2 AOI Metadata Tag Descriptions 9 2.1 Tag Formats 9 2.2 Levels of Requirement 9 3 Example Metadata 11 4 Metadata Definitions 14 4.1 Version Metadata 14 1
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Plasma Physics and Pulsars
Plasma Physics and Pulsars On the evolution of compact o bjects and plasma physics in weak and strong gravitational and electromagnetic fields by Anouk Ehreiser supervised by Axel Jessner, Maria Massi and Li Kejia as part of an internship at the Max Planck Institute for Radioastronomy, Bonn March 2010 2 This composition was written as part of two internships at the Max Planck Institute for Radioastronomy in April 2009 at the Radiotelescope in Effelsberg and in February/March 2010 at the Institute in Bonn. I am very grateful for the support, expertise and patience of Axel Jessner, Maria Massi and Li Kejia, who supervised my internship and introduced me to the basic concepts and the current research in the field. Contents I. Life-cycle of stars 1. Formation and inner structure 2. Gravitational collapse and supernova 3. Star remnants II. Properties of Compact Objects 1. White Dwarfs 2. Neutron Stars 3. Black Holes 4. Hypothetical Quark Stars 5. Relativistic Effects III. Plasma Physics 1. Essentials 2. Single Particle Motion in a magnetic field 3. Interaction of plasma flows with magnetic fields – the aurora as an example IV. Pulsars 1. The Discovery of Pulsars 2. Basic Features of Pulsar Signals 3. Theoretical models for the Pulsar Magnetosphere and Emission Mechanism 4. Towards a Dynamical Model of Pulsar Electrodynamics References 3 Plasma Physics and Pulsars I. The life-cycle of stars 1. Formation and inner structure Stars are formed in molecular clouds in the interstellar medium, which consist mostly of molecular hydrogen (primordial elements made a few minutes after the beginning of the universe) and dust. -
Panstamps Documentation Release V0.5.3
panstamps Documentation Release v0.5.3 Dave Young 2020 Getting Started 1 Installation 3 1.1 Troubleshooting on Mac OSX......................................3 1.2 Development...............................................3 1.2.1 Sublime Snippets........................................4 1.3 Issues...................................................4 2 Command-Line Usage 5 3 Documentation 7 4 Command-Line Tutorial 9 4.1 Command-Line..............................................9 4.1.1 JPEGS.............................................. 12 4.1.2 Temporal Constraints (Useful for Moving Objects)...................... 17 4.2 Importing to Your Own Python Script.................................. 18 5 Installation 19 5.1 Troubleshooting on Mac OSX...................................... 19 5.2 Development............................................... 19 5.2.1 Sublime Snippets........................................ 20 5.3 Issues................................................... 20 6 Command-Line Usage 21 7 Documentation 23 8 Command-Line Tutorial 25 8.1 Command-Line.............................................. 25 8.1.1 JPEGS.............................................. 28 8.1.2 Temporal Constraints (Useful for Moving Objects)...................... 33 8.2 Importing to Your Own Python Script.................................. 34 8.2.1 Subpackages.......................................... 35 8.2.1.1 panstamps.commonutils (subpackage)........................ 35 8.2.1.2 panstamps.image (subpackage)............................ 35 8.2.2 Classes............................................ -
Making Color Images with the GIMP Las Cumbres Observatory Global Telescope Network Color Imaging: the GIMP Introduction
Las Cumbres Observatory Global Telescope Network Making Color Images with The GIMP Las Cumbres Observatory Global Telescope Network Color Imaging: The GIMP Introduction These instructions will explain how to use The GIMP to take those three images and composite them to make a color image. Users will also learn how to deal with minor imperfections in their images. Note: The GIMP cannot handle FITS files effectively, so to produce a color image, users will have needed to process FITS files and saved them as grayscale TIFF or JPEG files as outlined in the Basic Imaging section. Separately filtered FITS files are available for you to use on the Color Imaging page. The GIMP can be downloaded for Windows, Mac, and Linux from: www.gimp.org Loading