The core mass function in the Orion Nebula Cluster region : what determines the final stellar masses?
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...
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2021 March 22 |
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Gesehen am 21.04.2021 |
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Enthalten in: The astrophysical journal. Part 2, Letters - London : Institute of Physics Publ., 1995, 910(2021), 1, Artikel-ID L6, Seite 1-7 |
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volume:910 ; year:2021 ; number:1 ; elocationid:L6 ; pages:1-7 ; extent:7 |
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10.3847/2041-8213/abe7dd |
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1755581637 |
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| 100 | 1 | |a Takemura, Hideaki |e verfasserin |0 (DE-588)1237007488 |0 (DE-627)1762864304 |4 aut | |
| 245 | 1 | 4 | |a The core mass function in the Orion Nebula Cluster region |b what determines the final stellar masses? |c Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper |
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| 520 | |a 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. | ||
| 700 | 1 | |a Nakamura, Fumitaka |e verfasserin |4 aut | |
| 700 | 1 | |a Kong, Shuo |e verfasserin |4 aut | |
| 700 | 1 | |a Arce, Héctor G. |e verfasserin |4 aut | |
| 700 | 1 | |a Carpenter, John M. |e verfasserin |4 aut | |
| 700 | 1 | |a Ossenkopf-Okada, Volker |e verfasserin |4 aut | |
| 700 | 1 | |a Klessen, Ralf S. |d 1968- |e verfasserin |0 (DE-588)120533820 |0 (DE-627)392381532 |0 (DE-576)178685399 |4 aut | |
| 700 | 1 | |a Sanhueza, Patricio |e verfasserin |4 aut | |
| 700 | 1 | |a Shimajiri, Yoshito |e verfasserin |4 aut | |
| 700 | 1 | |a Tsukagoshi, Takashi |e verfasserin |4 aut | |
| 700 | 1 | |a Kawabe, Ryohei |e verfasserin |4 aut | |
| 700 | 1 | |a Ishii, Shun |e verfasserin |4 aut | |
| 700 | 1 | |a Dobashi, Kazuhito |e verfasserin |4 aut | |
| 700 | 1 | |a Shimoikura, Tomomi |e verfasserin |4 aut | |
| 700 | 1 | |a Goldsmith, Paul F. |e verfasserin |4 aut | |
| 700 | 1 | |a Sánchez-Monge, Álvaro |e verfasserin |4 aut | |
| 700 | 1 | |a Kauffmann, Jens |e verfasserin |4 aut | |
| 700 | 1 | |a Pillai, Thushara G. S. |e verfasserin |4 aut | |
| 700 | 1 | |a Padoan, Paolo |e verfasserin |4 aut | |
| 700 | 1 | |a Ginsberg, Adam |e verfasserin |4 aut | |
| 700 | 1 | |a Smith, Rowan J. |e verfasserin |4 aut | |
| 700 | 1 | |a Bally, John |e verfasserin |4 aut | |
| 700 | 1 | |a Mairs, Steve |e verfasserin |4 aut | |
| 700 | 1 | |a Pineda, Jaime E. |e verfasserin |4 aut | |
| 700 | 1 | |a Lis, Dariusz C. |e verfasserin |4 aut | |
| 700 | 1 | |a Burkhart, Blakesley |e verfasserin |4 aut | |
| 700 | 1 | |a Schilke, Peter |e verfasserin |4 aut | |
| 700 | 1 | |a Chen, Hope How-Huan |e verfasserin |4 aut | |
| 700 | 1 | |a Isella, Andrea |e verfasserin |4 aut | |
| 700 | 1 | |a Friesen, Rachel K. |e verfasserin |4 aut | |
| 700 | 1 | |a Goodman, Alyssa A. |e verfasserin |4 aut | |
| 700 | 1 | |a Harper, Doyal A. |e verfasserin |4 aut | |
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10.3847/2041-8213/abe7dd doi (DE-627)1755581637 (DE-599)KXP1755581637 (OCoLC)1341405077 DE-627 ger DE-627 rda eng Takemura, Hideaki verfasserin (DE-588)1237007488 (DE-627)1762864304 aut The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper 2021 March 22 7 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 21.04.2021 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. Nakamura, Fumitaka verfasserin aut Kong, Shuo verfasserin aut Arce, Héctor G. verfasserin aut Carpenter, John M. verfasserin aut Ossenkopf-Okada, Volker verfasserin aut Klessen, Ralf S. 1968- verfasserin (DE-588)120533820 (DE-627)392381532 (DE-576)178685399 aut Sanhueza, Patricio verfasserin aut Shimajiri, Yoshito verfasserin aut Tsukagoshi, Takashi verfasserin aut Kawabe, Ryohei verfasserin aut Ishii, Shun verfasserin aut Dobashi, Kazuhito verfasserin aut Shimoikura, Tomomi verfasserin aut Goldsmith, Paul F. verfasserin aut Sánchez-Monge, Álvaro verfasserin aut Kauffmann, Jens verfasserin aut Pillai, Thushara G. S. verfasserin aut Padoan, Paolo verfasserin aut Ginsberg, Adam verfasserin