Journal
ASTROPHYSICAL JOURNAL
Volume 745, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/745/2/117
Keywords
ISM: individual objects (Oph A-N6); stars: formation; stars: low-mass
Categories
Funding
- National Science Foundation [0708158]
- Smithsonian Institution
- Academia Sinica
- INSU/CNRS (France)
- MPG (Germany)
- IGN (Spain)
- Science and Technology Facilities Council [ST/J003018/1, ST/I001557/1, ST/F002092/1] Funding Source: researchfish
- STFC [ST/F002092/1, ST/I001557/1, ST/J003018/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0708158] Funding Source: National Science Foundation
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We present high spatial (<300 AU) and spectral (0.07 km s(-1)) resolution Submillimeter Array observations of the dense starless cluster core Oph A-N6 in the 1 mm dust continuum and the 3-2 line of N2H+ and N2D+. The dust continuum observations reveal a compact source not seen in single-dish observations, of size similar to 1000 AU and mass 0.005-0.01 M-circle dot. The combined line and single-dish observations reveal a core of size 3000 x 1400 AU elongated in a NW-SE direction, with almost no variation in either line width nor line center velocity across the map, and very small non-thermal motions. The deuterium fraction has a peak value of similar to 0.15 and is >0.05 over much of the core. The N2H+ column density profile across the major axis of Oph A-N6 is well represented by an isothermal cylinder, with temperature 20 K, peak density 7.1 x 10(6) cm(-3), and N2H+ abundance 2.7 x 10(-10). The mass of Oph A-N6 is estimated to be 0.29 M-circle dot, compared to a value of 0.18 M-circle dot from the isothermal cylinder analysis, and 0.63 M-circle dot for the critical mass for fragmentation of an isothermal cylinder. Compared to isolated low-mass cores, Oph A-N6 shows similar narrow line widths and small velocity variation, with a deuterium fraction similar to evolved dense cores. It is significantly smaller than isolated cores, with larger peak column and volume density. The available evidence suggests that Oph A-N6 has formed through the fragmentation of the Oph A filament and is the precursor to a low-mass star. The dust continuum emission suggests that it may already have begun to form a star.
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