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Appendix A: Cluster parameters

In this section we detail the parameters of the open clusters and star forming regions whose rotational distributions we used to constrain our model simulations. Table A.1 summarizes their properties.

Appendix A.1: ONC

The Orion Nebula Cluster is a very young cluster, with an age of 0.8−2 Myr (Herbst et al. 2002; Hillenbrand 1997) and located at a distance of about 450 pc (Herbst et al. 2002; Hillenbrand 1997). The rotational data used in this study come from Herbst et al. (2002) and the mass estimates are from Hillenbrand (1997) who derived them using the D’Antona & Mazzitelli (1994) isochrone models. The metallicity of the ONC is [Fe/H]  =  −0.01 ± 0.04 (O’Dell & Yusef-Zadeh 2000).

Appendix A.2: NGC 6530

The age of NGC 6530 lies between 1 and 2.3 Myr (Prisinzano et al. 2005; Mayne et al. 2007; Henderson & Stassun 2012) and its distance is about 1250 pc (Prisinzano et al. 2005, 2012). The rotational data used here come from Henderson & Stassun (2012). Stellar masses were estimated by Prisinzano et al. (2005, 2007, 2012) by interpolating the theoretical tracks and isochrones of Siess et al. (2000) to the stars location in the V vs. V − I color−magnitude diagram. Prisinzano et al. (2005) assumed a solar metallicity and used the Siess et al. (2000) models with Z = 0.02, Y = 0.277, X = 0.703. In Prisinzano et al. (2012) a metallicity range of − 0.3 <  [Fe/H]  < 0.3 is considered.

Appendix A.3: NGC 2264

The NGC 2264 cluster is 2−3 Myr old (Sung et al. 2009; Teixeira et al. 2012; Affer et al. 2013) located at a distance between 750 and 950 pc (Flaccomio et al. 1999; Mayne & Naylor 2008; Baxter et al. 2009; Cauley et al. 2012; Affer et al. 2013). The rotational data used here, as well as mass estimates, come from Affer et al. (2013) who used the V vs. V − I CMD together with the Siess et al. (2000) isochrones to derive stellar masses. NGC 2264 has a metallicity estimated to range from solar to slightly metal-poor (Tadross 2003; Cauley et al. 2012).

Appendix A.4: NGC 2362

The age of NGC 2362 is about Myr (Moitinho et al. 2001; Mayne et al. 2007; Irwin et al. 2008a) and the cluster is located at a distance of about 1500 pc (Moitinho et al. 2001; Dahm & Hillenbrand 2007; Irwin et al. 2008a). The rotational data used here come from Irwin et al. (2008a) as well as the masses estimates. They used the I magnitude together with the Baraffe et al. (1998) 5 Myr isochrones to derive stellar masses. Dahm & Hillenbrand (2007) assumed a solar-metallicity for this cluster.

Appendix A.5: h PER

The h PER (NGC 869) clsuter is 14 ± 1 Myr old (Currie et al. 2010) located at a distance of about 2.1 kpc (Kharchenko et al. 2005; Currie et al. 2010). The rotational data and mass estimates used in this study come from Moraux et al. (2013). They used the I magnitude together with the Siess et al. (2000) 13.8 Myr isochrone with an extinction A_I = 1 mag (Currie et al. 2010) to derive stellar masses. Currie et al. (2010) reported a metallicity Z = 0.019.

Appendix A.6: NGC 2547

The age of NGC 2547 is about Myr (Naylor & Jeffries 2006; Irwin et al. 2008b) and it lies at a distance of pc (Kharchenko et al. 2005; Naylor & Jeffries 2006). The rotational periods and stellar masses used here come from Irwin et al. (2008b), who used the I magnitude together with the Baraffe et al. (1998) 40 Myr isochrones to determine the masses. The reddening corresponds to A_V = 0.186 (Naylor & Jeffries 2006). Paunzen et al. (2010) report sub-solar metallicity − 0.21 <  [Fe/H]  <  − 0.12.

Appendix A.7: Pleiades

The Pleiades is a 120−125 Myr old cluster (Stauffer et al. 1998) situated at 133 pc (Soderblom et al. 2005). The rotational data used in this study come from Hartman et al. (2010) as do the mass estimates. They used the M_K magnitude together with the Yonsei-Yale (Y2) isochrones (Yi et al. 2001) with an extinction A_K = 0.01 mag (Stauffer et al. 2007) to determine the masses. By using the Siess et al. (2000) 125 Myr isochrones models we recalculated the mass of the stars and we found that the ones derived with the Siess et al. (2000) models are higher by 5% at most. Soderblom et al. (1998) report a metallicity of [Fe/H]  = 0.03 ± 0.05.

