HD 80606: Searching the chemical signature of planet formationThe data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. 1footnote 11footnote 1Reduced spectra of HD 80606 and HD 80607 (FITS files) are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/

HD 80606: Searching the chemical signature of planet formationthanks: The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. 111Reduced spectra of HD 80606 and HD 80607 (FITS files) are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/

C. Saffe Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), C.C 467, 5400, San Juan, Argentina. csaffe,mflores@icate-conicet.gob.ar Universidad Nacional de San Juan (UNSJ), Facultad de Ciencias Exactas, Físicas y Naturales (FCEFN), San Juan, Argentina.    M. Flores Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), C.C 467, 5400, San Juan, Argentina. csaffe,mflores@icate-conicet.gob.ar    A. Buccino Instituto de Astronomía y Física del Espacio (IAFE-CONICET), Buenos Aires, Argentina. abuccino@iafe.uba.ar Departamento de Física, Facultad de Ciencias Exactas y Naturales (FCEN), Universidad de Buenos Aires (UBA), Buenos Aires, Argentina.
Received xxx, xxx ; accepted xxxx, xxxx
Key Words.:
Stars: abundances – Stars: planetary systems – Stars: binaries – Stars: individual: HD 80606, HD 80607
Abstract

Context:Binary systems with similar components are ideal laboratories which allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process.

Aims:We explore the probable chemical signature of planet formation in the remarkable binary system HD 80606 - HD 80607. The star HD 80606 hosts a giant planet with 4 M detected by both transit and radial velocity techniques, being one of the most eccentric planets detected to date. We study condensation temperature T trends of volatile and refractory element abundances to determine whether there is a depletion of refractories that could be related to the terrestrial planet formation.

Methods:We carried out a high-precision abundance determination in both components of the binary system, using a line-by-line strictly differential approach, using the Sun as a reference and then using HD 80606 as reference. The stellar parameters T, log g, [Fe/H] and v were determined by imposing differential ionization and excitation equilibrium of Fe I and Fe II lines, using an updated version of the program FUNDPAR, together with 1D LTE ATLAS9 model atmospheres and the MOOG code. Then, we derived detailed abundances of 24 different species using equivalent widths and spectral synthesis with the program MOOG. The chemical patterns were compared with the solar-twins T trends of Meléndez et al. (2009) and with a sample of solar-analog stars with [Fe/H]+0.2 dex from Neves et al. (2009). The T trends were also compared mutually between both stars of the binary system.

Results:From the study of T trends, we concluded that the stars HD 80606 and HD 80607 do not seem to be depleted in refractory elements, which is different for the case of the Sun. Then, following the interpretation of Meléndez et al. (2009), the terrestrial planet formation would have been less efficient in the components of this binary system than in the Sun. The lack of a trend for refractory elements with T between both stars implies that the presence of a giant planet do not neccesarily imprint a chemical signature in their host stars, similar to the recent result of Liu et al. (2014). This is also in agreement with Meléndez et al. (2009), who suggest that the presence of close-in giant planets might prevent the formation of terrestrial planets. Finally, we speculate about a possible (ejected or non-detected) planet around the star HD 80607.

Conclusions:

1 Introduction

Main-sequence stars with giant planets are, on average, metal-rich compared to stars without planetary mass companions (e.g. Santos et al., 2004, 2005; Fischer & Valenti, 2005). On the other hand, Neptune-like or super-Earth planets do not seem to be formed preferentially around metal-rich stars (e.g. Udry et al., 2006; Sousa et al., 2008). Meléndez et al. (2009, hereafter M09) have further suggested that small chemical anomalies (rather than a global excess of metallicity) are a possible signature of terrestrial planet formation. The authors showed that the Sun is deficient in refractory elements relative to volatile when compared to solar twins, suggesting that the refractory elements depleted in the solar photosphere are possibly locked up in terrestrial planets and/or in the cores of giant planets.

Most binary stars are believed to have formed from a common molecular cloud. This is supported both by observations of binaries in star forming regions (e.g. Reipurth et al., 2007; Vogt et al., 2012; King et al., 2012) and by numerical models of binary formation (e.g. Reipurth & Mikkola, 2012; Kratter, 2011). These systems are ideal laboratories to look for possible chemical differences between their components, specially for physically similar stars which help to minimize the errors. For the case of main-sequence stars, Desidera et al. (2004) studied the components of 23 wide binary stars and showed that most pairs present almost identical abundances, with only 4 pairs showing differences between 0.02 dex and 0.07 dex. A similar conclusion was reached by Desidera et al. (2006), showing that only 6 out of 33 southern binary stars with similar components present differences between 0.05 and 0.09 dex. The origin of the slight differences in these few cases is not totally clear, and a possible explanation is the planet formation process (e.g. Gratton et al., 2001; Desidera et al., 2004, 2006).

