NOAO-NSO Newsletter Issue 78 June 2004
Science Highlights Cerro Tololo Inter-American Observatory A Luminous Lyman-α Galaxy at z=6.535 ...... 3 New Blanco Instrumentation...... 23 A Spectroscopic Survey for Superwinds in Retirement of the Blanco Echelle and RC Spectrographs...... 23 Massive Starbursts...... 4 A Wonderful Day for SOAR Dedication...... 24 Faint Galaxy Counts and the Normalization SOAR Sees Stars at Last ...... 25 of the Galaxy Luminosity Function ...... 5 Metal Hydride Opacities in Brown Dwarfs...... 7 Kitt Peak National Observatory Predicting the Maximum of Solar Activity e International Dark-Sky Association: A Critical with NSO Coronal Data ...... 8 Resource for Astronomy...... 27 e New OTAs Are Here!...... 30 Director’s Office Calypso 1.2-Meter Telescope Seeking A Long-Range Plan for Optical/Infrared Permanent Home...... 31 Ground-Based Facilities ...... 10 Workshop Updates Adaptive Optics Roadmap...... 11 National Solar Observatory/GONG NOAO Astronomer and Tohono O’odham Schools From the NSO Director’s Office ...... 32 Official Honored by IDA ...... 12 Working toward a Preliminary Design for ATST...... 34 SOLIS ...... 35 NOAO Gemini Science Center GONG...... 37 Gemini Update...... 13 Gemini Data Comes Online ...... 13 Public Affairs & Educational Outreach GNIRS Commissioning and System Science Education Highlights: Frenzied Teachers Verication Go Well...... 15 in Atlanta and a Telescope Building Challenge NGSC Instrumentation Program Update ...... 17 for Students...... 40 Undergraduate Students Join in CTIO Research ...... 41 Observational Programs KOLD CBS-TV Live Weathercast from Kitt Peak...... 42 2004B Proposal Process Update...... 19 NOAO Hosts Math, Science, and Technology 2004B Instrument Request Statistics by Telescope...... 19 Fun Fest Booth at TCC ...... 43 2004B TAC Members...... 22 Tohono O’odham Family Night on Kitt Peak...... 43 e Road to Pachón...... 44 is issue of the NOAO/NSO Newsletter is dedicated to Jurgen On the Cover Stock, who passed away in Merida, Venezuela, on 22 April 2004. is image is a color-coded picture of the archetypal starburst galaxy M82. It shows the horizontal stellar Dr. Stock arrived in Chile in late spring 1959 and organized a disk of the galaxy, which harbors its active star telescope site-testing program together with University of Chile formation, and a perpendicular supergalactic wind personnel. Among the mountain sites they tested (carrying of ionized gas powered by the energy released in the instruments on mule back) were Morado and Tololo. He the starburst. then served as the rst director of Cerro Tololo Inter-American To make this image, data from the WIYN 3.5-meter Observatory from April 1963 to December 1965. telescope on Kitt Peak were combined with data from the WFPC2 camera on the Hubble Space Telescope. Purple represents emission in ionized hydrogen (Hα) and ionized nitrogen, and the green is ionized sulfur in the WIYN data. In the HST image, these colors refer to Hα and nitrogen separately.
ese data are being used in a study of the connection between structures within M82 and its galactic superwind. is image was rst presented at the “Essential Science in Hubble’s Final Years” symposium, held 3–6 May 2004 at the Space Telescope Science Institute.
e WIYN 3.5-meter and 0.9-meter telescopes on Kitt Peak are operated by a consortium of the University of Wisconsin, Indiana University, Yale University, and the National Optical Astronomy Observatory (NOAO).
Image Credit: Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin- Madison), Linda Smith (University College London), WIYN/NSF, NASA/ESA.
HH 666: e Axis of Evil in the Carina Nebula “We report the discovery of the iniquitous parsec-scale outow Herbig-Haro 666 The NOAO-NSO Newsletter is published quarterly [HH 666]—the rst protostellar jet in the Carina Nebula—as well as the infrared by the National Optical Astronomy Observatory identication of its embedded driving force. P.O. Box 26732, Tucson, AZ 85726 Condemned to toil in the inferno of the Carina Nebula, scorched by [ultraviolet] radiation from the hot stars that power the HII region, much of the jet is inuenced by Douglas Isbell, Editor radiative excitation.
Infrared images reveal a reddened star embedded in the molecular globule lying along the Section Editors jet axis. We identify this evildoer (HH 666 IRS) as the likely driving source of the jet. Joan Najita Science Highlights Herbig-Haro objects are emission nebulae that result primarily from shocks in the Dave Bell Observational Programs outowing jets from young stellar objects. ese outows are an integral part of Mia Hartman Observational Programs the accretion process for low- and intermediate-mass stars and thus give us a direct Nicole S. van der Bliek CTIO indication that star formation is still occurring nearby. So far, no such jets have been KPNO reported in the inhospitable Carina Nebula. Richard Green Ken Hinkle NGSC e chain of HH objects that comprise the devilishly elusive outow HH 666 is seen in Sally Adams NGSC narrowband optical and infrared images. John Leibacher NSO NSO [In summary], the diabolical protostellar outow HH 666 is a spectacular bipolar jet Priscilla Piano emerging from a molecular globule and is made up of several twisted knots and large Douglas Isbell Public Affairs & bow shocks. ese all conspire to form a single coherent outow…” Educational Outreach
—Selected excerpts from a May 2004 Astronomical Journal paper by Nathan Smith, John Bally, and Kate Brooks, using data acquired at NOAO South Production Staff Stephen Hopkins Managing Editor Have you seen an interesting comment in the news or heard Mark Hanna Digital Processing one during a NOAO-related meeting or workshop? Please Pete Marenfeld Design & Layout share them with the Newsletter Editor ([email protected]). Kathie Coil Production Support
2 June 2004 Science Highlights
A Luminous Lyman-α Galaxy at z=6.535
Based on a contribution solicited from Sangeeta Malhotra & James Rhoads (Space Telescope Science Institute)
ames Rhoads, Sangeeta Malhotra, and their collaborators have recently discovered a Lyman-α J(Lyα) emitting galaxy at z=6.535 in the Large Area Lyman Alpha (LALA) survey at Kitt Peak. is galaxy, and the other results of this survey, may provide new insights into the nature of the reionization epoch in the very early universe.
e LALA survey identies candidate Lyα-emitting galaxies based on wide- eld imaging in a set of narrowband and broadband lters. Emission line candidates at z=6.5 were selected by comparing a 9200 narrowband image with a continuum image obtained in the z´ lter. Long exposures, made with the Mosaic I camera on the Mayall 4-m telescope, were needed to identify the galaxy at z=6.535; the 9200 narrow- band image has a total integration time of 28 hours. Blue continuum images from the NOAO Deep Wide Field survey (Dey and Jannuzi; www.noao.edu/noao/ noaodeep) were used to distinguish high- redshi Lyα emitters from foreground [OII], [OIII], and Hα emitters. is strategy has proven successful in Spectrum of LALA J142442.24+353400.2, obtained with the GMOS spectrograph on earlier LALA searches at z=4.5 (see the Gemini North in nod-and-shuffle mode. The net integration time was 5 hours. December 1999 NOAO/NSO Newsletter), The solid histogram shows the measured flux; the dotted line shows the 1-σ flux and z=5.7. uncertainties. The asymmetry of the line is clearly visible. There is no emission at 9072Å, where the [OIII]4959 line would be expected if the 9160Å feature were ese selection criteria yielded three due to [OIII]. z=6.5 candidates that were then studied spectroscopically with Gemini North asymmetry; and a complete absence of matches the expected number density 11 + GMOS and/or Keck II + DEIMOS other emission lines in the spectrum. of 10 M§ halos at z=6.5 in a Press- through time allocated by the NOAO is places it at z=6.535. e second Schechter structure formation model. Time Allocation Committee. Two of object, LALA J142441.20+353405.1, is
the three sources were conrmed as identied as an [OIII] emitter at z=0.824 e Lyα line in LALA NOAO-NSO 78 Newsletter single, narrow emission line sources at based on a weak detection of the [OIII] J142442.24+353400.2 may have the wavelengths near 9160 (source LALA 4959 line in the Keck DEIMOS and highest luminosity and equivalent J142442.24+353400.2) and 9136 Gemini GMOS spectra. width yet found at z=6.5. e source (source LALA J142441.20+353405.1). SDF J132415.7+273058 (Kodaira e line in LALA J142442.24+353400.2 Given that only one z=6.5 source was et al. 2003) has about the same shows all the hallmarks of high- found in one-third of a square-degree, luminosity within the uncertainties, redshi Lyα emission: large equivalent the source likely corresponds to a and an equivalent width near width (>530 in the observer frame); high peak in the matter distribution: the 2-σ lower bound for LALA a strong and statistically signicant one object per survey volume roughly J142442.24+353400.2.) e luminosity
continued
June 2004 3 NOAO-NSO Newsletter 78 4 e high Lyα luminosity and and luminosity Lyα high e local object. for this the also holds universe in expected formation star and photons Lyα between conversion M >11 of rate s Ω with 1.1×10 is A Luminous Lyman-α continued Galaxy massive galaxies with the highest star formation rates. formation star highest the with most galaxies massive the in winds about little know we Finally, redshi). studied been (except at high very universe not outside of local the extensively have superwinds these incorporate Furthermore, of that winds. evolution simulations and to formation input the galaxy as important is knowledge hosting Such quantitatively. established galaxies be to yet have the winds these of properties the frequency and and occurrence of properties their between winds, relationship the galaxy-scale of knowledge increasing our Despite Way’s decit. baryon Milky the produce ellipticals, and of of forlow-mass account galaxies, under-production the relation mass-metallicity the explain levels, observed to medium intergalactic the heat and pollute may I intrinsic some by or and 2001), Malhotra Rhoads (e.g., sphere ow Stromgren galaxy’s Hubble parent their the traversing while in redshiing either by IGM, the encountering redshied before substantially are Lyα the photons if only avoided be can effect an Such (IGM). medium intergalactic neutral a in embedded when ux line their of attenuation considerable suffer may neutral galaxies by Lyα-emitting hydrogen, scattered resonantly are some photons Lyα regard Because reionization. with suggest to possibilities width interesting equivalent -1 Science Highlights Mpc cure” to cosmology’s ailments. Mechanical feedback feedback Mechanical ailments. cosmology’s to cure” “miracle a as hailed been has nuclei galactic active and n feedback recent from star years, mechanical formation -1 m . is implies a star formation formation star a implies is . =0.27, =0.27, Ω 43 rs s ergs June 2004 § yr Λ -1 A Spectroscopic Survey for Superwinds in =0.73, and H and =0.73, -1 (using a cosmology cosmology a (using , assuming that the the that assuming , 0 David Rupke &Sylvain of Maryland) Rupke (University Veilleux David =71 km =71 km LALA J142442.24+353400.2 would would like J142442.24+353400.2 source a LALA universe, neutral a In observed. none are and image, z´ lter LALA the in detected be brighter to a ought neighbors such of any neighbor, sphere occupy Stromgren principle the in could object the While sphere. optical Stromgren the outside center line t τ~4 depth a in imply 10 for would of lifetime source a ionizing given the source radius, t in 0.3 Mpc sphere Stromgren a should produce ionizing LALA~J142442.24+353400.2 e 2003). Santos (e.g., wavelength line emitted the and galaxy parent the of velocity systemic the between offset the absence of such a redshi. e e redshi. a such of absence the >400 and Santos, by suggested as width >120 equivalent intrinsic an require Massive Starbursts even if the Lyα line is redshied redshied is line Lyα the if even 7 -1/3 due to the neutral IGM neutral the to due rate in individual galaxies. Normalizing the mass outow outow mass the Normalizing galaxies. individual in rate complex with outow and mass the outow velocities tted to proles determine be can with feature is galaxies for redshis. modest micron 1 below located conveniently is which doublet, λλ5890,5896 D NaI the of spectroscopy line absorption- use we winds, these of properties the Toprobe star in range dynamic of magnitude). orders a of two rate formation to (leading rates lower formation with star galaxies of sample z=0.5, complementary a to as up (ultraluminous well redshis as rates with ULIRGs) or formation galaxies, star infrared interacting high of number with large a galaxies of consists sample galaxy galaxy Our preparation). in host 2004a,b, Sanders and Veilleux, of Rupke, function 2002; a Sanders and Veilleux, (Rupke, as redshi and properties statistical properties for starburst-driven wind searching in of galaxies, trends 75 survey over large in a superwinds conducting are We 7 t 7 yr, and and yr, in in 7 1/3
ese results have been accepted accepted the been in publication have for results ese at galaxies redshis. these Lyα of samples statistical yield will that surveys future and through measurement) rm a with width replace equivalent on bound lower current should the and Telescope Hubble the Space with planned are (which J142442.24+353400.2 LALA of images broadband deeper may through rened reionization be on constraint e if at z=6.5. understood ionized mostly is Universe the easily this most of are object properties the z=4.5 us, the for sample. even high 2002). is latter Rhoads e and (Malhotra at z=4.5 distribution width equivalent Lyα observed the with consistent is former Journal . Astrophysical Astrophysical continued Science Highlights June 2004
5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 4 Science Highlights June 2004 that dominate the galaxy population in the local universe. universe. local the in population galaxy the dominate that spirals and ellipticals notclassical are the evolution, galaxies faint most luminosity that is emerged has physical that formation, result important An to merging. star and time) as cosmic such (over processes types morphological of A star lower ULIRGs with in galaxies in common than frequency) more detection (64% are superwinds that nd We RC the spectrograph, workhorse Spectrograph. its using 4-m the Peak with Kitt obtained were data our of half wind Over the efficiency”). in entrainment “mass (the entrained stars into turned gas gas the to relative interstellar of amount the of measure a yields then rate formation star global the to rate legend. inthe labelled are and repr symbols no different The rate. is There m the of galaxies. dependence infrared-luminous frequency starbursting detection of wind sample our in rate and formation star of function a as (top) (bottom) rate outflow Mass in Massive StarburstsSuperwinds continued and to relate apparent changes in the distributions distributions the in changes apparent relate to and galaxies faint of morphology the study to been (HST) has Telescope Space Hubble the of focus major Faint Galaxy Counts and the Normalization of the ass outflow rate on the star formation formation star the on rate outflow ass esent different redshift bins redshift different esent Galaxy Luminosity Function Seth Cohen (Arizona State University) State (Arizona Cohen Seth order for the models to match the observed galaxy counts, counts, galaxy observed the match to models the for order In no (LF). function assumed luminosity that galaxy local the models in evolution of galaxy predictions mag) the (B>23–25 over faint counts the of excess an was FBG is excess mergers. late- and peculiars, local to irregulars, spirals, similar type morphologies have that composed galaxies be of to found in was detected surveys, ground-based excess, earlier (FBG) galaxy faint-blue the Instead, changes signicantly with SFR). with signicantly changes wind the of radius the (unless secure be to appears SFR on dependence the but geometry, its and gas absorbing the of somewhat is extent spatial the of knowledge quantity of lack our given this uncertain of normalization overall e (SFR). rate formation star to proportional inversely is 0.01–0.1, and range the in generally is 1, than smaller much is ULIRGs these for efficiency in entrainment mass the that rate nd also outow We rate. formation mass star the with correlated the not is galaxies that shows gure e escape. to more likely be medium. will metallicity) intergalactic the of much the (carrying winds enter these in gas hot However,the and galaxy the will winds escape these in material neutral cold, the of little that v with of a galaxy on Signicantly, are velocity escape velocities less the these than (isothermal) km/s km/s. ~700 of limit 325–425 upper an are with average, outowing the are in velocities that maximum components e (45%). rates formation infrared-luminous AGNs (Rupke, Veilleux, and Sanders Sanders preparation). in and 2004c, of Veilleux, sample (Rupke, large AGNs a in infrared-luminous found those with compared be galaxies will star-forming the of sample and our from preparation), derived in results 2004a,b Sanders and Veilleux, A of complete (Rupke, data description these is forthcoming outow. the drive to of environment denser available of energy amount the reducing the therefore ULIRGs, in signicant be to likely are losses radiative Secondly, galaxies, winds. these the in obstruct may which gas less- molecular in of the concentrations is those large possibility obvious One than Why? superwinds galaxies. efficient luminous massive less much powering therefore in are ULIRGs in Starbursts c =200–300 km/s. Weconclude km/s. tentatively =200–300 Science Highlights June 2004 continued
