Astrophysical Bulletin, 2007, vol.62
Optical spectrum of the post-AGB star HD 56126
in the region 4010–8790 Å
V.G. Klochkova1, E.L. Chentsov1, N.S. Tavolganskaya1 , and M.V. Shapovalov2
1 Special Astrophysical Observatory RAS, Nizhnij Arkhyz, 369167 Russia,
2 Rostov State University, Rostov-on-Don, Russia
October 23, 2018
Abstract We studied in detail the optical spectrum of the post-AGB star HD56126 associated with the
IR-source IRAS07134+1005. We use high resolution spectra (R=25000 and 60000) obtained with the
echelle spectrographs of the 6-m telescope. About one and a half thousand absorptions of neutral atoms
and ions, absorption bands of C2, CN, and CH molecules, and interstellar bands (DIBs) are identified in
the 4010 to 8790 ÅÅ wavelength region, and the depths and radial velocities of these spectral features
are measured. Differences are revealed between the variations of the radial velocities measured from
spectral features of different excitation. In addition to the well-known variability of the Hα profile, we
found variations in the profiles of a number of Feii, Yii, and Baii lines. We also produce an atlas⋆ of
the spectrum of HD56126 and its comparison star αPer.
1. Introduction
The star HD56126 is observed in the post-AGB phase of its evolution. While undergoing this short-lived
stage (according to Blöcker [1], this phase lasts for ∆T ≈ 103 ÷ 104 years), the star passes to the stage of a
planetary nebula and therefore post-AGB stars are also commonly referred to as “protoplanetary nebulae”
(PPNe). In the Hertzsprung–Russell diagram post-AGB stars move at almost constant luminosity leftward
of the AGB and become increasingly hotter. These objects, which are descendants of AGB-stars, can be used
to trace the physical and chemical parameters of the interstellar matter due to a change in the energy source,
which is accompanied by a change of the star structure, ejection of the envelope, and mixing of matter.
The main task of our research is to reveal the chemical composition anomalies that are due to the nuclear
synthesis of chemical elements in the interiors of low- and intermediate-mass stars (less than 8–9M⊙) and
subsequent dredge-up of the products of synthesis to the surface layers of stellar atmospheres. We use our
high-precision spectroscopic data not only to study the chemical composition, but also to perform a detailed
analysis of the velocity field in the atmospheres of these stars, which constitutes a separate astrophysical
problem. In addition, the high quality observational data allowed us to produce an atlas of the spectrum of a
typical post-AGB star over a wide wavelength interval. To this task, we chose the supergiant star HD 56126
(Sp=F5Iab), which is the optical component of the IR source IRAS07134+1005 with a double-peaked
spectral energy distribution (SED) typical of PPN. The star HD56126 is located outside the galactic plane,
its galactic coordinates are l=206.◦75, b=+9.◦99. Note that HD56126 is a generally recognized canonical
object in the phase of transition from the asymptotic giant branch to a planetary nebula. In addition to
the anomalous SED mentioned above, which is due to the circumstellar dust, this star exhibits other, highly
conspicuous, features specific for this class of objects [2]: the optical component of the PPN is an F5Iab-
type supergiant at a high galactic latitude; the central star is surrounded by an extended nebula, which,
according to HST observations [3], has the largest angular size β > 4′′ among PPN objects of this type; the
optical spectrum exhibits variable complex emission–absorption profile of the Hα and shows spectral features
that are indicative of the current mass outflow. Based on their high-resolution spectroscopy (R=860000,
FWHM=0.35km/s) of HD56126, Crawford and Barlow [4] revealed the multicomponent structure of the
Ki and C2 features, which is indicative of repeated episodes of mass ejection from the star.
⋆ The full version of the Atlas is available in electronic form from: http://www.sao.ru/hq/ssl/Atlas/Atlas.html
http://arxiv.org/abs/0704.0677v1
http://www.sao.ru/hq/ssl/Atlas/Atlas.html
2 Klochkova et al.: Spectroscopy of HD56126
Subsequent studies of HD56126 and of the associated IR source revealed a number of properties, which
allowed the object to acquire the canonical status in its class. First, an analysis of the spectra obtained with
the echelle spectrograph of the 6-m telescope, allowed Klochkova [5] to conclude that HD56126 is a metal-
poor star with [Fe/H ]⊙=−1.0 and high excess of carbon and s-process elements. Second, IRAS 07134+1005
was found to belong to the group of PPNe whose IR-spectra exhibit an emission feature at λ=21µm. Objects
of this small subgroup were found to exhibit a correlation between the presence of this 21µm–feature and
the manifestation of products of stellar nucleosynthesis in the outer atmospheric layers: overabundance of
carbon and heavy metals of the s-process. This so far unexplained correlation has been found independently
by Klochkova [6] and a group of other authors [7]. Thus HD56126 possesses the complete set of features
peculiar to the entire family of PPNe, and this fact determines the importance of the detailed spectroscopy
of this object and preparation of an atlas of its optical spectrum over a wide spectral region. This task is
facilitated by HD56126 being the brightest (B=9.m11, V=8.m27) star among carbon-rich PPNe and hence
the most accessible star for high-resolution spectroscopy among the objects of this type.
Section 2 gives a brief description of the methods of observation and data reduction employed in this
paper. Section 3 presents the peculiar features of the spectrum of HD56126, and section 4 describes the
field of radial velocities Vr in the atmosphere and envelope of the star. We also briefly discuss the radial-
velocity variability and the variability of selected spectral-line profiles. Section 5 describes the spectroscopic
atlas, identification of spectral features, and compares the spectrum of HD56126 with that of the standard
supergiant αPer (Sp = F5Iab).
2. Observations and reduction of spectra
We performed spectroscopic observations of HD 56126 and αPer with the 6-m telescope of the Special
Astrophysical Observatory. We obtained all spectra with NES [8, 9] and Lynx [10, 11] echelle spectrographs
operating in the Nasmyth focus. A 2048×2048 CCD and image slicer [12] with the NES spectrograph allows
taking spectra with a resolution of R≈ 60000, whereas the Lynx spectrograph equipped with a 1K×1K CCD
yields a resolution of R≈ 25000. The Table 1 gives the dates of observations and the spectral region recorded.
We use the modified ECHELLE context of MIDAS to extract data from two-dimensional echelle spectra
(see [13] for details). Cosmic-hit removal was performed via median averaging of two successive spectra.
Wavelength calibration was made using Th-Ar-lamps. We use DECH20 [14] code to perform spectropho-
tometric and position measurements. In particular, we determine the radial velocities from individual lines
and their components by superimposing the direct and mirror-reflected profiles. We determine the position
zero point for each spectrogram by referring it to the positions of ionospheric emission features of the night
sky and to those of telluric absorptions, which show up against the spectrum of the object. The accuracy
of single line velocity measurements in the spectra obtained is better than 1.0 and 1.5 km/s, for NES and
Lynx spectrographs, respectively.
3. Peculiarities of the optical spectrum of HD56126
Optical spectra of PPNe differ from the spectra of classical supergiants by the anomalous profiles of spectral
lines (Hi, Nai, Hei), and primarily, by the anomalous Hα profiles. Hα lines in the spectra of typical PPNe have
complex emission and absorption profiles with asymmetric cores, PCyg- or inverse PCyg-type profiles, and
profiles with two emission components. PPNe often exhibit a combination of several such features. Emission
in Hα may be due to mass outflow and/or pulsations and hence we must observe sporadic stellar wind in
many PPNe. The Doppler shift of the core is usually smaller than the escape velocity, i.e., we have evidence
only for motions at the wind base. The spectra of individual objects owe the great variety of their profiles to
the differences in the dynamical processes in their extended atmospheres: spherically symmetric outflow with
constant or height-dependent velocity, mass infall onto the photosphere, and pulsations. A two-component
emission profile is indicative of a nonspherical envelope, e.g., the presence of a circumstellar disk.
The peculiarity of the optical spectra of PPNe often shows up not only in specific Hi profiles, but also in
the distortions of the spectral features of the F −K-type supergiant due to chemical composition anomalies
and the presence of molecular features along with atomic and ion lines.
HD 56126 exhibits all these spectral peculiarities that distinguish PPN from a normal supergiant of the
same spectral type. As is evident from Fig. 1, the Hα line has a complex profile with absorption and emission
components, which are absent in the spectrum of the comparison star αPer. Figure 1 also shows well-defined
photospheric wings of the Hα line in the spectrum of HD56126. These wings are almost as extended as in
the spectrum of αPer. Figure 2, which shows all the data now available, demonstrates date-to-date variations
Klochkova et al.: Spectroscopy of HD56126 3
Table 1. Log of observations and results of Vr measurements. Column 4 gives the mean Vr averaged over weak
lines (r→ 1). For Feii(42), Hα and D lines of Nai we give the velocities inferred from the positions of the strongest
line components. The numbers in parentheses give the velocities inferred from weaker components. Slanted font in
column 5 indicates the velocities inferred from the IR oxygen triplet Oiλ 7773 Å. Semicolumn indicates uncertain
Date Spectro- ∆λ, Å Vr
graph r→ 1 Feii(42) Hβ Hα DNai C2 interstellar
1 2 3 4 5 6 7 8 9 10 11 12
HD56126
12.01.93 Lynx 5560–8790 88.8 91 – 78 (100:) 77 – – – –
10.03.93 Lynx 5560–8790 89.0 93 – 71 (43:) 75: – – – –
04.03.99 Lynx 5050–6640 85.9 77 – 76 (43:) 78 77.1 – – –
20.11.02 NES 4560–5995 89.6 95 (80:) 89 – 75 (89) 77.2 12.0 23.5 30.8
21.02.03 NES 5150–6660 88.8 96: – 88 (112:) 75 (89) 77.1 12 24 31
12.04.03 NES 5270–6760 88.4 – – 82 (103:) 75 (89:) – 13 23 30.5
14.11.03 NES 4518–6000 85.3 96 (87:) 97 – 75 (87:) 76.9 12.5 – –
10.01.04 NES 5270–6760 86.7 – – 54: 76 (86:) – 13.0 23.5 31
09.03.04 NES 5275–6767 89.8 – – 58 (74:) 76 (89) – 13 24 31
12.11.05 NES 4010–5460 82.5 97 (77:) 98 – – 77.5 – – –
04.03.99 Lynx 5050–6620 −1.2 −1 – −2 – – –
02.08.01 NES 3500–5000 −1.8 −1 : −2 – – – –
11.11.05 NES 4010–5460 −2.0 −2 −2 – – – –
12.11.05 NES 4560–6010 −1.9 −2 −2 – – – –
6540 6550 6560 6570
Figure 1. Fragment of the atlas containing the Hα profile in the spectra of HD 56126 (top) and αPer
(bottom). The y-axis gives the residual intensities, the continuum level is set equal to 100.
of the central part of the Hα profile. Earlier, Oudmaijer and Bakker [15] performed spectral monitoring of
HD56126 and also found the Hα to be highly variable over a two-months time scale. Hα-line variability can
be naturally explained in the case of post-AGB stars with signs of binarity (e.g., in the case of HR 4049 [16]),
however, it also shows up in post-AGB objects, which exhibit no regular radial-velocity or light variations
(the case of HD133656 [17]). Photometric variability would allow us (like in the case of RVTau type stars)
to invoke the mechanism where a shock wave stimulates mass outflow. Based on an extensive set of good
quality spectroscopic observations of HD56126, Barthès et al. [18] found that not only the profile of Hα but
4 Klochkova et al.: Spectroscopy of HD56126
6562 6564 6566
12.01.93
10.03.93
04.03.99
21.02.03
12.04.03
10.01.04
09.03.04
Wavelength, А
Figure 2. Variations of the Hα-line profile in the spectra of HD 56126 taken on different days. The y-axis
shows the residual intensities, the continuum level of the lower spectrum is set to 100 and every next spectrum
is shifted by 100 gradations with respect to the previous spectrum.
also that of Hβ to be variable. The above authors analyzed the variations of the profiles of both these lines
and concluded that no periodic component is present that could be associated with the radial-velocity and
photometric variations of the star.
The profiles of strong Feii lines (first and foremost, those of the members of the 42-nd multiplet), Baii,
and other elements in the spectrum of HD56126 are also variable. However, whereas either the blue or
red wing may have lower slopes in the absorption core of Hα, nonhydrogen absorptions preserve their
Klochkova et al.: Spectroscopy of HD56126 5
5160 5170 5180 5190
Figure 3. Same as Fig. 1, but for the spectral region containing the 5165 Å band of the Swan system of C2
molecule and the Feii(42) 5169 Å line.
asymmetry pattern unchanged: the blue wing is always more extended than the red wing. The profile of the
Feii (42)λ 5169 Å line in Fig.3 is a typical example.
Figures 3 and 4 show fragments of the spectra that may illustrate the differences between line intensities
of HD 56126 and αPer. Feii absorptions in the spectrum of the former star are much weaker than in those
of the latter star, and the ratio of the central depths of the same line in the spectra of the two stars depends
on the line intensity: it increases from 1.5 to 4 as one passes from weak to strong lines. Fei lines are also
depressed, on the average, by 0.1. On the contrary, Ci absorptions as well as those of Yii, Zrii, and other
s-process products are deeper by 0.1–0.2 in the spectra of HD 56126 compared to the corresponding features
in the spectrum of αPer.
Let us now analyze the molecular component of the spectrum of HD56126. Bakker et al. [19] were the
first to identify the Swan absorption bands of C2 molecule and of the red system of CN molecule in the
spectrum of the star. Later, Bakker et al. [20] used high-resolution spectra with R=50000 to perform a
detailed analysis of molecular bands in the spectra of HD 56126 and 16 other PPNe selected based on the
presence of carbon molecules C2, CN, CH
+ in their shells. Judging by the velocity corresponding to the
position of these bands, the molecular spectrum forms in a limited region of the shell close to the star [20].
Our spectra exhibit several bands of the Swan system (see Fig. 3).
Here it is pertinent to recall that the spectra of several PPNe were found to exhibit emission Swan bands
[19, 6]. However, the spectra of HD 56126 taken in different years show no signs of emission in these bands. D
lines of Nai neither show any signs of emission. This fact is consistent with the rather simple elliptical shape
of the nebula surrounding HD56126. Emissions in the Swan bands or in Nai D lines appear to show up only
in the spectra of PPNe with bright circumstellar nebulae with well-defined asymmetry. The spectroscopy of
the following PPNe corroborates this hypothesis: IRAS 04296+3429 [21], IRAS 23304+6147 [22], AFGL 2688
[23], IRAS 08005−2356 [24], IRAS 20056+1834 [25], and IRAS 20508+2011 [26]. On HST images [3], the
nebulae surrounding these PPNe are usually asymmetric and have a bipolar structure. Note also that most
of the objects listed above belong to type “1” according to the classification of Trammell et al. [27] — i.e.,
they are PPNe with polarized optical radiation.
Figure 5 shows the behavior of the D2 Nai line profile in the spectrum of HD56126, and here, like in
Table 1, to reveal the fine structure of lines, we analyze only the spectra taken with the highest resolution. The
positions of the three short-wavelength components remain constant within the errors. This stability confirms
that the components form in the interstellar medium. The wavelength shift of the deepest component agrees
6 Klochkova et al.: Spectroscopy of HD56126
5840 5850 5860 5870
Figure 4. Same as Fig. 1, but for the spectral region with the Baii λ 5853 Å line.
with that of the Swan bands (columns 8 and 9 in Table 1), and this fact indicates that the component in
question forms in the circumstellar shell. Finally, the longest-wavelength component forms in the photosphere:
its temporal behavior agrees with that of other photospheric absorptions (columns 4 and 8 in Table 1).
4. Radial velocities pattern
Much attention has been paid to the radial-velocity variations of HD 56126 and to study the differences
between the radial velocities inferred from lines of different types. Bujarrabal et al. [28] used CO millimeter-
wave observations to find Vr = 86.1 km/s, which is natural to adopt as the systemic radial velocity of
HD56126. Based on an extensive collection of spectrograms with high temporal resolution and high S/N
ratio, Oudmaijer and Bakker [15 analyzed the behavior of Vr and concluded that it is variable on a time
scale of several months with a small amplitude (Vr=84÷87± 2 km/s). The above authors demonstrated the
absence of variations on time scales ranging from several minutes to several hours. The variability of the radial
velocity of HD 56126 also showed up when the radial-velocity measurements made with the 6-m telescope were
compared to published data [5]. Lèbre et al. [29] performed a detailed spectroscopic monitoring of HD 56126.
Fourier analysis of the available radial-velocity and photometric data led the above researchers to conclude
that the dynamical state of the atmosphere of HD 56126 is similar to that of the atmospheres of RVTau-type
variables. The above authors interpreted the variability of Hα in terms of shock propagation. Later, Lèbre
et al. [30] analyzed the variability of two lines, Hα and Hβ. They obtained additional spectroscopic data and
determined the period of radial pulsations to be P = 36.8 days.
Barthès et al. [18] analyzed all the available reliable radial-velocity measurements made for HD56126 (89
measurements over eight years) and concluded that radial velocity of this star varies with a half-amplitude
of 2.7 km/s and the main period of P = 36.8 ±0.2d. The period of photometric variability is the same and
photometric amplitude is very small, 0.m02. However, the above authors found the variability pattern of
the star to differ significantly from pulsations observed in RVTau-type stars. Judging by its temperature
[5], HD 56126 evolved further beyond the stage of RVTau-type stars. The photometric and radial-velocity
variations of HD 56126 may be due to first-overtone radial pulsations driven by shocks that generate complex
asynchronous motions in the upper hydrogen layers of the star.
Table 1 presents the radial-velocity data we obtained for HD 56126. Given that a velocity gradient is very
likely in the upper layers of the star’s atmosphere, we report here the Vr values for individual lines and
groups of lines. As is evident from Table 1, velocity variations inferred from weak absorptions (their residual
Klochkova et al.: Spectroscopy of HD56126 7
5888 5889 5890 5891
20.11.02
21.02.03
14.11.03
12.04.03
10.01.04
09.03.04
Wavelength, А
Figure 5. Spectral fragment with the D2 Nai line on different observing dates.
intensities approach 1) are within the variability limits established by Barthès et al. [18]. The positions of
the circumstellar Nai D lines and Swan bands of the C2 molecule agree well with each other and match the
expansion velocity of the shell, Vexp ≈11 km/s. Note that the position of the wind component of the Hα line
is inconsistent with those of the wind components of other lines, whereas the variations of the Hβ profile is
synchronized with those of Feii(42) lines.
When intercomparing our data and comparing it with those of other authors one must control the zero
points of the corresponding radial-velocity systems. We used interstellar and circumstellar lines to control
the radial-velocity zero points. Three blueshifted interstellar components of Nai lines in the spectrum of
HD56126, which are barely visible in Fig. 5, yield Vr values listed in Column 10–12 of Table 1. The fourth
weak component with Vr ≈46km/s is barely visible in at least three our spectra. For each component, all our
Vr estimates agree with each other and with those of Bakker et al. [19] within the quoted errors. Furthermore,
as is evident from Fig. 5, the blend consisting of the three main components has sharp boundaries, which
allow the velocity of this entire feature to be confidently measured. Its mean velocity as inferred from our
data is equal to Vr = 20.3 ± 0.3 km/s and agrees with the velocity of 20±2km/s measured by Lèbre et
al. [29] from lower-resolution spectra. Crawford and Barlow [4] showed that when observed with superhigh
resolution, the circumstellar C2 and Ki features exhibit components that are about 1 km/s apart. These
components yield the same set of velocity values, but have different intensities. This effect may cause minor
systematic differences (also on the order of 1 km/s) between the velocities inferred from circumstellar atomic
and molecular lines in lower-resolution spectra. Our measurements reveal no variations of these velocities
with time, and their mean values, 77.2±0.5 and 75.4±0.3km/s for C2 and Nai, respectively, do not disagree
systematically with the radial velocities obtained by Lèbre et al. [29], Bakker et al. [19, 20], and Crawford
and Barlow [4]: 77.3÷77.6 and 75.3÷76.8km/s for C2 and Nai, Ki, respectively.
However, when comparing our Vr values with published data, one must take into account not only method-
ological effects, but also the spectroscopic peculiarity of the object itself. Line profiles in the spectrum of
HD56126 are asymmetric and their shape varies both with time and with line intensity. We plan to under-
take a detailed analysis of the velocity field at different depths in the atmosphere and in the circumstellar
envelope of HD 56126 in a separate paper.
8 Klochkova et al.: Spectroscopy of HD56126
As for the possible binarity of HD56126, it has neither been confirmed or finally disproved. In this
connection, of certain interest is a comment by Barthès et al. [18] who pointed out a weak trend in the star’s
radial velocity over several years of observations. This trend maybe indicative of a second companion in the
system with an orbital period longer than 16 years. Our eight spectra, which we took on more recent dates,
fail to clarify the situation. It would be therefore important to follow the behavior of Vr over a several-years
period taking one to two spectra every month on a regular basis.
The radial-velocity variability of HD 56126 is not a unique phenomenon. Part of candidate PPNe also
demonstrate radial-velocity variations on a time scale of several hundred days, which may be indicative
of the binary nature of these objects. Evidence for orbital motion has been obtained for several optically
bright objects with IR excess. For example, authors of papers [31, 32] and [33] proved the binary nature,
determined the orbital elements, and proposed models for the high-latitude supergiants 89Her and HR4049,
respectively. Van Winckel et al. [34] showed that HR4049, HD44179, and HD52961 to be spectral binaries
with the orbital periods of about one to two years. The above authors concluded that all extremely metal-
deficient PPNe studied so far (HR4049, HD44179, HD52961, HD46703, and BD+39o4926) are binary stars.
The observed correlation between the binarity and the presence of a hot dust envelope indicates that binarity
promotes the formation of an envelope. Bakker et al. [16] use high-resolution spectra of HR4049 to analyze
the variations of complex emission–absorption profiles of Na D lines and Hα lines over the orbital period.
Individual components of these lines may form under different conditions: in the atmosphere of the main
star; in the disk where both components of the binary are immersed, or in the interstellar medium. For such
binaries, of fundamental importance is the determination of the systemic velocity from radio spectroscopy.
The nature of the companions of suspected binary post-AGB stars remains unclear, because we see no
direct manifestations of these companions either in the continuum or in spectral lines (all known binary
post-AGB objects belong to type SB1). These companions may be either very hot object, or main-sequence
stars of very low luminosity. For example, Bakker et al. [16] believe that the secondary companion in HR 4049
is a cold (Te = 3500K) MS star with a mass of M=0.56M⊙, although it may also be a white dwarf, like in
the case of Ba-stars [35].
Unfortunately, because of the short history of PPN studies we are so far unable to make any definitive
conclusions concerning the cause of radial-velocity variability of a representative sample of these objects.
Moreover, the observed pattern of radial-velocity variations is often complicated by differential motions in
the extended atmospheres of these objects. A detailed analysis of radial velocities based on data taken with
high spectral and temporal resolution for selected — the brightest — PPNe reveals differences in the behavior
of radial velocities inferred from lines of different excitation, which form at different depths in the atmosphere
of the star. For example, Bakker et al. [36] analyzed the spectrum of the IRAS source identified with the
peculiar supergiant HD101584 and found eight categories of spectral lines with fundamentally different
temporal behavior of profiles, half-widths, and shifts (and hence of Vr values). In particular, the highest-
excitation absorption features, which form near the star’s photosphere, exhibit radial-velocity variations due
to the orbital motion in the binary system. At the same time, low-excitation lines with PCyg-type profiles
form in the stellar-wind region and are indicative of mass outflow. The systemic velocity has been confidently
determined from radio emissions of CO and OH molecules.
5. Spectral atlas
Table 2. Spectra used to create this atlas
αPer HD56126
∆λ, Date Spect- Date Spect-
Å rograph rograph
4010–5460 11.11.05 NES 12.11.05 NES
5460–6010 12.11.05 NES 9.03.04 NES
6010–6640 4.03.99 Lynx 9.03.04 NES
6640–8790 10.03.93 Lynx
Our comparative atlas of the spectra of HD56126 and αPer includes 94 plots representing 40 Å-long
spectral fragments. Some of them are shown in Figs. 1, 3, 4 and 6 to illustrate the differences between the
Klochkova et al.: Spectroscopy of HD56126 9
6310 6320 6330 6340 6350
Figure 6. Same as Fig. 1, but for spectral fragment containing the Siii λ 6347 Å line.
intensities and profiles of lines in the spectra of two stars of similar temperature and luminosity. The full
version of the atlas is available at http://www.sao.ru/hq/ssl/Atlas/Atlas.html.
In the wavelength interval 4010–6640ÅÅ the atlas gives the complete spectra of both objects. However,
in the more long-wavelength portion, up to 8790 Å, part of the spectrum has been lost in gaps between
echelle orders and the remaining portions are overcrowded by telluric lines. The atlas therefore gives only
the most informative fragments for this part of the spectrum of HD56126.
The spectrum of HD56126 is variable — line profiles, differential line shifts, and radial velocities vary
from date to date, and therefore we performed no averaging of any kind — different spectral intervals are
represented in the atlas by different spectra indicated in Table 2. For each wavelength interval, we selected
from among the available spectra the one with the highest resolution and signal-to-noise ratio.
We supplement graphic data in the atlas with tables. In Table 3 column 1 gives the results of identification
of spectral features; column 2, the laboratory wavelengths used to measure the radial velocities; columns
3 and 5, the central residual line intensities “r”, and columns 4 and 6, the heliocentric radial velocities Vr
measured from the line cores.
To identify atomic and molecular lines in the spectrum of HD56126, we use the atlases and tables of
solar spectrum [37, 38, 39, 40], the Moore tables for multiplets [41, 42], and electronic tables to the paper
by Bakker et al. [19]. We also use VALD database [43]. We supplement the standard identification criteria
(wavelength, relative line intensity, specific line profile) by two additional ones. One of these new criteria
uses the chemical composition anomalies of HD 56126 mentioned above and the spectrum of the comparison
star. The second new criterion can be applied only to sufficiently strong lines (r < 0.5), which in some of
our spectra exhibit a sharp variation of radial velocity with line depth. Several rather strong lines remained
unidentified in the spectrum of HD56126. Some of them can be seen in the fragments of the atlas presented
here: the λ 6550 Å line in Fig.1, the λ 5845 and 5852 Å lines in Fig. 4, and the λ 6347 Å line in Fig. 6.
Compared to the lines in the spectrum of αPer, those in the spectrum of HD56126 are less blended,
because they are narrower and, in addition, many of these lines are weaker due to low metallicity of the
star. However, by no means all absorptions can be used for reliable measurement of radial velocities. Table 3
lists about one and half thousand identifications for both stars and only 940 Vr measurements for HD 56126
obtained mostly from lines with minimal blending or from lines with the strongest difference of intensity in
the spectra of two stars.
http://www.sao.ru/hq/ssl/Atlas/Atlas.html
10 Klochkova et al.: Spectroscopy of HD56126
Conclusions
We use numerous high-resolution observations (R=25000 and 60000) made with the echelle spectrographs
of the 6-m telescope to perform a detailed analysis of the optical spectrum of the post-AGB star HD56126
identified with the IR source IRAS 07134+1005. We identified numerous absorptions of neutral atoms and
ions in the wavelength interval from 4010 to 8790 ÅÅ and measured their depths and the corresponding
radial velocities. We identified absorption bands of the C2, CN, and CH molecules, and interstellar bands
(DIB). In addition to the known variability of the profile of the Hα line, we found variations of the profiles
of a number of Feii and Baii lines. We produced an atlas of the spectra of HD56126 and its comparison star
αPer.
An analysis of our radial velocities determined from all spectra of our collection leads us to conclude
that:
– the accuracy of our radial-velocity data for HD 56126 allows them to be combined with the most accurate
of earlier published measurements;
– we found the behavior of Vr values to differ for lines of different excitation degree, which form at different
depth in the stellar atmosphere. The half-amplitude of the variations of radial velocities measured from
weak absorptions (r→ 1) is equal to 2–3 km/s;
– we confirm the stability of the expansion velocity of the circumstellar envelope of HD56126 as measured
from C2 and Nai lines;
– we reveal the complex and variable shape of the profiles of strong lines (not only hydrogen lines, but
also absorption features of Feii, Yii, Baii, and other elements), which form in the expanding atmosphere
(wind base) of the star. To study the kinematic state of the atmosphere, one needs measurements of
radial velocities for individual details of these profiles;
– we demonstrate the necessity of high and even superhigh spectral resolution for studying stellar and
circumstellar lines, respectively, in the spectrum of HD56126.
Acknowledgments
This work is supported by the Russian Foundation for Basic Research (project code 05–07–90087), the
Presidium of the Russian Academy of Sciences (program “Origin and Evolution of Stars and Galaxies“,
the Branch of Physical Sciences of the Russian Academy of Sciences (program “Extended Objects in the
Universe”). This publication is based on work supported by Award No. RUP1–2687–NA–05 of the U.S.
Civilian Research and Development Foundation (CRDF).
This work makes use of the SIMBAD, NASA ADS, and VALD astronomical databases.
