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V/73A Emission-Line Stars of the Orion Population (Herbig+ 1988)
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Third Catalog of Emission-Line Stars of the Orion Population
Herbig G.H., Bell K.R.
<Lick Observatory Bull. No. 1111 (1988)>
=1988LicOB1111....1H
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ADC_Keywords: Combined data ; Stars, pre-main sequence
Description:
This Catalog lists 735 pre-main sequence stars, members of the Orion
Population, that have been observed with slit spectrographs or at
equivalent resolution. It is intended to replace the Second Catalog of
Herbig and Rao (1972). It gives accurate coordinates (many determined
especially for this Catalog), light ranges for known variables, UBVRI
data near maximum light, references to ultraviolet, X-ray and radio
observations and to light curves, value of v sin i and the radial
velocity when known, spectral type, equivalent width of the H-alpha
emission line, references to spectral reproductions or scans and
spectroscopic studies and to identification charts, and a
classification (as a T Tau star, FU Ori object, etc.)
Introduction:
This is the third up-date of a listing of the pre-main sequence stars,
both certain and probable, that have emission lines and that have been
observed with slit spectrographs or at comparable resolution. The
first (Herbig 1962) contained 126 entries, the second (Herbig and Rao
1972: hereafter HRC) had 323, while the present Catalog contains 735.
Not only has the total number of stars increased due to a higher level
of observational activity and the improvement of spectroscopic
instrumentation, but there is a greater variety of significant
information to be referenced: for example, there was no occasion in
earlier listings to mention v sin i's, radial velocities,
far-ultraviolet, X-ray or radio-frequency data. The classification
scheme for pre-main sequence stars (described below) has also been
modified as the result of improved observational information.
In order to accommodate such new information as well as more
accurate astrometric coordinates within a double page, 264-column
format, it has been necessary to omit some information that is
relevant and would have been useful in some cases:
(a) IRAS identifications are not included.
(b) Light curve classifications are not included,
partly because such traditional observations have
not kept pace with the volume of other
information. Instead, references are given to
sources where such information as exists may be
found, except in cases where rotational
modulation has been detected; such results are
given in the Remarks to Table 1.
(c) No references are given to polarization
information; however, that subject has recently
been surveyed very thoroughly by Bastien (1988).
(d) The "emission line intensity" classification of
the Second Catalog, a rather subjective quantity
but all that was available in 1972, has been
replaced by the equivalent width of H-alpha emission,
which is now readily determinable as the result
of the widespread use of linear, red-sensitive
detectors.
(e) No references are given to proper motion
information.
The numbers assigned by Herbig and Rao (1972), prefixed HRC in the
past, have been retained for those of the 323 stars of the Second
Catalog that have survived subsequent examination. Thus the new
entries begin with 324 and extend through 742. The ordering is
strictly in order of right ascension for 1950.0. As the result of
improved coordinates, the original HRC ordering is sometimes
altered. It is suggested that Catalog entries be referred to by
their primary designation, which usually is in the 'name' column.
In circumstances where the Catalog number must be used, it is
recommended that HRC now be replaced by HBC. Note also that the
letter n or an asterisk (*) which often follow the HBC number are
not part of that designation, but are separate items of information.
It was suggested in the Second Catalog that many of the variables in
young clusters and associations that were not then known to have
line emission would turn out to have bright H-alpha or Ca II, H,K
lines upon closer examination. This has turned out to be so: many
such stars are now included as "weak-line T Tauris" (abbreviation:
wt). A large number of such stars have also been recognized as the
result of X-ray surveys of obscured regions, particularly the
Taurus-Auriga clouds. Walter and co-workers, who have done much of
this work, have called these objects "naked T Tauri stars", or NTTS.
It is our opinion that these do not constitute a separate class of
pre-main sequence stars, but are a quite natural extension of the T
Tauri class toward weaker line emission since the cutoff of
conventional T Tauri stars at W(H-alpha) ~ 5 A was set only by the
limitations of the early objective-prism or -grating surveys. The
existence of substantial numbers of such stars was in fact to be
expected (Herbig 1985) from the shape of the frequency distribution
of W(H-alpha). We prefer the non-committal classification "wt" for
these stars as a group rather than NTTS, partly because the latter
implies a physical picture of the phenomenon that is still
speculative.
