# ROTATION-ACTIVITY CORRELATIONS IN K AND M DWARFS. I. STELLAR PARAMETERS AND COMPILATIONS OF v sin i AND P /sin i FOR A LARGE SAMPLE OF LATE-K AND M DWARFS

E. Houdebine, D. Mullan, F. Paletou, M. Gebran

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E. Houdebine, D. Mullan, F. Paletou, M. Gebran. ROTATION-ACTIVITY CORRELATIONS IN K AND M DWARFS. I. STELLAR PARAMETERS AND COMPILATIONS OF v sin i AND P /sin i FOR A LARGE SAMPLE OF LATE-K AND M DWARFS. The Astrophysical Journal Letters, 2016, 822 (2), pp.97. 10.3847/0004-637X/822/2/97. hal-02105951

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ROTATION–ACTIVITY CORRELATIONS IN K AND M DWARFS. I. STELLAR PARAMETERS AND COMPILATIONS OF $v \sin i$ AND $P/\sin i$ FOR A LARGE SAMPLE OF LATE-K AND M DWARFS*

E. R. HOUDEBINE<sup>1,2,3</sup>, D. J. MULLAN<sup>4</sup>, F. PALETOU<sup>2,3</sup>, AND M. GEBRAN<sup>5</sup>

<sup>1</sup> Armagh Observatory, College Hill, BT61 9DG Armagh, Northern Ireland

<sup>2</sup> Université de Toulouse, UPS-Observatoire Midi-Pyrénées, IRAP, Toulouse, France

<sup>3</sup> CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 av. E. Belin, F-31400 Toulouse, France; eric_houdebine@yahoo.fr

<sup>4</sup> Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA

<sup>5</sup> Department of Physics & Astronomy, Notre Dame University-Louaize, P.O. Box 72, Zouk Mikael, Lebanon

Received 2015 May 4; accepted 2016 March 17; published 2016 May 11

ABSTRACT

The reliable determination of rotation–activity correlations (RACs) depends on precise measurements of the following stellar parameters: $T_{\text{eff}}$, parallax, radius, metallicity, and rotational speed $v \sin i$. In this paper, our goal is to focus on the determination of these parameters for a sample of K and M dwarfs. In a future paper (Paper II), we will combine our rotational data with activity data in order to construct RACs. Here, we report on a determination of effective temperatures based on the $(R-I)_C$ color from the calibrations of Mann et al. and Kenyon & Hartmann for four samples of late-K, dM2, dM3, and dM4 stars. We also determine stellar parameters ($T_{\text{eff}}$, log(g), and [M/H]) using the principal component analysis–based inversion technique for a sample of 105 late-K dwarfs. We compile all effective temperatures from the literature for this sample. We determine empirical radius–[M/H] correlations in our stellar samples. This allows us to propose new effective temperatures, stellar radii, and metallicities for a large sample of 612 late-K and M dwarfs. Our mean radii agree well with those of Boyajian et al. We analyze HARPS and SOPHIE spectra of 105 late-K dwarfs, and we have detected $v \sin i$ in 92 stars. In combination with our previous $v \sin i$ measurements in M and K dwarfs, we now derive $P/\sin i$ measures for a sample of 418 K and M dwarfs. We investigate the distributions of $P/\sin i$, and we show that they are different from one spectral subtype to another at a 99.9% confidence level.

Key words: stars: fundamental parameters – stars: late-type – stars: rotation

1. INTRODUCTION

The determination of fundamental stellar parameters ($T_{\text{eff}}$, $R_*$, [M/H], and $v \sin i$), notably for nearby stars, are essential to many astrophysical studies. This is especially true for studies of rotation–activity correlations (RACs), which are studies of how various indices of magnetic activity (such as $R'_{HK}$ and $L_X$) vary as a function of the rotation period of the star. In this paper, we focus on quantities that are relevant to determining rotational properties, including $T_{\text{eff}}$, $R_*$, [M/H], and $v \sin i$. We shall postpone the discussion of activity indices to Paper II, when the RACs will be constructed.

Various techniques have been used in the past to derive values of $T_{\text{eff}}$ and [M/H]. Here we use two different approaches to determine these parameters in samples of late-K and M dwarfs. In the first approach, we use the principal component analysis (PCA)–based inversion technique of Paletou et al. (2015a) by applying it to the Na I resonance doublet in our K dwarf sample (105 stars). For this sample of K dwarfs, we also compiled all published values of $T_{\text{eff}}$ in the literature and further derived new values of $T_{\text{eff}}$ based on measurements of the $(R-I)_C$ color: our conversion from $(R-I)_C$ to $T_{\text{eff}}$ uses the extensive calibration of Kenyon & Hartmann (1995). We find good agreement between our values rederived from $(R-I)_C$ and the published values ($3\sigma \sim 70$ K).

In the second approach, for our M dwarf samples (M2, M3, and M4), we find that a tight correlation between $T_{\text{eff}}$ and $(R-I)_C$ exists among the recent measurements of Mann et al. (2015). It had been shown in the past that the $(R-I)_C$ color is a

good effective temperature diagnostic for M dwarfs (e.g., Leggett 1992), with a relatively low sensitivity on the metallicity (e.g., Ramirez & Melendez 2005). In an ongoing determination of $T_{\text{eff}}$ derived from $(R-I)_C$ for samples of M dwarfs ranging in spectral subtype from M2 to M7, E. R. Houdebine et al. (2016, in preparation) find a very good agreement with a compilation of all published values of $T_{\text{eff}}$ in the literature. Therefore, for our present samples of M2, M3, and M4 dwarfs, we have used the calibration of Mann et al. (2015) to determine $T_{\text{eff}}$.

Houdebine (2008, Paper VII) found a relatively tight correlation between [M/H] and $R_*$ in a sample of M2 dwarfs. [M/H] decreases with decreasing $R_*$ in normal dwarfs and subdwarfs, such that all subdwarfs have very low [M/H] and $R_*$. In the present paper, we perform extensive compilations of [M/H] from the literature and correlate [M/H] and $R_*$ for our samples of late-K, M3, and M4 dwarfs. This allows us to obtain values of [M/H] for all of our target stars. The determination of [M/H] will be essential when we eventually attempt to construct meaningful RACs for the Ca II line fluxes. The reason is that an ongoing non-LTE radiation transfer modeling study (E. R. Houdebine & P. M. Panagi 2016, in preparation) of the Ca II line formation as a function of the metallicity confirms that the Ca II line resonance doublet is not a good diagnostic of magnetic activity unless it is first corrected for the influence of metallicity.

As a preliminary to constructing RACs in K and M dwarfs, over the past several years we have reported improved spectroscopic measurements of rotational broadening $v \sin i$ in stars of spectral subtypes dK4 (Houdebine 2011a, Paper XVI thereafter), dK6 (present study), dM2 (Houdebine 2008, Paper VIII, Houdebine 2010a, Paper XIV), dM3

<footnote>* Based on observations available at Observatoire de Haute Provence and the European Southern Observatory databases and on Hipparcos parallax measurements.</footnote>
(Houdebine & Mullan 2015), and dM4 (Houdebine 2012a, Paper XVII). An important aspect of our v sin i measurements has to do with the use of the HARPS and SOPHIE spectrographs: these spectrographs are designed initially for exoplanet searches and are therefore very stable in wavelength in the long term (about 1 m s⁻¹ for HARPS). These data give us access to rotational velocities that are significantly smaller than in previous spectroscopic studies of K and M dwarfs. Because of the smallness of some of our v sin i values, we need to verify the precision of our data. We assess the uncertainties on our v sin i measurements in Section 5. We shall find that the uncertainties δv in v sin i may be as small as ±σ = 0.27 km s⁻¹ for v sin i < 1 km s⁻¹, ±σ = 0.32 km s⁻¹ for 1 < v sin i < 5 km s⁻¹, and ±σ = 0.60 km s⁻¹ for v sin i > 5 km s⁻¹.

The occurrence of such uncertainties imposes an upper limit P_max/sin i on the rotational period of stars that are accessible to our approach. For example, for stars near the transition to complete convection (TTCC), where R* ≈ 0.3–0.4 R⊙, we can in principle measure the rotation periods of TTCC stars with confidence only up to values of P_max/sin i = 2πR*/δv ~ 15–40 days. With a random distribution of inclinations, the average value of sin i is 2/π = 0.64. Therefore, the longest rotational periods P_max that we can hope to measure near the TTCC would be no greater than 10–26 days. For our sample of dK6 stars, where the average R* = 0.647 R⊙ (see Table 6), the upper limit on P_max/sin i is 33–66 days. Again correcting for sin i = 0.64, we find P_max for dK6 stars to be 21–42 days. Interestingly, these ranges in period overlap with the upper limit (about 30 days) that was obtained from early studies of rotational modulation in *Kepler* photometry (Nielsen et al. 2013). It is encouraging to find that by pushing spectroscopic studies of rotation to better limits, we can now study stars whose rotational periods would previously have been accessible only to photometric studies. To be sure, our approach is still subject to the sin i limitation, whereas this does not affect the photometric analysis.

In the present study, we report on a new analysis of high-resolution (HR) HARPS and SOPHIE spectra of 105 late-K dwarfs. We have detected v sin i in 92 of these stars. By combining these data with the analyses in our earlier papers, we now investigate the distributions of P/sin i for our samples of stars of spectral subtypes dK6, dM2, dM3, and dM4. In total, the present compilation of P/sin i measures includes measurements for 418 different K and M dwarfs. As already reported in Paper XVI and in Houdebine & Mullan (2015, hereafter HM), we confirm here that these distributions vary with spectral subtype: the distributions among dK6, dM2, dM3, and dM4 stars are statistically different from one another. These findings imply that in order to study RACs one must construct RACs separately for each different spectral subtype.

Our data confirm that the mean rotation periods of stars in the range dK4–dM4 in general decrease with decreasing effective temperature for slow rotators (HM). However, we also find that something unusual happens in the rotation rates between dM2 and dM4. The overall trend toward decreasing rotation period as we go from dK4 to dM4 is interrupted at spectral subtype dM3, where the period increases to a local peak where the rotational period is longer than the overall trend would have predicted (HM). When the investigation is extended (as in the present paper) to include fast rotators among the dK4–dM4 stars, one finds the following overall

trend: the mean rotation period tends to increase slightly from dK4 to dM4. But once again, at dM3, an exception is found: the mean rotation period of fast rotators at dM3 is locally significantly longer than the overall trend would have predicted (HM). HM interpreted the abnormally long rotation periods at subtype dM3 as possibly being associated with the occurrence of increasing coronal loop lengths (reported by Mullan et al. 2006). The mean rotation period of the slow rotators is an important constraint on the past evolution of the dynamo mechanisms and magnetic braking mechanisms (HM and this study).

The plan of this paper is as follows. In Section 2, we describe how the spectroscopic data were selected for a sample of late-K dwarfs. In Section 3, we describe how values of T<sub>eff</sub>, R<sub>*</sub>, and [M/H] have been extracted for our target stars, first for the K dwarfs, and then for the M dwarfs. In Section 4, we describe how a cross-correlation technique is used to determine the value of v sin i for our sample of dK6 stars using all spectral lines within a preferred band of the spectrum. Uncertainties in the values of v sin i for K and M dwarfs are discussed in Section 5. In Section 6, we present the distributions of P/sin i values for the stars of different spectral subtypes, and we discuss the statistical significance of differences between the distributions. Our conclusions are in Section 7.

We stress that the contents of Paper I are only a first step in a two-step process that aims to derive RACs for each spectral subtype. The second step in this process will be discussed in Paper II. The present paper focuses on obtaining reliable data for the “rotation” axis of the RAC. The subsequent paper will focus at first on obtaining reliable data for the “activity” axis of the RAC. Once reliable data are available for both axes, a search will then be undertaken (in Paper II) to determine if any significant correlation exists between rotation and activity for each spectral subtype.

## 2. SELECTION OF SPECTROSCOPIC DATA

Stepien (1989, 1993, 1994) has reported that RACs exhibit certain differences at different spectral types. As an extension of this finding, we have found in previous studies (Paper XVIII, HM) that it is important in constructing RACs to select samples of stars with T<sub>eff</sub> values that are confined within a narrow range. There are two principal reasons for this, one related to our analysis of chromospheric emission lines, and one related to the choice of an optimal set of photospheric absorption lines.

