--------- - - --- - - - - - - - - - - -
- -- F- **** ------- --------- ---- - -
- ºr-º-º-º- - -
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| "…" - -- ºlº - - - - - - - - -


NASA
Reference
Publication
1312
1993
National Aeronautics and
Space Administration
Scientific and Technical
Information Branch
Spectral Classification With the
International Ultraviolet Explorer:
An Atlas of B-Type Spectra
Janet Rountree and
George Sonneborn
Goddard Space Flight Center
Greenbelt, Maryland

at T
^ E.
? H2,
, ſº 12.
|2|, ||
| (A2,
... . SPECTRAL CLASSIFICATION WITH
THE INTERNATIONAL ULTRAVIOLET EXPLORER:
AN ATLAS OF B-TYPE SPECTRA
by
Janet Rountree and George Sonneborn
Laboratory for Astronomy and Solar Physics
NASA/Goddard Space Flight Center
I. Introduction pose without reobserving the standard stars to make sure that there are no system-
A set of criteria for the spectral classification of B stars in the ultraviolet atic e
was published by Rountree & Sonneborn (1991, Paper I). In that paper it was
shown that photospheric absorption lines in the 1200–1900A wavelength region II. Data Processing
can be used to classify the spectra of B-type dwarfs, subgiants, and giants on a
two-dimensional system consistent with the optical MK system. The stellar wind
lines are not used for classification on this system. Stars with peculiar wind lines
are distinguished from "normal" stars, and are marked with the suffix "w." The
observational material used in Paper I consisted of high-resolution spectra from
the International Ultraviolet Explorer (IUE) archives, suitably resampled and dis-
played. Insofar as possible, the standard stars on which the ultraviolet classifica-
tion was based were chosen from among the MK standards.
The spectra comprising this Atlas were taken with the IUE short-
wavelength prime (SWP) spectrograph in the high-dispersion mode. The ex-
tracted spectral data, produced by the standard processing provided by the IUE
Project, were resampled to a resolution of 0.25A, normalized to a rough contin-
uum level between 1150–1900A, and plotted on 11 in. x 17in. paper on a laser
printer. For details of the data reduction steps, see Walborn, Nichols-Bohlin, &
Panek (1985) and Paper I. Our data processing procedures differ from those of the
previous authors only in that the continuum normalization has been made autono-
A number of representative spectra were shown in Paper I, in order to il- mous rather than interactive and that the plots were produced on a laser printer
lustrate the classification method. But these spectral plots were reduced in scale rather than a CalComp plotter. The software needed to resample and normalize
by approximately 50%, and thus were not suitable for practical classification the spectra is available at the IUE Regional Data Analysis Facility at Goddard
work. The purpose of the present Atlas is to make available a larger number of Space Flight Center. If the user does not have access to a laser printer that accom-
spectra at the scale used for classification. These spectra represent a dense matrix modates 11in. x 17in. paper, the spectral plots may be produced piecemeal on
of standard stars, and also some interesting individual cases. Readers may use the smaller paper, but the original scale (10A/cm) should be preserved. It is strongly
figures in this Atlas to classify their own IUE spectra, after processing the data as recommended that any spectra last processed before the improved extraction soft-
described in Section II below. The recommended procedure for spectral classifi- ware was put into production (1981 November) be reprocessed by the IUE Project
cation with the Atlas is described in Section IV. before undertaking the resampling procedure.
Although the Atlas should be useful as a guideline for ultraviolet spectral
classification with instruments other than IUE, it should not be used for this pur-
III. Description of the Atlas
All the stars whose spectra are presented in this Atlas were drawn from
the list in Table 2 of Paper I or from a second list of approximately 100 stars that
were subsequently classified (without knowledge of their previous MK types) on
the same ultraviolet system (Rountree & Sonneborn 1993, Paper II). In general,
these are stars with visual magnitudes brighter than about 6.5, having normal MK
types in the range B0—B8 III—V according to Rountree Lesh (1968), Hiltner,
Garrison, & Schild (1969), or Morgan & Keenan (1973). A few supergiants were
drawn from the work of Walborn & Nichols-Bohlin (1987).
The spectra are arranged in montages of four or five per two-page spread,
or "plate." The wavelength scale is indicated by tick marks at 10A intervals above
and below each spectrum, with numerical values of the wavelength in Angstroms
shown at the bottom of the page. The crosses along the wavelength scales mark
the echelle order splice points. The quantity plotted as a fine line at the top of
each spectrum is the normalized data quality factor, which in these plots primarily
indicates (by a downward spike) areas in which the data points may be contami-
nated by a camera reseau. The most important spectral lines, especially those used
in classification, are identified along the top of each plate. The stars are identified
to the left of their spectra. The spectral type given for each star is the ultraviolet
spectral type; in most cases, this is identical with the optical MK type. In Parts 2
and 3 of the Atlas the rotational velocity from Uesugi & Fukuda (1982) or the date
of observation is also given. Overall characteristics of the spectral type range cov-
ered by each plate are described in the text at the left of the spectra.
There are three parts to the Atlas. Part 1, Plates 1–14, contains se-
quences of spectra of standard stars for direct use in classification. Plates 1–7
show spectral-subtype (or temperature type) sequences for dwarf (class V),
subgiant (class IV), and giant (class III) stars. Almost all of these stars are stan-
dards listed by Morgan & Keenan (1973) or by Rountree Lesh (1968). On the
main sequence, where very fine subdivisions are possible, we provide some over-
lap between the groups of spectra on successive pages, so that the user will always
be able to bracket the spectrum to be classified between two standards. Plates 8–
14 present luminosity sequences at seven spectral subtypes. In these montages,
some of the standards in classes III—V have been replaced with other stars whose
spectra were judged to be equally representative of their type, so as to give as
many examples as possible of normal ultraviolet spectra. The supergiants (class
Ia) whose spectra appear here are the stars described by Walborn & Nichols-
Bohlin (1987). These stars have not been classified on the ultraviolet system —
the spectral types given are the optical MK types. The supergiant spectra are re-
produced in this Atlas in order to show the full range of variation of certain spec-
tral lines as a function of stellar luminosity.
Part 2 of the Atlas, Plates 15–20, illustrates the effect of rapid stellar ro-
tation on the ultraviolet spectrum. Each plate in this section displays two pairs of
spectra; each pair, closely matched in spectral type, consists of the spectrum of a
slowly rotating star (v sin i usually <50 km/s) and the spectrum of a rapidly rotat-
ing star (v sin i usually ~200 km/s). Although most of the rapid rotators are not
standards, these illustrations should be helpful to the user who wishes to classify
the spectrum of a broad-lined program star, since they show how these spectra are
likely to differ from the narrow-lined standards.
Finally, spectra with anomalous stellar wind lines, primarily strong ab-
sorption lines of C IV AA1548, 1550, Si IV AA1393, 1402, and/or N V AA1238,
1242, are illustrated in Part 3, Plates 21–26. These are stars whose ultraviolet
spectral types have a "w" suffix in the classification of Rountree & Sonneborn
(1991). As in Paper I, italics are used in the text accompanying Plates 21–26 to
distinguish ultraviolet spectral types from optical MK types. The spectrum of at
least one "normal" star of identical type is presented with each anomalous spec-
trum to show the good match in the photospheric absorption lines, which alone are
used in classification. More detailed studies of some of these stars are referenced
in the text opposite the spectrum in question.
IV. Use of the Atlas
After the user's program spectra have been processed as described in
Section II, they may be classified by direct comparison with the spectra in this At-
las. As in the MK system, the ultraviolet classification system is defined by its
standard stars, most of which are illustrated here. Therefore, a program star
should be assigned the type of the standard star that it most closely resembles. It
must be emphasized that the comparison should be made using only photospheric
absorption lines. The N V, Si IV, and C IV lines should not be used in classifica-
tion; they should be taken into account only in assigning the "w" suffix.
Table 1 lists the standard stars of the ultraviolet classification system, as
well as the photospheric lines used as classification criteria. This is a slightly up-
dated version of the similar table in Paper I.
In our experience, it is possible to assign a very accurate temperature type
to a star from its ultraviolet spectrum, while luminosity class may be more difficult
to identify accurately (see Paper II). Therefore, we recommend first locating the
spectrum of a program star among the standards on the main sequence, and then
going to the luminosity-effects plate at that spectral type to see if the star appears
to be a subgiant or giant. If it does, its temperature type should be verified by lo-
cating the spectrum on the subgiant or giant sequence. Of course, this is an itera-
tive procedure, since temperature type and luminosity class are not completely in-
dependent. Finally, the NV, Si IV, and C IV lines, if present, should be compared
with the same lines in the standard spectrum to see whether the program star has
an anomalous stellar wind. The behavior of the wind lines in the standard stars is
described in the text accompanying the spectra in Part 1. It is also noted in italics
in Table 1.
V. Conclusion
It is hoped that this Atlas will find extensive use in the classification of
IUE high-resolution spectra, especially for stars that have not been observed in the
visible region. Spectral types obtained by the procedures outlined here and in Pa-
per I should be entirely consistent with MK spectral types. In principle, the same
standards and criteria can be used for spectra obtained with a different ultraviolet
spectrograph, but in that case the standards should be reobserved with the other
instrument to avoid systematic effects.
References
Grady, C.A., Bjorkman, K.S., & Snow, T.P. 1987, Ap.J. 320,376.
Hiltner, W.A., Garrison, R.F., & Schild, R.E. 1969, Ap.J. 157, 313.
Hirata, R., & Asada, Y. 1976, Pub. Astr. Soc. Japan 28, 713.
Irvine, N.J. 1975, Ap.J. 196, 773.
Morgan, W.W., & Keenan, P.C. 1973, Ann. Rev. Astr. Ap. 11, 29.
Rountree Lesh, J. 1968, Ap.J.Supp. 17,371.
Rountree, J., & Sonneborn, G. 1991, Ap.J. 369,515 (Paper I).
Rountree, J., & Sonneborn, G. 1993, in preparation (Paper II).
Shore, S.N., & Brown, D.N. 1990, Ap.J. 365,665.
Slettebak, A. 1982, Ap.J.Supp. 50, 55.
Sonneborn, G., Garhart, M.P., & Grady, C.A. 1987, in Physics of Be Stars, ed.
A. Slettebak & T.P. Snow (Cambridge: Cambridge Univ. Press), 286.
Uesugi, A., & Fukuda, I. 1982, Revised Catalog of Stellar Rotational Velocities
(Kyoto: Kyoto Univ.).
Walborn, N.R., & Nichols-Bohlin, J. 1987, Pub. Astr. Soc. Pac. 99,40.
Walborn, N.R., Nichols-Bohlin, J., & Panek, J. 1985, IUE Atlas of O-Type
Spectra from 1200 to 1900A (NASA Ref. Pub. 1155).
BO
B0.5
B1
B1.5
B2
B2.5
B3
B4
U Ori
1640A (He ll) strong
1718A (NIV) strong
1748-51 (N III) marked
Si IV, C IV strong absorption
HD 36960,
N ill present
He ll, N IV moderate to strong
C Ill strong
Si IV, C IV strong absorption
o' Sco, 42 Ori
N IV weak to absent
He ll marked
1247A (C III) strong
1264A (Sill) present
Si IV strong, C IV wº, absorption
HD 35299
1264A marked but ºf 247A
He ll weak
Si IV absorp., C /V wº. to absent
22 SCO
1264A (Si II) = 1247A (C III)
1310A (Si II) × 1300A (Si III)
He ll weak to absent
Si TV moderate, C /V absent
o Sgr
1264A (Sill) > 1247A (C III)
1310A (Si II) < 1300A (Si III)
1485A (Si II blend) present
Si IV absorption
n UMa, n Aur
1264A (Si II) >> 1247A (C III)
1310A (Si II) > 1300A (Silll)
1485A (Sill blend) marked
Si IV weak
HD 20809
1310A (Sill) > 1300A (Si III)
1485A (Sill blend) prominent
Si IV weak to absent
Table 1 - Ultraviolet Spectral Classification Criteria and Standard Stars
IV
HD 75821
Interpolate between
V and Ill
Si IV, C IV absorption
A Lep
Interpolate between
V and ||
Si IV, C IV absorption
O. Vir
Interpolate between
V and Ill
Si IV, C IV absorption
A SCO
interpolate between
V and ||
Si IV, C IV absorption
y Peg
Si III, Al III, Fe III
stronger than B2 V
1600-10A (Fe II) stronger
Si IV stronger, C IV absent
HD 32612
Interpolate between
V and ||
Si TV present, C IV absent
HD 134687, 126 Tau
Interpolate between
V and III
Si IV present, C IV absent
53 Per
Sill, Si Ill, Al Ill stronger than
B4 V
Si IV present, C IV absent
HD 48434
N III, N IV stronger
1854-61A (Al Ill) stronger
1247A (C III) stronger
N V, Si IV, C IV P Cyg profile
1 Cas
N IV, Al Ill stronger
N Ill present but weak
SI IV, C IV absorption
o Per, o SCO
C III, Hell, N IV stronger
Silll 1300 multiplet stronger
Si IV, C IV absorption
12 LaC
Sill, C Ill stronger
Si IV, C IV stronger
* Ori
C III, Al III, Fell, Fe III
stronger than B2 IV
Si IV stronger, C IV present
*Cyg
Sill, Si III, C III, Fell, Fe III
Al Ill stronger
Si IV strong, C TV present
HD 89890
Sill, Si III, C III, Al III,
Fe Ill stronger
Si IV stronger, C IV present
No standard in program
B5
B6
B7
35 Eri, p Aur
Sill dominates spectrum
1655A (C I), Fell moderate
1670A (Al II), Al III strong
Si IV marginal to absent
6 Sex
Similar to B5 V but Al III
stronger
Fe Ill weaker
Si IV absent
o, Leo
Al II, C I prominent
Al Ill weaker than B6V
Fe ill absent
18 Tau
Sill dominant
Al II, C I prominent
Al Ill, Fe Ill absent
IV
t Her
Sill, Si III, Al III
stronger than B5V
Si IV present, C IV absent
19 Tau
Interpolate between
V and ||
Si IV, C IV absent
16 Tau
Interpolate between
V and ||
No standard in program
5 Per, t Ori
Sill stronger than B5IV
Si IV stronger, C IV absent
17 Tau
Sill stronger
Si IV, C IV absent
n Tau
Sill, Al II stronger
than B7V
27 Tau
Sill, Al Il stronger
than B8 V
Part 1
Standard Stars
Plate 1 a
C || Si || Si III Si || Si IV
Main Sequence [TTTT
I-1