Klochkova et al.: Spectroscopy of HD56126 11
References
1. T. Blöcker, Astrophys. J. 299, 755 (1995).
2. S. Kwok, Annu. Rev. Astron. & Astrophys. 31, 63 (1993).
3. T. Ueta, M. Meixner, and M. Bobrowsky, Astrophys. J. 528, 861 (2000).
4. I.A. Crawford and M.J. Barlow, MNRAS 311, 370 (2000).
5. V.G. Klochkova, MNRAS 272, 710 (1995).
6. V.G. Klochkova, Bull. Spec. Astrophys. Observ. 44, 5 (1998).
7. L. Decin, H. van Winckel, C. Waelkens, and E. Bakker, Astron. & Astrophys. 332, 928 (1998).
8. V.E. Panchuk, V.G. Klochkova, I.D. Najdenov, Preprint of the Special Astrophysical Observatory of the Russian
Academy of Sciences No. 135 (1999).
9. V.E. Panchuk, N.E. PIskunov, V.G. Klochkova, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 169 (2002).
10. V.G. Klochkova, S.V. Ermakov, V.E. Panchuk, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 137 (1999).
11. V.E. Panchuk, V.G. Klochkova, I.D. Najdenov, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 139 (1999).
12. V.E. Panchuk, M.V. Yushkin, I.D. Najdenov, Preprint of the Special Astrophysical Observatory of the Russian
Academy of Sciences No. 179 (2003).
13. M.V. Yushkin, V.G. Klochkova, Preprint of the Special Astrophysical Observatory of the Russian Academy of
Sciences, No. 206 (2005).
14. G.A. Galazutdinov, Preprint of the Special Astrophysical Observatory of the Russian Academy of Sciences No. 192
(1992).
15. R. Oudmaijer and E.J. Bakker, MNRAS 271, 615 (1994).
16. E.J. Bakker, D.L. Lambert, H. van Winckel, et al., Astron. & Astrophys. 336, 263 (1998).
17. H. van Winckel, R. Oudmaijer, and N.R. Trams., Astron. & Astrophys. 312, 553 (1996).
18. D. Barthès, A. Lèbre, D. Gillet, and N. Mauron, Astron. & Astrophys. 359, 168 (2000).
19. E.J. Bakker, L.B.F.M. Waters, H.J.G.L.M. Lamers, et.al., Astron. & Astrophys. 310, 893 (1996).
20. E.J. Bakker, E.F. Dishoeck, L.B.F.M. Waters, and T. Schoenmaker, Astron. & Astrophys. 323, 469 (1997).
21. V.G. Klochkova, R. Szczerba, V.E. Panchuk, and K. Volk, Astron. & Astrophys. 345, 905 (1998).
22. V.G. Klochkova, R. Szczerba, V.E. Panchuk, Astron. Lett. 26, 88 (2000).
23. V.G. Klochkova, R. Szczerba, V.E. Panchuk, Astron. Lett. 26, 439 (2000)
24. V.G. Klochkova, E.L. Chentsov, Astron. Rep. 48, 301 (2004)
25. N. Kameswara Rao, A. Goswami, and D.L. Lambert, MNRAS 334, 129 (2002).
26. V.G. Klochkova, V.E. Panchuk, N.S. Tavolganskaya, G. Zhao, Astron. Rep. 83, 265 (2006).
27. S. Trammell, H.L. Dinerstein, and R.W. Goodrich, Astrophys. J. 108, 984 (1994).
28. V. Bujarrabal, J. Alcolea, and P. Planesas, Astron. & Astrophys. 257, 701 (1992).
29. A. Lèbre, N. Mauron, D. Gillet, and D. Barthes, Astron. & Astrophys. 310, 923 (1996).
30. A. Lèbre, A. B. Fokin, D. Barthes, D. Gillet, and N. Mauron, Astrophys. Space Sci. 265, 105 (2001).
31. A.A. Ferro, PASP 96, 641 (1984).
32. L.B.F.M. Waters, C. Waelkens, M. Mayor, and N.R. Trams, Astron. & Astrophys. 269, 242 (1993).
33. C. Waelkens, H.J.G.L.M. Lamers, L.B.F.M. Waters, et al., Astron. & Astrophys. 242, 433 (1991).
34. H. van Winckel, C. Waelkens, and L.B.F.M. Waters, Astron. & Astrophys. 293, L25 (1995).
35. R.D. McClure, MNRAS 96, 117 (1984).
36. E. J. Bakker, H.J.G.L.M. Lamers, L.B.F.M. Waters, et al., Astron. & Astrophys. 307, 869 (1996).
37. R.L. Kurucz, I. Furenlid, and J.T.L. Brault, Nat. Solar Observ. Atlas, New Mexico: National Solar Observatory
(1984).
38. L. Wallace, K. Hinkle, and W. Livingston, Nat. Solar Obs. Techn. Rep. No.00–001, Tucson (2000).
39. A.K. Pierce and J.B. Breckinridge, Contr. Kitt Peak Nat. Obs. No. 559 (1973).
40. J.W. Swensson, W.S. Benedict, L. Delbouille, and G. Roland, “The solar spectrum from λ 7498 to λ 12016. A
table of measures and identifications”, Mem. Soc. Roy. Sci. Liege, Vol.hors ser. No.5 (1970).
41. C.E. Moore, Contrib. Princeton University Observ. No.20, part I (1945).
42. C.E. Moore, Contrib. Princeton University Observ. No.20, part II (1945).
43. N.E. Piskunov, F. Kupka, and T.A. Ryabchikova, A&AS 112, 525 (1995).
12 Klochkova et al.: Spectroscopy of HD56126
Table 3. List of lines identified in the spectra of HD 56126 and αPer. Columns 3 and 5 list the central
residual intensities of the lines (the continuum level is set to 1), and columns 4 and 6, the heliocentric
velocities Vr.
αPer HD56126
Element λ Å r Vr r Vr
TiII(11) 4012.39 0.13: −2.2 0.05 81.7
FeI(557) 4013.64
FeI(485) 4013.82 0.53:
ScII(8) 4014.53 0.32: −3.5 0.49
CeII(157) 4014.90 0.56
NiII(12) 4015.47 0.50: 0.64 84.8:
CeII(256) 4015.88 0.74: 83.0:
FeI(560) 4016.42 0.74: −1.0
FeI(279) 4017.10
FeI(527) 4017.15 0.50: −1.1 0.85:
NiI(171) 4017.47 0.7: 0.9:
MnI(5) 4018.10 0.47:
FeI(560) 4018.27
ZrII(54) 4018.38 0.53 82.5
NdII(19) 4018.83 0.89:
VII(201) 4019.05 0.86: −3.0:
FeI(556) 4020.07
NdII(19) 4020.87 0.80 82.4:
CoI(16) 4020.90 0.86: −2.3
NdII(36) 4021.33 0.79 82.0:
FeI(120) 4021.61
FeI(278) 4021.87 0.45: −3.9
FeI(654) 4022.74
NdII 4023.01 0.75: 81.2:
VII(32) 4023.38 0.47: −2.5: 0.56 82.5
FeI(277) 4024.10
ZrII(54) 4024.45 0.33: 85.1:
TiI(12) 4024.58 0.37: −1.5:
TiII(11) 4025.13 0.36: −2.3 0.42: 83.5:
TiII(87) 4028.34 0.29: −1.7 0.28: 84.8:
FeI(556) 4029.63 0.43: −0.6:
ZrII(41) 4029.68 0.28 83.4:
NdII(32) 4030.47 0.60:
FeI(560) 4030.50
MnI(2) 4030.76 0.18: 0.63 81.0:
CeII(108) 4031.34 0.52
FeII(151) 4031.44
LaII(40) 4031.68 0.42 84.6:
MnI 4031.78 0.46: −2.0
FeI(44) 4032.63 0.52:
FeII(126) 4032.95 0.63
MnI(2) 4033.06 0.26: −3.3:
ZrII(42) 4034.08 0.52: 83.7
MnI(2) 4034.48 0.39: −2.6:
Klochkova et al.: Spectroscopy of HD56126 13
αPer HD56126
Element λ Å r Vr r Vr
ZrII(70) 4034.84 0.85: 83.1:
VII(32) 4035.60 0.35: 0.61 85.1
MnI(5) 4035.72
VII(9) 4036.76 0.68: −2.0 0.81 82.2:
GdII(49) 4037.39 0.90: 0.83 84.1:
CeII(218) 4037.67 0.81: 82.7:
GdII(49) 4037.90 0.85: 0.81:
NdII(31) 4038.12 0.83:
VII(32) 4039.56 0.82: −2.0 0.89:
FeI 4040.09 0.76:
ZrII(54) 4040.24 0.58 83.5
FeI(655) 4040.64 0.52:
CeII(138) 4040.76 0.52 82.6:
NdII(30) 4040.80
MnI(5) 4041.35 0.48: −2.5 0.84:
CeII(140) 4042.58 0.60:
SmII(4) 4042.72 0.59
SmII(9) 4042.90 0.53 83.1:
FeI(276) 4043.90 0.56
FeII(172) 4044.01 0.89 81.2:
FeI(359) 4044.61 0.60 −3.3:
GdII(49) 4045.15 0.72:
ZrII(30) 4045.63
FeI(43) 4045.81 0.12 −4.6 0.22:
FeI(557) 4046.06
VII(177) 4046.27
CeII(81) 4046.34 0.72 80.5
ZrII(43) 4048.68 0.29 84.2
MnI(5) 4048.75 0.39 −4.3
ZrII(43) 4050.32 0.66 0.34 82.6:
VII(32) 4051.04
NdII(66) 4051.15 0.69 0.75
FeI(700) 4051.31
CrII(19) 4051.97 0.54 0.64:
TiII(87) 4053.82 0.33 0.39 83.2
FeI(698) 4054.82 0.51
CeII(82) 4054.99 0.70 81.2:
MnI(5) 4055.54 0.68 −3.1
TiII(11) 4056.19 0.60 −0.6 0.79 84.7
FeII(212) 4057.46 0.78 85:
MgI(16) 4057.50 0.48 −4.9
CoI(16) 4058.22 0.75 −4.2: 0.89
FeI(120) 4058.76 0.66 0.91
MnI(5) 4058.92
FeI(767) 4059.79 0.82 −3.3:
NdII(63) 4059.96 0.88
NdII(10) 4061.08 0.75 −2.4 0.66 81.0:
FeII(189) 4061.79 0.84:
CeII(34) 4062.23 0.79 82.3
14 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(359) 4062.44 0.56 −1.0
FeI(43) 4063.59 0.19 −4.0: 0.40 82.9
TiII(106) 4064.37 0.67 −1.5: 0.82 81.1:
VII(215) 4065.09 0.74 0.78
FeI(698) 4065.38
NiII(11) 4067.03 0.38 0.59 83.8
CeII(22) 4067.28 0.64 86:
FeI(559) 4067.98 0.54 −3.1 0.87 83.0
CeII(82) 4068.84 0.75 81.8
FeI(558) 4070.78 0.60
ZrII(54) 4071.09 0.59 82.3:
FeI(43) 4071.74 0.23 −3.8 0.46 82.8
CrII(26) 4072.56 0.68 −3.1 0.77 85.5:
CeII(109) 4072.92 0.78 83.8:
CeII(4) 4073.48 0.61 83.4:
FeI(558) 4073.76 0.64
GdII(44) 4073.76 0.70:
FeI(524) 4074.79 0.61 −2.8 0.95:
NdII(62) 4075.12 0.85:
CeII(57) 4075.70
SmII(51) 4075.85 0.53 −2.3: 0.51
FeI(558) 4076.63
LaII(11) 4076.71 0.37 −3.3: 0.74:
ZrII(54) 4077.05 0.53:
CrII(19) 4077.50
SrII(1) 4077.71 0.09 −2.8 0.10
DyII 4077.96
CeII(19) 4078.32 0.67:
FeI(217) 4078.35 0.56: −0.7:
MnI(5) 4079.3: 0.58 0.95:
FeI(359) 4079.84 0.69 −2.1:
FeI(558) 4080.21 0.74
CeII(44) 4080.44 0.72 82.4:
CrII(165) 4081.21 0.80: 0.74 82.4:
CrII(165) 4082.29 0.77
CeII(60) 4083.23 0.61 82.2
MnI(5) 4083.63 0.52 −1.8:
FeI(698) 4084.49 0.62 −1.9: 0.88
CeII(172) 4085.23 0.51 0.70 85.6
FeI(559) 4085.30
VII(214) 4085.67 0.61
ZrII(54) 4085.68 0.61 84.8:
CrII(26) 4086.13 0.70 −3.3: 0.85 84.0:
LaII(10) 4086.71 0.62 −2.1: 0.47 83.0
FeII(28) 4087.28 0.65 0.72 84.6:
FeII(39) 4088.75 0.74 −2.9:
CrII(19) 4088.90 0.76
ZrII(29) 4090.52 0.70 −3.7 0.43 82.4
CoI(29) 4092.39 0.62:
Klochkova et al.: Spectroscopy of HD56126 15
αPer HD56126
Element λ Å r Vr r Vr
HfII(6) 4093.16 0.84: −3.2: 0.65: 82.5
CeII(160) 4093.96 0.83: 82.0:
CaI(25) 4094.93 −1.1:
FeI(217) 4095.98
ZrII(15) 4096.63 0.50 83.6
FeI(558) 4097.08 −3.2:
Hδ 4101.74 0.08 −2.0 0.06 96.0:
SiI(2) 4102.94 −2.9:
DyII 4103.31 81.2:
FeI(356) 4104.12 −1.6:
CeII(156) 4105.00 0.67:
CeII(160) 4106.13 0.79:
FeI(217) 4106.26 0.64:
CeII(139) 4106.88 0.78:
SmII(50) 4107.39 0.63: 85.1:
FeI(354) 4107.49 0.47 −3.4
CaI(39) 4108.53 0.76:
FeI(558) 4109.06 0.67:
NdII(17) 4109.07 0.72: 83.3
NdII(10) 4109.46 0.61: 82.0
MgII(21) 4109.54
FeI(357) 4109.80 0.51:
ZrII(30) 4110.05 0.62: 82.4
CeII(29) 4110.39 0.74: 83.6:
CrII(18) 4110.99 0.52 −3.5 0.64 83.0:
CeII 4111.39 0.75:
FeII(188) 4111.90 0.75: 0.86 82.3
FeI(695) 4112.32 0.80:
CrII(18) 4112.55 0.91 82.5:
FeI(1103) 4112.96 0.62:
CrII(18) 4113.22 0.86 83.6
CeII(137) 4113.73 0.86 0.80 81.8:
FeI(357) 4114.45 0.69 −2.7 0.95: 82.5:
KII(2) 4114.99
CeII(22) 4115.37 0.79 81.6
CrII(181) 4116.66 0.86
CeII(35) 4117.01 0.79 82.4:
CeII(77) 4117.29 0.83: 82:
FeI(700) 4117.85
CeII(11) 4118.15 0.83: 0.69 81.7
FeI(801) 4118.54 0.38
SmII(51) 4118.55 0.72
CeII(89) 4119.01 0.83 80.7:
FeII(21) 4119.51 0.65: −1.6 0.77:
CeII(22) 4119.79 0.64 85:
FeI(423) 4120.21 0.72:
CeII(112) 4120.83 0.87 0.71 81.0
CoI(28) 4121.32 0.67: −1.6: 0.95:
FeI(356) 4121.81 0.70: −2.3 0.92
16 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(28) 4122.66 0.37 −4.6 0.50 82.5
LaII(41) 4123.23 0.59 0.46 83.8:
FeI(217) 4123.75 0.62
CeII(60) 4123.87 0.62 81.5
FeII(22) 4124.78
YII(14) 4124.91 0.52 0.46
FeI(1103) 4125.62
FeI(354) 4125.88 0.71: 0.95:
FeI(695) 4126.18 0.69: −3.8: 0.97 85:
CeII(4) 4127.37 0.65 82.4
FeI(357) 4127.61
FeI(558) 4127.80 0.42: 0.68:
SiII(8) 4128.07 0.41: −1.5: 0.50 84.2
FeII(27) 4128.74 0.49 0.63 82.7
CeII(227) 4129.18 0.61: 0.75
EuII(1) 4129.72 0.60 0.85 81.1:
BaII(4) 4130.65 0.44
CeII(209) 4130.71 0.56
FeI(43) 4132.06 0.26 −1.5 0.58 83.4:
FeI(357) 4132.90 0.60 −4.5:
CeII(4) 4133.80 0.61 −2.0 0.58 82.0
FeI(357) 4134.68 0.46 0.83 83.6
NdII 4135.33 0.83 0.73
CeII(188) 4135.44
FeI(726) 4137.00 0.61 −3.0
CeII(2) 4137.65 0.67 0.57: 80.7:
FeII(150) 4138.21 0.78:
FeII(39) 4138.40 0.70 0.73:
FeI(18) 4139.93 0.82 −4.1
FeI(695) 4140.41 0.86 −2.1
LaII(40) 4141.73 0.72 81.2
HfII(87) 4141.84 0.77:
CeII(10) 4142.40 0.68 0.69 81.8
VII(226) 4142.90 0.79
FeI(523) 4143.42 0.41: 0.78 82.7
FeI(43) 4143.87 0.29 −2.7 0.59 82.1
CeII(3) 4144.49 0.86 −1.8: 0.76 83.6
CeII(9) 4145.00 0.80 0.70 81.7
CrII(162) 4145.76 0.82
CeII(203) 4146.23 0.68 82.2
FeI(42) 4147.67 0.56 −3.7: 0.93 84.0:
ZrII(41) 4149.20 0.37 0.37
FeI(694) 4149.36
CeII 4149.94 0.72 0.61 81.0:
FeI(695) 4150.25 0.76
ZrII(42) 4150.97 0.67 −3.2 0.43 82.8
CeII(2) 4151.97 0.55 82.1
FeI(18) 4152.17 0.45
FeI(695) 4153.90 0.49 −0.2: 0.85 82.3
Klochkova et al.: Spectroscopy of HD56126 17
αPer HD56126
Element λ Å r Vr r Vr
FeI(355) 4154.50 0.43 0.88 83.2
FeI(694) 4154.81 0.88 83.5
ZrII(29) 4156.25 0.43 −4.2: 0.38 80.9:
FeI(354) 4156.80 0.46
FeI(695) 4157.78 0.58 −3.2
FeI(695) 4158.80
HfII(41) 4158.90 0.64
CeII(246) 4159.03 0.80 80.6:
ZrII(42) 4161.21 0.35 84.2:
TiII(21) 4161.52 0.35 0.41 81.2:
SrII(3) 4161.80 0.49
TiII(105) 4163.64 0.33 −2.4 0.38 82.6
CeII(10) 4165.59 0.72 0.64 83.7
BaII(4) 4166.00 0.75 82.0
MgI(15) 4167.27 0.53 −2.1 0.79 83.2
CeII(29) 4167.80 0.74 0.85 82.7
CeII(173) 4169.88 0.76 0.71
FeI(482) 4170.91 0.52
TiII(105) 4171.90 0.41 84.3
FeI(650) 4171.91 0.28
FeI(689) 4172.64 0.85 81.8:
FeI(19) 4172.75 0.46
FeII(27) 4173.46 0.22 −1.2 0.34 84.4
TiII(105) 4174.07 0.49 −2.2 0.74 84.2:
FeI(19) 4174.91 0.63 −2.9
FeI(354) 4175.64 0.53 −2.0 0.78 83.2
FeI(689) 4176.57 0.60 −0.6 0.82
FeI(18) 4177.59 0.22
FeII(21) 4177.68 0.29: 83.0:
FeII(28) 4178.85 0.31 −1.5 0.38 84.5
CrII(26) 4179.43 0.49 0.60 83.9:
ZrII(99) 4179.81 0.49 82.4
FeI(354) 4181.75 0.38 −1.0: 0.78 83.4
FeI(476) 4182.39 0.71: −2.1
VII(37) 4183.45 0.60 0.82 81.1:
TiII(21) 4184.31 0.49 0.62 82.0:
FeI(355) 4184.89 0.59 −1.8 0.87 85.1:
CeII(124) 4185.33 0.93: 0.84 82.0
CeII(1) 4186.61 0.43 85.8:
FeI(152) 4187.04 0.41 −2.4 0.71 82.8:
FeII(152) 4187.80 0.36 −4.5 0.69 82.9
FeI(1116) 4188.73 0.68 −1.4 0.96 83.6
PrII(8) 4189.52 0.90: 83.1
FeI(940) 4189.56 0.84
TiII(21) 4190.29 0.67 −2.4 0.89 82.3
VII(25) 4190.40
CeII(169) 4190.63 0.87 80.8:
GdII(34) 4191.07 83.2:
FeI(152) 4191.43 0.38
18 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
ZrII(108) 4191.50 0.57
LaII(78) 4192.35 0.87:
CeII(79) 4193.10 0.87 0.72 84.0:
CeII(85) 4193.87 0.89 0.84 81.5
FeI(693) 4195.33 0.50 0.87 83.7:
CrII(161) 4195.41
FeI(693) 4196.21 0.58
LaII(41) 4196.55 0.60:
CeII(136) 4197.67 0.81
CeII(209) 4198.00 0.79
FeI(152) 4198.30 0.30 0.68
CeII(207) 4198.43
CeII(7) 4198.67 0.64 81.1:
FeI(522) 4199.09 0.40
FeII(141) 4199.09
NdII(15) 4199.10
YII(5) 4199.27 0.60
FeI(3) 4199.99 0.85
FeI(689) 4200.93 0.73 −2.6:
FeI(42) 4202.03 0.28 0.58 82.9
VII(25) 4202.34 0.80 82.6
CeII(186) 4202.94 0.78 0.71 82.6
LaII(53) 4204.03 0.52 −2.5: 0.80 81.9:
YII(1) 4204.75 0.50 80.8
VII(37) 4205.07 0.41 −3.0 0.65
MnII(2) 4205.39 0.51 0.79:
ZrII(133) 4205.91 0.84 81.1
HfII(74) 4206.59 0.85 83.7:
FeI(3) 4206.70 0.67 −1.2
MnII(2) 4207.23 0.66 −3.2:
CrII(26) 4207.35 0.92 83.1
FeI(689) 4208.61 0.66:
ZrII(41) 4208.98 0.56 −2.3
CrII(162) 4209.02 0.42 82.6:
CeII(3) 4209.41
VII(25) 4209.74 0.73 0.88 83.5:
FeI(152) 4210.35 0.47 −1.0
ZrII(97) 4210.62 0.64 82.3
ZrII(15) 4211.89 0.57 −2.6 0.39 83.5
CeII(169) 4213.04 0.88
FeI(355) 4213.65 0.71 −2.5 0.95:
CeII(203) 4214.03 0.84 82.5
FeI(274) 4215.43
SrII(1) 4215.52 0.15 −0.6 0.16 96.9
FeI(3) 4216.18 0.51 −2.9
CdII(49) 4217.20 0.88 82.5:
FeI(693) 4217.55 0.61 −2.6 0.75 83.3
FeI(800) 4219.36 0.51 −2.1 0.85 83.7
CaII(16) 4220.13 0.88:
Klochkova et al.: Spectroscopy of HD56126 19
αPer HD56126
Element λ Å r Vr r Vr
NdII(32) 4220.26 0.68
FeI(482) 4220.35
FeII(152) 4222.21 0.48
ZrII(80) 4222.41
CeII(36) 4222.60 0.52:
FeI(689) 4224.17
ZrII(29) 4224.28 0.50: 0.66 81.0
FeI(689) 4224.52
CrII(162) 4224.85 0.83 83.6
VII(37) 4225.22
PrII(8) 4225.33 0.73:
FeI(693) 4225.45 0.44
FeI(521) 4225.95 0.74:
CaI(2) 4226.72 0.21 −3.6 0.43 80.7:
FeI(693) 4227.43 0.32 −4.7 0.59:
NdII(19) 4227.72 0.73: 82.6
NdII(36) 4228.20
CI 4228.32 0.86 0.77 81.9
SmII(4) 4229.70 0.76 0.92:
FeI(41) 4229.76
LaII(83) 4230.95 0.92 83.2:
NiI(136) 4231.03 0.91
ZrII(99) 4231.64 0.52 83.5
HfII(72) 4232.43 0.86: 0.78 82.2
FeII(27) 4233.17 0.23 0.34 86.5
FeI(152) 4233.60 0.40:
NdII(20) 4234.20 0.83 81.9
VII(24) 4234.22 0.83
MnI(23) 4235.14
MnI(23) 4235.29 0.73
VII(5) 4235.74 0.46
FeI(152) 4235.94 0.31
ZrII(110) 4236.54 0.84: 0.64 83.0
LaII(41) 4238.38 0.63 82.3
FeI(693) 4238.81 0.52 −2.6 0.79 81.6
FeI(18) 4239.85 0.51 −3.8 0.67
CeII(2) 4239.91
FeI(764) 4240.38
CaI(38) 4240.45 0.77
CrII(31) 4242.37 0.47 −1.2 0.53 83.3
NiII(9) 4244.80 0.84 0.88 81.0:
FeI(352) 4245.26 0.61 0.94
FeI(691) 4245.35
HfII(72) 4245.84 0.72
CeII(158) 4245.98
FeI(906) 4246.09 0.69
ScII(7) 4246.83 0.25 −2.1 0.39 88.7:
NdII(14) 4246.88
FeI(693) 4247.42 0.47 −2.7
20 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(482) 4248.23 0.72
CeII(1) 4248.68 0.82 −2.8: 0.69 81.8
FeI(152) 4250.12 0.41 −1.7 0.69 82.6
FeI(42) 4250.79 0.33 −2.2 0.58 81.8
GdII(15) 4251.74 0.84 0.80 82.1
CrII(31) 4252.63 0.64 −3.0 0.74 82.4
CeII(77) 4253.36 0.81 82.5
CrI(1) 4254.34 0.35 −1.3 0.68 82.8
CeII(81) 4255.78 0.76 83.0
CeII(172) 4256.16 0.83:
NdII(59) 4256.24 0.81 −3.1 0.84:
CeII(123) 4257.12 0.92 81.0:
ZrII(15) 4258.05
FeII(28) 4258.15 0.34 −0.5 0.36
FeI(3) 4258.32
FeI(476) 4260.13
FeI(152) 4260.47 0.31 −1.5 0.57 83.2
CeII(19) 4261.16 0.95 81.2
CrII(31) 4261.92 0.49 −2.2 0.55 83.5
SmII(37) 4262.68 0.94 81.5:
CeII(254) 4263.43 0.78
FeI(692) 4264.21 0.84 −2.3
CeII(239) 4264.37 0.91 81.2
FeI(993) 4264.74 0.90
YII(71) 4264.88 0.78
ZrII(98) 4264.92
FeI(993) 4265.26 0.87
MnI(23) 4265.92 0.91 −2.5
ZrII(8) 4266.72 0.86 82.9
FeI(273) 4266.97 0.78 −3.8
FeI(482) 4267.83 0.73 −1.9 0.93 84:
CrII(192) 4268.93 0.75:
CI(16) 4269.02 0.68
CrII(31) 4269.29 0.65 0.69:
CeII(204) 4270.19 0.90 −2.8 0.77 81.5
CeII(21) 4270.72 0.82 81.0:
FeI(152) 4271.16 0.40 −2.7 0.70 82.0
FeI(42) 4271.76 0.25 −1.3 0.44 82.8
FeII(27) 4273.32 0.44 0.43:
ZrII(28) 4273.52
FeI(478) 4273.88 0.90:
CrI(1) 4274.79 0.37 −2.1 0.72 82.7
CrII(31) 4275.56 0.54 −1.7 0.57 83.6
FeI(597) 4276.68 0.87
ZrII(40) 4277.37 0.84 0.70 82.4
FeII(32) 4278.16 0.59 −1.6 0.71 82.8
VII(225) 4278.89 0.90 0.83 82.4:
SmII(27) 4279.68 0.92 82.7:
FeI(351) 4279.87 0.82
Klochkova et al.: Spectroscopy of HD56126 21
αPer HD56126
Element λ Å r Vr r Vr
CeII(225) 4280.14 0.88 82.2:
GdII(15) 4280.48 0.82 0.89 82.4
SmII(46) 4280.79 0.84:
SmII 4281.01
CrII(17) 4281.03 0.79
MnI(23) 4281.10
ZrII(182) 4282.21 0.58
FeI(71) 4282.40 0.41 −1.7
CaI(5) 4283.01 0.58 −2.3 0.92 81.7
CrII(31) 4284.20 0.60 −1.2 0.69 83.1
MnII(6) 4284.43 0.82: 83.0:
NdII(10) 4284.51
CeII(11) 4285.37 0.82 82.8
FeI(597) 4285.44 0.71 −2.3
TiI(44) 4286.01 0.84
FeI(414) 4286.47 0.84 −1.9
ZrII(69) 4286.51 0.63 82.6