aut Smith, Rowan J. verfasserin aut Bally, John verfasserin aut Mairs, Steve verfasserin aut Pineda, Jaime E. verfasserin aut Lis, Dariusz C. verfasserin aut Burkhart, Blakesley verfasserin aut Schilke, Peter verfasserin aut Chen, Hope How-Huan verfasserin aut Isella, Andrea verfasserin aut Friesen, Rachel K. verfasserin aut Goodman, Alyssa A. verfasserin aut Harper, Doyal A. verfasserin aut Enthalten in The astrophysical journal. Part 2, Letters London : Institute of Physics Publ., 1995 910(2021), 1, Artikel-ID L6, Seite 1-7 Online-Ressource (DE-627)312189028 (DE-600)2006858-X (DE-576)090890876 2041-8213 nnns volume:910 year:2021 number:1 elocationid:L6 pages:1-7 extent:7 https://doi.org/10.3847/2041-8213/abe7dd Verlag Resolving-System lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 910 2021 1 L6 1-7 7 2013 01 DE-16-250 3914119977 00 --%%-- --%%-- --%%-- --%%-- l01 21-04-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 |
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10.3847/2041-8213/abe7dd doi (DE-627)1755581637 (DE-599)KXP1755581637 (OCoLC)1341405077 DE-627 ger DE-627 rda eng Takemura, Hideaki verfasserin (DE-588)1237007488 (DE-627)1762864304 aut The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper 2021 March 22 7 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 21.04.2021 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. Nakamura, Fumitaka verfasserin aut Kong, Shuo verfasserin aut Arce, Héctor G. verfasserin aut Carpenter, John M. verfasserin aut Ossenkopf-Okada, Volker verfasserin aut Klessen, Ralf S. 1968- verfasserin (DE-588)120533820 (DE-627)392381532 (DE-576)178685399 aut Sanhueza, Patricio verfasserin aut Shimajiri, Yoshito verfasserin aut Tsukagoshi, Takashi verfasserin aut Kawabe, Ryohei verfasserin aut Ishii, Shun verfasserin aut Dobashi, Kazuhito verfasserin aut Shimoikura, Tomomi verfasserin aut Goldsmith, Paul F. verfasserin aut Sánchez-Monge, Álvaro verfasserin aut Kauffmann, Jens verfasserin aut Pillai, Thushara G. S. verfasserin aut Padoan, Paolo verfasserin aut Ginsberg, Adam verfasserin aut Smith, Rowan J. verfasserin aut Bally, John verfasserin aut Mairs, Steve verfasserin aut Pineda, Jaime E. verfasserin aut Lis, Dariusz C. verfasserin aut Burkhart, Blakesley verfasserin aut Schilke, Peter verfasserin aut Chen, Hope How-Huan verfasserin aut Isella, Andrea verfasserin aut Friesen, Rachel K. verfasserin aut Goodman, Alyssa A. verfasserin aut Harper, Doyal A. verfasserin aut Enthalten in The astrophysical journal. Part 2, Letters London : Institute of Physics Publ., 1995 910(2021), 1, Artikel-ID L6, Seite 1-7 Online-Ressource (DE-627)312189028 (DE-600)2006858-X (DE-576)090890876 2041-8213 nnns volume:910 year:2021 number:1 elocationid:L6 pages:1-7 extent:7 https://doi.org/10.3847/2041-8213/abe7dd Verlag Resolving-System lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 910 2021 1 L6 1-7 7 2013 01 DE-16-250 3914119977 00 --%%-- --%%-- --%%-- --%%-- l01 21-04-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 |
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10.3847/2041-8213/abe7dd doi (DE-627)1755581637 (DE-599)KXP1755581637 (OCoLC)1341405077 DE-627 ger DE-627 rda eng Takemura, Hideaki verfasserin (DE-588)1237007488 (DE-627)1762864304 aut The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper 2021 March 22 7 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 21.04.2021 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. Nakamura, Fumitaka verfasserin aut Kong, Shuo verfasserin aut Arce, Héctor G. verfasserin aut Carpenter, John M. verfasserin aut Ossenkopf-Okada, Volker verfasserin aut Klessen, Ralf S. 1968- verfasserin (DE-588)120533820 (DE-627)392381532 (DE-576)178685399 aut Sanhueza, Patricio verfasserin aut Shimajiri, Yoshito verfasserin aut Tsukagoshi, Takashi verfasserin aut Kawabe, Ryohei verfasserin aut Ishii, Shun verfasserin aut Dobashi, Kazuhito verfasserin aut Shimoikura, Tomomi verfasserin aut Goldsmith, Paul F. verfasserin aut Sánchez-Monge, Álvaro verfasserin aut Kauffmann, Jens verfasserin aut Pillai, Thushara G. S. verfasserin aut Padoan, Paolo verfasserin aut Ginsberg, Adam verfasserin aut Smith, Rowan J. verfasserin aut Bally, John verfasserin aut Mairs, Steve