BO - B2
U Ori
BO V
The earliest main-sequence B
stars are characterized by lines of
He II A1640, N IV A1718, and N III
AA1748,1751, which decrease
smoothly from B0 to B1. C III
x1247 begins to weaken at B1, HD 3696O
while the photospheric Si II lines
A1264 and A1310 begin to increase
in strength. The ratio A1264/A1247 BO.5 V
is approximately unity at B2 V.
In these standard main- 6 Pé
sequence stars, Si IV AA1393, 1402
is mainly photospheric, and shows a | | | | | | | | | | |
><
>4
}<
| Sz
><
IS2 | NA
Prs ZN
2.
N
><
+
Pé
HP6
Hº
><H
lsz
HAK
>4
marked decrease at B2. The stellar
wind lines C IV AM1548, 1550 are 42 Ori
essentially absent by B2.
B1 V
ſt Sz 1 >2 l NJ 1 >|< R2 | L sº SA Yºu’ | Sz Sz I NL’ | Sz SA 1 NA | NA I |\, | Szl | N/ | NAſ | Sz
2^NTTzv | 2 N. U /N | /N I zS F-S TZN | 2^N. I zS Jyv | z \ I zSI ArN | 2 N ſ zS TIZN I ZN |^ U zSI TZN | ZN | 2^N.
HD 35299
B1.5 V
|\ Rz | >2 'l Sz SA YA | >2 NZ NU/ | Sz SA *S*_l Szu |NZ 1 Sz I 1 >2 l NAſ | NZ
Prs zS-T-zs- zS Jyv Izs-r-z ST AfN | zS- zS rz-T-2s |^ I-zs] zS- zSU | zS
22 Sco
B2 V
1\ a NJº Sz. 1 >2 l Sz SA NL’ Rz Sz I Sz S.A. NAA | >2 Sz Nuº | Sz SA 1S2 | >2 1 ls. 1 Szl Sz NAſ | Sz
2^N. 2^N ZN 2^N. z N 2^ 2 N z \ z \ 2 N. zºN 2^N. ZN z N z N 2^N. 2^N. ZN
12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 14OO 142O 1440 1460 1480 15OO
Plate 1b.
C IV He || N IV N || Al || Fe III
ſ | | T F- T
| | | I | | | | | | | | | | | | | I | T | T

><+
26
26
→r-r
T.
r—T-
I -
m".
F-
I-
>}
>4
2%
gºmº.–26
2é
Bé
}<
}%
96
26
26
2é
26
+
>é
><
t
—1->6– k, | SA 1 & I 1 & | NZ | NZ | NUZ | }< | NLZ | NJº | | NZ | —e-l | >el | 3. | | Sz | ><! | sº I l sk
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
Plate 2a
Main Sequence
B2 - B5
The ratio Si II A1264/C III
A1247 increases monotonically from
B2 to B5 on the main sequence, as
does the ratio Si II A1310/Si III
A1300. The photospheric Si II lines
A1485 and A1533 also become
prominent in this spectral type
range.
Si IV AA1393, 1402 decreases
to marginal strength, while C IV
AA1548, 1550 is not normally pre-
sent in main-sequence stars later
than B2.
* º II Si || º Si IV Si ||
I | I | I | I | I T I | I | I | I | I | I | I | I | I | TI I
22 SCO
B2 V
N.A./ IV ANZ ><——-1–s’ SA NL’ R2 Sz | Sz. 1 SA Nue' | Sz Sz I NU/ | Sz SA 1S2 | >2 |Sz Szl Sz I |
Tzv | /N I /N | 2^N. I zS ZIN Prs 2 N | 7 NTI zS Jyv | 2^N. I zS Aſ N | z \ I zS TZN | ZN I |^ I zS I /N | ZN | 2'N
o Sgr
B2.5 V
ſ\ R2 1 Sz | Sz SA NA’ | Sz—sz Nº Z | Sz SA isz–1–N2 |Sz | >2 Sz NAſ | Sz
PS 1 zS-I-zs- zS rs—T-2-1-2s Aſ N | Zs- zS zS-I-zsi Prs-T-zS rz S- /N I-zS
n UMa
B3 V
\/\ AZA R2 Sz | Nº 1 SA N/ | Sz Szl NU/ | Sz SA Sz | Sz IS2 I Sz 1 NZ NAſ | Sz
PS zS-I-zs- zS J’N Tzs-r-z ST AfN | zS- zS rzs—I-2s |zS -zS zS-I 2N. |-zS
HD 20809
B4 V
Sz Sz NA SA NLZ NZ | Sz SA NZ | Sz Sz Nue' | | SA I NA | NA 1 ls, | Sz 1 Sz NAſ | Sz
2^N. | ZN l 2^N. | ZN I zS PS /N | ZNTU zS J’N | 2 N I zS Aſ N | /N I zS I / N | ZN I |z S I zS I / N | zYU | 2 N
35 Eri
B5 V
S.A. Alº" Sz Sz Sz | " NZ Rz Sz | NZ SA ×2 " | NZ NZ I NL/ | Sz SA Sz Sz |NZ 1 NZ | Sz NAſ | NZ
ZN ZN /N 2N ZN ZN /N /N ZN /N /N /N /N ZN ZN /N ZN ZN ZN ZN ZN ZN ZN

12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 1 400 142O 1440 1460 1480 15OO
Plate 2b
%—l
%—l
|
9% |
1 NZ
ZN
|
1 & !
ZN
N2 |
ZN
l
3.
|
| \,
|
|
Si || F6 || C I Al Il Al || Fe ||
T TTT | F- T
H–H–H–I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-T-I-T-I-T-I-T-I-T-I-T-I-T-- I-
—He-Hºe-->4——º-Hº-H3–H54–He-He-Hei-He-H2–H–4–H–24-Hº-Hº-Hºd—H->e- >}—
r-I-T-I-I-I-I-I-I-T-I-i-m-----|--|-
––––be-Hºd——º-H->e-H2– → He-He-He-Hºe-Hº-Hº-Hº-Hº-Hº-Hºd—H->e- >{—
F-I-T-I-T-I-m- | |-m-m-m-m- rº-I-T--
—H·e-Hº-Hº-Hº-Hº-H%—Hº-Hº-Hº-Hº-Hº-H2—H->e-H–4–1–––Hº-Hºd—H-e- >{—
----|--|--|--|--|--|-m-m-m-m-m-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ
—l sº ls, | SA 1 \, . 1 sº I | NZ | RA/ | NUZ | NL’ | NUZ | NA | Lºz– | \, 1 sº I | J. 1 | < | | NZl | 1 sº I Sk |
|-z- Fºs I ^ -zs- | Zs- I Z\ | VN | ZºS | AN | 2.TV | WN | z- -zs- as I T I I-zs— | ZN | I-7s- T I
-v-Y- –-º-º-º:

1500
1840
1540
1820
1560
1800
1600
1780
1620
1760
1640
1740
1660
1720
1680
1700
10
Plate 3a
Main Sequence
B5 - B8
º ſº e S
*::: * t º | # s

range of main-sequence types.
Fe III AA1892, 1896 weakens at
types later than B5, while Al III
AA1854, 1861 reaches a maximum
at B6.
35 Eri
B5 V
6 Sex
B6 V
o, Leo
B7V
18 Tau
B8 V
Z\/vºy
Y.
º *NWA
ººze 4–4–4–5%—->{—HSé-º->4—941–H4––PéH%—H·4——4—£4–H4+->4––PéH3%—Hº-Hº
|
|
Aſ NZ 1 NZ I NA YA | NZ NZ NA | NZ NA 1NZ | \Z |NZ 1 NZ I 1 NZ I NA | NZ
\ pºw-r-zV-T-zV ZN yW Tzv -zVI AN Izv - ZN rzw-T-zv |zw r-zVI z\ | ZN I ZY
*— v. v — 4–1 v v_v_1 - 4 1NZ | \Z |NZ NZ I 1 NZ I NA | NZ
VN -zV-T-zV ZN yN Izv-r-zVI Aſ N. | z\ . zS rzV-T-zV |2V-Tzvi zST-I /N | z\
--|--|--|--|--|--
1 NZ I NZ 1 | % NZ 1 NZ | NZ NA \/ | NZ NZ | NA | NZ NA 1NZ | NZ 1 |NZ | NZ | 1 NZ I NAſ | NZ
ZN ZN /N /N /N ZN /N ZN ZN ZN ZN ZN ZN ZN /N ZN /N ZN /N /N
1200
1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
1220
11
Plate 3b

