A List of Galactic SNRs Interacting with Molecular Clouds
Name   Conventional Name SNR Type Evidence Group Ref. γ-ray detection CO obs.      
G0.0+0.0   Sgr A East TC OH, CS MA & LB, H2 Y 1,2,3,4,5 HESS(Aharonian et al. 2006, ApJ, 636, 777--a survey paper)      
G1.05-0.1   Sgr D SNR S OH Y 2,6   no CO obs.    
G1.4-0.1     S OH Y 2,6   no CO obs. Nor X-ray    
G5.4-1.2   Milne 56 C? OH Y 7   no diffuse study-> TC?    
G5.7-0.0     not listed in Green's catalog OH Y 7 HESS("coincident with TeV γ-ray source HESS J1800-240C, Aharonian et al. 2008,A&A, 481, 401)"      
G6.4-0.1   W28 TC OH,CO MA & LB,H2 MA, NIR,SiO Y 2,8,9,10 EGRET(Esposito et al. 1996, ApJ, 461, 820),TeV J1801-233, HESS J1801-233 (Aharonian, F. et al. 2008 A&A 481 p401-410), AGILE (Giuliani et al. 2010, arXiv:1005.0784)      
G8.7-0.1   W30 TC OH Y 7 HESS(Aharonian et al.2005,Science,307,1938; Aharonian et al. 2006, ApJ, 636, 777)  PMD(Delilngha)    
G9.7-0.0     S OH Y 7        
G16.7+0.1     C OH, CO MA Y 2,11,12   PMD(Delilngha)    
G18.8+0.3 18 23 58 −12 23  Kes 67 S CO MA & LB, CO ratio Y 13,14       MC shell (Tian et al. 2007)
G21.8-0.6   Kes 69 TC OH, CO MA & LB, HCO+, H2 Y 2,11,15,16   PMD(Delilngha)   MC shell (Zhou et al. 2009)
G29.7−0.3 18 46 25 −02 59 Kes 75 C CO MA & LB Y 17 HESS J1846-029/PWN (Djannati-Atai, A. et al., 2008, ICRC, 2, p823-826) PMD(Delilngha)   MC shell (Su et al. 2009)
G31.9+0.0   3C 391 TC OH, molecular MA & LB (CO, HCO+,CS), H2, NIR Y 2,18,19,20 Fermi (Castro & Slane, 2010)      
G32.8-0.1   Kes 78 S OH Y 21   PMD(Delilngha), KOSMA    
G34.7-0.4   W44 TC OH,molecular LB(CO?, HCO+,CS),H2 MA, NIR,CO ratio Y 2,8,10,22 Fermi-LAT (Abdo, A.A. et al. Science,2010,327,1103); EGRET?(Esposito et al. 1996, ApJ, 461, 820, "possible" on Green's)        
G39.2−0.3 19 04 08 +05 28 3C396 C H2 & NIR MA, CO MA & LB Y 16,23,24 HEGRA(Aharonian et al. 2001, A&A, 375,1008),"limit" on Green's  PMD(Delilngha)   MC shell (Lee et al. 2009)
G41.1-0.3 19 07 34 +07 08 3C397 TC CO MA & LB Y 25 γ-ray TeV: HEGRA,Aharonian et al. 2001, A&A, 375, 1008, "limit" on Green's PMD(Delilngha)    
G42.8+0.6     S OH absorption? Y? Chomiuk 2002AAS Near soft gamma repeater, and young pulsar.   young pulsar    
G43.3-0.2   W49B TC H2 MA, CO ratio Y 45,private communication with Zhou et al.(in preparation) HEGRA, Aharonian et al. 2001, A&A, 375, 1008, "limit" on Green's  PMD (Delingha)    
G49.2-0.7 19 23 50 +14 06 W51 TC OH, CO MA & LB, HCO+ LB Y 2,11,26 HESS J1923+141 (Feinstein, F. et al. 2009,AIPC, 1112, 54, Proc. 6th Science with the New Gen. of HE Gamma-Ray Expts (2008)), Milagro (Abdo  et al. 2009ApJL,700L,127)     MC shell (Koo & Moon 1997a,b)
G54.4-0.3 19 33 20 +18 56 HC40 S CO MA & LB, IR MA (wind-blown bubble and/or molecular cloud) "detection of shell structure in CO in striking coincidence with the radio/multi-ww features"(Junkes et al. 1992) Y 27,28   KOSMA "perhaps the 1st candidate for stellar wind induced SF"(Junkes et al. 1992) MC shell (Junkes et al. 1992; Reach et al. 2006
G89.0+4.7 20 45 00 +50 35 HB21 TC CO MA & LB, CO ratio, H2, NIR (IR Shocked H2 Gas in the North; Shinn et al. 2009, ApJ,693,1883) Y 29,30,31        
G109.1-1.0 23 01 35 +58 53 CTB 109 S CO MA & LB  Y 32   FCRAOPMD(Delilngha), KOSMA The most likely explanation for the high concentration of H II regions and SNRs is that the SF in this part of the Perseus arm is triggered by the spiral shock.  
