DOCSLIB.ORG

Detector Description and Performance for the First Coincidence

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Detector Description and Performance for the First Coincidence ARTICLE IN PRESS Nuclear Instruments and Methods in Physics Research A 517 (2004) 154–179 Detector description and performance for the first coincidence observations between LIGO and GEO B. Abbotta, R. Abbottb, R. Adhikaric, A. Ageevao,1, B. Allend, R. Amine, S.B. Andersona, W.G. Andersonf, M. Arayaa, H. Armandulaa, F. Asiria,2, P. Aufmuthg, C. Aulberth, S. Babaki, R. Balasubramaniani, S. Ballmerc, B.C. Barisha, D. Barkeri, C. Barker-Pattonj, M. Barnesa, B. Barrk, M.A. Bartona, K. Bayerc, R. Beausoleill,3, K. Belczynskim, R. Bennettk,4, S.J. Berukoffh,5, J. Betzwieserc, B. Bhawala, I.A. Bilenkoao, G. Billingsleya, E. Blacka, K. Blackburna, B. Bland-Weaverj, B. Bochnerc,6, L. Boguea, R. Borka, S. Bosen, P.R. Bradyd, V.B. Braginskya,o, J.E. Brauo, D.A. Brownd, S. Brozekg,7, A. Bullingtonl, A. Buonannop,8, R. Burgessc, D. Busbya, W.E. Butlerq, R.L. Byerl, L. Cadonatic, G. Cagnolik, J.B. Campr, C.A. Cantleyk, L. Cardenasa, K. Carterb, M.M. Caseyk, J. Castiglionee, A. Chandlera, J. Chapskya,9, P. Charltona, S. Chatterjic, Y. Chenp, V. Chickarmanes, D. Chint, N. Christensenu, D. Churchesi, C. Colacinog,v, R. Coldwelle, M. Colesb,10, D. Cookj, T. Corbittc, D. Coynea, J.D.E. Creightond, T.D. Creightona, D.R.M. Crooksk, P. Csatordayc, B.J. Cusackw, C. Cutlerh, E. D’Ambrosioa, K. Danzmanng,v,x, R. Daviesi, E. Daws,11, D. DeBral, T. Delkere,12, R. DeSalvoa, S. Dhurandary,M.D!ıazf, H. Dinga, R.W.P. Dreverz, R.J. Dupuisk, C. Ebelingu, J. Edlunda, P. Ehrensa, E.J. Elliffek, T. Etzela, M. Evansa, T. Evansb, C. Fallnichg, D. Farnhama, *Corresponding author. MIT NW17-161, 175 Albany Str., Cambridge, MA 02139, USA Tel.: +1-617-253-6411; fax: +1-617-253- 7014. E-mail addresses: [email protected] (D.H. Shoemaker). 1 Currently at Syracuse University. 2 Currently at Stanford Linear Accelerator Center. 3 Currently at HP Laboratories. 4 Currently at Rutherford Appleton Laboratory. 5 Currently at University of California, Los Angeles. 6 Currently at Hofstra University. 7 Currently at Siemens AG. 8 Permanent address: GReCO, Institut d’Astrophysique de Paris (CNRS). 9 Currently at NASA Jet Propulsion Laboratory. 10 Currently at National Science Foundation. 11 Currently at University of Sheffield. 12 Currently at Ball Aerospace Corporation. 0168-9002/$ - see front matter r 2003 Elsevier B.V. All rights reserved. doi:10.1016/j.nima.2003.11.124 ARTICLE IN PRESS B. Abbott et al. / Nuclear Instruments and Methods in Physics Research A 517 (2004) 154–179 155 M.M. Fejerl, M. Finea, L.S. Finnaa, E.! Flanaganab, A. Freisev,13, R. Freyo, P. Fritschelc, V. Frolovb, M. Fyffeb, K.S. Ganezerac, J.A. Giaimes, A. Gillespiea,14, K. Godac, G. Gonzalez! s,S.GoXlerg, P. Grandclement! m, A. Grantk, C. Grayj, A.M. Gretarssonb, D. Grimmetta, H. Grotev, S. Grunewaldh, M. Guentherj, E. Gustafsonl,15, R. Gustafsont, W.O. Hamiltons, M. Hammondb, J. Hansonb, C. Hardhaml, G. Harryc, A. Hartuniana, J. Heefnera, Y. Hefetzc, G. Heinzelv, I.S. Hengg, M. Hennessyl, N. Heplerv, A. Heptonstallk, M. Heursg, M. Hewitsonk, N. Hindmanj, P. Hoanga, J. Houghk, M. Hrynevycha,16, W. Hual, R. Ingleyad, M. Itoo, Y. Itohh, A. Ivanova, O. Jennrichk,17, W.W. Johnsons, W. Johnstonf, L. Jonesa, D. Jungwirtha,18, V. Kalogeram, E. Katsavounidisc, K. Kawabex,v, S. Kawamuraae, W. Kellsa, J. Kernb, A. Khanb, S. Killbournk, C.J. Killowk, C. Kimm, C. Kinga, P. Kinga, S. Klimenkoe, P. Kloevekornv, S. Korandad, K. Kotter. g, J. Kovalikb, D. Kozaka, B. Krishnanh, M. Landryj, J. Langdaleb, B. Lantzl, R. Lawrencec, A. Lazzarinia, M. Leia, V. Leonhardtg, I. Leonoro, K. Libbrechta, P. Lindquista, S. Liua, J. Logana,19, M. Lormandb, M. Lubinskij, H. Luck. g,v, T.T. Lyonsa,18, B. Machenschalkh, M. MacInnisc, M. Mageswarana, K. Mailanda, W. Majida,8, M. Malecg, F. Manna, A. Marinc,20,S.Marka! a, E. Marosa, J. Masona,21, K. Masonc, O. Mathernyj, L. Matonej, N. Mavalvalac, R. McCarthyj, D.E. McClellandw, M. McHughaf, P. McNamarak,22, G. Mendellj, S. Meshkova, C. Messengerad, V.P. Mitrofanovao, G. Mitselmakhere, R. Mittlemanc, O. Miyakawaa, S. Miyokia,23, S. Mohantyh, G. Morenoj, K. Mossaviv, B. Moursa,24, G. Muellere, S. Mukherjeeh, J. Myersj, S. Naganov, T. Nashag, H. Naundorfh, R. Nayaky, G. Newtonk, F. Noceraa, P. Nutzmanm, T. Olsonah, B. O’Reillyb, D. J. Ottawayc, A. Ottewilld,25, D. Ouimettea,17, H. Overmierb, B.J. Owenaa, M.A. Papah, C. Parameswariahb, V. Parameswariahj, M. Pedrazaa, S. Pennai, M. Pitkink, M. Plissik, M. Prattc, V. Quetschkeg, F. Raabj, H. Radkinsj, R. Rahkolao, M. Rakhmanove, S.R. Raoa, D. Reddinga,8, M.W. Regehra,8, T. Regimbauc, K.T. Reillya, K. Reithmaiera, D.H. Reitzee, 13 Currently at European Gravitational Observatory. 14 Currently at Intel Corp. 15 Currently at Lightconnect Inc. 16 Currently at Keck Observatory. 17 Currently at ESA Science and Technology Center. 18 Currently at Raytheon Corporation. 19 Currently at Mission Research Corporation. 20 Currently at Harvard University. 21 Currently at Lockheed-Martin Corporation. 22 Currently at NASA Goddard Space Flight Center. 23 Permanent address: University of Tokyo, Institute for Cosmic Ray Research. 24 Currently at Laboratoire d’Annecy-le-Vieux de Physique des Particules. 25 Permanent address: University College Dublin. ARTICLE IN PRESS 156 B. Abbott et al. / Nuclear Instruments and Methods in Physics Research A 517 (2004) 154–179 S. Richmanc,26, R. Riesenb, K. Rilest, A. Rizzib,27, D.I. Robertsonk, N.A. Robertsonk,l, L. Robisona, S. Roddyb, J. Rollinsc, J.D. Romanof, J. Romiea, H. Ronge,13, D. Rosea, E. Rotthoffaa, S. Rowank,A.Rudiger. v,x, P. Russella, K. Ryanj, I. Salzmana, G.H. Sandersa, V. Sannibalea, B. Sathyaprakashi, P.R. Saulsonaj, R. Savagej, A. Sazonove, R. Schillingv,x, K. Schlaufmanaa, V. Schmidta,28, R. Schofieldo, M. Schrempelg,29, B.F. Schutzh,i, P. Schwinbergj, S.M. Scottw, A.C. Searlew, B. Searsa, S. Seela, A.S. Senguptay, C.A. Shapiroaa,30, P. Shawhana, D.H. Shoemakerc,*, Q.Z. Shue,31, A. Sibleyb, X. Siemensd, L. Sieversa,8, D. Siggj, A.M. Sintesh,ak, K. Skeldonk, J.R. Smithv, M. Smithc, M.R. Smitha, P. Sneddonk, R. Speroa,8, G. Stapferb, K.A. Straink, D. Stromo, A. Stuveraa, T. Summerscalesaa, M.C. Sumnera, P.J. Suttonaa, J. Sylvestrea, A. Takamoria, D.B. Tannere, H. Tariqa, I. Taylori, R. Taylora, K.S. Thornep, M. Tibbitsaa, S. Tilava,32, M. Tintoz,8, K.V. Tokmakovao, C. Torresf, C. Torriea,k, S. Traegerg,33, G. Traylorb, W. Tylera, D. Ugolinial, M. Vallisnerip,8, M. van Puttenc, S. Vassa, A. Vecchioad, C. Vorvickj, S.P. Vyatchaninao, L. Wallacea, H. Waltherx, H. Wardk, B. Warea,8, K. Wattsb, D. Webbera, A. Weidnerv,x, U. Weilandg, A. Weinsteina, R. Weissc, H. Wellingg, L. Wena, S. Wens, J.T. Whelanaf, S.E. Whitcomba, B.F. Whitinge, P.A. Willemsa, P.R. Williamsh,34, R. Williamsz, B. Willkeg,v, A. Wilsona, B.J. Winjumaa,4, W. Winklerv,x, S. Wisee, A.G. Wisemand, G. Woank, R. Wooleyb, J. Wordenj, I. Yakushinb, H. Yamamotoa, S. Yoshidaam, I. Zawischag,35, L. Zhanga, N. Zotovan, M. Zuckerb, J. Zweiziga