L1498 is a classic example of a dense cold pre-protostellar core. To study the evolutionary status, the structure, dynamics, and chemical properties of this core we have obtained high spatial and high spectral resolution observations of molecules tracing densities of 10~3-10~5 cm~(-3). We observed CCS, NH_3, C_3H_2, and HC_7N with NASA's DSN 70 m antennas. We also present large-scale maps of C~(18)O and ~(13)CO observed with the AT&T 7 m antenna. For the high spatial resolution maps of selected regions within the core we used the VLA for CCS at 22 GHz, and the Owens Valley Radio Observatory (OVRO) MMA for CCS at 94 GHz and CS (2-1). The 22 GHz CCS emission marks a high-density [n(H_2) > 10~4 cm~(-3)] core, which is elongated with a major axis along the SE-NW direction. NH_3 and C_3H_2 emissions are located inside the boundary of the CCS emission. C~(18)O emission traces a lower density gas extending beyond the CCS boundary. Along the major axis of the dense core, CCS, NH_3 and C_3H_2 emission show evidence of limb brightening. The observations are consistent with a chemically differentiated onion-shell structure for the L1498 core, with NH_3 in the inner and CCS in the outer parts of the core. The high angular resolution (9″-12″) spectral line maps obtained by combining NASA Goldstone 70 m and VLA data resolve the CCS 22 GHz emission in the southeast and northwest boundaries into arclike enhancements, supporting the picture that CCS emission originates in a shell outside the NH_3 emitting region. Interferometric maps of CCS at 94 GHz and CS at 98 GHz show that their emitting regions contain several small-scale dense condensations. We suggest that the differences between the CCS, CS, C_3H_2, and NH_3 emission are caused by a time-dependent effect as the core evolves slowly. We interpret the chemical and physical properties of L1498 in terms of a quasi-static (or slowly contracting) dense core in which the outer envelope is still growing. The growth rate of the core is determined by the density increase in the CCS shell resulting from the accretion of the outer low-density gas traced by C~(18)O. We conclude that L1498 could become unstable to rapid collapse to form a protostar in less than 5 x 10~6 yr.
展开▼
