Science.gov

Sample records for great observatories origins

  1. The Great Observatories Origins Deep Survey: Imaging with ACS

    NASA Astrophysics Data System (ADS)

    Giavalisco, Mauro

    2002-07-01

    We propose a Treasury program of ACS imaging as part of the Great Observatories Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the two original WFPC2 HDFs, to within 0.5-0.8 mag of their depth in four ACS bands, BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep Field South, are the premier deep survey areas from X- ray to radio wavelengths. ACS data will provide unique angular resolution, sensitivity, and wavelength coverage to close the gap between the deepest Chandra and SIRTF observations. Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru, NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set will make it possible to map the evolution of the Hubble sequence with redshift, reconstruct the history of galaxy mass assembly, star formation and nuclear activity from the epoch of reionization to the present, trace the growth of density perturbations via cosmic shear, and, with properly phased z-band observations, detect 12 Type Ia supernovae at 1.2

  2. Search for cosmic strings in the Great Observatories Origins Deep Survey

    SciTech Connect

    Christiansen, J. L.; Albin, E.; James, K. A.; Goldman, J.; Maruyama, D.; Smoot, G. F.

    2008-06-15

    We search Hubble Space Telescope Treasury Program images collected as part of the Great Observatories Origins Deep Survey for pairs of galaxies consistent with the gravitational lensing signature of a cosmic string. Our technique includes estimates of the efficiency for finding the lensed galaxy pair. In the north (south) survey field we find no evidence out to a redshift of greater than 0.5 (0.3) for cosmic strings to a mass per unit length limit of G{mu}/c{sup 2}<3.0x10{sup -7} at 95% confidence limits (C.L.). In the combined 314.9 arcmin{sup 2} of the north and south survey fields this corresponds to a global limit on {omega}{sub strings}<0.02. Our limit on G{mu}/c{sup 2} is more than an order of magnitude lower than searches for individual strings in cosmic microwave background (CMB) data. Our limit is higher than other CMB and gravitational wave searches, however, we note that it is less model dependent than these other searches.

  3. The Great Observatories Origins Deep Survey High Redshift Search for Supernovae

    NASA Astrophysics Data System (ADS)

    Strolger, L.-G.; Riess, A. G.; Dahlen, T.; GOODS SN Searchers; HHZS Team

    2003-05-01

    We have recently concluded the Hubble Higher-z Supernova Team's search for high redshift supernovae in conjunction with the Great Observatories Origins Deep Survey (GOODS). Using the Advanced Camera for Surveys (ACS), we have surveyed ˜170 sq. arcmin fields about the CDF-S and HSF-N on five epochs each, with ˜45 day baselines. These deep observations have allowed us to discover ˜40 supernovae in the range of 0.2=1. A cosmic evolution of SN Ia luminosity or ``grey dust'' would cause SNe Ia to be systematically fainter at higher-z and thus show a different sign and shape on the Hubble diagram. We are also investigating the rate of SNe at /line{z}˜=0.8-1.0, the relation to the local rates, comparisons of host environments to low redshift host environments, and the implications of each to SN progenitors, star formation rate history, and possibly to cosmology.

  4. NASA'S Great Observatories

    NASA Technical Reports Server (NTRS)

    1998-01-01

    Why are space observatories important? The answer concerns twinkling stars in the night sky. To reach telescopes on Earth, light from distant objects has to penetrate Earth's atmosphere. Although the sky may look clear, the gases that make up our atmosphere cause problems for astronomers. These gases absorb the majority of radiation emanating from celestial bodies so that it never reaches the astronomer's telescope. Radiation that does make it to the surface is distorted by pockets of warm and cool air, causing the twinkling effect. In spite of advanced computer enhancement, the images finally seen by astronomers are incomplete. NASA, in conjunction with other countries' space agencies, commercial companies, and the international community, has built observatories such as the Hubble Space Telescope, the Compton Gamma Ray Observatory, and the Chandra X-ray Observatory to find the answers to numerous questions about the universe. With the capabilities the Space Shuttle provides, scientist now have the means for deploying these observatories from the Shuttle's cargo bay directly into orbit.

  5. NASA Great Observatories Witness a Galactic Spectacle

    NASA Image and Video Library

    2010-08-05

    This image of two tangled galaxies has been released by NASA Great Observatories. The Antennae galaxies are shown in this composite image from the Chandra X-ray Observatory, the Hubble Space Telescope, and the Spitzer Space Telescope.

  6. NASA's Great Observatories: Paper Model.

    ERIC Educational Resources Information Center

    National Aeronautics and Space Administration, Washington, DC.

    This educational brief discusses observatory stations built by the National Aeronautics and Space Administration (NASA) for looking at the universe. This activity for grades 5-12 has students build paper models of the observatories and study their history, features, and functions. Templates for the observatories are included. (MVL)

  7. Gamma-Ray Observatory - The next great observatory in space

    NASA Technical Reports Server (NTRS)

    Neal, Valerie; Fishman, Gerald; Kniffen, Donald

    1990-01-01

    The Gamma-Ray Observatory (GRO) which is part of NASA's Great Observatories space program is presented. The GRO is equipped with the Burst and Transient Source Experiment (which detects low-energy gamma-ray photons from 20 keV to 600 keV and locates sources of gamma-ray bursts), the Oriented Scintillation Spectrometer Experiment (which detects celestial gamma rays from 100 keV to 10 MeV and identifies the elements producing these rays by measuring the ray's spectra and time variability), the Imaging Compton Telescope (which images gamma rays with energies from 1 to 30 MeV created when cosmic rays interact with interstellar matter), and the Energetic Gamma-Ray Experiment Telescope (which detects high-energy photons associated with the most energetic processes occurring in nature). After the energies of photons from each source are classified, the gamma-ray mechanisms can be modelled. Nuclei, radioactive isotopes, and nuclear reactions can be identified, and the physical conditions at the radiation's source can also be modelled. From these models, theories can be developed about the creation of elements in the explosion and collapse of giant stars, the acceleration of charged particles to velocities approaching the speed of light, and the destruction of matter and antimatter.

  8. Gamma-Ray Observatory - The next great observatory in space

    SciTech Connect

    Neal, V.; Fishman, G.; Kniffen, D. Essex Corp., Huntsville, AL NASA, Marshall Space Flight Center, Huntsville, AL NASA, Goddard Space Flight Center, Greenbelt, MD )

    1990-08-01

    The Gamma-Ray Observatory (GRO) which is part of NASA's Great Observatories space program is presented. The GRO is equipped with the Burst and Transient Source Experiment (which detects low-energy gamma-ray photons from 20 keV to 600 keV and locates sources of gamma-ray bursts), the Oriented Scintillation Spectrometer Experiment (which detects celestial gamma rays from 100 keV to 10 MeV and identifies the elements producing these rays by measuring the ray's spectra and time variability), the Imaging Compton Telescope (which images gamma rays with energies from 1 to 30 MeV created when cosmic rays interact with interstellar matter), and the Energetic Gamma-Ray Experiment Telescope (which detects high-energy photons associated with the most energetic processes occurring in nature). After the energies of photons from each source are classified, the gamma-ray mechanisms can be modelled. Nuclei, radioactive isotopes, and nuclear reactions can be identified, and the physical conditions at the radiation's source can also be modelled. From these models, theories can be developed about the creation of elements in the explosion and collapse of giant stars, the acceleration of charged particles to velocities approaching the speed of light, and the destruction of matter and antimatter.

  9. Conceiving and Marketing NASA's Great Observatories

    NASA Astrophysics Data System (ADS)

    Harwit, Martin

    2009-01-01

    In late 1984, Dr. Charles P. (Charlie) Pellerin Jr., director of the Astrophysics Division of NASA's Office of Space Science and Applications (OSSA) faced a dilemma. Congress and the White House had given approval to work that would lead to the launch of the Gamma Ray Observatory and the Hubble Space Telescope, but competing segments of the astronomical community were clamoring for two additional missions, the Space Infrared Telescope Facility (SIRTF) and the Advanced X-ray Astrophysics Facility (AXAF). Pellerin knew that Congress would not countenance a request for another costly astronomical space observatory so soon after approving GRO and HST. He also foresaw that if he arbitrarily assigned priority to either AXAF or SIRTF he would split the astronomical community. The losing faction would be up on Capitol Hill, lobbying Congress to reverse the decision; and Congress would do what it always does with split communities --- nothing. Pellerin called a meeting of leading astrophysicists to see how a persuasive argument could be made for both these new observatories and to market them as vital to a first comprehensive inventory of the universe conducted across all wavelength ranges. The group provided Pellerin a rotating membership of astrophysicists, who could debate and resolve issues so that decisions he reached would have solid community support. It also helped him to market his ideas in Congress. Ultimately, the concept of the Great Observatories came to be accepted; but its implementation faced myriad difficulties. False starts, political alliances that never worked out, and dramatic changes of direction necessitated by the Challenger disaster of early 1986 continually kept progress off balance. My paper follows these twists and turns from late 1984 to the announcement, on February 1, 1988, that President Reagan's FY89 budget proposal to Congress had designated AXAF for a new start.

  10. NASA's Great Observatories Paper Model Kits.

    ERIC Educational Resources Information Center

    National Aeronautics and Space Administration, Washington, DC. Education Dept.

    The Hubble Space Telescope, the most complex and sensitive optical telescope ever made, was built to study the cosmos from low-Earth orbit for 10 to 15 years or more. The Compton Gamma Ray Observatory is a complex spacecraft fitted with four different gamma ray detectors, each of which concentrates on different but overlapping energy range and was…

  11. The great observatories for space astrophysics

    NASA Technical Reports Server (NTRS)

    Harwit, M.; Neal, V.

    1986-01-01

    Motivated by the ancient urge to observe, measure, compute, and understand the nature of the Universe, the available advanced technology is used to place entire observatories into space for investigations across the spectrum. Stellar evolution, development and nature of the Universe, planetary exploration, technology, NASA's role, and careers in asronomy are displayed.

  12. Great Observatories Present Rainbow of a Galaxy

    NASA Technical Reports Server (NTRS)

    2006-01-01

    NASA's Spitzer, Hubble and Chandra space observatories teamed up to create this multi-wavelength, false-colored view of the M82 galaxy. The lively portrait celebrates Hubble's 'sweet sixteen' birthday.

    X-ray data recorded by Chandra appears in blue; infrared light recorded by Spitzer appears in red; Hubble's observations of hydrogen emission appear in orange, and the bluest visible light appears in yellow-green.

    About the Movie M82 is shown in all its wavelength glory. Dissolving from Chandra X-ray Observatory images of three X-ray energy bands to images in three bands of the infrared spectrum taken by the Spitzer Space Telescope, and ending with the Hubble Space Telescope's visible- and near-infrared-light image. The three observatories' images were composited to reveal the galaxy's stars, as well as gas and dust features.

    Note: The size of the Full-Res TIFF for the still image is 4299 samples x 3490 lines.

  13. Conceiving and marketing NASA's Great Observatories

    NASA Astrophysics Data System (ADS)

    Harwit, Martin

    2009-08-01

    In early 1984, the astronomical community’s plans to launch a series of powerful telescopes able to study celestial sources at almost any wavelength were in trouble. The President of the United States had just declared his priority for a Space Station that was bound to be expensive, and Congress could not understand why yet another set of space observatories was needed when others were already being funded. To realize their aims, astronomers would have to advocate their needs much more effectively than in the past.

  14. Proposed Great Salt Lake Basin Hydrologic Observatory

    NASA Astrophysics Data System (ADS)

    Johnson, W. P.; Tarboton, D. G.

    2004-12-01

    The dynamic physiography and population growth within the Great Salt Lake Basin provide the opportunity to observe climate and human-induced land-surface changes affecting water availability, water quality, and water use, thereby making the Great Salt Lake Basin a microcosm of contemporary water resource issues and an excellent site to pursue interdisciplinary and integrated hydrologic science. Important societal concerns center on: How do climate variability and human-induced landscape changes affect hydrologic processes, water quality and availability, and aquatic ecosystems over a range of scales? What are the resource, social, and economic consequences of these changes? The steep topography and large climatic gradients of the Great Salt Lake Basin yield hydrologic systems that are dominated by non-linear interactions between snow deposition and snow melt in the mountains, stream flow and groundwater recharge in the mid-elevations, and evaporative losses from the desert floor at lower elevations. Because the Great Salt Lake Basin terminates in a closed basin lake, it is uniquely suited to closing the water, solute, and sediment balances in a way that is rarely possible in a watershed of a size sufficient for coupling to investigations of atmospheric processes. Proposed infrastructure will include representative densely instrumented focus areas that will be nested within a basin-wide network, thereby quantifying fluxes, residence times, pathways, and storage volumes over a range of scales and land uses. The significant and rapid ongoing urbanization presents the opportunity for observations that quantify the interactions among hydrologic processes, human induced changes and social and economic dynamics. One proposed focus area will be a unique, highly instrumented mountain-to-basin transect that will quantify hydrologic processes extending from the mountain ridge top to the Great Salt Lake. The transect will range in elevation from about 1200 m to 3200 m, with a

  15. NASA's Great Observatories Celebrate the International Year of Astronomy

    NASA Technical Reports Server (NTRS)

    2009-01-01

    [figure removed for brevity, see original site] Click on the image for larger version

    In 1609, Galileo improved the newly invented telescope, turned it toward the heavens, and revolutionized our view of the universe. In celebration of the 400th anniversary of this milestone, 2009 has been designated as the International Year of Astronomy.

    Today, NASA's Great Observatories are continuing Galileo's legacy with stunning images and breakthrough science from the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory.

    While Galileo observed the sky using visible light seen by the human eye, technology now allows us to observe in many wavelengths, including Spitzer's infrared view and Chandra's view in X-rays. Each wavelength region shows different aspects of celestial objects and often reveals new objects that could not otherwise be studied.

    This image of the spiral galaxy Messier 101 is a composite of views from Spitzer, Hubble, and Chandra. The red color shows Spitzer's view in infrared light. It highlights the heat emitted by dust lanes in the galaxy where stars can form. The yellow color is Hubble's view in visible light. Most of this light comes from stars, and they trace the same spiral structure as the dust lanes. The blue color shows Chandra's view in X-ray light. Sources of X-rays include million-degree gas, exploded stars, and material colliding around black holes.

    Such composite images allow astronomers to see how features seen in one wavelength match up with those seen in another wavelength. It's like seeing with a camera, night vision goggles, and X-ray vision all at once.

    In the four centuries since Galileo, astronomy has changed dramatically. Yet our curiosity and quest for knowledge remain the same. So, too, does our wonder at the splendor of the universe.

    The International Year of Astronomy Great Observatories Image Unveiling is supported by the NASA Science Mission Directorate

  16. NASA's Great Observatories Celebrate the International Year of Astronomy

    NASA Technical Reports Server (NTRS)

    2009-01-01

    [figure removed for brevity, see original site] Click on the image for larger version

    In 1609, Galileo improved the newly invented telescope, turned it toward the heavens, and revolutionized our view of the universe. In celebration of the 400th anniversary of this milestone, 2009 has been designated as the International Year of Astronomy.

    Today, NASA's Great Observatories are continuing Galileo's legacy with stunning images and breakthrough science from the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory.

    While Galileo observed the sky using visible light seen by the human eye, technology now allows us to observe in many wavelengths, including Spitzer's infrared view and Chandra's view in X-rays. Each wavelength region shows different aspects of celestial objects and often reveals new objects that could not otherwise be studied.

    This image of the spiral galaxy Messier 101 is a composite of views from Spitzer, Hubble, and Chandra. The red color shows Spitzer's view in infrared light. It highlights the heat emitted by dust lanes in the galaxy where stars can form. The yellow color is Hubble's view in visible light. Most of this light comes from stars, and they trace the same spiral structure as the dust lanes. The blue color shows Chandra's view in X-ray light. Sources of X-rays include million-degree gas, exploded stars, and material colliding around black holes.

    Such composite images allow astronomers to see how features seen in one wavelength match up with those seen in another wavelength. It's like seeing with a camera, night vision goggles, and X-ray vision all at once.

    In the four centuries since Galileo, astronomy has changed dramatically. Yet our curiosity and quest for knowledge remain the same. So, too, does our wonder at the splendor of the universe.

    The International Year of Astronomy Great Observatories Image Unveiling is supported by the NASA Science Mission Directorate

  17. Space Subaru: great science observatories in the space station ERA

    NASA Astrophysics Data System (ADS)

    Takahashi, Yoshiyuki; Ebisuzaki, Toshikazu

    1998-08-01

    A concept of 'Space Factory' on the International Space Station Alpha (ISSA) is described. Following the four great observatories deployed by the Space Transportation System (STS), the next generation of great observatories would require a very large, 10-meter class optical telescope. A telescope of this size will require careful assembly and tuning by astronauts on orbit before deployment. Once built, it could visualize the universe to the earliest galaxies, and could explore the earth-like planet in other star- system. The 'Space Factory' is conceived by including four or five frontier astrophysics programs. Less demanding experiments could precede the construction of the most demanding optical telescope. Space SUBARU is a 10 meter- diameter optical telescope with a diffraction limited optics. Space-Submillimeter-and-IR-Telescope is a 20 meter- diameter sub-millimeter telescope. A 10-meter-cube telescope is for observing gamma-rays from 1 GeV to 10 TeV. The Multiple-OWL is an earth's night-sky-watcher for the highest energy cosmic rays. Space SUBARU envisages a plan of orbital construction, fine-tuning and deployment of large scale astrophysical instruments into the desired free-flying orbit. It incorporates physical aids of the robotics and extra-vehicle activities of astronauts.

  18. The origin of the Hawaiian Volcano Observatory

    SciTech Connect

    Dvorak, John

    2011-05-15

    I first stepped through the doorway of the Hawaiian Volcano Observatory in 1976, and I was impressed by what I saw: A dozen people working out of a stone-and-metal building perched at the edge of a high cliff with a spectacular view of a vast volcanic plain. Their primary purpose was to monitor the island's two active volcanoes, Kilauea and Mauna Loa. I joined them, working for six weeks as a volunteer and then, years later, as a staff scientist. That gave me several chances to ask how the observatory had started.

  19. The Great Geospace Observatory and Simultaneous Missions of Opportunity

    NASA Technical Reports Server (NTRS)

    Donovan, Eric; Brandt, Pontus; Sibeck, David; Spann, James; Lester, Mark

    2011-01-01

    A predictive understanding of the sun to geospace environment is one of the main goals of ILWS. This can only be achieved through a "system-level" approach, meaning long-term, simultaneous, continuous observations across the relevant scales of the magnetosphere and ionosphere/thermosphere (IT). To date such an approach, which must involve simultaneous, multi-scale, global imaging of different geospace regions, has not been carried out for a complete geomagnetic storm. Such imagery, now routine for the Solar community, is of critical scientific importance and captures public imagination. Its absence in geospace studies has limited the growth and impact of geospace science. In this presentation, we discuss a concept called the Great Geospace Observatory, which would involve coordinated geospace imaging through an international effort of multiple, simultaneous Missions of Opportunity. In this way, the cost would be spread among different agencies as well as putting remote sensors in vantage points optimized for each type of imaging. 24/7 auroral imaging from weather satellites on Molniya (or similar) orbits, EUV imaging of the plasmasphere from high-inclination orbits, continuous and global ENA imaging from geosynchronous commercial satellites, and continuous X-ray imaging of the cusp and magnetosheath from a high-altitude dedicated probe would quantitatively track system-level dynamics at through substorms, sawtooth events, steady magnetospheric convection, and storms; studying energy and mass coupling between the solar wind, magnetosphere, and the upper atmosphere. In our minds, The Great Geospace Observatory represents the next strategic step for ILWS and needs to be seriously considered.

  20. NASA's Great Observatories Celebrate International Year of Astronomy

    NASA Astrophysics Data System (ADS)

    2009-11-01

    A never-before-seen view of the turbulent heart of our Milky Way galaxy is being unveiled by NASA on Nov. 10. This event will commemorate the 400 years since Galileo first turned his telescope to the heavens in 1609. In celebration of this International Year of Astronomy, NASA is releasing images of the galactic center region as seen by its Great Observatories to more than 150 planetariums, museums, nature centers, libraries, and schools across the country. The sites will unveil a giant, 6-foot-by-3-foot print of the bustling hub of our galaxy that combines a near-infrared view from the Hubble Space Telescope, an infrared view from the Spitzer Space Telescope, and an X-ray view from the Chandra X-ray Observatory into one multiwavelength picture. Experts from all three observatories carefully assembled the final image from large mosaic photo surveys taken by each telescope. This composite image provides one of the most detailed views ever of our galaxy's mysterious core. Participating institutions also will display a matched trio of Hubble, Spitzer, and Chandra images of the Milky Way's center on a second large panel measuring 3 feet by 4 feet. Each image shows the telescope's different wavelength view of the galactic center region, illustrating not only the unique science each observatory conducts, but also how far astronomy has come since Galileo. The composite image features the spectacle of stellar evolution: from vibrant regions of star birth, to young hot stars, to old cool stars, to seething remnants of stellar death called black holes. This activity occurs against a fiery backdrop in the crowded, hostile environment of the galaxy's core, the center of which is dominated by a supermassive black hole nearly four million times more massive than our Sun. Permeating the region is a diffuse blue haze of X-ray light from gas that has been heated to millions of degrees by outflows from the supermassive black hole as well as by winds from massive stars and by stellar

  1. SPASE: Metadata Interoperability in the Great Observatory Environment

    NASA Astrophysics Data System (ADS)

    Thieman, J. R.; King, T. A.; Roberts, D. A.; King, J. H.

    2006-05-01

    SPASE is the Space Physics Archive Search and Extract project. This project is funded by NASA to provide a data model for the Great Observatory data environment that can be used as a common basis for locating and retrieving data of interest for the space and solar physics community. Common terminology that maps to much of the disparate metadata being used by these systems enables unified searches across the archives and ready comparison of the results to determine time overlaps, data commonalities, applicability for research purposes, etc. The SPASE Data Model Version 1.0 has been created and will be described. The model now needs to be tested by the community by describing a wide variety of data holdings and providing feedback for further improvement of the model. The latest version of the Data Model can be obtained by clicking on the Link marked "Current Draft" at the following web site: http://www.igpp.ucla.edu/spase/. Hundreds of data descriptions created with this model in mind have been entered into the Virtual Space Physics Observatory search engine called the "Space and Solar Physics Product Finder". We recommend exercising this system to find data of interest and to see the value of a common data model for search and retrieval. The VSPO Product Finder is available at the following URL: http://vspo.gsfc.nasa.gov/websearch/dispatcher. Future enhancements of the SPASE Data Model will include more depth of description to more fully describe the science content of a data set as well as automated tools to ease the task of describing data according to the Data Model. As always, the value of the SPASE effort will depend on the use and feedback by the space physics community.

  2. NASA's Great Observatories May Unravel 400-Year Old Supernova Mystery

    NASA Astrophysics Data System (ADS)

    2004-10-01

    Four hundred years ago, sky watchers, including the famous astronomer Johannes Kepler, best known as the discoverer of the laws of planetary motion, were startled by the sudden appearance of a "new star" in the western sky, rivaling the brilliance of the nearby planets. Kepler's Supernova Remnant Multiple Images of Kepler's Supernova Remnant Modern astronomers, using NASA's three orbiting Great Observatories, are unraveling the mysteries of the expanding remains of Kepler's supernova, the last such object seen to explode in our Milky Way galaxy. When a new star appeared Oct. 9, 1604, observers could use only their eyes to study it. The telescope would not be invented for another four years. A team of modern astronomers has the combined abilities of NASA's Great Observatories, the Spitzer Space Telescope (SST), Hubble Space Telescope (HST), and Chandra X-ray Observatory, to analyze the remains in infrared radiation, visible light, and X-rays. Ravi Sankrit and William Blair of the Johns Hopkins University in Baltimore lead the team. The combined image unveils a bubble-shaped shroud of gas and dust, 14 light-years wide and expanding at 4 million mph. Observations from each telescope highlight distinct features of the supernova, a fast-moving shell of iron-rich material, surrounded by an expanding shock wave sweeping up interstellar gas and dust. Interview with Dr. Ravi Sankrit Interview with Dr. Ravi Sankrit "Multi-wavelength studies are absolutely essential for putting together a complete picture of how supernova remnants evolve," Sankrit said. Sankrit is an associate research scientist, Center for Astrophysical Sciences at Hopkins and lead for HST astronomer observations. "For instance, the infrared data are dominated by heated interstellar dust, while optical and X-ray observations sample different temperatures of gas," Blair added. Blair is a research professor, Physics and Astronomy Department at Hopkins and lead astronomer for SST observations. "A range of

  3. Briefings Set for Launch of Next "Great Observatory" in Space

    NASA Astrophysics Data System (ADS)

    1999-06-01

    NASA's next Space Shuttle flight will provide astronomers with a new look at the universe and make history with NASA's first female mission commander. Reporters can get an overview of the mission at a series of briefings July 7. The briefings will begin at 9 a.m. EDT at NASA's Johnson Space Center in Houston. The five-day flight is scheduled for launch no earlier than July 20. STS-93 will be led by U.S. Air Force Colonel Eileen Collins, the first woman to command an American space mission. The flight's primary objective will be to deploy the Chandra X-Ray Observatory, the third of NASA's Great Observatories. Collins and her crew of four will carry Chandra, the heaviest payload ever deployed from the shuttle, into orbit and deploy it approximately seven hours after launch. An upper stage will carry the observatory to its final orbit, more than one-third of the way to the Moon. Chandra will allow scientists to obtain unprecedented X-ray images of exploding stars, black holes and other exotic environments to help them understand the structure and evolution of the universe. The first two briefings will provide an overview of mission operations and science to be conducted by Chandra. The NASA Television Video File will follow at noon. The crew press conference will begin at 2 p.m. EDT. The briefings will be carried live on NASA Television, with question-and-answer capability for reporters covering the event from participating NASA centers. NASA Television is available on transponder 9C of the GE-2 satellite at 85 degrees West longitude, vertical polarization, frequency 3880 MHz, audio of 6.8 MHz. Media planning to attend the briefings must notify the Johnson Space Center newsroom by June 28 to ensure proper badging. Each reporter's name, affiliation and country of citizenship should be faxed to the newsroom at 281/483-2000. IMPORTANT NOTE: Reporters can schedule in-person or telephone interviews STS-93 crew. These interviews will begin at about 3:15 p.m. EDT. Media

  4. Great Observatories Unique Views of the Milky Way

    NASA Image and Video Library

    2009-11-10

    In celebration of the International Year of Astronomy 2009, NASA's Great Observatories -- the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory -- have produced a matched trio of images of the central region of our Milky Way galaxy. Each image shows the telescope's different wavelength view of the galactic center region, illustrating the unique science each observatory conducts. In this spectacular image, observations using infrared light and X-ray light see through the obscuring dust and reveal the intense activity near the galactic core. Note that the center of the galaxy is located within the bright white region to the right of and just below the middle of the image. The entire image width covers about one-half a degree, about the same angular width as the full moon. Spitzer's infrared-light observations provide a detailed and spectacular view of the galactic center region [Figure 1 (top frame of poster)]. The swirling core of our galaxy harbors hundreds of thousands of stars that cannot be seen in visible light. These stars heat the nearby gas and dust. These dusty clouds glow in infrared light and reveal their often dramatic shapes. Some of these clouds harbor stellar nurseries that are forming new generations of stars. Like the downtown of a large city, the center of our galaxy is a crowded, active, and vibrant place. Although best known for its visible-light images, Hubble also observes over a limited range of infrared light [Figure 2 (middle frame of poster)]. The galactic center is marked by the bright patch in the lower right. Along the left side are large arcs of warm gas that have been heated by clusters of bright massive stars. In addition, Hubble uncovered many more massive stars across the region. Winds and radiation from these stars create the complex structures seen in the gas throughout the image.This sweeping panorama is one of the sharpest infrared pictures ever made of the galactic center region. X

  5. Chandra: Ten Years of Amazing Science with a Great Observatory

    NASA Technical Reports Server (NTRS)

    Weisskopf, Martin C.

    2009-01-01

    We review briefly review the history of the development of the Chandra X-Ray Observatory, highlighting certain details that many attendees of this Conference might not be aware of. We then present a selection of scientific highlights of the first 10 years of this remarkable and unique mission.

  6. Estimation of Observatory Geoelectric Fields Induced during Great Magnetic Storms

    NASA Astrophysics Data System (ADS)

    Love, J. J.; Swidinsky, A.

    2014-12-01

    In support of a project for monitoring hazards for electric power grids, we present a new method for estimating electric fields that are induced in the Earth's interior at a particular site during magnetic storms. For this, we adopt a model of the electrical conductivity of the lithosphere that is simple but sufficient to model most variation in the induced geoelectric field: two horizontal layers, each with uniform electrical conductivity properties that can be parameterized by a galvanic distortion tensor. After Laplace transformation of the induction equations into the complex frequency domain, we obtain an electromagnetic impedance function. Upon inverse transformation back to the time domain, convolution of the impedance tensor with a geomagnetic time series yields an estimated geoelectric time series. We optimize the model conductivity parameters using 1-sec resolution magnetic and electric field data collected at the Kakioka magnetic observatory during the October 2003 Halloween storm. We validate the algorithm against Kakioka magnetic and electric field data for the July 2000 Bastille-Day storm. Finally, we infer 1-sec geoelectric fields that were realized (but not directly measured) in Japan during the 1989 Quebec storm. Results highlight the need for improved ground-level monitoring of geomagnetic and geoelectric fields. They also reveal the need for accommodating the galvanic distortion of three-dimensional conductivity when predicting geoelectric fields in the lithosphere and geomagnetically induced currents in electric power grids.

  7. The COMPTON Observatory: Reflections on its origins and history

    SciTech Connect

    Kniffen, D. A.; Gehrels, N.

    1997-05-10

    The Gamma Ray Observatory (GRO) was planned as a mission to make the first comprehensive study of the gamma-ray sky over the full gamma-ray spectrum. It followed on the heels of two successful small astronomy satellites with high energy gamma-ray telescopes, SAS-2 and COS-B, and the High Energy Astronomical Observatory (HEAO) with low-energy gamma-ray detectors. The guideline was to cover the spectrum from the high energy limit of the x-ray domain to the highest energies for which a detectable flux might be reasonably observed. The objective was to include transients as well as persistent sources. The efforts to get such a mission approved stands as a model for developing a consensus of the scientific community for a mission involving a relatively small community of observers. A broad and vigorous guest investigator program was a key element in this effort. The results of the guest investigator program are testimony to the wisdom of this plan. The great success of GRO (now the Compton Observatory) was a result of the dedicated efforts of a few individuals and a project management team that understood how to work with scientists. In spite of increasing budgetary pressure and long delays beyond their control, the project management brought GRO to its successful launch with a minimum of cost growth resulting from the delays. This development period set the stage for what has been one of the most successful scientific programs in NASA's history. The very exciting results presented at this conference by a very broad community of scientists is a testimony to the dedicated efforts of a small group of visionaries with the foresight to see the potential of such a mission.

  8. AVOCADO: A Virtual Observatory Census to Address Dwarfs Origins

    NASA Astrophysics Data System (ADS)

    Sánchez-Janssen, Rubén; Sánchez-Janssen

    2011-12-01

    Dwarf galaxies are by far the most abundant of all galaxy types, yet their properties are still poorly understood-especially due to the observational challenge that their intrinsic faintness represents. AVOCADO aims at establishing firm conclusions on their formation and evolution by constructing a homogeneous, multiwavelength dataset for a statistically significant sample of several thousand nearby dwarfs (-18 < Mi < -14). Using public data and Virtual Observatory tools, we have built GALEX+SDSS+2MASS spectral energy distributions that are fitted by a library of single stellar population models. Star formation rates, stellar masses, ages and metallicities are further complemented with structural parameters that can be used to classify them morphologically. This unique dataset, coupled with a detailed characterization of each dwarf's environment, allows for a fully comprehensive investigation of their origins and to track the (potential) evolutionary paths between the different dwarf types.

  9. The Great Observatories Origins Deep Survey (GOODS): Overview and Status

    NASA Astrophysics Data System (ADS)

    Hook, R. N.; GOODS Team

    2002-12-01

    GOODS is a very large project to gather deep imaging data and spectroscopic followup of two fields, the Hubble Deep Field North (HDF-N) and the Chandra Deep Field South (CDF-S), with both space and ground-based instruments to create an extensive multiwavelength public data set for community research on the distant Universe. GOODS includes a SIRTF Legacy Program (PI: Mark Dickinson) and a Hubble Treasury Program of ACS imaging (PI: Mauro Giavalisco). The ACS imaging was also optimized for the detection of high-z supernovae which are being followed up by a further target of opportunity Hubble GO Program (PI: Adam Riess). The bulk of the CDF-S ground-based data presently available comes from an ESO Large Programme (PI: Catherine Cesarsky) which includes both deep imaging and multi-object followup spectroscopy. This is currently complemented in the South by additional CTIO imaging. Currently available HDF-N ground-based data forming part of GOODS includes NOAO imaging. Although the SIRTF part of the survey will not begin until later in the year the ACS imaging is well advanced and there is also a huge body of complementary ground-based imaging and some follow-up spectroscopy which is already publicly available. We summarize the current status of GOODS and give an overview of the data products currently available and present the timescales for the future. Many early science results from the survey are presented in other GOODS papers at this meeting. Support for the HST GOODS program presented here and in companion abstracts was provided by NASA thorugh grant number GO-9425 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.

  10. The Sun-Solar System Connection Great Observatory: Virtual, but Nearing Reality

    NASA Astrophysics Data System (ADS)

    Roberts, D. A.; King, J.; Rezapkin, V.

    2005-05-01

    The collection of spacecraft and ground-based observatories that measure photons, fields, and particles from the Sun and solar system can function as a Great Observatory if the resulting data products are united through services that make them seamlessly available to researchers. Virtual Observatories, begun as ways of viewing the sky in all wavelengths from a desktop computer, should allow us to reach this goal. Major strides have been made in designing architectures and operational systems that allow scientists to rapidly gather, visualize, and process widely-distributed data from highly varied instruments. This talk will present the current state-of-the art and a vision for the future of "VS3O." The eGY is very well timed to be a focal point for these efforts on an international scale.

  11. Kepler's Supernova Studied Through the Combined Abilities of NASA's Great Observatories

    NASA Technical Reports Server (NTRS)

    2004-01-01

    Four hundred years ago, sky watchers, including the famous astronomer Johannes Kepler, best known as the discoverer of the laws of planetary motion, were startled by the sudden appearance of a new star in the western sky, rivaling the brilliance of the nearby planets. Modern astronomers, using NASA's three orbiting Great Observatories, are unraveling the mysteries of the expanding remains of Kepler's supernova, the last such object seen to explode in our Milky Way galaxy. When a new star appeared Oct. 9, 1604, observers could use only their eyes to study it. The telescope would not be invented for another four years. A team of modern astronomers has the combined abilities of NASA's Great Observatories, the Spritzer Space Telescope (SST), Hubble Space Telescope (HST), and Chandra X-Ray Observatory (CXO), to analyze the remains in infrared radiation, visible light, and X-rays. Visible-light images from Hubble's Advanced Camera for Surveys reveal where the supernova shock wave is slamming into the densest regions of surrounding gas. The astronomers used the SST to probe for material that radiates in infrared light, which shows heated microscopic dust particles that have been swept up by the supernova shock wave. The CXO data show regions of very hot gas. The combined image unveils a bubble-shaped shroud of gas and dust, 14 light-years wide and expanding at 4 million mph. There have been six known supernovas in our Milky Way over the past 1,000 years. Kepler's is the only one in which astronomers do not know what type of star exploded. By combining information from all three Great Observatories, astronomers may find the clues they need. Project management for both the HST and CXO programs is the responsibility of NASA's Marshall Space Flight Center in Huntsville, Alabama.

  12. Kepler's Supernova Studied Through the Combined Abilities of NASA's Great Observatories

    NASA Technical Reports Server (NTRS)

    2004-01-01

    Four hundred years ago, sky watchers, including the famous astronomer Johannes Kepler, best known as the discoverer of the laws of planetary motion, were startled by the sudden appearance of a new star in the western sky, rivaling the brilliance of the nearby planets. Modern astronomers, using NASA's three orbiting Great Observatories, are unraveling the mysteries of the expanding remains of Kepler's supernova, the last such object seen to explode in our Milky Way galaxy. When a new star appeared Oct. 9, 1604, observers could use only their eyes to study it. The telescope would not be invented for another four years. A team of modern astronomers has the combined abilities of NASA's Great Observatories, the Spritzer Space Telescope (SST), Hubble Space Telescope (HST), and Chandra X-Ray Observatory (CXO), to analyze the remains in infrared radiation, visible light, and X-rays. Visible-light images from Hubble's Advanced Camera for Surveys reveal where the supernova shock wave is slamming into the densest regions of surrounding gas. The astronomers used the SST to probe for material that radiates in infrared light, which shows heated microscopic dust particles that have been swept up by the supernova shock wave. The CXO data show regions of very hot gas. The combined image unveils a bubble-shaped shroud of gas and dust, 14 light-years wide and expanding at 4 million mph. There have been six known supernovas in our Milky Way over the past 1,000 years. Kepler's is the only one in which astronomers do not know what type of star exploded. By combining information from all three Great Observatories, astronomers may find the clues they need. Project management for both the HST and CXO programs is the responsibility of NASA's Marshall Space Flight Center in Huntsville, Alabama.

  13. The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry

    NASA Astrophysics Data System (ADS)

    Chu, Jason K.; Sanders, D. B.; Larson, K. L.; Mazzarella, J. M.; Howell, J. H.; Díaz-Santos, T.; Xu, K. C.; Paladini, R.; Schulz, B.; Shupe, D.; Appleton, P.; Armus, L.; Billot, N.; Chan, B. H. P.; Evans, A. S.; Fadda, D.; Frayer, D. T.; Haan, S.; Ishida, C. M.; Iwasawa, K.; Kim, D.-C.; Lord, S.; Murphy, E.; Petric, A.; Privon, G. C.; Surace, J. A.; Treister, E.

    2017-04-01

    Far-infrared images and photometry are presented for 201 Luminous and Ultraluminous Infrared Galaxies [LIRGs: log ({L}{IR}/{L}⊙ )=11.00{--}11.99, ULIRGs: log ({L}{IR}/{L}⊙ )=12.00{--}12.99], in the Great Observatories All-Sky LIRG Survey (GOALS), based on observations with the Herschel Space Observatory Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) instruments. The image atlas displays each GOALS target in the three PACS bands (70, 100, and 160 μm) and the three SPIRE bands (250, 350, and 500 μm), optimized to reveal structures at both high and low surface brightness levels, with images scaled to simplify comparison of structures in the same physical areas of ˜100 × 100 kpc2. Flux densities of companion galaxies in merging systems are provided where possible, depending on their angular separation and the spatial resolution in each passband, along with integrated system fluxes (sum of components). This data set constitutes the imaging and photometric component of the GOALS Herschel OT1 observing program, and is complementary to atlases presented for the Hubble Space Telescope, Spitzer Space Telescope, and Chandra X-ray Observatory. Collectively, these data will enable a wide range of detailed studies of active galactic nucleus and starburst activity within the most luminous infrared galaxies in the local universe. Based on Herschel Space Observatory observations. Herschel is an ESA space observatory with science instruments provided by the European-led Principal Investigator consortia, and important participation from NASA.

  14. Supporting the SSSC Great Observatory: S3C Active Archive Data and Services Today

    NASA Astrophysics Data System (ADS)

    Kovalick, T.; McGuire, R.; Bilitza, D.; Candey, R.; Chimiak, R.; Cooper, J.; Fung, S.; Han, D.; Harris, B.; Johnson, R.; Kessel, R.; Klipsch, C.; Leckner, H.; Liu, M.; Papatishvili, N.

    2005-12-01

    The next advances in Sun Solar System Connections (S3C) / Solar-Terrestrial science require an increasingly integrated and transparent data environment, where data can be easily accessed and used across the boundaries of both missions and traditional disciplines. While the data environment to best support the longterm strategic and science goals of the S3C Great Observatory will grow over time, the S3C Active Archive within the Space Physics Data Facility (SPDF) already operates uniquely important multi-mission data services with current data from most operating space physics missions. This paper reviews the range of services now available for data and how they are now evolving to meet the future science issues of the Great Observatory program and the needs of programs like LWS/ILWS. The Coordinated Data Analysis [Workshop] Web (CDAWeb) and Satellite Situation Center Web (SSCWeb), critically supported by the Common Data Format (CDF) effort and supplemented by more focused services such as data format translations, COHOWeb, ATMOWeb, FTPBrowser, ModelWeb and HelioWeb, are important current examples suggestive of the scope and functionality needed in the future. These systems serve the broad international community now and are already capable of significant contributions to eGY. Our new Java-based "CDAWeb Plus" interface integrates unified user access to this combined set. Key services increasingly support web services APIs to allow their ready invocation from distributed external middleware and clients expected to form the framework of a new Virtual discipline Observatory (VxO) paradigm for the data environment for NASA solar and space physics data.

  15. NASA's Great Observatories Celebrate the International Year of Astronomy With a National Unveiling of Spectacular Images

    NASA Astrophysics Data System (ADS)

    2009-02-01

    In 1609, Galileo first turned his telescope to the heavens and gave birth to modern astronomy. To commemorate four hundred years of exploring the universe, 2009 is designated the International Year of Astronomy. NASA's Great Observatories - the Hubble Space Telescope, Spitzer Space Telescope, and Chandra X-ray Observatory - are marking the occasion with the release of a suite of images at over 100 planetariums, museums, nature centers, and schools across the country in conjunction with Galileo's birthday on February 15. The selected sites will unveil a large 9-square-foot print of the spiral galaxy Messier 101 that combines the optical view of Hubble, the infrared view of Spitzer, and the X-ray view of Chandra into one multi-wavelength picture. "It's like using your eyes, night vision goggles, and X-ray vision all at the same time," says Dr. Hashima Hasan, lead scientist for the International Year of Astronomy at NASA Headquarters in Washington. Cas A animation Chandra X-ray Image of M101 Participating institutions also will display a matched trio of Hubble, Spitzer, and Chandra images of Messier 101. Each image shows a different wavelength view of the galaxy that illustrates not only the different science uncovered by each observatory, but also just how far astronomy has come since Galileo. Messier 101 is a face-on spiral galaxy about 22 million light-years away in the constellation Ursa Major. It is in many ways similar to, but larger than, our own Milky Way galaxy. Hubble's visible light view shows off the swirls of bright stars and glowing gas that give the galaxy its nickname the Pinwheel Galaxy. In contrast, Spitzer's infrared-light image sees into the spiral arms and reveals the glow of dust lanes where dense clouds can collapse to form new stars. Chandra's X-ray picture uncovers the high-energy features in the galaxy, such as remnants of exploded stars or matter zooming around black holes. The juxtaposition of observations from these three telescopes

  16. Great science observatories in the space station era and OWL efforts in Japan

    NASA Astrophysics Data System (ADS)

    Takahashi, Yoshiyuki

    1998-06-01

    A concept of ``Space Factory'' on the International Space Station Alpha (ISSA) is described. By following the four great observatories that purposefully took advantage of the Space Transportation System (STS), the next generation of great observatories is considered. These new astronomical projects require a very large optical telescope whose diameter is of the order of 10 m. Space telescope of this size will require careful assembly and tuning by astronauts on orbit before deployment. Once built, it could visualize the universe to the earliest galaxies, and could explore the earth-like planet in other star-system. The ``Space Factory'' would permit other large-scale observatories for construction in space. A step-by-step advancement of the ``Space Factory'' is conceived by including four or five frontier astrophysics programs. Less demanding experiments would precede the construction project of the most demanding optical telescope. A study in Japan to observe the highest energy cosmic rays from space is synchronized with those being carried out by the OWL team in the USA and the AIRWATCH team in Italy. The Japanese efforts are coordinated in a larger program study of the Space SUBARU, which envisages a plan of orbital construction, fine-tuning and eventual deployment of large scale astrophysical instruments into the desired free-flying orbit. A space observatory of the highest energy cosmic rays can be maximized by a cluster of 6 or 7 units of the wide-angle OWL telescopes, each having a field-of-view (FOV) of ~60°. The ultimate viewing area could be up to 6,000 km×6,000 km, the entire horizon for a 1000 km orbit. Within this large detection area about 105 cosmic hadronic events at above 1020 eV would be observed in a year. It also makes possible to observe the highest energy neutrinos from the known source mechanisms; including cosmic photo-production. Neutrino events from Topological Defects, Gamma Ray Burst fireballs and Blazers are observable as frequently

  17. Origin and status of the Great Lakes wolf.

    PubMed

    Koblmüller, Stephan; Nord, Maria; Wayne, Robert K; Leonard, Jennifer A

    2009-06-01

    An extensive debate concerning the origin and taxonomic status of wolf-like canids in the North American Great Lakes region and the consequences for conservation politics regarding these enigmatic predators is ongoing. Using maternally, paternally and biparentally inherited molecular markers, we demonstrate that the Great Lakes wolves are a unique population or ecotype of gray wolves. Furthermore, we show that the Great Lakes wolves experienced high degrees of ancient and recent introgression of coyote and western gray wolf mtDNA and Y-chromosome haplotypes, and that the recent demographic bottleneck caused by persecution and habitat depletion in the early 1900s is not reflected in the genetic data.

  18. Perchlorate in the Great Lakes: isotopic composition and origin.

    PubMed

    Poghosyan, Armen; Sturchio, Neil C; Morrison, Candice G; Beloso, Abelardo D; Guan, Yunbin; Eiler, John M; Jackson, W Andrew; Hatzinger, Paul B

    2014-10-07

    Perchlorate is a persistent and mobile contaminant in the environment with both natural and anthropogenic sources. Stable isotope ratios of oxygen (δ(18)O, Δ(17)O) and chlorine (δ(37)Cl) along with the abundance of the radioactive isotope (36)Cl were used to trace perchlorate sources and behavior in the Laurentian Great Lakes. These lakes were selected for study as a likely repository of recent atmospheric perchlorate deposition. Perchlorate concentrations in the Great Lakes range from 0.05 to 0.13 μg per liter. δ(37)Cl values of perchlorate from the Great Lakes range from +3.0‰ (Lake Ontario) to +4.0‰ (Lake Superior), whereas δ(18)O values range from -4.1‰ (Lake Superior) to +4.0‰ (Lake Erie). Great Lakes perchlorate has mass-independent oxygen isotopic variations with positive Δ(17)O values (+1.6‰ to +2.7‰) divided into two distinct groups: Lake Superior (+2.7‰) and the other four lakes (∼+1.7‰). The stable isotopic results indicate that perchlorate in the Great Lakes is dominantly of natural origin, having isotopic composition resembling that measured for indigenous perchlorate from preindustrial groundwaters of the western USA. The (36)Cl/Cl ratio of perchlorate varies widely from 7.4 × 10(-12) (Lake Ontario) to 6.7 × 10(-11) (Lake Superior). These (36)ClO4(-) abundances are consistent with an atmospheric origin of perchlorate in the Great Lakes. The relatively high (36)ClO4(-) abundances in the larger lakes (Lakes Superior and Michigan) could be explained by the presence of (36)Cl-enriched perchlorate deposited during the period of elevated atmospheric (36)Cl activity following thermonuclear bomb tests in the Pacific Ocean.

  19. Image of the Great Nebula in Andromeda, M31 Taken by the High Energy Astronomy Observatory (HEAO)-2

    NASA Technical Reports Server (NTRS)

    1978-01-01

    Both of the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory imaging devices were used to observe the Great Nebula in Andromeda, M31. This is a smaller field and more detailed view of the central region of the Great Nebula in Andromeda, M31, taken with the High Resolution Imager. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  20. NASA Astrophysics Education and Public Outreach: Engaging the Public with NASA's Next Great Observatory

    NASA Astrophysics Data System (ADS)

    Green, Joel David; Jirdeh, Hussein; Eisenhamer, Bonnie; Smith, Denise Anne

    2015-08-01

    The James Webb Space Telescope is the successor to the Hubble Space Telescope. STScI and the Office of Public Outreach are committed to bringing awareness of the technology, the excitement, and the future science potential of this great observatory to the public, to educators and students, and to the scientific community, prior to its 2018 launch. We currently engage the full range of the public and scientific communities using a variety of high impact, memorable initiatives, in combination with modern technologies to extend reach, linking the science goals of Webb to the ongoing discoveries being made by Hubble. We have injected Webb-specific content into ongoing E/PO programs: for example, active classroom learning via the STEM Innovation Project (SIP) and 3-D visualizations developed for modern inexpensive platforms, the production and collection of materials for speakers related to any Webb topic (engineering, science, or education), the addition of Webb materials to the Amazing Space programs and updating them for general usage, and the development of simulated Webb observations illustrating the science of the next decade.

  1. Spitzer Space Telescope Leads NASA's Great Observatories to Uncover Black Holes and Other Hidden Objects in the Distant Universe

    NASA Astrophysics Data System (ADS)

    2004-06-01

    Astronomers unveiled the deepest images from NASA's new Spitzer Space Telescope today, and announced the detection of distant objects -- including several supermassive black holes -- that are nearly invisible in even the deepest images from telescopes operating at other wavelengths. Mark Dickinson, of the National Optical Astronomy Observatory in Tucson, Ariz., and Principal Investigator for the new observations, says, "With these ultra-deep Spitzer images, we are easily seeing objects throughout time and space, out to redshifts of 6 or more, where the most distant known galaxies lie. Moreover, we see some objects that are completely invisible to optical telescopes, but whose existence was hinted at by previous observations from the Chandra and Hubble Observatories." Seven of the objects detected in the Spitzer images may be part of the long-sought population of "missing" supermassive black holes that powered the bright cores of the earliest active galaxies. The discovery finally completes a full accounting of all the X-ray sources seen in one of the deepest surveys of the universe ever taken. This detective story required no less than the combined power of NASA's three Great Observatories in space -- the Hubble Space Telescope, the Chandra X-ray Observatory, and the Spitzer Space Telescope. Each observatory works with different wavelengths of electromagnetic radiation, from the high-energy X-rays that Chandra detects, through visible light with Hubble, and into the infrared with Spitzer. The combination of these telescopes yields far more information than any single instrument would. All three telescopes peered out to distances of up to 13 billion light-years toward a small patch of the southern sky containing more than 10,000 galaxies, in a coordinated project called the Great Observatories Origins Deep Survey (or GOODS, for short). Chandra images detected over two hundred X-ray sources believed to be supermassive black holes lying in the centers of young

  2. NASA and Japanese X-ray observatories Clarify Origin of Cosmic Rays

    NASA Technical Reports Server (NTRS)

    2005-01-01

    Recent observations from NASA and Japanese X-ray observatories have helped clarify one of the long-standing mysteries in astronomy -- the origin of cosmic rays. This image from Japan's Suzaku X-ray observatory shows RXJ1713.7-3946. This supernova remnant is the gaseous remnant of a massive star that exploded. The remnant is about 1,600 years old. The contour lines show where gamma-ray intensity is highest, as measured by the High Energy Stereoscopic System (HESS) in Namibia.

  3. NASA and Japanese X-ray observatories Clarify Origin of Cosmic Rays

    NASA Technical Reports Server (NTRS)

    2005-01-01

    Recent observations from NASA and Japanese X-ray observatories have helped clarify one of the long-standing mysteries in astronomy -- the origin of cosmic rays. This image from Japan's Suzaku X-ray observatory shows RXJ1713.7-3946. This supernova remnant is the gaseous remnant of a massive star that exploded. The remnant is about 1,600 years old. The contour lines show where gamma-ray intensity is highest, as measured by the High Energy Stereoscopic System (HESS) in Namibia.

  4. The Virtual Great Observatory: Do We Know How to Make It Real?

    NASA Astrophysics Data System (ADS)

    McGuire, R. E.; Roberts, D. A.

    2005-12-01

    The goal of the SSSC Great Observatory (GO), to use "simultaneous measurements in multiple locations ... to resolve temporal and spatial changes and to understand the interactions of complex systems of regimes", demands a future data environment where users can see data resources as an integrated set. Where data from solar and space physics missions, models and services may be highly distributed, such an integrated view is the paradigm of a Virtual Observatory (VO) or inter-connected Virtual discipline Observatories (VxOs). A first concern to achieving an effective VO/VxO environment must always be that the maximum of potentially useful data and models are openly accessible and made readily findable, with appropriate keywords for search engines and registries of products and services for rapid and uniform access to data from geographically distributed sources in a range of formats and described by different sets of terms. But beyond this, there is no agreed and prioritized list of issues and most critical user requirements for the new data environment. The level of community commitment required to develop consensus on the most urgent needs and to make investigation data usefully accessible to the larger environment will be much deeper than has been seen in the past. At the highest level, we believe that science users want easy-to-use interfaces with reasonable functionality across different types of data and robust performance over a wide range of high resolution, high quality and current data. The skills of both solar/space physics investigators and technologists will be required to build and sustain effective coordination and overall data content. There has been some recent success in providing access to files and some basic services from many distributed sources (e.g., VSO, VSPO, and EGSO). But a possible next level of integration, in which variables are labeled and can be subsetted and supplied in standard ways for use by universal tools and in higher

  5. Cyberinfrastructure for remote environmental observatories: a model homogeneous sensor network in the Great Basin, USA

    NASA Astrophysics Data System (ADS)

    Strachan, Scotty; Slater, David; Fritzinger, Eric; Lyles, Bradley; Kent, Graham; Smith, Kenneth; Dascalu, Sergiu; Harris, Frederick

    2017-04-01

    Sensor-based data collection has changed the potential scale and resolution of in-situ environmental studies by orders of magnitude, increasing expertise and management requirements accordingly. Cost-effective management of these observing systems is possible by leveraging cyberinfrastructure resources. Presented is a case study environmental observation network in the Great Basin region, USA, the Nevada Climate-ecohydrological Assessment Network (NevCAN). NevCAN stretches hundreds of kilometers across several mountain ranges and monitors climate and ecohydrological conditions from low desert (900 m ASL) to high subalpine treeline (3360 m ASL) down to 1-minute timescales. The network has been operating continuously since 2010, collecting billions of sensor data points and millions of camera images that record hourly conditions at each site, despite requiring relatively low annual maintenance expenditure. These data have provided unique insight into fine-scale processes across mountain gradients, which is crucial scientific information for a water-scarce region. The key to maintaining data continuity for these remotely-located study sites has been use of uniform data transport and management systems, coupled with high-reliability power system designs. Enabling non-proprietary digital communication paths to all study sites and sensors allows the research team to acquire data in near-real-time, troubleshoot problems, and diversify sensor hardware. A wide-area network design based on common Internet Protocols (IP) has been extended into each study site, providing production bandwidth of between 2 Mbps and 60 Mbps, depending on local conditions. The network architecture and site-level support systems (such as power generation) have been implemented with the core objectives of capacity, redundancy, and modularity. NevCAN demonstrates that by following simple but uniform "best practices", the next generation of regionally-specific environmental observatories can evolve to

  6. Image of the Great Nebula in Andromeda, M31 Taken by the High Energy Astronomy Observatory (HEAO)-2

    NASA Technical Reports Server (NTRS)

    1978-01-01

    Both of the High Energy Astronomy Observatory (HEAO) 2/Einstein Observatory imaging devices were used to observe the Great Nebula in Andromeda, M31. This image is a wide field x-ray view of the center region of M31 by the HEAO-2's Imaging Proportional Counter. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  7. Prototyping a large-scale distributed system for the Great Observatories era - NASA Astrophysics Data System (ADS)

    NASA Technical Reports Server (NTRS)

    Shames, Peter

    1990-01-01

    The NASA Astrophysics Data System (ADS) is a distributed information system intended to support research in the Great Observatories era, to simplify access to data, and to enable simultaneous analyses of multispectral data sets. Here, the user agent and interface, its functions, and system components are examined, and the system architecture and infrastructure is addressed. The present status of the system and related future activities are examined.

  8. Prototyping a large-scale distributed system for the Great Observatories era - NASA Astrophysics Data System (ADS)

    NASA Technical Reports Server (NTRS)

    Shames, Peter

    1990-01-01

    The NASA Astrophysics Data System (ADS) is a distributed information system intended to support research in the Great Observatories era, to simplify access to data, and to enable simultaneous analyses of multispectral data sets. Here, the user agent and interface, its functions, and system components are examined, and the system architecture and infrastructure is addressed. The present status of the system and related future activities are examined.

  9. Perchlorate in The Great Lakes: Distribution, Isotopic Composition and Origin

    NASA Astrophysics Data System (ADS)

    Poghosyan, A.; Sturchio, N. C.; Jackson, W. A.; Guan, Y.; Eiler, J. M.; Hatzinger, P. B.

    2013-12-01

    Concentrations, stable chlorine and oxygen isotopic compositions, and 36Cl abundances of perchlorate were investigated in the five Laurentian Great Lakes. Samples were collected during monitoring cruises in 2007 and 2008 of the U.S. EPA's RV Lake Guardian and in 2010 at the water supply intake of Marquette, MI on the southern shore of Lake Superior. Concentrations of perchlorate were measured by IC/MS/MS at 24 locations, including one or two depth profiles in each lake. Mean concentrations (μg/L) are: Superior, 0.06 × 0.01; Michigan, 0.10 × 0.01; Huron, 0.11 × 0.01; Erie, 0.08 × 0.01, and Ontario, 0.09 × 0.01. Concentration vs. depth is nearly constant in each lake, indicating well-mixed conditions. Perchlorate was extracted from near-surface water by passing 15,000 to 80,000 L of water through 1-L cartridges containing Purolite A530E bifunctional anion-exchange resin. In the laboratory, perchlorate was eluted from the resin, purified, and precipitated as a >99% pure crystalline phase. Milligram amounts were recovered from each lake. Chlorine and oxygen isotopic analyses were performed at Caltech using the Cameca 7f-GEO SIMS instrument, following validation of the SIMS method with analyses of USGS-37 and USGS-38 isotopic reference materials. Results indicate a relatively narrow range in δ37Cl values (+2.9 to +3.9 ‰) and a wider range in δ18O values (-4.0 to +4.1 ‰), with a general geographic trend of increasing δ18O from west to east. Oxygen-17 was measured at UIC using dual-inlet IRMS of O2 produced by decomposition of KClO4. Great Lakes perchlorate has mass-independent oxygen isotopic variations with positive Δ17O values (+1.6 ‰ to +2.7 ‰) divided into two distinct groups: Lake Superior (+2.7 ‰) and the other four lakes (~ +1.7 ‰). The isotopic data indicate that perchlorate is dominantly of natural origin, having stable isotopic compositions resembling those of perchlorate from pre-industrial groundwaters in the western USA. The 36Cl

  10. The Star Formation Observatory (SFO) mission to study cosmic origins near and far

    NASA Astrophysics Data System (ADS)

    Scowen, Paul A.; Jansen, Rolf; Beasley, Matthew; Cooke, Brian; Nikzad, Shouleh; Siegmund, Oswald; Woodruff, Robert; Calzetti, Daniela; Desch, Steven; Fullerton, Alex; Gallagher, John; Malhotra, Sangeeta; McCaughrean, Mark; O'Connell, Robert; Oey, Sally; Padgett, Debbie; Rhoads, James; Roberge, Aki; Smith, Nathan; Stern, Daniel; Tumlinson, Jason; Windhorst, Rogier

    2008-07-01

    The Star Formation Observatory (SFO) is a 1.65m space telescope that addresses pivotal components in the 2007 NASA Science Plan, with a primary focus on Cosmic Origins. The design under consideration provides 100 times greater imaging efficiency and >10 times greater spectroscopic efficiency below 115 nm than existed on previous missions. The mission has a well-defined Origins scientific program at its heart: a statistically significant survey of local, intermediate, and high-redshift sites and indicators of star formation, to investigate and understand the range of environments, feedback mechanisms, and other factors that most affect the outcome of the star and planet formation process. This program relies on focused capabilities unique to space and that no other planned NASA mission will provide: near- UV/visible (20-1100 nm) wide-field, diffraction-limited imaging; and high-efficiency, low- and high- resolution (R~40,000) UV (100-175 nm) spectroscopy using far-UV optimized coatings and recent advances in Micro-Channel Plate (MCP) detector technology. The Observatory imager has a field of view in excess of 17' × 17' (>250 arcmin2) and uses a dichroic to create optimized UV/blue and red/near-IR channels for simultaneous observations, employing detectors that offer substantial quantum efficiency gains and that suffer lower losses due to cosmic rays.

