DOCSLIB.ORG

Journées De La SF2A 2011 20-23 Juin, Paris Liste Des Abstracts Book of Abstracts

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Journées De La SF2A 2011 20-23 Juin, Paris Liste Des Abstracts Book of Abstracts Journées de la SF2A 2011 20-23 juin, Paris Liste des abstracts Book of abstracts June 16, 2011 Contents Properties of unusual void LSBDs versus cosmological simulations pre- 1 A00 - Séance plénière SF2A 12 dictions : S.A.Pustilnik (SAO, Invited talks ................... 12 N.Arkhyz)J-M.Martin (OdP, Stellar Physics with GAIA : B. Plez . 12 GEPI)Kniazev A.Y. (SAAO, CFHT en route to a new era : Christian Cape Town; SAI, Moscow) . 14 Veillet . 12 Effects of asteroids on the orbital mo- ALMA early science cycle 0 : et après ? tions of terrestrial planets : S. : J. Pety . 12 ALJBAAE, J. SOUCHAY . 14 Quoi de neuf sous le soleil ?Observations Caractérisation orbitale de beta :Pictoris spatiales récentes et perspectives B et conséquences sur les mod- : Frédéric Auchère . 12 èles existants : Hervé Beust, Gael Astrochimie: chimie des origines? : Chauvin, Anne-Marie Lagrange . 15 Louis d’Hendecourt . 12 Le programme Cosmic Vision de l’ESA : 2 A01 - Les Grands Relevés Extragalac- Athena Coustenis . 13 tiques et Cosmologiques 15 Space Time Explorer & Quantum Test Invited talks ................... 15 of the Equivalence principle : A. Extragalactic Science with EMIR/GTC : Landragin & STE-QUEST team . 13 R. Pello & the GOYA collaboration 15 Comptes rendu du colloque RetD INSU Dernières nouvelles des programmes : Pierre Kern . 13 spatiaux en Astronomie- Migration planétaire et couplage migra- Astrophysique : Fabienne tion/accrétion : Aurélien Crida . 13 Casoli . 15 Champs Magnétiques à la surface des Physics of the Accelerating Universe étoiles géantes et supergéantes (PAU) and Dark Energy Survey avec Narval et ESPaDOnS : (DES) : Francisco J Castander- Michel Aurière . 13 PAU collaboration DES collabora- The Spanish Astronomical Society. tion . 15 Present and Future : Emilio J. The QUIJOTE CMB Experiment : Alfaro . 13 Rubino-Martin, for the QUI- Accélération de particules aux chocs non- JOTE Collaboration . 15 relativistes et relativistes : Guy Pelletier . 13 Planck: the largest extragalactic and cosmological survey in the sub- Etude des amas de galaxie par effet SZ millimeter! : G. Lagache, on be- avec Planck : M. Douspis pour la half of the Planck collaboration . 16 collaboration Planck . 14 Construire l’égalité professionnelle en- Review of Herschel HerMES and AT- tre les femmes et les hommes au LAS Results : I. Pérez-Fournon CNRS : Pascale Bukhari . 14 (on behalf of the HerMES and H- ATLAS consortia) . 16 The Virtual Observatory in action : E. Solano . 14 Oral contributions . 16 Poster contributions . 14 The formation of large galactic disks: ECHO : The Exoplanet CHaracteriza- survival or revival? : Hammer . 16 tion Observatory : Beaulieu J.P., Empreintes de l’énergie noire sur la for- Coudé du Forresto V., Ollivier mation des grandes structures : M., ECHO consortium . 14 Vincent Bouillot . 16 1 The Orbital distribution of the satel- Readying ALMA for extragalactic obser- lite galaxies:Cosmological corre- vations : Pere Planesas . 19 lations and Origin : LATIFA The Mass-Size Relation in High Redshift Benjouali, MARIA ANGELES Clusters : Lauriane Delaye, Marc Gómez Flechoso2, and ROSA Huertas-Company, Simona Mei . 19 Doménguez-Tenreiro . 16 The Next Generation CFHT: A Wide- The Effect and Influence of Star For- Field Spectroscopic Facility for mation and Gas Accretion on the the Coming Decade : P. Cote Turbulence in the ISM, on Self- on behalf of the ngCFHT Concept regulation and on the IMF. : Loic Study Team . 19 Le Tiran, Matthew Lehnert . 16 Distinctive rings in the 21-cm signal The Influence of the Environment in of the epoch of reionization : Compact Galaxy Groups : V. Patrick Vonlanthen & Benoît Charmandaris, T. Bitsakis . 17 Semelin . 19 Galaxy & AGN Evolution through Large Redshift Surveys or the Need The DAFT/FADA Survey status and for upgrading VIMOS towards latest results : Guennou L., the NIR : Tresse, Laurence & Adami C., Ulmer M.P., Clowe VIMOS-IR Team . 17 D., Durret F. et al . 