Thematische Bibliographien / Photometry, astronomical

Inhaltsverzeichnis

  1. Zeitschriftenartikel
  2. Dissertationen
  3. Bücher
  4. Buchteile
  5. Konferenzberichte

Auswahl der wissenschaftlichen Literatur zum Thema „Photometry, astronomical“

Autor: Grafiati
Veröffentlicht am 4. Juni 2021
Zuletzt aktualisiert am 28. Juli 2024

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Zeitschriftenartikel zum Thema "Photometry, astronomical"

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Prokhorov, M. E., A. I. Zakharov, V. G. Moshkalev, N. L. Krusanova und M. S. Tuchin. „Mass Computations of the Brightness of Stars in an Arbitrary Spectral Band“. Астрономический журнал 100, Nr. 6 (01.06.2023): 500–511. http://dx.doi.org/10.31857/s0004629923050092.

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The problem of calculating the brightness of an array of stars in an arbitrary photometric band, which is not the standard band of astronomical photometry, is considered from their multicolor photometry in some other photometric system. A similar problem is to transfer photometric measurements of stars from one multicolor photometric system to another. This task includes methods for calculating and comparing magnitudes, as well as merging photometric catalogs. The questions of choice of various zero-points of photometry and reduction of measurements for the atmosphere are considered. The issues of reducing the error of the proposed methods are discussed. The article is partly based on a report presented at the conference “Modern Stellar Astronomy-2022”, held at the Caucasian Mountain Observatory of the Sternberg State Astronomical Institute, Moscow State University, in November 8–10, 2022.
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Walker, Alistair, Saul Adelman, Eugene Milone, Barbara Anthony-Twarog, Pierre Bastien, Wen Ping Chen, Steve Howell et al. „DIVISION B COMMISSION 25: ASTRONOMICAL PHOTOMETRY AND POLARIMETRY“. Proceedings of the International Astronomical Union 11, T29A (August 2015): 159–70. http://dx.doi.org/10.1017/s1743921316000727.

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Commission 25 (C25) deals with the techniques and issues involved with the measurement of optical and infrared radiation intensities and polarization from astronomical sources. As such, in recent years attention has focused on photometric standard stars, atmospheric extinction, photometric passbands, transformation between systems, nomenclature, and observing and reduction techniques. At the start of the trimester C25 changed its name from Stellar Photometry and Polarization to Astronomical Photometry and Polarization so as to explicitly include in its mandate particular issues arising from the measurement of resolved sources, given the importance of photometric redshifts of distant galaxies for many of the large photometric surveys now underway. We begin by summarizing commission activities over the 2012-2014 period, follow with a report on Polarimetry, continue with Photometry topics that have been of interest to C25 members, and conclude with a Vision for the Future.
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Howell, Steve B. „CCD Time-Series Photometry of Astronomical Sources“. Symposium - International Astronomical Union 167 (1995): 167–72. http://dx.doi.org/10.1017/s0074180900056400.

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CCDs are essentially the only instrument available today for photometry at most observatories; they are also becoming more readily available to amateurs as well. Thus, obtaining good photometric data with these two-dimensional devices is something we all need to understand. The history of and recent developments in CCD time-series photometry will be reviewed with some comments on future directions.
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Jiang, Shiyang. „The Large-Field Bright-Star High-Precision CCD Photometer of BAO“. Symposium - International Astronomical Union 167 (1995): 325–26. http://dx.doi.org/10.1017/s007418090005662x.

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Time-series high-accuracy photometry is very important for research in stellar variability. For a long time photometry made by a photomultiplier was the only instrument for high precision stellar photometry. To overcome the atmospheric variation and instrumental problems, we must choose at least one stable star as a comparison star and move the telescope quickly between the targets. So the real efficiency is very low and one only can do it on photometric nights. To overcome this limitation, since 1989 we began to cooperate with the team of the STEPHI network. We used the Chevreton four-channel photometer which can observe the variable, two comparison stars and a chosen sky background simultaneously. The multi-channel photometer is much better than normal single channel photometer as we can see from the several STEPHI results. Now the very high quantum efficiency CCD becomes more and more popular, so we are trying to change to use CCDs. Here we give some general description of a large field high accuracy bright star CCD photometer being prepared for the Beijing Astronomical Observatory (BAO).
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Tinbergen, Jaap. „New Techniques“. International Astronomical Union Colloquium 136 (1993): 130–46. http://dx.doi.org/10.1017/s025292110000748x.

