Pos(BASH 2013)009 † ∗ [email protected] Speaker
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Arxiv:1402.6337V1 [Astro-Ph.HE] 25 Feb 2014 Novae (SN Ia) Prevent Studies from Conclusively Singling Et Al
A review of type Ia supernova spectra J. Parrent1,2, B. Friesen3, and M. Parthasarathy4 Abstract SN 2011fe was the nearest and best-observed fairly certain that the progenitor system of SN Ia com- type Ia supernova in a generation, and brought previ- prises at least one compact C+O white dwarf (Chan- ous incomplete datasets into sharp contrast with the drasekhar 1957; Nugent et al. 2011; Bloom et al. 2012). detailed new data. In retrospect, documenting spectro- However, how the state of this primary star reaches scopic behaviors of type Ia supernovae has been more a critical point of disruption continues to elude as- often limited by sparse and incomplete temporal sam- tronomers. This is particularly so given that less than pling than by consequences of signal-to-noise ratios, ∼ 15% of locally observed white dwarfs have a mass a telluric features, or small sample sizes. As a result, few 0.1M greater than a solar mass; very few systems 5 type Ia supernovae have been primarily studied insofar near the formal Chandrasekhar-mass limit ,MCh ≈ as parameters discretized by relative epochs and incom- 1.38 M (Vennes 1999; Liebert et al. 2005; Napiwotzki plete temporal snapshots near maximum light. Here we et al. 2005; Parthasarathy et al. 2007; Napiwotzki et al. discuss a necessary next step toward consistently mod- 2007). eling and directly measuring spectroscopic observables Thus far observational constraints of SN Ia have of type Ia supernova spectra. In addition, we analyze been inconclusive in distinguishing between the follow- current spectroscopic data in the parameter space de- ing three separate theoretical considerations about pos- fined by empirical metrics, which will be relevant even sible progenitor scenarios. -
Iptf14hls: a Unique Long-Lived Supernova from a Rare Ex- Plosion Channel
iPTF14hls: A unique long-lived supernova from a rare ex- plosion channel I. Arcavi1;2, et al. 1Las Cumbres Observatory Global Telescope Network, Santa Barbara, CA 93117, USA. 2Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA. 1 Most hydrogen-rich massive stars end their lives in catastrophic explosions known as Type 2 IIP supernovae, which maintain a roughly constant luminosity for ≈100 days and then de- 3 cline. This behavior is well explained as emission from a shocked and expanding hydrogen- 56 4 rich red supergiant envelope, powered at late times by the decay of radioactive Ni produced 1, 2, 3 5 in the explosion . As the ejected mass expands and cools it becomes transparent from the 6 outside inwards, and decreasing expansion velocities are observed as the inner slower-moving 7 material is revealed. Here we present iPTF14hls, a nearby supernova with spectral features 8 identical to those of Type IIP events, but remaining luminous for over 600 days with at least 9 five distinct peaks in its light curve and expansion velocities that remain nearly constant in 10 time. Unlike other long-lived supernovae, iPTF14hls shows no signs of interaction with cir- 11 cumstellar material. Such behavior has never been seen before for any type of supernova 12 and it challenges all existing explosion models. Some of the properties of iPTF14hls can be 13 explained by the formation of a long-lived central power source such as the spindown of a 4, 5, 6 7, 8 14 highly magentized neutron star or fallback accretion onto a black hole . -
Planning the VLT Interferometer
