Roadmap of Terahertz Imaging 2021
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Generation of High-Power, Tunable Terahertz Radiation from Laser Interaction with a Relativistic Electron Beam
PHYSICAL REVIEW ACCELERATORS AND BEAMS 20, 050701 (2017) Generation of high-power, tunable terahertz radiation from laser interaction with a relativistic electron beam Zhen Zhang,* Lixin Yan, Yingchao Du, Wenhui Huang, and Chuanxiang Tang Department of Engineering Physics, Tsinghua University, Beijing 100084, China † Zhirong Huang SLAC National Accelerator Laboratory, Menlo Park, California 94025, USA (Received 6 February 2017; published 5 May 2017) We propose a method based on the slice energy spread modulation to generate strong subpicosecond density bunching in high-intensity relativistic electron beams. A laser pulse with periodic intensity envelope is used to modulate the slice energy spread of the electron beam, which can then be converted into density modulation after a dispersive section. It is found that the double-horn slice energy distribution of the electron beam induced by the laser modulation is very effective to increase the density bunching. Since the modulation is performed on a relativistic electron beam, the process does not suffer from strong space charge force or coupling between phase spaces, so that it is straightforward to preserve the beam quality for terahertz (THz) radiation and other applications. We show in both theory and simulations that the tunable radiation from the beam can cover the frequency range of 1–10 THz with high power and narrow-band spectra. DOI: 10.1103/PhysRevAccelBeams.20.050701 I. INTRODUCTION which copropagates with the electron beam inside an undulator can create energy modulation on the scale of High-brightness electron beams have been used to drive the laser wavelength. The energy modulation can be free-electron lasers (FELs) [1–3], high-intensity terahertz converted into density modulation by letting the beam (THz) radiation [4,5], advanced accelerators [6–8] and beyond. -
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 -
High-Power Portable Terahertz Laser Systems
ARTICLES https://doi.org/10.1038/s41566-020-00707-5 High-power portable terahertz laser systems Ali Khalatpour1, Andrew K. Paulsen1, Chris Deimert 2, Zbig R. Wasilewski 2,3,4,5 and Qing Hu 1 ✉ Terahertz (THz) frequencies remain among the least utilized in the electromagnetic spectrum, largely due to the lack of pow- erful and compact sources. The invention of THz quantum cascade lasers (QCLs) was a major breakthrough to bridge the so-called ‘THz gap’ between semiconductor electronic and photonic sources. However, their demanding cooling requirement has confined the technology to a laboratory environment. A portable and high-power THz laser system will have a qualitative impact on applications in medical imaging, communications, quality control, security and biochemistry. Here, by adopting a design strategy that achieves a clean three-level system, we have developed THz QCLs (at ~4 THz) with a maximum operat- ing temperature of 250 K. The high operating temperature enables portable THz systems to perform real-time imaging with a room-temperature THz camera, as well as fast spectral measurements with a room-temperature detector. he terahertz (THz) spectral range (~1–10 THz) is a fertile The range of frequencies in the middle, ~1–10 THz, is the so-called ground for many applications1. For example, in biochemistry, THz gap. The invention of THz quantum cascade lasers (QCLs) THz applications have been developed to explore the bioac- held great promise to bridge this gap10. However, the demanding T 2,3 tivity of chemical compounds and identify protein structures . In cooling requirements for THz QCLs have been a showstopper for astrophysics, there is a plan to launch a suborbital THz observatory, achieving compact and portable systems, confining THz QCL sys- named GUSTO (Galactic/Extragalactic Ultra long Duration Balloon tems to the laboratory environment. -
Red Supergiants As Extragalactic Abundance Probes: Establishing the J-Band Technique
