The VRO: How Astronomy's Biggest Dataset Will Change Your Universe

Total Page：16

File Type：pdf, Size：1020Kb

The VRO: How Astronomy’s Biggest Dataset Will Change Your Universe Prof. Eric Morganson National Center for Supercomputing Applications University of Illinois July 20, 2020 The Name Thing Formerly: telescope and data were LSST (the Large Synoptic Survey Telescope) Telescope: Vera Rubin Observatory Data: LSST (Legacy Survey of Space and Time) Vera Rubin measured galaxy masses and discovered strong evidence for dark matter Outline How optical astronomy works How the Vera Rubin Observatory changes the game What we will learn How you can see the data How optical astronomy works Optical Surveys Are Big Maps Map by Pan-STARRS, a telescope with a 1.8 meter mirror Get Better Data with a Bigger Telescope SDSS, a 2.5 meter telescope (cheap) Subaru, an 8.1 meter telescope (expensive) Get Better Data with a Bigger Telescope Get Many Observations (A “Light Curve”) Get Different Observations (Radio, X-Ray, Spectra) Left: The ALMA Radio Array Top Right: The Chandra X-Ray Telescope Bottom Right: An optical Spectrum How the VRO changes the game Big Telescopes Have Small Fields of View ● Sky: 40,000 square degrees ● Moon: 0.2 square degrees ● Large telescopes: ~0.01 square degree ● ~4 million images to cover the sky ○ 12 Years Most 8-10 m telescopes image the red circle How VRO is Different ● Sky: 40,000 square degrees ● Moon: 0.2 square degrees ● VRO images: 9.6 square degrees ● 4,300 images to cover the sky ○ 5 nights Most 8-10 m telescopes image the red circle Legacy Survey of Space and Time ● 10 Year Survey ○ Starting 2023 ● Images very deep ○ 100x deeper than previous surveys ● Southern Sky 1000 times ○ Gets color information ○ Get light curve Why Didn’t We Do This Years Ago? Large mirror: expensive Large field of view: more precise engineering Large Mirror with Large Field of View: super expensive Gigantic CCD camera: super expensive and maybe impossible before 2010 The Telescope The Camera (In Mac Units) ● World’s Largest ○ 6200 LBS ● 3200 Megapixel ○ 267 iPhones ● Each Image 6 GB ● 540 GB/hour ○ 1 MacBook Pro ● 10 TB / Day ○ 20 MacBook Pros ● 30 PB over Survey ○ 60 K MacBook Pros ● 10x bigger than all astronomical data currently taken What we will learn Cosmology: Expansion and Galaxy Clustering Milky Way: History of Collisions Left: simulated galaxy mergers create “streams” Right: actual streams around the Milky Way Find 90% Asteroid bigger than 140 Meters LSST “Alerts”: Stuff Exploding Left: star falling into black hole in a “Tidal Disruption Event” Right: Two Neutron stars spinning into a black hole How you can see the data Yearly Release ● LSST will release maps yearly (starting 2024) ● Same pixels researchers use ● Many surveys do this now ○ Dark Energy Survey ○ des.ncsa.illinois.edu/easyweb Public Alerts ● Users can receive custom alerts: ○ Image ○ Brightness ○ Location ● Alerts could be: ○ Every observation of an object ○ Every new supernova* ○ Every observation of an asteroid ● Available as: ○ Download ○ Email ○ Tweet/text/??? *LSST will find 1,000 new supernova per night A Whole New Zooniverse ● Zooniverse: classify objects from large datasets ● Multiple astronomy and non-astronomy projects ● Fun, easy, clicky, addictive ● Contributes to real discoveries ● Astronomy projects will soon be dominated by LSST data https://www.zooniverse.org/.