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AbstractRoutine millimagnitude photometry may require a new approach to reduction of photometric errors. Such an approach is outlined in this paper; it stresses elimination of each error as close to its source as possible. The possibilities provided by modern technology are reviewed in this light. An engineering design group dedicated to photometry is a prerequisite and an on-site photometric technician may be necessary. In this concept, observers are mainly remote users of a database. Implied is the idea of accurate photometry necessarily developing into a single but multi-site astronomical facility (cf. VLBI) and the communal discipline that goes with it.
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Warner, Brian. „Astronomy in South Africa“. Highlights of Astronomy 10 (1995): 674–76. http://dx.doi.org/10.1017/s1539299600012545.

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This note reviews those aspects of astronomy in South Africa that may be useful for the support of astronomical development on the rest of the African continent.Optical and infrared astronomy is largely consolidated at the Sutherland site of the South African Astronomical Observatory (SAAO), about 300 km from Cape Town. The administrative and technical headquarters of this institution occupy the buildings of the old Royal Observatory (founded in 1820) in Cape Town. In Cape Town there is a twin 18/24 inch (0.45/0.6m) refractor and an 18-inch (0.45m) photometric reflector still operational. At Sutherland the 74-inch (1.8m Radcliffe) reflector is equipped for spectroscopy, CCD imaging and IR photometry. Newtonian and coudé foci are available but rarely used. Also at Sutherland there are 40-inch, 30-inch and 20-inch telescopes (approx. 1m, 0.75m and 0.5m) used primarily for CCD imaging (40-inch), optical and infrared photometry (30-inch) and UVBRI standard photometry (20-inch). An automatic photoelectric telescope (30-inch aperture) is nearing completion. Observing conditions at Sutherland provide about 50% photometric time.
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Osborn, J., D. Föhring, V. S. Dhillon und R. W. Wilson. „Atmospheric scintillation in astronomical photometry“. Monthly Notices of the Royal Astronomical Society 452, Nr. 2 (16.07.2015): 1707–16. http://dx.doi.org/10.1093/mnras/stv1400.

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Hudson, Hugh S. „Astronomical photometry from the moon“. Advances in Space Research 14, Nr. 6 (Juni 1994): 99–104. http://dx.doi.org/10.1016/0273-1177(94)90012-4.

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Brennan, S. J., und M. Fraser. „The Automated Photometry of Transients pipeline (AutoPhOT)“. Astronomy & Astrophysics 667 (November 2022): A62. http://dx.doi.org/10.1051/0004-6361/202243067.

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We present the Automated Photometry of Transients (AutoPhOT) package, a novel automated pipeline that is designed for rapid, publication-quality photometry of astronomical transients. AutoPhOT is built from the ground up using Python 3 – with no dependencies on legacy software. Capabilities of AutoPhOT include aperture and point-spread-function photometry, template subtraction, and calculation of limiting magnitudes through artificial source injection. AutoPhOT is also capable of calibrating photometry against either survey catalogues, or using a custom set of local photometric standards, and is designed primarily for ground-based optical and infrared images. We show that both aperture and point-spread-function photometry from AutoPhOT is consistent with commonly used software, for example, DAOPHOT, and also demonstrate that AutoPhOT can reproduce published light curves for a selection of transients with minimal human intervention.
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Pagul, Amanda, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt et al. „Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields“. Astrophysical Journal Supplement Series 273, Nr. 1 (01.07.2024): 10. http://dx.doi.org/10.3847/1538-4365/ad40a1.

