Supernova Remnants and Pulsar Wind Nebulae observed in TeV γ rays

Transcription

1 Supernova Remnants and Pulsar Wind Nebulae observed in TeV γ rays NOW 2014 Conca Specchiulla, Sept 7-14, 2014 Kathrin Valerius Erlangen Centre for Astroparticle Physics Univ. Erlangen-Nürnberg KCETA Karlsruhe Institute of Technology

2 Particle acceleration by stellar remnants Gamma-ray astronomy at energies ~100 MeV to ~10 TeV: rich evidence of particle acceleration in... supernova remnants pulsar wind nebulae SN 1006 Powered by explosion energy Crab Nebula young and rejuvenated pulsars talk by F. Calore pulsar rotation strong EM fields; accretion shocked wind polar cap, slot gap? few 10 kyr few 100 kyr Myr Acceleration at shock front Time scale after death of star few kyr 2 Adapted from F. Acero

3 Particle acceleration by stellar remnants Gamma-ray astronomy at energies ~100 MeV to ~10 TeV: rich evidence of particle acceleration in... supernova remnants SN 1006 pulsar wind nebulae young and rejuvenated pulsars talk by F. Calore Crab Nebula Major Galactic TeV γ-ray source classes: Important Fermi source class 5 shell-type, 9 interacting SNRs, 33 PWNe Flux and composition (hadr./e±?) Max. energy (~1 PeV?) of accelerated particles? Release & acceleration? Contribution to diffuse γ flux? 3

4 Supernova remnants W kyr Young SNRs Older SNRs Efficient particle acceleration in the shell Spectral features well reproduced by mixed hadr./lept. models SN kyr Hadronic scenario favoured Electron acceleration less efficient π0 2γ enhanced by mol. clouds: - interaction w/ shell or - illumination by escaping CR flux H.E.S.S. coll., Acero et al. (2010) Multi-band X-ray image (Chandra; F. Winkler 2013) 4

5 Pulsar wind nebulae: synopsis A bubble of shocked relativistic particles, produced when a pulsar's relativistic wind interacts with its environment Crab Nebula (infrared, optical, X-rays) (Gaensler & Slane, 2006) radio IR vis X γ VHE γ 5

6 Pulsar wind nebulae: synopsis A bubble of shocked relativistic particles, produced when a pulsar's relativistic wind interacts with its environment Crab Nebula (infrared, optical, X-rays) RL ~ 106 m (Gaensler & Slane, 2006) Synchrotron wind termination shock pulsar wind magnetized outflow e± Inv. Compton e± non-thermal nebula e± e± e± RPWN ~ several pc e± Rwind ~ 0.1 pc 6

7 Pulsar wind nebulae: evolution I. Free expansion II. Reverse shock interaction 2-6 kyr III. Relic phase kyr? SNR pulsar PWN Simplest phase R ~ t6/5 Well studied, e.g. via Crab Kennel & Coroniti 1964, Martín ,... Depends on SNR development Oscillatory reverberations Analytically: R ~ t0.3 Only over-idealized and/or numerical models Even more influenced by SNR evolution, surroundings R ~?? Only case-by-case studies e.g. Swaluw , 2004,... 7 Adapted from S. Klepser

8 Pulsar wind nebulae in TeV γ rays Weakest TeV PWN ever detected: L >1TeV ~0.65% Crab, ~10-5 Ė Probably young (τc~5 kyr) pulsar TeV source coincides with pulsar, size not resolved (r < 4 pc) 5 ~2 NEW! pc excess/backgrd 3C 58 H.E.S.S. coll., Aharonian et al. (2006) Funk et al. (2008) MAGIC coll., Aleksić et al. (2014) Middle-aged (τc~21 kyr, r~35 pc) Crushed shape (asymmetry, displacement) Synchr. burn-off of high-e particles 8

