NOAO/NSO Newsletter Issue 87 September 2006
Science Highlights Cerro Tololo Inter-American Observatory A Large Population of 1 < z < 2 Galaxy Clusters in the Dark Energy Survey Passes Fermilab Review...... 22 IRAC Shallow Survey of the NDWFS Bootes Field...... 3 Blanco Update...... 22 Filling in the Gaps: WIYN + Hydra Explores SOAR Update...... 23 Changing Carbon Abundances in Globular Clusters...... 5 CTIO Supports Award-Winning Science...... 24 A 6100-Gauss Sunspot Emerges...... 6 An Active Chromosphere on a 55 Jupiter-Mass Object...... 8 Kitt Peak National Observatory Collaborations Improve Capabilities of KPNO Director’s Office and Our Partners...... 25 CATCH Web Site Publicizes Availability of Telescope Time.....10 NSF Grant Helps Fund Development of Users Committee Meets October 5-6...... 10 New Imager for WIYN 0.9-meter telescope...... 27
NOAO Gemini Science Center National Solar Observatory/GONG Gemini Observing Opportunities for Semester 2007A...... 11 From the Director’s Office...... 28 Limited Phoenix Availability for 2007A...... 12 ATST Update: Preliminary Design Review Scheduled; An Update on bHROS for 2007A...... 12 Refinements Made to Optical Design...... 29 NGSC Staff Arrivals and Relocations...... 13 SOLIS...... 31 Plans for Gemini Science 2007 in Iguazú Falls, Brazil...... 13 Granulation Imaging in the K-band with the NGSC Instrumentation Program Update...... 14 NSO Array Camera...... 32 2007A Observing Proposals Due 2 October 2006...... 15 Successful First Summer School in Solar Physics...... 33 Two New NOAO Survey Projects...... 15 GONG...... 34
Observational Programs Public Affairs and Educational Outreach Community Access Time Available in 2007A The Dwarf Moves to a New Home...... 37 with Keck, HET, Magellan, and MMT...... 16 Hands-On Optics Engages Local Boys & Girls Clubs...... 38 Observing Request Statistics for 2006B The Gemini Virtual Tour - Version 4.0...... 39 Standard Proposals...... 17 CTIO REU Program 2007...... 40 KPNO Instruments Available for 2007A...... 18 Gemini Instruments Possibly Available for 2007A...... 19 CTIO Instruments Available for 2007A...... 20 Keck Instruments Available for 2007A...... 21 HET Instruments Available for 2007A...... 21 MMT Instruments Available for 2007A...... 21 Magellan Instruments Available for 2007A...... 21 Third Workshop on the Ground-Based On the Cover Optical/Infrared System This fisheye-lens view shows the A community workshop aimed at developing, identifying and adaptive optics laser guide star system prioritizing new instrument capabilities for medium and large ground- at Gemini North, partly illuminated based telescopes (3.5–10 meters in aperture), both public and private, is by the rising Moon, during testing on being planned for November 16–17 in the Phoenix, AZ, area. 13 July 2006.
The workshop will be limited to about 75 participants. There will be Credit: P. Michaud/Gemini Observatory some openings available for general applicants — watch the main NOAO Web page for an announcement and further details.
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NASA Funds Development of Destiny: The Dark Energy Space Telescope
A team led by Principal Investigator Tod Lauer of the National Optical Astronomy Observatory has been selected by NASA to further develop a concept for a space mission to characterize the mysterious “Dark Energy’’ that permeates the Universe and causes the The NOAO-NSO Newsletter is published quarterly expansion to accelerate. by the National Optical Astronomy Observatory P.O. Box 26732, Tucson, AZ 85726 Known as the Dark Energy Space [email protected] Telescope (Destiny), this small spacecraft would be launched as early as 2013 to detect and observe more than 3,000 supernovae over Douglas Isbell, Editor its two-year primary mission to measure the expansion history of the Universe. This mission would be followed by a year-long survey of 1,000 Section Editors square-degrees of sky at near-infrared wavelengths to measure how the large-scale distribution of matter in the Universe has evolved since Abhijit Saha Science Highlights the Big Bang. Used together, the data from these two surveys will have Dave Bell Observational Programs 10 times the sensitivity of current ground-based projects to explore the Mia Hartman Observational Programs properties of Dark Energy. Nicole S. van der Bliek CTIO Buell T. Jannuzi KPNO Dominic J. Benford of NASA’s Goddard Space Flight Center is the Tom Matheson NGSC Deputy Principal Investigator for Destiny. The Destiny team has Sally Adams NGSC strong connections to the state of Arizona, with members in Tucson at John Leibacher NSO NOAO, the University of Arizona’s astronomy department and Lunar Priscilla Piano NSO and Planetary Laboratory, and several astronomers and space scientists Douglas Isbell Public Affairs & from Arizona State University. Other team members (including several Educational Outreach that were part of the original discovery of Dark Energy) are based at the Space Telescope Science Institute, Harvard University, Texas A&M, Production Staff the University of California at Davis, Michigan State University, the Keith Ann Atkinson Managing Editor University of Chicago, and the Carnegie Observatories. Pete Marenfeld Design & Layout
Kathie Coil Production Support
2 September 2006 Science Highlights
A Large Population of 1 < z < 2 Galaxy Clusters in the IRAC Shallow Survey of the NDWFS Bootes Field
Mark Brodwin (JPL), Peter Eisenhardt (JPL), Anthony Gonzalez (University of Florida), Adam Stanford (University of California-Davis) & Daniel Stern (JPL)
ith their large numbers of galaxies at a common Previous surveys at X-ray and optical wavelengths have look-back time in the most massive gravitationally found large samples of galaxy clusters at z < 1, but have bound systems, galaxy clusters provide key largely failed at z > 1. This failure is due to both the lack of Winsights into both galaxy evolution and cosmology. Redshift sensitivity in the X-ray for all but the most massive clusters, 1 < z < 2 clusters are particularly ideal laboratories in which to and to the loss of the primary observational signal of early directly observe the assembly of massive galaxies as it occurs, type galaxies in the optical as the 4000Å break shifts out allowing us to determine the relative importance of early- of the optical window. One of the primary goals of the collapse and late-time hierarchical assembly mechanisms. Spitzer/IRAC Shallow Survey (Eisenhardt et al. 2004, ApJS, High-redshift clusters also allow us to study the properties of 154, 48) was to take advantage of the beneficial k-correction the dark matter halos in which they reside (via weak lensing in the mid-IR, illustrated in figure 1, whereby passively methods), and are sensitive to cosmological parameters, such evolving cluster elliptical galaxies have an approximately as ΩM, σ8, ΩΛ, and to both the equation of state of the dark flat selection function at 1 < z < 2. energy and its derivative. Our methodology consists of calculating accurate photometric redshift probability distributions (Brodwin et al. 2006, ApJ, in press, astro-ph/0607450) for a 4.5 µm flux-limited sample of 200,000 galaxies across the 8 deg2 common to the IRAC Shallow survey and the NOAO Deep Wide-Field Survey (NDWFS; Jannuzi & Dey 1999) in Boötes. It is therefore the combination of the infrared Spitzer data and the optical NDWFS photometry that make this survey possible.
Figure 1. Apparent magnitudes for passively evolving L* cluster galaxies in Bw, I, KS, and 4.5µm for a Bruzual & Charlot model where the stars form in a 0.1 Gyr burst beginning at zf = 3 in a {ΩΛ= 0.7, ΩM = 0.3, h = 0.7} cosmology. This model fits the observed L* in galaxy clusters to at least z ~ 1 (De Propris et NOAO-NSO 87 Newsletter al. 1999). The horizontal lines indicate the 5σ limits of these bands in 5” diameter apertures in the IRAC Shallow Survey and NDWFS, and at the 50% completeness limit in a 6” diameter Figure 2. Optical spectra of the five member galaxies aperture in KS in FLAMEX. Note that a 5” aperture is larger after being smoothed by a five pixel boxcar. The following than optimal for detection at BW and I; the 50% completeness spectral features (not present in every object) are marked limits in these bands are about 2 mag fainter. The selection in increasing wavelength by the dotted lines: Mg II λ2800, function at 4.5 µm is flat between 1 < z < 2, demonstrating B2900, B3260, [O II] λ3727, Mg I λ3830, Ca II K and H, and that 90-second IRAC exposures allow unbiased cluster detection D4000. The rest-frame wavelength at z = 1.4166 is shown out to z = 2 (Eisenhardt et al. in preparation). along the top (Stanford et al. 2005, ApJ, 634, L129). continued
September 2006 NOAO-NSO Newsletter 87 likelihood of random associations associations random in et prep).al. (Gonzalez data Near-IR of the to likelihood relative significance clusters the candidate assess of to us allow simulations Detailed 2. < z < 0 from slices redshift narrow in probability scales cluster on structures identify to redshift distributions the photometric uses algorithm search wavelet A IRAC of Survey Shallow the NDWFS Bootes Field continued p mliwvlnt dt, nldn HST/ACS, is redshifts. highest at the for those HST/NIC3 with Spitzer/MIPS, including and follow- for being acquired 18currently of z these > Deep 1 data, along clusters, Spitzer/IRAC Palomar/WIRC, multi-wavelength evolution. and studies up, formation for high-redshift laboratory galaxy ideal known of the of provides number and the clusters, in six- a represents increase This fold 1. > z at 93 including 3, figure illustrated in 2, < z < 0 from groups and candidates cluster 292 contains (ISCS) Survey Cluster Shallow IRAC full The ongoing. is analysis cosmological The Keck/Subaru/VLT. and NICMOS with up followed then and candidates discovered were good Several hosts. type late- in found those as many as nine times worth statistically the is supernova in such each uncertainty field, cosmology supernova primary the is correction dust the Because galaxies. host elliptical cluster high-redshift in were clusters forto S. Perlmutter search Type-Ia SNe 1 > 14by Cycle HST/ACS in z with targeted our of Seven panel). right upper 3, in figure shown is cluster this of image (an 2 figure in shown are known, cluster five redshift the highest recently, which until was, for cluster, latter Spectra the of members L129). 634, ApJ, 2005, in al. et al. (Stanford 1.41 et and prep); (Eisenhardt 1.37 and 1.16, in 1.26, 1.06, ApJ, 2006, astro-ph/0607450); al. press, et (Brodwin 816); 639, 1.24 ApJ, 2006, al. et (Elston, 1, 1.11 Gonzalez of > z redshifts mean at with has clusters seven spectroscopy confirmed Keck Follow-up Boötes. in deg ~4 the in redshifts photometric the improve to discovery, ApJ, 2006, 639,al. 816) were post- used, et Gonzalez Elston, (FLAMEX; Survey Extragalactic FLAMINGOS the from Science Highlights September 2006 September 2 common area area common full moon illustrates the extent of survey’s large 8deg large of survey’s extent the illustrates moon full combine the BW images (blue),These I (green) and 4.5 µm The (red) band images. right). 1.41, = upper from
KPNO Mayall 4-m telescope, the capability to efficiently efficiently to capability the at hand. is data these acquire telescope, the 4-m on Mayall NEWFIRM of KPNO commissioning imminent the With beyond. and 2 = z to redshifts will photometric area accurate produce survey full the over data demonstrated near-IR deep have adding that simulations Detailed z~1.5. to reliable only arecurrently which is redshifts, by photometric the limited algorithm the redshifts, these at clusters detect to enough sensitive are already data to Spitzer/IRAC z the = 2. Although sample cluster our extend to is project the of phase next The 2 area. Science Highlights
Filling in the Gaps: WIYN + Hydra Explores Changing Carbon Abundances in Globular Clusters
Michael Briley (University of Wisconsin-Oshkosh/NSF), Judy Cohen (California Institute of Technology) & Daniel Harbeck (University of Wisconsin-Madison)
ontrary to what we are taught in graduate school, This was rectified during a two-night run in July 2005 with individual Galactic globular clusters are not Hydra, the wide-field multi-object spectrograph on the chemically homogeneous populations. Every WIYN 3.5-m telescope at Kitt Peak, where two fields of Ccluster studied to date has revealed significant star-to- 30–40 stars each in M13 were observed. We used the 400 star variations in the elements C, N, and often O (by as g/mm grating, blue fiber bundle, and bench spectrograph much as a factor of 10), as well as other light elements such camera for a resolution of about 7.1 Å/spectral resolution as Na, Al, and Mg, am ong otherwise indistinguishable element. The setup was adjusted so the region of interest, stars. The underlying nature of these anomalies, i.e., 4000–4400 Å, was best focused. their characteristics and their origins, are still uncertain due in no small part to the limited parameter space 0.5 M13 Suntzeff (1981) RGB/SGB Stars sampled to date. Smith et al. (1996) RGB Stars Keck + Palomar RGB/SGB/MS WIYN Hydra Targets However, it appears likely that two separate processes 0.0 Fit are active at different times in cluster histories. The first process, occurring early in the cluster histories, modifies -0.5 [C/Fe] the light-element compositions of the stars (a “primordial” process). The second process, taking place during red giant -1.0 branch ascent, brings CN and possibly ON-cycle exposed material to the surface (a form of “extra-mixing” beyond -1.5 that expected from first dredge-up). Clearly, it is important to understand these variations not only for their clues to the 20 18 16 14 12 physics/evolution of low-mass stars and cluster formation, V but also to properly interpret the integrated spectra of GCs Figure 1. Carbon abundance distribution of red giant branch in external galaxies (e.g. the N-rich globulars of M31). stars in the globular cluster M13. The dotted vertical line indicates the luminosity of the red bump. Note how the The present project is primarily focused on improving mean C abundance starts dropping at the red bump, while a our understanding of the red giant branch extra-mixing substantial primordial variation in the Carbon is evident at mechanism (currently missing in standard models) that all luminosities. takes place within cluster giants of lower metallicity during the RGB ascent. Models which include various From these spectra, the strengths of the G-bands (a candidate mechanisms (meridional circulation, turbulent CH feature) were measured and compared with model diffusion, etc.) predict a noticeable change in CN(O) spectra following techniques in our earlier papers (Marcs surface abundances following the “red bump” in the red models from isochrones, and spectra from SSG). The giant branch luminosity function. The red bump (an over- resulting carbon abundances are plotted as filled circles in density in the luminosity function of the red giant branch) figure 1. Immediately obvious in figure 1 is the trend of corresponds to the destruction of the molecular gradient by rapidly decreasing carbon abundances with evolutionary the outward-moving H-burning shell. state for cluster giants having passed through the luminosity function bump (indicated by the dashed vertical line).
