Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Communications WF03 L

Total Page:16

File Type:pdf, Size:1020Kb

Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Communications WF03 L Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Communications WF03 L. Dussopt, F. Gianesello CEA-LETI, STMicroelectronics [email protected] , [email protected] 5G mobile communications above 6 GHz: timelines, key technologies and recent R&D M. Nekovee Samsung R&D, UK [email protected] WF03 Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Slide 1 Communications EMF user exposure due to mobile terminals in V-band Anda R. Guraliuc 1, M. Zhadobov 1, R. Sauleau 1, L. Marnat 2, L. Dussopt 2 1Institute of Electronics and Telecommunications of Rennes Rennes, France 2French Alternative Energies and Atomic Energy Commission Grenoble, France [email protected] Overview & Objectives www.miwaves.eu Evaluation of the user’s exposure to mmW frequencies for 1. Real case scenarios 2. Different antenna positions Front position Edge position Phone call Browsing Correlation of near-field exposure parameters to recommended safety limits A.R. Guraliuc, M. Zhadobov, R. Sauleau, L. Marnat, L. Dussopt, “Millimeter-wave exposure from mobile terminals” 2 2015 European Conf. on Networks and Commun. (EuCNC 2015) , Paris, France, pp. 82-85, June 29-July 2, 2015. mmW interaction with the human body At 60 GHz, normal incidence, the power transmission coefficient is around 60% and increases with the frequency. mmWaves Shallow penetration depth of mmWs in the skin Penetration depth is shallow induce SAR levels significantly higher than those (@ 60 GHz δ ≈ 0.5 mm) at microwaves for identical IPD values (e.g. 100 W/kg for IPD = 1 mW/cm 2). Absorption in the superficial layers Clothing impacts the absorption in the body (textile may increase the transmission, while an air gap between clothing and skin may reduce it). Primary biological targets are skin and cornea M. Zhadobov, N. Chahat, R. Sauleau, C. Le Quement, Y. Le Dréan, “Millimeter-wave interactions with the human body: state of knowledge and recent advances” 3 International Journal of Microwave and Wireless Technologies , 3, pp. 237-247, 2011. Exposure guidelines and standards Safety guidelines are set for Incident Power Density (IPD) Absorption is superficial & far-field region. Power Averaging Frequency Public Organization density Surface Time Safety factor (GHz) exposure (mW/cm 2) (cm 2) (min) 5 20 Occupational Occupational 100 1 ICNIRP [1] 10-300 68/ f1.05 1 20 General 20 1 5 20 Occupational F = 5 or 10 100 1 S CENELEC [2] 2-300 68/ f1.05 1 20 General General 20 1 30 - 300 10 100 2.524/ f0.47 3-96Occupational 200( f/3) 0.2 1 IEEE [3], [4] > 96 400 1 1 100 25.24/ f0.47 30 - 100 General 20 1 f – frequency in GHz [1] ICNIRP: “Guidelines for limiting exposure to time-varying electric, magnetic, and electromagnetic fields (up to 300 GHz)”, Health Phys., vol. 74, no. 4, pp. 494-522, 1998. [2] EN 50413 – 2008, “Basic standard on measurement and calculation procedures for human exposure to electric, magnetic and electromagnetic fields (0 Hz – 300 GHz)”. [3] IEEE Standard for safety levels with respect to human exposure to radio frequency electromagnetic fields, 3 kHz to 300 GHz, ISBN 0-7381-4835-0 SS95389, Apr. 2006. 4 [4] IEEE Standard for safety levels with respect to human exposure to radio frequency electromagnetic fields, 3 kHz to 300 GHz, ISBN 978-0-7381-6207-2 STD96039, Feb. 2010. Exposure limits - Considerations is the surface area of a cube with edge dimension 1.8 cm (related 2 20 cm to the human eye) used to establish exposure limits. is the surface area of the cornea used to establish localized 1 cm 2 Spatial exposure limits. Limits averaged over 1cm 2 should not exceed 20 times the values averaged over 20cm 2. 