# The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

## I. Sample definition and characterization*,*,*,***

S. Desidera<fnref n="1" />, E. Covino<fnref n="2" />, S. Messina<fnref n="3" />, J. Carson<fnref n="4" />,<fnref n="5" />, J. Hagelberg<fnref n="6" />, J. E. Schlieder<fnref n="5" />, K. Biazzo<fnref n="3" />, J. M. Alcalá<fnref n="2" />, G. Chauvin<fnref n="7" />, A. Vigan<fnref n="8" />, J. L. Beuzit<fnref n="7" />, M. Bonavita<fnref n="1" />, M. Bonnefoy<fnref n="5" />, P. Delorme<fnref n="7" />, V. D’Orazi<fnref n="9" />,<fnref n="1" />, M. Esposito<fnref n="10" />,<fnref n="2" />, M. Feldt<fnref n="5" />, L. Girardi<fnref n="1" />, R. Gratton<fnref n="1" />, T. Henning<fnref n="5" />, A. M. Lagrange<fnref n="7" />, A. C. Lanzafame<fnref n="3" />,<fnref n="11" />, R. Launhardt<fnref n="5" />, M. Marmier<fnref n="6" />, C. Melo<fnref n="12" />, M. Meyer<fnref n="13" />, D. Mouillet<fnref n="7" />, C. Moutou<fnref n="8" />, D. Segransan<fnref n="6" />, S. Udry<fnref n="6" />, and C. M. Zaidi<fnref n="7" />

Received 2 December 2013 / Accepted 22 April 2014

## ABSTRACT

**Context.** Young, close stars are ideal targets for searching planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results, particularly since the luminosity of substellar objects has a strong dependence on system age.

**Aims.** We have conducted a large program with NaCo at the VLT to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, and mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics.

**Methods.** We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and the results that are available in the literature. Additionally, we exploited photometric time-series, which are available in ASAS and Super-WASP archives, to derive a rotational period for a large fraction of our program stars.

**Results.** We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50 $M_\odot$, with a median value of 1.01 $M_\odot$. The typical metallicity is close to solar with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of close young moving groups. Eight spectroscopic binaries are identified.

**Key words.** stars: fundamental parameters – stars: rotation – stars: activity – stars: pre-main sequence – binaries: general – stars: kinematics and dynamics

## 1. Introduction

High-angular resolution deep imaging in the near-infrared maximizes the capability to detect faint circumstellar bodies amid the large brightness of the central star (Absil & Mawet 2010). The first detections of comoving companions with planetary mass were obtained using deep VLT/NaCo infrared imaging with contrasts up to 6–8 mag at $>0.5$ arcsec separation around very young objects, such as 2MASS J1207334–393254 (Chauvin et al. 2004) and AB Pic (Chauvin et al. 2005).

<footnote n="1">¹ INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
e-mail: silvano.desidera@oapd.inaf.it</footnote>

<footnote n="2">² INAF – Osservatorio Astronomico di Napoli, Salita Moiariello 16, 80131 Napoli, Italy</footnote>

<footnote n="3">³ INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy</footnote>

<footnote n="4">⁴ Department of Physics & Astronomy, College of Charleston, 58 Coming St. Charleston, SC 29424, USA</footnote>

<footnote n="5">⁵ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</footnote>

<footnote n="6">⁶ Geneva Observatory, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland</footnote>

<footnote n="7">⁷ Institut de Planétologie et d'Astrophysique de Grenoble, UJF, CNRS, 414 rue de la piscine, 38400 Saint-Martin d'Hères, France</footnote>

<footnote n="8">⁸ Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, France</footnote>

<footnote n="9">⁹ Department of Physics and Astronomy, Faculty of Science, Macquarie University, Sydney NSW, 2109, Australia</footnote>

<footnote n="10">¹⁰ Instituto de Astrofísica de Canarias, C/ Via Lactea, s/n, 38205 La Laguna, Tenerife, Spain</footnote>

<footnote n="11">¹¹ Università di Catania, Dipartimento di Fisica e Astronomia, via S. Sofia 78, 95123 Catania, Italy</footnote>

<footnote n="12">¹² European Southern Observatory, Casilla 19001 Santiago 19, Chile</footnote>

<footnote n="13">¹³ Institute for Astronomy, ETH Zurich, Wolfgang-Pauli Strasse 27, 8093 Zurich, Switzerland</footnote>

<footnote>* Based on observations collected at La Silla and Paranal Observatory, ESO (Chile) using FEROS, HARPS, and NaCo; with the CORALIE echelle spectrograph mounted on the 1.2 m Swiss telescope at La Silla Observatory; and on the All Sky Automated Survey (ASAS) photometric data.</footnote>

<footnote>** Tables 1–4, 6, 8 and Appendices are available in electronic form at http://www.aanda.org</footnote>

<footnote>*** Tables 9–12 and D.1 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/573/A126</footnote>
After these earliest discoveries, improvements in data acqui-
sition and data analysis techniques (e.g. the introduction of an-
gular differential imaging, Marois et al. 2006) allowed the detec-
tion of the first objects that were likely formed in protoplanetary
disks, such as the four-planet system orbiting HR 8799 (Marois
et al. 2008, 2010) and the giant planet orbiting at 8 AU from
the well known star-disk system β Pic (Lagrange et al. 2010). In
the last year, several additional discoveries of directly-imaged
planets have been reported (Rameau et al. 2013; Kuzuhara et al.
2013; Currie et al. 2014).

Several surveys were also carried out with published detec-
tion limits for hundreds of objects (e.g., Masciadri et al. 2005;
Lafrenière et al. 2007; Chauvin et al. 2010). These observa-
tions allowed a first estimate of the frequency of giant plan-
ets in wide orbits (Nielsen & Close 2010). There are exciting
prospects for the detection of planets of lower masses (below
1 *M*<sub>I</sub>), and of smaller semimajor axes, thanks to the availability
of new instrumentation, such as SPHERE at VLT (Beuzit et al.
2010), GPI at Gemini-South (Macintosh et al. 2008), SCExAO
at Subaru (Martinache & Guyon 2009), and LBTI (Hinz et al.
2008; Esposito et al. 2011).

As the luminosity of substellar objects is strongly dependent
on age (Burrows et al. 1997; Baraffe et al. 2003), the determina-
tion of the mass of a detected planet, or the derivation of detec-
tion limits in terms of planetary mass, requires a careful evalu-
ation of the stellar age. Other parameters, such as stellar mass,
metallicity, distance to the system, multiplicity, and membership
to associations are also required for a proper interpretation of the
results in terms of both positive detections and statistics of the
whole survey. Such comprehensive knowledge allows for mean-
ingful comparisons with the outcomes of other planet-search
projects using different techniques (e.g., Fischer & Valenti 2005;
Mayor et al. 2011) and outcomes from planet formation models
(Mordasini et al. 2009, 2012; Boss 1997; Vorobyov et al. 2013).

The determination of stellar age is a challenging task, espe-
cially for isolated field objects (Soderblom 2010). A variety of
indicators can be used, such as isochrone fitting, lithium con-
tent, chromospheric and coronal emission, stellar rotation, and
kinematics. The various indicators have complementary sensi-
tivities for stars of different spectral types and different ages.
Furthermore, some diagnostics like those related to rotation and
magnetic activity might give spuriously young ages as in the
case of tidally-locked binaries. Therefore, the best results are
obtained from a complete examination of all possible indicators
and by a careful and suitable combination of their results.

The NaCo Large Programme (NaCo-LP, PI. J.L. Beuzit) is
a coordinated European effort, aimed at conducting an homoge-
neous and systematic study of the occurrence of extrasolar gi-
ant planets (EGPs) and brown dwarfs (BDs) in wide orbit (5–
500 AU) around young, close stars. First epoch observations
were performed in 2009–2010 and the follow-up observations
for the confirmation of physical association of the candidates to
their central stars were completed in March 2013. First results
include the characterization of the debris disk around HD 61005
(Buenzli et al. 2010) and the study of the astrophysical false
alarm represented by the white dwarf around HIP 6177, which
mimics a substellar object at near-infrared (NIR) wavelengths
(Zurlo et al. 2013).

The goal of this paper is to provide detailed stellar character-
ization of the targets of the NaCo-LP, based on high-resolution
spectroscopic data acquired for this purpose, and the spectro-
scopic and photometric data available from public archives,
complemented by information from the literature. The com-
panion paper (Chauvin et al. 2015) presents the deep imaging

observations and their results. Results from the NaCo-LP sam-
ple are merged with those of other surveys of comparable depth
to produce a comprehensive statistical analysis of the occurrence
of giant planets in wide orbits around FGK stars (Vigan et al.,
in prep.) and a complementary study of the brown dwarf popu-
lation (Reggiani et al., in prep.).

The layout of this paper is the following. In Sect. 2, we in-
troduce the target sample while we present the spectroscopic
dataset and describe the data reduction procedures in Sect. 3.
In Sect. 4, we present the spectroscopic analysis performed to
determine radial and projected rotational velocities to measure
the lithium line 6707.8 Å strength and to derive effective tem-
perature. In Sect. 5, we present the analysis of photometric time
series to derive the rotation period; in Sect. 6, we examine mag-
netic activity diagnostics Ca II H and K and X-ray emission. In
Sect. 7, we report the presence of possible stellar companions;
we analyze the kinematic parameters supporting the membership
to known nearby associations in Sect. 8. We evaluate distances
and metallicities of the targets and infer stellar masses and ages
in Sect. 9. In Sect. 10, we summarize our results. In Appendix A,
we report the compilation of data available in the literature for
our targets and in Appendix B, we describe individual targets.
In Appendix C, we provide our calibration of chorospheric
emission for FEROS spectra; while the details of our search
for rotation period on photometric time series are presented in
Appendix D.

## 2. Sample selection

The target selection was based on an initial compilation of about
one thousand young nearby stars, based on various literature
sources and dedicated observations and assembled in prepara-
tion for the SPHERE GTO survey (Mouillet et al. 2010). The
youth diagnostics include high lithium content, Ca II H and
K line chromospheric emission, Hα emission, X-ray activity,
rotation rate, and kinematics. From that list, objects that were
within a distance horizon of 100 pc, were younger than 200 Myr<fnref n="1" />,
and had a magnitude limit of approximately *R* < 9.5 were
selected<fnref n="2" />. Furthermore, known spectroscopic and close visual
(separation <6 arcsec) binaries were rejected, to have a sample as
free as possible from dynamical perturbations to planets in wide
orbits and to avoid potential problems with the quality of adap-
tive optics (AO) wavefront sensing, as posed by the presence of
a close stellar companion. For spectroscopic binaries, there are
no technical difficulties for AO observations, as the components
are not spatially resolved, but we decided, nevertheless, to fo-
cus our attention on single stars and on individual components
of wide binaries. This allows us to get more statistically signif-
icant inferences and to have a sample more suited for compari-
son with the frequency of giant planets in wide orbits, as derived
from radial velocity (RV) surveys. The study of the frequency of
circumbinary planets is deferred for a separate study (Bonavita
et al., in prep.).

The resulting list was cross-correlated with that of recent
direct imaging surveys achieving similar sensitivities to our
project. The 90 objects that were already observed with ade-
quate depth were excluded and the final sample of the NaCo-
LP is formed by about 110 targets that were never observed

<footnote n="1">¹ Three objects slightly older than 200 Myr were observed in the July 2010 run because of the lack of suitable targets in the original target list.</footnote>

<footnote n="2">² More precisely, the sample selection is based on the expected sensi-
tivity limits for the SPHERE adaptive optics sensor, which also depends
on the color of the star.</footnote>
with deep imaging instruments. Eighty-six of these originally
selected 110 stars were observed at the telescope and form the
sample studied in this paper (Table 9). The remaining 25 were
not observed due to weather or technical losses. The previously
published wide companions of the targets were also considered
in our study even when they were not observed as part of NaCo-
LP because of the constraints they provided on the parameters of
the system (e.g., age, and distance). The pending statistical anal-
ysis on the frequency of planetary-mass objects in wide orbits
will be based on the whole sample of about 200 objects, which
combines targets observed by NaCo-LP and observational re-
sults from the literature (Vigan et al., in prep.).

Final values for the stellar parameters derived in this paper
might lie outside of the original selection criteria due to the avail-
ability of new observational determinations, improvements in
adopted calibrations, or a better understanding of the physical
nature of the systems being investigated.

**3. Spectroscopic data**

For the spectroscopic characterization of our targets, we used
data acquired with several instruments. Some of the spectra were
specifically acquired by us to characterize the targets. Other
spectra were accessed through the NaCo-LP collaboration and
from public archives.

**3.1. FEROS spectra**

High-resolution spectra were collected using FEROS as part
of preparatory observations for the SPHERE GTO sur-
vey. Observations were performed during several runs from
November 2008 to March 2010 as part of Max Planck Institut
für Astronomie (MPIA) observing time. The OBJ+SKY mode
of FEROS was preferred to avoid contamination by Th-Ar lines,
as we are more interested in having clean spectra for stellar char-
acterization purposes rather than attaining the highest RV preci-
sion. Integration times were selected to obtain a signal-to-noise
ratio of about 100 for stars brighter than V ~ 9. In addition, we
exploited FEROS spectra that are available from the ESO public
data archive<fnref n="3" />. These latter data were taken with various FEROS
instrument set-ups and have a variety of signal-to-noise ratios.
Altogether, we considered 77 spectra for 64 stars in this paper.

The FEROS spectra extend between 3600 Å and 9200 Å
with a resolving power R = 48 000 (Kaufer et al. 1999). All
the data were reduced using a modified version of the FEROS-
DRS pipeline (running under the ESO-MIDAS context FEROS),
which yields the wavelength-calibrated, merged, and normalized
spectrum. The reduction steps were the following: bias subtrac-
tion and bad-column masking; definition of the echelle orders
on flat-field frames; subtraction of the background diffuse light;
order extraction; order-by-order flat-fielding; determination of
wavelength-dispersion solution by means of ThAr calibration-
lamp exposures; order-by-order normalization; rebinning to a
linear wavelength-scale with barycentric correction; and merg-
ing of the echelle orders.

We also considered FEROS spectra of our targets obtained
by Torres et al. (2006), that were reduced with the instrument
pipeline and kindly provided to us by the SACY team. We re-
frained from systematically repeating the measurement of the
spectroscopic parameters, but we considered the SACY spectra
for in-depth evaluation of individual cases (e.g., suspected spec-
troscopic binaries), as reported in Appendix B.

**3.2. HARPS spectra**

For our investigation, we also considered the spectra obtained
with HARPS at the ESO 3.6 m telescope in La Silla (Mayor
et al. 2003) as part of planet search surveys by the Geneva team
(Mayor et al. 2011) and the Lagrange et al. (2009) RV survey
of early-type stars. We also retrieved additional HARPS spec-
tra available in the ESO archive. Most of these come from
the RV survey for planets around young stars by Guenther
& Esposito (2007) with a few individual spectra from other
projects. Overall, we have considered HARPS spectra for 13 ob-
jects with the number of spectra per object ranging from 1 to 77.

**3.3. CORALIE spectra**

Observations of 11 targets were performed with the CORALIE
spectrograph at the Euler 1.2 m telescope in La Silla from
January 2012 to August 2013 with the main goal of checking the
binarity of the objects in our sample through RV determination
and line profile evaluation. The spectra were reduced with the
instrument on-line pipeline. Spectra of six additional stars ob-
served as part of the CORALIE exoplanet search survey (Udry
et al. 2000) were also considered in our analysis.

**3.4. Other data**

Two spectra of HIP 46634 (kindly provided by the SOPHIE
Consortium) obtained with the SOPHIE spectrograph at
the Haute Provence 1.93 m telescope were considered to de-
rive the star’s activity level. We also analyzed the CES spectra
of the components of HD 16699 A and B obtained by Cutispoto
et al. (1999); kindly provided by L. Pastori) to understand the
origin of discrepancies between results from the literature and
results from our own analysis, which turned out to be due to
an exchange of binary system components (see Appendix B for
details).

**4. Determination of spectroscopic parameters**

We exploited the FEROS, HARPS, and CORALIE spectra to
measure several spectroscopic parameters that are useful for stel-
lar characterization and age determination. Our determinations
(i.e., heliocentric RV, v sin i, effective temperature, lithium equiv-
alent width, S-index, and log R<sub>HK</sub>) are listed in Tables 1–4 for
the different datasets, and the procedure to measure them are
described below. The final adopted values, including literature
measurements, are listed in Table 10 for RV and Table 11 for the
other spectroscopic parameters.

**4.1. Projected rotational velocity and radial velocity**

**4.1.1. FEROS**

The heliocentric RV and the projected rotational velocity (v sin i)
were determined by cross-correlating the object spectra with
low-v sin i template spectra (HD 80170, K5 III-IV, and RV ~
0 km s⁻¹), as obtained with the same instrument and reduced
in the same way. The normalized target spectra were prelim-
inarily rebinned to a logarithmic wavelength scale and split
into six wavelength-ranges that were free of emission lines and
of telluric absorptions (see Esposito et al. 2007). A Gaussian
profile was fitted to the peak of the cross-correlation function
(CCF), computed in each of the six distinct spectral ranges.
The resulting RV values were averaged with appropriate weights

<footnote n="3">³ archive.eso.org</footnote>
(Schisano et al. 2009). The projected rotational velocity $v \sin i$ was derived from the full width half maximum (FWHM) of the cross-correlation peak in each of the six ranges above. The relation FWHM-$v \sin i$ was obtained by convolving the template spectra with rotational profiles of $v \sin i$ from 1 to 100 km s$^{-1}$. Our measurements of heliocentric RV and $v \sin i$ are listed in Table 1.

### 4.1.2. HARPS and CORALIE

The RV and FWHM of CCF are directly delivered by the instrument pipelines, which are based on the Weighted CCF technique (Pepe et al. 2002). For moderately fast rotators, the correlation was performed by increasing the width of the region used in the CCF fit according to the line width. For some very fast rotators ($v \sin i \sim 50$ km s$^{-1}$) observed with CORALIE, we simply measured the positions of a few very strong lines in the spectra to derive the RVs. For fast-rotating A and F type stars observed with HARPS, we also obtained differential RV using the SAFIR code (Galland et al. 2005), which is optimized for this kind of analysis. The transformation between FWHM and $v \sin i$ was performed as described in Santos et al. (2002). Spectroscopic parameters derived from CORALIE and HARPS spectra are listed in Tables 2–4.

### 4.2. Lithium equivalent width

The equivalent width (EW) measurements of the Li 6707.8 Å resonance line were obtained by a Gaussian fit, and the results are reported in Tables 1 and 4 for FEROS and HARPS spectra respectively. The listed EW does not include corrections for blends with close lines, which occur for stars with significant rotation. Typical measurement errors are of the order of $\le 5$ mÅ, while they are up to $\sim 50$ mÅ for fast rotators.

### 4.3. $T_{\text{eff}}$ determinations

The determinations of the spectroscopic effective temperature in Tables 1 and 4 for FEROS and HARPS spectra, respectively, were obtained through the method based on EW ratios of spectral absorption lines. These were acquired by means of the ARES<fnref n="4" /> automatic code (Sousa et al. 2007) using the calibration for FGK dwarf stars by Sousa et al. (2010). The quoted errors are the internal ones and do not include calibration uncertainties. When multiple spectra are available, we list the mean values and the error of the mean, which are below 10 K and well below systematics. For rotational velocity above $\approx 20$ km s$^{-1}$, the number of measured line-ratios drops drastically with correspondingly larger errors due to increased line blending. The temperature determinations become less reliable for $v \sin i$ larger than 30 km s$^{-1}$ (Desidera et al. 2011). For five stars with both FEROS and HARPS spectra available, the spectroscopic temperatures resulting from the two instruments are fully consistent (mean difference $\Delta T_{\text{eff(FEROS-HARPS)}} = -4$ K with an rms dispersion of 34 K). Four stars have more than ten spectra with HARPS, enabling an estimate of the intrinsic variability of effective temperature, which results in 20–50 K rms. In some cases, as shown in Fig. 1 for HIP 32235, temperature variations show significant correlations with chromospheric activity. This is due to large spots covering the stellar photosphere when the star is active. This issue is further examined in a forthcoming study.

<figure><img src="image_1.png" /><figcaption>Fig. 1. Variations in effective temperature as measured by applying ARES on HARPS spectra of HIP 32235. The temperature is displayed as a function of S index chromospheric emission.</figcaption></figure>

(Messina et al., in prep.). Larger temperature variations ($\ge 100$ K) are expected to be present for the stars in our sample with very high levels of magnetic activity and photometric variability (see, e.g., Frasca et al. 2005).

Photometric temperatures were obtained from B-V, V-I, and V-K colors using the calibrations by Casagrande et al. (2010; adopting metallicity from the literature when available (see Sect. 9.2) and assuming solar metallicity otherwise). The comparison between photometric and spectroscopic temperatures (Fig. 2) shows that stars with faster rotation show larger dispersion, as expected for an increasing role of line blending. Large scatter is also observed for F-type stars. This is likely due to the moderately fast rotation of most of these stars in our sample and also due to an effective temperature, which is close to the limit of the Sousa et al. (2010) calibration or even beyond it in some cases. The available spectral types further support the photometric temperatures in these discrepant cases.

When considering only stars with $v \sin i \le 15$ km s$^{-1}$ and FEROS spectra (24 stars), the mean difference (photometric minus spectroscopic temperatures) is -52 K with an rms dispersion of 111 K. A systematic trend, with the spectroscopic temperature being warmer, appears to be present below 5300 K, while results for solar-type stars agree very well (mean difference -2 K with rms dispersion of 79 K for 16 stars with $v \sin i < 15$ km s$^{-1}$ and $T_{\text{eff}} > 5400$ K).

Small amounts of interstellar or circumstellar absorption might be present in some individual cases, therefore biasing the photometric temperature, but this is not a general explanation for the systematic offset observed for the coolest stars. A similar discrepancy in effective temperature for cool stars was observed by Sousa et al. (2008), when comparing their spectroscopic temperatures with those based on the infrared flux method as implemented by Casagrande et al. (2006). This was interpreted by Sousa et al. (2008) as being due to the increasing errors in the spectroscopic analysis at cooler temperatures, as the analysis is differential with respect to the Sun.

Considering the additional uncertainties that are specific to active young stars, such as photometric and spectroscopic variability, the effects of magnetic activity on the stellar atmospheric structure, and a slightly lower gravity for the youngest stars, we consider the agreement between photometric and spectroscopic temperature satisfactory. A full understanding of the

<footnote n="4">⁴ http://www.astro.up.pt/~sousasag/ares/</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 2.** Spectroscopic vs. photometric effective temperatures. Blue filled circles: stars with FEROS spectra and $v \sin i < 15$ km s$^{-1}$; blue empty circles: stars with FEROS spectra and $15 < v \sin i < 30$ km s$^{-1}$; blue empty triangles: stars with FEROS spectra and $v \sin i > 30$ km s$^{-1}$; red filled squares: stars with HARPS spectra.</figcaption></figure>

contribution of these source of errors on spectroscopic and pho-
tometric temperatures is beyond the scope of this paper.

