DOCSLIB.ORG

Luminous Supernovae

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Luminous Supernovae Robert Quimby (Caltech) 1 Wednesday, November 10, 2010 Super/Over/Extremely/Very Luminous Supernovae LSNe SNe with peak absolute (optical) magnitudes brighter than -21 are Luminous Supernovae (LSNe) Richardson et al. 2002 Robert Quimby 2 Wednesday, November 10, 2010 SN 2005ap Quimby et al. 2007 R = 23.5 mag host (not shown) Peak observed mag = 18.1 (unfiltered) Observed light curve rise = 7 days Estimated rise time >20 days? Robert Quimby 3 Wednesday, November 10, 2010 SN 2005ap Spectra z = 0.2832 Peak absolute mag = -22.7 (unfiltered) Temperature 17,000-20,000 Line velocities ~20,000 km/s Velocity drops by ~4,000 km/s in 9 days Quimby et al. 2007 Robert Quimby 4 Wednesday, November 10, 2010 Redshift Distrubution of TSS Supernovae Quimby et al. 2006 Robert Quimby 5 Wednesday, November 10, 2010 The Mysterious SCP 06F6 Barbary et al. 2009 Robert Quimby 6 Wednesday, November 10, 2010 SN 2006gy Smith et al. 2008 Peak absolute magnitude nearly -22 Brighter than -21 mag for ~100 days Integrated light >1051 erg Robert Quimby 7 Wednesday, November 10, 2010 Pair-Instability SNe First Proposed it the 1960’s (Rakavy et al. 1967; Barkat et al. 1967) Massive stars are supported by radiation pressure At high temperatures, photons are created with E > e+e- Losses to pair production soften the EOS, and lead to instability Expected fate of the first (low metal, high mass) stars Waldman 2008 Robert Quimby 8 Wednesday, November 10, 2010 SN 2006gy Late-Time Light CurveNo. 6, 2010 NEW OBSERVATIONS OF THE VERY LUMINOUS SUPERNOVA 2006gy 2223 1011 >400 days. The early-time measurements (< 250 days) come from Smith et al. (2010). The optical measurement near day ) 400 comes from photometric measurements by Kawabata et al. • O 10 (2009), while the optical luminosity on day 810 comes from a 10 Total Luminosity NIR Luminosity direct integration of our HST observations (see Section 3.3.1). Optical Luminosity The three late-time NIR luminosities represent lower limits based on the measured K#-band flux (see above, Section 3.2). 9 56 1 10 The decay rate of Co, 0.98 mag (100 day)− ,ismuchfaster than the observed decay of the K# flux from SN 2006gy, 1 0.2 mag (100 day)− . The late-time NIR excess declines at ∼ 56 108 aratethatistooslowtobeexplainedby Co heating alone. The PISN model of Nomoto et al. (2007), which provided Bolometric Luminosity (L 56 good agreement with the early-time light curve of SN 2006gy 2.5 MO • Ni 107 after an artificial reduction of the total ejecta mass from their evolutionary calculation, was able to reproduce the late-time 0 200 400 600 800 Days since explosion NIR luminosity observed by Smith et al. (2008b). This model required less than 100% efficiency in the conversion of gamma- Figure 5. Evolution of the bolometric luminosity of SN 2006gy during the first Miller et al. 2010 800 days after explosion. Optical data are shown as black circles, and NIR data rays (from radioactive decay) to optical/NIR emission, which are red squares. Early-time data (< 250 days) are from Smith et al. (2010). means that the light curve should decay faster than 0.98 mag Robert Quimby 1 9 The optical detection near day 400 is from Kawabata et al. (2009). All other (100 d)− . The possibility of a PISN was first invoked to explain Wednesday, November 10, 2010 data are from this work. NIR measurements are only lower limits to the total the large peak luminosity of SN 2006gy (Ofek et al. 2007;Smith IR luminosity, because our observations do not sample redward of 2.2 µm(see et al. 2007). This scenario would have required the production the text). The dashed line shows the expected decline if the luminosity were 56 powered by 2.5 M of 56Ni. The flat nature of the light curve indicates that of ! 