100 cm 2 is the surface area of human face / hand. is less restrictive than ICNIRP. safety limits rely on temperature increase in the eye and the potential adverse health effects caused by this increase. Temperature threshold in the eye ≈ 41 °C, over which cataract formation may Temperature appear. It corresponds to a temperature increase of 3-4°C. e.g. SAR @2.45GHz =10W/kg ∆T=4°C T<41 °C. Skin exposure at mmWs at the recommended limits (i.e. 1mW/cm2 and 5mW/cm 2 for an average surface of 20 cm 2) will increase its temperature by less than 0.7°C. [1] A. Guraliuc, M. Zhadobov, and R. Sauleau, “Dosimetric aspects related to the human body exposure to mm Waves”, MiWaveS project – Deliverable D1.3, Dec. 2014. Available online: http://www.miwaves.eu/MiWaveS_D1.3_v1.0.pdf [2] ICNIRP: “Guidelines for limiting exposure to time-varying electric, magnetic, and electromagnetic fields (up to 300 GHz)”, Health Phys., vol. 74, no. 4, pp. 494-522, 1998. [3] IEEE Standard for safety levels with respect to human exposure to radio frequency electromagnetic fields, 3 kHz to 300 GHz, ISBN 0-7381-4835-0 SS95389, Apr. 2006. 5 [4] EN 50413 – 2008, “Basic standard on measurement and calculation procedures for human exposure to electric, magnetic and electromagnetic fields (0 Hz – 300 GHz)”. Human body modeling - Plane wave exposure Plane waves TM d TE [1] N. Pavselj, D. Miklavcic, “Resistive heating and electropermeabilization of skin tissue during in vivo electroporation: A coupled nonlinear finite element model”, Int. J. of Heat and Mass Transfer , vol. 54, pp. 2294-2302, 2011. [2] S.I. Alekseev, M.C. Ziskin, “Human skin permittivity determined by millimeter wave reflection measurements”, Bioelectromagn., vol. 28, pp. 331-339, 2007. [3] T. Wu, T.S. Rappaport,, C.M. Collins, “Safe for generations to come”, IEEE Microw. Mag., vol 16. no. 2, pp. 65-84, Mar. 2015. [4] S. Gabriel, R.W. Lau, C. Gabriel, “The dielectric properties of biological tissues: II. Measurements in the frequency range 10 Hz to 20 GHz”, Phys. Med. Biol., vol. 41, pp. 2251-2269, 1996. [5] M. Zhadobov, C. Leduc, A. Guraliuc, N. Chahat, R. Sauleau, Chapter 5 “Antenna / human body interactions in the 60 GHz band: state of knowledge and recent advances”, State-of-the-art in Body-Centric Wireless Communications and Associated Applications , IET. 9 Human body modeling - Power density PD - power density at the skin surface ( z = 0) −δ2 − δ 0 () = ⋅2/z = ⋅−Γ⋅ 2/ z Γ 2 PDz PDe0 IPD(1 ) e - power reflection coefficient δ - penetration depth Normal Skin can be modeled as a incidence homogenous layer TM TE Oblique incidence M. Zhadobov, C. Leduc, A. Guraliuc, N. Chahat, R. Sauleau, Chapter 5: “Antenna / human body interactions in the 60 GHz band: state of knowledge and recent 10 advances”, State-of-the-art in Body-Centric Wireless Communications and Associated Applications , IET. Antenna module Realized gain [dB] @ 60GHz Ant1 Ant2 10 8.97 8.82 Head effect Geometrical head model : open source CAD file with skin- equivalent properties (ε*_60GHz =7.98-j·10.93) Impact of the human body on the antenna performance 11 Antenna in phone call mode Front Absorbed Module Input power Peak-SAR Peak-IPD power eq position mW W/kg mW/cm 2 mW Front 0.084 9.69 ×10 -8 3.99x10 -9 10 Edge 0.133 3×10 -7 1.24x10 -8 << ICNIRP recommended BRs (1 mW/cm 2 over 20cm 2; 20 mW/cm 2 over 1 cm 2) Edge - Maximum SAR occurs on the user’s ear helix. - Lower exposure is noticed for “Front” case than “Edge” case (“Front”: the antenna radiates towards the base station). - Exposure levels are significantly lower compared to the recommended limits. A.R. Guraliuc, M. Zhadobov, R. Sauleau, L. Marnat, L. Dussopt, “Millimeter-wave exposure from mobile terminals”, 2015 European Conf. on Networks and Commun. 