+
|
v-
|
+
++++++++------|--|--|--|--|--|-i-º-Hº-Hº-n
——e- bé l >é —e- 1–36 | 13% | % | }< | Sk | }< | % | 1–36 | 1–36 | I >e- 1 —k l |-> l | >él | 1–36 | | >{ I
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
12
Plate 4a
C || Si || Si || Si || Si IV Si ||
Subgiants
[TTTT F- |
I | U | I | I | I | I

BO - B2
HD 75821
BO IV
In the subgiants, He II A1640
remains prominent and C III A1247
×
><!-Hº-Hº-Hº-Hº->4—k—º-->4—Hº-Hº >é–HºëHé—Hº-Hºd—Pé–HºHº-HºHº
remains strong through B2. Spectral | | | | | N | |
type is determined by the relative
strength of the Si II photospheric
lines. C IV AA1548, 1550 can A Lep
Sometimes be seen as late as B2.
BO.5 IV
><+}<!-Hºº--><-Hºë—24–36–Pé—->é–H54——24—k—Hº-Hº-Hé–H54——4—Bé–H54—Pé–HºHº
HD 63578
B1 IV
|\ -- R2 | Sz | Sº I SA N/ | >z—sz NU/ | Sz SA 1S2 I sai lsz Szl
Prs TZN | ZY I zS PTN Tz's TI zS ] ACN |-zS I zS W ZN | ZN I |z S I zS]
X SCO
B1.5 IV
| | Sz NA. 1 SA NL’ R2 | >2 l Sz SA Y-Z Lez—sz | >2 SA Sz—l szl |\z | Szl
2^N. T^N. I 2^NTI zS I 2 Nºv I zS 2TV Prs Tzv | zVTI zS P’N Izs U zS Aſ N. |-zs U zS U ºf N | Z STI |^ lſ zSI
Ö Cet
B2 IV
I | Sz Sz | Nº 1 SA N/ Rz 1 S2 | Nº. 1 SA NZ | >2 Sz I Nuº | Sz SA 1S2 | Sz 1 |\,. 1 Szl
ZN ZN ZN ZN 2^N. ZN ZN ZN ZN z \ ZN 2 N ZN ZN ZN ZN
12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 1400 142O 1440 1460
Plate 4b

I-I-I-I- | H–I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-
- T-I-I-I-I-I-I-II | W- | —m-I-T-Y-T-I-T- | — IT | - - H-T-
He-Hºe-->4–H–2– ×—H>e-Hei-Hºt—Hº-Hºë—Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-H-4—
W w vºm-º TW
ſ— F-I-In |-|--|-
Hº-Hº-Hºd——º- *—H%—He-He-He-He-Hee-Hee-H->e-H-><!-H--->4–—Hºd—H-e-H->}—
—H·e-Hé-->4——º- ×—H*—He-Hº-Hº-Hº-Hº-Hº-Hº-H->e-H–4——Pe-Hº-Hº-H-4–
—He-Hºe-H4——º- ×–H%—He-He-Hº-He-Hºe-H2—H->e-H–2–H–k——Hee-Hé—H->e-H–4—-
→e-–4–4–4– *——º-1-36-1–%—l—4–1—º-->4–1—%—l—->e-Hº-l——4—Be--->e--->e-–—4—
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
14
Subgiants
B2.5 - B7
The photospheric Si IV lines
persist until type B5 in the
subgiants. The relative strength of
the Si II and Si III spectra makes a
useful spectral type criterion.
Plate 5a
C || Si II SI III Si II
[TTTT
SI IV
S. III

W | T | I | I | I | I | U | W | I |
HD 32612
B2.5 IV
W. zº R z NA | Sz | S2 Nue | Sz | SA 1 NJº | NAA | |\, | S.2 | 1_NA | NJAſ | Neº
º Lº N. IrSV Izs- zS Aſ N I-zs- zS Izs— 2^N. I |^ I zS] zS-I z \ |-z's
126 Tau |
B3 IV
D R2 1 >2 l Sz SA YA | Sz—sz NU/ | Sz SA 1NZ | Sz |Sz Sz i S-2 l NAſ | Sz
Fºs 1 zS-I-2S→ zS PTN Tzs- zS 2^N. I-2s- zS I /N | 2^N. I |^ I zS zS-I 2^N. I-zS
T Her
B5 IV
R2 I NAA | SA NA,” NJA I NA,” NU/ L S2 I NAA NA I |Sz | Nue' I NA | NAſ | Sz
—K– F-S-I-2s | I zS Jr.'N Hº I >< Aſ N. | zS- >4 TZN 2 N - |^ I >< I ZN | 2^N. I-z's
r—r—my— | | r) | | ſ
19 Tau
B6 IV
A M \ ANA - Lasſwº z Rz 1 \z | \, h NA NZ | >2 > YUZ | Sz SA Sz—l Szu ls. | Sz 1 NZ I NAſ | Sz
\ Prs I / V 2^N. I zS JºW Izs- zS 2^ I-2s- zS I ºf N | 2^N. I |^ I zS zS - I z \ |- zS
r—-r-ţ----|--|-- -I-T—ºr-
16 Tau
B7 IV
**.*.*-->el->e >é–Bé—->é——e->é >4–1->4––Pé! %—l—º-->4 *——e. Bé–—º ->é–1—24 |→e
12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 14OO 142O 1440 1460 1480 15OO
Plate 5b 15
Si || F6 || C | Al Il Al || Fe III
H- TTT --— F- T

→ p−r-T-I-T-Y-L-I-T-I-I-T-I-T-I-I-I-I-I-I-I-I-T-
He
*—
}<
9é
HX:
Hº-
Hºe
He-
He-
Hºd
He-
→
ZN
Fº
×
><
2é—
WZN
}<
>{
24
>{
Bé
>é
+
><
>{
Hº
><
><
Fº
>4
×–
TZN
IZN
}<
Hºt-
—l NA’ | k, l SA | NA’ | I NA | | N/ | NZ | NU/ | NLº | NUZ | NZ | 1 NA | | N/ | | sº I | J. | | NZ | | NZl | | N/ | | sk |
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
16
Plate 6a
Giants
N V f ||| Si || Si || Si || Si IV

TTT F-
BO - B2 ſ , --I-T-Yr-
HD 48434
In the giant stars He II A1640 BO III
persists to B2, N IV A1718 to B1,
and N III AA1748, 1751 to B0.5.
Although C III A1247 is stronger ><!--> *{-><--><-Hºë—4—k-Pé––––Pé——24—º-Hº-Hº-Hé–Hº-Hºd—Pé-Hºë—Pé–HºH-6–H4—Hº
than on the main sequence, the ratio | W | | | T | W WY
A1264/A1247 is still near unity at
B2 III. Si IV AA1393, 1402 and
C IV Ax1548, 1550 exhibit P Cygni 1 Cas
profiles at B0 III, and remain as
strong absorption lines throughout Bo.5 III
this spectral type range.
NJef I l NAC ><——2–1–Sz SA NLeº KZ 1 S2 | Sz SA NA’ | >< 1 >2 l Yue' | Sz SA 1S2 | Sz |\z 1 >2 l 1 >2 l NAſ | Sz
wV. TzY | zv TI /N | 2^N. I zºl 2TN Prs TZN I Tzvi-I. zS Jº V | ZN I zS Aſ N | /N I zS TZN | ZNTU |^ I zSI TZN | ZN | z \
o SCO
B1 ||
|
NA Sz. 1 NJ. 1 S2 NA 1 SA NLef K2 I NA | ſ SA N.Z. | Nue' | S2 | NL’ | NA’ | SA | N/ | NA’ I |S. | S2 | NAA | NAſ | Nue'
z \ TzY | zv TV 2N. | 2^N. I zS 2TN F’s TZN I 7\TI zS Jyv | 2 N I zSI Aſ N. | /N | zS I ºf N | ZN I Prs I zSI U ºr N | /N | 2^N.
12 LaC
B1.5 ||
1 \\z / sº I S. SA NL’ K2 | > || > | Y/ | | sº Yºu,” | >2 SA Sº I S.2 |NZ | >2 l Sz I NAſ | Sz
2^N. Tzv | z \TI 2^N. | /NTI zS /TN Prs ITZN | 2^NTI zS rN | , N I zS ZON | /N I zS Tz N | 2 NI |^ I zSI TZN | ZN | 2 N
Tr” Ori
B2 ||
| NA* 1 S2 | NA 1 SA Niz KZ 1 NA | Neº 1 SA NA | NA 1 Sz I Yue' | NA’ l SA | N/ | NA 1 |Sz | S2 | | N/ | NA | NA
/N 2^N. ZN /N 2 N 2^N. 2^N. /N z N /N 2^N. ZN 2^N. 2^N. 2^N. ZN /N 2^N. ZN ZN ZN
12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 14OO 142O 1440 1460 1480 15OO
Plate 6b 17
C IV He || N IV N || Al ||

×–
Hº-
Hº
Hº
Hº-
—l NZ kz | SA l Sz I | N/ | | N/ | | NJ’ | | NY | | NA' | NZ | | Sz | SA | Sz | | NZ | | | N/ | Szl
| ZN | Fº I ^ I ZN T I ZN | IZN I }< | 2^N. | >4 | ZY, | —%- | VN | Hºë | I ^- I ^ | Izs I | zºv I | Izº | } zS }
—Hº-Hº-Hºd——º-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-H->e-H–4——Pe--Hél–Hºe-H–24–
>{
24-
>{
Bé
><
26
>{
|
26
><
Hºë
>4
— NZ I k, | SA | NZ 1 NZ | | N/ | NUZ | NJº | NAſ | NJ’ | }<- | NZ | | N/ | _l Sz I | SA | | Sz | | NZ 1 | | NZ | l Sºl |
ZN. /N ZN ZN /N ZN ZN Tzv T ZN ZN
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
18
Giants
B3 - B8
Si IV persists to B5 and C IV
to B3 in normal giant stars, but the
spectrum of stars in the B3—B8
range is still dominated by Si II
lines.
Plate 7a
Si || Si || º Si IV Si ||
I | T | I | U | U | I | I | I | I | I | I | -I | I | I | I |
HD 89890 |
B3 ||
Wºwºwſ >2–1–N2 | NA I NL’ R2 Sz_l Sz_ SA Yue' | > 1 ><! NU/ | Sz SA | N/ | NA' | Nue' | S2 1 Sz NJAſ | Sz
| ZNTU /N | 2^N. I zS 2TV Prs TZN | ZNTTI zS JyS | /N I zS Aſ N | 2 N I zS I /N | 2^N. I |^ I zS TZN | ZN | ZN
Ö Per
B5 ||
AJYMAZ. A R2 Sz—l Sz SA NA,’ | >~1–41 NUZ | Sz SA | Sz | Sz I Sz Sz I NAſ | Sz
Prs zS-I-2s zS J’N F-2s-r-zs ACN Izs— zS Izs—I-zS |^ I zS rzs-I ZN |-zS
17 Tau
B6 ||
2 MA/MAN al R2 1 >2 l | SA N/ | Sz Sz NU/ | | SA Sz_l Sz. IS2 l Sz 1 Sz I NA | Sz
\ Prs r-z-T-zº- zS P^N. Tzs-r-z ST Aſ N. I-zs— zS Tzvi-T-zs IzS I zS Izs-I /N |-zS
n Tau
B7 III
AºAM, Z R2 | >2 l Sz SA YZ | >2 Sz NU/ | >2 SA | N/ | Sz |NZ l Sz Sz NAſ | Sz
\ Fºs 2s-T-2s- zS Jyv | Zs—T-zs Aſ N. I-zs— zS rzs-I-2s |z S I zS zS- 7W |-zS
27 Tau
B8 ||
Wy A 1AMMa al.ſvºw i S.2 Nue 1 NL’ K2 | N/ | S2 SA NA | Sz Sº I NUZ | Sz SA | N/ | Nue 1 |\,: | S2 | 1 Nat | NAſ | Sz
ZN 2^N. 2^N. 2^N. 2^N. 2N. 2^N. /N 2^N. 2 N. 2N ZN 2^N. zS 2 N ZN ZN ZN ZN 2 N z N 2N.