Images Loading TIFF/JPEG Files Users will be processing three separate images to make the RGB color images. When opening files in The GIMP, you can select multiple files at once by holding the Ctrl button and clicking on the TIFF or JPEG files you wish to use to make a color image. Go to File > Open. Image Mode RGB Mode Because these images are saved as grayscale, all three images need to be converted to RGB. This is because color images are made from (R)ed, (G)reen, and (B)lue picture elements (pixels). The different shades of gray in the image show the intensity of light in each of the wavelengths through the red, green, and blue filters. The colors themselves are not recorded in the image. Adding Color Information For the moment, these images are just grayscale. -
A Joint Chandra and Swift View of the 2015 X-Ray Dust Scattering Echo of V404 Cygni S
Draft version July 20, 2021 Preprint typeset using LATEX style emulateapj v. 5/2/11 A JOINT CHANDRA AND SWIFT VIEW OF THE 2015 X-RAY DUST SCATTERING ECHO OF V404 CYGNI S. Heinz1, L. Corrales2, R. Smith3, W.N. Brandt4,5,6, P.G. Jonker7,8, R.M. Plotkin9,10, and J. Neilsen2,11 Draft version July 20, 2021 Abstract We present a combined analysis of the Chandra and Swift observations of the 2015 X-ray echo of V404 Cygni. Using stacking analysis, we identify eight separate rings in the echo. We reconstruct the soft X-ray lightcurve of the June 2015 outburst using the high-resolution Chandra images and cross-correlations of the radial intensity profiles, indicating that about 70% of the outburst fluence occurred during the bright flare at the end of the outburst on MJD 57199.8. By deconvolving the intensity profiles with the reconstructed outburst lightcurve, we show that the rings correspond to eight separate dust concentrations with precise distance determinations. We further show that the column density of the clouds varies significantly across the field of view, with the centroid of most of the clouds shifted toward the Galactic plane, relative to the position of V404 Cyg, invalidating the assumption of uniform cloud column typically made in attempts to constrain dust properties from light echoes. We present a new XSPEC spectral dust scattering model that calculates the differential dust scattering cross section for a range of commonly used dust distributions and compositions and use it to jointly fit the entire set of Swift echo data. -
Arxiv:2002.01657V1 [Eess.IV] 5 Feb 2020 Port Lossless Model to Compress Images Lossless
LEARNED LOSSLESS IMAGE COMPRESSION WITH A HYPERPRIOR AND DISCRETIZED GAUSSIAN MIXTURE LIKELIHOODS Zhengxue Cheng, Heming Sun, Masaru Takeuchi, Jiro Katto Department of Computer Science and Communications Engineering, Waseda University, Tokyo, Japan. ABSTRACT effectively in [12, 13, 14]. Some methods decorrelate each Lossless image compression is an important task in the field channel of latent codes and apply deep residual learning to of multimedia communication. Traditional image codecs improve the performance as [15, 16, 17]. However, deep typically support lossless mode, such as WebP, JPEG2000, learning based lossless compression has rarely discussed. FLIF. Recently, deep learning based approaches have started One related work is L3C [18] to propose a hierarchical archi- to show the potential at this point. HyperPrior is an effective tecture with 3 scales to compress images lossless. technique proposed for lossy image compression. This paper In this paper, we propose a learned lossless image com- generalizes the hyperprior from lossy model to lossless com- pression using a hyperprior and discretized Gaussian mixture pression, and proposes a L2-norm term into the loss function likelihoods. Our contributions mainly consist of two aspects. to speed up training procedure. Besides, this paper also in- First, we generalize the hyperprior from lossy model to loss- vestigated different parameterized models for latent codes, less compression model, and propose a loss function with L2- and propose to use Gaussian mixture likelihoods to achieve norm for lossless compression to speed up training. Second, adaptive and flexible context models. Experimental results we investigate four parameterized distributions and propose validate our method can outperform existing deep learning to use Gaussian mixture likelihoods for the context model. -
Image Formats