12 (EuCNC 2015), Paris, France, pp. 82-85, June 29-July 2, 2015. Thank You! Cost effective mmW systems leveraging silicon technology and digital manufacturing C. Luxey, F. Gianesello, A. Bisognin, D. Titz, J. Costa, C. Fernandez, C. del Rio Bocio EpoC, University Nice-Sophia Antipolis [email protected] WF03 Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Slide 2 Communications of 53 Introduction • Rapid growth of wireless data drives the development of new technologies: - 5G - Wireless backhaul developments in V/E Bands • Availability of high performance and cost effective antenna is key • To address this need, fundamental enablers lie in manufacturing technologies able to handle complex 3D-Shapes while providing fast and low- cost prototyping as well as the ability to support medium-volume production • This presentation illustrates how 3D-Printing and digital manufacturing technologies might help to develop innovative and cost-effective antenna solutions in order to address new business challenges WF03 Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Slide 3 Communications of 53 Outline • Context and Motivation • Antenna-Solution • 3D-Printed Lens • 3D-Printed Horns • 3D-Printed Reflectors • Future Work • Conclusion WF03 Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Slide 4 Communications of 53 Context & Motivation • Following the growth of mobile devices, global mobile data traffic has exceeded 4200 Petabytes/month in 2nd Q 2015 Source : Ericsson mobility report June 2015 • Peak data rates of 5G will be close to 10 Gbit/s • Cell-edge data rates should be 100 Mbit/s • In order to address consumer demand, the development of high-speed, low-cost and low- power wireless technologies is a key challenge for our industry WF03 Millimetre-Wave Technologies for 5G Mobile Networks and Short-Range Slide 5 Communications of 53 Context & Motivation • Many current 5G researches are dealing with new RF/mmW radio technologies for access in order to increase peak data rates, but do we really need new radio technologiesg for access? ADSL2+ Under deployment VDSL2 Wired Under
Recommended publications
  • The Near-Infrared Multi-Band Ultraprecise Spectroimager for SOFIA
    NIMBUS: The Near-Infrared Multi-Band Ultraprecise Spectroimager for SOFIA Michael W. McElwaina, Avi Mandella, Bruce Woodgatea, David S. Spiegelb, Nikku Madhusudhanc, Edward Amatuccia, Cullen Blaked, Jason Budinoffa, Adam Burgassere, Adam Burrowsd, Mark Clampina, Charlie Conroyf, L. Drake Demingg, Edward Dunhamh, Roger Foltza, Qian Gonga, Heather Knutsoni, Theodore Muencha, Ruth Murray-Clayf, Hume Peabodya, Bernard Rauschera, Stephen A. Rineharta, Geronimo Villanuevaj aNASA Goddard Space Flight Center, Greenbelt, MD, USA; bInstitute for Advanced Study, Princeton, NJ, USA; cYale University, New Haven, CT, USA; dPrinceton University, Princeton, NJ, USA; eUniversity of California, San Diego, La Jolla, CA, USA; fHarvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA; gUniversity of Maryland, College Park, MD, USA; hLowell Observatory, Flagstaff, AZ, USA; iCalifornia Institute of Technology, Pasadena, CA; jCatholic University of America, Washington, DC, USA. ABSTRACT We present a new and innovative near-infrared multi-band ultraprecise spectroimager (NIMBUS) for SOFIA. This design is capable of characterizing a large sample of extrasolar planet atmospheres by measuring elemental and molecular abundances during primary transit and occultation. This wide-field spectroimager would also provide new insights into Trans-Neptunian Objects (TNO), Solar System occultations, brown dwarf atmospheres, carbon chemistry in globular clusters, chemical gradients in nearby galaxies, and galaxy photometric redshifts. NIMBUS would be the premier ultraprecise
