DOCSLIB.ORG

(Tev) Observations of Pulsar Wind Nebulae and Supernova Remnants

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
(Tev) Observations of Pulsar Wind Nebulae and Supernova Remnants Very-High-Energy (TeV) Observations of Pulsar Wind Nebulae and Supernova Remnants Nukri Komin University of the Witwatersrand Johannesburg, South Africa Nukri Komin 9th International Fermi Symposium (2021) 1 PWNe and SNRs in a Nutshell possible binary systems black holes supernova explosion isolated neutron stars of massive star rotating neutron star core contraction → pulsar rotation driven 28 38 e surrounded by electron wind Ė 10 ...10 erg/s xp (C) A Hitchhikers Gui an → pulsar wind nebula de to Space and Pla si sma Physics on o f o ut er composites la ye rs kinetic SN energy warf explosion supernova type Ia white d supernova remnant ~1051 erg Nukri Komin 9th International Fermi Symposium (2021) 2 TeV Instruments ➲ ground based observations of atmospheric showers ➲ Imaging Air Cherenkov Telescopes → Cherenkov light in air → small field of view, low-duty cycle → detailed studies of individual sources → H.E.S.S., MAGIC, VERITAS ➲ Extensive Air Shower Arrays → direct detection of shower particles → large field of view, large duty cycle → population studies, large sources → Cherenkov light in water tanks (HAWC) → scintillation counters (Tibet Air Shower Array) Nukri Komin 9th International Fermi Symposium (2021) 3 Hubble (NASA/ESA) Crab Nebula: TeV Observation Timeline ➲ 1989, Whipple [Weekes et al. 1989 ApJ v.342, p.379] → 9σ detection, >0.7 TeV ➲ 1996, HEGRA [HEGRA Collaboration 1996 APh v. 4-3, p. 199-215] H.E.S.S. 2006 → 10σ detection, 1-3 TeV, power law spectrum ➲ 2003, Milagro [Atkins et al. ApJ v. 595, Issue 2, pp. 803-811] → 3 6.4σ, 4 TeV median energy 186 MAGIC >25 GeV ➲ 2006, H.E.S.S. [H.E.S.S. Collaboration, A&A, v. 457-3, pp.899-915] 185 → ~100σ, 440 GeV – 40 TeV, spectral cut-off 184 ➲ 2008, MAGIC [MAGIC Collaboration, ApJ v. 674-2, p. 1037-1055] 183 -1 -0.5 0.501 → 60 GeV – 9 TeV, curved power law Phase ➲ pulsed emission → 2008, MAGIC [MAGIC Collaboration, Science, Volume 322, Issue 5905, pp. 1221] → 2011, VERITAS [VERITAS Collaboration, Science 334: 69] ➲ > 100 TeV photons → 2019, Tibet [Amenomori et al. PhysRevL, v. 123, Issue 5, id.051101] → 2019, HAWC [HAWC Collaboration ApJ, Volume 881, Issue 2, article id. 134] ➲ 2020, H.E.S.S. [H.E.S.S. Collaboration, NatAs Volume 4, p. 167-173] → extension ➲ many other publications and instruments (CTA prototypes, ...) [MAGIC, JHEAp, Volume 5, p. 30-38.] Nukri Komin 9th International Fermi Symposium (2021) 4 Crab Nebula ➲ PSR B0531+21 → P = 33.4 ms, Ṗ =4.2×10-13, Ė = 4.5×1038 erg/s, age ~1000 years → d = 2 kpc [MAGIC, JHEAp, Volume 5, p. 30-38.] ➲ gamma-ray luminosity → 50 GeV – 30 TeV → 1035 erg/s (0.02% Ė) ➲ Why is it so bright in TeV? → 2nd most luminous pulsar → point-like source ● X-ray extension 50’’ (0.5 pc) → strong synchrotron emission → SSC Nukri Komin 9th International Fermi Symposium (2021) 5 Crab Nebula with H.E.S.S. ➲ [HESS 2020, Nat. Astron,, v, 4, p. 167-173] ➲ increase angular resolution → simulate detector response on run-by-run basis → account for detector problems, night-sky-background, ... → 0.05° (68% containment) X C M h ➲ a 1.0 - 3.0 TeV Electrons Crab extension 52’’ (1σ of Gaussian) a M n d U 3.0 - 10.0 TeV Electrons r a −7 V 10 W 10.0 - 30.0 TeV Electrons H 1 . → E smaller than in UV . S . S ) −8 . 