Velocity measurement in the extensive [OIII] emission region 1.2 south-east of M 31

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dc.contributor.authorAmram, P.
dc.contributor.authorAdami, C.
dc.contributor.authorEpinat, B.
dc.contributor.authorChemin, L.
dc.date.accessioned2023-09-20T16:31:47Z
dc.date.available2023-09-20T16:31:47Z
dc.date.issued2023-03
dc.descriptionIndexación: Scopuses
dc.description.abstractContext. The discovery of a broad, ∼1.5 long filamentary [OIII] 5007 emission ∼1.2 south-east of the M 31 nucleus has recently been reported. More than 100 hours of exposures of a wide field (3.48 - 2.32) have allowed this pioneering detection based on 30 narrow-band filters and several small refractors equipped with large cameras. Aims. We report a first velocity measurement in this extensive [OIII] emission line region. Methods. We used the low-resolution spectrograph MISTRAL (R ∼ 750), a facility of the Haute-Provence Observatory 193 cm telescope. The velocity measurement is based on the Hα, [NII], [SII] and [OIII] lines. Results. The best solution to fit the spectrum indicates that the Hα and [OIII] emissions are at the same heliocentric line-of-sight velocity of 96±4 km s1. This was measured within an area of ∼250 arcsec2 selected on a bright knot along the long filament of ∼1.5, together with a [OIII]5007 surface brightness of 4.2±2.1Ã- 1017 erg s1 cm2 arcsec2. This agrees moderately well with the previous measurement. We also estimated the Hα/[NII] line ratio as ∼1.1. Conclusions. The radial velocities at which the Hα and [OIII] lines were detected seem to show that these hydrogen and oxygen atoms belong to the same layer, but we cannot exclude that another weaker [OIII] line, belonging to another structure, that is, at another velocity, is below our detection threshold. Different scenarios have been considered to explain this filamentary structure. The extra-galactic origin was excluded in favour of Galactic origins. We tentatively assume that this filament is a piece of a supernova remnant located at a distance of ∼0.7 kpc from the Sun, of which we only see a small fraction of the shells with a radius of ∼35 pc. The progenitor may be along the line of sight of the galaxy M 31, but this observation might also just be part of a large-scale filamentary structure that should be investigated further. © 2023 The Authors.es
dc.description.urihttps://www.aanda.org/articles/aa/full_html/2023/03/aa46311-23/aa46311-23.html
dc.identifier.citationAstronomy and Astrophysics Volume 6711 March 2023 Article number L13es
dc.identifier.doi10.1051/0004-6361/202346311
dc.identifier.issn0004-6361
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/53270
dc.language.isoenes
dc.publisherEDP Scienceses
dc.rights.licenseAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectGalaxies: ISMes
dc.subjectGalaxy: generales
dc.subjectIntergalactic mediumes
dc.subjectISM: atomses
dc.subjectISM: supernova remnantses
dc.titleVelocity measurement in the extensive [OIII] emission region 1.2 south-east of M 31es
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