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## (from tabmap V6.0 (2016-08-18)) 2024-05-07T14:32:25
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#-- V/73A Emission-Line Stars of the Orion Population (Herbig+ 1988)
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#---Table: V/73A/./remarks.dat Remarks (591 records)
# HBC I4 --- object HBC identification
# Cont A1 --- [a-g] Non-blank when several lines.
# reftext A121 --- remark text
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HBC|t|reftext
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324| |MC 1 . The position listed in the catalog (0 04 33.84 +65 22 32.2) corresponds to a nearby star MacC A.
324| | The position was corrected on 06-Jan-2008 at CDS (thanks to Tigran Yu. Magakian, Byurakan Obs., Armenia).
3| |V633 Cas . The spectral type is uncertain. Infrared observations are in [2,3,32,71,82,91,316].
329|a|VX Cas . There was some uncertainty in the identification of this star in the earlier literature. The coordinates
329|b| and other data in Table 1 refer to the star indicated as VX Cas in Aarhus Medd. no. 10, 150 (1937), Kasan Bull.
329|c| 26 (1951), Bull.A.F.O.E.V. 6, 93 (1937), Perem.Zvzd. 22, 9 (1983). It may be an Ae/Be star although there is no
329|d| bright nebulosity nearby.
330|a|V594 Cas . The absorption spectrum is confused by line emission; the types assigned range from O9.5 to B8,9:
330|b| see [138].
7| |LkH@ 201 . This is probably a background Be star.
334|a|RNO 6 . The photometry is of the star in the brighter lobe of this reflection nebulosity. A polarization
334|b| map is in [420].
8|a|LkH@ 262 . LkH@ 262, 263 are separated by about 15" in 22# . They and LkH@ 264 lie in L1457, but are not to be
8|b| identified with the X-ray source in that cloud found by Halpern and Patterson, Ap.J. Lett. 312, L31, 1987.
9|a|LkH@ 263 . (See remark for LkH@ 262.)
336|a|IRAS 0313 . This nebulous star was observed at the request of Iyengar. An underexposed Lick coude spectrogram in
336|b| 1986 showed only strong double H@ emission (R>V) on a weak continuous spectrum.
338|a| LZK 4 . A 1983 Lick coude spectrogram of the red region shows an unusually broad, structured H@ emission with
338|b| a reversal displaced somewhat shortward of center. A few weak absorption lines are present, and the D lines are
338|c| fairly strong, but Li I 6707 is not apparent. The type was classified as mid-K by [118a].
346|a|SSV 13 . No stellar absorption spectrum can be seen with certainty; H@, [O I] and [S II] are very strong, as in
346|b| H-H Objects [160].
348|a|IP Per . It is not certain if this is a pre-main sequence star. Two Lick coude spectrograms (1973, 1981)
348|b| showed strong, structureless H@ emission upon broad, stellar absorption wings. The only other stellar features
348|c| present were broad Na I D lines.
20| |LkH@ 330 . The spectral type is not well determined; a Lick coude spectrogram was classified as "about F6".
349|a|XY Per e . The star illuminates a large reflection nebula. XY Per is ADS 2788; coordinates and photometry refer
349|b| to the combined light. There has been no change in the relative position since 1904; the mean separation is
349|c| 1".35, p.a. 75#. The photometric range is so large that both components must be variable; the magnitude
349|d| differences noted by the double star observers can account for only a fraction of the amplitude [47]. The
349|e| eastern star (B) was the fainter at all the Lick observations (1961-73). It was earlier classified as B6,
349|f| but superior modern material indicates middle A in the blue, but late B in the red. The v sin i quoted is
349|g| from the metallic spectrum. There are fairly strong, double emission cores in the H@ absorption line.
350|a|XY Per w . The western star (A) has a peculiar spectrum. Originally called A2 II (Herbig 1952), modern coude
350|b| spectrograms show sharp, double core structure in Ca II K and the higher Balmer lines; this structure is
350|c| variable with time. The Fe I lines are the widest species (v sin i = 120-140 km/s), and suggest a type of
350|d| A2 or A5. Lines of Fe II and Ti II are narrower and strong; Ti II 3685, 3759, 3761 are prominent, as in
350|e| shell spectra. Broad central emission, divided by a central reversal, is present in H@. Weak, broad He I
350|f| absorption lines suggest a late B type.
355|a|NTTS 035135. Weak emission cores are present in the H,K lines but H@ is absent, presumably being filled-in to the
355|b| level of the continuum.
356|a|NTTS 040012. NTTS 040012+2545N and S are separated by about 1". The coordinates, photometry etc. are for the combined
356|b| light. The Li I 6707 is observed in the combined spectrum.
357| |NTTS 040012. (See remark for preceding star.)
363|a|PP 13 s . The s, brighter lobe shows a scattered M-type spectrum with prominent [O I], [S II] but no H@. The
363|b| illumination is from a heavily obscured infrared source near the ne edge. The n lobe is nearly stellar, and has a
363|c| T Tauri-like spectrum. The coordinates in both cases refer to the infrared peaks. Note this is PP 13, not Par 13.
364| |PP 13 n . (See remark for preceding entry.)
365|a|LkCa 1 . The radial velocitites of both [212] and [192] are well off that expected for a star associated with the
365|b| Taurus clouds.
366|a|Anon 1 . This is the "nebulous star 11' in 300 from HD 283447" of [212]. It is identified on the chart for
366|b| LkCa-1 in [219].
367| |V773 Tau . According to [408], there is a cyclic variation of 10.62-10.76 (in V) with period 3.43 days.
25|a|CW Tau . The radial velocity value quoted is from [189], but the velocity may be variable [123]. The [O I],
25|b| [S II] lines are unusually strong. The spectrum is discussed or reproduced in [93,123,404,458,500].
369|a|FO Tau . This is the star 2 mm north, 22 mm east of HD 283447 on the chart for the latter star in [410]; it is
369|b| also identified in [257]. The identity with the Haro s6-2 of [93] was confirmed by M. Cohen.
29|a|V410 Tau . Additional UBVRI observations are in [220,236,390,410]. A cyclic variation 10.82-11.04 (in V) with
29|b| period 1.92 days is present [408]. The radio source at the star is variable: [34,96,101,305].
373|a|Elias 1 . This is the star 6 mm north, 5.5 mm east of CZ Tau on the chart for that star in [410]; it is also
373|b| identified in [93]. It was discovered originally as an infrared source by D. A. Allen (private comm.).
374|a|Hubble 4 . This is the nebulous star 9 mm north, 9 mm east of CZ Tau on the chart for that star in [410]; it is
374|b| also identified in [93].
375| |CoKu Tau/1 . This star is 10 mm north, 12 mm east of CZ Tau on the chart for that star in [410].
377|a|FQ Tau . The star is identified in [182]; it is also identifiable as the image 9 mm north, 9 mm west of
377|b| "WK X-ray 1" on the chart for that star (V819 Tau) in [410].
32|a|BP Tau . [492] found a cyclic variation 12.07-12.27 (in V) with period 7.6 days. High-resolution line profiles
32|b| are shown in [340,423], and lower resolution spectra in [93,212,303,458].
378| |V819 Tau . According to [409], there is a cyclic variation with period 5.59 days.
