DOCSLIB.ORG

Spatially Resolved Manga Observations of the Host Galaxy of Superluminous Supernova 2017Egm

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Spatially Resolved Manga Observations of the Host Galaxy of Superluminous Supernova 2017Egm Draft version September 27, 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 SPATIALLY RESOLVED MANGA OBSERVATIONS OF THE HOST GALAXY OF SUPERLUMINOUS SUPERNOVA 2017EGM Ting-Wan Chen (sw,) 1, Patricia Schady1, Lin Xiao2, J.J. Eldridge2, Tassilo Schweyer1, Chien-Hsiu Lee (N見修) 3, Po-Chieh Yu (俞伯傑) 4, Stephen J. Smartt5 and Cosimo Inserra6 1Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße 1, 85748, Garching, Germany; [email protected] 2Department of Physics, University of Auckland, Private Bag 92019, Auckland, New Zealand 3Subaru Telescope National Astronomical Observatory of Japan, 650 N Aohoku Pl., Hilo, HI 96720, USA 4Graduate Institute of Astronomy, National Central University, No. 300, Zhongda Rd., Zhongli Dist., Taoyuan City 32001, Taiwan 5Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK 6Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK ABSTRACT Superluminous supernovae (SLSNe) are found predominantly in dwarf galaxies, indicating that their progenitors have a low metallicity. However, the most nearby SLSN to date, SN 2017egm, occurred in the spiral galaxy NGC 3191, which has a relatively high stellar mass and correspondingly high metallicity. In this paper, we present detailed analysis of the nearby environment of SN 2017egm using MaNGA IFU data, which provides spectral data on kiloparsec scales. From the velocity map we find no evidence that SN 2017egm occurred within some intervening satellite galaxy, and at the SN position most metallicity diagnostics yield a solar and above solar metallicity (12 + log (O=H) ∼ 8:8 − 9:1). Additionally we measure a small Hα equivalent width (EW) at the SN position of just 34 Å, which is one of the lowest EWs measured at any SLSN or Gamma-Ray Burst position, and indicative of the progenitor star being comparatively old. We also compare the observed properties of NGC 3191 with other SLSN host galaxies. The solar-metallicity environment at the position of SN 2017egm presents a challenge to our theoretical understanding, and our spatially resolved spectral analysis provides further constraints on the progenitors of SLSNe. Keywords: supernovae:general — supernovae:individual (SN 2017egm), galaxies:general — galax- ies:individual (NGC 3191) 1. INTRODUCTION larger sSFR, it is difficult to disentangle the relative impor- Superluminous supernovae (SLSNe)1 have been discov- tance of these properties towards the formation of SLSNe ered in recent wide field, untargeted surveys (e.g. Quimby (Perley et al. 2016; Chen et al. 2017a). From the ejecta et al. 2011). They are 100 times brighter (absolute mag- masses (Nicholl et al. 2015), and oxygen masses in the nitude of −21; Gal-Yam 2012) than typical core-collapse nebular spectra (Jerkstrand et al. 2017), it seems certain SNe, and the standard paradigm of iron-core collapse can- that the progenitors are above 20M , but whether they not account for their origin. Further constraints on the exclusively arise from higher mass stars (M > 40M ) progenitor properties arise from studying the nearby en- remains to be seen. arXiv:1708.04618v2 [astro-ph.GA] 26 Sep 2017 vironments. SLSNe appear to exclusively occur in dwarf The recent discovery of the closest SLSN to date, galaxies (Neill et al. 2011; Chen et al. 2013; Lunnan et al. SN 2017egm at z = 0:0307, which occurred in the massive, 2014; Leloudas et al. 2015; Angus et al. 2016) with less spiral galaxy NGC 3191 challenges the current hypothesis than around a half-solar metallicity (Perley et al. 2016; on the required host properties (Dong et al. 2017; Nicholl Chen et al. 2017a; Schulze et al. 2016). Their host galax- et al. 2017 and Bose et al. 2017). One major issue with ies also typically have high specific star formation rates these previous studies is they do not probe the local envi- ronment of SN 2017egm. The two available SDSS spectra (sSFR≡SFR/M∗), which may indicate that the progeni- tors are very young stars (Leloudas et al. 2015). Given analysed in Nicholl et al.