Probing Homogeneity with Standard Candles
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Arxiv:1103.2976V1 [Astro-Ph.CO] 15 Mar 2011 – 1 – a 3% Solution: Determination of the Hubble Constant with the Hubble Space Telescope and Wide Field Camera 3 1
arXiv:1103.2976v1 [astro-ph.CO] 15 Mar 2011 – 1 – A 3% Solution: Determination of the Hubble Constant with the Hubble Space Telescope and Wide Field Camera 3 1 Adam G. Riess2,3, Lucas Macri4, Stefano Casertano3, Hubert Lampeitl5, Henry C. Ferguson3, Alexei V. Filippenko6, Saurabh W. Jha7, Weidong Li6, and Ryan Chornock8 ABSTRACT We use the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) to determine the Hubble constant from optical and infrared observations of over 600 Cepheid variables in the host galaxies of 8 recent Type Ia supernovae (SNe Ia), which provide the calibration for a magnitude-redshift relation based on 240 SNe Ia. Increased precision over past measurements of the Hubble constant comes from five improvements: (1) more than doubling the number of infrared observations of Cepheids in the nearby SN hosts; (2) increasing the sample size of ideal SN Ia calibrators from six to eight with the addition of SN 2007af and SN 2007sr; (3) increasing by 20% the number of Cepheids with infrared observations in the megamaser host NGC 4258; (4) reducing the difference in the mean metallicity of the Cepheid comparison samples between NGC 4258 and the SN hosts from ∆log [O/H] = 0.08 to 0.05; and (5) calibrating all optical Cepheid colors with a single camera, WFC3, to remove cross-instrument zeropoint errors. The result is a reduction in the uncertainty in H0 due to steps beyond the first rung of the distance ladder from 3.5% to 2.3%. The measurement of H0 via the geometric distance to NGC 4258 is 74.8 3.1 km s−1 Mpc−1, a 4.1% measurement including ± systematic uncertainties. -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
Monthly Newsletter of the Durban Centre - March 2018
Page 1 Monthly Newsletter of the Durban Centre - March 2018 Page 2 Table of Contents Chairman’s Chatter …...…………………….……….………..….…… 3 Andrew Gray …………………………………………...………………. 5 The Hyades Star Cluster …...………………………….…….……….. 6 At the Eye Piece …………………………………………….….…….... 9 The Cover Image - Antennae Nebula …….……………………….. 11 Galaxy - Part 2 ….………………………………..………………….... 13 Self-Taught Astronomer …………………………………..………… 21 The Month Ahead …..…………………...….…….……………..…… 24 Minutes of the Previous Meeting …………………………….……. 25 Public Viewing Roster …………………………….……….…..……. 26 Pre-loved Telescope Equipment …………………………...……… 28 ASSA Symposium 2018 ………………………...……….…......…… 29 Member Submissions Disclaimer: The views expressed in ‘nDaba are solely those of the writer and are not necessarily the views of the Durban Centre, nor the Editor. All images and content is the work of the respective copyright owner Page 3 Chairman’s Chatter By Mike Hadlow Dear Members, The third month of the year is upon us and already the viewing conditions have been more favourable over the last few nights. Let’s hope it continues and we have clear skies and good viewing for the next five or six months. Our February meeting was well attended, with our main speaker being Dr Matt Hilton from the Astrophysics and Cosmology Research Unit at UKZN who gave us an excellent presentation on gravity waves. We really have to be thankful to Dr Hilton from ACRU UKZN for giving us his time to give us presentations and hope that we can maintain our relationship with ACRU and that we can draw other speakers from his colleagues and other research students! Thanks must also go to Debbie Abel and Piet Strauss for their monthly presentations on NASA and the sky for the following month, respectively. -
Asymmetries in Sn 2014J Near Maximum Light Revealed Through Spectropolarimetry
ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY Item Type Article Authors Porter, Amber; Leising, Mark D.; Williams, G. Grant; Milne, P. A.; Smith, Paul; Smith, Nathan; Bilinski, Christopher; Hoffman, Jennifer L.; Huk, Leah; Leonard, Douglas C. Citation ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY 2016, 828 (1):24 The Astrophysical Journal DOI 10.3847/0004-637X/828/1/24 Publisher IOP PUBLISHING LTD Journal The Astrophysical Journal Rights © 2016. The American Astronomical Society. All rights reserved. Download date 27/09/2021 22:28:24 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/622057 The Astrophysical Journal, 828:24 (12pp), 2016 September 1 doi:10.3847/0004-637X/828/1/24 © 2016. The American Astronomical Society. All rights reserved. ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY Amber L. Porter1, Mark D. Leising1, G. Grant Williams2,3, Peter Milne2, Paul Smith2, Nathan Smith2, Christopher Bilinski2, Jennifer L. Hoffman4, Leah Huk4, and Douglas C. Leonard5 1 Department of Physics and Astronomy, Clemson University, 118 Kinard Laboratory, Clemson, SC 29634, USA; [email protected] 2 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA 3 MMT Observatory, P.O. Box 210065, University of Arizona, Tucson, AZ 85721-0065, USA 4 Department of Physics and Astronomy, University of Denver, 2112 East Wesley Avenue, Denver, CO 80208, USA 5 Department of Astronomy, San Diego State University, PA-210, 5500 Campanile Drive, San Diego, CA 92182-1221, USA Received 2016 February 14; revised 2016 May 11; accepted 2016 May 12; published 2016 August 24 ABSTRACT We present spectropolarimetric observations of the nearby Type Ia supernova SN 2014J in M82 over six epochs: +0, +7, +23, +51, +77, +109, and +111 days with respect to B-band maximum. -
Evidence of Environmental Dependencies of Type Ia Supernovae from the Nearby Supernova Factory Indicated by Local Hα?
A&A 560, A66 (2013) Astronomy DOI: 10.1051/0004-6361/201322104 & c ESO 2013 Astrophysics Evidence of environmental dependencies of Type Ia supernovae from the Nearby Supernova Factory indicated by local Hα? M. Rigault1, Y. Copin1, G. Aldering2, P. Antilogus3, C. Aragon2, S. Bailey2, C. Baltay4, S. Bongard3, C. Buton5, A. Canto3, F. Cellier-Holzem3, M. Childress6, N. Chotard1, H. K. Fakhouri2;7, U. Feindt,5, M. Fleury3, E. Gangler1, P. Greskovic5, J. Guy3, A. G. Kim2, M. Kowalski5, S. Lombardo5, J. Nordin2;8, P. Nugent9;10, R. Pain3, E. Pécontal11, R. Pereira1, S. Perlmutter2;7, D. Rabinowitz4, K. Runge2, C. Saunders2, R. Scalzo6, G. Smadja1, C. Tao12;13, R. C. Thomas9, and B. A. Weaver14 (The Nearby Supernova Factory) 1 Université de Lyon, Université de Lyon 1; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, France e-mail: [email protected] 2 Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA 3 Laboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, France 4 Department of Physics, Yale University, New Haven, CT 06520-8121, USA 5 Physikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, Germany 6 Research School of Astronomy and Astrophysics, The Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek ACT 2611, Australia 7 Department of Physics, University of California Berkeley, 366 LeConte -
Publications for Richard Scalzo 2021 2020 2019 2018 2017 2016