Mixing is inhibited by the gradient before this point. Also present is a significant star-to-star scatter at every NOAO-NSO 87 Newsletter Indeed, our previous Keck and Palomar study of M13 evolutionary phase, which we attribute to the result of stars (Briley, Cohen, & Stetson 2003) has demonstrated “primordial” contamination (see above). that extra-mixing occurs in M13 giants on top of pre- existing “primordial” inhomogeneities (figure 1). The To help interpret figure 1, we fit the observations to a simple observation that extra-mixing takes place in M13 is not a model in which carbon abundances are allowed to linearly new result, however, the extent of the primordial variations change with luminosity at two independent rates: one to was very surprising. However (and unfortunately), even represent possible changes before extra-mixing sets in (i.e., when combined with data from previous investigations, on the sub-giant branch), and one after extra-mixing is the region immediately preceding the bump was in operation. We also allow the point at which the extra- woefully under-sampled, leaving the onset of the carbon continued depletions uncertain.
September 2006 NOAO-NSO Newsletter 87 and the behavior expected (anticipated) by theory. (anticipated) expected behavior the and the of (1998) al. et location Paltrinieri by found bump = 14.75 function V luminosity the to close remarkably is This is best fit bymixing ainchange slope extra- at V =of mag. 14.71±0.20 onset the Moreover, right). the (to extra-mixing [C/Fe], of in onset the after dex/mag decrease -0.23±0.02 to drop a by of followed rate dex/mag in -0.03±0.01 results 1 initial figure an in abundances C the of fit chi-squared A process. fitting the in chosen freely be to in sets mixing Filling +Hydra in the Gaps: WIYN continued decided to investigate properly and, with help from Larry Larry from help with and, properly investigate to further decided require Harvey to Jack at 52º. suffice rare hardly could This elaboration. too were fields strong Perhaps 32º. about with above 1º add to procedure worked a implemented and effect, who produce this recognized Wilson, angles Mt. Nicholson, at Hale Ellery larger George Seth but angles, plate small underestimates. glass tilted for a linear through is ray a of displacement The use. regular of record year 90+ a boast Few can astronomy in 2004. instruments through 1914 from Wilson Mt. at employed was 1) (figure device latter This micrometer. parallel-plate is by fields sunspot measure Hale-Nicholson the photography, with to or visually, spectral way sure The G. 2400 over fields recorded seldom Telescope Vacuum Peak Kitt The light. scattered of because umbrae sunspot fields, in fail butnetwork and plage for good are they sunspots: in do fact not that magnetographs modern synoptic work well the appreciate people Few were. actually fields measured strongest the what out find to decided I and Harvey Jack flares, with connection in G 1993, 5000 of excess in fields strong G., Tel.) V. Nebesnykh (Lozitsky, Fizika i article Kinematika Russian a by Prompted G. per was 1º 100 calibration nominal The coincidence. into line 617.33Fe spectrum the of nm components sigma Zeeman two the bring to required was Nicholson that the plate of tipping inclination the was angle 52º The 52º. as but (G), Gauss 6100 as not marked was it day, that for I thesteeper following bump. is significantly Whileenhanced extra-mixing during depletion carbon of rate the case, this However,M15.in cluster globular metal-poor more the for results similar presenting be paper, we will upcoming an In
Science Highlights it at the 150-foot tower. On the sunspot drawing drawing sunspot the On tower. 150-foot the at it since 1942, 28 when February Joe Hickox firstobserved us awaiting archives, Wilson Mount the in there was t September 2006 September A 6100-Gauss Sunspot Emerges n h psiiiy of possibility the on Bill Livingston & Jack Harvey &Jack Livingston Bill f usos t t Wlo Osraoy poo orey of courtesy (photo Observatory Webster). Larry Wilson Mt. at field magnetic sunspots the of of strength the measure to years 91 for used micrometer, parallel-plate Hale-Nicholson The 1. Figure not necessarily reflect the views of the National Science Science National the of views the Foundation. do reflect and authors the necessarily of not those are material this in recommendations expressed and conclusions, findings, opinions, Any the theory community to identify the underlying process. underlying the identify to community theory the by needed inputs the provide can these as such constraints observational that hope our is It diagram. color-magnitude entire the over metallicities, different of clusters globular in to luminosity others with composition and in changes Smith, definitive measure Norris, Hesser, Bell, Carbon, Kraft, Suntzeff, of works pioneering the upon build to now able are is with lower by predicted again mixing metallicity theory, we continued
Science Highlights
6100-Gauss Sunspot Emerges continued
Webster at Mt. Wilson, searched for the original equipment even though it was modified in 1962. It was still there! Jack and Larry recalibrated it to find the 52º implied a 6100 G field strength.
What about other strong field spots? What was their frequency, for example? In order to search for these, we went through the Mt. Wilson publications of Nicholson, together with the microfilm copies of the daily sunspot drawings. The early work was very complete, but with the onset of photoelectric magnetograms around 1960, the visual measurements were deemed less important and their quality became variable. Fortunately, other observatories initiated similar visual or photographic programs, so we went through the archives of Potsdam, Rome, and the Crimea. We had read of Nikolai Steshenko’s Crimean photographic observation of a 5300 G field, and Elena Malanushenko (formerly of NSO, now at Apache Point Observatory) had obtained the original plates for our study. We readily verified the 5300 G value. From records of 30,000 spot groups, we found 57 spots with fields in excess of 4000 G, and five of at least 5000 G.
What kinds of spots have such strong fields? From the US Naval Observatory collection of white-light full-disk images (1898–1970), which reside at the Kitt Peak solar facility, we found many examples on our list (see figure 2). Often the spots are complex, with light bridges across the umbra. But in some instances the spots are simple in form. Figure 2. A sampling of photographs (and one drawing) of sunspot groups with strong magnetic fields. Jack Harvey performed a statistical study of the distribution of strong fields, and found no particular location for them within the solar cycle. The distribution of fields above 3000 G is continuous and follows a power law. One notable feature is that odd-numbered cycles contain 30% more sunspot groups, but 60% fewer 3000 G or greater field- strength sunspot groups, compared to the preceding even- numbered cycles.
Given such interesting results, we are concerned that, at present, no systematic (synoptic) observations are being made of sunspot fields. NOAO-NSO 87 Newsletter
September 2006 NOAO-NSO Newsletter 87 of both low-mass, brown dwarf-like objects and active active and objects way. unexpected amost in dwarf-like chromospheres brown low-mass, both of study the into entered has group Our star. sequence main T flowing through the inner Lagrangian point, and when no when and point, Lagrangian inner the through low-flowing long-lived its is no mass during essentially when time the is, that state; accretion binary this studied have We secondary. of the behavior the and strong transfer mass but the MG), affect (13 greatly to enough polar a for end weak the at is dwarf white Eri’s EF Jupiter. can planet the object about than secondary larger no the be and apart radius solar a about are Eri EF in stars component two the minutes, 81 only of Eri EF polars, period (Nov.2006 orbital shortest the of one studied recently have (Lawrence myself and Laboratory), Huber National Livermore Mark University), State Mexico (New Harrison Thomas University), Brook (Stony Walter Fred poles. magnetic dwarf white of the both onto one of directly lines field strong the along stream tight a in funneled and plane, orbital the is of out pulled star captured, secondary the from the material because overflow Lobe disks, Roche accretion any contain not do systems These MG. 250 to up MG 10 from strength field magnetic high of lines dwarfs white contain stars, field poles. Herculis AM or Polars, magnetic two magnetic its at the dwarf white the follow onto accreting there roughly material to and confined disk, accretion is the of part inner dwarf the white (5 field the magnetic which measurable a in has CVs are polars Intermediate bandpass. optical the in components stellar both outshining often viscosity, the from material the to due irradiation heating both self-frictional and by dwarf white up heats disk This dwarf. white the around disk accretion an forms mass transferred the less, or MG ~5 of fields magnetic have to thought field, white the dwarf. For in white no magnetic with dwarfs discernible present is that field magnetic the of strength the by systems, These star. classified (CVs), variables primarily are cataclysmic termed primary smaller, but the higher-mass, to via secondary low-mass the transfer from mass overflow have lobe Roche they i.e. binaries, interacting are 70 every other orbits, each tight encircling very in be will systems the these low-of that majority predict a vast today and Galaxy the in primary star dwarf secondary mass white a containing binaries close of evolution and formation the of models Theoretical Science Highlights An Active Chromosphere on a55 Jupiter-Mass Object September 2006 September eeal lmtd o h suy f ige bet, or a with more paired massive objects, present in binaries those single is of study dwarfs the to brown limited and generally stars low-mass of study he ApJ , astro/ph 0607140) astro/ph , – 90 minutes. These systems systems These minutes. 90 . With an orbital period period orbital an With . – 10 MG) that disrupts disrupts that MG) 10 Steve Howell Howell Steve
strength and ratio to that of a typical active chromosphere star. chromosphere asolar-like in active typical a in of that consistent to ratio are and and strength object secondary the to from shown are emanate lines emission The species. sensitive activity other and He as well as emission, Balmer complete revealed for in overdeep quiescence andfive Keckspectroscopy years, hadbeen the binary after detected as Hα followed. emission, been has Eri EF of behavior spectroscopic and photometric long-term the Tololo Chile, in Cerro on telescopes SMARTS Using the occurs. ontodwarf white the accretion substantial sequence star (the present day white dwarf) and a brown brown a and dwarf) white day present (the star sequence main a of binary precursor a from present, at seen as binary, theof suchthat formation a close suggest models Theoretical but we clues. have do some yet, question this to answer the know not do We atmosphere? hydrogen the thin a is with covered core or helium remnant a object companion, secondary dwarf brown a with out start the Did binary object? dwarf-like brown a as of up end Giga-years to loss suffered mass simply has and star sequence main out as a start EF more-or-less normal Eri? Did secondary the in be to come object an such did how But dwarfs. brown of range a the in securely yield masses, Jupiter 55 to is secondary the of mass mass estimated The dwarf object. with white secondary the of combined the measurement were of radial line estimates emission observations, previous Hα SMARTS the of of velocities years two over Using field magnetic surface details. for the text See strength. reveal and split, Zeeman are lines absorption Balmer white dwarf underlying The views). expanded (see secondary the from lines emission of set the shown range at and at S/N top reveals quite left) good (full pass band optical the of majority the covers 2006. spectrum January The in II Keck by observed as Eri EF 1. Figure continued Science Highlights
Active Chromosphere on a 55 Jupiter-Mass Object continued dwarf is difficult. If the binary starts out well separated, it will never come into contact within a Hubble time. If it starts out too close, the brown dwarf will coalesce with the pre-white dwarf during the common envelope stage. Thus, the primordial brown dwarf scenario seems unlikely.
The presence of substantial stellar activity seems to argue against a helium core-type object, leaving us with a secondary that is probably a degenerate low-mass, remnant object, the result of aeons of mass transfer onto the white dwarf primary. The driving force for the stellar activity (starspots, flares, etc.) is also unknown, but the rapid rotation of the synchronously locked secondary, and the fact that the entire low-mass object is fully permeated by the white dwarf’s strong magnetic field are likely catalysts.
Three other polars have since been studied in detail during low-accretion states, and they all seem to show Figure 2. The Hα radial velocity curve for EF Eri based a similar result: the low-mass secondary stars have high on SMARTS spectroscopy. The solid line is our best fit, as chromospheric activity, which is probably also driven by described in the text. The top axis shows the photometric the fact that the secondary is continually bathed in the phase as determined by Bailey et al. (1982) and the bottom strong magnetic field of the white dwarf. axis show our new spectroscopic orbital phase.
Further work will continue to expand the sample of polars observed in low states, and observations of EF Eri and the like are being started to detail the atmospheric structure and inner workings of the “dynamo-like” mechanism responsible for the chromospheric activity seen in these low-mass stars. NOAO-NSO 87 Newsletter
September 2006 DIRECTOR’SOFFICE NATIONAL OPTICAL ASTRONOMY OBSERVATORY
CATCH Web Site Publicizes Availability of Telescope Time
Todd Boroson & Letizia Stanghellini
ne of the practical difficulties of using the diverse set of facilities that make up the ground-based optical/infrared (O/IR) system is just being familiar with all of the capabilities Othat are available.
This becomes obvious twice a year at NOAO, when we receive CATCH presents two views of the O/IR system: one organized proposals for time on 18 telescopes. Only three of these telescopes by capability, and the other by site and program. The capability are operated by NOAO independent of partners. Of the other 15, view allows the user to specify what type of observation is nine are run by partnerships that include NOAO, and six are private desired, then query the CATCH database. CATCH provides a telescopes for which community observing time is distributed table with all the potentially usable instruments, together with by NOAO. For a user, this array of possibilities must seem just as links to more detailed information. The site/program view lists daunting as it is to the members of the Time Allocation Committee, each observatory, providing pull-down menus for links to specific especially when the additional facilities supported by the NSF information, including how to obtain time. The listings include Program for Research and Education with Small Telescopes (PREST) all NOAO and NOAO-partner facilities, all TSIP-funded facilities, are added to the mix. and all PREST-funded facilities. We intend to offer the option of being included on this listing to other private observatories that We have just launched the Community Access Telescope make time available to the broader community. Clearing House (CATCH) Web site to address this problem (see www.noao.edu/system/catch/). This site aims to organize the Please send comments on CATCH and ideas for improving its information on all publicly available facilities and to present that usefulness to Letizia Stanghellini ([email protected]). information in a uniform way. Users Committee Meets October 5–6
James Lowenthal (Smith College) & Jeremy Mould
he NOAO Users Committee is seeking input from the Of further importance, the Users Committee and NOAO will astronomical community this month. The committee discuss what we currently know about implementation plans in provides the national observatory with feedback and advice response to the outcome of the NSF Senior Review. Whatever facilities Ton all aspects of operations that might impact you as a user of or programs the Senior Review Committee may recommend phasing NOAO facilities and services. out (unknown at this writing), NOAO’s goal remains to provide cutting- edge public access observing facilities for the foreseeable future. In its upcoming October meeting, the Users Committee will address current, near-term and medium-term issues relating to Your input, combined with these meetings and discussions, will be instrumentation, user access, Gemini, program efficiency, small and the start of a vitally important dialogue with the community, which medium telescopes, the TSIP and SMARTS programs, and public/ we hope will be in a mature state at the time of the January 2007 AAS private cost-sharing. The committee’s input to NOAO will be much meeting in Seattle. richer if users take a few minutes to send an email to one of the committee members providing positive or negative comments on 2006 NOAO Users Committee: the NOAO facilities that you currently use, or that you would like James Lowenthal, Smith College (Chair) ([email protected]) to see us offer. Timothy Beers, Michigan State University ([email protected]) Ian Dell’Antonio, Brown University ([email protected]) There will be two important special topics of the Users Committee Stacy McGaugh, University of Maryland ([email protected]) meeting this year. The first is a discussion about the next new Ata Sarajedini, University of Florida ([email protected]) instrument for the 4-meter telescopes, following the commissioning Nathan Smith, University of Colorado ([email protected]) of NEWFIRM at the end of this year. New instrumentation is a long Angela Speck, University of Missouri ([email protected]) lead-time item, essential to keeping a science facility on the frontier, Nicole Vogt, New Mexico State University ([email protected]) and must be a strategic addition to the optical/infrared system.