(2017) were from spectrograph that low mass and metal-poor galaxies have typically fibers that did not cover the SN site. Here we present a detailed analysis of the host galaxy of SN 2017egm 1 In this paper we use the term SLSN to refer only to hydrogen- poor, Type I SLSNe 0 90 2 70 100 2 0 ◦ 0 6 6 4 2 70 80 2 0 ◦ 0 6 3 4 2 70 60 2 0 ◦ 0 6 0 4 2 70 40 2 0 ◦ 0 6 7 4 1 70 20 2 0 ◦ 0 6 4 4 1 0 70 2 0 ◦ 0 6 1 SN2017egm km/s 4 1 20 70 2 0 ◦ 0 6 8 4 0 0 40 Declination (J2000) 7 2 0 ◦ 0 6 5 4 0 60 70 2 0 ◦ 0 6 2 80 4 0 70 2 ◦ 6 100 4 s s s s s s s s s s 5 2 9 6 3 0 7 4 1 8 . 6 6 5 5 5 5 4 4 4 3 m 0 m 0 m 0 m 0 m 0 m 0 m 0 m 0 m 0 m 0 9 9 9 9 9 9 9 9 9 9 h 1 h 1 h 1 h 1 h 1 h 1 h 1 h 1 h 1 h 1 0 0 0 0 0 0 0 0 0 0 1 1 1 1 1 1 1 1 1 1 Right Ascension (J2000) 2 Chen et al. Figure 1 redshift of just redward of the H masked-out the area where this unidentified feature appears. : Left: using SDSS/MaNGA z at APO; Bundy et al. 2015) data= obtained0 MaNGA from FOV the ofSDSS NGC 3191. Data Release 14 2016-Jan-17. The MaNGA field-of-view:031 provides spec- tral measurements across a large area of NGC 3191 (Fig. In the top right region of the map there are about 30 pixels that show an additional feature 1). Using these data, we present the direct measurement of metallicity at this SLSN site, use the EW to studyα the progenitor properties, and compare the gas-phase line that is clearly not intrinsic to the nebular line emission from NGC 3191, we therefore properties of NGC 3191 with other SLSN host galaxies. 2 3 . The observationsurvey (Mapping was conducted Nearby on Galaxies 2. RESULTS OF THE MANGA DATA OF NGC 3191 MaNGAWe datacube,used our own following inhouse a similar tools to procedure analyze as the de- large scribed in Krühler et al.(2017). To separate the stellar and gas-phase components of the galaxy, we used the spec- Right: tral synthesis code 2009) to fit stellar population models to each spaxel. By subtracting the best-fit stellar template from the observed Velocity map inferred from the position of the H spectra, we were left with a datacube only containing the contribution of the gas-phase, which we then used to derive the velocity and metallicity maps. starlight 2 3 http://www.sdss.org/surveys/manga http://skyserver.sdss.org/dr14/en/home.aspx satelliteMany galaxies spiral (e.g.galaxies the are Magellanic often accompanied satellites ofby the dwarf Milky Way), and thus SN 2017egm might reside in a (e.g. Cid Fernandes et al. nearby dwarf satellite galaxy along the line-of-sight, rather 2.1. than in NGC 3191 itself. Such a kinematically distinct galaxy (200-300 km s Velocity map served in emission lines if the SFR of the satellite were high enough. of theWe created a velocity map by measuring the position at each spatial pixel, assuming a redshift of As shown in Fig.1, the velocity map is smooth across α the SN 2017gemH explosion site with no indication of a α line relative a kinematically distinct component. Using the line with respect to the rest-frame− wavelength the SN position to derive our sensitivity to the detection1 of a foreground dwarf galaxy, we place a conservativemight be expected) could be ob- upper limit of corresponds to SFR limit with a nearby ( et al. 2017a), and only 2 of 19 hosts may have a SFR less than our limit (the remaining 17 hosts have SFRs > would0 be the true host galaxy, it is at the lowest end of the : f host SFR distribution.01 On the other hand,H the satellite would have to beM many times larger thanα the spatial < < yr 1 − 0 :9 1 z < :002 ). Therefore, if a line-of-sight× satellite 10 0 M z : − 3 16 = 0 ) SLSNyr host sample (Chen − erg s 1 :0307 ). We compared this H − α 1 . cm flux at − 2 (which Host galaxy of SLSN 2017egm 3 9. 20 a) b) 60 9. 16 1 ) 10− 2 9. 12 − 3 50 c 9. 08 2 p R ) k 1 9. 04 H / 40 − r O ( y 9. 00 g ¯ SN2017egm SN2017egm o 30 8. 96 l M + ( 8. 92 2 1 R 20 2 F 8. 88 10− S PSF PSF 8. 84 10 1 kpc 1 kpc 8. 80 10 20 30 40 50 60 0. 50 3. 0 c) d) 60 0. 45 2. 7 0. 40 2. 4 50 0. 35 2. 1 ) g a 1. 8 0. 30 40 m ( 1. 5 0. 25 SN2017egm V SN2017egm − 30 1. 2 0. 20 B E 0. 9 0. 15 log([SIII]/[SII]) 20 0. 6 0. 10 PSF PSF 0. 3 10 1 kpc 0. 05 1 kpc 10 20 30 40 50 60 e) f) 60 Hα 60 [OIII]λ5007 102 50 50 ) ) 101 40 Å 40 Å ( ( W W SN2017egm 1 SN2017egm 10 E E 30 30 20 20 PSF PSF 10 1 kpc 10 1 kpc 100 100 10 20 30 40 50 60 10 20 30 40 50 60 Figure 2: Reconstructed images of NGC 3191 from the MaNGA data cube.
