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Radio Supernovae

Radio Supernovae. Rob Beswick (JBO, University of Manchester UK). Outline. Introduction to supernovae Optical detection and monitoring Supernovae taxonomy Detected of radio supernovae Radio detection and monitoring of SNe Types of supernovae detected

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Radio Supernovae

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  1. Radio Supernovae Rob Beswick (JBO, University of Manchester UK)

  2. Outline • Introduction to supernovae • Optical detection and monitoring • Supernovae taxonomy • Detected of radio supernovae • Radio detection and monitoring of SNe • Types of supernovae detected • SNe rates (eg. M82 – see Tom Muxlow’s review) • Radio light curves (case studies 2004dj, 2004et etc etc ) • Determining progenitor properties • Radio imaging of supernova and remnants • VLBI, MERLIN etc (M82, SN1986J, SN1993J, SN2004et etc) • Radio supernovae and supernova remnants in other starbursts • Arp220, NGC7674-SN etc etc.. • Summary/ future work in the field 8th EVN symposium Toruń 2006

  3. Type IIb: CORE COLLAPSE Most H removed during evolution. Late-time spectra similar to Type Ib/c TYPE Ia: Thought to originate from thermonuclear deflagration on an accreting white dwarf. Si Type IIb Type I Type Ia Eg. 1993J Early optical spectra H He dominant Si, He Type IIL: CORE COLLAPSE Optical light-curve shows a linear decline in luminosity. Hydrogen? TYPE Ib & Ic: Core Collapse Outer layers stripped by pre-supernova winds or binary interactions. Ib H mantle removed Ic H & He mantle removed Type IIL Type Ib H dominant H Eg. 1979C Si, He Type IIP: CORE COLLAPSE Optical light-curve Shows little or no decline Forming a plateau lasting ~2-3months. Type II Type IIP H dominant Type Ic Eg. 1987A Basic supernovae taxonomy 8th EVN symposium Toruń 2006

  4. Supernovaetaxonomy • Classification is based on optical properties:- • TWO basic types (type I & II) • Type I  H poor, further sub-divided • Type Ia  Silicon rich • Type Ib  Si poor, He rich • Type Ic  Si poor, He rich • Type II  H rich, further sub-divided • Type IIb  He dominant  evolve to type Ib/c at late time • Type IIL  H dominant, optical light-curve has a linear decay • Type IIP  H dominant, optical light-curve has a Plateau followed by a decay • Type IIn  narrow emission lines (e.g. 1988Z) • +++ type IIpec……… 8th EVN symposium Toruń 2006

  5. Optical Supernovae • Number of optical supernovae • Since 1950 over 3500 (3412 Jan 1950- Jan 2006) optical SNe have been discovered. • 2006 - 199+ So far this year (up to SN2006gr reported on 21st Sept) • 2005 - 367 (149 brighter than 18th mag) • 2004 - 249 (148 >18th mag) • 2003 - 338 (148 >18th mag) • 2002 - 334 (122 >18th mag) • 2001 - 307 (94 >18th mag) 8th EVN symposium Toruń 2006

  6. 1998 2000 Radio detection of SNe • Whilst several hundred SNe are detected each year at optical wavelengths relatively few are detected at radio frequencies. • Detections from few dozen SNe. • ‘All’ radio detected SNe are core collapse (Type II, Type Ib/c etc) • Type 1a  No radio detections with current instruments (>30 upper limits) (see Panagia et al 2006, ApJ, 644, 369) • Even fewer have been resolved by radio observations (so every VLBI observation is of great value)…. • However some radio supernovae have not been detected in optical bands (e.g. in NGC7469 – Colina et al 2001, those in Arp220 – Smith et al., Lonsdale et al, Parra et al..) 8th EVN symposium Toruń 2006

  7. Radio emission from SNe • Thermonuclear: • Type Ia: SNe are NOT radio emitters (at least at the level of current instruments) • Core Collapse: • Type Ib/c: SNe are radio luminous. • Generally have steep spectra (< -1: S) • Fast turn-on/turn-off, peak @6cm near optical maximum. • Type II: large range in radio luminosities. • Relatively slow turn-on/turn-off, radio peak often significantly after optical peak. 8th EVN symposium Toruń 2006