    [Show full text]
  • And H-Band Spectra of Globular Clusters in The
    A&A 543, A75 (2012) Astronomy DOI: 10.1051/0004-6361/201218847 & c ESO 2012 ! Astrophysics Integrated J-andH-band spectra of globular clusters in the LMC: implications for stellar population models and galaxy age dating!,!!,!!! M. Lyubenova1,H.Kuntschner2,M.Rejkuba2,D.R.Silva3,M.Kissler-Patig2,andL.E.Tacconi-Garman2 1 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany 3 National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ, 85719 USA Received 19 January 2012 / Accepted 1 May 2012 ABSTRACT Context. The rest-frame near-IR spectra of intermediate age (1–2 Gyr) stellar populations aredominatedbycarbonbasedabsorption features offering a wealth of information. Yet, spectral libraries that include the near-IR wavelength range do not sample a sufficiently broad range of ages and metallicities to allowforaccuratecalibrationofstellar population models and thus the interpretation of the observations. Aims. In this paper we investigate the integrated J-andH-band spectra of six intermediate age and old globular clusters in the Large Magellanic Cloud (LMC). Methods. The observations for six clusters were obtained with the SINFONI integral field spectrograph at the ESO VLT Yepun tele- scope, covering the J (1.09–1.41 µm) and H-band (1.43–1.86 µm) spectral range. The spectral resolution is 6.7 Å in J and 6.6 Å in H-band (FWHM). The observations were made in natural seeing, covering the central 24"" 24"" of each cluster and in addition sam- pling the brightest eight red giant branch and asymptotic giant branch (AGB) star candidates× within the clusters’ tidal radii.
    [Show full text]
  • Stellar Spectra in the Hband
    110 Wing and Jørgensen, JAAVSO Volume 31, 2003 Stellar Spectra in the H Band Robert F. Wing Department of Astronomy, Ohio State University, Columbus, OH 43210 Uffe G. Jørgensen Niels Bohr Institute, and Astronomical Observatory, University of Copenhagen, DK-2100 Copenhagen, Denmark Presented at the 91st Annual Meeting of the AAVSO, October 26, 2002 [Ed. note: Since this paper was given, the AAVSO has placed 5 near-IR SSP-4 photometers with observers around the world; J and H observations of program stars are being obtained and added to the AAVSO International Database.] Abstract The H band is a region of the infrared centered at wavelength 1.65 microns in a clear window between atmospheric absorption bands. Cool stars such as Mira variables are brightest in this band, and the amplitudes of the light curves of Miras are typically 5 times smaller in H than in V. Since the AAVSO is currently exploring the possibility of distributing H-band photometers to interested members, it is of interest to examine the stellar spectra that these photometers would measure. In most red giant stars, the strongest spectral features in the H band are a set of absorption bands due to the CO molecule. Theoretical spectra calculated from model atmospheres are used to illustrate the pronounced flux peak in H which persists over a wide range of temperature. The models also show that the light in the H band emerges from deeper layers of the star’s atmosphere than the light in any other band. 1. Introduction When multicolor photometry in the infrared was first standardized in the 1960s, Harold Johnson and his colleagues acquired filters to match the windows in the atmospheric absorption and named them with letters of the alphabet (Johnson 1966).
