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The Wigglez Dark Energy Survey: Probing the Epoch of Radiation Domination Using Large-Scale Structure
MNRAS 429, 1902–1912 (2013) doi:10.1093/mnras/sts431 The WiggleZ Dark Energy Survey: probing the epoch of radiation domination using large-scale structure Gregory B. Poole,1,2‹ Chris Blake,1 David Parkinson,3 Sarah Brough,4 Matthew Colless,4 Carlos Contreras,1 Warrick Couch,1 Darren J. Croton,1 Scott Croom,5 Tamara Davis,3 Michael J. Drinkwater,3 Karl Forster,6 David Gilbank,7 Mike Gladders,8 Karl Glazebrook,1 Ben Jelliffe,5 Russell J. Jurek,9 I-hui Li,10 Barry Madore,11 D. Christopher Martin,6 Kevin Pimbblet,12 Michael Pracy,1,13 4,13 1,14 15 Rob Sharp, Emily Wisnioski, David Woods, Downloaded from Ted K. Wyder6 and H. K. C. Yee10 1Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia 2School of Physics, University of Melbourne, Parksville, VIC 3010, Australia 3School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, Australia 4Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia http://mnras.oxfordjournals.org/ 5Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia 6California Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USA 7South African Astronomical Observatory, PO Box 9, 7935 Observatory, Cape Town, South Africa 8Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA 9Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia 10Department of Astronomy and Astrophysics, -
The Wigglez Dark Energy Survey
The WiggleZ Dark Energy Survey Chris Blake (Swinburne University) Sarah Brough, Warrick Couch, Karl Glazebrook, Greg Poole (Swinburne University); Tamara Davis, Michael Drinkwater, Russell Jurek, Kevin Pimbblet (Uni. of Queensland); Matthew Colless, Rob Sharp (Anglo-Australian Observatory); Scott Croom (University of Sydney); Michael Pracy (Australian National University); David Woods (University of New South Wales); Barry Madore (OCIW); Chris Martin, Ted Wyder (Caltech) Abstract: The accelerating expansion rate of the Universe, attributed to “dark energy”, has no accepted theoretical explanation. The origin of this phenomenon unambiguously implicates new physics via a novel form of matter exerting neg- ative pressure or an alteration to Einstein’s General Relativity. These profound consequences have inspired a new generation of cosmological surveys which will measure the influence of dark energy using various techniques. One of the forerun- ners is the WiggleZ Survey at the Anglo-Australian Telescope, a new large-scale high-redshift galaxy survey which is now 50% complete and scheduled to finish in 2010. The WiggleZ project is aiming to map the cosmic expansion history using delicate features in the galaxy clustering pattern imprinted 13.7 billion years ago. In this article we outline the survey design and context, and predict the likely science highlights. Figure 1: Caption: The distribution of galaxies currently observed in the three WiggleZ Survey fields located near the Northern Galactic Pole. The observer is situated at the origin of the co-ordinate system. The radial distance of each galaxy from the origin indicates the observed redshift, and the polar angle indicates the galaxy right ascension. The faint patterns of galaxy clustering are visible in each field. -
The H-Index in Australian Astronomy
Addenda: The h-index in Australian Astronomy Kevin A. PimbbletA,B A School of Physics, Monash University, Clayton, VIC 3800, Australia B Email: [email protected] Abstract: Pimbblet (2011) published an evaluation of the Hirsch h-index in the context of the Aus- tralian astronomical community. This addenda adds treatment of changes of surname to the compu- tation of the h-index and presents derivative data on the m-index. Keywords: Errata, Addenda 1 Change of Surname Table 1: Top 10 h-index for Australian Astron- Pimbblet (2011) published a variety of analyses on the omy, excluding overseas professionals with correc- h-index (e.g. Hirsch 2005) in the context of Australian tion applied for surname changes. Astronomy. Alongside that, a discussion of a number Rank Name h of caveats was also made. One further caveat merits =1 KenFREEMAN 77 explicit attention in the interpretation of the h-index: =1 JeremyMOULD 77 changes of surname. In the Pimbblet (2011) analysis, 3 Karl GLAZEBROOK 71 no attempt was made to track surname changes. This 4 Dick MANCHESTER 68 has the effect of depressing the h-index of individuals 5 MichaelDOPITA 64 who have changed their names over the years. Its effect can readily be seen in Table 1 where we re-compute the 6 Warrick COUCH 61 top ten h-index for Australian Astronomy and account 7 Joss BLAND-HAWTHORN 57 for changing surnames: Bland-Hawthorn’s previous h- 8 MatthewCOLLESS 56 index was suppressed by 4 points by not taking this in 9 Brian SCHMIDT 54 to account. We emphasize that the same dataset was 10 MikeBESSELL 53 used for this re-computation as the original paper. -
