# The unexpected optical and ultraviolet variability of the standard star
$\alpha$ Sex (HD 87887)

Richard Monier LESIA, UMR 8109, Observatoire de Paris et Université Pierre et
Marie Curie Sorbonne Universités, place J. Janssen, Meudon, France.  Dominic
M. Bowman Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001
Leuven, Belgium  Yveline Lebreton LESIA, UMR 8109, Observatoire de Paris et
Université Pierre et Marie Curie Sorbonne Universités, place J. Janssen,
Meudon, France.  Univ Rennes, CNRS, IPR (Institut de Physique de Rennes) - UMR
6251, F-35000 Rennes, France.  Morgan Deal  Instituto de Astrofísica e
Ciências do EspaÃ§o, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762
Porto, Portugal  LESIA, UMR 8109, Observatoire de Paris et Université Pierre
et Marie Curie Sorbonne Universités, place J. Janssen, Meudon, France.

(Received July 4, 2022; Revised June 13, 2023; Accepted June 14, 2023)

###### Abstract

The analysis of the available TESS light curves of $\alpha$ Sex (HD 87887)
reveals low-frequency pulsations with a period of about 9.1 hours in this
spectroscopic A0 III standard star. The IUE observations in December 1992
reveal large flux variations both in the far UV and in the mid UV which are
accompanied by variations of the brightness in the V band recorded by the Fine
Error Sensor on board IUE. The ultraviolet variability could be due to an
eclipse by an hitherto undetected companion of smaller radius, possibly 2.5
$R_{\odot}$ but this needs confirmation by further monitoring possibly with
TESS. An abundance determination yields solar abundances for most elements.
Only carbon and strontium are underabundant and titanium, vanadium and barium
mildly overabundant. Identification is provided for most of the lines
absorbing more than 2% in the optical spectrum of $\alpha$ Sex. Stellar
evolution modeling shows that $\alpha$ Sex is near the terminal-age main
sequence, and its mass, radius and age are estimated to be $M=2.57\pm
0.32\,M_{\odot}$, $R=3.07\pm 0.90\,R_{\odot}$, $A=385\pm 77\,\mathrm{Myr}$,
respectively.

stars: chemically peculiar – stars: individual ($\alpha$ Sex, HD 87887)

††journal: AJ

##  1 Introduction

Although $\alpha$ Sex is a bright and standard A0 III giant (Gray & Garrison,
1987), it has not been extensively studied for a star of its brightness: only
91 references can be found in SIMBAD111http://simbad.u-strasbg.fr/simbad/. The
most recent abundance analysis is that of Pintado & Adelman (2004) who used
optical spectra and derived abundances for 19 elements. They found mostly
solar abundances including helium. The only species that deviated from solar
abundances are scandium, which is underabundant, sulfur and calcium marginally
underabundant, manganese marginally overabundant and barium overabundant. A
new determination of the iron abundance was made by Adelman (2014) who found a
slight underabundance.

Among intermediate-mass main-sequence stars of spectral type A and F, the most
common type of pulsator are the $\delta$ Sct stars. These stars have low-
radial order pressure modes with periods of order of hours that are excited by
a heat-engine mechanism (Breger, 2000). Approximately 50% of main-sequence A
and early-F stars are $\delta$ Sct stars based on modern high-precision space
photometry (Bowman & Kurtz, 2018; Murphy et al., 2019). The identification of
modeling of stellar pulsations, known as asteroseismology (Aerts et al.,
2010), yields important constraints on the physical processes at work within
stars such as rotation, mixing and atomic diffusion. Therefore, the
identification of high-quality pulsating stars is essential for follow-up
modelling.

In this paper, we report on work based on new high-precision light curves from
the NASA Transiting Exoplanet Survey Satellite (TESS) mission (Ricker et al.,
2015) and on a new abundance analysis. The TESS light curve reveals that
$\alpha$ Sex is a variable star with multi-periodic pulsations with periods of
the order of several hours. The IUE archival observations of $\alpha$ Sex over
3 days in December 1992 are also analysed

This article is organised as follows. Section 2 describes the TESS light
curves of $\alpha$ Sex and their analysis, section 3 the analysis of the IUE
spectra, and section 4 the abundance determinations for 19 chemical elements,
in section 5, we use the SPInS stellar parameter inference program (Lebreton &
Reese, 2020) and the BaSTI-IAC grid of stellar models (Hidalgo et al., 2018)
to derive the evolutionary status, mass, radius, and age of $\alpha$ Sex. We
discuss the nature of $\alpha$ Sex and conclude in the final section.

##  2 The TESS light curves of $\alpha$ Sex and their analysis

The TESS mission observed $\alpha$ Sex in sectors 8, 35 and 45 in its short
cadence (i.e. 2-min) mode. We retrieved both the simple aperture photometry
(SAP) and pre-data search conditioning (PDC-SAP) 2-min light curves from the
Mikulski Archive for Space Telescopes (MAST222https://archive.stsci.edu/),
which are extracted from the target pixel files using NASA’s SPOC pipeline
(see Jenkins et al. 2016 for details). Since $\alpha$ Sex is a relatively
bright star for the TESS mission, it is moderately saturated in its target
pixel files. However, the aperture mask assigned by the SPOC pipeline includes
sufficient pixels, which includes the short bleed columns, to extract a light
curve. In such cases, TESS light curves are more than adequate at detecting
and characterising pulsating stars (see e.g. Bowman et al. 2022). We checked
for possible sources of contamination, but could not verify any known and
sufficiently bright background or nearby sources. Using the Lightkurve
software (Lightkurve Collaboration, 2018) software in combination with Gaia
astrometry (Gaia Collaboration, 2020), there are a only a few very faint (Gaia
$G>14$ mag) sources located within the assigned target pixel aperture mask,
hence their flux contribution is negligible.

Given the large gaps between the sectors 8, 35 and 45 light curves, we opted
to analyse them separately for signatures of pulsations to avoid issues
arising from the complex spectral window pattern in a combined light curve.
Each TESS sector light curve maximally spans approximately 24 d with varying
duty cycles depending on the specific sector. This yields a resultant
frequency resolution following the Rayleigh criterion of approximately 0.042
d-1 for an individual sector. We converted the extracted PDC-SAP 2-min light
curves to have units of magnitudes and show them in Fig. 1. We calculated
discrete Fourier transforms (Kurtz, 1985) and show the resultant amplitude
spectra for each sector and the combined sectors 8, 35 and 45 light curve in
the middle panel of Fig. 1. A dominant frequency of 2.63 d-1, corresponding to
a period of 9.1 hr, is apparent in the amplitude spectra of all three
individual light curves. Additional multi-periodic variability is present in
the frequency range of 1.8 d-1 up to 5.3 d-1, with amplitudes ranging up 0.3
mmag.

We performed iterative pre-whitening to extract significant frequencies for
each of the three individual TESS sectors. Significant frequencies are those
that have an amplitude signal-to-noise ratio (S/N) of $\geq 5$, in which the
noise is calculated using a symmetric local window centred at the location of
the extracted frequency in the residual amplitude spectrum (Bowman &
Michielsen, 2021). In our frequency analysis of the individual TESS sectors,
two significant frequencies are extracted: the dominant frequency and a second
indistinguishable for its harmonic given the low resolving power of a single
TESS sector. Specifically in sector 45, however, several additional
frequencies are detected within the frequency regime of the dominant
frequency. This is not the signature of rotational modulation, but in fact is
evidence of multi-periodic pulsations. Moreover, for such a frequency to be
caused by rotational modulation, this implies an extremely rapid rate of
surface rotation, which we deem unlikely given the known projected surface
rotation rate from spectroscopy $v_{{\mathrm{e}}}\sin i$ = 21 km s-1(Abt et
al., 2002).

We provide the list of significant frequencies for each sector, which were
optimised using a multi-frequency non-linear least-squares fit to the light
curve (Bowman & Michielsen, 2021), in Table 1. In the bottom panel of Fig. 1,
we show the residual amplitude spectrum after the dominant frequency has been
optimised and removed from the combined sectors 8, 35 and 45 light curve. This
clearly demonstrates the multi-periodic variability of $\alpha$ Sex between
1.8 and 5.3 d-1, which is affected by the complex spectral window pattern
resulting from the combined light curves.

