Abundance analysis of the supergiant stars HD 80057 and HD 80404 based on their UVES Spectra
aa r X i v : . [ a s t r o - ph . S R ] D ec Abundance analysis of the supergiant stars HD 80057 andHD 80404 based on their UVES Spectra
T. Tanrıverdi a, ∗ , ¨O. Bas¸t¨urk b a Ni˘gde University, Faculty of Arts and Sciences, Department of Physics, TR-51240, Ni˘gde, Turkey b Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100,Tando˘gan, Ankara, Turkey
Abstract
This study presents elemental abundances of the early A-type supergiant HD 80057and the late A-type supergiant HD 80404. High resolution and high signal-to-noise ra-tio spectra published by the UVES Paranal Observatory Project (Bagnulo et al., 2003) were analysed to compute their elemental abundances using ATLAS9 (Kurucz, 1993,2005; Sbordone et al., 2004). In our analysis we assumed local thermodynamic equilib-rium. The atmospheric parameters of HD 80057 used in this study are from Firnstein & Przybilla(2012), and that of HD 80404 are derived from spectral energy distribution, ionizationequilibria of Cr i/ii and Fe i/ii , and the fits to the wings of Balmer lines and Paschenlines as T e ff = ±
150 K and log g = ± ± ± − . The rotational velocities are 15 ± ± − and their macroturbulencevelocities are 24 ± ± − . We have given the abundances of 27 ions of 20elements for HD 80057 and 39 ions of 25 elements for HD 80404. The abundances areclose to solar values, except for some elements (Na, Sc, Ti, V, Ba, and Sr). We havefound the metallicities [M / H] for HD 80057 and HD 80404 as -0.15 ± ± ∗ e-mail: [email protected] Based on data obtained with the UVES Paranal Observatory Project (ESO DDT Program ID 266.D-5655)
Preprint submitted to New Astronomy June 4, 2018 itrogen-to-carbon ( N / C ) and nitrogen-to-oxygen ( N / O ) ratios show that they are intheir blue supergiant phase before the red supergiant region. Keywords:
Stars: abundances - Stars: individual: HD 80057 - Stars: individual: HD 80404 -Techniques: spectroscopic
1. Introduction
A-type supergiants are attractive astrophysical targets for chemical abundance stud-ies. First of all, they are among the brightest stars at visual wavelengths, which makesthem observable with low exposure times, high resolution and high signal-to-noiseratios (S / N). Moreover, their spectra are unblended, hence the abundances of numer-ous elements with consecutive ionization levels such as light elements, α process el-ements, iron group and s-process elements can be derived from studies of their at-mospheres (Venn, 1995; Albayrak, 2000; Przybilla, 2002; Schiller & Przybilla, 2008;Firnstein & Przybilla, 2012; Tanrıverdi, 2013). With these results in hand, it is possibleto understand their nature and the environments in which they exist, and thereby studygalactic and extra-galactic abundance gradients and dispersions.This paper is a continuation of analyses of early and late A-type supergiants startedby Tanriverdi et al. (2004); Tanrıverdi (2013). In this study, elemental abundance anal-yses of two A-type supergiants, HD 80057 and HD 80404 ( iota Car), and their revisedatmospheric parameters, are presented in detail. These analyses are based on spectradistributed by the UVES Paranal Observatory Project (Bagnulo et al., 2003).
HD 80057 (HR 3688, HIP 45481, SAO 221010) was classified as A1 Iab by (Firnstein & Przybilla,2012) (see Table 1 for more information). It is a member of the Vela OB1 association ofstars, which is one of the largest OB star associations of the Galaxy, and is composed ofnumerous members (Reed, 2000). Although HD 80057 has been used as a photometric2tandard star, (Menzies et al., 1989; Cousins, 1990), and as a spectroscopic standardstar for its radial velocities (Reed & Kuhna, 1997; Gontcharov, 2006), a detailed studyof its atmosphere was published only very recently by Firnstein & Przybilla (2012).The authors determined the atmospheric parameters ( T e ff and log g ) using spectro-scopic indicators and spectroscopic data (see Table 2) in their study, as well as CNOabundances of HD 80057 computed using non-LTE methods. Car (HD 80404, HR 3699, HIP 45556, SAO 236808) is an MK Standard, whichis classified as A8 Ib (Malaroda, 1973; Monier & Parthasarathy, 1999) (see Table 1 formore information). It is one of the brightest stars in the southern sky in the visual regionof the electromagnetic spectrum. Adelman et al. (2000) listed it amongst the least vari-able Hipparcos targets, while Gray & Garrison (1989) gave its Str¨omgren photometricparameters.The atmosphere of iota
Car was first studied in detail by Boiarchuk & Liubimkov(1984), who gave its spectroscopic parameters as 7300 ±
200 K for its e ff ective tem-perature and 1.40 ± T e ff = ±
200 K, log g = ± ± − , respectively. Next, Luck & Lambert (1992) adopted the e ff ective tem-perature found by Luck & Lambert (1985) as 7500 K, and found a value of 1.6 ± MARCS code of Gustafsson et al. (1975) from its FeI / II ionization balance. Then, Takeda & Takada-Hidai (1995) re-calculated the CNOabundances of iota
Car using Luck & Lambert (1985)’s atmospheric parameters andequivalent widths (EW).Smiljanic et al. (2006), on the other hand, computed the e ff ective temperature tobe 7500 ±
200 K, surface gravity 2.40 ± ± − based on their high-resolution spectroscopic observations using fits to the H α i/ii ionization equilibrium and their photometric calibration (see Table 2).They also determined its C, N, O, and Fe abundances from their FEROS (Fiber-fedExtended Range Optical Spectrograph) spectra in the wavelength range 3500-9200 Åand a resolution, R =
2. The Spectra
The UVES spectra used in this study were obtained from the UVES-POP database.They have high resolution (R ∼ / N ratios (for most of the spectra S / N ratio ∼ λλ . The ultraviolet (UV), visual and infrared (IR) parts of UVES spectra were usedto determine the abundances of elements such as C, N, O, Mg and Al (see Table 3). Allspectra were continuum normalized using IRAF task continuum . Then, the EWs ofthe identified lines were measured using the splot package within IRAF. Main sourcesfor line identification are mentioned in Tanrıverdi (2013). International UltravioletExplorer (IUE)’s flux-calibrated spectra were downloaded from MAST archive. Forspectrophotometry of HD 80404, low-dispersion and large aperture spectra, SWP36720 and
LWP15980 , were used.