LaII(75) 4286.97 0.76 −3.3 0.75 81.7
TiII(20) 4287.88 0.36 0.1 0.51 82.9
CeII(135) 4289.45 0.79 82.0:
CrI(1) 4289.72 0.33:
TiII(41) 4290.21 0.24 −2.0: 0.36 85.0:
TiI(44) 4290.94 0.79 −3.5:
FeI(3) 4291.46 0.76 −1.4
MnII(6) 4292.25 0.82
CeII(205) 4292.77 0.88 83.0:
ZrII(110) 4293.14 0.91 0.63 82.0
TiII(20) 4294.10 0.28 −2.2 0.37 83.9
FeI(41) 4294.12
ScII(15) 4294.78 0.55 −2.3 0.73 82.5
LaII(53) 4296.05 0.73 0.65 83.1:
FeII(28) 4296.57 0.35 −0.4 0.37
CeII(2) 4296.68
PrII(7) 4297.76 0.92 84.3:
FeII(520) 4298.04 0.78
FeI(152) 4299.23 0.31 0.60
CeII(47) 4299.36
TiII(41) 4300.05 0.24 −0.7 0.31 93.0:
TiI(44) 4301.09 0.74:
ZrII(109) 4301.81
TiII(41) 4301.92 0.31 −0.8 0.40 81.5
CaI(5) 4302.53 0.46 −3.0: 0.79 83.2
FeII(27) 4303.17 0.34 −1.7 0.41 84.2:
NdII(10) 4303.59
FeI(414) 4304.55 0.86 −3.4
FeI(476) 4305.45 0.49 83.5:
ScII(15) 4305.71 0.37
CeII(1) 4306.72 0.81 0.75 82.3
CaI(5) 4307.75
22 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
TiII(41) 4307.89 0.21 −3.7: 0.40 82.4
FeI(42) 4307.90
ZrII(88) 4308.94 0.70 82.4
FeI(849) 4309.03 0.72:
YII(5) 4309.63 0.38 0.40 84.8:
CeII(126) 4309.74
CeII(133) 4310.70 0.91 82.1
ZrII(99) 4312.23 0.84 82.9
TiII(41) 4312.86 0.33 −2.3 0.41 83.5
ScII(15) 4314.09 0.22 0.36:
FeII(32) 4314.30
TiII(41) 4314.98 0.25 −1.1 0.43 83.8
GdII(43) 4316.05 0.97: 0.95 82.0:
TiII(94) 4316.80 0.58 −1.6 0.69 82.7
ZrII(40) 4317.32 0.82: 0.56 81.9
CaI(5) 4318.65 0.56 −0.1 0.90 83.4:
ScII(15) 4320.74 0.22 0.38
TiII(41) 4320.95
FeI 4321.79 0.87 −1.9
LaII(25) 4322.50 0.88 −0.9 0.75 82.7
ZrII(141) 4323.62 0.91 81.0
FeI(70) 4325.00
ScII(15) 4325.01 0.33 −2.6 0.46 81.9:
FeI(42) 4325.76 0.25 −2.4 0.43 81.4:
BaII(7) 4326.74 0.73 0.90
MnII(6) 4326.76
FeI(761) 4327.10
GdII(15) 4327.13 0.75 0.92 82.5
FeI(597) 4327.91 0.83 −1.6 0.89 83.0
SmII(15) 4329.03 0.89 −2.8 0.92
TiII(94) 4330.24 0.51 0.64
CeII(82) 4330.45
TiII(41) 4330.70 0.44 −3.5 0.59 81.8:
NiI(52) 4331.65 0.77 −2.7
VII(23) 4331.79 0.87
ZrII(132) 4333.28 0.59: 82.1
LaII(24) 4333.76 0.59 −0.7 0.53: 82.4
LaII(77) 4334.96 0.80: 81.7:
CaII(89) 4336.26 0.69:
FeI(41) 4337.05 0.36:
TiII(94) 4337.33
CeII(82) 4337.78 0.38:
TiII(20) 4337.92 0.23: −3.7: 0.33
NdII(68) 4338.70 0.49: 0.52 82.5:
Hγ 4340.47 0.09 −2.1 0.08 97.0:
TiII(32) 4341.36 0.30:
FeI(645) 4343.26 0.61:
TiII(20) 4344.29 0.30: 0.47: 82.1
CeII(251) 4345.96 0.80:
Klochkova et al.: Spectroscopy of HD56126 23
αPer HD56126
Element λ Å r Vr r Vr
FeI(598) 4346.56 0.74:
FeI(828) 4347.84 0.78
FeI(414) 4348.94 0.85: −1.8:
CeII(59) 4349.79 0.85 0.78 81.2
VII(36) 4349.97
TiII(94) 4350.84 0.52 0.71 83.2
FeII(27) 4351.77 0.23 −1.1 0.36: 85.6:
MgI(14) 4351.91
FeI(71) 4352.73 0.53 −2.5
CeII(220) 4352.73 0.76
FeII(213) 4354.36
LaII(58) 4354.40 0.70 83.3:
ScII(14) 4354.61 0.58 −5.7:
CaI(37) 4355.19 0.81 −3.3:
FeII 4357.57 0.90 83.8:
NdII(10) 4358.17 0.80 81.6
NdII(57) 4358.70
YII(5) 4358.72 0.58 −5.6 0.48 83.7
NiI(86) 4359.63
GdII(67) 4359.64 0.57
ZrII(79) 4359.74 0.43 82.8
FeII 4361.25 0.93 −1.7 0.92:
CeII(157) 4361.66 0.92:
SmII(45) 4362.04
NiII(9) 4362.09 0.80 −2.0 0.86 82.5
LaII(133) 4363.05 0.93 −1.9 0.95:
MoII(3) 4363.64 0.92: 81.5:
GdII(33) 4364.14 0.91: 81.9:
YII(70) 4364.17 0.96
CeII(135) 4364.66 0.88 −1.9 0.74 81.4
LaII(53) 4344.66
FeI(415) 4365.90 0.92
FeI(414) 4367.58
TiII(104) 4367.66 0.41 −0.6: 0.56 82.6
FeI(41) 4367.91
CeII(227) 4368.23 0.82: 0.79 83.0:
FeII 4368.26
NdII(11) 4368.63 0.93: 0.91: 82.3:
FeII(28) 4369.40 0.53 0.67 83.1
FeI(518) 4369.77 0.66: 0.90:
ZrII(79) 4370.96 0.73: 0.48 81.9
CI(14) 4371.37 0.69: 0.70 83.2:
FeII(33) 4372.22 0.92 0.92
FeI(214) 4373.57 0.83
CeII(202) 4373.82 0.83 81.5:
ScII(14) 4374.46 0.30 0.43
TiII(93) 4374.82 0.28 0.44: 81.6:
YII(13) 4374.94 0.29: 94.7:
NdII(8) 4375.04
24 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(2) 4375.93 0.49 −2.1 0.78 81.1
FeI(471) 4376.78 0.91 −1.5
MoII(3) 4377.77 0.94: −3.1: 0.92 82.3:
LaII(77) 4378.10 0.93
VI(22) 4379.23 0.82 −1.2:
ZrII(88) 4379.78 0.70 −3.3
CeII(155) 4380.06 0.43 83.0
CdII(68) 4380.64 0.91 0.98:
CeII(2) 4382.17 0.87 −2.9 0.73: 81.2:
FeI(799) 4382.78 0.82 −1.7:
ZrII(97) 4383.10 0.85:
FeI(41) 4383.54 0.25 −2.2 0.40 82.6
FeII(32) 4384.32 0.50 0.61 83.9
ScII(14) 4384.81 0.46 0.74
FeII(27) 4385.38 0.36 −2.2 0.44 84.0
NdII(50) 4385.66
CeII(57) 4386.84
TiII(104) 4386.85 0.51 0.57 81.0:
FeI(476) 4387.90 0.79
CeII(5) 4388.01 0.87 81.0:
FeI(830) 4388.41 0.72 −2.2
ZrII(140) 4388.50 0.90 80.0:
FeI(2) 4389.25 0.90 −3.1
VI(22) 4389.99 0.87 −2.0:
MgII(10) 4390.56 0.76
FeI(414) 4390.96
TiII(61) 4391.02 0.48 0.67 82.2
CeII(81) 4391.66 0.76 0.66 82.1
TiII(51) 4394.04 0.44 −2.6 0.54 83.2
TiII(19) 4395.03 0.25 −1.5 0.36 87.7
TiII(61) 4395.84 0.48 −2.5 0.58 83.0
YII(5) 4398.02 0.49 0.44 84.1
TiII(61) 4398.29
CeII(81) 4398.79 0.89 80.4:
CeII(81) 4399.20 0.75 82.4
TiII(51) 4399.77 0.34 −2.3 0.44 83.1
ScII(14) 4400.40 0.36 0.50 83.3
NdII(10) 4400.83 0.80
FeII(828) 4401.29 0.55
ZrII(68) 4401.35 0.84 83.6:
ZrII(79) 4403.35 0.76 0.60 81.9
FeI(41) 4404.75 0.28 −1.6 0.49 82.5
VI(22) 4406.65 0.90 −3.3
GdII(103) 4406.67 0.94 81.9:
CeII(64) 4407.28 0.90 81.1:
FeI(68) 4407.70 0.56 −2.6 0.79 81.5
FeI(68) 4408.42 0.58 −2.2 0.92 83.0:
PrII(4) 4408.84 0.85 82.0
TiII(61) 4409.24 0.50 0.77:
Klochkova et al.: Spectroscopy of HD56126 25
αPer HD56126
Element λ Å r Vr r Vr
TiII(61) 4409.52 0.75:
NiI(88) 4410.52
CeII(33) 4410.64 0.79:
TiII(115) 4411.08 0.58 −2.8 0.62 82.3
TiII(61) 4411.93 0.64 −1.1 0.78 84.2:
NdII(9) 4412.27 0.93
FeII(32) 4413.59 0.69 0.3: 0.79 84.5:
PrII(26) 4413.77
ZrII(79) 4414.54 0.82: 0.55 82.5
FeI(41) 4415.12 0.29 −0.7: 0.57 83.4
ScII(14) 4415.56 0.38: 0.54 82.3
FeII(27) 4416.82 0.38 −2.0 0.43 83.4
TiII(40) 4417.72 0.34 −2.2 0.41 82.9
TiII(51) 4418.34 0.48 −2.1 0.59 82.2
CeII(2) 4418.78 0.85: 0.70 81.6
SmII(32) 4420.53 0.87
ScII(14) 4420.67 0.79
SmII(37) 4421.13 0.94 0.88 82.3
TiII(93) 4421.94 0.58 −1.9 0.68 82.9
FeI(350) 4422.57 0.55 −1.4
YII(5) 4422.59 0.46 82.7
FeI(412) 4423.14 0.76
TiII(61) 4423.22 0.92 82.9
CeII(21) 4423.68 0.89 81.2
FeI(830) 4423.84 0.88
SmII(45) 4424.34 0.82 −4.2: 0.83 81.4
CaI(4) 4425.44 0.62 −1.5 0.93 81.3
FeI(2) 4427.31 0.46 0.87: 81.7:
TiII(61) 4427.90 0.82 −2.2: 0.79 82.5
CeII(19) 4429.27 0.86 −3.1 0.73 83.0
LaII(38) 4429.92 0.68 0.60 81.3
FeI(68) 4430.62 0.63 −2.9 0.95 81.3:
ScII(14) 4431.37 0.75 −2.7 0.92 81.3
TiII(51) 4432.10 0.79 0.94 83.6
LaII(11) 4432.95 0.94
FeI(830) 4433.22 0.77 −2.0
GdII(82) 4433.64 0.93
SmII(41) 4433.89 0.76 0.84 84.5:
SmII(36) 4434.32 0.86 80.7
CaI(4) 4434.96 0.49 0.0 0.89 82.2
FeI(2) 4435.15
EuII(4) 4435.58 0.89 83.9:
CaI(4) 4435.68 0.57
GdII(117) 4436.23 0.89 0.95
FeI(516) 4436.93 0.88 −1.4
CeII(169) 4437.61 0.95: −1.0: 0.93 81.7
GdII(67) 4438.13 0.97:
GdII(44) 4438.27
FeI(828) 4438.35 0.91 −2.7
26 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(32) 4439.16 0.95 −3.8 0.95 83.0:
FeI 4439.89 0.95
ZrII(79) 4440.45 0.81 −1.3: 0.57 83.4
CeII(238) 4440.88 0.89 0.89:
TiII(40) 4441.73 0.55 −2.0 0.69 82.8
FeI(68) 4442.34 0.52 −0.9
ZrII(53) 4442.50 0.72 80.8:
ZrII(88) 4443.00 0.53 0.43 83.1
FeI(350) 4443.20
TiII(19) 4443.80 0.29 −1.5 0.42 86.8
LaII(133) 4443.94
TiII(31) 4444.56 0.46 −2.9 0.56 83.3
ZrII(96) 4445.88 0.87 84.8
NdII(49) 4446.39 0.86 −2.3: 0.84 80.3
FeI(68) 4447.72 0.56 −1.6 0.89 83.1
CeII(202) 4449.33 0.81 0.74 82.4
FeII(222) 4449.66 0.88 0.85 82.0:
TiII(19) 4450.48 0.34 −1.4 0.47 84.7
FeII 4451.55 0.73 82.9
MnI(22) 4451.59 0.71 −2.9:
NdII(6) 4451.98 0.93:
SmII(26) 4452.73 0.91 0.91 81.0:
TiI(113) 4453.32 0.87
VII(199) 4453.35
FeII(350) 4454.39
SmII(49) 4454.63
CaI(4) 4454.78 0.41 −1.5 0.52 84.4
FeII 4455.26 0.89
LaII(53) 4455.79 0.87
CaI(4) 4455.89 0.63 −3.2
NdII(50) 4456.39 0.90 82.9
CaI(4) 4456.62 0.78 0.91 83.8:
ZrII(79) 4457.42 0.62 82.4
TiI(113) 4457.44 0.75
FeI(992) 4458.08
MnI(28) 4458.25 0.78
SmII(7) 4458.52 0.93 81.4
FeI(68) 4459.12 0.46 −1.8 0.85 82.1
CeII(2) 4460.21 0.77 −0.7 0.67 82.0
ZrII(67) 4461.22 0.52 82.9:
FeI(2) 4461.65 0.43
FeI(471) 4462.00
NdII(54) 4462.41 0.85
NdII(50) 4462.98 0.88 0.82 82.1
CeII(20) 4463.41 0.83 81.2
TiII(40) 4464.45 0.39 0.52 83.4:
MnI(22) 4464.68
HfII(72) 4466.41
CI 4466.48 0.76 84.3
Klochkova et al.: Spectroscopy of HD56126 27
αPer HD56126
Element λ Å r Vr r Vr
FeI(350) 4466.55 0.52 −2.1
SmII(53) 4467.34 0.88 1.2 0.82
TiII(31) 4468.49 0.29 −1.8 0.41 86.9
TiII(18) 4469.16 0.73 82.7
FeI(830) 4469.37 0.46
TiII(40) 4470.85 0.50 −1.7 0.62 84.0:
CeII(8) 4471.24 0.68 81.6:
FeI(595) 4472.72
FeII(37) 4472.92 0.52 0.64 82.9
FeII(17) 4474.19 0.96 0.98 81.0:
VII(199) 4475.70 0.98:
FeI(350) 4476.02 0.52 −1.1 0.88 84.0
YI(14) 4477.46 0.91 −1.8
CI 4477.47 0.85 82.5
CI 4478.59
SmII 4478.66 0.85 −1.2 0.81: 81.5
GdII(15) 4478.80
CI 4478.83 0.85:
CeII(203) 4479.36 0.77 81.7:
CeII(124) 4479.43
FeI(828) 4479.61 0.80:
FeI(515) 4480.14 0.82
MgII(4) 4481.22 0.28 −2.2 0.26 82.5
ZrII(131) 4482.04
FeI(2) 4482.17 0.48 0.86:
FeI(68) 4482.26
TiI(113) 4482.74 0.85 −2.0:
GdII(62) 4483.33 0.97 0.93 84.4
CeII(3) 4483.90 0.79 81.7
FeI(828) 4484.23 0.73
4484.80 0.92
ZrII(79) 4485.44 0.83 84.4
FeI(830) 4485.68 0.81 −3.6
HfII(23) 4486.14 0.97 83.4
CeII(57) 4486.91 0.85 −1.0 0.74 81.7
TiII(115) 4488.33 0.52 −3.9 0.60 82.7
FeII(37) 4489.17 0.42 −2.7 0.53 83.2
FeI(2) 4489.74 0.73:
FeI(973) 4490.77 0.83 −3.0: 0.97
FeII(37) 4491.40 0.42 −1.5 0.51 83.2
TiII(18) 4493.52 0.67 −1.5 0.81 81.7
ZrII(130) 4494.41 0.54 84.0:
FeI(68) 4494.56 0.47 −3.6
CeII(154) 4495.39
ZrII(79) 4495.44 0.82 0.76 82.7
TiII(40) 4495.46
FeII(147) 4495.52
TiI(146) 4496.15 0.88
TiI(8) 4496.25 0.90 82.5:
28 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CrI(10) 4496.86
ZrII(40) 4496.96 0.56 0.45 84.3
CeII(19) 4497.84 0.90 0.89 82.9
MnI(22) 4498.90 0.88
CrI(150) 4500.28
TiII(18) 4500.32 0.77 0.88
TiII(31) 4501.27 0.30 −2.1 0.44 86.0
MnI(22) 4502.22 0.90: −1.6:
CrII(16) 4504.52
FeI(555) 4504.83 0.93
NdII(7) 4506.58 0.93
TiII(30) 4506.74 0.83 −2.5
GdII(13) 4506.93
CrII(16) 4507.19
FeII(38) 4508.28 0.37 −2.3 0.46 83.8
CrII(191) 4511.82 0.90 −0.8
TiI(42) 4512.74 0.90 −1.7 0.95
FeII(37) 4515.35 0.37 −2.3 0.46 83.6
LaII 4516.38 0.92:
CrII(191) 4516.56 0.94
FeI(472) 4517.53 0.88 −1.7
TiI(42) 4518.03
TiII(18) 4518.30 0.60 −1.3: 0.77
VII(212) 4518.38
SmII(49) 4519.63 0.93: 0.87 80.5
FeII(37) 4520.22 0.38 −2.5 0.46 83.3
GdII(44) 4521.30 0.97:
FeII(38) 4522.63 0.30 −2.8 0.41 84.1:
TiI(42) 4522.80
CeII(2) 4523.08
BaII(3) 4524.94 0.72 81.5
LaII(50) 4526.12 0.82 80.8
FeI(969) 4526.45 0.73 −1.1
CeII(108) 4527.35 0.79: −2.0: 0.72 82.3
VII(56) 4528.50 0.61
FeI(68) 4528.61 0.36 −2.8
TiII(82) 4529.48 0.46 −0.1: 0.63 83.3
FeI(39) 4531.15 0.57 0.95 81.4
TiI(42) 4533.24 0.91 81.6:
TiII(50) 4533.96 0.23 0.34
FeII(37) 4534.16
TiI(42) 4534.78 0.78 −1.9 0.95
SmII(45) 4537.95 0.94 0.92
CrII(39) 4539.62 0.69
CeII(108) 4539.77 0.66
FeII(38) 4541.52 0.46 −2.9 0.55 82.5
TiII(60) 4544.02 0.64 −2.9 0.79 81.8
TiII(30) 4545.14 0.57 −2.4 0.74 81.3:
CrI(10) 4545.96 0.83 −2.8
Klochkova et al.: Spectroscopy of HD56126 29
αPer HD56126
Element λ Å r Vr r Vr
FeI(755) 4547.85 0.79 −1.9 0.97
FeII(38) 4549.47
TiII(82) 4549.62 0.15 0.28 90.5:
CeII(229) 4551.30 0.93: 0.86 80.0:
TiII(30) 4552.30 0.61: 0.86 82.2
BaII(1) 4554.03 0.29 −2.1 0.31 88.7
CrII(44) 4554.99 0.58 −2.2 0.64 83.0
FeII(37) 4555.89 0.33 0.45 84.0
CrII(44) 4558.65 0.38 −2.6 0.45 82.1
CeII(8) 4560.28 0.78 82.2
CeII(2) 4560.96 0.90 −1.8: 0.83 82.2
CeII(1) 4562.36 0.81 −2.0 0.69 81.9
TiII(50) 4563.76 0.32 −2.2 0.41 84.7
ZrII(116) 4565.41 0.82 84.2:
CrII(39) 4565.77 0.60: 0.71 83.0
TiII(60) 4568.32 0.73 −1.1 0.88 82.6
HfII(86) 4570.70 0.89 80.3:
MgI(1) 4571.10 0.82 −1.1
TiII(82) 4571.98 0.27 −1.5 0.36 91.3:
ZrII(139) 4574.48 0.69 84.6:
LaII(23) 4574.87 0.83: 0.78 80.6:
FeII(38) 4576.34 0.47 −2.1 0.54 83.0
FeII(26) 4580.06 0.59 0.70 82.7
CeII(7) 4582.50 0.75:
FeII(37) 4582.83 0.51 −2.2 0.58 82.6
TiII(39) 4583.41
FeII(38) 4583.84 0.28 −2.3 0.41 87.5
CrII(44) 4588.20 0.45 −2.0 0.49 83.1
CrII(44) 4589.94 0.43 −1.8 0.53 83.4
CrII(44) 4592.05 0.58 −1.7: 0.65 82.8
CeII(6) 4593.92 0.74: 0.72 81.1
FeI(820) 4596.06 0.87 80.1:
NdII(51) 4597.01 0.93 82.9
VII(56) 4600.19 0.67 0.90 82.8
FeII(43) 4601.36 0.84: −2.8 0.91 83.6
ZrII(138) 4601.97 0.86: −0.4: 0.89 82.6
FeI(39) 4602.94 0.63 −2.2 0.94 81.8
CeII(6) 4606.40 0.87: 0.83 82.1
TiII(39) 4609.27 0.85 −2.8 0.94 82.5
FeI(826) 4611.28 0.73 −2.4
ZrII(67) 4613.95 0.87 −1.2: 0.69 82.6
CrII(44) 4616.62 0.61 −2.0 0.68 83.3
CrII(44) 4618.82 0.49 −2.2 0.55 82.3
LaII(76) 4619.87 0.85 82.3
FeII(38) 4620.51 0.55 −1.7 0.63 83.4
CeII(27) 4624.90 0.77 83.7:
FeI(554) 4625.05 0.76
CeII(1) 4628.16 0.83 −1.9 0.67 82.6
ZrII(139) 4629.07
30 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(37) 4629.33 0.38 −2.7 0.44 82.7:
CrII(34) 4634.07 0.54 −2.1 0.59 83.0
FeII(186) 4635.31 0.79 −1.6 0.79 82.9
TiII(38) 4636.33 0.81 −2.4 0.91 82.9
FeI(822) 4638.02 0.80: 0.95 82.1
SmII(36) 4642.24 0.96 −2.7 0.93 82.5
LaII(8) 4645.28 0.95: 0.93 80.9:
CrI(21) 4646.17 0.71 −1.4 0.95
FeI(409) 4647.44 0.72 −2.6 0.91 80.8:
FeII(25) 4648.93 0.91 82.4:
CrI(21) 4651.29 0.86 −1.7
CrI(21) 4652.16 0.78 −1.7
CeII(154) 4654.29 0.77 83.4:
LaII(75) 4655.49 0.82 82.0
FeII(43) 4656.98 0.43 0.64
TiII(59) 4657.20
ZrII(129) 4661.78 0.74 82.3:
LaII(8) 4662.51 0.80 82.3:
FeII(44) 4663.71 0.69 −1.6 0.77 83.4
FeII(37) 4666.75 0.51 −2.0 0.61 83.1
LaII(76) 4668.91 0.91 82.1
FeII(25) 4670.19
ScII(24) 4670.40 0.43 0.60 82.1:
LaII(80) 4671.82 0.92 82.7:
CeII(18) 4680.13 0.92 81.6
YII(12) 4682.34 0.73 0.61 81.4
CeII(228) 4684.61 0.89 81.1:
ZrII(129) 4685.19 0.86 0.73 82.7
LaII(23) 4691.17 0.95 82.4:
FeI(409) 4691.42 0.75 −1.2:
LaII(75) 4692.50 0.91 81.4
TiII(59) 4698.67 0.93 81.9
MgI(11) 4702.99 0.52 −2.2
ZrII(138) 4703.03 0.63 81.9
NdII(3) 4706.55 0.92 −1.1: 0.89 82.2
TiII(49) 4708.66 0.59 0.76 82.5
C2 (1;0)R1(16) 4712.96 0.92:
C2 (1;0)R2(15) 4713.12 0.92: 77.2:
C2 (1;0)R1(15) 4714.38 0.91 77.6
C2 (1;0)R2(14) 4714.54 0.91: 78.0:
C2 (1;0)R3(13) 4714.72 0.93: 77.7
NdII(49) 4715.60 0.91:
C2 (1;0)R3(12) 4716.15 0.96 78.4:
LaII(52) 4716.44 0.92 82.2:
C2 (1;0)R1(13) 4717.08 0.93 77.4
C2 (1;0)R2(12) 4717.29 0.94 78.1
C2 (1;0)R3(11) 4717.48 78.0
C2 (1;0)R1(12) 4718.38 0.92 78.2
C2 (1;0)R2(11) 4718.60 0.93 77.4
Klochkova et al.: Spectroscopy of HD56126 31
αPer HD56126
Element λ Å r Vr r Vr
C2 (1;0)R3(10) 4718.84 0.95 77.8
C2 (1;0)R1(11) 4719.61 0.87: 78.3:
C2 (1;0)R1(10) 4720.81 0.93 77.7
C2 (1;0)R2(09) 4721.09 0.94 78.7
C2 (1;0)R3(08) 4721.36 0.95 77.4
C2 (1;0)R1(09) 4721.94 0.95 78.3
C2 (1;0)R2(08) 4722.27 0.91 78.8:
C2 (1;0)R3(07) 4722.53 0.94 77.8
C2 (1;0)R1(08) 4723.04 0.93 78.0
C2 (1;0)R2(07) 4723.44 0.90 77.2
C2 (1;0)R3(06) 4723.74 0.94 77.6
C2 (1;0)R1(07) 4724.08 0.93 77.7
C2 (1;0)R3(05) 4724.83 0.92 77.9
C2 (1;0)R1(06) 4725.07 0.88: 78.3:
C2 (1;0)R2(05) 4725.57 0.91 79.6
C2 (1;0)R1(05) 4725.99 0.86: 78.5:
C2 (1;0)R2(04) 4726.60 0.89 77.5
C2 (1;0)R1(02) 4728.47 0.77 77.9:
C2 (1;0)P1(34) 4730.77 0.90 78.0
FeII(43) 4731.47 0.51 −3.1 0.59 81.3
C2 (1;0)P2(03) 4732.81 0.89 78.3:
C2 (1;0)P2(04) 4733.40 0.84 78.6:
C2 (1;0)P2(05) 4733.93 0.83
FeI(554) 4736.77 0.63 −0.3 0.73 84.0:
LaII(8) 4740.27 0.84 0.78 81.9
LaII(75) 4743.08 0.92 0.85 82.7
PrII(3) 4744.93 0.95 82.2
CeII 4747.14 0.97 0.92 82.4
LaII(65) 4748.73 0.93 −0.9: 0.83 81.5
FeI(634) 4757.58 0.91 −0.8
CeII 4757.84 0.94 81.4
MnI(21) 4761.53 0.85 −2.5:
ZrII(107) 4761.67 0.63 82.1
CI(6) 4762.31
CI(6) 4762.54 0.63:
TiII 4763.90 0.58 −2.4 0.75 81.8:
TiII(48) 4764.53 0.64 −0.5: 0.83
MnI(21) 4766.43 0.76
CI(6) 4766.68 0.83 82.2
CI(6) 4770.03 0.88 −3.6 0.76 82.3
CI(6) 4771.75 0.54 81.9
CeII(17) 4773.94 0.93 −3.9 0.90 80.6
CI(6) 4775.91 0.84 −2.2 0.71 82.0
TiII(92) 4779.99 0.52 −2.7 0.60 82.3
MnI(16) 4783.42 0.70 −2.0 0.96 82.4
YII(22) 4786.58 0.59 82.5
TiII(17) 4798.53 0.64 −3.0 0.81 82.8
LaII(37) 4804.04 0.96 −1.1: 0.91 82.0
TiII(92) 4805.09 0.45 −1.5 0.53 83.2
32 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
LaII(37) 4809.00 0.89 82.4
NdII(3) 4811.35 0.93 0.91 82.0
CrII(30) 4812.35 0.73 −2.6 0.81 82.5
CI(5) 4812.92 0.95 83.0:
ZrII(66) 4816.47 0.97 0.87 82.5
CI(5) 4817.37 0.95: −1.5: 0.90 81.7
NdII(47) 4820.34 0.91 81.9
YII(22) 4823.31 0.53 82.6
MnI(16) 4823.51
CrII(30) 4824.14 0.47 −2.9 0.54 82.0
NdII(3) 4825.48 0.82: 0.86 82.0
CI(5) 4826.80 0.95 −2.1 0.91 82.7:
NiI(111) 4831.18 0.83 −1.9 0.95 81.4
FeII(30) 4833.19 0.85 −1.8 0.94 82.9
CrII(30) 4836.23 0.67 0.78 82.2
LaII(37) 4840.02 0.92 81.4:
ZrII(138) 4841.98 0.92 82.6
SmII(26) 4844.21 0.95 82.2:
CeII(17) 4846.57 0.96 81.1:
CrII(30) 4848.25 0.52 −2.0 0.59 82.9
YII(22) 4854.87 −2.1: 83.0
FeI(318) 4859.74 0.80
Hβ 4861.33 0.11 −1.7 0.13 98.2
CrII(30) 4864.32 −1.7: 83.3:
TiII(29) 4865.62 −2.6: 81.7:
FeI(318) 4871.32 0.50: −2.6: 0.75 81.2
FeI(318) 4872.14 0.55: −3.1: 0.83 81.9
TiII(114) 4874.01 0.65: −2.2: 0.70 82.5
CrII(30) 4876.40 0.61
CrII(30) 4876.48 0.51
CaI(35) 4878.14
FeI(318) 4878.22 0.56 0.90 81.0:
YII(12) 4881.44 0.92 81.1
CeII 4882.46 0.85 81.3
YII(22) 4883.69 0.51 −2.8 0.39 84.8
CrII(30) 4884.60 0.75 −0.9: 0.84 83.2
FeI(318) 4890.76 0.53 −2.2 0.78 80.8
FeI(318) 4891.49 0.49 −2.2 0.74 82.7
FeII(36) 4893.82 0.79 −1.6 0.86
ZrII(107) 4894.43 0.89 82.0
BaII(3) 4899.94
YII(22) 4900.12 0.46 0.38
FeI(318) 4903.31 0.66 −1.9 0.87 81.0
ZrII(145) 4908.67 0.97 80.8:
TiII(114) 4911.19 0.59 −1.1: 0.63 83.7:
ZrII(3) 4911.66 0.82 81.8:
FeI(318) 4918.99 0.52 −2.8 0.81 82.9