Load more

Recommended publications
  • Annual Report 2016–2017 AAVSO
    AAVSO The American Association of Variable Star Observers Annual Report 2016–2017 AAVSO Annual Report 2012 –2013 The American Association of Variable Star Observers AAVSO Annual Report 2016–2017 The American Association of Variable Star Observers 49 Bay State Road Cambridge, MA 02138-1203 USA Telephone: 617-354-0484 Fax: 617-354-0665 email: [email protected] website: https://www.aavso.org Annual Report Website: https://www.aavso.org/annual-report On the cover... At the 2017 AAVSO Annual Meeting.(clockwise from upper left) Knicole Colon, Koji Mukai, Dennis Conti, Kristine Larsen, Joey Rodriguez; Rachid El Hamri, Andy Block, Jane Glanzer, Erin Aadland, Jamin Welch, Stella Kafka; and (clockwise from upper left) Joey Rodriguez, Knicole Colon, Koji Mukai, Frans-Josef “Josch” Hambsch, Chandler Barnes. Picture credits In additon to images from the AAVSO and its archives, the editors gratefully acknowledge the following for their image contributions: Glenn Chaple, Shawn Dvorak, Mary Glennon, Bill Goff, Barbara Harris, Mario Motta, NASA, Gary Poyner, Msgr. Ronald Royer, the Mary Lea Shane Archives of the Lick Observatory, Chris Stephan, and Wheatley, et al. 2003, MNRAS, 345, 49. Table of Contents 1. About the AAVSO Vision and Mission Statement 1 About the AAVSO 1 What We Do 2 What Are Variable Stars? 3 Why Observe Variable Stars? 3 The AAVSO International Database 4 Observing Variable Stars 6 Services to Astronomy 7 Education and Outreach 9 2. The Year in Review Introduction 11 The 106th AAVSO Spring Membership Meeting, Ontario, California 11 The
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • The Host of the Type I SLSN 2017Egm: a Young, Sub-Solar Metallicity Environment in a Massive Spiral Galaxy
    Astronomy & Astrophysics manuscript no. PMAS2017egm_3 c ESO 2017 October 3, 2017 The host of the Type I SLSN 2017egm: A young, sub-solar metallicity environment in a massive spiral galaxy. L. Izzo1, C. C. Thöne1, R. García-Benito1, A. de Ugarte Postigo1,2, Z. Cano1, D. A. Kann1, K. Bensch 1, M. Della Valle3,4, D. Galadí-Enríquez5, R. P. Hedrosa5 1Instituto de Astrofisica de Andalucia (IAA-CSIC), Glorieta de la Astronomia s/n, 18008 Granada, Spain 2Dark Cosmology Centre, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark 3INAF-Capodimonte Observatory, Salita Moiariello 16, I-80131, Napoli, Italy 4International Center for Relativistic Astrophysics, Piazzale della Repubblica, 2, 65122, Pescara, Italy 5Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain ABSTRACT Context. Type-I Super-luminous-Supernova (SLSN) host galaxies are predominantly low-metallicity, highly star-forming dwarfs. One of the current key questions is whether SLSNe Type I can only occur in such environments and hosts. Aims. Here we present an integral-field study of the massive, high-metallicity spiral NGC 3191, the host of SN 2017egm, the closest SLSN Type I to date. We use data from PMAS/CAHA and the public MaNGA survey to shed light on the properties of the SLSN site and the origin of star-formation in this non-starburst spiral galaxy. Methods. We map the physical properties different H ii regions throughout the galaxy and characterize their stellar populations using the STARLIGHT fitting code. Kinematical information allows to study a possible interaction with its neighbouring galaxy as the origin of recent star formation activity which could have caused the SLSN.
