# Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

Victoria DiTomasso Chantanelle Nava Mercedes López-Morales Allyson Bieryla
Ryan Cloutier Center for Astrophysics $|$ Harvard ${\rm\&}$ Smithsonian, 60
Garden Street, Cambridge, MA 02138, USA  Luca Malavolta Dipartimento di Fisica
e Astronomia “Galileo Galilei”, Universitá di Padova, Vicolo del
l’Osservatorio 3, I-35122 Padova, Italy  Annelies Mortier KICC & Astrophysics
Group, Cavendish Laboratory, University of Cambridge, J.J. Thomson Avenue,
Cambridge CB3 0HE, UK  School of Physics & Astronomy, University of
Birmingham, Edgbaston, Birmingham, B15 2TT, UK  Lars A. Buchhave DTU Space,
National Space Institute, Technical University of Denmark, Elektrovej 328,
DK-2800 Kgs. Lyngby, Denmark  Keivan G. Stassun Department of Physics and
Astronomy, Vanderbilt University, Nashville, TN 37235, USA  Alessandro
Sozzetti INAF - Osservatorio Astrofisico di Torino, Via Osservaorio 20, I10025
Pino Torinese, Italy  Aldo Stefano Bonomo INAF - Osservatorio Astrofisico di
Torino, Via Osservaorio 20, I10025 Pino Torinese, Italy  David Charbonneau
Center for Astrophysics — Harvard and Smithsonian, 60 Garden Street,
Cambridge, MA 02138, USA  Andrew Collier Cameron  Centre for Exoplanet
Science, SUPA School of Physics and Astronomy, University of St Andrews, North
Haugh, St Andrews KY16 9SS, UK  Rosario Cosentino Fundación Galileo Galilei -
INAF, Rambla J. A. F. Perez, 7, E-38712 S.C. Tenerife, Spain  Mario Damasso
INAF - Osservatorio Astrofisico di Torino, Via Osservaorio 20, I10025 Pino
Torinese, Italy  Xavier Dumusque Department of Astronomy, University of
Geneva, Chemin Pegasi 51, Versoix, Switzerland  A. F. Martínez Fiorenzano
Fundación Galileo Galilei - INAF, Rambla J. A. F. Perez, 7, E-38712 S.C.
Tenerife, Spain  Adriano Ghedina Fundación Galileo Galilei - INAF, Rambla J.
A. F. Perez, 7, E-38712 S.C. Tenerife, Spain  Avet Harutyunyan  Fundación
Galileo Galilei - INAF, Rambla J. A. F. Perez, 7, E-38712 S.C. Tenerife, Spain
R. D. Haywood Astrophysics Group, University of Exeter, Exeter EX4 2QL, UK
STFC Ernest Rutherford Fellow  David Latham Center for Astrophysics — Harvard
and Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA  Emilio Molinari
INAF - Osservatorio Astronomico di Cagliari, Via della Scienza 5, I-09047,
Selargius, Italy  Francesco A. Pepe  Department of Astronomy, University of
Geneva, Chemin Pegasi 51, Versoix, Switzerland  Matteo Pinamonti INAF -
Osservatorio Astrofisico di Torino, Via Osservaorio 20, I10025 Pino Torinese,
Italy  Ennio Poretti Fundación Galileo Galilei - INAF, Rambla J. A. F. Perez,
7, E-38712 S.C. Tenerife, Spain  INAF – Osservatorio Astronomico di Brera, via
E. Bianchi 46, I-23807 Merate (LC), Italy  Ken Rice SUPA, Institute for
Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ,
Scotland, UK  Centre for Exoplanet Science, University of Edinburgh, Edinburgh
EH93FD, UK  Dimitar Sasselov Center for Astrophysics $|$ Harvard ${\rm\&}$
Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA  Manu Stalport
Observatoire de Geneva, Universite de Geneve, 51 ch. des Maillettes, CH-1290
Sauverny, Switzerland  Stéphane Udry Department of Astronomy, University of
Geneva, Chemin Pegasi 51, Versoix, Switzerland  Christopher Watson
Astrophysics Research Centre, School of Mathematics and Physics, Queen’s
University Belfast, Belfast, BT7 1NN, UK  Thomas G. Wilson Centre for
Exoplanet Science, SUPA School of Physics and Astronomy, University of St
Andrews, North Haugh, St Andrews KY16 9SS, UK

###### Abstract

We present high-precision radial velocities (RVs) from the HARPS-N
spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-
bound binary system. We detect a planet candidate with a period of
$24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs,
validating the planet candidate originally identified in CARMENES RV data
alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we
further refine the planet candidate parameters to $P=24.422\pm 0.014$ days,
$K=3.19\pm 0.27$ m/s, $M$ sin $i=10.6\pm 1.2M_{\oplus}$, and $a=0.142\pm
0.005$ au. We do not find any additional planet candidate signals in the data
of HD79211 nor do we find any planet candidate signals in HD79210. This system
adds to the number of exoplanets detected in binaries with M dwarf members,
and serves as a case study for planet formation in stellar binaries.

††thanks: National Science Foundation Graduate Research Fellow
Corresponding author: Victoria DiTomasso
<EMAIL_ADDRESS>
##  1 Introduction

M dwarfs are the most common stars, constituting as many as 75% of the stars
in our galaxy (Henry et al., 2006), and every M dwarf is predicted to host at
least one planet (Dressing & Charbonneau, 2015). The abundance of M dwarfs and
the prevalence of planets around them, combined with the relatively large
signals planets impose on low-mass stars, have made M dwarfs the primary
target for many exoplanet studies. Previous studies report that between 23%
and 46% of M dwarfs are in binaries (Ward-Duong et al., 2015; Winters et al.,
2019; Susemiehl & Meyer, 2021), but so far only about 30 exoplanets (less than
7% of the total found around M-dwarfs) have been found around binaries where
at least one member is an M dwarf. Approximately 20 planets have been found
orbiting M-dwarf components in an S-type configuration, characterized by the
planet orbiting around just one star in a binary, around M-dwarf components
(Thebault & Haghighipour, 2015), and less than 10 circumbinary planets have
been found around binaries with an M dwarf member (e.g. Doyle et al., 2011;
Orosz et al., 2012; Schwamb et al., 2013; Jain et al., 2017). Hundreds of
exoplanets have been, and will continue to be, discovered around M dwarfs,
allowing for studies of planet formation in binaries with M dwarf members.

HD79210 and HD79211 are a pair of M0V stars that comprise a gravitationally-
bound binary. These two stars are in many ways, twins. They are nearly
identical in mass, radius and effective temperature according to literature
measurements (see Table 1), varying by only a few percent at most. Together
they form one of only ten stellar binary exoplanet host systems with a binary
mass ratio greater than 0.9. With a period of $1295\pm 180$ years and semi-
major axis of $130.9\pm 5.1$ au (González-Álvarez et al., 2020), these stars
have a projected separation of 108.54 au and a semi-major axis of 130 au
(González-Álvarez et al., 2020). Many studies of disk evolution as well as
exoplanet formation and occurrence around binary stars cite 100 au either
projected separation or semi-major axis as a boundary for various behaviors.
For example: binaries with separations greater than 100 au do not seem to
affect planet populations, in comparison to single stars (Desidera & Barbieri,
2007; Mugrauer & Neuhäuser, 2009; Kraus et al., 2016); closer binaries ($<100$
au separation) are less likely to host planets (Roell et al., 2012; Bergfors
et al., 2013; Kraus et al., 2016); and planets in wide binaries (100 au $<a<$
700 au) tend to have inclinations that are aligned with those of the stellar
binary (Christian et al., 2022). With only around $4\%$ of all exoplanet-
hosting stars being members of binary or multiple systems (Marzari & Thebault,
2019), the HD79210/HD79211 binary system serves as a valuable edge-case data
point for these binary planet population studies.

While no transiting planet has yet been detected around either of these
targets, González-Álvarez et al. (2020) published an RV detection of a planet
candidate around HD79211 using high-precision radial velocities from the
CARMENES spectrograph (Quirrenbach et al., 2016). They reported a planet with
an orbital period of $24.45\pm 0.02$ days, a semi-major axis of $0.141\pm
0.005$ au, a semi-amplitude of $3.07\pm 0.37$ m/s, minimum mass of
$10.27^{+1.47}_{-1.38}$ or $9.97^{+1.47}_{-1.38}M_{\oplus}$, depending on
their adopted stellar mass. They found one significant periodic signal in the
RV data of HD79210 at 16.3 days, which they attributed to the stellar rotation
period.

In this paper, we search for the 24.4 day planet around HD79211 in the HARPS-N
data taken as part of the HARPS-N GTO Rocky Planet Search (RPS) program, as
well as HIRES data from Butler et al. (2017), in an effort to support this
planet’s presence and refine its parameters. We also look for additional
signals in the HARPS-N, HIRES and CARMENES data of both targets. In section 2,
we discuss the data used throughout this paper. In section 3, we discuss our
efforts to charactize the two stars. In section 4, we share our analysis of
the new photometric light curves taken with KeplerCam. In section 5, we
present our radial velocity (RV) analysis, and in section 6 we report our
results and discussion.

##  2 Data

###  2.1 HARPS-N Spectroscopy and White Light Radial Velocities

These two targets were observed using the HARPS-N spectrograph installed on
the 3.6 m Telescopio Nazionale Galileo (TNG) at the Observatorio del Roque de
los Muchachos in La Palma, Spain (Cosentino et al., 2012, 2014). HARPS-N is an
updated version of HARPS at the ESO 3.6 m telescope (Mayor et al., 2003), with
a proven RV stability better than 1 m/s.

There are a total of 81 observations of HD 79210 taken between January 2014
and March 2022 (Figure A1). There are a total of 114 observations of HD 79211
taken between December 2012 and March 2022 (Figure 1). Both objects were
observed as part of the HARPS-N guaranteed time observation (GTO) Rocky Planet
Search program. The aim of this program is to monitor the radial velocities of
nearby, bright, quiet stars in search of low-mass planets orbiting them
(Motalebi et al., 2015). For this program, targets were observed with
15-minute exposure times to minimize the effect of stellar noise with short
typical time scales, i.e. averaging out p-mode oscillations (Chaplin et al.,
2019). Additional measurements of the targets are spaced by two or five hours
during the night to minimize the effect of granulation (Pepe et al., 2011;
Dumusque et al., 2011; Motalebi et al., 2015).

These spectra were reduced with version 3.7 of the HARPS-N Data Reduction
Software (DRS, Pepe et al., 2011). This pipeline calculates the spectral
bisector inverse slope (BIS), full width at half maximum (FWHM) and contrast,
as well as each observation’s H$\alpha$, Na-Index, and Mount Wilson S-index
$S_{MW}$. We included all of the above values in our analysis as stellar
activity indicators.

We calculated radial velocities from these spectra using the HARPS-TERRA
software, which calculates radial velocities using a spectral template derived
from the observations themselves, and has been shown to be particularly
effective when applied to M dwarfs (see Anglada-Escudé & Butler (2012) for
more information). The resulting RV measurements have median uncertainties of
$0.65$ m/s for HD79210 and $0.62$ m/s for HD79211.

###  2.2 HARPS-N Chromatic Radial Velocities

We also used the HARPS-N spectra to calculate chromatic radial velocities for
HD79211 to test the potential effect of stellar activity. We divided the
spectra into three wavelength ranges, 383.0-446.89 nm, 443.26-513.87 nm and
510.39-690 nm, and then calculated the RV of the target based on each spectral
range independently. This procedure is explained in detail in Mortier et al.
(2020) and summarized here. We coadded all of the CCFs calculated using
version 3.7 of the HARPS-N Data Reduction Software (DRS) from each Echelle
order that belonged to the desired wavelength range, and performed a Gaussian
fit on the result in order to obtain the corresponding chromatic RV. We
estimated the RV error from the photon noise, the total counts of the coadded
CCFs, and the read-out noise. We applied a correction factor to the noise
estimate in order to closely reproduce the RV error from the full-spectrum
CCF, knowing that the chromatic RVs will inevitably be noisier than the full-
spectrum RVs. The average error on the full-spectrum HARPS-N DRS RVs for both
targets was 0.56 m/s, and the median error on the chromatic RVs determined by
each spectral range was 2.35 m/s, 1.14 m/s and 0.99 m/s, respectively. Note
that these chromatic radial velocities were calculated using the CCFs from the
HARPS-N DRS, not using the HARPS-TERRA software like the white light RVs used
in the rest of this work.

Figure 1: Radial velocities for HD79211 measured from CARMENES (orange, top
panel only), HARPS-N (blue, all panels) and HIRES (green, top panel only)
spectra. For most data points, the uncertainty in the RV is smaller than the
size of the point. We mark the binary trend, fit as a second-order polynomial,
with a dashed line in the top and middle panels. The bottom panel shows the
HARPS-N radial velocities with the binary trend subtracted. We use the HARPS-N
RVs with the binary trend removed when calculating the correlation between RV
and activity indicators (Figure 4), and when calculating periodograms (Figures
5, 6, 7, 8).

