Bibliografías temáticas / Techniques: photometric

Literatura académica sobre el tema "Techniques: photometric"

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Publicado: 4 de junio de 2021
Última modificación: 7 de febrero de 2022

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Artículos de revistas sobre el tema "Techniques: photometric"

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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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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 (agosto de 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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Davies, L. J. M., J. E. Thorne, A. S. G. Robotham, S. Bellstedt, S. P. Driver, N. J. Adams, M. Bilicki et al. "Deep Extragalactic VIsible Legacy Survey (DEVILS): consistent multiwavelength photometry for the DEVILS regions (COSMOS, XMMLSS, and ECDFS)". Monthly Notices of the Royal Astronomical Society 506, n.º 1 (5 de junio de 2021): 256–87. http://dx.doi.org/10.1093/mnras/stab1601.

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ABSTRACT The Deep Extragalactic VIsible Legacy Survey (DEVILS) is an ongoing high-completeness, deep spectroscopic survey of ∼60 000 galaxies to Y < 21.2 mag, over ∼6 deg2 in three well-studied deep extragalactic fields: D10 (COSMOS), D02 (XMMLSS), and D03 (ECDFS). Numerous DEVILS projects all require consistent, uniformly derived and state-of-the-art photometric data with which to measure galaxy properties. Existing photometric catalogues in these regions either use varied photometric measurement techniques for different facilities/wavelengths leading to inconsistencies, older imaging data and/or rely on source detection and photometry techniques with known problems. Here, we use the ProFound image analysis package and state-of-the-art imaging data sets (including Subaru-HSC, VST-VOICE, VISTA-VIDEO, and UltraVISTA-DR4) to derive matched-source photometry in 22 bands from the FUV to 500 $\mu$m. This photometry is found to be consistent, or better, in colour analysis to previous approaches using fixed-size apertures (which are specifically tuned to derive colours), but produces superior total source photometry, essential for the derivation of stellar masses, star formation rates, star formation histories, etc. Our photometric catalogue is described in detail and, after internal DEVILS team projects, will be publicly released for use by the broader scientific community.
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Cabayol-Garcia, L., M. Eriksen, A. Alarcón, A. Amara, J. Carretero, R. Casas, F. J. Castander et al. "The PAU Survey: background light estimation with deep learning techniques". Monthly Notices of the Royal Astronomical Society 491, n.º 4 (23 de noviembre de 2019): 5392–405. http://dx.doi.org/10.1093/mnras/stz3274.

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ABSTRACT In any imaging survey, measuring accurately the astronomical background light is crucial to obtain good photometry. This paper introduces BKGnet, a deep neural network to predict the background and its associated error. BKGnet has been developed for data from the Physics of the Accelerating Universe Survey (PAUS), an imaging survey using a 40 narrow-band filter camera (PAUCam). The images obtained with PAUCam are affected by scattered light: an optical effect consisting of light multiply reflected that deposits energy in specific detector regions affecting the science measurements. Fortunately, scattered light is not a random effect, but it can be predicted and corrected for. We have found that BKGnet background predictions are very robust to distorting effects, while still being statistically accurate. On average, the use of BKGnet improves the photometric flux measurements by $7{{\ \rm per\ cent}}$ and up to $20{{\ \rm per\ cent}}$ at the bright end. BKGnet also removes a systematic trend in the background error estimation with magnitude in the i band that is present with the current PAU data management method. With BKGnet, we reduce the photometric redshift outlier rate by $35{{\ \rm per\ cent}}$ for the best $20{{\ \rm per\ cent}}$ galaxies selected with a photometric quality parameter.
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Ackermann, Jens y Michael Goesele. "A Survey of Photometric Stereo Techniques". Foundations and Trends® in Computer Graphics and Vision 9, n.º 3-4 (2015): 149–254. http://dx.doi.org/10.1561/0600000065.

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Zhang, Yan-Xia y Yong-Heng Zhao. "Photometric Redshift Techniques in Big-data Era". Proceedings of the International Astronomical Union 11, S319 (agosto de 2015): 57. http://dx.doi.org/10.1017/s1743921315009886.

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AbstractPhotometric data increase with large survey projects running. The huge volume of data influences the means and methods to deal with them. As such, the techniques of photometric redshift estimation based on photometric data must be developed and improved.
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Lee, Bomee y Ranga-Ram Chary. "Improved photometric redshifts with colour-constrained galaxy templates for future wide-area surveys". Monthly Notices of the Royal Astronomical Society 497, n.º 2 (17 de julio de 2020): 1935–45. http://dx.doi.org/10.1093/mnras/staa2100.