9 PWN population study: aims Uniform analysis of TeV sources, selection and evaluation of candidates Upper limits for non-detections Observational data Link between properties of pulsar and TeV PWN? Benchmark common perceptions of PWN evolution Interpretation 9

10 PWN population study: ingredients (1) H.E.S.S. Galactic Plane Survey ~2800 h obs. of the inner Galaxy ( ) better than 2% Crab sensitivity discovery of ~60 new sources Position, size, F(1-10 TeV) (2) > 2000 pulsars (radio, X, γ) Position, P, Pdot, Edot, τc, d 10

11 PWN population study: methods Uniform analysis of TeV sources, selection and evaluation of candidates Upper limits for non-detections Link between properties of pulsar and TeV PWN? Benchmark common perceptions of PWN evolution Association & selection of candidates HGPS + ATNF catalogs (w/o SNR, GC Binaries, AGN) e PWN n w o kn not in HGPS, from TeVCat TeVCat online catalog of ~150 VHE γ-ray sources HGPS source + matching PSR no TeV dete ction Previously associated Externals New candidates Pulsars for limits 11

12 PWN population study: methods Uniform analysis of TeV sources, selection and evaluation of candidates Upper limits for non-detections Association & selection of candidates HGPS + ATNF catalogs (w/o SNR, GC Binaries, AGN) e PWN n w o kn not in HGPS, from TeVCat TeVCat online catalog of ~150 VHE γ-ray sources HGPS source + matching PSR no TeV dete ction Link between properties of pulsar and TeV PWN? Benchmark common perceptions of PWN evolution Population plots relating PSR to TeV properties Previously associated Externals New candidates Pulsars for limits Common trends? Theory expectations? Simple leptonic modeling Plausibility of candidates 12

13 Correlation of TeV sources and pulsars Ndetected/Nall candidate selection (a) energy-dep. detection fraction (b) angular separation criterion candidate selection High-Edot pulsars: TeV signal within ~0.5 log10 (Ė) No correlation beyond chance coincidences below ~1035 erg/s Klepser et al., arxiv: Carrigan et al., arxiv:

14 Selection of PWN candidates S. Klepser et al., arxiv:1307:7905 Preliminary Most PWNe likely in reverse shock interaction phase Candidates: more evolved 14

15 How far can we reach out? Preliminary PWNe trace close-by spiral arms Average distance: ~5 kpc Exposure covers ~1/4 of the Milky Way 1% 10% of Crab luminosity > 1 TeV Graphic: C. Deil, S. Klepser 15

16 Evolutionary trends S. Klepser et al., arxiv:1307:7905 Size RPWN RPWN ~t0.3 as a rough guideline, but large scatter due to surrounding medium or SNR interaction Good for evaluating candidates Efficiency L1-10TeV/Ė Compares accumulated e± population with momentary energy output of pulsar Time-dependent one-zone model based on M. Mayer et al., arxiv:1202:1455 (added free expansion phase) 16

17 Evolutionary trends S. Klepser et al., arxiv:1307:7905 Size RPWN Efficiency L1-10TeV/Ė Upper limits RPWN ~t0.3 as a rough guideline, but large scatter due to surrounding medium or SNR interaction Good for evaluating candidates Compares accumulated e± population with momentary energy output of pulsar Time-dependent one-zone model based on M. Mayer et al., arxiv:1202:1455 (added free expansion phase) 17

18 ter s ry a clu n bi Summary & outlook SNR (shell) SNR (int.) PWN VHE γ-rays allow to study most powerful particle accelerators in the Galaxy Data quality & quantity supports cumulative studies: SNRs, PWNe UNID Composition of Gal. TeV sources tevcat.uchicago.edu PWN population: biggest (& rather diverse) Galactic source class Many UNID sources might be ageing PWNe Modeling: need better understanding of evolved PWNe in particular for the leap ahead with CTA 18

