The resolved star-formation efficiency of early-type galaxies
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F25%3A00646703" target="_blank" >RIV/67985815:90106/25:00646703 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/staf498" target="_blank" >https://doi.org/10.1093/mnras/staf498</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/staf498" target="_blank" >10.1093/mnras/staf498</a>
Alternative languages
Result language
angličtina
Original language name
The resolved star-formation efficiency of early-type galaxies
Original language description
Understanding how and why star formation varies between galaxies is fundamental to our comprehension of galaxy evolution. In particular, the star-formation efficiency (SFE, star-formation rate or SFR per unit cold gas mass) has been shown to vary substantially both across and within galaxies. Early-type galaxies (ETGs) constitute an extreme case, as about a quarter have detectable molecular gas reservoirs but little to no detectable star formation. In this work, we present a spatially resolved view of the SFE in 10 ETGs, combining state-of-the-art Atacama Large Millimeter/submillimeter Array (ALMA) and Multi Unit Spectroscopic Explorer (MUSE) observations. Optical spectroscopic line diagnostics are used to identify the ionized emission regions dominated by star formation, and reject regions where the ionization arises primarily from other sources. We identify very few regions where the ionization is consistent with pure star formation. Using H alpha as our SFR tracer, we find that previous integrated measurements of the star-formation rate based on UV and 22 mu m emission are systematically higher than the SFR measured from H alpha. However, for the small number of regions where ionization is primarily associated with star formation, the SFEs are around 0.4 dex higher than those measured in star-forming galaxies at a similar spatial resolution (with depletion times ranging from 108 to 10(10) yr). Whilst the SFE of ETGs is overall low, we find that the SFEs of individual regions within ETGs can be similar to, or higher than, similar sized regions within star-forming galaxies.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
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Others
Publication year
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
538
Issue of the periodical within the volume
4
Country of publishing house
US - UNITED STATES
Number of pages
28
Pages from-to
3219-3246
UT code for WoS article
001458781700001
EID of the result in the Scopus database
2-s2.0-105002024779