Indigenous Use of Stellar Scintillation to Predict Weather and Seasonal Change
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High Precision Photometry of Transiting Exoplanets
McNair Scholars Research Journal Volume 3 Article 3 2016 High Precision Photometry of Transiting Exoplanets Maurice Wilson Embry-Riddle Aeronautical University and Harvard-Smithsonian Center for Astrophysics Jason Eastman Harvard-Smithsonian Center for Astrophysics John Johnson Harvard-Smithsonian Center for Astrophysics Follow this and additional works at: https://commons.erau.edu/mcnair Recommended Citation Wilson, Maurice; Eastman, Jason; and Johnson, John (2016) "High Precision Photometry of Transiting Exoplanets," McNair Scholars Research Journal: Vol. 3 , Article 3. Available at: https://commons.erau.edu/mcnair/vol3/iss1/3 This Article is brought to you for free and open access by the Journals at Scholarly Commons. It has been accepted for inclusion in McNair Scholars Research Journal by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Wilson et al.: High Precision Photometry of Transiting Exoplanets High Precision Photometry of Transiting Exoplanets Maurice Wilson1,2, Jason Eastman2, and John Johnson2 1Embry-Riddle Aeronautical University 2Harvard-Smithsonian Center for Astrophysics In order to increase the rate of finding, confirming, and characterizing Earth-like exoplanets, the MINiature Exoplanet Radial Velocity Array (MINERVA) was recently built with the purpose of obtaining the spectroscopic and photometric precision necessary for these tasks. Achieving the satisfactory photometric precision is the primary focus of this work. This is done with the four telescopes of MINERVA and the defocusing technique. The satisfactory photometric precision derives from the defocusing technique. The use of MINERVA’s four telescopes benefits the relative photometry that must be conducted. Typically, it is difficult to find satisfactory comparison stars within a telescope’s field of view when the primary target is very bright. -
Practical Observational Astronomy Photometry
Practical Observational Astronomy Lecture 5 Photometry Wojtek Pych Warszawa, October 2019 History ● Hipparchos 190 – 120 B.C. visible stars divided into 6 magnitudes ● John Hershel 1792- 1871 → Norman Robert Pogson A.D. 1829 - 1891 I m I 1 =100 m1−m2=−2.5 log( ) I m+5 I 2 Visual Observations ●Argelander method ●Cuneiform photometer ●Polarimetric photometer Visual Observations Copyright AAVSO The American Association of Variable Star Observers Photographic Plates Blink comparator Scanning Micro-Photodensitometer Photographic plates Liller, Martha H.; 1978IBVS.1527....1L Photoelectric Photometer ● Photomultiplier tubes – Single star measurement – Individual photons Photoelectric Photometer ● 1953 - Harold Lester Johnson - UBV system – telescope with aluminium covered mirrors, – detector is photomultiplier 1P21, – for V Corning 3384 filter is used, – for B Corning 5030 + Schott CG13 filters are used, – for U Corning 9863 filter is used. – Telescope at altitude of >2000 meters to allow the detection of sufficent amount of UV light. UBV System Extensions: R,I ● William Wilson Morgan ● Kron-Cousins CCD Types of photometry ● Aperture ● Profile ● Image subtraction Aperture Photometry Aperture Photometry Profile Photometry Profile Photometry DAOphot ● Find stars ● Aperture photometry ● Point Spread Function ● Profile photometry Image Subtraction Image Subtraction ● Construct a template image – Select a number of best quality images – Register all images into a selected astrometric position ● Find common stars ● Calculate astrometric transformation -
“Astrometry/Photometry of Solar System Objects After Gaia”
ISSN 1621-3823 ISBN 2-910015-77-7 NOTES SCIENTIFIQUES ET TECHNIQUES DE L’INSTITUT DE MÉCANIQUE CÉLESTE S106 Proceedings of the Workshop and colloquium held at the CIAS (Meudon) on October 14-18, 2015 “Astrometry/photometry of Solar System objects after Gaia” Institut de mécanique céleste et de calcul des éphémérides CNRS UMR 8028 / Observatoire de Paris 77, avenue Denfert-Rochereau 75014 Paris Mars 2017 Dépôt légal : Mars 2017 ISBN 2-910015-77-7 Foreword The modeling of the dynamics of the solar system needs astrometric observations made on a large interval of time to validate the scenarios of evolution of the system and to be able to provide ephemerides extrapolable in the next future. That is why observations are made regularly for most of the objects of the solar system. The arrival of the Gaia reference star catalogue will allow us to make astrometric reductions of observations with an increased accuracy thanks to new positions of stars and a more accurate proper motion. The challenge consists in increasing the astrometric accuracy of the reduction process. More, we should think about our campaigns of observations: due to this increased accuracy, for which objects, ground based observations will be necessary, completing space probes data? Which telescopes and targets for next astrometric observations? The workshop held in Meudon tried to answer these questions. Plans for the future have been exposed, results on former campaigns such as Phemu15 campaign, have been provided and amateur astronomers have been asked for continuing their participation to new observing campaigns of selected objects taking into account the new possibilities offered by the Gaia reference star catalogue. -