3. Stellar Parameters
The atmospheric models were produced using
ATLAS9 (Kurucz, 1993; Sbordone et al.,2004). LTE abundance analyses were performed based on EW measurements usingthe
WIDTH9 code(Kurucz, 1993). The e ff ective temperatures and surface gravities ( T e ff , http: // / sci / observing / tools / uvespop.html IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Asso-ciation of Universities for Research in Astronomy (AURA) under cooperative agreement with the NationalScience Foundation. http: // archive.stsci.edu g ) were determined via SED (Spectral Energy Distribution, see Fig. 1) analyses, fitsto Balmer and Paschen lines wings (see Figs. 2 & 3) and from the ionization equilibriaof Cr i/ii and Fe i/ii (see Fig. 4). The procedure used to determine these fundamentalparameters are illustrated on the T e ff – log g plane in Fig. 4. The microturbulent ve-locity was determined by finding the value where the correlation between the derivedabundances and the EWs ( ξ ) was minimised, and the minimum scatter about the abun-dance mean ( ξ ) was obtained (Blackwell et al., 1982). Microturbulent velocities weredetermined for HD 80057 and HD 80404 to be 4.30 and 2.20 km s − , respectively.The derived microturbulent velocities of di ff erent species are given in Table 4. Therotational velocity and the macroturbulent velocity of HD 80057 are determined usingsynthetic spectra produced by SYNSPEC and
SYNPLOT (Hubeny, 1988; Hubeny & Lanz,2011). The rotational and macroturbulence velocities for HD 80057 are 15 ± − and 24 ± − and those for HD 80404 are 7 ± − and 2 ± − .The SED in Fig. 1 was reproduced using ATLAS9 flux models. The spectropho-tometric data were obtained from Ruban et al. (2006). The photometric data, angulardiameter and E(B-V) are given in Table 1. The zero-points reported by Heber et al.(2002) were used to transform the various magnitudes into monochromatic fluxes. Itwas assumed that y = V to transform b-y, c and m indexes to u, v, b and y magnitudes.The computed fluxes of HD 80404 ( T e ff = g = δ increasing and decreasing ±
150 K or ± T e ff , and log g , respectively using SYNTHE (Kurucz & Avrett,1981). We also used the bluest part of the Balmer series. Di ff erent to the syntheticBalmer series spectrum, we also tried to determine the T e ff , log g pair of the Paschenseries, for which we obtained a good fit. Paschen lines were previously used bySchiller & Przybilla (2008) to determine the atmospheric parameters of Deneb. The ex-citation potentials of Fe i and Fe ii lines in our abundance analysis ranged from 0.00 eVto 10 eV. Their abundances and excitation potentials showed no correlation at T e ff = × − ± × − dex − . This is another method to determine the atmosphericparameters, such as T e ff . Moreover, the ionization equilibrium is also good tool to de-termine the stellar parameters. Ionization equilibrium for the consecutive ionizationstages of Cr i/ii and Fe i/ii were fullfilled in the atmospheres of HD 80404. The errorsin the determined values of T e ff and log g were assumed to be ±
150 K and ± δ fits, and the error of the microturbulent velocity value wasassumed to be 0.7 km s − , as obtained from microturbulence velocity determinationsof individual elements in Table 4 .
4. The results of the abundance analysis
The elemental abundances found in this study for HD 80057 and HD 80404 arepresented in Table 3 and Fig. 6, together with a comparison of our results with solarcomposition and previous studies. The systematic error calculated for the abundancesof HD 80404 are given in Table 5. The detailed abundances are given in Table 6, whichalso includes the elements used in the analysis, the wavelengths of the identified lines,gf values, and their references. The ionization equilibrium of di ff erent elements / ionsfor target stars are seen in Table 3.While the errors in T e ff have the strongest e ff ect on the abundances of Mg ii , Al i ,Fe i and Ba ii , the error in log g a ff ects most strongly those of Mg ii , S ii , Ca i and Ca ii .This might be due to the fact that these species have the strongest lines with the largeEWs.The sum of CNO abundances of both stars have a solar value. For HD 80057, α -process elements, except for Si and Ca, are also under-abundant. Al, Sc, Ti, and V arefound to be under-abundant. However, Cr, Mn, Fe, and Ni abundances are found to becloser to solar values. Sc, Ti, and V are susceptible to non-LTE e ff ects, which can beascribed to the value of their second ionization potentials. These are the lowest second6onisation potential in the Iron Group (Przybilla, 2002). The heavy elements (Sr, Y, Zr,Ba) are also underabundant with respect to solar abundances.In the atmospheres of HD 80404; α -process elements (Si, S and Ca) and the lightelement Al are closer to solar values, Mg is deficient, however Na is overabundant.Sc, Ti, V, Cr, Mn, Fe, Co and Ni are all closer to solar values in the atmosphere ofHD 80404. The heavy elements tend to have values slightly smaller than solar, Ba isoverabundant (see Fig. 1).