    [Show full text]
  • Near–Infrared Classification Spectroscopy: <I>H</I>–Band Spectra of Fundamental MK Standards
    Smith ScholarWorks Astronomy: Faculty Publications Astronomy 11-20-1998 Near–Infrared Classification Spectroscopy: H–band Spectra of Fundamental MK Standards Michael R. Meyer University of Massachusetts Amherst Suzan Edwards Smith College, [email protected] Kenneth H. Hinkle Kitt Peak National Stephen E. Strom University of Massachusetts Amherst Follow this and additional works at: https://scholarworks.smith.edu/ast_facpubs Part of the Astrophysics and Astronomy Commons Recommended Citation Meyer, Michael R.; Edwards, Suzan; Hinkle, Kenneth H.; and Strom, Stephen E., "Near–Infrared Classification Spectroscopy: H–band Spectra of Fundamental MK Standards" (1998). Astronomy: Faculty Publications, Smith College, Northampton, MA. https://scholarworks.smith.edu/ast_facpubs/15 This Article has been accepted for inclusion in Astronomy: Faculty Publications by an authorized administrator of Smith ScholarWorks. For more information, please contact [email protected] THE ASTROPHYSICAL JOURNAL, 508:397È409, 1998 November 20 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. NEAR-INFRARED CLASSIFICATION SPECTROSCOPY: H-BAND SPECTRA OF FUNDAMENTAL MK STANDARDS MICHAEL R. MEYER1 Five College Astronomy Department, University of Massachusetts, Amherst, MA 01003; mmeyer=as.arizona.edu SUZAN EDWARDS Five College Astronomy Department, Smith College, Northampton, MA 01063; edwards=makapuu.ast.smith.edu KENNETH H. HINKLE Kitt Peak NationalObservatory,2 National Optical Astronomy Observatories, Tucson, AZ 85721; hinkle=noao.edu AND STEPHEN E. STROM Five College Astronomy Department, University of Massachusetts, Amherst, MA 01003; sstrom=tsaile.phast.umass.edu Received 1998 April 7; accepted 1998 June 26 ABSTRACT We present a catalog of H-band spectra for 85 stars of approximately solar abundance observed at a resolving power of 3000 with the KPNO Mayall 4 m Fourier Transform Spectrometer.
    [Show full text]
  • The NIR Upgrade to the SALT Robert Stobie Spectrograph
    The NIR Upgrade to the SALT Robert Stobie Spectrograph Andrew I. Sheinis,1,a Marsha J. Wolf,1,b Matthew A. Bershady,1 David A.H. Buckley,2 Kenneth H. Nordsieck,1 Ted B. Williams3 1 University of Wisconsin – Madison, Dept. of Astronomy, 475 N. Charter St., Madison, WI 53706 2 South African Astronomical Observatory, Observatory 7935, South Africa 3 Dept. of Physics and Astronomy, Rutgers University, Piscataway, NJ 08855 ABSTRACT The near infrared (NIR) upgrade to the Robert Stobie Spectrograph (RSS) on the Southern African Large Telescope (SALT), RSS/NIR, extends the spectral coverage of all modes of the visible arm. The RSS/NIR is a low to medium resolution spectrograph with broadband imaging, spectropolarimetric, and Fabry-Perot imaging capabilities. The visible and NIR arms can be used simultaneously to extend spectral coverage from approximately 3200 Å to 1.6 !m. Both arms utilize high efficiency volume phase holographic gratings via articulating gratings and cameras. The NIR camera is designed around a 2048x2048 HAWAII-2RG detector housed in a cryogenic dewar. The Epps optical design of the camera consists of 6 spherical elements, providing sub-pixel rms image sizes of 7.5 " 1.0 !m over all wavelengths and field angles. The exact long wavelength cutoff is yet to be determined in a detailed thermal analysis and will depend on the semi-warm instrument cooling scheme. Initial estimates place instrument limiting magnitudes at J = 23.4 and H(1.4- 1.6 !m) = 21.6 for S/N = 3 in a 1 hour exposure. Keywords: astronomical spectrographs, optical design, near infrared spectroscopy, volume phase holographic gratings, Fabry-Perot imaging, spectropolarimetry 1.
