XRF 080109/SN 2008D and SN 2007Uy in NGC 2770
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SUPPLEMENTARY INFORMATION Soderberg Et Al., Nature Manuscript 2008-02-01442
doi: 10.1038/nature06997 SUPPLEMENTARY INFORMA1TION SUPPLEMENTARY INFORMATION Soderberg et al., Nature Manuscript 2008-02-01442 1 Spectral analysis of Swift/XRT data We use the xspec v11.3.2 X-ray spectral fitting package to fit both a power law and a blackbody model to the XRT outburst data. In both models we allow for excess neutral hydrogen absorption (NH ) above the Galactic value along the line of sight to NGC 2770, 20 −2 2 NH,Gal = 1.7 × 10 cm . The best-fit power law model (χ = 7.5 for 17 degrees of −1.3±0.3 freedom; probability, P = 0.98) has a photon index, Γ = 2.3 ± 0.3 (or, Fν ∝ ν ) and +1.8 × 21 −2 ± NH = 6.9−1.5 10 cm . The best-fit blackbody model is described by kT = 0.71 0.08 +1.0 × 21 −2 keV and NH = 1.3−0.9 10 cm . However, this model provides a much poorer fit to the data (χ2 = 26.0 for 17 degrees of freedom; probability, P = 0.074). We therefore adopt the power law model as the best description of the data. The resulting count rate to flux conversion is 1 counts s−1 = 5 × 10−11 erg cm−2 s−1. The outburst undergoes a significant hard-to-soft spectral evolution as indicated by the ratio of counts in the 0.3 − 2 keV band and 2−10 keV band. The hardness ratio decreases from 1.35±0.15 during the peak of the flare to 0.25 ± 0.10 about 400 s later. -
A Holistic View of the GRB-SN Connection Alicia M Soderberg
A Holistic View of the GRB-SN Connection Alicia M Soderberg Harvard University (Credit: M. Bietenholz) Monday, April 19, 2010 12 Years since GRB 980425 d=38 Mpc Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 12 Years since GRB 980425 d=38 Mpc Happy Birthday Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN Connection L ~ 1053 erg/s L ~ 1042 erg/s Emission Process =? Ni-56 decay Δt ~ seconds Δt ~ 1 month Hard X-ray Optical (Credit: P. Challis) Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003dh at z=0.169 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 SN 2006aj at z=0.03 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 Most GRBs accompanied by Broad-lined SNe Ic SN 2006aj at z=0.03 Alicia M. -
Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications
Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC. -
Issue 36, June 2008
June2008 June2008 In This Issue: 7 Supernova Birth Seen in Real Time Alicia Soderberg & Edo Berger 23 Arp299 With LGS AO Damien Gratadour & Jean-René Roy 46 Aspen Instrument Update Joseph Jensen On the Cover: NGC 2770, home to Supernova 2008D (see story starting on page 7 Engaging Our Host of this issue, and image 52 above showing location Communities of supernova). Image Stephen J. O’Meara, Janice Harvey, was obtained with the Gemini Multi-Object & Maria Antonieta García Spectrograph (GMOS) on Gemini North. 2 Gemini Observatory www.gemini.edu GeminiFocus Director’s Message 4 Doug Simons 11 Intermediate-Mass Black Hole in Gemini South at moonset, April 2008 Omega Centauri Eva Noyola Collisions of 15 Planetary Embryos Earthquake Readiness Joseph Rhee 49 Workshop Michael Sheehan 19 Taking the Measure of a Black Hole 58 Polly Roth Andrea Prestwich Staff Profile Peter Michaud 28 To Coldly Go Where No Brown Dwarf 62 Rodrigo Carrasco Has Gone Before Staff Profile Étienne Artigau & Philippe Delorme David Tytell Recent 31 66 Photo Journal Science Highlights North & South Jean-René Roy & R. Scott Fisher Photographs by Gemini Staff: • Étienne Artigau NICI Update • Kirk Pu‘uohau-Pummill 37 Tom Hayward GNIRS Update 39 Joseph Jensen & Scot Kleinman FLAMINGOS-2 Update Managing Editor, Peter Michaud 42 Stephen Eikenberry Science Editor, R. Scott Fisher MCAO System Status Associate Editor, Carolyn Collins Petersen 44 Maxime Boccas & François Rigaut Designer, Kirk Pu‘uohau-Pummill 3 Gemini Observatory www.gemini.edu June2008 by Doug Simons Director, Gemini Observatory Director’s Message Figure 1. any organizations (Gemini Observatory 100 The year-end task included) have extremely dedicated and hard- completion statistics 90 working staff members striving to achieve a across the entire M 80 0-49% Done observatory are worthwhile goal. -
