XMM-Newton Eric Gotthelf (Columbia University)
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
7.5 X 11.5.Doubleline.P65
Cambridge University Press 978-0-521-75618-1 - High Energy Astrophysics, Third Edition Malcolm S. Longair Index More information Name index Abell, George, 99, 101 Cappelluti, Nico, 729 Abraham, Robert, 733 Carter, Brandon, 434 Abramovitz, Milton, 206, 209 Caswell, James, 226 Adams, Fred, 353, 369 Cavaliere, Alfonso, 110 Amsler, Claude, 275 Cesarsky, Catherine, 187, 189 Anderson, Carl, 29, 30, 163 Challinor, Anthony, 115, 259 Arnaud, Monique, 110 Chandrasekhar, Subrahmanyan, 302, 429, 434, Arnett, David, 386 455 Arzoumanian, Zaven, 420 Charlot, Stephane,´ 729, 730, 747 Auger, Pierre, 29 Chwolson, O., 117 Cimatti, Andrea, 736, 748 Babbedge, T., 740 Clayton, Donald, 386 Backer, Donald, 417, 418 Clemmow, Phillip, 267 Bahcall, John, 55, 57, 58 Colless, Matthew, 108, 109 Bahcall, Neta, 105 Compton, Arthur, 231 Balbus, Steven, 455 Cordes, James, 420 Band, David, 264 Cowie, Lennox, 733, 736, 743, 745 Barger, Amy, 745 Cox, Donald, 357 Beckwith, Steven, 737, 744 Becquerel, Henri, 146 Damon, Paul, 297 Bekefi, George, 193 Davies, Rodney, 376 Bell(-Burnell), Jocelyn, 19, 406 Davis, Leverett, 373 Bennett, Charles, 16 Davis, Raymond, 32, 54, 55 Bethe, Hans, 57, 163, 166, 175 de Vaucouleurs, Gerard,´ 77, 78 Bignami, Giovanni, 197 Dermer, Charles, 505 Binney, James, 106, 153 Deubner, Franz-Ludwig, 51 Blaauw, Adriaan, 754 Diehl, Roland, 287 Blackett, Patrick, 29 Dirac, Adrian, 29 Blain, Andrew, 743 Djorgovski, George, 88 Bland-Hawthorn, Jonathan, 733 Dougherty, John, 267 Blandford, Roger, 251 Draine, Bruce, 351, 372, 373, 375, Blumenthal, George, 163, 175, -
Deep Optical Observations of Unusual Neutron Star Calvera with The
to appear in The Astrophysical Journal Deep optical observations of unusual neutron star Calvera with the GTC† Yury Shibanov1,2, Andrey Danilenko1, Sergey Zharikov3, Peter Shternin1, Dima Zyuzin1 ABSTRACT Calvera is an unusual isolated neutron star with pure thermal X-ray spectrum typical for central compact objects in supernova remnants. On the other hand, its rotation period and spin-down rate are typical for ordinary rotation-powered pulsars. It was discovered and studied in X-rays and not yet detected in other spectral domains. We present deep optical imaging of the Calvera field obtained with the Gran Telescopio Canarias in g′ and i′ bands. Within ≈ 1′′ vicinity of Calvera, we detected two point-like objects invisible at previous shallow observations. However, accurate astrometry showed that none of them can be identified with the pulsar. We put new upper limits on its optical brightness of g′ > 27.87 and i′ > 26.84. We also reanalyzed all available archival X-ray data on Calvera. Comparison of the Calvera thermal emission parameters and upper limits on optical and non-thermal X-ray emission with respective data on rotation- powered pulsars shows that Calvera might belong to the class of ordinary middle-aged pulsars, if we assume that its distance is in the range of 1.5–5 kpc. Subject headings: stars: neutron – pulsars: general – pulsars: individual: Calvera, 1RXS J141256.0+792204, PSR J1412+7922 1. Introduction High Galactic latitude, b ≈ +37◦, compact source 1RXS J141256.0+792204 in the ROSAT All-Sky Survey was proposed as a neutron star (NS) candidate by Rutledge et al. -
The Iso Handbook
THE ISO HANDBOOK Volume I: ISO – Mission & Satellite Overview Martin F. Kessler1,2, Thomas G. M¨uller1,4, Kieron Leech 1, Christophe Arviset1, Pedro Garc´ıa-Lario1, Leo Metcalfe1, Andy M. T. Pollock1,3, Timo Prusti1,2 and Alberto Salama1 SAI-2000-035/Dc, Version 2.0 November, 2003 1 ISO Data Centre, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Villafranca del Castillo, P.O. Box 50727, E-28080 Madrid, Spain 2 ESTEC, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Keplerlaan 1, Postbus 299, 2200 AG Noordwijk, The Netherlands 3 Computer & Scientific Co. Ltd., 230 Graham Road, Sheffield S10 3GS, England 4 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany ii Document Information Document: The ISO Handbook Volume: I Title: ISO - Mission & Satellite Overview Reference Number: SAI/2000-035/Dc Issue: Version 2.0 Issue Date: November 2003 Authors: M.F. Kessler, T. M¨uller, K. Leech et al. Editors: T. M¨uller, J. Blommaert & P. Garc´ıa-Lario Web-Editor: J. Matagne Document History The ISO Handbook, Volume I: ISO – Mission & Satellite Overview is mainly based on the following documents: • The ISO Handbook, Volume I: ISO – Mission Overview, Kessler M.F., M¨uller T.G., Arviset C. et al., earlier versions, SAI-2000-035/Dc. • The ISO Handbook, Volume II: ISO – The Satellite and its Data, K. Leech & A.M.T. Pollock, earlier versions, SAI-99-082/Dc. • The following ESA Bulletin articles: The ISO Mission – A Scientific Overview, M.F. Kessler, A. -
