Remnants of Type Ia Supernovae

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1 Remnants of Type Ia Supernovae Brian J. Williams NPP Fellow NASA GSFC Collaborators: Steve Reynolds, Kazik Borkowski, John Blondin (NCSU), Rob Petre, Jack Hewitt (GSFC), Frank Winkler (Middlebury), Knox Long (STScI), Bill Blair (JHU), John Raymond (CfA), Parviz Ghavamian (Towson), Satoru Katsuda (RIKEN), Ravi Sankrit, Jeonghee Rho (NASA Ames) Chandra image of SN 1006

2 The Great Debate OR? AND? None of the above??? Single-degenerate scenario Double-degenerate scenario

3 The Great Debate OR? AND? None of the above??? Single-degenerate scenario Double-degenerate scenario

4 The Great Debate OR? AND? None of the above??? Single-degenerate scenario Double-degenerate scenario Not the only question about Type Ia SNe...

5 (Some) Open Questions: 1) What are the progenitors (SD vs. DD vs... other?) 2) In what sort of environments do SNIa explode? 3) What is the delay time from star formation to SN? 4) Are the explosions symmetric?

6 (Some) Open Questions: 1) What are the progenitors (SD vs. DD vs... other?) 2) In what sort of environments do SNIa explode? 3) What is the delay time from star formation to SN? 4) Are the explosions symmetric? 5) Do any of the answers to these questions provide constraints that we can observe?

7 SN 1006 The remnants of the historical* Type Ia SNe Tycho's SNR (1572) Kepler's SNR (1604) *historical = in the Milky Way, reasonable documentation of event RCW 86 (185)

8 SN ks Chandra observation in 2012 (PI - Frank Winkler) - X-rays nonthermal in NW and SE, thermal everywhere else - Thermal X-rays consistent with low-ionization state gas; mixture of shocked ejecta and ISM

9 SN ks Chandra observation in 2012 (PI - Frank Winkler) - X-rays nonthermal in NW and SE, thermal everywhere else O Ne Mg Si S - Thermal X-rays consistent with low-ionization state gas; mixture of shocked ejecta and ISM

10 SN ks Chandra observation in 2012 (PI - Frank Winkler) - X-rays nonthermal in NW and SE, thermal everywhere else O Ne Mg Si S - Thermal X-rays consistent with low-ionization state gas; mixture of shocked ejecta and ISM

11 - Often considered prototypical case of Type Ia SNR - High gal. latitude; nearby (2.2 kpc), very large (~30' diameter); low-absorption = well-studied - Very low density environment, uniform expansion(?) Chandra (2012) Hα (courtesy F. Winkler) Spitzer IR

12 - Often considered prototypical case of Type Ia SNR - High gal. latitude; nearby (2.2 kpc), very large (~30' diameter); low-absorption = well-studied - Very low density environment, uniform expansion(?) Chandra (2012) Hα (courtesy F. Winkler) Spitzer IR Chandra proper motions over 9- year baseline; known distance = shock velocity Winkler, BJW+, in prep.

13 - Often considered prototypical case of Type Ia SNR - High gal. latitude; nearby (2.2 kpc), very large (~30' diameter); low-absorption = well-studied - Very low density environment, uniform expansion(?) Chandra (2012) Hα (courtesy F. Winkler) Spitzer IR 5000 km/s (Katsuda+ 2009) 3000 km/s (Katsuda,...,BJW+ 2013) Chandra proper motions over 9- year baseline; known distance = shock velocity Winkler, BJW+, in prep.

14 - IR emission is sensitive function of post-shock density (more on this later) - IR spectrum implies postshock density = 1 cm -3 (Winkler, BJW+ 2013), consistent with optical measurement (Heng+ 2007) Spitzer IRS spectrum from NW filament of SN 1006

15 - IR emission is sensitive function of post-shock density (more on this later) - IR spectrum implies postshock density = 1 cm -3 (Winkler, BJW+ 2013), consistent with optical measurement (Heng+ 2007) Spitzer IRS spectrum from NW filament of SN 1006 Here be dragons denser ISM Perhaps nothing paradigm-shifting about SNIa, but means significant ISM density inhomogeneities exist on parsec scales, even 500 pc above Galactic plane

16 Asymmetric explosion? Winkler, BJW+, in prep. Equivalent width image of Silicon (1.8 kev)

17 Asymmetric explosion? Winkler, BJW+, in prep. Equivalent width image of Silicon (1.8 kev) Evidence of asymmetric explosions in other Ia SNRs (Kepler, G )...