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 -
The James Webb Space Telescope: Mission Overview and Status
The James Webb Space Telescope: Mission Overview and Status Matthew A. Greenhouse and the JWST Science Working Group' Goddard Space Flight Center Code 443.2 Greenbelt, MD 20771 USA Abstract- The James Webb Space Telescope (JWST) is the Infrared The lWST architecture is prinuirily shaped by successor to tbe Hubble Space Telescope. It is a cryogenic infrared 2 requirements associated with answering the above questions. space observatory with • 25 m aperture (6 m class) telescope In contrast to the Hubble Space Telescope (HST), the lWST yielding diffraction limited IIDgular resolution at a wave1engtll of :z is designed as an infrared optimized telescope to observe um. The science instrument payload includes three passively cooled near-infrared instruments providing broad- and narrow-band the redshifted ultraviolet radiation from the first galaxies imagery, coronagraphy, as well as mulu-Gbject and Integral-field and supernovae of the flfSt stars. To achieve the nly spectroscopy over the 0.6 <).. < 5.0 um spectrum. An actively cooled sensitivity needed to observe this era (z - 6-20), the mid..fnfrared instrument provides broad-band imagery, observatory must have a telescope aperture that is larger in ooronagrapby, and integral-field spectroscopy over the 5.0 < A. < 29 diameter than the largest rocket faring, and the entire optical um spectrum. The JWST is being developed by NASA, in system must be cooled to -40-50 K. Finally, the resulting partRership with the European and Canadian Space Agencies, al a large deployable cryogenic telescope must achieve HST-like general user facility with science observations to be proposed by the angular resolution across the SWIR spectrum. -
Astro2020 Science White Paper: JWST GTO/ERS Deep Surveys
Astro2020 Science White Paper: JWST GTO/ERS Deep Surveys Thematic Areas: ☐ Planetary Systems ☐ Star and Planet Formation ☐Formation and Evolution of Compact Objects ☒ Cosmology and Fundamental Physics ☐Stars and Stellar Evolution ☐Resolved Stellar Populations and their Environments ☒Galaxy Evolution ☐Multi-Messenger Astronomy and Astrophysics Principal Author: Marcia Rieke University of Arizona [email protected] 520-621-2731 Co-authors: Santiago Arribas Centro de Astrobiología, Madrid Andrew Bunker University of Oxford Stephané Charlot Sorbonne Université Institut d ’Astrophysique de Paris Steve Finkelstein University of Texas Austin Roberto Maiolino University of Cambridge Brant Robertson UC Santa Cruz and Institute for Advanced Study Chris Willott Hertzberg Institute of Astrophysics Rogier Windhorst Arizona State University Harvard-Smithsonian Center for Astrophysics: Daniel Eisenstein Erica Nelson Sandro Tacchella University of Arizona: Eiichi Egami Ryan Endsley Brenda Frye Kevin Hainline Raphael Hviding George Rieke Christina Williams Christopher Willmer Charity Woodrum Abstract : Discovering and characterizing the first galaxies to form in the early Universe is one of the prime reasons for building a large, cold telescope in space, the James Webb Space Telescope (JWST). This white paper describes an integrated Guaranteed Time Observer program using 800 hours of prime time and 800 hours of parallel time to study the formation and evolution of galaxies from z ~2 to z~14, combining NIRSpec, NIRCam, and MIRI data in a coordinated -
Evidence for a Non-Zero L and a Low Matter Density from a Combined Analysis of the 2Df Galaxy Redshift Survey and Cosmic Microwa
Mon. Not. R. Astron. Soc. 330, L29–L35 (2002) Evidence for a non-zero L and a low matter density from a combined analysis of the 2dF Galaxy Redshift Survey and cosmic microwave background anisotropies Downloaded from https://academic.oup.com/mnras/article-abstract/330/2/L29/1085554 by California Institute of Technology user on 20 May 2020 G. Efstathiou,1,2P Stephen Moody,1 John A. Peacock,3 Will J. Percival,3 Carlton Baugh,4 Joss Bland-Hawthorn,5 Terry Bridges,5 Russell Cannon,5 Shaun Cole,4 Matthew Colless,6 Chris Collins,7 Warrick Couch,8 Gavin Dalton,9 Roberto De Propris,8 Simon P. Driver,10 Richard S. Ellis,11 Carlos S. Frenk,4 Karl Glazebrook,12 Carole Jackson,6 Ofer Lahav,1 Ian Lewis,5 Stuart Lumsden,13 Steve Maddox,14 Peder Norberg,4 Bruce A. Peterson,6 Will Sutherland3 and Keith Taylor11 (The 2dFGRS Team) 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA 2Theoretical Astrophysics, Caltech, Pasadena, CA 91125, USA 3Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ 4Department of Physics, University of Durham, South Road, Durham DH1 3LE 5Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia 6Research School of Astronomy and Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia 7Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD 8Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia 9Astrophysics, Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford OX1 3RH 10School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY6 9SS 11Department of Astronomy, Caltech, Pasadena, CA 91125, USA 12Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218-2686, USA 13Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT 14School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD Accepted 2001 November 26. -
