HBC REMARKS TO TABLE 1

     V633 Cas   

The spectral type is uncertain. Infrared observations are in [2,3,32,71,82,91,316].

   VX Cas  

There was some uncertainty in the identification of this star in the earlier literature. The coordinates and other data in Table 1 refer to the star indicated as VX Cas in Aarhus Medd. no. 10, 150 (1937), Kasan Bull. 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 bright nebulosity nearby.

   V594 Cas   

The absorption spectrum is confused by line emission; the types assigned range from O9.5 to B8,9: see [138].

     LkH 201   

This is probably a background Be star.

   RNO 6   

The photometry is of the star in the brighter lobe of this reflection nebulosity. A polarization map is in [420].

     LkH 262   

LkH 262, 263 are separated by about 15" in 22° . They and LkH 264 lie in L1457, but are not to be identified with the X-ray source in that cloud found by Halpern and Patterson, Ap.J. Lett. 312, L31, 1987.

     LkH 263   

(See remark for LkH 262.)

   IRAS 0313  

This nebulous star was observed at the request of Iyengar. An underexposed Lick coude spectrogram in 1986 showed only strong double H emission (R>V) on a weak continuous spectrum.

    LZK 4  

A 1983 Lick coude spectrogram of the red region shows an unusually broad, structured H emission with a reversal displaced somewhat shortward of center. A few weak absorption lines are present, and the D lines are fairly strong, but Li I 6707 Å is not apparent. The type was classified as mid-K by [118a].

   SSV 13  

No stellar absorption spectrum can be seen with certainty; H, [O I] and [S II] are very strong, as in H-H Objects [160].

   IP Per  

It is not certain if this is a pre-main sequence star. Two Lick coude spectrograms (1973, 1981) showed strong, structureless H emission upon broad, stellar absorption wings. The only other stellar features present were broad Na I D lines.

    LkH 330   

The spectral type is not well determined; a Lick coude spectrogram was classified as "about F6".

   XY Per e   

The star illuminates a large reflection nebula. XY Per is ADS 2788; coordinates and photometry refer to the combined light. There has been no change in the relative position since 1904; the mean separation is 1".35, p.a. 75° . The photometric range is so large that both components must be variable; the magnitude differences noted by the double star observers can account for only a fraction of the amplitude [47]. The eastern star (B) was the fainter at all the Lick observations (1961-73). It was earlier classified as B6, but superior modern material indicates middle A in the blue, but late B in the red. The v sini quoted is from the metallic spectrum. There are fairly strong, double emission cores in the H absorption line.

   XY Per w   

The western star (A) has a peculiar spectrum. Originally called A2 II (Herbig 1952), modern coude spectrograms show sharp, double core structure in Ca II K and the higher Balmer lines; this structure is variable with time. The Fe I lines are the widest species (v sini = 120-140 km/s), and suggest a type of A2 or A5. Lines of Fe II and Ti II are narrower and strong; Ti II 3685, 3759, 3761 Å are prominent, as in shell spectra. Broad central emission, divided by a central reversal, is present in H. Weak, broad He I absorption lines suggest a late B type.

   NTTS 035135

Weak emission cores are present in the H,K lines but H is absent, presumably being filled-in to the level of the continuum.

   NTTS 040012

NTTS 040012+2545N and S are separated by about 1". The coordinates, photometry etc. are for the combined light. The Li I 6707 Å is observed in the combined spectrum.

   NTTS 040012

(See remark for preceding star.)

   PP 13 s

The s, brighter lobe shows a scattered M-type spectrum with prominent [O I], [S II] but no H. The illumination is from a heavily obscured infrared source near the ne edge. The n lobe is nearly stellar, and has a T Tauri-like spectrum. The coordinates in both cases refer to the infrared peaks. Note this is PP 13, not Par 13.

   PP 13 n

(See remark for preceding entry.)

   LkCa 1  

The radial velocitites of both [212] and [192] are well off that expected for a star associated with the Taurus clouds.

   Anon 1  

This is the "nebulous star 11' in 300 from HD 283447" of [212]. It is identified on the chart for LkCa-1 in [219].

   V773 Tau   

According to [408], there is a cyclic variation of 10.62-10.76 (in V) with period 3.43 days.

    CW Tau  

The radial velocity value quoted is from [189], but the velocity may be variable [123]. The [O I], [S II] lines are unusually strong. The spectrum is discussed or reproduced in [93,123,404,458,500].

   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 also identified in [257]. The identity with the Haro s6-2 of [93] was confirmed by M. Cohen.

    V410 Tau   

Additional UBVRI observations are in [220,236,390,410]. A cyclic variation 10.82-11.04 (in V) with period 1.92 days is present [408]. The radio source at the star is variable: [34,96,101,305].

   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 identified in [93]. It was discovered originally as an infrared source by D. A. Allen (private comm.).

   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 also identified in [93].

   CoKu Tau/1 

This star is 10 mm north, 12 mm east of CZ Tau on the chart for that star in [410].

   FQ Tau  

The star is identified in [182]; it is also identifiable as the image 9 mm north, 9 mm west of "WK X-ray 1" on the chart for that star (V819 Tau) in [410].

    BP Tau  

[492] found a cyclic variation 12.07-12.27 (in V) with period 7.6 days. High-resolution line profiles are shown in [340,423], and lower resolution spectra in [93,212,303,458].

   V819 Tau   

According to [409], there is a cyclic variation with period 5.59 days.

    RY Tau  

The historical light curve is in Kholopov, Perem. Zvzd. 13, 430, 1961, and in [534]. Additional UBV/RI observations are in [220,225,227,229,266,281,284,410,492,511,528]. Observations of H are in [91,93,123,220,282,423,531], of the spectrum in [123,220,281,294,303,340,423,458], and of the variable nebulosity in [206]. Velocity variation was suspected in [212]. Extensive Lick observations gave inconsistent results: 1977-78, the velocity scattered between +5 and +30 km/s (14 plates); 1978-79, constant at +20.0 ± 1.0 km/s (12); 1979-80, constant at +18.3 ± 1.5 km/s (8). The higher-accuracy observations of [189] gave an apparently constant value of +16.5 ± 2.4 km/s in 1981-85. The possibility that the star is an unresolved double was raised by [353].

   HD 283572  

The light varies sinusoidally in a period of 1.548 days [505].

