Contents of: III/76A/./notes.dat

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## (from tabmap V6.0 (2016-08-18)) 2020-11-28T08:49:54
#---------------------------------------------------------------------------
#-- III/76A Luminous Stars in the Northern Milky Way (LS) (Hardorp+ 1959-1965)
#--------------------------------------------------------------------------
#---Table: III/76A/./notes.dat Remarks originally in volumes II, IV and VI.  (167 records)
#        LS A7     ---   *LS number, as in the file ls.dat
#       Vol I1     ---   *[1/6]  Volume number, as in the file ls.dat
#      Text A71    ---   Text of note
#Note on LS, Vol:
#     Columns are repeated when the note requires several lines.
#-------------------------------------------------------------------------------
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       |V|
       |o|
LS     |l|Text
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+40   1|2|May be B7 II.
+39  47|2|May be cA.
+39  55|2|ADS 14314AB.  The published delta m (Aitken, A New General Catalogue
+39  55|2|of Double Stars Within 120 deg of the North Pole) is so large that
+39  55|2|the observed spectrum must actually be entirely that of the primary.
+39  55|2|The primary is said to be composite in the Henry Draper Catalogue,
+39  55|2|and for this reason the star is given two HD numbers, HD 198287/8.
+39  55|2|The spectrum does not appear composite on our plates, and was charac-
+39  55|2|terized by Hynek (Perkins Contribution 1, No. 10, 1938) as one simu-
+39  55|2|lating compositeness because of high luminosity.  This conclusion is
+39  55|2|almost certainly correct.
+38  17|2|May be B6 Ia.
+38  83|2|May be B7 Ib.
+37  35|2|May be B8 II.
+37  72|2|May be B7 Ir.
+36   8|2|May be B7 II.
+36  11|2|May be cA.
+36  86|2|ADS 14724A.
+35  33|2|ADS 13374A.
+35  61|2|May be B9 II.
+35  73|2|May be cA.
+34  12|2|May be B8 Ib.
+32  15|2|ADS 13335A.
+31   1|2|H-beta in emission.
+31  15|2|The type given here is purely descriptive; among the grounds for
+31  15|2|doubting it is the fact that the spectrum shows no reddening despite
+31  15|2|its low Galactic latitude.  On the plate covering its position, an
+31  15|2|absorption feature which may be H-gamma is strong, while all other
+31  15|2|features, including the Balmer discontinuity, are at the limit of
+31  15|2|visiblity.
+30  17|2|May be B7 II.
+30  37|2|HR 8084.
+29   2|2|May be cA.
+29   5|2|P Cyg type. Strong H-alpha emission.
+29   6|2|Similar to AG Peg.
+29  22|2|May be cA.
+28   2|2|May be cA.
+24  26|2|B7 IV(e), Osawa, Ap. J. 130, 159, 1959.
+22   2|2|May be B8 Ib.
+22   3|2|ADS 12287AB.
+22   6|2|BDS 9287A.
+21   7|2|May be cA.
+17   3|2|ADS 11884A.
+16   4|2|Nucleus of planetary nebula No. 220 in Vorontsov-Velyaminov's catalogue
+16   4|2|(Gaseous Nebulae and New Stars, p. 563 ff. Moscow-Leningrad: Soviet
+16   4|2|Academy of Sciences, 1948).
+16   9|2|Perhaps B7 IIle.
+15   7|6|Weak ultraviolet.
+13   2|2|May be cA.
+13   9|6|Abnormal Balmer decrement.
+13  10|2|May be B6 Iab.
+11   2|2|ADS 12000AB.
+11   2|4|Flat continuum.
+11   3|6|K-line possibly present.
+11   5|2|Only one absorption spectrum is clearly identifiable in this overlap,
+11   5|2|and is assumed to belong to Aitken's component A.
+11   7|6|Weak ultraviolet.
+11   9|6|Ultraviolet also considered weak in this star.
+11  12|6|HR 2370, ADS 5153AB.
+10   2|4|Flat continuum.
+10   8|6|Nebulosity surrounds the star.
+09   3|4|May be composite.
+09  13|6|Precedes BD+09 1332 by only a few seconds of arc.
+09  14|6|ADS 5322AB, also S Mon; the slit classification is presumably for
+09  14|6|component A.
+09  15|6|ADS 5327AB.
+08   2|4|May be A0 I-II.
+08   3|6|May be composite.
