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]. 329a VX Cas . There was some uncertainty in the identification of this star in the earlier literature. The coordinates 329b and other data in Table 1 refer to the star indicated as VX Cas in Aarhus Medd. no. 10, 150 (1937), Kasan Bull. 329c 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 329d bright nebulosity nearby. 330a V594 Cas . The absorption spectrum is confused by line emission; the types assigned range from O9.5 to B8,9: 330b see [138]. 7 LkH@ 201 . This is probably a background Be star. 334a RNO 6 . The photometry is of the star in the brighter lobe of this reflection nebulosity. A polarization 334b map is in [420]. 8a LkH@ 262 . LkH@ 262, 263 are separated by about 15" in 22# . They and LkH@ 264 lie in L1457, but are not to be 8b identified with the X-ray source in that cloud found by Halpern and Patterson, Ap.J. Lett. 312, L31, 1987. 9a LkH@ 263 . (See remark for LkH@ 262.) 336a IRAS 0313 . This nebulous star was observed at the request of Iyengar. An underexposed Lick coude spectrogram in 336b 1986 showed only strong double H@ emission (R>V) on a weak continuous spectrum. 338a LZK 4 . A 1983 Lick coude spectrogram of the red region shows an unusually broad, structured H@ emission with 338b a reversal displaced somewhat shortward of center. A few weak absorption lines are present, and the D lines are 338c fairly strong, but Li I 6707 is not apparent. The type was classified as mid-K by [118a]. 346a SSV 13 . No stellar absorption spectrum can be seen with certainty; H@, [O I] and [S II] are very strong, as in 346b H-H Objects [160]. 348a IP Per . It is not certain if this is a pre-main sequence star. Two Lick coude spectrograms (1973, 1981) 348b showed strong, structureless H@ emission upon broad, stellar absorption wings. The only other stellar features 348c 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". 349a XY Per e . The star illuminates a large reflection nebula. XY Per is ADS 2788; coordinates and photometry refer 349b to the combined light. There has been no change in the relative position since 1904; the mean separation is 349c 1".35, p.a. 75#. The photometric range is so large that both components must be variable; the magnitude 349d differences noted by the double star observers can account for only a fraction of the amplitude [47]. The 349e eastern star (B) was the fainter at all the Lick observations (1961-73). It was earlier classified as B6, 349f but superior modern material indicates middle A in the blue, but late B in the red. The v sin i quoted is 349g from the metallic spectrum. There are fairly strong, double emission cores in the H@ absorption line. 350a XY Per w . The western star (A) has a peculiar spectrum. Originally called A2 II (Herbig 1952), modern coude 350b spectrograms show sharp, double core structure in Ca II K and the higher Balmer lines; this structure is 350c variable with time. The Fe I lines are the widest species (v sin i = 120-140 km/s), and suggest a type of 350d A2 or A5. Lines of Fe II and Ti II are narrower and strong; Ti II 3685, 3759, 3761 are prominent, as in 350e shell spectra. Broad central emission, divided by a central reversal, is present in H@. Weak, broad He I 350f absorption lines suggest a late B type. 355a NTTS 035135. Weak emission cores are present in the H,K lines but H@ is absent, presumably being filled-in to the 355b level of the continuum. 356a NTTS 040012. NTTS 040012+2545N and S are separated by about 1". The coordinates, photometry etc. are for the combined 356b light. The Li I 6707 is observed in the combined spectrum. 357 NTTS 040012. (See remark for preceding star.) 363a PP 13 s . The s, brighter lobe shows a scattered M-type spectrum with prominent [O I], [S II] but no H@. The 363b illumination is from a heavily obscured infrared source near the ne edge. The n lobe is nearly stellar, and has a 363c 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.) 365a LkCa 1 . The radial velocitites of both [212] and [192] are well off that expected for a star associated with the 365b Taurus clouds. 366a Anon 1 . This is the "nebulous star 11' in 300 from HD 283447" of [212]. It is identified on the chart for 366b 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. 25a CW Tau . The radial velocity value quoted is from [189], but the velocity may be variable [123]. The [O I], 25b [S II] lines are unusually strong. The spectrum is discussed or reproduced in [93,123,404,458,500]. 369a 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 369b also identified in [257]. The identity with the Haro s6-2 of [93] was confirmed by M. Cohen. 29a V410 Tau . Additional UBVRI observations are in [220,236,390,410]. A cyclic variation 10.82-11.04 (in V) with 29b period 1.92 days is present [408]. The radio source at the star is variable: [34,96,101,305]. 373a 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 373b identified in [93]. It was discovered originally as an infrared source by D. A. Allen (private comm.). 374a 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 374b 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]. 377a FQ Tau . The star is identified in [182]; it is also identifiable as the image 9 mm north, 9 mm west of 377b "WK X-ray 1" on the chart for that star (V819 Tau) in [410]. 