Table 1: Frequencies, amplitudes and phases of the significant pulsation modes in $\alpha$ Sex, and their $1\sigma$ uncertainties calculated from a non-linear least-squares fit to the light curve. Frequency | Amplitude | Phase
---|---|---
(d-1) | (mmag) | (rad)
Sector 8 |  |
$2.6313\pm 0.0001$ | $0.280\pm 0.002$ | $0.221\pm 0.007$
$5.2745\pm 0.0017$ | $0.024\pm 0.002$ | $-2.727\pm 0.083$
Sector 35 |  |
$2.6333\pm 0.0001$ | $0.271\pm 0.002$ | $1.157\pm 0.007$
$5.2753\pm 0.0013$ | $0.028\pm 0.002$ | $-0.863\pm 0.063$
Sector 45 |  |
$1.8139\pm 0.0008$ | $0.0409\pm 0.002$ | $-1.042\pm 0.034$
$1.9054\pm 0.0006$ | $0.0537\pm 0.002$ | $2.279\pm 0.026$
$2.5791\pm 0.0009$ | $0.0612\pm 0.002$ | $-2.150\pm 0.031$
$2.6329\pm 0.0004$ | $0.2800\pm 0.002$ | $2.290\pm 0.010$
$2.6826\pm 0.0042$ | $0.0316\pm 0.002$ | $-3.017\pm 0.081$
$2.7382\pm 0.0019$ | $0.0407\pm 0.002$ | $0.714\pm 0.041$
$2.9678\pm 0.0005$ | $0.0621\pm 0.002$ | $1.156\pm 0.023$
$3.0987\pm 0.0014$ | $0.0231\pm 0.002$ | $3.046\pm 0.062$
$5.2634\pm 0.0018$ | $0.0167\pm 0.002$ | $1.347\pm 0.082$
Figure 1: Top panels: TESS light curves for sectors 8, 35 and 45. Middle
panel: Amplitude spectra of each TESS sector and all three sectors combined.
Bottom panel: Residual amplitude spectrum of all three combined sectors after
the dominant frequency has been removed.

##  3 The ultraviolet variability of $\alpha$ Sex

Nine high resolution SWP and LWP spectra of $\alpha$ Sex were obtained with
the International Ultraviolet Explorer from 24 to 27 December 1992 through the
large apertures in the frame of program NA026 (PI: Richard Monier). These
spectra are calibrated into absolute fluxes, their resolving power is about
25000 and their signal-to-noise ratios is typically a 10-20. They were
retrieved from the MAST, and they are collected in Table 2.

Table 2: Log of IUE OBSERVATIONS Spectrum | Observation | Resolution | Observation | Exposition | FES
---|---|---|---|---|---
| Date |  | time | Time [s] | counts
SWP 46576 | 1992-12-24 | High | 13:47:20 | 390 | 3587
LWP 24572 | 1992-12-24 | High | 13:59:05 | 180 | 3696
SWP 46577 | 1992-12-24 | High | 16:12:40 | 1200 | 3632
LWP 24573 | 1992-12-24 | High | 16:27:19 | 390 | 3841
SWP 46584 | 1992-12-25 | High | 15:56:55 | 1200 | 3321
LWP 24589 | 1992-12-25 | High | 16:25:57 | 4200 | 3227
SWP 46598 | 1992-12-27 | High | 10:14:56 | 1800 | 5407
LWP 24605 | 1992-12-27 | Low | 11:05:42 | 420 | 5542
LWP 24606 | 1992-12-27 | High | 12:50:53 | 420 | 5443
SWP 46599 | 1992-12-27 | High | 16:46:54 | 600 | 5401

Figure 2: Left: The far UV flux variations of $\alpha$ Sex (SWP 46599, FUV max
in blue; SWP 46577 FUV min in red), Right: The mid UV flux variations (LWP
24606: midUV max in blue; LWP2 4589: midUV min in red).

These spectra have been degraded to a lower resolution of about 7 Å comparable
to the IUE low resolution in order to highlight the variations. The large
variations in the far and mean ultraviolet are shown in Figure 2. In the far
UV, four pseudo continuuum windows (regions free of strong lines) are present
at 1284, 1342, 1457 and 1756 Å. The ratio of maximum (SWP 46599) to minimum
flux (SWP 46577) is about the same in these three windows: 1.35 $\pm$ 0.03. In
the mean UV, two windows are observed at 2047 and 2650 Å, where the ratio is
about 1.38 $\pm$ 0.01, discarding the spectrum with very low flux LWP 24589.
Including this spectrum, the ratio becomes 44 at 2047 Å and 57 at 2650 Å.
Before each of these observations, the brightness of $\alpha$ Sex was
monitored with the Fine Error Sensor in a broad spectral band near 5000 Å. The
FES counts do folllow the UV flux variations: they are larger on December 27
(around 5450 counts) , minimum on December 25 (around 3270 counts) and
intermediate on December 24 (around 3690 counts) which means that the UV flux
varied in phase with the brightness of the star at 5000 Å. At ultraviolet
maximum, the lines in SWP 46599 are consistently redshifted by about 13.7 km
s-1with respect to the spectrum at FUV minimum SWP 46577.

The large diming of the flux by about 70 % at minimum in the far UV compared
to the maximum flux could be due to a partial eclipse of $\alpha$ Sex by an
hitherto undetected companion. The duration of the eclipse and the shape of
the light curve are poorly constrained with the available data, it is
therefore difficult to derive information on the radii, temperatures and
masses. We can crudely estimate the radius of the secondary star by using the
relationship between the flux decrease:

$\frac{f_{\rm min}}{f_{\rm max}}=\left(\frac{R_{B}}{R_{A}}\right)^{2}$ (1)

and the radii $R_{A}$ of $\alpha$ Sex and $R_{B}$ of the putative companion.
Assuming a radius of about 3.0 $R_{\odot}$ for $R_{A}$ (see section 3), this
yields a radius $R_{B}$ close to 2.5 $R_{\odot}$. If the system is indeed
eclipsing, it is seen edge-on ($i=\frac{\pi}{2}$). We can estimate a rotation
period of 7 days and 19 hours by using the projected equatorial velocity and
the estimated radius in section 6 where we discuss the evolutionary status of
$\alpha$ Sex. Since no eclipse is seen in the current TESS data, we can place
a lower limit on the orbital period of about 28 days, which means that the
semi-major axis of the ellipse must be large. Eggleton & Tokovinin (2008)
mentioned that $\alpha$ Sex could be a binary, presumably with a long period.
Kervella et al. (2019) also think that $\alpha$ Sex may be a binary system
considering the renormalised unit weight error from Gaia DR2. Note that the
large ultraviolet variations we observe for $\alpha$ Sex do not resemble those
of $\delta$ Scuti observed by Monier (1991) throughout its pulsation cycle.
The ultraviolet variations of $\delta$ Scuti have modest amplitudes which
increase towards shorter wavelengths as expected for a change in effective
temperature during the pulsation cycle. This is not the trend we observe for
$\alpha$ Sex for which the amplitude of the flux variations does not increase
towards shorter wavelengths (the far and mid-UV fluxes vary by a similar
amount with time).

##  4 The abundance pattern of $\alpha$ Sex

###  4.1 Observations

Four I high resolution profiles (R = 65000) of $\alpha$ Sex have been fetched
from the Polarbase archive333http://polarbase.irap.omp.eu/. These profiles
were acquired on 10 May 2018 with the spectropolarimeter NARVAL (Petit et al.,
2014) installed at the 2 meter TBL at Pic du Midi Observatory. NARVAL is a
cross-dispersed échelle spectrograph mounted on a bench and fed with a fiber
from a Cassegrain-mounted polarimeter unit with a wavelength coverage of 3690
up to 10480 Å. The individual I profiles which have a signal-to-noise ratio of
200 around 5000 Å were coadded into a mean spectrum of signal-to-noise of 350.
This final spectrum has been sliced into 200 Å wide intervals which were then
normalised to a continuum by fitting a cubic spline through narrow regions
free of absorption lines.

###  4.2 Fundamental parameters

The effective temperature ($T_{\mathrm{eff}}$) and surface gravity
($\mathrm{log}\ g$) of $\alpha$ Sex were determined using the UVBYBETA code
developed by Napiwotzki et al. (1993). This code is based on the Moon et al.
(1985) grid, which calibrates the $uvby\beta$ photometry in terms of
$T_{\mathrm{eff}}$ and $\mathrm{log}\ g$. The photometric data was taken from
Hauck et al. (1998). The derived effective temperature is $T_{\mathrm{eff}}$=
9950 $\pm$125 K and $\mathrm{log}\ g$= 3.60 $\pm$0.25 dex, respectively (see
Sec. 4.2 in Napiwotzki et al. 1993). This value is in good agreement with
previous determinations: Adelman (2014) derived $T_{\mathrm{eff}}$= 9875 K
from spectrophotometry and the fit to the $H_{\gamma}$ line; McDonald et al.
(2012) derived $T_{\mathrm{eff}}$= 9984 K by comparing the spectral energy
distribution of $\alpha$ Sex to model atmospheres; and Pintado & Adelman
(2004) derived $T_{\mathrm{eff}}$= 9950 K from calibration of uvby$\beta$
photometry.