10 M of Ni, which in turn would produce a large ! 56 radioactivity is not! the primary energy source for the late-time emission. late-time luminosity that decays at the rate of Co. The late- (A color version of this figure is available in the online journal.) time NIR luminosity is not accounted for in either the general PISN models or the artificial model of Nomoto et al. (2007); it therefore provides a serious challenge to the PISN hypothesis.12 dust with T 600 K11 could dominate the IR emission, in which case the≈ luminosity could be significantly higher than the 3.2.2. Collisional Heating of the Dust values quoted above. The location of this dust, and whether it is newly formed Another possibility is that the dust existed prior to the or pre-existing at the time of the SN explosion, remain to SN explosion, at large distances from the explosion site, and be determined. The dust-cooling time is short, meaning that was heated via collisions with the expanding material in the aprolongedheatsourceisneededtoexplaintheextended expanding blast wave. The intense UV/optical output from an excess. We consider four possibilities for heating the dust: (1) SN at its peak vaporizes any dust in the vicinity of the SN (Dwek radioactive heating from 56Co decay, (2) collisional excitation 1983). This radiation near peak creates a dust-free cavity into of pre-existing dust, (3) heating via radiation from circumstellar which the SN ejecta may expand at early times; however, the interaction, and (4) a late-time IR dust echo, where pre-existing ejecta blast wave will eventually reach the edge of the dust-free dust is heated by the radiation produced while the SN was near cavity, at which point collisional excitations of the dust may its optical peak. generate NIR emission. The large peak luminosity of SN 2006gy, 8 1010 L (Smith 3.2.1. Radioactive Heating from 56Co et al. 2010), provides significant challenges× to this collisional! heating scenario. Dwek (1983)showsthattheradiusofthedust- Smith et al. (2008b)notedthattheobservedK#-band de- free cavity can be determined from the peak luminosity and the cay between 2007 September and 2007 December could be dust vaporization temperature, assuming the grain emissivity explained with radioactive heating from a minimum of 2.5 M Q is proportional to (λ/λ ) 1: of 56Ni, if a sufficient amount of dust formed in order to move! v 0 − the luminosity into the NIR (though they favored another inter- 0.5 Qν L0(L ) pretation; see below). We show the bolometric evolution of R1(pc) 23 ¯ ! , (2) = λ (µm)T 5 SN 2006gy through the first 800 days post-explosion, in- ! 0 v " cluding both optical and NIR∼ detections, in Figure 5.From where R is the radius of the dust-free cavity, Q is the mean Equation 19 of Nadyozhin (1994), and the fact that the lumi- 1 ¯ ν 56 56 T nosity from Co decay dominates over Ni decay at times ! 