5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 6 Faint Counts continued Galaxy in all four panels of the plot. Also apparent from the plot the from apparent Also plot. the of panels four all in seen be can excess galaxy faint the and model, nonevolving the is line solid lower e classier. three galaxy network neural the into articial automated classied an using shown been classes have morphological galaxies HST the of All Survey. Parallel B-Band WFPC2 30-eld own our and Fields Deep Hubble southern (WFPC2) and 2 northern the for Camera surveys Planetary and Wide-Field the using magnitude. HST from B-band results a combined our are squares black and as lled e counts type galaxy morphological of the for function results our shows gure e normalization the type. on morphological of factor dependence possible in the investigating particular data, ground-based and HST both using factor normalization this studied have I) and Jochen ESO, at Liske RSAA/ANU, at Driver Simon ASU, Rogier at Windhorst Observatory, of McDonald group at A Odewahn (Stephen cosmology. us adopted the of regardless mag, at B=18 two of almost by a factor normalized to be had they -ad aay ons s fnto o mrhlgcl ye Te oes hw rpeet ifrn aons f luminosity of amounts different represent shown models The evolution. The type. lower solid line morphological is the nonevolving of model and the upper solid function line corresponds to aluminosity evolving as (1+z) as counts galaxy B-band Science Highlights June 2004 other and line up nicely with the HST data. HST the with up nicely line and other each with well quite agree surveys results different three the these from that shows plot e eye. by assigned were data ground-based the for types Morphological work. HST the for we used that soware same the with uxes their measure could we that so images actual the had we Itthat essential was al.). et Liske (MGC; Catalog Galaxy Millennium degree elds MOSAIC square 30 Tyson),the and (DLS; seven Survey Lens Deep the Dey), from & Jannuzi (NDWFS; Survey Field NOAO Deep-Wide the from elds MOSAIC four used We seeing. good with B-band the in images wide-eld deep with surveys ground-based available publicly three utilized We ground. the from can cameras that wide-eld limit with achieved seeing be typical the near is which arcsec, one at B=18 ofmag is about size a average the galaxy Fortunately, issue normalization the mag. at B=18 study enough properly not to are there galaxies elds, bright WFPC2 30 with even that is continued 2 . Science Highlights June 2004
7 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 6 Science Highlights June 2004 a function of temperature and pressure, incorporating all all incorporating pressure, and temperature as of depth) function absorption a radial over integrated strength (line opacity the calculating by starts basically that stars L-dwarf for model a into fed then was information is reevaluated. initio ab of methods the using computed were factors McMath-Pierce Line-strength Observatory’s were positions Line to extrapolated high Solar Peak. Kitt at Facility National Telescope Solar the recorded spectra at laboratory transform Fourier high- the resolution from generated were CrH and FeH for lists Line Gibbs to the temperature) of densities. and column and abundances compute function a functions as formation of partition energy (i.e., free thermochemistry needed Reliable also CrH. is near-infrared and these FeH for of strengths transitions the line and requires positions dwarfs brown line L-type of distribution energy A the of bands (9969Å) 0–1 and (8611Å) 0–0 the and FeH of F the of bands (8691Å) 1–0 and (9896Å) and by by oxides of of presence the absence the 0–0 the metal characterized thus are dwarfs brown L-type objects. L early for 2000K below drops temperature photospheric the as fade which bands, VO and TiO strong by characterized are stars M-type sunspots. in seen be also can and stars M-type late F the of band vibrational 0–0 the is which band, Wing-Ford e FeH. and to part such as H large species by molecular absorption in due are features spectral metals, predominant alkali the the from these lines of absorption exception of atomic the strong with the temperatures 2000K, below surface fall the objects and substellar Since planets stars. gaseous M-type Jupiter-like between surface in gap temperatures the bridge dwarfs brown and T-type cooler dwarfs the L-type objects. substellar of identication the W for or any of for as the types a the population whole. e best that are show results data e ground-based redshi. with law power a as evolves luminosity type- that cosmology, assume they type-dependent WMAP and (1998),k-corrections, dependent measured al. et the Marzke from use LF models plotted e Faint Counts continued Galaxy 6 Σ + 4 –X Δ Mike Dulick (NSO), Adam Burrows (University of Arizona) & Peter Bernath (University of Waterloo) (University Bernath &Peter of Arizona) (University Burrows Adam (NSO), Dulick Mike i –X 6 quantum chemistry, and the thermochemistry was was thermochemistry the and chemistry, quantum Σ + 4 transition of CrH. e simulation of the spectral spectral of the of CrH. e simulation transition Δ r ad e hv bcm cuil pce for species crucial L-type hydrides become have numerous FeH transition-metal and CrH the the of dwarfs, brown discovery the ith i transition of FeH, makes its rst appearance in in appearance rst its of FeH, makes transition Metal Hydride Opacities in Brown Dwarfs J and no need for a normalization factor normalization a for need no v values using molecular constants. values constants. using molecular 4 Δ 2 O, CO, CH i –X 4 Δ i transition transition 4 , CrH,
was higher in the past. the in higher was rate merger the that indicate could this z≈1.5, is mag B=25 at redshi median the Since mag. B<24 at counts Sabc the and faint-end, the at counts Sd-Irr the of excess an as such (1+z) as evolves luminosity is one the where model (uppertypes for line) solid all tting scattering by mineral cloud formations, until agreement agreement achieved. is density ux absolute measured the until with formations, cloud mineral by scattering Mie with associated size particle and eld gravitational the including factors, controlling important other of number a and species the of abundances the with along pressure and gravity, temperature, effective the model adjust to e proceeds then spectra. L-dwarf in identied species known is trace] [red curve purposes.) display for offset Calculated intentionally (Note: FeH. and CrH for L5 dwarf, 2MASS-1507, using data spectrum a with synthetic actual an from spectrum opacity measured a of Comparison Science Highlights 2 . ere are some discrepancies, discrepancies, some are . ere June 2004 continued
7 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 8 been furnished by radiative lifetime measurements and and measurements lifetime radiative by furnished been have could information this principle, In factors. Condon Franck- computing for potentials internuclear upper-state and lower- the and function moment dipole transition the Einstein Calculating about information supplemental required levels rovibronic 2000K. temperatures to of for up especially analysis strengths, insufficient line was the calculating alone in from spectra metal-hydride amassed laboratory information Spectral Metal Hydride in continued Opacities Brown Dwarfs and 22 are measured to be 8.11° per year and 11.32° per per 11.32° and year per 8.11° be 21 to cycles in measured Poles are the 22 to and Rush 21 the of cycles slopes solar e for Poles 22. the and to Rush the shows 1 Figure cycle. solar of the maximum the of date the predicting for method new a invent to used been has and prominences, polar-crown in identied rst “Rush the to poles. phenomenon, Poles,”the is called was the near disappear features the time which at years, four or three of period a for maintained is motion is poles. the to move toward begin and appear features emission coronal high-latitude cycle, solar the in Early Peak. Sacramento at Observatory Solar National the of Facility Solar Evans W. John the at photometer coronal photoelectric the 1973with 13-times- ofsince obtained been have nm at 530.3 line (Fe XIV) iron ionized spectral the in Sun the of limb, or edge, visible the above at corona 0.15radii solar solar of the Scans cycle. solar of the phase rise the in early occurs maximum the of timing the of indicator another However, question. in maximum the preceding minimum solar-cycle the before or at occurring conditions predictions physical on based Most are etc. designers, space-system operators, P these addition, In levels. electronic rovibronic actual these the in reect coupling that calculating to factors restricted Hönl-London was strengths line determining high-level initio from ab directly information to missing attractive this more obtain it made spectra the vibrational from sufficient information of lack the and measurements such making Rydberg- with associated the obstacles e using method. Klein-Rees levels rovibrational the of inversion Science Highlights 11-year solar activity cycle is controversial among among controversial is cycle the activity of solar maximum 11-year the of date exact the of rediction solar scientists and of some importance to satellite satellite to importance some of and scientists solar Predicting the Maximum of Solar Activity with NSO acltos Uae f xeietl aa for data experimental of Usage calculations. June 2004 Dick Altrock (Air Lab) Altrock ForceDick Research A -values for the the for -values Coronal Data (2002); and M. Dulick et al., al., et Dulick M. and (2002); al., et Phys. Chem. Bauschlicher W. C. see information, detailed For cloud. mineral of the size temperature, particle and gravity, effective the in adjustment minimal through achieved was is agreement. good remarkably gave FeH, and CrH for data generated the using spectrum synthetic a the power of with to 1000, 1.2 at 0.84 μm from a region resolving an in recorded from gure), (see 2MASS-1507 spectrum dwarf, L5 opacity actual measured a of comparison A to up for FeH. temperatures especially for 2000K, function partition the calculate to to up energies with cm 10,000 states electronic low-lying the about information essential provided also calculations theoretical maxima, as defined by the sunspot number.the sunspot by defined as maxima, solar of dates the show lines vertical The lines. dashed as latitudes for isolated 22, above 51°. and 21 The linear to fits the Rushto the are Poles shown cycles activity solar or for periods scans 530.3 1.15nm XIV Fe usable solar-radii all of rotation maxima intensity local of of 27-day density the of months) average six (seven approximately north-plus-south averages the 189-day of Contours 1. Figure -1 above the ground states, which made it possible possible it made which states, ground the above 115, 1312 (2001); A. Burrows et al. al. et 115, 1312 Burrows (2001); A. ApJ , 594, 651, 594, (2003). ApJ continued , 577,, 986 J. Science Highlights June 2004
9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 8 Science Highlights June 2004 line) dates of solar maximum. of solar dates line) (solid 21 and actual and 22. are the predicted lines Vertical cycles from fits 1997 and July through data using 23 cycle solar for Poles the to Rush coronal predicted The 2. Figure between at 2000.3. occurred occurring maximum 23 cycle maximum 23 for cycle 1999.32 an average of and 2000.28, 1999.80 ±0.48. Actual the we nd lags, above the would apply then we If 2002.02. and 2000.76 e 2). point would from poles that reach the between gure extrapolation (see latitude 54° at 1997.58 the on to began Rush Poles the that estimate and slopes 23 above cycle the solar use we for maximum of date the predict To poles. the moveto toward began features 1997, emission In Fe XIV of 1.59 ±0.15 years. lag average an yielding respectively, maximum, solar aer years 1.44 and 1.74 or 1991.04, and 1981.64 on poles the reaches cycles these for Poles year. the to Rush the per to t ±1.61° extrapolated e 9.72° of average an for respectively, year, Predicting the Maximum of Activity Solar continued is work is supported by the Air Force Office of Office Force Air the by supported Research. Scientic is work is maximum. of solar date the predict to used be can years, ±0.20 1.52 lag, average the then and at date of poles to Rush the Poles, the the arrival the predict to used be can year, ±1.71° per 9.38° 23, through 21 cycles slope foraverage the or occurs, or 2009. that When 2008 in 1997.58, on onset cycle-23 its aer years 11 approximately apparent, Poles to Rush the becomes be when the made can For solar cycle 24, a of prediction the date of solar maximum does not improve of the accuracy the prediction. solar maximum. Including more data as the cycle progresses date ofthe for othermethods competitivedetermining with is method this us, minimum. solar preceding the aer years 1.2 only is which maximum, solar of ahead years 2.7 was -0.50 ±0.48 years. is prediction could have been made maximum solar-cycle-23of date predicted the in error e 21, 22, 23. and Figure 3. Fits to the coronal Rush to the Poles for solar cycles Science Highlights June 2004
9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO DIRECTOR’SOFFICE Director’s Office NATIONAL OPTICAL ASTRONOMY OBSERVATORY
A Long-Range Plan for Optical/Infrared Ground-Based Facilities
Jeremy Mould
n the most recent decadal survey, Astronomy and Astrophysics in performance gains can go like diameter of their primary mirror the New Millennium, the Astronomy and Astrophysics Survey to the fourth power); amateur astronomy in real-time eld of view; Committee outlined the next generation of astronomical and, Kodak lm in the ability to store information. e digital sky Ifacilities and stressed that “effective national organizations are and the virtual observatory, in which data mining is an essential essential to coordinate, and to ensure the success and efficiency of, adjunct to new observing, will revolutionize optical/infrared these systems. ese national organizations should work with the (O/IR) astronomy. Realizing the scientic opportunities from universities and independent observatories in developing the next these changes will ll NOAO’s plate and that of its international generation of telescopes.” comparator, the European Southern Observatory, beyond 2020.
