Looking for the High-Mass Progenitors of Stripped-Envelope Supernovae
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Correction: Corrigendum: the Superluminous Transient ASASSN
LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,7, I. Arcavi8,9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,16, A. De Cia17, D. A. Howell8,18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,23,28, C. V. McCully8,18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,25, S. Schulze24,25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event. -
Rare Superluminous Supernova Shining with Borrowed Energy Source Spotted with the 3.6M DOT Facility an Extremely Bright, Hydrog
Rare superluminous supernova shining with borrowed energy source spotted with the 3.6m DOT facility An extremely bright, hydrogen deficient, fast-evolving supernovae that shines with the energy borrowed from an exotic type of neutron star with an ultra-powerful magnetic field has been spotted by Indian researchers. Deep study of such ancient spatial objects can help probe the mysteries of the early universe. Such type of supernovae called SuperLuminous Supernova (SLSNe) is very rare. This is because they are generally originated from very massive stars (minimum mass limit is more than 25 times to that of the Sun), and the number distribution of such massive stars in our galaxy or in nearby galaxies is sparse. Among them, SLSNe-I has been counted to about 150 entities spectroscopically confirmed so far. These ancient objects are among the least understood SNe because their underlying sources are unclear, and their extremely high peak luminosity is unexplained using the conventional SN power-source model involving Ni56 - Co56 - Fe56 decay. SN 2020ank, which was first discovered by the Zwicky Transient Facility on 2020 January 19, was studied by scientists from Aryabhatta Research Institute of Observational Sciences (ARIES) Nainital, an autonomous research institute under the Department of Science and Technology (DST) Govt. of India from February 2020 and then through the lockdown phase of March and April. The apparent look of the SN was very similar to other objects in the field. However, once the brightness was estimated, it turned out as a very blue object reflecting its brighter character. The team observed it using special arrangements at India’s recently commissioned Devasthal Optical Telescope (DOT-3.6m) along with two other Indian telescopes: Sampurnanand Telescope-1.04m and Himalayan Chandra Telescope-2.0m. -
Blue Stragglers in Open Clusters?
A&A 366, 490–497 (2001) Astronomy DOI: 10.1051/0004-6361:20000213 & c ESO 2001 Astrophysics Blue stragglers in open clusters? III. NGC 7789 D. Sch¨onberner1, S. M. Andrievsky1,2,3, and J. S. Drilling4 1 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany e-mail: [email protected] 2 Department of Astronomy, Odessa State University, Shevchenko Park, 65014, Odessa, Ukraine 3 Isaac Newton Institute of Chile, Odessa Branch, Chile e-mail: [email protected] 4 Louisiana State University, Department of Physics and Astronomy, Baton Rouge, Louisiana 70803, USA e-mail: [email protected] Received 8 September 2000 / Accepted 7 November 2000 Abstract. We performed for the first time a detailed LTE spectroscopic study of a sample of blue straggler stars in the moderately old open cluster NGC 7789. For eight stars the parameters and abundances of several elements were determined. The cluster members show a remarkable surface magnesium deficiency which is quite unusual for late B - early A stars. Iron and titanium abundances are in agreement with other photometric and spectroscopic estimates of the NGC 7789 metallicity. All the confirmed blue stragglers have rather low projected rotational velocities (with one exception for K88, v sin i =80kms−1). Key words. stars: open clusters and associations: individual: NGC 7789 – stars: blue stragglers – stars: abundances 1. Introduction internal mixing processes, but that they rather evolve like normal stars. The moderately old open cluster NGC 7789 is among those In recent years interest in the NGC 7789 blue strag- having very rich blue-straggler populations. -
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. -
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. -
Fundamental Properties of Core-Collapse Supernova and GRB Progenitors: Predicting the Look of Massive Stars Before Death
A&A 558, A131 (2013) Astronomy DOI: 10.1051/0004-6361/201321906 & c ESO 2013 Astrophysics Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death Jose H. Groh1, Georges Meynet1, Cyril Georgy2, and Sylvia Ekström1 1 Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics group, EPSAM, Keele University, Lennard-Jones Labs, ST5 5BG Keele, UK Received 16 May 2013 / Accepted 20 August 2013 ABSTRACT We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini = 9−20 M, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the + following types of SN progenitors: WO1–3 (Mini ≥ 32 M), WN10–11 (25 < Mini < 32 M), LBV (20 ≤ Mini ≤ 25 M), G1 Ia (18 < Mini < 20 M), and RSGs (9 ≤ Mini ≤ 18 M). For non-rotating models, we found spectral types WO1–3 (Mini > 40 M), WN7–8 (25 < Mini ≤ 40 M), WN11h/LBV (20 < Mini ≤ 25 M), and RSGs (9 ≤ Mini ≤ 20 M). -
BD+43° 3654 – a Blue Straggler?
