Erratum: "Rotation of Low-mass Stars in Taurus with K2" (2020, AJ, 159, 273)

L. M. Rebull, J. R. Stauffer, A. M. Cody, L. A. Hillenbrand, J. Bouvier, N.

Roggero, T. J. David

► To cite this version:

L. M. Rebull, J. R. Stauffer, A. M. Cody, L. A. Hillenbrand, J. Bouvier, et al. Erratum: "Rotation of Low-mass Stars in Taurus with K2" (2020, AJ, 159, 273). 2021, 10.3847/1538-3881/ac205f. insu-03705274

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# Erratum: “Rotation of Low-mass Stars in Taurus with K2” (2020, AJ, 159, 273)

L. M. Rebull¹ ID, J. R. Stauffer², A. M. Cody³, L. A. Hillenbrand⁴, J. Bouvier⁵, N. Roggero⁵, and T. J. David⁶

¹Infrared Science Archive (IRSA), IPAC, 1200 E. California Blvd., California Institute of Technology, Pasadena, CA 91125, USA; rebull@ipac.caltech.edu

²Spitzer Science Center (SSC), (IPAC), 1200 E. California Blvd., California Institute of Technology, Pasadena, CA 91125, USA

³Bay Area Environmental Research Institute, 625 2nd St. Ste. 209, Petaluma, CA 94952, USA

⁴Astronomy Department, California Institute of Technology, Pasadena, CA 91125, USA

⁵Université de Grenoble, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), F-38000 Grenoble, France; CNRS, IPAG, F-38000 Grenoble, France

⁶Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA

Received 2021 August 19; published 2021 September 27

*Supporting material: machine-readable tables*

Taurus was observed in K2 C4 and C13, with considerably more stars in C13. Table 2 and A1 inadvertently omitted periods from C4, and only included periods from C13.

