A. S. Miroshnichenko1,2 - H. Levato3 - K. S. Bjorkman1 - M. Grosso3
1 - Ritter Observatory, Dept. of Physics and Astronomy, University of
Toledo, Toledo, OH 43606-3390, USA
2 - Central Astronomical Observatory of the Russian Academy of Sciences
at Pulkovo, 196140 Saint-Petersburg, Russia
3 - Complejo Astronómico El Leoncito (CASLEO), Casilla de Correo 467,
5400 San Juan, Argentina
Received 27 February 2003 / Accepted 16 May 2003
Abstract
The emission-line object HDE 327083 has long been considered to be
one of the most luminous stars in the Milky Way. Nevertheless,
no reliable physical parameters have been published for it.
Our high-resolution optical spectroscopy revealed the presence
of photospheric lines of a cool luminous companion. We detected significant
antiphased radial velocity variations of the emission and absorption lines.
The data obtained are still insufficient to derive a reliable orbital solution;
however, the orbital period is most likely of the order of 6 months.
We conclude that HDE 327083 is a binary system consisting of an early
B-type primary and early F-type secondary, with luminosities
and
,
respectively, and whose
orbital plane is viewed nearly edge-on.
We also obtained new multicolour
optical and infrared photometry of HDE 327083. From both the photometric and
spectroscopic data, we found that the system is located at a distance of
kpc.
Most of the circumstellar gas seems to be orbiting the primary and is
distributed in a mildly flattened envelope with a height scale and velocity
decreasing outward from the star.
We suggest that HDE 327083 represents an advanced evolutionary stage of a
Lyrae type binary.
Key words: stars: emission-line, Be - stars: individual: HDE 327083 - techniques: spectroscopic - techniques: polarimetric
B[e] stars are a group of early-type galactic objects that show forbidden emission lines and near-IR excess due to circumstellar (CS) dust. Discovered in the 1970's (Allen & Swings 1976), they have not been intensively studied until recently, mostly due to their relative faintness and the inhomogeneity of their intrinsic parameters. The advent of high-resolution spectroscopy revealed new, sometimes unexpected, features of these objects and provided a tool for refining their properties. One of the subgroups of B[e] stars contains high-luminosity objects, whose fundamental parameters, nature and evolutionary state are still poorly known due to uncertainties in the distance determination and complexity of the observed features. Similar objects, B[e] supergiants, were found in the Magellanic Clouds (Zickgraf et al. 1985), where they are among the brightest stars, confirming their high luminosity. They show very strong emission-line spectra indicating a large amount of CS matter in the immediate vicinity of the radiation source. Their spectral line profiles suggest the presence of a fast and hot polar wind (UV lines) and a slower and cooler equatorial one (optical lines). B[e] supergiants may be LBV precursors (e.g., Conti 1997), which makes their investigation relevant for our understanding of high-mass stellar evolution.
At the same time, several galactic non-luminous B[e] stars share the properties of the Magellanic Clouds B[e] supergiants (see Miroshnichenko et al. 2002a for a recent review). This makes qualitative classification of B[e] stars ambiguous and calls for quantitative studies, which require different techniques and methods of analysis. This paper continues our series of studies of galactic B[e] stars that have been classified as supergiants. In the first paper (Miroshnichenko et al. 2002b) we presented the results of high-resolution spectroscopy of CI Cam, a binary system containing a B[e] star and a compact object (neutron star or black hole, e.g. Robinson et al. 2002). We did not find convincing evidence for a large distance and, hence, high luminosity of the B[e] companion in CI Cam, and we suggested some observational tests to further constrain the objects parameters.
In this paper we report the results of our spectroscopic and photometric study of
a southern object HDE 327083. This object was not included in the original list of
B[e] stars. Attention to this object was drawn by Carlson & Henize (1979),
who reported a strong emission-line spectrum containing lines of H I, He I, and Fe II. Optical UBV photometry (Kozok 1985)
showed that it was a very reddened early B-type star (
mag).
Near-IR spectroscopy (Whitelock et al. 1983; McGregor et al. 1988) revealed a strong near-IR excess and CO emission features at 2.3
m.
