Thematische Bibliographien / Astro Observatory (U.S.)

Inhaltsverzeichnis

  1. Zeitschriftenartikel
  2. Bücher
  3. Buchteile
  4. Konferenzberichte
  5. Berichte der Organisationen

Auswahl der wissenschaftlichen Literatur zum Thema „Astro Observatory (U.S.)“

Autor: Grafiati
Veröffentlicht am 25. Juli 2024

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Zeitschriftenartikel zum Thema "Astro Observatory (U.S.)"

1

Worley, Charles E., and Geoffrey G. Douglass. "Speckle Interferometry at the U. S. Naval Observatory." International Astronomical Union Colloquium 135 (1992): 583–85. http://dx.doi.org/10.1017/s0252921100007223.

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AbstractA new speckle interferometer began operation with the 66-cm refractor in Oct. 1990. The interferometer is an improved version of the one operated by CHARA at Georgia State University. We describe the instrument, its calibration, and first observational results.
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Schmidt, Richard E., and Steven J. Dick. "Meridian Circle Astrometry at the U. S. Naval Observatory." Cahiers François Viète, no. III-14 (June 1, 2023): 217–54. http://dx.doi.org/10.4000/cahierscfv.4086.

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3

Eglitis, Ilgmars, and Vitaly Andruk. "Astrometry and photometry of digitized plates of Baldone Schmidt telescope." Open Astronomy 30, no. 1 (2021): 12–23. http://dx.doi.org/10.1515/astro-2021-0002.

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Abstract During the 40-year photographic period of astronomical observations, the Baldone Astrophysical Observatory has accumulated more than 22,000 direct and 2,500 spectral images. In 2018, the digitization of direct astrophoto images with a resolution of 1200 dpi was completed. A processing methodology for obtaining the equatorial coordinates and photometric characteristics of the objects recorded in digitized astronegatives using the LINUX/MIDAS/ROMAFOT environment has been developed at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine. Program package with success already works in seven observatories. A description of the operation of this program complex in stages and analysis of the obtained results is given. The steps describe the astrometric and photometric reduction process of digital records, as well as the reduction of the obtained instrumental magnitudes to the Johnson UBVR photometric system. The methodology of characteristic curve construction in the case of one exposure is described in detail. From all digitized astrophotoplates to date Approximately 2200 V film negatives, 300 U plates and several R, B plates were processed. As a result, catalogs of the positions and magnitudes of Pluto, 1848 asteroids and comets were obtained. 31 new positions were recorded in the VizieR Pluto catalog VI/155. It was found that the root-mean-square errors of the reduction of the measured coordinates to the equatorial coordinate system of the Tycho-2 catalog have values σ RA , DEC = 0.1-0.2”, and the root-mean-square errors of the reduction of instrumental photometric quantities m to the Johnson system of stellar UBVR-values are also in within σ UBVR = 0.1 − 0.2 m .
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Sapozhnikov, Sergei, and Dana Kovaleva. "Application of clustering algorithm to wide stellar pairs for unsupervised search of parts of disrupting clusters." Open Astronomy 30, no. 1 (2021): 191–202. http://dx.doi.org/10.1515/astro-2021-0025.

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Abstract We introduce the application of the clustering algorithm to the preliminary compiled list of probable wide pairs of co-moving stars. The main aim of such development is a possibility of unsupervised blind search of coeval loose stellar structures over significant regions in space. Using Gaia EDR3 data, we investigated the application of the method to nearby region hosting recently discovered loose structures – tidal tails of Coma Ber star cluster and a nearby stellar group named Group X. We compare the results of straightforward clustering of stellar data with results of using our method with varying parameters. We then compare the results of our method to the recent results of the two groups of authors who independently discovered the discussed structures. We find parameters allowing the method to find the full scope of distributed stellar groups without preliminary knowledge of their characteristics. It decreases the risk of false positive clustering and improves the ability to discover loose stellar groups, in comparison with the application of clustering algorithm to the individual stars. Further we obtain a refined dataset of probable members of both stellar groups and independently obtain their ages (700 ± 70 Myr and 450 ± 100 Myr) and space velocities ((U,V,W) = (8.63 ± 0.13, 6.63 ± 0.20, 6.65 ± 0.95) km/s for Coma Ber star cluster, and (U,V,W) = (7.70 ± 0.12, 3.27 ± 0.45, 5.69 ± 0.80) km/s for Group X). Our results are in very good agreement with those of previous investigators.
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Odaka, Hirokazu. "Hitomi X-ray Astronomy Satellite: Power of High-Resolution Spectroscopy." Proceedings of the International Astronomical Union 11, S322 (2016): 197–203. http://dx.doi.org/10.1017/s1743921316012084.