32a BP Tau . [492] found a cyclic variation 12.07-12.27 (in V) with period 7.6 days. High-resolution line profiles 32b 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. 34a RY Tau . The historical light curve is in Kholopov, Perem. Zvzd. 13, 430, 1961, and in [534]. Additional UBV/RI 34b observations are in [220,225,227,229,266,281,284,410,492,511,528]. Observations of H@ are in [91,93,123,220,282, 34c 423,531], of the spectrum in [123,220,281,294,303,340,423,458], and of the variable nebulosity in [206]. Velocity 34d variation was suspected in [212]. Extensive Lick observations gave inconsistent results: 1977-78, the velocity 34e scattered between +5 and +30 km/s (14 plates); 1978-79, constant at +20.0 % 1.0 km/s (12); 1979-80, constant at 34f +18.3 % 1.5 km/s (8). The higher-accuracy observations of [189] gave an apparently constant value of +16.5 % 2.4 34g 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]. 381a Haro 6-5B . Haro 6-5B is a very red, presumably stellar source (probably a T Tauri star: [99,347]), in the sw corner 381b of a triangular reflection nebulosity 15" west of 6-5A [158,345,347]. It is not clear if the infrared colors [490] 381c apply to 6-5B or include another source to the ne [158]. 35a T Tau . The most extensive published light curve is in Lozinsky, Perem.Zvzd. 7, 76, 1950. Additional UBV/RI 35b observations are in [168,220,225,229,236,266,284,410]. Evidence for a photometric period of 2.80 days is in 35c [228]. Low-resolution spectroscopy is in [93,168,303,312], medium in [290,458], and high resolution profiles in 35d [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 35e compromise. Optical observations of the companions are in [121,352,424], radio structure and coordinates in [424, 35f 425], and optical astrometry in [180]. The history of the nebulae associated with T Tauri is given in [59] and 35g references therein. 386a FV Tau . An occultation observation by M. Simon (unpublished) shows the star to be double, with separation 386b 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#. 36a DF Tau . The profile of H@ is shown in [123,187,423]. The spectrum is reproduced or described in [93, 36b 123,187,303,413,423,458,500]. An occultation observation shows the star to be double, with separation 36c 0".011 projected upon p.a. 103#; the K magnitudes are 7.22 (eastern) and 7.73 (western component): M. Simon, 36d unpublished. 37a DG Tau . The emission spectrum is very rich. In the red, "a few vague minima are probably the absorption lines 37b of a late-type star" [212]. Near 8700 A, "broadened absorption features consistent with an early M type" are 37c present [451]. The spectrum is shown or described in [303,312,337,340,458,500]. There is a knot having an HH- 37d like emission spectrum about 8" in 228# from DG [341]. About 55" south-west of DG is a series of emission knots, 37e named "DG Tau B" by [341]. Infrared photometry is in [490], the spectrum described by Jones and Cohen, Ap.J. Lett. 37f 311, L23, 1986, long-slit spectroscopy in [347], CCD direct images in [341,347,451]. There is also reflection 37g nebulosity to the north of DG [206]. 389a GV Tau . A later-type star is imbedded in a very small, HH-like envelope. The object is variable at 2.2 microns, 389b and emission H@ may also vary [160]. Direct images are shown in [128,451]. 39a DI Tau . DI Tau is about 16" from DH in p.a. 125# . It is surprising that the H@ was detectable by [257] 39b if W(H@) is as low as reported in [93]. 390a Lick 6 . Detected by [28] as variable, compact radio sources, the coordinates are from the VLA observations. 390b 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#. 40a LkH@ 101 . The optical coordinates from [8] and [57] are essentially the same; the coordinates of the radio 40b continuum source are in [57,96]. The spectral type of the star, either as observed directly (Allen, M.N.R.A.S. 40c 161, 1P, 1972) as F8: II or as scattered off the nebulosity [200] as F, is in conflict with the Lyman continuum 40d type of early B, probably above the main sequence [57]. The near infrared is dominated by emission lines; 40e 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 43b to A was detected with an image intensifier; it was estimated to be at about 2" in 180# : [250], note to 43c Table II. This star (C) was much redder than A. However, speckle observations have not confirmed its 43d 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. 46a ZZ Tau . This is the variable discovered by Reinmuth; the confusion in HRC is explained in [250], note to 46b Table II. Two Lick spectrograms show narrow H@ and weak He I emission. The star has a very large infrared 46c excess: Rucinski, Astr.J.90, 2321, 1985. 393a L1551/IRS 5. There is an extensive literature on this object, the associated jet, and the more distant nebulosity 393b (Sh 239 = HH 102). Most of the references other than those cited here are in [451]. CCD images of the region are 393c in [341,350,441]. 49a HL Tau . This nebulous, non-stellar object (note in HRC; [453] Fig.6; Grasdalen et al. Ap.J. Lett. 283, L57, 49b 1984) has been classified as cont.(K7?) by [93], and as about M2 by [404], but the absorption spectrum apparently 49c cannot always be seen [101]. Infrared observations and photometry are in [88,100,328,410], and references therein. 