English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We aim to understand the contribution of the ionized, atomic and molecularphases of the ISM to the [CII] emission from clouds near the dynamical centerand the BCLMP302 HII region in the north of the nearby galaxy M33 at a spatialresolution of 50pc. We combine high resolution [CII] spectra taken with theHIFI spectrometer onboard the Herschel satellite with [CII] Herschel-PACS mapsand ground-based observations of CO(2-1) and HI. All data are at a commonspatial resolution of 50pc. Typically, the [CII] lines have widths intermediatebetween the narrower CO(2-1) and broader HI line profiles. We decomposed the[CII] spectra in terms of contribution from molecular and atomic gas detectedin CO(2-1) and HI, respectively. We find that the relative contribution ofmolecular and atomic gas traced by CO(2-1) and HI varies depends mostly on thelocal physical conditions and geometry. We estimate that 11-60% and 5-34% ofthe [CII] intensities in the center and in BCLMP302, respectively, arise atvelocities showing no CO(2-1) or HI emission and could arise in CO-darkmolecular gas. The deduced strong variation in the [CII] emission notassociated with CO and HI cannot be explained in terms of differences in A_v,far-ultraviolet radiation field, and metallicity between the two studiedregions. Hence the relative amounts of diffuse (CO-dark) and dense moleculargas possibly vary on spatial scales smaller than 50pc. Based on the emissionmeasure observed at radio wavelengths we estimate the contribution of ionizedgas at a few positions to lie between 10-25%. The correlations between theintensities of tracers corresponding to the same velocity range as [CII],differ from the correlation derived from PACS data. The results in this paperemphasize the need for velocity-resolved observations to discern thecontribution of different components of the ISM to [CII] emission. (abridged)

Velocity resolved [CII] spectroscopy of the center and the BCLMP302 region of M33 (HerM33es)