Observations of H??, iron, and oxygen lines in B, Be, and shell stars

Abstract

We have carried out a spectroscopic survey of several B, Be, and shell stars in optical and near-infrared regions. Line profiles of the Hα line and of selected Fe II and O I lines are presented.

Full text

arXiv:astro-ph/0512619v1 27 Dec 2005
Astronomy & Astrophysics
manuscript no. beir9101 February 3, 2008
(DOI: will be inserted by hand later)
Observations of Hα, iron, and oxygen lines in B, Be, and shell
stars
S. M. Saad1,2, J. Kub´at1, D. Korˇc´akov´a1, P. Koubsk´y1, P. ˇ
Skoda1, M. ˇ
Slechta1, A. Kawka1, A. Budoviˇcov´a1,
V. Votruba3,1, L. ˇ
Sarounov´a1, M. I. Nouh2
1Astronomick´y ´ustav, Akademie vˇed ˇ
Cesk´e republiky, CZ-251 65 Ondˇrejov, Czech Republic
2National Research Institute of Astronomy and Geophysics, 11421 Helwan, Cairo, Egypt
3´
Ustav teoretick´e fyziky a astrofyziky PˇrF MU, Kotl´aˇrsk´a 2, CZ-611 37 Brno, Czech Republic
Received 23 August 2004 / Accepted 21 December 2005
Abstract. We have carried out a spectroscopic survey of several B,Be, and shell stars in optical and near-infrared regions.
Line profiles of the Hαline and of selected Fe II and O Ilines are presented.
Key words. Stars: Be – line: profiles
1. Introduction
Observations of B, Be, and shell stars in different spectral re-
gions are important for putting constraints on modeling these
stars. Echelle spectrographs as well as the high sensitivity of
modern detectors in the red part of the spectrum provide a
wealth of the information contained in the whole visible and
near infrared regions obtained simultaneously. The aim of this
paper is a spectroscopic survey of line profiles of Hαand se-
lected non-hydrogenic lines of iron and oxygen in the visual
and near infrared region for selected bright B and Be stars. We
mainly use the echelle observations secured using the HEROS
(Heidelberg Extended Range Optical Spectrograph) spectro-
graph attached to the Ondˇrejov 2m telescope supplemented by
several CCD coud´e spectra.
2. Observations and data reduction
The present data are based on new spectroscopic observations
of 13 Bstars, 28 Be stars, and 8 shell stars. Our sample of stars
contains objects of spectral types B0 – B9.5 and luminosity
classes III, IV and V. Table 1 summarises the basic informa-
tion about the observed objects, their HD and HR no’s, their
name (if available), MK spectral type, luminosity class, and
Julian dates of the observations. Some of these stars have never
been observed before (to the best of our knowledge) in the
near-infrared region. The spectra of these stars were obtained
between January 2001 and November 2003 using the fiber-
fed echelle spectrograph HEROS (for a brief description see
ˇ
Stefl & Rivinius 2000, ˇ
Skoda & ˇ
Slechta 2002a) attached to the
Cassegrain focus of the 2m telescope at Ondˇrejov Observatory.
Send offprint requests to: J. Kub´at,
e-mail: kubat@sunstel.asu.cas.cz
All the basic data reduction processing, including bias subtrac-
tion, flat fielding, and wavelength calibration, have been done
using the HEROS pipeline written by O. Stahl and A. Kaufer
as an extension of basic MIDAS echelle context (see Stahl et
al 1995, also ˇ
Skoda & ˇ
Slechta 2002b). Additional observations
of several stars were secured using a CCD detector of a coud´e
spectrograph of the same telescope (ˇ
Slechta & ˇ
Skoda 2002)
and the data were reduced by the IRAF package.
