The Star Formation Histories, Star Formation Efficiencies and Ionizing Sources of ATLASGAL Clumps with H ii Regions
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10493634" target="_blank" >RIV/00216208:11320/24:10493634 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=qSAgt0-QNe" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=qSAgt0-QNe</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1088/1538-3873/ad77f4" target="_blank" >10.1088/1538-3873/ad77f4</a>
Alternative languages
Result language
angličtina
Original language name
The Star Formation Histories, Star Formation Efficiencies and Ionizing Sources of ATLASGAL Clumps with H ii Regions
Original language description
1226 ATLASGAL clumps with H ii regions (H II-clumps) were matched with radio sources in the CORNISH-North/South surveys, and 392 of them have corresponding radio sources. We determined the stellar luminosity L-*,L-T84 according to the Lyman continuum flux N Ly. When the bolometric luminosity of H ii-clumps is less than log(10)(L-bol,L-obs/L-circle dot) approximate to 3.7, corresponding to a clump mass log(10)(M-cl/M-circle dot) approximate to 2.55, the values of L-*,L-T84 derived from N Ly overestimate the actual stellar luminosities, because the accretion onto the protostars contributes significantly to the radio emission. After subtracting the accretion luminosity from L-*,L-T84, we obtained reasonable estimates of the stellar luminosity. Using the 0.5 Myr isochrone, we calculated the stellar masses according to the stellar luminosities, and found that they roughly follow the m(max)-M-ecl relation of embedded clusters, consistent with the ionizing sources representing the most massive stars in the embedded clusters of H ii-clumps. We also studied the contribution of the possible flaring activity to the observed stellar luminosity and found that they can be neglected. We further studied the change of SFE with the clump mass. According to the derived mass of the most massive star in each HII-clump, using the theoretical m(max)-M-ecl relation, we calculated the mass of the corresponding embedded cluster and then the SFE of the clump. The SFE decreases with increasing clump mass, with a median value of approximate to 0.3. We also independently derived the SFE for each H ii-clump based on the model developed in our previous work. The SFEs of H ii-clumps derived from the observation and the model are in good agreement. Concerning the star formation histories of the ATLASGAL clumps, low-mass clumps may reach the peak of star formation earlier than high-mass clumps, consistent with the shorter free-fall time of low-mass clumps.
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
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Publications of the Astronomical Society of the Pacific
ISSN
0004-6280
e-ISSN
1538-3873
Volume of the periodical
136
Issue of the periodical within the volume
9
Country of publishing house
US - UNITED STATES
Number of pages
11
Pages from-to
094302
UT code for WoS article
001324464800001
EID of the result in the Scopus database
2-s2.0-85205691220