Red Supergiants as Extragalactic Abundance Probes: Establishing the J-Band Technique J. Zachary Gazak Thesis Committee: Rolf Kudritzki (Chair), Josh Barnes, Fabio Bresolin, Ben Davies, Lisa Kewley, John Learned, and John Rayner ABSTRACT We propose to study the metallicity evolution of star forming galaxies and the ex- panding universe by developing, calibrating, and utilizing methods to extract elemental abundances from quantitative spectroscopy of red supergiants (RSGs). The extreme IR luminosities of RSGs allow for spectroscopic observations over extragalactic distances. By observing a population of RSGs in a target galaxy, the current enrichment as a function of spatial position allows insight into the evolution of the galaxy. By bypass- ing current methodologies (which demand spectral resolutions in excess of R=20,000) in favor of newly proposed analysis techniques requiring more modest resolutions of R ∼3000 in the J band (1.15 - 1.23 µm), our observational efficiency will far exceed current standards. With multi-object capable instruments on both Keck and Subaru we can extend what is possible both in terms of objects observed and accessible dis- tances. In recent years, the advent of quantitative spectroscopy of extragalactic blue supergiants has revolutionized how we understand chemical enrichment and extragalac- tic distances while exposing significant drawbacks in the assumptions and calibrations of non-stellar techniques. By extending our knowledge to an additional population we conduct a critical test of the existing techniques, increased confidence and spatial res- olution in metallicity gradients, and expose a rich new source of information on α/Fe abundances. Furthermore, we pose ourselves to fully exploit the capabilities of future telescopes. -
A Plea for a High-Multiplex J-Band Spectrograph @ VLT Alvio Renzini, MOS Workshop, ESO March 910, 2009
A Plea for a high-multiplex J-Band spectrograph @ VLT Alvio Renzini, MOS Workshop, ESO March 910, 2009 Beyond redshift 1.4 life gets hard for spectroscopists starforming weakly SF passive Getting redshifts of red galaxies by looking in the ultraviolet (!) Cimatti et al. 2008 13 GMASS Passive galaxies at <z>=1.6 30 to 60 hours per galaxy Total integration time for this stacked FORS2 spectrum: 480h (!) Getting redshifts of emission-line galaxies using absorption lines An example from zCOSMOS: The VIMOS spectrum of a typical SF galaxy @ z~2 Our Preferred playgroud: BzK-selected galaxies COSMOS Field, sBzK's 1.4<z<2.5 McCracken et al. 2009 pBzK's Today, some z>1.4 Pilot Experiments over the GOODS-South field, using the database from Daddi et al. 2007 stars SFR vs Mass for ~1000 BzK Galaxies SFR from rest- frame UV + extinction correction All mass & SFR data from Daddi et al. 2007! BzK-selected 1.4<z<2.5 galaxies in GOODS-S to KVega < 22 Data from Daddi et al 2007 16% 84% To B=25, the current limit of VIMOS w/ 5h integration, one picks only <~16% of the total SFR at 1.4<z<2.5. The most actively SF galaxies are fainter than B=25 The problem is that more actively SF galaxies are more extincted and with VIMOS we are forced to look at them in the rest-frame UV When Extinction is important, it helps going to the infrared One needs an high- multiplex Near-IR multiobject spectrograph! Getting just to the J band allows to do emission line ([OII]) redshifts Most actively SF galaxies are the brightest in the J band an d passive ones kick in Of course, more massive SF galaxies are more extincted And, again, with VIMOS we are forced to look at them in the most extincted rest-frame UV (!!!) And therefore we lose most of the stellar mass @z~2 in a B-magnitude limited sample, to which we are forced w/ VIMOS Again, going to Just the J band would help enormously! But where, how, and when? The same using 25,707 galaxies at 1.4<z<2.5 in the COSMOS field Star Formation Rate J mag B mag .. -
Advantage of Terahertz Radiation Versus X-Ray to Detect Hidden
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Archive Ouverte en Sciences de l'Information et de la Communication Advantage of terahertz radiation versus X-ray to detect hidden organic materials in sealed vessels Maryelle Bessou, Henri Duday, Jean-Pascal Caumes, Simon Salort, Bruno Chassagne, Alain Dautant, Anne Ziéglé, Emmanuel Abraham To cite this version: Maryelle Bessou, Henri Duday, Jean-Pascal Caumes, Simon Salort, Bruno Chassagne, et al.. Advan- tage of terahertz radiation versus X-ray to detect hidden organic materials in sealed vessels. Optics Communications, Elsevier, 2012, 285 (21-22), pp.4175-4179. 10.1016/j.optcom.2012.07.007. hal- 00731822 HAL Id: hal-00731822 https://hal.archives-ouvertes.fr/hal-00731822 Submitted on 13 Mar 2018 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. Distributed under a Creative Commons Attribution - NonCommercial - ShareAlike| 4.0 International License Advantage of terahertz radiation versus X-ray to detect hidden organic materials in sealed vessels Maryelle Bessou a, Henri Duday a, Jean-Pascal Caumes d, Simon Salort b, Bruno Chassagne b, Alain Dautant c, Anne Zie´gle´ d, Emmanuel Abraham e,n a Univ. -