###  4.3 Abundance determination

####  4.3.1 Model atmospheres and spectrum synthesis

The ATLAS9 code (Kurucz, 1992) was used to compute a first model atmosphere
for the effective temperature and surface gravity of $\alpha$ Sex assuming a
plane parallel geometry, a gas in hydrostatic and radiative equilibrium and
local thermodynamical equilibrium. The ATLAS9 model atmosphere contains 72
layers with a regular increase in $\log\tau_{\rm Ross}=0.125$ and was
calculated assuming a solar chemical composition (Grevesse et al., 1998). It
was converged up to $\log\tau=-5.00$ in order to attempt reproduce the cores
of the Balmer lines. This ATLAS9 version uses the new opacity distribution
function (ODF) of Castelli et al. (2003) computed for that solar chemical
composition. Once a first set of elemental abundances was derived using the
ATLAS9 model atmosphere, the atmospheric structure was recomputed for these
abundances using the Opacity sampling ATLAS12 code (Kurucz, 2005, 2013). New
slightly different abundances were then derived and a new ATLAS12 model
recomputed until the abundances of iteration (n-1) differed of those of
iteration (n) by less than $\pm$ 0.10 dex.

The abundances of nineteen chemical elements have been derived by iteratively
adjusting synthetic spectra to the normalized spectra and looking for the best
fit to carefully selected unblended lines. Specifically, synthetic spectra
were computed assuming LTE using Hubeny et al. (1992) SYNSPEC49 code which
computes lines for elements up to Z=99. The synthetic spectra were further
convolved with a rotation parabolic profile for $v_{{\mathrm{e}}}\sin i$ = 21
km s-1(Abt et al., 2002) and the appropriate FWHM of the instrumental profile
of NARVAL. The projected equatorial velocity has been checked by modeling the
Fe II lines in the range 4500-4550 Å, they all yield a $v_{{\mathrm{e}}}\sin
i$ of about 20.0 $\pm$ 1.0 km s-1which agrees well with the value provided by
Royer et al. (2002). In order to derive the microturbulenct velocity of
$\alpha$ Sex, we simultaneously derived the iron abundance [Fe/H] for 50
unblended Fe II lines and a set of microturbulent velocities ranging from 0.0
to 2.0 km s-1. The adopted microturbulent velocity, $\xi_{t}=1.5$ km s-1,
minimizes the standard deviations, i.e. for that value all Fe II lines yield a
similar iron abundance.

We used only unblended lines to derive the abundances. A grid of synthetic
spectra was computed with SYNSPEC49 (Hubeny et al., 1992) to model each
selected unblended line of the nineteen elements for $\alpha$ Sex. For each
modeled transition, the adopted abundance is that which provided the best fit
calculated with SYNSPEC49 to the observed normalized profile. Computations
were iterated varying the unknown abundance until minimization of the
$\chi^{2}$ between the observed and synthetic spectrum was achieved over the
spectral range limited to $\pm$ 1.5 Å from the line center. The selected lines
are well separated from their neighbours allowing to place the continuum
properly on both wings of the line. For a given element, the final abundance
is a weighted mean of the abundances derived for each transition (the weights
are derived from the NIST grade assigned to that particular transition).

##  5 Abundance determinations and line identifications for $\alpha$ Sex

The determined abundances for $\alpha$ Sex, expressed relative to hydrogen as
$\log(n_{X})-12.0$ (adopting $\log(n_{H})=12.0$) and their errors (standard
deviations) are collected in Table 3. Solar abundances are taken from Grevesse
et al. (2007). We find that the abundances of $\alpha$ Sex are close to the
solar composition.

Helium, nitrogen, oxygen, magnesium, aluminium, silicon, phosphorus, sulfur,
calcium, scandium, chromium, manganese, iron and nickel have solar abundances.
Only carbon and strontium are underabundant. Titanium, vanadium and baryum are
mildly overabundant. The final synthetic spectrum allows to identify most of
the lines which absorb more than 2% of the local continuum. It is compared to
the observed spectrum in the range 4500 to 4550 Å in Fig. 3. The
identifications of these lines are collected in Table LABEL:tab:ident where
$E_{\rm low}$ is the energy of the lower excitation level involved in the
transition.

Table 3: Elemental abundances and their errors for $\alpha$ Sex Element | Solar abundance | Absolute abundance | Error
---|---|---|---
He | -1.07 | -1.07 | 0.32
C | -3.61 | -3.37 | 0.09
N | -4.22 | -4.39 | 0.20
O | -3.34 | -3.31 | 0.19
Mg | -4.47 | -4.50 | 0.08
Al | -5.63 | -5.37 | 0.20
Si | -4.49 | -4.49 | 0.18
P | -6.64 | -6.64 | 0.16
S | -4.86 | -4.86 | 0.11
Ca | -5.69 | -5.71 | 0.05
Sc | -8.83 | -9.10 | 0.28
Ti | -7.10 | -6.80 | 0.13
V | -8.00 | -7.60 | 0.08
Cr | -6.36 | -6.36 | 0.05
Mn | -6.61 | -6.57 | 0.11
Fe | -4.55 | -4.69 | 0.10
Ni | -5.97 | -5.99 | 0.13
Sr | -9.08 | -9.23 | 0.09
Ba | -9.83 | -9.34 | 0.19
Figure 3: Comparison of the observed mean spectrum of HD 87887 (in black) and
the synthetic spectrum (in red) in the range 4500-4550 Å

##  6 The evolutionary status of $\alpha$ Sex

###  6.1 Estimations of mass, radius, and evolutionary stage

To estimate the mass, radius, and age of the star, we used the SPInS stellar
model optimization tool (Lebreton & Reese, 2020). SPInS uses a Bayesian
approach to find the probability distribution function of stellar parameters
from a set of constraints. At the heart of the code is a Markov Chain Monte
Carlo sampler coupled with interpolation within a pre-computed stellar model
grid. Here, we used the BaSTI-IAC grid of stellar models (Hidalgo et al.,
2018). This grid is for a solar-scaled heavy element distribution with the
solar mixture taken from Caffau et al. (2011) complemented by Lodders (2010),
which corresponds to $(Z/X)_{\odot}=0.0209$. The grid considers convective
core overshooting included as an instantaneous mixing between Schwarzschild’s
convective limit up to layers at a distance $\alpha_{\mathrm{ov}}=0.2H_{P}$
from it, where $H_{P}$ is the pressure scale height at the Schwarzschild
limit. Microscopic diffusion is not taken into account. In the calculation
process, SPInS can incorporate various priors on the initial mass function
(IMF), stellar formation rate (SFR) and metallicity distribution function
(MDF). Here we took Kroupa et al. (2013) as IMF and no priors on the SFR and
MDF.

With the observational constraints for HD 87887 derived in Sects. 4 and 5
($T_{\mathrm{eff}}=9950\pm 125\,\mathrm{K},\log g=3.60\pm 0.25$ dex and
$\mathrm{[Fe/H]}=-0.14\pm 0.10$), SPInS provided as mean values an age
$A=385\pm 77\,\mathrm{Myr}$, a mass $M=2.57\pm 0.32\,M_{\odot}$, a radius
$R=3.07\pm 0.90\,R_{\odot}$, a mean density $\overline{\rho}\simeq 0.13\pm
0.11\,\mathrm{g\,cm^{-3}}$, and a luminosity $L=90\pm 52\,L_{\odot}$. The
observed position of the star in the Kiel diagram is provided in Fig. 4
together with the isochrones for the $\pm 1\sigma$ age-values inferred by
SPInS showing that the star evolves at the vicinity of the main sequence turn-
off. We can compare the inferred radius with the observed one using the
Swihart et al. (2017)’s angular diameter obtained by interferometry,
$\theta\simeq 0.361\pm 0.065$ mas, and parallax values from the literature,
that is $\varpi_{\mathrm{G}}=7.66\pm 0.37$ mas (Gaia Collaboration, 2020, Gaia
DR3) and $\varpi_{\mathrm{H}}=11.51\pm 0.98$ mas (van Leeuwen, 2007,
Hipparcos). This leads to linear radius values of $R_{\mathrm{G}}\simeq 5.1\pm
1.2\,R_{\odot}$ and $R_{\mathrm{H}}\simeq 3.4\pm 0.9\,R_{\odot}$,
respectively, such that $R_{\mathrm{H}}$ is closer to our inferred radius
rather than $R_{\mathrm{G}}$. To assess our results, we also attempted to
derive the stellar parameters using absolute magnitude and a color index in
SPInS instead of the $T_{\mathrm{eff}}$ and $\log g$ values derived
previously. From the Hipparcos and Tycho-2 constraints on
$\varpi_{\mathrm{H}},V_{T}=4.474\pm 0.003$ mag and $(B-V)_{T}=-0.030\pm 0.004$
mag (Høg et al., 2000), we found an age $A=350\pm 25\,\mathrm{Myr}$, a mass
$M=2.87\pm 0.12\,M_{\odot}$, and a radius $R=3.66\pm 0.34\,R_{\odot}$, all
compatible with our results. On the other hand, we could not find a solution
when using the absolute Gaia G-magnitude and (BP-RP) color index, which may
indicate difficulties with the Gaia parallax. Indeed, the Gaia-DR3 parallax of
$\alpha$ Sex should be taken with care for three reasons: (i) the star is
bright; (ii) the astrometric excess noise of the source is around $2$
mas444see
https://gea.esac.esa.int/archive/documentation/GDR2/Gaia_archive/chap_datamodel/sec_dm_main_tables/ssec_dm_gaia_source.html
and https://www.cosmos.esa.int/web/gaia/science-performance (F. Arenou,
private communication).; and (iii) it is a member of a binary system (Kervella
et al., 2019).

