ASTR110G Astronomy Laboratory Exercises C the GEAS Project 2020
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Using Concrete Scales: a Practical Framework for Effective Visual Depiction of Complex Measures Fanny Chevalier, Romain Vuillemot, Guia Gali
Using Concrete Scales: A Practical Framework for Effective Visual Depiction of Complex Measures Fanny Chevalier, Romain Vuillemot, Guia Gali To cite this version: Fanny Chevalier, Romain Vuillemot, Guia Gali. Using Concrete Scales: A Practical Framework for Effective Visual Depiction of Complex Measures. IEEE Transactions on Visualization and Computer Graphics, Institute of Electrical and Electronics Engineers, 2013, 19 (12), pp.2426-2435. 10.1109/TVCG.2013.210. hal-00851733v1 HAL Id: hal-00851733 https://hal.inria.fr/hal-00851733v1 Submitted on 8 Jan 2014 (v1), last revised 8 Jan 2014 (v2) HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Using Concrete Scales: A Practical Framework for Effective Visual Depiction of Complex Measures Fanny Chevalier, Romain Vuillemot, and Guia Gali a b c Fig. 1. Illustrates popular representations of complex measures: (a) US Debt (Oto Godfrey, Demonocracy.info, 2011) explains the gravity of a 115 trillion dollar debt by progressively stacking 100 dollar bills next to familiar objects like an average-sized human, sports fields, or iconic New York city buildings [15] (b) Sugar stacks (adapted from SugarStacks.com) compares caloric counts contained in various foods and drinks using sugar cubes [32] and (c) How much water is on Earth? (Jack Cook, Woods Hole Oceanographic Institution and Howard Perlman, USGS, 2010) shows the volume of oceans and rivers as spheres whose sizes can be compared to that of Earth [38]. -
Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
Detection of PAH and Far-Infrared Emission from the Cosmic Eye
Accepted for publication in ApJ A Preprint typeset using LTEX style emulateapj v. 08/22/09 DETECTION OF PAH AND FAR-INFRARED EMISSION FROM THE COSMIC EYE: PROBING THE DUST AND STAR FORMATION OF LYMAN BREAK GALAXIES B. Siana1, Ian Smail2, A. M. Swinbank2, J. Richard2, H. I. Teplitz3, K. E. K. Coppin2, R. S. Ellis1, D. P. Stark4, J.-P. Kneib5, A. C. Edge2 Accepted for publication in ApJ ABSTRACT ∗ We report the results of a Spitzer infrared study of the Cosmic Eye, a strongly lensed, LUV Lyman Break Galaxy (LBG) at z =3.074. We obtained Spitzer IRS spectroscopy as well as MIPS 24 and 70 µm photometry. The Eye is detected with high significance at both 24 and 70 µm and, when including +4.7 11 a flux limit at 3.5 mm, we estimate an infrared luminosity of LIR = 8.3−4.4 × 10 L⊙ assuming a magnification of 28±3. This LIR is eight times lower than that predicted from the rest-frame UV properties assuming a Calzetti reddening law. This has also been observed in other young LBGs, and indicates that the dust reddening law may be steeper in these galaxies. The mid-IR spectrum shows strong PAH emission at 6.2 and 7.7 µm, with equivalent widths near the maximum values observed in star-forming galaxies at any redshift. The LP AH -to-LIR ratio lies close to the relation measured in local starbursts. Therefore, LP AH or LMIR may be used to estimate LIR and thus, star formation rate, of LBGs, whose fluxes at longer wavelengths are typically below current confusion limits. -
Close-Up View of a Luminous Star-Forming Galaxy at Z = 2.95 S
Close-up view of a luminous star-forming galaxy at z = 2.95 S. Berta, A. J. Young, P. Cox, R. Neri, B. M. Jones, A. J. Baker, A. Omont, L. Dunne, A. Carnero Rosell, L. Marchetti, et al. To cite this version: S. Berta, A. J. Young, P. Cox, R. Neri, B. M. Jones, et al.. Close-up view of a luminous star- forming galaxy at z = 2.95. Astronomy and Astrophysics - A&A, EDP Sciences, 2021, 646, pp.A122. 10.1051/0004-6361/202039743. hal-03147428 HAL Id: hal-03147428 https://hal.archives-ouvertes.fr/hal-03147428 Submitted on 19 Feb 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 646, A122 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039743 & c S. Berta et al. 2021 Astrophysics Close-up view of a luminous star-forming galaxy at z = 2.95? S. Berta1, A. J. Young2, P. Cox3, R. Neri1, B. M. Jones4, A. J. Baker2, A. Omont3, L. Dunne5, A. Carnero Rosell6,7, L. Marchetti8,9,10 , M. Negrello5, C. Yang11, D. A. Riechers12,13, H. Dannerbauer6,7, I. -
Ast110fall2015-Labmanual.Pdf