Copy Link

Recommended publications

David Kirkby University of California, Irvine, USA 4 August 2020 Expanding Universe
COSMOLOGY IN THE 2020S David Kirkby University of California, Irvine, USA 4 August 2020 Expanding Universe... 2 expansion history a(t |Ωm, ΩDE, …) 3 4 redshift 5 6 0.38Myr opaque universe last scatter 7 inflation opaque universe last scatter gravity waves? 8 CHIME SPT-3G DES 9 TCMB=2.7K, λ~2mm 10 CMB TCMB=2.7K, λ~2mm Galaxies 11 microwave projects: cosmic microwave background (primordial gravity waves, neutrinos, ...) CMB Galaxies optical & NIR projects: galaxy surveys (dark energy, neutrinos, ...) 12 CMB Galaxies telescope location: ground / above atmosphere 13 CMB Atacama desert, Chile CMB ground telescope location: Atacama desert / South Pole 14 Galaxies Galaxy survey instrument: spectrograph / imager 15 Dark Energy Spectroscopic Instrument (DESI) Vera Rubin Observatory 16 Dark Energy Spectroscopic Instrument (DESI) Vera Rubin Observatory 17 EXPANSION HISTORY VS STRUCTURE GROWTH Measurements of our cosmic expansion history constrain the parameters of an expanding homogenous universe: SN LSS , …) expansion historyDE m, Ω a(t |Ω CMB Small inhomogeneities are growing against this backdrop. Measurements of this structure growth provide complementary constraints. 18 Structure Growth 19 Redshift is not a perfect proxy for distance because of galaxy peculiar motions. Large-scale redshift-space distortions (RSD) trace large-scale matter fluctuations: signal! 20 Angles measured on the sky are also distorted by weak lensing (WL) as light is deflected by the same large-scale matter fluctuations: signal! Large-scale redshift-space distortions (RSD) trace large-scale matter fluctuations: signal! 21 CMB measures initial conditions of structure growth at z~1090: Temperature CMB photons also experience weak lensing! https://wiki.cosmos.esa.int/planck-legacy-archive/index.php/CMB_maps Polarization 22 CMB: INFLATION ERA SIGNATURES https://www.annualreviews.org/doi/abs/10.1146/annurev-astro-081915-023433 lensing E-modes lensing B-modes GW B-modes https://arxiv.org/abs/1907.04473 Lensing B modes already observed.
[Show full text]
A New Universe to Discover: a Guide to Careers in Astronomy
A New Universe to Discover A Guide to Careers in Astronomy Published by The American Astronomical Society What are Astronomy and Astrophysics? Ever since Galileo first turned his new-fangled one-inch “spyglass” on the moon in 1609, the popular image of the astronomer has been someone who peers through a telescope at the night sky. But astronomers virtually never put eye to lens these days. The main source of astronomical data is still photons (particles of light) from space, but the tools used to gather and analyze them are now so sophisticated that it’s no longer necessary (or even possible, in most cases) for a human eye to look through them. But for all the high-tech gadgetry, the 21st-Century astronomer is still trying to answer the same fundamental questions that puzzled Galileo: How does the universe work, and where did it come from? Webster’s dictionary defines “astronomy” as “the science that deals with the material universe beyond the earth’s atmosphere.” This definition is broad enough to include great theoretical physicists like Isaac Newton, Albert Einstein, and Stephen Hawking as well as astronomers like Copernicus, Johanes Kepler, Fred Hoyle, Edwin Hubble, Carl Sagan, Vera Rubin, and Margaret Burbidge. In fact, the words “astronomy” and “astrophysics” are pretty much interchangeable these days. Whatever you call them, astronomers seek the answers to many fascinating and fundamental questions. Among them: *Is there life beyond earth? *How did the sun and the planets form? *How old are the stars? *What exactly are dark matter and dark energy? *How did the Universe begin, and how will it end? Astronomy is a physical (non-biological) science, like physics and chemistry.
[Show full text]
What Happened Before the Big Bang?
