Academic literature on the topic 'Instrumentation, Techniques, and Astronomical Observations'
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Journal articles on the topic "Instrumentation, Techniques, and Astronomical Observations"
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Sawant, Sailee M., and Daniel Batcheldor. "Charge-injection Device Imaging of Sirius with Contrast Ratios Greater than 1:26 Million." Publications of the Astronomical Society of the Pacific 134, no. 1033 (March 1, 2022): 034503. http://dx.doi.org/10.1088/1538-3873/ac54c2.
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Abstract The intrinsic nature of many astronomical objects, such as binary and multiple systems, exoplanets, circumstellar and debris disks, and quasar host galaxies, introduces challenging requirements for observational instrumentation and techniques. In each case, we encounter situations where the light from bright sources hampers our ability to detect surrounding fainter targets. To explore all features of such astronomical scenes, we must perform observations at the maximum possible contrast ratios. Charge-injection devices (CIDs) are capable of potentially exceeding contrast ratios of log 10 ( CR ) > 9 (i.e., 1 part in 1 billion) due to their unique readout architectures and inherent anti-blooming abilities. An on-sky testing of a commercially available CID, SpectraCAM XDR (SXDR), demonstrated raw contrast ratios from sub-optimal ground-based astronomical observations that imposed practical limits on the maximum achievable contrast ratios using CIDs. Here, we demonstrate the extreme contrast ratio imaging capabilities of the SXDR using observations of Sirius with the 1.0 m Jacobus Kapteyn Telescope, La Palma, Spain. Based on wavelet-based analysis and precise photometric and astrometric calibrations, we report a direct contrast ratio of Δm r = 18.54, log 10 ( CR ) = 7.41 ± 0.08 , or 1 part in 26 million. This is an order of magnitude higher compared to the previous CID results.
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De la Luz, Victor, J. Americo Gonzalez-Esparza, Maria A. Sergeeva, Pedro Corona-Romero, L. Xavier González, Julio C. Mejia-Ambriz, Jose F. Valdés-Galicia, et al. "First joint observations of space weather events over Mexico." Annales Geophysicae 36, no. 5 (October 11, 2018): 1347–60. http://dx.doi.org/10.5194/angeo-36-1347-2018.
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Abstract. The Mexican Space Weather Service (SCiESMEX in Spanish) and National Space Weather Laboratory (LANCE in Spanish) were organized in 2014 and in 2016, respectively, to provide space weather monitoring and alerts, as well as scientific research in Mexico. In this work, we present the results of the first joint observations of two events (22 June and 29 September 2015) with our local network of instruments and their related products. This network includes the MEXART radio telescope (solar flare and radio burst), the Compact Astronomical Low-frequency, Low-cost Instrument for Spectroscopy in Transportable Observatories (CALLISTO) at the MEXART station (solar radio burst), the Mexico City Cosmic Ray Observatory (cosmic ray fluxes), GPS receiver networks (ionospheric disturbances), and the Teoloyucan Geomagnetic Observatory (geomagnetic field). The observations show that we detected significant space weather effects over the Mexican territory: geomagnetic and ionospheric disturbances (22 June 2015), variations in cosmic ray fluxes, and also radio communications' interferences (29 September 2015). The effects of these perturbations were registered, for the first time, using space weather products by SCiESMEX: total electron content (TEC) maps, regional geomagnetic index Kmex, radio spectrographs of low frequency, and cosmic ray fluxes. These results prove the importance of monitoring space weather phenomena in the region and the need to strengthening the instrumentation network. Keywords. Solar physics, astrophysics, and astronomy (instruments and techniques)
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Li, T. P. "Imaging in Hard X-ray Astronomy." Symposium - International Astronomical Union 214 (2003): 70–83. http://dx.doi.org/10.1017/s0074180900194173.
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The energy range of hard X-rays is a key waveband to the study of high energy processes in celestial objects, but still remains poorly explored. In contrast to direct imaging methods used in the low energy X-ray and high energy gamma-ray bands, currently imaging in the hard X-ray band is mainly achieved through various modulation techniques. A new inversion technique, the direct demodulation method, has been developed since early 90s. with this technique, wide field and high resolution images can be derived from scanning data of a simple collimated detector. The feasibility of this technique has been confirmed by experiment, balloon-borne observation and analyzing simulated and real astronomical data. Based the development of methodology and instrumentation, a high energy astrophysics mission – Hard X-ray Modulation Telescope (HXMT) has been proposed and selected in China for a four-year Phase-A study. The main scientific objectives are a full-sky hard X-ray (20–200 keV) imaging survey and high signal-to-noise ratio timing studies of high energy sources.
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Modiri, Sadegh, Robert Heinkelmann, Santiago Belda, Zinovy Malkin, Mostafa Hoseini, Monika Korte, José M. Ferrándiz, and Harald Schuh. "Towards Understanding the Interconnection between Celestial Pole Motion and Earth’s Magnetic Field Using Space Geodetic Techniques." Sensors 21, no. 22 (November 13, 2021): 7555. http://dx.doi.org/10.3390/s21227555.
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The understanding of forced temporal variations in celestial pole motion (CPM) could bring us significantly closer to meeting the accuracy goals pursued by the Global Geodetic Observing System (GGOS) of the International Association of Geodesy (IAG), i.e., 1 mm accuracy and 0.1 mm/year stability on global scales in terms of the Earth orientation parameters. Besides astronomical forcing, CPM excitation depends on the processes in the fluid core and the core–mantle boundary. The same processes are responsible for the variations in the geomagnetic field (GMF). Several investigations were conducted during the last decade to find a possible interconnection of GMF changes with the length of day (LOD) variations. However, less attention was paid to the interdependence of the GMF changes and the CPM variations. This study uses the celestial pole offsets (CPO) time series obtained from very long baseline interferometry (VLBI) observations and data such as spherical harmonic coefficients, geomagnetic jerk, and magnetic field dipole moment from a state-of-the-art geomagnetic field model to explore the correlation between them. In this study, we use wavelet coherence analysis to compute the correspondence between the two non-stationary time series in the time–frequency domain. Our preliminary results reveal interesting common features in the CPM and GMF variations, which show the potential to improve the understanding of the GMF’s contribution to the Earth’s rotation. Special attention is given to the corresponding signal between FCN and GMF and potential time lags between geomagnetic jerks and rotational variations.