34|a|RY Tau . The historical light curve is in Kholopov, Perem. Zvzd. 13, 430, 1961, and in [534]. Additional UBV/RI
34|b| observations are in [220,225,227,229,266,281,284,410,492,511,528]. Observations of H@ are in [91,93,123,220,282,
34|c| 423,531], of the spectrum in [123,220,281,294,303,340,423,458], and of the variable nebulosity in [206]. Velocity
34|d| variation was suspected in [212]. Extensive Lick observations gave inconsistent results: 1977-78, the velocity
34|e| scattered between +5 and +30 km/s (14 plates); 1978-79, constant at +20.0 % 1.0 km/s (12); 1979-80, constant at
34|f| +18.3 % 1.5 km/s (8). The higher-accuracy observations of [189] gave an apparently constant value of +16.5 % 2.4
34|g| km/s in 1981-85. The possibility that the star is an unresolved double was raised by [353].
380| |HD 283572 . The light varies sinusoidally in a period of 1.548 days [505].
381|a|Haro 6-5B . Haro 6-5B is a very red, presumably stellar source (probably a T Tauri star: [99,347]), in the sw corner
381|b| of a triangular reflection nebulosity 15" west of 6-5A [158,345,347]. It is not clear if the infrared colors [490]
381|c| apply to 6-5B or include another source to the ne [158].
35|a|T Tau . The most extensive published light curve is in Lozinsky, Perem.Zvzd. 7, 76, 1950. Additional UBV/RI
35|b| observations are in [168,220,225,229,236,266,284,410]. Evidence for a photometric period of 2.80 days is in
35|c| [228]. Low-resolution spectroscopy is in [93,168,303,312], medium in [290,458], and high resolution profiles in
35|d| [187,337,340,423]. Values of W(H@) ranging from 38 to 80 A have been reported [91,93,236]; the Table value is a
35|e| compromise. Optical observations of the companions are in [121,352,424], radio structure and coordinates in [424,
35|f| 425], and optical astrometry in [180]. The history of the nebulae associated with T Tauri is given in [59] and
35|g| references therein.
386|a|FV Tau . An occultation observation by M. Simon (unpublished) shows the star to be double, with separation
386|b| 0".56 projected upon p.a. 55#; the K magnitudes are 8.05 (eastern) and 8.50 (western component).
387| |FV Tau B . The quoted coordinates correspond to a separation from FV of 12" in 105#.
36|a|DF Tau . The profile of H@ is shown in [123,187,423]. The spectrum is reproduced or described in [93,
36|b| 123,187,303,413,423,458,500]. An occultation observation shows the star to be double, with separation
36|c| 0".011 projected upon p.a. 103#; the K magnitudes are 7.22 (eastern) and 7.73 (western component): M. Simon,
36|d| unpublished.
37|a|DG Tau . The emission spectrum is very rich. In the red, "a few vague minima are probably the absorption lines
37|b| of a late-type star" [212]. Near 8700 A, "broadened absorption features consistent with an early M type" are
37|c| present [451]. The spectrum is shown or described in [303,312,337,340,458,500]. There is a knot having an HH-
37|d| like emission spectrum about 8" in 228# from DG [341]. About 55" south-west of DG is a series of emission knots,
37|e| named "DG Tau B" by [341]. Infrared photometry is in [490], the spectrum described by Jones and Cohen, Ap.J. Lett.
37|f| 311, L23, 1986, long-slit spectroscopy in [347], CCD direct images in [341,347,451]. There is also reflection
37|g| nebulosity to the north of DG [206].
389|a|GV Tau . A later-type star is imbedded in a very small, HH-like envelope. The object is variable at 2.2 microns,
389|b| and emission H@ may also vary [160]. Direct images are shown in [128,451].
39|a|DI Tau . DI Tau is about 16" from DH in p.a. 125# . It is surprising that the H@ was detectable by [257]
39|b| if W(H@) is as low as reported in [93].
390|a|Lick 6 . Detected by [28] as variable, compact radio sources, the coordinates are from the VLA observations.
390|b| The spectral types and W(H@) values were estimated from the published scans.
41| |IQ Tau . There is another star of about m(pg) = 17 at 10" in 301#.
40|a|LkH@ 101 . The optical coordinates from [8] and [57] are essentially the same; the coordinates of the radio
40|b| continuum source are in [57,96]. The spectral type of the star, either as observed directly (Allen, M.N.R.A.S.
40|c| 161, 1P, 1972) as F8: II or as scattered off the nebulosity [200] as F, is in conflict with the Lyman continuum
40|d| type of early B, probably above the main sequence [57]. The near infrared is dominated by emission lines;
40|e| infrared observations are in [209,326,434,436,472]. A polarization map of the nebulosity is in [379].
391| |Lick 3 . (See the remark for Lick 6, NGC 1579.)
42| |UX Tau B . The coordinates given for HBC 42 on p. 16 are of the A component.
43| |UX Tau A . [189] note that the velocity may be variable. In 1975, at the 120-inch coude, a close, faint companion
43|b| to A was detected with an image intensifier; it was estimated to be at about 2" in 180# : [250], note to
43|c| Table II. This star (C) was much redder than A. However, speckle observations have not confirmed its
43|d| existence [22].
45| |DK Tau . The star is extremely variable in UBV. [93] gives W(H@) = 19 A, while [91] find a range of 37 to 150 A.
46|a|ZZ Tau . This is the variable discovered by Reinmuth; the confusion in HRC is explained in [250], note to
46|b| Table II. Two Lick spectrograms show narrow H@ and weak He I emission. The star has a very large infrared
46|c| excess: Rucinski, Astr.J.90, 2321, 1985.
393|a|L1551/IRS 5. There is an extensive literature on this object, the associated jet, and the more distant nebulosity
393|b| (Sh 239 = HH 102). Most of the references other than those cited here are in [451]. CCD images of the region are
393|c| in [341,350,441].
49|a|HL Tau . This nebulous, non-stellar object (note in HRC; [453] Fig.6; Grasdalen et al. Ap.J. Lett. 283, L57,
49|b| 1984) has been classified as cont.(K7?) by [93], and as about M2 by [404], but the absorption spectrum apparently
49|c| cannot always be seen [101]. Infrared observations and photometry are in [88,100,328,410], and references therein.
49|d| Scans of the optical spectrum are in [93,101,123,312] and in Cohen and Schmidt, Astr.J. 86, 1228, 1981. Long-
49|e| slit spectra and CCD direct images are in [341,347,416].
395|a|V710 Tau B . The separation is about 3".5 in 180#. The coordinates are of the photocenter. The photometry listed
395|b| for the northern component is of the combined light; [93] give V = 14.5: for the northern star alone.
51| |V710 Tau A . (See remark for V710 Tau B.)
397|a|L1551-51 . According to [506], the scatter in the individual velocity observations suggests that the star is a
397|b| spectroscopic binary.
399| |V827 Tau . [408] find a cyclic variation 12.06-12.28 (in V) with a period of 3.63 days.
400|a|V826 Tau . According to [408], there is a cyclic variation 12.07-12.14 (in V) with period 4.05 days. The star is
400|b| also a double-line spectroscopic binary [344] with a period of 3.9063 days; the systemic velocity is given in the
400|c| Table.
402| |FZ Tau . This star is erroneously called "FY Tau" in [250], Table II.
54| |GG Tau . According to [93], there is a star about 4 mag. fainter, at about 12" in 205#, which has H@ in emission.