Figure 4: Kiel diagram showing the observed position of HD 87887 together with
two isochrones computed for the $\pm 1\sigma$ age-values inferred by SPInS.

##  7 Discussion and Conclusions

To place the detected variability caused by pulsations in an evolutionary
context, we calculate the expected period of the fundamental radial pressure
mode of $\alpha$ Sex using its derived parameters. Following Ledoux (1945), we
estimate the period of the fundamental radial pressure mode of $\alpha$ Sex to
be:

$P=\left(\frac{3\pi}{G\overline{\rho}}\times\frac{1}{3\Gamma_{1}-4}\right)^{\frac{1}{2}}~{},$
(2)

assuming the adiabatic exponent is constant throughout the star. For an ideal
monoatomic gas for which $\Gamma_{1}\approx 5/3$, this yields $\nu=2.6\pm 1.1$
d-1 (i.e. $P=9.3\pm 4.1$ hours). This estimate is analogous and compatible
with that of the empirical $Q=P\sqrt{\frac{\rho}{\rho_{\odot}}}$ relation for
radial pressure modes in $\delta$ Sct stars (Breger & Bregman, 1975), in which
$Q=0.033$ for fundamental radial pressure modes. Our estimates are entirely
consistent with the observed dominant frequency in the TESS light curve of
$\alpha$ Sex. Therefore, we conclude that the observed variability is low-
radial order p-mode pulsations. Given its advanced evolutionary stage, it is
possible that the observed pulsation modes are of mixed pressure- and gravity-
mode character (Aerts et al., 2010). However, future forward asteroseismic
data based on much longer light curves with higher duty cycle are needed to
confirm this.

Although the pulsations observed in the TESS light curve of $\alpha$ Sex may
at first glance appear to resemble the frequency spectra of slowly pulsating B
(SPB) stars (e.g. Bowman et al. 2019; Sharma et al. 2022), we present several
reasons why this is not the case. SPB stars are mid-to-late B-type dwarf stars
and hence hotter and less evolved than $\alpha$ Sex. Moreover, SPB stars are
typically fast rotators (Pedersen et al., 2021) and $\alpha$ Sex is not.
Indeed, $\alpha$ Sex does not have the characteristic flat-bottomed Fe II
lines that Vega has, which is a fast rotator seen pole-on (Hill et al., 2010).
If, for example, $\alpha$ Sex were an SPB star and lies within an extension of
the SPB stars towards cooler temperatures and lower gravities, it would need
to be pulsating in gravity or perhaps Rossby modes (for which the restoring
force is the Coriolis force) rather than pressure modes. However, the low
$v\,\sin\,i$ combined with $i\simeq 90$ degrees given that the system is
eclipsing based on the indicative UV photometry eclipse, makes $\alpha$ Sex
unlikely to have gravito(inertial) modes. This is because the frequencies of
slowly rotating SPB pulsators are not as high as 2.5 c/d as seen in the TESS
light curve of $\alpha$ Sex (see e.g. Pedersen et al. 2021). For gravity-mode
frequencies to be so high in such a star, the impact of the Coriolis force
would also need to be large, thus $\alpha$ Sex would need to be rapidly
rotating. Finally, gravity modes are unlikely to exist above the fundamental
radial pressure mode frequency that we derive in this work. Hence we conclude
low-radial order pressure and/or mixed modes are the most likely
identification of the pulsations based on the fundamental parameters of
$\alpha$ Sex derived in this work.

On the issue of whether pressure mode pulsations are expected in a star such
as $\alpha$ Sex, we refer to Bowman & Kurtz (2018) and Murphy et al. (2019).
In these studies of thousands of $\delta$ Sct stars observed by the Kepler
space telescope, the observational hot edge of the classical instability strip
was determined to correspond to $T_{\rm eff}\simeq 9000$ K based on the
density of such stars in the Kiel and HR diagrams. However, there exist a non-
negligible number of outliers with hotter $T_{\rm eff}$ values. Pulsation
excitation models struggle to explain the observed pulsations in such stars,
because the heat-engine ($\kappa$) mechanism is inefficient at these
temperatures (Dupret et al., 2004). Indeed, other pulsation excitation
mechanisms operate in delta Scuti stars. Antoci et al. (2014) and Antoci et
al. (2019) describe the role of turbulent pressure in the excitation of
pulsations in $\delta$ Scuti stars, but such a mechanism typically excites
high-radial order and thus high-frequency pressure modes. The discovery of
pulsations in $\alpha$ Sex make it an interesting case study for follow-up
asteroseismic modeling. Further monitoring with TESS may confirm the presence
of eclipses too.

Acknowledgments. The authors gratefully acknowledge Dr. Frédéric Arenou for
enlightening discussion on Gaia parallaxes. The authors thank the TESS science
team for the excellent data, which were obtained from the Mikulski Archive for
Space Telescopes (MAST) at the Space Telescope Science Institute (STScI),
which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support to MAST for these
data is provided by the NASA Office of Space Science via grant NAG5-7584 and
by other grants and contracts. Funding for the TESS mission is provided by the
NASA Explorer Program. This research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France. This work was supported by FCT/MCTES
through the research grants UIDB/04434/2020, UIDP/04434/2020 and PTDC/FIS-
AST/30389/2017. DMB gratefully acknowledges a senior postdoctoral fellowship
from the Research Foundation Flanders (FWO) with grant agreement no. 1286521N.
MD is supported by national funds through FCT in the form of a work contract.