18 Tycho's SNR - Remnant of SN 1572 (Shakespeare?) - X-rays dominated by ejecta in interior; synchrotron emission at edge (Badenes+ 2006) - Little to no thermal X-rays from forward-shocked medium (Hwang+ 2002) - Detected in GeV (Giordano+ 2012) and TeV (Acciari+ 2011) Chandra image

19 Tycho's SNR - Remnant of SN 1572 (Shakespeare?) - X-rays dominated by ejecta in interior; synchrotron emission at edge (Badenes+ 2006) - Little to no thermal X-rays from forward-shocked medium (Hwang+ 2002) - Detected in GeV (Giordano+ 2012) and TeV (Acciari+ 2011) Chandra image This makes the remnant look fairly round and symmetric...

20 Tycho's SNR - Remnant of SN 1572 (Shakespeare?) - X-rays dominated by ejecta in interior; synchrotron emission at edge (Badenes+ 2006) - Little to no thermal X-rays from forward-shocked medium (Hwang+ 2002) - Detected in GeV (Giordano+ 2012) and TeV (Acciari+ 2011) this does not. Chandra image This makes the remnant look fairly round and symmetric... Proper motions, averaged between radio (Reynoso 1997) and X-ray (Katsuda 2010) measurements, scaled to 2.3 kpc. Clearly some asymmetries here...

21 Tycho in the mid-ir Spitzer 24 micron Spitzer 70 micron Herschel 70 micron Herschel 100 micron Wise 12 micron 70, 24, 12

22 Tycho in the mid-ir Spitzer 24 micron Spitzer 70 micron Herschel 70 micron Herschel 100 micron Wise 12 micron 70, 24, 12

23 - IR emission from young SNRs comes from warm ISM dust, heated by post-shock plasma - IR flux ratio is diagnostic of dust temperature which is sensitive to plasma density Values are ratio of 70 µm to 24 µm flux

24 - IR emission from young SNRs comes from warm ISM dust, heated by post-shock plasma - IR flux ratio is diagnostic of dust temperature which is sensitive to plasma density IR observations are a density diagnostic for shocked ISM gas Values are ratio of 70 µm to 24 µm flux

26 - To first order, consistent with density gradient of factor of ~5 from NE to SW - These are normalized densities; absolute numbers depend slightly on grain composition assumed, but... - Overall densities quite low (n p ~0.2 cm -3 ), consistent with lack of thermal emission at shock front Density map of Tycho

27 - To first order, consistent with density gradient of factor of ~5 from NE to SW - These are normalized densities; absolute numbers depend slightly on grain composition assumed, but... - Overall densities quite low (n p ~0.2 cm -3 ), consistent with lack of thermal emission at shock front Density map of Tycho Can remnant still be round?

28 Yes. BJW+ 2013

29 Yes. BJW Tycho is not 1-D, and center of explosion is not at center of remnant...

30 BJW+ 2013

31 Companion searches should not be limited only to small regions at SNR center BJW+ 2013

32 Comparing results with 3D simulations of Warren & Blondin (2013), we CAN match evolutionary state of Tycho, but: 1) Larger distances (~3.5 kpc) are favored 2) Porous grain models work much better than compact grains 3) better proper motion measurements are needed! Companion searches should not be limited only to small regions at SNR center BJW D simulations at various evolutionary stages (Warren & Blondin 2013)

Kepler's SNR - Controversial origin for a while, now generally accepted as Type Ia (Reynolds+ 2007) - Distance not well known, could be 3-7 kpc (Sankrit+ 2005,

33 Kepler's SNR - Controversial origin for a while, now generally accepted as Type Ia (Reynolds+ 2007) - Distance not well known, could be 3-7 kpc (Sankrit+ 2005, Patnaude+ 2012) - Systemic velocity ~300 km/s - FS interacting with circumstellar material, not interstellar (Blair+ 1991)... after 400 years!? Chandra, Hubble, and Spitzer image