Publications for Richard Scalzo 2021 2019 Olierook, H., Scalzo, R., Kohn, D., Chandra, R., Farahbakhsh, Scalzo, R., Kohn, D., Olierook, H., Houseman, G., Chandra, R., E., Clark, C., Reddy, S., Muller, R. (2021). Bayesian geological Girolami, M., Cripps, S. (2019). Efficiency and robustness in and geophysical data fusion for the construction and uncertainty Monte Carlo sampling for 3-Dgeophysical inversions with quantification of 3D geological models. Geoscience Frontiers, Obsidian v0.1.2: setting up for success. Geoscientific Model 12(1), 479-493. <a Development, 12, 2941-2960. <a href="http://dx.doi.org/10.1016/j.gsf.2020.04.015">[More href="http://dx.doi.org/10.5194/gmd-12-2941-2019">[More Information]</a> Information]</a> Sweeney, D., Norris, B., Tuthill, P., Scalzo, R., Wei, J., Betters, Scalzo, R., Parent, E., Burns, C., Childress, M., Tucker, B., C., Leon-Saval, S. (2021). Learning the lantern: neural network Brown, P., Contreras, C., Hsiao, E., Krisciunas, K., Morrell, N., applications to broadband photonic lantern modeling. Journal et al (2019). Probing type Ia supernova properties using of Astronomical Telescopes, Instruments, and Systems, 7(2), bolometric light curves from the Carnegie Supernova Project 028007-1-028007-20. <a and the CfA Supernova Group. Monthly Notices of the Royal href="http://dx.doi.org/10.1117/1.JATIS.7.2.028007">[More Astronomical Society, 483(1), 628-647. <a Information]</a> href="http://dx.doi.org/10.1093/mnras/sty3178">[More Wong, A., Norris, B., Tuthill, P., Scalzo, R., Lozi, J., Vievard, Information]</a> S., Guyon, O. (2021). Predictive control for adaptive optics Varidel, M., Croom, S., Lewis, G., Brewer, B., Di Teodoro, E., using neural networks. -
Type Ia Supernova Rate at a Redshift of ∼0.1
A&A 423, 881–894 (2004) Astronomy DOI: 10.1051/0004-6361:20035948 & c ESO 2004 Astrophysics Type Ia supernova rate at a redshift of ∼0.1 G. Blanc1,12,22,C.Afonso1,4,8,23,C.Alard24,J.N.Albert2, G. Aldering15,,A.Amadon1, J. Andersen6,R.Ansari2, É. Aubourg1,C.Balland13,21,P.Bareyre1,4,J.P.Beaulieu5, X. Charlot1, A. Conley15,, C. Coutures1,T.Dahlén19, F. Derue13,X.Fan16, R. Ferlet5, G. Folatelli11, P. Fouqué9,10,G.Garavini11, J. F. Glicenstein1, B. Goldman1,4,8,23, A. Goobar11, A. Gould1,7,D.Graff7,M.Gros1, J. Haissinski2, C. Hamadache1,D.Hardin13,I.M.Hook25, J. de Kat1,S.Kent18,A.Kim15, T. Lasserre1, L. Le Guillou1,É.Lesquoy1,5, C. Loup5, C. Magneville1, J. B. Marquette5,É.Maurice3,A.Maury9, A. Milsztajn1, M. Moniez2, M. Mouchet20,22,H.Newberg17,S.Nobili11, N. Palanque-Delabrouille1 , O. Perdereau2,L.Prévot3,Y.R.Rahal2, N. Regnault2,14,15,J.Rich1, P. Ruiz-Lapuente27, M. Spiro1, P. Tisserand1, A. Vidal-Madjar5, L. Vigroux1,N.A.Walton26, and S. Zylberajch1 1 DSM/DAPNIA, CEA/Saclay, 91191 Gif-sur-Yvette Cedex, France 2 Laboratoire de l’Accélérateur Linéaire, IN2P3 CNRS, Université Paris-Sud, 91405 Orsay Cedex, France 3 Observatoire de Marseille, 2 pl. Le Verrier, 13248 Marseille Cedex 04, France 4 Collège de France, Physique Corpusculaire et Cosmologie, IN2P3 CNRS, 11 pl. M. Berthelot, 75231 Paris Cedex, France 5 Institut d’Astrophysique de Paris, INSU CNRS, 98 bis boulevard Arago, 75014 Paris, France 6 Astronomical Observatory, Copenhagen University, Juliane Maries Vej 30, 2100 Copenhagen, Denmark 7 Departments of Astronomy and Physics, Ohio -
Cosmology the Reach of Gaia
11/15/2019 Cosmology TUM WS 2019/2020 Lecture 4 Wolfgang Hillebrandt and Bruno Leibundgut (http://www.eso.org/~bleibund/Cosmology) TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 1 The reach of Gaia Parallaxes to a fair fraction of the Milky Way – galaxy structure • spiral arms, disk, bulge, halo – galaxy dynamics – average distance to the LMC TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 2 1 11/15/2019 Milky Way Magellanic Clouds Large Magellanic Cloud (LMC) TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 3 Large Magellanic Cloud • Primary calibrator for many methods – primary Cepheids – RR Lyrae – Eclipsing binaries – SN 1987A • geometric – light travel time from circumstellar ring 39.8 kpc 43.7 52.5 57.5 kpc Freedman & Madore 2010 TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 4 2 11/15/2019 Eclipsing binaries • Binary star with the orbital axis