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## (from tabmap V6.0 (2016-08-18)) 2024-04-20T02:02:03
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#-- II/20A UBV Photometry of O and B Stars in Vela (Denoyelle 1977)
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#---Table: II/20A/./remarks.dat Original remarks (added in July 2016) (120 records)
# m_Seq I1 --- [1/5]? Multiplicity index to star
# Seq I3 --- [1/358] Running number
# Text A209 --- Text of note (original notes in "remarks.dat",
# notes added at CDS about problematic star
# identification in "notes.dat")
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m| |
_|Seq|Text
-|---|-----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------
| 3|Considerable differences suggest variability (or wrong identification?): V=11.54 and 12.84 at La Silla and 12.63 at Boyden; B-V=1.33 and 0.36; only one measurement for U-B.
| 7|Spectral type B1V according to Buscombe and Kennedy, with variable radial velocity.
| 8|IDS 08215-4227 (d=0.4"); measured together.
| 9|IDS 08216-4359AB (d=11.8"); our data refer to the component A.
| 23|IDS 08254-4215 (d=68.5"); the brighter component was measured. A difference of 0.24mag in V was noted between the Boyden and the La Silla values.
| 24|IDS 08257-4350 (d=0.3"); measured together.
1|027|Two stars of almost equal brightness; 1027 is situated NW of 2027.
2|027|Two stars of almost equal brightness; 1027 is situated NW of 2027.
1|031|Known physical binary IDS 08277-3844AB (d=4.4"). Spectral type as given by Hiltner et al. is B4V.
1|031|Star 1031 refers to the component A, measured at La Silla; 2031 concerns the whole system, measured at Boyden.
2|031|Known physical binary IDS 08277-3844AB (d=4.4"). Spectral type as given by Hiltner et al. is B4V.
2|031|Star 1031 refers to the component A, measured at La Silla; 2031 concerns the whole system, measured at Boyden.
| 33|IDS 08283-4142 (d=1.8"); measured together. _
| 35|IDS 08289-4345 (d=1.7"); measured together. (The fainter component is of the order of 14th magnitude).
| 38|The Boyden values (V=14.20, B-V=+1.82, no U-B) were discarded, as they probably refer to another star.
| 49|IDS 08355-4004 (d=0.6") measured together.
1|050|The fainter component is situated SW. 1050 is the brighter component, 2050 refers to the combined light.
2|050|The fainter component is situated SW. 1050 is the brighter component, 2050 refers to the combined light.
1|051|IDS 08366-3954 (d=3.8"); 1051 is the brighter component, 2051 refers to the combined light.
2|051|IDS 08366-3954 (d=3.8"); 1051 is the brighter component, 2051 refers to the combined light.
| 56|Only faint emission lines are visible on the blue plates, but a strong H{alpha} emission line is seen on the red plate. The identification is uncertain.
| 57|IDS 08410-4055AB (d=4.4") measured together.
| 62|Two discording Boyden values of U-B (-0.10 and +0.00) were neglected.
| 66|The Boyden value U-B=-0.02 was discarded.
| 76|IDS 08473-4323 (d=2.0"), measured together. Stephenson and Sanduleak give for the spectrum B1.5Iab, as mentioned in the second place by Jaschek et al.
| 82|The value U-B=-0.60 (La Silla) was discarded.
| 85|IDS 08515-4305 (d=2.0"), measured together.
| 87|The value U-B=+0.03 (Boyden) was discarded.
| 90|IDS 08535-4252 (d=3.1") measured together.
1|095|Two stars of about the same brightness; not measured at Boyden. 1095 is situated approximately 6"E of 2095.
2|095|Two stars of about the same brightness; not measured at Boyden. 1095 is situated approximately 6"E of 2095.
| 96|Measured together with a small companion at the WSW.
| 97|Spectrum B3Vne according to Stephenson and Sanduleak.
| 99|Spectrum B0.5Ib according to Stephenson and Sanduleak, also given in the second place by Jaschek et al.
|105|IDS 09041-4414 (d=0.3") measured together.
|109|The Boyden value V=10.81 was discarded. Combination with La Silla measurements would yield V=10.68.
|114|The Boyden value V=11.26 was discarded.
|115|Spectrum BSIa according to Hiltner et al.
|117|IDS 09088-4312ABC (d=0.1" for AB, d=2.8" for AB/C); only measurements of the whole system (ABC) at La Silla.