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Abstract This article presents new astronomical source catalogs using data from the BUFFALO Survey. These catalogs contain detailed information for over 100,000 astronomical sources in the six BUFFALO clusters: A370, A2744, AS1063, MACS 0416, MACS 0717, and MACS 1149 spanning a total of 240 arcmin2. The catalogs include positions and forced photometry measurements of these objects in the F275W, F336W, F435W, F606W, F814W, F105W, F125W, F140W, and F160W HST bands, Keck-NIRC2/VLT-HAWKI Ks band, and IRAC Channel 1 and 2 bands. Additionally, we include photometry measurements in the F475W, F625W, and F110W bands for A370. This catalog also includes photometric redshift estimates computed via template fitting using LePhare. When comparing to a spectroscopic reference, we obtain an outlier fraction of 8.6% and scatter, normalized median absolute deviation, of 0.059. The catalogs are publicly available for their use by the community (https://archive.stsci.edu/hlsp/buffalo/).
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Dissertationen zum Thema "Photometry, astronomical"

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Krisciunas, Kevin. „RR lyrae stars and type Ia supernovae : discovery and calibration of astronomical standard candles /“. Thesis, Connect to this title online; UW restricted, 2000. http://hdl.handle.net/1773/5446.

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Patterson, J. Douglas. „CCD photometry of three short-period binary systems“. Virtual Press, 1993. http://liblink.bsu.edu/uhtbin/catkey/865934.

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The goal of this study was to obtain photometry of three poorly studied close binary star systems. These observations were obtained at Lowell Observatory in Flagstaff, Arizona and the Ball State University Observatory. In both cases charged coupled device detectors were used. Light variations were detected in all three stars. For one of the binaries the temperatures of the component stars were found by fitting multi-color light curves with black body models. In addition, the temperature difference between the two hemispheres of the secondary star was found. This difference is believed to be the product of heating by the stellar companion.
Department of Physics and Astronomy
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Hill, Robert L. „Computational starspot photometry of contact binary stars“. Virtual Press, 2007. http://liblink.bsu.edu/uhtbin/catkey/1369918.

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Starspots are not well understood for contact binary star systems. The following properties of spots were systematically investigated: temperature, radius, colatitude, and longitude. Spots were modeled on an AE Phe like contact binary system. The spots were changed in a systematic manner. The light curve phases of primary minimum and primary maximum were affected by these parameter changes in a systematic manner, as well as the secondary minimum and maximum. It will be shown that it is possible to use the shift in these phases to study starspots over time. This information can also be used to identify the presence of spots in binary star systems.Starspots on contact binary systems are not commonly found at a longitude near 180°. The results of this study show that starspots near 180° should be the easiest to detect using photometric techniques. This is the most significant result from this study. Either there is an unknown physical reason why contact binary stars do not have starspots near a longitude of 180°, or the starspots are there and the photometric data has been misinterpreted.
Department of Physics and Astronomy
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Samaddar, Debasmita. „Photometric variability of three brown dwarfs“. Access to citation, abstract and download form provided by ProQuest Information and Learning Company; downloadable PDF file 2.24 Mb., 65 p, 2006. http://proquest.umi.com/pqdlink?did=1075713471&Fmt=7&clientId=8331&RQT=309&VName=PQD.

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Mason, Justin R. „In search of red dwarf stars application of three-color photometric techniques /“. Muncie, IN : Ball State University, 2009. http://cardinalscholar.bsu.edu/659.

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Dunn, Jacqueline Michelle. „The stellar content and star formation rates of dwarf irregular galaxies“. Fort Worth, Tex. : Texas Christian University, 2007. http://etd.tcu.edu/etdfiles/available/etd-12052007-121555/unrestricted/Dunn.pdf.

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Elston, Richard Joseph. „Search for rapidly star-forming galaxies at high redshift“. Diss., The University of Arizona, 1988. http://hdl.handle.net/10150/184574.