is is elaborated upon in a later chapter: “Community Of course, it is sobering to recollect that 20 years ago, dark participation in major national telescope initiatives must be led by energy, galaxies in the reionization epoch, Gamma Ray Bursters, an effective national astronomy organization working in concert protoplanetary disks, and exoplanets were all unknown. However, with universities and similar institutions. Such an organization the facilities and instruments that gave us these phenomena— should in turn be subject to close community oversight with Cosmic Microwave Background missions, Keck, Gemini, and appropriate advisory bodies. It should: the Very Large Telescope, NASA’s Great Observatories, and calibration-stabilized, high-resolution spectrographs—were • Lead the development of a strategic plan for the evolution being condently planned 20 years ago, with lead times as long as of the capabilities of the system by organizing discussions those we are now commencing. We should not hesitate to make involving the National Science Foundation (NSF), the long-term plans—indeed we must, to keep a steady advance of independent observatories, the academic community, astronomical knowledge. We also should not hesitate to adjust and industry. them as required. “Plans are useless; planning is essential.” • Be able to contribute to the scientic leadership and provide the technical expertise (e.g., professional As intended by Astronomy and Astrophysics in the New engineering and system management), the Millennium, NOAO plans to submit, with university and administrative skills, and the management experience independent observatory partners, proposals for two major new and infrastructure needed in the building of those facilities before the end of the decade, one for the Large Synoptic facilities that are too large or expensive to t within the Survey Telescope (LSST) and another for the Giant Segmented resources of single institutions or small partnerships. Mirror Telescope (GSMT). Recently, the Brinkman report (see • Ensure that the United States enters international www7.nationalacademies.org/NSF-Priorities) has charged the NSF collaborations with a clear scientic purpose and a well- to produce a roadmap for large research facility projects, covering considered technical and administrative approach, and the next 10–20 years, including ranking and sequencing. maintain these or modify them as appropriate for the duration of the project. NOAO serves the O/IR astronomy community and currently • Coordinate with the community to provide capabilities has the largest identiable pool of resources (30 percent of what that support the suite of state-of-the-art large telescopes; is required under decadal survey formulae) for operating LSST such capabilities may include telescopes, instruments, and GSMT. A requirement of the Cooperative Agreement archives, observing modes, and other channels for access between AURA and the NSF for managing NOAO is leadership to data.” of “community-based planning, design, and development efforts NOAO-NSO 78 Newsletter for proposed new federally-funded initiatives in ground-based Although there have been two other recent National Research optical and infrared astronomy, including the Telescope Systems Council studies focused on particle astrophysics and solar system Instrumentation Program, archiving of ground-based data for the astronomy, the science- and technology-based vision provided by National Virtual Observatory, LSST, and GSMT.” Astronomy and Astrophysics in the New Millennium is particularly cogent to the National Optical Astronomy Observatory (NOAO). To plot out a deliberate path, as opposed to a random walk, NOAO has been asked by the NSF to convoke a community-based long- Twenty-rst century technology has nally surpassed Galileo in range planning committee. While it is important to carefully optics (ground-based telescopes can be diffraction limited, and continued
10 June 2004 June 2004 11 DIRECTOR’SOFFICE Director’s Office NATIONAL OPTICAL ASTRONOMY OBSERVATORY A Long-Range Plan continued think through the membership of such a committee, it be solicited from relevant international groups, e.g., the would necessarily include representatives of the essential IAU Working Group on Large Scale Future Facilities. For specialist committees in the O/IR community, for example, a coordination with space-based facilities, the NASA space representative of the GSMT Science Working Group (SWG), science strategic plan is available. a representative of the LSST SWG, and a representative of the System Committee. e plan should include the broader Ideally, the length of such a report would not exceed the impacts of astronomy, and should outline appropriate Brinkman report, Setting Priorities for Large Research processes for making community decisions at times when Facility Projects Supported by the National Science decisions need to be made. Foundation. e body of that report runs approximately 32 pages. e report would be submitted to the NSF e System Program of NOAO would support the secretariat division of astronomical sciences. Coordination of the plan of the committee. e committee may have a kick-off in NOAO’s area with any similar plans for NSO and NRAO meeting as early as this summer. One or more meetings is a subject well suited to the Committee on Astronomy and would be required specically to maximize opportunities for Astrophysics. If you are interested in contributing to this input from the community at large. e January 2005 AAS effort, please contact me at [email protected]. meeting could provide one such opportunity. Input would
Workshop Updates Adaptive Optics Roadmap
Steve Ridgway
e Adaptive Optics Development Program (AODP) held a Roadmap Update Workshop 26–27 April 2004 in Tucson.
Panel Members Participants Co-Secretaries and Scribes Laird Close, Univ. of Arizona Sean Adkins, Keck Steve Ridgway, NOAO #Richard Dekany, Caltech #Roger Angel, Univ. of Arizona Steve Strom, NOAO Brent Ellerbroek, NOAO #Jacques Beckers, Univ. of Chicago *James Graham, UC Berkeley John Codova, Univ. of Arizona Robert Johnson, Kirtland **Craig Foltz, NSF #Edward Kibblewhite, Univ. of Chicago Paul Hillman, Kirtland Bruce Macintosh, LLNL #Matt Johns, Carnegie #Guy Monnet, ESO Michael Lloyd-Hart, Univ. of Arizona Paul Schechter, MIT #Claire Max, LLNL, UCSC * absent #Andrei Tokovinin, NOAO Ken Mighell, NOAO ** by diveo, intermittently Peter Wizinowich, Keck #Tom Rimmele, NSO # speaker Gary Sanders, Caltech Mark Trueblood, NOAO
e panel report will be published shortly. e panel found that the current roadmap still provides a sound description of decadal needs. However, a number of new systems concepts have been developed in the four years since its completion: • Ground layer adaptive optics (GLAO) NOAO-NSO 78 Newsletter • Extreme adaptive optics (ExAO) • Multi-object adaptive optics (MOAO) • Optically powered deformable mirrors • Alternative wavefront sensors • Mid-infrared adaptive optics continued
10 June 2004 June 2004 11 NOAO-NSO Newsletter 78 1 2 NOAO Astronomer and Tohono O’odham Schools Official (in priority order) (in priority Opportunity Funding Next for the AODP Priorities Recommended Workshop Updates Adaptive Roadmap Optics continued Kitt Peak National Observatory, 15 miles away. 15 miles Observatory, at National Peak Kitt walls building on shadows cast they that Arizona, bright so Sells, were in school high the at eld an football from lights existing that discovered he when Peak Kitt around for environment concern the a special demonstrated Carlyle reason!” like—within you would that anything about just do to you allows it cap, that Within luminaries. of a use mixture you can forindex, the formula the applying what exactly “By explains. them where,” and Schwarz place must be in xtures telling and law the prescribing are we feel people that is codes lighting with problems the of “One observatories. their near pollution and Tolololight articial Cerro measure to used be on can which Pachón, Cerro cameras all-sky for deploy and to work index” his effective interference an “luminescence developing lighting for civic award the received Schwarz Dark-Sky International the (IDA) Tucson 12. in on March Association of Meeting Annual 2004 the at Award Director’s Executive an with honored each were H shortly. announced be will opportunity 2funding Cycle e • • •
Director’s Office Oasis-Baboquivari Unied School District No. 40, 40, No. District School Unied Oasis-Baboquivari staff for Indian of operations director Carlyle, scientic Jerry and South NOAO the of Schwarz ugo Engineered components/subsystems Engineered leverage high potential with developments risky and/or Small/low-cost following the as such technologies ELT critical of testing technologies: example order) with on-telescope (in arbitrary and laboratory by validation Concept June 2004 —MID-IR AO —MID-IR interferometric pyramid, analyzers—e.g., wavefront —Alternative mirrors secondary deformable DFMs—e.g., powered —Optically segmented), massively to moderately ELTs, segmented-pupil (for coronagraphs/nullers WFS, —ExAO—e.g., —LTAO MEMs count hi-actuator WFS, tomography, NGS low-order —MOAO—e.g., open-loop WFS tomography, NGS low-order —MCAO—e.g., measurements atmospheric —GLAO—e.g., Hi-actuator count MEMs count Hi-actuator Honored by IDA Douglas Isbell Douglas in the Kitt Peak National Observatory section.) Observatory National Peak Kitt the in for Astronomy” Resource A Critical Association: Dark-Sky International “e IDA, our see on the (For more information should so and efforts, their observers.” visiting appreciate really We it effectively. by applying through followed and information, for asked it so observatory, the around sky night the respect to wanted organization “An Green. Richard Director Peak Kitt says experience,” neighbor’ ‘good excellent an was “is at all.” not objectionable was eld e Peak. was Peak Kitt from but well, its lit appearance very obviously well-shielded. Kitt and on well-aimed Support were “ey Scientic John of says on,” Supervisor Topawa came Glaspey, the they from when lights impressive were “e campus arranged. was Topawa at lights new the of demonstration a occurred, move the Once improve to how on situation. the information for Peak Kitt contacted an up Carlyle set move. the to aer Topawa intent at eld the sports new with entirely Sells, in school high the and Peak) Topawa in Kitt school (17of from miles intermediate the campuses swap to preparing was 40 No. District School NOAOGEMINISCIENCECENTER TUCSON, ARIZONA • LA SERENA, CHILE
Gemini Update
Ta Armandroff
he NOAO Gemini Science Center (NGSC) is pleased to GMOS-South IFU report several areas of noteworthy progress at Gemini e integral eld unit for GMOS-South has been commissioned Observatory. In addition to regular science observing and will be used for community science observing programs in Tfor the Gemini communities, progress is being made on semester 2004B. us, both southern and northern targets are commissioning and optimizing several observing capabilities. observable with the twin GMOS IFUs. ese newly available instruments or instrumental modes represent opportunities for the US community to attack challenging science T-ReCS questions using Gemini. e ermal-Region Camera and Spectrograph (T-ReCS) is performing well. Gemini South with T-ReCS provides the greatest GNIRS sensitivity for mid-infrared imaging of any ground-based telescope e Gemini Near-Infrared Spectrograph (GNIRS) has been and instrument combination. commissioned in its basic modes and is performing well. Gemini is on track to execute community queue observing programs 2004B Proposals with GNIRS in semester 2004B. e GNIRS integral eld unit NGSC saw a strong response from the US community to the Gemini (IFU) has been successfully installed and commissioned, and Call for Proposals for semester 2004B. Eighty-four proposals were Gemini expects to offer the GNIRS IFU for science observations received for Gemini North: 45 for GMOS-North, 18 for NIRI in semester 2005A. Please see the subsequent GNIRS article by Jay alone, 5 for NIRI with the Altair adaptive optics system, and 17 for Elias for more exciting details. Michelle. Ninety-three US proposals requested Gemini South: 29 for GNIRS, 28 for T-ReCS, 28 for GMOS-South, 9 for Phoenix, and Michelle 2 for the Acquisition Camera. In total, 161 US Gemini proposals e mid-infrared imager and spectrometer Michelle will be sought 371 nights on the two Gemini telescopes (note that some returning to Gemini from the United Kingdom Infra-Red proposals requested more than one instrument). Telescope (UKIRT) in May. Michelle will undergo work at Gemini’s Hilo Base Facility during May and June to adapt it for e numbers of US Gemini proposals and nights requested optimal use at Gemini. Michelle will then return to the Gemini represent all-time highs. e oversubscription factors of 3.1 at North telescope for additional commissioning. It is planned that Gemini North and 4.8 at Gemini South demonstrate healthy Michelle will carry out scientic observations during semester community demand. e large number of US proposals for 2004B and will remain at Gemini for the long term. GNIRS (29) during its rst semester of availability indicates wide community interest in this excellent instrument.
