HI 21-cm Study of Supernova Remnants in SKA Era
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1 SKA Meeting HI 21-cm Study of Supernova Remnants in SKA Era Bon-Chul Koo (SNU, KIAS)
2 Supernova Explosions SN explosions play a major role in the ecology and evolution of galaxies by supplying heavy elements, cosmic rays, and dust grains, and by dumping huge amount of energy/momentum to the ISM. Supernova Remnants (SNRs) are where we can observe and study those astrophysical phenomena. radio IR optical X-ray 2
3 HI SNRs and the Missing SNR Problem 1. Missing SNR Problem 2. HI SNRs (=SNRs with HI emission) 3. HI SNRs and Missing SNR Problem 3
4 Missing SNR Problem 294 SNRs in the Milky Way (Green 2014) Expected # of SNRs = SN rate lifetime ~ 1/40 yr 10 5 yrs ~ 2, (e.g.) Higdon & Lingenfelter 1980, 2005; Helfand+ 1989; Li, Z ; Green, D. 2004, 2015; Brogan+2006; Green, A Faint SNRs and small SNRs are difficult to detect. Most SNRs are missing! Bonn 11cm ( l = 26º ~ 56º, b = 5º +5º)
5 Galactic SNR Population from Green, D. Milne, D. Brogan et al. (2006): 35 new SNRs from 90 cm VLA survey Helfand et al. (2006): 12 SNR candidates from the MAGPIS Gerbrandt et al. (2013): 5 new SNRs in the DRAO survey Sabin et al. (2013): 4 new SNRs in the IPHAS survey Green, A. et al. (2014): 23 SNR candidates in the MGPS-2
6 Galactic SNR Distribution 38 (0.95 kpc -2 ) 0.85 kpc (0.50 kpc -2 ) 59 (0.52 kpc -2 ) 1.7 kpc kpc -2 Observed (Green 2014) 140 (0.76 kpc -2 ) 4.4 kpc -2 Model (Li+ 1991) Assuming that SNRs are within a disk of 12 kpc radius 6
7 Missing Young SNRs SNRs younger than 10 3 yrs ~ 1/40 yr 10 3 yrs ~ 25 (>6) Cassiopeia A (SN IIb) G Size distribution (Green, D. 2015) SN 1681±19 (1 = 1 pc) (R) [Fe II] μm (G) kev (B) kev (1 = 2.5 pc) 7
8 HI SNRs SNR Evolution & Radiative Shocks t sf E n yr v exp 180 km/s, R s 20 pc, N(H)~n 0 R s / cm -2 R t 2/5 R t 1/4 Sedov SNR Radiative SNR Cioffi+ (1988)
9 Difficulty in detecting HI SNRs Strong Galactic Background HI emission LAB HI Sky (Kalberla et al. 2005) gl=49 deg Russeil (2003)
10 HI SNRs can be identified if the line-of-sight velocities of their expanding shells are significantly beyond the maximum or minimum velocity permitted by the Galactic rotation. W44 HC40 HC40=G (Park, G ) (l,v) map from LD survey (Koo & Kang 2004)
11 HI Observations of SNRs Individual SNRs IC 443, W44, W51C, CTB 80, VRO , CTB 109, G , Surveys 15/103 Northern SNRs (Koo & Heiles 1991); 10/97 Southern SNRs (Koo, Kang, McClure-Griffith 2004); 4/39 SNRs in I-GALFA survey (Park, G. et al. 2013) IC 443 seen by Arecibo (Giovanneli & Haynes 1978) WSRT image of IC 443 (Braun & Strom 1986)
12 I-GALFA HI Survey I-GALFA = Inner-Galaxy ALFA ALFA (7-beam Arecibo L-band Feed Array) Purpose: Mapping all the H I in the inner Galactic disk, l = 32º to 77º & b 10º (1200 deg 2 ); sky visible to the Arecibo 305-m telescope Steven Gibson, Bon-Chul Koo, Ji-hyun Kang, Kevin Douglas, Geumsook Park, Joshua Peek, Eric Korpela, Carl Heiles, Jonathan Newton
