Gaseous nebulae and massive stars in the giant HI ring in Leo

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dc.contributor.authorCorbelli, Edvige
dc.contributor.authorMannucci, Filippo
dc.contributor.authorThilker, David
dc.contributor.authorCresci, Giovanni
dc.contributor.authorVenturi, Giacomo
dc.date.accessioned2025-01-20T22:13:18Z
dc.date.available2025-01-20T22:13:18Z
dc.date.issued2021
dc.description.abstractContext. Chemical abundances in the Leo ring, the largest HI cloud in the local Universe, have recently been determined to be close to or above Solar values. This is a finding that is incompatible with prior claims that the ring was primordial in origin. The gas, pre-enriched in a galactic disk and tidally stripped, did not manage to efficiently form stars in the intergalactic space.Aims. Using H alpha emission and a multi-wavelengths analysis of its extremely faint optical counterpart, we investigate the process of star formation and the slow build-up of a stellar population that could form diffuse and metal-rich dwarf galaxies in the Leo ring.Methods. We mapped nebular lines in three dense HI clumps and complemented the data with archival stellar continuum observations from the Galaxy Evolution Explorer and the Hubble Space Telescope, as well as with population synthesis models.Results. We detect a sparse population of stars in the main body of the ring, with individual young stars as massive as O7-types powering some HII regions. The average star-formation rate density in the ring is on order of 10(-5)M(circle dot) yr(-1) kpc(-2) and proceeds with local bursts a few hundred parsecs in size, where loose stellar associations of 500-1000 M-circle dot occasionally host massive outliers. The far ultraviolet-to-H alpha emission ratio in nebular regions implies recent stellar bursts, from 2 to 7 Myr ago. The relation between the local HI gas density and the star-formation rate in the ring is similar to what is found in dwarfs and outer disks with gas depletion times as long as 100 Gyr. We find a candidate planetary nebula in a compact and faint H alpha region with [OIII]/H alpha line enhancement, which is consistent with the estimated mean stellar surface brightness of the ring. The presence of a 1 kpc partial ring that is emitting weak H alpha lines around the brightest and youngest HII region suggests that local shocks might triggers future star-forming sites.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202140398
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202140398
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94445
dc.identifier.wosidWOS:000675664600005
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectstars: formation
dc.subjectHII regions
dc.subjectplanetary nebulae: general
dc.subjectgalaxies: interactions
dc.subjectintergalactic medium
dc.subjectstars: massive
dc.titleGaseous nebulae and massive stars in the giant HI ring in Leo
dc.typeartículo
dc.volumen651
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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