Quarks and the Cosmos ICHEP Public Lecture II Seoul, Korea 10 July 2018 Michael S. Turner Kavli Institute for Cosmological Physics University of Chicago 100 years of General Relativity 90 years of Big Bang 50 years of Hot Big Bang 40 years of Quarks & Cosmos deep connections between the very big & the very small 100 years of QM & atoms 50 years of the “Standard Model” The Universe is very big (billions and billions of everything) and often beyond the reach of our minds and instruments Big ideas and powerful instruments have enabled revolutionary progress a very big idea connections between quarks & the cosmos big telescopes on the ground Hawaii Chile and in space: Hubble, Spitzer, Chandra, and Fermi at the South Pole basics of our Universe • 100 billion galaxies • each lit with the light of 100 billion stars • carried away from each other by expanding space from a • big bang beginning 14 billion yrs ago Hubble (1925): nebulae are “island Universes” Universe comprised of billions of galaxies Hubble Deep Field: one ten millionth of the sky, 10,000 galaxies 100 billion galaxies in the observable Universe Universe is expanding and had a beginning … Hubble, 1929 Signature of big bang beginning Einstein: Big Bang = explosion of space with galaxies carried along The big questions circa 1978 just two numbers: H0 and q0 Allan Sandage, Hubble’s “student” H0: expansion rate (slope age) q0: deceleration (“droopiness” destiny) … tens of astronomers working (alone) to figure it all out Microwave echo of the big bang Hot MichaelBig S Turner Bang
[Show full text]
Beyond Einstein
QuarksQuarks toto thethe Cosmos:Cosmos: the deep connections between the largest and smallest scales in the Universe ScalesScales ofof thethe UniverseUniverse LectureLecture SeriesSeries 16 November 2007 Michael S. Turner Kavli Institute for Cosmological Physics The UniversityMichael S Turner of Chicago Full Scale Model of Universe a Fraction of a Second After the Beginning Amazing as it is, the connections go far beyond the fact that it began as Quark Soup NB: No deep connections between quarks and chemistry even though are made of quarks! ••TheThe AtomsAtoms wewe andand thethe starsstars ofof mademade ofof ••TheThe DarkDark MatterMatter thatthat holdsholds thethe UniverseUniverse togethertogether ••TheThe DarkDark EnergyEnergy thatthat isis causingcausing thethe expansionexpansion ofof thethe UniverseUniverse toto speedspeed upup ••TheThe SeedsSeeds ofof allall structuresstructures (clusters,(clusters, galaxies,galaxies, stars,stars, ……)) TheThe UniverseUniverse isis gettinggetting biggerbigger –– expandingexpanding ExpandingExpanding UniverseUniverse isis expandingexpanding spacespace • Hubble’s law (correlation between velocity and distance) • Redshift of light • General relativity NoNo CenterCenter JustJust DifferentDifferent PerspectivesPerspectives EvidenceEvidence forfor HotHot BigBig BangBang • Expansion of Universe • Cosmic microwave background: microwave echo of big bang • Abundance of the elements H, D, He, Li • Consistent age: expansion age, oldest stars, age of radioactive elements, cooling of white dwarf stars, age of oldest
[Show full text]
Center for History of Physics Newsletter, Spring 2008
One Physics Ellipse, College Park, MD 20740-3843, CENTER FOR HISTORY OF PHYSICS NIELS BOHR LIBRARY & ARCHIVES Tel. 301-209-3165 Vol. XL, Number 1 Spring 2008 AAS Working Group Acts to Preserve Astronomical Heritage By Stephen McCluskey mong the physical sciences, astronomy has a long tradition A of constructing centers of teaching and research–in a word, observatories. The heritage of these centers survives in their physical structures and instruments; in the scientific data recorded in their observing logs, photographic plates, and instrumental records of various kinds; and more commonly in the published and unpublished records of astronomers and of the observatories at which they worked. These records have continuing value for both historical and scientific research. In January 2007 the American Astronomical Society (AAS) formed a working group to develop and disseminate procedures, criteria, and priorities for identifying, designating, and preserving structures, instruments, and records so that they will continue to be available for astronomical and historical research, for the teaching of astronomy, and for outreach to the general public. The scope of this charge is quite broad, encompassing astronomical structures ranging from archaeoastronomical sites to modern observatories; papers of individual astronomers, observatories and professional journals; observing records; and astronomical instruments themselves. Reflecting this wide scope, the members of the working group include historians of astronomy, practicing astronomers and observatory directors, and specialists Oak Ridge National Laboratory; Santa encounters tight security during in astronomical instruments, archives, and archaeology. a wartime visit to Oak Ridge. Many more images recently donated by the Digital Photo Archive, Department of Energy appear on page 13 and The first item on the working group’s agenda was to determine through out this newsletter.