A&A 485, L29–L32 (2008) Astronomy DOI: 10.1051/0004-6361:200809860 & c ESO 2008 Astrophysics Letter to the Editor BD+43◦ 3654 – a blue straggler? V. V. Gvaramadze1,2 and D. J. Bomans1 1 Astronomical Institute, Ruhr-University Bochum, Universitätstr. 150, 44780 Bochum, Germany e-mail: [email protected] 2 Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia e-mail: [email protected] Received 27 March 2008 / Accepted 22 May 2008 ABSTRACT The astrometric data on the runaway star BD+43◦ 3654 are consistent with the origin of this O4If star in the center of the Cyg OB2 association, while BD+43◦ 3654 is younger than the association. To reconcile this discrepancy, we suggest that BD+43◦ 3654 is a blue straggler formed via a close encounter between two tight massive binaries in the core of Cyg OB2. A possible implication of this suggestion is that the very massive (and therefore apparently very young) stars in Cyg OB2 could be blue stragglers as well. We also suggest that the binary-binary encounter producing BD+43◦ 3654 might be responsible for ejection of two high-velocity stars (the stripped helium cores of massive stars) – the progenitors of the pulsars B2020+28 and B2021+51. Key words. stars: kinematics – pulsars: individual: PSR B2020+28 – open clusters and associations: individual: Cyg OB2 – stars: individual: BD+43◦ 3654 1. Introduction Interestingly, Cyg OB2 may be associated with the origin of + + ◦ ◦ two high-velocity pulsars, PSR B2020 28 and PSR B2021 51. BD+43 3654 is a massive (O4If) runaway star located ∼2.7 The high-precision proper motion and parallax measurements northeast of the Cyg OB2 association (Comerón & Pasquali ∼ ◦ ◦ for these pulsars (presently separated by 23 ) lead to the sug- 2007). -
ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure. -
Progenitors of Gamma-Ray Bursts and Supernovae
Progenitors of Gamma-Ray Bursts and Supernovae Chris Fryer (LANL) Types of supernova and GRBs Engines and their progenitor requirements Massive star progenitors and the circumstellar medium (single vs. binary) Specific examples – What have we learned? Supernova Types • Supernovae are distinguished by spectra and light curves. • Unfortunately, in core- collapse, the dividing lines are more like guidelines. • There are many “stand- outs” among these supernovae (e.g. SN87A). SN types - Rates • Core-collapse (Ib/c, II) SNe make up 75% of all supernovae. • Most Ib/c are Ic supernovae. • Plateau SNe make up most of the type II class. • New classes include Broad Line (tied to GRBs?) and Superluminous Supernova GRB Types • GRBs have been roughly Levan et al. (2013) divided into short/hard and long/ soft bursts. • A new class of ultra-long bursts have been discovered. Core-collapse Supernovae (Type II, Ib/c): Powered by SN Engines the potential energy released in collapse Source of convection (advective acoustic vs. Rayleigh Taylor), energy transport (neutrinos, pressure waves), role of magnetic fields. Massive Star Progenitors (binaries vs. single stars) Thermonuclear Supernovae Ignition site/sites White dwarf (double Degenerate vs. single degenerate) Possible Fates under the Convective Paradigm • Explosion within first ~200 ms, normal supernovae • Explosion delayed, weak supernova, considerable fallback (BH formation – Collapsar type II for rotating systems) • No explosion (BH Formation – Collapsar type I for rotating systems) Supernovae/Hypernovae Nomoto et al. (2003) EK (Jets!) Failed SN? 13M~15M BHAD GRB and Magnetar Engines Massive star Collapse (LGRB, very long GRB), only a very small fraction of massive stars (0.01-0.1% the supernova rate). -
The Possible Detection of a Binary Companion to a Type Ibn Supernova Progenitor J