No. 60 - -.June 1990 --, Planning the VLTVLT Interferometer J. M. BECKERS, ESO 1. The VlVLTT Interferometer: VLTVLT Reports 44 and 49), the interferointerfero- approved YLTVLT implementation. P. LemaLena One of the Operating Modes metric mode of the VLVLTT was indudedincluded in described the concept and planning torfor ofoftheVLT the VLT the VLTVLT proposal, and accepted inin theIhe the inlerferometricinterferometric mode of the VLTVLT at 1.1.11 Itsfts Context Adaptive Optics at the ESO 3.6-m Telescope The Very Large Telescope has three differenldifferent modes of being used. As four separate 8-metre telescopes it provides theIhe capabililycapability of carrying out in parallel tourfour different observing programmes, each with a sensitivitysensilivity which matches that of the other most powerful groundground- based telescopes available. In the secsec- ond mode the light of the four tele-lele scopes is combined in a single imageimage making ilit inin sensitivity the most powerful telescope on earth, almost 16t6 metres in diameter if the light losses in the beam eombinationcombination canean be kept low. In the third mode Ihethe light of the four tele-tele scopes is combined coherenlly,coherently, allowallow- This faise-colourfalse-colour photo illustrates the dramatiedramatic improvement in image sharpness whiehwhich is ing interferomelrlcinterferometric observations with the obtained with adaptive optiesoptics at the ESO 3.6·m3.6-m telescope. seeSee also the artielearticle on page 9. unparalleled sensitivity resulting fromtrom I1It shows the 5.5 magnitudemagnilude star HR 6658 in the galacticga/aeUe eluslercluster Messier 7 (NGC 6475), as the 8-metre apertures. In this mode theIhe observed in the infrared L·bandL-band (wavelength 3.5pm),3.Sllm), without ("ullcorrecled",("uncorrected", left) alldand with angular resolulionresolution is determined by the "corrected","corrected, right) the "VL"VLTT adaptive optics prototype" switched on. -
Ucalgary 2017 Welbankscamar
University of Calgary PRISM: University of Calgary's Digital Repository Graduate Studies The Vault: Electronic Theses and Dissertations 2017 Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh Welbanks Camarena, Luis Carlos Welbanks Camarena, L. C. (2017). Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh (Unpublished master's thesis). University of Calgary, Calgary, AB. doi:10.11575/PRISM/27339 http://hdl.handle.net/11023/3972 master thesis University of Calgary graduate students retain copyright ownership and moral rights for their thesis. You may use this material in any way that is permitted by the Copyright Act or through licensing that has been assigned to the document. For uses that are not allowable under copyright legislation or licensing, you are required to seek permission. Downloaded from PRISM: https://prism.ucalgary.ca UNIVERSITY OF CALGARY Photometric and Spectroscopic Signatures of Superluminous Supernova Events The puzzling case of ASASSN-15lh by Luis Carlos Welbanks Camarena A THESIS SUBMITTED TO THE FACULTY OF GRADUATE STUDIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE GRADUATE PROGRAM IN PHYSICS AND ASTRONOMY CALGARY, ALBERTA JULY, 2017 c Luis Carlos Welbanks Camarena 2017 Abstract Superluminous supernovae are explosions in the sky that far exceed the luminosity of standard supernova events. Their discovery shattered our understanding of stellar evolution and death. Par- ticularly, the discovery of ASASSN-15lh a monstrous event that pushed some of the astrophysical models to the limit and discarded others. In this thesis, I recount the photometric and spectroscopic signatures of superluminous super- novae, while discussing the limitations and advantages of the models brought forward to explain them. -
The Korean 1592--1593 Record of a Guest Star: Animpostor'of The