[Show full text]
[Your Letterhead Here]
FOR IMMEDIATE RELEASE Dr. Bruce Elmegreen, of IBM Research, to receive the 2021 Bruce Gold Medal The Astronomical Society of the Pacific (ASP) is proud to announce the 2021 recipient of its most prestigious award, the Catherine Wolfe Bruce Gold Medal honoring Dr. Bruce Elmegreen, in recognition of his pioneering work on dynamical processes of star formation. SAN FRANCISCO, California – August 24, 2021 After four decades of innovative research, Dr. Elmegreen has fundamentally changed our understanding of star formation. He studied widespread hierarchical structure in young stellar regions, discovered that star formation is rapid following turbulent compression and gravitational collapse of these regions, explained the formation of stellar clusters, and discovered the largest scales for these processes in galaxies beyond our own, spanning a wide range of cosmic time. Elmegreen was born in Milwaukee, Wisconsin, and received a B.S. in Physics and Astronomy from the University of Wisconsin, Madison. He earned his PhD at Princeton University under the guidance of Lyman Spitzer, Jr. (Bruce Medal awardee, 1973), studying the ionization of the local interstellar medium. His interests turned to interstellar dynamics as a Junior Fellow at Harvard University, where, together with a colleague, he proposed that ionization from one generation of stars can compress residual gas and form another generation. He followed that with observations of interstellar filaments as further evidence for triggered collapse and proposed the same process on the scale of spiral arms. General observations and acceptance of these ideas would take several decades. After six years on the faculty of Columbia University in the City of New York, Elmegreen moved to IBM Research in 1984 where he began studies of galactic spirals, making the first digitized color images of galaxies and examining their symmetries to find spiral modes.
[Show full text]
Arxiv:2108.02207V1 [Astro-Ph.CO] 4 Aug 2021 Without Many Localised FRB Sources [26]
Cosmology with the moving lens effect Selim C. Hotinli,1 Kendrick M. Smith,2 Mathew S. Madhavacheril,2 and Marc Kamionkowski1 1Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA 2Perimeter Institute for Theoretical Physics, 31 Caroline St N, Waterloo, ON N2L 2Y5, Canada (Dated: August 6, 2021) Velocity fields can be reconstructed at cosmological scales from their influence on the correlation between the cosmic microwave background and large-scale structure. Effects that induce such corre- lations include the kinetic Sunyaev Zel'dovich (kSZ) effect and the moving-lens effect, both of which will be measured to high precision with upcoming cosmology experiments. Galaxy measurements also provide a window into measuring velocities from the effect of redshift-space distortions (RSDs). The information that can be accessed from the kSZ or RSDs, however, is limited by astrophysical uncertainties and systematic effects, which may significantly reduce our ability to constrain cosmo- logical parameters such as fσ8. In this paper, we show how the large-scale transverse-velocity field, which can be reconstructed from measurements of the moving-lens effect, can be used to measure fσ8 to high precision. I. INTRODUCTION rameter, defined such that brsd = 1 in the absence of anisotropic selection effects.1 Anisotropic selection Next generation cosmic microwave background (CMB) effects could significantly degrade measurements of experiments such as the Simons Observatory (SO) [1,2] f σ8 from future galaxy surveys, due to degeneracy and CMB-S4 [3], and galaxy surveys such as DESI [4] with brsd. In this paper, we propose a complementary and the Vera Rubin Observatory (VRO) [5] will gener- method for measuring f σ8 in which all degeneracies ate a wealth of new data with unprecedented precision with astrophysical bias parameters are broken.