Image Formats Ioannis Rekleitis Many different file formats • JPEG/JFIF • Exif • JPEG 2000 • BMP • GIF • WebP • PNG • HDR raster formats • TIFF • HEIF • PPM, PGM, PBM, • BAT and PNM • BPG CSCE 590: Introduction to Image Processing https://en.wikipedia.org/wiki/Image_file_formats 2 Many different file formats • JPEG/JFIF (Joint Photographic Experts Group) is a lossy compression method; JPEG- compressed images are usually stored in the JFIF (JPEG File Interchange Format) >ile format. The JPEG/JFIF >ilename extension is JPG or JPEG. Nearly every digital camera can save images in the JPEG/JFIF format, which supports eight-bit grayscale images and 24-bit color images (eight bits each for red, green, and blue). JPEG applies lossy compression to images, which can result in a signi>icant reduction of the >ile size. Applications can determine the degree of compression to apply, and the amount of compression affects the visual quality of the result. When not too great, the compression does not noticeably affect or detract from the image's quality, but JPEG iles suffer generational degradation when repeatedly edited and saved. (JPEG also provides lossless image storage, but the lossless version is not widely supported.) • JPEG 2000 is a compression standard enabling both lossless and lossy storage. The compression methods used are different from the ones in standard JFIF/JPEG; they improve quality and compression ratios, but also require more computational power to process. JPEG 2000 also adds features that are missing in JPEG. It is not nearly as common as JPEG, but it is used currently in professional movie editing and distribution (some digital cinemas, for example, use JPEG 2000 for individual movie frames). -
IAU Division C Working Group on Star Names 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
THEORY of NAMES and COGNITIVE LINGUISTICS – the CASE of the METAPHOR Nikola Dobri Ć Alpen-Adria Universität Klagenfurt
31 This is a contribution from Filozofija i društvo , Vol. 21, No. 1, pp. 31-41, 2010 © 2010 Institute for Philosophy and Social Theory of the University of Belgrade This electronic file may not be altered or reproduced in any way. ________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________ THEORY OF NAMES AND COGNITIVE LINGUISTICS – THE CASE OF THE METAPHOR Nikola Dobri ć Alpen-Adria Universität Klagenfurt Abstract: The philosophical and, in a lesser degree, linguistic debate about the notion of names has been raging for a long time. The processes behind naming are presented and explained in various ways. This paper will try to give a new insight into the motivation behind the creation of new names as seen from the linguistics viewpoint. Metaphor, as one of the major sources of motivation from the perspective of cognitive linguistics, is the basic form of human conceptualization. The first part of the paper presents the current theories about names. The second part describes the basic principles of cognitive linguistics as related to metaphors. The third part deals with providing the evidence regarding metaphor involvement in original creation of people’s names, while -
Public Naming of Exoplanets and Their Stars: Implementation and Outcomes of the IAU100
Public Naming of Exoplanets and Their Stars: Implementation and Outcomes of the IAU100 Best Practice Best NameExoWorlds Global Project Eric Mamajek Debra Meloy Elmegreen Alain Lecavelier des Etangs Jet Propulsion Laboratory, California Vassar College Institut d’Astrophysique de Paris Institute of Technology [email protected] [email protected] [email protected] Eduardo Monfardini Penteado Lars Lindberg Christensen [email protected] NSF’s NOIRLab [email protected] Gareth Williams [email protected] Hitoshi Yamaoka National Astronomical Observatory of Guillem Anglada-Escudé Japan (NAOJ) Institute for Space Science (ICE/CSIC), [email protected] Queen Mary University of London Keywords [email protected] exoplanets, IAU nomenclature The IAU100 NameExoWorlds public naming campaign was a core project during the International Astronomical Union’s 100th anniversary (IAU100) in 2019, giving the opportunity to everyone, everywhere, to propose official names for exoplanets and their host stars. With IAU100 NameExoWorlds the IAU encouraged all peoples of Earth to consider themselves as “Citizens of the Universe”, united “under one sky”. The 113 