###  2.3 Absolute Astrometry

The Gaia EDR3 archive reports two statistical indicators of possible
deviations from a single-star solution that might indicate the presence of
orbiting companions, astrometric_excess_noise and RUWE (renormalized unit
weight error). The values of the two parameters are 0.127 mas, 1.08 and 0.138
mas, 1.11 mas, for HD 79210 and HD79211, respectively. The values of
astrometric_excess_noise are in line with those obtained for very bright
stars, for which the calibration of Gaia astrometry will require further
improvements. The RUWE values are clearly below the empirical threshold of 1.4
above which the single-star solution is deemed unsatisfactory (Lindegren et
al., 2018, 2021), and which might be an indication of the presence of an
unresolved companion. A more stringent threshold at RUWE $\gtrsim 1.1$ has
been proposed in recent studies (Belokurov et al., 2020; Stassun & Torres,
2021) for the identification of unresolved stellar systems, but this is better
used for selection of samples rather than a single source-basis. The
historical RV and astrometric time-series (see González-Álvarez et al. 2020,
and references therein) do not show obvious evidence of additional, massive
unresolved companions orbiting either HD 79210 or HD 79211. We finally note
that astrometric acceleration catalogues such as those from Kervella et al.
(2022) and Brandt (2021) show statistically significant (signal-to-noise ratio
$>$ 10) proper motion anomalies at the mean Gaia epoch for both components.
This information can be used to further improve the constraints on the binary
orbit, but such a study goes beyond the scope of this paper.

###  2.4 Previously Published High-Precision Radial Velocities

There are 70 high-precision RV measurements of HD79210 and 159 of HD79211
published in González-Álvarez et al. (2020). These measurements were obtained
with the VIS channel of the CARMENES spectrograph on the 3.5m telescope of the
Calar Alto Observatory (Quirrenbach et al., 2016). The observations were taken
from March 2016 to January 2019 and January 2016 to October 2018 respectively,
with median uncertainties of 2.2 and 2.0 m/s respectively. González-Álvarez et
al. (2020) also published NIR RVs, but with uncertainties averaging 9 m/s,
they did not have high enough precision to search for the $\approx 3$ m/s
signal at 24.4 days.

We also include 32 radial velocities of HD79210 that were obtained between
June 1997 and December 2013 with a median uncertainty of 1.27 m/s, and 32
radial velocities of HD79211 that were obtained between June 1997 and February
2013 with a median uncertainty of 1.53 m/s using the HIRES spectrograph (Vogt
et al., 1994) on the Keck telescope (Butler et al., 2017). With only one to a
few data points per season, these RVs are not sufficient to constrain any
planet candidate orbital parameters on their own, but are used in our
analysis, where we include them as additional points alongside the HARPS-N and
CARMENES radial velocities.

###  2.5 Photometric Light Curves

HD79210 and HD79211 are bright M dwarfs in a binary, and are separated by 17
arcseconds on the sky. Because of this small angular separation, these two
targets are blended in many photometric surveys, such as ASAS-SN (Shappee et
al., 2014; Kochanek et al., 2017), WASP (Pollacco et al., 2006) and TESS
(Ricker et al., 2015). González-Álvarez et al. (2020) did obtain optical
photometric timeseries of the two stars, but lacking adequate reference stars,
calculated their differential photometry using each member of the binary as a
reference for the other. Ultimately, they were not able to attribute any
photometric variability to one star or the other. Because of this, we
collected new light curves for these two targets.

We obtained new photometric light curves for both HD79210 and HD79211, with
the aim of determining their stellar rotation periods. We took images using
the KeplerCam wide-field CCD camera on the 1.2 m telescope at the Fred
Lawrence Whipple Observatory (FLWO) on Mount Hopkins, Arizona. The 4096 X
4096, 15-micron pixels format provides a 23.1 arcmin square field of view with
a resolution of 0.338 arcsec per pixel (Szentgyorgyi et al., 2005) and our
images were binned by two.

From February until June 2021, we took a total of 6081 images of HD79210 and
HD79211 using the B-band filter on KeplerCam. The exposure time of each image
was 2 seconds. We reduced the raw images, first by stitching together the four
individual images from each quadrant of the detector (Carter et al., 2011) and
then performing bias subtraction and flat-field correction. We performed
photometry using AstroImageJ (AIJ) (Collins et al., 2017). We used AIJ’s
variable radius, multi-aperature photometry function, by which AIJ determines
the aperture radius from an azimuthally averaged radial profile, centered on
the user-defined aperture. It then determines the net integrated counts within
the object aperature, as well as the average value of the pixels in the user-
defined sky annulus, not including background pixels that are more than two
sigma above the average background pixel value (Collins et al., 2017), and
returns the difference between those values as the Source-Sky counts. AIJ also
calculates an error value on the Source-Sky counts, which includes
contributions from read-out noise, dark current, and source and sky Poisson
noise as defined by Merline & Howell (1995).

We used AIJ to calculate the Source-Sky counts and error on those measurements
for our two targets, HD79210 and HD79211, as well as three comparison stars
found within the field: HD233614, HD79450 and TYC 3806-1026-1. We present
three sets of relative photometry: that of HD79210 calculated using TYC
3806-1026-1 as a comparison star, that of HD79211 calculated using TYC
3806-1026-1 as a comparison star, and that of HD79211 calculated using HD79210
as a comparison star (see Section 4 for more information). We opted to combine
the multiple exposures taken over the course of the night into nightly
measurements. The resulting light curves, after sigma clipping outlier points,
are shown in Figure 2.

Figure 2: Relative photometry for HD79210 using a comparison star (orange),
relative photometry for HD79211 using a comparison star (blue), and relative
photometry for HD79211 using HD79210 as a comparison star (green), plus an
offset, as taken with KeplerCam. Note the different y-axis scale between the
two separate light curves in the upper panel and the combined light curve in
the lower panel. The faint, round points represent the relative flux
measurement from each individual image. The darker, star-shaped points
represent the nightly averaged relative flux. These average, nightly fluxes
are what we used when calculating the periodograms (Figure 3). These two
separate light curves are highly affected by systematics, which we discuss in
detail in Section 4.

###  2.6 Literature Photometry

As with the time series surveys discussed in Section 2.5, HD79210 and HD79211
are blended in many past photometric surveys as well, due to their small
separation on the sky. In some surveys, such as WISE, these two stars are
blended beyond separability. We opt not to quote the magnitudes for the
blended source here. In other surveys, such as GALEX, 2MASS and SDSS, the
photometric values suffer from some amount of blending or diffraction spike
confusion which has been corrected in post-processing, and magnitudes for
these objects are reported in those survey catalogues. In even higher angular
resolution surveys, namely Hipparcos and Tycho, Gaia, and USNO, the two stars
are resolved. We have listed all available photometric values in Table B1,
noting those that come from surveys in which the two stars were originally
blended.

##  3 Stellar Characterization

The HD79210/HD79211 binary is located 6.332 parsecs from Earth (Gaia
Collaboration et al., 2020). These two stars are very similar to one another
and are in many ways twins. They are nearly identical in mass, radius and
effective temperature according to literature measurements (see Table 1),
varying by only a few percent at most. HD79210 had been classified as a K7V
star (Kirkpatrick et al., 1991), but more recently has been classified as an
M0V star, like HD79211 (Alonso-Floriano et al., 2015).

In Table 1, we summarize the previously published parameters for these two
stars. For the majority of the parameters, we cite the same sources used by
González-Álvarez et al. (2020), with one addition. These two stars have since
been included in Sarmento et al. (2021)’s sample of 313 M dwarf stars, for
which they derived $T_{\text{eff}}$ and metallicity using H-band APOGEE
spectra.

For our investigation, we attempted a number of different methods to calculate
the stellar parameters for the two stars in this system, namely Stellar
Parameter Classification (SPC) (Buchhave et al., 2012, 2014), isochrone
fitting (Morton, 2015; Mortier et al., 2020), empirical color-parameter
relations (Benedict et al., 2016; Boyajian et al., 2012; Mann et al., 2015)
and spectral energy distribution (SED) fitting (Stassun & Torres, 2016).
Ultimately, we decide to use the literature values for the stellar parameters
(Table 1) in our analysis, for the following reasons. SPC does not produce
reliable results for these targets as they are at the edge of the range of
stellar effective temperatures for which SPC is calibrated. The isochrone
fitting procedure takes the SPC-derived effective temperature and metallicity
as inputs, as well as the flagged 2MASS photometry, making the isochrone
results similarly unreliable. HD79210 and HD79211 fall at or beyond the upper
range of stellar masses, depending on the true mass of the stars, for which
the mass-luminosity relationship (Boyajian et al., 2012) was calibrated. The
color-temperature relationship (Mann et al., 2015) also relies on the flagged
2MASS photometry.

Finally, we determined the stellar masses, radii and effective temperatures
via spectral energy distribution (SED) fitting, following the procedure in
Stassun & Torres (2016). These results were the least consistent with the
other methods and the previously published values, finding that the stars are
cooler, more metal-poor and have larger radii than otherwise measured. This
could have an astrophysical origin: low-mass stars in much tighter, eclipsing
binaries ($P<10$ days) have been shown to have larger radii and cooler
temperatures than predicted by models. Current theory explains that tidal
effects between the two members of the binary cause the stars to rotate
quickly and be more active. Either through magnetic fields suppressing
convective energy transport or high spot coverage lowering the average
temperature of the stellar surface and forcing a larger radius to conserve
energy, the stars end up being larger and cooler than otherwise predicted
(Ribas et al. (2008) and the references therein). These stars’ wide binary
separation, lack of evidence of fast rotation and other activity indicators
not pointing toward them being extremely active, however, do not support this
explanation of radius inflation and temperature suppression. More likely, the
contamination between the stars in their photometry is causing an unreliable
SED fit. For these reasons, we decide not to report the stellar parameters
determined using these various methods, and opt use the literature values for
the stellar parameters (Table 1) in our analysis.

Table 1: Stellar parameters for HD 79210 and HD 79211 found in the literature. These are the values that we ultimately use for fitting the radial velocities and deriving the parameters of the planet candidate. In the cases where multiple values are listed for a single parameter, * denotes the value adopted in this work. Parameter | HD 79210 | HD 79211 | Ref.
---|---|---|---
RA [deg] | 138.5835616152243 | 138.5913117966687 | Gaia Collaboration et al. (2016)
DEC [deg] | 52.68408016691263 | 52.68342944184038 | Gaia Collaboration et al. (2016)
Spectral type | M0V | M0V | Alonso-Floriano et al. (2015)
Distance [pc] |  6.332 $\pm$ 0.002 |  6.332 $\pm$ 0.002 | Gaia Collaboration et al. (2020)
Parallax [mas] |  157.8879 $\pm$ 0.0197 |  157.8825 $\pm$ 0.0211 | Gaia Collaboration et al. (2020)
$\mu_{\alpha}$ cos $\delta$ [mas a-1] |  -1545.787 $\pm$ 0.018 |  -1573.040 $\pm$ 0.018 | Gaia Collaboration et al. (2020)
$\mu_{\delta}$ [mas a-1] |  -569.053 $\pm$ 0.018 |  -659.906 $\pm$ 0.019 | Gaia Collaboration et al. (2020)
U [ km s-1] |  -42.20 $\pm$ 0.36 |  -44.01 $\pm$ 0.36 | Cortes-Contreras et al. (2016)
V [ km s-1] |  -14.99 $\pm$ 0.10 |  -17.44 $\pm$ 0.10 | Cortes-Contreras et al. (2016)
W [ km s-1] |  -23.73 $\pm$ 0.34 |  -23.10 $\pm$ 0.34 | Cortes-Contreras et al. (2016)
Eff. temp., Teff [K] |  4001 $\pm$ 100* |  4014 $\pm$ 100* | Sarmento et al. (2021)
|  4024 $\pm$ 51 |  4005 $\pm$ 51 | Schweitzer et al. (2019)
Surface grav, $\log g$ [cgs] |  4.68 $\pm$ 0.07 |  4.68 $\pm$ 0.07 | Schweitzer et al. (2019)
Metallicity, $\rm[M/H]$ [dex] |  4.71 $\pm$ 0.1 |  4.63 $\pm$ 0.1 | Sarmento et al. (2021)
Metallicity, $\rm[Fe/H]$ |  -0.05 $\pm$ 0.16 |  -0.03 $\pm$ 0.16 | Schweitzer et al. (2019)
Luminosity [$L_{\odot}$] |  0.0789 $\pm$ 0.0038 |  0.0792 $\pm$ 0.0031 | Schweitzer et al. (2019)
Mass [$M_{\odot}$] |  0.69 $\pm$ 0.07* |  0.64 $\pm$ 0.07* | González-Álvarez et al. (2020)
|  0.591 $\pm$ 0.047 |  0.596 $\pm$ 0.042 | Schweitzer et al. (2019)
Radius [$R_{\rm\odot}$] |  0.58 $\pm$ 0.02 |  0.58 $\pm$ 0.03 | Schweitzer et al. (2019)
v sin i [km s-1] |  2.9 $\pm$ 1.2 |  2.3 $\pm$ 1.5 | Glebocki & Gnaciński (2005); Reiners et al. (2018)
$P_{rot}$ [days] |  16.3${}^{+3.5}_{-1.3}$ |  16.61 $\pm$ 0.04 | González-Álvarez et al. (2020)
Age [Gyr] | 1-7 | 1-7 | González-Álvarez et al. (2020)
vmic [ km s-1] | 4.71 | 4.63 | Sarmento et al. (2021)
vmac [ km s-1] | -0.06 | -0.11 | Sarmento et al. (2021)

##  4 Light Curve Analysis

We present three sets of relative photometry for these stars: that of HD79210
calculated using TYC 3801-1026-1 as a comparison star, that of HD79211
calculated using TYC 3801-1026-1 as a comparison star, and that of HD79211
calculated using HD79210 as a comparison star. There were three comparison
stars in the field of our observations, all of which are at least two orders
of magnitude fainter than the target stars (B magnitudes of 9.92, 9.33, 11.55
in comparison to HD79211’s B magnitude of 7.966) and are different spectral
types (all are F stars, as opposed to the targets, which are M0s) (Høg et al.,
2000). We decided to use TYC 3801-1026-1 as our comparison star when
calculating the separate relative photometry for HD79210 and HD79211, because
it best corrected for the effect of changing airmass over the course of our
observations.