13 basketweave mappig D C Z B A Tracks after several passes
14 I-GALFA Survey Parameters Mapping area l = 32º to 77º & b 15º (1,157 square deg) Observing time to >130 nights (310 hrs) of the Galactic plane dark hours Telescope beam Velocity resolution Spectral coverage RMS noise km/s ± 750 km/s (7.14 MHz) ~0.25 K
15 LAB survey vs I-GALFA survey (Koo+ 2012; Gibson+ 2013)
16 HI SNRs in the I-GALFA Survey 4 SNRs out of 39 W44, W51C, G , CTB 80 (Park+ 2013) middle aged ( yr) SNRs interacting with a relatively dense (> 1 cm -3 ) medium. 10 pc 16
![[Fe II] + UWISH2 H 2 10 pc](/docs-images/86/94590746/images/17-5.jpg "HI shell (Koo & Heiles 1995;")
17 SNR W44 (G ) Shocked HI Gas HI shell: v exp =135 km/s, M(H)=390 M, E K = ergs L H =90 L M(H 2 )~0.13 M Chevalier (1999) UWIFE [Fe II] + UWISH2 H 2 10 pc HI shell (Koo & Heiles 1995; Chandra Park X-ray )
18 SNR IC 443 (G ) 1 st SNR where shocked HI/CO gas have been discovered. Shocked HI HI shell: v exp ~100 km/s, M(H)=490 M, E K ~ ergs L H =11 L M(H 2 )~0.015 M Chandra X-ray 10 pc (G) [Fe II] ; (R) H 2 HI shell (Lee ) 18
19 Stellar Feedback SN momentum injection Driving turbulence Regulating star formation Momentum injection per SN = 2.8x10 5 n M km/s, insensitive to environmental details SNR in two phase ISM of n=8.9 and 0.14 cm -3 (Kim & Ostriker 2015)
20 Momentum of HI SNRs Cioffi+ (1988) IC 443 (Lee et al. 2004), W44 (Giacani+ 97; Koo & Heiles 95), W51 (Koo & Moon 1997), HB 21 (Koo & Heiles 91), CTB 80 (Castelletti+ 2003; Koo et al. 90), G (Koo+ 2004), G (Kang+ 2012), G (Park et al. 2013)
21 LMC SNRs AKARI LMC survey (Ita+08) SAGE survey (Meixner+06) O: N/MIR SNR O: MIR SNR O: No IR SNR Image: MCELS Ha, [SII], [OIII]
22 Where are all the HI SNRs? Astrophysical Factors Most (~80%) of SNe are ccsn. Most (80-90%) of ccsne occur in superbubbles Most of the IS space may be filled with very tenuous (~ cm -3 ) hot gas. Expected # of visible HI SNRs (Koo & Kang 2004) N = SN ƒ HI ƒ obs ~ 200 (>>25) Most HI SNRs are missing!!! 512 x 512 x 2048 pc 3 (Kim+ 2013)
23 Forbidden-Velocity Wings Extended Wings at Forbidden Velocities
24 FVW Fast expanding HI shell invisible in radio v s ~80 km/s, R s =110 (d/10kpc) pc SNR? For E 0 = erg, d=8 kpc, R s =88 pc, t ~ yr Sigma-D relation R 100 pc FVW represents a type of oldest SNRs which are hardly visible except in HI 21cm emission line. G in LD survey Color: HI, contour: radio continuum (Koo et al. 2006)
25 FVWs in the I-GALFA Survey I-GALFA HI 21cm VGPS 1.4 GHz continuum map
26 Summary There are about 300 SNRs in the Milky Way, but most SNRs including young ones are missing. In a handful of SNRs, high-velocity, shocked HI gas has been detected. They are laboratories for studying shock physics, cloud structure, and stellar feedback. Old HI SNRs are largely missing. FVWs are candidates for such missing old HI SNRs. SKA and SKA precursor/pathfinder observations of the Milky Way and nearby galaxies can address some of the issues related to the above. 26
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