national campaigns involved hundreds of thousands of people in a global effort to bring the public closer to science by allowing them to participate in the process of naming stars and planets, and learning more about astronomy in the process. The campaign resulted in nearly 425 000 votes, and 113 new IAU-recognised proper names for exoplanets and 113 new names for their stars. The IAU now officially recognises the chosen proper names in addition to their previous scientific designations, and they appear in popular databases. Introduction wished to contribute to the fraternity of all through international cooperation, the IAU people with a significant token of global is the authority responsible for assigning Over the past three decades, astronomers identity. -
Frequently Asked Questions
Frequently Asked Questions After more than 16 years of business, we’ve run into a lot of questions from a lot of different people, each with different needs and requirements. Sometimes the questions are about our company or about the exact nature of dynamic imaging, but, no matter the question, we’re happy to answer and discuss any imaging solutions that may help the success of your business. So take a look... we may have already answered your question. If we haven’t, please feel free to contact us at www.liquidpixels.com. How long has LiquidPixels been in business? Do you have an API? LiquidPixels started in 2000 and has been going strong since LiquiFire OS uses our easy-to-learn LiquiFire® Image Chains to then, bringing dynamic imaging to the world of e-commerce. describe the imaging manipulations you wish to produce. Can you point me to live websites that use your services? What is the average time required to implement LiquiFire OS LiquidPixels’ website features some of our customers who into my environment? benefit from the LiquiFire® Operating System (OS). Our Whether you choose our turnkey LiquiFire Imaging Server™ sales team will be happy to showcase existing LiquiFire OS solutions or our LiquiFire Hosted Service™, LiquiFire OS can solutions or show you how incredible your website and be implemented in less than a day. Then your creative team can product imagery would look with the power of LiquiFire OS get to the exciting part: developing your website’s interface, behind it. presentation, and workflow. What types of images are required (file format, quality, etc.)? LiquiFire OS supports all common image formats, including JPEG, PNG, TIFF, WebP, JXR, and GIF and also allows for PostScript and PDF manipulation. -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
3 Star and Planet Formation
3 Star and planet formation Part I: Star formation Abstract: All galaxies with a significant mass fraction of molecular gas show continuous formation of new stars. To form stars out of molecular clouds the physical properties of the gas have to change dramatically. Star formation is therefore all about: Initiating the collapse (Jeans criterion, demagnetization by ambipolar diffusion, external triggering) Compression of the gas by self-gravity Losing angular momentum (magnetic braking and fragmentation) 3.1 Criteria for gravitational collapse The basic idea to cause a molecular cloud to collapse due to its own gravity is to just make it massive enough, but the details are quite tricky. We look first at the Jeans criterion that gives the order of magnitude mass necessary for gravitational collapse. Then we consider the influence of a magnetic field before we discuss mechanisms for triggering a collapse by external forces. Jeans criterion (Sir James Jeans, 1877–1946): Let us consider the Virial theorem 20EEkin pot It describes the (time-averaged) state of a stable, gravitationally bound (and ergodic) system. Collins (1978) wrote a wonderful book on the Virial theorem including its derivation and applications in astrophysics, which has also been made available online (http://ads.harvard.edu/books/1978vtsa.book/). The Virial theorem applies to a variety of astrophysical objects including self-gravitating gas clouds, stars, planetary systems, stars in galaxies, and clusters of galaxies. Basically it describes the equilibrium situation of a gas for which pressure and gravitational forces are in balance. Depending on the values of kinetic and potential energies the following behavior results: Astrobiology: 3 Star and planet formation S.V.