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ABSTRACT Cosmology and galaxy evolution studies with LSST, Euclid, and Roman, will require accurate redshifts for the detected galaxies. In this study, we present improved photometric redshift estimates for galaxies using a template library that populates three-colour space and is constrained by HST/CANDELS photometry. For the training sample, we use a sample of galaxies having photometric redshifts that allows us to train on a large, unbiased galaxy sample having deep, unconfused photometry at optical-to-mid infrared wavelengths. Galaxies in the training sample are assigned to cubes in 3D colour space, V − H, I − J, and z − H. We then derive the best-fitting spectral energy distributions of the training sample at the fixed CANDELS median photometric redshifts to construct the new template library for each individual colour cube (i.e. colour-cube-based template library). We derive photometric redshifts (photo-z) of our target galaxies using our new colour-cube-based template library and with photometry in only a limited set of bands, as expected for the aforementioned surveys. As a result, our method yields σNMAD of 0.026 and an outlier fraction of 6 per cent using only photometry in the LSST and Euclid/Roman bands. This is an improvement of ∼10 per cent on σNMAD and a reduction in outlier fraction of ∼13 per cent compared to other techniques. In particular, we improve the photo-z precision by about 30 per cent at 2 < z < 3. We also assess photo-z improvements by including K or mid-infrared bands to the ugrizYJH photometry. Our colour-cube-based template library is a powerful tool to constrain photometric redshifts for future large surveys.
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8

Barry, D. J., W. G. Bagnuolo, B. D. Mason, H. A. McAlister y N. H. Turner. "Prospects for Rapid, Routine Speckle Photometry". International Astronomical Union Colloquium 135 (1992): 537–39. http://dx.doi.org/10.1017/s0252921100007077.

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Image reconstruction techniques have rapidly matured over the last decade, and increasing reference to full–aperture and masked aperture results appear in the literature. Although anomalies in morphology are understood, most work uses nonlinear iterative refinements of questionable photometric robustness. Recent development of linear least–squares phase reconstruction techniques from the bispectrum (Glindemann et al. 1991) offers hope for a robust technique using a computational tour de force. However, the field cannot be considered mature until routine photometry of a large number of speckle–resolved objects is performed and demonstrated to be repeatable. We review our work and our expectations for use of both computationally intensive and simple techniques in our routine speckle reductions.
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Newling, J., M. Varughese, B. Bassett, H. Campbell, R. Hlozek, M. Kunz, H. Lampeitl et al. "Statistical classification techniques for photometric supernova typing". Monthly Notices of the Royal Astronomical Society 414, n.º 3 (15 de abril de 2011): 1987–2004. http://dx.doi.org/10.1111/j.1365-2966.2011.18514.x.

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Subbarao, M. U., A. J. Connolly, A. S. Szalay y D. C. Koo. "Luminosity Functions From Photometric Redshifts. I. Techniques". Astronomical Journal 112 (septiembre de 1996): 929. http://dx.doi.org/10.1086/118066.

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Tesis sobre el tema "Techniques: photometric"

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Domeniconi, Federico. "Deep Learning Techniques applied to Photometric Stereo". Master's thesis, Alma Mater Studiorum - Università di Bologna, 2020. http://amslaurea.unibo.it/20031/.

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La tesi si focalizza sullo studio dello stato dell’arte della fotometria stereo con deep learning: Self-calibrating Deep Photometric Stereo Networks. Il modello è composto è composto di due reti, la prima predice la direzione e l’intensità delle luci, la seconda predice le normali della superficie. L’obiettivo della tesi è individuare i limiti del modello e capire se possa essere modifcato per avere buone prestazioni anche in scenari reali. Il progetto di tesi è basato su fine-tuning, una tecnica supervisionata di transfer learning. Per questo scopo un nuovo dataset è stato creato acquisendo immagini in laboratorio. La ground-truth è ottenuta tramite una tecnica di distillazione. In particolare la direzione delle luci è ottenuta utilizzando due algoritmi di calibrazione delle luci e unendo i due risultati. Analogamente le normali delle superfici sono ottenute unendo i risultati di vari algoritmi di fotometria stereo. I risultati della tesi sono molto promettenti. L’errore nella predizione della direzione e dell’intensità delle luci è un terzo dell’errore del modello originale. Le predizioni delle normali delle superfici possono essere analizzate solo qualitativamente, ma i miglioramenti sono evidenti. Il lavoro di questa tesi ha mostrato che è possibile applicare transfer-learning alla fotometria stereo con deep learning. Perciò non è necessario allenare un nuovo modello da zero ma è possibile approfittare di modelli già esistenti per migliorare le prestazioni e ridurre il tempo di allenamento.
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Bezanson, Rachel, David A. Wake, Gabriel B. Brammer, Pieter G. van Dokkum, Marijn Franx, Ivo Labbé, Joel Leja et al. "LEVERAGING 3D-HST GRISM REDSHIFTS TO QUANTIFY PHOTOMETRIC REDSHIFT PERFORMANCE". IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621218.