Gemini Data Comes Online
Marcel Bergmann
he Gemini Science Archive (GSA) telescopes. Raw data that have reached the While most Gemini data has some prototype was publicly released end of their proprietary periods (typically proprietary period, the header information in November 2003 and is now 18 months) may be downloaded directly is considered to be public immediately upon Toperating in a “shared risk” phase. e GSA from the archive, along with all the relevant ingestion into the archive. e headers prototype (see www.us-gemini.noao.edu/ calibration exposures and information. can be searched to determine whether sciops/data/dataArchive.html) provides e GSA prototype precedes the release of observations have been made of your searchable access to every bit of science the “basic” science archive, scheduled for favorite target, and if so, to determine when data taken with any of the instruments release this summer, which will bring added the data will become public. Calibration on either of the two 8-meter Gemini functionality to the archive. exposures including arc lamps, at elds,
continued
June 2004 13 NOAO-NSO Newsletter 78 1 4 query the are ese prototype. GSA the in included features search principal two are ere immediately. archive the from downloaded and for searched be can and period, standards proprietary no have (spectro)photometric and Gemini Data Online Comes continued page has a link to this UDF data. UDF this to alink has page GSA e top-level integration obtained. have been of hours 15 far, So GSA. the being through immediately are public made data all and observations, the for period proprietary the waived team GLARE e region. Field Deep Ultra Hubble/ACS the in targets on faint spectroscopy use multi-object shuffle to nod-and- of hours 75 obtain to GMOS program proposed Glazebrook; GS-2003B-Q-7) K. (PI GLARE team the 2003B, semester During is query science a the of case special A program those numbers. with identication calibrations) (including associated data nd to the query all exposure an use then and targets, of set a or target observed particular that programs of nd list to the query science a use probably observations, would a user the practice, In else. but little of range date instrument, and can telescope, user the a constrain limited: more are query e exposure an executing for fragment). parameters name (or name set data a on matching by time, same the at data calibration and science both for search to used be An can query exposure well. as data calibration nightly the to lead that links include do results search the though data, calibration not results e data, science only include will returned range. and date lter, particular a or a wavelength instrument, particular one results telescope, the one to limiting by further be constrained can search all e (or objects). pattern name particular whose a objects matches for location sky or the object on taken particular a observations near for search may NGSC D query UDF . In a science query, users users query, science a In . science query query science June 2004 (Ultra Deep Field). Field). Deep (Ultra and the the and exposure exposure n lc bfr s lgt curd at occurred light rst before place in e data was already plan to Gemini archive maps. weather satellite and data the execute environmental as well and as observations, dene to used logs, les xml observing the set-ups, instrument the of logs like things include were “meta-data” so-called ese observations executed. the which conditions under the information understand the to all needed provide must it data, proper the of a from calibration enable and To reduction spectra and telescopes. the images storing raw simply must the than archive more much useful do A variabilities space-based telescopes. from systematic observations than more subject to are with taken telescopes download Data ground-based and data. nd Gemini raw to users allow the using GSA ese searches prototype Archive. Science Gemini the accessing for form query Science and Gemini operations. e advanced advanced e operations. Gemini and users both to useful features new with archive advanced an for are plans there already summer, this line to on scheduled come is GSA basic the While archive. basic the scenes” in implemented be will prototype GSA the “behind don’t that improvements in the queries. yet exist other large have for also Many interface will batch It a appropriate les. most the calibration science and sets between data include linkage also will improved archive basic e meta-data. these access to function search a include will GSA “basic” full e meta-data. these all of tracking and production the facilitate to designed was infrastructure data- taking whole the and telescope, either continued June 2004 NGSC
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 1 4 NGSC June 2004 Operation with GPOL requires installation on the the on installation capability. No this for commissioning set been has date structure. requires support instrument the on GPOL port up-looking with spectropolarimetry. for Operation (GPOL) Polarimeter Gemini the is a equipped with also Wollaston prism to its permit use with GNIRS 2005. in available be will it too case which in 2004B, notis this to though likely been early in occur commissioned, has highest slit) arcsec e 0.1 with (R~18,000 mode resolution microns. spectral 2.5 with to 1 R=2000 from at coverage continuous spectroscopy cross-dispersed wavelength and full the range over R=6000 and R=2000 resolutions with spectroscopy long-slit include modes ese 2005A semester. the for users to available be will and commissioned have modes been most of GNIRS key the run, April the With tests. acceptance its Newsletter Gemini the of as issue June action, upcoming the in in article IFU related the the as of well illustration an for gure Gemini. the and (See AIG, NOAO, by jointly installed and March in (AIG) Group Instrumentation University Astronomical the Durham from of delivered was which (IFU), unit eld integral the commission to used was run last e members. by for NOAO led and Scientist staffGemini by other participation with Instrument GNIRS, been Gemini has the Rodgers, Commissioning Bernadette April. and February, S multitechnique and multiwavelength facilitate to data observatories other archived from the with associations machine. home may archive e include data advanced user’s a than rather computers archive high-performance done on the processing the all but with choose, they want, les calibration they the way with the in reduced data have could users that so congurable, user be even could OLDP e archive. the within data reduced fully produce will which contemplated (OLDP), Processing Data being On-Line of implementation an include capabilities Gemini Data Online Comes continued GNIRS Commissioning and System Verification Well Go rst stage of commissioning, with runs in January, January, in runs with its commissioning, completed of stage has rst (GNIRS) Spectrograph Infrared last the ince NOAO/NSO Newsletter NOAO/NSO ). GNIRS has now formally passed all of all passed formally now has GNIRS ). , the Gemini Near- Gemini the , Gemini data in projects such as the the as such Observatory. Virtual National projects of in inclusion data the Gemini to fundamental are spectroscopy) user. the to strength to ese enhancements the basic archive emission delivered in and and extracted or identication measurements data, line imaging photometry and in detection object (such as measurements automated catalog have source reduced and data are automatically both Gemini archived which in include extraction, spectroscopy) proposed Further features and analysis. archival imaging (e.g., Jay Elias pages for an announcement of this opportunity. of this announcement for an pages Web Gemini the Check IFU. the testing on focus the with year, the in later place take likely of round SV will A second reductions initial used provide is to which for users. and GNIRS, assurance for quality pipeline for data look” “quick Gemini the test to used being also are observations ese SV including e instrument, of the versatility of the completed. not advantage takes that selection a diverse comprise were programs programs most though sciops/instruments/nirs/nirsSVPlan.html (see programs SV top-ranked the were all for observations obtained were Data April. and and March in out carried January, of end proposals the from at selected submitted was e programs SV programs. of group selected rst competitively of variety a with instrument the science test to order in out carried actual are observations where (SV), verication system is users to available capabilities GNIRS making of process the of Part • • •
young stellar objects. objects. stellar young and embedded of spectra long-slit band M and L and object, aHerbig-Haro and cores, galactic galaxies, z=1.5 faint of spectra long-slit R=6000 objects brown candidate of to dwarfs, quasars red spectra from ranging R=2000 cross-dispersed see implemented ( implemented see to like know most would us you features let what and the now, out tools try archive to community user our encourage Gemini NOAOand stages. more away, but is well orinto the planning year a still sets. is archive data advanced e these to access basic improving e summer, this line on come public. will archive have data become Gemini already of years Several running. and up is prototype GSA e www.us-gemini.noao.edu www.us-gemini.noao.edu June 2004 [email protected] for summaries), summaries), for NGSC continued ).
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 1 6 GNIRS Commissioning and System Verication continued image is ~3.2×4.8 arcsec. The width of the image corresponds to one of the slices above. slices of the one to corresponds image of the width is ~3.2×4.8 The image arcsec. reconstructed The IFU. the on centering verifies This script. IRAF an using image an into assembled be can slices The Then insert the IFU and take another image through the IFU. The field is sliced up (not all slices are shown here). here). shown are slices up all (not IFU. is sliced the field The through image another IFU take and the insert Then IRAS nebula isshown). field protoplanetary acquisition the of the 10178-5958;portion of amagnified only case, this (in field the of image an taking by Start IFU.GNIRS the with Observing with the protoplanetary nebula. protoplanetary The the with object. the of spectrum sky-subtracted a of line is emission Br portion a shows below image The spectroscopy. for configure Now NGSC June 2004 γ (2.166 a by microns); sees associated fair dust amount of one due also to continuum scattered light June 2004 NGSC
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7 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 1 6 NGSC June 2004 more details, see the previous article by Jay Elias. article previous the see For details, more modes. GNIRS verication out basic two the carried in System been have observations testing Gemini. acceptance by nal its passed successfully also GNIRS spectroscopy. cross-dispersed and long-slit modes, basic its in commissioned was GNIRS GNIRS 2004 NOAO/NSO March Newsletter the since progress with States, United the in instrumentation developed science being Gemini on frontline status update a gives article of telescopes is programs. Gemini support the in provide for instrumen- to tation capable and efforts innovative its continues Program Instrumentation NGSC e (Project Scientist), and Dick Dick Scientist). Joyce (Co-Project and Scientist), Elias (Project Jay Manager), Gaughan (Project Neil of the leadership under Tucson in NOAO at out carried been has project is modes. cross-dispersed, integral-eld and long-slit, well as as dispersions, of a range scales, plate two offers and microns 5 to 1 from that operates telescope South Gemini the for spectrograph an infrared is Near-Infrared (GNIRS) Spectrograph Gemini e NGSC Instrumentation Program Update . and assembled. NICI was successfully successfully was NICI assembled. and appropriate), (where painted cleaned, been have parts dewar NICI the of All NICI Ta & Mark Armandroff Trueblood the successful cold test. cold successful the to the into NICIprior dewar lowered is NICI’sassembly wheel dichroic and filter is building NICI, under the the under Toomey. of Doug leadership NICI, building Hilo is in (MKIR) the Infrared Kea on coronagraphic Mauna telescope. South Gemini capability Infrared imaging 5-micron to dual-beam 1- a Near provide will (NICI) Imager Coronagraphic e planned for December 2004, has has 2004, is completed. been December which for Gemini, planned by acceptance nal are NICI to work the of and percent 75 that reports dened MKIR procured. been being have primary its star to a low-mass relative optimal companion of for imaging dichroics differential and lters e operation. the proper for tested manually cooldown, were mechanisms cold rst NICI this temperature. During operating reaching desired rst 2004, the March its in test 2004. had cold January NICI in Subsequently, tested vacuum June 2004 NGSC continued
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7 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 1 8 FLAMINGOS-2 NGSC Instrumentation Program Update continued Scientist and Principal Investigator. Principal and Scientist Project responsibilities of the assumed Co-Principal Investigator, has was who March the NOAO/NSO in Newsletter article (see on 26 January death tragic Richard’s Following the Project Scientist FLAMINGOS-2 and Principal conceived FLAMINGOS-2 Investigator. as served concepts and and Elston FLAMINGOS Richard NGSC period before being relocated relocated being before period some for there will Gemini used and North at it commissioned the be for telescopes; imager Gemini and near- graph spectro- a multi-object infrared is FLAMINGOS-2 FLAMINGOS-2. e of University is Florida building system. optics adaptive for multiconjugate South’s Gemini capability spectroscopic multi-object a Itprovide also will eld. 6.1×2-arcmin a spectra over will multi-object and provide mode, imaging in Gemini standard the at eld 6.1-arcmin-diameter a cover will It South. Gemini to June 2004 ), Steve Eikenberry, f /16 focus /16focus at Florida, with the analog-to-digital Gemini/ A complete. analog-to-digital boards converter the with Florida, at ongoing is electronics control detector the a of Fabrication at subcontractors. and few shops Florida the of at University well proceeding is fabrication Mechanical ordered. been have FLAMINGOS-2 optics the of all project. the Essentially of phase fabrication and procurement the in is FLAMINGOS-2 hs mg o te od lt o FAIGS2 ie a lms o pors in progress of glimpse a gives fabrication. mechanical FLAMINGOS-2 of plate cold the of image This LMNO- a acpac by to completed. hadGemini been acceptance work of the nal end of FLAMINGOS-2 the percent of 38 As March, 2004. March successfully in completed was FLAMINGOS-2 soware the of review NGSC OBSERVATIONALPROGRAMS NATIONAL OPTICAL ASTRONOMY OBSERVATORY 2004B Proposal Process Update
Dave Bell
OAO received 399 observing proposals for telescope time during the 2004B observing semester. ese included 161 proposals for Gemini, 116 for CTIO, 107 for KPNO, 26 for Keck, 9 for MMT, 8 for Magellan, and 5 for HET. Seventeen of the Cerro Tololo proposals were processed on behalf of the Chilean National Time Allocation Committee (TAC), and 7 of the Kitt Peak proposals Nwere processed on behalf of the University of Maryland TAC. esis projects accounted for 25 percent (98 proposals) of those received, and 16 proposals requested long-term status. Time-request statistics by telescope and instrument appear in the tables below. Subscription rate statistics will be published in the September 2004 issue of the NOAO/NSO Newsletter.
As of this writing, proposals are being reviewed by members of the NOAO TAC (see the following listing). We expect all telescope schedules to be completed by 11 June 2004, and plan to notify principal investigators of the status of their requests at that time. Mailed information packets will follow the e-mail notications by about two weeks.
Looking ahead to 2005A, Web information and forms will be available on line by late August 2004. e September 2004 NOAO/NSO Newsletter will contain updated instrument and proposal information. 2004B Instrument Request Statistics by Telescope
KPNO Telescope Instrument Proposals Runs Total Nights Dark Nights % Dark Avg. Nights/Run 4-m 50 62 178.8 71 40 2.9 ECH 8 8 25 4 16 3.1 FLMN 10 10 30 2 7 3 MARS 2 2 6 4 67 3 MOSA 18 26 75 58 77 2.9 RCSP 12 12 33 3 9 2.8 SQIID 4 4 9.8 0 0 2.5 WIYN 3.5-m 31 34 99.8 30.8 31 2.9 DSPK 2 3 7 0 0 2.3 HYDR 16 16 51 9 18 3.2 MIMO 8 10 25.8 16.8 65 2.6 SPSPK 2 2 4 3 75 2 VIS 2 2 10 0 0 5 WTTM 1 1 2 2 100 2 2.1-m 23 26 126.2 25 20 4.9 CFIM 4 4 19 15 79 4.8 FLMN 3 3 13 0 0 4.3 GCAM 10 12 55 3 5 4.6 SQIID 4 5 24.2 0 0 4.8 VIS 2 2 15 7 47 7.5 WIYN 0.9-m 9 9 48 17 35 5.3 MOSA 9 9 48 17 35 5.3
June 2004 19 NOAO-NSO Newsletter 78 2 0 1.0-m 1.3-m 1.5-m 4-m Telescope CTIO Gemini South Gemini Telescope Gemini North Telescope GEMINI 0.9-m Observational Programs June 2004 CFIM ANDI CSPEC VIS RCSP MOSAIC ISPI HYDRA ECH Instrument CFIM TReCS Phoenix GNIRS GMOSS AcqCam Instrument NIRI Michelle GMOSN Instrument Proposals Proposals Proposals 18 69 18 16 19 19 16 4 9 4 9 1 5 10 84 93 10 23 17 45 28 29 28 9 2 Runs Runs Runs 18 11 78 18 11 17 19 20 16 12 102 12 4 1 5 4 95 30 29 30 29 18 48 9 2 Total Nights Total Nights Total Nights 215.7 60.1 96.7 60.1 52.5 44.2 96.7 221.7 149.4 52 37 52 52 46 17 37 4 57.4 15.1 70.8 67.3 40.3 32.1 76.9 1.3 Dark NightsDark Dark NightsDark NightsDark 41.8 47.2 5.3 44 43.5 5.3 44 12 66 37 12 23 38 37 1.6 0.3 2.2 1.5 40 0 1 4 0 0 0 % Dark % Dark % Dark 19 32 46 100 59 21 57 46 100 23 31 0 0 2 5 5 23 44 73 9 9 0 2 9 0 Avg. Nights/Run Avg. Nights/Run Avg. Nights/Run 2.2 1.6 1.9 1.7 2.4 2.2 0.6 1.4 1.8 1.6 8.1 9.2 3.3 4.7 2.8 8.1 9.2 3.3 4.7 3.1 2.7 2.2 2.9 3.4 4 Observational Programs June 2004
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1 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 2 0 Observational Programs June 2004
HET Telescope Magellan-II Magellan-I Telescope MMT Telescope Keck-II Keck-I Telescope ACCESSCOMMUNITY LRS HRS Instrument MIKE BCSpec IMACS Instrument SPOL RCHAN BCHAN Instrument NIRSPEC NIRSPAO DEIMOS NIRC LWS LRIS HIRES Instrument Proposals Proposals Proposals Proposals 13 13 4 4 4 2 2 2 4 2 9 1 1 7 7 2 4 1 2 4 6 Runs Runs Runs Runs 10 14 14 4 4 4 2 2 2 2 4 2 1 7 8 2 4 1 3 4 6 Total Nights Total Nights Total Nights Total Nights 19.5 15.5 7.5 3.5 10 11 11 29 22 15 12 4 5 5 5 9 1 3 6 3 1 Observational Programs Dark NightsDark NightsDark Dark NightsDark NightsDark 5.2 8.5 3.2 6.5 3 8 2 3 0 8 9 6 0 0 9 0 0 5 1 2 0 % Dark % Dark % Dark % Dark 100 31 27 44 69 30 73 83 67 42 80 57 60 73 June 2004 0 0 0 0 8 0 0 Avg. Nights/Run Avg. Nights/Run Avg. Nights/Run Avg. Nights/Run 2.1 1.6 1.9 1.9 2.5 2.8 1.9 2.5 2.2 1.5 1.5 2.2 1.8 2.5 2.5 2.8 1 1 2 1 2
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1 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 2 2 Observational Programs Susan Wyckoff, Arizona State University State Arizona Wyckoff, Susan Observatory Lowell Millis, Robert LPL of Arizona, University Hubbard, William Fischer, UC Berkeley Debra NOAO Young, De Dave Chair, System (5 May 2004) Solar Wachter, Caltech/SIRTF Stefanie College Venn, Macalester Kim NOAO Stanghellini, Letizia Paso of Texas, El University Verne Smith, NOAO Ridgway, Steve of Arizona University Muzerolle, James NOAO Mighell, Ken of Washington University Lutz, Julie Caltech/IPAC Kirkpatrick, Davy University Clemson Jeremy King, of Texas, Austin University Hynes, Rob of Michigan University Haisch, Karl UCLA Burgasser, Adam of Wisconsin University Briley, Michael of Maryland University Balachandran, Suchitra Wolff, NOAOChair, Sidney of Hawaii University Chair, Williams, Jonathan of Cincinnati University Chair, Hanson, Margaret 2004) April (29–30 Galactic Dark Energy”scienceworkshop sponsoredbyNOAO ofview overall ofstate the day final the during 2004 March 20 on research, Energy Dark “Observing the of —Cosmologist Michael Turner, NSF assistant director for mathematical and physical sciences, describing his is having“Everybody agreat time, we’re getting all along…and there is plenty of work for everyone.” June 2004 2004B TAC2004B Members Notable Quote Philip Pinto, University of Arizona University Pinto, Philip University Ohio McNamara, Brian Barbara UC Santa Martin, Crystal Caltech/SIRTF Lacy, Mark Carolina of South University Varsha Kulkarni, Observatory Lick Holden, Brad of Florida University Gonzalez, Anthony Dey, NOAOArjun University Brown Dell’Antonio, Ian STScI Jong, De Roelof of Arizona University Davé, Romeel University Queens Courteau, Stephane Caltech/SIRTF Armus, Lee Observatories Carnegie Chair, Mulchaey, John Tod NOAO Lauer, Chair, NOAO Chair, Dickinson, Mark May 2004) (3–4 Extragalactic Howard Yee, Universityof Toronto Malcolm Smith,CTIO CTIO/CERROTOLOLO INTER-AMERICAN OBSERVATORY
New Blanco Instrumentation
Alistair Walker
n November 2003, CTIO issued an on the Dark Energy Camera and DES can variety of science projects by the general Announcement of Opportunity to be downloaded from www.ctio.noao.edu/ community. e proposal will be evaluated develop a major new instrument for telescopes/dec.html. by an external expert panel, which will Ithe Blanco 4-meter telescope. Letters of make a recommendation whether or not to intent were due by 15 February 2004. We Prior to February 15, the role of CTIO was actually build the instrument on this basis. received a single letter of intent from the mainly to answer technical questions from e announcement describes the process Dark Energy Survey (DES) Consortium the potential proposers, although direct in more detail (see www.ctio.noao.edu/ (Fermilab, University of Illinois, University participation of NOAO scientists in the telescopes/eFuture/Blanco_prop.html). of Chicago, and Lawrence Berkeley preparation of science cases was permitted National Laboratory) to build a very large under the terms of the solicitation. Given e DES Consortium will be publicizing mosaic CCD camera for the Blanco prime that only a single letter of intent was received, their project at the Denver AAS meeting, focus. e Dark Energy Camera would the character of the relationship can change, and we at CTIO will be actively working bridge the gap between the Blanco telescope and the timeline has been shortened a to solicit views and suggestions from and the Large Synoptic Survey Telescope little. However, the review process stays our community. We encourage you to (LSST) in time (2008–2012). e DES the same. Consequently, CTIO will work read about the camera and survey at would occupy 30 percent of the Blanco closely with the DES team so that their www.ctio.noao.edu/telescopes/dec/html and time over ve years, producing a deeper set proposal, due on 15 July 2004, describes respond to the questions asked there, and if of data than the Sloan Digital Sky Survey an instrument that, although optimized so inclined, give an opinion on any aspect of (SDSS), over a similar area. Presentations for the DES, will also be useful for a wide the instrument design and the project.