19 Non-thermal physics of galaxy clusters : Assessing the masses of black holes in ob- C. Ferrari . 17 scured environments: prospects Tracing a coherent picture of the Cos- for JWST and SPICA : K. mic Star Formation Rate Den- Dasyra, L. Ho, H. Netzer, sity in the past ∼ 12 Gyr with F. Combes, B. Traktenbrot, E. the VVDS Deep and Ultra-Deep Sturm, L. Armus, D. Elbaz . 20 spectroscopic surveys : Cucciati, Querying for heavily obscured AGN Tresse, Ilbert, Le Fevre et al. 17 via high 9.7 micron optical The ALMA capabilities for observing depths:results from the 12- dust settling in protoplanetary micron, GOODS, and FLS disks : Yann Boehler . 17 Spitzer spectroscopic samples. : The Polar Large Telescope, an Infrared K. Dasyra, I. Georgantopoulos, Large Synoptic Survey Telescope E. Rovilos, A. Pope, Y. Wu . 20 : N. Epchtein et le consortium PLT 18 Search and analysis of strong lenses in SC0028-0003 un superamas de galax- large surveys : F. Brault . 20 ies exceptionnel à z ∼ 0.23 pour ’IMAKA: a new powerful survey instru- tester le modèle de collapse grav- ment for CFHT. : Burgarella, itationnel. : Dominique Proust, Cuillandre et al. 20 Gastao Lima-Neto, Laerte Sodré, Mapping local properties and submm Hugo Capelato. 18 excess in nearby galaxies with Properties of LBGs from redshift 4 to Herschel and LABOCA : Maud 6 : Stéphane De BarrosDaniel Galametz, Marcus Albrecht, SchaererDan Stark . 18 Robert Kennicutt, Franck CFHTLS: The Distant Universe : Hervé Bertoldi, Axel Weiss, Bruce Aussel on behalf of the Steering Draine ... 20 Group . 18 Etude des galaxies hôtes des Super- The Next Generation Virgo Cluster Sur- Novae de type Ia dans le projet vey : Mei, Simona; Ferrarese, L. The Nearby SuperNovae Factory & the NGVS team . 18 (SNfactory) : Rigault Mickael . 20 Toward a Universal Formulation of the A new method for the cosmological anal- Halo Mass Function : P.S. ysis of X-ray galaxy cluster sur- Corasaniti, I. Achitouv . 18 veys. : Nicolas Clerc, Marguerite Early-type galaxies: mass-size relation at Pierre et al. 20 z∼1.3 for different environments : A. Raichoor, S. Mei, F. Nakata, Star formation in chemically young Local S. A. Stanford, B. P. Holden, A. Group galaxies : P. Gratier . 21 Rettura, M. Huertas-Company, A new explanation for the Disk of Satel- M. Postman, P. Rosati, J. P. lite : Sylvain Fouquet . 21 Blakeslee, R. Demarco, P. Eisen- Bulge formation patterns in AP3M- hardt, H. Ford, G. Illingworth, M. SPH simulations - questions J. Jee, T. Kodama, M. Tanaka, to be answered by future and R. L. White . 18 extragalactic missions : A. A Bayesian Approach to Gravitational Obreja, R. Domínguez-Tenreiro, Lens Model Selection : Irène M. Doménech-Moral, F. J. Balmès, Pier-Stefano Corasaniti 18 Martínez-Serrano and A. Serna . 21 2 Morphological classification of galaxy A panchromatic study of two pairs of clusters : F. Rostagni, C. Benoist galaxy clusters : Florence Dur- and S. Maurogordato . 22 ret, Tatiana F. Lagana, Markus Clustering of galaxies in the Cosmic Haider, Christophe Adami, Em- Infrared Background : Aurélie manuel Bertin . 24 Pénin, Guilaine Lagache, Olivier The baryon fraction in five galaxy groups Doré . 22 : Nicolas Martinet, Florence Dur- Unveiling the dusty star formation his- ret, Tatiana F. Lagana and Gas- tory of the Universe at z ∼ 2 tao B. Lima Neto . 24 : Laurie Riguccini, Emeric Le Dust-Obscured star formation and the Floc’h, Marc Sauvage . 22 contribution of galaxies escap- Selection, characterization and photo- ing UV/optical selections at z∼2 metric redshift determination for : Laurie Riguccini, Emeric Le QSOs in the ALHAMBRA sur- Floc’h, Olivier Ilbert, Hervé AUs- vey. : Matute, I., Márquez, sel, Mara Salvato, Peter Capak, I., Masegosa, J., del Olmo, Henry McCracken, Jeyhan Kar- A., Perea, J, Husillos, C. + taltepe, Dave Sanders, Nick Scoville 24 ALHMABRA team . 22 The Crab Nebula at high energy: re- Morphological classification of galaxy cent variability and flares : M. clusters : F. Rostagni, C. Benoist Lemoine-Goumard for the Fermi- and S. Maurogordato . 24 LAT collaboration . 22 The universality of galaxy colours and Coincident searches for neutrinos and star formation histories : I. gravitational waves with the Chilingarian, I. Zolotukhin . 