   Haro 6-5B  

Haro 6-5B is a very red, presumably stellar source (probably a T Tauri star: [99,347]), in the sw corner of a triangular reflection nebulosity 15" west of 6-5A [158,345,347]. It is not clear if the infrared colors [490] apply to 6-5B or include another source to the ne [158].

    T Tau   

The most extensive published light curve is in Lozinsky, Perem.Zvzd. 7, 76, 1950. Additional UBV/RI observations are in [168,220,225,229,236,266,284,410]. Evidence for a photometric period of 2.80 days is in [228]. Low-resolution spectroscopy is in [93,168,303,312], medium in [290,458], and high resolution profiles in [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 compromise. Optical observations of the companions are in [121,352,424], radio structure and coordinates in [424,425], and optical astrometry in [180]. The history of the nebulae associated with T Tauri is given in [59] and references therein.

   FV Tau  

An occultation observation by M. Simon Ap.J. 375 224c 1990, shows the star to be double, with separation 0".56 projected upon p.a. 55° ; the K magnitudes are 8.05 (eastern) and 8.50 (western component).

   FV Tau B   

The quoted coordinates correspond to a separation from FV of 12" in 105°

    DF Tau  

The profile of H is shown in [123,187,423]. The spectrum is reproduced or described in [93,123,187,303,413,423,458,500]. An occultation observation shows the star to be double, with separation 0".011 projected upon p.a. 103 ° ; the K magnitudes are 7.22 (eastern) and 7.73 (western component): M. Simon, unpublished.

    DG Tau  

The emission spectrum is very rich. In the red, "a few vague minima are probably the absorption lines of a late-type star" [212]. Near 8700 Å, "broadened absorption features consistent with an early M type" are present [451]. The spectrum is shown or described in [303,312,337,340,458,500]. There is a knot having an HH-like emission spectrum about 8" in 228° from DG [341]. About 55" south-west of DG is a series of emission knots, named "DG Tau B" by [341]. Infrared photometry is in [490], the spectrum described by Jones and Cohen, Ap.J. Lett. 311, L23, 1986, long-slit spectroscopy in [347], CCD direct images in [341,347,451]. There is also reflection nebulosity to the north of DG [206].

   GV Tau  

A later-type star is imbedded in a very small, HH-like envelope. The object is variable at 2.2 microns, and emission H may also vary [160]. Direct images are shown in [128,451].

    DI Tau  

DI Tau is about 16" from DH in p.a. 125° . It is surprising that the H was detectable by [257] if W(H) is as low as reported in [93].

   Lick 6  

Detected by [28] as variable, compact radio sources, the coordinates are from the VLA observations. The spectral types and W(H) values were estimated from the published scans.

    IQ Tau  

There is another star of about m(pg) = 17 at 10" in 301° .

    LkH 101   

The optical coordinates from [8] and [57] are essentially the same; the coordinates of the radio continuum source are in [57,96]. The spectral type of the star, either as observed directly (Allen, M.N.R.A.S. 161, 1P, 1972) as F8: II or as scattered off the nebulosity [200] as F, is in conflict with the Lyman continuum type of early B, probably above the main sequence [57]. The near infrared is dominated by emission lines; infrared observations are in [209,326,434,436,472]. A polarization map of the nebulosity is in [379].

   Lick 3  

(See the remark for Lick 6, NGC 1579.)

    UX Tau B   

The coordinates given are the coordinates of the A component.

    UX Tau A   

[189] note that the velocity may be variable. In 1975, at the 120-inch coude, a close, faint companion to A was detected with an image intensifier; it was estimated to be at about 2" in 180° : [250], note to Table II. This star (C) was much redder than A. However, speckle observations have not confirmed its existence [22].

    DK Tau  

The star is extremely variable in UBV. [93] gives W(H) = 19 Å, while [91] find a range of 37 to 150 Å.

    ZZ Tau  

This is the variable discovered by Reinmuth; the confusion in HRC is explained in [250], note to Table II. Two Lick spectrograms show narrow H and weak He I emission. The star has a very large infrared excess: Rucinski, Astr.J.90, 2321, 1985.

   L1551/IRS 5

There is an extensive literature on this object, the associated jet, and the more distant nebulosity (Sh 239 = HH 102). Most of the references other than those cited here are in [451]. CCD images of the region are in [341,350,441].

    HL Tau  

This nebulous, non-stellar object (note in HRC; [453] Fig.6; Grasdalen et al. Ap.J. Lett. 283, L57, 1984) has been classified as cont.(K7?) by [93], and as about M2 by [404], but the absorption spectrum apparently cannot always be seen [101]. Infrared observations and photometry are in [88,100,328,410], and references therein. Scans of the optical spectrum are in [93,101,123,312] and in Cohen and Schmidt, Astr.J. 86, 1228, 1981. Long-slit spectra and CCD direct images are in [341,347,416].

   V710 Tau B 

The separation is about 3".5 in 180° . The coordinates are of the photocenter. The photometry listed for the northern component is of the combined light; [93] give V = 14.5: for the northern star alone.

    V710 Tau A 

(See remark for V710 Tau B.)

   L1551-51   

According to [506], the scatter in the individual velocity observations suggests that the star is a spectroscopic binary.

   V827 Tau   

[408] find a cyclic variation 12.06-12.28 (in V) with a period of 3.63 days.

   V826 Tau   

According to [408], there is a cyclic variation 12.07-12.14 (in V) with period 4.05 days. The star is also a double-line spectroscopic binary [344] with a period of 3.9063 days; the systemic velocity is given in the Table.

   FZ Tau  

This star is erroneously called "FY Tau" in [250], Table II.

    GG Tau  

According to [93], there is a star about 4 mag. fainter, at about 12" in 205° , which has H in emission.

    UZ Tau e   

UZ Tau is double: in 1944, 3".68 in 271.5° [258]. The coordinates are of the photocenter; almost all the photometric data refer to combined light. The descriptions of the Mt. Wilson observations [256] leave no doubt but that the eastern star in the active component; it was the same star that was responsible for the very bright maximum in 1921 [213]. The eastern component was classified as M1,3 V(Li) in [212] and M1.5 by [93]. The two spectra are shown or discussed in [93,101,123,256,303,337,458]. The radial velocity of the eastern component appears to be variable [123].

    UZ Tau w   

(See the Note for UZ Tau e). The western star has been classified as: dM3e [258], M4 V(Li) [212], M0.5 [93]. The type given in the Table is a compromise.