The IRAS satellite (Olnon et al. 1986) detected a strong mid-IR flux from
HDE 327083, with a steep decrease towards longer wavelengths, and a featureless
spectrum in the 10
m region.
Although no solid-state features have been detected, the IR excess is too strong
to be attributed to CS gas alone and implies the presence of CS dust, which makes
the object similar to "Be stars with warm dust'', a subgroup of galactic B[e] stars
(Miroshnichenko et al. 2002a).
Optical spectroscopic observations of selected regions containing some emission
lines and interstellar features by Lopes et al. (1992)
confirmed the P Cyg-type profile of the hydrogen and singly ionized iron
lines earlier reported by Henize (1952) and Carlson & Henize (1979).
Lopes et al. also estimated the distance (D) towards HDE 327083
based on the strength of the interstellar sodium D-lines (D (kpc) = 2 EW (Å),
where EW is the average of the equivalent widths of the D1 (5895 Å)
and D2 (
5889 Å) lines, Allen 1955). At this distance (5 kpc)
the object's luminosity would be very high (MV=-10 mag), making it
one of the most luminous stars in the Milky Way. These authors also assigned a
spectral type of B6 I to the object.
Recently Machado et al. (2001) obtained new spectra
of HDE 327083 in the regions of H,
H
,
and several Fe II lines
and tried to model the Balmer line profiles. They suggested 2 different sets of
fundamental parameters for the star based on the line profile fits, although their
fits did not closely reproduce the profile shapes. Both models imply a very high
luminosity (
105
)
and mass loss rate (
10-5
yr-1). The assumed radiation source was a hot star with an effective
temperature (
)
of either 9000 K or 19 000 K.
These studies indicate that HDE 327083 is a complex object whose physical characteristics are not well constrained. This prompted us to undertake a new study of the object using both spectroscopic and photometric technique. The observations are described in Sect. 2, our new results in Sect. 3, analysis of the observed properties in Sect. 4, and our conclusions in Sect. 5.
The spectroscopic observations were obtained at the 2.1-m telescope of the Complejo
Astronómico El Leoncito (Argentina) with the échelle-spectrograph
REOSC, mounted in the Nasmyth-2 focus and equipped with a
CCD-chip. This setup allowed us to achieve a spectral resolving power
.
Additionally, 1 spectrum was obtained at the 2.1-m Otto Struve telescope of the
McDonald Observatory (Mt. Locke, Texas, USA) with the Sandiford
échelle-spectrometer (McCarthy et al. 1993) with a
.
A
pixel CCD was used. The spectrum was taken at a large air
mass of 4.5 due to the southern location of the object. As a result, it was a bit
noisy, but the line characteristics were consistent with those from
the Leoncito spectra.
There are small gaps between the spectral orders in the Leoncito spectra, while
all the orders of the McDonald spectrum are overlapped.
The log of the spectroscopic observations is presented in Table 1.
The standard data reduction was performed in IRAF.
Table 1: Log of spectroscopic observations of HDE 327083.
The optical (in the Johnson-Cousins system) and near-IR broadband photometric observations of HDE 327083 were obtained quasi-simultaneously on 1997 March 2 and 3 at the South-African Astronomical Observatory (SAAO). The 0.75-meter telescope with a single-element InSb photometer was used in the near-IR, while the 0.5-meter telescope with a GaAs photometer was used in the optical region. Additional IR observations were obtained on 2000 February 25 at Mauna Kea with the 3-meter NASA Infrared Telescope Facility (IRTF) and a single-element gallium-doped germanium bolometer. Our photometric data are presented in Table 2. The accuracy is about 0.01 mag. and 0.03 mag. for the SAAO optical and IR data, respectively, and 0.05 mag. for the IRTF data. A number of photometric standard stars were observed during the same nights at both observatories for calibration.
Table 2: New photometry of HDE 327083.
The previous spectroscopic observations of HDE 327083 discussed in
Sect. 1 were performed in selected narrow regions and
focused on emission lines. In contrast, we studied a much broader spectral
region and tried to find every possible spectral feature. The emission
line content and their profile shapes were found to be similar to those
reported in the literature. HDE 327083 clearly shows emission lines of
H I, He I, and Fe II, most of which have P Cyg type profiles.
