The Core Mass Function in the Orion Nebula Cluster Region: What Determines the Final Stellar Masses?. (arXiv:2103.08527v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Takemura_H/0/1/0/all/0/1">Hideaki Takemura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamura_F/0/1/0/all/0/1">Fumitaka Nakamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_S/0/1/0/all/0/1">Shuo Kong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arce_H/0/1/0/all/0/1">Héctor G. Arce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ossenkopf_Okada_V/0/1/0/all/0/1">Volker Ossenkopf-Okada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">Ralf Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanhueza_P/0/1/0/all/0/1">Patricio Sanhueza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimajiri_Y/0/1/0/all/0/1">Yoshito Shimajiri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tsukagoshi_T/0/1/0/all/0/1">Takashi Tsukagoshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawabe_R/0/1/0/all/0/1">Ryohei Kawabe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishii_S/0/1/0/all/0/1">Shun Ishii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobashi_K/0/1/0/all/0/1">Kazuhito Dobashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimoikura_T/0/1/0/all/0/1">Tomomi Shimoikura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goldsmith_P/0/1/0/all/0/1">Paul F. Goldsmith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Monge_A/0/1/0/all/0/1">Álvaro Sánchez-Monge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kauffmann_J/0/1/0/all/0/1">Jens Kauffmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pillai_T/0/1/0/all/0/1">Thushara Pillai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padoan_P/0/1/0/all/0/1">Paolo Padoan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginsberg_A/0/1/0/all/0/1">Adam Ginsberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Rowan J. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bally_J/0/1/0/all/0/1">John Bally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mairs_S/0/1/0/all/0/1">Steve Mairs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">Jaime E. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lis_D/0/1/0/all/0/1">Dariusz C. Lis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burkhart_B/0/1/0/all/0/1">Blakesley Burkhart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schilke_P/0/1/0/all/0/1">Peter Schilke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_H/0/1/0/all/0/1">Hope How-Huan Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">Andrea Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Friesen_R/0/1/0/all/0/1">Rachel K. Friesen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goodman_A/0/1/0/all/0/1">Alyssa A. Goodman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harper_D/0/1/0/all/0/1">Doyal A. Harper</a>
Applying dendrogram analysis to the CARMA-NRO C$^{18}$O ($J$=1–0) data
having an angular resolution of $sim$ 8″, we identified 692 dense cores in the
Orion Nebula Cluster (ONC) 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
$M_odot$, consistent with previous studies. Our CMF has a peak at a subsolar
mass of $sim$ 0.1 $M_odot$, 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 a 100% efficiency.
Thus, the mass accretion from the surroundings may play a crucial role in
determining the final stellar masses of stars.
Applying dendrogram analysis to the CARMA-NRO C$^{18}$O ($J$=1–0) data
having an angular resolution of $sim$ 8″, we identified 692 dense cores in the
Orion Nebula Cluster (ONC) 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
$M_odot$, consistent with previous studies. Our CMF has a peak at a subsolar
mass of $sim$ 0.1 $M_odot$, 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 a 100% efficiency.
Thus, the mass accretion from the surroundings may play a crucial role in
determining the final stellar masses of stars.
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