49d Scans of the optical spectrum are in [93,101,123,312] and in Cohen and Schmidt, Astr.J. 86, 1228, 1981. Long- 49e slit spectra and CCD direct images are in [341,347,416]. 395a V710 Tau B . The separation is about 3".5 in 180#. The coordinates are of the photocenter. The photometry listed 395b 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.) 397a L1551-51 . According to [506], the scatter in the individual velocity observations suggests that the star is a 397b spectroscopic binary. 399 V827 Tau . [408] find a cyclic variation 12.06-12.28 (in V) with a period of 3.63 days. 400a V826 Tau . According to [408], there is a cyclic variation 12.07-12.14 (in V) with period 4.05 days. The star is 400b also a double-line spectroscopic binary [344] with a period of 3.9063 days; the systemic velocity is given in the 400c 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. 52a UZ Tau e . UZ Tau is double: in 1944, 3".68 in 271#.5 [258]. The coordinates are of the photocenter; almost all 52b the photometric data refer to combined light. The descriptions of the Mt. Wilson observations [256] leave no 52c doubt but that the eastern star in the active component; it was the same star that was responsible for the very 52d bright maximum in 1921 [213]. The eastern component was classified as M1,3 V(Li) in [212] and M1.5 by [93]. 52e The two spectra are shown or discussed in [93,101,123,256,303,337,458]. The radial velocity of the eastern 52f component appears to be variable [123]. 53a UZ Tau w . (See the Note for UZ Tau e). The western star has been classified as: dM3e [258], M4 V(Li) [212], 53b 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]. 59a IS Tau . There is a mixup in the literature because the coordinates of Haro 6-23 (=IS Tau) and 6-26 (=IT Tau) 59b tabulated in [182] are reversed with respect to the stars marked on the identification charts in [182]. Following 59c GCVS3 and 4 and [250], we follow the table rather than the chart, and so take the southwestern star as 6-23 = IS Tau, 59d and the northeastern as 6-26 = IT Tau. Unfortunately this convention was not observed in HRC, which took the north- 59e eastern star as HRC 59 = Haro 6-23 = IS Tau, and as a consequence the identification chart in [410] reflects this 59f error. Another consequence is that HRC 59 is not the same star as HBC 59. 57a GK Tau . During the interval monitored in [492], the light curve showed a series of sharp, unevenly-spaced 57b 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. 408a 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 408b be a pre-main sequence star. 64 HO Tau . There is a mag. 16 star at 8" in 110#. 409a FF Tau . The star was found to be double in an occultation observation [435]. The separation was 0".037 409b projected upon about p.a. 257#. The K magnitudes are 10.06 (eastern component) and 9.06 (western). 65a DN Tau . Extensive photometric observations by [45] suggested rotational modulation with period 6 days; [492] 65b 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#. 413a L1642-1 . A nebulous double star; the very red secondary (1.9 mag. fainter in R) is at 5".8 in about 140# [416]. 413b The star is marked on a photograph in Sandell et al., Astr.Ap. 97, 317, 1981. It was observed (as an IRAS 413c galaxy) by [357]; that scan shows strong Balmer emission lines on an M-type background (D.E. Osterbrock, 413d private comm.). 414 CoKu HP Tau/G3. According to [101], the scans of HP Tau/G2 and /G3 in [93] are interchanged. 415a CoKu HP Tau/G2. (See the note to HP Tau/G3). Lick coude spectrograms of /G2 show H@ absorption with a weak, sharp 415b emission fringe to shortward, and an even weaker to longward. The absorption lines are very wide; Li I 6707 is 415c moderately strong. The spectral type quoted is from those plates. 418a HV Tau . The star has been variously referred to as "companion of DO Tau", "red nebulous star 2' east of DO Tau", 418b 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]. 68a VY Tau . The light curve is discussed in [213, 327]. The colors and type in the Table refer to minimum light. 68b Near maximum, the spectrum is completely different, being dominated by low-excitation emission lines of 68c 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.) 74a DR Tau . The star was faint, near B = 14, prior to about 1961. In 1946, it had been classified dK5e, "spectrum 74b veiled by continuous emission" [257]. It brightened 2-3 mag. in B between 1961 and 1980, with major fluctuations 74c [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, 74d 297,303,337,481]. The dK absorption spectrum is no longer detectable (at least in the red), but a spectrum 74e rather like that of an F star can be seen in the IUE ultraviolet [220]. 75a DS Tau . The dF0 companion, m(pg) = 13.7, is roughly 8" from DS (not 4" as in [257]); it was excluded from the 75b UBV observations of [25]. The mean velocity velocity of DS, +16.3 % 2.3 km/s from 3 observations [189], is 75c to be preferred to the value of 0 % 2 km/s of [219] from 6 spectrograms, but the discrepancy is puzzling. The 75d type in the Table (K5 V) is a reclassification from Lick coude material; [93] gave K3 and [257] dK4. 