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Association of Galactic supernova remnants with molecular clouds

Association of Galactic supernova remnants with molecular clouds. Bing Jiang (Nanjing Univ., China) in collaboration with Yang Chen, Junzhi Wang, Yang Su, Xin Zhou (Nanjing Univ.), Samar Safi-Harb (Univ. of Manitoba) & Tracey DeLaney (CfA) ApJ, 712, 1147 (2010). COSPAR, Bremen, July 2010.

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Association of Galactic supernova remnants with molecular clouds

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  1. Association of Galactic supernova remnants with molecular clouds Bing Jiang (Nanjing Univ., China) in collaboration with Yang Chen, Junzhi Wang, Yang Su, Xin Zhou (Nanjing Univ.), Samar Safi-Harb (Univ. of Manitoba) & Tracey DeLaney (CfA) ApJ, 712, 1147 (2010) COSPAR, Bremen, July 2010

  2. Why study SNR-MC Association (I) • Molecular gas takes up 1/2 mass of ISM (Dame et al. 2001) • Most core-collapse SNe are located close to GMCs -- their birth places (e.g. Huang & Thaddeus 1986) (Huang & Thaddeus 1986) • > 50% among 270 Galactic SNRs are expected to have been in interaction with MCs (Reynoso & Mangum 2000); How many? Little details of interaction are known. SNR-MC Association

  3. Why study SNR-MC Association (II) Unique Physical and Chemical effects, when SNR shocks against MCs … Wardle & Yusef-Zadeh 2002 • Compress, heat, and drive molecular gas • Excite, ionize, and even dissociate • molecules • C-type shock propagates in MCs • Influence chemical evolution & produce otherwise impossible molecular emission （e.g. 1720MHz OH maser, HCO+, etc.） • Shock-cloud p-p collision  0  2, Important source of GeV-TeV -rays ! • Last but not least: • With SNR-MC association established, • VLSR distance G347.3-0.5 (Fukui et al. 2003) 0.4-3 GeV (AGILE) MAGIC VERITAS IC443 (Tavani, M. et al. 2010) 3C391 Fermi (Castro & Slane, 2010) SNR-MC Association

  4. Evidence of Association • Physical signals • 1. 1720MHz OH masers • 2. Molecular line broadening (LB) • 3. High line ratio • 4. shocked NIRH2lines • 5. Specific (Spitzer) IR colors • Morphological signals • 6. Multi-wavelength morphological agreement (MA) SNR-MC Association

  5. 1. 1720MHz OH masers: Signposts First detection (Goss & Robinson 1968) Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) 2. Molecular line broadening (LB) e.g. CO, HCO+, CS, etc. 3. High line ratio e.g. 12CO(2-1)/12CO(1-0) 4. shocked NIR H2 lines 5. Specific (Spitzer) IR colors e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) 6. Multi-wavelength morphological agreement (MA) e.g., arc, shell, interface, etc. Evidence of Association Bing Jiang SNR-MC Association COSPAR2010, Bremen

  6. Evidence of Association • 1. 1720MHzOH masers: Signposts • First detection (Goss & Robinson 1968) • Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) • OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) • So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) • 2. Molecular line broadening (LB) • e.g. CO, HCO+, CS, etc. • 3. High line ratio • e.g. 12CO(2-1)/12CO(1-0) • 4. shocked NIR H2 lines • 5. Specific (Spitzer) IR colors • e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) • 6. Multi-wavelength morphological agreement (MA) • e.g., arc, shell, interface, etc. optical grey - 12CO 1-0 contours - radio Kes 75, 12CO 1-0 (Su et al. 2009) IC 443, 12CO 1-0 (Dickman et al. 1992) Bing Jiang SNR-MC Association COSPAR2010, Bremen

  7. Evidence of Association • 1. 1720MHzOH masers: Signposts • First detection (Goss & Robinson 1968) • Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) • OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) • So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) • 2. Molecular line broadening (LB) • e.g. CO, HCO+, CS, etc. • 3. Highline ratio • e.g. 12CO(2-1)/12CO(1-0) • 4. shocked NIR H2 lines • 5. Specific (Spitzer) IR colors • e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) • 6. Multi-wavelength morphological agreement (MA) • e.g., arc, shell, interface, etc. W44, 12CO 2-1/1-0 (Seta et al. 1998) IC443, 12CO 2-1/1-0 (Seta et al. 1998) SNR-MC Association

  8. Evidence of Association • 1. 1720MHzOH masers: Signposts • First detection (Goss & Robinson 1968) • Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) • OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) • So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) • 2. Molecular line broadening (LB) • e.g. CO, HCO+, CS, etc. • 3. Highline ratio • e.g. 12CO(2-1)/12CO(1-0) • 4. shockedNIRH2lines • 5. Specific (Spitzer) IR colors • e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) • 6. Multi-wavelength morphological agreement (MA) • e.g., arc, shell, interface, etc. H2 - red [FeII] - green X-ray - blue H2 2.12μm W44 (Reach et al. 2005) W49B (Keohane et al. 2007) SNR-MC Association