  11. Are the Odds Against the Origin of Life Too Great?

    ERIC Educational Resources Information Center

    Carrier, Richard

    2000-01-01

    Statistics are offered to "prove" odds against the origin of life. Presents a summary analysis of all known examples to be used to check these claims whenever they are brought up in conversations, debates, books, or articles. Addresses scientific work misused by anti-evolutionists and the pseudoscientific assertions of the…

  12. Are the Odds Against the Origin of Life Too Great?

    ERIC Educational Resources Information Center

    Carrier, Richard

    2000-01-01

    Statistics are offered to "prove" odds against the origin of life. Presents a summary analysis of all known examples to be used to check these claims whenever they are brought up in conversations, debates, books, or articles. Addresses scientific work misused by anti-evolutionists and the pseudoscientific assertions of the…

  13. What's New for the Orbiting Carbon Observatory-2? A Summary of Changes between the Original and Re-flight Missions

    NASA Astrophysics Data System (ADS)

    Boland, S. W.; Kahn, P. B.

    2012-12-01

    The original Orbiting Carbon Observatory mission was lost in 2009 when the spacecraft failed to achieve orbit due to a launch vehicle failure. In 2010, NASA authorized a re-flight mission, known as the Orbiting Carbon Observatory-2 (OCO-2) mission, with direction to re-use the original hardware, designs, drawings, documents, and procedures wherever possible in order to minimize cost, schedule, and performance risk. During implementation, it was realized that some changes were required due to parts obsolescence, incorporation of lessons learned from the original OCO mission, and to provide optimal science return. In response to the OCO and Glory launch vehicle failures, a change in launch vehicle was also recently announced. A summary of changes, including those to hardware, orbit, and launch vehicle is provided, along with rationale, implementation approach, and impact (if any) on mission science.

  14. Carnegie Observatories

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Carnegie Observatories were founded in 1902 by George Ellery Hale. Their first facility was the MOUNT WILSON OBSERVATORY, located in the San Gabriel Mountains above Pasadena, California. Originally a solar observatory, it moved into stellar, galactic and extragalactic research with the construction of the 60 in (1.5 m), and 100 in (2.5 m) telescopes, each of which was the largest in the world...

  15. Origin of atmospheric aerosols at the Pierre Auger Observatory using backward trajectory of air masses

    NASA Astrophysics Data System (ADS)

    Louedec, Karim; Pierre Auger Collaboration

    2013-02-01

    The Pierre Auger Observatory is the largest operating cosmic ray observatory ever built. Calorimetric measurements of extensive air showers induced by cosmic rays are performed with a fluorescence detector. Thus, one of the main challenges is the monitoring of the atmosphere, both in terms of atmospheric state variables and optical properties. To better understand the atmospheric conditions, a study of air mass trajectories above the site is presented. Such a study has been done using an air-modelling program well known in atmospheric sciences. Its validity has been checked using meteorological radiosonde soundings performed at the Pierre Auger Observatory. Finally, aerosol concentration values measured by the Central Laser Facility are compared to backward trajectories.

  16. AGN and Starbursts in Dusty Galaxy Mergers: Insights from the Great Observatories All-sky LIRG Survey

    NASA Astrophysics Data System (ADS)

    Mazzarella, Joseph M.

    2014-07-01

    The Great Observatories All-sky LIRG Survey (GOALS) is combining imaging and spectroscopic data from the Herschel, Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes augmented with extensive ground-based observations in a multiwavelength study of approximately 180 Luminous Infrared Galaxies (LIRGs) and 20 Ultraluminous Infrared Galaxies (ULIRGs) that comprise a statistically complete subset of the 60μm-selected IRAS Revised Bright Galaxy Sample. The objects span the full range of galaxy environments (giant isolated spirals, wide and close pairs, minor and major mergers, merger remnants) and nuclear activity types (Seyfert 1, Seyfert 2, LINER, starburst/HII), with proportions that depend strongly on the total infrared luminosity. I will review the science motivations and present highlights of recent results selected from over 25 peer-reviewed journal articles published recently by the GOALS Team. Statistical investigations include detection of high-ionization Fe K emission indicative of deeply embedded AGN, comparison of UV and far-IR properties, investigations of the fraction of extended emission as a function of wavelength derived from mid-IR spectroscopy, mid-IR spectral diagnostics and spectral energy distributions revealing the relative contributions of AGN and starbursts to powering the bolometric luminosity, and quantitative structure analyses that delineate the evolution of stellar bars and nuclear stellar cusps during the merger process. Multiwavelength dissections of individual systems have unveiled large populations of young star clusters and heavily obscured AGN in early-stage (II Zw 96), intermediate-stage (Mrk 266, Mrk 273), and late-stage (NGC 2623, IC 883) mergers. A recently published study that matches numerical simulations to the observed morphology and gas kinematics in mergers has placed four systems on a timeline spanning 175-260 million years after their first passages, and modeling of additional (U)LIRGs is underway. A very

  17. Contributions of the "Great" X-Ray Observatories (XMM-Newton and Chandra) to Astronomy and Astrophysics

    NASA Technical Reports Server (NTRS)

    Weisskopf, Martin

    2011-01-01

    NASA s Chandra X-ray Observatory and ESA s XMM-Newton made their first observations over a decade ago. The unprecedented and complementary capabilities of these observatories to detect, image, and measure the energy of cosmic X-rays, achieved less than 50 years after the first detection of an extra-solar X-ray source, represent an increase in sensitivity comparable in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. In this presentation we highlight some of the many discoveries made using these powerful X-ray observatories that have transformed 21st century astronomy. We briefly discuss future prospects for this truly exciting field.

  18. Origin of atmospheric aerosols at the Pierre Auger Observatory using studies of air mass trajectories in South America

    NASA Astrophysics Data System (ADS)

    Aab, A.; Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Antičić, T.; Aramo, C.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Badescu, A. M.; Barber, K. B.; Bardenet, R.; Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; BenZvi, S.; Berat, C.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.; Cheng, S. H.; Chiavassa, A.; Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Criss, A.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.; de Jong, S. J.; De La Vega, G.; de Mello Junior, W. J. M.; de Mello Neto, J. R. T.; De Mitri, I.; de Souza, V.; de Vries, K. D.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.; Diep, P. N.; Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dong, P. N.; Dorofeev, A.; dos Anjos, J. C.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Foerster, N.; Fox, B. D.; Fracchiolla, C. E.; Fraenkel, E. D.; Fratu, O.; Fröhlich, U.; Fuchs, B.; Gaior, R.; Gamarra, R. F.; Gambetta, S.; García, B.; Garcia Roca, S. T.; Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.; Gemmeke, H.; Ghia, P. L.; Giammarchi, M.; Giller, M.; Gitto, J.; Glaser, C.; Glass, H.; Gomez Albarracin, F.; Gómez Berisso, M.; Gómez Vitale, P. F.; Gonçalves, P.; Gonzalez, J. G.; Gookin, B.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.; Jansen, S.; Jarne, C.; Josebachuili, M.; Kadija, K.; Kambeitz, O.; Kampert, K. H.; Karhan, P.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Krause, R.; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kunka, N.; La Rosa, G.; LaHurd, D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Lyberis, H.; Maccarone, M. C.; Malacari, M.; Maldera, S.; Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marquez Falcon, H. R.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mićanović, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier Ragaigne, D.; Montanet, F.; Morales, B.; Morello, C.; Moreno, J. C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Münchmeyer, M.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nhung, P. T.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Nožka, L.; Oehlschläger, J.; Olinto, A.; Oliveira, M.; Ortiz, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parra, A.; Pastor, S.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrolini, A.; Petrov, Y.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Pontz, M.; Porcelli, A.; Preda, T.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rivera, H.; Rizi, V.; Roberts, J.; Rodrigues de Carvalho, W.; Rodriguez Cabo, I.; Rodriguez Fernandez, G.; Rodriguez Martino, J.; Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Ros, G.; Rosado, J.; Rossler, T.; Roth, M.; Rouillé-d'Orfeuil, B.; Roulet, E.; Rovero, A. C.; Rühle, C.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Salesa Greus, F.; Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos, E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.; Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, A.; Scholten, O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Sciutto, S. J.; Scuderi, M.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Spinka, H.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.; Straub, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Šuša, T.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Szuba, M.; Tapia, A.; Tartare, M.; Taşcău, O.; Thao, N. T.; Tiffenberg, J.; Timmermans, C.; Tkaczyk, W.; Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek, P.; Tridapalli, D. B.; Trovato, E.; Tueros, M.; Ulrich, R.; Unger, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Aar, G.; van den Berg, A. M.; van Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla, M.; Villaseñor, L.; Wahlberg, H.; Wahrlich, P.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Werner, F.; Westerhoff, S.; Whelan, B. J.; Widom, A.; Wieczorek, G.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Wundheiler, B.; Wykes, S.; Yamamoto, T.; Yapici, T.; Younk, P.; Yuan, G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zaw, I.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.; Ziolkowski, M.; Curci, G.

    2014-11-01

    The Pierre Auger Observatory is making significant contributions towards understanding the nature and origin of ultra-high energy cosmic rays. One of its main challenges is the monitoring of the atmosphere, both in terms of its state variables and its optical properties. The aim of this work is to analyse aerosol optical depth τa(z) values measured from 2004 to 2012 at the observatory, which is located in a remote and relatively unstudied area of Pampa Amarilla, Argentina. The aerosol optical depth is in average quite low - annual mean τa(3.5 km) ∼ 0.04 - and shows a seasonal trend with a winter minimum - τa(3.5 km) ∼ 0.03 -, and a summer maximum - τa(3.5 km) ∼ 0.06 -, and an unexpected increase from August to September - τa(3.5 km) ∼ 0.055. We computed backward trajectories for the years 2005 to 2012 to interpret the air mass origin. Winter nights with low aerosol concentrations show air masses originating from the Pacific Ocean. Average concentrations are affected by continental sources (wind-blown dust and urban pollution), whilst the peak observed in September and October could be linked to biomass burning in the northern part of Argentina or air pollution coming from surrounding urban areas.

  19. Gamma-Ray Flashes of Atmospheric Origin. The Compton Gamma-Ray Observatory Guest Investigator Program: Cycle 7

    NASA Technical Reports Server (NTRS)

    Mallozzi, Robert S.; Fishman, G. J.; Pendleton, G. N.; Inan, U. S.

    2000-01-01

    The BATSE detectors on the Compton Gamma-Ray Observatory have recorded the first observations of an unexplained terrestrial phenomenon: brief, intense flashes of MeV photons. These events, known as terrestrial gamma-ray flashes, must originate at altitudes above 30 km to be observed by the orbiting detectors. More than 70 of these events have been observed in nine years of observations. The most likely origin of these high-energy photons is bremsstrahlung from relativistic electrons from high altitude electrical discharges above thunderstorm regions. We proposed to analyze observations of temporal and spectral properties of these events, and to produce a catalog of event characteristics. Temporal correlations with radio observations made at Palmer Station, Antarctica and spatial correlations with satellite images of thunderstorm regions near GRO during these events were investigated, aiding in verification and testing of proposed theoretical models of the atmospheric processes believed to be responsible for these unique observations.

  20. On the origin and age of the Great Sand Dunes, Colorado

    NASA Astrophysics Data System (ADS)

    Madole, Richard F.; Romig, Joe H.; Aleinikoff, John N.; VanSistine, D. Paco; Yacob, Ezra Y.

    2008-07-01

    Over the past 100 yr, several hypotheses have been proposed for the origin and age of the Great Sand Dunes. These hypotheses differ widely in the descriptions of dune morphometry, the immediate source of eolian sand, and when sand transport occurred. The primary purpose of this paper is to evaluate these hypotheses and, where warranted, to present new ideas about the origin and age of the Great Sand Dunes. To evaluate the previous hypotheses, we had to develop more detailed information about the surficial geology of the northern San Luis Valley. Thus, we mapped the surficial geology of an area extending several tens of kilometers north, south, and west of the Great Sand Dunes and examined subsurface stratigraphy in more than 200 wells and borings. In addition, we used relative-dating criteria and several radiocarbon and OSL ages to establish the chronology of surficial deposits, and we determined the U-Pb ages of detrital zircons to obtain information about the sources of the sand in the Great Sand Dunes. The first principal finding of this study is that the lower part of the closed basin north of the Rio Grande, referred to here as the sump, is the immediate source of the sand in the Great Sand Dunes, rather than the late Pleistocene flood plain of the Rio Grande (the most widely accepted hypothesis). A second principal finding is that the Great Sand Dunes are older than late Pleistocene. They postdate the draining of Lake Alamosa, which began ˜ 440 ka, and predate the time when streams draining the west flank of the Sangre de Cristo Mountains were deflected by incipient dunes that formed near the mountain front. Geomorphic and stratigraphic evidence indicate that this deflection occurred prior to the end of the next to last glaciation (Bull Lake), i.e., prior to ˜ 130 ka.

  1. On the origin and age of the Great Sand Dunes, Colorado

    USGS Publications Warehouse

    Madole, R.F.; Romig, J.H.; Aleinikoff, J.N.; VanSistine, D.P.; Yacob, E.Y.

    2008-01-01

    Over the past 100??yr, several hypotheses have been proposed for the origin and age of the Great Sand Dunes. These hypotheses differ widely in the descriptions of dune morphometry, the immediate source of eolian sand, and when sand transport occurred. The primary purpose of this paper is to evaluate these hypotheses and, where warranted, to present new ideas about the origin and age of the Great Sand Dunes. To evaluate the previous hypotheses, we had to develop more detailed information about the surficial geology of the northern San Luis Valley. Thus, we mapped the surficial geology of an area extending several tens of kilometers north, south, and west of the Great Sand Dunes and examined subsurface stratigraphy in more than 200 wells and borings. In addition, we used relative-dating criteria and several radiocarbon and OSL ages to establish the chronology of surficial deposits, and we determined the U-Pb ages of detrital zircons to obtain information about the sources of the sand in the Great Sand Dunes. The first principal finding of this study is that the lower part of the closed basin north of the Rio Grande, referred to here as the sump, is the immediate source of the sand in the Great Sand Dunes, rather than the late Pleistocene flood plain of the Rio Grande (the most widely accepted hypothesis). A second principal finding is that the Great Sand Dunes are older than late Pleistocene. They postdate the draining of Lake Alamosa, which began ??? 440??ka, and predate the time when streams draining the west flank of the Sangre de Cristo Mountains were deflected by incipient dunes that formed near the mountain front. Geomorphic and stratigraphic evidence indicate that this deflection occurred prior to the end of the next to last glaciation (Bull Lake), i.e., prior to ??? 130??ka.

  2. The upGREAT 1.9 THz multi-pixel high resolution spectrometer for the SOFIA Observatory

    NASA Astrophysics Data System (ADS)

    Risacher, C.; Güsten, R.; Stutzki, J.; Hübers, H.-W.; Bell, A.; Buchbender, C.; Büchel, D.; Csengeri, T.; Graf, U. U.; Heyminck, S.; Higgins, R. D.; Honingh, C. E.; Jacobs, K.; Klein, B.; Okada, Y.; Parikka, A.; Pütz, P.; Reyes, N.; Ricken, O.; Riquelme, D.; Simon, R.; Wiesemeyer, H.

    2016-10-01

    We present a new multi-pixel high resolution (R ≳ 107) spectrometer for the Stratospheric Observatory for Far-Infrared Astronomy (SOFIA). The receiver uses 2 × 7-pixel subarrays in orthogonal polarization, each in an hexagonal array around a central pixel. We present the first results for this new instrument after commissioning campaigns in May and December 2015 and after science observations performed in May 2016. The receiver is designed to ultimately cover the full 1.8-2.5 THz frequency range but in its first implementation, the observing range was limited to observations of the [CII] line at 1.9 THz in 2015 and extended to 1.83-2.07 THz in 2016. The instrument sensitivities are state-of-the-art and the first scientific observations performed shortly after the commissioning confirm that the time efficiency for large scale imaging is improved by more than an order of magnitude as compared to single pixel receivers. An example of large scale mapping around the Horsehead Nebula is presented here illustrating this improvement. The array has been added to SOFIA's instrument suite already for ongoing observing cycle 4. The datacube of the Horsehead observations is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/595/A34

  3. Disseminated lymphoma of presumptive T-cell origin in a great horned owl (Bubo virginianus).

    PubMed

    Malka, Shachar; Crabbs, Torrie; Mitchell, Elizabeth B; Zehnder, Ashley; Kent, Michael S; Lowenstine, Linda J; Hawkins, Michelle G

    2008-09-01

    A geriatric male great horned owl (Bubo virginianus) that was a resident at a raptor center was presented for examination because of stridor and weight loss. Results of physical examination, diagnostic imaging, and biopsy were consistent with disseminated lymphoma involving the oropharynx, neck region (including thyroid and parathyroid glands), keel, spleen, and liver. Attempts to treat the owl with chlorambucil failed, and the owl was euthanatized 5 months later. Neoplastic cells from this owl were immunoreactive to CD-3 antibody, suggesting the lymphoma was of T-cell origin.

  4. Origin, Specification, and Plasticity of the Great Vessels of the Heart

    PubMed Central

    Nagelberg, Danielle; Wang, Jinhu; Su, Rina; Torres-Vázquez, Jesús; Targoff, Kimara L.; Poss, Kenneth D.; Knaut, Holger

    2015-01-01

    SUMMARY The pharyngeal arch arteries (PAAs) are a series of paired embryonic blood vessels that give rise to several major arteries that connect directly to the heart. During development, the PAAs emerge from nkx2.5-expressing mesodermal cells and connect the dorsal head vasculature to the outflow tract of the heart. Despite their central role in establishing the circulatory system, the embryonic origins of the PAA progenitors are only coarsely defined, and the factors that specify them and their regenerative potential are unclear. Using fate mapping and mutant analysis, we find that PAA progenitors are derived from the tcf21 and nkx2.5 double-positive head mesoderm and require these two transcription factors for their specification and survival. Unexpectedly, cell ablation shows that the tcf21+; nkx2.5+ PAA progenitors are not required for PAA formation. We find that this compensation is due to the replacement of ablated tcf21+; nkx2.5+ PAA cells by endothelial cells from the dorsal head vasculature. Together, these studies assign the embryonic origin of the great vessel progenitors to the interface between the pharyngeal and cardiac mesoderm, identify the transcription factor code required for their specification, and reveal an unexpected plasticity in the formation of the great vessels. PMID:26255850

  5. The Origin of Basin of Great Lakes in Western Mongolia: Glaciated Super Valley, Not Super Flooding

    NASA Astrophysics Data System (ADS)

    Khukhuudei, Ulambadrakh; Otgonbayar, Orolzodmaa

    2015-04-01

    Research for morphology, its origin of the Basin of Great Lakes in Western Mongolia, is few and far between, particularly, any in recent years. The origin of the morphology of the basin presents a new study, combining previous study materials, their results and interpreting the digital photos. Also the main bases of theory is Pleistocene Last Glacial Maximum distribution. Many scholars have proven that global glaciation covered many areas of the Northern Hemisphere during the Pleistocene era. This global glaciation occurred in the northwest part of Mongolia to Mongolian Altay, Khangay and Khuvsgul mountain range. At the same time, the present appearance of basin that developed inheriting since the Mesozoic era, forms by global glaciation. The morphology of Basin of Great Lakes is super trough or glaciated super valley. At current day, "knock and lochan" topography (scoured region) and rock drumlins lie in the central part of the basin. Huge meltwater from this glaciation formed Shargasub-basin as a super kettle hole by erosion and overflowed water from it formed pluvial basins or big lakes in the Lake Valley.

  6. Climatic influences on wood anatomy and tree-ring features of Great Basin conifers at a new mountain observatory1

    PubMed Central

    Ziaco, Emanuele; Biondi, Franco; Rossi, Sergio; Deslauriers, Annie

    2014-01-01

    • Premise of the study: A network of mountain observing stations has been installed in the Great Basin of North America. NevCAN (Nevada Climate-ecohydrological Assessment Network), which spans a latitudinal range of 2.5° and two elevation ranges of about 2000 m each, enabled us to investigate tree growth in relation to climate. • Methods: We analyzed wood anatomy and tree-ring characteristics of four conifer species in response to different levels of water availability by comparing a low- and a high-elevation population. Chronologies of earlywood and latewood widths, as well as cellular parameters, were developed from the year 2000 to 2012. • Results: At the southern (drier and warmer) sites, Pinus monophylla had smaller cell lumen, tracheid diameter, and cell wall thickness. Pinus monophylla and P. flexilis showed bigger cellular elements at the higher elevations, whereas the opposite pattern was found in Picea engelmannii and Pinus longaeva. When all species and sites were pooled together, stem diameter was positively related with earlywood anatomical parameters. • Discussion: We have provided a glimpse of the applications that NevCAN, as a new scientific tool, could allow in the general field of botany. In particular, we were able to investigate how differences in water stress related to elevation lead to changes in xylem anatomy. PMID:25309838

  7. Lunar Surface Origins Exploration (LunaSOX) -Virtual observatory facility for solar wind plasma interactions with the Moon

    NASA Astrophysics Data System (ADS)

    Cooper, John

    A new virtual observatory facility is being will be implemented in support of solar wind and terrestrial magnetospheric plasma interactions with the lunar surface and atmospheric envi-ronments. The NASA Heliophysics virtual observatory approach of open on-line metadata registration, discovery, access, and supporting value-added tools will be applied to selected data products from lunar surface, lunar orbital, and earth-orbiting solar wind monitors. The LunaSOX facilty at lunasox,gsfc.nasa.gov will be operated by a science focus group for NASA's Virtual Heliospheric Observatory. Initial primary focus will be on the Apollo ALSEP solar wind monitor data products already accessible on-line in through the Coordinated Data Anal-ysis Web (CDAWeb) service of the NASA Space Physics Data Facility (SPDF). These data will be recast in forms appropriate for support of the plasma interaction modeling and the new value-added data products will be posted through the virtual observatory. Supporting lunar and Earth orbit data of the Apollo era in the NASA archives will be similarly treated and posted on-line. The LunaSOX virtual observatory will also provide links to other available lunar data. Selected data analysis (e.g., OMNIWeb), orbital ephemeris (SSCWeb), and associated visualization tools of SPDF will be utilized in support of the modeling and virtual observatory efforts. Please contact the author for potential virtual observatory support of specific data products related to plasma interactions with the lunar surface and atmosphere.

  8. A unique Middle Miocene European hominoid and the origins of the great ape and human clade

    PubMed Central

    Moyà-Solà, Salvador; Alba, David M.; Almécija, Sergio; Casanovas-Vilar, Isaac; Köhler, Meike; De Esteban-Trivigno, Soledad; Robles, Josep M.; Galindo, Jordi; Fortuny, Josep

    2009-01-01

    The great ape and human clade (Primates: Hominidae) currently includes orangutans, gorillas, chimpanzees, bonobos, and humans. When, where, and from which taxon hominids evolved are among the most exciting questions yet to be resolved. Within the Afropithecidae, the Kenyapithecinae (Kenyapithecini + Equatorini) have been proposed as the sister taxon of hominids, but thus far the fragmentary and scarce Middle Miocene fossil record has hampered testing this hypothesis. Here we describe a male partial face with mandible of a previously undescribed fossil hominid, Anoiapithecus brevirostris gen. et sp. nov., from the Middle Miocene (11.9 Ma) of Spain, which enables testing this hypothesis. Morphological and geometric morphometrics analyses of this material show a unique facial pattern for hominoids. This taxon combines autapomorphic features—such as a strongly reduced facial prognathism—with kenyapithecine (more specifically, kenyapithecin) and hominid synapomorphies. This combination supports a sister-group relationship between kenyapithecins (Griphopithecus + Kenyapithecus) and hominids. The presence of both groups in Eurasia during the Middle Miocene and the retention in kenyapithecins of a primitive hominoid postcranial body plan support a Eurasian origin of the Hominidae. Alternatively, the two extant hominid clades (Homininae and Ponginae) might have independently evolved in Africa and Eurasia from an ancestral, Middle Miocene stock, so that the supposed crown-hominid synapomorphies might be homoplastic. PMID:19487676

  9. A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO). I. Science goals, sample selection, and analysis tools

    NASA Astrophysics Data System (ADS)

    Sánchez-Janssen, R.; Amorín, R.; García-Vargas, M.; Gomes, J. M.; Huertas-Company, M.; Jiménez-Esteban, F.; Mollá, M.; Papaderos, P.; Pérez-Montero, E.; Rodrigo, C.; Sánchez Almeida, J.; Solano, E.

    2013-06-01

    Context. Even though they are by far the most abundant of all galaxy types, the detailed properties of dwarf galaxies are still only poorly characterised - especially because of the observational challenge that their intrinsic faintness and weak clustering properties represent. Aims: AVOCADO aims at establishing firm conclusions on the formation and evolution of dwarf galaxies by constructing and analysing a homogeneous, multiwavelength dataset for a statistically significant sample of approximately 6500 nearby dwarfs (Mi - 5 log h100 > - 18 mag). The sample is selected to lie within the 20 < D < 60 h100-1 Mpc volume covered by the SDSS-DR7 footprint, and is thus volume-limited for Mi - 5 log h100 < -16 mag dwarfs - but includes ≈1500 fainter systems. We will investigate the roles of mass and environment in determining the current properties of the different dwarf morphological types - including their structure, their star formation activity, their chemical enrichment history, and a breakdown of their stellar, dust, and gas content. Methods: We present the sample selection criteria and describe the suite of analysis tools, some of them developed in the framework of the Virtual Observatory. We use optical spectra and UV-to-NIR imaging of the dwarf sample to derive star formation rates, stellar masses, ages, and metallicities - which are supplemented with structural parameters that are used to classify them morphologically. This unique dataset, coupled with a detailed characterisation of each dwarf's environment, allows for a fully comprehensive investigation of their origins and enables us to track the (potential) evolutionary paths between the different dwarf types. Results: We characterise the local environment of all dwarfs in our sample, paying special attention to trends with current star formation activity. We find that virtually all quiescent dwarfs are located in the vicinity (projected distances ≲ 1.5 h100-1 Mpc) of ≳ L∗ companions, consistent with

  10. Great ape origins of personality maturation and sex differences: a study of orangutans and chimpanzees.

    PubMed

    Weiss, Alexander; King, James E

    2015-04-01

    Human personality development evinces increased emotional stability, prosocial tendencies, and responsibility. One hypothesis offered to explain this pattern is Social-Investment Theory, which posits that culturally defined social roles, including marriage and employment, are responsible for the increased maturity. Alternatively, Five-Factor Theory emphasizes the role of biological factors, such as those governing physical development, which may predate the emergence of humans. Five-Factor Theory, unlike Social-Investment Theory, predicts that all or some of the human personality developmental trends should be present in great apes, our closest evolutionary relatives. To test this prediction and to better understand the evolutionary origins of sex differences, we examined age and sex differences in the chimpanzee and orangutan personality domains Extraversion, Dominance, Neuroticism, and Agreeableness. We also examined the Activity and Gregariousness facets of Extraversion and the orangutan Intellect domain. Extraversion and Neuroticism declined across age groups in both species, in common with humans. A significant interaction indicated that Agreeableness declined in orangutans but increased in chimpanzees, as it does in humans, though this may reflect differences in how Agreeableness was defined in each species. Significant interactions indicated that male chimpanzees, unlike male orangutans, displayed higher Neuroticism scores than females and maintained higher levels of Activity and Dominance into old age than female chimpanzees, male orangutans, and female orangutans. Personality-age correlations were comparable across orangutans and chimpanzees and were similar to those reported in human studies. Sex differences were stronger in chimpanzees than in humans or orangutans. These findings support Five-Factor Theory, suggest the role of gene-culture coevolution in shaping personality development, and suggest that sex differences evolved independently in different

  11. Coral reef origins of atmospheric dimethylsulfide at Heron Island, southern Great Barrier Reef, Australia

    NASA Astrophysics Data System (ADS)

    Swan, Hilton B.; Jones, Graham B.; Deschaseaux, Elisabeth S. M.; Eyre, Bradley D.

    2017-01-01

    Atmospheric dimethylsulfide (DMSa), continually derived from the world's oceans, is a feed gas for the tropospheric production of new sulfate particles, leading to cloud condensation nuclei that influence the formation and properties of marine clouds and ultimately the Earth's radiation budget. Previous studies on the Great Barrier Reef (GBR), Australia, have indicated coral reefs are significant sessile sources of DMSa capable of enhancing the tropospheric DMSa burden mainly derived from phytoplankton in the surface ocean; however, specific environmental evidence of coral reef DMS emissions and their characteristics is lacking. By using on-site automated continuous analysis of DMSa and meteorological parameters at Heron Island in the southern GBR, we show that the coral reef was the source of occasional spikes of DMSa identified above the oceanic DMSa background signal. In most instances, these DMSa spikes were detected at low tide under low wind speeds, indicating they originated from the lagoonal platform reef surrounding the island, although evidence of longer-range transport of DMSa from a 70 km stretch of coral reefs in the southern GBR was also observed. The most intense DMSa spike occurred in the winter dry season at low tide when convective precipitation fell onto the aerially exposed platform reef. This co-occurrence of events appeared to biologically shock the coral resulting in a seasonally aberrant extreme DMSa spike concentration of 45.9 nmol m-3 (1122 ppt). Seasonal DMS emission fluxes for the 2012 wet season and 2013 dry season campaigns at Heron Island were 5.0 and 1.4 µmol m-2 day-1, respectively, of which the coral reef was estimated to contribute 4 % during the wet season and 14 % during the dry season to the dominant oceanic flux.

  12. Variation of optical properties at Lucinda Jetty Coastal Observatory and its input into an optical model of coastal waters in Great Barrier Reef region.

    NASA Astrophysics Data System (ADS)

    Wozniak, Monika; Baird, Mark; Schroeder, Thomas; Clementson, Lesley; Jones, Emlyn

    2017-04-01

    The water column optical properties from an observation station located at the end of a 5.8 km long jetty in the coastal waters of the Great Barrier Reef World Heritage Area (18.52 S, 146.39 E) were studied. Due to the location of the Lucinda Jetty Coastal Observatory (LJCO), at the interface of large riverine nutrient and sediment sources and clear open ocean waters, it is an optically variable and interesting region. LJCO is the only Southern Hemisphere ocean colour validation site integrated into NASA's AERONET-OC global network of ground-based radiometers. LJCO has a 3 years long time series (2014-2016) of continuous in-water optical measurements of absorption (AC-S), scattering (AC-S) and backscattering (BB-9) spectra together with water-leaving radiance spectra (SeaPRISM) acquired above the water surface and concentration of water components (WQM). Further HPLC and spectrophotometrically-retrieved absorption and scattering were determined fortnightly. These detailed bio-optical observations are rarely available as a time-series for model assessment. We use these data to quantify the relationship between optical properties and water constituents and to developing a more accurate optical model for coastal, optically complex water like GBR model. Pigment analysis show that studied area is dominated by alternatively freshwater and oceanic phytoplankton species depending on weather condition, tides and season. Absorption spectra at 440 nm and 550 nm are dominated by detritus but also have a significant CDOM contribution, which influences reflectance values in that range of spectrum and negatively affects wavebands used in satellite and remote algorithms for water constituents. These emergent features are compared to the model outputs, demonstrating when the model produces accurate optical signals with realistic process representation.

  13. Great Minds? Great Lakes!

    ERIC Educational Resources Information Center

    Environmental Protection Agency, Chicago, IL. Great Lakes National Program Office.

    This book contains lesson plans that provide an integrated approach to incorporating Great Lakes environmental issues into elementary subjects. The book is divided into three subject areas: (1) History, which includes the origins of the Great Lakes, Great Lakes people, and shipwrecks; (2) Social Studies, which covers government, acid rain as a…

  14. Mitochondrial genes support a common origin of rodent malaria parasites and Plasmodium falciparum's relatives infecting great apes.

    PubMed

    Blanquart, Samuel; Gascuel, Olivier

    2011-03-15

    Plasmodium falciparum is responsible for the most acute form of human malaria. Most recent studies demonstrate that it belongs to a monophyletic lineage specialized in the infection of great ape hosts. Several other Plasmodium species cause human malaria. They all belong to another distinct lineage of parasites which infect a wider range of primate species. All known mammalian malaria parasites appear to be monophyletic. Their clade includes the two previous distinct lineages of parasites of primates and great apes, one lineage of rodent parasites, and presumably Hepatocystis species. Plasmodium falciparum and great ape parasites are commonly thought to be the sister-group of all other mammal-infecting malaria parasites. However, some studies supported contradictory origins and found parasites of great apes to be closer to those of rodents, or to those of other primates. To distinguish between these mutually exclusive hypotheses on the origin of Plasmodium falciparum and its great ape infecting relatives, we performed a comprehensive phylogenetic analysis based on a data set of three mitochondrial genes from 33 to 84 malaria parasites. We showed that malarial mitochondrial genes have evolved slowly and are compositionally homogeneous. We estimated their phylogenetic relationships using Bayesian and maximum-likelihood methods. Inferred trees were checked for their robustness to the (i) site selection, (ii) assumptions of various probabilistic models, and (iii) taxon sampling. Our results robustly support a common ancestry of rodent parasites and Plasmodium falciparum's relatives infecting great apes. Our results refute the most common view of the origin of great ape malaria parasites, and instead demonstrate the robustness of a less well-established phylogenetic hypothesis, under which Plasmodium falciparum and its relatives infecting great apes are closely related to rodent parasites. This study sheds light on the evolutionary history of Plasmodium falciparum, a

  15. On The Origins Of Cosmic Dust And The Evolution Of Nearby Galaxies With The Herschel Space Observatory

    NASA Astrophysics Data System (ADS)

    Clark, Christopher Jonathan Redfern

    2015-04-01

    Using multiwavelength observations, centred around the unique far-infrared and submillimetre window provided by the Herschel Space Observatory, this thesis investigates the origins and evolution of cosmic dust in the local Universe – by examining individual sources of dust in our own galaxy, and by studying dust in nearby galaxies. I search Herschel observations of the remnants of Kepler’s (SN1604) and Tycho’s (SN1572) supernovæ, both Type-Ia explosions, for evidence of dust creation by these events. Being the only Type-Ia supernovæ known to have occurred in our Galaxy within the past 1,000 years, these remnants are the only ones both close enough to resolve, and young enough that they are dominated by their ejecta dynamics. There is no indication of any recently manufactured dust associated with either supernova remnant. It therefore appears that Type-Ia supernovæ do not contribute significantly to the dust budgets of galaxies. The Crab Nebula, the result of a Type-II supernova (SN1054), is also investigated using Herschel and multiwavelength data. After accounting for other sources of emission, a temperature of Td = 63.1 K and mass of Md = 0.21 M⊙ is derived for the Crab Nebula’s dust component. I create a map of the distribution of dust in the Crab Nebula, the first of its kind, by means of a resolved component separation, revealing that the dust is located in the dense filamentary ejecta. We can be confident that this dust will survive in the long term, and be injected into the galactic dust budget. This is the first detection of manufactured supernova dust for which this can be said. Next I use the Herschel-ATLAS to assemble HAPLESS: the Herschel- ATLAS Phase-1 Limited Extent Spatial Sample – a blind, volume-limited, dust- selected sample of nearby galaxies. The majority of this sample is made up of curious very blue galaxies. Often irregular and/or flocculent in morphology, with extremely blue UV-NIR colours, these galaxies appear to be

  16. After a dozen years of progress the origin of angiosperms is still a great mystery.

    PubMed

    Frohlich, Michael W; Chase, Mark W

    2007-12-20

    Here we discuss recent advances surrounding the origin of angiosperms. Putatively primitive characters are now much better understood because of a vastly improved understanding of angiosperm phylogenetics, and recent discoveries of fossil flowers have provided an increasingly detailed picture of early diversity in the angiosperms. The 'anthophyte theory', the dominant concept of the 1980s and 1990s, has been eclipsed; Gnetales, previously thought to be closest to the angiosperms, are related instead to other extant gymnosperms, probably most closely to conifers. Finally, new theories of flower origins have been proposed based on gene function, duplication and loss, as well as on morphology. Further studies of genetic mechanisms that control reproductive development in seed plants provide a most promising avenue for further research, including tests of these recent theories. Identification of fossils with morphologies that convincingly place them close to angiosperms could still revolutionize understanding of angiosperm origins.

  17. New data on mitochondrial diversity and origin of Hemimysis anomala in the Laurentian Great Lakes

    USGS Publications Warehouse

    Questel, Jennifer M.; Walsh, Maureen G.; Smith, Randall J.; Welsh, Amy B.

    2012-01-01

    The most recent Ponto-Caspian species to invade the Laurentian Great Lakes is the crustacean Hemimysis anomala, first reported in 2006. A previous study described three haplotype groups (A, B, C) of H. anomala in native and invaded areas within Europe, but only one haplotype (A1) in a sample from Lake Michigan. Our study expands these results to additional populations in the Great Lakes basin, and evaluates relationships among North American and European populations. A 549-bp fragment of themitochondrial cytochrome oxidase I (COI) gene was analyzed from populations of H. anomala in Lakes Ontario, Erie, Huron, and the St. Lawrence River.Two different haplotypes, A1 and B1,were observed in the sampled populations of H. anomala and in a previous analysis from H. anomala in Oneida Lake (New York). Our results, in contrast with a previous study, detect an additional haplotype in North America.

  18. Origin of conglomerate stratigraphy in the Franciscan assemblage and Great Valley sequence, northern California

    USGS Publications Warehouse

    Seiders, V.M.

    1988-01-01

    In the northern California Coast Ranges, the forearc-basin Great Valley sequence of Late Jurassic and Cretaceous age contains three distinctive types of conglomerate; 1) chert-rich conglomerate of Tithonian to Valanginian age, 2) volcanic-rich conglomerate of mainly Valanginian age, and 3) mixed-clast conglomerate of Valenginian and younger age. All three types are found in stratigraphic sequence along the west side of the Sacramento Valley, but in three belts of outliers that overlie the Franciscan assemblage to the west, the oldest conglomerate present in each belt is progressively younger southwestward. The same three conglomerate types occur in coeval rocks of the accretionary-wedge Franciscan assemblage and show a similar southwestward progression in composition, possibly due to trench deposition of conglomerate with the same sources as the Great Valley sequence, each conglomerate type being accreted successively to the west side of the accretionary wedge. -from Author

  19. Characterization and origin of polar dissolved organic matter from the Great Salt Lake

    USGS Publications Warehouse

    Leenheer, J.A.; Noyes, T.I.; Rostad, C.E.; Davisson, M.L.

    2004-01-01

    Polar dissolved organic matter (DOM) was isolated from a surface-water sample from the Great Salt Lake by separating it from colloidal organic matter by membrane dialysis, from less-polar DOM fractions by resin sorbents, and from inorganic salts by a combination of sodium cation exchange followed by precipitation of sodium salts by acetic acid during evaporative concentration. Polar DOM was the most abundant DOM fraction, accounting for 56% of the isolated DOM. Colloidal organic matter was 14C-age dated to be about 100% modern carbon and all of the DOM fractions were 14C-age dated to be between 94 and 95% modern carbon. Average structural models of each DOM fraction were derived that incorporated quantitative elemental and infrared, 13C-NMR, and electrospray/mass spectrometric data. The polar DOM model consisted of open-chain N-acetyl hydroxy carboxylic acids likely derived from N-acetyl heteropolysaccharides that constituted the colloidal organic matter. The less polar DOM fraction models consisted of aliphatic alicyclic ring structures substituted with carboxyl, hydroxyl, ether, ester, and methyl groups. These ring structures had characteristics similar to terpenoid precursors. All DOM fractions in the Great Salt Lake are derived from algae and bacteria that dominate DOM inputs in this lake.

  20. Recently recovered Kenyapithecus mandible and its implications for great ape and human origins.

    PubMed Central

    McCrossin, M L; Benefit, B R

    1993-01-01

    We report here a Kenyapithecus africanus juvenile mandible recovered from middle Miocene (ca. 14-16 million years) deposits of Maboko Island (Lake Victoria), Kenya. Symphyseal and dental attributes of the mandible distinguish K. africanus, a species widely regarded as the earliest known member of the great ape and human clade, from other Miocene large-bodied hominoids. The Maboko Island mandible exhibits a markedly proclined symphyseal axis, massive inferior transverse torus, mesiodistally narrow, high-crowned, and strongly procumbent lateral incisor, and molars with cingula restricted to the median buccal cleft. Although the presence of some of these conditions in Kenyapithecus was suggested earlier, the fragmentary and ill-preserved nature of previously known specimens led certain authorities to doubt their validity. Our assessment of mandibular and dental morphology indicates that K. africanus diverged after Proconsul and Griphopithecus but prior to the last common ancestor of Sivapithecus, extant great apes, and humans. The robustly constructed mandibular symphysis and anterior dentition suggest that incisal biting played as important a role as thick molar enamel in the dietary adaptations of K. africanus. Images Fig. 1 Fig. 2 PMID:8446615

  1. Constraints on the Origin of Cosmic Rays above 1018 eV from Large-scale Anisotropy Searches in Data of the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Pierre Auger Collaboration; Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Antiči'c, T.; Aramo, C.; Arganda, E.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Badescu, A. M.; Balzer, M.; Barber, K. B.; Barbosa, A. F.; Bardenet, R.; Barroso, S. L. C.; Baughman, B.; Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellétoile, A.; Bellido, J. A.; BenZvi, S.; Berat, C.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I.; Brogueira, P.; Brown, W. C.; Bruijn, R.; Buchholz, P.; Bueno, A.; Buroker, L.; Burton, R. E.; Caballero-Mora, K. S.; Caccianiga, B.; Caramete, L.; Caruso, R.; Castellina, A.; Catalano, O.; Cataldi, G.; Cazon, L.; Cester, R.; Chauvin, J.; Cheng, S. H.; Chiavassa, A.; Chinellato, J. A.; Chirinos Diaz, J.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cook, H.; Cooper, M. J.; Coppens, J.; Cordier, A.; Coutu, S.; Covault, C. E.; Creusot, A.; Criss, A.; Cronin, J.; Curutiu, A.; Dagoret-Campagne, S.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.; De Donato, C.; de Jong, S. J.; De La Vega, G.; de Mello Junior, W. J. M.; de Mello Neto, J. R. T.; De Mitri, I.; de Souza, V.; de Vries, K. D.; del Peral, L.; del Río, M.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Díaz Castro, M. L.; Diep, P. N.; Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dong, P. N.; Dorofeev, A.; dos Anjos, J. C.; Dova, M. T.; D'Urso, D.; Dutan, I.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Fliescher, S.; Fracchiolla, C. E.; Fraenkel, E. D.; Fratu, O.; Fröhlich, U.; Fuchs, B.; Gaior, R.; Gamarra, R. F.; Gambetta, S.; García, B.; Garcia Roca, S. T.; Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.; Gemmeke, H.; Ghia, P. L.; Giller, M.; Gitto, J.; Glass, H.; Gold, M. S.; Golup, G.; Gomez Albarracin, F.; Gómez Berisso, M.; Gómez Vitale, P. F.; Gonçalves, P.; Gonzalez, J. G.; Gookin, B.; Gorgi, A.; Gouffon, P.; Grashorn, E.; Grebe, S.; Griffith, N.; Grillo, A. F.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holmes, V. C.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Ionita, F.; Italiano, A.; Jansen, S.; Jarne, C.; Jiraskova, S.; Josebachuili, M.; Kadija, K.; Kampert, K. H.; Karhan, P.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kelley, J. L.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Koang, D.-H.; Kotera, K.; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kulbartz, J. K.; Kunka, N.; La Rosa, G.; Lachaud, C.; LaHurd, D.; Latronico, L.; Lauer, R.; Lautridou, P.; Le Coz, S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Lyberis, H.; Maccarone, M. C.; Macolino, C.; Maldera, S.; Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, J.; Marin, V.; Maris, I. C.; Marquez Falcon, H. R.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mazur, P. O.; Medina-Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Mertsch, P.; Messina, S.; Meurer, C.; Meyhandan, R.; Mi'canovi'c, S.; Micheletti, M. I.; Minaya, I. A.; Miramonti, L.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier Ragaigne, D.; Montanet, F.; Morales, B.; Morello, C.; Moreno, E.; Moreno, J. C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Münchmeyer, M.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nhung, P. T.; Niechciol, M.; Niemietz, L.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Nožka, L.; Oehlschläger, J.; Olinto, A.; Ortiz, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parizot, E.; Parra, A.; Pastor, S.; Paul, T.; Pech, M.; Peķala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrolini, A.; Petrov, Y.; Pfendner, C.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Ponce, V. H.; Pontz, M.; Porcelli, A.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rivera, H.; Rizi, V.; Roberts, J.; Rodrigues de Carvalho, W.; Rodriguez, G.; Rodriguez Cabo, I.; Rodriguez Martino, J.; Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Ros, G.; Rosado, J.; Rossler, T.; Roth, M.; Rouillé-d'Orfeuil, B.; Roulet, E.; Rovero, A. C.; Rühle, C.; Saftoiu, A.; Salamida, F.; Salazar, H.; Salesa Greus, F.; Salina, G.; Sánchez, F.; Santo, C. E.; Santos, E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarkar, S.; Sato, R.; Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, A.; Scholten, O.; Schoorlemmer, H.; Schovancova, J.; Schovánek, P.; Schröder, F.; Schuster, D.; Sciutto, S. J.; Scuderi, M.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Silva Lopez, H. H.; Sima, O.; 'Smiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Spinka, H.; Squartini, R.; Srivastava, Y. N.; Stanic, S.; Stapleton, J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Šuša, T.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Szuba, M.; Tapia, A.; Tartare, M.; Taşcău, O.; Tcaciuc, R.; Thao, N. T.; Thomas, D.; Tiffenberg, J.; Timmermans, C.; Tkaczyk, W.; Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.; Travnicek, P.; Tridapalli, D. B.; Tristram, G.; Trovato, E.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Aar, G.; van den Berg, A. M.; van Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla, M.; Villaseñor, L.; Wahlberg, H.; Wahrlich, P.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Werner, F.; Westerhoff, S.; Whelan, B. J.; Widom, A.; Wieczorek, G.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Wommer, M.; Wundheiler, B.; Yamamoto, T.; Yapici, T.; Younk, P.; Yuan, G.; Yushkov, A.; Zamorano Garcia, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zaw, I.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.; Ziolkowski, M.

    2013-01-01

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 1018 eV at the Pierre Auger Observatory is reported. For the first time, these large-scale anisotropy searches are performed as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole moments. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Upper limits on dipole and quadrupole amplitudes are derived under the hypothesis that any cosmic ray anisotropy is dominated by such moments in this energy range. These upper limits provide constraints on the production of cosmic rays above 1018 eV, since they allow us to challenge an origin from stationary galactic sources densely distributed in the galactic disk and emitting predominantly light particles in all directions.

  2. CONSTRAINTS ON THE ORIGIN OF COSMIC RAYS ABOVE 10{sup 18} eV FROM LARGE-SCALE ANISOTROPY SEARCHES IN DATA OF THE PIERRE AUGER OBSERVATORY

    SciTech Connect

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2013-01-01

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is reported. For the first time, these large-scale anisotropy searches are performed as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole moments. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Upper limits on dipole and quadrupole amplitudes are derived under the hypothesis that any cosmic ray anisotropy is dominated by such moments in this energy range. These upper limits provide constraints on the production of cosmic rays above 10{sup 18} eV, since they allow us to challenge an origin from stationary galactic sources densely distributed in the galactic disk and emitting predominantly light particles in all directions.

  3. Performance as Promised: How the Chandra X-ray Observatory Accomplished One of Nasa's Most Challenging Missions for Billions of Dollars Less than Originally Planned

    NASA Technical Reports Server (NTRS)

    Davidson, Greg; Hefner, Keith

    2004-01-01

    As the nation looks toward bold new ventures in space, the Chandra X-ray Observatory program offers an example of how billion-dollar missions can be successfully developed within tightening fiscal constraints. Chandra experienced many of challenges facing bold space programs (state-of-the-art technical requirements and budget-induced slips and restructurings), and yet the Chandra team achieved nearly all the originally envisioned performance for dramatically lower cost. This was accomplished by a combination of team- work, systems engineering, advanced technology insertion, and effective approaches for program implementation. A thorough tradeoff of science utility vs. cost led to the selection of a highly elliptical orbit with uncrewed robotic delivery, deployment, and maintenance. Progressive, focused technology demonstrations were accomplished prior to commitment of major resources to critical elements of the system design, such as the high resolution mirror assembly (HRMA). Pathfinder hardware was developed to reduce risks. A variety of schedule risk reduction measures were implemented and resulted in the X-ray calibration taking place exactly within five days of its originally planned date after after five years of development. The team worked together in an effective manner to contain requirements creep. reductions such as the ACIS-2 chip device. It is estimated that the above combination of measures achieved the avoidance of over $4B in costs, while enabling a highly successful mission.

  4. Astronomical observatories

    NASA Technical Reports Server (NTRS)

    Ponomarev, D. N.

    1983-01-01

    The layout and equipment of astronomical observatories, the oldest scientific institutions of human society are discussed. The example of leading observatories of the USSR allows the reader to familiarize himself with both their modern counterparts, as well as the goals and problems on which astronomers are presently working.

  5. Observatories: History

    NASA Astrophysics Data System (ADS)

    Krisciunas, K.; Murdin, P.

    2000-11-01

    An astronomical OBSERVATORY is a building, installation or institution dedicated to the systematic and regular observation of celestial objects for the purpose of understanding their physical nature, or for purposes of time reckoning and keeping the calendar. At a bona fide observatory such work constitutes a main activity, not just an incidental one. While the ancient Egyptians, Babylonians, Chi...

  6. Amateur Observatories

    NASA Astrophysics Data System (ADS)

    Gavin, M.

    1997-08-01

    A roundup of amateur observatories in this country and abroad, with construction and location details, concluding with a detailed description and architect's drawing of the author's own observatory at Worcester Park, Surrey. The text of the 1996 Presidential Address to the British Astronomical Association.

  7. Taosi Observatory

    NASA Astrophysics Data System (ADS)

    Sun, Xiaochun

    Taosi observatory is the remains of a structure discovered at the later Neolithic Taosi site located in Xiangfen County, Shanxi Province, in north-central China. The structure is a walled enclosure on a raised platform. Only rammed-earth foundations of the structure remained. Archaeoastronomical studies suggest that this structure functioned as an astronomical observatory. Historical circumstantial evidence suggests that it was probably related to the legendary kingdom of Yao from the twenty-first century BC.

  8. Wise Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    Wise Observatory, in Mitzpe Ramon, Israel, is owned and operated by Tel Aviv University, and has a well-equipped 1 m telescope. Since construction in 1971, the large percentage of clear nights at its desert site and its unique longitude have made the observatory particularly useful for long-term monitoring projects (e.g. reverberation mapping of quasars and active galaxies), and as a part of glo...

  9. Spatial and Temporal Trends of Polyhalogenated Carbazoles in Sediments of Upper Great Lakes: Insights into Their Origin.

    PubMed

    Guo, Jiehong; Li, Zhuona; Ranasinghe, Prabha; Bonina, Solidea; Hosseini, Soheil; Corcoran, Margaret B; Smalley, Colin; Rockne, Karl J; Sturchio, Neil C; Giesy, John P; Li, An

    2017-01-03

    Polyhalogenated carbazoles (PHCZs) have been increasingly detected in the environment. Their similarities in chemical structure with legacy pollutants and their potential toxicity have caused increasing concern. In this work, 112 Ponar grab and 28 core sediment samples were collected from Lakes Michigan, Superior, and Huron, and a total of 26 PHCZs were analyzed along with unsubstituted carbazole using gas chromatography coupled with single- or triple-quadrupole mass spectrometry. Our results show that the total accumulation of PHCZs in the sediments of the upper Great Lakes is >3000 tonnes, orders of magnitude greater than those of polychlorinated biphenyls (PCBs) and decabromodiphenyl ether (BDE209). The 27 individual analytes differ in spatial distribution and temporal trend. Our results showed that PHCZs with substitution patterns of -Br2-5, -Cl1-2Br2-4, or having iodine, were more abundant in sediment of Lake Michigan deposited before 1900 than those deposited more recently, implying a natural origin. Some "emerging" PHCZs have been increasingly deposited into the sediment in recent decades, and deserve further environmental monitoring and research. Other PHCZs with low halogen substitution may form from in situ dehalogenation of PHCZs having more halogens. Anthropogenic sources of PHCZs may exist, particularly for the emerging and low molecular mass congeners.

  10. Keele Observatory

    NASA Astrophysics Data System (ADS)

    Theodorus van Loon, Jacco; Albinson, James; Bagnall, Alan; Bryant, Lian; Caisley, Dave; Doody, Stephen; Johnson, Ian; Klimczak, Paul; Maddison, Ron; Robinson, StJohn; Stretch, Matthew; Webb, John

    2015-08-01

    Keele Observatory was founded by Dr. Ron Maddison in 1962, on the hill-top campus of Keele University in central England, hosting the 1876 Grubb 31cm refractor from Oxford Observatory. It since acquired a 61cm research reflector, a 15cm Halpha solar telescope and a range of other telescopes. Run by a group of volunteering engineers and students under directorship of a Keele astrophysicist, it is used for public outreach as well as research. About 4,000 people visit the observatory every year, including a large number of children. We present the facility, its history - including involvement in the 1919 Eddington solar eclipse expedition which proved Albert Einstein's theory of general relativity - and its ambitions to erect a radio telescope on its site.

  11. Two year-long continuous monitoring of PM1 aerosol chemical composition at the Cyprus Atmospheric Observatory. Source apportionment of the Organic content and geographic origins.

    NASA Astrophysics Data System (ADS)

    Stavroulas, Iasonas; Pikridas, Michael; Oikonomou, Kostantina; Vasiliadou, Emily; Savvides, Chrysanthos; Vrekoussis, Mihalis; Mihalopoulos, Nikolaos; Gros, Valerie; Sciare, Jean

    2017-04-01

    Particulate matter with diameter smaller than 1{μ}m (PM1) induces direct and indirect effects on local and regional pollution, global climate and health. As of the beginning of 2015, the chemical composition of submicron aerosols, is continuously being monitored at the newly established Cyprus Atmospheric Observatory (CAO, http://www.cyi.ac.cy/index.php/cao.html), a national facility of the ACTRIS Research Infrastructure operated by The Cyprus Institute. Cyprus, an island located in the Eastern Mediterranean Middle East region and influenced by diverse air masses throughout the year, is ideal for monitoring photochemically aged aerosols and gaseous pollutants of both natural and anthropogenic origin. Furthermore this is a unique dataset for this area in such proximity to the Middle East, a poorly documented area in terms of atmospheric aerosol observations. An Aerodyne Quadrupole Aerosol Chemical Speciation Monitor (Q-ACSM) is currently deployed at the CAO premises (35.04N - 33.06E) situated at the rural area of Agia Marina Xyliatou on the foothill of mount Troodos at an elevation of 532m above sea level (asl). The ACSM delivers chemical composition of the major non-refractory aerosol (PM1) chemical constituents (organics, sulfate, nitrate, ammonium, chloride) with an effective (close to 100{%}) collection efficiency for particles in the diameter range of 65-700 nm at a 30 minute temporal resolution. Black Carbon (BC) was also monitored using both Magee Scientific AE-31 and AE-33 aethalometers. Quality control of the PM chemical dataset was conducted by comparison with chemical analysis performed on collocated 24-h filter samples (PM1) and comparison with 1-h PM2.5 derived from a Thermo Scientific TEOM (1400a) Monitor. Positive Matrix Factorization (PMF) was conducted and different organic aerosol factors were distinguished using the Igor based SoFi toolkit utilizing the ME-2 multilinear engine. Air mass origin was investigated for each measurement day using the

  12. Dudley Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Dudley Observatory, in Schenectady, New York, is a private foundation supporting research and education in astronomy, astrophysics and the history of astronomy. Chartered in 1852, it is the oldest organization in the US, outside academia and government, dedicated to the support of astronomical research. For more than a century it was a world leader in astrometry, with such achievements as pub...

  13. Evolution and origin of sympatric shallow-water morphotypes of Lake Trout, Salvelinus namaycush, in Canada's Great Bear Lake

    PubMed Central

    Harris, L N; Chavarie, L; Bajno, R; Howland, K L; Wiley, S H; Tonn, W M; Taylor, E B

    2015-01-01

    Range expansion in north-temperate fishes subsequent to the retreat of the Wisconsinan glaciers has resulted in the rapid colonization of previously unexploited, heterogeneous habitats and, in many situations, secondary contact among conspecific lineages that were once previously isolated. Such ecological opportunity coupled with reduced competition likely promoted morphological and genetic differentiation within and among post-glacial fish populations. Discrete morphological forms existing in sympatry, for example, have now been described in many species, yet few studies have directly assessed the association between morphological and genetic variation. Morphotypes of Lake Trout, Salvelinus namaycush, are found in several large-lake systems including Great Bear Lake (GBL), Northwest Territories, Canada, where several shallow-water forms are known. Here, we assess microsatellite and mitochondrial DNA variation among four morphotypes of Lake Trout from the five distinct arms of GBL, and also from locations outside of this system to evaluate several hypotheses concerning the evolution of morphological variation in this species. Our data indicate that morphotypes of Lake Trout from GBL are genetically differentiated from one another, yet the morphotypes are still genetically more similar to one another compared with populations from outside of this system. Furthermore, our data suggest that Lake Trout colonized GBL following dispersal from a single glacial refugium (the Mississippian) and support an intra-lake model of divergence. Overall, our study provides insights into the origins of morphological and genetic variation in post-glacial populations of fishes and provides benchmarks important for monitoring Lake Trout biodiversity in a region thought to be disproportionately susceptible to impacts from climate change. PMID:25204304

  14. Architecture, heterogeneity, and origin of late Miocene fluvial deposits hosting the most important aquifer in the Great Plains, USA

    NASA Astrophysics Data System (ADS)

    Joeckel, R. M.; Wooden, S. R.; Korus, J. T.; Garbisch, J. O.