The Astrophysical Journal, 833:128 (6pp), 2016 December 20 doi:10.3847/1538-4357/833/2/128 © 2016. The American Astronomical Society. All rights reserved. THE POSSIBLE DETECTION OF A BINARY COMPANION TO A TYPE IBN SUPERNOVA PROGENITOR J. R. Maund1,7, A. Pastorello2, S. Mattila3,4, K. Itagaki5, and T. Boles6 1 Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK 2 INAF—Osservatorio Astronomico di Padova. Vicolo Osservatorio 5, I-35122, Padova, Italy 3 Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 4 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 5 Itagaki Astronomical Observatory, Teppo-cho, 990-2492 Yamagata, Japan 6 Coddenham Astronomical Observatory, Suffolk IP6 9QY, UK Received 2016 April 28; revised 2016 August 23; accepted 2016 September 20; published 2016 December 13 ABSTRACT We present late-time observations of the site of the Type Ibn supernova (SN) 2006jc, acquired with the Hubble Space Telescope Advanced Camera for Surveys. A faint blue source is recovered at the SN position, with brightness mFW435 =26.76 0.20, mFW555 =26.60 0.23 and mFW625 =26.32 0.19 mag, although there is no detection in a contemporaneous narrow-band Ha image. The spectral energy distribution of the late-time source is well-fit by a stellar-like spectrum (logTeff > 3.7 and log LL > 4), subject to only a small degree of reddening —consistent with that estimated for SN2006jc itself at early-times. The lack of further outbursts after the explosion of SN2006jc suggests that the precursor outburst originated from the progenitor. -
OGLE-2014-SN-131: a Long-Rising Type Ibn Supernova from a Massive Progenitor E
Astronomy & Astrophysics manuscript no. output c ESO 2017 March 8, 2017 OGLE-2014-SN-131: A long-rising Type Ibn supernova from a massive progenitor E. Karamehmetoglu1, F. Taddia1, J. Sollerman1, Ł. Wyrzykowski2, S. Schmidl3, M. Fraser4, C. Fremling1, J. Greiner5; 6, C. Inserra7, Z. Kostrzewa-Rutkowska2; 8; 9, K. Maguire7, S. Smartt7, M. Sullivan10, and D. R. Young7 1 Department of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, Sweden. e-mail: [email protected] 2 Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland. 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany. 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. 5 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany. 6 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany. 7 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK. 8 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands. 9 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands. 10 Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK. Received date / Accepted date ABSTRACT Context. Type Ibn supernovae (SNe Ibn) are thought to be the core-collapse explosions of massive stars whose ejecta interact with He-rich circumstellar material (CSM). Aims. We report the discovery of a SN Ibn, with the longest rise-time ever observed, OGLE-2014-SN-131. We discuss the potential powering mechanisms and the progenitor nature of this peculiar stripped-envelope (SE), circumstellar-interacting SN. -
Download a PDF of the Abstracts Booklet
TALKS SN2016 ABSTRACTS BOOKLET 2 1.- SESSION: Cultural NAME: Cristian Moreno Pakarati AFFILIATION: Ahirenga Research TITTLE: A new proposal for a division of Easter Island's history ABSTRACT: This paper presents an original interpretation of the long-term history of the island, dividing it in three main periods. By this, it pretends to contribute a new vision on a topic long abandoned by the growingly specialized archaeology that focuses more and more on the smallest of details. The scheme is as follows: a first period, as an era of open ocean navigation and relatively frequent contact with other Polynesian people; a second period, as an era of extreme isolation where the Rapanui culture developed many of its unique traits within the Polynesian and World context; and a third period, of contacts with "the West", starting in 1722 with the Dutch expedition of Roggeveen. By this, it pretends to simplify the timeline of events on the island and contextualize better the statue-carving era and the Bird-cult of Easter Island. 2.- SESSION: 01 NAME: Edmundo Edwards AFFILIATION: Pacific Islands Research Institute TITTLE: Archeoastronomy of Eastern Polynesia and Easter Island ABSTRACT: Some 3,500 years ago in a span of about 500 years, the Lapita, the ancestors of the Polynesians, used their knowledge of the stars to settle an area 4,300 km wide in what is considered one of the speediest human expansions of the pre-historic world. Their descendants, the Polynesians, eventually settled hundreds of islands crossing millions of square kilometres of water without navigational instruments, guided by nothing more than complex astronomical observations and an understanding of natural signs.