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Table 4: Line identifications for $\alpha$ Sex $\lambda_{\mathrm{obs}}$ (Å) |  $\lambda_{\mathrm{lab}}$ (Å) | Species | $\log gf$ | $E_{low}$ | Ref.
---|---|---|---|---|---
3900.44 | 3900.55 | Ti II | -0.45 | 9118.260 | VALD
3903.78 | 3903.76 | Fe II | -1.49 | 60807.23 | VALD
3905.97 | 3906.04 | Fe II | -1.83 | 44929.549 | VALD
3913.47 | 3913.47 | Ti II | -0.53 | 8997.710 | VALD
3914.56 | 3914.50 | Fe II | -4.05 | 13474.411 | VALD
3917.28 | 3917.32 | Mn II | -1.15 | 55759.270 | VALD
3918.32 | 3918.30 | Fe II | -3.63 | 73054.879 | VALD
3918.76 | 3918.77 | Fe II | -2.30 | 79246.171 | VALD
3920.59 | 3920.64 | Fe II | -1.330 | 60628.698 | VALD
3923.43 | 3923.46 | S II | 0.440 | 130641.115 | VALD
3924.953 | 3924.842 | Fe II | -1.100 | 78138.990 | VALD
3926.527 | 3926.416 | Mn II | -1.600 | 55759.270 | VALD
3930.28 | 3930.30 | Fe I | -1.490 | 704.007 | VALD
3933.71 | 3933.66 | Ca II | 0.13 | 0.000 | VALD
3936.07 | 3935.96 | Fe II | -1.720 | 44915.056 | VALD
3938.29 | 3938.29 | Fe II | -4.100 | 13474.447 | VALD
3939.02 | 3938.97 | Fe II | -1.930 | 47674.729 | VALD
3941.18 | 3941.231 | Mn II | -2.430 | 43852.362 | VALD
3943.84 | 3943.86 | Mn II | -2.260 | 43699.122 | VALD
3947.33 | 3947.30 | O I | -2.100 | 73768.202 | VALD
3990.95 | 3990.91 | S II | -0.50 | 128233.19 | VALD
3993.52 | 3993.50 | S II | -0.82 | 115285.608 | VALD
3995.04 | 3995.00 | N II | 0.28 | 149187.803 | VALD
4002.42 | 4002.54 | Fe II | -2.070 | 48038.381 | VALD
4009.34 | 4009.26 | He I | -1.47 | 171134.998 | VALD
4012.53 | 4012.50 | Cr II | -0.89 | 45669.369 | VALD
4024.67 | 4024.552 | Fe II | -2.400 | 36252.930 | VALD
4026.26 | 4026.18 | He I | -2.62 | 169086.769 | hfs
| 4026.19 | He I | -0.70 | 169086.867 |
| 4026.19 | He I | -1.45 | 169086.769 |
| 4026.20 | He I | -0.98 | 169086.845 |
| 4026.20 | He I | -0.98 | 169086.845 |
4032.94 | 4032.940 | Fe II | -2.570 | 36254.622 | VALD
4045.85 | 4045.81 | Fe I | 0.280 | 11976.239 | VALD
4048.86 | 4048.83 | Fe II | -2.380 | 44917.017 | VALD
4057.43 | 4057.46 | Fe II | -1.680 | 58668.776 | VALD
4061.80 | 4061.78 | Fe II | -2.650 | 48039.087 | VALD
4063.60 | 4063.60 | Fe I | 0.060 | 12560.934 | VALD
4067.06 | 4067.03 | Ni II | -1.830 | 32496.075 | VALD
4075.63 | 4075.62 | Cr II | -3.470 | 25035.399 | VALD
4081.39 | 4081.44 | Mn II | -2.190 | 49288.543 | VALD
4111.85 | 4111.88 | Fe II | -2.670 | 48038.381 | VALD
4119.62 | 4119.62 | Fe II | -2.690 | 90780.019 | VALD
4120.86 | 4120.81 | He I | -1.740 | 169086.867 | hfs
| 4120.82 | He I | -1.960 | 169086.943 |
| 4120.99 | He I | -2.430 | 169087.931 |
4122.63 | 4122.67 | Fe II | -3.300 | 20830.553 | VALD
4124.67 | 4124.61 | Fe II | -4.200 | 20516.953 | VALD
4128.06 | 4128.07 | Si II | 0.360 | 79338.502 | VALD
4130.78 | 4130.872 | Si II | -0.780 | 79355.019 | VALD
| 4130.89 | Si II | 0.550 | 79355.019 | VALD
4136.90 | 4136.902 | Mn II | -1.250 | 49514.374 | VALD
4143.90 | 4143.76 | He I | -1.200 | 179134.998 | VALD
4162.63 | 4162.67 | S II | 0.780 | 128599.162 | VALD
4163.54 | 4163.65 | Ti II | -0.130 | 20891.790 | VALD
4164.92 | 4164.92 | Fe III | 1.010 | 198821.396 | VALD
4167.21 | 4167.30 | Fe II | -0.560 | 90300.626 | VALD
4169.04 | 4168.97 | He I | -2.340 | 171134.998 | VALD
4171.02 | 4171.03 | Mn II | -2.340 | 49425.654 | VALD
4171.85 | 4171.903 | Cr II | -2.940 | 25043.517 | VALD
| 4171.904 | Ti II | -0.290 | 20951.754 | VALD
4173.46 | 4173.46 | Fe II | -2.160 | 20830.553 | VALD
4174.17 | 4174.27 | S II | 0.800 | 140319.232 | VALD
4175.97 | 4175.99 | Fe II | -3.840 | 54902.315 | VALD
4178.61 | 4178.63 | Fe II | -4.290 | 60402.341 | VALD
4199.39 | 4199.49 | Fe II | -0.330 | 89922.758 | VALD
4200.47 | 4200.518 | Fe II | -0.410 | 90067.932 | VALD
4205.38 | 4205.38 | Mn II | -3.450 | 14593.834 | VALD
4206.44 | 4206.37 | Mn II | -1.540 | 43528.661 | VALD
4233.12 | 4233.17 | Fe II | -1.810 | 20830.553 | VALD
4239.05 | 4239.15 | Mn II | -2.240 | 43311.972 | VALD
4242.33 | 4242.33 | Mn II | -1.260 | 49820.865 | VALD
| 4242.36 | Cr II | -1.170 | 31221.723 | VALD
4244.46 | ? |  |  |  |
4246.85 | 4246.82 | Sc II | 0.240 | 2540.950 | VALD
4250.43 | 4250.44 | Fe II | -1.720 | 61974.931 | VALD
4251.64 | 4251.72 | Mn II | -1.060 | 49885.389 | VALD
4252.97 | 4252.96 | Mn II | -1.140 | 49893.458 | VALD
4258.17 | 4258.11 | Fe II | -3.500 | 21812.044 | VALD
4259.17 | 4259.17 | Mn II | -1.440 | 43537.186 | VALD
4261.92 | 4261.91 | Cr II | -1.340 | 31165.263 | VALD
4263.81 | 4263.87 | Fe II | -1.690 | 62048.230 | VALD
4267.15 | 4267.18 | C II | 0.720 | 145550.705 | VALD
4273.26 | 4273.33 | Fe II | -3.300 | 21812.044 | VALD
4278.29 | 4278.15 | Fe II | -3.950 | 21712.445 | VALD
4286.17 | 4286.16 | Fe III | 0.700 | 184316.573 | VALD
4288.05 | 4288.07 | Mn II | -2.760 | 43311.301 | VALD
4290.25 | 4290.22 | Ti II | -0.850 | 9395.802 | VALD
4292.17 | 4292.23 | Mn II | -1.540 | 43395.394 | VALD
4294.18 | 4294.10 | Ti II | -1.110 | 8744.341 | VALD
4296.57 | 4296.57 | Fe II | -2.900 | 21812.044 | VALD
4300.18 | 4300.04 | Ti II | -0.440 | 9518.152 | VALD
4303.10 | 4303.18 | Fe II | -2.610 | 21812.044 | VALD
4307.92 | 4307.87 | Ti II | -1.070 | 9395.802 | VALD
4312.98 | 4312.85 | Ti II | -1.100 | 9518.152 | VALD
4314.24 | 4314.31 | Fe II | -3.600 | 21583.397 | VALD
4320.92 | 4320.96 | Ti II | -1.800 | 9395.802 | VALD
4325.44 | 4325.44 | Fe II | -2.380 | 49506.310 | VALD
| 4325.53 | Fe II | -2.360 | 49103.030 | VALD
4326.59 | 4326.64 | Mn II | -1.370 | 43537.186 | VALD
4351.70 | 4351.76 | Fe II | -2.080 | 21812.044 | VALD
4354.39 | 4354.34 | Fe II | -1.350 | 61725.611 | VALD
4357.61 | 4357.58 | Fe II | -2.010 | 49100.956 | VALD
4361.15 | 4361.25 | Fe II | -2.260 | 49506.310 | VALD
4363.16 | 4363.26 | Mn II | -1.890 | 44900.887 | VALD
4365.20 | 4365.22 | Mn II | -1.340 | 53014.822 | VALD
4368.21 | 4368.242 | O I | -1.960 | 76794.977 | VALD
| 4368.250 | O I | -2.190 | 76794.977 | VALD
4369.42 | 4369.400 | Fe II | -3.600 | 22409.818 | VALD
4374.71 | 4374.82 | Ti II | -1.290 | 16625.110 | VALD
4377.61 |  | ? |  |  |
4379.62 | 4379.67 | Mn II | -1.870 | 43852.362 | VALD
4382.51 | 4382.51 | Fe III | -3.020 | 66522.952 | VALD
4384.40 | 4384.32 | Fe II | -3.700 | 21430.357 | VALD
