fundamental questions in to a large extent by undertaking the (Basri et al. 1996). It relies on locating allowing our diffraction-limited IPS stellar astrophysics. For example, they follow-up observations with a high gain, the boundary, in terms of mass, at which (inherently single-moded) to collect are frequently utilised to investigate the multi-object spectrograph which has a the element Li re-appears in the spectral the light propagating down the fibres. forms of the stellar/substellar initial wide field-of-view i.e. AAOmega. Here energy distributions of the completely Furthermore, we modified the IPS to mass function (e.g. Moraux et al. 2005; we briefly describe our recent work on convective very-low-mass stellar and simultaneously input twelve single-mode Lodieu et al. 2009) and the stellar initial IC2602 aimed at securing a LDB age for substellar members of a population fibres, thus increasing our observational Figure 2. The raw spectrum of Antares from IRIS2 showing the cross-dispersed output of the IPS. mass-final mass relation (e.g. Williams this population. (Rebolo et al. 1992). As a population efficiency by an order of magnitude. The The spectra from each of the twelve fibres is seen running diagonally, which is further separated into et al. 2004; Kalirai et al. 2005; Dobbie different orders of the IPS. IPS chips have a throughput of ~80% et al. 2009). Open cluster members are matures, up to 300Myr, the location of The initial identification of and a typical resolving power of R=7000. also frequently used to probe stellar this Li depletion boundary (LDB) migrates candidate low mass cluster The output face of the chips was imaged magnetism (e.g. Marsden et al. 2005), the to lower mass (corresponding to later members onto the IRIS2 detector, which we used in spectral types), providing a potentially evolution of stellar angular momentum We retrieved I band imaging for ~1.4 spectroscopic mode as a cross disperser (e.g. Irwin et al. 2009) and the mixing excellent handle on the age (D’Antona & for the astronomic H-Band (1480- (a) Mazzitelli 1994). However, the draw back square degrees towards IC2602 from the processes which occur within stars (e.g. European Southern Observatory’s (ESO) 1825nm), in which we were observing. Pinsonneault 1997). of this approach is that it is reliant on the availability of moderate signal-to-noise, data archive. This had been obtained The first spectrum of the night was of Critical to the success of many of these medium resolution optical spectroscopy with the 2.2m telescope and the Wide Antares ( Scorpii) as it was the brightest types of investigation is the availability of intrinsically faint red objects. Hence, Field Imager (WFI, Baade et al. 1999) sky up at the time, and served as a of a reliable age determination for the prior to this work there were only five during February 2001. These datasets calibrationα source for final alignment population under scrutiny. This allows young open clusters with LDB based age were processed and calibrated using adjustments (Figure 2). With a world-first meaningful comparisons to be drawn determinations. the Cambridge Astronomical Survey under our belts, we continued to observe (b) between the measured properties of Unit’s CCD reduction toolkit (Irwin & a Be star (alf Ara) (Figure 3a) and V* Pi 01 the members of different clusters and With the commencement of the operation Lewis 2001). The optical detections were Gru, a cold red giant (Figure 3b), as they aids in the judicious interpretation of the of near-IR survey instruments such as cross correlated with the Two Micron would hopefully contain more interesting observed trends in the theoretical context VISTA, which are capable of probing All-Sky Survey (2MASS, Skrutskie et al. spectral features in the H-band. (e.g. the variation of Li abundance in the sequences of young, nearby stellar 2006) point source catalogue to obtain This demonstration is, to our knowledge, stars of different effective temperatures populations down to planetary masses, corresponding J and K band magnitudes the first time a photonic spectrograph as a function of age; Randich et al. it is desirable to expand the set of for the brighter sources. Subsequently, southern open clusters for which LDB has successfully taken spectra of a Figure 3. a)The raw spectrum of alf Ara, a Be star. b)The raw spectrum of V* Pi 01 Gru, a cold red giant. 2001). In general, age estimates for these data were used to construct an source beyond the Earth, and the first open clusters are obtained using the ages are available so that these data I-J,J colour-magnitude for objects time such a device was interfaced to a main sequence turn-off technique sets can be fully exploited. The nearby classified as stellar, towards the cluster. telescope. With the success of the new (MSTO), where the observed location (d=150-170pc e.g. Braes 1961, van As our guide to the likely location of the Leeuwen 2009) pre-main-sequence prototype, we have shown the practicality References in the luminosity-temperature plane of cluster sequence we used a selection of such a device for astronomy. Further stars at the end of their main sequence population, IC2602 is potentially one of of low mass stellar members of the F.G. Watson, (ed. S.C.Barden), Proc.S.P.I.E., 2476, 68–74, 1995. work on the IPS continues with potential life is compared to the predictions of the most astrophysically interesting of Pleiades for which I and J photometry interfacing with adaptive-optics aided Bland-Hawthorn, J., & Horton, A., Proc. SPIE, 6269, 62690N, 2006 stellar evolutionary models (Meynet, these targets. Currently, it’s age, which are available in the literature (Stauffer et telescopes, and a large redesign and Bland-Hawthorn, J., & Kern, P., Opt. Exp., 17, 1880, 2009 Mermilliod & Maeder 1993). However, is estimated to lie in the range t~30–70 al. 1994, 1998). The photometry of these fabrication of new AWG chips more Cvetojevic, N., Lawrence, J.S., Ellis, S.C., Bland-Hawthorn, J., Haynes, R., & for all but the oldest populations Myr (e.g. Kharchenko et al. 2005), is Pleiades objects was shifted (from an Horton, A., Opt. Exp., 17, 18643, 2009 ideally suited for astronomy. While still a these age estimates are muddied by rather poorly determined. As this cluster assumed d=135pc; Pan et al. 2004) to the long way from becoming a fully-fledged Smit, M.K., & Van Dam, C., IEEE J. Sel. Topics Quantum Electron., 2, 236, 1996 uncertainties associated with the extra is located close to the Galactic plane new Hipparcos distance of IC2602 and instrument, the recent successes make convective mixing which is believed (b=–4.9˚) and spread over several square adjusted by 0.45 magnitudes to larger our ambition of having a spectrograph for to occur at the boundary between the degrees of sky, it is rather difficult to luminosities (based on the predictions of astronomy that you can fit in your hand, cores of stars and the overlying layers distinguish members from reddened evolutionary models for low mass stars) seem very bright indeed. (Woo & Demarque 2001). The degree of background field stars via photometric to account for the expected lower age of convective core overshooting adopted surveys. Therefore, assembling a this cluster (i.e. ~50Myr). Based on the in stellar evolutionary models impacts reasonably clean list of faint candidate minimum and maximum nuclear age both the predicted main sequence members for the (traditional) long- estimates for IC2602 in the literature, lifetimes and the luminosities of stars, slit spectroscopic follow-up program, we estimated the probable location