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We present a study of photometric redshift accuracy in the 3D-HST photometric catalogs, using 3D-HST grism redshifts to quantify and dissect trends in redshift accuracy for galaxies brighter than JH(IR) > 24 with an unprecedented and representative high-redshift galaxy sample. We find an average scatter of 0.0197 +/- 0.0003(1 + z) in the Skelton et al. photometric redshifts. Photometric redshift accuracy decreases with magnitude and redshift, but does not vary monotonically with color or stellar mass. The 1 sigma scatter lies between 0.01 and 0.03 (1 + z) for galaxies of all masses and colors below z. <. 2.5 (for JH(IR) < 24), with the exception of a population of very red (U - V > 2), dusty star-forming galaxies for which the scatter increases to similar to 0.1 (1+ z). We find that photometric redshifts depend significantly on galaxy size; the largest galaxies at fixed magnitude have photo-zs with up to similar to 30% more scatter and similar to 5 times the outlier rate. Although the overall photometric redshift accuracy for quiescent galaxies is better than that for star-forming galaxies, scatter depends more strongly on magnitude and redshift than on galaxy type. We verify these trends using the redshift distributions of close pairs and extend the analysis to fainter objects, where photometric redshift errors further increase to similar to 0.046 (1 + z) at H-F160W = 26. We demonstrate that photometric redshift accuracy is strongly filter dependent and quantify the contribution of multiple filter combinations. We evaluate the widths of redshift probability distribution functions and find that error estimates are underestimated by a factor of similar to 1.1 - 1.6, but that uniformly broadening the distribution does not adequately account for fitting outliers. Finally, we suggest possible applications of these data in planning for current and future surveys and simulate photometric redshift performance in the Large Synoptic Survey Telescope, Dark Energy Survey (DES), and combined DES and Vista Hemisphere surveys.
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Zou, Hu, Tianmeng Zhang, Zhimin Zhou, Jundan Nie, Xiyan Peng, Xu Zhou, Linhua Jiang et al. "The First Data Release of the Beijing-Arizona Sky Survey". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624694.

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The Beijing-Arizona Sky Survey (BASS) is a new wide-field legacy imaging survey in the northern Galactic cap using the 2.3 m Bok telescope. The survey will cover about 5400 deg(2) in the g and r bands, and the expected 5 sigma depths (corrected for the Galactic extinction) in these two bands are g = 24.0 and r = 23.4 mag (AB magnitude). BASS started observations in 2015 January. and had. completed about 41% of the. area as of 2016 July. The first data release contains calibrated images obtained in 2015 and 2016 and their corresponding single-epoch. and coadded catalogs. The actual depths of the. single-epoch images are g similar to 23.4 and r similar to 22.9 mag. The full depths of the. three epochs are g similar to 24.1 and r similar to 23.5 mag.
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Stritzinger, Maximilian. "Type Ia supernovae bolometric properties and new tools for photometric techniques /". [S.l.] : [s.n.], 2005. http://deposit.ddb.de/cgi-bin/dokserv?idn=979066697.

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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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Cartwright, Stephen J. "Application of digital image processing techniques to the photometric testing of vehicle headlamps". Thesis, Aston University, 1986. http://publications.aston.ac.uk/14614/.