    2014-08-01

    The Ash Hollow Formation (AHF) of the Ogallala Group is an important sedimentary archive of the emergence of the Great Plains and it contains major groundwater resources. Stratal patterns of constituent alluvial lithofacies demonstrate that the AHF is much more heterogeneous than is commonly assumed. Very fine- to fine-grained sandstone dominate overall, chiefly lithofacies Sm (massive to locally stratified sandstone). Stacked, thin sheets of Sm with accretionary macroform surfaces are common, indicating that many sandstone architectural elements originated as compound-bar deposits in dominantly sand-bed streams. Channel forms are difficult to identify and steep cutbanks are absent. Multiple units of lithofacies Sm show dense, and sometimes deep, burrowing by insects well above water tables under ancient floodplains. Massive, pedogenically modified siltstones (Fm), which compose floodplain fine architectural elements, are subsidiary in volumetric abundance to sandstones. Paleosols in these siltstones lack evidence for well-developed B horizons and advanced stages of maturity. Thin lenses of impure carbonate and laminated mud (lithofacies association Fl + C), which appear in most exposures, are deposits of ponded water in abandoned channels. Paleosols, ponded-water elements, and large vertebrate burrows in both Sm and Fm indicate that episodes of floodplain deposition, bar accretion, and channel filling were regularly followed by intervals of nondeposition on floodplains and by channel migration and abandonment. This study documents a major downdip change in the Ogallala Group overall, from source-proximal gravelly successions in the Wyoming Gangplank and deep, narrow paleovalley fills extending eastward into the Nebraska Panhandle. The lithofacies composition, stratigraphic architecture, and stratal dimensions of the AHF in the present study area are compatible with the planform geometries and floodplain soils of modestly-sized, sandy, low-sinuosity braided streams

  15. Evolution and origin of sympatric shallow-water morphotypes of Lake Trout, Salvelinus namaycush, in Canada's Great Bear Lake.

    PubMed

    Harris, L N; Chavarie, L; Bajno, R; Howland, K L; Wiley, S H; Tonn, W M; Taylor, E B

    2015-01-01

    Range expansion in north-temperate fishes subsequent to the retreat of the Wisconsinan glaciers has resulted in the rapid colonization of previously unexploited, heterogeneous habitats and, in many situations, secondary contact among conspecific lineages that were once previously isolated. Such ecological opportunity coupled with reduced competition likely promoted morphological and genetic differentiation within and among post-glacial fish populations. Discrete morphological forms existing in sympatry, for example, have now been described in many species, yet few studies have directly assessed the association between morphological and genetic variation. Morphotypes of Lake Trout, Salvelinus namaycush, are found in several large-lake systems including Great Bear Lake (GBL), Northwest Territories, Canada, where several shallow-water forms are known. Here, we assess microsatellite and mitochondrial DNA variation among four morphotypes of Lake Trout from the five distinct arms of GBL, and also from locations outside of this system to evaluate several hypotheses concerning the evolution of morphological variation in this species. Our data indicate that morphotypes of Lake Trout from GBL are genetically differentiated from one another, yet the morphotypes are still genetically more similar to one another compared with populations from outside of this system. Furthermore, our data suggest that Lake Trout colonized GBL following dispersal from a single glacial refugium (the Mississippian) and support an intra-lake model of divergence. Overall, our study provides insights into the origins of morphological and genetic variation in post-glacial populations of fishes and provides benchmarks important for monitoring Lake Trout biodiversity in a region thought to be disproportionately susceptible to impacts from climate change.

  16. Tools for Coordinated Planning Between Observatories

    NASA Technical Reports Server (NTRS)

    Jones, Jeremy; Fishman, Mark; Grella, Vince; Kerbel, Uri; Maks, Lori; Misra, Dharitri; Pell, Vince; Powers, Edward I. (Technical Monitor)

    2001-01-01

    With the realization of NASA's era of great observatories, there are now more than three space-based telescopes operating in different wavebands. This situation provides astronomers with a unique opportunity to simultaneously observe with multiple observatories. Yet scheduling multiple observatories simultaneously is highly inefficient when compared to observations using only one single observatory. Thus, programs using multiple observatories are limited not due to scientific restrictions, but due to operational inefficiencies. At present, multi-observatory programs are conducted by submitting observing proposals separately to each concerned observatory. To assure that the proposed observations can be scheduled, each observatory's staff has to check that the observations are valid and meet all the constraints for their own observatory; in addition, they have to verify that the observations satisfy the constraints of the other observatories. Thus, coordinated observations require painstaking manual collaboration among the observatory staff at each observatory. Due to the lack of automated tools for coordinated observations, this process is time consuming, error-prone, and the outcome of the requests is not certain until the very end. To increase observatory operations efficiency, such manpower intensive processes need to undergo re-engineering. To overcome this critical deficiency, Goddard Space Flight Center's Advanced Architectures and Automation Branch is developing a prototype effort called the Visual Observation Layout Tool (VOLT). The main objective of the VOLT project is to provide visual tools to help automate the planning of coordinated observations by multiple astronomical observatories, as well as to increase the scheduling probability of all observations.

  17. Grand Observatory

    NASA Astrophysics Data System (ADS)

    Young, Eric W.

    2002-01-01

    Various concepts have been recently presented for a 100 m class astronomical observatory. The science virtues of such an observatory are many: resolving planets orbiting around other stars, resolving the surface features of other stars, extending our temporal reach back toward the beginning (at and before stellar and galactic development), improving on the Next Generation Space Telescope, and other (perhaps as yet) undiscovered purposes. This observatory would be a general facility instrument with wide spectral range from at least the near ultraviolet to the mid infrared. The concept espoused here is based on a practical, modular design located in a place where temperatures remain (and instruments could operate) within several degrees of absolute zero with no shielding or cooling. This location is the bottom of a crater located near the north or south pole of the moon, most probably the South Polar Depression. In such a location the telescope would never see the sun or the earth, hence the profound cold and absence of stray light. The ideal nature of this location is elaborated herein. It is envisioned that this observatory would be assembled and maintained remotely through the use of expert robotic systems. A base station would be located above the crater rim with (at least occasional) direct line-of-sight access to the earth. Certainly it would be advantageous, but not absolutely essential, to have humans travel to the site to deal with unexpected contingencies. Further, observers and their teams could eventually travel there for extended observational campaigns. Educational activities, in general, could be furthered thru extended human presence. Even recreational visitors and long term habitation might follow.

  18. The Second Great Thermal Event from the History of the Solar System as Origin of the Lunar Asymmetries and Paleomagnetism

    NASA Astrophysics Data System (ADS)

    Neagu, A.

    1993-07-01

    To explain the origin of the natural remanent magnetism (NRM) of lunar rocks [1,2] and lunar asymmetries [3-5], many models suppose an asymmetric arrangement of matter within the early Moon [6,7]. Presented here is a model of lunar evolution that explains both the appearance of the lunar asymmetries and the presence of a high lunar palaeomagnetic field in the vicinity of 3.9 Ga starting from a symmetrically differentiated Moon. According to this model, less than 0.2 Ga after its formation as a completely molten planetary body, the Moon differentiated in concentric layers to form an anorthositic crust, a mantle, and an iron core [8]. Lunar asymmetries appeared at about 3.9 Ga ago when the Sun underwent a very violent explosive phase, generating the second great thermal event (SGTE) from the history of the solar system. Solar plasma into expansion interacted with the solar system bodies, erasing previous records on a large part of their surfaces and generating thermal effects of various kinds. Figure 1 presents the manner in which the solar plasma "excavated" within the lunar crust. The result was the displacement of the lunar center-of-figure (CF) and center-of mass (CM) from O in their present positions [3-5]. A similar "excavation" within the primordial crust of the Earth generated the appearance of a protocontinental land (Proto-Pangaea). Eccentric placement of the lunar core immediately after SGTE occurrence and its movement toward the new position of the lunar CM, along with change of the lunar spin into a synchronous rotation, generated lunar internal motions vigorously enough to drive lunar dynamo. Figure 2 presents the lunar palaeomagnetic field intensity as a function of time according to this scenario. Immediately after SGTE occurrence, the lunar crust was subjected to intensive bombardment with impacting masses belonging to Population II impactors [9]. The larger impacts generated zones of weakness and fissures within the lunar crust, but the isostatic

  19. [Clinical therapeutic aspects of the origin and the course of atherosclerosis in the veterans of the Great Patriotic War].

    PubMed

    Badaliants, I E

    2008-01-01

    The article presents the results of the research defining a number of features in development and course of some diseases typical for the veterans of the Great Patriotic war who got during the war craniocerebral traumas and wounds of various localization in compare with the patients of the same age who did not participate in the Great Patriotic war and did not have either brain traumas or wounds. Earlier development of ischemic heart disease, arterial hypertension, and cerebral atherosclerosis in veterans of Great Patriotic war has been found. The main intercurrent diseases in senior age persons have been distinguished. Some groups of psychopathological syndromes observed in persons of elderly and senile age and long-livers have been revealed.

  20. Culture in great apes: using intricate complexity in feeding skills to trace the evolutionary origin of human technical prowess.

    PubMed

    Byrne, Richard W

    2007-04-29

    Geographical cataloguing of traits, as used in human ethnography, has led to the description of 'culture' in some non-human great apes. Culture, in these terms, is detected as a pattern of local ignorance resulting from environmental constraints on knowledge transmission. However, in many cases, the geographical variations may alternatively be explained by ecology. Social transmission of information can reliably be identified in many other animal species, by experiment or distinctive patterns in distribution; but the excitement of detecting culture in great apes derives from the possibility of understanding the evolution of cumulative technological culture in humans. Given this interest, I argue that great ape research should concentrate on technically complex behaviour patterns that are ubiquitous within a local population; in these cases, a wholly non-social ontogeny is highly unlikely. From this perspective, cultural transmission has an important role in the elaborate feeding skills of all species of great ape, in conveying the 'gist' or organization of skills. In contrast, social learning is unlikely to be responsible for local stylistic differences, which are apt to reflect sensitive adaptations to ecology.

  1. The history of Vienna University Observatory - illustrated by its historical instruments and by a typoscript by Johann Steinmayr. (Original Title: Die Geschichte der Universitätssternwarte Wien - Dargestellt anhand ihrer historischen Instrumente und eines Typoskripts von Johann Steinmayr)

    NASA Astrophysics Data System (ADS)

    Hamel, Jürgen; Müller, Isolde; Posch, Thomas

    The present Institute for Astronomy of Vienna University comprises an important collection of historical instruments. They originate, among others, from the holdings of historical observatories, starting from the Jesuit observatory of the first half of the 18th century. The present volume offers a presentation of all instruments in photos and descriptions. Among those are telescopes from two centuries, angle measuring devices, clocks, globes, as well as various auxiliary instruments for positional astronomy and for astrophysical researches. Also instruments from Vienniese workshops, which document the high level of local instrument construction, are included in the collection. The second part of the book contains the first publication of the history of the Viennese observatories by Johann Steinmayr, written in 1932-1935, and preceded by a biographical essay by Nora Pärr. His text is based on an extensive study of sources and is until now the most complete of its kind, Steinmayr, who was a member of the Society of Jesus, was sentenced to death in 1944 by the national socialist People's Court because of his involvement in the Austrian resistance movement.

  2. Urania in the Marketplace: Observatories as Holiday Destinations

    NASA Astrophysics Data System (ADS)

    Rumstay, Kenneth S.

    2015-01-01

    During the twentieth century astronomical imagery was frequently incorporated, by manufacturers of industrial and consumer goods, into advertisements which appeared in popular magazines in America. The domes and telescopes of major observatories were often featured. In some cases, particularly within the Golden State of California, major astronomical facilities (notably the Lick and Mt. Wilson Observatories) were touted as tourist attractions and were publicized as such by tourist bureaus, railroads, and hotels.A particularly interesting example is provided by the Hotel Vendome in San Jose. With completion of the Lick Observatory (and the 36-inch Great Refractor) in 1887, the local business community felt that the city needed a first-class resort hotel. The architectural firm of Jacob Lenzen & Son was hired to design a grand hotel, comparable to those found in locales such as Monterey and Pasadena. The resulting four-story, 150-room structure cost 250,000, a phenomenal sum in those days. Yet, within just fourteen years, tourist demand led to the construction of a 36-room annex. Of course, a great resort hotel would not be complete without the opportunity for excursion, and the Mt. Hamilton Stage Company offered daily trips to the famous Lick Observatory.Farther south, the Mt. Wilson Observatory began construction of its own hotel in 1905.The original structure was destroyed by fire in 1913, and replaced by a second which was used by visitors until 1966.Early examples of advertisements for these observatories, recalling the heyday of astronomical tourism, are presented. A few more recent ones for Arecibo and Palomar are included for comparison.

  3. WIMPs search at OTO Cosmo Observatory

    NASA Astrophysics Data System (ADS)

    Fushimi, K.; Ichihara, K.; Koori, N.; Nakayama, S.; Shichijo, Y.; Ogawa, I.; Yoshida, S.; Ajimura, S.; Hazama, R.; Ishikawa, Y.; Itamura, M.; Kishimoto, T.; Kunitomi, G.; Matsuoka, K.; Miyawaki, H.; Shiomi, S.; Suzuki, N.; Tanaka, Y.; Umehara, S.; Ejiri, H.; Kudomi, N.; Kume, K.; Takahisa, K.; Ohsumi, H.; Yanagida, Y.

    2003-03-01

    WIMPs dark matter and double beta decays has been studied at OTO Cosmo Observatory. The observatory has great advantages of small cosmic ray flux, small neutron flux and small radon density. The recent status of WIMPs search by huge NaI (ELEGANT V), large CaF2Eu) (ELEGANT VI) and high sesitive NaI detector are reported.

  4. Genetic effects of habitat restoration in the Laurentian Great Lakes: an assessment of lake sturgeon origin and genetic diversity

    USGS Publications Warehouse

    Jamie Marie Marranca,; Amy Welsh,; Roseman, Edward F.

    2015-01-01

    Lake sturgeon (Acipenser fulvescens) have experienced significant habitat loss, resulting in reduced population sizes. Three artificial reefs were built in the Huron-Erie corridor in the Great Lakes to replace lost spawning habitat. Genetic data were collected to determine the source and numbers of adult lake sturgeon spawning on the reefs and to determine if the founder effect resulted in reduced genetic diversity. DNA was extracted from larval tail clips and 12 microsatellite loci were amplified. Larval genotypes were then compared to 22 previously studied spawning lake sturgeon populations in the Great Lakes to determine the source of the parental population. The effective number of breeders (Nb) was calculated for each reef cohort. The larval genotypes were then compared to the source population to determine if there were any losses in genetic diversity that are indicative of the founder effect. The St. Clair and Detroit River adult populations were found to be the source parental population for the larvae collected on all three artificial reefs. There were large numbers of contributing adults relative to the number of sampled larvae. There was no significant difference between levels of genetic diversity in the source population and larval samples from the artificial reefs; however, there is some evidence for a genetic bottleneck in the reef populations likely due to the founder effect. Habitat restoration in the Huron-Erie corridor is likely resulting in increased habitat for the large lake sturgeon population in the system and in maintenance of the population's genetic diversity.

  5. Haystack Observatory

    NASA Technical Reports Server (NTRS)

    1972-01-01

    Radio astronomy programs comprise three very-long-baseline interferometer projects, ten spectral line investigations, one continuum mapping in the 0.8 cm region, and one monitoring of variable sources. A low-noise mixer was used in mapping observations of 3C273 at 31 GHz and in detecting of a new methyl alcohol line at 36,169 MHz in Sgr B2. The new Mark 2 VLBI recording terminal was used in galactic H2O source observations using Haystack and the Crimean Observatory, USSR. One feature in W29 appears to have a diameter of 0.3 millisec of arc and a brightness temperature of 1.4 x 10 to the 15th power K. Geodetic baseline measurements via VLBI between Green Bank and Haystack are mutually consistent within a few meters. Radar investigations of Mercury, Venus, Mars, and the Moon have continued. The favorable opposition of Mars and improvements in the radar permit measurements on a number of topographic features with unprecedented accuracy, including scarps and crater walls. The floor of Mare Serenitatis slopes upward towards the northeast and is also the location of a strong gravitational anomaly.

  6. The great escape: World War II, neo-freudianism, and the origins of U.S. psychocultural analysis.

    PubMed

    Gitre, Edward J K

    2011-01-01

    Psychocultural analysis stands as a signal accomplishment of the 1930s U.S. assimilation of European refugee-intellectuals. Scholars in the U.S. had been moving toward a kind of psychocultural analysis well in advance of the Great Migration--the U.S. was not an intellectual vacuum or wasteland--nevertheless, it was through their interdisciplinary collaboration, fueled by the specter of war, that these international peers stimulated one of the most wide-ranging, dynamic, and productive exchanges of ideas of the century. Through the lens of Erich Fromm's Escape from Freedom, this article explores psychoculturalism's emergence in the interstices between cultures, nations, ideas, and disciplines--between Europeans and Americans, psychoanalysts and social scientists. © 2011 Wiley Periodicals, Inc.

  7. Do comets C/1861 G1 (Thatcher) and C/1861 J1 (Great comet) have a common origin?

    NASA Astrophysics Data System (ADS)

    Branham, R. L.

    2015-10-01

    A new orbit is calculated for Comet C/1861 G1 (Thatcher), associated with the Lyrid meteor shower, to replace Oppolzer's orbit of 1864. The new orbit is based upon 649 observations, 326 in right ascension and 323 in declination, made between 11 April 1861 and 7 Sept. 1861. The final orbit uses residuals calculated with the Welsch weighting function. The comet's period of 416.87 ± 0.56 yr agrees with Oppolzer's period of 415 yr athough other elements such as the inclination differ. Although the post-perihelion residuals are relatively random, 52.1% probability of randomness, pre-perihelion residuals lack randomness indicating possible deviations from Keplerian motion caused by ejection of meteoritic material. Comet Thatcher is unrelated to the Great comet of 1861.

  8. The great lunar hot spot and the composition and origin of the Apollo mafic (``LKFM'') impact-melt breccias

    NASA Astrophysics Data System (ADS)

    Korotev, Randy L.

    2000-02-01

    Thorium-rich, mafic impact-melt breccias from the Apollo 14-17 missions, that is, those breccias identified with the composition known as ``LKFM,'' are regarded largely as products of basin-forming impacts that penetrated the feldspathic crust and sampled underlying mafic material and magma-ocean residuum carrying the compositional signature of KREEP (potassium, rare earth elements, phosphorous). Despite considerable compositional variation among such breccias, compositions of all of them correspond to mixtures of only four components: (1) a norite with composition generally similar to that of Apollo 15 basalt (mean abundance: 58% range: ~30-95%), (2) Fo~90 dunite (mean: 13%, range: 1-27%), (3) feldspathic upper crust (mean: 29%, range: 4-50%), and FeNi metal (0.1-1.7%). Petrographic evidence has shown that much of the feldspathic component, but none of the KREEP component, is clastic. This observation and the high proportion of KREEP norite component in the breccias suggest that the melt zone of the impact or impacts forming the breccias contained little feldspathic material but consisted predominantly of material with the average composition of KREEP norite. The dunite component probably derives ultimately from the upper mantle. These conclusions support the hypothesis that the breccias were not formed in typical feldspathic crust but instead by one or more impacts into what is designated here ``the great lunar hot spot,'' that is, the anomalous Th-rich terrane in the Imbrium-Procellarum area identified by the Apollo and Lunar Prospector gamma-ray spectrometers. The LKFM composition is a special product of the great lunar hot spot and is not the average composition of the lower crust in typical feldspathic highlands. Similarly, Mg-suite and alkali-suite plutonic rocks of the Apollo collection are likely all differentiation products of the hot spot, not of plutons that might occur in typical feldspathic crust.

  9. New constraints on the origin of the Australian Great Barrier Reef: Results from an international project of deep coring

    NASA Astrophysics Data System (ADS)

    ConsortiumGreat Barrier Reef Drilling, International

    2001-06-01

    Two new boreholes provide the first direct evidence of the age of the Australian Great Barrier Reef. An inner shelf sequence (total depth, 86 m; basal age = 210 ± 40 ka) comprises a dominantly siliciclastic unit (thickness ˜52 86 m), overlain by four carbonate units (total thickness 0 34 m). A shelf-edge and slope sequence (total depth 210 m) reveals three major sections: (1) a lower section of resedimented flows deposited on a lower slope, (2) a mid-section including intervals of corals, rhodoliths, and calcarenites with low- angle graded laminae, and (3) an upper section of four shelf- margin coral-reef units separated by karst surfaces bearing paleosols. Sr isotope and magnetostratigraphic data indicate that the central Great Barrier Reef is relatively young (post Brühnes-Matuyama boundary time), and our best estimate for the onset of reef growth on the outer barrier system is ca. 600 ± 280 ka. This date suggests that reef initiation may have been related to the onset of full eccentricity-dominated glacio-eustatic sea-level oscillation as inferred from large-amplitude “saw-tooth” 100 k.y. δ18O cycles (after marine isotope stage 17), rather than to some regional environmental parameter. A major question raised by our study is whether reef margins globally display a similar growth history. The possibility of a global reef initiation event has important implications for basin to shelf partitioning of CaCO3, atmospheric carbon dioxide levels, and global temperature change during Quaternary time.

  10. Origins.

    PubMed

    Weinberg, S

    1985-10-04

    The farthest of the galaxies that can be seen through the large ground-based telescopes of modern astronomy, such as those on La Palma in the Canary Islands, are so far away that they appear as they did close to the time of the origin of the universe, perhaps some 10 billion years ago. Much has been learned, and much has still to be learned, about the young universe from optical and radio telescopes, but these instruments cannot be used to look directly at the universe in its first few hundred thousand years. Instead, they are used to search the relatively recent past for relics of much earlier times. Together with experiments planned for the next generation of elementary particle accelerators, astronomical observations should continue to extend what is known about the universe backward in time to the Big Bang and may eventually help to reveal the origins of the physical laws that govern the universe.

  11. The Great Wall in the CfA survey - Its origin and imprint on the microwave background radiation

    NASA Technical Reports Server (NTRS)

    Atrio-Barandela, F.; Kashlinsky, A.

    1992-01-01

    The paper models the evolution of the Great Wall (GW) after recombination and the influence of its time-dependent gravitational potential on the MBR. It is shown that within the framework of the Zel'dovich approximation the (pre)GW region can be treated as an ellipsoid. The GW is approximated as an oblate ellipsoid that started at recombination with an almost spherical shape, but with initial density contrast, delta-i, much smaller than it had to be in the spherical model in order to reach the observed density contrast of beta-f of 5. The resultant delta-i is compatible with the rms value of delta-rho/rho on the GW scale at recombination for models with the n less than 0 power spectrum of the primordial density field. It is shown that the time-dependent potential of the GW will induce a detectable fluctuation in MBR. The possibility of similar structures located at higher redshifts producing measurable and perhaps dominant statistical MBR anisotropies by this effect is also discussed.

  12. ESO's Two Observatories Merge

    NASA Astrophysics Data System (ADS)

    2005-02-01

    On February 1, 2005, the European Southern Observatory (ESO) has merged its two observatories, La Silla and Paranal, into one. This move will help Europe's prime organisation for astronomy to better manage its many and diverse projects by deploying available resources more efficiently where and when they are needed. The merged observatory will be known as the La Silla Paranal Observatory. Catherine Cesarsky, ESO's Director General, comments the new development: "The merging, which was planned during the past year with the deep involvement of all the staff, has created unified maintenance and engineering (including software, mechanics, electronics and optics) departments across the two sites, further increasing the already very high efficiency of our telescopes. It is my great pleasure to commend the excellent work of Jorge Melnick, former director of the La Silla Observatory, and of Roberto Gilmozzi, the director of Paranal." ESO's headquarters are located in Garching, in the vicinity of Munich (Bavaria, Germany), and this intergovernmental organisation has established itself as a world-leader in astronomy. Created in 1962, ESO is now supported by eleven member states (Belgium, Denmark, Finland, France, Germany, Italy, The Netherlands, Portugal, Sweden, Switzerland, and the United Kingdom). It operates major telescopes on two remote sites, all located in Chile: La Silla, about 600 km north of Santiago and at an altitude of 2400m; Paranal, a 2600m high mountain in the Atacama Desert 120 km south of the coastal city of Antofagasta. Most recently, ESO has started the construction of an observatory at Chajnantor, a 5000m high site, also in the Atacama Desert. La Silla, north of the town of La Serena, has been the bastion of the organization's facilities since 1964. It is the site of two of the most productive 4-m class telescopes in the world, the New Technology Telescope (NTT) - the first major telescope equipped with active optics - and the 3.6-m, which hosts HARPS

  13. Saturn's Great Storm of 2010-2011: Cloud particles containing ammonia and water ices indicate a deep convective origin. (Invited)

    NASA Astrophysics Data System (ADS)

    Sromovsky, L. A.; Baines, K. H.; Fry, P.

    2013-12-01

    Saturn's Great Storm of 2010-2011 was first detected by amateur astronomers in early December 2010 and later found in Cassini Imaging Science Subsystem (ISS) images taken on 5 December, when it took the form of a 1000 km wide bright spot. Within a week the head of the storm grew by a factor of ten in width and within a few months created a wake that encircled the planet. This is the sixth Great Saturn Storm in recorded history, all having appeared in the northern hemisphere, and most near northern summer solstice at intervals of roughly 30 years (Sanchez-Lavega et al. 1991, Nature 353, 397-401). That the most recent storm appeared 10 years early proved fortunate because Cassini was still operating in orbit around Saturn and was able to provide unique observations from which we could learn much more about these rare and enormous events. Besides the dramatic dynamical effects displayed at the visible cloud level by high-resolution imaging observations (Sayanagi et al. 2013, Icarus 223, 460-478), dramatic thermal changes also occurred in the stratosphere above the storm (Fletcher et al. 2011, Science 332, 1413), and radio measurements of lightning (Fischer et al., 2011, Nature 475, 75-77) indicated strong convective activity at deeper levels. Numerical models of Saturn's Giant storms (Hueso and Sanchez-Lavega 2004, Icarus 172, 255-271) suggest that they are fueled by water vapor condensation beginning at the 10-12 bar level, some 250 km below the visible cloud tops. That idea is also supported by our detection of water ice near the cloud tops (Sromovsky et al. 2013, Icarus 226, 402-418). From Cassini VIMS spectral imaging taken in February 2011, we learned that the storm's cloud particles are strong absorbers of sunlight at wavelengths from 2.8 to 3.1 microns. Such absorption is not seen on Saturn outside of storm regions, implying a different kind of cloud formation process as well as different cloud composition inside the storm region. We found compelling evidence

  14. Lowell Observatory's Discovery Channel Telescope

    NASA Astrophysics Data System (ADS)

    Hall, Jeffrey C.

    2017-01-01

    Lowell Observatory broke ground on its 4.3-meter Discovery Channel Telescope (DCT) in July 2005 and celebrated first light for the telescope in July 2012. In this overview to this special session, I will discuss the origin and development of the project, the telescope's general specifications and performance, its current operating status, and the initial instrument suite.

  15. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1959-01-01

    This image is of the Crab Nebula in visible light photographed by the Hale Observatory optical telescope in 1959. The faint object at the center had been identified as a pulsar and is thought to be the remains of the original star. It had been observed as a pulsar in visible light, radio wave, x-rays, and gamma-rays.

  16. Effects of coancestry on accuracy of individual assignments to population of origin: examples using Great Lakes lake trout (Salvelinus namaycush).

    PubMed

    Guinand, Bruno; Scribner, Kim T; Page, Kevin S; Filcek, Kristi; Main, Laura; Burnham-Curtis, Mary K

    2006-05-01

    Methods for assigning individuals to population of origin are widely used in ecological genetics, resources management, and forensics. Characteristics of genetic data obtained from putative source populations that enhance accuracy of assignment are well established. How non-independence within and among unknown individuals to be classified [i.e., gene correlations within individual (inbreeding) and gene correlations among individuals within group (coancestry)] affect assignment accuracy is poorly understood. We used empirical data for six microsatellite loci and offspring from full-sib crosses of hatchery strains of lake trout (Salvelinus namaycush; Salmonidae) representing known levels of coancestry (mean theta = 0.006 and 0.06) within families to investigate how gene correlations can affect assignment. Additional simulations were conducted to further investigating the influence of allelic diversity (2, 6 or 10 alleles per locus) and inbreeding (F = 0.00, 0.05, and 0.15) on assignment accuracy for cases of low and high inter-population variance in allele frequency (mean F (st) = 0.01 and 0.1, respectively). Inbreeding had no effect on accuracy of assignments. In contrast, variance in assignment accuracy across replicated simulations, and for each empirical case study increased with increasing coancestry, reflecting non-independence of probabilities of correct assignment among members of kin groups. Empirical estimates of assignment error rates should be interpreted with caution if appreciable levels of coancestry are suspected. Additional emphasis should be placed on sampling designs (spatially and temporally) that define or minimize the potential for sampling related individuals.

  17. Importance of geographic origin for invasion success: A case study of the North and Baltic Seas versus the Great Lakes-St. Lawrence River region.

    PubMed

    Casties, Isabel; Seebens, Hanno; Briski, Elizabeta

    2016-11-01

    Recently, several studies indicated that species from the Ponto-Caspian region may be evolutionarily predisposed to become nonindigenous species (NIS); however, origin of NIS established in different regions has rarely been compared to confirm these statements. More importantly, if species from certain area/s are proven to be better colonizers, management strategies to control transport vectors coming from those areas must be more stringent, as prevention of new introductions is a cheaper and more effective strategy than eradication or control of established NIS populations. To determine whether species evolved in certain areas have inherent advantages over other species in colonizing new habitats, we explored NIS established in the North and Baltic Seas and Great Lakes-St. Lawrence River regions-two areas intensively studied in concern to NIS, highly invaded by Ponto-Caspian species and with different salinity patterns (marine vs. freshwater). We compared observed numbers of NIS in these two regions to expected numbers of NIS from major donor regions. The expected numbers were calculated based on the available species pool from donor regions, frequency of shipping transit, and an environmental match between donor and recipient regions. A total of 281 NIS established in the North and Baltic Seas and 188 in the Great Lakes-St. Lawrence River. Ponto-Caspian taxa colonized both types of habitats, saltwater areas of the North and Baltic Seas and freshwater of the Great Lakes-St. Lawrence River, in much higher numbers than expected. Propagule pressure (i.e., number of introduced individuals or introduction effort) is of great importance for establishment success of NIS; however in our study, either shipping vector or environmental match between regions did not clarify the high numbers of Ponto-Caspian taxa in our study areas. Although we cannot exclude the influence of other transport vectors, our findings suggest that the origin of the species plays an important role

  18. Origin of an Eastern North America Great Escarpment, Based on (U-Th)/He Dating and Geomorphic Analysis

    NASA Astrophysics Data System (ADS)

    Bank, G. C.; Spotila, J. A.; Reiners, P. W.

    2001-12-01

    Many passive margin great escarpments have been interpreted as the result of slow, steady erosional processes following continental rifting. Rugged escarpments may be maintained by parallel slope retreat and drainage divide migration, driven by flexure of the lithosphere associated with rift flank uplift and the isostatic response to denudation and mass transfer from thickened mountain belts to offshore basins. In eastern North America, an escarpment bounding the eastern limit of the southern Appalachian Mountains stands high and rugged, despite a prolonged period of time since cessation of tectonic activity along this passive margin. Whether this feature is the product of slow, steady erosional processes along the continental margin since rifting in the early Mesozoic and cessation of orogenesis in the late Paleozoic, or the result of recent rejuvenation, has been the subject of debate. To investigate this, we have constrained the erosional kinematics of the Blue Ridge Escarpment in Virginia and North Carolina using radiogenic helium thermochronometry and other geomorphic data. Helium ages from rocks above and extending west of the escarpment are old (157-197 Ma), consistent with very slow cooling and denudation since the early Mesozoic. In contrast, helium ages are younger along the Piedmont surface, 500 m below and to the east of the escarpment (94-137 Ma). Although this difference may partly represent an age-elevation gradient associated with either slow exhumation and cooling or an exhumed helium partial retention zone, it cannot be fully explained without lateral variations in exhumation rate. Our working interpretation is that the western Piedmont has experienced as much as several km more exhumation than the Blue Ridge upland since samples cooled through their closure temperatures, effectively bending isochrons upwards to the east. The greater magnitude of denudation east of this east-facing escarpment is not consistent with escarpment formation by

  19. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1978-01-01

    Both of the High Energy Astronomy Observatory (HEAO) 2/Einstein Observatory imaging devices were used to observe the Great Nebula in Andromeda, M31. This image is a wide field x-ray view of the center region of M31 by the HEAO-2's Imaging Proportional Counter. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  20. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1970-01-01

    This artist's concept depicts the third observatory, the High Energy Astronomy Observatory (HEAO)-3 in orbit. Designed and developed by TRW, Inc. under the direction of the Marshall Space Flight Center, the HEAO-3's mission was to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit.

  1. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1977-01-01

    This photograph shows the High Energy Astronomy Observatory (HEAO)-1 being assembled at TRW Systems of Redondo Beach, California. The HEAO was designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit.

  2. Byurakan Astrophysical Observatory

    NASA Astrophysics Data System (ADS)

    Mickaelian, A. M.

    2016-09-01

    This booklet is devoted to NAS RA V. Ambartsumian Byurakan Astrophysical Observatory and is aimed at people interested in astronomy and BAO, pupils and students, BAO visitors and others. The booklet is made as a visiting card and presents concise and full information about BAO. A brief history of BAO, the biography of the great scientist Viktor Ambartsumian, brief biographies of 13 other deserved scientists formerly working at BAO (B.E. Markarian, G.A. Gurzadyan, L.V. Mirzoyan, M.A. Arakelian, et al.), information on BAO telescopes (2.6m, 1m Schmidt, etc.) and other scientific instruments, scientific library and photographic plate archive, Byurakan surveys (including the famous Markarian Survey included in the UNESCO Memory of the World International Register), all scientific meetings held in Byurakan, international scientific collaboration, data on full research staff of the Observatory, as well as former BAO researchers, who have moved to foreign institutions are given in the booklet. At the end, the list of the most important books published by Armenian astronomers and about them is given.

  3. Mission Planning for the CHANDRA X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    Mullins, Larry D.; Stone, Russell, L.; Evans, Steven W.

    1999-01-01

    The CHANDRA x-ray observatory started life as the Advanced X-ray Facility (AXAF) but was renamed Chandra in December of 1998 at the of a nationwide contest by NASA to name the new observatory. The honors the Nobel Prize winning astrophysicist S. Chandrasekar who astrophysics at the University of Chicago for more than 50 years, following graduate studies at Cambridge University in England. The observatory has been under construction for a decade under the management of the Observatory observatory, Projects office at the Marshall Space Flight Center; the same office that oversaw the construction of the Hubble Space Telescope and the Compton Gamma Ray Observatory. This observatory is a member of NASA's great observatory series of missions of which Hubble and Compton are members. This paper describes the mission planning that was conducted at MSFC to design the orbit and launch window that would permit the new observatory to function properly.

  4. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1982-01-01

    This artist's conception depicts the High Energy Astronomy Observatory (HEAO)-1 in orbit. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit. The HEAO project involved the launching of three unmarned scientific observatories into low Earth orbit between 1977 and 1979 to study some of the most intriguing mysteries of the universe; pulsars, black holes, neutron stars, and super nova. Hardware support for the imaging instruments was provided by American Science and Engineeing. The HEAO spacecraft were built by TRW, Inc. under project management of the Marshall Space Flight Center.

  5. Virtual Observatory Science Applications

    NASA Technical Reports Server (NTRS)

    McGlynn, Tom

    2005-01-01

    Many Virtual-Observatory-based applications are now available to astronomers for use in their research. These span data discovery, access, visualization and analysis. Tools can quickly gather and organize information from sites around the world to help in planning a response to a gamma-ray burst, help users pick filters to isolate a desired feature, make an average template for z=2 AGN, select sources based upon information in many catalogs, or correlate massive distributed databases. Using VO protocols, the reach of existing software tools and packages can be greatly extended, allowing users to find and access remote information almost as conveniently as local data. The talk highlights just a few of the tools available to scientists, describes how both large and small scale projects can use existing tools, and previews some of the new capabilities that will be available in the next few years.

  6. Molonglo Observatory: Building the Cross and MOST

    NASA Astrophysics Data System (ADS)

    McAdam, Bruce

    2008-03-01

    When Bernard Mills left the GSIRO in 1960 to establish a radio astronomy group in the School of Physics, University of Sydney, he had not only invented the principle of cross-type radio telescopes but proved their great efficiency at surveying the positions, intensity and structure of radio sources. He had ambitious plans for a second generation Cross - a radio telescope with arms one mile long. This paper describes the circumstances of Mills' appointment as Professor of Astrophysics and the recruitment of an international Department that achieved his vision with the Molonglo Cross: The construction involved interaction with many colleagues - engineers in other university departments and government agencies, and with the contracting firms. Formal links were set up with the Electrical Engineering Department through The Radio Astronomy Centre in the University of Sydney and then with Arecibo Observatory through the Cornell-Sydney University Astronomy Center. When the Molonglo Cross completed its main survey in 1978 after eleven years, it was switched off and the EW arm was then converted to the Molonglo Observatory Synthesis Telescope. Many of the staff involved with the MOST are now challenged by SKAMP, testing systems for the Square Kilometre Array with cylindrical geometry in the Molonglo Prototype. These two later developments out of the original Cross telescope are described briefly.

  7. Survey of the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Dova, T.; Pierre Auger Observatory Collaboration

    The question of the origin and nature of cosmic ray particles with energies exceeding the predicted GZK spectral cutoff is one of the present great challenges of astroparticle physics. The Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, is a broadly based international effort to explore the upper-end of the cosmic ray energy spectrum. The PAO is the first experiment designed to work in a hybrid detection mode. The combination of two complementary detection techniques -water Cerenkov tank arrays overlooked by atmospheric fluorescence detectorsto observe extensive air showers guarantees high-quality and statistically significant data. An updated overview of the science prospects for the PAO is presented. The concept of the experiment as well as the current status is described. 1 Physics motivation for the Pierre Auger Observatory The puzzle set by the existence of cosmic rays with energies above 1020 eV (Lawrence et al., 1991; Hayashida et al., 1994; Bird et al., 1995; Abu-Zayyad et al, 1999), which may be an indication of new physics or exotic particles, is at present one of the hot topics in high energy astroparticle physics. The underlying problem in trying to explain the origin of these extremely high energy cosmic rays (EHECR) is the well-known GZK (Greisen-Zatsepin-Kuzmin) effect: if the cosmic rays are extragalactic in origin, then a sharp cutoff at around several times 1019 eV in the observed spectrum is expected due to energy degradation of the cosmic ray particles through interaction with photons of the microwave background radiation (Greisen, 1965; Zatsepin and Kuzmin, 1966). This process limits the distance of the sources of particles with energies above 1020 eV to less than 100 Mpc from the Earth (Aharonian and Cronin, 1994; Puget et al., 1976; Stecker and Salomon, 1999; Berezinsky, 1970; Protheroe and Biermann, 1996). Since the energy loss mechanism depends on

  8. Great Lakes: Great Gardening.

    ERIC Educational Resources Information Center

    New York Sea Grant Inst., Albany, NY.

    This folder contains 12 fact sheets designed to improve the quality of gardens near the Great Lakes. The titles are: (1) "Your Garden and the Great Lakes"; (2) "Organic Gardening"; (3) "Fruit and Vegetable Gardening"; (4) "Composting Yard Wastes"; (5) "Herbicides and Water Quality"; (6)…

  9. Popularization of Astronomy Through Robotic Telescopes and Virtual Observatories

    NASA Astrophysics Data System (ADS)

    Aleksic, J.; Tomic, Z.

    2013-05-01

    Robotic telescopes and virtual observatories have great impact on popularization of astronomy. In this paper we will present several web services and observatories that allow remote control over their equipment, which have great contribution in astronomy promotion. In addition, the first Serbian amateur robotic observatory will be presented (Night Hawk, Bačka Palanka). Finally, an economic review of this concept is done to consider its attainability to the general audience.

  10. Proventricular adenocarcinoma in a Humboldt penguin (Spheniscus humboldti) and a great horned owl (Bubo virginianus); identification of origin by mucin histochemistry.

    PubMed

    Yonemaru, Kayoko; Sakai, Hiroki; Asaoka, Yoshiji; Yanai, Tokuma; Fukushi, Hideto; Watanabe, Ken; Hirai, Katsuya; Masegi, Toshiaki

    2004-02-01

    Cases of proventricular neoplasm in a Humboldt penguin (Spheniscus humboldti) and a great horned owl (Bubo virginianus) were observed. Microscopically, the neoplastic cells formed branching tubules or acini in both cases. Galactose oxidase-Schiff (GOS) staining revealed that the cytoplasm of the normal surface epithelium and surface mucosubstances of the proventriculus adjacent to the neoplasm were positive in both cases. The neoplastic cells in both cases were also classified as GOS-positive. Therefore, the two proventricular neoplasms in this report were diagnosed as proventricular adenocarcinoma that arose from the proventricular surface epithelium. This study suggests that the mucosubstances, which the neoplastic cells produced, were a useful index for identifying the origin of the neoplastic cells in the birds.

  11. Private Observatories in South Africa

    NASA Astrophysics Data System (ADS)

    Rijsdijk, C.

    2016-12-01

    Descriptions of private observatories in South Africa, written by their owners. Positions, equipment descriptions and observing programmes are given. Included are: Klein Karoo Observatory (B. Monard), Cederberg Observatory (various), Centurion Planetary and Lunar Observatory (C. Foster), Le Marischel Observatory (L. Ferreira), Sterkastaaing Observatory (M. Streicher), Henley on Klip (B. Fraser), Archer Observatory (B. Dumas), Overbeek Observatory (A. Overbeek), Overberg Observatory (A. van Staden), St Cyprian's School Observatory, Fisherhaven Small Telescope Observatory (J. Retief), COSPAR 0433 (G. Roberts), COSPAR 0434 (I. Roberts), Weltevreden Karoo Observatory (D. Bullis), Winobs (M. Shafer)

  12. Queen Jadwiga Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Wszołek, Bogdan

    2016-06-01

    Private Astronomical Observatory was open in June 2015. The main aim of the observatory is to provide and share astronomical and space knowledge. It collects research instruments and expands didactic infrastructure. Continuously, there is an open call for specialists to join the Honorary Staff of the Observatory.

  13. The Boulder magnetic observatory

    USGS Publications Warehouse

    Love, Jeffrey J.; Finn, Carol A.; Pedrie, Kolby L.; Blum, Cletus C.

    2015-08-14

    The Boulder magnetic observatory has, since 1963, been operated by the Geomagnetism Program of the U.S. Geological Survey in accordance with Bureau and national priorities. Data from the observatory are used for a wide variety of scientific purposes, both pure and applied. The observatory also supports developmental projects within the Geomagnetism Program and collaborative projects with allied geophysical agencies.

  14. The Pierre Auger Cosmic Ray Observatory

    DOE PAGES

    Aab, Alexander

    2015-07-08

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above 1017 eV and study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water Cherenkov particle detector stations spread over 3000 km2 overlooked by 24 air fluorescence telescopes. Additionally, three high elevation fluorescence telescopes overlook a 23.5 km2, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completionmore » in 2008 and has recorded data from an exposure exceeding 40,000 km2 sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Observatory.« less

  15. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1970-01-01

    This schematic details the third High Energy Astronomy Observatory (HEAO)-3. The HEAO-3's mission was to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit.

  16. The Chandra X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    Weisskopf, M. C.

    2001-01-01

    The Chandra X-Ray Observatory is the X-ray component of NASA's Great observatories which also includes the recently decommissioned Compton Gamma Ray Observatory, the Hubble Space Telescope, and the soon to be launched Space Infra Red Telescope Facility. Chandra is a unique X-ray astronomy facility for high-resolution imaging and for high-resolution spectroscopy. Chandra's performance advantage over other X-ray observatories is analogous to that of the Hubble Space Telescope over ground-based observatories. Chandra is a NASA facility that provides scientific data to the international astronomical community in response to proposals for its use. Data becomes public one year after the observation. The Observatory is the product of the efforts of many commercial, academic, and government organizations in the United States and Europe. NASA's Marshall Space Flight Center (MSFC) manages the Project and provides Project Science; TRW Space and Electronics Group served as prime contractor responsible for providing the spacecraft, the telescope, and assembling and testing the observatory; the Smithsonian Astrophysical Observatory (SAO) provides technical support and is responsible for ground operations.

  17. Planetary research at Lowell Observatory

    NASA Technical Reports Server (NTRS)

    Baum, William A.

    1988-01-01

    Scientific goals include a better determination of the basic physical characteristics of cometary nuclei, a more complete understanding of the complex processes in the comae, a survey of abundances and gas/dust ratios in a large number of comets, and measurement of primordial (12)C/(13)C and (14)N/(15)N ratios. The program also includes the observation of Pluto-Charon mutual eclipses to derive dimensions. Reduction and analysis of extensive narrowband photometry of Comet Halley from Cerro Tololo Inter-American Observatory, Perth Observatory, Lowell Observatory, and Mauna Kea Observatory were completed. It was shown that the 7.4-day periodicity in the activity of Comet Halley was present from late February through at least early June 1986, but there is no conclusive evidence of periodic variability in the preperihelion data. Greatly improved NH scalelengths and lifetimes were derived from the Halley data which lead to the conclusion that the abundance of NH in comets is much higher than previously believed. Simultaneous optical and thermal infrared observations were obtained of Comet P/Temple 2 using the MKO 2.2 m telescope and the NASA IRTF. Preliminary analysis of these observations shows that the comet's nucleus is highly elongated, very dark, and quite red.

  18. Great Minds? Great Lakes!

    ERIC Educational Resources Information Center

    Environmental Protection Agency, Chicago, IL. Great Lakes National Program Office.

    This booklet introduces an environmental curriculum for use in a variety of elementary subjects. The lesson plans provide an integrated approach to incorporating Great Lakes environmental issues into the subjects of history, social studies, and environmental sciences. Each of these sections contains background information, discussion points, and a…

  19. Impact of the Great East Japan earthquake on out-of-hospital cardiac arrest with cardiac origin in non-disaster areas [corrected].

    PubMed

    Kiyohara, Kosuke; Kitamura, Tetsuhisa; Iwami, Taku; Nishiyama, Chika; Kawamura, Takashi

    2015-02-01

    To examine changes in the incidence of out-of-hospital cardiac arrest (OHCA) with cardiac origin in the non-disaster areas of Japan before and after the Great East Japan Earthquake of 11 March 2011. The 35 prefectures in Japan with no dead or missing caused directly by the earthquake were defined as the non-disaster areas. Data of adult OHCA patients in the non-disaster areas from March 4 to 24 each year from 2005 to 2011 were obtained from the All-Japan Utstein Registry. Risk ratios (RRs) of OHCA incidence and 95% CIs were estimated for three specific weeks in 2011 (1 week before and 2 weeks after the earthquake) by applying multivariable Poisson regression model. Incidence in the corresponding periods of March 4-24 from 2005 to 2010 was set as the baseline risk. In the analyses from a total of 17,353 OHCA patients, the incidence statistically significantly increased in the first week after the earthquake in all adults (adjusted-RR=1.13, 95% CI=1.05 to 1.22, p=0.001) and in elderly women (adjusted-RR=1.23, 95% CI=1.11 to 1.37, p<0.001). The Great East Japan Earthquake caused the increase of OHCA among elderly women even in the non-disaster areas. Published by the BMJ Publishing Group Limited. For permission to use (where not already granted under a licence) please go to http://group.bmj.com/group/rights-licensing/permissions.

  20. Expanding the HAWC Observatory

    NASA Astrophysics Data System (ADS)

    Mori, Johanna; HAWC Collaboration; College of Idaho; HAWC Collaboration

    2017-01-01

    To increase the effective area and sensitivity of the High Altitude Water Cherenkov Observatory to gamma-ray photons with energies higher than 10 TeV, we are building 350 smaller outrigger tanks around the main array of 300 existing tanks. HAWC detects cascades of charged particles (``extensive air showers'') created by TeV gamma rays hitting the atmosphere. Increasing the size of the array will improve the sensitivity of the array by a factor of 2 to 4 above 10 TeV, allowing for more accurate gamma-ray origin reconstruction and energy estimation. Building the outrigger array requires carefully calibrated equipment, including PMTs and high voltage signal cables of the correct length. Origin reconstruction relies on precise signal timing, so the signal cables' lengths were standardized so that the signal transit time varied by less than 5 ns. Energy estimation depends on accurate photon counts from each tank, so the PMTs were calibrated with a laser and filter wheels to give the PMTs a known amount of light.

  1. Bathythermal habitat use by strains of Great Lakes- and Finger Lakes-origin lake trout in Lake Huron after a change in prey fish abundance and composition

    USGS Publications Warehouse

    Bergstedt, Roger A.; Argyle, Ray L.; Krueger, Charles C.; Taylor, William W.

    2012-01-01

    A study conducted in Lake Huron during October 1998–June 2001 found that strains of Great Lakes-origin (GLO) lake trout Salvelinus namaycush occupied significantly higher temperatures than did Finger Lakes-origin (FLO; New York) lake trout based on data from archival (or data storage) telemetry tags that recorded only temperature. During 2002 and 2003, we implanted archival tags that recorded depth as well as temperature in GLO and FLO lake trout in Lake Huron. Data subsequently recorded by those tags spanned 2002–2005. Based on those data, we examined whether temperatures and depths occupied by GLO and FLO lake trout differed during 2002–2005. Temperatures occupied during those years were also compared with occupied temperatures reported for 1998–2001, before a substantial decline in prey fish biomass. Temperatures occupied by GLO lake trout were again significantly higher than those occupied by FLO lake trout. This result supports the conclusion of the previous study. The GLO lake trout also occupied significantly shallower depths than FLO lake trout. In 2002–2005, both GLO and FLO lake trout occupied significantly lower temperatures than they did in 1998–2001. Aside from the sharp decline in prey fish biomass between study periods, the formerly abundant pelagic alewife Alosa pseudoharengus virtually disappeared and the demersal round goby Neogobius melanostomus invaded the lake and became locally abundant. The lower temperatures occupied by lake trout in Lake Huron during 2002–2005 may be attributable to changes in the composition of the prey fish community, food scarcity (i.e., a retreat to cooler water could increase conversion efficiency), or both.

  2. Recent results from the Pierre Auger Observatory

    SciTech Connect

    Gascón, Alberto; Collaboration: Pierre Auger Collaboration

    2014-07-23

    The Pierre Auger Observatory has been designed to investigate the origin and nature of Ultra High Energy Cosmic Rays (UHECR) using a hybrid detection technique. In this contribution we present some of the most recent results of the observatory, namely the upper-end of the spectrum of cosmic rays, state-of-the-art analyses on mass composition, the measurements of the proton-air cross-section, and the number of muons at ground.

  3. Recent results from the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Gascón, Alberto; Pierre Auger Collaboration

    2014-07-01

    The Pierre Auger Observatory has been designed to investigate the origin and nature of Ultra High Energy Cosmic Rays (UHECR) using a hybrid detection technique. In this contribution we present some of the most recent results of the observatory, namely the upper-end of the spectrum of cosmic rays, state-of-the-art analyses on mass composition, the measurements of the proton-air cross-section, and the number of muons at ground.

  4. Great Comets

    NASA Astrophysics Data System (ADS)

    Burnham, Robert

    2000-05-01

    Spectacular and mysterious objects that come and go in the night sky, comets have dwelt in our popular culture for untold ages. As remnants from the formation of the Solar system, they are objects of key scientific research and space missions. As one of nature's most potent and dramatic dangers, they pose a threat to our safety--and yet they were the origin of our oceans and perhaps even life itself. This beautifully illustrated book tells the story of the biggest and most awe-inspiring of all comets: those that have earned the title "Great." Robert Burnham focuses on the Great comets Hyakutake in 1996 and Hale-Bopp in 1997, which gripped attention worldwide because, for many, they were the first comets ever seen. He places these two recent comets in the context of their predecessors from past ages, among them the famous Comet Halley. Great Comets explains the exciting new discoveries that have come from these magnificent objects and profiles the spaceprobes to comets due for launch in the next few years. The book even takes a peek behind Hollywood's science-fiction fantasies to assess the real risks humanity faces from potential impacts of both comets and asteroids. For everyone interested in astronomy, this exciting book reveals the secrets of the Great Comets and provides essential tools for keeping up to date with comet discoveries in the future. Robert Burnham has been an amateur astronomer since the mid-1950s. He has been a senior editor of Astronomy magazine (1986-88) and is the author of many books and CD-ROMS, including Comet Hale-Bopp: Find and Enjoy the Great Comet and Comet Explorer.

  5. Overview of the Chandra X-Ray Observatory Facility

    NASA Technical Reports Server (NTRS)

    Weisskopf, M. C.; Six, N. Frank (Technical Monitor)

    2002-01-01

    The Chandra X-Ray Observatory (originally called the Advanced X-Ray Astrophysics Facility - AXAF) is the X-Ray component of NASA's "Great Observatory" Program. Chandra is a NASA facility that provides scientific data to the international astronomical community in response to scientific proposals for its use. The Observatory is the product of the efforts of many organizations in the United States and Europe. The Great Observatories also include the Hubble Space Telescope for space-based observations of astronomical objects primarily in the visible portion of the electromagnetic spectrum, the now defunct Compton Gamma- Ray Observatory that was designed to observe gamma-ray emission from astronomical objects, and the soon-to-be-launched Space Infrared Telescope Facility (SIRTF). The Chandra X-Ray Observatory (hereafter CXO) is sensitive to X-rays in the energy range from below 0.1 to above 10.0 keV corresponding to wavelengths from 12 to 0.12 nanometers. The relationship among the various parts of the electromagnetic spectrum, sorted by characteristic temperature and the corresponding wavelength, is illustrated. The German physicist Wilhelm Roentgen discovered what he thought was a new form of radiation in 1895. He called it X-radiation to summarize its properties. The radiation had the ability to pass through many materials that easily absorb visible light and to free electrons from atoms. We now know that X-rays are nothing more than light (electromagnetic radiation) but at high energies. Light has been given many names: radio waves, microwaves, infrared, visible, ultraviolet, X-ray and gamma radiation are all different forms. Radio waves are composed of low energy particles of light (photons). Optical photons - the only photons perceived by the human eye - are a million times more energetic than the typical radio photon, whereas the energies of X-ray photons range from hundreds to thousands of times higher than that of optical photons. Very low temperature systems

  6. The observatories and instruments of Tycho Brahe

    NASA Astrophysics Data System (ADS)

    Wolfschmidt, Gudrun

    Tycho Brahe (1546-1601) was the most important observational astronomer until the invention of the telescope in 1608. By construction new instruments and devising new observing methods, Tycho succeeded in significantly increasing measurement accuracy: He increased the size of his instruments (e.g. a large wooden quadrant of diameter 5.4 m and a mural quadrant); he used metal and masonry rather than wood; he modified construction techniques to achieve greater stability; to provide shelter from the wind, his instruments were in subterranean nooks; his instruments were permanently and solidly mounted; for better angular readings, he developed new subdivisions and diopters (Tycho used transversals to obtain the greatest possible angular resolution readings. His instrumental sights (diopters) were specially designed to minimize errors); he carefully analysed all the errors (Tycho's aim was to reduce thethe uncertainty to less than one minute of arc); he used fundamental stars for the first time; he preferred measuring equatorial coordinates directly instead of using the zodiacal system, i.e. using the equatorial armillary sphere instead of the zodiacal armillary sphere; he tried a new measuring method with clocks and his mural quadrant (1582) for determining the right ascension; he took atmospheric refraction into account. Most of his high-accuracy instruments have been distroyed. Only two sextants, made by Jost Bürgi and Erasmus Habermel around 1600, still exist in the Narodny Technicky Muzeum (NTM) [National Technical Museum] in Prague. A model of the wooden quadrant is in the old observatory in Copenhagen, in the round tower. But we have good descriptions of the instruments (half circles of 2.3 m radius, quadrants up to 2 m radius including the mural quadrant, sextants up to 1.6 m, armillary spheres of 1.5 m radius and the great equatorial armillary sphere of 2.7 m, triquetrum and celestial globe of 1.5 m) in Tycho's book Astronomiae instauratae mechanica

  7. The Origin of Carbon-bearing Volatiles in Surprise Valley Hot Springs in the Great Basin: Carbon Isotope and Water Chemistry Characterizations

    NASA Technical Reports Server (NTRS)

    Fu, Qi; Socki, Richard A.; Niles, Paul B.; Romanek, Christopher; Datta, Saugata; Darnell, Mike; Bissada, Adry K.

    2013-01-01

    There are numerous hydrothermal fields within the Great Basin of North America, some of which have been exploited for geothermal resources. With methane and other carbon-bearing compounds being observed, in some cases with high concentrations, however, their origins and formation conditions remain unknown. Thus, studying hydrothermal springs in this area provides us an opportunity to expand our knowledge of subsurface (bio)chemical processes that generate organic compounds in hydrothermal systems, and aid in future development and exploration of potential energy resources as well. While isotope measurement has long been used for recognition of their origins, there are several secondary processes that may generate variations in isotopic compositions: oxidation, re-equilibration of methane and other alkanes with CO2, mixing with compounds of other sources, etc. Therefore, in addition to isotopic analysis, other evidence, including water chemistry and rock compositions, are necessary to identify volatile compounds of different sources. Surprise Valley Hot Springs (SVHS, 41 deg 32'N, 120 deg 5'W), located in a typical basin and range province valley in northeastern California, is a terrestrial hydrothermal spring system of the Great Basin. Previous geophysical studies indicated the presence of clay-rich volcanic and sedimentary rocks of Tertiary age beneath the lava flows in late Tertiary and Quaternary. Water and gas samples were collected for a variety of chemical and isotope composition analyses, including in-situ pH, alkalinity, conductivity, oxidation reduction potential (ORP), major and trace elements, and C and H isotope measurements. Fluids issuing from SVHS can be classified as Na-(Cl)-SO4 type, with the major cation and anion being Na+ and SO4(2-), respectively. Thermodynamic calculation using ORP and major element data indicated that sulfate is the most dominant sulfur species, which is consistent with anion analysis results. Aquifer temperatures at depth

  8. The Origin of Carbon-bearing Volatiles in Surprise Valley Hot Springs in the Great Basin: Carbon Isotope aud Water Chemistry Characterizations

    NASA Technical Reports Server (NTRS)

    Fu, Qi; Socki, Richard A.; Niles, Paul B.; Romanek, Christopher; Datta, Saugata; Darnell, Mike; Bissada, Adry K.

    2013-01-01

    There are numerous hydrothermal fields within the Great Basin of North America, some of which have been exploited for geothermal resources. With methane and other carbon-bearing compounds being observed, in some cases with high concentrations, however, their origins and formation conditions remain unknown. Thus, studying hydrothermal springs in this area provides us an opportunity to expand our knowledge of subsurface (bio)chemical processes that generate organic compounds in hydrothermal systems, and aid in future development and exploration of potential energy resources as well. While isotope measurement has long been used for recognition of their origins, there are several secondary processes that may generate variations in isotopic compositions: oxidation, re-equilibration of methane and other alkanes with CO2, mixing with compounds of other sources, etc. Therefore, in addition to isotopic analysis, other evidence, including water chemistry and rock compositions, are necessary to identify volatile compounds of different sources. Surprise Valley Hot Springs (SVHS, 41º32'N, 120º5'W), located in a typical basin and range province valley in northeastern California, is a terrestrial hydrothermal spring system of the Great Basin. Previous geophysical studies indicated the presence of clay-rich volcanic and sedimentary rocks of Tertiary age beneath the lava flows in late Tertiary and Quaternary. Water and gas samples were collected for a variety of chemical and isotope composition analyses, including in-situ pH, alkalinity, conductivity, oxidation reduction potential (ORP), major and trace elements, and C and H isotope measurements. Fluids issuing from SVHS can be classified as Na-(Cl)-SO4 type, with the major cation and anion being Na+ and SO4 2-, respectively. Thermodynamic calculation using ORP and major element data indicated that sulfate is the most dominant sulfur species, which is consistent with anion analysis results. Aquifer temperatures at depth estimated

  9. The Little Thompson Observatory

    NASA Astrophysics Data System (ADS)

    Schweitzer, A.; Melsheimer, T.; Rideout, C.; Vanlew, K.