   V830 Tau   

There is a cyclic variation in light with period 2.76 days [409].

    GI Tau  

There is evidence for a cyclic variation in light with period 7.2 days [492].

    IS Tau  

There is a mixup in the literature because the coordinates of Haro 6-23 (= IS Tau) and 6-26 (= IT Tau) tabulated in [182] are reversed with respect to the stars marked on the identification charts in [182]. Following GCVS3 and 4 and [250], we follow the table rather than the chart, and so take the southwestern star as 6-23 = IS Tau, and the northeastern as 6-26 = IT Tau. Unfortunately this convention was not observed in HRC, which took the northeastern star as HRC 59 = Haro 6-23 = IS Tau, and as a consequence the identification chart in [410] reflects this error. Another consequence is that HRC 59 is not the same star as HBC 59.

    GK Tau  

During the interval monitored in [492], the light curve showed a series of sharp, unevenly-spaced minima. The maxima between suggested a period of 4.6 days.

   HN Tau/c   

The companion is at 3".3 in 205° [93]. The coordinates are those of the primary.

   Wa Tau/1   

There is weak emission at H and emission cores in H,K, but Li I 6707 Å is not detected, so this may not be a pre-main sequence star.

    HO Tau  

There is a mag. 16 star at 8" in 110° .

   FF Tau  

The star was found to be double in an occultation observation [435]. The separation was 0".037 projected upon about p.a. 257° . The K magnitudes are 10.06 (eastern component) and 9.06 (western).

    DN Tau  

Extensive photometric observations by [45] suggested rotational modulation with period 6 days; [492] found P = 6.6 days, and a V range 12.29-12.42.

   L1642-2

Nebulous; there is a red companion (1.1 mag. fainter in R) at 2".7 in about 13° .

   L1642-1

A nebulous double star; the very red secondary (1.9 mag. fainter in R) is at 5".8 in about 140° [416]. The star is marked on a photograph in Sandell et al., Astr.Ap. 97, 317, 1981. It was observed (as an IRAS galaxy) by [357]; that scan shows strong Balmer emission lines on an M-type background (D.E. Osterbrock, private comm.).

   CoKu HP Tau/G3

According to [101], the scans of HP Tau/G2 and /G3 in [93] are interchanged.

   CoKu HP Tau/G2

(See the note to HP Tau/G3). Lick coude spectrograms of /G2 show H absorption with a weak, sharp emission fringe to shortward, and an even weaker to longward. The absorption lines are very wide; Li I 6707 Å is moderately strong. The spectral type quoted is from those plates.

   HV Tau  

The star has been variously referred to as "companion of DO Tau", "red nebulous star 2' east of DO Tau", 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].

    VY Tau  

The light curve is discussed in [213, 327]. The colors and type in the Table refer to minimum light. Near maximum, the spectrum is completely different, being dominated by low-excitation emission lines of neutral metals. A brief H flare was observed [236] at minimum light in 1985.

   Haro 6-37/c

[93] gives the separation as 3".5 in 40° . The coordinates are those of the primary.

    Haro 6-37  

(See remark for Haro 6-37/c.)

    DR Tau  

The star was faint, near B = 14, prior to about 1961. In 1946, it had been classified dK5e, "spectrum veiled by continuous emission" [257]. It brightened 2-3 mag. in B between 1961 and 1980, with major fluctuations [69,165]. The spectrum is now a hot continuum with strong emission lines of H, He I, Fe II [1,14,33,123,212,220,297,303,337,481]. The dK absorption spectrum is no longer detectable (at least in the red), but a spectrum rather like that of an F star can be seen in the IUE ultraviolet [220].

    DS Tau  

The dF0 companion, m(pg) = 13.7, is roughly 8" from DS (not 4" as in [257]); it was excluded from the UBV observations of [25]. The mean velocity velocity of DS, +16.3 ± 2.3 km/s from 3 observations [189], is to be preferred to the value of 0 ± 2 km/s of [219] from 6 spectrograms, but the discrepancy is puzzling. The type in the Table (K5 V) is a reclassification from Lick coude material; [93] gave K3 and [257] dK4.

    UY Aur  

The star is a close double; [258] give 0".82 in 212° in 1944; the companion was about 0.5 mag. the fainter at that time.

    GM Aur  

Repeated velocity observations by [189] give a constant value of +15.0 ± 1.3 km/s, which is quite different from the mean of -3 ± 4 km/s, from 6 plates, of [219]. The discrepancy is unexplained. [257] gave +24 km/s, but from 2 low-dispersion plates. The type of K3 V of [212] is confirmed on reexamination; [93] gave K7,M0.

   LkCa 19

The type is K5 (Li) according to [506]. The W(H) is a compromise of values from [189,219,506].

    AB Aur  

Since HRC, the star has been studied in detail by Catala, Praderie and co-workers. References to their earlier work are in [68]; their IUE spectroscopy is in Ap.J. 254, 658, 1982 and 303, 311, 1986; Astr.Ap. 140, 421,1984 and 182, 115, 1987. Further UBV/RI observations are in [31,50,225,229,430], and infrared in [3,31,32,55,81,87,91,155,316,372,452]. There is evidence for rotational modulation in the line profiles with a period of 40-50 hours; see also [137].

    SU Aur  

Additional UBV data are in [50,167,225,229,236,375,410]. The W(H) is usually 2-6 Å but on one occasion was found to be 14 Å. There is suspicion of a rotational modulation in light with a period of either 2.73 or 1.55 days [229].

   NTTS 045251

According to [506], this is a single-line spectroscopic binary.

   V347 Aur   

The star illuminates a variable nebula. The light curve resembles that of a long period variable. A 1978 Lick coude spectrogram shows strong, rather narrow H, fairly strong [O I] anf Fe II, and probably He I emission.

   V836 Tau   

The cyclic variation found by [409] has a period of 6.99 days. The star was identified incorrectly on the original chart [132].

   UX Ori  

The star is not convincingly associated with nebulosity, so it may not belong to the Ae/Be class. There have been extensive UBV observations: [226,229,273,276,478,527,530].

    RW Aur B   

The coordinates are based on the offset from A; the only actual double star measurement is that of [258]: 1".22 in 254.3° , made in 1944. When A is near minimum light, the companion contributes significantly to the light and spectrum.

