The c2d Spitzer spectroscopy survey of ices around low-mass young stellar objects, III: CH4

TL;DR

This study uses Spitzer/IRS infrared spectra to measure solid methane (CH4) abundances around low-mass young stellar objects, revealing consistent levels and formation pathways on grain surfaces, which differ from other proposed theories.

Contribution

First large-scale measurement of solid CH4 in low-mass star forming regions using Spitzer, confirming formation via hydrogenation on grain surfaces.

Findings

Solid CH4 detected in 25 out of 52 sources.

CH4 abundances are mostly 4.7% relative to H2O.

Solid CH4 correlates more with H2O and CO2 than with CO or CH3OH.

Abstract

CH4 is proposed to be the starting point of a rich organic chemistry. Solid CH4 abundances have previously been determined mostly toward high mass star forming regions. Spitzer/IRS now provides a unique opportunity to probe solid CH4 toward low mass star forming regions as well. Infrared spectra from the Spitzer Space Telescope are presented to determine the solid CH4 abundance toward a large sample of low mass young stellar objects. 25 out of 52 ice sources in the $c2d$ (cores to disks) legacy have an absorption feature at 7.7 um, attributed to the bending mode of solid CH4. The solid CH4 / H2O abundances are 2-8%, except for three sources with abundances as high as 11-13%. These latter sources have relatively large uncertainties due to small total ice column densities. Toward sources with H2O column densities above 2E18 cm-2, the CH4 abundances (20 out of 25) are nearly constant at 4.7+/-1.6%. Correlation plots with solid H2O, CH3OH, CO2 and CO column densities and abundances relative to H2O reveal a closer relationship of solid CH4 with CO2 and H2O than with solid CO and CH3OH. The inferred solid CH4 abundances are consistent with models where CH4 is formed through sequential hydrogenation of C on grain surfaces. Finally the equal or higher abundances toward low mass young stellar objects compared with high mass objects and the correlation studies support this formation pathway as well, but not the two competing theories: formation from CH3OH and formation in gas phase with subsequent freeze-out.