As regards chromospheric analysis, it is important to deal with stars with closely similar T<sub>eff</sub> when we are attempting to quantify with as much precision as possible the EW of the chromospheric lines (Ca II resonance doublet and Hα). These lines inevitably include some contributions from the background photospheric continuum and from the temperature minimum region (e.g., Houdebine & Doyle 1994; Cram & Mullan 1979; Houdebine & Stempels 1997, Paper XV). Initially, our samples of stars had been selected for the purpose of chromospheric modeling studies (e.g., Houdebine & Stempels 1997; Houdebine 2009b Paper XII, 2010b Paper IX), and in these studies the selection of stars with closely similar spectral types was essential in order to develop reliable grids of semiempirical model chromospheres, each of which would be superposed on a particular photospheric model.
<table><caption>Table 1
Stellar Parameters for Our Sample of Late-K Dwarfs and Computed [M/H] Values Derived from the [M/H]-Radius Correlation (See the Text)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub> or (B-V)<br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>T<sub>eff</sub>±σ<br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Distance<br>(pc)</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>R<sub>*</sub><sup>a</sup><br>(R<sub>☉</sub>)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>b</sup><br>(dex)</th></tr></thead><tbody><tr><td>GJ 1056</td><td>9.259</td><td>0.686</td><td>4230 ± 100</td><td>4365 ± 103</td><td>dK4.9</td><td>46.06 ± 1.08</td><td>21.7</td><td>7.576 ± 0.055</td><td>0.687 ± 0.061</td><td>0.660</td><td>...</td><td>-0.175</td></tr><tr><td>GJ 1066</td><td>8.847</td><td>0.680</td><td>4250 ± 100</td><td>4397 ± 107</td><td>dK4.8</td><td>56.31 ± 0.82</td><td>17.8</td><td>7.600 ± 0.036</td><td>0.667 ± 0.052</td><td>0.634</td><td>...</td><td>-0.215</td></tr><tr><td>GJ 1067</td><td>9.70</td><td>0.680</td><td>4250 ± 100</td><td>4385 ± 135</td><td>dK4.9</td><td>38.26 ± 1.27</td><td>26.1</td><td>7.614 ± 0.091</td><td>0.665 ± 0.071</td><td>0.634</td><td>...</td><td>-0.215</td></tr><tr><td>GJ 1177A</td><td>8.94</td><td>0.731</td><td>4130 ± 100</td><td>4260 ± 130</td><td>PMS K5.6</td><td>69.01 ± 1.35</td><td>14.5</td><td>8.135 ± 0.062</td><td>0.576 ± 0.055</td><td>0.569</td><td>...</td><td>-0.471</td></tr><tr><td>GJ 1213</td><td>10.18</td><td>0.781</td><td>4030 ± 100</td><td>4155 ± 125</td><td>dK6.4</td><td>39.64 ± 1.14</td><td>25.2</td><td>8.171 ± 0.082</td><td>0.624 ± 0.072</td><td>0.634</td><td>...</td><td>-0.236</td></tr><tr><td>GJ 1248</td><td>12.99</td><td>0.790</td><td>4010 ± 100</td><td>4010 ± 100</td><td>sdK7.3</td><td>80.2 ± 4.3</td><td>12.5</td><td>12.51 ± 0.13</td><td>0.090 ± 0.012</td><td>0.140</td><td>...</td><td>...</td></tr><tr><td>GJ 1267</td><td>8.992</td><td>0.800</td><td>4000 ± 100</td><td>4107 ± 117</td><td>dK6.7</td><td>73.90 ± 1.21</td><td>13.5</td><td>8.335 ± 0.040</td><td>0.606 ± 0.058</td><td>0.629</td><td>...</td><td>-0.225</td></tr><tr><td>GJ 1279</td><td>8.39</td><td>0.686</td><td>4230 ± 100</td><td>4397 ± 121</td><td>dK4.8</td><td>66.74 ± 0.83</td><td>15.0</td><td>7.512 ± 0.047</td><td>0.697 ± 0.059</td><td>0.664</td><td>-0.10</td><td>-0.169</td></tr><tr><td>GJ 3072</td><td>9.993</td><td>0.778</td><td>4030 ± 100</td><td>4070 ± 40</td><td>dK6.9</td><td>49.06 ± 1.88</td><td>20.4</td><td>8.447 ± 0.086</td><td>0.571 ± 0.068</td><td>0.604</td><td>...</td><td>-0.319</td></tr><tr><td>GJ 3411</td><td>10.16</td><td>0.731</td><td>4130 ± 100</td><td>4130 ± 100</td><td>dK6.5</td><td>36.32 ± 1.65</td><td>27.5</td><td>7.961 ± 0.116</td><td>0.664 ± 0.083</td><td>0.683</td><td>...</td><td>-0.169</td></tr><tr><td>GJ 3494</td><td>9.748</td><td>0.740</td><td>4110 ± 100</td><td>4290 ± 180</td><td>dK5.4</td><td>41.22 ± 1.74</td><td>24.3</td><td>7.824 ± 0.094</td><td>0.660 ± 0.074</td><td>0.648</td><td>+0.71</td><td>-0.192</td></tr><tr><td>GJ 3551</td><td>9.531</td><td>0.728</td><td>4140 ± 100</td><td>4239 ± 71</td><td>dK5.8</td><td>43.13 ± 1.04</td><td>23.2</td><td>7.705 ± 0.057</td><td>0.708 ± 0.066</td><td>0.705</td><td>-0.40</td><td>-0.139</td></tr><tr><td>GJ 3996</td><td>10.333</td><td>0.812</td><td>3980 ± 100</td><td>4088 ± 110</td><td>dK6.8</td><td>36.73 ± 1.84</td><td>27.2</td><td>8.158 ± 0.12</td><td>0.673 ± 0.092</td><td>0.701</td><td>-0.11</td><td>-0.140</td></tr><tr><td>GJ 4140</td><td>10.168</td><td>0.812</td><td>3980 ± 100</td><td>4143 ± 117</td><td>dK6.4</td><td>49.33 ± 1.46</td><td>20.3</td><td>8.634 ± 0.068</td><td>0.526 ± 0.057</td><td>0.542</td><td>+0.42</td><td>-0.583</td></tr><tr><td>GJ 9073B</td><td>10.49</td><td>0.719</td><td>4160 ± 100</td><td>4160 ± 100</td><td>dK6.3</td><td>32 ± 4</td><td>31.3</td><td>8.016 ± 0.276</td><td>0.632 ± 0.133</td><td>0.645</td><td>...</td><td>-0.196</td></tr><tr><td>GJ 9250</td><td>10.14</td><td>0.719</td><td>4160 ± 100</td><td>4268 ± 107</td><td>dK5.6</td><td>34.17 ± 1.89</td><td>29.3</td><td>7.808 ± 0.137</td><td>0.661 ± 0.089</td><td>0.653</td><td>...</td><td>-0.185</td></tr><tr><td>GJ 9299</td><td>9.742</td><td>0.728</td><td>4140 ± 100</td><td>4259 ± 93</td><td>dK5.6</td><td>41.24 ± 1.46</td><td>24.2</td><td>7.819 ± 0.080</td><td>0.665 ± 0.070</td><td>0.659</td><td>+0.15</td><td>-0.176</td></tr><tr><td>GJ 9667</td><td>9.958</td><td>0.698</td><td>4210 ± 100</td><td>4210 ± 100</td><td>dK6.0</td><td>43.28 ± 1.64</td><td>23.1</td><td>8.139 ± 0.086</td><td>0.575 ± 0.061</td><td>0.578</td><td>...</td><td>-0.433</td></tr><tr><td>GJ 9714</td><td>9.326</td><td>0.728</td><td>4140 ± 100</td><td>4333 ± 148</td><td>dK5.1</td><td>49.23 ± 1.45</td><td>20.3</td><td>7.787 ± 0.068</td><td>0.652 ± 0.064</td><td>0.631</td><td>+0.10</td><td>-0.221</td></tr><tr><td>GJ 9827</td><td>10.39</td><td>0.716</td><td>4170 ± 100</td><td>4220 ± 50</td><td>dK5.9</td><td>32.98 ± 1.78</td><td>30.3</td><td>7.981 ± 0.13</td><td>0.623 ± 0.082</td><td>0.624</td><td>...</td><td>-0.236</td></tr><tr><td>Gl 14</td><td>9.00</td><td>0.812</td><td>3980 ± 100</td><td>4175 ± 195</td><td>dK6.2</td><td>66.65 ± 0.91</td><td>15.0</td><td>8.119 ± 0.049</td><td>0.657 ± 0.065</td><td>0.667</td><td>...</td><td>-0.165</td></tr><tr><td>Gl 40A</td><td>8.930</td><td>0.702</td><td>4200 ± 100</td><td>4284 ± 85</td><td>dK5.5</td><td>63.96 ± 1.07</td><td>15.6</td><td>7.960 ± 0.041</td><td>0.604 ± 0.051</td><td>0.593</td><td>-0.61</td><td>-0.365</td></tr><tr><td>Gl 45</td><td>9.482</td><td>0.696</td><td>4210 ± 100</td><td>4252 ± 62</td><td>dK5.7</td><td>50.87 ± 0.98</td><td>19.7</td><td>8.014 ± 0.047</td><td>0.596 ± 0.051</td><td>0.591</td><td>+0.00</td><td>-0.375</td></tr><tr><td>Gl 50</td><td>10.47</td><td>0.684</td><td>4240 ± 100</td><td>4240 ± 100</td><td>dK5.8</td><td>30.55 ± 1.79</td><td>32.7</td><td>7.895 ± 0.31</td><td>0.628 ± 0.142</td><td>0.625</td><td>+0.56</td><td>-0.232</td></tr><tr><td>Gl 52</td><td>8.97</td><td>0.740</td><td>4110 ± 100</td><td>4195 ± 85</td><td>dK6.1</td><td>66.97 ± 1.31</td><td>14.9</td><td>8.099 ± 0.062</td><td>0.608 ± 0.059</td><td>0.614</td><td>...</td><td>-0.278</td></tr><tr><td>Gl 57</td><td>10.130</td><td>0.874</td><td>3906 ± 100</td><td>4040 ± 90</td><td>dK7.1</td><td>59.86 ± 1.54</td><td>16.7</td><td>9.016 ± 0.060</td><td>0.411 ± 0.039</td><td>0.448</td><td>...</td><td>-1.514</td></tr><tr><td>Gl 105.5</td><td>9.509</td><td>0.680</td><td>4250 ± 100</td><td>4250 ± 100</td><td>dK5.7</td><td>42.91 ± 1.47</td><td>23.3</td><td>7.672 ± 0.078</td><td>0.692 ± 0.070</td><td>0.687</td><td>...</td><td>-0.149</td></tr><tr><td>Gl 112.1</td><td>8.574</td><td>0.664</td><td>4280 ± 100</td><td>4224 ± 56</td><td>dK5.8</td><td>62.46 ± 1.37</td><td>16.0</td><td>7.552 ± 0.052</td><td>0.731 ± 0.065</td><td>0.731</td><td>...</td><td>-0.128</td></tr><tr><td>Gl 116</td><td>9.608</td><td>0.725</td><td>4150 ± 100</td><td>4100 ± 50</td><td>sdK6.7</td><td>68.47 ± 1.43</td><td>14.6</td><td>8.786 ± 0.049</td><td>0.459 ± 0.042</td><td>0.484</td><td>...</td><td>-1.100</td></tr><tr><td>Gl 123</td><td>9.055</td><td>0.783</td><td>4020 ± 100</td><td>4065 ± 45</td><td>dK7.0</td><td>66.94 ± 1.94</td><td>14.9</td><td>8.183 ± 0.067</td><td>0.650 ± 0.071</td><td>0.685</td><td>...</td><td>-0.150</td></tr><tr><td>Gl 142</td><td>8.367</td><td>0.752</td><td>4080 ± 100</td><td>4127 ± 47</td><td>dK6.5</td><td>80.04 ± 0.99</td><td>12.5</td><td>7.884 ± 0.032</td><td>0.700 ± 0.058</td><td>0.719</td><td>...</td><td>-0.133</td></tr><tr><td>Gl 143.1</td><td>9.991</td><td>0.799</td><td>4000 ± 100</td><td>4070 ± 113</td><td>dK6.9</td><td>45.28 ± 1.97</td><td>22.1</td><td>8.271 ± 0.097</td><td>0.634 ± 0.079</td><td>0.667</td><td>+0.45</td><td>-0.165</td></tr><tr><td>Gl 146</td><td>8.60</td><td>0.725</td><td>4150 ± 100</td><td>4220 ± 50</td><td>dK5.9</td><td>73.49 ± 0.71</td><td>13.6</td><td>7.931 ± 0.041</td><td>0.642 ± 0.055</td><td>0.643</td><td>+0.38</td><td>-0.199</td></tr><tr><td>Gl 153A</td><td>9.35</td><td>0.728</td><td>4140 ± 100</td><td>4245 ± 105</td><td>dK5.7</td><td>57.68 ± 3.06</td><td>17.3</td><td>8.155 ± 0.13</td><td>0.574 ± 0.075</td><td>0.570</td><td>...</td><td>-0.467</td></tr><tr><td>Gl 156</td><td>9.015</td><td>0.750</td><td>4080 ± 100</td><td>4135 ± 55</td><td>dK6.5</td><td>64.24 ± 1.08</td><td>15.6</td><td>8.054 ± 0.041</td><td>0.644 ± 0.056</td><td>0.662</td><td>...</td><td>-0.172</td></tr><tr><td>Gl 162.2</td><td>9.72</td><td>0.692</td><td>4220 ± 100</td><td>4377 ± 111</td><td>dK4.9</td><td>38.53 ± 0.83</td><td>26.0</td><td>7.649 ± 0.066</td><td>0.664 ± 0.062</td><td>0.635</td><td>...</td><td>-0.213</td></tr><tr><td>Gl 182</td><td>10.107</td><td>1.37</td><td>4073 ± 100</td><td>4073 ± 100</td><td>PMS K7</td><td>38.64 ± 2.54</td><td>25.9</td><td>8.042 ± 0.14</td><td>0.946 ± 0.109</td><td>0.978</td><td>...</td><td>-0.002</td></tr><tr><td>Gl 186A</td><td>10.02</td><td>0.744</td><td>4100 ± 100</td><td>4244 ± 102</td><td>dK5.7</td><td>40.23 ± 2.08</td><td>24.9</td><td>8.046 ± 0.13</td><td>0.611 ± 0.080</td><td>0.607</td><td>+0.09</td><td>-0.307</td></tr><tr><td>Gl 186B</td><td>10.02</td><td>0.744</td><td>4100 ± 100</td><td>4244 ± 102</td><td>dK5.7</td><td>40.23 ± 2.08</td><td>24.9</td><td>8.046 ± 0.13</td><td>0.611 ± 0.080</td><td>0.607</td><td>+0.09</td><td>-0.307</td></tr><tr><td>Gl 208</td><td>8.841</td><td>0.801</td><td>3990 ± 100</td><td>4055 ± 65</td><td>dK7.0(e)</td><td>88.97 ± 1.02</td><td>11.2</td><td>8.587 ± 0.030</td><td>0.554 ± 0.050</td><td>0.591</td><td>+0.01</td><td>-0.375</td></tr><tr><td>Gl 221</td><td>9.693</td><td>0.744</td><td>4100 ± 100</td><td>4134 ± 34</td><td>dK6.5</td><td>49.23 ± 1.65</td><td>20.3</td><td>8.154 ± 0.077</td><td>0.613 ± 0.064</td><td>0.631</td><td>+0.19</td><td>-0.221</td></tr><tr><td>Gl 226.2</td><td>9.75</td><td>0.645</td><td>4320 ± 100</td><td>4357 ± 37</td><td>dK5.0</td><td>40.87 ± 1.85</td><td>24.5</td><td>7.807 ± 0.116</td><td>0.603 ± 0.072</td><td>0.577</td><td>...</td><td>-0.438</td></tr><tr><td>Gl 249</td><td>8.96</td><td>0.657</td><td>4294 ± 100</td><td>4321 ± 27</td><td>dK5.2</td><td>53.89 ± 0.98</td><td>18.6</td><td>7.618 ± 0.059</td><td>0.675 ± 0.061</td><td>0.656</td><td>...</td><td>-0.180</td></tr><tr><td>Gl 256</td><td>9.157</td><td>0.645</td><td>4320 ± 100</td><td>4361 ± 41</td><td>dK5.0</td><td>46.08 ± 1.23</td><td>21.7</td><td>7.475 ± 0.062</td><td>0.702 ± 0.065</td><td>0.676</td><td>...</td><td>-0.156</td></tr><tr><td>Gl 296</td><td>9.65</td><td>0.765</td><td>4050 ± 100</td><td>4044 ± 7</td><td>dK7.1</td><td>51.00 ± 8.00</td><td>19.6</td><td>8.188 ± 0.336</td><td>0.642 ± 0.164</td><td>0.683</td><td>...</td><td>-0.152</td></tr><tr><td>Gl 322</td><td>9.28</td><td>0.764</td><td>4050 ± 100</td><td>4260 ± 210</td><td>dK5.6</td><td>60.46 ± 1.36</td><td>16.5</td><td>8.187 ± 0.069</td><td>0.578 ± 0.062</td><td>0.571</td><td>...</td><td>-0.463</td></tr><tr><td>Gl 369</td><td>10.016</td><td>0.780</td><td>3800 ± 100</td><td>3866 ± 66</td><td>sdM1</td><td>82.92 ± 1.82</td><td>12.1</td><td>9.609 ± 0.052</td><td>0.371 ± 0.039</td><td>0.463</td><td>...</td><td>-1.341</td></tr></tbody></table>
<table><caption>Table 1
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub> or (B-V)<br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>T<sub>eff</sub>±σ<br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Distance<br>(pc)</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>R<sub>*</sub><sup>a</sup><br>(R<sub>☉</sub>)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>b</sup><br>(dex)</th></tr></thead><tbody><tr><td>Gl 389.1</td><td>9.99</td><td>0.692</td><td>4220 ± 100</td><td>4220 ± 188</td><td>dK5.9</td><td>36.54 ± 2.16</td><td>27.4</td><td>7.804 ± 0.14</td><td>0.664 ± 0.089</td><td>0.665</td><td>...</td><td>-0.168</td></tr><tr><td>Gl 397</td><td>8.83</td><td>0.743</td><td>4100 ± 100</td><td>4140 ± 40</td><td>dK6.4</td><td>63.55 ± 1.09</td><td>15.7</td><td>7.846 ± 0.057</td><td>0.717 ± 0.068</td><td>0.734</td><td>...</td><td>-0.126</td></tr><tr><td>Gl 401</td><td>11.02</td><td>0.775</td><td>3810 ± 100</td><td>3810 ± 100</td><td>sdM1</td><td>49.95 ± 2.26</td><td>20.0</td><td>9.513 ± 0.12</td><td>0.392 ± 0.051</td><td>0.500</td><td>...</td><td>-0.916</td></tr><tr><td>Gl 412.3A</td><td>9.34</td><td>0.695</td><td>4220 ± 100</td><td>4263 ± 76</td><td>dK5.6</td><td>35.46 ± 2.84</td><td>28.2</td><td>7.842 ± 0.19</td><td>0.641 ± 0.102</td><td>0.634</td><td>...</td><td>-0.215</td></tr><tr><td>Gl 412.3B</td><td>9.34</td><td>0.695</td><td>4220 ± 100</td><td>4263 ± 76</td><td>dK5.6</td><td>35.46 ± 2.84</td><td>28.2</td><td>7.842 ± 0.19</td><td>0.641 ± 0.102</td><td>0.634</td><td>...</td><td>-0.215</td></tr><tr><td>Gl 414A</td><td>8.34</td><td>0.776</td><td>4030 ± 100</td><td>4185 ± 155</td><td>dK6.1</td><td>87.23 ± 0.86</td><td>11.5</td><td>8.043 ± 0.042</td><td>0.649 ± 0.062</td><td>0.660</td><td>...</td><td>-0.175</td></tr><tr><td>Gl 416</td><td>9.038</td><td>0.706</td><td>4190 ± 100</td><td>4330 ± 140</td><td>dK5.1</td><td>46.36 ± 1.31</td><td>21.6</td><td>7.369 ± 0.065</td><td>0.778 ± 0.075</td><td>0.758</td><td>...</td><td>-0.116</td></tr><tr><td>Gl 421B</td><td>10.01</td><td>0.788</td><td>4020 ± 100</td><td>4030 ± 69</td><td>sdK7.1</td><td>62.53 ± 29.8</td><td>16.0</td><td>8.990 ± 0.87</td><td>0.459 ± 0.278</td><td>0.504</td><td>-1.50</td><td>-0.870</td></tr><tr><td>Gl 425B</td><td>8.61</td><td>0.820</td><td>3960 ± 100</td><td>4227 ± 192</td><td>dK5.8</td><td>63.5 ± 8.2</td><td>15.7</td><td>7.624 ± 0.28</td><td>0.812 ± 0.180</td><td>0.812</td><td>+0.19</td><td>-0.093</td></tr><tr><td>Gl 455.1</td><td>10.016</td><td>0.751</td><td>4082 ± 100</td><td>4172 ± 90</td><td>dK6.2</td><td>45.45 ± 1.39</td><td>22.0</td><td>8.304 ± 0.070</td><td>0.564 ± 0.057</td><td>0.575</td><td>...</td><td>-0.446</td></tr><tr><td>Gl 466</td><td>10.38</td><td>0.686</td><td>4230 ± 100</td><td>4230 ± 100</td><td>dK5.8</td><td>26.74 ± 2.27</td><td>37.4</td><td>7.516 ± 0.20</td><td>0.751 ± 0.124</td><td>0.750</td><td>...</td><td>-0.120</td></tr><tr><td>Gl 496.1</td><td>9.057</td><td>0.783</td><td>4020 ± 100</td><td>4040 ± 20</td><td>dK7.1</td><td>63.03 ± 1.36</td><td>15.9</td><td>8.055 ± 0.051</td><td>0.698 ± 0.071</td><td>0.740</td><td>-0.11</td><td>-0.124</td></tr><tr><td>Gl 509.1</td><td>9.74</td><td>0.764</td><td>4050 ± 100</td><td>4275 ± 225</td><td>dK5.5</td><td>40.35 ± 1.10</td><td>24.8</td><td>7.769 ± 0.078</td><td>0.696 ± 0.078</td><td>0.686</td><td>...</td><td>-0.150</td></tr><tr><td>Gl 517</td><td>9.348</td><td>0.722</td><td>4510 ± 100</td><td>4510 ± 100</td><td>dK4.4e</td><td>49.48 ± 0.72</td><td>20.2</td><td>7.820 ± 0.037</td><td>0.588 ± 0.046</td><td>0.552</td><td>-0.11</td><td>-0.542</td></tr><tr><td>Gl 522</td><td>9.710</td><td>0.712</td><td>4180 ± 100</td><td>4220 ± 40</td><td>dK5.9</td><td>42.30 ± 1.48</td><td>23.6</td><td>7.842 ± 0.079</td><td>0.662 ± 0.069</td><td>0.663</td><td>-0.22</td><td>-0.170</td></tr><tr><td>Gl 524.1</td><td>10.480</td><td>0.742</td><td>4100 ± 100</td><td>4275 ± 193</td><td>dK5.5</td><td>39.84 ± 1.97</td><td>25.1</td><td>8.482 ± 0.11</td><td>0.492 ± 0.059</td><td>0.482</td><td>-0.22</td><td>-1.123</td></tr><tr><td>Gl 542.2</td><td>9.112</td><td>0.711</td><td>4180 ± 100</td><td>4296 ± 89</td><td>dK5.4</td><td>45.97 ± 1.59</td><td>21.8</td><td>7.424 ± 0.079</td><td>0.774 ± 0.080</td><td>0.760</td><td>...</td><td>-0.115</td></tr><tr><td>Gl 546</td><td>8.610</td><td>0.716</td><td>4170 ± 100</td><td>4320 ± 150</td><td>dK5.2</td><td>69.70 ± 0.82</td><td>14.3</td><td>7.826 ± 0.031</td><td>0.638 ± 0.051</td><td>0.620</td><td>...</td><td>-0.253</td></tr><tr><td>Gl 558</td><td>9.58</td><td>0.740</td><td>4110 ± 100</td><td>4250 ± 140</td><td>dK5.7</td><td>49.43 ± 1.07</td><td>20.2</td><td>8.050 ± 0.066</td><td>0.606 ± 0.059</td><td>0.601</td><td>...</td><td>-0.332</td></tr><tr><td>Gl 562</td><td>9.23</td><td>0.716</td><td>4170 ± 100</td><td>4285 ± 115</td><td>dK5.4</td><td>65.8 ± 7.2</td><td>15.2</td><td>8.321 ± 0.25</td><td>0.517 ± 0.100</td><td>0.505</td><td>...</td><td>-0.862</td></tr><tr><td>Gl 570.2</td><td>11.110</td><td>0.806</td><td>3990 ± 100</td><td>3987 ± 3</td><td>dK7.4</td><td>25.76 ± 4.32</td><td>38.8</td><td>8.165 ± 0.342</td><td>0.700 ± 0.182</td><td>0.757</td><td>...</td><td>-0.117</td></tr><tr><td>Gl 571</td><td>10.14</td><td>0.716</td><td>4170 ± 100</td><td>4170 ± 100</td><td>dK6.2</td><td>40.79 ± 1.47</td><td>24.5</td><td>8.193 ± 0.097</td><td>0.579 ± 0.065</td><td>0.590</td><td>...</td><td>-0.380</td></tr><tr><td>Gl 571.1</td><td>9.472</td><td>0.805</td><td>3990 ± 100</td><td>4076 ± 69</td><td>dK6.9</td><td>51.70 ± 1.97</td><td>19.3</td><td>8.039 ± 0.087</td><td>0.708 ± 0.085</td><td>0.739</td><td>+0.37</td><td>-0.124</td></tr><tr><td>Gl 576</td><td>9.815</td><td>0.748</td><td>4090 ± 100</td><td>4197 ± 107</td><td>dK6.1</td><td>53.80 ± 2.80</td><td>18.6</td><td>8.469 ± 0.115</td><td>0.516 ± 0.064</td><td>0.522</td><td>...</td><td>-0.734</td></tr><tr><td>Gl 583</td><td>9.459</td><td>0.721</td><td>4160 ± 100</td><td>4213 ± 41</td><td>dK5.9</td><td>52.92 ± 1.60</td><td>18.9</td><td>8.077 ± 0.070</td><td>0.600 ± 0.060</td><td>0.603</td><td>+0.37</td><td>-0.324</td></tr><tr><td>Gl 585.1</td><td>10.23</td><td>0.743</td><td>4100 ± 100</td><td>4152 ± 52</td><td>dK6.4</td><td>37.96 ± 1.90</td><td>26.3</td><td>8.127 ± 0.126</td><td>0.614 ± 0.080</td><td>0.628</td><td>...</td><td>-0.227</td></tr><tr><td>Gl 619</td><td>8.98</td><td>0.746</td><td>4090 ± 100</td><td>4205 ± 115</td><td>dK6.0</td><td>63.62 ± 0.73</td><td>15.7</td><td>7.998 ± 0.045</td><td>0.637 ± 0.056</td><td>0.641</td><td>...</td><td>-0.202</td></tr><tr><td>Gl 626</td><td>8.85</td><td>0.651</td><td>4306 ± 100</td><td>4306 ± 100</td><td>dK5.3</td><td>57.08 ± 1.26</td><td>17.5</td><td>7.632 ± 0.067</td><td>0.672 ± 0.064</td><td>0.656</td><td>...</td><td>-0.180</td></tr><tr><td>Gl 629.1</td><td>10.53</td><td>0.754</td><td>4080 ± 100</td><td>4120 ± 40</td><td>dK6.6</td><td>30.53 ± 2.51</td><td>32.8</td><td>7.954 ± 0.19</td><td>0.681 ± 0.112</td><td>0.702</td><td>...</td><td>-0.140</td></tr><tr><td>Gl 659B</td><td>9.36</td><td>0.645</td><td>4320 ± 100</td><td>4378 ± 58</td><td>dK4.9</td><td>49.46 ± 4.03</td><td>20.2</td><td>7.831 ± 0.190</td><td>0.591 ± 0.093</td><td>0.573</td><td>...</td><td>-0.454</td></tr><tr><td>Gl 673</td><td>7.530</td><td>0.760</td><td>4060 ± 100</td><td>4078 ± 18</td><td>dK6.9</td><td>129.86 ± 0.73</td><td>7.70</td><td>8.097 ± 0.017</td><td>0.654 ± 0.049</td><td>0.685</td><td>...</td><td>-0.150</td></tr><tr><td>Gl 707</td><td>8.372</td><td>0.675</td><td>4260 ± 100</td><td>4267 ± 106</td><td>dK5.6</td><td>76.31 ± 1.06</td><td>13.1</td><td>7.785 ± 0.035</td><td>0.648 ± 0.052</td><td>0.640</td><td>+0.34</td><td>-0.204</td></tr><tr><td>Gl 708</td><td>10.020</td><td>0.694</td><td>4220 ± 100</td><td>4232 ± 12</td><td>dK5.8</td><td>34.05 ± 1.76</td><td>29.4</td><td>7.681 ± 0.114</td><td>0.700 ± 0.084</td><td>0.699</td><td>...</td><td>-0.142</td></tr><tr><td>Gl 710</td><td>9.660</td><td>0.755</td><td>4070 ± 100</td><td>4120 ± 37</td><td>dK6.6</td><td>51.12 ± 1.63</td><td>19.6</td><td>8.203 ± 0.073</td><td>0.608 ± 0.063</td><td>0.629</td><td>+0.00</td><td>-0.225</td></tr><tr><td>Gl 726</td><td>8.810</td><td>0.700</td><td>4210 ± 100</td><td>4270 ± 60</td><td>dK5.6</td><td>70.04 ± 1.17</td><td>14.3</td><td>8.037 ± 0.041</td><td>0.586 ± 0.048</td><td>0.577</td><td>-0.97</td><td>-0.437</td></tr><tr><td>Gl 728</td><td>9.155</td><td>0.776</td><td>4030 ± 100</td><td>4100 ± 70</td><td>dK6.7</td><td>58.82 ± 1.34</td><td>17.0</td><td>8.003 ± 0.054</td><td>0.689 ± 0.071</td><td>0.714</td><td>...</td><td>-0.135</td></tr><tr><td>Gl 747.2</td><td>9.73</td><td>0.743</td><td>4100 ± 100</td><td>4141 ± 41</td><td>dK6.4</td><td>33.35 ± 1.16</td><td>30.0</td><td>7.345 ± 0.094</td><td>0.885 ± 0.101</td><td>0.902</td><td>...</td><td>-0.005</td></tr><tr><td>Gl 747.3</td><td>9.342</td><td>0.730</td><td>4130 ± 100</td><td>4203 ± 70</td><td>dK6.0</td><td>48.59 ± 1.53</td><td>20.6</td><td>7.775 ± 0.072</td><td>0.698 ± 0.071</td><td>0.702</td><td>+0.33</td><td>-0.140</td></tr><tr><td>Gl 757</td><td>10.95</td><td>0.802</td><td>3990 ± 100</td><td>4069 ± 97</td><td>sdK6.9</td><td>34.11 ± 2.11</td><td>29.3</td><td>8.614 ± 0.15</td><td>0.544 ± 0.083</td><td>0.577</td><td>...</td><td>-0.437</td></tr><tr><td>Gl 763</td><td>9.326</td><td>0.790</td><td>4010 ± 100</td><td>4065 ± 55</td><td>sdK7.0</td><td>69.32 ± 1.55</td><td>14.4</td><td>8.530 ± 0.053</td><td>0.559 ± 0.057</td><td>0.594</td><td>...</td><td>-0.361</td></tr><tr><td>Gl 773</td><td>9.285</td><td>0.737</td><td>4115 ± 100</td><td>4288 ± 173</td><td>dK5.4</td><td>53.54 ± 1.29</td><td>18.7</td><td>7.928 ± 0.057</td><td>0.628 ± 0.058</td><td>0.616</td><td>...</td><td>-0.269</td></tr><tr><td>Gl 782</td><td>8.890</td><td>0.691</td><td>4220 ± 100</td><td>4332 ± 80</td><td>dK5.1</td><td>64.04 ± 1.50</td><td>15.6</td><td>7.922 ± 0.056</td><td>0.597 ± 0.053</td><td>0.576</td><td>-0.88</td><td>-0.442</td></tr><tr><td>Gl 786.1</td><td>10.16</td><td>0.800</td><td>4000 ± 100</td><td>4140 ± 140</td><td>dK6.4</td><td>40.58 ± 1.10</td><td>24.6</td><td>8.202 ± 0.079</td><td>0.634 ± 0.073</td><td>0.651</td><td>...</td><td>-0.187</td></tr><tr><td>Gl 795A</td><td>9.348</td><td>0.707</td><td>4190 ± 100</td><td>4190 ± 100</td><td>dK6.1</td><td>59.80 ± 3.42</td><td>16.7</td><td>8.232 ± 0.13</td><td>0.559 ± 0.072</td><td>0.566</td><td>...</td><td>-0.484</td></tr><tr><td>Gl 795B</td><td>9.348</td><td>0.707</td><td>4190 ± 100</td><td>4190 ± 100</td><td>dK6.1</td><td>59.80 ± 3.42</td><td>16.7</td><td>8.232 ± 0.13</td><td>0.559 ± 0.072</td><td>0.566</td><td>...</td><td>-0.484</td></tr><tr><td>Gl 798</td><td>8.82</td><td>0.748</td><td>4090 ± 100</td><td>4135 ± 120</td><td>dK6.5</td><td>82.31 ± 1.07</td><td>12.1</td><td>8.397 ± 0.048</td><td>0.549 ± 0.050</td><td>0.567</td><td>-1.50</td><td>-0.478</td></tr><tr><td>Gl 801</td><td>9.88</td><td>0.704</td><td>4200 ± 100</td><td>4203 ± 118</td><td>dK6.0</td><td>40.04 ± 1.92</td><td>25.0</td><td>7.892 ± 0.12</td><td>0.648 ± 0.082</td><td>0.652</td><td>-0.21</td><td>-0.186</td></tr></tbody></table>
<table><caption>Table 1
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub> or (B-V)<br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>T<sub>eff</sub>±σ<br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Distance<br>(pc)</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>R<sub>*</sub><sup>a</sup><br>(R<sub>☉</sub>)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>b</sup><br>(dex)</th></tr></thead><tbody><tr><td>Gl 818</td><td>8.272</td><td>0.680</td><td>4250 ± 100</td><td>4342 ± 88</td><td>dK5.1</td><td>66.41 ± 0.95</td><td>15.1</td><td>7.383 ± 0.036</td><td>0.756 ± 0.060</td><td>0.733</td><td>+0.12</td><td>-0.127</td></tr><tr><td>Gl 820B</td><td>7.40</td><td>1.37</td><td>4073 ± 100</td><td>4073 ± 100</td><td>sdK6.9</td><td>285.88 ± 0.54</td><td>3.50</td><td>9.681 ± 0.024</td><td>0.316 ± 0.025</td><td>0.348</td><td>...</td><td>-2.664</td></tr><tr><td>Gl 826.1</td><td>9.086</td><td>0.749</td><td>4090 ± 100</td><td>4243 ± 111</td><td>dK5.1</td><td>61.65 ± 1.13</td><td>16.2</td><td>8.036 ± 0.044</td><td>0.616 ± 0.054</td><td>0.613</td><td>...</td><td>-0.282</td></tr><tr><td>Gl 828.1</td><td>10.480</td><td>0.803</td><td>3990 ± 100</td><td>4212 ± 222</td><td>dK5.9</td><td>36.93 ± 2.28</td><td>27.1</td><td>8.317 ± 0.135</td><td>0.583 ± 0.083</td><td>0.586</td><td>...</td><td>-0.399</td></tr><tr><td>Gl 830</td><td>9.075</td><td>0.728</td><td>4140 ± 100</td><td>4178 ± 65</td><td>dK6.2</td><td>54.33 ± 1.18</td><td>18.4</td><td>7.750 ± 0.052</td><td>0.713 ± 0.065</td><td>0.722</td><td>-0.21</td><td>-0.131</td></tr><tr><td>Gl 836.9AB</td><td>8.85</td><td>0.775</td><td>4040 ± 100</td><td>4140 ± 100</td><td>dK6.4</td><td>52.1 ± 8.5</td><td>19.2</td><td>7.434 ± 0.348</td><td>0.876 ± 0.229</td><td>0.893</td><td>...</td><td>-0.006</td></tr><tr><td>Gl 842</td><td>9.715</td><td>1.039</td><td>3780 ± 100</td><td>3700 ± 80</td><td>dM1</td><td>83.43 ± 1.77</td><td>12.0</td><td>9.322 ± 0.050</td><td>0.446 ± 0.042</td><td>0.585</td><td>...</td><td>-0.404</td></tr><tr><td>Gl 847A</td><td>10.97</td><td>0.761</td><td>4060 ± 100</td><td>4110 ± 50</td><td>sdK6.7</td><td>33.13 ± 1.87</td><td>30.2</td><td>8.571 ± 0.14</td><td>0.518 ± 0.076</td><td>0.541</td><td>...</td><td>-0.591</td></tr><tr><td>Gl 857.1</td><td>8.770</td><td>0.728</td><td>4140 ± 100</td><td>4300 ± 160</td><td>dK5.3</td><td>46.33 ± 1.09</td><td>21.6</td><td>7.099 ± 0.056</td><td>0.909 ± 0.084</td><td>0.894</td><td>...</td><td>-0.058</td></tr><tr><td>Gl 884</td><td>7.869</td><td>0.770</td><td>4040 ± 100</td><td>4063 ± 64</td><td>dK7.0</td><td>121.69 ± 0.69</td><td>8.22</td><td>8.295 ± 0.017</td><td>0.609 ± 0.051</td><td>0.644</td><td>-1.16</td><td>-0.198</td></tr><tr><td>Gl 885A</td><td>9.57</td><td>0.749</td><td>4090 ± 100</td><td>4196 ± 106</td><td>dK6.1</td><td>63 ± 16</td><td>15.9</td><td>8.567 ± 0.511</td><td>0.493 ± 0.172</td><td>0.499</td><td>...</td><td>-0.927</td></tr><tr><td>Gl 889A</td><td>9.640</td><td>0.756</td><td>4070 ± 100</td><td>4241 ± 126</td><td>dK5.8</td><td>47.76 ± 1.82</td><td>20.9</td><td>8.035 ± 0.087</td><td>0.620 ± 0.067</td><td>0.617</td><td>+0.74</td><td>-0.265</td></tr><tr><td>Gl 891</td><td>9.75</td><td>0.820</td><td>3963 ± 100</td><td>3963 ± 100</td><td>dK7.4</td><td>62.17 ± 3.27</td><td>16.1</td><td>8.718 ± 0.131</td><td>0.558 ± 0.081</td><td>0.622</td><td>...</td><td>-0.245</td></tr><tr><td>Gl 894</td><td>10.38</td><td>0.728</td><td>4140 ± 100</td><td>4240 ± 73</td><td>dK5.8</td><td>30.61 ± 1.90</td><td>32.7</td><td>7.809 ± 0.15</td><td>0.674 ± 0.095</td><td>0.671</td><td>-0.23</td><td>-0.159</td></tr><tr><td>Gl 895.3</td><td>10.19</td><td>0.691</td><td>4220 ± 100</td><td>4275 ± 55</td><td>dK5.5</td><td>37.04 ± 1.99</td><td>27.0</td><td>8.033 ± 0.13</td><td>0.582 ± 0.074</td><td>0.572</td><td>...</td><td>-0.459</td></tr><tr><td>Gl 898</td><td>8.607</td><td>0.716</td><td>4170 ± 100</td><td>4258 ± 129</td><td>dK5.6</td><td>65.98 ± 1.96</td><td>15.2</td><td>7.704 ± 0.069</td><td>0.695 ± 0.069</td><td>0.689</td><td>+0.01</td><td>-0.147</td></tr><tr><td>Gl 900</td><td>9.546</td><td>0.814</td><td>3970 ± 100</td><td>4165 ± 195</td><td>dK6.3</td><td>52.56 ± 1.29</td><td>19.0</td><td>8.149 ± 0.058</td><td>0.652 ± 0.068</td><td>0.664</td><td>...</td><td>-0.169</td></tr><tr><td>Gl 906</td><td>9.91</td><td>0.776</td><td>4030 ± 100</td><td>4065 ± 35</td><td>dK7.0</td><td>52.14 ± 1.66</td><td>19.2</td><td>8.496 ± 0.088</td><td>0.558 ± 0.067</td><td>0.593</td><td>...</td><td>-0.365</td></tr><tr><td>Gl 907.1</td><td>9.63</td><td>0.774</td><td>4040 ± 100</td><td>4040 ± 100</td><td>dK7.1</td><td>35.46 ± 2.20</td><td>28.2</td><td>7.379 ± 0.151</td><td>0.943 ± 0.145</td><td>0.985</td><td>...</td><td>-0.002</td></tr><tr><td>HIP 3121</td><td>10.46</td><td>0.742</td><td>4100 ± 100</td><td>4194 ± 94</td><td>dK6.1</td><td>27.72 ± 1.65</td><td>36.1</td><td>7.674 ± 0.146</td><td>0.741 ± 0.104</td><td>0.747</td><td>...</td><td>-0.121</td></tr><tr><td>HIP 6290</td><td>10.39</td><td>0.743</td><td>4100 ± 100</td><td>4192 ± 92</td><td>sdK6.1</td><td>49.77 ± 2.10</td><td>20.1</td><td>8.875 ± 0.110</td><td>0.427 ± 0.052</td><td>0.434</td><td>...</td><td>-1.675</td></tr><tr><td>HIP 11437</td><td>10.19</td><td>0.667</td><td>4267 ± 100</td><td>4180 ± 88</td><td>dK6.2</td><td>25.03 ± 2.25</td><td>40.0</td><td>7.182 ± 0.207</td><td>0.887 ± 0.151</td><td>0.896</td><td>...</td><td>-0.006</td></tr><tr><td>HIP 14593A</td><td>10.06</td><td>0.716</td><td>4170 ± 100</td><td>4260 ± 90</td><td>dK5.6</td><td>31.43 ± 2.52</td><td>31.8</td><td>7.547 ± 0.19</td><td>0.747 ± 0.121</td><td>0.740</td><td>...</td><td>-0.124</td></tr><tr><td>HIP 19410A</td><td>11.39</td><td>0.704</td><td>4200 ± 100</td><td>4302 ± 77</td><td>dK5.3</td><td>22.51 ± 2.20</td><td>44.4</td><td>8.152 ± 0.22</td><td>0.549 ± 0.098</td><td>0.761</td><td>+0.01</td><td>-0.115</td></tr><tr><td>HIP 19410B</td><td>12.15</td><td>0.704</td><td>4200 ± 100</td><td>4302 ± 77</td><td>dK5.3</td><td>22.51 ± 2.20</td><td>44.4</td><td>8.908 ± 0.23</td><td>0.388 ± 0.071</td><td>0.373</td><td>...</td><td>...</td></tr><tr><td>HIP 19410C</td><td>12.15</td><td>0.704</td><td>4200 ± 100</td><td>4302 ± 77</td><td>dK5.3</td><td>22.51 ± 2.20</td><td>44.4</td><td>8.908 ± 0.23</td><td>0.388 ± 0.071</td><td>0.373</td><td>...</td><td>...</td></tr><tr><td>HIP 21865</td><td>10.03</td><td>0.680</td><td>4250 ± 100</td><td>4393 ± 103</td><td>dK4.8</td><td>32.77 ± 1.30</td><td>30.5</td><td>7.607 ± 0.10</td><td>0.665 ± 0.074</td><td>0.632</td><td>-0.19</td><td>-0.219</td></tr><tr><td>HIP 40170</td><td>10.14</td><td>0.706</td><td>4190 ± 100</td><td>4290 ± 100</td><td>dK5.4</td><td>39.18 ± 2.12</td><td>25.5</td><td>8.105 ± 0.134</td><td>0.565 ± 0.075</td><td>0.553</td><td>...</td><td>-0.538</td></tr><tr><td>HIP 42108A</td><td>11.03</td><td>0.716</td><td>4170 ± 100</td><td>4160 ± 10</td><td>dK6.3</td><td>28.19 ± 1.71</td><td>35.5</td><td>8.283 ± 0.15</td><td>0.558 ± 0.079</td><td>0.571</td><td>...</td><td>-0.463</td></tr><tr><td>HIP 42108B</td><td>11.03</td><td>0.716</td><td>4170 ± 100</td><td>4160 ± 10</td><td>dK6.3</td><td>28.19 ± 1.71</td><td>35.5</td><td>8.283 ± 0.15</td><td>0.558 ± 0.079</td><td>0.571</td><td>...</td><td>-0.463</td></tr><tr><td>HIP 42910</td><td>10.16</td><td>0.752</td><td>4080 ± 100</td><td>4299 ± 193</td><td>dK5.4</td><td>27.45 ± 1.91</td><td>36.4</td><td>7.353 ± 0.17</td><td>0.824 ± 0.125</td><td>0.810</td><td>+0.16</td><td>-0.094</td></tr><tr><td>HIP 50773</td><td>10.69</td><td>0.788</td><td>4020 ± 100</td><td>4100 ± 80</td><td>dK6.7</td><td>33.56 ± 1.55</td><td>29.8</td><td>8.319 ± 0.12</td><td>0.604 ± 0.082</td><td>0.629</td><td>...</td><td>-0.225</td></tr><tr><td>HIP 51073</td><td>10.75</td><td>0.697</td><td>4210 ± 100</td><td>4285 ± 55</td><td>dK5.4</td><td>25.43 ± 2.63</td><td>39.3</td><td>7.777 ± 0.23</td><td>0.654 ± 0.118</td><td>0.642</td><td>-0.72</td><td>-0.200</td></tr><tr><td>HIP 51263A</td><td>10.44</td><td>0.692</td><td>4220 ± 100</td><td>4321 ± 76</td><td>dK5.2</td><td>28.09 ± 1.64</td><td>35.6</td><td>7.686 ± 0.14</td><td>0.669 ± 0.089</td><td>0.650</td><td>...</td><td>-0.189</td></tr><tr><td>HIP 51263B</td><td>10.44</td><td>0.692</td><td>4220 ± 100</td><td>4321 ± 76</td><td>dK5.2</td><td>28.09 ± 1.64</td><td>35.6</td><td>7.686 ± 0.14</td><td>0.669 ± 0.089</td><td>0.650</td><td>...</td><td>-0.189</td></tr><tr><td>HIP 53175</td><td>10.69</td><td>0.788</td><td>4020 ± 100</td><td>4250 ± 230</td><td>dK5.7</td><td>25.62 ± 2.02</td><td>39.0</td><td>7.733 ± 0.18</td><td>0.736 ± 0.122</td><td>0.731</td><td>...</td><td>-0.128</td></tr><tr><td>HIP 56838</td><td>10.03</td><td>0.698</td><td>4210 ± 100</td><td>4240 ± 160</td><td>dK5.7</td><td>32.73 ± 1.30</td><td>30.6</td><td>7.605 ± 0.10</td><td>0.724 ± 0.082</td><td>0.721</td><td>...</td><td>-0.132</td></tr><tr><td>HIP 58945</td><td>11.12</td><td>0.752</td><td>4080 ± 100</td><td>4255 ± 175</td><td>dK5.7</td><td>23.76 ± 2.06</td><td>42.1</td><td>7.999 ± 0.20</td><td>0.625 ± 0.105</td><td>0.619</td><td>...</td><td>-0.257</td></tr><tr><td>HIP 59247</td><td>11.04</td><td>0.776</td><td>4030 ± 100</td><td>4195 ± 165</td><td>dK6.1</td><td>23.95 ± 1.91</td><td>41.8</td><td>7.936 ± 0.20</td><td>0.678 ± 0.121</td><td>0.684</td><td>...</td><td>-0.151</td></tr><tr><td>HIP 60438A</td><td>10.78</td><td>0.781</td><td>4026 ± 100</td><td>4095 ± 69</td><td>dK6.8</td><td>22.31 ± 2.06</td><td>44.8</td><td>8.275 ± 0.212</td><td>0.613 ± 0.114</td><td>0.639</td><td>...</td><td>-0.206</td></tr><tr><td>HIP 60438B</td><td>10.78</td><td>0.781</td><td>4026 ± 100</td><td>4095 ± 69</td><td>dK6.8</td><td>22.31 ± 2.06</td><td>44.8</td><td>8.275 ± 0.212</td><td>0.613 ± 0.114</td><td>0.639</td><td>...</td><td>-0.206</td></tr><tr><td>HIP 60501</td><td>10.58</td><td>0.716</td><td>4170 ± 100</td><td>4295 ± 125</td><td>dK5.4</td><td>17.66 ± 2.09</td><td>56.6</td><td>6.815 ± 0.26</td><td>1.029 ± 0.206</td><td>1.015</td><td>...</td><td>-0.007</td></tr><tr><td>HIP 72044</td><td>9.91</td><td>0.680</td><td>4250 ± 100</td><td>4405 ± 155</td><td>dK4.8</td><td>38.54 ± 1.42</td><td>25.9</td><td>7.840 ± 0.10</td><td>0.595 ± 0.066</td><td>0.573</td><td>...</td><td>-0.454</td></tr><tr><td>HIP 76550</td><td>11.35</td><td>0.747</td><td>4090 ± 100</td><td>4095 ± 5</td><td>sdK6.8</td><td>31.45 ± 4.57</td><td>31.8</td><td>8.838 ± 0.31</td><td>0.457 ± 0.105</td><td>0.483</td><td>...</td><td>-1.111</td></tr><tr><td>HIP 78395</td><td>10.33</td><td>0.716</td><td>4170 ± 100</td><td>4322 ± 135</td><td>dK5.2</td><td>32.90 ± 2.05</td><td>30.4</td><td>7.916 ± 0.15</td><td>0.612 ± 0.086</td><td>0.593</td><td>+0.11</td><td>-0.365</td></tr><tr><td>HIP 80083</td><td>11.4</td><td>0.712</td><td>4180 ± 100</td><td>4514 ± 314</td><td>dK4.3</td><td>20.78 ± 2.76</td><td>48.1</td><td>7.988 ± 0.37</td><td>0.541 ± 0.140</td><td>0.504</td><td>-0.81</td><td>-0.870</td></tr><tr><td>HIP 95223</td><td>9.93</td><td>0.645</td><td>4318 ± 100</td><td>4355 ± 37</td><td>dK5.0</td><td>33.73 ± 1.25</td><td>29.6</td><td>7.570 ± 0.099</td><td>0.674 ± 0.075</td><td>0.649</td><td>...</td><td>-0.190</td></tr></tbody></table>
<table><caption>Table 1
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub> or (B-V)<br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>T<sub>eff</sub>±σ<br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Distance<br>(pc)</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>R<sub>*</sub><sup>a</sup><br>(R<sub>☉</sub>)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>b</sup><br>(dex)</th></tr></thead><tbody><tr><td>HIP 103150</td><td>11.18</td><td>0.812</td><td>3980 ± 100</td><td>4149 ± 198</td><td>sdK6.4</td><td>29.22 ± 2.05</td><td>34.2</td><td>8.508 ± 0.17</td><td>0.556 ± 0.090</td><td>0.571</td><td>-0.20</td><td>-0.463</td></tr><tr><td>HIP 110245</td><td>10.17</td><td>0.728</td><td>4140 ± 100</td><td>4387 ± 175</td><td>dK4.8</td><td>26.99 ± 2.23</td><td>37.1</td><td>7.326 ± 0.19</td><td>0.787 ± 0.126</td><td>0.756</td><td>+0.04</td><td>-0.117</td></tr><tr><td>HIP 110714</td><td>10.52</td><td>0.770</td><td>4040 ± 100</td><td>4116 ± 54</td><td>dK6.6</td><td>32.20 ± 1.90</td><td>31.1</td><td>8.059 ± 0.14</td><td>0.661 ± 0.097</td><td>0.682</td><td>+0.37</td><td>-0.152</td></tr><tr><td>HIP 113597</td><td>9.65</td><td>0.756</td><td>4070 ± 100</td><td>4186 ± 116</td><td>dK6.1</td><td>32.74 ± 2.03</td><td>30.5</td><td>7.226 ± 0.151</td><td>0.924 ± 0.132</td><td>0.932</td><td>...</td><td>-0.004</td></tr><tr><td>HIP 116011</td><td>11.80</td><td>0.704</td><td>4200 ± 100</td><td>4295 ± 95</td><td>dK5.4</td><td>18.41 ± 3.47</td><td>54.3</td><td>8.125 ± 0.40</td><td>0.558 ± 0.156</td><td>0.545</td><td>...</td><td>-0.571</td></tr><tr><td>LHS 3060</td><td>10.10</td><td>0.706</td><td>4190 ± 100</td><td>4190 ± 100</td><td>dK6.1</td><td>39.40 ± 0.29</td><td>25.4</td><td>8.077 ± 0.036</td><td>0.600 ± 0.050</td><td>0.607</td><td>...</td><td>-0.307</td></tr><tr><td>STKM 1-607</td><td>9.56</td><td>0.756</td><td>4070 ± 100</td><td>4070 ± 100</td><td>dK6.9</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>

Notes.

a Radius corrected for T<sub>eff</sub> effects.

b Computed from the [M/H]-radius relationship.
As regards photospheric analysis, our principal goal is to
extract precise v sin i values by applying cross-correlation
methods to multiple absorption lines over a ~100 Å swath of
the spectrum. We have found that it is important to select
certain optimal ranges of wavelengths so that the spectral lines
that lie within those ranges will contribute maximally to
enhancing the precision of v sin i: the precision is optimized in
spectral ranges where there are large numbers of weak and
unsaturated narrow spectral lines. As it turns out, the photo-
spheric continuum also contributes to which wavelength ranges
are optimal for our purposes: even within the relatively narrow
range of dK4 to dM4, changes in the continuum from one
spectral subtype to another give rise to detectable differences in
optimizing the choice of the wavelength range. These factors
reinforce our decision to study homogeneous samples where
the stars are confined to a narrow range of T<sub>eff</sub> (e.g.,
Papers XIV, XVI, XVII, this study). Not only do RACs vary
with the spectral type (e.g., Stepien 1989, 1993, 1994;
Houdebine et al. 2016), but also the distributions of rotation
periods vary from one spectral subtype to another (HM and this
paper).