10 September 2006 NOAOGEMINISCIENCECENTER TUCSON, ARIZONA • LA SERENA, CHILE Gemini Observing Opportunities for Semester 2007A
Verne V. Smith
he NOAO Gemini Science Center (NGSC) encourages the • Bench-mounted High-Resolution Optical Spectrograph (bHROS). US community to take advantage of Gemini observing • Acquisition Camera for time-series photometry. opportunities for semester 2007A (1 February 2007–31 • Phoenix high-resolution infrared spectrograph, for a limited time TJuly 2007). US Gemini observing proposals are submitted to and during the first part of 2007A (see following article). Phoenix is evaluated by the NOAO Time Allocation Committee (TAC). The available only in classical mode (in whole nights with no three- formal Gemini “Call for Proposals” for 2007A will be released night minimum). NGSC Staff will provide training and start-up on or about 1 September 2006, with a US proposal deadline assistance to Phoenix classical observers. of 2 October 2006. As this article was prepared well before the • All modes for GMOS-South, bHROS, GNIRS, and T-ReCS are release of the Call for Proposals, the following list of instruments offered for both queue and classical observing. Classical runs are and capabilities represents only our expectations of what will be offered only to programs with a length of three nights or longer offered in semester 2007A. Watch the NGSC Web page www.noao.( (except in the case of Phoenix). edu/usgp) for the Gemini Call for Proposals, which will list in clear detail the instruments and capabilities that will be offered. Detailed information on all of the above instruments and their respective capabilities is available at www.gemini.edu/sciops/ NGSC anticipates the following instruments and modes on Gemini instruments/instrumentIndex.html. telescopes in 2007A: The percentage of telescope time devoted to science program Gemini North: observations in 2007A is planned to be greater than 85 percent at • Near-infrared Integral Field Spectrometer (NIFS). Gemini North and greater than 70 percent at Gemini South. • The Near Infra-Red Imager/spectrograph (NIRI) will be offered with both imaging and grism spectroscopy modes. We remind the US community that Gemini proposals can be • Altair adaptive optics (AO) system in Natural Guide Star submitted jointly with collaborators from other Gemini partners. (NGS) mode, as well as in Laser Guide Star (LGS) mode. LGS An observing team requests time from each relevant partner. commissioning and system verification (SV) runs are taking Multi-partner proposals are encouraged because they access a place in 2006A/B. LGS full science mode will be offered in 2007A, large fraction of the available Gemini time, thus enabling larger contingent on the success of these runs. Altair is available with programs that are likely to have substantial scientific impact. NIRI imaging and spectroscopy, with NIFS IFU imaging and Please note that all multi-partner proposals must be submitted spectroscopy, and with NIFS IFU spectral coronagraphy. using the Gemini Phase I Tool (PIT). • Michelle, mid-infrared (7–26 micron) imager and spectrometer including an imaging polarimetry mode. Efficient operation of the Gemini queue requires that it be populated • Gemini Multi-Object Spectrograph (GMOS-North) and imager. with programs that can effectively use the full range of observing Science Modes are multi-object spectroscopy (MOS), long- conditions. Gemini proposers and users have become increasingly slit spectroscopy, integral-field unit (IFU) spectroscopy, and experienced at specifying the conditions required to carry out imaging. Nod-and-shuffle mode is also available. their observations using the on-line Gemini Integration Time • All instruments and modes are offered for both queue and Calculators (ITCs) for each instrument. NGSC reminds you that a classical observing. Classical runs are offered only to programs program has a higher probability of being awarded time and being with a length of three nights or longer. executed if ideal observing conditions are not requested. The two • Time trades will allow community access to the Keck Telescope conditions that are in greatest demand are excellent image quality high-resolution optical spectrograph, HIRES, and to the Subaru and no cloud cover. We understand the natural high demand Telescope Suprime-Cam wide-field imager and the infrared for these excellent conditions, but wish to remind proposers that imager and spectrograph (MOIRCS). programs that make use of less-than-ideal conditions are also needed for the queue. Gemini South: • Gemini Near Infra-Red Spectrograph (GNIRS). NOAO accepts Gemini proposals via the standard NOAO Web • Thermal-Region Camera Spectrograph (T-ReCS) mid-infrared proposal form and the Gemini PIT software. We remind proposers (2–26 micron) imager and spectrograph. that they can save their proposals as a PDF file to view the version • Gemini Multi-Object Spectrograph (GMOS-South) and imager. that will be used by the NOAO TAC (please see www.noao.edu/ Science modes are multi-object spectroscopy (MOS), long- noaoprop/help/pit.html). slit spectroscopy, integral-field unit (IFU) spectroscopy, and imaging. Nod-and-shuffle mode is also available. Feel free to contact me at NGSC ([email protected]) if you have any questions about proposing for US Gemini observing time.
September 2006 11 NOAO-NSO Newsletter 87 12 typically a single instrument assigned to each instrument instrument each to assigned Gemini instrument single a with typically changes, year. instrument this minimize to expired strive operations Phoenix of use shared for T information on bHROS can be found on the Gemini Web page ( page Web ( Cunha Katia Gemini the on found be can bHROS on information 2005 December The high relatively and them. consider to time resolution 2007A the is semester of bHROS, throughput spectral superior the from benefit could that programs observing have you If telescope. 8-meter an class for capability unique nearly and powerful a presents bHROS (R=150,000), resolution spectral high very its With the meets it that such demand in increase an not rule. 16-night is there if 2007A in telescope the on go ( not will Proposals bHROS for that possible is Call it and Overview Semester semesters. two Gemini these the for waived in was noted rule As used 16-night the be to although offered, criterion been has minimum it 16-night semesters the two the meet over not telescope did the bHROS on proposals, submitted of number small the of result a As minimal. were also partners Gemini other T the in announced be will dates available of range final the in mind. should If keep availability limited is this Phoenix offered, 2007A in Phoenix request to planning Proposers (February–mid-March). 2007A semester of part a for availability Phoenix possible South Gemini shows in timeline Gemini current The is limited. dedicated Pachón instrument a at as time expected Phoenix’s is so MCAO 2007A, telescope. Multi-Conjugate Phoenix the the displace from Pachón, will at system (MCAO) Optics arrival Adaptive its On port. NGSC September 2006 September instrument in semester 2006A. During its first two semesters of availability, the US community submitted seven seven submitted community US the availability, of semesters two for first fortwo were 2006B: and proposals forsix and time from two 2006A awarded forproposals 2006A Requests 2006B. facility a its During as offered first 2006A. was semester South in Gemini instrument at (bHROS) Spectrograph Optical Resolution High bench-mounted he agreement NOAO/Gemini The 2002A. semester since South Gemini on offered been has Phoenix, spectrograph, infrared high-resolution NOAO he [email protected] NOAO/NSONewsletter Limited Phoenix Availability for 2007A An Update on bHROS for 2007A ). contains an article summarizing the capabilities of bHROS (page 19). Detailed Detailed 19). (page bHROS of capabilities the summarizing article an contains Katia Cunha &Verne Cunha V.Katia Smith Ken Hinkle &Verne Hinkle V.Ken Smith
community informed of Phoenix’s future. of Phoenix’s US informed the community keep will NOAO and NGSC available. become they as publications Phoenix refereed of copies us send to Phoenix of users previous encourage strongly we effort, this in To aid SOAR telescope. the involve may Phoenix of use Future date. future some at again offered Phoenix see to like NOAOwould southern hemisphere. the in community Gemini spectrograph and US the infrared to available high-resolution only the is semesters. Phoenix 10 last the for semester each scheduled nights 16 at with use South onleast Gemini has had Phoenix substantial dates. availability ( site Web ( page Web NGSC The 2007A for to Call Proposals be posted about 1 2006. September www.gemini.edu/sciops/instruments/hros www.gemini.edu/sciops/ObsProcess/ObsProcIndex.html www.gemini.edu www.noao.edu/usgp/ ) will keep you current on Phoenix Phoenix on current you keep will ) ) or by contacting contacting by or ) ) or the Gemini Gemini the or ) ),
NGSC
NGSC Staff Arrivals and Relocations
Verne V. Smith
e are pleased to announce the following two Jayadev Rajagopal arrived as an NGSC Staff member in La additions to the scientific staff of the NOAO Serena on the same date. Previously a Michaelson Fellow Gemini Science Center (NGSC). Please join us at NASA’s Goddard Space Flight Center in Greenbelt, MD, Win welcoming them. Jayadev brings research expertise in interferometry, and he will split his observatory support duties between NGSC and Susan Ridgway joined the NGSC Staff in La Serena, Chile, the New Initiatives Office. on 1 July 2006, arriving from her previous position at The Johns Hopkins University in Baltimore, MD. She is expert In mid-June 2006, Bob Blum relocated from NOAO South on Active Galactic Nuclei, radio galaxies, and quasars. in La Serena to NOAO North in Tucson. Bob continues Susan will support US users of Gemini’s increasingly his work with NGSC in support of AO programs, as powerful adaptive optics (AO) capabilities, such as the well as Phoenix; he is also working on the Thirty Meter Laser Guide Star system on Gemini North with NIFS and Telescope project. NIRI, and AO on Gemini South with the arrival of MCAO. She will also help support the heavily used Gemini Multi- Object Spectrographs (GMOS).
Plans for Gemini Science 2007 in Iguazú Falls, Brazil
Verne V. Smith & Sally Adams
uilding upon the first Gemini Science meeting in May 2004, the next meeting in the series will be held in the second half of May 2007 at Iguazú Falls (Foz do BIguaçú), Brazil. Hosted by the Brazilian National Gemini Office, the three-day meeting will highlight and discuss science results from the Gemini South and North telescopes. The meeting will consist of oral and poster presentations, as well as a users’ session including talks about future Gemini instruments and software development, with plenty of time for discussion and feedback.
Foz do Iguaçú is located in southeastern Brazil near its borders with Paraguay and Argentina. The spectacular Iguazú Falls are wider than Victoria Falls and higher than Niagara Falls, and surrounded by the virgin jungle of Iguazú National Park, home to an estimated 2,000 species of flora and 400 species of birds. Iguazú Falls, Brazil NOAO-NSO 87 Newsletter The main points of entry for travel to Brazil are Sao Paulo Keep an eye on the NGSC (www.noao.edu/usgp) and Gemini (airport code GRU) and Rio de Janeiro (airport code GIG). Observatory (www.gemini.edu) Web pages for information Domestic airline service from these airports to Foz do on Gemini Science 2007. Iguaçú is readily available.