G189.1+3.0   IC 443 TC OH,CO ratio,H2,molecular MA & LB Y 2,8,22,33,34,35 TeV J0616+223: EGRET, 2EG J0618+2234(Esposito et al. 1996, ApJ, 461,820), 3EG (Casandjian & Grenier 2008, A&A, 489, 849),MAGIC J0616+225 (Albert et al. 2007, ApJL, 664L, 87); VERITAS(Acciari, V.A. et al.2009, ApJL,698L,133), Milagro (Abdo, A.A. et al. 2009,ApJL,700L,127), AGILE(Tavani, M. et al. 2010, ApJ, 710, L151), Fermi(Abdo et al. 2010, ApJ, 712, 459)      
G304.6+0.1 13 05 59 −62 42 Kes 17 S H2,IR MA & colors  Y 16,28   no CO obs.    
G332.4-0.4 16 17 33 −51 02 RCW 103 S IR MA & colors, NIR, H2 & HCO+ MA Y 28,36,37    ("The coincidence between the shock front position and the change in the HCO+ intensity strongly suggests the existence of a physical interaction between the SNR and the molecular gas","12CO is used as a reference molecule"(Paron et al. 2006))    
G337.0-0.1   CTB 33 S OH Y 18   no CO obs.    
G337.8-0.1   Kes 41 S OH Y 21   no CO obs.    
G346.6-0.2     S OH, H2, IR colors Y 21,16,28   (no X-ray obs.)    
G347.3-0.5 17 13 50 −39 45   S? CO MA & LB Y 38 TeV: RX J1713.7-3946?,TeV J1713-394 HESS J1713.7-3946, CANGAROO, diffuse, "Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons" (Muraishi et al. 2000, A&A,354L,57); HESS  (Aharonian et al.2004, Natur,432,75; Aharonian et al. 2007,A&A,464,235); Fermi (Funk, presentation, 2009)      
G348.5-0.0     S? OH, H2, IR MA Y 2,16,28(mentioned in 12)        
G348.5+0.1   CTB 37A S OH, CO MA Y 2,12,18 HESS, HESS J1714-385, TeV J1714-383 (Aharonian et al. 2008,A&A,490,685); "In this region, three SNRs are seen." G348.7+0.3(CTB 37B), G348.5+0.1(CTB 37A), G348.5-0.0      
G349.7+0.2     S OH, CO MA & LB, CO ratio, H2, IR MA Y 2,18,13,16,28        
G357.7+0.3   Square Nebula S OH Y 2,6        
G357.7-0.1   Tornado Nebula, MSH 17−39 TC OH, CO & H2 MA Y 2,18,39   SEST-15m; UNSWIRF   H2 shell (Lazendic et al. 2004)
G359.1-0.5     TC OH, CO & H2 MA, HCO+ & CS absorption Y 2,40,41,42 HESS, HESS J1745-303 (Aharonian et al. 2008, A&A,483,509), or G359.0-0.9  15m-SEST; University of New South Wales Infrared Fabry-Perot (UNSWIRF: Ryder et al. 1998) on the Anglo-Australian Telescope(AAT)    
G33.6+0.1   Kes 79 TC CO MA, HCO+ MA ("these results provide a direct indication of interaction of SNR with the adjacent MC" --Green & Dewdney 1992), broad OH absorption features at the same velocity(Green 1989) Y? 43   NRAO-12m, PMD (Delingha), KOSMA    
G40.5-0.5 19 07 10 +06 31   S CO MA Y? 44 TeV J1908+060,MGRO J1908+06, HESS J1908+063: HEGRA, Limit on high energy γ-rays (Aharonian et al. 2001, A&A, 375, 1008), Milagro, MGRO J1908+06? "at a median energy of ~20 TeV "(Abdo et al. 2007, ApJ, 664, L91), 8 sources; HESS J1908+063 (Aharonian, F. et al. 2009, A&A, 499, 723) PMD (Delingha)   MC shell? (Yang et al. 2006)