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AbstractHitomi (ASTRO-H) is an X-ray observatory developed by an international collaboration led by JAXA. An X-ray microcalorimeter onboard this satellite has opened a new window of high-resolution spectroscopy with an unprecedented energy resolution of 5 eV (FWHM) at 6 keV. The spacecraft was launched on February 17, 2016 from Tanegashima Island, Japan, and we completed initial operations including deployment of the hard X-ray imagers on the extensible optical bench. All scientific instruments had successfully worked until the sudden loss of the mission on March 26. We have obtained a spectrum showing fully resolved emission lines through the first-light observation of the Perseus Cluster. The line-of-sight velocity dispersion of 164 ± 10 km s−1 reveals the quiescent environment of intracluster medium at the cluster core, implying that measured cluster mass requires little correction for the turbulent pressure. We also discuss observations to the Galactic Center which could be performed with Hitomi.
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Long, Knox S. "Far Ultraviolet Observations of Dwarf Novae made with the Hopkins Ultraviolet Telescope." International Astronomical Union Colloquium 158 (1996): 233–41. http://dx.doi.org/10.1017/s0252921100038756.

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AbstractObservations with the Hopkins Ultraviolet Telescope on the Astro-1 and Astro-2 space shuttle missions have provided the first set of moderate (3 Å) resolution far ultraviolet (FUV) spectra of dwarf novae to include the wavelength range between Lyα and the Lyman limit. Important lines which are detected in the HUT spectra of dwarf novae in this wavelength range include S VI λλ933,945, C III λ977, O VI λλ1032,1038, P V λλ1118,1128 and C III λ1176, as well as the higher order Lyman lines. The observations confirm earlier IUE observations that two dwarf novae – U Gem and VW Hyi – have quiescent FUV spectra dominated by the white dwarf, but suggest that the quiescent FUV emission from three other dwarf novae – SS Cyg, WX Hyi and YZ Cnc – are dominated by emission from a hot portion of the disk or a disk corona. The spectra obtained of the dwarf novae Z Cam and EM Cyg in outburst and also of the nova-like variable IX Vel can be modeled reasonably successfully in terms of steady state disks constructed by adding appropriately-weighted stellar model spectra.
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Martin, Frederick. "A Dresden Codex Eclipse Sequence: Projections for the Years 1970–1992." Latin American Antiquity 4, no. 1 (1993): 74–93. http://dx.doi.org/10.2307/972138.

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Data from the U. S. Naval Observatory annual astronomical almanacs (1970–1992) in “correlation” with the Maya Calendar Round (CR) sequence indicate that the Dresden Codex lunar table (51a-58b) very probably counted simultaneous sequences of both lunar and solar eclipses on the same set of day names. The contemporary sequence of day names in the CR and the astronomy consistent with it parallels Classic-period Maya observational experience between 9.16.0.0.0 and 9.17.0.0.0.
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Fan, Zhou, Gang Zhao, Wei Wang, et al. "The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)." Astrophysical Journal Supplement Series 268, no. 1 (2023): 9. http://dx.doi.org/10.3847/1538-4365/ace04a.