September 2006 13 NOAO-NSO Newsletter 87 14 in the US, with progress since the June 2006 2006 June the since progress with US, the in developed being instrumentation on update Gemini status a gives article This programs. science frontline of support T work to NICI final acceptance by Gemini is complete. is Gemini by acceptance final work NICI to As of the end ofthat 99 percent reported ofJune, MKIR the testing. for acceptance preparation in made being are fixes software Final levels. previous from electronic the Furthermore, noise in the combination has array/controller been reduced arrays. NICI the on signal background elevated the reducing in made was Progress encouraging. results initial with characterized, fully yet but tested not performance and the dynamic characterized been tested. As of July, the AO static has been performance end of (AO)optics summer. NICITheadaptive has system the by begin to expected testing acceptance pre-ship with NICI is in the finalassembly and testing phase ofthe project, NICI Newsletter. Mauna Kea Infrared (MKIR) in Hilo is building building is Hilo in Toomey. of Doug leadership the under NICI, (MKIR) Infrared Kea telescope. South Mauna Gemini the on capability imaging coronagraphic dual-beam 5-micron to 1- a provide will (NICI) Imager Coronagraphic Infrared The Near NGSC September 2006 September instrumentation for the Gemini telescopes in in telescopes Gemini capable the and for innovative provide instrumentation continues to mission Program its Instrumentation NGSC he NGSC Instrumentation Program Update FLAMINGOS-2 from the entrance window of the MOS Dewar Dewar wheel. slit the on inplace MOS port imaging the with the of window entrance the from FLAMINGOS-2 Verne V. Smith &Mark Trueblood NOAO/NSO R ~ grism have3000 been resolved. Thescience-grade detector and testing phase of the project. Previous integration issues the in with obtaining the continuing is Team FLAMINGOS-2 The FLAMINGOS-2 percent of work to FLAMINGOS-2 final acceptance by acceptance final FLAMINGOS-2 complete. is Gemini to 93 work that reports of team Florida percent of University the June, of As proceeding to pre-ship acceptance testing. preventing the team from completing the integration work and issues technical majorno are July,there of As Gainesville. to engineer Roberto Rojas software a visit by during June Gemini the hardware. Integration with the Gemini software was begun control to use in is and complete is software control detector and Instrument corrected. was times restricting integration of range the severely was that controller array detector the software/hardware in A used devices array logic programmable the detector.in incompatibility engineering-grade the delamination of catastrophic sudden a following installed was FLAMINGOS-2, under the leadership of Principal Principal of leadership Eikenberry. Steve Investigator the building is under Florida of FLAMINGOS-2, University The system. optics adaptive multi-conjugate South’s Gemini spectroscopic for multi-object a capability provide also will It field. 2-arcmin 6.1× a over spectroscopy multi-object provide multi-object the Gemini standard near-infrared field at cover a 6.1-arcmin-diameter will FLAMINGOS-2 a and for imager South telescope. the Gemini spectrograph is FLAMINGOS-2 f /16 focus in mode, imaging and will OBSERVATIONALPROGRAMS NATIONAL OPTICAL ASTRONOMY OBSERVATORY 2007A Observing Proposals Due 2 October 2006
Todd Boroson
tandard proposals for NOAO-coordinated observing time for can then be edited locally and the proposal submitted by email. semester 2007A (February—July 2007) are due by Monday Please carefully follow the instructions in the LaTeX template for evening, 2 October 2006, midnight MST. Facilities available submitting proposals and figures. Sthis semester include the Gemini North and South telescopes, Cerro Tololo Inter-American Observatory (including SOAR), Kitt • Gemini Phase-I Tool (PIT): Investigators proposing for Gemini Peak National Observatory, and community-access time with time only may optionally use Gemini’s tool, which runs on Solaris, Keck, HET, Magellan, and MMT. RedHat Linux, and Windows platforms, and can be downloaded from www.gemini.edu/sciops/P1help/p1Index.html. Proposal materials and information are available on our Web page (www.noao.edu/noaoprop/). There are three options for submission: Note that proposals for Gemini time may also be submitted using the standard NOAO form, and that proposals which request time • Web submission: The Web form may be used to complete and on Gemini plus other telescopes MUST use the standard NOAO submit all proposals. The information provided on the Web form is form. PIT-submitted proposals will be converted for printing at formatted and submitted as a LaTeX file, including figures that are NOAO, and are subject to the same page limits as other NOAO “attached” to the Web proposal as encapsulated PostScript files. proposals. To ensure a smooth translation of your proposal, please see the guidelines at www.noao.edu/noaoprop/help/pit.html . • E-mail submission: As in previous semesters, a customized LaTeX file may be downloaded from the Web proposal form, after The addresses below are available to help with proposal preparation certain required fields have been completed. “Essay” sections and submission:
Web Proposal materials and information www.noao.edu/noaoprop/ Request help for proposal preparation [email protected] Address for thesis and visitor instrument letters, as well as consent letters, for use of PI instruments on the MMT [email protected] Address for submitting LaTeX proposals by email [email protected] Gemini-related questions about operations or instruments [email protected] www.noao.edu/gateway/gemini/support.html CTIO-specific questions related to an observing run [email protected] KPNO-specific questions related to an observing run [email protected] HET-specific questions related to an observing run [email protected] Keck-specific questions related to an observing run [email protected] MMT-specific questions related to an observing run [email protected] Magellan-specific questions related to an observing run [email protected]
Two New NOAO Survey Projects
Tod R. Lauer
wo new NOAO survey projects have been approved, with in order to address the proposers’ scientific research goals. Survey observations beginning in the second semester of 2006. projects may run for up to three years, and can receive larger blocks The projects were selected from ten proposals submitted in of time than are usually awarded in the standard observing-time Tresponse to an announcement of opportunity for new surveys. allocation process. In return for the large allocation of resources, the survey teams are required to deliver their reduced survey The NOAO Survey Program is designed to foster observing data products to the NOAO Science Archive (NSA) for follow-on proposals that require the generation of a large, coherent data set investigations by other interested astronomers. continued
September 2006 15 NOAO-NSO Newsletter 87 16 Spectrographs. For the latest information on HET HET on Low-Resolution information and latest the Medium-, For High, Spectrographs. the include instruments Available Hobby-Eberly Observatory. McDonald at aperture Telescope effective be 9.1-meter to the at expected are available observations queue of hours 76 About Telescope • Hobby-Eberly see For details, latest the Interferometer. the including available, are modes instruments and facility All Kea. W.M.Mauna on the at Observatory Keck telescopes 10-meter the with available be will time observing scheduled of of A classically nights total eight Telescopes • Keck astronomical general the to 2007A: in facilities following available at the community is time telescope A archival research value of the data products, and 25 and percent products, of data value the research archival 25 percent the for goals, scientific of primary the for quality percent 50 of sum weighted a comprising grades final the with categories, three in proposals the graded Committee Allocation Time Survey the Overall, itself. team survey the of goals scientific primary the of follow-on part as conducted be not interesting will that that products data the with done be is can investigations likelihood proposals survey the the of evaluation determining the of part key A Two New NOAO Projects Survey continued band-passes to determine ages and abundances. abundances. and ages determine to band-passes Washington using stars, turnoff main-sequence oldest below the magnitudes 1.5 reach to designed are out-lying stellar observations extreme deep the in obtain regions of Clouds. areas both the Large and Magellanic The Small to selected imager in photometry Mosaic and 4-meter Blanco CTIO the telescope use will survey al. et Saha The Principal Imaging Sources,” (Harvard/CfA). IR Grindlay E. Jonathan Investigator X-Ray and ChaMPlane Spectra of (NOAO); Optical Identification II: Saha “ChaMPlane Abhijit and Investigator Magellanic Principal the of Clouds,” Extremities the at Populations Stellar Survey: Limits Outer “The selected: were Twosurveys new plan. management survey of the credibility for the Observational Programs Program (TSIP) and a similar earlier program, program, earlier similar a and Instrumentation (TSIP) Program System Telescope Foundation’s s a result of awards made through the National Science Community Access Time Available in 2007A with September 2006 September www.noao.edu/gateway/keck/. Keck, HET, Magellan, and MMT Todd Boroson & Dave Bell Todd Bell &Dave Boroson reddened fields that could not be probed with the Mosaic Mosaic highly the survey. initial of the with of imagery probed be imagery not K-band could that and fields H-, reddened J-, obtain to camera theandISPI infrared forclassification, source spectra obtain to spectrograph multi-object Hydra the with 4-meter CTIO the use will survey new Way.The Milky the sources of plane the X-ray in Chandra of identifications optical provided which survey, infrared ChaMPlane NOAO and earlier their spectroscopic a to follow-up is survey al. et Grindlay The clouds. the of outskirts the in used distribution subsequently matter dark be the probe to may that tracers stellar identify will and clouds, the of composition structural the elucidate also past of Way.will diagnostics Milky the Theobservations with or of interactions as the well in as clouds to the gave rise that phases systems stellar of mergers smaller clouds, earliest stellar the the very use of the to of formation are probe a survey as this of properties goals scientific The mass X-ray binaries and Be-high mass X-ray binaries to to binaries X-ray Galaxy. of the content mass source accretion the constrain Be-high and low- binaries quiescent X-ray identify mass to galactic as of well as function longitude, a and as radius space the variables cataclysmic understand to of density are goals scientific survey’s This minute changes before starting aproposal. starting before changes minute last- any for site WebNOAO the check to encouraged are investigators always, As section. end at ofbe found the this 2007Ain to can be available we expect of A instruments list MMT gateway/mmt/. the of see telescope information, further For 6.5-meter Observatory. the with available be will time observing classically-scheduled of Twelvenights Observatory • MMT proposal and see instructions, instrumentation updated For available on Observatory. information Campanas Clay Las and at Baade telescopes 6.5-meter the with programs observing A total of fivenights willbe available forscheduled classically Telescopes • Magellan observing writing see proposals, for instructions and instrumentation
www.noao.edu/gateway/het/ www.noao.edu/gateway/magellan/ . www.noao.edu/ .
Observational Programs
Observing Request Statistics for 2006B Standard Proposals No. of of No. Requests Nights Requested Average Request Nights Allocated (*) Nights DD Previously Nights Allocated ScheduledNights Programs New For Over-Subscription Programs New For GEMINI
GEM-N 170 206.88 1.22 55.14 0.23 0 55.14 3.75 GEM-S 113 175.82 1.56 47.42 0.77 4 43.42 4.05
CTIO
CT-4m 56 196.9 3.52 86.5 0 0 86.5 2.28 SOAR 11 25.1 2.28 21.5 0 0 21.5 1.17 CT-1.5m 10 36.4 3.64 8.7 0 0 8.7 4.18 CT-1.3m 13 58.3 4.48 9.6 0 1.9 7.7 7.57 CT-1.0m 8 63 7.88 37 0 0 37 1.7 CT-0.9m 20 85 4.25 45.5 0 0.6 44.9 1.89
KPNO
KP-4m 57 203.6 3.57 112 0 0 112 1.82 WIYN 28 79.8 2.85 40 0 0 40 1.99 KP-2.1m 23 123.2 5.36 93 0 0 93 1.32 KP-0.9m 8 45 5.62 17.5 0 0 17.5 2.57
Community Access
Keck I 14 20 1.43 7 0 0 7 2.86 Keck II 18 25.5 1.42 6 0 0 6 4.25 HET 12 18.08 1.51 7.45 0 0 7.45 2.43 Magellan-I 5 12 2.4 2 0 0 2 6 Magellan-II 5 10 2 2 0 0 2 5 MMT 20 49.5 2.48 13.5 0 0 13.5 3.67 NOAO-NSO 87 Newsletter
*Nights allocated by NOAO Director
September 2006 17 NOAO-NSO Newsletter 87 18 8 7 6 5 4 3 2 1 The instrument shouldbe available forscheduling through 1 February April 15,2007. instrument. isFLAMINGOS an instrument built by Richard Elston and his collaborators at University the of is currently Florida. Steve PI the of Eikenberry the We anticipate that OPTIC again available will be through an agreement with John Tonry of University the of Hawaii. support schedulingobservatory Fast needs. guiding of mode operation of OPTIC is now asupported for mode NOAO users of instrument. the OPTIC Camera from Uof Hawaii may assigned as alternative be ifit proposed meets imaging and needs making such an assignment would further capable of providing Doppler precision of 4.4m/sin2minutes for aV=3.5mag. G8Vstar. measurements of velocities radial for suitably bright enough targets. regarding Details instrument this are available our via instrument web pages. It is Exoplanet Tracker (ET) is an instrument provided by Jian of Ge University the of Florida and his colleagues. It precision high enables very Integral Field Unit, 80”x80” field, graduated 5” fibers, spacing Integral Field Unit: 30”x45” field,alsofiber spacing 3” 4” fibers, @f/6.5; available Cass at atf/13. IRMOS, built by John MacKenty and collaborators. Availability on depend proposal will demand and block scheduling constraints. Resolution for 2-pixel slit. Not slits all cover field; check instrument full manual Observational Programs IRMOS FLAMINGOS Echelle Spectrograph MARS Spectrograph R-C Spectrograph CCD Mayall 4m Spectroscopy CCD MosaicCCD WIYN 0.9m FLAMINGOS SQIID ImagerCCD 2.1m WTTM OPTIC Mini-Mosaic WIYN 3.5m FLAMINGOS SQIID MosaicCCD Mayall 4m Imaging Exoplanet Tracker (ET) FLAMINGOS Spectrograph CCD GoldCam 2.1m SparsePak DensePak Hydra Spectrograph +Bench WIYN 3.5m 7 2 3 September 2006 September 4 6 8 1 1 KPNO Instruments Available for 2007A 5 8Kx8K HgCdTe (2048x2048) InSb (4-512x512) T2KB/F3KB CCD 4Kx2K CCD 4Kx4K CCD 4Kx4K CCD HgCdTe (2048x2048) InSb (4-512x512) 8Kx8K Detector (4kx4k,5000-5640Å) CCD HgCdTe (2048x2048,0.9-2.5μm) F3KA CCD T2KA CCD T2KA CCD T2KA CCD HgCdTe (1024x1024,0.9-2.5μm) HgCdTe (2048x2048,0.9-2.5μm) T2KB/F3KB CCD (1980x800) LB CCD T2KB/LB1A/F3KB CCD Detector 1000-1900 300-4500 700-22000 700-22000 700-22000 300,1000,3000 1000-1900 18000-65000 300-1500 300-5000 Resolution 3500-9700Å JHK JHK +L(NB) 3300-9700Å 3700-9700Å 3500-11000 Å 3300-9700Å JHK JHK +L(NB) 3500-9700Å Range Spectral Note See 20.0 ‘ 5.2’ IFU IFU NA 3.4’ 10.3’ 2.0’ 5.4’ 5.4’ Slit 0.43 0.61 0.68 0.305 0.11 0.11 0.14 0.32 0.39 0.26 (“/pixel) Scale Fiber (2.5’’) ~82 fibers ~90 fibers ~100 fibers single/multi single/multi single/multi single/multi Multi-object 59’ 20.0’ 5.8’ 10.4’ 4.6’x3.8’ 9.3’ 9.3’ 10.3’ 3.3’ 35.4’ Field Observational Programs
Gemini Instruments Possibly Available for 2007A*
GEMINI NORTH Detector Spectral Range Scale (“/pixel) Field
NIRI 1024x1024 Aladdin Array 1-5μm 0.022, 0.050, 0.116 22.5”, 51”, 119” R~500-1600 NIRI + Altair (AO) 1024x1024 Aladdin Array 1-2.5μm 0.022 22.5” R~500-1600 GMOS-N 3x2048x4608 CCDs 0.36-1.0μm 0.072 5.5’ R~670-4400 5” IFU
Michelle 320x240 Si:As IBC 8-26μm 0.10 img, 0.20 spec 32”x24” R~100-30,000 43” slit length NIFS 2048x2048 HAWAII-2RG 1-2.5μm 0.04 x 0.10 3” x 3” R~5000 NIFS + Altair (AO) 2048x2048 HAWAII-2RG 1-2.5μm 0.04 x 0.10 3” x 3”
R~5000
GEMINI SOUTH Detector Spectral Range Scale (“/pixel) Field
GNIRS 1Kx1K Aladdin Array 1-5.5μm 0.05, 0.15 3”-99” slit length R~1700, 6000, 18000 5” IFU
GMOS-S 3x2048x4608 CCDs 0.36-1.0μm 0.072 5.5’ R~670-4400 5” IFU
T-ReCS 320x240 Si:As IBC 8-26μm 0.09 28” x 21” R~100,1000 Phoenix 512x1024 Aladdin Array 1-5μm 0.085 14” slit length R ≤70,000 bHROS 2048x4608 CCD 0.4-1.0μm 0.7” or 1” fiber R~150000 NOAO-NSO 87 Newsletter Acquisition Camera 1Kx1K frame-transfer CCD BVRI 0.12 2’ x 2’
* Please refer to the NOAO Proposal Web pages in September 2006 for confirmation of available instruments. * Due to time trades, Gemini time is also available with HIRES on Keck and with Suprime-Cam and MOIRCS on Subaru.