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of the LDB to be J~13.2-15.5 mag stars, which are known to be a major We also measured the radial velocities Astrometry using 2dF’s Focal together very close to the location of 1997; Pinfield et al. 2003). Of course, (corresponding to mid-M spectral types). issue for photometric studies of this of our 17 candidate low mass candidates Plane Imager known bright cluster stars, supporting with the available data were unable We initially selected all sources within cluster (e.g. Foster et al. 1997). To using the SPLOT routine in IRAF to fit a our conclusion that these are members to exclude the possibility that these As one final probe of cluster membership these magnitude limits and on or to the assess more quantitatively the spectral Voigt profile to the observed H lines. of IC2602. An additional source, 2MASS are simply young field star interlopers status, we determined the relative proper red of the line defined loosely by the types of the 17 remaining candidates we The members of a star cluster display J10432126−6419594, lies well away from but their spectral classifications are motions of a number of candidates using Pleiades objects as candidate members computed spectral indices based on the only a small dispersion (delta vα<1kms−1) the four other objects but we had earlier consistent with the binary hypothesis. Li r the ESO WFI data and frames acquired of the cluster. After visually inspecting strengths of the TiO and CaH bands (TiO5, about the cluster mean value. Indeed, discounted it on the basis of spectral type was positively detected in the spectra of with the Focal Plane Imager (FPI) of these sources to weed out blended stars, CaH1, CaH2, and CaH3; Reid et al. 1995; Marsden et al. (2009) recently determined and radial velocity. all four candidate members fainter than the AAOmega spectrograph. The FPI we were left with 249 for spectroscopic Cruz & Reid 2002) which are present in v =17.4±1.0kms−1 from a high-resolution 2MASS J10430890−6356228 which has r is an Apogee imaging camera which is follow-up. the wavelength range covered by our study of solar type cluster members. J=14.04±0.03 mag (K =13.17±0.04 mag). mounted in front of the skyward facing S AAOmega observations. As an additional We estimated the uncertainties in our field plate of 2dF. It contains a 512×512 The brightest Li rich candidate with a check we also compared all the spectra −1 Multi-object spectroscopy of measurements to be ~7kms based pixel Kodak KAF-0261E CCD and has position in the colour-magnitude diagram to each other in order to define a spectral candidate low mass members of on the dispersion seen in the radial a field of view of 2.6’×2.6’. We acquired which was found to be consistent with the sequence and then matched them to IC2602 velocities determined from each of the 3×10s exposures through a RG630 single star sequence defined by the other low resolution spectroscopic templates We used the AAOmega + 2dF facility four unstacked spectra of a subsample filter for 2MASS J10422712−6421401, members is 2MASS J10439236−6402132 of the young M3–M6 dwarfs members (Sharp et al. 2006, Lewis et al. 2002) at of the candidates. We verified their 2MASS J10420463−6434373, which has J=14.25±0.05 mag of the Chamaeleontis region (Luhman internal accuracy by using the IRAF (K =13.30±0.04 mag). Following Manzi et the Anglo-Australian Telescope for a 2MASS J10430890−6356228, 2MASS S 2004; Luhman & Steeghs 2004). We found mere 2 hours during February 2010 to FXCOR routine to estimate the radial J10430236−6402132 and 2MASS al. (2008), on the basis of the photometry our objects to lie within the range M3.0 obtain medium resolution spectroscopy velocities of each targets with respect to J10432126−6419594 in the twilight prior of these two objects we concluded that to M5.5. While a substantial proportion of 219 of our 249 candidate members 2MASS J10430236−6402132, the brightest to the regular AAOmega observing the LDB of IC2602 lies within the range of field stars of these spectral types object in our sample. We found a broad J=14.01–14.30 mag. (K =13.13–13.34 of IC2602. These observations were nights during May 2010. On these S display H emission, scrutiny of the large performed using the 1000R grating on peak in the distribution of radial velocity evenings, the sky was clear and seeing mag), allowing for the uncertainties in the spectroscopic sample studied by West et −1 the red arm to cover the wavelength measurements centered around 15kms . was substantially better than the Siding 2MASS photometry. Spectroscopy around al. (2008) αsuggests that only 15-20% of range 6200-7300angstroms, within which This likely corresponds to the cluster Spring median value (i.e. 0.9-1.2”). We the 6707.8 Å line for the four objects M4/M5 dwarfs within 50pc of the Galactic the resonance line of Li is located. Our population. We chose to select as radial reduced the images following standard closest to either side of the LDB is shown plane should be expected to have H velocity members those objects which in Figure 3. science observations were bracketed procedures within the IRAF software Figure 2: The vector point plot of the relative equivalent widths <−6°A. Since our were within 2 of the recent Marsden by fiber-flat and arc calibration frames. environment, namely bias and dark proper motions of several candidate members We used the derived M and M spectroscopic investigation unearthedα et al. (2009) measurement i.e. v =3.4- of IC2602 (black triangles with error bars). J K Simultaneous observations were obtained r subtraction, flat fielding, astrometric magnitudes of the LDB and the a total of 16 M4/M5 dwarfs, we found 31.4kms−1. Thisσ led to the rejection of a Overplotted are the UCAC3 proper motions with the 580V grating on the blue arm calibration and co-addition. theoretical near-IR photometry of that relative to the field population our further three sources that as it turned of known bright cluster members (grey open but these are not relevant to this study. circles). The relative proper motions of other Baraffe et al. (1998) to estimate the age remaining sample contained a significant out, had by at least 1.5 subclasses, the We used the IRAF routine DAOFIND to The red arm data were processed using objects within the FPI fields are also shown for IC 2602. To derive these absolute excess (10) of these strong H emitting earliest spectral types (all are M3.0). determine the positions of reference a slightly modified procedure to the (small dots). magnitudes we adopted a distance objects. Many of these sources were Up to this point our combined selection objects of comparable or greater standard reduction implemented by modulus of (m-M) =5.86±0.1, which is found to lie on a relatively tightα sequence criteria should have rejected almost 80- brightness to our candidates in the 0 2DFDR. Due to the presence of weak based on the most recent Hipparcos in the I-J, J colour-magnitude diagram, 90% of mid-M field stars. If the remaining two images. We cross-matched these The LDB and the age of IC2602 but slowly spatially variable H emission determination and is consistent with bracketed by 20Myr and 50Myr old sample of 14 candidates was in fact lists of positions using the STARLINK across our AAOmega field-of-view we We examined the spectra of the 14 the majority of other distance estimates α theoretical isochrones (Figure 1). dominated by field dwarfs (as opposed TOPCAT software. Subsequently, we used a median of the background counts remaining candidate members of IC2602 in the literature (Whiteoak 1961; Braes to cluster members) then, in our entire employed routines in the STARLINK from the closest ~8 sky fibres to each for the presence of the 6707.8 angstrom 1961; Robichon et al. 1999; van Leeuwen science fiber to obtain an estimate of spectroscopic sample we should have SLALIB library to construct a six co- Li absorption line. Compelling evidence 2009). We assumed reddening of AJ=0.03 the night sky spectrum. An analysis of unearthed ~80 objects of mid-M spectral efficient linear transform between the of this feature was found in the spectra of and AK=0.01 based on E(B-V)=0.035 the residuals in each of the sky fibres type. two images of each candidate, where six objects. We used the SPLOT routine in (Hill & Perry 1969) and AJ /E(B-V )=0.86 showed a noticeable improvement to the >3 outliers were iteratively clipped IRAF to measure the equivalent width of and AK/E(B-V )=0.36 (Fitzpatrick 1999). background subtraction accuracy using from the fits. The proper motion, in the line in these six spectra and also to pixels,Σ was determined by taking the We also considered the finite depth this approach. set upper limits on the equivalent width in of the cluster since it is effectively a difference between the observed and the remaining datasets where there is no Out of the total of 219 objects observed further uncertainty on the distance to Figure 1: The I−J,J colour-magnitude plot of predicted location of a candidate in convincing detection. Notably, we found spectroscopically we found only 22 had all point sources in the ESO WFI field-of-view each individual member. We estimated the 2nd epoch dataset. This was then two objects with clear detections of the Li energy distributions that resembled which have a 2MASS counterpart. As a guide that most low mass stars should lie converted into milli-arcseconds per year line that are substantially brighter than mid-M spectral types. As young very-low- to the location of the cluster sequence, a in right ascension and declination using within 4 pc of the cluster centre which selection of Pleiades low mass stars (open the four other Li rich candidates. The mass stars typically display strong (EW< corresponds to ±0.06 on the distance stars) and a NextGen theoretical isochrone the world co-ordinate system of the 1st location of these objects approximately −few angstroms, Barrado y Navascues modulus of individual members. Adding for 50Myr (dashed line), both shifted to the epoch imaging and dividing by the time +0.75 mag above the sequence defined et al. 2004) H emission, based on distance of IC2602 have been overplotted. the uncertainties in quadrature we found baseline between the two observations by the other spectroscopic members our by-eye inspection of the AAOmega Objects that were selected for spectroscopy are (9.23 years). The relative proper motion that the LDB in IC2602 occurs within the highlighted (large dots) as are spectroscopic could indicate that these two objects datasets, we αconditionally labelled as ranges MJ=8.03–8.49 mag and MK=7.17– members with (filled squares) and without vector point diagram for these objects are near equal mass binary stars. We candidate spectroscopic members 17 of 7.56 mag. These were compared to the (filled triangles) lithium in absorption at 6707.8 (triangles with error bars) is shown in could have expected to detect one or these 22 sources. The vast majority of angstroms 20Myr and 32Myr theoretical theoretical predictions of the Lyon group Figure 2. 2MASS J10422712−6421401, two binary members in a sample of the spectroscopically observed objects NextGen isochrones, adjusted as per the 50Myr 2MASS J10420463−6434373, 2MASS (Chabrier & Baraffe 1997; Baraffe et al. model, are also shown (solid and dot-dashed this size since the binary fraction of 1998) for M and M as a function of age, that we rejected appeared to be of K or J10430890−6356228 and 2MASS J K grey lines respectively). low mass field and open cluster stars very-early M spectral types and were at which 99% of a stars primordial Li has J10430236−6402132 appear clumped is estimated to be 30% (Leinert et al. presumed to be reddened background been burned (Figure 4). Based on these

