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the ferret an owners guide to a happy healthy pet your happy healthy p LINK 1 ENTER SITE >>> http://merky.de/vj2orh <<< Download LINK 2 ENTER SITE >>> <!DOCTYPE HTML PUBLIC "-//IETF//DTD HTML 2.0//EN"> <html><head> <title>403 Forbidden</title> </head><body> <h1>Forbidden</h1> <p>You don't have permission to access /api.php on this server.</p> <p>Additionally, a 403 Forbidden error was encountered while trying to use an ErrorDocument to handle the request.</p> <hr> <address>Apache/2.2.3 (CentOS) Server at chilp.it Port 80</address> </body></html> <<< Download PDF File Name:the ferret an owners guide to a happy healthy pet your happy healthy p.pdf Size: 2979 KB Type: PDF, ePub, eBook Uploaded: 30 May 2019, 23:46 Rating: 4.6/5 from 813 votes. Status: AVAILABLE Last checked: 2 Minutes ago! eBook includes PDF, ePub and Kindle version In order to read or download the ferret an owners guide to a happy healthy pet your happy healthy p ebook, you need to create a FREE account. ✔ Register a free 1 month Trial Account. ✔ Download as many books as you like (Personal use) ✔ Cancel the membership at any time if not satisfied. ✔ Join Over 80000 Happy Readers the ferret an owners guide to a happy healthy pet your happy healthy p The 13-digit and 10-digit formats both work. Please try again.Please try again.Please try again. Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture,field of view, and angluar coverage. Digital Image Formats: Covers the file formats that astronomers use, including FITS, TIFF, BMP, and JPEG. Learn file format basics, how your image data is arranged inside the file on your computer's hard disk. Imaging Tools: All about sensors, optics, cameras, and telescopes. Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems. Then you can start reading Kindle books on your smartphone, tablet, or computer - no Kindle device required. Register a free business account Full content visible, double tap to read brief content. Videos Help others learn more about this product by uploading a video. Upload video To calculate the overall star rating and percentage breakdown by star, we don’t use a simple average. Instead, our system considers things like how recent a review is and if the reviewer bought the item on Amazon. It also analyzes reviews to verify trustworthiness. Please try again later. Sean Raybun 4.0 out of 5 stars Unfortunately the included software is outdated unless you are using an older SBIG ST CCD's. It only errors out when I tried opening images from a Starshoot Pro II. Not a big issue for I use MaximDL and DeepSkyStacker for my processing anyways. But I have been looking for something that explains the advanced image processing features. Playing with sliders all day such as in the wavelet filter and never understanding what is really going on has become a limit that needs overcoming. Now I can find the basic descriptions and the math behind all these functions. There is so much in this book that one could write a complete image processing program around the math in this book. http://gregoryshow.ru/files/file/dell-studio-xps-13-user-manual.xml the ferret an owners guide to a happy healthy pet your happy healthy p, the ferret an owners guide to a happy healthy pet your happy healthy person, the ferret an owners guide to a happy healthy pet your happy healthy pet, the ferret an owners guide to a happy healthy pet your happy healthy people, the ferret an owners guide to a happy healthy pet your happy healthy pets. Unlike the software, the book has been written with the future enhancements in mind, so that the pages are still up to date and useful.Just don't confuse the two. Even if you have image processing software now you NEED this book!This book is different, it dives into the physics of actual photon counting (yes, there are a lots of formulas!) and into very depths of image processing. It's the first book which truly explained to me what image calibration is all about. It describes what wavelets and deconvolution are and how to apply them to astrophotography. Don't worry about an old publication date - this book describes principles which are still true and will be for a long time. Highly recommended for a serious astrophotographers!It is much more than that. It explains the theory behind the software in terms of the processing of astronomical images. In that respect you are going to run into much of the same material you would encounter in Gonzales and Woods' Digital Image Processing, just from a different perspective. It would probably be good if you already know the basics of image processing from a book like Gonzalez and Woods before reading this one. This book's primary aim is not explaining DIP, but explaining how it is used to perform the processing of astronomical images. The following is the table of contents of the book and each chapter's summary. Basic imaging: How the light that falls on your CCD becomes an image. Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture, field of view, and angluar coverage. Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems. Imaging Techniques: Good equipment is just part of the story. Covers the techniques that experienced imagers use to obtain high-quality images. http://agendatourvietnam.com/hinhanh/dell-studio-xps-13-repair-manual.xml Includes polar alignment, good guiding, critical focus, correct exposure, darks and flats, light boxes, and special considerations for DSLR cameras. Image Calibration: Examines the details of image calibration. All about bias, dark noise, flat-fielding, standard and scalable darks, cosmic rays, making master dark frames, flats, standard calibration protocols, and defect mapping and correction. Image Analysis: Locked within the numerical values that make up a calibrated CCD image is a staggering amount of information. Covers pixel coordinates, pixel value, image statistics, the image histogram, feature analysis, the centroid, distances, and image profiles. Measuring CCD Performance: How to measure the performance of your CCD camera. Discusses goals in measuring CCD performance, how to shoot test images, and the determination of bias level, dark current, gain, linearity, and readout noise. Astrometry: Asteroid hunters measure the postions of new-found objects using astrometry. Covers the theory behind finding right ascension and declination from a CCD image, practical astrometry, and the uses of astrometry. Photometry: Amateur observers now work side by side with professional astronomers to measure the variations of variable stars, supernovae, asteroids, and comets using the CCD to capture precise measures of brightness. Spectroscopy: An emerging area for amateus astronomers brought to you by the CCD camera. Covers spectra and spectrographs, gratings, prisms, slit- and slitless systems, and the properties and meaning of stellar spectra. Geometric Transforms: Covers translation, rotation, scaling, flipping, cropping, floating, and resampling. Demystifies the basic geometric operations used in astronomical image processing. Point Operations: Learn how software converts the pixel values your CCD camera captures into the sparkling images you see in popular magazines and amateur websites. Remapping, transfer functions, linear, log, and exponential scalings explained. https://events.citeve.pt/chat-conversation/boss-gt-6-manual-free-download Covers endpoint