There are very few binary systems with similar components (where one of them host a planet) studied in the literature, comparing in detail the chemical composition between them. For instance, the binary system 16 Cyg is composed of a pair of stars with spectral types G1 V + G2 V, and the B component hosts a giant planet of 1.5 M (Cochran et al., 1997). This system have received the attention of many different abundance works. Takeda (2005) and Schuler et al. (2011) suggested that both stars present the same chemical composition, while other studies found that 16 Cyg A is more metal-rich than the B component (Laws & Gonzalez, 2001; Ramírez et al., 2011; Tucci Maia et al., 2014). In particular, Tucci Maia et al. (2014) also find a trend between refractories and the condensation temperature T, which could be interpreted as a signature of the rocky accretion core of the giant planet 16 Cyg Bb. Another example is the binary system HAT-P-1 composed of an F8 V + G0 V pair, in which the cooler star hosts a 0.53 M transiting planet (Bakos et al., 2007). Recently, Liu et al. (2014) found almost the same chemical abundances on both stars and concluded that the presence of giant planets does not necessarily imply differences in their composition. Both members of the binary system present an identical positive correlation with T, suggesting that the terrestrial formation process was probably less efficient in this system. Liu et al. (2014) also discuss why the chemical signature of planet formation is detected in the binary system 16 Cyg but not in the HAT-P-1 system. The planet 16 Cyg Bb (1.5 M) is more massive than the planet HAT-P-1 Bb (0.5 M), allowing to imprint the chemical signature in their host stars. The stellar masses in the binary system HAT-P-1 (1.16 and 1.12 M, Bakos et al., 2007) are slightly higher than in the system 16 Cyg (1.05 and 1.00 M, Ramírez et al., 2011). This implies less massive convection zones in the stars of the system HAT-P-1 (i.e. more prone to imprint the chemical signature) but also shorter pre-main-sequence disc lifetimes (i.e. more difficult to imprint the chemical signature). These points illustrate how complicated and challenging could be to determine the possible effects of planet formation using stellar abundances. Then, there is a need for additional stars hosting planets in binary systems to be compared through a high-precision abundance determination.

Using radial-velocity measurements, Naef et al. (2001) detected first a giant planet around the solar-type star HD 80606, which is the primary of the wide binary system HD 80606 - HD 80607 (components A and B). To date, there is no planet detected around the B component. The separation between A and B stars is 21.1” (e.g. Dommanget & Nys, 2002), corresponding to 1000 AU at the distance of about 60 pc (Laughlin et al., 2009). This binary system is particularly notable for several reasons. Both stars present very similar fundamental parameters (their effective temperatures differ only in 67 K and their superficial gravities in 0.01 dex, as we see later). The reported spectral types are G5 V + G5 V, as described in the Hipparcos catalog. This makes this system a new member of the selected group of binaries with very similar components. The exoplanet HD 80606 b have a period of 111.8 days and one of the most eccentric orbits to date (e = 0.927, Naef et al., 2001), probably due to the influence of the B star (Wu & Murray, 2003). Besides the radial-velocity detection, Laughlin et al. (2009) reported a secondary transit for HD 80606 b using 8 m Spitzer observations, while Moutou et al. (2009) detected the primary transit of the planet and measured a planet radius of 0.9 M. Then, future observations of the atmosphere of this transiting planet could be compared to the natal chemical environment established by a binary star elemental abundances, as suggested by Teske et al. (2013). These significant features motivated this study, exploring the possible chemical signature of planet formation in this remarkable system.

There are some previous abundance measurements of HD 80606 in the literature. A number of elements show noticeable discrepancies in the reported values. Notably, using the same stellar parameters, the Na abundance have been reported as +0.300.05 dex and +0.530.12 dex (Beirao et al., 2005; Mortier et al., 2013) while the Si abundance resulted +0.400.09 dex and +0.270.06 dex (Mortier et al., 2013; Gilli et al., 2006). These differences also encouraged this work. We perform a high-precision abundance study analyzing both members of this unique binary system using a line-by-line differential approach, aiming to detect a slight contrast between their components.

This work is organized as follows. In Section 2 we describe the observations and data reduction, while in Section 3 we present the stellar parameters and chemical abundance analysis. In Section 4 we show the results and discussion, and finally in Section 5 we highlight our main conclusions.

2 Observations and data reduction

Stellar spectra of HD 80606 and HD 80607 were obtained with the High Resolution Echelle Spectrometer (HIRES) attached on the right Nasmyth platform of the Keck 10-meter telescope on Mauna Kea, Hawaii. The slit used was B2 with a width of 0.574 arcsec, which provides a measured resolution of 67000 at 5200 Å222http://www2.keck.hawaii.edu/inst/hires/slitres.html. The spectra were downloaded from the Keck Observatory Archive (KOA)333http://www2.keck.hawaii.edu/koa/koa.html, under the program ID A271Hr.

The observations were taken on March, 15th 2011 with HD 80607 observed immediately after HD 80606, using the same spectrograph configuration. The exposure times were 3 x 300 s for both targets. We measured a S/N 330 for each of the binary components. The asteroid Iris was also observed with the same spectrograph setup achieving a similar S/N, to acquire the solar spectrum useful for reference in our (initial) differential analysis. We note however that the final differential study with the highest abundance precision is between HD 80606 and HD 80607, due to their high degree of similarity.

Our resolving power is 40 higher than those reported in previous works (Ecuvillon et al., 2006; Gilli et al., 2006; Mortier et al., 2013). However, even for a similar resolution and S/N, the differential line-by-line approach applied here results in a significant improvement on the derived abundances, as we show in the next sections.

We reduced the HIRES spectra using the data reduction package MAKEE444http://www.astro.caltech.edu/ tb/makee/ (MAuna Kea Echelle Extraction), which performs the usual reduction process including bias subtraction, flat fielding, spectral order extractions, and wavelength calibration. The continuum normalization and other operations (Doppler correction and combining spectra) was perfomed using IRAF555IRAF is distributed by the National Optical Astronomical Observatories which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation..

3 Stellar parameters and chemical abundance analysis

We start by measuring the equivalent widths (EW) of Fe I and Fe II lines in the spectra of our program stars using the IRAF task splot, and then continued with other chemical species. The lines list and relevant laboratory data (such as excitation potential and oscilator strengths) were taken from Liu et al. (2014), Meléndez et al. (2014), and then extended with data from Bedell et al. (2014) who carefully selected lines for a high-precision abundance determination. This data including the measured EWs are presented in the Table 2.

