Issue |
A&A
Volume 651, July 2021
|
|
---|---|---|
Article Number | A77 | |
Number of page(s) | 15 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/202140398 | |
Published online | 16 July 2021 |
Gaseous nebulae and massive stars in the giant H I ring in Leo
1
INAF-Osservatorio di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
e-mail: edvige.corbelli@inaf.it
2
Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD, USA
3
Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
Received:
22
January
2021
Accepted:
12
April
2021
Context. Chemical abundances in the Leo ring, the largest H I 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 Hα 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 H I 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 H II regions. The average star-formation rate density in the ring is on order of 10−5 M⊙ yr−1 kpc−2 and proceeds with local bursts a few hundred parsecs in size, where loose stellar associations of 500−1000 M⊙ occasionally host massive outliers. The far ultraviolet-to-Hα emission ratio in nebular regions implies recent stellar bursts, from 2 to 7 Myr ago. The relation between the local H I 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 Hα region with [OIII]/Hα 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 Hα lines around the brightest and youngest H II region suggests that local shocks might triggers future star-forming sites.
Key words: stars: formation / HII regions / planetary nebulae: general / galaxies: interactions / intergalactic medium / stars: massive
© ESO 2021
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