Retirement of the Blanco Echelle and RC Spectrographs
Alistair Walker
ith some regret, we announce the imminent retirement of made available through the Telescope System Instrumentation two work-horse instruments, the Blanco Echelle and RC Program. ere is a less direct upgrade path for Echelle users. spectrographs (though see below for a possible temporary Part of the reason for the sharp decline in demand for the Blanco Wreprieve for the latter). e need to simplify operations on the Blanco Echelle must surely be due to the overwhelming superiority of as we begin to operate the SOAR 4.1-meter on Cerro Pachón, plus the UVES on the VLT. For US users, MIKE on Magellan is the only availability of superior facilities on SOAR, Gemini, and Magellan, has large-telescope high-resolution optical spectrograph presently driven the decision to retire these instruments aer semester 2004B. available. In 2005, bHROS on Gemini, with R=150,000 and ber-feed, may become available, and STELES, a beam-fed bench e RC spectrograph, with its long slit, good range of resolutions, echelle for SOAR (see www.lna.br/~bruno/Steles), is not likely to high throughput, and for the past several years, its use of the appear before 2006. e high-resolution infrared spectrograph UV-ooded high-QE Loral 3K CCD with Air Schmidt camera, has Phoenix is available on Gemini, and will be shared between always been very popular, averaging 27 percent of the time through Gemini and SOAR, perhaps as early as mid-2005. the 1990s. Requests still are at the 15 to 20 percent level. us, we will review the retirement decision for the RC spectrograph shortly e Blanco Echelle and RC spectrographs were delivered in the before proposals are due for 2005A (approximately 1 September mid-1970s. Since then, each has gone through a series of detector 2004), in case commissioning of the SOAR Goodman Spectrograph upgrades, from photographic plates to thinned large-format is delayed. If that were the case, we would likely offer the Blanco CCDs, via the SIT vidicon, 2D-Frutti, and early generation RC Spectrograph in severely blocked mode in 2005A. CCDs. Keeping the instruments state-of-the-art and operational for more than two decades on the southern hemisphere’s largest ere are some other good options for spectroscopists. Users of telescope enabled users to make some of the most exciting and the RC Spectrograph can migrate to the Goodman Spectrograph important scientic discoveries of these years. on SOAR, GMOS on Gemini, or IMACS on Magellan via time
June 2004 23 NOAO-NSO Newsletter 78 2 4 Professor João Steiner, President of the SOAR Board, and his wife Eliana Steiner speak with a fellow dedication guest; Hugo guest; dedication fellow a Schwarz of theNOAOwith Southscientificstafftalks withChileanRegionIVIntendente FelipedelRíoGoudie. speak Steiner Eliana Brazilian wife his South; and Gemini Board, from SOAR seen the of as President Steiner,held, João was Professor ceremony dedication the where tent white the to next parked attendees for who chaired the SOAR Board of Directors in its formative years through 2003; the SOAR telescope and one of the transport buses (Clockwise from upper left) The crowd at the SOAR telescope dedication on 17 April 2004, including Sidney Wolff (front center), T CTIO the formal inauguration of the $32 million telescope facility. telescope million $32 of the inauguration formal the celebrating officials former and project bright current many and a guests 200 more than with during Chile, 17 central day north in April sunny on Pachón Cerro on dedicated was (SOAR) Telescope Research Astrophysical Southern he June 2004 A Wonderful Day for SOAR Dedication Douglas Isbell Douglas continued June 2004 June 2004 CTIO
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 2 4 CTIO June 2004 calibrated and adjusted with the help of the facility facility in the improvement of steady help a in the resulting with sensor, wavefront carefully adjusted was system and optical the calibrated Over rst nights, 18. very several March of next the night the the testing, on and collected were alignment photons optical of the support period in 120-actuator installed 25 was on its assembly telescope complete with the and integrated system, Gemini was the primary SOAR mirror in 4.1-meter the plant, aluminization mirror-coating South successful its Following 2004. on 17 April telescope the of dedication formal the for time in just images rst very its T see For more NOAO dedication, the from photos Associated related with story, the reported Michigan reaching stories and wire Press Carolina North in outlets the media around US went local dedication the numerous on story and world, service wire news Reuters A event. the covered reporters TV Chilean several and the of 1 page on appeared dedication SOAR the from photos color and Articles said. he of projects,” types these for important is very it that “We know astrotourism. in efforts local popular increasingly actively is government to foster and research future to enable Chilean both country, of the regions key the three in that contamination light noted articial Goudie, to limit seeking Río del Felipe region, fourth Chile’s of (governor) Intendente e students. science for their tool motivational and educational as an to serve of Universe,” its the ability and mysteries deepest ofabout clues “the promise SOAR for uncovering State the and University, cited theHill at Michigan ofCarolina Chapel University Brazil, from North partners SOAR Officials (AURA), Inc. Astronomy in for Research for Universities Association the of president Smith, William job,” said magnicent a done have they and team, small very a was team project SOAR “e chemical bright.” very is the future e SOAR. from and come will Universe of the images galaxies highest-resolution the of ecology the understand fully us help Way “Aer present,” to added. the off,days Mould Hubble early Telescopeits the Space to from is turned of Milky evolution the and form, stars how discover to SOAR expect “We telescope. Director NOAO said soul,” the of blessing the his forduring Serena La of treat Archbishop the by a echoed later were and that dedication treat the at remarks in Mould, astronomical Jeremy an both is SOAR and astronomers, for heaven is “Chile SOAR Dedication continued Telescope (SOAR), culminating in the acquisition of acquisition the in culminating (SOAR), Telescope Research Astrophysical Southern and the at exciting time very hectic a been have months few past he
February 2004. Following an intensive intensive an Following 2004. February USA TODAYUSA SOAR Sees Stars at Last , CNN.com, Yahoo.com, and other national venues. national other Yahoo.com, and , CNN.com, www.noao.edu/outreach/press/soar. Steve Heathcote Steve work will proceed on the scientic commissioning and and Imager. Optical SOAR the of commissioning scientic characterization the on time, same proceed the At will work mirror. steering tertiary the fast- drive to a using needed signals error the correction generate to camera guide readout tip-tilt including of system, implementation optical the the of further on calibration focus and will tuning efforts months, few next operations. the in science Over regular for involved ready are work instruments its hard and the telescope the the before remain ceremony, that to tasks the completing dedication returned the team for SOAR pause brief a Aer night. on the seeing site prevailing with images the from able obtain indistinguishable to were half-max, 0.74full-width arcsec Imager we 12 Optical SOAR April the of use night to the On quality. image El Mercurio El and and El Día El June 2004 June 2004 newspapers in Chile, Chile, in newspapers CTIO continued
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 2 6 CTIO made available on a limited basis basis be limited will a on instruments available made these that anticipated both currently goes is all it If well, August. and July during imager/spectrometer infrared the OSIRIS the of to commissioning and installation turn then foci, the way Nasmyth preparing for the will Attention SOAR continued Stars at Sees Last they should be available during the the during semester. 2005A available be should they telescope the and year, the of quarter to last the during delivery for Goodman are slated Spectrograph and High-roughput Camera, Infrared Spartan the Both semester. 2004B observing the of part second the during June 2004 The SOARThe team. KPNO/KITTPEAK NATIONAL OBSERVATORY
The International Dark-Sky Association: A Critical Resource for Astronomy
David Crawford & Richard Green
he International Dark-Sky Association (IDA) is the leading e Value of IDA organization encouraging the preservation of dark skies IDA’s mission is to preserve the nighttime environment for through the promotion of quality outdoor lighting practices. the benet of everybody, and that includes extensive activities TWith more than ten thousand members and a staff of seven, IDA to preserve the prime dark skies so necessary for cutting-edge has worked effectively throughout the world with the professional astronomy. Brighter skies mean a higher background level and a lighting community, community authorities, and elected officials to higher noise level. Articial sky glow (light pollution) reduces the produce results in dark-sky preservation through outdoor lighting value of large investments by both public and private institutions ordinances, public education, technical committee service, and in state-of-the-art astronomical telescopes. Table 1 demonstrates alliance development. continued
These matched images show the growth of lighting in the Tucson metropolitan area, as seen from Kitt Peak. The measured increase in sky glow is considerably lower than the increase of population, by more than a factor of two.