24 ANTARES and LIGO/VIRGO Study of physical properties of type Ia detectors : B. Bouhou et al . 22 supernovae and cosmological ap- Results from the first 3 years of opera- plications : comparison between tion of the Supernova Legacy Sur- observations and simulations : vey (SNLS) : Balland, C. and the Flora Cellier-Holzem . 25 SNLS collaboration . 23 On the evolution of the distribution XXL - An overview of the ultimate XMM of baryons in a simulated local extragalactic survey : M. Pierre . 23 group univers : S. Peirani . 25 New diagnostics of Lyman-alpha blobs - implications for massive high- Instrumental calibration of wide field redshift haloes and galaxy forma- imagers. : Francesca Villa tion : Matthew Hayes . 23 (LPNHE) for the SNDice Collab- Poster contributions . 23 oration . 25 Looking for high-redshift galaxies behind SNFactory spectral data : A.Canto, the lensing cluster A2667. : Nico- S.Bongard . 25 las Laporte, Roser Pello, Daniel The ALMA capabilities for observing Schaerer, Johan Richard, Jean- dust settling in protoplanetary Paul Kneib, Frederic Boone . 23 disks : Yann Boehler . 25 A reionization scenario from HII regions merging histories : Jonathan Chardin, Dominique Aubert . 23 3 A02 - Helio et asterosismologie, avancées et perspectives dans le contexte des nou- ”Cinématique du nuage moléculaire en velles missions spatiales et instruments effondrement” : Amaury de Ker- terrestres
Load more

Recommended publications
  • The X-Ray Universe 2011
    THE X-RAY UNIVERSE 2011 27 - 30 June 2011 Berlin, Germany A conference organised by the XMM-Newton Science Operations Centre, European Space Astronomy Centre (ESAC), European Space Agency (ESA) ABSTRACT BOOK Oral Communications and Posters Edited by Andy Pollock with the help of Matthias Ehle, Cristina Hernandez, Jan-Uwe Ness, Norbert Schartel and Martin Stuhlinger Organising Committees Scientific Organising Committee Giorgio Matt (Universit`adegli Studi Roma Tre, Italy) Chair Norbert Schartel (XMM-Newton SOC, Madrid, ESA) Co-Chair M. Ali Alpar (Sabanci University, Istanbul, Turkey) Didier Barret (Centre d’Etude Spatiale des Rayonnements, Toulouse, France) Ehud Behar (Technion Israel Institute of Technology, Haifa, Israel) Hans B¨ohringer (MPE, Garching, Germany) Graziella Branduardi-Raymont (University College London-MSSL, Dorking, UK) Francisco J. Carrera (Instituto de F´ısicade Cantabria, Santander, Spain) Finn E. Christensen (Danmarks Tekniske Universitet, Copenhagen, Denmark) Anne Decourchelle (Commissariat `al’´energie atomique et aux ´energies alternatives, Saclay, France) Jan-Willem den Herder (SRON, Utrecht, The Netherlands) Rosario Gonzalez-Riestra (XMM-Newton SOC, Madrid, ESA) Coel Hellier (Keele University, UK) Stefanie Komossa (MPE, Garching, Germany) Chryssa Kouveliotou (NASA/Marshall Space Flight Center, Huntsville, Alabama, USA) Kazuo Makishima (University of Tokyo, Japan) Sera Markoff (University of Amsterdam, The Netherlands) Brian McBreen (University College Dublin, Ireland) Brian McNamara (University of Waterloo, Canada)
    [Show full text]
  • Weak Lensing Galaxy Cluster Field Reconstruction
    Mon. Not. R. Astron. Soc. 000, 1–12 (2012) Printed 14 October 2018 (MN LATEX style file v2.2) Weak Lensing Galaxy Cluster Field Reconstruction E. Jullo1, S. Pires2, M. Jauzac3 & J.-P. Kneib4;1 1Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France 2Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp-SEDI, Service d’Astrophysique, CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France 3Astrophysics and Cosmology Research Unit, School of Mathematical Sciences, University of KwaZulu-Natal, Durban 4041, South Africa 4LASTRO, Ecole polytechnique fédérale de Lausanne, Suisse Released 2013 Xxxxx XX ABSTRACT In this paper, we compare three methods to reconstruct galaxy cluster density fields with weak lensing data. The first method called FLens integrates an inpainting concept to invert the shear field with possible gaps, and a multi-scale entropy denoising proce- dure to remove the noise contained in the final reconstruction, that arises mostly from the random intrinsic shape of the galaxies. The second and third