The fundamental parameters (T, log g, [Fe/H], v) of HD 80606 and HD 80607 were derived by imposing excitation and ionization balance of Fe I and Fe II lines. We used an updated version of the program FUNDPAR (Saffe, 2011), which uses the MOOG code (Sneden, 1973) together with ATLAS9 model atmospheres (Kurucz, 1993) to search the appropriate solution. The procedure uses explicity calculated (i.e. non-interpolated) 1D LTE Kurucz’s model atmospheres with ATLAS9 and NEWODF opacities (Castelli & Kurucz, 2003).

We tested the model atmospheres by using the PERL program ifconv.pl, which is available in the web666http://atmos.obspm.fr/index.php/documentation/7 together with the Linux port of the Kurucz’s programs. The code checks both the convergence of the stellar flux and the flux derivative in the ATLAS9 models, at different Rosseland optical depths. The convergence could be a problem in the outermost layers of models calculated with very low T (3500 K or less) and very low log g, as reported in the same page. Under these conditions, even the LTE hypothesis probably does not hold. However, the Kurucz’s models used here are far from these values and have been tested using the mentioned program.

The relative spectroscopic equilibrium was achieved using differential abundances for each line i, defined as:

(1)

where and are the abundances in the star of interest and in the reference star777We use the usual abundance definition . The same equilibrium conditions used in Saffe (2011) are written for the differential case as:

(2)
(3)
(4)
(5)

where is the excitation potential and EW is the logarithm of the reduced equivalent width. The symbol ”¡ ¿” denote the abundance average of the different lines, while and correspond to the input and output abundances in the program MOOG. The values and are the slopes in the plots of abundance vs and abundance vs EW. In this way, equations 2 and 3 shows the independence of differential abundances with the excitation potential and equivalent widths (by requiring null slopes and ), and equation 4 is the differential equilibrium between Fe I and Fe II abundances. Equation 5 expresses the imposed condition to the input and output abundances in the final solution. The updated version of the program FUNDPAR searches a solution that simultaneously verifies the conditions 2 to 5. The use of the 4 mentioned conditions (2 to 5) were previously tested (for the ”classical” non-differential case) using 61 main-sequence stars (Saffe, 2011), 223 giant stars (Jofré et al., 2015) and 9 early-type stars (Saffe & Levato, 2014), obtaining very similar parameters to the literature. Then, we applied these conditions for the differential line-by-line case, deriving for both stars stellar parameters in agreement with the literature and with lower errors, as we see later.

Stellar parameters of HD 80606 and HD 80607 were differentially determined using the Sun as standard in a first approach, and then we recalculate the parameters of HD 80607 but using HD 80606 as reference. First, we determined absolute abundances for the Sun using 5777 K for T, 4.44 dex for log g and an initial v of 1.0 km/s. Then, we estimated v for the Sun by the usual method of requiring zero slope in the absolute abundances of Fe I lines versus EW and obtained a final v of 0.91 km/s. We note however that the exact values are not crucial for our strictly differential study (see e.g. Bedell et al., 2014).

The next step was the determination of stellar parameters of HD 80606 and HD 80607 using the Sun as standard. For HD 80606 the resulting stellar parameters were T = 557343 K, log g = 4.320.14 dex, [Fe/H] = 0.3300.005 dex and v = 0.890.09 km/s. For HD 80607 we obtained T = 550621 K, log g = 4.310.11 dex, [Fe/H] = 0.3160.006 dex and v = 0.860.17 km/s. The metallicity of the A star is slightly higher than B by 0.014 dex. The Figures 1 and 2 shows the plots of abundance vs excitation potential and abundance vs EW for both stars. Filled and empty points correspond to Fe I and Fe II, while the dashed lines are linear fits to the differential abundance values.

Figure 1: Differential abundance vs excitation potential (upper panel) and differential abundance vs reduced EW (lower panel), for HD 80606 relative to the Sun. Filled and empty points correspond to Fe I and Fe II, respectively. The dashed line is a linear fit to the abundance values.
Figure 2: Differential abundance vs excitation potential (upper panel) and differential abundance vs reduced EW (lower panel), for HD 80607 relative to the Sun. Filled and empty points correspond to Fe I and Fe II, respectively. The dashed line is a linear fit to the abundance values.

The errors in the stellar parameters were derived as follows. We estimated the change in the ”observables” quantities (i.e. the slopes and and the abundance differences showed in equations 4 and 5), corresponding to individual changes in the ”measured” parameters T, log g, [Fe/H] and v (50 K, 0.05 dex, 0.05 dex, 0.05 km/s). The mentioned changes in the ”observables” are easily read in a normal execution of FUNDPAR. A similar procedure was used previously to calculate these changes (see e.g. Table 2 of Epstein et al., 2010). The differences are then used to estimate the standard deviation terms which correspond to independent parameters in the usual error propagation. For instance, the mentioned variation of 0.05 dex in log g for HD 80606 produce a variation in D (the abundance difference between Fe I and Fe II defined in equation 4) of 0.028 dex. Then, the individual error term in log g which corresponds only to the variation with D is estimated in a first-order approximation as , where is the standard deviation of the D values (estimated here using different Fe lines as ). Then, we also take into account the covariance terms by using the Cauchy-Schwarz inequality888The inequality for two variables x and y is where is the mutual covariance term and , are the individual dispersions., which allows us to calculate the mutual covariances using the (previously calculated) individual standard deviations. In this way, the inequality ensures that our final error adopted is not underestimated.