  8. 1993J Radio ‘light’-curves • Multi-frequency observations of the radio ‘light-curves’ of SNe can be understood as a blastwave interacting with the surrounding circumstellar medium. Detailed modelling of radio light-curves allows estimations of the physical conditions of the CSM (see Weiler et al 2002). 8th EVN symposium Toruń 2006

  9. 10” telescope in Manchester city centre! (Argo et al) An example Radio ‘light’-curves: 2004dj • 2004dj was the brightest visual SNe for over a decade. • July 31st 2004 • In NGC2403 • D=3.2 kpc • Peak mag = 11.2 • Type IIP • Progenitor 8th EVN symposium Toruń 2006

  10. 8.4GHz 8.4GHz 5GHz 5GHz 1.4GHz 1.4GHz Single baseline 4.9GHz radio ‘maps’ An example Radio ‘light’-curves: 2004dj • 2004dj was detected with a single MERLIN baseline (Ca-De) and the VLA a few days after the optical discovery • V. Low luminosity radio emission • Intensive monitoring  Well sampled radio light curve • 2004dj MERLIN & VLA monitoring • Prompt monitoring caught 5GHz radio peak ~ 15 days after optical detection. • One of only a handful of Type-IIP SNe detected in the radio (1987A, 1999em, 2004et – see latter) • One of the least luminous radio SNe detected (~21018 WHz-1). (Beswick et al., ’05, Argo PhD, ‘06) • Modelling of the radio light-curve  detonation date after 11th July. • Optical spectra  ~14th July. 8th EVN symposium Toruń 2006

  11. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612++) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J (Bartel et al .. etc) • SN 1993J (Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et (Marti-Vidal, Marcaide et al..) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted.) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  12. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J (Bartel et al .. etc) • SN 1993J (Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et (Marti-Vidal, Marcaide et al..) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted.) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  13. M82 Supernova remnants • >50compact sources discovered in M82 • All resolved with MERLIN &/or VLBI • Most are SNR– although ~16 are HII regions 8th EVN symposium Toruń 2006

  14. Global VLBI 18cm images 1998 2001 2005 1986 1997 ~20 years of ‘EVN-only’ images (15mas beam) 43.31+529 in M82 • Ongoing Monitoring of SNR in M82 • 43.31+592 Vexp ~9800kms-1 • In ‘near’ free-expansion • Infer 1 Supernova every ~15 years For next epoch (See Danielle Fenech’s Talk) 8th EVN symposium Toruń 2006

  15. Resolved by global VLBI @1.6GHz (3.3 mas beam) (From Danielle Fenech’s & Tom Muxlow’s talks yesterday) 41.95+575 in M82Supernovae? – Or something more exotic? • 41.95+575 • Most compact source in M82 • Bi-polar structure • SNR??? • Slow ‘Expansion’ rate Vexp~<1000-2000kms-1??? 8th EVN symposium Toruń 2006

  16. Yet More Sources in M82 • As we heard on Wednesday from Danielle Fenech recently combined 1.6GHz MERLIN+GVLBI detect and resolve many more SNR…. 8th EVN symposium Toruń 2006

  17. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J(Bartel et al .. etc) • SN 1993J (Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et (Marti-Vidal, Marcaide et al. in prep.) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  18. 5GHz 15GHz SN1986J in NGC891 • SN1986J in NGC891 (Bartel et al ’91, Bietenholz et al’ 04, Perez-Torres et al ’02 etc etc) • Type IIn, D~12Mpc. Radio luminous source • SN1986J in NGC891 (Bartel et al ’91, Bietenholz et al’ 04, Perez-Torres et al ’02 etc etc) • Type IIn, D~12Mpc. Radio luminous source • Bright expanding ring • Moderately strong deceleration • M=0.710.11 (Bartel et al) • Expansion velocity slowed to ~6000km/s at t=16yr compared to an initial extrapolated velocity ~20,000km/s • Although a far more mild deceleration is stated by Perez-Torres et al) • Central component • Inverted radio spectrum • (above ~10GHz) • Possibly indication of an • emerging pulsar nebular? • (Obs: Bietenholz et al., 2004, Sci., • Theory: Chevalier 1987, Nat) 8th EVN symposium Toruń 2006

  19. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J (Bartel et al ., ++ Perez-Torres ++ etc) • SN 1993J(Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et (Marti-Vidal, Marcaide et al. in prep.) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  20. VLBI imaging of 1993J • SN1993J in M81 (D=3.64Mpc) • At the time the brightest visual SNe since 1954D • Type II • Strong radio emitter • Resolved with VLBI in the first few months & imaged for the next decade. (Bartel et al 1994++, Marcaide et al 1995++) (Bartel et al. ) 8th EVN symposium Toruń 2006