    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 photometric observations are collected in [410]. The optical spectrum has been reproduced or discussed in [1,16,60,93,174,187,303,340,413,423,458]. IUE observations are in [15,65,239,240,241]. There is evidence for a 5-day cycle in both the light (Herbig 1962) and in the line structure [174]. Repeated radial velocity observations by [189] suggest that the velocity may be variable, with a range of about 10 km/s.

   V1012 Ori  

This object was observed as an IRAS galaxy by [357], but found to be a Be star. The variability was discovered by Morgenroth (Astr.Nach.253, 441, 1934 [with chart]; 254, 366, 1935). The scan of the red region by [357] shows H emission central on broad absorption wings, and strong Na I D lines.

    V534 Ori   

The coordinates are for St 37, identified with V534 Ori by [444], but [118a] identify the variable with St 38.

    CO Ori  

Elvey and Babcock (Ap.J. 97, 412, 1943) classified the spectrum as early F, with peculiarities; it has since been typed gF3 (Joy and Wilson, Ap.J. 109, 231, 1949), F8:n [212] and G5 [93]. When the star was near minimum light about 1950, Herbig saw it as double (about 1" in 280° ), but [22] could detect no such companion in 1980, with CO near maximum. Additional UBVRI observations are in [91,225,229,236,328].

    GW Ori  

The spectrum has been classified as G5 (Zappala, Ap.J.172, 57, 1972); G5: [93]; G5,8 V [212]; and dK3 [257]. Additional RI observations are in [236,328].

    V649 Ori   

There is a faint companion at 1".41 in 350° ; m is about 2 mag. The UBV photometry of [338] includes both stars. There was marginal evidence [22] for another star at 0".47, p.a. 36° or 216° . Other spectral classifications have been dK3 [257] and K4 [93].

   P102

The H emission was first noted by MacConnell, Astr.Ap.Suppl. 48, 355, 1982.

    V370 Ori   

The strength of H emission must be variable, because the W(H) reported by [93] would not have been detectable on objective prism plates. See the note in HRC regarding the clustering of emission-line stars around GX Ori.

   V447 Ori/c 

This star is about 5" in 30° from V447 Ori [119]. The coordinates are those of the primary.

   Rst 137B   

This star is at 9".3 in about 344° from A [487]. The coordinates are those of the primary.

   AB Dor  

Additional UBVRI observations are by Lloyd Evans, Circ.So.African Astr.Obs. no. 11, 73, 1987, and by Collier Cameron, ibid. p. 57. The reasons for suspecting that this may be a pre-main sequence star are in [486]. The mean radial velocity in the Table is that of [103]; the velocity may be variable with a range of about 22 km/sec: [244].

    HK Ori  

This star is at the apex of the reflection nebula PP 29. There have been numerous infrared observations: [3,32,81,91,100,157,273,316,452].

    V453 Ori   

The star is double: 3" in 190° , the companion being about 2 mag. the fainter [119].

   RY Ori  

The spectrum may be composite: He I 5875 Å suggest a B star, yet the remainder of the spectrum in the red is about F8. H is a strong double emission line, and Li I 6707 Å is present in moderate strength. The star can be identified from the chart by Wolf, Astr.Nach.171, 77, 1906, where it is 117.1904.

   P1207/c

The companion is at 25" in 75° from A [93]; it has weak H emission. [93] found no H emission, despite the objective-prism detection. The UBV colors in [11] must be in error. The coordinates are those of the primary.

   VY Ori  

There is a fainter star about 15" from VY in p.a. 135° . According to [497], its colors are: V=16.35, B-V=+1.39, U-B=+0.71.

   WX Ori/c   

The companion is at 11" in 10° from WX [93]. The coordinates are those of the primary.

   P1540   

According to [324], the star is a double-line binary with P = 33 days; both stars show strong Li I 6707 Å 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 the Table is from a Lick coude plate. According to [483], the star is not a member of the Orion cluster.

   P1724   

A non-member of the Orion cluster according to [483], although the spectroscopic criteria indicate that it is a pre-main sequence star.

   MR Ori  

The star is projected upon very bright nebulosity, so it is has not been possible to determine whether there is emission in the core of H or not; certainly no stellar emission lines are present elsewhere in the spectrum. The star is included in this Catalog solely on the basis of its (alleged) variability and location in the Orion Trapezium cluster.

   AE Ori  

The nebulosity is very bright, and from the single Lick spectrogram it was impossible to determine whether stellar H emission is present or not.

   P1925   

A Lick CCD spectrogram shows a fairly strong Li I 6707 Å line, but there is no evidence for emission at H, although the background nebulosity is so bright that a weak stellar emission core could have been concealed.

   TU Ori  

There is a large dispersion in the assigned spectral types: see [221].

   CQ Tau  

The UBV data are for maximum light [166]. The H region was described by Bonsack and Greenstein (Ap.J. 131, 93, 1960). A Lick coude plate of 1973 showed double H emission upon broad absorption wings. The absorption spectrum otherwise is like an early F star.

   AH Ori  

The spectrum was classified K0 IV,V by [248]. A Lick coude plate shows H in absorption, with no certain emission component; this appears to be a genuine example of a pre-main sequence star without obvious line emission, at least in the red.

   NV Ori  

[270] regard this star as constant, but [227] report a V range of 0.6 mag. there is complex emission in H, supertimposed upon absorption wings. Li I 6707 Å is present but not unusually strong.

   NY Ori  

The star is normally faint, but when near maximum has the emission spectrum described in [197]. It is about 5" se of P2118.

   TV Ori  

The photometry of [338] and of [497] are not in good agreement.

   AN Ori  

A Lick CCD scan shows H filled in to the level of the continuum.

   V1018 Ori  

The companion is at 22" in 127° from CE Ori [93].

   T Ori   

According to Shevchenko (Flare Stars and Related Objects [ed. L. Mirzoyan], p. 230, 1986), T Ori is a single-line spectroscopic binary with P = 14.268 days. A cyclic light variation having the same period is present.

   AR Ori  

There is a companion about 2" distant.

   P2292   

According to [483], the star is not a member of the Orion cluster. [499] finds variable radial velocity.

   AV Ori/c   

The separation is 6" in 305° [93]. The coordinates are those of the primary.