However, one kind of weak-emission star that has been omitted from
the Third Catalog are the rapid-rotating G- and K-type dwarfs in
young clusters, such as alpha Per and the Pleiades, most of which have
emission at H-alpha. They have not been included because they lie
on or near the main sequence. There are probably such stars in the
field as well, and consequently we have omitted objects such as
W92/NGC 2264 (= V642 Mon), Gliese 182 (= V1005 Ori), and any others
that appear to be BY Dra-like variables. On the other hand, we have
included many weak-emission G and K stars in the Orion Nebula region
and in NGC 2264, on the grounds that they lie well above the main
sequence and are therefore clearly pre-main sequence objects.
The lower boundary of the Orion population, insofar as it is
represented in this Catalog, thus is not well defined. Nor is it
always apparent whether a late-type star having no more than weak
H-alpha and Ca II emission is pre-main sequence or not. This is a
relatively recent problem. The sample of emission objects that were
turned up in the early H-alpha surveys were mostly classical T Tauri
stars, where emission-line criteria clearly provide the
identification. Foreground dMe stars were not detected, because
such stars in the field and in older aggregates like the Hyades
rarely have W(H-alpha) greater than about 6 A. But in younger
clusters like the Pleiades, emission H-alpha has now been found in M
dwarfs at W(H-alpha) values as large as 18 A, although the most are
less than 12 A (Stauffer and Hartmann 1986). When such stars
attract scrutiny as the consequence of some special activity, such
as variability or X-ray emission, unless their luminosity is well
enough known to locate them above the main sequence, there is no
obvious way to distinguish a pre-main sequence star from its young
main sequence counterpart. It is possible that refinement of the
lithium abundance criterion might clarify this situation.
It must be stressed that the stars listed here have been discovered
by a variety of techniques, through searches that have been
concentrated in certain areas while other regions have been almost
neglected. Therefore, no one should consider the Catalog as
complete even to a fairly modest limiting magnitude over any large
fraction of the sky.
The Catalog references those sources and papers that were available
to us through March 1988. We shall be grateful for any errors that
are called to our attention.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 360 735 *Catalog Data
refs.dat 153 544 References
remarks.dat 130 588 Remarks
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Note on catalog.dat:
Catalog.dat contains both real data as well as references to published
papers, the latter have been listed in refs.dat. In the following
text, the numbers assigned to papers in the Reference list are in
[square brackets]. Within that list, for journals which exist both
in the original language and in English translation, the
English-language citation is given first, followed by the original
in brackets (thus: Sov.Astr.-A.J. 7, 219 [7, 398]).
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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2- 4 I3 --- HBC *HBC number.
5 A1 --- nebu_flg [ n] Nebulosity association flag.
6 A1 --- rem [ *] Remark flag. See file remarks.dat
8- 18 A11 --- name *Star name.
20- 56 A37 --- alt *Other designation.
59- 60 I2 h RAh *Hours of right ascension (1950.0).
62- 63 I2 min RAm *Minutes of right ascension.
65- 69 F5.2 s RAs *Seconds of right ascension.
71 A1 --- DE- *Sign of declination (1950.0).
72- 73 I2 deg DEd *Degrees of declination.
75- 76 I2 arcmin DEm *Minutes of declination.
78- 81 F4.1 arcsec DEs *Seconds of declination.
82 A1 --- u_RAs [: ] Position uncertainty flag (:)
83- 90 A8 --- r_RAh References to the position.
92- 96 F5.1 deg GLON *Galactic longitude.
98-102 F5.1 deg GLAT *Galactic latitude.
105-116 A12 --- phot_range *Photometric range.
118-119 A2 --- mag_sys *Code to the magnitude system.
121-127 A7 --- phot_ref *Photometric references.
128 A1 --- l_Vmag Inequality sign to the V magnitude.
129-133 F5.2 mag Vmag *? V magnitude.
134-135 A2 --- n_Vmag [:*mv ] Note to the V magnitude.
136-140 F5.2 mag B-V *? B-V color.
141 A1 --- n_B-V [:*v] Note on the B-V color.
143-147 F5.2 mag U-B *? U-B color.
148 A1 --- n_U-B [:v] Note to the U-B color.
150-164 A15 --- refs_UBV *References to the UBV data.
166-170 F5.2 mag V-R *? V-R color.
171 A1 --- n_V-R [:v*M] Note to the V-R color.
173-177 F5.2 mag V-I *? V-I color.