34 Wednesday s APOD

35 Summaries of some recent papers Spitzer 24 µm image Blair,...,BJW,...+ (2007) used IR observations to conclude that CSM in North is order of magnitude denser than in South

36 Summaries of some recent papers Spitzer 24 µm image Blair,...,BJW,...+ (2007) used IR observations to conclude that CSM in North is order of magnitude denser than in South Chiotellis find Kepler is consistent with a symbiotic binary progenitor (i.e. singledegenerate) of WD M sun AGB star, favor large (> 6 kpc) distance

37 Patnaude Interacting with slow (10-20 km/s) wind, mass loss rate > 4 x 10-6 M yr -1 - Low-density cavity near SN prior to explosion - Subenergetic explosions, large distances (> 7 kpc) required

- Burkey+ 2013 confirm that Kepler is most consistent with SD scenario - Spatial morphology explained by dense equatorial wind Patnaude+ 2012 - Interacting with slow (10-20 km/s) wind, mass loss rate

38 - Burkey confirm that Kepler is most consistent with SD scenario - Spatial morphology explained by dense equatorial wind Patnaude Interacting with slow (10-20 km/s) wind, mass loss rate > 4 x 10-6 M yr -1 - North/south density gradient explained by system's movement in northward direction - Low-density cavity near SN prior to explosion - Subenergetic explosions, large distances (> 7 kpc) required

39 Tsebrenko & Soker (2013) want coredegenerate scenario. and jets! See Tsebrenko poster and Soker talk.

40 Tsebrenko & Soker (2013) want coredegenerate scenario. and jets! See Tsebrenko poster and Soker talk.

5-14 μm - spectral map allows creation of data cube, where IR spectra can be

41 Back to the IR 3-color mosaic using Spitzer 24 µm, WISE 12 µm, Spitzer 8 µm - Full spectral map from μm, select regions mapped from μm - spectral map allows creation of data cube, where IR spectra can be extracted from any location in the remnant - Data cube created using IRS contributed software CUBISM (Smith+ 2007)

42 Kepler mid-ir spectroscopy BJW+ 2012

43 Kepler mid-ir spectroscopy BJW Strong 18 μm silicate features observed throughout, progenitor AGB must have been O-rich

44 Absorption cross-section for crystalline silicates (Fabien+ 2001) No evidence for strong spectral features from crystalline silicates, so mass loss rate of Kepler progenitor was <10-5 M sun yr -1 (Watson 2010). Patnaude want mass loss > 4 x (Possible crystalline silicates quickly amorphized in shock; need JWST res. to test)

45 Absorption cross-section for crystalline silicates (Fabien+ 2001) No evidence for strong spectral features from crystalline silicates, so mass loss rate of Kepler progenitor was <10-5 M sun yr -1 (Watson 2010). Patnaude want mass loss > 4 x (Possible crystalline silicates quickly amorphized in shock; need JWST res. to test) We use the remnant of a Type Ia SN to study the mass loss history of an evolved star. Can this be done for other SNRs as well?

46 Kepler may be member of prompt SNe Ia (Reynolds+ 2007); exploding within few hundred Myr of star formation... could this class be connected to Type Ia SNe observed with dense CSM? 15 of these objects thus far identified (Silverman+ 2013)

47 Kepler may be member of prompt SNe Ia (Reynolds+ 2007); exploding within few hundred Myr of star formation... could this class be connected to Type Ia SNe observed with dense CSM? 15 of these objects thus far identified (Silverman+ 2013) Called SNe Ia/IIn, Ian, IIa, IIan, IIna, and Ia-CSM...

48 Kepler may be member of prompt SNe Ia (Reynolds+ 2007); exploding within few hundred Myr of star formation... could this class be connected to Type Ia SNe observed with dense CSM? 15 of these objects thus far identified (Silverman+ 2013) Called SNe Ia/IIn, Ian, IIa, IIan, IIna, and Ia-CSM... ;8"<9"4,018=>! A824B,-#*(#,01#22! 6#?#"(#,018=>! 694'8B,C'('D2#B,ECFG$"9H, ;"87,;8"<9"4,9*4,6#?#"(#,018=>(! 3'4$56,%7'(('8*, 018=>#4,:'*4! 0/#229",:'*4! Figure courtesy of Ori Fox; see Fox & Filippenko 2013

15 of these objects thus far identified (Silverman+ 2013) Called SNe Ia/IIn, Ian, IIa, IIan, IIna, and Ia-CSM... %@#=/9! ;8"<9"4,018=>! A824B,-#*(#,01#22! 6#?#"(#,018=>!