The temperature calibration by Casagrande et al. (2010) is mostly based on old stars. Its application to our sample should then be checked. Pecaut & Mamajek (2013) have recently developed an effective temperature scale which is optimized for 5–30 Myr old stars, and then applicable to a significant fraction of our targets. We considered the stars in their Table 9 with an effective temperature range between 4000 to 7000 K and compared to the effective temperatures derived from Casagrande et al. (2010) calibration using B–V, V–I and V–K colors. The results are shown in Fig. 3. These results show that there is no significant offset between the two temperature scales (mean difference of +3 K and median –3 K for single stars) with a scatter of 34 K with a possible trend vs temperature. We also compared the effective temperatures for Sco-Cen members from Pecaut et al. (2012) and find comparable results.

Therefore, the differences of effective temperatures from col-
ors (at least for the combination of colors we used) are quite
small. This is consistent with the difference of 40 K with respect
to Casagrande et al. (2011) for six stars in common as quoted in
Pecaut & Mamajek (2013). The difference is instead much larger
for temperatures derived from spectral types.

There is another concern in the application of Pecaut &
Mamajek (2013) relations to our sample stars: if the origin for
the differences in temperature scale of main sequence and pre-
main sequence stars is linked to the lower stellar gravity at the
youngest age, its use should be limited to stars younger than
about 30 Myr (and possibly even younger for F-G stars). If in-
stead this is due to the effects of phenomena related to the mag-
netic activity, as plages and star spots (see their Sect. 5), then the
calibration should be applied also to stars up to 100–120 Myr
old, which have similar activity levels of β Pic and Tuc-Hor MGs
members, and old tidally-locked binaries.

Henceforth, we adopt the photometric temperatures using
the Casagrande et al. (2010) scale, as these are homogeneously

<figure><img src="image_3.png" /><figcaption>**Fig. 3.** Comparison between photometric effective temperatures obtained using Casagrande et al. (2010) calibration for B − V, V − I, and V − K color to the effective temperatures of the 5–30 Myr stars considered in Pecaut & Mamajek (2013; their Table 9, BT-Settl models). Close visual binaries and spectroscopic binaries are plotted as open circles; single stars and components of wide binaries are filled circles.</figcaption></figure>

available for all targets and are likely more accurate than the
spectroscopic temperature for cool stars and objects with high
$v \sin i$, as discussed above.

**5. Rotational periods**

**5.1. Data**

In the present study, we use photometric time-series data to in-
vestigate the variability of our targets and, specifically, to infer
their rotational periods, brightest (least spotted) magnitudes, and
levels of magnetic activity at a photospheric level.

The photometric data were retrieved mainly from three pub-
lic archives: the All Sky Automated Survey (ASAS<sup>5</sup>, Pojmanski
1997, 2002), the Wide Angle Search for Planets (SuperWASP<sup>6</sup>,
Pollacco et al. 2006; Butters et al. 2010), and the HIPPARCOS
catalog<sup>7</sup> (Perryman et al. 1997).

5.1.1. The ASAS photometry

The ASAS project monitors all stars brighter than V = 14 mag at declinations δ < +28° with a typical sampling of 2 days. Since the ASAS archive contains data from 1997 to date, the time-series that it provides are particularly suitable for investigating variability over different time scales, specifically for probing the activity-induced rotational modulation. The ASAS program provides aperture photometry through five apertures. For each star in our sample, we adopted the aperture that gave the highest photometric precision (i.e., the minimum average magnitude uncertainty), which is the range 0.02–0.03 mag for target stars under analysis.

<footnote n="5">⁵ www.astrouw.edu.pl/asas/</footnote>

<footnote n="6">⁶ www.wasp.le.ac.uk/public/</footnote>

<footnote n="7">⁷ vizier.u-strasbg.fr/viz-bin/VizieR?-source=I%2F239</footnote>
### 5.1.2. The SuperWASP photometry

The public SuperWASP light curves are available for a time interval from 2004 to 2008 for both the northern and southern observatories. Although temporal and spatial coverage are irregular, SuperWASP stars at the most favorable sky declinations have observation sequences up to nine hours long with a sampling of about ten minutes, making the data more sensitive than that of ASAS for revealing periods <1 d. Our analysis is based on the processed flux measurements obtained through the application of the SYSREM algorithm (Tamuz et al. 2005). The typical photometric accuracy for the targets under study is on the order of 0.01–0.02 mag. Owing to differences with respect to the standard Johnson V-band ASAS photometry, we decided to analyze the SuperWASP dataset independently without merging it with ASAS data. SuperWASP observations from 2004 to 2005 were collected without a filter with the spectral transmission being defined by the optics, detector, and atmosphere. In the subsequent years, observations were collected through a wide-band filter (400–700 nm).

### 5.1.3. The HIPPARCOS photometry

For a limited number of targets, HIPPARCOS photometry was also available. However, owing to very irregular sampling and low photometric precision, we were able to derive rotation periods for only a handful of these stars.

### 5.1.4. Data from the literature

For all of our targets, we searched the literature for published period determinations. We focused on published measurements that used the same time-series as our own measurements, which includes the ASAS Catalogue of Variable Stars (ACVS), and the search for variable stars from SuperWASP (Norton et al. 2007). We also retrieved 17 rotation periods from Messina et al. (2010, 2011), and 22 rotation periods from other sources (see Appendix B). For most of the published periods, we were able to confirm the values with our own analyses. We relied solely on literature values for only HIP 46637 and HIP 71908.

## 5.2. Photometry rotation period search

We used the Lomb-Scargle periodogram method (Press et al. 1992; Scargle 1982; Horne & Baliunas 1986) and the Clean algorithm (Roberts et al. 1987) to search for the rotation periods. As demonstrated in Messina et al. (2010, 2011), the most accurate approach to infer the rotation period of late-type stars from the light rotational modulation is to perform the period search on the whole time-series and on associated time segments when a sufficiently long time-series is available (generally longer than one observing season). This approach not only speeds up the period detection process but also prevents other phenomena, such as the growth and decay of active regions, whose typical timescales are longer than the period of the rotational modulation from distorting period determinations.

For the present investigation, we had at our disposal the ASAS time-series up to 10 yr long and the SuperWASP time-series up to 4 yr long. We therefore segmented both datasets into sub-time-series, with each series corresponding typically to one yearly observation season. This approach was unsuitable for HIPPARCOS data, owing to low and uneven sampling; in this case, the analysis was only performed on the whole time-series.

A detailed description of the period search method is given in Messina et al. (2010). We briefly recall here that the false alarm probability (FAP) associated with the period determination is computed by using Monte Carlo bootstrap methods on 1000 simulated light curves; the FAP is the probability that a peak of a given height in the periodogram is caused simply by statistical variations, which is due to Gaussian noise. For each complete time-series and for each time segment, a corresponding FAP was computed. Only periods with FAP ≤ 1% were retained for subsequent analysis. The uncertainty associated with each period was computed from the FWHM of the main power peak in the window function, following the methods of Lamm et al. (2004).

## 5.3. Period results

The results of our period search are summarized in Table 11, where we list the rotation period, its uncertainty, and a flag on the confidence level of the determination for each target. On a sample of 99 targets, we were able to determine the rotation period for 70 objects. Specifically, 27 periods are determined in this study for the first time, while the remaining 43 are retrieved from the literature (17 out of 43 from Messina et al. 2010, 2011). For 25 out of these 43 targets, we were able to retrieve either ASAS or SuperWASP photometry, carry out our independent analysis, and confirm the literature values. As described in Messina et al. (2011), periods derived in at least five segments or fewer than five segments with an independent confirmation from the literature, and that are consistent with $v \sin i$, are referred to as *confirmed periods* (C). Periods derived from fewer than five time segments but are consistent with $v \sin i$, and that produce mean sinusoidal fit residuals smaller than the light-curve amplitude in at least five segments, are referred to as *likely periods* (L). Periods derived from fewer than five segments that produce mean sinusoidal fit residuals that are lower than the light-curve amplitude in fewer than five segments, or with only 1–2 determinations in the literature, or that are inconsistent with $v \sin i$, are referred to as *uncertain periods* (U). We have 40 *confirmed* periods, 14 *likely* periods, 14 *uncertain* periods, and two taken from the literature alone.

We could not determine the rotation periods for 29 out of 99 stars in our sample. Sixteen of the 29 stars with unknown periods have spectral types earlier than F8. These stars are expected to have very shallow external convection zones and, consequently, very low activity levels. Therefore, any eventual rotational modulation is unlikely to be detected by analysis of ground-based data<fnref n="8" />. In the case of HIP 71908 (F1Vp), a low-amplitude (~5 mmag) modulation was detected by space-based observations (Bruntt et al. 2009). The remaining 13 stars, although of late spectral type, exhibited non-periodic variability. In several cases, they are members of binary systems which are not spatially resolved in ASAS and Super-WASP images; ASAS and Super-WASP have pixel scales of 15.5 and 13.7 arcsec respectively (Pojmański 2001). Individual cases are discussed in Appendix B. A summary of the results of our period search for the individual seasons and additional details are provided in Appendix D.

<footnote n="8">⁸ An exception is represented by HD 32981 (F8V). F-type stars occasionally exhibit spots sufficiently large enough to induce light modulation with amplitude of a few hundredths of a magnitude (see, e.g., García-Alvarez et al. 2011), thus enabling detection from ground-based observatories.</footnote>
**6. Activity diagnostics**

Magnetic activity and related phenomena are known to depend on rotational period and also on stellar age for stars of spectral types from mid-F to mid-M. In this section, we consider indicators of chromospheric and coronal activity.

**6.1. Ca II H and K emission**

Chromospheric emission in CaII H and K lines was determined by measuring the *S*-index on the FEROS spectra, as described in Desidera et al. (2006). Details on the calibration of our instrumental *S*-index into the standard Mt. Wilson scale are provided in Appendix C. The procedures adopted for HARPS and CORALIE are described in Lovis et al. (2011) and Marmier (2012), respectively. The activity measurements obtained with the three instruments are presented in Tables 1, 2, and 4. Most of the measurements obtained with FEROS are single-epoch, while those from the CORALIE planet search and some of those from HARPS archive are multi-epoch over months or years, which then partially average the variability of the chromospheric emission on timescales of the rotation period and the activity cycle of the star. The activity measurement of HIP 46634 was obtained by the SOPHIE Consortium by following the procedures described in Boisse et al. (2010). When available, we also considered additional data from the literature (Appendix A).

**6.2. X-ray emission**

The target list was cross-correlated with the ROSAT all-sky survey (RASS) catalog (Voges et al. 1999, 2000), adopting a matching radius of 30 arcsec. The X-ray fluxes were derived using the calibration by Hünsch et al. (1999). For wide multiple systems that were unresolved by ROSAT (see Table 6), a suitable correction to the flux was included on the basis on the bolometric flux ratio of the components. In a couple of cases (HD 16699 A and B; HIP 72399/72400), the availability of XMM observations at higher spatial resolution enabled us to identify the main source of the X-ray emission in a binary system. For the systems HIP 35564 and HIP 25434/6, whose primaries are early-F stars, we assumed that the whole X-ray emission comes from the secondary. However, this assumption is uncertain, as both primaries are spectroscopic binaries and then the additional late-type star might contribute significantly to the integrated X-ray flux.

The hardness-ratios $HR1 = (B - A)/(B + A)$ and $HR2 = (D-C)/(D+C)$, where A, B, C and D are the integrated counts in the energy range 0.11–0.41 keV, 0.52–2.01 keV, 0.52–0.90 keV, and 0.91–2.01 keV, respectively, are plotted in Fig. 4. The two stars TYC 7743-1091-1 and TYC 6781-0415-1 are found to be hard X-ray sources with HR1 close to 1. Three stars, HIP 71933, TYC 6818-1336-1 and TYC 5736-0649-1, are moderately hard sources (HR1 ~ 0.4–0.6). The hardness-ratios can be used to derive clues on stellar age, as the members of young moving groups 10–30 Myr old typically have soft X-ray emission, while hard emission is observed for classical T Tauri stars (Neuhaeuser et al. 1995; Kastner et al. 2003). Hard X-ray emission might in principle be due to interstellar or circumstellar absorption (Kastner et al. 2003), but the aforementioned hard X-ray sources are likely to exhibit emission due to flare activity (see Stelzer et al. 2000, and references therein).

For stars which are not detected by ROSAT, upper limits on X-ray luminosity were derived by considering the integration time of the nearest X-ray source in the ROSAT Faint Source Catalog.

<figure><img src="image_4.png" /><figcaption>**Fig. 4.** Hardness-ratios diagram for the NaCo-LP targets. The two sources with HR1 closest to 1 are TYC 7743-1091-1 and TYC 6781-0415-1.</figcaption></figure>

To estimate the ratio of X-ray to bolometric luminosity $R_X = \log(L_X/L_{bol})$, we derived the luminosities of the targets using the apparent *V* magnitude, the bolometric correction from Flower (1996) and the distances derived in Sect. 9.1. We converted the bolometric magnitude, defined as $M_{bol} = V + BC_V + 5 \log \pi + 5$ to $L/L_{\odot}$ by using $M_{bol\odot} = 4.73$, as recommended by Torres (2010). The interstellar extinction was assumed to be negligible since all targets are relatively nearby, except for a few individual cases where evidence of modest reddening existed (see Sect. 9.1 and Appendix B). X-ray luminosities and $\log(L_X/L_{bol})$ are listed in Table 11.

**6.3. Correlations of activity indicators and rotation**

Coronal and chromospheric emissions are in general expected to show correlation with the rotation period, as their origin is tied to the rotation itself (see, e.g., Pizzolato et al. 2003). On the other hand, at very fast rotational velocities and activity levels, correlations are no longer observed, as the star enters the so-called “saturated regime”. To evaluate the status of our targets and also to check for peculiar discrepant cases that might distort the observed quantities (e.g., aliases of the true rotation period), we evaluate here the correlation between activity and rotation. Figure 5 shows the correlation between $\log R_{HK}$ vs. $\log L_X/L_{bol}$ for the stars in our sample. A similar slope is observed for the whole range of emission levels.

Figure 6 shows the Rossby number (used here to take the dependence of the rotation period on color into account, Noyes et al. 1984) vs. $\log R_{HK}$ and $\log L_X/L_{bol}$. The change in slope due to the saturation effects is clearly seen in the $\log L_X/L_{bol}$ plot.

We also compared the measured rotation period with the expected one based on the Ca II H and K and X-ray coronal emission and calibrations by Mamajek & Hillenbrand (2008). In the first case (Fig. 7; upper panel), the correlation between the predicted and observed rotation period is low for stars with fast rotation. This effect was also noted by Mamajek & Hillenbrand (2008), who propose that this may be explained by 1) a larger intrinsic variability compared to stars with slower rotation rates; 2) a sparseness of activity measurements; and 3) a spread in convective turnover times due to a mixing of main sequence and
<figure><img src="image_5.png" /><figcaption>Fig. 5. log R<sub>HK</sub> vs. log L<sub>X</sub>/L<sub>bol</sub> for the stars in our sample.</figcaption></figure>

<figure><img src="image_6.png" /></figure>

<figure><img src="image_7.png" /><figcaption>Fig. 6. log R<sub>HK</sub> and log L<sub>X</sub>/L<sub>bol</sub> (upper and lower panels respectively) vs. Rossby number for the stars in our sample. Filled circles represent stars with *confirmed* or *likely* rotation period. Empty circles represent stars with an *uncertain* rotation period.</figcaption></figure>

pre-main sequence stars. One should also consider that a proper calibration of the *S* index into the standard Mt. Wilson scale is challenging at high activity levels due to the paucity of suitable calibrators and the presence of intrinsic variability of the chromospheric emission. Therefore, mixing results from independent sources (as done here) might result in an increased scatter. Furthermore, for projected rotational velocities larger than about 40 km s<sup>-1</sup>, the emission of the Ca II H and K cores is spread out beyond the ~1 Å window typically used for the measurement of the *S*-Index (Desidera et al. 2006). X-ray derived periods (Fig. 7; lower panel) can be derived only for stars outside the saturated

<figure><img src="image_8.png" /></figure>

<figure><img src="image_9.png" /><figcaption>Fig. 7. Observed rotation period vs. the expected rotation period from the value of log R<sub>HK</sub> (upper panel) and R<sub>X</sub> (lower panel), as derived by using the Mamajek & Hillenbrand (2008) calibrations. Filled circles represent stars with *confirmed* or *likely* rotation period. Empty circles represent stars with *uncertain* rotation period. The outlier in the upper panel is represented by HIP 79958. As the measured rotation period appears to be robust, the discrepancy may be due to poor sampling of H and K variability or due to calibration issues resulting from the low temperature of the star. See Appendix B for further details.</figcaption></figure>

regime (Mamajek & Hillenbrand 2008). The plot shows the ex-
pected correlation for unsaturated stars.

6.4. Ultraviolet flux

Ultraviolet NUV and FUV magnitudes from the GALEX satel-
lite (Martin et al. 2005) were checked to identify or confirm
WD companions (see Zurlo et al. 2013, for the case of HIP 6177)
and to indirectly evaluate the level of magnetic activity when di-
rect measurements were not available. The GALEX magnitudes
were available for 34 objects in our sample. With the exception
of HIP 6177, we did not identify additional objects with peculiar
FUV and NUV fluxes.

**7. Multiplicity, close companions, and discs**

We summarize here the evidence for additional stellar compan-
ions at either wide or close separations. A complete census of
stellar multiplicity is important for several reasons. For instance,
the presence of a close companion can bias the derivation of stel-
lar parameters, as is the case for photometric distance. A wide
companion may also be used to provide additional diagnostics to
constrain the properties of the target. More generally, knowledge
<table><caption>**Table 5.** Close visual binaries discovered or confirmed by NaCo-LP AO observations.</caption><thead><tr><th>Target</th><th>Sep (mas)</th><th>Sep (AU)</th><th>ΔH (mag)</th></tr></thead><tbody><tr><td>TYC 0603-0461-1</td><td>74 ± 14</td><td>4.3</td><td>0.1 ± 0.2</td></tr><tr><td>HIP 6177</td><td>1566 ± 6</td><td>52.6</td><td>7.1 ± 0.2</td></tr><tr><td>HIP 8038</td><td>437 ± 7</td><td>12.8</td><td>2.5 ± 0.2</td></tr><tr><td>TYC 8484-1507-1</td><td>60 ± 14</td><td>3.6</td><td>0.2 ± 0.2</td></tr><tr><td>TYC 9181-0466-1</td><td>1891 ± 7</td><td>146.9</td><td>1.5 ± 0.2</td></tr><tr><td>TYC 8927-3620-1</td><td>87 ± 14</td><td>7.1</td><td>0.5 ± 0.2</td></tr><tr><td>TYC 9231-1566-1</td><td>1975 ± 7</td><td>193.6</td><td>3.0 ± 0.2</td></tr><tr><td>TYC 8989-0583-1</td><td>2584 ± 8</td><td>169.0</td><td>2.6 ± 0.2</td></tr><tr><td>TYC 9010-1272-1</td><td>262 ± 8</td><td>24.0</td><td>1.0 ± 0.2</td></tr><tr><td>TYC 7835-2569-1</td><td>901 ± 7</td><td>63.3</td><td>0.1 ± 0.2</td></tr><tr><td>TYC 6786-0811-1</td><td>120 ± 10</td><td>9.4</td><td>0.3 ± 0.2</td></tr><tr><td>HIP 80290</td><td>3340 ± 2</td><td>278.2</td><td>1.9 ± 0.2</td></tr><tr><td>HIP 94235</td><td>506 ± 7</td><td>31.0</td><td>3.8 ± 0.3</td></tr><tr><td>HD 199058</td><td>471 ± 7</td><td>31.1</td><td>2.5 ± 0.2</td></tr><tr><td>HIP 107684</td><td>326 ± 7</td><td>29.4</td><td>2.8 ± 0.3</td></tr><tr><td>HIP 108422</td><td>170 ± 7</td><td>9.9</td><td>3.0 ± 0.2</td></tr></tbody></table>

**Notes.** We list the name of the star, the projected separation measured with NaCo (from the companion paper Chauvin et al. 2015) in mas and in AU and the magnitude difference in H band.

of target environment is important for the proper interpretation of the astrophysical results of our NaCo imaging program and for comparisons with other surveys. Beside stellar multiplicity, the presence of disks is also relevant in this context. There are four stars with resolved debris disks in our sample: HIP 11360, HD 61005, HIP 76829, and HIP 99273. They are discussed in Appendix B.

## 7.1. Visual binaries

Several new close binaries were discovered as part of the NaCo-LP. The details of their discovery are reported in the companion paper presenting the direct imaging results (Chauvin et al. 2015). We summarize here their properties, as the binarity has to be considered to correct photometric distances and temperatures; binarity is also relevant for a proper interpretation of the age indicators. Three close binaries were previously known: HIP 108422 (Chauvin et al. 2003, physical association confirmed by our NaCo observations), TYC 7835-2569-1 (Brandner et al. 1996), and TYC 6786-0811-1 (Köhler et al. 2000). Three of the newly discovered companions are proposed members of the AB Dor moving group (MG) and one belongs to the ϵ Cha group. These discoveries contribute to the census of stellar multiplicity at young ages in loose associations (Duchêne & Kraus 2013).

Several targets have wide companions (defined here as those with projected separation larger than 6 arcsec) whose presence and association either were already established in the literature or are proposed here. They are listed in Table 6. These wide companions are outside NaCo's field of view, so they did not impact target selection. To estimate the reliability of these wide pairs as true bound systems, we followed the methods of Lépine & Bongiorno (2007) to calculate the separation, projected separation (assuming identical distance as the brighter companion), and proper motion difference for all candidate wide binaries. We used relations in Dupuy & Liu (2012) and Lépine & Bongiorno (2007) to place statistical constraints on the likelihood that binary pairs are real and physically bound. From the fractional proper motion difference of the components, $fr_μ = Δ_μ/avg_μ$,

where $Δ_μ$ is the proper motion difference and $avg_μ$ is the average proper motion of the components, Dupuy & Liu (2012) show that a $fr_μ ≤ 0.2$ indicates that the pair is likely physically bound. We also used the statistic $Δ_χ$ from Lépine & Bongiorno (2007), which uses a power law to describe the relationship between separation, $Δ_μ$, and $avg_μ$. If $Δ_χ < 1.0$, the pair is likely bound. This statistic is calibrated only for stars with 150 mas/yr $< μ < 450$ mas/yr. Thus, it could be less useful for stars with smaller proper motion where the relationship may not follow a power law.

The analysis shows that most of the wide pairs in Table 6 are likely bound. Measured parameters such as age, distance, and moving group membership can therefore be shared between the components. All stars for which $Δ_χ > 1.0$ are stars that have $avg_μ < 150$ mas/yr, implying that this statistic is less useful. For these stars, the $fr_μ$ is probably a better indication of a physically bound nature, although it is not as strong a constraint as $Δ_χ$. Finally, we note that several of the proposed binaries are actually hierarchical multiples, as revealed by imaging of tight visual companions and observed RV variations (see Appendix B).