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the more recent evolutionary models Kalirai J. S., Richer H. B., Reitzel D., Hansen B. M. S., of Girardi et al. (2000). However, their Rich R.M., Fahlman G. G., Gibson B. K., von Hippel T., 2005, ApJL, 618, L123 estimate is based on the location in the Making MANIFEST fibres for the Giant HR diagram of just two stars and should Kharchenko N. V., Piskunov A. E., R¨oser S., Schilbach E., Scholz R.-D., 2005, A&A, 438, 1163 also be taken in the context of their larger Magellan Telescope Leinert C., Henry T., Glindemann A., McCarthy Jr. D. age determination (75Myr) for the similar W., 1997, A&A, 325, 159 Matthew Colless, Guy Monnet, Julia Tims, Will Saunders, Andrew Hopkins, Jon cluster, IC2391 (also based on just two Lewis I. J., Cannon R. D., Taylor K., Glazebrook K., Lawrence, Jeroen Heijmans, Greg Smith, Lew Waller, Jurek Brzeski, James Gilbert, stars). Bailey J. A., Baldry I. K., Barton J. R., 16 co-authors Michael Goodwin, Scott Smedley, Scott Case, Rolf Muller (AAO) 2002, MNRAS, 333, 279 We found IC2602 to be consistent with the general trend delineated by the Lodieu N., Zapatero Osorio M. R., Rebolo R.,Mart´ın E. L., Hambly N. C., 2009, A&A, 505, 1115 Pleiades, -Per, IC2391 and NGC2457, The AAO is proposing a concept for compared to the other ELTs. Although instruments. MANIFEST expands the Luhman K. L., 2004, ApJ, 616, 1033 whereby the LDB age is 120-160% of the the Giant Magellan Telescope’s Facility GMT is the ELT with the smallest accessible parameter space and enhances Luhman K. L., Steeghs D., 2004, ApJ, 609, 917 estimatesα derived using more traditional Multi-Object Fibre System called aperture (A), it has the equal-largest field the long-term potentialities of GMT’s techniques. This trend is only currently Maeder A., Mermilliod J. C., 1981, A&A, 93, 136 MANIFEST, the Many Instrument Fibre of view (Ω). It cannot beat the other ELTs instrument suite. Manzi S., Randich S., deWitW. J., Palla F., 2008, A&A, System. MANIFEST is a fibre-feed at science where the figure of merit is the bucked by IC4665 where the MSTO age The AAO has now completed the 479, 141 system for GMT that offers access to primary mirror diameter (D) to powers determination (36Myr; Mermilliod 1981) MANIFEST Feasibility Study for GMT and Marsden S. C., Carter B. D., Donati J., 2009, MNRAS, larger fields of view, higher multiplex greater than unity (so-called Dn science). is larger than the LDB age by a factor 1.3 is currently carrying out a targeted R&D 399, 888 gains, versatile reformatting of the focal However it can dominate wide field and (see Manzi et al. 2008). program while awaiting the outcome of Marsden S. C., Waite I. A., Carter B. D., Donati J., 2005, plane via IFUs and image-slicers, and in survey astronomy (so-called AΩ science), the selection process for the GMT first- MNRAS, 359, 711 some cases higher spatial and spectral because the other ELTs are not making References light instruments, a decision on which is Mermilliod J. C., 1981, A&A, 97, 235 resolution. Coupled to the seeing- use of the full field of view delivered by Baade D., Meisenheimer K., Iwert O., Alonso J., Meynet G., Mermilliod J., Maeder A., 1993, A&AS, 98, expected early in 2012. Augusteijn T., Beletic J., Bellemann H., Benesch W., limited instruments GMACS, G-CLEF the telescope. 477 30 co-authors 1999, The Messenger, 95, 15 and NIRMOS, it provides qualitative and Moraux E., Bouvier J., Clarke C., 2005, Astronomische Enhanced functionality: MANIFEST Baraffe I., Chabrier G., Allard F., Hauschildt P. H., quantitative gains over each instrument’s Nachrichten, 326, 985 offers GMT spectrographs a wide range 1998, A&A, 337, 403 standalone capabilities in terms of both Oliveira J. M., Jeffries R. D., Devey C. R., Barrado y of enhanced functionality: (1) increased Barrado y Navascúes D., Stauffer J. R., Jayawardhana instrumental parameter space coverage Navascu´es D., Naylor T., Stauffer J. R., Totten E. J., fields of view; (2) multiple deployable R., 2004, ApJ, 614, 386 and scientific grasp and performance. 2003, MNRAS, 342, 651 IFUs; (3) increased resolution via Figure 3: AAOmega optical spectroscopy centered Basri G., Marcy G. W., Graham J. R., 1996, ApJ, 458, Pan X., Shao M., Kulkarni S. R., 2004, Nat, 427, 326 The top right figure shows a schematic around 6700 Å for seven probable members 600 image-slicing; (4) efficient detector Parker Q. A., Phillipps S., PierceM. J., HartleyM., diagram of the main elements of located closest to the LDB. The Li absorption line Braes L. L. E., 1961, Monthly Notes of the packing, both spectrally and spatially; Hambly N. C., Read M. A., MacGillivray H. T., 15 co- MANIFEST. at 6707.8 angstroms can be clearly seen in the Astronomical Society of South Africa, 20, 7 (5) efficiency gains from working at VPH top four datasets. authors 2005, MNRAS, 362, 689 Chabrier G., 2003, PASP, 115, 763 MANIFEST is not an instrument per se, super-blaze angles; (6) simultaneous Pinfield D. J., Dobbie P. D., Jameson R. F., Steele I. A., rather a generic telescope facility, like observations with multiple instruments; Chabrier G., Baraffe I., 1997, A&A, 327, 1039 Jones H. R. A., Katsiyannis A. C., 2003, MNRAS, 342, an adaptive optics adapter. Its Starbug (7) gravity-invariant spectrograph photometric bands we determined the Cruz K. L., Reid I. N., 2002, AJ, 123, 2828 1241 age of IC2602 to be 46(+6/-5) Myr. This system uses semi-autonomous probes mounting; and (8) OH suppression D’Antona F., Mazzitelli I., 1994, ApJS, 90, 467 Pinsonneault M., 1997, ARA&A, 35, 557 LDB derived age is larger by a factor 1.8 hanging down under a glass field plate in the NIR. Capabilities such as the Dobbie P. D., Napiwotzki R., Burleigh M. R., Williams Randich S., Pallavicini R.,Meola G., Stauffer J. R., than the age (25Myr; Stauffer et al. 1997) K. A., Sharp R., Barstow M. A., Casewell S. L., Hubeny Balachandran S. C., 2001, A&A, 372, 862 that hold and position optical fibres (see deployable IFUs, increased multiplex and obtained by comparing the position in I., 2009, MNRAS, 395, 2248 Reid I. N., Hawley S. L., Gizis J. E., 1995, AJ, 110, 1838 middle right figure). It allows hundreds increased resolution enable entirely new the HR diagram of the low mass cluster Fitzpatrick E. L., 1999, PASP, 111, 63 Robichon N., Arenou F.,Mermilliod J.-C., Turon C., of astronomical targets to be selected science with GMT; other functionality sequence to the predictions of the models Foster D. C., Byrne P. B., Hawley S. L., Rolleston W. R. 1999, A&A, 345, 471 over the full GMT Gregorian focal plane, offers efficiency gains ranging from of D’Antona & Mazzitelli (1994). It is also J., 1997, A&AS, 126, 81 Sharp R., Saunders W., Smith G., Churilov V., Correll redirecting the light to the slit entrances incremental (e.g. efficient detector greater by a factor 1.3 than the MSTO age 13. Girardi L., Bressan A., Bertelli G., Chiosi C., 2000, D., Dawson J., Farrel T., Frost G., Haynes R., Heald R., of the 3 GMT seeing-limited instruments packing and working at the superblaze of 35Myr determined by Mermilliod (1981) A&AS, 141, 371 Lankshear A., Mayfield D.,Waller L.,Whittard D., 2006, (NIRMOS, GMACS & G-CLEF). angle), to substantial (increased fields in Ground-based and Airborne Instrumentation for using stellar evolutionary models which Hill G., Perry C. L., 1969, AJ, 74, 1011 of view and simultaneous observations), Astronomy. Edited by McLean, Ian S.; Iye, Masanori. “Starbugs” are discrete stepping devices allow for modest levels of convective core to transformative (multi-IFUs and OH Irwin J., Aigrain S., Bouvier J., Hebb L., Hodgkin S., Proceedings of the SPIE, Volume 6269, pp. 62690G using two co-axial piezoceramic tubes overshoot (Maeder & Mermilliod 1981). Irwin M., Moraux E., 2009, MNRAS, 392, 1456 suppression). (2006). Vol. 6269 of Presented at the Society of Photo- joined at their top ends to produce a In contrast, Kharchenko et al. (2005) Irwin J., Hodgkin S., Aigrain S., Bouvier J., Hebb L., Optical Instrumentation Engineers (SPIE) Conference, ‘walking’ motion. The movement is Versatility: The MANIFEST concept determined a MSTO age of 67Myr using Irwin M., Moraux E., 2008, MNRAS, 384, 675 Performanceof AAOmega: the AAT multi-purpose fiber-fed spectrograph analogous to a one-legged person increases the versatility of GMT by Skrutskie M. F., Cutri R.M., Stiening R.,WeinbergM. D., operating a walking frame. Starbugs embodying three principles in its Schneider S., Carpenter J. M., 25 co-authors 2006, AJ, positioning is via a closed-loop control technical design – (1) selectability: 131, 1163 system with feedback via a high- instruments can work either in their Stauffer J. R., Hamilton D., Probst R. G., 1994, AJ, resolution camera located above the field native mode or with fibre feeds that 108, 155 plate. Each Starbug has a set of back- reformat the focal plane in a variety of Stauffer J. R., Hartmann L. W., Prosser C. F., Randich illuminated fibres used as metrology ways; (2) modularity: new instruments S., Balachandran S., Patten B. M., Simon T., Giampapa markers. The asymmetric distribution of can easily be accommodated by adding M., 1997, ApJ, 479, 776 these fibres allows determination of the new fibre modules; and (3) upgradeability: Stauffer J. R., Schild R., Barrado y Navascues D., Backman D. E., Angelova A. M., Kirkpatrick J. D., Starbug’s orientation without movement the system can provide new functionality Hambly N., Vanzi L., 1998a, ApJ, 504, 805 or calibration routines. The prototype via straightforward and relatively low Stauffer J. R., Schultz G., Kirkpatrick J. D., 1998b, system with 10 Starbugs is shown in the cost upgrades of the fibre modules. ApJL, 499, 219 bottom right figure. MANIFEST is not an instrument but rather an integrated telescope facility, van Leeuwen F., 2009, A&A, 497, 209 World-leading capabilities: MANIFEST is analogous to the adaptive optics systems Whiteoak J. B., 1961, MNRAS, 123, 245 not only a major force multiplier for GMT in providing broad scientific utility and Williams K. A., Bolte M., Koester D., 2004, ApJL, 615, instruments and science; it also provides Figure 4: Theoretical relationships between age and absolute J and KS magnitudes for a 99% level of L49 enhanced performance for a variety of Li depletion (Chabrier & Baraffe 1997; Baraffe et al. 1998). Our determination of the LDB in terms of GMT with world-leading capabilities Woo J., Demarque P., 2001, AJ, 122, 1602 magnitude and age is highlighted (dashed lines) as are our estimated uncertainties on this (dotted lines).