methods are based on a model of the density field made of a multi-scale grid of radial basis functions. In one case, the model parameters are computed with a linear inversion involving a singular value decomposition. In the other case, the model parameters are estimated using a Bayesian MCMC optimization implemented in the lensing software Lenstool. Methods are compared on simulated data with varying galaxy density fields. We pay particular attention to the errors estimated with resampling. We find the multi-scale grid model optimized with MCMC to provide the best results, but at high computational cost, especially when considering resampling.
    [Show full text]
  • CONDUCTIVE KERATOPLASTY: a RADIOFREQUENCY-BASED TECHNIQUE for the CORRECTION of HYPEROPIA by Marguerite B
    CONDUCTIVE KERATOPLASTY: A RADIOFREQUENCY-BASED TECHNIQUE FOR THE CORRECTION OF HYPEROPIA BY Marguerite B. McDonald MD ABSTRACT Purpose: To evaluate the data on the safety, effectiveness, and stability of conductive keratoplasty (CK), a thermal, radiofrequency- based technique for treating 0.75 to 3.00 diopters (D) of spherical hyperopia. Methods: A prospective, consecutive series, multicenter clinical trial involving 400 hyperopic eyes was conducted by 19 surgeons at 12 centers. The treatment goal was emmetropia. Cohort follow-up was up to 2 years. Results: At 12 months postoperatively, data were available for 97.5% (354/363) of eyes for efficacy variables and 98% (391/400) of eyes for safety variables. A total of 54% of the CK eyes showed 20/20 or better uncorrected visual acuity, and 92% showed 20/40 or better at 12 months. The mean postoperative manifest refractive spherical equivalent was within 0.50 D in 61% and within 1.00 D in 88%. After CK, eyes were approximately 0.50 D myopic at month 1 and effectively emmetropic at 6 months. At 24 months, there was a 20% loss of initial effect. Safety results showed a 2-line loss of best-corrected visual acuity in 2% of the CK-treated eyes. The incidence of induced cylinder of 2.00 D or greater was below 1%. Conclusion: The CK technique corrects low to moderate hyperopia effectively and safely and with acceptable stability. It spares the visual axis, does not require the creation of a large flap, and is not associated with postoperative dry eye. CK has value as an alternative to hyperopic LASIK for patients with hyperopia.
    [Show full text]
  • Soft Tissue Laser Dentistry and Oral Surgery Peter Vitruk, Phd
    Soft Tissue Laser Dentistry and Oral Surgery Peter Vitruk, PhD Introduction The “sound scientific basis and proven efficacy in order to ensure public safety” is one of the main eligibility requirements of the ADA CERP Recognition Standards and Procedures [1]. The outdated Laser Dentistry Curriculum Guidelines [2] from early 1990s is in need of an upgrade with respect to several important laser-tissue interaction concepts such as Absorption Spectra and Hot Glass Tip. This position statement of The American Board of Laser Surgery (ABLS) on soft tissue dentistry and oral surgery is written and approved by the ABLS’s Board of Directors. It focuses on soft tissue ablation and coagulation science as it relates to both (1) photo-thermal laser-tissue interaction, and (2) thermo-mechanical interaction of the hot glass tip with the tissue. Laser Wavelengths and Soft Tissue Chromophores Currently, the lasers that are practically available to clinical dentistry operate in three regions of the electromagnetic spectrum: near-infrared (near-IR) around 1,000 nm, i.e. diode lasers at 808, 810, 940, 970, 980, and 1,064 nm and Nd:YAG laser at 1,064 nm; mid-infrared (mid-IR) around 3,000 nm, i.e. erbium lasers at 2,780 nm and 2,940 nm; and infrared (IR) around 10,000 nm, i.e. CO2 lasers at 9,300 and 10,600 nm. The primary chromophores for ablation and coagulation of oral soft tissue are hemoglobin, oxyhemoglobin, melanin, and water [3]. These four chromophores are also distributed spatially within oral tissue. Water and melanin, for example, reside in the 100-300 µm-thick epithelium [4], while water, hemoglobin, and oxyhemoglobin reside in sub-epithelium (lamina propria and submucosa) [5], as illustrated in Figure 1.