    1998-12-01

    The Little Thompson Observatory is believed to be the first observatory built as part of a high school and accessible to other schools remotely, via the Internet. This observatory is the second member of the Telescopes in Education (TIE) project. Construction is nearly completed and first light is planned for fall 1998. The observatory is located on the grounds of Berthoud High School in northern Colorado. Local schools and youth organizations will have prioritized access to the telescope, and there will also be opportunities for public viewing. After midnight, the telescope will be open to world-wide use by schools via the Internet following the model of the first TIE observatory, the 24" telescope on Mt. Wilson. That telescope has been in use for the past four years by up to 50 schools per month. Students remotely connect to the observatory over the Internet, and then receive the images on their local computers. The observatory grew out of grassroots support from the local community surrounding Berthoud, Colorado, a town of 3,500 residents. TIE has provided the observatory with a Tinsley 18" Cassegrain telescope on a 10-year loan. The facility has been built with tremendous support from volunteers and the local school district. We have applied for an IDEAS grant to provide teacher training workshops which will allow K-12 schools in northern Colorado to make use of the Little Thompson Observatory, including remote observing from classrooms.

  10. The Little Thompson Observatory

    NASA Astrophysics Data System (ADS)

    Schweitzer, A.; Melsheimer, T.; Sackett, C.

    1999-05-01

    The Little Thompson Observatory is believed to be the first observatory built as part of a high school and accessible to other schools remotely, via the Internet. This observatory is the second member of the Telescopes in Education (TIE) project. Construction of the building and dome has been completed, and first light is planned for spring 1999. The observatory is located on the grounds of Berthoud High School in northern Colorado. Local schools and youth organizations will have prioritized access to the telescope, and there will also be opportunities for public viewing. After midnight, the telescope will be open to world-wide use by schools via the Internet following the model of the first TIE observatory, the 24" telescope on Mt. Wilson. Students remotely connect to the observatory over the Internet, and then receive the images on their local computers. The observatory grew out of grassroots support from the local community surrounding Berthoud, Colorado, a town of 3,500 residents. TIE has provided the observatory with a Tinsley 18" Cassegrain telescope on a 10-year loan. The facility has been built with tremendous support from volunteers and the local school district. We have received an IDEAS grant to provide teacher training workshops which will allow K-12 schools in northern Colorado to make use of the Little Thompson Observatory, including remote observing from classrooms.

  11. Royal Observatory, Edinburgh

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Royal Observatory, Edinburgh (ROE) comprises the UK Astronomy Technology Centre (ATC) of the PARTICLE PHYSICS AND ASTRONOMY RESEARCH COUNCIL, and the University of Edinburgh's Institute for Astronomy....

  12. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1982-01-01

    This artist's concept depicts the High Energy Astronomy Observatory (HEAO)-2 in orbit. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978. The HEAO-2 was originally identified as HEAO-B but the designation was changed once the spacecraft achieved orbit.

  13. The MicroObservatory Net

    NASA Astrophysics Data System (ADS)

    Brecher, K.; Sadler, P.

    1994-12-01

    A group of scientists, engineers and educators based at the Harvard-Smithsonian Center for Astrophysics (CfA) has developed a prototype of a small, inexpensive and fully integrated automated astronomical telescope and image processing system. The project team is now building five second generation instruments. The MicroObservatory has been designed to be used for classroom instruction by teachers as well as for original scientific research projects by students. Probably in no other area of frontier science is it possible for a broad spectrum of students (not just the gifted) to have access to state-of-the-art technologies that would allow for original research. The MicroObservatory combines the imaging power of a cooled CCD, with a self contained and weatherized reflecting optical telescope and mount. A microcomputer points the telescope and processes the captured images. The MicroObservatory has also been designed to be used as a valuable new capture and display device for real time astronomical imaging in planetariums and science museums. When the new instruments are completed in the next few months, they will be tried with high school students and teachers, as well as with museum groups. We are now planning to make the MicroObservatories available to students, teachers and other individual users over the Internet. We plan to allow the telescope to be controlled in real time or in batch mode, from a Macintosh or PC compatible computer. In the real-time mode, we hope to give individual access to all of the telescope control functions without the need for an "on-site" operator. Users would sign up for a specific period of time. In the batch mode, users would submit jobs for the telescope. After the MicroObservatory completed a specific job, the images would be e-mailed back to the user. At present, we are interested in gaining answers to the following questions: (1) What are the best approaches to scheduling real-time observations? (2) What criteria should be used

  14. 150 years of magnetic observatories: Recent researches on world data

    NASA Astrophysics Data System (ADS)

    Barraclough, D. R.; Clark, T. D. G.; Cowley, S. W. H.; Hibberd, F. H.; Hide, R.; Kerridge, D. J.; Lowes, F. J.; Malin, S. R. C.; Murphy, T.; Rishbeth, H.; Runcorn, S. K.; Soffel, H. C.; Stewart, D. N.; Stuart, W. F.; Whaler, K. A.; Winch, D. E.

    1992-01-01

    A joint Discussion Meeting of the Royal Astronomical Society and the Royal Irish Academy, held on January 11th, 1991, commemorated the establishment of some early magnetic observatories, discussed recent research using global geomagnetic data and described the present status of magnetic observatories in the United Kingdom. The observatory and instruments at the Dublin magnetic observatory; the origins of the Greenwich magnetic observatory, and why it eventually had to be resited; and the history of the Munich magnetic observatory formed the historical part of the proceedings. Current research topics discussed were the geomagnetic secular variation and deep Earth structure and dynamics; fluid flow patterns near the top of the core; the origin of the annual variation of the geomagnetic field; results of an analysis of monthly means from some British observatories; a new theory of the geomagnetic daily variation; and the interactions between ionospheric science and geomagnetism. The present-day observatory scene was described in terms of the information that can be derived from the almost 40 year series of data from Hartland magnetic observatory; of the methods used to process data from the three UK magnetic observatories, which nowadays are operated automatically and remotely; and (a look into the future) of a new project, INTERMAGNET, which aims to make available, in near real time, data from the world-wide network of magnetic observatories.

  15. Carter National Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Carter National Observatory is situated in the Botanic Gardens in Wellington, New Zealand. Opened in 1941, the observatory is equipped with a 41 cm Boller and Chivens, an historic 23 cm Cooke photo-visual refractor and a 36 seat Zeiss planetarium. The staff are involved in research, school and tertiary education programs....

  16. Svetloe Radio Astronomical Observatory

    NASA Technical Reports Server (NTRS)

    Smolentsev, Sergey; Rahimov, Ismail

    2013-01-01

    This report summarizes information about the Svetloe Radio Astronomical Observatory activities in 2012. Last year, a number of changes took place in the observatory to improve some technical characteristics and to upgrade some units to their required status. The report provides an overview of current geodetic VLBI activities and gives an outlook for the future.

  17. Zelenchukskaya Radio Astronomical Observatory

    NASA Technical Reports Server (NTRS)

    Smolentsev, Sergey; Dyakov, Andrei

    2013-01-01

    This report summarizes information about Zelenchukskaya Radio Astronomical Observatory activities in 2012. Last year a number of changes took place in the observatory to improve some technical characteristics and to upgrade some units to the required status. The report provides an overview of current geodetic VLBI activities and gives an outlook for the future.

  18. INTERMAGNET and magnetic observatories

    USGS Publications Warehouse

    Love, Jeffrey J.; Chulliat, Arnaud

    2012-01-01

    A magnetic observatory is a specially designed ground-based facility that supports time-series measurement of the Earth’s magnetic field. Observatory data record a superposition of time-dependent signals related to a fantastic diversity of physical processes in the Earth’s core, mantle, lithosphere, ocean, ionosphere, magnetosphere, and, even, the Sun and solar wind.

  19. The Space Telescope Observatory

    NASA Technical Reports Server (NTRS)

    Bahcall, J. N.; Odell, C. R.

    1979-01-01

    A convenient guide to the expected characteristics of the Space Telescope Observatory for astronomers and physicists is presented. An attempt is made to provide enough detail so that a professional scientist, observer or theorist, can plan how the observatory may be used to further his observing programs or to test theoretical models.

  20. Beijing Ancient Observatory

    NASA Astrophysics Data System (ADS)

    Shi, Yunli

    The Beijing Ancient Observatory is now the only complete example of an observatory from the seventeenth century in the world. It is a monument to the prosperity of astronomy in traditional China. Its instruments are emblems of the encounter and amalgamation of Chinese and European Science in the seventeenth and eighteenth centuries.

  1. The Norwegian Naval Observatories

    NASA Astrophysics Data System (ADS)

    Pettersen, Bjørn Ragnvald

    2007-07-01

    Archival material has revealed milestones and new details in the history of the Norwegian Naval Observatories. We have identified several of the instrument types used at different epochs. Observational results have been extracted from handwritten sources and an extensive literature search. These allow determination of an approximate location of the first naval observatory building (1842) at Fredriksvern. No physical remains exist today. A second observatory was established in 1854 at the new main naval base at Horten. Its location is evident on military maps and photographs. We describe its development until the Naval Observatory buildings, including archives and instruments, were completely demolished during an allied air bomb raid on 23 February 1945. The first director, C.T.H. Geelmuyden, maintained scientific standards at the the Observatory between 1842 and 1870, and collaborated with university astronomers to investigate, develop, and employ time-transfer by telegraphy. Their purpose was accurate longitude determination between observatories in Norway and abroad. The Naval Observatory issued telegraphic time signals twice weekly to a national network of sites, and as such served as the first national time-service in Norway. Later the Naval Observatory focused on the particular needs of the Navy and developed into an internal navigational service.

  2. Orbiting Carbon Observatory Briefing

    NASA Image and Video Library

    2009-01-29

    Anna Michalak, an Orbiting Carbon Observatory science team member from the University of Michigan, Ann Arbor, speaks during a media briefing to discuss the upcoming Orbiting Carbon Observatory mission, the first NASA spacecraft dedicated to studying carbon dioxide, Thursday, Jan. 29, 2009, at NASA Headquarters in Washington. Photo Credit: (NASA/Paul E. Alers)

  3. Latest results from the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Lhenry-Yvon, Isabelle

    2016-07-01

    The Pierre Auger Observatory has been designed to investigate the origin and nature of Ultra High Energy Cosmic Rays (UHECR) with energies from 1017 to 1020 eV. In this paper we will review some of the most recent results obtained from data of the Pierre Auger Observatory, namely the spectrum of cosmic rays, the anisotropies in arrival directions and the studies related to mass composition and to the number of muons measured at the ground. We will also discuss the implication of these results for assembling a consistent description of the composition, origin and propagation of cosmic rays.

  4. The Millennium Run Observatory: first light

    NASA Astrophysics Data System (ADS)

    Overzier, R.; Lemson, G.; Angulo, R. E.; Bertin, E.; Blaizot, J.; Henriques, B. M. B.; Marleau, G.-D.; White, S. D. M.

    2013-01-01

    Simulations of galaxy evolution aim to capture our current understanding as well as to make predictions for testing by future experiments. Simulations and observations are often compared in an indirect fashion: physical quantities are estimated from the observational data and compared to models. However, many applications can benefit from a more direct approach, where the observing process is also simulated, so that the models are seen fully from the observer's perspective. To facilitate this, we have developed the Millennium Run Observatory (MRObs), a theoretical virtual observatory which uses virtual telescopes to `observe' semi-analytic galaxy formation simulations based on the suite of Millennium Run (MR) dark matter simulations. The MRObs produces data that can be processed and analysed using the standard observational software packages developed for real observations. At present, we produce images in 40 filters covering the rest-frame ultraviolet to infrared for two stellar population synthesis models, for three different models of absorption by the intergalactic medium, and in two cosmologies (Wilkinson Microwave Anisotropy Probe year 1 and 7). Galaxy distributions for a large number of mock light cones can be `observed' using models of major ground- and space-based telescopes. The data include light cone catalogues linked to structural properties of galaxies, pre-observation model images, mock telescope images and Source Extractor products that can all be traced back to the higher level dark matter, semi-analytic galaxy and light cone catalogues available in the MR data base. Here, we describe our methods and announce a first public release of simulated observations that emulate a large number of extragalactic surveys [e.g. Sloan Digital Sky Survey, Canada-France-Hawaii Telescope Legacy Survey (CFHT-LS), Great Observatories Origins Deep Survey (GOODS), GOODS/Early Release Science (ERS), Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (CANDELS

  5. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1977-01-01

    This photograph is of the High Energy Astronomy Observatory (HEAO)-2 telescope being evaluated by engineers in the clean room of the X-Ray Calibration Facility at the Marshall Space Flight Center (MSFC). The MSFC was heavily engaged in the technical and scientific aspects, testing and calibration, of the HEAO-2 telescope The HEAO-2 was the first imaging and largest x-ray telescope built to date. The X-Ray Calibration Facility was built in 1976 for testing MSFC's HEAO-2. The facility is the world's largest, most advanced laboratory for simulating x-ray emissions from distant celestial objects. It produced a space-like environment in which components related to x-ray telescope imaging are tested and the quality of their performance in space is predicted. The original facility contained a 1,000-foot long by 3-foot diameter vacuum tube (for the x-ray path) cornecting an x-ray generator and an instrument test chamber. Recently, the facility was upgraded to evaluate the optical elements of NASA's Hubble Space Telescope, Chandra X-Ray Observatory and Compton Gamma-Ray Observatory.

  6. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1975-07-01

    This illustration is a schematic of the High Energy Astronomy Observatory (HEAO)-2 and its experiments. It shows the focal plane instruments (at the right) plus the associated electronics for operating the telescope as it transmitted its observations to the ground. A fifth instrument, the Monitor Proportional Counter, is located near the front of the telescope. Four separate astronomical instruments are located at the focus of this telescope and they could be interchanged for different types of observations as the observatory pointed at interesting areas of the Sky. Two of these instruments produced images; a High Resolution Imaging Detector and an Imaging Proportional Counter. The other two instruments, the Solid State Spectrometer and the Crystal Spectrometer, measured the spectra of x-ray objects. A fifth instrument, the Monitor Proportional Counter, continuously viewed space independently to study a wider band of x-ray wavelengths and to examine the rapid time variations in the sources. The HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978. The HEAO-2 was originally identified as HEAO-B but the designation was changed once the spacecraft achieved orbit.

  7. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1977-06-01

    This photograph is of the High Energy Astronomy Observatory (HEAO)-2 telescope being checked by engineers in the X-Ray Calibration Facility at the Marshall Space Flight Center (MSFC). The MSFC was heavily engaged in the technical and scientific aspects, testing and calibration, of the HEAO-2 telescope. The HEAO-2 was the first imaging and largest x-ray telescope built to date. The X-Ray Calibration Facility was built in 1976 for testing MSFC's HEAO-2. The facility is the world's largest, most advanced laboratory for simulating x-ray emissions from distant celestial objects. It produced a space-like environment in which components related to x-ray telescope imaging are tested and the quality of their performance in space is predicted. The original facility contained a 1,000-foot long by 3-foot diameter vacuum tube (for the x-ray path) cornecting an x-ray generator and an instrument test chamber. Recently, the facility was upgraded to evaluate the optical elements of NASA's Hubble Space Telescope, Chandra X-Ray Observatory and Compton Gamma-Ray Observatory.

  8. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1978-01-01

    This photograph was taken during the assembly of the High Energy Astronomy Observatory (HEAO)-2 at TRW, Inc., the prime contractor for the HEAOs. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. TRW, Inc. designed and developed the HEAO, under the project management of the Marshall Space Flight Center. The HEAO-2 was originally identified as HEAO-B but the designation was changed once the spacecraft achieved orbit.

  9. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-09-20

    This Atlas/Centaur launch vehicle, carrying the High Energy Astronomy Observatory (HEAO)-3, lifted off on September 20, 1979. The HEAO-3's mission was to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit.

  10. The Virtual Observatory: I

    NASA Astrophysics Data System (ADS)

    Hanisch, R. J.

    2014-11-01

    The concept of the Virtual Observatory arose more-or-less simultaneously in the United States and Europe circa 2000. Ten pages of Astronomy and Astrophysics in the New Millennium: Panel Reports (National Academy Press, Washington, 2001), that is, the detailed recommendations of the Panel on Theory, Computation, and Data Exploration of the 2000 Decadal Survey in Astronomy, are dedicated to describing the motivation for, scientific value of, and major components required in implementing the National Virtual Observatory. European initiatives included the Astrophysical Virtual Observatory at the European Southern Observatory, the AstroGrid project in the United Kingdom, and the Euro-VO (sponsored by the European Union). Organizational/conceptual meetings were held in the US at the California Institute of Technology (Virtual Observatories of the Future, June 13-16, 2000) and at ESO Headquarters in Garching, Germany (Mining the Sky, July 31-August 4, 2000; Toward an International Virtual Observatory, June 10-14, 2002). The nascent US, UK, and European VO projects formed the International Virtual Observatory Alliance (IVOA) at the June 2002 meeting in Garching, with yours truly as the first chair. The IVOA has grown to a membership of twenty-one national projects and programs on six continents, and has developed a broad suite of data access protocols and standards that have been widely implemented. Astronomers can now discover, access, and compare data from hundreds of telescopes and facilities, hosted at hundreds of organizations worldwide, stored in thousands of databases, all with a single query.

  11. The Little Thompson Observatory

    NASA Astrophysics Data System (ADS)

    Schweitzer, A. E.; VanLew, K.; Melsheimer, T.; Sackett, C.

    1999-12-01

    The Little Thompson Observatory is the second member of the Telescopes in Education (TIE) project. Construction of the dome and the remote control system has been completed, and the telescope is now on-line and operational over the Internet. The observatory is located on the grounds of Berthoud High School in northern Colorado. Local schools and youth organizations have prioritized access to the telescope, and there are monthly opportunities for public viewing. In the future, the telescope will be open after midnight to world-wide use by schools following the model of the first TIE observatory, the 24" telescope on Mt. Wilson. Students remotely connect to the observatory over the Internet, and then receive the images on their local computers. The observatory grew out of grassroots support from the local community surrounding Berthoud, Colorado, a town of 3,500 residents. TIE has provided the observatory with a Tinsley 18" Cassegrain telescope on a 10-year loan. The facility has been built with tremendous support from volunteers and the local school district. With funding from an IDEAS grant, we have begun teacher training workshops which will allow K-12 schools in northern Colorado to make use of the Little Thompson Observatory, including remote observing from classrooms.

  12. Light Phenomena over the ESO Observatories II: Red Sprites

    NASA Astrophysics Data System (ADS)

    Horálek, P.; Christensen, L. L.; Bór, J.; Setvák, M.

    2016-03-01

    A rare atmospheric phenomenon, known as red sprites, was observed and captured on camera from the La Silla Observatory. This event signalled the first time that these extremely short-lived flashes of red light, originating in the Earth’s upper atmosphere, were photographed from a major astronomical observatory. Further images of red sprites from the La Silla Paranal Observatory sites are presented and the nature of red sprites is discussed.

  13. Using Robotic Operating System (ROS) to control autonomous observatories

    NASA Astrophysics Data System (ADS)

    Vilardell, Francesc; Artigues, Gabriel; Sanz, Josep; García-Piquer, Álvaro; Colomé, Josep; Ribas, Ignasi

    2016-07-01

    Astronomical observatories are complex systems requiring the integration of numerous devices into a common platform. We are presenting here the firsts steps to integrate the popular Robotic Operating System (ROS) into the control of a fully autonomous observatory. The observatory is also equipped with a decision-making procedure that can automatically react to a changing environment (like weather events). The results obtained so far have shown that the automation of a small observatory can be greatly simplified when using ROS, as well as robust, with the implementation of our decision-making algorithms.

  14. Transient Astrophysics Observatory (TAO)

    NASA Astrophysics Data System (ADS)

    Racusin, J. L.; TAO Team

    2016-10-01

    The Transient Astrophysics Observatory (TAO) is a NASA MidEx mission concept (formerly known as Lobster) designed to provide simultaneous wide-field gamma-ray, X-ray, and near-infrared observations of the sky.

  15. Observatory Improvements for SOFIA

    NASA Technical Reports Server (NTRS)

    Peralta, Robert A.; Jensen, Stephen C.

    2012-01-01

    The Stratospheric Observatory for Infrared Astronomy (SOFIA) is a joint project between NASA and Deutsches Zentrum fuer Luft- und Raumfahrt (DLR), the German Space Agency. SOFIA is based in a Boeing 747 SP and flown in the stratosphere to observe infrared wavelengths unobservable from the ground. In 2007 Dryden Flight Research Center (DFRC) inherited and began work on improving the plane and its telescope. The improvements continue today with upgrading the plane and improving the telescope. The Observatory Verification and Validation (V&V) process is to ensure that the observatory is where the program says it is. The Telescope Status Display (TSD) will provide any information from the on board network to monitors that will display the requested information. In order to assess risks to the program, one must work through the various threats associate with that risk. Once all the risks are closed the program can work towards improving the observatory.

  16. Orbiting Carbon Observatory Briefing

    NASA Image and Video Library

    2009-01-29

    Charles Miller talks during a media briefing to discuss the upcoming Orbiting Carbon Observatory mission, the first NASA spacecraft dedicated to studying carbon dioxide, Thursday, Jan. 29, 2009, at NASA Headquarters in Washington. Photo Credit: (NASA/Paul E. Alers)

  17. Orbiting Carbon Observatory Briefing

    NASA Image and Video Library

    2009-01-29

    Panelists are seen during a media briefing to discuss the upcoming Orbiting Carbon Observatory mission, the first NASA spacecraft dedicated to studying carbon dioxide, Thursday, Jan. 29, 2009, at NASA Headquarters in Washington. Photo Credit: (NASA/Paul E. Alers)

  18. Orbiting Carbon Observatory Briefing

    NASA Image and Video Library

    2009-01-29

    Ralph Basilio talks during a media briefing to discuss the upcoming Orbiting Carbon Observatory mission, the first NASA spacecraft dedicated to studying carbon dioxide, Thursday, Jan. 29, 2009, at NASA Headquarters in Washington. Photo Credit: (NASA/Paul E. Alers)

  19. Orbiting Carbon Observatory Briefing

    NASA Image and Video Library

    2009-01-29

    Eric Ianson speaks during a media briefing to discuss the upcoming Orbiting Carbon Observatory mission, the first NASA spacecraft dedicated to studying carbon dioxide, Thursday, Jan. 29, 2009, at NASA Headquarters in Washington. Photo Credit: (NASA/Paul E. Alers)

  20. Global Health Observatory (GHO)

    MedlinePlus

    ... UNFPA, UNICEF, UN Women, WHO and the World Bank), other UN organizations - including the UN Statistics Division ... data systems Country statistics Regional Health Observatories Africa Americas South-East Asia Europe Eastern Mediterranean Western Pacific ...

  1. History of Chandra X-Ray Observatory

    NASA Image and Video Library

    2000-03-01

    The Chandra X-Ray Observatory has captured this spectacular image of G292.0+1.8, a young, oxygen-rich supernova remnant with a pulsar at its center surrounded by outflowing material. This image shows a rapidly expanding shell of gas that is 36 light-years across and contains large amounts of elements such as oxygen, neon, magnesium, silicon and sulfur. Embedded in this cloud of multimillion-degree gas is a key piece of evidence linking neutron stars and supernovae produced by the collapse of massive stars. With an age estimated at 1,600 years, G292.0+1.8 is one of three known oxygen-rich supernovae in our galaxy. These supernovae are of great interest to astronomers because they are one of the primary sources of the heavy elements necessary to form planets and people. Scattered through the image are bluish knots of emissions containing material that is highly enriched in newly created oxygen, neon, and magnesium produced deep within the original star and ejected by the supernova explosion.

  2. INTEGRATING GEOPHYSICS, GEOLOGY, AND HYDROLOGY TO DETERMINE BEDROCK GEOMETRY CONTROLS ON THE ORIGIN OF ISOLATED MEADOW COMPLEXES WITHIN THE CENTRAL GREAT BASIN, NEVADA

    EPA Science Inventory

    Riparian meadow complexes found in mountain ranges of the Central Great Basin physiographic region (western United States) are of interest to researchers as they contain significant biodiversity relative to the surrounding basin areas. These meadow complexes are currently degradi...

  3. INTEGRATING GEOPHYSICS, GEOLOGY, AND HYDROLOGY TO DETERMINE BEDROCK GEOMETRY CONTROLS ON THE ORIGIN OF ISOLATED MEADOW COMPLEXES WITHIN THE CENTRAL GREAT BASIN, NEVADA

    EPA Science Inventory

    Riparian meadow complexes found in mountain ranges of the Central Great Basin physiographic region (western United States) are of interest to researchers as they contain significant biodiversity relative to the surrounding basin areas. These meadow complexes are currently degradi...

  4. Hawaiian Volcano Observatory

    USGS Publications Warehouse

    Venezky, Dina Y.; Orr, Tim R.

    2008-01-01

    Lava from Kilauea volcano flowing through a forest in the Royal Gardens subdivision, Hawai'i, in February 2008. The Hawaiian Volcano Observatory (HVO) monitors the volcanoes of Hawai'i and is located within Hawaiian Volcanoes National Park. HVO is one of five USGS Volcano Hazards Program observatories that monitor U.S. volcanoes for science and public safety. Learn more about Kilauea and HVO at http://hvo.wr.usgs.gov.

  5. Advancing the Gemini Observatory

    NASA Astrophysics Data System (ADS)

    Hammel, Heidi B.; Levenson, Nancy A.

    2012-11-01

    Gemini Science and User Meeting; San Francisco, California, 17-20 July 2012 More than 100 astronomers gathered in San Francisco to discuss results from the Gemini Observatory and to plan for its future. The Gemini Observatory consists of twin 8.1 meter diameter optical/infrared telescopes located on mountaintops in Hawai'i and Chile. Gemini was built and is operated by an international partnership that currently includes the United States, the United Kingdom, Canada, Chile, Australia, Brazil, and Argentina.

  6. The Pierre Auger Observatory

    SciTech Connect

    Hojvat, C.

    1997-03-01

    The Pierre Auger Observatory is an international collaboration for the detailed study of the highest energy cosmic rays. It will operate at two similar sites, one in the northern hemisphere and one in the southern hemisphere. The Observatory is designed to collect a statistically significant data set of events with energies greater than 10{sup 19} eV and with equal exposures for the northern and southern skies.

  7. Observatories and Telescopes of Modern Times

    NASA Astrophysics Data System (ADS)

    Leverington, David

    2016-11-01

    Preface; Part I. Optical Observatories: 1. Palomar Mountain Observatory; 2. The United States Optical Observatory; 3. From the Next Generation Telescope to Gemini and SOAR; 4. Competing primary mirror designs; 5. Active optics, adaptive optics and other technical innovations; 6. European Northern Observatory and Calar Alto; 7. European Southern Observatory; 8. Mauna Kea Observatory; 9. Australian optical observatories; 10. Mount Hopkins' Whipple Observatory and the MMT; 11. Apache Point Observatory; 12. Carnegie Southern Observatory (Las Campanas); 13. Mount Graham International Optical Observatory; 14. Modern optical interferometers; 15. Solar observatories; Part II. Radio Observatories: 16. Australian radio observatories; 17. Cambridge Mullard Radio Observatory; 18. Jodrell Bank; 19. Early radio observatories away from the Australian-British axis; 20. The American National Radio Astronomy Observatory; 21. Owens Valley and Mauna Kea; 22. Further North and Central American observatories; 23. Further European and Asian radio observatories; 24. ALMA and the South Pole; Name index; Optical observatory and telescope index; Radio observatory and telescope index; General index.

  8. Using Virtual Observatory Tools for Astronomical Research

    NASA Astrophysics Data System (ADS)

    Kim, Sang Chul; Taylor, John D.; Panter, Benjamin; Sohn, Sangmo Tony; Heavens, Alan F.; Mann, Robert G.

    2005-06-01

    Construction of the Virtual Observatory (VO) is a great concern to the astronomical community in the 21st century. We present an outline of the concept and necessity of the VO and the current status of various VO projects including the 15 national ones and the International Virtual Observatory Alliance (IVOA). %, and of Grid project. We summarize the possible science cases that could be solved by using the VO data/tools, real science cases which are the results of using current VO tools, and our own work of using AstroGrid, the United Kingdom national VO, for a research on star formation history of galaxies.

  9. Chicago's Dearborn Observatory: a study in survival

    NASA Astrophysics Data System (ADS)

    Bartky, Ian R.

    2000-12-01

    The Dearborn Observatory, located on the Old University of Chicago campus from 1863 until 1888, was America's most promising astronomical facility when it was founded. Established by the Chicago Astronomical Society and directed by one of the country's most gifted astronomers, it boasted the largest telescope in the world and virtually unlimited operating funds. The Great Chicago Fire of 1871 destroyed its funding and demolished its research programme. Only via the sale of time signals and the heroic efforts of two amateur astronomers did the Dearborn Observatory survive.

  10. A home-built, fully automated observatory

    NASA Astrophysics Data System (ADS)

    Beales, M.

    2010-12-01

    This paper describes the design of an automated observatory making use of off-the-shelf components and software. I make no claims for originality in the design but it has been an interesting and rewarding exercise to get all the components to work together.

  11. Mechanical Overview of the International X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    Robinson, David W.; McClelland, Ryan S.

    2009-01-01

    The International X-ray Observatory (IXO) is a new collaboration between NASA, ESA, and JAXA which is under study for launch in 2020. IXO will be a large 6600 kilogram Great Observatory-class mission which will build upon the legacies of the Chandra and XMM-Newton X-ray observatories. It combines elements from NASA's Constellation-X program and ESA's XEUS program. The observatory will have a 20-25 meter focal length, which necessitates the use of a deployable instrument module. Currently the project is actively trading configurations and layouts of the various instruments and spacecraft components. This paper will provide a snapshot of the latest observatory configuration under consideration and summarize the observatory from the mechanical engineering perspective.

  12. Five Years of Observations with the Chandra X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    Weisskopf, M. C.

    2005-01-01

    The Chandra X-ray Observatory is the X-ray component of NASA's Great Observatory Program. The Chandra X-Ray Observatory has now been operating successfully for over five years. We present here brief overview of the technical performance and some of the remarkable discoveries that have been made.

  13. Creating Griffith Observatory

    NASA Astrophysics Data System (ADS)

    Cook, Anthony

    2013-01-01

    Griffith Observatory has been the iconic symbol of the sky for southern California since it began its public mission on May 15, 1935. While the Observatory is widely known as being the gift of Col. Griffith J. Griffith (1850-1919), the story of how Griffith’s gift became reality involves many of the people better known for other contributions that made Los Angeles area an important center of astrophysics in the 20th century. Griffith began drawing up his plans for an observatory and science museum for the people of Los Angeles after looking at Saturn through the newly completed 60-inch reflector on Mt. Wilson. He realized the social impact that viewing the heavens could have if made freely available, and discussing the idea of a public observatory with Mt. Wilson Observatory’s founder, George Ellery Hale, and Director, Walter Adams. This resulted, in 1916, in a will specifying many of the features of Griffith Observatory, and establishing a committee managed trust fund to build it. Astronomy popularizer Mars Baumgardt convinced the committee at the Zeiss Planetarium projector would be appropriate for Griffith’s project after the planetarium was introduced in Germany in 1923. In 1930, the trust committee judged funds to be sufficient to start work on creating Griffith Observatory, and letters from the Committee requesting help in realizing the project were sent to Hale, Adams, Robert Millikan, and other area experts then engaged in creating the 200-inch telescope eventually destined for Palomar Mountain. A Scientific Advisory Committee, headed by Millikan, recommended that Caltech Physicist Edward Kurth be put in charge of building and exhibit design. Kurth, in turn, sought help from artist Russell Porter. The architecture firm of John C. Austin and Fredrick Ashley was selected to design the project, and they adopted the designs of Porter and Kurth. Philip Fox of the Adler Planetarium was enlisted to manage the completion of the Observatory and become its

  14. The Astronomical Observatory of the University of Coimbra (1772--1799): its Instruments and Scientific Activity

    NASA Astrophysics Data System (ADS)

    Figueiredo, Fernando B.

    2012-09-01

    The establishment of scientific education at the University of Coimbra was one of the most important features of the Reform of the University in 1772. One of the best examples is the creation of the Faculty Mathematics and of the Astronomical Observatory (OAUC) - it was here that Alexandre Gouveia (1731--1808), who would be bishop of Beijing (1785--1808), obtained his degree in Mathematics. The foundation of the OAUC was fundamental in the institutionalization of astronomical science in Portugal, during a period when astronomy, supported by the great theoretical advances of the celestial mechanics and applied mathematics, could finally provide some important solutions to the most prominent scientific problems since Newton (questions about celestial mechanics, navigation, geodesy, etc.). Such questions were also central in the conception and planning of OAUC - the first Portuguese university-based astronomical observatory, although with aspects of a National Observatory. Jose Monteiro da Rocha (1734--1819) was the central personality in the conception, planning and construction of OAUC, as well in its instrument's provision (purchased and assembled throughout the 1780s) and posterior scientific activity. The construction of the OAUC was originally planned for the site of the Castle of the city of Coimbra. In 1775, when only the first floor of the Observatory was built, the construction stopped. However, to fulfill the teaching needs a small provisional Observatory was built inside the courtyard of the University. This provisional Observatory would eventually run for about 15 years! The definitive OAUC was built between the years 1790--99. In this communication we pretend to study the establishment of the OAUC and its primary astronomical collection (a transit instrument, a portable quadrant, a sector, several telescopes, etc.) and how that collection was responsible for the construction plan of the OAUC and the establishment of its Astronomical Ephemeris (1803).

  15. The un-uniform observatories location effect in the Dst index

    NASA Astrophysics Data System (ADS)

    Wu, Y.

    2012-12-01

    The Dst index is a major planetary magnetic activity index proposed by Sugiura in 1964, which is designed to depict the temporal development of the magnetic storm and the intensity of the ring current system flowing in the equatorial plane of the magnetosphere at 3 to 8 Earth radii. It is an hourly index derived from the average value of the horizontal component of the geomagnetic field at four low latitudinal observatories (namely, HER, HON, KAK and SJG). For a long time, the Dst index is greatly doubted. Researchers have pointed out that a great proportion of the Dst index is originated from the Substorm Wedge current system, the Cross-tail current and the Partial ring current system [Turner et al., 2000; Liemohn et al., 2001; Ohtani et al., 2001; Rostoker, 2000; Friedrich et al., 1999; Maltsev, 2003; Huang, 2004; Hakkinen et al., 2002]. The ring current system and its disturbed storm-time field (Dst field) take on an enhanced dawn-dusk asymmetry during disturbed time. Therefore, the influence of the non-uniform location of four observatories of the Dst index will enhance. The purpose of this paper is to study the influence of the observatories' location on the Dst index. The hourly data of the horizontal component of the geomagnetic field in the observatories in geomagnetic latitude between 45°S and -45°N is used, to derive the local-time distribution model of the Dst field by the method of Nature Orthogonal Component and Cubic Polynomial Fitting. Results suggest that the maximum difference to the LT-model with four Dst index stations is about 5% lowness on 16UTmp, 3% highness on 05UTmp, and the minimum difference is around 11UTmp (UTmp corresponds to the universal time of the minimum of the Dst index). It proves some certain extent efficiency afforded by adding observatories in the SYM index.

  16. Everyday astronomy @ Sydney Observatory

    NASA Astrophysics Data System (ADS)

    Parello, S. L.

    2008-06-01

    Catering to a broad range of audiences, including many non-English speaking visitors, Sydney Observatory offers everything from school programmes to public sessions, day care activities to night observing, personal interactions to web-based outreach. With a history of nearly 150 years of watching the heavens, Sydney Observatory is now engaged in sharing the wonder with everybody in traditional and innovative ways. Along with time-honoured tours of the sky through two main telescopes, as well as a small planetarium, Sydney Observatory also boasts a 3D theatre, and offers programmes 363 days a year - rain or shine, day and night. Additionally, our website neversleeps, with a blog, YouTube videos, and night sky watching podcasts. And for good measure, a sprinkling of special events such as the incomparable Festival of the Stars, for which most of northern Sydney turns out their lights. Sydney Observatory is the oldest working observatory in Australia, and we're thrilled to be looking forward to our 150th Anniversary next year in anticipation of the International Year of Astronomy immediately thereafter.

  17. Gamma Ray Observatory (GRO) Prelaunch Mission Operations Report (MOR)

    NASA Technical Reports Server (NTRS)

    1991-01-01

    The NASA Astrophysics Program is an endeavor to understand the origin and fate of the universe, to understand the birth and evolution of the large variety of objects in the universe, from the most benign to the most violent, and to probe the fundamental laws of physics by examining their behavior under extreme physical conditions. These goals are pursued by means of observations across the entire electromagnetic spectrum, and through theoretical interpretation of radiations and fields associated with astrophysical systems. Astrophysics orbital flight programs are structured under one of two operational objectives: (1) the establishment of long duration Great Observatories for viewing the universe in four major wavelength regions of the electromagnetic spectrum (radio/infrared/submillimeter, visible/ultraviolet, X-ray, and gamma ray), and (2) obtaining crucial bridging and supporting measurements via missions with directed objectives of intermediate or small scope conducted within the Explorer and Spacelab programs. Under (1) in this context, the Gamma Ray Observatory (GRO) is one of NASA's four Great Observatories. The other three are the Hubble Space Telescope (HST) for the visible and ultraviolet portion of the spectrum, the Advanced X-ray Astrophysics Facility (AXAF) for the X-ray band, and the Space Infrared Telescope Facility (SIRTF) for infrared wavelengths. GRO's specific mission is to study the sources and astrophysical processes that produce the highest energy electromagnetic radiation from the cosmos. The fundamental physical processes that are known to produce gamma radiation in the universe include nuclear reactions, electron bremsstrahlung, matter-antimatter annihilation, elementary particle production and decay, Compton scattering, synchrotron radiation. GRO will address a variety of questions relevant to understanding the universe, such as: the formation of the elements; the structure and dynamics of the Galaxy; the nature of pulsars; the existence

  18. Arecibo Observatory and the National Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Ojalvo, Isobel

    2006-12-01

    The United States Virtual Observatoryw as established in 2001 to provide worldwide access to data acquired by U.S. observatories, including Arecibo Observatory at the National Astronomy and Ionosphere Center in Puerto Rico. Arecibo's 7-element L-band Feed Array (ALFA) is being used to survey line and continuum radiation over large areas of the 21cm-wavelength sky. Two surveys were the focus of this project: the Galactic interstellar medium HI 21cm line survey (GALFA) and the Arecibo Galaxy Environment HI Survey (AGES). Both surveys are producing large volumes of data in ``cubes'' of intensity as a function of right ascension, declination, and line-of-sight doppler velocity. An essential objective of both GALFA and AGES is to make the data available over the World Wide Web. This will require a user interface that returns the appropriate cube for a given set of coordinates, or computes a new cube on the fly covering a desired coordinate range. To implement this service, computationally efficient processing and serving methods are required. This presentation will discuss the current methods used for remote data access as well as new methods that can be used to analyze data cubes online with web tools. This work has been supported by the Research Experiences for Undergraduates program of the National Science Foundation and by the National Astronomy and Ionosphere Center operated by Cornell University under Cooperative Agreement with the NSF.

  19. Digital Data Preservation and Curation: A Collaboration Among Libraries, Publishers, and the Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Hanisch, R. J.; Steffen, J.; Choudhury, S.; Dilauro, T.; Szalay, A.; Vishniac, E.; Ehling, T.; Milkey, R.; Plante, R.

    2007-10-01

    Astronomers are producing and analyzing data at ever more prodigious rates. NASA's Great Observatories, ground-based national observatories, and major survey projects have archive and data distribution systems in place to manage their standard data products, and these are now interlinked through the protocols and metadata standards agreed upon in the Virtual Observatory. However, the digital data associated with peer-reviewed publications is only rarely archived. Most often, astronomers publish graphical representations of their data but not the data themselves. Other astronomers cannot readily inspect the data to either confirm the interpretation presented in a paper or extend the analysis. Highly processed data sets reside on departmental servers and the personal computers of astronomers, and may or may not be available a few years hence. We are investigating ways to preserve and curate the digital data associated with peer-reviewed journals in astronomy. The technology and standards of the VO provide one component of the necessary technology. A variety of underlying systems can be used to physically host a data repository, and indeed this repository need not be centralized. The repository, however, must be managed and data must be documented through high quality, curated metadata. Multiple access portals must be available: the original journal, the host data center, the Virtual Observatory, or any number of topically-oriented data services utilizing VO-standard access mechanisms.

  20. The Compton Gamma Ray Observatory

    NASA Technical Reports Server (NTRS)

    Gehrels, N.; Chipman, E.; Kniffen, D.

    1994-01-01

    The Arthur Holly Compton Gamma Ray Observatory Compton) is the second in NASA's series of great Observatories. Launched on 1991 April 5, Compton represents a dramatic increase in capability over previous gamma-ray missions. The spacecraft and scientific instruments are all in good health, and many significant discoveries have already been made. We describe the capabilities of the four scientific instruments, and the observing program of the first 2 years of the mission. Examples of early discoveries by Compton are enumerated, including the discovery that gamma-ray bursts are isotropic but spatially inhomogeneous in their distribution; the discovery of a new class of high-energy extragalacatic gamma-ray sources, the gamma-ray AGNs; the discovery of emission from SN 1987A in the nuclear line of Co-57; and the mapping of emission from Al-26 in the interstellar medium (ISM) near the Galactic center. Future observations will include deep surveys of selected regions of the sky, long-tem studies of individual objects, correlative studies of objects at gamma-ray and other energies, a Galactic plane survey at intermediate gamma-ray energies, and improved statistics on gamma-ray bursts to search for small anisotropies. After completion of the all-sky survey, a Guest Investigator program is in progress with guest observers' time share increasing from 30% upward for the late mission phases.

  1. The Compton Gamma Ray Observatory

    NASA Astrophysics Data System (ADS)

    Gehrels, N.; Chipman, E.; Kniffen, D.

    1994-06-01

    The Arthur Holly Compton Gamma Ray Observatory Compton) is the second in NASA's series of great Observatories. Launched on 1991 April 5, Compton represents a dramatic increase in capability over previous gamma-ray missions. The spacecraft and scientific instruments are all in good health, and many significant discoveries have already been made. We describe the capabilities of the four scientific instruments, and the observing program of the first 2 years of the mission. Examples of early discoveries by Compton are enumerated, including the discovery that gamma-ray bursts are isotropic but spatially inhomogeneous in their distribution; the discovery of a new class of high-energy extragalacatic gamma-ray sources, the gamma-ray AGNs; the discovery of emission from SN 1987A in the nuclear line of Co-57; and the mapping of emission from Al-26 in the interstellar medium (ISM) near the Galactic center. Future observations will include deep surveys of selected regions of the sky, long-tem studies of individual objects, correlative studies of objects at gamma-ray and other energies, a Galactic plane survey at intermediate gamma-ray energies, and improved statistics on gamma-ray bursts to search for small anisotropies. After completion of the all-sky survey, a Guest Investigator program is in progress with guest observers' time share increasing from 30% upward for the late mission phases.

  2. Toward a green observatory

    NASA Astrophysics Data System (ADS)

    Weilenmann, Ueli; Ramírez, Christian; Vanderheyden, Pierre

    2010-07-01

    Many of the modern observatories are located at remote sites, far from larger cities and away from infrastructure like power grids, water supplies and roads. On-site power generation in island mode is often the only choice to provide electricity to an observatory. During the 2008 petrol price rally, conventional power generation has received special attention and alternatives are being studied now in many organisations to keep energy prices at bay. This paper shall outline the power generation at the ESO VLT/VLTI observatory at Paranal as it is now and a plan for a possible way out of the dependency on fossil fuels in the near future. A discussion of several alternatives including wind energy, solar energy and heat recovery from a conventional power plant shall be analysed and compared. Finally, a project is being proposed to equip the VLT/VLTI with a modern alternative energy supply, based on a novel concept: Solar cooling.

  3. Iranian National Observatory

    NASA Astrophysics Data System (ADS)

    Khosroshahi, H. G.; Danesh, A.; Molaeinezhad, A.

    2016-09-01

    The Iranian National Observatory is under construction at an altitude of 3600m at Gargash summit 300km southern Tehran. The site selection was concluded in 2007 and the site monitoring activities have begun since then, which indicates a high quality of the site with a median seeing of 0.7 arcsec through the year. One of the major observing facilities of the observatory is a 3.4m Alt-Az Ritchey-Chretien optical telescope which is currently under design. This f/11 telescope will be equipped with high resolution medium-wide field imaging cameras as well as medium and high resolution spectrographs. In this review, I will give an overview of astronomy research and education in Iran. Then I will go through the past and present activities of the Iranian National Observatory project including the site quality, telescope specifications and instrument capabilities.

  4. Wendelstein Observatory control software

    NASA Astrophysics Data System (ADS)

    Snigula, Jan M.; Gössl, Claus; Kodric, Mihael; Riffeser, Arno; Wegner, Michael; Schlichter, Jörg

    2016-07-01

    LMU Munchen operates an astrophysical observatory on Mt. Wendelstein1. The 2m Fraunhofer telescope2, 3 is equipped with a 0.5 x 0.5 square degree field-of-view wide field camera4 and a 3 channel optical/NIR camera5, 6. Two fiber coupled spectrographs7-9 and a wavefront sensor will be added in the near future. The observatory hosts a multitude of supporting hardware, i.e. allsky cameras, webcams, meteostation, air conditioning etc. All scientific hardware can be controlled through a single, central "Master Control Program" (MCP). At the last SPIE astronomy venue we presented the overall Wendelstein Observatory software concept10. Here we explain concept and implementation of the MCP as a multi-threaded Python daemon in the area of conflict between debuggability and Don't Repeat Yourself (DRY).

  5. Swift Observatory Space Simulation Testing

    NASA Technical Reports Server (NTRS)

    Espiritu, Mellina; Choi, Michael K.; Scocik, Christopher S.

    2004-01-01

    The Swift Observatory is a Middle-Class Explorer (MIDEX) mission that is a rapidly re-pointing spacecraft with immediate data distribution capability to the astronomical community. Its primary objectives are to characterize and determine the origin of Gamma Ray Bursts (GRBs) and to use the collected data on GRB phenomena in order to probe the universe and gain insight into the physics of black hole formation and early universe. The main components of the spacecraft are the Burst Alert Telescope (BAT), Ultraviolet and Optical Telescope (UVOT), X-Ray Telescope (XRT), and Optical Bench (OB) instruments coupled with the Swift spacecraft (S/C) bus. The Swift Observatory will be tested at the Space Environment Simulation (SES) chamber at the Goddard Space Flight Center from May to June 2004 in order to characterize its thermal behavior in a vacuum environment. In order to simulate the independent thermal zones required by the BAT, XRT, UVOT, and OB instruments, the spacecraft is mounted on a chariot structure capable of maintaining adiabatic interfaces and enclosed in a modified, four section MSX fixture in order to accommodate the strategic placement of seven cryopanels (on four circuits), four heater panels, and a radiation source burst simulator mechanism. There are additionally 55 heater circuits on the spacecraft. To mitigate possible migration of silicone contaminants from BAT to the XRT and UVOT instruments, a contamination enclosure is to be fabricated around the BAT at the uppermost section of the MSX fixture. This paper discuses the test requirements and implemented thermal vacuum test configuration for the Swift Observatory.

  6. Arecibo Observatory for All

    NASA Astrophysics Data System (ADS)

    Isidro, Gloria M.; Pantoja, C. A.; Bartus, P.; La Rosa, C.

    2006-12-01

    We describe new materials available at Arecibo Observatory for visitors with visual impairments. These materials include a guide in Braille that describes the telescope, some basic terms used in radio astronomy and frequently asked questions. We have also designed a tactile model of the telescope. We are interested that blind visitors can participate of the excitement of the visit to the worlds largest radio telescope. We would like to thank the "Fundacion Comunitaria de Puerto Rico" for the scholarship that allowed GMI to work on this project. We would like to express our gratitude to the Arecibo Observatory/NAIC for their support.

  7. Yellowstone Volcano Observatory

    USGS Publications Warehouse

    Venezky, Dina Y.; Lowenstern, Jacob

    2008-01-01

    Eruption of Yellowstone's Old Faithful Geyser. Yellowstone hosts the world's largest and most diverse collection of natural thermal features, which are the surface expression of magmatic heat at shallow depths in the crust. The Yellowstone system is monitored by the Yellowstone Volcano Observatory (YVO), a partnership among the U.S. Geological Survey (USGS), Yellowstone National Park, and the University of Utah. YVO is one of five USGS Volcano Hazards Program observatories that monitor U.S. volcanoes for science and public safety. Learn more about Yellowstone and YVO at http://volcanoes.usgs.gov/yvo.

  8. The Sudbury Neutrino Observatory

    NASA Astrophysics Data System (ADS)

    Boger, J.; Hahn, R. L.; Rowley, J. K.; Carter, A. L.; Hollebone, B.; Kessler, D.; Blevis, I.; Dalnoki-Veress, F.; DeKok, A.; Farine, J.; Grant, D. R.; Hargrove, C. K.; Laberge, G.; Levine, I.; McFarlane, K.; Mes, H.; Noble, A. T.; Novikov, V. M.; O'Neill, M.; Shatkay, M.; Shewchuk, C.; Sinclair, D.; Clifford, E. T. H.; Deal, R.; Earle, E. D.; Gaudette, E.; Milton, G.; Sur, B.; Bigu, J.; Cowan, J. H. M.; Cluff, D. L.; Hallman, E. D.; Haq, R. U.; Hewett, J.; Hykawy, J. G.; Jonkmans, G.; Michaud, R.; Roberge, A.; Roberts, J.; Saettler, E.; Schwendener, M. H.; Seifert, H.; Sweezey, D.; Tafirout, R.; Virtue, C. J.; Beck, D. N.; Chan, Y. D.; Chen, X.; Dragowsky, M. R.; Dycus, F. W.; Gonzalez, J.; Isaac, M. C. P.; Kajiyama, Y.; Koehler, G. W.; Lesko, K. T.; Moebus, M. C.; Norman, E. B.; Okada, C. E.; Poon, A. W. P.; Purgalis, P.; Schuelke, A.; Smith, A. R.; Stokstad, R. G.; Turner, S.; Zlimen, I.; Anaya, J. M.; Bowles, T. J.; Brice, S. J.; Esch, E.-I.; Fowler, M. M.; Goldschmidt, A.; Hime, A.; McGirt, A. F.; Miller, G. G.; Teasdale, W. A.; Wilhelmy, J. B.; Wouters, J. M.; Anglin, J. D.; Bercovitch, M.; Davidson, W. F.; Storey, R. S.; Biller, S.; Black, R. A.; Boardman, R. J.; Bowler, M. G.; Cameron, J.; Cleveland, B.; Ferraris, A. P.; Doucas, G.; Heron, H.; Howard, C.; Jelley, N. A.; Knox, A. B.; Lay, M.; Locke, W.; Lyon, J.; Majerus, S.; Moorhead, M.; Omori, M.; Tanner, N. W.; Taplin, R. K.; Thorman, M.; Wark, D. L.; West, N.; Barton, J. C.; Trent, P. T.; Kouzes, R.; Lowry, M. M.; Bell, A. L.; Bonvin, E.; Boulay, M.; Dayon, M.; Duncan, F.; Erhardt, L. S.; Evans, H. C.; Ewan, G. T.; Ford, R.; Hallin, A.; Hamer, A.; Hart, P. M.; Harvey, P. J.; Haslip, D.; Hearns, C. A. W.; Heaton, R.; Hepburn, J. D.; Jillings, C. J.; Korpach, E. P.; Lee, H. W.; Leslie, J. R.; Liu, M.-Q.; Mak, H. B.; McDonald, A. B.; MacArthur, J. D.; McLatchie, W.; Moffat, B. A.; Noel, S.; Radcliffe, T. J.; Robertson, B. C.; Skensved, P.; Stevenson, R. L.; Zhu, X.; Gil, S.; Heise, J.; Helmer, R. L.; Komar, R. J.; Nally, C. W.; Ng, H. S.; Waltham, C. E.; Allen, R. C.; Bühler, G.; Chen, H. H.; Aardsma, G.; Andersen, T.; Cameron, K.; Chon, M. C.; Hanson, R. H.; Jagam, P.; Karn, J.; Law, J.; Ollerhead, R. W.; Simpson, J. J.; Tagg, N.; Wang, J.-X.; Alexander, C.; Beier, E. W.; Cook, J. C.; Cowen, D. F.; Frank, E. D.; Frati, W.; Keener, P. T.; Klein, J. R.; Mayers, G.; McDonald, D. S.; Neubauer, M. S.; Newcomer, F. M.; Pearce, R. J.; de Water, R. G. V.; Berg, R. V.; Wittich, P.; Ahmad, Q. R.; Beck, J. M.; Browne, M. C.; Burritt, T. H.; Doe, P. J.; Duba, C. A.; Elliott, S. R.; Franklin, J. E.; Germani, J. V.; Green, P.; Hamian, A. A.; Heeger, K. M.; Howe, M.; Drees, R. M.; Myers, A.; Robertson, R. G. H.; Smith, M. W. E.; Steiger, T. D.; Wechel, T. V.; Wilkerson, J. F.

    2000-07-01

    The Sudbury Neutrino Observatory is a second-generation water Cherenkov detector designed to determine whether the currently observed solar neutrino deficit is a result of neutrino oscillations. The detector is unique in its use of D2O as a detection medium, permitting it to make a solar model-independent test of the neutrino oscillation hypothesis by comparison of the charged- and neutral-current interaction rates. In this paper the physical properties, construction, and preliminary operation of the Sudbury Neutrino Observatory are described. Data and predicted operating parameters are provided whenever possible.

  9. Cascades Volcano Observatory

    USGS Publications Warehouse

    Venezky, Dina Y.; Driedger, Carolyn; Pallister, John

    2008-01-01

    Washington's Mount St. Helens volcano reawakens explosively on October 1, 2004, after 18 years of quiescence. Scientists at the U.S. Geological Survey's Cascades Volcano Observatory (CVO) study and observe Mount St. Helens and other volcanoes of the Cascade Range in Washington, Oregon, and northern California that hold potential for future eruptions. CVO is one of five USGS Volcano Hazards Program observatories that monitor U.S. volcanoes for science and public safety. Learn more about Mount St. Helens and CVO at http://vulcan.wr.usgs.gov/.

  10. WFIRST Observatory Performance

    NASA Technical Reports Server (NTRS)

    Kruk, Jeffrey W.

    2012-01-01

    The WFIRST observatory will be a powerful and flexible wide-field near-infrared facility. The planned surveys will provide data applicable to an enormous variety of astrophysical science. This presentation will provide a description of the observatory and its performance characteristics. This will include a discussion of the point spread function, signal-to-noise budgets for representative observing scenarios and the corresponding limiting sensitivity. Emphasis will be given to providing prospective Guest Observers with information needed to begin thinking about new observing programs.

  11. Long Valley Observatory

    USGS Publications Warehouse

    Venezky, Dina Y.; Hill, David

    2008-01-01

    The ~300-year-old lava on Paoha Island in Mono Lake was produced by the most recent eruption in the Long Valley Caldera area in east-central California. The Long Valley Caldera was formed by a massive volcanic eruption 760,000 years ago. The region is monitored by the Long Valley Observatory (LVO), one of five USGS Volcano Hazards Program observatories that monitor U.S. volcanoes for science and public safety. Learn more about the Long Valley Caldera region and LVO at http://volcanoes.usgs.gov/lvo.

  12. Large Solar Observatory

    NASA Technical Reports Server (NTRS)

    Choudhary, Debi Prasad

    2003-01-01

    This article summarizes the scientific aim, design considerations and observatory site of a large optical solar telescope. The day time "seeing" is better on the islands, surrounded by large body of water, compared to the mountain sites. Therefore, in order to obtain the solar images with sub-arcsec resolution, the observatory site should be preferably located on an island. A list of potential sites on Himalayas and surrounding region is given. A brief description of the telescope design, enclosure and back-end instruments are also presented.

  13. First Light of the Renovated Thacher Observatory

    NASA Astrophysics Data System (ADS)

    O'Neill, Katie; Yin, Yao; Edwards, Nick; Swift, Jonathan

    2017-01-01

    The Thacher Observatory, originally a collaboration between UCLA (P.I. G. Abell), Caltech, Pomona College, and the Thacher School, was built in the early 1960s. The goal of the facility was to serve as a training ground for undergraduate and graduate students in Los Angeles area colleges and also to provide hands-on technical training and experience for Thacher students. It was the birthplace of the Summer Science Program which continues today at other campuses. The observatory has now been fully renovated and modernized with a new, 0.7m telescope and dome that can be controlled remotely and in an automated manner. Science programs involving accurate and precise photometry have been initiated, and we project that we will be presenting the first scientific results of the renovated observatory at this meeting.

  14. High Energy Astronomy Observatory (HEAO)-1

    NASA Technical Reports Server (NTRS)

    1978-01-01

    This drawing is a schematic of the High Energy Astronomy Observatory (HEAO)-1. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit. The HEAO project involved the launching of three unmarned scientific observatories into low Earth orbit between 1977 and 1979 to study some of the most intriguing mysteries of the universe; pulsars, black holes, neutron stars, and super nova. Hardware support for the imaging instruments was provided by American Science and Engineeing. The HEAO spacecraft were built by TRW, Inc. under project management of the Marshall Space Flight Center.

  15. High Energy Astronomy Observatory (HEAO)-1

    NASA Technical Reports Server (NTRS)

    1982-01-01

    This artist's conception depicts the High Energy Astronomy Observatory (HEAO)-1 in orbit. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit. The HEAO project involved the launching of three unmarned scientific observatories into low Earth orbit between 1977 and 1979 to study some of the most intriguing mysteries of the universe; pulsars, black holes, neutron stars, and super nova. Hardware support for the imaging instruments was provided by American Science and Engineeing. The HEAO spacecraft were built by TRW, Inc. under project management of the Marshall Space Flight Center.

  16. The Chandra X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    Weisskopf, Martin C.

    2013-01-01

    The Chandra X-ray Observatory, the third of NASA's four Great Observatories and its flagship mission for X-ray astronomy, was launched by NASA's Space Shuttle Columbia on July 23, 1999. The first X-ray sources were observed on August 12, 1999. The brightest of these sources named Leon X-1 in honor of Chandra's Telescope Scientist who played the leading role in establishing the key to Chandra's great advance in angular resolution. Over the past years, the Observatory's ability to provide sub-arc second X-ray images and high resolution spectra has established it as one of the most versatile and powerful tools for astrophysical research in the 21st century. Chandra explores the high-energy regions of the universe, observing X-ray sources with fluxes ranging over more than 10 orders of magnitude. The longevity of Chandra also provides a long observing baseline enabling temporal studies over time-scales of years. I will discuss how the Observatory works, the current operational status, and scientific highlights covering a variety of objects from stars with nearby planets that impact the stellar activity to the deepest Chandra surveys.