G54.1+0.3 19 30 31 +18 52   F? CO MA (morphological association of the PWN with a CO molecular cloud at a velocity of sime53 km s-1(Leahy et al. 2008, AJ, 136, 1477) Y? 46; Koo et al. 2008, 673, L147 VERITAS (Acciari, et al. 2010, arXiv:1005.0032) FCRAO, PMD (Delingha), KOSMA Post-MS triggered SF? (Koo et al. 2008)) MC shell around PWN? (Leathy et al. 2008)                                                                                                    
G74.0-8.5   Cygnus Loop S CO MA(coincident with optical emission only on the west, a small protrude of radio emission ); Graham et al. 1991, AJ,101,175--H2, but not related to MC "much of H2 emission in Cygnus Loop comes not from the regions where the shock is moving slowly (90km/s) into the densest materal (8cm^-3),but rather where the shock is the fastest (170km/s) and is moving into the lowest density (2 cm^-3) preshock medium" Y? 47   further CO obs. toward west of Cygnus Loop as Scoville did?    
G78.2+2.1 20 20 50 +40 26 γ Cygni SNR, DR4 S CO MA(Higgs et al. 1983, AJ, 88, 97) suggested that "No corresponding features are apparent in the CO observations" with NRAO, while Fukui & Tatematsu (1988, in SNRISM, p261) argued that "evidence is obtained for the interaction between the supernova remnants and molecular gas" with 4-m radio telescope at Nagoya.) Y? 48 EGRET, 2EG J2020+4026 (Esposito et al. 1996, ApJ, 461, 820; 3EG, Casandjian & Grenier 2008, A&A, 489, 849); MGRO J2031+41?(Abdo et al. 2007, ApJ, 664, L91)      PMD (Delingha)    
G84.2−0.8     S CO MA("we find the most striking coincidence between ´at´-17 km/s rather than near -40 km/s (Huang & Thaddeus 1986)´indicates a possible interaction between ..." (Feldt & Green 1993, but not striking enough) Y? 49,50   KOSMA, higher-resolution CO obs.?    
G120.1+1.4   Tycho, 3C10, SN1572 S CO MA Y? 51   Nobeyama-45m, good shell; KOSMA   MC shell (Lee et al. 2004;
G132.7+1.3   HB3 TC CO MA("a bright CO 'bar'´surrounded by enhanced radio continum", "physical connection between HB3 and CO in the MC") Y? 52 Not in TeVCat, EGRET, EGRJ0225+6240? (Casandjian & Grenier 2008, A&A, 489, 849) source catalog Columbia-1.2m, need higher-resolution CO obs. "Our results show ´ that SNR shock may play a role in current SF acitivity there" (Routledge et al. 1991, 247, 529)  
G263.9−3.3  08 34 00 −45 50 Vela C CO MA (good shell agreed with ROSAT, radio, optical ) Y? 53 RX J0852.0-4622,TeV J0852-462,HESS J0852-463: CANGAROO (Katagiri, H. et al., ApJ 619 pL163-L166 2005), HESS (Aharonian, F. et al., A&A 437 pL7-L10 2005) "extended" "likely related to inverse Compton emission" (Aharonian et al. 2006, A&A, 448, L43);  NANTEN-4m   MC shell (Moriguchi et al. 2001)
G284.3−1.8   MSH 10−53 S CO MA & possible LB(?poor) Y? 54   Columbia 1.2m, need higher-resolution CO obs.    
G18.9-1.1     C? CO MA ("The CO distribution between +24 and +26 km/s suggests that this gas has been swept by the expanding SNR""no line broadening") ? Traverso et al. 1999 (Bulletin, no published CO obs.)   Bulletin, no published CO obs.    
