Nitrogen enrichment through stellar chemical feedback at parsec scale in NGC 5253 as seen with MUSE–NFM

Pruijt, BGA ORCID: 0009-0007-5947-2343, Monreal-Ibero, A ORCID: 0000-0002-6455-2491, Weilbacher, PM, Walsh, JR ORCID: 0000-0002-8008-910X, Kamann, S ORCID: 0000-0001-6604-0505, Soemitro, AA ORCID: 0000-0001-6213-4117, Kusakabe, H ORCID: 0000-0002-3801-434X and Boogaard, L ORCID: 0000-0002-3952-8588 (2026) Nitrogen enrichment through stellar chemical feedback at parsec scale in NGC 5253 as seen with MUSE–NFM. Monthly Notices of the Royal Astronomical Society, 549 (1). pp. 1-21. ISSN 0035-8711

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Abstract

NGC 5253 is a nearby (D = 3.6 Mpc) Blue Compact Dwarf galaxy, notable for its three massive young super star clusters (SSCs) and nitrogen enrichment. Its similarity to extreme star-forming galaxies at high redshift makes it a good local analogue for studying chemical enrichment at high spatial resolution. We characterize the ionized gas and dust in the giant H ii region in the proximity of the three SSCs in the centre of NGC 5253 using new Multi-Unit Spectroscopic Explorer Narrow Field Mode adaptive optics-assisted data at unprecedented spatial resolution of 0(Formula presented) 15 ((Formula presented) 2.3 pc). We derive the attenuation for the central SSCs and, for the first time, map the extinction parameter ((Formula presented)) in an extragalactic object. (Formula presented) varies among SSCs, suggesting differences in dust physics. Electron temperature and density diagnostics yield flat temperature distributions (Formula presented) ([N ii])(Formula presented)  K and (Formula presented) ([S iii])(Formula presented)  K, and a structured (Formula presented) ([S ii]) of maximum (Formula presented)  cm(Formula presented). The direct method gives a flat helium abundance ((Formula presented)) and uniform oxygen abundance ((Formula presented)). N/O shows a factor 2–3 enhancement around the SSCs, mapped here for the first time at such high spatial resolution. The total excess nitrogen mass is (Formula presented) 0.3 (Formula presented), which we estimate is producible by the observed WN-type Wolf–Rayet (WR) stars. Since there is no direct spatial overlap between the enrichment and WR star positions, the N-rich material appears to have been expelled from the original sites.

Item Type:	Article
Uncontrolled Keywords:	ISM: abundances; dust, extinction; galaxies: dwarf; galaxies: individual: NGC 5253; galaxies: ISM; galaxies: starburst; 5101 Astronomical Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects:	Q Science > QB Astronomy
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press (OUP)
Date of acceptance:	21 April 2026
Date of first compliant Open Access:	5 June 2026
Date Deposited:	05 Jun 2026 14:57
Last Modified:	05 Jun 2026 14:57
DOI or ID number:	10.1093/mnras/stag794
URI:	https://researchonline.ljmu.ac.uk/id/eprint/28755

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