18 Australian Astronomical Observatory Newsletter - AUGUST 2011 Australian Astronomical Observatory Newsletter - AUGUST 2011 19 SCIENCE HIGHLIGHTS SCIENCE HIGHLIGHTS

analyses: a small blip (star burst) in star This article necessarily represents a M., Tegmark M., Bahcall N., Brinkmann J., 2005, ApJ, formation rate at a few Mpc away from very quick whip-around of our results, 624, 463 A Voyage Through FOG cluster centres (Porter et al. 2008). We largely derived from AAO data products Lewis I., et al., 2002, MNRAS, 334, 673 hypothesize that this starburst is caused —particularly redshift surveys conducted Pimbblet K. A., Smail I., Edge A. C., Kevin A. Pimbblet (Monash University) by first time harassment. with 2dF and AAOmega. It is a pleasure Couch W. J., O’Hely E., Zabludoff A. I., 2001, MNRAS, to thank the dedicated staff of the 327, 588 FOGs should also contain most of the observatory and colleagues in large- Pimbblet K. A., Drinkwater M. J., Hawkrigg M. C., mass of the Universe (Cen & Ostriker field surveys that made observational 2004, MNRAS, 354, L61 1999; Aragon-Calvo et al. 2010). Using research in to FOGs a very promising Pimbblet K. A., Edge A. C., Couch W. J., 2005, archival data and a knowledge of where MNRAS, 357, L45 avenue of investigation. FOGs reside (i.e. PDH), we searched Pimbblet K. A., 2005, PASA, 22, 136 for X-ray emission from filaments and Filaments of Galaxies (FOGs) have long trivial manner (Pimbblet et al. 2005). This The relative fractions of morphological REFERENCES Pimbblet K. A., Andernach H., Fishlock C. K., through a stacking process (carefully Roseboom I. G., Owers M. S., 2011, MNRAS, 410, 1837 been known about in the literature opened up a large number of questions types are found to be entirely consistent Aragon-Calvo M. A., van de Weygaert R., Jones B. J. avoiding known contaminants such as Porter S. C., Raychaudhury S., Pimbblet K. A., and discussed with a variety of mixed that included (but were not limited to): with predictions from models (Colberg T., 2010, MNRAS, 408, 2163 other galaxy clusters) combined with a Drinkwater M. J., 2008, MNRAS, 388, 1152 nomenclature (e.g. Walls, Sheets, what role filaments have in the growth of et al. 2005). However, the length of the Cen R., Ostriker J. P., 1999, ApJ, 514, 1 statistical background correction, derived Yaryura C. Y., Baugh C. M., Angulo R. E., 2011, Filaments), a famous early example being clusters that they inter-connect? What filaments can stretch from to tens, to an estimate for the electron density Colberg J. M., Krughoff K. S., Connolly A. J., 2005, MNRAS, 413, 1311 the CfA Great Wall (Geller & Huchra effect do FOGs have on the evolution of sometimes hundreds of Mpc which could MNRAS, 359, 272 inside FOGs at z~0.1 n = (4.7 ± 0.2) x 10-4 1989) and more recently the Sloan galaxies contained therein? Can they pose a problem for models (cf. Yaryura et e Colless M., et al., 2003, arXiv:astro-ph/0306581 h 1/2 cm-3 (Fraser-McKelvie et al. 2011). Great Wall (Gott et al. 2005; Pimbblet et be used as a cosmological probe to test al. 2011). 100 De Propris R., et al., 2002, MNRAS, 329, 87 This is, perhaps, a higher than expected al. 2011). Over recent years, there has theories of structure formation? If galaxies spend a lot of their lifespan density and may reflect the stacking & Fraser-McKelvie A., Pimbblet K. A., Lazendic J. S., been increased interest in FOGs from 2011, MNRAS, in press Using the final data release of the 2dF inside FOGs, flowing toward clusters background subtraction process and/ the ready availability of large-volume Geller M. J., Huchra J. P., 1989, Sci, 246, 897 Galaxy Redshift Survey (Colless et al. (see Pimbblet 2005), then presumably or the modelling of the X-ray count rate. redshift surveys N-body simulations (see 2003) coupled with a knowledge to the there could be some evolutionary Future work with new satellites such as Gomez P. L., et al., 2003, ApJ, 584, 210 Pimbblet 2005 for a general discussion). location of the galaxy clusters contained pre-processing occurring inside FOGs Suzaku should clarify this preliminary Gott J. R., III, Juric M., Schlegel D., Hoyle F., Vogeley My own interest in FOGs began during therein (De Propris et al. 2002), we before they ever encounter the hostile estimate. my PhD when I was undertaking undertook a systematic search for high-density cluster core regions. observations of rich galaxy clusters using inter-cluster filaments (Pimbblet et al. We know from Lewis et al. (2002) and a new spectrograph that was called 2004; PDH). PDH extracted all possible Gomez et al. (2003) that star formation 2dF (e.g., Pimbblet et al. 2001). Fig. 1 combinations of pairs of clusters within suppression starts to occur on a mass displays a plot of one of these clusters 10 degrees and cz<1000 km/s of each scale of galaxy groups. However those (Abell 22; Pimbblet et al. 2005) where other. This generated a sample of 805 studies considered a radially averaged in front of the cluster (z~0.14), there unique inter-clusterΔ areas which were (or density averaged) star-formation appears to be coherent “wall” of galaxies visually inspected for the presence of rate. Hence the detail of what happens in RA at lower redshift (z~0.11). This is FOGs. Each filament that was confirmed to galaxies inside filaments is «lost» in clearly not the same mass regime or in this manner was also given a the averaging process. If we consider physical dimensions as the classic Great morphological classification (straight, the star-formation rate as a function 1 Wall from CfA. However, we find that it curved, wall or sheet-like, complex) and of distance away from a galaxy cluster, Are You Biased? appears to connect up a set of distant a length (explicitly, the inter-cluster axis but only along a FOG vector, we find a Sarah Brough (AAO), Tanya Hill (Melbourne Planetarium), Amanda E. Bauer (AAO), galaxy cluster pairs together in non- regardless of morphology) was computed. result that was not seen in the previous Andrew Hopkins (AAO), Sarah Maddison (Swinburne University)