5. Results and Discussion
As a result, the [M / H] ratio of HD 80057 is found to be -0.15 ± , 0.24 dex whenwe exclude the over-abundant Na due to NLTE e ff ects (Takeda & Takada-Hidai, 1994;Venn, 1995; Takeda, 2008), the under-abundant Sc and Ti, which are all susceptible tonon-LTE e ff ects. The [M / H] ratio of HD 80404 is estimated to be -0.02 ± N / C , N / O and Σ CNO valuesare given in Table 7.
Light-element, the sum of
CNO composition reflects mixing process present in theinterior of the star. Both stars show a deficiency of C and O, and an enrichment of N.Hence, the combined
CNO abundances were found to be close to the solar value (seeTable 7). Both stars also have solar metallicity. The values of N / C and N / O predictedfrom a linear interpolation of the closest isochrones are consistent with their calculatedvalues (see Table 7). The N / O ratio of HD 80057 is found to be slightly smaller thanthe theoretical value 0.52.The early CNO contamination in the surface layers of stars can be explained byrotating models. Rotation is an essential factor of stellar models that have a profounde ff ect on the evolution of especially massive stars. Red giants or supergiants, whoseprogenitor is fast rotating progenitors, rotate six times faster and show N / C ratios three7ime higher than those formed by slow rotators (Przybilla et al., 2010; Georgy et al.,2013; Maeder et al., 2014). Georgy et al. (2013) provide extended data of stellar mod-els including the mass range from 1.7 to 15 M ⊙ with three di ff erent metallicities andwith nine di ff erent initial rotation velocity models. In the framework of their study, onecan see that C, N, and O abundances varies with di ff erent initial rotating models. So,we take into account, initial rotational velocities, N / C and N / O ratios, besides T e ff andlog g in stellar evolution models.In order to investigate the evolutionary states of our targets, we used the GenevaStellar Model (Georgy et al., 2013) interactive tools to interpolate between the exist-ing evolutionary tracks that would lead to models with parameters matching those ofour targets. We used the relevant parameters (log T e f f and log g ) from Firnstein & Przybilla(2012) for HD 80057 and our own measurements for HD 80404.We experimented by interpolating models for di ff erent masses of grids that cov-ered a wide range of masses between 1.7 and 15 M ⊙ . We kept the metallicity at solarcomposition (Z = / crit = ff ective temper-atures and surface gravities). We found that both of our stars have masses between10 M ⊙ and 14 M ⊙ . While HD 80057 has a mass consistent with the track for 13 M ⊙ ,HD 80404 is very close to the track for 12 M ⊙ . The latter result is based on its funda-mental parameters (Fig. 7), which assumes solar composition and rotation with valuesof Ω / Ω crit = T e ff - log g plane, we also computed isochrones using the same onlinetools and selected the ones to which our stars’ parameters had the closest matches http: // / Recherche / evoldb / index / N / C that we computedin this study (2.45 for HD 80057 and 1.57 for HD 80404) are somewhat consistent(within the uncertainty limits) with the stars’ positions on the log T e ff – log g plane,for which the expected N / C ratios are printed next to each of the isochrones in Fig.8.The derived values of the N / C and N / O ratios from the isochrones are given in Table 7.These ratios reveal that CNO mixing processes are active, and that these stars are atthe Blue Supergiant (BSG) phase in their evolution prior to the Red Supergiant (RSG)phase, as according to Saio et al. (2013).
6. Acknowledgements
This research utilised the SIMBAD database, which is operated at CDS, Strasbourg,France. This work, made use of the MAST-IUE archive (http: // archive.stsci.edu / iue / ) ofSAO / NASA ADS, is based on data obtained from UVES Paranal Observatory Project(ESO DDT Program ID 266.D-5655), of the VALD database, operated at Uppsala Uni-versity, the Institute of Astronomy RAS in Moscow, and the University of Vienna.Atomic data compiled in the DREAM data base (E. Biemont, P. Palmeri & P. Quinet,Astrophys. Space Sci. 269-270, 635, 1999) were extracted via VALD (Kupka et al.,1999, A&AS 138, 119, and references therein). The authors thank the anonymousreferee, whose useful comments helped to improve this work.