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

Contents of Table: Periods and Supporting Data for Taurus Members with K2 Light Curves</caption><thead><tr><th>Number</th><th>Column</th><th>Contents</th></tr></thead><tbody><tr><td>1</td><td>EPIC</td><td>Number in the Ecliptic Plane Input Catalog (EPIC) for K2</td></tr><tr><td>2</td><td>Coord</td><td>Right ascension and decl. (J2000) for target</td></tr><tr><td>3</td><td>OName</td><td>Alternate name for target</td></tr><tr><td>4</td><td>Gaia</td><td>Gaia DR2 ID</td></tr><tr><td>5</td><td>Vmag</td><td>V magnitude (in Vega mags), if observed</td></tr><tr><td>6</td><td>Ksmag</td><td>K<sub>s</sub> magnitude (in Vega mags), if observed</td></tr><tr><td>7</td><td>(V - K<sub>s</sub>)<sub>0</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub>, as directly observed (in Vega mags), if V and K<sub>s</sub> exist</td></tr><tr><td>8</td><td>(V - K<sub>s</sub>)<sub>u</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub> used, in Vega mags (observed or inferred; see text)</td></tr><tr><td>9</td><td>E(V - K<sub>s</sub>)</td><td>E(V - K<sub>s</sub>) adopted for this star (in mags; see Section 2.5)</td></tr><tr><td>10</td><td>Ksmag0</td><td>Dereddened K<sub>s,0</sub> magnitude (in Vega mags), as inferred (see Section 2.5)</td></tr><tr><td>11</td><td>(V - K<sub>s</sub>)<sub>0</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub>, dereddened V - K<sub>s</sub> (in Vega mags), as inferred (see Section 2.5; rounded to nearest 0.1 to emphasize the relatively low accuracy)</td></tr><tr><td>12</td><td>Uncert</td><td>Two digit code denoting origin of (V - K<sub>s</sub>)<sub>0</sub> and (V - K<sub>s</sub>)<sub>0</sub> (see Section 2.3 and 2.5): first digit (origin of (V - K<sub>s</sub>)<sub>0</sub>): 1 = V measured directly from the literature (including SIMBAD) and K<sub>s</sub> from 2MASS; 2 = V from APASS and K<sub>s</sub> from 2MASS; 3 = (V - K<sub>s</sub>)<sub>0</sub> inferred from Gaia g and K<sub>s</sub> from 2MASS (see Section 2.3); 4 = (V - K<sub>s</sub>)<sub>0</sub> inferred from Pan-STARRS1 g and K<sub>s</sub> from 2MASS (see Section 2.3); 5 = (V - K<sub>s</sub>)<sub>0</sub> inferred from membership work (see Section 2.2; rare); 6 = V inferred from well-populated optical SED and K<sub>s</sub> from 2MASS (see Section 2.3); -9 = no measure of (V - K<sub>s</sub>)<sub>0</sub>. Second digit (origin of E(V - K<sub>s</sub>) leading to (V - K<sub>s</sub>)<sub>0</sub>): 1 = dereddening from JHK<sub>s</sub> diagram (see Section 2.5); 2 = dereddening back to (V - K<sub>s</sub>)<sub>0</sub> expected for the spectral type; 3=used median E(V - K<sub>s</sub>) = 0.7 (see Section 2.5); -9 = no measure of E(V - K<sub>s</sub>)</td></tr><tr><td>13</td><td>P1</td><td>Primary period, in days (taken to be rotation period in cases where there is >1 period)</td></tr><tr><td>14</td><td>P2</td><td>Secondary period, in days</td></tr><tr><td>15</td><td>P3</td><td>Tertiary period, in days</td></tr><tr><td>16</td><td>P4</td><td>Quaternary period, in days</td></tr><tr><td>17</td><td>Member</td><td>Highest quality member, possible member, foreground young star (see Section 2.2)</td></tr><tr><td>18</td><td>IRexcess</td><td>Whether an IR excess is present or not (see Section 4)</td></tr><tr><td>19</td><td>IRexStr</td><td>Minimum wavelength at which the IR excess is detected or the limit of our knowledge of where there is no excess (see Section 4)</td></tr><tr><td>20</td><td>Slope</td><td>Slope of SED fit to all available detections between 2 and 25 µm</td></tr><tr><td>21</td><td>Class</td><td>SED class (I, flat, II, III)</td></tr><tr><td>22</td><td>dip</td><td>LC matches dipper characteristics (see Section 6.2)</td></tr><tr><td>23</td><td>burst</td><td>LC matches burster characteristics (see Section 6.2)</td></tr><tr><td>24</td><td>sin/mult</td><td>Single or multiperiod star</td></tr><tr><td>25</td><td>dd</td><td>LC and power spectrum matches double-dip characteristics (see Section 6.2)</td></tr><tr><td>26</td><td>ddmove</td><td>LC and power spectrum matches moving double-dip characteristics (see Section 6.2)</td></tr><tr><td>27</td><td>shape</td><td>LC matches shape changer characteristics (see Section 6.2)</td></tr><tr><td>28</td><td>beat</td><td>LC has beating visible (see Section 6.2)</td></tr><tr><td>29</td><td>complex</td><td>Power spectrum has a complex, structured peak and/or has a wide peak (see Section 6.2)</td></tr><tr><td>30</td><td>closep</td><td>Power spectrum has resolved close peaks (see Section 6.2)</td></tr><tr><td>31</td><td>distp</td><td>Power spectrum has resolved distant peaks (see Section 6.2)</td></tr><tr><td>32</td><td>pulse</td><td>Power spectrum and LC match pulsator characteristics (see Section 6.2)</td></tr></tbody></table>

(This table is available in its entirety in machine-readable form.)
<table><caption>**Table A1**