3. Observed lines
3.1. The hydrogen Hαline
The Hαline in the stars of our sample was found to be either
in absorption or in emission, however,an intermediate case be-
tween emission and absorption was also found. Our set of stars
exhibits basically five different shapes of Hαline. We introduce
corresponding stellar subclasses for our sample, namely
i. Emission is present, but it is completely below the contin-
uum level. We will denote this subclass as AbEm (absorp-
tion with emission).
ii. The absorption part is below the level of continuum while
the emission peak is above the continuum. The ratio of
these two parts often varies at different phases for the same
star. We will denote this subclass as EmAb (emission with
absorption).
iii. The whole emission feature is completely above the con-
tinuum level. They will be denoted by Em (pure emission).
iv. We may also define the shell stars characterised by ex-
tremely sharp Hαabsorption cores as one of the Be star
phases. Since there is no intrinsic difference between Be
and shell stars, we denoted them by Sh. Besides the shape
of the Hαemission line profile, the presence of other sharp

2 S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars
Table 1. List of the B and Be stars in our sample. References to the spectral type are denoted by superscript numbers in paren-
theses, and the values of Teff are from Theodossiou & Danezis (1991).
HD HR Name Sp. Type Teff JD–24 00 000 JD–24 00 000 Shape
22780 1113 B6V(1) 12915 ±393 53217.5656 53217.5434 AbEm
23302 1142 17 Tau B6III(1) 13810 ±383 52619.9573 AbEm
36408B 1847B B7IV(4) 12940 ±1230 52721.8196 AbEm
217675 8762 o And B6III(1) 13810 ±383 51779.0595 AbEm
144 7 10 Cas B9III(1) 10700 ±385 52931.3284 53204.5171 EmAb
6811 335 φAnd B7III(1) 12940 ±1230 52566.8285 EmAb
58050 2817 OT Gem B2V(1) 22400 ±1393 52697.9049 EmAb
58715 2845 βCMi B8Vn(1) 12120 ±623 52620.0981 EmAb
164447 6720 V974 Her B8Vn(1) 12120 ±623 53215.4018 53215.4485 EmAb
171780 6984 B6V(1) 15310 ±750 53070.6629 53182.4968 EmAb
200310 8053 60 Cyg B1V(1) 25570 ±3652 52567.9192 EmAb
205021 8238 βCep B2III(5) 22160 ±1145 52113.0762 EmAb
216200 8690 V360 Lac B3III(2) 18445 ±1426 52527.0736 EmAb
4180 193 o Cas B5III(1) 15310 ±750 52694.8389 Em
5394 264 γCas B0.5IV(1) 30025 ±2160 52682.7532 Em
10516 496 φPer B1.5(V:)e-sh(2) 25570 ±3652 52465.0435 Em
18552 894 B7IVe(2) 12120 ±623 51954.7961 Em
22192 1087 ψPer B3IIIe-sh(2) 15310 ±750 53216.5315 53216.4905 Em
23630 1165 ηTau B7IIIe(2) 12940 ±1230 52648.8068 Em
29866 1500 B7IV(1) 12120 ±623 52526.1050 Em
109387 4787 κDra B5IIIe(2) 15310 ±750 52720.9752 Em
175863 BD+59 1929 B4Ve (3) 17100 ±386 53182.4428 53182.4642 Em
193911 7789 25 Vul B6IVe(2) 14340 ±570 52525.9284 Em
200120 8047 59 Cyg B1Ve(2) 25340 ±2164 51795.9049 Em
203467 8171 6 Cep B2.5Ve(2) 18445 ±1426 52721.0674 Em
206773 BD+57◦2374 B0V:pe(5) 29230 ±208 52484.0447 Em
217891 8773 βPsc B5Ve(2) 15310 ±750 53216.5717 53216.5525 Em
EE Cep B5:neβ(13) 53217.5020 53217.4567 Em
23862 1180 28 Tau B8(V:)e-sh(2) 12120 ±623 51797.0884 Sh
37202 1910 ζTau B1IVe-sh(2) 25570 ±3652 51897.9234 Sh
50658 2568 ψ9Aur B6IV(2) 12300 ±945 52721.9337 Sh
142926 5938 4 Her B7IVe-sh(2) 12300 ±945 52488.8992 Sh
162732 6664 88 Her B7Vn(1) 12915 ±393 53217.4040 53217.4229 Sh
