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## (from tabmap V6.0 (2016-08-18)) 2024-03-28T15:02:47 #--------------------------------------------------------------------------- #-- VII/50 CO Radial Velocities Toward Galactic H II Regions (Blitz+ 1982) #-------------------------------------------------------------------------- #---Table: VII/50/./notes.dat Notes & References (260 records) # ID A5 --- Source designation, as in cogal.dat, # or letter A to E for notes on "cosouth.dat" # Text A144 --- Text of note ------------------------------------------------------------------------------------------------------------------------------------------------------ ID |Text -----|------------------------------------------------------------------------------------------------------------------------------------------------ S5 |Weak line (T=3K, V=-18km/s) which does not appear to be associated. S6 |No CO detected. S16 |S16-S20 appear to be related to a single giant molecular cloud complex. S17 |See S16; too many strong (T=15K) lines at various velocities to clearly S17 | associate with the HII region. S18 |See S16. S19 |See S16. S20 |See S16. S21 |May also be part of S16-S20 complex. S22 |T=6K line at V=19km/s may be associated with this object. S24 |Bright dark cloud. S25 |S25, S29, S31, S32 appear to be related to a single giant molecular cloud complex. S27 |eta Oph excites; related to Sco-Cen association. S29 |See S25. S30 |Component at V=17.5km/s is probably associated. S31 |See S25. S32 |See S25. S33 |Bright dark cloud. S34 |Two strong (T=10-15K) lines occur in this vicinity at V=18.1, V=37.5km/s. S36 |Bright dark cloud. S38 |Components at V=26, V=31km/s both appear to be related. S39 |A line at T=7K, V=39.0 is not obviously associated. S40 |Two strong lines T=12K, V=17.3km/s; T=10K, V=30km/s are present. S40 | Low velocity line seems more closely associated; may be part of S45 complex. S41 |May be part of S045 complex. S42 |Two T=6K lines at V=25, V=28km/s are present, but needs mapping to show association with HII region. S43 |Two strong (T=11K) lines at V=18, V=40km/s are present. Needs mapping. Possibly related to S45 complex. S44 |Possibly related to S45 complex. S45 |Quoted line width is 13CO line width. Possibly related to S40, S41, S43, S44. S52 |Note that the Sharpless position is incorrect; should be RADEC_1950=19 43 35 -23 15 00. S55 |There is a weak (T=4K) line at V=50km/s, which is close to the H{alpha} velocity of 46km/s (ref 36), S55 | but the sources needs to be mapped to show an association. S56 |Velocity assignment is based on H{alpha} [ref 36] velocity. There are other strong lines in this vicinity. S57 |Although the 99km/s component reaches a maximum in the vicinity of the HII region, the very large velocity S57 | and the difference between the CO and H{{alpha}} velocity [ref 22, 55] make velocity assignment doubtful. S60 |Although there are other observed components, the V=44km/s component is most closely associated S60 | and is near the H{alpha} velocity [ref 55]. S62 |There are several weak features with 2.6<V<=13.5km/s and 25<T<=5K. S63 |Bright dark cloud. S66 |At least five lines with 8 < V=< 120km/s. S67 |Although the detection seems convincing, the high velocity is significantly different from the H{alpha} S67 | velocity (ref 58) and must be considered doubtful. S68 |Blair et al. [ref 6] found a bright cloud near the HII region, but its brightest part is almost a degree S68 | away. We found only weak lines near the position of the HII region, but with a velocity similar to that S68 | of Blair et al. It appears that the optical HII region may be a background object, and the cloud is S68 | visible only in relief against the HII region. No H{alpha} velocity is available. S70 |Bright dark cloud. S71 |Possible CO detection T=4K, V=33.0km/s but not definitely associated. S74 |The V=48.1km/s component is almost certainly related but there is an additional moderately strong line S74 | at V=13km/s, which is probably a foreground cloud. S75 |There is line at V=29km/s which is the only component present but there is S75 | no clear association wIth the HII region. S76 |There are components at V=29 and