The process was repeated but using HD 80606 as the reference star instead of the Sun, fixing the parameters of the A component to perform the differential analysis. The Figure 3 shows the plots of abundance vs excitation potential and abundance vs EW, using similar symbols to those used in Figures 1 and 2. A visual inspection of the Figures 3 and 1 shows the lower dispersion in the HD 80607 differential abundance values using HD 80606 as a reference star. The resulting stellar parameters for HD 80607 resulted the same as using the Sun as a reference, but with lower dispersions: T = 550614 K, log g = 4.310.08 dex, [Fe/H] = -0.0140.003 dex and v = 0.860.07 km/s. Then, the metallicity of HD 80607 resulted slightly lower than HD 80606 by 0.014 dex, equal to the value found using the Sun as reference.

Figure 3: Differential abundance vs excitation potential (upper panel) and differential abundance vs reduced EW (lower panel), for HD 80607 relative to HD 80606. Filled and empty points correspond to Fe I and Fe II, respectively. The dashed line is a linear fit to the data.

The stellar parameters derived for the A and B stars are similar to those previously determined in the literature. Gonzalez & Laws (2007) derived [Fe/H] = 0.3490.073 dex for HD 80606, while Santos et al. (2004) derived (T, log g, [Fe/H], v) = (557472 K, 4.460.20 dex, 0.320.09 dex, 1.140.09 km/s) for HD 80606 i.e. only 1 K of difference compared to our result and 0.01 dex of difference in [Fe/H]. The log g and v values differ by 0.14 dex and 0.25 km/s, respectively. The stellar parameters derived by Santos et al. were then adopted in other works (Ecuvillon et al., 2006; Gilli et al., 2006; Mortier et al., 2013). For HD 80607, Koleva & Vazdekis (2012) derived T = 538945 K, log g = 3.990.18 dex and [Fe/H] = +0.350.06 dex, but adopting a fixed v = 2.0 km/s for all the stars in their sample.

Once the stellar parameters of the binary components were determined using iron lines, we computed abundances for all remaining elements: C I, O I, Na I, Mg I, Al I, Si I, S I, Ca I, Sc I, Sc II Ti I, Ti II, V I, Cr I, Cr II, Mn I, Fe I, Fe II, Co I, Ni I, Cu I, Sr I, Y II and Ba II. The hyperfine structure splitting was considered for V I, Mn I, Co I, Cu I and Ba II using the HFS constants of Kurucz & Bell (1995) and performing spectral synthesis for these species. In the Figure 4 we show an example of the observed and synthethic spectra in the region of the line Ba II 5853.67 Å for the star HD 80606. The same spectral lines were measured in both stars. NLTE corrections were applied to the O I triplet following Ramírez et al. (2007) instead of Fabbian et al. (2009) or Takeda (2003), because those works do not include corrections for [Fe/H]0. The NLTE abundances for O I are 0.11 dex lower than LTE values, adopting the same correction within errors for both stars given the very similar stellar parameters. We also applied NLTE corrections to Ba II following Korotin et al. (2011), who clearly shows that NLTE abundances are higher than LTE values for [Fe/H]0.

Figure 4: Observed and synthethic spectra (continuous and dotted lines) near the line Ba II 5853.67 Å for HD 80606. Some line identifications are showed.

In Table 1 we present the final differential abundances [X/Fe]999We used the standard notation [X/Fe] [X/H] [Fe/H] of HD 80606 and HD 80607 relative to the Sun, and the differential abundances of HD 80607 using HD 80606 as the reference star. We present both the observational errors (estimated as where is the standard deviation of the different lines) and systematic errors due to uncertainties in the stellar parameters (by adding quadratically the abundance variation when modifying the stellar parameters by their uncertainties) , as well as the total error obtained by adding quadratically , and the error in [Fe/H].

(HD 80606 - Sun) (HD 80607 - Sun) (HD 80607 - HD 80606)
Element [X/Fe] [X/Fe] [X/Fe]
[C I/Fe] -0.040 0.000 0.057 0.058 -0.036 0.000 0.039 0.040 +0.004 0.000 0.028 0.028
[O I/Fe] -0.193 0.041 0.041 0.058 -0.179 0.057 0.029 0.064 +0.014 0.031 0.020 0.037
[Na I/Fe] -0.022 0.017 0.016 0.024 -0.048 0.028 0.011 0.030 -0.026 0.015 0.006 0.017
[Mg I/Fe] 0.078 0.050 0.019 0.054 0.054 0.033 0.017 0.038 -0.024 0.021 0.011 0.024
[Al I/Fe] 0.003 0.064 0.016 0.066 0.007 0.068 0.012 0.069 +0.004 0.007 0.009 0.012
[Si I/Fe] 0.027 0.010 0.002 0.011 0.030 0.012 0.003 0.014 +0.003 0.004 0.002 0.005
[S I/Fe] -0.052 0.032 0.026 0.041 -0.043 0.050 0.021 0.055 +0.009 0.025 0.013 0.029
[Ca I/Fe] -0.048 0.016 0.015 0.022 -0.047 0.016 0.013 0.021 +0.001 0.003 0.008 0.009
[Sc I/Fe] 0.073 0.035 0.023 0.043 0.074 0.041 0.013 0.043 +0.002 0.006 0.009 0.011
[Sc II/Fe] 0.034 0.014 0.025 0.029 0.027 0.017 0.021 0.028 -0.007 0.004 0.015 0.015
[Ti I/Fe] 0.033 0.012 0.009 0.016 0.042 0.011 0.009 0.016 +0.008 0.005 0.004 0.007
[Ti II/Fe] 0.013 0.022 0.019 0.029 0.021 0.020 0.017 0.027 +0.008 0.014 0.012 0.019
[V I/Fe] 0.085 0.016 0.013 0.021 0.091 0.019 0.013 0.024 +0.006 0.006 0.008 0.011
[Cr I/Fe] 0.003 0.014 0.011 0.018 0.016 0.016 0.010 0.019 +0.013 0.005 0.005 0.008
[Cr II/Fe] 0.000 0.054 0.040 0.067 0.014 0.070 0.038 0.080 +0.014 0.016 0.023 0.029
[Mn I/Fe] -0.023 0.029 0.023 0.037 0.014 0.055 0.027 0.061 +0.037 0.012 0.014 0.019
[Co I/Fe] 0.191 0.020 0.016 0.027 0.231 0.024 0.016 0.030 +0.040 0.008 0.010 0.013
[Ni I/Fe] 0.078 0.007 0.004 0.009 0.078 0.007 0.005 0.010 -0.001 0.004 0.003 0.005
[Cu I/Fe] -0.070 0.050 0.040 0.064 -0.086 0.060 0.040 0.072 -0.016 0.020 0.025 0.032
[Sr I/Fe] 0.120 0.050 0.086 0.100 0.094 0.060 0.106 0.120 -0.026 0.020 0.055 0.058
[Y II/Fe] -0.002 0.028 0.034 0.044 0.030 0.027 0.042 0.050 +0.032 0.009 0.025 0.026
[Ba II/Fe] 0.190 0.050 0.040 0.064 0.177 0.060 0.040 0.072 -0.013 0.020 0.025 0.032
Table 1: Differential abundances for the stars HD 80606 and HD 80607 relative to the Sun, and HD 80607 relative to HD 80606. We also present the observational errors , errors due to stellar parameters , as well as the total error .