4385.35 | 4385.39 | Fe II | -2.600 | 22409.818 | VALD
4388.04 | 4387.93 | He I | -0.887 | 171134.897 | VALD
4390.55 | 4390.514 | Mg II | -1.480 | 80650.022 | VALD
| 4390.564 | Mg II | -0.520 | 80650.022 | VALD
4395.04 | 4395.031 | Ti II | -0.660 | 8744.341 | VALD
4395.83 | 4395.76 | Fe III | -2.600 | 66591.679 | VALD
4402.92 | 4402.879 | Fe II | -2.600 | 49506.924 | VALD
4404.87 | 4404.75 | Fe I | -0.140 | 12560.934 | VALD
4407.74 | 4407.68 | Fe II | 0.780 | 109473.634 | VALD
4409.54 | 4409.53 | Fe II | 0.950 | 109489.771 | VALD
4411.14 | 4411.072 | Ti II | -0.670 | 24961.191 | VALD
| 4411.15 | C II | 0.530 | 198425.425 | VALD
4413.62 | 4413.60 | Fe II | -4.200 | 21581.615 | VALD
4416.81 | 4416.83 | Fe II | -2.600 | 22409.818 | VALD
4417.70 | 4417.71 | Ti II | -1.430 | 9395.802 | VALD
4418.73 | 4418.78 | Ce II | 0.180 | 6967.547 | VALD
4419.56 | 4419.60 | Fe III | -2.210 | 66468.153 | VALD
| 4419.60 | Cr II | -0.260 | 94365.189 | VALD
4428.01 | 4427.99 | Mg II | -1.210 | 80619.500 | VALD
4430.99 | 4431.02 | Fe III | -2.570 | 66522.952 | VALD
4434.00 | 4433.99 | Mg II | -0.910 | 80650.022 | VALD
4437.58 | 4437.55 | He I | -2.030 | 171134.998 | VALD
4443.81 | 4443.79 | Ti II | -0.720 | 8710.567 | VALD
4451.49 | 4451.55 | Fe II | -1.910 | 49506.924 | VALD
4455.33 | 4455.27 | Fe II | -2.000 | 50216.076 | VALD
4461.65 | 4461.71 | Fe II | -2.100 | 50212.834 | VALD
4463.43 | 4463.41 | Ce II | -0.110 | 7722.285 | VALD
4464.46 | 4464.45 | Ti II | -2.080 | 9363.620 | VALD
4468.51 | 4468.51 | Ti II | -0.620 | 9118.285 | VALD
4469.93 | 4469.90 | Mn II | -3.170 | 49882.153 |
4471.46 | 4471.470 | He I | -2.210 | 169086.769 | hfs
| 4471.474 | He I | -1.040 | 169086.769 |
| 4471.474 | He I | -0.240 | 169086.769 |
| 4471.486 | He I | -1.040 | 169086.769 |
| 4471.489 | He I | -0.560 | 169086.769 |
4472.73 | 4472.62 | Fe II | -2.340 | 61974.931 |
4478.67 | 4478.64 | Mn II | -0.940 | 53595.541 | VALD
4481.21 | 4481.130 | Mg II | 0.750 | 71490.190 | VALD
| 4481.150 | Mg II | -0.550 | 71490.190 | VALD
| 4481.327 | Mg II | 0.590 | 71491.058 | VALD
4483.49 | 4483.43 | S II | -0.320 | 128233.197 | VALD
4489.19 | 4489.19 | Fe II | -3.000 | 22810.345 | VALD
4491.37 | 4491.40 | Fe II | -2.640 | 23031.283 | VALD
4493.47 | 4493.53 | Fe II | -1.560 | 63876.325 | VALD
4494.41 | 4494.42 | Zr II | -0.480 | 19433.239 | VALD
4501.24 | 4501.27 | Ti II | -0.770 | 8997.787 | VALD
| 4501.28 | Fe II | -0.950 | 90387.870 | VALD
4515.39 | 4515.34 | Fe II | -2.360 | 22939.352 | VALD
4518.91 | 4518.96 | Mn II | -1.310 | 53595.541 | VALD
4520.15 | 4520.22 | Fe II | -2.600 | 22637.195 | VALD
4522.57 | 4522.63 | Fe II | -1.990 | 22939.352 | VALD
4524.87 | 4524.94 | S II | 0.030 | 121530.021 | VALD
4526.50 | 4526.40 | Fe II | -2.330 | 62962.204 | VALD
4529.28 | ? |  |  |  |
4534.00 | 4533.97 | Ti II | -0.770 | 9975.999 | VALD
4541.45 | 4541.52 | Fe II | -3.000 | 23031.283 | VALD
4549.39 | 4549.47 | Fe II | -1.730 | 22810.345 | VALD
4552.47 | 4552.41 | S II | -0.100 | 121528.718 | VALD
4555.01 | 4554.99 | Cr II | -1.370 | 32836.653 | VALD
4555.86 | 4555.89 | Fe II | -2.250 | 22810.345 | VALD
4558.61 | 4558.64 | Cr II | -0.660 | 32854.249 | VALD
4563.69 | 4563.76 | Ti II | -0.960 | 9851.014 | VALD
4571.96 | 4571.97 | Ti II | -0.320 | 12677.106 | VALD
4576.34 | 4576.33 | Fe II | -2.920 | 22939.352 | VALD
4579.67 | 4579.72 | Ti II | -1.950 | 40581.490 | VALD
4582.69 | 4582.84 | Fe II | -3.060 | 22939.352 | VALD
4583.81 | 4583.84 | Fe II | -1.740 | 22637.195 | VALD
4588.12 | 4588.20 | Cr II | -0.640 | 32836.653 | VALD
4589.87 | 4589.95 | Ti II | -1.780 | 9975.999 | VALD
4595.95 | 4596.02 | Fe II | -1.960 | 50212.834 | VALD
4598.43 | 4598.49 | Fe II | -1.540 | 62945.045 | VALD
4616.63 | 4616.63 | Cr II | -1.290 | 32844.706 | VALD
4618.79 | 4618.81 | Cr II | -1.110 | 32854.941 | VALD
4620.50 | 4620.51 | Fe II | -3.190 | 22810.345 | VALD
4621.51 | 4621.40 | N II | -0.540 | 148940.167 | VALD
4625.70 | 4625.64 | C II | 0.700 | 199941.414 | VALD
4629.31 | 4629.29 | Ti II | -2.250 | 9518.152 | VALD
| 4629.332 | Fe II | -2.260 | 22637.195 | VALD
4634.09 | 4634.07 | Cr II | -1.240 | 32844.706 | VALD
4635.21 | 4635.32 | Fe II | -1.580 | 48039.109 | VALD
4638.05 | 4638.04 | Fe II | -1.540 | 62169.219 | VALD
4656.90 | 4656.98 | Fe II | -3.570 | 23317.635 | VALD
4663.34 | ? |  |  |  |
4713.31 | 4713.38 | He I | -1.920 | 169087.931 | VALD
4716.40 | 4716.267 | S II | -0.370 | 109831.595 | VALD
4727.92 | 4727.84 | Mn II | -1.950 | 43311.972 | VALD
4730.37 | 4730.40 | Mn II | -2.020 | 43336.173 | VALD
4731.49 | 4731.44 | Fe II | -3.100 | 23317.635 | VALD
4738.23 | 4738.29 | Mn II | -1.870 | 43395.394 | VALD
4755.72 | 4755.73 | Mn II | -1.220 | 43529.741 | VALD
4764.64 | 4764.728 | Mn II | -1.330 | 43537.810 | VALD
4784.52 | 4784.63 | Mn II | -1.500 | 53014.822 | VALD
4791.82 | 4791.78 | Mn II | -1.680 | 49885.389 | VALD
4806.71 | 4806.860 | Mn II | -1.840 | 43696.217 | VALD
4815.51 | 4815.55 | S II | 0.070 | 110268.595 | VALD
| 4815.49 | Mn II | -3.780 | 43696.190 |
4824.11 | 4824.06 | S II | 0.180 | 110268.595 | VALD
| 4824.13 | Cr II | -1.230 | 31219.331 | VALD
4826.53 | 4826.51 | Mn II | -3.000 | 94230.896 |
4848.18 | 4848.24 | Cr II | -1.130 | 31168.575 | VALD
4876.37 | 4876.40 | Cr II | -1.460 | 31084.610 | VALD
4883.28 | 4883.28 | Fe II | -0.600 | 82853.704 | VALD
4908.12 | 4908.15 | Fe II | -0.270 | 83308.242 | VALD
4909.75 | 4909.75 | Fe II | -2.610 | 82978.679 | VALD
4911.52 | ? |  |  |  |
4913.29 | 4913.30 | Fe II | 0.050 | 82978.717 | VALD
4917.22 | 4917.21 | S II | -0.380 | 112937.572 | VALD
4921.86 | ? |  |  |  |
4923.90 | 4923.92 | Fe II | -1.210 | 23317.635 | VALD
4948.42 | 4948.49 | Mn II | -3.220 | 62572.200 | VALD
4951.58 | 4951.58 | Fe II | 0.210 | 83136.510 | VALD
4954.03 | 4953.98 | Fe II | -2.810 | 44933.149 | VALD
4977.02 | 4977.04 | Fe II | -0.040 | 83558.566 | VALD
4984.52 | 4984.49 | Fe II | 0.080 | 83308.242 | VALD
| 4984.58 | Fe II | -1.260 | 83990.065 | VALD
4990.51 | 4990.51 | Fe II | 0.200 | 83308.242 | VALD
4991.70 | ? |  |  |  |
4993.38 | 4993.36 | Fe II | -3.700 | 22637.195 | VALD
5001.86 | 5001.95 | Fe II | 0.920 | 82853.704 | VALD
5004.19 | 5004.19 | Fe II | 0.500 | 82853.704 | VALD