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The aim of this Interdisciplinary Higher Degrees project was the development of a high-speed method of photometrically testing vehicle headlamps, based on the use of image processing techniques, for Lucas Electrical Limited. Photometric testing involves measuring the illuminance produced by a lamp at certain points in its beam distribution. Headlamp performance is best represented by an iso-lux diagram, showing illuminance contours, produced from a two-dimensional array of data. Conventionally, the tens of thousands of measurements required are made using a single stationary photodetector and a two-dimensional mechanical scanning system which enables a lamp's horizontal and vertical orientation relative to the photodetector to be changed. Even using motorised scanning and computerised data-logging, the data acquisition time for a typical iso-lux test is about twenty minutes. A detailed study was made of the concept of using a video camera and a digital image processing system to scan and measure a lamp's beam without the need for the time-consuming mechanical movement. Although the concept was shown to be theoretically feasible, and a prototype system designed, it could not be implemented because of the technical limitations of commercially-available equipment. An alternative high-speed approach was developed, however, and a second prototype syqtem designed. The proposed arrangement again uses an image processing system, but in conjunction with a one-dimensional array of photodetectors and a one-dimensional mechanical scanning system in place of a video camera. This system can be implemented using commercially-available equipment and, although not entirely eliminating the need for mechanical movement, greatly reduces the amount required, resulting in a predicted data acquisiton time of about twenty seconds for a typical iso-lux test. As a consequence of the work undertaken, the company initiated an 80,000 programme to implement the system proposed by the author.
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Toyozumi, Hiroyuki Physics Faculty of Science UNSW. "The intra-pixel sensitivity variation of a CCD". Awarded by:University of New South Wales. School of Physics, 2005. http://handle.unsw.edu.au/1959.4/25995.

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The effect of Intra-pixel sensitivity variation (IPSV) in charge-coupled devices (CCDs) can be important in astronomical applications. This thesis studies the IPSV in a front-illuminated three-phase EEV05-20 CCD used in the Automated Patrol Telescope (APT), from multiple points of view. To explore the detailed sensitivity variation within pixels, the CCD was scanned using a 4 \mu meter diameter light beam in four colour bands: B, V, R and I. The resulting images clearly show the IPSVs due to the CCD electrode structure, and its dependence on wavelength. Unexpected ghost images appear in the scan images that are most likely due to the charge transfer inefficiency (CTI) of the CCD. A correction procedure for the CTI effect is presented. Using the pixel response function (PRF) which was derived from the CCD scans, instrumental point spread functions (iPSFs) were calculated from dithered images observed by the APT. The accurate iPSFs allowed us to generate a variety of simulated images of APT observations, enabling us to analyse in detail the effect of IPSV on astronomical observations. One of the astronomical impacts of IPSV is on photometry. The IPSV effect on the precision for estimating star fluxes was studied using both observed and simulated images. The IPSV effect can be expressed as magnitude estimation error maps plotted against the fractional part of a star's coordinates. The IPSV effect introduces \pm 4% errors in star fluxes for observed images with the APT in V band. Another astronomical impact of IPSV is on astrometry. IPSV influences the precision for estimating star coordinates, and this was studied using a number of simulated images. The IPSV effect can be expressed as coordinate estimation error maps plotted against the fractional part of a star's coordinates. The IPSV effect introduces \sim 0.02 pixel errors in RMS for images observed with the APT in V band. The appearance of the unexpected ghost images in the CCD scans suggested that CTI might also affect observed images. We examined the effects on PSFs and photometry. The CTI effect does affect the shapes of PSFs, but only to a small fraction. Its effect on photometry is negligible.
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Li, Linlin, Shiyin Shen, Jinliang Hou, Fangting Yuan, Jing Zhong, Hu Zou, Xu Zhou et al. "GALACTIC EXTINCTION AND REDDENING FROM THE SOUTH GALACTIC CAP u -BAND SKY SURVEY: u -BAND GALAXY NUMBER COUNTS AND u − r COLOR DISTRIBUTION". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623264.

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We study the integral Galactic extinction and reddening based on the galaxy catalog of the South Galactic Cap u-band Sky Survey (SCUSS), where u-band galaxy number counts and u - r color distribution are used to derive the Galactic extinction and reddening respectively. We compare these independent statistical measurements with the reddening map of Schlegel et al. (SFD) and find that both the extinction and reddening from the number counts and color distribution are in good agreement with the SFD results at low extinction regions (E(B - V)(SFD) < 0.12 mag). However, for high extinction regions (E(B - V)(SFD) > 0.12 mag), the SFD map overestimates the Galactic reddening systematically, which can be approximated by a linear relation Delta E(B - V)= 0.43[ E(B - V)(SFD) - 0.12]. By combining the results from galaxy number counts and color distribution, we find that the shape of the Galactic extinction curve is in good agreement with the standard R-V = 3.1 extinction law of O'Donnell.
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Christiansen, Jessie L., Andrew Vanderburg, Jennifer Burt, B. J. Fulton, Konstantin Batygin, Björn Benneke, John M. Brewer et al. "Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625817.