1 10 − → significantly larger than in X-rays s 2 − −9 m 10 c ➲ g H.E.S.S. probes electron energies r e −10 ( 10 ν that are not well observed in F synchrotron emission ν 10−11 10−12 10−7 10−4 10−1 102 105 108 1011 1014 Energ (eV) Nukri Komin 9th International Fermi Symposium (2021) 6 HESS J1825–137 ➲ [HESS 2019, A&A 621, A116] ➲ PSR B1823–13 → Ė = 2.8×1036 erg/s, age 21 kyrs → d ~ 4 kpc ➲ PWN at TeV → ~0.8° (~56 pc) ● larger than X-ray nebula (15’) [Uchiyama et al., PASJ 2009, v.61, pp.S189] ● larger than 1-100GeV nebula (0.56°) [Grondin et al 2011 ApJ 738 42] → L = 3.1×1035 erg/s = 11% Ė Nukri Komin 9th International Fermi Symposium (2021) 7 HESS J1825–137 ➲ energy dependent morphology → highest energy electrons do not travel too far away from pulsar → >16 TeV photons come only from X-ray nebula Table 3. Extent measurements as a function of energy for analyses A and B, with statistical and systematic errors. Energy range Extent (A) Extent (B) <1 ! "e# $ %.37◦ ±%.15◦ ±%.3◦ 1 !− !% "e# $ %.63◦ ±%.%&◦ ±%.%&◦ < !% "e# %.''◦ ±%.%(◦ ±%.3◦ $ !%−!%% "e# %.&'◦ ±%.03◦ ±%. ◦ %.71◦ ±%.%)◦ ±%.01◦ !%% "e#−1 Te# %.& ◦ ±%.% ◦ ±%.%!◦ %.& ◦ ±%.%!◦ ±%. ◦ 1− Te# %.'(◦ ±%.% ◦ ±%.11◦ %.' ◦ ±%.%&◦ ±%.(◦ −( Te# %.(&◦ ±%.%(◦ ±%.%*◦ %.51◦ ±%.%!◦ ±%.1◦ (−* Te# %.38◦ ±%.%(◦ ±%.13◦ %.33◦ ±%.%&◦ ±%.%(◦ *−16 Te# %. &◦ ±%.%&◦ ±%.%'◦ %.30◦ ±%.12◦ ±%.3◦ >16 Te# $ %. ◦ ±%.12◦ ±%. ◦ 16−32 Te# %.19◦ ±%.%*◦ ±%.14◦ $ X-ray nebula >32 Te# %.14◦ ±%.1◦ ±%.%!◦ $ Nukri Komin 9th International Fermi Symposium (2021) 8 Particle Transport in HESS J1825–137 ) o ➲ energy dependent diffusion ( ! t n e → size would increase with energy t 1 $ E ! l a ➲ diffusion and cooling # d a → maximum extend at energy where cooling " time meets age ● Ee = 4 TeV, B ≈12 μG (BX-rays ≈5 μG) → nebula becomes smaller with energy ➲ advection So%th!& South!' → nebula confined by ISM δ 10-1 EDGE (0 → nebula even smaller than for diffusion EDGE δ(1 Fit!&nal sis & ➲ energy-dependent morphology allows F#t!&nal sis B )#+%s#on the study of the particle transport Advection → more prominent at larger distance from 10-1 1 10 pulsar Energy!TeV Nukri Komin 9th International Fermi Symposium (2021) 9 TeV J2032+4130 VERITAS ➲ first unidentified and extended TeV source → HEGRA [A&A, v.431, p.197-202 (2005)] → Whipple [A&A, v.423, p.415-419 (2004)] → MAGIC [ApJL, Volume 675, Issue 1, pp. L25 (2008)] → VERITAS [ApJ, Volume 783, Issue 1, article id. 16, 9 pp. (2014)] ➲ PSR J2032+4127 → Ė = 1.5×1035 erg/s, age 2×105 years, distance 1.3 kpc ➲ nebula → TeV extension 9.5’ × 4.0’ (3.6 pc × 1.5 pc), L ~ 0.3% Ė → X-ray extension 12’ → good PWN candidate ➲ binary system on 50-years orbit → detected at periastron by VERITAS and MAGIC ● [ApJL, Volume 867, Issue 1, article id. L19, 8 pp. (2018)] → orbit < 200 AU MAGIC → binary system inside a PWN (?) Nukri Komin 9th International Fermi Symposium (2021) 10 TeV PWN Population 20 PSRs > 1034 erg/s/kpc 2 Randomised PSRs > 1034 erg/s/kpc 2 15 N 10 5 ➲ PWN in the H.E.S.S. Galactic Plane Survey 0 0.0 0.5 1.0 1.5 2.0 → [A&A, Volume 612, id.A2, 25] Squared Angular Distance PSR-TeV [deg 2] 28 34 2 → 140 PSRs 10 - 10 erg/s/kpc correlation