Based on our previous papers, we have found that the most
suitable initial selection parameter when we wish to identify a
homogeneous sample of K or M dwarfs belonging to a specific
subtype is the (R-I) color: this color is sensitive to T<sub>eff</sub>, but less
so to metallicity (e.g., Leggett 1992; Ramirez & Melendez
2005). Moreover, broadband colors of high precision are
widely available in the literature for many of the cool dwarfs
that are of interest to us.

## 2.1. Selection of a Sample of Late-K Dwarfs

We selected a sample of 419 late-K dwarfs on the basis of
(R-I) measurements available in the literature. Our sample
contains stars with (R-I)C (the (R-I) color in the Cousins
system) in the range [0.684; 0.816], which also corresponds to
(R-I)K (R-I) in the Kron system) in the range [0.503; 0.613]
according to the transformation formulae of Leggett (1992) (see
Leggett 1992 for more information on the Cousins and Kron
photometric systems). According to Kenyon & Hartmann
(1995), this range of colors is centered on (R-I)C = 0.75, i.e.,
the spectral type dK7. However, when we compiled and
derived effective temperatures with the PCA-based inversion
method (see Paletou et al. 2015a and Section 3) for this sample
of late-K dwarfs, we found on average higher temperatures
than what would be expected from the (R-I)C-Teff tabulation of
Kenyon & Hartmann (1995). We give the stellar parameters
and spectral types of our late-K dwarf sample in Table 1. One
can see in this table that most stars are dK5 or dK6 stars, with a
few dK4 and dK7 stars. In view of this relatively large range of
spectral types, we decided to restrict our sample to the range
dK5.7 to dK7.3 in order to obtain a better-defined RAC
(Houdebine et al. 2016). This restricted sample is centered on
the spectral subtype dK5.9. We shall therefore refer to this
sample as the dK6 stars. Our dK6 stellar sample contains stars
that have similar (R-I) colors and the same effective
temperatures to within ±110 K. We refer to HM for a
discussion of corresponding data for our sample of dM3 stars.
The values of (R-I)C for our samples of stars were taken from
the following papers: Veeder (1974), Eggen (1974,
1976a, 1976b, 1978, 1979, 1980, 1987), Rodgers & Eggen
(1974), Weis & Upgren (1982), Upgren & Lu (1986), Booth
et al. (1988), Leggett & Hawkins (1988), Bessel (1990), Weis

(1991a, 1991b, 1993), Dawson & Forbes (1992), and
Leggett (1992).

These papers provided us with a starting list of a large
number (419) of late-K dwarfs. Searching through databases at
the European Southern Observatory (ESO) and Observatoire de
Haute Provence (OHP), we identified spectra of 112 different
stars that are suitable for our purposes. The final list of 105
stars in our late-K dwarf sample is provided in Table 1 (note
that in Table 1 we also added other stars with known v sin i and
[M/H]; see next sections).

The spectra that we use to determine v sin i came from two
different échelle spectrographs: HARPS (High Accuracy
Radial velocity Planet Search, ESO) and SOPHIE (OHP).
These two high-resolution échelle spectrographs are designed
for planet-search programs and are very stable in wavelength
and resolution. The instrumental stability makes the spectra
well suited for the measurement of rotation in M dwarfs
(see HM). We included in our sample the SOPHIE observa-
tions obtained in the high-efficiency (HE) mode for the purpose
of measuring the Ca II and Hα line equivalent widths
(Houdebine et al. 2016). For further details of the spectro-
graphs, see HM. For measuring v sin i with SOPHIE spectra,
we used observations in the HR mode only (R = 75,000 and an
image scrambler).

For comparison, when we were studying dM3 stars
(see HM), we started off with a list of 381 dM3 objects based
on (R-I)C data in the literature. Searching through the same
databases as above, we found suitable observations for 86
different dM3 stars.

## 2.2. Biases in Our Sample Stars

The stars in our sample include all stars from all observing
programs that have been carried out with HARPS and SOPHIE.
These programs are mostly planet-search programs, although
some programs are dedicated to magnetic activity. Because of
requirements of achieving high signal-to-noise ratios (S/N) in
the spectra, the selection of stars is brightness limited.

Our initial target list of 419 late-K dwarfs (based on
broadband colors) is estimated to be complete down to an
apparent brightness of $m_V \approx 11$. In our sample of 105 stars with
sufficiently high S/N spectra for our present purposes, the list
is estimated to be complete down to $m_V \approx 10$ for the slow
rotators. Assuming an absolute magnitude $M_V \approx 8.5$ as the
boundary between normal disk stars and subdwarfs, our sample
of 105 late-K dwarfs is estimated to be complete out to a
distance of 20 pc for our slow rotators. For subdwarfs, we
cannot claim that our target list is complete.

As far as the bias toward bright stars at spectral type dM3 is concerned, HM reported that this bias has little effect on the mean rotation period of low-activity M dwarfs. This is because the rotation period does not change much with the stellar radius for disk stars (see HM). Analogously, the brightness-limited bias in our late-K dwarf sample is expected to have only minor effects in the RAC. The bias may contribute somewhat to the density of sampling at different parts of the RAC, but this is not expected to cause significant discrepancies as regards the overall RAC (Houdebine et al. 2016).

In the planet-search programs, observers tend to avoid stars
with high levels of magnetic activity: spot modulation in such
stars can mimic the effects of planets and can also add
significant noise to the data. Therefore our spectral samples are
likely to be biased in general toward low-activity stars, that is,
stars that are far removed from “saturated” magnetic effects. Despite this “antiactivity” bias, we found that a small percentage of more active (i.e., dMe) stars did survive in our samples: 2% of our late-K dwarf sample are cataloged as dKe, and 10% of our dM3 sample are cataloged as dM3e. We note that the latter figure is not far from the report of West et al. (2008) that 10%–20% of dM3 stars are dM3e. However, we completed our own samples with v sin i measures and Ca II and Hα line equivalent width measures from the literature, including notably many new, fast rotators. Therefore, the samples of stars studied in this paper do not contain *only* low-activity stars (i.e., slow rotators).

### 3. STELLAR PARAMETERS

Here, we discuss the methods we use to derive $T_{\text{eff}}$ and radius for each of our samples of stars. The radius is necessary for the determination of the projected rotation periods, $P/\sin i$.

#### 3.1. PCA-based Inversion of Stellar Fundamental Parameters for Late-K Dwarfs

In order to derive estimates of effective temperatures ($T_{\text{eff}}$) for our late-K dwarfs in Table 1, we used the calibration of Kenyon & Hartmann (1995, hereafter KH). We derived the effective temperature as a function of $(R-I)_C$ according to this tabulation. We searched the literature for other $T_{\text{eff}}$ measurements for our late-K targets (we used the tutorial developed by Paletou & Zolotukhin 2014).<fnref n="6" /> We found a relatively good agreement between these temperatures and effective temperatures previously published: the mean difference is only on the order of 75 K.

As an independent method of determining values of $T_{\text{eff}}$ for our sample of late-K dwarfs, we used the PCA-based method to derive $T_{\text{eff}}$ and also [Fe/H], log(g), and v sin i (Paletou et al. 2015b). HARPS and SOPHIE spectra were inverted using the PCA method introduced for stellar fundamental parameters by Paletou et al. (2015a). In the latter paper, stellar spectra of FGK stars were inverted using a so-called “learning database” made from the Elodie stellar spectra library (see Prugniel et al. 2007): the “learning” occurs by using *observed* spectra for which fundamental parameters had already been evaluated. We note that the spectra considered in Paletou et al. (2015a) had typical spectral resolutions $R$ of 50,000 and 65,000: these are significantly lower than the resolution of the HARPS and SOPHIE data that will be analyzed in the present paper.

For the present study, we used the PCA method, but with a difference: the “learning” was achieved by referring to synthetic spectra. A grid of 6336 spectra was computed using the SYNSPEC-48 synthetic spectra code (Hubeny & Lanz 1992) and Kurucz ATLAS-12 model atmospheres (Kurucz 2005). The line list was built from Kurucz (1992) gfhyperall.dat.<fnref n="7" /> In order to deal with stars close to dK6, we adopted a grid of parameters such that $T_{\text{eff}}$ is in the range 3500–4600 K (with steps of 100 K), logg is in the range 4–5 cgs (with steps of 0.2 dex), metallicity [Fe/H] is in the range from -2 to +0.5 (with steps of 0.25 dex), and, finally, v sin i is in the range from 0 to 14 km s⁻¹ (with steps of 2 km s⁻¹). For all models, the microturbulent velocity was fixed at $\xi_t = 1$ km s⁻¹, and [α/Fe] was set to 0. Also, to produce the reference spectra, we adopted

<table><caption>**Table 2**

Inverted Stellar Parameters $T_{\text{eff}}$, log g, [Fe/H], and v sin i for HARPS and SOPHIE Objects Using Our Atlas-based PCA Method</caption><thead><tr><th>Object</th><th><i>T</i><sub>eff</sub> [K]</th><th>log g [dex]</th><th>[Fe/H] [dex]</th><th>v sin i [km s<sup>-1</sup>]</th></tr></thead><tbody><tr><td>GJ 1056</td><td>4480</td><td>4.8</td><td>-0.20</td><td>2.4</td></tr><tr><td>GJ 1066</td><td>4500</td><td>5.0</td><td>-0.25</td><td>1.0</td></tr><tr><td>GJ 1067</td><td>4520</td><td>4.8</td><td>-0.22</td><td>2.4</td></tr><tr><td>GJ 1267</td><td>4270</td><td>5.0</td><td>-0.50</td><td>2.5</td></tr><tr><td>GJ 1279</td><td>4450</td><td>4.9</td><td>-0.12</td><td>2.5</td></tr><tr><td>GJ 3072</td><td>4110</td><td>4.8</td><td>-0.50</td><td>2.2</td></tr><tr><td>GJ 3494</td><td>4470</td><td>4.9</td><td>-0.25</td><td>3.3</td></tr><tr><td>GJ 3551</td><td>4270</td><td>4.7</td><td>-0.50</td><td>1.3</td></tr><tr><td>GJ 3996</td><td>4240</td><td>4.8</td><td>-0.36</td><td>2.9</td></tr><tr><td>GJ 4140</td><td>4250</td><td>4.9</td><td>-0.50</td><td>3.0</td></tr><tr><td>GJ 9299</td><td>4270</td><td>4.8</td><td>-0.25</td><td>2.0</td></tr><tr><td>GJ 9714</td><td>4500</td><td>5.0</td><td>-0.25</td><td>2.0</td></tr><tr><td>GJ 9827</td><td>4270</td><td>4.9</td><td>-0.50</td><td>1.3</td></tr><tr><td>Gl 14</td><td>4370</td><td>4.9</td><td>-0.25</td><td>3.0</td></tr><tr><td>Gl 17.1</td><td>3810</td><td>4.8</td><td>-0.72</td><td>2.0</td></tr><tr><td>Gl 40A</td><td>4400</td><td>4.9</td><td>-0.33</td><td>2.3</td></tr><tr><td>Gl 45</td><td>4340</td><td>4.9</td><td>-0.25</td><td>1.6</td></tr><tr><td>Gl 50</td><td>4240</td><td>4.7</td><td>-0.44</td><td>2.0</td></tr><tr><td>Gl 52</td><td>4280</td><td>4.9</td><td>-0.46</td><td>2.0</td></tr><tr><td>Gl 57</td><td>4030</td><td>4.8</td><td>-0.75</td><td>2.2</td></tr><tr><td>Gl 116</td><td>4050</td><td>4.5</td><td>-1.10</td><td>2.2</td></tr><tr><td>Gl 143.1</td><td>3980</td><td>4.7</td><td>-0.40</td><td>2.1</td></tr><tr><td>Gl 146</td><td>4260</td><td>4.8</td><td>-0.25</td><td>2.4</td></tr><tr><td>Gl 153A</td><td>4350</td><td>4.8</td><td>-0.43</td><td>2.5</td></tr><tr><td>Gl 156</td><td>4190</td><td>4.8</td><td>-0.25</td><td>1.6</td></tr><tr><td>Gl 162.2</td><td>4460</td><td>4.8</td><td>-0.19</td><td>3.0</td></tr><tr><td>Gl 186</td><td>4310</td><td>4.7</td><td>-0.19</td><td>7.3</td></tr><tr><td>Gl 191</td><td>&le;3500</td><td>4.6</td><td>-1.00</td><td>2.0</td></tr><tr><td>Gl 208</td><td>4120</td><td>4.8</td><td>-0.47</td><td>3.1</td></tr><tr><td>Gl 221</td><td>4180</td><td>4.8</td><td>-0.46</td><td>1.7</td></tr><tr><td>Gl 322</td><td>4470</td><td>5.0</td><td>-0.25</td><td>2.5</td></tr><tr><td>Gl 369</td><td>3790</td><td>4.8</td><td>-0.86</td><td>2.4</td></tr><tr><td>Gl 389.1</td><td>4450</td><td>4.9</td><td>-0.25</td><td>2.0</td></tr><tr><td>Gl 401</td><td>3810</td><td>4.9</td><td>-0.94</td><td>2.2</td></tr><tr><td>Gl 412.3</td><td>4370</td><td>4.8</td><td>-0.25</td><td>3.5</td></tr><tr><td>Gl 414A</td><td>4340</td><td>4.9</td><td>-0.20</td><td>2.0</td></tr><tr><td>Gl 416</td><td>4470</td><td>4.8</td><td>-0.25</td><td>4.0</td></tr><tr><td>Gl 421B</td><td>4120</td><td>4.7</td><td>-0.44</td><td>2.2</td></tr><tr><td>Gl 425B</td><td>4400</td><td>4.8</td><td>-0.25</td><td>4.5</td></tr><tr><td>Gl 496.1</td><td>4060</td><td>4.7</td><td>-0.25</td><td>2.0</td></tr><tr><td>Gl 509.1</td><td>4500</td><td>5.0</td><td>-0.25</td><td>3.0</td></tr><tr><td>Gl 517</td><td>4510</td><td>4.6</td><td>-0.14</td><td>10.0</td></tr><tr><td>Gl 522</td><td>4260</td><td>4.8</td><td>-0.25</td><td>1.8</td></tr><tr><td>Gl 524.1</td><td>4180</td><td>4.8</td><td>-0.43</td><td>2.4</td></tr><tr><td>Gl 546</td><td>4470</td><td>4.9</td><td>-0.21</td><td>2.3</td></tr><tr><td>Gl 558</td><td>4390</td><td>4.9</td><td>-0.44</td><td>2.2</td></tr><tr><td>Gl 562</td><td>4400</td><td>4.9</td><td>-0.39</td><td>3.1</td></tr><tr><td>Gl 571.1</td><td>4160</td><td>4.8</td><td>-0.27</td><td>2.4</td></tr><tr><td>Gl 583</td><td>4260</td><td>4.8</td><td>-0.38</td><td>2.3</td></tr><tr><td>Gl 619</td><td>4320</td><td>4.8</td><td>-0.33</td><td>2.4</td></tr><tr><td>Gl 629.1</td><td>4160</td><td>4.7</td><td>-0.33</td><td>2.3</td></tr><tr><td>Gl 707</td><td>4400</td><td>5.0</td><td>-0.25</td><td>2.0</td></tr><tr><td>Gl 710</td><td>4160</td><td>4.8</td><td>-0.50</td><td>2.0</td></tr><tr><td>Gl 726</td><td>4330</td><td>4.9</td><td>-0.39</td><td>2.6</td></tr><tr><td>Gl 728</td><td>4170</td><td>4.8</td><td>-0.50</td><td>2.0</td></tr><tr><td>Gl 747.3</td><td>4180</td><td>4.7</td><td>-0.25</td><td>5.4</td></tr><tr><td>Gl 757</td><td>4010</td><td>4.8</td><td>-0.73</td><td>2.2</td></tr><tr><td>Gl 763</td><td>4120</td><td>4.9</td><td>-0.57</td><td>5.9</td></tr><tr><td>Gl 782</td><td>4400</td><td>4.8</td><td>-0.25</td><td>3.0</td></tr><tr><td>Gl 786.1</td><td>4280</td><td>4.9</td><td>-0.21</td><td>2.6</td></tr><tr><td>Gl 798</td><td>4300</td><td>5.0</td><td>-0.50</td><td>2.0</td></tr><tr><td>Gl 801</td><td>4350</td><td>4.9</td><td>-0.50</td><td>1.0</td></tr><tr><td>Gl 818</td><td>4460</td><td>4.8</td><td>-0.12</td><td>1.5</td></tr><tr><td>Gl 826.1</td><td>4290</td><td>4.8</td><td>-0.28</td><td>2.8</td></tr></tbody></table>

<footnote n="6">⁶ http://www.astropy.org/</footnote>

<footnote n="7">⁷ http://kurucz.harvard.edu</footnote>
<table><caption>**Table 2**
(Continued)</caption><thead><tr><th>Object</th><th><i>T</i><sub>eff</sub> [K]</th><th>log <i>g</i> [dex]</th><th>[Fe/H] [dex]</th><th><i>v</i> sin <i>i</i> [km s<sup>-1</sup>]</th></tr></thead><tbody><tr><td>Gl 830</td><td>4270</td><td>4.7</td><td>-0.38</td><td>1.7</td></tr><tr><td>Gl 842</td><td>3770</td><td>4.8</td><td>-0.78</td><td>2.5</td></tr><tr><td>Gl 847A</td><td>4160</td><td>4.9</td><td>-0.50</td><td>2.4</td></tr><tr><td>Gl 855</td><td>3830</td><td>4.8</td><td>-0.75</td><td>2.8</td></tr><tr><td>Gl 857.1</td><td>4460</td><td>4.7</td><td>-0.09</td><td>6.6</td></tr><tr><td>Gl 884</td><td>4150</td><td>4.8</td><td>-0.45</td><td>2.4</td></tr><tr><td>Gl 889A</td><td>4370</td><td>4.8</td><td>-0.25</td><td>2.6</td></tr><tr><td>Gl 894</td><td>4270</td><td>4.8</td><td>-0.25</td><td>2.4</td></tr><tr><td>Gl 895.5</td><td>4330</td><td>4.8</td><td>-0.25</td><td>3.0</td></tr><tr><td>Gl 898</td><td>4440</td><td>4.8</td><td>-0.15</td><td>4.0</td></tr><tr><td>Gl 900</td><td>4360</td><td>4.8</td><td>-0.14</td><td>7.4</td></tr><tr><td>Gl 906</td><td>4100</td><td>4.8</td><td>-0.67</td><td>2.1</td></tr><tr><td>HIP 14593A</td><td>4350</td><td>4.8</td><td>-0.28</td><td>2.0</td></tr><tr><td>HIP 19410</td><td>4320</td><td>4.8</td><td>-0.25</td><td>12.4</td></tr><tr><td>HIP 21865</td><td>4440</td><td>4.8</td><td>-0.14</td><td>2.0</td></tr><tr><td>HIP 42108</td><td>4150</td><td>4.6</td><td>-0.37</td><td>12.7</td></tr><tr><td>HIP 42910</td><td>4550</td><td>5.0</td><td>-0.06</td><td>2.0</td></tr><tr><td>HIP 50773</td><td>4180</td><td>4.8</td><td>-0.44</td><td>2.2</td></tr><tr><td>HIP 51073</td><td>4340</td><td>4.9</td><td>-0.50</td><td>1.3</td></tr><tr><td>HIP 51263</td><td>4340</td><td>4.9</td><td>-0.71</td><td>3.4</td></tr><tr><td>HIP 53175</td><td>4480</td><td>4.9</td><td>-0.12</td><td>3.7</td></tr><tr><td>HIP 56838</td><td>4450</td><td>4.9</td><td>-0.25</td><td>2.0</td></tr><tr><td>HIP 58945</td><td>4430</td><td>4.9</td><td>-0.18</td><td>2.5</td></tr><tr><td>HIP 59247</td><td>4360</td><td>4.8</td><td>-0.33</td><td>1.8</td></tr><tr><td>HIP 60501</td><td>4420</td><td>5.0</td><td>-0.10</td><td>1.6</td></tr><tr><td>HIP 72044</td><td>4560</td><td>4.9</td><td>-0.25</td><td>2.4</td></tr><tr><td>HIP 76550</td><td>4100</td><td>4.7</td><td>-1.00</td><td>2.0</td></tr><tr><td>HIP 78395</td><td>4500</td><td>5.0</td><td>-0.25</td><td>3.0</td></tr><tr><td>HIP 80083</td><td>4200</td><td>4.8</td><td>-0.75</td><td>1.0</td></tr><tr><td>HIP 103150</td><td>4040</td><td>4.7</td><td>-0.75</td><td>2.6</td></tr><tr><td>HIP 110245</td><td>4500</td><td>4.7</td><td>-0.17</td><td>4.0</td></tr><tr><td>HIP 110714</td><td>4150</td><td>4.7</td><td>-0.22</td><td>2.0</td></tr><tr><td>HIP 116011</td><td>4390</td><td>4.7</td><td>-0.65</td><td>2.9</td></tr></tbody></table>

the spectral resolution of the HARPS or SOPHIE spectrographs: $R = 115,000$ or $R = 75,000$. We finally limited the PCA study to a spectral band almost 100 Å wide centered on the Na I D doublet, ranging from 585.3 to 593.2 nm.

Even though the choice of ATLAS-12 for such cool stars, as well as the choice of the synthetic spectral band we considered, may be open to debate, we believe that the parameters inverted from HARPS and SOPHIE data using our PCA approach are realistic enough for an initial analysis (see Paletou et al. 2015b).

Table 2 provides the results we have obtained from our PCA approach to the sample of 112 late-K dwarfs for $T_{eff}$, logg, [Fe/H], and $v \sin i$. Typical uncertainties for these four parameters are respectively of order 100 K, 0.2, 0.1 dex, and 1.5 km s$^{-1}$. It is important to note that the $v \sin i$ values derived from PCA are only preliminary estimates in order to obtain synthetic spectra to be used for “learning.” Later on (Section 4), we shall derive more precise $v \sin i$ values based on the cross-correlation analysis; then we shall compare (Section 5) the precise values with the estimates derived from PCA (see Figure 12). Note that the spectra of GJ 1248 and Gl 747.1 were not inversed with the PCA method because they were too noisy.

In our sample of 112 stars, the PCA approach indicated that seven stars have significantly lower $T_{eff}$ values than those expected for a late-K dwarf: the seven stars are GJ 1248, Gl 17.1, Gl 369, Gl 401, Gl 747.1, Gl 842, and Gl 855 (see

Table 2). It appears that our sample of late-K dwarfs is polluted by a few cooler stars with spectral types that are actually later than dK7. Confirmation of the unusual coolness of seven stars in our list of 112 is provided by our PCA determinations of $T_{eff}$ in Table 2. Clearly, some of the $(R-I)_C$ values in our sample are discrepant. In view of this, we have excluded the seven discrepant stars from our initial sample of 112 objects (Table 1).

Now let us compare the results for $T_{eff}$ that we have derived by means of the two different methods: KH and PCA. For our sample, we obtained a mean effective temperature of 4130 ± 100 K when we use the $(R-I)_C$ color calibration method (KH). However, for the same sample of stars, we obtained a mean effective temperature of 4270 ± 100 K when we use the PCA approach. There is a systematic difference of 140 K between PCA and color calibration. Comparatively, the $(R-I)_C$ color calibration method (KH) is in better agreement with the values given in the literature (see references therein), with a systematic difference of only 75 K. We show in Figure 2 the values of $T_{eff}$ derived from the $(R-I)_C$ color as a function of the $T_{eff}$ values compiled from the literature (left-hand panel). The solid line is the one-to-one correlation. The dashed line shows the smoothed data. There is a significant scatter among the data, typically ±70 K. Our measures inferred from $(R-I)_C$ agree rather well with other published values, typically within 50 K, up to a temperature of 4200 K. For larger values, our temperatures inferred from $(R-I)_C$ tend to be lower than published values, up to a value of 100 K. However, this latter difference is still reasonable. We can say that globally the temperatures inferred from $(R-I)_C$ are good evaluations. E. R. Houdebine et al. (2016, in preparation) show that $(R-I)_C$ is a good effective temperature diagnostic (based on the calibration of Boyajian et al. 2012) from spectral types dK3 to dM7, with typical differences from a large compilation of effective temperatures from the literature of only ±40 K.

We show in Figure 2 (right-hand panel) the values of $T_{eff}$ derived from the PCA inversion method as a function of the $T_{eff}$ values compiled from the literature. One can note that the PCA method tends to globally overestimate $T_{eff}$ at low and large values. The maximum difference on average is on the order of 200 K.

The differences we find between the different approaches are to be compared with the systematic difference of typically 200–300 K between the results obtained by various investigators for K dwarfs (e.g., Ramirez & Melendez 2005; Ammons et al. 2006; Morales et al. 2008; Jenkins et al. 2009; Soubiran et al. 2010). We found during the course of our compilation of $T_{eff}$ from the literature for our objects that differences between authors are often different by more than 100–200 K. In some cases, the differences may be more than 500 K. These systematic differences seem relatively large compared to the precisions that are claimed by the various authors (typically ±100 K). In view of these systematic differences already in the literature, we believe that the $T_{eff}$ differences that we encounter between our two methods are not excessive: in fact, given the scatter in the data, we consider our results to be reasonable and consistent with values in the literature. In what follows, we have taken the mean of the three different values (KH, PCA, and mean of published values) in order to obtain reliable estimates of our effective temperatures for our sample of late-K dwarfs (Table 1).
According to our PCA approach, the mean metallicity of our sample is -0.316 dex (excluding dKe stars and subdwarfs). Therefore, on average, our late-K dwarfs are metal-poor. However, if we compare this value to the average of the metallicities for dM2 stars (-0.154 dex, Paper XIV), we find that the present metallicities for our sample may be underestimated. As a matter of fact, for dM2 stars, we obtained a good RAC after correction from the metallicity effects in Paper XIV, which somewhat confirms a posteriori the accuracy of those metallicities. On the other hand, when we attempt to correct the dK6 star RAC for metallicity effects (Houdebine et al. 2016), we obtain a larger scatter in the RAC. This may arise from the larger uncertainty we have on the metallicity for dK6 stars (0.2 dex).

## 3.2. Effective Temperatures for Our Samples of M Dwarfs and the Stellar Radii

In order to derive radii for the stars in our dK6 and other samples, we used the classical formula

$$M_v + BC = 42.36 - 5 \times \log \frac{R_*}{R_{\odot}} - 10 \times \log T_{\text{eff}}, \quad (1)$$

where symbols take their usual meaning. We used the bolometric correction (BC) tabulation as a function of $(R-I)_C$ from KH: these authors compiled data on BC as a function of various colors from the literature. We estimate that their tabulation yields an uncertainty of about 10% in BC at spectral type K6 (see KH). Using Equation (1), we obtained the radii for our late-K dwarfs as listed in Table 1. In this table, we give the mean of the effective temperatures derived from the $(R-I)_C$ color from KH, the values of the PCA method, and values previously published. The sources of the published effective temperatures are Wright et al. (2003), Valenti & Fischer (2005), Ammons et al. (2006), Masana et al. (2006), Sanchez-Blazquez et al. (2006), Sousa et al. (2006), Cenarro et al. (2007), Morales et al. (2008), Jenkins et al. (2009), Lafrasse et al. (2010), Soubiran et al. (2010), Casagrande et al. (2011), Prugniel et al. (2011), McDonald et al. (2012), Chen et al. (2014), and Gaidos et al. (2014). We estimate the errors as the $\sigma$ of these measures. The errors on the radii in Table 1 were computed taking into account the combination of the error on the absolute magnitude, an assumed error of 0.02 magnitudes on the $(R-I)_C$ color, and a typical 100 K error in $T_{\text{eff}}$. The mean $T_{\text{eff}}$ and radius for our dK6 sample are 4226 K and 0.6469 $R_{\odot}$, respectively. The value of the radius for this $T_{\text{eff}}$ given by Boyajian et al. (2012) is 0.6457 $R_{\odot}$. Therefore, the two values agree within 0.19%. We generally considered that, in our dK6 sample, stars with [M/H] < -0.5 ($M_v \approx 8.6$) are subdwarfs.

For our samples of dM2 and dM4 stars, we used in previous studies the calibration of Jones et al. (1994). However, a more recent study that should be more precise (Mann et al. 2015) indicates that the values from Jones et al. (1994) may be underestimated by about 170 K. We show the calibrations of $T_{\text{eff}}$ as a function of $(R-I)_C$ of Jones et al. (1994), KH, and Mann et al. (2015, filled circles) in Figure 1. We also show a smoothing of the data of Mann et al. (2015, dotted line). The calibration of Kenyon & Hartmann (1995) agrees well with the more recent measures of Mann et al. (2015) up to $(R-I)_c = 1.3$, but it tends to overestimate $T_{\text{eff}}$ for later spectral types. Therefore, the stellar radii have been overestimated in our previous studies of dM2 and dM4 stars on the order of 10%–15%.

In the coming subsections, our measurements of $v \sin i$ have been compared with, and supplemented by, those from other authors. For comparison between the different spectral subtypes used in this study, we overplot the $(R-I)_C$ domains of our samples of stars from dK4 to dM4. However, we recall that there are systematic differences of the order of 200–300 K in the $T_{\text{eff}}$-radius plane between the interferometric calibrations of Boyajian et al. (2012) and the double-eclipsing binaries calibrations (see Boyajian et al. 2012 for a comparison) for K and M dwarfs. Therefore, the calibration of Mann et al. (2015) may not be definitive and may still be subject to improvements.

