CURRICULUM VITÆ Rychard J. Bouwens
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Dwarf Galaxies: Probes for Galaxy Formation and Evolution
JD2 Dwarf Galaxies: Probes for Galaxy Formation and Evolution Chairpersons and Editors: E. Brinks &; T. X. Thuan Downloaded from https://www.cambridge.org/core. IP address: 170.106.40.139, on 30 Sep 2021 at 22:48:50, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S1539299600020074 MULTI-SPECTRAL STUDIES OF THE NEARBY DWARF GALAXIES UGCA86 AND LMC/SMC G. M. RICHTER Astrophysikalisches Institut Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany gmrichter@aip. de M. BRAUN ESA-VILSPA ISOPHOT IDT Villafranca del Castillo, Satellite Tracking Station Apartado 50727, E-28080 Madrid, Spain [email protected] AND R. ASSENDORP Astrophysikalisches Institut Potsdam An der Sternwarte 16, D-14482 Potsdam, Germany rassendorp @aip. de 1. Background UGCA 86 is an irregular dwarf galaxy in the IC 342 / Maffei I group, just next to the Local Group. It was first mentioned by Zwicky (1968) as VII Zw 009, but not contained in his "Catalogue of Selected Compact Galaxies and of Post-eruptive Galaxies" (1971). It was independently rediscovered by Nilson (1974) and Rots (1979) as UGCA 86 and A 0355 resp. Rots found it by HI observations, and from peculiarities in the HI morphology and kinematics he suspected that it was interacting with IC 342. Thus, the tentatively interesting items: a starforming, low surface brightness dwarf galaxy in an interacting system (one of the nearest), triggered us to engage in more detailed studies. In a first step, we made detailed surface photometry in U, B and V (Richter et al. -
Publications for Dr. Peter L. Capak 1 of 21 Publication Summary 369
Publications for Dr. Peter L. Capak Publication Summary 369 Publications 319 Refereed Publications Accepted or Submitted 50 Un-refereed Publications Top 1% of Cited Researchers in 2017-2019 >30,000 Citations >1,600 Citations on first author papers 99 papers with >100 citations, 6 as first author. H Index = 99 First Author publications 1) Capak et al., 2015, “Galaxies at redshifts 5 to 6 with systematically low dust content and high [C II] emission”, Nature, 522, 455 2) Capak et al., 2013, “Keck-I MOSFIRE Spectroscopy of the z ~ 12 Candidate Galaxy UDFj-39546284”, ApJL, 733, 14 3) Capak et al., 2011, “A massive protocluster of galaxies at a redshift of z~5.3” , Nature, 470, 233 4) Capak et al., 2010, “Spectroscopy and Imaging of three bright z>7 candidates in the COSMOS survey”, ApJ, 730, 68 5) Capak et al., 2008, "Spectroscopic Confirmation Of An Extreme Starburst At Redshift 4.547", ApJL, 681, 53 6) Capak et. al., 2007, "The effects of environment on morphological evolution between 0<z<1.2 in the COSMOS Survey", ApJS, 172, 284 7) Capak et. al., 2007, "The First Release COSMOS Optical and Near-IR Data and Catalog", ApJS, 172, 99 8) Capak, 2004, “Probing global star and galaxy formation using deep multi-wavelength surveys”, Ph.D. Thesis 9) Capak et. al., 2004, "A Deep Wide-Field, Optical, and Near-Infrared Catalog of a Large Area around the Hubble Deep Field North", AJ, 127, 180 Other Publications (P. Capak was a leading author in bolded entries) 10) Faisst et al., 2020, “The ALPINE-ALMA [CII] survey: Multi-Wavelength Ancillary Data. -
Mathématiques Et Espace
Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée. -
Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born. -
CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, -
Science in the Urantia Papers
