1. Association of Galactic supernova remnants with molecular clouds COSPAR, Bremen, July 2010 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)

2. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen Why study SNR - MC Association (I) (Dame et al. 2001) (Huang & Thaddeus 1986) Molecular gas takes up 1/2 mass of ISM Most core-collapse SNe are located close to GMCs -- their birth places (e.g. 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.

3. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen 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, V LSR  distance Unique Physical and Chemical effects, when SNR shocks against MCs … 3C391 Fermi (Castro & Slane, 2010) IC443 (Tavani, M. et al. 2010) 0.4-3 GeV (AGILE) VERITAS MAGIC G347.3-0.5 (Fukui et al. 2003) Wardle & Yusef-Zadeh 2002 Why study SNR - MC Association (II)

4. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen Physical signals –1. 1720MHz OH masers –2. Molecular line broadening (LB) –3. High line ratio –4. shocked NIR H 2 lines –5. Specific (Spitzer) IR colors Morphological signals –6. Multi-wavelength morphological agreement (MA) Evidence of Association

5. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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

6. 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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 JiangSNR-MC AssociationCOSPAR2010, Bremen grey - 12 CO 1-0 contours - radio Kes 75, 12 CO 1-0 (Su et al. 2009) IC 443, 12 CO 1-0 (Dickman et al. 1992) optical

7. 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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 JiangSNR-MC AssociationCOSPAR2010, Bremen IC443, 12 CO 2-1/1-0 (Seta et al. 1998)W44, 12 CO 2-1/1-0 (Seta et al. 1998)

8. 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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 JiangSNR-MC AssociationCOSPAR2010, Bremen H 2 - red [FeII] - green X-ray - blue W49B (Keohane et al. 2007) H 2 2.12μm W44 (Reach et al. 2005)

9. 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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 JiangSNR-MC AssociationCOSPAR2010, Bremen Kes 17 (Reach et al. 2006)RCW 103 (Reach et al. 2006) 3.6/8 4.5/8 5.8/8 filament: 0.12 0.30 0.39 shell: 0.33 0.34 0.67 3.6/8 4.5/8 5.8/8 filament: <0.07 0.14 0.59 shell: 0.19 0.38 0.79 Radio Whiteoak & Green (1996) Radio Whiteoak & Green (1996) Mid-infrared (Spitzer IRAC)

10. 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. 12 CO(2-1)/ 12 CO(1-0) 4. shocked NIR H 2 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 JiangSNR-MC AssociationCOSPAR2010, Bremen Kes 69 (Zhou et al. 2009) Kes 75 (Su et al. 2009) Red – CO 1-0 Green – IR Bule - X-ray Green – CO 1-0 White contours – X-ray Red contours – radio 79-82 km/s

11. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen Physical evidence –1. 1720MHz OH masers –2. Molecular line broadening (LB) –3. High line ratio –4. shocked NIR H 2 lines –5. Specific (Spitzer) IR colors Morphological evidence –6. Multi-wavelength morphological agreement (MA) Evidence of Association

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

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

14. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen 3C397: in a mol. cavity Characteristics: 1. Rectangular-shaped 2. SE-NW elongation Jiang et al. 2010, ApJ Unsharp masking 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)

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

16. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen 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

17. Bing JiangSNR-MC AssociationCOSPAR2010, Bremen Thank you for your attention!