Matches in SemOpenAlex for { <https://semopenalex.org/work/W2896983056> ?p ?o ?g. }
- W2896983056 endingPage "2554" @default.
- W2896983056 startingPage "2530" @default.
- W2896983056 abstract "Archival WFC3/UVIS imaging of Arp 299 (NGC 3690E+ NGC 3690W) is retrieved to investigate the young massive cluster (YMC) population of this ongoing merger. We extract 2182 cluster candidates, including 1323 high confidence photometric sources. Multiband photometry is matched with Yggdrasil models to estimate the age, mass, and extinction of each cluster. A Schechter fit of the truncated cluster mass function results in a characteristic mass |${M_{star } = 1.6 times 10^6, M_{odot }}$|. Our results confirm that intensely star-forming galaxies such as Arp 299 host more massive clusters than quiescent dwarf and normal spirals. In the case of NGC 3690E, we find that the cluster masses decrease with an increasing galactocentric radius likely due to the gas density distribution. On the other hand, the fitted age distributions of a mass-limited sample suggest that YMCs of the western component undergo stronger disruption than those hosted by the eastern galaxy. This is in agreement with the properties of the underlying cluster luminosity functions: a clear truncation at high luminosities with slopes generally shallower by |${sim }, 0.3$| dex than the ones of the NGC 3690E. Finally, the derived cluster formation efficiency, Γ ∼ 19 per cent, indicates that Arp 299 has ∼3–5 times more star formation happening in bound clusters compared to the cases of gas-poor spirals like NGC 2997 and NGC 4395. The merger generally follows the Γ − star formation rate density relation from the literature. The YMC photometric study of Arp 299 thus reveals that both formation and disruption mechanisms of the star cluster population are most likely environment dependent." @default.
- W2896983056 created "2018-10-26" @default.
- W2896983056 creator A5024639898 @default.
- W2896983056 creator A5028585861 @default.
- W2896983056 creator A5030741782 @default.
- W2896983056 creator A5052635891 @default.
- W2896983056 date "2018-10-22" @default.
- W2896983056 modified "2023-10-14" @default.
- W2896983056 title "Young massive clusters in the interacting LIRG Arp 299: evidence for the dependence of star cluster formation and evolution on environment" @default.
- W2896983056 cites W1513927617 @default.
- W2896983056 cites W1669413277 @default.
- W2896983056 cites W1853912930 @default.
- W2896983056 cites W1860678232 @default.
- W2896983056 cites W1889917103 @default.
- W2896983056 cites W1920021936 @default.
- W2896983056 cites W1956570792 @default.
- W2896983056 cites W1968035073 @default.
- W2896983056 cites W1978280011 @default.
- W2896983056 cites W1978700834 @default.
- W2896983056 cites W1979326205 @default.
- W2896983056 cites W1984757459 @default.
- W2896983056 cites W1994671833 @default.
- W2896983056 cites W1998045888 @default.
- W2896983056 cites W2003324213 @default.
- W2896983056 cites W2009747152 @default.
- W2896983056 cites W2024304937 @default.
- W2896983056 cites W2027645915 @default.
- W2896983056 cites W2030703638 @default.
- W2896983056 cites W2046620005 @default.
- W2896983056 cites W2055966314 @default.
- W2896983056 cites W2066034174 @default.
- W2896983056 cites W2066505012 @default.
- W2896983056 cites W2074609460 @default.
- W2896983056 cites W2074747635 @default.
- W2896983056 cites W2094578261 @default.
- W2896983056 cites W2097831112 @default.
- W2896983056 cites W2099338922 @default.
- W2896983056 cites W2100828932 @default.
- W2896983056 cites W2100908305 @default.
- W2896983056 cites W2102221834 @default.
- W2896983056 cites W2112254754 @default.
- W2896983056 cites W2138111676 @default.
- W2896983056 cites W2142238829 @default.
- W2896983056 cites W2146944257 @default.
- W2896983056 cites W2151062050 @default.
- W2896983056 cites W2152221540 @default.
- W2896983056 cites W2154174189 @default.
- W2896983056 cites W2154986370 @default.
- W2896983056 cites W2155991952 @default.
- W2896983056 cites W2172061719 @default.
- W2896983056 cites W2177399614 @default.
- W2896983056 cites W2252488643 @default.
- W2896983056 cites W2347268829 @default.
- W2896983056 cites W2396454142 @default.
- W2896983056 cites W2400690548 @default.
- W2896983056 cites W2483396289 @default.
- W2896983056 cites W2516406733 @default.
- W2896983056 cites W2600822636 @default.
- W2896983056 cites W2611690120 @default.
- W2896983056 cites W2617775199 @default.
- W2896983056 cites W2756393264 @default.
- W2896983056 cites W2758943010 @default.
- W2896983056 cites W3040946362 @default.
- W2896983056 cites W3098247218 @default.
- W2896983056 cites W3098558211 @default.
- W2896983056 cites W3098650804 @default.
- W2896983056 cites W3099915657 @default.
- W2896983056 cites W3099970198 @default.
- W2896983056 cites W3100265020 @default.
- W2896983056 cites W3100299581 @default.
- W2896983056 cites W3100341808 @default.
- W2896983056 cites W3100640042 @default.
- W2896983056 cites W3100728189 @default.
- W2896983056 cites W3101398752 @default.
- W2896983056 cites W3101763298 @default.
- W2896983056 cites W3101803932 @default.
- W2896983056 cites W3103196060 @default.
- W2896983056 cites W3103299938 @default.
- W2896983056 cites W3103574620 @default.
- W2896983056 cites W3104415880 @default.
- W2896983056 cites W3104416848 @default.
- W2896983056 cites W3104418093 @default.
- W2896983056 cites W3104485092 @default.
- W2896983056 cites W3104532808 @default.
- W2896983056 cites W3104985187 @default.
- W2896983056 cites W3105094438 @default.
- W2896983056 cites W3105140485 @default.
- W2896983056 cites W3105710181 @default.
- W2896983056 cites W3106183421 @default.
- W2896983056 cites W3122846358 @default.
- W2896983056 cites W3123371988 @default.
- W2896983056 cites W3125228767 @default.
- W2896983056 cites W3125356176 @default.
- W2896983056 cites W4293183662 @default.
- W2896983056 cites W4299539453 @default.
- W2896983056 doi "https://doi.org/10.1093/mnras/sty2837" @default.
- W2896983056 hasPublicationYear "2018" @default.
- W2896983056 type Work @default.