June 2004 27 NOAO-NSO Newsletter 78 2 8 background has been increasing almost everywhere, and and everywhere, almost increasing been sky-brightness has the background time, long a for apparent been has As future. glow, the now or in No present standards. site is too remote to by be sky affected by that are expensive very those as including well, telescopes future all for hold will pattern a Such glow. sky in growth the with telescopes in value of loss real) (and potential the e International Dark-Sky Association continued D hs eeoe efcie otcs ih ot f the of most level the on impact an with make do and can that contacts organizations effective developed has IDA the these for work of staff. small time-consuming number is It the growing. is and networks maintained, continuously individuals is lighting and astronomical local with necessary. Contact when obtained are updates regular and California, these places, of most in southern established been have Codes Chile, others. and Hawaii, observatories— Arizona, major to with southern relative locales working key the of years all in the officials related over and engineers, lighting staff, effective governmental been has IDA a be should and locales. for other can model It protection. local the for of need because critical and Tucson in based is IDA because both issues, local these on time its of fraction large a spends staff IDA nationally. and locally required of networking areas range effective wider much metropolitan the to other and and observatories, Tucson impacting of due growth years, the earlier to requires in it than more and much today, time, continues work considerable is area. the in astronomy for skies dark preserving in the to success continuing critical was basis international even and national a to efforts of expansion this locally, not nationally, made are xtures all lighting of and manufacturing the to recommendations related decisions lighting outdoor many Since the throughout beyond. well indeed and counties state, and and towns activity, other to continuing it this expanded of much over 1988, took in staff incorporated the its was of IDA When growth glow. the sky adverse wavelengths) some (at reversed even and slowed have years, the over revisions many with along enforcement for over sustained ordinance 30 ordinances, ese years. a been effective and has ordinances lighting outdoor there effective for push where Arizona, such southern locations to as are exceptions degradation sky only of rate e increasing this sites. observing prime of telescope vicinity large the in including rate, accelerating an at KPNO June 2004 more to do, and it takes daily attention. attention. daily it takes and more do, to but progress, there is much, We much signicant are making (a lot of which is in observatories). the same that areas attract brighter and more for growth grow the population even more than rapidly lighting pressures the and grow. little, do help efforts for pressures Halfway consuming. is time very protection international Environmental and time national adequate devote as to difficult increasingly getting is It IDA of Needs e IDA it. do will. can No observatory work. this do IDA to healthy scally a takes it and time, takes networking Effective allies. active them make to and well them know to us for essential is It well- companies. and and large organizations make for funded work oen they ey and xtures. designs, lighting the the the do make ey they developed. recommendations, consistently and up kept are can be allies organizations effective ese glow. sky adverse the on hence and lighting, night of Office section.) Office Honored by Official O’odham Schools IDA”Director’s the in (For more on IDA,the see “NOAO Tohonoand Astronomer support. showyour and amember become IDA Web the to goWe site, to you urge our of preservation skies. dark the resource: prime support to organizations, as and for us to step up, astronomers professional both as individual time is It efforts. IDA of beneciary major a is astronomical community IDA e supporters. are more of the members involvement through and active AAS scally of both help, needs IDA fraction members. tiny a only IDA. of Sadly, support in $2,000 only contributed observatories complement astronomical entire of the In 2003, professional workload. increasing out the in order resources to needs to staff carry restore and increase IDA But organization. line the in preserve thus and expenses income, with bring to order in recently staff dramatically reduce to have had IDAhas slowdown. economic staff recent the to part in due IDA on suffered, IDAof have nances the years, recent in increased demands the While time. with grow only will effort of level is $99,000. approximately of cost a at astronomy, for preservation dark-sky to relating staff directly onissues effort of percent 25 approximately spent staff IDA 2003, In only if these relationships www.darksky.org, www.darksky.org, continued to to June 2004 KPNO
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9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 2 8 KPNO June 2004 e International Dark-Sky Association continued * A value of 1.0 is the natural sky background. A value of 1.2 means a 20 percent increase above that level. that above increase percent a20 means 1.2 of Avalue background. sky natural the 1.0is of A value For a 16-m Telescope a16-m For Telescope 8-m an For Wilson atMt. 2.5-m the For Observatory atLick 3-m the For atPalomar 5-m the For Peak onKitt 4-m the For Telescope Aperture a4-m For SKY GLOW GLOW SKY RELATIVE RELATIVE LEVEL* 1.050 1.025 1.100 1.010 is is the loss of capital value due to increased sky glow! sky due to increased value of capital loss the is is 2.00 5.00 3.00 1.00 1.20 1.50 1.06 1.25 1.05 1.12 1.10 1.10 5 3 2 Table 1. Sky Glow Effects on Large Large on Telescopes Effects Table Glow 1. Sky (Based on IDA Information Sheet No. 20) Sheet on IDA Information (Based APERTURE IN IN APERTURE EQUIVALENT EQUIVALENT METERS 15.80 15.26 15.92 15.61 4.00 2.83 3.54 3.58 3.89 3.27 3.65 2.31 3.78 3.81 1.79 1.73 1.12 7.63 7.81 PERCENT OF PERCENT ORIGINAL ORIGINAL VALUE 99% 88% 88% 88% 94% 94% 58% 86% 92% 39% 39% 23% 23% 78% 97% 74% 11% 11% 1 COST 65.0 10.0 60.8 57.1 422 408 395 371 417 8.6 9.2
COST COST LOSS 26.9 13.8 51.0 0.8 5.6 4.1 1.4 7.8 June 2004 KPNO
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9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 3 0 is the four-layer poly gate structure of OTCCDs, which which OTCCDs, of structure gate poly four-layer the CCDs is conventional and CCDs (OT) transfer orthogonal T cells, and guide star or bright star locations. locations. star or bright star guide and dead cells, any gaps, OTA the remove to data dithering science simple for with used be will subarrays steering, the of image most and while readout rapid for regions of star idea the guide dene naturally single- cells unit small, ese enormously. to failures yield usable overall the manufacturing increasing thereby OTCCD regions, limits it view, of elds and large in present be bright always very will which of stars, impact the connes it because interesting very is cell unit pixels 500-square e the arrays.” of combining “array an into and pixels, OTCCD and CCD for design proven a on building of mix clever a is design is 500×500 pixels. 12-micron approximately of array 8×8 an of consists OTA Each edges. the CCDs, around devices test 800×1200 small of number a and two CCD, normal 2600×4000 a as well as chips) looking checkerboard (the it on OTAs three gure has the in shown wafer silicon initial mechanical the e of CCDs. tests (this on-sky soon with OTAs very completed and to year) production, wafer actual made to design, have OTA full-up we a to idea ago, conceptual the from years progress rapid four were OTAs only Since contemplated OTAs. rst 72 provides run Our foundry rst Associates/DALSA. Technology Semiconductor by Hawaii/MIT of WIYN for produced being is it University groups, Laboratory Lincoln the with collaboration close ( Luppino and Tonry, Kaiser, by described rst was OTA the OTCCD, of breed newest e 2003, al., 109, et Howell 1154 in and 1997, al., et Tonry in described are camera OTCCD WTTM. prototype the as with observations such and calibration typical systems (Scientic tip-tilt with mechanical in-line from gains quality image improved has produced camera this with option tip-tilt” “electronic the example, using For OTCCDs. of abilities and properties the of of Hawaii), has been used at to demonstrations WIYN allow by built John Tonry OTCCD (University camera, prototype A effects. ill no with CCDs normal as exactly used be also 6×10 than (better precision electronic longer) high-photometric and and (millisecond include high-speed to parts” expanded has moving use OTCCD “no corrections, tip-tilt to real-time, developed fast, Originally perform four integration. all in during moved be to directions pixel a within charge the allows KPNO e IN osrim a be dvlpn a between difference main (OTA). e developing array transfer been orthogonal an called CCD has of type new-technology Consortium WIYN he June 2004 -4 ) observations. OTCCDs can can OTCCDs observations. ) PASP, The New OTAs Are Here! PASP, Steve Howell, Richard Green & George Jacoby &George Green Richard Howell, Steve 2000, 112, 768). In In 768). 112, 2000, 115, 1340.) PASP, NOAO (MONSOON) and the University of Hawaii (IOTA). of Hawaii NOAO University the (MONSOON) and at both for to such devices new develop controllers underway are efforts so OTAs, run to inadequate Present-day are controllers CCD cells. independent on-chip 64 the other of each and run to lines logic control necessary the and all gure, the in contain seen be can called, are they as streets, or OTCCDs the between gaps e defective). if (e.g., desired if off or be or turned can a cell, rapid guide readout science cell, a as assigned be can OTCCD 500×500 Each independently. controlled be to has OTA single a within OTCCDs 64 the of each as complex, quite is OTAs of operation and design e will upgrade WIYN spectroscopic applications.upgrade WIYN will run are additional 12-micron-pixel CCDs (2600×4000), which will have 0.11-arcsec pixels. By-products of the WIYN foundry 8×8 OTAs (32K×32K) to be completed cameras Both in 2008. of array an (ODI)WIYN, imagerfor one-degree planned the 16×16 eldarcmin and a be available in have2006. Itbe awill step to will OTAs, of array 4×4 a large- in QUOTA, new on-skyimagers. format two into and OTAs implement dewar to plan a We in OTA fall. the an have to are Plans WIYN at Hawaii). of (University Luppino Gerry devices by mounting designed custom includes and for (ITL) Lesser ready by done Mike be devices will OTAs the of be thinned Packaging toAugust. with by testing expected 2004, May are by devices delivered OTA thick completed Fully each of the 64 independent cells. cells. independent 64 of the each run to logic on-chip other and lines control necessary the all OTCCDs) contain the between (gaps streets The edges). the OTAs two (around three CCD, devices test small of 2600×4000 number a 800×1200and CCDs, a incorporates chips), looking wafer checkerboard (the silicon mechanical This June 2004 KPNO
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1 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 3 0 KPNO June 2004 acquiring or operating the Calypso Observatory are urged to contact contact to urged are in Observatory [email protected] interested Calypso the organizations operating or or Astronomers acquiring considered. be also will management and operation long-term for proposals purchase, of lieu In than see better details, For further nights. is on better than seeing better median is arcsec 0.3 as good as camera been has and tip-tilt, adaptive using when 0.7 arcsec camera high-resolution e wide-eld the arcsec. on 1 quality image median e changer. lter acassette-style in lters six up to accommodate can camera Each imager. Loral backside-illuminated thinned 2K×2K a imager from Imaging. e Fairchild incorporates camera high-resolution CCD 4K×4K backside-illuminated thinned, a wide- incorporates e camera eld guider. adaptive tip-tilt a with equipped is and eld a square has camera wide-eld 80-arcsec an has camera the high-resolution the and eld, square cameras: 10-arcmin imaging two has telescope e ridge. southwest Peak’s of Kitt edge at the airow completely laminar the to retracts exposed telescope the building leaving telescope, telescope the from the seeing, dome of effects the 1/17 than better is mirrors tertiary and secondary, high- primary, smooth the for error wavefront rms combined extremely the and have surfaces, on optics quality telescope operational e became 2002. and in Peak completed Kitt was It imaging. high-quality T Calypso 1.2-Meter Telescope Seeking Permanent Home ot o qaie isiuin r osrim I uiie a for utilizes specically It designed telescope consortium. or Crétien Ritchey institution 1.2-meter qualied a to cost modest at purchase for offered being is Observatory Calypso he science workshop inTucson sponsoredbyNOAO Energy” Dark “Observing the of day final the of end the at 2004 March 20 on speaking sciences, physical and mathematical for director assistant Turner,NSF Michael cosmologist from comments of collection —A just crazy!” ideas that make predictions. is crazy idea solutionthe not Because every to a profound problem—some are to solve, or it might solved be next month withor observation a new experiment. But we ideas… new need true.’ be years toIt’s 100 everyone’scaught good take ‘toohas mightnotthatproblem it isfancy, a because ‘colda notIt is fusion’ science. of situation,all profounditand mostin mystery the be may Energy “Dark . www.calypso.org th Notable Quote wave. To eliminate Toeliminate wave. Edgar Smith Edgar . Calypso Telescope (Photo copyright Adeline Caulet.) June 2004 KPNO
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1 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NATIONALSOLAROBSERVATORY NSO TUCSON, ARIZONA • SAC PEAK, NEW MEXICO
From the NSO Director’s Office
Steve Keil
URA completed its review of my rst ve years as NSO Director, and as a result, I started my second term as director on 9 May 2004. I look forward to working with e NSO AO program, led by omas Rimmele, continues to Athe solar community over the next ve years to obtain the resources progress at a rapid pace. e NSO low-order AO system has needed to construct the Advanced Technology Solar Telescope been upgraded to high-order (76 degrees of freedom) this scal (ATST) and to maximize the usefulness and impact of the new year. Currently there are two high-order AO systems in the capabilities provided through adaptive optics (AO), new infrared Dunn Solar Telescope (DST), one feeding the new Diffraction- (IR) arrays, the Synoptic Optical Long-term Investigations of the Limited Spectro-Polarimeter (DLSP) and the other feeding the Sun (SOLIS), and the upgraded, high-resolution capabilities of the Advanced Stokes Polarimeter (ASP) and the narrowband lter of Global Oscillation Network Group (GONG). To exploit the new the Italian Interferometric BI-dimensional Spectrometer (IBIS). AO and IR capabilities, NSO will upgrade the operational and data Both ports have room to set up additional lters and cameras. e collection systems at its major facilities, the Dunn Solar Telescope port with the DLSP will be dedicated to the DLSP and the setup and the McMath-Pierce Solar Telescope. We will also continue to frozen to minimize set-up time between users. is system will be collaborate with other groups to provide instrumentation capable commissioned for routine use in the next few months. In addition of exploiting the diffraction-limited images delivered by AO. Some to the AO systems on the DST, the AO team delivered and installed of the current collaborations include development of diffraction- a high-order AO system at the Big Bear Solar Observatory. HAO, limited Stokes polarimetry with the High Altitude Observatory in collaboration with NSO, plans to develop a more capable (HAO), diffraction-limited narrowband imaging with Arcetri replacement for the ASP that will take advantage of the diffraction- Observatory and Marshall Space Flight Center, and thermal IR limited imaging. e new project, the Spectro-Polarimeter imaging and spectroscopy with NASA Goddard Space Flight for Infrared and Optical Regions (SPINOR), will extend the Center. ese efforts will require the allocation of additional functionality of the ASP through the next decade and add IR engineering time on our facilities, but the payoff will be worth it. capabilities. e SPINOR instrument will demonstrate ATST concepts for the spectropolarimeter being designed by HAO. For their role in developing the AO systems, Steve Hegwer and e ATST construction proposal is currently being reviewed, while Kit Richards received the NSO 2004 AURA service and technical the ATST design continues to progress. NSO is holding a public achievement awards, respectively. Congratulations to both of session on the ATST at the Solar Physics Division (SPD) meeting them on a job well done, and to omas for leading this very of the American Astronomical Society in Denver on Wednesday, successful effort. June 2 from 12:30–1:30 PM. e current status of ATST science and design will be discussed and opportunity provided for public input.