## 7.2. Spectroscopic and astrometric binaries

We summarize the presence of spectroscopic binarity among our targets in Table 7 by considering both RV variability and the presence of multiple components in the spectra (SB2). Two critical issues prevent firm conclusions in some specific cases. 1) For single-epoch spectra, line-profile analysis of young, active stars often reveals deformation due to star spots crossing the stellar disk. It is difficult to distinguish between such effects and the presence of a companion. 2) The evaluation of the significance of the proposed RV variations depends on the adopted error bars, which are often not available in the literature data. Furthermore, there are cases where significant RV variations of amplitudes up to a few km s⁻¹, can be caused by stellar or circumstellar phenomena, such as variable obscuration from a circumstellar disk (see, e.g., Schisano et al. 2009, for the case of T Cha) or stellar oscillations in the case of early-type stars. A couple of suspected astrometric binaries is also included in Table 7.

# 8. Kinematics and membership to nearby associations

## 8.1. Kinematic parameters and space velocities

Proper motions were taken from Tycho2 (Høg et al. 2000) and van Leeuwen (2007) when available. For HIP 46634/7 and HIP 58240/1, we adopted instead the original HIPPARCOS values Perryman et al. (1997; see Sect. 9.1). For HIP 25434/6, we adopted the long term proper motion from Tycho2 as there are indications that the HIPPARCOS astrometry is biased by the presence of an additional component (see Appendix B). Absolute RVs were derived from our own spectra and extensive literature compilation (see Table 10). A minimum error bar of 0.5 km s⁻¹ was adopted to take the uncertainties in the absolute RV and the uncertainties in the zero-point systematics between different instruments into account. The determination of distances is discussed in Sect. 9.1.

The space positions, space velocities, and their uncertainties were derived using relations from Johnson & Soderblom (1987). In these calculations, we have used the J2000 transformation matrix, which have been taken from the introduction of the HIPPARCOS catalog, to convert to Galactic coordinates.
<table><caption>**Table 7.** Spectroscopic and astrometric binaries in the NaCo-LP sample.</caption><thead><tr><th>Target</th><th>Remarks</th></tr></thead><tbody><tr><td colspan="2" style="text-align:center; font-weight:bold;">confirmed SB</td></tr><tr><td>TYC 5839-0596-1</td><td>SB2</td></tr><tr><td>HIP 3924</td><td>SB2</td></tr><tr><td>HIP 72399</td><td>SB1</td></tr><tr><td>TYC 7835-2569-1</td><td>SB2 + close VIS</td></tr><tr><td>HIP 35564</td><td>SB1</td></tr><tr><td>HIP 36414</td><td>SB1</td></tr><tr><td>TYC 7188-575-1</td><td>SB1</td></tr><tr><td>TYC 5206-0915-1</td><td>SB1</td></tr><tr><td colspan="2" style="text-align:center; font-weight:bold;">suspected SB</td></tr><tr><td>TYC 7796-2110-1</td><td>SB2?</td></tr><tr><td>TYC 9010-1272-1</td><td>SB2? + close VIS</td></tr><tr><td>TYC 8128-1946-1</td><td>RV Var ?</td></tr><tr><td>HIP 71933</td><td>RV var ?; astr. acceleration</td></tr><tr><td>TYC 6815-0874-1</td><td>SB2?</td></tr><tr><td>HIP 13008</td><td>astrom. acceleration</td></tr><tr><td>TYC 9245-0617-1</td><td>RV var</td></tr></tbody></table>

Notes. See notes in Appendix B for further details.

## 8.2. Membership to nearby associations

Table 8 presents the list of moving groups, associations, and solar-neighborhood open clusters considered in our kinematic analysis. Adopted parameters are described for each group. If the uncertainties in the *U*, *V*, and *W* space velocities of the associations were quoted in the literature, we included those in the analysis. If no uncertainties were quoted, we used a conservative uncertainty estimate of ±1 km s⁻¹ for moving groups and ±2 km s⁻¹ for open clusters. We considered the young, nearby population to be represented by stars within the *U*, *V*, and *W* boundaries defined by Zuckerman & Song (2004), which are also shown in Fig. 10. Zuckerman & Song (2004) noted that the majority of solar-neighborhood stars within ~60 pc that are younger than 50 Myr have kinematic parameters within these boundaries. However, it should be considered that old stars in the same kinematic space outnumber true young stars. Therefore, independent indicators of youth are required for a firm inference on stellar age. HIP 71908 is an example of a moderately old star with kinematics similar to those of young stars (see Appendix B). The adopted ages are presented in Sect. 8.3.

We then calculated the significance in the difference (Sig D) among *U*, *V*, and *W* galactic velocities, which are calculated for each NaCo-LP target and each association in the above list. As an example, the Sig D for the *U* velocity is defined as

$$ \text{SigD}_U = \frac{(U_{\text{star}} - U_{\text{group}})}{\sqrt{(dU_{\text{star}})^2 + (dU_{\text{group}})^2}} \quad (1) $$

The SigD value represents how many sigma that separates the space velocity of the target from that of the group being considered. In our analyses of NaCo-LP targets, we considered *U*, *V*, and *W* space velocities to be consistent with membership if it had a SigD ≤ 2.0 in each of the *U*, *V*, and *W* velocities. This is only one indication that a star may belong to a given association, but it serves as a first step in the process to define bona fide membership. We further checked the moving group membership by calculating Bayesian membership probabilities using the online tools BANYAN I and II (Malo et al. 2013; Gagné et al. 2014).

The online versions of these tools use only the available kinematics for this star as input and do not consider the star's age (e.g. CMD position). We used all available kinematic information for each star as input (coordinates, our adopted proper motions, radial velocities, and distances). In several cases, the two versions of BANYAN yielded highly discrepant results. This is likely caused by changes to the prior, the UVWXYX distributions, and the definition of the Galactic field between the first and second iterations of BANYAN (Gagné et al. 2014). A detailed comparison of the differences between the two tools is beyond the scope of this paper. We indicate the targets where discrepancies arise along with further details regarding target ages and group membership in Appendix B.

In most cases, we confirm the membership assignments by Torres et al. (2008) and Malo et al. (2013), and we identify some possible additional members. Discrepancies for individual cases are mostly due to differences in the kinematic data (e.g., RV in the case of HIP 11360). Different membership criteria adopted in the various studies also play a role. A large number of the NaCo-LP targets are found to be kinematically consistent with the young, nearby population.

## 8.3. Absolute ages of nearby moving groups

Our age determination is mostly based on comparison of indirect indicators as measured for individual NACO-LP targets to those of members of groups and clusters, such as β Pic, Tucana, Columbia, Carina, AB Dor, Pleiades, and Hyades. While the age ranking of these groups is mostly defined, the absolute values of their ages is widely debated in the literature. A full assessment of the issue of the absolute ages is beyond the scope of this paper but we present the motivation of our adopted ages for the youngest groups for which members are found within the NACO-LP sample. For some of the groups considered below (β Pic, IC 2391, Pleiades) we anticipate that there is a systematic discrepancy between ages obtained using the lithium depletion boundary of low-mass stars with respect to isochrone fitting with the first method yielding older ages. This trend is common to several other open clusters (e.g., Dobbie et al. 2010).

### 8.3.1. β Pic, ε Cha, and Sco-Cen groups

The most widely adopted age for the β Pic is 12 Myr, based on the isochrone fitting by Zuckerman et al. (2001; $12^{+8}_{-4}$ Myr) and the kinematic traceback analysis by Ortega et al. (2002) and Song et al. (2003). Torres et al. (2008) adopted instead 10 Myr. Very recently, a significantly older age ($21 \pm 4$ Myr) has been derived by Binks & Jeffries (2014) using the lithium depletion boundary of low-mass stars. An age around 20 Myr is only marginally compatible with the isochrone fitting results by Zuckerman et al. (2001).

The kinematic traceback age nominally have a small error bar (about 1 Myr) but is based on the list of members known in 2002–2004. The current enlarged list of members and the improvement in the kinematic parameters, due to the release of the revised HIPPARCOS parallaxes by van Leeuwen (2007), additional RV data, and more complete census of multiplicity, indicate the need of updating the analysis. The study by Mamajek et al. (in prep., preliminary results presented in Soderblom et al. 2013) claims that the group was not smaller in the past, ruling out a 12 Myr age at >3 sigma.

An older age for β Pic would allow us to reconcile the result by Song et al. (2012) that stars in LCC and UCL are slightly
younger than those of β Pic MG (from the comparison of lithium EW as a function of color) to the absolute ages of UCL and LCC of 16 and 17 Myr respectively, which are derived using an isochrone fitting, which includes the recent work by Pecaut et al. (2012).

Performing an isochrone fitting to β Pic MG members with a trigonometric parallax, adopting the photometric temperatures as in Sect. 4.3, and using Bressan et al. (2012) models as described in Sect. 9.3 yields an age of $16 \pm 2$ Myr (internal error only) midway between the original 12 Myr estimate and the recent estimate based on lithium depletion boundary. To check the reliability of our result, we considered the F-type stars in the Sco-Cen region that were recently studied by Song et al. (2012) and we got very similar results, with our ages being older by about 1 Myr.

Considering the uncertainties related to the various techniques, we adopt $16 \pm 6$ Myr as our age for the β Pic MG. This estimate has the additional advantage of being homogeneous with the age determination from isochrone fitting performed for our program stars in Sect. 9.3. For the Sco-Cen subgroups, the ages by Pecaut et al. (2012) were adopted with lower limits at the ages proposed by Song et al. (2012) for UCL and LCC and by Preibisch et al. (2002) and Preibisch & Mamajek (2008) for US.

In our sample, there are also two members of the $\epsilon$ Cha group. Torres et al. (2008) adopt an age of 6 Myr. As we adopt older ages for young groups, such as β Pic MG and Upper Scorpius, an upward revision of the age of this group is also possible. The analysis by da Silva et al. (2009) based on lithium shows that $\epsilon$ Cha is younger than TW Hya, which is younger than β Pic MG. Therefore, we adopt 10 Myr as the age for the $\epsilon$ Cha group, allowing for the younger age proposed by Torres et al. (2008) as lower limit.

### 8.3.2. Tucana, Columba, Carina, and Argus

The most widely adopted age for Tucana, Columba, and Carina is 30 Myr (Zuckerman & Song 2004; Torres et al. 2008). Argus and IC 2391 open cluster are considered to be slightly older (35–40 Myr). The absolute age of the IC 2391 open cluster was estimated to be 40 Myr by using a isochrone fitting (Platais et al. 2007) and 50 Myr using the lithium depletion boundary (Barrado y Navascués et al. 2004). The very recent determination of the lithium depletion boundary for Tucana from Kraus et al. (2014) yields an age of about 40 Myr. Our isochrone fitting yields an age of 35 Myr for the members of these latter groups, which are compatible with the previously adopted age.

Considering that Tucana, Columba, and Carina appear to be younger than Argus based on Li EW vs. effective temperature graph and Li depletion boundary (da Silva et al. 2009; Kraus et al. 2014) and the absolute age determination of IC 2391 appears sound within 10 Myr, there are only limited margins for any upward revision of age of these groups with respect to the values adopted in Torres et al. (2008). Additional evidence for a young age of the Columba association comes from the interferometric measurements of the proposed member HR 8799 (Zuckerman et al. 2011), where the radius of the star is consistent with an age ~30 Myr (Baines et al. 2012)<fnref n="9" />. Dynamical stability studies of the planetary system that orbits HR 8799 provide additional indirect evidence for a young system age. An older stellar age implied larger planet masses that would lead to a dynamically unstable system (Currie et al. 2011; Sudol & Haghighipour 2012; Esposito et al. 2013).

Therefore, we adopt a value of 30 Myr for Tucana, Columba, and Carina and 45 Myr for Argus (the mean between isochrone and lithium depletion boundary ages).

### 8.3.3. AB Dor moving group

The age of AB Dor MG is highly debated in the literature, ranging from 50 Myr in the first paper that presented the association (Zuckerman et al. 2004) to about 150 Myr. Janson et al. (2007) found an age of 50–100 Myr for the AB Dor quadruple system, while Guirado et al. (2011) favor an age of 40–50 Myr from the size of AB Dor A derived through interferometric measurements. Luhman et al. (2005) suggest a link to the Pleiades open cluster with a common origin and a similar age. Torres et al. (2008) and da Silva et al. (2009) adopt 70 Myr, which is equal to their adopted age for the Pleiades. Barenfeld et al. (2013) cast doubt of the existence of the group as a whole, finding that only half of the proposed members might share a common origin and setting an age lower limit at 110 Myr from the position of K dwarfs on color-magnitude diagram. Messina et al. (2010) noted the similar distribution of rotation periods among AB Dor and Pleiades members, while that of the $\alpha$ Per open cluster is clearly different, indicating its younger age. On the other hand, the comparison of Li EW of AB Dor and Pleiades members show that the median values for AB Dor are above those of Pleiades for B–V between 0.7 to 0.9 (Fig. 10), suggesting a slightly younger age for AB Dor. X-ray luminosity is also slightly larger for AB Dor members on average. Adopting 125 Myr as an absolute age for the Pleiades (Stauffer et al. 1998), we assume 100 Myr as the age for AB Dor MG in the following, with the caveat that stars with slightly different ages but sharing kinematics may be mixed in the adopted target list.

## 9. Fundamental parameters

### 9.1. Photometric and trigonometric distances

Our adopted distances are based on trigonometric parallaxes from van Leeuwen (2007) when available. For multiple systems where separate parallaxes were available, their weighted average was adopted. For HIP 25434/6, HIP 46634/7 and HIP 58240/1, the weighted averages of parallaxes from the original HIPPARCOS catalog were adopted, as they lead to more consistent positions in the color-magnitude diagrams. However, formal parallax errors for these pairs may be underestimated. For TYC 8484-1507-1, TYC 8128-1946-1, and TYC 9339-2158-1, we used the trigonometric parallaxes of their bound wide companions in our analysis, though these companions were not a part of our target sample. For TWA 21, the parallax is from Weinberger et al. (2013).

For stars without trigonometric parallax, photometric distances were obtained using BVIJHK photometry (Table 9). Reference sequences at various ages were built using members of moving groups with available trigonometric parallaxes. Target distance was then derived based on the multiband photometry, adopted age, and the reference calibration. Typical scatter in these standard relations implies errors of about 15–20% in the photometric distances (Fig. 8). The presence of known companions was taken into account by including correction to the unresolved photometry when applicable. Interstellar reddening was checked by comparing photometric temperature, spectroscopic temperatures when available, and spectral types from the literature. In a few cases of stars with a distance close or slightly above 100 pc, the presence of small amounts of reddening

<footnote n="9">⁹ See Hinz et al. (2010) for a different view on Columns membership.</footnote>
<figure><img src="image_10.png" /><figcaption>**Fig. 8.** Comparison of trigonometric and photometric distances for the stars in the sample with available trigonometric parallax. The rms scatter in the difference is 17%.</figcaption></figure>

$(E(B - V) \le 0.1 \text{ mag})$ was suggested. Photometric distances have larger errors for very young stars (age 5–20 Myr). In these instances, the absolute magnitude and derived distances depend sensitively on the adopted ages; the derived values would be systematically underestimated for unidentifed cases of evolved RS CVn variables.

## 9.2. Metallicity

Metallicity has been found to have a strong correlation with planet frequency at least for RV detections of giant planets around solar type stars (Fischer & Valenti 2005). Whether the planet metallicity connection extends from the separations accessible with RV surveys to those considered in direct imaging surveys is highly uncertain and depends on the main formation and migration mechanisms.

The determination of the metallicity of young stars, such as those in our sample, is made difficult by the high level of magnetic activity, the fast rotational velocities, and the possibility of veiling in the spectra. These phenomena cause larger errors in the abundance analysis with respect to older stars of similar spectral types. Differences in the atmospheric structure of young, active stars with respect to old, inactive main sequence stars might introduce spurious effects (see, e.g., Padgett 1996).

In spite of these challenges, a number of studies have addressed the issue of the metallicity of close young stars with a rather general agreement on a typical solar or slightly subsolar metallicity and the lack of metal-rich very young stars (see, e.g., James et al. 2006; Santos et al. 2008; Biazzo et al. 2011).

The study of the chemical composition of several stars in young associations resulted in no significant scatter between the individual members (Viana Almeida et al. 2009; D’Orazi et al. 2009; De Silva et al. 2013). Therefore, mean values (derived from stars both inside and external to our sample) were adopted for all association members.

To have the largest number of associations analyzed in an homogeneous way, we adopted the metallicities by Viana Almeida et al. (2009) for β Pic, Tuc, Col, Car, AB Dor, and ε Cha MGs<fnref n="10" />. Metallicity of the Carina-Near MG is from Biazzo et al. (2012). Metallicity of the Her-Lyr MG is from Fuhrmann (2004).

A few other stars have spectroscopic metallicity determinations in the literature. Photometric metallicities based on Strömgren photometry were not considered, except for the few cases of moderately old stars, as the strong magnetic activity is known to bias toward lower values the metallicity derived from this method (Morale et al. 1996).

## 9.3. Isochrone fitting, stellar masses, and radii

Stellar masses and isochrone ages were derived through interpolation of stellar models by Bressan et al. (2012), which include pre- and post-main sequence evolutionary phases in a homogeneous way. We used the tool *param* (da Silva et al. 2006)<fnref n="11" />, adapted to use the Bressan et al. (2012) stellar evolutionary models. *Param* performs a Bayesian determination of the most likely stellar intrinsic properties, weighting all the isochrone sections compatible with the measured parameters (metallicity, effective temperature, parallax, apparent magnitude) and their errors. It adopts a flat distribution of ages within a given interval, as a prior. We found that Bressan et al. (2012) models are very similar to those of Tognelli et al. (2011) and Dotter et al. (2008) at least for effective temperatures warmer than 4500–4000 K. Differences at $T_{\text{eff}} < 4000$ K are not of concern for the analysis of the stars in our sample.

In most cases, isochrone fitting yields very poor constraints on stellar ages (e.g., errors of a few Gyrs), which is expected for stars close to the main sequence (Fig. 9). Tighter constraints are derived from indirect indicators, such as lithium and rotation-activity phenomena (see Sect. 9.4). The stellar masses and ages resulting from isochrone fitting within the whole range of input stellar parameters are correlated, with older ages yielding lower stellar masses. To infer the stellar masses corresponding to the plausible ages of our targets, we run the *param* interface a second time for these targets, by adopting the minimum and maximum ages from Table 10 and keeping fixed the other input parameters. Differences in stellar masses with respect to the unconstrained run are typically of about 0.02–0.04 $M_{\odot}$, with larger masses that occur when adopting the age limits from the indirect indicators. The *param* tool also provides the stellar radii, which were coupled with the measured $v \sin i$ to estimate the reliability of detected rotation periods (see Appendix B for discussion on individual objects). The isochrone ages of the few targets for which this method contributes significantly in the determination of stellar ages are listed in Table 10.

## 9.4. Stellar ages

Our approach to age determination is to consider all the indicators available to us to better understand the properties of each object and derive stellar age. The lesson we got from the case of HIP 6177 (Zurlo et al. 2013) is that significant discrepancies

<footnote n="10">¹⁰ Viana Almeida et al. (2009) noted a trend of metallicity with effective temperatures, possibly due to the effects of stellar activity. Removing it by assuming that no correction is needed for a solar type star would increase the metallicities by about 0.1 dex. Since the origin of this trend is uncertain and the assumption of its null value for solar temperature is questionable, we do not apply such shifts.</footnote>

<footnote n="11">¹¹ http://stev.oapd.inaf.it</footnote>
<figure><img src="image_11.png" /><figcaption>**Fig. 9.** HR diagram (upper panel: effective temperature vs. *M*<sub>V</sub>; lower panel: effective temperature vs. *M*<sub>K</sub>) for stars in the NaCo-LP sample. Stars with different ages are plotted with different colors. Overplotted are pre-main sequence, solar-metallicity isochrones for 5, 12, 30, 70, and 200 Myr (from Bressan et al. 2012). The two B-type stars HIP 10602 and HIP 12394 and the Li-rich giant HD 99409 are outside plot limits.</figcaption></figure>

between age indicators may hide an astrophysical situation that
is different from a normal young star (the expected typical target
in our survey) and, therefore, requires an in-depth investigation.

In the previous sections, we provided several parameters
(lithium EW, Ca II H and K emission, X-ray emission, rotation
period), which are known to depend on stellar age. The stellar
age from lithium was estimated for each target from a compari-
son of measured lithium EW with that of the confirmed members
of young moving groups and clusters of similar color (Fig. 10).

For Ca II H and K emission, X-ray emission, and rotation pe-
riod, we adopted the age calibration by Mamajek & Hillenbrand
(2008)<fnref n="12" />. Our target stars have colors extending outside some of
the validity limits of these calibrations (B − V between 0.5 to
0.9 for log R<sub>HK</sub> and X-ray emission). As shown in Fig. 10, the
results from known group members support the use of these re-
lations for most of our target stars, even when they are slightly
outside the formal boundaries, leaning toward the red side (from
B−V = 0.9 up to B−V = 1.2–1.3). On the blue side, the situation
is different, as both log R<sub>HK</sub> and R<sub>X</sub> become smaller when tem-
perature increases at fixed age, due the vanishing of the stellar
magnetic activity when the external convective zone of the star
becomes too thin. Therefore, the extrapolation of the Mamajek
& Hillenbrand (2008) calibrations would provide a significant
overestimation of the stellar age<fnref n="13" />. The results of the age cali-
bration are included in Table 12 as upper limits.

The measurement of stellar age from the rotation period (gyrochronology) is becoming increasingly popular, as it is not vulnerable to the time variability that characterizes the choro-mospheric and coronal emissions. However, it should be noted that a group of coeval young stars usually distributes along two sequences: that of very fast rotators (“C” sequence following the nomenclature by Barnes 2007) and that of slower rotators with the rotation period increasing with color (“I” sequence; Fig. 10). The gyrochronology calibration applies only to stars on the “I” sequence; for stars on the “C”, its use is not appropriate and only supports a young age for the star.

Age from isochrone fitting has been derived in Sect. 9.3. As discussed above, isochrone fitting does not add tighter constraints on stellar age in most cases when compared to other methods, since the star position on the CMD is very close to the main sequence. For stars that are off of the main sequence, the use of other age indicators (e.g., lithium) allows us to conclusively discriminate between the case of young pre-main sequence stars and evolved post-main sequence stars and to assign corresponding ages. Position on the CMD is also affected by the presence of companions. Having sensitivity with NaCo imaging down to a few-AU separation for stellar companions and having checked for the presence of blended components in high resolution spectra for most of our target stars, we think that we have identified most cases of binary companions contributing significantly to the integrated flux of the system. However, the possibility of a few remaining cases cannot be excluded.

