13CO(J=1-0) Depression in Luminous Starburst Mergers, Revisited

TL;DR

This study investigates the cause of high $R_{1-0}$ ratios in luminous starburst mergers, finding evidence that ^{13}CO may be underabundant, though excitation effects cannot be entirely ruled out.

Contribution

The paper extends previous work by analyzing higher transition lines, providing new evidence that ^{13}CO depletion may explain the elevated line ratios in starburst mergers.

Findings

^{13}CO(J=2-1) is also depressed relative to ^{12}CO(J=2-1) in starburst mergers.

Results suggest ^{13}CO underabundance may be responsible for high $R_{1-0}$ ratios.

Further observations at higher J transitions are needed for conclusive insights.

Abstract

It is known that merging galaxies with luminous starbursts and high far-infrared luminosities tend to have higher $R_{1-0} =^{12}CO(J=1-0)/^{13}CO(J=1-0)$ integrated line intensity ratios ($R_{1-0} \simeq 20-50$) than normal spiral galaxies ($R_{1-0} \simeq 5-15$). Comparing far-infrared luminosities [L(FIR)] with those of ^{12}CO(J=1-0) and ^{13}CO(J=1-0) for a sample of normal and starburst galaxies, Taniguchi & Ohyama found that the observed high $R_{1-0}$ values for the luminous starburst mergers are attributed to their lower ^{13}CO line intensities by a factor of 3 on the average. They suggested the following two possibilities; in the luminous starburst mergers, 1) ^{13}CO is underabundant with respect to ^{12}CO, or 2) exitation and/or optical depth effects are responsible for the change in $R_{1-0}$. In this paper, we investigate the second possibility using higher transition data of both ^{12}CO and ^{13}CO emission lines. Applying the same method proposed by Taniguchi & Ohyama to both ^{12}CO(J=2-1) and ^{13}CO(J=2-1), we find that ^{13}CO(J=2-1) is also depressed with respect to ^{12}CO(J=2-1). This suggests that the ^{13}CO gas may be underabundant in the high-$R_{1-0}$ starburst mergers although we cannot rule out the possibility that excitation and optical depth effects are still affecting $R_{2-1}$, for example due to the large velocity widths in the CO emission lines. Additional observations of both ^{12}CO and ^{13}CO lines at $J \geq 3$ are required to better constrain the conditions of the molecular gas in luminous starburst galaxies.