between pulsar and TeV emission Randomised PSRs 1028 - 1034 erg/s/kpc 2 for Ė/d2 > 1034 erg/s/kpc2 120 100 80 → 14 firmly identified PWN N 60 → 18 PWN candidates 40 20 0 0.0 0.5 1.0 1.5 2.0 Squared Angular Distance PSR-TeV [deg 2] Nukri Komin 9th International Fermi Symposium (2021) 11 TeV PWN Population r yr ky ➲ -11 1 k 0 young, high-Ė pulsars 10 Kes 75 1 MSH 15-52 yr ➲ exception -12 0 k 10 10 Crab Nebula CTA 1 → PSR B1742−30 3C 58 r ] Vela X ky 1 -13 00 − 10 J1825-137 10 33 s N157B ● Ė = 8.5×10 erg/s s [ ● 5 e τ = 5.5×10 years t -14 s a 10 / g R r e ● 9 d = 200 pc n 3 0 w 1 o -15 → d 10 2 candidate TeV sources - n i ● p very small: 0.2°, 0.06° S -16 /s 10 g r ● e unlikely PWN candidates 7 3 Firm identifications 0 1 -17 Candidate PWNe 10 /s /s g g PWNe outside HGPS r r e e 5 3 3 3 ATNF pulsars 0 0 10 -18 1 1 10 -2 10 -1 10 0 10 1 Period [s] Nukri Komin 9th International Fermi Symposium (2021) 12 TeV PWN Population 10 2 ➲ efficiency: Firm identifications 10 1 Candidate PWNe PWNe outside HGPS Lim its → 0 Ė of pulsar at present time 10 Varied Model ˙ E / V Baseline Model → e L1-10TeV from electrons injected over T -1 0 1 10 − J1825-137 life time of pulsar 1 L y -2 c 10 ➲ efficiency grows with age n e MSH 15-52 i c i N157B CTA 1 f f -3 Kes 75 e 10 V e T -4 Vela X 10 Crab Nebula 10 -5 3C 58 10 -6 10 0 10 1 10 2 Characteristic age τc [kyr] Nukri Komin 9th International Fermi Symposium (2021) 13 TeV PWN Population ➲ offset of pulsar from TeV 10 2 emission centroid J1825-137 ➲ increases with age N157B 10 1 ] → proper motion of pulsar c MSH 15-52 CTA 1 p [ t Kes 75 3C 58 Vela X → e inhomogeneous medium leads to s f f o 0 asymmetric (“crushed”) PWN 10 r Crab Nebula a s l u P Firm identifications Candidate PWNe -1 10 PWNe outside HGPS Min. offset (0.0056 deg) at 5.1 kpc Max. offset (0.5 deg) at 5.1 kpc 500 km /s 10 -2 10 0 10 1 10 2 Characteristic age τc [kyr] Nukri Komin 9th International Fermi Symposium (2021) 14 TeV PWN Population Firm identifications 10 3 ➲ extension of nebula Candidate PWNe PWNe outside HGPS increases with age Varied Model Baseline Model ] c p 2 N157B [ 10 N W P R J1825-137 n o i s n e MSH 15-52 t 1 x 10 e CTA 1 V 3C 58 e Crab Nebula T Kes 75 Vela X on teracti hock in n rse s o reve si n a 0 p 10 x e e e fr 10 0 10 1 10 2 Characteristic age τc [kyr] Nukri Komin 9th International Fermi Symposium (2021) 15 Composite Supernova Remnants ➲ radio/X-rays: PWN and SNR shell visible ➲ HESS J1554–550 → pulsar not identified Chandra X-rays → TeV emission smaller then shall [Temim et al., ApJ 2015, 808, 100] → most likely PWN emission ➲ HESS J1119–614 → PSR J1119−6127, Ė = 2.3×1036 erg/s → d = 8.4 ± 0.4 kpc → emission from PWN or shell? Nukri Komin 9th International Fermi Symposium (2021) 16 Supernova Remnants and Cosmic Rays up to 1015 eV ➲ Are SNRs the sources of Galactic CRs (protons) up to 1015 eV? → is the emission hadronic? → what is the cut-off of the spectrum? AB IC 443 W44 10-10 10-10 ) ) 1 1 - - s s / / - - m m c c ! ! g g r -11 r -111 e 10 e 10 ( ( ! ! E E d d 1 1 0 0 d Best-fit!3ro4en!5o6er la6 d / / Best-fit!3ro4en!5o6er la6 Ferm#-7&T E VE"8T&S!( ) E Ferm#-7&T -1/ M&*8C!( ) -1/ &*87E!( ) 10 &*87E!( ) 10 π0-deca π0-deca Bremsstrahl%ng Bremsstrahl%ng Bremsstrahl%ng!6#th!'rea4 Bremsstrahl%ng!6#th!Brea4 10- 10.
