Gravitational Lensing in Astronomy
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Using the Microlensing Technique, Astronomers Discover an Earth-Like Planet Outside Our Solar System
S&TR July/August 2006 11 Using the microlensing technique, astronomers discover an Earth-like planet outside our solar system. OOKING out to the vastness of the L night sky, stargazers often ponder questions about the universe, many wondering if planets like ours can be found somewhere out there. But teasing out the details in astronomical data that point to a possible Earth-like planet is exceedingly difficult. To find an extrasolar planet—a planet that circles a star other than the Sun— astrophysicists have in the past searched for Doppler shifts, changes in the wavelength emitted by an object because of its motion. When an astronomical object moves toward an observer on Earth, the light it emits becomes higher in frequency and shifts to the blue end of the spectrum. When the object moves away from the observer, its light becomes lower in frequency and shifts to the red end. By measuring these changes in wavelength, astrophysicists can precisely calculate how quickly objects are moving toward or away from Earth. When This artist’s rendition shows the Earth-like extrasolar planet discovered in 2005. (Reprinted courtesy of the European Southern Observatory.) Lawrence Livermore National Laboratory 12 An Earth-Like Extrasolar Planet S&TR July/August 2006 a giant planet orbits a star, the planet’s About the New Planet we consider the number of stars out there,” gravitational pull on the star produces a According to Livermore astrophysicist Cook says, “the fact that we stumbled on small (meters-per-second) back-and-forth Kem Cook, OGLE-2005-BLG-290-Lb is a one small planet means that thousands Doppler shift in the star’s light. -
Arxiv:1804.03516V1 [Physics.Gen-Ph] 4 Apr 2018 ∗ Mi:[email protected] Email: Hc Erhtemglei Lusadmauelgtcre Ihdura with Curves Years
April 2018 On the Origin and Nature of Dark Matter P.H. Frampton∗ Brasenose College, Oxford OX1 4AJ, UK Abstract It is discussed how the ideas of entropy and the second law of thermodynamics, conceived long ago during the nineteenth century, underly why cosmological dark matter exists and originated in the first three years of the universe in the form of primordial black holes, a very large number of which have many solar masses including up to the supermassive black holes at the centres of galaxies. Certain upper bounds on dark astrophysical objects with many solar masses based on analysis of the CMB spectrum and published in the literature are criticised. For completeness we discuss WIMPs and axions which are leading particle theory candidates for the constituents of dark matter. The PIMBHs (Primordial Intermediate Mass Black Holes) with many solar masses should be readily detectable in microlensing experiments which search the Magallenic Clouds and measure light curves with durations of from one year up to several years. arXiv:1804.03516v1 [physics.gen-ph] 4 Apr 2018 ∗email: [email protected] Introduction We assume Newton’s universal law for the gravitational force F between every two point particles GM1M2 F = (1) R2 where G is a constant, M1, M2 are the two masses and R is the separation, to be valid at the scale of galaxies and clusters of galaxies. Then there is overwhelming observational evidence [1, 2] for the existence of dark matter which does not radiate electromagnetically but which, by assumption, interacts gravitationally according to Eq.(1). -
A Review of the History, Theory and Observations Of
A REVIEW OF THE HISTORY, THEORY AND OBSERVATIONS OF GRAVITATIONAL MICROLENSING UP UNTIL THE PRESENT DAY A thesis submitted in fulfilment of the requirements for the Degree of Master of Science in Astronomy in the University of Canterbury by T. McClelland University of Canterbury 2008 TABLE OF CONTENTS ABSTRACT CHAPTERS 1 The Early History of Lensing Theory ...............................................................................................................................4 Newtonian Mechanics General Relativity 1960 developments Detection 2 Lens Theory and Lensing Phenomena .............................................................................................................................40 The Deflection of Light by Massive Objects Newtonian Mechanics General Relativistic Mechanics Gravitational Lensing Lens Equation Einstein Rings Gravitational Microlensing Quasar Microlensing Light curve variations and implications Parallax Caustic Curves 3 Modern Techniques and their Applications .............................................................................................................................66 Inverse Ray Technique Inverse Polygon Mapping Difference Imaging Astrometry 4 Applications .............................................................................................................................70 Dark Matter Binary Systems Extrasolar Planets Black Holes Stellar Mass Stellar Atmospheres Quasar Abnormalities Understanding Galactic Structure 5 Systematic Observational Networks .............................................................................................................................84 -
Microlensing Searches for Exoplanets
