Searching for Gamma-Ray Binaries in Multiwavelength Catalogs
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Star Maps: Where Are the Black Holes?
BLACK HOLE FAQ’s 1. What is a black hole? A black hole is a region of space that has so much mass concentrated in it that there is no way for a nearby object to escape its gravitational pull. There are three kinds of black hole that we have strong evidence for: a. Stellar-mass black holes are the remaining cores of massive stars after they die in a supernova explosion. b. Mid-mass black hole in the centers of dense star clusters Credit : ESA, NASA, and F. Mirabel c. Supermassive black hole are found in the centers of many (and maybe all) galaxies. 2. Can a black hole appear anywhere? No, you need an amount of matter more than 3 times the mass of the Sun before it can collapse to create a black hole. 3. If a star dies, does it always turn into a black hole? No, smaller stars like our Sun end their lives as dense hot stars called white dwarfs. Much more massive stars end their lives in a supernova explosion. The remaining cores of only the most massive stars will form black holes. 4. Will black holes suck up all the matter in the universe? No. A black hole has a very small region around it from which you can't escape, called the “event horizon”. If you (or other matter) cross the horizon, you will be pulled in. But as long as you stay outside of the horizon, you can avoid getting pulled in if you are orbiting fast enough. 5. What happens when a spaceship you are riding in falls into a black hole? Your spaceship, along with you, would be squeezed and stretched until it was torn completely apart as it approached the center of the black hole. -
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. -
Astrophysics in 2002
UC Irvine UC Irvine Previously Published Works Title Astrophysics in 2002 Permalink https://escholarship.org/uc/item/8rz4m3tt Journal Publications of the Astronomical Society of the Pacific, 115(807) ISSN 0004-6280 Authors Trimble, V Aschwanden, MJ Publication Date 2003 DOI 10.1086/374651 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Publications of the Astronomical Society of the Pacific, 115:514–591, 2003 May ᭧ 2003. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Invited Review Astrophysics in 2002 Virginia Trimble Department of Physics and Astronomy, University of California, Irvine, CA 92697; and Astronomy Department, University of Maryland, College Park, MD 20742; [email protected] and Markus J. Aschwanden Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Department L9-41, Building 252, 3251 Hanover Street, Palo Alto, CA 94304; [email protected] Received 2003 January 29; accepted 2003 January 29 ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well. -
Repetitive Patterns in Rapid Optical Variations in the Nearby Black-Hole Binary V404 Cygni
Repetitive Patterns in Rapid Optical Variations in the Nearby Black-hole Binary V404 Cygni Mariko Kimura1, Keisuke Isogai1, Taichi Kato1, Yoshihiro Ueda1, Satoshi Nakahira2, Megumi Shidatsu3, Teruaki Enoto1,4, Takafumi Hori1, Daisaku Nogami1, Colin Littlefield5, Ryoko Ishioka6, Ying-Tung Chen6, Sun-Kun King6, Chih-Yi Wen6, Shiang-Yu Wang6, Matthew J. Lehner6,7,8, Megan E. Schwamb6, Jen-Hung Wang6, Zhi-Wei Zhang6, Charles Alcock8, Tim Axelrod9, Federica B. Bianco10, Yong-Ik Byun11, Wen-Ping Chen12, Kem H. Cook6, Dae-Won Kim13, Typhoon Lee6, Stuart L. Marshall14, Elena P. Pavlenko15, Oksana I. Antonyuk15, Kirill A. Antonyuk15, Nikolai V. Pit15, Aleksei A. Sosnovskij15, Julia V. Babina15, Aleksei V. Baklanov15, Alexei S. Pozanenko16,17, Elena D. Mazaeva16, Sergei E. Schmalz18, Inna V. Reva19, Sergei P. Belan15, Raguli Ya. Inasaridze20, Namkhai Tungalag21, Alina A. Volnova16, Igor E. Molotov22, Enrique de Miguel23,24, Kiyoshi Kasai25, William Stein26, Pavol A. Dubovsky27, Seiichiro Kiyota28, Ian Miller29, Michael Richmond30, William Goff31, Maksim V. Andreev32,33, Hiromitsu Takahashi34, Naoto Kojiguchi35, Yuki Sugiura35, Nao Takeda35, Eiji Yamada35, Katsura Matsumoto35, Nick James36, Roger D. Pickard37,38, Tamás Tordai39, Yutaka Maeda40, Javier Ruiz41,42,43, Atsushi Miyashita44, Lewis M. Cook45, Akira Imada46 & Makoto Uemura47 1Department of Astronomy, Graduate School of Science, Kyoto University, Oiwakecho, Kitashirakawa, Sakyo-ku, Kyoto 606-8502, Japan! 2JEM Mission Operations and Integration Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan 3MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan 4The Hakubi Center for Advanced Research, Kyoto University, Kyoto 606-8302, Japan 5Astronomy Department, Wesleyan University, Middletown, CT 06459 USA !6Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU. -
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. -
Pos(MQW7)111 Ce