   V380 Ori   

This is nearly unique among the T Tauri stars in having an A-type spectrum. It is ADS 4209, but that companion (mag. 13.0, about 3" in 220° ) and another suspected by Jonckheere (Mem.R.A.S. 61, 57, 1917) were probably only structure in the nebula NGC 1999. No such stars are detectable on modern photographs, nor can any be seen visually at the 120-inch telescope. Additional UBVRI observations are in [116,229,328,378], and additional spectroscopy in [413]. A polarization map of the nebulsoity by Warren-Smith et al. is in M.N.R.A.S. 192, 339, 1980.

   P2441/c

The separation is 4".5 in 145° [93]. The coordinates are those of the primary.

   P2441   

Spectral types assigned have been: G1 IV [411], G3 [329], G5 [93], and "about G8n" from Lick spectrograms in the red. All conflict with the blue-region type of F5: in HRC. There is very strong, slightly asymmetric emission in H. There is a nebulous patch (HH 63) about 30" southwest (Reipurth and Graham, priv. comm.).

   V586 Ori   

Lick spectrograms showed strong complex emission, variable with time, in H. It is superposed upon the absorption wings of an early-type star. A few He I and Fe II lines suggest a type of late B or early A.

   BF Ori  

Additional UBVRI observations are in [229,273,391,430].

   V883 Ori   

This is the faint red variable slightly west of the apex of the reflection nebula IC 430 = Haro 13a (see [453], Fig. 5). The entry is retained although there is no evidence that the star has ever exhibited H emission: [7,181,312,363].

   Haro 2-249/c

The coordinates are approximate. These two stars and the ring-shaped nebula associated with the primary are shown on a CCD image in [161] and on [453] Fig. 5.

   +26° 887   

This is the "nebulous star 3' from RR Tau" in [203]. No emission was present in the photographic region on early Lick spectrograms, but P Cyg structure is present at H on a 1982 coude plate.

   V350 Ori   

A 1973 Lick spectrogram showed complex H emission, with narrow central reversal, superposed upon the absorption wings of an early-type star. He I 5875 Å is rather strong, so a B type is indicated.

   Reipurth 50

The coordinates are of the approximate center of a nebulosity that is believed [386] to be illuminated by a heavily obscured star about 1'.5 north. The nebula is variable in brightness.

   San 6   

A 1978 Lick coude spectrogram showed a strong, symmetric H emission line and a well-defined K-type absorption spectrum. The observation of San 6 in [93] must refer to another star.

   V631 Ori   

[93] found no H emission in 1976, yet rather strong emission in the photographic region was observed at Lick in 1960, and the star was originally detected on the basis of a bright H line [322].

   FU Ori  

The coordinates are from Duerbeck, Sp.Sci.Rev. 45, 1, 1987. The earlier history of FU Ori is summarized in [207,213]. It remains not far below maximum light. The UBVRI data in the Table are rough means from extensive observations in 1984-85, during which time a cyclic variation of length 9 or 18 days was present [286]. The spectrum is very complex, and the type assigned appears to depend on wavelength; the value in the Table is for the red region. References to infrared and recent high-resolution spectroscopy, and other properties of the spectrum, are [188,190,191]. Although not expressed in terms of v sini, [190] gives line widths measured in a variety of spectral regions.

   SSV 61  

This star, in a complex reflection nebulosity, is object 140 in [448], Fig. 1a; it is also in [211], Fig. 8. It was classified as an M2,4 giant by [448]; a Lick CCD spectrum indicates a slightly earlier type.

   +1° 1156   

This peculiar star illuminates the nebulosity Par 3 = PP 46. The presence of Li I 6707 Å is confirmed on a Lick CCD spectrum, on which H is filled to continuum level with emission.

   LkH 336   

(See the following remark for LkH 336/c.)

   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 apparent on the identification chart in HRC. According to [93], there is another star at 6" in 140° , 5 mag. fainter than A.

   LkH 208   

An optical polarization map of the nebulosity is in Shirt et al., M.N.R.A.S. 204, 1257, 1983.

   MWC 137

As noted in HRC, this is a high-luminosity object that may not be pre-main sequence. The star is surrounded by a 56" x 80" ring of nebulosity; it is 195 -0° Sh 2-266 in Perek and Kohoutek Catalogue of Galactic Planetary nebulae, which gives an identification chart.

   LkH 340   

The labels on the charts for LkH 340 and 341 in Figs. 4 and 5 of HRC were interchanged. Drs. U. Bastian and M. Cohen have confirmed that their respective observations [25,93] were of the stars at the coordinates given in HRC, not of the stars on the incorrectly labelled charts.

   LkH 341   

(See the preceding remark for LkH 340.)

   V486 Mon   

There is a faint companion at about 6" in 73° .

   LkH 215   

The coordinates are only approximate on account of interference by the bright nebulosity.

   HD 259431  

Although this star is often considered a member of the Ae/Be class [203], the possibility still exists that it is a conventional Be star. The modern spectral classifications range from B2e [138] to B5 [452] and B6pe [224].

   R Mon   

The coordinates are those of feature "a" at the apex of the small (about 3") triangular nebulosity known as "R Mon" [251]. Its brightness dpends heavily upon aperture size and angular resolution. The spectrum is peculiar and variable: see [208,251] and references therein. Infrared speckle observations are in [29], and infrared spectrophotometry in [87]. The structure of the nebulosity in [S II] is described by Brugel et al. (Ap.J. Lett. 287, L73, 1984), and photometry and polarimetry of NGC 2261 are in [21] and in Warren-Smith et al. 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] and Walsh and Malin, M.N.R.A.S. 217, 31, 1985.

   G-G 405

There is a faint companion at about 4" in 150°.

   VSB 2   

The type F7 V [526] in the Table is in conflict with the K0 of [488].

   W68 

The various spectral classifications are not in good agreement, probably because of the very broad lines: F2 [488], F4 V [526], G0 IV,V [494].

   V590 Mon   

The spectrum is peculiar, and at low resolution there has been considerable disagreement in the classification: B4 V [526], B9-A0 [93], B8 + shell [203], A2-3 [199].

   W108

Spectral classifications range from F7 V [526], F8 [458] to F9 [93] and G0 [488,494].

   W121

The star is located very near S Mon, which may account for the large discrepancies is the published UBV photometry, amounting to 2 mag. in V: [414,433,494]. A Lick CCD spectrogram showed moderately strong H emission with central reversal, and strong Li I 6707 Å absorption.