2 grain emissivity, L0 is the peak luminosity, and v is the dust weeks after explosion, we arrive at the following expression for vaporization temperature. Following Dwek (1983), if we assume 18 Qν 1andthatλ0 0.2 µm, we find that R1 1.4 10 cm, the radioactivity-powered luminosity of an SN, assuming 100% ¯ = = ≈ × trapping of gamma-rays: for a vaporization temperature Tv 1000 K. If the absorption ≈ 2 coefficient is instead proportional to λ− ,thenthecavity 43 t/(111.3d) 1 L56Co 1.45 10 exp− MNi/M erg s− , (1) becomes even larger. Based on the observed width of the Hα = × ! line from SN 2006gy, Smith et al. (2007)estimatethespeedof 1 where t is the time since SN explosion in days and MNi is the the blast wave to be 4000 km s− , which would mean that this total mass of 56Ni produced. Using Equation (1)wealsoshowin material would take 112 yr to reach the edge of the dust-free Figure 5 the expected light curve from 2.5 M of 56Ni at times cavity. Even if there∼ are ejecta traveling at more typical SN ! 11 Smith et al. (2008b) show that the combination of the peak luminosity and 12 The pulsational pair-instability model of Woosley et al. (2007) has not, distance to the dust suggests an equilibrium temperature around 600 K. however, been excluded; see also Smith et al. (2010). SN 2006gy Spectra Smith et al. 2010 Robert Quimby 10 Wednesday, November 10, 2010 SN 2007bi: The PISN Case Gal-Yam et al. 2009 Optical light curve decay rate consistent with the production 56 of ~7 M of Ni Iron abundance in nebular spectra also consistent with the 56 decay of ~4-7 M of Ni Robert Quimby 11 Wednesday, November 10, 2010 SN 2008es Gezari et al. 2009; see also Miller et al. 2009 Robert Quimby 12 Wednesday, November 10, 2010 2009: PTF Finds LSNe PTF09cwl PTF09cnd PTF09atu Before After Robert Quimby 13 Wednesday, November 10, 2010 LSNe (Candidates) from PTF Name Notes LSN-Ic LSN-IIn PTF09uy LSN-IIn Bright BL-Ic PTF09atu LSN-Ic PTF09cnd LSN-Ic PTF09cwl LSN-Ic PTF10bfz BL-Ic PTF10bjp LSN-Ic 10% PTF10cwr LSN-Ic PTF10fel LSN-IIn PTF10heh LSN-IIn PTF10hgi LSN-Ic PTF10jwd LSN-IIn 50% PTF10nmn LSN-Ic 40% PTF10ooe BL-Ic PTF10qaf LSN-IIn PTF10qwu LSN-IIn PTF10scc LSN-IIn PTF10tpz LSN-IIn? PTF10uhf LSN-Ic PTF10xee LSN-Ic? PTF10vqv LSN-Ic Observed numbers--not volumetric rates! Robert Quimby 14 Wednesday, November 10, 2010 LSN-Ic Spectra Quimby et al. 2010 Robert Quimby 15 Wednesday, November 10, 2010 PTF09cnd: Spectal Comparison (near r- band maximum) Robert Quimby 16 Wednesday, November 10, 2010 LSN-Ic Light Curves Quimby et al. 2010 Absolute V-band Magnitude V-band Absolute Robert Quimby 17 Wednesday, November 10, 2010 PTF09cnd: Late-Time Photometry Robert Quimby 18 Wednesday, November 10, 2010 PTF09cnd: Late-Time Spectra Robert Quimby 19 Wednesday, November 10, 2010 Summary of the Observations There are observationally distinct (but perhaps still physically related) groups of LSNe Rise times are typically ~50 days, but not always well constrained and not always the same LSN-Ic lack metal lines through maximum light (temperature or composition effect?) LSN-Ic photospheres persist for ~6 months past maximum light Some LSN-Ic show slow photometric declines, consistent with a large production of 56Ni, others must produce far less Robert Quimby 20 Wednesday, November 10, 2010 Power Sources 1 Radioactive Decay Energy released by the radioactive decay of elements synthesized in the explosion (e.g.
Recommended publications
  • Copyright by Robert Michael Quimby 2006 the Dissertation Committee for Robert Michael Quimby Certifies That This Is the Approved Version of the Following Dissertation