There were a number of nights of observations that we opted not to use from
our KeplerCam photometric measurements. The seven nights of observation
between March 21, 2021 and March 29, 2021 were significantly offset in both
relative and absolute flux from the rest of the nights’ fluxes for both
targets, likely due to moon contamination. Since we were not able to correct
for this offset in the relative photometry using the available comparison
stars, we decided to exclude these nights from of our analysis. We also opted
not to use two other nights, April 4th and April 13th, 2021, because the
seeing changed significantly over the course of the night, resulting in
unreliable flux measurements.

The resulting light curves from the two stars (Figure 2, in orange and blue)
and their periodograms (Figure 3, upper two panels) clearly show the influence
of systematics. Even by eye, the time variations of these two light curves
appear to be identical, indicating that they are the results of systematics
affecting the images from which both stars’ light curves were reduced. We rule
out the far less likely scenario that the two stars were undergoing identical
variation during the time of our observations. Due to the available comparison
stars being bluer and fainter than our targets, these systematics persist
despite using other stars in the field for calibration.

Although the other stars in the field are poorly-suited comparisons for
HD79210 and HD79211, each target serves as an ideal comparison for the other,
because of their similar masses, shared spectral type, and close proximity on
the sky. We calculated relative photometry of HD79211 using HD79210 as a
comparison (Figure 2, in green), which corrects for the systematics found in
the other light curves. A periodogram of this combined light curve shows a
statistically significant ($<0.1\%$ FAP) peak at a period of 17.34 days and
frequency of $0.057\pm 0.003\text{ days}^{-1}$ (Figure 3, bottom panel).
Alone, we cannot attribute this periodicity to one star or the other. A nearby
peak, however, at 17.74 days / $0.056\pm 0.003\text{ days}^{-1}$ is present in
the periodogram of HD79211’s separate light curve but not in HD79210’s
separate light curve. Although this 17.74 day peak is not statistically
significant, its presence suggests that this approximately 17.5 day
periodicity originates in HD79211’s photometric variability. We attribute this
variability to HD79211’s rotation period.

Figure 3: Lomb-Scargle periodogram of the nightly-averaged relative fluxes for
HD79210 using a separate comparison star (top), HD79211 using a separate
comparison star (middle) and HD79211 using HD79210 as a comparison star
(bottom). The vertical, grey dashes note the shared peaks between the two
stars’ periodograms, which are likely caused by systematics in the images. The
statistically significant ($<0.1\%$ FAP) peak in the bottom periodogram is
marked with the dotted green line, and the shaded region marks one standard
deviation around the peak (P=17.34 days, freq $=0.057\pm 0.003\text{
days}^{-1}$). This peak corresponds to the one peak in HD79211’s periodogram
which is not present in that of HD79210, marked with the blue dotted line in
the middle panel, at 17.74 days (freq $=0.056\pm 0.003\text{ days}^{-1}$).
Although the 17.74 day peak is not statistically signficant, this suggests
that this photometric variability originates in HD79211, and we attribute it
to this star’s rotation period.

##  5 Radial Velocity Analysis

###  5.1 Stellar Binary Trend Removal

The stellar binary, with its 1300 year period and nearly 1 km/s amplitude,
introduces a significant RV trend to HD79210 and HD79211. Following (González-
Álvarez et al., 2020), we tried approximating the stellar binary trend as a
line, but found that a line fit did not capture the curvature introduced by
extending our RV time baseline with the addition of the HIRES and HARPS-N
datasets. We ultimately opted for modeling the stellar binary as a second-
order polynomial, fit to the combined HARPS-N, CARMENES and HIRES data set
(Figures 1, A1). In order to find correlations between the HARPS-N RVs and the
various activity indicators (Section 5.2) and calculate periodograms of the
radial velocities (Sections 5.3, 5.4), we subtracted offsets between these
three datasets and the binary polynomial trend. We used RadVel to fit for
these offsets and binomial parameters (Fulton et al., 2018).

When fitting the RVs to find the planetary parameters, we chose to fit a
polynomial trend (to model the binary trend), a Keplerian (to model the
planet) and Gaussian Processes (GPs, to model stellar activity)
simultaneously. We did this using PyORBIT (Malavolta, 2016), which allows the
user to specify which datasets are use to fit which models – allowing us to
fit the binary trend using the combined HARPS-N, HIRES and CARMENES datasets,
while varying which datasets contributed to the Keplerian and GP fits (Section
5.5).

###  5.2 HARPS-N RV Correlation with Stellar Activity Signatures

The HARPS-N stellar activity indicators were calculated as described in
section 2.1. We calculate the Pearson correlation coefficients ($r$) for the
HARPS-N radial velocities and activity indicators using SciPy’s pearsonr
function (Oliphant, 2007) for HD79210 and HD79211 (Figures A2 and 4,
respectively). We define a moderate correlation as $0.5>r\geq 0.3$ and a weak
correlation as $r<0.3$. HD79211’s radial velocities are weakly correlated with
all activity indicators. Radial velocities from HD79210, however, are
moderately correlated with FWHM and weakly correlated with the rest.

Figure 4: Various HARPS-N stellar activity indicators versus HD79211’s radial
velocities after the stellar binary trend has been subtracted. The r-values
are Pearson correlation coefficients. All of these parameters are weakly
correlated, with r-values less than 0.3.

###  5.3 Periodograms of the White Light HARPS-N RVs

Periodograms of the HARPS-N RVs of HD79210 and HD79211 with the binary trend
removed, calculated using Astropy’s LombScargle function (The Astropy
Collaboration et al., 2018), are shown in Figures A3 and 5, respectively. The
False Alarm Probabilities (FAPs) are calculated via bootstrap simulations. The
periodogram of HD79211’s radial velocities reveals signals with less than
0.01% FAP at the following periods: 24.41 and 24.76 days. The signal at 24.41
days is the most significant and we attribute it to the planet candidate. When
plotted with the periodograms of the various stellar activity indicators and
the window function (Figure 6), we see that these signals in the RV
periodograms do not correspond with peaks in the stellar activity indicators.
We attribute the other significant peak, at 24.76 days to an alias of the 1550
day peak in the window function interacting with the 24.41 day peak (Figure
7). Aliases can appear in periodograms at frequencies equal to the true
frequency of a signal, in this case 1/24.4 days, plus or minus the frequency
in the window function caused by the data sampling, in this case 1/1550 days.
We support this interpretation by plotting the periodogram of the best-fit
Keplerian planetary orbit over that of the data with the binary trend removed
in Figure 7. While the uncertainty of the data and the effects of stellar
activity prevent the model and data periodograms from matching precisely, this
shows that we are capable of detecting a 24.42 day signal with the observing
cadence of our data, and that many of the aliases in our data correspond to
those in the model. The periodogram of HD79210’s RVs, after the binary trend
is subtracted, does not reveal any signals with less than a 0.01% FAP (Figure
A3).

We also present the stacked Bayesian General Lomb-Scargle periodogram (Figure
8, calculated via the procedure in Mortier & Collier Cameron (2017)). This
stacked periodogram shows that the 24.41 day signal becomes stronger as more
observations are added, as we would expect for a planet signal. We also note
that the approximately 24.4 day periodic signal is present in the periodogram
of HD79211’s RVs regardless of how we corrected for the binary trend, whether
as a line, Keplerian or as a second-order polynomial, as we are showing here.
We suspect that the stellar rotation period is not present as a significant
signal in these periodograms because, over the course of the observations, the
magnetically active regions of the star evolved such that the stellar rotation
fell out of phase.

Figure 5: Periodograms of HARPS-N radial velocities of HD79211, without the
binary trend removed (top) and with the binary trend removed (bottom). Signals
with frequencies from 0 to 0.33 $\text{ days}^{-1}$ are plotted. Signals with
False Alarm Probabilities less than 0.1% are marked. Before the binary trend
is removed, there are many significant low frequency signals (blue shaded
region), as we would expect from the long period binary. Two signals with FAPs
less than 0.01% are marked for HD79211 once the binary trend is removed, at
24.41, and 24.76 days. The signal at 24.41 days is attributed to the planet
candidate, and has the highest power of the present peaks.  Figure 6:
Periodograms of HD79211’s white light HARPS-N radial velocities with the
binary trend removed, activity indicators, and the window function. All of
significant peaks ($<0.01\%$ FAP) are marked with dashed vertical lines. The
most significant peak is at 24.41 days, which we attribute to the planet
candidate. We attribute the other significant peak, at 24.76 days, to aliases
of the planet candidate signal (see Figure 7). Figure 7: Zoomed in periodogram
of the HD79211 white light HARPS-N RVs, highlighting the strongest peak in the
periodogram at 24.41 days, and the aliases that result in its interaction with
the 365 day and 1550.8 day peaks in the window function. The periodogram
calculated from the best fit Keplerian planet orbit, sampled with the
observing cadence of the HARPS-N data, is plotted in light blue. There is
variation between the periodograms of the model and the data, caused by the
data’s uncertainties and the influence of stellar activity in the data, but
much of the aliasing structure can be seen in both periodograms. The 24.76 day
peak (above the 0.01% FAP line) can be explained as an alias. Figure 8:
Stacked Bayesian Generalized Lomb Scargle periodograms (SBGLS) for the HD79211
HARPS-N white light radial velocities, with the binary trend removed. The
horizonal axis is the frequency of the signal, the color is the power and the
vertical axis shows how the periodogram changes as observations are added to
the calculation. This periodogram is oversampled by a factor of 5. The same
peaks are highlighted from the 2D periodogram, Figure 6. The strongest peak at
24.41 days gets stronger as more observations are added, as we would expect
for a planet signal.

###  5.4 Periodograms of the Chromatic HARPS-N RVs

The significant peaks from the periodograms of the white light HARPS-N radial
velocities are also highlighted in the periodograms of the chromatic radial
velocities (Figure 9). Both signals from the white light RVs are present in
these chromatic periodograms, with increasing significance as we look to the
redder RVs. Because this signal is not larger in the bluer wavelengths, as we
would expect if the signal were caused by stellar activity, we do not take
this as clear evidence that the 24.41 day signal is caused by stellar
activity. We investigate the variation in the amplitude of the 24.41 day
signal by fitting each set of chromatic radial velocities using PyORBIT, and
discuss those results in Section 5.5.

Figure 9: Periodograms of the three chromatic HARPS-N RV sets and the window
function. The top panel shows chrom1 RVs (calculated using the bluest portion
of the spectrum), followed by chrom2, and chrom3 in the lowest RV panel
(calculated using the reddest portion of the spectrum). The window function is
shown in the bottom panel. The same significant peaks that are marked in the
white light RV periodogram (Figure 6) are marked here with vertical dashed
lines. Both signals are present in these chromatic periodograms, with
increasing significance as we look to the redder RVs. Because this signal is
not larger in the bluer wavelengths, as we would expect if the signal were
caused by stellar activity, we do not take this as evidence that the 24.41 day
signal is caused by stellar activity.

###  5.5 Radial Velocity Fits

To determine the planetary parameters, we fit the radial velocities via an
MCMC fitting routine using PyORBIT (Malavolta, 2016). We fit the data with a
second order polynomial to model the stellar binary, a Keplerian to model the
planet candidate, GPs to model stellar activity, as well as offset and jitter
parameters for all of the datasets. As described in Section 2.1, we
simultaneously fit a second order polynomial (to model the binary trend) to
the combined HARPS-N, CARMENES and HIRES datasets, while fitting GPs (to model
the stellar activity) and a Keplerian (to model the planet) to various
combinations of the three datasets. We used this procedure to fit for a planet
signal in the data of HD79210 and HD79211, but were not able to identify any
planet candidates in the HD79210 data. In this section, we present the
resulting best-fit parameters for the planet candidate around HD79211.

Using PyORBIT (Malavolta, 2016), we fit the HARPS-N RVs of HD79211 with the
priors described in the appendix (Section A). We performed similar fits for
HD79210 and were not able to find any planet signals. We report the results of
six fits for HD79211: fitting just the HARPS-N radial velocities, fitting the
combined HARPS-N + CARMENES RVs, and fitting the combined HARPS-N + CARMENES +
HIRES RVs, with both a circular and an eccentric orbit and with GPs to model
stellar activity. The priors and results of our fits to the RVs from HD79211
can be found in Table 2 and the phase-folded best-fit models are shown in
Figure 10. The results of all of these runs are consistent within their quoted
uncertainties

We adopt the results of fitting the HARPS-N + CARMENES dataset with an
eccentric orbit as our final results for the planet candidate around HD79211
(full posteriors shown in Figure A5). This is the model favored by an AIC
model comparison. Although the results of fitting the combination of all three
datasets are consistent with those of fitting the HARPS-N + CARMENES dataset,
an aliasing effect caused by a peak in the window function which is unique to
the HARPS-N + CARMENES + HIRES dataset causes the posterior of the planet
period to be double-peaked, at 24.44 and 24.38 days. Ultimately, we identify a
signal with a period of $24.422\pm 0.014$ days and attribute it to a planet
candidate orbiting HD79211, with an $M$ sin $i$ of $10.6\pm 1.2M_{\oplus}$ and
$a=0.142\pm 0.005$ au (Figure 11).

