A population of very young brown dwarfs and free‐floating planets in Orion

By P. Lucas, P. Roche. 2000

229 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bb40107cd8bda0c74dcc1410c667df262715ac47

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Citations in the corpus

Infrared Spectroscopy of Substellar Objects in Orion (2001, background): “The second reason to expect significant extinction is that HC used an optical:infrared extinction conversion based on the interstellar medium, which significantly underestimates the infrared extinction in Orion (Cardelli et al. 1989) because of the presence of slightly larger dust grains in the envi”
The formation of a star cluster: predicting the properties of stars and brown dwarfs (2002, background): “Surveys of young star clusters are beginning to probe masses down to this theoretical minimum mass (Zapatero Osorio et al. 1999; Lucas & Roche 2000; Béjar et al. 2001; Mart́in et al. 2001b; Lucas et al. 2001), with the masses of some objects estimated to be as low as 3 Jupiter-masses (Zapatero…”
Embedded Clusters in Molecular Clouds (2003, methodology): “Deep infrared surveys of this cluster have been performed using the HST (Luhman et al 2000), the Keck Telescope (Hillenbrand & Carpenter 2000), UKIRT (Lucas & Roche 2000), and the NTT (Muench et al. 2002) and have produced infrared luminosity functions and mass functions that sample well into the su”
Revisiting the cosmic cooling crisis (2001, background): “Although these objects are likely to be a significant component of the mass budget, there is no strong evidence that they are more abundant than expected from standard IMFs (Fuchs et al. 1998; Gizis et al. 2000; Lucas & Roche 2000).”
The Orion Nebula and Its Associated Population (2001, background): “Recent IHK observations to very faint limits (Lucas & Roche 2000) find several objects below the deuterium-burning (planetary) threshold of 0.013 M¯, which they identify as free-floating planets, i.e., planets not gravitationally attached to a specific star.”
Identifying Young Brown Dwarfs Using Gravity-Sensitive Spectral Features (2003, background): “…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).”
Young Massive Star Clusters (2010, background): “Several such free-floating objects have been found in the Orion Trapezium cluster (Lucas & Roche 2000).”
X-Ray-emitting Young Stars in the Orion Nebula (2002, background): “…Objects (Brown Dwarfs) The ONC is perhaps the best laboratory available to study the magnetic activity of PMS brown dwarfs (BDs) as over 100 such objects have been found in recent deep nearinfrared imaging of the cluster (Hillenbrand & Carpenter 2000; Luhman et al. 2000; Lucas & Roche 2000).”
SpeX SPECTROSCOPY OF UNRESOLVED VERY LOW MASS BINARIES. I. IDENTIFICATION OF 17 CANDIDATE BINARIES STRADDLING THE L DWARF/T DWARF TRANSITION (2009, background): “…Muench et al. 2007), and sources specifically noted to have peculiar spectra associated with low surface gravities, subsolar metallicites or unusual cloud properties (e.g., Lucas & Roche 2000; Burgasser et al. 2003a; Knapp et al. 2004; Chiu et al. 2006; Cruz et al. 2007, 2009; Looper et al. 2008b).”
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).”
Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, background): “Finally, the planet–planet scattering model predicts a significant number of extremely loosely bound and free floating giant planets, which may also be observable (Lucas & Roche 2000; Zapatero Osorio et al. 2002; Veras et al. in prep).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “…to the Trapezium Cluster at the center of the ONC because it is very compact and is located in front of a dense molecular cloud, reducing the contamination from background stars (Hillenbrand & Carpenter 2000; Lucas & Roche 2000; Lucas, Roche & Tamura 2005; Luhman et al. 2000; Muench et al. 2002).”
Toward Spectral Classification of L and T Dwarfs: Infrared and Optical Spectroscopy and Analysis (2001, background): “Young brown dwarfs have been discovered in large numbers in star-forming regions (see, e.g., Hambly et al. 1999 ; PinÐeld et al. 2000 ; Luhman et al. 2000 ; Lucas & Roche 2000).”
The Substellar Mass Function in σ Orionis (2001, background): “8 below the starÈsubstellar mass borderline have been obtained recently for other young clusters (Luhman et al. 2000 ; Lucas & Roche 2000 ; Hillenbrand & Carpenter 2000 ; Najita et al. 2000 ; et al. 2000 ;Mart• n Moraux et al. 2001), showing that the formation of brown dwarfs is a quite common…”