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REMNANT HUNTING a SEARCH for YOUNG SUPERNOVA REMNANTS DATE 04/06/2010 CLIENT VANESSA MOSS 1 Talk Structure

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REMNANT HUNTING a SEARCH for YOUNG SUPERNOVA REMNANTS DATE 04/06/2010 CLIENT VANESSA MOSS 1 Talk Structure PROJECT REMNANT HUNTING A SEARCH FOR YOUNG SUPERNOVA REMNANTS DATE 04/06/2010 CLIENT VANESSA MOSS 1 Talk Structure Background: What are supernova remnants? Are they missing? Why are they important? Algorithm: Automated approach to searching Results: Candidate overview Discussion: Investigation and completeness Conclusion 2 Introduction: what is a supernova remnant? Energetic remnant of an exploded star Core collapse (Type II/Ib/Ic): massive star (> 8M☼) Accretion (Type Ia): white dwarf detonation Supernova (SN) - optical/gamma rays/neutrinos SNR - radio/x-ray/gamma rays Complex multi-wavelength phenomena Animations: J. Tucciarone, G. Rieke 3 Introduction: what is a supernova remnant? Energetic remnant of an exploded star Core collapse (Type II/Ib/Ic): massive star (> 8M☼) Accretion (Type Ia): white dwarf detonation Supernova (SN) - optical/gamma rays/neutrinos SNR - radio/x-ray/gamma rays Complex multi-wavelength phenomena Animations: J. Tucciarone, G. Rieke 3 MULTI-WAVELENGTH IMAGES OF SNRS CLOCKWISE FROM TOP: CAS A, N63 A, SN 386 AD, N49, CRAB NEBULA, E0102-72.3 4 RADIO X-RAY OPTICAL MULTI-WAVELENGTH IMAGES OF SNRS CLOCKWISE FROM TOP: CAS A, N63 A, SN 386 AD, N49, CRAB NEBULA, E0102-72.3 4 Case of the missing Galactic supernova remnants Current predictions do not agree with observations Extragalactic SN rates: ~1 SN/century Historical SN rate: ~5 SN/century SNR lifetime ~105 years: 1000-5000 SNRs 274 known Galactic SNRs (Green catalogue, 2009) It is believed that many of the missing SNRs are within the detection limits of current telescopes 5 Young Galactic SNRs Discovery of young SNRs (whose SNe were missed) Cassiopeia A (~1650) G1.9+0.3 (~1860) ~20 young Galactic SNRs (< 2000 years old) Finding young SNRs will extend evolution theory at a stage not well understood 6 Radio/infrared anti-correlation SNRs are morphologically RADIO similar to HII regions COMPOSITE INFRARED HII regions emit most of their energy in infrared (IR) (Emerson, 1987) SNRs comparatively emit very weak IR (Fürst/ Broadbent, 1989) Very successful technique in discerning SNRs - but manually intensive! 7 HII region supernova remnant α = -0.1 α = -0.6 radio galaxy α = -0.8 http://www.cv.nrao.edu/course/astr534/FreeFreeEmission.html http://w0.sao.ru/cats/~satr/SNR/snr_map.html EXAMPLE RADIO SPECTRA Condon, 1992 PUPPIS SUPERNOVA REMNANT, MODEL HII REGION AND M82 RADIO GALAXY 8 SNR RADIO HII REGION INFRARED DATA SETS USED IN THIS PROJECT 2ND EPOCH MOLONGLO GALACTIC PLANE SURVEY/MIDCOURSE SPACE EXPERIMENT 9 Data sets: MGPS-2 and MSX RADIO INFRARED Radio Infrared Frequency: 843 MHz Frequency: 37 THz Wavelength: 36 cm Wavelength: 8 µm Longitude: 245º < l < 5º Longitude: 0 < l < 360º Latitude: | b | < 10º Latitude: | b | < 5º Resolution: 45” x 45” cosec|∂| Resolution: 18” x 18” Sensitivity: 1 mJy/beam Sensitivity: comparable 10 Algorithm Design Percentile clipping Normalisation Weighting equation Floodfill source-finder: Peak Ratio (% of peak) Point source filter 11 Future Improvements I optimised my algorithm by experimenting with parameters on a set of test fields Pixel-by-pixel: Resolution: convolve incomplete overlap IR data to match radio gives detections data resolution Extension: radio Point source filter: galaxies extended improved method of at small sizes filtering Artifacts: bright RMS: more local elongated spokes/ determination e.g. noise detected sextractor SELECTED CANDIDATES LEFT TO RIGHT: G311.4-0.1, G318.9-0.5, G325.0-0.3, G334.9-0.3, G345.1+0.1, G345.1-0.2 13 Multi-wavelength crossmatch (X-ray, gamma ray, radio) RADIO X-RAY No previous identifications as known objects Radio: 15 counterparts at 1.4 GHz (SGPS) X-rays: 7 possible matches (ASCA/XMM/ROSAT) Gamma rays: no clear matches in FERMI/HESS 14 G311.4-0.1: Young pulsar wind nebula (PWN)? PWN: nebula with an exciting pulsar core High-energy suggests potential PWN or AGN X-ray (BeppoSAX): extended source Gamma ray (INTEGRAL): point source This could be a very young SNR! BeppoSAX image: R. Landi 15 Completeness: a simulated SNR distribution Model distribution of SNRs: to obtain an idea of completeness and interpret known distribution Statistical: dgc, øgc, z, tyrs (uniform) Physical: rpc (2 stage model) We can then derive observables R FREE EXPANSION SLOWING EXPANSION 16 SIMULATED DISTRIBUTION VS. KNOWN DISTRIBUTION INCLUDING DISTRIBUTION, VIEW FROM EARTH AND OBSERVABLES (SIMULATED/KNOWN) 17 MGPS-2 ASKAP Instrument Type Source Minimum 120” 30” Angular Size # SNRs 27±5 34±6 < 5’ (res.) # SNRs 1±1 3±2 < 5 pc (res.) # SNRs < 2000 yrs 4±2 10±3 (res.) Telescope images:ATNF/MOST website 18 The Significance of Higher Resolution (ASKAP) MODEL SNR MGPS-2 ASKAP My analysis of search completeness highlights the importance of future radio surveys MGPS-2 represents the resolving power of the current generation of telescopes ASKAP/SKA will resolve smaller, further objects 19 Conclusions We have identified 17 promising young SNR candidates including a potentially young PWN Future observations with ATCA, SKAMP-2 and SWIFT will help better characterise candidates My algorithm encoded the human approach in a systematic and easily repeatable way Future radio surveys will overcome selection effects Finding more young SNRs is the missing link in the crucial transition stage between SN and SNR This will help answer many longstanding questions! 20 G287.5-0.4 G305.4-0.7 G345.1+0.1 THANK YOU! G345.1-0.2 Questions? G311.4-0.1 G341.5-0.4 G318.9-0.5 G342.4+2.2 G320.0+0.2 G334.9-0.3 G325.0-0.3 G338.5+2.7 G338.6+0.1 G327.2+0.2 G336.1+0.4 G331.3+0.2 G340.4+0.9 21.
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