[Show full text]
Blossoms Video Module Galaxies And
BLOSSOMS VIDEO MODULE GALAXIES AND DARK MATTER BY PETER FISHER So hello! My name is Peter Fisher. I’m a professor here at MIT and this is a Blossoms module on galaxies and dark matter. In the next hour we’re going to talk about what a galaxy is and a little bit about how it works. Then we’re going to talk about how, in order to understand how a galaxy works, we need to introduce a new form of matter which is called dark matter. Dark matter is one of the most pressing issues for physicists today because we really don’t have any idea what dark matter is. We’ll talk a little bit toward the end about dark matter’s properties but really the main message is that the shape of our galaxy is really determined by the presence of dark matter. Many of you probably know that galaxies are large collections of stars but we didn’t always know that. Around the turn of the century people looked at images like this one, which shows a cluster of actually 1,000 galaxies called the Coma Cluster and they saw that in contrast to the surrounding stars, galaxies were fuzzy, they were extended, whereas stars looked like little light points, and they were different colors. Astronomers referred to them at nebulae. The word comes from the Latin for fog or mist, so they were like these little blobs of mist. And it was some time before astronomers realized, about the turn of the century as I mentioned, that galaxies were really very large collections of stars.
[Show full text]
Carnegie Institution Carnegie
C68099_CVR.qxd:CVR 3/29/11 7:58 Page 1 2009-2010 CARNEGIE INSTITUTION FOR 2009-2010 SCIENCE YEAR BOOK 1530 P Street, N.W. Washington DC 20005 Phone: 202.387.6400 Carnegie Institution Fax: 202.387.8092 www.CarnegieScience.edu FOR SCIENCE CARNEGIE INSTITUTION FOR SCIENCE INSTITUTION FOR CARNEGIE YEAR BOOK The paper used in the manufacturing this year book contains 30% post-consumer recycled fiber. By using recycled fiber in place of virgin fiber, the Carnegie Institution preserved 41 trees, saved 126 pounds of waterborne waste, saved 18,504 gallons of water and prevented 4031 pounds of greenhouse gasses. The energy used to print the report was produced by wind power. Designed by Tina Taylor, T2 Design Printed by Monroe Litho ISSN 0069-066X C68099_CVR.qxd:CVR 3/29/11 7:58 Page 2 Department of Embryology 3520 San Martin Dr. / Baltimore, MD 21218 410.246.3001 Geophysical Laboratory 5251 Broad Branch Rd., N.W. / Washington, DC 20015-1305 202.478.8900 Department of Global Ecology 260 Panama St. / Stanford, CA 94305-4101 650.462.1047 The Carnegie Observatories 813 Santa Barbara St. / Pasadena, CA 91101-1292 626.577.1122 Las Campanas Observatory Casilla 601 / La Serena, Chile Department of Plant Biology 260 Panama St. / Stanford, CA 94305-4101 650.325.1521 Department of Terrestrial Magnetism 5241 Broad Branch Rd., N.W. / Washington, DC 20015-1305 202.478.8820 Office of Administration 1530 P St., N.W. / Washington, DC 20005-1910 202.387.6400 www.CarnegieScience.edu 2 009-2010 YEAR BOOK The President’s Report July 1, 2009 - June 30, 2010 CARNEGIE INSTITUTION FOR SCIENCE Former Presidents Former Trustees Daniel C.
[Show full text]
About Dark Matter and Gravitation Alain Haraux
About dark matter and gravitation Alain Haraux To cite this version: Alain Haraux. About dark matter and gravitation. 2020. hal-02883031 HAL Id: hal-02883031 https://hal.archives-ouvertes.fr/hal-02883031 Preprint submitted on 28 Jun 2020 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. About dark matter and gravitation. Alain Haraux Sorbonne Universit´e,Universit´eParis-Diderot SPC, CNRS, INRIA, Laboratoire Jacques-Louis Lions, LJLL, F-75005, Paris, France. e-mail: [email protected] Abstract A close inspection of Zwicky's seminal papers on the dynamics of galaxy clusters reveals that the discrepancy discovered between the dynamical mass and the luminous mass of clusters has been widely overestimated in 1933 as a consequence of several factors, among which the excessive value of the Hubble constant H0, then believed to be about seven times higher than today's average estimate. Taking account, in addition, of our present knowledge of classical dark matter inside galaxies, the contradiction can be reduced by a large factor. To explain the rather small remaining discrepancy of the order of 5, instead of appealing to a hypothetic exotic dark matter, the possibility of a inhomogeneous gravity is suggested.