Radio Emission in Ultracool Dwarfs: the Nearby Substellar Triple System VHS 1256–1257 J
A&A 610, A23 (2018) https://doi.org/10.1051/0004-6361/201732130 Astronomy & © ESO 2018 Astrophysics Radio emission in ultracool dwarfs: The nearby substellar triple system VHS 1256–1257 J. C. Guirado1,2, R. Azulay1,3, B. Gauza4,5,6, M. A. Pérez-Torres7,8, R. Rebolo4,5,9, J. B. Climent1, and M. R. Zapatero Osorio10 1 Departament d’Astronomia i Astrofísica, Universitat de València, C. Dr. Moliner 50, 46100 Burjassot, València, Spain e-mail: [email protected] 2 Observatori Astronòmic, Universitat de València, Parc Científic, C. Catedrático José Beltrán 2, 46980 Paterna, València, Spain 3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 4 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain 5 Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain 6 Departamento de Astronomía, Universidad de Chile, Camino el Observatorio 1515, Casilla 36-D, Las Condes, Santiago, Chile 7 Instituto de Astrofísica de Andalucía (IAA, CSIC), Glorieta de la Astronomía, s/n, 18008 Granada, Spain 8 Departamento de Física Teórica, Facultad de Ciencias, Universidad de Zaragoza, 50009 Zaragoza, Spain 9 Consejo Superior de Investigaciones Científicas, 28006 Madrid, Spain 10 Centro de Astrobiología (CSIC-INTA), Crta. Ajalvir km 4, 28850 Torrejón de Ardoz, Madrid, Spain Received 19 October 2017 / Accepted 1 December 2017 ABSTRACT Aims. With the purpose of investigating the radio emission of new ultracool objects, we carried out a targeted search in the recently discovered system VHS J125601.92–125723.9 (hereafter VHS 1256–1257); this system is composed by an equal-mass M7.5 binary and a L7 low-mass substellar object located at only 15.8 pc. -
Modeling the Near-Infrared Lines of O-Type Stars
A&A 422, 275–288 (2004) Astronomy DOI: 10.1051/0004-6361:20047174 & c ESO 2004 Astrophysics Modeling the near-infrared lines of O-type stars A. Lenorzer1,M.R.Mokiem1,A.deKoter1,andJ.Puls2 1 Astronomical Institute “Anton Pannekoek”, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands 2 Institut f¨ur Astronomie und Astrophysik, Universit¨atssternwarte, Scheinerstr. 1, 81679 M¨unchen, Germany Received 30 January 2004 / Accepted 30 March 2004 Abstract. We use a grid of 30 line-blanketed unified stellar photosphere and wind models for O-type stars; computed with the code in order to evaluate its potential in the near-infrared spectral domain. The grid includes dwarfs, giants and supergiants. We analyse the equivalent width behaviour of the 20 strongest lines of hydrogen and helium in spectral windows that can be observed using ground-based instrumentation and compare the results with observations. Our main findings are that: i) He /He line ratios in the J, H and K bands correlate well with the optical ratio employed in spectral classification, and can therefore be used to determine the spectral type; ii) in supergiant stars the transition from the stellar photosphere to the wind follows a shallower density gradient than the standard approach followed in our models, which can be mimicked by adopting a lower gravity in our prescription of the density stratification; iii) the Brγ line poses a number of peculiar problems which might partly be related to wind clumping; and iv) the Brα line is an excellent mass-loss indicator. For the first and last item we provide quantitative calibrations. -
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. -
Terahertz (Thz) Generator and Detection
Electrical Science & Engineering | Volume 02 | Issue 01 | April 2020 Electrical Science & Engineering https://ojs.bilpublishing.com/index.php/ese REVIEW Terahertz (THz) Generator and Detection Jitao Li#,* Jie Li# School of Precision Instruments and OptoElectronics Engineering, Tianjin University, Tianjin, 300072, China #Authors contribute equally to this work. ARTICLE INFO ABSTRACT Article history In the whole research process of electromagnetic wave, the research of Received: 26 March 2020 terahertz wave belongs to a blank for a long time, which is the least known and least developed by far. But now, people are trying to make up the blank Accepted: 30 March 2020 and develop terahertz better and better. The charm of terahertz wave origi- Published Online: 30 April 2020 nates from its