The H line has a slightly variable double-peaked profile with the
peak intensity ratio
.
The central depression is narrow with
the minimum intensity below continuum at high-resolution (Fig. 1a).
The He I lines display a weak emission component, which almost vanishes
at a low signal-to-noise ratio (SNR). Their absorption components reach the continuum
at a heliocentric radial velocity (HRV) of
-400 km s-1 and have a mean HRV of
-200 km s-1 (derived by fitting the component with a Gaussian),
which corresponds to that of the H
blue emission peak.
In the high SNR spectra we also detected the Si II 6347 and 6371 Å lines with both an emission and absorption component (Fig. 2b);
however, these are not parts of a P Cyg type profile (see below).
As in the spectra published by Lopes et al. (1992) and Machado et al.
(2001), we detected a number of Fe II lines with P Cyg type profiles.
Their absorption components are strong in lines blueward of
Å, while they are weak or undetectable in redder lines. The emission components
are definitely double-peaked. The split is barely seen in the red Leoncito spectra
(see Fig. 2), but it becomes obvious in the blue Leoncito and the McDonald
spectrum (Fig. 3).
The only detection of the [Fe II] line at 5158 Å in the blue Leoncito
spectrum of 2000 July 19. It was also previously reported by Machado et al.
(2001).
The forbidden [N II] line at 5755 Å and the [O I] lines at 6300 and
6363 Å are seen in some of our spectra, but most likely have telluric nature.
They are unshifted from laboratory wavelengths and have a narrower
width (8 km s-1 at half maximum in the Mcdonald spectrum) than the other
emission features. The forbidden [N II] lines at 6548 and 6583 Å are
extremely weak and hardly noticeable at R=15 000. The [N II] line at 6548 Å was detected in the Mcdonald spectrum with the same width as the other
forbidden lines. This suggests that the density virtually everywhere in the
gaseous envelope of HDE 327083 is above 106 cm-3 (Osterbrock 1989).
It may be even
above 107 cm-3 because of the absence of the [S II] lines at 6312 Å.
However, the latter could be due to an insufficiently high
of the
radiation source responsible for the emission line spectrum.
Since we do not see He II lines in emission and the He I
lines have weak emission components, we can place an upper limit of B2 on the hot star
spectral type (e.g., Miroshnichenko 1996).
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Figure 1:
Portions of the spectrum of HDE 327083. Panels a) and b) show the H![]() ![]() |
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Figure 2:
Portions of the 2002 June 25 Leoncito spectrum containing the secondary's
absorption lines. The object's spectrum with the primary's continuum subtracted
is shown by solid lines. The theoretical spectrum for
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The Leoncito spectra show the IR triplet of Ca II at 8498, 8542, and 8662 Å. These lines have strong emission and weak absorption components. In some of our
spectra the emission components are double-peaked, with a peak separation of
75 km s-1 (Fig. 1c). The absorption components have similar
shapes to those of the He I lines and are due to the Paschen lines (P12, P13,
and P15), which have much weaker emission components than those of the Ca II
lines. For example, the
8498 Å calcium line is fully located inside the P12 line absoprtion component.
Table 3: Absorption lines of the secondary companion in the spectrum of HDE 327083.
The sodium D-lines at 5889 and 5995 Å have very weak emission components which
are not noticeable in every spectrum. At R=15 000 two absorption components
are seen. One of them is deep and narrow, has its position unchanged in all the
spectra (HRV= -25 km s-1), and is certainly of interstellar origin.
At higher resolution it splits into 2 components at HRVs of -11 km s-1and -35 km s-1. The red component seems to be formed
in the local spiral arm and is saturated, while the blue one originates in the
Sagittarius arm and is close to saturation (Fig. 1b). There is also another
absorption component of the D-lines, which is weak and broad and has a HRV of
-130 km s-1. This component is most likely CS, with the
position close to that of the H
central depression.