Search for Very High-Energy Gamma-Ray Emission from Pulsar-Pwn Systems with the Magic Telescope
SUBMITTED TO THE ASTROPHYSICAL JOURNAL ON JUNE XX,2008 Preprint typeset using LATEX style emulateapj v. 10/09/06 SEARCH FOR VERY HIGH-ENERGY GAMMA-RAY EMISSION FROM PULSAR-PWN SYSTEMS WITH THE MAGIC TELESCOPE. 1 2 3 4 5 3 3 6 H. ANDERHUB ,L.A.ANTONELLI , P. ANTORANZ ,M.BACKES ,C.BAIXERAS ,S.BALESTRA ,J.A.BARRIO ,D.BASTIERI , 7 4 8 8 9 1 10 6 J. BECERRA GONZALEZ´ ,J.K.BECKER , W. BEDNAREK ,K.BERGER ,E.BERNARDINI ,A.BILAND ,R.K.BOCK , , 11 12 10 12 3 1 13 10 G. BONNOLI , P. BORDAS ,D.BORLA TRIDON , V. BOSCH-RAMON ,D.BOSE ,I.BRAUN , T.BRETZ ,D.BRITZGER , 3 10 2 10 1 3 14 7 15 M. CAMARA ,E.CARMONA ,A.CAROSI , P. COLIN ,S.COMMICHAU ,J.L.CONTRERAS ,J.CORTINA ,M.T.COSTADO , , 2 16 26 16 17 3 29 16 16 S. COVINO , F.DAZZI , ,A.DE ANGELIS , E. DE CEA DEL POZO ,R.DE LOS REYES , ,B.DE LOTTO ,M.DE MARIA , 16 7 27 18 19 1 6 13 F. DE SABATA ,C.DELGADO MENDEZ , ,A.DOM´INGUEZ ,D.DOMINIS PRESTER ,D.DORNER ,M.DORO ,D.ELSAESSER , 14 20 14 14 3 5 10 7 15 M. ERRANDO ,D.FERENC ,E.FERNANDEZ´ ,R.FIRPO ,M. V.FONSECA ,L.FONT ,N.GALANTE ,R.J.GARC´IA LOPEZ´ , , 14 7 19 10 28 5 7 15 1 M. GARCZARCZYK ,M.GAUG ,N.GODINOVIC , F.GOEBEL , ,D.HADASCH ,A.HERRERO , ,D.HILDEBRAND , 13 10 19 10 10 14 1 2 D. HOHNE¨ -MONCH¨ ,J.HOSE ,D.HRUPEC ,C.C.HSU , T. -
CONSTELLATION URSA MINOR, the LITTLE BEAR Ursa Minor
CONSTELLATION URSA MINOR, THE LITTLE BEAR Ursa Minor (Latin: "Smaller She-Bear", to contrast with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the North American name, Little Dipper. It has seven main stars with four in its bowl, like its partner the Big Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, because of Polaris (at the end of the tail) being the North Star. Alpha Ursae Minoris, better known as Polaris, is the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from an apparent magnitude of 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Gamma Ursae Minoris, magnitude 3 and Kochab have been called the "guardians of the pole star". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered, with a surface temperature of 200,000 K. HISTORY AND MYTHOLOGY In the Babylonian star catalogues, Ursa Minor was known as the Wagon of Heaven, Damkianna. -
The Very High Energy Characteristics of Shell-Type Snrs and Pulsar Wind Nebulae at Different Ages
Journal of Physics: Conference Series PAPER • OPEN ACCESS Related content - Non-Thermal Photon Emission from Shell- The very high energy characteristics of shell-type Type Supernova Remnants Dou Ya-Nan and Zhang Li SNRs and Pulsar Wind Nebulae at different ages - Waveguide CO2 laser with a power per unit length of about 1 W/cm W J Witteman, M Ilieva, B I Ilyukhin et al. To cite this article: V G Sinitsyna et al 2016 J. Phys.: Conf. Ser. 718 052045 - Pulse-periodic YAG laser system with phase conjugation I Yu Anikeev, A A Gordeev, I G Zubarev et al. View the article online for updates and enhancements. This content was downloaded from IP address 131.169.5.251 on 08/02/2019 at 23:15 XIV International Conference on Topics in Astroparticle and Underground Physics (TAUP 2015) IOP Publishing Journal of Physics: Conference Series 718 (2016) 052045 doi:10.1088/1742-6596/718/5/052045 The very high energy characteristics of shell-type SNRs and Pulsar Wind Nebulae at different ages V G Sinitsyna, A Y Alaverdyan, M S Andreeva, K A Balygin, S S Borisov, I A Ivanov, A M Kirichenko, A I Klimov, I P Kozhukhova, R M Mirzafatikhov, N I Moseiko, S I Nikolsky, I E Ostashev, A I Palamarchuk,V Y Sinitsyna, I G Volokh P.N. Lebedev Physical Institute, Leninsky pr. 53, Moscow, Russia E-mail: [email protected] Abstract. The investigation of VHE gamma-ray sources by any methods, including mirror Cherenkov telescopes, touches on the problem of the cosmic ray origin and, accordingly, the role of the Galaxy in their generation. -
