Standing in the shadow of dark gas: ALMA observations of absorption from dark CO in the molecular DNM of Chamaeleon

Abstract: % context We had detected J=1-0 HCO+ absorption in 12 directions lacking detected CO emission in the outskirts of the Chamaeleon complex and on 1 sightline with integrated CO emission 2.4 K-\kms. 8 sightlines had a much larger mean column density of dark neutral medium (DNM)-gas not represented in H I or CO emission-and were found to have much higher mean molecular column density. The 5 other sightlines had little or no DNM and were found to have much smaller but still detectable N(HCO+). % aims To determine N(CO) along previously-observed Chamaeleon sightlines and to determine why CO emission was not detected in directions where molecular gas is present. % methods We took \cotw\ J=1-0 absorption profiles on 5 sightlines having higher DNM and HCO+ column densities and 1 sightline with smaller N(DNM) and N(HCO+). We converted the integrated HCO+ optical depths to N(H2) in the weak-excitation limit using N(HCO+)/N(H2)$=3\times10^{-9}$ and converted the integrated CO optical depths \ICO\ to CO column density N(CO) $= 1.861\times 10^{15}\pcc \ICO^{1.131}$ as found along comparable lines of sight previously studied in J=1-0 and J=2-1 CO absorption&emission. %results CO absorption was detected along the 5 sightlines in the higher-DNM group, with CO column densities $4\times 10^{13} \pcc<$ N(CO) $<10^{15}\pcc$ that are generally below the detectability limit of CO emission surveys. %conclusions In the outskirts of the Chamaeleon complex, the presence of molecular DNM resulted primarily from small CO column densities at the onset of CO formation around the HI/\HH\ transition in diffuse molecular gas. CO relative abundances N(CO)/N(H2) $< 2\times 10^{-6}$ in the outskirts of Chamaeleon are comparable to those seen in UV absorption toward early-type stars, including in Chamaeleon.