Journal of the Korean Astronomical Society 49: 00 ∼ 00, 2016 December c 2016. The Korean Astronomical Society. All rights reserved. http://jkas.kas.org THE KOREAN 1592–1593 RECORD OF A GUEST STAR: AN ‘IMPOSTOR’ OF THE CASSIOPEIA ASUPERNOVA? Changbom Park1, Sung-Chul Yoon2, and Bon-Chul Koo2,3 1Korea Institute for Advanced Study, 85 Hoegi-ro, Dongdaemun-gu, Seoul 02455, Korea; [email protected] 2Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Seoul 08826, Korea [email protected], [email protected] 3Visiting Professor, Korea Institute for Advanced Study, Dongdaemun-gu, Seoul 02455, Korea Received |; accepted | Abstract: The missing historical record of the Cassiopeia A (Cas A) supernova (SN) event implies a large extinction to the SN, possibly greater than the interstellar extinction to the current SN remnant. Here we investigate the possibility that the guest star that appeared near Cas A in 1592{1593 in Korean history books could have been an `impostor' of the Cas A SN, i.e., a luminous transient that appeared to be a SN but did not destroy the progenitor star, with strong mass loss to have provided extra circumstellar extinction. We first review the Korean records and show that a spatial coincidence between the guest star and Cas A cannot be ruled out, as opposed to previous studies. Based on modern astrophysical findings on core-collapse SN, we argue that Cas A could have had an impostor and derive its anticipated properties. It turned out that the Cas A SN impostor must have been bright (MV = −14:7 ± 2:2 mag) and an amount of dust with visual extinction of ≥ 2:8 ± 2:2 mag should have formed in the ejected envelope and/or in a strong wind afterwards. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
Central Engines and Environment of Superluminous Supernovae
Central Engines and Environment of Superluminous Supernovae Blinnikov S.I.1;2;3 1 NIC Kurchatov Inst. ITEP, Moscow 2 SAI, MSU, Moscow 3 Kavli IPMU, Kashiwa with E.Sorokina, K.Nomoto, P. Baklanov, A.Tolstov, E.Kozyreva, M.Potashov, et al. Schloss Ringberg, 26 July 2017 First Superluminous Supernova (SLSN) is discovered in 2006 -21 1994I 1997ef 1998bw -21 -20 56 2002ap Co to 2003jd 56 2007bg -19 Fe 2007bi -20 -18 -19 -17 -16 -18 Absolute magnitude -15 -17 -14 -13 -16 0 50 100 150 200 250 300 350 -20 0 20 40 60 Epoch (days) Superluminous SN of type II Superluminous SN of type I SN2006gy used to be the most luminous SN in 2006, but not now. Now many SNe are discovered even more luminous. The number of Superluminous Supernovae (SLSNe) discovered is growing. The models explaining those events with the minimum energy budget involve multiple ejections of mass in presupernova stars. Mass loss and build-up of envelopes around massive stars are generic features of stellar evolution. Normally, those envelopes are rather diluted, and they do not change significantly the light produced in the majority of supernovae. 2 SLSNe are not equal to Hypernovae Hypernovae are not extremely luminous, but they have high kinetic energy of explosion. Afterglow of GRB130702A with bumps interpreted as a hypernova. Alina Volnova, et al. 2017. Multicolour modelling of SN 2013dx associated with GRB130702A. MNRAS 467, 3500. 3 Our models of LC with STELLA E ≈ 35 foe. First year light ∼ 0:03 foe while for SLSNe it is an order of magnitude larger. -
Luminous Blue Variables: an Imaging Perspective on Their Binarity and Near Environment?,??
A&A 587, A115 (2016) Astronomy DOI: 10.1051/0004-6361/201526578 & c ESO 2016 Astrophysics Luminous blue variables: An imaging perspective on their binarity and near environment?;?? Christophe Martayan1, Alex Lobel2, Dietrich Baade3, Andrea Mehner1, Thomas Rivinius1, Henri M. J. Boffin1, Julien Girard1, Dimitri Mawet4, Guillaume Montagnier5, Ronny Blomme2, Pierre Kervella7;6, Hugues Sana8, Stanislav Štefl???;9, Juan Zorec10, Sylvestre Lacour6, Jean-Baptiste Le Bouquin11, Fabrice Martins12, Antoine Mérand1, Fabien Patru11, Fernando Selman1, and Yves Frémat2 1 European Organisation for Astronomical Research in the Southern Hemisphere, Alonso de Córdova 3107, Vitacura, 19001 Casilla, Santiago de Chile, Chile e-mail: [email protected] 2 Royal Observatory of Belgium, 3 avenue Circulaire, 1180 Brussels, Belgium 3 European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany 4 Department of Astronomy, California Institute of Technology, 1200 E. California Blvd, MC 249-17, Pasadena, CA 91125, USA 5 Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l’Observatoire, France 6 LESIA (UMR 8109), Observatoire de Paris, PSL, CNRS, UPMC, Univ. Paris-Diderot, 5 place Jules Janssen, 92195 Meudon, France 7 Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 8 ESA/Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, -