  17. Observatory Sponsoring Astronomical Image Contest

    NASA Astrophysics Data System (ADS)

    2005-05-01

    and to provide a showcase for a broad range of astronomical research and celestial objects," Adams added. In addition, NRAO is developing enhanced data visualization techniques and data-processing recipes to assist radio astronomers in making quality images and in combining radio data with data collected at other wavelengths, such as visible-light or infrared, to make composite images. "We encourage all our telescope users to take advantage of these techniques to showcase their research," said Juan Uson, a member of the NRAO scientific staff and the observatory's EPO scientist. "All these efforts should demonstrate the vital and exciting roles that radio telescopes, radio observers, and the NRAO play in modern astronomy," Lo said. "While we want to encourage images that capture the imagination, we also want to emphasize that extra effort invested in enhanced imagery also will certainly pay off scientifically, by revealing subtleties and details that may have great significance for our understanding of astronomical objects," he added. Details of the NRAO Image Contest, which will become an annual event, are on the observatory's Web site. The observatory will announce winners on October 15. The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.

  18. Torun Radio Astronomy Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    Torun Center for Astronomy is located at Piwnice, 15 km north of Torun, Poland. A part of the Faculty of Physics and Astronomy of the Nicolaus Copernicus University, it was created by the union of Torun Radio Astronomy Observatory (TRAO) and the Institute of Astronomy on 1 January 1997....

  19. Improving Arecibo Observatory's Hardware

    NASA Astrophysics Data System (ADS)

    Van Rooy, Paula; Whitlow, Dana; Seymour, Andrew

    2017-01-01

    The Puerto-rican Ultimate Pulsar Processing Instrument (PUPPI) is a key backend for time-domain observations at Arecibo Observatory. PUPPI enables pulsar timing used for gravitational wave studies, single pulse studies of pulsars, searches for new pulsars, and allows in depth studies of Fast Radio Bursts (FRBs). Unfortunately, PUPPI is presently restricted to only certain Arecibo receivers due to its input frequency and bandwidth requirements. Here we present the design process, building, bench testing, and updates on the implementation of a one-channel breadboard of a new frequency mixer at the Arecibo Observatory. The function of the frequency mixer design is to translate a 1.1-1.9 GHz band to 0.8 - 1.6 GHz band, where PUPPI samples the data at the second Nyquist zone. When this seemingly simple device is fully implemented, it will allow for the further expansion of the abilities of PUPPI. Mainly it will expand PUPPI's frequency agility to higher frequencies from 4 to 10 GHz, by enabling it to work with many more of Arecibo's receivers. We hope this becomes particularly useful, now that a FRB has been detected at these higher frequencies. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Méndez-Universidad Metropolitana, and the Universities Space Research Association. The Arecibo Observatory REU is funded under grant AST-1559849 to Universidad Metropolitana

  20. The IT Observatory.

    ERIC Educational Resources Information Center

    Kent, Kai Iok Tong; Sousa, Antonio C. M.

    1999-01-01

    Describes the IT Observatory, a service of the Macau Productivity and Technology center (CPTTM) that provides information on demand using information technology. The CPTTM is a nonprofit organization funded by the Macau government and private businesses to enhance the productivity of Macau businesses by introducing new technologies and new…

  1. Arecibo Observatory for All

    ERIC Educational Resources Information Center

    Bartus, P.; Isidro, G. M.; La Rosa, C.; Pantoja, C. A.

    2007-01-01

    We describe new materials available at the Arecibo Observatory for visitors with visual impairments. These materials include a guide in Braille that describes the telescope, explains some basic terms used in radio astronomy, and lists frequently asked questions. We have also designed a tactile model of the telescope. Our interest is in enabling…

  2. The Baksan Neutrino Observatory

    NASA Astrophysics Data System (ADS)

    Kuzminov, V. V.

    2012-09-01

    An overall view of the history of the Baksan Neutrino Observatory INR RAS creation is presented. Ground-based and underground facilities used to study cosmic rays, rare nuclear reactions and decays, register solar neutrinos, observe various geophysical phenomena are described. Some main results obtained with these facilities are given.

  3. Armenian Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Mickaelian, A. M.

    2015-07-01

    Vast amount of information continuously accumulated in astronomy requires finding new solutions for its efficient storage, use and dissemination, as well as accomplishing new research projects. Virtual Observatories (VOs) have been created in a number of countries to set up a new environment for these tasks. Based on them, the International Virtual Observatory Alliance (IVOA) was created in 2002, which unifies 19 VO projects, including Armenian Virtual Observatory (ArVO) founded in 2005. ArVO is a project of Byurakan Astrophysical Observatory (BAO) aimed at construction of a modern system for data archiving, extraction, acquisition, reduction, use and publication. ArVO technical and research projects are presented, including the Global Spectroscopic Database, which is being built based on Digitized First Byurakan Survey (DFBS). Quick optical identification of radio, IR or X-ray sources will be possible by plotting their positions in the DFBS or other spectroscopic plate and matching all available data. Accomplishment of new projects by combining data is so important that the International Council of Scientific Unions (ICSU) recently created World Data System (WDS) for unifying data coming from all science areas, and BAO has also joined it.

  4. Trieste Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    Founded in 1866 as the Austrian K. u. K. Maritimes Observatorium, in 1898 the Trieste Astronomical Observatory became an independent institute for research in astronomy. Now it is part of INAF (Istituto Nazionale di Astrofisica) and the Italian council for research in astrophysics. Staff include 20 researchers and 42 technicians and administrators. Research fields are extragalactic, stellar physi...

  5. Strasbourg's "First" astronomical observatory

    NASA Astrophysics Data System (ADS)

    Heck, André

    2011-08-01

    The turret lantern located at the top of the Strasbourg Hospital Gate is generally considered as the first astronomical observatory of the city, but such a qualification must be treated with caution. The thesis of this paper is that the idea of a tower-observatory was brought back by a local scholar, Julius Reichelt (1637-1717), after he made a trip to Northern Europe around 1666 and saw the "Rundetårn" (Round Tower) recently completed in Copenhagen. There, however, a terrace allowed (and still allows) the full viewing of the sky, and especially of the zenith area where the atmospheric transparency is best. However, there is no such terrace in Strasbourg around the Hospital Gate lantern. Reichelt had also visited Johannes Hevelius who was then developing advanced observational astronomy in Gdansk, but nothing of the kind followed in Strasbourg. Rather, the Hospital Gate observatory was built essentially for the prestige of the city and for the notoriety of the university, and the users of this observing post did not make any significant contributions to the progress of astronomical knowledge. We conclude that the Hospital Gate observatory was only used for rudimentary viewing of bright celestial objects or phenomena relatively low on the horizon.

  6. Observatory of Shiraz University

    NASA Astrophysics Data System (ADS)

    Bordbar, G. H.; Bahrani, F.

    2016-12-01

    Here we write about the observatory of Shiraz University, which has the largest active telescope in Iran but now, because of problems like light pollution of the nearby city and exhaustion of its largest telescope we need a plan for modernization and automatization in a new place.

  7. Arecibo Observatory for All

    ERIC Educational Resources Information Center

    Bartus, P.; Isidro, G. M.; La Rosa, C.; Pantoja, C. A.

    2007-01-01

    We describe new materials available at the Arecibo Observatory for visitors with visual impairments. These materials include a guide in Braille that describes the telescope, explains some basic terms used in radio astronomy, and lists frequently asked questions. We have also designed a tactile model of the telescope. Our interest is in enabling…

  8. Solar Dynamics Observatory Briefing

    NASA Image and Video Library

    2010-01-21

    Richard Fisher, Heliophysics Division Director at NASA Headquarters, left, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, as Madhulika Guhathakurta, SDO Program Scientist looks on at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

  9. Solar Dynamics Observatory Briefing

    NASA Image and Video Library

    2010-01-21

    Richard Fisher, Heliophysics Division Director at NASA Headquarters, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

  10. Solar Dynamics Observatory Briefing

    NASA Image and Video Library

    2010-01-21

    Madhulika Guhathakurta, SDO Program Scientist, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

  11. High Energy Astronomy Observatory

    NASA Technical Reports Server (NTRS)

    1980-01-01

    An overview of the High Energy Astronomy Observatory 2 contributions to X-ray astronomy is presented along with a brief description of the satellite and onboard telescope. Observations relating to galaxies and galactic clusters, black holes, supernova remnants, quasars, and cosmology are discussed.

  12. The Sudbury Neutrino Observatory

    SciTech Connect

    Hime, A.

    1996-09-01

    A report is given on the status of the Sudbury Neutrino Observatory, presently under construction in the Creighton nickel mine near Sudbury, Ontario in Canada. Focus is upon the technical factors involving a measurement of the charged-current and neutral-current interactions of solar neutrinos on deuterium.

  13. Stratospheric Observatory for Infrared Astronomy (SOFIA)

    NASA Astrophysics Data System (ADS)

    Becklin, E. E.; Gehrz, R. D.; Roellig, T. L.

    2012-10-01

    The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), a program to develop and operate a 2.5-meter infrared airborne telescope in a Boeing 747SP, has obtained first science with the FORCAST camera in the 5 to 40 micron spectral region and the GREAT heterodyne spectrometer in the 130 to 240 micron spectral region. We briefly review the characteristics and status of the observatory. Spectacular science results on regions of star formation will be discussed. The FORCAST images show several discoveries and the potential for determining how massive stars form in our Galaxy. The GREAT heterodyne spectrometer has made mapping observations of the [C II] line at 158 microns, high J CO lines, and other molecular lines including SH. The HIPO high speed photometer and the high speed camera FDC were used to observe the 2011 June 23 UT stellar occultation by Pluto.

  14. Abnormal origin of the right subclavian artery from the right pulmonary artery in a patient with D-transposition of the great vessels and left juxtaposition of the right atrial appendage: an unusual anatomical variant.

    PubMed

    Mosieri, Jackmerry; Chintala, Kavitha; Delius, Ralph E; Walters, Henry L; Hakimi, Mehdi

    2004-01-01

    Isolation of the left subclavian artery (LSCA) or its anomalous origin from the pulmonary artery (PA) has been documented in several cases, especially in association with a right-sided aortic arch. Similar anomalies involving the right subclavian artery (RSCA) are less frequent. Anomalous origin of the RSCA from the PA in association with D-transposition of the great arteries (D-TGA) is exceedingly rare and only two cases have been reported so far. We present here, a case of aberrant origin of the RSCA from the right PA in a patient with D-TGA, in whom the diagnosis was rendered difficult due to the partial occlusion of the intervening ductus arteriosus (DA). We discuss the embryological basis of this anomaly and review its clinical and surgical implications.

  15. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This photograph was taken during encapsulation of the High Energy Astronomy Observatory (HEAO)-3. Designed and developed by TRW, Inc. under the direction of the Marshall Space Flight Center, the objectives of the HEAO-3 were to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit. The Marshall Space Flight Center had the project management responsibilities for the HEAO missions.

  16. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This photograph shows the High Energy Astronomy Observatory (HEAO)-3 being assembled at TRW, Inc. Designed and developed by TRW, Inc. under the direction of the Marshall Space Flight Center, the objectives of the HEAO-3 were to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit. The Marshall Space Flight Center had the project management responsibilities for the HEAO missions.

  17. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This photograph shows the High Energy Astronomy Observatory (HEAO)-3 being prepared for encapsulation. Designed and developed by TRW, Inc. under the direction of the Marshall Space Flight Center, the objectives of the HEAO-3 were to survey and map the celestial sphere for gamma-ray flux and make detailed measurements of cosmic-ray particles. It carried three scientific experiments: a gamma-ray spectrometer, a cosmic-ray isotope experiment, and a heavy cosmic-ray nuclei experiment. The HEAO-3 was originally identified as HEAO-C but the designation was changed once the spacecraft achieved orbit. The Marshall Space Flight Center had the project management responsibilities for the HEAO missions.

  18. Astrometry and early astrophysics at Kuffner Observatory in the late 19th century

    NASA Astrophysics Data System (ADS)

    Habison, Peter

    The astronomer and mathematician Norbert Herz encouraged Moriz von Kuffner, owner of the beer brewery in Ottakring, to finance a private scientific observatory in the western parts of Vienna. In the years 1884-87 the Kuffner Observatory was built at the Gallitzinberg in Wien-Ottakring. It was an example of enlighted patronage and noted at the time for its rapid acquisition of new instruments and by increasing international recognition. It contained the largest heliometer in the world and the largest meridian circle in the Austrian-Hungarian Empire. Of the many scientists who worked here we mention Leo de Ball, Gustav Eberhard, Johannes Hartmann and we should not forget Karl Schwarzschild. Here in Vienna he published papers on celestial mechanics, measuring techniques, optics and his fundamental papers concerning photographic photometry, in particular the quantitative determination of the departure of the reciprocity law. The telescope and the associated camera with which he carried out his measurements are still in existence at the observatory. The observatory houses important astronomical instruments from the 19th century. All telescopes were made by Repsold und Söhne in Hamburg, and Steinheil in Munich. These two German companies were best renowned for quality and precision in high standard astronomical instruments. The Great Refractor (270/3500 mm) is still the third largest refractor in Austria. It was installed at the observatory in 1886 and was used together with the Schwarzschild Refractor for early astrophysical work including photography. It is this double refractor, where Schwarzschild carried out his measurements on photographic photometry. The Meridian Circle (132/1500 mm) was the largest meridian passage instrument of the Austro-Hungarian Empire. Today it is the largest meridian circle in Austria and still one of the largest in Europe. The telescope is equipped with one of the first impersonal micrometers of that time. First observations were carried

  19. Placental invasion, preeclampsia risk and adaptive molecular evolution at the origin of the great apes: evidence from genome-wide analyses.

    PubMed

    Crosley, E J; Elliot, M G; Christians, J K; Crespi, B J

    2013-02-01

    Recent evidence from chimpanzees and gorillas has raised doubts that preeclampsia is a uniquely human disease. The deep extravillous trophoblast (EVT) invasion and spiral artery remodeling that characterizes our placenta (and is abnormal in preeclampsia) is shared within great apes, setting Homininae apart from Hylobatidae and Old World Monkeys, which show much shallower trophoblast invasion and limited spiral artery remodeling. We hypothesize that the evolution of a more invasive placenta in the lineage ancestral to the great apes involved positive selection on genes crucial to EVT invasion and spiral artery remodeling. Furthermore, identification of placentally-expressed genes under selection in this lineage may identify novel genes involved in placental development. We tested for positive selection in approximately 18,000 genes using the ratio of non-synonymous to synonymous amino acid substitution for protein-coding DNA. DAVID Bioinformatics Resources identified biological processes enriched in positively selected genes, including processes related to EVT invasion and spiral artery remodeling. Analyses revealed 295 and 264 genes under significant positive selection on the branches ancestral to Hominidae (Human, Chimp, Gorilla, Orangutan) and Homininae (Human, Chimp, Gorilla), respectively. Gene ontology analysis of these gene sets demonstrated significant enrichments for several functional gene clusters relevant to preeclampsia risk, and sets of placentally-expressed genes that have been linked with preeclampsia and/or trophoblast invasion in other studies. Our study represents a novel approach to the identification of candidate genes and amino acid residues involved in placental pathologies by implicating them in the evolution of highly-invasive placenta. Copyright © 2012 Elsevier Ltd. All rights reserved.

  20. Cultural heritage of astronomical observatories

    NASA Astrophysics Data System (ADS)

    Wolfschmidt, Gudrun

    2011-06-01

    We present the results of the ICOMOS international symposium ``Cultural Heritage of Astronomical Observatories (around 1900) - From Classical Astronomy to Modern Astrophysics'' (Oct. 2008). The objective of the symposium was to discuss the relevance of modern observatories to the cultural heritage of humankind and to select partner observatories which, due to the date of their construction or to their architectural or scientific importance are comparable to Hamburg Observatory, as international cooperation partners for a serial trans-national application.

  1. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1978-01-01

    Managed by the Marshall Space Flight Center and built by TRW, the second High Energy Astronomy Observatory was launched November 13, 1978. The observatory carried the largest X-ray telescope ever built and was renamed the Einstein Observatory after achieving orbit.

  2. The Origin of Carbon-Bearing Volatiles in a Continental Hydrothermal System in the Great Basin: Water Chemistry and Isotope Characterizations

    NASA Technical Reports Server (NTRS)

    Fu, Qi; Socki, Richard A.; Niles, Paul B.; Romanek, Christopher; Datta, Saugata; Darnell, Mike

    2012-01-01

    Hydrothermal systems on Earth are active centers in the crust where organic molecules can be synthesized biotically or abiotically under a wide range of physical and chemical conditions [1-3]. Not only are volatile species (CO, CO2, H2, and hydrocarbons) a reflection of deep-seated hydrothermal alteration processes, but they also form an important component of biological systems. Studying carbon-bearing fluids from hydrothermal systems is of specific importance to understanding (bio-)geochemical processes within these systems. With recent detection of methane in the martian atmosphere [4-7] and the possibility of its hydrothermal origin [8, 9], understanding the formation mechanisms of methane may provide constraints on the history of the martian aqueous environments and climate.

  3. Alaska Volcano Observatory

    USGS Publications Warehouse

    Venezky, Dina Y.; Murray, Tom; Read, Cyrus

    2008-01-01

    Steam plume from the 2006 eruption of Augustine volcano in Cook Inlet, Alaska. Explosive ash-producing eruptions from Alaska's 40+ historically active volcanoes pose hazards to aviation, including commercial aircraft flying the busy North Pacific routes between North America and Asia. The Alaska Volcano Observatory (AVO) monitors these volcanoes to provide forecasts of eruptive activity. AVO is a joint program of the U.S. Geological Survey (USGS), the Geophysical Institute of the University of Alaska Fairbanks (UAFGI), and the State of Alaska Division of Geological and Geophysical Surveys (ADGGS). AVO is one of five USGS Volcano Hazards Program observatories that monitor U.S. volcanoes for science and public safety. Learn more about Augustine volcano and AVO at http://www.avo.alaska.edu.

  4. The Ultimate Private Observatory

    NASA Astrophysics Data System (ADS)

    Aymond, J.

    2009-03-01

    An amateur astronomer from Washington Parish, Southeast Louisiana, USA has designed and built an amazing observatory. It is not only an astronomical observatory, but a home theater, and tornado shelter designed to take a direct hit from an F5 tornado. The facility is fully equipped and automated, with a hydraulically driven roof that weighs 20,571 lbs., which lifts up, then rolls away to the end of the tracks. This leaves the user sitting inside of four 14-foot high walls open to the night sky. It has two premium quality telescopes for viewing deep space and objects inside the solar system. The chair that the observer sits on is also hydraulically driven.

  5. Expanding the HAWC Observatory

    SciTech Connect

    Mori, Johanna

    2016-08-17

    The High Altitude Water Cherenkov Gamma-Ray Observatory is expanding its current array of 300 water tanks to include 350 outrigger tanks to increase sensitivity to gamma rays above 10 TeV. This involves creating and testing hardware with which to build the new tanks, including photomultiplier tubes, high voltage supply units, and flash analog to digital converters. My responsibilities this summer included preparing, testing and calibrating that equipment.

  6. Mount Wilson Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    Mount Wilson Observatory, located in the San Gabriel Mountains near Pasadena, California, was founded in 1904 by George Ellery Hale with financial support from Andrew Carnegie. In the 1920s and 1930s, working at the 2.5 m Hooker telescope, Edwin Hubble made two of the most important discoveries in the history of astronomy: first, that `nebulae' are actually island universes—galaxies—each with bil...

  7. Arecibo Observatory for All

    NASA Astrophysics Data System (ADS)

    Bartus, P.; Isidro, G. M.; La Rosa, C.; Pantoja, C. A.

    We describe new materials available at the Arecibo Observatory for visitors with visual impairments. These materials include a guide in Braille that describes the telescope, explains some basic terms used in radio astronomy, and lists frequently asked questions. We have also designed a tactile model of the telescope. Our interest is in enabling blind visitors to participate in the excitement of visiting the world's largest radio telescope.

  8. Jodrell Bank Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Jodrell Bank Observatory is part of the University of Manchester and was founded by Bernard Lovell in December 1945. Its prime instrument, the 76 m, MK1 radio-telescope, was completed in 1957. It was given a major upgrade in 1971 and is now known as the Lovell Telescope. In its early years it pioneered the technique of long baseline interferometry which led to the discovery of quasars. A majo...

  9. Calar Alto Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Calar Alto Observatory, or `Centro Astronomico Hispano-Aleman', is located at an altitude of 2168 m in the `Sierra de los Filabres', in southern Spain. Its construction on Calar Alto mountain began in 1973. It is operated jointly by the MAX-PLANCK-INSTITUT FÜR ASTRONOMIE in Heidelberg (MPIA), Germany, and the `Comision Nacional de Astronomia'. The MPIA provides four telescopes of diameters 3....

  10. Dominion Radio Astrophysical Observatory

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    The Dominion Radio Astrophysical Observatory began operating in 1959, and joined the NATIONAL RESEARCH COUNCIL in 1970. It became part of the Herzberg Institute of Astrophysics in 1975. The site near Penticton, BC has a 26 m radio telescope, a seven-antenna synthesis telescope on a 600 m baseline and two telescopes dedicated to monitoring the solar radio flux at 10.7 cm. This part of the Institu...

  11. Sierra Remote Observatories

    NASA Astrophysics Data System (ADS)

    Ringwald, Fred; Morgan, G. E.; Barnes, F. S., III; Goldman, D. S.; Helm, M. R.; Mortfield, P.; Quattrocchi, K. B.; Van Vleet, L.

    2009-05-01

    We report the founding of a new facility for astrophotography and small-telescope science. Sierra Remote Observatories are eight small observatories at 4610' altitude in the Sierra Nevada Mountains of California. The sky brightness during New Moon typically rates 3 on the Bortle scale. Typical seeing is 1.2", with a one-sigma range between 1.0" and 1.6", measured during 2007 June-September. All eight observatories are operated by remote control over the Internet, from as far away as Toronto and South Carolina. The telescopes range in aperture from 106 mm to 16 inches. Color images have so far been published in several magazines (Astronomy, Practical Astronomer, and Sky & Telescope) and on NASA's Astronomy Picture of the Day website. Science programs include time-resolved photometry of cataclysmic variables including the discovery of a 3.22-hour periodicity in the light curve of the nova-like V378 Pegasi, the serendipitous discovery of a previously undesignated spherical bubble in Cygnus, the discovery of three asteroids, and monitoring of Comet Lulin.

  12. Megalithic observatory Kokino

    NASA Astrophysics Data System (ADS)

    Cenev, Gj.

    2006-05-01

    In 2001, on the footpath of a mountain peak, near the village of Kokino, archeologist Jovica Stankovski discovered an archeological site from The Bronze Age. The site occupies a large area and is scaled in two levels. Several stone seats (thrones) are dominant in this site and they are pointing towards the east horizon. The high concentration of the movable archeological material found on the upper platform probably indicates its use in a function containing still unknown cult activities. Due to precise measurements and a detailed archaeoastronomical analysis of the site performed in the past three years by Gjore Cenev, physicist from the Planetarium in Skopje, it was shown that the site has characteristics of a sacred site, but also of a Megalithic Observatory. The markers found in this observatory point on the summer and winter solstices and spring and autumn equinoxes. It can be seen that on both sides of the solstice markers, that there are markers for establishing Moon's positions. The markers are crafted in such a way that for example on days when special rites were performed (harvest rites for example) the Sun filled a narrow space of the marker and special ray lighted the man sitting on only one of the thrones, which of course had a special meaning. According to the positions of the markers that are used for Sun marking, especially on the solstice days, it was calculated that this observatory dates from 1800 B.C.

  13. The solar terrestrial observatory

    NASA Technical Reports Server (NTRS)

    Chappell, C. R.

    1978-01-01

    The larger system of the earth environment is controlled externally by electromagnetic and particle energy from the sun. Recent studies have shown that the sun is a variable star with changes in its radiation which produce significant effects in the earth's climate and weather. The study of the solar-terrestrial system requires simultaneous, long-duration observations of the different elements or 'links' in the solar-terrestrial chain. Many investigations must be conducted in space from a vantage point above the earth's atmosphere where all of the sun's emissions can be observed free from atmospheric distortion, where the magnetospheric particles and fields can be measured directly, and where the atmosphere can be observed on a global scale. The extension of the Shuttle on-orbit capability in connection with the development of the power module will offer an important near-term step in an evolutionary process leading toward a permanent manned Solar Terrestrial Observatory capability in low-earth orbit. Attention is given to the required solar-terrestrial measurements, the operation of the Solar Terrestrial Observatory, and an evolutionary approach to the Solar Terrestrial Observatory.

  14. The Russian Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Dluzhnevskaya, O. B.; Malkov, O. Yu.; Kilpio, A. A.; Kilpio, E. Yu.; Kovaleva, D. A.; Sat, L. A.

    The Russian Virtual Observatory (RVO) will be an integral component of the International Virtual Observatory (IVO). The RVO has the main goal of integrating resources of astronomical data accumulated in Russian observatories and institutions (databases, archives, digitized glass libraries, bibliographic data, a remote access system to information and technical resources of telescopes etc.), and providing transparent access for scientific and educational purposes to the distributed information and data services that comprise its content. Another goal of the RVO is to provide Russian astronomers with on-line access to the rich volumes of data and metadata that have been, and will continue to be, produced by astronomical survey projects. Centre for Astronomical Data (CAD), among other Russian institutions, has had the greatest experience in collecting and distributing astronomical data for more than 20 years. Some hundreds of catalogs and journal tables are currently available from the CAD repository. More recently, mirrors of main astronomical data resources (VizieR, ADS, etc) are now maintained in CAD. Besides, CAD accumulates and makes available for the astronomical community information on principal Russian astronomical resources.

  15. Building International Space Observatories

    NASA Astrophysics Data System (ADS)

    Tananbaum, Harvey

    2013-04-01

    In this brief presentation I will focus on international collaborations for building x-ray observatories. Two primary approaches seem relevant for discussion: 1. Contribution of an instrument by one Agency to a mission led by another 2. Substantial participation by 2 or more Agencies in designing and building an Observatory - close to equal partnerships. Most of our experience in x-ray astronomy falls into the first category, and I will illustrate by briefly summarizing Chandra. The second case will be assessed by reviewing the community's and Agencies' efforts on the International X-ray Observatory (IXO). What can we distill from the successes and difficulties encountered over the past several years? Thoughts about how we might proceed in the future will be shared during the subsequent Panel Discussion. Independent of the development approach, we seem to have general agreement that the bulk of the observing time should be open to scientists world-wide through Peer Review to optimize the science return.

  16. Two New Permanent GPS Observatories In The Czech Republic - Snezka and Biskup

    NASA Astrophysics Data System (ADS)

    Schenk, V.; Kottnauer, P.; Schenkova, Z.; Rucki, A.; Psenicka, J.; Rehak, J., Jr.

    In summer 2001 the Institute of Rock Structure and Mechanics bought GPS receivers Ashtech Z-18 equipped with Choke-Ring antennas to establish two GPS observatories in the area of geodynamic networks "East" and "West Sudeten". For the permanent monitoring of the GPS satellite signals following two sites were tested and adopted: (a) a top of the highest mount Snezka of the Krkonose Mts. and (b) the old stone watchtower on the mount Biskupská Kupa in Silesia. The Ashtech Z - 18 receivers that monitor simultaneously NAVSTAR and GLONASS satellite signals are connected to a standard PC equipped with a capable HD to store a great amount of observed data. Just monitored data are regularly put to the HD in binary and RINEX forms, respectively. When GPS day terminates and the binary and RINEX files are successfully stored, the standard Ashtech software closes them and new binary and RINEX files for the next GPS day creates. To protect the receivers and the PCs against a power failure they are powered by 230V AC/ 12V DC power source/charger and backed up by 12V/240Ah batteries. As evident, the observatories operate without operators and approximately once per two months the stored data are copied to any PC medium. Thus, valuable databases for an intensive research in geodynamics of the north-east part of the Bo- hemian Massif and naturally for a fundamental tasks in geodesy are originated. Since each observatory is located within one of two existing GPS networks, the "East" and "West Sudeten", there is an assumption that annual campaign network data together with observatory ones will distinctly contribute to understanding and/or explanation of existing regional geodynamical movements in the Sudeten area. The establishment of the GPS observatories was essentially supported from funds of the MEYS research programme, from a Project LN00A005 "Dynamics of the Earth", and of the GA CR research project No. 205/01/0480.

  17. Great Practices

    EPA Pesticide Factsheets

    The National Great Practice Compendium highlights outstanding activities, technologies, and programs that prevent trash from entering the aquatic environment and/or that reduce the overall volume of trash that is generated.

  18. Great Apes

    USGS Publications Warehouse

    Sleeman, Jonathan M.; Cerveny, Shannon

    2014-01-01

    Anesthesia of great apes is often necessary to conduct diagnostic analysis, provide therapeutics, facilitate surgical procedures, and enable transport and translocation for conservation purposes. Due to the stress of remote delivery injection of anesthetic agents, recent studies have focused on oral delivery and/or transmucosal absorption of preanesthetic and anesthetic agents. Maintenance of the airway and provision of oxygen is an important aspect of anesthesia in great ape species. The provision of analgesia is an important aspect of the anesthesia protocol for any procedure involving painful stimuli. Opioids and nonsteroidal anti-inflammatory drugs (NSAIDs) are often administered alone, or in combination to provide multi-modal analgesia. There is increasing conservation management of in situ great ape populations, which has resulted in the development of field anesthesia techniques for free-living great apes for the purposes of translocation, reintroduction into the wild, and clinical interventions.

  19. SOFIA: Stratospheric Observatory For Infrared Astronomy

    NASA Technical Reports Server (NTRS)

    Kunz, Nans; Bowers, Al

    2007-01-01

    This viewgraph presentation reviews the great astronomical observatories both space and land based that are now operational. It shows the history of the development of SOFIA, from its conception in 1986 through the contract awards in 1996 and through the planned first flight in 2007. The major components of the observatory are shown and there is a comparison of the SOFIA with the Kuiper Airborne Observatory (KAO), which is the direct predecessor to SOFIA. The development of the aft ramp of the KAO was developed as a result of the wind tunnel tests performed for SOFIA development. Further slides show the airborne observatory layout and the telescope's optical layout. Included are also vies of the 2.5 Meter effective aperture, and the major telescope's components. The presentations reviews the technical challenges encountered during the development of SOFIA. There are also slides that review the wind tunnel tests, and CFD modeling performed during the development of SOFIA. Closing views show many views of the airplane, and views of SOFIA.

  20. Three-D Simulation of the Origin of the Pollutant Ozone Maxima in the Great African Plume: New Meteorology, New Chemistry for TRACE-A

    NASA Technical Reports Server (NTRS)

    Chatfeild, Robert; Vastano, John; Singh, Hanwant; Chan, K. Roland (Technical Monitor)

    1996-01-01

    Burning in South Central Africa is primarily responsible for the vast buildup of ozone in the mid-Atlantic noticeable in the Belem, Brazil, ozonesondes, and also visible in analyses using the Total Ozone Mapping Spectrometer (TOMS). We report on full-scale chemistry simulations for the SAFARI/TRACE-A field period of September-October, 1992. These observational programs provided a wealth of comparison data, including spectacular depictions of the vertical structure of ozone and particulate pollution over Africa, South America, and the Equatorial Atlantic [Browell JGR, 1996, submitted] above and below the NASA DC-8 airplane path. These depictions provide strict tests on the ability of a 3-d simulation and its controlling input parameters, most notably the biomass burning emissions strength. We use meteorology from MM5 used as a synoptic assimilation model and our own GRACES Global Regional Air Chemistry Event Simulator. This report will focus on the unique meteorology of the Equatorial Atmosphere around the Gulf of Guinea during the TRACE-A period, which we describe as "the opening of the gate," "the Great African Plume," and the "African Recirculatory System." We expect to assess whether the ozone observed is primarily "transported African smog," the standard view, or whether "re-$NO_[x)$-ification" of the Central Atlantic troposphere (reduction of nitric acid to active nitrogen oxides in clouds or aerosol) may be required for "extended intercontinental ozone production." A status report on a second nitrogen problem, "lower-tropospheric missing NO(y)," in which we find a serious imbalance in the $NO_ {x }$ and $NO_{y}$ budgets when compared with similar atmospheric tracers, will be given. An elaboration of the concepts set off by quotation marks in this abstract will be given in the talk.

  1. Astronomical publications of Melbourne Observatory

    NASA Astrophysics Data System (ADS)

    Andropoulos, Jenny Ioanna

    2014-05-01

    During the second half of the 19th century and the first half of the 20th century, four well-equipped government observatories were maintained in Australia - in Melbourne, Sydney, Adelaide and Perth. These institutions conducted astronomical observations, often in the course of providing a local time service, and they also collected and collated meteorological data. As well, some of these observatories were involved at times in geodetic surveying, geomagnetic recording, gravity measurements, seismology, tide recording and physical standards, so the term "observatory" was being used in a rather broad sense! Despite the international renown that once applied to Williamstown and Melbourne Observatories, relatively little has been written by modern-day scholars about astronomical activities at these observatories. This research is intended to rectify this situation to some extent by gathering, cataloguing and analysing the published astronomical output of the two Observatories to see what contributions they made to science and society. It also compares their contributions with those of Sydney, Adelaide and Perth Observatories. Overall, Williamstown and Melbourne Observatories produced a prodigious amount of material on astronomy in scientific and technical journals, in reports and in newspapers. The other observatories more or less did likewise, so no observatory of those studied markedly outperformed the others in the long term, especially when account is taken of their relative resourcing in staff and equipment.

  2. Portable coastal observatories

    USGS Publications Warehouse

    Frye, Daniel; Butman, Bradford; Johnson, Mark; von der Heydt, Keith; Lerner, Steven

    2000-01-01

    Ocean observational science is in the midst of a paradigm shift from an expeditionary science centered on short research cruises and deployments of internally recording instruments to a sustained observational science where the ocean is monitored on a regular basis, much the way the atmosphere is monitored. While satellite remote sensing is one key way of meeting the challenge of real-time monitoring of large ocean regions, new technologies are required for in situ observations to measure conditions below the ocean surface and to measure ocean characteristics not observable from space. One method of making sustained observations in the coastal ocean is to install a fiber optic cable from shore to the area of interest. This approach has the advantage of providing power to offshore instruments and essentially unlimited bandwidth for data. The LEO-15 observatory offshore of New Jersey (yon Alt et al., 1997) and the planned Katama observatory offshore of Martha's Vineyard (Edson et al., 2000) use this approach. These sites, along with other cabled sites, will play an important role in coastal ocean science in the next decade. Cabled observatories, however, have two drawbacks that limit the number of sites that are likely to be installed. First, the cable and the cable installation are expensive and the shore station needed at the cable terminus is often in an environmentally sensitive area where competing interests must be resolved. Second, cabled sites are inherently limited geographically to sites within reach of the cable, so it is difficult to cover large areas of the coastal ocean.

  3. Unesco's Global Ethics Observatory

    PubMed Central

    Have, H ten; Ang, T W

    2007-01-01

    The Global Ethics Observatory, launched by the United Nations Educational, Scientific, and Cultural Organization in December 2005, is a system of databases in the ethics of science and technology. It presents data on experts in ethics, on institutions (university departments and centres, commissions, councils and review boards, and societies and associations) and on teaching programmes in ethics. It has a global coverage and will be available in six major languages. Its aim is to facilitate the establishment of ethical infrastructures and international cooperation all around the world. PMID:17209103

  4. NASA's Heliophysics System Observatory

    NASA Astrophysics Data System (ADS)

    Clarke, Steven

    2016-04-01

    NASA formulates and implements a national research program for understanding the Sun and its interactions with the Earth and the solar system and how these phenomena impact life and society. This research provides theory, data, and modeling development services to national and international space weather efforts utilizing a coordinated and complementary fleet of spacecraft, called the Heliophysics System Observatory (HSO), to understand the Sun and its interactions with Earth and the solar system, including space weather. This presentation will focus on NASA's role in space weather research and the contributions the agency continues to provide to the science of space weather, leveraging inter-agency and international collaborations for the benefit of society.

  5. DSN Transient Observatory

    NASA Astrophysics Data System (ADS)

    Kuiper, T. B. H.; Monroe, R. M.; White, L. A.; Miro, C. Garcia; Levin, S. M.; Majid, W. A.; Soriano, M.

    2016-03-01

    The Deep Space Network (DSN) Transient Observatory (DTO) is a signal processing facility that can monitor up to four DSN downlink bands for astronomically interesting signals. The monitoring is done commensally with reception of deep space mission telemetry. The initial signal processing is done with two CASPERa ROACH1 boards, each handling one or two baseband signals. Each ROACH1 has a 10 GBe interface with a GPU-equipped Debian Linux workstation for additional processing. The initial science programs include monitoring Mars for electrostatic discharges, radio spectral lines, searches for fast radio bursts and pulsars and SETI. The facility will be available to the scientific community through a peer review process.

  6. The HAWC observatory

    NASA Astrophysics Data System (ADS)

    DeYoung, Tyce; HAWC Collaboration

    2012-11-01

    The High Altitude Water Cherenkov (HAWC) observatory is a new very high energy water Cherenkov gamma ray telescope, now under construction at 4100 m altitude at Sierra Negra, Mexico. Due to its increased altitude, larger surface area and improved design, HAWC will be about 15 times more sensitive than its predecessor, Milagro. With its wide field of view and high duty factor, HAWC will be an excellent instrument for the studies of diffuse gamma ray emission, the high energy spectra of Galactic gamma ray sources, and transient emission from extragalactic objects such as GRBs and AGN, as well as surveying a large fraction of the VHE sky.

  7. Museum of history of Kyiv Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Kazantseva, L. V.

    2007-09-01

    It is possible to name Astronomical Observatory of the Kiev University as a complex monument to a history of science without exaggeration. Though officially museum hardly exists only for 10 years, the efforts of several generations of the employees keep 160 years of its history. There is a building, which V. beretti has projected and has constructed in 1840-1845 specially for Observatory, pavilions of different design for instruments, great collection of tools and devices, the oldest of which was made by the order in 1838. Besides, scientific and personal archives of many employees attract the large interest. Manuscripts and documents are dated from 1832. The museum contains more than 200 journals of observations, materials of 20 expeditions for observations of solar eclipses, about13000 photo snapshots.

  8. The Compton Gamma Ray Observatory: mission status.

    NASA Astrophysics Data System (ADS)

    Gehrels, N.; Chipman, E.; Kniffen, D. A.

    The Arthur Holly Compton Gamma Ray Observatory (Compton) is the second in NASA's series of Great Observatories. Compton has now been operating for over two and a half years, and has given a dramatic increase in capability over previous gamma-ray missions. The spacecraft and scientific instruments are all in good health, and many significant discoveries have already been made and continue to be made. The authors describe the capabilities of the four scientific instruments and the observing programs for the first three years of the mission. During Phases 2 and 3 of the mission a Guest Investigator program has been in progress with the Guest Observers' time share increasing from 30% to over 50% for the later mission phases.

  9. How To Cover NASA's Chandra X-ray Observatory

    NASA Astrophysics Data System (ADS)

    1999-07-01

    NASA's newest space telescope, the Chandra X-ray Observatory, is scheduled for launch not earlier than July 20, 1999, aboard Space Shuttle mission STS-93. The world's most powerful X-ray observatory, Chandra will join the Hubble Space Telescope and NASA's other great observatories in an unprecedented study of our universe. With its capability to "see" an otherwise invisible but violent, vibrant and ever-changing universe, Chandra will provide insights into the universe's structure and evolution. The following information is designed to assist news media representatives cover launch and activation of the Chandra X-ray Observatory. Covering from the Chandra Control Center NASA will establish a news center at the Chandra X-ray Observatory Operations Control Center in Cambridge, Mass., during the critical period of launch and early activation. The news center will be open from approximately two days prior to launch until the observatory is established in its operating orbit approximately 11 days after launch. The telephone numbers for the news center are: (617) 496-4454 (617) 496-4462 (617) 496-4484 The news center will be staffed around the clock during the Shuttle mission by media relations officers knowledgeable about the Chandra mission and its status. Media covering from the news center will be provided work space and have opportunities for face-to-face interviews with Chandra management, control team members and Chandra scientists. They will be able to participate in daily Chandra status briefings and have access to a special control room viewing area. Additionally, media covering from Cambridge will receive periodic status reports on Chandra and the STS-93 mission, and will be able to participate in interactive televised briefings on the STS-93 mission originating from other NASA centers. While advance accreditation is not required, media interested in covering Chandra from the Operations Control Center should contact Dave Drachlis by telephone at (256) 544

  10. The Gamma Ray Observatory

    NASA Technical Reports Server (NTRS)

    Kniffen, Donald A.

    1991-01-01

    The Gamma Ray Observatory (GRO), scheduled for launch by the Space Shuttle in April 1991, weighs 35,000 lbs and will offer 10 to 20 times better sensitivity than any previous gamma ray mission. The four instruments aboard GRO are described. The Burst and Transient Source Experiment (BATSE) will continuously monitor the entire sky for transient gamma-ray events using eight identical, wide-field detectors capable of measuring brightness variations lasting only milliseconds at energies from about 50,000 to 600,000 eV. The Oriented Scintillation Spectrometer Experiment (OSSE) will make comprehensive observations of discrete sources at energies from 100,000 to 10 million eV, where many radioactive elements have emission lines. The observatory's Imaging Compton Telescope will conduct a deep survey of the entire sky at gamma-ray energies between 1 and 30 MeV. The Energetic Gamma Ray Experiment Telescope will cover a broad high-energy spectral range, from about 20 million to 30 billion eV and conduct a sensitive all-sky survey with a wide field of view and good angular resolution.

  11. The Sudbury Neutrino Observatory

    NASA Astrophysics Data System (ADS)

    McDonald, A. B.; SNO Collaboration

    1999-12-01

    The Sudbury Neutrino Observatory (SNO) is a 1,000 tonne heavy water Cerenkov detector situated 2,000 meters underground in INCO's Creighton mine near Sudbury, Ontario, Canada. The project is a Canadian, US and UK collaboration. Through the use of heavy water SNO will be able to detect a number of neutrino reactions, including one sensitive specifically to solar electron neutrinos and another to all active neutrino types. With these two reactions the detector will be able to search for neutrino flavor change without the requirement of electron neutrino flux normalization by solar model calculations. It will have a relatively high counting rate, on the order of 10 per day for solar neutrinos, and will also provide unusual sensitivity for measurements of other solar neutrino properties, atmospheric neutrinos and suprenova neutrinos. For supernova neutrinos, SNO will have high sensitivity for muon and tau neutrinos and anti-neutrinos as well as specific sensitivity for electron neutrinos and anti-neutrinos. It will have excellent timing and moderate directional sensitivity. The observatory has been in almost continuous operation since May, 1999. SNO Collaboration: Queen's University, University of British Columbia, CRPP at Carleton University, University of Guelph, Laurentian University, Brookhaven National Laboratory, Lawrence Berkeley National Laboratory, Los Alamos National Laboratory, University of Pennsylvania, University of Washington, Oxford University.

  12. The HAWC Observatory

    NASA Astrophysics Data System (ADS)

    Smith, Andrew

    2009-05-01

    The High Altitude Water Cherenkov (HAWC) observatory is a proposed, large field of view (˜2 sr), high duty cycle (>95%) TeV gamma-ray detector to be constructed using a dense array of water tanks covering an area greater than 25,000m^2. HAWC will be located at an elevation of 4100m near the Sierra Negra mountain in Mexico. The instrument will use 900 photomultiplier tubes to observe the relativistic particles and secondary gamma rays in extensive air showers. This technique has been used successfully by the Milagro observatory to detect known, as well as new, TeV sources. The PMTs and much of the data acquisition system of Milagro will be reused for HAWC, resulting in a cost effective detector that can be built quickly (2-3 years). The improvements of HAWC will give 15 times the sensitivity of Milagro. I will present the results of recent detector optimization and engineering studies for HAWC as well as present a detailed analysis of the flux and energy sensitivity of the proposed instrument.

  13. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1978-11-13

    The launch of an Atlas/Centaur launch vehicle is shown in this photograph. The Atlas/Centaur, launched on November 13, 1978, carried the High Energy Astronomy Observatory (HEAO)-2 into the required orbit. The second observatory, the HEAO-2 (nicknamed the Einstein Observatory in honor of the centernial of the birth of Albert Einstein) carried the first telescope capable of producing actual photographs of x-ray objects.

  14. Lessons from the MicroObservatory Net

    NASA Astrophysics Data System (ADS)

    Brecher, K.; Sadler, P.; Gould, R.; Leiker, S.; Antonucci, P.; Deutsch, F.

    1998-12-01

    Over the past several years, we have developed a fully integrated automated astronomical telescope system which combines the imaging power of a cooled CCD, with a self-contained and weatherized 15 cm reflecting optical telescope and mount. Each telescope can be pointed and focused remotely, and filters, field of view and exposure times can be changed easily. The MicroObservatory Net consists of five of these telescopes. They are being deployed around the world at widely distributed longitudes for access to distant night skies during local daytime. Remote access to the MicroObservatories over the Internet has been available to select schools since 1995. The telescopes can be controlled in real time or in delay mode, from any computer using Web-based software. Individuals have access to all of the telescope control functions without the need for an `on-site' operator. After a MicroObservatory completes a job, the user is automatically notified by e-mail that the image is available for viewing and downloading from the Web site. Images are archived at the Web site, along with sample challenges and a user bulletin board, all of which encourage collaboration between schools. The Internet address of the telescopes is http://mo-www.harvard.edu/MicroObservatory/. The telescopes were designed for classroom instruction by teachers, as well as for use by students and amateur astronomers for original scientific research projects. In this talk, we will review some of the experiences we, students and teachers have had in using the telescopes. Support for the MicroObservatory Net has been provided by the NSF, Apple Computer, Inc. and Kodak, Inc.

  15. The Conrad Observatory Research Facility

    NASA Astrophysics Data System (ADS)

    Lenhardt, W.; Melichar, P.

    2009-04-01

    The Conrad Observatory in Austria belongs to the group of most modern geophysical observatories worldwide. The observatory is situated 55 km SW of Vienna in the Eastern Alps. Since 2002 - when the observatory was officially opened - several research tasks, projects, training courses and workshops were carried out at this venue. The site is also magnetically very quiet - one of the requirements for establishing the second part of the observatory, which will serve as the magnetic base observatory for Austria in the future. So far, a tunnel of 145 m length equipped with seismometers, 3 boreholes of 100 m depth and one borehole of 50 m depth, as well as a laboratory, where the gravity is continuously moni-tored, are in operation. In addition an outside station has been built according to Austrian standards for reasons of comparison. Refraction profiles and borehole seismic was used to describe the subsurface conditions for H/V measurements and other scientific tasks. The underground observatory provides ex-cellent conditions to test seismometers under controlled conditions, and a newly developed calibration table assists in the determination of the generator constants of seismometers. Internet connection is available together with a re-distributed GPS-timing signal in the observatory. The NERIES Transnational Access activity TA-5 has attracted already project teams from Germany, Slovenia and The Netherlands to conduct specific instrument tests and comparisons between sensors. See also www.zamg.ac.at/conrad_observatory.

  16. GPM Core Observatory Launch Animation

    NASA Image and Video Library

    This animation depicts the launch of the Global Precipitation Measurement (GPM) Core Observatory satellite from Tanegashima Space Center, Japan. The launch is currently scheduled for Feb. 27, 2014....

  17. Great Expectations for "Great Expectations."

    ERIC Educational Resources Information Center

    Ridley, Cheryl

    Designed to make the study of Dickens'"Great Expectations" an appealing and worthwhile experience, this paper presents a unit of study intended to help students gain (1) an appreciation of Dickens' skill at creating realistic human characters; (2) an insight into the problems of a young man confused by false values and unreal ambitions…

  18. High Energy Astronomy Observatory (HEAO)-2

    NASA Technical Reports Server (NTRS)

    1982-01-01

    This artist's concept depicts the High Energy Astronomy Observatory (HEAO)-2 in orbit. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978. The HEAO-2 was originally identified as HEAO-B but the designation was changed once the spacecraft achieved orbit.

  19. Latest results from the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Dembinski, Hans P.; Pierre Auger Collaboration

    2012-02-01

    The Pierre Auger Observatory, located in the Province of Mendoza, Argentina, is the World's largest detector for cosmic rays at ultra-high energies. In its seven years of operation it has collected an exposure of more than 20000 km2 sr yr, larger than all previous experiments combined. Its original design, optimized for the energy range 1018 eV to 1020 eV, is currently enhanced to cover energies down to almost 1017 eV. We give an overview of the latest results with a focus on the prospect to study nuclear interactions with cosmic rays and conclude with a brief outlook on developments and extensions of the observatory. Full author list

  20. 150th Anniversary of the Astronomical Observatory Library of Sciences

    NASA Astrophysics Data System (ADS)

    Solntseva, T.

    The scientific library of the Astronomical observatory of Kyiv Taras Shevchenko University is one of the oldest ones of such a type in Ukraine. Our Astronomical Observatory and its scientific library will celebrate 150th anniversary of their foundation. 900 volumes of duplicates of Olbers' private library underlay our library. These ones were acquired by Russian Academy of Sciences for Poulkovo observatory in 1841 but according to Struve's order were transmitted to Kyiv Saint Volodymyr University. These books are of great value. There are works edited during Copernicus', Kepler's, Galilei's, Newton's, Descartes' lifetime. Our library contains more than 100000 units of storage - monographs, periodical astronomical editions from the first (Astronomische Nachrichten, Astronomical journal, Monthly Notices etc.), editions of the majority of the astronomical observatories and institutions of the world, unique astronomical atlases and maps

  1. The Great Astronomical Ear.

    ERIC Educational Resources Information Center

    Hiatt, Blanchard

    1980-01-01

    Presents a description of the world's largest radio/radar antenna, the Areciba Observatory in Puerto Rico. Activities at the observatory are discussed as well as the scientific research in the field of radio astronomy. (SA)

  2. The Great Astronomical Ear.

    ERIC Educational Resources Information Center

    Hiatt, Blanchard

    1980-01-01

    Presents a description of the world's largest radio/radar antenna, the Areciba Observatory in Puerto Rico. Activities at the observatory are discussed as well as the scientific research in the field of radio astronomy. (SA)

  3. The Lorenzoni-Tacchini Correspondence at Padova Observatory Archives:the "True" History of Italian Astronomy of the Second Half of the Nineteenth Century

    NASA Astrophysics Data System (ADS)

    Pigatto, L.; Salmaso, M.; Zanini, V.

    2004-12-01

    The correspondence between Giuseppe Lorenzoni and Pietro Tacchini covers the period from 1870 to 1905. Two hundred and ninety original letters written by Tacchini to Lorenzoni and 177 rough copies of letters by Lorenzoni to Tacchini are preserved at the Padova Observatory Archives. Their friendship, which started in 1870 during the expedition to the total solar eclipse in Sicily, as well as their astronomical ability, were of great importance for many events in Italian astronomy during the 2nd half of the 19th century. We are able to gather from this correspondence the following things: 1) the hard work that was put into the founding of the 'Società degli Spettroscopisti Italiani' which succeeded in 1871 mainly thanks to the willingness of three astronomers, Secchi, Tacchini and Lorenzoni; 2) important details about the preparation for the Italian party to India to observe the transit of Venus in 1874; 3) the role of both Lorenzoni and the workshop of the Observatory of Padova in successfully making two large equatorial mountings for the new Catania Observatory and the Bellini Observatory on Mount Etna, and later those for the Italian Observatories of Turin, `Collegio Romano' in Rome, and Arcetri in Florence.

  4. Orbiting Carbon Observatory

    NASA Technical Reports Server (NTRS)

    Miller, Charles E.

    2005-01-01

    Human impact on the environment has produced measurable changes in the geological record since the late 1700s. Anthropogenic emissions of CO2 today may cause the global climate to depart for its natural behavior for many millenia. CO2 is the primary anthropogenic driver of climate change. The Orbiting Carbon Observatory goals are to help collect measurements of atmospheric CO2, answering questions such as why the atmospheric CO2 buildup varies annually, the roles of the oceans and land ecosystems in absorbing CO2, the roles of North American and Eurasian sinks and how these carbon sinks respond to climate change. The present carbon cycle, CO2 variability, and climate uncertainties due atmospheric CO2 uncertainties are highlighted in this presentation.

  5. The Sudbury Neutrino Observatory

    NASA Astrophysics Data System (ADS)

    Duncan, Fraser; SNO Collaboration

    2000-12-01

    Located 2,000 meters below the surface of the earth in the Creighton Nickel Mine near Sudbury, Ontario, Canada, is the Sudbury Neutrino Observatory (SNO). Operational for almost a year now, SNO is a 1000 tonne heavy water Cerenkov detector designed to observe solar neutrinos. The use of heavy water allows SNO to detect neutrinos with an interaction sensitive only to electron neutrinos and with another interaction that is sensitive to all neutrino flavors. SNO's unique ability to separately measure the total solar neutrino flux and electron neutrino fluxes allows the experiment to make a search for flavor oscillations in solar neutrinos in a model independent fashion. The status of the experiment will be described.

  6. The Sudbury Neutrino Observatory

    DOE PAGES

    Bellerive, Alain; Klein, J. R.; McDonald, A. B.; ...

    2016-04-27

    This review paper provides a summary of the published results of the Sudbury Neutrino Observatory (SNO) experiment that was carried out by an international scientific collaboration with data collected during the period from 1999 to 2006. By using heavy water as a detection medium, the SNO experiment demonstrated clearly that solar electron neutrinos from 8B decay in the solar core change into other active neutrino flavors in transit to Earth. The reaction on deuterium that has equal sensitivity to all active neutrino flavors also provides a very accurate measure of the initial solar flux for comparison with solar models. Thismore » review summarizes the results from three phases of solar neutrino detection as well as other physics results obtained from analyses of the SNO data.« less

  7. LCOGT network observatory operations

    NASA Astrophysics Data System (ADS)

    Pickles, Andrew; Hjelstrom, Annie; Boroson, Todd; Burleson, Ben; Conway, Patrick; De Vera, Jon; Elphick, Mark; Haworth, Brian; Rosing, Wayne; Saunders, Eric; Thomas, Doug; White, Gary; Willis, Mark; Walker, Zach

    2014-08-01

    We describe the operational capabilities of the Las Cumbres Observatory Global Telescope Network. We summarize our hardware and software for maintaining and monitoring network health. We focus on methodologies to utilize the automated system to monitor availability of sites, instruments and telescopes, to monitor performance, permit automatic recovery, and provide automatic error reporting. The same jTCS control system is used on telescopes of apertures 0.4m, 0.8m, 1m and 2m, and for multiple instruments on each. We describe our network operational model, including workloads, and illustrate our current tools, and operational performance indicators, including telemetry and metrics reporting from on-site reductions. The system was conceived and designed to establish effective, reliable autonomous operations, with automatic monitoring and recovery - minimizing human intervention while maintaining quality. We illustrate how far we have been able to achieve that.

  8. Sudbury Neutrino Observatory

    SciTech Connect

    Beier, E.W.

    1992-03-01

    This document is a technical progress report on work performed at the University of Pennsylvania during the current year on the Sudbury Neutrino Observatory project. The motivation for the experiment is the measurement of neutrinos emitted by the sun. The Sudbury Neutrino Observatory (SNO) is a second generation dedicated solar neutrino experiment which will extend the results of our work with the Kamiokande II detector by measuring three reactions of neutrinos rather than the single reaction measured by the Kamiokande experiment. The collaborative project includes physicists from Canada, the United Kingdom, and the United States. Full funding for the construction of this facility was obtained in January 1990, and its construction is estimated to take five years. The motivation for the SNO experiment is to study the fundamental properties of neutrinos, in particular the mass and mixing parameters, which remain undetermined after decades of experiments in neutrino physics utilizing accelerators and reactors as sources of neutrinos. To continue the study of neutrino properties it is necessary to use the sun as a neutrino source. The long distance to the sun makes the search for neutrino mass sensitive to much smaller mass than can be studied with terrestrial sources. Furthermore, the matter density in the sun is sufficiently large to enhance the effects of small mixing between electron neutrinos and mu or tau neutrinos. This experiment, when combined with the results of the radiochemical {sup 37}Cl and {sup 71}Ga experiments and the Kamiokande II experiment, should extend our knowledge of these fundamental particles, and as a byproduct, improve our understanding of energy generation in the sun.

  9. Global geodetic observatories

    NASA Astrophysics Data System (ADS)

    Boucher, Claude; Pearlman, Mike; Sarti, Pierguido

    2015-01-01

    Global geodetic observatories (GGO) play an increasingly important role both for scientific and societal applications, in particular for the maintenance and evolution of the reference frame and those applications that rely on the reference frame for their viability. The International Association of Geodesy (IAG), through the Global Geodetic Observing System (GGOS), is fully involved in coordinating the development of these systems and ensuring their quality, perenniality and accessibility. This paper reviews the current role, basic concepts, and some of the critical issues associated with the GGOs, and advocates for their expansion to enhance co-location with other observing techniques (gravity, meteorology, etc). The historical perspective starts with the MERIT campaign, followed by the creation of international services (IERS, IGS, ILRS, IVS, IDS, etc). It provides a basic definition of observing systems and observatories and the build up of the international networks and the role of co-locations in geodesy and geosciences and multi-technique processing and data products. This paper gives special attention to the critical topic of local surveys and tie vectors among co-located systems in sites; the agreement of space geodetic solutions and the tie vectors now place one of the most significant limitations on the quality of integrated data products, most notably the ITRF. This topic focuses on survey techniques, extrapolation to instrument reference points, computation techniques, systematic biases, and alignment of the individual technique reference frames into ITRF. The paper also discusses the design, layout and implementation of network infrastructure, including the role of GGOS and the benefit that would be achieved with better standardization and international governance.

  10. Global Ionosphere Radio Observatory

    NASA Astrophysics Data System (ADS)

    Galkin, I. A.; Reinisch, B. W.; Huang, X. A.

    2014-12-01

    The Global Ionosphere Radio Observatory (GIRO) comprises a network of ground-based high-frequency vertical sounding sensors, ionosondes, with instrument installations in 27 countries and a central Lowell GIRO Data Center (LGDC) for data acquisition and assimilation, including 46 real-time data streams as of August 2014. The LGDC implemented a suite of technologies for post-processing, modeling, analysis, and dissemination of the acquired and derived data products, including: (1) IRI-based Real-time Assimilative Model, "IRTAM", that builds and publishes every 15-minutes an updated "global weather" map of the peak density and height in the ionosphere, as well as a map of deviations from the classic IRI climate; (2) Global Assimilative Model of Bottomside Ionosphere Timelines (GAMBIT) Database and Explorer holding 15 years worth of IRTAM computed maps at 15 minute cadence;. (3) 17+ million ionograms and matching ionogram-derived records of URSI-standard ionospheric characteristics and vertical profiles of electron density; (4) 10+ million records of the Doppler Skymaps showing spatial distributions over the GIRO locations and plasma drifts; (5) Data and software for Traveling Ionospheric Disturbance (TID) diagnostics; and (6) HR2006 ray tracing software mated to the "realistic" IRTAM ionosphere. In cooperation with the URSI Ionosonde Network Advisory Group (INAG), the LGDC promotes cooperative agreements with the ionosonde observatories of the world to accept and process real-time data of HF radio monitoring of the ionosphere, and to promote a variety of investigations that benefit from the global-scale, prompt, detailed, and accurate descriptions of the ionospheric variability.

  11. Great Lakes

    USGS Publications Warehouse

    Edsall, Thomas A.; Mac, Michael J.; Opler, Paul A.; Puckett Haecker, Catherine E.; Doran, Peter D.