a LIGO—California Institute of Technology, Pasadena, CA 91125, USA b LIGO Livingston Observatory, Livingston, LA 70754, USA c LIGO—Massachusetts Institute of Technology, Cambridge, MA 02139, USA d University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA e University of Florida, Gainsville, FL 32611, USA f The University of Texas at Brownsville and Texas Southmost College, Brownsville, TX 78520, USA g Universitat. Hannover, D-30167 Hannover, Germany h Albert-Einstein-Institut, Max-Planck-Institut fur. Gravitationsphysik, D-14476 Golm, Germany i Cardiff University, Cardiff CF2 3YB, UK j LIGO Hanford Observatory, Richland WA 99352, USA k University of Glasgow, Glasgow G12 8QQ, UK l Stanford University, Stanford, CA 94305, USA 26 Currently at Research Electro-Optics Inc. 27 Currently at Institute of Advanced Physics, Baton Rouge, LA. 28 Currently at European Commission, DG Research, Brussels, Belgium. 29 Currently at Spectra Physics Corporation. 30 Currently at University of Chicago. 31 Currently at LightBit Corporation. 32 Currently at University of Delaware. 33 Currently at Carl Zeiss GmbH. 34 Currently at Shanghai Astronomical Observatory. 35 Currently at Laser Zentrum Hannover. ARTICLE IN PRESS B. Abbott et al. / Nuclear Instruments and Methods in Physics Research A 517 (2004) 154–179 157 m Northwestern University, Evanston, IL 60208, USA n Washington State University, Pullman, WA 99164, USA o University of Oregon, Eugene, OR 97403, USA p Caltech-CaRT, Pasadena, CA 91125, USA q University of Rochester, Rochester, NY 14627, USA r NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA s Louisiana State University, Baton Rouge, LA 70803, USA t University of Michigan, Ann Arbor, MI 48109, USA u Carleton College, Northfield, MN 55057, USA v Albert-Einstein-Institut, Max-Planck-Institut fur. Gravitationsphysik, D-30167 Hannover, Germany w Australian National University, Canberra 0200, Australia x Max Planck Institut fur. Quantenoptik, D-85748 Garching, Germany y Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India z California Institute of Technology, Pasadena, CA 91125, USA aa The Pennsylvania State University, University Park, PA 16802, USA ab Cornell University, Ithaca, NY 14853, USA ac California State University Dominguez Hills, Carson, CA 90747, USA ad University of Birmingham, Birmingham, B15 2TT, UK ae National Astronomical Observatory of Japan, Tokyo 181-8588, Japan af Loyola University, New Orleans, LA 70118, USA ag Fermi National Accelerator Laboratory, Batavia, IL 60510, USA ah Salish Kootenai College, Pablo, MT 59855, USA ai Hobart and William Smith Colleges, Geneva, NY 14456, USA aj Syracuse University, Syracuse, NY 13244, USA ak Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain al Trinity University, San Antonio, TX 78212, USA am Southeastern Louisiana University, Hammond, LA 70402, USA an Louisiana Tech University, Ruston, LA 71272, USA ao Physics Faculty, Moscow State University, Moscow 119992, Russia The LIGO Scientific Collaboration Received 30 September 2003 Abstract For 17 days in August and September 2002, the LIGO and GEO interferometer gravitational wave detectors were operated in coincidence to produce their first data for scientific analysis.