Strong diffuse interstellar bands (DIB) are seen in our spectra. They have
single-peaked and nearly gaussian profiles with a mean HRV of km s-1,
averaged over all our spectra. There is a sign of a split in the strongest DIBs
at 5780 and 5797 Å in the McDonald spectrum, where the red component is much
stronger than the blue one. This may be due to the components formation in
different spiral arms, similar to that in the Na I D-lines. At the same
time, the other DIBs detected in this spectrum (6269, 6379, 6613, 6660, and 6699 Å) do not show such a split. Furthermore, a low SNR in the continuum of this
spectrum (
30) makes this split uncertain.
Photospheric lines have not been reported previously for HDE 327083. We also do
not find those appropriate for a hot star in our spectra. At the same time, we
detected a large number of relatively weak absorption lines, most of which were
identified with neutral metals (see Table 3 and
Figs. 2-4). Moreover, we found that the mean HRV of these lines
varies with time (see Fig. 5), and its amplitude
(80 km s-1) is much higher than its statistical accuracy
(
5 km s-1, Table 4).
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Figure 3: A portion of the spectrum of HDE 327083 containing Fe II lines. The solid line shows the Leoncito spectrum of 2002 June 25, while the dashed line shows the Mcdonald spectrum of 2002 September 25. The displacement of the photospheric lines is clearly seen. The intensities are in continuum units, and the heliocentric wavelengths are in Å. |
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The absorption components of the Si II
lines have the same HRVs as those of the other absorption lines, suggesting that
they belong to the atmosphere of a cool companion, while the emission components
may be formed in the CS envelope. The presence of the Si II lines in the
spectrum of the cool companion sets a lower limit on its
,
because
these lines are not seen in K-type stars. Moreover, in G-type stars these lines are weaker
than others in this spectral region (e.g., Fe I (Mult. 13)
6358 Å).
A comparison of the spectra of HDE 327083 and MWC 623, a B[e] binary with
a K-type secondary companion (Zickgraf 2001), shows that HDE 327083 has a
much poorer absorption line content than MWC 623 (Fig. 4). Therefore, the
cool companion most likely has an A- or F-type.
Photospheric absorption lines were detected in our spectra redward of
4700 Å. We do not see them in the bluer regions for the following
reasons. First, our only blue spectrum has a low SNR, and, second, the hot
companion's continuum becomes dominant in this spectral region. However,
the observed absorption-line spectrum suggests that the companions
are almost equally bright in the V-band. Indeed, the comparison of the secondary's
spectrum (which was obtained by subtraction of the featureless primary's
continuum from the normalized observed spectrum) with theoretical spectra shows
a very good agreement for
K,
,
and
-40 km s-1 (see Fig. 2). The continuum intensities
of the companions were fixed as equal. The estimated secondary's parameters correspond
to those of an early F-type supergiant.
One of the prominent spectral features is a strong O I triplet at 7771-7775 Å
(Fig. 1d). It is usually weak in hot (B-type) and low-luminosity stars,
and thus can be attributed to the secondary's atmosphere. According to a recent
luminosity calibration by Klochkova et al. (2002), the most luminous stars
(
mag) show EW(O I) = 2.0-2.7 Å.
The observed EW(O I) in the spectrum of HDE 327083 is
Å, which
becomes
Å after subtracting a featureless contribution of the primary
using a reasonable component brightness ratio at the triplet's wavelength (
).
This result would suggest that the primary's luminosity is above the Eddington level,
which seems unreliable. Moreover, in our spectrum of CPD
9243,
a B[e] star with very similar observed features, the EW(O I) = 4.8 Å.
Thus, CS matter may contribute to the observed strength of the triplet, restricting
reliable luminosity estimates based on this EW to normal stars and objects with weak
emission-line spectra.
The emission line components seem to change their HRVs (measured by matching the original and mirrored line profiles) in antiphase to those of the absorption lines (see Figs. 5-6). However, due to the weak and broad nature of most of the emission lines, their HRVs are less reliable. Their profiles may also be affected by the envelope's kinematics. This is why we consider the emission-line HRVs, shown in Fig. 5 and listed in Table 3, to have a lower statistical weight than those of the photospheric lines. As seen in Fig. 5, their HRVs do not closely agree with the solution obtained for the photospheric lines.