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Drew, Patrick M., and Caitlin M. Casey. "No Redshift Evolution of Galaxies’ Dust Temperatures Seen from 0 < z < 2." Astrophysical Journal 930, no. 2 (May 1, 2022): 142. http://dx.doi.org/10.3847/1538-4357/ac6270.
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Abstract Some recent literature has claimed there to be an evolution in galaxies’ dust temperatures toward warmer (or colder) spectral energy distributions (SEDs) between low and high redshift. These conclusions are driven by both theoretical models and empirical measurement. Such claims sometimes contradict one another and are prone to biases in samples or SED fitting techniques. What has made direct comparisons difficult is that there is no uniform approach to fitting galaxies’ infrared/millimeter SEDs. Here we aim to standardize the measurement of galaxies’ dust temperatures with a python-based SED fitting procedure, MCIRSED. 1 1 Publicly available at github.com/pdrew32/mcirsed. We draw on reference data sets observed by Infrared Astronomical Satellite, Herschel, and Scuba-2 to test for redshift evolution out to z ∼ 2. We anchor our work to the L IR–λ peak plane, where there is an empirically observed anticorrelation between IR luminosity and rest-frame peak wavelength (an observational proxy for luminosity-weighted dust temperature) such that λ peak = λ t ( L IR / L t ) η where η = −0.09 ± 0.01, Lt = 1012 L ⊙, and λ t = 92 ± 2 μm. We find no evidence for redshift evolution of galaxies’ temperatures, or λ peak, at fixed L IR from 0 < z < 2 with >99.99% confidence. Our finding does not preclude evolution in dust temperatures at fixed stellar mass, which is expected from a nonevolving L IR–λ peak relation and a strongly evolving SFR–M⋆ relation. The breadth of dust temperatures ( σ log λ peak ) at a given L IR is likely driven by variation in galaxies’ dust geometries and sizes, and it does not evolve. Testing for L IR–λ peak evolution toward higher redshift (z ∼ 5−6) requires better sampling of galaxies’ dust SEDs near their peaks (observed ∼200–600 μm) with ≲1 mJy sensitivity. This poses a significant challenge to current instrumentation.
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Yoshizawa, M. "New Astrometric Instrumentation in Japan." Symposium - International Astronomical Union 166 (1995): 31–34. http://dx.doi.org/10.1017/s0074180900227794.
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The meridian circle is one of the most fundamental instrument in the field of astrometry where the astronomical objects are studied observationally for positions and their changes on the celestial sphere. At the Tokyo Astronomical Observatory (= National Astronomical Observatory since July, 1988) the Gautier Meridian Circle of 1903 was used until 1982 for various international meridian circle observations like SRS and NPZT programs, as well as for observations of OB stars, and the Moon and planets.
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Davydov, V. Yu. "Compensation of refraction in astronomical interference observations." Measurement Techniques 36, no. 6 (June 1993): 662–67. http://dx.doi.org/10.1007/bf00980011.
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Branham, Richard L. "Techniques for dealing with discordant observations." Symposium - International Astronomical Union 114 (1986): 229–31. http://dx.doi.org/10.1017/s0074180900148247.
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To test any theory such as theories of motion–Newtonian or relativistic–of solar system objects, one must compare the predictions of theory with observation. But discordant observations habitually plague the reducer of astronomical data. To alleviate the baleful effects, particularly harmful when the observations are reduced by the method of least squares, of discordant data investigators almost invariably reject observations whose corresponding (0-C)'s or post-solution residuals exceed a cutoff. But techniques that are insensitive to the assumption that the observational errors are normally distributed, called robust estimation in the literature, have also been developed.
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Guélin, Michel. "Radio and Millimetre Observations of Less Complex Molecules." Symposium - International Astronomical Union 120 (1987): 171–81. http://dx.doi.org/10.1017/s0074180900153987.
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Progress in laboratory and astronomical instrumentation has renewed the already large interest for simple astrophysical molecules. On the laboratory side, one of the most notable advances has been the spectroscopic observation of an increasing number of small reactive molecular species. On the astronomical side, the access to submillimetre wavelengths and the completion of millimetric interferometers and large single-dish telescopes, have allowed the detection of many new molecular species and open the way for detailed studies of the distribution of molecules in interstellar and circumstellar clouds.
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Edberg, Stephen J. "Working with Amateur Astronomers." International Astronomical Union Colloquium 98 (1988): 95–99. http://dx.doi.org/10.1017/s0252921100092307.
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Amateur astronomers have a vast store of talent and expertise in making astronomical observations. When carefully channelled, their enthusiasm coupled with these characteristics can lead to the acquisition of large volumes of high-quality astronomical data. The Amateur Observation Network of the International Halley Watch (IHW) was organized to encourage comet observations by amateurs, standardize techniques whenever possible, and then collect and archive these observations for use by the astronomical community in the near and distant future as part of the whole IHW archive. The lessons learned from this experience will be useful to organizers who plan observation campaigns involving amateur astronomers in the future.
Dissertations / Theses on the topic "Instrumentation, Techniques, and Astronomical Observations"
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Isaak, Katherine Gudrun. "Low-noise instrumentation and astronomical observations of high-redshift objects in submillimetre wavelengths." Thesis, University of Cambridge, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.364389.
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Chippendale, Aaron Paul. "Detecting cosmological reionization on large scales through the 21 cm HI line." University of Sydney, 2009. http://hdl.handle.net/2123/6256.
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Doctor of Philosophy (PhD)This thesis presents the development of new techniques for measuring the mean redshifted 21 cm line of neutral hydrogen during reionization. This is called the 21 cm cosmological reionization monopole. Successful observations could identify the nature of the first stars and test theories of galaxy and large-scale structure formation. The goal was to specify, construct and calibrate a portable radio telescope to measure the 21 cm monopole in the frequency range 114 MHz to 228 MHz, which corresponds to the redshift range 11.5 > z > 5.2. The chosen approach combined a frequency independent antenna with a digital correlation spectrometer to form a correlation radiometer. The system was calibrated against injected noise and against a modelled galactic foreground. Components were specified for calibration of the sky spectrum to 1 mK/MHz relative accuracy. Comparing simulated and measured spectra showed that bandpass calibration is limited to 11 K, that is 1% of the foreground emission, due to larger than expected frequency dependence of the antenna pattern. Overall calibration, including additive contributions from the system and the radio foreground, is limited to 60 K. This is 160 times larger than the maximum possible monopole amplitude at redshift eight. Future work will refine and extend the system known as the Cosmological Reionization Experiment Mark I (CoRE Mk I).
