Contents of: VII/50/./notes.dat

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## (from tabmap V6.0 (2016-08-18)) 2020-02-26T02:02:08
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#-- VII/50 CO Radial Velocities Toward Galactic H II Regions (Blitz+ 1982)
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#---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
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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.
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