    [Show full text]
  • The Superluminous Supernova Sn 2017Egm in the Nearby Galaxy Ngc 3191: a Metal-Rich Environment Can Support a Typical Slsn Evolution
    DRAFT VERSION SEPTEMBER 21, 2018 Preprint typeset using LATEX style AASTeX6 v. 1.0 THE SUPERLUMINOUS SUPERNOVA SN 2017EGM IN THE NEARBY GALAXY NGC 3191: A METAL-RICH ENVIRONMENT CAN SUPPORT A TYPICAL SLSN EVOLUTION MATT NICHOLL1 ,EDO BERGER1 ,RAFFAELLA MARGUTTI2 ,PETER K. BLANCHARD1 ,JAMES GUILLOCHON1 ,JOEL LEJA1 AND RYAN CHORNOCK3 1Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA; [email protected] 2Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 3Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USA ABSTRACT At redshift z = 0:03, the recently-discovered SN 2017egm is the nearest Type I superluminous supernova (SLSN) to date, and first near the center of a massive spiral galaxy (NGC 3191). Using SDSS spectra of NGC 3191, we find a metallicity ∼ 2 Z at the nucleus and ∼ 1:3 Z for a star forming region at a radial offset similar -1 to SN 2017egm. Archival radio-to-UV photometry reveals a star-formation rate ∼ 15 M yr (with ∼ 70% 10:7 dust-obscured), which can account for a Swift X-ray detection, and stellar mass ∼ 10 M . We model the early UV-optical light curves with a magnetar central-engine model, using the Bayesian light curve fitting tool 14 MOSFiT. The fits indicate ejecta mass 2 - 4 M , spin period 4 - 6 ms, magnetic field (0:7 - 1:7) × 10 G, and kinetic energy 1-2×1051 erg. These parameters are consistent with the overall distributions for SLSNe, modeled by Nicholl et al.(2017b), although the derived mass and spin are towards the low end, possibly indicating enhanced loss of mass and angular momentum before explosion.
    [Show full text]
  • The Astronomer Magazine Index
    The Astronomer Magazine Index The numbers in brackets indicate approx lengths in pages (quarto to 1982 Aug, A4 afterwards) 1964 May p1-2 (1.5) Editorial (Function of CA) p2 (0.3) Retrospective meeting after 2 issues : planned date p3 (1.0) Solar Observations . James Muirden , John Larard p4 (0.9) Domes on the Mare Tranquillitatis . Colin Pither p5 (1.1) Graze Occultation of ZC620 on 1964 Feb 20 . Ken Stocker p6-8 (2.1) Artificial Satellite magnitude estimates : Jan-Apr . Russell Eberst p8-9 (1.0) Notes on Double Stars, Nebulae & Clusters . John Larard & James Muirden p9 (0.1) Venus at half phase . P B Withers p9 (0.1) Observations of Echo I, Echo II and Mercury . John Larard p10 (1.0) Note on the first issue 1964 Jun p1-2 (2.0) Editorial (Poor initial response, Magazine name comments) p3-4 (1.2) Jupiter Observations . Alan Heath p4-5 (1.0) Venus Observations . Alan Heath , Colin Pither p5 (0.7) Remarks on some observations of Venus . Colin Pither p5-6 (0.6) Atlas Coeli corrections (5 stars) . George Alcock p6 (0.6) Telescopic Meteors . George Alcock p7 (0.6) Solar Observations . John Larard p7 (0.3) R Pegasi Observations . John Larard p8 (1.0) Notes on Clusters & Double Stars . John Larard p9 (0.1) LQ Herculis bright . George Alcock p10 (0.1) Observations of 2 fireballs . John Larard 1964 Jly p2 (0.6) List of Members, Associates & Affiliations p3-4 (1.1) Editorial (Need for more members) p4 (0.2) Summary of June 19 meeting p4 (0.5) Exploding Fireball of 1963 Sep 12/13 .
