Discovery of Young, Isolated Planetary Mass Objects in the σ Orionis Star Cluster

By M. Z. Osorio, V. Béjar, E. Martín, R. Rebolo, D. B. Navascues, Coryn A. L. Bailer-Jones, R. Mundt. 2000

281 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

The Orion Nebula and Its Associated Population (2001, background): “Similar claims of discovery of isolated planetary mass objects have also been made for the σ Ori cluster (Zapatero Osorio et al. 2000).”
The formation of free-floating brown dwarves and planetary-mass objects by photo-erosion of prestellar cores (2004, background): “Similar explanations for the formation of free-floating low-mass objects have been proposed by Zapatero Osorio et al. (2000) and Kroupa (2002), but they do not appear to have been explored in detail before now.”
Infrared Spectroscopy of Substellar Objects in Orion (2001, methodology): “Ital., 68, 607 Delfosse X., Tinney C. G., Forveille T., Epchtein N., Borsenberger J., Fouque P., Kimeswenger S., Tiphene D., 1999, A&AS, 135, 41 Hauschildt P. H., Allard F., Baron E., 1999, ApJ, 512, 377 Hillenbrand L. A., 1997, AJ, 113, 1733 Hillenbrand L. A., Carpenter J. M., 2000, ApJ, 540, 236 (”
Identifying Young Brown Dwarfs Using Gravity-Sensitive Spectral Features (2003, methodology): “…groups have reported deep infrared surveys of young star-forming regions at distances ranging from 140- 450 pc (Luhman et al. 1998, 1999ab, 2000ab; Béjar et al. 1999; Stauffer et al. 1999; Ardila et al. 2000; Lucas & Roche 2000; Zapatero Osorio et al. 2000; Mainzer & McLean 2003, among others).”
The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation (2008, background): “Free floating planetary-mass stars – i.e. single field stars with masses < 13M J – have been observed in Orion (Lucas & Roche 2000), in the σ Orionis cluster (Zapatero Osorio et al. 2000) and in IC 348 (Najita et al. 2000).”
Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation (2011, background): “Perhaps more importantly, the minimum mass is also greater than the estimated masses of some objects observed in star-forming regions (Zapatero Osorio et al. 2000, 2002; Kirkpatrick et al. 2001, 2006; Lodieu et al. 2008; Luhman et al. 2008, 2009b; Bihain et al. 2009; Burgess et al. 2009; Weights et…”
Galactic Stellar and Substellar Initial Mass Function (2003, background): “Sigma-Orionis cluster, in spite of its relatively young age, exhibits negligible extinction (Zapatero Osorio et al. 2000), and masses can be inferred from MMRs at the proper age.”
Planet formation and migration (2005, background): “Recently, a population of about 30 very young (a few Myr) free–floating objects with planetary masses (from a few to 13 MJ) has been found in the Sigma Orionis open cluster (Zapatero Osorio et al 2000) and in the Trapezium (Lucas and Roche 2000).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “Examples of such populations include σ Ori (Béjar, Zapatero Osorio & Rebolo 1999), λOri (Barrado y Navascués et al. 2004), and Upper Sco (Slesnick, Carpenter & Hillenbrand 2006).”
Signature of life on exoplanets: Can Darwin produce false positive detections? (2002, background): “Recently, the discovery of 15 “free floating” massive planets (i.e. not orbiting around a star) has been announced in a star forming region (Zapatero Osorio et al. 2000).”
The great escape: how exoplanets and smaller bodies desert dying stars (2011, background): “J. Non-linear Mech., 5, 617 Villaver E., Livio M., 2007, ApJ, 661, 1192 Villaver E., Livio M., 2009, ApJ, 705, L81 Wickramasinghe D. T., Farihi J., Tout C. A., Ferrario L., Stancliffe R. J., 2010, MNRAS, 404, 1984 Wolszczan A., 1994, Sci, 264, 538 Wolszczan A., Frail D. A., 1992, Nature, 355, 145 Wo”
New spectral types L and T (2005, background): “J. 469:706–14 Martı́n EL, Zapatero Osorio MR. 2003.”
The “Mysterious” Origin of Brown Dwarfs (2002, background): “…dwarfs (BDs) have been discovered in the last few years, both within stellar clusters (e.g., Bouvier et al. 1998; Martı́n et al. 1998, 2001; Zapatero Osorio et al. 2000; Luhman et al. 2000; Hillenbrand & Carpenter 2000; Najita et al. 2000; Comerón et al. 2000; Luhman 2000; Moraux et al. 2001;…”
The Substellar Mass Function in σ Orionis (2001, methodology): “Despite the incompleteness of our survey and the possible contamination by several nonmembers of the cluster at these very low masses (see details in Zapatero Osorio et al. 2000), the planetary-mass interval is rather well populated.”
TIDALLY HEATED TERRESTRIAL EXOPLANETS: VISCOELASTIC RESPONSE MODELS (2009, background): “…exists, tides may support island habitable zones around nonluminous primaries such as outer planets, pulsars, ultracool dwarfs (Mart́ın et al. 1999), isolate planets (Osorio et al. 2000), and ejected planets that either retain or accumulate large resonant satellites (Debes & Sigurdsson 2007).”