4 Results and discussion

We present in the Figures 5 and 6 the differential abundances of HD 80606 and HD 80607 relative to the Sun. The condensation temperatures were taken from the 50% T values derived by Lodders (2003). The individual comparison between one component (e.g. HD 80606) and the Sun, is possibly affected by Galactic Chemical Evolution (GCE) effects, due to their different chemical natal environments (see e.g. Tayouchi & Chiba, 2014; Mollá et al., 2015, and references therein). On the other hand, supossing that the stars of the binary system born at the same place/time, we discard GCE effects when comparing differentially the components between them, which is an important advantage of this method. Then, we corrected by GCE effects (only when comparing star-Sun) by adopting the fitting trends of González Hernández et al. (2013) (see their Figure 2, the plots of [X/Fe] vs [Fe/H]) to derive the values of [X/Fe] at [Fe/H]0.32 dex. A similar procedure was previously used by Liu et al. (2014) to correct by GCE the abundances in the binary system HAT-P-1. Filled points in the Figures 5 and 6 correspond to the differential abundances for the stars HD 80606 and HD 80607, respectively. For reference, we also included in these Figures the solar-twins trend of M09 using a continuous line, vertically shifted to compare the slopes. We included a weighted linear fit101010We used as weight the inverse of the total abundance error . to all abundance values, showed with dashed lines in the Figures 5 and 6. It is interesting to note that the slopes of the linear fits are similar to the trend of the solar-twins of M09 for the refractory elements.

Figure 5: Differential abundances (HD 80606 - Sun) vs condensation temperature T. The dashed line is a weighted linear fit to the differential abundance values, while the continuous line shows the solar-twins trend of Meléndez et al. (2009).
Figure 6: Differential abundances (HD 80607 - Sun) vs condensation temperature T. The dashed line is a weighted linear fit to the differential abundance values, while the continuous line shows the solar-twins trend of Meléndez et al. (2009).

In the Figures 5 and 6, the abundance of O I presents a low value compared to other volatile elements, while the abundances of Co I and Ca I seem to deviate from the general trend of the refractory elements (see also the next Figures 7 and 8). For both stars, we derived the O I abundance by measuring EWs of the O I triplet at 7771 Å and applied NLTE corrections following Ramírez et al. (2007). As we noted previously, the NLTE corrections decrease the abundance in 0.11 dex, However, even the LTE values seem to be relatively low; we do not find a clear reason for this. The forbidden [O I] lines at 6300.31 Å and 6363.77 Å are weak and slightly asymetric in our stars. Both [O I] lines are blended in the solar spectra: with two N I lines in the red wing of [O I] 6300.31 Å and with CN near [O I] 6363.77 Å (Lambert, 1978; Johansson et al., 2003; Bensby et al., 2004). Then, we prefer to avoid these weak [O I] lines in our calculation and use only the O I triplet. For the case of Co I, we take into account the HFS in the abundance calculation, however NLTE effects could also play a role in the Co I lines of solar-type stars (see e.g. Bergemann, 2008; Bergemann et al., 2010). Mashonkina et al. (2007) studied NLTE effects in the Ca I lines of late-type stars, and derived higher NLTE abundances than in LTE for most Ca I lines, using a model with T = 5500 K and [Fe/H] = 0. For these stellar parameters the corrections amount up to 0.08 dex, with an average of 0.05 dex. However, we caution that these studies for Co I and Ca I do not include corrections for stars with [Fe/H]0. Therefore, we excluded these species (O I, Co I and Ca I) from the calculation of the linear fits.

Ramírez et al. (2010, hereafter R10) studied the abundance results from six different abundance surveys and verified the findings of M09 about the T trends in the Sun and the terrestrial planet formation signature. They studied the possible dependence of the T trends with [Fe/H] using in particular the sample of Neves et al. (2009, hereafter N09). The authors showed that the ”solar anomaly” (i.e. the T trend for the refractory elements in the Sun) is also observed comparing the Sun with solar-analogs at both [Fe/H]-0.2 dex and [Fe/H]0.0 dex. However, for an average metallicity of [Fe/H]+0.2 dex, the solar analogs from N09 shows a T trend for refractories similar to the Sun (see e.g. their Figure 7). R10 interpret this result suggesting that, at high metallicity values, the probability of stars with and without T trends should be similar, and then, in average, no general trend with T result for the refractory elements. The authors also propose that it may be possible to distinguish metal-rich stars that show and do not show the planet formation signature from the T slopes of the refractory elements. Then, given that HD 80606 and HD 80607 present high metallicity values, it seems reasonable also a comparison of the refractories with the solar-analog stars with [Fe/H]+0.2 dex from N09.