49 Kepler may be member of prompt SNe Ia (Reynolds+ 2007); exploding within few hundred Myr of star formation... could this class be connected to Type Ia SNe observed with dense CSM? 15 of these objects thus far identified (Silverman+ 2013) Called SNe Ia/IIn, Ian, IIa, IIan, IIna, and Ia-CSM... ;8"<9"4,018=>! A824B,-#*(#,01#22! 6#?#"(#,018=>! 694'8B,C'('D2#B,ECFG$"9H, ;"87,;8"<9"4,9*4,6#?#"(#,018=>(! Dense CSM incompatible with Patnaude+ (2012) model for Kepler, which requires a cavity, but perhaps some SNe Ia-CSM explode before shutting off wind? 018=>#4,%@#=/9! 018=>#4,:'*4!!"#$%&'()*+,-.(/,01#22, 3'4$56,%7'(('8*, 0/#229",:'*4! Figure courtesy of Ori Fox; see Fox & Filippenko 2013

50 RCW 86 - Long thought to be corecollapse, only recently shown to be most likely Type Ia (BJW+ 2011) - Independently confirmed as Type Ia by Yamaguchi Likely remnant of SN 185 A.D. - D = 2.5 kpc Spitzer, WISE, Chandra, XMM-Newton mosaic

51 Evidence for Ia origin of RCW 86

52 Evidence for Ia origin of RCW 86 I) IR derived densities constrain amount of neutral hydrogen; CC SNe ionize surrounding medium before/ during explosion, can rule out most (Ib/c, IIP, IIL, IIb, IIn; Chevalier 2005) Blue supergiant still possible, but... Hα image (Smith 1991)

53 Evidence for Ia origin of RCW 86 I) IR derived densities constrain amount of neutral hydrogen; CC SNe ionize surrounding medium before/ during explosion, can rule out most (Ib/c, IIP, IIL, IIb, IIn; Chevalier 2005) Blue supergiant still possible, but... Hα image (Smith 1991) II) BSGs surrounded by N-rich wind (see 1987A), but no N enhancement here (McCray+ 1993, Leibowitz+ 1983); exploding BSGs create dense clumps of O-rich material not observed (Li+ 1993, BJW+ 2008)

54 Evidence for Ia origin of RCW 86 I) IR derived densities constrain amount of neutral hydrogen; CC SNe ionize surrounding medium before/ during explosion, can rule out most (Ib/c, IIP, IIL, IIb, IIn; Chevalier 2005) Blue supergiant still possible, but... Hα image (Smith 1991) II) BSGs surrounded by N-rich wind (see 1987A), but no N enhancement here (McCray+ 1993, Leibowitz+ 1983); exploding BSGs create dense clumps of O-rich material not observed (Li+ 1993, BJW+ 2008) III) Lots of iron, no evidence for over-solar oxygen. Only modest N H (6 x ), so O hard to hide; plasma plenty ionized enough XMM-Newton mosaic

55 Evidence for Ia origin of RCW 86 I) IR derived densities constrain amount of neutral hydrogen; CC SNe ionize surrounding medium before/ during explosion, can rule out most (Ib/c, IIP, IIL, IIb, IIn; Chevalier 2005) Blue supergiant still possible, but... Hα image (Smith 1991) II) BSGs surrounded by N-rich wind (see 1987A), but no N enhancement here (McCray+ 1993, Leibowitz+ 1983); exploding BSGs create dense clumps of O-rich material not observed (Li+ 1993, BJW+ 2008) III) Lots of iron, no evidence for over-solar oxygen. Only modest N H (6 x ), so O hard to hide; plasma plenty ionized enough IV) No central point source (again, low N H /A V ) Optical: M V < 18.5 (Fesen+ 1979) X-ray: L NS < 0.1 L Cas A NS (Kaplan+ 2004) Radio: No radio pulsar or PWN (Kaspi+ 1996) XMM-Newton mosaic