The H
line was saturated in half
of our spectra, because we tried to achieve a high SNR in the continuum.
In those spectra where the observed H
profile was not affected by
the detector non-linearity, the positions of the emission peaks and central
depression were stable within
10 km s-1.
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Figure 4: Portions of the spectra of HDE 327083 (upper solid line) and MWC 623 (lower solid line) obtained at the McDonald Observatory. The dashed line represents the theoretical spectrum with the same parameters as in Fig. 2. Most of the unlabeled lines in the spectrum of MWC 623 are those of Fe I. The intensities are in continuum units, and the heliocentric wavelengths are in Å. |
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The described behaviour caused us to suspect that the pure absorption-line spectrum belongs to a cooler star, the secondary companion of the B-type primary. The possible parameters of the binary system are discussed in Sect. 4.
Our optical photometry obtained in 1997 showed that HDE 327083 was about 0.2 mag fainter in the V-band with respect to the 1979/80 data of Kozok
(1985), while the U-B and B-V colour-indices were very close
in both data sets. The broadband IR photometric data for HDE 327083 were
obtained by us
for the first time. Earlier McGregor et al. (1988) published
continuum fluxes in the H and K bands (13.1 and 21.8 Jy, respectively)
measured from their absolutely calibrated low-resolution spectra.
These fluxes are in good agreement with our results. Also our result for
the N band (10.4 m) obtained in 2000 turned out to be close to the
IRAS 12-
m flux measured in 1983 and to the MSX A-band (8.28
m)
flux measured in 1996. The spectral energy distribution (SED) of HDE 327083
corrected for the reddening is shown in Fig. 7. The de-reddening
procedure and the SED features are further discussed in Sect. 4.
Thus, the object may be photometrically variable in the optical region. The IR brightness seems to be more stable. However, the small amount of data does not allow us to draw a more definite conclusion about the variability level.
In general, the IR excess of HDE 327083 is similar to those of other Be stars
with warm dust (e.g., Miroshnichenko et al. 2001). It comprises about 1
per cent of the total illuminating radiation, which corresponds to an optical
depth of 0.01 if the dust is spherically distributed around the system.
However, this distribution seems to be unlikely for a supposedly evolved
binary. Furthermore, the IR spectrum in the 10
m region is essentially
flat, implying either a moderate optical depth or the presence of amorphous
carbon as the dominant dusty component. The former case is more attractive
as the dust was probably formed in the system, which has a preferential plane
for CS matter concentration. The latter case implies that at least one of
the companions is so evolved that carbon from the stellar interiors has reached
beyond its surface. Since the spectral line content of HDE 327083 does not show
an obvious CNO overabundance, it is more likely that the dusty envelope has
a chemical composition similar to the IS. This suggestion is consistent with the
results of our SED analysis discussed below in Sect. 4.1.
The steep decrease of the IR flux longward of m implies that the
dusty envelope is compact. In turn, this might imply that it was formed
recently, so that it is still close to the illuminating sources. The dust
might have been formed during a phase of a rapid mass exchange, which is
expected in many binary systems.
Table 4: Radial velocities of the spectral lines of HDE 327083.
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Figure 5:
The radial velocity curve for HDE 327083. The average HRV of the
photospheric lines measured in different spectra are shown by filled
circles. The HRV of the 2000 Leoncito spectra are not shown to provide
a better scale for visual comparison of the data and calculations.
The lines represent calculated RV curves for the following parameters:
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Figure 6:
Emission line profiles in the Leoncito spectra of HDE 327083. a) The Balmer lines.
The H![]() ![]() ![]() |
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Figure 7:
The spectral energy distribution of HDE 327083. The reddening correction
was applied using the extinction values derived from the photometry and adopted
spectral types. The IRAS filter photometry is shown by open triangles, the
ground-based data by filled circles, the MSX data by open squares, and the IRAS
low-resolution spectrum by the solid line. The dotted line represents the Kurucz
(1994) theoretical SED for the primary (
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We now discuss the findings described above, derive new estimates for the object's parameters, and suggest follow-up observations to further refine our understanding of its nature and evolutionary state.