    [Show full text]
  • Objektauswahl NGC Seite 1
    UMa – Objektauswahl NGC Seite 1 NGC 2600 NGC 2654 NGC 2688 NGC 2742 NGC 2810 NGC 2895 NGC 3009 NGC 3079 NGC 2602 NGC 2656 NGC 2689 NGC 2756 NGC 2814 NGC 2950 NGC 3010 NGC 3102 NGC 2603 NGC 2692 NGC 2762 NGC 2820 NGC 2959 NGC 3027 NGC 3111 Seite 2 NGC 2605 NGC 2675 NGC 2693 NGC 2767 NGC 2841 NGC 2961 NGC 3031 NGC 3135 NGC 2606 NGC 2676 NGC 2694 NGC 2768 NGC 2854 NGC 2976 NGC 3034 NGC 3164 Seite 3 NGC 2614 NGC 2701 NGC 2681 NGC 2769 NGC 2856 NGC 2985 NGC 3043 NGC 3168 Seite 4 NGC 2629 NGC 2684 NGC 2710 NGC 2771 NGC 2857 NGC 2998 NGC 3065 NGC 3179 NGC 2639 NGC 2685 NGC 2726 NGC 2787 NGC 2870 NGC 3005 NGC 3066 NGC 3180 Seite 5 NGC 2641 NGC 2686 NGC 2739 NGC 2800 NGC 2880 NGC 3006 NGC 3073 NGC 3181 NGC 2650 NGC 2687 NGC 2740 NGC 2805 NGC 2892 NGC 3008 NGC 3077 NGC 3182 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken UMa – Objektauswahl NGC Seite 2 NGC 3184 NGC 3225 NGC 3298 NGC 3394 NGC 3445 NGC 3530 NGC 3553 NGC 3594 NGC 3188 NGC 3231 NGC 3310 NGC 3398 NGC 3448 NGC 3536 NGC 3554 NGC 3595 Seite 1 NGC 3191 NGC 3236 NGC 3319 NGC 3406 NGC 3470 NGC 3539 NGC 3556 NGC 3600 NGC 3198 NGC 3237 NGC 3320 NGC 3407 NGC 3471 NGC 3540 NGC 3558 NGC 3610 NGC 3202 NGC 3238 NGC 3348 NGC 3408 NGC 3478 NGC 3542 NGC 3561 NGC 3613 Seite 3 NGC 3205 NGC 3259 NGC 3353 NGC 3410 NGC 3488 NGC 3543 NGC 3569 NGC 3614 Seite 4 NGC 3206 NGC 3264 NGC 3359 NGC 3415 NGC 3499 NGC 3545 NGC 3577 NGC 3619 NGC 3207 NGC 3266 NGC 3364 NGC 3416 NGC 3516 NGC 3549 NGC 3583
    [Show full text]
  • Meteor , ,{ > Csillagászati Évkönyv 1994
    M meteor , ,{ > csillagászati * i évkönyv 1994 Számítástechnika kulcsrakészen! — 386SX, 386, 486 számítógépek minden kiépítésben, 3 év garanciával — Laptop, Notebook számítógépek — EPSON, STAR, Hewlett Packard nyomtatók — Discovery és US Robotics modemek — APC szünetmentes tápegységek — ASHTON-TATE, BORLAND, MICROSOFT, NANTUCKET, LOTUS szoftverek — Modemes távadatátviteli és BBS-rendszerek szállítása — NOVELL-hálózati szoftverek, hálózatépítés — Számítógépek és tartozékok javítása QUU€RTY High Tech Kft. Címünk: 1114 Budapest, Orlay u. 4. Üzlet: 1114 Budapest, Bartók Béla út 9. Tel.: 18-68-858, 18-52-687, 16-63-098 Fax: 18-52-687 BBS: 11-87-950 (Budapest BBS) NE FELEDJE: nevünk ott található az ÖN számítógépének billentyűzetén is! A MAGYAR CSILLAGÁSZAT) C- íYESt KÖNYVTÁRA meteor csillagászati évkönyv 1994 szerkesztette: Mizser Attila Taracsák Gábor Az évkönyv összeállításában közreműködtek: EAON (Belgium) Guman István