G22.7-0.2     S IR RC (CO MA & possible LB? --Su et al. private communication) ? 28   PMD(Delilngha), KOSMA    
G23.3-0.3 18 34 45 −08 48 W41 S HI MA & CO RC, extended TeV ? Tian et al. 2007; 55 extended TeV counterpart: HESS J1834-087? HESS (Aharonian et al.2006a; Aharonian et al. 2005; Tian et al. 2007a), MAGIC (Albert et al. 2006) PMD(Delilngha), KOSMA    
G39.7−2.0   W50, SS433 ? CO RC (only positional coincidence; suggested from similar distances and both displacing nearly two molecular scale heights from the galactic plane) ? 56 HEGRA, Limit on high energy γ-rays (Aharonian et al. 2001, A&A, 375, 1008)       
G63.7+1.1     F CO RC (Suspected CO void) ? 57(HI,CO,IR)   cfa 1.2m, new CO obs.?    
G74.9+1.2 20 16 02 +37 12 CTB 87 F CO RC("We do not find any indication of interaction of the SNR with the MC" because no broadening no velocity feature, profile etc.(Cho et al.); "CO (1-0) and CO (3-2) data reveal evidence for associated molecular material surrounding parts of CTB 87"(Kothes et al.)) ? 49,58(CO),59(CO,SF); Wallace et al. 1997, A&A(HI?) TeV: MGRO  J2019+37?        Cho: Negoya 4m;   Kothes: 12CO(1-0)--SRAO, Seoul; 12CO(3-2)-- Heinrich Hertz Telescope (HHT), Arizona; further better CO obs.?    
G94.0+1.0   3C434.1 S CO RC (simple CO+radio overlap) ? 49        
G106.3+2.7 22 27 30 +60 50   C? CO RC (mostly with HI, CO is not good) ? 60 TeV J2227+608; 3EG (Casandjian & Grenier 2008, A&A, 489, 849.), Milagro(Abdo et al. 2007, ApJ, 664, L91.), VER J2227+608 VERITAS(Acciari et al. 2009,ApJ,703,L6) FCRAO,PMD(Delilngha), KOSMA "relics of triggered SF in a complex environment" (Kothes et al. 2001, ApJ, 560, 236) pusar out of shell
G111.7−2.1   Cassiopeia A, 3C461 S H2CO absorption("A striking correlation between the continuum emission and the H2CO absorption distribution, and slight spectral broadenings toward the west, are the only evidence that may suggest that Cas A is interacting with an external cloud. However, the evidence is not enough to draw any definitive conclusion. "),IR RC(either interaction of explosion with ISM or fast-moving ejecta), CO RC ? 61(H2CO),62(IR); FIR and molecular: Krause et al. 2004, Nature, 432,596; NIR: Rho et al. 2003ApJ,592,299 TeV J2323+584, HEGRA (Aharonian, F. et al. 2001A&A,370,112), MAGIC (Albert et al. 2007, A&A, 474, 937), VERITAS (Humensky et al. 2009,arXiv:0912.4304), Fermi-LAT (Abdo et al. 2010, ApJ,L710,92) NIR(dust continuum is not significant in the NIR emission of Cas A; show unambiguous evidence that the NIR Ks-band emission is from synchrotron emission by accelerated cosmic-ray electrons.), FIR and molecular line(no cold dust within CasA,  most from interstellar dust in a molecular cloud complex located between the Earth and Cas A.The argument that type II supernovae produce copious amounts of dust is not supported by the case of Cas A)PMD(Delilngha)    
G160.4+2.8   HB9 S CO RC (simple CO+radio overlap) ? 49        
G166.0+4.3   VRO 42.05.01 TC unusual shape; CO RC (simple CO+radio overlap) ? 49   no CO obs.    
G166.3+2.5   OA 184 not listed in Green's CO RC (simple CO+radio overlap) ? 49        
G192.8-1.1   PKS 0607+17 S CO RC (simple CO+radio overlap) ? 49        
G205.5+0.5 06 39 00 +06 30 Monoceros Nebula S CO RC ? 63 γ-ray detection (Jaffe et al. 1997, ApJ, 484, L129.); 3EG(Casandjian & Grenier 2008, A&A,489, 849.); HESS J0632+057? (Aharonian, F. A. et al. 2007,A&A,469,L1) CfA 1.2 m millimeter-wave radio telescope, need higher-resolution CO obs. "nearby clouds are undergoing SF" (Oliver 1996)  
G260.4−3.4   Puppis A, MSH 08−44 S CO RC(yes on N & E part, no on E part), OH(negative) ? 64(N & E part),65(CO,E part), Woermann et al. 2000, MNRAS, 317, 421. (OH)      
G290.1−0.8   MSH 11-61A TC CO RC (d=7kpc=>CO, bad infer??) ? 66   NANTEN-4m, only 13CO, re-visit/better CO obs. is needed    
G310.8-0.4   Kes 20A S IR RC & colors ? 28        
G311.5−0.3     S IR MA & color(complete shell following radio, some filament with color suggestive of shocked gas) ? 28   no CO obs.    