76a UY Aur . The star is a close double; [258] give 0".82 in 212# in 1944; the companion was about 0.5 mag. the 76b fainter at that time. 77a GM Aur . Repeated velocity observations by [189] give a constant value of +15.0 % 1.3 km/s, which is quite diff- 77b erent from the mean of -3 % 4 km/s, from 6 plates, of [219]. The discrepancy is unexplained. [257] gave +24 km/s, 77c 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]. 78a AB Aur . Since HRC, the star has been studied in detail by Catala, Praderie and co-workers. References to their 78b earlier work are in [68]; their IUE spectroscopy is in Ap.J. 254, 658, 1982 and 303, 311, 1986; Astr.Ap. 140, 78c 421,1984 and 182, 115, 1987. Further UBV/RI observations are in [31,50,225,229,430], and infrared in [3,31,32, 78d 55,81,87,91,155,316,372,452]. There is evidence for rotational modulation in the line profiles with a period 78e of 40-50 hours; see also [137]. 79a 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 79b was found to be 14 A. There is suspicion of a rotational modulation in light with a period of either 2.73 or 79c 1.55 days [229]. 427 NTTS 045251. According to [506], this is a single-line spectroscopic binary. 428a V347 Aur . The star illuminates a variable nebula. The light curve resembles that of a long period variable. A 428b 1978 Lick coude spectrogram shows strong, rather narrow H@, fairly strong [O I] anf Fe II, and probably He I 428c emission. 429a V836 Tau . The cyclic variation found by [409] has a period of 6.99 days. The star was identified incorrectly on 429b the original chart [132]. 430a UX Ori . The star is not convincingly associated with nebulosity, so it may not belong to the Ae/Be class. There 430b have been extensive UBV observations: [226,229,273,276,478,527,530]. 81a RW Aur B . The coordinates are based on the offset from A; the only actual double star measurement is that of 81b [258]: 1".22 in 254#.3, made in 1944. When A is near minimum light, the companion contributes significantly to the 81c light and spectrum. 80a 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 80b photometric observations are collected in [410]. The optical spectrum has been reproduced or discussed in [1,16, 80c 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 80d cycle in both the light (Herbig 1962) and in the line structure [174]. Repeated radial velocity observations 80e by [189] suggest that the velocity may be variable, with a range of about 10 km/s. 431a V1012 Ori . This object was observed as an IRAS galaxy by [357], but found to be a Be star. The variability was 431b discovered by Morgenroth (Astr.Nach.253, 441, 1934 [with chart]; 254, 366, 1935). The scan of the red region by 431c [357] shows H@ emission central on broad absorption wings, and strong Na I D lines. 83a V534 Ori . The coordinates are for St 37, identified with V534 Ori by [444], but [118a] identify the variable 83b with St 38. 84a CO Ori . Elvey and Babcock (Ap.J. 97, 412, 1943) classified the spectrum as early F, with peculiarities; it has 84b since been typed gF3 (Joy and Wilson, Ap.J. 109, 231, 1949), F8:n [212] and G5 [93]. When the star was near 84c minimum light about 1950, Herbig saw it as double (about 1" in 280#), but [22] could detect no such companion 84d in 1980, with CO near maximum. Additional UBVRI observations are in [91,225,229,236,328]. 85a GW Ori . The spectrum has been classified as G5 (Zappala, Ap.J.172, 57, 1972); G5: [93]; G5,8 V [212]; and dK3 85b [257]. Additional RI observations are in [236,328]. 86a V649 Ori . There is a faint companion at 1".41 in 350#; $m is about 2 mag. The UBV photometry of [338] 86b includes both stars. There was marginal evidence [22] for another star at 0".47, p.a. 36# or 216#. Other 86c 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. 88a V370 Ori . The strength of H@ emission must be variable, because the W(H@) reported by [93] would not have been 88b detectable on objective prism plates. See the note in HRC regarding the clustering of emission-line stars around 88c 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. 435a AB Dor . Additional UBVRI observations are by Lloyd Evans, Circ.So.African Astr.Obs. no. 11, 73, 1987, and by 435b Collier Cameron, ibid. p. 57. The reasons for suspecting that this may be a pre-main sequence star are in [486]. 435c The mean radial velocity in the Table is that of [103]; the velocity may be variable with a range of about 22 435d km/sec: [244]. 94a HK Ori . This star is at the apex of the reflection nebula PP 29. There have been numerous infrared observations: 94b [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]. 436a RY Ori . The spectrum may be composite: He I 5875 suggest a B star, yet the remainder of the spectrum in the red 436b is about F8. H@ is a strong double emission line, and Li I 6707 is present in moderate strength. The star can 436c be identified from the chart by Wolf, Astr.Nach.171, 77, 1906, where it is 117.1904. 437a P1207/c . The companion is at 25" in 75# from A [93]; it has weak H@ emission. [93] found no H@ emission, despite 437b the objective-prism detection. The UBV colors in [11] must be in error. The coordinates are those of the primary. 104a VY Ori . There is a fainter star about 15" from VY in p.a. 135# . According to [497], its colors are: V=16.35, 104b 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. 