Load more

Recommended publications
  • Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396
    Chandra Detection of a Pulsar Wind Nebula Associated With Supernova Remnant 3C 396 C.M. Olbert',2, J.W. Keohane'l2v3, K.A. Arnaud4, K.K. Dyer5, S.P. Reynolds', S. Safi-Harb7 ABSTRACT We present a 100 ks observation of the Galactic supernova remnant 3C396 (G39.2-0.3) with the Chandra X-Ray Observatory that we compare to a 20cm map of the remnant from the Verp Large Array'. In the Chandra images, a non- thermal nebula containing an embedded pointlike source is apparent near the center of the remnant which we interpret as a synchrotron pulsar wind nebula surrounding a yet undetected pulsar. From the 2-10 keV spectrum for the nebula (NH = 5.3 f 0.9 x cm-2, r=1.5&0.3) we derive an unabsorbed X-ray flux of SZ=1.62x lo-'* ergcmV2s-l, and from this we estimate the spin-down power of the neutron star to be fi = 7.2 x ergs-'. The central nebula is morphologi- cally complex, showing bent, extended structure. The radio and X-ray shells of the remnant correlate poorly on large scales, particularly on the eastern half of the remnant, which appears very faint in X-ray images. At both radio and X-ray wavelengths the western half of the remnant is substantially brighter than the east. Subject headings: ISM: individual (3C396 / G39.2-0.3) - stars: neutron - pulsars: general - supernova remnants lNorth Carolina School of Science and Mathematics, 1219 Broad St., Durham, NC 27705 2Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599 3Current Address: SIRTF Science Center, California Institute of Technology, MS 220-6, 1200 East Cali- fornia Boulevard, Pasedena, CA 91125 *Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 5National Radio Astronomy Observatory, P.O.
    [Show full text]
  • Exploring CTA Science with Ted and Friends - Activities
    Exploring CTA Science with Ted and Friends - Activities This handbook proposes questions and exercises for educators related to the animated series “Exploring CTA Science with Ted and Friends.” The goal is to reinforce the concepts the students learn in each episode about high-energy astrophysics and the future gamma-ray observatory, the Cherenkov Telescope Array (CTA), as well as to develop their scientific thinking and logic. The questions are divided according to each episode - we recommend educators to perform these activities following each episode in order to consolidate new ideas before staring the next episode. Age range: 5-11 years Supplementary material: https://www.cta-observatory.org/outreach-education/ Questions? Contact CTAO Outreach and Education Coordinator, Alba Fernández-Barral ([email protected]) Exploring CTA Science with Ted and Friends EPISODE 1: “CTA: Searching the Skies” How many CTA telescopes will be located around the world? More than 100 (Note for educators: specifically, 118 – 19 in La Palma, Spain, and 99 near Paranal, Chile). Where are they going to be located? One group will be in Chile (South America) while the other will be in La Palma (a Spanish island in the Canary Islands, off the coast of west Africa). What do CTA telescopes search for? They search the sky for gamma rays. What are gamma rays? Gamma rays are like X-rays, which are used to see human bones in the hospitals, but much more energetic (Note for educators: gamma rays are the most energetic light -electromagnetic radiation- that exists in the Universe. Light can be classified according to its energy, which is known as the electromagnetic spectrum.