V=34km/s. Both may be associated, but the S76 | 34km/s component seems more closely associated with the nebula. S79 |There is a T=4k line at V=15.7km/s, but not clearly related to the HII region. S80 |No CO detected; listed as a planetary but may be the shell of a Wolf Rayet star. S81 |Bright dark cloud. S87 |Appears related to S88. S88 |See S87. S90 |Uncertainty in CO velocity is estimated. S91 |A T=1.2K line at V=19.7km/s occurs in this vicinity but does not appear to be related to the complex S95 |No CO detected. S99 |Appears related to S100; error in CO velocity is estimated. S100 |See S99. S101 |There is another moderately strong component at 6km/s. The 13.7km/s component is more closely associated S101 | with the ionization front and is nearly equal to the H{alpha} velocity [ref 22,55]. S103 |There is associated CO at V=11km/s. T=20K [ref 53]. S108 |Strong emission from several lines with -12 < V=< +7 and V=45km/s. S109 |Too large to find dust clouds which appear to be interacting. S115 |Several lines were detected with -20 < V=< +6km/s. S116 |Weak CO line at V=-10.6km/s, not necessarily associated. S120 |The H{alpha} velocity is -74.4km/s [ref 55]. Therefore, in spite of the weakness of the line, S120 | it appears to be associated with the HII region. S121 |CO appears to be definitely related in spite of the weakness of the line, especially since it peaks at S121 | the position of the HII region. S125 |Line width quoted is for 13CO. S128 |Listed as planetary nebula, Abell 63, in [ref 48], but the strength of the CO line and its clear S128 | association with the nebula suggest that object has probably been misidentified. S131 |The best estimate of the velocity is 0+-5km/s, but the object needs extensive mapping to determine the S131 | velocity accurately. Small scale mapping shows clouds, each apparently associated with the HII region S131 | with velocities of -1, -1.6, +1.0 and -8km/s. S133 |A line of T=2K, V=0.8km/s was found but is not obviously related. S135 |Israel's [ref 30] velocity of -20.8km/s differs from that of Blair et al. [ref 6] S135 |by 4km/s. We observed three positions near the eastern peak of Blair et al. and S135 |obtained a mean velocity of -20.7+-0.4km/s. The reason for the discrepancy S135 |between Israel and Blair al. is unclear and we adopt our values for consistency. S136 |Bright dark cloud. Weak emission (T=3K, V=2.6km/s) was found but does not appear to be related to S136 | the clearly evident obscuration. S139 |Although there are a few weak components at other velocities, the velocity assignment is confirmed S139 | by H{alpha} measurements [ref 22, 55]. S140 |The error in the CO velocity is estimated S141 |The velocity assignment is based on the H{alpha} velocity of -64.6km/s [ref 55]. S141 | There is a foreground cloud at V=-7km/s, which has a small intensity variation S141 | near the position of the HII region. S143 |CO observgtions were not made at the optimum position. S144 |There are weak (T<2K) lines at V=-52km/s, but there is no evidence that they are associated. S147 |See S149. S148 |See S149. S149 |Related to S147 and S148. S152 |Probably related to S153. S153 |See S152. S154 |Distance given is the mean of both determinations. S157 |Error in CO velocity is estimated. S159 |Error in CO velocity is estimated. S160 |There is a component at V=-30.6+-1.0km/s which may be related, but other components are also present. S161 |There appear to be two HII regions in the same line of sight. There are two widely separated velocities S161 | for the CO clouds, and both lines are strong. Furthermore, the H{alpha} spectrum [ref 55] shows two S161 | velocity components at V=-44.8 and V=-8.9m/s, each close to the CO velocities. It is unclear S161 | which HII region is at the distance given by ref. 8. S162 |Although the line is weak, the velocity assignment is made on the basis of agreement with the H{alpha} S162 | velocity [ref 22]. S163 |There are two almost equally strong lines at V=-40 and V=-47km/s both of which appear to be related to S163 | the HII region. The given velocity is the weighted mean of all the CO data. S166 |Weak lines (T<1K) at V=-48.7km/s are near the H{alpha} velocity [ref 55], but are