Finally, as discussed in Sect. 8.2, kinematic parameters alone
cannot be considered as conclusive proof of a given stellar age
value, as numerous old stars occupy the same kinematic space of
young stars. Final assignment of membership to groups is based
on both the kinematic analysis and the consistency of the age
indicators with the age of the group. Ambiguous cases arise for
stars where the other age indicators yield poor constraints, such
as early F stars. The existence of space velocities firmly outside
the kinematic space on which confirmed young stars are found
(see for example the Montes et al. 2001 boundaries, also shown
in Fig. 10) is considered a strong indication for an age older than
about 500 Myr.

<footnote n="12">¹² There are some differences between our adopted ages for groups and clusters and those on which the Mamajek & Hillenbrand (2008) calibration is based, but they are mostly confined to the youngest groups (β Pic and Upper Scorpius), which is an age range where our age estimate is primarily based on other indicators.</footnote>

<footnote n="13">¹³ Actually, a result from Fig. 10 show that R<sub>X</sub> is smaller for stars with B − V ~ 0.5 with respect to coeval stars with redder colors, indicating that the color dependence starts to become already important in the range of the Mamajek & Hillenbrand (2008) calibration.</footnote>
<figure><img src="image_12.png" /><figcaption>**Fig. 10.** Age indicators for the stars in the sample. From top-left: $R_X = \log L_X/L_{bol}$ vs. $B-V$; $\log R_{HK}$ vs. $B-V$; rotation period vs. $B-V$; lithium equivalent width vs. $B-V$; $U$ vs. $V$ space velocities; and $U$ vs. $W$ space velocities. In all the panels, the black stars represent the targets. In the $R_X$, $\log R_{HK}$, rotation period, and lithium plots, orange circles represent $\beta$ Pic MG; red circles: Tucana-Columba-Carina MG; light blue circles: AB Dor MG; green circles: Pleiades OC; purple circles: Hyades OC. In the $R_X$ vs. $B-V$ and $EW$ Li vs. $B-V$ panels, the filled squares represent the median value of $R_X$ and $EW$ Li for the corresponding color bin. In the $\log R_{HK}$ plot, green and purple lines represent the locus populated by Pleiades and Hyades stars, respectively. In the latter two panels, the positions of some young moving groups are marked as open circles. The dashed-line box in both panels is the locus of the Nearby Young Population as defined in Zuckerman & Song (2004). The dotted contours in the $U$ vs. $V$ plot show the locus of kinematically young stars proposed by Montes et al. (2001).</figcaption></figure>
<figure><img src="image_13.png" /><figcaption>**Fig. 11.** Distribution of stellar age, distance, mass, and metallicity for the stars in the NaCo-LP sample.</figcaption></figure>

The spread in rotation rates for coeval young stars (see, e.g., *Messina et al. 2010*), and the saturation of X-ray emission at fast rotation periods (*Pizzolato et al. 2003*) make the dependence of these indicators shallow for young ages (ages smaller than the Pleiades), as discussed in *Soderblom et al. (2013)*, for example. As an example, β Pic, Tucana, Columba, and Carina and AB Dor members overlap on the log L<sub>X</sub>/L<sub>bol</sub> vs. B-V diagram in Fig. 10. Therefore, the exact numerical values resulting from age calibrations cannot be taken at face value, but the consistency of activity and rotation is a strong indication of youth unless fast rotation is due to alternative causes (see below). For such candidate young stars, lithium EW, kinematics, and isochrone fitting in a few cases are more robust indicators of the stellar age.

Special care is required for close spectroscopic binaries.
Tidal locking represents a viable alternative to young age for
explaining the fast rotational velocity and high levels of chro-
mospheric and coronal activity<fnref n="14" />. In these cases, indicators such

as rotation period, and coronal emission, and chromospheric
emission are not considered for age determination, and we rely
only on indicators that are not directly linked to rotation, such
as lithium, kinematics, and isochrone fitting. For the spectro-
scopic binaries in our sample, the orbital period is typically
not available, as the binarity was identified with just a hand-
ful of RV measurements, or even one single spectrum in the
case of SB2. Therefore, we cannot conclusively infer the tidal
locking nature of active binary stars like TYC 7188-575-1 and
TYC 5206-0915-1. Furthermore, the lack of an RV orbital solu-
tion prevents the determination of a system RV, adding uncer-
tainties on the space velocities and effectively making them use-
less in some cases. Lithium EW is available in most cases, and
age estimates for candidate tidally-locked binaries are primar-
ily based on this diagnostic. However, it is possible that lithium
abundance is also affected in close binaries, as it is often ob-
served in RS CVn systems (Pallavicini et al. 1992).

By applying these techniques, we derived ages for our tar-
get stars. The ages from individual indicators and the final
adopted values are given in Table 10. Most of them are con-
firmed to be young. Besides the tidally-locked systems and
the star rejuvenated by the progenitor of its WD companion

<footnote n="14">¹⁴ It should be noted that the two explanations are not mutually exclud-
sive. There are cases of close tidally locked binaries that are found to
be young based on lithium EW, membership to groups, or presence of
disks (e.g., V4046 Sgr).</footnote>
<figure><img src="image_14.png" /><figcaption>Fig. 12. Age vs. distance for the stars in the NaCo-LP sample.</figcaption></figure>

(HIP 6177, Zurlo et al. 2013), other cases of old stars spually included in our sample are represented by the Li-rich giant HD 99409, by stars for which our determinations of age indicators are in contrast with the literature value (HIP 13008; HIP 114046), and by old interlopers in the kine-matic space of young stars (HIP 71908, formerly classified as an Her-Lyr member).

Most of our target stars have not been previously observed in deep imaging, and in several cases, their ages have not been studied in detail. However, some of them were included indepen-dently in NICI imaging surveys (Wahhaj et al. 2013; Biller et al. 2013). For the seven stars in common, we obtained identical ages for one member of AB Dor MG (HIP 14684) and one of Her-Lyr (HD 139664). The objects HIP 99273 and TYC 8728-2262-1 were assigned to the β Pic MG in both cases, but there is a slight difference in the adopted group age. For HIP 11360, the star is classified as a β Pic member in NICI papers, while we adopt membership in the Tucana association, based on our revised sys-tem RV. For HD 61005, we adopt membership in Argus (40 Myr) while Wahhaj et al. (2013) adopt an age of 100 Myr without as-signing membership to any known group. Finally, HIP 71908 is included in the Her-Lyr membership in Biller et al. (2013), while we claim it is a significantly older star with similar kinematics. While we are convinced of our adopted choices, this comparison is a further indication of the challenges represented by the age determination of young stars.

## 10. Discussion and conclusions

We have performed a characterization of the targets of the NaCo-LP to probe the occurrence of exoplanets and brown dwarfs in wide orbits. With this aim, we acquired spectroscopic data us-ing FEROS, HARPS, and CORALIE and retrieved additional spectroscopic data from public archives. From these spectra, we determined radial and projected rotational velocities, lithium equivalent widths, effective temperatures, and chromospheric emission of the targets. We also analyzed photometric time se-ries available from ASAS and Super-WASP archives to derive rotational periods and investigate the stellar variability phenom-ena. These data were used to investigate basic properties of the targets of our deep-imaging planet search program. These ba-sic properties included ages, distances, masses, and multiplicity. Such information is needed for a proper interpretation of the di-rect imaging results, which are presented in the companion paper by Chauvin et al. (2015).

Histograms showing the distribution of age, distance, mass, and metallicity are in Fig. 11. The irregular behavior of the age distribution is due to members of MGs, which cluster at the same age in the histogram. The median age of the targets is 100 Myr. Few targets have estimated ages below 20 Myr and even fewer have ages older than 500 Myr, which represent old interlopers for which our original selection criteria failed to remove. The presence of older interlopers is due to a variety of causes related to age estimation, as discussed in Sect. 9.4. The median distance of the stars in our sample is 63.7 pc. Considering that the region closest to the star is saturated or hidden by the coronagraph in our imaging observations (Chauvin et al. 2015), our survey is then typically sensitive to projected separations down to about 20 AU. Stellar age and distance from the Sun are correlated, as shown in Fig. 12. This correlation is the result of the low space density of very young stars in the solar neighborhood and of several nearby young stars being previously observed in other direct imaging surveys.

The average metallicity of stars in the NaCo-LP sample is close to solar (median value [Fe/H] = -0.03) with a dispersion that is significantly smaller than that of old nearby stars studied in RV surveys, which include both moderately metal-poor stars and metal-rich stars (Fischer & Valenti 2005; Sousa et al. 2008). Furthermore, the stars with the lowest and highest metallicity in our sample are typically among the oldest ones, thus carrying limited weight in terms of detection limits of planetary compan-ions. Therefore, the exploration of any correlation between the frequency of giant planets in wide orbits and metallicity appears to be challenging for the direct imaging technique.

The median stellar mass is 1.01 $M_\odot$ with 94% of the stars having masses between 0.70 and 1.50 $M_\odot$. Therefore, our sam-ple is tuned to the study of the occurrence of planets in wide orbit around solar-type stars and complements the results of RV surveys, which are mostly focused in the same range of stellar masses. Young, low mass stars are virtually excluded by our adopted magnitude limits, while few early type stars with confirmed young ages were known at the time of our sample selection. However, dedicated imaging surveys devoted to the search for planets around early-type stars were performed in re-cent years (Janson et al. 2011; Vigan et al. 2012), while other authors focused their attention on low-mass stars (Delorme et al. 2012). Appropriate merging of these samples and of those of other surveys, which are mostly focused on solar-type stars (e.g., Lafrenière et al. 2007), will allow a preliminary evaluation of the frequency of planets in wide orbits. We will address this issue in the forthcoming paper by Vigan et al. (2014). The soon-to-come new generation instruments, such as SPHERE and GPI, will al-low an extension of these results to lower planetary masses and closer separations to the star and thus provide, when coupled with RV results, a complete view of the occurrence of giant plan-ets over a wide range of separations.

**Acknowledgements.** Based on observations collected at La Silla and Paranal Observatory, ESO (Chile): Programs 70.D-0081A, 072.D-0021, 072.C-0393, 074.D-0016, 074.A-9002, 074.A-9020, 076.C-0578, 076.A-9013, 077.C-0138, 077.D-0525, 081.A-9005, 082.A-9007, 083.A-9003, 083.A-9011, 083.A-9013, 084.A-9004, 084.A-9011 (FEROS), 072.C-0488, 074.C-0037, 075.C-0689, 076.C-0010, 077.C-0012, 077.D-0085, 077.C-0295, 079.C-0046, 079.C-0170, 080.D-0151, 080.C-0712, 080.C-0664, 081.D-0008, 081.C-0779, 082.C-0390, 184.C-0815 (HARPS), 184.C-0157 (NaCo). Based on data obtained from the ESO Science Archive Facility. This research has made use of the SIMBAD database and Vizier services, operated at CDS, Strasbourg, France and of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. We have used data from the WASP public archive in this research. The WASP con-sortium comprises of the University of Cambridge, Keele University, University of Leicester, The Open University, The Queen's University Belfast, St. Andrews University and the Isaac Newton Group. Funding for WASP comes from the
consortium universities and from the UK's Science and Technology Facilities Council. We thank the SACY team for providing reduced spectra of NaCo-LP targets from their archive. We thank the SOPHIE Consortium for providing unpublished activity measurements. We thank L. Pastori for providing the CES spectra of HD 16699 A and B. We thank B. Mason for providing astrometric data for individual objects collected in the Washington Double Star Catalog. We acknowledge partial support from PRIN-INAF 2010 "Planetary systems at young ages and the interactions with their active host stars". JC was supported by the US National Science Foundation under Award No. 1009203.

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<table><caption>Table 1. Measured parameters of NACO-LP targets on FEROS spectra.</caption><thead><tr><th>Name</th><th>HJD<br>-2 450 000</th><th>HRV<br>km s<sup>-1</sup></th><th>v sin i<br>km s<sup>-1</sup></th><th>T<sub>eff</sub><br>K</th><th>EW (Li)<br>mÅ</th><th>S-index</th><th>log R<sub>HK</sub></th><th>Remarks</th></tr></thead><tbody><tr><td>TYC 5839 0596 1a</td><td>5106.75256</td><td>+51.5 ± 1.5</td><td>18.0 ± 2.0</td><td></td><td></td><td>2.135</td><td>-3.990</td><td>deblended</td></tr><tr><td>TYC 5839 0596 1b</td><td>5106.75256</td><td>+21.3 ± 1.5</td><td>17.0 ± 2.0</td><td></td><td></td><td></td><td></td><td>deblended</td></tr><tr><td>HD 4944</td><td>5056.95069</td><td>+1.5 ± 0.5<br>~19</td><td>8.0 ± 2.0</td><td>5609 ± 105</td><td>37</td><td>0.257</td><td>-4.572</td><td>A<br>B</td></tr><tr><td>HD 15115</td><td>5399.87305</td><td>+2.9 ± 4.1</td><td></td><td></td><td>99</td><td>0.199</td><td>-4.748</td><td></td></tr><tr><td>HD 15115</td><td>5399.87922</td><td>+1.9 ± 2.8</td><td></td><td></td><td>90</td><td>0.194</td><td>-4.769</td><td></td></tr><tr><td>HD 16699</td><td>5106.82452</td><td>+15.5 ± 0.5</td><td>22.0 ± 2.0</td><td>5979 ± 85</td><td>46</td><td>0.305</td><td>-4.443</td><td></td></tr><tr><td>HIP 13008</td><td>5198.57549</td><td>+1.5 ± 1.0</td><td>fast-rot</td><td></td><td></td><td>0.228</td><td>-4.642</td><td></td></tr><tr><td>HD 19668</td><td>3331.69115</td><td>+14.1 ± 0.5</td><td>5.5 ± 0.6</td><td>5463 ± 20</td><td>175</td><td>0.502</td><td>-4.370</td><td></td></tr><tr><td>HD 19668</td><td>3981.86578</td><td>+14.0 ± 0.4</td><td>5.6 ± 0.8</td><td>5478 ± 38</td><td>180</td><td>0.489</td><td>-4.383</td><td></td></tr><tr><td>TYC 8060 1673 1</td><td>5100.82602</td><td>+14.1 ± 0.4</td><td>9.7 ± 1.2</td><td>4882 ± 28</td><td>223</td><td>1.790</td><td>-4.212</td><td></td></tr><tr><td>TYC 8060 1673 1</td><td>5100.83814</td><td>+14.1 ± 0.4</td><td>9.7 ± 1.2</td><td>4869 ± 27</td><td>225</td><td>1.829</td><td>-4.203</td><td></td></tr><tr><td>HIP 19775</td><td>5109.79537</td><td>+20.4 ± 0.5</td><td>13.1 ± 0.8</td><td>5840 ± 45</td><td>170</td><td>0.433</td><td>-4.261</td><td></td></tr><tr><td>HIP 23316</td><td>5204.73415</td><td>22.5 ± 0.1</td><td>7.7 ± 2.1</td><td>5552 ± 33</td><td>225</td><td>0.659</td><td>-4.108</td><td></td></tr><tr><td>HD 32981</td><td>4787.64545</td><td>+25.5 ± 0.0</td><td>4.8 ± 0.6</td><td>5975 ± 30</td><td>127</td><td>0.366</td><td>-4.357</td><td></td></tr><tr><td>BD-09 1108</td><td>4787.66125</td><td>+20.5 ± 0.8</td><td>15.7 ± 1.1</td><td>5660 ± 45</td><td>205</td><td>0.595</td><td>-4.151</td><td></td></tr><tr><td>HIP 25434</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Desidera et al. (2006)</td></tr><tr><td>HIP 25436</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Desidera et al. (2006)</td></tr><tr><td>HD 269620</td><td>5203.69027</td><td>18.6 ± 0.5</td><td>20.2 ± 2.6</td><td>5811 ± 105</td><td>212</td><td>0.482</td><td>-4.232</td><td></td></tr><tr><td>TYC 5346 0132 1</td><td>5198.74360</td><td>+24.0 ± 1.5</td><td></td><td>5324 ± 87</td><td>280</td><td>0.937</td><td>-3.992</td><td></td></tr><tr><td>HD 44748</td><td>5203.72205</td><td>+24.5 ± 0.4</td><td>9.2 ± 0.8</td><td>5657 ± 37</td><td>186</td><td>0.445</td><td>-4.296</td><td></td></tr><tr><td>TYC 9181 0466 1</td><td>3807.58722</td><td>+15.6 ± 0.7</td><td>11.9 ± 1.2</td><td>5682 ± 45</td><td>214</td><td>0.538</td><td>-4.181</td><td></td></tr><tr><td>TYC 9181 0466 1</td><td>3815.59140</td><td>+16.1 ± 0.6</td><td>11.6 ± 0.9</td><td>5670 ± 40</td><td>205</td><td>0.535</td><td>-4.184</td><td></td></tr><tr><td>HD 49855</td><td>4167.58778</td><td>+20.1 ± 0.4</td><td>11.6 ± 1.1</td><td>5444 ± 36</td><td>237</td><td>0.621</td><td>-4.154</td><td></td></tr><tr><td>HIP 35564</td><td>5109.83766</td><td>+24.0 ± 2.0</td><td>fastrot</td><td></td><td></td><td>0.218</td><td>-4.667</td><td></td></tr><tr><td>HIP 36312</td><td>4908.52828</td><td>+17.1 ± 2.3</td><td></td><td></td><td>130</td><td>0.276</td><td>-4.515</td><td></td></tr><tr><td>HIP 36414</td><td>4782.87637</td><td>+24.7 ± 1.3</td><td>31.5 ± 3.3</td><td>5753 ± 110</td><td>72</td><td>0.288</td><td>-4.490</td><td></td></tr><tr><td>HIP 37563</td><td>3809.65732</td><td>+17.1 ± 0.4</td><td>14.3 ± 1.0</td><td>5801 ± 56</td><td>130</td><td>0.356</td><td>-4.405</td><td></td></tr><tr><td>HD 63581</td><td>3338.82012</td><td>+18.1 ± 0.1</td><td>5.1 ± 0.8</td><td>5428 ± 22</td><td>116</td><td>0.505</td><td>-4.338</td><td></td></tr><tr><td>HD 63608</td><td>3777.62320</td><td>+16.9 ± 0.3</td><td>3.0 ± 1.0</td><td>5375 ± 20</td><td>64</td><td>0.465</td><td>-4.384</td><td></td></tr><tr><td>HIP 47646</td><td>4783.86693</td><td>+51.0 ± 1.0</td><td>15.0 ± 1.5</td><td>6615 ± 115</td><td></td><td>0.179</td><td>-4.830</td><td></td></tr><tr><td>TWA 21</td><td>3807.65310</td><td>+18.0 ± 0.1</td><td>8.7 ± 1.3</td><td>4898 ± 21</td><td>364</td><td>1.777</td><td>-4.039</td><td></td></tr><tr><td>TYC 7188 0575 1</td><td>5254.70678</td><td>+44.7 ± 2.0</td><td></td><td></td><td></td><td>3.786</td><td>-3.885</td><td></td></tr><tr><td>HD 296790</td><td>4944.71070</td><td>+8.8 ± 0.8</td><td>31.5 ± 6.5</td><td>5400 ± 50</td><td>190</td><td>0.845</td><td>-4.129</td><td></td></tr><tr><td>TYC 7743-1091-1</td><td>3926.5215</td><td>+21.9 ± 0.1</td><td></td><td>4931 ± 59</td><td>113.4</td><td></td><td></td><td></td></tr><tr><td>HIP 58240</td><td>5254.76079</td><td>+5.9 ± 0.1</td><td>4.0 ± 0.5</td><td>5835 ± 24</td><td>115</td><td>0.365</td><td>-4.415</td><td></td></tr><tr><td>HIP 58241</td><td>5254.75374</td><td>+6.9 ± 0.5</td><td>8.2 ± 0.8</td><td>5710 ± 22</td><td>114</td><td>0.394</td><td>-4.350</td><td></td></tr><tr><td>HD 104467</td><td>3069.79015</td><td>+11.4 ± 0.7</td><td>26.8 ± 2.1</td><td>5730 ± 100</td><td>230</td><td>0.498</td><td>-4.244</td><td></td></tr><tr><td>TYC 9231 1566 1</td><td>5254.83929</td><td>+13.5 ± 0.1</td><td>12.5 ± 0.8</td><td>5530 ± 40</td><td>270</td><td>0.645</td><td>-4.118</td><td>E(B-V) = 0.08</td></tr><tr><td>TYC 8979 1683 1</td><td>4942.79040</td><td>+12.1 ± 2.6</td><td></td><td>5650 ± 145</td><td>290</td><td>0.868</td><td>-4.059</td><td></td></tr><tr><td>TYC 9245 0617 1</td><td>3420.79277</td><td>+13.2 ± 2.4</td><td>28.2 ± 6.2</td><td>5083 ± 70</td><td>391</td><td>1.597</td><td>-3.873</td><td>E(B-V) = 0.09</td></tr><tr><td>TYC 9245 0617 1</td><td>3421.77760</td><td>+14.1 ± 0.5</td><td>26.7 ± 2.2</td><td>5090 ± 70</td><td>410</td><td>1.595</td><td>-3.874</td><td></td></tr><tr><td>TYC 9245 0617 1</td><td>3421.88252</td><td>+14.7 ± 0.7</td><td>28.8 ± 2.0</td><td>5114 ± 62</td><td>415</td><td></td><td></td><td></td></tr><tr><td>TYC 9245 0617 1</td><td>3422.76198</td><td>+12.2 ± 0.6</td><td>26.2 ± 3.1</td><td>5059 ± 65</td><td>410</td><td>1.592</td><td>-3.874</td><td></td></tr><tr><td>TYC 9245 0617 1</td><td>4582.77483</td><td>+9.6 ± 0.9</td><td>26.0 ± 1.7</td><td>5071 ± 65</td><td>393</td><td>1.441</td><td>-3.919</td><td></td></tr><tr><td>HD 113553</td><td>3447.88101</td><td>+1.3 ± 0.1</td><td>10.6 ± 0.9</td><td>5760 ± 32</td><td>145</td><td>0.416</td><td>-4.347</td><td></td></tr><tr><td>HD 113553</td><td>3447.86976</td><td>+1.3 ± 0.1</td><td>10.6 ± 1.0</td><td>5729 ± 25</td><td>141</td><td>0.415</td><td>-4.347</td><td></td></tr><tr><td>TYC 7796 2110 1</td><td>5256.82087</td><td>+21.6 ± 9.6</td><td></td><td></td><td>339</td><td>0.881</td><td>-4.183</td><td>fast-rot/SB</td></tr><tr><td>HD 124831</td><td>3909.59212</td><td>+11.5 ± 0.8</td><td></td><td>5324 ± 92</td><td>200</td><td>0.534</td><td>-4.137</td><td></td></tr><tr><td>HIP 70351</td><td>4940.77047</td><td>-8.6 ± 0.2</td><td>12.3 ± 0.7</td><td>5624 ± 50</td><td>164</td><td>0.460</td><td>-4.301</td><td></td></tr><tr><td>GJ 560 A</td><td>3423.83863</td><td>+6.2 ± 0.2</td><td>14.5 ± 1.8</td><td>6067 ± 172</td><td></td><td></td><td></td><td></td></tr><tr><td>GJ 560 B</td><td>3423.82772</td><td>+6.6 ± 0.4</td><td>3.0 ± 1.2</td><td>4761 ± 35</td><td></td><td></td><td></td><td></td></tr><tr><td>HD 129181</td><td>4496.86468</td><td>+4.8 ± 4.6</td><td></td><td></td><td>135</td><td>0.672</td><td>-4.705</td><td></td></tr><tr><td>HD 129181</td><td>4496.87658</td><td>+2.8 ± 4.0</td><td></td><td></td><td>130</td><td>0.379</td><td>-4.352</td><td></td></tr><tr><td>HIP 78747</td><td>4940.86043</td><td>-8.2 ± 0.5</td><td>24.0 ± 3.0</td><td>6005 ± 55</td><td>23</td><td>0.175</td><td>-4.861</td><td></td></tr><tr><td>HIP 80758</td><td>4940.86585</td><td>+6.0 ± 0.1</td><td>10.8 ± 1.0</td><td>5328 ± 28</td><td>262</td><td>0.878</td><td>-4.065</td><td></td></tr><tr><td>TYC 6815-0874-1</td><td></td><td></td><td></td><td></td><td></td><td>0.491</td><td>-4.321</td><td></td></tr><tr><td>CD-25 11942</td><td>3909.79462</td><td>-1.5 ± 5.4</td><td></td><td>5300 ± 150</td><td>240</td><td>0.879</td><td>-4.184</td><td>E(B-V) = 0.08; fast-rot. SB2?</td></tr><tr><td>TYC 8728 2262 1</td><td>4941.87270</td><td>-0.2 ± 0.9</td><td></td><td>5245 ± 110</td><td>325</td><td>1.228</td><td>-3.992</td><td></td></tr><tr><td>TYC 7401 2446 1</td><td>5106.60454</td><td>-15.0 ± 0.1</td><td>4.3 ± 0.7</td><td>5311 ± 18</td><td>155</td><td>0.618</td><td>-4.289</td><td></td></tr><tr><td>TYC 6893 1391 1</td><td>5052.76453</td><td>-13.9 ± 0.5</td><td>3.7 ± 1.0</td><td>5005 ± 25</td><td>121</td><td>0.780</td><td>-4.334</td><td></td></tr><tr><td>BD-14 5534</td><td></td><td></td><td></td><td></td><td></td><td>0.401</td><td>-4.360</td><td></td></tr><tr><td>HD 189285</td><td>3906.84485</td><td>-19.5 ± 0.0</td><td>8.3 ± 0.9</td><td>5545 ± 35</td><td>141</td><td>0.455</td><td>-4.325</td><td></td></tr><tr><td>HD 189285</td><td>4782.52813</td><td>-19.6 ± 0.2</td><td>8.3 ± 0.7</td><td>5620 ± 23</td><td>135</td><td>0.449</td><td>-4.331</td><td></td></tr></tbody></table>
<table><caption>**Table 1.** continued.</caption><thead><tr><th>Name</th><th>HJD<br/>-2 450 000</th><th>HRV<br/>km s<sup>-1</sup></th><th>v sin i<br/>km s<sup>-1</sup></th><th>T<sub>eff</sub><br/>K</th><th>EW (Li)<br/>mÅ</th><th>S-index</th><th>log R<sub>HK</sub></th><th>Remarks</th></tr></thead><tbody><tr><td>HD 189245</td><td>5052.80066</td><td>-10.0 ± 2.0</td><td></td><td></td><td></td><td>0.303</td><td>-4.442</td><td>ultrafast-rot</td></tr><tr><td>TYC 5164 0567 1</td><td>3906.85805</td><td>-16.5 ± 0.0</td><td>7.8 ± 0.9</td><td>5140 ± 20</td><td>280</td><td>0.916</td><td>-4.333</td><td></td></tr><tr><td>TYC 5164 0567 1</td><td>4783.49700</td><td>-16.5 ± 0.1</td><td>7.7 ± 0.9</td><td>5197 ± 25</td><td>260</td><td>0.821</td><td>-4.382</td><td></td></tr><tr><td>HD 191089</td><td>3102.88426</td><td>-6.4 ± 1.7</td><td></td><td>5629 ± 165</td><td>91</td><td>0.200</td><td>-4.735</td><td>fast-rot.</td></tr><tr><td>HD 191089</td><td>3102.8</td><td></td><td></td><td></td><td></td><td>0.201</td><td>-4.733</td><td></td></tr><tr><td>HD 199058</td><td>3908.85303</td><td>-18.7 ± 0.7</td><td>13.2 ± 0.6</td><td>5680 ± 60</td><td>160</td><td>0.392</td><td>-4.345</td><td></td></tr><tr><td>HD 199058</td><td>4783.51539</td><td>-18.7 ± 0.7</td><td>14.5 ± 0.5</td><td>5752 ± 41</td><td>160</td><td>0.377</td><td>-4.367</td><td></td></tr><tr><td>TYC 1090 0543 1</td><td>3908.85620</td><td>-19.5 ± 0.0</td><td>17.3 ± 1.4</td><td>4775 ± 45</td><td>115</td><td>2.650</td><td>-3.975</td><td></td></tr><tr><td>TYC 5206 0915 1</td><td>5068.62201</td><td>+0.9 ± 0.6</td><td>22.9 ± 1.6</td><td>5170 ± 65</td><td>40</td><td>1.115</td><td>-4.011</td><td></td></tr><tr><td>HD 203019</td><td>3904.90932</td><td>+23.9 ± 0.2</td><td>5.3 ± 1.0</td><td>5661 ± 22</td><td></td><td>0.429</td><td>-4.337</td><td></td></tr><tr><td>HIP 105612</td><td>5054.77872</td><td>-2.7 ± 0.5</td><td>3.0 ± 1.0</td><td>5647 ± 25</td><td>29</td><td>0.327</td><td>-4.491</td><td></td></tr><tr><td>CD-40 14901</td><td>4788.51865</td><td>-11.0 ± 0.5</td><td>15.0 ± 1.5</td><td>5653 ± 51</td><td>164</td><td>0.502</td><td>-4.239</td><td></td></tr><tr><td>HD 217987</td><td>4784.54545</td><td>+7.5 ± 0.5</td><td>2.7 ± 0.5</td><td></td><td>0</td><td></td><td></td><td></td></tr><tr><td>HD 220054</td><td>4778.57584</td><td>+7.3 ± 1.7</td><td></td><td></td><td>221</td><td>0.568</td><td>-4.167</td><td></td></tr><tr><td>HIP 116063</td><td>5004.94059</td><td>+3.1 ± 0.0</td><td>2.6 ± 0.9</td><td>5963 ± 30</td><td>110</td><td>0.311</td><td>-4.465</td><td></td></tr></tbody></table>

