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GRB 180418A: a Possibly Short Gamma-Ray Burst with a Wide-Angle Outflow in a Faint Host Galaxy
GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy Item Type Article; text Authors Rouco Escorial, A.; Fong, W.; Veres, P.; Laskar, T.; Lien, A.; Paterson, K.; Lally, M.; Blanchard, P.K.; Nugent, A.E.; Tanvir, N.R.; Cornish, D.; Berger, E.; Burns, E.; Cenko, S.B.; Cobb, B.E.; Cucchiara, A.; Goldstein, A.; Margutti, R.; Metzger, B.D.; Milne, P.; Levan, A.; Nicholl, M.; Smith, N. Citation Rouco Escorial, A., Fong, W., Veres, P., Laskar, T., Lien, A., Paterson, K., Lally, M., Blanchard, P. K., Nugent, A. E., Tanvir, N. R., Cornish, D., Berger, E., Burns, E., Cenko, S. B., Cobb, B. E., Cucchiara, A., Goldstein, A., Margutti, R., Metzger, B. D., … Smith, N. (2021). GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy. Astrophysical Journal, 912(2). DOI 10.3847/1538-4357/abee85 Publisher IOP Publishing Ltd Journal Astrophysical Journal Rights © 2021. The American Astronomical Society. All rights reserved. Download date 28/09/2021 16:20:20 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/660724 The Astrophysical Journal, 912:95 (19pp), 2021 May 10 https://doi.org/10.3847/1538-4357/abee85 © 2021. The American Astronomical Society. All rights reserved. GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy A. Rouco Escorial1, W. Fong1 , P. Veres2 , T. Laskar3 , A. Lien4,5, K. Paterson1 , M. Lally1 , P. K. -
GRIPS-Gamma-Ray Imaging, Polarimetry and Spectroscopy
Experimental Astronomy manuscript No. (will be inserted by the editor) GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy www.grips-mission.eu? Jochen Greiner · Karl Mannheim · Felix Aharonian · Marco Ajello · Lajos G. Balasz · Guido Barbiellini · Ronaldo Bellazzini · Shawn Bishop · Gennady S. Bisnovatij-Kogan · Steven Boggs · Andrej Bykov · Guido DiCocco · Roland Diehl · Dominik Els¨asser · Suzanne Foley · Claes Fransson · Neil Gehrels · Lorraine Hanlon · Dieter Hartmann · Wim Hermsen · Wolfgang Hillebrandt · Rene Hudec · Anatoli Iyudin · Jordi Jose · Matthias Kadler · Gottfried Kanbach · Wlodek Klamra · J¨urgenKiener · Sylvio Klose · Ingo Kreykenbohm · Lucien M. Kuiper · Nikos Kylafis · Claudio Labanti · Karlheinz Langanke · Norbert Langer · Stefan Larsson · Bruno Leibundgut · Uwe Laux · Francesco Longo · Kei'ichi Maeda · Radoslaw Marcinkowski · Martino Marisaldi · Brian McBreen · Sheila McBreen · Attila Meszaros · Ken'ichi Nomoto · Mark Pearce · Asaf Peer · Elena Pian · Nikolas Prantzos · Georg Raffelt · Olaf Reimer · Wolfgang Rhode · Felix Ryde · Christian Schmidt · Joe Silk · Boris M. Shustov · Andrew Strong · Nial Tanvir · Friedrich-Karl Thielemann · Omar Tibolla · David Tierney · Joachim Tr¨umper · Dmitry A. Varshalovich · J¨orn Wilms · Grzegorz Wrochna · Andrzej Zdziarski · Andreas Zoglauer Received: 21 April 2011 / Accepted: 2011 ? See this Web-site for the author's affiliations. Jochen Greiner Karl Mannheim MPI f¨urextraterrestrische Physik Inst. f. Theor. Physik & Astrophysik, Univ. W¨urzburg arXiv:1105.1265v1 [astro-ph.HE] 6 May 2011 85740 Garching, Germany 97074 W¨urzburg,Germany Tel.: +49-89-30000-3847 Tel.: +49-931-318-500 E-mail: [email protected] E-mail: [email protected] 2 Abstract We propose to perform a continuously scanning all-sky survey from 200 keV to 80 MeV achieving a sensitivity which is better by a factor of 40 or more compared to the previous missions in this energy range (COMPTEL, INTEGRAL; see Fig. -
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. -
JOHN R. THORSTENSEN Address