perpendicular to the line of sight compare the size of the star (from the duration of the eclipses) to its apparent angle on the sky (from the surface brightness of the star; uses Stefan-Boltzmann law) → angular size distance r(km) d(pc) 1.337105 (mas) TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 5 Eclipsing binaries • Binary star with the orbital axis perpendicular to the line of sight excellent distance to the Large Magellanic Cloud Pietrzynski et al. 2013 (e.g., Pietrzynski et al. 2013) TUM WS19/20 Cosmology 4 Wolfgang Hillebrandt and Bruno Leibundgut 6 3 11/15/2019 SN 1987A as geometric distance -
Type Ia Supernovae As Stellar Endpoints and Cosmological Tools
REVIEW Published 14 Jun 2011 | DOI: 10.1038/ncomms1344 Type Ia supernovae as stellar endpoints and cosmological tools D. Andrew Howell1,2 Empirically, Type Ia supernovae are the most useful, precise, and mature tools for determining astronomical distances. Acting as calibrated candles they revealed the presence of dark energy and are being used to measure its properties. However, the nature of the Type Ia explosion, and the progenitors involved, have remained elusive, even after seven decades of research. But now, new large surveys are bringing about a paradigm shift—we can finally compare samples of hundreds of supernovae to isolate critical variables. As a result of this, and advances in modelling, breakthroughs in understanding all aspects of these supernovae are finally starting to happen. uest stars (who could have imagined they were distant stellar explosions?) have been surprising humans for at least 950 years, but probably far longer. They amazed and confounded the likes of Tycho, Kepler and Galileo, to name a few. But it was not until the separation of these events G 1 into novae and supernovae by Baade and Zwicky that progress understanding them began in earnest . This process of splitting a diverse group into related subsamples to yield insights into their origin would be repeated again and again over the years, first by Minkowski when he separated supernovae of Type I (no hydrogen in their spectra) from Type II (have hydrogen)2, and then by Elias et al. when they deter- mined that Type Ia supernovae (SNe Ia) were distinct3. We now define Type Ia supernovae as those without hydrogen or helium in their spectra, but with strong ionized silicon (SiII), which has observed absorption lines at 6,150, 5,800 and 4,000 Å (ref. -
Kasliwal Phd Thesis
Bridging the Gap: Elusive Explosions in the Local Universe Thesis by Mansi M. Kasliwal Advisor Professor Shri R. Kulkarni In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 2011 (Defended April 26, 2011) ii c 2011 Mansi M. Kasliwal All rights Reserved iii Acknowledgements The first word that comes to my mind to describe my learning experience at Caltech is exhilarating. I have no words to thank my “Guru”, Professor Shri Kulkarni. Shri taught me the “Ps” necessary to Pursue the Profession of a Professor in astroPhysics. In addition to Passion & Perseverance, I am now Prepared for Papers, Proposals, Physics, Presentations, Politics, Priorities, oPPortunity, People-skills, Patience and PJs. Thanks to the awesomely fantastic Palomar Transient Factory team, especially Peter Nugent, Robert Quimby, Eran Ofek and Nick Law for sharing the pains and joys of getting a factory off-the-ground. Thanks to Brad Cenko and Richard Walters for the many hours spent taming the robot on mimir2:9. Thanks to Avishay Gal-Yam and Lars Bildsten for illuminating discussions on different observational and theoretical aspects of transients in the gap. The journey from idea to first light to a factory churning out thousands of transients has been so much fun that I would not trade this experience for any other. Thanks to Marten van Kerkwijk for supporting my “fishing in new waters” project with the Canada France Hawaii Telescope. Thanks to Dale Frail for supporting a “kissing frogs” radio program. Thanks to Sterl Phinney, Linqing Wen and Samaya Nissanke for great discussions on the challenge of finding the light in the gravitational sound wave. -
