Rosemary F.G. Wyse Curriculum Vitae
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The Rich Structure of the Nearby Stellar Halo Revealed by Gaia and RAVE Amina Helmi1, Jovan Veljanoski1, Maarten A
A&A 598, A58 (2017) Astronomy DOI: 10.1051/0004-6361/201629990 & c ESO 2017 Astrophysics A box full of chocolates: The rich structure of the nearby stellar halo revealed by Gaia and RAVE Amina Helmi1, Jovan Veljanoski1, Maarten A. Breddels1, Hao Tian1, and Laura V. Sales2 1 Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands e-mail: [email protected] 2 Department of Physics & Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USA Received 1 November 2016 / Accepted 21 December 2016 ABSTRACT Context. The hierarchical structure formation model predicts that stellar halos should form, at least partly, via mergers. If this was a predominant formation channel for the Milky Way’s halo, imprints of this merger history in the form of moving groups or streams should also exist in the vicinity of the Sun. Aims. We study the kinematics of halo stars in the Solar neighbourhood using the very recent first data release from the Gaia mission, and in particular the TGAS dataset, in combination with data from the RAVE survey. Our aim is to determine the amount of substructure present in the phase-space distribution of halo stars that could be linked to merger debris. Methods. To characterise kinematic substructure, we measured the velocity correlation function in our sample of halo (low- metallicity) stars. We also studied the distribution of these stars in the space of energy and two components of the angular momentum, in what we call “integrals of motion” space. Results. The velocity correlation function reveals substructure in the form of an excess of pairs of stars with similar velocities, well above that expected for a smooth distribution. -
Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties. -
The Dynamic Duo: RAVE Complements Gaia 19 September 2016
The Dynamic Duo: RAVE complements Gaia 19 September 2016 "The Tycho-Gaia stars that were also serendipitously observed by RAVE contain the best proper motions and parallaxes recently released by Gaia and can now be combined with the radial velocities and stellar parameters from RAVE", says Andrea Kunder, lead author of the RAVE data release and astronomer at the Leibniz Institute for Astrophysics Potsdam (AIP), "So these stars can be used to probe the Milky Way more precisely than ever before. Just like wearing glasses allows you to see your surroundings in sharper view, the Gaia-RAVE data will allow the galaxy to be seen with more detail." Among existing spectroscopic surveys, RAVE easily boasts the largest overlap with the Tycho-Gaia astrometric solution catalogue. Screenshot from a movie flying through the RAVE stars from Data Release 5. Credit: K. Riebe, AIP The four previous data releases have been the foundation for a number of studies, which have especially advanced our understanding of the disk of the Milky Way. The fifth RAVE data release The new data release of the Radial Velocity includes not only the culminating RAVE Experiment (RAVE) is the fifth spectroscopic observations taken in 2013, but also also earlier release of a survey of stars in the southern discarded observations recovered from previous celestial hemisphere. It contains radial velocities years, resulting in an additional 30,000 RAVE for 520 781 spectra of 457 588 unique stars that spectra. were observed over ten years. With these measurements RAVE complements the first data For the new data release atmospheric parameters release of the Gaia survey published by the such as the effective temperature, surface gravity European Space Agency ESA last week by and metallicities have been refined using gravities providing radial velocities and stellar parameters, from asteroseismology and high-precison stellar like temperatures, gravities and metallicities of atmospheric parameters. -