We give in Tables 3–5 the stellar parameters for our samples of dM2, dM3, and dM4 stars, respectively. The mean $T_{\text{eff}}$ and radii for our samples of dK4, dK6, dM2, dM3, and dM4 stars are given in Table 6. We find values of 4600 K, 4226 K, 3658 K, 3462 K, and 3317 K for the mean $T_{\text{eff}}$ of our samples of dK4, dK6, dM2, dM3, and dM4 stars, respectively. The mean radii are 0.6469 $R_{\odot}$, 0.5082 $R_{\odot}$, 0.4090 $R_{\odot}$, and 0.3008 $R_{\odot}$ for the dK6, dM2, dM3, and dM4 samples, respectively. These radii agree with those of Boyajian et al. (2012) within 0.19%, 6.3%, 4.3%, and 8.2%, respectively, which is acceptable for the studies of the $P \sin i$ distributions and the RACs.

For our sample of dK5 stars (Houdebine 2011a, 2012b Papers XVI and XVIII), we found that the mean temperature is 4600 K (Table 6). Effective temperatures for these stars were computed from values published in the literature (see Paper XVI). The stars were initially selected with $(R-I)_C = [0.56:0.68]$, which corresponds to the spectral subtype ~K5 (KH). However, as in the case of dK6 stars, we found that the published effective temperatures were somewhat higher and instead correspond on average to the spectral subtype dK4 (KH). Therefore, we shall refer to the dK4 stars for this sample of stars thereafter. We do not repeat the stellar parameters of our dK4 stellar sample here because the effective temperatures have not changed, and the data are available in Paper XVI.

## 3.3. Stellar Metallicities

We saw in Paper XV that a correction for metallicity effects in dM2 stars is essential in order to obtain a good correlation between the Ca II EW and $P/\sin i$. This is because the Ca II line formation depends sensitively on the Ca abundance (E. R. Houdebine & P. M. Panagi, in preparation). The same applies to dK6 stars and to the Ca II surface fluxes. Therefore, we compiled [M/H] measures from the literature for our dK6 stellar sample in order to obtain a metallicity-radius empirical correlation, as in Houdebine (2008, Paper VII), and we correct our Ca II surface fluxes for metallicity effects, assuming a proportionality between [M/H] and Ca II surface fluxes. We found several measures of [M/H] from the following authors: Marsakov & Shevelev (1988), Alonso et al. (1996), Valenti & Fischer (2005), Ammons et al. (2006), Sanchez-Blazquez et al. (2006), Sousa et al. (2006), Cenarro et al. (2007), Mishenina et al. (2008), Soubiran et al. (2010), Casagrande et al. (2011), Milone et al. (2011), Prugniel et al. (2011), Wu et al. (2011), Anderson & Francis (2012), and Gaidos et al. (2014). We averaged the values from the literature with those from our PCA-based inversion method.

We plot in Figure 3 these average values of [M/H] as a function of radius for our dK6 stars. One can see in this diagram that the scatter is large. We show the error box in
<figure><img src="image_4.png" /><figcaption>**Figure 1.** Values of $T_{\text{eff}}$ as a function of the $(R-I)_C$ color for the data of Mann et al. (2015, filled circles) and a smoothing of this data (dotted line). Also shown for comparison are the values of Jones et al. (1994, solid line) used in some of our previous studies. A difference of about ~170 K exists between the two correlations. Also shown is the calibration of Kenyon & Hartmann (1995). This later calibration agrees well with the more recent measures of Mann et al. up to $(R-I)_C = 1.3$, but it tends to overestimate $T_{\text{eff}}$ for later spectral types. We overplot the $(R-I)_C$ domains of our samples of stars from dK4 to dM4.</figcaption></figure>

Figure 3, which gives in [M/H] the mean of the differences between the values from the literature and our values from the PCA-based inversion method, and in radius, the mean of the errors on the radii for our stars. Both errors are large and explain the poor correlation between these two parameters for dK6 stars as well as the large scatter at about the running mean (solid line). As a consequence, the corrections from metallicity turn out to be rather poor; in fact, we do not obtain an improved RAC after corrections for [M/H] compared to the RAC without such corrections (see Houdebine et al. 2016).

For our dM2 stellar sample, we used the empirical correlation found by Houdebine (2008, Paper VII) to determine the metallicity for each star as a function of its radius. These values were computed in Paper XV and are reported in Table 3.

We show the correlation between [M/H] and stellar radius for stars with spectral subtype dM3 in Figure 4. The correlation is relatively tight, as in dM2 stars (Paper VII), in spite of the relatively large error on the radius (see the error box in Figure 4). The scatter in this correlation is about three times less than in the same correlation for dK6 stars (Figure 3). We can see that, as in dM2 and dK6 stars, the metallicity decreases with decreasing radius for a given $(R-I)_C$. We show some obvious outliers as open circles, and the continuous line represents the data smoothed by a Gaussian. We derived the metallicities for dM3 stars according to this mean correlation. We report the values of [M/H] in Table 6.

We also decided to compile all the metallicities published for our initial selection list of 395 dM4 stars and try to obtain a metallicity–radius correlation for these stars. We found

metallicities from the literature for 179 dM4 stars. We give these metallicities in Table 5. Our measures of [M/H] for our list of dM4 stars were collected from the following authors: Marsakov & Shevelev (1988), Ivanov et al. (2004), Ammons et al. (2006), Sanchez-Blazquez et al. (2006), Cenarro et al. (2007), Holmberg et al. (2009), Jenkins et al. (2009), Soubiran et al. (2010), Casagrande et al. (2011), Milone et al. (2011), Prugniel et al. (2011), Wu et al. (2011), Anderson & Francis (2012), Koleva & Vazdekis (2012), Rojas-Ayala et al. (2012), Kordopatis et al. (2013), Mann et al. (2013), Pace (2013), Gaidos et al. (2014), Gomez da Silva et al. (2014), Newton et al. (2014), and Mann et al. (2015). We show the empirical relationship between [M/H] and stellar radius for stars with spectral subtype dM4 in Figure 5.

The correlation is not as tight as in dM2 stars or dM3 stars, particularly for small radii where the scatter is large (about ±0.5 dex). We have no simple explanation for this relatively large scatter at this stage. We also note that the mean of the data (continuous line) is rather flat and stands at [M/H] of about 0 dex over a large range of radii. This was not the case for dK6, dM2, and dM3 stars, for which [M/H] starts to diminish more rapidly at small radii. In Figure 5, we show some obvious outliers as open circles, and the continuous line represents the data smoothed by a Gaussian. Also, for dM4 stars, the minimum values of [M/H] do not fall below −0.5 dex for the smoothed curve even for the smallest radii, which brings into question the presence of subdwarfs in our sample, in spite of the fact that individual measures of [M/H] include about 10
<table><caption>Table 3
Stellar Parameters and the Values of v sin i from Paper XIV for Our dM2 Stars</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m<sup>′′</sup>)</th><th>M<sub>v</sub><br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>km s<sup>-1</sup></th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th></tr></thead><tbody><tr><td>GJ 1010A</td><td>11.31</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>50.01 ± 2.02</td><td>9.805 ± 0.106</td><td>0.517 ± 0.065</td><td>...</td><td>...</td><td>-0.098</td></tr><tr><td>GJ 1062</td><td>13.015</td><td>1.184</td><td>3602 ± 100</td><td>sdM2</td><td>33 ± 3.6</td><td>10.608 ± 0.245</td><td>0.372 ± 0.076</td><td>9.8</td><td>1.92-0.53 + 0.65</td><td>-0.584</td></tr><tr><td>GJ 1114</td><td>11.523</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>54.53 ± 3.60</td><td>10.206 ± 0.144</td><td>0.430 ± 0.063</td><td>3.8</td><td>5.73-1.50 + 2.07</td><td>-0.339</td></tr><tr><td>GJ 1264</td><td>9.641</td><td>1.112</td><td>3674 ± 100</td><td>PMS M2e</td><td>61.29 ± 1.54</td><td>8.578 ± 0.059</td><td>0.870 ± 0.088</td><td>6.46</td><td>6.82-1.51 + 2.06</td><td>+0.378</td></tr><tr><td>GJ 2085</td><td>11.185</td><td>1.058</td><td>3724 ± 100</td><td>dM2</td><td>46.81 ± 2.39</td><td>9.537 ± 0.113</td><td>0.525 ± 0.067</td><td>2.46</td><td>10.80-3.23 + 5.31</td><td>+0.000</td></tr><tr><td>GJ 3084</td><td>10.791</td><td>1.064</td><td>3718 ± 100</td><td>dM2</td><td>48.83 ± 10.7</td><td>9.234 ± 0.435</td><td>0.608 ± 0.187</td><td>3.16</td><td>9.74-4.07 + 5.98</td><td>+0.023</td></tr><tr><td>GJ 3098</td><td>11.155</td><td>1.088</td><td>3696 ± 100</td><td>dM2</td><td>55.98 ± 1.91</td><td>9.895 ± 0.078</td><td>0.461 ± 0.051</td><td>2.60</td><td>8.97-2.49 + 3.98</td><td>-0.200</td></tr><tr><td>GJ 3207</td><td>11.51</td><td>1.160</td><td>3626 ± 100</td><td>dM2</td><td>57 ± 14</td><td>10.289 ± 0.497</td><td>0.420 ± 0.147</td><td>...</td><td>...</td><td>-0.346</td></tr><tr><td>GJ 3340</td><td>11.542</td><td>1.070</td><td>3713 ± 100</td><td>dM2</td><td>44.54 ± 4.06</td><td>9.786 ± 0.194</td><td>0.475 ± 0.081</td><td>2.67</td><td>9.00-2.91 + 4.59</td><td>-0.048</td></tr><tr><td>GJ 3215</td><td>11.779</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>46.29 ± 2.98</td><td>10.106 ± 0.140</td><td>0.450 ± 0.065</td><td>...</td><td>...</td><td>-0.314</td></tr><tr><td>GJ 3440</td><td>11.75</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>44 ± 8</td><td>9.967 ± 0.383</td><td>0.479 ± 0.127</td><td>2.71</td><td>8.95-3.56 + 5.59</td><td>-0.165</td></tr><tr><td>GJ 3759</td><td>10.929</td><td>1.090</td><td>3694 ± 100</td><td>dM2</td><td>58.94 ± 2.40</td><td>9.781 ± 0.092</td><td>0.487 ± 0.057</td><td>2.71</td><td>9.10-2.52 + 3.95</td><td>-0.121</td></tr><tr><td>GJ 3778</td><td>11.9</td><td>1.186</td><td>3600 ± 100</td><td>dM2</td><td>44 ± 8</td><td>10.117 ± 0.463</td><td>0.471 ± 0.133</td><td>1.72</td><td>13.86-6.49 + 13.4</td><td>+0.002</td></tr><tr><td>GJ 3915</td><td>11.65</td><td>1.132</td><td>3654 ± 100</td><td>dM2</td><td>26 ± 8</td><td>8.725 ± 0.603</td><td>0.836 ± 0.340</td><td>1.88</td><td>22.51-12.4 + 24.0</td><td>+0.413</td></tr><tr><td>GJ 4155</td><td>12.10</td><td>1.184</td><td>3602 ± 100</td><td>dM2</td><td>44 ± 8</td><td>10.317 ± 0.383</td><td>0.425 ± 0.121</td><td>...</td><td>...</td><td>-0.231</td></tr><tr><td>GJ 9381</td><td>11.56</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>38.05 ± 2.85</td><td>9.462 ± 0.177</td><td>0.606 ± 0.099</td><td>2.19</td><td>14.01-4.81 + 8.44</td><td>+0.100</td></tr><tr><td>GL 2</td><td>9.949</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>87.0 ± 1.41</td><td>9.647 ± 0.040</td><td>0.531 ± 0.049</td><td>2.76</td><td>9.74-2.48 + 3.85</td><td>-0.018</td></tr><tr><td>Gl 15A</td><td>8.13</td><td>1.130</td><td>3656 ± 100</td><td>dM2</td><td>278.76 ± 0.77</td><td>10.356 ± 0.026</td><td>0.392 ± 0.033</td><td>1.43</td><td>13.87-4.92 + 12.0</td><td>-0.386</td></tr><tr><td>Gl 16</td><td>10.864</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>61.21 ± 2.12</td><td>9.798 ± 0.079</td><td>0.519 ± 0.057</td><td>2.34</td><td>11.23-3.27 + 5.53</td><td>-0.105</td></tr><tr><td>GL 27.1</td><td>11.401</td><td>1.078</td><td>3705 ± 100</td><td>dM2</td><td>43.64 ± 2.59</td><td>9.609 ± 0.145</td><td>0.520 ± 0.075</td><td>2.63</td><td>10.01-3.03 + 4.83</td><td>-0.016</td></tr><tr><td>Gl 29.1A</td><td>11.11</td><td>1.136</td><td>3650 ± 100</td><td>dM2e</td><td>42.0 ± 2.0</td><td>9.226 ± 0.121</td><td>0.661 ± 0.084</td><td>10.6</td><td>3.16-0.64 + 0.77</td><td>+0.101</td></tr><tr><td>Gl 29.1B</td><td>11.11</td><td>1.136</td><td>3650 ± 100</td><td>dM2e</td><td>42.0 ± 2.0</td><td>9.226 ± 0.121</td><td>0.661 ± 0.084</td><td>9.5</td><td>3.52-0.74 + 0.91</td><td>+0.101</td></tr><tr><td>Gl 49</td><td>9.564</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>99.4 ± 1.4</td><td>9.551 ± 0.035</td><td>0.582 ± 0.051</td><td>2.49</td><td>11.83-3.13 + 5.12</td><td>+0.026</td></tr><tr><td>Gl 63</td><td>11.22</td><td>1.10</td><td>3685 ± 100</td><td>dM2</td><td>61.0 ± 8</td><td>10.167 ± 0.288</td><td>0.413 ± 0.092</td><td>&lt;1</td><td>&gt;20.90</td><td>-0.309</td></tr><tr><td>Gl 87</td><td>10.042</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>96.02 ± 1.66</td><td>9.954 ± 0.042</td><td>0.462 ± 0.043</td><td>3.99</td><td>5.86-1.24 + 1.68</td><td>-0.027</td></tr><tr><td>Gl 91</td><td>10.324</td><td>1.175</td><td>3611 ± 100</td><td>dM2</td><td>79.68 ± 1.69</td><td>9.831 ± 0.051</td><td>0.525 ± 0.053</td><td>1.68</td><td>15.82-5.34 + 11.3</td><td>-0.090</td></tr><tr><td>GL 114.1A</td><td>10.717</td><td>1.181</td><td>3605 ± 100</td><td>dM2</td><td>77.19 ± 1.64</td><td>10.155 ± 0.051</td><td>0.456 ± 0.046</td><td>1.82</td><td>12.68-4.11 + 8.14</td><td>-0.242</td></tr><tr><td>Gl 130</td><td>11.51</td><td>1.160</td><td>3626 ± 100</td><td>sdM2</td><td>70 ± 7</td><td>10.735 ± 0.227</td><td>0.341 ± 0.060</td><td>1.27</td><td>13.59-5.98 + 16.7</td><td>-0.766</td></tr><tr><td>Gl 133</td><td>11.21</td><td>1.208</td><td>3579 ± 100</td><td>dM2</td><td>71.21 ± 1.56</td><td>10.473 ± 0.067</td><td>0.409 ± 0.045</td><td>&lt;1</td><td>&gt;20.70</td><td>-0.466</td></tr><tr><td>Gl 134</td><td>10.29</td><td>1.124</td><td>3662 ± 100</td><td>dM2</td><td>57.8 ± 2.20</td><td>9.100 ± 0.101</td><td>0.695 ± 0.078</td><td>2.53</td><td>13.90-3.93 + 6.37</td><td>+0.128</td></tr><tr><td>Gl 140AB</td><td>10.422</td><td>1.160</td><td>3626 ± 100</td><td>dM2</td><td>51.31 ± 4.66</td><td>9.726 ± 0.194</td><td>0.544 ± 0.094</td><td>9.4</td><td>2.93-0.74 + 0.92</td><td>-0.002</td></tr><tr><td>Gl 150.1B</td><td>10.763</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>59.92 ± 2.39</td><td>9.651 ± 0.090</td><td>0.531 ± 0.062</td><td>3.7</td><td>7.26-1.74 + 2.42</td><td>-0.084</td></tr><tr><td>Gl 153B</td><td>10.79</td><td>1.16</td><td>3626 ± 100</td><td>dM2</td><td>57.5 ± 2.68</td><td>9.588 ± 0.119</td><td>0.580 ± 0.077</td><td>1.4</td><td>20.97-8.24 + 20.6</td><td>+0.017</td></tr><tr><td>Gl 155.1</td><td>11.044</td><td>1.063</td><td>3719 ± 100</td><td>dM2</td><td>59.36 ± 2.42</td><td>9.911 ± 0.092</td><td>0.444 ± 0.052</td><td>2.93</td><td>7.67-2.05 + 3.10</td><td>+0.175</td></tr><tr><td>Gl 162</td><td>10.17</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>74.37 ± 2.71</td><td>9.527 ± 0.098</td><td>0.539 ± 0.065</td><td>2.35</td><td>11.61-3.48 + 5.86</td><td>+0.019</td></tr><tr><td>Gl 173</td><td>10.331</td><td>1.196</td><td>3590 ± 100</td><td>dM2</td><td>90.10 ± 1.74</td><td>10.105 ± 0.047</td><td>0.477 ± 0.048</td><td>2.35</td><td>10.27-2.91 + 4.91</td><td>-0.225</td></tr><tr><td>Gl 191</td><td>8.853</td><td>1.058</td><td>3724 ± 100</td><td>sdM2</td><td>255.66 ± 0.91</td><td>10.891 ± 0.013</td><td>0.281 ± 0.022</td><td>9.15</td><td>1.55-0.26 + 0.33</td><td>-1.024</td></tr><tr><td>Gl 205</td><td>7.967</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>176.77 ± 1.18</td><td>9.204 ± 0.019</td><td>0.643 ± 0.052</td><td>2.73</td><td>11.92-2.94 + 4.59</td><td>+0.101</td></tr><tr><td>Gl 212</td><td>9.779</td><td>1.052</td><td>3729 ± 100</td><td>dM2</td><td>80.40 ± 1.69</td><td>9.298 ± 0.051</td><td>0.581 ± 0.056</td><td>1.98</td><td>14.85-4.55 + 8.51</td><td>+0.067</td></tr><tr><td>Gl 218</td><td>10.736</td><td>1.151</td><td>3635 ± 100</td><td>dM2</td><td>66.54 ± 1.43</td><td>9.851 ± 0.051</td><td>0.508 ± 0.049</td><td>1.66</td><td>15.49-5.21 + 11.1</td><td>-0.099</td></tr><tr><td>Gl 229</td><td>8.125</td><td>1.064</td><td>3718 ± 100</td><td>dM2</td><td>173.81 ± 0.99</td><td>9.325 ± 0.017</td><td>0.583 ± 0.046</td><td>2.63</td><td>11.22-2.80 + 4.46</td><td>+0.060</td></tr><tr><td>Gl 250B</td><td>10.05</td><td>1.268</td><td>3526 ± 100</td><td>dM2</td><td>108.9 ± 5.4</td><td>10.235 ± 0.125</td><td>0.495 ± 0.070</td><td>...</td><td>...</td><td>-0.247</td></tr><tr><td>Gl 275.1</td><td>10.84</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>39.75 ± 2.28</td><td>8.837 ± 0.141</td><td>0.740 ± 0.106</td><td>2.7</td><td>13.87-4.14 + 6.51</td><td>+0.172</td></tr><tr><td>Gl 289</td><td>11.418</td><td>1.148</td><td>3638 ± 100</td><td>sdM2</td><td>67.69 ± 2.65</td><td>10.571 ± 0.088</td><td>0.363 ± 0.042</td><td>&lt;1</td><td>&gt;18.37</td><td>-0.741</td></tr><tr><td>Gl 330</td><td>10.593</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>58.79 ± 2.72</td><td>9.440 ± 0.103</td><td>0.580 ± 0.071</td><td>3.05</td><td>9.62-2.57 + 3.82</td><td>+0.023</td></tr><tr><td>Gl 361</td><td>10.370</td><td>1.208</td><td>3579 ± 100</td><td>dM2</td><td>88.81 ± 1.68</td><td>10.112 ± 0.046</td><td>0.483 ± 0.048</td><td>1.95</td><td>12.54-3.90 + 7.37</td><td>-0.212</td></tr><tr><td>Gl 366</td><td>10.635</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>61.68 ± 1.42</td><td>9.586 ± 0.054</td><td>0.547 ± 0.054</td><td>&lt;1</td><td>&gt;27.69</td><td>-0.014</td></tr></tbody></table>
<table><caption>Table 3
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>M<sub>v</sub><br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>km s<sup>-1</sup></th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th></tr></thead><tbody><tr><td>Gl 378</td><td>10.11</td><td>1.256</td><td>3537 ± 100</td><td>dM2</td><td>67.1 ± 1.7</td><td>9.244 ± 0.074</td><td>0.769 ± 0.088</td><td>2.25</td><td>17.30-5.20 + 8.99</td><td>+0.096</td></tr><tr><td>Gl 382</td><td>9.264</td><td>1.184</td><td>3602 ± 100</td><td>dM2</td><td>127.08 ± 1.90</td><td>9.784 ± 0.037</td><td>0.544 ± 0.051</td><td>2.9</td><td>9.49-2.37 + 3.60</td><td>-0.059</td></tr><tr><td>Gl 390</td><td>10.139</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>81.00 ± 1.91</td><td>9.681 ± 0.056</td><td>0.524 ± 0.052</td><td>2.46</td><td>10.78-2.97 + 4.89</td><td>-0.030</td></tr><tr><td>Gl 411</td><td>7.508</td><td>1.184</td><td>3602 ± 100</td><td>dM2</td><td>392.64 ± 0.67</td><td>10.478 ± 0.0087</td><td>0.395 ± 0.032</td><td>0.61</td><td>32.77-11.9 + 30.8</td><td>-0.442</td></tr><tr><td>Gl 412A</td><td>8.798</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>206.27 ± 1.00</td><td>10.370 ± 0.015</td><td>0.365 ± 0.029</td><td>1.6</td><td>11.55-3.82 + 8.40</td><td>-0.435</td></tr><tr><td>Gl 430.1</td><td>10.270</td><td>1.060</td><td>3722 ± 100</td><td>dM2</td><td>62.92 ± 1.45</td><td>9.264 ± 0.054</td><td>0.597 ± 0.058</td><td>0.46</td><td>65.7-28.3 + 108</td><td>+0.089</td></tr><tr><td>Gl 433</td><td>9.813</td><td>1.160</td><td>3626 ± 100</td><td>dM2</td><td>112.58 ± 1.44</td><td>10.070 ± 0.032</td><td>0.465 ± 0.041</td><td>&lt;1</td><td>&gt;23.54</td><td>-0.199</td></tr><tr><td>Gl 450</td><td>9.762</td><td>1.136</td><td>3650 ± 100</td><td>dM2</td><td>116.48 ± 1.19</td><td>10.093 ± 0.027</td><td>0.446 ± 0.038</td><td>2.47</td><td>9.14-2.41 + 3.96</td><td>-0.247</td></tr><tr><td>Gl 477</td><td>11.092</td><td>1.190</td><td>3596 ± 100</td><td>dM2</td><td>52.67 ± 3.05</td><td>9.700 ± 0.127</td><td>0.570 ± 0.080</td><td>1.95</td><td>14.79-5.07 + 9.57</td><td>-0.057</td></tr><tr><td>Gl 490A</td><td>10.57</td><td>1.088</td><td>3696 ± 100</td><td>dM2e</td><td>51.93 ± 3.00</td><td>9.178 ± 0.142</td><td>0.642 ± 0.092</td><td>8.4</td><td>3.87-0.91 + 1.15</td><td>+0.078</td></tr><tr><td>Gl 494AB</td><td>9.757</td><td>1.112</td><td>3674 ± 100</td><td>dM2e</td><td>85.54 ± 1.53</td><td>10.171 ± 0.043</td><td>0.418 ± 0.039</td><td>9.75</td><td>2.17-0.39 + 0.47</td><td>-0.339</td></tr><tr><td>Gl 507.1</td><td>10.617</td><td>1.160</td><td>3626 ± 100</td><td>dM2</td><td>58.86 ± 1.49</td><td>9.466 ± 0.059</td><td>0.614 ± 0.062</td><td>2.32</td><td>13.39-3.83 + 6.49</td><td>+0.065</td></tr><tr><td>Gl 508.2</td><td>10.66</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>62.33 ± 1.76</td><td>9.633 ± 0.080</td><td>0.528 ± 0.058</td><td>1.78</td><td>15.01-5.01 + 10.1</td><td>-0.002</td></tr><tr><td>Gl 510</td><td>11.015</td><td>1.172</td><td>3614 ± 100</td><td>dM2</td><td>59.72 ± 2.43</td><td>9.896 ± 0.092</td><td>0.508 ± 0.062</td><td>2.49</td><td>10.33-3.02 + 4.93</td><td>-0.162</td></tr><tr><td>Gl 514</td><td>9.039</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>130.62 ± 1.05</td><td>9.619 ± 0.022</td><td>0.516 ± 0.042</td><td>2.07</td><td>12.62-3.63 + 6.59</td><td>-0.030</td></tr><tr><td>Gl 521</td><td>10.243</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>76.87 ± 1.61</td><td>9.672 ± 0.050</td><td>0.518 ± 0.050</td><td>0.85</td><td>30.84-9.69 + 18.7</td><td>-0.017</td></tr><tr><td>Gl 526</td><td>8.464</td><td>1.124</td><td>3662 ± 100</td><td>dM2</td><td>185.49 ± 1.10</td><td>9.806 ± 0.018</td><td>0.502 ± 0.040</td><td>1.00</td><td>25.41-6.99 + 12.1</td><td>-0.086</td></tr><tr><td>Gl 536</td><td>9.707</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>99.72 ± 1.57</td><td>9.701 ± 0.039</td><td>0.519 ± 0.047</td><td>&lt;1</td><td>&gt;26.27</td><td>-0.032</td></tr><tr><td>Gl 537AB</td><td>9.16</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>89.1 ± 4.3</td><td>9.662 ± 0.122</td><td>0.506 ± 0.067</td><td>3.6</td><td>7.11-1.82 + 2.55</td><td>-0.046</td></tr><tr><td>Gl 540</td><td>10.37</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>59.10 ± 1.18</td><td>9.228 ± 0.063</td><td>0.618 ± 0.063</td><td>2.09</td><td>14.97-4.52 + 8.16</td><td>+0.073</td></tr><tr><td>Gl 552</td><td>10.676</td><td>1.208</td><td>3579 ± 100</td><td>dM2</td><td>71.39 ± 2.10</td><td>9.944 ± 0.068</td><td>0.522 ± 0.058</td><td>0.58</td><td>45.55-17.9 + 49.1</td><td>-0.100</td></tr><tr><td>Gl 563.2A</td><td>11.656</td><td>1.124</td><td>3662 ± 100</td><td>sdM2</td><td>235.2 ± 22.4</td><td>13.513 ± 0.202</td><td>0.091 ± 0.016</td><td>2.24</td><td>2.06-0.72 + 1.24</td><td>-1.742</td></tr><tr><td>Gl 563.2B</td><td>12.066</td><td>1.196</td><td>3590 ± 100</td><td>sdM2</td><td>221.8 ± 22.4</td><td>13.796 ± 0.214</td><td>0.087 ± 0.016</td><td>1.82</td><td>2.42-0.93 + 1.85</td><td>-1.754</td></tr><tr><td>Gl 618.4</td><td>11.783</td><td>1.156</td><td>3630 ± 100</td><td>dM2</td><td>41.77 ± 3.59</td><td>9.887 ± 0.184</td><td>0.503 ± 0.084</td><td>1.45</td><td>17.56-7.21 + 17.4</td><td>-0.119</td></tr><tr><td>Gl 634</td><td>11.58</td><td>1.184</td><td>3602 ± 100</td><td>dM2</td><td>54 ± 5</td><td>10.242 ± 0.212</td><td>0.440 ± 0.082</td><td>&lt;0.6</td><td>&gt;37.12</td><td>-0.303</td></tr><tr><td>Gl 637</td><td>11.326</td><td>1.105</td><td>3681 ± 100</td><td>dM2</td><td>62.97 ± 1.99</td><td>10.322 ± 0.073</td><td>0.387 ± 0.042</td><td>2.19</td><td>8.94-2.68 + 4.71</td><td>-0.415</td></tr><tr><td>Gl 645</td><td>11.44</td><td>1.122</td><td>3664 ± 100</td><td>dM2</td><td>55 ± 6</td><td>10.142 ± 0.245</td><td>0.429 ± 0.086</td><td>2.80</td><td>7.75-2.64 + 4.09</td><td>-0.257</td></tr><tr><td>Gl 649</td><td>9.676</td><td>1.088</td><td>3696 ± 100</td><td>dM2</td><td>96.67 ± 1.39</td><td>9.602 ± 0.036</td><td>0.528 ± 0.047</td><td>2.27</td><td>11.77-3.29 + 5.65</td><td>-0.020</td></tr><tr><td>Gl 654AB</td><td>10.071</td><td>1.172</td><td>3614 ± 100</td><td>dM2</td><td>94.59 ± 1.85</td><td>9.950 ± 0.047</td><td>0.495 ± 0.049</td><td>5.7</td><td>4.40-1.02 + 1.46</td><td>-0.090</td></tr><tr><td>Gl 672.1</td><td>11.635</td><td>1.119</td><td>3667 ± 100</td><td>dM2</td><td>41.78 ± 4.12</td><td>9.740 ± 0.209</td><td>0.514 ± 0.092</td><td>2.99</td><td>8.70-2.75 + 4.13</td><td>-0.086</td></tr><tr><td>Gl 686</td><td>9.599</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>123.67 ± 1.61</td><td>10.060 ± 0.033</td><td>0.440 ± 0.038</td><td>2.49</td><td>8.94-2.35 + 3.85</td><td>-0.245</td></tr><tr><td>Gl 701</td><td>9.367</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>128.89 ± 1.43</td><td>9.918 ± 0.029</td><td>0.463 ± 0.040</td><td>1.6</td><td>14.65-4.91 + 10.8</td><td>-0.169</td></tr><tr><td>Gl 724</td><td>10.630</td><td>1.088</td><td>3696 ± 100</td><td>dM2</td><td>61.15 ± 2.07</td><td>9.562 ± 0.077</td><td>0.538 ± 0.059</td><td>2.97</td><td>9.17-2.37 + 3.58</td><td>-0.005</td></tr><tr><td>Gl 737B</td><td>10.13</td><td>1.094</td><td>3691 ± 100</td><td>dM2</td><td>69 ± 8</td><td>9.324 ± 0.258</td><td>0.604 ± 0.125</td><td>...</td><td>...</td><td>+0.134</td></tr><tr><td>Gl 745A</td><td>10.774</td><td>1.196</td><td>3590 ± 100</td><td>sdM2</td><td>117.45 ± 2.28</td><td>11.123 ± 0.047</td><td>0.298 ± 0.030</td><td>3.0</td><td>5.03-1.25 + 1.89</td><td>-1.03</td></tr><tr><td>Gl 745B</td><td>10.771</td><td>1.196</td><td>3590 ± 100</td><td>sdM2</td><td>114.25 ± 2.30</td><td>11.060 ± 0.048</td><td>0.307 ± 0.031</td><td>2.8</td><td>5.55-1.44 + 2.22</td><td>-1.07</td></tr><tr><td>Gl 767A</td><td>9.760</td><td>1.148</td><td>3638 ± 100</td><td>dM2</td><td>74.9 ± 2.9</td><td>9.132 ± 0.087</td><td>0.705 ± 0.082</td><td>2.9</td><td>12.30-3.29 + 5.01</td><td>+0.126</td></tr><tr><td>Gl 781</td><td>11.975</td><td>1.064</td><td>3718 ± 100</td><td>sdM2e</td><td>63.17 ± 3.82</td><td>10.978 ± 0.132</td><td>0.272 ± 0.038</td><td>12.7</td><td>1.08-0.22 + 0.25</td><td>-1.10</td></tr><tr><td>Gl 800A</td><td>10.735</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>55.72 ± 2.38</td><td>9.465 ± 0.096</td><td>0.570 ± 0.068</td><td>2.34</td><td>12.33-3.68 + 6.22</td><td>-0.113</td></tr><tr><td>Gl 803</td><td>8.794</td><td>1.100</td><td>3685 ± 100</td><td>PMS M2e</td><td>100.91 ± 1.06</td><td>8.814 ± 0.028</td><td>0.770 ± 0.065</td><td>9.68</td><td>4.03-0.68 + 0.84</td><td>+0.154</td></tr><tr><td>Gl 806</td><td>10.79</td><td>1.196</td><td>3590 ± 100</td><td>dM2</td><td>81.17 ± 1.73</td><td>10.305 ± 0.063</td><td>0.435 ± 0.047</td><td>0.46</td><td>47.86-20.9 + 80.5</td><td>-0.336</td></tr><tr><td>Gl 808</td><td>11.86</td><td>1.184</td><td>3602 ± 100</td><td>sdM2</td><td>56 ± 8</td><td>10.591 ± 0.310</td><td>0.375 ± 0.090</td><td>1.27</td><td>14.94-7.23 + 20.1</td><td>-0.882</td></tr><tr><td>Gl 809</td><td>8.575</td><td>1.064</td><td>3718 ± 100</td><td>dM2</td><td>141.87 ± 0.64</td><td>9.336 ± 0.022</td><td>0.580 ± 0.047</td><td>2.66</td><td>11.04-2.76 + 4.36</td><td>+0.067</td></tr><tr><td>Gl 815AB</td><td>10.12</td><td>1.184</td><td>3602 ± 100</td><td>dM2e</td><td>65.40 ± 1.84</td><td>9.951 ± 0.080</td><td>0.503 ± 0.059</td><td>7.61</td><td>3.35-0.73 + 0.95</td><td>-0.167</td></tr><tr><td>Gl 821</td><td>10.869</td><td>1.112</td><td>3674 ± 100</td><td>sdM2</td><td>82.18 ± 2.17</td><td>10.443 ± 0.059</td><td>0.369 ± 0.037</td><td>2.63</td><td>7.10-1.89 + 3.02</td><td>-0.484</td></tr><tr><td>Gl 832</td><td>8.663</td><td>1.196</td><td>3590 ± 100</td><td>dM2</td><td>201.87 ± 1.01</td><td>10.195 ± 0.019</td><td>0.458 ± 0.039</td><td>...</td><td>...</td><td>-0.268</td></tr><tr><td>Gl 842</td><td>9.737</td><td>1.039</td><td>3741 ± 100</td><td>dM2</td><td>84.26 ± 1.74</td><td>9.365 ± 0.049</td><td>0.556 ± 0.053</td><td>2.80</td><td>10.05-2.56 + 3.96</td><td>+0.050</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>M<sub>v</sub><br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>km s<sup>-1</sup></th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th></tr></thead><tbody><tr><td>Gl 855</td><td>10.708</td><td>1.052</td><td>3729 ± 100</td><td>dM2</td><td>51.57 ± 1.98</td><td>9.270 ± 0.087</td><td>0.589 ± 0.067</td><td>2.99</td><td>9.97-2.61 + 3.92</td><td>+0.049</td></tr><tr><td>Gl 863</td><td>10.373</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>78.68 ± 2.69</td><td>9.852 ± 0.078</td><td>0.464 ± 0.051</td><td>2.64</td><td>8.90-2.44 + 3.88</td><td>-0.132</td></tr><tr><td>Gl 867A</td><td>9.074</td><td>1.196</td><td>3590 ± 100</td><td>dM2e</td><td>115.01 ± 1.32</td><td>9.378 ± 0.030</td><td>0.667 ± 0.061</td><td>7.02</td><td>4.81-0.98 + 1.31</td><td>+0.080</td></tr><tr><td>Gl 880</td><td>8.657</td><td>1.124</td><td>3662 ± 100</td><td>dM2</td><td>146.09 ± 1.00</td><td>9.480 ± 0.020</td><td>0.583 ± 0.047</td><td>2.07</td><td>14.25-4.09 + 7.43</td><td>+0.040</td></tr><tr><td>Gl 887</td><td>7.351</td><td>1.088</td><td>3696 ± 100</td><td>dM2</td><td>305.26 ± 0.70</td><td>9.765 ± 0.011</td><td>0.490 ± 0.037</td><td>...</td><td>...</td><td>-0.092</td></tr><tr><td>Gl 895</td><td>10.033</td><td>1.112</td><td>3674 ± 100</td><td>dM2</td><td>77.15 ± 1.29</td><td>9.470 ± 0.041</td><td>0.577 ± 0.053</td><td>0.52</td><td>56.16-22.6 + 71.4</td><td>+0.049</td></tr><tr><td>Gl 908</td><td>8.993</td><td>1.100</td><td>3685 ± 100</td><td>dM2</td><td>167.29 ± 1.23</td><td>10.110 ± 0.017</td><td>0.424 ± 0.033</td><td>2.25</td><td>9.54-2.59 + 4.48</td><td>-0.271</td></tr><tr><td>St 497</td><td>10.59</td><td>1.112</td><td>3674 ± 100</td><td>dM2e</td><td>68 ± 12</td><td>9.753 ± 0.373</td><td>0.507 ± 0.138</td><td>6.5</td><td>3.95-1.45 + 1.98</td><td>-0.027</td></tr><tr><td>St 928</td><td>10.85</td><td>1.136</td><td>3650 ± 100</td><td>dM2</td><td>68 ± 12</td><td>10.013 ± 0.373</td><td>0.463 ± 0.127</td><td>2.1</td><td>11.16-4.86 + 8.74</td><td>-0.176</td></tr><tr><td>G192-11A</td><td>10.255</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>73.89 ± 1.64</td><td>9.598 ± 0.053</td><td>0.521 ± 0.051</td><td>2.6</td><td>10.14-2.71 + 4.33</td><td>-0.009</td></tr><tr><td>MCC 354A</td><td>10.91</td><td>1.184</td><td>3602 ± 100</td><td>dM2</td><td>51.05 ± 1.75</td><td>9.450 ± 0.093</td><td>0.634 ± 0.078</td><td>2.47</td><td>12.99-3.82 + 6.27</td><td>+0.109</td></tr><tr><td>MCC 452</td><td>10.264</td><td>1.064</td><td>3718 ± 100</td><td>dM2</td><td>50.80 ± 3.74</td><td>9.793 ± 0.159</td><td>0.470 ± 0.071</td><td>...</td><td>...</td><td>+0.360</td></tr><tr><td>MCC 488</td><td>11.20</td><td>1.076</td><td>3707 ± 100</td><td>dM2</td><td>37.21 ± 2.45</td><td>9.053 ± 0.158</td><td>0.670 ± 0.102</td><td>3.2</td><td>10.60-3.03 + 4.43</td><td>+0.113</td></tr><tr><td>LHS 1155</td><td>12.65</td><td>1.196</td><td>3590 ± 100</td><td>dM2</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>