September 2006 19 NOAO-NSO Newsletter 87 20 5 4 3 2 1 Classical or service, alternating orClassical 7-night service, If runs. proposing requests for for classical observing, 7nights are strongly preferred. may only—Observers asked be to execute observing upClassical night to 1hrper of monitoring projects have which transferred been Proposers optical considered the need only be who will for request Note 1.0munlessthey the otherwise. that data from both only. observing Service The amount timescience of available (i.e.on SOARClassical between 40-60%. visitor) the be is only will in2007A observing region of interest. to telescope this from 1.3m. Inacorresponding the be there case, this will increase time. scheduled inthe No filters, specialty no ANDICAM imagers is binned 2x2. offered mode observing for NOAO proposals. Observational Programs 1.3-m CPAPIR IRImager 1.5-m OSIRIS IRImaging spectrograph ImagerOptical 4-m SOAR ISPI IRImager Mosaic IIImager 4-m BLANCO Imaging SpectrographCass 1.5-m OSIRIS IRImaging spectrograph 4-m SOAR R-C Spectrograph CCD Hydra +Fiber Spectrograph 4-m Blanco Spectroscopy Direct Imaging 0.9-m Direct Imaging 1.0m ANDICAM Camera Optical/IR 4 5 2 3 2 2 September 2006 September 1 1 CTIO Instruments Available for 2007A SITe 2Kx2KCCD Fairchild 4Kx4K CCD HgCdTe 1Kx1KIR Fairchild 2Kx2K CCD HgCdTe 2Kx2K HgCdTe 1Kx1K E2V 4Kx4KMosaic HgCdTe (2Kx2K1.0-2.4μm) Mosaic8Kx8K CCD Detector 1200x800CCD,Loral 3100-11,000Å HgCdTe 1Kx1K,JHKwindows 3Kx1KCCD,Loral 3100-11,000Å SITe 2Kx4KCCD, 3300-11,000Å Detector 0.3 0.27 (“/pixel)Scale <1300 1200, 3000 300-5000 300-2000 Resolution 0.40 0.29 0.11 0.17 0.9 0.14, 0.35 0.08 11’ 36’ Field 7.7’ 1.3’, 3.3’ 5.5’ 138 fibers, 2” aperture Slit 13.6’ 20’ 2.0’ 5.8’ 30’ 1.3’, 3.3’ 5.5’ Observational Programs
Keck Instruments Available for 2007A Detector Resolution Spectral Range Scale ("/pixel) Field Keck I HIRESb/r (optical echelle) Tek 2048 × 2048 30k-80k 0.35-1.0µm 0.19 70” slit NIRC (near-IR img/spec) 256 × 256 InSb 60-120 1-5µm 0.15 38” LRIS (img/lslit/mslit) Tek 2048 × 2048 300-5000 0.31-1.0µm 0.22 6×7.8’
Keck II ESI (optical echelle) MIT-LL 2048 × 4096 1000-6000 0.39-1.1µm 0.15 2×8’ NIRSPEC (near-IR echelle) 1024 × 1024 InSb 2000, 25000 1-5µm 0.18 (slitcam) 46” NIRSPAO (NIRSPEC w/AO) 1024 × 1024 InSb 2000, 25000 1-5µm 0.18 (slitcam) 46” NIRC2 (near-IR AO img) 1024 × 1024 InSb 5000 1-5µm .01-.04 10-40” DEIMOS (img/lslit/mslit) 8192 × 8192 mosaic 1200-10000 0.41-1.1µm 0.12 16.7×5’ OSIRIS (IR IFU w/AO) 2048 × 2048 3800 1-2.4µm 0.02-0.10 0.32x1.28”- 3.2x6.4”
Interferometer IF (See http://msc.caltech.edu/so ware/KISupport/) HET Instruments Available for 2007A Detector Resolution Slit Multi-object LRS (Marcario low-res spec) Ford 3072 × 1024 4100-10,000Å 600 1.0”-10”×4’ 13 slitlets, 15” × 1.3” in 4’ × 3’ eld 4300-7400Å 1,300 1.0”-10”×4’ 13 slitlets, 15” × 1.3” in 4’ × 3’ eld 6250-9100 Å 1,900 1.0”-10”×4’ 13 slitlets, 15” × 1.3” in 4’ × 3’ eld MRS (med-res spectrograph) (2) 2K × 4K, 4200-9000 Å 7,000 2.0” ber single 9,000 1.5” ber single HRS (high-res spectrograph) (2) 2K × 4K 4200-11,000Å 15,000-120,000 2”or 3” ber single
MMT Instruments Available for 2007A Detector Resolution Spectral Range Scale ("/pixel) Field BCHAN (spec, blue-channel) Loral 3072 × 1024 CCD 800-11,000 0.32-0.8µm 0.3 150” RCHAN (spec, red-channel) Loral 1200 × 800 CCD 200-3,000 0.5-1.0µm 0.3 150” MIRAC3 (mid-IR img, PI inst) 128 × 128 Si:As BIB array 2-25µm 0.14, 0.28 18.2, 36” MegaCam (optical imager, PI) 36 2048 × 4608 CCDs 0.32-1.0µm 0.08 24’ Hectospec (300- ber MOS, PI) 2 2048 × 4608 CCDs R ~1K 0.38-1.1µm 0.9 60’ Hectochelle (240- ber MOS, PI) 2 2048 × 4608 CCDs R ~ 32K 0.38-1.1µm 0.9 60’ SPOL (img/spec polarimeter, PI) Loral 1200 × 800 CCD 0.38-0.9µm 0.2 20” ARIES (near-IR imager, PI) 1024 × 1024 HgCdTe 1.1-2.5µm 1.1, 2.1 20”, 40” CLIO (med near-IR imager, PI) 320 × 256 InSb 3-5µm 0.05 15.5” × 12.4”
Magellan Instruments Available for 2007A NOAO-NSO 87 Newsletter Detector Resolution Spectral Range Scale ("/pixel) Field Magellan I (Baade) PANIC (IR imager) 1024 × 1024 Hawaii 1-2.5µm 0.125 2’ IMACS (img/lslit/mslit) 8192 × 8192 CCD R~2100-28000 0.34-1.1µm 0.11, 0.2 15.5’, 27.2’
Magellan II (Clay) MagIC (optical imager) 2048 × 2048 CCD BVRI, u’g’r’i’z’ 0.07 2.36’ LDSS2 (mslit spec/img) SITe#1 CCD R~200-1000 0.4-0.8 µm 0.38 6.4’ MIKE (echelle/multi spec) 2K × 4K CCD R~19000-65000 0.32-1.0µm 0.14 30’ (~200 bers)
September 2006 21 CTIO/CERROTOLOLO INTER-AMERICAN OBSERVATORY Dark Energy Survey Passes Fermilab Review
Timothy Abbott
he Fermilab Director’s CD-1 Review of the Dark mechanical system, using a hexapod to drive a large mass to higher Energy Survey/Camera project (equivalent precision than previously attempted in astronomy, but no major to a Conceptual Design Review) was impediments have been identified. Theld 25–27 July 2006 at Fermilab in Batavia, IL. Project staff gave a range of presentations on Significant work remains in the areas of survey science and design, camera design, cost, instrument control and integration with schedule, and management to a committee of CTIO facilities, although CTIO has done physicists and astronomers with a wide range of much to improve the performance of expertise in the development of instrumentation the Blanco 4-meter telescope. While the projects. The committee close-out report states Dark Energy Survey has been predicated that the project is in good health, and should on the current performance of the Blanco move on to the US Department of Energy + Mosaic II imager, DECam is expected to CD-1 approval stage immediately, and to the improve significantly on this combination. CD-2 review next year. The committee urged that a high priority be placed on DECam commissioning at the Detector packaging and testing facilities are now Blanco in 2010. well established at Fermilab, and a solid base of expertise has been developed. Monsoon detector controller development is Further details on the instrument design can be found well in hand, and the optical design for the Dark Energy Camera in the proceedings of the May 2006 SPIE meeting in Florida, (DECam) is now mature and ready to move into vendor selection. where the instrument team presented several papers. The instrument design explores new territory for the opto- (Image Credit: R. French Leger/Fermilab)
Blanco Update
Timothy Abbott
fter suffering an extended shutdown in October-November 2005, the V. M. Blanco 4-meter telescope has shown considerable improvement in performance. Initial efforts Ato repair and retune the broken radial supports were frustrated when the telescope was reassembled at the end of October, and four additional supports failed within a short period. CTIO staff quickly identified the problem and resolved it. A single radial support did fail again immediately after the second reassembly, but the cause is known and no others have failed since.
Tests have shown that the primary mirror is no longer moving around in its cell, and coma has been relegated to third place (after spherical and astigmatic aberration, not including defocus) from its previous number one position. The measured coma is also stable, and the majority of the remaining measurable translations between the primary mirror and prime focus appear to be the Improvment in image quality obtained at the Blanco result of flexure of the telescope structure. The improvement 4-meter telescope by the SuperMacho program, semester 2005B, in performance is reflected in the figure, showing the change in air-mass corrected, VR filter. Dates: 5 September 2005–31 December seeing distribution before and after the shutdown, as found in data 2005. Light color: pre-shutdown, darker color: post-shutdown, with from the SuperMacho program, which is obtained under similar approximately equal number of exposures (~580) each. conditions throughout.
22 September 2006 CTIO
SOAR Update
Steve Heathcote
s of July 2006, the SOAR team is busy making the CCDs were unsuitable for science use. A crash program is final preparations for the start of regular science currently under way to procure a new detector package, operations, with the first NOAO users scheduled consisting of a custom version of a camera manufactured by Ato observe at the telescope in mid-August. In all, Spectral Instruments containing a 4K x 4K Fairchild CCD 42 percent of semester 2006B time is scheduled for science 486. Work on commissioning the spectrograph itself, using use, with the rest of the time scheduled for ongoing the current detector package, will continue in parallel in order commissioning work. to minimize the time required to bring the instrument into service, once the new camera is delivered. Looking ahead to the 2007A semester, we anticipate scheduling 50 percent of the time for science (with a goal of Meanwhile integration and testing of the Spartan infrared 60 percent) so that approximately 27 nights will be available camera continues at Michigan State University, with delivery through the NOAO Time Allocation Committee. Again, to Chile and the start of commissioning now expected to take the instruments available will be the SOAR Optical Imager place toward the end of this calendar year. and the OSIRIS near-infrared imaging spectrometer (see www.soartelescope.org for further information on these An update on the status of these two new instruments, and instruments). in particular a decision on whether or not they will be offered for the 2007B semester, will be provided in the March 2007 Progress on commissioning the Goodman spectrograph NOAO/NSO Newsletter. suffered a major set back when it was found that the NOAO-NSO 87 Newsletter
Credit: M. Urzúa Zuñiga/Gemini Observatory
September 2006 23 NOAO-NSO Newsletter 87 24 leadership roles on roles leadership their of recognition “in Schmidt Brian T distance calibration based on the Calan/Tololo data, data, parameters. Calan/Tololo the cosmological measure to on campaign independent an began based calibration distance of these use the pursue to in the candles study of cosmology. 1994 TheSCP, using a in similar team SN High-z the started Schmidt and Suntzeff findings, these upon Based cosmology. in candles” “standard accurate most the them making percent, six accuracy of an of to supernovae method these to a distances discover measuring to used was light sample SNe This low-redshift curves. of sample first high-quality the uniform, provided Suntzeff, Nicholas Hamuy, and Mario Phillips, astronomers Mark survey CTIO also by Calan/Tololo was led The using (1990–1995), telescopes. indicators of CTIO basis distance with done the precise as forms SNe that Type-Ia work pioneering The acceleration. of the measurements with confirmatory SNe provided HubbleTelescope, which Space the redshift higher even of study the in leadership for his for recognized also was evidence Riess Adam member team SN High-z the Energy.” “Dark mysterious the derive and and acceleration distances cosmological Both measure to used Perlmutter. were that (SNe) Type-Ia supernovae the by led to discover telescope 4-meter Blanco CTIO the (SCP) used teams Project Cosmology Supernova High-z made the Search was (High-z by SN) team led universe by 1998 Schmidt, in and the accelerating contemporaneously the of discovery The Universe.” of the expansion of the rate the in an acceleration of discovery remarkable the made that teams two the
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KPNO/KITTPEAK NATIONAL OBSERVATORY
Collaborations Improve Capabilities of KPNO and Our Partners
Buell T. Jannuzi, Sylvain Veilleux (University of Maryland) & Jeremy King (Clemson University)
ith the encouragement and advice of the NSF, the AURA Maryland’s resources have supported the purchase of large optics Board of Directors, and the Observatory Council, Kitt for the NEWFIRM camera and helped in the procurement of Peak National Observatory (KPNO) has been working some key NEWFIRM components through competitive bidding to Wto continue support of its operations and improve its capabilities by outside contractors. Maryland resources enabled the acquisition of forming collaborations that further the scientific and educational a suite of narrow-band filters not otherwise in the baseline budget, missions of the National Optical Astronomy Observatory. We which will be available for use by the astronomical community. are happy to report the renewal of a successful partnership and Maryland personnel Rob Swaters, Brian Thomas, and Ping the formation of a new collaboration, both of which further the Huang are fully integrated into the NOAO pipeline and archive ability of NOAO to provide first-class observing capabilities to the development teams, and their participation has been essential to community and our partners. Several smaller instrumentation meeting the delivery schedule for the NEWFIRM system. collaborations are also continuing into FY 2007. The guaranteed access to the Kitt Peak Early in 2006, an external committee was telescopes provided to Maryland has had impaneled to review proposals for the a strong positive impact on the scientific formation of collaborations in support of productivity of the university’s department. NOAO 4-meter telescope operations, and The high level of interest in these facilities one proposal for the renewal of an existing necessitated the formation of an internal partnership to develop instrumentation for review committee to prioritize the requests KPNO. We thank the committee for their for telescope time. The Maryland users of the careful and thorough review of the proposals. KPNO facilities cover a broad cross-section Following the committee’s recommendations, of the department: nine professorial faculty, and past guidance from the Observatory seven postdocs and research scientists, and 11 Council, NOAO has finalized agreements graduate students have used these facilities with the University of Maryland and Clemson since semester 2003B. Of the 11 students, University. nine are using the telescopes in support of their PhD research. Renewal of the KPNO-University of Maryland Collaborative Agreement Science highlights include successful searches A partnership was established between for and studies of comets and asteroids (e.g., KPNO and the Astronomy Department at the the NASA Deep Impact Mission), detailed University of Maryland in 2003, following an ground-based follow-ups of star-forming Announcement of Opportunity in the March molecular clouds in our Galaxy mapped by 2002 NOAO/NSO Newsletter and a series of University of Maryland faculty and the Spitzer Space Telescope, and analyses of reviews (see the August 2004 Newsletter). undergraduate summer school students the mass distribution, star formation history, This partnership, judged to be beneficial to at Kitt Peak in 2004. and impact of nuclear activity in nearby and both parties, has served as an example for distant galaxies. Science results have already developing other new collaborations. appeared in more than a half-dozen publications, and several other papers are in preparation. The smaller KPNO telescopes have also The initial focus of the KPNO-Maryland partnership has been the served as excellent training tools for beginning students. A Kitt production of the NOAO Extremely Wide-Field Infrared Imager Peak summer school has been organized in 2004 (see photo) and (NEWFIRM) as a complete scientific system. This instrument 2005 to provide pre-thesis astronomy graduate students with some is scheduled to see first light in 2007. Maryland has provided hands-on experience at the facilities of KPNO. financial and in-kind support to this project in exchange for guaranteed access to 20 percent of science nights on the Mayall A proposal to extend the collaborative agreement for an additional 4-meter telescope (with possibility of trading for equivalent WIYN three years was submitted by Maryland in late 2005. The extension or 2.1-meter telescope time). proposal was reviewed as described above, and accepted in