    Copyright by Robert Michael Quimby 2006 the Dissertation Committee for Robert Michael Quimby Certifies That This Is the Approved Version of the Following Dissertation

    Copyright by Robert Michael Quimby 2006 The Dissertation Committee for Robert Michael Quimby certifies that this is the approved version of the following dissertation: The Texas Supernova Search Committee: J. Craig Wheeler, Supervisor Peter H¨oflich Carl Akerlof Gary Hill Pawan Kumar Edward L. Robinson The Texas Supernova Search by Robert Michael Quimby, A.B., M.A. DISSERTATION Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT AUSTIN December 2006 Acknowledgments I would like to thank J. Craig Wheeler, Pawan Kumar, Gary Hill, Peter H¨oflich, Rob Robinson and Christopher Gerardy for their support and advice that led to the realization of this project and greatly improved its quality. Carl Akerlof, Don Smith, and Eli Rykoff labored to install and maintain the ROTSE-IIIb telescope with help from David Doss, making this project possi- ble. Finally, I thank Greg Aldering, Saul Perlmutter, Robert Knop, Michael Wood-Vasey, and the Supernova Cosmology Project for lending me their image subtraction code and assisting me with its installation. iv The Texas Supernova Search Publication No. Robert Michael Quimby, Ph.D. The University of Texas at Austin, 2006 Supervisor: J. Craig Wheeler Supernovae (SNe) are popular tools to explore the cosmological expan- sion of the Universe owing to their bright peak magnitudes and reasonably high rates; however, even the relatively homogeneous Type Ia supernovae are not intrinsically perfect standard candles. Their absolute peak brightness must be established by corrections that have been largely empirical.
  • Arxiv:0709.0302V1 [Astro-Ph] 3 Sep 2007 N Ro,M,414 USA 48104, MI, Arbor, Ann USA As(..Mcayne L 01.Sc Aeilcudslow Could Material Such Some 2001)

    Arxiv:0709.0302V1 [Astro-Ph] 3 Sep 2007 N Ro,M,414 USA 48104, MI, Arbor, Ann USA As(..Mcayne L 01.Sc Aeilcudslow Could Material Such Some 2001)

    DRAFT VERSION NOVEMBER 4, 2018 Preprint typeset using LATEX style emulateapj v. 03/07/07 SN 2005AP: A MOST BRILLIANT EXPLOSION ROBERT M. QUIMBY1,GREG ALDERING2,J.CRAIG WHEELER1,PETER HÖFLICH3,CARL W. AKERLOF4,ELI S. RYKOFF4 Draft version November 4, 2018 ABSTRACT We present unfiltered photometric observations with ROTSE-III and optical spectroscopic follow-up with the HET and Keck of the most luminous supernova yet identified, SN 2005ap. The spectra taken about 3 days before and 6 days after maximum light show narrow emission lines (likely originating in the dwarf host) and absorption lines at a redshift of z =0.2832, which puts the peak unfiltered magnitude at −22.7 ± 0.1 absolute. Broad P-Cygni features corresponding to Hα, C III,N III, and O III, are further detected with a photospheric velocity of ∼ 20,000kms−1. Unlike other highly luminous supernovae such as 2006gy and 2006tf that show slow photometric evolution, the light curve of SN 2005ap indicates a 1-3 week rise to peak followed by a relatively rapid decay. The spectra also lack the distinct emission peaks from moderately broadened (FWHM ∼ 2,000kms−1) Balmer lines seen in SN 2006gyand SN 2006tf. We briefly discuss the origin of the extraordinary luminosity from a strong interaction as may be expected from a pair instability eruption or a GRB-like engine encased in a H/He envelope. Subject headings: Supernovae, SN 2005ap 1. INTRODUCTION the ultra-relativistic flow and thus mask the gamma-ray bea- Luminous supernovae (SNe) are most commonly associ- con announcing their creation, unlike their stripped progeni- ated with the Type Ia class, which are thought to involve tor cousins.
  • Radioactive Decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10, 4.1, 4.2, 4.3, 4.4, 5.2, 5.4 (Binary Stars and Accretion Disks)

    Radioactive Decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10, 4.1, 4.2, 4.3, 4.4, 5.2, 5.4 (Binary Stars and Accretion Disks)