Figure 10: Phase-folded, best-fit Keplerian orbital model, after the GPs and
binary star trend have been removed, as well as their residuals. The top row
shows the best-fit model to the HARPS-N data alone, the middle row shows the
combined HARPS-N + CARMENES dataset, and the bottom row shows the HARPS-N +
CARMENES + HIRES dataset. The left hand column shows the circular fits to
these datasets and the right hand column shows the corresponding eccentric
fits. The blue line is the best-fit model with the orbital parameters printed
in the legend and listed in Table 2. Red circles are the same velocities
binned in 0.1 units of orbital phase. The middle, right hand panel, marked
with a bold border, shows our final, adopted parameters for the planet
candidate. Figure 11: Posterior distributions of the combined HARPS-N and
CARMENES dataset for HD79211b’s parameters derived from fitting an eccentric
orbit.

We also fit the chromatic RVs (described in section 2.1) using RadVel, to see
if the semi-amplitude of the signal in HD79211 varies with the wavelength of
light used to calculate the radial velocities. Fixing the parameters and
hyperparameters except for $K_{b}$ (i.e. $P_{b}$, $e_{b}$, $T_{conj}$, $Hamp$,
$Pdec$, $Prot$, $Oamp$, $\sigma_{HN}$, c1, c2, x zero) to the best-fit values
found from fitting the white-light HARPS-N DRS RVs, we fit the chromatic light
curves and compare their semi-amplitudes. Note that we used the HARPS-N RVs as
calculated by the DRS, not by HARPS-TERRA, to find these parameters. These
results are shown in Figure 12. We found that the semi-amplitudes were
consistent, within errorbars, across the chromatic RV sets and in comparison
to the white light semi-amplitude. Although we caution against over
interpreting these results, we could expect stellar activity to cause stronger
signals in bluer light and smaller signals in redder light, whereas we expect
a planet signal to be consistent across colors.

Figure 12: We fit the chromatic radial velocities using RadVel, fixing all of
the parameters and hyperparameters except for $K_{b}$ to the best-fit values
found from fitting the white-light HARPS-N DRS RVs (the white light
counterpart to the chromatic RVs), not the HARPS-TERRA RVs that we use in the
rest of this work. Here, we plot the resulting $K_{b}$ versus the wavelength
band used to calculate those radial velocities. The white light RV result from
fitting the HARPS-N DRS RVs is noted by the black point. All of these values
agree within their errorbars, and they do not show the trend of increasing
semi-amplitude with decreasing wavelength that we would expect of a signal
caused by stellar activity. Table 2: RV fits for three sets of HD79211 RVs
using PyORBIT. We fit HARPS-N RVs alone, HARPS-N + CARMENES RVs and HARPS-N +
CARMENES + HIRES RVs with both eccentric and circular orbits. We adopt the
results of fitting the HARPS-N + CARMENES RVs with an eccentric orbit as our
final results. U in the prior column denotes a Uniform prior and G denotes a
Gaussian prior.

|  |  |  |  |  | HARPS-N + | HARPS-N +
---|---|---|---|---|---|---|---
|  | HARPS-N | HARPS-N | HARPS-N + | HARPS-N + | CARMENES + | CARMENES +
Parameter | Prior | Only | Only | CARMENES | CARMENES* | HIRES | HIRES
|  | $e=0$ | $e<0.3$ | $e=0$ | $e<0.3$ | $e=0$ | $e<0.3$
Planet Orbit |  |  |  |  |  |  |
$P_{b}$ (days) | U: 10-50 | $24.426_{-0.016}^{+0.015}$ | $24.421^{+0.016}_{-0.017}$ | $24.425_{-0.014}^{+0.013}$ |  $24.422\pm 0.014$* | $24.438_{-0.012}^{+0.009}$ | $24.435_{-0.019}^{+0.011}$
$K_{b}$ (m/s) | U: 0.01-10 | $3.68\pm 0.50$ | $3.71^{0.52}_{-0.51}$ | $3.19\pm 0.27$ |  $3.19\pm 0.27$* | $3.14\pm 0.27$ | $3.14\pm 0.27$
$e_{b}$ | Varies | $\equiv 0.0$ | $0.142^{+0.113}_{-0.100}$ | $\equiv 0.0$ |  $0.109_{-0.075}^{+0.100}$* | $\equiv 0.0$ | $0.097_{-0.067}^{+0.096}$
$T\rm{conj}_{b}$ (JD-2.4e6) | G: $57517.06\pm 6.15$ | $57522.08_{-0.54}^{+0.52}$ | $57521.72^{+1.02}_{-1.38}$ | $57521.99_{-0.36}^{+0.35}$ |  $57521.43_{-0.90}^{+0.72}$* | $57521.81\pm 0.35$ | $57521.34_{-0.83}^{+0.66}$
Derived |  |  |  |  |  |  |
$a_{b}$ (au) | - | $0.142\pm 0.005$ | $0.142\pm 0.005$ | $0.142\pm 0.005$ |  $0.142\pm 0.005$* | $0.142\pm 0.005$ | $0.142\pm 0.005$
$M_{b}$ sin $i(M_{\oplus})$ | - | $12.3_{-1.9}^{+2.0}$ | $12.3^{+2.0}_{-1.8}$ | $10.7\pm 1.2$ |  $10.6\pm 1.2$* | $10.6\pm 1.2$ | $10.4\pm 1.2$
Gaussian Process |  |  |  |  |  |  |
Hamp HN (m/s) | - | $4.00_{-0.65}^{+0.82}$ | $4.03^{+0.85}_{-0.68}$ | $3.79_{-0.62}^{+0.77}$ |  $3.74_{-0.62}^{+0.76}$* | $3.70_{-0.61}^{+0.75}$ | $3.67_{-0.61}^{+0.74}$
Hamp CAR (m/s) | - | - | - | $3.71_{-0.70}^{+0.94}$ |  $3.75_{-0.71}^{+0.97}$* | $3.70_{-0.70}^{+0.95}$ | $3.72_{-0.72}^{+0.96}$
Hamp HIRES (m/s) | - | - | - | - | - | $5.16_{-2.36}^{+1.57}$ | $5.23_{-2.44}^{+1.54}$
Pdec (days) | U: 15-1000 | $180_{-68}^{+69}$ | $197_{-76}^{+89}$ | $200_{-40}^{+47}$ |  $203_{-43}^{+49}$* | $209_{-43}^{+49}$ | $213_{-45}^{+51}$
Prot (days) | U: 16.419-18.623 | $16.70_{-0.09}^{+0.22}$ | $16.75_{-0.12}^{+0.29}$ | $16.60\pm 0.05$ | $16.58_{-0.06}^{+0.05}*$ | $16.59\pm 0.05$ | $16.59\pm 0.05$
Oamp | G: 0.5$\pm$0.05 | $0.48\pm 0.05$ | $0.48\pm 0.05$ | $0.46\pm 0.05$ |  $0.46\pm 0.05$* | $0.46\pm 0.05$ | $0.46\pm 0.05$
Binary Trend |  |  |  |  |  |  |
c1: | - | $-0.01\pm 0.001$ | $-0.01\pm 0.001$ | $-0.009\pm 0.001$ |  $-0.01\pm 0.001$* | $-0.002\pm 0.001$ | $-0.009\pm 0.001$
c2 (e-07): | - | $-1.86_{-1.17}^{+1.14}$ | $-1.94_{-1.16}^{+1.13}$ | $-1.04_{-1.25}^{+1.23}$ |  $-1.06_{-1.26}^{+1.21}$* | $-.46_{-1.40}^{+1.33}$ | $-.54_{-1.45}^{+1.35}$
x zero (JD-2.4e6): | - | 57773.91 | 57871.94 | 57871.94 | 57871.94* | 57773.91 | 57773.91
Offset and Jitter |  |  |  |  |  |  |
Off HN (m/s): | - | $0.63_{-1.12}^{+1.25}$ | $-0.38_{-1.14}^{+1.26}$ | $-0.59_{-1.09}^{+1.13}$ |  $-0.61_{-1.07}^{+1.12}$* | $0.22_{-1.10}^{+1.14}$ | $0.23_{-1.09}^{+1.12}$
Off CAR (m/s): | - | $0.81\pm 0.37$ | $-0.20\pm 0.36$ | $-0.19_{-1.50}^{+1.51}$ |  $-0.17_{-1.52}^{+1.54}$* | $0.72_{-1.50}^{+1.52}$ | $0.74_{-1.52}^{+1.55}$
Off HIRES (m/s): | - | $-46.49\pm 2.59$ | $-47.59_{-2.67}^{+2.64}$ | $-45.93_{-2.90}^{+2.81}$ |  $-46.06_{-2.82}^{+2.86}$* | $-45.42_{-3.21}^{+3.19}$ | $-45.43_{-3.23}^{+3.17}$
Jit HN (m/s): | - | $1.47_{-0.19}^{+0.20}$ | $1.49_{-0.19}^{+0.20}$ | $1.51_{-0.18}^{+0.20}$ |  $1.53_{-0.19}^{+0.20}$* | $1.54_{-0.18}^{+0.20}$ | $1.55_{-0.18}^{+0.20}$
Jit CAR (m/s): | - | $3.88_{-0.28}^{+0.30}$ | $3.88_{-0.28}^{+0.30}$ | $1.66\pm-0.28$ |  $1.64\pm 0.28$* | $1.67\pm 0.28$ | $1.65_{-0.27}^{+0.28}$
Jit HIRES (m/s): | - | $5.60_{-0.73}^{+0.91}$ | $5.58_{-0.72}^{+0.89}$ | $5.63_{-0.73}^{+0.89}$ |  $5.63_{-0.73}^{+0.90}$* | $3.02_{-1.88}^{+2.13}$ | $2.99_{-1.91}^{+2.16}$

* Adopted fit values

##  6 Results and Discussion

We present the results of analyzing HARPS-N, CARMENES and HIRES radial
velocities from HD79210 and HD79211. We ultimately conclude that there likely
is a planet orbiting HD79211, with a period of $24.422\pm 0.014$ days, semi-
amplitude of $3.19\pm 0.27$ m/s, $M$ sin $i=10.6\pm 1.2M_{\oplus}$, and
$a=0.142\pm 0.005$ au, and find no evidence of any planet candidates around
HD79210.

There are discrepancies between the periodograms of HD79211’s radial
velocities from HARPS-N alone (Figure 5) and CARMENES alone (González-Álvarez
et al., 2020). Periodograms of the CARMENES RVs show three peaks significant
above the 0.1% FAP level at 8.3, 24.4 and 16.6 days, explained by González-
Álvarez et al. (2020) as a harmonic of the stellar rotation period, the
planet’s orbital period and the stellar rotation period, respectively. The
periodograms of the HARPS-N RVs, however, show two significant peaks above the
0.01% FAP level at 24.41 and 24.76 days. We suspect that these discrepancies
are caused by the fluctuation in stellar activity between seasons. Due to the
low time-density of HARPS-N data, however, we are not able to isolate the
HARPS-N data from the seasons where the two datasets overlap in order to
perform a direct comparison.

All of our RV fits (Table 2) found a periodic signal at $\approx 24.4$ days,
with all parameters agreeing within their errorbars. Ultimately, this work
supports the detection of the 24.4 day planet candidate around HD79211
originally published by González-Álvarez et al. (2020), and finds no
additional candidates around either HD79211 or its binary companion HD79210.
As discussed in that work, this planet candidate is one of the lowest mass
planets discovered orbiting one member of a stellar binary with a semi-major
axis below 400 au. It likely lies on the inner edge of its star’s habitable
zone, but it is likely non-transiting, with only a $5^{+2}_{-1}\%$ chance that
it is transiting (González-Álvarez et al., 2020). Even so, with these two
stars’ borderline-wide separation of a=130 au, this system can serve as a
valuable datapoint in future studies of exoplanet formation and occurance
around stellar binaries.

## Acknowledgements

This material is based upon work supported by the National Science Foundation
Graduate Research Fellowship under Grant No. DGE1745303. The HARPS-N project
was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard-
University Origin of Life Initiative (HUOLI), the Scottish Universities
Physics Alliance (SUPA), the University of Geneva, the Smithsonian
Astrophysical Observatory (SAO), the Italian National Astrophysical Institute
(INAF), University of St. Andrews, Queen’s University Belfast, and University
of Edinburgh. Parts of this work have been supported by the National
Aeronautics and Space Administration under grant No. NNX17AB59G, issued
through the Exoplanets Research Program. Parts of this work have been
supported by the Brinson Foundation. R.D.H. is funded by the UK Science and
Technology Facilities Council (STFC)’s Ernest Rutherford Fellowship (grant
number ST/V004735/1). T.G.W and A.C.C acknowledge support from STFC
consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant
ST/R003203/1. This work has made use of data from the European Space Agency
(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia
Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has
been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement.

##  Appendix A Selection of Priors for Radial Velocity Fits

When fitting for a planet candidate around HD79211, we used the time of
conjunction for the 24.4 day planet candidate published in González-Álvarez et
al. (2020) as our Gaussian prior (2457517.06 $\pm$ 6.15 days). We ran both
circular-orbit fits and eccentric fits. We started with a wide prior on
eccentricity ($e<0.8$), but found that it favored highly eccentric and
physically unlikely orbits, resulting from fitting a gap in data with the peak
RV. We then narrowed to $e<0.3$. We kept the prior on our semi-amplitude
($K_{b}$) wide throughout our fits, with a Jeffery’s prior from 0.01-10 m/s.

We initially set a wide, uniform prior on orbital period (3-50 days), which
resulted in a double-peaked posterior, with one peak tending toward the lower
end of this prior range and another at around $\approx 25$ days. After
constraining the orbital period to the lower range, we found that the lower
peak resulted from the code trying to fit a one day periodic signal which
originates in the window function. We then opted to increase the lower bound
of our orbital period prior (uniform prior from $10$-$50$ days), preventing
the MCMC from fitting that one-day periodicity.