Load more

Recommended publications
  • A Basic Michelson Laser Interferometer for the Undergraduate Teaching Laboratory Demonstrating Picometer Sensitivity Kenneth G
    A basic Michelson laser interferometer for the undergraduate teaching laboratory demonstrating picometer sensitivity Kenneth G. Libbrechta) and Eric D. Blackb) 264-33 Caltech, Pasadena, California 91125 (Received 3 July 2014; accepted 4 November 2014) We describe a basic Michelson laser interferometer experiment for the undergraduate teaching laboratory that achieves picometer sensitivity in a hands-on, table-top instrument. In addition to providing an introduction to interferometer physics and optical hardware, the experiment also focuses on precision measurement techniques including servo control, signal modulation, phase-sensitive detection, and different types of signal averaging. Students examine these techniques in a series of steps that take them from micron-scale sensitivity using direct fringe counting to picometer sensitivity using a modulated signal and phase-sensitive signal averaging. After students assemble, align, and characterize the interferometer, they then use it to measure nanoscale motions of a simple harmonic oscillator system as a substantive example of how laser interferometry can be used as an effective tool in experimental science. VC 2015 American Association of Physics Teachers. [http://dx.doi.org/10.1119/1.4901972] 8–14 I. INTRODUCTION heterodyne readouts, and perhaps multiple lasers. Modern interferometry review articles tend to focus on complex optical Optical interferometry is a well-known experimental tech- configurations as well,15 as they offer improved sensitivity and nique for making precision displacement measurements, stability over simpler designs. While these advanced instru- with examples ranging from Michelson and Morley’s famous ment strategies are becoming the norm in research and indus- aether-drift experiment to the extraordinary sensitivity of try, for educational purposes we sought to develop a basic modern gravitational-wave detectors.
    [Show full text]
  • THE MICHELSON INTERFEROMETER Intermediate ( First Part) to Advanced (Latter Parts)
    THE MICHELSON INTERFEROMETER Intermediate ( first part) to Advanced (latter parts) Goal: There is a progression of goals for this experiment but you do not have to do Reading: the last goal. The first goal is to align the interferometer and calibrate it. Calibration ADC should be done both mechanically and Michelson program writeup optically with a HeNe laser. The second Stepper motors goal is a study of the sodium doublet. One measures the average wavelength of the two Good optics text lines and the separation of the lines. The Fourier transforms and FFT final experimental goal is to find interference fringes for white light and measure it’s coherence length. Homework: 1. Indicate how the standard michelson interferometer optics is the same as the Introduction: optics shown in fig. 2. Figure 1 The optics of the Michelson Interferometer. Note the light directed away from the mirrors is offset from the light directed toward the mirrors for clarity Note: The observation of fringes associated with the sodium doublet is a rather difficult Figure 2 The optics of the Michelson experiment and the observation of white Interferometer is equivalent to the that of light fringes is even more difficult. two sources S1 ans S2, that are emitting Understanding how the concept of light that is in phase. Note: source S1 is coherence length relates to this experiment movable. is almost essential to complete these goals. 2. Explain changes the optics in fig.1 and 2 required to account for the finite size of the light source Page -1- 3. For the optics shown in fig.2, at what Experimental tasks distance should the detector (eye) be There are three experimental tasks, focused? but only the first two are required.