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We have conducted three surveys to try and locate distant star forming galaxies. The most general survey used deep 2μ images with optical CCD photometry to locate objects with peculiar SEDs. Using the IR data we should be able to locate rapidly star forming galaxies to z = 25. With a 3σ detection limit of 18.5 at K we have found no objects with z > 5 but we have found several blue objects at z < 4 in 16min² of sky. This suggests tha there is no extremely luminous early phase of galaxy formation. We have found several blue objects at z < 4 in 10min² of sky. Of particular interest is an object which has a flat SED from V to K but shows a strong spectral break between B and V and a weaker break at 5800Å. We suggest these may be Lyman limit and Lyman α forest absorption at z-3.8 in a galaxy forming ≈400M(⊙) year⁻¹ of stars. A large sample of galaxies (100 objects) selected to have similar properties (R – I < .5, B – R > 1) has also been found. From this sample it appears this possible high redshift star forming phase only contributes 1/10 of the metal present in disks or spheroids. We have also found 30 Lyman α emission line companions to 12 z = 3 quasars. These objects have Lyman α equivalent widths (50Å) and luminosities (V = 24) consistent with galaxies forming ≈100M(⊙) year⁻¹ of stars. Also, 2 of the quasars have 8 companions and may be in cluster environments. A final survey analyzed optical to IR SEDs of luminous blue radio galaxies at z > 1. In these objects we find SEDs indicative of star formation rates between 10 and 100M(⊙) year⁻¹ but interpretation is difficult due to the AGN component of the sources. While these data seem to suggest a significant star forming phase taking place in galaxies at z ≈ 3-4, interpreting this result is difficult since we cannot determine if we are observing disk or spheroidal populations. In the case of the quasar companions and the radio galaxies, consideration of their dense environments and current epoch morphology suggest that these may be spheroids but these galaxies may not be typical of galaxies in general.
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DeCocq, John D. „The impact of abundance variations on photometric luminosity indicators“. Virtual Press, 1996. http://liblink.bsu.edu/uhtbin/catkey/1014853.

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Red dwarf stars are one proposed solution to the dark matter problem in the Milky Way Galaxy These cool, low luminosity stars are difficult to detect and segregate in surveys. This study utilizes photometric data obtained on the Kron-Cousins photometric system to develop criteria that classifies stars as red. Two of the color indices are then used to create a two-color diagram to allow separation of giant and dwarf stars. An algorithm based on calculated equations is provided to separate the giant and dwarf stars after detection. A third class of stars, subdwarfs, is addressed as a potential problem in future surveys. Some suggestions for detecting and removing these contaminating stars from the data are offered. Finally, a colormagnitude diagram is developed for red dwarf stars with KronCousins photometry. This curve allows for fairly accurate determination of photometric parallaxes for the red dwarf stars.An attempt was made to segregate the red dwarfs into velocity classes prior to calibrating the color-magnitude diagram. It was found that this approach offered no additional useful information.
Department of Physics and Astronomy
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Jeffers, Sandra Victoria. „Surface brightness distributions of late-type stars“. Thesis, University of St Andrews, 2005. http://hdl.handle.net/10023/12941.

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The aim of this work has been to increase our understanding of the surface brightness distributions of late-type stars through Doppler imaging and eclipse mapping techniques. Combining spectroscopic and photometric observations with the technique of Doppler Imaging, I have reconstructed surface images of the G2V star He 699 (for 08 October 2000), which show high latitude and polar structures. In the case of the KOV star AB Dor, the Doppler images for January 1992 and November 1993 show a large polar cap with small dark features also present at intermediate to high latitudes. As the phase sampling of the observations was insufficient to apply the sheared-image method it was not possible to detect any differential rotation. In the second part of my thesis I determine the surface brightness distribution of the primary component of the RS CVn eclipsing binary SV Cam. I have used extrapolated size distributions of sunspots to an active star to synthesize images of stellar photospheres with high spot filling factors. The resulting surface images, reconstructed with the Maximum Entropy eclipse mapping technique, show large spurious spot features at the quadrature points. It is concluded that two-spot modelling or chi-squared minimisation techniques are more susceptible to spurious structures being generated by systematic errors, arising from incorrect assumptions about photospheric surface brightness, than simple Fourier analysis of the light-curves. Spectrophotometric data from 9 HST orbits, observed in November 2001, have been used to eclipse-map the primary component of SV Cam. In combination with its HIPPAR- COS parallax it is found that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. This flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. However, when the spottedness from the eclipsed region is applied to the entire surface of the primary star, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48+/-6 deg. When the Maximum Entropy eclipse mapping technique is used to fit SV Cam's lightcurve, the observed minus computed residuals show strong spurious peaks at the quadrature points. It is only possible to reduce these peaks with the addition of a polar cap and the reduction of the primary star's temperature, to account for the star being peppered with unresolvable spots. Motivated by this result we investigate the limb darkening of the primary component of SV Cam. The wavelength dependence of the limb darkening is analysed by sub-dividing the HST lightcurve into 10 bands of equal emission flux. Flux variations between the first and fourth contact of the primary eclipse indicate that the limb darkening decreases towards longer wavelengths, in accordance with published limb darkening laws. Comparing fits of ATLAS and PHOENIX model atmospheres we find a wavelength dependence of the best fitting model. Due to its smooth cutoff at the stellar limb, the spherical geometry of the PHOENIX model atmosphere gives the best fit during partial eclipse. Between the second and third contact the difference between spherical and plane-parallel geometry is less important.
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Spencer, Locke Dean, und University of Lethbridge Faculty of Arts and Science. „Spectral characterization of the Herschel SPIRE photometer“. Thesis, Lethbridge, Alta. : University of Lethbridge, Faculty of Arts and Science, 2005, 2005. http://hdl.handle.net/10133/291.