In our fits using Gaussian processes to model stellar activity, we used a
quasi-periodic kernel with four hyperparameters: variability amplitude (Hamp),
non-periodic characteristic length (associated with the spot decay timescale,
Pdec), variability period (associated with the stellar rotation period, Prot)
and periodic characteristic length (associated with the number of spots/spot
regions on the surface of the star, Oamp).

We set a wide uniform prior on Pdec from 15.0-1000.0 days. The lower limit is
associated with the approximate lower limit on the estimated rotation period
of the star, since if the stellar magnetically active regions are evolving
more quickly than the star is rotating, we would not see a periodic signal at
all. The upper limit is many times the rotation period of the star, to allow
for a fit to stable, long-lived magnetically active regions on the star.

We then set a uniform prior on Prot from 16.419-18.623 days, restricting this
value to the one-standard deviation range around the peaks in the periodograms
of the light curves for HD79211 (see Section 4). We set a Gaussian prior of
$0.5\pm 0.05$ on Oamp (Jeffers & Keller, 2009; Haywood et al., 2018). This
accounts for the fact that the photometric and RV variability effect of even
highly complex spot distributions on a star will average out to those caused
by two or three large spots on the visible surface of the star.

When fitting the chromatic HARPS-N radial velocities, we aim to detect
differences in the semi-amplitude of the periodic signal at the suspected
planet’s period. To do this, we decided to fix all of the free parameters -
$T_{conj}$, $P_{b}$, Hamp, Pdec, Prot, Oamp, c1, c2, x zero - to the best-fit
values returned from fitting the white-light HARPS-N DRS and CARMENES joint
data set. Note that, for this step, we used the HARPS-N RVs as calculated by
the DRS (which are the white light counterpart to the chromatic radial
velocities), and not those calculated by HARPS-TERRA, to find these
parameters. Although we do expect the chromatic nature of stellar activity to
cause changes in the amplitude of the stellar activity signal (Hamp) between
chromatic sets of RV data, we opted to fix this value in order to remove the
degeneracy between the change in amplitude induced by stellar activity and by
the planet candidate.

##  Appendix B Figures

Figure A1: Radial velocities for HD79210 measured from CARMENES (orange, top
panel only), HARPS-N (blue, all panels) and HIRES (green, top panel only)
spectra. For most data points, the uncertainty in the RV is smaller than the
size of the point. We mark the binary trend, fit as a second-order polynomial,
with a dashed line in the first and third panels. The bottom panel shows the
HARPS-N radial velocities with the binary trend subtracted. We use the HARPS-N
RVs with the binary trend removed in our periodograms and when calculating
correlation with stellar activity indicators analysis (Figures A2, A3, A4).
Figure A2: Various HARPS-N stellar activity indicators versus HD79210’s radial
velocities after the stellar binary trend has been subtracted. The r-values
are Pearson correlation coefficients. FWHM is moderately correlated ($r\geq
0.3$), with an r-value of 0.39. Figure A3: Periodograms of HARPS-N radial
velocities of HD79210, without the binary trend removed (top) and with the
binary trend removed (bottom). Signals with frequencies from 0 to 0.33 $\text{
days}^{-1}$ are plotted. Before the binary trend is removed, there are many
significant low frequency signals (blue shaded region), as we would expect
from the long period binary. Once the binary trend is removed, there are no
signals with less than 0.01% FAP.  Figure A4: Periodograms of HD79210’s white
light HARPS-N radial velocities with the binary trend removed, activity
indicators, and the window function. The three most significant peaks
($<0.1\%$ FAP) are marked with dashed vertical lines. Note that there are no
periodic signals in the RVs with FAP$<0.01\%$. The 25.16 day and 26.98 day
signals are just offset from significant ($<0.01\%$ FAP and $<0.1\%$ FAP,
respectively) peaks in the periodogram of BIS. We suspect that the RV signals
correspond to these BIS signals, as BIS signals has been shown to be offset in
time from RV variability (Dumusque et al., 2014; Collier Cameron et al.,
2019). We suspect that the 225.54 day signal is a harmonic of the 25.16 day
variability signal. Figure A5: Posterior distributions of the free parameters
when fitting HD79211’s combined HARPS-N and CARMENES RV dataset with an
eccentric orbit and a quasic-periodic GP kernel.

##  Appendix C Tables

Table B1: All available magnitudes from survey photometry for HD79210 and
HD79211. We also note the flags associated with these photometry, which denote
the extent to which the two sources were blended in the original images.

Survey | Band | HD79210 | HD79211 | Flags
---|---|---|---|---
The Hipparcos and Tycho Catalogues${}^{\text{a}}$ | BTmag | 9.388 $\pm$ 0.03 |  |
The Hipparcos and Tycho Catalogues${}^{\text{a}}$ | VTmag | 7.791 $\pm$ 0.016 |  |
The Hipparcos and Tycho Catalogues${}^{\text{a}}$ | Hpmag | 7.7796 $\pm$ 0.0728 | 7.9664 $\pm$ 0.0824 |
The Hipparcos and Tycho Catalogues${}^{\text{a}}$ | Vmag | 7.64 | 7.7 |
Gaia EDR3${}^{\text{b}}$ | Gmag | 6.976026 | 7.054455 |
Gaia EDR3${}^{\text{b}}$ | BPmag | 7.863408 | 7.959406 |
Gaia EDR3${}^{\text{b}}$ | RPmag | 6.046104 | 6.112957 |
GALEX-DR5${}^{\text{c}}$ | FUV | 19.471 $\pm$ 0.166 | 19.467 $\pm$ 0.165 | 1
GALEX-DR5${}^{\text{c}}$ | NUV | 16.317 $\pm$ 0.016 | 16.35 $\pm$ 0.016 | 1
The Tycho-2 Catalogue${}^{\text{d}}$ | Tycho-2 BT mag | 9.412 | 9.549 |
The Tycho-2 Catalogue${}^{\text{d}}$ | Tycho-2 VT mag | 7.789 | 7.882 |
2MASS All-Sky Catalog of Point Sources${}^{\text{e}}$ | Jmag | 4.889 $\pm$ 0.037 | 4.779 $\pm$ 0.174 | 2,3
2MASS All-Sky Catalog of Point Sources${}^{\text{e}}$ | Hmag | 3.987 $\pm$ 0.188 | 4.043 $\pm$ 0.206 | 3
2MASS All-Sky Catalog of Point Sources${}^{\text{e}}$ | Kmag | 3.988 $\pm$ 0.036 | 4.136 $\pm$ 0.020 ” | 2,3
The USNO-B1.0 Catalog${}^{\text{f}}$ | B1mag | 9.28 | 9.41 |
The USNO-B1.0 Catalog${}^{\text{f}}$ | B2mag | 6.85 | 6.92 |
The USNO-B1.0 Catalog${}^{\text{f}}$ | R1mag | 8.35 | 8.46 |
The USNO-B1.0 Catalog${}^{\text{f}}$ | R2mag | 6.78 | 6.85 |
SDSS DR13${}^{\text{g}}$ | u | 13.529892 $\pm$ 0.0379 | 12.307867 $\pm$ 0.0102 | 4
SDSS DR13${}^{\text{g}}$ | g | 14.218927 $\pm$ 0.2757 | 8.6298 $\pm$ 2.83E-04 | 4
SDSS DR13${}^{\text{g}}$ | r | 14.097498 $\pm$ 1.0859 | 7.2558894 $\pm$ 1.33E-04 | 4
SDSS DR13${}^{\text{g}}$ | i | 13.7924185 $\pm$ 1.0859 | 6.7036 $\pm$ 1.68E-04 | 4
SDSS DR13${}^{\text{g}}$ | z | 11.406796 $\pm$ 1.0869 | 6.7336 $\pm$ 6.48E-04 | 4

Flags: 1 The object was originally blended with another one 2 This category
includes detections where the goodness-of-fit quality of the profile-fit
photometry was very poor 3 Diffraction spike confusion 4 unclean

References: ${}^{\text{a}}$ ESA (1997) ${}^{\text{b}}$ Gaia Collaboration
(2020) ${}^{\text{c}}$ Bianchi et al. (2011) ${}^{\text{d}}$ Høg et al. (2000)
${}^{\text{e}}$ Cutri et al. (2003) ${}^{\text{f}}$ Monet et al. (2003)
${}^{\text{g}}$ Blanton et al. (2017)