52|a|UZ Tau e . UZ Tau is double: in 1944, 3".68 in 271#.5 [258]. The coordinates are of the photocenter; almost all
52|b| the photometric data refer to combined light. The descriptions of the Mt. Wilson observations [256] leave no
52|c| doubt but that the eastern star in the active component; it was the same star that was responsible for the very
52|d| bright maximum in 1921 [213]. The eastern component was classified as M1,3 V(Li) in [212] and M1.5 by [93].
52|e| The two spectra are shown or discussed in [93,101,123,256,303,337,458]. The radial velocity of the eastern
52|f| component appears to be variable [123].
53|a|UZ Tau w . (See the Note for UZ Tau e). The western star has been classified as: dM3e [258], M4 V(Li) [212],
53|b| M0.5 [93]. The type given in the Table is a compromise.
405| |V830 Tau . There is a cyclic variation in light with period 2.76 days [409].
56| |GI Tau . There is evidence for a cyclic variation in light with period 7.2 days [492].
59|a|IS Tau . There is a mixup in the literature because the coordinates of Haro 6-23 (=IS Tau) and 6-26 (=IT Tau)
59|b| tabulated in [182] are reversed with respect to the stars marked on the identification charts in [182]. Following
59|c| GCVS3 and 4 and [250], we follow the table rather than the chart, and so take the southwestern star as 6-23 = IS Tau,
59|d| and the northeastern as 6-26 = IT Tau. Unfortunately this convention was not observed in HRC, which took the north-
59|e| eastern star as HRC 59 = Haro 6-23 = IS Tau, and as a consequence the identification chart in [410] reflects this
59|f| error. Another consequence is that HRC 59 is not the same star as HBC 59.
57|a|GK Tau . During the interval monitored in [492], the light curve showed a series of sharp, unevenly-spaced
57|b| minima. The maxima between suggested a period of 4.6 days.
406| |HN Tau/c . The companion is at 3".3 in 205# [93]. The coordinates are those of the primary.
408|a|Wa Tau/1 . There is weak emission at H@ and emission cores in H,K, but Li I 6707 is not detected, so this may not
408|b| be a pre-main sequence star.
64| |HO Tau . There is a mag. 16 star at 8" in 110#.
409|a|FF Tau . The star was found to be double in an occultation observation [435]. The separation was 0".037
409|b| projected upon about p.a. 257#. The K magnitudes are 10.06 (eastern component) and 9.06 (western).
65|a|DN Tau . Extensive photometric observations by [45] suggested rotational modulation with period 6 days; [492]
65|b| found P = 6.6 days, and a V range 12.29-12.42.
410| |L1642-2 . Nebulous; there is a red companion (1.1 mag. fainter in R) at 2".7 in about 13#.
413|a|L1642-1 . A nebulous double star; the very red secondary (1.9 mag. fainter in R) is at 5".8 in about 140# [416].
413|b| The star is marked on a photograph in Sandell et al., Astr.Ap. 97, 317, 1981. It was observed (as an IRAS
413|c| galaxy) by [357]; that scan shows strong Balmer emission lines on an M-type background (D.E. Osterbrock,
413|d| private comm.).
414| |CoKu HP Tau/G3. According to [101], the scans of HP Tau/G2 and /G3 in [93] are interchanged.
415|a|CoKu HP Tau/G2. (See the note to HP Tau/G3). Lick coude spectrograms of /G2 show H@ absorption with a weak, sharp
415|b| emission fringe to shortward, and an even weaker to longward. The absorption lines are very wide; Li I 6707 is
415|c| moderately strong. The spectral type quoted is from those plates.
418|a|HV Tau . The star has been variously referred to as "companion of DO Tau", "red nebulous star 2' east of DO Tau",
418|b| or "DO Tau/east". It is 4 mm east of DO Tau on the chart for that star in [410]. It was classified M2 in [93].
68|a|VY Tau . The light curve is discussed in [213, 327]. The colors and type in the Table refer to minimum light.
68|b| Near maximum, the spectrum is completely different, being dominated by low-excitation emission lines of
68|c| neutral metals. A brief H@ flare was observed [236] at minimum light in 1985.
424| |Haro 6-37/c. [93] gives the separation as 3".5 in 40#. The coordinates are those of the primary.
73| |Haro 6-37 . (See remark for Haro 6-37/c.)
74|a|DR Tau . The star was faint, near B = 14, prior to about 1961. In 1946, it had been classified dK5e, "spectrum
74|b| veiled by continuous emission" [257]. It brightened 2-3 mag. in B between 1961 and 1980, with major fluctuations
74|c| [69,165]. The spectrum is now a hot continuum with strong emission lines of H, He I, Fe II [1,14,33,123,212,220,
74|d| 297,303,337,481]. The dK absorption spectrum is no longer detectable (at least in the red), but a spectrum
74|e| rather like that of an F star can be seen in the IUE ultraviolet [220].
75|a|DS Tau . The dF0 companion, m(pg) = 13.7, is roughly 8" from DS (not 4" as in [257]); it was excluded from the
75|b| UBV observations of [25]. The mean velocity velocity of DS, +16.3 % 2.3 km/s from 3 observations [189], is
75|c| to be preferred to the value of 0 % 2 km/s of [219] from 6 spectrograms, but the discrepancy is puzzling. The
75|d| type in the Table (K5 V) is a reclassification from Lick coude material; [93] gave K3 and [257] dK4.
76|a|UY Aur . The star is a close double; [258] give 0".82 in 212# in 1944; the companion was about 0.5 mag. the
76|b| fainter at that time.
77|a|GM Aur . Repeated velocity observations by [189] give a constant value of +15.0 % 1.3 km/s, which is quite diff-
77|b| erent from the mean of -3 % 4 km/s, from 6 plates, of [219]. The discrepancy is unexplained. [257] gave +24 km/s,
77|c| but from 2 low-dispersion plates. The type of K3 V of [212] is confirmed on reexamination; [93] gave K7,M0.
426| |LkCa 19 . The type is K5 (Li) according to [506]. The W(H@) is a compromise of values from [189,219,506].
78|a|AB Aur . Since HRC, the star has been studied in detail by Catala, Praderie and co-workers. References to their
78|b| earlier work are in [68]; their IUE spectroscopy is in Ap.J. 254, 658, 1982 and 303, 311, 1986; Astr.Ap. 140,
78|c| 421,1984 and 182, 115, 1987. Further UBV/RI observations are in [31,50,225,229,430], and infrared in [3,31,32,
78|d| 55,81,87,91,155,316,372,452]. There is evidence for rotational modulation in the line profiles with a period
78|e| of 40-50 hours; see also [137].
79|a|SU Aur . Additional UBV data are in [50,167,225,229,236,375,410]. The W(H@) is usually 2-6 A but on one occasion
79|b| was found to be 14 A. There is suspicion of a rotational modulation in light with a period of either 2.73 or
79|c| 1.55 days [229].
427| |NTTS 045251. According to [506], this is a single-line spectroscopic binary.
428|a|V347 Aur . The star illuminates a variable nebula. The light curve resembles that of a long period variable. A
428|b| 1978 Lick coude spectrogram shows strong, rather narrow H@, fairly strong [O I] anf Fe II, and probably He I
428|c| emission.
429|a|V836 Tau . The cyclic variation found by [409] has a period of 6.99 days. The star was identified incorrectly on
429|b| the original chart [132].
430|a|UX Ori . The star is not convincingly associated with nebulosity, so it may not belong to the Ae/Be class. There
430|b| have been extensive UBV observations: [226,229,273,276,478,527,530].