1|119|IDS 09107-4249 (d=5.8"); spectrum B4V according to Hiltner et al. 1119 refers to the brighter component; 2119 to the combined light.
2|119|IDS 09107-4249 (d=5.8"); spectrum B4V according to Hiltner et al. 1119 refers to the brighter component; 2119 to the combined light.
|121|IDS 09124-4429 (d=6.8"); the influence of the companion (14th magnitude) is negligible.
1|128|Two stars about 6" apart in declination. 1128 is the southern component.
2|128|Two stars about 6" apart in declination. 1128 is the southern component.
|140|The Boyden value U-B=+0.71 was discarded.
|141|For V only the Boyden value and for U-B only one measurement of La Silla was retained.
|142|IDS 09248-4504AB (d=9.3"); our data refer to the component A only.
|143|The Boyden value for U-B was discarded, because of a too great uncertainty.
|145|The Boyden value for U-B was discarded, because of a too great uncertainty.
|146|The Boyden value for U-B was discarded, because of a too great uncertainty.
|149|The physical binary IDS 09302-4834 (d=2.6"), measured together. According to Hiltner et al. the spectrum is B4IV.
|156|According to Hiltner et al. the spectrum is B2IV-V.
|159|The Boyden value V=8.82 was discarded; possible variability because of the emission feature.
|165|The blue plates show faint emission lines, but the H{alpha} line presents a strong emission on the red plate.
|165|This object is listed as no. 275-4.1 = PB4 in the "Catalogue of the Planetary Nebulae" (Perek and Kohoutek). In our opinion, possibly a Wolf-Rayet star (class WN5?).
|169|Listed as no. 275~3.1 = He2-25 in the "Catalogue of Planetary Nebulae" (Perek and Kohoutek). In our opinion possibly a Be star.
1|170|1170 is the brighter component. (Companion to the N.)
2|170|2170 refers to the combined light.
|172|Hiltner et al. give B5V for the spectral type.
1|177|A companion to the S. 1170 refers to the brighter component, 2177 to the combined light.
2|177|A companion to the S. 1170 refers to the brighter component, 2177 to the combined light.
|179|The measurements at La Silla are quite dubious (V=11.88, B-V=038, U-B=+0.29) and were discarded.
|183|Jaschek et al. give as second value for the spectral type B0IV.
|188|IDS 09213-5341 (d=2.4") measured together.
1|197|Probably considered as an OB star because of blending of the spectra. 1197 lies NW of 2197, both measured at La Silla, 3197 (N of 1197) was measured at Boyden.
2|197|Probably considered as an OB star because of blending of the spectra. 1197 lies NW of 2197, both measured at La Silla, 3197 (N of 1197) was measured at Boyden.
3|197|Probably considered as an OB star because of blending of the spectra. 1197 lies NW of 2197, both measured at La Silla, 3197 (N of 1197) was measured at Boyden.
1|207|A companion to the NE. 1207 refers to the brighter component, 2207 to the combined light.
2|207|A companion to the NE. 1207 refers to the brighter component, 2207 to the combined light.
1|208|A faint companion to the N. 1208 refers to the brighter component, 2208 to the combined light.
2|208|A faint companion to the N. 1208 refers to the brighter component, 2208 to the combined light.
|212|Jaschek et al. give as second spectral classifiation: B1V:pe.
|220|Two stars 10" in declination apart, with overlapping spectra. Not measured.
|221|The Boyden value U-B=1.14 was discarded.
1|223|IDS 09347-5413 (d=3.6"); 1223 refers to the brighter component, 2223 to the combined light.
2|223|IDS 09347-5413 (d=3.6"); 1223 refers to the brighter component, 2223 to the combined light.
5|228|The planetary nebula 274+2.2 = He 2-35 in the catalogue of Perek and Kohoutek.
|239|IDS 09431-5230 (d=3.9") measured together.
1|242|IDS 09435-5135 (d=6.4"); 1242 refers to the brighter component, 2242 to the combined light.
2|242|IDS 09435-5135 (d=6.4"); 1242 refers to the brighter component, 2242 to the combined light.
|249|IDS 09477-5243AP (d=0.2") measured together.
|255|According to Hiltner et al. the spectrum is B1IV, or according to Jaschek et al. B1V.
|261|Hiltner et al. give a spectral type B2V.
1|264|Three different stars in the Vicinity of the planetary nebula 280-2.1 = He 2~38 (on our plates very difficult to identify).