171406 6971 V532 Lyr B5V(1) 17100 ±386 53182.3954 53182.4168 Sh
179343 BD+02◦3815 B9V(1) 10580 ±373 53216.4505 53216.4034 Sh
217050 8731 EW Lac B3IVe-sh(2) 18445 ±1426 53217.3848 53217.3731 Sh
358 15 αAnd B9p(11) 10700 ±385 51779.1187 Ab
886 39 γPeg B2IV(3) 22400 ±1393 51771.0511 Ab
23873 BD+23◦561 B9.5V(12) 10340 ±465 52651.0012 Ab
24760 1220 ǫPer B0.5V(5) 30000 52648.7495 Ab
34759 1749 ρAur B3V(7) 15310 ±750 52351.9306 Ab
36408 1847A B7III(4) 12940 ±1230 52720.8740 Ab
44743 2294 βCMa B1II/III(5) 26105 ±1779 52720.7954 Ab
87901 3982 αLeo B7Vn(6) 12120 ±623 51925.0219 Ab
120315 5191 ηUMa B3V(7) 18445 ±1426 52618.2262 Ab
138749 5778 θCrB B6Vn(1) 14340 ±570 52693.1422 Ab
155763 6396 ζDra B7III(8) 13810 ±383 52002.1433 Ab
160762 6588 ιHer B3V SB(9) 18445 ±1426 51787.9064 Ab
164852 6738 96 Her B3IV(10) 18445 ±1426 52722.1490 Ab
References:
(1) – Jaschek et al. (1980); (2) – Slettebak (1982); (3) – SIMBAD; (4) – Levato (1975); (5) – Morgan et al. (1955); (6) – Murphy

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars 3
photospheric absorption lines which will be referred to as
“shell lines” were also used for defining this subgroup.
v. The last subclass consists of normal Bstars with Hαab-
sorption lines. They are included in our analysis as a kind
of standard star. We denote them by Ab.
Our five subclasses represent a qualitative estimate of the
Hαline profile in our present observations. Table 1 lists the
stars according to these subclasses.
3.2. Non-hydrogen emission lines
There is a number of non-hydrogen emission lines in the spec-
tra of Be stars. The most striking emission features are pro-
duced by iron, helium, and oxygen. In addition to the hydrogen
lines, these non-hydrogenic lines carry supplementary informa-
tion coming from different regions of the stellar envelope de-
pending on their depth of formation.
3.2.1. Iron lines
Iron lines bring a lot of information from the circumstellar en-
velope depending on their depth of formation. They are often
present in the spectra of Be stars. An interesting fact about Fe II
lines is that they appear in the emission spectrum, however,
in the approximate theoretical spectrum, which was calculated
under the simplified assumption of a LTE static plane-parallel
atmosphere, they are completely missing. This indicates that
the excitation mechanism is connected more probably with the
atomic structure of Fe II and the corresponding NLTE pump-
ing than with some global density changes or even iron over-
abundance. However, such a conclusion is to be verified by
detailed NLTE calculations. We selected several strong lines
mostly from the quartet system for our measurements.
Although the list of available Fe II lines is quite long, only
several of them are useful for further analysis, in particular the
4233 ˚
A line from the multiplet (27), the 4584 ˚
A line from the
multiplet (38), 6148 and 6456 ˚
A lines from the multiplet (74),
and 7516 and 7712 ˚
A lines from the multiplet (73). Note that
the 6148 ˚
A line itself is a blend of two neighbouring Fe II lines.
Due to its vicinity to the Hαline the Fe II 6456 ˚
A line was
present in the Hαspectrograms that were obtained with the
CCD coud´e camera.