Supernova Remnants and the Life Cycle of Interstellar Dust
Design Reference Mission Case Study Stratospheric Observatory for Infrared Astronomy Science Steering Committee Supernova Remnants and the Life Cycle of Interstellar Dust Program contacts: Eli Dwek, Richard Arendt, Jesse Bregman, Sean Colgan, Harriet Dinerstein, Robert Gehrz, Harvey Moseley Scientific category: INTERSTELLAR MEDIUM Instruments: EXES, FLITECAM/CAM, FORCAST, FIFI-LS, HAWC, SAFIRE Hours of observation: 110 Abstract We propose to use the unique instrumental capabilities of SOFIA to conduct imaging and spectroscopic studies of supernovae (SNe), of young supernova remnants (SNRs) for which the ejecta have not yet fully mixed with the ISM, and select regions in older remnants which are interacting with the ambient ISM. These observations will address key issues within NASA’s Visions for Science quest for discovering the origin, structure, evolution and destiny of the universe: What is the origin of dust in early universe? How efficient are supernovae in producing interstellar dust? How efficient are their blast waves in destroying, processing, or even forming dust as they expand into the circumstellar and interstellar medium? How do interstellar shocks facilitate chemical reaction on the surfaces of dust grains? The answers to these questions are crucial for understanding the evolutionary cycle of interstellar dust, the role of dust in the processing of starlight and in determining the thermal balance and chemistry of the ISM, and its role in the formation of protoplanetary objects. Our proposed observations will explore crucial stages of this evolutionary cycle, most readily observed at wavelengths between ∼ 5 − 300 µm with spectral resolution from ∼ 30 − 3 × 104, and at spatial resolution of a few arcseconds, requiring therefore the unique capabilities of the different SOFIA instruments. -
Exoplanet Secondary Atmosphere Loss and Revival Edwin S
Exoplanet secondary atmosphere loss and revival Edwin S. Kitea,1 and Megan N. Barnetta aDepartment of the Geophysical Sciences, University of Chicago, Chicago, IL 60637 Edited by Mark Thiemens, University of California San Diego, La Jolla, CA, and approved June 19, 2020 (received for review April 3, 2020) The next step on the path toward another Earth is to find atmo- atmosphere? Or does the light (H2-dominated) and transient pri- spheres similar to those of Earth and Venus—high–molecular- mary atmosphere drag away the higher–molecular-weight species? weight (secondary) atmospheres—on rocky exoplanets. Many rocky Getting physical insight into thetransitionfromprimarytosec- exoplanets are born with thick (>10 kbar) H2-dominated atmo- ondary atmospheres is particularly important for rocky exoplanets spheres but subsequently lose their H2; this process has no known that are too hot for life. Hot rocky exoplanets are the highest signal/ Solar System analog. We study the consequences of early loss of a noise rocky targets for upcoming missions such as James Webb thick H atmosphere for subsequent occurrence of a high–molecular- 2 Space Telescope (JWST) (8) and so will be the most useful for weight atmosphere using a simple model of atmosphere evolution (including atmosphere loss to space, magma ocean crystallization, and checking our understanding of this atmospheric transition process. volcanic outgassing). We also calculate atmosphere survival for rocky Secondary atmospheres are central to the exoplanet explora- tion strategy (9, 10). Previous work on the hypothesis that pri- worlds that start with no H2.Ourresultsimplythatmostrockyexo- planets orbiting closer to their star than the habitable zone that were mary atmospheres played a role in forming secondary atmospheres formed with thick H2-dominated atmospheres lack high–molecular- includes that of Eucken in the 1940s (11), Urey (12), Cameron and weight atmospheres today. -
X-Ray Properties of the Pulsar Psr J0205+6449 in 3C 58