    [Show full text]
  • (NASA/Chandra X-Ray Image) Type Ia Supernova Remnant – Thermonuclear Explosion of a White Dwarf
    Stellar Evolution Card Set Description and Links 1. Tycho’s SNR (NASA/Chandra X-ray image) Type Ia supernova remnant – thermonuclear explosion of a white dwarf http://chandra.harvard.edu/photo/2011/tycho2/ 2. Protostar formation (NASA/JPL/Caltech/Spitzer/R. Hurt illustration) A young star/protostar forming within a cloud of gas and dust http://www.spitzer.caltech.edu/images/1852-ssc2007-14d-Planet-Forming-Disk- Around-a-Baby-Star 3. The Crab Nebula (NASA/Chandra X-ray/Hubble optical/Spitzer IR composite image) A type II supernova remnant with a millisecond pulsar stellar core http://chandra.harvard.edu/photo/2009/crab/ 4. Cygnus X-1 (NASA/Chandra/M Weiss illustration) A stellar mass black hole in an X-ray binary system with a main sequence companion star http://chandra.harvard.edu/photo/2011/cygx1/ 5. White dwarf with red giant companion star (ESO/M. Kornmesser illustration/video) A white dwarf accreting material from a red giant companion could result in a Type Ia supernova http://www.eso.org/public/videos/eso0943b/ 6. Eight Burst Nebula (NASA/Hubble optical image) A planetary nebula with a white dwarf and companion star binary system in its center http://apod.nasa.gov/apod/ap150607.html 7. The Carina Nebula star-formation complex (NASA/Hubble optical image) A massive and active star formation region with newly forming protostars and stars http://www.spacetelescope.org/images/heic0707b/ 8. NGC 6826 (Chandra X-ray/Hubble optical composite image) A planetary nebula with a white dwarf stellar core in its center http://chandra.harvard.edu/photo/2012/pne/ 9.
    [Show full text]
  • Repeating Fast Radio Bursts Caused by Small Bodies Orbiting a Pulsar Or a Magnetar Fabrice Mottez, Philippe Zarka, Guillaume Voisin
    Repeating fast radio bursts caused by small bodies orbiting a pulsar or a magnetar Fabrice Mottez, Philippe Zarka, Guillaume Voisin To cite this version: Fabrice Mottez, Philippe Zarka, Guillaume Voisin. Repeating fast radio bursts caused by small bodies orbiting a pulsar or a magnetar. Astronomy and Astrophysics - A&A, EDP Sciences, 2020. hal- 02490705v3 HAL Id: hal-02490705 https://hal.archives-ouvertes.fr/hal-02490705v3 Submitted on 3 Jul 2020 (v3), last revised 2 Dec 2020 (v4) HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astronomy & Astrophysics manuscript no. 2020˙FRB˙small˙bodies˙revision˙3-GV-PZ˙referee c ESO 2020 July 3, 2020 Repeating fast radio bursts caused by small bodies orbiting a pulsar or a magnetar Fabrice Mottez1, Philippe Zarka2, Guillaume Voisin3,1 1 LUTH, Observatoire de Paris, PSL Research University, CNRS, Universit´ede Paris, 5 place Jules Janssen, 92190 Meudon, France 2 LESIA, Observatoire de Paris, PSL Research University, CNRS, Universit´ede Paris, Sorbonne Universit´e, 5 place Jules Janssen, 92190 Meudon, France. 3 Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester, Manchester M19 9PL, UK July 3, 2020 ABSTRACT Context.
    [Show full text]
  • Study of Pulsar Wind Nebulae in Very-High-Energy Gamma-Rays with H.E.S.S
    Study of Pulsar Wind Nebulae in Very-High-Energy gamma-rays with H.E.S.S. Michelle Tsirou To cite this version: Michelle Tsirou. Study of Pulsar Wind Nebulae in Very-High-Energy gamma-rays with H.E.S.S.. As- trophysics [astro-ph]. Université Montpellier, 2019. English. NNT : 2019MONTS096. tel-02493959 HAL Id: tel-02493959 https://tel.archives-ouvertes.fr/tel-02493959 Submitted on 28 Feb 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. THÈSE POUR OBTENIR LE GRADE DE DOCTEUR DE L’UNIVERSITÉ DE MONTPELLIER En Astrophysiques École doctorale I2S Unité de recherche UMR 5299 Study of Pulsar Wind Nebulae in Very-High-Energy gamma-rays with H.E.S.S. Présentée par Michelle TSIROU Le 17 octobre 2019 Sous la direction de Yves A. GALLANT Devant le jury composé de Elena AMATO, Chercheur, INAF - Acetri Rapporteur Arache DJANNATI-ATAȈ, Directeur de recherche, APC - Paris Examinateur Yves GALLANT, Directeur de recherche, LUPM - Montpellier Directeur de thèse Marianne LEMOINE-GOUMARD, Chargée de recherche, CENBG - Bordeaux Rapporteur Alexandre MARCOWITH, Directeur de recherche, LUPM - Montpellier Président du jury Study of Pulsar Wind Nebulae in Very-High-Energy gamma-rays with H.E.S.S.1 Michelle Tsirou 1High Energy Stereoscopic System To my former and subsequent selves, may this wrenched duality amalgamate ultimately.