The PLATO Antarctic Site Testing Observatory
PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie The PLATO Antarctic site testing observatory J. S. Lawrence, G. R. Allen, M. C. B. Ashley, C. Bonner, S. Bradley, et al. J. S. Lawrence, G. R. Allen, M. C. B. Ashley, C. Bonner, S. Bradley, X. Cui, J. R. Everett, L. Feng, X. Gong, S. Hengst, J. Hu, Z. Jiang, C. A. Kulesa, Y. Li, D. Luong-Van, A. M. Moore, C. Pennypacker, W. Qin, R. Riddle, Z. Shang, J. W. V. Storey, B. Sun, N. Suntzeff, N. F. H. Tothill, T. Travouillon, C. K. Walker, L. Wang, J. Yan, J. Yang, H. Yang, D. York, X. Yuan, X. G. Zhang, Z. Zhang, X. Zhou, Z. Zhu, "The PLATO Antarctic site testing observatory," Proc. SPIE 7012, Ground-based and Airborne Telescopes II, 701227 (10 July 2008); doi: 10.1117/12.787166 Event: SPIE Astronomical Telescopes + Instrumentation, 2008, Marseille, France Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 7/12/2018 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use The PLATO Antarctic site testing observatory J.S. Lawrence*a, G.R. Allenb, M.C.B. Ashleya, C. Bonnera, S. Bradleyc, X. Cuid, J.R. Everetta, L. Fenge, X. Gongd, S. Hengsta, J.Huf, Z. Jiangf, C.A. Kulesag, Y. Lih, D. Luong-Vana, A.M. Moorei, C. Pennypackerj, W. Qinh, R. Riddlek, Z. Shangl, J.W.V. Storeya, B. Sunh, N. Suntzeffm, N.F.H. Tothilln, T. Travouilloni, C.K. Walkerg, L. Wange/m, J. Yane/f, J. Yange, H.Yangh, D. Yorko, X. Yuand, X.G. -
69-22,173 MARKOWITZ, Allan Henry, 1941- a STUDY of STARS
This dissertation has been microfilmed exactly u received 6 9 -2 2 ,1 7 3 MARKOWITZ, Allan Henry, 1941- A STUDY OF STARS EXHIBITING COM POSITE SPECTRA. The Ohio State University, Ph.D., 1969 A stron om y University Microfilms, Inc., Ann Arbor, Michigan A STUDY OF STARS EXHIBITING COMPOSITE SPECTRA DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Allan Henry Markowitz, A.B., M.Sc. ******** The Ohio S ta te U n iv e rsity 1969 Approved by UjiIjl- A dviser Department of Astronomy ACKNOWLEDGMENTS It is a sincere pleasure to thank my adviser, Professor Arne Slettebak, who originally suggested this problem and whose advice and encouragement were indispensable throughout the course of the research. I am also greatly indebted to Professor Philip Keenan for help in classifying certain late-type spectra and to Professor Terry Roark for instructing me in the operation of the Perkins Observatory telescope, I owe a special debt of gratitude to Dr. Carlos Jaschek of the La Plata Observatory for his inspiration, advice, and encourage ment. The Lowell Observatory was generous in providing extra telescope time when the need arose. I wish to particularly thank Dr. John Hall for this and for his interest. I also gratefully acknowledge the assistance of the Perkins Observatory staff. To my wife, Joan, I owe my profound thanks for her devotion and support during the seemingly unending tenure as a student. I am deeply grateful to my mother for her eternal confidence and to my in-laws for their encouragement. -
Nature Detectives
Winter 2015 Star Light, Star Bright, Let’s Find Some Stars Tonight! Finding specific stars in the night sky might seem overwhelming. All those stars! At a glance stars look like a million twinkling points of light that are impossible to sort out. But with a little information, you may discover hunting some stars is not so difficult. Turns out we don’t see a million stars. Less than a couple thousand – and usually many fewer than that – are visible to most people’s unaided eyes. The brightest and nearest stars are easily found without a telescope or binoculars. Stars Are Not Star-shaped Stars are big balls of gas that give off heat and light. Sound familiar? Isn’t that what our Sun does? Guess what, our Sun is a star. It seems confusing, but all stars are suns. Like our Sun, stars are also in the daytime sky. During the day, the Sun lights up the atmosphere so we can’t see other suns… er…stars. Pull Out and Save Our Sun isn’t even the brightest star. In fact all the stars we see at night are bigger and brighter than the Sun. It wins the brightness contest during the day simply because it is incredibly closer than all the other stars. (At night we don’t see the Sun because of Earth’s rotation. Our Sun is shining on the opposite side of Earth and we are in darkness.) Suns or Stars Appear to Rise and Set Our view of the stars changes through the night as Earth makes its daily rotation. -
Lecture Notes