Review Microlensing Searches for Exoplanets Yiannis Tsapras Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12–14, 69120 Heidelberg, Germany; [email protected] Received: 3 July 2018; Accepted: 26 September 2018; Published: 29 September 2018 Abstract: Gravitational microlensing finds planets through their gravitational influence on the light coming from a more distant background star. The presence of the planet is then inferred from the tell-tale brightness variations of the background star during the lensing event, even if no light is detectable from the planet or the host foreground star. This review covers fundamental theoretical concepts in microlensing, addresses how observations are performed in practice, the challenges of obtaining accurate measurements, and explains how planets reveal themselves in the data. It concludes with a presentation of the most important findings to-date, a description of the method’s strengths and weaknesses, and a discussion of the future prospects of microlensing. Keywords: extrasolar planets; general relativity; microlensing; galactic bulge; planetary systems; exoplanets 1. Introduction 1.1. Discovering Exoplanets Planets begin forming in the gaseous disks surrounding young stars, but the exact physical processes that drive their formation and evolution are still not fully understood [1]. Theory predicts that these disks should last for a few million years and that planetary embryos can migrate while they are still embedded in them [2]. Some are eventually engulfed by their host stars. Others survive and grow by accreting gas and dust from the surrounding disk but end up far from where they first started forming. A question may then be posed: How are these planets distributed around their host stars and are there similarities with our own system or is the Solar system in some ways unique? The presence of liquid water on a planetary surface is no guarantee for the existence of life, although it was a necessary ingredient for the development of life on Earth. -
Gravitational Lensing in Astronomy
Gravitational Lensing in Astronomy Joachim Wambsganss Astrophysikalisches Institut Potsdam An der Sternwarte 16 14482 Potsdam Germany [email protected] Published 2 November 1998 (Last Amended 31 August 2001) Living Reviews in Relativity www.livingreviews.org/Articles/Volume1/1998-12wamb Published by the Max-Planck-Institute for Gravitational Physics Albert Einstein Institute, Potsdam, Germany Abstract Deflection of light by gravity was predicted by General Relativity and observationally confirmed in 1919. In the following decades, various as- pects of the gravitational lens effect were explored theoretically. Among them were: the possibility of multiple or ring-like images of background sources, the use of lensing as a gravitational telescope on very faint and distant objects, and the possibility of determining Hubble's constant with lensing. It is only relatively recently, (after the discovery of the first doubly imaged quasar in 1979), that gravitational lensing has became an observational science. Today lensing is a booming part of astrophysics. In addition to multiply-imaged quasars, a number of other aspects of lensing have been discovered: For example, giant luminous arcs, quasar microlensing, Einstein rings, galactic microlensing events, arclets, and weak gravitational lensing. At present, literally hundreds of individual gravitational lens phenomena are known. Although still in its childhood, lensing has established itself as a very useful astrophysical tool with some remarkable successes. It has con- tributed significant new results in areas as different as the cosmological distance scale, the large scale matter distribution in the universe, mass and mass distribution of galaxy clusters, the physics of quasars, dark mat- ter in galaxy halos, and galaxy structure. -
Euclid Imaging Consortium Science Book
EIC Science Book by the Euclid Imaging Consortium EDITED BY: Alexandre R´efr´egier and Adam Amara Thomas Kitching Ana¨ıs Rassat Roberto Scaramella Jochen Weller 1st January 2010 Euclid Imaging Consortium Euclid Imaging Consortium Members PI: Alexandre Refregier (CEA Saclay) Co-PIs: Ralf Bender (MPE Germany), Mark Cropper (MSSL, UK), Roberto Scaramella (INAF- Oss. Roma, Italy), Simon Lilly (ETH Zurich, Switzerland), Nabila Aghanim (IAS Orsay, France), Francisco Castander (IEEC Barcelona, Spain), Jason Rhodes (JPL, USA) Study Manager: Jean-Louis Augueres (CEA Saclay) System engineer: Jerome Amiaux (CEA Saclay) Instrument scientists: Mario Schweitzer (MPE), Mark Cropper (MSSL) Olivier Boulade (CEA Saclay), Adam Amara (ETH Zurich), Jeff Booth (JPL), Anna Maria di Giorgio (INAF-IFSI) Co-Investigators: France: Marian Douspis (IAS Orsay), Yannick Mellier (IAP Paris), Olivier Boulade (CEA Saclay), Germany: Peter Schneider (U. Bonn), Oliver Krause (MPIA Heidelberg), Frank Eisenhauer (MPE Garching), Italy: Lauro Moscardini (U. Bologna), Luca Amendola (INAF-Oss. Roma and University of Heidelberg), Fabio Pasian (INAF-OATS), Spain: Ramon Miquel (IFAE Barcelona), Eusebio Sanchez (CIEMAT Madrid), Switzerland: George Meylan (EPFL-UniGE), Marcella Carollo (ETH Zurich), Francois Widi (EPFL-UniGE), UK: John Peacock (IfA Edinburgh), Sarah Bridle (UCL, London), Ian Bryson (IfA Edinburgh), USA: Jeff Booth (JPL), Steven Kahn (Stanford U.) Science working group coordinators: Weak Lensing: Adam Amara (ETH Zurich), Andy Taylor (IfA Edinburgh) Clusters/CMB: Jochen Weller (U. Munich/MPE), Nabila Aghanim (IAS Orsay) BAO (photometric): Francisco Castander (IEEC Barcelona), Anais Rassat (CEA Saclay) Supernovae: Isobel Hook (Oxford, and Obs. Rome), Massimo Della Valle (Oss. Capodi- monte/ICRA) Theory: Luca Amendola (INAF-Oss. Roma), Martin Kunz (U. -