5007.21 | ? |  |  |  |
5009.54 | 5009.56 | S II | -0.230 | 109831.595 | VALD
5014.03 | 5014.04 | S II | 0.050 | 113461.537 | VALD
5015.63 | 5015.68 | He I | -0.820 | 166277.440 | VALD
| 5015.75 | Fe II | -0.030 | 83459.720 | VALD
5018.37 | 5018.44 | Fe II | -1.350 | 23317.635 | VALD
5019.70 | ? |  |  |  |
5021.42 | 5021.47 | Ni II | 0.920 | 100309.295 | VALD
5022.60 | 5022.42 | Fe II | -0.070 | 83459.720 | VALD
5026.91 | 5026.80 | Fe II | -0.440 | 83136.510 | VALD
5028.95 | 5028.98 | Ni II | 0.170 | 100389.516 | VALD
5030.63 | 5030.63 | Fe II | 0.430 | 82978.717 | VALD
5032.58 | 5032.45 | S II | 0.190 | 110268.595 | VALD
5034.21 | 5034.17 | Fe II | -0.800 | 83558.566 | VALD
5035.69 | 5035.71 | Fe II | 0.630 | 82978.717 | VALD
5036.856 | 5036.713 | Fe II | -0.560 | 83812.350 | VALD
5040.92 | 5041.02 | Si II | 0.030 | 81191.341 | VALD
5045.11 | 5045.11 | Fe II | 0.000 | 83136.510 | VALD
5047.62 | 5047.64 | Fe II | -0.240 | 83136.510 | VALD
| 5047.74 | He I | -1.600 | 171134.198 | VALD
5056.07 | 5055.98 | Si II | 0.520 | 81251.320 | VALD
5061.74 | 5061.72 | Fe II | 0.280 | 83136.510 | VALD
5067.89 | 5067.890 | Fe II | -0.080 | 83308.242 | VALD
5070.90 | 5070.90 | Fe II | 0.270 | 83136.510 | VALD
5073.94 | 5073.896 | Fe II | -0.720 | 84266.595 | VALD
| 5074.051 | Fe II | -2.200 | 54904.243 | VALD
| 5073.90 | Fe III | -2.560 | 69788.188 | VALD
5075.80 | 5075.760 | Fe II | 0.180 | 84326.965 | VALD
5082.10 | 5082.23 | Fe II | -0.130 | 83990.103 | VALD
5087.33 | 5087.300 | Fe II | -0.420 | 83713.585 | VALD
| 5087.419 | Y II | -0.170 | 8743.050 | VALD
5089.25 | 5089.21 | Fe II | 0.010 | 83308.242 | VALD
5093.62 | 5093.58 | Fe II | -2.320 | 54869.899 | VALD
5097.19 | 5097.27 | Fe II | 0.320 | 83713.585 | VALD
5098.70 | 5098.68 | Fe II | -0.490 | 84268.805 | VALD
5100.71 | 5100.73 | Fe II | 0.720 | 83726.416 | VALD
5102.54 | 5102.52 | Mn II | -1.900 | 48320.677 | VALD
5106.12 | 5106.11 | Fe II | -0.250 | 83308.242 | VALD
5107.33 | 5107.25 | Fe II | -3.960 | 50075.908 | VALD
5116.99 | 5117.031 | Fe II | -0.040 | 84131.623 | VALD
5123.31 | 5123.33 | Mn II | -1.850 | 48336.810 | VALD
5127.53 | 5127.63 | Fe III | -2.560 | 69837.758 | VALD
5129.96 | ? |  |  |  |
5132.58 | 5132.66 | Fe II | -4.100 | 22637.195 | VALD
5133.97 | 5134.07 | Fe II | 0.290 | 104916.599 | VALD
5144.28 | 5144.32 | Fe II | 0.310 | 84424.421 | VALD
5145.85 | 5145.730 | Fe II | -0.210 | 83990.103 | VALD
| 5145.822 | Fe II | -0.140 | 83990.103 | VALD
5149.25 | 5149.19 | Fe II | 0.410 | 103601.919 |
5152.850 | 5152.88 | Fe II | -0.990 | 83990.065 | VALD
5154.24 | ? |  |  |  |
5156.31 | 5156.28 | Fe II | -3.750 | 93487.649 |
5157.40 | 5157.28 | Fe II | -0.170 | 84326.965 | VALD
5160.83 | 5160.840 | Fe II | -2.600 | 44915.056 | VALD
5163.37 | ? |  |  |  |
5166.17 | 5166.20 | Fe II | 0.930 | 108134.747 | VALD
5168.92 | 5169.03 | Fe II | -0.870 | 23317.635 | VALD
5170.49 | ? |  |  |  |
5172.97 | 5173.13 | Fe II | 0.460 | 105061.784 | VALD
5177.37 | 5177.37 | Fe II | 1.160 | 103642.253 | VALD
5180.21 | 5180.31 | Fe II | -0.090 | 83812.350 | VALD
5183.57 | 5183.53 | Fe II | -0.850 | 84131.564 | VALD
5188.80 | 5188.687 | Ti II | -1.220 | 12758.260 | VALD
5189.96 | 5190.00 | Fe II | 0.490 | 105400.535 | VALD
5192.70 | 5192.62 | Fe II | 0.200 | 103101.857 | VALD
5196.01 | 5195.94 | Fe II | 0.920 | 104174.580 | VALD
5197.55 | 5197.57 | Fe II | -2.050 | 26055.412 | VALD
5199.00 | 5199.12 | Fe II | 0.120 | 83713.585 | VALD
5200.92 | 5200.80 | Fe II | -0.040 | 83812.350 | VALD
| 5201.03 | S II | 0.430 | 121528.718 | VALD
5210.58 | 5210.550 | Fe II | 0.790 | 103166.386 | VALD
5212.61 | 5212.62 | S II | 0.320 | 121530.021 | VALD
5213.97 | 5213.95 | Fe II | -0.260 | 84527.806 | VALD
| 5214.003 | Fe II | 0.860 | 104069.717 | VALD
5215.48 | 5215.35 | Fe II | 0.000 | 83713.585 | VALD
5216.90 | 5216.86 | Fe II | 0.670 | 84527.806 | VALD
| 5216.859 | Fe II | 0.480 | 84710.751 | VALD
5218.70 | 5218.84 | Fe II | -0.170 | 83726.416 | VALD
5223.26 | 5223.20 | Fe II | 0.450 | 103876.141 | VALD
| 5223.260 | Fe II | -0.170 | 83812.350 | VALD
5225.26 | 5225.21 | Fe II | 0.980 | 105287.615 | VALD
| 5225.35 | Fe II | 0.710 | 103190.571 | VALD
5227.44 | 5227.32 | Fe II | 0.190 | 84844.864 | VALD
| 5227.49 | Fe II | 0.850 | 84296.883 | VALD
5228.71 | 5228.63 | Fe II | 0.900 | 108779.995 | VALD
5232.76 | 5232.78 | Fe II | -0.080 | 83726.416 | VALD
5234.53 | 5234.44 | Fe II | -2.210 | 25981.646 | VALD
| 5236.621 | Fe II | -0.680 | 84326.965 | VALD
5237.90 | 5237.95 | Fe II | 0.100 | 84266.595 | VALD
5239.62 | 5239.65 | Mn II | -3.430 | 82419.479 |
5241.00 | 5241.06 | Fe II | -0.580 | 83812.350 | VALD
5245.11 | 5245.07 | Fe II | 0.870 | 108465.440 | VALD
5247.95 | 5247.96 | Fe II | 0.550 | 84938.264 | VALD
5251.20 | 5251.21 | Fe II | -0.660 | 84325.265 | VALD
| 5251.23 | Fe II | 0.420 | 84844.864 | VALD
5254.77 | 5254.920 | Fe II | -3.340 | 26051.708 | VALD
5257.02 | 5256.93 | Fe II | -4.180 | 23317.488 | VALD
| 5257.12 | Fe II | 0.160 | 84685.247 | VALD
5258.08 | 5258.03 | Fe II | -2.100 | 84685.198 | VALD
| 5258.12 | Fe II | -0.920 | 84424.372 | VALD
5260.15 | 5260.254 | Fe II | 1.090 | 84035.172 | VALD
5262.462 | 5262.313 | Fe II | -0.370 | 85048.655 | VALD
5264.169 | 5264.020 | Fe II | -0.440 | 84685.247 | VALD
5264.328 | 5264.179 | Fe II | 0.300 | 84710.751 | VALD
5264.364 | 5264.215 | Mg II | -0.370 | 93310.590 | VALD
5264.49 | 5264.36 | Mg II | -0.530 | 93311.112 | VALD
5272.38 | 5272.41 | Fe II | -2.010 | 48039.109 | VALD
5274.83 | 5274.965 | Cr II | -1.560 | 32834.831 | VALD
5275.92 | 5275.997 | Fe II | -1.900 | 25805.326 | VALD
5284.02 | 5284.07 | Fe II | -3.200 | 23317.635 | VALD
| 5284.11 | Fe II | -3.190 | 23317.632 | VALD
5291.67 | 5291.67 | Fe II | 0.580 | 84527.779 | VALD
5296.99 | 5297.000 | Mn II | -0.240 | 79550.458 | hfs
| 5297.028 | Mn II | 0.400 | 79550.458 |
| 5297.060 | Mn II | 0.620 | 79550.502 |
5299.29 | 5299.302 | Mn II | -0.440 | 79558.533 | hfs
| 5299.330 | Mn II | 0.380 | 79558.533 |
| 5299.370 | Mn II | 0.830 | 79558.560 |
5302.39 | 5302.402 | Mn II | 0.200 | 79566.596 | hfs
| 5302.440 | Mn II | 1.000 | 79569.219 |
5306.06 | 5306.18 | Fe II | 0.040 | 84870.912 | VALD