   IP Mon  

The star is very closely nebulous. The type K3 was assigned by [93,401], while [488] give K2 and [526] gives G8 V:. The H emission is rapidly variable:Marcy, Astr.J. 85, 230, 1980.

   W154

The type G2 III,IVp is from [494], while [526] gives G2 V and [488] G7.

   V360 Mon   

The type F8 is from [93], but [401] gives K2 or earlier, and [526] G8 V.

   V365 Mon   

This star is 7" from V591 Mon.

   OX Mon  

The emission originates in the northeast component of a close pair (7" in 35° : [93]). The photometry refers to the combined light. No emission is seen in the other component [93].

   NGC 2313   

The involved star has a complex emission structure at H, and in the red an absorption spectrum perhaps of type G with very strong Ba II lines.

   LkH 218   

This may be an ordinary Be star.

   Z CMa   

The spectrum is very complex and possibly composite. References to earlier spectroscopic work are in HRC; more recent papers: [104,123,452]. The optical and VLA coordinates are not in close agreement [96]. An optical companion was reported in [139] but has not been confirmed. Infrared speckle observations show the star to be slightly extended in the east-west direction [311]. UBV/RI photometry is in [50,91,225,229,275]. Many infrared observations have been reported: [3,31,32,81,87,155,224,273,316,372,452]. The VLA observations are in [34,96,101].

   LkH 220   

This may be an ordinary Be star.

   NX Pup  

The spectral type in the Table is a compromise: the star has variously been classified as A0-1 III [478], A1 [138], F0 Ipe [245], F1-2 [381], and F2 III [49]. H is in emission but the decrement is very steep.

   ESO313-N*10

At least 9 condensations, most of them red with H in emission, are imbedded in a bluish nebulosity about 35" in diameter having an early-type absorption spectrum.

   SY Cha  

The type M0: is from [17]; an earlier classification was K2 V [12]. The star has shown a cyclic variation in brightness with range 1.6 mag. in B and a period of 6.129 days [259,325,422].

   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 also concurrent changes in the emission spectrum [259].

   TW Hya  

The spectrum is in all respects like that of a T Tau star, but there is no nearby cloud. Three Lick spectrograms gave velocities of -9, +12 and +9 km/s, a range large enough to raise the suspicion that the star may be a binary.

   CS Cha  

The spectral type in the Table is a compromise of K2 [196], K5 [403] and M0 [17]. The value W(H) = 13 Å from [17] differs from the 59 Å in [403].

   CT Cha  

The type K7: is from [17]; [196] give G8:.

   VW Cha  

Variability of H was suspected from the first observations [196], and confirmed by later results [17, 403]. A mean value is given in the Table. The K2 type is from [17], but the star was classified earlier as G1 V: [12].

   CU Cha  

The spectral type is from the Michigan Spectral Catalogue 1, 1975; it was given as B9.5e V in [196,403].

   VZ Cha  

A cyclic variation with a V range of about 0.7 mag. and period 7.2 days has been observed [259].

   WY Cha  

The star was classified K0: (Li) by [196].

   WZ Cha  

[196] give the type as G:.

   Sz 41   

The coordinates and photometric data are for Sz 41, while the infrared references and spectral type refer to HJM E1-9a. The coordinates of the two objects agree within about 10", and it is assumed that they are the same. [238] state only that line emission is present, giving no details.

   T Cha   

T Cha has sometimes been regarded as a pre-main sequence star on the grounds of its rapid, irregular variability and location on the edge of a small dark cloud [232,233], but spectroscopic proof is lacking. There is no obvious emission at H or elsewhere; unfortunately the Li I 6707 Å region has not been observed adequately. A cyclic variation with a period of 3.2 days has been suggested [325].

   Bipolar nebula

The spectral type refers to the northern lobe [351]. The southern extension has an HH-like spectrum; there is probably an A0 star involved. Polarimetry of the nebulosity is in [461]. The UBV data were taken through a 23" aperture [508]. It is uncertain whether this is a pre-main sequence object.

   S2  

S2 is considered [421] to be the central object of a nebulous cluster, but earlier [58] was regarded as the central star of a bipolar nebula. The coordinates are approximate.

   RU Lup  

Additional UBV/RI observations are in [25,145,266,427].

   RY Lup  

A quasiperiodic variation of length 3.76 to 4 days was discovered by Hoffmeister [232], and confirmed by more recent work [46,129,314]. W(H) ranges from invisibility [17] to about 25 Å [314], apparently in antiphase with the light cycle.

   EX Lup  

The photometry refers to minimum light, but the values in the Table are the brightest of 7 observations [25]. References to earlier work on the star, especially near maximum, are in HRC and [213].

   Sz 102  

The spectrum contains strong emission lines of [O I], [N II], [S II],..., characteristic of HH Objects, superposed upon a late-type continuum and stellar absorption spectrum [17,295,299,426]. Two isolated patches of emission nebulosity lie about 13" e and w of the star [295].

   V856 Sco   

Observations in the Stromgren and Walraven photmetries are in [467,468,469]. The star is reputed to have a close companion (Rst 3930B, at 1".3, mag. 12), but it was not detected in speckle observations [22].

   Sz 124  

The fact that the star was detected by objective prism observers [426,463] seems incompatible with the low value of W(H) = 1.6 Å in [17].

   V866 Sco B 

The companion is about 1".4 in 20° from the (slightly) brighter primary. Both stars have the infrared Ca II lines strongly in emission. The coordinates and photometry refer to the combined light.

   V866 Sco A 

The type K0 assigned in [93] was not in acceptable agreement with the M0: of [212]. Reexamination of the Lick material shows that it clearly lies betwee K3 V and M0 V, hence the K5 V in the Table. Narrow He I emission lines are present. The coordinates and photometry refer to the combined light.

   Wa Oph/3   

H emission was discovered by The [465], which is surprising considering the low value of W(H) = 0.3 Å in [502].

   DoAr 21

H emission was reported by objective-prism observers between 1949 and 1960, but has not been seen on slit spectrograms since 1973. The object at that position is very variable as observed with the VLA, and moderately so in X-rays [133]. No optical variability was detected on Lick Astrograph plates [369].

   DoAr 24

The X-ray coordinates [332] are in better agreement with DoAr 24 than with DoAr 24E.

   DoAr 22

The coordinates are those of the m(pg)=13.0 star, type F5:e, listed in HRC. The emission-H object 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; its spectrum has not been observed.