The near-infrared line Fe II 7712 ˚
A was severely contami-
nated by telluric lines in the band 7600 – 7700 ˚
A. However, this
line was sometimes strong enough to be measurable in 13 stars
of our sample. In ten of them the line was in emission. Other
Fe II lines, namely the 7516, 6456, and 6148 ˚
A lines are also in
emission. However, another Fe II line, which is not listed in the
multiplet tables of Moore (1972), appeared to be quite strong
in the synthetic spectra and may be possibly misidentified with
the Fe II 7516 ˚
A line. This line has a wavelength of 7513.162 ˚
A
and arises from the transition 5s e 6De
9/2→5p w 6Po
7/2. For
simplicity we will identify this feature with the wavelength
7516 ˚
A in the figures. In most cases the iron line Fe II 6516 ˚
A
was not detectable due to the huge number of telluric lines.
Table 2. List presented Fe II line profiles. For all stars the Hα
and O I7772−5˚
A lines are presented as well.
Star
4233
4584
5169
5235
5317
5363
6432
6456
7462
7516
7712
HR 1847B + + +
o And + + +
10 Cas +
φAnd + +
βCMi + + + + +
V974 Her +
o Cas + + + + + + +
γCas + + + + + + +
φPer + + + + + + +
HR 894 + + +
ψPer + + +
HR 1500 + + +
κDra + + + + + + + + +
HD 175863 + +
25 Vul + + +
59 Cyg + +
6 Cep + + + + + + + +
HD 206773 + +
βPsc + +
EE Cep + +
28 Tau + + + + + + +
ζTau + + + + + + +
4 Her + + + + + +
88 Her + +
HD 179343 +
EW Lac + + +
HD 23873 +
ρAur + + +
βCMa +
αLeo +
ηUMa +
θCrB +
ζDra + + + + + +
ιHer + + +
3.2.2. The oxygen infrared triplet O I7772−5˚
A
The most dominant oxygen line in the visible and near infrared
spectra of Be stars is the near IR triplet line at 7772, 7774,
7775 ˚
A emerging from the transition 3s5So→3p5P. Other
transitions between quintet levels which fall into the visual re-
gion are missing in the spectra.
4. Description of the online material
Results of our observations are plotted in the online Appendix.
It contains an atlas of the individual line profiles sorted and
ordered according to the Table 1. For each star, the Hαand
OI7772−5˚
A lines are plotted. Iron lines are plotted for each
observation where they were available. The list of Fe II lines
presented is listed in the Table 2.
Acknowledgements. This research has made use of the NASA’s
Astrophysics Data System Abstract Service (Kurtz et al. 2000,
Eichhorn et al. 2000, Accomazzi et al. 2000, Grant et al. 2000).
Our work was supported by grants of the Grant Agency of the

4 S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars
Czech Republic 205/02/0445 and 102/02/1000. Astronomical Institute
Ondˇrejov is supported by a project Z10030501.
References
Accomazzi, A., Eichhorn, G., Kurtz, M. J., Grant, C. S., & Murray, S.
S. 2000, A&AS 143, 85
Cowley, A. Cowley, C., Jaschek, M., & Jaschek, C. 1969, AJ, 74, 375.
Eichhorn, G., Kurtz, M. J., Accomazzi, A., Grant, C. S., & Murray, S.
S. 2000, A&AS, 143, 61
Grant, C. S., Accomazzi, A., Eichhorn, G., Kurtz, M. J., & Murray, S.
S. 2000, A&AS 143, 111
Herbig, G. H. 1960, ApJ 131, 632
Jaschek, M., Hubert-Delplace, A. M., Hubert, H. & Jaschek, C. 1980,
A&AS, 42, 103
Johnson, H. L., & Morgan, W. W. 1953, ApJ, 117, 313
Kurtz, M. J., Eichhorn, G., Accomazzi, A. et al. 2000, A&AS, 143, 41
Lesh, J. R. 1968, ApJS, 17, 371
Levato, H. 1975, A&AS, 19, 91
Mendoza, V. E. E. 1956, ApJ, 123, 54
Molnar, M. R. 1972, ApJ, 175, 453
Morgan, W. W., Code, A. C., & Whitford, A. E. 1955, ApJS, 2, 41.