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The European Space Agency's Herschel Space Observatory is comprised of three cryogenically cooled instruments commissioned to explore the far infrared/submillimetre universe. The Spectral and Photometric Imaging REceiver (SPIRE) is one of Herschel's instruments and consists of a three band imaging photometer and a two band imaging spectrometer. Canada is involved in the SPIRE project through provision of instrument development hardware and software, mission flight software, and support personnel. This thesis discusses Fourier transform spectroscopy (FTS) and FTS data processing. A detailed discussion is included on FTS phase correction, with results presented from the optimization of an enhanced Forman phase correction routine developed for this work. This thesis discusses the design, verification, and use of the hardware and software provided by Dr. Naylor's group as it relates to SPIRE verification testing. Results of the photometer characterization are presented. The current status of SPIRE and its future schedule is also discussed.
xvii, 239 leaves : ill. (some col.) ; 28 cm.
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Bücher zum Thema "Photometry, astronomical"

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Milone, Eugene F., und C. Sterken, Hrsg. Astronomical Photometry. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2.

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Warner, Brian. High speed astronomical photometry. Cambridge [Cambridgeshire]: Cambridge University Press, 1988.

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Warner, Brian. High speed astronomical photometry. Cambridge: Cambridge University Press, 1988.

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Sterken, C. Astronomical photometry: A guide. Dordrecht: Kluwer Academic Publishers, 1992.

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Sterken, Chr, und J. Manfroid. Astronomical Photometry, a Guide. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2476-8.

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25, IAU Commission, American Astronomical Society. Historical Astronomy Division und American Astronomical Society, Hrsg. Astronomical photometry: Past, present, and future. New York: Springer, 2011.

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J, Borucki William, und Ames Research Center, Hrsg. Second workshop on improvements to photometry. Moffett Field, Calif: NASA Ames Research Center, 1988.

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Workshop on Improvements to Photometry (2nd 1987 Gaithersburg, Md.). Second Workshop on Improvements to Photometry. Moffett Field, Calif: NASA Ames Research Center, 1988.

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J, Butler C., und Elliott I. 1936-, Hrsg. Stellar photometry: Current techniques and future developments : proceedings of the IAU Colloquium no. 136 held in Dublin, Ireland, 4-7 August 1992. Cambridge: Cambridge University Press, 1993.

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Milone, E. F., und C. Sterken. Astronomical photometry: Past, present, and future. Herausgegeben von IAU Commission 25, American Astronomical Society. Historical Astronomy Division und American Astronomical Society. New York: Springer, 2011.

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Buchteile zum Thema "Photometry, astronomical"

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Stetson, Peter B. „Astronomical Photometry“. In Planets, Stars and Stellar Systems, 1–34. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5618-2_1.

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Milone, E. F., und Jan Willem Pel. „The High Road to Astronomical Photometric Precision: Differential Photometry“. In Astronomical Photometry, 33–68. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_2.