56 Evidence for Ia origin of RCW 86 I) IR derived densities constrain amount of neutral hydrogen; CC SNe ionize surrounding medium before/ during explosion, can rule out most (Ib/c, IIP, IIL, IIb, IIn; Chevalier 2005) Blue supergiant still possible, but... Hα image (Smith 1991) II) BSGs surrounded by N-rich wind (see 1987A), but no N enhancement here (McCray+ 1993, Leibowitz+ 1983); exploding BSGs create dense clumps of O-rich material not observed (Li+ 1993, BJW+ 2008) III) Lots of iron, no evidence for over-solar oxygen. Only modest N H (6 x ), so O hard to hide; plasma plenty ionized enough IV) No central point source (again, low N H /A V ) Optical: M V < 18.5 (Fesen+ 1979) X-ray: L NS < 0.1 L Cas A NS (Kaplan+ 2004) Radio: No radio pulsar or PWN (Kaspi+ 1996) XMM-Newton mosaic RCW 86 is either a Type Ia or a highly unusual CC SN

57 Radius ~ 13 pc Age = 1825 yrs V sh = 600 km/s n 0 = 0.5 cm -3

58 Expansion into uniform medium cannot explain RCW 86, so what can?

59 Expansion into uniform medium cannot explain RCW 86, so what can? Wind-blown bubble (Hachisu+ 1996, Badenes+ 2007): accretion wind (SD!) from optically-thick material bubble n 0,I =? R b =? shell n 0,II = 0.5 cm -3 t = 1825 yrs R = 12 pc V = 600 km/s

60 Expansion into uniform medium cannot explain RCW 86, so what can? Wind-blown bubble (Hachisu+ 1996, Badenes+ 2007): accretion wind (SD!) from optically-thick material bubble n 0,I =? R b =? shell n 0,II = 0.5 cm -3 t = 1825 yrs R = 12 pc V = 600 km/s FS R b = 10.8 pc n 0,I = cm -3 RS CD

61 Expansion into uniform medium cannot explain RCW 86, so what can? Wind-blown bubble (Hachisu+ 1996, Badenes+ 2007): accretion wind (SD!) from optically-thick material bubble n 0,I =? R b =? shell n 0,II = 0.5 cm -3 t = 1825 yrs R = 12 pc V = 600 km/s Advantages RS R b = 10.8 pc n 0,I = cm -3 CD FS - Good agreement with observations (V = 740 km/s, within errors) - accurately predicts ionization state of plasma - no special circumstances - reasonable physical parameters - looks a lot like model from Badenes+ 2007, though not constrained to be similar

64 2D Simulation RCW 86 most consistent with a SD Type Ia SN into a wind-blown bubble Red: shocked shell material White: shocked bubble material Blue: reverse-shocked ejecta

65 2D Simulation RCW 86 most consistent with a SD Type Ia SN into a wind-blown bubble Red: shocked shell material White: shocked bubble material Blue: reverse-shocked ejecta

66 Summary

67 Summary 1) Remnants of Type Ia SNe can provide clues to their origin

68 Summary 1) Remnants of Type Ia SNe can provide clues to their origin 2) The single degenerate channel is not all dead! (Only mostly dead?)

69 Summary 1) Remnants of Type Ia SNe can provide clues to their origin 2) The single degenerate channel is not all dead! (Only mostly dead?) 3) Still no sign of runaway companion; but center of explosion may not be center of remnant

70 Summary 1) Remnants of Type Ia SNe can provide clues to their origin 2) The single degenerate channel is not all dead! (Only mostly dead?) 3) Still no sign of runaway companion; but center of explosion may not be center of remnant 4) What would Kepler and RCW 86 look like as SNe?

Progenitor signatures in Supernova Remnant Morphology. Jacco Vink Utrecht University

Progenitor signatures in Supernova Remnant Morphology Jacco Vink Utrecht University The evolution of SNRs Heating by two shocks: 1. forward shocks heating ISM/CSM 2. reverse shock heating ejecta radius