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September 2006 25 NOAO-NSO Newsletter 87 26 renewal period. Maryland will contribute both financially financially both contribute will Maryland period. renewal Science NOAO the of for(NSA), Archive versions planned this represent major milestones expanded of release the and WIYN, (ODI)on Imager One-Degree the by followed The (QUOTA), advent of Transfer Arrary the QUad Council. Orthogonal the Observatory telescope, Mayall the on NEWFIRM of commissioning the the follow of agreement new recommendations this of terms The 2006. June Collaborations of KPNO and Our Partners continued in the US national system. US national the in telescopes optical other on nights for time 4-meter KPNO their of half exchange to astronomers Clemson allows also with needed funds. operating Signed in June, the agreement KPNO providing year, while each time observing telescope to access 10 guaranteed percent and with students of Mayall the new three-year agreement provides Clemson researchers Astronomy, and Physics of Department university’s the in with is presence CTIO) University. astrophysics Clemson a With growing with pending those (beyond panel our review by recommended KPNO for partnership new The Partnership KPNO-Clemson A New catalogs. and of images for analysis services Web new of construction and holdings, NSA queries enable the in to catalogs heterogeneous multiple across generic capability on query work catalog of continuation images, from NSA holdings of Mosaic and NEWFIRM of pipelines to create the higher-level data products to contribute development potential include the construction to continue of development areas of NSA. the The exciting most will Maryland Finally, effort. this arole in playing Maryland ODI, with highly the adapt of to demands QUOTA,the higher pipelines and eventually to be Mosaic/NEWFIRM the of framework will scalable and flexible effort collaborative the of component important another so pipeline, reduction data ODI QUOTAand the of implementation the and development in staff (DPP) Program Products Data NOAO of participation the welcomed consortium has WIYN The quality. data and processing data the monitor and pipeline the control to interface user the fine-tuning and to adding the documentation, pipelines, both for procedure installation the streamlining on focus will effort the of Much pipelines. reduction data NEWFIRM and Mosaic the finalize to be will priority software top The collaboration its through KPNO. projects with these to in-kind and KPNO September 2006 September
research opportunities at the university. university. at the astrophysics opportunities research graduate strengthening in Foundation Clemson Curry the of support generous resources. continuing the research appreciates greatly frontier and training, and extremely to commitment world-class basic inquiry, graduate education Charles Clemson’s an demonstrates Seneca-based agreement The by Foundation. the Curry from possible grant made $100,000 generous was partnership This lae otc Bel anz ( Jannuzi Buell contact Please to KPNO telescopes. instruments their in interested bringing teams Wewith collaborations are open to additional forming see KPNO; and STScI, Center, Flight Space Goddard NASA’s between collaboration Science a being Telescope instrument the with Space (STScI), Institute the of MacKenty John (IRMOS, and ideas new test to instrument new opportunities provide and with of community developers development the to the new capabilities bring agreements These further technology. important instrumentation vitally to but smaller collaborations form to continues of KPNO University the Continue Goddard and STScI, Florida, with Collaborations Instrumentation expressions of interest. expressions ufl.edu/ technology. technology. Clemson astronomers will use their guaranteed guaranteed their use will astronomers Clemson and interiors of stars in the Milky Way. For more Way.For Milky the in stars of interiors and hyper-energetic gamma-ray bursts, track the the of track origin bursts, the gamma-ray investigate hyper-energetic to access telescope www.noao.edu/manuals/flmn www.noao.edu/manuals/flmn evolution of supernovae explosions, determine determine explosions, supernovae of evolution ); and, the Infrared Multi-Object Spectrograph Spectrograph Multi-Object Infrared the and, ); information on at information astrophysics Clemson, see atmospheres the of physics the probe and stars, astro.clemson.edu www.noao.edu/manuals/irmos_perf.pdf of planets in circumstellar disks around other other around disks circumstellar in planets of h cmoiin f ihrdhf gs n the in formation the for gas search medium, intergalactic high-redshift of composition the Eikenberry and the University of Florida, see see Florida, of University the and Eikenberry with the Exoplanet Tracker (ET, Jian Jian (ET, Tracker time Exoplanet observing the we providing with agreements, currently of kinds are these Through .-ee tlsoe FAIGS (Steve FLAMINGOS telescope; 2.1-meter Ge and the University of Florida, see see Florida, and of University www.noao.edu/noaoprop/help/etmemo.html the and Ge www.astroufl.edu/et/ . [email protected] and ) on the KPNO KPNO the on ) flamingos.astro. ). ) with with ) www.
KPNO
NSF Grant Helps Fund Development of New Imager for WIYN 0.9-meter Telescope
Buell T. Jannuzi and Heidi Schweiker
he NSF has awarded a Program for Research and Education with Small Telescopes (PREST) grant to Con Deliyannis and the University of Indiana to Tsupport the development of a new wide-field imager for the WIYN 0.9-meter telescope on Kitt Peak, plus observatory upgrades and some new outreach activities.
While the KPNO Mosaic-I imager is already available for use at the 0.9-meter telescope for a portion of each observing semester, Mosaic is predominantly scheduled on the Mayall 4-meter telescope, leaving the 0.9-meter without a wide- field imager for most available nights. The NSF funds will enable the construction of the Half-Degree Imager (HDI).
HDI will use monolithic four-amp 4K x 4K CCDs with 15 micron pixels providing a 29 arcminute field of view sampled with 0.43-arcsecond pixels. HDI will be available to members of the WIYN 0.9-meter consortium On 27 June 2006, the WIYN 0.9-meter telescope was struck by (see www.noao.edu/0.9m/general.html) and the general lightning. Portions of the recently awarded PREST grant will be astronomical community. Approximately 10 percent of the used to improve the lightning protection of this observatory. telescope nights that HDI is scheduled will be available to the general community. There will also be public access to the WIYN 0.9-meter special observing queues (the long- term synoptic and “opportunity” queues).
Together with Mosaic, HDI will provide a competitive imaging capability in support of the scientific and education missions of the WIYN 0.9-meter. NOAO-NSO 87 Newsletter
The KPNO Mosaic camera is available for use with the WIYN 0.9-meter telescope (above), but is primarily used with the Mayall 4-meter telescope. With the 0.9-meter, Mosaic provides a When Mosaic is not scheduled on the 0.9-meter, the available one-degree fleld of view with approximately 0.6-arcsecond pixels. imager is the KPNO CCD S2KB, which is not competitive The new Half-Degree Imager, while providing only a 0.5-degree with the characteristics of the detectors planned for the field of view, will have smaller pixels (0.43 arcseconds), a better Half-Degree Imager. HDI will provide a wider field of view match to the good image quality provided by the telescope and than S2KB and a more sensitive system. the site.
September 2006 27 NATIONALSOLAROBSERVATORY TUCSON, ARIZONA • SAC PEAK, NEW MEXICO From the Director’s Office
Steve Keil
he NSO Long Range Plan, covering FY 2006 through FY with IRAO, remains a shared-risk user instrument, as filter and 2010, is now available on the NSO Web site (/www.nso. modulator tests continue this fall. edu/general/docs/). Upcoming major Tmilestones in the plan include commissioning ✴ of SOLIS in 2007, with the long awaited release of the SOLIS full-disk vector magnetograms. The NSO Users Committee met in Durham, More time than expected has been spent on NH, during the June AAS Solar Physics calibrating the vector data, but great care has Division meeting. The combined report from been taken to ensure that reliable data are that meeting and from the December 2005 released. A VSM vector working group has meeting is available at www.nso.edu/general/ recently been formed to finalize the vector data committees/. The committee highlighted the processing pipeline. importance of releasing SOLIS vector field data, given the imminent launches of STEREO The Advanced Technology Solar Telescope and Solar-B, and the expected synergism of (ATST) project approaches a major milestone these missions with the SOLIS project. this fall, when the NSF conducts a Preliminary Design Review with the aim of understanding ✴ all cost and management issues associated The current cooperative agreement between with construction of the ATST. A successful the National Science Foundation and AURA to review should result in the ATST project being operate NSO and NOAO is mid-way through forwarded to the Major Research Will Rogers with granddaughter Kyaa its five-year term. The NSF conducted a review Equipment and Facilities Construction Gilliam during the farewell gathering of AURA management in July to determine (MREFC) Panel for approval, and followed at Sunspot. whether the agreement should be renewed or by submission to the National Science reopened for competition. This review is one of several factors that Board (NSB) early next spring. The NSB will then decide if and when would enter into such a decision. NSO prepared a self-evaluation ATST should enter the MREFC queue, and its ranking with respect for the review and has participated in the panel review. Meanwhile, to other projects in the queue. This could then lead to funding in we await the report of the NSF Senior Review on all its ground- the 2009–2010 period. The ATST project will hold its next Science based facilities. This review could have broad impact on future Working Group meeting this October, with a meeting of members NSO long-range planning. of the newly forming ATST International Organization occurring shortly after. ✴
Other milestones that will greatly enhance This summer, NSO bid farewell to two observing capabilities at NSO include long-term staff at Sac Peak. William A. commissioning of the Diffraction-Limited “Will” Rogers retired from the facility Spectro-Polarimeter (DLSP) as a user crew at Sunspot, where he operated heavy instrument at the Dunn Solar Telescope equipment, ran the “one man” motor pool, (DST) in 2007. NSO and the High Altitude and generally assisted with facility projects. Observatory are jointly purchasing a Will has been with the observatory since new infrared camera for the Spectro- 1982, and he will be deeply missed. We Polarimeter for Infrared and Optical wish him well in his retirement. Kathy Regions (SPINOR). The DST observing Plum, who has served as cook at Sunspot crew is quickly learning the ins and outs for the past 11 years, had to leave her of SPINOR, which should become a user Kathy Plum with her farewell gift, a painting position due to health issues exacerbated instrument (no longer shared-risk) within by artist Wesley Keil. by the high altitude. Kathy’s excellent the 2007–2008 time frame. At the McMath- lunches and outstanding catering of meetings and workshops are Pierce, we are rapidly gaining experience in the near-infrared with well known throughout the solar community. Just as an army does, the NSO Array Camera (NAC). The combination of the NAC an observatory advances on its stomach, and Kathy will be missed with the infrared adaptive optics system (IRAO) is a powerful by all of us who have enjoyed her cooking. We hope that moving to tool for studying solar magnetic fields, as demonstrated by high- a lower altitude will quickly restore her health, and we wish her all resolution sunspot granulation videos collected in May. The NAC, the best for the future.