2015/2016 (http://astronomy.nmsu.edu/astro/Ast110Fall2015.pdf) 1 2 Contents 1IntroductiontotheAstronomy110Labs 5 2TheOriginoftheSeasons 21 3TheSurfaceoftheMoon 41 4ShapingSurfacesintheSolarSystem:TheImpactsofCometsand Asteroids 55 5IntroductiontotheGeologyoftheTerrestrialPlanets 69 6Kepler’sLawsandGravitation 87 7TheOrbitofMercury 107 8MeasuringDistancesUsingParallax 121 9Optics 135 10 The Power of Light: Understanding Spectroscopy 151 11 Our Sun 169 12 The Hertzsprung-Russell Diagram 187 3 13 Mapping the Galaxy 203 14 Galaxy Morphology 219 15 How Many Galaxies Are There in the Universe? 241 16 Hubble’s Law: Finding the Age of the Universe 255 17 World-Wide Web (Extra-credit/Make-up) Exercise 269 AFundamentalQuantities 271 BAccuracyandSignificantDigits 273 CUnitConversions 274 DUncertaintiesandErrors 276 4 Name: Lab 1 Introduction to the Astronomy 110 Labs 1.1 Introduction Astronomy is a physical science. Just like biology, chemistry, geology, and physics, as- tronomers collect data, analyze that data, attempt to understand the object/subject they are looking at, and submit their results for publication. Along thewayas- tronomers use all of the mathematical techniques and physics necessary to understand the objects they examine. Thus, just like any other science, a largenumberofmath- ematical tools and concepts are needed to perform astronomical research. In today’s introductory lab, you will review and learn some of the most basic concepts neces- sary to enable you to successfully complete the various laboratory exercises you will encounter later this semester. When needed, the weekly laboratory exercise you are performing will refer back to the examples in this introduction—so keep the worked examples you will do today with you at all times during the semester to use as a refer- ence when you run into these exercises later this semester (in fact, on some occasions your TA might have you redo one of the sections of this lab for review purposes). -
12 Strong Gravitational Lenses
12 Strong Gravitational Lenses Phil Marshall, MaruˇsaBradaˇc,George Chartas, Gregory Dobler, Ard´ısEl´ıasd´ottir,´ Emilio Falco, Chris Fassnacht, James Jee, Charles Keeton, Masamune Oguri, Anthony Tyson LSST will contain more strong gravitational lensing events than any other survey preceding it, and will monitor them all at a cadence of a few days to a few weeks. Concurrent space-based optical or perhaps ground-based surveys may provide higher resolution imaging: the biggest advances in strong lensing science made with LSST will be in those areas that benefit most from the large volume and the high accuracy, multi-filter time series. In this chapter we propose an array of science projects that fit this bill. We first provide a brief introduction to the basic physics of gravitational lensing, focusing on the formation of multiple images: the strong lensing regime. Further description of lensing phenomena will be provided as they arise throughout the chapter. We then make some predictions for the properties of samples of lenses of various kinds we can expect to discover with LSST: their numbers and distributions in redshift, image separation, and so on. This is important, since the principal step forward provided by LSST will be one of lens sample size, and the extent to which new lensing science projects will be enabled depends very much on the samples generated. From § 12.3 onwards we introduce the proposed LSST science projects. This is by no means an exhaustive list, but should serve as a good starting point for investigators looking to exploit the strong lensing phenomenon with LSST. -
Cosmos: a Spacetime Odyssey (2014) Episode Scripts Based On
Cosmos: A SpaceTime Odyssey (2014) Episode Scripts Based on Cosmos: A Personal Voyage by Carl Sagan, Ann Druyan & Steven Soter Directed by Brannon Braga, Bill Pope & Ann Druyan Presented by Neil deGrasse Tyson Composer(s) Alan Silvestri Country of origin United States Original language(s) English No. of episodes 13 (List of episodes) 1 - Standing Up in the Milky Way 2 - Some of the Things That Molecules Do 3 - When Knowledge Conquered Fear 4 - A Sky Full of Ghosts 5 - Hiding In The Light 6 - Deeper, Deeper, Deeper Still 7 - The Clean Room 8 - Sisters of the Sun 9 - The Lost Worlds of Planet Earth 10 - The Electric Boy 11 - The Immortals 12 - The World Set Free 13 - Unafraid Of The Dark 1 - Standing Up in the Milky Way The cosmos is all there is, or ever was, or ever will be. Come with me. A generation ago, the astronomer Carl Sagan stood here and launched hundreds of millions of us on a great adventure: the exploration of the universe revealed by science. It's time to get going again. We're about to begin a journey that will take us from the infinitesimal to the infinite, from the dawn of time to the distant future. We'll explore galaxies and suns and worlds, surf the gravity waves of space-time, encounter beings that live in fire and ice, explore the planets of stars that never die, discover atoms as massive as suns and universes smaller than atoms. Cosmos is also a story about us. It's the saga of how wandering bands of hunters and gatherers found their way to the stars, one adventure with many heroes. -