    [Show full text]
  • Discovery of a Pulsar Wind Nebula Around PSR B0950+08
    Draft version May 13, 2020 Typeset using LATEX default style in AASTeX62 Discovery of a Pulsar Wind Nebula around B0950+08 with the ELWA Dilys Ruan1 | Advisor Gregory B. Taylor1 1Department of Physics and Astronomy, University of New Mexico, 210 Yale Blvd NE, Albuquerque, NM 87106, USA ABSTRACT With the Expanded Long Wavelength Array (ELWA) and pulsar binning techniques, we searched for off-pulse emission from PSR B0950+08 at 76 MHz. Previous studies suggest that off-pulse emission can be due to pulsar wind nebulae (PWNe) in younger pulsars. Other studies, such as that done by Basu et al. (2012), propose that in older pulsars this emission extends to some radius that is on the order of the light cylinder radius, and is magnetospheric in origin. Through imaging analysis we conclude that this older pulsar with a spin-down age of 17 Myr has a surrounding PWN, which is unexpected since as a pulsar ages its PWN spectrum is thought to shift from being synchrotron to inverse-Compton-scattering dominated. At 76 MHz, the average flux density of the off-pulse emission is 0:59 ± 0:16 Jy. The off-pulse emission from B0950+08 is ∼ 110 ± 17 arcseconds (0.14 ± 0.02 pc) in size, extending well-beyond the light cylinder diameter and ruling out a magnetospheric origin. Using data from our observation and the surveys VLSSr, TGSS, NVSS, FIRST, and VLASS, we have found that the spectral index for B0950+08 is about −1:36 ± 0:20, while the PWN's spectral index is steeper than −1:85 ± 0:45.
    [Show full text]
  • EM Counterparts from Long-Lived BNS Merger Remnants 2/8 Product of BNS Mergers
    THE UNIVERSITY IDENTITY The design of the Columbia identity incorporates the core elements of well- Pantone 286 thought-out branding: name, font, color, and visual mark. The logo was designed using the official University font, Trajan Pro, and features specific proportions of type height in relation to the visual mark. The official Colum- bia color is Columbia Blue, or Pantone Black 290. On a light color background, the logo can also be rendered in black, grey (60% black), Pantone 280, or Pantone 286; on a darker color background, the logo can be rendered in Pantone 290, 291, or 284, depending on which color works best with the overall design of your product, the media in which it will 4-color Process be4D.M.S reproduced, and its intendedIEGEL use.&R.CIOLFI 100% Cyan magnetosphere. Via dipole spin-down, the NS starts power- ing a highly relativistic, Poynting-flux dominated outflow of charged particles (mainly electrons and positrons; see Sec- 72% Magenta tion 4.2.1) or ‘pulsar wind’ at the expense of rotational en- ergy. This occurs at a time t = tpul,in and marks the beginning of Phase II. The pulsar wind inflates a PWN behind the less rapidly ex- panding ejecta, a plasma of electrons, positrons and photons EM counterparts from long-lived BNS (see Section 4.3.1 for a detailed discussion). As this PWN is highly overpressured with respect to the confining ejecta en- velope, it drives a strong hydrodynamical shock into the fluid, which heats up the material upstream of the shock and moves radially outward at relativistic speeds, thereby sweeping up all the material behind the shock front into a thin shell.