The optical colour-indices of HDE 327083 imply a large reddening which is supported by the strong interstellar (IS) lines and DIBs. At least a part of it may be CS. However as we learned studying other Be stars with warm dust, the CS part of the reddening is usually small, and relationships between the IS extinction and colour-excesses can be applied to unveil the intrinsic SED of these objects (e.g., Miroshnichenko et al. 2000).
Since the IS extinction law varies within the galactic plane, we collected
published multicolour photometric data for stars projectionally close to
HDE 327083. These data allowed us to constrain the IS extinction law in the
object's direction. In particular, we found that the total-to-selective
extinction ratio
R=AV/E(B-V) is close to the mean galactic value of 3.1.
The colour-excess ratios were found to be as follows:
E(U-B)/E(B-V)=0.83,
,
,
E(V-J)/E(B-V)=2.20,
and
E(V-K)/E(B-V)=2.70. This is in agreement with the results of He et al.
(1995), who used the same data for the stars of our sample as part of
their study of the IS extinction in the southern Milky Way.
Application of the
E(U-B)/E(B-V) ratio to HDE 327083 gives a reddening
independent parameter
QUBV = (U-B) - 0.83 (B-V)= - 0.86, which
corresponds to a spectral type of B1/2 I or B2/3 V
(Strajzhys 1977). These estimates agree with the emission line content
discussed in Sect. 3.1. The companion's spectral types and equal
brightnesses give a total (IS + CS) colour-excess
mag and an extinction
mag. The DIBs strength gives
a similar
(Herbig 1993), which may also contain
some CS contribution.
Nevertheless, these results confirm that the hot companion is an early B-type
star as follows from the spectroscopic analysis.
The
and
colour-excesses, which were
0.63 and 1.28, respectively, are also in good agreement with these IS
values. This indicates no significant contribution from the cool companion, thus
supporting its relatively high
.
The colour-excess ratios for the
near-IR bands (JHKLM) are higher than the IS ones due to the radiation of CS dust.
The dereddened SED of HDE 327083 is shown in Fig. 7 along with the
theoretical SEDs for the companions.
Using the estimated reddening we can put constraints on the location of
HDE 327083, whose galactic coordinates (
,
)
are close to the direction toward the galactic center. A relationship
between the
and D in a field close to the object's direction
(
,
)
was constructed by Neckel & Klare (1980).
It shows that
is about
mag at D=1-4 kpc.
However, HDE 327083 is closer to the galactic plane than most of this
field, which may imply a higher extinction level. Inspection of photometric
data for the stars within 1
of HDE 327083 (mainly from He et al.
1995) shows that AV of 3 and even 5 mag is reached at D=1.5-3 kpc.
However, the distance estimates toward these stars are based on spectroscopic
parallaxes, which may not be accurate because of possible errors in the luminosity
classification.
On the other hand, it is thought that stars are usually confined
within spiral arms. According to Rydgren (1974), in addition to the
local arm where the Sun is located, two outer spiral arms can be traced in the
object's direction. The Sagittarius arm is located at D=1-2 kpc from the Sun,
while the Norma-Scutum arm is located at D=3.5-4.5 kpc. Optical H II
regions at 320
at
kpc show
45 km s-1. We detect no IS feature in the object's spectrum with such a high RV.
Also the Na I D-lines only show 2 components (see Sect. 3.1), which
most likely belong to the local and the Sagittarius arms. This argument would constrain the
location of HDE 327083 within the Sagittarius arm. Thus, the first order estimate
for its D is
kpc. The strong blue components of the Na I D-lines
favor a location deep within the arm.
The D estimate can then be used to estimate the companions' luminosities.
Assuming that they have equal V-band brightnesses and taking the mean brightness
of the whole system (
mag), the individual companions
turn out to be
mag. With an
and a
kpc mag, the companions' absolute visual magnitudes are
mag.