5308.36 | 5308.41 | Fe II | 0.550 | 104118.119 | VALD
| 5308.41 | Cr II | -1.810 | 32836.653 | VALD
5316.62 | 5316.61 | Fe II | -1.780 | 25428.789 | VALD
5316.78 | 5316.78 | Fe II | -2.800 | 25981.646 | VALD
5318.21 | 5318.06 | Fe II | -0.230 | 84527.806 | VALD
5320.68 | 5320.72 | S II | 0.430 | 121530.021 | VALD
5322.01 | 5321.86 | Fe II | 0.670 | 106021.587 | VALD
5325.38 | 5325.543 | Fe II | -3.260 | 25981.646 | VALD
5330.78 | 5330.73 | O I | -2.570 | 86631.453 | VALD
| 5330.74 | O I | -1.570 | 86631.453 | VALD
| 5330.740 | O I | -0.980 | 86631.453 | VALD
| 5330.78 | Ne I | -1.040 | 148257.789 |
5339.50 | 5339.594 | Fe II | 0.520 | 84296.883 | VALD
5362.75 | 5362.74 | Fe II | -0.190 | 84710.751 | VALD
5370.43 | 5370.28 | Fe II | -0.570 | 84266.595 | VALD
5375.83 | 5375.842 | Fe II | -0.330 | 84296.883 | VALD
5375.994 | 5375.842 | Fe II | -0.700 | 85048.655 | VALD
5387.00 | 5387.06 | Fe II | 0.500 | 84863.380 | VALD
5393.80 | 5393.84 | Fe II | -0.250 | 84296.883 | VALD
5395.83 | 5395.86 | Fe II | 0.280 | 85495.368 | VALD
5401.95 | 5401.89 | Fe II | -0.840 | 85462.859 |
5405.14 | 5405.09 | Fe II | -0.430 | 85172.826 | VALD
5411.49 | 5411.373 | Fe II | -0.050 | 85495.368 | VALD
5414.42 | ? |  |  |  |
5427.89 | 5427.83 | Fe II | -1.580 | 54232.199 | VALD
5429.93 | 5429.987 | Fe II | 0.430 | 85462.908 | VALD
5432.85 | 5432.82 | S II | 0.200 | 109831.595 | VALD
5442.36 | 5442.359 | Fe II | -0.310 | 85048.655 | VALD
5443.80 | ? |  |  |  |
5444.25 | 5444.39 | Fe II | -0.170 | 85495.368 | VALD
5445.67 | 5445.80 | Fe II | -0.110 | 85048.655 | VALD
5455.98 | 5455.930 | Fe II | -0.510 | 84527.806 | VALD
5457.70 | 5457.72 | Fe II | -0.140 | 85728.844 | VALD
5465.91 | 5465.932 | Fe II | 0.350 | 85679.757 | VALD
5467.049 | 5466.894 | Si II | -0.080 | 101024.349 | VALD
| 5466.912 | Fe II | -1.870 | 54902.288 | VALD
5473.15 | 5473.15 | Fe II | -1.440 | 86844.832 | VALD
5475.89 | 5475.83 | Fe II | -0.080 | 84685.247 | VALD
5478.32 | 5478.365 | Cr II | -1.970 | 33697.843 | VALD
| 5479.399 | Fe II | -0.350 | 85172.826 | VALD
5479.44 | 5479.40 | Fe II | -0.410 | 87172.810 | VALD
5482.22 | 5482.31 | Fe II | 0.410 | 85184.772 | VALD
5487.53 | 5487.62 | Fe II | 0.290 | 85462.908 | VALD
5492.23 | 5492.078 | Fe II | 0.090 | 85679.757 | VALD
5493.91 | 5493.83 | Fe II | 0.260 | 84685.247 | VALD
5502.95 | ? |  |  |  |
5506.20 | 5506.199 | Fe II | 0.860 | 84863.380 | VALD
5510.87 | 5510.78 | Fe II | 0.100 | 85184.772 | VALD
5529.47 | 5529.47 | Cr II | -2.890 | 97899.412 |
5532.05 | 5532.09 | Fe II | -0.100 | 84870.912 | VALD
5534.83 | 5534.839 | Fe II | -2.900 | 26170.181 | VALD
| 5534.894 | Fe II | -0.440 | 85048.655 | VALD
5544.46 | ? |  |  |  |
5549.01 | 5549.000 | Fe II | -0.190 | 84870.912 | VALD
5554.89 | 5554.910 | Fe II | -0.460 | 85680.279 | VALD
5558.94 | 5559.05 | Mn II | -1.310 | 49885.389 | VALD
5561.30 | 5561.43 | Mn II | -2.420 | 49893.458 | VALD
5567.86 | 5567.84 | Fe II | -1.870 | 54283.234 | VALD
5570.49 | 5570.54 | Mn II | -1.430 | 49820.865 | VALD
5577.96 | 5577.912 | Fe II | -0.110 | 85462.908 | VALD
| 5578.008 | Fe II | -0.620 | 85495.368 | VALD
5586.94 | 5586.842 | Cr II | 0.930 | 88003.158 | VALD
5588.21 | 5588.221 | Fe II | 0.160 | 85462.908 | VALD
5606.14 | 5606.15 | S II | 0.120 | 110766.562 | VALD
5645.47 | 5645.39 | Fe II | 0.190 | 85184.772 | VALD
5648.830 | 5648.90 | Fe II | -0.170 | 85184.772 | VALD
5651.40 | 5651.52 | Fe II | -0.610 | 85728.844 | VALD
5660.15 | 5659.99 | S II | -0.220 | 110313.403 | VALD
5726.59 | 5726.55 | Fe II | -0.040 | 86416.369 | VALD
5780.09 | 5780.13 | Fe II | 0.420 | 86124.348 | VALD
5783.75 | 5783.62 | Fe II | 0.370 | 86416.369 | VALD
5811.73 | 5811.634 | Fe II | -0.610 | 86124.348 | VALD
| 5811.79 | Fe II | -0.640 | 86124.299 | VALD
5813.59 | 5813.67 | Fe II | -2.700 | 44929.533 | VALD
5842.19 | 5842.29 | Fe II | -0.330 | 86599.791 | VALD
5852.44 | 5852.49 | Ne I | -0.450 | 135888.715 | VALD
5854.12 | 5854.19 | Fe II | -0.110 | 86599.791 | VALD
5871.67 | 5871.80 | Fe II | -0.640 | 86124.299 | VALD
5875.75 | 5875.599 | He I | -1.510 | 169086.769 | hfs
| 5875.614 | He I | -0.340 | 169086.769 |
| 5875.615 | He I | 0.410 | 169086.769 |
| 5875.615 | He I | -0.340 | 169086.845 |
| 5875.640 | He I | 0.140 | 169086.845 |
| 5875.966 | He I | -0.210 | 169087.834 |
5902.95 | 5902.83 | Fe II | 0.420 | 86416.331 | VALD
5961.68 | 5961.71 | Fe II | 0.700 | 86124.299 | VALD
5978.85 | 5978.93 | Si II | 0.000 | 81251.320 | VALD
6096.19 | 6096.16 | Ne I | -0.300 | 134459.290 | VALD
6122.48 | 6122.45 | Mn II | 0.950 | 82136.483 | VALD
6143.04 | 6143.06 | Ne I | -0.100 | 134041.838 | VALD
6147.65 | 6147.74 | Fe II | -2.800 | 31364.454 | VALD
6149.28 | 6149.26 | Fe II | -2.800 | 31368.453 | VALD
6156.57 | 6155.961 | O I | -1.360 | 86625.757 | hfs
| 6155.980 | O I | -1.010 | 86625.757 |
| 6155.989 | O I | -1.120 | 86625.757 |
| 6156.737 | O I | -1.490 | 86627.777 |
| 6156.755 | O I | -0.900 | 86627.777 |
| 6156.770 | O I | -0.690 | 86627.777 |
6158.14 | 6158.172 | O I | -1.000 | 86631.453 | hfs
| 6158.180 | O I | -0.410 | 89511.404 |
6163.69 | 6163.59 | Fe II | -3.170 | 50157.455 | VALD
6175.13 | 6175.14 | Fe II | -2.090 | 50187.824 | VALD
6238.32 | 6238.39 | Fe II | -2.800 | 31364.454 | VALD
6239.65 | 6239.610 | Si II | 0.180 | 103556.025 | VALD
| 6239.660 | Si II | 0.020 | 103556.156 | VALD
6247.47 | 6247.56 | Fe II | -2.400 | 31387.979 | VALD
6334.33 | 6334.43 | Ne I | -0.310 | 134041.838 | VALD
6347.00 | 6346.737 | Mg II | 0.030 | 93310.590 | VALD
| 6346.962 | Mg II | -0.130 | 93311.112 | VALD
| 6347.100 | Si II | 0.150 | 65500.472 | VALD
6357.19 | 6357.16 | Fe II | 0.240 | 87985.668 | VALD
6371.23 | 6371.36 | Si II | -0.080 | 65500.472 | VALD
6383.22 | ? |  |  |  |
6402.19 | 6402.25 | Ne I | 0.350 | 134041.838 | VALD
6416.84 | 6416.92 | Fe II | -2.900 | 31387.979 | VALD
6432.67 | 6432.68 | Fe II | -3.500 | 23317.635 | VALD
| 6432.68 | Fe II | -3.710 | 23317.632 | VALD
6456.22 | 6456.38 | Fe II | -2.200 | 31483.198 | VALD
6506.56 | 6506.53 | Ne I | 0.030 | 134459.290 | VALD
6577.99 | 6578.05 | C II | 0.120 | 116537.649 | VALD
6582.92 | 6582.88 | C II | -0.180 | 116537.649 | VALD
6678.10 | 6678.15 | He I | 0.329 | 171134.897 | VALD