Morgan, W. W. & Keenan, P. C. 1973, ARA&A, 11, 29
Moore, C. E., 1972, A Multiplet Table of Astrophysical Interest,
NSRDS-NBS 40
Murphy, R. E. 1969, AJ, 74, 1082
ˇ
Skoda, P., & ˇ
Slechta, M. 2002a, Publ. Astron. Inst. Czech 90, 1
ˇ
Skoda, P., & ˇ
Slechta, M. 2002b, Publ. Astron. Inst. Czech 90, 40
ˇ
Slechta, M., & ˇ
Skoda, P. 2002, Publ. Astron. Inst. Czech 90, 9
Slettebak, A. 1982, ApJS 50, 55
Stahl, O., Kaufer, A., Wolf, B. et al. 1995, J. Astron. Data 1, 3
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Stefl, S., & Rivinius, T. 2000, in The Be Phenomenon in Early Type
Stars, IAU Coll. 175, M. A. Smith, H. F. Henrichs, & J. Fabregat
eds., ASP Conf. Ser. Vol. 214, p. 356
Theodossiou, E. & Danezis, E. 1991, Ap&SS, 183, 91

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 1
Online Material

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 2
Appendix A: Atlas of individual line profiles
Note that the panels which contain more than one profile the spectra are arbitrarly shifted by 0.2, 0.4 and 0.6 below or above the
continuum level.
A.1. AbEm subclass
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 1113
Hα
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 1113
OI 7772
Fig.A.1. Profiles of Hαand O I7772−5˚
A lines of HR 1113.
0.6
0.8
1
1.2
1.4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
17 Tau
Hα
0.8
0.85
0.9
0.95
1
1.05
1.1
1.15
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
17 Tau
OI 7772
Fig.A.2. Profiles of Hαand O I7772−5˚
A lines of 17 Tau.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 3
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 1847B
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 1847B
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.3. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of HR 1847B.
0
0.2
0.4
0.6
0.8
1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ο And
Hα
0.6
0.8
1
1.2
1.4
1.6
1.8
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ο And
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.4. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of oAnd.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 4
A.2. EmAb subclass
0.6
0.8
1
1.2
1.4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
10 Cas
Hα
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
10 Cas
FeII 6456
OI 7772
Fig.A.5. Profiles of Hα, Fe II 6456 ˚
A, and O I7772−5˚
A lines of 10 Cas.
0.8
1
1.2
1.4
1.6
1.8
2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
φ And
Hα
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
φ And
FeII 4233
FeII 4584
OI 7772
Fig.A.6. Profiles of Hα, Fe II 4233, 4584 ˚
A, and O I7772−5˚
A lines of φAnd.
1
1.5
2
2.5
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
OT Gem
Hα
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
OT Gem
OI 7772
Fig.A.7. Profiles of Hαand O I7772−5˚
A lines of OT Gem.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 5
0.6
0.8
1
1.2
1.4
1.6
1.8
2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
β CMi
Hα
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
β CMi
FeII 5317
FeII 5235
FeII 5169
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
β CMi
FeII 6456
FeII 7712
OI 7772
Fig.A.8. Profiles of Hα, Fe II 5169, 5235, 5317, 6456, 7712, and O I7772−5˚
A lines of βCMi.
0.8
1
1.2
1.4
1.6
1.8
2
2.2
2.4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
V974 Her
Hα
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
V974 Her
FeII 7712
OI 7772
Fig.A.9. Profiles of Hα, Fe II 77712 ˚
A, and O I7772−5˚
A lines of V974 Her (HD 164447).