  21. SN 1993J: Expansion Curve • Initial expansion ~2.4µarcsec/day • Vexp~ 15000 -> 17000 km/s • Where size goes as   tm (m~0.79 0.9) • Detection of break in expansion? • Now apparent self-similar deceleration (Marcaide et al ’06) • break at t=1550 days due to changes in changes in he absorption and magnetic fields (biasing the size measurements) 8th EVN symposium Toruń 2006

  22. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J (Bartel et al .. etc) • SN 1993J (Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et(Marti-Vidal, Marcaide et al..) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  23. Global VLBI @8.4GHz 20th Feb. 2005 (day 153) (Marti-Vidal et al., ) (Argo, PhD ’06) SN2004et in NGC6946 • Bright, nearby type II supernovae (mag 12) • Marginally resolved by global VLBI (measured diameter=0.5mas) 8th EVN symposium Toruń 2006

  24. These are the residuals for a fit of a simple point-like emitter to the visibilities (i.e., the source must contain some structure at the mas scale). Sfit = 0.65  0.03 mJy VLBI flux density = 0.83mJy VLA flux density (same epoch & freq) = 1.23mJy Global VLBI 8.4GHz image of SN2004et on Feb 20th 2005 (Marti-Vidal et al.,) These are the residuals for a fit with 2 point-like emitters. more flux density is recovered from this fit. Sfit1 = 0.57  0.05 mJy Sfit2 = 0.26  0.05 mJy Residual maps of SN2004et 8th EVN symposium Toruń 2006

  25. SN2004et in NGC6946 Results from fitted models to the radio emission from ‘04et Flux density from VLBI: 0.83 mJy, Flux density from VLA (same epoch and freq): 1.23 mJy (Marti-Vidal et al., ) 8th EVN symposium Toruń 2006

  26. Imaging radio supernovae • Resolved/partially resolved VLBI imaging of SNe • SNR in M82 (43.31+529, 41.95+575, 44.01+596 & 45.17+612) (Pedlar et al, 1999, McDonald et al 2002, Beswick et al., 2006, Fenech et al in prep) • SN 1979C (Bartel et al.. etc) • SN 1986J (Bartel et al .. etc) • SN 1993J (Marcaide et al.++, Bartel et al.++) • J103851+532927 in NGC 3310 (Argo, 2006 PhD) • SN 2001gd (Perez-Torres et al 2005) • SN 2004et (Marti-Vidal, Marcaide et al..) ++ other such as SN 2001em (Type Ib/c – Paragi et al 2005) • Others: • Arp220 - many SNe & SNR (Smith et al 1998, Lonsdale et al 2006, Parra et al. submitted etc) • NGC253 (LBA – Tingay 2004; Lenc & Tingay 2006) ++++ etc etc… 8th EVN symposium Toruń 2006

  27. SNe/SNR in Arp 220 • Arp220 – sensitive VLBI observations • New RSNe detected (See Rodrigo Parra’s Talk yesterday) • Many Radio supernova remnants and new supernovae • Highly optically extincted. THERE ARE MANY MORE RADIO SUPERNOVAE OUT THERE THAT ARE NEVER SEEN OPTICALLY…… 8th EVN symposium Toruń 2006

  28. Summary • Radio detections & light curves • Radio monitoring the light curves of SNe provides vital information about SNe progenitors and their environments • Can use number counts of SNe to calculate SFR and SNe…. • Relatively few optically reported SNe are detected at radio wavelengths • All detections so far are from core collapse SNe • VLBI imaging of young SNe provides a direct probe of the shockwave interaction with the circumstellar medium 8th EVN symposium Toruń 2006

  29. Summary 2 • Embedded deep within highly obscured starburst galaxies optical monitoring is not possible. • Eg Arp220, M82 radio supernovae & remnants etc.... • Great signposts of recent and ongoing star-formation… 8th EVN symposium Toruń 2006

  30. (Marcaide et al. ) (Bartel et al. ) VLBI imaging of 1993J: The Movies 8th EVN symposium Toruń 2006

  31. THE END 8th EVN symposium Toruń 2006

  32. THE END maybe…… 8th EVN symposium Toruń 2006

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