81|a|RW Aur B . The coordinates are based on the offset from A; the only actual double star measurement is that of
81|b| [258]: 1".22 in 254#.3, made in 1944. When A is near minimum light, the companion contributes significantly to the
81|c| light and spectrum.
80|a|RW Aur A . Since the work referenced in HRC, UBV/RI data have been published in [1,60,91,226,328,377]; much of the
80|b| photometric observations are collected in [410]. The optical spectrum has been reproduced or discussed in [1,16,
80|c| 60,93,174,187,303,340,413,423,458]. IUE observations are in [15,65,239,240,241]. There is evidence for a 5-day
80|d| cycle in both the light (Herbig 1962) and in the line structure [174]. Repeated radial velocity observations
80|e| by [189] suggest that the velocity may be variable, with a range of about 10 km/s.
431|a|V1012 Ori . This object was observed as an IRAS galaxy by [357], but found to be a Be star. The variability was
431|b| discovered by Morgenroth (Astr.Nach.253, 441, 1934 [with chart]; 254, 366, 1935). The scan of the red region by
431|c| [357] shows H@ emission central on broad absorption wings, and strong Na I D lines.
83|a|V534 Ori . The coordinates are for St 37, identified with V534 Ori by [444], but [118a] identify the variable
83|b| with St 38.
84|a|CO Ori . Elvey and Babcock (Ap.J. 97, 412, 1943) classified the spectrum as early F, with peculiarities; it has
84|b| since been typed gF3 (Joy and Wilson, Ap.J. 109, 231, 1949), F8:n [212] and G5 [93]. When the star was near
84|c| minimum light about 1950, Herbig saw it as double (about 1" in 280#), but [22] could detect no such companion
84|d| in 1980, with CO near maximum. Additional UBVRI observations are in [91,225,229,236,328].
85|a|GW Ori . The spectrum has been classified as G5 (Zappala, Ap.J.172, 57, 1972); G5: [93]; G5,8 V [212]; and dK3
85|b| [257]. Additional RI observations are in [236,328].
86|a|V649 Ori . There is a faint companion at 1".41 in 350#; $m is about 2 mag. The UBV photometry of [338]
86|b| includes both stars. There was marginal evidence [22] for another star at 0".47, p.a. 36# or 216#. Other
86|c| spectral classifications have been dK3 [257] and K4 [93].
432| |P102 . The H@ emission was first noted by MacConnell, Astr.Ap.Suppl. 48, 355, 1982.
88|a|V370 Ori . The strength of H@ emission must be variable, because the W(H@) reported by [93] would not have been
88|b| detectable on objective prism plates. See the note in HRC regarding the clustering of emission-line stars around
88|c| GX Ori.
433| |V447 Ori/c . This star is about 5" in 30# from V447 Ori [119]. The coordinates are those of the primary.
434| |Rst 137B . This star is at 9".3 in about 344# from A [487]. The coordinates are those of the primary.
435|a|AB Dor . Additional UBVRI observations are by Lloyd Evans, Circ.So.African Astr.Obs. no. 11, 73, 1987, and by
435|b| Collier Cameron, ibid. p. 57. The reasons for suspecting that this may be a pre-main sequence star are in [486].
435|c| The mean radial velocity in the Table is that of [103]; the velocity may be variable with a range of about 22
435|d| km/sec: [244].
94|a|HK Ori . This star is at the apex of the reflection nebula PP 29. There have been numerous infrared observations:
94|b| [3,32,81,91,100,157,273,316,452].
96| |V453 Ori . The star is double: 3" in 190#, the companion being about 2 mag. the fainter [119].
436|a|RY Ori . The spectrum may be composite: He I 5875 suggest a B star, yet the remainder of the spectrum in the red
436|b| is about F8. H@ is a strong double emission line, and Li I 6707 is present in moderate strength. The star can
436|c| be identified from the chart by Wolf, Astr.Nach.171, 77, 1906, where it is 117.1904.
437|a|P1207/c . The companion is at 25" in 75# from A [93]; it has weak H@ emission. [93] found no H@ emission, despite
437|b| the objective-prism detection. The UBV colors in [11] must be in error. The coordinates are those of the primary.
104|a|VY Ori . There is a fainter star about 15" from VY in p.a. 135# . According to [497], its colors are: V=16.35,
104|b| B-V=+1.39, U-B=+0.71.
441| |WX Ori/c . The companion is at 11" in 10# from WX [93]. The coordinates are those of the primary.
447|a|P1540 . According to [324], the star is a double-line binary with P = 33 days; both stars show strong Li I 6707
447|b| and intense Ca II H,K emission. The integrated type has been given as K1 IV-V [364] and K4 V [483]; the K3 III: in
447|c| the Table is from a Lick coude plate. According to [483], the star is not a member of the Orion cluster.
452|a|P1724 . A non-member of the Orion cluster according to [483], although the spectroscopic criteria indicate that
452|b| it is a pre-main sequence star.
456|a|MR Ori . The star is projected upon very bright nebulosity, so it is has not been possible to determine whether
456|b| there is emission in the core of H@ or not; certainly no stellar emission lines are present elsewhere in the
456|c| spectrum. The star is included in this Catalog solely on the basis of its (alleged) variability and location in
456|d| the Orion Trapezium cluster.
457|a|AE Ori . The nebulosity is very bright, and from the single Lick spectrogram it was impossible to determine
457|b| whether stellar H@ emission is present or not.
459|a|P1925 . A Lick CCD spectrogram shows a fairly strong Li I 6707 line, but there is no evidence for emission at
459|b| H@, although the background nebulosity is so bright that a weak stellar emission core could have been concealed.
461| |TU Ori . There is a large dispersion in the assigned spectral types: see [221].
464|a|CQ Tau . The UBV data are for maximum light [166]. The H@ region was described by Bonsack and Greenstein (Ap.J.
464|b| 131, 93, 1960). A Lick coude plate of 1973 showed double H@ emission upon broad absorption wings. The absorption
464|c| spectrum otherwise is like an early F star.
466|a|AH Ori . The spectrum was classified K0 IV,V by [248]. A Lick coude plate shows H@ in absorption, with no certain
466|b| emission component; this appears to be a genuine example of a pre-main sequence star without obvious line emission,
466|c| at least in the red.
471|a|NV Ori . [270] regard this star as constant, but [227] report a V range of 0.6 mag. there is complex emission in
471|b| H@, supertimposed upon absorption wings. Li I 6707 is present but not unusually strong.
148|a|NY Ori . The star is normally faint, but when near maximum has the emission spectrum described in [197]. It is
148|b| about 5" se of P2118.
147| |TV Ori . The photometry of [338] and of [497] are not in good agreement.
150| |AN Ori . A Lick CCD scan shows H@ filled in to the level of the continuum.
477| |V1018 Ori . The companion is at 22" in 127# from CE Ori [93].
154|a|T Ori . According to Shevchenko (Flare Stars and Related Objects [ed. L. Mirzoyan], p. 230, 1986), T Ori is a
154|b| single-line spectroscopic binary with P = 14.268 days. A cyclic light variation having the same period is present.
155| |AR Ori . There is a companion about 2" distant.
480| |P2292 . According to [483], the star is not a member of the Orion cluster. [499] finds variable radial velocity.
481| |AV Ori/c . The separation is 6" in 305# [93]. The coordinates are those of the primary.