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Wu, Ya-Lin, Laird M. Close, Vanessa P. Bailey, Timothy J. Rodigas, Jared R. Males, Katie M. Morzinski, Katherine B. Follette, et al. "MAGELLAN AO SYSTEM z ′, Y S , AND L ′ OBSERVATIONS OF THE VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621262.
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We analyze archival data from Bailey and co-workers from the Magellan adaptive optics system and present the first 0.9 mu m detection (z' = 20.3 +/- 0.4 mag; Delta z' = 13.0 +/- 0.4 mag) of the 11 M-Jup circumbinary planet HD 106906AB b, as well as 1 and 3.8 mu m detections of the debris disk around the binary. The disk has an east-west asymmetry in length and surface brightness, especially at 3.8 mu m where the disk appears to be one-sided. The spectral energy distribution of b, when scaled to the K-S-band photometry, is consistent with 1800 K atmospheric models without significant dust reddening, unlike some young, very red, low-mass companions such as CT Cha B and 1RXS 1609 B. Therefore, the suggested circumplanetary disk of Kalas and co-workers might not contain much material, or might be closer to face-on. Finally, we suggest that the widest (a greater than or similar to 100 AU) low mass ratio (M-p/M-star = q less than or similar to 0.01) companions may have formed inside protoplanetary disks but were later scattered by binary/planet interactions. Such a scattering event may have occurred for HD 106906AB b with its central binary star, but definitive proof at this time is elusive.
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Mate, Sujay. "Développement d'un simulateur du ciel pour les instruments à grand champ de vue X-gamma en orbite terrestre basse : application à l'évaluation des performances du spectro-imageur SVOM-ECLAIRs." Thesis, Toulouse 3, 2021. http://www.theses.fr/2021TOU30031.
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Les sursauts gamma (Gamma-Ray Bursts ou GRBs) sont les explosions les plus lumineuses de l'univers. On les observe sous la forme de bouffées de rayons X/ƴ (d'une durée de quelques millisecondes à quelques dizaines de secondes) suivies d'une émission rémanente (généralement à de plus grandes longueurs d'onde). Ils résultent soit de la fusion de deux objets compacts (une paire d'étoiles à neutrons ou une étoile à neutrons et un trou noir), soit de l'effondrement du noyau d'une étoile massive (>15 masse solaire). Les GRBs sont d'excellents candidats pour étudier la physique aux énergies et densités extrêmes et un outil astrophysique pour sonder l'histoire de l'univers car ils sont observés à tous les âges de celui-ci. La mission spatiale Sino-Française SVOM (lancement prévu en juin 2022) a pour objectif la détection et l'étude des GRBs à l'aide d'instruments spatiaux et terrestres dédiés afin d'obtenir une couverture multi-longueurs d'onde. Le principal instrument à bord du satellite SVOM est ECLAIRs, un imageur à masque codé à grand champ de vue (~2 sr) fonctionnant dans la bande d'énergie de 4 à 150 keV. ECLAIRs détectera et localisera les GRBs (ainsi que d'autres sources transitoires à hautes énergies) en temps quasi réel grâce à son " trigger " embarqué. Le bruit de fond d'ECLAIRs est élevé et variable en raison du grand champ de vue et de la stratégie de pointage de SVOM qui amène la Terre à transiter dans le champ de vue. Une nouvelle méthode (appelée "Particle Interaction Recycling Approach" ou PIRA en anglais), basée sur des simulations de Monte-Carlo (GEANT4), a été développée pour estimer précisément et rapidement le bruit de fond variable. Les simulations du bruit de fond sont complétées avec des sources X et des sursauts gamma afin de générer des scénarios d'observation complets. Le bruit de fond variable d'ECLAIRs pose des problèmes pour la détection des GRBs et affecte la sensibilité de l'instrument. Nous avons évalué les performances du "trigger" embarqué, notamment l'impact du bruit de fond sur la détection des sources transitoires et sa sensibilité aux caractéristiques des GRBs (durée, profil temporel, forme spectrale, position dans le champ de vue). ECLAIRs enverra au sol tous les photons détectés. De plus, la disponibilité d'une plus grande puissance de calcul et une meilleure connaissance du contexte (par exemple, les variations du bruit de fond, les sources dans le champ de vue, etc.) au sol, nous ont conduits à développer un "trigger" sol pour surmonter les difficultés rencontrées par le "trigger" embarqué. Ainsi, nous proposons un algorithme basé sur des transformées en ondelettes pour détecter les GRBs dans le cadre du "trigger" sol. Les travaux de cette thèse, à savoir le développement de PIRA, l'évaluation des performances et le développement d'un nouvel algorithme de détection de sursauts, fournissent une base solide pour construire un "trigger" sol efficace, qui complétera le "trigger" embarqué et améliorera les performances globales de la mission SVOMGamma-Ray Bursts (GRBs) are the most luminous explosions in the universe. They are observed as bright flashes of gamma/X-rays (lasting a few milliseconds to a few tens of seconds) followed by an "afterglow" emission (usually at longer wavelengths). They are produced either due to the merger of two compact objects (a pair of neutron stars or a neutron star and a black hole) or due to the core collapse of a massive star (> 15 solar mass). GRBs are excellent candidates to study physics at extreme energies and densities. They also constitute important astrophysical tools to probe the history of the universe as they are observed at all epochs. The upcoming (June 2022) Sino-French mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) aims to detect and study GRBs using dedicated space and ground based instruments to obtain multi-wavelength coverage. The primary instrument onboard SVOM spacecraft is ECLAIRs, a wide-field (~ 2 sr) coded-mask imager sensitive in the 4 - 150 keV energy range. ECLAIRs will detect and localise GRBs (and other high energy transients) in near real time using an onboard trigger. ECLAIRs will encounter a high and variable background due to the wide field-of-view (FoV) and the pointing strategy of SVOM which makes the Earth transit through the FoV. A new method (called Particle Interaction Recycling Approach or PIRA), based on Monte-Carlo simulations (GEANT4), was developed to estimate the variable background accurately and rapidly. The simulations of the background are complemented with simulations of X-ray sources and gamma-ray bursts to generate complete observation scenarios. The variable background of ECLAIRs poses challenges to detect GRBs and affects the sensitivity of the instrument. We use the simulated data to evaluate the performance of the onboard trigger, in particular, the impact of the variable background and its sensitivity to the GRB characteristics (duration, temporal profile, spectral shape,position in the FoV). ECLAIRs will send all detected photons to the ground. In addition, the availability of a larger computational power and the better knowledge of the context (e.g. background variations, sources in the FoV, etc.) on the ground motivates us to develop an "offline trigger" to overcome the challenges faced by the onboard trigger. An algorithm based on wavelet transforms is proposed to detect GRBs as part of the offline trigger. The work in this thesis, i.e. the development of PIRA, instrument's performance evaluation and development of a trigger method, provides a sound basis to build an effective offline trigger that will complement the onboard trigger and improve the overall performance of the SVOM mission
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Daigle, Olivier. "Spectro-imagerie optique à faible flux et comparaison de la cinématique Hα et HI d'un échantillon de galaxies proches." Aix-Marseille 1, 2010. http://www.theses.fr/2010AIX10141.