    [Show full text]
  • H-Band Spectroscopic Classification of OB Stars
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server H−Band Spectroscopic Classification of OB Stars R. D. Blum1,T.M.Ramond,P.S.Conti JILA, University of Colorado Campus Box 440, Boulder, CO, 80309 [email protected] [email protected] [email protected] D. F. Figer Division of Astronomy, Department of Physics & Astronomy, University of California, Los Angeles, CA, 90095 fi[email protected] K. Sellgren Department of Astronomy, The Ohio State University 174 W. 18th Ave., Columbus, OH, 43210 [email protected] accepted for publication in the AJ ABSTRACT We present a new spectroscopic classification for OB stars based on H−band (1.5 µmto1.8µm) observations of a sample of stars with optical spectral types. Our initial sample of nine stars demonstrates that the combination of He I 1.7002 µm and H Brackett series absorption can be used to determine spectral types for stars between ∼ O4 and B7 (to within ∼±2 sub–types). We find that the Brackett series exhibits luminosity effects similar to the Balmer series for the B stars. This classification scheme will be useful in studies of optically obscured high mass star forming regions. In addition, we present spectra for the OB stars near 1.1 µmand1.3µm which may be of use in analyzing their atmospheres and winds. Subject headings: infrared: stars — stars: early–type — stars: fundamental parameters 1Hubble Fellow –2– 1. INTRODUCTION OB stars are massive and thus short lived. Because they have short lives, they will be confined to regions relatively close to their birthplaces and will be found close to the Galactic plane.
    [Show full text]
  • Arxiv:Astro-Ph/0501349V1 17 Jan 2005
    DRAFT VERSION SEPTEMBER 10, 2018 Preprint typeset using LATEX style emulateapj v. 10/10/03 MULTI-WAVELENGTH OBSERVATIONS OF THE 2002 OUTBURST OF GX 339–4: TWO PATTERNS OF X-RAY–OPTICAL/NEAR-INFRARED BEHAVIOR JEROEN HOMAN1,2 , MICHELLE BUXTON3,SERA MARKOFF1 ,CHARLES D. BAILYN 3 ,ELISA NESPOLI2, AND TOMASO BELLONI2 Draft version September 10, 2018 ABSTRACT We report on quasi-simultaneous Rossi X-ray Timing Explorer and optical/near-infrared (nIR) observations of the black hole candidate X-ray transient GX 339–4. Our observations were made over a time span of more than eight months in 2002 and cover the initial rise and transition from a hard to a soft spectral state in X-rays. Two distinct patterns of correlated X-ray–optical/nIR behavior were found. During the hard state the optical/nIR and X-ray fluxes correlated well, with a nIR vs. X-ray flux power-law slope similar to that of the correlation found between X-ray and radio fluxes in previous studies of GX 339–4 and other black hole binaries. As the source went through an intermediate state the optical/nIR fluxes decreased rapidly and once it had entered the spectrally soft state, the optical/nIR spectrum of GX 339–4 was much bluer and the ratio of X-ray to nIR flux was higher by a factor of more than 10 compared to the hard state. In the spectrally soft state changes in the nIR preceded those in the soft X-rays by more than two weeks, indicating a disk origin of the nIR emission, and providinga measure of the viscous time scale.