12OO 122O 1240 1260 128O 13OO 132O 1340 1360 1380 14OO 142O 1440 1460 1480 15OO
19
Plate 7b
Si | C IV F8 | C | A | AI |
[] [-T | | [–]
| U | | | J | I | T | J | | | | | | | J | | | U | T | J | I | | | | | | I | |
→ | ~m~+++++
WWW |
––– Rz | NA 1–sz ! 1 sz_| I NA | NU/ | \/ | NA! | \AY | >< | |NA | 1 sz_ 1_sz ! | NA | | »» |_> | 1 sz_| | »| 1
|-zs+ KN I zN I z> | I-7V | I/\ | AN | ZYK | Z\ | ZY. | | VN | I"Z\ | | zx | | z] | | » | ZN I | I ZW | | zs| |

→+—pe++++++++++++++++++++++++++++++++++ –––––––
| | | | | | | | W | | [T | | [T | | | | + [] | – | [` T-
→+—+—–>4––><+———+—–*—–><~+–––––––Pe+––><–––><+–––––>< |-><++><––––
→ ~T~~~~~ – m-I- | | | | T [~
→e+–pe-->4––><++>+++++ – |—+—–łe--be--Pe-+><+––><+––||–––>< |—>4–––><+—+—>+
→
→→–be+−→é–→→→→→→→→→→→→→→→→–k–––>< –><~~~><—–––
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880
1900
20
Luminosity Effects
at BO
The indicated lines of C III,
N IV, N III, and Al III all increase
in going up the luminosity sequence
from main sequence to giants. The
wind lines of N V, Si IV, and C IV
exhibit P Cygni profiles in giants
and supergiants.
Plate 8a
N V Si IV
T H
| 'J | | | I | | | | I. . I. T | - I | U T
e Ori
B0 la
ſ N º NZ NZ | NZ 1 NA | NZ NZ | | N/ NA 1NZ | NZ lNZ NZ | 1 NZ | NAſ | NZ
\ VN zS-I-zs zS I z\ z\ | Izs ZN rzV-I ZS |ZN zSI Izs I ZN | zS
| ſ | | | | | | | | | T | | I r- | | -T T-I-T-I-I-I-T-Yr-
HD 48434
BO ||
NZ 1 NZ | NZ NA N/ | NZ NZ Yuz | NZ NA 1 NZ | NZ IN/ NZ | 1 NZ | NA | NZ
WN I-zV-T-Zw ZN J/N Tzvi-r-zVI Aſ N. I Zw zS rzv-T-zv |ZY z\| z\- ZN | zS
HD 75821
BO IV
×!--k+x+x+x+-->4–2–3–2–H3-H4—k H-4––XHK–H3––4–3–H54—be-i-kH%–H4—Hº
u Ori
B0 V
w Z 94–1–24–1–24–1–24—94–1->4—24:1–3%—l->4–1–24—24–1–24–94—24:1–24–1–24—1–2%

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
21
Plate 8b
}IV º | * N || Al III
| U | I | I I I | I | I | I | U | I | I | I | U | U | T | I | I | I | I | | TI
| T-T-I-I-T-I-T-
| Sº I 1 \Z | | N/ | NU/ | NJ’ NA \Af | | N/ | ſ' N," | NZ | SA l | \, f | NZ 1 | N/ | l Szl |
I zs-I I ZV | IZN | ATN | AN | zw ZN | —%— | wV | I ºv | I ×– U zº I |^ I | AV I | IZN. | I zS I
-T-I-T-I-T-Y- Tºſſ-yr-ſwi-MI-
—l NJ’ ſ | SA | S. 1 \Z | | N/ | NL’ | NJ’ \/ NJP | | NZ | | N/ l NAA ſº J | | Sz | | NZ 1 | 1 \Z l Szl l
I-7s- Bé U ^ as I I ZN. | IZN | Aſ N | AA | /N ZY, | }<— | L^N. | TZN | I ×– U ^ I |^ I | /NT | TZN | I zS I
ºs- I- —e- W
--T-I-I-T-I-T-I-T-I-T-Y-L-I-T-I-I-T-I-T-m |-T | |
—l NAZ | ſ SA | Sz I | N/ | | N/ | NUZ | NJº NA NY | | NZ | | N/ | NZ | SA | | Sz | | N/ | | | N/ | | Sol l
I-z- Pé U ^ l ^-I U | IZN | ZIN | &\s | zºn | ZY. | —}<- | VN | ZN | I ×– U ^ T |^ I | zVTI | Izv | I ^ —I.
r −ſ r——-r-r-ţ- | -r] T. |- 1')
—l ><—l bé I >é | ×-l 1—2% | 1-26 | % | }< | }% | }< | % | 1->6 | 1—2% | | ×- | Sk | |→e ſ | ><l | 1–2% | l >{ |

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
22
Plate 9a
Luminosity Effects
at B0.5
The C III, N IV, N III, and N V C || - Si IV Si III
Al III lines are luminosity indica- I I T] | U T- I I I | I | | I | lſ —I T I
tors. The stellar wind lines are in | J | | | | I | | '... | | | | T
absorption, except in the supergi– |
antS.
1: Ori
B0.5 la
NZ 1 \\zll SZ —NZ | NZ NA }< NZ 1 NZ | NZ NA N/ | SZ —NZl Y-Z | NZ NA 1NZ | NZ IN/ 1 NZ I NZ N/ſ | NZ
r—zº-T-7s-1-Zvi /NT /N VN I ZV-I-Zw ZN J/N I-7s- z\ | ArN I-zV- ZN IZN | ZN I |ZN I ZN | I /N | ZN | zS
6 Cru
B0.5 ||
NZ 1 1–4–1–4–1–Y >4—K–Pé 1 NZ | NZ SA YZ | SZ —NZ | YUZ | NZ NA 1NZ || >zu lNZ NZ | 1 NZ 1 NAſ | NZ
ZN ZN ZvT-zvi zS VN r-zV-T-zV zS J/N TZS-I-ZVI Aſ N I-zV- zS rz-T-7s |ZN r-zVI Izv | /N I-zº
A Lep |
B0.5 IV
NZ NZ | NZ NA Y/ L \Z NZ Yue | NZ NA NZ | >2 |NZ 1 NZ 1 NZ I NA | NZ
WN zvi-T—zvi zS yN | Zs-r-zvi ArN I-zV- zS rzw-T-zs |zw r—zvi zS - ZN T-zº
—I-I-I-I-I-I-I-T-r-
HD 36960 |
B0.5 V
NZ 1 | >z 1 >2 l NZ 1 NA }% NZ 1 NZ | NZ NA YZ | NZ 1 NZ I Nua | NZ 1. NA 1 NZ | NZ 1 INZ | NZ 1 NZ I NA | NZ
ZN ZN ZN /N ZN /N /N ZN ZN ZN

1200 ºz26 1240° 260 ° 1260 °isoo (320 ° 1346 1360 ° 1386 200 °1420° 1440 1260 °1480 ° 1506
23
Plate 9b
C IV N IV Al Ill
ſ | F-
| U | U | I I l !--- J. – U | I | – T | U I | I | I | U | I
I-II-T-ſ-ſ-TIT-T
—Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-H-4––Pei-Hº Hº-H-4–
—Hºe--be-Hé——º-Hº-H%—He- Hº–Hé-Hº-H2−H->e-H–e1–1–4––Hº-Hºë—H-e-H-4–
—t-tº-m-t-t-t-t-r-T-I-T-I-T-I-T-I-m- —t-I-I-I-
—Hºe-Hºe-H4——º-H->e-H%—Hºe- He-He-Hº-Hº-Hº-Hº- —k——Hºe-H *— He-H->}—
rº-rºr-r-T-I-I-I-I-I-I-T-I-T-I-T-I-T-I-T-Y-I-I-I-I-I-T-
—l—e- bé ſl >é —e- |->e- 12% | –36 | & N. | >é | >{ | >{ | bé | |->e-l —e- > l |->e- | >é–1 | 1->6 | l >d l

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880
1900
24
Luminosity Effects
at B1
The Si III multiplet at AA1290–
1300 is luminosity-sensitive in the
B1—B3 spectral type range. C II,
Si IV, C IV, and Al III exhibit P
Cygni profiles in supergiants, but
not in stars of luminosity class
III—V.
Plate 10a
C || Si || C|| Si IV Si ||
| - H |
I | I | I | I | I | lſ | I | U | U | I | I | l | T | U | I |
HD 148688
B1 la
MA M. Jºſ | NZ NZ | | NZ NA YA | NZ –Az Yuz' | NZ NZ | \Z |NZ NZ 1 NZ | NA | NZ
\ |^ z\ |-|zV ZN J/N Tzvi-r-zVI ArN I-zv- ZN rzV-I-Zvi |zV- * Izs T-I ZN |-z\
r—-T-I-m-m-m-
O Per
B1 ||
>é+*H*——24-HºH)4—3–Pé–H54—H·4––24—%—H·4––PéHé–Hº-Hº!—#4–H4+->é——24–36–H4—Hº
-T-T-
HD 63578
B1 IV
|\ º Rz LSZ | NZ NA NZ | NZ v Y-Z | NZ NA Y | Szil. |NZ NZ 1 NZ NAſ | NZ
W VN zvi-T-Zvi ZN yN I-zV-r-zVI Aſ N |-zV- ZN rzV-I-ZN |zV-T-7s z\- ZN | zS
to' Sco
B1 V
NZ N/ NZ 1 NZ | NZ NA N/ NZ NZ | NZ NA YZ | NZ NZ I Y/ | NZ NA NZ | NZ |NZ 1 NZ | 1 NZ | NA | NZ
ZN ZN ZN ZN /N ZN ZN ZN ZN /N /N ZN ZN ZN /N ZN ZN ZN ZN /N ZN ZN ZN ZN

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
25
Plate 10b
C IV Al Ill Fe ||
| | -I | I | I | I | I | I | I | I | T | I | | | I | I | l | I | ſ | I | | T
rº-r-T-I- |
NZ NZ NJ’ | NA/ | | N/ | NA J | Sz | | NZ 1 | º NZ I
NAA NA’ NA’ \A | NZ J l | Sz I | NA' | | vzl |
Hº: pe-H4——xe-H-x-H%— Hº-Hº-Hº-Hº- H->e-H–2–H r—I A-I-T-Z-- ^ -