164|a|V380 Ori . This is nearly unique among the T Tauri stars in having an A-type spectrum. It is ADS 4209, but that
164|b| companion (mag. 13.0, about 3" in 220#) and another suspected by Jonckheere (Mem.R.A.S. 61, 57, 1917) were
164|c| probably only structure in the nebula NGC 1999. No such stars are detectable on modern photographs, nor can
164|d| any be seen visually at the 120-inch telescope. Additional UBVRI observations are in [116,229,328,378], and
164|e| additional spectroscopy in [413]. A polarization map of the nebulsoity by Warren-Smith et al. is in M.N.R.A.S.
164|f| 192, 339, 1980.
484| |P2441/c . The separation is 4".5 in 145# [93]. The coordinates are those of the primary.
167|a|P2441 . Spectral types assigned have been: G1 IV [411], G3 [329], G5 [93], and "about G8n" from Lick spectrograms
167|b| in the red. All conflict with the blue-region type of F5: in HRC. There is very strong, slightly asymmetric
167|c| emission in H@. There is a nebulous patch (HH 63) about 30" southwest (Reipurth and Graham, priv. comm.).
485|a|V586 Ori . Lick spectrograms showed strong complex emission, variable with time, in H@. It is superposed upon the
485|b| absorption wings of an early-type star. A few He I and Fe II lines suggest a type of late B or early A.
169| |BF Ori . Additional UBVRI observations are in [229,273,391,430].
489|a|V883 Ori . This is the faint red variable slightly west of the apex of the reflection nebula IC 430 = Haro 13a
489|b| (see [453], Fig. 5). The entry is retained although there is no evidence that the star has ever exhibited H@
489|c| emission: [7,181,312,363].
490|a|Haro 2-249/c. The coordinates are approximate. These two stars and the ring-shaped nebula associated with the primary
490|b| are shown on a CCD image in [161] and on [453] Fig. 5.
492|a|+26# 887 . This is the "nebulous star 3' from RR Tau" in [203]. No emission was present in the photographic region
492|b| on early Lick spectrograms, but P Cyg structure is present at H@ on a 1982 coude plate.
493|a|V350 Ori . A 1973 Lick spectrogram showed complex H@ emission, with narrow central reversal, superposed upon the
493|b| absorption wings of an early-type star. He I 5875 is rather strong, so a B type is indicated.
494|a|Reipurth 50. The coordinates are of the approximate center of a nebulosity that is believed [386] to be illuminated
494|b| by a heavily obscured star about 1'.5 north. The nebula is variable in brightness.
182|a|San 6 . A 1978 Lick coude spectrogram showed a strong, symmetric H@ emission line and a well-defined K-type
182|b| absorption spectrum. The observation of San 6 in [93] must refer to another star.
185|a|V631 Ori . [93] found no H@ emission in 1976, yet rather strong emission in the photographic region was observed at
185|b| Lick in 1960, and the star was originally detected on the basis of a bright H@ line [322].
186|a|FU Ori . The coordinates are from Duerbeck, Sp.Sci.Rev. 45, 1, 1987. The earlier history of FU Ori is summarized
186|b| in [207,213]. It remains not far below maximum light. The UBVRI data in the Table are rough means from extensive
186|c| observations in 1984-85, during which time a cyclic variation of length 9 or 18 days was present [286]. The
186|d| spectrum is very complex, and the type assigned appears to depend on wavelength; the value in the Table is for
186|e| the red region. References to infrared and recent high-resolution spectroscopy, and other properties of the
186|f| spectrum, are [188,190,191]. Although not expressed in terms of v sin i, [190] gives line widths measured in
186|g| a variety of spectral regions.
502|a|SSV 61 . This star, in a complex reflection nebulosity, is object 140 in [448], Fig. 1a; it is also in [211],
502|b| Fig. 8. It was classified as an M2,4 giant by [448]; a Lick CCD spectrum indicates a slightly earlier type.
515|a|+1# 1156 . This peculiar star illuminates the nebulosity Par 3 = PP 46. The presence of Li I 6707 is confirmed on
515|b| a Lick CCD spectrum, on which H@ is filled to continuum level with emission.
190| |LkH@ 336 . (See the following remark for LkH@ 336/c.)
516|a|LkH@ 336/c . This, the brighter companion of LkH@ 336, is at 15" in 90#; it is 2 mag. fainter than A [93]. It is
516|b| apparent on the identification chart in HRC. According to [93], there is another star at 6" in 140#, 5 mag.
516|c| fainter than A.
193| |LkH@ 208 . An optical polarization map of the nebulosity is in Shirt et al., M.N.R.A.S.204, 1257, 1983.
199|a|MWC 137 . As noted in HRC, this is a high-luminosity object that may not be pre-main sequence. The star is sur-
199|b| rounded by a 56" x 80" ring of nebulosity; it is 195 -0# 1 = Sh 2-266 in Perek and Kohoutek "Catalogue of
199|c| Galactic Planetary nebulae", which gives an identification chart.
200|a|LkH@ 340 . The labels on the charts for LkH@ 340 and 341 in Figs. 4 and 5 of HRC were interchanged. Drs. U.
200|b| Bastian and M. Cohen have confirmed that their respective observations [25,93] were of the stars at the coordinates
200|c| given in HRC, not of the stars on the incorrectly labelled charts.
201| |LkH@ 341 . (See the preceding remark for LkH@ 340.)
525| |V486 Mon . There is a faint companion at about 6" in 73#.
528| |LkH@ 215 . The coordinates are only approximate on account of interference by the bright nebulosity.
529|a|HD 259431 . Although this star is often considered a member of the Ae/Be class [203], the possibility still exists
529|b| that it is a conventional Be star. The modern spectral classifications range from B2e [138] to B5 [452] and
529|c| B6pe [224].
207|a|R Mon . The coordinates are those of feature "a" at the apex of the small (about 3") triangular nebulosity
207|b| known as "R Mon" [251]. Its brightness dpends heavily upon aperture size and angular resolution. The spectrum
207|c| is peculiar and variable: see [208,251] and references therein. Infrared speckle observations are in [29], and
207|d| infrared spectrophotometry in [87]. The structure of the nebulosity in [S II] is described by Brugel et al.
207|e| (Ap.J. Lett. 287, L73, 1984), and photometry and polarimetry of NGC 2261 are in [21] and in Warren-Smith et al.
207|f| Ap.J. 315, 500, 1987. The HH Object HH 39 lies on the axis of NGC 2261 about 7' north of R Mon: see [251]
207|g| and Walsh and Malin, M.N.R.A.S. 217, 31, 1985.
209| |G-G 405 . There is a faint companion at about 4" in 150#.
531| |VSB 2 . The type F7 V [526] in the Table is in conflict with the K0 of [488].
534|a|W68 . The various spectral classifications are not in good agreement, probably because of the very broad lines:
534|b| F2 [488], F4 V [526], G0 IV,V [494].
219|a|V590 Mon . The spectrum is peculiar, and at low resolution there has been considerable disagreement in the classi-
219|b| fication: B4 V [526], B9-A0 [93], B8 + shell [203], A2-3 [199].
222| |W108 . Spectral classifications range from F7 V [526], F8 [458] to F9 [93] and G0 [488,494].
535|a|W121 . The star is located very near S Mon, which may account for the large discrepancies is the published UBV
535|b| photometry, amounting to 2 mag. in V: [414,433,494]. A Lick CCD spectrogram showed moderately strong H@ emission
535|c| with central reversal, and strong Li I 6707 absorption.
227|a|IP Mon . The star is very closely nebulous. The type K3 was assigned by [93,401], while [488] give K2 and [526]
227|b| gives G8 V:. The H@ emission is rapidly variable: Marcy, Astr.J.85, 230, 1980.