verfasserin aut Pineda, Jaime E. verfasserin aut Lis, Dariusz C. verfasserin aut Burkhart, Blakesley verfasserin aut Schilke, Peter verfasserin aut Chen, Hope How-Huan verfasserin aut Isella, Andrea verfasserin aut Friesen, Rachel K. verfasserin aut Goodman, Alyssa A. verfasserin aut Harper, Doyal A. verfasserin aut Enthalten in The astrophysical journal. Part 2, Letters London : Institute of Physics Publ., 1995 910(2021), 1, Artikel-ID L6, Seite 1-7 Online-Ressource (DE-627)312189028 (DE-600)2006858-X (DE-576)090890876 2041-8213 nnns volume:910 year:2021 number:1 elocationid:L6 pages:1-7 extent:7 https://doi.org/10.3847/2041-8213/abe7dd Verlag Resolving-System lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 910 2021 1 L6 1-7 7 2013 01 DE-16-250 3914119977 00 --%%-- --%%-- --%%-- --%%-- l01 21-04-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 |
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10.3847/2041-8213/abe7dd doi (DE-627)1755581637 (DE-599)KXP1755581637 (OCoLC)1341405077 DE-627 ger DE-627 rda eng Takemura, Hideaki verfasserin (DE-588)1237007488 (DE-627)1762864304 aut The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper 2021 March 22 7 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 21.04.2021 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. Nakamura, Fumitaka verfasserin aut Kong, Shuo verfasserin aut Arce, Héctor G. verfasserin aut Carpenter, John M. verfasserin aut Ossenkopf-Okada, Volker verfasserin aut Klessen, Ralf S. 1968- verfasserin (DE-588)120533820 (DE-627)392381532 (DE-576)178685399 aut Sanhueza, Patricio verfasserin aut Shimajiri, Yoshito verfasserin aut Tsukagoshi, Takashi verfasserin aut Kawabe, Ryohei verfasserin aut Ishii, Shun verfasserin aut Dobashi, Kazuhito verfasserin aut Shimoikura, Tomomi verfasserin aut Goldsmith, Paul F. verfasserin aut Sánchez-Monge, Álvaro verfasserin aut Kauffmann, Jens verfasserin aut Pillai, Thushara G. S. verfasserin aut Padoan, Paolo verfasserin aut Ginsberg, Adam verfasserin aut Smith, Rowan J. verfasserin aut Bally, John verfasserin aut Mairs, Steve verfasserin aut Pineda, Jaime E. verfasserin aut Lis, Dariusz C. verfasserin aut Burkhart, Blakesley verfasserin aut Schilke, Peter verfasserin aut Chen, Hope How-Huan verfasserin aut Isella, Andrea verfasserin aut Friesen, Rachel K. verfasserin aut Goodman, Alyssa A. verfasserin aut Harper, Doyal A. verfasserin aut Enthalten in The astrophysical journal. Part 2, Letters London : Institute of Physics Publ., 1995 910(2021), 1, Artikel-ID L6, Seite 1-7 Online-Ressource (DE-627)312189028 (DE-600)2006858-X (DE-576)090890876 2041-8213 nnns volume:910 year:2021 number:1 elocationid:L6 pages:1-7 extent:7 https://doi.org/10.3847/2041-8213/abe7dd Verlag Resolving-System lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 910 2021 1 L6 1-7 7 2013 01 DE-16-250 3914119977 00 --%%-- --%%-- --%%-- --%%-- l01 21-04-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 |
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10.3847/2041-8213/abe7dd doi (DE-627)1755581637 (DE-599)KXP1755581637 (OCoLC)1341405077 DE-627 ger DE-627 rda eng Takemura, Hideaki verfasserin (DE-588)1237007488 (DE-627)1762864304 aut The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper 2021 March 22 7 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 21.04.2021 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. Nakamura, Fumitaka verfasserin aut Kong, Shuo verfasserin aut Arce, Héctor G. verfasserin aut Carpenter, John M. verfasserin aut Ossenkopf-Okada, Volker verfasserin aut Klessen, Ralf S. 1968- verfasserin (DE-588)120533820 (DE-627)392381532 (DE-576)178685399 aut Sanhueza, Patricio verfasserin aut Shimajiri, Yoshito verfasserin aut Tsukagoshi, Takashi verfasserin aut Kawabe, Ryohei verfasserin aut Ishii, Shun verfasserin aut Dobashi, Kazuhito verfasserin aut Shimoikura, Tomomi verfasserin aut Goldsmith, Paul F. verfasserin aut Sánchez-Monge, Álvaro verfasserin aut Kauffmann, Jens verfasserin aut Pillai, Thushara G. S. verfasserin aut Padoan, Paolo verfasserin aut Ginsberg, Adam verfasserin aut Smith, Rowan J. verfasserin aut Bally, John verfasserin aut Mairs, Steve verfasserin aut Pineda, Jaime E. verfasserin aut Lis, Dariusz C. verfasserin aut