178 A1 --- n_V-I [:v] Note to the V-I color.
180 A1 --- RIsyst *[JCi?cE] Code to the (R,I) system.
182-189 A8 --- refs_VRI *References to the VRI data
191-213 A23 --- refs_IR *References to the infrared magnitudes.
215-229 A15 --- refs_UVX *X-ray references.
231-245 A15 --- refs_radio *Radio references.
247-261 A15 --- refs_lc *References to the light curves.
263 A1 --- l_vsini [ <>^] Inequality sign to the (v sin i).
264-266 I3 km/s vsini *? (v sin i) data.
267 A1 --- u_vsini [*:?] Uncertainty flag to the (v sin i) data.
269-273 F5.1 km/s RV *? Radial velocity.
274-275 A2 --- q_RV *Quality code to the radial velocity.
277-283 A7 --- r_RV *References to the radial velocity and
(v sin i).
286-296 A11 --- Sp *Spectral type.
298-305 A8 --- r_Sp *References to the spectral type.
307-311 F5.1 --- EW *? Equivalent width of H-alpha emission.
312-314 A3 --- n_EW *Note to the equivalent width of H-alpha
emission.
316-322 A7 --- refs_Halpha References to the H-alpha emission.
324-338 A15 --- refs_spec *References to the spectrum data.
340-341 A2 --- type *Type of the object.
343-349 A7 --- refs_chart *References to the identification chart.
351-360 A10 --- location *Location in the nebulosity.
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Note on HBC:
The running number is followed by n when the star itself
is involved in, or illuminates bright nebulosity.
An asterisk (*) indicates that a Remark follows the Table.
Note on name:
This is the preferred designation of the object; if a variable
star name has been assigned that is always given preference.
If the preferred name is too long, a > symbol indicates that
it follows in col. 3.
Note on alt:
Other designation: The conventional designations (AS, LkHalpha,
Haro ...) are explained in HRC. We have found it necessary in
some cases to expand the prefix system, usually abbreviating
discoverers' names by two-letter symbols rather than one to
avoid confusion with variable star designations (thus: CoKu
for Cohen and Kuhi). We have also retained the discoverer's
name for an object wherever possible, rather than substituting
what might seem a more rational designation (thus: P2441/c
for the companion of P2441, rather than P2441 B). The prefixes
used in cols. 2, 3 are as follows:
CD Cape Photographic Durchmusterung
CoD Cordoba Durchmusterung
CoKu Cohen and Kuhi [93]
Eggen [125]
Elias Tau-Aur [128]; Oph [127]; IC 5146 [126]
FK Feigelson and Kriss [132]
GlPe Glass and Penston [157]
GM Gyulbudaghian and Magakyan [177]
HaGr Hartigan and Graham [186]
He 3- Henize [195]
HH Herbig [211] and later publications by a variety of authors.
HJ Herbig and Jones [218]
HJM Hyland, Jones and Mitchell [238]
HM Henize and Mendoza [196]
JH Jones and Herbig [250]
Kn Knacke et al. [274]
LkCa Herbig, Vrba and Rydgren [219]
LZK Liu, Zhang and Kimura [315]
MacC MacConnell 1968: Cep-Cas; 1981: Pup
MaRy Marraco and Rydgren [323]
MC Cohen [90]
NTTS Walter et al. [506]
OgHa Ogura and Hasegawa [355]
P 4 digits: Parenago [359]
1 digit: Mundt et al. [344]
Par Parsamian [360]
PC Parsamian and Chavira [363]: PC numbers
have been assigned to all the confirmed
Tonantzintla discoveries in the Orion
Nebula region, but Table 1 gives only those
that have no Haro 6- designations.
PH Pettersson [370, 371]
PP Parsamian and Petrossian [362]
ROX Montmerle et al [332]
RNO Cohen [85]
S Sonneberg variable star
San Sanduleak [417]
SS 1 Sanduleak and Stephenson [419a]
SS 2 Stephenson and Sanduleak [444a]
SSS Strom, Strom and Stocke [450]
SSV Strom, Vrba and Strom [455]
St Stephenson [444]
Sz Schwartz [426]
TH The: see Table 3
vBH van den Bergh and Herbst [482]
VSB Vasilevskis, Sanders and Balz [485]
W Walker, NGC 2264 [494]; IC 5146 [495]
Wa Walter [502]
WK Walter and Kuhi [504]
Wray Wackerling 1970
Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs:
The coordinates indicated by B in col. 6 were determined by one of us
(KRB) with the Lick Automatic Measuring Machine on yellow (in most
cases) plates of the Lick astrometric program. Usually 15 to 20
reference stars from the AGK3, with proper motions applied, were used.