    Friday, March 10, 2017 Reading for Exam 3: Chapter 6, end of Section 6 (binary evolution), Section 6.7 (radioactive decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10, 4.1, 4.2, 4.3, 4.4, 5.2, 5.4 (binary stars and accretion disks). Plus superluminous supernovae, not in the book. Astronomy in the news? Potatoes can grow just about anywhere, including Mars, according to researchers who tested the idea put forth in the movie "The Martian." Scientists are growing potatoes in Mars-like soil from a Peruvian desert inside a CubeSat under extreme conditions, and the findings could not only benefit future Mars colonists but also help undernourished populations here on Earth. Goal: To understand the nature and importance of SN 1987A for our understanding of massive star evolution and iron core collapse. Chapter 7 Image of SN 1987A and environs in Large Magellanic Cloud, taken by Hubble Space Telescope, January 2017 One Minute Exam What was the most important thing about SN 1987A in terms of the basic physics of core collapse? It exploded in a blue, not a red supergiant It was surrounded by three rings It produced radioactive nickel and cobalt Neutrinos were detected from it Saw neutrinos! Neutron star must have formed and survived for at least 10 seconds. If a black hole had formed in the first instants, neither light nor neutrinos could have been emitted. No sign of neutron star since, despite looking hard for 30 years. Whatever is in the center of Cas A, most likely a neutron star, is too dim to be seen at the distance of the LMC, so SN 1987A might have made one of those (probably a neutron star, but not bright like the one in the Crab Nebula).
  • HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land

    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land

    HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land 1 Executive Summary • There are now 420 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 27 November, nineteen published papers in 2020 • HET papers have 29363 citations – Average of 70, median of 39 citations per paper – H-number of 90 – 81 papers have ≥ 100 citations; 175 have ≥ 50 cites • Wide angle surveys account for 26% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 47% of the papers and 47% of the citations, respectively. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 420 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2020 a total of fifteen HET papers appeared; nineteen have been published to date in 2020. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time.
  • 10/12/07 Reading - Chapter 6, 7 Test 2, Friday, October 19, Review Sheet Next Week, Review Session Thursday, 5 PM Room RLM 4.102

    10/12/07 Reading - Chapter 6, 7 Test 2, Friday, October 19, Review Sheet Next Week, Review Session Thursday, 5 PM Room RLM 4.102

    10/12/07 Reading - Chapter 6, 7 Test 2, Friday, October 19, Review sheet next week, review session Thursday, 5 PM room RLM 4.102 Astronomy in the news? First Woman Commander of the International Space Station Allen Telescope Array, first 42 of planned 350 radio telescopes activated, search for exterrestrial life, astrophysics Pic of the Day: The Whale Galaxy Press Coverage of new bright supernova, SN 2005ap Space.com http://www.space.com/scienceastronomy/071011-brightest- supernova.html MSNBC http://www.msnbc.msn.com/id/21259692/ Sky Watch Can only count each objects once for credit, but can do any objects missed earlier in later reports. Add relevant objects that I don’t specifically mention in class, other examples of planetary nebulae, main sequence stars, red giants, binary stars, supernovae…. Don’t wait until the last minute. It might be cloudy. The Earth orbits around the Sun, some objects that were visible at night become in the direction of the Sun, “up” in daylight, impossible to see, other objects that were inaccessible become visible at night. Check it out. Sky Watch Objects mentioned so far Lyra - Ring Nebula, planetary nebula in Lyra Sirius - massive blue main sequence star with white dwarf companion Algol - binary system in Perseus Vega - massive blue main sequence star in Lyra Antares - red giant in Scorpius Betelgeuse - Orion, Red Supergiant due to explode “soon” 15 solar masses Rigel - Orion, Blue Supergiant due to explode later, 17 solar masses Aldebaran - Bright Red Supergiant in Taurus, 2.5 solar masses (WD not SN) CP Pup, classical nova toward constellation Puppis in 1942 Pup 91, classical nova toward Puppis in 1991 QU Vul, classical nova toward constellation Vulpecula, GK Per toward constellation Perseus, has had both a classical nova eruption 1901 and dwarf nova eruptions.
  • Astronomy Magazine 2012 Index Subject Index