Table B2: HD79211 radial velocities and activity indicators. RVs as calculated using TERRA, and activity indicators as calculated by the HARPS-N DRS 3.7. Date | RV | eRV | FWHM | eFWHM | BIS | eBIS | Contrast | eContrast | Smw | eSmw | Ha | eHa | Na | eNa
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
(jdb-2.45e6) | (m s-1) | (m s-1) |  |  |  |  |  |  |  |  |  |  |  |
6285.612891 | 20.3 | 0.8 | 6117.3 | 8.7 | 61.8 | 1.0 | 34.232862 | 0.000001 | 1.869 | 0.004 | 0.577 | 0.001 | 0.1229 | 0.0002
6671.615209 | 8.7 | 0.3 | 6029.1 | 8.5 | 56.8 | 1.0 | 34.624995 | 0.000001 | 0.000 | 0.000 | 0.551 | 0.001 | 0.1257 | 0.0002
6671.724181 | 8.7 | 0.6 | 6025.1 | 8.5 | 58.0 | 1.1 | 34.621989 | 0.000001 | 0.000 | 0.000 | 0.545 | 0.001 | 0.1241 | 0.0002
6672.512178 | 10.8 | 0.3 | 6040.1 | 8.5 | 57.7 | 1.1 | 34.550935 | 0.000001 | 0.000 | 0.000 | 0.556 | 0.001 | 0.1244 | 0.0002
6672.609691 | 12.4 | 0.4 | 6133.3 | 8.7 | 60.7 | 0.9 | 34.136966 | 0.000001 | 1.724 | 0.003 | 0.558 | 0.001 | 0.1243 | 0.0002
7014.621385 | -0.2 | 0.6 | 5984.5 | 8.5 | 66.2 | 1.1 | 35.042534 | 0.000001 | 1.498 | 0.005 | 0.534 | 0.001 | 0.1206 | 0.0002
7014.732420 | -1.8 | 0.6 | 5984.8 | 8.5 | 68.9 | 1.0 | 35.034022 | 0.000001 | 1.480 | 0.004 | 0.533 | 0.001 | 0.1207 | 0.0002
7018.726754 | 5.8 | 0.5 | 5994.5 | 8.5 | 67.2 | 1.2 | 34.991576 | 0.000001 | 1.437 | 0.006 | 0.523 | 0.001 | 0.1214 | 0.0003
7020.717072 | 2.8 | 0.6 | 5990.4 | 8.5 | 74.4 | 1.2 | 35.018739 | 0.000001 | 1.581 | 0.006 | 0.540 | 0.001 | 0.1199 | 0.0003
7020.785177 | 4.9 | 0.5 | 5991.4 | 8.5 | 72.8 | 0.9 | 34.986452 | 0.000001 | 1.536 | 0.004 | 0.532 | 0.001 | 0.1167 | 0.0002
7044.748325 | 6.0 | 0.5 | 6002.1 | 8.5 | 72.3 | 0.9 | 34.923610 | 0.000001 | 1.561 | 0.004 | 0.535 | 0.001 | 0.1200 | 0.0002
7045.530040 | 3.3 | 0.5 | 5998.6 | 8.5 | 68.7 | 1.2 | 34.967085 | 0.000001 | 1.542 | 0.006 | 0.545 | 0.001 | 0.1217 | 0.0003
7045.722216 | 3.8 | 0.6 | 5995.6 | 8.5 | 68.6 | 1.3 | 34.983797 | 0.000001 | 1.536 | 0.007 | 0.535 | 0.001 | 0.1219 | 0.0003
7046.602067 | 4.5 | 0.5 | 5997.0 | 8.5 | 68.1 | 0.9 | 34.963493 | 0.000001 | 1.518 | 0.004 | 0.528 | 0.001 | 0.1206 | 0.0002
7046.737819 | 4.5 | 0.4 | 5995.3 | 8.5 | 67.9 | 0.9 | 34.966771 | 0.000001 | 1.502 | 0.003 | 0.532 | 0.001 | 0.1197 | 0.0002
7048.470341 | 6.0 | 0.6 | 5989.9 | 8.5 | 62.4 | 1.3 | 35.022517 | 0.000001 | 1.471 | 0.007 | 0.518 | 0.001 | 0.1206 | 0.0003
7048.557574 | 6.4 | 0.5 | 5988.5 | 8.5 | 63.3 | 1.4 | 35.022603 | 0.000001 | 1.474 | 0.007 | 0.520 | 0.001 | 0.1211 | 0.0003
7051.507932 | 14.6 | 0.5 | 6006.5 | 8.5 | 65.8 | 1.1 | 34.896503 | 0.000001 | 1.526 | 0.005 | 0.531 | 0.001 | 0.1218 | 0.0002
7051.628868 | 14.2 | 0.5 | 6009.1 | 8.5 | 65.9 | 1.0 | 34.883580 | 0.000001 | 1.603 | 0.004 | 0.549 | 0.001 | 0.1227 | 0.0002
7052.598236 | 9.2 | 0.6 | 6014.2 | 8.5 | 71.9 | 1.4 | 34.869929 | 0.000001 | 1.546 | 0.008 | 0.539 | 0.001 | 0.1220 | 0.0003
7052.673872 | 9.3 | 1.0 | 6004.5 | 8.5 | 68.8 | 2.3 | 34.884387 | 0.000001 | 1.551 | 0.016 | 0.535 | 0.002 | 0.1228 | 0.0005
7053.433842 | 7.3 | 0.7 | 6008.7 | 8.5 | 72.7 | 1.5 | 34.889942 | 0.000001 | 1.588 | 0.009 | 0.547 | 0.001 | 0.1213 | 0.0003
7053.572232 | 7.9 | 0.7 | 6007.6 | 8.5 | 72.1 | 1.3 | 34.881916 | 0.000001 | 1.612 | 0.007 | 0.553 | 0.001 | 0.1211 | 0.0003
7054.587638 | 9.7 | 0.5 | 6009.7 | 8.5 | 68.7 | 0.9 | 34.781720 | 0.000001 | 1.710 | 0.004 | 0.560 | 0.001 | 0.1235 | 0.0002
7054.675635 | 9.5 | 0.5 | 6005.7 | 8.5 | 70.3 | 0.9 | 34.885117 | 0.000001 | 1.590 | 0.003 | 0.547 | 0.001 | 0.1214 | 0.0002
7106.458292 | 5.8 | 0.5 | 6002.2 | 8.5 | 69.3 | 1.2 | 34.941747 | 0.000001 | 1.434 | 0.005 | 0.504 | 0.001 | 0.1176 | 0.0002
7106.581258 | 5.1 | 0.5 | 6005.6 | 8.5 | 68.8 | 1.2 | 34.936934 | 0.000001 | 1.435 | 0.006 | 0.500 | 0.001 | 0.1165 | 0.0002
7107.383100 | 3.7 | 0.5 | 5996.2 | 8.5 | 71.5 | 0.8 | 34.948208 | 0.000001 | 1.462 | 0.003 | 0.525 | 0.001 | 0.1202 | 0.0002
7107.511736 | 3.0 | 0.5 | 5996.9 | 8.5 | 73.1 | 1.0 | 34.955592 | 0.000001 | 1.452 | 0.005 | 0.512 | 0.001 | 0.1180 | 0.0002
7324.740802 | 2.0 | 0.7 | 6013.2 | 8.5 | 71.9 | 1.4 | 34.906742 | 0.000001 | 1.612 | 0.008 | 0.537 | 0.001 | 0.1240 | 0.0003
7324.746300 | 1.5 | 0.6 | 6001.4 | 8.5 | 71.3 | 1.4 | 34.895632 | 0.000001 | 1.599 | 0.008 | 0.534 | 0.001 | 0.1231 | 0.0003
7325.700001 | 2.5 | 0.5 | 6004.0 | 8.5 | 74.8 | 1.2 | 34.916968 | 0.000001 | 1.549 | 0.006 | 0.515 | 0.001 | 0.1208 | 0.0003
7325.705464 | 2.4 | 0.6 | 6003.9 | 8.5 | 74.7 | 1.2 | 34.925492 | 0.000001 | 1.556 | 0.006 | 0.518 | 0.001 | 0.1209 | 0.0003
7332.667583 | 0.6 | 0.6 | 5996.4 | 8.5 | 67.9 | 1.0 | 34.961330 | 0.000001 | 1.572 | 0.005 | 0.533 | 0.001 | 0.1225 | 0.0002
7332.753053 | 1.7 | 0.6 | 5998.0 | 8.5 | 69.0 | 1.0 | 34.960201 | 0.000001 | 1.542 | 0.004 | 0.525 | 0.001 | 0.1225 | 0.0002
7333.681902 | 1.3 | 0.4 | 6001.3 | 8.5 | 67.8 | 0.8 | 34.925854 | 0.000001 | 1.555 | 0.003 | 0.540 | 0.001 | 0.1245 | 0.0002
7333.753366 | 2.0 | 0.5 | 6002.1 | 8.5 | 69.3 | 0.8 | 34.924959 | 0.000001 | 1.538 | 0.003 | 0.538 | 0.001 | 0.1248 | 0.0002
7334.624478 | 0.6 | 0.7 | 6010.6 | 8.5 | 67.6 | 0.9 | 34.885663 | 0.000001 | 1.598 | 0.004 | 0.544 | 0.001 | 0.1236 | 0.0002
7334.727032 | 2.3 | 0.7 | 6009.3 | 8.5 | 66.7 | 0.8 | 34.888516 | 0.000001 | 1.567 | 0.003 | 0.533 | 0.001 | 0.1224 | 0.0002
7335.664700 | -0.0 | 0.6 | 6008.8 | 8.5 | 69.4 | 1.6 | 34.925364 | 0.000001 | 1.553 | 0.010 | 0.517 | 0.001 | 0.1247 | 0.0004
7335.751223 | -7.1 | 0.6 | 6009.7 | 8.5 | 68.5 | 1.0 | 34.878111 | 0.000001 | 1.536 | 0.004 | 0.526 | 0.001 | 0.1235 | 0.0002
7379.570185 | -1.7 | 0.6 | 5993.8 | 8.5 | 71.2 | 1.1 | 34.968125 | 0.000001 | 1.494 | 0.005 | 0.506 | 0.001 | 0.1207 | 0.0002
7379.667493 | -1.5 | 0.4 | 5990.6 | 8.5 | 69.7 | 0.8 | 34.966462 | 0.000001 | 1.494 | 0.003 | 0.506 | 0.001 | 0.1208 | 0.0002
7380.564210 | 0.1 | 0.6 | 5992.2 | 8.5 | 70.4 | 1.3 | 34.972041 | 0.000001 | 1.556 | 0.007 | 0.517 | 0.001 | 0.1217 | 0.0003
7380.689505 | 1.0 | 0.5 | 5992.5 | 8.5 | 67.9 | 0.9 | 34.957374 | 0.000001 | 1.545 | 0.004 | 0.522 | 0.001 | 0.1213 | 0.0002
7381.620483 | 0.5 | 0.4 | 5994.3 | 8.5 | 69.8 | 1.2 | 34.972357 | 0.000001 | 1.522 | 0.006 | 0.515 | 0.001 | 0.1218 | 0.0003
7381.708704 | 1.2 | 0.3 | 5994.9 | 8.5 | 65.6 | 0.9 | 34.942763 | 0.000001 | 1.533 | 0.004 | 0.521 | 0.001 | 0.1225 | 0.0002
7384.566887 | 1.8 | 0.6 | 6007.8 | 8.5 | 68.6 | 1.0 | 34.896642 | 0.000001 | 1.555 | 0.005 | 0.532 | 0.001 | 0.1234 | 0.0002
7384.665722 | -0.7 | 0.5 | 6005.1 | 8.5 | 70.2 | 1.1 | 34.899071 | 0.000001 | 1.552 | 0.005 | 0.531 | 0.001 | 0.1240 | 0.0002
7385.535905 | -1.7 | 0.7 | 6014.2 | 8.5 | 70.7 | 1.8 | 34.896648 | 0.000001 | 1.592 | 0.011 | 0.518 | 0.001 | 0.1226 | 0.0004
7385.677403 | -0.3 | 0.5 | 6009.3 | 8.5 | 68.4 | 1.2 | 34.863785 | 0.000001 | 1.618 | 0.006 | 0.527 | 0.001 | 0.1212 | 0.0002
7407.475529 | 2.5 | 0.6 | 6036.3 | 8.5 | 71.0 | 0.9 | 34.716908 | 0.000001 | 1.686 | 0.004 | 0.567 | 0.001 | 0.1246 | 0.0002
7407.717522 | 2.7 | 0.5 | 6037.7 | 8.5 | 72.8 | 0.9 | 34.710184 | 0.000001 | 1.642 | 0.004 | 0.556 | 0.001 | 0.1248 | 0.0002
7408.512642 | -0.8 | 0.5 | 6032.4 | 8.5 | 74.3 | 0.9 | 34.759374 | 0.000001 | 1.637 | 0.003 | 0.554 | 0.001 | 0.1238 | 0.0002
7408.706636 | -1.2 | 0.6 | 6029.6 | 8.5 | 80.3 | 1.2 | 34.772884 | 0.000001 | 1.668 | 0.006 | 0.550 | 0.001 | 0.1239 | 0.0003
7409.461119 | -1.0 | 0.6 | 6018.8 | 8.5 | 79.1 | 0.9 | 34.791592 | 0.000001 | 1.646 | 0.004 | 0.555 | 0.001 | 0.1237 | 0.0002
