The Star-Formation History And Accretion Disk Fraction Of The Scorpius-Centaurus Ob Association
Creators: name: Pecaut, Mark
Publisher: name: Zenodo
Year: 2013
Subjects: Pure sciences
Accretion disk fraction
Intrinsic colors
Pre-main sequence stars
Scorpius-centaurus
Stellar ages
Temperatures

description: We present a study of the star-formation history and accretion disk fraction of ~0.6-1.8 Msun stars in the nearest OB Association, Scorpius-Centaurus (Sco-Cen; 10-20 Myr; 100-200 pc). We have performed a low-resolution spectroscopic survey for new, low-mass K- and M-type members of all three subgroups - Upper Scorpius (US), Upper Centaurus-Lupus (UCL) and Lower Centaurus-Crux (LCC). We find that young, pre-main sequence stars have different intrinsic colors for a given spectral type than their main-sequence (MS) counterparts and therefore MS colors and temperatures are unsuitable for de-reddening the low-mass members of Sco-Cen and placing them on an H-R diagram. Using nearby, pre-MS, unreddened moving groups, we derive a spectral type-intrinsic color sequence appropriate for 5-30 Myr old pre-MS stars, and use synthetic spectral energy distribution fits to infer the proper temperature and bolometric correction scale for these young stars. We use this new pre-MS intrinsic color and temperature calibration to place our ~150 newly identified members of Sco-Cen on an H-R diagram. We derive isochronal ages for the B-type MS turn-off and the pre-MS F-type, G-Type members and the K- and M-type members of Sco-Cen. We find a Teff-dependent age trend in the K/M-type stars, similar to previous studies of other nearby star-forming regions. Our F- and G-type isochronal ages for Upper Centaurus-Lupus (UCL; 16±2 Myr;=142 pc) and Lower Centaurus-Crux (LCC; 16±3 Myr; =118 pc) are consistent with previous results. However, our results for Upper Scorpius (US; 10±3 Myr; =145 pc) indicate it is a factor of two older than previously thought. Using ~650 of the pre-MS members of Sco-Cen, we construct an age map, which reveals regions which are systematically younger or older than the mean Sco-Cen age, suggesting that the star-formation history of the three subgroups is more complex than the simple division into three subgroups would imply. Finally, we find a primordial disk fraction for US, UCL and LCC of 9+4-2%, 5+2 -1% and 3+3-1%, respectively, for K-type stars decreasing to &lt;19% (95% CL), 2+5-1%, and 2 +4-1%, respectively, for F-type stars at ~10 Myr, ~16 Myr, and ~16 Myr, respectively.
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