The epoch (minus 1900), rounded off to the nearest year, follows the
B. The coordinates indicated by Aw in col. 6 were originally measured
by C.A. Wirtanen, from blue plates of the Lick program, for the HRC.
The epoch of those coordinates is approximately 1950. We do not regard
either B or Aw coordinates to be of astrometric quality. Coordinates
drawn from other sources are referenced accordingly. Those brought
forward to 1950.0 have not had proper motions applied, so remain at
their original epoch.
Note on GLON, GLAT:
Galactic coordinates in the lII, bII system
Note on phot_range, mag_sys, phot_ref:
Photometric range if the star is a known variable, expressed in the
magnitude system indicated. Values taken from the 4th edition (1985,
1987) of the General Catalogue of Variable Stars, or recent
Supplements, are indicated by a C. (Note that the conventional
practice is followed in that < means "fainter than".) Stars believed
to be variable are indicated var. A number of stars not known to be
variable have their mean, or estimated magnitudes in these columns if
that magnitude is not visual or in the Johnson V system; otherwise
that value is in the "Vmag" column.
Note on Vmag, B-V, U-B:
V, B-V, U-B photometry: for stars observed more than once, unlike HRC
practice (where mean values were given regardless of phase) these
columns contain the values observed when the star was brightest in V
and a full set of UBVRI magnitudes were measured at essentially the
same time. In some cases, the colors show a substantial scatter at the
same value of V; such colors are marked with a v. For those stars
where there is only a small scatter about a mean V, or where a
small-range cyclic variation is superposed upon irregular activity,
mean rather than maximum-V values are tabulated; such stars have an m
following their V magnitude.
Note on refs_UBV:
Photometric references: the first number is the source from which the
tabulated values are taken. Additional sources of UBV data follow. For
stars having an extensive photometric history, a * means that details
are in a Remark to Table 1. An hrc means that some information given
in the Second Catalog is not repeated here.
Note on V-R, V-I:
V-R, V-I values, usually obtained simultaneously (i.e., at maximum V)
with the UBV data of cols. V, B-V, U-B; this is so if the first
reference in col. refs_VRI is the same as the first in col. refs_UBV.
Note on RIsyst:
A single letter (J, C) shows whether the R, I values are on the
Johnson or Cousins system. An i indicates an instrumental (r,i)
system; conversion relations for the photometry by Rydgren and
co-workers are given in [407].
Note on refs_VRI:
References to the V-R, V-I data, as described for col. refs_UBV.
Note on refs_IR:
References for infrared magnitudes, spectrophotometry and
spectroscopy. However, low angular resolution far-infrared
observations are not usually cited.
Note on refs_UVX:
UV, X-ray references: these usually refer to IUE spectroscopy and to
X-ray detections from the Einstein survey.
Note on refs_radio:
Radio references are to VLA observations or to detection of the star
by some other means. No attempt is made to cite radio frequency
molecular line observations of the cloud in the general neighborhood
of the star.
Note on refs_lc:
Light curve: references to photometric studies published since HRC.
An hrc means that significant references in the Second Catalog are
not repeated here.
Note on vsini:
v sin i, the projected axial rotational velocity, given only to the
nearest km/s. If no radial velocity value appears in col. RV, then
that reference is to the source of the v sin i; if a value for the
radial velocity is given, then the second reference is
(usually) the source of the v sin i.
Note on RV, q_RV, r_RV:
Radial velocity (heliocentric, in km/s), quality, and reference. In
all cases, these velocities are from the absorption line spectrum.
Velocities obtained with modern equipment usually replace those
obtained at low dispersion by the early observers. The quality letter
(a, b, c) expresses our judgement as to the uncertainty of the quoted
velocity: a indicates a velocity of the highest quality, with an
uncertainty of 1-2 km/s; b means a value with an uncertainty of 3-5
km/s; and c a velocity of still lower accuracy. For some stars we have
not given the published velocities at all. Comments on several special
objects (*) appear in the Remarks.
Note on Sp:
Spectral type. With the growing employment of red-sensitive detectors,
spectral types determined since the HRC have increasingly been
dependent upon criteria in the region longward of about 5000 A.