NSO hosted the planning workshop for the 2007 International Heliophysical Year (IHY) at Sunspot, New Mexico, from 20–22 April 2004. Researchers from several communities, including solar, interplanetary, magnetospheric, ionospheric, atmospheric, and climate, participated in the workshop. IHY, NOAO-NSO 78 Newsletter along with the Electronic Geophysical Year (e-GY), is being held on the 50th anniversary of the International Geophysical Year (IGY). IHY planners hope to bring together researchers from various disciplines to develop joint observational and theoretical programs leading toward a comprehensive picture of the coupled processes in the heliosphere, from the Sun to Earth and out to the boundary of the interstellar medium. e initial meeting explored NSO 2004 AURA service and technical achievement award winners ideas in each of the subdisciplines, including areas of common Steve Hegwer (left) and Kit Richards. interest and overlapping needs. continued
32 June 2004 June 2004 33 NATIONALSOLAROBSERVATORY NSO TUCSON, ARIZONA • SAC PEAK, NEW MEXICO NSO Director’s Office continued
Arizona University), advisors Han Uitenbroek and K. Sankarasubramanian. Undergraduate and graduate SRAs Aer several months of operation at the GONG will be Cheryl-Annette Kincaid (AF Scholar, University farm in Tucson, the SOLIS mount and the vector of North Texas), advisor Joel Mozer; Anna Malanushenko spectromagnetograph (VSM) were installed on Kitt Peak on (St. Petersburg State University, Russia), advisor John April 13 and May 4, respectively. Power, helium, data, and Leibacher; Leah Simon (Macalester College), advisor cooling uid connections have been restored to the VSM. omas Rimmele; and Maria Kazachenko (St. Petersburg e mount has been roughly aligned to the polar axis, but State University, Russia), advisor Alexei Pevtsov. RET one of the position encoders is not working correctly. at participants are Mark Calhoun (Sabino High School, problem will be xed and daily observations are expected to Tucson), advisor Bill Livingston; Matt Dawson (Brockton resume very shortly. High School, Boston), advisor Rob Hubbard; Michael Sinclair (Kalamazoo Math & Science Center, Michigan), advisor Joel Mozer; and Creighton Wilson (Lovelady High e DST at Sacramento Peak has been the mainstay of School, Huntsville, Texas), advisor Alexei Pevtsov. high-resolution ground-based solar observing for decades. In recent years, aging systems and general wear on the New graduate students starting this summer and working telescope have resulted in more frequent breakdowns and throughout the academic year with K.S. Balasubramaniam loss of valuable observing time. In an effort to address and as their research advisor will be Brian Harker-Lundberg mitigate some of these issues and to enhance the quality and (Utah State University) and Drew Medlin (New Mexico quantity of DST observations, NSO needs to allocate large Tech). Brian Robinson (University of Alabama, Huntsville) blocks of time for systems upgrades. To accomplish some will be an NSO/ATST Postdoctoral Fellow working on the of the more critical and immediate needs, we dedicated a design of tunable lters with K.S. Balasubramaniam and substantial amount of engineering time during the April– Allen Gary (NASA/MSFC). June quarter. is required postponing many of the science proposals submitted for both that quarter and the July– September quarter. us, during July–September 2004, Our congratulations to Yukio Katsukawa (University the DST will be open for new proposals (which were due of Tokyo) for successfully defending his PhD thesis on on May 15) only for the month of September. e telescope “Photospheric Magnetic Fields and the Coronal Heating,” time allocation will return to regular scheduling during the under the supervision of S. Tsuneta, National Astronomical October–December 2004 quarter, with proposals due on Observatory, Japan. Yukio used the HAO/NSO Advanced August 15. Stokes Polarimeter at the DST for portions of his work, combining ASP data with data from Yohkoh, SoHO, and TRACE. Selections for the 2004 NSO Research Experience for And nally, congratulations to Christoph Keller, who Undergraduates/Research Experience for Teachers was formally presented with a Friedrich Wilhelm Bessel (REU/RET) and Summer Research Assistantship (SRA) Research Award of the Humboldt Foundation on March programs have been completed. Our students this summer 26 in Bamberg, Germany. is prestigious award, which include the following REUs: Frances Edelman (Yale is supporting Christoph’s sabbatical leave at the Max University), advisor Frank Hill; Statia Luszcz (Cornell Planck Institute for Aeronomy in Katlenburg-Lindau, University), advisor Matt Penn; Stuart Robbins (Case is in recognition of Christoph’s contributions to the Western Reserve University), advisors Carl Henney and development of advanced instrumentation for solar physics, Jack Harvey; Heidi Gerhardt (Towson University), advisor high-precision polarimetry techniques, and image K. Sankarasubramanian; Joel Lamb (University of Iowa),
reconstruction methods. NOAO-NSO 78 Newsletter advisor Alexei Pevtsov; Michelle McMillan (Northern
32 June 2004 June 2004 33 NOAO-NSO Newsletter 78 3 4 expectations of a face-to-face review later this summer. summer. this later review with face-to-face (NSF), in a Foundation of currently Science expectations is National proposal the e at review systems. supporting and A issues discussed at the CoDR: the need to control the the control to need the CoDR: the at discussed biggest the of issues one addressing on progress making are We Interface Lab Telescope/Coudé plane. focal input instrument the to train optical complete the of study tolerance a for up been set has contract A area. this in instruments the feed will Liang Ming (NOAO) which directions. optics, is on camera working the nal adding all in quality image uniform very in resulting rotation, lab coudé and performance tuned balance to ne been has feed optical coudé simplied new e Lab Coudé model. CFD the to obscuration telescope the on adding also is 1. in shown gure Fluent, Inc. Warner Mark with is working analysis (CFD) dynamics uid computational new the of example dome, An CoDR. the at goal throughput the stated our into wind exceeded ow.is air the in increase percent 250 a in resulted direct help which vents shades, larger and the of combination e opening. sunshades each are above included Also August. last design (CoDR) conceptual review the at presented much were shows than 1, vents larger gure in depicted e arrangement, vent system. new ventilation enclosure the through airow of the has amount been progress made in increasing Signicant Enclosure winter. fall/early late the in held be to is (PDR),which review for design preliminary required the issues address help to workshops instrument interface small of series a planning Weare thermal options. feed instrument lab, Gregorian and environment, coudé lab and telescope the between enclosure, the areas, key including several in continues progress meantime, the In NSO Figure 1. New enclosure vent arrangement and and arrangement example. analysis CFD flow corresponding vent enclosure New 1. Figure addressing various design aspects of the telescope telescope the with of aspects resumed design various and addressing proposal phase construction last the of s June 2004 Working toward aPreliminary Design for ATST Newsletter , we had just submitted our our submitted just had we , Jim Oschmann & the ATST &the Jim Oschmann Team e leading option at this point for supporting a Gregorian Gregorian a supporting for point this at option leading e Rotator Gregorian quantitative for Center Sciences measurements. interferometer Optical Arizona of University the NOAO. to system at the move interface will we this this, interferometric of Following quality initial optical for the of up testing setting currently are We design. knife also airow We laminar rst-cut a tests. implemented have these for built “box” the outside to inside from difference temperature 30°C a nearly able to maintain We are testing. thermal qualitative initial some undergone in the last as our described lab experiment built laboratory has (NOAO) the Schoening in Bill air coudé. at controlled environment the of that the of to air telescope ambient colder typically the between interface to the project team so that a concept can be designed in in designed be can ofPDR support year. the later this concept a that so team project the to input more provide to working been have team HAO the and Elmore David requirements. module polarization the majorA area of emphasis for is these reviews toHawaii. dene in detail of University the and HAO by designed being concentrates on the optical and that infrared spectropolarimeters May) of end the for (scheduled workshop rst the instrument by choice this this conrm to with hope and work arrangement will that concepts instrument on Hawaii) evaluating of (University Mickey Don with We working 2. are gure in shown is relay polarization optical e best the performance. and gravity with, easier contend somewhat to a environment option, other any than space a utilizes that rotator for relay. more allows instrument optical is three-mirror Nasmyth a actually is instrument feed the Nasmyth instrument (formerly the the (formerly to instrument used Nasmyth system instrument). Gregorian relay the feed Three-mirror 2. Figure Newsletter continued . It has June 2004 NSO
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 3 4 NSO June 2004 GONG site. Subject to availability of personnel to operate operate to personnel of availability to Subject site. the GONG at observations for case the was as capacity, recording day per gigabytes 100 a to constrained be longer no will we daily resumed and a aer of “vacation” observations a mount few weeks. On Peak, Kitt the to attached been have will this time the By Advanced future Technology Solar Telescope (ATST) site. Kitt Peak until NSO consolidates its facilities atobserving the Peak a Kitt few days later, on 15.April on remain SOLIS will to transported carefully and slowly 1). VSMwas e gure to lied (see 13 April and on tower TelescopeVacuum old the of Peak top the Kitt to transported then 30, March on changes some for builder the to returned was It 28. March through it service was completed and into placed temporary Tucson,where in site test was GONG the at mount installed 13-ton e originally Peak. Kitt on instrument (VSM) spectromagnetograph vector and mount the of installation e major SOLIS event of of the second was quarter the 2004 European Our rm activities. to partner efforts funding extending are potential and up frame, through time required June be construction the may any that for activities In review prepare proposal to year. the continue in we later addition, review design preliminary the for on are focused preparations e activities project’s principal Milestones Upcoming Working toward aPreliminary for ATST Design continued tower in April. (Photographs by David Jaksha.) David by (Photographs inApril. tower Figure 1. on Peak Kitt The SOLIS and to mount was arrived the top lifted of the old Vacuum Telescope Newsletter is published, the 1.7-ton VSM 1.7-ton the published, is Jack Harvey & the SOLIS Team &the Harvey Jack SOLIS developed further. developed is pipeline reduction data the as observing potential full its to program regular the up ramp to plan we instrument, the information. latest for the periodically it visit to interested anyone encourage and Web site our update to continue We summer. this expected is which effort, this on feedback await We eagerly areas. many in phase Development and Design current the to adding for Union to European a the have proposal submitted colleagues full-disk magnetograms and average the resulting values values an from aside 2, gure resulting in shown As disk. solar the full the over observed average and are magnetograms daily to full-disk correction components constant a apply We instrumental simultaneously). identical but and solar magnetic different with lines at- two (possible spectrum because separate Daily problem to error zero-point the to used contributions obvious. instrumental been not expected. have is was calibrations problem eld none the of when origin offset e zero-point stable persistent but a the show that magnetograms is component result line-of-sight interesting NASA/NSO of One old the data by produced spectromagnetograph. producing pipeline. was on that reduction type been same has data the emphasis the primary e streamlining and calibration details on centered has reduction data VSM on Work June 2004 NSO continued
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5 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 3 6 6mco-ie lt lsr u it a -irntik ol of foil 2-micron-thick a into cut laser slit, 16-micron-wide the spectrograph that found We inspection. for removed was the it so beam, unltered the that in changed slowly had slit evidence entrance showed Observations quieter. signicantly be to appear results SOLIS the and Observatory, Solar Wilcox from measurements eld magnetic Sun-as-a-star daily with well very agree values these difference, factor scale expected SOLIS continued of these areas is underway, but a small staffing level is a level staffing all small a on impediment. common but Work underway, is will areas investment. these science SOLIS of the excellent from and that produced users, be operating ensuring of issues, community importantly, the algorithms, most to calibration data reduction providing with SOLIS, FDP, good and dealing project ISS implementing SOLIS and the the commissioning understanding facing and now completing are challenges major e that guider is common to it and the VSM. high-speed todebug the used e FDPbeing power is glitch. common a torelated be may failures these that We speculate inoperative. became also instrument (FDP) patrol full-disk the of cameras CCD two e repair.for manufacturer its to and suffered was returned testing a majordaily failure during e CCD camera of the integrated sunlight spectrometer (ISS) the We calibrate VSM. of the to properties polarization used optics slit). the of the some at replacing also polarization are foil less 1-micron-thick produce tendency. using foils curling fabricated (thinner the being are eliminate slits and New slit the at changes property material any reduce should melts is than material. foil rather the ablates that available now is laser new a that us advised manufacturer e length. 36-millimeter its along places few a in slightly curled had nickel, aluminized NSO June 2004 f /6 solar solar /6 of the line-of-sight component of the solar magnetic field magnetic solar the of component line-of-sight the of Figure 2. The solid line shows daily SOLIS VSM measurements ouain s asd y oa rtto ad h irregular distribution theof magnetic fields onthe solar and surface. rotation solar by caused is modulation 27-day The WilcoxSolarObservatory.sunlightthe at made component ofintegrated measurementsline-of-sight ofthe pointwas error applied tothesedata. The dashed linesare averaged over the full disk. A constant correction for a zero- GLOBALOSCILLATIONNETWORKGROUP
EL TEIDE • UDAIPUR • LEARMONTH • MAUNA LOA • BIG BEAR • CERRO TOLOLO
GONG
John Leibacher & the GONG Team
ith the local helioseismology pipeline approaching science products to be added to the data distribution system. routine science capability, growing interest in the excellent GONG coverage of the “Halloween Flares” is year’s annual meeting, GONG 2004/SoHO 14, is being Wof October–November 2003, and the run-up to the biennial organized by Sarbani Basu at Yale University, and will be held GONG/SoHO/SDO meeting in July, things have been exciting 12–16 July 2004 in New Haven, Connecticut (www.astro.yale.edu/ on the GONG science front. e instrument team has its hands sogo04). full with a bundle of repair projects—including a very promising x that should reduce quite substantially the uncertainty in the In a press release last year, Cliff Toner said, “Success with the zero point of the magnetograms—and developing plans for the Mercury transits sets the stage for next year’s Venus transit, which replacement shelter and near-real-time data recovery, in addition will allow more accurate calculations because Venus is farther to long sought “routine operations.” Meanwhile, the data reduction than Mercury from the Sun.” Well, it’s nearly upon us and we team has made major strides toward the automation of the pipeline are beginning to count down to this year’s transit of Venus. e processing and scored big in slashing the calibration backlog. same three GONG sites that captured last year’s Mercury transit— Learmonth, Western Australia; Udaipur, India; and Tenerife, e fun, however, hasn’t been just in-house, as the quarter was Spain—will observe the path of Venus as it transits the solar disk also busy with meetings. A successful Local Helioseismology on June 8. In addition to the educational and outreach benets, we Comparison (LoHCo) group meeting—number seven in a hope to be able to verify the absolute angular orientation and image continuing series—was held in Tucson on February 10–11. scale for these three instruments. Visit our Web site (gong.nso.edu/ Twenty-six participants discussed the latest progress in local venus2004) for history, links to other live sites, information, and helioseismology. See the detailed discussion below. education programs.