FeI(318) 4920.50 0.42 −1.1 0.64 85.0:
LaII(7) 4920.98 0.63 81.9:
Klochkova et al.: Spectroscopy of HD56126 33
αPer HD56126
Element λ Å r Vr r Vr
LaII(7) 4921.80 0.79 0.67 82.3
FeII(42) 4923.92 0.29 −1.8 0.55: 78.0:
0.39 93.9
CI(13) 4932.05 0.81 −3.4 0.64 81.3
BaII(1) 4934.08 0.32 −2.9 0.35 85.5
FeI(687) 4946.39 0.79 −1.9
LaII(36) 4946.47 0.92 80.8
FeII(168) 4953.98 0.93 −1.6: 0.94 83.3:
FeI(318) 4957.30
FeI(318) 4957.60 0.31 0.65 81.8:
NdII(1) 4959.13 0.92 −1.1 0.92 81.4
NdII(22) 4961.40 0.96 0.93 82.4
SrI(4) 4962.29 0.78 83.3
FeI(687) 4966.09 0.71 −2.3 0.94 83.2
OI(14) 4967.88 0.95
FeI(1067) 4967.90 0.83 −1.9
OI(14) 4968.79 0.96: 82.1:
LaII(37) 4970.39 0.85 81.7
CeII 4971.48 0.88 82.2
FeI(984) 4973.11 0.82 −2.0
TiII(71) 4981.35 0.94 80.8
TiII(38) 4981.74 0.72 −1.2
YII(20) 4982.13 0.69 82.4
LaII(22) 4986.82 0.93 0.86 82.8
NdII 4989.96 0.95 −2.0: 0.90 81.4:
FeII(36) 4993.35 0.65 −1.1: 0.75 82.9
FeI(16) 4994.14 0.73 −2.4: 0.93 82.0:
LaII(37) 4999.46 0.78 82.6
TiI(38) 4999.49 0.75 −2.1
TiII(71) 5005.17 0.78: 0.92 82.2
FeI(984) 5005.72
FeI(318) 5006.12 0.54: 0.88 82.1
TiII(113) 5010.21 0.77 −2.9 0.87 82.8
BaII(10) 5013.00 0.92 80.1
TiII(71) 5013.69 0.64 −2.7 0.81 82.0
CI 5017.09 0.91: 82.8:
FeII(42) 5018.44 0.28 −2.2 0.55: 77.0:
0.34 96.4
CaII(15) 5019.98 0.72 −3.0: 0.82 82.8:
TiI(38) 5020.03
FeI(965) 5022.24 0.74:
CeII(16) 5022.87 0.90 81.3:
CI 5023.85 0.94: 0.87 82.7
TiI(38) 5024.85 0.90:
CI 5024.92 0.94 81.8
ScII(23) 5031.02 0.53 −2.6 0.63 82.5
CI(4) 5039.07 0.76 82.3
CI 5040.13 0.90 82.4:
SiII(5) 5041.03 0.77 80.5:
34 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CeII(16) 5044.01 0.89 81.9
FeI(318) 5044.22 0.86
FeI(114) 5049.82 0.64 −2.1 0.93 81.8
FeI(16) 5051.64 0.62 −0.9:
CI(12) 5052.17 0.74: 0.54 81.7
CI 5053.52 0.95 83.6
SiII(5) 5055.98 0.83 −1.1: 0.75 83.3:
SiII(5) 5056.31
FeI(1094) 5065.02 0.66 −1.7: 0.93: 81.3:
FeI(383) 5068.77 0.68 0.95:
TiII(113) 5069.09 0.93 83.0:
FeI(1089) 5272.08
TiII(113) 5072.29 0.63 0.79 82.4
FeI(1094) 5074.75 0.71 −1.7 0.94 81.6
CeII(15) 5079.68 0.80 81.6
FeI(16) 5079.75 0.74
NiI(143) 5080.54 0.74 −2.1 0.94 81.4
FeI(16) 5083.35 0.72 −2.1 0.97
YII(20) 5087.42 0.62 −2.4 0.51 84.3
FeI(1090) 5090.78 0.82 −2.0 0.94 82.9:
NdII(48) 5092.80 0.94 −1.2 0.92 82.0
C2 (0;0)R1(33) 5095.15 0.98 77.5:
C2 (0;0)R1(32) 5098.13 0.98 77.3:
C2 (0;0)R3(30) 5098.30 0.98: 78.3:
FeII 5100.74 0.70 0.81 82.3:
C2 (0;0)R1(29) 5106.36 0.95 77.5
FeI(16) 5107.45
LaII(164) 5107.54 0.57 0.90 83.0:
FeI(36) 5107.65
FeI(1) 5110.42 0.68 −2.1
ZrII(95) 5112.27 0.89 −1.9 0.62 82.7
LaII(36) 5114.55 0.91: 0.82 81.6:
C2 (0;0)R1(25) 5116.66 0.93 77.7
C2 (0;0)R3(23) 5116.89 0.95 77.6
CeII 5117.18 0.97 0.90 81.4:
YII(20) 5119.12 0.88 −2.1 0.69 80.9:
FeII(35) 5120.34 0.80 −1.0: 0.91 82.7
C2 (0;0)R1(23) 5121.44 0.93 77.3
C2 (0;0)R3(21) 5121.69 0.94 77.7
LaII(36) 5123.00
YII(21) 5123.22 0.70 0.53
C2 (0;0)R1(22) 5123.79 77.3:
C2 (0;0)R3(20) 5124.04 77.3:
C2 (0;0)R1(21) 5125.98 0.91 77.5
C2 (0;0)R3(19) 5126.26 0.93 77.5
C2 (0;0)R3(20) 5128.19 0.90 77.3
C2 (0;0)R3(18) 5128.49 0.93 77.9
TiII(86) 5129.16 0.50
C2 (0;0)R1(19) 5130.27 0.89 77.9
Klochkova et al.: Spectroscopy of HD56126 35
αPer HD56126
Element λ Å r Vr r Vr
C2 (0;0)R1(18) 5132.36 0.86 77.7
FeII(35) 5132.66 0.77 −2.6: 82.2:
FeI(1092) 5133.69 0.64 −2.0 0.88 82.9
C2 (0;0)R1(17) 5134.32 0.89 77.1
C2 (0;0)R3(15) 5134.67 0.91 77.4
C2 (0;0)R1(16) 5136.27 0.89 77.6
C2 (0;0)R2(15) 5136.44 0.94 77.7
C2 (0;0)R3(14) 5136.66 0.89 77.7
C2 (0;0)R1(15) 5138.11 0.89 77.3
C2 (0;0)R2(14) 5138.32 0.93 77.1
C2 (0;0)R3(13) 5138.51 0.90 77.6
C2 (0;0)R1(14) 5139.93 0.88 77.5
C2 (0;0)R2(13) 5140.14 0.92 77.8
C2 (0;0)R3(12) 5140.38 0.89 77.6
C2 (0;0)R1(13) 5141.65 0.87 77.2
C2 (0;0)R2(12) 5141.90 0.89 77.1
C2 (0;0)R3(11) 5142.11 0.89 77.7
C2 (0;0)R1(12) 5143.33 0.86 77.6
C2 (0;0)R2(11) 5143.60 0.89 77.4
C2 (0;0)R3(10) 5143.86 0.88 77.7
C2 (0;0)R1(11) 5144.92 0.85 77.5
C2 (0;0)R2(10) 5145.23 0.87 77.6
C2 (0;0)R3(09) 5145.48 0.87 77.5
FeII(35) 5146.11 0.73: 0.86 83.1:
C2 (0;0)R1(10) 5146.46 0.83 77.5
C2 (0;0)R2(09) 5146.81 0.88 77.6
C2 (0;0)R3(08) 5146.12 0.88 77.2
C2 (0;0)R1(09) 5147.93 0.84 77.4
C2 (0;0)R2(08) 5148.33 0.83 77.0
C2 (0;0)R3(07) 5148.61 0.84 77.3
C2 (0;0)R1(08) 5149.33 0.84 77.8
C2 (0;0)R2(07) 5149.79 0.85 77.1
C2 (0;0)R3(06) 5150.14 0.86 77.6
FeI(16) 5150.85 0.70 −0.9:
C2 (0;0)R2(06) 5151.17 0.83 77.3
C2 (0;0)R2(05) 5152.52 0.81 77.0
C2 (0;0)R2(04) 5153.77 0.74 77.2
TiII(70) 5154.07 0.51 0.57:
C2 (0;0)R2(03) 5154.99 0.82 77.4
C2 (0;0)R1(02) 5156.11 0.77 77.2
C2 (0;0)R2(01) 5157.16 0.86 77.8
C2 (0;0)P2(04) 5161.98 0.75 76.6
FeI(1089) 5162.27 0.66 −1.6
C2 (0;0)P2(05) 5162.58 0.66 77.3
C2 (0;0)P2(07) 5163.13 0.75 77.4
C2 (0;0)P1(14) 5165.03 0.56 78.0
C2 (0;0) head 5165.24 0.72:
MgI(2) 5167.32 0.30 0.55
FeI(37) 5167.49
36 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(42) 5169.03 0.27 −2.7 0.56: 77.0:
0.33 97.4
FeI(36) 5171.60 0.56 −1.7 0.88 82.6
MgI(2) 5172.68 0.37 −1.4 0.51 82.7
NdII 5179.78 0.94 81.6
FeI(1166) 5180.07 0.92
MgI(2) 5183.60 0.32 −2.1 0.45 81.6
TiII(86) 5185.91 0.54 −2.1 0.69 82.0
CeII(46) 5187.46 0.93: 0.81 81.4
TiII(70) 5188.69 0.41 0.57
CaI(49) 5188.85
FeI(383) 5191.45 0.56
FeII(52) 5191.58 0.58 82.8:
FeI(383) 5192.35 0.57 0.83:
NdII(75) 5192.61 0.81:
YII(28) 5196.43 0.75 81.8
FeII(49) 5197.58 0.46 −2.4 0.59 83.3
YII(20) 5200.41 0.70 −2.8: 0.61 83.7:
FeI(66) 5202.34 0.67 0.94 81.4
YII(20) 5205.73 0.55 84.8:
CrI(7) 5206.04 0.42
TiII(103) 5211.54 0.72 −2.7 0.83 82.3
NdII(44) 5212.37 0.96 −2.0: 0.95 81.1
FeII 5216.85 0.94 82.2
PrII(35) 5220.11 0.94 82.0
TiII(70) 5226.54
FeI(383) 5226.87 0.37: −1.9: 0.60 83.6:
FeI(37) 5227.19 0.79 81.6
FeI(1091) 5228.38 0.89
NdII(46) 5228.43
FeI(553) 5229.85 0.74 −1.3 0.95 82.8
FeII(49) 5234.63 0.45 −2.3 0.57 83.8
CrII(43) 5237.32 0.60 −1.9 0.68 82.7:
ScII(26) 5239.82 0.66 −1.8 0.76 82.4
CrII(23) 5246.77 0.80: 0.91 83.1
FeII(49) 5254.93 0.62 −1.3 0.74 82.0
NdII(43) 5255.51 0.91 81.6:
FeII(41) 5256.93 0.80 −1.7 0.89 83.2
FeII 5260.26 0.92: 0.90 81.9:
TiII(70) 5262.11 0.33: 0.81
CaI(22) 5262.24
FeII(48) 5264.81 0.60 −2.0 0.56 87.4:
FeI(383) 5266.55 0.58 −1.8 0.88 82.3
TiII(103) 5268.62 0.73: 0.86: 83.0:
FeI(15) 5269.54 0.42 −2.0 0.70 82.1
FeII(185) 5272.39 0.86 0.91 83.3:
CeII(15) 5274.23 0.92: 0.80 81.9
CrII(43) 5274.98 0.60: 0.71 82.9
FeII(49) 5276.00 0.42 −3.0 0.56 84.8
Klochkova et al.: Spectroscopy of HD56126 37
αPer HD56126
Element λ Å r Vr r Vr
FeI(383) 5281.79 0.70 −2.1 0.95 81.3
FeII(41) 5284.10 0.53: 0.68 83.1
YII(20) 5289.82 0.95 −2.3 0.87 81.2
LaII(6) 5290.83 0.96 −1.8: 0.93 81.1:
NdII(75) 5293.16 0.90 −1.4 0.84 82.2
HfII(49) 5298.06 0.94 82.7:
CrII(24) 5305.86 0.76 −1.5 0.84 82.9
CrII(43) 5308.43 0.79 −2.1 0.85 82.7
CrII(43) 5310.69 0.84: 0.92 82.7
CrII(43) 5313.58 0.70 −1.6 0.78 82.9
FeII(49,48) 5316.66 0.34 −1.3: 0.48 88.0:
ScII(22) 5318.35 0.85 −1.4 0.95 83.2:
NdII(75) 5319.82 0.92: 0.85 81.5
YII(20) 5320.78 0.94 82.0
FeI(553) 5324.18 0.58 −2.4 0.81 82.6
FeII(49) 5325.56 0.65 −2.5 0.73 82.6
FeI(15) 5328.04 0.37: 0.74 82.4
OI(12) 5328.69 0.93 83.3
CrII(43) 5334.87 0.72 −2.1 0.80 82.9
TiII(69) 5336.79 0.55 −2.2 0.71 81.9
FeII(48) 5337.73 0.71
CrII(43) 5337.79 0.81
FeI(37) 5341.02 0.61 −1.6 0.94 81.5
ZrII(115) 5350.09
ZrII(115) 5350.35 0.87: 0.64
FeI(1062) 5353.38 0.79:
CeII(15) 5353.53 0.79 81.3
FeII(48) 5362.86 0.51 −1.9 0.63 83.5
FeI(1146) 5364.87 0.72 0.93 82.6
FeI(1146) 5367.47 0.70 −2.1 0.90 82.4
CrII(29) 5369.35 0.96 82.2
FeI(1146) 5369.96 0.65 −2.1 0.88 82.9
FeI(15) 5371.49 0.46 −2.2 0.82 81.8
NdII(79) 5371.92 0.92 81.5:
LaII(95) 5377.05 0.94 82.3
CI(11) 5380.34 0.85: −1.9: 0.68 81.9
TiII(69) 5381.03 0.63 −2.8 0.78 81.8
FeI(1146) 5383.37 0.63 −2.2 0.86 82.6
FeI(553) 5393.17 0.71
CeII(24) 5393.39 0.81
FeI(553) 5393.17 0.71
CeII(24) 5393.39 0.81
FeI(15) 5397.13 0.52 −2.1 0.89 81.6
YII(35) 5402.78 0.85 −2.1 0.59 81.9
FeI(1145) 5404.14 0.59 0.87 82.2
FeI(15) 5405.77 0.50 −1.9 0.89 81.4
CeII(23) 5409.22 0.90 81.4
FeI(1165) 5410.91 0.70 −1.5 0.91 82.8:
FeII(48) 5414.07 0.74 −2.2 0.84 82.5
38 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(1165) 5415.20 0.64 −2.1 0.87 82.2
ZrII(94) 5418.01 0.96 80.6:
TiII(69) 5418.77 0.67 −2.0 0.82 82.4
CrII(23) 5420.93 0.79 0.90 83.0
FeI(1146) 5424.07 0.60 −1.8 0.84 82.7
FeII(49) 5425.25 0.67 −2.0 0.75 82.7
FeII 5427.80 0.94 −1.4 0.96 81.4:
FeI(15) 5434.52 0.56 −1.8 0.91 81.8
OI(11) 5435.18 0.97
OI(11) 5435.78 0.97 82.4
OI(11) 5436.86 0.95:
NdII(76) 5442.29 0.97 81.0:
FeI(1163) 5445.04 0.74 −1.9 0.95 82.1
FeI(15) 5446.92 0.48 0.89 81.0:
NdII 5451.12 0.97: 0.96 81.5:
CeII(24) 5468.38 0.96 0.92 89.5
CeII(24) 5472.30 0.90 89.0
YII(27) 5473.39 0.87: 0.66 90.0
ZrII(115) 5477.79 0.89 89.7
CrII(50) 5478.37 0.76 −1.7 0.83 89.3
YII(27) 5480.74 0.83: 0.66 90.0
NdII(79) 5485.71 0.97 −1.3: 0.92 90.3:
TiII(68) 5490.68 0.82 −1.2: 0.93 90.4:
YII(27) 5497.41 0.62 0.51 90.5
FeI(15) 5497.52
FeI(15) 5501.47 0.72
CrII(50) 5502.08 0.80 −2.7: 0.87 90.2
FeI(15) 5506.79 0.67 −0.9: 0.96 90.3:
CrII(50) 5508.62 0.82 −2.9: 0.89 89.0:
YII(19) 5509.90 0.80 −1.4 0.65 90.9:
CrII(23) 5510.71 0.83 −1.9 0.90 90.7:
YII(27) 5521.56 0.92 −2.1 0.69 90.3
ScII(31) 5526.81 0.55 −2.1 0.60 90.4
MgI(9) 5528.41 0.58 −2.4 0.76 88.7
FeII(55) 5534.84 0.57 −1.8 0.63 90.0
FeI(926) 5543.19 0.90 −2.1 0.97 89.8
FeI(1062) 5543.94 0.89 −2.4 0.96 89.0:
YII(27) 5544.61 0.89: 0.65 91.0
CI 5545.07 0.92: 0.82: 88.0:
YII(27) 5546.01 0.90: 0.66 90.1
CI 5547.27 0.95 89.5
CI 5551.03 0.95 87.8:
CI 5551.59 0.92 88.5
FeI(1183) 5554.90 0.84 −2.7 0.95 90.8:
FeI(686) 5569.62 0.71 −1.8 0.93 89.0
FeI(686) 5572.84 0.63 0.89 90.0
FeI(686) 5586.76 0.61 −1.4 0.84 89.2
CaI(21) 5588.76 0.65 −2.0 0.90 88.8
CaI(21) 5594.47 0.66: 0.89 88.4
Klochkova et al.: Spectroscopy of HD56126 39
αPer HD56126
Element λ Å r Vr r Vr
CaI(21) 5601.28 0.80 −2.9 0.97 88.7
CeII(26) 5610.26 0.97:
YII(19) 5610.36 0.93
FeI(686) 5615.64 0.57 0.82 89.5
NdII(86) 5620.65 0.93 88.5
FeI(686) 5624.54 0.75 −2.4 0.93 90.2:
FeII(57) 5627.49 0.87 −1.6 0.93 90.3
CI 5629.93 0.98: −1.5: 0.96 88.5
FeI(1314) 5633.95 0.89 −2.0
FeI(1087) 5638.27 0.87 −2.3
ScII(29) 5640.98 0.73 0.82 90.6
ScII(29) 5657.87 0.56: 0.72 90.3
ScII(29) 5658.34 0.83: 88.5
FeI(1087) 5662.52
YII(38) 5662.94 0.66: 0.42 90.6
ScII(29) 5667.15 0.77 −1.3 0.87 90.0
CI 5668.95 0.72 90.4
ScII(29) 5669.03 0.72 −2.9
LaII(95) 5671.54 0.96 91.2:
NaI(6) 5682.64 0.79: 0.96 88.8:
ScII(29) 5684.19 0.70: 0.83 90.5
NaI(6) 5688.21 0.72 −0.9: 0.92 91.2:
NdII(79) 5688.54 0.91 89.6:
CI 5693.11 0.98: 0.94 89.5
MgI(8) 5711.09 0.85 −1.6 0.98:
NiI(231) 5715.09 0.90 −1.6
CI 5720.78 0.98 89.5:
YII(34) 5728.89 0.94 −1.9 0.75 90.3
FeI(1087) 5731.77 0.92 −2.1 0.98
FeII(57) 5732.72 0.94 0.97 90.0
FeI(1180) 5752.04 0.93 −2.2
FeI(1107) 5763.00 0.80 −3.0: 0.96: 89.3:
LaII(70) 5769.06 0.96 −1.2: 0.86 88.9
SiI(17) 5772.15 0.91 −1.8 0.98:
FeI(1087) 5775.08 0.93 −1.7
YII(34) 5781.69 0.84 90.5
CI 5793.12 0.89 0.87 88.9
CI 5794.46 0.97 90.6:
LaII(4) 5797.59 0.87 89.9
SiI(9) 5797.86 0.90
CI 5800.59 0.95: 0.91 89.2
NdII(79) 5804.02 0.93 90.5
CI 5805.19 0.94: 0.94 90.5
LaII(4) 5805.78 0.94 −2.7: 0.86 89.9
FeI(1180) 5806.73 0.93 −2.2 0.98 90.2
LaII(4) 5808.31 0.98: 0.97 91.5:
FeI(982) 5809.22 0.95 −1.3 0.98:
VII(99) 5819.93 0.95 −1.4 0.98: 90.0:
FeII(164) 5823.15 0.96 −2.5: 0.97 89.6:
40 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
NdII(86) 5842.39 0.99: 0.96 88.3:
FeI(1178) 5852.22 0.96 −1.8
BaII(2) 5853.68 0.63 −2.1 0.53 90.8
CaI(47) 5857.45 0.72 0.94 88.9
FeI(1180) 5862.36 0.85 −1.9 0.96 88.8
LaII(62) 5863.70 0.98 0.97 89.8
LaII(35) 5880.63 0.96 90.7:
NaI(1) 5889.95 0.45: −1.2: 0.21 13.0
0.05 +2.2 0.32 24.0
0.37 31.4
0.10 75.7
0.40 89.0
NaI(1) 5895.92 0.50: −0.9: 0.38 13.2
0.06 +2.3 0.51 24.7
0.48 32.0
0.16 76.3
0.45 89.8
FeI(982) 5934.66 0.89 −2.2
SiI(16) 5948.54 0.83 −3.0 0.97:
SiII(4) 5957.56 0.93 88.0:
CeII(80) 5975.83 0.94 89.9
SiII(4) 5978.93 0.88 87.5
FeI(1175) 5983.68 0.89 −0.7 0.95: 89.0:
FeI(1260) 5984.82 0.86 −1.9 0.96: 88.0:
FeII(46) 5991.37 0.75 −1.7 0.84 90.3
CI 6001.13 0.98: 0.92 89.5
CI 6002.98 0.95 89.7:
FeI(959) 6003.02 0.88 −2.4
CI 6006.03 0.96: 0.86 89.5
CI 6010.68 0.98 −1.2 0.92 88.8
CI 6012.24 0.98: −1.5: 0.94 90.3:
CI 6013.32 0.80 87.7:
MnI(27) 6013.49 0.89:
CI 6016.45 0.93 89.2:
MnI(27) 6016.64 0.91: −2.0:
MnI(27) 6021.80 0.90 −2.0:
FeI(1178) 6024.07 0.82 −2.2 0.94 88.8
ZrII(136) 6028.64 0.97: 0.91 89.1
CeII(30) 6034.20 0.98 −1.7 0.96 90.8:
CeII(30) 6043.40 0.99 −1.5: 0.94 89.7
FeI(207) 6065.49 0.81 −1.4 0.98:
FeII(46) 6084.10 0.83 −1.5 0.90
ZrII(106) 6106.47 0.97: 0.93 90.9
FeII(46) 6113.32 0.88 −1.6 0.93 88.6
ZrII(93) 6114.78 0.98 −1.5: 0.92 92.2:
CI 6120.82 0.99: 0.97 89.8
CaI(3) 6122.22 0.69 −0.9 0.93 89.5
FeI(169) 6136.62 0.75 0.95 89.0:
FeI(207) 6137.70 0.78 −2.0 0.96 89.2:
Klochkova et al.: Spectroscopy of HD56126 41
αPer HD56126
Element λ Å r Vr r Vr
BaII(2) 6141.72 0.56 −1.4 0.37 92.3
FeII(74) 6147.74 0.74 −1.4 0.77 90.2
FeII(74) 6149.25 0.75 −1.5 0.77 90.0
SiI(29) 6155.98 0.89
OI(10) 6155.98 0.95: 0.82 87.0:
OI(10) 6156.17 0.95: 0.82 87.1
OI(10) 6158.18 0.79 88.0
FeI(1260) 6170.51 0.90 −1.5 0.97 89.7
FeII(200) 6175.14 0.95 90.2
LuII(2) 6221.88 0.98: 0.90 89.9:
FeII(74) 6238.39 0.74 −1.7 0.76 90.0
SeII(28) 6245.62 0.80: −0.5: 0.90 90.0:
FeII(74) 6247.56 0.66 −2.2 0.70 89.9:
FeII 6248.90 0.94 −1.4 0.94 89.3
FeI(169) 6252.56 0.81 −1.9 0.97 89.5
LaII(33) 6262.30 0.96 −0.6: 0.89 90.2
FeII 6317.99 0.81 −1.0: 0.86 88.8:
FeI(168) 6318.03
SiII(2) 6347.10 0.65 −2.0 0.51 89.7
FeII(40) 6369.46 0.84 −1.6 0.91 90.5
SiII(2) 6371.36 0.72 −1.8 0.57 89.5
FeII 6383.72 0.91 −1.6 0.92 89.8
FeII 6385.46 0.93 −2.0 0.94 88.4:
LaII(33) 6390.49 0.97 0.89 90.3
FeI(168) 6393.61 0.79 −2.5 0.96 90.5:
CI 6397.98 0.98: 0.94 89.2
FeII(74) 6416.92 0.75 −1.0 0.80 90.2
FeI(62) 6430.85 0.83 −1.6 0.97 90.6:
FeII(40) 6432.68 0.75 −1.4 0.81 90.0
CaI(18) 6439.08 0.69 −1.6 0.89 90.0
FeII 6442.95 0.95 −1.2 0.95 88.9
FeII(199) 6446.41 0.95 −1.2 0.95 91.1:
OI(9) 6453.60 0.97: 0.94 87.9
OI(9) 6454.45 0.98: −2.0: 0.94 88.0
FeII(74) 6456.39 0.60 −0.2: 0.66 91.0:
TiII(91) 6491.57 0.78: 0.91 90.7:
BaII(2) 6496.91 0.55 0.52
FeII(40) 6516.08 0.66 −2.0 0.77 90.2
LaII(33) 6526.99 0.91 90.7:
MgII(23) 6545.97 0.93 89.8
FeI(268) 6546.25 0.92:
Hα 6562.81 0.19 −2.1 0.32 58.0
0.40: 74.0:
0.89 82.8:
CI(22) 6587.61 0.89 −1.7 0.72 89.5
SeII(19) 6604.59 0.89 0.94 91.1:
TiII(91) 6606.95 0.95 −2.2: 0.96 89.5
CI 6611.35 0.96 90.6:
YII 6613.75 0.91 0.73 90.0
42 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CI 6654.61 0.94 89.5:
CI 6655.51 0.91 90.5
YII(26) 6795.42 0.88 90.0
CI 7087.83 0.90 89.3
CI 7100.12 0.91 89.7
SiI(23) 7415.95 0.95: 87.5:
SiI(23) 7423.50 0.92 91.0:
EuII(8) 7426.57 0.93: 85.0:
CI 7476.18 0.89: 86.0:
CI 7483.44 0.90 85.0:
LaII(1) 7483.48
FeI(1077) 7511.03 0.97: 87.0
KI(1) 7664.91 0.83 77.5
OI(1) 7771.94 0.34 93.5
OI(1) 7774.17 0.35 94.8:
OI(1) 7775.39 0.42:
CI 7860.89 0.91: 88.0:
MgII(8) 7877.05 0.89 90.5:
YII(32) 7881.90 0.89 90.5:
MgII(8) 7896.37 0.80 88.7:
H(P27) 8306.12 0.91: 91.0:
H(P25) 8323.43 0.91: 91.0:
H(P20) 8392.40 0.64 87.0:
H(P19) 8413.32 0.62 88.0:
H(P18) 8437.96 0.60 92.0:
OI(4) 8446.5: 0.26 94.0:
H(P17) 8467.25 0.58 93.0:
CaII(2) 8542.11 0.40 85.0:
H(P15) 8545.38 0.53 94.0:
NI(8) 8567.74 0.90 89.0:
NI(8) 8594.01 90.0:
H(P14) 8598.39 0.49 93.0:
NI(8) 8629.24 0.78: 88.0:
NI(1) 8703.25 0.85: 90.0:
NI(1) 8711.70 0.83 87.0:
NI(1) 8718.83 0.84 89.0:
H(P12) 8750.47 0.43 98.0:
	Introduction
	Observations and reduction of spectra
	Peculiarities of the optical spectrum of HD56126
	Radial velocities pattern
	Spectral atlas

  We studied in detail the optical spectrum of the post-AGB star HD56126
(IRAS07134+1005). We use high resolution spectra (R=25000 and 60000) obtained
with the echelle spectrographs of the 6-m telescope. About one and a half
thousand absorptions of neutral atoms and ions, absorption bands of C_2, CN,
and CH molecules, and interstellar bands (DIBs) are identified in the 4010 to
8790 AA wavelength region, and the depths and radial velocities of these
spectral features are measured. Differences are revealed between the variations
of the radial velocities measured from spectral features of different
excitation. In addition to the well-known variability of the Halpha profile, we
found variations in the profiles of a number of FeII, YII, and BaII lines. We
also produce an atlas of the spectrum of HD56126 and its comparison staralpha
Per. The full version of the atlas is available in electronic form from
Web-address: http://www.sao.ru/hq/ssl/Atlas/Atlas.html

Introduction
The star HD56126 is observed in the post-AGB phase of its evolution. While undergoing this short-lived
stage (according to Blöcker [1], this phase lasts for ∆T ≈ 103 ÷ 104 years), the star passes to the stage of a
planetary nebula and therefore post-AGB stars are also commonly referred to as “protoplanetary nebulae”
(PPNe). In the Hertzsprung–Russell diagram post-AGB stars move at almost constant luminosity leftward
of the AGB and become increasingly hotter. These objects, which are descendants of AGB-stars, can be used
to trace the physical and chemical parameters of the interstellar matter due to a change in the energy source,
which is accompanied by a change of the star structure, ejection of the envelope, and mixing of matter.