specification and histogram specification. Linear Operators: All about one of the most useful tools in the amateur astronomer's digital toolbox. Describes how digital convolution performs crispening, sharpening, smoothing. Learn about low-pass and high-pass kernels, Sobel, Kirsch, and Prewitt operators, and that most useful of linear tools: the unsharp mask. Non-Linear Operators: Non-linear operators perform useful services like cleaning up noisy images. Cover rank-order processes, the median filter, local adaptive sharpening, noise filters, and morphological operators. Image Operations: Multi-image operations are the basic tool for making superior astro-images. Covers image math, median-combine stacking, image registration, blinking, and track-and-stack image summing. Images in Frequency Space: Unlocks the mysteries of the Fourier Transform and image processing in the spatial frequency domain. These powerful techniques used by profession astronomers are now accessible to amateurs Wavelets: Explores the hottest new image processing and restoration techniques. Covers the wavelet transform, the inverse wavelet transform, spatial filtering, the wavelet noise filter, and iterative filtering techniques. Deconvolution: Deconvolution attempts to restore images degraded by a turbulent atmosphere, poor telescope optics, and tracking errors. Discusses algorithms used to sharpen Hubble Space Telescope images, how they work, and how amateurs can use them. Building Color Images: You've seen fantastic astro-images on the web and in popular magazines and books. Learn how astronomers capture and build color images from multiple exposures through different color filters. Covers the colors of astronomical objects, luminace, chrominance, color space, white balance, G2V stars, RGB and LRGB color image capture. Processing Color Images: The digital SLR camera has done much to bring color imaging to the average amateur astronomer. http://www.neem-tree.com/images/950-john-deere-manual.pdf Explains the Bayer array, color image bit depth, noise, dark current, vignetting, calibration, image stacking, and luminace enhancement techniquesThis book has undergone five printings within the second edition, each successive printing correcting several errors, many quite serious. The current printing is the fifth, is softcover, and has ISBN 9781942675082. The books on this page are older printings, in hardcover, and should be avoided. The continued availability of this wonderful book is uncertain. Get it if you can.Buyer beware!High detailed from file structure to image processing. Both theory and practical stuff with enclosed CD with AIP4WIN software.My previous copy of this book got left out in the rain. I was very happy to find a replacment and even happier with the service I received from the vendor. Please try again.Please try again.Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture,field of view, and angluar coverage.Learn file format basics, how your image data is arranged inside the file on your computer's hard disk.Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems.Please try your search again later.Today's affordable astro-imaging capable digital single-lens-reflex cameras (DSLRs), the growing power of personal computers, and the proliferation of telescopes and imaging accessories has brought imaging capabilities within the reach of practically every amateur astronomer - and this second edition of the Handbook plus AIP4Win 2.0 is ready, willing, and able to assist every observer in making great astronomical images. In the Handbook, we amplified the original chapters on astronomical equipment and imaging techniques, revised our discussions of astrometry and photometry to reflect the steady growth in these scientific fields, and expanded tutorials in the back of the book to help you get up to speed quickly. On the accompanying CDROM (found on the inside back cover) you will find hundreds of megabytes of sample images you can use to learn techniques such as image registration and stacking that guarantee good results even from those living with suburban and urban skies. Also new are comprehensive chapters on color imaging with astronomical CCD cameras and processing color images from digital cameras, and photon-counting fundamentals every serious astro-imager needs toFull content visible, double tap to read brief content. Gene Salamin 5.0 out of 5 stars The book offered here is not the latest. The latest printing comes with version 2.4 software. In addition, the latest printing corrects numerous errors in prior printings, some of which are quite serious. Buy this book directly from the publisher, Willmann-Bell at willbell.com. Request full-text Download citation Copy link Link copied Request full-text Download citation Copy link Link copied To read the full-text of this research, you can request a copy directly from the authors. Request full-text PDF Citations (252) References (0). Knowing the RA (?) and DEC (?) of a star, we can determine the standard coordinates on the plane tangent to the celestial sphere at the point (. The foundation for multiwavelength astronomy is given by Astrometry; the science of position and motion determination of celestial bodies. We present a technique of determining equatorial coordinates of celestial bodies from their pixel coordinates. We also present the subsequent results of using this technique in achieving the initial few steps required for the multiwavelength studies of young open clusters. View Show abstract. The CCD-camera is equipped with B, V and I c filters manufactured to match the Johnson-Cousins Bessell prescription. Instrumental readings were reduced to catalog-based magnitudes using the AAVSO Photometric All-Sky Survey (APASS) star fields (Henden et al. 2009(Henden et al., 2010Smith et al. 2011) built into MPO Canopus v10.7.1.3.. The full derivation of this expression can be found in Breger (1990). No other statistically significant frequency shared by all bandpasses was resolved following successive pre-whitening of each residual signal. Except for 36 new times-of-maximum light produced from the present study, no other values were found in the literature; therefore, potential secular period changes could not be evaluated. This signal accumulates with exposure time and is temperature dependent... Many cultural heritage imaging projects implement one or several techniques to reduce the amount of noise in the image and try to extract the photon signal. Besides those elementary image correction techniques, there are many other post-processing techniques that can be called upon at a specific stage in a particular imaging workflow: examples are white and black point compensation, contrast adjustments, image alignment and mosaicking, lens distortion correction and image deconvolution.. Basics of photography for cultural heritage imaging Chapter Full-text available Aug 2016 Geert J J Verhoeven View. After the algorithm determines the exact duration (i.e. the beginning and ending frames) of the event, centroiding is performed by reconstructing each frame of the event and again extracting a strip around the event. A center-ofmass calculation is performed, using pixel intensities as weights ( Berry and Burnell, 2005 ). A regression procedure is performed to fit the well-known intensity vs. The new algorithm produced an order of magnitude better results, although results of the subsequent