    [Show full text]
  • The Fuv to Near-Ir Morphologies of Luminous Infrared Galaxies in the Goals Sample S
    The Astronomical Journal, 148:111 (15pp), 2014 December doi:10.1088/0004-6256/148/6/111 © 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE FUV TO NEAR-IR MORPHOLOGIES OF LUMINOUS INFRARED GALAXIES IN THE GOALS SAMPLE S. M. Petty1, L. Armus2, V. Charmandaris3,4,5, A. S. Evans6,7, E. Le Floc’h8, C. Bridge9, T. Díaz-Santos2, J. H. Howell2, H. Inami10, A. Psychogyios3, S. Stierwalt6, and J. A. Surace2 1 Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA 2 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA 3 Department of Physics, University of Crete, GR-71003, Heraklion, Greece 4 Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, GR-15236, Penteli, Greece 5 Chercheur Associé, Observatoire de Paris, F-75014, Paris, France 6 Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA 7 National Radio Astronomy Observatory, Charlottesville, VA 22903, USA 8 CEA-Saclay, Orme des Merisiers, Bat. 709, F-91191 Gif-sur-Yvette, France 9 Div. of Physics, Math & Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 10 National Optical Astronomy Observatory, Tucson, AZ, 85719, USA Received 2014 March 31; accepted 2014 August 3; published 2014 October 30 ABSTRACT We compare the morphologies of a sample of 20 luminous infrared galaxies (LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS) in the FUV, B, I, and H bands, using the Gini (G) and M20 parameters to quantitatively estimate the distribution and concentration of flux as a function of wavelength.
    [Show full text]
  • Chapter 17: IR Spectroscopy
    Chapter 17: IR Spectroscopy An important tool of the organic chemist is Infrared Spectroscopy, or IR. IR spectra are acquired on a special instrument, called an IR spectrometer. IR is used both to gather information about the structure of a compound and as an analytical tool to assess the purity of a compound. IR spectra are quick and easy to run, and since the teaching labs are fortunate enough to have four of these instruments, students are encouraged to acquire spectra of compounds made in the laboratory throughout the first and second semesters of the lab course. 17.1 The Electromagnetic Spectrum Infrared refers to that part of the electromagnetic spectrum between the visible and microwave regions. Electromagnetic spectrum refers to the seemingly diverse collection of radiant energy, from cosmic rays to X-rays to visible light to microwaves, each of which can be considered as a wave or particle traveling at the speed of light. These waves differ from each other in the length and frequency (Figure 17-1). Figure 17-1: The electromagnetic spectrum. Frequency, ѵ (nu), is the number of wave cycles that pass through a point in one second. It is measured in Hz, where 1 Hz = 1 cycle/sec. Wavelength, λ (lambda), is the length of one complete wave cycle. It is often measured in cm (centimeters). Wavelength and frequency are inversely related: c c ν = and λ = λ ν 141 Chapter 17: IR Spectroscopy where c is the speed of light, 3 x 10 10 cm/s. Energy is related to wavelength and frequency by the following formulas: hc E = hν = where h is Planck’s constant, 6.6 x 10 -34 J/Hz or Js.
    [Show full text]
  • Chandra Multi-Wavelength Project (Champ). II. First Results of X-Ray Source Properties
    Chandra Multi-wavelength Project (ChaMP). II. First Results of X-ray Source Properties D.-W. Kim, B. J. Wilkes, P. J. Green, R. A. Cameron, J. J. Drake, N. R. Evans, P. Freeman, T. J. Gaetz, H. Ghosh, F. R. Harnden, Jr., M. Karovska, V. Kashyap, P. W. Maksym, P. W. Ratzlaff, E. M., Schlegel, J. D. Silverman, H. D. Tananbaum, and A. A. Vikhlinin (Smithsonian Astrophysical Observatory, Cambridge, MA 02138) August 26, 2003 Abstract The Chandra Multi-wavelength Project (ChaMP) is a wide-area (~14 deg2) survey of serendipitous Chandra X-ray sources, aiming to establish fair statistical samples covering a wide range of -15 -14 characteristics (such as absorbed AGNs, high z clusters of galaxies) at flux levels (fX ~ 10 – 10 erg sec-1 cm-2) intermediate between the Chandra Deep surveys and previous missions. We present the first results of X-ray source properties obtained from the initial sample of 62 observations. The data have been uniformly reduced and analyzed with techniques specifically developed for the ChaMP and then validated by visual examination. Utilizing only near on-axis, bright X-ray sources (to avoid problems caused by incompleteness and the Eddington bias), we derive the Log(N)- Log(S) relation in soft (0.5-2 keV) and hard (2-8 keV) energy bands. The ChaMP data are consistent with previous results of ROSAT, ASCA and Chandra deep surveys. In particular, our data nicely fill in the flux gap in the hard band between the Chandra Deep Field data and the previous ASCA data. We check whether there is any systematic difference in the source density between cluster and non-cluster fields and also search for field-to-field variations, both of which have been previously reported.