1/17/2020 Topics in Observational astrophysics Ian Parry, Lent 2020 Lecture 1 • Electromagnetic radiation from the sky. • What is a telescope? What is an instrument? • Effects of the Earth’s atmosphere: transparency, seeing, refraction, dispersion, background light. • Basic definition of magnitudes. • Imperfections in imaging systems. Lecture notes • www.ast.cam.ac.uk/~irp/teaching • Username: topics • Password: dotzenblobs • Email me ([email protected]) so that I can put you on my course email list. 1 1/17/2020 Introduction • Observational astronomy is mostly about measuring electromagnetic radiation HERE (on Earth and nearby) and NOW. Astronomy is an evidence based science. • We measure the intensity, arrival direction, wavelength, arrival time and polarisation state. • Astronomical sources are so far away that the parts of the spherical wavefronts that are ultimately collected by the telescope aperture are essentially flat just before they enter the Earth’s atmosphere. • A telescope is a device that collects pieces of incoming wavefronts and focuses them, i.e. turns them into converging spherical wavefronts. • An instrument is a device that comes after the telescope. It receives the wavefronts and further processes them by either optically manipulating them or converting the energy into measurable signals, or both. Telescope Instrument Primary Optional Optional Detector optics and telescope instrument initial pupil optics optics 2 1/17/2020 Examples • The human eye can be thought of as a telescope (pupil + lens) and an instrument (retina). • Similarly the camera in a phone or a laptop can be thought of as a telescope (pupil + lens) and an instrument (cmos detector). • The lens of an SLR camera is the telescope and the camera body is the instrument. -
Atmosphere Observation by the Method of LED Sun Photometry
Atmosphere Observation by the Method of LED Sun Photometry A Senior Project presented to the Faculty of the Physics Department California Polytechnic State University, San Luis Obispo In Partial Fulfillment of the Requirements of the Degree Bachelor of Science by Gregory Garza April 2013 1 Introduction The focus of this project is centered on the subject of sun photometry. The goal of the experiment was to use a simple self constructed sun photometer to observe how attenuation coefficients change over longer periods of time as well as the determination of the solar extraterrestrial constants for particular wavelengths of light. This was achieved by measuring changes in sun radiance at a particular location for a few hours a day and then use of the Langley extrapolation method on the resulting sun radiance data set. Sun photometry itself is generally involved in the practice of measuring atmospheric aerosols and water vapor. Roughly a century ago, the Smithsonian Institutes Astrophysical Observatory developed a method of measuring solar radiance using spectrometers; however, these were not usable in a simple hand-held setting. In the 1950’s Frederick Volz developed the first hand-held sun photometer, which he improved until coming to the use of silicon photodiodes to produce a photocurrent. These early stages of the development of sun photometry began with the use of silicon photodiodes in conjunction with light filters to measure particular wavelengths of sunlight. However, this method of sun photometry came with cost issues as well as unreliability resulting from degradation and wear on photodiodes. A more cost effective method was devised by amateur scientist Forrest Mims in 1989 that incorporated the use of light emitting diodes, or LEDs, that are responsive only to the light wavelength that they emit. -
Indigenous Astronomies and Progress in Modern Astronomy
Indigenous Astronomies and Progress in Modern Astronomy Clive Ruggles1 School of Archaeology and Ancient History, University of Leicester University Road, LEICESTER LE1 7RH, U.K. E-mail: [email protected] From an anthropological point of view, the whole concept of a ‘path of progress’ in astronomical discovery is anathema, since it implicitly downgrades other cultural perspectives, such as the many ‘indigenous cosmologies’ that still exist in the modern world. By doing so, one risks provoking those who hold them and—as is most obvious in places such as Hawaii where the two ‘world-views’ come into direct contact—creating avoidable resistance to that very progress. The problem is complicated by the existence of ‘fringe’ and ‘new-age’ views that are increasingly confused with, and even passed off as, indigenous perceptions. In a modern world where widespread public perceptions include many that are unscientific in the broadest sense of the term, I shall argue that there are actually a range of positive benefits for progress in scientific astronomy to be derived from the mutual awareness and comprehension of ‘genuine’ cultural world-views whose goals—in common with those of modern science—are to make sense of the cosmos within which people live. While two-way education is clearly a prerequisite, I shall argue that the necessary level of reconciliation can only be achieved through more fundamental attempts by modern astronomers to understand, and ultimately to respect, both the non-Western frameworks of thought that give rise to other cultural perspectives and the heritage associated with them. One of the most obvious potential benefits could derive from common attitudes towards the natural heritage of astronomy, namely dark skies. -