    [Show full text]
  • A Direct Localization of a Fast Radio Burst and Its Host
    UC Berkeley UC Berkeley Previously Published Works Title A direct localization of a fast radio burst and its host Permalink https://escholarship.org/uc/item/8131z4sx Journal Nature, 541(7635) ISSN 0028-0836 1476-4687 Authors Chatterjee, S. Law, C. J Wharton, R. S et al. Publication Date 2017-01-04 DOI 10.1038/nature20797 Peer reviewed eScholarship.org Powered by the California Digital Library University of California LETTER doi:10.1038/nature20797 A direct localization of a fast radio burst and its host S. Chatterjee1, C. J. Law2, R. S. Wharton1, S. Burke-Spolaor3,4,5, J. W. T. Hessels6,7, G. C. Bower8, J. M. Cordes1, S. P. Tendulkar9, C. G. Bassa6, P. Demorest3, B. J. Butler3, A. Seymour10, P. Scholz11, M. W. Abruzzo12, S. Bogdanov13, V. M. Kaspi9, A. Keimpema14, T. J. W. Lazio15, B. Marcote14, M. A. McLaughlin4,5, Z. Paragi14, S. M. Ransom16, M. Rupen11, L. G. Spitler17 & H. J. van Langevelde14,18 Fast radio bursts1,2 are astronomical radio flashes of unknown These bursts were initially detected with real-time de-dispersed imag- physical nature with durations of milliseconds. Their dispersive ing and confirmed by a beam-formed search (Fig. 1). From these arrival times suggest an extragalactic origin and imply radio detections, the average J2000 position of the burst source is right luminosities that are orders of magnitude larger than those of all ascension α =​ 05 h 31 min 58.70 s, declination δ = +33° 08 ′ 52.5 ″, with known short-duration radio transients3. So far all fast radio bursts a 1σ uncertainty of about 0.1″, consistent with the Arecibo localization 9 have been detected with large single-dish telescopes with arcminute but with three orders of magnitude better precision.
    [Show full text]
  • The Discovery of a Pulsar Wind Nebula Around the Magnetar Candidate Axp 1E1547.0-5408
    The Astrophysical Journal, 707:L148–L152, 2009 December 20 doi:10.1088/0004-637X/707/2/L148 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE DISCOVERY OF A PULSAR WIND NEBULA AROUND THE MAGNETAR CANDIDATE AXP 1E1547.0-5408 Jacco Vink1 and Aya Bamba2,3 1 Astronomical Institute, Utrecht University, P.O. Box 80000, 3508TA Utrecht, The Netherlands; [email protected] 2 Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland 3 ISAS/JAXA Department of High Energy Astrophysics, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan Received 2009 September 21; accepted 2009 November 17; published 2009 December 4 ABSTRACT We report the detection of extended emission around the anomalous X-ray pulsar 1E1547.0-5408 using archival data of the Chandra X-ray satellite. The extended emission consists of an inner part, with an extent of 45, and an outer part with an outer radius of 2.9, which coincides with a supernova remnant shell previously detected in the radio. We argue that the extended emission in the inner part is the result of a pulsar wind nebula (PWN), which would be the first detected PWN around a magnetar candidate. Its ratio of X-ray luminosity versus pulsar spin-down power is comparable to that of other young PWNe, but its X-ray spectrum is steeper than most PWNe. We discuss the importance of this source in the context of magnetar evolution. Key words: stars: magnetic fields – stars: neutron 1. INTRODUCTION ratesofmostAXPs/SGRs imply that they are young sources (typically <105 yr), only a few of them are associated with Among the various types of neutron stars, soft gamma-ray SNRs (Gaensler 2004).
    [Show full text]
  • Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB ∼ 180916.J0158+65
    UvA-DARE (Digital Academic Repository) Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB ∼ 180916.J0158+65 Scholz, P.; Cook, A.; Cruces, M.; Hessels, J.W.T.; Kaspi, V.M.; Majid, W.A.; Naidu, A.; Pearlman, A.B.; Spitler, L.G.; Bandura, K.M.; Bhardwaj, M.; Cassanelli, T.; Chawla, P.; Gaensler, B.M.; Good, D.C.; Josephy, A.; Karuppusamy, R.; Keimpema, A.; Kirichenko, A. Yu.; Kirsten, F.; Kocz, J.; Leung, C.; Marcote, B.; Masui, K.; Mena-Parra, J.; Merryfield, M.; Michilli, D.; Naudet, C.J.; Nimmo, K.; Pleunis, Z.; Prince, T.A.; Rafiei-Ravandi, M.; Rahman, M.; Shin, K.; Smith, K.M.; Stairs, I.H.; Tendulkar, S.P.; Vanderlinde, K. DOI 10.3847/1538-4357/abb1a8 Publication date 2020 Document Version Final published version Published in Astrophysical Journal Link to publication Citation for published version (APA): Scholz, P., Cook, A., Cruces, M., Hessels, J. W. T., Kaspi, V. M., Majid, W. A., Naidu, A., Pearlman, A. B., Spitler, L. G., Bandura, K. M., Bhardwaj, M., Cassanelli, T., Chawla, P., Gaensler, B. M., Good, D. C., Josephy, A., Karuppusamy, R., Keimpema, A., Kirichenko, A. Y., ... Vanderlinde, K. (2020). Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB ∼ 180916.J0158+65. Astrophysical Journal, 901(2), [165]. https://doi.org/10.3847/1538-4357/abb1a8 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons).