538| |W154 . The type G2 III,IVp is from [494], while [526] gives G2 V and [488] G7.
231| |V360 Mon . The type F8 is from [93], but [401] gives K2 or earlier, and [526] G8 V.
236| |V365 Mon . This star is 7" from V591 Mon.
543|a|OX Mon . The emission originates in the northeast component of a close pair (7" in 35# : [93]). The photometry
543|b| refers to the combined light. No emission is seen in the other component [93].
546|a|NGC 2313 . The involved star has a complex emission structure at H@, and in the red an absorption spectrum perhaps
546|b| of type G with very strong Ba II lines.
548| |LkH@ 218 . This may be an ordinary Be star.
243|a|Z CMa . The spectrum is very complex and possibly composite. References to earlier spectroscopic work are in
243|b| HRC; more recent papers: [104,123,452]. The optical and VLA coordinates are not in close agreement [96]. An
243|c| optical companion was reported in [139] but has not been confirmed. Infrared speckle observations show the star
243|d| to be slightly extended in the east-west direction [311]. UBV/RI photometry is in [50,91,225,229,275]. Many
243|e| infrared observations have been reported: [3,31,32,81,87,155,224,273,316,372,452]. The VLA observations are
243|f| in [34,96,101].
551| |LkH@ 220 . This may be an ordinary Be star.
552|a|NX Pup . The spectral type in the Table is a compromise: the star has variously been classified as A0-1 III
552|b| [478], A1 [138], F0 Ipe [245], F1-2 [381], and F2 III [49]. H@ is in emission but the decrement is very steep.
563|a|ESO313-N*10. At least 9 condensations, most of them red with H@ in emission, are imbedded in a bluish nebulosity about
563|b| 35" in diameter having an early-type absorption spectrum.
565|a|SY Cha . The type M0: is from [17]; an earlier classification was K2 V [12]. The star has shown a cyclic
565|b| variation in brightness with range 1.6 mag. in B and a period of 6.129 days [259,325,422].
567|a|TW Cha . A cyclic variation is present with a period of 8.6 days and a range of about 1.0 mag. in V. There are
567|b| also concurrent changes in the emission spectrum [259].
568|a|TW Hya . The spectrum is in all respects like that of a T Tau star, but there is no nearby cloud. Three Lick
568|b| spectrograms gave velocities of -9, +12 and +9 km/s, a range large enough to raise the suspicion that the star may
568|c| be a binary.
569|a|CS Cha . The spectral type in the Table is a compromise of K2 [196], K5 [403] and M0 [17]. The value W(H@) = 13 A
569|b| from [17] differs from the 59 A in [403].
570| |CT Cha . The type K7: is from [17]; [196] give G8:.
575|a|VW Cha . Variability of H@ was suspected from the first observations [196], and confirmed by later results [17,
575|b| 403]. A mean value is given in the Table. The K2 type is from [17], but the star was classified earlier as
575|c| G1 V: [12].
246| |CU Cha . The spectral type is from the Michigan Spectral Catalogue 1, 1975; it was given as B9.5e V in [196,403].
578| |VZ Cha . A cyclic variation with a V range of about 0.7 mag. and period 7.2 days has been observed [259].
583| |WY Cha . The star was classified K0: (Li) by [196].
585| |WZ Cha . [196] give the type as G:.
588|a|Sz 41 . The coordinates and photometric data are for Sz 41, while the infrared references and spectral type
588|b| refer to HJM E1-9a. The coordinates of the two objects agree within about 10", and it is assumed that they are
588|c| the same. [238] state only that line emission is present, giving no details
591|a|T Cha . T Cha has sometimes been regarded as a pre-main sequence star on the grounds of its rapid, irregular
591|b| variability and location on the edge of a small dark cloud [232,233], but spectroscopic proof is lacking. There
591|c| is no obvious emission at H@ or elsewhere; unfortunately the Li I 6707 region has not been observed adequately.
591|d| A cyclic variation with a period of 3.2 days has been suggested [325].
592|a|Bipolar nebula. The spectral type refers to the northern lobe [351]. The southern extension has an HH-like spectrum;
592|b| there is probably an A0 star involved. Polarimetry of the nebulosity is in [461]. The UBV data were taken through
592|c| a 23" aperture [508]. It is uncertain whether this is a pre-main sequence object.
595|a|S2 . S2 is considered [421] to be the central object of a nebulous cluster, but earlier [58] was regarded as
595|b| the central star of a bipolar nebula. The coordinates are approximate.
251| |RU Lup . Additional UBV/RI observations are in [25,145,266,427].
252|a|RY Lup . A quasiperiodic variation of length 3.76 to 4 days was discovered by Hoffmeister [232], and confirmed by
252|b| more recent work [46,129,314]. W(H@) ranges from invisibility [17] to about 25 A [314], apparently in
252|c| antiphase with the light cycle.
253|a|EX Lup . The photometry refers to minimum light, but the values in the Table are the brightest of 7 observations
253|b| [25]. References to earlier work on the star, especially near maximum, are in HRC and [213].
617|a|Sz 102 . The spectrum contains strong emission lines of [O I], [N II], [S II],..., characteristic of HH Objects,
617|b| superposed upon a late-type continuum and stellar absorption spectrum [17,295,299,426]. Two isolated patches of
617|c| emission nebulosity lie about 13" e and w of the star [295].
619|a|V856 Sco . Observations in the Stromgren and Walraven photmetries are in [467,468,469]. The star is reputed to have
619|b| a close companion (Rst 3930B, at 1".3, mag. 12), but it was not detected in speckle observations [22].
631|a|Sz 124 . The fact that the star was detected by objective prism observers [426,463] seems incompatible with the
631|b| low value of W(H@) = 1.6 A in [17].
632|a|V866 Sco B . The companion is about 1".4 in 20# from the (slightly) brighter primary. Both stars have the infrared
632|b| Ca II lines strongly in emission. The coordinates and photometry refer to the combined light.
254|a|V866 Sco A . The type K0 assigned in [93] was not in acceptable agreement with the M0: of [212]. Reexamination of the
254|b| Lick material shows that it clearly lies betwee K3 V and M0 V, hence the K5 V in the Table. Narrow He I emission
254|c| lines are present. The coordinates and photometry refer to the combined light.
634|a|Wa Oph/3 . H@ emission was discovered by The [465], which is surprising considering the low value of W(H@) = 0.3 A
634|b| in [502].
637|a|DoAr 21 . H@ emission was reported by objective-prism observers between 1949 and 1960, but has not been seen on
637|b| slit spectrograms since 1973. The object at that position is very variable as observed with the VLA, and moderately
637|c| so in X-rays [133]. No optical variability was detected on Lick Astrograph plates [369].
638| |DoAr 24 . The X-ray coordinates [332] are in better agreement with DoAr 24 than with DoAr 24E.
260|a|DoAr 22 . The coordinates are those of the m(pg)=13.0 star, type F5:e, listed in HRC. The emission-H@ object
260|b| 33 identified in [524] as DoAr 22 is a much fainter star located 1 mm south, 3 mm east of DoAr 22 on [524] Fig. 1;
260|c| its spectrum has not been observed.
639|a|DoAr 24E . According to [539], the star is double, separation 1".95 in p.a. 0# . The only positive detection of H@
639|b| emission is by [524]. The X-ray emission probably originates in DoAr 24.