7410.511099 | 1.6 | 0.9 | 6011.7 | 8.5 | 79.3 | 1.6 | 34.697860 | 0.000001 | 1.607 | 0.009 | 0.510 | 0.001 | 0.1210 | 0.0004
7411.517177 | -5.0 | 0.6 | 5992.5 | 8.5 | 72.5 | 1.2 | 34.905516 | 0.000001 | 1.567 | 0.005 | 0.517 | 0.001 | 0.1209 | 0.0002
7411.761853 | -1.4 | 0.8 | 5978.0 | 8.5 | 73.1 | 2.3 | 34.518417 | 0.000001 | 1.507 | 0.015 | 0.513 | 0.001 | 0.1296 | 0.0005
7412.515048 | 3.3 | 0.5 | 5992.8 | 8.5 | 71.4 | 0.9 | 34.934547 | 0.000001 | 1.608 | 0.004 | 0.520 | 0.001 | 0.1192 | 0.0002
7412.678358 | 2.9 | 0.5 | 5990.6 | 8.5 | 71.7 | 1.1 | 34.956586 | 0.000001 | 1.585 | 0.005 | 0.510 | 0.001 | 0.1188 | 0.0002
7459.508092 | 3.1 | 0.8 | 6027.6 | 8.5 | 67.0 | 2.0 | 34.808038 | 0.000001 | 1.622 | 0.012 | 0.544 | 0.002 | 0.1233 | 0.0005
7459.612820 | 2.0 | 0.8 | 6025.7 | 8.5 | 73.0 | 1.8 | 34.792587 | 0.000001 | 1.644 | 0.011 | 0.544 | 0.001 | 0.1231 | 0.0004
7460.614946 | 2.9 | 0.5 | 6013.5 | 8.5 | 72.7 | 1.0 | 34.819873 | 0.000001 | 1.554 | 0.005 | 0.541 | 0.001 | 0.1235 | 0.0002
7461.556115 | 2.8 | 0.6 | 6010.7 | 8.5 | 74.2 | 1.2 | 34.852056 | 0.000001 | 1.599 | 0.006 | 0.539 | 0.001 | 0.1231 | 0.0003
7461.559865 | 1.9 | 0.5 | 6008.2 | 8.5 | 72.1 | 1.2 | 34.855077 | 0.000001 | 1.617 | 0.006 | 0.545 | 0.001 | 0.1240 | 0.0003
7461.563661 | 1.6 | 0.6 | 6011.8 | 8.5 | 73.1 | 1.3 | 34.834035 | 0.000001 | 1.617 | 0.006 | 0.544 | 0.001 | 0.1235 | 0.0003
7462.570242 | 1.8 | 0.7 | 6005.5 | 8.5 | 72.6 | 1.3 | 34.894691 | 0.000001 | 1.575 | 0.007 | 0.545 | 0.001 | 0.1228 | 0.0003
7462.576318 | 1.7 | 0.7 | 6009.3 | 8.5 | 71.9 | 1.3 | 34.900651 | 0.000001 | 1.576 | 0.007 | 0.542 | 0.001 | 0.1225 | 0.0003
7463.478321 | 6.4 | 0.6 | 5999.6 | 8.5 | 68.9 | 1.2 | 34.918489 | 0.000001 | 1.537 | 0.005 | 0.534 | 0.001 | 0.1220 | 0.0003
7463.483760 | 5.0 | 0.6 | 5998.8 | 8.5 | 67.2 | 1.2 | 34.933660 | 0.000001 | 1.539 | 0.006 | 0.531 | 0.001 | 0.1222 | 0.0003
7463.592711 | 5.2 | 0.7 | 6000.1 | 8.5 | 67.6 | 1.5 | 34.920505 | 0.000001 | 1.519 | 0.008 | 0.521 | 0.001 | 0.1211 | 0.0004
7463.598243 | 5.1 | 0.8 | 5998.8 | 8.5 | 70.1 | 1.8 | 34.950547 | 0.000001 | 1.519 | 0.010 | 0.520 | 0.001 | 0.1210 | 0.0004
7752.639756 | 0.9 | 0.8 | 6023.6 | 8.5 | 65.8 | 1.7 | 34.820135 | 0.000001 | 1.635 | 0.010 | 0.530 | 0.001 | 0.1273 | 0.0004
7753.564001 | 1.3 | 1.1 | 6024.4 | 8.5 | 69.0 | 2.8 | 34.816407 | 0.000001 | 1.624 | 0.020 | 0.536 | 0.002 | 0.1371 | 0.0006
7753.786752 | 1.9 | 0.6 | 6028.4 | 8.5 | 61.5 | 1.4 | 34.754533 | 0.000001 | 1.652 | 0.008 | 0.536 | 0.001 | 0.1244 | 0.0003
8075.656797 | -1.4 | 0.5 | 6005.1 | 8.5 | 71.8 | 0.9 | 34.921503 | 0.000001 | 1.572 | 0.003 | 0.519 | 0.001 | 0.1208 | 0.0002
8119.563946 | -3.8 | 0.9 | 5995.9 | 8.5 | 62.6 | 1.6 | 34.942547 | 0.000001 | 1.467 | 0.008 | 0.515 | 0.001 | 0.1201 | 0.0003
8120.610033 | -5.8 | 0.7 | 6002.2 | 8.5 | 62.6 | 1.6 | 34.907409 | 0.000001 | 1.480 | 0.008 | 0.551 | 0.001 | 0.1361 | 0.0004
8122.652629 | -0.7 | 0.7 | 5998.8 | 8.5 | 65.9 | 1.3 | 34.960728 | 0.000001 | 1.507 | 0.005 | 0.519 | 0.001 | 0.1203 | 0.0003
8143.542711 | -5.1 | 0.7 | 5983.7 | 8.5 | 74.7 | 1.6 | 35.038470 | 0.000001 | 1.463 | 0.010 | 0.506 | 0.001 | 0.1191 | 0.0003
8147.611456 | -3.2 | 0.7 | 5976.1 | 8.5 | 66.9 | 1.1 | 35.055493 | 0.000001 | 1.390 | 0.006 | 0.489 | 0.001 | 0.1186 | 0.0002
8477.691075 | -13.5 | 0.9 | 6055.6 | 8.6 | 78.6 | 1.5 | 34.556499 | 0.000001 | 1.775 | 0.007 | 0.555 | 0.001 | 0.1250 | 0.0003
8477.757699 | -13.7 | 0.8 | 6064.4 | 8.6 | 89.5 | 2.0 | 34.565657 | 0.000001 | 1.818 | 0.011 | 0.570 | 0.001 | 0.1267 | 0.0004
8526.411740 | -7.9 | 0.7 | 6076.2 | 8.6 | 76.5 | 1.3 | 34.461290 | 0.000001 | 1.881 | 0.006 | 0.581 | 0.001 | 0.1277 | 0.0003
8536.630177 | 0.1 | 0.7 | 6042.3 | 8.5 | 60.1 | 1.2 | 34.635809 | 0.000001 | 1.699 | 0.005 | 0.532 | 0.001 | 0.1236 | 0.0002
8538.634332 | 4.9 | 0.7 | 6054.7 | 8.6 | 65.7 | 1.2 | 34.566339 | 0.000001 | 1.743 | 0.006 | 0.546 | 0.001 | 0.1256 | 0.0003
8805.645794 | -3.5 | 0.9 | 6029.3 | 8.5 | 74.1 | 1.4 | 34.783666 | 0.000001 | 1.630 | 0.006 | 0.516 | 0.001 | 0.1250 | 0.0003
8805.741588 | -2.1 | 0.7 | 6026.6 | 8.5 | 72.6 | 0.9 | 34.739513 | 0.000001 | 1.623 | 0.003 | 0.519 | 0.001 | 0.1246 | 0.0002
8816.605286 | -5.7 | 0.7 | 6010.7 | 8.5 | 73.4 | 1.2 | 34.858948 | 0.000001 | 1.587 | 0.005 | 0.516 | 0.001 | 0.1223 | 0.0002
8816.723732 | -6.6 | 0.9 | 6017.1 | 8.5 | 69.9 | 1.5 | 34.879021 | 0.000001 | 1.589 | 0.007 | 0.511 | 0.001 | 0.1229 | 0.0003
8818.625772 | -6.5 | 0.7 | 6016.5 | 8.5 | 69.0 | 0.9 | 34.815676 | 0.000001 | 1.643 | 0.003 | 0.531 | 0.001 | 0.1245 | 0.0002
8818.749021 | -6.4 | 0.7 | 6017.3 | 8.5 | 67.1 | 0.9 | 34.812491 | 0.000001 | 1.613 | 0.003 | 0.519 | 0.001 | 0.1223 | 0.0002
8830.770218 | -4.4 | 0.8 | 6031.1 | 8.5 | 75.9 | 2.1 | 34.753263 | 0.000001 | 1.643 | 0.011 | 0.521 | 0.001 | 0.1253 | 0.0005
8832.775143 | 0.9 | 0.8 | 6037.4 | 8.5 | 86.0 | 2.7 | 34.791074 | 0.000001 | 1.598 | 0.015 | 0.525 | 0.002 | 0.1443 | 0.0007
8841.672974 | -2.7 | 1.5 | 6024.0 | 8.5 | 53.6 | 4.0 | 34.995432 | 0.000001 | 1.776 | 0.029 | 0.539 | 0.003 | 0.1596 | 0.0009
8847.594680 | -11.1 | 0.7 | 6018.0 | 8.5 | 75.5 | 1.0 | 34.836482 | 0.000001 | 1.573 | 0.004 | 0.513 | 0.001 | 0.1223 | 0.0002
8847.756271 | -9.0 | 0.8 | 6019.6 | 8.5 | 75.7 | 1.0 | 34.838014 | 0.000001 | 1.612 | 0.004 | 0.518 | 0.001 | 0.1218 | 0.0002
8854.646741 | -3.0 | 0.8 | 6008.0 | 8.5 | 69.4 | 0.9 | 34.899571 | 0.000001 | 1.579 | 0.003 | 0.543 | 0.001 | 0.1257 | 0.0002
8883.554321 | -7.5 | 1.0 | 6008.8 | 8.5 | 74.6 | 2.0 | 34.980193 | 0.000001 | 1.619 | 0.011 | 0.526 | 0.001 | 0.1214 | 0.0005
8883.640535 | -6.1 | 2.3 | 6010.4 | 8.5 | 67.4 | 4.8 | 35.207201 | 0.000001 | 1.783 | 0.041 | 0.517 | 0.003 | 0.1243 | 0.0010
8887.479981 | -4.4 | 0.7 | 6005.1 | 8.5 | 71.7 | 0.8 | 34.894021 | 0.000001 | 1.523 | 0.003 | 0.497 | 0.000 | 0.1184 | 0.0001
8887.585245 | -3.4 | 0.7 | 6004.0 | 8.5 | 71.6 | 0.8 | 34.900044 | 0.000001 | 1.547 | 0.003 | 0.505 | 0.000 | 0.1198 | 0.0001
8908.546480 | -4.2 | 0.7 | 6019.9 | 8.5 | 68.5 | 1.0 | 34.828600 | 0.000001 | 1.690 | 0.004 | 0.537 | 0.001 | 0.1208 | 0.0002
8908.666000 | -5.1 | 0.6 | 6020.9 | 8.5 | 66.0 | 1.3 | 34.832169 | 0.000001 | 1.678 | 0.006 | 0.535 | 0.001 | 0.1193 | 0.0003
8910.496814 | -2.2 | 0.7 | 6020.3 | 8.5 | 69.4 | 0.9 | 34.833626 | 0.000001 | 1.625 | 0.004 | 0.526 | 0.001 | 0.1216 | 0.0002
8915.453070 | -6.7 | 0.6 | 6009.5 | 8.5 | 71.8 | 0.8 | 34.885467 | 0.000001 | 1.536 | 0.003 | 0.515 | 0.000 | 0.1189 | 0.0002
8915.546282 | -9.3 | 0.8 | 6011.3 | 8.5 | 68.6 | 1.4 | 34.935664 | 0.000001 | 1.523 | 0.007 | 0.508 | 0.001 | 0.1187 | 0.0003
9655.557594 | -19.1 | 0.7 | 6012.9 | 8.5 | 69.6 | 1.2 | 34.793949 | 0.000001 | 1.679 | 0.006 | 0.549 | 0.001 | 0.1235 | 0.0003
9656.551881 | -19.9 | 1.1 | 6013.2 | 8.5 | 70.1 | 1.5 | 34.813970 | 0.000001 | 1.612 | 0.008 | 0.524 | 0.001 | 0.1235 | 0.0003
9658.456802 | -19.7 | 0.9 | 6014.8 | 8.5 | 72.4 | 1.2 | 34.825784 | 0.000001 | 1.584 | 0.006 | 0.521 | 0.001 | 0.1227 | 0.0002
9659.579979 | -18.2 | 0.7 | 6005.5 | 8.5 | 68.6 | 0.9 | 34.840340 | 0.000001 | 1.605 | 0.004 | 0.540 | 0.001 | 0.1230 | 0.0002
9661.603197 | -15.8 | 0.9 | 6002.3 | 8.5 | 64.1 | 1.8 | 34.905553 | 0.000001 | 1.594 | 0.012 | 0.523 | 0.001 | 0.1211 | 0.0004
9662.554508 | -13.6 | 0.8 | 6003.4 | 8.5 | 71.5 | 1.4 | 34.893858 | 0.000001 | 1.594 | 0.008 | 0.518 | 0.001 | 0.1209 | 0.0003