    1998-01-01

    The Great Lakes region, as defined here, includes the Great Lakes and their drainage basins in Minnesota, Wisconsin, Illinois, Indiana, Ohio, Pennsylvania, and New York. The region also includes the portions of Minnesota, Wisconsin, and the 21 northernmost counties of Illinois that lie in the Mississippi River drainage basin, outside the floodplain of the river. The region spans about 9º of latitude and 20º of longitude and lies roughly halfway between the equator and the North Pole in a lowland corridor that extends from the Gulf of Mexico to the Arctic Ocean.The Great Lakes are the most prominent natural feature of the region (Fig. 1). They have a combined surface area of about 245,000 square kilometers and are among the largest, deepest lakes in the world. They are the largest single aggregation of fresh water on the planet (excluding the polar ice caps) and are the only glacial feature on Earth visible from the surface of the moon (The Nature Conservancy 1994a).The Great Lakes moderate the region’s climate, which presently ranges from subarctic in the north to humid continental warm in the south (Fig. 2), reflecting the movement of major weather masses from the north and south (U.S. Department of the Interior 1970; Eichenlaub 1979). The lakes act as heat sinks in summer and heat sources in winter and are major reservoirs that help humidify much of the region. They also create local precipitation belts in areas where air masses are pushed across the lakes by prevailing winds, pick up moisture from the lake surface, and then drop that moisture over land on the other side of the lake. The mean annual frost-free period—a general measure of the growing-season length for plants and some cold-blooded animals—varies from 60 days at higher elevations in the north to 160 days in lakeshore areas in the south. The climate influences the general distribution of wild plants and animals in the region and also influences the activities and distribution of the human

  12. GREAT optics

    NASA Astrophysics Data System (ADS)

    Wagner-Gentner, Armin; Graf, Urs U.; Philipp, Martin; Rabanus, David; Stutzki, Jürgen

    2004-10-01

    The German REceiver for Astronomy at Terahertz frequencies (GREAT) is a first generation PI instrument for the SOFIA telescope, developed by a collaboration between the MPIfR, KOSMA, DLR, and the MPAe. The first three institutes each contribute one heterodyne receiver channel to operate at 1.9, 2.7 and 4.7 THz, respectively. A later addition of a e.g. 1.4 THz channel is planned. The GREAT instrument is developed to carry two cryostats at once. That means that any two of the three frequencies can be observed simultaneously. Therefore, we need to be able to quickly exchange the optics benches, the local oscillator (LO) subsystems, and the cryostats containing the mixer devices. This demands a high modularity and flexibility of our receiver concept. Our aim is to avoid the need for realignment when swapping receiver channels. After an overview of the common GREAT optics, a detailed description of several parts (optics benches, calibration units, diplexer, focal plane imager) is given. Special emphasis is given to the LO optics of the KOSMA 1.9 THz channel, because its backward wave oscillator has an astigmatic output beam profile, which has to be corrected for. We developed astigmatic off-axis mirrors to compensate this astigmatism. The mirrors are manufactured in-house on a 5 axis CNC milling machine. We use this milling machine to obtain optical components with highest surface accuracy (about 5 microns) appropriate for these wavelengths. Based on the CNC machining capabilities we present our concept of integrated optics, which means to manufacture optical subsystems monolithically. The optics benches are located on three point mounts, which in conjunction with the integrated optics concept ensure the required adjustment free optics setup.

  13. The Pierre Auger Observatory Upgrade

    NASA Astrophysics Data System (ADS)

    Marsella, Giovanni

    2017-03-01

    It is planned to operate the Pierre Auger Observatory until at least the end of 2024. An upgrade of the experiment has been proposed in order to provide additional measurements to allow one to elucidate the mass composition and the origin of the flux suppression at the highest energies, to search for a flux contribution of protons up to the highest energies and to reach a sensitivity to a contribution as small as 10% in the flux suppression region, to study extensive air showers and hadronic multi-particle production. With operation planned until 2024, event statistics will more than double compared with the existing Auger data set, with the critical added advantage that every event will now have mass information. Obtaining additional composition-sensitive information will not only help to better reconstruct the properties of the primary particles at the highest energies, but also improve the measurements in the energy range just above the ankle. Furthermore, measurements with the new detectors will help to reduce systematic uncertainties related to the modelling hadronic showers and to limitations in the reconstruction algorithms. A description of the principal proposed Auger upgrade will be presented. The Auger upgrade promises high-quality future data, and real scope for new physics.

  14. Great Quotes for Great Educators

    ERIC Educational Resources Information Center

    Whitaker, Todd; Lumpa, Dale

    2005-01-01

    Over 600 insightful, witty nuggets to motivate and inspire you... and everyone else at your school. Teachers--display these quotes in your classrooms! Administrators--insert them into your faculty memos and share them at staff meetings! Why is this book unique? (1) it includes over 100 original quotes from internationally acclaimed speaker and…

  15. Rolloff Roof Observatory Construction (Abstract)

    NASA Astrophysics Data System (ADS)

    Ulowetz, J. H.

    2015-12-01

    (Abstract only) Lessons learned about building an observatory by someone with limited construction experience, and the advantages of having one for imaging and variable star studies. Sample results shown of composite light curves for cataclysmic variables UX UMa and V1101 Aql with data from my observatory combined with data from others around the world.

  16. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1977-08-01

    This picture is of an Atlas/Centaur launch vehicle, carrying the High Energy Astronomy Observatory (HEAO)-1, on Launch Complex 36 at the Air Force Eastern Test Range prior to launch on August 12, 1977. The Kennedy Space Center managed the launch operations that included a pre-aunch checkout, launch, and flight, up through the observatory separation in orbit.

  17. Solar Terrestrial Relations Observatory (STEREO)

    NASA Technical Reports Server (NTRS)

    Davila, Joseph M.; SaintCyr, O. C.

    2003-01-01

    The solar magnetic field is constantly generated beneath the surface of the Sun by the solar dynamo. To balance this flux generation, there is constant dissipation of magnetic flux at and above the solar surface. The largest phenomenon associated with this dissipation is the Coronal Mass Ejection (CME). The Solar and Heliospheric Observatory (SOHO) has provided remarkable views of the corona and CMEs, and served to highlight how these large interplanetary disturbances can have terrestrial consequences. STEREO is the next logical step to study the physics of CME origin, propagation, and terrestrial effects. Two spacecraft with identical instrument complements will be launched on a single launch vehicle in November 2007. One spacecraft will drift ahead and the second behind the Earth at a separation rate of 22 degrees per year. Observation from these two vantage points will for the first time allow the observation of the three-dimensional structure of CMEs and the coronal structures where they originate. Each STEREO spacecraft carries a complement of 10 instruments, which include (for the first time) an extensive set of both remote sensing and in-situ instruments. The remote sensing suite is capable of imaging CMEs from the solar surface out to beyond Earth's orbit (1 AU), and in-situ instruments are able to measure distribution functions for electrons, protons, and ions over a broad energy range, from the normal thermal solar wind plasma to the most energetic solar particles. It is anticipated that these studies will ultimately lead to an increased understanding of the CME process and provide unique observations of the flow of energy from the corona to the near-Earth environment. An international research program, the International Heliophysical Year (IHY) will provide a framework for interpreting STEREO data in the context of global processes in the Sun-Earth system.

  18. The brazilian indigenous planetary-observatory

    NASA Astrophysics Data System (ADS)

    Afonso, G. B.

    2003-08-01

    We have performed observations of the sky alongside with the Indians of all Brazilian regions that made it possible localize many indigenous constellations. Some of these constellations are the same as the other South American Indians and Australian aborigines constellations. The scientific community does not have much of this information, which may be lost in one or two generations. In this work, we present a planetary-observatory that we have made in the Park of Science Newton Freire-Maia of Paraná State, in order to popularize the astronomical knowledge of the Brazilian Indians. The planetary consists, essentially, of a sphere of six meters in diameter and a projection cylinder of indigenous constellations. In this planetary we can identify a lot of constellations that we have gotten from the Brazilian Indians; for instance, the four seasonal constellations: the Tapir (spring), the Old Man (summer), the Deer (autumn) and the Rhea (winter). A two-meter height wooden staff that is posted vertically on the horizontal ground similar to a Gnomon and stones aligned with the cardinal points and the soltices directions constitutes the observatory. A stone circle of ten meters in diameter surrounds the staff and the aligned stones. During the day we observe the Sun apparent motions and at night the indigenous constellations. Due to the great community interest in our work, we are designing an itinerant indigenous planetary-observatory to be used in other cities mainly by indigenous and primary schools teachers.

  19. Ancient "Observatories" - A Relevant Concept?

    NASA Astrophysics Data System (ADS)

    Belmonte, Juan Antonio

    It is quite common, when reading popular books on astronomy, to see a place referred to as "the oldest observatory in the world". In addition, numerous books on archaeoastronomy, of various levels of quality, frequently refer to the existence of "prehistoric" or "ancient" observatories when describing or citing monuments that were certainly not built with the primary purpose of observing the skies. Internet sources are also guilty of this practice. In this chapter, the different meanings of the word observatory will be analyzed, looking at how their significances can be easily confused or even interchanged. The proclaimed "ancient observatories" are a typical result of this situation. Finally, the relevance of the concept of the ancient observatory will be evaluated.

  20. Origin of sulfur and crustal recycling of copper in polymetallic (Cu-Au-Co-Bi-U ± Ag) iron-oxide-dominated systems of the Great Bear Magmatic Zone, NWT, Canada

    NASA Astrophysics Data System (ADS)

    Acosta-Góngora, P.; Gleeson, S. A.; Samson, I. M.; Corriveau, L.; Ootes, L.; Jackson, S. E.; Taylor, B. E.; Girard, I.

    2017-06-01

    The Great Bear Magmatic Zone, in northwest Canada, contains numerous polymetallic mineral occurrences, prospects, and deposits of the iron oxide copper-gold deposit (IOCG) family. The mineralization is hosted by the Treasure Lake Group and igneous rocks of the Great Bear arc and was deposited concomitantly with the arc magmatism (ca. 1.88 to 1.87 Ga). In situ δ 34S (n = 48) and δ 65Cu (n = 79) analyses were carried out on ore-related sulfides from a number of these systems. The δ 34S values mainly vary between 0 and +5‰, consistent with derivation of sulfur from the mantle. Lower δ 34S values (-7.7 to +1.4‰) from the Sue-Dianne breccia may indicate SO2 disproportionation of a magmatic hydrothermal fluid. The δ 65Cu values vary between -1.2 and -0.3‰, and are lower than the igneous δ 65Cu range of values (0.0 ± 0.27‰). The S and Cu isotopic data are decoupled, which suggests that Cu (and possibly some S) was dissolved and remobilized from supracrustal rocks during early stages of alteration (e.g., sodic alteration) and then precipitated by lower temperature, more oxidizing fluids (e.g., Ca-Fe-K alteration). A limited fluid inclusion dataset and δ 13C and δ 18O values are also presented. The δ 18Ofluid values are consistent with a magmatic origin or a host-rock equilibrated meteoric water source, whereas the δ 13Cfluid values support a marine carbonate source. Combined, the S and Cu isotopic data indicate that while the emplacement of the Great Bear magmatic bodies may have driven fluid convection and may be the source of fluids and sulfur, metals such as Cu could have been recycled from crustal sources.

  1. The Sudbury Neutrino Observatory

    NASA Astrophysics Data System (ADS)

    Ewan, G. T.

    1992-04-01

    The Sudbury Neutrino Observatory (SNO) detector is a 1000 ton heavy water (D2O) Cherenkov detector designed to study neutrinos from the sun and other astrophysical sources. The use of heavy water allows both electron neutrinos and all other types of neutrinos to be observed by three complementary reactions. The detector will be sensitive to the electron neutrino flux and energy spectrum shape and to the total neutrino flux irrespective of neutrino type. These measurements will provide information on both vacuum neutrino oscillations and matter-enhanced oscillations, the MSW effect. In the event of a supernova it will be very sensitive to muon and tau neutrinos as well as the electron neutrinos emitted in the initial burst, enabling sensitive mass measurements as well as providing details of the physics of stellar collapse. On behalf of the Sudbury Neutrino Observatory (SNO) Collaboration : H.C . Evans, G.T . Ewan, H.W. Lee, J .R . Leslie, J .D. MacArthur, H .-B . Mak, A.B . McDonald, W. McLatchie, B.C . Robertson, B. Sur, P. Skensved (Queen's University) ; C.K . Hargrove, H. Mes, W.F. Davidson, D. Sinclair, 1 . Blevis, M. Shatkay (Centre for Research in Particle Physics) ; E.D. Earle, G.M. Milton, E. Bonvin, (Chalk River Laboratories); J .J . Simpson, P. Jagam, J . Law, J .-X . Wang (University of Guelph); E.D . Hallman, R.U. Haq (Laurentian University); A.L. Carter, D. Kessler, B.R . Hollebone (Carleton University); R. Schubank . C.E . Waltha m (University of British Columbia); R.T. Kouzes, M.M. Lowry, R.M. Key (Princeton University); E.W. Beier, W. Frati, M. Newcomer, R. Van Berg (University of Penn-sylvania), T.J . Bowles, P.J . Doe, S.R . Elliott, M.M. Fowler, R.G.H. Robertson, D.J . Vieira, J .B . Wilhelmy, J .F. Wilker-son, J .M. Wouters (Los Alamos National Laboratory) ; E. Norman, K. Lesko, A. Smith, R. Fulton, R. Stokstad (Lawrence Berkeley Laboratory), N.W. Tanner, N. JCIILY, P. Trent, J . Barton, D.L . Wark (University of Oxford).

  2. High Energy Astronomy Observatory (HEAO)-2

    NASA Technical Reports Server (NTRS)

    1975-01-01

    This illustration is a schematic of the High Energy Astronomy Observatory (HEAO)-2 and its experiments. It shows the focal plane instruments (at the right) plus the associated electronics for operating the telescope as it transmitted its observations to the ground. A fifth instrument, the Monitor Proportional Counter, is located near the front of the telescope. Four separate astronomical instruments are located at the focus of this telescope and they could be interchanged for different types of observations as the observatory pointed at interesting areas of the Sky. Two of these instruments produced images; a High Resolution Imaging Detector and an Imaging Proportional Counter. The other two instruments, the Solid State Spectrometer and the Crystal Spectrometer, measured the spectra of x-ray objects. A fifth instrument, the Monitor Proportional Counter, continuously viewed space independently to study a wider band of x-ray wavelengths and to examine the rapid time variations in the sources. The HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978. The HEAO-2 was originally identified as HEAO-B but the designation was changed once the spacecraft achieved orbit.

  3. The Solid Earth Research Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Donnellan, A.; Rundle, J. B.; Fox, G.; Pierce, M.; McLeod, D.; Parker, J. W.; Tullis, T.; Grant, L.

    2003-12-01

    Under the auspices of NASA we are developing the Solid Earth Research Virtual Observatory (SERVO). The initial focus of the observatory is spaced-based observational data, ground-based sensor data (GPS, seismicity), simulation data, and published/historical fault measurements, coupled with earthquake fault and tectonic modeling and pattern recognition software. This observatory will enable investigators to seamlessly merge multiple data sets and models, and create new queries. In the SERVO framework, simulation data will be archived together with analysis/animation tools and the original simulation code. Observational data, which is heterogeneous and distributed in nature, will be accessible through cooperative federated databases. SERVO will include tools for visualization, datamining and pattern recognition, with data fusion into a web services (portal) based Problem Solving Environment (PSE). SERVO couples distributed data sources, applications, and hardware resources through an XML-based Web Services framework. Users access the services (and thus distributed resources) through Web browser-based Problem Solving Environment clients. The Web services approach defines standard, programming language-independent application programming interfaces, so non-browser client applications may also be built. Initial application codes in SERVO are GeoFEST, a parallel 3D finite element code, Virtual California, a boundary element code to simulate fault interactions, PARK, a boundary element code for studying unstable slip on faults, and two pattern recognizers RDAHMM, which uses a modification of Hidden Markov Models to analyze time series data, and PDPC, which looks for anomalies in seismicity data.

  4. Hawaiian Volcano Observatory 1956 Quarterly Administrative Reports

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. This report consists of four parts.

  5. Klimovskaya: A new geomagnetic observatory

    NASA Astrophysics Data System (ADS)

    Soloviev, A. A.; Sidorov, R. V.; Krasnoperov, R. I.; Grudnev, A. A.; Khokhlov, A. V.

    2016-05-01

    In 2011 Geophysical Center RAS (GC RAS) began to deploy the Klimovskaya geomagnetic observatory in the south of Arkhangelsk region on the territory of the Institute of Physiology of Natural Adaptations, Ural Branch, Russian Academy of Sciences (IPNA UB RAS). The construction works followed the complex of preparatory measures taken in order to confirm that the observatory can be constructed on this territory and to select the optimal configuration of observatory structures. The observatory equipping stages are described in detail, the technological and design solutions are described, and the first results of the registered data quality control are presented. It has been concluded that Klimovskaya observatory can be included in INTERMAGNET network. The observatory can be used to monitor and estimate geomagnetic activity, because it is located at high latitudes and provides data in a timely manner to the scientific community via the web-site of the Russian-Ukrainian Geomagnetic Data Center. The role of ground observatories such as Klimovskaya remains critical for long-term observations of secular variation and for complex monitoring of the geomagnetic field in combination with low-orbiting satellite data.

  6. Health observatories in iran.

    PubMed

    Rashidian, A; Damari, B; Larijani, B; Vosoogh Moghadda, A; Alikhani, S; Shadpour, K; Khosravi, A

    2013-01-01

    The Islamic Republic of Iran, in her 20 year vision by the year 2025, is a developed country with the first economic, scientific and technological status in the region, with revolutionary and Islamic identity, inspiring Islamic world, as well as effective and constructive interaction in international relations. Enjoying health, welfare, food security, social security, equal opportunities, fair income distribution, strong family structure; to be away from poverty, corruption, and discrimination; and benefiting desirable living environment are also considered out of characteristics of Iranian society in that year. Strategic leadership towards perceived vision in each setting requires restrictive, complete and timely information. According to constitution of National Institute for Health Researches, law of the Fifth Development Plan of the country and characteristics of health policy making, necessity of designing a Health Observatory System (HOS) was felt. Some Principles for designing such system were formulated by taking following steps: reviewing experience in other countries, having local history of the HOS in mind, superior documents, analysis of current production and management of health information, taking the possibilities to run a HOS into account. Based on these principles, the protocol of HOS was outlined in 3 different stages of opinion poll of informed experts responsible for production on management of information, by using questionnaires and Focus Group Discussions. The protocol includes executive regulations, the list of health indicators, vocabulary and a calendar for periodic studies of the community health situation.

  7. The Solar Dynamics Observatory

    NASA Technical Reports Server (NTRS)

    Pesnell, William D.

    2008-01-01

    The Solar Dynamics Observatory (SDO) is the first Space Weather Mission in NASA's Living With a Star Program. SDO's main goal is to understand, driving towards a predictive capability, those solar variations that influence life on Earth and humanity's technological systems. The past decade has seen an increasing emphasis on understanding the entire Sun, from the nuclear reactions at the core to the development and loss of magnetic loops in the corona. SDO's three science investigations (HMI, AIA, and EVE) will determine how the Sun's magnetic field is generated and structured, how this stored magnetic energy is released into the heliosphere and geospace as the solar wind, energetic particles, and variations in the solar irradiance. SDO will return full-disk Dopplergrams, full-disk vector magnetograms, full-disk images at nine EIUV wavelengths, and EUV spectral irradiances, all taken at a rapid cadence. This means you can 'observe the database' to study events, but we can also move forward in producing quantitative models of what the Sun is doing today. SDO is scheduled to launch in 2008 on an Atlas V rocket from the Kennedy Space Center, Cape Canaveral, Florida. The satellite will fly in a 28 degree inclined geosynchronous orbit about the longitude of New Mexico, where a dedicated Ka-band ground station will receive the 150 Mbps data flow. How SDO data will transform the study of the Sun and its affect on Space Weather studies will be discussed.

  8. 10 meter airborne observatory

    NASA Astrophysics Data System (ADS)

    Ditto, Thomas D.; Ritter, Joseph M.

    2008-07-01

    Inside an aircraft fuselage there is little room for the mass of all the instrumentation of a ground-based observatory much less a primary objective aperture at the scale of 10 meters. We have proposed a solution that uses a primary objective grating (POG) which matches the considerable length of the aircraft, approximately 10 meters, and conforms to aircraft aerodynamics. Light collected by the POG is diffracted at an angle of grazing exodus inside the aircraft where it is disambiguated by an optical train that fits within to the interior tunnel. Inside the aircraft, light is focused by a parabolic mirror onto a spectrograph slit. The design has a special benefit in that all objects in the field-of-view of the free spectral range of the POG can have their spectra taken as the aircraft changes orientation. We suggest flight planes that will improve integration times, angular resolution and spectral resolution to acquire targets of high stellar magnitudes or alternatively increase the number of sources acquired per flight at the cost of sensitivity.

  9. The Solar Dynamics Observatory

    NASA Technical Reports Server (NTRS)

    Pesnell, William D.

    2008-01-01

    The Solar Dynamics Observatory (SDO) is the first Space Weather Mission in NASA's Living With a Star Program. SDO's main goal is to understand, driving towards a predictive capability, those solar variations that influence life on Earth and humanity's technological systems. The past decade has seen an increasing emphasis on understanding the entire Sun, from the nuclear reactions at the core to the development and loss of magnetic loops in the corona. SDO's three science investigations (HMI, AIA, and EVE) will determine how the Sun's magnetic field is generated and structured, how this stored magnetic energy is released into the heliosphere and geospace as the solar wind, energetic particles, and variations in the solar irradiance. SDO will return full-disk Dopplergrams, full-disk vector magnetograms, full-disk images at nine EIUV wavelengths, and EUV spectral irradiances, all taken at a rapid cadence. This means you can 'observe the database' to study events, but we can also move forward in producing quantitative models of what the Sun is doing today. SDO is scheduled to launch in 2008 on an Atlas V rocket from the Kennedy Space Center, Cape Canaveral, Florida. The satellite will fly in a 28 degree inclined geosynchronous orbit about the longitude of New Mexico, where a dedicated Ka-band ground station will receive the 150 Mbps data flow. How SDO data will transform the study of the Sun and its affect on Space Weather studies will be discussed.

  10. GPM Core Observatory

    NASA Image and Video Library

    2017-09-27

    The GPM Microwave Imager instrument being constructed in a lab by Ball Aerospace & Technology Corporation. Credit: Ball Aerospace & Technology Corporation The Global Precipitation Measurement (GPM) mission is an international partnership co-led by NASA and the Japan Aerospace Exploration Agency (JAXA) that will provide next-generation global observations of precipitation from space. GPM will study global rain, snow and ice to better understand our climate, weather, and hydrometeorological processes. As of Novermber 2013 the GPM Core Observatory is in the final stages of testing at NASA Goddard Space Flight Center. The satellite will be flown to Japan in the fall of 2013 and launched into orbit on an HII-A rocket in early 2014. For more on the GPM mission, visit gpm.gsfc.nasa.gov/. NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

  11. GPM Core Observatory

    NASA Image and Video Library

    2017-09-27

    NASA engineers Rob Gallagher (left), Ken Smith (right) and Deneen Ferro (inside the spacecraft, center) work on the Global Precipitation Measurement mission's Core satellite in the clean room at Goddard Space Flight Center, Greenbelt Md. Credit: NASA/GSFC/Rebecca Roth The Global Precipitation Measurement (GPM) mission is an international partnership co-led by NASA and the Japan Aerospace Exploration Agency (JAXA) that will provide next-generation global observations of precipitation from space. GPM will study global rain, snow and ice to better understand our climate, weather, and hydrometeorological processes. As of Novermber 2013 the GPM Core Observatory is in the final stages of testing at NASA Goddard Space Flight Center. The satellite will be flown to Japan in the fall of 2013 and launched into orbit on an HII-A rocket in early 2014. For more on the GPM mission, visit gpm.gsfc.nasa.gov/. NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

  12. The great asteroid nomenclature controversy of 1801

    NASA Technical Reports Server (NTRS)

    Cunningham, Clifford J.

    1992-01-01

    With the almost complete neglect of 19th century asteroid research by professional historians of science, it is scarcely surprising that great gaps exist in our knowledge of that important field. This paper focuses on issue of naming the first asteroid. This seemingly innocuous issue assumed great importance because many believed the object discovered by Giuseppe Piazzi at Palermo Observatory to be the eighth primary planet of the solar system.

  13. Great Lakes

    NASA Image and Video Library

    2017-09-28

    Bands of lake effect snow drift eastward from the western Great Lakes in this true-color image captured by the NOAA/NASA Suomi NPP satellite's Visible Infrared Imaging Radiometer Suite (VIIRS) instrument on January 5, 2017. National Weather Service forecasters expect light to moderate lake effect snow showers to continue throughout the day today and into Saturday (1/7). Lake-effect snow forms when cold air passes over the warmer waters of a lake. This causes some lake water to evaporate into the air and warm it. This warmer, wetter air rises and cools as it moves away from the lake. When it cools, it releases that moisture and, if it’s cold enough, that moisture turns into snow. Although true-color images like this may appear to be photographs of Earth, they aren't. They are created by combining data from the three color channels on the VIIRS instrument sensitive to the red, green and blue (or RGB) wavelengths of light into one composite image. In addition, data from several other channels are often also included to cancel out or correct atmospheric interference that may blur parts of the image. Credit: NOAA/NASA/Suomi NPP via NOAA's Environmental Visualization Laboratory

  14. OSO-6 Orbiting Solar Observatory

    NASA Technical Reports Server (NTRS)

    1972-01-01

    The description, development history, test history, and orbital performance analysis of the OSO-6 Orbiting Solar Observatory are presented. The OSO-6 Orbiting Solar Observatory was the sixth flight model of a series of scientific spacecraft designed to provide a stable platform for experiments engaged in the collection of solar and celestial radiation data. The design objective was 180 days of orbital operation. The OSO-6 has telemetered an enormous amount of very useful experiment and housekeeping data to GSFC ground stations. Observatory operation during the two-year reporting period was very successful except for some experiment instrument problems.

  15. Development of Mykolaiv Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Mazhaev, A.; Protsyuk, Yu.

    Results obtained in 2010-2013 on the development of astronomical databases and web services are presented. Mykolaiv Virtual Observatory (MVO) is a part of the Ukrainian Virtual Observatory (UkrVO). At present, MVO consists of three major databases containing data on: astrometric catalogues, photographic plates, CCD observations. The databases facilitate the process of data mining and provide easy access to the textual and graphic information on the results of observations and their reduction obtained during the whole history of Nikolaev Astronomical Observatory (NAO).

  16. The Farid & Moussa Raphael Observatory

    NASA Astrophysics Data System (ADS)

    Hajjar, R.

    2017-06-01

    The Farid & Moussa Raphael Observatory (FMRO) at Notre Dame University Louaize (NDU) is a teaching, research, and outreach facility located at the main campus of the university. It located very close to the Lebanese coast, in an urbanized area. It features a 60-cm Planewave CDK telescope, and instruments that allow for photometric and spetroscopic studies. The observatory currently has one thinned, back-illuminated CCD camera, used as the main imager along with Johnson-Cousin and Sloan photometric filters. It also features two spectrographs, one of which is a fiber fed echelle spectrograph. These are used with a dedicated CCD. The observatory has served for student projects, and summer schools for advanced undergraduate and graduate students. It is also made available for use by the regional and international community. The control system is currently being configured for remote observations. A number of long-term research projects are also being launched at the observatory.

  17. Haystack Observatory Technology Development Center

    NASA Technical Reports Server (NTRS)

    Beaudoin, Chris; Corey, Brian; Niell, Arthur; Cappallo, Roger; Whitney, Alan

    2013-01-01

    Technology development at MIT Haystack Observatory were focused on four areas in 2012: VGOS developments at GGAO; Digital backend developments and workshop; RFI compatibility at VLBI stations; Mark 6 VLBI data system development.

  18. An astronomical observatory for Peru

    NASA Astrophysics Data System (ADS)

    del Mar, Juan Quintanilla; Sicardy, Bruno; Giraldo, Víctor Ayma; Callo, Víctor Raúl Aguilar

    2011-06-01

    Peru and France are to conclude an agreement to provide Peru with an astronomical observatory equipped with a 60-cm diameter telescope. The principal aims of this project are to establish and develop research and teaching in astronomy. Since 2004, a team of researchers from Paris Observatory has been working with the University of Cusco (UNSAAC) on the educational, technical and financial aspects of implementing this venture. During an international astronomy conference in Cusco in July 2009, the foundation stone of the future Peruvian Observatory was laid at the top of Pachatusan Mountain. UNSAAC, represented by its Rector, together with the town of Oropesa and the Cusco regional authority, undertook to make the sum of 300,000€ available to the project. An agreement between Paris Observatory and UNSAAC now enables Peruvian students to study astronomy through online teaching.

  19. The Russian Virtual Observatory Project

    NASA Astrophysics Data System (ADS)

    Dluzhnevskaya, O. B.; Malkov, O. Yu.

    2005-12-01

    We describe the Russian Virtual Observatory (RVO), a prestigious international project sponsored by the Russian Academy of Sciences (RAS). In 2001, the RAS Scientific Council on Astronomy included this project in a list of the most important international projects of the RAS. Its main goal to create and develop the RVO, intended to provide Russian astronomers with direct and effective access to worldwide astronomical data resources. The RVO is one component of the International Virtual Observatory (IVO), a system in which vast astronomical archives and databases around the world, together with analysis tools and computational services, are linked together into an integrated facility. The IVO unites all important national and international projects to create virtual observatories, coordinated by the International Virtual Observatory Alliance. The RVO is one of the organizers and an important participant of the IVO Alliance.

  20. Aquarius Principal Investigator with Observatory

    NASA Image and Video Library

    2011-04-19

    NASA Aquarius Principal Investigator Gary Lagerloef photographed in front of the Aquarius/SAC-D satellite observatory as it is being readied for transportation from Brazil to Vandenberg Air Force Base in California for a June 2011 launch.

  1. The Infrared Space Observatory (ISO)

    NASA Technical Reports Server (NTRS)

    Helou, George; Kessler, Martin F.

    1995-01-01

    ISO, scheduled to launch in 1995, will carry into orbit the most sophisticated infrared observatory of the decade. Overviews of the mission, instrument payload and scientific program are given, along with a comparison of the strengths of ISO and SOFIA.

  2. Islamic Astronomical Instruments and Observatories

    NASA Astrophysics Data System (ADS)

    Heidarzadeh, Tofigh

    This chapter is a brief survey of astronomical instruments being used and developed in Islamic territories from the eighth to the fifteenth centuries as well as a concise account of major observatories and observational programs in this period.

  3. Zoellner studies at Archenhold Observatory

    NASA Astrophysics Data System (ADS)

    Herrmann, D.

    Historical research at Archenhold Observatory revealed that Karl Friedrich Zoellner was one of the central figures in the early history of astrophysics in Germany. Without his work the genesis of the new scientific discipline of astrophysics cannot be understood.

  4. The Infrared Space Observatory (ISO)

    NASA Technical Reports Server (NTRS)

    Helou, George; Kessler, Martin F.

    1995-01-01

    ISO, scheduled to launch in 1995, will carry into orbit the most sophisticated infrared observatory of the decade. Overviews of the mission, instrument payload and scientific program are given, along with a comparison of the strengths of ISO and SOFIA.

  5. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    Managed by the Marshall Space Flight Center and built by TRW, the third High Energy Astronomy Observatory was launched September 20, 1979. HEAO-3 was designed to study gamma-rays and cosmic ray particles.

  6. Status of the SOFIA Observatory

    NASA Technical Reports Server (NTRS)

    Roellig, Thomas L.

    2015-01-01

    The SOFIA observatory has been in routine science operations since returning in January from a 6 month-long heavy maintenance period for the aircraft and the telescope assembly. These operations include a successful 6 week deployment to the Southern hemisphere. This presentation will provide an update to the current operational status of the SOFIA observatory, concentrating on the improvements and upgrades that have been implemented since the heavy maintenance period.

  7. Sofia Observatory Performance and Characterization

    NASA Technical Reports Server (NTRS)

    Temi, Pasquale; Miller, Walter; Dunham, Edward; McLean, Ian; Wolf, Jurgen; Becklin, Eric; Bida, Tom; Brewster, Rick; Casey, Sean; Collins, Peter; Jakob, Holger; Killebrew, Jana; Lampater, Ulrich; Mandushev, Georgi; Marcum, Pamela; Meyer, Allan; Pfueller, Enrico; Reinacher, Andreas; Roeser, Hans-Peter; Savage, Maureen; Teufel, Stefan; Wiedemann, Manuel

    2012-01-01

    The Stratospheric Observatory for Infrared Astronomy (SOFIA) has recently concluded a set of engineering flights for Observatory performance evaluation. These in-flight opportunities have been viewed as a first comprehensive assessment of the Observatory's performance and will be used to address the development activity that is planned for 2012, as well as to identify additional Observatory upgrades. A series of 8 SOFIA Characterization And Integration (SCAI) flights have been conducted from June to December 2011. The HIPO science instrument in conjunction with the DSI Super Fast Diagnostic Camera (SFDC) have been used to evaluate pointing stability, including the image motion due to rigid-body and flexible-body telescope modes as well as possible aero-optical image motion. We report on recent improvements in pointing stability by using an Active Mass Damper system installed on Telescope Assembly. Measurements and characterization of the shear layer and cavity seeing, as well as image quality evaluation as a function of wavelength have been performed using the HIPO+FLITECAM Science Instrument configuration (FLIPO). A number of additional tests and measurements have targeted basic Observatory capabilities and requirements including, but not limited to, pointing accuracy, chopper evaluation and imager sensitivity. SCAI activities included in-flight partial Science Instrument commissioning prior to the use of the instruments as measuring engines. This paper reports on the data collected during the SCAI flights and presents current SOFIA Observatory performance and characterization.

  8. SOFIA observatory performance and characterization

    NASA Astrophysics Data System (ADS)

    Temi, Pasquale; Marcum, Pamela M.; Miller, Walter E.; Dunham, Edward W.; McLean, Ian S.; Wolf, Jurgen; Becklin, Eric E.; Bida, Thomas A.; Brewster, Rick; Casey, Sean C.; Collins, Peter L.; Horner, Scott D.; Jakob, Holger; Jensen, Stephen C.; Killebrew, Jana L.; Lampater, Ulrich; Mandushev, Georgi I.; Meyer, Allen W.; Pfueller, Enrico; Reinacher, Andreas; Rho, Jeonghee; Roellig, Thomas L.; Savage, Maureen L.; Smith, Erin C.; Teufel, Stefan; Wiedemann, Manuel

    2012-09-01

    The Stratospheric Observatory for Infrared Astronomy (SOFIA) has recently concluded a set of engineering flights for Observatory performance evaluation. These in-flight opportunities have been viewed as a first comprehensive assessment of the Observatory's performance and will be used to address the development activity that is planned for 2012, as well as to identify additional Observatory upgrades. A series of 8 SOFIA Characterization And Integration flights have been conducted from June to December 2011. The HIPO science instrument in conjunction with the DSI Super Fast Diagnostic Camera (SFDC) have been used to evaluate pointing stability, including the image motion due to rigid-body and flexible-body telescope modes as well as possible aero-optical image motion. We report on recent improvements in pointing stability by using an Active Mass Damper system installed on Telescope Assembly. Measurements and characterization of the shear layer and cavity seeing, as well as image quality evaluation as a function of wavelength have been performed using the HIPO+FLITECAM Science Instrument conguration (FLIPO). A number of additional tests and measurements have targeted basic Observatory capabilities and requirements including, but not limited to, pointing accuracy, chopper evaluation and imager sensitivity. This paper reports on the data collected during these flights and presents current SOFIA Observatory performance and characterization.

  9. Light Phenomena over the ESO Observatories III: Zodiacal Light

    NASA Astrophysics Data System (ADS)

    Horálek, P.; Christensen, L. L.; Nesvorný, D.; Davies, R.

    2016-06-01

    The zodiacal light is often seen at the ESO observatories in the hours after sunset and before sunrise. The origin of the zodiacal light is described and recent research briefly summarised. Some fine images of the zodiacal light from Paranal and La Silla, including the full extent of the night sky are presented.

  10. Automation of Coordinated Planning Between Observatories: The Visual Observation Layout Tool (VOLT)

    NASA Technical Reports Server (NTRS)

    Maks, Lori; Koratkar, Anuradha; Kerbel, Uri; Pell, Vince

    2002-01-01

    Fulfilling the promise of the era of great observatories, NASA now has more than three space-based astronomical telescopes operating in different wavebands. This situation provides astronomers with the unique opportunity of simultaneously observing a target in multiple wavebands with these observatories. Currently scheduling multiple observatories simultaneously, for coordinated observations, is highly inefficient. Coordinated observations require painstaking manual collaboration among the observatory staff at each observatory. Because they are time-consuming and expensive to schedule, observatories often limit the number of coordinated observations that can be conducted. In order to exploit new paradigms for observatory operation, the Advanced Architectures and Automation Branch of NASA's Goddard Space Flight Center has developed a tool called the Visual Observation Layout Tool (VOLT). The main objective of VOLT is to provide a visual tool to automate the planning of coordinated observations by multiple astronomical observatories. Four of NASA's space-based astronomical observatories - the Hubble Space Telescope (HST), Far Ultraviolet Spectroscopic Explorer (FUSE), Rossi X-ray Timing Explorer (RXTE) and Chandra - are enthusiastically pursuing the use of VOLT. This paper will focus on the purpose for developing VOLT, as well as the lessons learned during the infusion of VOLT into the planning and scheduling operations of these observatories.

  11. Great Lakes, No Clouds

    NASA Image and Video Library

    2017-09-28

    NASA image acquired August 28, 2010 Late August 2010 provided a rare satellite view of a cloudless summer day over the entire Great Lakes region. North Americans trying to sneak in a Labor Day weekend getaway on the lakes were hoping for more of the same. The Great Lakes comprise the largest collective body of fresh water on the planet, containing roughly 18 percent of Earth's supply. Only the polar ice caps contain more fresh water. The region around the Great Lakes basin is home to more than 10 percent of the population of the United States and 25 percent of the population of Canada. Many of those people have tried to escape record heat this summer by visiting the lakes. What they found, according to The Hamilton Spectator, was record-breaking water temperatures fueled by record-breaking air temperatures in the spring and summer. By mid-August, the waters of Lake Superior were 6 to 8°C (11 to 14°F) above normal. Lake Michigan set records at about 4°C (7°F) above normal. The other three Great Lakes – Huron, Erie, and Ontario -- were above normal temperatures, though no records were set. The image was gathered by the Moderate Resolution Imaging Spectroradiometer (MODIS) on NASA’s Aqua satellite at 1:30 p.m. Central Daylight Time (18:30 UTC) on August 28. Open water appears blue or nearly black. The pale blue and green swirls near the coasts are likely caused by algae or phytoplankton blooms, or by calcium carbonate (chalk) from the lake floor. The sweltering summer temperatures have produced an unprecedented bloom of toxic blue-green algae in western Lake Erie, according to the Cleveland Plain Dealer. NASA image by Jeff Schmaltz, MODIS Rapid Response Team, Goddard Space Flight Center. Caption by Mike Carlowicz. Instrument: Aqua - MODIS Click here to see more images from NASA Goddard’s Earth Observatory NASA Goddard Space Flight Center is home to the nation's largest organization of combined scientists, engineers and technologists that build spacecraft

  12. Two 18th Century Observatories of Ireland

    NASA Astrophysics Data System (ADS)

    Hambleton, Robert

    A visit to the two major observatories of Ireland, Armagh Observatory in Northern Ireland, and Dunsink Observatory in Dublin. Mentioned are Herschel, Thomas Grubb, Thomas Jones transit instrument, Howard Grubb, Kew Observatory, John Arnold & Sons clocks, Birr Castle, and the Earl of Rosse.

  13. The Carl Sagan solar and stellar observatories as remote observatories

    NASA Astrophysics Data System (ADS)

    Saucedo-Morales, J.; Loera-Gonzalez, P.

    In this work we summarize recent efforts made by the University of Sonora, with the goal of expanding the capability for remote operation of the Carl Sagan Solar and Stellar Observatories, as well as the first steps that have been taken in order to achieve autonomous robotic operation in the near future. The solar observatory was established in 2007 on the university campus by our late colleague A. Sánchez-Ibarra. It consists of four solar telescopes mounted on a single equatorial mount. On the other hand, the stellar observatory, which saw the first light on 16 February 2010, is located 21 km away from Hermosillo, Sonora at the site of the School of Agriculture of the University of Sonora. Both observatories can now be remotely controlled, and to some extent are able to operate autonomously. In this paper we discuss how this has been accomplished in terms of the use of software as well as the instruments under control. We also briefly discuss the main scientific and educational objectives, the future plans to improve the control software and to construct an autonomous observatory on a mountain site, as well as the opportunities for collaborations.

  14. Great Basin Experimental Range: Annotated bibliography

    Treesearch

    E. Durant McArthur; Bryce A. Richardson; Stanley G. Kitchen

    2013-01-01

    This annotated bibliography documents the research that has been conducted on the Great Basin Experimental Range (GBER, also known as the Utah Experiment Station, Great Basin Station, the Great Basin Branch Experiment Station, Great Basin Experimental Center, and other similar name variants) over the 102 years of its existence. Entries were drawn from the original...

  15. Invited review article: The Chandra X-ray Observatory.

    PubMed

    Schwartz, Daniel A

    2014-06-01

    The Chandra X-ray Observatory is an orbiting x-ray telescope facility. It is one of the National Aeronautics and Space Administration's four "Great Observatories" that collectively have carried out astronomical observations covering the infrared through gamma-ray portion of the electromagnetic spectrum. Chandra is used by astronomers world-wide to acquire imaging and spectroscopic data over a nominal 0.1-10 keV (124-1.24 Å) range. We describe the three major parts of the observatory: the telescope, the spacecraft systems, and the science instruments. This article will emphasize features of the design and development driven by some of the experimental considerations unique to x-ray astronomy. We will update the on-orbit performance and present examples of the scientific highlights.

  16. GEOSCOPE Observatory Recent Developments

    NASA Astrophysics Data System (ADS)

    Leroy, N.; Pardo, C.; Bonaime, S.; Stutzmann, E.; Maggi, A.

    2010-12-01

    The GEOSCOPE observatory consists of a global seismic network and a data center. The 31 GEOSCOPE stations are installed in 19 countries, across all continents and on islands throughout the oceans. They are equipped with three component very broadband seismometers (STS1 or STS2) and 24 or 26 bit digitizers, as required by the Federation of Seismic Digital Network (FDSN). In most stations, a pressure gauge and a thermometer are also installed. Currently, 23 stations send data in real or near real time to GEOSCOPE Data Center and tsunami warning centers. In 2009, two stations (SSB and PPTF) have been equipped with warpless base plates. Analysis of one year of data shows that the new installation decreases long period noise (20s to 1000s) by 10 db on horizontal components. SSB is now rated in the top ten long period stations for horizontal components according to the LDEO criteria. In 2010, Stations COYC, PEL and RER have been upgraded with Q330HR, Metrozet electronics and warpless base plates. They have been calibrated with the calibration table CT-EW1 and the software jSeisCal and Calex-EW. Aluminum jars are now installed instead of glass bells. A vacuum of 100 mbars is applied in the jars which improves thermal insulation of the seismometers and reduces moisture and long-term corrosion in the sensor. A new station RODM has just been installed in Rodrigues Island in Mauritius with standard Geoscope STS2 setup: STS2 seismometer on a granite base plate and covered by cooking pot and thermal insulation, it is connected to Q330HR digitizer, active lightning protection, Seiscomp PC and real-time internet connection. Continuous data of all stations are collected in real time or with a delay by the GEOSCOPE Data Center in Paris where they are validated, archived and made available to the international scientific community. Data are freely available to users by different interfaces according data types (see : http://geoscope.ipgp.fr) - Continuous data in real time coming

  17. Development of solar tower observatories

    NASA Astrophysics Data System (ADS)

    Wolfschmidt, Gudrun

    Because the horizontal solar telescope, the Snow Telescope in Yerkes Observatory, was affected by air-currents from the warmed-up soil, George Ellery Hale had the idea of a tower telescope. In 1904, the 60-foot tower in Mt. Wilson was ready, in 1908 the 150-foot tower was built with the help of the Carnegie foundation. After World War I, Germany made heavy efforts to regain its former strong position in the field of science. Already in December 1919 - after the spectacular result of the English eclipse expedition in October 1919 - Erwin Finlay-Freundlich started a successful fund raising (“Einstein-Stiftungrdquo;) among German industrialists. The company Zeiss in Jena was responsible for the instrumentation of the 20-m solar tower, built in 1920-22. The optical design of the Einstein Tower in respect to light intensity surpassed even the Mt. Wilson solar observatory. Also abroad solar tower observatories were built in the 1920s: Utrecht,The Netherlands (1922), Canberra, Australia (1924), Arcetri, Italy (1926), Pasadena, California (1926) and Tokyo, Japan (1928). In the thirties, solar physics became important because of the solar maximum in 1938 and the new observational possibilities created by Bernard Lyot. At the end of the 1930s, Karl-Otto Kiepenheuer proposed to establish a solar tower observatory on Wendelstein in order to improve the predictions of radio interference by observing sunspots. By stressing the importance of the solar research for war efforts, Otto Heckmann of Göttingen observatory finally succeeded in winning the “Reichsluftfahrtministerium” to finance several solar observatories, like Wendelstein, Hainberg/Göttingen, Kanzelhöhe/Villach, and Schauinsland/Freiburg. Solar astronomy profited by the foundation of the new observatories - four of them existed still after the war. Abroad only the solar observatories of Oxford (1935) and the 50 foot tower of the McMath-Hulbert Observatory, University of Michigan (1936) should be mentioned. Only

  18. Assembling the High Energy Astronomy Observatory (HEAO)-1

    NASA Technical Reports Server (NTRS)

    1977-01-01

    This photograph shows the High Energy Astronomy Observatory (HEAO)-1 being assembled at TRW Systems of Redondo Beach, California. The HEAO was designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit.

  19. Assembling the High Energy Astronomy Observatory (HEAO)-1

    NASA Technical Reports Server (NTRS)

    1977-01-01

    This photograph shows the High Energy Astronomy Observatory (HEAO)-1 being assembled at TRW Systems of Redondo Beach, California. The HEAO was designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center. The first observatory, designated HEAO-1, was launched on August 12, 1977 aboard an Atlas/Centaur launch vehicle and was designed to survey the sky for additional x-ray and gamma-ray sources as well as pinpointing their positions. The HEAO-1 was originally identified as HEAO-A but the designation was changed once the spacecraft achieved orbit.

  20. Observatory Bibliographies as Research Tools

    NASA Astrophysics Data System (ADS)

    Rots, Arnold H.; Winkelman, S. L.

    2013-01-01

    Traditionally, observatory bibliographies were maintained to provide insight in how successful a observatory is as measured by its prominence in the (refereed) literature. When we set up the bibliographic database for the Chandra X-ray Observatory (http://cxc.harvard.edu/cgi-gen/cda/bibliography) as part of the Chandra Data Archive ((http://cxc.harvard.edu/cda/), very early in the mission, our objective was to make it primarily a useful tool for our user community. To achieve this we are: (1) casting a very wide net in collecting Chandra-related publications; (2) including for each literature reference in the database a wealth of metadata that is useful for the users; and (3) providing specific links between the articles and the datasets in the archive that they use. As a result our users are able to browse the literature and the data archive simultaneously. As an added bonus, the rich metadata content and data links have also allowed us to assemble more meaningful statistics about the scientific efficacy of the observatory. In all this we collaborate closely with the Astrophysics Data System (ADS). Among the plans for future enhancement are the inclusion of press releases and the Chandra image gallery, linking with ADS semantic searching tools, full-text metadata mining, and linking with other observatories' bibliographies. This work is supported by NASA contract NAS8-03060 (CXC) and depends critically on the services provided by the ADS.

  1. Galaxies Gather at Great Distances

    NASA Technical Reports Server (NTRS)

    2006-01-01

    [figure removed for brevity, see original site] Distant Galaxy Cluster Infrared Survey Poster [figure removed for brevity, see original site] [figure removed for brevity, see original site] Bird's Eye View Mosaic Bird's Eye View Mosaic with Clusters [figure removed for brevity, see original site] [figure removed for brevity, see original site] [figure removed for brevity, see original site] 9.1 Billion Light-Years 8.7 Billion Light-Years 8.6 Billion Light-Years

    Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang.

    A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots.

    Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes.

    These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0

  2. Local, regional and global signals in longterm time series of gravity, tilt and strain at the Geodynamic Observatory Moxa/Germany

    NASA Astrophysics Data System (ADS)

    Jahr, T.; Kukowski, N.; Schindler, P.; Weise, A.; Jentzsch, G.

    2012-04-01

    For the past 15 years geodynamic signals in gravity, tilt and strain are recorded continuously at the Observatory Moxa in Thuringia/Germany. In the period range between minutes and years signals of interest are the free modes of the Earth, the tides, the polar motion with the Chandler Wobble up to the very long- and non-periodic effects. These global signals can be overlain or masked by local signals, caused by sources in the nearby surroundings of the observatory. These recorded local signals originate from fluctuations of meteorological and hydrological parameters as well as by anthropogenic effects. Modelling and elimination of the effects of environmental parameters in the time series are a great challenge for geodynamic observatories worldwide. For the past several years, the work at the Observatory Moxa is focusing on the separation of local, regional and global parts of the signals. Here, we present several signals in gravity, tilt and strain, e.g. barometric pressure, preciptation and groundwater level, separated from our time series, showing the broad application in geodynamics.

  3. Tsunami Research and Monitoring Enabled through Ocean Network Canada's NEPTUNE Cabled Observatory

    NASA Astrophysics Data System (ADS)

    Heesemann, M.; Insua, T. L.; Mihaly, S. F.; Thomson, R.; Rabinovich, A.; Fine, I.; Scherwath, M.; Moran, K.

    2014-12-01

    Ocean Networks Canada (ONC; http://www.oceannetworks.ca/) operates the multidisciplinary NEPTUNE and VENUS cabled ocean observatories off the west coast of Canada and an increasing number of miniature ocean observatories, such as in the Canadian Arctic. All data collected by these observatories are archived and publicly available through ONC's Oceans 2.0 data portal. Much of the data are related to marine geohazards, such as earthquakes, submarine landslides, and tsunamis and are delivered in real-time to various agencies, including early warning centers. The NEPTUNE and VENUS cabled observatories consist of over 850 km of cable deployed inshore and offshore off Vancouver Island and covers the coastal zones, the northern part of the Cascadia subduction zone, Cascadia Basin, and the Endeavour Segment of the Juan de Fuca Ridge. Geological evidence suggests that there is a 25-40% probability of a magnitude 8 or greater megathrust earthquake along the Cascadia subduction zone in the next 50 years and that the most recent great earthquake (estimated magnitude ~9.0) that occurred in 1700 caused widespread tsunami damage. However, most of the tsunamis that arrive in the area originate from distant sources around the Pacific. Over the last 100 years, numerous major tsunamis have occurred in the Pacific Ocean, killing many tens of thousands of people. The NEPTUNE observatory includes high-precision bottom pressure recorders (BPRs) at each major nodes and a tsunami meter consisting of three BPRs arranged on a ~20 km radius circle around the flat Cascadia Basin site. On September 30, 2009, just days after the first NEPTUNE instruments were installed, the first tsunami waves of 2.5-6.0 cm amplitude generated by the Mw 8.1 Samoa earthquake were recorded by six BPRs. The Samoan tsunami was followed by several other events recorded by the network, including the 2010 Chilean tsunami, the 2011 Tōhoku-Oki earthquake and tsunami, and the 2012 Haida Gwaii tsunami. These open

  4. Delaware River and Catskill Region Hydrologic Observatory

    NASA Astrophysics Data System (ADS)

    Bain, M. B.; Brutsaert, W. H.; Walter, M. T.; Degaetano, A. T.; Steenhuis, T. S.

    2004-12-01

    This poster presents the nationally unique opportunities for hydrology-based research in the Delaware River and Catskill Mountain (DelCat) Region. The DelCat region encompasses all of the Delaware river Basin and the New York City Catskills' source watersheds. It has been a key water resource region prior to the founding of our country. This mountain-river-estuary hydrologic system together with other watersheds in the Catskills has supported the population and economic growth of major metropolitan areas of the early United States by providing water supply, land and forests, transportation, power generation, fisheries, recreation, and pollution elimination. The presentation is an account of a forthcoming effort designed to elicit support and participation. After greatly expanding the user and research community for the DelCat observatory, we will design the facility to serve a large user base interested in studies on a wide range of basic and applied hydrologic science topics and issues. Our current plans are to define the form of the hydrologic observatory, and to forecast the nature of what hydrologic sciences can achieve in the DelCat Region.

  5. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1975-01-01

    The family of High Energy Astronomy Observatory (HEAO) instruments consisted of three unmarned scientific observatories capable of detecting the x-rays emitted by the celestial bodies with high sensitivity and high resolution. The celestial gamma-ray and cosmic-ray fluxes were also collected and studied to learn more about the mysteries of the universe. High-Energy rays cannot be studied by Earth-based observatories because of the obscuring effects of the atmosphere that prevent the rays from reaching the Earth's surface. They had been observed initially by sounding rockets and balloons, and by small satellites that do not possess the needed instrumentation capabilities required for high data resolution and sensitivity. The HEAO carried the instrumentation necessary for this capability. In this photograph, an artist's concept of three HEAO spacecraft is shown: HEAO-1, launched on August 12, 1977; HEAO-2, launched on November 13, 1978; and HEAO-3, launched on September 20. 1979.

  6. Virtual Observatory for stellar astronomy

    NASA Astrophysics Data System (ADS)

    Malkov, O.; Zolotukhin, I.

    2013-10-01

    The principal idea of the Virtual Observatory is to achieve real transparency for astronomical data, similar to transparency for all the world's documents in the World Wide Web. In the Virtual Observatory, all the world's astronomical data is available from one's desktop. All archives understand the same query language, can be accessed through a uniform interface, and diverse data can be analyzed with the same tools. In particular, facilities of the Virtual Observatory allow users to make a fast and correct analysis of objects from various surveys. It yields multi-photometry data on registered objects and makes it possible to determine stellar parameters. Methods of astronomical data analysis as well as their application to various areas of stellar astronomy are discussed in this paper.

  7. The UK National Schools' Observatory

    NASA Astrophysics Data System (ADS)

    Simcoe, M. W.; Newsam, A. M.; Bode, M. F.

    2000-10-01

    Robotic Telescopes provide a unique opportunity for the general public, especially school children, to get direct experience of the excitement of science and perform their own research. Here we describe the National Schools Observatory - a UK project to bring data from large robotic telescopes such as the Liverpool Telescope directly into the classroom. In this way, we can use students fascination with astronomy to enhance teaching and promote science as a whole. As well as the technical aspects of the project, we discuss the importance of dealing directly with teachers and students in the creation of the necessary resources. We also outline the development of the Observatory as a focus for collaborative projects between students in countries all over the world. The National Schools' Observatory is funded by the UK Particle Physics and Astronomy Research Council and the European Social Fund of the EU.

  8. Observatory Publishes Memoir of Pioneer Radio Astronomer

    NASA Astrophysics Data System (ADS)

    2006-07-01

    One of the pioneers of radio astronomy tells her story of the formative years of that science in a memoir published by the National Radio Astronomy Observatory. Dr. Nan Dieter Conklin's book, Two Paths to Heaven's Gate, recounts her experiences making important scientific discoveries in an era when astronomy's "vision" was first extending beyond the light discernable to human eyes. Book Cover CREDIT: NRAO/AUI/NSF Conklin's story is remarkable not only because of her impressive scientific achievements, but also "because she was a woman who nevertheless pursued and succeeded in science -- the first U.S. woman whose Ph.D. thesis was based on her own radio astronomy research and the first U.S. woman to publish original radio astronomy research in a refereed journal -- and because she lived and worked with the degenerative disease multiple sclerosis," according to Claire Hooker of the University of Toronto. In the memoir, Conklin recounts her career and life from the awakening stirred by her first astronomy course at Goucher College in Baltimore, to junior research jobs in Washington, D.C., to graduate school at Harvard and ultimately to the faculty of the University of California at Berkeley. In addition to providing an insider's view of the process of scientific discovery, Conklin also gives the reader a fascinating look at a scientific community and social structure that, though only a half-century removed from the present, was vastly different from today's. Along the way, Conklin candidly reveals the person behind the science -- the person who dealt with the joys and tragedies of life while remaining dedicated to unlocking the secrets of the Universe. "Nan was and remains an inspiration to myself and hundreds of others in the field, both for her scientific acumen and for her ability to overcome extraordinary personal challenges," said Miller Goss of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National

  9. GAIA virtual observatory - development and practices

    NASA Astrophysics Data System (ADS)

    Syrjäsuo, Mikko; Marple, Steve

    2010-05-01

    The Global Auroral Imaging Access, or GAIA, is a virtual observatory providing quick access to summary data from satellite and ground-based instruments that remote sense auroral precipitation (http://gaia-vxo.org). This web-based service facilitates locating data relevant to particular events by simultaneously displaying summary images from various data sets around the world. At the moment, there are GAIA server nodes in Canada, Finland, Norway and the UK. The development is an international effort and the software and metadata are freely available. The GAIA system is based on a relational database which is queried by a dedicated software suite that also creates the graphical end-user interface if such is needed. Most commonly, the virtual observatory is used interactively by using a web browser: the user provides the date and the type of data of interest. As the summary data from multiple instruments are displayed simultaneously, the user can conveniently explore the recorded data. The virtual observatory provides essentially instant access to the images originating from all major auroral instrument networks including THEMIS, NORSTAR, GLORIA and MIRACLE. The scientific, educational and outreach use is limited by creativity rather than access. The first version of the GAIA was developed at the University of Calgary (Alberta, Canada) in 2004-2005. This proof-of-concept included mainly THEMIS and MIRACLE data, which comprised of millions of summary plots and thumbnail images. However, it was soon realised that a complete re-design was necessary to increase flexibility. In the presentation, we will discuss the early history and motivation of GAIA as well as how the development continued towards the current version. The emphasis will be on practical problems and their solutions. Relevant design choices will also be highlighted.

  10. The Compton Observatory Science Workshop

    NASA Technical Reports Server (NTRS)

    Shrader, Chris R. (Editor); Gehrels, Neil (Editor); Dennis, Brian (Editor)

    1992-01-01

    The Compton Observatory Science Workshop was held in Annapolis, Maryland on September 23-25, 1991. The primary purpose of the workshop was to provide a forum for the exchange of ideas and information among scientists with interests in various areas of high energy astrophysics, with emphasis on the scientific capabilities of the Compton Observatory. Early scientific results, as well as reports on in-flight instrument performance and calibrations are presented. Guest investigator data products, analysis techniques, and associated software were discussed. Scientific topics covered included active galaxies, cosmic gamma ray bursts, solar physics, pulsars, novae, supernovae, galactic binary sources, and diffuse galactic and extragalactic emission.

  11. Science operations at Gemini Observatory

    NASA Astrophysics Data System (ADS)

    Rutten, René; Adamson, Andy; Leggett, Sandy

    2016-07-01

    Gemini Observatory operates two 8m telescopes, one on Cerro Pachón in Chile and one on Maunakea Hawaíi, on behalf of an international partnership. The telescopes, their software and supporting infrastructure (and some of the instrumentation) are identical at the two sites. We describe the operation of the observatory, present some key performance indicators, and discuss the outcomes in terms of publications and program completion rates. We describe how recent initiatives have been introduced into the operation in parallel with accommodating a significant budget reduction and changes in the partnership.