Appendix A.8: M 50

The age of M50 (NGC 2323) is about 130 Myr (Kalirai et al. 2003; Irwin et al. 2009) and its distance pc (Kalirai et al. 2003). The rotational data and mass estimates used here come from Irwin et al. (2009) who used the I magnitude together with the Baraffe et al. (1998) 130 Myr isochrones to determine the masses. The reddening of the cluster is E(B − V) = 0.22 mag corresponding to A_V = 0.68 (Kalirai et al. 2003). The metallicity of M50 is believed to be solar (Kalirai et al. 2003; Irwin et al. 2009).

Appendix A.9: M 35

The age estimate for M35 (NGC 2168) ranges from 150 Myr (von Hippel et al. 2002; Meibom et al. 2009) to 180 Myr (Kalirai et al. 2003) and its distance is pc (Kalirai et al. 2003). The rotational data used here come from Meibom et al. (2009). We used the Siess et al. (2000) 130 Myr isochrones together with the (B − V)₀ measurements from Meibom et al. (2009) to estimate the stellar masses. The reddening of the cluster is E(B − V) = 0.20 mag, corresponding to A_V = 0.62 (Kalirai et al. 2003). The metallicity of M35 is [Fe/H]  =  −0.21 ± 0.10 (Z = 0.012) (Barrado y Navascués et al. 2001; Kalirai et al. 2003).

Appendix A.10: M 37

The age of M37 (NGC 2099) is about 550 ± 30 Myr (Hartman et al. 2008) and its distance 1383 − 1490 ± 120 pc (Hartman et al. 2008; Wu et al. 2009). The rotational data used here come from Hartman et al. (2009). We used the Siess et al. (2000) 550 Myr isochrones together with the I magnitude measurements from Hartman et al. (2009) to estimate the mass of the stars. The reddening of the cluster is E(B − V) = 0.227 ± 0.038 mag, corresponding to A_V = 0.70 (assuming R_V = 3.1, Hartman et al. 2008) and A_I = 0.852. The metallicity of M37 has been estimated to be [Fe/H]  = 0.045 ± 0.044 and 0.09 (Hartman et al. 2008; Wu et al. 2009) and Z = 0.011 ± 0.001 − 0.019 (Kalirai et al. 2005; Kang et al. 2007).

Appendix A.11: Praesepe

Praesepe (M44, NGC 2632) is a 578 ± 12 Myr old cluster (Delorme et al. 2011) located at a distance of 182 ± 6 − 187 pc (Kharchenko et al. 2005; van Leeuwen 2009). The rotational data used here come from Delorme et al. (2011). We used the Siess et al. (2000) 578 Myr isochrones together with the (J − K) measurements from Delorme et al. (2011) to estimate the mass of the stars. The reddening of the cluster is E(B − V) = 0.027 ± 0.004 mag, corresponding to A_V = 0.083 (Taylor 2006) and E(J − K) = 0.012. Metallicity estimates range from [Fe/H]  = 0.038 ± 0.039 to 0.27 ± 0.10 (Friel & Boesgaard 1992; Pace et al. 2008).

Appendix A.12: Hyades

The Hyades (Melotte 25) is a 628 ± 14 Myr old cluster (Delorme et al. 2011) located at a distance of 46.45 ± 0.5 pc

(van Leeuwen 2009). The rotational data used here come from Delorme et al. (2011). We used the Siess et al. (2000) 625 Myr isochrones together with the (J − K) measurements from Delorme et al. (2011) to estimate the mass of the stars. The reddening of the cluster is negligible, E(B − V) ≤ 0.0014 mag (Taylor 2006). The metallicity of the Hyades is [Fe/H]  = 0.14 ± 0.05 (Perryman et al. 1998).

Appendix A.13: NGC 6811

The cluster NGC 6811 is 1000 ± 170 Myr old (Kharchenko et al. 2005; Meibom et al. 2011; Janes et al. 2013) located at a distance of pc (Kharchenko et al. 2005; Janes et al. 2013). The rotational data used here come from Meibom et al. (2011). We used the Siess et al. (2000) 1 Gyr isochrones together with the 2MASS J, H, and K measurements from the Kepler archives (http://archive.stsci.edu/kepler/kepler_fov/search.php) to estimate the mean mass of the stars adopting a distance of 1240 pc. The reddening of the cluster is E(B − V) = 0.074 ± 0.024 mag, corresponding to A_V = 0.23 (Janes et al. 2013). The metallicity of NGC 6811 is [Fe/H]  =  −0.19 and Z = 0.012 ± 0.004 (Janes et al. 2013).

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