CURRICULUM VITAE: JOHN R. THORSTENSEN Address: Department of Physics and Astronomy Dartmouth College 6127 Wilder Laboratory Hanover, NH 03755-3528; (603)-646-2869 [email protected] Undergraduate Studies: Haverford College, B. A. 1974 Astronomy and Physics double major, High Honors in both. Graduate Studies: Ph. D., 1980, University of California, Berkeley Astronomy Department Dissertation : \Optical Studies of Faint Blue X-ray Stars" Graduate Advisor: Professor C. Stuart Bowyer Employment History: Department of Physics and Astronomy, Dartmouth College: { Professor, July 1991 { present { Associate Professor, July 1986 { July 1991 { Assistant Professor, September 1980 { June 1986 Research Assistant, Space Sciences Lab., U.C. Berkeley, 1975 { 1980. Summer Student, National Radio Astronomy Observatory, 1974. Summer Student, Bartol Research Foundation, 1973. Consultant, IBM Corporation, 1973. (STARMAP program). Honors and Awards: Phi Beta Kappa, 1974. National Science Foundation Graduate Fellow, 1974 { 1977. Dorothea Klumpke Roberts Award of the Berkeley Astronomy Dept., 1978. Professional Societies: American Astronomical Society Astronomical Society of the Pacific International Astronomical Union Lifetime Publication List * \Can Collapsed Stars Close the Universe?" Thorstensen, J. R., and Partridge, R. B. 1975, Ap. J., 200, 527. \Optical Identification of Nova Scuti 1975." Raff, M. I., and Thorstensen, J. 1975, P. A. S. P., 87, 593. \Photometry of Slow X-ray Pulsars II: The 13.9 Minute Period of X Persei." Margon, B., Thorstensen, J., Bowyer, S., Mason, K. O., White, N. E., Sanford, P. W., Parkes, G., Stone, R. P. S., and Bailey, J. 1977, Ap. J., 218, 504. \A Spectrophotometric Survey of the A 0535+26 Field." Margon, B., Thorstensen, J., Nelson, J., Chanan, G., and Bowyer, S. -
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. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
GRB 190114C: an Upgraded Legend Arxiv:1901.07505V2 [Astro-Ph.HE] 25 Mar 2019
GRB 190114C: An Upgraded Legend Yu Wang1;2, Liang Li 1, Rahim Moradi 1;2, Remo Ruffini 1;2;3;4;5;6 1ICRANet, P.zza della Repubblica 10, 65122 Pescara, Italy. 2ICRA and Dipartimento di Fisica, Sapienza Universita` di Roma, P.le Aldo Moro 5, 00185 Rome, Italy. 3ICRANet - INAF, Viale del Parco Mellini 84, 00136 Rome, Italy. 4Universite´ de Nice Sophia Antipolis, CEDEX 2, Grand Chateauˆ Parc Valrose, Nice, France. 5ICRANet-Rio, Centro Brasileiro de Pesquisas F´ısicas, Rua Dr. Xavier Sigaud 150, 22290–180 Rio de Janeiro, Brazil. 6ICRA, University Campus Bio-Medico of Rome, Via Alvaro del Portillo 21, I-00128 Rome, Italy. [email protected], [email protected], [email protected], ruffi[email protected] arXiv:1901.07505v2 [astro-ph.HE] 25 Mar 2019 1 Gamma-ray burst (GRB) 190114C first resembles the legendary GRB 130427A: Both are strong sources of GeV emission, exhibiting consistent GeV spectral evolution, and almost identical in detail for the morphology of light-curves in X-ray, gamma-ray and GeV bands, inferring a standard system with differ- ent scales. GRB 190114C is richer than GRB 130427A: a large percentage of ∼ 30% energy is thermal presenting in the gamma-ray prompt emission, mak- ing it as one of the most thermal-prominent GRBs; Moreover, GRB 190114C extends the horizon of GRB research, that for the first time the ultra-high energy TeV emission (> 300 GeV) is detected in a GRB as reported by the MAGIC team. Furthermore, GRB 190114C urges us to revisit the traditional theoretical framework, since most of the GRB’s energy may emit in the GeV and TeV range, not in the conventional MeV range. -
Urania Nr 5/2001