    [Show full text]
  • Increasing the Sensitivity of the Michelson Interferometer Through Multiple Reflection Woonghee Youn
    Rose-Hulman Institute of Technology Rose-Hulman Scholar Graduate Theses - Physics and Optical Engineering Graduate Theses Summer 8-2015 Increasing the Sensitivity of the Michelson Interferometer through Multiple Reflection Woonghee Youn Follow this and additional works at: http://scholar.rose-hulman.edu/optics_grad_theses Part of the Engineering Commons, and the Optics Commons Recommended Citation Youn, Woonghee, "Increasing the Sensitivity of the Michelson Interferometer through Multiple Reflection" (2015). Graduate Theses - Physics and Optical Engineering. Paper 7. This Thesis is brought to you for free and open access by the Graduate Theses at Rose-Hulman Scholar. It has been accepted for inclusion in Graduate Theses - Physics and Optical Engineering by an authorized administrator of Rose-Hulman Scholar. For more information, please contact bernier@rose- hulman.edu. Increasing the Sensitivity of the Michelson Interferometer through Multiple Reflection A Thesis Submitted to the Faculty of Rose-Hulman Institute of Technology by Woonghee Youn In Partial Fulfillment of the Requirements for the Degree of Master of Science in Optical Engineering August 2015 © 2015 Woonghee Youn 2 ABSTRACT Youn, Woonghee M.S.O.E Rose-Hulman Institute of Technology August 2015 Increase a sensitivity of the Michelson interferometer through the multiple reflection Dr. Charles Joenathan Michelson interferometry has been one of the most famous and popular optical interference system for analyzing optical components and measuring optical metrology properties. Typical Michelson interferometer can measure object displacement with wavefront shapes to one half of the laser wavelength. As testing components and devices size reduce to micro and nano dimension, Michelson interferometer sensitivity is not suitable. The purpose of this study is to design and develop the Michelson interferometer using the concept of multiple reflections.
    [Show full text]
  • The Holometer: a Measurement of Planck-Scale Quantum Geometry
    The Holometer: A Measurement of Planck-Scale Quantum Geometry Stephan Meyer November 3, 2014 1 The problem with geometry Classical geometry is made of definite points and is based on “locality.” Relativity is consistent with this point of view but makes geometry “dynamic” - reacts to masses. Quantum physics holds that nothing happens at a definite time or place. All measurements are quantum and all known measurements follow quantum physics. Anything that is “real” must be measurable. How can space-time be the answer? Stephan Meyer SPS - November 3, 2014 2 Whats the problem? Start with - Black Holes What is the idea for black holes? - for a massive object there is a surface where the escape velocity is the speed of light. Since nothing can travel faster than the speed of light, things inside this radius are lost. We can use Phys131 to figure this out Stephan Meyer SPS - November 3, 2014 3 If r1 is ∞, then To get the escape velocity, we should set the initial kinetic energy equal to the potential energy and set the velocity equal to the speed of light. Solving for the radius, we get Stephan Meyer SPS - November 3, 2014 4 having an object closer than r to a mass m, means it is lost to the world. This is the definition of the Schwarzshild radius of a black hole. So for stuff we can do physics with we need: Stephan Meyer SPS - November 3, 2014 5 A second thing: Heisenberg uncertainty principle: an object cannot have its position and momentum uncertainty be arbitrarily small This can be manipulated, using the definition of p and E to be What we mean is that to squeeze something to a size λ, we need to put in at least energy E.