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Un nouveau contrôleur de EMCCD (Electron multiplying Charge Coupled Device) est présenté. Il permet de diminuer significativement le bruit qui domine lorsque la puce EMCCD est utilisé pour du comptage de photons: le bruit d'injection de charge. À l'aide de ce contrôleur, une caméra EMCCD scientifique a été construite, caractérisée en laboratoire et testée à l'observatoire du mont Mégantic. Cette nouvelle caméra permet, entre autres, de réaliser des observations de la cinématique des galaxies par spectroscopie de champ intégral par interférométrie de Fabry-Perot en lumière Ha beaucoup plus rapidement, ou de galaxies de plus faible luminosité, que les caméras à comptage de photon basées sur des tubes amplificateurs. Le temps d'intégration nécessaire à l'obtention d'un rapport signal sur bruit donné est environ 4 fois moindre qu'avec les anciennes caméras. Les applications d'un tel appareil d'imagerie sont nombreuses: photométrie rapide et faible flux, spectroscopie à haute résolution spectrale et temporelle, imagerie limitée par la diffraction à partir de télescopes terrestres (lucky imaging), etc. D'un point de vue technique, la caméra est dominée par le bruit de Poisson pour les flux lumineux supérieurs à 0. 002 photon/pixel/image. D'un autre côté, la raie d'hydrogène neutre (HI) à 21 cm a souvent été utilisée pour étudier la cinématique des galaxies. L'hydrogène neutre a l'avantage de se retrouver en quantité détectable au-delà du disque optique des galaxies. Cependant, la résolution spatiale de ces observations est moindre que leurs équivalents réalisés en lumière visible. Lors de la comparaison des données HI, avec des données à plus haute résolution, certaines différences étaient simplement attribuées à la faible résolution des observations HI. Le projet THINGS (The HI Nearby Galaxy Survey a observé plusieurs galaxies de l'échantillon SINGS (Spitzer Infrared Nearby Galaxies Survey). Les données cinématiques du projet THIGNS seront comparées aux données cinématiques obtenues en lumière Ha, afin de déterminer si la seule différence de résolution spatiale peut expliquer les différences observées. Les résultats montrent que des différences intrinsèques aux traceurs utilisées (hydrogène neutre ou ionisé), sont responsables de dissemblances importantes. La compréhension de ces particularités est importante: la distribution de la matière sombre, dérivée de la rotation des galaxies, est un test de certains modèles cosmologiquesA new EMCCD (Electron multiplying Charge Coupled Device) controller is presented. It allows the EMCCD to be used for photon counting by drastically taking down its dominating source of noise : the clock induced charges. A new EMCCD camera was built using this controller. It has been characterized in laboratory and tested at the observatoire du mont Mégantic. When compared to the previous generation of photon counting cameras based on intensifier tubes, this new camera renders the observation of the galaxies kinematics with an integral field spectrometer with a Fabry-Perot interferometer in Ha light much faster, and allows fainter galaxies to be observed. The integration time required to reach a given signal-to-noise ratio is about 4 times less than with the intensifier tubes. Many applications could benefit of such a camera: fast, faint flux photometry, high spectral and temporal resolution spectroscopy, earth-based diffraction limited imagery (lucky imaging), etc. Technically, the camera is dominated by the shot noise for flux higher than 0. 002 photon/pixel/image. The 21 cm emission line of the neutral hydrogen (HI) is often used to map the galaxies kinematics. The extent of the distribution of the neutral hydrogen in galaxies, which goes well beyond the optical disk, is one of the reasons this line is used so often. However, the spatial resolution of such observations is limited when compared to their optical equivalents. When comparing the HI data to higher resolution ones, some differences were simply attributed to the beam smearing of the HI caused by its lower resolution. The THINGS (The HI Nearby Galaxy Survey) project observed many galaxies of the SINGS (Spitzer Infrared Nearby Galaxies Survey) project. The kinematics of THINGS will be compared to the kinematic data of the galaxies obtained in Ha light. The comparison will try to determine whether the sole beam smearing is responsible of the differences observed. The results shows that intrinsic dissimilarities between the kinematical tracers used are responsible of some of the observed disagreements. The understanding of theses differences is of a high importance as the dark matter distribution, inferred from the rotation of the galaxies, is a test to some cosmological models
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Lamb, Masen. "On the calibration and use of Adaptive Optics systems: RAVEN observations of metal-poor stars in the Galactic Bulge and the application of focal plane wavefront sensing techniques." Thesis, 2017. https://dspace.library.uvic.ca//handle/1828/8368.
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Adaptive optics holds a fundamental role in the era of thirty meter class telescopes; this technology has gained such import that is incorporated into all first light instruments of both the upcoming E-ELT and TMT telescopes. Moreover, each of these telescopes are planning to use advanced forms of adaptive optics to exploit unprecedented scientific niches, such as Multi-Conjugate Adaptive Optics and Multi-Object Adaptive Optics. The complexity of these systems requires careful preliminary considerations, such as demonstration of the technology on existing telescopes and effective calibration procedures. In this thesis I address these two considerations through two different approaches. First, I demonstrate the use of the Multi-Object Adaptive Op- tics demonstrator RAVEN to gather high-resolution spectroscopy for the first time with this technology, and I identify some of the most metal-poor stars in the Galactic bulge to date. Secondly, I develop two focal plane wavefront sensing techniques to calibrate the internal aberrations of RAVEN and explore their applications to other adaptive optics systems.