The differential abundances of the refractory species are showed in the Figures 7 and 8. We include in these Figures the trend of the solar-analog stars with [Fe/H]+0.2 dex from N09 using a short-dased line, which shows almost an horizontal tendence. The solar-twins T trend of M09 is also showed with a continuous line. The tendences of N09 and M09 are vertically shifted for comparison. A weighted linear fit to the refractory species of HD 80606 and HD 80607 is presented with a long-dashed line. The refractory elements does not seem to follow an horizontal trend such as the sample of N09. The general trend of refractory species for both HD 80606 and HD 80607, are more similar to the solar-twins of M09 than to the solar-analogs stars with [Fe/H]+0.2 dex from N09. The Sun is depleted in refractory elements compared to the solar-twins of M09, however the solar-analogs with [Fe/H]+0.2 dex from N09 present a similar T trend compared to the Sun, as showed by R10. Then, following a reasoning similar to M09 and R10, the stars HD 80606 and HD 80607 do not seem to be depleted in refractory elements with respect to solar twins, which is different for the case of the Sun. In other words, the terrestrial planet formation would have been less efficient in the stars of this binary system than in the Sun.

Figure 7: Differential abundances (HD 80606 - Sun) vs condensation temperature T for the refractory elements. The long-dashed line shows a weighted linear fit to the abundance values. The continuous and short-dashed lines correspond to the solar-twins trend of M09, and the solar-analogs with [Fe/H]+0.2 dex from N09.
Figure 8: Differential abundances (HD 80607 - Sun) vs condensation temperature T for the refractory elements. The symbols are the same of Figure 7.

The line-by-line differential abundances between HD 80606 and HD 80607 greatly diminishes the errors in the calculation and GCE effects in the results, due to their remarkably similar stellar parameters and due to the same (initial) chemical composition. In the Figure 9 we show the differential abundances of HD 80607 vs T but using HD 80606 as the reference star. The continuous line in this Figure presents the solar-twins trend of M09 (vertically shifted), while the long-dashed line is a weighted linear fit to the refractory elements. We included an horizontal line at 0.0 dex for reference.

Figure 9: Differential abundances (HD 80607 - HD 80606) vs condensation temperature T. The long-dashed line is a weighted linear fit to the refractory species. The solar-twins trend of Meléndez et al. (2009) is showed with a continuous line. The horizontal line at 0.0 dex is included for reference.

Most elements present slightly higher abundance values in HD 80606 compared to HD 80607, with an average difference of +0.0100.019 dex. In particular, the difference for the Fe I abundances is +0.0140.003 dex i.e. HD 80606 slightly more metal-rich than HD 80607. From the Figure 9, the abundances of the volatile does not seem to be different from the refractory elements. Their average abundances are -0.0050.005 dex and -0.0110.005 dex i.e. almost the same within the errors. In the Figure 9, the slope of the differential abundances is -1.2016.5 10 dex/K for the refractory elements. For comparison, the slope of refractories between the components of the binary system 16 Cyg resulted 1.880.79 10 dex/K and showing clearly a higher abundance in refractory than volatile elements (Tucci Maia et al., 2014). Then, although HD 80606 seems to present a slightly higher Fe I abundance than HD 80607, there is no clear difference between refractory and volatile elements nor a significative trend with T. This would imply that there is no clear evidence of terrestrial planet formation in this binary system. Similarly, Liu et al. (2014) did not find a trend with T in the binary system HAT-P-1 and concluded that the presence of a giant planet does not neccesarily introduce a chemical signature in their host stars. This is in line with some previous literature works, who propose that the presence of close-in giant planets might prevent the formation of terrestrial planets (Meléndez et al., 2009; Steffen et al., 2012). For the case of eccentric giant planets, numerical simulations also found that the early dynamical evolution of giant planets clear out most of the terrestrial planets in the inner zone (Veras & Armitage, 2005, 2006; Raymond et al., 2011).

4.1 A planet around HD 80607?

Up to now, there is no planet detected around HD 80607. The photometry of HD 80607 is relatively flat i.e. a transit-like event is not observed (Fossey et al., 2009; Pont et al., 2009). To our knowledge, this object is not included in the current radial velocity surveys.

However, given the abundance results of this study and the confirmed presence of a giant planet (with very high eccentricity) only around HD 80606, we can speculate about a possible planet formation scenario in this binary system. The occurrence of planets was fit by Fischer & Valenti (2005) using a power law as a function of the metallicity: P 0.03 (N/N)/(N/N). Then, the probability increases by a factor of 5 when the Fe abundance increase from [Fe/H] = 0.0 dex to [Fe/H] = 0.3 dex. This high probability together with the fact that HD 80606 already host a giant planet, and given the very similar stellar parameters with HD 80607, suggest that the giant planet formation process in HD 80607 could be also a very plausible hypothesis. Possibly, the metals missing in HD 80607 compared to HD 80606 have been used to form this (hypothetic) giant planet. Tucci Maia et al. (2014) make a similar suggestion to explain the slightly different metallicities between the components of the binary system 16 Cyg. Moreover, there are binary systems where each component hosts a planet and the metallicity resulted slightly different between their stars, such as in the system XO-2 (Damasso et al., 2015). Then, probably due to the mutual interactions in this binary system, HD 80606 resulted with one of the most eccentric planets to date (see e.g. Wu & Murray, 2003), while the HD 80607 system may have had its giant planet ejected. In fact, the possible companion around HD 80607 could be an ejected or maybe an undetected (such as a long period) planet. We stress, however, that this is only a speculative comment and should be taken with caution.