G318.9+0.4     C CO MA ("a chain of clouds with a morphology coincident with the SNR in radio continuum, and extends from ~-28 km/s to ~-44 km/s""No broadenings") ? Traverso et al. 1999 (Bulletin, no published CO obs.)   Bulletin, no published CO obs.    
G344.7-0.1     C? IR RC & colors ? 28        
G353.6-0.7 17 32 00 −34 44   S CO spectra toward the center ? Tian et al. 2010; arXiv:0910.1684 HESS J1731-347 Delingha    
G11.2-0.3     C IR MA & colors, H2 & [FeII] MA ? Or N? 28(molecular shock); Koo et al.2007(a dense red supergaint wind) soft(20-100keV)γ-ray: INTEGRAL (Dean et al. 2008, MNRAS,384,L29,"its associated pulsar PSR J1811-1925 is an unlikely counterpart to HESS J1809-193" no CO obs.    
G13.3-1.3     S? CO obs. (no comment on interaction, no radio)(poor resolution=>new?) ?? Seward et al. 1995, ApJ, 449, 681   cfa-1.2m; new better CO obs.?                                                                                                        
G12.8−0.0     C? CO no MA ("Even though there is no direct positional coincidence, this giant cloud may have influenced the evolution of the γ-ray source and its surroundings.") N? Funk et al. 2007, A&A, 470, 249. INTEGAL(Ubertini et al. 2005, ApJ, 629, L109); HESS,HESS J1813-178? (Aharonian et al. 2006, ApJ, 636, 777), MAGIC(Albert et al. 2006, ApJ, 637, L41) NANTEN                                                                                                        
G69.0+2.7   CTB 80 ? HI cloud, CO RC, velocity trend ("we may safely conclude that there is no certain indication of the interaction between the MC and SNR", "MCs ´ probably not related to the SNR" (Koo 1993)) N? Koo et al. 1990, ApJ, 364, 178 (p-v, v=+8~+16km/s) & Koo et al. 1993, ApJ, 417, 196 MAGIC obs. Of PSR B1951+32 (in CTB 80) (Albert et al. 2007, ApJ, 669, 1143) FCRAO 12CO(1-0)   pulsar on the shell (figure: Koo et al. 1993, ApJ, 417, 196)
G93.7-0.2   CTB104A, DA551 TC HI & CO M ("identified signatures of the interaction of CTB 104A with the surrounding neutral material", "could not find any structure which might be related" from CO data (Uyaniker 2002)) a background HII region associated with a massive MC N? Uyanıker et al. 2002, ApJ, 565, 1022.    FCRAO 12CO(1-0); further CO obs.?    
G184.6-5.8   Crab F H2(formed early in the expansion of the remnant when the densities were higher), HI void(No clear evidence for an interaction between the Crab and the surrounding H I is found, the presence of a wind-blown H I bubble near the Crab is confirmed) N? Graham et al. 1990, ApJ,352, 172 (H2); Wallace et al. 1994, A&A,286,565,-1999, ApJS,124,181(HI) COMPTEL(1-10MeV,van der Meulen et al. 1998), CANGAROO (7-50TeV, Tanimori et al. 1998, ApJ, 492, L33), Whipple (500GeV-8TeV, Hillas et al. 1998, ApJ, 503, 744), HEGRA (1-20TeV, Aharonian et al. 2000, ApJ, 539, 317), STACEE(Oser et al. 2001, 547, 9490), Milagro (Atkins et al. 2003, 595, 803, background rejection method), HEGRA (500GeV-80TeV, Aharonian et al. 2004,614, 897), HESS (440GeV-40TeV?, Aharonian et al. 2006, 457,899) KOSMA  
G310.8−0.4   Kes 20A S IR MA & color ("the emission that appears plausibly
associated with Kes 20A could be a chance association or a
second-generation association due to younger stars that formed in
a wind-blown bubble generated by the progenitor; the color 0.13/0.13/0.67/1 generally similar to those of photodissociation
N? 26   no CO obs.  