−1–º
be
|
>é
1 sº I
ZN
|
|
>k-
|
|
% |
|
—e-
|
×-l
—k-
|
|→
l
| Szi |
º
#
>{
1500
1900
1520
1880
1540
1820 1840
1560
1800
1600
1780
1620
1760
1640
1740
1660
1720
1680
1700
26
Luminosity Effects
at B2
Lines of C III, Si III, Fe II, and
Fe III are luminosity indicators for
main-sequence, subgiants, and giant
stars at spectral type B2. C II,
Si IV, C IV, and Al III exhibit
P Cygni profiles in supergiants.
X* Ori
B2 la
T* Ori
B2 ||
k Cen
B2 IV
o Cen
B2 V
NZ
NZ
NZ I
/N
NZ 1
NA
NZ T
%—9é——%
| NZ
| NZ
I
NZ |
| NZ
NA
Plate 11a
C || Si || C II Si IV Si ||
| TTT | H | l
U I I | I | I | U | I | W | U | l | I | U | I | U | ſ | |
NZ 1 NZ | NZ 1 NA | NZ l NZ | Nº. | NZ 1 NZ | N/ 1 IN/ | NZ | 1 NZ | NA | NZ
VN z\-T-Zvi zS *-i- T-zV ATN I-zV-1 ZN rzV-T-Zvi I/N -zVI rzV-I ZN |-z\
ſ - - - - -
l
NZ NZ | NZ NA Y/ | SZ 1 NZ YA L NZ NA 1 NZ | SZ |NZ | NZ | NZ | NAſ | NZ
Prs zv-T-zv- ZN J’N Tzv --zvi ATN I-zV- zS rzº—T-zs |ZN I zSI rzV-I /N |-zS
|-|--|--
ſ NZ 1 NZ | NZ NA N/ | NZ NZ NA/ | NZ NA 1NZ | NZ 1 |NZ 1 NZ 1 NZ I NAſ | NZ
WN zv-T-z- zS J’N | z\-r-zVI /N I-zV- zS rzV-I-ZS |ZN Tzvi z\-I ZN | zS
}<!-
%
NA

1206
1420
12
1200
/N
/N
1380
1240
/N
ZN
1360
1260
1340
1280 1300
ZN
27
Plate 11b
}IV F6 || Al || F6 ||
T-H-I-T-I-T-I-T-I-T-HTH −I-I-I-I-I-H-I-T-Y-L----T—T-HTH −
T- W’’ ~r wry w w y wry
T-I- m-ſ-ſ-ſ-ſ-
k, I SA | sº I 1 N.A | 1NZ | NL’ | NJ’ | NA | N/ | | N/ | | N/ | 1 < | SA | | N/ | | | I ~! |
Fº I ^ I ZN T TZN | IZN | AN | 2\, | zºw | ZY, | >< | VN | I ºv | U ZN | + ^ I | zVTI | I | I- ^l U

T-I-T-I-I-T-I-T-I-T-I-T-m
be-->4——º-l——e-->4–1—%—l—k——k——3– —e-l-->4–1–1–3%——->e--->e——->e-l——º-
%
I NAA
1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 ^ 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
28
Luminosity Effects
at B2.5
The principal luminosity indica-
tors at spectral type B2.5 remain the
lines of C III, Si III, Fe II, and
Fe III. The Si II blend at A1485
makes its first appearance at this
spectral type. The supergiant wind
features of C II, Si IV, C IV, and
Al III are weaker than at B2.
Plate 12a
C || Si || C || Si IV Si || Si ||
| TTT || |
| | —I- | I | | I | I | I | | I | | | U |
HD 92964 |
B2.5 la
v. A NZ NZ | | NA N/ | NZ 1–Azil NA L NZ NA 1NZ | NZ |NZ 1 NZ | 1 NZ NA | NZ
PS zv-T-zº- ZN yV F-7s-r-zvi ArN | Zs-r-zV rzw-T-zs tº -zVI z\-I ZN | z\
tº Cyg
B2.5 ||
f", x N/ L NZ l' NZ NA NZ | NZ NZ Yue L NZ NA 1NZ | >Zu |NZ 1 NZ I 1 NZ I NAſ | NZ
Prs z\-T-zv- ZN yN Tzvi-i-zVI ArN I-zV- ZN rzw- ^: 2N−zvi z\-I /N | zS
HD 32612
B2.5 IV
\ſº NZ LSZ | NZ NA N/ | NZ v N.Z. | NZ NA 1NZ || >zi |N/ 1 NZ 1 NZ NAſ | N/
TVN zv-T-z- ZN yS TzV-1-zS AN |-zV- ZN rzv-T-Zvi tº as º | ZN I Zw
- -I-I-T-I-
A Lib
B2.5 V d
-4- >é–24—26–%—->é——26–24—3%—l->é——24:1–3%—l->é——24—124–1–24–94—24:1–24–1–24—1–2%

1200 1220 1240 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
Plate 12b 29
C IV F6 || He || A| || Fe ||
26
+2%
%
}<
Bé
Hé
><
26
26
><!
ZN
>{
--T-I-T-I
26
><
Hºč
}é
>{
24-
>{
Bé
26
H
26
>{
Izs
+
><
Hºč
zS
26
Pé
>4
2%
26
º
9%
}<
}<
9%
Hé
2%
26
|
>é
>é.
+
*
—H
>}
—l-e--be-->4——º-l—re-->4–1—3–1—º-Hº-1–24–1–24–1–9–1–1->4–1—24–1–1–24——Be--—e--—º-|-->el—

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
30
Plate 13a
Luminosity Effects
at B3
Lines of C III, Si III, Fe II, and C || Si || C || Si IV Si ||
Fe III remain luminosity-sensitive at J U |- I I TTT I ſ I -T- I U U I
type B3, but show less variation | | | | | | | | | | | |
than at earlier types. The most t ſ ſ d
prominent wind feature in B3
supergiants is C IV AA1548, 1550. o°CMa
B3 la
M. NZ NZ I l'NZ NA Yuº | SZ —NZ NA | NZ NA 1NZ 1–NZ |NZ
yv-r-zv-T-Z- zS rvi-Tzv z\ | Arv Izv- zS rzw-I-Zw tº ſ
- T-I-I-I -
HD 198820 ||| ||||Wh | |
B3 ||
| \"\hw →–be-i-k-Hé-4→et-Hº-Hº-Hº-Hº-->4—e-Hº-be-->4—e
HD 134687 M WWW MW NW t
B3 IV
Jº Aſ NZ 1 NZ I NZ NA MA | NZ v. Y-Z | NZ NA 1 NZ | N/ I IN/ |
WN zV-T—Zvi zS J/N TzV- ZN | ZON |-zV-1 ZN I ZN | ZN I * -msmº,
|- | T
n Aur
B3V
|→él–º-4→6––24–1–24–24—24–94—->{—1–24–1–24—24–1–1->4—24–36–1–24–24—24–1–24–%— ZN

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1480 1500
31
Plate 13b
Fe III
T
A||||
[-
Fe ||
TTT
C IV
ſ
-
II-
TV


1500
1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
32
Luminosity Effects
at B5
Lines of Si II, Si III and Al III
are luminosity indicators for classes
III, IV, and V. In the supergiants,
the wind lines of C II, Si IV, C IV,
and Al III are in absorption.
Plate 14a
Si || Si || Si || C || Si IV Si ||
| TTTT | H |
| T | | T | I I I | I | I | U | I | I | U | I | I |
n CMa
B5 la | | ſ
M
Y!!!'ſ "...T. >4—K–Pé–H%——bé+->4—94"–H54–1–24–3—H·4–1–24 Bé–H54 }{-|->{ HK–H54 HK
-------|--|--|--|--|-m------|--|--|--|-
HD 2094.19
B5 || H
NA NZ_l Szu |NZ 1 NZ NZ | NA | NZ
ZN rzº—T-zs Izs-r-zº] rzs-T-Zw | zS
T Her
B5 IV
NA 1NZ | \Zu |NZ 1 NZ 1 NZ | NA | NZ
zS zV-T-Zw |zV-I-ZVI z \ | ZN | zS
p Aur |
B5 V
"A. 4–1–2é—%—->é——24–1–24—94–1–24–1–24–36–1–24–24—24–1–24–94—24:1–24–1–24—1–2%
1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

—º
Plate 14b
Si || ſ Fe II C || º | A|||| º
| I | l | I I I | I | I | I | lſ | I I I | I | I | I | I I I I I | I | I | W I
ſt-I-T- T-T
—l sz R2 | SA | Sº I | N/ | | N/ | NU/ | NJ’ | NA | N/ | | N/ | | N/ | Sz_l | SA l | \, | | NZ 1 | | NZ | | __
I-zs- Fºs I ^ I zs I TZN | IZN | AN | *N | /N | ZN. | —2%- | VN | Tzº | T-zs I ^ I Izs I | /N. I | IZN | TI I

><
-º-
—Hº-Hº-Hº-Hº-He H*—Hº-He-He —k—Hº-Hº-H-e-H->e H–3——Hº-Hºd—H-e-H->}—
—r-— -T-I-T-I-T-m-m-m-m-T-I-T-I-I-I-I-I-I-Hº-
—Hºe-Hºe-H4——º-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-H-e-H-4––Pe--Hél–H36–H–4—
-Yº v-Y Wy— I
-tº-m-m-m-m-m-m-m-m-I-T-r-ţ-T- F-ºr- r-m-- F-I-T-
— NZ | be | >é | 26 | | 2% | 12% | % | }< | >k | }< | % | 1->6 | | 26 | | ><- | >k | | 26 l | ><! | 1–2% | l >{ |
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
35
Part 2
Effects of Stellar Rotation
36
Plate 15a
Rotation Effects
at B0.5
* * e o C Si i
crº in # - am

these stars are photospheric. They
are broader and shallower in the --------|--|--|--|--|--|--|--|--|--|-r r—T-
rapid rotators HD 135160 and 6 Sco
than in the slow rotators HD 36960 A Lep
and A Lep. Both width and depth
must be taken into account in esti-
mating the strength of these lines for B0.5 IV
classification purposes. v sin i = 50 km/s
NZ 1 |->4–1–4–1–Y >4– NZ 1 \Z | NZ NA Yvº | \Z 1–Azil Yue | NZ NA 1NZ | \Z. |NZ.
zº—r-z-T-7s-1-ZvT-zºn }<- yv-r-zv-T-z-r-zº y \ Tzvi-r-zvi 2^N | Zs-r-zº rzw-T-ZS IzY
Ö SCO
B0.3 IV
y sin i = 180 km/s
NZ 1 \, NZ SZ — 4–1–Y >4—K 1 NZ | NZ NA \/ | \Z–1—Az Yua | NZ NA 1NZ_1–4. IN/
T-7s-1-2\ I-zvi zS VN 1 z\-T—Zvi zS yW Tzvi-i- ZN 2^N. I-7s- ZN rz-T-7s IZV
+--T-I-T-I-m-m-m-
HD 36960
B0.5 V
y sin i = 35 km/s
NZ 1 NZ | NZ NZ NZ I YZ L \Z NA 1NZ I-Azu IN/
VN I ZN ZN Tzvi-I-ZVI ATN I-zV- ZN rzv-T-zs |ZW
*
}<
HD 135160
B0.5 V
y sin i = 180 km/s
NZ 1 NZ | NZ NA NZ | NZ NZ | | NZ NA 1 NZ | NZ |NZ
/N ZN (320 1340 1860 & 1386 200 °1420° 1206 (i226 (240° 1260 ° 1260 Tisoo /N ZN
1440
Plate 15b