The main task of our research is to reveal the chemical composition anomalies that are due to the nuclear
synthesis of chemical elements in the interiors of low- and intermediate-mass stars (less than 8–9M⊙) and
subsequent dredge-up of the products of synthesis to the surface layers of stellar atmospheres. We use our
high-precision spectroscopic data not only to study the chemical composition, but also to perform a detailed
analysis of the velocity field in the atmospheres of these stars, which constitutes a separate astrophysical
problem. In addition, the high quality observational data allowed us to produce an atlas of the spectrum of a
typical post-AGB star over a wide wavelength interval. To this task, we chose the supergiant star HD 56126
(Sp=F5Iab), which is the optical component of the IR source IRAS07134+1005 with a double-peaked
spectral energy distribution (SED) typical of PPN. The star HD56126 is located outside the galactic plane,
its galactic coordinates are l=206.◦75, b=+9.◦99. Note that HD56126 is a generally recognized canonical
object in the phase of transition from the asymptotic giant branch to a planetary nebula. In addition to
the anomalous SED mentioned above, which is due to the circumstellar dust, this star exhibits other, highly
conspicuous, features specific for this class of objects [2]: the optical component of the PPN is an F5Iab-
type supergiant at a high galactic latitude; the central star is surrounded by an extended nebula, which,
according to HST observations [3], has the largest angular size β > 4′′ among PPN objects of this type; the
optical spectrum exhibits variable complex emission–absorption profile of the Hα and shows spectral features
that are indicative of the current mass outflow. Based on their high-resolution spectroscopy (R=860000,
FWHM=0.35km/s) of HD56126, Crawford and Barlow [4] revealed the multicomponent structure of the
Ki and C2 features, which is indicative of repeated episodes of mass ejection from the star.
⋆ The full version of the Atlas is available in electronic form from: http://www.sao.ru/hq/ssl/Atlas/Atlas.html
http://arxiv.org/abs/0704.0677v1
http://www.sao.ru/hq/ssl/Atlas/Atlas.html
2 Klochkova et al.: Spectroscopy of HD56126
Subsequent studies of HD56126 and of the associated IR source revealed a number of properties, which
allowed the object to acquire the canonical status in its class. First, an analysis of the spectra obtained with
the echelle spectrograph of the 6-m telescope, allowed Klochkova [5] to conclude that HD56126 is a metal-
poor star with [Fe/H ]⊙=−1.0 and high excess of carbon and s-process elements. Second, IRAS 07134+1005
was found to belong to the group of PPNe whose IR-spectra exhibit an emission feature at λ=21µm. Objects
of this small subgroup were found to exhibit a correlation between the presence of this 21µm–feature and
the manifestation of products of stellar nucleosynthesis in the outer atmospheric layers: overabundance of
carbon and heavy metals of the s-process. This so far unexplained correlation has been found independently
by Klochkova [6] and a group of other authors [7]. Thus HD56126 possesses the complete set of features
peculiar to the entire family of PPNe, and this fact determines the importance of the detailed spectroscopy
of this object and preparation of an atlas of its optical spectrum over a wide spectral region. This task is
facilitated by HD56126 being the brightest (B=9.m11, V=8.m27) star among carbon-rich PPNe and hence
the most accessible star for high-resolution spectroscopy among the objects of this type.
Section 2 gives a brief description of the methods of observation and data reduction employed in this
paper. Section 3 presents the peculiar features of the spectrum of HD56126, and section 4 describes the
field of radial velocities Vr in the atmosphere and envelope of the star. We also briefly discuss the radial-
velocity variability and the variability of selected spectral-line profiles. Section 5 describes the spectroscopic
atlas, identification of spectral features, and compares the spectrum of HD56126 with that of the standard
supergiant αPer (Sp = F5Iab).
2. Observations and reduction of spectra
We performed spectroscopic observations of HD 56126 and αPer with the 6-m telescope of the Special
Astrophysical Observatory. We obtained all spectra with NES [8, 9] and Lynx [10, 11] echelle spectrographs
operating in the Nasmyth focus. A 2048×2048 CCD and image slicer [12] with the NES spectrograph allows
taking spectra with a resolution of R≈ 60000, whereas the Lynx spectrograph equipped with a 1K×1K CCD
yields a resolution of R≈ 25000. The Table 1 gives the dates of observations and the spectral region recorded.
We use the modified ECHELLE context of MIDAS to extract data from two-dimensional echelle spectra
(see [13] for details). Cosmic-hit removal was performed via median averaging of two successive spectra.
Wavelength calibration was made using Th-Ar-lamps. We use DECH20 [14] code to perform spectropho-
tometric and position measurements. In particular, we determine the radial velocities from individual lines
and their components by superimposing the direct and mirror-reflected profiles. We determine the position
zero point for each spectrogram by referring it to the positions of ionospheric emission features of the night
sky and to those of telluric absorptions, which show up against the spectrum of the object. The accuracy
of single line velocity measurements in the spectra obtained is better than 1.0 and 1.5 km/s, for NES and
Lynx spectrographs, respectively.
3. Peculiarities of the optical spectrum of HD56126
Optical spectra of PPNe differ from the spectra of classical supergiants by the anomalous profiles of spectral
lines (Hi, Nai, Hei), and primarily, by the anomalous Hα profiles. Hα lines in the spectra of typical PPNe have
complex emission and absorption profiles with asymmetric cores, PCyg- or inverse PCyg-type profiles, and
profiles with two emission components. PPNe often exhibit a combination of several such features. Emission
in Hα may be due to mass outflow and/or pulsations and hence we must observe sporadic stellar wind in
many PPNe. The Doppler shift of the core is usually smaller than the escape velocity, i.e., we have evidence
only for motions at the wind base. The spectra of individual objects owe the great variety of their profiles to
the differences in the dynamical processes in their extended atmospheres: spherically symmetric outflow with
constant or height-dependent velocity, mass infall onto the photosphere, and pulsations. A two-component
emission profile is indicative of a nonspherical envelope, e.g., the presence of a circumstellar disk.
The peculiarity of the optical spectra of PPNe often shows up not only in specific Hi profiles, but also in
the distortions of the spectral features of the F −K-type supergiant due to chemical composition anomalies
and the presence of molecular features along with atomic and ion lines.
HD 56126 exhibits all these spectral peculiarities that distinguish PPN from a normal supergiant of the
same spectral type. As is evident from Fig. 1, the Hα line has a complex profile with absorption and emission
components, which are absent in the spectrum of the comparison star αPer. Figure 1 also shows well-defined
photospheric wings of the Hα line in the spectrum of HD56126. These wings are almost as extended as in
the spectrum of αPer. Figure 2, which shows all the data now available, demonstrates date-to-date variations
Klochkova et al.: Spectroscopy of HD56126 3
Table 1. Log of observations and results of Vr measurements. Column 4 gives the mean Vr averaged over weak
lines (r→ 1). For Feii(42), Hα and D lines of Nai we give the velocities inferred from the positions of the strongest
line components. The numbers in parentheses give the velocities inferred from weaker components. Slanted font in
column 5 indicates the velocities inferred from the IR oxygen triplet Oiλ 7773 Å. Semicolumn indicates uncertain
Date Spectro- ∆λ, Å Vr
graph r→ 1 Feii(42) Hβ Hα DNai C2 interstellar
1 2 3 4 5 6 7 8 9 10 11 12
HD56126
12.01.93 Lynx 5560–8790 88.8 91 – 78 (100:) 77 – – – –
10.03.93 Lynx 5560–8790 89.0 93 – 71 (43:) 75: – – – –
04.03.99 Lynx 5050–6640 85.9 77 – 76 (43:) 78 77.1 – – –
20.11.02 NES 4560–5995 89.6 95 (80:) 89 – 75 (89) 77.2 12.0 23.5 30.8
21.02.03 NES 5150–6660 88.8 96: – 88 (112:) 75 (89) 77.1 12 24 31
12.04.03 NES 5270–6760 88.4 – – 82 (103:) 75 (89:) – 13 23 30.5
14.11.03 NES 4518–6000 85.3 96 (87:) 97 – 75 (87:) 76.9 12.5 – –
10.01.04 NES 5270–6760 86.7 – – 54: 76 (86:) – 13.0 23.5 31
09.03.04 NES 5275–6767 89.8 – – 58 (74:) 76 (89) – 13 24 31
12.11.05 NES 4010–5460 82.5 97 (77:) 98 – – 77.5 – – –
04.03.99 Lynx 5050–6620 −1.2 −1 – −2 – – –
02.08.01 NES 3500–5000 −1.8 −1 : −2 – – – –
11.11.05 NES 4010–5460 −2.0 −2 −2 – – – –
12.11.05 NES 4560–6010 −1.9 −2 −2 – – – –
6540 6550 6560 6570
Figure 1. Fragment of the atlas containing the Hα profile in the spectra of HD 56126 (top) and αPer
(bottom). The y-axis gives the residual intensities, the continuum level is set equal to 100.
of the central part of the Hα profile. Earlier, Oudmaijer and Bakker [15] performed spectral monitoring of
HD56126 and also found the Hα to be highly variable over a two-months time scale. Hα-line variability can
be naturally explained in the case of post-AGB stars with signs of binarity (e.g., in the case of HR 4049 [16]),
however, it also shows up in post-AGB objects, which exhibit no regular radial-velocity or light variations
(the case of HD133656 [17]). Photometric variability would allow us (like in the case of RVTau type stars)
to invoke the mechanism where a shock wave stimulates mass outflow. Based on an extensive set of good
quality spectroscopic observations of HD56126, Barthès et al. [18] found that not only the profile of Hα but
4 Klochkova et al.: Spectroscopy of HD56126
6562 6564 6566
12.01.93
10.03.93
04.03.99
21.02.03
12.04.03
10.01.04
09.03.04
Wavelength, А
Figure 2. Variations of the Hα-line profile in the spectra of HD 56126 taken on different days. The y-axis
shows the residual intensities, the continuum level of the lower spectrum is set to 100 and every next spectrum
is shifted by 100 gradations with respect to the previous spectrum.
also that of Hβ to be variable. The above authors analyzed the variations of the profiles of both these lines
and concluded that no periodic component is present that could be associated with the radial-velocity and
photometric variations of the star.
The profiles of strong Feii lines (first and foremost, those of the members of the 42-nd multiplet), Baii,
and other elements in the spectrum of HD56126 are also variable. However, whereas either the blue or
red wing may have lower slopes in the absorption core of Hα, nonhydrogen absorptions preserve their
Klochkova et al.: Spectroscopy of HD56126 5
5160 5170 5180 5190
Figure 3. Same as Fig. 1, but for the spectral region containing the 5165 Å band of the Swan system of C2
molecule and the Feii(42) 5169 Å line.
asymmetry pattern unchanged: the blue wing is always more extended than the red wing. The profile of the
Feii (42)λ 5169 Å line in Fig.3 is a typical example.
Figures 3 and 4 show fragments of the spectra that may illustrate the differences between line intensities
of HD 56126 and αPer. Feii absorptions in the spectrum of the former star are much weaker than in those
of the latter star, and the ratio of the central depths of the same line in the spectra of the two stars depends
on the line intensity: it increases from 1.5 to 4 as one passes from weak to strong lines. Fei lines are also
depressed, on the average, by 0.1. On the contrary, Ci absorptions as well as those of Yii, Zrii, and other
s-process products are deeper by 0.1–0.2 in the spectra of HD 56126 compared to the corresponding features
in the spectrum of αPer.
Let us now analyze the molecular component of the spectrum of HD56126. Bakker et al. [19] were the
first to identify the Swan absorption bands of C2 molecule and of the red system of CN molecule in the
spectrum of the star. Later, Bakker et al. [20] used high-resolution spectra with R=50000 to perform a
detailed analysis of molecular bands in the spectra of HD 56126 and 16 other PPNe selected based on the
presence of carbon molecules C2, CN, CH
+ in their shells. Judging by the velocity corresponding to the
position of these bands, the molecular spectrum forms in a limited region of the shell close to the star [20].
Our spectra exhibit several bands of the Swan system (see Fig. 3).
Here it is pertinent to recall that the spectra of several PPNe were found to exhibit emission Swan bands
[19, 6]. However, the spectra of HD 56126 taken in different years show no signs of emission in these bands. D
lines of Nai neither show any signs of emission. This fact is consistent with the rather simple elliptical shape
of the nebula surrounding HD56126. Emissions in the Swan bands or in Nai D lines appear to show up only
in the spectra of PPNe with bright circumstellar nebulae with well-defined asymmetry. The spectroscopy of
the following PPNe corroborates this hypothesis: IRAS 04296+3429 [21], IRAS 23304+6147 [22], AFGL 2688
[23], IRAS 08005−2356 [24], IRAS 20056+1834 [25], and IRAS 20508+2011 [26]. On HST images [3], the
nebulae surrounding these PPNe are usually asymmetric and have a bipolar structure. Note also that most
of the objects listed above belong to type “1” according to the classification of Trammell et al. [27] — i.e.,
they are PPNe with polarized optical radiation.
Figure 5 shows the behavior of the D2 Nai line profile in the spectrum of HD56126, and here, like in
Table 1, to reveal the fine structure of lines, we analyze only the spectra taken with the highest resolution. The
positions of the three short-wavelength components remain constant within the errors. This stability confirms
that the components form in the interstellar medium. The wavelength shift of the deepest component agrees
6 Klochkova et al.: Spectroscopy of HD56126
5840 5850 5860 5870
Figure 4. Same as Fig. 1, but for the spectral region with the Baii λ 5853 Å line.
with that of the Swan bands (columns 8 and 9 in Table 1), and this fact indicates that the component in
question forms in the circumstellar shell. Finally, the longest-wavelength component forms in the photosphere:
its temporal behavior agrees with that of other photospheric absorptions (columns 4 and 8 in Table 1).
4. Radial velocities pattern
Much attention has been paid to the radial-velocity variations of HD 56126 and to study the differences
between the radial velocities inferred from lines of different types. Bujarrabal et al. [28] used CO millimeter-
wave observations to find Vr = 86.1 km/s, which is natural to adopt as the systemic radial velocity of
HD56126. Based on an extensive collection of spectrograms with high temporal resolution and high S/N
ratio, Oudmaijer and Bakker [15 analyzed the behavior of Vr and concluded that it is variable on a time
scale of several months with a small amplitude (Vr=84÷87± 2 km/s). The above authors demonstrated the
absence of variations on time scales ranging from several minutes to several hours. The variability of the radial
velocity of HD 56126 also showed up when the radial-velocity measurements made with the 6-m telescope were
compared to published data [5]. Lèbre et al. [29] performed a detailed spectroscopic monitoring of HD 56126.
Fourier analysis of the available radial-velocity and photometric data led the above researchers to conclude
that the dynamical state of the atmosphere of HD 56126 is similar to that of the atmospheres of RVTau-type
variables. The above authors interpreted the variability of Hα in terms of shock propagation. Later, Lèbre
et al. [30] analyzed the variability of two lines, Hα and Hβ. They obtained additional spectroscopic data and
determined the period of radial pulsations to be P = 36.8 days.
Barthès et al. [18] analyzed all the available reliable radial-velocity measurements made for HD56126 (89
measurements over eight years) and concluded that radial velocity of this star varies with a half-amplitude
of 2.7 km/s and the main period of P = 36.8 ±0.2d. The period of photometric variability is the same and
photometric amplitude is very small, 0.m02. However, the above authors found the variability pattern of
the star to differ significantly from pulsations observed in RVTau-type stars. Judging by its temperature
[5], HD 56126 evolved further beyond the stage of RVTau-type stars. The photometric and radial-velocity
variations of HD 56126 may be due to first-overtone radial pulsations driven by shocks that generate complex
asynchronous motions in the upper hydrogen layers of the star.
Table 1 presents the radial-velocity data we obtained for HD 56126. Given that a velocity gradient is very
likely in the upper layers of the star’s atmosphere, we report here the Vr values for individual lines and
groups of lines. As is evident from Table 1, velocity variations inferred from weak absorptions (their residual
Klochkova et al.: Spectroscopy of HD56126 7
5888 5889 5890 5891
20.11.02
21.02.03
14.11.03
12.04.03
10.01.04
09.03.04
Wavelength, А
Figure 5. Spectral fragment with the D2 Nai line on different observing dates.
intensities approach 1) are within the variability limits established by Barthès et al. [18]. The positions of
the circumstellar Nai D lines and Swan bands of the C2 molecule agree well with each other and match the
expansion velocity of the shell, Vexp ≈11 km/s. Note that the position of the wind component of the Hα line
is inconsistent with those of the wind components of other lines, whereas the variations of the Hβ profile is
synchronized with those of Feii(42) lines.
When intercomparing our data and comparing it with those of other authors one must control the zero
points of the corresponding radial-velocity systems. We used interstellar and circumstellar lines to control
the radial-velocity zero points. Three blueshifted interstellar components of Nai lines in the spectrum of
HD56126, which are barely visible in Fig. 5, yield Vr values listed in Column 10–12 of Table 1. The fourth
weak component with Vr ≈46km/s is barely visible in at least three our spectra. For each component, all our
Vr estimates agree with each other and with those of Bakker et al. [19] within the quoted errors. Furthermore,
as is evident from Fig. 5, the blend consisting of the three main components has sharp boundaries, which
allow the velocity of this entire feature to be confidently measured. Its mean velocity as inferred from our
data is equal to Vr = 20.3 ± 0.3 km/s and agrees with the velocity of 20±2km/s measured by Lèbre et
al. [29] from lower-resolution spectra. Crawford and Barlow [4] showed that when observed with superhigh
resolution, the circumstellar C2 and Ki features exhibit components that are about 1 km/s apart. These
components yield the same set of velocity values, but have different intensities. This effect may cause minor
systematic differences (also on the order of 1 km/s) between the velocities inferred from circumstellar atomic
and molecular lines in lower-resolution spectra. Our measurements reveal no variations of these velocities
with time, and their mean values, 77.2±0.5 and 75.4±0.3km/s for C2 and Nai, respectively, do not disagree
systematically with the radial velocities obtained by Lèbre et al. [29], Bakker et al. [19, 20], and Crawford
and Barlow [4]: 77.3÷77.6 and 75.3÷76.8km/s for C2 and Nai, Ki, respectively.
However, when comparing our Vr values with published data, one must take into account not only method-
ological effects, but also the spectroscopic peculiarity of the object itself. Line profiles in the spectrum of
HD56126 are asymmetric and their shape varies both with time and with line intensity. We plan to under-
take a detailed analysis of the velocity field at different depths in the atmosphere and in the circumstellar
envelope of HD 56126 in a separate paper.
8 Klochkova et al.: Spectroscopy of HD56126
As for the possible binarity of HD56126, it has neither been confirmed or finally disproved. In this
connection, of certain interest is a comment by Barthès et al. [18] who pointed out a weak trend in the star’s
radial velocity over several years of observations. This trend maybe indicative of a second companion in the
system with an orbital period longer than 16 years. Our eight spectra, which we took on more recent dates,
fail to clarify the situation. It would be therefore important to follow the behavior of Vr over a several-years
period taking one to two spectra every month on a regular basis.
The radial-velocity variability of HD 56126 is not a unique phenomenon. Part of candidate PPNe also
demonstrate radial-velocity variations on a time scale of several hundred days, which may be indicative
of the binary nature of these objects. Evidence for orbital motion has been obtained for several optically
bright objects with IR excess. For example, authors of papers [31, 32] and [33] proved the binary nature,
determined the orbital elements, and proposed models for the high-latitude supergiants 89Her and HR4049,
respectively. Van Winckel et al. [34] showed that HR4049, HD44179, and HD52961 to be spectral binaries
with the orbital periods of about one to two years. The above authors concluded that all extremely metal-
deficient PPNe studied so far (HR4049, HD44179, HD52961, HD46703, and BD+39o4926) are binary stars.
The observed correlation between the binarity and the presence of a hot dust envelope indicates that binarity
promotes the formation of an envelope. Bakker et al. [16] use high-resolution spectra of HR4049 to analyze
the variations of complex emission–absorption profiles of Na D lines and Hα lines over the orbital period.
Individual components of these lines may form under different conditions: in the atmosphere of the main
star; in the disk where both components of the binary are immersed, or in the interstellar medium. For such
binaries, of fundamental importance is the determination of the systemic velocity from radio spectroscopy.
The nature of the companions of suspected binary post-AGB stars remains unclear, because we see no
direct manifestations of these companions either in the continuum or in spectral lines (all known binary
post-AGB objects belong to type SB1). These companions may be either very hot object, or main-sequence
stars of very low luminosity. For example, Bakker et al. [16] believe that the secondary companion in HR 4049
is a cold (Te = 3500K) MS star with a mass of M=0.56M⊙, although it may also be a white dwarf, like in
the case of Ba-stars [35].
Unfortunately, because of the short history of PPN studies we are so far unable to make any definitive
conclusions concerning the cause of radial-velocity variability of a representative sample of these objects.
Moreover, the observed pattern of radial-velocity variations is often complicated by differential motions in
the extended atmospheres of these objects. A detailed analysis of radial velocities based on data taken with
high spectral and temporal resolution for selected — the brightest — PPNe reveals differences in the behavior
of radial velocities inferred from lines of different excitation, which form at different depths in the atmosphere
of the star. For example, Bakker et al. [36] analyzed the spectrum of the IRAS source identified with the
peculiar supergiant HD101584 and found eight categories of spectral lines with fundamentally different
temporal behavior of profiles, half-widths, and shifts (and hence of Vr values). In particular, the highest-
excitation absorption features, which form near the star’s photosphere, exhibit radial-velocity variations due
to the orbital motion in the binary system. At the same time, low-excitation lines with PCyg-type profiles
form in the stellar-wind region and are indicative of mass outflow. The systemic velocity has been confidently
determined from radio emissions of CO and OH molecules.
5. Spectral atlas
Table 2. Spectra used to create this atlas
αPer HD56126
∆λ, Date Spect- Date Spect-
Å rograph rograph
4010–5460 11.11.05 NES 12.11.05 NES
5460–6010 12.11.05 NES 9.03.04 NES
6010–6640 4.03.99 Lynx 9.03.04 NES
6640–8790 10.03.93 Lynx
Our comparative atlas of the spectra of HD56126 and αPer includes 94 plots representing 40 Å-long
spectral fragments. Some of them are shown in Figs. 1, 3, 4 and 6 to illustrate the differences between the
Klochkova et al.: Spectroscopy of HD56126 9
6310 6320 6330 6340 6350
Figure 6. Same as Fig. 1, but for spectral fragment containing the Siii λ 6347 Å line.
intensities and profiles of lines in the spectra of two stars of similar temperature and luminosity. The full
version of the atlas is available at http://www.sao.ru/hq/ssl/Atlas/Atlas.html.
In the wavelength interval 4010–6640ÅÅ the atlas gives the complete spectra of both objects. However,
in the more long-wavelength portion, up to 8790 Å, part of the spectrum has been lost in gaps between
echelle orders and the remaining portions are overcrowded by telluric lines. The atlas therefore gives only
the most informative fragments for this part of the spectrum of HD56126.
The spectrum of HD56126 is variable — line profiles, differential line shifts, and radial velocities vary
from date to date, and therefore we performed no averaging of any kind — different spectral intervals are
represented in the atlas by different spectra indicated in Table 2. For each wavelength interval, we selected
from among the available spectra the one with the highest resolution and signal-to-noise ratio.
We supplement graphic data in the atlas with tables. In Table 3 column 1 gives the results of identification
of spectral features; column 2, the laboratory wavelengths used to measure the radial velocities; columns
3 and 5, the central residual line intensities “r”, and columns 4 and 6, the heliocentric radial velocities Vr
measured from the line cores.
To identify atomic and molecular lines in the spectrum of HD56126, we use the atlases and tables of
solar spectrum [37, 38, 39, 40], the Moore tables for multiplets [41, 42], and electronic tables to the paper
by Bakker et al. [19]. We also use VALD database [43]. We supplement the standard identification criteria
(wavelength, relative line intensity, specific line profile) by two additional ones. One of these new criteria
uses the chemical composition anomalies of HD 56126 mentioned above and the spectrum of the comparison
star. The second new criterion can be applied only to sufficiently strong lines (r < 0.5), which in some of
our spectra exhibit a sharp variation of radial velocity with line depth. Several rather strong lines remained
unidentified in the spectrum of HD56126. Some of them can be seen in the fragments of the atlas presented
here: the λ 6550 Å line in Fig.1, the λ 5845 and 5852 Å lines in Fig. 4, and the λ 6347 Å line in Fig. 6.
Compared to the lines in the spectrum of αPer, those in the spectrum of HD56126 are less blended,
because they are narrower and, in addition, many of these lines are weaker due to low metallicity of the
star. However, by no means all absorptions can be used for reliable measurement of radial velocities. Table 3
lists about one and half thousand identifications for both stars and only 940 Vr measurements for HD 56126
obtained mostly from lines with minimal blending or from lines with the strongest difference of intensity in
the spectra of two stars.
http://www.sao.ru/hq/ssl/Atlas/Atlas.html
10 Klochkova et al.: Spectroscopy of HD56126
Conclusions
We use numerous high-resolution observations (R=25000 and 60000) made with the echelle spectrographs
of the 6-m telescope to perform a detailed analysis of the optical spectrum of the post-AGB star HD56126
identified with the IR source IRAS 07134+1005. We identified numerous absorptions of neutral atoms and
ions in the wavelength interval from 4010 to 8790 ÅÅ and measured their depths and the corresponding
radial velocities. We identified absorption bands of the C2, CN, and CH molecules, and interstellar bands
(DIB). In addition to the known variability of the profile of the Hα line, we found variations of the profiles
of a number of Feii and Baii lines. We produced an atlas of the spectra of HD56126 and its comparison star
αPer.
An analysis of our radial velocities determined from all spectra of our collection leads us to conclude
that:
– the accuracy of our radial-velocity data for HD 56126 allows them to be combined with the most accurate
of earlier published measurements;
– we found the behavior of Vr values to differ for lines of different excitation degree, which form at different
depth in the stellar atmosphere. The half-amplitude of the variations of radial velocities measured from
weak absorptions (r→ 1) is equal to 2–3 km/s;
– we confirm the stability of the expansion velocity of the circumstellar envelope of HD56126 as measured
from C2 and Nai lines;
– we reveal the complex and variable shape of the profiles of strong lines (not only hydrogen lines, but
also absorption features of Feii, Yii, Baii, and other elements), which form in the expanding atmosphere
(wind base) of the star. To study the kinematic state of the atmosphere, one needs measurements of
radial velocities for individual details of these profiles;
– we demonstrate the necessity of high and even superhigh spectral resolution for studying stellar and
circumstellar lines, respectively, in the spectrum of HD56126.
Acknowledgments
This work is supported by the Russian Foundation for Basic Research (project code 05–07–90087), the
Presidium of the Russian Academy of Sciences (program “Origin and Evolution of Stars and Galaxies“,
the Branch of Physical Sciences of the Russian Academy of Sciences (program “Extended Objects in the
Universe”). This publication is based on work supported by Award No. RUP1–2687–NA–05 of the U.S.
Civilian Research and Development Foundation (CRDF).
This work makes use of the SIMBAD, NASA ADS, and VALD astronomical databases.
Klochkova et al.: Spectroscopy of HD56126 11
References
1. T. Blöcker, Astrophys. J. 299, 755 (1995).
2. S. Kwok, Annu. Rev. Astron. & Astrophys. 31, 63 (1993).
3. T. Ueta, M. Meixner, and M. Bobrowsky, Astrophys. J. 528, 861 (2000).
4. I.A. Crawford and M.J. Barlow, MNRAS 311, 370 (2000).
5. V.G. Klochkova, MNRAS 272, 710 (1995).
6. V.G. Klochkova, Bull. Spec. Astrophys. Observ. 44, 5 (1998).
7. L. Decin, H. van Winckel, C. Waelkens, and E. Bakker, Astron. & Astrophys. 332, 928 (1998).
8. V.E. Panchuk, V.G. Klochkova, I.D. Najdenov, Preprint of the Special Astrophysical Observatory of the Russian
Academy of Sciences No. 135 (1999).