    [Show full text]
  • 1 Laboratory 8: Michelson Interferometer 1.1 Theory: References:Optics,E.Hecht,Sec 9.4
    1051-232-20033 Imaging Systems Laboratory II Week of 5/3/2004, Writeup Due 5/18/2004 (T) 1 Laboratory 8: Michelson Interferometer 1.1 Theory: References:Optics,E.Hecht,sec 9.4 1.1.1 Division-of-Wavefront Interferometry In the last lab, you saw that coherent (single-wavelength) light from point sources two different locations in an optical beam could be combined after having traveled along two different paths. The recombined light exhibited sinusoidal fringes whose spatial frequency depended on the difference in angle of the light beams when recombined. The regular variation in relative phase of the light beams resulted in constructive interference (when the relative phase difference is 2πn,wheren is an integer) and destructive interference where the relative phase difference is 2πn + π. The centers of the “bright” fringes occur where the optical paths differ by an integer multiple of λ0. “Division-of-Wavefront” Interferometry via Young’s Two-Slit Experiment. The period of the intensity fringes at the observation plane is D Lλ . ' d 1.1.2 Division-of-Amplitude Interferometry This laboratory will introduce a second class of interferometer where the amplitude of the light is separated into two (or more) parts at the same point in space via partial reflection by a beamsplitter. The beamsplitter is the light-dividing element in several types of interferometers. This lab will demostrate the action of the Michelson interferometer for both coherent light from a laser and for white light (with some luck!). Coherence of a Light Source If two points within the same beam of light exhibit a consistent and measurable phase difference, then the light at the two points is said to be coherent, and thus 1 the light at these two locations may be combined to create interference.
    [Show full text]
  • Chapter 6: Speed of Light
    Physics 341 Experiment 6 Page 6-1 Chapter 6: Speed of Light 6.1 Introduction The speed of light is one of the most fundamental constants in physics. It ties the dimension of time to Euclidean 3-space to form a four-dimensional entity called spacetime. In ordinary three dimensional Euclidean space, there is a familiar invariant, the distance between two points given by: !s 2 = !x 2 + !y 2 + !z 2 (6.1) The value of !s is independent of the orientation of coordinate axes, x, y and z. Any rotation transformation on these coordinates must maintain the same value for the Pythagorean distance. In spacetime, the equivalent invariant is: !s 2 = !x 2 + !y 2 + !z 2 + c2!t 2 (6.2) This extended definition describes an invariant not only under rotations of x, y and z but also including transformations that relate inertial reference frames with constant relative velocities. In our everyday experience, relativistic effects are almost unobservable simply because the speed of light is so high, c =299,792,458 meters/second. This means that the time delays that can be measured in a classroom are too small to be detected by our biological senses. The point of this experiment is to circumvent this problem by using fast electronics to record time differences that otherwise would be hard to measure. The speed of light is large but it is not infinite. As a prelude to this experiment, you will first become familiar with an oscilloscope and the handling of short electrical pulses. This provides nice examples of one-dimensional wave behavior that are otherwise only easy to exhibit with mechanical models.
    [Show full text]
  • Michelson Laser Interferometer 4747112 EN
    P5.8.8.1 Michelson Laser Interferometer 4747112 EN Laser Sicherheitshinweise Hiermit erklärt die Firma LD Didactic GmbH, dass es sich bei dem angebotenen Lasersystem um einen Aufbau handelt, der sowohl in Komponenten als auch im fertigen Aufbau einem Laser der Klasse 3A, 3B oder 4 nach DIN EN 60 825-1 entspricht. Typischerweise ist die Pumpdiode eine Nd:YAG Laser Klasse 4, ein HeNe Laser mit Auskoppler Klasse 3A, aber ein HeNe mit zwei hochreflektierenden Spiegeln nur Klasse 1. Bitte die Anleitung oder Aufkleber beachten. Aus Haftungsgründen dürfen diese Geräte oder Gerätesammlungen nicht an Privatleute verkauft werden. Der Einsatz von Lasern oberhalb Klasse 2 an allgemeinbildendenden Schulen ist in Deutschland nicht gestattet. Gewerbliche Abnehmer, Schulen und Universitäten werden hiermit darauf hingewiesen, dass aus dem missbräuchlichen Betrieb der Geräte ein Verletzungsrisiko, speziell für die Augen, resultiert. Dem Benutzer obliegt insbesondere: - Die relevanten Unfallverhütungsvorschriften zu beachten, zur Zeit beispielsweise BGV B2 und BGI 832 - die OstrV zu beachten „Verordnung zum Schutz der Beschäftigten vor Gefährdungen durch künstliche optische Strahlung“ - Der Betrieb der Geräte muss rechtzeitig beim Gewerbeaufsichtsamt und der Berufsgenossenschaft angezeigt werden. - Der Betreiber muss schriftlich einen Laserschutzbeauftragten benennen, der für die Einhaltung der Schutzmaßnahmen verantwortlich ist. - Die Geräte sind nur für den Betreib in umschlossenen Räumen vorgesehen, deren Wände die Ausbreitung des Laserstrahls begrenzen. - Der Laserbereich ist deutlich und dauerhaft zu kennzeichnen. - Ab Laserklasse 4 ist eine Laser-Warnleuchte am Raumzugang notwendig. - Die Geräte sind zur Lehre und Ausbildung in Berufsschulen, Universitäten oder ähnlichen Einrichtungen gedacht. - Die Geräte nur innerhalb der in den Anleitungen vorgegebenen Betriebsbedingungen betreiben. - Die Geräte nur von entsprechend unterwiesenen Mitarbeitern und Studierenden benutzen lassen.