Picture this: you are running late for a If you feel ostracised by these comments astronomy at the mid-career level but meeting. You race down the corridor – well that’s the point isn’t it? It’s a basic the conclusions we drew have positive and there are two rooms to choose human desire to feel like we belong. But implications for many members of the from. One is full of blokes vigorously can you recognise your unconscious astronomy community. debating something, the other contains biases? Do you know how this affects a group of women animatedly discussing your interactions with people, especially Unconscious Bias something else. Which door would you in the workplace? Why is unconscious bias relevant? choose? This article follows from a recent In a non-gender balanced field like It’s a bit of a cliché, and there will be “Women in Astronomy” workshop astronomy, historically driven by senior plenty of exceptions, but, regardless organised by the Women in Astronomy men, unconscious bias leads to non- of the subject being discussed, a good Chapter of the Astronomical Society diversification which loses us the variety many of us would simply choose the of Australia (ASA) and sponsored by of opinion and thought processes that are door that contains those of the same the AAO, as well as the Centre for vital to research excellence. Unconscious gender as us. Even if the conversation All-sky ASTROphsyics (CAASTRO) and bias also means that people who are bores you crazy, at least among CSIRO Astrophysics and Space Science not part of the dominant group feel members of your own gender, you can (CASS). The aim of the workshop was ostracised and that their contributions mostly disappear into the background to investigate why many women leave are not respected. without too much fuss. Figure 1: Wedge plots of right ascension and declination versus redshift in the direction of Abell 22. The X-ray centre of the cluster is located at = = 0. Note the ensemble of galaxies in the foreground of the cluster. Although one may expect this plot to exhibit a ‘finger of god’ effect for the cluster, arising from the distorting effects in redshift space, this is not seen, as the elongation in redshift space of the αclusterδ is small in comparison to the depth of redshift space covered. 1 This article is based on the Women in Astronomy Workshop 2011 Report, available at http://asawomeninastronomy.org/meetings/wia2011/

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by the same length of time as the that they work part-time, all to compete. called pink tasks. These are tasks parental leave taken, researchers can get For researchers of this generation, our that need to be done on time and to a their research done and institutions can challenge is to make all these normal high standard, but where there is little get the research they employed someone and open to acceptance. Not hidden away. substantive development or increased to do! visibility for the person assigned the Imposter syndrome task. While these tasks are necessary, CSIRO (amongst others) has also when they are assigned to the same shown that flexible grants designed to Despite external evidence of their person over and over again, that encourage parents to return to research competence, individuals with imposter person is unlikely to advance. If you after parental leave are incredibly syndrome remain convinced that they are find yourself repeatedly taking these valuable, not just to the recipients but frauds and do not deserve the success tasks that do not drive your career the research community around them. they have achieved. Proof of personal forwards, you need to say no. The point Several recent workshops at CSIRO success is dismissed as luck, timing, is not to be liked, but to be respected. Astrophysics and Space Science have or as a result of deceiving others into been fully or partially funded by Ruby thinking they are more intelligent and An ongoing theme in the workshop Payne-Scott awards. competent than they believe themselves was that people who had asked for to be. Imposter syndrome affects dispensation or consideration or a For employees with children, there are everyone. As individuals we need to special case received it! Bear that in things that institutions can do to make Attendees at the recent Women in Astronomy Workshop. Image credit: Bryan Gaensler face this, stand up to it and then be mind: If you want something, you will themselves Family Friendly. They can empowered by overcoming it! Managers not get it without asking, so Ask! You make sure that important meetings need to be aware that their staff may never know what will happen if you are held between 10am and 2pm, and suffer from this and that they can help! We all find it easier to work with people spring to mind immediately for these appointment panels, recipients of awards ask. that meetings finish on time, as this For whatever reason, some people need with whom we have something in positions, but they are there. The more and numbers of invited talks will bring helps everyone be able to engage with a champion to help them apply for jobs, common. On this basic level, a male exposure given to women, the more they different views into play as decisions Summary their families. Surely that is their most promotions, or to ask a question in a manager (and they’re in the majority) will spring to mind, equally. are made for astronomy’s future, Very few career paths are actually important role in life?! Institutions also meeting. A good manager can do this but might choose to give a big job to a encouraging future diversity. ‘traditional’ and they do not need to There are unwritten rules for how we need to think seriously about ensuring additional mentoring is crucial. Having younger male colleague because he be. Take it for what it is. We should judge people based on gender. Men the availability of childcare close to a senior member of the community remembers the conversation they had Family vs Career not need to contort ourselves to fit and women will judge a strong man as work and at professional meetings, (male or female) providing advice and after a meeting about a shared interest in the ‘traditional’ path and should successful and want to work for them, This is a major cause of women leaving especially national meetings. The closer/ encouragement is vital no matter what footy, for example. Recognising that you never accept being told otherwise. while a strong woman is often seen to be astronomy at every level. For those of cheaper/easier the childcare, the more career stage you are at. Anything we might have a tendency do this is a good Whilst enjoying our varied careers, aggressive and not someone you would you who have not noticed, there is a researchers will return to work quicker can do, as a community to help people start. Then trying 50% of the time to go we need to accept the differences want to follow (Steinpreis et al. 1999). neat correlation between the age when and happier. Childcare at professional forge the links that result in mentoring outside your comfort sphere and offer the our colleagues bring to the table and When reading or writing reference letters people are beginning to get ongoing meetings means that more primary is essential. If your institution is small, job to someone else, who might be just use our understanding of the positive it is important to think carefully about positions and the biological deadline caregivers can participate in those there may be suitable external mentors as deserving but not having an obvious benefits of such diversity to help us the adjectives used. Madera et al. (2009) when women need to think very seriously meetings they may not have been able to from collaborative organisations, and common interest, will impact positively work together. Which is really what found that it is common for women to if they have not had children yet. Having attend otherwise. there are companies who can provide not only on the diversity of people this article is all about - creating be described in nurturing terms (happy, children means taking time off and being mentoring. working in astronomy, but the happiness As we continue to peer-review each environments where we all feel we contributes ...) and men in strong terms less research productive for a period of of those people. Everyone wants to be other’s grant, award or job applications, belong, can contribute and will be (go-getter, confident ... ) where generally time, making it even harder to get that we need to actively take into account Handy Hints for Individuals valued. elusive ongoing position. As a community respected. it is the strong terms that are sought career breaks (of all varieties), and Individuals need to recognise that what we need to recognize the existence of It is not clear whether the lack of women after by selection committees. non-100% research roles, when taking you say/do does not have to be perfect. References on committees, in invited talks, and this correlation and that we must have responsibility for such judgments. Also, This all sounds very negative but it is Do not think you need to know everything Madera, J. M., Hebl, M. R., Martin, R. C. (2009). appointment panels is forgetfulness or the flexibility and foresight to allow relatively easy to fix. Firstly, we all need in assessing candidates for job/grant and be 110% precise before you speak “Gender and Letters of Recommendation for unconscious bias, but it certainly does astronomers the opportunity to have a to be aware of our personal biases, applications, we should be asking for up. Your vocal contribution of substance Academia: Agentic and Communal Differences”, not help address the problem of diversity. career and a family. Institutions must J. Applied Psychology, 94, 1591 and think carefully before selecting best N years of publications, rather than IS valuable and IS necessary for you to Not only do these people make decisions not be penalised for having flexibility and committee members, recipients of previous N years, to account for those be noticed, heard, acknowledged and Steinpreis, R. E., Anders, K. A., Ritzke D. (1999). for the future of our community, the foresight and no colleague should have to “The Impact of Gender on the Review of the awards, invited talks or writing reference career breaks. appreciated. invitations, awards and committee choose “Family vs Career”. Curricula Vitae of Job Applicants and Tenure letters. Secondly, by stacking our Candidates: A National Empirical Study”, Sex membership also confer community Amazing researchers even in recent Recognise when you are being handed committees with women. Trying to For those researchers on fixed-term Roles, 41, 718 respect, necessary for grant applications times have had to “hide” the fact that a task that will not benefit your career, achieve 50% balance in committees, contracts, if their contracts are increased amongst much else. Women may not they have kids, have taken time off, or anecdotally given to women and hence