Previous works showed that the global frequency of planets in wide binaries is not statistically different from that of planets in single stars, with no significant dependence of the binary separation (Bonavita & Desidera, 2007). Also, the properties of planets in wide binaries are compatible with those of planets orbiting single stars, except for a possible increase of high-excentricity planets (Desidera & Barbieri, 2007). However, the presence of closer stellar companions with separation 100-300 AU could modify the evolution of giant planets around binary components (Desidera & Barbieri, 2007).

More recently, Wang et al. (2015) studied 84 KOIs (Kepler Object of Interest) with al least one gas giant planet detected within 1 AU and a control sample of field stars in the solar neighborhood. The authors found a dependence of the stellar multiplicity rate (MR) as a function of the stellar separation a. They derived MRs of 0%, 34% and 34% for binary separations of a 20 AU, 20 AU a 200 AU, and a 200 AU, respectively. In other words, no stellar companion has been found within 20 AU for Kepler stars with gas giant planets, while gas giant planet formation is not significantly affected by stellar companions beyond 200 AU. Then, this work shows that the binary separation plays a role in close binaries rather than in wide binaries, such as HD 80606 (a 1000 AU). This is in agreement with Zuckerman (2014), who found that the the presence of a wide stellar companion (a 1000 AU) does not diminish the likelihood of a wide-orbit planetary system.

Wang et al. (2015) also studied the possible physical differences between the components of binaries hosting planets. They suggest that the stellar companions of host stars with a planet period P70 d tend to be fainter than the shorter-period counterparts. However, they caution that this apparent effect may be due to a lack of sensivity for fainter stellar companions and suggest more follow-up observations to support or disprove it.

Using numerical simulations, Wu & Murray (2003) suggest that the high exccentricity of the planet HD 80606 b is probably due to the influence of the companion HD 80607 through a Kozai mechanism111111The Kozai mechanism are oscilations in the eccentricity and inclination of a planet due to the presence of a remote stellar companion, see e.g. Kozai (1962). combined with a tidal dissipation. On the other hand, Kaib et al. (2013) showed a possible variable nature of wide binaries due to the Milky Way tidal field, including a reshape of their planetary systems. In this scenario, they obtained an instability fraction (i.e. number of planetary ejections within 10 Gyr of evolution) depending on the binary’s mass and separation. Using the binary parameters of HD 80606, they obtained a fraction 50% (see their Fig. 2). Although these simulations do not include the possibility of a planet around HD 80607, they showed that the planetary configuration in this binary system could be strongly affected, and the possible ejection of a planet could not be totally ruled out.

5 Conclusions

Following the aims of this study, we performed a high-precision differential abundance determination in both components of the remarkable binary system HD 80606 - HD 80607, in order to possibly detect a signature of terrestrial planet formation. Both stars present very similar stellar parameters, which greatly diminishes the errors in the abundance determination and GCE effects. The star HD 80606 hosts a giant (high-eccentricity) planet while there is no planet detected around HD 80607. First, we derived stellar parameters and differential abundances of both stars using the Sun as the reference star. We compared the possible temperature condensation T trends of the stars with the solar-twins trend of Meléndez et al. (2009) and then with a sample of solar-analog stars with [Fe/H]+0.2 dex from Neves et al. (2009). Our calculation included NLTE corrections for O I and Ba II as well as GCE corrections for all chemical species. From these comparisons, we concluded that the stars HD 80606 and HD 80607 do not seem to be depleted in refractory elements, different to the case of the Sun (Meléndez et al., 2009). In other words, the terrestrial planet formation would have been less efficient in the stars of this binary system than in the Sun.

Then, we also compared differentially HD 80607 but using HD 80606 as the reference star. HD 80606 resulted slightly more metal-rich than HD 80607 by +0.0140.003 dex. However, we do not find a clear difference between refractory and volatile elements nor a significative trend with T between both stars. In comparing the stars to each other, the lack of a trend for refractory elements with T implies that the presence of a giant planet does not necessarily imprint a chemical signature on its host star, similar to the result of Liu et al. (2014) for the binary system HAT-P-1. This is in agreement with Meléndez et al. (2009), who suggest that the presence of close-in giant planets might prevent the formation of terrestrial planets. Finally, we speculate about a possible (ejected or non-detected) planet around HD 80607. We strongly encourage high-precision abundance studies in binary systems with similar components, which is a crucial tool for helping to detect the possible chemical pattern of the planet formation process.

Acknowledgements.
We thank the anonymous referee for their constructive comments that greatly improved the paper. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The authors also thank Drs. R. Kurucz and C. Sneden for making their codes available to them.