9. V.E. Panchuk, N.E. PIskunov, V.G. Klochkova, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 169 (2002).
10. V.G. Klochkova, S.V. Ermakov, V.E. Panchuk, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 137 (1999).
11. V.E. Panchuk, V.G. Klochkova, I.D. Najdenov, et al., Preprint of the Special Astrophysical Observatory of the
Russian Academy of Sciences No. 139 (1999).
12. V.E. Panchuk, M.V. Yushkin, I.D. Najdenov, Preprint of the Special Astrophysical Observatory of the Russian
Academy of Sciences No. 179 (2003).
13. M.V. Yushkin, V.G. Klochkova, Preprint of the Special Astrophysical Observatory of the Russian Academy of
Sciences, No. 206 (2005).
14. G.A. Galazutdinov, Preprint of the Special Astrophysical Observatory of the Russian Academy of Sciences No. 192
(1992).
15. R. Oudmaijer and E.J. Bakker, MNRAS 271, 615 (1994).
16. E.J. Bakker, D.L. Lambert, H. van Winckel, et al., Astron. & Astrophys. 336, 263 (1998).
17. H. van Winckel, R. Oudmaijer, and N.R. Trams., Astron. & Astrophys. 312, 553 (1996).
18. D. Barthès, A. Lèbre, D. Gillet, and N. Mauron, Astron. & Astrophys. 359, 168 (2000).
19. E.J. Bakker, L.B.F.M. Waters, H.J.G.L.M. Lamers, et.al., Astron. & Astrophys. 310, 893 (1996).
20. E.J. Bakker, E.F. Dishoeck, L.B.F.M. Waters, and T. Schoenmaker, Astron. & Astrophys. 323, 469 (1997).
21. V.G. Klochkova, R. Szczerba, V.E. Panchuk, and K. Volk, Astron. & Astrophys. 345, 905 (1998).
22. V.G. Klochkova, R. Szczerba, V.E. Panchuk, Astron. Lett. 26, 88 (2000).
23. V.G. Klochkova, R. Szczerba, V.E. Panchuk, Astron. Lett. 26, 439 (2000)
24. V.G. Klochkova, E.L. Chentsov, Astron. Rep. 48, 301 (2004)
25. N. Kameswara Rao, A. Goswami, and D.L. Lambert, MNRAS 334, 129 (2002).
26. V.G. Klochkova, V.E. Panchuk, N.S. Tavolganskaya, G. Zhao, Astron. Rep. 83, 265 (2006).
27. S. Trammell, H.L. Dinerstein, and R.W. Goodrich, Astrophys. J. 108, 984 (1994).
28. V. Bujarrabal, J. Alcolea, and P. Planesas, Astron. & Astrophys. 257, 701 (1992).
29. A. Lèbre, N. Mauron, D. Gillet, and D. Barthes, Astron. & Astrophys. 310, 923 (1996).
30. A. Lèbre, A. B. Fokin, D. Barthes, D. Gillet, and N. Mauron, Astrophys. Space Sci. 265, 105 (2001).
31. A.A. Ferro, PASP 96, 641 (1984).
32. L.B.F.M. Waters, C. Waelkens, M. Mayor, and N.R. Trams, Astron. & Astrophys. 269, 242 (1993).
33. C. Waelkens, H.J.G.L.M. Lamers, L.B.F.M. Waters, et al., Astron. & Astrophys. 242, 433 (1991).
34. H. van Winckel, C. Waelkens, and L.B.F.M. Waters, Astron. & Astrophys. 293, L25 (1995).
35. R.D. McClure, MNRAS 96, 117 (1984).
36. E. J. Bakker, H.J.G.L.M. Lamers, L.B.F.M. Waters, et al., Astron. & Astrophys. 307, 869 (1996).
37. R.L. Kurucz, I. Furenlid, and J.T.L. Brault, Nat. Solar Observ. Atlas, New Mexico: National Solar Observatory
(1984).
38. L. Wallace, K. Hinkle, and W. Livingston, Nat. Solar Obs. Techn. Rep. No.00–001, Tucson (2000).
39. A.K. Pierce and J.B. Breckinridge, Contr. Kitt Peak Nat. Obs. No. 559 (1973).
40. J.W. Swensson, W.S. Benedict, L. Delbouille, and G. Roland, “The solar spectrum from λ 7498 to λ 12016. A
table of measures and identifications”, Mem. Soc. Roy. Sci. Liege, Vol.hors ser. No.5 (1970).
41. C.E. Moore, Contrib. Princeton University Observ. No.20, part I (1945).
42. C.E. Moore, Contrib. Princeton University Observ. No.20, part II (1945).
43. N.E. Piskunov, F. Kupka, and T.A. Ryabchikova, A&AS 112, 525 (1995).
12 Klochkova et al.: Spectroscopy of HD56126
Table 3. List of lines identified in the spectra of HD 56126 and αPer. Columns 3 and 5 list the central
residual intensities of the lines (the continuum level is set to 1), and columns 4 and 6, the heliocentric
velocities Vr.
αPer HD56126
Element λ Å r Vr r Vr
TiII(11) 4012.39 0.13: −2.2 0.05 81.7
FeI(557) 4013.64
FeI(485) 4013.82 0.53:
ScII(8) 4014.53 0.32: −3.5 0.49
CeII(157) 4014.90 0.56
NiII(12) 4015.47 0.50: 0.64 84.8:
CeII(256) 4015.88 0.74: 83.0:
FeI(560) 4016.42 0.74: −1.0
FeI(279) 4017.10
FeI(527) 4017.15 0.50: −1.1 0.85:
NiI(171) 4017.47 0.7: 0.9:
MnI(5) 4018.10 0.47:
FeI(560) 4018.27
ZrII(54) 4018.38 0.53 82.5
NdII(19) 4018.83 0.89:
VII(201) 4019.05 0.86: −3.0:
FeI(556) 4020.07
NdII(19) 4020.87 0.80 82.4:
CoI(16) 4020.90 0.86: −2.3
NdII(36) 4021.33 0.79 82.0:
FeI(120) 4021.61
FeI(278) 4021.87 0.45: −3.9
FeI(654) 4022.74
NdII 4023.01 0.75: 81.2:
VII(32) 4023.38 0.47: −2.5: 0.56 82.5
FeI(277) 4024.10
ZrII(54) 4024.45 0.33: 85.1:
TiI(12) 4024.58 0.37: −1.5:
TiII(11) 4025.13 0.36: −2.3 0.42: 83.5:
TiII(87) 4028.34 0.29: −1.7 0.28: 84.8:
FeI(556) 4029.63 0.43: −0.6:
ZrII(41) 4029.68 0.28 83.4:
NdII(32) 4030.47 0.60:
FeI(560) 4030.50
MnI(2) 4030.76 0.18: 0.63 81.0:
CeII(108) 4031.34 0.52
FeII(151) 4031.44
LaII(40) 4031.68 0.42 84.6:
MnI 4031.78 0.46: −2.0
FeI(44) 4032.63 0.52:
FeII(126) 4032.95 0.63
MnI(2) 4033.06 0.26: −3.3:
ZrII(42) 4034.08 0.52: 83.7
MnI(2) 4034.48 0.39: −2.6:
Klochkova et al.: Spectroscopy of HD56126 13
αPer HD56126
Element λ Å r Vr r Vr
ZrII(70) 4034.84 0.85: 83.1:
VII(32) 4035.60 0.35: 0.61 85.1
MnI(5) 4035.72
VII(9) 4036.76 0.68: −2.0 0.81 82.2:
GdII(49) 4037.39 0.90: 0.83 84.1:
CeII(218) 4037.67 0.81: 82.7:
GdII(49) 4037.90 0.85: 0.81:
NdII(31) 4038.12 0.83:
VII(32) 4039.56 0.82: −2.0 0.89:
FeI 4040.09 0.76:
ZrII(54) 4040.24 0.58 83.5
FeI(655) 4040.64 0.52:
CeII(138) 4040.76 0.52 82.6:
NdII(30) 4040.80
MnI(5) 4041.35 0.48: −2.5 0.84:
CeII(140) 4042.58 0.60:
SmII(4) 4042.72 0.59
SmII(9) 4042.90 0.53 83.1:
FeI(276) 4043.90 0.56
FeII(172) 4044.01 0.89 81.2:
FeI(359) 4044.61 0.60 −3.3:
GdII(49) 4045.15 0.72:
ZrII(30) 4045.63
FeI(43) 4045.81 0.12 −4.6 0.22:
FeI(557) 4046.06
VII(177) 4046.27
CeII(81) 4046.34 0.72 80.5
ZrII(43) 4048.68 0.29 84.2
MnI(5) 4048.75 0.39 −4.3
ZrII(43) 4050.32 0.66 0.34 82.6:
VII(32) 4051.04
NdII(66) 4051.15 0.69 0.75
FeI(700) 4051.31
CrII(19) 4051.97 0.54 0.64:
TiII(87) 4053.82 0.33 0.39 83.2
FeI(698) 4054.82 0.51
CeII(82) 4054.99 0.70 81.2:
MnI(5) 4055.54 0.68 −3.1
TiII(11) 4056.19 0.60 −0.6 0.79 84.7
FeII(212) 4057.46 0.78 85:
MgI(16) 4057.50 0.48 −4.9
CoI(16) 4058.22 0.75 −4.2: 0.89
FeI(120) 4058.76 0.66 0.91
MnI(5) 4058.92
FeI(767) 4059.79 0.82 −3.3:
NdII(63) 4059.96 0.88
NdII(10) 4061.08 0.75 −2.4 0.66 81.0:
FeII(189) 4061.79 0.84:
CeII(34) 4062.23 0.79 82.3
14 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(359) 4062.44 0.56 −1.0
FeI(43) 4063.59 0.19 −4.0: 0.40 82.9
TiII(106) 4064.37 0.67 −1.5: 0.82 81.1:
VII(215) 4065.09 0.74 0.78
FeI(698) 4065.38
NiII(11) 4067.03 0.38 0.59 83.8
CeII(22) 4067.28 0.64 86:
FeI(559) 4067.98 0.54 −3.1 0.87 83.0
CeII(82) 4068.84 0.75 81.8
FeI(558) 4070.78 0.60
ZrII(54) 4071.09 0.59 82.3:
FeI(43) 4071.74 0.23 −3.8 0.46 82.8
CrII(26) 4072.56 0.68 −3.1 0.77 85.5:
CeII(109) 4072.92 0.78 83.8:
CeII(4) 4073.48 0.61 83.4:
FeI(558) 4073.76 0.64
GdII(44) 4073.76 0.70:
FeI(524) 4074.79 0.61 −2.8 0.95:
NdII(62) 4075.12 0.85:
CeII(57) 4075.70
SmII(51) 4075.85 0.53 −2.3: 0.51
FeI(558) 4076.63
LaII(11) 4076.71 0.37 −3.3: 0.74:
ZrII(54) 4077.05 0.53:
CrII(19) 4077.50
SrII(1) 4077.71 0.09 −2.8 0.10
DyII 4077.96
CeII(19) 4078.32 0.67:
FeI(217) 4078.35 0.56: −0.7:
MnI(5) 4079.3: 0.58 0.95:
FeI(359) 4079.84 0.69 −2.1:
FeI(558) 4080.21 0.74
CeII(44) 4080.44 0.72 82.4:
CrII(165) 4081.21 0.80: 0.74 82.4:
CrII(165) 4082.29 0.77
CeII(60) 4083.23 0.61 82.2
MnI(5) 4083.63 0.52 −1.8:
FeI(698) 4084.49 0.62 −1.9: 0.88
CeII(172) 4085.23 0.51 0.70 85.6
FeI(559) 4085.30
VII(214) 4085.67 0.61
ZrII(54) 4085.68 0.61 84.8:
CrII(26) 4086.13 0.70 −3.3: 0.85 84.0:
LaII(10) 4086.71 0.62 −2.1: 0.47 83.0
FeII(28) 4087.28 0.65 0.72 84.6:
FeII(39) 4088.75 0.74 −2.9:
CrII(19) 4088.90 0.76
ZrII(29) 4090.52 0.70 −3.7 0.43 82.4
CoI(29) 4092.39 0.62:
Klochkova et al.: Spectroscopy of HD56126 15
αPer HD56126
Element λ Å r Vr r Vr
HfII(6) 4093.16 0.84: −3.2: 0.65: 82.5
CeII(160) 4093.96 0.83: 82.0:
CaI(25) 4094.93 −1.1:
FeI(217) 4095.98
ZrII(15) 4096.63 0.50 83.6
FeI(558) 4097.08 −3.2:
Hδ 4101.74 0.08 −2.0 0.06 96.0:
SiI(2) 4102.94 −2.9:
DyII 4103.31 81.2:
FeI(356) 4104.12 −1.6:
CeII(156) 4105.00 0.67:
CeII(160) 4106.13 0.79:
FeI(217) 4106.26 0.64:
CeII(139) 4106.88 0.78:
SmII(50) 4107.39 0.63: 85.1:
FeI(354) 4107.49 0.47 −3.4
CaI(39) 4108.53 0.76:
FeI(558) 4109.06 0.67:
NdII(17) 4109.07 0.72: 83.3
NdII(10) 4109.46 0.61: 82.0
MgII(21) 4109.54
FeI(357) 4109.80 0.51:
ZrII(30) 4110.05 0.62: 82.4
CeII(29) 4110.39 0.74: 83.6:
CrII(18) 4110.99 0.52 −3.5 0.64 83.0:
CeII 4111.39 0.75:
FeII(188) 4111.90 0.75: 0.86 82.3
FeI(695) 4112.32 0.80:
CrII(18) 4112.55 0.91 82.5:
FeI(1103) 4112.96 0.62:
CrII(18) 4113.22 0.86 83.6
CeII(137) 4113.73 0.86 0.80 81.8:
FeI(357) 4114.45 0.69 −2.7 0.95: 82.5:
KII(2) 4114.99
CeII(22) 4115.37 0.79 81.6
CrII(181) 4116.66 0.86
CeII(35) 4117.01 0.79 82.4:
CeII(77) 4117.29 0.83: 82:
FeI(700) 4117.85
CeII(11) 4118.15 0.83: 0.69 81.7
FeI(801) 4118.54 0.38
SmII(51) 4118.55 0.72
CeII(89) 4119.01 0.83 80.7:
FeII(21) 4119.51 0.65: −1.6 0.77:
CeII(22) 4119.79 0.64 85:
FeI(423) 4120.21 0.72:
CeII(112) 4120.83 0.87 0.71 81.0
CoI(28) 4121.32 0.67: −1.6: 0.95:
FeI(356) 4121.81 0.70: −2.3 0.92
16 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(28) 4122.66 0.37 −4.6 0.50 82.5
LaII(41) 4123.23 0.59 0.46 83.8:
FeI(217) 4123.75 0.62
CeII(60) 4123.87 0.62 81.5
FeII(22) 4124.78
YII(14) 4124.91 0.52 0.46
FeI(1103) 4125.62
FeI(354) 4125.88 0.71: 0.95:
FeI(695) 4126.18 0.69: −3.8: 0.97 85:
CeII(4) 4127.37 0.65 82.4
FeI(357) 4127.61
FeI(558) 4127.80 0.42: 0.68:
SiII(8) 4128.07 0.41: −1.5: 0.50 84.2
FeII(27) 4128.74 0.49 0.63 82.7
CeII(227) 4129.18 0.61: 0.75
EuII(1) 4129.72 0.60 0.85 81.1:
BaII(4) 4130.65 0.44
CeII(209) 4130.71 0.56
FeI(43) 4132.06 0.26 −1.5 0.58 83.4:
FeI(357) 4132.90 0.60 −4.5:
CeII(4) 4133.80 0.61 −2.0 0.58 82.0
FeI(357) 4134.68 0.46 0.83 83.6
NdII 4135.33 0.83 0.73
CeII(188) 4135.44
FeI(726) 4137.00 0.61 −3.0
CeII(2) 4137.65 0.67 0.57: 80.7:
FeII(150) 4138.21 0.78:
FeII(39) 4138.40 0.70 0.73:
FeI(18) 4139.93 0.82 −4.1
FeI(695) 4140.41 0.86 −2.1
LaII(40) 4141.73 0.72 81.2
HfII(87) 4141.84 0.77:
CeII(10) 4142.40 0.68 0.69 81.8
VII(226) 4142.90 0.79
FeI(523) 4143.42 0.41: 0.78 82.7
FeI(43) 4143.87 0.29 −2.7 0.59 82.1
CeII(3) 4144.49 0.86 −1.8: 0.76 83.6
CeII(9) 4145.00 0.80 0.70 81.7
CrII(162) 4145.76 0.82
CeII(203) 4146.23 0.68 82.2
FeI(42) 4147.67 0.56 −3.7: 0.93 84.0:
ZrII(41) 4149.20 0.37 0.37
FeI(694) 4149.36
CeII 4149.94 0.72 0.61 81.0:
FeI(695) 4150.25 0.76
ZrII(42) 4150.97 0.67 −3.2 0.43 82.8
CeII(2) 4151.97 0.55 82.1
FeI(18) 4152.17 0.45
FeI(695) 4153.90 0.49 −0.2: 0.85 82.3
Klochkova et al.: Spectroscopy of HD56126 17
αPer HD56126
Element λ Å r Vr r Vr
FeI(355) 4154.50 0.43 0.88 83.2
FeI(694) 4154.81 0.88 83.5
ZrII(29) 4156.25 0.43 −4.2: 0.38 80.9:
FeI(354) 4156.80 0.46
FeI(695) 4157.78 0.58 −3.2
FeI(695) 4158.80
HfII(41) 4158.90 0.64
CeII(246) 4159.03 0.80 80.6:
ZrII(42) 4161.21 0.35 84.2:
TiII(21) 4161.52 0.35 0.41 81.2:
SrII(3) 4161.80 0.49
TiII(105) 4163.64 0.33 −2.4 0.38 82.6
CeII(10) 4165.59 0.72 0.64 83.7
BaII(4) 4166.00 0.75 82.0
MgI(15) 4167.27 0.53 −2.1 0.79 83.2
CeII(29) 4167.80 0.74 0.85 82.7
CeII(173) 4169.88 0.76 0.71
FeI(482) 4170.91 0.52
TiII(105) 4171.90 0.41 84.3
FeI(650) 4171.91 0.28
FeI(689) 4172.64 0.85 81.8:
FeI(19) 4172.75 0.46
FeII(27) 4173.46 0.22 −1.2 0.34 84.4
TiII(105) 4174.07 0.49 −2.2 0.74 84.2:
FeI(19) 4174.91 0.63 −2.9
FeI(354) 4175.64 0.53 −2.0 0.78 83.2
FeI(689) 4176.57 0.60 −0.6 0.82
FeI(18) 4177.59 0.22
FeII(21) 4177.68 0.29: 83.0:
FeII(28) 4178.85 0.31 −1.5 0.38 84.5
CrII(26) 4179.43 0.49 0.60 83.9:
ZrII(99) 4179.81 0.49 82.4
FeI(354) 4181.75 0.38 −1.0: 0.78 83.4
FeI(476) 4182.39 0.71: −2.1
VII(37) 4183.45 0.60 0.82 81.1:
TiII(21) 4184.31 0.49 0.62 82.0:
FeI(355) 4184.89 0.59 −1.8 0.87 85.1:
CeII(124) 4185.33 0.93: 0.84 82.0
CeII(1) 4186.61 0.43 85.8:
FeI(152) 4187.04 0.41 −2.4 0.71 82.8:
FeII(152) 4187.80 0.36 −4.5 0.69 82.9
FeI(1116) 4188.73 0.68 −1.4 0.96 83.6
PrII(8) 4189.52 0.90: 83.1
FeI(940) 4189.56 0.84
TiII(21) 4190.29 0.67 −2.4 0.89 82.3
VII(25) 4190.40
CeII(169) 4190.63 0.87 80.8:
GdII(34) 4191.07 83.2:
FeI(152) 4191.43 0.38
18 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
ZrII(108) 4191.50 0.57
LaII(78) 4192.35 0.87:
CeII(79) 4193.10 0.87 0.72 84.0:
CeII(85) 4193.87 0.89 0.84 81.5
FeI(693) 4195.33 0.50 0.87 83.7:
CrII(161) 4195.41
FeI(693) 4196.21 0.58
LaII(41) 4196.55 0.60:
CeII(136) 4197.67 0.81
CeII(209) 4198.00 0.79
FeI(152) 4198.30 0.30 0.68
CeII(207) 4198.43
CeII(7) 4198.67 0.64 81.1:
FeI(522) 4199.09 0.40
FeII(141) 4199.09
NdII(15) 4199.10
YII(5) 4199.27 0.60
FeI(3) 4199.99 0.85
FeI(689) 4200.93 0.73 −2.6:
FeI(42) 4202.03 0.28 0.58 82.9
VII(25) 4202.34 0.80 82.6
CeII(186) 4202.94 0.78 0.71 82.6
LaII(53) 4204.03 0.52 −2.5: 0.80 81.9:
YII(1) 4204.75 0.50 80.8
VII(37) 4205.07 0.41 −3.0 0.65
MnII(2) 4205.39 0.51 0.79:
ZrII(133) 4205.91 0.84 81.1
HfII(74) 4206.59 0.85 83.7:
FeI(3) 4206.70 0.67 −1.2
MnII(2) 4207.23 0.66 −3.2:
CrII(26) 4207.35 0.92 83.1
FeI(689) 4208.61 0.66:
ZrII(41) 4208.98 0.56 −2.3
CrII(162) 4209.02 0.42 82.6:
CeII(3) 4209.41
VII(25) 4209.74 0.73 0.88 83.5:
FeI(152) 4210.35 0.47 −1.0
ZrII(97) 4210.62 0.64 82.3
ZrII(15) 4211.89 0.57 −2.6 0.39 83.5
CeII(169) 4213.04 0.88
FeI(355) 4213.65 0.71 −2.5 0.95:
CeII(203) 4214.03 0.84 82.5
FeI(274) 4215.43
SrII(1) 4215.52 0.15 −0.6 0.16 96.9
FeI(3) 4216.18 0.51 −2.9
CdII(49) 4217.20 0.88 82.5:
FeI(693) 4217.55 0.61 −2.6 0.75 83.3
FeI(800) 4219.36 0.51 −2.1 0.85 83.7
CaII(16) 4220.13 0.88:
Klochkova et al.: Spectroscopy of HD56126 19
αPer HD56126
Element λ Å r Vr r Vr
NdII(32) 4220.26 0.68
FeI(482) 4220.35
FeII(152) 4222.21 0.48
ZrII(80) 4222.41
CeII(36) 4222.60 0.52:
FeI(689) 4224.17
ZrII(29) 4224.28 0.50: 0.66 81.0
FeI(689) 4224.52
CrII(162) 4224.85 0.83 83.6
VII(37) 4225.22
PrII(8) 4225.33 0.73:
FeI(693) 4225.45 0.44
FeI(521) 4225.95 0.74:
CaI(2) 4226.72 0.21 −3.6 0.43 80.7:
FeI(693) 4227.43 0.32 −4.7 0.59:
NdII(19) 4227.72 0.73: 82.6
NdII(36) 4228.20
CI 4228.32 0.86 0.77 81.9
SmII(4) 4229.70 0.76 0.92:
FeI(41) 4229.76
LaII(83) 4230.95 0.92 83.2:
NiI(136) 4231.03 0.91
ZrII(99) 4231.64 0.52 83.5
HfII(72) 4232.43 0.86: 0.78 82.2
FeII(27) 4233.17 0.23 0.34 86.5
FeI(152) 4233.60 0.40:
NdII(20) 4234.20 0.83 81.9
VII(24) 4234.22 0.83
MnI(23) 4235.14
MnI(23) 4235.29 0.73
VII(5) 4235.74 0.46
FeI(152) 4235.94 0.31
ZrII(110) 4236.54 0.84: 0.64 83.0
LaII(41) 4238.38 0.63 82.3
FeI(693) 4238.81 0.52 −2.6 0.79 81.6
FeI(18) 4239.85 0.51 −3.8 0.67
CeII(2) 4239.91
FeI(764) 4240.38
CaI(38) 4240.45 0.77
CrII(31) 4242.37 0.47 −1.2 0.53 83.3
NiII(9) 4244.80 0.84 0.88 81.0:
FeI(352) 4245.26 0.61 0.94
FeI(691) 4245.35
HfII(72) 4245.84 0.72
CeII(158) 4245.98
FeI(906) 4246.09 0.69
ScII(7) 4246.83 0.25 −2.1 0.39 88.7:
NdII(14) 4246.88
FeI(693) 4247.42 0.47 −2.7
20 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(482) 4248.23 0.72
CeII(1) 4248.68 0.82 −2.8: 0.69 81.8
FeI(152) 4250.12 0.41 −1.7 0.69 82.6
FeI(42) 4250.79 0.33 −2.2 0.58 81.8
GdII(15) 4251.74 0.84 0.80 82.1
CrII(31) 4252.63 0.64 −3.0 0.74 82.4
CeII(77) 4253.36 0.81 82.5
CrI(1) 4254.34 0.35 −1.3 0.68 82.8
CeII(81) 4255.78 0.76 83.0
CeII(172) 4256.16 0.83:
NdII(59) 4256.24 0.81 −3.1 0.84:
CeII(123) 4257.12 0.92 81.0:
ZrII(15) 4258.05
FeII(28) 4258.15 0.34 −0.5 0.36
FeI(3) 4258.32
FeI(476) 4260.13
FeI(152) 4260.47 0.31 −1.5 0.57 83.2
CeII(19) 4261.16 0.95 81.2
CrII(31) 4261.92 0.49 −2.2 0.55 83.5
SmII(37) 4262.68 0.94 81.5:
CeII(254) 4263.43 0.78
FeI(692) 4264.21 0.84 −2.3
CeII(239) 4264.37 0.91 81.2
FeI(993) 4264.74 0.90
YII(71) 4264.88 0.78
ZrII(98) 4264.92
FeI(993) 4265.26 0.87
MnI(23) 4265.92 0.91 −2.5
ZrII(8) 4266.72 0.86 82.9
FeI(273) 4266.97 0.78 −3.8
FeI(482) 4267.83 0.73 −1.9 0.93 84:
CrII(192) 4268.93 0.75:
CI(16) 4269.02 0.68
CrII(31) 4269.29 0.65 0.69:
CeII(204) 4270.19 0.90 −2.8 0.77 81.5
CeII(21) 4270.72 0.82 81.0:
FeI(152) 4271.16 0.40 −2.7 0.70 82.0
FeI(42) 4271.76 0.25 −1.3 0.44 82.8
FeII(27) 4273.32 0.44 0.43:
ZrII(28) 4273.52
FeI(478) 4273.88 0.90:
CrI(1) 4274.79 0.37 −2.1 0.72 82.7
CrII(31) 4275.56 0.54 −1.7 0.57 83.6
FeI(597) 4276.68 0.87
ZrII(40) 4277.37 0.84 0.70 82.4
FeII(32) 4278.16 0.59 −1.6 0.71 82.8
VII(225) 4278.89 0.90 0.83 82.4:
SmII(27) 4279.68 0.92 82.7:
FeI(351) 4279.87 0.82
Klochkova et al.: Spectroscopy of HD56126 21
αPer HD56126
Element λ Å r Vr r Vr
CeII(225) 4280.14 0.88 82.2:
GdII(15) 4280.48 0.82 0.89 82.4
SmII(46) 4280.79 0.84:
SmII 4281.01
CrII(17) 4281.03 0.79
MnI(23) 4281.10
ZrII(182) 4282.21 0.58
FeI(71) 4282.40 0.41 −1.7
CaI(5) 4283.01 0.58 −2.3 0.92 81.7
CrII(31) 4284.20 0.60 −1.2 0.69 83.1