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Gemini Town Hall meeting Observational Techniques staff, together with data reduction tutorials. Details of the workshop are AUSGO Corner As part of the Gemini Observatory’s effort workshop available at http://www.aao.gov.au/AAO/ to engage with their user community on Stuart Ryder (Australian Gemini Office, AAO) From 30 Aug–2 Sep 2011 the AusGO AUSGO-AAO_Workshop/ a regular basis, Associate Director for and AAT Science Workgroups will run Operations Dr Andy Adamson followed an optical/IR observational techniques Gemini e-newscast up his visit to Australia last September workshop in Sydney. This is the first with a Gemini “Town Hall” meeting time such a workshop has been run by To help stay in touch with recent held in conjunction with the ASA ASM the AAO for a decade; the early level of developments, announcements, and in Adelaide. He provided an update on interest in attendance by students and news releases, why not subscribe the status of the Gemini Observatory, even postdocs highlights that such a to Gemini’s e-newscast service? To Proposal Statistics Gemini High-resolution While initial results are promising, much including recent changes in management workshop is long overdue. Presentations subscribe to the list, send a message to work remains to be done to tune the full and a review of developments in the on all aspects of imaging, photometry, [email protected] with a subject of For Semester 2011B ATAC received a Optical Spectrograph system and the many control loops which “transition plan” for the observatory and spectroscopy available on the wide “subscribe Gemini-eNewscast” (without total of 34 Gemini proposals, of which 21 On 6 May 2011, the Gemini Observatory must operate to correct for atmospheric as they move into the final year of variety of instrumentation offered on the the quotation marks). Previous issues were for time on Gemini North, 4 were issued a Request for Proposals for turbulence across the full field of view UK membership. The instrument AAT, Gemini, and Magellan will be given can be accessed at http://www.gemini. for exchange time on Keck or Subaru, Conceptual Design Studies for a Gemini (unlike ALTAIR on Gemini North, for development program was also reviewed, primarily by AAO and Gemini Observatory edu/enewscast. and 9 were for time on Gemini South. High-resolution Optical Spectrograph which the correction deteriorates going followed by a Q&A session afterwards. The overall oversubscription (1.81) was (GHOS). A team led by Dr Michael Ireland radially outward from the natural or up on 2011A, although Gemini South from AAO/Macquarie University with laser guide star). The image shown here was barely oversubscribed. At the ITAC involvement from AAO and RSAA, as well is an “engineering first light” image meeting Australia was able to schedule as KiwiStar Optics in New Zealand has from GeMS taken on 19 April 2011 and 24 programs into Bands 1–3 (half of submitted a bid for a concept design demonstrates that already the system which involved joint allocations with study, building upon the AAO’s experience can deliver remarkably uniform images other Gemini partners), and one more with the CYCLOPS image slicer and fibre- across most of the GSAOI field. A call in the expanded Poor Weather Queue. feed for UCLES, as well as HERMES for System Verification observations For Magellan we received 12 proposals, and the multi-object fibre positioner with GeMS is likely to be issued during resulting in the highest Magellan MANIFEST for GMT. Semester 2012B. oversubscription ever of 4.86, due in part to the availability of the new wide-field NIRI Replacement near-IR camera FourStar. Gemini School Astronomy With the commencement of the GHOS Contest In 2010B, all but one of the seven Band procurement, the Gemini Science Building on the success of the 2009 (IYA) 1 programs were completed or had Committee (GSC) is now turning its and 2010 Gemini School Astronomy insufficient Target of Opportunity (ToO) attention to the next Gemini instrument. Contests, AusGO is running a similar triggers; 4 of 6 Band 2 programs got 90% With concern growing about the contest in 2011 for high school students or more of their data or did not trigger reliability of NIRI, the GSC asked all to win one hour of time with GMOS- ToOs; while no Band 3 programs were National Gemini Offices to poll their user South allocated by ATAC in 2011A. The even started. While Australia used barely communities on their future needs and number of entries was up by 20% on half its allocated time in 2010B, nearly desired capabilities for near-infrared 2010. The winning entry was submitted by 80% of that time went to programs that imaging on Gemini North. AusGO ran Benjamin Reynolds from the Sutherland were completed. a survey for the Australian community, Shire Christian School (NSW), to observe with results forwarded to the GSC on 8 the barred spiral galaxy NGC 7552 June. Our findings were that: (a) only 20% Magellan and Gemini travel with its nuclear star-forming ring. The support an L’ & M band capability for a funding two runners-up were Ryan Soars from replacement instrument; (b) two-thirds The ANSTO-administered Access to Trinity College (WA) who suggested the see no need for a spectroscopic or other Major Research Facilities Program YSO NGC 6729, and students from St additional modes in any replacement; (c) (AMRFP) which has supported travel to Margaret’s Anglican Girls School (QLD) about half plan to use NIRI in “wide-field” overseas observatories for a number of who suggested “Burbidge’s Chain” of (2’) or Adaptive Optics mode in coming years finished in June 2011. AusGO and galaxies. Observations for the winning years; (d) 87% are fully or mostly satisfied AAL approached DIISR with a request entry are now in the Gemini South queue with current NIRI performance; and (e) to use some uncommitted travel funds awaiting observation. about half feel that NICI could substitute from the National Collaborative Research for NIRI if need be. The images for the two previous winners Infrastructure Strategy (NCRIS) to cover have been incorporated into A3-sized Magellan observer travel in Semester posters promoting the contest, Gemini, 2011B, which DIISR approved as a one-off GeMS First Light the AAO, and AAL. These were distributed gesture and not a precedent. However The Gemini Multi-Conjugate Adaptive at the ASA Annual Scientific Meeting with NCRIS itself also finishing in 2011, Optics System (GeMS) consisting of the in Adelaide and are freely available for the AAO and AAL are actively exploring Canopus optical bench; a 50 W laser outreach purposes. options to ensure that users who are to produce a “constellation” of 5 laser fortunate to be awarded classical time on guide stars over an 85” field; and the Magellan, Gemini, or Gemini exchange RSAA-built Gemini South Adaptive Optics time on Subaru or Keck are actually able Imager (GSAOI) has been undergoing Figure 1: “First light” image obtained with GeMS and GSAOI on Gemini South at a wavelength of 2.12 microns. Strehl ratio and full- to take up that opportunity. commissioning in 5 night blocks each month throughout Semester 2011A. width at half-maximum values for all stars are shown in the insets. The poorer image quality on the left edge is expected, as these stars are outside the constellation defined by the three bright stars in the right half used to provide the tip-tilt correction.

24 Australian Astronomical Observatory Newsletter - AUGUST 2011 Australian Astronomical Observatory Newsletter - AUGUST 2011 25 OBSERVATORY NEWS OBSERVATORY NEWS

