The physical and chemical properties of the $\rho$ ophiuchi A dense core

TL;DR

This study investigates the physical and chemical characteristics of the $ ho$ Ophiuchi A dense core using multi-line observations, revealing temperature variations, chemical depletion patterns, and signs of outflow activity in embedded sources.

Contribution

It provides detailed combined interferometric and single-dish observations of the $ ho$ Oph A core, highlighting external heating effects and chemical depletion in dense gas regions.

Findings

C$^{18}$O emission peaks at the edges of the core, indicating external heating.

C$^{18}$O and N$_2$H$^+$ show anti-correlation and depletion in dense regions.

Evidence of outflow activity from the embedded source SM1.

Abstract

The physical and chemical properties of the $\rho$ Ophiuchi A core were studied using 1.3 mm continuum and molecular lines such as C$^{18}$O, C$^{17}$O, CH$_3$OH and H$_2$CO observed with the Submillimeter Array (SMA). The continuum and C$^{18}$O data were combined with the single-dish data obtained with the IRAM 30m telescope and the James Clerk Maxwell Telescope (JCMT), respectively. The combined 1.3 mm continuum map reveals three major sources, SM1, SM1N and VLA1623 embedded in the extended emission running along the north-south direction, and two additional compact condensations in the continuum ridge connecting SM1 and VLA1623.The spatial distribution of the C$^{18}$O emission is significantly different from that of the continuum emission; the C$^{18}$O emission is enhanced at the eastern and western edges of the continuum ridge, with its peak brightness temperature of 40--50 K. This supports the picture that the $\rho$-Oph A core is heated externally from the nearby stars Oph S1 and HD147889. In contrast, the C$^{18}$O intensity is lower than 15--20 K at the center of the ridge where the continuum emission is bright. The C$^{18}$O abundance decreases inside the ridge, and shows anti-correlation with the N$_2$H$^+$ abundance. However, both C$^{18}$O and N$_2$H$^+$ show strong depletion at the Class 0 protostar VLA1623, implying that the dense gas surrounding VLA1623 is colder than the freeze-out temperature of N$_2$. The blue- and red-shifted components of CH$_3$OH and H$_2$CO lines are seen at SM1, suggesting outflow activity of embedded source in SM1, although the spatial distributions do not show clear bipolarity.