Curriculum Vitae
CURRICULUM VITAE FULL NAME: George Petros EFSTATHIOU NATIONALITY: British DATE OF BIRTH: 2nd Sept 1955 QUALIFICATIONS Dates Academic Institution Degree 10/73 to 7/76 Keble College, Oxford. B.A. in Physics 10/76 to 9/79 Department of Physics, Ph.D. in Astronomy Durham University EMPLOYMENT Dates Academic Institution Position 10/79 to 9/80 Astronomy Department, Postdoctoral Research Assistant University of California, Berkeley, U.S.A. 10/80 to 9/84 Institute of Astronomy, Postdoctoral Research Assistant Cambridge. 10/84 to 9/87 Institute of Astronomy, Senior Assistant in Research Cambridge. 10/87 to 9/88 Institute of Astronomy, Assistant Director of Research Cambridge. 10/88 to 9/97 Department of Physics, Savilian Professor of Astronomy Oxford. 10/88 to 9/94 Department of Physics, Head of Astrophysics Oxford. 10/97 to present Institute of Astronomy, Professor of Astrophysics (1909) Cambridge. 10/04 to 9/08 Institute of Astronomy, Director Cambridge. 10/08 to present Kavli Institute for Cosmology, Director Cambridge. PROFESSIONAL SOCIETIES Fellow of the Royal Society since 1994 Fellow of the Instite of Physics since 1995 Fellow of the Royal Astronomical Society 1983-2010 Member of the International Astronomical Union since 1986 Associate of the Canadian Institute of Advanced Research since 1986 1 AWARDS/Fellowships/Major Lectures 1973 Exhibition Keble College Oxford. 1975 Johnson Memorial Prize University of Oxford. 1977 McGraw-Hill Research Prize University of Durham. 1980 Junior Research Fellowship King’s College, Cambridge. 1984 Senior Research Fellowship King’s College, Cambridge. 1990 Maxwell Medal & Prize Institute of Physics. 1990 Vainu Bappu Prize Astronomical Society of India. -
President's Column
March/AprilAAS 2011, Issue 157 - TheNewsletter Online Publication for the members of the American Astronomical Society CONTENTS President's Column Debra Meloy Elmegreen, [email protected] 3 From the Seattle was the scene for a grand, fast-paced and entertaining Executive Officer 217th meeting, filled with exciting new results presented by our wonderful AAS members. We set a record for the West Coast and achieved the largest AAS meeting ever, outside of DC, with over 5 2900 participants, including over 600 junior members. As usual, Council Actions the hard work of AAS Executive Officer Kevin Marvel and his staff resulted in a smooth meeting experience for us. We were captivated by plenary sessions covering the gamut from exoplanets to the 6 early universe. The inaugural Lancelot Berkeley prizewinners, Bill Borucki and David Koch, gave Boston Meeting inspiring talks about the exciting Kepler results, and the first Kavli Prize lecturer, Dr. Carolyn Porco, 22-26 May described the Cassini mission. Our Warner prizewinner Scott Ransom expounded on exotic pulsars, while Pierce prizewinner Tommaso Treu discussed the growth of black holes and galaxy evolution, 8 and Cannon prizewinner Anna Frebel explored the oldest known stars. Rossi prizewinners Felix Committee News Aharonian, Werner Hoffmann, and Heinz Voelk described the successful H.E.S.S collaboration, while Heineman awardees Michael Turner and Rocky Kolb entertained us with a lively cosmology and particle astrophysics lecture. 10 With these prizewinners and so many other exciting talks still fresh in mind, I exhort you to nominate Seattle Meeting your colleagues for the next round of AAS prizes. -
Astro2010: the Astronomy and Astrophysics Decadal Survey
