Large-Scale Structure of the Molecular Gas in Taurus Revealed by High Linear Dynamic Range Spectral Line Mapping

TL;DR

This study provides a detailed, high-resolution map of the Taurus Molecular Cloud, revealing complex structures, magnetic field alignments, and refined mass estimates, offering new insights into the cloud's morphology and star formation activity.

Contribution

It presents the first large-scale, high dynamic range spectral line maps of Taurus, uncovering detailed structures and improving mass and star formation estimates with a novel column density-dependent model.

Findings

Revealed complex filamentary and cavity structures in Taurus.

Derived a total cloud mass of 24,000 solar masses, three times higher than previous estimates.

Estimated a low star formation efficiency of 0.3-1.2%.

Abstract

We report the results of a 100 square degree survey of the Taurus Molecular Cloud region in the J = 1-0 transition of 12CO and 13CO. The image of the cloud in each velocity channel includes ~ 3 million Nyquist sampled pixels on a 20" grid. The high sensitivity and large linear dynamic range of the maps in both isotopologues reveal a very complex, highly structured cloud morphology. There are large scale correlated structures evident in 13CO emission having very fine dimensions, including filaments, cavities, and rings. The 12CO emission shows a quite different structure, with particularly complex interfaces between regions of greater and smaller column density defining the boundaries of the largest-scale cloud structures. The axes of the striations seen in the 12CO emission from relatively diffuse gas are aligned with the direction of the magnetic field. Using a column density-dependent model for the CO fractional abundance, we derive the mass of the region mapped to be 24,000 solar masses, a factor of three greater than would be obtained with canonical CO abundance restricted to the high column density regions. We determine that half the mass of the cloud is in regions having column density below 2.1x10^{21} per square cm. The distribution of young stars in the region covered is highly nonuniform, with the probability of finding a star in a pixel with a specified column density rising sharply for N(H2) = 6x10^{21} cm^{-2}. We determine a relatively low star formation efficiency (mass of young stars/mass of molecular gas), between 0.3 and 1.2 %, and an average star formation rate during the past 3 Myr of 8x10^{-5} stars yr^{-1}.