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\onltab

1

Element EP log gf
[Å] [eV] [dex] [mÅ] [mÅ] [mÅ]
6.00 5052.167 7.680 -1.240 42.0 39.4 33.6
6.00 6587.610 8.540 -1.050 16.6 14.8 12.1
8.00 7771.944 9.150 0.370 65.7 58.4 66.9
8.00 7774.166 9.150 0.220 61.5 59.3 62.1
8.00 7775.388 9.150 0.000 49.8 47.2 45.0
11.00 4751.822 2.100 -2.080 36.7 38.5 15.7
11.00 5148.838 2.100 -2.040 31.0 31.7 13.8
11.00 6154.225 2.100 -1.550 75.3 80.6 39.2
11.00 6160.747 2.100 -1.250 91.8 94.1 56.9
12.00 4730.040 4.340 -2.390 112.1 108.7 68.6
12.00 5711.088 4.340 -1.730 147.0 144.6 106.6
12.00 6318.717 5.110 -1.950 62.1 63.8 37.3
12.00 6319.236 5.110 -2.160 52.1 51.5 24.2
13.00 5557.070 3.140 -2.210 25.5 25.6 13.4
13.00 6696.018 3.140 -1.480 62.3 64.7 36.0
13.00 6698.667 3.140 -1.780 47.0 48.6 20.8
14.00 5488.983 5.610 -1.690 38.1 36.8 18.5
14.00 5517.540 5.080 -2.500 24.6 23.6 12.2
14.00 5645.611 4.930 -2.040 56.7 56.7 35.8
14.00 5665.554 4.920 -1.940 65.0 65.5 39.3
14.00 5684.484 4.950 -1.550 81.2 80.6 61.0
14.00 5690.425 4.930 -1.770 67.7 67.6 48.5
14.00 5701.104 4.930 -1.950 58.6 56.1 40.3
14.00 5753.640 5.620 -1.330 71.6 72.7 43.5
14.00 5772.145 5.082 -1.653 74.1 74.7 51.8
14.00 5793.073 4.930 -1.960 64.7 62.2 42.9
14.00 5948.540 5.080 -1.208 108.8 108.3 84.4
14.00 6125.021 5.610 -1.500 51.2 49.6 31.7
14.00 6145.015 5.620 -1.410 59.4 58.8 38.7
14.00 6195.460 5.870 -1.666 33.8 34.2 15.2
14.00 6243.823 5.620 -1.270 61.8 59.2 43.9
14.00 6244.476 5.620 -1.320 71.4 70.4 45.4
14.00 6741.630 5.980 -1.650 28.6 27.8 15.2
14.00 7034.903 5.870 -0.780 81.6 82.4 62.8
14.00 7405.770 5.614 -0.720 112.3 111.8 88.7
16.00 4695.443 6.530 -1.830 12.0 12.6 8.2
16.00 6046.000 7.870 -0.150 28.4 24.8 20.3
16.00 6052.656 7.870 -0.400 17.8 16.9 13.2
16.00 6743.540 7.870 -0.600 12.6 10.8 9.7
20.00 5260.387 2.520 -1.720 52.2 54.1 32.5
20.00 5261.710 2.520 -0.680 127.8 131.5 100.6
20.00 5512.980 2.930 -0.460 114.2 116.0 83.8
20.00 5590.114 2.520 -0.570 110.9 113.6 92.8
20.00 5867.562 2.930 -1.570 42.5 43.5 23.5
20.00 6156.020 2.520 -2.497 19.8 19.8 8.7
20.00 6161.297 2.520 -1.270 82.9 84.9 59.5
20.00 6166.439 2.520 -1.140 94.1 95.8 69.6
20.00 6169.550 2.520 -0.580 139.9 141.8 108.7
20.00 6455.598 2.520 -1.340 80.3 82.6 55.2
20.00 6471.662 2.530 -0.690 112.6 115.6 91.0
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39.10 5087.420 1.084 -0.170 58.3 57.9 47.0
39.10 5200.413 0.992 -0.570 47.8 47.2 37.9
56.00 5853.686 0.604 -2.066
56.00 5853.687 0.604 -2.066
56.00 5853.687 0.604 -2.009
56.00 5853.688 0.604 -2.009
56.00 5853.689 0.604 -2.215
56.00 5853.689 0.604 -2.215
56.00 5853.690 0.604 -1.010
56.00 5853.690 0.604 -1.466
56.00 5853.690 0.604 -1.914
56.00 5853.690 0.604 -2.620
56.00 5853.690 0.604 -1.010
56.00 5853.690 0.604 -1.466
56.00 5853.690 0.604 -1.914
56.00 5853.690 0.604 -2.620
56.00 5853.690 0.604 -1.010
56.00 5853.691 0.604 -2.215
56.00 5853.692 0.604 -2.215
56.00 5853.693 0.604 -2.009
56.00 5853.693 0.604 -2.009
56.00 5853.694 0.604 -2.066
56.00 5853.694 0.604 -2.066
56.00 6141.725 0.704 -2.456
56.00 6141.725 0.704 -2.456
56.00 6141.727 0.704 -1.311
56.00 6141.727 0.704 -1.311
56.00 6141.728 0.704 -2.284
56.00 6141.728 0.704 -2.284
56.00 6141.729 0.704 -0.503
56.00 6141.729 0.704 -1.214
56.00 6141.729 0.704 -0.503
56.00 6141.729 0.704 -1.214
56.00 6141.730 0.704 -0.077
56.00 6141.730 0.704 -0.077
56.00 6141.730 0.704 -0.077
56.00 6141.731 0.704 -0.709
56.00 6141.731 0.704 -1.327
56.00 6141.731 0.704 -0.709
56.00 6141.731 0.704 -1.327
56.00 6141.732 0.704 -0.959
56.00 6141.732 0.704 -1.281
56.00 6141.732 0.704 -0.959
56.00 6141.733 0.704 -1.281
56.00 6496.898 0.604 -1.886
56.00 6496.899 0.604 -1.886
56.00 6496.901 0.604 -1.186
56.00 6496.902 0.604 -1.186
56.00 6496.906 0.604 -0.739
56.00 6496.906 0.604 -0.739
56.00 6496.910 0.604 -0.380
56.00 6496.910 0.604 -0.380
56.00 6496.910 0.604 -0.380
56.00 6496.916 0.604 -1.583
56.00 6496.916 0.604 -1.583
56.00 6496.917 0.604 -1.186
56.00 6496.918 0.604 -1.186
56.00 6496.920 0.604 -1.186
56.00 6496.922 0.604 -1.186
Table 2: Continued.
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