<table><caption>**Table 2.** Measurements of spectroscopic parameters from CORALIE RV survey.</caption><thead><tr><th>ID1</th><th>ID2</th><th>N</th><th>RV<br/>km s<sup>-1</sup></th><th>v sin i<br/>km s<sup>-1</sup></th><th>log R<sub>HK</sub></th><th>Remarks</th></tr></thead><tbody><tr><td>HIP 6177</td><td>HD 8049</td><td></td><td></td><td>3.52</td><td>-4.252</td><td>RV trend, Zurlo et al. (2013)</td></tr><tr><td>HIP 14684</td><td>HD 19668</td><td>4</td><td>14.65</td><td>6.29</td><td>-4.38</td><td></td></tr><tr><td>HIP 37923</td><td>HD 63608</td><td>5</td><td>17.73</td><td>2.67</td><td>-4.372</td><td></td></tr><tr><td>HIP 79958</td><td>HD 146464</td><td>3</td><td>1.74</td><td></td><td>-4.445</td><td></td></tr><tr><td>HIP 105384</td><td>HD 203019</td><td>10</td><td>24.43</td><td>5.86</td><td>-4.356</td><td></td></tr><tr><td>HIP 105612</td><td>HD 202732</td><td>3</td><td>-1.7</td><td>3.28</td><td>-4.476</td><td></td></tr></tbody></table>

<table><caption>**Table 3.** Measurements of spectroscopic parameters from dedicated CORALIE observations.</caption><thead><tr><th>ID1</th><th>JD -2 450 000</th><th>RV<br/>km s<sup>-1</sup></th><th>FWHM<br/>km s<sup>-1</sup></th><th>S/N</th><th>Remarks</th></tr></thead><tbody><tr><td>TYC 8128-1946-1</td><td>5927.6395</td><td>17.0 ± 0.5</td><td>...</td><td>94</td><td>individual lines, v sin i ~ 50 km s<sup>-1</sup></td></tr><tr><td>HIP 36312</td><td>5931.8242</td><td>16.62 ± 0.07</td><td>40.1</td><td>43</td><td>pipeline</td></tr><tr><td>TYC 7796-2110-1</td><td>5931.8261</td><td>1.3 ± 4.5</td><td>...</td><td>15</td><td>individual lines, v sin i ~ 90 km s<sup>-1</sup></td></tr><tr><td>TYC 7188-0575-1</td><td>5931.8654</td><td>-38.75 ± 0.05</td><td>42.9</td><td>32</td><td>manual recorrelation</td></tr><tr><td>HIP 25436</td><td>6360.6450</td><td>21.8 ± 3.8</td><td>...</td><td>32</td><td>individual lines, v sin i ~ 110 km s<sup>-1</sup></td></tr><tr><td>HIP 25434</td><td>6360.6380</td><td>24.2 ± 1.5</td><td>...</td><td>17</td><td>individual lines, v sin i ~ 50 km s<sup>-1</sup></td></tr><tr><td>TYC 7188-0575-1</td><td>6357.7972</td><td>-24.71 ± 0.08</td><td>39.1</td><td>14</td><td>manual recorrelation</td></tr><tr><td>HIP 35564</td><td>6357.7330</td><td>13.7 ± 1.1</td><td>...</td><td>108</td><td>individual lines, v sin i ~ 60 km s<sup>-1</sup></td></tr><tr><td>HIP 72399</td><td>6357.7867</td><td>30.31 ± 0.05</td><td>15.1</td><td>17</td><td>pipeline</td></tr><tr><td></td><td>6357.8246</td><td>33.24 ± 0.06</td><td>16.7</td><td>16</td><td>pipeline</td></tr><tr><td>HIP 72400</td><td>6360.7397</td><td>1.35 ± 0.02</td><td>8.1</td><td>23</td><td>pipeline</td></tr><tr><td>HIP 13008</td><td>6509.9063</td><td>0.6 ± 1.6</td><td>...</td><td>27</td><td>individual lines, v sin i ~ 80 km s<sup>-1</sup></td></tr><tr><td>TYC 5606-0915-1</td><td>6508.6744</td><td>17.47 ± 0.06</td><td>31.0</td><td>21</td><td>pipeline</td></tr></tbody></table>
<table><caption>**Table 4.** Measurements of spectroscopic parameters from HARPS spectra.</caption><thead><tr><th>ID1</th><th>N</th><th>JD start<br>-2450 000</th><th>JD end<br>-2450 000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>rms RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>FWHM<br>(km s<sup>-1</sup>)</th><th>log R<sub>HK</sub></th><th>EW(Li)<br>(mÅ)</th><th>T<sub>eff</sub><br>(K)</th><th>Remarks</th></tr></thead><tbody><tr><td>HIP 6177</td><td>1</td><td>3263.</td><td>—</td><td>42.00</td><td>—</td><td>7.19</td><td>—</td><td>—</td><td>0</td><td>5045 ± 17</td><td>Zurlo et al. (2013)</td></tr><tr><td>HIP 11360</td><td>8</td><td>4439.68</td><td>4479.58</td><td>0.81</td><td>2.13<br>0.12</td><td>—</td><td>~20</td><td>—</td><td>95</td><td>—</td><td>pipeline<br>SAFIR</td></tr><tr><td>HIP 14684</td><td>12</td><td>3311.79</td><td>3805.53</td><td>14.72</td><td>0.05</td><td>—</td><td>10.304</td><td>—</td><td>179</td><td>5451 ± 7</td><td>—</td></tr><tr><td>HIP 32235</td><td>17</td><td>2948.87</td><td>3805.62</td><td>20.72</td><td>0.13</td><td>17.38</td><td>18.124</td><td>-4.169</td><td>239</td><td>5493 ± 11</td><td>—</td></tr><tr><td>HIP 36948</td><td>12</td><td>5343.45</td><td>5347.47</td><td>22.64</td><td>0.04</td><td>—</td><td>12.830</td><td>—</td><td>173</td><td>5493 ± 15</td><td>—</td></tr><tr><td>TWA 21</td><td>24</td><td>3402.83</td><td>4877.76</td><td>18.05</td><td>0.17</td><td>—</td><td>13.805</td><td>-4.06</td><td>364</td><td>4929 ± 4</td><td>—</td></tr><tr><td>TYC 9245-0617-1</td><td>1</td><td>4594.78</td><td>—</td><td>11.49</td><td>—</td><td>—</td><td>—</td><td>—</td><td>438</td><td>5052 ± 111</td><td>—</td></tr><tr><td>HIP 71908</td><td>15</td><td>—</td><td>—</td><td>7.07</td><td>0.15</td><td>—</td><td>19.459</td><td>—</td><td>—</td><td>—</td><td>subset of data</td></tr><tr><td>HIP 72399</td><td>1</td><td>3409.89</td><td>—</td><td>-11.71</td><td>—</td><td>14.15</td><td>—</td><td>-4.148</td><td>0</td><td>4903 ± 32</td><td>pipeline<br>SAFIR</td></tr><tr><td>HIP 76829</td><td>8</td><td>4542.72</td><td>4546.72</td><td>-7.08</td><td>0.63<br>0.03</td><td>—</td><td>~23</td><td>—</td><td>0</td><td>—</td><td>pipeline<br>SAFIR</td></tr><tr><td>HIP 79958</td><td>1</td><td>3828.80</td><td>—</td><td>1.74</td><td>—</td><td>—</td><td>29.978</td><td>—</td><td>117</td><td>4838 ± 44</td><td>pipeline<br>SAFIR, subset of data, Lagrange et al. (2009)</td></tr><tr><td>HIP 98470</td><td>33</td><td>3622.54</td><td>5726.84</td><td>-10.27</td><td>2.02<br>0.09</td><td>100</td><td>—</td><td>—</td><td>90</td><td>—</td><td>pipeline<br>SAFIR, subset of data, Lagrange et al. (2009)</td></tr><tr><td>HIP 114046</td><td>77</td><td>2985.57</td><td>4392.68</td><td>9.00</td><td>0.01</td><td>—</td><td>3.184</td><td>—</td><td>0</td><td>—</td><td>pipeline<br>SAFIR, subset of data, Lagrange et al. (2009)</td></tr></tbody></table>

**Notes.** The mean measurement of individual spectra is listed when more than one spectrum is available. For early-type stars we list both the absolute RV obtained with the HARPS pipeline and the RV dispersion of the differential RV obtained with the SAFIR code.

<table><caption>**Table 6.** Wide binaries in the NaCo-LP sample.</caption><thead><tr><th>NaCo LP<br>Target</th><th>Companion</th><th>Sep.<br>(arcsec)</th><th>Sep.<br>(AU)</th><th>avg<sub>μ</sub><br>(mas/yr)</th><th>Δ<sub>μ</sub><br>(mas/yr)</th><th>ΔV<br>(mag)</th><th>fr<sub>μ</sub></th><th>Δ<sub>X</sub></th><th>|ΔRV|<br>(km s<sup>-1</sup>)</th><th>N<sub>comp</sub></th></tr></thead><tbody><tr><td>HIP 8038</td><td>HIP 8039</td><td>15.0</td><td>435</td><td>51.7</td><td>7.0</td><td>1.88</td><td>0.14</td><td>2.7</td><td>0.75</td><td>3</td></tr><tr><td>TYC 8484-1507-1</td><td>HIP 12326</td><td>8.7</td><td>535</td><td>87.1</td><td>7.9</td><td>0.51</td><td>0.09</td><td>0.7</td><td>0.00</td><td>4</td></tr><tr><td>TYC 8484-1507-1</td><td>HIP 12361</td><td>213.2</td><td>12557</td><td>88.4</td><td>6.7</td><td>1.58</td><td>0.072</td><td>3.0</td><td>1.10</td><td>—</td></tr><tr><td>HIP 25434</td><td>HIP 25436</td><td>12.0</td><td>976</td><td>27.1</td><td>3.7</td><td>0.80</td><td>0.14</td><td>6.2</td><td>0.60</td><td>3</td></tr><tr><td>HIP 35564</td><td>HD 57853</td><td>9.2</td><td>275</td><td>151.6</td><td>47.9</td><td>0.58</td><td>0.37</td><td>0.9</td><td>3.20</td><td>5</td></tr><tr><td>TYC 8128-1946-1</td><td>HIP 36312</td><td>81.7</td><td>6853</td><td>51.9</td><td>3.6</td><td>1.05</td><td>0.07</td><td>4.4</td><td>2.20</td><td>2</td></tr><tr><td>HIP 37923</td><td>HIP 37918</td><td>23.1</td><td>836</td><td>166.2</td><td>15.4</td><td>0.08</td><td>0.09</td><td>0.5</td><td>0.10</td><td>2</td></tr><tr><td>HIP 46634</td><td>HIP 46637</td><td>14.0</td><td>508</td><td>202.7</td><td>5.3</td><td>0.18</td><td>0.03</td><td>0.02</td><td>1.33</td><td>3</td></tr><tr><td>HIP 47646</td><td>HIP 47645</td><td>16.5</td><td>1161</td><td>123.2</td><td>3.2</td><td>2.78</td><td>0.03</td><td>0.3</td><td>—</td><td>2</td></tr><tr><td>HIP 58240</td><td>HIP 58241</td><td>18.6</td><td>649</td><td>174.9</td><td>34.5</td><td>0.03</td><td>0.2</td><td>0.5</td><td>0.90</td><td>2</td></tr><tr><td>HIP 71908</td><td>SAO 252852</td><td>15.8</td><td>263</td><td>302.6</td><td>0.7</td><td>5.22</td><td>0.0024</td><td>0.03</td><td>0.50</td><td>2</td></tr><tr><td>HIP 72399</td><td>HIP 72400</td><td>11.0</td><td>609</td><td>142.7</td><td>12.2</td><td>1.06</td><td>0.09</td><td>0.4</td><td>4.50</td><td>3</td></tr><tr><td>TYC 6786-0811-1</td><td>HIP 77235</td><td>50.5</td><td>3588</td><td>64.5</td><td>10.0</td><td>2.38</td><td>0.15</td><td>3.3</td><td>3.30</td><td>2–5?</td></tr><tr><td>HD 199058</td><td>TYC 1090-0543-1</td><td>245.1</td><td>16200</td><td>68.0</td><td>3.3</td><td>2.92</td><td>0.05</td><td>4.0</td><td>0.70</td><td>3</td></tr><tr><td>TYC 9339-2158-1</td><td>HIP 116063</td><td>36.3</td><td>1109</td><td>220.4</td><td>4.2</td><td>1.89</td><td>0.02</td><td>0.2</td><td>0.50</td><td>2</td></tr></tbody></table>

**Notes.** We list the name of the star observed with NaCo, the name of the wide companion, the projected separations in arcsec and in AU, the average proper motion of the components, the proper motion difference, the magnitude difference ΔV, the fractional proper motion difference, the Δχ index, the absolute value of the RV difference and the number of components. For high-multiplicity systems, additional remarks are listed. Note on high-multiplicity systems: HIP 8038: close visual binary (VB); TYC 8484-1507-1: close VB and SB2 (likely same companion); HIP 12361: wide companion to TYC 8484-1507-1 and HIP 12326 triple system; HIP 25436: spectroscopic and astrometric binary; HIP 35564: SB; HD 57853: SB3; HIP 46637: SB; HIP 72399: SB; TYC 6786-0811-1: close VB; HIP 77235: triple system but physical link to TYC 6786-0811-1 needs confirmation; HD 199058: close VB. See Appendix B for further details and references.
<table><caption>**Table 8.** Properties of young moving groups (MGs).</caption><thead><tr><th>MG</th><th>U<br>km s<sup>-1</sup></th><th>V<br>km s<sup>-1</sup></th><th>W<br>km s<sup>-1</sup></th><th>Ref.</th><th>Age<br>best</th><th>Age<br>min</th><th>Age<br>max</th><th>Ref.</th><th>N</th></tr></thead><tbody><tr><td>TW Hydrae Association</td><td>-9.87 ± 4.15</td><td>-18.06 ± 1.44</td><td>-4.52 ± 2.80</td><td>Mal13</td><td>8</td><td>6</td><td>12</td><td>ZS04</td><td>0</td></tr><tr><td>β Pictoris Moving Group</td><td>-10.94 ± 2.06</td><td>-16.25 ± 1.30</td><td>-9.27 ± 1.54</td><td>Mal13</td><td>16</td><td>10</td><td>22</td><td>Des14</td><td>3</td></tr><tr><td>Tucana/Horologium Association</td><td>-9.88 ± 1.51</td><td>-20.70 ± 1.87</td><td>-0.90 ± 1.31</td><td>Mal13</td><td>30</td><td>20</td><td>40</td><td>Tor08</td><td>5+3?</td></tr><tr><td>Columba Association</td><td>-12.24 ± 1.03</td><td>-21.32 ± 1.18</td><td>-5.58 ± 1.89</td><td>Mal13</td><td>30</td><td>20</td><td>40</td><td>Tor08</td><td>5+1?</td></tr><tr><td>Carina Association</td><td>-10.50 ± 0.99</td><td>-22.36 ± 0.55</td><td>-5.84 ± 0.14</td><td>Mal13</td><td>30</td><td>20</td><td>40</td><td>Tor08</td><td>1</td></tr><tr><td>Argus Association</td><td>-21.78 ± 1.32</td><td>-12.08 ± 1.97</td><td>-4.52 ± 0.50</td><td>Mal13</td><td>45</td><td>30</td><td>55</td><td>Des14</td><td>2</td></tr><tr><td>AB Doradus Moving Group</td><td>-7.12 ± 1.39</td><td>-27.31 ± 1.31</td><td>-13.81 ± 2.16</td><td>Mal13</td><td>100</td><td>50</td><td>150</td><td>Des14</td><td>8+1?</td></tr><tr><td>Octans Association</td><td>-14.5 ± 0.9</td><td>-3.6 ± 1.6</td><td>-11.2 ± 1.4</td><td>Tor08</td><td>20</td><td>10</td><td>30</td><td>Tor08</td><td>0</td></tr><tr><td>ε Chamaeleon</td><td>-11.0 ± 1.2</td><td>-19.9 ± 1.2</td><td>-10.4 ± 1.6</td><td>Tor08</td><td>6</td><td>4</td><td>8</td><td>Tor08</td><td>2</td></tr><tr><td>η Chamaeleon</td><td>-12.0 ± 1.0</td><td>-19.0 ± 1.0</td><td>-10.0 ± 1.0</td><td>ZS04</td><td>8</td><td>6</td><td>10</td><td>ZS04</td><td>0</td></tr><tr><td>Cha-Near Association</td><td>-11.0 ± 1.0</td><td>-16.0 ± 1.0</td><td>-8.0 ± 1.0</td><td>ZS04</td><td>10</td><td>6</td><td>15</td><td>ZS04</td><td>0</td></tr><tr><td>Carina-Near Moving Group</td><td>-25.9 ± 1.0</td><td>-18.1 ± 1.0</td><td>-2.3 ± 1.0</td><td>Zuk06</td><td>200</td><td>150</td><td>300</td><td>Zuk06</td><td>4+1?</td></tr><tr><td>Ursa Majoris Moving Group</td><td>14.0 ± 1.0</td><td>1.0 ± 1.0</td><td>-9.0 ± 1.0</td><td>ZS04</td><td>500</td><td>400</td><td>600</td><td>Kin03</td><td>0</td></tr><tr><td>Hercules-Lyra Association</td><td>-13.2 ± 2.5</td><td>-20.6 ± 1.6</td><td>-11.9 ± 1.0</td><td>LoS06</td><td>200</td><td>150</td><td>300</td><td>LoS06</td><td>1</td></tr><tr><td>Corona Australis Association</td><td>-3.8 ± 1.2</td><td>-14.3 ± 1.7</td><td>-8.3 ± 2.0</td><td>Qua01</td><td>10</td><td>6</td><td>20</td><td>Qua01</td><td>3?</td></tr><tr><td>IC 2391 Open Cluster</td><td>-20.6 ± 2.0</td><td>-15.7 ± 2.0</td><td>-9.1 ± 2.0</td><td>Mon01</td><td>45</td><td>30</td><td>55</td><td>Des14</td><td>0</td></tr><tr><td>Hyades Open Cluster</td><td>-40.0 ± 2.0</td><td>-17.0 ± 2.0</td><td>-3.0 ± 2.0</td><td>ZS04</td><td>625</td><td>575</td><td>675</td><td>Per98</td><td>0</td></tr><tr><td>Pleiades Open Cluster</td><td>-12.0 ± 2.0</td><td>-21.0 ± 2.0</td><td>-11.0 ± 2.0</td><td>ZS04</td><td>125</td><td>110</td><td>140</td><td>Sta98</td><td>0</td></tr><tr><td>Upper Scorpius Association</td><td>-6.4 ± 0.5</td><td>-15.9 ± 0.7</td><td>-7.4 ± 0.2</td><td>Che11</td><td>11</td><td>5</td><td>14</td><td>Pec12</td><td>2?</td></tr><tr><td>Upper Centaurus Lupus Ass.</td><td>-5.1 ± 0.6</td><td>-19.7 ± 0.4</td><td>-4.6 ± 0.3</td><td>Che11</td><td>16</td><td>10</td><td>18</td><td>Pec12</td><td>1?</td></tr><tr><td>Lower Centaurus Crux Ass.</td><td>-7.8 ± 0.5</td><td>-20.7 ± 0.6</td><td>-6.0 ± 0.3</td><td>Che11</td><td>17</td><td>10</td><td>19</td><td>Pec12</td><td>3?</td></tr></tbody></table>

**Notes.** We list the MG name and the *U*, *V*, and *W* space velocity with corresponding literature source. We give the most probable age, minimum and maximum values, and the associated literature source. The final column gives the number of members in the NaCo-LP sample (wide companions not observed with NaCo are not included).

