TY - JOUR
T1 - The core mass function in the Orion Nebula Cluster region
T2 - What Determines the Final Stellar Masses?
AU - Takemura, Hideaki
AU - Nakamura, Fumitaka
AU - Kong, Shuo
AU - Arce, Héctor G.
AU - Carpenter, John M.
AU - Ossenkopf-Okada, Volker
AU - Klessen, Ralf
AU - Sanhueza, Patricio
AU - Shimajiri, Yoshito
AU - Tsukagoshi, Takashi
AU - Kawabe, Ryohei
AU - Ishii, Shun
AU - Dobashi, Kazuhito
AU - Shimoikura, Tomomi
AU - Goldsmith, Paul F.
AU - Sánchez-Monge, Álvaro
AU - Kauffmann, Jens
AU - Pillai, Thushara
AU - Padoan, Paolo
AU - Ginsberg, Adam
AU - Smith, Rowan J.
AU - Bally, John
AU - Mairs, Steve
AU - Pineda, Jaime E.
AU - Lis, Dariusz C.
AU - Burkhart, Blakesley
AU - Schilke, Peter
AU - Chen, Hope How-Huan
AU - Isella, Andrea
AU - Friesen, Rachel K.
AU - Goodman, Alyssa A.
AU - Harper, Doyal A.
N1 - Funding: European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130) (R.S.K.).
PY - 2021/3/22
Y1 - 2021/3/22
N2 - Applying dendrogram analysis to the CARMA-NRO C18O (J = 1–0) data having an angular resolution of ∼8'', we identified 692 dense cores in the Orion Nebula Cluster region. Using this core sample, we compare the core and initial stellar mass functions in the same area to quantify the step from cores to stars. About 22% of the identified cores are gravitationally bound. The derived core mass function (CMF) for starless cores has a slope similar to Salpeter's stellar initial mass function (IMF) for the mass range above 1 M⊙, consistent with previous studies. Our CMF has a peak at a subsolar mass of ∼0.1 M⊙, which is comparable to the peak mass of the IMF derived in the same area. We also find that the current star formation rate is consistent with the picture in which stars are born only from self-gravitating starless cores. However, the cores must gain additional gas from the surroundings to reproduce the current IMF (e.g., its slope and peak mass), because the core mass cannot be accreted onto the star with 100% efficiency. Thus, the mass accretion from the surroundings may play a crucial role in determining the final stellar masses of stars.
AB - Applying dendrogram analysis to the CARMA-NRO C18O (J = 1–0) data having an angular resolution of ∼8'', we identified 692 dense cores in the Orion Nebula Cluster region. Using this core sample, we compare the core and initial stellar mass functions in the same area to quantify the step from cores to stars. About 22% of the identified cores are gravitationally bound. The derived core mass function (CMF) for starless cores has a slope similar to Salpeter's stellar initial mass function (IMF) for the mass range above 1 M⊙, consistent with previous studies. Our CMF has a peak at a subsolar mass of ∼0.1 M⊙, which is comparable to the peak mass of the IMF derived in the same area. We also find that the current star formation rate is consistent with the picture in which stars are born only from self-gravitating starless cores. However, the cores must gain additional gas from the surroundings to reproduce the current IMF (e.g., its slope and peak mass), because the core mass cannot be accreted onto the star with 100% efficiency. Thus, the mass accretion from the surroundings may play a crucial role in determining the final stellar masses of stars.
UR - https://www.scopus.com/pages/publications/85103655990
U2 - 10.3847/2041-8213/abe7dd
DO - 10.3847/2041-8213/abe7dd
M3 - Article
SN - 2041-8205
VL - 910
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L6
ER -