A Complete Search for Dense Cloud Cores in Taurus

By T. Onishi, A. Mizuno, A. Kawamura, K. Tachihara, Y. Fukui. 2002

167 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/dba96837773dc40d19bca2815ed1f564d2031e15

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Citations in the corpus

Galactic Stellar and Substellar Initial Mass Function (2003, background): “If confirmed, the difference in BD detection for instance between isolated regions like Taurus (n ∼ 1-10 pc−3) and high-density starforming regions like e.g. Orion, Ophiucus or Trapezium (n ∼ 103-104 pc−3) might thus reflect the importance of the level of turbulence in the cloud on the low-mass end ”
On the Rapid Collapse and Evolution of Molecular Clouds (2007, background): “Inside the denser cores where individual stars form, it can be as short as several ×105 years (e.g., Onishi et al. 2002).”
A SCUBA survey of Orion -the low-mass end of the core mass function (2006, result): “The high mass side of the mass function declines as a power-law to higher masses, in agreement with previous studies of both Orion and other star-forming regions (Testi & Sargent 1998; Motte et al. 1998, 2001; Johnstone et al. 2001; Onishi et al. 2002; Johnstone et al. 2006).”
The Mass Distribution and Lifetime of Prestellar Cores in Perseus, Serpens, and Ophiuchus (2008, background): “Evidence for a direct link between the CMD and the IMF has been found previously based on dust emission surveys of small regions (Testi & Sargent 1998; Motte et al. 1998), as well as molecular line observations of dense cores (Onishi et al. 2002).”
The “Mysterious” Origin of Brown Dwarfs (2002, background): “…of prestellar condensations is indistinguishable from the stellar IMF (Motte et al. 1998, 2001; Testi & Sargent 1998; Onishi et al. 1999; Johnstone et al. 2000b, 2000a, 2001; Onishi et al. 2002), both in the functional shape and in the range of masses, including BD mass cores (Walsh et al. 2004).”
Magnetic Braking and Protostellar Disk Formation: The Ideal MHD Limit (2007, background): “For example, in the Taurus molecular clouds, the dense HCO+ cores typically contain a few to several solar masses (Onishi et al. 2002), whereas the typical mass of the YSOs is only ∼ 0.5 M⊙ (Kenyon & Hartmann 1995).”
Protostellar Turbulence Driven by Collimated Outflows (2007, background): “For example, Onishi et al. (2002) derived an average virial mass of about 5M⊙ for the H 13CO+ cores in the Taurus molecular clouds.”
On the Evolutionary Status of Class I Stars and Herbig-Haro Energy Sources in Taurus-Auriga (2004, background): “The 44 starless cores in Taurus (Onishi et al. 2002) may contain a yet hidden population of class 0 stars.”
Theory of Star Formation (2007, unknown): “Similar core mass functions (CMFs) may be derived using extinction data from well-sampled maps (Lada, Alves, & Lombardi, 2007), and molecular line maps in high-density tracers (Onishi et al., 2002).”
Large-Scale Structure of the Molecular Gas in Taurus Revealed by High Linear Dynamic Range Spectral Line Mapping (2008, methodology): “Some examples include Langer et al. (1995) employing CCS, Onishi et al. (1996, 1998) using C18O, Onishi et al. (2002) using H13CO+, and Tatematsu et al. (2004) employing N2H +.”
Magnetically Regulated Star Formation in Three Dimensions: The Case of the Taurus Molecular Cloud Complex (2008, background): “The mean density of the core so identified is estimated at ∼ 105 cm−3, comparable to those of H13CO+ cores in Taurus studied by Onishi et al. (2002).”
WHAT DRIVES THE EXPANSION OF GIANT H ii REGIONS?: A STUDY OF STELLAR FEEDBACK IN 30 DORADUS (2010, background): “The physical properties of these clouds set the initial conditions for protostellar collapse and may define the stellar initial mass function (IMF) [Motte et al. 1998; Testi & Sargent 1998; Onishi et al. 2002].”
AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, background): “…al. 1983; Reipurth et al. 1990; Sartoretti et al. 1998; Walter 1986; Walter et al. 1988; White & Basri 2003; Zaitseva et al. 1985, 1990) and the median radial velocity of the dense gas based on observations of C18O, CS, N2H +, and H13CO+ (Lee et al. 1999; Onishi et al. 2002; Tatematsu et al. 2004).”
The mass function of dense molecular cores and the origin of the IMF (2006, methodology): “Tachihara et al. (2002) and Onishi et al. (2002), using C18O and H13CO+ as tracers of dense gas, suggest that the stellar and core mass distributions are similar.”
The Global Evolution of Giant Molecular Clouds. I. Model Formulation and Quasi-Equilibrium Behavior (2006, unknown): “…expect if the star formation rate were simply following the column density to some power, suggesting that magnetic fields may play a secondary role – Onishi et al. 1998, 1999, 2002; Johnstone et al. 2004 – though see Hatchell et al. 2005 who find that low column densities reduce but do not…”
The stellar and sub-stellar IMF of simple and composite populations (2011, result): “Similar results have indeed been obtained for the Serpens clouds and for the clouds in Taurus–Auriga (Testi & Sargent 1998; Onishi et al. 2002, respectively).”
The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X (2007, background): “This is particularly surprising since the lifetime of pre-stellar cores and condensations in nearby,lowmass star-forming regions is more than two orders of magnitude longer (1− 4 × 105 yr, e.g. Onishi et al. 2002; Kirk et al. 2005; André et al. 2007).”
Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region (2013, background): “…in the relatively low-density CO-emitting gas of L1495/B213, lies a population of dense cores, which has been explored by Benson & Myers (1989) and Onishi et al. (2002) using NH3 and H13CO+ observations, respectively, with additional and more limited N2H+ observations presented by Tatematsu et…”