High-resolution HI and CO observations of high-latitude intermediate-velocity clouds^⋆

¹ Argelander-Institut für Astronomie (AIfA), Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
e-mail: troehser@astro.uni-bonn.de
² Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany

Received: 22 June 2015
Accepted: 6 June 2016

Abstract

Context. Intermediate-velocity clouds (IVCs) are HI halo clouds that are likely related to a Galactic fountain process. In-falling IVCs are candidates for the re-accretion of matter onto the Milky Way.

Aims. We study the evolution of IVCs at the disk-halo interface, focussing on the transition from atomic to molecular IVCs. We compare an atomic IVC to a molecular IVC and characterise their structural differences in order to investigate how molecular IVCs form high above the Galactic plane.

Methods. With high-resolution HI observations of the Westerbork Synthesis Radio Telescope and ¹²CO(1 → 0) and ¹³CO(1 → 0) observations with the IRAM 30 m telescope, we analyse the small-scale structures within the two clouds. By correlating HI and far-infrared (FIR) dust continuum emission from the Planck satellite, the distribution of molecular hydrogen (H₂) is estimated. We conduct a detailed comparison of the HI, FIR, and CO data and study variations of the X_CO conversion factor.

Results. The atomic IVC does not disclose detectable CO emission. The atomic small-scale structure, as revealed by the high-resolution HI data, shows low peak HI column densities and low HI fluxes as compared to the molecular IVC. The molecular IVC exhibits a rich molecular structure and most of the CO emission is observed at the eastern edge of the cloud. There is observational evidence that the molecular IVC is in a transient and, thus, non-equilibrium phase. The average X_CO factor is close to the canonical value of the Milky Way disk.

Conclusions. We propose that the two IVCs represent different states in a gradual transition from atomic to molecular clouds. The molecular IVC appears to be more condensed allowing the formation of H₂ and CO in shielded regions all over the cloud. Ram pressure may accumulate gas and thus facilitate the formation of H₂. We show evidence that the atomic IVC will evolve also into a molecular IVC in a few Myr.