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Figure 1: A comparison of the observed and computed fluxes ( T e ff = g = N o r m a li ze d − F l ux l ( Å ) H ATLAS9UVES N o r m a li ze d − F l ux l ( Å ) H N o r m a li ze d − F l ux l ( Å ) H e N o r m a li ze d − F l ux l ( Å ) H d N o r m a li ze d − F l ux l ( Å ) H g N o r m a li ze d − F l ux l ( Å ) H b N o r m a li ze d − F l ux l ( Å ) P N o r m a li ze d − F l ux l ( Å ) P Figure 2: Synthetic spectrum fits of Balmer and Paschen series in the UVES spectra of HD 80404 for T e ff = g = N o r m a li ze d − F l ux l ( Å ) − + UVES N o r m a li ze d − F l ux l ( Å ) +
150 K −
150 K UVES
Figure 3: Synthetic spectrum fits of H δ lines in HD 80404 spectra using T e ff = ±
150 K), log g = ± l og g T eff (K) Fe I - IICr I - IIBalmer-linesFe I - IICr I - IIBalmer-linesFe I - IICr I - IIBalmer-linesFe I - IICr I - IIBalmer-linesFe I - IICr I - IIBalmer-linesFe I - IICr I - IIBalmer-lines
Figure 4: T e ff - log g planes for T e ff = g = i/ii , Fe i/ii ionizationlevels and Balmer line fits. −5.6 −5.4 −5.2 −5.0 −4.8 −4.6 −4.4 −4.2 −4.0 −3.8 −3.6−1 0 1 2 3 4 5 6 7 8 9 10 11 12 F e abundan c e s excitation potential(eV) Fe IFe II −5.6 −5.4 −5.2 −5.0 −4.8 −4.6 −4.4 −4.2 −4.0 −3.8 −3.6 0 50 100 150 200 F e abundan c e s equivalent widths(mÅ) Fe IFe II Figure 5: Fe abundances versus their equivalent widths and the di ff erent excitation potential values areplotted. The correlation between excitation potentials and Fe abundances is minimum at T e ff = [ X / H ] Elements HD80057HD80404
Figure 6: The chemical abundances of HD 80057 and HD 80404 compared to the solar values inGrevesse & Sauval (1996). l og g ( c g s ) logT eff (K) HD80404HD80057 12M solar solar
Figure 7: The positions of HD 80057 and HD 80404 on log T e ff log g plane, and evolutionary tracks for 12and 13 M ⊙ , found by interpolation between existing tracks of Geneva stellar models Georgy et al. (2013).We labelled certain N / C values (by mass ratio) on each of the tracks for comparison with our measurements. l og g ( c g s ) logT eff (K) HD80404HD80057
Figure 8: The positions of HD 80057 and HD 80404 on log T e ff - log g plane, and two isochrones (10 . and 10 . years) computed by making use of Geneva stellar models Georgy et al. (2013) in solid curves. Welabelled certain N / C values (by mass ratio) on each of the isochrones for comparison with our measurements. able 1: Stellar parameters of HD 80057 and HD 80404 from other authors. HD 80057 HD 80404
Basic
Name . . . ι CarAssociation Vela OB1 a . . .Spectral type A1-Iab b A8-Ib f Distance ( kpc) 1.449 ± c , b ± c Radial velocity ( km s − ) 25.7 ± d ± d Atmospheric T e ff (K) 9300 ± b ± g log g (cgs) 1.75 ± b ± g ξ ( km s − ) 5 ± b ± g ζ ( km s − ) 27 ± b . . . v sin i ( km s − ) 13 ± b ± d Photometric(Johnson) V m ± m .016 b m h B − V m ± m .006 b m h U − B -0. m ± m .021 b m h (Str¨omgren) b − y ± e ± i m -0.009 ± e ± i c ± e ± i M V -6. m ± m a -5. m j ( m − M ) m ± m a m j M bol -6. m ± m a -5. m k BC -0. m
09 0. m k E ( B − V ) 0. m ± b m j θ D ( mas ) . . . 1. m ± la Reed (2000), b Firnstein & Przybilla (2012), c van Leeuwen (2007), d Gontcharov (2006), e Hauck & Mermilliod (1998), f Tetzla ff et al. (2011), g Smiljanic et al. (2006), h Ducati (2002), i Arellano Ferro & Mantegazza (1996), j Snow et al. (1994) k van der Wal & van Genderen(1988) l Davis et al. (2009) able 2: Atmospheric parameters of HD 80057 and HD 80404 from various sources. Source T e ff (K) log g ξ (km s − ) ζ (km s − ) Spectra MethodHD 80057Firnstein & Przybilla (2012) 9300 ±