Holl András Jean Meeus (Belgium) Sárneczky Krisztián Tepliczky István T ó th Éva Zajácz György Zalezsák Tamás A szerkesztés a Fővárosi Önkormányzat Tudományos Alapja és az M TA Csillagászati Kutatóintézete támogatásával készült Magyar Csillagászati Egyesület Budapest, 1993 Szakmailag ellenőrizte: Benkő József Szabados László Műszaki szerkesztés és illusztrációk: Taracsák Gábor ISSN 0866-2851 Felelős kiadó: Mizser Attila Készült a Kertészeti és Élelmiszeripari Egyetem Nyomdájában Felelős vezető: Wilpert Gábor Terjedelem: 13 (A5) ív Példányszám: 4000 1993. október Tartalom Bevezető..........................................................................................................................................................5
    [Show full text]
  • Alexei V. Filippenko PUBLICATIONS (∗ = Refereed Journals); 18 July 2021
    Alexei V. Filippenko PUBLICATIONS (∗ = refereed journals); 18 July 2021 Citations: >128k (ADS), >168k (Google Scholar). h-index: 150 (ADS), 172 (Google Scholar) ∗1) A. V. Filippenko and R. S. Simon (1981). Astron. Jour., 86, 671{686. \A Study of 52 RR Lyrae Stars in M15." ∗2) A. V. Filippenko (1982). Publ. Astron. Soc. Pacific, 94, 715{721. \The Importance of Atmospheric Differential Refraction in Spectrophotometry." ∗3) A. V. Filippenko and V. Radhakrishnan (1982). Astrophys. Jour., 263, 828{834. \Pulsar Nulling and Drifting Subpulse Phase Memory." 4) A. V. Filippenko, A. C. S. Readhead, and M. S. Ewing (1983). In Positron-Electron Pairs in Astrophysics (Proceedings of AIP Conference 101), ed. M. L. Burns, A. K. Harding, and R. Ramaty (New York: American Institute of Physics), 113{117. \The Effect of Nulls on the Drifting Subpulses in PSR 0809+74." ∗5) M. A. Malkan and A. V. Filippenko (1983). Astrophys. Jour., 275, 477{492. \The Stellar and Nonstellar Continua of Seyfert Galaxies: Nonthermal Emission in the Near-Infrared." ∗6) A. V. Filippenko and J. L. Greenstein (1984). Publ. Astron. Soc. Pacific, 96, 530{536. \Faint Spectrophotometric Standard Stars for Large Optical Telescopes. I." ∗7) A. V. Filippenko and J. P. Halpern (1984). Astrophys. Jour., 285, 458{474. \NGC 7213: A Key to the Nature of Liners?" ∗8) J. P. Halpern and A. V. Filippenko (1984). Astrophys. Jour., 285, 475{482. \The Nonstellar Continuum of the Seyfert Galaxy NGC 7213." 9) A. V. Filippenko (1984). Ph.D. thesis, California Institute of Technology. (Ann Arbor: University Microfilms International), \Physical Conditions in Low-Luminosity Active Galactic Nuclei." ∗10) A.