Hºd
Hºe-
He-H
Hº
%
}<
><
H
%
—l Sz ſ R2 l >é l Sz_l | >< | -->{ | 9% | }< | }< | }< | 9% | | N/ | I >< | _l ><!- | }< | | 2% _l | ><! | | >é | | >k
1 500 1 520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880
38
Rotation Effects
B1 - B1.5 Main Sequence
Unlike the photospheric and
stellar wind lines, the interstellar
lines are unaffected by rotation.
They are easily picked out in the
stellar spectra of rapid rotators HD
154445 and HD 37303 by their very
sharp profiles. Some lines, e.g. Si II
A1526, have both stellar ind inter-
stellar components.
Plate 16a
C || Si || Si || Si || Si IV
U | | I T | I | J | I | I | | | U | U | U | I | I |
HD 36959 |
B1 V
y sin i = 25 km/s
- NZ | >2 'l NZ SA \/ | Sz–1–szl NZ L NZ NA 1NZ I A2 |NZ 1 NZ I 1 NZ | NAſ | NZ
Prs z\-Tzvi zS J’N Tzs z\ | ArN I-zV- zS rzs I C- IzV--zVI z\- ZN Izs
HD 154445
B1 V
y sin i = 185 km/s |\
HD 35299
B1.5 V
v sin i = 35 km/s
HD 37303
B1.2 v |
y sin i = 240 km/s
w 94 –24–1–24– >4 × |→4—24. }< |→4— >4 24–1–24. Bé —24: |X— >4 | NZ

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
39
Plate 16b

—r-r-I-I-I-I-I-T-Y-L-T-I-I-I-I-I-I-I-I-I-m-T-I-T-I-m-
NZ NZ M.A. NL2 _l 1. NA’ | NA’ NA | NZ | | N.A. i | 1 \Z ſ J
| N/ | N/ NZ l | NZ | NZl | | N/ | Sk
×-H2–Hºe-He –––––be-Hº-H->e-H-e-He--He-Hºd—H->e-H->}—-
NZ
| N/
%
}{
ZN ZN |→-1–%— %—l—º- —e- —e- —k— |→e- —e | |->e-l——º i
1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
40
Rotation Effects
B1.5 - B2 Giants and Subgiants
Rotation effects tend to be less
pronounced for stars above the main
sequence, but they can produce
apparent differences in the signal-to-
noise ratio (S/N). Note that the in-
strumental S/N is about 30 for all
the digital plots in this Atlas.
o: Pyx
B1.5 ||
y sin i = 20 km/s
HD 70930
B1.5 ||
y sin i = 220 km/s
HD 39777
B2 IV
y sin i = 40 km/s
p Sco
B1.7 IV
y sin i = 155 km/s
1200
Plate 17a
C || Si || Si || Si || Si IV
| | TTTT - H
I | I | I I | I | TI | I | I | | I | I | I | I | I |
A NZ SZ | NZ SA YA | \Z–1–4 Yuº | NZ NA 1NZ || Azu |NZ NZ I 1 NZ I NAſ | NZ
WN ZN-T—ZS-T-zV J/N Tzvi-T-ZVI ArN | Zs ZN rzV-T-zV |zV-I-zVI z\-I /N | zS
|
Hº-Hº-Hº-Hé –3–2–1->4–H54–H54—) ("Hº-HºHé–H4–1–1->4—Bé–Hé-Bé–HºH)4–H54—Hº
|\ NZ NZ || NZ NA *4–1–1–4––4. Yuº | N/ NA 1NZ_1=>4. |NZ 1 NZ | 1 NZ | NAſ | NZ
PS /N-I ZS- zS yN Izs z\| ArS | zS zS rzº—T-7s |zY -zVI z\,-] ZN Tzv
| | NZ NZ | NZ NZ NZ l NZ NA NZ | NZ NZ I YA | NZ NA 1NZ | NZ |NZ 1 NZ 1 NZ I NA | NZ
/N ZN ZN /N ZN /N ZN ZN ZN ZN /N ZN ZN /N ZN ZN ZN ZN ZN ZN ZN ZN
1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500

Plate 17b 41

×—
Hº
}<
Hºt
Hº
Hºt
><—
Đé
Hé
He-
HA
Hº:
Hº-
H*
Hºd
Hº-Hºº-º-º-º-º-º-º-º-º-º-º-º-º-º-T
— »e H be -->4——º-Hº-H2—He-He-He He–He-H2–H–4–H–e1––––Hº-Hº-Hº-H-4–
– sº be-->4 —e- | Nº | Bé-l %—l }< | >k- | }é | %—l *— —e- Sz I l Sk l | S. |→e | 1 sº I 1–4 .
1 500 1 520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
42
Rotation Effects
B2.5 - B3 Subgiants
Line broadening can pose a less
severe problem for the classification
of the mid-B stars, where the stellar
wind is weak and the photospheric
Si II lines are not yet saturated. For
example, HD 150745, with a v sin i
of 285 km/s, is one of the fastest ro-
tators in this program, yet its spec-
trum is quite comparable to that of
the moderate rotator Ö Ori B.
Plate 182
C || Si || Si || Si || Si IV
TTTT H
U | | lſ | | U | I | I | | I | U I I I U | U | I I U |
Ö Ori B
B2.5 IV
y sin i = 35 km/s
N º NZ 1 NZ | NZ NA MA | NZ NZ | Y-Z LAZ 1 NA 1NZ | Sz. NZ —NZ! LNZ NA | NZ
\ VN z\-T-Zvi ZN yS I/S zSI ATN Izvi- ZN I /N | ZNT |ZN I zSI º | /N | zS
------------|--|--|--|-m-m-m-m-m-m-m-m-m-m-m-tº-
HD 150745
B2.5 IV
v sin i = 285 km/s
Aſ) NZ 1 NZ | NZ SA Yvº | NZ NZ | NA LAZ NA |SA-I-4- |NZ 1 \z I | >2 l NA | NZ
Prs TZN | ZN I zS Jyv TZN ZN I AN |-zv- zS IZN I ZN I |z\ I ZN | IZV | /N | zS
HD 134687
B3 IV
y sin i = 40 km/s
*4-x-->4–4–4–4–3–2–Hºe-4→e-P-->4–2–3–4–3–H54–B––4–3–H54–Hº
---T-Y-m-T-I-I-I-T-I-T-I-m-m-
T Tau
B3 IV
y sin i = 180 km/s
Aſ A T z bé –24–1–24– >4 % |→é >é! % |→4— >4 |X: | ><+ Bé l ><! HX | >é | NZ

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
Plate 18b
Al III Fe III
*— T- T
| I | | I I | W | | U I I- I W | U | I | ſ T I | I | I | U I I T | I
—m----|--|--|-m-m-m-m-m-m-m-m-m-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-ſ-
—Hºe-Hº-Hºd—-24– ×—H2−. He-Hº-Hº-Hº-H2–H–2– ×- —k——Hº Hºë—H->e-H–4–
--tº-r-ţ-T-I-I-T-Y-T-I-m-m-m-m-m-ſ-ſ-ſ-ſ-ſ-ſ-r-ţ-tº-m-
—Hº-Hºe >4——xe-H->e-H2— He-He-He-Hº-H2—H-e- ×- —k— Hº Hº!—H->e-H–4—
I– F-U-N-y—- -V
Fir-I-m-ſ-ſ-ſ- |
—Hº-Hº >4——º- ×-H*— He-Hº-Hei-Hºº-H2—H->e— ×- —k— Hºe Hº!—H->e-H–4—
——4––% >é——º- Hº-1–3——º-l–4–1–24–1–3——%—l—->e- >e- >{ |→ |→e——º-1-->4—

