HIFI spectroscopy of low-level water transitions in M82

TL;DR

This study reports the first extragalactic detections of specific water transitions in M82, revealing that water exists in a widespread, diffuse gas component rather than dense cores, with high spectral resolution crucial for understanding line formation.

Contribution

First detection of para-H2O and H2O+ lines in an extragalactic source, showing water's distribution in diffuse gas in M82 using Herschel HIFI data.

Findings

Water absorption region is about 50 pc from galaxy center.

Water lines originate from widespread diffuse gas, not dense cores.

High spectral resolution is essential for interpreting line profiles.

Abstract

We present observations of the rotational ortho-water ground transition, the two lowest para-water transitions, and the ground transition of ionised ortho-water in the archetypal starburst galaxy M82, performed with the HIFI instrument on the Herschel Space Observatory. These observations are the first detections of the para-H2O(111-000) (1113\,GHz) and ortho-H2O+(111-000) (1115\,GHz) lines in an extragalactic source. All three water lines show different spectral line profiles, underlining the need for high spectral resolution in interpreting line formation processes. Using the line shape of the para-H2O(111-000) and ortho-H2O+(111-000) absorption profile in conjunction with high spatial resolution CO observations, we show that the (ionised) water absorption arises from a ~2000 pc^2 region within the HIFI beam located about ~50 pc east of the dynamical centre of the galaxy. This region does not coincide with any of the known line emission peaks that have been identified in other molecular tracers, with the exception of HCO. Our data suggest that water and ionised water within this region have high (up to 75%) area-covering factors of the underlying continuum. This indicates that water is not associated with small, dense cores within the ISM of M82 but arises from a more widespread diffuse gas component.