Long-term optical activity of the microquasar V4641 Sgr PoS(MQW7)111 Vojtechˇ Šimon Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondˇrejov, Czech Republic E-mail: [email protected] Arne Henden AAVSO, 49 Bay State Road, Cambridge, MA 02138, USA E-mail: [email protected] We present an analysis of the optical activity of the microquasar V4641 Sgr using the visual and photographic data. We analyze four smaller (echo) outbursts that followed the main outburst (1999). Their mean recurrence time TC is 377 days, with a trend of a decrease. We interpret the characteristic features of the recent activity of V4641 Sgr (the narrow outbursts separated by a long quiescence, a clear trend in the evolution of their TC) as the thermal instability of the accre- tion disk operating in dwarf novae and soft X-ray transients. We argue that the luminosity of four echo outbursts is too high to be explained by the thermal emission of the accretion disk. We inter- pret them as due to the thermal instability, in which the outburst gives rise to a jet radiating also in the optical. This supports the finding by Uemura et al., PASJ 54, L79 (2002). The pre-outburst observations (1964–1967) reveal ongoing activity of the system. It displays low-amplitude fluc- tuations on the timescale of several weeks, independent on the orbital phase. In addition, a larger brightening which lasted for several tens of days and occurred from the level of brightness higher than in other years can be resolved. VII Microquasar Workshop: Microquasars and Beyond September 1 - 5, 2008 Foca, Izmir, Turkey c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. -
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. -
Glossary of Terms Absorption Line a Dark Line at a Particular Wavelength Superimposed Upon a Bright, Continuous Spectrum
Glossary of terms absorption line A dark line at a particular wavelength superimposed upon a bright, continuous spectrum. Such a spectral line can be formed when electromag- netic radiation, while travelling on its way to an observer, meets a substance; if that substance can absorb energy at that particular wavelength then the observer sees an absorption line. Compare with emission line. accretion disk A disk of gas or dust orbiting a massive object such as a star, a stellar-mass black hole or an active galactic nucleus. An accretion disk plays an important role in the formation of a planetary system around a young star. An accretion disk around a supermassive black hole is thought to be the key mecha- nism powering an active galactic nucleus. active galactic nucleus (agn) A compact region at the center of a galaxy that emits vast amounts of electromagnetic radiation and fast-moving jets of particles; an agn can outshine the rest of the galaxy despite being hardly larger in volume than the Solar System. Various classes of agn exist, including quasars and Seyfert galaxies, but in each case the energy is believed to be generated as matter accretes onto a supermassive black hole. adaptive optics A technique used by large ground-based optical telescopes to remove the blurring affects caused by Earth’s atmosphere. Light from a guide star is used as a calibration source; a complicated system of software and hardware then deforms a small mirror to correct for atmospheric distortions. The mirror shape changes more quickly than the atmosphere itself fluctuates. -
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. -
Modeling Tev Γ-Rays from LS 5039: an Active OB Star at the Extreme Stan P
Active OB stars: structure, evolution, mass loss, and critical limits Proceedings IAU Symposium No. 272, 2010 c International Astronomical Union 2011 C. Neiner, G. Wade, G. Meynet & G. Peters, eds. doi:10.1017/S1743921311011471 Modeling TeV γ-rays from LS 5039: an active OB star at the extreme Stan P. Owocki1, Atsuo T. Okazaki2 and Gustavo Romero2 1 Bartol Research Institute, Department of Physics & Astronomy, University of Delaware Newark, DE 19716, USA email: [email protected] 2 Faculty of Engineering, Hokkai-Gakuen University Toyohira-ku, Sapporo 062-8605, Japan email: [email protected] 3 Facultad de Ciencias Astron´omicas y Geof´ısicas, Universidad Nacional de La Plata Paseo del Bosque, 1900 La Plata, Argentina email: [email protected] Abstract. Perhpas the most extreme examples of “Active OB stars” are the subset of high-mass X-ray binaries – consisting of an OB star plus compact companion – that have recently been observed by Fermi and ground-based Cerenkov telescopes like HESS to be sources of very high energy (VHE; up to 30 TeV!) γ-rays. This paper focuses on the prominent γ-ray source, LS5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical (e ≈ 0.24) orbit with its companion, assumed here to be a black-hole or unmagnetized neutron star. Using 3-D SPH simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle- Lyttleton (BHL) rate for the local radius and wind speed.