multiple attributes, including electromagnetic field attribute, photon attribute and thermal attribute, which also attracts the attention of Keywords: researchers in different fields and different countries, and also terahertz Terahertz technology have been rated as one of the top ten technologies to change the future world by the United States. The multiple attributes of terahertz make Generation it have broad application prospects in military and civil fields, such as med- Detection ical imaging, astronomical observation, 6G communication, environmental monitoring and material analysis. It is no exaggeration to say that mastering terahertz technology means mastering the future. However, it is because of the multiple attributes of terahertz that the terahertz wave is difficult to be mastered. Although terahertz has been applied in some fields, controlling terahertz (such as generation and detection) is still an important issue. Now- adays, a variety of terahertz generation and detection technologies have been developed and continuously improved. -
24 Electromagnetic Waves.Pdf
CHAPTER 24 | ELECTROMAGNETIC WAVES 861 24 ELECTROMAGNETIC WAVES Figure 24.1 Human eyes detect these orange “sea goldie” fish swimming over a coral reef in the blue waters of the Gulf of Eilat (Red Sea) using visible light. (credit: Daviddarom, Wikimedia Commons) Learning Objectives 24.1. Maxwell’s Equations: Electromagnetic Waves Predicted and Observed • Restate Maxwell’s equations. 24.2. Production of Electromagnetic Waves • Describe the electric and magnetic waves as they move out from a source, such as an AC generator. • Explain the mathematical relationship between the magnetic field strength and the electrical field strength. • Calculate the maximum strength of the magnetic field in an electromagnetic wave, given the maximum electric field strength. 24.3. The Electromagnetic Spectrum • List three “rules of thumb” that apply to the different frequencies along the electromagnetic spectrum. • Explain why the higher the frequency, the shorter the wavelength of an electromagnetic wave. • Draw a simplified electromagnetic spectrum, indicating the relative positions, frequencies, and spacing of the different types of radiation bands. • List and explain the different methods by which electromagnetic waves are produced across the spectrum. 24.4. Energy in Electromagnetic Waves • Explain how the energy and amplitude of an electromagnetic wave are related. • Given its power output and the heating area, calculate the intensity of a microwave oven’s electromagnetic field, as well as its peak electric and magnetic field strengths Introduction to Electromagnetic Waves The beauty of a coral reef, the warm radiance of sunshine, the sting of sunburn, the X-ray revealing a broken bone, even microwave popcorn—all are brought to us by electromagnetic waves. -
Optical Frequency Combs for Stable Radiation in the Microwave, Terahertz and Optical Domains
Optical frequency combs for stable radiation in the microwave, terahertz and optical domains Qudsia Quraishi Department of Physics, University of Colorado Time and Frequency Division, National Institute of Standards and Technology Boulder, CO 1 overview stabilized frequency combs from mode-locked femtosecond lasers provide new opportunities for…. § optical frequency metrology § optical clocks § measuring distance § time & frequency transfer § laboratory tests of fundamental physics § carrier-envelope phase control (key technology for attosecond science) § femtosecond pulse synthesis & arbitrary optical waveform generation § generation of ultralow noise microwaves § new spectroscopic techniques § harmonic generation § coherent control § spread-spectrum secure communications § part of a Nobel Prize! 2 overview stabilized frequency combs from mode-locked femtosecond lasers provide new opportunities for…. § optical frequency metrology § optical clocks § measuring distance § time & frequency transfer § laboratory tests of fundamental physics § carrier-envelope phase control (key technology for attosecond science) § femtosecond pulse synthesis & arbitrary optical waveform generation Jan Hall § generation of ultralow noise microwaves § new spectroscopic techniques § harmonic generation § coherent control Ted Hänsch § spread-spectrum secure communications § part of a Nobel Prize! 2 microwave frequency synthesizers power RF signal carrier frequenc y specifications 250 kHz – 20 GHz + low phase noise 10, 007, 482, 279 GHz Agilent E8257D frequency