    [Show full text]
  • Steven Villanueva Jr
    Steven Villanueva Jr. – Cirriculum Vitae David G. Price Instrumentation Fellow Office: +1 (614) 292 2076 The Ohio State University, Department of Astronomy Mobile: +1 (469) 288 5037 4055 McPherson Laboratory, 140 West 18th Avenue [email protected] Columbus, OH 43210-1173 http://www.astronomy.ohio-state.edu/∼svillan/ Personal Profile United States Air Force Veteran, PhD candidate at The Ohio State University, National Science Founda- tion Graduate Research Fellow, and David G. Price Instrumentation Fellow. Interested in the discovery and characterization of exoplanets, primarily through ground-based transits, and instrumentation. Actively involved in outreach, the Society for the Advancement of Chicano/Hispanic and Native American Scientists (SACNAS), the National Society of Hispanic Physicists, and increasing diversity and minority participation in science. Employment 2017 - Present David G. Price Instrumentation Fellow, The Ohio State University, Columbus, OH 2014 - 2017 NSF GRFP Fellow, The Ohio State University, Columbus, OH 2012 - 2014 Teaching Assistant, The Ohio State University, Columbus, OH 2009 - 2012 Undergraduate Research Assistant, Texas A&M University, College Station, TX 2003 - 2007 Aerospace Ground Equipment Mechanic, United States Air Force, RAF Lakenheath, UK Education 2016 M.S. in Astronomy, The Ohio State University 2012 B.S. in Physics, Texas A&M University Fellowships and Awards 2017 David G. Price Fellowship for Instrumentation 2017 Honorable Mention, Ford Foundation Graduate Dissertation Fellowship 2016
    [Show full text]
  • CURRICULUM VITAE Benjamin John Shappee
    CURRICULUM VITAE Benjamin John Shappee Assistant Professor University of Hawaii [email protected] Institute for Astronomy http://www.ifa.hawaii.edu/users/shappee/ 2680 Woodlawn Drive Citizenship: United States of America Honolulu, HI 96822-1839 USA Research Interests Observational astrophysics with an emphasis on optical surveys, the transient universe, tidal disruption events, changing-look active galactic nuclei, and type Ia supernovae progenitors. Positions Held 2017 − : Assistant Professor University of Hawaii, Institute for Astronomy 2014 − 2017 : Hubble, Carnegie-Princeton Fellow, Carnegie Observatories 2013 − 2014 : OSU Presidential Fellow, Department of Astronomy, The Ohio State University 2013 : Research Associate, Department of Astronomy, The Ohio State University 2010 − 2013 : National Science Foundation Graduate Research Fellow, Department of Astronomy, The Ohio State University 2009 − 2010 : Teaching Associate, Department of Astronomy, The Ohio State University 2008 − 2009 : Research Assistant, Department of Physics and Astronomy, Rutgers University Advisor: Prof. Saurabh W. Jha 2006 − 2008 : Physics Demonstration Assistant, Department of Physics and Astronomy, Rutgers University Education June, 2014 : Ph.D., Astronomy, The Ohio State University, Columbus, Ohio Thesis: The Transient Universe Advisor: Professor Krzysztof Z. Stanek June, 2012 : M.S., Astronomy, The Ohio State University, Columbus, Ohio May, 2009 : B.A., Physics, Astronomy & Math, Rutgers University, New Brunswick, New Jersey Honors: Summa Cum Laude Honors & Awards 2014 : NASA Hubble Fellowship, Carnegie Observatories (National) 2014 : Carnegie-Princeton Fellowship, Carnegie Observatories (National) 2013 : Presidential Fellowship, The Ohio State University (University) 2013 : Allan Markowitz Award in Observational Astronomy, The Ohio State University (Departmental) 2010 : National Science Foundation’s Graduate Research Fellow, The Ohio State University (National) 2009 : Richard T. Weidner Prize, Rutgers University (Departmental) 2008 : Herman Y.