    [Show full text]
  • Interferometers 1. Introduction 2. Michelson Interferometer: Theory
    Interferometers (Two weights for all experiments with Michelson interferometer and one weight more for experiments with Fabry-Per´ot interferometer) 1. Introduction Interferometers are devices employed in the study of interference patterns produced by various light sources. They are conveniently divided into two main classes: those based on division of wavefront, and those based on division of amplitude. 2. Michelson interferometer: theory The Michelson interferometer employs a division of amplitude scheme. It can be used to carry out the following principal measurements: Width and fine structure of spectral lines. Lengths or displacements in terms of wavelengths of light. Refractive indices of transparent solids. Differences in the velocity of light along 2 different directions. It operates as follows: we “divide” the wave amplitude by partial reflection using a beam splitter G1, with the two resulting wave fronts maintaining the original width by having reduced amplitudes [1]. A beam splitter is nothing more than a plate of glass, which is made partially reflective: as such, the splitting occurs because part of the light is reflected off of the surface, and part is transmitted through it. The two beams obtained by amplitude division are sent in different directions against plane mirrors, then reflected back along their same respected paths to the beam splitter to form an interference pattern. The core optical setup, which is labelled in Fig.1, consists of two highly polished plates, A1 and A2, acting as the above-mentioned mirrors, and two parallel plates of glass G1 and G2 - one is the beam splitter, and the other is a compensating plate, whose purpose will be described below.
    [Show full text]
  • Craig Hogan, Fermilab PAC, November 2009 1 Interferometers Might Probe Planck Scale Physics
    The Fermilab Holometer a program to measure Planck scale indeterminacy A. Chou, R. Gustafson, G. Gutierrez, C. Hogan, S. Meyer, E. Ramberg, J.Steffen, C.Stoughton, R. Tomlin, S.Waldman, R.Weiss, W. Wester, S. Whitcomb Craig Hogan, Fermilab PAC, November 2009 1 Interferometers might probe Planck scale physics One interpretation of ‘t Hooft-Susskind holographic principle predicts a new kind of uncertainty leading to a new detectable effect: "holographic noise” Different from gravitational waves or quantum field fluctuations Predicts Planck-amplitude noise spectrum with no parameters We propose an experiment to test this hypothesis Craig Hogan, Fermilab PAC, November 2009 2 Planck scale seconds The physics of this “minimum time” is unknown 1.5 ×10−35 m Black hole radius particle energy ~1016 TeV € Quantum particle energy size Particle confined to Planck volume makes its own black hole 3 Quantum limits on measuring event positions Spacelike-separated event intervals can be defined with clocks and light But transverse position measured with waves is uncertain by the diffraction limit Lλ This is much larger than the wavelength € Lλ L λ Add second€ dimension: small phase difference of events over Wigner (1957): quantum limits large transverse patch with one spacelike dimension € 4 € A new uncertainty of spacetime? Suppose the Planck scale is a minimum wavelength Then transverse event positions may be fundamentally uncertain by the Planck diffraction limit Classical path ~ ray approximation of a Planck wave Craig Hogan, Fermilab PAC, November
    [Show full text]
  • Fourier Transform Infrared (FTIR) Spectroscopy
    Fourier Transform Infrared (FTIR) Spectroscopy • Basis of many IR satellite remote sensing instruments • Ground-based FTIR spectrometers also used for various applications Interference • Consequence of the wave properties of light • Coherence required for interference: only occurs if two waves have the same frequency and polarization Ordinary light is not coherent because it comes from independent atoms which emit on time scales of about 10-8 seconds. Laser light is an example of a coherent light source – a common stimulus triggers the emission of photons, so the resulting light is coherent. Laser light is also monochromatic (has a single spectral color or wavelength, related to one set of atomic energy levels) and collimated (consists of parallel beams, with little divergence; e.g. laser pointer spot size) Constructive vs. destructive interference Waves