Note. We computed the projected rotational period *P*/sin*i* as well as [M/H] derived from the [M/H]–radius correlation (Paper XVII).
<table><caption>Table 4
Stellar Parameters and the Values of v sin i from HM and [M/H] Compiled from the Literature for Our Targets in Our List of dM3 Stars</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GJ 1046</td><td>11.595</td><td>1.292</td><td>3506 ± 100</td><td>dM3</td><td>71.06 ± 3.23</td><td>10.85 ± 0.101</td><td>0.385 ± 0.050</td><td>2.63</td><td>7.41-1.1 + 1.2</td><td>...</td><td>-0.078</td></tr><tr><td>GJ 1050</td><td>11.730</td><td>1.322</td><td>3484 ± 100</td><td>dM3</td><td>66 ± 13</td><td>10.83 ± 0.435</td><td>0.404 ± 0.128</td><td>0.59</td><td>34.4-18 + 310</td><td>-1.20</td><td>-0.035</td></tr><tr><td>GJ 1054B</td><td>13.095</td><td>1.363</td><td>3456 ± 100</td><td>dM3e</td><td>52.08 ± 2.13</td><td>11.68 ± 0.091</td><td>0.288 ± 0.036</td><td>32.13</td><td>0.45-0.07 + 0.08</td><td>-0.09</td><td>-0.323</td></tr><tr><td>GJ 1077AB</td><td>11.91</td><td>1.38</td><td>3444 ± 100</td><td>dM3</td><td>77.5 ± 11</td><td>12.11 ± 0.308</td><td>0.243 ± 0.060</td><td>...</td><td>...</td><td>-0.64</td><td>-0.499</td></tr><tr><td>GJ 1080</td><td>12.81</td><td>1.344</td><td>3469 ± 100</td><td>dM3</td><td>50 ± 3</td><td>11.30 ± 0.150</td><td>0.334 ± 0.052</td><td>...</td><td>...</td><td>-0.44</td><td>-0.187</td></tr><tr><td>GJ 1097</td><td>11.456</td><td>1.400</td><td>3431 ± 100</td><td>dM3</td><td>81.38 ± 2.49</td><td>11.01 ± 0.068</td><td>0.415 ± 0.048</td><td>&lt;0.5</td><td>&gt;41.91</td><td>-0.05</td><td>-0.033</td></tr><tr><td>GJ 1110AB</td><td>13.08</td><td>1.324</td><td>3482 ± 100</td><td>dM3</td><td>45.2 ± 3.2</td><td>12.11 ± 0.168</td><td>0.225 ± 0.037</td><td>...</td><td>...</td><td>-0.71</td><td>-0.579</td></tr><tr><td>GJ 1125</td><td>11.710</td><td>1.125</td><td>3661 ± 100</td><td>sdM3</td><td>103.46 ± 3.94</td><td>11.78 ± 0.085</td><td>0.202 ± 0.023</td><td>0.99</td><td>10.3-2.9 + 8.3</td><td>-0.16</td><td>-0.691</td></tr><tr><td>GJ 1146</td><td>13.57</td><td>1.388</td><td>3439 ± 100</td><td>sdM3</td><td>54.2 ± 4.2</td><td>12.24 ± 0.189</td><td>0.231 ± 0.041</td><td>...</td><td>...</td><td>-0.56</td><td>-0.552</td></tr><tr><td>GJ 1197</td><td>13.25</td><td>1.304</td><td>3496 ± 100</td><td>dM3</td><td>45.9 ± 3.7</td><td>11.56 ± 0.195</td><td>0.282 ± 0.051</td><td>...</td><td>...</td><td>-0.12</td><td>-0.342</td></tr><tr><td>GJ 1200AB</td><td>12.93</td><td>1.419</td><td>3415 ± 100</td><td>dM3</td><td>55.9 ± 3.3</td><td>12.42 ± 0.148</td><td>0.222 ± 0.035</td><td>...</td><td>...</td><td>-0.57</td><td>-0.592</td></tr><tr><td>GJ 1202</td><td>12.76</td><td>1.401</td><td>3430 ± 100</td><td>dM3</td><td>53.5 ± 2.9</td><td>11.40 ± 0.138</td><td>0.346 ± 0.053</td><td>...</td><td>...</td><td>-0.22</td><td>-0.166</td></tr><tr><td>GJ 1203</td><td>12.158</td><td>1.352</td><td>3463 ± 100</td><td>dM3</td><td>59.63 ± 3.55</td><td>11.04 ± 0.131</td><td>0.381 ± 0.056</td><td>0.82</td><td>23.5-7.1 + 18</td><td>...</td><td>-0.087</td></tr><tr><td>GJ 1209</td><td>12.25</td><td>1.300</td><td>3499 ± 100</td><td>dM3</td><td>58.2 ± 3.2</td><td>11.07 ± 0.140</td><td>0.351 ± 0.052</td><td>...</td><td>...</td><td>-0.12</td><td>-0.157</td></tr><tr><td>GJ 1212A</td><td>12.032</td><td>1.403</td><td>3428 ± 100</td><td>dM3</td><td>53.41 ± 4.76</td><td>11.42 ± 0.196</td><td>0.344 ± 0.063</td><td>0.69</td><td>25.3-9.6 + 57</td><td>...</td><td>-0.170</td></tr><tr><td>GJ 1212B</td><td>12.032</td><td>1.403</td><td>3428 ± 100</td><td>dM3</td><td>53.41 ± 4.76</td><td>11.42 ± 0.196</td><td>0.344 ± 0.063</td><td>0.90</td><td>19.3-7.1 + 13</td><td>...</td><td>-0.170</td></tr><tr><td>GJ 1271</td><td>11.704</td><td>1.298</td><td>3500 ± 100</td><td>dM3</td><td>47.52 ± 2.82</td><td>10.09 ± 0.131</td><td>0.552 ± 0.080</td><td>1.39</td><td>20.0-5.1 + 7.7</td><td>0.15</td><td>+0.127</td></tr><tr><td>GJ 1292</td><td>11.72</td><td>1.425</td><td>3410 ± 100</td><td>dM3</td><td>72.8 ± 2.7</td><td>11.03 ± 0.101</td><td>0.425 ± 0.056</td><td>...</td><td>...</td><td>0.89</td><td>-0.030</td></tr><tr><td>GJ 2121</td><td>12.280</td><td>1.386</td><td>3440 ± 100</td><td>dM3</td><td>44.58 ± 5.36</td><td>10.53 ± 0.264</td><td>0.508 ± 0.112</td><td>2.06</td><td>12.5-3.1 + 4.2</td><td>0.14</td><td>+0.059</td></tr><tr><td>GJ 3139</td><td>11.770</td><td>1.333</td><td>3476 ± 100</td><td>dM3</td><td>50.68 ± 2.53</td><td>10.29 ± 0.110</td><td>0.524 ± 0.071</td><td>0.90</td><td>29.4-7.8 + 14</td><td>0.47</td><td>+0.084</td></tr><tr><td>GJ 3160A</td><td>12.01</td><td>1.292</td><td>3506 ± 100</td><td>dM3</td><td>38.45 ± 3.15</td><td>10.69 ± 0.198</td><td>0.415 ± 0.071</td><td>0.95</td><td>22.0-6.2 + 9.9</td><td>-0.07</td><td>-0.033</td></tr><tr><td>GJ 3160B</td><td>12.01</td><td>1.292</td><td>3506 ± 100</td><td>dM3</td><td>38.45 ± 3.15</td><td>10.69 ± 0.198</td><td>0.415 ± 0.071</td><td>1.06</td><td>19.8-5.3 + 7.4</td><td>-0.07</td><td>-0.033</td></tr><tr><td>GJ 3189</td><td>12.67</td><td>1.318</td><td>3487 ± 100</td><td>sdM3</td><td>95.5 ± 10.9</td><td>12.57 ± 0.269</td><td>0.180 ± 0.040</td><td>1.42</td><td>6.43-1.8 + 1.6</td><td>-0.60</td><td>-0.801</td></tr><tr><td>GJ 3242</td><td>12.70</td><td>1.336</td><td>3474 ± 100</td><td>dM3</td><td>54 ± 10</td><td>11.36 ± 0.427</td><td>0.322 ± 0.101</td><td>...</td><td>...</td><td>0.18</td><td>-0.212</td></tr><tr><td>GJ 3279</td><td>11.8</td><td>1.324</td><td>3482 ± 100</td><td>dM3</td><td>65 ± 13</td><td>10.86 ± 0.640</td><td>0.399 ± 0.179</td><td>0.85</td><td>23.7-13 + 26</td><td>...</td><td>-0.045</td></tr><tr><td>GJ 3293</td><td>12.0</td><td>1.308</td><td>3493 ± 100</td><td>dM3</td><td>55 ± 9</td><td>10.70 ± 0.559</td><td>0.421 ± 0.166</td><td>0.85</td><td>25.0-12 + 25</td><td>0.11</td><td>-0.031</td></tr><tr><td>GJ 3404A</td><td>11.73</td><td>1.412</td><td>3421 ± 100</td><td>dM3</td><td>64 ± 9</td><td>10.76 ± 0.327</td><td>0.473 ± 0.122</td><td>0.90</td><td>26.5-9.8 + 17</td><td>0.12</td><td>-0.005</td></tr><tr><td>GJ 3412A</td><td>11.028</td><td>1.393</td><td>3435 ± 100</td><td>sdM3</td><td>95.43 ± 2.36</td><td>11.68 ± 0.056</td><td>0.301 ± 0.033</td><td>...</td><td>...</td><td>...</td><td>-0.280</td></tr><tr><td>GJ 3412B</td><td>11.028</td><td>1.393</td><td>3435 ± 100</td><td>sdM3</td><td>95.43 ± 2.36</td><td>11.68 ± 0.056</td><td>0.301 ± 0.033</td><td>...</td><td>...</td><td>...</td><td>-0.280</td></tr><tr><td>GJ 3447B</td><td>13.48</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>30.57 ± 3.72</td><td>10.92 ± 0.286</td><td>0.372 ± 0.085</td><td>...</td><td>...</td><td>-0.09</td><td>-0.108</td></tr><tr><td>GJ 3459</td><td>11.712</td><td>1.390</td><td>3437 ± 100</td><td>sdM3</td><td>94.31 ± 3.31</td><td>11.58 ± 0.078</td><td>0.314 ± 0.038</td><td>0.69</td><td>23.1-7.7 + 48</td><td>-0.20</td><td>-0.238</td></tr><tr><td>GJ 3501B</td><td>12.36</td><td>1.313</td><td>3490 ± 100</td><td>dM3</td><td>37.95 ± 2.70</td><td>10.26 ± 0.175</td><td>0.520 ± 0.088</td><td>...</td><td>...</td><td>-0.26</td><td>+0.078</td></tr><tr><td>GJ 3508</td><td>11.749</td><td>1.319</td><td>3486 ± 100</td><td>dM3</td><td>52.74 ± 3.69</td><td>10.36 ± 0.154</td><td>0.500 ± 0.079</td><td>...</td><td>...</td><td>-0.01</td><td>+0.047</td></tr><tr><td>GJ 3528</td><td>11.728</td><td>1.300</td><td>3499 ± 100</td><td>dM3</td><td>51.25 ± 3.72</td><td>10.28 ± 0.160</td><td>0.507 ± 0.081</td><td>0.90</td><td>28.4-8.1 + 15</td><td>...</td><td>+0.057</td></tr><tr><td>GJ 3553</td><td>13.335</td><td>1.394</td><td>3435 ± 100</td><td>sdM3</td><td>60.8 ± 4.2</td><td>12.25 ± 0.152</td><td>0.232 ± 0.037</td><td>...</td><td>...</td><td>-0.28</td><td>-0.548</td></tr><tr><td>GJ 3563</td><td>11.953</td><td>1.311</td><td>3491 ± 100</td><td>dM3</td><td>63.47 ± 3.54</td><td>10.97 ± 0.123</td><td>0.374 ± 0.053</td><td>0.85</td><td>22.2-6.3 + 14</td><td>...</td><td>-0.104</td></tr><tr><td>GJ 3598</td><td>12.46</td><td>1.292</td><td>3506 ± 100</td><td>dM3</td><td>45 ± 9</td><td>10.73 ± 0.460</td><td>0.408 ± 0.136</td><td>0.69</td><td>30.0-15 + 80</td><td>...</td><td>-0.035</td></tr><tr><td>GJ 3634</td><td>11.95</td><td>1.291</td><td>3507 ± 100</td><td>dM3</td><td>56 ± 11</td><td>10.69 ± 0.452</td><td>0.414 ± 0.136</td><td>0.85</td><td>24.6-11 + 22</td><td>-0.15</td><td>-0.033</td></tr><tr><td>GJ 3643</td><td>12.369</td><td>1.346</td><td>3467 ± 100</td><td>dM3</td><td>50.90 ± 4.58</td><td>10.90 ± 0.198</td><td>0.403 ± 0.073</td><td>1.00</td><td>20.4-5.7 + 9.0</td><td>-0.11</td><td>-0.036</td></tr><tr><td>GJ 3708A</td><td>11.709</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>79.43 ± 2.36</td><td>11.21 ± 0.067</td><td>0.366 ± 0.042</td><td>0.50</td><td>37.0-17 + ∞</td><td>-0.01</td><td>-0.122</td></tr><tr><td>GJ 3747</td><td>12.600</td><td>1.401</td><td>3430 ± 100</td><td>dM3</td><td>52 ± 13</td><td>11.18 ± 0.557</td><td>0.384 ± 0.152</td><td>...</td><td>...</td><td>-0.27</td><td>-0.080</td></tr><tr><td>GJ 3795</td><td>12.5</td><td>1.367</td><td>3453 ± 100</td><td>dM3</td><td>50 ± 12</td><td>10.99 ± 0.732</td><td>0.396 ± 0.202</td><td>...</td><td>...</td><td>0.18</td><td>-0.052</td></tr><tr><td>GJ 3810</td><td>12.730</td><td>1.413</td><td>3420 ± 100</td><td>dM3</td><td>48 ± 11</td><td>11.14 ± 0.509</td><td>0.398 ± 0.146</td><td>...</td><td>...</td><td>0.13</td><td>-0.047</td></tr><tr><td>GJ 3836</td><td>11.82</td><td>1.347</td><td>3467 ± 100</td><td>dM3</td><td>61.3 ± 4.6</td><td>10.76 ± 0.183</td><td>0.431 ± 0.075</td><td>...</td><td>...</td><td>0.18</td><td>-0.029</td></tr><tr><td>GJ 3842</td><td>11.79</td><td>1.313</td><td>3490 ± 100</td><td>dM3e</td><td>49 ± 10</td><td>10.24 ± 0.469</td><td>0.524 ± 0.177</td><td>...</td><td>...</td><td>0.03</td><td>+0.084</td></tr><tr><td>GJ 3846</td><td>12.257</td><td>1.399</td><td>3431 ± 100</td><td>sdM3</td><td>70.03 ± 4.89</td><td>11.48 ± 0.154</td><td>0.333 ± 0.053</td><td>0.82</td><td>20.5-6.4 + 16</td><td>-0.12</td><td>-0.189</td></tr><tr><td>GJ 3892</td><td>11.473</td><td>1.340</td><td>3472 ± 100</td><td>dM3</td><td>69.19 ± 2.60</td><td>10.67 ± 0.084</td><td>0.444 ± 0.054</td><td>0.82</td><td>27.4-7.6 + 20</td><td>...</td><td>-0.026</td></tr></tbody></table>
<table><caption>Table 4
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>c</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GJ 3895</td><td>13.45</td><td>1.427</td><td>3408 ± 100</td><td>dM3</td><td>42.3 ± 3.1</td><td>11.58 ± 0.179</td><td>0.331 ± 0.058</td><td>...</td><td>...</td><td>-0.24</td><td>-0.193</td></tr><tr><td>GJ 3916A</td><td>11.279</td><td>1.306</td><td>3495 ± 100</td><td>dM3</td><td>66.21 ± 3.18</td><td>11.13 ± 0.106</td><td>0.345 ± 0.045</td><td>1.24</td><td>14.1-3.1 + 3.8</td><td>0.02</td><td>-0.168</td></tr><tr><td>GJ 3916B</td><td>11.279</td><td>1.306</td><td>3495 ± 100</td><td>dM3</td><td>66.21 ± 3.18</td><td>11.13 ± 0.106</td><td>0.345 ± 0.045</td><td>3.51</td><td>4.97-0.7 + 0.7</td><td>0.02</td><td>-0.168</td></tr><tr><td>GJ 4004</td><td>12.1</td><td>1.455</td><td>3384 ± 100</td><td>sdM3</td><td>81 ± 16</td><td>11.64 ± 0.635</td><td>0.335 ± 0.151</td><td>0.59</td><td>28.6-18 + 290</td><td>...</td><td>-0.186</td></tr><tr><td>GJ 4026</td><td>12.67</td><td>1.408</td><td>3424 ± 100</td><td>dM3</td><td>69.2 ± 2.4</td><td>11.87 ± 0.095</td><td>0.282 ± 0.037</td><td>...</td><td>...</td><td>-0.34</td><td>-0.342</td></tr><tr><td>GJ 4048A</td><td>11.87</td><td>1.363</td><td>3456 ± 100</td><td>dM3</td><td>88.0 ± 3.6</td><td>11.59 ± 0.109</td><td>0.299 ± 0.040</td><td>...</td><td>...</td><td>-0.13</td><td>-0.287</td></tr><tr><td>GJ 4117</td><td>12.20</td><td>1.291</td><td>3507 ± 100</td><td>dM3</td><td>72.1 ± 7.3</td><td>11.49 ± 0.241</td><td>0.287 ± 0.058</td><td>...</td><td>...</td><td>0.78</td><td>-0.326</td></tr><tr><td>GJ 4129</td><td>11.95</td><td>1.304</td><td>3496 ± 100</td><td>dM3</td><td>63.1 ± 3.8</td><td>10.95 ± 0.151</td><td>0.374 ± 0.058</td><td>0.50</td><td>37.9-18 + ∞</td><td>-0.26</td><td>-0.104</td></tr><tr><td>GJ 4149</td><td>11.96</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>37.20 ± 10.98</td><td>9.81 ± 0.681</td><td>0.618 ± 0.293</td><td>...</td><td>...</td><td>0.04</td><td>+0.229</td></tr><tr><td>GJ 4176A</td><td>12.29</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>59 ± 8</td><td>11.14 ± 0.316</td><td>0.377 ± 0.094</td><td>...</td><td>...</td><td>-0.03</td><td>-0.096</td></tr><tr><td>GJ 4231</td><td>12.11</td><td>1.388</td><td>3439 ± 100</td><td>dM3e</td><td>64 ± 13</td><td>11.14 ± 0.467</td><td>0.384 ± 0.131</td><td>80.00</td><td>0.24-0.08 + 0.09</td><td>...</td><td>-0.080</td></tr><tr><td>GJ 4282AB</td><td>12.41</td><td>1.401</td><td>3430 ± 100</td><td>dM3e</td><td>59 ± 12</td><td>11.26 ± 0.468</td><td>0.369 ± 0.126</td><td>15.00</td><td>1.25-0.48 + 0.54</td><td>-0.16</td><td>-0.115</td></tr><tr><td>GJ 4368</td><td>11.50</td><td>1.362</td><td>3457 ± 100</td><td>dM3</td><td>77 ± 16</td><td>10.93 ± 0.478</td><td>0.405 ± 0.139</td><td>...</td><td>...</td><td>0.16</td><td>-0.035</td></tr><tr><td>GJ 9801B</td><td>13.52</td><td>1.407</td><td>3425 ± 100</td><td>dM3</td><td>37.25 ± 0.76</td><td>11.37 ± 0.064</td><td>0.354 ± 0.040</td><td>...</td><td>...</td><td>-0.23</td><td>-0.150</td></tr><tr><td>Gl 12</td><td>12.61</td><td>1.415</td><td>3418 ± 100</td><td>sdM3</td><td>84 ± 11</td><td>12.23 ± 0.306</td><td>0.241 ± 0.059</td><td>0.95</td><td>12.8-4.4 + 6.9</td><td>-0.26</td><td>-0.508</td></tr><tr><td>GL 48</td><td>9.99</td><td>1.363</td><td>3456 ± 100</td><td>dM3e</td><td>121.41 ± 1.25</td><td>10.41 ± 0.042</td><td>0.516 ± 0.052</td><td>2.45</td><td>10.7-2.9 + 4.9</td><td>0.04</td><td>+0.071</td></tr><tr><td>Gl 70</td><td>10.915</td><td>1.274</td><td>3521 ± 100</td><td>dM3</td><td>87.62 ± 2.00</td><td>10.63 ± 0.052</td><td>0.416 ± 0.043</td><td>1.01</td><td>20.8-5.4 + 10</td><td>-0.17</td><td>-0.033</td></tr><tr><td>GL 84</td><td>10.189</td><td>1.290</td><td>3507 ± 100</td><td>dM3</td><td>109.38 ± 1.92</td><td>10.38 ± 0.040</td><td>0.476 ± 0.047</td><td>...</td><td>...</td><td>-0.08</td><td>-0.094</td></tr><tr><td>GL 100C</td><td>12.84</td><td>1.351</td><td>3464 ± 100</td><td>dM3</td><td>51.16 ± 1.33</td><td>11.38 ± 0.076</td><td>0.324 ± 0.038</td><td>...</td><td>...</td><td>-0.28</td><td>-0.205</td></tr><tr><td>Gl 109</td><td>10.563</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>133.16 ± 2.26</td><td>11.18 ± 0.039</td><td>0.370 ± 0.037</td><td>1.34</td><td>13.9-3.2 + 4.8</td><td>-0.12</td><td>-0.113</td></tr><tr><td>GL 118.1B</td><td>12.97</td><td>1.357</td><td>3460 ± 100</td><td>dM3</td><td>34.58 ± 0.85</td><td>10.66 ± 0.073</td><td>0.455 ± 0.053</td><td>...</td><td>...</td><td>-0.10</td><td>-0.023</td></tr><tr><td>Gl 119B</td><td>11.65</td><td>1.313</td><td>3490 ± 100</td><td>dM3</td><td>44.8 ± 3.9</td><td>9.91 ± 0.201</td><td>0.610 ± 0.111</td><td>4.00</td><td>7.72-2.2 + 3.0</td><td>...</td><td>+0.217</td></tr><tr><td>GL 120AB</td><td>13.04</td><td>1.407</td><td>3425 ± 100</td><td>sdM3</td><td>54 ± 12</td><td>12.45 ± 0.456</td><td>0.215 ± 0.052</td><td>...</td><td>...</td><td>-0.57</td><td>-0.626</td></tr><tr><td>GL 121.1</td><td>11.792</td><td>1.304</td><td>3496 ± 100</td><td>dM3e</td><td>51.08 ± 3.99</td><td>10.33 ± 0.172</td><td>0.496 ± 0.083</td><td>...</td><td>...</td><td>-0.02</td><td>+0.040</td></tr><tr><td>Gl 140C</td><td>11.89</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>60 ± 8</td><td>10.78 ± 0.292</td><td>0.396 ± 0.092</td><td>6.70</td><td>2.99-1.0 + 1.3</td><td>...</td><td>-0.052</td></tr><tr><td>Gl 145</td><td>11.47</td><td>1.339</td><td>3472 ± 100</td><td>sdM3</td><td>93.11 ± 1.94</td><td>11.31 ± 0.065</td><td>0.330 ± 0.037</td><td>0.85</td><td>19.6-5.1 + 12</td><td>-0.28</td><td>-0.194</td></tr><tr><td>Gl 163</td><td>11.811</td><td>1.416</td><td>3417 ± 100</td><td>dM3</td><td>66.69 ± 1.82</td><td>10.93 ± 0.061</td><td>0.439 ± 0.049</td><td>0.85</td><td>26.0-6.8 + 16</td><td>-0.02</td><td>-0.027</td></tr><tr><td>GL 173.1B</td><td>14.19</td><td>1.401</td><td>3430 ± 100</td><td>dM3</td><td>32.69 ± 1.51</td><td>11.76 ± 0.120</td><td>0.293 ± 0.042</td><td>...</td><td>...</td><td>-0.33</td><td>-0.307</td></tr><tr><td>Gl 204.2</td><td>12.010</td><td>1.343</td><td>3470 ± 100</td><td>dM3</td><td>49 ± 5</td><td>10.46 ± 0.224</td><td>0.491 ± 0.096</td><td>0.69</td><td>36.1-14 + 83</td><td>...</td><td>+0.033</td></tr><tr><td>Gl 207.1</td><td>11.53</td><td>1.335</td><td>3475 ± 100</td><td>dM3e</td><td>62.75 ± 4.02</td><td>10.52 ± 0.159</td><td>0.474 ± 0.076</td><td>9.52</td><td>2.51-0.4 + 0.4</td><td>0.09</td><td>+0.006</td></tr><tr><td>Gl 226</td><td>10.50</td><td>1.309</td><td>3493 ± 100</td><td>dM3</td><td>106.69 ± 1.31</td><td>10.64 ± 0.047</td><td>0.434 ± 0.044</td><td>1.12</td><td>19.6-5.1 + 9.0</td><td>...</td><td>-0.028</td></tr><tr><td>GL 228AB</td><td>10.42</td><td>1.313</td><td>3490 ± 100</td><td>dM3</td><td>91.65 ± 3.50</td><td>10.98 ± 0.103</td><td>0.373 ± 0.049</td><td>...</td><td>...</td><td>-0.04</td><td>-0.106</td></tr><tr><td>Gl 238</td><td>11.592</td><td>1.331</td><td>3478 ± 100</td><td>dM3</td><td>60.77 ± 1.94</td><td>10.51 ± 0.071</td><td>0.473 ± 0.054</td><td>0.85</td><td>28.0-7.3 + 17</td><td>...</td><td>+0.005</td></tr><tr><td>Gl 251AB</td><td>10.01</td><td>1.425</td><td>3410 ± 100</td><td>sdM3</td><td>179.01 ± 1.60</td><td>12.03 ± 0.039</td><td>0.268 ± 0.038</td><td>1.14</td><td>16.9-4.4 + 7.5</td><td>-0.45</td><td>-0.388</td></tr><tr><td>GL 257AB</td><td>10.846</td><td>1.420</td><td>3414 ± 100</td><td>dM3e</td><td>124.85 ± 2.13</td><td>11.33 ± 0.039</td><td>0.368 ± 0.037</td><td>...</td><td>...</td><td>-0.15</td><td>-0.118</td></tr><tr><td>GL 268.3</td><td>10.87</td><td>1.388</td><td>3439 ± 100</td><td>dM3</td><td>93.09 ± 2.84</td><td>10.71 ± 0.086</td><td>0.467 ± 0.058</td><td>...</td><td>...</td><td>-0.14</td><td>-0.005</td></tr><tr><td>GL 277A</td><td>10.57</td><td>1.376</td><td>3447 ± 100</td><td>PMS M3e</td><td>84.26 ± 3.45</td><td>10.20 ± 0.109</td><td>0.583 ± 0.080</td><td>8.00</td><td>3.69-0.86 + 1.1</td><td>0.10</td><td>+0.175</td></tr><tr><td>GL 298</td><td>11.745</td><td>1.398</td><td>3432 ± 100</td><td>dM3</td><td>60.68 ± 2.48</td><td>10.66 ± 0.091</td><td>0.485 ± 0.062</td><td>1.00</td><td>24.6-5.7 + 9.2</td><td>...</td><td>+0.023</td></tr><tr><td>GL 319C</td><td>11.76</td><td>1.338</td><td>3473 ± 100</td><td>dM3</td><td>66.96 ± 3.91</td><td>10.89 ± 0.147</td><td>0.401 ± 0.062</td><td>...</td><td>...</td><td>0.04</td><td>-0.040</td></tr><tr><td>GL 326AB</td><td>11.89</td><td>1.390</td><td>3437 ± 100</td><td>dM3</td><td>77 ± 11</td><td>11.32 ± 0.332</td><td>0.354 ± 0.092</td><td>...</td><td>...</td><td>-0.25</td><td>-0.150</td></tr><tr><td>GL 333.2A</td><td>12.36</td><td>1.380</td><td>3444 ± 100</td><td>dM3</td><td>40.77 ± 6.57</td><td>10.41 ± 0.373</td><td>0.531 ± 0.151</td><td>...</td><td>...</td><td>0.01</td><td>+0.095</td></tr><tr><td>GL 333.2B</td><td>12.688</td><td>1.410</td><td>3422 ± 100</td><td>dM3</td><td>47.75 ± 7.95</td><td>11.08 ± 0.367</td><td>0.406 ± 0.114</td><td>...</td><td>...</td><td>0.01</td><td>-0.035</td></tr><tr><td>GL 347A</td><td>12.104</td><td>1.333</td><td>3476 ± 100</td><td>dM3e</td><td>61.58 ± 3.98</td><td>11.05 ± 0.143</td><td>0.370 ± 0.056</td><td>...</td><td>...</td><td>0.02</td><td>-0.113</td></tr><tr><td>GL 350B</td><td>14.27</td><td>1.338</td><td>3473 ± 100</td><td>dM3</td><td>29.51 ± 2.39</td><td>11.62 ± 0.196</td><td>0.286 ± 0.052</td><td>...</td><td>...</td><td>-0.03</td><td>-0.329</td></tr><tr><td>GL 352</td><td>10.067</td><td>1.336</td><td>3474 ± 100</td><td>dM3</td><td>99.88 ± 3.60</td><td>10.06 ± 0.080</td><td>0.585 ± 0.070</td><td>0.90</td><td>7.6-1.0 + 1.0</td><td>-0.01</td><td>+0.178</td></tr><tr><td>Gl 357</td><td>10.906</td><td>1.280</td><td>3516 ± 100</td><td>sdM3</td><td>110.82 ± 1.92</td><td>11.13 ± 0.040</td><td>0.333 ± 0.032</td><td>1.21</td><td>18.7-4.3 + 8.2</td><td>-0.19</td><td>-0.189</td></tr><tr><td>Gl 358</td><td>10.694</td><td>1.356</td><td>3461 ± 100</td><td>dM3e</td><td>105.63 ± 1.64</td><td>10.81 ± 0.036</td><td>0.425 ± 0.041</td><td>1.10</td><td>17.7-3.3 + 4.2</td><td>-0.01</td><td>-0.030</td></tr></tbody></table>
<table><caption>Table 4
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>c</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>Gl 377</td><td>11.440</td><td>1.364</td><td>3455 ± 100</td><td>dM3</td><td>61.39 ± 2.55</td><td>10.38 ± 0.092</td><td>0.524 ± 0.066</td><td>...</td><td>24.1-5.4 + 7.2</td><td>0.40</td><td>+0.084</td></tr><tr><td>Gl 381</td><td>10.629</td><td>1.274</td><td>3521 ± 100</td><td>dM3e</td><td>81.08 ± 2.87</td><td>10.17 ± 0.079</td><td>0.513 ± 0.060</td><td>...</td><td>...</td><td>-0.07</td><td>+0.067</td></tr><tr><td>Gl 386</td><td>10.998</td><td>1.329</td><td>3479 ± 100</td><td>dM3</td><td>73.30 ± 2.62</td><td>10.32 ± 0.080</td><td>0.514 ± 0.061</td><td>0.69</td><td>37.8-12 + 79</td><td>0.17</td><td>+0.068</td></tr><tr><td>Gl 388</td><td>9.32</td><td>1.420</td><td>3414 ± 100</td><td>dM3e</td><td>213.00 ± 4.00</td><td>10.96 ± 0.061</td><td>0.436 ± 0.049</td><td>2.63</td><td>8.38-1.1 + 1.2</td><td>0.08</td><td>-0.028</td></tr><tr><td>Gl 399</td><td>11.281</td><td>1.280</td><td>3516 ± 100</td><td>dM3</td><td>60.80 ± 3.14</td><td>10.20 ± 0.114</td><td>0.511 ± 0.069</td><td>0.59</td><td>43.6-17 + 330</td><td>0.15</td><td>+0.064</td></tr><tr><td>Gl 408</td><td>10.020</td><td>1.338</td><td>3473 ± 100</td><td>dM3</td><td>150.10 ± 1.70</td><td>10.90 ± 0.027</td><td>0.399 ± 0.037</td><td>1.12</td><td>18.1-4.6 + 8.1</td><td>-0.12</td><td>-0.045</td></tr><tr><td>Gl 414.1AB</td><td>10.88</td><td>1.351</td><td>3464 ± 100</td><td>dM3</td><td>59.16 ± 2.54</td><td>10.49 ± 0.113</td><td>0.490 ± 0.067</td><td>...</td><td>...</td><td>0.07</td><td>+0.031</td></tr><tr><td>Gl 422</td><td>11.516</td><td>1.395</td><td>3434 ± 100</td><td>dM3</td><td>78.91 ± 2.60</td><td>11.00 ± 0.074</td><td>0.413 ± 0.049</td><td>0.90</td><td>23.1-5.8 + 11</td><td>...</td><td>-0.033</td></tr><tr><td>Gl 436</td><td>10.66</td><td>1.351</td><td>3464 ± 100</td><td>dM3</td><td>98.8 ± 2.9</td><td>10.63 ± 0.084</td><td>0.458 ± 0.055</td><td>0.86</td><td>27.0-9.0 + 26</td><td>-0.02</td><td>-0.019</td></tr><tr><td>Gl 443</td><td>11.700</td><td>1.360</td><td>3458 ± 100</td><td>dM3</td><td>50.02 ± 3.10</td><td>10.20 ± 0.137</td><td>0.567 ± 0.084</td><td>0.90</td><td>31.8-8.7 + 16</td><td>0.35</td><td>+0.150</td></tr><tr><td>Gl 452A</td><td>11.894</td><td>1.363</td><td>3456 ± 100</td><td>dM3</td><td>51.10 ± 3.58</td><td>10.44 ± 0.154</td><td>0.510 ± 0.081</td><td>0.95</td><td>27.1-7.3 + 12</td><td>0.12</td><td>+0.062</td></tr><tr><td>Gl 452.1</td><td>12.74</td><td>1.424</td><td>3410 ± 100</td><td>sdM3e</td><td>92 ± 12</td><td>12.56 ± 0.305</td><td>0.210 ± 0.051</td><td>1.60</td><td>6.66-1.9 + 2.2</td><td>...</td><td>-0.651</td></tr><tr><td>Gl 455AB</td><td>12.83</td><td>1.419</td><td>3415 ± 100</td><td>dM3</td><td>55 ± 12</td><td>11.53 ± 0.502</td><td>0.237 ± 0.084</td><td>...</td><td>...</td><td>-1.10</td><td>-0.526</td></tr><tr><td>Gl 463</td><td>11.58</td><td>1.338</td><td>3473 ± 100</td><td>dM3</td><td>54.54 ± 2.03</td><td>10.26 ± 0.101</td><td>0.535 ± 0.069</td><td>1.17</td><td>23.1-6.4 + 10</td><td>...</td><td>+0.101</td></tr><tr><td>Gl 479</td><td>10.663</td><td>1.357</td><td>3460 ± 100</td><td>dM3</td><td>103.18 ± 2.31</td><td>10.73 ± 0.051</td><td>0.442 ± 0.046</td><td>1.06</td><td>21.1-4.4 + 6.3</td><td>0.54</td><td>-0.026</td></tr><tr><td>Gl 480</td><td>11.502</td><td>1.423</td><td>3411 ± 100</td><td>dM3</td><td>69.59 ± 2.79</td><td>10.71 ± 0.089</td><td>0.491 ± 0.062</td><td>0.73</td><td>34.0-12 + 53</td><td>0.15</td><td>+0.033</td></tr><tr><td>Gl 507B</td><td>12.12</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>75.38 ± 1.54</td><td>11.51 ± 0.064</td><td>0.319 ± 0.036</td><td>...</td><td>...</td><td>-0.14</td><td>-0.221</td></tr><tr><td>Gl 512A</td><td>11.336</td><td>1.394</td><td>3435 ± 100</td><td>dM3e</td><td>72.00 ± 2.83</td><td>10.62 ± 0.087</td><td>0.491 ± 0.062</td><td>...</td><td>...</td><td>0.12</td><td>+0.033</td></tr><tr><td>Gl 513</td><td>11.92</td><td>1.412</td><td>3421 ± 100</td><td>dM3</td><td>62.9 ± 6.7</td><td>10.91 ± 0.252</td><td>0.441 ± 0.094</td><td>0.77</td><td>29.0-11 + 39</td><td>-0.20</td><td>-0.027</td></tr><tr><td>Gl 581</td><td>10.56</td><td>1.409</td><td>3423 ± 100</td><td>dM3e</td><td>160.91 ± 2.62</td><td>11.59 ± 0.055</td><td>0.321 ± 0.035</td><td>...</td><td>...</td><td>-0.15</td><td>-0.215</td></tr><tr><td>Gl 588</td><td>9.311</td><td>1.326</td><td>3481 ± 100</td><td>dM3</td><td>168.66 ± 1.30</td><td>10.45 ± 0.019</td><td>0.484 ± 0.042</td><td>0.77</td><td>31.8-8.3 + 35</td><td>0.07</td><td>+0.022</td></tr><tr><td>Gl 589A</td><td>12.37</td><td>1.308</td><td>3493 ± 100</td><td>dM3</td><td>69 ± 3</td><td>11.56 ± 0.114</td><td>0.283 ± 0.039</td><td>...</td><td>...</td><td>-0.25</td><td>-0.339</td></tr><tr><td>Gl 595AB</td><td>11.855</td><td>1.410</td><td>3422 ± 100</td><td>sdM3</td><td>95.90 ± 5.59</td><td>11.76 ± 0.129</td><td>0.297 ± 0.044</td><td>1.62</td><td>9.25-2.1 + 2.8</td><td>-0.13</td><td>-0.293</td></tr><tr><td>Gl 617B</td><td>10.69</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>93.09 ± 1.48</td><td>10.53 ± 0.055</td><td>0.499 ± 0.054</td><td>1.12</td><td>22.6-6.0 + 11</td><td>-0.54</td><td>+0.045</td></tr><tr><td>Gl 618A</td><td>10.586</td><td>1.370</td><td>3451 ± 100</td><td>dM3</td><td>130.0 ± 8.2</td><td>11.16 ± 0.139</td><td>0.369 ± 0.055</td><td>0.82</td><td>22.8-6.9 + 18</td><td>-0.08</td><td>-0.115</td></tr><tr><td>Gl 623</td><td>10.26</td><td>1.300</td><td>3499 ± 100</td><td>dM3</td><td>124.12 ± 1.16</td><td>10.73 ± 0.040</td><td>0.412 ± 0.040</td><td>0.94</td><td>22.3-6.4 + 16</td><td>...</td><td>-0.034</td></tr><tr><td>Gl 634</td><td>12.73</td><td>1.376</td><td>3447 ± 100</td><td>sdM3</td><td>54 ± 5</td><td>11.39 ± 0.222</td><td>0.337 ± 0.066</td><td>1.00</td><td>17.1-5.0 + 7.8</td><td>...</td><td>-0.182</td></tr><tr><td>Gl 644A</td><td>9.023</td><td>1.370</td><td>3451 ± 100</td><td>dM3e</td><td>161.41 ± 5.64</td><td>10.81 ± 0.078</td><td>0.433 ± 0.051</td><td>1.79</td><td>12.2-2.0 + 2.2</td><td>-0.21</td><td>-0.029</td></tr><tr><td>Gl 644B</td><td>9.023</td><td>1.370</td><td>3451 ± 100</td><td>dM3e</td><td>161.41 ± 5.64</td><td>10.81 ± 0.078</td><td>0.433 ± 0.051</td><td>2.78</td><td>7.88-1.1 + 1.1</td><td>-0.21</td><td>-0.029</td></tr><tr><td>Gl 655</td><td>11.677</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>74.84 ± 3.07</td><td>11.05 ± 0.091</td><td>0.394 ± 0.050</td><td>&lt;0.5</td><td>&gt;39.88</td><td>...</td><td>-0.057</td></tr><tr><td>Gl 660A</td><td>11.393</td><td>1.425</td><td>3410 ± 100</td><td>dM3</td><td>98.19 ± 12.09</td><td>11.35 ± 0.271</td><td>0.367 ± 0.083</td><td>0.82</td><td>22.6-8.3 + 20</td><td>-0.22</td><td>-0.120</td></tr><tr><td>Gl 661AB</td><td>9.40</td><td>1.410</td><td>3422 ± 100</td><td>dM3</td><td>167.29 ± 5.02</td><td>11.27 ± 0.084</td><td>0.373 ± 0.066</td><td>...</td><td>...</td><td>-0.38</td><td>-0.106</td></tr><tr><td>Gl 671</td><td>11.37</td><td>1.326</td><td>3481 ± 100</td><td>dM3</td><td>80.77 ± 1.66</td><td>10.91 ± 0.065</td><td>0.392 ± 0.043</td><td>0.94</td><td>21.2-6.3 + 15</td><td>-0.15</td><td>-0.061</td></tr><tr><td>Gl 674</td><td>9.407</td><td>1.330</td><td>3478 ± 100</td><td>dM3</td><td>220.24 ± 1.42</td><td>11.12 ± 0.019</td><td>0.357 ± 0.031</td><td>0.90</td><td>20.0-4.5 + 8.6</td><td>-0.46</td><td>-0.143</td></tr><tr><td>Gl 687AB</td><td>9.22</td><td>1.410</td><td>3422 ± 100</td><td>dM3</td><td>220.84 ± 0.94</td><td>11.69 ± 0.029</td><td>0.434 ± 0.042</td><td>0.73</td><td>30.3-11 + 130</td><td>-0.01</td><td>-0.028</td></tr><tr><td>Gl 693</td><td>10.783</td><td>1.412</td><td>3421 ± 100</td><td>sdM3</td><td>171.48 ± 2.31</td><td>11.95 ± 0.031</td><td>0.273 ± 0.026</td><td>0.82</td><td>16.8-4.3 + 12</td><td>-0.30</td><td>-0.372</td></tr><tr><td>Gl 694</td><td>10.45</td><td>1.313</td><td>3490 ± 100</td><td>dM3</td><td>105.50 ± 1.18</td><td>10.57 ± 0.044</td><td>0.451 ± 0.045</td><td>1.29</td><td>17.7-4.2 + 6.2</td><td>-0.01</td><td>-0.024</td></tr><tr><td>Gl 712</td><td>12.60</td><td>1.413</td><td>3420 ± 100</td><td>dM3</td><td>72 ± 3</td><td>11.89 ± 0.111</td><td>0.282 ± 0.039</td><td>...</td><td>...</td><td>-0.48</td><td>-0.342</td></tr><tr><td>Gl 725AB</td><td>8.90</td><td>1.390</td><td>3437 ± 100</td><td>sdM3</td><td>280.18 ± 2.18</td><td>11.89 ± 0.037</td><td>0.273 ± 0.027</td><td>0.85</td><td>22.5-7.0 + 18.4</td><td>-0.57</td><td>-0.372</td></tr><tr><td>Gl 735A</td><td>10.194</td><td>1.368</td><td>3452 ± 100</td><td>dM3e</td><td>84.94 ± 1.72</td><td>10.59 ± 0.046</td><td>0.478 ± 0.048</td><td>1.86</td><td>13.0-2.0 + 2.4</td><td>0.09</td><td>+0.012</td></tr><tr><td>Gl 735B</td><td>10.194</td><td>1.368</td><td>3452 ± 100</td><td>dM3e</td><td>84.94 ± 1.72</td><td>10.59 ± 0.046</td><td>0.478 ± 0.048</td><td>1.83</td><td>13.2-2.1 + 3.1</td><td>0.09</td><td>+0.012</td></tr><tr><td>Gl 739</td><td>11.142</td><td>1.298</td><td>3500 ± 100</td><td>dM3</td><td>70.95 ± 2.56</td><td>10.40 ± 0.080</td><td>0.478 ± 0.057</td><td>3.19</td><td>7.59-1.0 + 1.0</td><td>...</td><td>+0.012</td></tr><tr><td>Gl 752A</td><td>9.115</td><td>1.287</td><td>3510 ± 100</td><td>dM3</td><td>170.36 ± 1.00</td><td>10.27 ± 0.015</td><td>0.499 ± 0.043</td><td>1.19</td><td>21.2-4.3 + 6.7</td><td>0.05</td><td>+0.045</td></tr><tr><td>Gl 781.1A</td><td>12.22</td><td>1.395</td><td>3434 ± 100</td><td>dM3e</td><td>67.08 ± 5.02</td><td>11.35 ± 0.183</td><td>0.351 ± 0.062</td><td>9.20</td><td>1.93-0.50 + 0.62</td><td>-0.07</td><td>-0.157</td></tr><tr><td>Gl 791</td><td>11.433</td><td>1.357</td><td>3460 ± 100</td><td>dM3e</td><td>67.38 ± 3.01</td><td>10.58 ± 0.099</td><td>0.474 ± 0.061</td><td>...</td><td>...</td><td>0.06</td><td>+0.062</td></tr><tr><td>Gl 793</td><td>10.55</td><td>1.388</td><td>3439 ± 100</td><td>dM3</td><td>125.07 ± 1.08</td><td>11.04 ± 0.039</td><td>0.403 ± 0.040</td><td>1.26</td><td>16.2-4.0 + 5.9</td><td>-0.09</td><td>-0.036</td></tr><tr><td>Gl 811.1</td><td>11.487</td><td>1.331</td><td>3478 ± 100</td><td>dM3e</td><td>65.29 ± 3.11</td><td>10.56 ± 0.106</td><td>0.462 ± 0.061</td><td>...</td><td>...</td><td>0.11</td><td>-0.012</td></tr></tbody></table>
<table><caption>Table 4
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GL 813</td><td>12.013</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>72.58 ± 3.16</td><td>11.32 ± 0.097</td><td>0.309 ± 0.039</td><td>...</td><td>...</td><td>-0.33</td><td>-0.254</td></tr><tr><td>GL 816</td><td>11.219</td><td>1.319</td><td>3486 ± 100</td><td>dM3</td><td>69.53 ± 2.93</td><td>10.43 ± 0.094</td><td>0.484 ± 0.061</td><td>...</td><td>...</td><td>0.03</td><td>+0.022</td></tr><tr><td>GL 836.4</td><td>12.83</td><td>1.395</td><td>3434 ± 100</td><td>dM3</td><td>41 ± 8</td><td>10.89 ± 0.449</td><td>0.434 ± 0.143</td><td>...</td><td>...</td><td>-0.06</td><td>-0.028</td></tr><tr><td>GL 843</td><td>12.03</td><td>1.394</td><td>3435 ± 100</td><td>dM3</td><td>77 ± 10</td><td>11.46 ± 0.304</td><td>0.334 ± 0.081</td><td>...</td><td>...</td><td>-0.16</td><td>-0.187</td></tr><tr><td>GL 844</td><td>10.653</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>61.79 ± 2.23</td><td>9.61 ± 0.080</td><td>0.679 ± 0.080</td><td>3.46</td><td>9.92-1.4 + 1.4</td><td>1.30</td><td>+0.324</td></tr><tr><td>GL 849</td><td>10.366</td><td>1.416</td><td>3417 ± 100</td><td>dM3</td><td>109.94 ± 2.07</td><td>10.57 ± 0.043</td><td>0.519 ± 0.053</td><td>0.85</td><td>30.8-7.8 + 18</td><td>0.24</td><td>+0.076</td></tr><tr><td>GL 856AB</td><td>10.75</td><td>1.401</td><td>3430 ± 100</td><td>dM3e</td><td>64.47 ± 6.49</td><td>10.55 ± 0.228</td><td>0.513 ± 0.103</td><td>11.00</td><td>2.36-0.63 + 0.76</td><td>0.15</td><td>+0.067</td></tr><tr><td>GL 875.1</td><td>11.63</td><td>1.401</td><td>3430 ± 100</td><td>dM3e</td><td>68.78 ± 2.77</td><td>10.82 ± 0.107</td><td>0.453 ± 0.062</td><td>11.00</td><td>2.08-0.44 + 0.52</td><td>0.11</td><td>-0.024</td></tr><tr><td>GL 877</td><td>10.377</td><td>1.346</td><td>3467 ± 100</td><td>dM3</td><td>116.07 ± 1.19</td><td>10.70 ± 0.024</td><td>0.442 ± 0.040</td><td>0.95</td><td>23.5-5.0 + 8.2</td><td>-0.01</td><td>-0.026</td></tr><tr><td>GL 896A</td><td>10.165</td><td>1.424</td><td>3410 ± 100</td><td>dM3e</td><td>161.76 ± 1.66</td><td>11.21 ± 0.024</td><td>0.391 ± 0.037</td><td>14.03</td><td>1.41-0.14 + 0.14</td><td>0.10</td><td>-0.064</td></tr><tr><td>GL 897AB</td><td>10.395</td><td>1.315</td><td>3489 ± 100</td><td>dM3e</td><td>77.5 ± 9</td><td>10.59 ± 0.244</td><td>0.447 ± 0.092</td><td>7.10</td><td>3.18-0.97 + 1.29</td><td>...</td><td>-0.025</td></tr><tr><td>GL 898BC</td><td>10.43</td><td>1.326</td><td>3481 ± 100</td><td>dM3</td><td>65.98 ± 1.96</td><td>10.28 ± 0.084</td><td>0.523 ± 0.063</td><td>...</td><td>...</td><td>0.01</td><td>+0.082</td></tr><tr><td>GL 905.2A</td><td>11.70</td><td>1.388</td><td>3439 ± 100</td><td>dM3</td><td>55.6 ± 1.7</td><td>10.43 ± 0.086</td><td>0.534 ± 0.067</td><td>...</td><td>...</td><td>0.06</td><td>+0.099</td></tr><tr><td>L 977-17</td><td>13.45</td><td>1.401</td><td>3430 ± 100</td><td>dM3</td><td>46.42 ± 3.24</td><td>11.78 ± 0.172</td><td>0.290 ± 0.049</td><td>...</td><td>...</td><td>-0.23</td><td>-0.316</td></tr><tr><td>LP 24-330</td><td>13.93</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>25.72 ± 1.17</td><td>10.98 ± 0.119</td><td>0.407 ± 0.058</td><td>...</td><td>...</td><td>0.28</td><td>-0.035</td></tr><tr><td>LHS 218</td><td>14.835</td><td>1.331</td><td>3478 ± 100</td><td>sdM3</td><td>29.4 ± 3.5</td><td>12.18 ± 0.262</td><td>0.220 ± 0.048</td><td>...</td><td>...</td><td>0.24</td><td>-0.601</td></tr><tr><td>LHS 375</td><td>15.68</td><td>1.425</td><td>3410 ± 100</td><td>sdM3</td><td>41.7 ± 1</td><td>13.78 ± 0.072</td><td>0.120 ± 0.014</td><td>...</td><td>...</td><td>-1.10</td><td>-1.100</td></tr><tr><td>LHS 1104</td><td>12.56</td><td>1.288</td><td>3509 ± 100</td><td>dM3</td><td>62.1 ± 9.1</td><td>11.53 ± 0.341</td><td>0.281 ± 0.073</td><td>...</td><td>...</td><td>0.02</td><td>-0.346</td></tr><tr><td>LHS 1384</td><td>14.35</td><td>1.285</td><td>3512 ± 100</td><td>dM3</td><td>...</td><td>...</td><td>...</td><td>14.00</td><td>...</td><td>...</td><td>...</td></tr><tr><td>LHS 2942</td><td>14.27</td><td>1.401</td><td>3430 ± 100</td><td>dM3</td><td>...</td><td>...</td><td>...</td><td>5.33</td><td>...</td><td>...</td><td>...</td></tr><tr><td>LHS 3375AB</td><td>13.74</td><td>1.412</td><td>3421 ± 100</td><td>dM3</td><td>33 ± 4</td><td>12.08 ± 0.268</td><td>0.257 ± 0.057</td><td>...</td><td>...</td><td>-0.56</td><td>-0.437</td></tr><tr><td>LHS 3673</td><td>13.60</td><td>1.358</td><td>3459 ± 100</td><td>dM3</td><td>43.0 ± 9.4</td><td>11.77 ± 0.502</td><td>0.274 ± 0.099</td><td>...</td><td>...</td><td>-0.05</td><td>-0.369</td></tr><tr><td>G 212-26</td><td>13.42</td><td>1.376</td><td>3447 ± 100</td><td>dM3</td><td>...</td><td>...</td><td>...</td><td>5.40</td><td>...</td><td>...</td><td>...</td></tr><tr><td>G 247-35</td><td>12.71</td><td>1.275</td><td>3520 ± 100</td><td>dM3</td><td>34.54 ± 1.67</td><td>10.40 ± 0.125</td><td>0.463 ± 0.065</td><td>...</td><td>...</td><td>0.75</td><td>-0.011</td></tr><tr><td>HIP 28940BC</td><td>15.08</td><td>1.363</td><td>3456 ± 100</td><td>dM3</td><td>18.77 ± 3.21</td><td>12.20 ± 0.363</td><td>0.226 ± 0.062</td><td>...</td><td>...</td><td>-0.68</td><td>-0.574</td></tr></tbody></table>