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HD 3167 is a bright (V = 8.9), nearby KO star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 +/- 0.38 M-circle plus for HD 3167 b, a hot super-Earth with a likely rocky composition (rho(b) = 5.6(-1.43)(+2.15) g cm(-3)), and 9.80(-1.24)(+1.30) M-circle plus for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (rho(c) = 1.97(-0.59)(+0.94) g cm(-3)). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 +/- 0.045 d (between planets b and c) and a minimum mass of 6.90 +/- 0.71 M-circle plus. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.degrees 3 because we do not observe transits of planet d. From 1.degrees 3 to 40 degrees, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time.
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Stefansson, Gudmundur, Suvrath Mahadevan, Leslie Hebb, John Wisniewski, Joseph Huehnerhoff, Brett Morris, Sam Halverson et al. "Toward Space-like Photometric Precision from the Ground with Beam-shaping Diffusers". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626043.

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We demonstrate a path to hitherto unachievable differential photometric precisions from the ground, both in the optical and near-infrared (NIR), using custom-fabricated beam-shaping diffusers produced using specialized nanofabrication techniques. Such diffusers mold the focal plane image of a star into a broad and stable top-hat shape, minimizing photometric errors due to non-uniform pixel response, atmospheric seeing effects, imperfect guiding, and telescope-induced variable aberrations seen in defocusing. This PSF reshaping significantly increases the achievable dynamic range of our observations, increasing our observing efficiency and thus better averages over scintillation. Diffusers work in both collimated and converging beams. We present diffuser-assisted optical observations demonstrating 62(-16)(+26) ppm precision in 30 minute bins on a nearby bright star 16 Cygni A (V = 5.95) using the ARC 3.5 m telescope-within a factor of similar to 2 of Kepler's photometric precision on the same star. We also show a transit of WASP-85-Ab (V = 11.2) and TRES-3b (V = 12.4), where the residuals bin down to 180(-41)(+66) ppm in 30 minute bins for WASP-85-Ab-a factor of similar to 4 of the precision achieved by the K2 mission on this target-and to 101 ppm for TRES-3b. In the NIR, where diffusers may provide even more significant improvements over the current state of the art, our preliminary tests demonstrated 137(-36)(+64) ppm precision for a K-S = 10.8 star on the 200 inch. Hale Telescope. These photometric precisions match or surpass the expected photometric precisions of TESS for the same magnitude range. This technology is inexpensive, scalable, easily adaptable, and can have an important and immediate impact on the observations of transits and secondary eclipses of exoplanets.
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Libros sobre el tema "Techniques: photometric"

1

Cartwright, Stephen John. Application of digital image processing techniques to the photometric testing of vehicle headlamps. Birmingham: Aston University. Department of Vision Sciences, 1986.

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J, Butler C. y Elliott I. 1936-, eds. 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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IAU Colloquium (136th 1992 Dublin, Ireland). 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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Parr, A. C. A national measurement system for radiometry, photometry, and pyrometry based upon absolute detectors. Gaithersburg, MD: U.S. Department of Commerce, Technology Administration, National Institute of Standards and Technology, 1996.

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Nicolau, Dan V., Daniel L. Farkas y Robert C. Leif. Imaging, manipulation, and analysis of biomolecules, cells, and tissues X: 21-23 January 2012, San Francisco, California, United States. Bellingham, Wash: SPIE, 2012.

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1927-, Eichhorn Heinrich K., Leacock Robert J y Kerrick Jeanne M, eds. Astrometric techniques: Proceedings of the 109th Symposium of the International Astronomical Union held in Gainesville, Florida, U.S.A., 9-12 January 1984. Dordrecht Holland: Reidel, 1986.

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Stetson, Peter B. The techniques of least squares and stellar photometry with CCDs: A series of five lectures presented at: V Escola Avançada de Astrofísica, 1989 July 30 - August 3, Aguas de São Pedro, Brazil. [S.l: s.n., 1990.

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Nicolau, Dan V., Daniel L. Farkas y Robert C. Leif. Imaging, manipulation, and analysis of biomolecules, cells, and tissues IX: 22-25 January 2011, San Francisco, California, United States. Bellingham, Wash: SPIE, 2011.