28 September 2006 NSO
ATST Update: Preliminary Design Review Scheduled; Refinements Made to Optical Design
The ATST Team
he NSF Division of (SDR) were conducted by the project the M2 and M5 (tip/tilt) mirrors, and Astronomical Sciences and in late 2005 and early 2006, covering the deformable mirror (DM) for the Office of the Deputy Director the telescope mount assembly, M1 high-order adaptive optics. Tfor Large Facility Projects will conduct assembly, enclosure, support facilities the Preliminary Design Review (PDR) and building, and site infrastructure. The wavefront correction system for the Advanced Technology Solar Instrument-focused SDRs have also encompasses several systems designed Telescope (ATST) in Tucson, Arizona been conducted. to “iron out the wrinkles” in the in October. The review committee will incoming solar image. At the heart of assess the progress of planning for the The MREFC process defined in the system is the high-order adaptive ATST project. The proposed ATST, a November 2005 stipulates that a optics (HOAO), with a DM that is four-meter aperture, off-axis Gregorian requirement for a project’s exit from reshaped so it is the reverse of the telescope with integrated adaptive the Readiness phase is the successful constantly changing, distorted lens optics and coronal capability, will be completion of an NSF conducted PDR. formed by Earth’s atmosphere. A used for high-resolution studies of the The PDR committee will consider our tip/tilt mirror compensates for gross solar atmosphere — the photosphere, site-specific design, major subsystems image motions caused by atmospheric chromosphere, and corona — with and their interconnections, cost turbulence and telescope vibration. emphasis on the generation and estimates, and risk analysis, evolution of magnetic fields that including contingency estimates. The optical arrangement of the ATST are key to our understanding of Upon successful completion of the has been refined in recent months to solar activity. NSF conducted PDR, the project will improve performance and incorporate be considered for submission to the recommendations from instrument Construction funds for the ATST would National Science Board (NSB) as partners and the Science Working come from the NSF’s Major Research early as March 2007, as a candidate Group. In the refined design, the DM Equipment and Facilities Construction for inclusion in a future NSF budget. has been moved from the M5 position (MREFC) account. The construction of Following positive NSB consideration, inside the elevation axis for the Optical the ATST is a specific recommendation Congress and the Office of Management Support Structure, down to M9 of a number of National Research and Budget will then determine when inside the support tower in the coudé Council-level studies, including the and if funding for ATST construction laboratory, with the tip/tilt mirror most recent astronomy and astrophysics will begin. Under reasonable current shifted to the M5 position. This shift decadal survey. The NSF has supported assumptions, the earliest start date for was an early recommendation of the the design and development of the ATST construction is FY 2009. Given Conceptual Design Review committee ATST facility and instrumentation the federal budget and appropriations in its report. since FY 2001 with funds from the processes, this would imply an divisions of Astronomical Sciences and initiation of construction funds early There are several advantages to Atmospheric Sciences. Both internal in calendar year 2009. the refined design, both from and external panels, including the performance and functional aspects. MREFC panel and the Mathematics A near-term milestone for ATST is the If the deformable mirror was at the and Physical Sciences Advisory release of the Draft Environmental top, which rotates with the telescope, Committee, have scrutinized the Impact Statement, scheduled for then the wavefront correction system NOAO-NSO 87 Newsletter project with respect to its scientific late August, to be followed by public would have to translate. With the DM relevancy, broader impacts, preliminary hearings in late September. The next in the coudé lab, compensation for management plans, and preliminary Science Working Group meeting will pupil rotation is no longer necessary. bottom-up cost estimate. NSF Director be held October 16–19 on Maui. Arden Bement promoted the project to As part of the shift, the tip/tilt mirror “Readiness” stage in September 2004. Meanwhile, the project has initiated was moved from M6 to M5. Because several industry contracts to further this mirror has a much smaller angle ATST design and planning have define aspects of the telescope design, of incidence, the beam footprint, and been reviewed by several external including work on the site-specific therefore the mirror dimension, can committees. Systems Design Reviews foundations, aspects of the heat stop, be significantly smaller. This reduces
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September 2006 29 NOAO-NSO Newsletter 87 30 concerned about meeting the the meeting are engineers about Project concerned mirrors. secondary M2 and analyses now tip/tilt M5 risk the on perform is to underway Germany) Instrumente (Waldbromm, Physik with contract A performance. tip-tilt improves turn in which optic, the of weight the experiments with two DMs at the the at DMs two leading with been experiments has Rimmele Scientist of Project Thomas end, field that To wider view. a over observations diffraction-limited (MCAO) providing optics system adaptive multi- conjugate a with form to replaced mirrors deformable be potentially they so could ago months several adjusted were positions mirror M8 and M7 The degrees Centigrade. –2 to 0 is also which mirror, the of control and thermal for essential is systems, liquid mitigation Risk analysis. performance and air include both may which evaluating control, thermal including of also mirror, deformable design M9 the mechanical is for proposals project The corona. all-reflective the of the observations for focus Nasmyth uses image the ATST stabilize when help to used be will which mirror, M2 the for similar analysis a loads. perform to predict will react company The will that mirror the models how develop Instrumente will Physik specifications, performance-based project’s the Using ambient. of Centigrade must back the at 0 to –2 temperature degrees the keep on jets air In addition, rates. high these at mirror the on pulling and pushing while the maintained be must stabilize performance to Optical , image. 200 second to per up times move arcseconds, must ±40 mirror rapidly, The Telescope. for Solar Dunn the on millimeters mirror tip/tilt 35 the to diameter, compared in as millimeters mirror, large 230 because relatively about a still is requirements M5 bandwidth ATST Update continued September 2006 September NSO imaging system. Sizing and uniform uniform and red/near-infrared Sizing system. two- and imaging a be blue to to expensive, in-one and proved slow which too system, zoom a lens from design switched recently systems was design VBI The also a summer. this review is for (VBI) scheduled Imager Visible the Broadband side, instrument the On of view. of field capability corrected the increasing substantially the the clearly experiments demonstrating the with with made, been has progress MCAO solar of development at Significant other just kilometers. nine to the two from altitudes telescope, turbulence the outside atmospheric focused on) (i.e., conjugated one Dunn: as the smaller filters). smaller the as area much as times nine to four (over precision greater requiring angstroms, 0.2 just of of bandpasses have will which some filters, centimeter-diameter 7.5 require will VBI The 10 angstroms. about of 5 bandpasses at with to centimeters, 2.5 used of diameters filters have Dunn band the narrow most as the of challenge, a be will coating with a minimum number of reflections. aminimum number with image smaller a forms which position, Nasmyth the at focused be can beam the Alternatively, instruments. light selected near-infrared to beam the steer to as well as and beams, visible the divide to M13 and system, wavefront correction the to light the of percent five pass to M12 beamsplitters: as act optics (MCAO) is performed. Two mirrors adaptive multi-conjugate high-order upgrade to future anticipated easy the mirrors when allow deformable will with replacement This kilometers, 11 atmospheric and respectively. 6 with at conjugate turbulence be to adjusted were M8 and M7 of Positions ATST. the of layout optical current The NSO
SOLIS
The SOLIS Team
nterest remains high in the SOLIS with a double major in physics and imagery to improve the treatment of vector spectromagnetograph (VSM) mathematics, and is taking this year VSM flat fields. Brittany left Tucson magnetograms. With the return to prepare for graduate school. Jessica following graduation, but her work was Ito nominal operation of the VSM has made great progress de-trending a good start toward more robust flat- instrument following modulator and removing instrumental artifacts field reduction. replacement, work has resumed in from VSM continuum images, and earnest on the vector algorithms. has improved limb-profile fitting and Our most recent data processing In addition to finalizing the vector modified overall radial fits to compensate assistant, Alex Toussaint, was hired in calibration procedures for the new for imperfect tracking across the disk. June. Alex graduated in May with a modulators, the Milne-Eddington Nathan Hadder will be working to major in mathematics, and was drawn inversion code is in the process of complete a third major in mathematics to this position by the opportunity to being updated to work with full-disk at the University of Arizona this fall, compress calibrated vector data using data. The original inversion code was in addition to already completed Hermite functions. Thus far, he has not designed to treat the full-disk, so degrees in physics and astronomy. He been exploring windowing techniques development time is needed to create has reprocessed longitudinal 630.2 to properly select lines and the and apply position dependent “quiet- nanometer photospheric magnetograms surrounding continuum. Sun” line profiles. from 2004 to include improvements Correlation between solar disk- integrated spectra from the Integrated Sunlight Spectrometer (ISS) and the McMath-Pierce Solar Telescope began this summer, with the help of NSO Research Experiences for Undergraduates student Tiffany Hayes (University of New Mexico). This initial investigation compares the parameters pertaining to width, intensity, integrated area, and position of absorption features within the Ca II K line. ISS resolution is approximately 50 percent higher than resolution at the McMath-Pierce spectrograph, but interpolation of both datasets enables spectral features to be measured identically. Figures 2 and 3 show Figure 1. SOLIS data processing aides Nathan Hadder, Jessica Goodman and Alex comparisons of K3 core intensity and Toussaint pause a moment from their work in the SOLIS area. All three are supple- the 1Å K-index from spectra acquired menting their studies at the University of Arizona with projects related to VSM during the first week of June at the ISS magnetogram data. and McMath-Pierce.
in dark subtraction and camera cross- Integrated sunlight Ca II K-line spectra NOAO-NSO 87 Newsletter Three data processing aides — Jessica talk elimination, and he streamlined have been acquired at the McMath- Goodman, Nathan Hadder and Brittany the offline data reduction process. Pierce scanning spectrometer for Shaw — joined the SOLIS team in early Nathan is currently revising the the past three decades. Correlation February 2006 to help reprocess and browser interface to allow quick search between spectra at the McMath- reorganize VSM longitudinal 630.2 and and display of VSM data based on user Pierce telescope and ISS provides an 854.2 nanometer data, and to remove queries, and translating code between important benchmark for ISS instrumentation artifacts and outliers programming languages. Brittany calibration, and achieves continuity from flat-field and continuum images. Shaw graduated from the University with the invaluable dataset obtained by of Arizona in May with a double major Bill Livingston (NSO) at the McMath- Jessica Goodman graduated in May in physics and astronomy. She applied Pierce in the multi-decadal program he from the University of Arizona her experience with open cluster CCD began in 1974. continued
September 2006 31 NOAO-NSO Newsletter 87 32 SOLIS continued that move the granules in the region surrounding the the surrounding flows region are the sunspot. small in as granules clearly, the seen move that is sequence, granulation time of two-hour evolution the During show to granulation. enhanced the highly arcseconds is 40 contrast about image The only figure, is across. view accompanying of field the the in which in shown is sequence time the from frame A view. of field entire the for correction wavefront the compute to sunspot small the used system optics adaptive IR sunspot The small 10880. number the region NOAA in around K-band the in sequence collected time was granulation two-hour a day, the During Moon. the and Jupiter, Saturn stars, including K-band, the in observed were objects nighttime to system the Several tests. forinitial from to relay these image camera an the removed slit in the used and was zeroth-order, grating diffraction the spectrograph; main the with conjunction in used was system optics adaptive I 0.1756. was point this at reference the intensity The and line. K the features, of wing of 3935.046red at the in taken Å was measurement to spectra both for point previous normalization spectra intensity ISS to applied were correction flat and subtraction Dark 2006. June 1–8 period time the during (open circles) scanning spectrometer photoelectric ISS SOLIS the and McMath-Pierce (crosses) with 2 Figures (left) and 3 (right). of Initial comparison K3 and core 1 intensity Å K-index for Ca II K at the McMath-Pierce facility. The infrared (IR) (IR) infrared The facility. McMath-Pierce the at telescope main the on system (NAC) Camera NSO the Array with done were tests imaging 2006, May n September 2006 September NSO Granulation Imaging in the K-band with the NSO Array Camera Matt Penn Matt
40 arcseconds across, and the small sunspot in region NOAA NOAA 10880 is visible. region in sunspot small the and across, arcseconds 40 about is view of 2006. field in May The facility McMath-Pierce the at NAC the system with 2.2 at imaged microns Granulation λ 3933 acquired spectra from
NSO
Successful First Summer School in Solar Physics
Dave Dooling
ore than 30 students and faculty attended the first of five, week-long Summer Solar Physics Schools held by the National Solar Observatory M(NSO) and the University of Arizona’s Lunar and Planetary Laboratory (LPL). The school was held June 11–16 at the NSO Sacramento Peak (Sac Peak) site in Sunspot, NM.
“This was a highly successful first session,” said LPL conference organizer Joe Giacalone. “We were fully subscribed and we were pleasantly surprised to find some faculty interested in attending so they could enhance how they teach solar physics.” The latter included two representatives from the Space Studies Department at the University of North Dakota, which is expanding its astronomy offerings. “I am the very model of a modern solar scientist.” Thomas Bogdan, director of the Space Environment Center The workshop was designed for advanced undergraduate in Boulder, responded to a challenge from the audience by and beginning graduate students interested in the physics reciting these words from General Stanley’s song in the Pirates of the Sun and possible careers in solar physics, space of Penzance. Bogdan described Major General Edward Sabine physics, or related fields. Lectures were given by Giacalone as a modern major general for his 1859 prediction that “In our on solar energetic particles, Rachel Howe and Rudi Komm present ignorance of the physical agency by which periodical (NSO) on helioseismology, Randy Jokipii (University of magnetic variations are produced, the possibility of discovery Arizona) on solar magnetohydrodynamics, Gordon Petrie of some cosmic connection which may throw light on a subject (NSO/Tucson) on the solar interior, Han Uitenbroek yet so obscure, should not be altogether overlooked.” (NSO) on radiative transfer, K. S. Balasubramaniam (NSO) on photospheric and chromospheric fields, and by Tom Bogdan (Director, Space Environment Center, Boulder, CO) on solar-terrestrial history.
Social activities included a pizza/stargazing party, a barbecue, a trip to White Sands National Monument, and a visit from a brown bear attracted to the breakfast foods available at one of the morning lectures.
The summer school was supported in part by a grant from the National Science Foundation. NOAO-NSO 87 Newsletter Summer 2006 Solar Physics School participants at Sunspot, NM.
