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dc.contributor.authorMingozzi, M
dc.contributor.authorBelfiore, F
dc.contributor.authorCresci, G
dc.contributor.authorBundy, K
dc.contributor.authorBershady, M
dc.contributor.authorBizyaev, D
dc.contributor.authorBlanc, G
dc.contributor.authorBoquien, M
dc.contributor.authorDrory, N
dc.contributor.authorFu, H
dc.contributor.authorMaiolino, Roberto
dc.contributor.authorRiffel, R
dc.contributor.authorSchaefer, A
dc.contributor.authorStorchi-Bergmann, T
dc.contributor.authorTelles, E
dc.contributor.authorTremonti, C
dc.contributor.authorZakamska, N
dc.contributor.authorZhang, K
dc.date.accessioned2020-04-01T14:36:03Z
dc.date.available2020-04-01T14:36:03Z
dc.date.issued2020-04-13
dc.identifier.issn0004-6361
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/303995
dc.description.abstractWe measured gas-phase metallicity, ionisation parameter and dust extinction for 1795 representative local star-forming galaxies using integral field spectroscopy from the SDSS-IV MaNGA survey. We self-consistently derive these quantities by comparing observed line fluxes with photoionisation models using a Bayesian framework. We also present the first comprehensive study of the [SIII]$\lambda\lambda$9069,9532 nebular lines, which have long been predicted to be ideal tracers of the ionisation parameter. Unfortunately, we find that current photoionisation models substantially over-predict [SIII] lines intensity, while broadly reproducing other observed optical line ratios. We discuss how to nonetheless make use of the information provided by [SIII] lines by setting a prior on the ionisation parameter. Following this approach, we derive spatially-resolved maps and radial profiles of metallicity and ionisation parameter. The metallicity radial profiles are comparable with previous works, with metallicity declining toward the outer parts and a flattening in the central regions, in agreement with infall models of galaxy formation, that predict that spiral discs build up through accretion of material, which leads to an inside-out growth. On the other hand, ionisation parameter radial profiles are flat for low-mass galaxies, while their slope becomes positive as galaxy mass increases. However, the ionisation parameter maps we obtain are clumpy, especially for low-mass galaxies. Ionisation parameter is tightly correlated with the H$\alpha$ equivalent width [EW(H$\alpha$)], following a nearly universal relation, which we attribute to the change of the spectral shape of ionising sources due to ageing of HII regions. We derive a positive correlation between ionisation parameter and metallicity at fixed EW(H$\alpha$), in disagreement with previous theoretical works expecting an anti-correlation.
dc.description.sponsorshipSTFC and ERC
dc.publisherEDP Sciences
dc.rightsAll rights reserved
dc.titleSDSS IV MaNGA: Metallicity and ionisation parameter in local star-forming galaxies from Bayesian fitting to photoionisation models
dc.typeArticle
prism.publicationDate2020
prism.publicationNameAstronomy and Astrophysics
prism.volume636
dc.identifier.doi10.17863/CAM.51076
dcterms.dateAccepted2020-02-13
rioxxterms.versionofrecord10.1051/0004-6361/201937203
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2020-04-01
dc.contributor.orcidMaiolino, Roberto [0000-0002-4985-3819]
dc.identifier.eissn1432-0746
rioxxterms.typeJournal Article/Review
pubs.funder-project-idEuropean Research Council (695671)
pubs.funder-project-idScience and Technology Facilities Council (ST/M001172/1)
cam.orpheus.successMon Jul 20 07:59:07 BST 2020 - The item has an open VoR version.
cam.orpheus.counter4
rioxxterms.freetoread.startdate2100-01-01


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