447a P1540 . According to [324], the star is a double-line binary with P = 33 days; both stars show strong Li I 6707 447b 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 447c the Table is from a Lick coude plate. According to [483], the star is not a member of the Orion cluster. 452a P1724 . A non-member of the Orion cluster according to [483], although the spectroscopic criteria indicate that 452b it is a pre-main sequence star. 456a MR Ori . The star is projected upon very bright nebulosity, so it is has not been possible to determine whether 456b there is emission in the core of H@ or not; certainly no stellar emission lines are present elsewhere in the 456c spectrum. The star is included in this Catalog solely on the basis of its (alleged) variability and location in 456d the Orion Trapezium cluster. 457a AE Ori . The nebulosity is very bright, and from the single Lick spectrogram it was impossible to determine 457b whether stellar H@ emission is present or not. 459a P1925 . A Lick CCD spectrogram shows a fairly strong Li I 6707 line, but there is no evidence for emission at 459b 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]. 464a CQ Tau . The UBV data are for maximum light [166]. The H@ region was described by Bonsack and Greenstein (Ap.J. 464b 131, 93, 1960). A Lick coude plate of 1973 showed double H@ emission upon broad absorption wings. The absorption 464c spectrum otherwise is like an early F star. 466a AH Ori . The spectrum was classified K0 IV,V by [248]. A Lick coude plate shows H@ in absorption, with no certain 466b emission component; this appears to be a genuine example of a pre-main sequence star without obvious line emission, 466c at least in the red. 471a NV Ori . [270] regard this star as constant, but [227] report a V range of 0.6 mag. there is complex emission in 471b H@, supertimposed upon absorption wings. Li I 6707 is present but not unusually strong. 148a NY Ori . The star is normally faint, but when near maximum has the emission spectrum described in [197]. It is 148b 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]. 154a T Ori . According to Shevchenko (Flare Stars and Related Objects [ed. L. Mirzoyan], p. 230, 1986), T Ori is a 154b 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. 164a V380 Ori . This is nearly unique among the T Tauri stars in having an A-type spectrum. It is ADS 4209, but that 164b companion (mag. 13.0, about 3" in 220#) and another suspected by Jonckheere (Mem.R.A.S. 61, 57, 1917) were 164c probably only structure in the nebula NGC 1999. No such stars are detectable on modern photographs, nor can 164d any be seen visually at the 120-inch telescope. Additional UBVRI observations are in [116,229,328,378], and 164e additional spectroscopy in [413]. A polarization map of the nebulsoity by Warren-Smith et al. is in M.N.R.A.S. 164f 192, 339, 1980. 484 P2441/c . The separation is 4".5 in 145# [93]. The coordinates are those of the primary. 167a P2441 . Spectral types assigned have been: G1 IV [411], G3 [329], G5 [93], and "about G8n" from Lick spectrograms 167b in the red. All conflict with the blue-region type of F5: in HRC. There is very strong, slightly asymmetric 167c emission in H@. There is a nebulous patch (HH 63) about 30" southwest (Reipurth and Graham, priv. comm.). 485a V586 Ori . Lick spectrograms showed strong complex emission, variable with time, in H@. It is superposed upon the 485b 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]. 489a V883 Ori . This is the faint red variable slightly west of the apex of the reflection nebula IC 430 = Haro 13a 489b (see [453], Fig. 5). The entry is retained although there is no evidence that the star has ever exhibited H@ 489c emission: [7,181,312,363]. 490a Haro 2-249/c. The coordinates are approximate. These two stars and the ring-shaped nebula associated with the primary 490b are shown on a CCD image in [161] and on [453] Fig. 5. 492a +26# 887 . This is the "nebulous star 3' from RR Tau" in [203]. No emission was present in the photographic region 492b on early Lick spectrograms, but P Cyg structure is present at H@ on a 1982 coude plate. 493a V350 Ori . A 1973 Lick spectrogram showed complex H@ emission, with narrow central reversal, superposed upon the 493b absorption wings of an early-type star. He I 5875 is rather strong, so a B type is indicated. 494a Reipurth 50. The coordinates are of the approximate center of a nebulosity that is believed [386] to be illuminated 494b by a heavily obscured star about 1'.5 north. The nebula is variable in brightness. 182a San 6 . A 1978 Lick coude spectrogram showed a strong, symmetric H@ emission line and a well-defined K-type 182b absorption spectrum. The observation of San 6 in [93] must refer to another star. 185a V631 Ori . [93] found no H@ emission in 1976, yet rather strong emission in the photographic region was observed at 185b Lick in 1960, and the star was originally detected on the basis of a bright H@ line [322]. 186a FU Ori . The coordinates are from Duerbeck, Sp.Sci.Rev. 45, 1, 1987. The earlier history of FU Ori is summarized 186b in [207,213]. It remains not far below maximum light. The UBVRI data in the Table are rough means from extensive 186c observations in 1984-85, during which time a cyclic variation of length 9 or 18 days was present [286]. The 186d spectrum is very complex, and the type assigned appears to depend on wavelength; the value in the Table is for 186e the red region. References to infrared and recent high-resolution spectroscopy, and other properties of the 186f spectrum, are [188,190,191]. Although not expressed in terms of v sin i, [190] gives line widths measured in 186g a variety of spectral regions. 