    [Show full text]
  • Near–Infrared Classification Spectroscopy: H–Band Spectra of Fundamental MK Standards
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Near–Infrared Classification Spectroscopy: H–band Spectra of Fundamental MK Standards Michael R. Meyer1 Five College Astronomy Department University of Massachusetts Amherst, MA 01003 [email protected] Suzan Edwards Five College Astronomy Department Smith College, Northampton, MA 01063 [email protected] Kenneth H. Hinkle Kitt Peak National Observatory2 National Optical Astronomy Observatories, Tucson, AZ 85721 [email protected] Stephen E. Strom Five College Astronomy Department University of Massachusetts, Amherst, MA 01003 [email protected] 1Current Address: Hubble Fellow, Steward Observatory, The University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721–0065 2Operated by the Association of Universities for Research in Astronomy, Inc. under cooperative agreement with the National Science Foundation. –2– ABSTRACT We present a catalogue of H–band spectra for 85 stars of approximately solar abundance observed at a resolving power of 3000 with the KPNO Mayall 4m FTS. The atlas covers spectral types O7–M5 and luminosity classes I-V as defined on the MK system. We identify both atomic and molecular indices and line–ratios which are temperature and luminosity sensitive allowing spectral classification to be carried out in the H–band. The line ratios permit spectral classification in the presence of continuum excess emission, which is commonly found in pre–main sequence and evolved stars. We demonstrate that with spectra of R = 1000 obtained at SNR > 50 it is possible to derive spectral types within ±2 subclasses for late–type stars.
    [Show full text]
  • The Laser Frequency Comb As a High Precision Wavelength Reference
    The CU/NIST Laser Frequency Comb Calibrator for High-Precision NIR Spectroscopy Steve Osterman1, John Bally1, Scott Diddams2, Frank Quinlan2, Gabriel Ycas2,3 1University of Colorado, Center for Astrophysics and Space Astronomy, Boulder, CO 2National Institute for Sciencde and Technology, Time and Frequency Division, Boulder, CO 3University of Colorado, Department of Physics, Boulder, CO Abstract HARPS, HIRES, etc. have shown the value of high precision spectroscopy for RV planet searches at visible We have developed a broad-band laser frequency comb at NIST to support high-precision H-Band wavelengths, but visible light RV planet searches are best suited to to solar like stars, making detection of spectroscopy at resolutions of 50,000 and higher. We present an overview of laser frequency comb an earth-analog extremely challenging. Alternatively, low mass M Dwarfs are promising subjects but are not technology and detailed capabilities of the existing H-band laser frequency comb. In addition to ground-based J easily observed at visible wavelengths. Precision NIR spectroscopy is becoming a reality with advances in applications, we will discuss the possibility of performing high-precision spectroscopy from the SOFIA aircraft. laser comb technology, making high precision RV studies of low mass stars a possibility. Why look for planets around low mass The Laser Frequency Comb as a High The CU/NIST H-Band Laser Comb stars? Precision Wavelength Reference: ! 250 MHz Er fiber comb (0.002nm/mode at 1550nm) ! Larger RV signature for a given planet mass in the habitable zone ! Two levels of mode filtering increase spacing to 12.5GHz (0.11nm/ ! An LFC represents an ideal wavelength standard: ! Lower mass " Lower temperature mode, or !/"!=15,500 at 1550nm) w/ > 50nm band width ! Dense array of uniformly spaced, uniformly bright lines ! Habitable zone is closer to the host, increasing RV signature ! Post filter non-linear broadening increases band width to 400nm ! Lower host mass increases RV signature ! Frequencies traceable to a fundamental standard.
    [Show full text]