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The environment of supernova remnants (SNRs) is a key factor in theirevolution, particularly at later stages of their existence. It is often assumedthat mixed-morphology (MM) SNRs evolve in very dense environments, and thattheir centre-filled X-ray morphology is due to interactions between the SNRsand their surroundings. We aim to determine whether MMSNR VRO 42.05.01 isembedded in, and interacting with, a dense molecular environment. We used theIRAM telescope in Pico Veleta, Spain, to search for interaction between the SNRand neighbouring molecular clouds. We observed a region of $26'\times14'$towards the west of VRO 42.05.01 and a region of $8'\times4'$ towards the northof the remnant in the $^{12}$CO $J=1-0$, $^{13}$CO $J=1-0$, and $^{12}$CO$J=2-1$ transitions with the EMIR receiver. We made maps of the properties ofthe observed molecular clouds (peak temperatures, central velocities, velocitydispersions), column density along the line of sight, and ratio of the$^{12}$CO $J=2-1$ to $^{12}$CO $J=1-0$ transitions. We analyse archivaloptical, infrared, and radio spectroscopic data for other hints on the natureof the medium. We do not find conclusive physical proof that the SNR isinteracting with the few, clumpy molecular clouds that surround it in theregion of our observations, although there is some suggestion of suchinteraction (in a region outside our map) from infrared emission. There is avelocity gradient in one of the molecular clouds that is consistent with astellar wind blown by a $12-14$ $M_{\odot}$ progenitor star. We reassess theliterature distance to VRO 42.05.01, and propose that it has a local standardof rest velocity of $-6$ km s$^{-1}$, and that it is located $1.0\pm0.4$ kpcaway (the earlier distance value was $4.5\pm1.5$ kpc). We find that a dustsheet intersects VRO 42.05.01 and is possibly related to its doubleshell-shaped morphology.

The environment of supernova remnant VRO 42.05.01 as probed with IRAM 30m molecular line observations