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Achilefu, Samuel. Genetically engineered and optical probes for biomedical applications IV: 23-24 January 2007, San Jose, California, USA. Editado por Society of Photo-optical Instrumentation Engineers. Bellingham, Wash: SPIE, 2007.

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United States. National Aeronautics and Space Administration., ed. Infrared imaging, spectroscopic, & photometric studies of comets: Final report, NASA/NAGW-2324. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Capítulos de libros sobre el tema "Techniques: photometric"

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Schneider, J. "Photometric Search for Extrasolar Planets". En The Search for Extra-Solar Terrestrial Planets: Techniques and Technology, 35–42. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-011-5808-4_3.

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Ohmori, Harunori. "Photometric Patch Electrode to Simultaneously Measure Neural Electrical Activity and Optical Signal in the Brain Tissue". En Basic Neurobiology Techniques, 131–53. New York, NY: Springer US, 2019. http://dx.doi.org/10.1007/978-1-4939-9944-6_6.

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Vetrekar, N. T., R. Raghavendra, R. S. Gad y G. M. Naik. "Photometric Normalization Techniques for Extended Multi-spectral Face Recognition: A Comparative Analysis". En Computer Vision, Graphics, and Image Processing, 27–38. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-68124-5_3.

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Lapasset, E., M. Gomez y R. Fariñas. "Test of the Optimization Techniques for the Photometric Analysis of Contact Binaries". En Evolutionary Processes in Interacting Binary Stars, 387–90. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2542-0_55.

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Kitchin, C. R. "Photometry". En Astrophysical Techniques, 287–311. Seventh edition. | Boca Raton : CRC Press, 2020.: CRC Press, 2020. http://dx.doi.org/10.1201/9780429491139-3.

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Kitchin, C. R. "Photometry". En Telescopes and Techniques, 213–21. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-4891-4_11.

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Kitchin, Chris. "Photometry". En Telescopes and Techniques, 207–17. London: Springer London, 2003. http://dx.doi.org/10.1007/978-1-4471-0023-2_11.

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Kitchin, Christopher Robert. "Photometry". En Telescopes and Techniques, 169–76. London: Springer London, 1995. http://dx.doi.org/10.1007/978-1-4471-3370-4_11.

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Høg, E. "Tycho Astrometry and Photometry". En Astrometric Techniques, 625–35. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4676-7_78.

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Dymock, Roger. "Lightcurve Photometry Tools and Techniques". En Astronomers' Observing Guides, 139–56. New York, NY: Springer New York, 2010. http://dx.doi.org/10.1007/978-1-4419-6439-7_12.

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Actas de conferencias sobre el tema "Techniques: photometric"

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Zheng, Hongwen y Yanxia Zhang. "Review of techniques for photometric redshift estimation". En SPIE Astronomical Telescopes + Instrumentation, editado por Nicole M. Radziwill y Gianluca Chiozzi. SPIE, 2012. http://dx.doi.org/10.1117/12.925314.

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Hashimoto, Naoki y Koki Kosaka. "Continuous photometric compensation for deformable objects". En SIGGRAPH '17: Special Interest Group on Computer Graphics and Interactive Techniques Conference. New York, NY, USA: ACM, 2017. http://dx.doi.org/10.1145/3102163.3102167.

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Vo, Quang Nhat, Anh Khoa Tran y Gueesang Lee. "Illumination Invariant L1 Tracker Using Photometric Normalization Techniques". En 2013 2nd IAPR Asian Conference on Pattern Recognition (ACPR). IEEE, 2013. http://dx.doi.org/10.1109/acpr.2013.104.

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Turri, Paolo, Alan W. McConnachie, Peter B. Stetson, David R. Andersen, Jean-Pierre Véran, Giuliana Fiorentino y Davide Massari. "Photometric techniques, performance and PSF characterization of GeMS". En SPIE Astronomical Telescopes + Instrumentation, editado por Enrico Marchetti, Laird M. Close y Jean-Pierre Véran. SPIE, 2016. http://dx.doi.org/10.1117/12.2233109.

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Hashimoto, Naoki y Koki Kosaka. "Photometric compensation for practical and complex textures". En SIGGRAPH '15: Special Interest Group on Computer Graphics and Interactive Techniques Conference. New York, NY, USA: ACM, 2015. http://dx.doi.org/10.1145/2787626.2787647.