    Astronomy Magazine 2012 Index Subject Index

    Astronomy Magazine 2012 Index Subject Index A AAR (Adirondack Astronomy Retreat), 2:60 AAS (American Astronomical Society), 5:17 Abell 21 (Medusa Nebula; Sharpless 2-274; PK 205+14), 10:62 Abell 33 (planetary nebula), 10:23 Abell 61 (planetary nebula), 8:72 Abell 81 (IC 1454) (planetary nebula), 12:54 Abell 222 (galaxy cluster), 11:18 Abell 223 (galaxy cluster), 11:18 Abell 520 (galaxy cluster), 10:52 ACT-CL J0102-4915 (El Gordo) (galaxy cluster), 10:33 Adirondack Astronomy Retreat (AAR), 2:60 AF (Astronomy Foundation), 1:14 AKARI infrared observatory, 3:17 The Albuquerque Astronomical Society (TAAS), 6:21 Algol (Beta Persei) (variable star), 11:14 ALMA (Atacama Large Millimeter/submillimeter Array), 2:13, 5:22 Alpha Aquilae (Altair) (star), 8:58–59 Alpha Centauri (star system), possibility of manned travel to, 7:22–27 Alpha Cygni (Deneb) (star), 8:58–59 Alpha Lyrae (Vega) (star), 8:58–59 Alpha Virginis (Spica) (star), 12:71 Altair (Alpha Aquilae) (star), 8:58–59 amateur astronomy clubs, 1:14 websites to create observing charts, 3:61–63 American Astronomical Society (AAS), 5:17 Andromeda Galaxy (M31) aging Sun-like stars in, 5:22 black hole in, 6:17 close pass by Triangulum Galaxy, 10:15 collision with Milky Way, 5:47 dwarf galaxies orbiting, 3:20 Antennae (NGC 4038 and NGC 4039) (colliding galaxies), 10:46 antihydrogen, 7:18 antimatter, energy produced when matter collides with, 3:51 Apollo missions, images taken of landing sites, 1:19 Aristarchus Crater (feature on Moon), 10:60–61 Armstrong, Neil, 12:18 arsenic, found in old star, 9:15
  • Light Curve Powering Mechanisms of Superluminous Supernovae

    Light Curve Powering Mechanisms of Superluminous Supernovae

    Light Curve Powering Mechanisms of Superluminous Supernovae A dissertation presented to the faculty of the College of Arts and Science of Ohio University In partial fulfillment of the requirements for the degree Doctor of Philosophy Kornpob Bhirombhakdi May 2019 © 2019 Kornpob Bhirombhakdi. All Rights Reserved. 2 This dissertation titled Light Curve Powering Mechanisms of Superluminous Supernovae by KORNPOB BHIROMBHAKDI has been approved for the Department of Physics and Astronomy and the College of Arts and Science by Ryan Chornock Assistant Professor of Physics and Astronomy Joseph Shields Interim Dean, College of Arts and Science 3 Abstract BHIROMBHAKDI, KORNPOB, Ph.D., May 2019, Physics Light Curve Powering Mechanisms of Superluminous Supernovae (111 pp.) Director of Dissertation: Ryan Chornock The power sources of some superluminous supernovae (SLSNe), which are at peak 10{ 100 times brighter than typical SNe, are still unknown. While some hydrogen-rich SLSNe that show narrow Hα emission (SLSNe-IIn) might be explained by strong circumstellar interaction (CSI) similar to typical SNe IIn, there are some hydrogen-rich events without the narrow Hα features (SLSNe-II) and hydrogen-poor ones (SLSNe-I) that strong CSI has difficulties to explain. In this dissertation, I investigate the power sources of these two SLSN classes. SN 2015bn (SLSN-I) and SN 2008es (SLSN-II) are the targets in this study. I perform late-time multi-wavelength observations on these objects to determine their power sources. Evidence supports that SN 2008es was powered by strong CSI, while the late-time X-ray non-detection we observed neither supports nor denies magnetar spindown as the most preferred power origin of SN 2015bn.
  • DISCOVERY of the ULTRA-BRIGHT TYPE II-L SUPERNOVA 2008Es