Models of the Galaxy and the Massive Spectroscopic Stellar Survey RAVE
Forschungsabteilung “The Milky Way and the Local Volume” Models of the Galaxy and the massive spectroscopic stellar survey RAVE Dissertation zur Erlangung des akademischen Grades “doctor rerum naturalium” (Dr. rer. nat.) in der Wissenschaftsdisziplin “Astrophysik” eingereicht an der Mathematisch-Naturwissenschaftlichen Fakultät der Universität Potsdam von Tilmann Piffl Potsdam, 25.10.2013 This work is licensed under a Creative Commons License: Attribution - Noncommercial - Share Alike 3.0 Germany To view a copy of this license visit http://creativecommons.org/licenses/by-nc-sa/3.0/de/ Betreuer: Prof. Matthias Steinmetz (Leibniz-Institut für Astrophysik Potsdam (AIP)) Published online at the Institutional Repository of the University of Potsdam: URL http://opus.kobv.de/ubp/volltexte/2014/7037/ URN urn:nbn:de:kobv:517-opus-70371 http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-70371 Abstract Numerical simulations of galaxy formation and observational Galactic Astronomy are two fields of research that study the same objects from different perspectives. Simulations try to understand galaxies like our Milky Way from an evolutionary point of view while observers try to disentangle the current structure and the building blocks of our Galaxy. Due to great advances in computational power as well as in massive stellar surveys we are now able to compare resolved stellar populations in simulations and in observations. In this thesis we use a number of approaches to relate the results of the two fields to each other. The major observational data set we refer to for this work comes from the Radial Velocity Experiment (RAVE), a massive spectroscopic stellar survey that observed almost half a million stars in the Galaxy. -
Chemical Gradients in the Milky Way from the RAVE Data II
A&A 568, A71 (2014) Astronomy DOI: 10.1051/0004-6361/201423974 & c ESO 2014 Astrophysics Chemical gradients in the Milky Way from the RAVE data II. Giant stars C. Boeche1,A.Siebert2,T.Piffl3,4,A.Just1, M. Steinmetz3,E.K.Grebel1,S.Sharma5, G. Kordopatis6,G.Gilmore6, C. Chiappini3, K. Freeman7,B.K.Gibson8,9, U. Munari10,A.Siviero11,3, O. Bienaymé2,J.F.Navarro12, Q. A. Parker13,14,15,W.Reid13,15,G.M.Seabroke16,F.G.Watson14,R.F.G.Wyse17, and T. Zwitter18 1 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany e-mail: [email protected] 2 Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, 67000 Strasbourg, France 3 Leibniz Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 4 Rudolf Peierls Centre for Theoretical Physics, Keble Road, Oxford OX1 3NP, UK 5 Sydney Institute for Astronomy, School of Physics A28, University of Sydney, Sydney NSW 2006, Australia 6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 7 Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd., ACT 2611 Weston, Australia 8 Institute for Computational Astrophysics, Dept of Astronomy and Physics, Saint Mary’s University, Halifax, NS, BH3 3C3, Canada 9 Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK 10 INAF Osservatorio Astronomico di Padova, via dell’Osservatorio 8, 36012 Asiago, Italy 11 Department -
Rediscovering Our Galaxy Edited By