Eta Carinae To zdjęcie mgławicy otaczającej gwiazdę // Carinae uzyskano za po mocą telskopu kosmicznego Hubble a (K. Davidson i J. Mors). Porównując je z innymi zdjęciami, a w szczególności z obrazem wyko nanym 17 miesięcy wcześniej, Auto rzy stwierdzili rozprężanie się mgła wicy z szybkością ok. 2,5 min km/h, co prowadzi do wniosku, że rozpo częła ona swe istnienie około 150 lat temu. To bardzo ciekawy i intrygujący wynik. Otóż największy znany roz błysk )j Carinae miał miejsce w roku 1840. Wtedy gwiazda ta stała się naj jaśniejszą gwiazdą południowego nie ba i jasność jej przez krótki czas znacznie przewyższała blask gwiaz dy Canopus. Jednak pyłowy dysk ob serwowany wokół)/ Carinae wydaje się być znacznie młodszy - jego wiek (ekspansji) jest oceniany na 100 lat, co może znaczyć, że powstał w cza sie innego, mniejszego wybuchu ob serwowanego w roku 1890. Więcej na temat tego intrygują cego obiektu przeczytać można we wnątrz numeru, w artykule poświę conym tej gwieździe. NGC 6537 Obserwacje przeprowadzone teleskopem Hubble’a pokazały istnienie wielkich falowych struktur w mgławicy Czerwonego Pająka (NGC 6537) w gwiazdozbiorze Strzelca.Ta gorąca i „wietrzna” mgławica powstała wokół jednej z najgorętszych gwiazd Wszech świata, której wiatr gwiazdowy wiejący z prędkością 2000-4500 kilometrów na sekundę wytwarza fale o wysokości 100 miliardów kilometrów. Sama mgławica rozszerza się z szybkością 300 km/s. Jest też ona wyjątkowo gorąca — ok. 10000 K. Sama gwiazda, która utworzyła mgławicę, jest obecnie białym karłem i musi mieć temperaturę nie niższą niż pół miliona stopni — jest tak gorąca, że nie widać jej w obszarach uzyskanych teleskopem Hubble’a, a świeci głównie w promieniowaniu X. -
Staff, Visiting Scientists and Graduate Students 2010
Staff, Visiting Scientists and Graduate Students at the Pescara Center November 2010 2 Contents ICRANet Faculty Staff……………………………………………………………………. p. 17 Adjunct Professors of the Faculty .……………………………………………………… p. 31 Lecturers……………………………………………………………………………………..p. 67 Research Scientists ……………………………………………………………………….. p. 93 Short-term Visiting Scientists …………………………………………………………... p. 109 Long-Term Visiting Scientists …………………………………………………………... p. 129 IRAP Ph. D. Students …………………………………………………………………….. p. 141 IRAP Ph. D. Erasmus Mundus Students………………………………………………. p. 161 Administrative and Secretarial Staff …………………………………………………… p. 171 3 4 ICRANet Faculty Staff Belinski Vladimir ICRANet Bianco Carlo Luciano ICRANet Novello Mario Cesare Lattes-ICRANet Chair CBPF, Rio de Janeiro, Brasil Rueda Jorge A. ICRANet Ruffini Remo Università di Roma "Sapienza"and ICRANet Vereshchagin Gregory ICRANet Xue She-Sheng ICRANet 5 Adjunct Professors Of The Faculty Aharonian Felix Albert Benjamin Jegischewitsch Markarjan Chair Dublin Institute for Advanced Studies, Dublin, Ireland Max-Planck-Institut für Kernphysis, Heidelberg, Germany Amati Lorenzo Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy Arnett David Subramanyan Chandrasektar- ICRANet Chair University of Arizona, Tucson, USA Chakrabarti Sandip P. Centre for Space Physics, India Chardonnet Pascal Université de la Savoie, France Chechetkin Valeri Mstislav Vsevolodich Keldysh-ICRANet Chair Keldysh institute for Applied Mathematics Moscow, Russia Christodoulou Dimitrios ETH, Zurich, Switzerland Coppi Bruno -
Astronomical Distances
The Act of Measurement I: Astronomical Distances B. F. Riley The act of measurement causes astronomical distances to adopt discrete values. When measured, the distance to the object corresponds through an inverse 5/2 power law – the Quantum/Classical connection – to a sub-Planckian mass scale on a level or sub-level of one or both of two geometric sequences, of common ratio 1/π and 1/e, that descend from the Planck mass and may derive from the geometry of a higher-dimensional spacetime. The distances themselves lie on the levels and sub-levels of two sequences, of common ratio π and e, that ascend from the Planck length. Analyses have been performed of stellar distances, the semi-major axes of the planets and planetary satellites of the Solar System and the distances measured to quasars, galaxies and gamma-ray bursts. 