GONG’s Data Users’ Committee (DUC) met in Tucson on Site and Instrument Operations February 12 to evaluate progress and set objectives. e on- e year began with preparations for a relatively busy schedule site meeting gave the Data Management and Analysis Center of preventive maintenance visits to the sites through the spring. (DMAC) staff an opportunity to share their results with visiting Modications to the light-feed turret that should help prevent DUC members. Highlights included unveiling the rst version water leakage were underway through January. Testing of the of the new Web-based soware documentation, which includes turret and other upgraded hardware to be installed at the eld sites schematic maps of the global and local pipelines and links to took place in February. program and data product descriptions, operator instructions, algorithms and denitions, background science, and related data e rst preventive maintenance trip of the year was in March products (gong.nso.edu/DMAC_documentation). e transition at Mauna Loa, where the newly modied turret was installed. from separate-workstation-based processing to automation and Other improvements included the replacement of the Lyot Filter/ shared resources reached a major milestone. e long-awaited Michaelson interferometer assembly, the uninterruptible power announcement that sneaker net is history and the data processing supply, camera power supplies, analog-to-digital converter boards, backlog is at its lowest point in history prompted applause and and implementation of the new optical table earthquake protection. high-ves from around the table. e DUC gave its blessing, In spite of many cloudy days, all of the work was completed on pending a couple of nal acceptance tests, for the implementation schedule. of the Automatic bad-Image Rejection (AIR) module into the processing pipeline. e automated image reduction package e network sites continued to run well. Interruptions of data was developed by Richard Clark, and should accelerate this acquisition occurred because of a failure of a signal generator card part of the data processing and signicantly reduce the time to at Cerro Tololo and during troubleshooting at Learmonth when a produce science products. A lot of discussion was devoted to nonfunctional guider card was discovered. e Udaipur instrument the local helioseismology pipelines, including nalizing angular failed to guide for a few days in January, but began working again in orientation procedures using MDI and noon dri scans before the midst of troubleshooting. Mirror fogging at Big Bear continued routine production begins, and nalizing the specications of the to appear during particularly cold mornings. is issue should be
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June 2004 37 NOAO-NSO Newsletter 78 3 8 GONG continued re o mgiue s ral ipoe te ult of quality the improves greatly is magnitude. of an order than more by background instrumental eld magnetic low-spatial-frequency the amplitudeof the reduced has is modulator. the ofstates polarization between time switching the equalizes that circuit modulator-driver new a installed haveStover Ed Shroff, and Chirag Harvey,JackLuis, George installed. turretin the be will mirrorsheat the modicationto a when resolvedfall bynext Charlie Lindsey, Doug Braun, and Anna Malanushenko Malanushenko Anna and Braun, Doug Lindsey, Charlie Goodrich, tachocline. Jean by the progress recent image showed large-aperture Leibacher to John designed a analysis diagram presented ring Gonzalez-Hernandez Irene maps. ow the computedfrom vorticity vertical the showed Komm Rudi years. three next the for pattern the predicted boldly and 11+11/3-year sinusoid, a as oscillation the torsional modeling from results latest the showed Howe posters. Rachel ve of total a presented Boulder group e in March. meeting late (LWS) at in Star represented a With well Living recent was the team research GONG/SOI e search for possible systematic changes. the map to subsurface is horizontal goalow eld before andaer etheares and observed. ever energetic most the periodof the time so-called “Halloween 2003—theFlares,” Novemberwhich were among and diagram October covering ring analyses for data the processing completed have We Data Processing, Analysis, and Management prototype developed. be will eld a potential before required for is testing use breadboard More their calculations. enabling to lead should GONG, and by obtained magnetograms once-per-minute the GONG June 2004 and proceeding through the prelter, Lyot, Michelson Michelson Lyot, We prelter, constructed. been has modulators line the and interferometer, spectral through nickel proceeding the and from starting of model observations, numerical the A elds. GONG magnetic the to of fall measurement response last the at look activity fresh solar a in motivated has spike strong the of advent e signal in terms of the real physical changes of the Sun. GONG is also seeking a postdoc to calibratedistribute timelyfarsidebasis.regularandtheproxya images on farside “bounce” imaging near-real-timefrom the six GONG instruments, developand to produce and to Research compression grant Targeted and transmission LWS (TR&T)of the images Technologyneeded NASAfor farside & a awarded was GONG at line on the of are All posters images, results. divergence time-distance Kholikov’s Rudi’s Shukur and imaging variations, farside parameter mode real-time near localized Rachel’s contained poster Hill’s Frank capability. the implementing in for GONG+ data products, which is currently down down currently is which products, 141to days. data GONG+ for data e backlog requests. cumulative the to reduce continues data team reduction 30 distributed to DSDS response in e gigabytes 460 archived. been also have period time same the for results frequency Mode (DSDS). System of factor Distribution and ll Storage Data 86 the average into archived were 0.87, an through with 79 (36-day) 2003), months October month-long 27 GONG (ending for months, series three time velocity past the During shape. line spectral the distort elds strong when instrument the of response the study to model this use will solar cycle can be seen emerging in the 2003 inthe data. emerging seen be can cycle solar next the with associated be will that branch The pattern. flow the of phase the of variation depth possible the about inferences within make to deep begin can we penetrate and to zone, convection the seen be can flows second The the for period. years 11/2 as such choices possible solar other the complete to than prediction stable a more gives This combination extrapolated cycle. al. fits et the Vorontsov and 2002), (after sinusoids 11/3-year with and fitted were 11-year inversions RLS from mean temporal a of subtraction after residuals rotation-rate the plot, above the To make before. ever than detail more in seen be can zone and MDI from GONG, ofthe pattern zonal migrating observations flows inthe convection combined of years nine With gong.nso.edu/Images/posters.html . June 2004 GONG
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9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 3 8 GONG June 2004 and statistical differences. A second point point second A differences. statistical and systematic of nature the and is understand work to more required that methods but promising, are different sets data between the similarities that concluded group e 1998). Rotation (Carrington of 2002 April covering data MDI GONG and of group comparison ongoing the on e focused Stanford, from telecon via six and France, from 2004. one Taiwan, from one including participants, 26 February 10–11 seven, on Tucson number in held and GONG by workshop, organized was LoHCo latest and e TON MDI/SoHO, HMI/SDO). toward building and Wilson, Mt. data (GONG, different between sources and holography) and time-distance, (ring-diagram, helioseismology local of methods different between consistency e establish to 2003 (LoHCo) February in formed was group Comparison potential. toward Helioseismology scientic progress Local full to the sets the achieving data helioseismology and inferences, local methods of the need intercomparison the of for recognized community subtlety helioseismic methodologies, the helioseismology and local the state developmental of the Given hemispheres). southern and cannot northern the which between distinguish and averages longitudinal only Group Comparison Helioseismology Local e which produces produces y, g o l o m s which i e s global o i l e h to (in contrast scales temporal and horizontal at small solar zone the convection possible study to it makes Local helioseismology differences occur mainly at high latitudes. high at mainly occur differences flux.magnetic MDIand GONG data show similar very results; large of locations at mainly occur areas) (white downflows 80, 40, Strong magnetograms. 20, Peak Kitt NSO (5, from 120 Gauss) and flux magnetic indicate lines contour The upflows/downflows. indicate values MDI);Positive/negative 7.1ofbottom: depth GONG; a (Top: at Mm velocity Vertical agenda, presentations, and participants. and presentations, agenda, Web the visit site at can You necessarily effort. not comparison the to helioseismology discussed related from also results group latest e the useful so helioseismology. proved global that for exercises to similar “hare-and-hound” be needed will the sets sets data ese data methods. articial local test of to creation the on centered gong.nso.edu/lohco/workshop7.html to view pictures, pictures, to view June 2004 GONG
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9 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO EDUCATIONALOUTREACH Public Affairs PUBLIC AFFAIRS AND EDUCATIONAL OUTREACH
Science Education Highlights: Frenzied Teachers in Atlanta and a Telescope Building Challenge for Students
Stephen Pompea & Douglas Isbell
ttending the National Science Teachers Association have used to convert their classrooms into astronomical research (NSTA) annual meeting each spring is not for the timid or centers. For example, Michigan teacher Ardis Maciolek described faint of heart. e meeting is lled with the country’s best her involvement with a student’s astronomy research project Aand most energetic teachers, eager to increase their professional that was later chosen for the Intel International Science and knowledge and to examine each other’s teaching practices. is Engineering Fair in Portland, OR, the most prestigious science fair year, thousands of teachers converged upon Atlanta’s main in the world. convention center in early April to attend workshops on best practices in science education and teaching pedagogy, and to roam Walker and TLRBSE Director Stephen Pompea also led a workshop the NSTA convention oor in search of new activities, teaching titled “Awesome Experiments in Light and Color,” attended by materials, and free books. an overow crowd. “We were hoping to get 30 teachers at our workshop since it was on Sunday morning at the end of the It was an intellectual madhouse, but one that the NOAO science convention, and in an obscure location,” Pompea says, “but we had education staff looks forward to each year as a way to reach over a hundred teachers attended. e room was completely full signicant numbers of engaged science teachers. With workshop 15 minutes before the workshop began.” is was the third year a slots that must be applied for a year light and color workshop has been in advance, the annual meeting given to standing room only crowds is an important opportunity to by NOAO under the cosponsorship disseminate NOAO’s education of the Optical Society of America, work to a broad national teacher who provided educational kits for audience. NOAO’s specialty in each teacher to take home. is bringing astronomical research into year’s workshop tested a new laser the classroom was well-represented activity developed by Pompea and in 2004 workshops sponsored by Walker under the NSF-funded its NSF-funded Teacher Leaders in Hands-On Optics (HOO) program Research Based Science Education at NOAO. HOO is a joint informal (TLRBSE) program. is year, education project of the Optical NOAO staff were leaders in seven Society of America, SPIE, NOAO, workshops and one short course for and MESA of California that teachers, and nearly all were lled is aimed at middle school-age to capacity. e NSTA efforts were students in aer-school programs. organized by NOAO Public Affairs Senior Program Coordinator Pompea also was a copresenter with MESA program students (from left) Daniela Castillo, Miriam Kathie Coil, Senior Science University of California at Berkeley Flores, and Armando Castillo from Nogales High School in Education Specialists Connie colleagues in a short course on Nogales, Arizona, pose with a Newtonian reflecting telescope Walker and Steven Cro, and the teacher activity guides Living that they built as part of a science competition designed by TLRBSE Co-Principal Investigators with a Star and e Real Reasons
NOAO educational outreach staff. NOAO-NSO 78 Newsletter Jeff Lockwood and Travis Rector. for Seasons, which are part of the University of California at Berkeley Most of the NOAO workshops, including one offered jointly with Lawrence Hall of Science’s Great Explorations in Math and Science the National Solar Observatory, introduced teachers to research series, which has proven to be extremely popular with teachers. projects that they can pursue with students. Some of the projects covered in these workshops were research using high-quality data While the NSTA meeting was happening in Atlanta, another on novae, solar magnetic eld phenomena, active solar longitudes, NOAO educational outreach activity was being conducted back and active galactic nuclei spectroscopy. In another workshop, in Arizona. An NOAO-designed student competition to build a past TLRBSE teachers briefed other teachers on techniques they Newtonian reecting telescope was being held at Arizona State
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40 June 2004 June 2004 41 EDUCATIONALOUTREACH Public Affairs PUBLIC AFFAIRS AND EDUCATIONAL OUTREACH Science Education Highlights continued
University in Tempe as part of a state-wide competition In the reecting telescope challenge, student teams for middle and high school students. Also developed in determined the focal lengths of lenses and mirrors and connection with the HOO project, the competition was assembled Newtonian telescopes from surplus optical parts. part of a set of educational activities developed with the e teams were judged on a test of telescope knowledge, as Mathematics, Engineering, Science Achievement (MESA) well as on the assembly, focusing ability, and resolution of program of Arizona, a college preparation program that their telescopes. e success of this competition has led strives to increase the number of ethnic minority, low NOAO to begin designing a team competition for next year income, and rst-generation college-bound students who that will be held throughout California as well as Arizona. are eligible to enter a degree program at a university.
Undergraduate Students Join in CTIO Research
Alan Whiting
or most of the (southern) summer just past, Cerro notes on living and working in La Serena, can be found on Tololo once again hosted a group of undergraduate the 2004 REU/PIA Web pages at www.ctio.noao.edu/REU/ students learning about astronomy by participating ctioreu_2004/REU2004.html. Fin research. Six US students of the Research Experiences for Undergraduates (REU) program joined two Chilean All students participated in a dedicated REU/PIA observing students in the Práctica de Investigaciones en Astronomía run, using both the 1.5-meter (spectroscopy) and the (PIA) program for a ten-week experience involving 0.9-meter (imaging) telescopes for a variety of targets. astronomical observing, data analysis, and presentation of e rst night of observing included the spectrum of a results. An important ingredient of those summer student new supernova, the basis of an IAU circular published programs is living and working together with foreign three days later. e students were cautioned that there students in the international environment of the AURA is generally a longer delay before an observation generates Observatories in Chile. a publication.
e summer program ended in March with oral presentations by the students to all interested CTIO and Gemini staff, completely lling the new AURA Lecture Hall in the Gemini South building! e students will gather again next January to present their results as posters at the winter AAS meeting in San Diego.
Nick Suntzeff and Alice Globus reducing data in the 1.5-meter control room during the student observing run. NOAO-NSO 78 Newsletter Each student was matched with a staff mentor, who supervised an individual research project carried out over the ten weeks. is year mentors came not only from CTIO, but from Gemini South (Bryan Miller and James Turner) and even from the European Southern Observatory (Linda Schmidtobreick). Projects ranged from multiple and variable stars to planetary nebulae, and from E+A galaxies to distant galaxy clusters. Some of the projects Brazilian graduate student Hektor Monteiro explains some involved observing with the CTIO telescopes or Gemini of the intricacies of modelling planetary nebulae to REU South. Summaries of the projects, as well as the students’ student Melissa Rice. continued
40 June 2004 June 2004 41 NOAO-NSO Newsletter 78 4 2 Undergrad Join Students in CTIO Research continued Public Affairs KOLD CBS-TV Live Weathercast from Kitt Peak June 2004 (Mount Holyoke College), and Ethan Knox (Humboldt State University). Barlow RebeccaCollege),(Wellesley RiceSerena), Melissa La de(Universidad Alice Globus (Wells College), Kyle Walker (Ohio State University), Chile),Javier (UniversidaddeRojas Fuentes Bárbara College),(ColoradoGalli Luke right, to Undergraduates for left Experiences from programs:(PIA) Astronomía Research en Investigaciones de CTIO (REU)/Práctica 2004 the of students The telescope at the Visitor Center Observatory. Observatory. Center Visitor the at telescope Peak of Saturn, the Moon, and Jupiter as seen from the 20-inch from Kitt views livetelevision by first-ever the 10 PM half-hour inthe off topped was event economy. The local the on impact Peak’s Kitt about factoids of slides graphical many plus skies, dark of importance the to Center Visitor the at activities new NOAO Public Manager Affairs Doug Isbell on topics ranging from of interviews included segments five the telescopes, Peak Kitt of views various with panoramas scenic to showing In addition 5. March night, Friday on Peak Kitt from live reports weather his evening broadcast Tucson’s from KOLD CBS-TV George Chuck Public Affairs June 2004
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3 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 4 2 Public Affairs June 2004 to support the event. the support to and efforts time their for and volunteers NOAO the to all staff Thanks guests. to 500 400 special estimated the for experience the enhanced wind) a bit of(with brisk sky evening A clear crafts. and sold foods local served Nation the from band. Vendors scratch chicken a and troupes dance traditional two by entertained were and Visitors staff by Association. deployed Astronomy Amateur Tucson the telescopes Mayall small some The with along sunset, 24.after monitors April TV acquisition on the viewing through for Nation and treasures daylight, O’odham celestial during Tohonotouring for open the were oftelescopes families 0.9-meter WIYN and 2.1-meter, for 3.5-meter, house WIYN open 4-meter, an held Observatory National Peak Kitt of one was it said fest! the at booths fun most the participants student several planetarium; portable Lab Star the as well as ASTRO, Project and Family from activities numerous featured NOAO’s booth 7,400 than attendees. more and student 70 exhibits about featured event popular extremely This 2004. mid-March in Math, mornings the three at during Center booth Convention Tucson lively the at a Fest Funhosted Technology and Affairs Science, Public NOAO staff, scientific North NOAO the of members several of help the With NOAO Hosts Math, Science, and Technology Tohono O’odham Family Night on Kitt Peak Fun Fest Booth at TCC Public Affairs June 2004
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3 NOAO-NSO Newsletter 78 Newsletter NOAO-NSO NOAO-NSO Newsletter 78 4 4 NOAO, the University of North Carolina at Chapel Hill, Michigan State University, and the country of Brazil. country the and State University, Michigan Hill, Chapel at Carolina of North NOAO, University the This photo was taken on 17 between of project the 2004, SOAR the dedication a April a before cooperative hours few telescope, background. inthe Pachón on visible telescopes South A local by Chilean man the side rests of the road that up leads to Pachón Cerro central Chile, in the with SOARnorth and Gemini Public Affairs June 2004 The Road to Pach ó n