I analyze spectra of individual stars in two Globular Clusters to establish infrared techniques that can be used with the RAVEN instrument. Detailed chemical abundances for five stars in NGC 5466 and NGC 5024, are presented from high-resolution optical (from the Hobby-Eberley Telescope) and infrared spectra (from the SDSS- III APOGEE survey). I find [Fe/H] = -1.97 ± 0.13 dex for NGC 5466, and [Fe/H] = -2.06 ± 0.13 dex for NGC 5024, and the typical abundance pattern for globular clusters for the remaining elements, e.g. both show evidence for mixing in their light element abundance ratios (C, N), and asymptotic giant branch contributions in their heavy element abundances (Y, Ba, and Eu). These clusters were selected to examine chemical trends that may correlate them with the Sgr dwarf galaxy remnant, but at these low metallicities no obvious differences from the Galactic abundance pattern are found. Regardless, I compare my results from the optical and infrared analyses to find that oxygen and silicon abundances determined from the infrared spectral lines are in better agreement with the other α-element ratios and with smaller random errors.
Using the aforementioned infrared techniques, I derive the chemical abundances for five metal-poor stars in and towards the Galactic bulge from the H-band spectroscopy taken with RAVEN at the Subaru 8.2-m telescope. Three of these stars are in the Galactic bulge and have metallicities between -2.1 < [Fe/H] < -1.5, and high [α/Fe] ∼ +0.3, typical of Galactic disc and bulge stars in this metallicity range; [Al/Fe] and [N/Fe] are also high, whereas [C/Fe] < +0.3. An examination of their orbits suggests that two of these stars may be confined to the Galactic bulge and one is a halo trespasser, though proper motion values used to calculate orbits are quite uncertain. An additional two stars in the globular cluster M22 show [Fe/H] values consistent to within 1σ , although one of these two stars has [Fe/H] = -2.01 ± 0.09, which is on the low end for this cluster. The [α/Fe] and [Ni/Fe] values differ by 2, with the most metal-poor star showing significantly higher values for these elements. M22 is known to show element abundance variations, consistent with a multipopulation scenario though our results cannot discriminate this clearly given our abundance uncertainties. This is the first science demonstration of multi-object adaptive optics with high-resolution infrared spectroscopy, and we also discuss the feasibility of this technique for use in the upcoming era of 30-m class telescope facilities.
Lastly, I develop two focal plane wavefront sensing techniques to calibrate the non-common path aberrations (NCPA) in adaptive optics systems. I first demonstrate these techniques in a detailed simulation of the future TMT instrument NFIRAOS. I then validate these techniques on an experimental bench subject to NFIRAOS-like wavefront errors. The two techniques are subsequently used to identify and correct the NCPA on both RAVEN and the NFIRAOS test-bench knowns as HeNOS. The application of these techniques is also explored on the VLT/SPHERE system to identify what is known as the ‘Low Wind Effect’ (LWE). I first quantify the LWE in simulation and then validate the technique on an experimental bench. I then estimate the LWE from on-sky data taken with the VLT/SPHERE adaptive optics system. Lastly, I apply my focal plane wavefront sensing techniques to estimate residual mirror co-phasing errors seen on Keck with the NIRC2 adaptive optics system data. I first demonstrate the ability of my techniques to quantify these errors in a simulation of Keck/NIRC2 data. I then apply their capabilities to estimate the mirror co-phasing errors of Keck with on-sky data.Graduate
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Damjanov, Ivana. "Structural Evolution of Quiescent Galaxies from the Peak of the Cosmic Star Formation Epoch." Thesis, 2011. http://hdl.handle.net/1807/31729.
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The main focus of this thesis is the investigation of an interesting new population of massive passively evolving galaxies found at high redshifts. We use a sample of these galaxies at redshifts 1
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Steinbring, Eric. "Techniques in high resolution observations from the ground and space, and imaging of the merging environments of radio galaxies at redshift 1 to 4." Thesis, 2000. https://dspace.library.uvic.ca//handle/1828/9861.
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High resolution imaging and spectroscopy are invaluable tools for extragalactic astronomy. Galaxies with redshifts of 1 or more subtend a very small angle on the sky—typically, only about an arcsecond. Unfortunately, this is also approximately the angular resolution achieved with a ground-based telescope regardless of its aperture. Atmospheric turbulence ruins the image before it reaches the telescope but the emerging technology of adaptive optics (AO) gives the observer the possibility, within limitations, of correcting for these effects. This is the case for instruments such as the Canada-France-Hawaii Telescope (CFHT) Adaptive Optics Bonnette (AOB) and the Gemini North Telescope (Gemini) Altitude-Conjugate Adaptive Optics for the Infrared (Altair) systems. The alternative is to rise above the limitations of the atmosphere entirely and put the telescope in space, for example, the Hubble Space Telescope (HST) and its successor, the Next-Generation Space Telescope (NGST).
I discuss several techniques that help overcome the limitations of AO observations with existing instruments in order to make them more comparable to imaging from space. For example, effective dithering and flat-fielding techniques as well as methods to determine the effect of the instrument on the image of, say, a galaxy. The implementation of these techniques as a software package called AOTOOLS is discussed. I also discuss computer simulations of AO systems, notably the Gemini Altair instrument, in order to understand and improve them. I apply my AO image processing techniques to observations of high-redshift radio galaxies (HzRGS) with the CFHT AOB and report on deep imaging in near-infrared (NIR) bands of 6 HzRGs in the redshift range 1.1 ≤ z ≤ 3.8. The NIR is probing the restframe visible light—mature stellar populations—at these redshifts. The radio galaxy is resolved in all of these observations and its ‘clumpier’ appearance at higher redshift leads to the main result—although the sample is very small—that these galaxy environments are undergoing mergers at high redshift. Finally, I look to the future of high resolution observations and discuss simulations of imaging and spectroscopy with the NGST. The computer software NGST VI/MOS is a ‘virtual reality’ simulator of the NGST observatory providing the user with the opportunity to test real observing campaigns.Graduate
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Ingraham, Patrick. "Détection et caractérisation de naines brunes et exoplanètes avec un filtre accordable pour applications dans l'espace." Thèse, 2013. http://hdl.handle.net/1866/9194.
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Cette thèse porte sur la capacité à détecter des compagnons de faible intensité en présence de bruit de tavelures dans le contexte de l’imagerie à haute gamme dynamique pour l’astronomie spatiale. On s’intéressera plus particulièrement à l’imagerie spectrale différentielle (ISD) obtenue en utilisant un étalon Fabry-Pérot comme filtre accordable. Les performances d’un tel filtre accordable sont présentées dans le cadre du Tunable Filter Imager (TFI), instrument conçu pour le télescope spatial James Webb (JWST).