**References.** Mal13: Malo et al. (2013); Tor08: Torres et al. (2008); ZS04: Zuckerman & Song (2004); Mon01: Montes et al. (2001); Zuk06: Zuckerman et al. (2006); Kin03: King et al. (2003); LoS06: López-Santiago et al. (2006); Qua01: Quast et al. (2001); Per98: Perryman et al. (1998); Sta98: Stauffer et al. (1998); Che11: Chen et al. (2011); Pec12: Pecaut et al. (2012); Des14: this paper.
**Appendix A: Literature compilation**

The compilation of literature values for several stellar parame-
ters (RV, v sin i, EW of Li 6707.8 Å resonance line, log R<sub>HK</sub>,
T<sub>eff</sub>) is shown in Table A.1.
<table><caption>**Table A.1.** Summary of measurements of spectroscopic parameters available in the literature.</caption><thead><tr><th>Star</th><th>JD<br>-2450 000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub></th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td>TYC 5839-0596-1</td><td></td><td>20.0</td><td>36.5 ± 3.7</td><td>100</td><td></td><td></td><td></td><td>SACY</td><td>N = 1, SB2, Halpha emission</td></tr><tr><td>TYC 5839-0596-1a</td><td>5106.75</td><td>+51.5 ± 1.5</td><td>18.0 ± 2.0</td><td></td><td>2.135</td><td>-3.990</td><td></td><td>Des14</td><td>FEROS, deblended</td></tr><tr><td>TYC 5839-0596-1b</td><td>5106.75</td><td>+21.3 ± 1.5</td><td>17.0 ± 2.0</td><td></td><td></td><td></td><td></td><td>Des14</td><td>FEROS, deblended</td></tr><tr><td>TYC 0603-0461-1</td><td></td><td>-12.9</td><td></td><td>160</td><td></td><td></td><td></td><td>SACY</td><td>N = 1 Halpha emission</td></tr><tr><td rowspan="4">HIP 3924</td><td></td><td>10.7</td><td>28</td><td>138</td><td></td><td></td><td></td><td>Wic03</td><td></td></tr><tr><td></td><td></td><td>33.5 ± 1.9</td><td>132 ± 5</td><td></td><td></td><td></td><td>Wei10</td><td></td></tr><tr><td>5056.95</td><td>+1.5 ± 0.5</td><td>8.0 ± 2.0</td><td>37</td><td>0.257</td><td>-4.572</td><td>5609 ± 105</td><td>Des14</td><td>FEROS, A component</td></tr><tr><td>5056.95</td><td>~19</td><td></td><td></td><td></td><td></td><td></td><td>Des14</td><td>FEROS, B component</td></tr><tr><td></td><td>5056.95</td><td>~9</td><td></td><td></td><td></td><td></td><td></td><td>Des14</td><td>approx. center of mass RV</td></tr><tr><td>HIP 6177</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>SACY</td><td>see Zurlo et al. (2013)</td></tr><tr><td>HIP 8038</td><td></td><td>8.7</td><td>5.0</td><td>80</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td rowspan="2">HIP 8039</td><td></td><td>9.5</td><td>5.0</td><td>80</td><td></td><td>0.459</td><td>-4.457</td><td>Gra06</td><td>N = 1</td></tr><tr><td></td><td>9.4 ± 0.3</td><td>5.0</td><td></td><td></td><td></td><td></td><td>Nor04</td><td>N = 3, rms RV 0.6 km s<sup>-1</sup></td></tr><tr><td>HIP 10602</td><td></td><td>10.4 ± 1.3</td><td></td><td>240</td><td>0</td><td></td><td>15665</td><td>BaB00</td><td>N = 8</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>12470 ± 560</td><td>DaS09</td><td></td></tr><tr><td rowspan="5">HIP 11360</td><td></td><td>8.8 ± 3.0</td><td></td><td>40</td><td></td><td></td><td></td><td>Deb08</td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Moo06</td><td></td></tr><tr><td>5399.87</td><td>2.9 ± 4.1</td><td></td><td>99</td><td>0.199</td><td>-4.748</td><td>6755 ± 71</td><td>Mas06</td><td></td></tr><tr><td>5399.88</td><td>1.9 ± 2.8</td><td></td><td>90</td><td>0.194</td><td>-4.769</td><td></td><td>Des14</td><td>FEROS</td></tr><tr><td>4439–4479</td><td>0.8 ± 0.8</td><td></td><td>95</td><td></td><td></td><td></td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Des14</td><td>HARPS N = 8</td></tr><tr><td rowspan="6">HIP 12326</td><td></td><td>16.0 ± 0.2</td><td>22.3 ± 0.4</td><td>50</td><td></td><td></td><td>6200</td><td>SACY</td><td>N = 3; rms RV 0.3 km s<sup>-1</sup></td></tr><tr><td></td><td>15.9</td><td>22</td><td>55</td><td></td><td></td><td></td><td>Tor00</td><td></td></tr><tr><td>-44.21</td><td>16.1 ± 0.7</td><td>21 ± 2</td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td>-42.24</td><td>16.4 ± 2.6</td><td></td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td>-40.21</td><td>15.6 ± 2.1</td><td></td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td></td><td>16.1</td><td></td><td></td><td></td><td></td><td></td><td>Mon01</td><td></td></tr><tr><td></td><td></td><td></td><td>20</td><td>58</td><td></td><td>6200</td><td>Fav95</td><td></td></tr><tr><td></td><td>16.2 ± 0.2</td><td>20</td><td>40</td><td></td><td></td><td></td><td>Moo11</td><td></td></tr><tr><td></td><td>15.5 ± 0.5</td><td>22.0 ± 2.0</td><td>46</td><td>0.305</td><td>-4.443</td><td>5979 ± 85</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="5">TYC 8484-1507-1</td><td></td><td>16.8 ± 0.9</td><td>6.0 ± 0.2</td><td>250</td><td></td><td></td><td>5600</td><td>SACY</td><td>N = 3 rms RV = 1.6 km s<sup>-1</sup>, SB?</td></tr><tr><td></td><td>15.9</td><td>8</td><td>255</td><td></td><td></td><td></td><td>Tor00</td><td></td></tr><tr><td>-44.24</td><td>16.4 ± 0.7</td><td>11 ± 3</td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td>-42.22</td><td>16.2 ± 0.9</td><td></td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td>-40.19</td><td>15.9 ± 1.1</td><td></td><td></td><td></td><td></td><td></td><td>Cut99</td><td>components exchanged</td></tr><tr><td></td><td></td><td></td><td>&lt;8</td><td>193</td><td></td><td>5610</td><td>Fav95</td><td></td></tr><tr><td></td><td>15.8 ± 0.3</td><td></td><td>220</td><td></td><td></td><td></td><td>Moo11</td><td></td></tr><tr><td>HIP 12361</td><td></td><td>17.3 ± 8.5</td><td>100</td><td></td><td></td><td></td><td></td><td>Moo11</td><td></td></tr><tr><td rowspan="3">HIP 12394</td><td></td><td>13.6 ± 0.9</td><td></td><td></td><td></td><td></td><td></td><td>XHIP</td><td></td></tr><tr><td></td><td></td><td>96 ± 8</td><td></td><td></td><td></td><td></td><td>Roy02</td><td></td></tr><tr><td></td><td></td><td>98</td><td></td><td></td><td></td><td></td><td>Pau05</td><td></td></tr><tr><td></td><td></td><td></td><td>99.5 ± 18.6</td><td></td><td></td><td></td><td>Zor12</td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Rei04</td><td></td></tr><tr><td rowspan="6">HIP 13008</td><td></td><td>3.2 ± 2.0</td><td></td><td></td><td></td><td></td><td></td><td>Nor04</td><td></td></tr><tr><td></td><td>3.2 ± 2.0</td><td></td><td></td><td></td><td></td><td></td><td>BaB00</td><td>N = 3, RV var</td></tr><tr><td></td><td>2.4 ± 0.7</td><td></td><td></td><td></td><td></td><td></td><td>Gon06</td><td>N = 2 rms 0.8 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Mas06</td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>Gra06</td><td></td></tr><tr><td></td><td>2.12 ± 0.73</td><td></td><td></td><td></td><td>0.428</td><td>-4.161</td><td>6678 ± 76</td><td>N = 1, Suspected SB</td></tr><tr><td></td><td>5198.58</td><td>1.5 ± 1.0</td><td></td><td></td><td>0.228</td><td>-4.642</td><td>6721</td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td>6509.91</td><td>0.6 ± 1.6</td><td>80</td><td></td><td></td><td></td><td></td><td>Des14</td><td>CORALIE</td></tr></tbody></table>