  12. High Energy Astronomy Observatory (HEAO)

    NASA Technical Reports Server (NTRS)

    1972-01-01

    This is an artist's concept describing the High Energy Astronomy Observatory (HEAO). The HEAO project involved the launching of three unmarned scientific observatories into low Earth orbit between 1977 and 1979 to study some of the most intriguing mysteries of the universe; pulsars, black holes, neutron stars, and super nova. This concept was painted by Jack Hood of the Marshall Space Flight Center (MSFC). Hardware support for the imaging instruments was provided by American Science and Engineering. The HEAO spacecraft were built by TRW, Inc. under project management of the MSFC.

  13. TRW Ships NASA's Chandra X-ray Observatory To Kennedy Space Center

    NASA Astrophysics Data System (ADS)

    1999-04-01

    Two U.S. Air Force C-5 Galaxy transport planes carrying the observatory and its ground support equipment landed at Kennedy's Space Shuttle Landing Facility at 2:40 p.m. EST this afternoon. REDONDO BEACH, CA.--(Business Wire)--Feb. 4, 1999--TRW has shipped NASA's Chandra X-ray Observatory ("Chandra") to the Kennedy Space Center (KSC), in Florida, in preparation for a Space Shuttle launch later this year. The 45-foot-tall, 5-ton science satellite will provide astronomers with new information on supernova remnants, the surroundings of black holes, and other celestial phenomena that produce vast quantities of X-rays. Cradled safely in the cargo hold of a tractor-trailer rig called the Space Cargo Transportation System (SCTS), NASA's newest space telescope was ferried on Feb. 4 from Los Angeles International Airport to KSC aboard an Air Force C-5 Galaxy transporter. The SCTS, an Air Force container, closely resembles the size and shape of the Shuttle cargo bay. Over the next few months, Chandra will undergo final tests at KSC and be mated to a Boeing-provided Inertial Upper Stage for launch aboard Space Shuttle Columbia. A launch date for the Space Shuttle STS-93 mission is expected to be announced later this week. The third in NASA's family of Great Observatories that includes the Hubble Space Telescope and the TRW-built Compton Gamma Ray observatory, Chandra will use the world's most powerful X-ray telescope to allow scientists to "see" and monitor cosmic events that are invisible to conventional optical telescopes. Chandra's X-ray images will yield new insight into celestial phenomena such as the temperature and extent of gas clouds that comprise clusters of galaxies and the superheating of gas and dust particles as they swirl into black holes. A TRW-led team that includes the Eastman Kodak Co., Raytheon Optical Systems Inc., and Ball Aerospace & Technologies Corp. designed and built the Chandra X-ray Observatory for NASA's Marshall Space Flight Center. The

  14. AUGO II: a comprehensive subauroral zone observatory

    NASA Astrophysics Data System (ADS)

    Schofield, I. S.; Connors, M. G.

    2010-12-01

    A new geophysical observatory dedicated to the study of the aurora borealis will be built 25 km southwest of the town of Athabasca, Alberta, Canada. It is anticipated to see first light in the winter of 2010/2011 and be fully operational in the fall of 2011. Based on the highly successful Athabasca University Geophysical Observatory (AUGO), opened in 2002 at the Athabasca University campus in Athabasca, Alberta, AUGO II will have expanded observational capacity featuring up to eight climate-controlled domed optical observation suites for instrumentation, on-site accommodation for up to six researchers, and most importantly, dark skies free of light pollution from urban development. AUGO II will share the same advantages as its predecessor, one being its location in central Alberta, allowing routine study of the subauroral zone, auroral oval studies during active times, and very rarely of the polar cap. Like the original AUGO, AUGO II will be in close proximity to major highways, be connected to a high bandwidth network, and be within two hour driving distance to the city of Edmonton and its international airport. Opportunities are open for guest researchers in space physics to conduct auroral studies at this new, state-of-the-art research facility through the installation of remotely controlled instruments and/or campaigns. An innovative program of instrument development will accompany the new observatory’s enhanced infrastructure with a focus on magnetics and H-beta meridian scanning photometry.

  15. On-orbit assembly and servicing of future space observatories

    NASA Astrophysics Data System (ADS)

    Lillie, C. F.

    2006-06-01

    NASA's experience servicing the Hubble Space Telescope, including the installation of optical elements to compensate for a mirror manufacturing error; replacement of failed avionics and worn-out batteries, gyros, thermal insulation and solar arrays; upgrades to the data handling subsystem; installation of far more capable instruments; and retrofitting the NICMOS experiment with a mechanical cryocooler has clearly demonstrated the advantages of on-orbit servicing. This effort has produced a unique astronomical observatory that is orders of magnitude more capable than when it was launched and can be operated for several times its original design life. The in-space operations capabilities that are developed for NASA's Exploration Program will make it possible to assemble and service spacecraft in space and to service them in cis-lunar and L2 orbits. Future space observatories should be designed to utilize these capabilities. This paper discusses the application of the lessons learned from HST and our plans for servicing the Advanced X-ray Astrophysical Observatory with the Orbital Maneuvering Vehicle and the Space Station Freedom Customer Servicing Facility to future space observatories, such as SAFIR and LifeFinder that are designed to operate in heliocentric orbits. It addresses the use of human and robotic in-space capabilities that would be required for on-orbit assembly and servicing for future space observatories, and describes some of our design concepts for these activities.

  16. First results from the first Croatian geomagnetic observatory

    NASA Astrophysics Data System (ADS)

    Mandic, Igor; Herak, Davorka; Heilig, Balazs

    2013-04-01

    The first Croatian geomagnetic observatory was established in the area of the Nature Park Lonjsko Polje, after a century of sporadic efforts originating from the proposals of Andrija Mohorovicic. The location was chosen after exhaustive surveys of possible sites. It is located far enough from sources of civilization noise, and was found to be an area without magnetic anomalies and with a low field gradient. The construction of the observatory buildings was completed in the autumn of 2011. The furnishing and installation of instruments and test measurements were completed by the beginning of summer 2012, ever since we have continuous recordings of the geomagnetic elements. In the beginning of December 2012 the fluxgate magnetometer LEMI-035 (H,D,Z orientation) has been installed under the framework of the PLASMON project in cooperation with the Tihany Observatory (Hungary). Permanent data of high quality from our observatory will contribute to the monitoring of the Earth's magnetic field on the regional and global levels, thus enabling further development of geomagnetism in Croatia through collaboration with scientists from the other countries, participation in the international projects, eventual membership in the International Real-time Magnetic Observatory Network (INTERMAGNET), etc. The field elements for the epoch 2012,75 and the baselines are presented together with highlights of some recorded geomagnetic events so far. Furthermore, the comparison between the variation data recorded by the dIdD and the fluxgate LEMI-035 magnetometer is presented.

  17. Cosmic ray composition studies with the Pierre Auger Observatory

    NASA Astrophysics Data System (ADS)

    Boncioli, Denise

    2014-04-01

    The Pierre Auger Observatory in Argentina is the largest cosmic ray detector array ever built. Although the construction was completed in 2008, the Observatory has been taking data continuously since January 2004. Its main goal is to measure ultra high energy cosmic rays (UHECRs, energy above 1018 eV) with unprecedented statistics and precision. Measurements of the energy spectrum, chemical composition (including neutrinos and photons) and arrival directions of UHECRs can provide hints for understanding their origin, propagation and interactions. The fluorescence detector of the Pierre Auger Observatory measures the atmospheric depth, Xmax, where the longitudinal profile of a high energy air shower reaches its maximum. This is sensitive to the nuclear mass composition of the cosmic ray and to the characteristics of the hadronic interactions at very high energy. Due to its hybrid design, the Pierre Auger Observatory also provides independent experimental observables obtained from the surface detector for the study of the shower development. A selection of the Pierre Auger Observatory results on the study of the UHECRs will be presented, focusing on composition results. In particular, the measurements and the different roles of the observables with respect to mass composition will be discussed.

  18. Historical Examples of Lobbying: The Case of Strasbourg Astronomical Observatories

    NASA Astrophysics Data System (ADS)

    Heck, Andre

    2012-08-01

    Several astronomical observatories have been established in Strasbourg in very differing contexts. In the late 17th century, an observing post (scientifically sterile) was put on top of a tower, the Hospital Gate, essentially for the prestige of the city and the notoriety of the university. In the 19th century, the observatory built on the Académie hosting the French university was the first attempt to set up in the city a real observatory equipped with genuine instrumentation with the purpose of carrying out serious research, but the succession of political regimes in France and the continual bidding for moving the university to other locations, together with the faltering of later scholars, torpedoed any significant scientific usage of the place. After the 1870-1871 Franco-Prussian war, the German authorities set up a prestigious university campus with a whole range of institutes together with a modern observatory consisting of several buildings and hosting a flotilla of excellent instruments, including the then largest refractor of the country. This paper illustrates various types of lobbying used in the steps above while detailing, from archive documents largely unexploited so far, original research on the two first observatories.

  19. The Coronal Solar Magnetism Observatory

    NASA Astrophysics Data System (ADS)

    Tomczyk, S.; Landi, E.; Zhang, J.; Lin, H.; DeLuca, E. E.

    2015-12-01

    Measurements of coronal and chromospheric magnetic fields are arguably the most important observables required for advances in our understanding of the processes responsible for coronal heating, coronal dynamics and the generation of space weather that affects communications, GPS systems, space flight, and power transmission. The Coronal Solar Magnetism Observatory (COSMO) is a proposed ground-based suite of instruments designed for routine study of coronal and chromospheric magnetic fields and their environment, and to understand the formation of coronal mass ejections (CME) and their relation to other forms of solar activity. This new facility will be operated by the High Altitude Observatory of the National Center for Atmospheric Research (HAO/NCAR) with partners at the University of Michigan, the University of Hawaii and George Mason University in support of the solar and heliospheric community. It will replace the current NCAR Mauna Loa Solar Observatory (http://mlso.hao.ucar.edu). COSMO will enhance the value of existing and new observatories on the ground and in space by providing unique and crucial observations of the global coronal and chromospheric magnetic field and its evolution. The design and current status of the COSMO will be reviewed.

  20. The gamma-ray observatory

    NASA Technical Reports Server (NTRS)

    1991-01-01

    An overview is given of the Gamma Ray Observatory (GRO) mission. Detection of gamma rays and gamma ray sources, operations using the Space Shuttle, and instruments aboard the GRO, including the Burst and Transient Source Experiment (BATSE), the Oriented Scintillation Spectrometer Experiment (OSSE), the Imaging Compton Telescope (COMPTEL), and the Energetic Gamma Ray Experiment Telescope (EGRET) are among the topics surveyed.

  1. Solar Dynamics Observatory Artist Concept

    NASA Image and Video Library

    2010-02-11

    The Solar Dynamics Observatory SDO spacecraft, shown above the Earth as it faces toward the Sun. SDO is designed to study the influence of the Sun on the Earth and the inner solar system by studying the solar atmosphere. http://photojournal.jpl.nasa.gov/catalog/PIA18169

  2. COMETS - ASTRONOMY - KOHUTEK - CATALINA OBSERVATORY

    NASA Image and Video Library

    1974-02-02

    S74-17688 (11 Jan. 1974) --- This color photograph of the comet Kohoutek was taken by members of the lunar and planetary laboratory photographic team from the University of Arizona, at the Catalina Observatory with a 35mm camera on Jan. 11, 1974. Photo credit: NASA

  3. The Virtual Observatory in Transition

    NASA Astrophysics Data System (ADS)

    Hanisch, R. J.

    2006-07-01

    In the past several years, the Virtual Observatory has progressed from concept to implementation. There is now a well-established International Virtual Observatory Alliance {http://ivoa.net/} with formal processes for the development and promotion of technical standards. The national VO projects have developed science applications layered on the core technologies, and these applications are providing new research opportunities for the astronomy community. The VO projects are also actively engaging the community through technical training programs such as the EuroVO Workshop (June 2005), AstroGrid Workshop (July 2005), and the US National Virtual Observatory Summer School (September 2005). As the research community begins to adopt VO tools and technology and rely on VO services, the VO projects need to prepare for something akin to routine observatory operations. System integration and testing, revision tracking, version/platform support, documentation, resource allocation, service reliability, metadata curation, and user support all need to be taken seriously in an environment/system that is inherently distributed, uncentralized, and undergoing continuing enhancements to the infrastructure.

  4. ISS images for Observatory protection

    NASA Astrophysics Data System (ADS)

    Sánchez de Miguel, Alejandro; Zamorano, Jaime

    2015-08-01

    Light pollution is the main factor of degradation of the astronomical quality of the sky along the history. Astronomical observatories have been monitoring how the brightness of the sky varies using photometric measures of the night sky brightness mainly at zenith. Since the sky brightness depends in other factors such as sky glow, aerosols, solar activity and the presence of celestial objects, the continuous increase of light pollution in these enclaves is difficult to trace except when it is too late.Using models of light dispersion on the atmosphere one can determine which light pollution sources are increasing the sky brightness at the observatories. The input satellite data has been provided by DMSP/OLS and SNPP/VIIRS. Unfortunately their panchromatic bands (color blinded) are not useful to detect in which extension the increase is due to the dramatic change produced by the irruption of LED technology in outdoor lighting. The only instrument in the space that is able to distinguish between the various lighting technologies are the DSLR cameras used by the astronauts onboard the ISS.Current status for some astronomical observatories that have been imaged from the ISS is presented. We are planning to send an official request to NASA with a plan to get images for the most important astronomical observatories. We ask support for this proposal by the astronomical community and especially by the US-based researchers.

  5. Michelson geostationary gravitational wave observatory.

    NASA Astrophysics Data System (ADS)

    Anderson, A. J.

    Studies made during the previous year are outlined. These studies have indicated that a Michelson mm wave interferometer observatory (MGO) operating in geostationary orbit is the best configuration satisfying both current operational and design constraints. It is proposed to study the design of this space laboratory interferometer and to study the inclusion of an inertial transponder in this design.

  6. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1977-01-01

    Managed by the Marshall Space Flight Center and designed by TRW, the first High Energy Astronomy Observatory was launched August 12, 1977 aboard an Atlas Centaur rocket. HEAO-1, devoted to the study of X-rays in space, carried four instruments all used primarily in a scarning mode. The mission lasted seventeen months.

  7. Norwegian Ocean Observatory Network (NOON)

    NASA Astrophysics Data System (ADS)

    Ferré, Bénédicte; Mienert, Jürgen; Winther, Svein; Hageberg, Anne; Rune Godoe, Olav; Partners, Noon

    2010-05-01

    The Norwegian Ocean Observatory Network (NOON) is led by the University of Tromsø and collaborates with the Universities of Oslo and Bergen, UniResearch, Institute of Marine Research, Christian Michelsen Research and SINTEF. It is supported by the Research Council of Norway and oil and gas (O&G) industries like Statoil to develop science, technology and new educational programs. Main topics relate to ocean climate and environment as well as marine resources offshore Norway from the northern North Atlantic to the Arctic Ocean. NOON's vision is to bring Norway to the international forefront in using cable based ocean observatory technology for marine science and management, by establishing an infrastructure that enables real-time and long term monitoring of processes and interactions between hydrosphere, geosphere and biosphere. This activity is in concert with the EU funded European Strategy Forum on Research Infrastructures (ESFRI) roadmap and European Multidisciplinary Seafloor Observation (EMSO) project to attract international leading research developments. NOON envisions developing towards a European Research Infrastructure Consortium (ERIC). Beside, the research community in Norway already possesses a considerable marine infrastructure that can expand towards an international focus for real-time multidisciplinary observations in times of rapid climate change. PIC The presently established cable-based fjord observatory, followed by the establishment of a cable-based ocean observatory network towards the Arctic from an O&G installation, will provide invaluable knowledge and experience necessary to make a successful larger cable-based observatory network at the Norwegian and Arctic margin (figure 1). Access to large quantities of real-time observation from the deep sea, including high definition video, could be used to provide the public and future recruits to science a fascinating insight into an almost unexplored part of the Earth beyond the Arctic Circle

  8. The Instruments of Dudley Observatory

    NASA Astrophysics Data System (ADS)

    Gino, M. C.

    2002-12-01

    Dudley Observatory, founded in 1852, is the nation's oldest independent organization dedicated to astronomical research and education. While Dudley no longer operates a physical observatory, it is home to a number of historically important scientific instruments and telescopes. Dudley's first operating telescope, a Clark Comet-seeker, remains in Dudley's collection today. This 4-inch refractor provided the first discovery of a comet by a Dudley astronomer in 1857 and is one of only four telescopes of this size produced by Alvan Clark. Also in Dudley's collection is the Olcott Meridian Circle which was the primary working telescope at the observatory for over 75 years. This telescope, made by Pistor & Martins and which operated both at the Dudley Observatory in Albany, NY and the San Luis Observatory in Argentina, was used to conduct all of the observations for the Preliminary General Catalog of 6788 Stars (1908) and the General Catalog of 33,343 Stars (1937). The gem of Dudley's collection is the Pruyn Equatorial Telescope, built by the Warner and Swasey Company and equipped with a 12-inch lens made by John Brashear. It was installed in 1893 to conduct both research observations and public observing sessions. After remaining in storage for many decades, this historic telescope will soon resume its role after being refurbished and installed at the Arunah Hill Natural Science Center in Cummington, MA. While Dudley retains its interest in astronomical instruments it has also moved into the areas of space studies and astronomical education. The key projects in the areas of instrumentation and astronomical outreach, which include the instruments above as well as the Rising Star Internship and Space Campership educational programs, will be detailed in the remainder of this paper.

  9. Role of the Chandra X-Ray Observatory Observations for the Study of Ionized Plasmas

    NASA Technical Reports Server (NTRS)

    Weisskopf, Martin C.

    2010-01-01

    The Chandra X-Ray Observatory, launched in 1999, is now beginning its 12-th year of operation. Chandra, the X-ray component of NASA s Great Observatory program, continues to operate efficiently, somewhat remarkable considering that the Observatory was designed for three years of operation with a goal of five. The Observatory features X-ray optics with sub-arcsecond angular resolution and a small suite of instruments, including transmission gratings, which allow for high-resolution spectroscopy of point sources. We will detail the capabilities of the Observatory for making such spectroscopic measurements and discuss a number of examples of what has been learned about the astrophysical plasmas capable of producing bright X-ray emission.

  10. SOFIA: Stratospheric Observatory for Infrared Astronomy

    NASA Technical Reports Server (NTRS)

    Becker, Eric; Kunz, Nans; Bowers, Al

    2007-01-01

    This viewgraph presentation reviews the Stratospheric Observatory for Infrared Astronomy (SOFIA). The contents include: 1) Heritage & History; 2) Level 1 Requirements; 3) Top Level Overview of the Observatory; 4) Development Challenges; and 5) Highlight Photos.

  11. Solar Terrestrial Relations Observatory Spacecraft Artist Concept

    NASA Image and Video Library

    2011-06-01

    An artist conception of one of NASA Solar Terrestrial Relations Observatory STEREO spacecraft. The two observatories currently lie on either side of the sun, providing views of the entire sun simultaneously.

  12. Armenian virtual observatory simple image access service

    NASA Astrophysics Data System (ADS)

    Knyazyan, A. V.; Astsatryan, H. V.; Mickaelian, A. M.

    2017-04-01

    The aim of the article is to introduce the data sharing service of the Armenian Virtual Observatory (ArVO) based on the Simple Image Access (SIA) Protocol of the International Virtual Observatory Alliance (IVOA).

  13. SOFIA - Stratospheric Observatory for Infrared Astronomy

    NASA Technical Reports Server (NTRS)

    Kunz, Nans; Bowers, Al

    2007-01-01

    This viewgraph presentation reviews the Stratospheric Observatory for Infrared Astronomy (SOFIA). The contents include: 1) Heritage & History; 2) Level 1 Requirements; 3) Top Level Overview of the Observatory; 4) Development Challenges; and 5) Highlight Photos.

  14. Geochronology and isotopic geochemistry of the A-type granites from the Huanggang Sn-Fe deposit, southern Great Hinggan Range, NE China: Implication for their origin and tectonic setting

    NASA Astrophysics Data System (ADS)

    Zhou, Zhen-Hua; Mao, Jing-Wen; Lyckberg, Peter

    2012-04-01

    The Huanggang Sn-Fe deposit, Inner Mongolia, is located in southern Great Hinggan Range metallogenic belt. LA-ICP-MS zircon U-Pb dating show that the K-feldspar granite and granite-porphyry in the Huanggang mine were formed at 136.7 ± 1.1 Ma and 136.8 ± 0.57 Ma, respectively. Sr-Nd-Pb isotope of the rocks and In situ zircon Hf isotopic systematics show that (87Sr/86Sr)i values range from 0.70211 to 0.70729, close to the (87Sr/86Sr)i of oceanic basalts and lower than those of continental crust. The ɛNd(t) values and Nd model ages (TDM) vary from -0.8 to 0.9 and 855 to 993 Ma, respectively. The Pb isotopic compositions are also variable with 206Pb/204Pb, 207Pb/204Pb and 208Pb/204Pb values of 18.974-26.107, 15.554-15.914 and 38.894-39.890, respectively, suggesting that the lead is derived from a mixed source. The 176Hf/177Hf values range from 0.282744 to 0.282922, with corresponding ɛHf(t) values ranging from 1.9 to 18.3, and two-stage Hf model ages (TDM2) of between 561 and 888 Ma. The isotope composition shows that Huanggang granites were derived from partial melting of juvenile lower crust that originated from depleted mantle, perhaps contaminated by small amounts of ancient continental crust. Younger Nd, Hf isotope model ages imply that an important crustal growth event took place in this area during the Neoproterozoic. Integrating our data with previously published results and the Late Mesozoic regional tectonic setting, we conclude that the Huanggang granites were generated in an intraplate tectonic-magmatic setting. Asthenospheric mantle upwelling due to lithospheric delamination and magma underplating, caused the partial melting of a mantle wedge metasomatized by the fluids released from subducted oceanic crust or by decompression of depleted mantle. This resulted in remelting, differentiation and a continued evolution of the mafic juvenile crust, producing a large quantity of granitic magma. The tectonic setting for these processes may be linked to the

  15. The Magnetic Observatory Buildings at the Royal Observatory, Cape

    NASA Astrophysics Data System (ADS)

    Glass, I. S.

    2015-10-01

    During the 1830s there arose a strong international movement, promoted by Carl Friedrich Gauss and Alexander von Humboldt, to characterise the earth's magnetic field. By 1839 the Royal Society in London, driven by Edward Sabine, had organised a "Magnetic Crusade" - the establishment of a series of magnetic and meteorological observatories around the British Empire, including New Zealand, Australia, St Helena and the Cape. This article outlines the history of the latter installation, its buildings and what became of them.

  16. Observatory bibliographies: a vital resource in operating an observatory

    NASA Astrophysics Data System (ADS)

    Winkelman, Sherry; Rots, Arnold

    2016-07-01

    The Chandra Data Archive (CDA) maintains an extensive observatory bibliography. By linking the published articles with the individual datasets analyzed in the paper, we have the opportunity to join the bibliographic metadata (including keywords, subjects, objects, data references from other observatories, etc.) with the meta- data associated with the observational datasets. This rich body of information is ripe for far more sophisticated data mining than the two repositories (publications and data) would afford individually. Throughout the course of the mission the CDA has investigated numerous questions regarding the impact of specific types of Chandra programs such as the relative science impact of GTO, GO, and DDT programs or observing, archive, and theory programs. Most recently the Chandra bibliography was used to assess the impact of programs based on the size of the program to examine whether the dividing line between standard and large projects should be changed and whether another round of X-ray Visionary Programs should be offered. Traditionally we have grouped observations by proposal when assessing the impact of programs. For this investigation we aggregated observations by pointing and instrument configuration such that objects observed multiple times in the mission were considered single observing programs. This change in perspective has given us new ideas for assessing the science impact of Chandra and for presenting data to our users. In this paper we present the methodologies used in the recent study, some of its results, and most importantly some unexpected insights into assessing the science impact of an observatory.

  17. Astronomical observatory for shuttle. Phase A study

    NASA Technical Reports Server (NTRS)

    Guthals, D. L.

    1973-01-01

    The design, development, and configuration of the astronomical observatory for shuttle are discussed. The characteristics of the one meter telescope in the spaceborne observatory are described. A variety of basic spectroscopic and image recording instruments and detectors which will permit a large variety of astronomical observations are reported. The stDC 37485elines which defined the components of the observatory are outlined.

  18. The Gamma-Ray Observatory

    SciTech Connect

    Kniffen, D.A. )

    1989-01-01

    The scientific goals and the design of the NASA Gamma-Ray Observatory (GRO), planned for launch in mid-1990, are described together with the experiments to be performed on the GRO mission and the instruments to be flown on the Observatory. GRO contains a complement of four instruments to span the spectrum from 0.03 to 20,000 MeV in energy, three of which are optimized to make gamma-ray observations using either the photoelectric effect, the Compton scatter, or the pair production processes; the fourth instrument is optimized for high-sensitivity observations of transient events and time-variable sources. The instruments are the Oriented Scintillation Spectrometer Experiment, the Compton Telescope, the Energetic Gamma-Ray Experiment Telescope, and the Burst and Transient Source Experiment.

  19. International Ultraviolet Explorer Observatory operations

    NASA Technical Reports Server (NTRS)

    1985-01-01

    This volume contains the final report for the International Ultraviolet Explorer IUE Observatory Operations contract. The fundamental operational objective of the International Ultraviolet Explorer (IUE) program is to translate competitively selected observing programs into IUE observations, to reduce these observations into meaningful scientific data, and then to present these data to the Guest Observer in a form amenable to the pursuit of scientific research. The IUE Observatory is the key to this objective since it is the central control and support facility for all science operations functions within the IUE Project. In carrying out the operation of this facility, a number of complex functions were provided beginning with telescope scheduling and operation, proceeding to data processing, and ending with data distribution and scientific data analysis. In support of these critical-path functions, a number of other significant activities were also provided, including scientific instrument calibration, systems analysis, and software support. Routine activities have been summarized briefly whenever possible.

  20. Boscovich and the Brera Observatory

    NASA Astrophysics Data System (ADS)

    Antonello, E.

    2013-04-01

    In the mid 18th century both theoretical and practical astronomy were cultivated in Milan by Barnabites and Jesuits. In 1763 R.G. Boscovich was appointed to the chair of mathematics of the University of Pavia in the Duchy of Milan, and the following year he designed an observatory for the Jesuit Collegium of Brera. The Specola was built in 1765 and it became quickly one of the main European observatories. We discuss the relation between Boscovich and Brera in the framework of a short biography. An account is given of the initial research activity in the Specola, of the departure of Boscovich from Milan in 1773 and his coming back just before his death.

  1. New Geophysical Observatory in Uruguay

    NASA Astrophysics Data System (ADS)

    Sanchez Bettucci, L.; Nuñez, P.; Caraballo, R. R.; Ogando, R.

    2013-05-01

    In 2011 began the installation of the first geophysical observatory in Uruguay, with the aim of developing the Geosciences. The Astronomical and Geophysical Observatory Aiguá (OAGA) is located within the Cerro Catedral Tourist Farm (-34 ° 20 '0 .89 "S/-54 ° 42 '44.72" W, h: 270m). This has the distinction of being located in the center of the South Atlantic Magnetic Anomaly. Geologically is emplaced in a Neoproterozoic basement, in a region with scarce anthropogenic interference. The OAGA has, since 2012, with a GSM-90FD dIdD v7.0 and GSM-90F Overhauser, both of GEM Systems. In addition has a super-SID receiver provided by the Stanford University SOLAR Center, as a complement for educational purposes. Likewise the installation of a seismograph REF TEK-151-120A and VLF antenna is being done since the beginning of 2013.

  2. International ultraviolet explorer observatory operations

    NASA Technical Reports Server (NTRS)

    1986-01-01

    This volume contains the Final Report for the International Ultraviolet Explorer (IUE) Observatory Operations contract, NAS5-28787. The report summarizes the activities of the IUE Observatory over the 13-month period from November 1985 through November 1986 and is arranged in sections according to the functions specified in the Statement of Work (SOW) of the contract. In order to preserve numerical correspondence between the technical SOW elements specified by the contract and the sections of this report, project management activities (SOW element 0.0.) are reported here in Section 7, following the reports of technical SOW elements 1.0 through 6.0. Routine activities have been summarized briefly whenever possible; statistical compilations, reports, and more lengthy supplementary material are contained in the Appendices.

  3. Boscovich and the Brera Observatory .

    NASA Astrophysics Data System (ADS)

    Antonello, E.

    In the mid 18th century both theoretical and practical astronomy were cultivated in Milan by Barnabites and Jesuits. In 1763 Boscovich was appointed to the chair of mathematics of the University of Pavia in the Duchy of Milan, and the following year he designed an observatory for the Jesuit Collegium of Brera in Milan. The Specola was built in 1765 and it became quickly one of the main european observatories. We discuss the relation between Boscovich and Brera in the framework of a short biography. An account is given of the initial research activity in the Specola, of the departure of Boscovich from Milan in 1773 and his coming back just before his death.

  4. The TAROT observatory data management

    NASA Astrophysics Data System (ADS)

    Bringer, M.; Boër, M.; Peignot, C.; Fontan, G.; Merce, C.

    1999-09-01

    TAROT (Tálescope a Action Rapide pour les Objets Transitoires, Rapid Action Telescope for Transient Objects) is an autonomous ground based observatory (Calern, France) whose primary goal is the rapid detection of variable objects, peculiarly optical counterparts of Gamma Ray Burst (GRB) sources. We present the observatory data management architecture which is composed of 3 main modules: The MAJORDOME module whose aim is to optimally schedule the observation requests sent to the telescope through socket connections, e-mail or even a web interface, The CONTROL module which monitors the hardware, and a data processing software TAITAR which detects, deblends, measures, classifies sources and detects variable objects by comparison with a catalogue. This paper will mainly focus on the MAJORDOME.

  5. Ny-Alesund Geodetic Observatory

    NASA Technical Reports Server (NTRS)

    Sieber, Moritz

    2013-01-01

    In 2012 the 20-m telescope at Ny-Alesund, Svalbard, operated by the Norwegian Mapping Authority (NMA), took part in 163 out of 168 scheduled sessions of the IVS program. Since spring, all data was transferred by network, and the receiver monitoring computer was replaced by a bus-coupler. In autumn, the NMA received building permission for a new observatory from the Governor of Svalbard. The bidding process and first construction work for the infrastructure will start in 2013.

  6. ESA extends solar observatory mission

    NASA Astrophysics Data System (ADS)

    Zielinski, Sarah

    2006-06-01

    The European Space Agency (ESA) announced on 24 May that it would extend the life of its Solar and Heliospheric Observatory (SOHO) from April 2007 to December 2009. Since it was launched in December 1995, SOHO has provided scientists with a view of the Sun's surface. ``This mission extension will allow SOHO to cement its position as the most important spacecraft in the history of solar physics,'' said SOHO project scientist Bernhard Fleck.

  7. SOHO (Solar and Heliospheric Observatory)

    NASA Astrophysics Data System (ADS)

    Martens, P.; Murdin, P.

    2000-11-01

    The Solar and Heliospheric Observatory (SOHO) is a project of international cooperation between ESA (the EUROPEAN SPACE AGENCY) and NASA to study the Sun, from its deep core to the outer corona, and the solar wind. SOHO was launched on 2 December 1995, on top of an Atlas/Centaur combination, from Cape Canaveral Air-Force Base in Florida. It reached its operating orbit around the L1 Sun-Earth Lagr...

  8. The Compton Gamma Ray Observatory: highlights from the first three years of the mission.

    NASA Astrophysics Data System (ADS)

    Gehrels, N.; Shrader, C.; Kniffen, D. A.

    The Arthur Holly Compton Gamma Ray observatory is the second in NASA's series of Great Observatories. It has been in operation for over three years, and has given a dramatic increase in capability over previous gamma-ray missions. The spacecraft and scientific instruments continue to function nearly flawlessly, and many significant discoveries have been made. The authors describe the capabilities of the four scientific instruments, and highlight some of the results from the first three years of the mission.

  9. STS-37 Gamma Ray Observatory (GRO) at KSC Payload Hazardous Servicing Fac

    NASA Technical Reports Server (NTRS)

    1990-01-01

    At the Kennedy Space Center (KSC) Payload Hazardous Servicing Facility, the overhead crane lifts the Gamma Ray Observatory (GRO) from its storage container. GRO, one of four NASA Great Observatories, arrived at KSC on 02-06-90 from the California plant of builder TRW. Weighing a massive 34,700 pounds, GRO will be the heaviest payload without an upper stage ever carried aboard the Space Shuttle. It is scheduled for deployment from Atlantis, Orbiter Vehicle (OV) 104, during STS-37.

  10. STS-37 Gamma Ray Observatory (GRO) at KSC Payload Hazardous Servicing Fac

    NASA Technical Reports Server (NTRS)

    1990-01-01

    Kennedy Space Center (KSC) workers at the Payload Hazardous Servicing Facility are removing the Gamma Ray Observatory (GRO) from its storage container. GRO, one of four NASA Great Observatories, arrived at KSC on 02-06-90 from the California plant of builder TRW. Weighing a massive 34,700 pounds, GRO will be the heaviest payload without an upper stage ever carried aboard the Space Shuttle. It is scheduled for deployment from Atlantis, Orbiter Vehicle (OV) 104, during STS-37.

  11. Solar initiative at Oukaimeden Observatory

    NASA Astrophysics Data System (ADS)

    Benkaldoun, Zouhair; Makela, Jonathan J.; Meriwether, John W.

    2013-07-01

    The solar research program at Oukaimeden Observatory started in 1988 with the helioseimological IRIS network. The Moroccan researchers involved in this research have analyzed solar observations in order to detect and characterize the solar sphere modes of oscillations. In the coming year, the researchers at the Oukaimeden Observatory will add new research capabilities by joining the International Space Weather Initiative (ISWI), installing a suite of optical instruments, comprising a Remote Equatorial Nighttime Observatory of Ionospheric Regions (RENOIR). The scope and objectives to be achieved in this proposed project are to: • deploy a Fabry-Perot interferometer and wide-angle imaging system to the Observatoire Astronomique Universitaire de LOukaimeden; • train students and researchers from Cadi Ayyad University on the operation of the equipment and related analysis techniques; • collect and analyze data from the equipment to study properties of upper-atmospheric winds and temperatures and how they relate to the occurrence of space weather; and • develop an international collaboration network with other researchers using similar instrumentation in Brazil and Peru. We will present here the plan we intend to develop for the Moroccan solar program in connection with ISWI.

  12. Vibration budget for observatory equipment

    NASA Astrophysics Data System (ADS)

    MacMartin, Douglas G.; Thompson, Hugh

    2015-07-01

    Vibration from equipment mounted on the telescope and in summit support buildings has been a source of performance degradation at existing astronomical observatories, particularly for adaptive optics performance. Rather than relying only on best practices to minimize vibration, we present here a vibration budget that specifies allowable force levels from each source of vibration in the observatory (e.g., pumps, chillers, cryocoolers, etc.). This design tool helps ensure that the total optical performance degradation due to vibration is less than the corresponding error budget allocation and is also useful in design trade-offs, specifying isolation requirements for equipment, and tightening or widening individual equipment vibration specifications as necessary. The vibration budget relies on model-based analysis of the optical consequences that result from forces applied at different locations and frequencies, including both image jitter and primary mirror segment motion. We develop this tool here for the Thirty Meter Telescope but hope that this approach will be broadly useful to other observatories, not only in the design phase, but for verification and operations as well.

  13. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1980-01-01

    This image of the suspected Black Hole, Cygnus X-1, was the first object seen by the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory. According to the theories to date, one concept of a black hole is a star, perhaps 10 times more massive than the Sun, that has entered the last stages of stelar evolution. There is an explosion triggered by nuclear reactions after which the star's outer shell of lighter elements and gases is blown away into space and the heavier elements in the stellar core begin to collapse upon themselves. Once this collapse begins, the inexorable force of gravity continues to compact the material until it becomes so dense it is squeezed into a mere point and nothing can escape from its extreme gravitational field, not even light. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy.

  14. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This image is an x-ray view of Eta Carinae Nebula showing bright stars taken with the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory. The Eta Carinae Nebula is a large and complex cloud of gas, crisscrossed with dark lanes of dust, some 6,500 light years from Earth. Buried deep in this cloud are many bright young stars and a very peculiar variable star. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  15. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This image is an observation of Quasar 3C 273 by the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory. It reveals the presence of a new source (upper left) with a red shift that indicates that it is about 10 billion light years away. Quasars are mysterious, bright, star-like objects apparently located at the very edge of the visible universe. Although no bigger than our solar system, they radiate as much visible light as a thousand galaxies. Quasars also emit radio signals and were previously recognized as x-ray sources. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2 was designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center.

  16. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1980-01-01

    The dramatic change in x-ray emission from the Terzan 2 cluster is shown in this series of 2.5-minute exposures taken with the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory immediately before, during, and after the burst. Total exposure (20 minutes) of the object, including the outburst, is shown in the fourth photograph. These images represent the first observation of an x-ray burst in progress. The actual burst lasted 50 seconds. Among the rarest, and most bizarre, phenomena observed by x-ray astronomers are the so-called cosmic bursters (x-ray sources that suddenly and dramatically increase in intensity then subside). These sudden bursts of intense x-ray radiation apparently come from compact objects with a diameter smaller than 30 miles (48 kilometers). Yet, despite their minuscule size, a typical x-ray burster can release more x-ray energy in a single brief burst than our Sun does in an entire week. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO was designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center.

  17. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1979-01-01

    This is an x-ray image of the Crab Nebula taken with the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory. The image is demonstrated by a pulsar, which appears as a bright point due to its pulsed x-ray emissions. The strongest region of diffused emissions comes from just northwest of the pulsar, and corresponds closely to the region of brightest visible-light emission. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  18. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1980-01-01

    This supernova in the constellation Cassiopeia was observed by Tycho Brahe in 1572. In this x-ray image from the High Energy Astronomy Observatory (HEAO-2/Einstein Observatory produced by nearly a day of exposure time, the center region appears filled with emissions that can be resolved into patches or knots of material. However, no central pulsar or other collapsed object can be seen. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  19. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1980-01-01

    This x-ray photograph of the Supernova remnant Cassiopeia A, taken with the High Energy Astronomy Observatory (HEAO) 2/Einstein Observatory, shows that the regions with fast moving knots of material in the expanding shell are bright and clear. A faint x-ray halo, just outside the bright shell, is interpreted as a shock wave moving ahead of the expanding debris. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  20. High Energy Astronomy Observatory (HEAO)

    NASA Image and Video Library

    1980-01-01

    Like the Crab Nebula, the Vela Supernova Remnant has a radio pulsar at its center. In this image taken by the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory, the pulsar appears as a point source surrounded by weak and diffused emissions of x-rays. HEAO-2's computer processing system was able to record and display the total number of x-ray photons (a tiny bundle of radiant energy used as the fundamental unit of electromagnetic radiation) on a scale along the margin of the picture. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

  1. The solar observations at Armagh Observatory in 1795-1797

    NASA Astrophysics Data System (ADS)

    Arlt, R.

    2009-04-01

    This article reports on solar observations by J.A. Hamilton and W. Gimingham at Armagh Observatory made in 1795-1797. A number of sunspot positions were obtained from the original observing notes, mostly from micrometer measurements. The period is particularly interesting for the understanding of the onset of the Dalton minimum and a possible minor cycle between the Cycles 4 and 5. For the same period, sunspot positions recorded by Staudacher were measured and published in an earlier paper.

  2. Great Britain and Ireland

    NASA Image and Video Library

    2017-09-28

    NASA image acquired March 26, 2012 This nearly cloud-free view of Great Britain and Ireland was acquired by the Moderate Resolution Imaging Spectroradiometer (MODIS) aboard NASA’s Terra satellite on March 26, 2012. Just a few days into spring, most of the land appears green, although not quite as brilliant as the summertime hues that give Ireland the nickname “the Emerald Island”. The islands of Ireland (west) and Great Britain (east) are separated by the Irish Sea, which is filled with the turquoise, green and tan swirls typical of sediment, although blooming algae could also contribute some color to the waters. To the southeast, the English Channel separates the island of Great Britain from France (south) and Belgium (north). London can be seen as a gray circle situated inland on the tan-colored River Thames. The sediment from the Thames flows into the English Channel due east of London. The United Kingdom is made up of Wales, Scotland and England, all located primarily on the island of Great Britain, and of Northern Ireland, which comprises the northern section of the island of Ireland. Dublin, in the Republic of Ireland, can be seen as a gray smudge on the eastern coast of the island. Almost due west Galway can be seen as a linear gray streak on the northern coast of Galway Bay, with the blue waters of Loch Corrib to the north. Most of the United Kingdom and Ireland are part of the Celtic broadleaf forest ecoregion, where acid-loving oak and mixed oak forests abound, along with fen and swamp forests and ombrotrophic mires. A portion of the Scottish Highlands, in the north of Great Britain, are covered by the Caledon conifer forest ecoregion. The Caledonia conifers once covered a large area of Scotland, but now only about 1% of the original forest survives, mostly high in the cooler areas of the Highlands. NASA/GSFC/Jeff Schmaltz/MODIS Land Rapid Response Team NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four

  3. McDonald Observatory Visitor Center Education Programs

    NASA Astrophysics Data System (ADS)

    Hemenway, M. K.; Armosky, B. J.; Wetzel, M.; Preston, S.

    2002-12-01

    The opening of the new Visitor Center at McDonald Observatory in Fort Davis, Texas provided an opportunity to greatly expand the Observatory's outreach efforts to students and teachers. In addition to a theater, outdoor telescope park, and amphitheater, the facility contains a classroom and an exhibit entitled ``Decoding Starlight." In preparation for the opening, new teacher-friendly materials were written to provide standards aligned (both state and national) classroom activities for students. These activities form the core for both the multi-day Professional Development Program for teachers and the Student Field Experience Program. Student Field Experiences often begin with a tour specifically designed for student groups to emphasize careers and life at the Observatory. The group then interacts with the exhibit using Exhibit Guides that were developed for various grade levels. When their schedule allows, student groups may also participate in nighttime observing activities. Smaller groups (under 30 members) may choose from a menu of hands-on activities offered within the classroom. The positive reception of these activities has led to their inclusion in the existing Elderhostel program for senior citizens. We gratefully acknowledge the support of NSF 96-26965 ``Fingerprinting the Universe - An Interactive, Bilingual Exhibit on Spectroscopy," NSF 97-05340 ``Universo, Hispanic Heritage Month Programs, and StarDate in the Classroom," and NASA IDEAS HST-ED-90234-.01 ``Enriching the Experience at McDonald Observatory: Pre/Post Visit Materials for Teachers and Students."

  4. NASA Names Premier X-Ray Observatory and Schedules Launch

    NASA Astrophysics Data System (ADS)

    1998-12-01

    NASA's Advanced X-ray Astrophysics Facility has been renamed the Chandra X-ray Observatory in honor of the late Indian-American Nobel laureate, Subrahmanyan Chandrasekhar. The telescope is scheduled to be launched no earlier than April 8, 1999 aboard the Space Shuttle Columbia mission STS-93, commanded by astronaut Eileen Collins. Chandrasekhar, known to the world as Chandra, which means "moon" or "luminous" in Sanskrit, was a popular entry in a recent NASA contest to name the spacecraft. The contest drew more than six thousand entries from fifty states and sixty-one countries. The co-winners were a tenth grade student in Laclede, Idaho, and a high school teacher in Camarillo, CA. The Chandra X-ray Observatory Center (CXC), operated by the Smithsonian Astrophysical Observatory, will control science and flight operations of the Chandra X-ray Observatory for NASA from Cambridge, Mass. "Chandra is a highly appropriate name," said Harvey Tananbaum, Director of the CXC. "Throughout his life Chandra worked tirelessly and with great precision to further our understanding of the universe. These same qualities characterize the many individuals who have devoted much of their careers to building this premier X-ray observatory." "Chandra probably thought longer and deeper about our universe than anyone since Einstein," said Martin Rees, Great Britain's Astronomer Royal. "Chandrasekhar made fundamental contributions to the theory of black holes and other phenomena that the Chandra X-ray Observatory will study. His life and work exemplify the excellence that we can hope to achieve with this great observatory," said NASA Administrator Dan Goldin. Widely regarded as one of the foremost astrophysicists of the 20th century, Chandrasekhar won the Nobel Prize in 1983 for his theoretical studies of physical processes important to the structure and evolution of stars. He and his wife immigrated from India to the U.S. in 1935. Chandrasekhar served on the faculty of the University of

  5. Great cities look small

    PubMed Central

    Sim, Aaron; Yaliraki, Sophia N.; Barahona, Mauricio; Stumpf, Michael P. H.

    2015-01-01

    Great cities connect people; failed cities isolate people. Despite the fundamental importance of physical, face-to-face social ties in the functioning of cities, these connectivity networks are not explicitly observed in their entirety. Attempts at estimating them often rely on unrealistic over-simplifications such as the assumption of spatial homogeneity. Here we propose a mathematical model of human interactions in terms of a local strategy of maximizing the number of beneficial connections attainable under the constraint of limited individual travelling-time budgets. By incorporating census and openly available online multi-modal transport data, we are able to characterize the connectivity of geometrically and topologically complex cities. Beyond providing a candidate measure of greatness, this model allows one to quantify and assess the impact of transport developments, population growth, and other infrastructure and demographic changes on a city. Supported by validations of gross domestic product and human immunodeficiency virus infection rates across US metropolitan areas, we illustrate the effect of changes in local and city-wide connectivities by considering the economic impact of two contemporary inter- and intra-city transport developments in the UK: High Speed 2 and London Crossrail. This derivation of the model suggests that the scaling of different urban indicators with population size has an explicitly mechanistic origin. PMID:26179988

  6. Great cities look small.

    PubMed

    Sim, Aaron; Yaliraki, Sophia N; Barahona, Mauricio; Stumpf, Michael P H

    2015-08-06

    Great cities connect people; failed cities isolate people. Despite the fundamental importance of physical, face-to-face social ties in the functioning of cities, these connectivity networks are not explicitly observed in their entirety. Attempts at estimating them often rely on unrealistic over-simplifications such as the assumption of spatial homogeneity. Here we propose a mathematical model of human interactions in terms of a local strategy of maximizing the number of beneficial connections attainable under the constraint of limited individual travelling-time budgets. By incorporating census and openly available online multi-modal transport data, we are able to characterize the connectivity of geometrically and topologically complex cities. Beyond providing a candidate measure of greatness, this model allows one to quantify and assess the impact of transport developments, population growth, and other infrastructure and demographic changes on a city. Supported by validations of gross domestic product and human immunodeficiency virus infection rates across US metropolitan areas, we illustrate the effect of changes in local and city-wide connectivities by considering the economic impact of two contemporary inter- and intra-city transport developments in the UK: High Speed 2 and London Crossrail. This derivation of the model suggests that the scaling of different urban indicators with population size has an explicitly mechanistic origin.

  7. Three Great Eyes on Kepler's Supernova Remnant

    NASA Technical Reports Server (NTRS)

    2004-01-01

    [figure removed for brevity, see original site] Composite

    [figure removed for brevity, see original site] [figure removed for brevity, see original site] Chandra X-Ray Data (blue) Chandra X-Ray Data (green)Hubble Telescope (visible-light)Spitzer Telescope (infrared)

    NASA's three Great Observatories -- the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory -- joined forces to probe the expanding remains of a supernova, called Kepler's supernova remnant, first seen 400 years ago by sky watchers, including astronomer Johannes Kepler.

    The combined image unveils a bubble-shaped shroud of gas and dust that is 14 light-years wide and is expanding at 4 million miles per hour (2,000 kilometers per second). Observations from each telescope highlight distinct features of the supernova remnant, a fast-moving shell of iron-rich material from the exploded star, surrounded by an expanding shock wave that is sweeping up interstellar gas and dust.

    Each color in this image represents a different region of the electromagnetic spectrum, from X-rays to infrared light. These diverse colors are shown in the panel of photographs below the composite image. The X-ray and infrared data cannot be seen with the human eye. By color-coding those data and combining them with Hubble's visible-light view, astronomers are presenting a more complete picture of the supernova remnant.

    Visible-light images from the Hubble telescope (colored yellow) reveal where the supernova shock wave is slamming into the densest regions of surrounding gas. The bright glowing knots are dense clumps from instabilities that form behind the shock wave. The Hubble data also show thin filaments of gas that look like rippled sheets seen edge-on. These filaments reveal where the shock wave is encountering lower-density, more uniform interstellar material.

    The Spitzer telescope shows microscopic dust particles (colored red) that have been heated by the

  8. Three Great Eyes on Kepler's Supernova Remnant

    NASA Technical Reports Server (NTRS)

    2004-01-01

    [figure removed for brevity, see original site] Composite

    [figure removed for brevity, see original site] [figure removed for brevity, see original site] Chandra X-Ray Data (blue) Chandra X-Ray Data (green)Hubble Telescope (visible-light)Spitzer Telescope (infrared)

    NASA's three Great Observatories -- the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory -- joined forces to probe the expanding remains of a supernova, called Kepler's supernova remnant, first seen 400 years ago by sky watchers, including astronomer Johannes Kepler.

    The combined image unveils a bubble-shaped shroud of gas and dust that is 14 light-years wide and is expanding at 4 million miles per hour (2,000 kilometers per second). Observations from each telescope highlight distinct features of the supernova remnant, a fast-moving shell of iron-rich material from the exploded star, surrounded by an expanding shock wave that is sweeping up interstellar gas and dust.

    Each color in this image represents a different region of the electromagnetic spectrum, from X-rays to infrared light. These diverse colors are shown in the panel of photographs below the composite image. The X-ray and infrared data cannot be seen with the human eye. By color-coding those data and combining them with Hubble's visible-light view, astronomers are presenting a more complete picture of the supernova remnant.

    Visible-light images from the Hubble telescope (colored yellow) reveal where the supernova shock wave is slamming into the densest regions of surrounding gas. The bright glowing knots are dense clumps from instabilities that form behind the shock wave. The Hubble data also show thin filaments of gas that look like rippled sheets seen edge-on. These filaments reveal where the shock wave is encountering lower-density, more uniform interstellar material.

    The Spitzer telescope shows microscopic dust particles (colored red) that have been heated by the

  9. Composition of the ultramafic-mafic contact interval of the Great Dyke of Zimbabwe at Ngezi mine: Comparisons to the Bushveld Complex and implications for the origin of the PGE reefs

    NASA Astrophysics Data System (ADS)

    Maier, W. D.; Määttää, S.; Yang, S.; Oberthür, T.; Lahaye, Y.; Huhma, H.; Barnes, S.-J.

    2015-12-01

    The Great Dyke contains the world's second largest platinum resource after the Bushveld Complex. Isotopic and trace element data from the interval straddling the contact between the Ultramafic and Mafic Sequences of the Great Dyke indicate a less enriched composition than in the Bushveld Complex (Great Dyke: Sri 0.7024-0.7028, εNd mostly - 1 to + 1, Ce/Sm 2-6; Bushveld: Sri 705-0.709, εNd - 5 to - 7, Ce/Sm 5-15). These data are interpreted to reflect relatively moderate amounts of contamination of the Great Dyke parent magma. All analyzed isotopes show little variation across the Main Sulfide Zone and the ultramafic-mafic contact. This corroborates earlier work by other researchers that the Great Dyke crystallized from a single magma type. Mixing of compositionally distinct magmas, proposed to have caused sulfide melt saturation in the Bushveld Complex, seemingly played little or no role in the formation of the PGE mineralization in the Main Sulfide Zone, and neither did enhanced crustal contamination of specific magma batches. Instead, sulfide melt saturation of the magma was likely triggered by silicate fractionation. The mechanism of concentration of the sulfide melt remains uncertain, but theoretical considerations suggest that phase sorting in response to slumping of crystal mushes, possibly caused by chamber subsidence, played an important role. This model is consistent with the highly irregular, undulating nature of the contact between the mafic and ultramafic zones of the intrusion, in the hanging wall of the Main Sulfide Zone.

  10. Making Kew Observatory: the Royal Society, the British Association and the politics of early Victorian science.

    PubMed

    Macdonald, Lee T

    2015-09-01

    Built in 1769 as a private observatory for King George III, Kew Observatory was taken over in 1842 by the British Association for the Advancement of Science (BAAS). It was then quickly transformed into what some claimed to be a 'physical observatory' of the sort proposed by John Herschel - an observatory that gathered data in a wide range of physical sciences, including geomagnetism and meteorology, rather than just astronomy. Yet this article argues that the institution which emerged in the 1840s was different in many ways from that envisaged by Herschel. It uses a chronological framework to show how, at every stage, the geophysicist and Royal Artillery officer Edward Sabine manipulated the project towards his own agenda: an independent observatory through which he could control the geomagnetic and meteorological research, including the ongoing 'Magnetic Crusade'. The political machinations surrounding Kew Observatory, within the Royal Society and the BAAS, may help to illuminate the complex politics of science in early Victorian Britain, particularly the role of 'scientific servicemen' such as Sabine. Both the diversity of activities at Kew and the complexity of the observatory's origins make its study important in the context of the growing field of the 'observatory sciences'.

  11. Hawaiian Volcano Observatory 1977 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  12. Hawaiian Volcano Observatory 1978 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  13. Hawaiian Volcano Observatory 1984 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  14. Hawaiian Volcano Observatory 1961 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  15. Hawaiian Volcano Observatory 1960 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  16. Hawaiian Volcano Observatory 1981 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  17. Hawaiian Volcano Observatory 1957 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  18. Hawaiian Volcano Observatory 1968 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  19. Hawaiian Volcano Observatory 1969 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  20. Hawaiian Volcano Observatory 1967 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  1. Hawaiian Volcano Observatory 1970 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  2. Hawaiian Volcano Observatory 1971 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  3. Hawaiian Volcano Observatory 1974 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  4. Hawaiian Volcano Observatory 1965 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  5. Hawaiian Volcano Observatory 1958 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  6. Hawaiian Volcano Observatory 1975 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  7. Hawaiian Volcano Observatory 1982 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  8. Hawaiian Volcano Observatory 1966 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  9. Hawaiian Volcano Observatory 1972 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  10. Hawaiian Volcano Observatory 1963 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  11. Hawaiian Volcano Observatory 1959 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  12. Hawaiian Volcano Observatory 1983 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  13. Hawaiian Volcano Observatory 1985 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  14. Hawaiian Volcano Observatory 1976 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  15. Hawaiian Volcano Observatory 1964 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  16. Hawaiian Volcano Observatory 1973 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  17. Hawaiian Volcano Observatory 1980 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  18. Hawaiian Volcano Observatory 1979 Annual Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  19. Hawaiian Volcano Observatory 1962 Quarterly Administrative Report

    USGS Publications Warehouse

    Nakata, Jennifer S.

    2007-01-01

    INTRODUCTORY NOTE The Hawaiian Volcano Observatory Summaries have been published in the current format since 1956. The Quarterly Summaries (1956 through 1973) and the Annual Summaries (1974 through 1985) were originally published as Administrative Reports. These reports have been compiled and published as U.S. Geological Survey Open-File Reports. The quarterly reports have been combined and published as one annual summary. All the summaries from 1956 to the present are now available as .pdf files at http://www.usgs.gov/pubprod. The earthquake summary data are presented as a listing of origin time, depth, magnitude, and other location parameters. Network instrumentation, field station sites, and location algorithms are described. Tilt and other deformation data are included until Summary 77, January to December 1977. From 1978, the seismic and deformation data are published separately, due to differing schedules of data reduction. There are eight quarters - from the fourth quarter of 1959 to the third quarter of 1961 - that were never published. Two of these (4th quarter 1959, 1st quarter 1960) have now been published, using handwritten notes of Jerry Eaton (HVO seismologist at the time) and his colleagues. The seismic records for the remaining six summaries went back to California in 1961 with Jerry Eaton. Other responsibilities intervened, and the seismic summaries were never prepared.

  20. The Pierre Auger Observatory status and latest results

    NASA Astrophysics Data System (ADS)

    Berat, Corinne

    2017-03-01

    The Pierre Auger Observatory, in Argentina, is the present flagship experiment studying ultrahigh-energy cosmic rays (UHECRs). Facing the challenge due to low cosmic-ray flux at the highest energies, the Observatory has been taking data for more than a decade, reaching an exposure of over 50 000 km2 sr yr. The combination of a large surface detector array and fluorescence telescopes provides a substantial improvement in energy calibration and extensive air shower measurements, resulting in data of unprecedented quality. Moreover, the installation of a denser subarray has allowed extending the sensitivity to lower energies. Altogether, this contributes to provide important information on key questions in the UHECR field in the energy range from 0.1 EeV up to 100 EeV. A review of main results from the Pierre Auger Observatory is presented with a particular focus on the energy spectrum measurements, the mass composition studies, the arrival directions analyses, the search for neutral cosmic messengers, and the investigation of high-energy hadronic interactions. Despite this large amount of valuable results, the understanding of the nature of UHECRs and of their origin remains an open science case that the Auger collaboration is planning to address with the AugerPrime project to upgrade the Observatory.

  1. The Pierre Auger Observatory status and the AugerPrime upgrade program

    NASA Astrophysics Data System (ADS)

    Martello, Daniele

    2017-06-01

    The nature and the origin of ultra-high energy cosmic rays (UHECRs), above 1017 eV, are still unknown. The Pierre Auger Observatory with its huge exposure provides us with a large set of high quality data. The analysis of these data has led to major breakthroughs in the last decade, but a coherent interpretation is still missing. To answer the open questions the Observatory has started a major upgrade, with an emphasis on improved mass composition determination using the surface detectors. The latest results and the planned detector upgrade will be presented. The expected performance and the improved physics sensitivity of the Observatory will be discussed.

  2. The Arecibo Observatory Space Academy

    NASA Astrophysics Data System (ADS)

    Rodriguez-Ford, Linda A.; Zambrano-Marin, Luisa; Petty, Bryan M.; Sternke, Elizabeth; Ortiz, Andrew M.; Rivera-Valentin, Edgard G.

    2015-11-01

    The Arecibo Observatory Space Academy (AOSA) is a ten (10) week pre-college research program for students in grades 9-12. Our mission is to prepare students for academic and professional careers by allowing them to receive an independent and collaborative research experience on topics related to space and aide in their individual academic and social development. Our objectives are to (1) Supplement the student’s STEM education via inquiry-based learning and indirect teaching methods, (2) Immerse students in an ESL environment, further developing their verbal and written presentation skills, and (3) To foster in every student an interest in science by exploiting their natural curiosity and knowledge in order to further develop their critical thinking and investigation skills. AOSA provides students with the opportunity to share lectures with Arecibo Observatory staff, who have expertise in various STEM fields. Each Fall and Spring semester, selected high school students, or Cadets, from all over Puerto Rico participate in this Saturday academy where they receive experience designing, proposing, and carrying out research projects related to space exploration, focusing on four fields: Physics/Astronomy, Biology, Engineering, and Sociology. Cadets get the opportunity to explore their topic of choice while practicing many of the foundations of scientific research with the goal of designing a space settlement, which they present at the NSS-NASA Ames Space Settlement Design Contest. At the end of each semester students present their research to their peers, program mentors, and Arecibo Observatory staff. Funding for this program is provided by NASA SSERVI-LPI: Center for Lunar Science and Exploration with partial support from the Angel Ramos Visitor Center through UMET and management by USRA.