La capacité de l’étalon à supprimer les tavelures avec ISD est démontrée expérimentalement grâce à un prototype de l’étalon installé sur un banc de laboratoire. Les améliorations de contraste varient en fonction de la séparation, s’étendant d’un facteur 10 pour les séparations supérieures à 11 lambda/D jusqu’à un facteur 60 à 5 lambda/D. Ces résultats sont cohérents avec une étude théorique qui utilise un modèle basé sur la propagation de Fresnel pour montrer que les performances de suppression de tavelures sont limitées par le banc optique et non pas par l’étalon. De plus, il est démontré qu’un filtre accordable est une option séduisante pour l’imagerie à haute gamme dynamique combinée à la technique ISD. Une seconde étude basée sur la propagation de Fresnel de l’instrument TFI et du télescope, a permis de définir les performances de la technique ISD combinée avec un étalon pour l’astronomie spatiale. Les résultats prévoient une amélioration de contraste de l’ordre de 7 jusqu’à 100, selon la configuration de l’instrument. Une comparaison entre ISD et la soustraction par rotation a également été simulée. Enfin, la dernière partie de ce chapitre porte sur les performances de la technique ISD dans le cadre de l’instrument Near-Infrared Imager and Slitless Spectrograph (NIRISS), conçu pour remplacer TFI comme module scientifique à bord du Fine Guidance Sensor du JWST.
Cent quatre objets localisés vers la région centrale de la nébuleuse d’Orion ont été caractérisés grâce à un spectrographe multi-objet, de basse résolution et multi-bande (0.85-2.4 um). Cette étude a relevé 7 nouvelles naines brunes et 4 nouveaux candidats de masse planétaire. Ces objets sont utiles pour déterminer la fonction de masse initiale sous-stellaire et pour évaluer les modèles atmosphériques et évolutifs futurs des jeunes objets stellaires et sous-stellaires. Combinant les magnitudes en bande H mesurées et les valeurs d’extinction, les objets classifiés sont utilisés pour créer un diagramme de Hertzsprung-Russell de cet amas stellaire. En accord avec des études antérieures, nos résultats montrent qu’il existe une seule époque de formation d’étoiles qui a débuté il y a environ 1 million d’années. La fonction de masse initiale qui en dérive est en accord avec des études antérieures portant sur d’autres amas jeunes et sur le disque galactique.This thesis determines the capability of detecting faint companions in the presence of speckle noise when performing space-based high-contrast imaging through spectral differential imagery (SDI) using a low-order Fabry-Perot etalon as a tunable filter. The performance of such a tunable filter is illustrated through the Tunable Filter Imager (TFI), an instrument designed for the James Webb Space Telescope (JWST). Using a TFI prototype etalon and a custom designed test bed, the etalon’s ability to perform speckle-suppression through SDI is demonstrated experimentally. Improvements in contrast vary with separation, ranging from a factor of 10 at working angles greater than 11 lambda/D and increasing up to a factor of 60 at 5 lambda/D. These measurements are consistent with a Fresnel optical propagation model which shows the speckle suppression capability is limited by the test bed and not the etalon. This result demonstrates that a tunable filter is an attractive option to perform high-contrast imaging through SDI. To explore the capability of space-based SDI using an etalon, we perform an end-to-end Fresnel propagation of JWST and TFI. Using this simulation, a contrast improvement ranging from a factor of 7 to 100 is predicted, depending on the instrument’s configuration. The performance of roll-subtraction is simulated and compared to that of SDI. The SDI capability of the Near-Infrared Imager and Slitless Spectrograph (NIRISS), the science instrument module to replace TFI in the JWST Fine Guidance Sensor is also determined. Using low resolution, multi-band (0.85-2.4 um) multi-object spectroscopy, 104 objects towards the central region of the Orion Nebular Cluster have been assigned spectral types including 7 new brown dwarfs, and 4 new planetary mass candidates. These objects are useful for determining the substellar initial mass function and for testing evolutionary and atmospheric models of young stellar and substellar objects. Using the measured H band magnitudes, combined with our determined extinction values, the classified objects are used to create an Hertzsprung-Russell diagram for the cluster. Our results indicate a single epoch of star formation beginning 1 Myr ago. The initial mass function of the cluster is derived and found to be consistent with the values determined for other young clusters and the galactic disk.
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Della, Ceca Lara Sofía. "Análisis espacio-temporal de la distribución de aerosoles atmosféricos en la ciudad de Córdoba (Argentina) y desarrollo de un modelo predictivo de los niveles de material particulado." Master's thesis, 2018. http://hdl.handle.net/11086/6009.
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Tesis (Magister en Aplicaciones Espaciales de Alerta y Respuesta Temprana a Emergencias)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía, Física y Computación, 2018.Maestría conjunta con el Instituto de Altos Estudios Espaciales "Mario Gulich"-CONAE.
