The circumstellar environment of low-mass protostars: A millimeter continuum mapping survey ?

By Fr'ed'erique Motte, P. Andre'. 2001

310 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/0268d7bd1ff0aff09a2fea1dc9119015018e75db

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atmospheric Science

In Spectroscopy

Citations in the corpus

Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores (2007, unknown): “− (1) Spitzer observations from this work; (2) André et al. (1999); (3) Wu et al. (2007); (4) 2MASS; (5) IRAS ; (6) Young et al. (2006a); (7) Motte & André (2001); (8) Bourke et al. (2006); (9) M. Dunham et al. (2008), in preparation; (10) Kirk et al. (2005); (11) Kauffmann et al. (2008); (12)…”
Star formation in Perseus - Clusters, filaments and the conditions for star formation (2005, background): “…dd:mm:ss mJy/bm K km s−1 75 03:28:42.6 31:06:10 NGC 1333 None 153 2.2 76 03:32:17.8 30:49:46 None No SMM/MM source 1916 1.7 77 03:31:21.0 30:45:28 None I03282+3035 Bachiller et al. (1994); Motte & André (2001) 892 1.1 78 03:47:41.6 32:51:44 None(5) B5 IRS1 Motte & André (2001) 424 ?”
Does IRAS 16293–2422 have a hot core? Chemical inventory and abundance changes in its protostellar environment (2002, background): “However, any disk emission would be significantly diluted in the relatively large beams used here (e.g., Motte & André 2001).”
Systematic Molecular Differentiation in Starless Cores (2001, unknown): “This problem, discussed in detail by Motte & André (2001), requires that a simulation of the onthe-fly observation be carried out before comparison with the data.”
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION (2010, methodology): “The MAMBO beam model resulting from the chopping-scanning observing strategy is described in the Appendix of Motte & André (2001).”
A Survey and Analysis of Spitzer Infrared Spectrograph Spectra of T Tauri Stars in Taurus (2006, background): “The object 04385+2550, also known as Haro 6-33, has been considered as a Class I object by some authors based on its SED shape and bolometric temperature (e.g., Motte & André 2001; Young et al. 2003).”
A Spitzer Census of the IC 348 Nebula (2007, methodology): “Indeed such SED modeling by Eisner et al. of one these Motte & André (2001) “peculiar” class I objects, L1489, nonetheless prefers a disk+envelope structure; thus, for now we retained the SED based protostellar classification. starless cores on the western edge of the ridge.”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “…et al. 1998; Dent et al. 1998; Akeson et al. 1998; Guilloteau & Dutrey 1998; Guilloteau et al. 1999, 2011; Looney et al. 2000; Duvert et al. 2000; Motte & André 2001; Klein et al. 2003; Jensen & Akeson 2003; Duchêne et al. 2003, 2010; Corder et al. 2005; Piétu et al. 2005, 2006, 2011; Lin et…”
The physics of star formation (2003, background): “Motte et al (1998) and Motte and André (2001a) found that when core masses are measured in this way, their distribution of masses resembles the stellar initial mass function, and they suggested on this basis that these cores represent direct stellar progenitors that collapse into stars with…”
Probing the formation of intermediate- to high-mass stars in protoclusters - A detailed millimeter study of the NGC 2264 clumps (2005, result): “Assuming isothermal dust emission in the Rayleigh-Jeans regime, this translates into an average spherical density profile ρ(r) ∝ r−1.4 (cf. Motte & André 2001), which has been normalized so as to yield a total mass of 1650 M⊙ within a radius of 0.4 pc, as observed (cf. Table 6 below).”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, methodology): “…in the Taurus-Auriga star-forming region to address these issues, most of which were carried out at 1.3mm (Weintraub, Sandell, & Duncan 1989; Beckwith et al. 1990; Adams, Emerson, & Fuller 1990; Beckwith & Sargent 1991; Mannings & Emerson 1994; Osterloh & Beckwith 1995; Motte & André 2001).”
The Evolution of Outflow-Envelope Interactions in Low-Mass Protostars (2006, background): “Dust continuum emission surrounding the source was mapped at 1.3 mm (at ∼ 12′′ resolution) by Motte & André (2001).”
Initial highlights of the HOBYS key program, the Herschel imaging survey of OB young stellar objects (2010, background): “This size-wavelength relation is thus most likely related to the classical distribution of gas under the influence of gravity observed with optically-thin column density tracers (Motte & André 2001; Beuther et al. 2002)1.”
Tracing the Mass during Low-Mass Star Formation. II. Modeling the Submillimeter Emission from Preprotostellar Cores (2000, methodology): “Our model is consistent with 1.3 mm continuum models of Motte & André (2001), which assume a power law temperature distribution, Td(r) ∝ r−q, (p = 1.2 ± 0.6 for q = 0.2 ∓ 0.2).”
THE LEGACY OF SCUPOL: 850 μm IMAGING POLARIMETRY FROM 1997 TO 2005 (2009, unknown): “…Curran et al. (2007); et al. (2004); Curran et al. (2007) Girart et al. (2006, 1999); (IRAS 2 only) Glenn et al. (1999) IRAS 03282+3035 YSO 12 0.3 Motte & André (2001) Y Barnard 1 SFR 13 0.250 ± 0.050 Enoch et al. (2006) N Matthews & Wilson (2002b) Matthews et al. (2003, 2008) HH211/IC348…”