1 Introduction Using Planck units the Quantum/Classical connection, characterised by the equation (1) maps astronomical distances R – in previous papers only the radii of astronomical bodies [1, 2] – onto sub-Planckian mass scales m on the mass levels and sub-levels1 of two geometric sequences that descend from the Planck mass: Sequence 1 of common ratio 1/π and Sequence 3 of common ratio 1/e.2 The sequences may derive from the geometry of a higher-dimensional spacetime [3]. First, we show that several distances associated with the Alpha Centauri system correspond through (1) to the mass scales of principal levels3 in Sequences 1 and 3. We then show that the mass scales corresponding through (1) to the distances from both Alpha Centauri and the Sun to the other stars lie on the levels and sub-levels of Sequences 1 and 3. -
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: Gw170817 and Grb 170817A
Draft version October 15, 2017 Typeset using LATEX twocolumn style in AASTeX61 GRAVITATIONAL WAVES AND GAMMA-RAYS FROM A BINARY NEUTRON STAR MERGER: GW170817 AND GRB 170817A B. P. Abbott,1 R. Abbott,1 T. D. Abbott,2 F. Acernese,3, 4 K. Ackley,5, 6 C. Adams,7 T. Adams,8 P. Addesso,9 R. X. Adhikari,1 V. B. Adya,10 C. Affeldt,10 M. Afrough,11 B. Agarwal,12 M. Agathos,13 K. Agatsuma,14 N. Aggarwal,15 O. D. Aguiar,16 L. Aiello,17, 18 A. Ain,19 P. Ajith,20 B. Allen,10, 21, 22 G. Allen,12 A. Allocca,23, 24 M. A. Aloy,25 P. A. Altin,26 A. Amato,27 A. Ananyeva,1 S. B. Anderson,1 W. G. Anderson,21 S. V. Angelova,28 S. Antier,29 S. Appert,1 K. Arai,1 M. C. Araya,1 J. S. Areeda,30 N. Arnaud,29, 31 K. G. Arun,32 S. Ascenzi,33, 34 G. Ashton,10 M. Ast,35 S. M. Aston,7 P. Astone,36 D. V. Atallah,37 P. Aufmuth,22 C. Aulbert,10 K. AultONeal,38 C. Austin,2 A. Avila-Alvarez,30 S. Babak,39 P. Bacon,40 M. K. M. Bader,14 S. Bae,41 P. T. Baker,42 F. Baldaccini,43, 44 G. Ballardin,31 S. W. Ballmer,45 S. Banagiri,46 J. C. Barayoga,1 S. E. Barclay,47 B. C. Barish,1 D. Barker,48 K. Barkett,49 F. Barone,3, 4 B. Barr,47 L. Barsotti,15 M. Barsuglia,40 D. Barta,50 J. -
List of Easy Double Stars for Winter and Spring = Easy = Not Too Difficult = Difficult but Possible
List of Easy Double Stars for Winter and Spring = easy = not too difficult = difficult but possible 1. Sigma Cassiopeiae (STF 3049). 23 hr 59.0 min +55 deg 45 min This system is tight but very beautiful. Use a high magnification (150x or more). Primary: 5.2, yellow or white Seconary: 7.2 (3.0″), blue 2. Eta Cassiopeiae (Achird, STF 60). 00 hr 49.1 min +57 deg 49 min This is a multiple system with many stars, but I will restrict myself to the brightest one here. Primary: 3.5, yellow. Secondary: 7.4 (13.2″), purple or brown 3. 65 Piscium (STF 61). 00 hr 49.9 min +27 deg 43 min Primary: 6.3, yellow Secondary: 6.3 (4.1″), yellow 4. Psi-1 Piscium (STF 88). 01 hr 05.7 min +21 deg 28 min This double forms a T-shaped asterism with Psi-2, Psi-3 and Chi Piscium. Psi-1 is the uppermost of the four. Primary: 5.3, yellow or white Secondary: 5.5 (29.7), yellow or white 5. Zeta Piscium (STF 100). 01 hr 13.7 min +07 deg 35 min Primary: 5.2, white or yellow Secondary: 6.3, white or lilac (or blue) 6. Gamma Arietis (Mesarthim, STF 180). 01 hr 53.5 min +19 deg 18 min “The Ram’s Eyes” Primary: 4.5, white Secondary: 4.6 (7.5″), white 7. Lambda Arietis (H 5 12). 01 hr 57.9 min +23 deg 36 min Primary: 4.8, white or yellow Secondary: 6.7 (37.1″), silver-white or blue 8.