Science ¾ Scientific Validation of the UB z By Denver Pearson z By Phil Calabrese ¾ Seraphic Velocities ¾ Astronomy The Scientific Integrity of the Urantia Book by Denver Pearson As scientifically minded readers first peruse the Urantia Book, it soon occurs to them that many of its statements on the natural sciences conflict with currently held data and theories. In the minds of many this gives rise to doubts about the truthfulness of those statements. Wisdom would lead us to realize that nothing short of perfection is perfect, and anything touched by human hands has fingerprints. This should be our guiding thoughts as we contemplate the accuracy of the scientific content of the Urantia Papers. Several years ago, at the first scientific symposium, it was implied by one of the speakers that the revelation contains errors. This implication is alarming. More recently, at the second symposium held in Oklahoma, an interesting publication named "The Science Content of The Urantia Book" was made available (this document is obtainable from the Brotherhood of Man Library). In this publication is an article entitled "Time Bombs" in which the author suggests that the revelators planted certain inaccurate scientific statements in the book in order to prevent it from becoming a fetish. He states "...the revelators incorporated safeguards in the papers that would form The Urantia Book to diminish the tendency to regard it as an object of worship. What safeguards did they use? Suppose they decided to make sure that mortals reading it understood that some cosmological statements in the book would be found to be inaccurate". -
Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆
A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis. -
Highlights and Discoveries from the Chandra X-Ray Observatory1
Highlights and Discoveries from the Chandra X-ray Observatory1 H Tananbaum1, M C Weisskopf2, W Tucker1, B Wilkes1 and P Edmonds1 1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138. 2 NASA/Marshall Space Flight Center, ZP12, 320 Sparkman Drive, Huntsville, AL 35805. Abstract. Within 40 years of the detection of the first extrasolar X-ray source in 1962, NASA’s Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond X-ray images with 100-200 eV energy resolution for energies in the range 0.08<E<10 keV, locating X-ray sources to high precision, detecting extremely faint sources, and obtaining high resolution spectra of selected cosmic phenomena. The extended Chandra mission provides a long observing baseline with stable and well-calibrated instruments, enabling temporal studies over time-scales from milliseconds to years. In this report we present a selection of highlights that illustrate how observations using Chandra, sometimes alone, but often in conjunction with other telescopes, have deepened, and in some instances revolutionized, our understanding of topics as diverse as protoplanetary nebulae; massive stars; supernova explosions; pulsar wind nebulae; the superfluid interior of neutron stars; accretion flows around black holes; the growth of supermassive black holes and their role in the regulation of star formation and growth of galaxies; impacts of collisions, mergers, and feedback on growth and evolution of groups and clusters of galaxies; and properties of dark matter and dark energy. -
Quarterly Report, July
NATIONAL RADIO ASTRONOMY OBSERVATORY Quarterly Report July – September 2005 Cover Image: The First Prize image from the NRAO/AUI 2005 Image Contest. Table of Contents Executive Summary ..................................................................................... 1 Science Highlights........................................................................................ 4 NAASC .......................................................................................................... 6 Expanded Very Large Array....................................................................... 8 Green Bank Telescope................................................................................ 16 Very Large Array and Very Long Baseline Array ................................. 26 Central Development Laboratory ............................................................ 37 Computer and Information Services ....................................................... 51 Education and Public Outreach ............................................................... 54 Environment, Safety, and Security .......................................................... 59 Telescope Usage ......................................................................................... 62 GBT Observing Programs ......................................................................... 63 VLA Observing Programs......................................................................... 76 VLBA Observing Programs ..................................................................... -