runs on the same dataset varied slightly because of the random sampling of the images from which the stars are used.. Open-source meteor detection software for low-cost single-board computers Conference Paper Full-text available Jun 2016 Denis Vida Dario Zubovic Damir Segon Robert Cupec This work aims to overcome the current price threshold of meteor stations which can sometimes deter meteor enthusiasts from owning one. In recent years small card-sized computers became widely available and are used for numerous applications. To utilize such computers for meteor work, software which can run on them is needed. In this paper we present a detailed description of newly-developed open-source software for fireball and meteor detection optimized for running on low-cost single board computers. Furthermore, an update on the development of automated open-source software which will handle video capture, fireball and meteor detection, astrometry and photometry is given. The study of W UMa stars is essential for modern astrophysics because they are probes for investigation of the processes of tidal interactions, mass loss and mass transfer, angular momentum loss, merging or fusion of the stars (Martin et al., 2011). According to the thermal relaxation oscillation (TRO) model each component of the W UMa stars is out of thermal equilibrium and oscillates around the inner Roche lobe (Lucy, 1976; Flannery, 1976; Robertson and Eggleton, 1977;Yakut and Eggleton, 2005). The light curve solutions revealed that these binaries have overcontact configurations with small fillout factors (within 0.1-0.2). Seven of them undergo total eclipses and their photometric mass ratios should be accepted with confidence. Thus, the optical coordinates of 6 mentioned ERS objects were determined.. CCD OBSERVATIONS OF ERS WITH THE 60 cm TELESCOPE AT ASV Conference Paper Full-text available Sep 2012 Ivana Milic Zitnik View. Our photometric observations were reduced with AIP4WIN2.0 ( Berry and Burnell, 2005 ). An aperture ensemble photometry was performed with the software VPHOT using six standard stars ( Table 2 ) in the observed field whose coordinates were taken from the catalogue UCAC4 ( Zacharias et al., 2013 ) and their magnitudes from the catalogue APASS DR9 ( Henden et al., 2016 )... Obviously, the reproducing of data required another geometry of the system. Its main peculiarity is the big increasing of eclipse depth during outburst. We qualitatively modelled the folded light curves at quiescence and outburst in order to explain the reason for increase of the primary luminosity about two hundred times. The light curve fits revealed that such an effect can be reproduced by a flat disc whose radius and temperature are several times bigger than those of the primary at quiescence. Stacking or accumulating camera frames is a well-known technique in astrophysics (see Berry and Burnell, 2005). The track-and-stack technique is an effective method to obtain long exposures from many short ones of faint deep-sky objects while tracking... There is also a color shift from faint green-yellow to pink with increasing boxcar width in Fig. 5 associated with change in color balance in the composite images, indicating that our technique is not conservative. The use of wavelets has become a popular method to enhance details in images (Berry and Burnell, 2005). By interactively recombining wavelet transforms at different spatial scales and layers, small-scale features are enhanced and large-scale shading effects are reduced.. Video cascade accumulation of the total solar eclipse on Svalbard 2015 Article Full-text available Jan 2017 F. Sigernes Pal Gunnar Ellingsen Noora Partamies Shadia Habbal This work presents a novel image accumulation filter technique that reveals small-scale features and details from intense luminosity or high dynamic range (HDR) video recordings. The result of the filter is fused with a HDR image of the corona and the Solar Dynamic Observatory (SDO) image of the solar disk. The procedure is implemented in a function that takes in input the two times of flight, the geocentric positions vectors of the observer (R 1, R 2, R 3 ) and the topocentric direction cosine vector (? 1,? 2,? 3 ).. Image processing of multiclass satellite tracklets for initial orbit determination based on optical telescopes Thesis Apr 2018 Giovanni Lavezzi Satellites orbiting around the Earth are used for many purposes; they can be ofThe growth in space satelliteIn fact an in-orbit collision mayFor these reasons, mitigation strategies haveAwareness (SSA) program, able to provide Europe with timely and precise informationInside the SSA program, the Space Surveillance and. Tracking (SST) segment is targeted at tracking and maintaining the informationTo perform these observation tasks, nowadays, radar orThis thesis fits in the field of SSA and SST. In particular, the main goal isView Show abstract. In the determination of the separations and position angle the AIP4WIN program was used, whereas the IRAF package was also used, in addition to the determination of separations and position angle, to determine the magnitude difference between the components of the pairs.. CCD Measurements of Double and Multiple Stars at NAO Rozhen and ASV in 2015 Article Apr 2017 S. Boeva Z. Cvetkovic Rade Pavlovic Results of CCD observations of 154 double or multiple stars, made with the 2 m telescope of the Bulgarian National Astronomical Observatory at Rozhen over five nights in 2015, are presented. This is the ninth series of measurements of CCD frames obtained at Rozhen. We also present results of CCD observations of 323 double or multiple stars made with the 0.6 m telescope of the Serbian Astronomical Station on the mountain of Vidojevica over 23 nights in 2015. This is the fourth series of measurements of CCD frames obtained at this station. This paper contains the results for the position angle and angular separation for 801 pairs and residuals for 127 pairs with published orbital elements or linear solutions. The angular separations are in the range from 152 to 20156, with a median angular separation of 826. We also present eight pairs that are measured for the first time and linear elements for five pairs. The frames were combined into a single master bias, and dark and flat frames. The periods of these binaries are in the range of 0.26-0.43 d. The light curve solutions revealed that the components of each binary system are almost equal in temperature. The stellar components are of G and K spectral types and undergo total eclipses. The photometric data were reduced by AIP4WIN2.0 (Berry, Burnell 2006). As a result their initial epochs were determined. The target periods turned out almost equal to the previous values. Their stellar components seem to obey the relations mass-temperature of MS stars. They allowed the improvement of system ephemerides. The errors are formal 1-.All images were corrected for bias and flat-fielded in the standard way.. The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7-311525 Article Jan 2017 MON NOT R ASTRON SOC Vitaly V. Neustroev T. R. Marsh S. Zharikov J. P. Moore We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7-311525 during its unusual double superoutburst, the following decline and in quiescence. The colours then became bluer again, but it took at least 250 days to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 days