1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
44
Rotation Effects
B5 - B6 Giants and Subgiants
The spectrum of the late B stars
is dominated by lines of Si II, whose
relative strength is the principal
classification criterion. In order to
ensure that both depth and width of
the lines are accurately taken into
account, it is useful to have both
broad-lined and narrow- lined stan-
dard spectra.
Plate 193
Si || Si || Si || Si ||
| TTTT |
| | lſ | I | I | U | I | ſ | U | TI | I | I | U | I | I | I |
T Ori
B5 ||
v sin i = 45 km/s
o Cas
B5 ||
y sin i = 255 km/s
AVY'Ax, be-º-Hº-1-4—k-Hº-->4–*—Hº-Hºº-º-Hº-be-->H2-H2—Hº
-—t-m-m-T- -T-T r-i-m-m-m-
2 Lac
B6 IV
v sin i = 60 km/s |
*%+x+x+x+x—k—x–Hei-4—kº-Hº-->4–3—Ex-->4–ee-Hºº-ºº-->4–2–H54–Hº
-----|--|--|--|--|--|--|--|--|--|--|--|--|--|-rr-
23 Tau
B6 IV
~~~~r,
4Thºë-ºf-><– >é- >él >é % bé –24–1–24– >4 >< |→é——24 % |→4— >4 Bé——24. Bé —24! Bé—l >é |→é

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
Plate 190 45
Si || Fe || C | Al Il A|||| Fe ||

—H··m−1·ſ−trº-H- Twſ
><
|
><
Hº
}<
>{
24
>{
Bé
><
><
×
Hºe
26
º
×
\Zl |
| Sk
/NI | I ZN | I zł
>é
$é
}<
—%
He
+
bé
Hºč
Hºe-
Hº-
Hº-
He-
}
k,
>4
26
><
HP6
}<
>{
24
>{
Pé
><
><
+
×
H
Hº
><
Hº
×
|->e--be-i-4——º-l——º-l—º-l—%——3–
| NUZ | NZ | | N/ | | NZ | l & | J, | | Sz l | NZl | 1 NZ | l Sk |
ZN ZN ZN ZN ZN ZN ZN ZN
3%
1 soo 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
46
Plate 20a
Rotation Effects
B6 - B7 Giants
Many of the late B giant stan- º | # - º |
dards, including 16 Tau, 17 Tau, I U | U | lſ Uſ T I I I U U U U | I | U
and n Tau, are members of the Ple- | | | I | | | | | | |
iades cluster. This cluster is a par- -
ticularly good source of broad-lined
standards, although narrow-lined Ç Dra
stars are found there also.
B6 ||
v sin i = 30 km/s
Hº-Hº->4—%l-H4––2éHé–H4+-4—24–H54—Pé–H4–3—Hº-Hº
| T I- |
17 Tau
B6 ||
y sin i = 215 km/s
A MAT %—Pé—->{—Heli->4—94–H54–1–24–36–H4——24—126–H4+-Pé–H54—3–H54—Hº
20 Tau
B7 ||
y sin i = 45 km/s
| NA NZ | \Z. |NZ 1 NZ I 1 NZ | NAſ | NZ
r—zV-2N-I-2\, |zV-r-zVI z\ I-zw-T-zº
F-T -T-I-T-
n Tau
B7 ||
y sin i = 210 km/s
AMVMM. z NZ 1–2% | ><– NA NZ | NZ >é! YA | NZ >4 1 NZ | NZ |NZ ſ ><! |->< | >é |→é


1200 ºz26 1240° 260 ° 1280 isoo (320 1346 1360 ° 1386 200 1420° 1440 1260 ° 1480 ° 1506
Plate 200 47

-T-I-T-
| NA l Rz | SA | N/ | i__N/ | | N/ | NZ | NLZ | | NLZ MA | NA | N/ | Sz | | NA | NA' | | N/ | l S} |
T ZVTI I ZN I | TZ'N | I /N | y^N. | AN | —}<— | ATN | VN | +26 | | /N | | zS –H —k— I | ZN | | /NI | H26 | I I
| d | | | || || || |
| i
|
| Sz R2 NA sz | Sz ! NZ | NUZ | Nº | S.A. | | | IN/ | |->~! sº SA | Sz | Sz | I X- | l NZ |
|-ZS | PS I zS } | z-T IZN. | ZIN | /N | Zºn | >{ | —}<- | L^N. | Tzv | --~~ } zi ; T^ | | Z\TI | I ZN I ^ I
| Sz Rz | SA 1 & 1 & 1 Sz NZ | NLZ | NL’ | NZ | NZ | 1 Sz 1 so I 1 & | N. l | Sz_1 | Sz | 1 & | Sk l
/N ZN ZN /N ZN ZN ZN ZN ZN ZN ZN
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
49
Part 3
Stellar Wind Effects
5O
Plate 21 a
Stellar Wind Effects * sº # *
at BO - BO.5 ---T-T-I-T-prºnºv-ºf-wºrn

U Ori
BO V
Both U Ori and t Sco are MK
standards for type B0 V. In the ul- ><l— |->~1–4–1–sº
traviolet, however, t Sco exhibits |
zS-2's | zS
greatly enhanced lines of N V, | | | r-I-T-----------|--|--|--|--|--|-- ---T-
Si IV, and C IV. We use u Ori as
the standard for ultraviolet classifi- r sco | |W. J \||Nº||N|M||
cation at B0 V, while t Sco is desig- d
nated B0 VW, indicating that the º
stellar wind lines appear to be "ab- B0 Vw
normal" in comparison with the
standard. The two spectra of t Sco 1984 Jul 1 NA
presented here were taken over three 2 N.
><+-><!—24—k—#4 +*—H·4–1–4—º-Hº SA l Nueſ
years apart; there is no indication of | | | T |-|--|--|--|--|--|--|-- T-I-T-Y-r --~
R2
| | NA l l S2 | NU/ | NA |
Tzv | 7~-l N I zS Aſ N /N I
long-term variability in the stellar
wind, but variations on a shorter | U \ || || || ſ
time scale cannot be ruled out. * * || || | | | | || Wººl | | | | | ||
Walborn, Nichols-Bohlin, & Panek
(1985) also describe the enhanced BO VW
stellar wind features of t Sco,
which they classify as B0.2 V. 1987 Aug 18
Sz_1 \z || >z—sº-->4–
zs-r-zs-I-2s /N I
><
><
+2%
>4
><
PS
>4
TPS
F-ZS
Although it is a fl Cephei vari-
R. ><+
able, f Cru has a normal optical MK T | ſ | rin_T----|--|--|-- —-T- | | | m— T-I-T-I
type of B0.5 III and a normal ultra- |
violet spectrum. In contrast, HD f Cru \ t + M. W
53974, whose optical type is also
B0.5 III (Rountree Lesh 1968), was |
given the ultraviolet classification of B0.5 III |
B05 IIIw by Rountree & Sonneborn
(1991), who cited its broad stellar
wind lines and especially the P
Cygni profiles of NV and C IV. ––p-r T-T-I-T- | | rº-º-º-º-º-º-º-º-º-Hº- - - - −) -
HD 53974 º
BO.5 |||W
NA > A Sz Sz NA. I SA NLef KZ Sz | Sz SA NA | Sz S2 | Nue' | Sz SA 1 NA | NZ 1 |Sz | Sz | N/ | NA | Sz
ZN 2N 2^N. 2^N. z \ 2^N. ZN 2^N. 2 N 2^N. ZN 2^N. 2^N. 7 S. 2 N 2N 2^ 2N ZN 2N 2^ ZN
12OO 122O 1240 1260 128O 1300 132O 1340 1360 1380 1400 142O 1440 1460 1480 15OO
51
Plate 21b
A||||
N IV
He ||
C IV

~
ſ
|
----
|
I-m-m-ſ-ſ-ſ
T
r—-tº-T—w-T-I-m-m-n
IT-I
II-
><—
-T
|
T
1500
1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
52
Plate 22a
Stellar Wind Effects * * # *

I | T I | I I I | W I I | W | I | I | W | I | I | I | I |
at B1
O Per
B1 III
The MK standard for B1 III is
o Per; o Sco is a fl Cephei variable >< *H*——º-><!-->4—k—Pé–H54–Hº-Hºd—4–Hºº--><Hé–H54––4—Pé–Hº-Pé–HºH ><–H-4—Hº
and a spectroscopic binary, but at | N | | N | | | zS | | |
classification dispersion both its op-
tical and its ultraviolet spectra are
normal for B1 III. However 1
--~~~~~ CMa
& CMa, another 6 Cephei variable, &
is classified B1 IIIw because of the |
P Cygni profiles of the N V and B1 Illw
C IV lines, and the weakness of the
Si IV absorption lines. Rountree NJ’ 1 | >2–1 ><– NA I SA NLeº R2 | | | SA NJef H-4- S.2 | NU/ | | SA *—l—- Pé I S2 | HP6 | Nueſ | Sz
and Sonneborn (1991) cite evidence zº—2-T-2s I-2sr−. as—Ps—-2s—T-2-1-2- rS-I-2S zSI as H-2-1-2S rzº—I-2s | zS] I-2s |-z's
for a variable stellar wind in this
Star.
Grady, Bjorkman, and Snow or Sco
(1987) describe 2 Vul as a Be star
with a variable wind and a partially
resolved discrete absorption compo- B1 ||
nent. In the example displayed here,
the C IV doublet is greatly enhanced Sz". Sz_1^2–1–1–4–sz | > | > −4—2–1–4–4–4–1–2 – S4 Sz—1–4– Bez—Szl_i > 1–sº | Sz
in comparison with the normal spec- ~–~–T-7--~ 2sr−2T→r-P---|--|--|--|--|-2sr−1s− r^-I-2s 2N–1–2s. | 2N–I-2N-I-2s
trum of HD 63578. The latter star is d
a rapid rotator (vsin i = 200 km/s).
HD 63578
B1 IV "A
1 \\A | NA NA I NL^ | N/ NZ | YA | NZ Yue' NZ 1 1 Nº NZ 1 | | Neº 1 N-Z Nef
2^N. ITZN | 2^NTI ><- z N I >4 /TN Pé Tzv ZNTI >4 Jº N 2 N I >< Aſ N | /N T >4 IZN. ZN I Prs I >< ITZN | /N | ZN
2 Vul
B1 |VVV "A
|\! >4–4–1–24–34—we Bé-->4——4––4—94–1->4––Pél–36–1–4–4–4–e4–1–24–94—ººl—eº-I->é——º
12OO 122O 1240 126O 128O 13OO 132O 1340 1360 1380 14OO 142O 1440 1460 1480 15OO
53
Plate 22b
>é
}<
+
26
+
><
Fºs
>{
24
>{
Bé
><
+
|→e--be-i-4–4–3–1–––. | | So I
| Sz
! SA NA | 1NZ | NUZ | NJ’ NA N/ | | N/ | | \Z | 1. sz SA ! | Sz I | NA' | | 1 NZ | | Szl |
I-A U Fº I ^ I ^T TZN | IZN | ATN | ZN ZN | ZN Hº– VN | I ZN | -zs- | ^ I |^ I | ZN I | TZN | I ^I I
—t-m-m-m-T-I-T-I-I-I-I-I-I-T-I-T-I-I-I-II-I-I-I-I-
NZ | NZ l SA Sz I | N/ I NA | NL’ | NJ’ NA/ NZ | | N/ | I NA/ | I | S, I NJe. I | NZ | s/l |
| ZNTU Pé I ^ I ^ - Tzvi | IZN | ZIN | Z\ | 24 | ZY | —%– VN | I ZV | I ×– T >{ I Izs I | z \ I | I /N I I ^ I
|
Sz I
ZN
ZN ZN zºN
9%
1 S. 1 N. L
ZN
NZl | _1 \Z | l
ZN

1500 1520 1540
1560 1580 1600 1620 1640 1660 1680
1840 1860 1880 1900
1820
1740
1700 1720
1760 1780 1800
54
Stellar Wind Effects
at B1.5
HD 85871 and HD 166596
have anomalously strong C IV lines,
in comparison with the normal
B1.5 III spectrum of HD 70930.
The Si IV lines have peculiar pro-
files, in addition to enhanced line
strength.
The C IV lines, normally absent
at B1.5 V, are prominent in the spec-
trum of 19 Mon. Grady, Bjorkman,
& Snow (1987) describe this star as
having a variable stellar wind.
Emission at Ho is cited by Irvine
(1975) and Hirata & Asada (1976).
HD 7093O
B1.5 ||
HD 85871
B1.5 |||W
HD 166596
B1.5 |||W
HD 35299
B1.5 V
19 MOn
B1.5 VVV
Plate 23a
f ||| º | Si || º Si IV
l | I | I | I | I | I | I | I | l | | I T I | I | I | I |
|
NA. W. 1 | 1 Sz Neº 1 NA NLef R2 | Sz_l Sz SA NA | 1 Sz NUZ | Sz SA I NA | Nº 1 |\,. I NZ | I NA | | Sz
2^N. I ZN | ZN I /N | /N I zS 2TN Prs TZN | 2^NTI zS P^N. I 2^ I zS 2^N. | 2^N. zS I 2 N. | Z STI Izs I zSI I / N | /N | ZN
}<!--Sk—Hº-Hº-Hºë—4—k—Pé–H54–H54–1–24—k—Hº-Hº-Hé–H54 >4—Pé–Hº-Pé–HºHº-Hº-Hº
ſº Hº-Hº-Hºë—24—k—Bé-->4–H54–1–24—º-Hº-Hº-Hé—Hº-Hºd—Pé-Hºë—Pé–HºHº-Hºd—Hº
ſ Rz 1 Sz 'l Sz. 1 SA Y/ | Sz Sz NUZ | Sz SA 1S2–1–2– IS2 1 Nz I Sz NAſ | Sz
Prs TZN | /N I zS J’N | ZN I zS ATN | ZN zS I ZN | ZN I |^ I zS I ZN | ZN | ZN
NZ 1 | Sz Sz | Sz SA N/ Rz 1 >2 l Sz SA NZ | Sz Szl NU/ | Sz SA 1S2 | Sz lsz | NZ | Sz NAſ | Sz