Contents of Table: Periods and Supporting Data for Taurus Likely Nonmembers with K2 Light Curves</caption><thead><tr><th>Number</th><th>Label</th><th>Contents</th></tr></thead><tbody><tr><td>1</td><td>EPIC</td><td>Number in the Ecliptic Plane Input Catalog (EPIC) for K2</td></tr><tr><td>2</td><td>Coord</td><td>Right ascension and decl. (J2000) for target</td></tr><tr><td>3</td><td>OName</td><td>Alternate name for target</td></tr><tr><td>4</td><td>Gaia</td><td>Gaia DR2 ID</td></tr><tr><td>5</td><td>Vmag</td><td>V magnitude (in Vega mags), if observed</td></tr><tr><td>6</td><td>Ksmag</td><td>K<sub>s</sub> magnitude (in Vega mags), if observed</td></tr><tr><td>7</td><td>(V - K<sub>s</sub>)<sub>0</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub>, as directly observed (in Vega mags), if V and K<sub>s</sub> exist</td></tr><tr><td>8</td><td>(V - K<sub>s</sub>)<sub>u</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub> used, in Vega mags (observed or inferred; see text)</td></tr><tr><td>9</td><td>E(V - K<sub>s</sub>)</td><td>E(V - K<sub>s</sub>) adopted for this star (in mags; see Section 2.5)</td></tr><tr><td>10</td><td>Ksmag0</td><td>Dereddened K<sub>s,0</sub> magnitude (in Vega mags), as inferred (see Section 2.5)</td></tr><tr><td>11</td><td>(V - K<sub>s</sub>)<sub>0</sub></td><td>(V - K<sub>s</sub>)<sub>0</sub>, dereddened V - K<sub>s</sub> (in Vega mags), as inferred (see Section 2.5; rounded to the nearest 0.1 to emphasize the relatively low accuracy)</td></tr><tr><td>12</td><td>Uncert</td><td>Two digit code denoting origin of (V - K<sub>s</sub>)<sub>0</sub> and (V - K<sub>s</sub>)<sub>0</sub> (see Section 2.3 and 2.5): first digit (origin of (V - K<sub>s</sub>)<sub>0</sub>): 1 = V measured directly from the literature (including SIMBAD) and K<sub>s</sub> from 2MASS; 2 = V from APASS and K<sub>s</sub> from 2MASS; 3 = (V - K<sub>s</sub>)<sub>0</sub> inferred from Gaia g and K<sub>s</sub> from 2MASS (see Section 2.3); 4 = (V - K<sub>s</sub>)<sub>0</sub> inferred from Pan-STARRS1 g and K<sub>s</sub> from 2MASS (see Section 2.3); 5 = (V - K<sub>s</sub>)<sub>0</sub> inferred from membership work (see Section 2.2; rare); 6 = V inferred from well-populated optical SED and K<sub>s</sub> from 2MASS (see Section 2.3); -9 = no measure of (V - K<sub>s</sub>)<sub>0</sub>. Second digit (origin of E(V - K<sub>s</sub>) leading to (V - K<sub>s</sub>)<sub>0</sub>): 1 = dereddening from JHK<sub>s</sub> diagram (see Section 2.5); 2 = dereddening back to (V - K<sub>s</sub>)<sub>0</sub> expected for the spectral type; 3 = used median E(V - K<sub>s</sub>) = 0.7 (see Section 2.5); -9 = no measure of E(V - K<sub>s</sub>)</td></tr><tr><td>13</td><td>P1</td><td>Primary period, in days (taken to be rotation period in cases where there is &gt; 1 period)</td></tr><tr><td>14</td><td>P2</td><td>Secondary period, in days</td></tr><tr><td>15</td><td>P3</td><td>Tertiary period, in days</td></tr><tr><td>16</td><td>P4</td><td>Quaternary period, in days</td></tr><tr><td>17</td><td>IRexcess</td><td>Whether an IR excess is present or not (see Section 4)</td></tr><tr><td>18</td><td>IRexStr</td><td>Minimum wavelength at which the IR excess is detected or the limit of our knowledge of where there is no excess (see Section 4)</td></tr><tr><td>19</td><td>Slope</td><td>Slope of SED fit to all available detections between 2 and 25 µm</td></tr><tr><td>20</td><td>Class</td><td>SED class (I, flat, II, III)</td></tr><tr><td>21</td><td>sin/mult</td><td>Single or multiperiod star</td></tr><tr><td>22</td><td>dd</td><td>LC and power spectrum matches double-dip characteristics (see Section 6.2)</td></tr><tr><td>23</td><td>ddmove</td><td>LC and power spectrum matches moving double-dip characteristics (see Section 6.2)</td></tr><tr><td>24</td><td>shape</td><td>LC matches shape changer characteristics (see Section 6.2)</td></tr><tr><td>25</td><td>beat</td><td>LC has beating visible (see Section 6.2)</td></tr><tr><td>26</td><td>complex</td><td>Power spectrum has a complex, structured peak and/or has a wide peak (see Section 6.2)</td></tr><tr><td>27</td><td>closep</td><td>Power spectrum has resolved close peaks (see Section 6.2)</td></tr><tr><td>28</td><td>distp</td><td>Power spectrum has resolved distant peaks (see Section 6.2)</td></tr><tr><td>29</td><td>pulse</td><td>Power spectrum and LC match pulsator characteristics (see Section 6.2)</td></tr></tbody></table>

(This table is available in its entirety in machine-readable form.)

## ORCID iDs

L. M. Rebull https://orcid.org/0000-0001-6381-515X