after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess View Show abstract. C onsumer grade digital cameras have been applied for astronomical image processing, the analysis of cloud cover, photogrammetry, high dynamic range imaging, and luminance measurement ( Berry and Burnell 2006; Roy 2001; Hadwan 2002; Reinhard 2006). High-resolution luminance maps with a wide field of view (FOV) offer new opportunities for image based photometry, statistical image analysis, and derived lighting metrics, such as spherical illuminance distributions and glare.. Accuracy of Luminance Maps Obtained from High Dynamic Range Images Article Full-text available Jan 2006 Smita Anaokar Martin Moeck Abstract—High dynamic range (HDR) imaging offers the potential toTherefore, they may also be usedThe luminance maps obtained from HDRThe corresponding illuminanceThis allows a new wayThis paper explains how to properlyHarrisburg, Pennsylvania. Although the designs can be very attractive due to factors such as appearance and light redirection and rejection, very little is known about their daylighting performance and no daylight distribution data have been published. Monitoring these buildings would require multiple illuminance sensors or luminance calibrated CCD cameras (Andersen and others 2001; Berry and Burnell 2000). Measuring the bi-directional transmittance of these DODs in the laboratory is a major undertaking, and few software tools can manipulate the data (Apian-Bennewitz 1994;Breitenbach and Rosenfeld 1998;Mitanchey and others 1995;Murray-Coleman and Smith 1990;Papamichael and others 1988).. Modeling Intensity Distributions of Advanced Daylight Systems Surrounded by Arbitrary Luminance Maps Article Full-text available Jul 2005 Youn Ju Yoon Martin Moeck Abstract—For more than a decade, daylighting optical devices (DOD)Some of these systems show considerableHowever, their daylight performance is not clearlyThe first is the generation of aThe second problem is theWe shows how toResults of testsVarious software packages haveView Show abstract. Also, the proper motions of many double or multiple stars are unreliable due to the short epoch span of Hipparcos observations, and van Leeuwen (2007) The main characteristics of CCD camera are: 1340x1300 pixels, the pixel size is 20x20 mkm, one pixel is 0 ??.258. The AIP4WIN image processing package (Berry and Burnell, 2002) was used. All frames were reduced individually.. CCD MEASUREMENTS IN OPTICAL DOMAIN AND ASTROMETRIC POSITIONS OF ICRF2 RADIO SOURCES Conference Paper Full-text available Jan 2011 Ivana Milic Zitnik At the IAU XXIIIth GA in 1997, the International Celestial Reference Frame (ICRF) was adopted; hereafter referred to as ICRF1. After the original list of radio objects there were two extensions, ICRF-ext1 and ICRF-ext2. All together, there were 717 sources: 212 defining ones, 109 new ones, 294 candidate ones, and 102 additional ones. At the IAU XXVIIth GA in 2009, the second realization of the ICRF (the ICRF2) was adopted with the list of precise positions for 3414 compact radio astronomical sources. At that moment there were nearly 30 years of VLBI observations. The ICRF2 has a noise floor of about 0.04 mas (near six times better than ICRF1) and an axis stability of about 0.01 mas (nearly twice as stable as ICRF1). Also, it is of importance to make the observations of some ICRF2 extragalactic radio sources (ERS) which are visible in the optical domain, and to compare their optical (calculated via the reference stars) and radio positions (VLBI ones). About 30 frames were observed at the end of March 2011. The main steps of our calculations and some preliminary results (comparison between the measured optical positions and the radio ones) for a few ERS from ICRF2 list were presented here. 1. CALCULATION AND RESULTS Regular maintenance of the system and improvement of the frame is necessary. The ERS coordinates are continuously improving via VLBI observations (a large number of observations of defining ERS over a long data span). The frame's stability is based upon the assumption that there is no global rotation of the universe. The ERS positions are known to better than 1 mas, and the ultimate accuracy is limited because of the structure instability of ERS in radio wavelengths. From 1 January 2010, the realization of the ICRS is the ICRF2. That accuracy degrades over time because of the error in proper motions of stars, and it is necessary to verify and refine the relation between the HCRF and the ICRF2. It can be done via different telescopes and methods. The position of objects in the frames were measured by using the AIP4WIN software (Berry and Burnell 2002).. Professional paper FOCAL LENGTH DETERMINATION FOR THE 60 cm TELESCOPE AT ASTRONOMICAL STATION VIDOJEVICA Article Full-text available Jan 2012 Z. Cvetkovic G. Damljanovic Rade Pavlovic Milan Stojanovic View. Thereby, the removal of Poisson noise is of fundamental importance especially for further processing, such as image segmentation and recognition.. Poisson Noise Reduction with Higher-Order Natural Image Prior Model Article Full-text available Sep 2016 Wensen Feng Hong Qiao Yunjin Chen Poisson denoising is an essential issue for various imaging applications, such as night vision, medical imaging and microscopy. State-of-the-art approaches are clearly dominated by patch-based non-local methods in recent years. In this paper, we aim to propose a local Poisson denoising model with both structure simplicity and good performance. To this end, we consider a variational modeling to integrate the so-called Fields of Experts (FoE) image prior, that has proven an effective higher-order Markov Random Fields (MRF) model for many classic image restoration problems. We exploit several feasible variational variants for this task. We start with a direct modeling in the original image domain by taking into account the Poisson noise statistics, which performs generally well for the cases of high SNR. However, this strategy encounters problem in cases of low SNR. Then we turn to an alternative modeling strategy by using the Anscombe transform and Gaussian statistics derived data term. We retrain the FoE prior model directly in the transform domain. With the newly trained FoE model, we end up with a local variational model providing strongly competitive results against state-of-the-art non-local approaches, meanwhile bearing the property of simple structure. Furthermore, our proposed model comes along with an additional advantage, that the inference is very efficient as it is well-suited for parallel computation on GPUs. We created these images by subtracting a median lunar image based on the 5 frames before and 5 frames after the event. Optimal apertures corresponding to the maximum in the signal-to-noise of the flux measurement were used for the flashes to avoid adding noise from the subtracted background, while large apertures were used for the standards.. NELIOTA: First temperature measurement of lunar impact flashes Article Full-text available Oct 2017 ASTRON ASTROPHYS C. Avdellidou A. Maroussis A. Z. Bonanos Alexios Liakos We report the first scientific results from the NELIOTA (NEO Lunar Impacts and Optical TrAnsients) project, which has recently begun lunar monitoring observations with the 1.2-m Kryoneri telescope.