Blasts from the Past Historic Supernovas
BLASTS from the PAST: Historic Supernovas 185 386 393 1006 1054 1181 1572 1604 1680 RCW 86 G11.2-0.3 G347.3-0.5 SN 1006 Crab Nebula 3C58 Tycho’s SNR Kepler’s SNR Cassiopeia A Historical Observers: Chinese Historical Observers: Chinese Historical Observers: Chinese Historical Observers: Chinese, Japanese, Historical Observers: Chinese, Japanese, Historical Observers: Chinese, Japanese Historical Observers: European, Chinese, Korean Historical Observers: European, Chinese, Korean Historical Observers: European? Arabic, European Arabic, Native American? Likelihood of Identification: Possible Likelihood of Identification: Probable Likelihood of Identification: Possible Likelihood of Identification: Possible Likelihood of Identification: Definite Likelihood of Identification: Definite Likelihood of Identification: Possible Likelihood of Identification: Definite Likelihood of Identification: Definite Distance Estimate: 8,200 light years Distance Estimate: 16,000 light years Distance Estimate: 3,000 light years Distance Estimate: 10,000 light years Distance Estimate: 7,500 light years Distance Estimate: 13,000 light years Distance Estimate: 10,000 light years Distance Estimate: 7,000 light years Distance Estimate: 6,000 light years Type: Core collapse of massive star Type: Core collapse of massive star Type: Core collapse of massive star? Type: Core collapse of massive star Type: Thermonuclear explosion of white dwarf Type: Thermonuclear explosion of white dwarf? Type: Core collapse of massive star Type: Thermonuclear explosion of white dwarf Type: Core collapse of massive star NASA’s ChANdrA X-rAy ObServAtOry historic supernovas chandra x-ray observatory Every 50 years or so, a star in our Since supernovas are relatively rare events in the Milky historic supernovas that occurred in our galaxy. Eight of the trine of the incorruptibility of the stars, and set the stage for observed around 1671 AD. -
A DEEP SEARCH for PROMPT RADIO EMISSION from THERMONUCLEAR SUPERNOVAE with the VERY LARGE ARRAY Laura Chomiuk1,11, Alicia M
Draft version July 1, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 A DEEP SEARCH FOR PROMPT RADIO EMISSION FROM THERMONUCLEAR SUPERNOVAE WITH THE VERY LARGE ARRAY Laura Chomiuk1;11, Alicia M. Soderberg2, Roger A. Chevalier3, Seth Bruzewski1, Ryan J. Foley4,5, Jerod Parrent2, Jay Strader1, Carles Badenes6 Claes Fransson7 Atish Kamble2, Raffaella Margutti8, Michael P. Rupen9, & Joshua D. Simon10 Draft version July 1, 2018 ABSTRACT Searches for circumstellar material around Type Ia supernovae (SNe Ia) are one of the most powerful tests of the nature of SN Ia progenitors, and radio observations provide a particularly sensitive probe of this material. Here we report radio observations for SNe Ia and their lower-luminosity thermonu- clear cousins. We present the largest, most sensitive, and spectroscopically diverse study of prompt (∆t . 1 yr) radio observations of 85 thermonuclear SNe, including 25 obtained by our team with the unprecedented depth of the Karl G. Jansky Very Large Array. With these observations, SN 2012cg joins SN 2011fe and SN 2014J as a SN Ia with remarkably deep radio limits and excellent temporal −1 _ −9 M yr coverage (six epochs, spanning 5{216 days after explosion, yielding M=vw . 5 × 10 100 km s−1 , assuming B = 0:1 and e = 0:1). All observations yield non-detections, placing strong constraints on the presence of circumstellar material. We present analytical models for the temporal and spectral evolution of prompt radio emission from thermonuclear SNe as expected from interaction with either wind-stratified or uniform density media. These models allow us to constrain the progenitor mass loss rates, with limits ranging _ −9 −4 −1 −1 from M . -
