prikaz prve stranice dokumenta The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope
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Scientific paper - Original scientific paper
The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope
Astronomy & Astrophysics, 682 (2024); A162. https://doi.org/10.1051/0004-6361/202348055
Werle, A.; Giunchi, E.; Poggianti, B.; Gullieuszik, M.; Moretti, A.; Zanella, A.; Tonnesen, S.; Fritz, J.; Vulcani, B.; Bacchini, C.; Akerman, N.; Kulier, A.; Tomicic, N.; Smith, R.; Wolter, A. More authors...

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Werle, A., Giunchi, E., Poggianti, B., Gullieuszik, M., Moretti, A., Zanella, A. ... Wolter, A. (2024). The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope. Astronomy & Astrophysics, 682.. doi: 10.1051/0004-6361/202348055

Werle, A., et al. "The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope." Astronomy & Astrophysics, vol. 682, 2024. https://doi.org/10.1051/0004-6361/202348055

Werle, A., E. Giunchi, B. Poggianti, M. Gullieuszik, A. Moretti, A. Zanella, S. Tonnesen, et al. "The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope." Astronomy & Astrophysics 682 (2024). https://doi.org/10.1051/0004-6361/202348055

Werle, A., et al. (2024) 'The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope', Astronomy & Astrophysics, 682. doi: 10.1051/0004-6361/202348055

Werle A, Giunchi E, Poggianti B, Gullieuszik M, Moretti A, Zanella A, and sur.. The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope. Astronomy & Astrophysics [Internet]. 2024 February 19 [cited 2024 October 06];682. doi: 10.1051/0004-6361/202348055

A. Werle, et al., "The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope", Astronomy & Astrophysics, vol. 682, February 2024. [Online]. Available at: https://urn.nsk.hr/urn:nbn:hr:217:669379. [Accessed: 06 October 2024]

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Metadata
Title (english)The history of star-forming regions in the tails of six GASP jellyfish galaxies observed with the Hubble Space Telescope
AuthorA. Werle
AuthorE. Giunchi
AuthorB. Poggianti
AuthorM. Gullieuszik
AuthorA. Moretti
AuthorA. Zanella
AuthorS. Tonnesen
AuthorJ. Fritz
AuthorB. Vulcani
AuthorC. Bacchini
AuthorN. Akerman
AuthorA. Kulier
AuthorN. Tomicic
AuthorR. Smith
AuthorA. Wolter
Author's institutionUniversity of Zagreb
Faculty of Science
(Department of Physics)
Scientific / art field,
discipline and subdiscipline		NATURAL SCIENCES
Physics
Abstract (english)
Aims. In this work, we aim to characterize the stellar populations of star-forming regions detached from the stellar disks of galaxies undergoing ram-pressure stripping. Methods. Using images collected with the WFC3 camera on board of the Hubble Space Telescope, we detected stellar clumps in continuum-subtracted Hα and the ultraviolet (F275W filter); such clumps are often embedded in larger regions (star-forming complexes) detected in the optical (F606W filter). Our sample includes 347 Hα clumps, 851 F275W clumps, and 296 star-forming complexes. We modeled the photometry of these objects in five bands using bagpipes to obtain their stellar population parameters. Results. The median mass-weighted stellar ages are 27 Myr for Hα clumps and 39 Myr for F275W clumps and star-forming complexes, but the oldest stars in the complexes can be older than ∼300 Myr which indicates that star formation is sustained for long periods of time. Stellar masses vary from 103.5 to 107.1 M, with star-forming complexes being more massive objects in the sample. Clumps and complexes found further away from the host galaxy are on average younger, less massive, and less obscured by dust. We interpret these trends as due to the effect of ram pressure in different phases of the interstellar medium. Hα clumps form a well-defined sequence in the stellar mass–SFR plane with a slope of 0.73. Some F275W clumps and star-forming complexes follow the same sequence while others stray away from it and passively age. The difference in mean stellar age between a complex and its youngest embedded clump scales with the distance between the clump and the center of the optical emission of the complex, with the most displaced clumps being hosted by the most elongated complexes. This is consistent with a fireball-like morphology, where star formation proceeds in a small portion of the complex while older stars are left behind producing a linear stellar population gradient. The stellar masses of star-forming complexes are consistent with the ones of globular clusters, but their stellar mass surface densities are lower by 2 dex, and their properties are more consistent with the population of dwarf galaxies in clusters.
Keywords (english)
Languageenglish
Publication typeScientific paper - Original scientific paper
Publication statusPublished
Peer reviewPeer review - international
Publication versionPublished version
Journal titleAstronomy & Astrophysics
Numberingvol. 682, A162
p-ISSN0004-6361
e-ISSN1432-0746
DOIhttps://doi.org/10.1051/0004-6361/202348055
URN:NBNurn:nbn:hr:217:669379
Publication2024-02-19
Document URLhttps://www.aanda.org/10.1051/0004-6361/202348055
Type of resourceText
Access conditionsOpen access
Terms of useLicence Attribution 4.0 International (CC BY 4.0) icon
Public noteOpen Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication. Received 24 September 2023. Accepted 10 December 2023. Published online 19 February 2024.
Created on2024-07-23 20:05:14