En esta tesis se estudia la variabilidad espacio-temporal de los aerosoles atmosféricos en la ciudad de Córdoba (Argentina) y sus alrededores para un período mayor a 10 años (2003-2013), mediante el uso del producto satelital espesor óptico de aerosoles (o AOD por Aerosol Optical Depth, en inglés) de frecuencia diaria obtenido con el algoritmo denominado implementación de corrección atmosférica multi-ángulo (MAIAC) que ha sido recientemente desarrollado para los datos obtenidos con el sensor MODIS (a bordo de los satélites Terra y Aqua/NASA). Hasta el momento; los productos de AOD disponibles presentaban resoluciones espaciales mayores a 3 km, adecuados para estudios a escala regional. Sin embargo no proveían suficiente detalle para el estudio de áreas urbanas o para estudios epidemiológicos. Con este objetivo se desarrolló este nuevo algoritmo, aún en fase de prueba, que mejora sensiblemente la resolución espacial a 1 km, con lo cual resulta más apropiado para el estudio de los aerosoles atmosféricos a escala urbana. En este trabajo, en una primera instancia se evaluó la performance del producto AOD-MAIAC mediante la comparación con valores de AOD obtenidos desde superficie en la estación Córdoba-CETT de la red AERONET. Se analizó la concentración y variación anual de los aerosoles, así como su variación mensual y estacional. Por último, se estudió la relación entre los valores satelitales de AOD-MAIAC y valores de material particulado (PM) obtenidos desde la superficie por una estación de monitoreo de la Municipalidad de Córdoba que funcionó en el centro de la ciudad durante enero-agosto de 2009. En general, el algoritmo MAIAC presentó una buena performance en el área de estudio. Los resultados reflejaron que, a pesar de que los valores de AOD son bajos respecto a otros sitios del mundo muy contaminados, existe una tendencia de incremento de AOD a lo largo del tiempo particularmente en algunas zonas de la ciudad (como por ejemplo el acceso a Sierras Chicas y la zona norte de la ciudad) que podría estar vinculado al aumento de la densidad poblacional en esa área y el consecuente incremento del tránsito vehicular. Además se observó un patrón de incremento o disminución en los niveles de AOD en determinados momentos del año. Durante los meses de verano (diciembre-febrero) se observaron valores relativamente altos concentrados en la ciudad de Córdoba, en las principales vías de acceso hacia las zonas turísticas así como en el anillo de circunvalación de la ciudad Hacia el otoño los valores de AOD comienzan a disminuir hasta alcanzar los valores más bajos durante los meses de invierno. A partir de agosto se observa un gran incremento del AOD que tiene su pico máximo durante septiembre y se mantiene elevado durante el resto de la primavera. Este incremento de AOD coincide con 2la estación de quema de biomasa en la provincia de Córdoba, el norte argentino y otras regiones de Sudamérica (Bolivia, Paraguay, Amazonia y Cerrado en Brasil) y evidencia la importancia del transporte atmosférico a escala regional pero también continental de material particulado que es liberado a la atmósfera durante los incendios. Los modelos de regresión lineal desarrollados en este estudio para evaluar la relación entre AOD-PM y variables meteorológicas no son suficientes para explicar la variabilidad de los datos de PM medidos en superficie a partir de los valores satelitales de AOD y las variables meteorológicas. Sin embargo, los resultados presentados constituyen un primer estudio exploratorio para la ciudad de Córdoba. Dada la falta de estaciones superficiales de monitoreo de material particulado en Argentina, y en particular en la ciudad de Córdoba, este estudio intentó ser una línea de base para el estudio de la dinámica de los aerosoles atmosféricos a escala urbana a partir de información satelital y constituye una primera aproximación a la problemática.
Fil: Della Ceca, Lara Sofía. Universidad Nacional de Córdoba. Facultad de Matemática, Astronomía, Física y Computación; Argentina.
Fil: Della Ceca, Lara Sofía. Universidad Nacional de Córdoba. Instituto de Altos Estudios Espaciales Mario Gulich; Argentina.
Books on the topic "Instrumentation, Techniques, and Astronomical Observations"
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Observational astronomy: Techniques and instrumentation. Cambridge: Cambridge University Press, 2011.
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(Society), SPIE, ed. Solar physics and space weather instrumentation III: 4-6 August 2009, San Diego, California, United States. Bellingham, Wash: SPIE, 2009.
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(Society), SPIE, ed. Solar physics and space weather instrumentation II: 26-27 August 2007, San Diego, California, USA. Bellingham, Wash: SPIE, 2007.
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Society, American Astronomical, and SPIE (Society), eds. Modern technologies in space- and ground-based telescopes and instrumentation: 27 June-2 July 2010, San Diego, California, United States. Bellingham, Wash: SPIE, 2010.
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service), SpringerLink (Online, ed. Ancient Astronomical Observations and the Study of the Moon’s Motion (1691-1757). Boston, MA: Springer US, 2012.
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Topical Meeting on Laser and Optical Remote Sensing (1987 North Falmouth, Mass.). Topical Meeting on Laser and Optical Remote Sensing: Instrumentation and techniques technical digest : summaries of papers presented at the Laser and Optical Remote Sensing : instrumentation and techniques Topical Meeting, September 28-October 1, 1987, North Falmo[u]th, Massachusetts. Washington, D.C: Optical Society of America, 1987.
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service), SpringerLink (Online, ed. One-Shot Color Astronomical Imaging: In Less Time, For Less Money! Boston, MA: Springer US, 2012.
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service), SpringerLink (Online, ed. Grating Spectroscopes and How to Use Them. Boston, MA: Springer US, 2012.
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Soffel, Michael. Space-Time Reference Systems. Berlin, Heidelberg: Springer Berlin Heidelberg, 2013.
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Sherrod, P. Clay, and Thomas L. Koed. Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations. Dover Publications, Incorporated, 2012.
Find full textBook chapters on the topic "Instrumentation, Techniques, and Astronomical Observations"
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Heidt, Jochen. "Hardware for Near-Infrared Observations—Adaptive Optics, Instrumentation, and Detectors." In Astronomy in the Near-Infrared - Observing Strategies and Data Reduction Techniques, 61–129. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-030-98441-0_4.
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Moon, Dae-Sik. "Calibration Techniques." In The WSPC Handbook of Astronomical Instrumentation, 227–44. WORLD SCIENTIFIC, 2021. http://dx.doi.org/10.1142/9789811203787_0012.
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Clarke, Fraser, and Matthias Tecza. "Integral Field Techniques." In The WSPC Handbook of Astronomical Instrumentation, 257–83. WORLD SCIENTIFIC, 2021. http://dx.doi.org/10.1142/9789811203794_0014.
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Beckers, J. M. "Techniques for High Angular Resolution Astronomical Imaging." In Instrumentation for Large Telescopes, 1–34. Cambridge University Press, 1997. http://dx.doi.org/10.1017/cbo9780511564932.002.
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Hopmans, Jan W., and Jan M. H. Hendrickx. "Emerging Measurement Techniques for Vadose Zone Characterization." In Vadose Zone Hydrology. Oxford University Press, 1999. http://dx.doi.org/10.1093/oso/9780195109900.003.0015.
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Variables and parameters required to characterize soil water flow and solute transport are often measured at different spatial scales from those for which they are needed. This poses a problem since results from field and laboratory measurements at one spatial scale are not necessarily valid for application at another. Herein lies a challenge that vadose zone hydrologists are faced with. For example, vadose zone studies can include flow at the groundwater-unsaturated zone as well as at the soil surface-atmosphere interface at either one specific location or representing an entire field or landscape unit. Therefore, vadose zone measurements should include techniques that can monitor at large depths and that characterize landsurface processes. On the other end of the space spectrum, microscopic laboratory measurement techniques are needed to better understand fundamental flow and transport mechanisms through observations of pore-scale geometry and fluid flow. The Vadose Zone Hydrology (VZH) Conference made very clear that there is an immediate need for such microscopic information at fluid-fluid and solid-fluid interfaces, as well as for methodologies that yield information at the field/landscape scale. The need for improved instrumentation was discussed at the ASA-sponsored symposium on “Future Directions in Soil Physics” by Hendrickx (1994) and Hopmans (1994). Soil physicists participating in the 1994-1999 Western Regional Research Project W-188 (1994) focused on “improved characterization and quantification of flow and transport processes in soils,” and prioritized the need for development and evaluation of new instrumentation and methods of data anlysis to further improve characterization of water and solute transport. The regional project documents the critical need for quantification of water flow and solute transport in heterogeneous, spatially variable field soils, specifically to address preferential and accelerated contaminant transport. Cassel and Nielsen (1994) describe the contributions in computed tomography (CT) using x-rays or magnetic resonance imaging (MRI) as “an awakening,” and they envision these methodologies to become an integral part of vadose zone research programs. The difference in size between measurement and application scales poses a dilemma for the vadose zone hydrologist.