    DISCOVERY of the ULTRA-BRIGHT TYPE II-L SUPERNOVA 2008Es

    The Astrophysical Journal, 690:1313–1321, 2009 January 10 doi:10.1088/0004-637X/690/2/1313 c 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DISCOVERY OF THE ULTRA-BRIGHT TYPE II-L SUPERNOVA 2008es S. Gezari1, J. P. Halpern2,D.Grupe3,F.Yuan4, R. Quimby5, T. McKay4, D. Chamarro4,M.D.Sisson4, C. Akerlof4, J. C. Wheeler6,P.J.Brown3,S.B.Cenko7,A.Rau5, J. O. Djordjevic8, and D. M. Terndrup8 1 Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA; [email protected] 2 Department of Astronomy, Columbia University, New York, NY 10027, USA 3 Pennsylvania State University, Department of Astronomy & Astrophysics, University Park, PA 16802, USA 4 University of Michigan, Randall Laboratory of Physics, 450 Church St., Ann Arbor, MI, 48109-1040, USA 5 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 6 Department of Astronomy, University of Texas, Austin, TX 78712, USA 7 Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA 8 Department of Astronomy, Ohio State University, Columbus, OH 43210, USA Received 2008 August 20; accepted 2008 September 4; published 2008 December 12 ABSTRACT We report the discovery by the Robotic Optical Transient Search Experiment (ROTSE-IIIb) telescope of SN 2008es, an overluminous supernova (SN) at z = 0.205 with a peak visual magnitude of −22.2. We present multiwavelength follow-up observations with the Swift satellite and several ground-based optical telescopes. The ROTSE-IIIb observations constrain the time of explosion to be 23 ± 1 rest-frame days before maximum.
  • Meteor ISSN 0866 - 2851 Csillagászati Évkönyv Ár: 3000 Ft 9 7 7 0 8 6 6 2 8 5 0 0 2

    Meteor ISSN 0866 - 2851 Csillagászati Évkönyv Ár: 3000 Ft 9 7 7 0 8 6 6 2 8 5 0 0 2

    3 01 2 2013 csillagászati évkönyv r o e t e m meteor ISSN 0866 - 2851 csillagászati évkönyv Ár: 3000 Ft 9 7 7 0 8 6 6 2 8 5 0 0 2 METEOR CSILLAGÁSZATI ÉVKÖNYV 2013 METEOR CSILLAGÁSZATI ÉVKÖNYV 2013 MCSE – 2012. NOVEMBER METEOR CSILLAGÁSZATI ÉVKÖNYV 2013 MCSE – 2012. NOVEMBER meteor csillagászati évkönyv 2013 Szerkesztette: Benkõ József Mizser Attila Magyar Csillagászati Egyesület www.mcse.hu Budapest, 2012 METEOR CSILLAGÁSZATI ÉVKÖNYV 2013 MCSE – 2012. NOVEMBER Az évkönyv kalendárium részének összeállításában közremûködött: Csák Balázs Görgei Zoltán Kaposvári Zoltán Kernya János Gábor Kiss Áron Keve Kovács József Landy-Gyebnár Mónika Molnár Péter Sárneczky Krisztián Sánta Gábor Szabó M. Gyula Szabó Sándor Szöllôsi Attila A kalendárium csillagtérképei az Ursa Minor szoftverrel készültek. www.ursaminor.hu Szakmailag ellenôrizte: Szabados László A kiadvány támogatói: Közigazgatási és Igazságügyi Minisztérium „Csillagászat a fejlôdésért és a tehetségekért” Mindazok, akik az SZJA 1%-ával támogatják a Magyar Csillagászati Egyesületet. Adószámunk: 19009162-2-43 Felelôs kiadó: Mizser Attila Nyomdai elôkészítés: Kármán Stúdió, www.karman.hu Nyomtatás, kötészet: OOK-Press Kft., www.ookpress.hu Felelôs vezetô: Szathmáry Attila Terjedelem: 18,75 ív fekete-fehér + 12 oldal színes melléklet 2012. november ISSN 0866-2851 METEOR CSILLAGÁSZATI ÉVKÖNYV 2013 MCSE – 2012. NOVEMBER Tartalom Bevezetô ................................................... 7 Kalendárium ............................................... 11 Cikkek Kálmán Béla: A napkutatás új eredményeibôl
  • HET Publication Report HET Board Meeting 4/5 June 2020 Zoom Land

