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dc.contributorEuropean Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Keplerlaan 1, NL-2201 AZ Noordwijk, the Netherlands; SRON Netherlands Institute for Space Research, Niels Bohrweg 4, NL-2333 CA Leiden, the Netherlands
dc.contributorDepartment of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotlářská 2, Brno CZ-611 37, Czech Republic
dc.contributorDepartment of Physics and Astronomy, University of Kentucky, 505 Rose Street, Lexington, KY 40506, USA
dc.contributorINAF - IASF Palermo, Via U. La Malfa 153, I-90146 Palermo, Italy
dc.contributorDepartment of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotlářská 2, Brno CZ-611 37, Czech Republic; Dipartimento di Fisica, Universita degli Studi di Torino, via Pietro Giuria 1, I-10125 Torino, Italy
dc.contributorSRON Netherlands Institute for Space Research, Niels Bohrweg 4, NL-2333 CA Leiden, the Netherlands; Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands; Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa 277-8583, Japan
dc.contributorINAF - Astronomical Observatory of Capodimonte, via Moiariello 16, I-80131 Napoli, Italy
dc.contributorArmagh Observatory and Planetarium, College Hill, Armagh BT61 DG, UK
dc.contributorInstitute of Physics, Eötvös University, Pázmány Péter sétány 1/A, Budapest 1117, Hungary
dc.contributor.authorMernier, F.
dc.contributor.authorWerner, N.
dc.contributor.authorSu, Y.
dc.contributor.authorPinto, C.
dc.contributor.authorGrossová, R.
dc.contributor.authorSimionescu, A.
dc.contributor.authorIodice, E.
dc.contributor.authorSarzi, M.
dc.contributor.authorGörgei, A.
dc.date.accessioned2024-02-01T17:11:31Z
dc.date.available2024-02-01T17:11:31Z
dc.date.issued2022-04-01T00:00:00Z
dc.identifier.doi10.1093/mnras/stac253
dc.identifier.doi10.48550/arXiv.2201.05161
dc.identifier.other2022arXiv220105161M
dc.identifier.other2022MNRAS.tmp..230M
dc.identifier.otherastro-ph.GA
dc.identifier.otherastro-ph.HE
dc.identifier.other10.1093/mnras/stac253
dc.identifier.other10.48550/arXiv.2201.05161
dc.identifier.otherarXiv:2201.05161
dc.identifier.other2022arXiv220105161M
dc.identifier.other2022MNRAS.tmp..230M
dc.identifier.other2022MNRAS.511.3159M
dc.identifier.other0000-0002-7031-4772
dc.identifier.other0000-0003-0392-0120
dc.identifier.other0000-0002-3886-1258
dc.identifier.other0000-0003-2532-7379
dc.identifier.other0000-0003-3471-7459
dc.identifier.other0000-0002-9714-3862
dc.identifier.other0000-0003-4291-0005
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1439
dc.description.abstractHot atmospheres pervading galaxy clusters, groups, and early-type galaxies are rich in metals, produced during epochs and diffused via processes that are still to be determined. While this enrichment has been routinely investigated in clusters, metals in lower mass systems are more challenging to probe with standard X-ray exposures and spectroscopy. In this paper, we focus on very deep XMM-Newton (~350 ks) observations of NGC 1404, a massive elliptical galaxy experiencing ram-pressure stripping of its hot atmosphere while infalling towards the centre of the Fornax cluster, with the aim to derive abundances through its hot gas extent. Importantly, we report the existence of a new fitting bias - the 'double Fe bias' - leading to an underestimate of the Fe abundance when two thermal components cannot realistically model the complex temperature structure present in the outer atmosphere of the galaxy. Contrasting with the 'metal conundrum' seen in clusters, the Fe and Mg masses of NGC 1404 are measured 1-2 orders of magnitude below what stars and supernovae could have reasonably produced and released. In addition, we note the remarkable Solar abundance ratios of the galaxy's halo, different from its stellar counterpart but similar to the chemical composition of the ICM of rich clusters. Completing the clusters regime, all these findings provide additional support towards a scenario of early enrichment, at play over two orders of magnitude in mass. A few peculiar and intriguing features, such as a possible double metal peak as well as an apparent ring of enhanced Si near the galaxy core, are also discussed.
dc.publisherMonthly Notices of the Royal Astronomical Society
dc.titleThe cycle of metals in the infalling elliptical galaxy NGC 1404
dc.typearticle
dc.source.journalMNRAS
dc.source.journalMNRAS.511
dc.source.volume511
refterms.dateFOA2024-02-01T17:11:31Z
dc.identifier.bibcode2022MNRAS.511.3159M


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