502a SSV 61 . This star, in a complex reflection nebulosity, is object 140 in [448], Fig. 1a; it is also in [211], 502b Fig. 8. It was classified as an M2,4 giant by [448]; a Lick CCD spectrum indicates a slightly earlier type. 515a +1# 1156 . This peculiar star illuminates the nebulosity Par 3 = PP 46. The presence of Li I 6707 is confirmed on 515b 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.) 516a 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 516b apparent on the identification chart in HRC. According to [93], there is another star at 6" in 140#, 5 mag. 516c 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. 199a MWC 137 . As noted in HRC, this is a high-luminosity object that may not be pre-main sequence. The star is sur- 199b rounded by a 56" x 80" ring of nebulosity; it is 195 -0# 1 = Sh 2-266 in Perek and Kohoutek "Catalogue of 199c Galactic Planetary nebulae", which gives an identification chart. 200a LkH@ 340 . The labels on the charts for LkH@ 340 and 341 in Figs. 4 and 5 of HRC were interchanged. Drs. U. 200b Bastian and M. Cohen have confirmed that their respective observations [25,93] were of the stars at the coordinates 200c 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. 529a HD 259431 . Although this star is often considered a member of the Ae/Be class [203], the possibility still exists 529b that it is a conventional Be star. The modern spectral classifications range from B2e [138] to B5 [452] and 529c B6pe [224]. 207a R Mon . The coordinates are those of feature "a" at the apex of the small (about 3") triangular nebulosity 207b known as "R Mon" [251]. Its brightness dpends heavily upon aperture size and angular resolution. The spectrum 207c is peculiar and variable: see [208,251] and references therein. Infrared speckle observations are in [29], and 207d infrared spectrophotometry in [87]. The structure of the nebulosity in [S II] is described by Brugel et al. 207e (Ap.J. Lett. 287, L73, 1984), and photometry and polarimetry of NGC 2261 are in [21] and in Warren-Smith et al. 207f 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] 207g 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]. 534a W68 . The various spectral classifications are not in good agreement, probably because of the very broad lines: 534b F2 [488], F4 V [526], G0 IV,V [494]. 219a V590 Mon . The spectrum is peculiar, and at low resolution there has been considerable disagreement in the classi- 219b 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]. 535a W121 . The star is located very near S Mon, which may account for the large discrepancies is the published UBV 535b photometry, amounting to 2 mag. in V: [414,433,494]. A Lick CCD spectrogram showed moderately strong H@ emission 535c with central reversal, and strong Li I 6707 absorption. 227a IP Mon . The star is very closely nebulous. The type K3 was assigned by [93,401], while [488] give K2 and [526] 227b 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. 543a OX Mon . The emission originates in the northeast component of a close pair (7" in 35# : [93]). The photometry 543b refers to the combined light. No emission is seen in the other component [93]. 546a NGC 2313 . The involved star has a complex emission structure at H@, and in the red an absorption spectrum perhaps 546b of type G with very strong Ba II lines. 548 LkH@ 218 . This may be an ordinary Be star. 243a Z CMa . The spectrum is very complex and possibly composite. References to earlier spectroscopic work are in 243b HRC; more recent papers: [104,123,452]. The optical and VLA coordinates are not in close agreement [96]. An 243c optical companion was reported in [139] but has not been confirmed. Infrared speckle observations show the star 243d to be slightly extended in the east-west direction [311]. UBV/RI photometry is in [50,91,225,229,275]. Many 243e infrared observations have been reported: [3,31,32,81,87,155,224,273,316,372,452]. The VLA observations are 243f in [34,96,101]. 551 LkH@ 220 . This may be an ordinary Be star. 552a NX Pup . The spectral type in the Table is a compromise: the star has variously been classified as A0-1 III 552b [478], A1 [138], F0 Ipe [245], F1-2 [381], and F2 III [49]. H@ is in emission but the decrement is very steep. 563a ESO313-N*10. At least 9 condensations, most of them red with H@ in emission, are imbedded in a bluish nebulosity about 563b 35" in diameter having an early-type absorption spectrum. 565a SY Cha . The type M0: is from [17]; an earlier classification was K2 V [12]. The star has shown a cyclic 565b variation in brightness with range 1.6 mag. in B and a period of 6.129 days [259,325,422]. 567a 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 567b also concurrent changes in the emission spectrum [259]. 568a TW Hya . The spectrum is in all respects like that of a T Tau star, but there is no nearby cloud. Three Lick 568b spectrograms gave velocities of -9, +12 and +9 km/s, a range large enough to raise the suspicion that the star may 568c be a binary. 