150 1.75 ± ± ∼ / N > ±
200 1.40 ± / mm LTE, Kurucz (1979)Luck & Lambert (1985) 7500 0.90 2.5 1 LTE, Fe I / IIionization balanceLuck & Lambert (1992) 7500 1.6 2.2 1 CTIO, R ∼ = H α , and Fe I / II3500-9200 Å, S / N >
150 ionization balance able 3: The comparison of derived abundances of target stars relative to the solar values and literature. Solar HD 80057 HD 80404Species n This Study FP , n This Study n LL , C i -3.45 5 -3.72 ± ± ± ii -3.45 2 -3.78 ± ± i -4.03 1 -3.42 ± ± ± ii -4.03 . . . . . . -3.71 . . . . . . . . . . . .O i -3.13 3 -3.11 ± ± i -5.67 . . . . . . . . . 3 -5.26 ± ± i -4.42 2 -4.78 ± ± ± ii -4.42 5 -4.71 ± ± ± i -5.53 2 -6.08 ± ± ii -5.53 1 -6.03 . . . 1 -5.81 . . . . . .Si i -4.45 . . . . . . . . . 2 -4.16 ± ± ii -4.45 11 -4.57 ± ± i -4.67 . . . . . . . . . 3 -4.63 ± ± ii -4.67 2 -5.04 ± ± i -5.64 1 -5.75 . . . 24 -5.64 ± ± ii -5.64 2 -5.79 ± ± ± ii -8.83 7 -9.34 ± ± ± i -6.98 . . . . . . . . . 40 -6.89 ± ii -6.98 43 -7.49 ± ± i -8.00 . . . . . . . . . 4 -8.05 ± ii -8.00 7 -8.38 ± ± i -6.33 . . . . . . . . . 40 -6.40 ± ii -6.33 50 -6.44 ± ± i -6.61 . . . . . . . . . 25 -6.56 ± ii -6.61 8 -6.78 ± ± i -4.50 25 -4.70 ± ± ± ii -4.50 105 -4.62 ± ± ± iii -4.50 3 -4.69 ± i -7.08 . . . . . . . . . 7 -7.17 ± ii -7.08 1 -7.15 . . . 5 -6.95 ± i -5.75 . . . . . . . . . 17 -5.73 ± ii -5.75 3 -5.99 ± ± i -7.40 . . . . . . . . . 2 -7.61 ± ii -9.03 2 -9.77 ± ± ii -9.76 . . . . . . . . . 15 -9.90 ± ± ii -9.40 3 -9.62 ± ± ii -9.87 1 -10.11 . . . 4 -9.54 ± ± ii -10.83 . . . . . . . . . 12 -10.77 ± ii -10.42 . . . . . . . . . 9 -10.32 ± ii -11.49 . . . . . . . . . 4 -11.74 ± ± T e ff ( K) . . . 9300 . . . 7700log g (cgs) . . . 1.75 . . . 1.601. Grevesse & Sauval (1996), 2. Firnstein & Przybilla (2012),3. Grevesse & Sauval (1998), 4. Luck & Lambert (1992), 5. Grevesse (1984) able 4: Microturbulence determinations from various elements / ions Element n ξ (scatter) log (N / N T ) ξ (slope) log (N / N T ) Referencekm s − km s − HD 80057Fe II 105 4.3 -4.62 ± ± + N4avg 4.4 + VALDstdev 0.1 HD 80404C I 13 4.1 -3.71 ± ± ± ± + WSadopted 2.2Fe I 152 2.0 -4.56 ± ± + N4adopted 2.0 + VALDFe II 139 2.3 -4.63 ± ± + N4adopted 2.4 + VALDCr I 40 1.7 -6.36 ± ± ± ± + KXadopted 2.0 + NLSr II 4 1.8 -9.02 ± ± + WMadopted 1.9Y II 15 1.7 -9.77 ± ± ± ± + BGadopted 1.7avg 2.2stdev 0.7References of gf-values:B = Brage et al. (1998) ; BG = Biemont et al. (1981);HL = Hannaford et al. (1982);FW = Fuhr & Wiese (2002) and Fuhr et al. (1988);KX = Kurucz (1995), LN = Ljung et al. (2006);NL = Nilsson et al. (2006), N4 = Fuhr & Wiese (2006),MF = Fuhr et al. (1988) and Martin et al. (1988);WF = Wiese et al. (1996); WM = Wiese & Martin (1980), WS = Wiese et al. (1969);VALD,VALD2 data = Piskunov et al. (1995), Ryabchikova et al. (1997),Kupka et al. (1999), Kupka et al. (2000); able 5: Error reasons for the abundances of HD 80404 Species σ ( T e ff ) ∆ (log g ) ∆ ( ξ ) EW σ TOTAL ( + + + − ) (10%EW) C I 0.06 -0.04 -0.02 0.07 0.10N I 0.06 0.01 0.04 0.08 0.08O I 0.00 0.01 -0.02 0.04 0.04Na I 0.11 -0.07 -0.03 0.06 0.14Mg I 0.13 -0.08 -0.14 0.02 0.20Mg II 0.00 0.02 -0.09 0.03 0.10Al I 0.15 -0.07 -0.31 -0.13 0.37Al II -0.05 0.07 -0.02 0.03 0.09Si I 0.12 -0.07 -0.01 0.04 0.15Si II -0.02 0.04 -0.10 0.01 0.11S I 0.11 -0.07 -0.01 0.05 0.14S II -0.10 0.18 -0.02 0.06 0.19Ca I 0.17 -0.10 -0.05 0.07 0.22Ca II 0.06 -0.10 -0.07 0.08 0.12Sc II 0.10 -0.01 -0.14 0.12 0.21Ti I 0.16 -0.08 -0.01 0.00 0.19Ti II 0.10 0.02 -0.16 0.16 0.25V I 0.16 -0.08 -0.01 0.04 0.18V II 0.08 0.00 -0.09 0.09 0.15Cr I 0.16 -0.07 -0.04 0.04 0.19Cr II 0.05 0.01 -0.11 0.10 0.16Mn I 0.14 -0.08 -0.05 0.07 0.18Mn II 0.03 0.01 -0.03 0.05 0.07Fe I 0.15 -0.09 -0.13 0.13 0.25Fe II 0.06 0.06 -0.05 0.13 0.16Co I 0.17 -0.07 -0.03 0.06 0.20Co II 0.02 -0.04 -0.17 0.06 0.19Ni I 0.13 -0.08 -0.02 0.05 0.16Ni II 0.04 0.02 -0.04 0.07 0.09Zn I 0.14 -0.07 0.00 0.05 0.16Sr II 0.17 -0.04 -0.33 0.18 0.41Y II 0.04 -0.01 -0.10 0.10 0.15Zr II 0.03 0.00 0.06 0.08 0.10Ba II -0.08 0.12 -0.30 0.19 0.38La II 0.14 -0.04 -0.03 0.06 0.16Ce II 0.13 -0.03 -0.02 0.05 0.14Eu II 0.17 -0.04 -0.02 0.05 0.18 σ tot . = σ tef f + σ logg + σ EW + σ ξ able 6: Elemental Abundances of HD 80057 and HD 80404 HD 80057 HD 80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T C I log C / N T = -3.72 ± ± / N T = -3.78 ± + / N T = -3.36 ± ± = Aldenius et al. (2007); B = Brage et al. (1998) BB = Blackwell-Whitehead & Bergemann (2007);BG = Biemont et al. (1981), Biemont et al. (1989); CB = Corliss & Bozman (1962);CR = Wiese & Fuhr (2007)DS = Davidson et al. (1992) FW = Fuhr & Wiese (2002) and Fuhr et al. (1988);HL = Hannaford et al. (1982)JK = J¨onsson et al. (1984) KG = Kling & Griesmann (2000); KS = Kling et al. (2001);KX = Kurucz (1995)LA = Lanz & Artru (1985); LB = Lawler et al. (2001) LD = Lawler & Dakin (1989);LN = Ljung et al. (2006)LW = Lawler et al. (2001); MC = Meggers et al. (1975) ;NL = Nilsson et al. (2006)N4 = Fuhr & Wiese (2006); MF = Fuhr et al. (1988) and Martin et al. (1988);RP = Raassen et al. (1998)PT = Pickering et al. (2001);Pickering et al. (2002); PQ = Palmeri et al. (2000);SG = Schulz-Gulde (1969)WF = Wiese et al. (1996); WM = Wiese & Martin (1980); WS = Wiese et al. (1969);VALD,VALD2 data = Piskunov et al. (1995), Ryabchikova et al. (1997), Kupka et al. (1999), Kupka et al. (2000)-The lines marked with * are ignored in average calculations.-This table is given electronically. able 7: The derived abundances and stellar parameters of HD 80057 and HD 80404 based on isochronesand evolutionary tracks of Georgy et al. (2013) for Ω / Ω crit = HD80057 HD80404 Ω / C 2.44 ± ± ± ± / O 0.43 ± ± ± ± Σ CNO ± ± / H -0.15 ± ± crit ± ± vsini ± ± R / R ⊙ ± ± M spec / M ⊙ ± ± M ZAMS / M ⊙ ± ± M evol / M ⊙ ± ± L / L ⊙ ± ± able A1: Elemental Abundances of HD 80057 and HD 80404 HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T C i log C / N T = -3.72 ± ± i log C / N T = -3.78 ± + / N T = -3.36 ± ± / N T = -3.11 ± ± / N T = -4.56 ± ± / N T = -4.68 ± / N T = -4.71 ± ± / N T = -6.08 ± ± / N T = -6.03 -5.812 4663.10 -0.28 FW 31.0 -6.03 16.0 -5.81Si I log Si / N T = ... -4.21 ± / N T = -4.57 ± ± A29 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Si II (continued) / N T = ... -4.63 ± / N T = -5.04 ± ± / N T = -5.75 -5.64 ± + / N T = -5.79 ± ± / N T = -9.34 ± ± + A30 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Ti I log Ti / N T = ... -7.53 ± + + + + + + + + / N T = -7.49 ± ± A31 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Ti II (continued)