**References.** Des14: this paper; SACY: Torres et al. (2006); Aar08: Aarnio et al. (2008); Alc96: Alcala et al. (1996); Alc00: Alcalá et al. (2000); Amm12: Ammler-von Eiff & Reiners (2012); Baa97: Baade & Kjeldsen (1997); BaB00: Barbier-Brossat & Figon (2000); Bia12: Biazzo et al. (2012); Bub11: Bubar et al. (2011); Cin07: Cincunegui et al. (2007); Cut99: Cutispoto et al. (1999); Cut02: Cutispoto et al. (2002); Cut03: Cutispoto et al. (2003); DaS09: da Silva et al. (2009); Deb08: Debes et al. (2008); Des06: Desidera et al. (2006); DOr12: D’Orazi et al. (2012); Fav95: Favata et al. (1995); Feh74: Fehrenbach & Duflot (1974); Gal05: Gálvez et al. (2005); Gal06: Gálvez et al. (2006); Gle05: Glebocki & Gnicinski (2005); Gon06: Gontcharov (2006); Gra06: Gray et al. (2006); Gre99: Grenier et al. (1999); Gui09: Guillout et al. (2009); Hen96: Henry et al. (1996); Jen06: Jenkins et al. (2006); Jen11: Jenkins et al. (2011); Lag08: Lagrange et al. (2009); LoS06: López-Santiago et al. (2006); Mam02: Mamajek et al. (2002); Mam04: Mamajek (2004); Mas06: Masana et al. (2006); Men08: Mentuch et al. (2008); Mon01: Montes et al. (2001) Moo06: Moór et al. (2006); Moo11: Moór et al. (2011); Moo13: Moór et al. (2013); Nid02: Nidever et al. (2002); Nor04: Nordström et al. (2004); Pau05: Paunzen et al. (2005); Pau06: Paulson & Yelda (2006); RAVE3: Siebert et al. (2011); Rei03: Reid (2003); Rei04: Reiners & Royer (2004); Rei06: Reiners (2006); Rhe07: Rhee et al. (2007); RoP02: Rocha-Pinto et al. (2002); Roy02: Royer et al. (2002); Roy07: Royer et al. (2007); Saa90: Saar et al. (1990); Sch07: Scholz et al. (2007); Sch09: Schröder et al. (2009); Son02: Song et al. (2002); Son03: Song et al. (2003); Son12: Song et al. (2012); Sou10: Soubiran et al. (2010); Str00: Strassmeier et al. (2000); Str12: Strassmeier et al. (2012); Tor00: Torres et al. (2000); ViA09: Viana Almeida et al. (2009); VSOP: Dall et al. (2007); Wai05: Waite et al. (2005); Wai11: Waite et al. (2011); Wei10: Weise et al. (2010); Whi07: White et al. (2007); Wic99: Wichmann et al. (1999); Wic03: Wichmann et al. (2003); Woo05: Woolf & Wallerstein (2005); Wri04: Wright et al. (2004); XHIP: Anderson & Francis (2012); Zor12: Zorec & Royer (2012); Zuk06: Zuckerman et al. (2006).
<table><caption>Table A.1. continued.</caption><thead><tr><th>Star</th><th>JD<br>-2450000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub></th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td>HIP 14684</td><td></td><td></td><td>7.1 ± 1.1<br>7<br>14.2 ± 1.8<br>14.46 ± 0.70<br>14.6 ± 0.7</td><td>165 ± 5<br>191<br>6.2/6.4<br>10.0<br>7.0<br></td><td>0.476<br>0.444</td><td>-4.40<br>-4.40 ± 0.11</td><td>5383<br>5500 ±</td><td>Wei10<br>DaS09<br>Jen11<br>Whi07<br>Pau06<br>Mon01<br>Wri04<br>Str00</td><td>FEROS<br>N = 5</td></tr><tr><td></td><td>3331.69</td><td>14.1 ± 0.5</td><td>5.5 ± 0.6</td><td>175</td><td>0.502</td><td>-4.370</td><td>5463 ± 20</td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td>3981.87</td><td>14.0 ± 0.4</td><td>5.6 ± 0.8</td><td>180</td><td>0.489</td><td>-4.383<br>-4.38</td><td>5478 ± 38</td><td>Des14<br>Des14<br>Des14</td><td>FEROS<br>CORALIE, N = 4</td></tr><tr><td></td><td>3311–3805</td><td>14.65<br>14.71</td><td>6.29</td><td>179</td><td></td><td></td><td>5451 ± 7</td><td>Des14</td><td>HARPS, N = 12</td></tr><tr><td>TYC 8060-1673-1</td><td></td><td>15.3</td><td></td><td>229</td><td></td><td></td><td></td><td>SACY<br>DaS09<br>ViA09<br>Des14</td><td>N = 2, rms RV 0.5 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td>10</td><td></td><td></td><td></td><td>4487<br>4777 ± 70<br>4876 ± 28</td><td></td><td>FEROS N = 2 (same night)</td></tr><tr><td>HIP 19775</td><td></td><td>20.8</td><td>13.9 ± 0.1</td><td>183</td><td></td><td></td><td></td><td>SACY<br>DaS09<br>ViA09<br>Nor04<br>Des14</td><td>N = 3, rms RV 0.3 km s<sup>-1</sup></td></tr><tr><td></td><td>5109.79</td><td>20.4 ± 0.5</td><td>13.1 ± 0.8</td><td>170</td><td>0.433</td><td>-4.261</td><td>5840 ± 45</td><td></td><td>FEROS</td></tr><tr><td>HIP 23316</td><td></td><td>23.5</td><td>7.9 ± 1.2</td><td>210<br>8<br>7</td><td></td><td></td><td></td><td>SACY<br>DaS09<br>ViA09<br>Des14</td><td>N = 1</td></tr><tr><td></td><td>5204.73</td><td>22.5 ± 0.1</td><td>7.7 ± 2.1</td><td>225</td><td>0.659</td><td>-4.108</td><td>5552 ± 33</td><td></td><td>FEROS</td></tr><tr><td>HD 32981</td><td></td><td></td><td>6<br>5.0 ± 2.0<br>4.8 ± 0.6</td><td>140</td><td></td><td></td><td></td><td>DaS09<br>DOr12<br>Des14</td><td></td></tr><tr><td></td><td>4787.65</td><td>25.00 ± 0.00</td><td></td><td></td><td>0.366</td><td>-4.357</td><td>5975</td><td></td><td>FEROS</td></tr><tr><td>BD-09 1108</td><td></td><td></td><td>18.0<br>15.7 ± 1.1</td><td>245<br>205</td><td>0.595</td><td>-4.151</td><td>5645 ±<br>5660 ± 45</td><td>DaS09<br>Des14</td><td>FEROS</td></tr><tr><td>HIP 25434</td><td></td><td>2721.03<br>2721.03<br>Jul.–Aug. 09<br>6360.64</td><td>24.94 ± 0.33<br>23.6 ± 1.8<br>24.2 ± 1.5</td><td>40<br>183<br>158 ± 10</td><td>0.39</td><td>-4.30</td><td></td><td>Des06<br>Des14<br>Moo13<br>Des14</td><td>FEROS, same spec as Des06<br>CORALIE</td></tr><tr><td>HIP 25436</td><td></td><td>2721.01<br>2721.01<br>Jul.–Aug. 09<br>6360.65</td><td>32.17 ± 1.30<br>22.6 ± 6.7<br>21.8 ± 3.8</td><td>112<br>107<br>&lt;41</td><td>0.25</td><td>-4.57</td><td></td><td>Des06<br>Des14<br>Moo13<br>Des14</td><td>FEROS, same spec as Des06<br>CORALIE</td></tr><tr><td>TYC 9162-698-1</td><td></td><td>18.7<br>14 ± 7<br>18.6 ± 0.5</td><td>22.3 ± 3.1<br>20.2 ± 2.6</td><td>226<br>212</td><td>0.482</td><td>-4.232</td><td>5811 ± 105</td><td>SACY<br>Feh74<br>Des14</td><td>N = 7, rms RV 1.0 km s<sup>-1</sup></td></tr><tr><td>TYC 5346-132-1</td><td></td><td>24.5 ± 1.5<br>26.2 ± 1.0</td><td>30<br>29</td><td>290 ± 10<br>350<br>280</td><td>0.937</td><td>-3.992</td><td>5324 ± 87</td><td>Alc00<br>Alc00<br>Alc96<br>Des14</td><td>FEROS</td></tr><tr><td>HIP 30261</td><td></td><td>24.8<br>25.1 ± 0.3</td><td>8.0</td><td>200</td><td></td><td></td><td></td><td>SACY<br>Nor04<br>Mas06<br>Des14</td><td>N = 1<br>N = 1<br>FEROS</td></tr><tr><td>TYC 7617-549-1</td><td></td><td>25.0 ±</td><td>11.6 ± 1.2</td><td>310</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>TYC 9181-0466-1</td><td></td><td>16.4 ± 0.1</td><td>13.5 ± 3.3<br>11.6 ± 0.9</td><td>210<br>198 ± 3</td><td></td><td></td><td></td><td>SACY<br>Wei10<br>Des14<br>Des14</td><td>N = 4<br>FEROS<br>FEROS</td></tr><tr><td></td><td>3807.59</td><td>15.6 ± 0.7</td><td>11.9 ± 1.2</td><td>214</td><td>0.538</td><td>-4.181</td><td>5682 ± 45</td><td></td><td>FEROS</td></tr><tr><td></td><td>3815.59</td><td>16.1 ± 0.6</td><td>11.6 ± 0.9</td><td>205</td><td>0.535</td><td>-4.184</td><td>5670 ± 40</td><td></td><td>FEROS</td></tr><tr><td>HIP 32235</td><td></td><td>20.7 ± 0.1<br>20.1 ± 0.4<br>20.72</td><td>12.4 ± 0.3<br>11.6 ± 1.1<br>17.38</td><td>233<br>237<br>239</td><td>0.621</td><td>-4.154<br>-4.169</td><td>5444 ± 36<br>5493 ± 11</td><td>SACY<br>Des14<br>Des14</td><td>N = 3<br>FEROS<br>HARPS N = 17</td></tr><tr><td>HIP 35564</td><td></td><td>17.3 ± 1.5<br>2721.99<br>Jan. 2006</td><td>26.85 ± 0.79<br>18.6 ± 2.0<br>22.54 ± 0.68<br>21.40 ± 0.60</td><td>68<br>65.6 ± 3.3</td><td>0.23</td><td>-4.64</td><td></td><td>Nor04<br>Des06<br>Zuk06<br>Gre99<br>Gra06<br>XHIP<br>Amm12<br>Des14<br>Des14</td><td>N = 1<br>N = 1<br>N = 1<br>N = 1<br>FEROS<br>CORALIE</td></tr><tr><td></td><td>5109.84</td><td>24.0 ± 2.0</td><td></td><td></td><td>0.218</td><td>-4.667</td><td>6366</td><td></td><td></td></tr><tr><td></td><td>6357.73</td><td>13.7 ± 1.1</td><td>~60</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>HD 57853</td><td></td><td>15.5 ± 3.9<br>2721.99</td><td>0.32 ± 0.18</td><td>20<br>19.5</td><td>0.29<br>0.333</td><td>-4.49</td><td></td><td>Nord04<br>Des06<br>Gra06<br>Saa90</td><td>SB2<br>orbit</td></tr><tr><td></td><td></td><td></td><td>17.6 ± 0.7</td><td>22.0 ± 1.5</td><td></td><td></td><td></td><td></td><td></td></tr></tbody></table>
<table><caption>Table A.1. continued.</caption><thead><tr><th>Star</th><th>JD<br>-2450 000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub></th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td rowspan="3">TYC 7743-1091-1</td><td></td><td>17.4</td><td>17</td><td>114/82</td><td></td><td></td><td></td><td>Wic03</td><td></td></tr><tr><td>3926.52</td><td></td><td>17.6 ± 1.1</td><td>95 ± 1</td><td></td><td></td><td></td><td>Wei10</td><td></td></tr><tr><td>3926.52</td><td>+21.9 ± 0.1</td><td></td><td>113.4 ± 2.0</td><td></td><td></td><td>4931 ± 59</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="5">HIP 58240</td><td></td><td>5.8</td><td>5.2 ± 1.2</td><td>110</td><td></td><td>0.354<br>0.325</td><td>-4.43<br>-4.482</td><td>5749</td><td>Hen96<br>Gra06<br>SACY<br>N = 1<br>Nor04<br>Zuc06<br>DOr12<br>Des14</td><td></td></tr><tr><td></td><td>6.2 ± 0.2</td><td>5</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td>6.0 ± 0.4</td><td></td><td>111</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>5.0 ± 2.0</td><td></td><td></td><td></td><td></td><td>5900</td><td></td></tr><tr><td></td><td>5254.76</td><td>+5.9 ± 0.1</td><td>4.0 ± 0.5</td><td>115</td><td>0.365</td><td>-4.15</td><td>5835 ± 24</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="5">HIP 58241</td><td></td><td>6.9</td><td>9.0 ± 1.2</td><td>110</td><td></td><td>0.398<br>0.388</td><td>-4.34<br>-4.359</td><td>5784</td><td>Hen96<br>Gra06<br>SACY<br>N = 1<br>Nor04<br>Zuc06<br>DOr12<br>Bia12<br>Des14</td><td></td></tr><tr><td></td><td>6.9 ± 0.1</td><td>7</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td>6.7 ± 0.3</td><td></td><td>110</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>9.0 ± 2.0</td><td></td><td></td><td></td><td></td><td>5800</td><td></td></tr><tr><td></td><td>5254.75</td><td>6.9 ± 0.5</td><td>8.2 ± 0.8</td><td>114</td><td>0.394</td><td>-4.350</td><td>5710 ± 22</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="4">TYC 9231-1566-1</td><td></td><td>14.2</td><td>13.1 ± 1.2</td><td>280</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td></td><td>13</td><td>280</td><td></td><td></td><td></td><td>DaS09</td><td></td></tr><tr><td></td><td></td><td>12</td><td>140</td><td></td><td></td><td></td><td>ViA09<br>Mam02<br>Bub11</td><td></td></tr><tr><td></td><td>5254.84</td><td>13.5 ± 0.1</td><td>12.5 ± 0.8</td><td>270</td><td>0.645</td><td>-4.118</td><td>5530 ± 40</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="3">TYC 8979-1683-1</td><td></td><td>13.3</td><td>31.9 ± 3.2</td><td>290</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>4942.79</td><td>12.1 ± 2.6</td><td></td><td>290</td><td>0.868</td><td>-4.059</td><td>5650 ± 145</td><td>Des14<br>Son12</td><td>FEROS<br>N = 3</td></tr><tr><td></td><td>13.9 ± 1.9</td><td></td><td>260</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">TYC 8989-0583-1</td><td></td><td>10.8</td><td>47.0 ± 4.7</td><td>350</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td>10.50 ± 3.0</td><td></td><td>260</td><td></td><td></td><td></td><td>Son12</td><td>N = 3</td></tr><tr><td rowspan="10">TYC 9245-0617-1</td><td></td><td>12.8</td><td>24.3 ± 2.4</td><td>400</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td></td><td>24</td><td>400</td><td></td><td></td><td></td><td>DaS09</td><td></td></tr><tr><td></td><td></td><td></td><td>370</td><td></td><td></td><td>4917<br>5176</td><td>Mam02<br>Gle05<br>Weil0</td><td></td></tr><tr><td></td><td></td><td>20.0 ± 3.0</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>26.0 ± 1.5</td><td>400 ± 6</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>3420.79</td><td>13.2 ± 2.4</td><td>28.2 ± 6.2</td><td>391</td><td>1.597</td><td>-3.873</td><td>5083 ± 70</td><td>Des14</td><td>FEROS</td></tr><tr><td>3421.78</td><td>14.1 ± 0.5</td><td>26.7 ± 2.2</td><td>410</td><td>1.595</td><td>-3.874</td><td>5090 ± 70</td><td>Des14</td><td>FEROS</td></tr><tr><td>3421.88</td><td>14.7 ± 0.7</td><td>28.8 ± 2.0</td><td>415</td><td></td><td></td><td>5114 ± 62</td><td>Des14</td><td>FEROS</td></tr><tr><td>3422.76</td><td>12.2 ± 0.6</td><td>26.2 ± 3.1</td><td>410</td><td>1.592</td><td>-3.874</td><td>5059 ± 65</td><td>Des14</td><td>FEROS</td></tr><tr><td>4582.77</td><td>9.6 ± 0.9</td><td>26.0 ± 1.7</td><td>393</td><td>1.441</td><td>-3.919</td><td>5071 ± 65</td><td>Des14</td><td>FEROS</td></tr><tr><td>4594.78</td><td>11.5</td><td></td><td>438</td><td></td><td></td><td>5052 ± 111</td><td>Des14</td><td>HARPS, N = 1</td></tr><tr><td></td><td>11.1 ± 1.5</td><td></td><td>350</td><td></td><td></td><td></td><td>Son12</td><td>N = 3</td></tr><tr><td rowspan="10">HIP 63862</td><td></td><td>1.1</td><td>10.9 ± 1.2</td><td>140.0</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td>1.1 ± 0.2</td><td>11</td><td></td><td></td><td></td><td></td><td>Nor04<br>Weil0<br>Wai05</td><td>N = 5</td></tr><tr><td></td><td>2</td><td>11.6 ± 0.9</td><td>139 ± 1</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>10</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>12</td><td>155</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td>1.1</td><td>11</td><td>154</td><td></td><td></td><td></td><td>Cut02-03<br>Wic03<br>Hen96</td><td>N = 1</td></tr><tr><td>3447.88</td><td>1.3 ± 0.1</td><td>10.6 ± 0.9</td><td>145</td><td>0.460</td><td>-4.30</td><td>5760 ± 32</td><td>Des14</td><td>FEROS</td></tr><tr><td>3447.87</td><td>1.3 ± 0.1</td><td>10.6 ± 1.0</td><td>141</td><td>0.416</td><td>-4.347</td><td>5729 ± 25</td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="3">TYC 7796-2110-1</td><td></td><td>25.0</td><td>113.0 ± 11.3</td><td>400:</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td></td><td></td><td>315</td><td></td><td></td><td></td><td>Son12</td><td>N = 1</td></tr><tr><td></td><td>5256.82</td><td>21.6 ± 9.6</td><td>fast</td><td>339</td><td>0.881</td><td>-4.183</td><td>Des14<br>Des14</td><td>FEROS<br>CORALIE</td></tr><tr><td></td><td>5931.83</td><td>1.3 ± 4.5</td><td>~90</td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="3">TYC 9010-1272-1</td><td></td><td>10.2</td><td>38 ± 3.8</td><td>210</td><td></td><td></td><td></td><td>SACY</td><td>N = 2, rms RV 0.5 km s<sup>-1</sup>, SB2?</td></tr><tr><td></td><td>43.4 ± 4.9</td><td>8</td><td></td><td></td><td></td><td></td><td>Nor04<br>Des14</td><td>N = 5 rms RV 11 km s<sup>-1</sup><br>FEROS, SB2</td></tr><tr><td></td><td>3909.59</td><td>11.5 ± 0.8</td><td>200</td><td>0.534</td><td>-4.137</td><td>5324 ± 92</td><td>Des14</td><td></td></tr><tr><td rowspan="2">HIP 70351</td><td></td><td>-8.3</td><td>16.9 ± 1.2</td><td>170</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td>4940.77</td><td>-8.6 ± 1.2</td><td>12.3 ± 0.7</td><td>164</td><td>0.460</td><td>-4.301</td><td>5624 ± 50</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="2">α Cir</td><td></td><td>3423.84</td><td>6.2 ± 0.2</td><td>14.5 ± 1.8</td><td></td><td></td><td></td><td>Des14</td><td>N = 1</td></tr><tr><td></td><td></td><td>7.07</td><td></td><td></td><td></td><td></td><td>Des14</td><td>HARPS, N = 15 subset of data</td></tr><tr><td rowspan="3">GJ 560B</td><td></td><td>7.0 ± 4.0</td><td></td><td></td><td></td><td></td><td></td><td>LoS06</td><td>N = 1</td></tr><tr><td></td><td>3423.83</td><td>6.6 ± 0.4</td><td>3.0 ± 1.2</td><td>0</td><td>0.672</td><td>-4.705</td><td>4761 ± 35</td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="4">HIP 71933</td><td></td><td>8.7</td><td></td><td></td><td></td><td></td><td></td><td>SACY</td><td>N = 1, SB?</td></tr><tr><td></td><td>12.1 ± 0.4</td><td>2.0</td><td></td><td></td><td></td><td></td><td>Nor04<br>Wai11</td><td>N = 1, discr. v sin i</td></tr><tr><td></td><td>4.0</td><td>75</td><td>139 ± 7</td><td></td><td></td><td></td><td>Des14</td><td>N = 2, same night</td></tr><tr><td></td><td>4496.86</td><td>3.8 ± xxx</td><td>132</td><td>0.377</td><td>-4.356</td><td></td><td></td><td></td></tr><tr><td rowspan="3">HIP 72399</td><td></td><td>-25.9</td><td></td><td>0</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td></td><td></td><td></td><td></td><td>2.076</td><td>-4.114</td><td>4903 ± 32</td><td>Gra06<br>Des14<br>Des14</td><td>HARPS N = 1<br>CORALIE</td></tr><tr><td></td><td>3409.89</td><td>-11.71</td><td>14.15</td><td>0</td><td></td><td></td><td></td><td></td></tr><tr><td></td><td>6357.79</td><td>30.31 ± 0.05</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr></tbody></table>
<table><caption>Table A.1. continued.</caption><thead><tr><th>Star</th><th>JD<br>-2450000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub></th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td></td><td>6357.82</td><td>33.24 ± 0.06</td><td></td><td></td><td></td><td></td><td></td><td>Des14</td><td>CORALIE</td></tr><tr><td>HIP 72400</td><td></td><td>0.3</td><td></td><td>0</td><td></td><td>1.176</td><td></td><td>SACY<br>Gra06<br>Des14</td><td>N = 1<br>CORALIE</td></tr><tr><td>TYC 7835-2569-1</td><td></td><td>3.3<br>-10.0 ± 5.0<br>1.9</td><td>17.0<br>17<br>16.0</td><td>150<br>157</td><td></td><td></td><td></td><td>SACY<br>Nor04<br>Wic99</td><td>N = 1<br>N = 2, rms 2.1 km s<sup>-1</sup>, SB</td></tr><tr><td>HIP 76829</td><td></td><td>-5.4 ± 1.8<br>-5.4 ± 2.0</td><td></td><td>71.6 ± 3.6</td><td></td><td>0.234</td><td></td><td>Nor04<br>Mon01<br>Gra06<br>Rei06<br>Sch09<br>Des14</td><td>HARPS N = 8</td></tr><tr><td></td><td>4542-4546</td><td>-7.1</td><td></td><td>0</td><td></td><td></td><td></td><td>SACY<br>Aar08</td><td>N = 1</td></tr><tr><td>TYC 6781-0415-1</td><td></td><td>-6.7<br>-3.0 ± 2.1</td><td>29</td><td>410<br>409/429</td><td></td><td></td><td>5410</td><td>XIP<br>Roy07</td><td>N = 1</td></tr><tr><td>HIP 77235</td><td></td><td>-20.7 ± 1.8</td><td></td><td>68</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>TYC 6786-0811-1</td><td></td><td>-24.0</td><td></td><td>180.0</td><td></td><td></td><td></td><td>Rei03<br>BaB00<br>Gra06<br>Sch09<br>Des14</td><td>N = 1</td></tr><tr><td>HIP 78747</td><td></td><td>-6.2 ± 3.7</td><td>23.7 ± 1.2</td><td></td><td></td><td></td><td></td><td>SACY<br>Nor04<br>Gra06<br>VSOP<br>Des14<br>Des14</td><td>N = 1<br>N = 2 rms 0.4 km s<sup>-1</sup><br>from VSOP web site<br>HARPS<br>CORALIE, N = 3</td></tr><tr><td>TYC 6209-0769-1</td><td></td><td>3.0</td><td></td><td>140</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>HIP 79958</td><td></td><td>2.0<br>1.8 ± 0.4</td><td>16.8 ± 1.2<br>17</td><td>110<br></td><td></td><td>1.725</td><td>-4.147</td><td>SACY<br>Nor04<br>Gra06<br>VSOP<br>Des14<br>Des14</td><td>N = 1<br>N = 2 rms 0.3 km s<sup>-1</sup><br>FEROS</td></tr><tr><td></td><td>3828.80</td><td>1.68<br>1.74<br>1.74</td><td></td><td>117</td><td></td><td>1.912</td><td>4838 ± 44</td><td>SACY<br>Aar08</td><td>N = 1<br>US ?</td></tr><tr><td>HIP 80290</td><td></td><td>-5.0</td><td>37.0 ± 3.7</td><td>200</td><td></td><td></td><td></td><td>SACY</td><td>N = 2 rms 0.2 SB2?</td></tr><tr><td>HIP 80758</td><td></td><td>6.9<br>6.3 ± 0.3<br>6.0 ± 0.1</td><td>11.1 ± 1.2<br>11<br>10.8 ± 1.0</td><td>280<br>262</td><td></td><td>0.878</td><td>-4.065</td><td>SACY<br>Nor04<br>Des14</td><td>N = 2 rms 0.3 km s<sup>-1</sup><br>FEROS</td></tr><tr><td>TYC 6818-1336-1</td><td></td><td>-2.4<br>-4.3 ± 1.6</td><td>71.0 ± 7.1<br>56</td><td>150<br></td><td>180/198</td><td></td><td></td><td>SACY<br>Aar08</td><td>N = 1<br>US ?</td></tr><tr><td>TYC 6815-0874-1</td><td></td><td>0.8</td><td>90.0 ± 2.8</td><td>270</td><td></td><td></td><td></td><td>SACY</td><td>N = 2 rms 0.2 SB2?</td></tr><tr><td>TYC 6815-0084-1</td><td></td><td>-4.4 ± 1.5<br>-1.5 ± 5.4</td><td>57.0 ± 53<br>fast</td><td>310.0<br>307/324<br>240</td><td></td><td>0.879</td><td>5250<br>-4.087</td><td>SACY<br>Aar08<br>Des14</td><td>N = 2 SB2?<br>Upper Sco? dist>100pc</td></tr><tr><td>TYC 7362-0724-1</td><td></td><td>-3.1</td><td>36.7 ± 3.7</td><td>270</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>TYC 8728-2262-1</td><td></td><td>1.6</td><td>35.3 ± 1.4<br>35</td><td>360<br>360<br>325<br>310</td><td></td><td>1.228</td><td>-3.992</td><td>SACY<br>DaS09<br>Des14<br>Son12</td><td>N = 4rms 1.4 km s<sup>-1</sup><br>FEROS<br>N = 2</td></tr><tr><td>HIP 86672</td><td></td><td>-6.2 ± 1.0<br>-5.8 ± 0.5<br>-5.7 ± 2.5</td><td>17<br>15.5 ± 0.2</td><td>260</td><td></td><td></td><td></td><td>Nor04<br>SACY<br>RAVE3</td><td>N = 2 rms RV 1.4 km s<sup>-1</sup><br>N = 4 rms RV 1.3 km s<sup>-1</sup></td></tr><tr><td>HIP 89829</td><td></td><td>-7.0<br>-4.7</td><td>114.7 ± 2.5<br>115<br>114</td><td>290<br>290<br>211 ± 13</td><td></td><td></td><td>5645</td><td>SACY<br>DaS09<br>Wai11</td><td>N = 3 rms RV 2.6 km s<sup>-1</sup></td></tr><tr><td>HIP 93375</td><td></td><td>-5.7<br>-5.8 ± 0.5<br>-6.6 ± 2.2<br>-6.2 ± 2.2</td><td>17<br>17</td><td>140<br></td><td></td><td></td><td>6254<br>6383<br>6577<br>6073 ± 60</td><td>SACY<br>Nor04<br>DaS09<br>RAVE3<br>RAVE3<br>Mas06</td><td>N = 1<br>N = 2 rms RV 0.3 km s<sup>-1</sup></td></tr><tr><td>HIP 94235</td><td></td><td>8.1 ± 0.6</td><td>24<br>24<br>24</td><td>165<br>165<br>165</td><td></td><td></td><td>6102<br>6010 ± 53</td><td>SACY<br>Nor04<br>DaS09<br>Cut02<br>Mas06</td><td>N = 4 rms RV 1.1 km s<sup>-1</sup><br>N = 4 rms RV 1.1 km s<sup>-1</sup></td></tr><tr><td>TYC 6893-1391-1</td><td></td><td>-12.7</td><td>4.5 ± 1.2</td><td>125</td><td></td><td>0.780</td><td>-4.334</td><td>SACY<br>Des14</td><td>N = 1<br>FEROS</td></tr><tr><td>TYC 5736-0649-1</td><td></td><td>-7.0</td><td>206.0 ± 20.6</td><td>250</td><td></td><td>0.401</td><td>-4.360</td><td>SACY<br>Des14</td><td>N = 3, rms RV 3.5 km s<sup>-1</sup>, SB?<br>FEROS</td></tr><tr><td>HD 189285</td><td></td><td></td><td>9.0<br>8.0 ± 2.0<br>8.3 ± 0.9<br>8.3 ± 0.7</td><td>140<br>141<br>135</td><td></td><td>0.455</td><td>-4.325<br>-4.331</td><td>DaS09<br>DOr12<br>Des14<br>Des14</td><td>N = 3, rms RV 3.5 km s<sup>-1</sup>, SB?<br>FEROS<br>FEROS</td></tr></tbody></table>
<table><caption>Table A.1. continued.</caption><thead><tr><th>Star</th><th>JD<br>-2 450 000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub></th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td rowspan="7">HIP 98470</td><td></td><td></td><td>100<br>72.6<br>-13.2 ± 3.7</td><td></td><td>0.339</td><td>-4.309</td><td>6259</td><td>Lag08<br>Sch09<br>Nor04<br>Rei06</td><td>rms RV 86 m/s<br>N = 2, rms RV 2.5 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td>72.6 ± 3.6</td><td></td><td>0.470</td><td>-4.164</td><td>6333</td><td>Gra06<br>Mon01<br>BaB00<br>Baa97</td><td></td></tr><tr><td></td><td></td><td>-8.20 ± 5.0<br>-8.20</td><td>86</td><td></td><td></td><td></td><td></td><td>flagged as SB</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>6399 ± 67</td><td>Mas06<br>Des14<br>Des14</td><td>FEROS<br>HARPS, N = 33</td></tr><tr><td></td><td></td><td>5052.80<br>3622-5726</td><td>-10.0 ± 2.0<br>-10.27</td><td>90</td><td>0.303</td><td>-4.442</td><td></td><td></td><td></td></tr><tr><td rowspan="2">TYC 5164-0567-1</td><td></td><td></td><td>8.00<br>7.8 ± 0.9<br>-16.50 ± 0.00</td><td>290<br>280<br>7.7 ± 0.9</td><td>0.916</td><td>-4.333</td><td>5083<br>5140 ± 20</td><td>DaS09<br>Des14</td><td>FEROS</td></tr><tr><td></td><td></td><td>4783.50<br>-16.50 ± 0.10</td><td>260</td><td>0.821</td><td>-4.382</td><td>5197 ± 25</td><td>Des14</td><td>FEROS</td></tr><tr><td rowspan="7">HIP 99273</td><td></td><td></td><td>-5.8 ± 2.2<br>-7.8 ± 2.2</td><td>45<br>37.7<br>37.0 ± 1.6</td><td>0.247<br>0.257 ± 0.091</td><td>-4.603<br>-4.49 ± 0.24</td><td></td><td>Nor04<br>Sch09<br>Whi07<br>Mam04</td><td>N = 2, rms RV 3.1 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>6521<br>6600<br>6473 ± 68</td><td>DaS09<br>Rhe07<br>Mas06<br>Wei10</td></tr><tr><td></td><td></td><td></td><td>45</td><td>95</td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td></td><td>48.8 ± 3.0<br>fast</td><td>101 ± 5<br>91</td><td>0.200</td><td>-4.734</td><td></td><td>Des14</td><td>FEROS</td></tr><tr><td></td><td></td><td>3102.88<br>-6.4 ± 1.7</td><td>14.00<br>11.00</td><td>160<br>160.5</td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">HD 199058</td><td></td><td></td><td>-19.09 ± 0.99<br>-19.00 ± 1.31<br>-19.18 ± 1.49</td><td></td><td></td><td></td><td></td><td>5894<br>5721</td><td>DaS09<br>Gui09<br>Gui09<br>Gui09</td></tr><tr><td></td><td></td><td>2480.51<br>2481.44<br>3908.85<br>4783.52</td><td>13.20 ± 0.6<br>-18.70 ± 0.70<br>-18.70 ± 0.70</td><td>160<br>160<br>14.50 ± 0.5</td><td>0.392<br>0.377</td><td>-4.345<br>-4.367</td><td>5680 ± 60<br>5752 ± 41</td><td>Des14<br>Des14</td><td></td></tr><tr><td rowspan="2">TYC 1090-0543-1</td><td></td><td></td><td>18.0<br>17.3</td><td>120<br>115</td><td>2.650</td><td>-3.975</td><td>4589<br>4775 ± 45</td><td>DaS09<br>Des14</td><td></td></tr><tr><td></td><td></td><td>3908.86<br>-19.5 ± 0.0</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">TYC 5206-0915-1</td><td></td><td></td><td>-23.3<br>5068.62<br>6508.67</td><td>22.9 ± 1.6</td><td>40<br>40</td><td>1.115</td><td>-4.011</td><td>5170 ± 65</td><td>SACY<br>Des14<br>Des14</td><td>N = 1<br>FEROS<br>CORALIE</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="7">HIP 105384</td><td></td><td></td><td>24.1<br>24.0 ± 0.1</td><td>6.5 ± 1.2<br>6</td><td>0</td><td></td><td></td><td>N = 1<br>Nor04<br>Hen96<br>Gra06<br>Cin07</td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>5774 ± 51</td><td>Mas06<br>Wai05</td><td></td></tr><tr><td></td><td></td><td>23.9<br>+23.9 ± 0.2<br>24.43</td><td>7<br>5.3 ± 1.0<br>5.9</td><td>0<br>0</td><td>0.429</td><td>-4.337<br>-4.356</td><td>5661 ± 22</td><td>Des14<br>Des14</td><td>N = 2<br>FEROS<br>N = 10, CORALIE</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">HIP 105612</td><td></td><td></td><td>-2.8<br>-2.1 ± 0.2</td><td>~5<br>3</td><td>7.6</td><td></td><td></td><td>N = 2<br>Nor04<br>Hen96<br>Gra06</td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>5566<br>5694 ± 44<br>Mas06</td><td></td></tr><tr><td></td><td></td><td>5054.78<br>-2.7 ± 0.5<br>-1.7</td><td>3.0 ± 1.0<br>3.3</td><td>29</td><td>0.327</td><td>-4.491<br>-4.48</td><td>5647 ± 25</td><td>Des14<br>Des14</td><td>FEROS<br>N = 3, CORALIE</td></tr><tr><td rowspan="4">HIP 107684</td><td></td><td></td><td>3.6</td><td>10.4 ± 1.2<br>10<br>9<br>11.2 ± 0.9</td><td>190<br>190<br>190 ± 1</td><td></td><td></td><td>SACY<br>DaS09<br>ViA09<br>Wei10</td><td>N = 2 rms RV 0.5 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td>1.1</td><td>128.2 ± 1.7<br>139.8 ± 9.4</td><td>294<br>261 ± 20</td><td></td><td></td><td>SACY<br>Sch07<br>Men08</td><td>N = 11, rms RV 2.1 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">TYC 8004-0083-1</td><td></td><td></td><td>-9.1<br>-11.0 ± 0.5</td><td>15.1 ± 1.2<br>14.9 ± 1.0<br>15.0 ± 1.5</td><td>175<br>175<br>164</td><td>0.502</td><td>-4.239</td><td>5653 ± 51</td><td>SACY<br>Wei10<br>Des14</td><td>N = 1<br>FEROS</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="7">HIP 114046</td><td></td><td></td><td>8.81<br>7.50<br>7.5 ± 0.2</td><td>1.0</td><td>50</td><td></td><td></td><td>Nid02<br>SACY<br>Nor04<br>Wri04<br>Jen06</td><td>N = 4, rms RV 0.1 km s<sup>-1</sup><br>=4, rms RV 0.1 km s<sup>-1</sup><br>HK outside cal range</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>3680 ± 130</td><td>Woo005<br>Des14<br>Des14</td><td>FEROS<br>HARPS, N = 77</td></tr><tr><td></td><td></td><td>4784.55<br>2985-4392</td><td>+7.5 ± 0.5<br>+9.0</td><td>2.7 ± 0.5</td><td>0</td><td></td><td></td><td></td><td></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td rowspan="2">TYC 9338-2016-1</td><td></td><td></td><td>9.5<br>5.5 ± 1.9</td><td>29.9 ± 0.5</td><td>259</td><td></td><td></td><td>SACY<br>RAVE3</td><td>N = 9, rms RV 0.8 km s<sup>-1</sup></td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr></tbody></table>
<table><caption>**Table A.1.** continued.</caption><thead><tr><th>Star</th><th>JD<br>-2 450 000</th><th>RV<br>(km s<sup>-1</sup>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>EW Li<br>(mÅ)</th><th>S</th><th>log R<sub>HK</sub><br>(K)</th><th>T<sub>eff</sub><br>(K)</th><th>Reference</th><th>Remarks</th></tr></thead><tbody><tr><td></td><td>4778.58</td><td>7.3 ± 1.7</td><td>31.8 ± 1.9</td><td>259 ± 4<br>221</td><td>0.568</td><td>-4.167</td><td></td><td>Wei10<br>Des14</td><td>FEROS</td></tr><tr><td>TYC 9529-0340-1</td><td></td><td>9.2</td><td>73.9 ± 1.4<br>74</td><td>276<br>276</td><td></td><td></td><td>5481</td><td>SACY<br>DaS09</td><td>N = 11 rms RV = 2.0 km s<sup>-1</sup></td></tr><tr><td>TYC 9339-2158-1</td><td></td><td>4.3<br>3.6 ± 0.2</td><td>4.1 ± 1.2<br>4</td><td>30</td><td></td><td></td><td></td><td>SACY<br>Nor04</td><td>N = 1<br>N = 4, rms 0.2 km s<sup>-1</sup></td></tr><tr><td>HIP 116063</td><td></td><td>3.9<br>3.6 ± 0.2</td><td>3.4 ± 1.2<br>4</td><td>110</td><td></td><td>0.284<br>0.277</td><td>-4.51</td><td>SACY<br>Nor04<br>Hen96<br>Gra06<br>RoP02</td><td>N = 1<br>N = 5, rms RV 0.3 km s<sup>-1</sup></td></tr><tr><td></td><td>1384.75<br>5004.94</td><td>2<br>3.1 ± 0.1</td><td>2.6 ± 0.9</td><td>110</td><td>0.311</td><td>-4.465</td><td>5911<br>5910<br>5963 ± 30</td><td>Des14</td><td>FEROS</td></tr><tr><td>TYC 6406-0180-1</td><td></td><td>-9.7</td><td>5.5 ± 1.2</td><td>30</td><td></td><td></td><td></td><td>SACY</td><td>N = 1</td></tr><tr><td>HIP 116910</td><td></td><td>11.1</td><td>31.1 ± 3.1</td><td>230</td><td></td><td>5567</td><td></td><td>SACY<br>DaS09</td><td>N = 4 rms 1.7 km s<sup>-1</sup></td></tr></tbody></table>

