(1998).

Also we indicate the reddening direction based on Cohen et al. (1981). The diagram is consistent in indicating that these sources are 1-Myr old PMS stars with masses less than ∼3 solar masses. The vast majority of these sources measured in this study are cluster members (Jones and Walker 1988; Sirolimus nmr Getman et al. 2005; Hillenbrand 1997; Lucas et al. 2001). The proper motions and radial velocities of ONC members show a dispersion of a few km s−1 (Jones and Walker 1988; Fűrész et al. 2008), implying that these stars will move within about 1 pc, in 1 Myr. In Fig. 2, the measured degree of CP for each source is generally small. We conclude that none of the detected point sources clearly show significant integrated circular polarizations (>than 1.5 % both in

K s and H bands in the same handedness); one source does have a CP > 1.5%, both in the K s and H bands, but is embedded in the western Bioactive Compound Library ic50 high CP region and hence substantially contaminated. OMC-1S shows aperture circular polarimetry of about 0.3% in K s band. These results are consistent with previous observations (Clayton et al. 2005). Fig. 2 Histograms of circular polarization degree (%) of 353 point-like sources. a in the K s band (2.14 μm); b in the H band (1.63 μm). The histograms are constructed using a bin width of 0.2% Fig. 3 Color-magnitude mafosfamide diagram for 353 point-like sources used in Fig. 2, using their J-band (1.25 μm) and H-band (1.63 μm) data in the same observation. The vertical axis shows J magnitude, and the horizontal axis shows J-H magnitude. Our observational data are plotted with crosses. The filled circles denote the loci of 1 Myr old PMS stars at 460 pc, according to the stellar evolution model by Testi et al. (1998). The assumed masses are 0.1, 0.2, 0.4, 0.6, 0.8, 1, 1.2, 1.5, 2, 2.5, 3, and 3.5 solar masses, from bottom to top (the second point from the top for 3.5 solar

masses), connected by the solid line. The dashed line identifies the reddening law through the loci of the 2.5 solar masses (Cohen et al. 1981) CP in Massive Star-forming Regions: Possible Implications for the Origins of Homochirality We will now discuss the implications of these results for the origin of biomolecular homochirality. Bailey (2001) discusses how CPL in star-forming regions might be important in producing EEs and ultimately seeding homochirality on terrestrial planets. Imaging circular polarimetry of several YSOs (Gledhill et al. 1996; Chrysostomou et al. 1997; Bailey et al. 1998; Chrysostomou et al. 2000; Clark et al. 2000; Ménard et al. 2000; Chrysostomou et al. 2007; Fukue et al. 2009; Clayton et al. 2005) and numerical simulations (Fischer et al. 1996; Wolf et al. 2002; Whitney and Wolff 2002; Lucas et al. 2004; Lucas et al. 2005; Chrysostomou et al.