We were advised not to lecture, information We were fortunate to be able to attend Supernovae and their Host Galaxies Scientist Meets dump, whinge about funding, offer mixed new Chief Scientist Professor Ian Chubb’s messages or have nothing to say. Also that first National Press Club Address. This Sydney, Australia, 20-24 June 2011 we should be careful about how uncertainty was fascinating, as well as being the best Parliament is communicated, as ‘almost certain’ is not meal of the two days. Professor Chubb Chris Lidman (AAO) Sarah Brough (AAO) really understood. It was emphasised that reiterated the ‘Respect the Science’ preparation on our part is key - to research and peer review process message that our assigned minister and their interests underpinned this meeting. He also - and that “what excites a teenager will showed his experience in expertly handling excite a parliamentarian”. questions from journalists. It is clear that he will take the science agenda to The end of Day 1 was the dinner in During a marvellously sunny week at A wide range of topics were covered at wines, including one of his own, from I was invited to attend the 2011 Science parliament. the end of June (as can be verified by the conference: from the progenitors Australia and New Zealand, we got to Meets Parliament in Canberra in June Parliament House. Sadly several politicians From the Press Club we sat in the the group photo), 150 astronomers from of core-collapse and thermonuclear see Saturn through telescopes at the this year as the representative of the were unable to attend so there was no parliamentarian at our table. Over dinner Public Gallery of the National House of all parts of the world came to Sydney supernovae to the influence that Sydney Observatory that were probably Astronomical Society of Australia (ASA), Former Victorian Premier John Brumby, Representatives to watch Question Time. to talk about supernovae and their host supernovae have on the properties of older than any of the participants, and we along with several other astronomers from gave an overview of science funding This was also fascinating with The Speaker galaxies. The week long conference was their hosts and visa-versa. Of special enjoyed some nice views and nice food at around Australia. The event is organised by during his years in the Victorian Labor of the House introducing the Science held at the Australian National Maritime interest to the author of these lines the conference dinner at Doltone House. Science & Technology Australia (formerly the Federation of Australian Scientific and government. Followed by FASTS President Meets Parliament delegates to the House, Museum in Darling Harbour, and was the are the new types of supernovae being The conference would not have been Technological Societies; FASTS) to give Cathy Foley introducing the ‘Respect the resulting in a wave from Prime Minister fourth conference in the Southern Cross discovered by the current wide-field possible without the dedicated work scientists the opportunity to meet Federal Science’ video and the new name for Julia Gillard (we all waved back). Astrophysics Conference Series, which transient surveys. We also heard about of the local and scientific organising politicians and discuss science issues with FASTS: Science & Technology, Australia. is jointly sponsored and organised by the future new surveys for transients, committees, the members of which are My meeting with Senator Chris Evans, them. In preparation for that meeting we AAO and CASS. including surveys for transients at radio listed below, and to the many people The second day started early with a Minister for Tertiary Education, Skills, Jobs also had a day of training in communicating wavelengths. There was also a special who helped at the conference: Robert breakfast briefing on the Excellence in and Workplace Relations, was scheduled The conference started with a public science to the media, general public and session on SN 2011dh, a supernova that Barone-Nugent, Erica Rosenblum, Research for Australia (ERA) process shortly after the formal end of the day. talk given by Prof. Robert Kirshner politicians. was discovered in the Whirlpool Galaxy Philippa Morley, Janine Myszka, Stacey- from Professor Margaret Sheil, CEO of John O’Byrne (University of Sydney), two at the Powerhouse Museum. Prof. the Australian Research Council. It was other scientists and I went to meet the (M51) just a couple of weeks before the Jo Dyas, Billy Robbins, Kitty Lo, Jason The event started with the launch of the Kirshner captivated the audience with his interesting to hear the reasoning for having Senator. As he was still speaking in the start of the conference. Spyromilio, and Amanda Bauer. On behalf ‘Respect the Science’ campaign to explain description how astronomers uncovered of the participants, I thank all of you. A to the general public how the scientific and the ERA process, the acknowledgement Senate we ended up meeting with one of what is now considered one of the biggest Even though the scientific program was very special word of thanks goes out to peer review processes weight information that the choice of assessment metric his advisors, Andrew Dempster. Luckily I unsolved mysteries of physics - the very active, there was time for social Vanessa Bugueno, Angel Lopez-Sanchez, from scientists, against those whose words drives behaviour so has to be thought was well-prepared by the previous day’s reason why the expansion of the Universe activities. Brian Schmidt hosted a wine and Paul Hancock for the great work have not gone through those processes. through, as well as some of the outcomes presentations and I spoke quickly on the is accelerating. His talk also reminded tasting event at the Museum, where that they did before, during and after the Followed by a presentation on the current and the improvements that are being value of Square Kilometre Array (SKA) some of us that doing science is fun. we were able to sample a range of conference. political climate, informing us that it is very, implemented for the next round in 2012. to galaxy research and broader issues such as enthusiasm in science, jobs and very local, and very hard to get a mention in Following the breakfast briefing the technological skills with processing of such between the current ‘BIG’ issues. imminent closure of Canberra airport The Scientific Organising huge quantities of data. I was impressed due to the Chilean volcano ash cloud Committee: We had a ‘Meet the Press’ session with by Mr Dempster’s awareness of the SKA. political reporters from the parliamentary caused a brief hiatus as everyone tried to Alex Filippenko, Claes press gallery helping us understand make new arrangements for travel and I greatly enjoyed myself at Science Meets Fransson, Bryan Gaensler, how to get our science into the general accommodation. Parliament and found meeting so many Andy Howell (co-chair), other scientists very valuable. I would media. Some of the messages I took away Our second presentation of the day was Rubina Kotak, Chris Lidman like to thank the ASA for sponsoring were, if you do have an interesting press from Senator Kim Carr, the Minister for (co-chair), Filippo Mannucci, me to attend and Science & Technology release, send it out before the release day Innovation, Industry, Science and Research. Seppo Mattila, Ken’ichi Australia for organising the event. I to a targeted journalist so that they have He gave a very good, impassioned speech Nomoto, Giuliano Pignata, would definitely recommend it to anyone the ‘hint of exclusivity’ as that will help about the value of science evidence-based Brian Schmidt, Alicia interested in science communication or the you get coverage. Also that pictures are policy and the new ‘Respect the Science’ Soderberg parliamentary process. appreciated, as well as, if possible, case campaign. The Local Organising studies to humanise the story (although I’m not sure this is applicable to astronomy). Committee: Foyer of new Robert Braun, Ricardo After lunch each person prepared and Parliament House before Dinner Covarrubias, Paul Dobbie, presented a 45s piece on our research (in - John O’Byrne Andrew Hopkins, Chris less than the time it takes a sparkler to (centre),Sarah Lidman (chair), Angel burn). This turned out to be a very valuable Brough (right). R. Lopez-Sanchez, Tara exercise prior to our meeting the politician Image credit: Murphy, Quentin Parker, on the second day. Lorna Sim / Science & Stuart Ryder, Helen Sim, In the afternoon we had presentations on Technology Max Spolaor Australia how to convey our message to politicians. We were informed to leave plenty of time for small talk, to be able to think up good Conference Group Photo stories with our science, and come up with verbal pictures to connect large numbers to reality, to go in to have a conversation in their language (emphasising what is important to them) and form a relationship.

26 Australian Astronomical Observatory Newsletter - AUGUST 2011 Australian Astronomical Observatory Newsletter - AUGUST 2011 27 LOCAL NEWS LOCAL NEWS

between institutes. Her undergraduate Chris Lidman to identify white dwarfs in the Faustine Cantalloube is an optics Epping News studies were at University College London deep field images from the Canada France engineer masters student at the where she recently obtained a Natural Hawaii Telescope Legacy Survey. These may “Institut d’Optique, Graduate school” Sarah Brough (AAO) Science MSci. Stacey-Jo’s final year project ultimately serve as high fidelity calibrators in France (in partnership with the investigated the impact of image quality on for the studies which use these datasets. Paris-11 University, Orsay). Faustine is cosmological measurements for the Dark Janine enjoys observing the Coriolis effect working at the AAO for eleven weeks in Energy Survey. In October, she begins in her everyday life and hopes she doesn’t the astronomical instrumentation field. work on her doctorate at the Institute of meet a funnel web spider during her stay. Her project is to build an experimental Astronomy, University of Cambridge. Stacey- Erica Rosenblum, grew up and went set-up which could verify the liquid Jo has previously held summer research to school in New York State, USA. She atmospheric dispersion compensator placements with the Royal Astronomical recently received her bachelor’s degree in (LADC) concept. Faustine will therefore Two members of AAO staff have won directly from his thesis, which was also at the AAO following Sam Barden’s Society (2010) and the European Southern Physics from Stony Brook University and investigate the subject and performing annual prizes announced by the awarded an internal prize for best PhD departure. We wish him a quiet Observatory (2009). Astronomical Society of Australia (ASA) thesis at Swinburne University. retirement from now on. is looking forward to working in New York simulations with the Zemax software recently: Janine Myszka has just finished her third City in the fall. Here at the AAO, Erica is to check the consistency of her work. We congratulate them both! After 10 years at the AAO, Scott year as an undergraduate at Villanova working with Dr. Maritza Lara-Lopez on a She will also build and calibrate a Gayandhi De Silva has won the Louise Smedley has decided to move on and Sarah Brough (and that’s me so I will University in Philadelphia, Pennsylvania, project involving the relationships between compact optical layout in the AAO Webster prize. This prize is awarded in undertake a new challenge. For the continue in the first person) - I have where she is currently studying for her B.S. metallicity, star formation rate and stellar laboratory. This will enable future tests recognition of outstanding research by next phase of his career, he is going to accepted a new position within the AAO as in Astronomy & Astrophysics. She is working mass in galaxy pairs using the GAMA of the potential chemicals that can a scientist early in their post-doctoral be using his Linux/C++ skills developing a Research Astronomer for the next five under the tutelage of Dr. Paul Dobbie and Dr. (Galaxy and Mass Assembly) Database. play the role of a prism. career. Gayandhi’s award was based on trading systems in the Finance world. years. I will be continuing and developing the research she published establishing This will surely be very different to his my research with the Galaxy And Mass the viability of the chemical tagging past experiences! Assembly (GAMA) survey, Brightest Cluster technique and setting the stage for the Galaxies and Integral Field Spectroscopy We farewell-ed Denis Whittard who will Vale Tom Cragg (1927-2011) field of Galactic Archaeology: Detailed and hoping to combine the three in the be retiring, again, from the AAO after 23 chemical abundance patterns of stars Steve Lee (AAO) near future. I will also be taking on the years of service. offer the possibility to reconstruct some AAOmega Instrument Scientist role and I’ve always thought that Tom Cragg could best be described as a components of the protogalactic disk Max Spolaor is leaving after just a year seeing through the planned AAOmega professional amateur astronomer. Throughout most of his working and so improve our understanding of the as an AAO Research Fellow having refurbishment. life he had been able to mix his love of astronomy with earning a Galactic disk formation process. If star- taken on the AAOmega Instrument living. Tom was Chief Night Assistant at the AAT from 1976 until his forming aggregates can preserve unique We have two new faces in the Mechanical Scientist role and been responsible for retirement in 1992. Hired during the early years of the AAT to bring chemical signatures within its member Group in Epping: Nicholas Staszak is the setting in motion refurbishment plans some experience to the new telescope, Tom came from Mt. Wilson stars, we can use this signature to tag New Mechanical Manager and started in for the AAOmega instrument. Max has Observatory where he had worked for the previous 24 years. dispersed individual stars to a common March and Naveen Pai has joined us as been awarded a NASA Postdoctoral formation site. This is the concept of a mechanical technician, in which role fellowship based at the University of Born in 1927 in St. Louis, Missouri his family moved to Los chemical tagging. he will be taking over many of the duties California, Los Angeles. Angeles when he was 8. Like many of us, he formed an interest currently undertaken by Denis Whittard. in astronomy during his early school years and never let it go. He De Silva et al. 2007 (AJ, 133, 694) was Summer Students joined the LA Astronomical Society, and also became a volunteer the first to demonstrate the viability We have also enjoyed a morning tea to at the Griffith Planetarium, showing visitors the wonders of the of the chemical tagging technique. celebrate everyone who has been at the The AAO runs a twice-yearly fellowship night sky. A chance encounter with renown solar astronomers Using UCLES/ AAT data they derived observatory and/or in the public service for programme to enable undergraduate Seth Nicholson and Robert Richardson while he was visiting Mt abundances for elements of various more than 20 years: Helen Davies, Tony students to gain 10-12 weeks first-hand Wilson Observatory led him to him working at the Pasadena office nucleosynthesis origins for stars in the Farrell, Garry Kitley, Ed Penny, Keith experience of astronomical-related reducing solar observations, and eventually to becoming resident HR 1614 moving group. They discovered Shortridge, Lew Waller, and Helen Woods research. The current crop of students solar observer at the 150-foot solar tower on Mt. Wilson - a these dispersed stars were metal rich (who spent 13 years in the foreign service are from all around the world, enjoying position he held for the 14 years prior to coming to Australia. with [Fe/H] > 0.25 dex, and that the with DFAT) got certificates. More recently spending our winter learning new skills. star-to-star abundance scatter was less Don Mayfield joined this list of luminaries. During his time at Mt Wilson he was able to talk - “chew the fat”, Stacey-Jo Dyas is working under the than 0.03 dex across all elements. This as Tom would say - with many famous astronomers at a time when Sadly people have also left the AAO. supervision of Gayandhi de Silva on a was the first time that stars which are astronomy was making rapid advances in the understanding of We wish them all the best in their new chemical analysis of the open cluster, physically dispersed and located all over the universe. Tom has many momentos of his time there. He has endeavours! IC 4756. Such a study allows for the sky, were found to have near identical a picture when Einstein came to visit the observatory; he has the the investigation of many processes abundances and kinematics. Hence this Ricardo Covarrubias was one of the mechanical calculator that was used to calculate the orbit of Pluto occurring within the cluster; mixing was the first identification of an ancient first Magellan Fellows. He was initially and many of the newly discovered smaller satellites of the giant mechanisms in stellar envelopes are relic star forming event in the disk and seconded to the Carnegie Observatories planets; and he has a painting of probably the rarest observation one example. In addition, this type of paved the way for large scale applications for 2 years supporting visiting Magellan ever made - a transit of the satellite Triton over the face of research is crucial for the success of of the chemical tagging technique. observers at Las Campanas Observatory, Neptune, which he made at the eyepiece of the 100-inch telescope. HERMES. HERMES aims to unravel the followed by a 6 month extension. In his the telescope were properly recorded and archived for posterity. Max Spolaor has won the Charlene formation history of the Milky Way by He moved on from that when offered a job as Chief Night Assistant time as a Magellan Fellow, Ricardo set He also helped optimise the telescope observing schedules, Heisler prize. This prize is awarded identifying stars that formed from the at the newly completed 3.9-m Anglo-Australian Telescope. The new standards for observer support at kept an eye on the library, fielded calls from the public when for the most outstanding PhD thesis monolithic collapse of a single gas cloud new (to him) southern skies were the lure, so he and his wife, Magellan. He spent his last 15 months they had astronomical (or flying saucer) question. He helped in astronomy or a closely related field, and tracing their paths through time, Mary, came to Coonabarabran in 1976. here at the AAO working on various with instruments changes, usually doing the top end changes accepted by an Australian university. The back to an earlier, common position. In aspects of supernova research as well as At the AAT, Tom helped shape the way support was given at the and telescope balance and anything else that was needed. In thesis research must show outstanding order to identify members of the same serving on the LOC of the Southern Cross telescope. Night assistants who knew and understood how the the days when we had instruments which needed solid nitrogen excellence and originality. Max’s thesis clusters it is necessary to understand Astrophysics Conference on “Supernovae telescope operated were employed, but who also had a daytime (pumped from liquid) he took daily charge of ensuring that it was produced important results relating the the key chemical signatures that cluster and their Host Galaxies”, held in June. role in running the observatory were Tom’s preferred model. No done properly. On open days, even after he had retired, he would metallicity gradient and host galaxy mass members share. “us and them” faction as he had seen happen in some other bring along his telescope to show the Sun to the visitors and for early-type galaxies. At least 5 first- In May, Guy Monnet retired from his Stacey-Jo comes from the United places. He was also key to making sure that the data recorded at answer questions. author refereed publications resulted position as acting Head of Instrumentation Kingdom and is currently transitioning

