Astronomy and Astrophysics, volume 487, 993-1017 (2008/9-1)
MAMBO mapping of Spitzer c2d small clouds and cores.
KAUFFMANN J., BERTOLDI F., BOURKE T.L., EVANS II N.J. and LEE C.W.
Abstract (from CDS):
To study the structure of nearby (<500 pc) dense starless and star-forming cores with the particular goal to identify and understand evolutionary trends in core properties, and to explore the nature of Very Low Luminosity Objects (≤0.1 L☉; VeLLOs). Using the MAMBO bolometer array, we create maps unusually sensitive to faint (few mJy per beam) extended (≃5 ') thermal dust continuum emission at 1.2 mm wavelength. Complementary information on embedded stars is obtained from Spitzer, IRAS, and 2MASS. Our maps are very rich in structure, and we characterize extended emission features (``subcores'') and compact intensity peaks in our data separately to pay attention to this complexity. We derive, e.g., sizes, masses, and aspect ratios for the subcores, as well as column densities and related properties for the peaks. Combination with archival infrared data then enables the derivation of bolometric luminosities and temperatures, as well as envelope masses, for the young embedded stars. Starless and star-forming cores occupy the same parameter space in many core properties; a picture of dense core evolution in which any dense core begins to actively form stars once it exceeds some fixed limit in, e.g., mass, density, or both, is inconsistent with our data. A concept of necessary conditions for star formation appears to provide a better description: dense cores fulfilling certain conditions can form stars, but they do not need to, respectively have not done so yet. Comparison of various evolutionary indicators for young stellar objects in our sample (e.g., bolometric temperatures) reveals inconsistencies between some of them, possibly suggesting a revision of some of these indicators. Finally, we challenge the notion that VeLLOs form in cores not expected to actively form stars, and we present a first systematic study revealing evidence for structural differences between starless and candidate VeLLO cores.
stars: formation - ISM: evolution - ISM: structure - ISM: dust, extinction - ISM: clouds
VizieR on-line data:
<Available at CDS (J/A+A/487/993): object.dat table3.dat table4.dat table5.dat fits/*>
Table 3: [KBB2008] LNNNN CN, [KBB2008] LNNNNA CN, [KBB2008] LNNNNA-N CN, [KBB2008] LNNNN-N CN, [KBB2008] B18-N CN, [KBB2008] TMC-N CN, [KBB2008] TMC-NA CN, [KBB2008] IRAS05413 CN, [KBB2008] CB188 CN, [KBB2008] Bern48 CN, [KBB2008] LNNNN PN, [KBB2008] LNNNNA PN, [KBB2008] LNNNNA-N PN, [KBB2008] LNNNN-N PN, [KBB2008] B18-N PN, [KBB2008] TMC-N PN, [KBB2008] TMC-NA PN, [KBB2008] IRAS05413 PN, [KBB2008] CB188 PN, [KBB2008] Bern48 PN N=86+108..
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