MnII(6) 4284.43 0.82: 83.0:
NdII(10) 4284.51
CeII(11) 4285.37 0.82 82.8
FeI(597) 4285.44 0.71 −2.3
TiI(44) 4286.01 0.84
FeI(414) 4286.47 0.84 −1.9
ZrII(69) 4286.51 0.63 82.6
LaII(75) 4286.97 0.76 −3.3 0.75 81.7
TiII(20) 4287.88 0.36 0.1 0.51 82.9
CeII(135) 4289.45 0.79 82.0:
CrI(1) 4289.72 0.33:
TiII(41) 4290.21 0.24 −2.0: 0.36 85.0:
TiI(44) 4290.94 0.79 −3.5:
FeI(3) 4291.46 0.76 −1.4
MnII(6) 4292.25 0.82
CeII(205) 4292.77 0.88 83.0:
ZrII(110) 4293.14 0.91 0.63 82.0
TiII(20) 4294.10 0.28 −2.2 0.37 83.9
FeI(41) 4294.12
ScII(15) 4294.78 0.55 −2.3 0.73 82.5
LaII(53) 4296.05 0.73 0.65 83.1:
FeII(28) 4296.57 0.35 −0.4 0.37
CeII(2) 4296.68
PrII(7) 4297.76 0.92 84.3:
FeII(520) 4298.04 0.78
FeI(152) 4299.23 0.31 0.60
CeII(47) 4299.36
TiII(41) 4300.05 0.24 −0.7 0.31 93.0:
TiI(44) 4301.09 0.74:
ZrII(109) 4301.81
TiII(41) 4301.92 0.31 −0.8 0.40 81.5
CaI(5) 4302.53 0.46 −3.0: 0.79 83.2
FeII(27) 4303.17 0.34 −1.7 0.41 84.2:
NdII(10) 4303.59
FeI(414) 4304.55 0.86 −3.4
FeI(476) 4305.45 0.49 83.5:
ScII(15) 4305.71 0.37
CeII(1) 4306.72 0.81 0.75 82.3
CaI(5) 4307.75
22 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
TiII(41) 4307.89 0.21 −3.7: 0.40 82.4
FeI(42) 4307.90
ZrII(88) 4308.94 0.70 82.4
FeI(849) 4309.03 0.72:
YII(5) 4309.63 0.38 0.40 84.8:
CeII(126) 4309.74
CeII(133) 4310.70 0.91 82.1
ZrII(99) 4312.23 0.84 82.9
TiII(41) 4312.86 0.33 −2.3 0.41 83.5
ScII(15) 4314.09 0.22 0.36:
FeII(32) 4314.30
TiII(41) 4314.98 0.25 −1.1 0.43 83.8
GdII(43) 4316.05 0.97: 0.95 82.0:
TiII(94) 4316.80 0.58 −1.6 0.69 82.7
ZrII(40) 4317.32 0.82: 0.56 81.9
CaI(5) 4318.65 0.56 −0.1 0.90 83.4:
ScII(15) 4320.74 0.22 0.38
TiII(41) 4320.95
FeI 4321.79 0.87 −1.9
LaII(25) 4322.50 0.88 −0.9 0.75 82.7
ZrII(141) 4323.62 0.91 81.0
FeI(70) 4325.00
ScII(15) 4325.01 0.33 −2.6 0.46 81.9:
FeI(42) 4325.76 0.25 −2.4 0.43 81.4:
BaII(7) 4326.74 0.73 0.90
MnII(6) 4326.76
FeI(761) 4327.10
GdII(15) 4327.13 0.75 0.92 82.5
FeI(597) 4327.91 0.83 −1.6 0.89 83.0
SmII(15) 4329.03 0.89 −2.8 0.92
TiII(94) 4330.24 0.51 0.64
CeII(82) 4330.45
TiII(41) 4330.70 0.44 −3.5 0.59 81.8:
NiI(52) 4331.65 0.77 −2.7
VII(23) 4331.79 0.87
ZrII(132) 4333.28 0.59: 82.1
LaII(24) 4333.76 0.59 −0.7 0.53: 82.4
LaII(77) 4334.96 0.80: 81.7:
CaII(89) 4336.26 0.69:
FeI(41) 4337.05 0.36:
TiII(94) 4337.33
CeII(82) 4337.78 0.38:
TiII(20) 4337.92 0.23: −3.7: 0.33
NdII(68) 4338.70 0.49: 0.52 82.5:
Hγ 4340.47 0.09 −2.1 0.08 97.0:
TiII(32) 4341.36 0.30:
FeI(645) 4343.26 0.61:
TiII(20) 4344.29 0.30: 0.47: 82.1
CeII(251) 4345.96 0.80:
Klochkova et al.: Spectroscopy of HD56126 23
αPer HD56126
Element λ Å r Vr r Vr
FeI(598) 4346.56 0.74:
FeI(828) 4347.84 0.78
FeI(414) 4348.94 0.85: −1.8:
CeII(59) 4349.79 0.85 0.78 81.2
VII(36) 4349.97
TiII(94) 4350.84 0.52 0.71 83.2
FeII(27) 4351.77 0.23 −1.1 0.36: 85.6:
MgI(14) 4351.91
FeI(71) 4352.73 0.53 −2.5
CeII(220) 4352.73 0.76
FeII(213) 4354.36
LaII(58) 4354.40 0.70 83.3:
ScII(14) 4354.61 0.58 −5.7:
CaI(37) 4355.19 0.81 −3.3:
FeII 4357.57 0.90 83.8:
NdII(10) 4358.17 0.80 81.6
NdII(57) 4358.70
YII(5) 4358.72 0.58 −5.6 0.48 83.7
NiI(86) 4359.63
GdII(67) 4359.64 0.57
ZrII(79) 4359.74 0.43 82.8
FeII 4361.25 0.93 −1.7 0.92:
CeII(157) 4361.66 0.92:
SmII(45) 4362.04
NiII(9) 4362.09 0.80 −2.0 0.86 82.5
LaII(133) 4363.05 0.93 −1.9 0.95:
MoII(3) 4363.64 0.92: 81.5:
GdII(33) 4364.14 0.91: 81.9:
YII(70) 4364.17 0.96
CeII(135) 4364.66 0.88 −1.9 0.74 81.4
LaII(53) 4344.66
FeI(415) 4365.90 0.92
FeI(414) 4367.58
TiII(104) 4367.66 0.41 −0.6: 0.56 82.6
FeI(41) 4367.91
CeII(227) 4368.23 0.82: 0.79 83.0:
FeII 4368.26
NdII(11) 4368.63 0.93: 0.91: 82.3:
FeII(28) 4369.40 0.53 0.67 83.1
FeI(518) 4369.77 0.66: 0.90:
ZrII(79) 4370.96 0.73: 0.48 81.9
CI(14) 4371.37 0.69: 0.70 83.2:
FeII(33) 4372.22 0.92 0.92
FeI(214) 4373.57 0.83
CeII(202) 4373.82 0.83 81.5:
ScII(14) 4374.46 0.30 0.43
TiII(93) 4374.82 0.28 0.44: 81.6:
YII(13) 4374.94 0.29: 94.7:
NdII(8) 4375.04
24 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(2) 4375.93 0.49 −2.1 0.78 81.1
FeI(471) 4376.78 0.91 −1.5
MoII(3) 4377.77 0.94: −3.1: 0.92 82.3:
LaII(77) 4378.10 0.93
VI(22) 4379.23 0.82 −1.2:
ZrII(88) 4379.78 0.70 −3.3
CeII(155) 4380.06 0.43 83.0
CdII(68) 4380.64 0.91 0.98:
CeII(2) 4382.17 0.87 −2.9 0.73: 81.2:
FeI(799) 4382.78 0.82 −1.7:
ZrII(97) 4383.10 0.85:
FeI(41) 4383.54 0.25 −2.2 0.40 82.6
FeII(32) 4384.32 0.50 0.61 83.9
ScII(14) 4384.81 0.46 0.74
FeII(27) 4385.38 0.36 −2.2 0.44 84.0
NdII(50) 4385.66
CeII(57) 4386.84
TiII(104) 4386.85 0.51 0.57 81.0:
FeI(476) 4387.90 0.79
CeII(5) 4388.01 0.87 81.0:
FeI(830) 4388.41 0.72 −2.2
ZrII(140) 4388.50 0.90 80.0:
FeI(2) 4389.25 0.90 −3.1
VI(22) 4389.99 0.87 −2.0:
MgII(10) 4390.56 0.76
FeI(414) 4390.96
TiII(61) 4391.02 0.48 0.67 82.2
CeII(81) 4391.66 0.76 0.66 82.1
TiII(51) 4394.04 0.44 −2.6 0.54 83.2
TiII(19) 4395.03 0.25 −1.5 0.36 87.7
TiII(61) 4395.84 0.48 −2.5 0.58 83.0
YII(5) 4398.02 0.49 0.44 84.1
TiII(61) 4398.29
CeII(81) 4398.79 0.89 80.4:
CeII(81) 4399.20 0.75 82.4
TiII(51) 4399.77 0.34 −2.3 0.44 83.1
ScII(14) 4400.40 0.36 0.50 83.3
NdII(10) 4400.83 0.80
FeII(828) 4401.29 0.55
ZrII(68) 4401.35 0.84 83.6:
ZrII(79) 4403.35 0.76 0.60 81.9
FeI(41) 4404.75 0.28 −1.6 0.49 82.5
VI(22) 4406.65 0.90 −3.3
GdII(103) 4406.67 0.94 81.9:
CeII(64) 4407.28 0.90 81.1:
FeI(68) 4407.70 0.56 −2.6 0.79 81.5
FeI(68) 4408.42 0.58 −2.2 0.92 83.0:
PrII(4) 4408.84 0.85 82.0
TiII(61) 4409.24 0.50 0.77:
Klochkova et al.: Spectroscopy of HD56126 25
αPer HD56126
Element λ Å r Vr r Vr
TiII(61) 4409.52 0.75:
NiI(88) 4410.52
CeII(33) 4410.64 0.79:
TiII(115) 4411.08 0.58 −2.8 0.62 82.3
TiII(61) 4411.93 0.64 −1.1 0.78 84.2:
NdII(9) 4412.27 0.93
FeII(32) 4413.59 0.69 0.3: 0.79 84.5:
PrII(26) 4413.77
ZrII(79) 4414.54 0.82: 0.55 82.5
FeI(41) 4415.12 0.29 −0.7: 0.57 83.4
ScII(14) 4415.56 0.38: 0.54 82.3
FeII(27) 4416.82 0.38 −2.0 0.43 83.4
TiII(40) 4417.72 0.34 −2.2 0.41 82.9
TiII(51) 4418.34 0.48 −2.1 0.59 82.2
CeII(2) 4418.78 0.85: 0.70 81.6
SmII(32) 4420.53 0.87
ScII(14) 4420.67 0.79
SmII(37) 4421.13 0.94 0.88 82.3
TiII(93) 4421.94 0.58 −1.9 0.68 82.9
FeI(350) 4422.57 0.55 −1.4
YII(5) 4422.59 0.46 82.7
FeI(412) 4423.14 0.76
TiII(61) 4423.22 0.92 82.9
CeII(21) 4423.68 0.89 81.2
FeI(830) 4423.84 0.88
SmII(45) 4424.34 0.82 −4.2: 0.83 81.4
CaI(4) 4425.44 0.62 −1.5 0.93 81.3
FeI(2) 4427.31 0.46 0.87: 81.7:
TiII(61) 4427.90 0.82 −2.2: 0.79 82.5
CeII(19) 4429.27 0.86 −3.1 0.73 83.0
LaII(38) 4429.92 0.68 0.60 81.3
FeI(68) 4430.62 0.63 −2.9 0.95 81.3:
ScII(14) 4431.37 0.75 −2.7 0.92 81.3
TiII(51) 4432.10 0.79 0.94 83.6
LaII(11) 4432.95 0.94
FeI(830) 4433.22 0.77 −2.0
GdII(82) 4433.64 0.93
SmII(41) 4433.89 0.76 0.84 84.5:
SmII(36) 4434.32 0.86 80.7
CaI(4) 4434.96 0.49 0.0 0.89 82.2
FeI(2) 4435.15
EuII(4) 4435.58 0.89 83.9:
CaI(4) 4435.68 0.57
GdII(117) 4436.23 0.89 0.95
FeI(516) 4436.93 0.88 −1.4
CeII(169) 4437.61 0.95: −1.0: 0.93 81.7
GdII(67) 4438.13 0.97:
GdII(44) 4438.27
FeI(828) 4438.35 0.91 −2.7
26 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(32) 4439.16 0.95 −3.8 0.95 83.0:
FeI 4439.89 0.95
ZrII(79) 4440.45 0.81 −1.3: 0.57 83.4
CeII(238) 4440.88 0.89 0.89:
TiII(40) 4441.73 0.55 −2.0 0.69 82.8
FeI(68) 4442.34 0.52 −0.9
ZrII(53) 4442.50 0.72 80.8:
ZrII(88) 4443.00 0.53 0.43 83.1
FeI(350) 4443.20
TiII(19) 4443.80 0.29 −1.5 0.42 86.8
LaII(133) 4443.94
TiII(31) 4444.56 0.46 −2.9 0.56 83.3
ZrII(96) 4445.88 0.87 84.8
NdII(49) 4446.39 0.86 −2.3: 0.84 80.3
FeI(68) 4447.72 0.56 −1.6 0.89 83.1
CeII(202) 4449.33 0.81 0.74 82.4
FeII(222) 4449.66 0.88 0.85 82.0:
TiII(19) 4450.48 0.34 −1.4 0.47 84.7
FeII 4451.55 0.73 82.9
MnI(22) 4451.59 0.71 −2.9:
NdII(6) 4451.98 0.93:
SmII(26) 4452.73 0.91 0.91 81.0:
TiI(113) 4453.32 0.87
VII(199) 4453.35
FeII(350) 4454.39
SmII(49) 4454.63
CaI(4) 4454.78 0.41 −1.5 0.52 84.4
FeII 4455.26 0.89
LaII(53) 4455.79 0.87
CaI(4) 4455.89 0.63 −3.2
NdII(50) 4456.39 0.90 82.9
CaI(4) 4456.62 0.78 0.91 83.8:
ZrII(79) 4457.42 0.62 82.4
TiI(113) 4457.44 0.75
FeI(992) 4458.08
MnI(28) 4458.25 0.78
SmII(7) 4458.52 0.93 81.4
FeI(68) 4459.12 0.46 −1.8 0.85 82.1
CeII(2) 4460.21 0.77 −0.7 0.67 82.0
ZrII(67) 4461.22 0.52 82.9:
FeI(2) 4461.65 0.43
FeI(471) 4462.00
NdII(54) 4462.41 0.85
NdII(50) 4462.98 0.88 0.82 82.1
CeII(20) 4463.41 0.83 81.2
TiII(40) 4464.45 0.39 0.52 83.4:
MnI(22) 4464.68
HfII(72) 4466.41
CI 4466.48 0.76 84.3
Klochkova et al.: Spectroscopy of HD56126 27
αPer HD56126
Element λ Å r Vr r Vr
FeI(350) 4466.55 0.52 −2.1
SmII(53) 4467.34 0.88 1.2 0.82
TiII(31) 4468.49 0.29 −1.8 0.41 86.9
TiII(18) 4469.16 0.73 82.7
FeI(830) 4469.37 0.46
TiII(40) 4470.85 0.50 −1.7 0.62 84.0:
CeII(8) 4471.24 0.68 81.6:
FeI(595) 4472.72
FeII(37) 4472.92 0.52 0.64 82.9
FeII(17) 4474.19 0.96 0.98 81.0:
VII(199) 4475.70 0.98:
FeI(350) 4476.02 0.52 −1.1 0.88 84.0
YI(14) 4477.46 0.91 −1.8
CI 4477.47 0.85 82.5
CI 4478.59
SmII 4478.66 0.85 −1.2 0.81: 81.5
GdII(15) 4478.80
CI 4478.83 0.85:
CeII(203) 4479.36 0.77 81.7:
CeII(124) 4479.43
FeI(828) 4479.61 0.80:
FeI(515) 4480.14 0.82
MgII(4) 4481.22 0.28 −2.2 0.26 82.5
ZrII(131) 4482.04
FeI(2) 4482.17 0.48 0.86:
FeI(68) 4482.26
TiI(113) 4482.74 0.85 −2.0:
GdII(62) 4483.33 0.97 0.93 84.4
CeII(3) 4483.90 0.79 81.7
FeI(828) 4484.23 0.73
4484.80 0.92
ZrII(79) 4485.44 0.83 84.4
FeI(830) 4485.68 0.81 −3.6
HfII(23) 4486.14 0.97 83.4
CeII(57) 4486.91 0.85 −1.0 0.74 81.7
TiII(115) 4488.33 0.52 −3.9 0.60 82.7
FeII(37) 4489.17 0.42 −2.7 0.53 83.2
FeI(2) 4489.74 0.73:
FeI(973) 4490.77 0.83 −3.0: 0.97
FeII(37) 4491.40 0.42 −1.5 0.51 83.2
TiII(18) 4493.52 0.67 −1.5 0.81 81.7
ZrII(130) 4494.41 0.54 84.0:
FeI(68) 4494.56 0.47 −3.6
CeII(154) 4495.39
ZrII(79) 4495.44 0.82 0.76 82.7
TiII(40) 4495.46
FeII(147) 4495.52
TiI(146) 4496.15 0.88
TiI(8) 4496.25 0.90 82.5:
28 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CrI(10) 4496.86
ZrII(40) 4496.96 0.56 0.45 84.3
CeII(19) 4497.84 0.90 0.89 82.9
MnI(22) 4498.90 0.88
CrI(150) 4500.28
TiII(18) 4500.32 0.77 0.88
TiII(31) 4501.27 0.30 −2.1 0.44 86.0
MnI(22) 4502.22 0.90: −1.6:
CrII(16) 4504.52
FeI(555) 4504.83 0.93
NdII(7) 4506.58 0.93
TiII(30) 4506.74 0.83 −2.5
GdII(13) 4506.93
CrII(16) 4507.19
FeII(38) 4508.28 0.37 −2.3 0.46 83.8
CrII(191) 4511.82 0.90 −0.8
TiI(42) 4512.74 0.90 −1.7 0.95
FeII(37) 4515.35 0.37 −2.3 0.46 83.6
LaII 4516.38 0.92:
CrII(191) 4516.56 0.94
FeI(472) 4517.53 0.88 −1.7
TiI(42) 4518.03
TiII(18) 4518.30 0.60 −1.3: 0.77
VII(212) 4518.38
SmII(49) 4519.63 0.93: 0.87 80.5
FeII(37) 4520.22 0.38 −2.5 0.46 83.3
GdII(44) 4521.30 0.97:
FeII(38) 4522.63 0.30 −2.8 0.41 84.1:
TiI(42) 4522.80
CeII(2) 4523.08
BaII(3) 4524.94 0.72 81.5
LaII(50) 4526.12 0.82 80.8
FeI(969) 4526.45 0.73 −1.1
CeII(108) 4527.35 0.79: −2.0: 0.72 82.3
VII(56) 4528.50 0.61
FeI(68) 4528.61 0.36 −2.8
TiII(82) 4529.48 0.46 −0.1: 0.63 83.3
FeI(39) 4531.15 0.57 0.95 81.4
TiI(42) 4533.24 0.91 81.6:
TiII(50) 4533.96 0.23 0.34
FeII(37) 4534.16
TiI(42) 4534.78 0.78 −1.9 0.95
SmII(45) 4537.95 0.94 0.92
CrII(39) 4539.62 0.69
CeII(108) 4539.77 0.66
FeII(38) 4541.52 0.46 −2.9 0.55 82.5
TiII(60) 4544.02 0.64 −2.9 0.79 81.8
TiII(30) 4545.14 0.57 −2.4 0.74 81.3:
CrI(10) 4545.96 0.83 −2.8
Klochkova et al.: Spectroscopy of HD56126 29
αPer HD56126
Element λ Å r Vr r Vr
FeI(755) 4547.85 0.79 −1.9 0.97
FeII(38) 4549.47
TiII(82) 4549.62 0.15 0.28 90.5:
CeII(229) 4551.30 0.93: 0.86 80.0:
TiII(30) 4552.30 0.61: 0.86 82.2
BaII(1) 4554.03 0.29 −2.1 0.31 88.7
CrII(44) 4554.99 0.58 −2.2 0.64 83.0
FeII(37) 4555.89 0.33 0.45 84.0
CrII(44) 4558.65 0.38 −2.6 0.45 82.1
CeII(8) 4560.28 0.78 82.2
CeII(2) 4560.96 0.90 −1.8: 0.83 82.2
CeII(1) 4562.36 0.81 −2.0 0.69 81.9
TiII(50) 4563.76 0.32 −2.2 0.41 84.7
ZrII(116) 4565.41 0.82 84.2:
CrII(39) 4565.77 0.60: 0.71 83.0
TiII(60) 4568.32 0.73 −1.1 0.88 82.6
HfII(86) 4570.70 0.89 80.3:
MgI(1) 4571.10 0.82 −1.1
TiII(82) 4571.98 0.27 −1.5 0.36 91.3:
ZrII(139) 4574.48 0.69 84.6:
LaII(23) 4574.87 0.83: 0.78 80.6:
FeII(38) 4576.34 0.47 −2.1 0.54 83.0
FeII(26) 4580.06 0.59 0.70 82.7
CeII(7) 4582.50 0.75:
FeII(37) 4582.83 0.51 −2.2 0.58 82.6
TiII(39) 4583.41
FeII(38) 4583.84 0.28 −2.3 0.41 87.5
CrII(44) 4588.20 0.45 −2.0 0.49 83.1
CrII(44) 4589.94 0.43 −1.8 0.53 83.4
CrII(44) 4592.05 0.58 −1.7: 0.65 82.8
CeII(6) 4593.92 0.74: 0.72 81.1
FeI(820) 4596.06 0.87 80.1:
NdII(51) 4597.01 0.93 82.9
VII(56) 4600.19 0.67 0.90 82.8
FeII(43) 4601.36 0.84: −2.8 0.91 83.6
ZrII(138) 4601.97 0.86: −0.4: 0.89 82.6
FeI(39) 4602.94 0.63 −2.2 0.94 81.8
CeII(6) 4606.40 0.87: 0.83 82.1
TiII(39) 4609.27 0.85 −2.8 0.94 82.5
FeI(826) 4611.28 0.73 −2.4
ZrII(67) 4613.95 0.87 −1.2: 0.69 82.6
CrII(44) 4616.62 0.61 −2.0 0.68 83.3
CrII(44) 4618.82 0.49 −2.2 0.55 82.3
LaII(76) 4619.87 0.85 82.3
FeII(38) 4620.51 0.55 −1.7 0.63 83.4
CeII(27) 4624.90 0.77 83.7:
FeI(554) 4625.05 0.76
CeII(1) 4628.16 0.83 −1.9 0.67 82.6
ZrII(139) 4629.07
30 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(37) 4629.33 0.38 −2.7 0.44 82.7:
CrII(34) 4634.07 0.54 −2.1 0.59 83.0
FeII(186) 4635.31 0.79 −1.6 0.79 82.9
TiII(38) 4636.33 0.81 −2.4 0.91 82.9
FeI(822) 4638.02 0.80: 0.95 82.1
SmII(36) 4642.24 0.96 −2.7 0.93 82.5
LaII(8) 4645.28 0.95: 0.93 80.9:
CrI(21) 4646.17 0.71 −1.4 0.95
FeI(409) 4647.44 0.72 −2.6 0.91 80.8:
FeII(25) 4648.93 0.91 82.4:
CrI(21) 4651.29 0.86 −1.7
CrI(21) 4652.16 0.78 −1.7
CeII(154) 4654.29 0.77 83.4:
LaII(75) 4655.49 0.82 82.0
FeII(43) 4656.98 0.43 0.64
TiII(59) 4657.20
ZrII(129) 4661.78 0.74 82.3:
LaII(8) 4662.51 0.80 82.3:
FeII(44) 4663.71 0.69 −1.6 0.77 83.4
FeII(37) 4666.75 0.51 −2.0 0.61 83.1
LaII(76) 4668.91 0.91 82.1
FeII(25) 4670.19
ScII(24) 4670.40 0.43 0.60 82.1:
LaII(80) 4671.82 0.92 82.7:
CeII(18) 4680.13 0.92 81.6
YII(12) 4682.34 0.73 0.61 81.4
CeII(228) 4684.61 0.89 81.1:
ZrII(129) 4685.19 0.86 0.73 82.7
LaII(23) 4691.17 0.95 82.4:
FeI(409) 4691.42 0.75 −1.2:
LaII(75) 4692.50 0.91 81.4
TiII(59) 4698.67 0.93 81.9
MgI(11) 4702.99 0.52 −2.2
ZrII(138) 4703.03 0.63 81.9
NdII(3) 4706.55 0.92 −1.1: 0.89 82.2
TiII(49) 4708.66 0.59 0.76 82.5
C2 (1;0)R1(16) 4712.96 0.92:
C2 (1;0)R2(15) 4713.12 0.92: 77.2:
C2 (1;0)R1(15) 4714.38 0.91 77.6
C2 (1;0)R2(14) 4714.54 0.91: 78.0:
C2 (1;0)R3(13) 4714.72 0.93: 77.7
NdII(49) 4715.60 0.91:
C2 (1;0)R3(12) 4716.15 0.96 78.4:
LaII(52) 4716.44 0.92 82.2:
C2 (1;0)R1(13) 4717.08 0.93 77.4
C2 (1;0)R2(12) 4717.29 0.94 78.1
C2 (1;0)R3(11) 4717.48 78.0
C2 (1;0)R1(12) 4718.38 0.92 78.2
C2 (1;0)R2(11) 4718.60 0.93 77.4
Klochkova et al.: Spectroscopy of HD56126 31
αPer HD56126
Element λ Å r Vr r Vr
C2 (1;0)R3(10) 4718.84 0.95 77.8
C2 (1;0)R1(11) 4719.61 0.87: 78.3:
C2 (1;0)R1(10) 4720.81 0.93 77.7
C2 (1;0)R2(09) 4721.09 0.94 78.7
C2 (1;0)R3(08) 4721.36 0.95 77.4
C2 (1;0)R1(09) 4721.94 0.95 78.3
C2 (1;0)R2(08) 4722.27 0.91 78.8:
C2 (1;0)R3(07) 4722.53 0.94 77.8
C2 (1;0)R1(08) 4723.04 0.93 78.0
C2 (1;0)R2(07) 4723.44 0.90 77.2
C2 (1;0)R3(06) 4723.74 0.94 77.6
C2 (1;0)R1(07) 4724.08 0.93 77.7
C2 (1;0)R3(05) 4724.83 0.92 77.9
C2 (1;0)R1(06) 4725.07 0.88: 78.3:
C2 (1;0)R2(05) 4725.57 0.91 79.6
C2 (1;0)R1(05) 4725.99 0.86: 78.5:
C2 (1;0)R2(04) 4726.60 0.89 77.5
C2 (1;0)R1(02) 4728.47 0.77 77.9:
C2 (1;0)P1(34) 4730.77 0.90 78.0
FeII(43) 4731.47 0.51 −3.1 0.59 81.3
C2 (1;0)P2(03) 4732.81 0.89 78.3:
C2 (1;0)P2(04) 4733.40 0.84 78.6:
C2 (1;0)P2(05) 4733.93 0.83
FeI(554) 4736.77 0.63 −0.3 0.73 84.0:
LaII(8) 4740.27 0.84 0.78 81.9
LaII(75) 4743.08 0.92 0.85 82.7
PrII(3) 4744.93 0.95 82.2
CeII 4747.14 0.97 0.92 82.4
LaII(65) 4748.73 0.93 −0.9: 0.83 81.5
FeI(634) 4757.58 0.91 −0.8
CeII 4757.84 0.94 81.4
MnI(21) 4761.53 0.85 −2.5:
ZrII(107) 4761.67 0.63 82.1
CI(6) 4762.31
CI(6) 4762.54 0.63:
TiII 4763.90 0.58 −2.4 0.75 81.8:
TiII(48) 4764.53 0.64 −0.5: 0.83
MnI(21) 4766.43 0.76
CI(6) 4766.68 0.83 82.2
CI(6) 4770.03 0.88 −3.6 0.76 82.3
CI(6) 4771.75 0.54 81.9
CeII(17) 4773.94 0.93 −3.9 0.90 80.6
CI(6) 4775.91 0.84 −2.2 0.71 82.0
TiII(92) 4779.99 0.52 −2.7 0.60 82.3
MnI(16) 4783.42 0.70 −2.0 0.96 82.4
YII(22) 4786.58 0.59 82.5
TiII(17) 4798.53 0.64 −3.0 0.81 82.8
LaII(37) 4804.04 0.96 −1.1: 0.91 82.0
TiII(92) 4805.09 0.45 −1.5 0.53 83.2
32 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
LaII(37) 4809.00 0.89 82.4
NdII(3) 4811.35 0.93 0.91 82.0
CrII(30) 4812.35 0.73 −2.6 0.81 82.5
CI(5) 4812.92 0.95 83.0:
ZrII(66) 4816.47 0.97 0.87 82.5
CI(5) 4817.37 0.95: −1.5: 0.90 81.7
NdII(47) 4820.34 0.91 81.9
YII(22) 4823.31 0.53 82.6
MnI(16) 4823.51
CrII(30) 4824.14 0.47 −2.9 0.54 82.0
NdII(3) 4825.48 0.82: 0.86 82.0
CI(5) 4826.80 0.95 −2.1 0.91 82.7:
NiI(111) 4831.18 0.83 −1.9 0.95 81.4
FeII(30) 4833.19 0.85 −1.8 0.94 82.9
CrII(30) 4836.23 0.67 0.78 82.2
LaII(37) 4840.02 0.92 81.4:
