Exploring the Full Stellar Population of the Upper Scorpius OB Association

By T. Preibisch, Anthony G. A. Brown, T. Bridges, E. Guenther, H. Zinnecker. 2002

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In Astronomy and Astrophysics

Citations in the corpus

The T Tauri Phase Down to Nearly Planetary Masses: Echelle Spectra of 82 Very Low Mass Stars and Brown Dwarfs (2005, methodology): “MOHANTY, JAYAWARDHANA, & BASRI500 (Luhman et al. 2003b, Luhman 2004), 3Myr for RCrA (Wilking et al. 1997), 5 Myr for Upper Sco (Preibisch et al. 2002), and 10 Myr for TW HyA (Webb et al. 1999; Jayawardhana et al. 1999).”
Optical Spectroscopy of the Surface Population of the ρ Ophiuchi Molecular Cloud: The First Wave of Star Formation (2005, methodology): “…H-R diagrams for low-mass members of the Upper Scorpius subgroup, using the same set of theoretical evolutionary tracks and isochrones and not corrected for unresolved binaries, shows no discernible difference in age or age spread (e.g., Preibisch & Zinnecker 1999; Preibisch et al. 2001, 2002).”
The primordial binary population. I. A near-infrared adaptive optics search for close visual companions to A star members of Scorpius OB2 (2004, unknown): “IMF α is equal to the IMF in US that was derived by Preibisch et al. (2002). histogram).”
Inverse dynamical population synthesis: Constraining the initial conditions of young stellar clusters by studying their binary populations (2012, background): “USco-A’s stellar IMF between 0.1 and 20M⊙ is consistent with the field (i.e. canonical) stellar mass function and the total stellar mass is estimated to be about 2060M⊙ (Preibisch et al. 2002).”
New constraints on the multiplicity of massive young stars in Upper Scorpius (2015, background): “In a series of spectroscopic studies, Preibisch & Zinnecker (1999) and Preibisch et al. (2002) have identified a large and statistically complete sample of low-mass members and then investigated the stellar population and star formation history of Upper Scorpius over the full stellar mass range…”
Radiative Shock-induced Collapse of Intergalactic Clouds (2003, background): “…may also be applied to radiative shocks and resulting star formation triggered by other mechanisms, such as in the wake of supernova blast waves (Preibisch et al. 2002), collisions of interstellar or intergalactic clouds (Smith 1980), and ram pressure on gas-rich galaxies that fall into galaxy…”
Astrophysics with Extraterrestrial Materials (2016, background): “Although still a viable model supported by observations of triggered star formation (Preibisch et al. 2002), in the intervening years many additional ideas have been put forward to explain the relatively high abundances of 26Al and other SLRs with lifetimes shorter than ∼10 Myr.”
ALMA OBSERVATIONS OF CIRCUMSTELLAR DISKS IN THE UPPER SCORPIUS OB ASSOCIATION (2016, background): “This is in conflict with the canonical age of ∼ 5 Myr based on the HR diagram positions of lower mass stars (de Geus et al. 1989; Preibisch et al. 2002; Slesnick et al. 2008).”
A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, background): “Selection of Young Stars with GALEX Stellar activity is known to be an indicator of youth (Preibisch et al. 2002, 2005), so X-ray and UV all-sky surveys are well-suited to finding active young stars.”
Direct Imaging and Spectroscopy of a Planetary-Mass Candidate Companion to a Young Solar Analog (2008, background): “Furthermore, for this effective temperature, the predictions of the NextGen evolutionary models (Baraffe et al. 1998, 2002), usingαmix = 1.9, are in very good agreement with the photometric measurements of the primary for an age of 5 Myr and a distance of 150 pc (see Fig.”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, methodology): “For these we have adopted ensemble ages from the literature: 5 Myr for the Upper Scorpius OB association (Preibisch et al. 2002), 80 Myr for α Persei (Ventura et al. 1998), 120 Myr for the Pleiades (Ventura et al. 1998), and 600 Myr for the Hyades (Perryman et al. 1998).”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “…to Mdust∼0.3 M⊕ and Mgas∼1.0 MJup, respectively; Barenfeld et al. (2016), who observed 106 disks in the more evolved Upper Sco region (∼5–10 Myr at 145 pc; Preibisch et al. 2002; Pecaut et al. 2012) with sensitivities of Mdust∼0.1 M⊕; and Pascucci et al. (2016), who surveyed 93 protoplanetary…”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “6 ) is, for instance, observed for massive stars in the Orion nebula (Preibisch et al. 2002).”
Evidence for Mass-dependent Circumstellar Disk Evolution in the 5 Myr Old Upper Scorpius OB Association (2006, background): “…de Zeeuw et al. 1999), (b) optical color–magnitude diagrams and spectroscopic verification of lithium (G, K, and M stars; Preibisch & Zinnecker 1999; Preibisch et al. 2002), and (c) x–ray sources subsequently verified as lithium-rich, pre-mainsequence stars (G, K, & M stars; Walter et al. 1994;…”
Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics (2008, methodology): “Members of Upper Sco were taken from Preibisch & Zinnecker (1999) and Walter et al. (1994); we adopt the mean group age (5 Myr) from Preibisch et al. (2002).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “5 Myr which is consistent with the earlier results (e.g., de Geus et al. 1989; Preibisch et al. 2002).”
Herbig Ae/Be Stars in nearby OB Associations (2004, background): “For this reason, OB associations are excellent for studying young stellar objects covering a complete range of mass (e.g., Preibisch et al. 2002).”