  3. The CEOS Recovery Observatory Pilot

    NASA Astrophysics Data System (ADS)

    Hosford, S.; Proy, C.; Giros, A.; Eddy, A.; Petiteville, I.; Ishida, C.; Gaetani, F.; Frye, S.; Zoffoli, S.; Danzeglocke, J.

    2015-04-01

    Over the course of the last decade, large populations living in vulnerable areas have led to record damages and substantial loss of life in mega-disasters ranging from the deadly Indian Ocean tsunami of 2004 and Haiti earthquake of 2010; the catastrophic flood damages of Hurricane Katrina in 2005 and the Tohoku tsunami of 2011, and the astonishing extent of the environmental impact of the Deepwater Horizon explosion in 2009. These major catastrophes have widespread and long-lasting impacts with subsequent recovery and reconstruction costing billions of euros and lasting years. While satellite imagery is used on an ad hoc basis after many disasters to support damage assessment, there is currently no standard practice or system to coordinate acquisition of data and facilitate access for early recovery planning and recovery tracking and monitoring. CEOS led the creation of a Recovery Observatory Oversight Team, which brings together major recovery stakeholders such as the UNDP and the World Bank/Global Facility for Disaster Reduction and Recovery, value-adding providers and leading space agencies. The principal aims of the Observatory are to: 1. Demonstrate the utility of a wide range of earth observation data to facilitate the recovery and reconstruction phase following a major catastrophic event; 2. Provide a concrete case to focus efforts in identifying and resolving technical and organizational obstacles to facilitating the visibility and access to a relevant set of EO data; and 3. Develop dialogue and establish institutional relationships with the Recovery phase user community to best target data and information requirements; The paper presented here will describe the work conducted in preparing for the triggering of a Recovery Observatory including support to rapid assessments and Post Disaster Needs Assessments by the EO community.

  4. The Orbiting Carbon Observatory (OCO)

    NASA Technical Reports Server (NTRS)

    Miller, Charles E.

    2005-01-01

    CO2 is the principal human generated driver of climate change. Accurate forecasting of future climate requires an improved understanding of the global carbon cycle and its interaction with the climate system. The Orbiting Carbon Observatory (OCO) will make global, space-based observations of atmospheric CO2 with the precision, resolution, and coverage needed to understand sources and sinks. OCO data will provide critical information for decision makers including the scientific basis for policy formulation, guide for carbon management strategies and treaty monitoring.

  5. Gamma ray observatory productivity showcase

    NASA Technical Reports Server (NTRS)

    Davis, R. L.; Molgaard, D. A.

    1985-01-01

    The Gamma Ray Observatory (GRO) Program has been proclaimed to be the showcase productivity program for NASA and TRW. Among the multiple disciplines of a large-scale program, there is opportunity and need for improved efficiency, effectiveness, and reduction in the cost of doing business. The efforts and tools that will or have been implemented to achieve this end are described. Since the GRO Program is mainly an engineering program with the build of one satellite, the primary emphasis is placed on improving the efficiency and quality of management and engineering.

  6. Light pollution around Tonantzintla Observatory

    NASA Astrophysics Data System (ADS)

    Vázquez-Mata, José A.; Hernández-Toledo, Héctor M.; Martínez-Vázquez, Luis A.; Pani-Cielo, Atanacio

    2011-06-01

    Being close to the cities of Puebla to east and Cholula to the north, both having potential for large growth, the National Astronomical Observatory in Tonantzintla (OAN-Tonantzintla) faces the danger of deteriorating its sky conditions even more. In order to maintain competitiveness for education and scientific programs, it is important to preserve the sky brightness conditions. through: 1) our awareness of the night sky characteristics in continuous monitoring campaigns, doing more measurements over the next years to monitor changes and 2) encouraging local authorities about the need to regulate public lighting at the same time, showing them the benefits of such initiatives when well planed and correctly implemented.

  7. the Large Aperture GRB Observatory

    SciTech Connect

    Bertou, Xavier

    2009-04-30

    The Large Aperture GRB Observatory (LAGO) aims at the detection of high energy photons from Gamma Ray Bursts (GRB) using the single particle technique (SPT) in ground based water Cherenkov detectors (WCD). To reach a reasonable sensitivity, high altitude mountain sites have been selected in Mexico (Sierra Negra, 4550 m a.s.l.), Bolivia (Chacaltaya, 5300 m a.s.l.) and Venezuela (Merida, 4765 m a.s.l.). We report on the project progresses and the first operation at high altitude, search for bursts in 6 months of preliminary data, as well as search for signal at ground level when satellites report a burst.

  8. Stratospheric Observatory for Infrared Astronomy

    NASA Technical Reports Server (NTRS)

    Becklin, Eric E.

    2001-01-01

    The joint U.S. and German SOFIA project to develop and operate a 2.5-meter infrared airborne telescope in a Boeing 747-SP is now well into development. First science flights will begin in 2004 with 20% of the observing time assigned to German investigators. The observatory is expected to operate for over 20 years. The sensitivity, characteristics and science instrument complement are discussed. Present and future instrumentation will allow unique astrobiology experiments to be carried out. Several experiments related to organic molecules in space will be discussed.

  9. The Virtual Heliospheric Observatory (VHO)

    NASA Technical Reports Server (NTRS)

    Szabo, A.; Narock, T.

    2005-01-01

    Based on the experience gained through the development of the distributed L1 data environment for magnetic field and solar wind plasma observations from ACE, WIND, SOHO and Genesis, a Virtual Heliospheric Observatory (VHO) proposal was submitted to the NASA VxO opportunity. This presentation will detail what specific architecture and methods will be implemented for VHO, should this proposal be funded. Also, examples will be given how typical users will be able to take advantage the rich VHO feature set. Finally, the envisioned method of query exchange between VHO and other VxOs will be discussed.

  10. Reading the Cosmic Landscape: An Observatory in the Nevada Desert

    NASA Astrophysics Data System (ADS)

    McDonald, Hilary Jane

    This thesis aims to restore value to the phenomenological experience of the desert through architecture, exploring the desert as a physical, cultural and experiential landscape that ideally lends itself to the study of astronomy and to a greater understanding of a universal order. This project will create a recreational observatory allowing amateur observers to study the skies. The observatory will be located on the desert peak of Mount Washington, located in Great Basin National Park in Nevada. It will provide a venue for the astronomy-focused activities which already exist within the park, and will serve as a destination highlighting the cosmic properties of the desert. This thesis proposes that architecture can play a role in realizing the essential qualities of this unique landscape and can enhance the study of astronomy as an endeavor that goes beyond science to access a greater understanding of the human condition.

  11. Exploring the Digital Universe with Europe's Astrophysical Virtual Observatory

    NASA Astrophysics Data System (ADS)

    2001-12-01

    N° 73-2001 - Paris, 5 December 2001 The aim of AVO is to give astronomers instant access to the vast databanks now being built up by the world's observatories and forming what is in effect a "digital sky". Using AVO astronomers will be able, for example, to retrieve the elusive traces of the passage of an asteroid as it passes the Earth and so predict its future path and perhaps warn of a possible impact. When a giant star comes to the end of its life in a cataclysmic explosion called a supernova, they will be able to access the digital sky and pinpoint the star shortly before it exploded, adding invaluable data to the study of the evolution of stars. Modern observatories observe the sky continuously and data accumulates remorselessly in the digital archives. The growth rate is impressive and many hundreds of terabytes of data -corresponding to many thousands of billions of pixels - are already available to scientists. The real sky is being digitally reconstructed in the databanks. The volume and complexity of data and information available to astronomers are overwhelming. Hence the problem of how astronomers can possibly manage, distribute and analyse this great wealth of data. The Astrophysical Virtual Observatory will enable them to meet the challenge and "put the Universe online". AVO is a three-year project, funded by the European Commission under its Research and Technological Development (RTD) scheme, to design and implement a virtual observatory for the European astronomical community. The Commission has awarded a contract valued at EUR 4m for the project, starting on 15 November. AVO will provide software tools to enable astronomers to access the multi-wavelength data archives over the Internet and so give them the capability to resolve fundamental questions about the Universe by probing the digital sky. Equivalent searches of the "real" sky would, in comparison, both be prohibitively costly and take far too long. Towards a Global Virtual Observatory The

  12. ``Route of astronomical observatories'' project: Classical observatories from the Renaissance to the rise of astrophysics

    NASA Astrophysics Data System (ADS)

    Wolfschmidt, Gudrun

    2016-10-01

    Observatories offer a good possibility for serial transnational applications. For example one can choose groups like baroque or neoclassical observatories, solar physics observatories or a group of observatories equipped with the same kind of instruments or made by famous firms. I will discuss what has been achieved and show examples, like the route of astronomical observatories, the transition from classical astronomy to modern astrophysics. I will also discuss why the implementation of the World Heritage & Astronomy initiative is difficult and why there are problems to nominate observatories for election in the national tentative lists.

  13. Review of "Great Teachers and Great Leaders"

    ERIC Educational Resources Information Center

    Shaker, Paul

    2010-01-01

    "Great Teachers and Great Leaders" (GTGL) is one of six research summaries issued by the U.S. Department of Education in support of its Blueprint for Reform. This review examines the presentation of research about improving teacher and administrator quality in GTGL. The review concludes that there are serious flaws in the research summary. The…

  14. Taking Charge: Walter Sydney Adams and the Mount Wilson Observatory

    NASA Astrophysics Data System (ADS)

    Brashear, R.

    2004-12-01

    The growing preeminence of American observational astronomy in the first half of the 20th century is a well-known story and much credit is given to George Ellery Hale and his skill as an observatory-building entrepreneur. But a key figure who has yet to be discussed in great detail is Walter Sydney Adams (1876-1956), Hale's Assistant Director at Mount Wilson Observatory. Due to Hale's illnesses, Adams was Acting Director for much of Hale's tenure, and he became the second Director of Mount Wilson from 1923 to 1946. Behind his New England reserve Adams was instrumental in the growth of Mount Wilson and thus American astronomy in general. Adams was hand-picked by Hale to take charge of stellar spectroscopy work at Yerkes and Mount Wilson and the younger astronomer showed tremendous loyalty to Hale and Hale's vision throughout his career. As Adams assumed the leadership role at Mount Wilson he concentrated on making the observatory a place where researchers worked with great freedom but maintain a high level of cooperation. This paper will concentrate on Adams's early years and look at his growing relationship with Hale and how he came to be the central figure in the early history of Mount Wilson as both a solar and stellar observatory. His education, his years at Dartmouth and Yerkes (including his unfortunate encounter with epsilon Leonis), and his formative years on Mount Wilson are all important in learning how he shaped the direction of Mount Wilson and the development of American astronomy in the first half of the 20th century. This latter history cannot be complete until we bring Adams into better focus.

  15. Protection of the Guillermo Haro Astrophysical Observatory

    NASA Astrophysics Data System (ADS)

    Carrasco, E.; Carraminana, A. P.

    The Guillermo Haro Astrophysical Observatory, with a 2m telescope, is one of only two professional observatories in Mexico. The observatory, run by the InstitutoNacional de Astrofisica, Optica y Electronica (INAOE), is located in the north of Mexico, in Cananea, Sonora. Since 1995 the observatory has faced the potential threat of pollution by an open cast mine to be opened at 3kms from the observatory. In the absence of national or regional laws enforcing protection to astronomical sites in Mexico, considerable effort has been needed to guarantee the conditions of the site. We present the studies carried out to ensure the protection of the Guillermo Haro Observatory from pollution due to dust, light and vibrations.

  16. Cosmology in the Bucharest Observatory

    NASA Astrophysics Data System (ADS)

    Suran, Marian Doru

    2008-09-01

    At the Bucharest Observatory cosmology started in the early'80s as a theoretical branch directly related to the computational facilities available in our Observatory. With the help of our instruments, from a small Z8080 computer (early'80s) to a superscalar supercomputer of 44 processors (now), our cosmology team has developed models, methods and techniques related to: the investigation of 2D and 3D catalogues of galaxies, clusters and superclusters; investigation of the log tails of the 2-points correlation functions; cosmological simulations (N-body+SPH) of the Large Scale Structure of the Universe (LSS) investigation of environmental effects in clusters of galaxies; application of neural methods in cosmology. The use of such models and techniques has permitted us to study problems concerning: correlated signals in the long tail of the correlation functions for galaxies, clusters and superclusters (due to baryon oscillations) HD simulations of the LSS and of the evolution of the first and secondary Web structures; studies of the epochs of the formation of DM halos in a LCDM scenario (earlier than z 15) studies of the evolution of halos and galaxies due to the parental merging phenomena; detection of the Butcher-Oemler and Oemler-Butcher effects in far or close clusters; studies of E+A galaxies; study of the synthetic spectra of galaxies and of the chemo-spectro-photometrical evolution of galaxies (for z<30) photometric redshift determination (for z<10).

  17. History of Chandra X-Ray Observatory

    NASA Image and Video Library

    1999-07-01

    A crew member of the STS-93 mission took this photograph of the Chandra X-Ray Observatory, still attached to the Inertial Upper Stage (IUS), backdropped against the darkness of space not long after its release from Orbiter Columbia. Two firings of an attached IUS rocket placed the Observatory into its working orbit. The primary duty of the crew of this mission was to deploy the 50,162-pound Observatory, the world's most powerful x-ray telescope.

  18. SOFIA Observatory Obtains 'First Light' Images

    NASA Image and Video Library

    NASA's Stratospheric Observatory for Infrared Astronomy, or SOFIA, successfully obtained its "First Light"" images during an overnight flight May 26. Scientists are now processing the data gathered...

  19. The Stratospheric Observatory for Infrared Astronomy (SOFIA)

    NASA Astrophysics Data System (ADS)

    Becklin, Eric

    2015-08-01

    The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), a 2.5-meter infrared airborne telescope in a Boeing 747SP, is now fully operational with cameras and spectrometers in the 1 to 240 micron region. It will be one of the major observatories for the next 20 years to observe the local ISM in this spectral region. We will give a brief overview of the SOFIA observatory, telescope, instrumentation and recent science. Future observing opportunities and participation in future instrument developments, over the lifetime of the SOFIA observatory will be discussed.

  20. Byurakan Astrophysical Observatory as Cultural Centre

    NASA Astrophysics Data System (ADS)

    Mickaelian, A. M.; Farmanyan, S. V.

    2017-07-01

    NAS RA V. Ambartsumian Byurakan Astrophysical Observatory is presented as a cultural centre for Armenia and the Armenian nation in general. Besides being scientific and educational centre, the Observatory is famous for its unique architectural ensemble, rich botanical garden and world of birds, as well as it is one of the most frequently visited sightseeing of Armenia. In recent years, the Observatory has also taken the initiative of the coordination of the Cultural Astronomy in Armenia and in this field, unites the astronomers, historians, archaeologists, ethnographers, culturologists, literary critics, linguists, art historians and other experts. Keywords: Byurakan Astrophysical Observatory, architecture, botanic garden, tourism, Cultural Astronomy.

  1. NASA capabilities roadmap: advanced telescopes and observatories

    NASA Technical Reports Server (NTRS)

    Feinberg, Lee D.

    2005-01-01

    The NASA Advanced Telescopes and Observatories (ATO) Capability Roadmap addresses technologies necessary for NASA to enable future space telescopes and observatories collecting all electromagnetic bands, ranging from x-rays to millimeter waves, and including gravity-waves. It has derived capability priorities from current and developing Space Missions Directorate (SMD) strategic roadmaps and, where appropriate, has ensured their consistency with other NASA Strategic and Capability Roadmaps. Technology topics include optics; wavefront sensing and control and interferometry; distributed and advanced spacecraft systems; cryogenic and thermal control systems; large precision structure for observatories; and the infrastructure essential to future space telescopes and observatories.

  2. Solar Dynamics Observatory Launch and Commissioning

    NASA Technical Reports Server (NTRS)

    O'Donnell, James R., Jr.; Kristin, D.; Bourkland, L.; Hsu, Oscar C.; Liu, Kuo-Chia; Mason, Paul A. C.; Morgenstern, Wendy M.; Russo, Angela M.; Starin, Scott R.; Vess, Melissa F.

    2011-01-01

    The Solar Dynamics Observatory (SDO) was launched on February 11, 2010. Over the next three months, the spacecraft was raised from its launch orbit into its final geosynchronous orbit and its systems and instruments were tested and calibrated in preparation for its desired ten year science mission studying the Sun. A great deal of activity during this time involved the spacecraft attitude control system (ACS); testing control modes, calibrating sensors and actuators, and using the ACS to help commission the spacecraft instruments and to control the propulsion system as the spacecraft was maneuvered into its final orbit. This paper will discuss the chronology of the SDO launch and commissioning, showing the ACS analysis work performed to diagnose propellant slosh transient and attitude oscillation anomalies that were seen during commissioning, and to determine how to overcome them. The simulations and tests devised to demonstrate correct operation of all onboard ACS modes and the activities in support of instrument calibration will be discussed and the final maneuver plan performed to bring SDO on station will be shown. In addition to detailing these commissioning and anomaly resolution activities, the unique set of tests performed to characterize SDO's on-orbit jitter performance will be discussed.

  3. History of Chandra X-Ray Observatory

    NASA Image and Video Library

    1999-01-01

    This Chandra X-Ray Observatory image of the mysterious superstar Eta Carinae reveals a surprising hot irner core, creating more questions than answers for astronomers. The image shows three distinct structures: An outer, horseshoe shaped ring about 2 light-years in diameter, a hot inner core about 3 light-months in diameter, and a hot central source less than a light-month in diameter which may contain the superstar. In 1 month, light travels a distance of approximately 489 billion miles (about 788 billion kilometers). All three structures are thought to represent shock waves produced by matter rushing away from the superstar at supersonic speeds. The temperature of the shock-heated gas ranges from 60 million degrees Kelvin in the central regions to 7 million degrees Kelvin on the outer structure. Eta Carinae is one of the most enigmatic and intriguing objects in our galaxy. Between 1837 and 1856, it increased dramatically in brightness to become the most prominent star in the sky except for Sirius, even through it is 7,500 light-years away, more than 80 times the distance to Sirius. This "Great Eruption," as it is called, had an energy comparable to a supernova, yet did not destroy the star, which faded to become a dim star, invisible to the naked eye. Since 1940, Eta Carinae has begun to brighten again, becoming visible to the naked eye. Photo credit: NASA/CXC/SAO

  4. Astronomical Research with the MicroObservatory Net

    NASA Astrophysics Data System (ADS)

    Brecher, K.; Sadler, P.; Gould, R.; Leiker, S.; Antonucci, P.; Deutsch, F.

    1997-05-01

    We have developed a fully integrated automated astronomical telescope system which combines the imaging power of a cooled CCD, with a self-contained and weatherized 15 cm reflecting optical telescope and mount. The MicroObservatory Net consists of five of these telescopes. They are currently being deployed around the world at widely distributed longitudes. Remote access to the MicroObservatories over the Internet has now been implemented. Software for computer control, pointing, focusing, filter selection as well as pattern recognition have all been developed as part of the project. The telescopes can be controlled in real time or in delay mode, from a Macintosh, PC or other computer using Web-based software. The Internet address of the telescopes is http://cfa- www.harvard.edu/cfa/sed/MicroObservatory/MicroObservatory.html. In the real-time mode, individuals have access to all of the telescope control functions without the need for an `on-site' operator. Users can sign up for a specific period of ti me. In the batch mode, users can submit requests for delayed telescope observations. After a MicroObservatory completes a job, the user is automatically notified by e-mail that the image is available for viewing and downloading from the Web site. The telescopes were designed for classroom instruction, as well as for use by students and amateur astronomers for original scientific research projects. We are currently examining a variety of technical and educational questions about the use of the telescopes including: (1) What are the best approaches to scheduling real-time versus batch mode observations? (2) What criteria should be used for allocating telescope time? (3) With deployment of more than one telescope, is it advantageous for each telescope to be used for just one type of observation, i.e., some for photometric use, others for imaging? And (4) What are the most valuable applications of the MicroObservatories in astronomical research? Support for the MicroObservatory

  5. Status and perspectives of the Pierre Auger cosmic ray observatory

    NASA Astrophysics Data System (ADS)

    Argirò, Stefano

    The problem of the origin of Ultra High Energy Cosmic Rays, that is those with an energy of the Primary above 1019 eV, is a challenging one. The expected flux at those energies is around 1/yr/km2, thus requiring an unprecedented size of the detector in order to achieve consistent statistics. The Pierre Auger Observatory will be the largest cosmic ray detector ever built, consisting of two sites, one for each hemisphere, equipped with 1600 water Cherenkov detectors and four fluorescence detectors, covering each 3000 km 2. The combination of the two techniques, referred to as the hybrid technique, results in unprecedented accuracy in the reconstruction of the air showers. The concept has been validated with an Engineering Array of 32 water tanks and two fluorescence telescopes, during which the apparatus demonstrated very good performances. This paper will summarize the features of the data, the reconstruction methods and the strategy toward completion of the full Observatory.

  6. EUSO angular resolution based on Pierre Auger Observatory reconstruction methodology

    NASA Astrophysics Data System (ADS)

    Painter, William

    2015-04-01

    Ultra high energy cosmic rays (UHECRs) are astro-particles with energies above 1018 eV and are a readily detected phenomena. Their origin is yet undetermined due to the exceedingly low flux, 1 particle per km2 per century at 1020 eV. The proposed Extreme Universe Space Observatory (EUSO) utilizes the bottom 20 km of the atmosphere as a detection volume resulting in a detection area of nearly 150 , 000 km2 in nadir mode. We have developed an UHECR angular reconstruction algorithm based on the methodology developed at the Pierre Auger Observatory. This algorithm shows improved angular resolution over previous EUSO methods and has been applied to simulated showers over the expected energy and zenith angle ranges. William Painter with Dr. Fred Sarazin.

  7. The Role of Project Science in the Chandra X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    O'Dell, Stephen L.; Weisskopf, Martin C.

    2006-01-01

    The Chandra X-Ray Observatory, one of NASA's Great Observatories, has an outstanding record of scientific and technical success. This success results from the efforts of a team comprising NASA, its contractors, the Smithsonian Astrophysical Observatory, the instrument groups, and other elements of the scientific community, including thousands of scientists who utilize this powerful facility for astrophysical research. We discuss the role of NASA Project Science in the formulation, development, calibration, and operation of the Chandra X-ray Observatory. In addition to representing the scientific community within the Project, Project Science performed what we term "science systems engineering". This activity encompasses translation of science requirements into technical requirements and assessment of the scientific impact of programmatic and technical trades. We briefly describe several examples of science systems engineering conducted by Chandra Project Science.

  8. The role of project science in the Chandra X-ray Observatory

    NASA Astrophysics Data System (ADS)

    O'Dell, Stephen L.; Weisskopf, Martin C.

    2006-06-01

    The Chandra X-ray Observatory, one of NASA's Great Observatories, has an outstanding record of scientific and technical success. This success results from the efforts of a team comprising NASA, its contractors, the Smithsonian Astrophysical Observatory, the instrument groups, and other elements of the scientific community-including the thousands of scientists who utilize this powerful facility for astrophysical research. We discuss the role of NASA Project Science in the formulation, development, calibration, and operation of the Chandra X-ray Observatory. In addition to serving as an interface between the scientific community and the Project, Project Science performed what we term "science systems engineering". This activity encompasses translation of science requirements into technical requirements and assessment of the scientific impact of programmatic and technical trades. We briefly describe several examples of science systems engineering conducted by Chandra Project Science.

  9. The Role of Project Science in the Chandra X-Ray Observatory

    NASA Technical Reports Server (NTRS)

    O'Dell, Stephen L.; Weisskopf, Martin C.

    2006-01-01

    The Chandra X-Ray Observatory, one of NASA's Great Observatories, has an outstanding record of scientific and technical success. This success results from the efforts of a team comprising NASA, its contractors, the Smithsonian Astrophysical Observatory, the instrument groups, and other elements of the scientific community, including thousands of scientists who utilize this powerful facility for astrophysical research. We discuss the role of NASA Project Science in the formulation, development, calibration, and operation of the Chandra X-ray Observatory. In addition to representing the scientific community within the Project, Project Science performed what we term "science systems engineering". This activity encompasses translation of science requirements into technical requirements and assessment of the scientific impact of programmatic and technical trades. We briefly describe several examples of science systems engineering conducted by Chandra Project Science.

  10. Virtual Energetic Particle Observatory (VEPO)

    NASA Technical Reports Server (NTRS)

    Cooper, John F.; Lal, Nand; McGuire, Robert E.; Szabo, Adam; Narock, Thomas W.; Armstrong, Thomas P.; Manweiler, Jerry W.; Patterson, J. Douglas; Hill, Matthew E.; Vandergriff, Jon D.; McKibben, Robert B.; Lopate, Clifford; Tranquille, Cecil

    2008-01-01

    The Virtual Energetic Particle Observatory (VEPO) focuses on improved discovery, access, and usability of heliospheric energetic particle and ancillary data products from selected spacecraft and sub-orbital instruments of the heliophysics data environment. The energy range of interest extends over the full range of particle acceleration from keV energies of suprathermal seed particles to GeV energies of galactic cosmic ray particles. Present spatial coverage is for operational and legacy spacecraft operating from the inner to the outer heliosphere, e.g. from measurements by the two Helios spacecraft to 0.3 AU to the inner heliosheath region now being traversed by the two Voyager spacecraft. This coverage will eventually be extended inward to ten solar radii by the planned NASA solar probe mission and at the same time beyond the heliopause into the outer heliosheath by continued Voyager operations. The geospace fleet of spacecraft providing near-Earth interplanetary measurements, selected magnetospheric spacecraft providing direct measurements of penetrating interplanetary energetic particles, and interplanetary cruise measurements from planetary spacecraft missions further extend VEPO resources to the domain of geospace and planetary interactions. Ground-based (e.g., neutron monitor) and high-altitude suborbital measurements can expand coverage to the highest energies of galactic cosmic rays affected by heliospheric interaction and of solar energetic particles. Science applications include investigation of solar flare and coronal mass ejection events. acceleration and transport of interplanetary particles within the inner heliosphere, cosmic ray interactions with planetary surfaces and atmospheres, sources of suprathermal and anomalous cosmic ray ions in the outer heliosphere, and solar cycle modulation of galactic cosmic rays. Robotic and human exploration, and eventual habitation, of planetary and space environments beyond the Earth require knowledge of radiation

  11. Virtual Energetic Particle Observatory (VEPO)

    NASA Technical Reports Server (NTRS)

    Cooper, John F.; Lal, Nand; McGuire, Robert E.; Szabo, Adam; Narock, Thomas W.; Armstrong, Thomas P.; Manweiler, Jerry W.; Patterson, J. Douglas; Hill, Matthew E.; Vandergriff, Jon D.; hide

    2008-01-01

    The Virtual Energetic Particle Observatory (VEPO) focuses on improved discovery, access, and usability of heliospheric energetic particle and ancillary data products from selected spacecraft and sub-orbital instruments of the heliophysics data environment. The energy range of interest extends over the full range of particle acceleration from keV energies of suprathermal seed particles to GeV energies of galactic cosmic ray particles. Present spatial coverage is for operational and legacy spacecraft operating from the inner to the outer heliosphere, e.g. from measurements by the two Helios spacecraft to 0.3 AU to the inner heliosheath region now being traversed by the two Voyager spacecraft. This coverage will eventually be extended inward to ten solar radii by the planned NASA solar probe mission and at the same time beyond the heliopause into the outer heliosheath by continued Voyager operations. The geospace fleet of spacecraft providing near-Earth interplanetary measurements, selected magnetospheric spacecraft providing direct measurements of penetrating interplanetary energetic particles, and interplanetary cruise measurements from planetary spacecraft missions further extend VEPO resources to the domain of geospace and planetary interactions. Ground-based (e.g., neutron monitor) and high-altitude suborbital measurements can expand coverage to the highest energies of galactic cosmic rays affected by heliospheric interaction and of solar energetic particles. Science applications include investigation of solar flare and coronal mass ejection events. acceleration and transport of interplanetary particles within the inner heliosphere, cosmic ray interactions with planetary surfaces and atmospheres, sources of suprathermal and anomalous cosmic ray ions in the outer heliosphere, and solar cycle modulation of galactic cosmic rays. Robotic and human exploration, and eventual habitation, of planetary and space environments beyond the Earth require knowledge of radiation

  12. Sensor networks for cabled ocean observatories

    NASA Astrophysics Data System (ADS)

    Howe, B. M.; McGinnis, T.; Kirkham, H.

    2003-04-01

    This paper considers the development of a support infrastructure for subsea observatory sensors and networks. Some sensors will be self-contained individual items, others will be part of a sensor network using, for example, secondary cables and junction boxes to extend the horizontal reach 10s to 100s of km from backbone nodes, or using moorings to distribute observatory capabilities throughout the water column and (equivalently) down boreholes into the crust. Included in the support infrastructure could be acoustic navigation and communications systems, free-swimming AUVs, and bottom rovers that could carry sensors and could provide data and energy "tanker" service. Because of the likely long term observatory application of sensors, and the high cost of access, methods of self-calibration of sensors will also be useful. The sensor infrastructure would supplement the observatory infrastructure that is part of the NSF Ocean Observatories Initiative (OOI). This Initiative plans to provide junction box nodes on the seafloor that furnish power and communications, and distribute time. There are three elements of the OOI: a regional scale cabled observatory (such as NEPTUNE) with dozens of nodes; a sparse global array of buoys with seafloor nodes; and an expanded system of coastal observatories. Each of these observatories will depend on suites of sensors from a number of investigators, and it is likely that once the observatory infrastructure itself has been installed and commissioned, most of the physical interaction with an observatory will be for installing, operating, servicing, and recovering sensors. These activities will be supported by the proposed infrastructure, enabling the full potential of the observatory to be reached.

  13. Goddard Geophysical and Astronomical Observatory

    NASA Technical Reports Server (NTRS)

    Figueroa, Ricardo

    2013-01-01

    This report summarizes the technical parameters and the technical staff of the VLBI system at the fundamental station GGAO. It also gives an overview about the VLBI activities during the report year. The Goddard Geophysical and Astronomical Observatory (GGAO) consists of a 5-meter radio telescope for VLBI, a new 12-meter radio telescope for VLBI2010 development, a 1-meter reference antenna for microwave holography development, an SLR site that includes MOBLAS-7, the NGSLR development system, and a 48" telescope for developmental two-color Satellite Laser Ranging, a GPS timing and development lab, a DORIS system, meteorological sensors, and a hydrogen maser. In addition, we are a fiducial IGS site with several IGS/IGSX receivers. GGAO is located on the east coast of the United States in Maryland. It is approximately 15 miles NNE of Washington, D.C. in Greenbelt, Maryland.

  14. Autonomous Infrastructure for Observatory Operations

    NASA Astrophysics Data System (ADS)

    Seaman, R.

    This is an era of rapid change from ancient human-mediated modes of astronomical practice to a vision of ever larger time domain surveys, ever bigger "big data", to increasing numbers of robotic telescopes and astronomical automation on every mountaintop. Over the past decades, facets of a new autonomous astronomical toolkit have been prototyped and deployed in support of numerous space missions. Remote and queue observing modes have gained significant market share on the ground. Archives and data-mining are becoming ubiquitous; astroinformatic techniques and virtual observatory standards and protocols are areas of active development. Astronomers and engineers, planetary and solar scientists, and researchers from communities as diverse as particle physics and exobiology are collaborating on a vast range of "multi-messenger" science. What then is missing?

  15. Iranian National Observatory: project overview

    NASA Astrophysics Data System (ADS)

    Khosroshahi, Habib G.; Jenab, Hooshdad; Bidar, Masoud; Mohajer, Mohammad; Saeidifar, Mahdi

    2016-07-01

    The Iranian National Observatory site is under construction at an altitude of 3600m at Mount Gargash in central Iran. It offers a promising site for optical and near-IR observations with a 0.7 arcsec median seeing and thus a number of observing facilities have been planned. The largest facility is a 3.4m Alt- Az reflecting Ritchey-Chretien optical telescope under development with an exit focal ratio of f/11 providing a generous 20 arcmin field of view at the main Cassegrain focus. This telescope will be equipped with high resolution medium-wide field imaging camera as well as medium and high resolution spectrographs. The telescope will benefit from an active support for the primary mirror. The primary mirror has been manufactured, polished and delivered. In this project overview, the design parameters for the 3.4m telescope and the current status of the project are presented.

  16. HELIO: The Heliophysics Integrated Observatory

    NASA Technical Reports Server (NTRS)

    Bentley, R. D.; Csillaghy, A.; Aboudarham, J.; Jacquey, C.; Hapgood, M. A.; Bocchialini, K.; Messerotti, M.; Brooke, J.; Gallagher, P.; Fox, P.; hide

    2011-01-01

    Heliophysics is a new research field that explores the Sun-Solar System Connection; it requires the joint exploitation of solar, heliospheric, magnetospheric and ionospheric observations. HELIO, the Heliophysics Integrated Observatory, will facilitate this study by creating an integrated e-Infrastructure that has no equivalent anywhere else. It will be a key component of a worldwide effort to integrate heliophysics data and will coordinate closely with international organizations to exploit synergies with complementary domains. HELIO was proposed under a Research Infrastructure call in the Capacities Programme of the European Commission's 7th Framework Programme (FP7). The project was selected for negotiation in January 2009; following a successful conclusion to these, the project started on 1 June 2009 and will last for 36 months.

  17. The Virtual Wave Observatory (VWO)

    NASA Technical Reports Server (NTRS)

    Fung, Shing F.

    2008-01-01

    Heliophysics wave data are currently not easily searchable by computers, making identifying pertinent wave data features for analyses and cross comparisons difficult and laborious. Since wave data analysis requires specialized knowledge about waves, which spans the spectrum of microphysics to macrophysics, researchers having varied expertise cannot easily use wave data. To resolve these difficulties and to allow wave data to contribute more fully to Heliophysics research, we are developing a Virtual Wave Observatory (VWO) whose goal is to enable all Heliophysics wave data to become searchable, understandable and usable by the Heliophysics community. The VWO objective is to enable search of multiple and distributed wave data (from both active and passive measurements). This presentation provides and overview of the VWO, a new VxO component within the emerging distributed Heliophysics data and model environment.

  18. HELIO: The Heliophysics Integrated Observatory

    NASA Astrophysics Data System (ADS)

    Bentley, R. D.; Csillaghy, A.; Aboudarham, J.; Jacquey, C.; Hapgood, M. A.; Bocchialini, K.; Messerotti, M.; Brooke, J.; Gallagher, P.; Fox, P.; Hurlburt, N.; Roberts, D. A.; Duarte, L. Sanchez

    2011-06-01

    Heliophysics is a new research field that explores the Sun-Solar System Connection; it requires the joint exploitation of solar, heliospheric, magnetospheric and ionospheric observations.HELIO, the Heliophysics Integrated Observatory, will facilitate this study by creating an integrated e-Infrastructure that has no equivalent anywhere else. It will be a key component of a worldwide effort to integrate heliophysics data and will coordinate closely with international organizations to exploit synergies with complementary domains.HELIO was proposed under a Research Infrastructure call in the Capacities Programme of the European Commission’s 7th Framework Programme (FP7). The project was selected for negotiation in January 2009; following a successful conclusion to these, the project started on 1 June 2009 and will last for 36 months.

  19. HELIO: The Heliophysics Integrated Observatory

    NASA Technical Reports Server (NTRS)

    Bentley, R. D.; Csillaghy, A.; Aboudarham, J.; Jacquey, C.; Hapgood, M. A.; Bocchialini, K.; Messerotti, M.; Brooke, J.; Gallagher, P.; Fox, P.; Hurlburt, N.; Roberts, D. A.; Sanchez Duarte, L.

    2011-01-01

    Heliophysics is a new research field that explores the Sun-Solar System Connection; it requires the joint exploitation of solar, heliospheric, magnetospheric and ionospheric observations. HELIO, the Heliophysics Integrated Observatory, will facilitate this study by creating an integrated e-Infrastructure that has no equivalent anywhere else. It will be a key component of a worldwide effort to integrate heliophysics data and will coordinate closely with international organizations to exploit synergies with complementary domains. HELIO was proposed under a Research Infrastructure call in the Capacities Programme of the European Commission's 7th Framework Programme (FP7). The project was selected for negotiation in January 2009; following a successful conclusion to these, the project started on 1 June 2009 and will last for 36 months.

  20. OPTICON and the Virtual Observatory

    NASA Astrophysics Data System (ADS)

    Gilmore, Gerry

    The challenges of multi-wavelength astrophysics require new outlooks from those appropriate to traditional astronomy. The next generation of research scientists must be trained to exploit the potentiality now being provided for the first time. Just as importantly, the full range of available information must be indexed and made available, to avoid wasteful repeat observations, or incomplete analyses. Perhaps the greatest challenge in the immediate future is to ensure the wealth of multi-wavelength data already available, and being accumulated, is available for efficient scientific exploitation. The difference between observations in a depositary and a fully-operational data archive is the difference between waste and cutting-edge science. The EU Optical Infrared Coordination Network for Astronomy (OPTICON) provides a forum to coordinate and develop the many national and international efforts and desires leading towards an operational virtial observatory.

  1. The Virtual Wave Observatory (VWO)

    NASA Technical Reports Server (NTRS)

    Fung, Shing F.

    2008-01-01

    Heliophysics wave data are currently not easily searchable by computers, making identifying pertinent wave data features for analyses and cross comparisons difficult and laborious. Since wave data analysis requires specialized knowledge about waves, which spans the spectrum of microphysics to macrophysics, researchers having varied expertise cannot easily use wave data. To resolve these difficulties and to allow wave data to contribute more fully to Heliophysics research, we are developing a Virtual Wave Observatory (VWO) whose goal is to enable all Heliophysics wave data to become searchable, understandable and usable by the Heliophysics community. The VWO objective is to enable search of multiple and distributed wave data (from both active and passive measurements). This presentation provides and overview of the VWO, a new VxO component within the emerging distributed Heliophysics data and model environment.

  2. TUM Critical Zone Observatory, Germany

    NASA Astrophysics Data System (ADS)

    Völkel, Jörg; Eden, Marie

    2014-05-01

    Founded 2011 the TUM Critical Zone Observatory run by the Technische Universität München and partners abroad is the first CZO within Germany. TUM CZO is both, a scientific as well as an education project. It is a watershed based observatory, but moving behind this focus. In fact, two mountainous areas are integrated: (1) The Ammer Catchment area as an alpine and pre alpine research area in the northern limestone Alps and forelands south of Munich; (2) the Otter Creek Catchment in the Bavarian Forest with a crystalline setting (Granite, Gneiss) as a mid mountainous area near Regensburg; and partly the mountainous Bavarian Forest National Park. The Ammer Catchment is a high energy system as well as a sensitive climate system with past glacial elements. The lithology shows mostly carbonates from Tertiary and Mesozoic times (e.g. Flysch). Source-to-sink processes are characteristic for the Ammer Catchment down to the last glacial Ammer Lake as the regional erosion and deposition base. The consideration of distal depositional environments, the integration of upstream and downstream landscape effects are characteristic for the Ammer Catchment as well. Long term datasets exist in many regards. The Otter Creek catchment area is developed in a granitic environment, rich in saprolites. As a mid mountainous catchment the energy system is facing lower stage. Hence, it is ideal comparing both of them. Both TUM CZO Catchments: The selected catchments capture the depositional environment. Both catchment areas include historical impacts and rapid land use change. Crosscutting themes across both sites are inbuilt. Questions of ability to capture such gradients along climosequence, chronosequence, anthroposequence are essential.

  3. The Compton Gamma Ray Observatory

    NASA Astrophysics Data System (ADS)

    Gehrels, N.; Chipman, E.; Kniffen, D. A.

    1993-01-01

    The Arthur Holly Compton Gamma Ray Observatory (Compton) was launched by the Space Shuttle Atlantis on 5 April 1991. The spacecraft and instruments are in good health and returning exciting results. The mission provides nearly six orders of magnitude in spectral coverage, from 30 keV to 30 GeV, with sensitivity over the entire range an order of magnitude better than that of previous observations. The 16,000 kilogram observatory contains four instruments on a stabilized platform. The mission began normal operations on 16 May 1991 and is now over half-way through a full-sky survey. The mission duration is expected to be from six to ten years. A Science Support Center has been established at Goddard Space Flight Center for the purpose of supporting a vigorous Guest Investigator Program. New scientific results to date include: (1) the establishment of the isotropy, combined with spatial inhomogeneity, of the distribution of gamma-ray bursts in the sky; (2) the discovery of intense high energy (100 MeV) gamma-ray emission from 3C 279 and other quasars and BL Lac objects, making these the most distant and luminous gamma-ray sources ever detected; (3) one of the first images of a gamma-ray burst; (4) the observation of intense nuclear and position-annihilation gamma-ray lines and neutrons from several large solar flares; and (5) the detection of a third gamma-ray pulsar, plus several other transient and pulsing hard X-ray sources.

  4. Golden legacy from ESA's observatory

    NASA Astrophysics Data System (ADS)

    2003-07-01

    ISO was the first space observatory able to see the sky in infrared light. Using its eyes, we have discovered many new phenomena that have radically changed our view of the Universe. Everybody knows that when something is heated it glows. However, things also glow with a light our eyes cannot detect at room temperature: infrared light. Infrared telescopes do not work well on the Earth’s surface because such light is absorbed by the atmosphere. ISO looked at the cold parts of the universe, usually the 'cold and dusty' parts. It peered into clouds of dust and gas where stars were being born, observing for the first time the earliest stages of star formation. It discovered, for example, that stars begin to form at temperatures as low as -250°C or less. Scientists were able to follow the evolution of dust from where it is produced (that is, old stars - the massive 'dust factories') to the regions where it forms new planetary systems. ISO found that most young stars are surrounded by discs of dust that could harbour planets. The observatory also analysed the chemical composition of cosmic dust, thereby opening up a new field of research, ‘astromineralogy’. With ISO we have been able to discover the presence of water in many different regions in space. Another new discipline, 'astrochemistry', was boosted when ISO discovered that the water molecule is common in the Universe, even in distant galaxies, and complex organic molecules like benzene readily form in the surroundings of some stars. "ISO results are impacting most fields of astronomical research, almost literally from comets to cosmology," explains Alberto Salama, ISO Project Scientist. "Some results answer questions. Others open new fields. Some are already being followed up by existing telescopes; others have to await future facilities." When ISO's operational life ended, in 1998, its observations became freely available to the world scientific community via ISO’s data archive. In May 2003 the

  5. Investigations of the interstellar medium at Washburn Observatory 1930-58

    NASA Astrophysics Data System (ADS)

    Liebl, David S.; Fluke, Christopher

    2004-12-01

    Between 1930 and 1958, the Washburn Observatory of the University of Wisconsin-Madison was home to pioneering photometric research into the interstellar medium by Joel Stebbins and Albert Whitford. Between 1933 and 1941, Stebbins and Whitford published seminal research on the photometry of stellar reddening, using the Washburn 15-inch refractor and the 60- and 100-inch reflectors at Mount Wilson Observatory. Many factors were responsible for the Washburn Observatory's pre-eminence in this area. This paper reviews their research on interstellar dust during the years 1922-58, the observational technology and scientific methods that were developed at the Washburn Observatory during that time and the scientific discoveries that originated there. We discuss the factors that enabled Washburn Observatory to become a leader in photometry during the first half of the twentieth century. We also draw on the recollections of past and present Washburn Observatory scientists to understand how Washburn's standing led to a subsequent programme of research into the interstellar medium at the University of Wisconsin-Madison. The resulting portrayal of Washburn Observatory provides insights into the evolution of astronomical research in America, from the beginning of the twentieth century until today.

  6. The Rapid Ice Sheet Change Observatory (RISCO)

    NASA Astrophysics Data System (ADS)

    Morin, P.; Howat, I. M.; Ahn, Y.; Porter, C.; McFadden, E. M.

    2010-12-01

    The recent expansion of observational capacity from space has revealed dramatic, rapid changes in the Earth’s ice cover. These discoveries have fundamentally altered how scientists view ice-sheet change. Instead of just slow changes in snow accumulation and melting over centuries or millennia, important changes can occur in sudden events lasting only months, weeks, or even a single day. Our understanding of these short time- and space-scale processes, which hold important implications for future global sea level rise, has been impeded by the low temporal and spatial resolution, delayed sensor tasking, incomplete coverage, inaccessibility and/or high cost of data available to investigators. New cross-agency partnerships and data access policies provide the opportunity to dramatically improve the resolution of ice sheet observations by an order of magnitude, from timescales of months and distances of 10’s of meters, to days and meters or less. Advances in image processing technology also enable application of currently under-utilized datasets. The infrastructure for systematically gathering, processing, analyzing and distributing these data does not currently exist. Here we present the development of a multi-institutional, multi-platform observatory for rapid ice change with the ultimate objective of helping to elucidate the relevant timescales and processes of ice sheet dynamics and response to climate change. The Rapid Ice Sheet Observatory (RISCO) gathers observations of short time- and space-scale Cryosphere events and makes them easily accessible to investigators, media and general public. As opposed to existing data centers, which are structured to archive and distribute diverse types of raw data to end users with the specialized software and skills to analyze them, RISCO focuses on three types of geo-referenced raster (image) data products in a format immediately viewable with commonly available software. These three products are (1) sequences of images

  7. The Pierre Auger Observatory offline software

    NASA Astrophysics Data System (ADS)

    Allen, J.; Argirò, S.; Barroso, S. L. C.; Ben Zvi, S. Y.; Cataldi, G.; Ding, M.; Gonzalez, J.; McCauley, T.; Nellen, L.; Paul, T.; Porter, T. A.; Prado, L., Jr.; Roth, M.; Ulrich, R.; Unger, M.; Veberič, D.

    2008-07-01

    The Pierre Auger Observatory aims to discover the nature and origins of the highest energy cosmic rays. The large number of physicists involved in the project and the diversity of simulation and reconstruction tasks pose a challenge for the offline analysis software, not unlike the challenges confronting software for very large high energy physics experiments. Previously we have reported on the design and implementation of a general purpose but relatively lightweight framework which allows collaborators to contribute algorithms and sequencing instructions to build up the variety of applications they require. In this report, we update the status of this work and describe some of the successes and difficulties encountered over the last few years of use. We explain the machinery used to manage user contributions, to organize the abundance of configuration files, to facilitate multi-format file handling, and to provide access to event and time-dependent detector information residing in various data sources. We also describe the testing procedures used to help maintain stability of the code in the face of a large number of contributions. Foundation classes will also be discussed, including a novel geometry package which allows manipulation of abstract geometrical objects independent of coordinate system choice.

  8. HAWC observatory catches first gamma rays

    NASA Astrophysics Data System (ADS)

    Frías Villegas, Gabriela

    2013-06-01

    The world's largest and most modern gamma-ray observatory has carried out its first successful observations. Located inside the Pico de Orizaba national park in the Mexican state of Puebla, the High-Altitude Water Cherenkov Observatory (HAWC) is a collaboration between 26 Mexican and US institutions.

  9. Scientific Workflows and the Sensor Web for Virtual Environmental Observatories

    NASA Astrophysics Data System (ADS)

    Simonis, I.; Vahed, A.

    2008-12-01

    Virtual observatories mature from their original domain and become common practice for earth observation research and policy building. The term Virtual Observatory originally came from the astronomical research community. Here, virtual observatories provide universal access to the available astronomical data archives of space and ground-based observatories. Further on, as those virtual observatories aim at integrating heterogeneous ressources provided by a number of participating organizations, the virtual observatory acts as a coordinating entity that strives for common data analysis techniques and tools based on common standards. The Sensor Web is on its way to become one of the major virtual observatories outside of the astronomical research community. Like the original observatory that consists of a number of telescopes, each observing a specific part of the wave spectrum and with a collection of astronomical instruments, the Sensor Web provides a multi-eyes perspective on the current, past, as well as future situation of our planet and its surrounding spheres. The current view of the Sensor Web is that of a single worldwide collaborative, coherent, consistent and consolidated sensor data collection, fusion and distribution system. The Sensor Web can perform as an extensive monitoring and sensing system that provides timely, comprehensive, continuous and multi-mode observations. This technology is key to monitoring and understanding our natural environment, including key areas such as climate change, biodiversity, or natural disasters on local, regional, and global scales. The Sensor Web concept has been well established with ongoing global research and deployment of Sensor Web middleware and standards and represents the foundation layer of systems like the Global Earth Observation System of Systems (GEOSS). The Sensor Web consists of a huge variety of physical and virtual sensors as well as observational data, made available on the Internet at standardized

  10. Searching Across Multiple Datasets with the Virtual ITM Observatory

    NASA Astrophysics Data System (ADS)

    Morrison, D.; Weiss, M.; Immer, E. A.; Patrone, D.; Potter, M.; Barnes, R. J.; Colclough, C.; Holder, R.; McGuire, R. E.; Candey, R. M.; Bilitza, D.; Harris, B.

    2010-12-01

    One of the great time-saving features of Virtual Observatories is the ability to have a single search find products from many different sites at one time. High fidelity search tools allow the user to triage the vast data holdings down to a smaller set of particular interest. The Virtual ITM Observatory (VITMO) provides many methods by which the user can search for and select data of interest including restricting selections based on geophysical conditions (solar wind speed, Kp, etc) as well as finding those datasets that overlap in time and/or space. The ability of a Virtual Observatory to add in external services allows search to be enhanced and provide higher fidelity searching for the end user. In this presentation we will discuss planned and future additions to search in VITMO that are based on user feedback and will include an indication of the types of ITM research that this enhanced search will facilitate. This presentation will include the addition of existing external services into VITMO as well as future proposed services.

  11. EARLY SCIENCE WITH SOFIA, THE STRATOSPHERIC OBSERVATORY FOR INFRARED ASTRONOMY

    SciTech Connect

    Young, E. T.; Becklin, E. E.; De Buizer, J. M.; Andersson, B.-G.; Casey, S. C.; Helton, L. A.; Marcum, P. M.; Roellig, T. L.; Temi, P.; Herter, T. L.; Guesten, R.; Dunham, E. W.; Backman, D.; Burgdorf, M.; Caroff, L. J.; Erickson, E. F.; Davidson, J. A.; Gehrz, R. D.; Harper, D. A.; Harvey, P. M.; and others

    2012-04-20

    The Stratospheric Observatory For Infrared Astronomy (SOFIA) is an airborne observatory consisting of a specially modified Boeing 747SP with a 2.7 m telescope, flying at altitudes as high as 13.7 km (45,000 ft). Designed to observe at wavelengths from 0.3 {mu}m to 1.6 mm, SOFIA operates above 99.8% of the water vapor that obscures much of the infrared and submillimeter. SOFIA has seven science instruments under development, including an occultation photometer, near-, mid-, and far-infrared cameras, infrared spectrometers, and heterodyne receivers. SOFIA, a joint project between NASA and the German Aerospace Center Deutsches Zentrum fuer Luft und-Raumfahrt, began initial science flights in 2010 December, and has conducted 30 science flights in the subsequent year. During this early science period three instruments have flown: the mid-infrared camera FORCAST, the heterodyne spectrometer GREAT, and the occultation photometer HIPO. This Letter provides an overview of the observatory and its early performance.

  12. Science Initiatives of the US Virtual Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Hanisch, R. J.

    2012-09-01

    The United States Virtual Astronomical Observatory program is the operational facility successor to the National Virtual Observatory development project. The primary goal of the US VAO is to build on the standards, protocols, and associated infrastructure developed by NVO and the International Virtual Observatory Alliance partners and to bring to fruition a suite of applications and web-based tools that greatly enhance the research productivity of professional astronomers. To this end, and guided by the advice of our Science Council (Fabbiano et al. 2011), we have focused on five science initiatives in the first two years of VAO operations: 1) scalable cross-comparisons between astronomical source catalogs, 2) dynamic spectral energy distribution construction, visualization, and model fitting, 3) integration and periodogram analysis of time series data from the Harvard Time Series Center and NASA Star and Exoplanet Database, 4) integration of VO data discovery and access tools into the IRAF data analysis environment, and 5) a web-based portal to VO data discovery, access, and display tools. We are also developing tools for data linking and semantic discovery, and have a plan for providing data mining and advanced statistical analysis resources for VAO users. Initial versions of these applications and web-based services are being released over the course of the summer and fall of 2011, with further updates and enhancements planned for throughout 2012 and beyond.

  13. Science Initiatives of the us Virtual Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Hanisch, Robert J.

    The United States Virtual Astronomical Observatory program is the operational facility successor to the National Virtual Observatory development project. The primary goal of the US VAO is to build on the standards, protocols, and associated infrastructure developed by NVO and the International Virtual Observatory Alliance partners and to bring to fruition a suite of applications and web-based tools that greatly enhance the research productivity of professional astronomers. To this end, and guided by the advice of our Science Council (advisory committee), we are focusing on five science initiatives in the first two years of VAO operations: (1) scalable cross-comparisons between astronomical source catalogs, (2) dynamic spectral energy distribution construction, visualization, and model fitting, (3) integration and periodogram analysis of time series data from the Harvard Time Series Center and NASA Star and Exoplanet Database, (4) integration of VO data discovery and access tools into the IR AF data analysis environment, and (5) a web-based portal to VO data discovery, access, and display tools. We are also developing tools for data linking and semantic discovery, and have a plan for providing data mining and advanced statistical analysis resources for VAO users. Initial versions of these applications and web-based services are being released over the course of the summer and fall of 2011, with further updates and enhancements planned for throughout 2012 and beyond.

  14. Medicine Wheels of the Great Plains

    NASA Astrophysics Data System (ADS)

    Vogt, David

    Medicine Wheels are unexplained aboriginal boulder configurations found primarily on hilltops and river valley vistas across the northwest Great Plains of North America. Their varied, complex designs have inspired diverse hypotheses concerning their meaning and purpose, including astronomical ones. While initial "observatory" speculations were unfounded, and quests to "decode" these structures remain unfulfilled and possibly misguided, the Medicine Wheels nevertheless represent a uniquely worthwhile case study in archaeoastronomical theory and method. In addition, emerging technologies for data acquisition and analysis pertinent to Medicine Wheels offer prospectively important new sight lines for the future of archaeoastronomy.

  15. Cosmic Ray Observatories for Space Weather Studies.

    NASA Astrophysics Data System (ADS)

    González, Xavier

    2016-07-01

    The Mexican Space Weather Service (SCiESMEX) was created in October 2014. Some observatories measure data for the service at different frequencies and particles. Two cosmic ray observatories detect the particle variations attributed to solar emissions, and are an important source of information for the SCiESMEX. The Mexico City Cosmic Ray Observatory consists of a neutron monitor (6-NM-64) and a muon telescope, that detect the hadronic and hard component of the secondary cosmic rays in the atmosphere. It has been in continous operation since 1990. The Sierra Negra Cosmic Ray Observatory consists of a solar neutron telescope and the scintillator cosmic ray telescope. These telescopes can detect the neutrons, generated in solar flares and the hadronic and hard components of the secondary cosmic rays. It has been in continous operation since 2004. We present the two observatories and the capability to detect variations in the cosmic rays, generated by the emissions of the solar activity.

  16. The Telescope Array's Middle Drum Observatory

    NASA Astrophysics Data System (ADS)

    Blake, S.A.; Cady, R.; Jui, C.C.H.; Matthews, J.N.; Rodribuez, D.; Smith, J.D.; Thomas, S.B.

    The Telescope Array Project (TA) is an Ultra High Energy Cosmic Ray Observatory in central Utah. It performs a hybrid measurement of the extensive air showers induced by cosmic rays. The two detector systems are 1) an array of 576 scintillation detectors and 2) three fluorescence telescope observatories which overlook the ground array. The Telescope Array will measure the study spectral shape, chemical composition of primary cosmic rays, and search for sources. Additionally, it seeks to understand the difference between the HiRes (High Resolution Fly's Eye) and AGASA (Akeno Giant Air Shower Array) spectra. The Middle Drum Observatory has been instrumented using refurbished telescopes from the HiRes-I Observatory at Dugway. We will discuss the detectors, modifications to aid calibration and analysis, and the first data from this observatory.

  17. Stratospheric Observatory for Infrared Astronomy (SOFIA)

    NASA Astrophysics Data System (ADS)

    Savage, M. L.; Becklin, E. E.

    2015-09-01

    The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), project has been operating airborne astronomy flights from Palmdale, California since 2011. The observatory consists of a modified 747sp aircraft with a 2.5meter telescope in the tail section. In addition to observing flights out of Palmdale, Ca. this airborne observatory has been able to take advantage of its mobility to observe in the southern hemisphere (New Zealand), to perform multi-wavelength observations of the Super Novae (SN 2014b) in 2014, and to intersect the track of a Pluto Occultation in the southern hemisphere just a few weeks prior to the New Horizons mission fly by of the planet in summer 2015. Science results, observatory operations, current instrument status and participation in future instrument developments, over the lifetime of the observatory will be discussed.

  18. The Pulkovo Observatory on the Centuries' Borderline

    NASA Astrophysics Data System (ADS)

    Abalakin, Viktor K.

    The present paper deals with the development of astrophysical research at the Pulkovo Observatory (now: the Central (Pulkovo) Astronomical Observatory of the Russian Academy of Sciences) at adjacent time periods separated by the threshold between the 19th and the 20th centuries. The Pulkovo Observatory had been inaugurated in 1839. Its traditional field of research work was astrometry. The confirmation of light absorption phenomenon in interstellar space by Friedrich Georg Wilhelm Struve marked the turn of the Observatory's research programs toward astrophysics. New tendencies in the development of contemporaneous astronomy in Russia were pointed out by Otto Struve in his paper “About the Place of Astrophysics in Astronomy” presented in 1866 to the Saint-Petersburg Academy of Sciences. Wide-scale astrophysical studies were performed at Pulkovo Observatory around 1900 during the directorships of Theodore Bredikhin, Oscar Backlund and Aristarchos Belopolsky.

  19. Status of the Frisco Peak Observatory

    NASA Astrophysics Data System (ADS)

    Ricketts, Paul; Springer, Wayne; Dawson, Kyle; Kieda, Dave; Gondolo, Paolo; Bolton, Adam

    2009-10-01

    The University of Utah has constructed an astronomical observatory located at an elevation of approximately 9600 feet of Frisco Peak west of Milford, Utah. This site was chosen after performing a survey of potential observatory sites throughout Southern Utah. At the time of writing this abstract, the dome and control buildings have been completed. Installation of a 32'' telescope manufactured by DFM Engineering is scheduled to start October 5, 2009. Commissioning of the telescope will take place this fall. A study of the photometric quality of the observatory site will be performed as well. A description of the observatory site survey and the construction and commissioning of the Frisco Peak Observatory will be presented.

  20. The Chandra X-Ray Observatory and its Role for the Study of Ionized Plasmas

    NASA Technical Reports Server (NTRS)

    Weisskopf, Martin C.

    2010-01-01

    NASA's Chandra X-Ray Observatory was launched in July of 1999. Featuring a 1000cm2-class X-ray telescope with sub-arcsecond angular resolution, the Observatory has observed targets from the solar system including the earth s moon, comets, and planets to the most distant galaxy clusters and active galactic nuclei. Capable of performing moderate energy resolution image-resolved spectroscopy using its CCD detectors, and high-resolution grating spectroscopy, the Observatory has produced, and continues to produce, valuable data and insights into the emission mechanisms of the ionized plasmas in which the X-rays originate. We present a brief overview of the Observatory to provide insight as to how to use it for your investigations. We also present an, admittedly brief and biased, overview of some of the results of investigations performed with Chandra that may be of interest to this audience.