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Photometry and Spectroscopy of the Luminous Red Nova PSNJ14021678+5426205 in the Galaxy M101
CORE Metadata, citation and similar papers at core.ac.uk Provided by Kazan Federal University Digital Repository Astrophysical Bulletin 2016 vol.71 N1, pages 82-94 Photometry and spectroscopy of the luminous red nova PSNJ14021678+5426205 in the galaxy M101 Goranskij V., Barsukova E., Spiridonova O., Valeev A., Fatkhullin T., Moskvitin A., Vozyakova O., Cheryasov D., Safonov B., Zharova A., Hancock T. Kazan Federal University, 420008, Kremlevskaya 18, Kazan, Russia Abstract © 2016, Pleiades Publishing, Ltd.We present the results of the study of a red nova from the observations carried out with the Russian 6-m telescope (BTA) along with other telescopes of SAO RAS and SAI MSU. To investigate the nova progenitor,we used the data from the Digital Sky Survey and amateur photos available on the Internet. In the period between April 1993 and July 2014, the brightness of the progenitor gradually increased by (Formula presented.) in the V- band. At the peak of the first outburst in mid-November 2014, the star reached an absolute visual magnitude of (Formula presented.) but was discovered later, in February 2015, in a repeated outburst at the magnitude of (Formula presented.). The amplitude of the outburst was minimum among the red novae, only (Formula presented.) in V-band. The Hα emission line and the background of a cool supergiant continuum with gradually decreasing surface temperature were observed in the spectra. Such process is typical for red novae, although the object under study showed extreme parameters: maximum luminosity, maximum outburst duration, minimum outburst amplitude, unusual shape of the light curve. This event is interpreted as a massive OB star system components’merging accompanied by formation of a common envelope and then the expansion of this envelope with minimal energy losses. -
Stellar Tidal Streams As Cosmological Diagnostics: Comparing Data and Simulations at Low Galactic Scales
RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Author: Referees: Gustavo MORALES Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL Astronomisches Rechen-Institut Heidelberg Graduate School of Fundamental Physics Department of Physics and Astronomy 14th May, 2018 ii DISSERTATION submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of DOCTOR OF NATURAL SCIENCES Put forward by GUSTAVO MORALES born in Copiapo ORAL EXAMINATION ON JULY 26, 2018 iii Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Referees: Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL iv NOTE: Some parts of the written contents of this thesis have been adapted from a paper submitted as a co-authored scientific publication to the Astronomy & Astrophysics Journal: Morales et al. (2018). v NOTE: Some parts of this thesis have been adapted from a paper accepted for publi- cation in the Astronomy & Astrophysics Journal: Morales, G. et al. (2018). “Systematic search for tidal features around nearby galaxies: I. Enhanced SDSS imaging of the Local Volume". arXiv:1804.03330. DOI: 10.1051/0004-6361/201732271 vii Abstract In hierarchical models of galaxy formation, stellar tidal streams are expected around most galaxies. Although these features may provide useful diagnostics of the LCDM model, their observational properties remain poorly constrained. Statistical analysis of the counts and properties of such features is of interest for a direct comparison against results from numeri- cal simulations. In this work, we aim to study systematically the frequency of occurrence and other observational properties of tidal features around nearby galaxies. -
HERD Proposal
HERD proposal The Joint Working Team for the HERD collaboration O. Adriani1,2, G. Ambrosi3, Y. Bai4, B. Bertucci3,5, X. Bi6, J. Casaus7, I. De Mitri8,9, M. Dong10, Y. Dong6, I. Donnarumma11, F. Gargano12, E. Liang13, H. Liu13, C. Lyu10, G. Marsella14,15, M.N. Maziotta12, N. Mori2, M. Su16, A. Surdo14, L. Wang4, X. Wu17, Y. Yang10, Q. Yuan18, S. Zhang6, T. Zhang10, L. Zhao10, H. Zhong10, and K. Zhu6 ii 1University of Florence, Department of Physics, I-50019 Sesto Fiorentino, Florence, Italy 2Istituto Nazionale di Fisica Nucleare, Sezione di Firenze, I-50019 Sesto Fiorentino, Florence, Italy 3Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy 4Xi’an Institute of Optics and Precision Mechanics of CAS, 17 Xinxi Road, New Industrial Park, Xi’an Hi-Tech Industrial Development Zone, Xi’an, Shaanxi, China 5Dipartimento di Fisica e Geologia, Universita degli Studi di Perugia, I-06123 Perugia, Italy 6Institute of High Energy Physics, Chinese Academy of Sciences, No. 19B Yuquan Road, Shijingshan District, Beijing 