## Appendix B: Notes on individual objects

* **TYC 5839-0596-1:** (ASAS 001208-1550.5) The star is flagged as SB2 in SACY and we confirm this classification. Kiraga (2012) reports a photometric rotation period *P* = 2.532 d based on the ASAS photometry. We find two significant photometric periods, *P* = 1.644 d and *P* = 2.53 d, of comparable powers in almost all the seasonal Lomb-Scargle and Clean periodograms. The longer period is more consistent with *v sin i* = 18 km s⁻¹ and with the radius of a K0IV PMS subgiant. The period *P* = 1.644 d is an alias, specifically a beat period between the star’s rotation period and the ~1 d data sampling. This is a result of the rotation of the Earth and the fixed longitude of the observation site. The star has also a very large X-ray luminosity (log *L*<sub>X</sub>/L<sub>bol</sub> = -3.0). While we do not have the orbital period of the SB2, the similar *v sin i* of the two components suggests that this is a tidally locked system. The star also shows a moderately large lithium abundance, which is compatible with an age similar to the Pleiades. We are unable to conclude whether this is a true young binary or if the system is a RS CVn variable with a relatively large lithium abundance (see, e.g., Pallavicini et al. 1992). The photometric distance was obtained by assuming equal magnitudes for the components.

* **TYC 0603-0461-1 = BD +07 85:** (ASAS 003858+0829.0) New close visual binary from the NaCo-LP; Δ*H* = 0.10 mag at a projected separation of 74 mas, corresponding to 4.3 AU at the photometric distance after correction for binarity. It is kinematically consistent with the nearby, young population. We find three photometric periods: *P* = 3.60 d, *P* = 0.566 d, and *P* = 1.381 d. Although they are all significant, their relative power changes from season to season. We have no *v sin i* measurements, which with the *R* = 1.026 *R*<sub>☉</sub> stellar radius, could allow us to fix an upper value to the rotation period. The period *P* = 1.381 d is the most significant period also revealed by the Clean analysis and may be the stellar rotation period. However, the other periods cannot be ruled out. Considering the binarity and the small magnitude difference between the components, the multiple periodicities reported in the photometric analysis might be due to the different components.

* **HIP 3924 = HD 4944:** (ASAS 005024-6404.1; 1SWASP+J005024.31-640404.0) Our FEROS spectra indicate the presence of an additional component, which is more evident in

the red part of the spectrum. Binarity is further supported by the RV difference of about 9 km s⁻¹ between our RV and that measured by Wichmann et al. (2003). Therefore, the star is classified as SB2. We measured an RV difference of about 18 km s⁻¹ between the components with a line depth for the secondary that is about 30% that of the primary at 6450 Å. Our projected rotational velocity and Li EW are significantly different from those reported in the literature by Wichmann et al. (2003) and Weise et al. (2010). The first discrepancy might be due to a different RV separation between the components at the time of observation. For Li EW, our FEROS spectrum indicates that the two components have a similar lithium line depth. We find various significant photometric periodicities. Only one, *P* = 9.3 d, is consistent with *v sin i* = 8 km s⁻¹ and the stellar radius. It is found in the complete ASAS series as well as in one segment. As the primary is classified as F7, it is possible that the photometric period belongs to the secondary. No period is derived from the HIPPARCOS photometric data. Lithium and log *R*<sub>HK</sub> indicators are consistent with an age comparable to the Hyades, while X-ray emission yields younger ages than the other indicators. These discrepancies may be linked to the blending of the components. The target’s kinematics are only consistent with IC 2391 and with the nearby, young population. We adopt an age of 500 Myr, with a lower limit at the age of the IC 2391 MG.

* **HIP 6177 = HD 8049:** Moderately old star rejuvenated by stellar wind from the progenitor of its WD companion. The properties of the K dwarf and the WD companion and a description of the most probable evolution of the system are presented in Zurlo et al. (2013).

* **HIP 8038:** New close binary from the NaCo-LP (Δ*H* = 2.5 mag at 0.44 arcsec). There is also a wide companion, **HIP 8039**, which is 1.9 mag brighter and at a projected separation of 14.97 arcsec. This star was not observed as part of the NaCo-LP. All the components are included in the aperture photometry of ASAS and SuperWASP (referred to as ASAS 014314-2136.7 and 1SWASP+J014314.17-213656.5, respectively). Each season exhibits its own most significant period, which differs from season to season in both ASAS and SuperWASP data. The most likely period in SuperWASP seems to be *P* = 1.668 d but with a scattered phase light curve. No clear periodicity comes out from the Clean analysis or from the HIPPARCOS photometry.
As the wide companion HIP 8039 is 1.9 mag brighter, the tentative rotation period most likely belongs to the brighter component. The target's kinematics and age are only consistent with the young, nearby population.

HIP 10602 = HD 14228 = $\phi$ Eri (ASAS 021631–5130.7) Proposed in Torres et al. (2008) and Malo et al. (2013) as a high probability member of Tuc/Hor. Our analysis confirms that it has consistent kinematics, at the $\le 1.0$ sigma level, with the Tuc/Hor association and Gagné et al. (2014) tools also yield a very high membership probability. Torres et al. investigated color-magnitude diagram placement and found it to be consistent with Tuc/Hor membership. The star is quoted as a binary in Zuckerman & Song (2004) but the identification and properties of the companion are not provided. The candidate at about 90 arcsec ($\phi$ Eri B = CPD-52 284) is not physically associated, as reported in the Washington Double Star (WDS) catalog (Mason et al. 2013). This early-type star exhibits non-periodic photometric variability.

HIP 11360 = HD 15115 (ASAS 022616+0617.6). This F-type star's membership to the $\beta$ Pic MG was first proposed by Moór et al. (2006). Torres et al. (2008) concluded a possible membership (prob. 60%). Malo et al. (2013) instead propose that the star is a bona fide member of the Columba association. These estimates are based on the only RV measurement available in the literature previous to our work ($8.8 \pm 3.0$ km s$^{-1}$; Moór et al. 2006). Our RV determination ($1.7 \pm 1.0$ km s$^{-1}$), which includes eight HARPS and two FEROS spectra, has better accuracy and concludes a value quite different from the previously published one. Adopting our RV value, Malo et al. (2013) and Gagné et al. (2014) tools support a high membership probability (98%) for the Tuc/Hor association. The discrepancy between Moór et al. (2006) RV and our value is marginally significant (about two sigma). It might be due to the presence of a close companion. However, the high-precision differential RVs obtained with the SAFIR code applied to HARPS data show a dispersion of only 120 m/s over 40 days with intra-night RV and line bisector variations suggestive of pulsation occurrences. The age determination from indirect indicators is inconclusive, as expected for an F star. Both the young ages of the Tucana association and older ages, up to about 200 Myr, are compatible with the data. Verifying the true membership requires further investigation, including confirmation of the adopted RV value with longer baseline observations. The star exhibits non-periodic photometric variability. HIP 11360 hosts a debris disk that is unique for its large asymmetry, being detected out to 315 AU on the east side and more than 550 AU on the west side (Kalas et al. 2007). Rodigas et al. (2012) showed that the geometry is wavelength dependent and found indications of a gap in the disk at about 1 arcsec.

TYC 8484-1507-1 = HD 16699B This star is a new close visual binary from the NaCo-LP observations (sep. 0.06 arcsec = 3.6 AU, $\Delta H$ = 0.23 mag). SACY lists it as a possible SB. There is an additional component (HIP 12326 = HD 16699) at 8.7 arcsec, corresponding to a projected separation of 530 AU. According to Cutispoto et al. (1999), HD 16699 shows a composite spectrum, with one system of sharp lines and another system of broad lines superimposed. Since the RV is constant, this was interpreted as being due to a companion at moderately large separation. This would indicate a quadruple system. However, we note that the $v \sin i$ values of the two components in Cutispoto et al. (1999) are roughly exchanged with respect to other studies in the literature (Table A.1). An analysis of the CES spectra

used in Cutispoto et al. (1999) indicates that the components were indeed exchanged in the original study. In light of this, the new companion seen in the NaCo-LP is likely the same one appearing in the composite spectra by Cutispoto et al. (1999). The separation of a few AU is compatible with the lack of a measurable RV variation, given the short time baseline of the observations. Indeed, our FEROS spectrum of the primary does shows no indication of additional components, while a check of the spectra in the Torres et al. (2006) database confirms the composite nature of the secondary's spectrum. The two components of TYC 8484-1507-1 have similar magnitudes but very different $v \sin i$ values, pointing to an intrinsically large difference between their rotational velocities, or to a strong misalignment of their rotation axes, which would be unusual for such a close binary (Hale 1994). The two stars are indistinguishable by the ASAS photometry (ASAS 023844–5257.0). The blended light curve shows variability but exhibits no significant periodicity. The target's kinematics match only the IC 2391 open cluster, with a correspondence of $<2.0$ sigma. The target's sky position is inconsistent with confirmed IC 2391 members, which all lie around RA = 8 h. However, the system could be an outlier of the kinematic association of young stars that Torres et al. (2008) proposes to comprise IC 2391 and Argus. The age indicators are somewhat puzzling. The secondary has a lithium line above that of Pleiades stars with similar colors (which would be consistent with the possible association with Argus) while that of the primary is below. Ca II H and K emission is also much stronger in the secondary (as was seen in SACY spectra). The system is not resolved in the ROSAT All Sky catalog, but XMM observations clearly indicate that the X-ray emission is concentrated on TYC 8484-1507-1 (the close visual pair seen with NaCo). These differences are not easy to reconcile. The composite nature of TYC 8484-1507-1 might somewhat alter some of the parameters. The very young isochrone age derived by Moór et al. (2011; 12 Myr) for TYC 8484-1507-1 is due to this. After correcting the photometry for the flux of the new visual component, the star lies close to the main sequence. Considering these uncertainties, we adopt an age of 100 Myr, with a lower limit of 40 Myr and an upper limit of 500 Myr. The system has an additional very wide (216 arcsec = 13 000 AU projected separation) common proper motion star, HIP 12361 = HD 16743. Moór et al. (2011) measured for this star a similar RV to those of HD 16699 A and B, and noted a fully consistent trigonometric parallax. It is then likely that the stars form a quadruple system. As expected for an early F star, HIP 12361 provides little additional contribution to the determination of the age of the system. Isochrone age analyses yield an upper limit to stellar age of about 1.7 Gyr. Finally, HIP 12361 hosts a debris disk (Moór et al. 2011).

HIP 12394 = HD 16978 = $\epsilon$ Hyi (ASAS 023932–6816.1) Early type star, proposed as a member of Tuc/Hor by Torres et al. (2008) and Malo et al. (2013). Our kinematics analysis shows that its motion does indeed match ($<1.0$ sigma) those of the Tuc/Hor group in *U*, *V*, and *W* velocities, and BANYAN II on-line tool further supports membership. The star meets the age requirement of Torres et al. A small X-ray luminosity is derived from ROSAT. The star exhibits non-periodic photometric variability.

HIP 13008 = HD 17438 = HR 827 Fast-rotating mid-F star. It is a possible binary, based on the HIPPARCOS acceleration and the difference between the HIPPARCOS and the historical
proper motion (Makarov & Kaplan 2005). The fast rotation does not allow an accurate RV measurement, but the existent RVs and line profile analysis present no compelling evidence for binarity. The star was originally flagged as young because of the high level of chromospheric activity reported by Gray et al. (2006). However, our own measurement indicates a significantly lower value (log $R_{HK}$ = -4.64). Similar discrepancies between Gray et al. (2006) and other sources are observed for other F-type stars in our sample (HIP 35564, HIP 78747). These discrepancies might be due to the larger width of the spectral region used by Gray et al. (2006) to derive the S-Index (3 Å vs. the usual 1 Å). This may induce spurious effects for F-type stars due to their shallow Ca II H and K absorptions. HIP 13008 exhibits non-periodic photometric variability. A slightly sub-solar metallicity was reported from Strömgren photometry (Casagrande et al. 2011). The isochrone age is $1.288 \pm 0.912$ Gyr. The target's kinematics are consistent with the young, nearby population. We adopt the isochronal age, which is consistent with our activity measurement and kinematics.

HIP 14684 = HD 19668 = IS Eri (ASAS 030942–0934.8) Malo et al. (2013) propose this star to be a bona fide member of the AB Dor MG. The target's kinematics match the AB Dor group within the 2.0 sigma threshold; the BANYAN II online tool yields high membership probability, and age indicators support this assignment. The rotation period $P = 5.46$ d was discovered by Messina et al. (2010) and subsequently confirmed by Wright et al. (2011). There is no X-ray counterpart in the ROSAT all sky catalog. The closest source in the ROSAT Faint Source Catalog has an integration time significantly lower than the typical ones. This may be an indication of some instrumental issues that caused the non-validation of a source, as found for HD 61005 in Desidera et al. (2011). Therefore, we do not list in Table 11 any upper limit on X-ray luminosity. The effective temperature resulting from the spectral type quoted in Simbad and HIPPARCOS catalog (G0) is more than 500 K warmer than our photometric and spectroscopic ones. This is likely due to a wrong spectral classification. We adopt the revised classification (G8/K0V) by Meyer et al. (2006).

TYC 8060-1673-1 = CD-46 1064 (ASAS 033049–4555.9) Proposed as a 100% probability member of Tuc/Hor by Torres et al. (2008). Our kinematic analysis shows that it matches both the Tuc/Hor and TW Hydrae associations at the 1.0 sigma level in U, V, and W. The star's sky position and XYZ galactic distances are inconsistent with other known members of TWA. All the age indicators are consistent with an age younger than 100 Myr. Malo et al. (2013) and Gagné et al. (2014) Bayesian analysis tools predict a very high probability of Tuc/Hor membership at a distance of 43.5 pc. This predicted distance for membership is consistent with the photometric distance of 40.4 pc. The rotation period $P = 3.74$ d was discovered by Messina et al. (2010) from ASAS data and was subsequently confirmed by SuperWASP data (Messina et al. 2011) and by Kiraga (2012).

HIP 19775 = HD 26980 (ASAS 041423–3819.0) Proposed as a bona fide member of Columba by Torres et al. (2008) and Malo et al. (2013). The kinematic analysis shows that its UVW motion matches Columba at the <2.0 sigma level, and the BANYAN II on-line tool yields high membership probability. The ages from various youth indicators are also consistent with the age of Columba. Messina et al. (2010) reported a rotation period $P = 2.53$ d based on ASAS data. From the analysis of SuperWASP data, Messina et al. (2011)

found $P = 1.684$ d to be the most significant periodicity. Considering the $v \sin i = 13.9$ kms$^{-1}$ and the stellar radius $R = 1.015 R_⊙$, we infer rotation axis inclination values of $i = 43^\circ$ and $i = 27^\circ$, respectively. The observed maximum light curve amplitude up to $\Delta V = 0.07$ mag is compatible with both inclinations, although it is most consistent with the larger $i = 43^\circ$ value. This suggests $P = 2.53$ d as the more likely rotation period.

HIP 23316 = HD 32372 (ASAS 050052–4101.1; 1SWASP+J050051.86-410106.7) Proposed as a high-probability member of Columba by Torres et al. (2008) and Malo et al. (2013). Our kinematic analysis shows that its UVW motion matches Columba at the <2.0 sigma level, reinforcing the membership assignment, which is also confirmed by the Gagné et al. (2014) on line tool. Also, the ages from various youth indicators are consistent with the age of Columba. The most significant period we find in the SuperWASP data is $P = 2.183$ d. Another significant period is $P = 1.8$ d, which is the 1-d beat period of the $P = 2.183$ d rotation period. The ASAS data analysis does not provide any conclusion on the rotation period. The highest peak of the HIPPARCOS data periodogram is at $P = 17.8$ d, which coincides with the maximum of the window function.

HD 32981 = BD-16 1042 = TYC 5901-1109-1 Proposed as a 100% probability member of AB Dor by Torres et al. (2008). The kinematic analysis shows that its UVW motion matches AB Dor at the <1.0 sigma level. The age of the star from various youth indicators is also broadly consistent with the age of the AB Dor group. Malo et al. (2013) Bayesian analysis tools predict a 97% probability of AB Dor membership at a distance of 79 pc while Gagné et al. (2014) return a very low membership probability, as most of the proposed AB Dor members. The predicted distance for membership is roughly consistent with the photometric distance of 86.7 pc. Messina et al. (2010) found a rotation period $P = 0.985$ d.

BD–09 1108: (ASAS 051537–0930.8) Proposed as an 85% probability member of Tuc/Hor by Torres et al. (2008). The kinematic analysis shows that its UVW motion matches Tuc/Hor at the <2.0 sigma level, reinforcing the membership assignment. The age of the star from various youth indicators is also consistent with the age of the Tuc/Hor association. Malo et al. (2013) Bayesian analysis tools predict a 17% probability of Tuc/Hor membership and a 78% probability of Columba membership at distances of 80.5 pc and 74.0 pc respectively. These predicted distances for membership are both smaller than the photometric distance of 93.6 pc. Instead, the Gagné et al. (2014) on line tool returns a very low membership probability on both associations when our photometric distance is included while a 54% membership probability for Columba at a distance of 67 pc. Messina et al. (2010) found a rotation period $P = 2.72$ d, which was subsequently confirmed by Kiraga (2012).

HIP 25434 = HD 274197 This is the secondary of a wide binary system with the star HIP 25436 = HD 35996 being the primary. HIP 25436 is brighter by 0.8 mag in V band. The two components have a separation of about 12 arcsec. Using three epoch RV measurements (Desidera et al. 2006; Moór et al. 2013, and our CORALIE observations), we found that the primary is an SB. There is also additional evidence that one of the components is itself a binary. The slope of -0.070 deg/year for the position angle measured by HIPPARCOS is not compatible with the much smaller long term trend seen in the visual measurements (as derived by us from the individual measurements