569a 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 569b from [17] differs from the 59 A in [403]. 570 CT Cha . The type K7: is from [17]; [196] give G8:. 575a VW Cha . Variability of H@ was suspected from the first observations [196], and confirmed by later results [17, 575b 403]. A mean value is given in the Table. The K2 type is from [17], but the star was classified earlier as 575c 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:. 588a Sz 41 . The coordinates and photometric data are for Sz 41, while the infrared references and spectral type 588b refer to HJM E1-9a. The coordinates of the two objects agree within about 10", and it is assumed that they are 588c the same. [238] state only that line emission is present, giving no details 591a T Cha . T Cha has sometimes been regarded as a pre-main sequence star on the grounds of its rapid, irregular 591b variability and location on the edge of a small dark cloud [232,233], but spectroscopic proof is lacking. There 591c is no obvious emission at H@ or elsewhere; unfortunately the Li I 6707 region has not been observed adequately. 591d A cyclic variation with a period of 3.2 days has been suggested [325]. 592a Bipolar nebula. The spectral type refers to the northern lobe [351]. The southern extension has an HH-like spectrum; 592b there is probably an A0 star involved. Polarimetry of the nebulosity is in [461]. The UBV data were taken through 592c a 23" aperture [508]. It is uncertain whether this is a pre-main sequence object. 595a S2 . S2 is considered [421] to be the central object of a nebulous cluster, but earlier [58] was regarded as 595b the central star of a bipolar nebula. The coordinates are approximate. 251 RU Lup . Additional UBV/RI observations are in [25,145,266,427]. 252a RY Lup . A quasiperiodic variation of length 3.76 to 4 days was discovered by Hoffmeister [232], and confirmed by 252b more recent work [46,129,314]. W(H@) ranges from invisibility [17] to about 25 A [314], apparently in 252c antiphase with the light cycle. 253a EX Lup . The photometry refers to minimum light, but the values in the Table are the brightest of 7 observations 253b [25]. References to earlier work on the star, especially near maximum, are in HRC and [213]. 617a Sz 102 . The spectrum contains strong emission lines of [O I], [N II], [S II],..., characteristic of HH Objects, 617b superposed upon a late-type continuum and stellar absorption spectrum [17,295,299,426]. Two isolated patches of 617c emission nebulosity lie about 13" e and w of the star [295]. 619a V856 Sco . Observations in the Stromgren and Walraven photmetries are in [467,468,469]. The star is reputed to have 619b a close companion (Rst 3930B, at 1".3, mag. 12), but it was not detected in speckle observations [22]. 631a Sz 124 . The fact that the star was detected by objective prism observers [426,463] seems incompatible with the 631b low value of W(H@) = 1.6 A in [17]. 632a V866 Sco B . The companion is about 1".4 in 20# from the (slightly) brighter primary. Both stars have the infrared 632b Ca II lines strongly in emission. The coordinates and photometry refer to the combined light. 254a V866 Sco A . The type K0 assigned in [93] was not in acceptable agreement with the M0: of [212]. Reexamination of the 254b Lick material shows that it clearly lies betwee K3 V and M0 V, hence the K5 V in the Table. Narrow He I emission 254c lines are present. The coordinates and photometry refer to the combined light. 634a Wa Oph/3 . H@ emission was discovered by The [465], which is surprising considering the low value of W(H@) = 0.3 A 634b in [502]. 637a DoAr 21 . H@ emission was reported by objective-prism observers between 1949 and 1960, but has not been seen on 637b slit spectrograms since 1973. The object at that position is very variable as observed with the VLA, and moderately 637c 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. 260a DoAr 22 . The coordinates are those of the m(pg)=13.0 star, type F5:e, listed in HRC. The emission-H@ object 260b 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; 260c its spectrum has not been observed. 639a DoAr 24E . According to [539], the star is double, separation 1".95 in p.a. 0# . The only positive detection of H@ 639b emission is by [524]. The X-ray emission probably originates in DoAr 24. 262a SR 24 s . The coordinates are of the photocenter of the pair (6" in 60# ); individual positions are in [524]. The 262b ROX observation included both stars. A variation 16.4-17.1 (pg) is observed in the combined light [369]. Attention 262c 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). 640a ROX 20-1 nw. The separation of the pair is about 13" in 302# . X-ray flaring has been detected in the unresolved 640b 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). 263a S-R 12 . Speckle observations show the star to be a close double (0".30 in about 85#), with K magnitudes 263b 9.34 (eastern) and 9.17 (western). It was also resolved in an occultation observation [435]. 642a ROX 31 . The coordinates are from a VLA observation. The spectroscopic observation is by Bouvier and Appen- 642b zeller, quoted in [10]. The star was not detected in the H@ surveys of the region. An occultation observation 642c [435] showed the star to be double with separation 0".13 projected upon p.a. 337#. The K magnitudes are 8.72 642d (eastern) and 9.00 (western component). 