Fireworks from Outer Space, a Gift from Betelgeuse Understanding the Life of an Iconic Star from Astronomers’ Recent Observations
Astronomy Fireworks from Outer Space, A Gift from Betelgeuse Understanding the Life of an Iconic Star From Astronomers’ Recent Observations Written by Sabrina Helck Illustrated by Mahamad Salah ave you ever looked up on a clear night and been fuses to carbon, carbon fuses to neon, and then neon to silicon. curious about the thousands of stars twinkling in the Finally, silicon fuses to iron. Once iron begins to form in that final sky? Well, maybe you do not think about it too much, step, the star's days are numbered. As fusion occurs, the center of H but all of those stars go through life cycles, and they are the star gets denser and denser. At this point, gravity takes over, each at different stages in their life. Sadly, an iconic star named and the star collapses in on itself. When this happens, it sets off an Betelgeuse seems to near the end of its life after astronomers explosion known as a supernova, and it looks spectacular. noticed it dimming. With the death of Betelgeuse comes an incredible celestial First, let us get to know Betelgeuse. Betelgeuse, performance, which is why the recent observations of Betelgeuse pronounced like the 1988 film, Beetlejuice, is the tenth brightest dimming are so exciting. It raises the possibility that the star may star in our night sky. It sits on the top left shoulder of the winter die soon and result in a supernova! Other astronomers speculate constellation, Orion. Although we can see Betelgeuse shining that the reason for its dimming was just a giant dust cloud, but let brightly in the sky, it is actually 642.5 light-years away, so about 385 us stick to the more exciting hypothesis. -
Astronomy 113 Laboratory Manual
UNIVERSITY OF WISCONSIN - MADISON Department of Astronomy Astronomy 113 Laboratory Manual Fall 2011 Professor: Snezana Stanimirovic 4514 Sterling Hall [email protected] TA: Natalie Gosnell 6283B Chamberlin Hall [email protected] 1 2 Contents Introduction 1 Celestial Rhythms: An Introduction to the Sky 2 The Moons of Jupiter 3 Telescopes 4 The Distances to the Stars 5 The Sun 6 Spectral Classification 7 The Universe circa 1900 8 The Expansion of the Universe 3 ASTRONOMY 113 Laboratory Introduction Astronomy 113 is a hands-on tour of the visible universe through computer simulated and experimental exploration. During the 14 lab sessions, we will encounter objects located in our own solar system, stars filling the Milky Way, and objects located much further away in the far reaches of space. Astronomy is an observational science, as opposed to most of the rest of physics, which is experimental in nature. Astronomers cannot create a star in the lab and study it, walk around it, change it, or explode it. Astronomers can only observe the sky as it is, and from their observations deduce models of the universe and its contents. They cannot ever repeat the same experiment twice with exactly the same parameters and conditions. Remember this as the universe is laid out before you in Astronomy 113 – the story always begins with only points of light in the sky. From this perspective, our understanding of the universe is truly one of the greatest intellectual challenges and achievements of mankind. The exploration of the universe is also a lot of fun, an experience that is largely missed sitting in a lecture hall or doing homework. -
ASTR 101 the Earth and the Sky August 29, 2018
ASTR 101 The Earth and the Sky August 29, 2018 • Sky and the atmosphere • Twinkling of stars • The celestial sphere • Constellations • Star brightness and the magnitude system • Naming of stars Scattering of light and color of the sky Sun light more less scattering scattering air particle • During the daytime we cannot see stars due to the glare in the atmosphere (from sunlight). • When sunlight travels through the Earth’s atmosphere some of the light is scattered (deflected) off air molecules. • White light is a combination of different colors, blue light is scattered far more than red light. Blue Sky during the day Sun Earth atmosphere • During the day we see this scattered sunlight in the atmosphere. • Since most of it is blue, a lot of blue light is seen in the atmosphere in all directions, which makes the sky look blue. • Light from stars are fainter than scattered sunlight in the atmosphere, so we cannot see them (unless a star happen to be very bright) In the outer space sky is always dark • Away from the atmosphere (in outer space, on moon…) sky is always dark. • It is possible to see stars and the sun at the same time. The Sun looks red at Sunrise/Sunset Sun atmosphere Earth • At sunrise and sunset, Sun is close to the horizon. Sunlight has to travel a longer distance in the atmosphere to reach us. • By the time sunlight reaches ground most of the blue light has scattered off. Only red light remains. • So the Sun (moon…) looks red at sunrise or sunset.