262|a|SR 24 s . The coordinates are of the photocenter of the pair (6" in 60# ); individual positions are in [524]. The
262|b| ROX observation included both stars. A variation 16.4-17.1 (pg) is observed in the combined light [369]. Attention
262|c| was called to the duplicity and the associated nebulosity by Haro and Chavira, Inf.Bull.Var.Sts. 926, 1974.
262| |SR 24 n . (See remark for SR 24 s).
640|a|ROX 20-1 nw. The separation of the pair is about 13" in 302# . X-ray flaring has been detected in the unresolved
640|b| image [332]. H@ emission in both stars was originally noted on a Lick slitless spectrogram.
641| |ROX 20-2 se. (See remark to ROX 20-1 nw).
263|a|S-R 12 . Speckle observations show the star to be a close double (0".30 in about 85#), with K magnitudes
263|b| 9.34 (eastern) and 9.17 (western). It was also resolved in an occultation observation [435].
642|a|ROX 31 . The coordinates are from a VLA observation. The spectroscopic observation is by Bouvier and Appen-
642|b| zeller, quoted in [10]. The star was not detected in the H@ surveys of the region. An occultation observation
642|c| [435] showed the star to be double with separation 0".13 projected upon p.a. 337#. The K magnitudes are 8.72
642|d| (eastern) and 9.00 (western component).
265|a|SR 10 . There is a large difference between the W(H@) values of [17] and those of [93,402]; the mean of the
265|b| latter is given in the Table.
644|a|Haro 1-14/c. Haro 1-14 is actually the fainter, southeastern component of the pair of stars (separation about 10") at
644|b| this position. The UBV photometry refers to the combined light. The brighter star, here called Haro 1-14/c, has
644|c| emission cores in H,K [404].
267| |Haro 1-14 . (See remark for Haro 1-14/c).
645|a|Reipurth 13. This a a faint, extended nebulosity (6" x 8"), apparently scattering the light of an imbedded star
645|b| having H@ in emission [9].
646|a|V346 Nor . This very red star is at the edge of HH 57 [426]. Originally discovered as an infrared source [384], it
646|b| became detectable in the visual region about 1983: [102,169,382] and references therein.
271|a|AK Sco . The type is from the Michigan Spectral Catalogue and Lick coude material. The spectrum in the red
271|b| appears composite. Two Lick CCD scans show double lines with a splitting of about 200 km/s; at other times the
271|c| lines have been single. Clearly, the star is a double-line binary. Li I 6707 is strong in both components.
655|a|V921 Sco . The emission spectrum of this nebulous star was noted independently by Vandervoort and The
655|b| (priv.comm.), by Henize (Astr.J. 67, 612, 1962), and by N. Irvine.
656| |AS 216 . There is a faint companion at about 5" in 200#, about 4 magnitude fainter than AS 216.
272|a|IX Oph . Lick coude spectrograms show sharp H@ emission on a weak metallic-line spectrum; Li I 6707 is not
272|b| present. The star's image is marked on Pl. I of [464], but no number was assigned.
273|a|KK Oph . The star was noted as double at the 120-inch in 1987: the separation is 1-2" in p.a. about 240# , the
273|b| magnitude difference about 1 mag. Narrow [N II] and [S II] lines are present in the brighter component; [Fe II]
273|c| emission has been reported in the blue [6].
275|a|LkH@ 346 nw. [93] give 6".5 in 130# as the position of the se component with respect to the nw. The coordinates
275|b| are those of the photocenter.
275| |LkH@ 346 se. (See remark for LkH@ 346 nw).
658| |RNO 92 . The star is double: 4".4 in 65# ; direct images are shown in [388].
280|a|SV Sgr . The star is superimposed on the very bright H II region NGC 6523. Lick coude spectrograms show P Cyg
280|b| structure at H@ and very strong emission at the infrared Ca II triplet.
281| |LkH@ 118 . The classification as B5 Vp [139] conflicts with the description of the spectrum in [201].
662|a|V4046 Sgr . [113] find the star to be a single-line binary with P = 2.43 days; [62] suspect double lines. W(H@)
662|b| varies between 30 and 120 A. Flaring was observed by [61]. The star can be identified from the HDE chart (Harv.
662|c| Ann. 112, 1949).
663|a|-10# 4662 B. The star is double (1".33 in 11#.5 in 1972: Walker, Pub.U.S.Nav.Obs.25, pt.2, 1985); the coordinates and
663|b| photometry refer to the combined image. It is not known which component is the flaring variable. According to
663|c| [77], there is also a sinusoidal variation with P = 5.20 days, amplitude 0.1 mag., in the integrated light.
664| |-10# 4662 A. (See remark to -10 4662 B).
666| |CoKu Ser/G1/c. This companion is at 3".5 in 140# from G1; the coordinates are of the photocenter.
667| |CoKu Ser/G1. (See remark for CoKu Ser/G1/c).
282| |VV Ser . The coordinates are from Reinmuth, Astr.Nach.225, 386, 1925.
672|a|CoKu Ser/G7. This is probably star 2 of [456], Table II. Warren-Smith et al. (M.N.R.A.S.227, 449, 1987) present a
672|b| polarization map of the nebula (called the "Serpens object" in [453]). Their Fig.1 identifies the infrared
672|c| sources in the area; their Pl. 1, and Fig. 7 of [453], are photographs of the region.
284|a|AS 310 . See the remarks in HRC. The photometry contains the contribution of a faint companion at 3-4" [25,139].
284|b| A Lick coude spectrogram shows shallow absorption under the sharp central H@ emission, and narrow He I absorption
284|c| lines. Strong interstellar features are present. Clearly, this is a hot, high luminosity object.
673| |Kn H@ 10 . [323] find no line emission. The spectral type is K, but it may be a giant.
675| |Kn anon 2 . A late-type absorption spectrum was found by [323], but no line emission.
286|a|S CrA . The emission spectrum is very strong, and the underlying absorption spectrum can be seen only with
286|b| difficulty. The star is a close double, usually not resolved photometrically or spectroscopically. Discovered
286|c| by [258], it was remeasured by [22]: separation 1".37, p.a. 147#, $m about 1 mag. in 1981. Additional UBV
286|d| photometry is in [25,263,266,323,336]. The spectrum is reproduced or discussed in [17,18,122,212,323,336,337,
286|e| 400,401].
287|a|TY CrA . See the remarks in HRC. there may be a weak emission component in H@ [139]. According to [264], the
287|b| star is an eclipsing variable with P = 2.888797 days. The other bright star in NGC 6726/7, CoD-37# 13023, has a
287|c| close companion discovered by Hubble. At the 120-inch coude, this star was estimated of mag. 13-14, at 3" in 160# .
677| |MaRy/H@ 2 . H@ emission was first noted by [274], and the star was marked but not numbered in their Fig. 1.
288|a|R CrA . Published V's show large scatter, due either to real variability or the effect of the nebular background.
288|b| Rapid changes in the nebula and in the H@ profiles in nebula and star have been described by Graham and Phillips
288|c| (Pub.A.S.P.99, 91, 1987).
289|a|DG CrA . See the remark in HRC. Since that time, H@ emission has apparently been detected by [274] and [323].
289|b| The coordinates are approximate, from Van Gent (B.A.N.7, 21, 1933).
290|a|T CrA . There is a difference of about 2 mag. between the V's of [329] and those of [273] and [323], possibly due
290|b| to variability.