Radio Supernovae and the Square Kilometer Array
RADIO SUPERNOVAE AND THE SQUARE KILOMETER ARRAY SCHUYLER D. VAN DYK IPAC/Caltech, MS 100-22, Pasadena, CA 91125, USA E-mail: [email protected] KURT W. WEILER & MARCOS J. MONTES Naval Research Lab, Code 7214, Washington, DC 20375-5320 USA E-mail: [email protected], [email protected] RICHARD A. SRAMEK NRAO/VLA, PO Box 0, Socorro, NM 87801 USA E-mail: [email protected] NINO PANAGIA STScI/ESA, 3700 San Martin Dr., Baltimore, MD 21218 USA E-mail: [email protected] Detailed radio observations of extragalactic supernovae are critical to obtaining valuable informa- tion about the nature and evolutionary phase of the progenitor star in the period of a few hundred to several tens-of-thousands of years before explosion. Additionally, radio observations of old super- novae (>20 years) provide important clues to the evolution of supernovae into supernova remnants, a gap of almost 300 years (SN 1680, Cas A, to SN 1923A) in our current knowledge. Finally, new empirical relations indicate that it may be possible to use some types of radio supernovae as distance yardsticks, to give an independent measure of the distance scale of the Universe. However, the study of radio supernovae is limited by the sensitivity and resolution of current radio telescope arrays. Therefore, it is necessary to have more sensitive arrays, such as the Square Kilometer Array and the several other radio telescope upgrade proposals, to advance radio supernova studies and our understanding of supernovae, their progenitors, and the connection to supernova remnants. 1 Supernovae Supernovae (SNe) play a vital role in galactic evolution through explosive nucleosynthesis and chemical enrichment, through energy input into the interstellar medium, through production of stellar remnants such as neutron stars, pulsars, and black holes, and by the production of cosmic rays. -
Supernovae in Dense and Dusty Environments
TURUN YLIOPISTON JULKAISUJA ANNALES UNIVERSITATIS TURKUENSIS SARJA - SER. A I OSA - TOM. 456 ASTRONOMICA - CHEMICA - PHYSICA - MATHEMATICA SUPERNOVAE IN DENSE AND DUSTY ENVIRONMENTS by Erkki Kankare TURUN YLIOPISTO UNIVERSITY OF TURKU Turku 2013 From Department of Physics and Astronomy University of Turku FI-20014 Turku Finland Supervised by Dr. Seppo Mattila Department of Physics and Astronomy University of Turku Finland Reviewed by Prof. Juri Poutanen Dr. Dovi Poznanski Astronomy Division School of Physics and Astronomy Department of Physics Tel Aviv University University of Oulu Israel Finland Opponent Dr. Bruno Leibundgut European Southern Observatory Germany ISBN 978-951-29-5291-5 (PRINT) ISBN 978-951-29-5292-2 (PDF) ISSN 0082-7002 Painosalama Oy - Turku, Finland 2013 Acknowledgements First of all a big thank you to my supervisor Seppo Mattila who introduced me to supernovae and relentlessly guided me through my long PhD process and never stopped listening to his student who so often walked into his office to bother him. Many thanks too to my MSc supervisor Pekka Teerikorpi who intro- duced me into making science in the first place. I would also like to thank Stuart Ryder for the very successful collaboration on the Gemini programme, and Stefano Benetti for including me in the ESO/NTT Large Programme. Similar thanks go to Rubina Kotak, Peter Lundqvist, Andrea Pastorello, Miguel Angel´ P´erez-Torres, Cristina Romero-Ca˜nizales, Jason Spyromilio, Stefano Valenti, Petri V¨ais¨anen and all the other colleagues with whom I have had the honour to work, but who are unfortunately far too many to name here.