The Initial Mass Function in the Taurus Star-forming Region

By C. Briceño, K. Luhman, L. Hartmann, J. Stauffer, J. D. Kirkpatrick. 2002

282 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/1a808bc5807c20ab3b98e251f959fc2bca75528e

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Citations in the corpus

An Empirical Criterion to Classify T Tauri Stars and Substellar Analogs Using Low-Resolution Optical Spectroscopy (2003, unknown): “These results are depicted in Figure 4, which includes the Orion population (from Herbig & Bell 1988; Alcalá et al. 1996, 1998, 2000), Taurus (Briceño et al. 1993, 1998, 1999, 2002; Alencar & Basri 2001; Mart́ın et al. 2001a; Luhman et al. 2003a; White & Basri 2003; Muzerolle et al. 2003) IC348 (H”
Implications for the formation of star clusters from extragalactic star formation rates (2004, methodology): “The data for these assumptions are taken from Briceño et al. (2002), Kroupa (2001), Hartmann (2002), Massey & Hunter (1998), Palla & Stahler (2002) and Selman et al. (1999).”
Characterizing Young Brown Dwarfs Using Low-Resolution Near-Infrared Spectra (2006, background): “Spectral types of several young, lateM-type brown dwarfs have been determined by comparing observed optical spectra to spectra of giants and dwarfs, with the best fit usually being an average of giant and dwarf spectra (Guieu et al. 2006; Luhman 2004; Briceño et al. 2002).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “However, beyond a spectral type of ∼M9, young objects become redder than their older counterparts in J − K (Allers et al. 2010; Bihain et al. 2010; Briceño et al. 2002; Cruz, Kirkpatrick & Burgasser 2009; Faherty et al. 2009; Kirkpatrick et al. 2006, 2008; Schmidt et al. 2010).”
Accretion in Young Stellar/Substellar Objects (2003, background): “Since our observations were obtained, many more such objects have been discovered in star-forming regions and young clusters (see, e.g., Briceño et al. 2002), and thus, our sample is not complete, although it is likely to be representative of these very low masses.”
Identifying Young Brown Dwarfs Using Gravity-Sensitive Spectral Features (2003, methodology): “The spectrum of KPNO-Tau 4 shows spectroscopic characteristics intermediate between the field dwarf and the giant (cf. Briceño et al. 2002).”
The Spectroscopically Determined Substellar Mass Function of the Orion Nebula Cluster (2004, background): “Briceño et al. (2002) defines the ratio of the numbers of substellar and stellar objects as: RSS = N(0.02 ≤ M/M⊙ ≤ 0.08) N(0.08 < M/M⊙ ≤ 10) .”
A Census of the Young Cluster IC 348 (2003, methodology): “The values for the latter three clusters were compiled by Briceño et al. (2002).”
The stellar and sub-stellar IMF of simple and composite populations (2011, background): “Based on some additional observations, Luhman (2004) revised the Briceño et al. (2002) results by finding that the number of BDs per star had been underestimated in Taurus-Auriga.”
On the Evolutionary Status of Class I Stars and Herbig-Haro Energy Sources in Taurus-Auriga (2004, background): “This distribution of class I star masses agrees very well with the initial mass function measured from T Tauri stars in Taurus (Briceño et al. 2002).”
The “Mysterious” Origin of Brown Dwarfs (2002, background): “The deficit of BDs in Taurus relative to the Trapezium cluster has been confirmed in a more recent work by Briceño et al. (2002), although reduced to approximately a factor of 2 between the BD abundance of Orion and Taurus.”
The relation between the most-massive star and its parental star cluster mass (2009, unknown): “…(1990, 1993), 2: Faustini et al. (2009), 3: Testi et al. (1997, 1998, 1999); Wang & Looney (2007), 4: Kaas et al. (2004), 5: Cohen & Kuhi (1979); Briceño et al. (2002), 6: Sellgren (1983); Depoy et al. (1990); Lada et al. (1991), 7: Gutermuth et al. (2004); Wang & Looney (2007), 8: Luhman…”
The T Tauri Phase Down to Nearly Planetary Masses: Echelle Spectra of 82 Very Low Mass Stars and Brown Dwarfs (2005, methodology): “The significance of this is unclear with the present errors; better number statistics, especially in Oph, can tell us whether there is a decline by the age of IC 348 and Cha I, compared to the younger Oph and Taurus, or whether Taurus has a larger CTTS fraction relative to both the younger Oph and o”
The Disk Population of the Chamaeleon I Star-forming Region (2008, background): “5 as cooler objects were discovered in Taurus and Chamaeleon I (Briceño et al. 2002; Luhman et al. 2004; Luhman 2007).”
AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, methodology): “Meanwhile, the XEST fields have been fully covered at optical and near-IR wavelengths by either deep wide-field imaging (Briceño et al. 2002; Luhman 2004c; Guieu et al. 2006) or all-sky catalogs (Luhman 2006), which have produced a high level of completeness for classes II and III between 0.1-0.02…”
The origin of the initial mass function and its dependence on the mean Jeans mass in molecular clouds (2004, background): “The m agnitudeand senseofthedependenceoftheproportion of brown dwarfs on the density ofthe star-form ing cloud reproduce the observed result that the Taurus star-form ing region has a lower abundance of brown dwarfs than the O rion Trapezium Cluster (Briceno et al.2002;Slesnick et al.2004;Luhm an 20”