However, it is apparent that significant differences exist in T Tauri
spectra between such types and those assigned by the early observers
of the 4000-4500 A region ([498] and Appenzeller 1985). Furthermore,
it is not clear whether the spectral types of such stars change during
their light variations or at other times. Therefore, it may not be
possible to assign a MK type to a T Tauri star without further
qualification. We have not faced up to such issues: the types given
here for those stars for which more than a single classification is
available are either compromise values (usually indicated by :), or in
case of conflict that value which seems most reasonable to us. No
indication is given of the spectral region in which the type was
assigned. Several special cases are explained in the Remarks. Many of
the types in HRC were based on unwidened, very low-dispersion, often
underexposed Lick spectrograms; in all but a very few cases, those
classifications have here been disregarded. The conventions in col. Sp
are as in HRC: type K7, M0 means either K7 or M0, while K7-M0 means a
type between K7 and M0. If the Li I 6707 A line has been detected in
absorption, the type is followed by (Li). The very fact that the star
is included in this Catalog indicates that emission lines have been
detected (except in a very few special cases, all explained in the
Remarks), so the suffix e for emission is not printed for types G and
later in col. Sp although it properly is a part of the classification;
the e should be added if these types are quoted. However, in order to
avoid possible misunderstanding, that e has been included for all the
B, A and F types where line emission is present. An hrc means that
some significant information either in the Second Catalog, or
referenced there, is not repeated.
Note on r_Sp:
References to the source of the type quoted. Information in col. Sp
which does not appear in the papers cited is usually from unpublished
Lick material; a blank reference has that specific meaning.
Note on EW, n_EW:
Equivalent width of H-alpha emission (in A): These are from the
original sources, and are often mean values. Different observers at
different times sometimes quote very different results and it is often
uncertain whether this represents real variation or is an instrumental
effect; when real variations seem to be present, the mean is given
followed by a v. A number of cases where the W(H-alpha) value from
slit spectroscopy seems incompatible with the fact of detection of
H-alpha on an objective-prism plate are mentioned in the Remarks. A hk
in col. EW means that there is no information on H-alpha, but that
emission is present in the H,K lines of Ca II. A pr means that H-alpha
emission has been detected, but that no value for the equivalent width
is available. An abs means that H-alpha is in absorption. An em means
that unspecified emission lines have been observed [238]. A * means
that there is a Remark (see remarks.dat) .
Note on refs_spec:
Spectrum references show where the spectrum is reproduced (either
photographically or as a scan), or the spectrum is described or
discussed.
Note on type:
Type gives our judgment as to which group the star belongs.
The abbreviations are:
tt T Tauri star
wt weak-line T Tauri star, usually having W(H-alpha) less
than about 10 A and no other emission in the
optical region except Ca II H,K. This includes
most of the so-called "Naked T Tauri Stars".
su A star like SU Aur: type late F to K, weak
emission at H-alpha and Ca II, very broad absorption
lines (v sin i > 50 km/s), and relatively high
luminosity.
ae An Ae or Be star such as those described in [203].
fu A star of the type of FU Ori.
? Type uncertain: the information is adequate, but
the object does not fit into any established
group; these stars are usually described in more
detail in the Remarks. Also, one of the original
criteria for membership in the Ae, Be group was
that the star illuminate bright nebulosity, but
now a number of irregular variables are known
which are photometrically and spectroscopically
similar but are not nebulous or associated with
obvious obscuration (UX Ori, WW Vul, SV Cep, BO
Cep, ...). These questionable objects are also
marked ? , or in some cases a?, in the Table.
-- A blank means that the observational information
is inadequate.
Note on refs_chart:
Reference to an identification chart or photograph.
Note on location:
The name of the bright nebulosity, dark cloud, cluster, association,
or other object with which the star is associated or projected upon.
A number of southern cloud complexes are designated by the
abbreviations used by Schwartz [426]; note that these are not the
T-association designations of Kholopov (1959) or the R associations
of Herbst (1975).