   DoAr 24E   

According to [539], the star is double, separation 1".95 in p.a. 0°. The only positive detection of H emission is by [524]. The X-ray emission probably originates in DoAr 24.

   SR 24 s

The coordinates are of the photocenter of the pair (6" in 60°); individual positions are in [524]. The ROX observation included both stars. A variation 16.4-17.1 (pg) is observed in the combined light [369]. Attention 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).

   ROX 20-1 nw

The separation of the pair is about 13" in 302° . X-ray flaring has been detected in the unresolved image [332]. H emission in both stars was originally noted on a Lick slitless spectrogram.

   ROX 20-2 se

(See remark to ROX 20-1 nw).

   S-R 12  

Speckle observations show the star to be a close double (0".30 in about 85°), with K magnitudes 9.34 (eastern) and 9.17 (western). It was also resolved in an occultation observation [435].

   ROX 31  

The coordinates are from a VLA observation. The spectroscopic observation is by Bouvier and Appenzeller, quoted in [10]. The star was not detected in the H surveys of the region. An occultation observation [435] showed the star to be double with separation 0".13 projected upon p.a. 337°. The K magnitudes are 8.72 (eastern) and 9.00 (western component).

   SR 10   

There is a large difference between the W(H) values of [17] and those of [93,402]; the mean of the latter is given in the Table.

   Haro 1-14/c

Haro 1-14 is actually the fainter, southeastern component of the pair of stars (separation about 10") at this position. The UBV photometry refers to the combined light. The brighter star, here called Haro 1-14/c, has emission cores in H,K [404].

   Haro 1-14  

(See remark for Haro 1-14/c).

   Reipurth 13

This is a faint, extended nebulosity (6" x 8"), apparently scattering the light of an imbedded star having H in emission [9].

   V346 Nor   

This very red star is at the edge of HH 57 [426]. Originally discovered as an infrared source [384], it became detectable in the visual region about 1983: [102,169,382] and references therein.

   AK Sco  

The type is from the Michigan Spectral Catalogue and Lick coude material. The spectrum in the red appears composite. Two Lick CCD scans show double lines with a splitting of about 200 km/s; at other times the lines have been single. Clearly, the star is a double-line binary. Li I 6707 Å is strong in both components.

   V921 Sco   

The emission spectrum of this nebulous star was noted independently by Vandervoort and The (priv.comm.), by Henize (Astr.J. 67, 612, 1962), and by N. Irvine.

   AS 216  

There is a faint companion at about 5" in 200°, about 4 magnitude fainter than AS 216.

   IX Oph  

Lick coude spectrograms show sharp H emission on a weak metallic-line spectrum; Li I 6707 Å is not present. The star's image is marked on Pl. I of [464], but no number was assigned.

   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 magnitude difference about 1 mag. Narrow [N II] and [S II] lines are present in the brighter component; [Fe II] emission has been reported in the blue [6].

   LkH 346 nw

[93] give 6".5 in 130° as the position of the se component with respect to the nw. The coordinates are those of the photocenter.

 275  LkH 346 se

(See remark for LkH 346 nw).

   RNO 92  

The star is double: 4".4 in 65° ; direct images are shown in [388].

   SV Sgr  

The star is superimposed on the very bright H II region NGC 6523. Lick coude spectrograms show P Cyg structure at H and very strong emission at the infrared Ca II triplet.

   LkH 118   

The classification as B5 Vp [139] conflicts with the description of the spectrum in [201].

   V4046 Sgr  

[113] find the star to be a single-line binary with P = 2.43 days; [62] suspect double lines. W(H) varies between 30 and 120 Å. Flaring was observed by [61]. The star can be identified from the HDE chart (Harv. Ann. 112, 1949).

   -10deg 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 photometry refer to the combined image. It is not known which component is the flaring variable. According to [77], there is also a sinusoidal variation with P = 5.20 days, amplitude 0.1 mag., in the integrated light.

   -10deg 4662 A

(See remark to -10 4662 B).

   CoKu Ser/G1/c

This companion is at 3".5 in 140° from G1; the coordinates are of the photocenter.

   CoKu Ser/G1

(See remark for CoKu Ser/G1/c).

   VV Ser  

The coordinates are from Reinmuth, Astr.Nach. 225, 386, 1925.

   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 polarization map of the nebula (called the "Serpens object" in [453]). Their Fig.1 identifies the infrared sources in the area; their Pl. 1, and Fig. 7 of [453], are photographs of the region.

   AS 310  

See the remarks in HRC. The photometry contains the contribution of a faint companion at 3-4" [25,139]. A Lick coude spectrogram shows shallow absorption under the sharp central H emission, and narrow He I absorption lines. Strong interstellar features are present. Clearly, this is a hot, high luminosity object.

   Kn H 10   

[323] find no line emission. The spectral type is K, but it may be a giant.

   Kn anon 2  

A late-type absorption spectrum was found by [323], but no line emission.

   S CrA   

The emission spectrum is very strong, and the underlying absorption spectrum can be seen only with difficulty. The star is a close double, usually not resolved photometrically or spectroscopically. Discovered by [258], it was remeasured by [22]: separation 1".37, p.a. 147°, m about 1 mag. in 1981. Additional UBV photometry is in [25,263,266,323,336]. The spectrum is reproduced or discussed in [17,18,122,212,323,336,337,400,401].

   TY CrA  

See the remarks in HRC. there may be a weak emission component in H [139]. According to [264], the star is an eclipsing variable with P = 2.888797 days. The other bright star in NGC 6726/7, CoD-37deg 13023, has a close companion discovered by Hubble. At the 120-inch coude, this star was estimated of mag. 13-14, at 3" in 160°.

   MaRy/H 2  

H emission was first noted by [274], and the star was marked but not numbered in their Fig. 1.

   R CrA   

Published V's show large scatter, due either to real variability or the effect of the nebular background. Rapid changes in the nebula and in the H profiles in nebula and star have been described by Graham and Phillips (Pub.A.S.P. 99, 91, 1987).

   DG CrA  

See the remark in HRC. Since that time, H emission has apparently been detected by [274] and [323]. The coordinates are approximate, from Van Gent (B.A.N. 7, 21, 1933).

   T CrA   

There is a difference of about 2 mag. between the V's of [329] and those of [273] and [323], possibly due to variability.

   FG Aql  

The type in the Table (K2) is from [93], but a Lick coude spectrogram in 1977 was classified as K7,M0 V with strong Li I 6707 Å, and double H emission (R>V).