60 4568.31 -2.94 PT ... ... 42.8 -7.084580.45 -2.94 PT 3.2 -7.11 33.9 -7.214600.26 -3.54 VALD2 ... ... ... ...61 4391.03 -2.28 PT 5.9 -7.49 100.2 -6.894411.93 -2.52 PT 3.2 -7.52 58.0. -7.274423.24 -2.67 KX ... ... ... ...60 5154.07 -1.75 PT ... ... 97.1 -7.305188.68 -1.05 PT ... ... 130.2 -7.465226.54 -1.26 PT ... ... 163.6 -6.6972 3757.68 -0.42 PT 83.3 -7.69 146.5 -7.303776.05 -1.25 PT 18.8 -7.71 ... ...82 4529.48 -1.64 PT 19.9 -7.36 106.7 -7.194571.97 -0.32 PT 108.7 -7.65 ... ...86 5129.14 -1.24 PT ... ... 116.1 -7.265131.28 -3.02 VALD ... ... 18.2 -7.005185.90 -1.49 PT ... ... 104.9 -7.1987 4028.34 -0.96 PT 41.5 -7.43 127.4 -7.084053.83 -1.13 PT ... ... 140.5 -6.6392 4779.99 -1.26 VALD2 27.8 -7.29 111.5 -7.144805.09 -0.96 VALD2 26.3 -7.61 144.8 -6.8493 4374.83 -1.61 PT ... ... 112.3 -6.704421.95 -1.66 PT ... ... 78.3 -7.2194 4316.80 -1.58 PT ... ... 78.3 -7.294350.80 -1.74 PT ... ... 63.8 -7.32101 7214.78 -1.74 VALD ... ... 44.7 -7.267355.46 -1.92 VALD ... ... 37.5 -7.19104 4367.66 -0.86 PT ... ... 114.0 -7.014386.84 -0.96 PT ... ... 92.0 -7.29105 4163.64 -0.13 PT 58.0 -7.63 149.7 -6.964171.90 -0.29 PT 53.2 -7.52 153.2 -6.724174.05 -1.26 PT 13.7 -7.25 67.5 -7.32106 4064.35 -1.60 PT 4.5 -7.40 43.3 -7.32113 5010.21 -1.29 PT ... ... 44.5 -7.315013.68 -1.91 PT ... ... 80.1 -7.365069.09 -1.82 PT ... ... 33.3 -6.945072.28 -1.06 PT ... ... 69.4 -7.17114 4874.01 -0.80 PT 11.4 -7.52 ... ...4911.18 -0.61 PT 18.4 -7.47 90.4 -7.32115 4411.07 -0.67 PT 18.4 -7.40 86.0 -7.304488.34 -0.51 PT 23.5 -7.43 105.9 -7.12V I log V / N T = ... -8.05 ± / N T = -8.38 ± ± / N T = ... -6.40 ± + + A32 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Cr I (continued) log Cr / N T = ... -6.40 ± / N T = -6.45 ± ± A33 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Cr II (continued) log Cr / N T = -6.46 ± ± / N T = ... -6.56 ± / N T = -6.78 ± ± / N T = -4.59 ± ± A34 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Fe I (continued)
16 5041.07 -3.09 VALD ... ... 69.6 -4.705051.63 -2.80 N4 ... ... 44.1 -4.445079.73 -3.22 N4 ... ... 24.5 -4.3120 3840.44 -0.51 N4 24.7 -4.94 132.7 -4.8722 3850.82 -1.73 N4 5.4 -4.44 87.2 -4.6542 4147.63 -2.10 N4 ... ... 46.0 -4.604202.02 -0.71 N4 14.3 -4.74 ... ...42 4250.79 -0.71 N4 14.5 -4.69 113.5 -4.714271.76 -0.16 N4 31.8 -4.89 136.5 -5.054307.90 -0.07 N4 ... ... 138.8 -4.934325.75 -0.01 N4 ... ... 136.8 -4.9943 4005.25 -0.61 N4 11.4 -4.88 119.5 -4.5554063.60 + + A35 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Fe I (continued)
522 4199.10 + + / N T = -4.61 ± ± A36 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Fe II (continued)
32 4439.13 -5.50 VALD ... ... 6.2 -4.5036 4993.35 -3.68 N4 38.5 -4.78 ... ...37 4472.92 -3.53 N4 58.3 -4.66 82.1 -4.754489.18 -2.97 N4 122.8 -4.58 ... ...4491.40 -2.64 N4 152.0 -4.58 ... ...4515.34 -2.36 N4 ... ... 167.8 -4.214520.23 -2.62 N4 109.3 -5.15 148.1 -4.4337 4555.89 -2.25 N4 ... ... 156.3 -4.654582.84 -3.06 N4 98.2 -4.72 107.1 -4.784629.34 -2.26 N4 182.6 -4.65 157.6 -4.654666.76 -3.33 N4 ... ... 9.88 -4.6938 4508.28 -2.35 N4 ... ... 173.9 -4.314522.63 -1.99 N4 220.1 -4.45 161.8 -4.854541.52 -2.97 N4 110.5 -4.69 121.9 -4.584576.33 -2.92 N4 110.6 -4.74 118.7 -4.714583.83 -1.74 N4 220.4 -4.73 ... ...4595.68 -4.58 VALD 4.8 -4.85 28.6 -4.894620.51 -3.19 N4 ... ... 105.7 -4.6139 4088.76 -4.68 VALD 4.3 -4.79 20.0 -4.514138.40 -4.32 VALD ... ... 42.3 -4.4241 5256.93 -4.18 VALD ... ... 52.3 -4.655284.10 -3.20 N4 ... ... 111.5 -4.6743 4656.97 -3.57 N4 48.4 -4.71 90.7 -4.564731.44 -3.13 N4 76.3 -4.85 112.6 -4.6044 4663.70 -3.89 VALD ... ... 66.9 -4.6548 5264.81 -3.32 N4 ... ... 97.2 -4.525316.78 -2.78 N4 ... ... 148.5 -4.215362.87 -2.62 VALD ... ... 158.3 -4.305414.07 -3.65 VALD ... ... 62.9 -4.7349 5197.57 -2.05 N4 187.9 -4.63 177.9 -4.435234.62 -2.21 N4 ... ... 