Core-Collapse Supernovae Overview with Swift Collaboration
Publications Spring 2015 Core-Collapse Supernovae Overview with Swift Collaboration Kiranjyot Gill Embry-Riddle Aeronautical University, [email protected] Michele Zanolin Embry-Riddle Aeronautical University, [email protected] Marek Szczepańczyk Embry-Riddle Aeronautical University, [email protected] Follow this and additional works at: https://commons.erau.edu/publication Part of the Astrophysics and Astronomy Commons, and the Physics Commons Scholarly Commons Citation Gill, K., Zanolin, M., & Szczepańczyk, M. (2015). Core-Collapse Supernovae Overview with Swift Collaboration. , (). Retrieved from https://commons.erau.edu/publication/3 This Report is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Core-Collapse Supernovae Overview with Swift Collaboration∗ Kiranjyot Gill,y Dr. Michele Zanolin,z and Marek Szczepanczykx Physics Department, Embry Riddle Aeronautical University (Dated: June 30, 2015) The Core-Collapse supernovae (CCSNe) mark the dynamic and explosive end of the lives of massive stars. The mysterious mechanism, primarily focused with the shock revival phase, behind CCSNe explosions could be explained by detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, as a hint of the times where to search for the emission of GWs. More of these hints would be very helpful. For the first time in history a Harvard group has observed X-ray transients in coincidence with optical CCSNe. -
Notions Abordées En Cours De Physique -Chimie ( Classe De Secon
Notions abordées en cours de physique-chimie et situations de la vie courante I. Exploration de l’espace 1- De l’atome aux galaxies Notion Illustrations/Situations 1.1- Présentation de l’univers L’atome, la Terre, le système solaire, la Galaxie, les autres - Des quarks aux galaxies galaxies. 1.2- Echelle des longueurs. Echelle des distances de l’atome aux galaxies. - Plus c’est gros, moins c’est dense Unités de longueur. - Comment mesurer la largeur du sillon d’un CD ou d’un DVD ? Taille comparée des différents systèmes. Evaluer expérimentalement une distance : Méthode des parallaxes, technique de la visée, diamètre apparent. Comment déterminer les ordres de grandeur (taille d’une molécule, épaisseur d’un cheveu). 1.3-L’année de lumière. Propagation rectiligne de la lumière. Comment mesurer le - Pythagore versus Thalès ou Eratosthène revisité rayon de la Terre ? Méthode d’Eratosthène. - Voiliers et avions furtifs Vitesse de la lumière dans le vide et dans l’air. - Ils partirent à plus de 1021 mais se virent moins de 100 en Comment mesurer la distance Terre- Lune, de la profondeur arrivant au port d’un fond marin ? Usage du sonar. Intérêt de l’année de lumière. Comprendre que « voir loin, c’est voir dans le passé » - Notre présent n’a conscience que du passé extérieur - Une galaxie de prime jeunesse car fort lointaine 2- Messages de la lumière Notion Illustrations/Situations 2.1- Un système dispersif, le prisme. Radiation, réfraction, indice d’un milieu transparent, lois de - Comment reconnaître une gemme grâce à sa réfraction ? Descartes. - Mirage, mon beau mirage.. -
OCA CLUB MEETING STAR PARTIES COMING up the Free and Open Club the Black Star Canyon Site Will Be Open on the Next Session of the Meeting Will Be Held September 20Th