   WL 22   

This object was found by Wooden and Lada (unpublished). A 1981 Lick spectrogram showed narrow H emission line flanked by an extremely broad, strong P Cyg-type absorption structure.

   V1352 Aql  

This is the "exciting star" of HH 32. The V, B-V values are means from [288]. The emission spectrum has been investigated by [40,218,293,294,337,342,423]. Perhaps on account of P Cyg structure, the various W(H)'s do not agree well [93,293,423]. No absorption line spectrum is detectable.

   WW Vul  

Additional UBV/R photometry is in [226,475,529,530].

   LH 483-41 

A 1972 Lick coude plate showed double H emission (V<R) superposed upon broad absorption wings.

   Par 21  

This object did not appear stellar to visual examination at the 120-inch coude, but rather as a nebulous blob 3-4" in diameter. Two 1974 spectrograms showed H in absorption.

   V1685 Cyg  

A comprehensive discussion of the UBV data is in [392]. The spectrum is described in [138,139,203,452].

   V1515 Cyg  

The earlier history of this FU Ori-type variable is in [213]. Subsequent spectroscopic observations are in [27,108,188,190,285]. The UBV data are means for the 1981 season [285]. The coordinates are those given for "P22" in [83]. A direct image of the nebulosity, and its spectrum, are discussed in [161].

   +41deg 3731  

This may be an ordinary Be star.

   Par 22  

The star is central in a bipolar nebula. It is identified as "P22a" in [83].

   PV Cep  

The star is associated with a variable nebulosity [92,95,313,351].

   AS 442/c   

The coordinates are of AS-442 itself, a Be star. The companion is 5" in 45° from the primary [93].

   LkH 138   

LkH 138 is the southwest and brighter component of a pair, separation 5" in 48°.

   LkH 138/c 

(See the remark for LkH 138).

   V1531,1532 Cyg

= LkH 142, 143: an unresolved pair separated by about 2".5 in 91°. The coordinates are of the photocenter.

   LkH 151/c 

According to [93], this star is 9" in 20° from LkH 151.

   LkH 168   

This may be a background Be star.

   V751 Cyg   

It is still not clear whether this is a pre-main sequence star or not: see the remarks in HRC.

   LkH 172   

Welin [509] has noted that LkH 172 is at the place of the "missing" BD star +43deg 3749.

   V1057 Cyg  

The best-studied FU Ori-type star; history and references through 1976 are in [213]. UBVR light curves and references are in [287]; more recent photometry is in [3,87]. Spectroscopic references are: [27,108,188,190,278,335,337,458,480], and infrared: [3,87]. The fading of the reflection nebula is described in [120].

   V1331 Cyg  

The emission spectrum is very rich, and no underlying absorption spectrum is apparent. The spectrum is displayed or discussed in [70,72,302,303,337,367].

   HD 200775  

There is some dispersion in the published spectral classifications: B2.5 [138], B3 V [24], B5 [378].

   LkH 324   

LkH 324 is marked on the HRC identification photograph as the bright star at the nw tip of an elongated nebulosity. In fact, the H emission was originally detected in the fainter star at the se end: the HRC chart was marked incorrectly. As proposed by [73], the "LkH 324" identification will remain attached to the nw star, as in HRC. H emission has actually been observed in this star on two occasions. Photometry in 1983-85 gave: 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 refer to a time of temporary brightening at some time between 1975 and 1980. This object deserves closer attention.

   LkH 324-SE

See the remark for LkH 324; the star at the se edge of the nebula is now designated LkH 324-SE.

   LkH 349/c 

This companion is approximately 16" in 305° from the brighter star.

   LkH 349   

The coordinates in HRC are incorrect. The star is probably no. 60 in Marschall and Van Altena (Astr.J. 94, 71, 1987). It can be identified in Osterbrock, Ap.J. 125, 622, 1957, at 56.5 mm below and 37 mm inside the upper left corner of Fig.2. Strong, double P Cyg-type absorption components are present on a Lick coude plate.

   Star in RNO 138

= star 6 of [456].

   V1735 Cyg  

The star illuminates a red reflection nebula. P Cyg structure at H is clearly detectable on a Lick coude spectrogram.

   BH Cep  

A Lick coude spectrogram shows wide, P Cyg-type structure at H; some later-type absorption lines are present, suggesting a type of about F. A light curve is given by Hoffmeister, Astr.Nach. 274, 232, 1944.

   BO Cep  

A Lick coude spectrogram shows widely double, sharp emission upon broad H absorption wings. No other lines except narrow, presumably interstellar, Na I D lines are present in the red. See the Hoffmeister reference in the remark for BH Cep for a light curve.

   SV Cep  

Lick coude plates show double H emission superposed upon broad absorption wings; He I 5875 Å is present, and interstellar Na I. The type may be slightly earlier than A0. Other classifications are in [205,268,474,530].

   LkH 233   

Photometry and polarization maps of the nebulosity are in [20]. The object is also known as Markarian 914 [460].

   LkH 350   

This may be an ordinary Be star.

   DI Cep  

W(H) is highly and rapidly variable: [26,91,93,147,173]. Much detailed information on the photometric and spectroscopic variations is in [147,173]. Spectroscopic observations are in [26,187,257,294,303,413].

   AS 501  

[115] found a V range of 12.3-13.1, but [443] saw no variation beyond normal photographic scatter. H emission is strong and double; there are no other emission lines in the red. Despite the M giant absorption spectrum, the star does not appear to be a symbiotic. It is unlike any recognized pre-main sequence star.

   MWC 1080/c 

[93] gives the separation from MWC 1080 as 10" in 75° , magnitude difference = 4 mag., but the separation seems to be more nearly 25".

   MWC 1080   

This is a hot, high-luminosity object, showing strong He I absorptions, hazy Fe II emission, complex P Cyg-like emission at H; the interstellar lines are strong. Although involved in bright nebulosity, it is not obvious that this is a pre-main sequence star, although the companion appears to be so. W(H) values: [91,93,139].

   BM And  

The spectral type given is for the red region; there is some suspicion that it may depend upon wavelength [212,498].

   MacC H18 n 

There are two stars at this position; the coordinates given are for the brighter, northeastern of the pair. The fainter star is at about 10" in 196° . It is not obvious whether data of [93] or [90] refer to the brighter star or to the pair together.