100049, China 7Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas, CIEMAT. Av. Complutense 40, Madrid E-28040, Spain 8Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100, L’Aquila, Italy 9INFN Laboratori Nazionali del Gran Sasso, Assergi, L’Aquila, Italy 10Technology and Engineering Center for Space Utilization, Chinese Academy of Sciences, 9 Dengzhuang South Rd., Haidian Dist., Beijing 100094, China 11Agenzia Spaziale Italiana (ASI), I-00133 Roma, Italy 12Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70125, Bari, Italy 13Guangxi University, 100 Daxue East Road, Nanning City, Guangxi, China 14Istituto Nazionale di Fisica Nucleare, Sezione di Lecce, I-73100, Lecce, Italy 15Universita del Salento - Dipartimento di Matematica e Fisica ”E. -
ORBITAL X-RAY VARIABILITY of the MICROQUASAR LS 5039 Valentı´ Bosch-Ramon,1 Josep M
The Astrophysical Journal, 628:388–394, 2005 July 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. ORBITAL X-RAY VARIABILITY OF THE MICROQUASAR LS 5039 Valentı´ Bosch-Ramon,1 Josep M. Paredes,1 Marc Ribo´,2 Jon M. Miller,3, 4 Pablo Reig,5, 6 and Josep Martı´7 Receivedv 2004 October 14; accepted 2005 February 26 ABSTRACT The properties of the orbit and the donor star in the high-mass X-ray binary microquasar LS 5039 indicate that accretion processes should mainly occur via a radiatively driven wind. In such a scenario, significant X-ray variability would be expected due to the eccentricity of the orbit. The source has been observed at X-rays by several missions, although with a poor coverage that prevents reaching any conclusion about orbital variability. Therefore, we conducted RXTE observations of the microquasar system LS 5039 covering a full orbital period of 4 days. Individual observations are well fitted with an absorbed power law plus a Gaussian at 6.7 keV, to account for iron- line emission that is probably a diffuse background feature. In addition, we have taken into account that the continuum is also affected by significant diffuse background contamination. Our results show moderate power-law flux variations on timescales of days, as well as the presence of miniflares on shorter timescales. The new orbital ephemerides of the system recently obtained by Casares et al. have allowed us to show, for the first time, that an increase of emission is seen close to the periastron passage, as expected in an accretion scenario. -
Curriculum Vitae Avishay Gal-Yam
January 27, 2017 Curriculum Vitae Avishay Gal-Yam Personal Name: Avishay Gal-Yam Current address: Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel. Telephones: home: 972-8-9464749, work: 972-8-9342063, Fax: 972-8-9344477 e-mail: [email protected] Born: March 15, 1970, Israel Family status: Married + 3 Citizenship: Israeli Education 1997-2003: Ph.D., School of Physics and Astronomy, Tel-Aviv University, Israel. Advisor: Prof. Dan Maoz 1994-1996: B.Sc., Magna Cum Laude, in Physics and Mathematics, Tel-Aviv University, Israel. (1989-1993: Military service.) Positions 2013- : Head, Physics Core Facilities Unit, Weizmann Institute of Science, Israel. 2012- : Associate Professor, Weizmann Institute of Science, Israel. 2008- : Head, Kraar Observatory Program, Weizmann Institute of Science, Israel. 2007- : Visiting Associate, California Institute of Technology. 2007-2012: Senior Scientist, Weizmann Institute of Science, Israel. 2006-2007: Postdoctoral Scholar, California Institute of Technology. 2003-2006: Hubble Postdoctoral Fellow, California Institute of Technology. 1996-2003: Physics and Mathematics Research and Teaching Assistant, Tel Aviv University. Honors and Awards 2012: Kimmel Award for Innovative Investigation. 2010: Krill Prize for Excellence in Scientific Research. 2010: Isreali Physical Society (IPS) Prize for a Young Physicist (shared with E. Nakar). 2010: German Federal Ministry of Education and Research (BMBF) ARCHES Prize. 2010: Levinson Physics Prize. 2008: The Peter and Patricia Gruber Award. 2007: European Union IRG Fellow. 2006: “Citt`adi Cefal`u"Prize. 2003: Hubble Fellow. 2002: Tel Aviv U. School of Physics and Astronomy award for outstanding achievements. 2000: Colton Fellow. 2000: Tel Aviv U. School of Physics and Astronomy research and teaching excellence award. -
Variable Star Section Circular No