too weak to conclude S166 | they are associated. S168 |Apparently related to S169. S169 |See S168. S170 |Other weak components (T<3.5K) near zero velocity are unrelated. S170 |This is confirmed by H{alpha} velocity [ref 22, 55]. S171 |Velocity structure is too fragmented and chaotic to get good center of mass velocity without complete mapping. S174 |Because of high latitude, we expect any CO detected to be related to the emission nebula in spite of S174 | the weakness of the line. S178 |Bright dark clouds. S179 |Weak lines at V=-22 and V=-53.8km/s. S183 |Bright dark cloud. S185 |It is not clear whether the CO is associated. S186 |The error in the CO velocity is estimated. S189 |There are weak lines at -9 < V=< 0km/s, but none appear to be associated. S191 |Weak lines at -43 < V=< 0km/s. None appear to be associated. S192 |S192, S193, S194 appear to be related to a single molecular complex. S193 |See S192. S194 |See S192. S195 |Weak lines (T<1.7K) with -12 < V=< 10km/s all of which are probably unrelated. S196 |Possibly related to S192-S194 complex. S197 |A weak line at T=< 1.5K, V=-1.7km/s is probably unrelated. S198 |A few weak T=< 2K lines are present but almost surely are unrelated. S199 |Error in CO velocity is estimated. S202 |There are two components, equally strong at V=-13.5 and V=-10km/s. S202 | Both are probably related to the HII region. S203 |There are numerous moderately strong (T=6K) lines over a wide range of velocities S203 | in the positions we searched. S205 |Probable velocity assignment based on H{alpha} [ref 55] velocity. There is another line present S205 | at one position at V=-7km/s which is probably foreground. S206 |There are two components with T=6K at V=-6, V=-26. S207 |No CO detected; extensively searched. S209 |Velocity assignment based on Em velocity [ref 55]. Another line is present at V=-25km/s, T=4K. S210 |There are weak lines with -33 < V=< -3km/s, none is clearly associated. S211 |The component at V=37.6km/s peaks directly on the HII region. Another component at V=0km/s, S211 | T=5K is also present and appears to be due to a foreground cloud. S215 |There are weak lines at V=-7.8+-0.4 and -1.6+-0.3km/s; Neither is clearly associated. S216 |There are weak lines at V=-4.7+-0.7 and +4.6+-0.4km/s; Neither is clearly associated. S218 |Bright dark cloud S220 |The velocity is the center of mass velocity of the extended molecular complex. S220 | Interaction of the association members with the HII region and molecular cloud S220 | indicates S220 is related to Per 0B2 cloud mapped by [3,50]. In immediate vicinity S220 | of S220, [20] finds V(CO) -3.8+-2.0km/s, T=15K at RADEC(1950) =03 53 28 +36 59 56. S221 |CO detected at V=-14.7+-0.7km/s, T=3K; V=-7.2+-0.5, T_A=5K. S223 |No CO detected. S224 |Distance may not be meaningful because the observed stars may not be responsible S224 | for the ionization. Possible detection at V=-3km/s S229 |The CO cloud may not be related to the HII region. S230 |Large diffuse nebula probably related to S229, S236, S234, and S237. S232 |There are other weak unrelated components. S239 |Part of the Taurus dark cloud complex. S243 |There are two components present at V=+5.3 and 2.1km/s. It is unclear whether S243 | one or both are related to the HII region. S245 |Weak (T=1K), narrow lines at V=6, 7.5km/s. It is unclear whether they are associated with the HII region. S246 |Bright dark cloud. S248 |V(CO)=2.8+-1.0km/s [ref 15]. S254 |S254, S255, S256, S257, and S258 are all related to a single giant molecular cloud complex. S255 |See S254. S256 |See S254. S257 |See S254. S258 |See s254. S261 |Distance given may not be meaningful because stars may be unrelated to the ionization. S261 | Possibly associated CO at V=11.3+-1.8km/s. S265 |Bright dark cloud. S267 |Probable CO detection at T=1.6K, V=11.6+-0.5km/s. S271 |Related to S272. S272 |See S271. S274 |No CO detected. S276 |Related to Orion A complex (S281) and Ori OB1 association. S277 |See S281; Part of Ori OB1. S278 |See S281; Part of Ori OB1. S279 |See S281; Velocity is center of mass velocity for the associated giant molecular cloud complex; S279 | Part of Ori OB1. S280 |There are two lines present; V=24km/s, T=2.9K, V=11km/s, T=2.1K. S281 |Related to S276, S277, S278, S279; velocity is center of mass velocity for the associated giant molecular S281 | cloud complex. Temperature and line width are for BN-KL object; Part of Ori OB1. S282 |In spite of its weakness, the given velocity component appears to be related to the HII region. S282 | It is also close to the H{alpha} velocity [55]. S290 |No CO detected. S291 |There is a weak line (T=1.5K, V=32.1km/s) not obviously related to the HII region. S292 |Related to S293, S295, S296, S279. S293 |See S292. S295 |See S292. S296 |See S292. S297 |See S292. S298 |Wolf-Rayet Shell source; CO has three widely separated components [ref 52]. S298 | CO velocity is estimate of center of mass velocity and is quite uncertain. S298 | Velocity components at V=37, 54 and 67km/s, but 37km/s component is most massive. S303 |Related to S308. S306 |Weakness of the line and proximity in space and velocity to S305 may mean that the S306 | CO is not related to this HII region, but is part of the complex related to S305. S308 |Possible 1K line at V=37.3; Wolf-Rayet shell source, related to S303. S310 |Related to VY CMa. S312 |Too large and diffuse for meaningful observations. S313 |No CO detected; extensively searched. # BFS2 |Source consists of 3 closely spaced HII regions each 1' diameter. BFS3 |Cluster of stars with small (~20") circumstellar emission. BFS5 |There are many lines present. BFS6 |There are other weaker components present in the spectra. BFS7 |There is an apparently local feature at T=3.2K , V~0.7km/s. The region needs to be BFS7 | mapped or an H{alpha} velocity needs to be obtained to assure association. BFS8 |There are two components present at V=-51.2km/s, T=8K and V=-58km/s, BFS8 | T=4K both of which appear to be associated. BFS10|There is a T=5K line near 0 velocity, but it shows no intensity variation BFS10| with position as the high velocity line does; probably a foreground feature. BFS12|The line is weak, but is strongest at the optical center of the HII region. BFS14|Probably related to S156. BFS15|Probably related to S156. BFS16|Probably related to S156. BFS17|Probably related to S156. BFS18|Probably related to S156. BFS19|Probably related to S156; a few weak (T < 1K) lines near V=-52km/s are BFS19|probably outer parts of cloud related to 18, 14-17. BFS22|Weak line at V=-2.8km/s, T 1K is present but is probably not associated. BFS23|Many weak lines. BFS26|Cluster of stars with red nebulosity each 1' diameter. BFS26| The entire region is 4' in diameter. BFS27|A line at V=2.3km/s is as strong as T=4K , but is probably unrelated. BFS28|Probably related to S202. BFS29|Probably related to S202. BFS32|Listed as a planetary nebula in referance 45, but the strength of the BFS32| CO and its clear association with the nebula suggest that the object BFS32| has probably been misidentified. BFS35|With BFS36, there are diffuse circular nebulae which appear to be part of a BFS35| single bright dark cloud. BFS36|See 35. BFS37|Related to BFS38, BFS39, BFS41. BFS38|See 37. BFS39|See 37. BFS40|Weak (T < 1.3K) lines at V=0.3 +/- 0.4km/s. BFS41|See 37. BFS42|CO not definitely related. BFS43|There are two lines (V=-15km/s, T=2.5K; V=-30km/s, T=3.5K) present. BFS43| It is unclear if they are related to the nebula. BFS44|A component at V=4.2km/s, T=4-5K is also present, but does not vary in BFS44|intensity across field. Almost surely foreground. BFS46|Probably related to BFS47. BFS47|See BFS46. BFS52|Group of 3 HII regions/reflection nebulae. BFS56|Probably related to BFS57. BFS57|See BFS56, BFS59. BFS59|May be related to BFS57. A |Observed in 1975. There may be a systematic difference in T between these sources and others. B |10micron infrared source (Frogel and Persson 1974ApJ...192..351F; Persson et al. 1976ApJ...208..753P) C |40-350micron infrared source (Furniss et al. 1975ApJ...202..400F; Emerson et al. 1973ApJ...184..401E) D |Observed over a 118km/s velocity range. E |Orion has a measured T=45K when observed with the AAT, consistent with T=70K when observed with a 1'-beam. ------------------------------------------------------------------------------------------------------------------------------------------------------