681|a|FG Aql . The type in the Table (K2) is from [93], but a Lick coude spectrogram in 1977 was classified as K7,M0 V
681|b| with strong Li I 6707, and double H@ emission (R>V).
684|a|WL 22 . This object was found by Wooden and Lada (unpublished). A 1981 Lick spectrogram showed narrow H@
684|b| emission line flanked by an extremely broad, strong P Cyg-type absorption structure.
292|a|V1352 Aql . This is the "exciting star" of HH 32. The V, B-V values are means from [288]. The emission spectrum has
292|b| been investigated by [40,218,293,294,337,342,423]. Perhaps on account of P Cyg structure, the various W(H@)'s do
292|c| not agree well [93,293,423]. No absorption line spectrum is detectable.
686| |WW Vul . Additional UBV/R photometry is in [226,475,529,530].
293| |LH@ 483-41 . A 1972 Lick coude plate showed double H@ emission (V<R) superposed upon broad absorption wings.
687|a|Par 21 . This object did not appear stellar to visual examination at the 120-inch coude, but rather as a
687|b| nebulous blob 3-4" in diameter. Two 1974 spectrograms showed H@ in absorption.
689| |V1685 Cyg . A comprehensive discussion of the UBV data is in [392]. The spectrum is described in [138,139,203,452].
692|a|V1515 Cyg . The earlier history of this FU Ori-type variable is in [213]. Subsequent spectroscopic observations are
692|b| in [27,108,188,190,285]. The UBV data are means for the 1981 season [285]. The coordinates are those given for
692|c| "P22" in [83]. A direct image of the nebulosity, and its spectrum, are discussed in [161].
693| |+41# 3731 . This may be an ordinary Be star.
694| |Par 22 . The star is central in a bipolar nebula. It is identified as "P22a" in [83].
696| |PV Cep . The star is associated with a variable nebulosity [92,95,313,351].
697| |AS 442/c . The coordinates are of AS-442 itself, a Be star. The companion is 5" in 45# from the primary [93].
699| |LkH@ 138 . LkH@ 138 is the southwest and brighter component of a pair, separation 5" in 48# .
700| |LkH@ 138/c . (See the remark for LkH@ 138).
703|a|V1531,1532 Cyg. = LkH@ 142, 143: an unresolved pair separated by about 2".5 in 91# . The coordinates are of the
703|b| photocenter.
708| |LkH@ 151/c . According to [93], this star is 9" in 20# from LkH@ 151.
717| |LkH@ 168 . This may be a background Be star.
297| |V751 Cyg . It is still not clear whether this is a pre-main sequence star or not: see the remarks in HRC.
298| |LkH@ 172 . Welin [509] has noted that LkH@ 172 is at the place of the "missing" BD star +43# 3749.
300|a|V1057 Cyg . The best-studied FU Ori-type star; history and references through 1976 are in [213]. UBVR light curves
300|b| and references are in [287]; more recent photometry is in [3,87]. Spectroscopic references are: [27,108,188,190,
300|c| 278,335,337,458,480], and infrared: [3,87]. The fading of the reflection nebula is described in [120].
302|a|V1331 Cyg . The emission spectrum is very rich, and no underlying absorption spectrum is apparent. The spectrum is
302|b| displayed or discussed in [70,72,302,303,337,367].
726| |HD 200775 . There is some dispersion in the published spectral classifications: B2.5 [138], B3 V [24], B5 [378].
305|a|LkH@ 324 . LkH@ 324 is marked on the HRC identification photograph as the bright star at the nw tip of an elongated
305|b| nebulosity. In fact, the H@ emission was originally detected in the fainter star at the se end: the HRC chart
305|c| was marked incorrectly. As proposed by [73], the "LkH@ 324" identification will remain attached to the nw star,
305|d| as in HRC. H@ emission has actually been observed in this star on two occasions. Photometry in 1983-85 gave:
305|e| V=12.75, B-V=+1.13, U-B=+0.44, with a V range of 12.64-12.83 [279]. Thus the values given in the Table may
305|f| refer to a time of temporary brightening at some time between 1975 and 1980. This object deserves closer
305|g| attention.
727| |LkH@ 324-SE. See the remark for LkH@ 324; the star at the se edge of the nebula is now designated LkH@ 324-SE.
729| |LkH@ 349/c . This companion is approximately 16" in 305# from the brighter star.
308|a|LkH@ 349 . The coordinates in HRC are incorrect. The star is probably no. 60 in Marschall and Van Altena (Astr.J.
308|b| 94, 71, 1987). It can be identified in Osterbrock, Ap.J.125, 622, 1957, at 56.5 mm below and 37 mm inside the
308|c| upper left corner of Fig.2. Strong, double P Cyg-type absorption components are present on a Lick coude plate.
731| |Star in RNO 138. = star 6 of [456].
733|a|V1735 Cyg . The star illuminates a red reflection nebula. P Cyg structure at H@ is clearly detectable on a Lick
733|b| coude spectrogram.
734|a|BH Cep . A Lick coude spectrogram shows wide, P Cyg-type structure at H@; some later-type absorption lines are
734|b| present, suggesting a type of about F. A light curve is given by Hoffmeister, Astr.Nach.274, 232, 1944.
735|a|BO Cep . A Lick coude spectrogram shows widely double, sharp emission upon broad H@ absorption wings. No other
735|b| lines except narrow, presumably interstellar, Na I D lines are present in the red. See the Hoffmeister reference
735|c| in the remark for BH Cep for a light curve.
736|a|SV Cep . Lick coude plates show double H@ emission superposed upon broad absorption wings; He I 5875 is present,
736|b| and interstellar Na I. The type may be slightly earlier than A0. Other classifications are in [205,268,474,530].
313|a|LkH@ 233 . Photometry and polarization maps of the nebulosity are in [20]. The object is also known as Markarian
313|b| 914 [460].
314| |LkH@ 350 . This may be an ordinary Be star.
315|a|DI Cep . W(H@) is highly and rapidly variable: [26,91,93,147,173]. Much detailed information on the photometric
315|b| and spectroscopic variations is in [147,173]. Spectroscopic observations are in [26,187,257,294,303,413].
316|a|AS 501 . [115] found a V range of 12.3-13.1, but [443] saw no variation beyond normal photographic scatter. H@
316|b| emission is strong and double; there are no other emission lines in the red. Despite the M giant absorption
316|c| spectrum, the star does not appear to be a symbiotic. It is unlike any recognized pre-main sequence star.
740|a|MWC 1080/c . [93] gives the separation from MWC 1080 as 10" in 75# , magnitude difference = 4 mag., but the separation
740|b| seems to be more nearly 25".
317|a|MWC 1080 . This is a hot, high-luminosity object, showing strong He I absorptions, hazy Fe II emission, complex
317|b| P Cyg-like emission at H@; the interstellar lines are strong. Although involved in bright nebulosity, it is not
317|c| obvious that this is a pre-main sequence star, although the companion appears to be so. W(H@) values: [91,93,139].
318|a|BM And . The spectral type given is for the red region; there is some suspicion that it may depend upon wavelength
318|b| [212,498].
323|a|MacC H18 n . There are two stars at this position; the coordinates given are for the brighter, northeastern of the
323|b| pair. The fainter star is at about 10" in 196# . It is not obvious whether data of [93] or [90] refer to the
323|c| brighter star or to the pair together.
412| |NTTS 043230+1746 . The position is in error by 10s in RA, position corrected on 16-Mar-2008 at CDS (NTTS-ID is OK)
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