2010
DOI: 10.1088/0004-637x/712/2/1010
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Complex Structure in Class 0 Protostellar Envelopes

Abstract: We use archived IRAC images from the Spitzer Space Telescope to show that many Class 0 protostars exhibit complex, irregular, and non-axisymmetric structure within their dusty envelopes. Our 8 µm extinction maps probe some of the densest regions in these protostellar envelopes. Many of the systems are observed to have highly irregular and non-axisymmetric morphologies on scales 1000 AU, with a quarter of the sample exhibiting filamentary or flattened dense structures. Complex envelope structure is observed in … Show more

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Cited by 114 publications
(155 citation statements)
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References 103 publications
(119 reference statements)
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“…); using our fitted prestellar core mass and temperature, we find that the ratio of gravitational energy to thermal and turbulent energy is E grav /(E therm + E turb ) 0.9, a marginally sub-critical value which is expected for prestellar cores. For comparison, Tobin et al (2010) derive a mass of ∼3-4 M for the prestellar core (integrated over a similar area and scaled to a distance of 200 pc) using the 8 μm shadow (see Fig. 1), a good agreement given the uncertainties in both mass derivation methods.…”
Section: Discussionmentioning
confidence: 77%
See 1 more Smart Citation
“…); using our fitted prestellar core mass and temperature, we find that the ratio of gravitational energy to thermal and turbulent energy is E grav /(E therm + E turb ) 0.9, a marginally sub-critical value which is expected for prestellar cores. For comparison, Tobin et al (2010) derive a mass of ∼3-4 M for the prestellar core (integrated over a similar area and scaled to a distance of 200 pc) using the 8 μm shadow (see Fig. 1), a good agreement given the uncertainties in both mass derivation methods.…”
Section: Discussionmentioning
confidence: 77%
“…The CB 244 globule contains two submm peaks, one associated with a Class 0 protostar located at RA = 23 h 25 m 46.3 s , Dec = +74 • 17 39.1 , and one associated with a starless core located at RA = 23 h 25 m 27.1 s , Dec = +74 • 18 25.3 . The protostar drives a molecular outflow (e.g., Clemens et al 1991), while the detection of the CB 244 starless core was first published as an additional source inside the globule by Launhardt (1996) and Shirley et al (2000) and produces both an 8 μm (Tobin et al 2010) and a 24 μm shadow. The YSO and starless core are separated by ∼90 , and are therefore well resolved throughout the PACS and SPIRE bands.…”
Section: Introductionmentioning
confidence: 99%
“…The light source can thus be spatially extended relative to the projected spatial scale of ice abundance structures, even if it looks like a point source (e.g. Tobin et al 2008Tobin et al , 2010, and the absorbing material in the envelope and/or disk also has non-uniform spatial distributions. Although the radiative transfer modeling of such an envelope and disk system is beyond the scope of the present work, it is important to discuss the location of ice in our targets.…”
Section: Location Of the Icementioning
confidence: 99%
“…The maps show a dark patch against the nebulous far-IR emission that closely resembles the dark patch seen at visible wavelengths. The MSX, ISO, and Spitzer space telescopes have detected clouds in absorption at mid-IR (5-30 μm) wavelengths against the diffuse IR background of the Galaxy (e.g., Bacmann et al 2000;Stutz et al 2008;Tobin et al 2010;Stutz et al 2009a), in a few cases even at 70 μm (Stutz et al 2009b). However, the detection of the NGC 1999 globule by PACS would be the first detection of a dark globule in absorption at 160 μm.…”
Section: Introductionmentioning
confidence: 99%