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the ferret an owners guide to a happy healthy pet your happy healthy p LINK 1 ENTER SITE >>> http://merky.de/vj2orh <<< Download LINK 2 ENTER SITE >>> <!DOCTYPE HTML PUBLIC "-//IETF//DTD HTML 2.0//EN"> <html><head> <title>403 Forbidden</title> </head><body> <h1>Forbidden</h1> <p>You don't have permission to access /api.php on this server.</p> <p>Additionally, a 403 Forbidden error was encountered while trying to use an ErrorDocument to handle the request.</p> <hr> <address>Apache/2.2.3 (CentOS) Server at chilp.it Port 80</address> </body></html> <<< Download PDF File Name:the ferret an owners guide to a happy healthy pet your happy healthy p.pdf Size: 2979 KB Type: PDF, ePub, eBook Uploaded: 30 May 2019, 23:46 Rating: 4.6/5 from 813 votes. Status: AVAILABLE Last checked: 2 Minutes ago! eBook includes PDF, ePub and Kindle version In order to read or download the ferret an owners guide to a happy healthy pet your happy healthy p ebook, you need to create a FREE account. ✔ Register a free 1 month Trial Account. ✔ Download as many books as you like (Personal use) ✔ Cancel the membership at any time if not satisfied. ✔ Join Over 80000 Happy Readers the ferret an owners guide to a happy healthy pet your happy healthy p The 13-digit and 10-digit formats both work. Please try again.Please try again.Please try again. Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture,field of view, and angluar coverage. Digital Image Formats: Covers the file formats that astronomers use, including FITS, TIFF, BMP, and JPEG. Learn file format basics, how your image data is arranged inside the file on your computer's hard disk. Imaging Tools: All about sensors, optics, cameras, and telescopes. Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems. Then you can start reading Kindle books on your smartphone, tablet, or computer - no Kindle device required. Register a free business account Full content visible, double tap to read brief content. Videos Help others learn more about this product by uploading a video. Upload video To calculate the overall star rating and percentage breakdown by star, we don’t use a simple average. Instead, our system considers things like how recent a review is and if the reviewer bought the item on Amazon. It also analyzes reviews to verify trustworthiness. Please try again later. Sean Raybun 4.0 out of 5 stars Unfortunately the included software is outdated unless you are using an older SBIG ST CCD's. It only errors out when I tried opening images from a Starshoot Pro II. Not a big issue for I use MaximDL and DeepSkyStacker for my processing anyways. But I have been looking for something that explains the advanced image processing features. Playing with sliders all day such as in the wavelet filter and never understanding what is really going on has become a limit that needs overcoming. Now I can find the basic descriptions and the math behind all these functions. There is so much in this book that one could write a complete image processing program around the math in this book. http://gregoryshow.ru/files/file/dell-studio-xps-13-user-manual.xml the ferret an owners guide to a happy healthy pet your happy healthy p, the ferret an owners guide to a happy healthy pet your happy healthy person, the ferret an owners guide to a happy healthy pet your happy healthy pet, the ferret an owners guide to a happy healthy pet your happy healthy people, the ferret an owners guide to a happy healthy pet your happy healthy pets. Unlike the software, the book has been written with the future enhancements in mind, so that the pages are still up to date and useful.Just don't confuse the two. Even if you have image processing software now you NEED this book!This book is different, it dives into the physics of actual photon counting (yes, there are a lots of formulas!) and into very depths of image processing. It's the first book which truly explained to me what image calibration is all about. It describes what wavelets and deconvolution are and how to apply them to astrophotography. Don't worry about an old publication date - this book describes principles which are still true and will be for a long time. Highly recommended for a serious astrophotographers!It is much more than that. It explains the theory behind the software in terms of the processing of astronomical images. In that respect you are going to run into much of the same material you would encounter in Gonzales and Woods' Digital Image Processing, just from a different perspective. It would probably be good if you already know the basics of image processing from a book like Gonzalez and Woods before reading this one. This book's primary aim is not explaining DIP, but explaining how it is used to perform the processing of astronomical images. The following is the table of contents of the book and each chapter's summary. Basic imaging: How the light that falls on your CCD becomes an image. Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture, field of view, and angluar coverage. Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems. Imaging Techniques: Good equipment is just part of the story. Covers the techniques that experienced imagers use to obtain high-quality images. http://agendatourvietnam.com/hinhanh/dell-studio-xps-13-repair-manual.xml Includes polar alignment, good guiding, critical focus, correct exposure, darks and flats, light boxes, and special considerations for DSLR cameras. Image Calibration: Examines the details of image calibration. All about bias, dark noise, flat-fielding, standard and scalable darks, cosmic rays, making master dark frames, flats, standard calibration protocols, and defect mapping and correction. Image Analysis: Locked within the numerical values that make up a calibrated CCD image is a staggering amount of information. Covers pixel coordinates, pixel value, image statistics, the image histogram, feature analysis, the centroid, distances, and image profiles. Measuring CCD Performance: How to measure the performance of your CCD camera. Discusses goals in measuring CCD performance, how to shoot test images, and the determination of bias level, dark current, gain, linearity, and readout noise. Astrometry: Asteroid hunters measure the postions of new-found objects using astrometry. Covers the theory behind finding right ascension and declination from a CCD image, practical astrometry, and the uses of astrometry. Photometry: Amateur observers now work side by side with professional astronomers to measure the variations of variable stars, supernovae, asteroids, and comets using the CCD to capture precise measures of brightness. Spectroscopy: An emerging area for amateus astronomers brought to you by the CCD camera. Covers spectra and spectrographs, gratings, prisms, slit- and slitless systems, and the properties and meaning of stellar spectra. Geometric Transforms: Covers translation, rotation, scaling, flipping, cropping, floating, and resampling. Demystifies the basic geometric operations used in astronomical image processing. Point Operations: Learn how software converts the pixel values your CCD camera captures into the sparkling images you see in popular magazines and amateur websites. Remapping, transfer functions, linear, log, and exponential scalings explained. https://events.citeve.pt/chat-conversation/boss-gt-6-manual-free-download Covers endpoint specification and histogram specification. Linear Operators: All about one of the most useful tools in the amateur astronomer's