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Kallio, Ulla, Thomas Klügel, Simo Marila, Swetlana Mähler, Markku Poutanen, Timo Saari, Torben Schüler, and Heli Suurmäki. "Datum Problem Handling in Local Tie Surveys at Wettzell and Metsähovi." In International Association of Geodesy Symposia. Berlin, Heidelberg: Springer Berlin Heidelberg, 2022. http://dx.doi.org/10.1007/1345_2022_155.
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AbstractThe datum problem is a fundamental issue in the network adjustment when connecting a local measurement network to an external reference frame. Datum elements in 3D networks are scale, translation, and orientation. We consider here the local tie network at geodetic core stations, where the external reference frame is the latest ITRF realization, ITRF2014, in the mean epoch of terrestrial observations.Accurate distance measurements are used for the determination of the network scale. Thus the improvement of its accuracy and the inclusion of weather measurements to account for refraction errors are essential. For rotation and translation of the network, we need external information. Angle observations are related to the coordinate system of the instrument (e.g. a tachymeter) which is usually aligned to the plumb line. Instruments have different vertical orientation at every station point and the direction of the plumb line does not coincide with the normal vector of the reference ellipsoid. Horizontally the observed set of angles are oriented in arbitrary or approximately oriented directions.External information which is needed for solving the absolute orientation are datum points, providing the link to the global coordinate system, and correction terms for the vertical orientation (deflection of the vertical), which can be derived from combined terrestrial/GNSS observations, from a gravity based geoid model, or from astronomical observations.In this article, we present the solutions/options for the datum problem in the framework of the EMPIR GeoMetre project using the example of the ITRF core stations Metsähovi and Wettzell using transformation-free approaches. The inclusion of distant targets is promising, since in small networks even a millimeter change in the coordinates of a datum point can significantly affect a local tie vector. It is shown that at both stations the determination of the deflection of the vertical using different techniques yield the same results within the measurement error.
Conference papers on the topic "Instrumentation, Techniques, and Astronomical Observations"
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Maire, Jerome, Aziz Ziad, Julien Borgnino, Francois Martin, and Denis Mourard. "Optimization of the observations of the high angular resolution techniques (adaptive optics and interferometry)." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2004. http://dx.doi.org/10.1117/12.562957.
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Demangeon, Olivier, Peter A. Schuller, Alain Léger, and Philippe Duret. "Toward the stability required for direct observations of exoplanets with nulling interferometry technique." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2010. http://dx.doi.org/10.1117/12.857209.
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Cramer, Claire E., Steven W. Brown, Keith R. Lykke, John T. Woodward, Stephen Bailey, David J. Schlegel, Adam S. Bolton, et al. "Tunable laser techniques for improving the precision of observational astronomy." In SPIE Astronomical Telescopes + Instrumentation, edited by Ramón Navarro, Colin R. Cunningham, and Eric Prieto. SPIE, 2012. http://dx.doi.org/10.1117/12.925198.
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Millar-Blanchaer, Maxwell A., Marshall D. Perrin, Li-Wei Hung, Michael P. Fitzgerald, Jason J. Wang, Jeffrey Chilcote, James R. Graham, Sebastian Bruzzone, and Paul G. Kalas. "GPI observational calibrations XIV: polarimetric contrasts and new data reduction techniques." In SPIE Astronomical Telescopes + Instrumentation, edited by Christopher J. Evans, Luc Simard, and Hideki Takami. SPIE, 2016. http://dx.doi.org/10.1117/12.2233071.
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Haig, Douglas J., Peter A. R. Ade, James E. Aguirre, James J. Bock, Samantha F. Edgington, Melissa L. Enoch, Jason Glenn, et al. "Bolocam: status and observations." In SPIE Astronomical Telescopes + Instrumentation, edited by Jonas Zmuidzinas, Wayne S. Holland, and Stafford Withington. SPIE, 2004. http://dx.doi.org/10.1117/12.553154.
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Stecklum, Bringfried, Thomas Henning, Markus Feldt, P. Hofner, M. G. Hoare, and Thomas L. Hayward. "Adaptive optics observations of young massive stars." In Astronomical Telescopes & Instrumentation, edited by Domenico Bonaccini and Robert K. Tyson. SPIE, 1998. http://dx.doi.org/10.1117/12.321737.
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Klvaňa, Miroslav, Michal Sobotka, and Michal Švanda. "Optimisation of solar synoptic observations." In SPIE Astronomical Telescopes + Instrumentation, edited by Alison B. Peck, Robert L. Seaman, and Fernando Comeron. SPIE, 2012. http://dx.doi.org/10.1117/12.925317.
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Goodwin, Michael, Charles Jenkins, Peter Conroy, and Andrew Lambert. "Observations of ground-layer turbulence." In SPIE Astronomical Telescopes + Instrumentation, edited by Norbert Hubin, Claire E. Max, and Peter L. Wizinowich. SPIE, 2008. http://dx.doi.org/10.1117/12.787732.
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Keller, Christoph U. "SOLIS: a modern facility for synoptic solar observations." In Astronomical Telescopes & Instrumentation, edited by Larry M. Stepp. SPIE, 1998. http://dx.doi.org/10.1117/12.319288.
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Hochedez, Jean-Francois E., Udo H. Schuehle, Jose L. Pau, Jose Alvarez, Olivier Hainaut, Thierry P. Appourchaux, F. D. Auret, et al. "New UV detectors for solar observations." In Astronomical Telescopes and Instrumentation, edited by Stephen L. Keil and Sergey V. Avakyan. SPIE, 2003. http://dx.doi.org/10.1117/12.460367.
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