Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 
lensed dusty star-forming galaxy SDP.81

Rybak, Matus; Hodge, J. A.; Vegetti, S.; van der Werf, P.; Andreani, P.; Graziani, L.; McKean, J. P.

doi:10.1093/mnras/staa879

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Journal Article

Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 lensed dusty star-forming galaxy SDP.81

MPS-Authors

/persons/resource/persons134701

Vegetti, S.
Cosmology, MPI for Astrophysics, Max Planck Society;

External Resource

No external resources are shared

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Rybak, M., Hodge, J. A., Vegetti, S., van der Werf, P., Andreani, P., Graziani, L., et al. (2020). Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 lensed dusty star-forming galaxy SDP.81. Monthly Notices of the Royal Astronomical Society, 494(4), 5542-5567. doi:10.1093/mnras/staa879.

Cite as: https://hdl.handle.net/21.11116/0000-0006-C0E0-3

Abstract

We present a sub-kpc resolved study of the interstellar medium properties in SDP.81, a z = 3.042 strongly gravitationally lensed, dusty star-forming galaxy, based on high-resolution, multiband ALMA observations of the far-infrared (FIR) continuum, CO ladder, and the [C ii] line. Using a visibility-plane lens modelling code, we achieve a median source-plane resolution of ∼200 pc. We use photon-dominated region (PDR) models to infer the physical conditions – far-ultraviolet (FUV) field strength, density, and PDR surface temperature – of the star-forming gas on 200-pc scales, finding a FUV field strength of ∼10³−10⁴G₀, gas density of ∼10⁵ cm⁻³, and cloud surface temperatures up to 1500 K, similar to those in the Orion Trapezium region. The [C ii] emission is significantly more extended than that FIR continuum: ∼50 per cent of [C ii] emission arises outside the FIR-bright region. The resolved [C ii]/FIR ratio varies by almost 2 dex across the source, down to ∼2 × 10⁻⁴ in the star-forming clumps. The observed [C ii]/FIR deficit trend is consistent with thermal saturation of the C⁺ fine-structure-level occupancy at high gas temperatures. We make the source-plane reconstructions of all emission lines and continuum data publicly available.