12.748 Lecture 2 Cosmic Abundances, Nucleosynthesis and Element Origins
12.748 Lecture 2 Cosmic Abundances, Nucleosynthesis and Element Origins Our intent is to shed further light on the reasons for the abundance of the elements. We made progress in this regard when we discussed nuclear stability and nuclear binding energy explaining the zigzag structure, along with the broad maxima around Iron and Lead. The overall decrease with mass, however, arises from the creation of the universe, and the fact that the universe started out with only the most primitive building blocks of matter, namely electrons, protons and neutrons. The initial explosion that created the universe created a rather bland mixture of just hydrogen, a little helium, and an even smaller amount of lithium. The other elements were built from successive generations of star formation and death. The Origin of the Universe It is generally accepted that the universe began with a bang, not a whimper, some 15 billion years ago. The two most convincing lines of evidence that this is the case are observation of • the Hubble expansion: objects are receding at a rate proportional to their distance • the cosmic microwave background (CMB): an almost perfectly isotropic black-body spectrum Isotopes 12.748 Lecture 2: Cosmic Abundances, Nucleosynthesis and Element Origins 1 In the initial fraction of a second, the temperature is so hot that even subatomic particles like neutrons, electrons and protons fall apart into their constituent pieces (quarks and gluons). These temperatures are well beyond anything achievable in the universe since. As the fireball expands, the temperature drops, and progressively higher-level particles are manufactured. By the end of the first second, the temperature has dropped to a mere billion degrees or so, and things are starting to get a little more normal: electrons, neutrons and protons can now exist. -
A Detailed Study of Gas and Star Formation in a Highly Magnified Lyman Break Galaxy at Z= 3.07
Draft version October 30, 2018 A Preprint typeset using L TEX style emulateapj v. 11/12/01 A DETAILED STUDY OF GAS AND STAR FORMATION IN A HIGHLY MAGNIFIED LYMAN BREAK GALAXY AT Z =3.07 K.E.K. Coppin1, A.M. Swinbank1, R. Neri2, P. Cox2, Ian Smail1, R. S. Ellis3, J. E. Geach1, B. Siana4, H. Teplitz4, S. Dye5, J.-P. Kneib6, A.C. Edge1, J. Richard3 Draft version October 30, 2018 ABSTRACT We report the detection of CO(3–2) emission from a bright, gravitationally lensed Lyman Break Galaxy, LBGJ213512.73–010143 (the “Cosmic Eye”), at z =3.07 using the Plateau de Bure Interferom- eter. This is only the second detection of molecular gas emission from an LBG and yields an intrinsic 9 molecular gas mass of (2.4 ± 0.4) × 10 M⊙. The lens reconstruction of the UV morphology of the LBG indicates that it comprises two components separated by ∼ 2 kpc. The CO emission is unresolved, ′′ θ <∼ 3 , and appears to be centered on the intrinsically fainter (and also less highly magnified) of the 9 2 two UV components. The width of the CO line indicates a dynamical mass of (8 ± 2) × 10 csc i M⊙ within the central 2 kpc. Employing mid-infrared observations from Spitzer we infer a stellar mass of 9 −1 M∗ ∼ (6 ± 2)×10 M⊙ and a star-formation rate of ∼ 60 M⊙ yr , indicating that the molecular gas will be consumed in <∼ 40 Myr. The gas fractions, star-formation efficiencies and line widths suggests that LBG J213512 is a high-redshift, gas-rich analog of a local luminous infrared galaxy. -
Moon Observing Certificate