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Dati, F., U. Becker, J. Keller, J. Huber, U. Schmitz-Huebner, H. Ostermann, A. Gressner y R. Zimmermann. "RESULTS OF THE MULTICENTRIC EVALUATION OF A NEW SYSTEM FOR PHOTOMETRIC DETERMINATION OF COAGULATION PARAMETERS". En XIth International Congress on Thrombosis and Haemostasis. Schattauer GmbH, 1987. http://dx.doi.org/10.1055/s-0038-1643258.

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Resumen
The classic coagulation analyses based on the clot formation present basic disadvantages which make a standardization of reagents difficult. The use of photometry for coagulation methods represents nowadays an important step towards test optimization.We have evaluated a new analytical system (ChromoTimeSystem, Behringwerke AG, Marburg/FRG) based on a special instrument and reagents for photometric tests for coagulation and fibrinolysis. The instrument is a microprocessor-controlled 4-channel-photometer operating at 37°C and connected to a microcomputer. Photometric methods for prothrombin time (PT: Chromoquick®) and activated partial thromboplastin time (aPTT: Partochrom®) have been developed using a new chromogenic substrate (Tos-Gly-Pro-Arg-5-amino-2-nitro-benzoic-acid-isopropy-lamide) specific for thrombin. These tests are based on the time necessary to attain a fixed increase of absorbance (0.1 A). Tests for thrombin time (TT), batroxobin time and fibrinogen rely on turbidimetric techniques. In the screening tests PT, aPTT and fibrinogen 25 μl sample (TT: 50 μl) and 250 μl reagent are used. Single coagulation factors are assayed by mixing an undiluted sample (10 μl) with the correspondent factor deficient plasma (50 μl) in connection with the chromogenic PT or aPTT reagent (500 μl). The evaluated specific chromogenic substrate methods are: antithrombin III, α2-antiplasmin and plasminogen.Tne characteristics of the ChromoTimeSystem are: fibrinogen-independent PT and PTT, small sample volumes (10-50 μl), no predilution or preincubation, PT standardization according to WHO recommendations, coefficients of variation between 1 and 4 %, good correlation between photometric and coagulometric tests, the reference values for photom. PTT being 90-120 sec.
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Khastavaneh, Hassan, Hossein Ebrahimpour-Komleh y Majid Joudaki. "Face image quality assessment based on photometric features and classification techniques". En 2017 IEEE 4th International Conference on Knowledge-Based Engineering and Innovation (KBEI). IEEE, 2017. http://dx.doi.org/10.1109/kbei.2017.8324988.

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Landstrom, Anders, Matthew J. Thurley y Hakan Jonsson. "Sub-Millimeter Crack Detection in Casted Steel Using Color Photometric Stereo". En 2013 International Conference on Digital Image Computing: Techniques and Applications (DICTA). IEEE, 2013. http://dx.doi.org/10.1109/dicta.2013.6691532.

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Lei, Jinyu, Enjun Wang, Juan Zeng, Weifeng Wang y Jianbo Wu. "Research of acquisition method for pavement surface texture based on photometric stereo techniques". En 2014 IEEE 17th International Conference on Intelligent Transportation Systems (ITSC). IEEE, 2014. http://dx.doi.org/10.1109/itsc.2014.6957921.

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Kornilov, M. V., M. V. Pruzhinskaya, K. L. Malanchev, E. E. O. Ishida, F. Mondon, A. A. Volnova y V. S. Korolev. "Machine learning techniques for analysis of photometric data from the Open Supernova catalog". En The multi-messenger astronomy: gamma-ray bursts, search for electromagnetic counterparts to neutrino events and gravitational waves. Sneg, 2019. http://dx.doi.org/10.26119/sao.2019.1.35517.

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Informes sobre el tema "Techniques: photometric"

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Jackson, Bernard V., Andrew Buffington y P. P. Hick. Development of Data Analysis Techniques to Provide Photometric Images for a Heliospheric Imager. Fort Belvoir, VA: Defense Technical Information Center, octubre de 2008. http://dx.doi.org/10.21236/ada519141.

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Stubbs, Christopher. Developing the Optimal Technique for Cluster Photometric Redshift Determination: An Essential Ingredient in Measuring Dark Energy with Cluster Abundances. Office of Scientific and Technical Information (OSTI), abril de 2009. http://dx.doi.org/10.2172/951183.

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