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Abstract The Stellar Abundances and Galactic Evolution Survey (SAGES) of the northern sky is a specifically designed multiband photometric survey aiming to provide reliable stellar parameters with accuracy comparable to those from low-resolution optical spectra. It was carried out with the 2.3 m Bok telescope of Steward Observatory and three other telescopes. The observations in the u s and v s passband produced over 36,092 frames of images in total, covering a sky area of ∼9960 deg2. The median survey completenesses of all observing fields for the two bands are u s = 20.4 mag and v s = 20.3 mag, respectively, while the limiting magnitudes with signal-to-noise ratio of 100 are u s ∼ 17 mag and v s ∼ 18 mag, correspondingly. We combined our catalog with the data release 1 (DR1) of the first Panoramic Survey Telescope And Rapid Response System (Pan-STARRS, PS1) catalog, and obtained a total of 48,553,987 sources that have at least one photometric measurement in each of the SAGES u s and v s and PS1 grizy passbands. This is the DR1 of SAGES, released in this paper. We compared our gri point-source photometry with those of PS1 and found an rms scatter of ∼2% difference between PS1 and SAGES for the same band. We estimated an internal photometric precision of SAGES to be of the order of ∼1%. Astrometric precision is better than 0.″2 based on comparison with DR1 of the Gaia mission. In this paper, we also describe the final end-user database, and provide some science applications.
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9

Canzian, B. "The 488,006,860 Sources in the USNO-A1.0 Catalog." Symposium - International Astronomical Union 179 (1998): 422–23. http://dx.doi.org/10.1017/s0074180900129201.

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The USNO-A1.0 catalog was generated from the U. S. Naval Observatory's digitization of the Palomar Observatory Sky Survey IOandEsurvey plates for fields with central declination δ ≥ −30°, and from the European Southern ObservatoryRand Science Research CouncilJsurvey plates for fields with central δ ≤–35° using the Precision Measuring Machine (PMM) located at the Flagstaff Station. It lists positions (α and δ in J2000) and brightnesses (red and blue magnitudes on the parent plate system) for all objects. A flag indicates if the entry also exists in GSC1.1.
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Zalinian, V. P., A. A. Karapetian, and H. M. Tovmassian. "Two-colour observations of spikes and flares by high time resolution." Symposium - International Astronomical Union 137 (1990): 33–34. http://dx.doi.org/10.1017/s0074180900187364.

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Observations of flare stars with high time resolution permit to register spiky type flares and also to study in detail bright curves of flares. In Byurakan observatory observations of EV Lac have been made with 0.1 s time resolution simultaneouslyin two filters “U” and “B” [1-3]. These observations permited to detect flares of a burst type (Fig.1) and also to reveil multipeak structure of long duration flares. It is necessary to stress that simultaneous observations in two colours increas appresiably the thrustworthiness of the registered spiky flares.
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Bücher zum Thema "Astro Observatory (U.S.)"

1

Observatory, U. S. Naval. 2012 U. S. Naval Observatory Nautical Almanac. Skyhorse Publishing Company, Incorporated, 2012.

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2

2012 U. S. Naval Observatory Nautical Almanac. Skyhorse Publishing Company, Incorporated, 2012.

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3

Akademiia Nauk Sssr. Krymskaia Astrofizicheskaia Observatoriia. Bulletin of the Crimean Astrophysical Observatory (U S S R Academy of Sciences Astrophysical Observatory Series). Allerton Pr, 1985.

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4

Dick, Steven J. Sky and Ocean Joined: The U. S. Naval Observatory 18302000. Cambridge University Press, 2007.

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5

(Washington, DC) Naval Observatory. Astronomical Observations Made At The U. S. Naval Observatory: During The Years. Arkose Press, 2015.

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6

Gough, D. O. Problems of Solar and Stellar Oscillations: Proceedings of the 66th IAU Colloquium Held at the Crimean Astrophysical Observatory, U. S. S. R. , 1-5 September 1981. Springer London, Limited, 2012.

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7

Hazard, Daniel L. Results of Observations Made at the U. S. Coast and Geodetic Survey Magnetic Observatory at Vieques, Porto Rico 1911 And 1912. Creative Media Partners, LLC, 2018.

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8

Ulrich, Roger K., Judit M. Pap, and Claus öhlich. Solar Electromagnetic Radiation Study for Solar Cycle 22: Proceedings of the SOLERS22 Workshop Held at the National Solar Observatory, Sacramento Peak, Sunspot, New Mexico, U. S. A. , June 17-21 1996. Springer London, Limited, 2012.