155.3 -4.625276.00 -1.90 N4 ... ... 189.9 -4.465316.61 -1.85 N4 ... ... 173.7 -4.775425.25 -3.39 N4 ... ... 9.18 -4.56126 4032.94 -2.57 VALD 47.0 -4.79 68.5 -4.564046.81 -4.37 VALD ... ... 7.4 -4.53127 4024.55 -2.44 N4 90.3 -4.43 76.0 -4.69141 4147.27 -3.79 VALD 5.3 -4.58 ... ...150 4138.21 -3.47 VALD 15.2 -4.35 21.6 -4.76151 4031.41 -3.16 VALD ... ... 28.1 -4.67152 3863.38 -3.51 VALD 20.9 -4.15 ... ...153 3827.08 -2.36 N4 67.7 -4.61 ... ...167 5127.86 -2.45 VALD ... ... 33.6 -4.555160.83 -2.56 VALD ... ... 33.9 -4.44169 4760.15 -3.64 VALD ... ... 2.9 -4.764810.74 -3.29 VALD ... ... 8.4 -4.60171 4474.19 -3.37 VALD 7.1 -4.33 9.7 -4.63172 4041.64 -3.38 VALD 5.1 -4.48 16.0 -4.394044.01 -2.67 VALD 21.1 -4.52 ... ...4048.83 -2.38 VALD 41.5 -4.45 ... ...173 3906.04 -1.70 N4 81.9 -4.64 ... ...186 4625.91 -2.55 VALD 15.0 -4.59 ... ...4635.33 -1.58 N4 70.3 -4.66 ... ...187 4446.25 -2.78 VALD 7.2 -4.70 12.1 -4.96188 4111.90 -2.67 VALD 13.3 -4.54 ... ...190 3938.97 -1.93 N4 55.7 -4.52 ... ...205 5074.05 -2.17 VALD ... ... 9.1 -4.96212 3960.90 -1.56 VALD 28.4 -4.56 ... ...213 4354.34 -1.35 VALD 15.8 -4.85 24.2 -4.514507.10 -1.76 VALD 7.9 -4.63 ... ...219 4598.53 -1.54 VALD 13.1 -4.65 ... ...4625.55 -2.13 VALD 3.7 -4.60 ... ...4318.19 -1.88 VALD ... ... 5.7 -4.594319.68 -1.64 VALD 16.8 -4.43 10.4 -4.564321.31 -1.74 VALD 11.0 -4.52 7.3 -4.65221 5081.90 -1.06 VALD ... ... 2.0 -4.75222 4431.64 -1.79 VALD ... ... 8.2 -4.524449.66 -1.70 VALD 6.2 -4.89 10.5 -4.59D 3844.79 -1.02 VALD 8.3 -4.77 ... ...3894.63 -2.08 VALD 4.0 -4.82 13.1 -4.273898.62 -1.71 VALD 12.8 -4.66 13.1 -4.653922.04 -1.07 VALD 5.5 -4.87 5.9 -4.973926.68 -2.50 VALD ... ... 5.5 -4.284202.52 -2.36 VALD 11.2 -4.46 8.0 -4.694319.42 -1.99 VALD ... ... 6.5 -4.484384.08 -2.58 VALD ... ... 21.6 -4.344418.98 -1.85 VALD ... ... 7.1 -4.514467.97 -2.50 VALD ... ... 3.3 -4.374487.50 -2.14 VALD ... ... 6.5 -4.414563.15 -2.39 VALD ... ... 2.2 -4.45G 3924.83 -1.10 VALD ... ... 2.3 -4.844213.52 -1.84 VALD ... ... 8.9 -4.184377.34 -2.93 VALD ... ... 3.2 -4.53J 4263.87 -1.69 VALD 17.5 -4.44 17.3 -4.404357.58 -2.01 VALD 39.7 -4.55 33.8 -4.744361.25 -2.26 VALD 17.2 -4.72 ...4402.87 -2.56 VALD ... ... 23.2 -4.38
A37 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Fe II (continued)
J 4451.55 -1.91 VALD ... ... 57.1 -4.424455.27 -2.00 VALD ... ... 43.4 -4.494480.68 -2.56 VALD ... ... 19.6 -4.414579.53 -2.34 VALD 22.5 -4.45 ... ...4640.84 -1.74 VALD 6.7 -4.82 ... ...4820.85 -0.72 VALD 7.0 -4.46 ... ...4824.84 -2.17 VALD 4.8 -4.57 2.2 -4.554836.95 -2.24 VALD ... ... 4.5 -4.144843.21 -2.48 VALD 6.3 -4.48 6.3 -4.134845.36 -2.38 VALD 3.9 -4.44 ... ...4883.28 -0.60 VALD 10.7 -4.36 2.9 -4.684893.82 -4.27 N4 9.4 -4.87 43.2 -4.484908.15 -0.27 VALD 9.9 -4.70 5.7 -4.654913.29 + + + + + + + + + + / N T = -4.69 ± ± / N T = -7.16 -6.95 ± / N T = ... -5.73 ± + A38 able A1: - continued
HD80057 HD80404Species Multiplet λ (Å) log gf Ref. W λ (mÅ) log N / N T W λ (mÅ) log N / N T Ni I (continued)
117 3908.91 -0.57 KX ... ... 10.1 -5.73130 4855.40 0.00 FW ... ... 25.7 -5.95131 4829.01 -0.33 FW ... ... 21.6 -5.71132 4752.43 -0.70 FW ... ... 9.1 -5.684913.96 -0.63 FW ... ... 9.6 -5.65163 4806.97 -0.64 FW ... ... 12.9 -5.57163 4546.92 -0.27 KX ... ... 13.1 -5.55Ni II log Ni / N T = -5.99 ± ± / N T = ... -7.61 ± / N T = -9.77 ± ± + / N T = ... -9.90 ± + + / N T = -9.62 ± ± / N T = -10.11 -9.54 ± + / N T = ... -10.77 ± + + + + + / N T = ... -10.32 ± A39 able A1: - continued