0.8
1
1.2
1.4
1.6
1.8
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 6984
Hα
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 6984
OI 7772
Fig.A.10. Profiles of Hαand O I7772−5˚
A lines of HR 6984 (HD 171780).

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 6
0.8
0.85
0.9
0.95
1
1.05
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
60 Cyg
Hα
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
60 Cyg
OI 7772
Fig.A.11. Profiles of Hαand O I7772−5˚
A lines of 60 Cyg.
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
β Cep
Hα
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
β Cep
OI 7772
Fig.A.12. Profiles of Hαand O I7772−5˚
A lines of βCep.
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
V360 Lac
Hα
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
V360 Lac
OI 7772
Fig.A.13. Profiles of Hαand O I7772−5˚
A lines of V 360 Lac.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 7
A.3. Em subclass
1
2
3
4
5
6
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ο Cas
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ο Cas
FeII 5317
FeII 5235
FeII 5169
FeII 4233
FeII 4584
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ο Cas
FeII 7516
FeII 7712
OI 7772
Fig.A.14. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7516, 7712 ˚
A, and O I7772−5˚
A lines of oCas.
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
−30 −20 −10 0 10 20 30
Relative Intensity
∆λ (Å)
γ Cas
Hα
0
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
γ Cas
FeII 5317
FeII 5235
FeII 5169
FeII 4233
FeII 4584
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
γ Cas
FeII 7516
FeII 7712
OI 7772
Fig.A.15. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7516, 7712 ˚
A, and O I7772−5˚
A lines of γCas.
1
1.5
2
2.5
3
3.5
4
4.5
5
5.5
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
φ Per
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
φ Per
FeII 5317
FeII 5235
FeII 5169
FeII 4233
FeII 4584
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
φ Per
FeII 7516
FeII 7712
OI 7772
Fig.A.16. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7516, 7712 ˚
A, and O I7772−5˚
A lines of φPer.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 8
0.5
1
1.5
2
2.5
3
3.5
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 894
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 894
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.17. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of HR 894.
1
2
3
4
5
6
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ψ Per
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ψ Per
FeII 6432
FeII 6456
OI 7772
FeII 7712
Fig.A.18. Profiles of Hαand Fe II 6432, 6456, 7712 ˚
A lines of ψPer.
0.5
1
1.5
2
2.5
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
η Tau
Hα
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
η Tau
OI 7772
Fig.A.19. Profiles of Hαand O I7772−5˚
A lines of ηTau.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 9
1
1.5
2
2.5
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 1500
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 1500
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.20. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of HR 1500.
1
1.5
2
2.5
3
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
κ Dra
Hα
0
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
κ Dra
FeII 4233
FeII 4584
FeII 5363
FeII 5317
FeII 5235
FeII 5169
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
1.3
1.4
−15−10 −5 0 5 10 15
Relative Intensity
∆λ (Å)
κ Dra
FeII 6456
FeII 7516
FeII 7712
OI 7772
Fig.A.21. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 5363, 6456, 7516, 7712 ˚
A, and O I7772−5˚
A lines of κDra.
0.5
1
1.5
2
2.5
3
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HD 175863
Hα
0.5
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HD 175863
OI 7772
FeII 7712
FeII 6456
Fig.A.22. Profiles of Hα, Fe II 6456, 7712 ˚
A, and O I7772−5˚
A lines of HD 175863.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 10
0.5
1
1.5
2
2.5
3
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
25 Vul
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
25 Vul
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.23. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of 25 Vul.
0.6
0.8
1
1.2
1.4
1.6
1.8
2
2.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
59 Cyg
Hα
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
59 Cyg
FeII 7516
FeII 7712
OI 7772
Fig.A.24. Profiles of Hα, Fe II 7516, 7712 ˚
A, and O I7772−5˚
A lines of 59 Cyg.