    [Show full text]
  • Remembering Bill Bogardus Photographing the Moon
    Published by the Astronomical League Vol. 71, No. 2 March 2019 REMEMBERING BILL BOGARDUS PHOTOGRAPHING THE MOON 7.20.69 5 YEARS TREASURES OF THE LINDA HALL LIBRARY APOLLO 11 THE COSMIC WEB ONOMY T STR O T A H G E N P I E Contents G O N P I L R E B 4 . Reflector Mail ASTRONOMY DAY Join a Tour This Year! 4 . President’s Corner May 11 & 5 . International Dark-Sky Association From 37,000 feet above the Pacific Total Eclipse Flight: Chile October 5, 2019 6 . Night Sky Network Ocean, you’ll be high above any clouds, July 2, 2019 For a FREE 76-page seeing up to 3¼ minutes of totality in a dark sky that makes the Sun’s corona look 6 . Deep-Sky Objects Astronomy Day Handbook incredibly dramatic. Our flight will de- full of ideas and suggestions, part from and return to Santiago, Chile. 9 . Remembering Bill Bogardus skyandtelescope.com/2019eclipseflight go to: 10 . From Around the League www.astroleague.org Click on "Astronomy Day” African Stargazing Safari Join astronomer Stephen James PAGE 19 13 . Observing Awards Scroll down to "Free O’Meara in wildlife-rich Botswana July 29–August 4, 2019 Astronomy Day Handbook" for evening stargazing and daytime 14 . Basic Small-Scope Lunar Imaging safari drives at three luxury field For more information, contact: camps. Only 16 spaces available! 18 . The Vault of Heaven – Gary Tomlinson Optional extension to Victoria Falls. ̨̨̨̨̨̨̨̨̨̨̨̨̨̨̨Treasures of the Linda Hall Library Astronomy Day Coordinator skyandtelescope.com/botswana2019 [email protected] 24 . The Cosmic Web Iceland Aurorae 27 .
    [Show full text]
  • Is the Butcher-Oemler Effect a Function of the Cluster Redshift? S. Andreon
    THE ASTROPHYSICAL JOURNAL, 516:647È659, 1999 May 10 ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. IS THE BUTCHER-OEMLER EFFECT A FUNCTION OF THE CLUSTER REDSHIFT? S. ANDREON Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy; andreon=na.astro.it AND S. ETTORI Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, England, UK; settori=ast.cam.ac.uk Received 1998 May 29; accepted 1998 December 18 ABSTRACT Using PSPC ROSAT data, we measure the X-ray surface brightness proÐles, size, and luminosity of the Butcher-Oemler (BO) sample of clusters of galaxies. The cluster X-ray size, as measured by the Pet- rosianrg/2 radius, does not change with redshift and is independent of X-ray luminosity. On the other hand, the X-ray luminosity increases with redshift. Considering that fair samples show no evolution, or negative luminosity evolution, we conclude that the BO sample is not formed from the same class of objects observed at di†erent look-back times. This is in conÑict with the usual interpretation of the Butcher-Oemler as an evolutionary (or redshift dependent) e†ect, based on the assumption that we are comparing the same class of objects at di†erent redshifts. Other trends present in the BO sample reÑect selection criteria rather than di†erences in look-back time, as independently conÐrmed by the fact that trends lose strength when we enlarge the sample with an X-rayÈselected sample of clusters. The variety of optical sizes and shapes of the clusters in the Butcher-Oemler sample and the Malmquist-like bias are the reasons for these selection e†ects that mimic the trends usually interpreted as changes due to evolu- tion.