Astro2010: The Astronomy and Astrophysics Decadal Survey Notices of Interest 1. 4 m space telescope for terrestrial planet imaging and wide field astrophysics Point of Contact: Roger Angel, University of Arizona Summary Description: The proposed 4 m telescope combines capabilities for imaging terrestrial exoplanets and for general astrophysics without compromising either. Extremely high contrast imaging at very close inner working angle, as needed for terrestrial planet imaging, is accomplished by the powerful phase induced amplitude apodization method (PIAA) developed by Olivier Guyon. This method promises 10-10 contrast at 2.0 l/D angular separation, i.e. 50 mas for a 4 m telescope at 500 nm wavelength. The telescope primary mirror is unobscured with off-axis figure, as needed to achieve such high contrast. Despite the off-axis primary, the telescope nevertheless provides also a very wide field for general astrophysics. A 3 mirror anastigmat design by Jim Burge delivers a 6 by 24 arcminute field whose mean wavefront error of 12 nm rms, i.e.diffraction limited at 360 nm wavelength. Over the best 10 square arcminutes the rms error is 7 nm, for diffraction limited imaging at 200 nm wavelength. Any of the instruments can be fed by part or all of the field, by means of a flat steering mirror at the exit pupil. To allow for this, the field is curved with a radius equal to the distance from the exit pupil. The entire optical system fits in a 4 m diameter cylinder, 8 m long. Many have considered that only by using two spacecraft, a conventional on-axis telescope and a remote occulter, could high contrast and wide field imaging goals be reconciled. -
Nobel Lecture: Measuring the Acceleration of the Cosmic Expansion Using Supernovae*
REVIEWS OF MODERN PHYSICS, VOLUME 84, JULY–SEPTEMBER 2012 Nobel Lecture: Measuring the acceleration of the cosmic expansion using supernovae* Saul Perlmutter University of California at Berkeley and Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA (published 13 August 2012) DOI: 10.1103/RevModPhys.84.1127 The ‘‘discovery of the acceleration of the expansion of the were studying supernovae. They saw that in principle, you Universe’’ does not flow trippingly off the tongue—which is could use a very bright exploding star, a supernova, to fitting, since the work that led to it was comparably long and perhaps answer this question. I will show you why that would tortuous. In this Lecture, I would like to give you a feel for be possible. some of the science issues we were facing over the ten years You could take the brightness of a supernova as an indi- leading up to the discovery. I will primarily use the graphics cator of how far away it is: the fainter it is, the farther away it from the original overhead projector transparencies we were is from us—and hence its light has taken more time to reach using in those years. Although they are not as beautiful as our us. So with the fainter supernovae, you are looking farther and modern-day graphics, I hope they will help give some of the farther back in time. You can also use the colors of the texture of what was going on during that period. spectral features of a supernova: a supernova would look The question that motivated all this work is something you blue if it were seen nearby, but when you see it very, very can imagine that the very first humans might have asked when far away it looks red. -
Annual Report Astronomy Australia Limited
2012 / 13 Annual Report Astronomy Australia Limited Vision Astronomers in Australia will have access to the best astronomical research infrastructure. Mission AAL will achieve its vision by: 1. Engaging with Australian astronomers to advance the national research infrastructure priorities of the Australian astronomy decadal plan. 2. Advising the Australian Government on future investments in national astronomical research infrastructure. 3. Managing investments in national astronomical research infrastructure as required. Principles 1. Access to major astronomical research infrastructure should be available to any Australian-based astronomer purely on scientific merit. 2. The concept of national astronomical research infrastructure includes Australian participation in international facilities. 3. The AAO and CSIRO are empowered by the Australian Government to provide a component of the national astronomical research infrastructure and there is no need for AAL to directly manage investments to upgrade or operate the AAT and ATNF. About AAL Astronomy Australia Limited (AAL) is a not-for-profit company whose members are all the Australian universities and research organisations with a significant astronomical research capability. AAL works with Australia’s National Observa- tories, astronomers and the Australian Government to advance the infrastructure goals in the 2006-2015 Decadal Plan for Australian Astronomy. Since its incorporation in 2007, AAL has coordinated the Australian astronomy response to, and managed the funding for, a number of national schemes and projects, including the Australian Government’s investments in astronomy infra- structure through the National Collaborative Research Infrastructure Strategy (NCRIS), the Education Investment Fund (EIF) and the Collaborative Research Infrastructure Scheme (CRIS). Background image 5x2-minute snapshot of the Galactic centre taken using 121 tiles of the Murchison Widefield Array at 150MHz, mosaicked together in the im- age domain.