Notes. We computed the projected rotational period *P*/sin *i* as well as [M/H] derived from the [M/H]-radius correlation.

ª Metallicity from the radius-metallicity relation.
<table><caption>Table 5
Stellar Parameters and the Values of $v \sin i$ and [M/H] Compiled from the Literature for Our Targets in Our List of dM4 Stars</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GJ 1001A</td><td>12.84</td><td>1.556</td><td>3297 ± 100</td><td>dM4</td><td>76.86 ± 3.97</td><td>12.27 ± 0.132</td><td>0.291 ± 0.044</td><td>1.15</td><td>12.81-5.66 + 18.02</td><td>...</td><td>+0.047</td></tr><tr><td>GJ 1005AB</td><td>11.483</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>200.53 ± 9.41</td><td>12.99 ± 0.104</td><td>0.202 ± 0.028</td><td>3.00</td><td>3.41-0.96 + 1.44</td><td>-0.47</td><td>-0.210</td></tr><tr><td>GJ 1010B</td><td>14.10</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>63.7 ± 5.3</td><td>13.12 ± 0.201</td><td>0.190 ± 0.036</td><td>...</td><td>...</td><td>0.01</td><td>-0.249</td></tr><tr><td>GJ 1013</td><td>12.75</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>62.3 ± 4.2</td><td>11.72 ± 0.167</td><td>0.370 ± 0.063</td><td>...</td><td>...</td><td>-0.07</td><td>+0.064</td></tr><tr><td>GJ 1034</td><td>15.05</td><td>1.613</td><td>3250 ± 100</td><td>dM4</td><td>48.1 ± 4.5</td><td>13.46 ± 0.224</td><td>0.182 ± 0.037</td><td>4.50</td><td>2.05-0.61 + 0.79</td><td>-0.38</td><td>-0.275</td></tr><tr><td>GJ 1045</td><td>14.47</td><td>1.672</td><td>3211 ± 100</td><td>dM4</td><td>48.8 ± 3.4</td><td>12.91 ± 0.172</td><td>0.258 ± 0.047</td><td>...</td><td>...</td><td>0.30</td><td>-0.018</td></tr><tr><td>GJ 1065</td><td>12.79</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>104 ± 3</td><td>12.88 ± 0.083</td><td>0.213 ± 0.027</td><td>4.00</td><td>2.70-0.65 + 0.88</td><td>0.20</td><td>-0.172</td></tr><tr><td>GJ 1068</td><td>13.58</td><td>1.643</td><td>3231 ± 100</td><td>dM4</td><td>80 ± 22</td><td>13.10 ± 0.633</td><td>0.226 ± 0.104</td><td>...</td><td>...</td><td>0.06</td><td>-0.126</td></tr><tr><td>GJ 1092</td><td>13.775</td><td>1.584</td><td>3273 ± 100</td><td>dM4</td><td>71.321 ± -</td><td>13.04 ± 0.628</td><td>0.212 ± 0.095</td><td>...</td><td>...</td><td>-0.40</td><td>-0.176</td></tr><tr><td>GJ 1105</td><td>12.01</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>116.06 ± 3.67</td><td>12.33 ± 0.089</td><td>0.274 ± 0.035</td><td>2.00</td><td>6.93-2.28 + 4.24</td><td>0.24</td><td>+0.022</td></tr><tr><td>GJ 1122A</td><td>14.51</td><td>1.689</td><td>3200 ± 100</td><td>dM4e</td><td>49 ± 4</td><td>12.96 ± 0.198</td><td>0.259 ± 0.051</td><td>...</td><td>...</td><td>0.16</td><td>-0.015</td></tr><tr><td>GJ 1129</td><td>12.60</td><td>1.607</td><td>3254 ± 100</td><td>dM4</td><td>98 ± 17</td><td>12.56 ± 0.401</td><td>0.274 ± 0.083</td><td>3.00</td><td>4.62-1.94 + 2.91</td><td>0.05</td><td>+0.022</td></tr><tr><td>GJ 1134</td><td>12.97</td><td>1.654</td><td>3223 ± 100</td><td>dM4</td><td>96.7 ± 2.3</td><td>12.90 ± 0.072</td><td>0.252 ± 0.032</td><td>4.10</td><td>3.11-0.74 + 1.00</td><td>-0.16</td><td>-0.036</td></tr><tr><td>GJ 1138AB</td><td>13.01</td><td>1.640</td><td>3233 ± 100</td><td>dM4</td><td>102.9 ± 3.2</td><td>13.07 ± 0.088</td><td>0.227 ± 0.031</td><td>3.24</td><td>3.55-0.96 + 1.40</td><td>-0.57</td><td>-0.122</td></tr><tr><td>GJ 1157</td><td>13.63</td><td>1.649</td><td>3227 ± 100</td><td>dM4</td><td>69 ± 11</td><td>12.82 ± 0.369</td><td>0.258 ± 0.076</td><td>...</td><td>...</td><td>0.61</td><td>-0.018</td></tr><tr><td>GJ 1174</td><td>12.763</td><td>1.533</td><td>3317 ± 100</td><td>dM4</td><td>60 ± 4</td><td>11.65 ± 0.147</td><td>0.373 ± 0.059</td><td>...</td><td>...</td><td>0.09</td><td>+0.068</td></tr><tr><td>GJ 1193</td><td>13.825</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>48.5 ± 3.4</td><td>12.25 ± 0.154</td><td>0.284 ± 0.046</td><td>...</td><td>...</td><td>-0.09</td><td>+0.037</td></tr><tr><td>GJ 1204</td><td>13.77</td><td>1.610</td><td>3252 ± 100</td><td>dM4e</td><td>64 ± 4</td><td>12.80 ± 0.156</td><td>0.246 ± 0.041</td><td>...</td><td>...</td><td>0.43</td><td>-0.054</td></tr><tr><td>GJ 1207</td><td>12.315</td><td>1.566</td><td>3288 ± 100</td><td>dM4e</td><td>115.39 ± 1.51</td><td>12.63 ± 0.030</td><td>0.250 ± 0.025</td><td>10.70</td><td>1.18-0.21 + 0.25</td><td>-0.15</td><td>-0.042</td></tr><tr><td>GJ 1215</td><td>13.68</td><td>1.493</td><td>3351 ± 100</td><td>dM4</td><td>73 ± 6</td><td>13.00 ± 0.199</td><td>0.190 ± 0.035</td><td>...</td><td>...</td><td>0.07</td><td>-0.249</td></tr><tr><td>GJ 1216</td><td>14.42</td><td>1.572</td><td>3283 ± 100</td><td>dM4</td><td>57 ± 5</td><td>13.20 ± 0.211</td><td>0.194 ± 0.038</td><td>...</td><td>...</td><td>-0.40</td><td>-0.236</td></tr><tr><td>GJ 1218AB</td><td>12.73</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>61.56 ± 1.62</td><td>12.43 ± 0.077</td><td>0.267 ± 0.033</td><td>...</td><td>...</td><td>-0.95</td><td>+0.010</td></tr><tr><td>GJ 1222</td><td>13.13</td><td>1.563</td><td>3291 ± 100</td><td>dM4</td><td>60 ± 3.7</td><td>12.02 ± 0.154</td><td>0.329 ± 0.054</td><td>...</td><td>...</td><td>0.06</td><td>+0.055</td></tr><tr><td>GJ 1225</td><td>15.39</td><td>1.697</td><td>3195 ± 100</td><td>dM4</td><td>57 ± 4</td><td>14.17 ± 0.173</td><td>0.150 ± 0.028</td><td>...</td><td>...</td><td>-0.49</td><td>-0.395</td></tr><tr><td>GJ 1235</td><td>13.36</td><td>1.643</td><td>3231 ± 100</td><td>dM4</td><td>100.1 ± 3.5</td><td>13.36 ± 0.096</td><td>0.200 ± 0.028</td><td>...</td><td>...</td><td>0.14</td><td>-0.217</td></tr><tr><td>GJ 1254</td><td>12.55</td><td>1.568</td><td>3287 ± 100</td><td>dM4</td><td>61 ± 3</td><td>11.48 ± 0.127</td><td>0.426 ± 0.064</td><td>4.00</td><td>5.39-1.41 + 1.90</td><td>0.22</td><td>+0.122</td></tr><tr><td>GJ 1263</td><td>12.74</td><td>1.511</td><td>3336 ± 100</td><td>dM4</td><td>79.8 ± 4.5</td><td>12.25 ± 0.143</td><td>0.275 ± 0.043</td><td>...</td><td>...</td><td>0.22</td><td>+0.023</td></tr><tr><td>GJ 1265</td><td>13.64</td><td>1.643</td><td>3231 ± 100</td><td>dM4</td><td>96.0 ± 1.73</td><td>13.55 ± 0.059</td><td>0.183 ± 0.022</td><td>...</td><td>...</td><td>-0.12</td><td>-0.271</td></tr><tr><td>GJ 1270</td><td>13.245</td><td>1.607</td><td>3254 ± 100</td><td>dM4</td><td>72.5 ± 2.9</td><td>12.55 ± 0.089</td><td>0.276 ± 0.036</td><td>...</td><td>...</td><td>0.04</td><td>+0.025</td></tr><tr><td>GJ 1289</td><td>12.62</td><td>1.631</td><td>3239 ± 100</td><td>dM4</td><td>123.5 ± 2.9</td><td>13.08 ± 0.071</td><td>0.223 ± 0.029</td><td>2.60</td><td>4.34-1.27 + 2.04</td><td>0.12</td><td>-0.137</td></tr><tr><td>GJ 2036B</td><td>13.92</td><td>1.625</td><td>3242 ± 100</td><td>sdM4e</td><td>89.4 ± 1.98</td><td>13.68 ± 0.067</td><td>0.168 ± 0.020</td><td>19.8</td><td>0.429-0.07 + 0.08</td><td>...</td><td>-0.327</td></tr><tr><td>GJ 2043B</td><td>14.68</td><td>1.619</td><td>3246 ± 100</td><td>dM4</td><td>46 ± 6</td><td>12.99 ± 0.305</td><td>0.228 ± 0.057</td><td>...</td><td>...</td><td>0.34</td><td>-0.118</td></tr><tr><td>GJ 2069A</td><td>11.89</td><td>1.595</td><td>3263 ± 100</td><td>PMS M4e</td><td>90.37 ± 8.22</td><td>11.67 ± 0.218</td><td>0.406 ± 0.081</td><td>6.43</td><td>3.20-0.98 + 1.34</td><td>0.27</td><td>+0.102</td></tr><tr><td>GJ 3078B</td><td>13.90</td><td>1.582</td><td>3274 ± 100</td><td>dM4</td><td>64.6 ± 2.7</td><td>12.95 ± 0.111</td><td>0.221 ± 0.031</td><td>...</td><td>...</td><td>0.05</td><td>-0.144</td></tr><tr><td>GJ 3092B</td><td>14.85</td><td>1.769</td><td>3148 ± 100</td><td>dM4</td><td>33.83 ± 1.00</td><td>12.50 ± 0.083</td><td>0.366 ± 0.050</td><td>3.80</td><td>4.87-1.24 + 1.70</td><td>...</td><td>+0.064</td></tr><tr><td>GJ 3142</td><td>13.62</td><td>1.572</td><td>3283 ± 100</td><td>dM4e</td><td>60 ± 11</td><td>12.51 ± 0.423</td><td>0.266 ± 0.084</td><td>...</td><td>...</td><td>0.12</td><td>+0.006</td></tr><tr><td>GJ 3149B</td><td>13.10</td><td>1.595</td><td>3263 ± 100</td><td>dM4e</td><td>88 ± 17</td><td>12.82 ± 0.445</td><td>0.239 ± 0.079</td><td>4.00</td><td>3.02-1.26 + 1.71</td><td>0.09</td><td>-0.078</td></tr><tr><td>GJ 3198</td><td>12.35</td><td>1.508</td><td>3338 ± 100</td><td>dM4</td><td>65 ± 13</td><td>11.41 ± 0.460</td><td>0.402 ± 0.136</td><td>...</td><td>...</td><td>0.07</td><td>+0.098</td></tr><tr><td>GJ 3235</td><td>13.010</td><td>1.550</td><td>3302 ± 100</td><td>dM4</td><td>66 ± 12</td><td>12.11 ± 0.401</td><td>0.311 ± 0.094</td><td>...</td><td>...</td><td>-0.04</td><td>+0.051</td></tr><tr><td>GJ 3263</td><td>12.38</td><td>1.506</td><td>3340 ± 100</td><td>dM4</td><td>81 ± 16</td><td>11.92 ± 0.455</td><td>0.317 ± 0.106</td><td>...</td><td>...</td><td>0.09</td><td>+0.053</td></tr><tr><td>GJ 3283B</td><td>14.97</td><td>1.654</td><td>3223 ± 100</td><td>dM4e</td><td>42 ± 5</td><td>13.09 ± 0.264</td><td>0.230 ± 0.054</td><td>6.00</td><td>1.94-0.67 + 0.93</td><td>...</td><td>-0.111</td></tr><tr><td>GJ 3322</td><td>11.520</td><td>1.572</td><td>3283 ± 100</td><td>PMS M4e</td><td>30.12 ± 9.56</td><td>8.914 ± 0.604</td><td>1.396 ± 0.602</td><td>7.68</td><td>9.20-4.57 + 5.94</td><td>...</td><td>...</td></tr><tr><td>GJ 3372B</td><td>13.57</td><td>1.654</td><td>3223 ± 100</td><td>dM4e</td><td>76 ± 9</td><td>12.97 ± 0.278</td><td>0.243 ± 0.059</td><td>...</td><td>...</td><td>0.15</td><td>-0.063</td></tr><tr><td>GJ 3386C</td><td>13.13</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>39.78 ± 1.31</td><td>11.13 ± 0.092</td><td>0.477 ± 0.062</td><td>...</td><td>...</td><td>0.24</td><td>+0.175</td></tr><tr><td>GJ 3398</td><td>14.22</td><td>1.643</td><td>3231 ± 100</td><td>dM4</td><td>54.7 ± 2.4</td><td>12.91 ± 0.113</td><td>0.246 ± 0.037</td><td>4.00</td><td>3.11-0.81 + 1.10</td><td>...</td><td>-0.054</td></tr><tr><td>GJ 3405B</td><td>13.33</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>64 ± 9</td><td>12.36 ± 0.327</td><td>0.276 ± 0.072</td><td>...</td><td>...</td><td>0.12</td><td>+0.025</td></tr><tr><td>GJ 3466AB</td><td>12.85</td><td>1.678</td><td>3208 ± 100</td><td>dM4</td><td>80 ± 13</td><td>12.37 ± 0.376</td><td>0.335 ± 0.100</td><td>...</td><td>...</td><td>0.09</td><td>+0.057</td></tr></tbody></table>
<table><caption>Table 5
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GJ 3522</td><td>10.895</td><td>1.607</td><td>3254 ± 100</td><td>dM4e</td><td>224 ± 36</td><td>12.65 ± 0.354</td><td>0.263 ± 0.073</td><td>...</td><td>...</td><td>-0.01</td><td>-0.003</td></tr><tr><td>GJ 3573</td><td>14.2</td><td>1.674</td><td>3210 ± 100</td><td>dM4</td><td>62 ± 10</td><td>13.16 ± 0.553</td><td>0.230 ± 0.094</td><td>...</td><td>...</td><td>0.25</td><td>-0.111</td></tr><tr><td>GJ 3577A</td><td>13.89</td><td>1.548</td><td>3304 ± 100</td><td>dM4e</td><td>45 ± 6</td><td>12.16 ± 0.311</td><td>0.303 ± 0.076</td><td>...</td><td>...</td><td>0.19</td><td>+0.050</td></tr><tr><td>GJ 3577B</td><td>14.16</td><td>1.572</td><td>3283 ± 100</td><td>dM4e</td><td>45 ± 6</td><td>12.43 ± 0.311</td><td>0.277 ± 0.070</td><td>...</td><td>...</td><td>0.19</td><td>+0.027</td></tr><tr><td>GJ 3599</td><td>13.17</td><td>1.537</td><td>3313 ± 100</td><td>dM4</td><td>59 ± 11</td><td>12.02 ± 0.430</td><td>0.317 ± 0.101</td><td>...</td><td>...</td><td>0.30</td><td>+0.053</td></tr><tr><td>GJ 3631AB</td><td>14.40</td><td>1.619</td><td>3246 ± 100</td><td>dM4e</td><td>46 ± 8</td><td>13.46 ± 0.402</td><td>0.184 ± 0.056</td><td>19.10</td><td>0.49-0.16 + 0.18</td><td>-0.64</td><td>-0.268</td></tr><tr><td>GJ 3637</td><td>14.06</td><td>1.619</td><td>3246 ± 100</td><td>dM4</td><td>71.9 ± 3.1</td><td>13.34 ± 0.114</td><td>0.194 ± 0.028</td><td>...</td><td>...</td><td>-0.30</td><td>-0.236</td></tr><tr><td>GJ 3666</td><td>12.56</td><td>1.523</td><td>3325 ± 100</td><td>dM4</td><td>63.8 ± 8.5</td><td>11.58 ± 0.311</td><td>0.380 ± 0.095</td><td>...</td><td>...</td><td>-0.07</td><td>+0.075</td></tr><tr><td>GJ 3707</td><td>12.06</td><td>1.568</td><td>3287 ± 100</td><td>dM4</td><td>112 ± 21</td><td>12.31 ± 0.432</td><td>0.291 ± 0.094</td><td>2.0</td><td>7.36-3.53 + 6.55</td><td>0.35</td><td>+0.047</td></tr><tr><td>GJ 3764</td><td>12.86</td><td>1.493</td><td>3351 ± 100</td><td>dM4</td><td>62 ± 16</td><td>11.82 ± 0.593</td><td>0.326 ± 0.138</td><td>...</td><td>...</td><td>-0.09</td><td>+0.055</td></tr><tr><td>GJ 3779</td><td>12.93</td><td>1.578</td><td>3278 ± 100</td><td>dM4</td><td>72.5 ± 2.6</td><td>12.23 ± 0.098</td><td>0.306 ± 0.041</td><td>...</td><td>...</td><td>-0.26</td><td>+0.050</td></tr><tr><td>GJ 3780</td><td>12.90</td><td>1.566</td><td>3288 ± 100</td><td>dM4e</td><td>62.5 ± 14.4</td><td>11.88 ± 0.529</td><td>0.353 ± 0.135</td><td>...</td><td>...</td><td>-0.21</td><td>+0.061</td></tr><tr><td>GJ 3789</td><td>12.19</td><td>1.595</td><td>3263 ± 100</td><td>dM4e</td><td>126 ± 22</td><td>12.69 ± 0.403</td><td>0.253 ± 0.077</td><td>56.50</td><td>0.227-0.07 + 0.07</td><td>0.07</td><td>-0.033</td></tr><tr><td>GJ 3800</td><td>13.5</td><td>1.666</td><td>3216 ± 100</td><td>dM4e</td><td>82 ± 13</td><td>13.07 ± 0.547</td><td>0.237 ± 0.096</td><td>...</td><td>...</td><td>0.10</td><td>-0.085</td></tr><tr><td>GJ 3801</td><td>11.97</td><td>1.511</td><td>3336 ± 100</td><td>dM4</td><td>107.77 ± 3.22</td><td>12.13 ± 0.085</td><td>0.290 ± 0.037</td><td>4.00</td><td>3.67-0.88 + 1.20</td><td>0.14</td><td>+0.047</td></tr><tr><td>GJ 3804</td><td>11.872</td><td>1.497</td><td>3348 ± 100</td><td>dM4</td><td>97.62 ± 5.03</td><td>11.82 ± 0.114</td><td>0.328 ± 0.046</td><td>2.50</td><td>6.64-2.04 + 3.32</td><td>0.09</td><td>+0.055</td></tr><tr><td>GJ 3832C</td><td>13.95</td><td>1.572</td><td>3283 ± 100</td><td>dM4e</td><td>40 ± 6</td><td>11.96 ± 0.348</td><td>0.343 ± 0.094</td><td>...</td><td>...</td><td>0.59</td><td>+0.059</td></tr><tr><td>GJ 3843</td><td>13.04</td><td>1.491</td><td>3353 ± 100</td><td>dM4</td><td>59 ± 14</td><td>11.89 ± 0.545</td><td>0.314 ± 0.123</td><td>...</td><td>...</td><td>-0.02</td><td>+0.052</td></tr><tr><td>GJ 3873</td><td>12.355</td><td>1.585</td><td>3272 ± 100</td><td>dM4</td><td>53.5 ± 10.8</td><td>11.00 ± 0.446</td><td>0.545 ± 0.181</td><td>4.00</td><td>6.90-2.89 + 3.91</td><td>0.11</td><td>+0.245</td></tr><tr><td>GJ 3900</td><td>12.840</td><td>1.572</td><td>3283 ± 100</td><td>dM4</td><td>75 ± 23</td><td>12.22 ± 0.690</td><td>0.305 ± 0.149</td><td>3.00</td><td>5.15-2.95 + 4.43</td><td>0.46</td><td>+0.050</td></tr><tr><td>GJ 3907</td><td>14.19</td><td>1.641</td><td>3232 ± 100</td><td>dM4</td><td>51.1 ± 4.4</td><td>12.73 ± 0.207</td><td>0.266 ± 0.053</td><td>2.50</td><td>5.39-1.91 + 3.11</td><td>0.06</td><td>+0.006</td></tr><tr><td>GJ 3908</td><td>13.70</td><td>1.500</td><td>3345 ± 100</td><td>dM4</td><td>43 ± 8</td><td>11.87 ± 0.429</td><td>0.323 ± 0.103</td><td>...</td><td>...</td><td>0.04</td><td>+0.054</td></tr><tr><td>GJ 3919</td><td>13.21</td><td>1.588</td><td>3269 ± 100</td><td>dM4</td><td>56.6 ± 3.9</td><td>11.97 ± 0.170</td><td>0.349 ± 0.060</td><td>...</td><td>...</td><td>0.17</td><td>+0.060</td></tr><tr><td>GJ 4020B</td><td>14.70</td><td>1.631</td><td>3239 ± 100</td><td>dM4e</td><td>30.19 ± 2.00</td><td>12.10 ± 0.159</td><td>0.350 ± 0.061</td><td>16.16</td><td>1.10-0.24 + 0.27</td><td>...</td><td>+0.060</td></tr><tr><td>GJ 4030</td><td>13.50</td><td>1.515</td><td>3332 ± 100</td><td>dM4</td><td>44.8 ± 4.1</td><td>11.76 ± 0.219</td><td>0.347 ± 0.069</td><td>4.50</td><td>3.90-1.14 + 1.49</td><td>-0.04</td><td>+0.059</td></tr><tr><td>GJ 4049B</td><td>13.54</td><td>1.572</td><td>3283 ± 100</td><td>dM4</td><td>88.0 ± 3.6</td><td>13.26 ± 0.109</td><td>0.188 ± 0.026</td><td>2.50</td><td>3.81-1.16 + 1.89</td><td>-0.13</td><td>-0.255</td></tr><tr><td>GJ 4063AB</td><td>11.42</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>138 ± 40</td><td>12.87 ± 0.668</td><td>0.214 ± 0.101</td><td>2.17</td><td>4.99-2.93 + 5.16</td><td>-0.54</td><td>-0.169</td></tr><tr><td>GJ 4108</td><td>15.35</td><td>1.690</td><td>3200 ± 100</td><td>dM4</td><td>47.6 ± 4.1</td><td>13.74 ± 0.199</td><td>0.181 ± 0.036</td><td>4.50</td><td>2.04-0.60 + 0.78</td><td>...</td><td>-0.278</td></tr><tr><td>GJ 4169</td><td>13.975</td><td>1.660</td><td>3219 ± 100</td><td>dM4</td><td>72.2 ± 2.9</td><td>13.27 ± 0.089</td><td>0.214 ± 0.030</td><td>...</td><td>...</td><td>0.07</td><td>-0.169</td></tr><tr><td>GJ 4177B</td><td>13.12</td><td>1.511</td><td>3336 ± 100</td><td>dM4</td><td>59 ± 8</td><td>11.97 ± 0.316</td><td>0.312 ± 0.079</td><td>...</td><td>...</td><td>-0.03</td><td>+0.052</td></tr><tr><td>GJ 4178AB</td><td>13.1</td><td>1.497</td><td>3348 ± 100</td><td>dM4</td><td>57 ± 11</td><td>12.63 ± 0.624</td><td>0.237 ± 0.105</td><td>...</td><td>...</td><td>-1.65</td><td>-0.085</td></tr><tr><td>GJ 4185A</td><td>12.68</td><td>1.548</td><td>3304 ± 100</td><td>PMS M4e</td><td>50.7 ± 6</td><td>11.21 ± 0.278</td><td>0.469 ± 0.109</td><td>...</td><td>...</td><td>0.18</td><td>+0.166</td></tr><tr><td>GJ 4186A</td><td>12.68</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>51.4 ± 9</td><td>11.23 ± 0.404</td><td>0.463 ± 0.141</td><td>...</td><td>...</td><td>0.18</td><td>+0.160</td></tr><tr><td>GJ 4186B</td><td>13.49</td><td>1.560</td><td>3293 ± 100</td><td>dM4</td><td>51.4 ± 9</td><td>12.04 ± 0.404</td><td>0.324 ± 0.099</td><td>...</td><td>...</td><td>0.18</td><td>+0.054</td></tr><tr><td>GJ 4207</td><td>12.57</td><td>1.505</td><td>3341 ± 100</td><td>dM4</td><td>57 ± 21</td><td>11.35 ± 0.859</td><td>0.412 ± 0.251</td><td>...</td><td>...</td><td>0.01</td><td>+0.108</td></tr><tr><td>GJ 4214A</td><td>13.65</td><td>1.584</td><td>3273 ± 100</td><td>dM4</td><td>57 ± 6</td><td>12.43 ± 0.249</td><td>0.281 ± 0.061</td><td>...</td><td>...</td><td>0.21</td><td>+0.033</td></tr><tr><td>GJ 4232AB</td><td>14.06</td><td>1.517</td><td>3330 ± 100</td><td>dM4</td><td>39 ± 7</td><td>12.77 ± 0.414</td><td>0.218 ± 0.068</td><td>...</td><td>...</td><td>-0.40</td><td>-0.155</td></tr><tr><td>GJ 4248</td><td>11.80</td><td>1.484</td><td>3359 ± 100</td><td>dM4</td><td>134.29 ± 1.31</td><td>12.44 ± 0.041</td><td>0.242 ± 0.025</td><td>1.58</td><td>7.75-2.71 + 6.04</td><td>...</td><td>-0.066</td></tr><tr><td>GJ 4277A</td><td>13.68</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>39.1 ± 3.3</td><td>11.64 ± 0.204</td><td>0.384 ± 0.073</td><td>...</td><td>...</td><td>0.24</td><td>+0.079</td></tr><tr><td>GJ 4333</td><td>11.710</td><td>1.578</td><td>3278 ± 100</td><td>dM4</td><td>91.00 ± 2.89</td><td>11.51 ± 0.071</td><td>0.427 ± 0.051</td><td>2.50</td><td>8.64-2.51 + 4.09</td><td>0.25</td><td>+0.123</td></tr><tr><td>GJ 4338B</td><td>12.43</td><td>1.619</td><td>3246 ± 100</td><td>PMS M4e</td><td>67.5 ± 2.5</td><td>11.58 ± 0.099</td><td>0.437 ± 0.059</td><td>14.50</td><td>1.53-0.29 + 0.33</td><td>...</td><td>+0.134</td></tr><tr><td>GJ 4367</td><td>13.45</td><td>1.601</td><td>3258 ± 100</td><td>dM4</td><td>66 ± 12</td><td>12.55 ± 0.419</td><td>0.273 ± 0.086</td><td>...</td><td>...</td><td>0.28</td><td>+0.020</td></tr><tr><td>GJ 4378A</td><td>12.93</td><td>1.560</td><td>3293 ± 100</td><td>dM4</td><td>56 ± 8</td><td>11.67 ± 0.310</td><td>0.386 ± 0.096</td><td>4.00</td><td>4.88-1.69 + 2.29</td><td>...</td><td>+0.081</td></tr><tr><td>GJ 4387AB</td><td>12.6</td><td>1.542</td><td>3309 ± 100</td><td>dM4</td><td>78 ± 14</td><td>12.81 ± 0.594</td><td>0.222 ± 0.094</td><td>...</td><td>...</td><td>-0.62</td><td>-0.140</td></tr><tr><td>GJ 9652B</td><td>13.27</td><td>1.542</td><td>3309 ± 100</td><td>dM4e</td><td>52.40 ± 2.94</td><td>11.87 ± 0.142</td><td>0.343 ± 0.054</td><td>...</td><td>...</td><td>-0.09</td><td>+0.059</td></tr><tr><td>GJ 15B</td><td>11.07</td><td>1.580</td><td>3276 ± 100</td><td>dM4</td><td>278.76 ± 0.77</td><td>13.30 ± 0.026</td><td>0.188 ± 0.018</td><td>1.90</td><td>5.01-1.57 + 3.01</td><td>-0.95</td><td>-0.255</td></tr><tr><td>GJ 46</td><td>11.801</td><td>1.508</td><td>3338 ± 100</td><td>dM4</td><td>80.95 ± 3.21</td><td>11.34 ± 0.088</td><td>0.416 ± 0.053</td><td>1.29</td><td>16.32-6.60 + 18.1</td><td>0.15</td><td>+0.112</td></tr></tbody></table>