IAU IAU Symposium Proceedings of the International Astronomical Union IAU Symposium No. 334 Symposium 10–14 July 2017 Astronomers are at a crucial point in our understanding of the Milky Way. Deciphering the assembly history of our galaxy requires 334 Potsdam, Germany detailed mapping of the structure, dynamics, chemical composition, and age distribution of its stellar populations. In the last decade, astrometric, spectroscopic, photometric, and asteroseismic surveys have started to unveil the inner- and 10–14 July 2017 334 Rediscovering 10–14 July 2017 outermost regions of the Milky Way. IAU Symposium 334 explores Potsdam, Germany Our Galaxy the still open questions and focusses on the concepts emerging Potsdam, Germany Rediscovering from the analysis of these large, new, and complex datasets. This volume presents a summary of these topics, including the current novel data and the challenges they already pose to modeling, Our Galaxy before Gaia end-of-mission, PLATO, and large spectroscopic surveys such as WEAVE and 4MOST are about to start. Graduate students and researchers will learn that, in this golden era of Galactic Archaeology, we are about to rediscover our galaxy. Proceedings of the International Astronomical Union Editor in Chief: Dr Piero Benvenuti This series contains the proceedings of major scientifi c meetings held by the International Astronomical Union. Each volume contains a series of articles on a topic of current interest in astronomy, giving a timely overview of research in the fi eld. With contributions by leading -
An Outsiders View on the Metallicity and Abundance Distribution of The
An outsider’s view on the metallicity and α-abundance distribution of the Milky Way KO report Author: Supervisor: Omar Choudhury Prof. Dr. S.C. Trager Figure 1: Metallicity and α-abundance distributions of the Milky Way as viewed from outside. February 2011 Chapter Contents Contents 3 1 Introduction 5 1.1 Background..................................... 5 1.2 Goaloftheproject ................................ 5 1.3 Metallicity and α-abundance ........................... 6 1.4 Methods....................................... 7 2 Data: the thin disk 9 2.1 Space velocity calculation . ..... 10 2.2 SEGUE ....................................... 11 2.3 RAVEdata ..................................... 13 3 Data: the bulge 15 3.1 Bulgefieldstars.................................. 16 3.2 Bulgeglobularclusters. 17 3.3 Combining field stars and globular clusters . ........ 18 4 From inside the galaxy to outside 21 4.1 Luminosityfunction .............................. 23 5 Discussion 25 6 Conclusions 27 7 Acknowledgement 29 8 Bibliography 31 A SEGUE SQL query 35 B Colour transformations 37 3 Chapter 1 Introduction 1.1 Background In the first seconds after the Big Bang the first elements were created. Most of the particles, ∼ 92%, are in the form of hydrogen and approximately 8% is in the form of helium. Except for a small amount of lithium, no other metals were created. As the Universe expanded and cooled down, the first stars and galaxies started to form. In the very centre of a star hydrogen is burned into helium. At the end of a star’s lifetime, helium is burned into heavier elements. The mass of the heaviest element that a star can produce becomes larger for more massive stars. This continues until iron is reached. -
YMCA-1: a New Remote Star Cluster of the Milky Way?∗
Draft version July 23, 2021 Typeset using LATEX manuscript style in AASTeX631 YMCA-1: a new remote star cluster of the Milky Way?