that combine Constructive in phase add up to interference relatively high irradiance. = (coherent) Waves that combine 180° out Destructive of phase cancel out and yield = interference zero irradiance. (coherent) Waves that combine with lots of different phases Incoherent nearly cancel out and yield = addition very low irradiance. Measuring the spectrum of an EM wave Remote sensing requires measurements of the frequencies (or wavelengths) present in an EM wave. This is defined as the spectrum of the wave. Plane waves have only one frequency, ω. Light electric field Time This light wave has many frequencies. And the frequency increases in time (from red to blue). Spectra can be measured
    [Show full text]
  • The Application and Improvement of Fourier Transform Spectrometer Experiment
    The Application and Improvement of Fourier transform Spectrometer Experiment Liu Zhi-min*，Gao En-duo, Zhou Feng-qi*，Wang Lan-lan, Feng Xiao-hua, Qi Jin-quan, Ji Cheng, Wang Luning Department of Optoelectronic Information Science and Engineering, School of Science, East China Jiaotong University, Nan chang 330013 China [email protected],[email protected] ABSTRACT According to teaching and experimental requirements of Optoelectronic information science and Engineering，in order to consolidate theoretical knowledge and improve the students practical ability, the Fourier transform spectrometer ( FTS) experiment, its design, application and improvement are discussed in this paper. The measurement principle and instrument structure of Fourier transform spectrometer are introduced, and the spectrums of several common Laser devices are measured. Based on the analysis of spectrum and test，several possible improvement methods are proposed. It also helps students to understand the application of Fourier transform in physics. Keywords: Fourier transform; Spectrum; Experiment. 1． INTRODUCTION Fourier Transform Spectrometer (FTS) [1] is based on the Fourier transform of the measured interference pattern to obtain spectrum. It has many advantages, such as multi-channel, high throughput, high precision, high signal to noise ratio, wide spectrum, non-contact, digital and so on[2,3]. FTS is very important for the study of atomic and molecular physics, astronomy and physics, spectroscopy, atmospheric remote sensing, analytical chemistry and other fields [4-6]. And it is also essential equipment for industrial inspection, customs inspection and so on [7]. Michelson interferometer and Fourier Transform Spectrometer are the instruments of measuring wavelength which is used frequently in college physics experiment teaching.
    [Show full text]
  • The Fermilab Holometer a Program to Meas'ure Planck Scale Indeterminacy
    FERMILAB-PROPOSAL-0990 The Fermilab Holometer A program to meas'ure Planck scale indeterminacy Aaron Chou, Craig Hogan (Spokesperson), Erik Ramberg Jason Steffen, Chris Stoughton, Ray Tomlin, William Wester Fermilab Center for Particle Astrophysics Sam Waldman, Rainer Weiss Massachusetts Institute of Technology Stephan Meyer University of Chicago H. Richard Gustafson University of Michigan Stanley Whitcomb California Institute of Technology Abstract We propose an experiment at Fermilab to study a conjectured effect called "holo­ graphic noise" that may arise from new Planck scale physics: the measured posi­ tions of bodies may wander randomly from ideal geodesics of classical relativity, in measurement-dependent directions, by about a Planck length per Planck time. The experiment will search for this holographic jitter in the relation of mass-energy and space-time by looking for correlated phase noise between two neighboring 40 meter interferometers. The goal of the experiment is to provide convincing evidence for or against the hypothesis that relative transverse positions of bodies display this particu­ lar new kind of quantum noise, whose power spectrum is independent of frequency and has a spectral density determined only by the Planck time. A positive result of the experiment would be a major step forward in understanding the emergence of space­ time and mass-energy from a unified theory of spacetime and quantum mechanics. A negative result will impact the macroscopic interpretation of unified theories. Contents A Introduction 5 1 5 9 A.3 measurement 11 B Experimental 13 C 15 C.l C.2 response. 17 18 21 C.6 21 24 Cost . .. 24 Electronics 25 1 .
    [Show full text]