The British Astronomical Association Variable Star Section Circular No. 176 June 2018 Office: Burlington House, Piccadilly, London W1J 0DU Contents Joint BAA-AAVSO meeting 3 From the Director 4 V392 Per (Nova Per 2018) - Gary Poyner & Robin Leadbeater 7 High-Cadence measurements of the symbiotic star V648 Car using a CMOS camera - Steve Fleming, Terry Moon and David Hoxley 9 Analysis of two semi-regular variables in Draco – Shaun Albrighton 13 V720 Cas and its close companions – David Boyd 16 Introduction to AstroImageJ photometry software – Richard Lee 20 Project Melvyn, May 2018 update – Alex Pratt 25 Eclipsing Binary news – Des Loughney 27 Summer Eclipsing Binaries – Christopher Lloyd 29 68u Herculis – David Conner 36 The BAAVSS Eclipsing Binary Programme lists – Christopher Lloyd 39 Section Publications 42 Contributing to the VSSC 42 Section Officers 43 Cover image V392 Per (Nova Per 2018) May 6.129UT iTelescope T11 120s. Martin Mobberley 2 Back to contents Joint BAA/AAVSO Meeting on Variable Stars Warwick University Saturday 7th & Sunday 8th July 2018 Following the last very successful joint meeting between the BAAVSS and the AAVSO at Cambridge in 2008, we are holding another joint meeting at Warwick University in the UK on 7-8 July 2018. This two-day meeting will include talks by Prof Giovanna Tinetti (University College London) Chemical composition of planets in our Galaxy Prof Boris Gaensicke (University of Warwick) Gaia: Transforming Stellar Astronomy Prof Tom Marsh (University of Warwick) AR Scorpii: a remarkable highly variable -
LS 5039: a Runaway Microquasar Ejected from the Galactic Plane
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) LS 5039: a runaway microquasar ejected from the galactic plane M. Rib´o1, J. M. Paredes1, G. E. Romero2, P. Benaglia2, J. Mart´ı3, O. Fors1, and J. Garc´ıa-S´anchez1 1 Departament d’Astronomia i Meteorologia, Universitat de Barcelona, Av. Diagonal 647, 08028 Barcelona, Spain 2 Instituto Argentino de Radioastronom´ıa, C.C.5, (1894) Villa Elisa, Buenos Aires, Argentina 3 Departamento de F´ısica, Escuela Polit´ecnica Superior, Universidad de Ja´en, Virgen de la Cabeza 2, 23071 Ja´en, Spain Received 10 December 2001 / Accepted 10 January 2002 Abstract. We have compiled optical and radio astrometric data of the microquasar LS 5039 and derived its proper motion. This, together with the distance and radial velocity of the system, allows us to state that this source is escaping from its own regional standard of rest, with a total systemic velocity of about 150 km s−1 − and a component perpendicular to the galactic plane larger than 100 km s 1. This is probably the result of an acceleration obtained during the supernova event that created the compact object in this binary system. We have computed the trajectory of LS 5039 in the past, and searched for OB associations and supernova remnants in its path. In particular, we have studied the possible association between LS 5039 and the supernova remnant G016.8−01.1, which, despite our efforts, remains dubious. We have also discovered and studied an H i cavity in the ISM, which could have been created by the stellar wind of LS 5039 or by the progenitor of the compact object in the system. -
Optical and Near-Infrared Monitoring of Gamma-Ray Binaries Hosting Be Stars
universe Article Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars Yuki Moritani 1,2,* and Akiko Kawachi 3 1 Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan 2 Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama Higashi-Hiroshima, Hiroshima 739-8526, Japan 3 Department of Physics, School of Science, Tokai University, 4-1-1 Kita-kaname, Hiratsuka 259-1292, Japan; [email protected] * Correspondence: [email protected] Abstract: Optical and near-infrared observations are compiled for the three gamma-ray binaries hosting Be stars: PSR B1259−63, LSI+61 303, and HESS J0632+057. The emissions from the Be disk are considered to vary according to the changes in its structure, some of which are caused by interactions with the compact object (e.g., tidal forces). Due to the high eccentricity and large orbit of these systems, the interactions—and, hence the resultant observables—depend on the orbital phase. To explore such variations, multi-band photometry and linear polarization were monitored for the three considered systems, using two 1.5 m-class telescopes: IRSF at the South African Astronomical Observatory and Kanata at the Higashi–Hiroshima Observatory. Keywords: gamma-ray binaries; optical and near-infrared; Be stars; circumstellar disk; gamma-ray binaries—individual (PSR B1259−63, LSI+61 303, HESS J0632+057) Citation: Moritani, Y.; Kawachi, A. Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars. -
Libro Resumen Sea2016v55 0.Pdf