    [Show full text]
  • Object Type RA Dec Mag Size Constellation
    Object Type RA Dec Mag Size Constellation ------ ---- -- --- --- ---- ------------- IC 43 Galaxy 00h 42m 30.4s +29° 39' 19" 14.0 1.6'x1.4' Andromeda IC 65 Galaxy 01h 01m 03.9s +47° 41' 40" 13.5 3.9'x1.1' Andromeda IC 179 Galaxy 02h 00m 20.6s +38° 02' 02" 13.4 1.8'x1.5' Andromeda IC 239 Galaxy 02h 36m 37.5s +38° 58' 50" 11.9 4.6'x4.2' Andromeda IC 1525 Galaxy 23h 59m 23.4s +46° 54' 06" 13.2 1.9'x1.4' Andromeda M 31 Galaxy 00h 42m 52.7s +41° 16' 54" 4.3 189.1'x61.7' Andromeda M 32 Galaxy 00h 42m 50.2s +40° 52' 43" 9.1 8.5'x6.5' Andromeda M 110 Galaxy 00h 40m 30.4s +41° 41' 53" 8.9 19.5'x11.5' Andromeda NGC 21 Galaxy 00h 10m 55.2s +33° 21' 54" 13.6 1.5'x0.7' Andromeda NGC 43 Galaxy 00h 13m 09.1s +30° 55' 43" 13.7 1.6'x1.5' Andromeda NGC 76 Galaxy 00h 19m 46.0s +29° 56' 50" 14.0 1.0'x0.9' Andromeda NGC 80 Galaxy 00h 21m 19.2s +22° 22' 17" 13.2 2.2'x2.0' Andromeda NGC 83 Galaxy 00h 21m 30.9s +22° 26' 52" 13.6 1.3'x1.2' Andromeda NGC 97 Galaxy 00h 22m 38.3s +29° 45' 31" 13.4 1.5'x1.3' Andromeda NGC 108 Galaxy 00h 26m 08.0s +29° 13' 31" 13.1 2.0'x1.6' Andromeda NGC 140 Galaxy 00h 31m 28.7s +30° 48' 18" 14.0 1.5'x1.2' Andromeda NGC 160 Galaxy 00h 36m 12.5s +23° 58' 18" 13.5 2.9'x1.6' Andromeda NGC 169 Galaxy 00h 37m 00.1s +24° 00' 18" 13.2 1.8'x0.6' Andromeda NGC 183 Galaxy 00h 38m 37.7s +29° 31' 30" 13.6 2.1'x1.6' Andromeda NGC 214 Galaxy 00h 41m 36.4s +25° 30' 46" 13.0 1.9'x1.5' Andromeda NGC 233 Galaxy 00h 43m 44.9s +30° 36' 01" 13.8 1.7'x1.6' Andromeda NGC 252 Galaxy 00h 48m 10.1s +27° 38' 12" 13.4 1.4'x1.0' Andromeda NGC 262 Galaxy 00h 48m
    [Show full text]
  • Far-UV HST Spectroscopy of an Unusual Hydrogen-Poor Superluminous Supernova: Sn2017egm
    The Astrophysical Journal, 858:91 (10pp), 2018 May 10 https://doi.org/10.3847/1538-4357/aabad5 © 2018. The American Astronomical Society. All rights reserved. Far-UV HST Spectroscopy of an Unusual Hydrogen-poor Superluminous Supernova: SN2017egm Lin Yan1, D. A. Perley2 , A. De Cia3, R. Quimby4 , R. Lunnan5 , Kate H. R. Rubin4 , and P. J. Brown6 1 Caltech Optical Observatories and IPAC, California Institute of Technology, Pasadena, CA 91125, USA; [email protected] 2 Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK 3 European Southern Observatory, Karl-Schwarzschild Str. 2, D-85748 Garching bei Muenchen, Germany 4 Department of Astronomy, San Diego State University, San Diego, CA 92182, USA 5 Oskar Klein Center, Astronomy Department, Stockholm University, SE-106 91 Stockholm, Sweden 6 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics &Astronomy, Texas A. &M. University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843, USA Received 2017 October 31; revised 2018 March 8; accepted 2018 March 24; published 2018 May 10 Abstract SN2017egm is the closest (z=0.03) H-poor superluminous supernova (SLSN-I) detected to date, and a rare example of an SLSN-I in a massive, metal-rich galaxy. We present the HST UV and optical spectra covering 1000–5500 Å, taken at +3 day relative to the peak. Our data reveal two absorption systems at redshifts matching the host galaxy NGC 3191 (z=0.0307) and its companion galaxy (z=0.0299) 73″ apart. Weakly damped Lyα absorption lines are detected at these two redshifts, with H I column densities of (3.0±0.8)×1019 and − (3.7±0.9)×1019 cm 2, respectively.
    [Show full text]