    [Show full text]
  • The Design of the Ali CMB Polarization Telescope Receiver
    The design of the Ali CMB Polarization Telescope receiver M. Salatinoa,b, J.E. Austermannc, K.L. Thompsona,b, P.A.R. Aded, X. Baia,b, J.A. Beallc, D.T. Beckerc, Y. Caie, Z. Changf, D. Cheng, P. Chenh, J. Connorsc,i, J. Delabrouillej,k,e, B. Doberc, S.M. Duffc, G. Gaof, S. Ghoshe, R.C. Givhana,b, G.C. Hiltonc, B. Hul, J. Hubmayrc, E.D. Karpela,b, C.-L. Kuoa,b, H. Lif, M. Lie, S.-Y. Lif, X. Lif, Y. Lif, M. Linkc, H. Liuf,m, L. Liug, Y. Liuf, F. Luf, X. Luf, T. Lukasc, J.A.B. Matesc, J. Mathewsonn, P. Mauskopfn, J. Meinken, J.A. Montana-Lopeza,b, J. Mooren, J. Shif, A.K. Sinclairn, R. Stephensonn, W. Sunh, Y.-H. Tsengh, C. Tuckerd, J.N. Ullomc, L.R. Valec, J. van Lanenc, M.R. Vissersc, S. Walkerc,i, B. Wange, G. Wangf, J. Wango, E. Weeksn, D. Wuf, Y.-H. Wua,b, J. Xial, H. Xuf, J. Yaoo, Y. Yaog, K.W. Yoona,b, B. Yueg, H. Zhaif, A. Zhangf, Laiyu Zhangf, Le Zhango,p, P. Zhango, T. Zhangf, Xinmin Zhangf, Yifei Zhangf, Yongjie Zhangf, G.-B. Zhaog, and W. Zhaoe aStanford University, Stanford, CA 94305, USA bKavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94305, USA cNational Institute of Standards and Technology, Boulder, CO 80305, USA dCardiff University, Cardiff CF24 3AA, United Kingdom eUniversity of Science and Technology of China, Hefei 230026 fInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049 gNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 hNational Taiwan University, Taipei 10617 iUniversity of Colorado Boulder, Boulder, CO 80309, USA jIN2P3, CNRS, Laboratoire APC, Universit´ede Paris, 75013 Paris, France kIRFU, CEA, Universit´eParis-Saclay, 91191 Gif-sur-Yvette, France lBeijing Normal University, Beijing 100875 mAnhui University, Hefei 230039 nArizona State University, Tempe, AZ 85004, USA oShanghai Jiao Tong University, Shanghai 200240 pSun Yat-Sen University, Zhuhai 519082 ABSTRACT Ali CMB Polarization Telescope (AliCPT-1) is the first CMB degree-scale polarimeter to be deployed on the Tibetan plateau at 5,250 m above sea level.
    [Show full text]
  • The QUIJOTE CMB Experiment: Status and First Results with the Multi-Frequency Instrument
    The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument M. L´opez-Caniegoa, R. Rebolob;c;h, M. Aguiarb, R. G´enova-Santosb;c, F. G´omez-Re~nascob, C. Gutierrezb, J.M. Herrerosb, R.J. Hoylandb, C. L´opez-Caraballob;c, A.E. Pelaez Santosb;c, F. Poidevinb, J.A. Rubi~no-Mart´ınb;c, V. Sanchez de la Rosab, D. Tramonteb, A. Vega-Morenob, T. Viera-Curbelob, R. Vignagab, E. Mart´ınez-Gonzaleza, R.B. Barreiroa, B. Casaponsa a, F.J. Casasa, J.M. Diegoa, R. Fern´andez-Cobosa, D. Herranza, D. Ortiza, P. Vielvaa, E. Artald, B. Ajad, J. Cagigasd, J.L. Canod, L. de la Fuented, A. Mediavillad, J.V. Ter´and, E. Villad, L. Piccirilloe, R. Battyee, E. Blackhurste, M. Browne, R.D. Daviese, R.J. Davise, C. Dickinsone, K. Graingef , S. Harpere, B. Maffeie, M. McCulloche, S. Melhuishe, G. Pisanoe, R.A. Watsone, M. Hobsonf , A. Lasenbyf;g, R. Saundersf , and P. Scottf aInstituto de F´ısica de Cantabria, CSIC-UC, Avda. los Castros, s/n, E-39005 Santander, Spain bInstituto de Astrof´ısica de Canarias, C/Via Lactea s/n, E-38200 La Laguna, Tenerife, Spain cDepartamento de Astrof´ısica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain dDepartamento de Ingenier´ıade COMunicaciones (DICOM), Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain eJodrell Bank Centre for Astrophysics, University of Manchester, Oxford Rd, Manchester M13 9PL, UK f Astrophysics Group, Cavendish Laboratory, University of Cambridge, Cambridge CB3 0HE, UK gKavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA hConsejo Superior de Investigaciones Cient´ıficas, Spain arXiv:1401.4690v2 [astro-ph.IM] 5 Feb 2014 The QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment is designed to observe the polar- ization of the Cosmic Microwave Background and other Galactic and extragalactic signals at medium and large angular scales in the frequency range of 10{40 GHz.