ZN 2^N. ZN /N ZN ZN ZN 2^N. TZN ZN ZN /N ZN ZN ZN ZN /N ZN ZN ZN /N ZN /N
122O 
12OO
1240
126O 128O 13OO 132O 1340 1360 1380 1400 142O 1440 1460 1480 15OO
Plate 23b 55

| I | I | I |
m-m-m-m-ſ-ſ-ſ-ſ-ſ
rº-H-I-T-I-T-I-T-I-I-T-Y-H-I-T-I-
26
Bé
}<
#
}<
F-
TI-
T-
HPé
96
NUZ
|
}<
NZ
Hº
><
26
><
><!
*—
H
+
|→e--be-->4——º-l—e-Hee-i-º-He-l–k—l
|→e-l—ee-H->{-1–––––.k——->e--->4—1––––––
}<
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900
56
Plate 24a
Stellar Wind Effects sº º | I mº *
B2 Dwarfs -----|--|--|--|--|--|--|--|--|--|--|--|--|--|--|-m-
13 SCO
B2 V
The ultraviolet spectrum of
13 Sco is normal for a rapidly rotat- →3'→4–4–24–1–2– +:
ing B2 V star (v sin i = 225 km/s). -
| NA | SA | N/ | NA I ls, | NA | NAſ
T^N | | z STI zS I /N | ZNTI |^ ZN | ZN | 2^N.
In particular, the C IV lines are van- | | I----- | | +----|--|--|--|--|--|--|--
NA | NA
2^N.
NLZ Sz–1–4– SA NA | >2 Sz NU/
2TN 7~-I zS PN | z I | 2TV
Sz |
N /N I / |
| SA
I zS N
I
ishingly weak. The other B2 dwarfs
depicted here exhibit different de- HD 3701 7
grees of C IV enhancement. The
choppiness of the spectra of HD |
57150 and HD 161056, due to a B2 Vw
poor echelle ripple correction in the
data processing, makes precise clas-
sification difficult. zs-r-zs-
NZ I SA NZ | | NZ l SA
PS | zS-I zS J’N | | ZN I zS
--- - --> l - * - -
Shore & Brown (1990) reported Y-- H-H - | | d T | I-m-m- —I- T-I-T-I-T- -mſ-TI-
C IV and Si IV line variations in HD
37017. Balmer line emission in HD 57150
HD 57150 and HD 72067 has been
described by Slettebak (1982).
B2 VW:
NA | 1 |→-->4–1—- SA NZ KZ Sz Sz | —sz YUZ | | sº-Hº- |Sz | S2 | Sz NJT | N/
Z S I-2-I-2s I zS /NTI zS- 2IN PS TZN | zS-I zS J’N Izs I zS ACN |-zs- zS I ZN | ZN I |zs I zS TZN | ZY |-z-S
{- --|--|--|--|--|--|--|--|-- T----|--|--
HD 72O67 W *.
B2 VVV
><!-->44–4––24-Hº->4—k—Bé-->4––––54—k"—Hº-Hº-Hº-Hº-Hºd—º- |--→4–1–2%
- --- --- —ſ *T*Tº-s— —ir--------
--tº-T-I-T-Y-r --I-y F-T- | | | | |
HD 1615O6 wº
i
{
| r
B2:VV |
"...l 1 S2 Neº i SA NZ Rz Sz S2 SA Y/ | Sz Sz NLZ | Sz SA | N/ | NA I ls, I NZ 1 NA | NA | Sz
2^N. 2^N. ZN ZN /N ZN ZN ZN 2^N. 2^N. 2^N ZN 2^ ZTS 2^N. ZN ZN ZN ZN 2^N 2 N 2^N.

12OO 122O 1240 1260 128O 13OO 132O 1340 1360 1380 1400 142O 1440 1460 1480 15OO
57
Plate 24b
C IV A| ||
H–I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I-I I-
Hº-Hº-Hºd——x–H–3–H54—Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hºd—H->e-H->{–

| NZ l |\, _l
ZN
>é
|
l
Sz I
| NZ
ZN
| NZ R. SA I NZ º | N/ | | N/ | | NJ’ | NA NA’ | |
NZ 1–4
^- r—zº ſ
|
| Sz
l
N/ SA | < | Sz | N/ | | | | MA | | Sz_l NZ | NZ | I | < | | NZ I | 1 & | Sk |
I-7s l Fº I ^ I ^-I Tzv | IZN | Pé | }< | }<– | }< | VN | I /\ | Tzv | | ^T + —k— I-7s I | /NI | Tzv | I zł I
Hº-Hº-Hºd——x-H-e-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-Hº-H-4––Pei--|->e—H·e-H–24—
NZ | 1 sº | | | \, . | Sz | usz 1–szl |
VN | zº- l zS I | z \TI | TZN | I ^ I
1 N.A | l J. |
|-}=1–3—1–*—l—k——%—l
Sz 1 \, . I
ZN
ZN ×–1–––
1500 1520 1540
1860 1880 1900
1
1840
560
1820
1580
1800
1600 1620 1640 1660 1680 1700
1760 1780
1720 1740
58 Plate 25a
Stellar Wind Effects º Fº Si || hº *

I | I I | I | I | I | U | I | I | I | I | I | I | I | I |
The B2 Subgiant Ç Cas —t-m-m-
Ö Cet
B2 IV
The fl Cephei variable 6 Cet has
a normal ultraviolet spectrum for a l | >2 – 2 | Sz SA NLZ Rz Sz—l sz– SA Yue' | >2 Sz Nue' | Sz SA Sz—l—sz- |Sz l S2 | | >2 l | Sz
I 2 N | /N I /N | ZNT zS 2TV Prs TZN | zºv I zS J’N | ZN I zS I 2^ | ZTS I zS Tz N | 2^N. I |^ I zS I ºf N | 2N. | 2 N
B2 V slow rotator (v sin i = 10
km/s). The N V lines are absent, | | | | H-I-T-I-T-I-T-I-T- | T
Si IV lines are moderately strong,
and C IV is very weak. In C. Cas,
which is not a 6 Cephei variable, the
wind lines are all enhanced and are
variable in strength. This variation B2 IVw
Ç Cas
is especially remarkable in the CIV
lines. Sonneborn, Garhart, and 1982 Sep 7
e l |→4–1–4–1–sº SA ->|<- KZ Sz I Sz. 1 SA NA |->4–1–sz Nue' | Sz SA Sz_1=z- lsz 1 Sz | Sz NAſ | Sz
Grady (1987) set an upper limit of →-T-7s-1-2s /NT zS PS r-z-T-zs zS PTN Izs- zS ACN |-zS- zS TZN | ZN I |z S I zSI I ZN | ZN |-zS
several months for the time scale of | | | | | | | | | | | s
the wind variability in this star.
HD 163472 (B2 IVW) has an Ç Cas
ultraviolet spectrum very similar to
Ç Cas. Its potential variability has
not been studied. B2 |VW
1982 Nov 25 | | |
>Al-Hº-Hº-Hº-Hºë—4—k—Pé–H54–H54–1–24–36–H4––PéHé—Hº-Hºd—Pé–Hº-Pé——24–24–H54—Hº
Ç Cas
B2 IVW
1983 Oct 2
| | > 1–2–1–sz SA ->|<– Rz l | NZ N/ | >2 Szl | Sz I NA | Sz ls, | Sz | Sz | NAſ | Sz
ZN I ZN | ZNTI zS I /NT zS PS I / N I ZNTI zS J’N Izs I zS ACN | ZN T zS I/N | ZN I |^ I zS TZN | ZN | /N
Ç Cas
B2 (VW
1934 Feb 12 ^
º º º N | | Sz. 1 SA NZ | Sz Sz | Nº | Sz. 1 SA 1S2 | Sz |Sz 1. Szl Sz | NA | Sz
ZN ZN ZN ZN /N ZN /N ZN ZN 2 N ZN ZN ZN ZN /N /N
12OO 122O 1240 1260 128O 13OO 132O 1340 1360 1380 1400 142O 1440 1460 1480 15OO
59
Plate 250
A| ||
C IV

ſæTSZ-}-*- ţ-*--*- †-X
- –==-e-） →«-， -ę•）
）—«æ， ae«）， →
T U ）-r- （>=）�'） ）;├─TĒ=+— !=–”Tº !== --•■
|} }X | k !* !*
}）×|-SKSKŠK|-Sk
X|-XE-XX|-X
）|-z-|-+!+|+
T !=–-r-• •†�■ ■ ■•）
）|ºg5ºTºgºTºgº5k
XXXKX*
）;–||–||–—— | —•） →«） →•）
►X|X|XXX
====~）
ſæ,= ==）«■■|• → →–f– P →æ：
XXX|*
>）•====
-
1900
60
Stellar Wind Effects
Mid-B Dwarfs
HD 192685 is essentially iden-
tical with the B2.5 V standard
o Sgr, except for the abnormal
profiles of the Si IV lines and the
abnormal strength of the C IV
doublet. In HD 72356, all the stellar
wind lines are enhenced in compari-
son with the B4 V standard HD
20809.
Plate 26a
C || Si || Si || Si || Si IV
| | TTTT H
I | | I | I | I | I | I | I |-r | I | I | | | I | I | I |
o Sgr
B2.5 V
>é!-->4+H=4––2é–H4+->4—3–54–1->4—H·k——4—%—Hº-HºHé–H54——24—1%—Hº!—Pé——*H*—Hº-Hº
HD 192685 f
B2.5 VW
>éHº-Hº-Hº-Hºë— 4—3–94—1->4–H54–1–24—%—H·4––PéHé–H54——34—Bé–H4+->é–H4H2—H24—Hº
HD 20809
B4 V
ALſ "TM' NZ 1 NZ | NZ NA Y/ | NZ NZ | NA | NZ NA 1 NZ | N/ 1 |NZ | NZ | 1 NZ I NAſ | NZ
VN rizV-Tzvi ZN J/N Tzvi-r-zVI ATN Izs- ZN rzw-T—ZN LV-I-ZVI rzV- /N | z\
—Y-
HD 72356
B4 VW
"W.M.A.J Z % 94 1–2% H-54– >4 × 1-1-X— ×l % |→4— >4 Lé | ><l Bé | ><! 1-4 | 24 |->{

1200 1220 1240 1260 1280 1300 1320 1340 1360 1380 1400 1420 1440 1460 1480 1500
Plate 260 61

><
*
>4
><
><
+
H26
%
}<
}<
}<
Pé
Hº
><
><
><
><;
><
+
t
+
NZł
26
><
| –
-T-
.
TIT
Fº
W|
*
| [ . . .
|-><--be-->4–1–2–––2–1–9–1–3–1—º-->4——d-1–%—l–%—l—->e-l——º-H4—12––––––Be-1––24—
1500 1520 1540 1560 1580 1600 1620 1640 1660 1680 1700 1720 1740 1760 1780 1800 1820 1840 1860 1880 1900

|||
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RE PORT DOC U M E N TAT I O N P A GE | OMB No. 0704-0188
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1. AGENCY USE ONLY (Leave blank) || 2. REPORT DATE 3. REPORT TYPE AND DATES COVERED
August 1993 Reference Publication
4. TITLE AND SUBTITLE 5. FUNDING NUMBERS
Spectral Classification With the International Ultraviolet Explorer:
An Atlas of B-Type Spectra
6. AUTHOR(S) 680
Janet Rountree and George Sonneborn
7. PERFORMING ORGANIZATION NAME(s) AND ADDRESS (ES) - 8. PEFORMING ORGANIZATION
REPORT NUMBER
Goddard Space Flight Center
Greenbelt, Maryland 20771 93B00096
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ADGENCY REPORT NUMBER
National Aeronautics and Space Administration
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11. SUPPLEMENTARY NOTES
Rountree and Sonneborn: Goddard Space Flight Center, Greenbelt, Maryland 20771
12a. DISTRIBUTION / AVAILABILITY STATMENT 12b. DISTRIBUTION CODE
Unclassified - Unlimited
Subject Category 90
13. ABSTRACT (Maximum 200 words)
New Criteria for the spectral classification of B stars in the ultraviolet show that photospheric absorption lines in the
1200-1900A wavelength region can be used to classify the spectra of B-type dwarfs, subgiants, and giants on a two-
dimensional system consistent with the optical MK system. This atlas illustrates a large number of such spectra at
the scale used for classification. These spectra provide a dense matrix of standard Stars, and also show the effects of
rapid stellar rotation and stellar winds on the spectra and their classification. The observational material consists of
high-dispersion spectra from the International Ultraviolet Explorer archives, resampled to a resolution of 0.25A,
uniformly normalized, and plotted at 10A/cm. The atlas displays such spectra for about 100 stars, arranged in
spectral-type, luminosity, and rotational velocity sequences. The atlas should be useful for the classification of other
IUE high-dispersion spectra, especially for stars that have not been observed in the optical.
14. SUBJECT TERMS 15. NUMBER OF PAGES
65
IUE; B-type stars; stellar classification; stellar rotation; stellar winds 16. PRICE CODE
17. SECURITY CLASSIFICATION | 18. SECURITY CLASSIFICATION 19. SECURITY CLASSIFICATION 20. LIMITATION OF ABSTRACT
OF REPORT OF THIS PAGE OF ABSTRACT UL
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