  9. Evidence of Association • 1. 1720MHzOH masers: Signposts • First detection (Goss & Robinson 1968) • Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) • OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) • So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) • 2. Molecular line broadening (LB) • e.g. CO, HCO+, CS, etc. • 3. Highline ratio • e.g. 12CO(2-1)/12CO(1-0) • 4. shockedNIRH2lines • 5. Specific (Spitzer)IR colors • e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) • 6. Multi-wavelength morphological agreement (MA) • e.g., arc, shell, interface, etc. Radio Whiteoak & Green (1996) Radio Whiteoak & Green (1996) Mid-infrared (Spitzer IRAC) 3.6/8 4.5/8 5.8/8 filament: <0.07 0.14 0.59 shell: 0.19 0.38 0.79 3.6/8 4.5/8 5.8/8 filament: 0.12 0.30 0.39 shell: 0.33 0.34 0.67 Kes 17 (Reach et al. 2006) RCW 103 (Reach et al. 2006) SNR-MC Association

  10. Evidence of Association • 1. 1720MHz OH masers: Signposts • First detection (Goss & Robinson 1968) • Theory (Lockett et al. 1999; Green,A.J. 2002; Wardle & Yusef-Zadeh 2002) • OH survey (Yusef-Zadeh et al. 1995, 1996, 1997; Frail et al. 1996; Claussen et al. 1997; Green et al. 1997; Koralesky et al. 1998; Hewitt et al. 2008, 2009) • So far, 25 detections: 17 (Green et al. 1997) + 3 (Koralesky et al. 1998)+ 4 (Hewitt et al. 2008, 2009) • 2. Molecular line broadening (LB) • e.g. CO, HCO+, CS, etc. • 3. Highline ratio • e.g. 12CO(2-1)/12CO(1-0) • 4. shockedNIRH2lines • 5. Specific (Spitzer)IR colors • e.g. 3.6μm/8μm, 4.5μm/8μm, 5.8μm/8μm (Reach et al. 2006) • 6. Multi-wavelength morphological agreement (MA) • e.g., arc, shell, interface, etc. 79-82 km/s Green – CO 1-0 White contours – X-ray Red contours – radio Red – CO 1-0 Green – IR Bule - X-ray Kes 75 (Su et al. 2009) Kes 69 (Zhou et al. 2009) SNR-MC Association

  11. Physical evidence 1. 1720MHz OH masers 2. Molecular line broadening (LB) 3. High line ratio 4. shocked NIRH2lines 5. Specific (Spitzer) IR colors Morphological evidence 6. Multi-wavelength morphological agreement (MA) Evidence of Association Bing Jiang SNR-MC Association COSPAR2010, Bremen

  12. Our List of SNR-MC Association (I) Jiang et al. 2010, ApJ 64 in total 34 confirmed Evidence: 1. OH maser 2. Molecular LB 3. High line ratio 4. NIRH2 lines 5. IRcolors 6. MA of molecular features SNR-MC Association

  13. Our List of SNR-MC Association (I) Jiang et al. 2010, ApJ 11 probable … … 6. MA of molecular features http:// astronomy.nju.edu.cn/~ygchen/others/bjiang/interSNR6.htm 19 possible … … 5. Rough IRcolors … 7.Rough correspondence (RC) of molecular features 64 in total >21 γ-ray detections

  14. 3C397: in a mol. cavity Jiang et al. 2010, ApJ Characteristics: 1. Rectangular-shaped 2. SE-NW elongation Red - 24μm, Spitzer Blue – X-ray, Chandra Green - 12CO 1-0, 27-35 km/s (by the mm telescope at of the Purple Mountain Observatory at Delingha, China) Unsharp masking SNR-MC Association

  15. 3C397: line broadening Jiang et al. 2010, Sci. China Asymmetric SN explosion Also see Safi-Harb & Franzmann, poster Thu-265 E19-0061-10 Association  distance ~ 10.3 kpc Mean molecular density: Pressure balance:  shocked gas:

  16. Summary • In our list of Galactic SNR-MC associations, 64 ones are presently known and suggested to be in physical contact with MCs • SNR 3C397 is confined in a molecular cavity with direct evidence of interaction of line broadening on the boundary with the kinematic distance ~ 10.3 kpc Outlook • More identifications, details of interaction and molecular environment • Candidates for the gamma-ray sources and to study hadronic model of cosmic ray acceleration SNR-MC Association

  17. Thank you for your attention! SNR-MC Association

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