September 2006 33 NOAO-NSO Newsletter 87 34 K Te ewr oeain staff operations network The our Sheffield, for UK. in meeting preparing biennial been major has staff I Experiences for Undergraduates Undergraduates for Research with worked Experiences Jain and Kiran Tripathy Sushant further summer, This being now predictors. weather space as developed are diagrams ring the mind, in this With velocity. associated subsurface of always pattern particular a with almost are strong flares of number large a regions producing helioseismology analysis, active that revealed recently ring-diagram local technique, Another signal. farside of the magnitude the important determining in an factor is sunspot the the of that area suggest results Preliminary visible. directly are active they when the regions of properties the to signal the comparing by signal farside the of calibration empirical an on working is Hernández González Irene sunspots. predict level the activity of to approaching signal farside the use to yet as way no is the there However, onto side. front Sun’s them brings rotation solar before weeks large two to up regions detect active can holography farside example, For goal. this to contribute modern certainly can local techniques of and helioseismic prediction, goals weather space the for tools develop to is helioseismology of One Highlights Science meetings. international of number a in participating globe, the GONG this, crisscrossing have been members team all of magnetogram top On a pipeline. constructing been has busy group processing data launch, the STEREO upcoming the and magnetograms improved and new the shelter of the anticipation In Learmonth. at swap completed successfully a variety of projects. The scientific scientific The projects. of variety a in quarter, engaged team busy GONG the very with a been has t September 2006 September NSO Rachel Howe, along with Satoshi Morita Morita Satoshi Howe, Rachel with along and Komm Rudi CME. a of onset to the prior occur rings the of widths amplitudes and the in changes distinctive (CMEs). Ejections haveThey that found Wet Mass ring- Coronal and of parameters diagram de study a on Stephanie University) (Rice student (REU) active region emergence. region active for large indicator A reliable a of search a in analyzed complex. being currently indeed is sample is statistical regions the of evolution temporal the and flows the between relationship the that confirm we regions, active four of sample small very case of AR10365, inthe downflows caseand to ofeven stronger AR10375. thisFrom during their disk passage. After new fluxtheemerges, flows change to upflows the in emerges flux new where by downflow characterized regions aging are left), (bottom (negative values) is present. The other two regions, AR10365 (top right) and the after AR10375isregion visible on the (days surface 302 shortly but emerges, region the while downflow or up- pronounced no shows right) AR10488(bottom of 70–74). (days location The emerges region the before values) (positive upflow an shows AR10314left) of (top location The surface. the below megameters 8.5 at the measured (squares) with velocity (stars) vertical area the region’sof the variation temporal by indicated regions, active four of evolution the compares figure The region. active the of evolution of state the on depending characteristics offlow less variety a see to depths expect we Thus at 10 about megameters. than surface the near shown downflows have exhibit regions studies active previous established addition, that In flows. subsurface in regions signatures active of pre-emergence for search to is approach one upflows, by accompanied typically isflux of the Sun.on magnetic the surface emerge they emerging Because Figure 1. One of the current goals of helioseismology is to detect active regions before Frank GONG Hill &the Team GONG on the surface. on the appeared flux magnetic the before days two upflowapproximately was detected results for one case, where an increasing emergence. Figure 1 shows encouraging region active of signs for flow search to field vertical subsurface the analyzed Agency), Aerospace Exploration (Japan – 308) the characteristic downflow 308) the characteristic continued
NSO
GONG continued
GONG staff mentored two participants School in Walker, LA, worked with improvement was the replacement of a in the Research Experiences for Gordon Petrie on solar wind predictions malfunctioning CCD camera. Teachers (RET) program this summer. using coronal hole maps derived from Charlene Olson, a physical science, SOLIS synoptic spectroheliograms and The major undertaking for this quarter integrated chemistry and physics magnetograms. was the replacement of the Learmonth teacher from Central Middle School shelter. The first group arrived on site in Kansas City, MO, worked with Cliff Network Operations & Engineering during the second week of May. People Toner on temporal variations in the Installation of the new magnetogram came and went as the work progressed, solar limb darkening to determine if the modulator hardware continued with a in response to the quantity of work shape of the Sun changes with the solar visit to Cerro Tololo in April. While and skills needed, until the instrument cycle. Dalfra Lynn Fleming, a physics, on site, preventive maintenance tasks became operational in the third week chemistry, and computer science were performed for the first time in of June. programming teacher at Walker High almost two years. One significant continued NOAO-NSO 87 Newsletter
Figure 2. This figure shows a portion of the new GONG monitor Web page, available at http://gong.nso.edu/monitor/ monitor.html, allowing a real-time assessment of instrument health network-wide. The page shows information about the operation of all of the sites in the GONG network at a particular time. The “monitor” shows the progress of data collection for each station over the previous three days and the information is updated every five minutes. The top panel shows the status of the sites including instrument mode, instrument computer load and disk usage, and the number of good and bad images collected during the current observing day. The lines in the middle panel represent the number of good images, as a function of time, for each site. The bottom panel shows the sky brightness as a function of time at each site. Clear days are visible as smooth curves, where cloudy days have a jagged appearance. Simultaneous coverage and duty cycle can also be inferred from the plots.
September 2006 35 NOAO-NSO Newsletter 87 36 Learmonth when the the at when installed Learmonth was hard- ware modulator new The August. in began chassis and rack the electronics of system Wiring Shop. Instrument the in done being work the of most with progress, in is Spare Hot the on Work GONG continued near-real-time magnetograms and and science STEREO the to maps synoptic magnetograms near-real-time 2006. August 31for nowscheduled launch, STEREO NASA the is development pipeline the is for driver The group’spriority. top the which pipeline, of magnetogram parts the various on working is team software the of majority The and Development Maintenance Software &Analysis Processing Data modulator. that realign to trip follow-up a prevented requiring installation alignment, proper Loa Mauna the at during weather poor that indicate being monitored, and results are sites the from Data sites. swap, GONG all at upgrade the of shelter installation the completing the after reassembled was instrument
September 2006 September NSO GONG will be GONG providing will and Ron Kroll. Ron and Sang Poczulp, Nguyen, Dave Villegas, Hauth, Gary Bert Dryden, Dave Montijo, Guillermo above, Luis, George right) to pictured left is (from with overlap, two and one be teams to team as together, largest The shelter. GONG new a of installation Tucson-based of the team initiate to Australia first in arrived the personnel operations 2006, GONG May 9 On 3. Figure consequently, we expect a significant backlog. significant and processing our in reduction a code, expect we Solaris consequently, current faster our times than several runs The port platform. Linux Linux the to pipeline the calibration in Solaris-based our of porting made being is progress Steady science. mission’s coronal the in role active an playing thus team,
tool” has been developed and and developed been quick a allows tool This implemented. has tool” monitoring Network “GONG new A (DSDS) distributed 1.5 terabytes in in terabytes requests. 21 to data response 1.5 distributed (DSDS) System Distribution and Storage Data the quarter, Last 106. Month through Frequency Mode are available Tables and Diagrams Ring 108-day 0.93. of
Data Operations Data the main GONG Web page. on link Status” the “Network through accessible is 2. Thetool figure in shown the of is 2006 July 20 for monitor view A remote stations. diagnosing the at be in problems to prove helpful also tool may The development. essential pipeline near-real-time for is which wide, of network-instrumenthealth assessment real-time 2005), with a fill factor factor fill 107 a with 2005), November Month 03 at (centered through GONG spectra and (36-day) power series time velocity month-long includes to date Processing
EDUCATIONALOUTREACH PUBLIC AFFAIRS AND EDUCATIONAL OUTREACH
The Dwarf Moves to a New Home
Hugo Ochoa & Dara Norman
ong-time visitors to Cerro Tololo will notice that one of the smallest domes has left the summit. This three-meter diameter dome housed “El Enano” or “The Dwarf,” as it was Laffectionately nicknamed: a commercial Cannon 50-millimeter camera lens (operated at f/1.6) mounted in front of a 1025 x 1025 Texas Instruments CCD with 12 micron pixels, for a field of view of 13 x 13 degrees.
The robotic telescope first appeared on Tololo in 1997 to begin observations for the Southern H-Alpha Sky Survey Atlas (SHASSA). The resulting atlas covers the entire southern sky south of +15 degrees declination to a brightness level of two Rayleighs (PASP, 113, 1326, 2001). For comparison, the faintest nebulosities visible on the Palomar Sky survey (POSS I) are about 100 Rayleighs. The atlas has also been used to confirm that the WMAP spacecraft survey of microwave background anisotropies was not being confused by foreground emission from Galactic hydrogen.
In 2002, a second phase of the project was begun to obtain images at the wavelength of [SII] emission lines for all those regions showing H-alpha emission. The brightness ratio of [SII]/H-alpha will differentiate between HII regions heated by ultraviolet light from stars and those heated by shock waves from supernovae.
In June of this year, El Enano was donated by John Gaustad (Swarthmore College) and Wayne Rosing (Las Cumbres Observatory Inc.) to the Centro de Apoyo a la Didáctica de la Astronomía (CADIAS, Center for the Support of Astronomy Education) and Colegio Seminario Conciliar (Conciliar Seminary School) in La Serena. CADIAS receives funding from NOAO and Gemini to conduct local astronomy outreach, and this group works closely with the seminary school.
The telescope currently resides at CADIAS in Altovalsol, a 15-minute drive from downtown La Serena, but it will eventually for Chilean students and amateur astronomers, and 3) to enhance be moved to Cerro Mayu, 25 kilometers east of La Serena, where awareness and protection of Chilean dark skies. Colegio Seminario Conciliar is building their new observatory. With additional support from the University of La Serena, El Enano While El Enano begins new life as an educational tool, Tololo looks will be used by local educational institutions for several purposes: forward to its sequel, El Enano II, for which there are plans to begin 1) to promote astronomical education and involve students in a third phase of the survey by gathering images of [OIII], which astronomical activities, 2) to develop high-level astronomy projects should aid in temperature determinations.
September 2006 37 NOAO-NSO Newsletter 87 38 the science of optics to the kids through entertaining entertaining through kids the to optics of science the onTohono the introduced Nation. O’odham The program T Observing Program. Program. Observing Nightly Center’s Visitor the in participate to National Peak Observatory Kitt to traveled weeks three first program the the over for record children attendance 18 the highest the 6, had July who On program). many the for as audience twice about target usual (the and 11-14olds as year olds year girls, seven-to-ten and boys of equal numbers approximately classes, were There students day. 22 each program of average participating an the with week of a twice aspect met which some children in 73 Club participated Girls and Boys Tucson South the At serving clubs southwestern students. American Native other to as well as in Club Tucson, Girls & Boys other to looking year also next the is in the expand project to The through locations. both continue at year will next programs HOO-based The in audiences. us younger with aid use for to materials these and adapting in settings, materials education our develop informal further different to chance a as well Clubs as Girls & outreach, local Boys effective for opportunity ideal these an provided at program the Establishing and infrared communications. laser and light, ultraviolet telescopes, mirrors, lasers, using activities HOO Module 3. Module HOO from 1.Figure built a using an Focusing telescope activity Public Affairs September 2006 September in the city of South Tucson and in the town of Sells, Tucson ofof town South Sells, the city in the and in went program on the road to the Boys & Clubs Girls (HOO) Optics NOAOHands-On the summer, his Hands-On Optics Engages Local Boys &Girls Clubs Stephen Pompea Stephen t OO Uiest o Aioa cec euain Ph.D. education science Arizona of University NOAO; at group outreach the in working students undergraduate four of consisted NOAO at team program Club Girls & Boys The “Tohono the with camp. day summer Truckof Love” O’odham association in Pisinemo, at event optics special a in participated NOAOteam HOO the Sells, in Club their raised at the Boys & Girls activities children hands. to In addition conducting the of percent 90 continue—likewise, program the having in interested be would many how asked then She hands. their raised children program— the of percent 90 HOO about the in participated had kids many how of well a show of also hands among in the dozen attendance three children was Club Girls & for asked director day, club program last the On the received. Boys Sells the at program The Stephen Pompea ( Pompea Stephen to on-optics.org go project, the about information more For (CO), Longmont Albuquerque, Boston. and Tucson, Baltimore, in the by fall team this conducted NOAO be also will and and CA, Angeles Livermore, Los in summer this offered were educators for workshops Optics Hands-On in states. seven in used classes school being is HOO after- in and country, the across centers International science and museums Engineering. SPIE–The Optical and for America, Society of Society the NOAO, Optical by created students school middle for education program informal NSF-sponsored an is Optics Hands-On Figure 2. An HOO demonstration of how a polarization filter works. effort. team the managed Walker, who Connie and Garmany, Katy Sparks, Rob NOAO members staff and project HOO Dokter; Erin Fellow GK-12 NSF and candidate or contact Hands-On Optics project director director project Optics Hands-On contact or [email protected] ). www.hands- Public Affairs
The Gemini Virtual Tour - Version 4.0
Peter Michaud (Gemini Observatory)
he Gemini Observatory Public Information and Outreach (PIO) office recently completed a new Tversion of its popular Virtual Tour CD-ROM. This new incarnation has several important additions, particularly the inclusion of Spanish language text and audio to make the tour entirely bilingual.
The new release (scheduled for duplication in September 2006) builds on the diverse educational content of the Virtual Tour, from simulated observations using actual Gemini data, to a Screen-Saver Maker that allows users to make a custom computer screen-saver from an assortment of spectacular Gemini images.
All of the elements of the previous tour have remained in this version. These include an interactive walking tour of a Gemini observatory (with hidden surprises), “news reports” updated from the Web, several games, and the Electromagnetic Radiation Explorer. As always, the tour can be installed on Mac or Windows computers, and is available in an entirely mouse-driven mode for bulletproof use in a public kiosk.
The addition of the Spanish translations was completed by Antonieta Garcia of the Gemini South PIO office, assisted by Guillermo Bosch of the Argentina Gemini Office, and Gemini Staff Astronomer Eleazar Rodrigo Carrasco Damele.
Plans are currently underway to produce a complete French translation of the program, in an effort led by Stephanie Coté of the Herzberg Institute of NOAO-NSO 87 Newsletter Astrophysics/National Research Council, Victoria, Canada.
To request a copy of the tour on CD-ROM, please send an email (including your postal mailing address) to [email protected].
September 2006 39 NOAO-NSO Newsletter 87 40 The CTIO REU program provides an exceptional exceptional career a an considering provides undergraduates program for REU opportunity CTIO The Foundation. Science National by the funded program under for the Experiences Research Undergraduates (REU) C star formation, variable stars, and and stars, variable nebulae, formation, planetary star populations, supernovae, stellar lensing, clusters, the galaxy as of gravitational such research members subjects on with staff, specific scientific collaboration local on close work in will projects, participants Student program. parallel a in participating undergraduates Chilean students alongside work REU These SOAR). and South, observatories Gemini (CTIO, international major three of environment stimulating the in place takes research This activities astrophysics. contemporary of research forefront the at substantive working scientists in with engage to science in
Credit: M. Urzúa Zuñiga/Gemini Observatory Zuñiga/Gemini M. Urzúa Credit: Tololo! Cerro on occasionally appear to known wildlife only the not are REU students Public Affairs September 2006 September assistant positions from January to March 2007 2007 March to January from research positions undergraduate assistant six offering anticipates (CTIO) Observatory Inter-American Tololo erro CTIO REU Program 2007 2007/reuad2007.html at online are Applications recommendation, official of letters information, 2006. three 2October than no later submitted be should to applicant two and necessary transcripts, all including applications, Complete cost. added an for compound CTIO Serena covered, housing and provided atfurnished La the AURA/ to costs travel roundtrip with full-time, are positions The 15 2007. to 24, March for January 10run approximately weeks will program The States. United or the of citizens residents be permanent must undergraduate and program, full-time REU the as during students enrolled be must Participants instrumentation. and telescopes art REU CTIO CTIO’susing state-of-the- experience for direct opportunities the provides and techniques, Additionally, observational emphasizes program medium. interstellar the [email protected]
. . For additional information, contact contact information, additional For . www.ctio.noao.edu/REU/ctioreu_