Table B3: HD79210 radial velocities and activity indicators. RVs as calculated using TERRA, and activity indicators as calculated by the HARPS-N DRS 3.7. Date | RV | eRV | FWHM | eFWHM | BIS | eBIS | Contrast | eContrast | Smw | eSmw | Ha | eHa | Na | eNa
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
(jdb-2.45e6) | (m s-1) | (m s-1) |  |  |  |  |  |  |  |  |  |  |  |
6671.602883 | -17.9 | 0.6 | 6205.3 | 8.8 | 64.7 | 0.9 | 34.702755 | 0.000001 | 1.715 | 0.004 | 0.548 | 0.001 | 0.1255 | 0.0002
6671.712040 | -18.3 | 0.5 | 6204.8 | 8.8 | 64.6 | 1.1 | 34.709181 | 0.000001 | 1.731 | 0.005 | 0.545 | 0.001 | 0.1245 | 0.0002
6672.500523 | -20.4 | 0.4 | 6202.7 | 8.8 | 64.0 | 0.9 | 34.709411 | 0.000001 | 1.730 | 0.004 | 0.543 | 0.001 | 0.1237 | 0.0002
6672.597364 | -19.5 | 0.3 | 6196.4 | 8.8 | 64.6 | 0.9 | 34.701540 | 0.000001 | 1.735 | 0.003 | 0.546 | 0.001 | 0.1237 | 0.0002
6968.679139 | -17.4 | 0.7 | 6059.3 | 8.6 | 65.8 | 1.3 | 35.474655 | 0.000001 | 1.556 | 0.007 | 0.520 | 0.001 | 0.1204 | 0.0003
7014.608861 | -19.2 | 0.7 | 6078.1 | 8.6 | 69.9 | 1.0 | 35.392864 | 0.000001 | 1.683 | 0.005 | 0.539 | 0.001 | 0.1228 | 0.0002
7014.721910 | -25.5 | 0.5 | 6081.7 | 8.6 | 70.6 | 1.1 | 35.379604 | 0.000001 | 1.689 | 0.005 | 0.544 | 0.001 | 0.1229 | 0.0002
7016.648683 | -17.1 | 0.6 | 6073.7 | 8.6 | 68.7 | 0.9 | 35.415204 | 0.000001 | 1.630 | 0.004 | 0.527 | 0.001 | 0.1224 | 0.0002
7016.744011 | -18.1 | 0.6 | 6076.2 | 8.6 | 64.2 | 1.3 | 35.436469 | 0.000001 | 1.659 | 0.007 | 0.533 | 0.001 | 0.1229 | 0.0003
7018.694229 | -17.3 | 0.7 | 6071.9 | 8.6 | 68.9 | 1.2 | 35.443635 | 0.000001 | 1.701 | 0.006 | 0.555 | 0.001 | 0.1258 | 0.0003
7020.676238 | -20.7 | 0.5 | 6053.7 | 8.6 | 71.7 | 0.9 | 35.505181 | 0.000001 | 1.581 | 0.004 | 0.515 | 0.001 | 0.1189 | 0.0002
7020.773116 | -19.7 | 0.5 | 6052.8 | 8.6 | 68.1 | 0.9 | 35.509273 | 0.000001 | 1.634 | 0.004 | 0.519 | 0.001 | 0.1174 | 0.0002
7044.618278 | -11.2 | 0.6 | 6046.5 | 8.6 | 65.1 | 0.9 | 35.588323 | 0.000001 | 1.540 | 0.004 | 0.516 | 0.001 | 0.1201 | 0.0002
7379.547614 | -9.9 | 0.6 | 6081.2 | 8.6 | 67.8 | 1.3 | 35.395780 | 0.000001 | 1.624 | 0.007 | 0.525 | 0.001 | 0.1223 | 0.0003
7379.558946 | -11.0 | 0.5 | 6083.7 | 8.6 | 69.1 | 1.0 | 35.365167 | 0.000001 | 1.657 | 0.005 | 0.532 | 0.001 | 0.1226 | 0.0002
7379.650825 | -9.8 | 0.5 | 6082.0 | 8.6 | 69.3 | 0.8 | 35.364910 | 0.000001 | 1.613 | 0.003 | 0.530 | 0.001 | 0.1228 | 0.0002
7381.632555 | -16.3 | 0.5 | 6069.3 | 8.6 | 75.5 | 1.0 | 35.459527 | 0.000001 | 1.584 | 0.005 | 0.523 | 0.001 | 0.1226 | 0.0002
7381.719966 | -15.8 | 0.5 | 6068.5 | 8.6 | 78.3 | 1.0 | 35.473583 | 0.000001 | 1.579 | 0.005 | 0.521 | 0.001 | 0.1224 | 0.0002
7407.463307 | -16.5 | 0.7 | 6087.3 | 8.6 | 78.5 | 1.0 | 35.347004 | 0.000001 | 1.657 | 0.005 | 0.548 | 0.001 | 0.1224 | 0.0002
7407.705901 | -14.6 | 0.6 | 6085.3 | 8.6 | 76.3 | 0.9 | 35.348105 | 0.000001 | 1.687 | 0.004 | 0.562 | 0.001 | 0.1245 | 0.0002
7411.506298 | -23.9 | 0.7 | 6080.3 | 8.6 | 61.9 | 1.4 | 35.292921 | 0.000001 | 1.710 | 0.007 | 0.546 | 0.001 | 0.1253 | 0.0003
7411.628022 | -15.4 | 0.8 | 6073.3 | 8.6 | 53.6 | 1.8 | 34.952576 | 0.000001 | 1.632 | 0.010 | 0.538 | 0.001 | 0.1362 | 0.0004
7458.514008 | -11.5 | 0.7 | 6072.9 | 8.6 | 69.6 | 1.1 | 35.445024 | 0.000001 | 1.589 | 0.005 | 0.530 | 0.001 | 0.1224 | 0.0003
7458.519656 | -11.9 | 0.7 | 6069.2 | 8.6 | 67.8 | 1.2 | 35.447314 | 0.000001 | 1.605 | 0.006 | 0.531 | 0.001 | 0.1226 | 0.0003
7458.594999 | -11.8 | 0.7 | 6069.1 | 8.6 | 71.8 | 1.1 | 35.452089 | 0.000001 | 1.663 | 0.005 | 0.549 | 0.001 | 0.1237 | 0.0003
7458.600508 | -11.2 | 0.6 | 6069.7 | 8.6 | 68.3 | 1.1 | 35.444495 | 0.000001 | 1.651 | 0.006 | 0.547 | 0.001 | 0.1237 | 0.0003
7462.478835 | -14.8 | 0.7 | 6078.5 | 8.6 | 63.9 | 1.1 | 35.442927 | 0.000001 | 1.626 | 0.005 | 0.534 | 0.001 | 0.1219 | 0.0002
7462.484310 | -14.5 | 0.6 | 6075.8 | 8.6 | 65.5 | 1.1 | 35.439044 | 0.000001 | 1.628 | 0.005 | 0.533 | 0.001 | 0.1214 | 0.0002
7723.698932 | -8.7 | 0.8 | 6069.4 | 8.6 | 72.2 | 1.9 | 35.488947 | 0.000001 | 1.593 | 0.011 | 0.548 | 0.002 | 0.1394 | 0.0005
7732.568598 | -6.0 | 0.6 | 6066.9 | 8.6 | 66.4 | 1.1 | 35.454995 | 0.000001 | 1.681 | 0.005 | 0.545 | 0.001 | 0.1217 | 0.0002
7732.575995 | -5.2 | 0.5 | 6068.3 | 8.6 | 67.0 | 1.1 | 35.455369 | 0.000001 | 1.685 | 0.005 | 0.543 | 0.001 | 0.1211 | 0.0002
7732.732312 | -6.2 | 0.5 | 6069.2 | 8.6 | 67.7 | 0.8 | 35.427932 | 0.000001 | 1.648 | 0.003 | 0.539 | 0.000 | 0.1225 | 0.0001
7752.629201 | -6.5 | 0.8 | 6070.5 | 8.6 | 65.9 | 1.5 | 35.467998 | 0.000001 | 1.730 | 0.009 | 0.553 | 0.001 | 0.1278 | 0.0004
7753.542357 | -7.3 | 1.0 | 6071.2 | 8.6 | 56.4 | 2.4 | 35.480444 | 0.000001 | 1.613 | 0.016 | 0.520 | 0.002 | 0.1358 | 0.0006
7753.774564 | -3.8 | 0.6 | 6074.2 | 8.6 | 64.6 | 1.2 | 35.429545 | 0.000001 | 1.674 | 0.006 | 0.536 | 0.001 | 0.1237 | 0.0003
7764.562994 | -10.8 | 0.7 | 6094.4 | 8.6 | 56.8 | 1.5 | 35.267229 | 0.000001 | 1.679 | 0.008 | 0.548 | 0.001 | 0.1280 | 0.0004
7817.518062 | -7.9 | 0.6 | 6094.8 | 8.6 | 67.5 | 1.2 | 35.290803 | 0.000001 | 1.717 | 0.006 | 0.539 | 0.001 | 0.1215 | 0.0003
8075.643996 | 2.6 | 0.6 | 6125.3 | 8.7 | 66.3 | 0.9 | 35.088364 | 0.000001 | 1.823 | 0.003 | 0.557 | 0.001 | 0.1261 | 0.0002
8086.621865 | -0.5 | 0.8 | 6092.6 | 8.6 | 65.5 | 1.9 | 35.338213 | 0.000001 | 1.692 | 0.012 | 0.530 | 0.001 | 0.1294 | 0.0004
8120.622082 | -1.0 | 0.8 | 6112.7 | 8.6 | 69.1 | 1.8 | 35.180743 | 0.000001 | 1.742 | 0.010 | 0.569 | 0.001 | 0.1415 | 0.0004
8121.702763 | -1.3 | 0.7 | 6108.6 | 8.6 | 70.2 | 1.5 | 35.197757 | 0.000001 | 1.776 | 0.008 | 0.544 | 0.001 | 0.1273 | 0.0003
8122.640152 | 2.3 | 0.7 | 6105.8 | 8.6 | 69.4 | 1.2 | 35.174412 | 0.000001 | 1.834 | 0.006 | 0.560 | 0.001 | 0.1263 | 0.0003
8142.664448 | 4.6 | 1.2 | 6118.9 | 8.7 | 69.7 | 3.3 | 35.097965 | 0.000001 | 1.838 | 0.033 | 0.543 | 0.002 | 0.1314 | 0.0007
8143.527815 | -3.6 | 0.6 | 6114.1 | 8.6 | 66.2 | 1.7 | 35.142612 | 0.000001 | 1.802 | 0.012 | 0.553 | 0.001 | 0.1259 | 0.0004
8143.646565 | -1.9 | 1.1 | 6126.8 | 8.7 | 67.6 | 2.4 | 35.101413 | 0.000001 | 1.904 | 0.018 | 0.561 | 0.002 | 0.1283 | 0.0005
8147.598157 | 3.2 | 0.7 | 6140.6 | 8.7 | 71.1 | 1.1 | 34.965033 | 0.000001 | 1.876 | 0.007 | 0.585 | 0.001 | 0.1273 | 0.0002
8239.368652 | 6.1 | 0.4 | 6103.9 | 8.6 | 66.4 | 0.9 | 35.225081 | 0.000001 | 1.668 | 0.004 | 0.543 | 0.001 | 0.1224 | 0.0002
8454.691049 | 12.6 | 0.5 | 6126.2 | 8.7 | 68.3 | 0.9 | 35.053999 | 0.000001 | 1.778 | 0.003 | 0.551 | 0.001 | 0.1273 | 0.0002
8454.736712 | 12.1 | 0.6 | 6126.0 | 8.7 | 68.6 | 1.0 | 35.057840 | 0.000001 | 1.789 | 0.004 | 0.544 | 0.001 | 0.1267 | 0.0002
8526.425177 | 5.0 | 1.2 | 6144.3 | 8.7 | 83.4 | 2.4 | 35.034133 | 0.000001 | 1.968 | 0.014 | 0.593 | 0.002 | 0.1282 | 0.0005
8536.616161 | 13.5 | 0.6 | 6111.9 | 8.6 | 56.2 | 1.0 | 35.167891 | 0.000001 | 1.735 | 0.005 | 0.532 | 0.001 | 0.1247 | 0.0002
8538.621890 | 10.0 | 0.6 | 6136.6 | 8.7 | 66.9 | 1.1 | 35.008712 | 0.000001 | 1.854 | 0.005 | 0.562 | 0.001 | 0.1256 | 0.0002
8544.459923 | -0.4 | 0.6 | 6116.8 | 8.7 | 82.0 | 0.9 | 35.109791 | 0.000001 | 1.858 | 0.003 | 0.565 | 0.001 | 0.1242 | 0.0002
8544.595796 | -0.5 | 0.7 | 6117.2 | 8.7 | 84.5 | 1.0 | 35.143497 | 0.000001 | 1.780 | 0.005 | 0.546 | 0.001 | 0.1226 | 0.0002
8545.458728 | -3.2 | 0.7 | 6098.3 | 8.6 | 82.3 | 1.1 | 35.239870 | 0.000001 | 1.737 | 0.005 | 0.528 | 0.001 | 0.1218 | 0.0002
8545.572797 | -0.8 | 0.6 | 6095.5 | 8.6 | 80.0 | 1.0 | 35.231555 | 0.000001 | 1.781 | 0.004 | 0.536 | 0.001 | 0.1213 | 0.0002
8546.411967 | 0.8 | 0.7 | 6086.8 | 8.6 | 75.8 | 1.4 | 35.331340 | 0.000001 | 1.708 | 0.007 | 0.525 | 0.001 | 0.1210 | 0.0003
8546.513687 | 2.1 | 0.5 | 6083.9 | 8.6 | 75.4 | 1.1 | 35.317667 | 0.000001 | 1.723 | 0.005 | 0.533 | 0.001 | 0.1223 | 0.0002
8548.397384 | 2.2 | 0.9 | 6066.5 | 8.6 | 67.4 | 1.4 | 35.421875 | 0.000001 | 1.652 | 0.008 | 0.508 | 0.001 | 0.1179 | 0.0003
8816.630520 | 12.3 | 1.0 | 6082.9 | 8.6 | 68.2 | 2.7 | 35.492177 | 0.000001 | 1.815 | 0.018 | 0.540 | 0.002 | 0.1337 | 0.0006
8818.637903 | 6.4 | 0.7 | 6081.4 | 8.6 | 74.0 | 0.9 | 35.367111 | 0.000001 | 1.688 | 0.003 | 0.527 | 0.001 | 0.1245 | 0.0002
8841.694745 | 13.8 | 1.1 | 6126.3 | 8.7 | 70.1 | 2.4 | 35.303118 | 0.000001 | 1.862 | 0.015 | 0.557 | 0.002 | 0.1371 | 0.0006
8843.649122 | 8.9 | 0.8 | 6120.0 | 8.7 | 70.0 | 1.3 | 35.200034 | 0.000001 | 1.883 | 0.006 | 0.572 | 0.001 | 0.1280 | 0.0003
8847.607122 | 7.8 | 0.5 | 6116.3 | 8.6 | 75.4 | 1.1 | 35.215659 | 0.000001 | 1.813 | 0.005 | 0.553 | 0.001 | 0.1249 | 0.0002
8847.769535 | 7.7 | 0.6 | 6112.1 | 8.6 | 73.6 | 0.9 | 35.215072 | 0.000001 | 1.895 | 0.004 | 0.574 | 0.001 | 0.1249 | 0.0002
8854.634287 | 9.0 | 0.6 | 6094.6 | 8.6 | 64.1 | 0.9 | 35.308292 | 0.000001 | 1.762 | 0.003 | 0.567 | 0.001 | 0.1284 | 0.0002
8861.624299 | 16.1 | 0.8 | 6117.1 | 8.7 | 71.8 | 1.1 | 35.214263 | 0.000001 | 1.806 | 0.005 | 0.545 | 0.001 | 0.1241 | 0.0002
8861.707136 | 14.6 | 0.7 | 6113.0 | 8.6 | 70.8 | 0.9 | 35.198146 | 0.000001 | 1.795 | 0.004 | 0.537 | 0.001 | 0.1227 | 0.0002
8883.567735 | 15.6 | 1.0 | 6088.7 | 8.6 | 75.0 | 1.7 | 35.455835 | 0.000001 | 1.721 | 0.009 | 0.533 | 0.001 | 0.1215 | 0.0004
8887.493210 | 11.7 | 0.6 | 6098.0 | 8.6 | 67.3 | 0.9 | 35.326083 | 0.000001 | 1.735 | 0.003 | 0.528 | 0.001 | 0.1214 | 0.0002
8887.596530 | 13.0 | 0.7 | 6097.9 | 8.6 | 67.8 | 0.9 | 35.313566 | 0.000001 | 1.750 | 0.003 | 0.538 | 0.001 | 0.1227 | 0.0002
8899.553769 | 11.8 | 0.7 | 6093.7 | 8.6 | 72.3 | 1.0 | 35.331840 | 0.000001 | 1.725 | 0.004 | 0.533 | 0.001 | 0.1210 | 0.0002
8908.534212 | 15.5 | 0.6 | 6117.8 | 8.7 | 64.7 | 0.9 | 35.174930 | 0.000001 | 1.829 | 0.004 | 0.551 | 0.001 | 0.1219 | 0.0002
8908.651325 | 16.2 | 0.6 | 6119.5 | 8.7 | 67.8 | 1.1 | 35.199129 | 0.000001 | 1.791 | 0.005 | 0.548 | 0.001 | 0.1225 | 0.0002
8910.484569 | 13.5 | 0.6 | 6121.2 | 8.7 | 72.1 | 0.9 | 35.157370 | 0.000001 | 1.795 | 0.004 | 0.557 | 0.001 | 0.1239 | 0.0002
8915.440466 | 13.7 | 0.6 | 6096.9 | 8.6 | 74.5 | 0.8 | 35.285193 | 0.000001 | 1.763 | 0.003 | 0.543 | 0.001 | 0.1211 | 0.0002
8915.533771 | 11.6 | 0.5 | 6088.2 | 8.6 | 77.4 | 1.2 | 35.348770 | 0.000001 | 1.721 | 0.006 | 0.533 | 0.001 | 0.1212 | 0.0003
9656.565329 | 16.8 | 0.9 | 6063.3 | 8.6 | 62.0 | 1.3 | 35.432578 | 0.000001 | 1.693 | 0.007 | 0.529 | 0.001 | 0.1235 | 0.0003
9658.443411 | 18.9 | 0.8 | 6079.5 | 8.6 | 65.7 | 1.3 | 35.369161 | 0.000001 | 1.702 | 0.008 | 0.529 | 0.001 | 0.1241 | 0.0003
9659.567838 | 16.5 | 0.8 | 6078.8 | 8.6 | 68.7 | 0.8 | 35.317963 | 0.000001 | 1.740 | 0.004 | 0.543 | 0.001 | 0.1243 | 0.0002
9670.406369 | 13.2 | 0.7 | 6067.5 | 8.6 | 68.3 | 0.9 | 35.399315 | 0.000001 | 1.742 | 0.004 | 0.544 | 0.001 | 0.1229 | 0.0002

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