The Brightest Stars Seite 1 Von 9
The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10. -
Mo Ab H Appenings
MOAB HAPPENINGS Volume 25 Number 11 FEBRUARY 2014 Come visit us at 225 S. Main Street YOUTH CLIMBING & CANYONEERING ADULTS (under 16) YOUTH RIVER ADVENTURES ADULTS (under 16) EPHEDRAS GROTTO CANYONEERING $ $ FULL-DAY RIVER ADVENTURE Excellent canyoneering intro gives you access to seldom ...... 99...... 84...... World-famous scenery and a barbecue lunch rafting the ...... $ $ seen canyons with exciting rappels! 4 hrs (min age: 10) 85 ...... 65 ...... Colorado River. 8:15am – 4:00pm (min age: 5) . DESERT ROCK CLIMBING COLORADO RIVER A.M. HALF-DAY Climbing, instruction, and fun on rope and rock! All $ $ ...... 99...... 84...... Raft the river from Fisher Towers to Rocky Rapid. equipment provided. 5 hrs (min age: 5) . $ $ ...... ...... 54 44 ...... 8:15am – 12:30pm (min age: 5) . HIGH ROPES COURSE COLORADO RIVER P.M. HALF-DAY Challenge course, safety gear & instruction, and Raft from Rocky Rapid to Takeout. Includes BBQ lunch $ $ ...... ...... southern Utah’s highest swing! 2 hrs (min age: 10) ...... 60 50 . $ $ ...... ...... 65 55 ...... along the river. 11:00am – 4:00pm (min age: 5) . WESTWATER CANYON FULL-DAY Enjoy exciting whitewater rapids & lunch in this unique FLIGHTS & HORSEBACK ADULTS YOUTH $ $ ...... ...... Canyon. 7:30am – 6:00pm (min age: 10) ...... 175 175 . HOT AIR BALLOON RIDES TWO-DAY RAFT & CAMP Soar over the sandstone valleys and spires of Moab All meals and camping equipment provided, rafting $ $ ...... ...... from an unforgettable perspective. (Approx 3.5 hours) ...... 259 259 . $ $ ...... ...... moderate rapids, relax into the scenery. (min age: 5) 255 185 ...... CANYONLANDS SCENIC FLIGHT See all 4 districts of Canyonlands NP in just one hour $ $ ...... ...... ® YOUTH ...... 173 173 . HUMMER SAFARIS ADULTS (under 16) with a bird’s eye view! Departs 9am . -
Prof. Scott Christopher Chapman Current Address: Dalhousie University Dept
CURRICULUM VITAE Name: Prof. Scott Christopher Chapman Current Address: Dalhousie University Dept. of Physics and Atmospheric Science Coburg Road Halifax, B3H1A6, Canada Phone: (902) 494 2370 Fax: (902) 494 2377 e-mail: [email protected] Citizenship: Canadian Birthdate: May 13, 1971 Work/Educational Background 08/2012{present Dalhousie University Professor in Astrophysics 06/2011{08/2012 University of Cambridge, IoA Professor in Astrophysics 10/2007{05/2011 University of Cambridge, IoA Reader, Associate Professor in Astrophysics 06/2006{10/2007 University of Victoria Adjunct assistant professor, Canadian Space Agency Fellow (6 months deferred for parental leave) 06/2001{01/2006 California Institute of Technology Senior Postdoctoral Fellow 05/1999{06/2001 Carnegie Observatories Magellan Fellow 10/1996{09/1999 University of British Columbia PhD, supervisors: Gordon Walker, Simon Morris \The nature of active galaxies" 09/1995{10/1996 University of British Columbia MSc, supervisor: Gordon Walker \A precisely aligned CCD mosaic for astronomy" 09/1990{05/1995 University of British Columbia BSc (Honours Physics/Math) 09/1988{05/1990 Van. Academy of Music/ Diploma (violin performance, minor: philosophy) Simon Fraser University Grants and Awards (totaling over US$3mil) 2012 PI CFI - Leaders Opportunity Fund (Dalhousie) 5 years 2012 PI NSERC - Discovery grant (Dalhousie) 5 years 2012 PI Dalhousie faculty startup grant 2009 CoI Cambridge, IoA Observational Rolling Grant \Obscured star formation at high-z" 2008 PI Spitzer research grant, cycle