digital toolbox. Describes how digital convolution performs crispening, sharpening, smoothing. Learn about low-pass and high-pass kernels, Sobel, Kirsch, and Prewitt operators, and that most useful of linear tools: the unsharp mask. Non-Linear Operators: Non-linear operators perform useful services like cleaning up noisy images. Cover rank-order processes, the median filter, local adaptive sharpening, noise filters, and morphological operators. Image Operations: Multi-image operations are the basic tool for making superior astro-images. Covers image math, median-combine stacking, image registration, blinking, and track-and-stack image summing. Images in Frequency Space: Unlocks the mysteries of the Fourier Transform and image processing in the spatial frequency domain. These powerful techniques used by profession astronomers are now accessible to amateurs Wavelets: Explores the hottest new image processing and restoration techniques. Covers the wavelet transform, the inverse wavelet transform, spatial filtering, the wavelet noise filter, and iterative filtering techniques. Deconvolution: Deconvolution attempts to restore images degraded by a turbulent atmosphere, poor telescope optics, and tracking errors. Discusses algorithms used to sharpen Hubble Space Telescope images, how they work, and how amateurs can use them. Building Color Images: You've seen fantastic astro-images on the web and in popular magazines and books. Learn how astronomers capture and build color images from multiple exposures through different color filters. Covers the colors of astronomical objects, luminace, chrominance, color space, white balance, G2V stars, RGB and LRGB color image capture. Processing Color Images: The digital SLR camera has done much to bring color imaging to the average amateur astronomer. http://www.neem-tree.com/images/950-john-deere-manual.pdf Explains the Bayer array, color image bit depth, noise, dark current, vignetting, calibration, image stacking, and luminace enhancement techniquesThis book has undergone five printings within the second edition, each successive printing correcting several errors, many quite serious. The current printing is the fifth, is softcover, and has ISBN 9781942675082. The books on this page are older printings, in hardcover, and should be avoided. The continued availability of this wonderful book is uncertain. Get it if you can.Buyer beware!High detailed from file structure to image processing. Both theory and practical stuff with enclosed CD with AIP4WIN software.My previous copy of this book got left out in the rain. I was very happy to find a replacment and even happier with the service I received from the vendor. Please try again.Please try again.Covers image formation, cameras, telescopes, detectors, sensor geometry, image capture,field of view, and angluar coverage.Learn file format basics, how your image data is arranged inside the file on your computer's hard disk.Explains how to calculate the field of view and resolution of your system, telescope optics for imagers, auxiliary optics, mounts, drives, tracking, filters, and how to recognize and correct common equipment problems.Please try your search again later.Today's affordable astro-imaging capable digital single-lens-reflex cameras (DSLRs), the growing power of personal computers, and the proliferation of telescopes and imaging accessories has brought imaging capabilities within the reach of practically every amateur astronomer - and this second edition of the Handbook plus AIP4Win 2.0 is ready, willing, and able to assist every observer in making great astronomical images. In the Handbook, we amplified the original chapters on astronomical equipment and imaging techniques, revised our discussions of astrometry and photometry to reflect the steady growth in these scientific fields, and expanded tutorials in the back of the book to help you get up to speed quickly. On the accompanying CDROM (found on the inside back cover) you will find hundreds of megabytes of sample images you can use to learn techniques such as image registration and stacking that guarantee good results even from those living with suburban and urban skies. Also new are comprehensive chapters on color imaging with astronomical CCD cameras and processing color images from digital cameras, and photon-counting fundamentals every serious astro-imager needs toFull content visible, double tap to read brief content. Gene Salamin 5.0 out of 5 stars The book offered here is not the latest. The latest printing comes with version 2.4 software. In addition, the latest printing corrects numerous errors in prior printings, some of which are quite serious. Buy this book directly from the publisher, Willmann-Bell at willbell.com. Request full-text Download citation Copy link Link copied Request full-text Download citation Copy link Link copied To read the full-text of this research, you can request a copy directly from the authors. Request full-text PDF Citations (252) References (0). Knowing the RA (?) and DEC (?) of a star, we can determine the standard coordinates on the plane tangent to the celestial sphere at the point (. The foundation for multiwavelength astronomy is given by Astrometry; the science of position and motion determination of celestial bodies. We present a technique of determining equatorial coordinates of celestial bodies from their pixel coordinates. We also present the subsequent results of using this technique in achieving the initial few steps required for the multiwavelength studies of young open clusters. View Show abstract. The CCD-camera is equipped with B, V and I c filters manufactured to match the Johnson-Cousins Bessell prescription. Instrumental readings were reduced to catalog-based magnitudes using the AAVSO Photometric All-Sky Survey (APASS) star fields (Henden et al. 2009(Henden et al., 2010Smith et al. 2011) built into MPO Canopus v10.7.1.3.. The full derivation of this expression can be found in Breger (1990). No other statistically significant frequency shared by all bandpasses was resolved following successive pre-whitening of each residual signal. Except for 36 new times-of-maximum light produced from the present study, no other values were found in the literature; therefore, potential secular period changes could not be evaluated. This signal accumulates with exposure time and is temperature dependent... Many cultural heritage imaging projects implement one or several techniques to reduce the amount of noise in the image and try to extract the photon signal. Besides those elementary image correction techniques, there are many other post-processing techniques that can be called upon at a specific stage in a particular imaging workflow: examples are white and black point compensation, contrast adjustments, image alignment and mosaicking, lens distortion correction and image deconvolution.. Basics of photography for cultural heritage imaging Chapter Full-text available Aug 2016 Geert J J Verhoeven View. After the algorithm determines the exact duration (i.e. the beginning and ending frames) of the event, centroiding is performed by reconstructing each frame of the event and again extracting a strip around the event. A center-ofmass calculation is performed, using pixel intensities as weights ( Berry and Burnell, 2005 ). A regression procedure is performed to fit the well-known intensity vs. The new algorithm produced an order