2 ...................................................................................................................................... 4 .................................................................................................. 4 ........................................................................................................... 4 PATROCINADORES .................................................................................................................... 5 RESUMEN PROGRAMA GENERAL ............................................................................................ 7 PLANO BIZKAIA ARETOA .......................................................................................................... 8 .......................................................................................... 9 CONFERENCIAS PLENARIAS ................................................................................................... 14 ............................................................................................. 19 ................................................................................................ 21 ............... 23 CIENCIAS PLANETARIAS ......................................................................................................... 25 - tarde ....................................................................................................... 25 - ............................................................................................ 28 - tarde ................................................................................................ -
On the Radio Emitting High Mass X-Ray Binary LS 5039
A&A 376, 476–483 (2001) Astronomy DOI: 10.1051/0004-6361:20010919 & c ESO 2001 Astrophysics On the radio emitting high mass X-ray binary LS 5039 J. S. Clark1,2,P.Reig3,4,S.P.Goodwin1,5,V.M.Larionov6,7,P.Blay8,M.J.Coe9, J. Fabregat8, I. Negueruela10, I. Papadakis3, and I. A. Steele11 1 Astronomy Centre, CPES, University of Sussex, Brighton, BN1 9QH, UK 2 Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, England, UK 3 Physics Department, University of Crete, PO Box 2208, 71003, Heraklion, Greece 4 Foundation for Research and Technology–Hellas, 71110, Heraklion, Greece 5 Department of Physics and Astronomy, University of Wales, Cardiff, CF24 3YB, Wales, UK 6 Astronomical Institute of St. Petersburg University, St. Petersburg 198904, Russia 7 Isaac Newton Institute of Chile, St. Petersburg Branch 8 Departmento de Astronomia, Universidad de Valencia, 46100 Burjassot, Valencia, Spain 9 Department of Physics & Astronomy, University of Southampton, Highfield, Southampton, SO17 1BJ, UK 10 Observatoire de Strasbourg, 11 rue de l’Universit´e, 67000 Strasbourg, France 11 Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L41 1LD, UK Received 24 April 2001 / Accepted 26 June 2001 Abstract. We present new optical – near–IR spectroscopic and photometric observations of the newly discovered galactic microquasar LS 5039, which indicate a classification for the mass donor in the system of O6.5V((f)). Optical spectroscopy and photometry shows no variability over a timescale of years, and we find no evidence of modulation by, or emission from the compact companion in these data. -
Observing the Unique Binary PSR B1259−63/LS 2883
Observing the unique binary PSR B1259−63/LS 2883 P.H.T. Tam, A.K.H. Kong, R.H.H. Huang, J.H.K. Wu, Phyllis Yen National Tsing Hua University, Taiwan K. S. Cheng, Gene Leung, J. Takata, E.W.H.Wu The University of Hong Kong, Hong Kong C. Y. Hui Chungnam National University, Korea on behalf of the Fermi Asian Network 1 Introduction A new class of high-mass X-ray binaries (HMXBs) have been recently discovered as γ-ray emitters. These binaries contain a compact object orbiting an OB companion star. It is commonly believed that energetic particles are either accelerated in jets or in the collision shocks between the stellar wind and pulsar wind, in turn up- scattering the optical to UV lights to GeV{TeV γ-rays. Pulsed γ-rays from pulsar magnetosphere might also contribute to the observed photons up to a few GeV. Several groups of authors have proposed phenomenological models to explain the high-energy emission behaviors of γ-ray binaries (e.g., Dubus 2006, Takata & Taam 2009, Kong et al. 2011, Zabalza et al. 2013). Up to now, the following five systems are confirmed GeV and/or TeV γ-ray bi- nary systems (in ascending order of the orbital periods): LS 5039 (3.9 days), 1FGL J1018.6−5856 (16.6 days), LS I +61 303 (26.5 days), HESS J0632+057 (321 days), and PSR B1259−63 (3.4 years). For LS 5039 and LS I +61 303, GeV and/or TeV γ-ray emission are modulated on the orbital period but is easily detected throughout the whole orbit. -
University of Groningen Warps in Disk Galaxies Garcнa Ruiz, Iсigo
University of Groningen Warps in disk galaxies García Ruiz, Iñigo IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2001 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): García Ruiz, I. (2001). Warps in disk galaxies. s.n. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 07-10-2021 4 Neutral Hydrogen and Optical Observations of Edge-on Galaxies: The data Based on a paper by I. Garc´ıa-Ruiz, R. Sancisi & K.