    [Show full text]
  • X-Ray Calibration of SZ Scaling Relations with the ACCEPT
    Mon. Not. R. Astron. Soc. 000, 1–10 (2011) Printed 11 October 2018 (MN LATEX style file v2.2) X-ray calibration of SZ scaling relations with the ACCEPT catalogue of galaxy clusters observed by Chandra B. Comis1⋆, M. De Petris1, A. Conte1, L. Lamagna1 and S. De Gregori1 1Sapienza University of Rome, Department of Physics, P.le A. Moro, 2 Rome, Italy Accepted for publication in MNRAS ABSTRACT We explore the scaling relation between the flux of the Sunyaev-Zel’dovich (SZ) ef- fect and the total mass of galaxy clusters using already reduced Chandra X-ray data present in the ACCEPT (Archive of Chandra Cluster Entropy Profile Tables) cata- logue. The analysis is conducted over a sample of 226 objects, examining the relatively small scale corresponding to a cluster overdensity equal to 2500 times the critical density of the background universe, at which the total masses have been calculated exploiting the hydrostatic equilibrium hypothesis. Core entropy (K0) is strongly corre- lated with the central cooling time, and is therefore used to identify cooling-core (CC) objects in our sample. Our results confirm the self-similarity of the scaling relation between the integrated Comptonization parameter (Y ) and the cluster mass, for both CC and NCC (non-cooling-core) clusters. The consistency of our calibration with re- cent ones has been checked, with further support for Y as a good mass proxy. We also investigate the robustness of the constant gas fraction assumption, for fixed overden- sity, and of the YX proxy (Kravtsov et al. 2007) considering CC and NCC clusters, again sorted on K0 from our sample.
    [Show full text]
  • Calibration of a Polarimetric Microwave Radiometer Using a Double Directional Coupler
    remote sensing Article Calibration of a Polarimetric Microwave Radiometer Using a Double Directional Coupler Luisa de la Fuente 1,* , Beatriz Aja 1 , Enrique Villa 2 and Eduardo Artal 1 1 Departamento de Ingeniería de Comunicaciones, Universidad de Cantabria, 39005 Santander, Spain; [email protected] (B.A.); [email protected] (E.A.) 2 IACTEC, Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain; [email protected] * Correspondence: [email protected] Abstract: This paper presents a built-in calibration procedure of a 10-to-20 GHz polarimeter aimed at measuring the I, Q, U Stokes parameters of cosmic microwave background (CMB) radiation. A full-band square waveguide double directional coupler, mounted in the antenna-feed system, is used to inject differently polarized reference waves. A brief description of the polarimetric microwave radiometer and the system calibration injector is also reported. A fully polarimetric calibration is also possible using the designed double directional coupler, although the presented calibration method in this paper is proposed to obtain three of the four Stokes parameters with the introduced microwave receiver, since V parameter is expected to be zero for the CMB radiation. Experimental results are presented for linearly polarized input waves in order to validate the built-in calibration system. Keywords: radiometer; polarimeter calibration; microwave polarimeter; radiometer calibration; radio astronomy receiver; cosmic microwave background receiver; Stokes parameters Citation: de la Fuente, L.; Aja, B.; Villa, E.; Artal, E. Calibration of a 1. Introduction Polarimetric Microwave Radiometer Remote sensing applications employ sensitive instruments to fulfill the scientific goals Using a Double Directional Coupler. of dedicated missions or projects, either space or terrestrial.