1
2
3
4
5
6
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
6 Cep
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
6 Cep
FeII 5317
FeII 5235
FeII 5169
FeII 4233
FeII 4584
0.6
0.8
1
1.2
1.4
1.6
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
6 Cep
FeII 6456
FeII 7516
FeII 7712
OI 7772
Fig.A.25. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 6456, 7516, 7712 ˚
A, and O I7772−5˚
A lines of 6 Cep.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 11
0.8
0.9
1
1.1
1.2
1.3
1.4
1.5
1.6
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HD 206773
Hα
0.5
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HD 206773
FeII 7516
FeII 7712
OI 7772
Fig.A.26. Profiles of Hα, Fe II 7516, 7712 ˚
A, and O I7772−5˚
A lines of HD 206773.
1
2
3
4
5
6
7
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
β Psc
Hα
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
β Psc
FeII 7516
FeII 7712
OI 7772
Fig.A.27. Profiles of Hα, Fe II 7516, 7712 ˚
A, and O I7772−5˚
A lines of βPsc.
1
2
3
4
5
6
7
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
EE Cep
Hα
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−15−10 −5 0 5 10 15
Relative Intensity
∆λ (Å)
EE Cep
FeII 7712
FeII 7516
OI 7772
Fig.A.28. Profiles of Hα, Fe II 7516, 7712 ˚
A, and O I7772−5˚
A lines of EE Cep.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 12
A.4. Sh subclass
0
1
2
3
4
5
6
7
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
28 Tau
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
28 Tau
FeII 5169
FeII 5235
FeII 5317
FeII 4233
FeII 4584
0.8
1
1.2
1.4
1.6
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
28 Tau
FeII 7516
FeII 7712
OI 7772
Fig.A.29. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7516, 7712 ˚
A, and O I7772−5˚
A lines of 28 Tau.
1
1.5
2
2.5
3
3.5
4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ζ Tau
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ζ Tau
FeII 5317
FeII 5235
FeII 5169
FeII 4233
FeII 4584
0
0.2
0.4
0.6
0.8
1
1.2
1.4
1.6
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ζ Tau
FeII 7516
FeII 7712
OI 7772
Fig.A.30. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7516, 7712 ˚
A, and O I7772−5˚
A lines of ζTau.
0.6
0.8
1
1.2
1.4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ψ9 Aur
Hα
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ψ9 Aur
OI 7772
Fig.A.31. Profiles of Hαand O I7772−5˚
A lines of ψ9Aur.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 13
0.6
0.8
1
1.2
1.4
1.6
1.8
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
4 Her
Hα
0.2
0.4
0.6
0.8
1
1.2
1.4
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
4 Her
FeII 5317
FeII 5235
FeII 5169
FeII 4584
FeII 4233
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
4 Her
FeII 7712
OI 7772
Fig.A.32. Profiles of Hα, Fe II 4233, 4584, 5169, 5235, 5317, 7712 ˚
A, and O I7772−5˚
A lines of 4 Her.
0.2
0.4
0.6
0.8
1
1.2
1.4
1.6
1.8
2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
88 Her
Hα
0.4
0.6
0.8
1
1.2
1.4
1.6
1.8
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
88 Her
FeII 6456
FeII 7712
OI 7772
Fig.A.33. Profiles of Hα, Fe II 6456, 7712 ˚
A, and O I7772−5˚
A lines of 88 Her.
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
V532 Lyr
Hα
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
V532 Lyr
OI 7772
Fig.A.34. Profiles of Hα, Fe II 6516 ˚
A, and O I7772−5˚
A lines of HR 6971 (HD 171406, V 532 Lyr).

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 14
0.5
1
1.5
2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HD 179343
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HD 179343
FeII 7712
OI 7772
Fig.A.35. Profiles of Hα, Fe II 7712 ˚
A, and O I7772−5˚
A lines of HD 179343.