28 Australian Astronomical Observatory Newsletter - AUGUST 2011 Australian Astronomical Observatory Newsletter - AUGUST 2011 29 LOCAL NEWS

It was to amateur astronomy that Tom really devoted himself. His For his dedication he was given many awards and accolades by loves were close to home - the Sun in particular and the planets, his peers, but perhaps the most long-lived recognition was that and variable stars. None of this cosmology rubbish (science fiction a celestial body was named after him. On his retirement from he called it) - you had to understand the stars before you could the AAT, Rob McNaught named asteroid number 5068 (originally understand galaxies and the rest of the universe. designated as 1990TC) as Cragg. Tom was one of the growing band of amateur scientists; making You might think from this that Tom was only interested in contributions to astronomy through his own personal observations. astromomy. Far from it. Amongst his other interests were From 1944 - at the age of about 17 to put it in perspective - he music, war history and playing war games when he could, plus started making drawings of the Sun. He carried on his daily chess and bridge. He was a founding member of the local solar drawings for most of the rest of his life - including taking astronomical society, as well as a regular player the bridge club his telescope on holidays so that he didn’t miss out. Thousands and chess clubs in Coonabarabran (when there was one) and in of drawings in all. I remember him occasionally photocopying Gunnedah. He played flute with the town orchestra, as well as drawings to mail back to the observers at Mt Wilson when they had occasionally accompanying Mary who plays harp. extended cloudy periods - “just so they knew what was happening Tom’s funeral at the Coonabarabran Native Grove Cemetry on the Sun.” was held on a pleasant sunny day in May and was attended At the same time he started his regular solar observations, he by wide variety of people, many of whom had met him since started making variable star observations. Long before the days his retrement and were surprised to learn of his interest in of computer controlled telescopes a very detailed knowledge astronomy. of the sky was required to locate the star to be observed. The I shared an office with Tom for most of the 16 years he was at comparison was then done by eye, judging the difference in the AAT. We shared an interest in astronomy, and I was always brightness between the variable and reference field stars. Good fascinated when he would tell stories of the astronomers he’d observers, like Tom, could do this with almost photometric worked with, the telescopes he’d used and things he’d seen. precision. Exacting work. You then went to the next star in your He was a gentleman, always polite and thinking of others, very list. Tom could do perhaps 20 an hour on a good night, although generous with both his time and toys (letting me come and use sometimes the going was much slower. He did this for several his telescope when he was away) and wonderfully keen and hours every clear night. For many nights a year. For many years. dedicated to astronomy. Astronomy has lost a great observer He amassed well over 160,000 variable star observations in his life. and recorder of the sky with his passing.

Letter from Coona Katrina Harley (AAO)

Well it has been a very busy couple of Earlier last year, Doug Gray made a wager Ending on a high, during the months at site, with many attending with another staff member, (who wants to refurbishment of the lifts at the AAT, training courses for First Aid and Heights remain anonymous) that if the unnamed the OTIS Contractors found a small Rescue. In early May the fire team on the staff member can go without a cigarette Black-Headed Python, along with mountain conducted burn-offs around the for 12 months, then Doug would have to bones of other little critters, in the mountain top. Members of the fire team cycle up the mountain. Doug did manage visitor’s lift well. Once the python thought it was great experience for the to cycle up the mountain earlier this year was rescued from the lift well, it team, and they were very happy with the and then collapsing in a heap on the was released back in the bush - outcome of the burn. ground floor after his accomplishment. one very lucky python. In February, Tim Connors left sunny Coonabarabran for Melbourne. Tim is now working for the Bureau of Meteorology. Imogen Cosier joined us in April from Canberra. Imogen is the new IT Support Officer at site, and has settled in well and enjoying Coona life. In June, the RAVE Workshop was held over two days in Coonabarabran, with reports from many stating it was a very successful and enjoyable meeting. The Acacia Motor Lodge did an excellent job accommodating all of the RAVErs. Many attendees of the workshop travelled back to Vaucluse, to attend a cocktail reception at the residence of the German Consul General.

30 Australian Astronomical Observatory Newsletter - AUGUST 2011 ABOVE: Dragonfly is an optical stellar interferometer taking a EDITOR: Sarah Brough revolutionary approach to the design of such instrumentation. DESIGN AND PRODUCTION: Corporate Media and Communication, This is the power spectrum of the fringes detected from Antares Department of Innovation, Industry, Science and Research during the Dragonfly commissioning run. Dragonfly is described further on page 7. ISSN 0728-5833 Published by the Australian Astronomical Observatory PO BOX 296, Epping NSW 1710, AUSTRALIA

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