    [Show full text]
  • A Dispersion Excess from Pulsar Wind Nebulae and Supernova Remnants: Implications for Pulsars and Frbs S
    A&A 634, A105 (2020) https://doi.org/10.1051/0004-6361/201833376 Astronomy & © ESO 2020 Astrophysics A dispersion excess from pulsar wind nebulae and supernova remnants: Implications for pulsars and FRBs S. M. Straal1,2,3,4, L. Connor1,2, and J. van Leeuwen2,1 1 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, PO Box 94249, 1090 GE Amsterdam, The Netherlands e-mail: [email protected] 2 ASTRON, The Netherlands Institute for Radio Astronomy, PO Box 2, 7790 AA Dwingeloo, The Netherlands 3 NYU Abu Dhabi, PO Box 129188, Abu Dhabi, UAE 4 Center for Astro, Particle, and Planetary Physics (CAP3), NYU Abu Dhabi, PO Box 129188, Abu Dhabi, UAE Received 6 May 2018 / Accepted 13 January 2020 ABSTRACT Young pulsars and the pulsar wind nebulae (PWNe) or supernova remnants (SNRs) that surround them are some of the most dynamic and high-powered environments in our Universe. With the rise of more sensitive observations, the number of pulsar-SNR and PWN associations (hereafter, SNR/PWN) has increased, yet we do not understand to which extent this environment influences the pulsars’ impulsive radio signals. We studied the dispersive contribution of SNRs and PWNe on Galactic pulsars, and considered their relevance to fast radio bursts (FRBs) such as FRB 121102. We investigated the dispersion measure (DM) contribution of SNRs and PWNe by comparing the measured DMs of Galactic pulsars in a SNR/PWN to the DM expected only from the intervening interstellar electrons, using the NE2001 model. We find that a two-σ DM contribution of SNRs and PWNe to the pulsar signal exists, amounting to 21:1 ± 10:6 pc cm−3.
    [Show full text]
  • Grand Unification of Neutron Stars
    Grand Unification of Neutron Stars ∗ Victoria M. Kaspi ∗Department of Physics, McGill University, Montreal, Canada Submitted to Proceedings of the National Academy of Sciences of the United States of America The last decade has shown us that the observational properties of several different sub-classes of generally radio-quiet neutron neutron stars are remarkably diverse. From magnetars to rotating star have emerged in the Chandra era. The ‘isolated neu- radio transients, from radio pulsars to ‘isolated neutron stars,’ from tron stars’ (INS; poorly named as most RPPs are also iso- central compact objects to millisecond pulsars, observational mani- lated but are not ‘INSs’) have as defining properties quasi- festations of neutron stars are surprisingly varied, with most proper- thermal X-ray emission with relatively low X-ray luminosity, ties totally unpredicted. The challenge is to establish an overarching physical theory of neutron stars and their birth properties that can great proximity, lack of radio counterpart, and relatively long explain this great diversity. Here I survey the disparate neutron stars periodicities (P =3–11 s). classes, describe their properties, and highlight results made possi- Then there are the “drama queens” of the neutron-star ble by the Chandra X-ray Observatory, in celebration of its tenth population: the ‘magnetars’. Magnetars have as their true anniversary. Finally, I describe the current status of efforts at phys- defining properties occasional huge outbursts of X-rays and ical ‘grand unification’ of this wealth of observational phenomena, soft-gamma rays, as well as luminosities in quiescence that are and comment on possibilities for Chandra’s next decade in this field.
    [Show full text]