Journal of the Korean Astronomical Society https://doi.org/10.5303/JKAS.2021.54.1.1 54: 1 ∼ 8, 2021 February pISSN: 1225-4614 · eISSN: 2288-890X Published under Creative Commons license CC BY-SA 4.0 http://jkas.kas.org X-RAY PROPERTIES OF THE PULSAR PSR J0205+6449 IN 3C 58 Minjun Kim and Hongjun An Department of Astronomy and Space Science, Chungbuk National University, Cheongju 28644, Republic of Korea; [email protected], [email protected] Received August 10, 2020; accepted December 24, 2020 Abstract: We report X-ray timing and spectral properties of the pulsar PSR J0205+6449 measured using NuSTAR and Chandra observatories. We measure the pulsar's rotation frequency ν = 15:20102357(9) s−1 and its derivative ν_ = −4:5(1) × 10−11 s−2 during the observation period, and model the 2{30 keV on-pulse spectrum of the pulsar with a power law having a photon index Γpsr = 1:07 ± 0:16 and a 2{30 keV flux −13 −2 −1 F2−30 keV = 7:3±0:6 × 10 erg cm s . The Chandra 0.5{10 keV data are analyzed for an investigation of the pulsar's thermal emission properties. We use thermal and non-thermal emission models to fit the Chandra spectra and infer the surface temperature T1 and luminosity Lth of the neutron star to be 32 −1 T1 = 0:5 − 0:8 MK and Lth = 1 − 5 × 10 erg s . This agrees with previous results which indicated that PSR J0205+6449 has a low surface temperature and luminosity for its age of 800{5600 yrs. -
Sommaire Des Annexes
Liste des publications 2001-2003 Sommaire des annexes Liste des publications 2001 - 2003_____________________________________________ 73 Refereed Journal Papers _______________________________________________________ 73 2001______________________________________________________________________________ 73 2002______________________________________________________________________________ 76 2003______________________________________________________________________________ 78 Conference Papers ____________________________________________________________ 83 2001______________________________________________________________________________ 83 2002______________________________________________________________________________ 89 2003______________________________________________________________________________ 93 Non-Refereed Journal Papers ___________________________________________________ 98 2002______________________________________________________________________________ 98 2003______________________________________________________________________________ 99 Livres ______________________________________________________________________ 101 2002_____________________________________________________________________________ 101 2003_____________________________________________________________________________ 101 Personnel du SAp au 1er janvier 2004 _________________________________________ 102 Légende ____________________________________________________________________ 102 Les activités d'interprétation ___________________________________________________ -
The Peculiar Isolated Neutron Star in the Carina Nebula Deep XMM-Newton and ESO-VLT Observations of 2XMM J104608.7-594306
A&A 544, A17 (2012) Astronomy DOI: 10.1051/0004-6361/201219161 & c ESO 2012 Astrophysics The peculiar isolated neutron star in the Carina Nebula Deep XMM-Newton and ESO-VLT observations of 2XMM J104608.7-594306 A. M. Pires1,C.Motch2, R. Turolla3,4,A.Schwope1, M. Pilia5,A.Treves6,S.B.Popov7, and E. Janot-Pacheco8 1 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany e-mail: [email protected] 2 CNRS, Université de Strasbourg, Observatoire Astronomique, 11 rue de l’Université, 67000 Strasbourg, France 3 Universitá di Padova, Dipartimento di Fisica e Astronomia, via Marzolo 8, 35131 Padova, Italy 4 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK 5 Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands 6 Universitá dell’Insubria, Dipartimento di Fisica e Matematica, via Valleggio 11, 22100 Como, Italy 7 Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, 119991 Moscow, Russia 8 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, R. do Matão 1226, 05508-090 São Paulo, Brazil Received 2 March 2012 / Accepted 7 May 2012 ABSTRACT While fewer in number than the dominant rotation-powered radio pulsar population, peculiar classes of isolated neutron stars (INSs) – which include magnetars, the ROSAT-discovered “Magnificent Seven” (M7), rotating radio transients (RRATs), and central compact objects in supernova remnants (CCOs) – represent a key element in understanding the neutron star phenomenology. We report the results of an observational campaign to study the properties of the source 2XMM J104608.7-594306, a newly discovered thermally emitting INS.