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Sterken, Christiaan, E. F. Milone und Andrew T. Young. „Photometric Precision and Accuracy“. In Astronomical Photometry, 1–32. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_1.

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Bastien, Pierre. „Measurement of Polarized Light in Astronomy“. In Astronomical Photometry, 201–12. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_10.

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Howell, Steve B. „High Precision Differential Photometry with CCDs: A Brief History“. In Astronomical Photometry, 71–84. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_3.

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Ambruster, Carol W., Anthony B. Hull, Robert H. Koch und Richard J. Mitchell. „The Pierce-Blitzstein Photometer“. In Astronomical Photometry, 85–107. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_4.

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Landolt, Arlo U. „Johnson Photometry and Its Descendants“. In Astronomical Photometry, 109–25. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_5.

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Milone, E. F., und Andrew T. Young. „The Rise and Improvement of Infrared Photometry“. In Astronomical Photometry, 127–43. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_6.

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Wing, Robert F. „On the Use of Photometry in Spectral Classification“. In Astronomical Photometry, 145–78. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_7.

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Cohen, Martin. „Absolute Photometry: Past and Present“. In Astronomical Photometry, 179–88. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8050-2_8.

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Konferenzberichte zum Thema "Photometry, astronomical"

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Gupta, Shivank. „IOT enabled astronomical photometry“. In 2016 5th International Conference on Wireless Networks and Embedded Systems (WECON). IEEE, 2016. http://dx.doi.org/10.1109/wecon.2016.7993494.

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Ferrero, Alejandro, Riccardo Felletti, Lorraine Hanlon, Joaquin Campos und Alicia Pons. „Electron-multiplying CCD astronomical photometry“. In IS&T/SPIE Electronic Imaging, herausgegeben von Erik Bodegom und Valérie Nguyen. SPIE, 2010. http://dx.doi.org/10.1117/12.840225.

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Selman, Fernando J. „Photometric flats: an essential ingredient for photometry with wide-field imagers“. In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2004. http://dx.doi.org/10.1117/12.551357.

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Joko, Satria A., Mohd Zambri Zainuddin, Swee-Ping Chia, Kurunathan Ratnavelu und Muhamad Rasat Muhamad. „Fried Parameter Analysis of Astronomical Photometry“. In FRONTIERS IN PHYSICS: 3rd International Meeting. AIP, 2009. http://dx.doi.org/10.1063/1.3192247.

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Pugliese, Giovanna, und Domenico Bonaccini Calia. „Photometry and astrometry with anisoplanatic AO images“. In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2004. http://dx.doi.org/10.1117/12.553116.

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Takato, Naruhisa. „Pupil-segmented photometry for lunar occultation observation“. In Astronomical Telescopes and Instrumentation, herausgegeben von Masanori Iye und Alan F. M. Moorwood. SPIE, 2003. http://dx.doi.org/10.1117/12.459998.

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Fiorentino, Giuliana, Davide Massari, Alan McConnachie, Peter B. Stetson, Giuseppe Bono, Paolo Turri, David Andersen et al. „Stellar photometry with multi conjugate adaptive optics“. In SPIE Astronomical Telescopes + Instrumentation, herausgegeben von Enrico Marchetti, Laird M. Close und Jean-Pierre Véran. SPIE, 2016. http://dx.doi.org/10.1117/12.2234448.

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Dravins, Dainis, Daniel Faria und Bo Nilsson. „Avalanche diodes as photon-counting detectors in astronomical photometry“. In Astronomical Telescopes and Instrumentation, herausgegeben von Masanori Iye und Alan F. M. Moorwood. SPIE, 2000. http://dx.doi.org/10.1117/12.395485.

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Elliott, David G. „DPhot photometry method for the Spitzer Space Telescope“. In SPIE Astronomical Telescopes + Instrumentation, herausgegeben von John C. Mather, Howard A. MacEwen und Mattheus W. M. de Graauw. SPIE, 2006. http://dx.doi.org/10.1117/12.659989.

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Tulloch, Simon M. „Photon counting and fast photometry with L3 CCDs“. In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2004. http://dx.doi.org/10.1117/12.550353.

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