∗ M. Gatto ,1, 2 V. Ripepi,1 M. Bellazzini ,3 M. Tosi,3 C. Tortora,1 M. Cignoni,1, 4, 5 M. Spavone ,1 M. Dall'ora,1 G. Clementini,3 F. Cusano,3 G. Longo,2 I. Musella,1 M. Marconi,1 and P. Schipani1 1INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131, Naples, Italy 2Dept. of Physics, University of Naples Federico II, C.U. Monte Sant'Angelo, Via Cinthia, 80126, Naples, Italy 3INAF-Osservatorio di Astrofisica e Scienza dello Spazio, Via Gobetti 93/3, I-40129 Bologna, Italy 4Physics Departement, University of Pisa, Largo Bruno Pontecorvo, 3, I-56127 Pisa, Italy 5INFN, Largo B. Pontecorvo 3, 56127, Pisa, Italy ABSTRACT We report the possible discovery of a new stellar system (YMCA-1), identified during a search for small scale overdensities in the photometric data of the YMCA survey. The object's projected position lies on the periphery of the Large Magellanic Cloud about 13◦ apart from its center. The most likely interpretation of its color-magnitude diagram, as well as of its integrated properties, is that YMCA-1 may be an old and remote star cluster of the Milky Way at a distance of 100 kpc from the Galactic center. If this scenario could be confirmed, then the cluster would be significantly fainter and more compact than most of the known star clusters residing in the extreme outskirts of arXiv:2107.10312v1 [astro-ph.GA] 21 Jul 2021 the Galactic halo, but quite similar to Laevens 3. -
IAU Symp 269, POST MEETING REPORTS
IAU Symp 269, POST MEETING REPORTS C.Barbieri, University of Padua, Italy Content (i) a copy of the final scientific program, listing invited review speakers and session chairs; (ii) a list of participants, including their distribution on gender (iii) a list of recipients of IAU grants, stating amount, country, and gender; (iv) receipts signed by the recipients of IAU Grants (done); (v) a report to the IAU EC summarizing the scientific highlights of the meeting (1-2 pages). (vi) a form for "Women in Astronomy" statistics. (i) Final program Conference: Galileo's Medicean Moons: their Impact on 400 years of Discovery (IAU Symposium 269) Padova, Jan 6-9, 201 Program Wednesday 6, location: Centro San Gaetano, via Altinate 16.0 0 – 18.00 meeting of Scientific Committee (last details on the Symp 269; information on the IYA closing ceremony program) 18.00 – 20.00 welcome reception Thursday 7, morning: Aula Magna University 8:30 – late registrations 09.00 – 09.30 Welcome Addresses (Rector of University, President of COSPAR, Representative of ESA, President of IAU, Mayor of Padova, Barbieri) Session 1, The discovery of the Medicean Moons, the history, the influence on human sciences Chair: R. Williams Speaker Title 09.30 – 09.55 (1) G. Coyne Galileo's telescopic observations: the marvel and meaning of discovery 09.55 – 10.20 (2) D. Sobel Popular Perceptions of Galileo 10.20 – 10.45 (3) T. Owen The slow growth of human humility (read by Scott Bolton) 10.45 – 11.10 (4) G. Peruzzi A new Physics to support the Copernican system. Gleanings from Galileo's works 11.10 – 11.35 Coffee break Session 1b Chair: T. -
Eight Ultra-Faint Galaxy Candidates Discovered in Year Two of the Dark Energy Survey A
The Astrophysical Journal, 813:109 (20pp), 2015 November 10 doi:10.1088/0004-637X/813/2/109 © 2015. The American Astronomical Society. All rights reserved. EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY A. Drlica-Wagner1, K. Bechtol2,3, E. S. Rykoff4,5, E. Luque6,7, A. Queiroz6,7,Y.-Y.Mao4,5,8, R. H. Wechsler4,5,8, J. D. Simon9, B. Santiago6,7, B. Yanny1, E. Balbinot7,10, S. Dodelson1,11, A. Fausti Neto7, D. J. James12,T.S.Li13, M. A. G. Maia7,14, J. L. Marshall13, A. Pieres6,7, K. Stringer13, A. R. Walker12, T. M. C. Abbott12, F. B. Abdalla15,16, S. Allam1, A. Benoit-Lévy15, G. M. Bernstein17, E. Bertin18,19, D. Brooks15, E. Buckley-Geer1, D. L. Burke4,5, A. Carnero Rosell7,14, M. Carrasco Kind20,21, J. Carretero22,23, M. Crocce22, L. N. da Costa7,14, S. Desai24,25, H. T. Diehl1, J. P. Dietrich24,25, P. Doel15,T.F.Eifler17,26, A. E. Evrard27,28, D. A. Finley1, B. Flaugher1, P. Fosalba22, J. Frieman1,11, E. Gaztanaga22, D. W. Gerdes28, D. Gruen29,30, R. A. Gruendl20,21, G. Gutierrez1, K. Honscheid31,32, K. Kuehn33, N. Kuropatkin1, O. Lahav15, P. Martini31,34, R. Miquel23,35, B. Nord1, R. Ogando7,14, A. A. Plazas26, K. Reil5, A. Roodman4,5, M. Sako17, E. Sanchez36, V. Scarpine1, M. Schubnell28, I. Sevilla-Noarbe20,36, R. C. Smith12, M. Soares-Santos1, F. Sobreira1,7, E. Suchyta31,32, M. E. C. Swanson21, G. Tarle28, D. Tucker1, V. Vikram37, W. Wester1, Y. Zhang28, and J. -