of magnitude better results, although results of the subsequent runs on the same dataset varied slightly because of the random sampling of the images from which the stars are used.. Open-source meteor detection software for low-cost single-board computers Conference Paper Full-text available Jun 2016 Denis Vida Dario Zubovic Damir Segon Robert Cupec This work aims to overcome the current price threshold of meteor stations which can sometimes deter meteor enthusiasts from owning one. In recent years small card-sized computers became widely available and are used for numerous applications. To utilize such computers for meteor work, software which can run on them is needed. In this paper we present a detailed description of newly-developed open-source software for fireball and meteor detection optimized for running on low-cost single board computers. Furthermore, an update on the development of automated open-source software which will handle video capture, fireball and meteor detection, astrometry and photometry is given. The study of W UMa stars is essential for modern astrophysics because they are probes for investigation of the processes of tidal interactions, mass loss and mass transfer, angular momentum loss, merging or fusion of the stars (Martin et al., 2011). According to the thermal relaxation oscillation (TRO) model each component of the W UMa stars is out of thermal equilibrium and oscillates around the inner Roche lobe (Lucy, 1976; Flannery, 1976; Robertson and Eggleton, 1977;Yakut and Eggleton, 2005). The light curve solutions revealed that these binaries have overcontact configurations with small fillout factors (within 0.1-0.2). Seven of them undergo total eclipses and their photometric mass ratios should be accepted with confidence. Thus, the optical coordinates of 6 mentioned ERS objects were determined.. CCD OBSERVATIONS OF ERS WITH THE 60 cm TELESCOPE AT ASV Conference Paper Full-text available Sep 2012 Ivana Milic Zitnik View. Our photometric observations were reduced with AIP4WIN2.0 ( Berry and Burnell, 2005 ). An aperture ensemble photometry was performed with the software VPHOT using six standard stars ( Table 2 ) in the observed field whose coordinates were taken from the catalogue UCAC4 ( Zacharias et al., 2013 ) and their magnitudes from the catalogue APASS DR9 ( Henden et al., 2016 )... Obviously, the reproducing of data required another geometry of the system. Its main peculiarity is the big increasing of eclipse depth during outburst. We qualitatively modelled the folded light curves at quiescence and outburst in order to explain the reason for increase of the primary luminosity about two hundred times. The light curve fits revealed that such an effect can be reproduced by a flat disc whose radius and temperature are several times bigger than those of the primary at quiescence. Stacking or accumulating camera frames is a well-known technique in astrophysics (see Berry and Burnell, 2005). The track-and-stack technique is an effective method to obtain long exposures from many short ones of faint deep-sky objects while tracking... There is also a color shift from faint green-yellow to pink with increasing boxcar width in Fig. 5 associated with change in color balance in the composite images, indicating that our technique is not conservative. The use of wavelets has become a popular method to enhance details in images (Berry and Burnell, 2005). By interactively recombining wavelet transforms at different spatial scales and layers, small-scale features are enhanced and large-scale shading effects are reduced.. Video cascade accumulation of the total solar eclipse on Svalbard 2015 Article Full-text available Jan 2017 F. Sigernes Pal Gunnar Ellingsen Noora Partamies Shadia Habbal This work presents a novel image accumulation filter technique that reveals small-scale features and details from intense luminosity or high dynamic range (HDR) video recordings. The result of the filter is fused with a HDR image of the corona and the Solar Dynamic Observatory (SDO) image of the solar disk. The procedure is implemented in a function that takes in input the two times of flight, the geocentric positions vectors of the observer (R 1, R 2, R 3 ) and the topocentric direction cosine vector (? 1,? 2,? 3 ).. Image processing of multiclass satellite tracklets for initial orbit determination based on optical telescopes Thesis Apr 2018 Giovanni Lavezzi Satellites orbiting around the Earth are used for many purposes; they can be ofThe growth in space satelliteIn fact an in-orbit collision mayFor these reasons, mitigation strategies haveAwareness (SSA) program, able to provide Europe with timely and precise informationInside the SSA program, the Space Surveillance and. Tracking (SST) segment is targeted at tracking and maintaining the informationTo perform these observation tasks, nowadays, radar orThis thesis fits in the field of SSA and SST. In particular, the main goal isView Show abstract. In the determination of the separations and position angle the AIP4WIN program was used, whereas the IRAF package was also used, in addition to the determination of separations and position angle, to determine the magnitude difference between the components of the pairs.. CCD Measurements of Double and Multiple Stars at NAO Rozhen and ASV in 2015 Article Apr 2017 S. Boeva Z. Cvetkovic Rade Pavlovic Results of CCD observations of 154 double or multiple stars, made with the 2 m telescope of the Bulgarian National Astronomical Observatory at Rozhen over five nights in 2015, are presented. This is the ninth series of measurements of CCD frames obtained at Rozhen. We also present results of CCD observations of 323 double or multiple stars made with the 0.6 m telescope of the Serbian Astronomical Station on the mountain of Vidojevica over 23 nights in 2015. This is the fourth series of measurements of CCD frames obtained at this station. This paper contains the results for the position angle and angular separation for 801 pairs and residuals for 127 pairs with published orbital elements or linear solutions. The angular separations are in the range from 152 to 20156, with a median angular separation of 826. We also present eight pairs that are measured for the first time and linear elements for five pairs. The frames were combined into a single master bias, and dark and flat frames. The periods of these binaries are in the range of 0.26-0.43 d. The light curve solutions revealed that the components of each binary system are almost equal in temperature. The stellar components are of G and K spectral types and undergo total eclipses. The photometric data were reduced by AIP4WIN2.0 (Berry, Burnell 2006). As a result their initial epochs were determined. The target periods turned out almost equal to the previous values. Their stellar components seem to obey the relations mass-temperature of MS stars. They allowed the improvement of system ephemerides. The errors are formal 1-.All images were corrected for bias and flat-fielded in the standard way.. The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7-311525 Article Jan 2017 MON NOT R ASTRON SOC Vitaly V. Neustroev T. R. Marsh S. Zharikov J. P. Moore We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7-311525 during its unusual double superoutburst, the following decline and in quiescence. The colours then became bluer again, but it took at least 250 days