<table><caption>Table 5
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>☉</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>Gl 54.1</td><td>12.074</td><td>1.708</td><td>3188 ± 100</td><td>dM4e</td><td>271.01 ± 8.36</td><td>14.24 ± 0.069</td><td>0.148 ± 0.019</td><td>2.50</td><td>3.00-0.89 + 1.45</td><td>-0.33</td><td>-0.402</td></tr><tr><td>Gl 73</td><td>14.12</td><td>1.624</td><td>3243 ± 100</td><td>dM4</td><td>60 ± 12</td><td>13.01 ± 0.460</td><td>0.228 ± 0.078</td><td>...</td><td>...</td><td>0.15</td><td>-0.118</td></tr><tr><td>Gl 84.1B</td><td>12.77</td><td>1.497</td><td>3348 ± 100</td><td>dM4</td><td>43.03 ± 2.08</td><td>10.94 ± 0.125</td><td>0.492 ± 0.072</td><td>2.00</td><td>12.45-4.27 + 7.94</td><td>-0.18</td><td>+0.190</td></tr><tr><td>Gl 102</td><td>12.96</td><td>1.66</td><td>3219 ± 100</td><td>dM4e</td><td>129 ± 12</td><td>13.51 ± 0.223</td><td>0.192 ± 0.040</td><td>...</td><td>...</td><td>0.03</td><td>-0.243</td></tr><tr><td>Gl 105B</td><td>11.660</td><td>1.607</td><td>3254 ± 100</td><td>dM4</td><td>129.4 ± 4.3</td><td>12.22 ± 0.074</td><td>0.320 ± 0.039</td><td>2.45</td><td>6.61-1.95 + 3.21</td><td>-0.09</td><td>+0.053</td></tr><tr><td>Gl 166C</td><td>11.19</td><td>1.63</td><td>3239 ± 100</td><td>dM4e</td><td>207.1 ± 2.5</td><td>12.77 ± 0.046</td><td>0.256 ± 0.028</td><td>2.90</td><td>4.47-1.17 + 1.78</td><td>-0.10</td><td>-0.024</td></tr><tr><td>Gl 169.1A</td><td>11.07</td><td>1.60</td><td>3259 ± 100</td><td>dM4</td><td>180 ± 0.8</td><td>12.35 ± 0.030</td><td>0.299 ± 0.030</td><td>1.94</td><td>7.80-2.44 + 4.62</td><td>0.29</td><td>+0.049</td></tr><tr><td>Gl 179</td><td>11.98</td><td>1.492</td><td>3352 ± 100</td><td>dM4</td><td>81.38 ± 4.04</td><td>11.53 ± 0.128</td><td>0.372 ± 0.055</td><td>2.50</td><td>7.53-2.35 + 3.84</td><td>0.22</td><td>+0.065</td></tr><tr><td>Gl 190</td><td>10.29</td><td>1.50</td><td>3345 ± 100</td><td>dM4</td><td>107.85 ± 2.10</td><td>10.45 ± 0.062</td><td>0.618 ± 0.071</td><td>...</td><td>...</td><td>0.06</td><td>+0.320</td></tr><tr><td>Gl 203</td><td>12.49</td><td>1.492</td><td>3352 ± 100</td><td>dM4</td><td>113.50 ± 5.01</td><td>12.76 ± 0.116</td><td>0.211 ± 0.030</td><td>4.00</td><td>2.67-0.68 + 0.92</td><td>-0.23</td><td>-0.179</td></tr><tr><td>Gl 206A</td><td>12.28</td><td>1.510</td><td>3336 ± 100</td><td>dM4e</td><td>78.16 ± 3.70</td><td>12.49 ± 0.123</td><td>0.246 ± 0.051</td><td>6.37</td><td>1.95-0.62 + 0.84</td><td>0.19</td><td>-0.054</td></tr><tr><td>Gl 206B</td><td>12.28</td><td>1.510</td><td>3336 ± 100</td><td>dM4e</td><td>78.16 ± 3.70</td><td>12.49 ± 0.123</td><td>0.246 ± 0.051</td><td>6.11</td><td>2.04-0.65 + 0.90</td><td>0.19</td><td>-0.054</td></tr><tr><td>Gl 213</td><td>11.550</td><td>1.608</td><td>3254 ± 100</td><td>dM4e</td><td>171.55 ± 3.99</td><td>12.72 ± 0.053</td><td>0.254 ± 0.028</td><td>2.70</td><td>4.76-1.29 + 2.03</td><td>-0.16</td><td>-0.030</td></tr><tr><td>Gl 232</td><td>13.06</td><td>1.63</td><td>3239 ± 100</td><td>dM4</td><td>120 ± 2.3</td><td>13.46 ± 0.062</td><td>0.187 ± 0.022</td><td>3.10</td><td>3.05-0.80 + 1.18</td><td>-0.25</td><td>-0.259</td></tr><tr><td>Gl 234A</td><td>11.12</td><td>1.700</td><td>3193 ± 100</td><td>dM4e</td><td>242.1 ± 1.7</td><td>13.04 ± 0.035</td><td>0.254 ± 0.028</td><td>4.73</td><td>2.72-0.57 + 0.74</td><td>...</td><td>-0.030</td></tr><tr><td>Gl 268A</td><td>11.47</td><td>1.701</td><td>3192 ± 100</td><td>dM4e</td><td>158.87 ± 3.35</td><td>12.48 ± 0.066</td><td>0.331 ± 0.042</td><td>10.65</td><td>1.57-0.32 + 0.38</td><td>0.16</td><td>+0.056</td></tr><tr><td>Gl 268B</td><td>11.47</td><td>1.701</td><td>3192 ± 100</td><td>dM4e</td><td>158.87 ± 3.35</td><td>12.48 ± 0.066</td><td>0.331 ± 0.042</td><td>10.65</td><td>1.57-0.32 + 0.38</td><td>0.16</td><td>+0.056</td></tr><tr><td>Gl 273</td><td>9.850</td><td>1.533</td><td>3317 ± 100</td><td>dM4</td><td>262.98 ± 1.39</td><td>11.95 ± 0.013</td><td>0.326 ± 0.029</td><td>2.36</td><td>6.99-1.91 + 3.22</td><td>-0.08</td><td>+0.055</td></tr><tr><td>Gl 277B</td><td>11.78</td><td>1.550</td><td>3302 ± 100</td><td>dM4e</td><td>84.26 ± 3.45</td><td>11.41 ± 0.109</td><td>0.429 ± 0.060</td><td>6.40</td><td>3.39-0.87 + 1.19</td><td>0.10</td><td>+0.125</td></tr><tr><td>Gl 285</td><td>11.15</td><td>1.696</td><td>3196 ± 100</td><td>dM4e</td><td>167.88 ± 2.31</td><td>12.27 ± 0.050</td><td>0.359 ± 0.042</td><td>6.16</td><td>2.95-0.71 + 0.98</td><td>0.24</td><td>+0.062</td></tr><tr><td>Gl 299</td><td>12.83</td><td>1.71</td><td>3187 ± 100</td><td>dM4</td><td>148 ± 2.6</td><td>13.68 ± 0.058</td><td>0.193 ± 0.024</td><td>2.96</td><td>3.30-0.90 + 1.35</td><td>-0.43</td><td>-0.239</td></tr><tr><td>Gl 300</td><td>12.07</td><td>1.68</td><td>3206 ± 100</td><td>dM4</td><td>125.60 ± 0.97</td><td>12.56 ± 0.037</td><td>0.306 ± 0.034</td><td>3.00</td><td>5.16-1.34 + 2.01</td><td>0.20</td><td>+0.050</td></tr><tr><td>Gl 317</td><td>12.00</td><td>1.497</td><td>3348 ± 100</td><td>dM4</td><td>65.3 ± 0.4</td><td>11.07 ± 0.033</td><td>0.463 ± 0.046</td><td>2.50</td><td>9.37-2.56 + 4.18</td><td>-0.10</td><td>+0.160</td></tr><tr><td>Gl 319B</td><td>11.83</td><td>1.523</td><td>3325 ± 100</td><td>dM4</td><td>64.80 ± 2.35</td><td>10.89 ± 0.099</td><td>0.524 ± 0.070</td><td>3.70</td><td>7.17-1.82 + 2.53</td><td>0.04</td><td>+0.223</td></tr><tr><td>Gl 324B</td><td>13.15</td><td>1.640</td><td>3233 ± 100</td><td>dM4</td><td>76.8 ± 2.4</td><td>12.58 ± 0.088</td><td>0.285 ± 0.039</td><td>2.36</td><td>6.11-1.90 + 3.20</td><td>0.42</td><td>+0.039</td></tr><tr><td>Gl 347B</td><td>15.01</td><td>1.619</td><td>3246 ± 100</td><td>dM4</td><td>60.5 ± 4.1</td><td>13.92 ± 0.167</td><td>0.149 ± 0.026</td><td>...</td><td>...</td><td>0.02</td><td>-0.398</td></tr><tr><td>Gl 375A</td><td>11.28</td><td>1.501</td><td>3344 ± 100</td><td>dM4e</td><td>64.70 ± 1.75</td><td>11.08 ± 0.078</td><td>0.464 ± 0.057</td><td>10.0</td><td>2.35-0.48 + 0.58</td><td>...</td><td>+0.161</td></tr><tr><td>Gl 375B</td><td>11.28</td><td>1.501</td><td>3344 ± 100</td><td>dM4e</td><td>64.70 ± 1.75</td><td>11.08 ± 0.078</td><td>0.464 ± 0.057</td><td>10.0</td><td>2.35-0.48 + 0.58</td><td>...</td><td>+0.161</td></tr><tr><td>Gl 398</td><td>12.636</td><td>1.520</td><td>3328 ± 100</td><td>dM4e</td><td>71 ± 10</td><td>11.89 ± 0.310</td><td>0.328 ± 0.082</td><td>...</td><td>...</td><td>0.03</td><td>+0.055</td></tr><tr><td>Gl 402</td><td>11.650</td><td>1.582</td><td>3274 ± 100</td><td>dM4e</td><td>147.92 ± 3.52</td><td>12.50 ± 0.054</td><td>0.272 ± 0.030</td><td>2.40</td><td>5.74-1.65 + 2.75</td><td>0.12</td><td>+0.019</td></tr><tr><td>Gl 431</td><td>11.52</td><td>1.490</td><td>3354 ± 100</td><td>dM4e</td><td>96.56 ± 2.39</td><td>11.44 ± 0.074</td><td>0.386 ± 0.046</td><td>20.36</td><td>0.960-0.15 + 0.17</td><td>...</td><td>+0.081</td></tr><tr><td>Gl 445</td><td>10.82</td><td>1.520</td><td>3328 ± 100</td><td>dM4</td><td>186.86 ± 1.70</td><td>12.18 ± 0.040</td><td>0.288 ± 0.030</td><td>2.25</td><td>6.48-1.90 + 3.28</td><td>-0.30</td><td>+0.044</td></tr><tr><td>Gl 447</td><td>11.160</td><td>1.678</td><td>3208 ± 100</td><td>dM4</td><td>298.04 ± 2.30</td><td>13.53 ± 0.019</td><td>0.196 ± 0.020</td><td>2.20</td><td>4.51-1.33 + 2.32</td><td>-0.04</td><td>-0.230</td></tr><tr><td>Gl 458BC</td><td>13.33</td><td>1.523</td><td>3325 ± 100</td><td>sdM4</td><td>64.43 ± 1.43</td><td>13.13 ± 0.068</td><td>0.186 ± 0.022</td><td>5.40</td><td>1.74-0.45 + 0.65</td><td>-0.53</td><td>-0.262</td></tr><tr><td>Gl 469</td><td>12.06</td><td>1.519</td><td>3329 ± 100</td><td>dM4</td><td>75.85 ± 3.99</td><td>11.46 ± 0.134</td><td>0.400 ± 0.057</td><td>1.58</td><td>12.81-4.94 + 11.0</td><td>0.14</td><td>+0.095</td></tr><tr><td>Gl 486</td><td>11.390</td><td>1.537</td><td>3313 ± 100</td><td>dM4</td><td>119.47 ± 2.69</td><td>11.78 ± 0.051</td><td>0.355 ± 0.039</td><td>2.25</td><td>7.99-2.37 + 4.10</td><td>-0.05</td><td>+0.061</td></tr><tr><td>Gl 487A</td><td>12.10</td><td>1.475</td><td>3367 ± 100</td><td>dM4</td><td>97.91 ± 1.83</td><td>12.05 ± 0.061</td><td>0.285 ± 0.032</td><td>1.65</td><td>8.74-3.05 + 6.54</td><td>-0.04</td><td>+0.039</td></tr><tr><td>Gl 487B</td><td>12.10</td><td>1.475</td><td>3367 ± 100</td><td>dM4</td><td>97.91 ± 1.83</td><td>12.05 ± 0.061</td><td>0.285 ± 0.032</td><td>1.22</td><td>11.87-4.79 + 14.05</td><td>-0.04</td><td>+0.039</td></tr><tr><td>Gl 487C</td><td>12.10</td><td>1.475</td><td>3367 ± 100</td><td>dM4e</td><td>97.91 ± 1.83</td><td>12.05 ± 0.061</td><td>0.285 ± 0.032</td><td>2.60</td><td>5.55-1.55 + 2.47</td><td>-0.04</td><td>+0.039</td></tr><tr><td>Gl 490B</td><td>13.20</td><td>1.595</td><td>3263 ± 100</td><td>dM4</td><td>51.93 ± 3.00</td><td>11.78 ± 0.146</td><td>0.386 ± 0.062</td><td>8.60</td><td>2.27-0.56 + 0.71</td><td>0.07</td><td>+0.081</td></tr><tr><td>Gl 512B</td><td>13.69</td><td>1.652</td><td>3225 ± 100</td><td>dM4</td><td>83.8 ± 11.2</td><td>13.31 ± 0.312</td><td>0.208 ± 0.054</td><td>4.00</td><td>2.63-0.94 + 1.27</td><td>0.12</td><td>-0.190</td></tr><tr><td>Gl 520C</td><td>14.47</td><td>1.584</td><td>3273 ± 100</td><td>dM4e</td><td>45.17 ± 1.84</td><td>12.74 ± 0.109</td><td>0.243 ± 0.034</td><td>8.20</td><td>1.50-0.35 + 0.45</td><td>-0.14</td><td>-0.063</td></tr><tr><td>Gl 540.2AB</td><td>13.86</td><td>1.726</td><td>3176 ± 100</td><td>dM4e</td><td>86 ± 18</td><td>14.28 ± 0.481</td><td>0.150 ± 0.055</td><td>...</td><td>...</td><td>-0.80</td><td>-0.395</td></tr><tr><td>Gl 544B</td><td>14.50</td><td>1.643</td><td>3231 ± 100</td><td>dM4</td><td>52.6 ± 6.2</td><td>13.10 ± 0.277</td><td>0.225 ± 0.054</td><td>4.66</td><td>2.44-0.80 + 1.03</td><td>-0.13</td><td>-0.129</td></tr><tr><td>Gl 545</td><td>12.84</td><td>1.517</td><td>3330 ± 100</td><td>dM4</td><td>87 ± 12</td><td>12.54 ± 0.321</td><td>0.243 ± 0.062</td><td>4.00</td><td>3.07-1.08 + 1.46</td><td>-0.12</td><td>-0.063</td></tr><tr><td>Gl 553.1</td><td>11.95</td><td>1.488</td><td>3355 ± 100</td><td>dM4</td><td>92.44 ± 3.94</td><td>11.78 ± 0.113</td><td>0.330 ± 0.046</td><td>2.50</td><td>6.68-2.04 + 3.33</td><td>0.26</td><td>+0.056</td></tr><tr><td>Gl 555</td><td>11.320</td><td>1.609</td><td>3253 ± 100</td><td>dM4</td><td>164.99 ± 3.29</td><td>12.41 ± 0.045</td><td>0.295 ± 0.032</td><td>2.60</td><td>5.74-1.58 + 2.53</td><td>0.20</td><td>+0.048</td></tr></tbody></table>
<table><caption>Table 5
(Continued)</caption><thead><tr><th>Star</th><th>v<br>(mag)</th><th>(R-I)<sub>c</sub><br>(mag)</th><th>T<sub>eff</sub><br>(K)</th><th>Spect.<br>Type</th><th>π<br>(m")</th><th>Mv<br>(mag)</th><th>R<sub>*</sub><br>(R<sub>c</sub>)</th><th>v sin i<br>(km s<sup>-1</sup>)</th><th>P/sin i<br>(days)</th><th>[M/H]<br>(dex)</th><th>[M/H]<sup>a</sup><br>(dex)</th></tr></thead><tbody><tr><td>GL 568AB</td><td>11.680</td><td>1.538</td><td>3312 ± 100</td><td>dM4</td><td>98.40 ± 4.42</td><td>11.64 ± 0.100</td><td>0.378 ± 0.051</td><td>4.00</td><td>4.78-1.18 ± 1.60</td><td>0.45</td><td>+0.073</td></tr><tr><td>GL 592</td><td>12.720</td><td>1.561</td><td>3293 ± 100</td><td>dM4</td><td>74.9 ± 3.8</td><td>12.09 ± 0.112</td><td>0.318 ± 0.045</td><td>3.00</td><td>5.36-1.53 ± 2.29</td><td>0.14</td><td>+0.053</td></tr><tr><td>GL 609</td><td>12.570</td><td>1.595</td><td>3263 ± 100</td><td>dM4</td><td>99 ± 4</td><td>12.55 ± 0.090</td><td>0.271 ± 0.035</td><td>3.00</td><td>4.57-1.25 ± 1.88</td><td>-0.06</td><td>+0.017</td></tr><tr><td>GL 630.1AB</td><td>12.995</td><td>1.684</td><td>3204 ± 100</td><td>dM4e</td><td>68 ± 4</td><td>12.91 ± 0.130</td><td>0.263 ± 0.042</td><td>27.50</td><td>0.484-0.09 ± 0.10</td><td>-0.34</td><td>-0.003</td></tr><tr><td>GL 643AB</td><td>11.79</td><td>1.546</td><td>3305 ± 100</td><td>dM4</td><td>148.92 ± 4.00</td><td>12.65 ± 0.078</td><td>0.240 ± 0.030</td><td>2.73</td><td>4.45-1.26 ± 1.97</td><td>-0.21</td><td>-0.074</td></tr><tr><td>GL 644B</td><td>11.74</td><td>1.529</td><td>3320 ± 100</td><td>dM4</td><td>161.41 ± 5.64</td><td>12.78 ± 0.096</td><td>0.221 ± 0.029</td><td>2.73</td><td>4.10-1.18 ± 1.84</td><td>-0.21</td><td>-0.144</td></tr><tr><td>Gl 669A</td><td>11.43</td><td>1.530</td><td>3319 ± 100</td><td>PMS M4e</td><td>86.27 ± 4.10</td><td>11.11 ± 0.123</td><td>0.478 ± 0.070</td><td>6.30</td><td>3.84-1.01 ± 1.39</td><td>0.08</td><td>+0.176</td></tr><tr><td>GL 682</td><td>10.95</td><td>1.59</td><td>3268 ± 100</td><td>dM4</td><td>196.90 ± 2.15</td><td>12.42 ± 0.044</td><td>0.285 ± 0.030</td><td>3.00</td><td>4.80-1.22 ± 1.83</td><td>0.11</td><td>+0.039</td></tr><tr><td>GL 695B</td><td>10.8</td><td>...</td><td>3345 ± 100</td><td>dM4</td><td>120.33 ± 0.16</td><td>11.20 ± 0.103</td><td>0.439 ± 0.059</td><td>7.33</td><td>3.03-0.72 ± 0.95</td><td>...</td><td>+0.136</td></tr><tr><td>Gl 699</td><td>9.511</td><td>1.592</td><td>3266 ± 100</td><td>dM4</td><td>548.31 ± 1.51</td><td>13.21 ± 0.008</td><td>0.199 ± 0.018</td><td>2.02</td><td>4.99-1.49 ± 2.75</td><td>-0.40</td><td>-0.220</td></tr><tr><td>GL 720B</td><td>13.00</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>64.32 ± 0.95</td><td>12.04 ± 0.052</td><td>0.319 ± 0.035</td><td>2.30</td><td>7.02-2.06 ± 3.52</td><td>-0.16</td><td>+0.053</td></tr><tr><td>GL 725B</td><td>9.69</td><td>1.51</td><td>3336 ± 100</td><td>dM4</td><td>289.48 ± 3.21</td><td>11.25 ± 0.044</td><td>0.435 ± 0.086</td><td>5.09</td><td>4.33-1.42 ± 2.12</td><td>-0.57</td><td>-0.155</td></tr><tr><td>GL 729</td><td>10.455</td><td>1.550</td><td>3302 ± 100</td><td>dM4e</td><td>336.72 ± 2.03</td><td>13.09 ± 0.015</td><td>0.197 ± 0.018</td><td>4.72</td><td>2.11-0.41 ± 0.53</td><td>-0.14</td><td>-0.227</td></tr><tr><td>GL 732A</td><td>12.70</td><td>1.560</td><td>3293 ± 100</td><td>dM4e</td><td>72 ± 7</td><td>11.99 ± 0.232</td><td>0.333 ± 0.069</td><td>...</td><td>...</td><td>-0.01</td><td>+0.056</td></tr><tr><td>GL 747AB</td><td>11.260</td><td>1.487</td><td>3356 ± 100</td><td>dM4</td><td>123 ± 4</td><td>11.71 ± 0.073</td><td>0.340 ± 0.041</td><td>...</td><td>...</td><td>-0.08</td><td>+0.058</td></tr><tr><td>GL 754</td><td>12.23</td><td>1.687</td><td>3202 ± 100</td><td>dM4</td><td>169 ± 8</td><td>13.37 ± 0.123</td><td>0.214 ± 0.033</td><td>...</td><td>...</td><td>-0.17</td><td>-0.169</td></tr><tr><td>GL 766AB</td><td>12.380</td><td>1.654</td><td>3223 ± 100</td><td>dM4</td><td>97 ± 6</td><td>12.31 ± 0.136</td><td>0.329 ± 0.054</td><td>...</td><td>...</td><td>0.04</td><td>+0.055</td></tr><tr><td>GL 781.1B</td><td>12.51</td><td>1.582</td><td>3274 ± 100</td><td>dM4e</td><td>68.5 ± 5.2</td><td>11.69 ± 0.185</td><td>0.395 ± 0.071</td><td>9.20</td><td>2.17-0.56 ± 0.70</td><td>-0.07</td><td>+0.090</td></tr><tr><td>GL 783.2B</td><td>13.94</td><td>1.603</td><td>3257 ± 100</td><td>dM4</td><td>51.0 ± 6.0</td><td>12.48 ± 0.277</td><td>0.283 ± 0.066</td><td>1.76</td><td>8.14-3.48 ± 7.09</td><td>-0.15</td><td>+0.036</td></tr><tr><td>GL 791.2A</td><td>13.04</td><td>1.672</td><td>3212 ± 100</td><td>dM4e</td><td>110 ± 1.9</td><td>13.25 ± 0.058</td><td>0.221 ± 0.027</td><td>31.90</td><td>0.351-0.05 ± 0.05</td><td>0.06</td><td>-0.144</td></tr><tr><td>GL 792</td><td>13.49</td><td>1.559</td><td>3294 ± 100</td><td>dM4</td><td>62 ± 11</td><td>12.45 ± 0.409</td><td>0.268 ± 0.083</td><td>...</td><td>...</td><td>-0.11</td><td>+0.013</td></tr><tr><td>GL 810A</td><td>12.47</td><td>1.615</td><td>3249 ± 100</td><td>dM4</td><td>76 ± 11</td><td>11.87 ± 0.337</td><td>0.380 ± 0.101</td><td>...</td><td>...</td><td>0.02</td><td>+0.075</td></tr><tr><td>GL 812A</td><td>11.916</td><td>1.530</td><td>3319 ± 100</td><td>PMS M4e</td><td>56.54 ± 3.92</td><td>10.68 ± 0.153</td><td>0.583 ± 0.096</td><td>10.00</td><td>2.95-0.71 ± 0.87</td><td>0.12</td><td>+0.284</td></tr><tr><td>GL 838.1B</td><td>14.93</td><td>1.625</td><td>3242 ± 100</td><td>dM4</td><td>41.00 ± 7.00</td><td>12.99 ± 0.394</td><td>0.230 ± 0.069</td><td>...</td><td>...</td><td>0.05</td><td>-0.111</td></tr><tr><td>GL 860B</td><td>10.30</td><td>1.49</td><td>3354 ± 100</td><td>dM4e</td><td>251.9 ± 2.3</td><td>12.31 ± 0.040</td><td>0.260 ± 0.027</td><td>4.05</td><td>3.25-0.71 ± 0.96</td><td>-0.13</td><td>-0.012</td></tr><tr><td>Gl 865A</td><td>12.23</td><td>1.530</td><td>3319 ± 100</td><td>dM4e</td><td>75.87 ± 5.83</td><td>12.38 ± 0.187</td><td>0.266 ± 0.048</td><td>7.09</td><td>1.90-0.53 ± 0.71</td><td>-0.10</td><td>+0.006</td></tr><tr><td>Gl 865B</td><td>12.23</td><td>1.530</td><td>3319 ± 100</td><td>dM4e</td><td>75.87 ± 5.83</td><td>12.38 ± 0.187</td><td>0.266 ± 0.048</td><td>6.20</td><td>2.17-0.64 ± 0.88</td><td>-0.10</td><td>+0.006</td></tr><tr><td>Gl 867B</td><td>11.45</td><td>1.511</td><td>3336 ± 100</td><td>dM4e</td><td>115.01 ± 1.32</td><td>11.75 ± 0.045</td><td>0.345 ± 0.036</td><td>7.01</td><td>2.48-0.54 ± 0.72</td><td>0.15</td><td>+0.059</td></tr><tr><td>GL 873A</td><td>10.26</td><td>1.523</td><td>3325 ± 100</td><td>dM4e</td><td>195.22 ± 1.87</td><td>11.71 ± 0.041</td><td>0.358 ± 0.037</td><td>5.99</td><td>3.02-0.70 ± 0.98</td><td>-0.05</td><td>+0.062</td></tr><tr><td>GL 876A</td><td>10.14</td><td>1.548</td><td>3304 ± 100</td><td>dM4</td><td>213.28 ± 2.12</td><td>11.78 ± 0.041</td><td>0.360 ± 0.038</td><td>2.57</td><td>7.09-1.95 ± 3.13</td><td>...</td><td>+0.062</td></tr><tr><td>GL 896B</td><td>12.4</td><td>1.62</td><td>3246 ± 100</td><td>dM4e</td><td>161.76 ± 1.66</td><td>13.44 ± 0.122</td><td>0.207 ± 0.031</td><td>15.81</td><td>1.14-0.18 ± 0.21</td><td>0.10</td><td>+0.062</td></tr><tr><td>LHS 1655</td><td>15.32</td><td>1.562</td><td>3292 ± 100</td><td>dM4</td><td>26 ± 4</td><td>12.39 ± 0.357</td><td>0.277 ± 0.077</td><td>...</td><td>...</td><td>0.18</td><td>+0.027</td></tr><tr><td>LHS 2795</td><td>15.0</td><td>1.612</td><td>3251 ± 100</td><td>dM4</td><td>...</td><td>...</td><td>(0.301)</td><td>6.40</td><td>(2.38)</td><td>...</td><td>...</td></tr><tr><td>LHS 3279</td><td>14.04</td><td>1.567</td><td>3287 ± 100</td><td>dM4e</td><td>...</td><td>...</td><td>(0.301)</td><td>30.0</td><td>(0.508)</td><td>...</td><td>...</td></tr><tr><td>LDS 1751</td><td>15.71</td><td>1.560</td><td>3293 ± 100</td><td>dM4</td><td>22.79 ± 1.12</td><td>12.50 ± 0.127</td><td>0.263 ± 0.039</td><td>...</td><td>...</td><td>0.75</td><td>-0.003</td></tr><tr><td>MCC 85B</td><td>11.01</td><td>1.572</td><td>3283 ± 100</td><td>dM4e</td><td>278.76 ± 0.77</td><td>13.24 ± 0.026</td><td>0.191 ± 0.019</td><td>...</td><td>...</td><td>-0.95</td><td>-0.246</td></tr><tr><td>MCC 475B</td><td>14.88</td><td>1.511</td><td>3336 ± 100</td><td>dM4</td><td>33.00 ± 1.82</td><td>12.47 ± 0.140</td><td>0.248 ± 0.038</td><td>...</td><td>...</td><td>0.04</td><td>-0.047</td></tr><tr><td>G 32-37</td><td>14.12</td><td>1.523</td><td>3325 ± 100</td><td>dM4</td><td>35.3 ± 1.8</td><td>11.86 ± 0.131</td><td>0.335 ± 0.050</td><td>...</td><td>...</td><td>0.19</td><td>+0.057</td></tr><tr><td>G 32-38</td><td>14.36</td><td>1.523</td><td>3325 ± 100</td><td>dM4</td><td>35.3 ± 1.8</td><td>12.10 ± 0.131</td><td>0.300 ± 0.045</td><td>...</td><td>...</td><td>0.19</td><td>+0.049</td></tr><tr><td>G 97-52B</td><td>13.62</td><td>1.535</td><td>3315 ± 100</td><td>dM4</td><td>...</td><td>...</td><td>(0.301)</td><td>4.00</td><td>(3.81)</td><td>...</td><td>...</td></tr><tr><td>G 255-12</td><td>15.71</td><td>1.560</td><td>3293 ± 100</td><td>dM4</td><td>24.6 ± 4.7</td><td>12.66 ± 0.440</td><td>0.244 ± 0.080</td><td>...</td><td>...</td><td>0.75</td><td>-0.060</td></tr></tbody></table>