+08   8|6|Probably not a true Wolf-Rayet, since Hiltner (Ap.J. Suppl. 2, No. 24,
+08   8|6|1956) refers to this star merely as showing high-excitation emission
+08   8|6|superposed on about an O9 spectrum.
+08  11|6|K-line present.
+08  12|6|Nebulosity surrounds the star.
+07   2|4|May be composite.
+07   7|6|K-line and perhaps 4026 present.
+06   1|6|Appears to be composite.
+06   2|6|K-line may be present.
+06   2|4|Very flat continuum.
+06   5|4|Flat continuum.
+06   6|4|G band possibly visible.
+05   3|4|Rather flat continuum.
+05   6|4|May be composite.
+05  13|6|Probably a double star.
+05  20|6|H-epsilon somewhat enhanced.
+05  21|6|K-line may be present; ultraviolet weak; composite?
+05  25|6|May be composite.
+04   1|4|Weak or variable K-line?
+04   8|6|May be composite.
+04  16|6|Helium I lines appear to be visible.
+04  35|6|K-line may be present.
+03   6|6|May be composite.
+03  12|4|May be composite.
+02  13|6|The small angular separation of this binary star assures that the pub-
+02  13|6|lished spectral type of B0 III:p pertains to the combined light of the
+02  13|6|system.
+02  14|6|Possibly composite.
+02  16|6|K-line may be present.
+01   5|4|May be composite.
+01   8|4|May be composite.
+01  10|4|May be composite.
+00   1|6|AGK2 asumes Aitken's position angle for AC is 180 degrees in error and
+00   1|6|calls this star component C; this seems true on a blue plate, but our
+00   1|6|red (H-alpha) plate supports Aitken.
+00   3|4|Flat continuum.
+00   5|4|Classified only from H-alpha plates.
+00  10|4|May be B8 II.
+00  21|4|Flat continuum.
-00   5|4|May be B7 II.
-00   7|6|May be composite.
-00  15|4|K-line visible?
-00  20|4|Composite?
-01   1|6|ADS 4141AB.
-01  16|6|May be B7 III.
-01  18|4|May be composite.
-02   1|6|ADS 4241ABC; a published spectral type of O9.5 V exists.
-02   3|4|K-line may be variable on our plates.
-02   6|4|May be B8 II-III.
-02  10|6|The published spectral type of B0.5 IV (2) must refer to the combined
-02  10|6|light of both components, in view of their small angular separation.
-02  14|4|May be composite.
-02  28|4|May be B8 II-III.
-03   9|4|Roberts 90.
-03  13|6|A spectral type of O9 V has been published for what is presumably
-03  13|6|component A.
-03  19|6|Flat continuum.
-04   8|4|May be composite.
-04  14|4|Roberts 89.
-04  24|6|May be B7 II-III.
-04  33|4|Roberts 91.
-05   1|6|May be double.
-05  12|6|K-line probably present.
-05  30|4|Composite?
-06   1|6|Nebulosity surrounds this star.
-06   7|4|Roberts 88.
-06  11|4|K-line present?
-06  29|4|K-line present?
-07   3|4|Composite?
-07  17|4|Composite?
-07  18|4|May be B7 II-III.
-07  24|4|May be B8 II-III.
-07  31|4|Flat continuum.
-08  27|4|K-line visible?
-08  29|4|K-line visible?
-09   7|6|Ultraviolet continuum weak.
-09  10|4|May be B7 II.
-09  11|4|Lambda 4686 emission?
-09  29|4|K-line visible?
-10  11|4|ADS 11414A; component B may be A- type.
-10  15|4|May be B7 II-III.
-10  16|4|May be B7 II.
-10  18|4|Composite?
-10  24|4|ADS 11670AB.
-10  29|4|Flat continuum.
-11  14|4|Roberts 85.
-11  15|4|Spectral appearance differs considerably between two plates; may be
-11  15|4|less luminous than OB-.
-11  20|4|Of?
-11  33|4|May be B7 II.
-12   5|4|The published spectral type is taken form Hiltner, but does not check
-12   5|4|with the star's appearance on our plates.
-12  56|4|May be composite.
-12  59|4|Classified only from an H-alpha plate.
-13  16|4|Close pair, both OB stars, originally classified as one star.  The
-13  16|4|magnitude refers to the combined light.
-13  40|4|Roberts 86.
-13  71|4|May be composite.
-14  56|4|Roberts 87.
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