Dark Matter' in Astronomy and Astrophysics
ResearchOnline@JCU This file is part of the following reference: Montgomery, Colin Robert Lister (2014) From Michell to MACHO: changing chronological perspectives on the concept of 'Dark Matter' in astronomy and astrophysics. MPhil thesis, James Cook University. Access to this file is available from: http://researchonline.jcu.edu.au/41364/ The author has certified to JCU that they have made a reasonable effort to gain permission and acknowledge the owner of any third party copyright material included in this document. If you believe that this is not the case, please contact [email protected] and quote http://researchonline.jcu.edu.au/41364/ DARK MATTER from MICHELL to MACHOS From Michell to MACHO: Changing Chronological Perspectives on the Concept of ‘Dark Matter’ in Astronomy and Astrophysics Thesis submitted by Colin Robert Lister MONTGOMERY, ASTC (UT, Syd.), Master of Astronomy (UWS) October, 2014 for the degree of Master of Philosophy (Natural and Physical Sciences) in the School of Engineering and Physical Sciences, James Cook University 1 DARK MATTER from MICHELL to MACHOS STATEMENT OF ACCESS I, the undersigned, author of this work, understand that James Cook University will make this thesis available for use within the University Library and, via the Australian Digital Thesis network, for use elsewhere. I understand that, as an unpublished work, a thesis has significant protection under the Copyright Act and; I do not wish to place any further restriction on access to this work. Colin R L Montgomery 20. 10. 14 Date Signature 2 DARK MATTER from MICHELL to MACHOS STATEMENT OF SOURCES DECLARATION I declare that this thesis is my own work and has not been submitted in any form for another degree or diploma at any university of tertiary education. -
Letter of Interest Halometry: Searching for Dark
Snowmass2021 - Letter of Interest Halometry: Searching for Dark Structures with Astrometric Surveys Thematic Areas: (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astroparticle Physics & Cosmology Contact Information: Ken Van Tilburg (New York University and Flatiron Institute) [[email protected]] Authors: Siddharth Mishra-Sharma (New York University), Cristina Mondino (Perimeter Institute for Theoretical Physics), Anna-Maria Taki (University of Oregon), Ken Van Tilburg (New York University and Flatiron Institute), Neal Weiner (New York University) Abstract: In this research program, we aim to detect low-mass dark matter substructures in the Milky Way solely through their gravitational lensing signatures on luminous background sources. We have developed several analysis techniques and protocols that can tease out these lensing-induced angular deflections, which im- print correlated distortions on the motions of background stars, quasars, and galaxies. Ongoing astrometric surveys such as Gaia will probe large parts of viable parameter space where structure formation is enhanced at small scales. Upcoming and proposed surveys such as the Nancy Grace Roman Space Telescope, Square Kilometer Array, and Theia will greatly extend the discovery reach, and may be sufficiently sensitive to detect dark subhalos, entirely devoid of stars. Such a discovery would have far-reaching implications for early structure formation, astroparticle physics, and (in)direct detection of dark matter. 1 Background: The precise nature of the constituents of the dark matter (DM) and their microphysical prop- erties is not known. -
Microlensing and Its Degeneracy Breakers: Parallax, Finite Source, High-Resolution Imaging, and Astrometry
universe Review Microlensing and Its Degeneracy Breakers: Parallax, Finite Source, High-Resolution Imaging, and Astrometry Chien-Hsiu Lee Subaru Telescope, National Astronomical Observatory of Japan, 650 N Aohoku Place, Hilo, HI 96720, USA; [email protected]; Tel.: +1-808-934-7788 Academic Editors: Valerio Bozza, Francesco De Paolis and Achille A. Nucita Received: 28 April 2017; Accepted: 4 July 2017; Published: 7 July 2017 Abstract: First proposed by Paczynski in 1986, microlensing has been instrumental in the search for compact dark matter as well as discovery and characterization of exoplanets. In this article, we provide a brief history of microlensing, especially on the discoveries of compact objects and exoplanets. We then review the basics of microlensing and how astrometry can help break the degeneracy, providing a more robust determination of the nature of the microlensing events. We also outline prospects that will be made by on-going and forth-coming experiments/observatories. Keywords: gravitational lensing: micro; exoplanets; dark matter 1. Introduction According to Einstein’s theory of general relativity [1], massive foreground objects can induce strong space-time curvature, serving as gravitational lenses and focus the lights of background sources into multiple and magnified images that are projected along the observer’s line-of-sight. Such gravitational lensing systems provide us unique opportunities to study dark matter that hardly reveal their existences via electromagnetic radiations, or very faint objects that are beyond the sensitivity of state-of-the-art instruments. However, based on the calculations of Chwolson [2] and Einstein himself ([3], upon the request of R. W. Mandl), if the foreground object is as compact and light as a stellar object, the chance of gravitational lensing is very slim and, given the telescopes and instruments in the early 20th century, it is unlikely to observe such an event.