    HET Publication Report HET Board Meeting 4/5 June 2020 Zoom Land

    HET Publication Report HET Board Meeting 4/5 June 2020 Zoom Land 1 Executive Summary • There are now 410 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 22 May, nine published papers in 2020 • HET papers have 28229 citations – Average of 69, median of 38 citations per paper – H-number of 90 – 76 papers have ≥ 100 citations; 170 have ≥ 50 cites • Wide angle surveys account for 27% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 46% of the papers and 47% of the citations. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 410 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2019 a total of fifteen HET papers appeared; nine have been published to date in 2019. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time.
  • Ultra-Bright Optical Transients Are Linked with Type Ic Supernovae

    Ultra-Bright Optical Transients Are Linked with Type Ic Supernovae

    Ultra-bright Optical Transients are Linked with Type Ic Supernovae Pastorello, A., Smartt, S. J., Botticella, M. T., Maguire, K., Fraser, M., Smith, K., Kotak, R., Magill, L., Valenti, S., Young, D. R., Gezari, S., Bresolin, F., Kudritzki, R., Howell, D. A., Rest, A., Metcalfe, N., Mattila, S., Kankare, E., Huang, K. Y., ... Wynn-Williams, C. G. (2010). Ultra-bright Optical Transients are Linked with Type Ic Supernovae. The Astrophysical Journal Letters, 724(1), L16- L21. https://doi.org/10.1088/2041-8205/724/1/L16 Published in: The Astrophysical Journal Letters Document Version: Publisher's PDF, also known as Version of record Queen's University Belfast - Research Portal: Link to publication record in Queen's University Belfast Research Portal Publisher rights Copyright 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. General rights Copyright for the publications made accessible via the Queen's University Belfast Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy The Research Portal is Queen's institutional repository that provides access to Queen's research output. Every effort has been made to ensure that content in the Research Portal does not infringe any person's rights, or applicable UK laws. If you discover content in the Research Portal that you believe breaches copyright or violates any law, please contact [email protected]. Download date:06. Oct. 2021 The Astrophysical Journal Letters, 724:L16–L21, 2010 November 20 doi:10.1088/2041-8205/724/1/L16 C 2010.
  • LJMU Research Online

    LJMU Research Online

    LJMU Research Online Miller, AA, Chornock, R, Perley, DA, Ganeshalingam, M, Li, W, Butler, NR, Bloom, JS, Smith, N, Modjaz, M, Poznanski, D, Filippenko, AV, Griffith, CV, Shiode, JH and Silverman, JM The exceptionally luminous type II-linear supernova 2008es http://researchonline.ljmu.ac.uk/id/eprint/6497/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Miller, AA, Chornock, R, Perley, DA, Ganeshalingam, M, Li, W, Butler, NR, Bloom, JS, Smith, N, Modjaz, M, Poznanski, D, Filippenko, AV, Griffith, CV, Shiode, JH and Silverman, JM (2009) The exceptionally luminous type II- linear supernova 2008es. The Astrophysical Journal, 690 (2). pp. 1303-1312. LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ The Astrophysical Journal, 690:1303–1312, 2009 January 10 doi:10.1088/0004-637X/690/2/1303 c 2009.