19 References Selection of recent reports on progress of Galactic TeV survey & source census: H.E.S.S. Galactic Plane Survey Carrigan et al., Charting the TeV Milky Way, arxiv: Carrigan et al., The H.E.S.S. Galactic Plane Survey, arxiv: PWN population study SNR population study Klepser et al., A population of Teraelectronvolt Pulsar Wind Nebulae in the H.E.S.S. Galactic Plane Survey, arxiv: Fernandez et al., Study of the Very High Energy emission from Supernova Remnants with H.E.S.S., arxiv: Future perspectives: 'CTA special edition', Astrop. Phys. 43 (2013) Aharonian, Gamma rays from supernova remnants, p. 71 Acero et al., Gamma-ray signatures of cosmic-ray acceleration, propagation, and confinement in the era of CTA, p. 276 de Ona Wilhelmi et al., Prospects for observations of pulsars and pulsar wind nebulae with CTA, p

20 Supplementary slides 20

21 Galactic Sources of VHE γ rays ~90 sources of VHE γ rays (E > 100 GeV) in the Milky Way known today*: Different origin of γ-ray emission Dominant source class 26 9 How many are ancient PWNe? *) tevcat.uchicago.edu, Aug

22 The TeV gamma-ray sky today 22

23 Old PWNe as unidentified VHE γ-ray sources? Comparison of X-ray and VHE γ-ray luminosities for several identified PWNe Time-dependent leptonic model of broad-band emission for a generic PWN Mattana et al. (2009) M. J. Mayer, J. Brucker, I. Jung, KV, C. Stegmann, arxiv:

24 PWN population study: potential selection bias Closer objects tend to have larger lower efficiencies and smaller extensions Far away sources need to be more efficient in order to get detected Clipping of large, nearby sources due to limited field of view? Far, small sources cannot be resolved upper limits on extension S. Klepser et al., ICRC'13 24

25 Why study (multi-wavelength) properties of PWNe? We can learn something about the pulsar: spin-down characteristics/history, proper motion, the pulsar wind: composition, energetics, geometry, termination shock, the ambient medium: local density/homogeneity, magnetic field, Increasing sample of detected PWNe allows to identify general properties investigate various evolutionary stages Multi-wavelength observational data + Detailed modeling 25

26 Imaging Atmospheric Cherenkov Technique for ground-based gamma-ray detection (Eγ ~ 100 GeV 10 TeV) Photon Particle shower lig ht ~ 10 km Ch ere n ko v ~ 10 km ~ 120 m Shower image: Intensity energy Orientation direction Shape primary particle Air shower observed simultaneously by multiple telescopes 26

27 What is a Pulsar Wind Nebula? Aharonian, Bogovalov & Khangulyan (2012) 27

28 Pulsar Wind Nebulae: Overview Hydrodynamical simulations, Van der Swaluw, Downes & Keegan (2004) 28

29 Time-dependent leptonic model of non-thermal emission from PWNe Characteristic age and spin-down timescale Time evolution of energy output and magn. field (see Zhang et al., 2008): Cooling processes (see Zhang et al., 2008): PWN evolution (Gaensler & Slane, 2006): free expansion after RS interaction 29

30 Dissecting the broad-band SED into contributions from different epochs Generic middle-aged PWN: P0 = 30 ms, P = 100 ms B0 = 50 µg Ė = erg/s Mayer, Brucker, Holler, Jung, KV, Stegmann: Predicting the X-ray flux of evolved pulsar wind nebulae based on VHE gamma-ray observations, arxiv:1202:

31 Supernova Remnants Paradigm of galactic cosmic rays (E 1015 ev): young SNRs as acceleration sites ('PeVatrons'?) p (e±) Both high-energy hadrons (p, nuclei) and leptons can be present VHE γ-ray production via π0 decay or inverse Compton scattering γ SN 1006 TeV γ-rays coincident with non-thermal X-rays from the shell Spectral energy distribution well reproduced by mixed hadronic-leptonic model H.E.S.S. coll., Acero et al. (2010) Multi-band X-ray image (Chandra; F. Winkler 2013) 31