Gaia EDR3 View on Galactic Globular Clusters
MNRAS 505, 5978–6002 (2021) https://doi.org/10.1093/mnras/stab1475 Advance Access publication 2021 May 24 Gaia EDR3 view on galactic globular clusters Eugene Vasiliev 1,2‹ and Holger Baumgardt 3 1Institute of Astronomy, Madingley road, Cambridge CB3 0HA, UK 2Lebedev Physical Institute, Leninsky prospekt 53, Moscow 119991, Russia 3School of Mathematics and Physics, The University of Queensland, St Lucia, QLD 4072, Australia Accepted 2021 May 17. Received 2021 May 11; in original form 2021 March 17 Downloaded from https://academic.oup.com/mnras/article/505/4/5978/6283730 by UQ Library user on 09 August 2021 ABSTRACT We use the data from Gaia Early Data Release 3 (EDR3) to study the kinematic properties of Milky Way globular clusters. We measure the mean parallaxes and proper motions (PM) for 170 clusters, determine the PM dispersion profiles for more than 100 clusters, uncover rotation signatures in more than 20 objects, and find evidence for radial or tangential PM anisotropy in a dozen richest clusters. At the same time, we use the selection of cluster members to explore the reliability and limitations of the Gaia catalogue itself. We find that the formal uncertainties on parallax and PM are underestimated by 10−20 per cent in dense central regions even for stars that pass numerous quality filters. We explore the spatial covariance function of systematic errors, and determine a lower limit on the uncertainty of average parallaxes and PM at the level 0.01 mas and 0.025 mas yr−1 , respectively. Finally, a comparison of mean parallaxes of clusters with distances from various literature sources suggests that the parallaxes for stars with G>13 (after applying the zero-point correction suggested by Lindegren et al.) are overestimated by ∼ 0.01 ± 0.003 mas. -
Arxiv:1508.03622V2 [Astro-Ph.GA] 6 Nov 2015
SLAC-PUB-16631 Eight Ultra-faint Galaxy Candidates Discovered in Year Two of the Dark Energy Survey 1; 2;3; 4;5 6;7 6;7 8;4;5 A. Drlica-Wagner ∗, K. Bechtol y, E. S. Rykoff , E. Luque , A. Queiroz , Y.-Y. Mao , R. H. Wechsler8;4;5, J. D. Simon9, B. Santiago6;7, B. Yanny1, E. Balbinot10;7, S. Dodelson1;11, A. Fausti Neto7, D. J. James12, T. S. Li13, M. A. G. Maia7;14, J. L. Marshall13, A. Pieres6;7, K. Stringer13, A. R. Walker12, T. M. C. Abbott12, F. B. Abdalla15;16, S. Allam1, A. Benoit-L´evy15, G. M. Bernstein17, E. Bertin18;19, D. Brooks15, E. Buckley-Geer1, D. L. Burke4;5, A. Carnero Rosell7;14, M. Carrasco Kind20;21, J. Carretero22;23, M. Crocce22, L. N. da Costa7;14, S. Desai24;25, H. T. Diehl1, J. P. Dietrich24;25, P. Doel15, T. F. Eifler17;26, A. E. Evrard27;28, D. A. Finley1, B. Flaugher1, P. Fosalba22, J. Frieman1;11, E. Gaztanaga22, D. W. Gerdes28, D. Gruen29;30, R. A. Gruendl20;21, G. Gutierrez1, K. Honscheid31;32, K. Kuehn33, N. Kuropatkin1, O. Lahav15, P. Martini31;34, R. Miquel35;23, B. Nord1, R. Ogando7;14, A. A. Plazas26, K. Reil5, A. Roodman4;5, M. Sako17, E. Sanchez36, V. Scarpine1, M. Schubnell28, I. Sevilla-Noarbe36;20, R. C. Smith12, M. Soares-Santos1, F. Sobreira1;7, E. Suchyta31;32, M. E. C. Swanson21, G. Tarle28, D. Tucker1, V. Vikram37, W. Wester1, Y. Zhang28, J. Zuntz38 (The DES Collaboration) arXiv:1508.03622v2 [astro-ph.GA] 6 Nov 2015 This material is based upon work supported by the U.S.