G327.4+0.4   Kes 27 TC HI cloud, X-ray M N? Chen et al.2008, McClure-Griffiths et al. 2001   no CO obs.  
G327.6+14.6   SN1006 S CO (only a possible detection at 2 sigma) N? Dubner et al. 2002, A&A, 387, 1047 CANGAROO 3.8m (Tanimori et al. 1998, ApJ, 497, L25.); Koyama et al. 1995, Nature, 378, 255; Ozaki & Koyama 1998; HESS ("limit",Aharonian et al. 2005, A&A, 437, 135); INTEGRAL (Kalemci et al. 2006, ApJ, 640, L55, --2006, ApJ, 644, 274) 15m SEST  
G329.7+0.2     S OH? IR MA & color ("it is unlikely to be emission from shocked dust and gas") N?->Y 26, ??          
G352.7−0.1     S Interaction with an asymmetric progenitor wind resulting in a ^barrel-shaped ̄ SNR plus viewing angle and projection N? Giacani et al. 2009,A&A,507, 841      
SNR Type: almost come from Green's Catalog of Galactic SNRs, some come from literatures. S: shell type, C: composite type, F: plerion (Crab-like) type, TC: thermal composite (mixed-morphology) type, ?: not classified or not sure yet  
Evidence: chief evidence that suggests the interaction between SNR and MC. LB=line broadening, MA=morphology agreement, H2=vibrational/rotational lines of molecular hydrogen [e.g. H2 1-0 S(1) line (2.12 um), H2 0-0 S(0)-S(7) lines], NIR=Near-Infrared (e.g. [Fe II] line), OH=1720 MHz OH maser, RC=rough morphological correspondence, etc.; see the text in Appendix in 25 for detailed explanations.  
Group: Y=solid, Y?=probable,?=possible, N?=may be not  
References.--(1) Yusef-Zadeh et al. 1996; (2) Hewitt et al. 2008; (3) Serabyn et al. 1992; (4) Yusef-Zadeh et al. 2001; (5) Lee et al. 2008; (6) Yusef-Zadeh et al. 1999; (7) Hewitt et al. 2009a; (8) Claussen et al. 1997; (9) Arikawa et al. 1999; (10) Reach et al. 2005; (11) Green et al. 1997; (12) Reynoso & Mangum 2000; (13) Dubner et al. 2004; (14) Tian et al. 2007b; (15) Zhou et al. 2009; (16) Hewitt et al. 2009b; (17) Su et al. 2009; (18) Frail et al. 1996; (19) Reach & Rho 1999; (20) Reach et al. 2002; (21) Koralesky et al. 1998; (22) Seta et al. 1998; (23) Lee et al. 2009; (24) Su et al. to be submitted; (25) this work; (26) Koo & Moon 1997; (27) Junkes et al. 1992; (28) Reach et al. 2006; (29) Koo et al. 2001; (30) Byun et al. 2006; (31) Shinn et al. 2009; (32) Sasaki et al. 2006; (33) Rosado et al. 2007; (34) Turner et al. 1992; (35) Zhang et al. 2009; (36) Oliva et al. 1999; (37) Paron et al. 2006; (38) Moriguchi et al. 2005; (39) Lazendic et al. 2004; (40) Uchida et al. 1992; (41) Yusef-Zadeh et al. 1995; (42) Lazendic et al. 2002; (43) Green & Dewdney 1992; (44) Yang et al. 2006; (45) Keohane et al. 2007; (46) Leahy et al. 2008; (47) Scoville et al. 1977; (48) Fukui & Tatematsu 1988; (49) Huang & Thaddeus 1986; (50) Feldt & Green 1993; (51) Lee et al. 2004; (52) Routledge et al. 1991; (53) Moriguchi et al. 2001; (54) Ruiz & May 1986; (55) Leahy & Tian 2008; (56) Huang et al. 1983; (57) Wallace et al. 1997; (58) Cho et al. 1994; (59) Kothes et al. 2003; (60) Kothes et al. 2001; (61) Reynoso & Goss 2002; (62) Hines et al. 2004; (63) Oliver et al. 1996; (64) Dubner et al., 1988; (65) Paron et al., 2008; (66) Filipovic et al. 2005.  
Last updated: 16 July 2010
Copyright © Bing Jiang 2010
Bing Jiang/Nanjing University, China/bjiang@nju.edu.cn