265a SR 10 . There is a large difference between the W(H@) values of [17] and those of [93,402]; the mean of the 265b latter is given in the Table. 644a Haro 1-14/c. Haro 1-14 is actually the fainter, southeastern component of the pair of stars (separation about 10") at 644b this position. The UBV photometry refers to the combined light. The brighter star, here called Haro 1-14/c, has 644c emission cores in H,K [404]. 267 Haro 1-14 . (See remark for Haro 1-14/c). 645a Reipurth 13. This a a faint, extended nebulosity (6" x 8"), apparently scattering the light of an imbedded star 645b having H@ in emission [9]. 646a V346 Nor . This very red star is at the edge of HH 57 [426]. Originally discovered as an infrared source [384], it 646b became detectable in the visual region about 1983: [102,169,382] and references therein. 271a AK Sco . The type is from the Michigan Spectral Catalogue and Lick coude material. The spectrum in the red 271b appears composite. Two Lick CCD scans show double lines with a splitting of about 200 km/s; at other times the 271c lines have been single. Clearly, the star is a double-line binary. Li I 6707 is strong in both components. 655a V921 Sco . The emission spectrum of this nebulous star was noted independently by Vandervoort and The 655b (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. 272a IX Oph . Lick coude spectrograms show sharp H@ emission on a weak metallic-line spectrum; Li I 6707 is not 272b present. The star's image is marked on Pl. I of [464], but no number was assigned. 273a 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 273b magnitude difference about 1 mag. Narrow [N II] and [S II] lines are present in the brighter component; [Fe II] 273c emission has been reported in the blue [6]. 275a LkH@ 346 nw. [93] give 6".5 in 130# as the position of the se component with respect to the nw. The coordinates 275b 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]. 280a SV Sgr . The star is superimposed on the very bright H II region NGC 6523. Lick coude spectrograms show P Cyg 280b 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]. 662a V4046 Sgr . [113] find the star to be a single-line binary with P = 2.43 days; [62] suspect double lines. W(H@) 662b varies between 30 and 120 A. Flaring was observed by [61]. The star can be identified from the HDE chart (Harv. 662c Ann. 112, 1949). 663a -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 663b photometry refer to the combined image. It is not known which component is the flaring variable. According to 663c [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. 672a 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 672b polarization map of the nebula (called the "Serpens object" in [453]). Their Fig.1 identifies the infrared 672c sources in the area; their Pl. 1, and Fig. 7 of [453], are photographs of the region. 284a AS 310 . See the remarks in HRC. The photometry contains the contribution of a faint companion at 3-4" [25,139]. 284b A Lick coude spectrogram shows shallow absorption under the sharp central H@ emission, and narrow He I absorption 284c 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. 286a S CrA . The emission spectrum is very strong, and the underlying absorption spectrum can be seen only with 286b difficulty. The star is a close double, usually not resolved photometrically or spectroscopically. Discovered 286c by [258], it was remeasured by [22]: separation 1".37, p.a. 147#, $m about 1 mag. in 1981. Additional UBV 286d photometry is in [25,263,266,323,336]. The spectrum is reproduced or discussed in [17,18,122,212,323,336,337, 286e 400,401]. 287a TY CrA . See the remarks in HRC. there may be a weak emission component in H@ [139]. According to [264], the 287b star is an eclipsing variable with P = 2.888797 days. The other bright star in NGC 6726/7, CoD-37# 13023, has a 287c 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. 288a R CrA . Published V's show large scatter, due either to real variability or the effect of the nebular background. 288b Rapid changes in the nebula and in the H@ profiles in nebula and star have been described by Graham and Phillips 288c (Pub.A.S.P.99, 91, 1987). 289a DG CrA . See the remark in HRC. Since that time, H@ emission has apparently been detected by [274] and [323]. 289b The coordinates are approximate, from Van Gent (B.A.N.7, 21, 1933). 290a T CrA . There is a difference of about 2 mag. between the V's of [329] and those of [273] and [323], possibly due 290b to variability. 681a FG Aql . The type in the Table (K2) is from [93], but a Lick coude spectrogram in 1977 was classified as K7,M0 V 681b with strong Li I 6707, and double H@ emission (R>V). 684a WL 22 . This object was found by Wooden and Lada (unpublished). A 1981 Lick spectrogram showed narrow H@ 684b emission line flanked by an extremely broad, strong P Cyg-type absorption structure. 292a V1352 Aql . This is the "exciting star" of HH 32. The V, B-V values are means from [288]. The emission spectrum has 292b been investigated by [40,218,293,294,337,342,423]. Perhaps on account of P Cyg structure, the various W(H@)'s do 292c 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