[ American Lunar Society Lunar Study and Observing Certificate Program Cosponsored by the Moon Society This project was designed for those who want to move beyond the simple observing stages. In completing the Certificate, you will observe not just 'craters and maria', but also sinuous rilles and volcanoes, flooded craters and secondary craters, arcuate rilles and mare ridges. Further, you will come to understand just how these features formed, and what they tell us about the history of the moon. In short, this project will produce competent observers, who are qualified to teach others about the wonders of the moon. May you enjoy the learning and the hunt. Eric Douglass To earn the ALS Study and Observing Certificate one must complete the following steps: 1. Read the the article "Geologic Processes On The Moon" 2. Complete an 'open book' test based on this article This is not a difficult test; it is only designed to ensure that the article was read Passing score occurs at 80% correct answers. 3. Observe a list of objects listed below, and keep a log of what was seen. Only 90% of these objects need observed to complete this requirement. 4. Turn in your completed Moon Observing Log to the CFAS Observing Chairman. CFAS will submit your Log to the American Lunar Society. Observers Certificate - List of Objects to be Observed - Page 1 LOG: List of Objects on the Moon to be Observed Please include brief descriptions of what you see. Only 90% of objects (81 of 90) need be observed to meet this requirement. NOTE: a lunar atlas is necessary to find the objects in this list. -
Lunar Mare Volcanism in the Eastern Nearside Inferred from Clementine Uvvis Data
Lunar and Planetary Science XXXIII (2002) 1284.pdf LUNAR MARE VOLCANISM IN THE EASTERN NEARSIDE INFERRED FROM CLEMENTINE UVVIS DATA. S. Kodama and Y. Yamaguchi, Department of Earth and Planetary Sciences, Nagoya University, Nagoya, Japan, [email protected], [email protected]. Introduction: The lunar mare basalts cover about the central northern Serenitatis. Se5 is exposed in the 17% of the lunar surface, but occupy only about 1% of east and west margins. Ejecta and/or floors of Bessel the total volume of the lunar crust [1]. In spite of their crater and Deseilligny crater, both located in Se3, indi- small proportion, they play a very important roll for cate higher contents of TiO2 than Se3. These materials understanding lunar thermal evolution, because mare are probably mixtures of Se2 and Se3, and this fact basalts are the results of lunar volcanism which was suggests that Se2 is distributed in the whole mare and caused by thermal evolution of the lunar interior, and is covered by Se3 and Se4. Stratigraphy and chemistry their composition reflects distribution of their source of the mare basalts in this region suggest that the vol- region. Information about spatial and temporal changes canism migrated from south to north, and TiO2 content of mare volcanism allows us to constrain the composi- decreased with time. tional distribution of lunar interior and thermal evolu- Mare Tranquillitatis. Mare Tranquillitatis lies in tional history. Therefore, it is necessary to establish the center of the study area (center: 7N, 40E; diameter: local and regional stratigraphy of mare basalts. -
Recent Extensional Tectonics on the Moon Revealed by the Lunar Reconnaissance Orbiter Camera Thomas R
LETTERS PUBLISHED ONLINE: 19 FEBRUARY 2012 | DOI: 10.1038/NGEO1387 Recent extensional tectonics on the Moon revealed by the Lunar Reconnaissance Orbiter Camera Thomas R. Watters1*, Mark S. Robinson2, Maria E. Banks1, Thanh Tran2 and Brett W. Denevi3 Large-scale expressions of lunar tectonics—contractional of the Pasteur scarp (∼8:6◦ S, 100:6◦ E; Supplementary Fig. S1) are wrinkle ridges and extensional rilles or graben—are directly ∼1:2 km from the scarp face (Fig. 1b). Unlike the Madler graben, related to stresses induced by mare basalt-filled basins1,2. the orientation of the Pasteur graben are subparallel to the scarp and Basin-related extensional tectonic activity ceased about extend for ∼1:5 km, with the largest ∼300 m in length and 20–30 m 3.6 Gyr ago, whereas contractional tectonics continued until wide (Supplementary Note S3). about 1.2 Gyr ago2. In the lunar highlands, relatively young Lunar graben not located in the proximal back-limb terrain contractional lobate scarps, less than 1 Gyr in age, were first of lobate scarps have also been revealed in LROC NAC images. identified in Apollo-era photographs3. However, no evidence Graben found in the floor of Seares crater (∼74:7◦ N, 148:0◦ E; of extensional landforms was found beyond the influence of Supplementary Fig. S1) occur in the inter-scarp area of a cluster of mare basalt-filled basins and floor-fractured craters. Here seven lobate scarps (Fig. 1c). These graben are found over an area we identify previously undetected small-scale graben in the <1 km2 and have dimensions comparable to those in back-scarp farside highlands and in the mare basalts in images from the terrain, ∼150–250 m in length and with maximum widths of Lunar Reconnaissance Orbiter Camera.