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Buchteile zum Thema "Astro Observatory (U.S.)"

1

Dick, Steven J. "John Quincy Adams, the Smithsonian Bequest and the Founding of the U. S. Naval Observatory." In Space, Time, and Aliens. Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-41614-0_25.

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2

Yao, Zhen-Guo, and Clayton Smith. "Equator and Equinox Solutions from Meridian Circle Observations of The Sun, Mercury and Venus at the Cape of Good Hope and the U. S. Naval Observatory from 1907 to 1971." In Developments in Astrometry and Their Impact on Astrophysics and Geodynamics. Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1711-1_74.

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Konferenzberichte zum Thema "Astro Observatory (U.S.)"

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Martin, H. M., D. S. Anderson, J. H. Burge, and S. C. West. "Stressed-lap Polishing of Large, Highly Aspheric Primary Mirrors." In Optical Fabrication and Testing. Optica Publishing Group, 1992. http://dx.doi.org/10.1364/oft.1992.tha5.

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Stressed-lap polishing has been used to complete three fast borosilicate honeycomb-sandwich mirrors. The 1.8-m f/1 primary mirror for the Lennon Telescope being built by the Vatican Observatory and the University of Arizona has been figured to an accuracy of 17 nm rms surface error, the 3.5-m f/1.5 primary mirror for the Starfire Optical Range of the U. S. Air Force Phillips Laboratory to 21 nm rms, and the 3.5-m f/1.75 primary mirror for the Astrophysical Research Consortium to 19 nm rms. The 3.5-m mirrors were figured in a new polishing facility, using a computer-controlled polishing machine and vibration-isolated test tower both sized for 8-m mirrors.
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Sarlashkar, Avinash, Derrell Lorthridge, Matthew Harrigan, et al. "Progress Towards Autonomous Structural Health Management." In Vertical Flight Society 75th Annual Forum & Technology Display. The Vertical Flight Society, 2019. http://dx.doi.org/10.4050/f-0075-2019-14613.

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The Autonomous Sustainment Technologies for Rotorcraft Operations-Structures (ASTRO-S) project between U. S. Army Combat Capability Missile Center, Aviation Development Directorate-Eustis (FCDD-AMV-E) and Sikorsky developed and validated a range of technologies to enable reduced airframe maintenance burden, increase operational availability, and provide key enabling technologies relative to Army's transition to the new paradigm of Maintenance Free Operational Periods (MFOP) for the rotorcraft of the future. Methods were developed for autonomous characterization of major damage and residual strength expressed as a Structural Health Index (SHI) for advanced durable and damage tolerant composite aerospace structural assemblies with redundant load paths, enabling targeted inspections and strength-based fly / watch / repair decisions. A number of sensing technologies including fiber-optic strain measurement and piezo-based structural health assessment, along with a number of innovative advanced algorithms that intelligently use changes in monitored structural responses, were implemented in a comprehensive architecture to detect, localize, and assess the severity of structural damage. Extensive testing on full-scale, multiload-path composite structures to assess feasibility and effectiveness of the developed technologies, as well as understand application and transition challenges, has convincingly shown that damage detection, localization, and severity assessment in an autonomous fashion is feasible. Further, it was shown that the concept of a trendable SHI to assess residual strength, is viable, although additional full-scale test cases are needed to further validate and mature the approach. Overall, these key findings affirm suitability of the technical approach and associated algorithms for reducing maintenance burden by triggering rather than scheduling inspections and potentially deferring repairs in high op-tempo environments. These structural health management technologies will be key enablers supporting Army's future rotorcraft when operating in an untethered multi-domain battle space.
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Berichte der Organisationen zum Thema "Astro Observatory (U.S.)"

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Boboltz, David A., Alan L. Fey, Nicole Geiger, Chris Dieck, and David M. Hall. U. S. Naval Observatory VLBI Analysis Center. Defense Technical Information Center, 2013. http://dx.doi.org/10.21236/ada583997.

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