    [Show full text]
  • Wide-Survey of the QUIJOTE CMB Experiment Presented By: Federica Guidi (IAC, ULL), on Behalf of the QUIJOTE Collaboration
    Wide-survey of the QUIJOTE CMB experiment Presented by: Federica Guidi (IAC, ULL), on behalf of the QUIJOTE collaboration. I present the status and the recent results of the QUIJOTE (Q-U-I JOint TEnerife) experiment. QUIJOTE is a project that operates from the Teide Observatory, with the aim to characterize the emission of the galactic foregrounds at microwave wavelengths, and to study the polarization of the Cosmic Microwave Background, targeting the detection of the primordial gravitational waves, the so called ”B-modes”, down to a value of the tensor to scalar ratio of r = 0.05. Recently, one of the two instruments of QUIJOTE, the Multi Frequency Instrument (MFI), concluded a wide-survey campaign, during which we observed the full northern sky, at 11, 13, 17 and 19 GHz. The wide survey maps of QUIJOTE will be delivered soon to the community. Here I present the current status of the maps, and I summarize few scientific results related to them, with special emphasis on the low frequency Galactic foregrounds, such as the Synchrotron and the Anomalous Microwave Emission. XIV.0 Reunión Científica 13-15 julio 2020 Context of the research: QUIJOTE: a polarimetric CMB experiment for the characterization of the low frequency galactic foregrounds ● CMB polarization experiments are searching for the polarization pattern imprinted by primordial gravitational waves: the “B-modes”. ● QUIJOTE is a polarimetric CMB experiment installed at the Teide observatory since 2012. ● QUIJOTE extends the Planck and WMAP coverage to low frequency, with two instruments: ○ Multi Frequency Instrument (MFI): 11, 13, 17, 19 GHz; ○ Thirty and Forty GHz Instrument (TFGI): Q Q Q Q J J 30-40 GHz.
    [Show full text]
  • Galaxy Data Name Constell
    Galaxy Data name constell. quadvel km/s z type width ly starsDist. Satellite Milky Way many many 0 0.0000 SBbc 106K 200M 0 M31 Andromeda NQ1 -301 -0.0010 SA 220K 1T 2.54Mly M32 Andromeda NQ1 -200 -0.0007 cE2 Sat. 5K 2.49Mly M31 M110 Andromeda NQ1 -241 -0.0008 dE 15K 2.69M M31 NGC 404 Andromeda NQ1 -48 -0.0002 SA0 no 10M NGC 891 Andromeda NQ1 528 0.0018 SAb no 27.3M NGC 680 Aries NQ1 2928 0.0098 E pec no 123M NGC 772 Aries NQ1 2472 0.0082 SAb no 130M Segue 2 Aries NQ1 -40 -0.0001 dSph/GC?. 100 5E5 114Kly MW NGC 185 Cassiopeia NQ1 -185 -0.0006dSph/E3 no 2.05Mly M31 Dwingeloo 1 Cassiopeia NQ1 110 0.0004 SBcd 25K 10Mly Dwingeloo 2 Cassiopeia NQ1 94 0.0003Iam no 10Mly Maffei 1 Cassiopeia NQ1 66 0.0002 S0pec E3 75K 9.8Mly Maffei 2 Cassiopeia NQ1 -17 -0.0001 SABbc 25K 9.8Mly IC 1613 Cetus NQ1 -234 -0.0008Irr 10K 2.4M M77 Cetus NQ1 1177 0.0039 SABd 95K 40M NGC 247 Cetus NQ1 0 0.0000SABd 50K 11.1M NGC 908 Cetus NQ1 1509 0.0050Sc 105K 60M NGC 936 Cetus NQ1 1430 0.0048S0 90K 75M NGC 1023 Perseus NQ1 637 0.0021 S0 90K 36M NGC 1058 Perseus NQ1 529 0.0018 SAc no 27.4M NGC 1263 Perseus NQ1 5753 0.0192SB0 no 250M NGC 1275 Perseus NQ1 5264 0.0175cD no 222M M74 Pisces NQ1 857 0.0029 SAc 75K 30M NGC 488 Pisces NQ1 2272 0.0076Sb 145K 95M M33 Triangulum NQ1 -179 -0.0006 SA 60K 40B 2.73Mly NGC 672 Triangulum NQ1 429 0.0014 SBcd no 16M NGC 784 Triangulum NQ1 0 0.0000 SBdm no 26.6M NGC 925 Triangulum NQ1 553 0.0018 SBdm no 30.3M IC 342 Camelopardalis NQ2 31 0.0001 SABcd 50K 10.7Mly NGC 1560 Camelopardalis NQ2 -36 -0.0001Sacd 35K 10Mly NGC 1569 Camelopardalis NQ2 -104 -0.0003Ibm 5K 11Mly NGC 2366 Camelopardalis NQ2 80 0.0003Ibm 30K 10M NGC 2403 Camelopardalis NQ2 131 0.0004Ibm no 8M NGC 2655 Camelopardalis NQ2 1400 0.0047 SABa no 63M Page 1 2/28/2020 Galaxy Data name constell.
    [Show full text]