ZrII(138) 4841.98 0.92 82.6
SmII(26) 4844.21 0.95 82.2:
CeII(17) 4846.57 0.96 81.1:
CrII(30) 4848.25 0.52 −2.0 0.59 82.9
YII(22) 4854.87 −2.1: 83.0
FeI(318) 4859.74 0.80
Hβ 4861.33 0.11 −1.7 0.13 98.2
CrII(30) 4864.32 −1.7: 83.3:
TiII(29) 4865.62 −2.6: 81.7:
FeI(318) 4871.32 0.50: −2.6: 0.75 81.2
FeI(318) 4872.14 0.55: −3.1: 0.83 81.9
TiII(114) 4874.01 0.65: −2.2: 0.70 82.5
CrII(30) 4876.40 0.61
CrII(30) 4876.48 0.51
CaI(35) 4878.14
FeI(318) 4878.22 0.56 0.90 81.0:
YII(12) 4881.44 0.92 81.1
CeII 4882.46 0.85 81.3
YII(22) 4883.69 0.51 −2.8 0.39 84.8
CrII(30) 4884.60 0.75 −0.9: 0.84 83.2
FeI(318) 4890.76 0.53 −2.2 0.78 80.8
FeI(318) 4891.49 0.49 −2.2 0.74 82.7
FeII(36) 4893.82 0.79 −1.6 0.86
ZrII(107) 4894.43 0.89 82.0
BaII(3) 4899.94
YII(22) 4900.12 0.46 0.38
FeI(318) 4903.31 0.66 −1.9 0.87 81.0
ZrII(145) 4908.67 0.97 80.8:
TiII(114) 4911.19 0.59 −1.1: 0.63 83.7:
ZrII(3) 4911.66 0.82 81.8:
FeI(318) 4918.99 0.52 −2.8 0.81 82.9
FeI(318) 4920.50 0.42 −1.1 0.64 85.0:
LaII(7) 4920.98 0.63 81.9:
Klochkova et al.: Spectroscopy of HD56126 33
αPer HD56126
Element λ Å r Vr r Vr
LaII(7) 4921.80 0.79 0.67 82.3
FeII(42) 4923.92 0.29 −1.8 0.55: 78.0:
0.39 93.9
CI(13) 4932.05 0.81 −3.4 0.64 81.3
BaII(1) 4934.08 0.32 −2.9 0.35 85.5
FeI(687) 4946.39 0.79 −1.9
LaII(36) 4946.47 0.92 80.8
FeII(168) 4953.98 0.93 −1.6: 0.94 83.3:
FeI(318) 4957.30
FeI(318) 4957.60 0.31 0.65 81.8:
NdII(1) 4959.13 0.92 −1.1 0.92 81.4
NdII(22) 4961.40 0.96 0.93 82.4
SrI(4) 4962.29 0.78 83.3
FeI(687) 4966.09 0.71 −2.3 0.94 83.2
OI(14) 4967.88 0.95
FeI(1067) 4967.90 0.83 −1.9
OI(14) 4968.79 0.96: 82.1:
LaII(37) 4970.39 0.85 81.7
CeII 4971.48 0.88 82.2
FeI(984) 4973.11 0.82 −2.0
TiII(71) 4981.35 0.94 80.8
TiII(38) 4981.74 0.72 −1.2
YII(20) 4982.13 0.69 82.4
LaII(22) 4986.82 0.93 0.86 82.8
NdII 4989.96 0.95 −2.0: 0.90 81.4:
FeII(36) 4993.35 0.65 −1.1: 0.75 82.9
FeI(16) 4994.14 0.73 −2.4: 0.93 82.0:
LaII(37) 4999.46 0.78 82.6
TiI(38) 4999.49 0.75 −2.1
TiII(71) 5005.17 0.78: 0.92 82.2
FeI(984) 5005.72
FeI(318) 5006.12 0.54: 0.88 82.1
TiII(113) 5010.21 0.77 −2.9 0.87 82.8
BaII(10) 5013.00 0.92 80.1
TiII(71) 5013.69 0.64 −2.7 0.81 82.0
CI 5017.09 0.91: 82.8:
FeII(42) 5018.44 0.28 −2.2 0.55: 77.0:
0.34 96.4
CaII(15) 5019.98 0.72 −3.0: 0.82 82.8:
TiI(38) 5020.03
FeI(965) 5022.24 0.74:
CeII(16) 5022.87 0.90 81.3:
CI 5023.85 0.94: 0.87 82.7
TiI(38) 5024.85 0.90:
CI 5024.92 0.94 81.8
ScII(23) 5031.02 0.53 −2.6 0.63 82.5
CI(4) 5039.07 0.76 82.3
CI 5040.13 0.90 82.4:
SiII(5) 5041.03 0.77 80.5:
34 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CeII(16) 5044.01 0.89 81.9
FeI(318) 5044.22 0.86
FeI(114) 5049.82 0.64 −2.1 0.93 81.8
FeI(16) 5051.64 0.62 −0.9:
CI(12) 5052.17 0.74: 0.54 81.7
CI 5053.52 0.95 83.6
SiII(5) 5055.98 0.83 −1.1: 0.75 83.3:
SiII(5) 5056.31
FeI(1094) 5065.02 0.66 −1.7: 0.93: 81.3:
FeI(383) 5068.77 0.68 0.95:
TiII(113) 5069.09 0.93 83.0:
FeI(1089) 5272.08
TiII(113) 5072.29 0.63 0.79 82.4
FeI(1094) 5074.75 0.71 −1.7 0.94 81.6
CeII(15) 5079.68 0.80 81.6
FeI(16) 5079.75 0.74
NiI(143) 5080.54 0.74 −2.1 0.94 81.4
FeI(16) 5083.35 0.72 −2.1 0.97
YII(20) 5087.42 0.62 −2.4 0.51 84.3
FeI(1090) 5090.78 0.82 −2.0 0.94 82.9:
NdII(48) 5092.80 0.94 −1.2 0.92 82.0
C2 (0;0)R1(33) 5095.15 0.98 77.5:
C2 (0;0)R1(32) 5098.13 0.98 77.3:
C2 (0;0)R3(30) 5098.30 0.98: 78.3:
FeII 5100.74 0.70 0.81 82.3:
C2 (0;0)R1(29) 5106.36 0.95 77.5
FeI(16) 5107.45
LaII(164) 5107.54 0.57 0.90 83.0:
FeI(36) 5107.65
FeI(1) 5110.42 0.68 −2.1
ZrII(95) 5112.27 0.89 −1.9 0.62 82.7
LaII(36) 5114.55 0.91: 0.82 81.6:
C2 (0;0)R1(25) 5116.66 0.93 77.7
C2 (0;0)R3(23) 5116.89 0.95 77.6
CeII 5117.18 0.97 0.90 81.4:
YII(20) 5119.12 0.88 −2.1 0.69 80.9:
FeII(35) 5120.34 0.80 −1.0: 0.91 82.7
C2 (0;0)R1(23) 5121.44 0.93 77.3
C2 (0;0)R3(21) 5121.69 0.94 77.7
LaII(36) 5123.00
YII(21) 5123.22 0.70 0.53
C2 (0;0)R1(22) 5123.79 77.3:
C2 (0;0)R3(20) 5124.04 77.3:
C2 (0;0)R1(21) 5125.98 0.91 77.5
C2 (0;0)R3(19) 5126.26 0.93 77.5
C2 (0;0)R3(20) 5128.19 0.90 77.3
C2 (0;0)R3(18) 5128.49 0.93 77.9
TiII(86) 5129.16 0.50
C2 (0;0)R1(19) 5130.27 0.89 77.9
Klochkova et al.: Spectroscopy of HD56126 35
αPer HD56126
Element λ Å r Vr r Vr
C2 (0;0)R1(18) 5132.36 0.86 77.7
FeII(35) 5132.66 0.77 −2.6: 82.2:
FeI(1092) 5133.69 0.64 −2.0 0.88 82.9
C2 (0;0)R1(17) 5134.32 0.89 77.1
C2 (0;0)R3(15) 5134.67 0.91 77.4
C2 (0;0)R1(16) 5136.27 0.89 77.6
C2 (0;0)R2(15) 5136.44 0.94 77.7
C2 (0;0)R3(14) 5136.66 0.89 77.7
C2 (0;0)R1(15) 5138.11 0.89 77.3
C2 (0;0)R2(14) 5138.32 0.93 77.1
C2 (0;0)R3(13) 5138.51 0.90 77.6
C2 (0;0)R1(14) 5139.93 0.88 77.5
C2 (0;0)R2(13) 5140.14 0.92 77.8
C2 (0;0)R3(12) 5140.38 0.89 77.6
C2 (0;0)R1(13) 5141.65 0.87 77.2
C2 (0;0)R2(12) 5141.90 0.89 77.1
C2 (0;0)R3(11) 5142.11 0.89 77.7
C2 (0;0)R1(12) 5143.33 0.86 77.6
C2 (0;0)R2(11) 5143.60 0.89 77.4
C2 (0;0)R3(10) 5143.86 0.88 77.7
C2 (0;0)R1(11) 5144.92 0.85 77.5
C2 (0;0)R2(10) 5145.23 0.87 77.6
C2 (0;0)R3(09) 5145.48 0.87 77.5
FeII(35) 5146.11 0.73: 0.86 83.1:
C2 (0;0)R1(10) 5146.46 0.83 77.5
C2 (0;0)R2(09) 5146.81 0.88 77.6
C2 (0;0)R3(08) 5146.12 0.88 77.2
C2 (0;0)R1(09) 5147.93 0.84 77.4
C2 (0;0)R2(08) 5148.33 0.83 77.0
C2 (0;0)R3(07) 5148.61 0.84 77.3
C2 (0;0)R1(08) 5149.33 0.84 77.8
C2 (0;0)R2(07) 5149.79 0.85 77.1
C2 (0;0)R3(06) 5150.14 0.86 77.6
FeI(16) 5150.85 0.70 −0.9:
C2 (0;0)R2(06) 5151.17 0.83 77.3
C2 (0;0)R2(05) 5152.52 0.81 77.0
C2 (0;0)R2(04) 5153.77 0.74 77.2
TiII(70) 5154.07 0.51 0.57:
C2 (0;0)R2(03) 5154.99 0.82 77.4
C2 (0;0)R1(02) 5156.11 0.77 77.2
C2 (0;0)R2(01) 5157.16 0.86 77.8
C2 (0;0)P2(04) 5161.98 0.75 76.6
FeI(1089) 5162.27 0.66 −1.6
C2 (0;0)P2(05) 5162.58 0.66 77.3
C2 (0;0)P2(07) 5163.13 0.75 77.4
C2 (0;0)P1(14) 5165.03 0.56 78.0
C2 (0;0) head 5165.24 0.72:
MgI(2) 5167.32 0.30 0.55
FeI(37) 5167.49
36 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeII(42) 5169.03 0.27 −2.7 0.56: 77.0:
0.33 97.4
FeI(36) 5171.60 0.56 −1.7 0.88 82.6
MgI(2) 5172.68 0.37 −1.4 0.51 82.7
NdII 5179.78 0.94 81.6
FeI(1166) 5180.07 0.92
MgI(2) 5183.60 0.32 −2.1 0.45 81.6
TiII(86) 5185.91 0.54 −2.1 0.69 82.0
CeII(46) 5187.46 0.93: 0.81 81.4
TiII(70) 5188.69 0.41 0.57
CaI(49) 5188.85
FeI(383) 5191.45 0.56
FeII(52) 5191.58 0.58 82.8:
FeI(383) 5192.35 0.57 0.83:
NdII(75) 5192.61 0.81:
YII(28) 5196.43 0.75 81.8
FeII(49) 5197.58 0.46 −2.4 0.59 83.3
YII(20) 5200.41 0.70 −2.8: 0.61 83.7:
FeI(66) 5202.34 0.67 0.94 81.4
YII(20) 5205.73 0.55 84.8:
CrI(7) 5206.04 0.42
TiII(103) 5211.54 0.72 −2.7 0.83 82.3
NdII(44) 5212.37 0.96 −2.0: 0.95 81.1
FeII 5216.85 0.94 82.2
PrII(35) 5220.11 0.94 82.0
TiII(70) 5226.54
FeI(383) 5226.87 0.37: −1.9: 0.60 83.6:
FeI(37) 5227.19 0.79 81.6
FeI(1091) 5228.38 0.89
NdII(46) 5228.43
FeI(553) 5229.85 0.74 −1.3 0.95 82.8
FeII(49) 5234.63 0.45 −2.3 0.57 83.8
CrII(43) 5237.32 0.60 −1.9 0.68 82.7:
ScII(26) 5239.82 0.66 −1.8 0.76 82.4
CrII(23) 5246.77 0.80: 0.91 83.1
FeII(49) 5254.93 0.62 −1.3 0.74 82.0
NdII(43) 5255.51 0.91 81.6:
FeII(41) 5256.93 0.80 −1.7 0.89 83.2
FeII 5260.26 0.92: 0.90 81.9:
TiII(70) 5262.11 0.33: 0.81
CaI(22) 5262.24
FeII(48) 5264.81 0.60 −2.0 0.56 87.4:
FeI(383) 5266.55 0.58 −1.8 0.88 82.3
TiII(103) 5268.62 0.73: 0.86: 83.0:
FeI(15) 5269.54 0.42 −2.0 0.70 82.1
FeII(185) 5272.39 0.86 0.91 83.3:
CeII(15) 5274.23 0.92: 0.80 81.9
CrII(43) 5274.98 0.60: 0.71 82.9
FeII(49) 5276.00 0.42 −3.0 0.56 84.8
Klochkova et al.: Spectroscopy of HD56126 37
αPer HD56126
Element λ Å r Vr r Vr
FeI(383) 5281.79 0.70 −2.1 0.95 81.3
FeII(41) 5284.10 0.53: 0.68 83.1
YII(20) 5289.82 0.95 −2.3 0.87 81.2
LaII(6) 5290.83 0.96 −1.8: 0.93 81.1:
NdII(75) 5293.16 0.90 −1.4 0.84 82.2
HfII(49) 5298.06 0.94 82.7:
CrII(24) 5305.86 0.76 −1.5 0.84 82.9
CrII(43) 5308.43 0.79 −2.1 0.85 82.7
CrII(43) 5310.69 0.84: 0.92 82.7
CrII(43) 5313.58 0.70 −1.6 0.78 82.9
FeII(49,48) 5316.66 0.34 −1.3: 0.48 88.0:
ScII(22) 5318.35 0.85 −1.4 0.95 83.2:
NdII(75) 5319.82 0.92: 0.85 81.5
YII(20) 5320.78 0.94 82.0
FeI(553) 5324.18 0.58 −2.4 0.81 82.6
FeII(49) 5325.56 0.65 −2.5 0.73 82.6
FeI(15) 5328.04 0.37: 0.74 82.4
OI(12) 5328.69 0.93 83.3
CrII(43) 5334.87 0.72 −2.1 0.80 82.9
TiII(69) 5336.79 0.55 −2.2 0.71 81.9
FeII(48) 5337.73 0.71
CrII(43) 5337.79 0.81
FeI(37) 5341.02 0.61 −1.6 0.94 81.5
ZrII(115) 5350.09
ZrII(115) 5350.35 0.87: 0.64
FeI(1062) 5353.38 0.79:
CeII(15) 5353.53 0.79 81.3
FeII(48) 5362.86 0.51 −1.9 0.63 83.5
FeI(1146) 5364.87 0.72 0.93 82.6
FeI(1146) 5367.47 0.70 −2.1 0.90 82.4
CrII(29) 5369.35 0.96 82.2
FeI(1146) 5369.96 0.65 −2.1 0.88 82.9
FeI(15) 5371.49 0.46 −2.2 0.82 81.8
NdII(79) 5371.92 0.92 81.5:
LaII(95) 5377.05 0.94 82.3
CI(11) 5380.34 0.85: −1.9: 0.68 81.9
TiII(69) 5381.03 0.63 −2.8 0.78 81.8
FeI(1146) 5383.37 0.63 −2.2 0.86 82.6
FeI(553) 5393.17 0.71
CeII(24) 5393.39 0.81
FeI(553) 5393.17 0.71
CeII(24) 5393.39 0.81
FeI(15) 5397.13 0.52 −2.1 0.89 81.6
YII(35) 5402.78 0.85 −2.1 0.59 81.9
FeI(1145) 5404.14 0.59 0.87 82.2
FeI(15) 5405.77 0.50 −1.9 0.89 81.4
CeII(23) 5409.22 0.90 81.4
FeI(1165) 5410.91 0.70 −1.5 0.91 82.8:
FeII(48) 5414.07 0.74 −2.2 0.84 82.5
38 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
FeI(1165) 5415.20 0.64 −2.1 0.87 82.2
ZrII(94) 5418.01 0.96 80.6:
TiII(69) 5418.77 0.67 −2.0 0.82 82.4
CrII(23) 5420.93 0.79 0.90 83.0
FeI(1146) 5424.07 0.60 −1.8 0.84 82.7
FeII(49) 5425.25 0.67 −2.0 0.75 82.7
FeII 5427.80 0.94 −1.4 0.96 81.4:
FeI(15) 5434.52 0.56 −1.8 0.91 81.8
OI(11) 5435.18 0.97
OI(11) 5435.78 0.97 82.4
OI(11) 5436.86 0.95:
NdII(76) 5442.29 0.97 81.0:
FeI(1163) 5445.04 0.74 −1.9 0.95 82.1
FeI(15) 5446.92 0.48 0.89 81.0:
NdII 5451.12 0.97: 0.96 81.5:
CeII(24) 5468.38 0.96 0.92 89.5
CeII(24) 5472.30 0.90 89.0
YII(27) 5473.39 0.87: 0.66 90.0
ZrII(115) 5477.79 0.89 89.7
CrII(50) 5478.37 0.76 −1.7 0.83 89.3
YII(27) 5480.74 0.83: 0.66 90.0
NdII(79) 5485.71 0.97 −1.3: 0.92 90.3:
TiII(68) 5490.68 0.82 −1.2: 0.93 90.4:
YII(27) 5497.41 0.62 0.51 90.5
FeI(15) 5497.52
FeI(15) 5501.47 0.72
CrII(50) 5502.08 0.80 −2.7: 0.87 90.2
FeI(15) 5506.79 0.67 −0.9: 0.96 90.3:
CrII(50) 5508.62 0.82 −2.9: 0.89 89.0:
YII(19) 5509.90 0.80 −1.4 0.65 90.9:
CrII(23) 5510.71 0.83 −1.9 0.90 90.7:
YII(27) 5521.56 0.92 −2.1 0.69 90.3
ScII(31) 5526.81 0.55 −2.1 0.60 90.4
MgI(9) 5528.41 0.58 −2.4 0.76 88.7
FeII(55) 5534.84 0.57 −1.8 0.63 90.0
FeI(926) 5543.19 0.90 −2.1 0.97 89.8
FeI(1062) 5543.94 0.89 −2.4 0.96 89.0:
YII(27) 5544.61 0.89: 0.65 91.0
CI 5545.07 0.92: 0.82: 88.0:
YII(27) 5546.01 0.90: 0.66 90.1
CI 5547.27 0.95 89.5
CI 5551.03 0.95 87.8:
CI 5551.59 0.92 88.5
FeI(1183) 5554.90 0.84 −2.7 0.95 90.8:
FeI(686) 5569.62 0.71 −1.8 0.93 89.0
FeI(686) 5572.84 0.63 0.89 90.0
FeI(686) 5586.76 0.61 −1.4 0.84 89.2
CaI(21) 5588.76 0.65 −2.0 0.90 88.8
CaI(21) 5594.47 0.66: 0.89 88.4
Klochkova et al.: Spectroscopy of HD56126 39
αPer HD56126
Element λ Å r Vr r Vr
CaI(21) 5601.28 0.80 −2.9 0.97 88.7
CeII(26) 5610.26 0.97:
YII(19) 5610.36 0.93
FeI(686) 5615.64 0.57 0.82 89.5
NdII(86) 5620.65 0.93 88.5
FeI(686) 5624.54 0.75 −2.4 0.93 90.2:
FeII(57) 5627.49 0.87 −1.6 0.93 90.3
CI 5629.93 0.98: −1.5: 0.96 88.5
FeI(1314) 5633.95 0.89 −2.0
FeI(1087) 5638.27 0.87 −2.3
ScII(29) 5640.98 0.73 0.82 90.6
ScII(29) 5657.87 0.56: 0.72 90.3
ScII(29) 5658.34 0.83: 88.5
FeI(1087) 5662.52
YII(38) 5662.94 0.66: 0.42 90.6
ScII(29) 5667.15 0.77 −1.3 0.87 90.0
CI 5668.95 0.72 90.4
ScII(29) 5669.03 0.72 −2.9
LaII(95) 5671.54 0.96 91.2:
NaI(6) 5682.64 0.79: 0.96 88.8:
ScII(29) 5684.19 0.70: 0.83 90.5
NaI(6) 5688.21 0.72 −0.9: 0.92 91.2:
NdII(79) 5688.54 0.91 89.6:
CI 5693.11 0.98: 0.94 89.5
MgI(8) 5711.09 0.85 −1.6 0.98:
NiI(231) 5715.09 0.90 −1.6
CI 5720.78 0.98 89.5:
YII(34) 5728.89 0.94 −1.9 0.75 90.3
FeI(1087) 5731.77 0.92 −2.1 0.98
FeII(57) 5732.72 0.94 0.97 90.0
FeI(1180) 5752.04 0.93 −2.2
FeI(1107) 5763.00 0.80 −3.0: 0.96: 89.3:
LaII(70) 5769.06 0.96 −1.2: 0.86 88.9
SiI(17) 5772.15 0.91 −1.8 0.98:
FeI(1087) 5775.08 0.93 −1.7
YII(34) 5781.69 0.84 90.5
CI 5793.12 0.89 0.87 88.9
CI 5794.46 0.97 90.6:
LaII(4) 5797.59 0.87 89.9
SiI(9) 5797.86 0.90
CI 5800.59 0.95: 0.91 89.2
NdII(79) 5804.02 0.93 90.5
CI 5805.19 0.94: 0.94 90.5
LaII(4) 5805.78 0.94 −2.7: 0.86 89.9
FeI(1180) 5806.73 0.93 −2.2 0.98 90.2
LaII(4) 5808.31 0.98: 0.97 91.5:
FeI(982) 5809.22 0.95 −1.3 0.98:
VII(99) 5819.93 0.95 −1.4 0.98: 90.0:
FeII(164) 5823.15 0.96 −2.5: 0.97 89.6:
40 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
NdII(86) 5842.39 0.99: 0.96 88.3:
FeI(1178) 5852.22 0.96 −1.8
BaII(2) 5853.68 0.63 −2.1 0.53 90.8
CaI(47) 5857.45 0.72 0.94 88.9
FeI(1180) 5862.36 0.85 −1.9 0.96 88.8
LaII(62) 5863.70 0.98 0.97 89.8
LaII(35) 5880.63 0.96 90.7:
NaI(1) 5889.95 0.45: −1.2: 0.21 13.0
0.05 +2.2 0.32 24.0
0.37 31.4
0.10 75.7
0.40 89.0
NaI(1) 5895.92 0.50: −0.9: 0.38 13.2
0.06 +2.3 0.51 24.7
0.48 32.0
0.16 76.3
0.45 89.8
FeI(982) 5934.66 0.89 −2.2
SiI(16) 5948.54 0.83 −3.0 0.97:
SiII(4) 5957.56 0.93 88.0:
CeII(80) 5975.83 0.94 89.9
SiII(4) 5978.93 0.88 87.5
FeI(1175) 5983.68 0.89 −0.7 0.95: 89.0:
FeI(1260) 5984.82 0.86 −1.9 0.96: 88.0:
FeII(46) 5991.37 0.75 −1.7 0.84 90.3
CI 6001.13 0.98: 0.92 89.5
CI 6002.98 0.95 89.7:
FeI(959) 6003.02 0.88 −2.4
CI 6006.03 0.96: 0.86 89.5
CI 6010.68 0.98 −1.2 0.92 88.8
CI 6012.24 0.98: −1.5: 0.94 90.3:
CI 6013.32 0.80 87.7:
MnI(27) 6013.49 0.89:
CI 6016.45 0.93 89.2:
MnI(27) 6016.64 0.91: −2.0:
MnI(27) 6021.80 0.90 −2.0:
FeI(1178) 6024.07 0.82 −2.2 0.94 88.8
ZrII(136) 6028.64 0.97: 0.91 89.1
CeII(30) 6034.20 0.98 −1.7 0.96 90.8:
CeII(30) 6043.40 0.99 −1.5: 0.94 89.7
FeI(207) 6065.49 0.81 −1.4 0.98:
FeII(46) 6084.10 0.83 −1.5 0.90
ZrII(106) 6106.47 0.97: 0.93 90.9
FeII(46) 6113.32 0.88 −1.6 0.93 88.6
ZrII(93) 6114.78 0.98 −1.5: 0.92 92.2:
CI 6120.82 0.99: 0.97 89.8
CaI(3) 6122.22 0.69 −0.9 0.93 89.5
FeI(169) 6136.62 0.75 0.95 89.0:
FeI(207) 6137.70 0.78 −2.0 0.96 89.2:
Klochkova et al.: Spectroscopy of HD56126 41
αPer HD56126
Element λ Å r Vr r Vr
BaII(2) 6141.72 0.56 −1.4 0.37 92.3
FeII(74) 6147.74 0.74 −1.4 0.77 90.2
FeII(74) 6149.25 0.75 −1.5 0.77 90.0
SiI(29) 6155.98 0.89
OI(10) 6155.98 0.95: 0.82 87.0:
OI(10) 6156.17 0.95: 0.82 87.1
OI(10) 6158.18 0.79 88.0
FeI(1260) 6170.51 0.90 −1.5 0.97 89.7
FeII(200) 6175.14 0.95 90.2
LuII(2) 6221.88 0.98: 0.90 89.9:
FeII(74) 6238.39 0.74 −1.7 0.76 90.0
SeII(28) 6245.62 0.80: −0.5: 0.90 90.0:
FeII(74) 6247.56 0.66 −2.2 0.70 89.9:
FeII 6248.90 0.94 −1.4 0.94 89.3
FeI(169) 6252.56 0.81 −1.9 0.97 89.5
LaII(33) 6262.30 0.96 −0.6: 0.89 90.2
FeII 6317.99 0.81 −1.0: 0.86 88.8:
FeI(168) 6318.03
SiII(2) 6347.10 0.65 −2.0 0.51 89.7
FeII(40) 6369.46 0.84 −1.6 0.91 90.5
SiII(2) 6371.36 0.72 −1.8 0.57 89.5
FeII 6383.72 0.91 −1.6 0.92 89.8
FeII 6385.46 0.93 −2.0 0.94 88.4:
LaII(33) 6390.49 0.97 0.89 90.3
FeI(168) 6393.61 0.79 −2.5 0.96 90.5:
CI 6397.98 0.98: 0.94 89.2
FeII(74) 6416.92 0.75 −1.0 0.80 90.2
FeI(62) 6430.85 0.83 −1.6 0.97 90.6:
FeII(40) 6432.68 0.75 −1.4 0.81 90.0
CaI(18) 6439.08 0.69 −1.6 0.89 90.0
FeII 6442.95 0.95 −1.2 0.95 88.9
FeII(199) 6446.41 0.95 −1.2 0.95 91.1:
OI(9) 6453.60 0.97: 0.94 87.9
OI(9) 6454.45 0.98: −2.0: 0.94 88.0
FeII(74) 6456.39 0.60 −0.2: 0.66 91.0:
TiII(91) 6491.57 0.78: 0.91 90.7:
BaII(2) 6496.91 0.55 0.52
FeII(40) 6516.08 0.66 −2.0 0.77 90.2
LaII(33) 6526.99 0.91 90.7:
MgII(23) 6545.97 0.93 89.8
FeI(268) 6546.25 0.92:
Hα 6562.81 0.19 −2.1 0.32 58.0
0.40: 74.0:
0.89 82.8:
CI(22) 6587.61 0.89 −1.7 0.72 89.5
SeII(19) 6604.59 0.89 0.94 91.1:
TiII(91) 6606.95 0.95 −2.2: 0.96 89.5
CI 6611.35 0.96 90.6:
YII 6613.75 0.91 0.73 90.0
42 Klochkova et al.: Spectroscopy of HD56126
αPer HD56126
Element λ Å r Vr r Vr
CI 6654.61 0.94 89.5:
CI 6655.51 0.91 90.5
YII(26) 6795.42 0.88 90.0
CI 7087.83 0.90 89.3
CI 7100.12 0.91 89.7
SiI(23) 7415.95 0.95: 87.5:
SiI(23) 7423.50 0.92 91.0:
EuII(8) 7426.57 0.93: 85.0:
CI 7476.18 0.89: 86.0:
CI 7483.44 0.90 85.0:
LaII(1) 7483.48
FeI(1077) 7511.03 0.97: 87.0
KI(1) 7664.91 0.83 77.5
OI(1) 7771.94 0.34 93.5
OI(1) 7774.17 0.35 94.8:
OI(1) 7775.39 0.42:
CI 7860.89 0.91: 88.0:
MgII(8) 7877.05 0.89 90.5:
YII(32) 7881.90 0.89 90.5:
MgII(8) 7896.37 0.80 88.7:
H(P27) 8306.12 0.91: 91.0:
H(P25) 8323.43 0.91: 91.0:
H(P20) 8392.40 0.64 87.0:
H(P19) 8413.32 0.62 88.0:
H(P18) 8437.96 0.60 92.0:
OI(4) 8446.5: 0.26 94.0:
H(P17) 8467.25 0.58 93.0:
CaII(2) 8542.11 0.40 85.0:
H(P15) 8545.38 0.53 94.0:
NI(8) 8567.74 0.90 89.0:
NI(8) 8594.01 90.0:
H(P14) 8598.39 0.49 93.0:
NI(8) 8629.24 0.78: 88.0:
NI(1) 8703.25 0.85: 90.0:
NI(1) 8711.70 0.83 87.0:
NI(1) 8718.83 0.84 89.0:
H(P12) 8750.47 0.43 98.0:
	Introduction
	Observations and reduction of spectra
	Peculiarities of the optical spectrum of HD56126
	Radial velocities pattern
	Spectral atlas