The D=5 kpc derived by Lopes et al. (1992) from the Na I D-line strength is most likely an overestimate, because their interstellar components are saturated (see Fig. 1b). Moreover, their equivalent widths (EW) depend on the spectral resolution. For example, in our Leoncito spectra the sum of the EWs for both lines is 2.3 Å, while in the McDonald spectrum it is 2.0 Å. Also it is hard to use our RV data to derive a D estimate using the galactic rotation curve. These data do not allow us to determine the systemic RV with confidence.
Our discovery of the absorption lines of neutral metals in the spectrum of HDE 327083 unambiguously indicates the presence of the secondary companion, which is cooler than the primary responsible for the emission-line spectrum. The secondary should not be much fainter than the primary, since its spectral lines are clearly seen. It does not dominate in the optical region either, as the observed SED is consistent with that of a reddened early B-type star (Sect. 4.1). It seems reasonable that the companions' luminosities and probably masses are comparable. This is followed from comparison of the RV amplitudes of the emission (Fe II) and absorption lines, which are close to one another. Nevertheless, this fact is not well established, since in our spectra we detected only a few Fe II lines with reliably measured RVs. In most cases these lines are weak, and their profiles are affected by close absorption lines.
From our RV data, although sparse, we can roughly estimate some parameters of
the binary. Since the system is not close to us, the companions are large and
the orbital period (
)
cannot be small. The lowest
consistent with our RV data is
55 days (see Fig. 5). If we assume
that we observed the full RV amplitude (the semi-amplitude
km s-1),
then one can calculate the secondary's mass function
f(m2)=0.5
.
In order to estimate the companion masses, we need to know the inclination angle
of the system's rotation axis (i) with respect to the
line of sight. It is most likely large (probably even close to 90
),
because the emission line profiles have a P Cyg type shape. This suggests
a large optical depth for bound-bound transitions in the line of sight. Since
it is hard to expect a spherical CS envelope in a binary system, we can assume
that it is flattened and the plane of preferential matter concentration
coincides with the orbital plane. Therefore
should not be far from 1,
suggesting the companion masses of
2
if equal. This is too low
for such distant and hot stars.
This consideration prompted us to suggest that
and/or K2 are larger.
Our calculations of different RV curves for both circular and eccentric orbits
show that our data set is in the best agreement with
days,
km s-1, and
.
Low-eccentricity with such a long period
does not agree with the obtained RV data. The best long-period solution gives
f(m2)=3 (1-e2)3/2
or
.
Such masses still seem too low for such luminous stars as the system's
companions. This might be due to an underestimation of the RV amplitude, which
must be verified by follow up spectroscopic observations at more orbital
phases. Even a small increase in this parameter may raise the companions' masses
significantly, as masses K3. On the other
hand, even an intermediate-mass binary with a short initial orbital period may
evolve into an object similar to that of HDE 327083 (cf. van den Heuvel 1994).
We can estimate other parameters of the binary on the basis of the
longer-period solution and the secondary's parameters derived in Sect. 3.1
and 4.1. The companions'
(20 000 K and 7000 K) imply
bolometric corrections of -2 mag and 0 mag, respectively (Miroshnichenko
1998a). This gives bolometric luminosities
mag
(
)
for the primary and
mag
(
)
for the secondary. Therefore, the radii would
be
for the primary and
for the secondary.
Assuming that the total mass of the binary is
20
,
one can derive
the orbital semi-major axis
or 1.7 A.U. The mass does not
crucially affect this parameter, since it is proportional to a1/3.
The companions' separation, even at periastron with
,
is consistent
with their size estimates. On the other hand, an evolved
long-period binary is likely to have a less-eccentric orbit due to circularization.
The latter suggestion is supported with small intensity variations of the
emission-line spectrum.
At the same time, the estimated orbital and stellar parameters suggest that the
system may experience mass-exchange at least at phases near periastron.
The emission-line profiles contain information about the CS matter distribution
in the system. Most of them have P Cyg types, indicating the presence of a
high opacity region in front of the hot companion. At the same time, the line
absorption components are centered at two different HRVs (-200 km s-1for the He lines and
-120 km s-1 for the Balmer lines, see
Fig. 6). The absorption components of the Fe II lines blueward of
Å have HRVs of
-120 km s-1. As mentioned in
Sect. 3.1, they become weaker in the redded Fe II lines,
and their RV are difficult to measure. This effect is most likely due to the
increasing contribution of the secondary companion.