0.5
1
1.5
2
2.5
3
3.5
4
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
EW Lac
Hα
0
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
EW Lac
FeII 7712
FeII 6456
OI 7772
FeII 7516
Fig.A.36. Profiles of Hα, Fe II 6456, 7516, 7712 ˚
A, and O I7772−5˚
A lines of EW Lac.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 15
A.5. Ab subclass
0.4
0.6
0.8
1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
α And
Hα
0.85
0.9
0.95
1
1.05
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
α And
OI 7772
Fig.A.37. Profiles of Hαand O I7772−5˚
A lines of αAnd.
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
γ Peg
Hα
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−15−10 −5 0 5 10 15
Relative Intensity
∆λ (Å)
γ Peg
OI 7772
Fig.A.38. Profiles of Hαand O I7772−5˚
A lines of γPeg.
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HD 23873
Hα
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HD 23873
FeII 7712
OI 7772
Fig.A.39. Profiles of Hα, Fe II 7712 ˚
A, and O I7772−5˚
A lines of HD 23873.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 16
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ε Per
Hα
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ε Per
OI 7772
Fig.A.40. Profiles of Hα, Fe II 6516 ˚
A, and O I7772−5˚
A lines of εPer.
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ρ Aur
Hα
0.2
0.4
0.6
0.8
1
1.2
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ρ Aur
FeII 5169
FeII 6456
FeII 7516
OI 7772
Fig.A.41. Profiles of Hα, Fe II 5169, 6456, 7516, and O I7772−5˚
A lines of ρAur.
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
HR 1847A
Hα
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
HR 1847A
OI 7772
Fig.A.42. Profiles of Hαand O I7772−5˚
A lines of HR 1847A.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 17
0.4
0.6
0.8
1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
β CMa
Hα
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
β CMa
FeII 7462
OI 7772
Fig.A.43. Profiles of Hα, Fe II 7462 ˚
A, and O I7772−5˚
A lines of βCMa.
0.6
0.7
0.8
0.9
1
1.1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
α Leo
Hα
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
α Leo
FeII 5169
OI 7772
Fig.A.44. Profiles of Hα, Fe II 5169 ˚
A, and O I7772−5˚
A lines of αLeo.
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
η UMa
Hα
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
η UMa
FeII 5169
OI 7772
Fig.A.45. Profiles of Hα, Fe II 5169 ˚
A, and O I7772−5˚
A lines of ηUMa.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 18
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
θ CrB
Hα
0.65
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
θ CrB
FeII 5169
OI 7772
Fig.A.46. Profiles of Hα, Fe II 5169 ˚
A, and O I7772−5˚
A lines of θCrB.
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ζ Dra
Hα
0
0.2
0.4
0.6
0.8
1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ζ Dra
FeII 4233
FeII 4584
FeII 5235
FeII 5169
FeII 5317
0.6
0.7
0.8
0.9
1
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
ζ Dra
FeII 6456
OI 7772
Fig.A.47. Profiles of Hα, Fe II 4233. 4584, 5169, 5235, 5317, 6456 ˚
A and O I7772−5˚
A lines of ζDra.
0.2
0.4
0.6
0.8
1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
ι Her
Hα
0.6
0.8
1
1.2
1.4
1.6
1.8
−15 −10 −5 0 5 10 15
Relative Intensity
∆λ (Å)
ι Her
FeII 5317
FeII 5235
FeII 5169
OI 7772
Fig.A.48. Profiles of Hα, Fe II 5169, 5235, 5317 ˚
A, and O I7772−5˚
A lines of ιHer.

S. M. Saad et al.: Observations of Hα, iron, and oxygen lines in B, Be, and shell stars,Online Material p 19
0.4
0.6
0.8
1
1.2
−40 −20 0 20 40
Relative Intensity
∆λ (Å)
96 Her
Hα
0.85
0.9
0.95
1
1.05
1.1
−20 −10 0 10 20
Relative Intensity
∆λ (Å)
96 Her
OI 7772
Fig.A.49. Profiles of Hαand O I7772−5˚
A lines of 96 Her.