1|264|The blue plate shows many emission lines and suggests a Wolf-Rayet type star (WN5??). 2264 is situated N of 1264 and 3264 W of 1264.
2|264|Three different stars in the Vicinity of the planetary nebula 280-2.1 = He 2~38 (on our plates very difficult to identify).
2|264|The blue plate shows many emission lines and suggests a Wolf-Rayet type star (WN5??). 2264 is situated N of 1264 and 3264 W of 1264.
3|264|Three different stars in the Vicinity of the planetary nebula 280-2.1 = He 2~38 (on our plates very difficult to identify).
3|264|The blue plate shows many emission lines and suggests a Wolf-Rayet type star (WN5??). 2264 is situated N of 1264 and 3264 W of 1264.
|268|IDS 09518-5334(d=8.7" in declination). Probably considered as an OB star because of overlapping spectra.
|272|Measured with a faint companion to the SW.
|273|IDS 09534-5406 (d=37.2"). Our values refer to the bright component. The spectral type is B5Ib according to Hiltner et al.; B5II is given as second value by Jaschek et al.
|275|According to Hiltner et al. the spectral type is B3IV.
1|282|Overlapping spectra render the identification troublesome. 1282 refers to the southern star and was measured at Boyden; 2282 was measured at La Silla.
2|282|Overlapping spectra render the identification troublesome. 1282 refers to the southern star and was measured at Boyden; 2282 was measured at La Silla.
1|288|The companion is situated to the E. 1288 refers to the brighter component; 2288 to the combined light.
2|288|The companion is situated to the E. 1288 refers to the brighter component; 2288 to the combined light.
|291|The deviating value V=10.68 (La Silla) was discarded.
1|297|Probably two OB stars with spectra partly overlapping in right ascension. 1297 was measured at La Silla, 2297 at Boyden.
2|297|Probably two OB stars with spectra partly overlapping in right ascension. 1297 was measured at La Silla, 2297 at Boyden.
|302|P Cygni type. The colours, derived at Boyden and La Silla are identical, but the V magnitudes differ;
|302|V=8.69 (La Silla, without a faint companion to the SE) and V=9.03 (Boyden, with companion). Maybe variable in V?
|305|V and B-V are well-determined. U-B is doubtful both for La Silla (=0.71) and for Boyden (=1.02).
|310|Hiltner et al. give B3IV for the spectral type, Jaschek et al. give also B2V.
|322|Spectral type BSIab according to Humphreys.
|326|Not measured but numbered on the spectral plates because of its peculiarity. Later on identified as the planetary nebula 278+5.1 = PB6 ("Catalogue of Perek and Kohoutek").
1|328|Difficult to identify: 1328 (measured at La Silla) is probably the wrong star; 2328 was measured at Boyden.
2|328|Difficult to identify: 1328 (measured at La Silla) is probably the wrong star; 2328 was measured at Boyden.
|334|According to Hiltner et al. the spectral type is B2IV-V.
|337|According to Humphreys the spectral type is B1Ia; U-B disagrees considerably between Boyden (-0.65) and La Silla (-0.29).
|341|U-B=+0.77 (La Silla) and +1.46 (Boyden). Intended to be the star 115 in the list of Graham and Lynga; this star is, in our opinion, no OB star and is not mentioned in the catalogue of Stephenson and Sanduleak.
|341|Our star is very close to their star and showed (questionable) traces of emission on the blue plate. The red plate indicated later on, a very late spectral type.
|347|The eclipsing binary HP Car = IDS 10160-5654 (d=0.4"); V=8.72 (Boyden) and 8.90 (La Silla).
1|349|IDS 10172-5532AB (d=7.2"). 1349 is the component A (measured at La Silla), 2349 refers to the combined light.
1|349|According to Buscombe and Kennedy the type is BSIVe, Hiltner et al. give B3III and Jaschek et al. give also B3IV and BSIII-IV.
2|349|IDS 10172-5532AB (d=7.2"). 1349 is the component A (measured at La Silla), 2349 refers to the combined light.
2|349|According to Buscombe and Kennedy the type is BSIVe, Hiltner et al. give B3III and Jaschek et al. give also B3IV and BSIII-IV.
|350|IDS 10189-5710 (d=1.6"), measured together.
|354|IDS 10203-5657 (d=2.9"), measured together.
|358|Jaschek et al. give also B4I.
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