to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 days after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess View Show abstract. C onsumer grade digital cameras have been applied for astronomical image processing, the analysis of cloud cover, photogrammetry, high dynamic range imaging, and luminance measurement ( Berry and Burnell 2006; Roy 2001; Hadwan 2002; Reinhard 2006). High-resolution luminance maps with a wide field of view (FOV) offer new opportunities for image based photometry, statistical image analysis, and derived lighting metrics, such as spherical illuminance distributions and glare.. Accuracy of Luminance Maps Obtained from High Dynamic Range Images Article Full-text available Jan 2006 Smita Anaokar Martin Moeck Abstract—High dynamic range (HDR) imaging offers the potential toTherefore, they may also be usedThe luminance maps obtained from HDRThe corresponding illuminanceThis allows a new wayThis paper explains how to properlyHarrisburg, Pennsylvania. Although the designs can be very attractive due to factors such as appearance and light redirection and rejection, very little is known about their daylighting performance and no daylight distribution data have been published. Monitoring these buildings would require multiple illuminance sensors or luminance calibrated CCD cameras (Andersen and others 2001; Berry and Burnell 2000). Measuring the bi-directional transmittance of these DODs in the laboratory is a major undertaking, and few software tools can manipulate the data (Apian-Bennewitz 1994;Breitenbach and Rosenfeld 1998;Mitanchey and others 1995;Murray-Coleman and Smith 1990;Papamichael and others 1988).. Modeling Intensity Distributions of Advanced Daylight Systems Surrounded by Arbitrary Luminance Maps Article Full-text available Jul 2005 Youn Ju Yoon Martin Moeck Abstract—For more than a decade, daylighting optical devices (DOD)Some of these systems show considerableHowever, their daylight performance is not clearlyThe first is the generation of aThe second problem is theWe shows how toResults of testsVarious software packages haveView Show abstract. Also, the proper motions of many double or multiple stars are unreliable due to the short epoch span of Hipparcos observations, and van Leeuwen (2007) The main characteristics of CCD camera are: 1340x1300 pixels, the pixel size is 20x20 mkm, one pixel is 0 ??.258. The AIP4WIN image processing package (Berry and Burnell, 2002) was used. All frames were reduced individually.. CCD MEASUREMENTS IN OPTICAL DOMAIN AND ASTROMETRIC POSITIONS OF ICRF2 RADIO SOURCES Conference Paper Full-text available Jan 2011 Ivana Milic Zitnik At the IAU XXIIIth GA in 1997, the International Celestial Reference Frame (ICRF) was adopted; hereafter referred to as ICRF1. After the original list of radio objects there were two extensions, ICRF-ext1 and ICRF-ext2. All together, there were 717 sources: 212 defining ones, 109 new ones, 294 candidate ones, and 102 additional ones. At the IAU XXVIIth GA in 2009, the second realization of the ICRF (the ICRF2) was adopted with the list of precise positions for 3414 compact radio astronomical sources. At that moment there were nearly 30 years of VLBI observations. The ICRF2 has a noise floor of about 0.04 mas (near six times better than ICRF1) and an axis stability of about 0.01 mas (nearly twice as stable as ICRF1). Also, it is of importance to make the observations of some ICRF2 extragalactic radio sources (ERS) which are visible in the optical domain, and to compare their optical (calculated via the reference stars) and radio positions (VLBI ones). About 30 frames were observed at the end of March 2011. The main steps of our calculations and some preliminary results (comparison between the measured optical positions and the radio ones) for a few ERS from ICRF2 list were presented here. 1. CALCULATION AND RESULTS Regular maintenance of the system and improvement of the frame is necessary. The ERS coordinates are continuously improving via VLBI observations (a large number of observations of defining ERS over a long data span). The frame's stability is based upon the assumption that there is no global rotation of the universe. The ERS positions are known to better than 1 mas, and the ultimate accuracy is limited because of the structure instability of ERS in radio wavelengths. From 1 January 2010, the realization of the ICRS is the ICRF2. That accuracy degrades over time because of the error in proper motions of stars, and it is necessary to verify and refine the relation between the HCRF and the ICRF2. It can be done via different telescopes and methods. The position of objects in the frames were measured by using the AIP4WIN software (Berry and Burnell 2002).. Professional paper FOCAL LENGTH DETERMINATION FOR THE 60 cm TELESCOPE AT ASTRONOMICAL STATION VIDOJEVICA Article Full-text available Jan 2012 Z. Cvetkovic G. Damljanovic Rade Pavlovic Milan Stojanovic View. Thereby, the removal of Poisson noise is of fundamental importance especially for further processing, such as image segmentation and recognition.. Poisson Noise Reduction with Higher-Order Natural Image Prior Model Article Full-text available Sep 2016 Wensen Feng Hong Qiao Yunjin Chen Poisson denoising is an essential issue for various imaging applications, such as night vision, medical imaging and microscopy. State-of-the-art approaches are clearly dominated by patch-based non-local methods in recent years. In this paper, we aim to propose a local Poisson denoising model with both structure simplicity and good performance. To this end, we consider a variational modeling to integrate the so-called Fields of Experts (FoE) image prior, that has proven an effective higher-order Markov Random Fields (MRF) model for many classic image restoration problems. We exploit several feasible variational variants for this task. We start with a direct modeling in the original image domain by taking into account the Poisson noise statistics, which performs generally well for the cases of high SNR. However, this strategy encounters problem in cases of low SNR. Then we turn to an alternative modeling strategy by using the Anscombe transform and Gaussian statistics derived data term. We retrain the FoE prior model directly in the transform domain. With the newly trained FoE model, we end up with a local variational model providing strongly competitive results against state-of-the-art non-local approaches, meanwhile bearing the property of simple structure. Furthermore, our proposed model comes along with an additional advantage, that the inference is very efficient as it is well-suited for parallel computation on GPUs. We created these images by subtracting a median lunar image based on the 5 frames before and 5 frames after the event. Optimal apertures corresponding to the maximum in the signal-to-noise of the flux measurement were used for the flashes to avoid adding noise from the subtracted background, while large apertures were used for the standards.. NELIOTA: First temperature measurement of lunar impact flashes Article Full-text available Oct 2017 ASTRON ASTROPHYS C. Avdellidou A. Maroussis A. Z. Bonanos Alexios Liakos We report the first scientific results from the NELIOTA (NEO Lunar Impacts and Optical TrAnsients) project, which has recently begun lunar monitoring observations with the 1.2-m Kryoneri telescope.
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