September 2008 Free to members, subscriptions $12 for 12 issues Volume 35, Number 9 REMINDER: SEPTEMBER MEETING MOVED TO SEPTEMBER 5TH! Don Lynn captured this image of NGC 6193 (cluster) and NGC 6188 (nebula) via an Internet-linked telescope in Australia on June 5, 2008. For those of us presently unable to afford a lengthy stay Down Under, Internet observing is a handy way to clear out one’s Southern Hemisphere list! OCA CLUB MEETING STAR PARTIES COMING UP The free and open club The Black Star Canyon site will be open on The next session of the meeting will be held September 20th. The Anza site will be open Beginners Class will be held on Friday, September 5th at on September 27th. Members are Friday, September 5th at the 7:30 PM in the Irvine encouraged to check the website calendar, Centennial Heritage Museum at Lecture Hall of the for the latest updates on star parties and 3101 West Harvard Street in Hashinger Science Center other events. Santa Ana. at Chapman University in GOTO SIG: TBA (contact Orange. The main Please check the website calendar for the coordinator for details) speaker is yet to be outreach events this month! Volunteers Astro-Imagers SIG: Sep. 16th, announced as of press are always welcome! Oct. 21st time, so be 65sure to You are also reminded to check the web EOA SIG: Sep. 24th, Oct. 22nd check the website for site frequently for updates to the calendar Astrophysics SIG:Sep. 19th, updates. of events and other club news. Oct. 17th Dark Sky Group: TBA (contact NEXT MEETING: October coordinator for details) 10th President’s Message By Barbara Toy My apologies – I’m afraid I fell down a bit on the job last month, as I didn’t realize until after the August issue of the Sirius Astronomer went to press that I had forgotten to give notice of the fact that our September general meeting had been moved to the first Friday of the month instead of our usual second Friday, because Chapman University needs to use the Chapman Auditorium for another function on our usual night. -
Observations of an X-Ray Transient in NGC 2770 1 Introduction 2 BAT
GCN Report 110.1 15-Jan-08 1 Observations of an X-ray transient in NGC 2770 K.L. Page (U. Leicester), S. Immler (NASA/UMCP/GSFC), A.P. Beardmore (U. Leicester), D.N. Burrows (PSU), N. Gehrels (GSFC) on behalf of the Swift Team and A. Soderberg (Princeton), E. Berger (Princeton) on behalf of a larger collaboration 1 Introduction During Swift observations of SN 2007uy beginning at 13:32:48.9 UT on 2008-01-09 (Obs ID 00031081002), a transient X-ray source was serendipitously identified and reported on Jan 10.58 (Berger & Soderberg, GCN Circ. 7159 and ATel 1353; Kong & Maccarone, ATel 1355). The source was observed to rise to a maximum flux about 65 seconds after the observation began, and then subsequently decay; the observed duration of the event is roughly 600 seconds. The X-ray emission was already in progress when this observation began, so the start time of the event is uncertain. The object was within the BAT field of view for approximately 30 minutes prior to the observation in which it was first detected (Burrows et al., GCN Circ 7179), but never triggered the instrument. Target of opportunity Swift follow-up observations were promptly scheduled to reveal the nature of the transient. The first announcement of an optical counterpart was reported by Deng & Zhu (GCN Circ. 7160) on Jan 10.76 UT, and confirmed by NOT observations on Jan 11.0 UT (Thoene et al., GCN Circ. 7161). A comparison of Asiago Observatory data taken Jan 7.0 and Jan 10.0 indicated that the optical counterpart brightened rapidly (Valenti et al., GCN Circ. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Astronomy 2009 Index
Astronomy Magazine 2009 Index Subject Index 1RXS J160929.1-210524 (star), 1:24 4C 60.07 (galaxy pair), 2:24 6dFGS (Six Degree Field Galaxy Survey), 8:18 21-centimeter (neutral hydrogen) tomography, 12:10 93 Minerva (asteroid), 12:18 2008 TC3 (asteroid), 1:24 2009 FH (asteroid), 7:19 A Abell 21 (Medusa Nebula), 3:70 Abell 1656 (Coma galaxy cluster), 3:8–9, 6:16 Allen Telescope Array (ATA) radio telescope, 12:10 ALMA (Atacama Large Millimeter/sub-millimeter Array), 4:21, 9:19 Alpha (α) Canis Majoris (Sirius) (star), 2:68, 10:77 Alpha (α) Orionis (star). See Betelgeuse (Alpha [α] Orionis) (star) Alpha Centauri (star), 2:78 amateur astronomy, 10:18, 11:48–53, 12:19, 56 Andromeda Galaxy (M31) merging with Milky Way, 3:51 midpoint between Milky Way Galaxy and, 1:62–63 ultraviolet images of, 12:22 Antarctic Neumayer Station III, 6:19 Anthe (moon of Saturn), 1:21 Aperture Spherical Telescope (FAST), 4:24 APEX (Atacama Pathfinder Experiment) radio telescope, 3:19 Apollo missions, 8:19 AR11005 (sunspot group), 11:79 Arches Cluster, 10:22 Ares launch system, 1:37, 3:19, 9:19 Ariane 5 rocket, 4:21 Arianespace SA, 4:21 Armstrong, Neil A., 2:20 Arp 147 (galaxy pair), 2:20 Arp 194 (galaxy group), 8:21 art, cosmology-inspired, 5:10 ASPERA (Astroparticle European Research Area), 1:26 asteroids. See also names of specific asteroids binary, 1:32–33 close approach to Earth, 6:22, 7:19 collision with Jupiter, 11:20 collisions with Earth, 1:24 composition of, 10:55 discovery of, 5:21 effect of environment on surface of, 8:22 measuring distant, 6:23 moons orbiting, -
The Center of the Crab Nebula
Michael Bietenholz, Hartebeesthoek Radio Observatory, South Africa 4 1984, 1.7 GHz 1 • 9 5 + 5 7 5 20 mas Wilkinson & de Bruyn, 1984 1988.8, 8 GHz S N 1 9 8 6 J 1 mas Bartel et al., 1990 Introduction and History • Radio emission from a supernova was first detected in the 1972 (SN 1970G; Gottesman et al., Goss et al.) • First paper about supernova and VLBI was in 1974 – Cass A at meter wavelengths • First determination of the size of a supernova in 1983: SN 1979C (Bartel et al.) • First image of a radio supernova in 1984: 41.95+575 in M82 (Wilkinson & de Bruyn) Radio Emission from Supernovae • Thermonuclear: – Type Ia: no detections to radio date (see Panagia et al 2006) • Core Collapse: – Type Ib/c (no Hydrogen in spectrum; stripped envelope stars) • Generally have steep spectra: α <~ −1 (S∝να) • Fast turn-on/turn-off, peak at 5 GHz near optical maximum – Type II: (Hydrogen in spectrum; supergiant progenitors) large range in radio luminosities • Relatively slow turn-on/turn-off, radio peak often significantly after optical peak. • Approximately 30 RSNe (all core-collapse) with flux densities > 1 mJy have been detected, and >100 have upper limits (Weiler et al.) Most are at <30 Mpc Radio Detection of SNe • Several hundred SNe are detected each year in optical • Only a few SNe detected each year in radio – Total radio SNe detections: a few dozen – ‘All’ radio detected SNe are core collapse (Type II, Type Ib/c etc) • Even fewer have been resolved by radio observations (so every VLBI observation is of great value)…. -
NGC 2770-A Supernova Ib Factory?
Draft July 2008 Preprint typeset using LATEX style emulateapj v. 12/14/05 NGC 2770 - A SUPERNOVA IB FACTORY? ∗ Christina C. Thone¨ 1, MichalJ. Micha lowski 1, Giorgos Leloudas 1, Nick L. J. Cox 2, Johan P. U. Fynbo 1, Jesper Sollerman 1,3, Jens Hjorth 1 and Paul M. Vreeswijk 1 Draft July 2008 ABSTRACT NGC 2770 has been the host of three supernovae of Type Ib during the last 10 years, SN 1999eh, SN 2007uy and SN 2008D. SN 2008D attracted special attention due to the serendipitous discovery of an associated X-ray transient. In this paper, we study the properties of NGC 2770 and specifically the three SN sites to investigate whether this galaxy is in any way peculiar to cause a high frequency of SNe Ib. We model the global SED of the galaxy from broadband data and derive a star-formation and SN rate comparable to the values of the Milky Way. We further study the galaxy using longslit spectroscopy covering the major axis and the three SN sites. From the spectroscopic study we find subsolar metallicities for the SN sites, a high extinction and a moderate star-formation rate. In a high resolution spectrum, we also detect diffuse interstellar bands in the line-of-sight towards SN 2008. A comparison of NGC 2770 to the global properties of a galaxy sample with high SN occurance (≥ 3 SN in the last 100 years) suggests that NGC 2770 is not particularly destined to produce such an enhancement of observed SNe observed. Its properties are also very different from gamma-ray burst host galaxies.