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.