Notes. We computed the projected rotational period *P*/*sin i* as well as [M/H] derived from the [M/H]-radius correlation.

<sup>a</sup> Metallicity from the radius-metallicity relation.
<table><caption>**Table 6**
Mean Parameters of Our Stellar Samples with the Mean Effective Temperature and the Convective Overturning Time $\tau_c$
According to Noyes et al. (1984) and Spada et al. (2013)</caption><thead><tr><th>Spectral Type</th><th>(R-I)<sub>c</sub> domain (mag)</th><th>(R-I)<sub>c</sub> (mag)</th><th>T<sub>eff</sub> (K)</th><th>R<sub>*</sub> (R<sub>☉</sub>)</th><th>(B-V) (mag)</th><th>τ<sub>c</sub><sup>a</sup> (days)</th><th>τ<sub>c</sub><sup>b</sup> (days)</th></tr></thead><tbody><tr><td>dK4</td><td>[0.560; 0.680]</td><td>0.617</td><td>4600</td><td>0.815</td><td>1.151</td><td>24.16</td><td>51.3</td></tr><tr><td>dK6</td><td>[0.684;0.816]</td><td>0.738</td><td>4226</td><td>0.6469</td><td>1.340</td><td>25.68</td><td>76.5</td></tr><tr><td>dM2</td><td>[1.064;1.196]</td><td>1.128</td><td>3658</td><td>0.5082</td><td>1.511</td><td>27.14</td><td>119</td></tr><tr><td>dM3</td><td>[1.284;1.416]</td><td>1.354</td><td>3462</td><td>0.4090</td><td>1.548</td><td>27.46</td><td>175</td></tr><tr><td>dM4</td><td>[1.500;1.700]</td><td>1.532</td><td>3317</td><td>0.3008</td><td>1.581</td><td>27.75</td><td>454</td></tr></tbody></table>

**Notes.**

<sup>a</sup> From Noyes et al. (1984).

<sup>b</sup> From Spada et al. (2013).

<figure><img src="image_5.png" /></figure>

<figure><img src="image_6.png" /><figcaption>**Figure 2.** Values of $T_{\text{eff}}$ derived from the $(R-I)_c$ color as a function of the $T_{\text{eff}}$ values compiled from the literature (left panel). The solid line is the one-to-one correlation. The dashed line shows the smoothed data. Right panel: values of $T_{\text{eff}}$ derived from the PCA inversion method as a function of the $T_{\text{eff}}$ values compiled from the literature. Same description as the left panel.</figcaption></figure>

stars below −0.5 dex (Table 7). We give the [M/H] values from the smoothed data in Table 7.

## 4. ROTATION OF THE DK6 STARS

In view of the inhomogeneity of our sample of 105 late-K dwarfs, which includes several K4, K5, and K6 dwarfs and a few K7 dwarfs, we selected a subsample of stars from K5.7 to K7.3, with an effective temperature of 4226 ± 110 K. For this subsample of K6 dwarfs, it is possible to intercompare the spectra and identify rotational broadening effects in the absorption lines. The profiles of the photospheric lines depend on four main parameters: rotational broadening, microturbulence, macroturbulence, and Zeeman broadening. Micro- and macroturbulence (typically of order 1 km s⁻¹) are not expected to vary much among our subsample of dK6 stars. Metallicity plays a role in the line strengths but not in macro- or microturbulence. The molecular lines we use for our cross-correlations have Landé factors that are generally lower than those of atomic spectral lines (e.g., Afram & Berdyugina 2015). Only two well-defined molecular bands have larger Landé factors (e.g., Reiners & Basri 2006): TiO at 7050 Å and FeH at 9900 Å. For high-activity stars, the Zeeman broadening effect

could be significant even for small Landé factors. But considering the large $v \sin i$ for these stars (6–18 km s⁻¹), the Zeeman broadening effect should be completely negligible.

In order to extract rotational information, we carefully selected the spectral domain that we used for the cross-correlations: in Paper XIV, in our study of dM2 stars, we chose a 125 Å wide spectral domain between 5460 and 5585 Å. Here, in order to obtain cleaner cross-correlation functions for dK6 stars, trial and error has led us to prefer a 120 Å wide spectral domain between 5730 and 5850 Å. In this latter domain, there are fewer weak and unsaturated narrow spectral lines that yield clean cross-correlation functions, as far as the cross-correlation background is concerned (see Section 5). Unfortunately, in the present study, we cannot exploit spectral lines in molecular bands at the red end of the spectrum (such as we could do for dM3 and dM4 stars): in the warmer dK6 stars, the bands are not strong enough to be useful. This is unfortunate because molecular bands give the best results for the cross-correlations (see Paper XVII, HM). As we shall see below, the noise in the background is central to reaching the highest precision in the $v \sin i$ measurements. We show in Figure 6 the spectral domain we have chosen for our rotational analysis of dK6 stars, using as an example the star Gl 798: this star, with $m_V = 8.82$, is
<figure><img src="image_7.png" /><figcaption>**Figure 3.** Correlation between the metallicity [M/H] and the stellar radius for stars of spectral subtype dK6. The two parameters do correlate for dK6 stars, but the scatter is large. This large scatter is essentially due to the large errors on the stellar radii and [M/H], as indicated by the error box.</figcaption></figure>

<figure><img src="image_8.png" /><figcaption>**Figure 4.** Correlation between [M/H] and stellar radius for stars with spectral subtype dM3. The correlation is relatively tight, as in dM2 stars (Paper VII), in spite of the relatively large error on the radius (error box). We can see that, as in dM2 and dK6 stars, the metallicity decreases with decreasing radius for a given (R-I)C. We show some obvious outliers as open circles, and the continuous line represents the data smoothed by a Gaussian.</figcaption></figure>
<figure><img src="image_9.png" /><figcaption>**Figure 5.** Correlation between [M/H] and stellar radius $R_*$ for stars with spectral subtype dM4. The open circles are outliers that were not included in the smoothing of the data (solid line).</figcaption></figure>

neither the brightest nor the faintest star in our sample, which ranges from $m_V = 7.87$ to 11.80. In Figure 6, the level of the continuum has been normalized to 1.

For each star in our sample, we cross-correlated the spectra with themselves in order to identify at first our “zero-rotation” template stars. For each spectral subtype, we chose our template empirically as the star with the lowest FWHM of the cross-correlation peak among the sample of stars of that subtype. We found that the best template for our dK6 stars in the HARPS database is Gl 57 with a FWHM = 0.1236 Å, which corresponds to a Gaussian with a width of 6.40 km s⁻¹. This is slightly broader than the 0.1006 Å FWHM (5.40 km s⁻¹) at 5585 Å that we measured in the HARPS spectra of dM2 stars, and it is slightly narrower than the 0.1455 Å FWHM (7.54 km s⁻¹) at 5790 Å that we measured for the dK4 stars. This is consistent with a decrease in the widths of photospheric lines as we go to later spectral type among K and M dwarfs. Gl 57 lies at the lower end of our selection range. Our mean effective temperature for this star is 4040 K, which implies a spectral type of K7.1. Our PCA-based inversion for this star gives a temperature of 4030 K, which also yields a spectral type K7.1. We trust the effective temperatures more than the $(R-I)_C$ color because, for the late-K dwarfs, $T_{\text{eff}}$ may vary a lot for a given $(R-I)_C$ because the gradient of $T_{\text{eff}}$ versus $(R-I)_C$ increases a lot in late-K dwarfs (see Figure 1). Therefore, Gl 57 appears to agree with our selection of dK6 stars. We emphasize that, during the course of this study, we also investigated the cross-correlation with Gl 847A, a low $v \sin i$ star with a somewhat higher effective temperature ($(R-I)_C = 0.761$ and $T_{\text{eff}} = 4110$ K) and earlier spectral type (K6.7). But finally we found little difference in the $v \sin i$ measures between these two templates. We therefore

conclude that Gl 57 is a reliable template, although it has a bit lower effective temperature than the rest of the sample.

In the SOPHIE spectra, we found that Gl 728 has the narrowest cross-correlation function, and we used that as our template spectrum in analyzing SOPHIE spectra. Note that the cross-correlation of Gl 116 with Gl 728 yields a FWHM of 0.1583 Å, which is a bit narrower than the cross-correlation function of Gl 728 with itself (0.1611 Å). The cross-correlation of Gl 116 with itself yields a FWHM of 0.1475 Å, which is significantly smaller than that of most other dK6 stars. We believe this star has a spectral type later than dK6.

We show in Figure 7 the cross-correlation profiles obtained with the HARPS observations for five late-K dwarfs in our sample: Gl 57 (0 km s⁻¹), GJ 9299 (1.78 km s⁻¹), GJ 9714 (2.51 km s⁻¹), Gl 425B (3.35 km s⁻¹), and Gl 517 (9.77 km s⁻¹) (from narrowest to broadest). The FWHM of the peak for any particular star (in units of Å) is used to determine the value of $v \sin i$ for that star. In order to measure the FWHM of the cross-correlation functions, we measured the background level on each side of the cross-correlation functions. Then we subtracted the linear interpolation of this background and normalized the functions. This ensures that we isolate only the cross-correlation profiles in our results, with little influence from the background. We then measured directly the FWHM from the profiles. We note that we have very high S/N values (typically several hundreds) and a good sampling for the cross-correlation functions (0.01 Å).

As in our previous papers, we take into account limb darkening effects before we can derive significant $v \sin i$ measures for our rotators. We computed synthetic rotational profiles that include limb darkening. The synthetic profiles were computed according to the formulation of Gray (1988, p.