Also, like the He I lines, the entire Fe II line profiles follow the
primary's orbital motion. The only Balmer line (H
)
exhibits a double-peaked profile with the blue emission peak located at virtually the
same RV as that of the He I absorption component. Also the Fe II lines
and the Ca II IR triplet show double-peaked emission-line profiles with the
peak separation
3 times smaller than that in the H
line.
Since the He I lines have the highest excitation potential among the considered species, they seem to be formed in the most inner region of the primary's envelope. The Balmer lines are usually formed throughout the entire gaseous envelope, while the Fe II and Ca II lines with even lower excitation potentials are formed in the envelope's outer parts (at least their emission components).
The described variety of the line profiles suggests a velocity distribution decelerating outwards from the stellar surface rather than an accelerating one, usual for early-type supergiants. For example, in the spectrum of P Cyg, a supergiant with a slowly accelerated mostly spherical wind, absorption components of the He I lines are located at lower RVs than those of the Balmer lines (Najarro et al. 1997). The P Cyg type profiles indicate that the envelope is not very flattened, otherwise double-peaked profiles centered at the star's position would be observed. The absorption components of the Fe II lines may be formed in this part of the envelope. The double-peaked shape of the emission components of the Fe II and Ca II lines may indicate that the envelope becomes flatter at large distances from the primary.
The presence of the blue emission peak in the H
profile suggests that
there is an emitting region near the stellar surface. The problem is why such
a peak is not observed in the other Balmer lines. This might be due to a high
density at the envelope's base responsible for a steep decrease of the higher
level populations, or to the CS dust in front of the star absorbing the
blueshifted line emission. Both these possibilities might work together.
Summarizing all the information about the emission line profiles,
we can conclude that the primary's CS envelope: a) is dense, so that forbidden
lines are extremely weak; b) is optically-thick in most of the observed
transitions; and c) has a height scale and velocity that decrease outward from
the stellar surface.
There are no signs of line emission originating in the vicinity of the secondary companion. This suggests that there is much less CS matter around it than around the primary. There may be two major sources of the CS matter in the system: the primary's stellar wind and the matter transfer from the secondary, especially if it fills its Roche lobe at least at periastron. Since we do not see the primary's photospheric lines even in spectra with high SNR, the star may be a fast rotator, so the lines are shallow. Our suggestion about a high velocity at the envelope's base would agree with this picture. The primary could be additionally spun up through angular momentum transfer from the secondary's material. The decelerating outwards velocity distribution may explain why the Balmer line profile modeling presented by Machado et al. (2001), who employed an accelerating wind kinematics, was not successful. We do not attempt to model the line profiles here, because this task requires a thorough theoretical investigation of the radiation transfer in a complex CS medium. More high-resolution and high SNR spectroscopy than we have is needed to further constrain the latter's properties.
Our spectroscopic observations of a southern emission-line object HDE 327083 obtained in 2000-2002 resulted in the following findings, most of which have not been reported before.
HDE 327083 becomes the fifth binary system among the Be stars with warm dust (the other four are MWC 623, CI Cam, AS 381, and V669 Cep), so that binaries are presently about 1/4 of the total number of these objects (see Miroshnichenko et al. 2002a). This result strengthens the support for our hypothesis that the complicated observed features of the group are due to a binary nature. It also shows the importance and effectiveness of long-term multi-technique observational programs in revealing their true properties.
Acknowledgements
This paper uses observations made at the South-African Astronomical Observatory (SAAO). We thank T. Lloyd Evans, D. Kilkenny, F. Marang, and F. Van Wyk for obtaining the multicolour photometry of HDE 327083. We are also grateful to the referee M. van den Ancker for his valuable comments. A. M. and K. S. B. acknowledge support from NASA grant NAG5-8054 and thank the IRTF staff for their assistance during the observations. Karen Bjorkman is a Cottrell Scholar of the Research Corporation, and gratefully acknowledges their support. This research has made use of the SIMBAD database operated at CDS, Strasbourg, France.