1. The Molecular Environment of the SNR HESS J1731-347 (G353.6-0.7) refs: 1503.06717 1405.2599 By: Zhang, Xiao (2015-04-14)

2. HESS J1731-347 (G353.6-0.7)  It is the first shell-type SNR discovered on the basis of very high energy gamma-ray observations (Aharonian et al. 2008)  Tian et al. (2008) found the radio counterpart and identified it as a SNR  faint radio emission (2.5 Jy at 1 GHz)  radio size: 0.5 degree in diameter (30 pc @ 3.2 kpc)  distance: 3.2 +- 0.8 kpc (HI & CO, Tian et al. 2008), > 3.2 kpc (X-ray absorption, Abramowski et al. 2011), 5.2-6.1 kpc (Fukuda 2014)  Age: 27000 yr (Tian et al. 2008), 4000 yr (Fukuda 2014)  X-ray: dominated by the non-thermal emission (Bamba 2012)  a CCO exist in its center (Klochkov et al. 2013) 1.4 GHz very similar to RX J1713.7-3946 J1729-345 J1731-347

3. CO and HI observation (Fukuda et al. 2014) datasets HI: SGPS (McClure-Griffiths et al. 2005) 12CO (J = 1-0): NANTEN2, HPBW 2.7 min, 0.2 km/s

4. Results: from -40 km/s to 0 km/s H I CO H II region contour: TeV

5. Results: from -90 km/s to -70 km/s H I CO contour: TeV association 1

6. Large scale distribution of HI HI: color CO: contour white dashed line: 3-kpc expanding arm Kinematic of the associated gas

7. HI: color CO: contour

8. association 2

9. sun GC 3-kpc arm Association with clump

10. color: CO ( -90 km/s to -75 km/s ) contour: 1.4 GHz continuum color: CO ( -90 km/s to -75 km/s ) contour: TeV color: HI black contour: CO ( -82 km/s to -80 km/s ) white contour: TeV Comparison with other wavelengths

11. color: CO + HI ( -90 km/s to -75 km/s ) contour: TeV color: CO + HI ( -90 km/s to -75 km/s ) contour: 1.4 GHz continuum Comparison with other wavelengths

12. + Leptonic component 0 deg 90 deg Hadronic (80%) + Leptonic (20%) The ISM proton distribution and Gamma-ray association 3

13. Fermi Observation (Yang, et al. 2014) residual counts map (> 2 GeV). contour: TeV

15. CS observation (1503.06717) data: Mopra Results CS (1-0) clumps were discovered at three velocity range the critical density: ~ 10^4 cm^{-3}

16. 3 kpc-expanding arm d ~ 6 kpc (~ - 85 km/s) J1731: no detection J1729: ~1000 Msun

17. Norma-Cygnus Arm d ~ 5 kpc (- 55 km/s) J1731: no detection J1729: ~5000 Msun

18. Scutum-Crux Arm d ~ 3.2 kpc (from -23.5 to -7.0 km/s) J1731: ~ 5x10^5 Msun J1729: ~ 6000 Msun HII region; C 34 S(1-0), CH 3 OH(7-6), HC 3 N(5-4), SiO(1-0)

19. Evolutionary Models for Type Ib/c Supernova progenitors Yoon, Sung-Chul 1504.01205

20. ( Vink 2012 ) Minkowski 1941

21. 2. SINGLE STAR MODELS 2.1 Mass loss and final Mass Wolf-Rayet (WR) stars: their observational counterparts (e.g. Meynet & Maeder 2003; Massey 2003; Crowther 2007; Smartt 2009). 'isolation' (van der Hucht 2001; Crowther 2007), 'The Conti scenario' (Conti 1976) The mass lower limit for WR stars observation: L > 5.3 Lsun, M_He ~ 10 Msun → > 25 Msun theory: > 40 Msun (no rotation, Z=0.02, at RSG mass loss rate) 'increase mass loss' (rotation, pulsation,...)

22. Final Mass Once a star becomes a WR star, further mass loss due to WR winds determines its final mass. Difficulty for Mf > 10 Msun 1. easily collapse to a BH (Heger et al. 2013) 2. light curves will be too broad HD 45166

23. 2.2 surface properties large convective cores → chemically homogeneous theoretical difficulty: higher T (e.g., Hamann et al. 2006; Crowther 2007; Sander et al. 2012). only one: SN Ib iPTF13bvn (Cao et al. 2013) more compact lowest T highest T observation 'envelope inflation' favor binary Mv < - 4 in optical but Yoon et al. 2012b:

24. 2.3 Helium Remaining He mass Ib: He, lower limit ~ 0.5-0.6 Msun Ic: no He, upper limit ~ 0.14 Msun (Hachinger et al. 2012) Georgy et al. (2012): 0.28 - 2.2 Msun Woosley et al. (1993): a 60 Msun star → 4.25 Msun with 0.18 Msun He very large mass loss rate He star He mass fraction Dessart et al. 2011 ~ 0.9, He I lines < 0.5, no He I lines even for 1 Msun He Meynet & Maeder 2003, 2005; Georgy et al. 2012 < 0.4 for sigle star model ~ 0.9 for binary star model He I lines depend on the total He mass and on the He distribution

25. 2.4 Rotation SLSNe and GRBs can be driven by rapid rotation All of GRBs + most of SLSNe → Type Ic the collapsar scenario → GRBs (Woosley & Bloom 2006) the magnetar scenario → SLSNe Ic (e.g., Chomiuk et al. 2011) observation: massive star with rapid rotation model without B-field ( Meynet & Maeder 1997; Heger et al. 2000) : angular momentum can be hold to the pre-SN stage. Magnetic model with the Tayler-Spruit dynamo (Heger et al. 2005): effectively slow down 'question' (Zahn et al. 2007; Gellert et al. 2008)

26. Binary star model

28. Distance of HESS J1731-347 possible correspondence of the SNR with the HI and CO in a velocity range from -90 km/s to -75 km/s.  the elliptical ring model v~320 km/s, a ~ 4.1 kpc, b ~ 2.2 kpc d ~ 6.1 kpc  the expanding circular ring model v~201 km/s, v_r ~48 km/s, R~3.4 kpc d ~ 5.2 kpc d: 5.2 - 6.1 kpc Vallee, 2008 @ 5.2 kpc, n ~ 0.01 cm^{-3} → t ~ 4000 yr, V ~ 2100 km/s