[Show full text]
Vera C Rubin (1928–2016)
ARTICLE-IN-A-BOX Vera C Rubin (1928–2016) Then even nothingness was not, nor existence, .... At first there was only darkness wrapped in darkness. All this was only unillumined water. Rg Veda, As quoted by Vera Rubin at IAU Meeting, New Delhi. Science, once in a while, takes great leaps forward. Sometimes through brilliant flashes of insight that illumine a backdrop of knowledge acquired through hard groundwork. Sometimes through meticulous data, which is incontrovertible due to the hard groundwork and the deep insight that goes into the obtention, characterization and analysis of it. Vera Rubin’s landmark work, pointing out the flat rotation curves of spiral galaxies and the non-Keplerian motions these implied, falls in the latter class. Through her work, dark matter entered our consciousness as the dominant component of the Universe, relegating the familiar visible component to a mere less than 10 percent of the total. Autobiographical sketches of eminent astronomers grace some of the volumes of The Annual Review of Astronomy and Astrophysics. ‘Cosmology’, ‘dark matter’, ‘family’, ‘galaxies’, ‘ro- tation curves’, ‘students’ – so goes the keywords to the biographical sketch Vera gave to the Annual Reviews in 2011. She titled it ‘An Interesting Voyage’. Vera Florence Cooper was born in Philadelphia in 1928, of Jewish parents, Rose Applebaum, whose mother had immigrated from Bessarabia, sailing alone to the US at age 16, and Pete Cooper, born Pesach Kobchefski, who had reached the US at age seven to join his father who had immigrated to the US a year or two earlier from Latvia. Their two children, Ruth and Vera, grew up through the Great De- pression, amid a cheery scatter of grandparents, aunts, uncles, and cousins, shielded from the financial difficulties of the time.
[Show full text]
Vera Rubin Finding
Vera C. Rubin Photograph Collection, circa 1942-2012 Carnegie Institution of Washington Department of Terrestrial Magnetism Archives Washington, DC Finding aid written by: Mary Ferranti and Shaun Hardy March 2018 Revised July 2019 Vera C. Rubin Photograph Collection, circa 1942-2012 TABLE OF CONTENTS Page Introduction 1 Biographical Sketch 1 Scope and Content 2 Image Listing 3 Subject Terms 26 Bibliography 26 Related Collections 27 Vera C. Rubin Photograph Collection, circa 1942-2012 Table of Contents Vera C. Rubin Photograph Collection, circa 1942-2012 DTM-2016-03 Introduction Abstract: This collection consists of photographs documenting the professional and personal life of astronomer Vera C. Rubin. Extent: 3 linear feet: 5 three-ring album boxes, 1 flat print box. Acquisition: The collection was donated by Vera Rubin in 2012 and formally deeded to the archives by her son, Allan M. Rubin, in 2018. Access Restrictions: There are no access restrictions. Copyright: Copyright is held by the Department of Terrestrial Magnetism, Carnegie Institution of Washington. For permission to reproduce or publish please contact the archivist. Preferred Citation: Vera C. Rubin Photograph Collection, circa 1942-2012, Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, D.C. Processing: Maria V. Lobanova processed the collection in December 2016-April 2017 and identified as many individuals, places, and events as possible. Shaun Hardy and Mary Ferranti prepared the finding aid in 2018. Biographical Sketch Vera Rubin was born the younger daughter of Philip and Rose Cooper on July 23, 1928, in Philadelphia, PA. At the age of 10, she and her family moved to Washington, DC, when her father accepted a job offer there.
[Show full text]