The prefixes used are:
B Barnard (1927)
FS Feitzinger and Stuwe (1984)
Gum the Gum Nebula region
L Lynds (1962)
Ori the Orion Nebula region
Sh Sharpless (1959)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- RefCode Code number for reference
6-153 A148 --- reftext text reference
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Byte-by-byte Description of file: remarks.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- HBC object HBC identification
5 A1 --- Cont [a-g] Non-blank when several lines.
10-130 A121 --- reftext remark text
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Use of Special Symbols:
In remarks.dat and catalog.dat special symbols have been used
to replace greek letters and other symbols as follows:
SYMBOL USED MEANING
@ lower case greek alpha
^ less than or equal
% plus or minus
$ upper case greek Delta
# degrees
The Lick H-alpha lists:
Following the main catalog table in the reference (Table 1) are two
shorter lists which may be found useful, of the Lick LH-alpha and
LkH-alpha assignments, and of the H-alpha star discoveries made at
Bosscha Observatory by The and co-workers.
Acknowledgements:
We are greatly indebted to A. Klemola for his help with the
astrometric measurements, to B.F. Jones for unpublished coordinates
and other assistance, and to many colleagues for preprints and
unpublished information. We are also very grateful for partial support
by the National Science Foundation, most recently under Grant NSF
AST82-03115, for much of the observational work at Lick Observatory
that is included here as well as for the preparation of the Catalog
itself.
References:
Appenzeller, I. 1985, Phys. Scripta T11, 76.
Barnard, E.E. 1927, Carnegie Inst. Wash. Publ. 247.
Bastien, P. 1988, in Polarized Radiation of Circumstellar Origin
(Vatican Conference, June 1987).
Feitzinger, J.V. and Stuwe, J.A. 1984, Astr.Ap. Suppl. 58, 365.
(1984A&AS...58..365F ; Catalog <VII/68>)
Herbig, G.H. 1962, Adv.Astr.Ap. 1, 47.
Herbig, G.H. and Rao, N.K. 1972, Ap.J. 174, 401 (1972ApJ...174..401H)
Herbig, G.H. 1985, Birth and Infancy of Stars, ed. R. Lucas,
A. Omont, and R. Stora (North Holland), p. 535.
Herbst, W. 1975, Astr.J. 80, 503.
Kholopov, P.N. 1959, Sov.Astr.-A.J. 3, 291, 425 [36, 295, 434].
Lynds, B.T. 1962, Ap.J. Suppl. 7, 1. (Catalog <VII/7>)
MacConnell, D.J. 1968, Ap.J. Suppl. 16, 275 (Cep-Cas).
(1968ApJS...16..275M)
MacConnell, D.J. 1981, Astr.Ap. Suppl. 44, 387 (Pup).
(1981A&AS...44..387M)
Stauffer, J.R. and Hartmann, L.W. 1986, Ap.J.Suppl. 61, 531.
(1986ApJS...61..531S)
Wackerling, L.R. 1970, Mem. R.A.S. 73, 153. (Catalog <III/17>)
Modifications and Updates:
* August 1988 (George Herbig):
The only differences between this tape and the original paper
version are that a few small errors have been corrected, and
literature citations have been provided for several papers
that were only in press in June 1988.
Note that the stars in Table 1 having second-line entries
must have those read out of files epage1a and fpage2a, whether
first-line data is being taken from cpage1, dpage2 or from
epage1, fpage2.
Note also that in neither paper nor tape version of this
Catalogue was it possible to insert umlauts or accent marks in
authors' names.
The person who prepared this tape (G.H.) is hardly an an expert, and
does not intend to become one. The formatting can undoubtedly be
improved, but the tape is (hopefully) readable. Suggestions for the
improvement of any future editions would be welcomed.
* August 1992 (Shiro Nishimura):
Reformatting of the catalogue has been made at the Astronomical Data
Analysis Center of the National Astronomical Observatory of Japan. The
file, epage1 (the main file for the left page), and the file, fpage2
(the main file for the right page), were concatenated with entries of
the files, epage1a and fpage2a (the second line data files), being
inserted at the corresponding columns. Efforts were made to homogenize
each entry by correcting column shifts and by separating code flags
from numerical data. No essential change of data was, however, made
except for only one case: The v sin i data for HBC 419 was rounded off
from 12.5 to 13 according to the relevant description in the text
file. The file, iref (the literature references in single-column
format), was reconstructed into the format of one reference per line.
This and together with other two files, btext and grem, were updated
by deleting page numbers and surplus blank lines. Finally, corrections
have been made according to the list communicated by Dr. Herbig.
* August 1995 (Paul Kuin):
Reformatted the documentation to standard form.
* February 1997 (F. Ochsenbein, CDS):
Added missing galactic positions for HBC 370, 441, 148
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(End) N.P.M. Kuin (NASA/SSDOO/ADC) 03-Aug-1995