The Crab Nebula Imaged by the Hubble Space Telescope in 1999 and 2000
Astronomers’ Observing Guides Other titles in this series The Moon and How to Observe It Peter Grego Double & Multiple Stars, and How to Observe Them James Mullaney Saturn and How to Observe it Julius Benton Jupiter and How to Observe it John McAnally Star Clusters and How to Observe Them Mark Allison Nebulae and How to Observe Them Steven Coe Galaxies and How to Observe Them Wolfgang Steinicke and Richard Jakiel Related titles Field Guide to the Deep Sky Objects Mike Inglis Deep Sky Observing Steven R. Coe The Deep-Sky Observer’s Year Grant Privett and Paul Parsons The Practical Astronomer’s Deep-Sky Companion Jess K. Gilmour Observing the Caldwell Objects David Ratledge Choosing and Using a Schmidt-Cassegrain Telescope Rod Mollise Martin Mobberley Supernovae and How to Observe Them with 167 Illustrations Martin Mobberley [email protected] Library of Congress Control Number: 2006928727 ISBN-10: 0-387-35257-0 e-ISBN-10: 0-387-46269-4 ISBN-13: 978-0387-35257-2 e-ISBN-13: 978-0387-46269-1 Printed on acid-free paper. © 2007 Springer Science+Business Media, LLC All rights reserved. This work may not be translated or copied in whole or in part without the written permission of the publisher (Springer Science+Business Media, LLC, 233 Spring Street, New York, NY 10013, USA), except for brief excerpts in connection with reviews or scholarly analysis. Use in connection with any form of information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed is forbidden. The use in this publication of trade names, trademarks, service marks, and similar terms, even if they are not identified as such, is not to be taken as an expression of opinion as to whether or not they are subject to proprietary rights. -
2011 Annual Report Ernest Orlando Lawrence Berkeley National Laboratory 1 Cyclotron Road, Berkeley, CA 94720-8148
Complexed Adsorbed H3 L2 L7 H3 HP1 HP1 L2 L7 National Energy Research Scientific Computing Center 2011 Annual Report Ernest Orlando Lawrence Berkeley National Laboratory 1 Cyclotron Road, Berkeley, CA 94720-8148 This work was supported by the Director, Office of Science, Office of Advanced Scientific Computing Research of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. National Energy Research Scientific Computing Center 2011 Annual Report Table of Contents 6 The Year in Perspective 10 Research News 10 New Mathematical Method Reveals Where Genes Switch On or Off 12 Small Particles Have Big Impact 14 Detailed Model Changes View of Ancient Climate Change 16 A Better Way to Find Extreme Weather Events in Climate Modeling Data 18 Turning Grass into Gas for Less 20 Bubbles Help Break Energy Storage Record for Lithium–Air Batteries 22 New Anode Boosts Capacity of Lithium–Ion Batteries 24 Speeding Up Design of Organic Semiconductors 26 Solving the Mystery of LED “Droop” 28 Modeling the Bonds of Iron and Water 30 Discovering the Molecular Details of CO2 Reservoirs 32 Simulating Magnetic Instabilities in NSTX and ITER 34 Fusion PIC Code Optimization on Emerging Architectures 36 Proton Dripping Tests a Basic Force of Nature 38 Heaviest Antimatter Particle Detected with NERSC Help 40 Boosting the Next Wave of Accelerators 42 Supernova Caught in the Act Reveals First Direct Evidence of Its Progenitor System 44 Solar System’s Magnetic Edge More Turbulent Than Expected 46 Measuring the Distant Universe in 3D 48 NISE Program Encourages