Burkhart, Blakesley verfasserin aut Schilke, Peter verfasserin aut Chen, Hope How-Huan verfasserin aut Isella, Andrea verfasserin aut Friesen, Rachel K. verfasserin aut Goodman, Alyssa A. verfasserin aut Harper, Doyal A. verfasserin aut Enthalten in The astrophysical journal. Part 2, Letters London : Institute of Physics Publ., 1995 910(2021), 1, Artikel-ID L6, Seite 1-7 Online-Ressource (DE-627)312189028 (DE-600)2006858-X (DE-576)090890876 2041-8213 nnns volume:910 year:2021 number:1 elocationid:L6 pages:1-7 extent:7 https://doi.org/10.3847/2041-8213/abe7dd Verlag Resolving-System lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 910 2021 1 L6 1-7 7 2013 01 DE-16-250 3914119977 00 --%%-- --%%-- --%%-- --%%-- l01 21-04-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a2200265 4500</leader><controlfield tag="001">1755581637</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220819172332.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">210421s2021 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.3847/2041-8213/abe7dd</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)1755581637</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)KXP1755581637</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(OCoLC)1341405077</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rda</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Takemura, Hideaki</subfield><subfield code="e">verfasserin</subfield><subfield code="0">(DE-588)1237007488</subfield><subfield code="0">(DE-627)1762864304</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The core mass function in the Orion Nebula Cluster region</subfield><subfield code="b">what determines the final stellar masses?</subfield><subfield code="c">Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2021 March 22</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">7</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">Gesehen am 21.04.2021</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">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. 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2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_32 2013 01 DE-16-250 03 s s_7 2013 01 DE-16-250 04 p (DE-627)1445553155 Klessen, Ralf S. 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_7 The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper |
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2013 hd2021 2013 wissenschaftlicher Artikel (Zeitschrift) 2013 per_32 2013 s_7 2013 Klessen, Ralf S. 2013 ZAH Institut für Theoretische Astrophysik 2013 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 Verfasser 2013 pos_7 |
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The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? |
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The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? Hideaki Takemura, Fumitaka Nakamura, Shuo Kong, Héctor G. Arce, John M. Carpenter, Volker Ossenkopf-Okada, Ralf Klessen, Patricio Sanhueza, Yoshito Shimajiri, Takashi Tsukagoshi, Ryohei Kawabe, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Paul F. Goldsmith, Álvaro Sánchez-Monge, Jens Kauffmann, Thushara G.S. Pillai, Paolo Padoan, Adam Ginsberg, Rowan J. Smith, John Bally, Steve Mairs, Jaime E. Pineda, Dariusz C. Lis, Blakesley Burkhart, Peter Schilke, Hope How-Huan Chen, Andrea Isella, Rachel K. Friesen, Alyssa A. Goodman, and Doyal A. Harper |
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Takemura, Hideaki Nakamura, Fumitaka Kong, Shuo Arce, Héctor G. Carpenter, John M. Ossenkopf-Okada, Volker Klessen, Ralf S. Sanhueza, Patricio Shimajiri, Yoshito Tsukagoshi, Takashi Kawabe, Ryohei Ishii, Shun Dobashi, Kazuhito Shimoikura, Tomomi Goldsmith, Paul F. Sánchez-Monge, Álvaro Kauffmann, Jens Pillai, Thushara G. S. Padoan, Paolo Ginsberg, Adam Smith, Rowan J. Bally, John Mairs, Steve Pineda, Jaime E. Lis, Dariusz C. Burkhart, Blakesley Schilke, Peter Chen, Hope How-Huan Isella, Andrea Friesen, Rachel K. Goodman, Alyssa A. Harper, Doyal A. |
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what determines the final stellar masses? |
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core mass function in the orion nebula cluster regionwhat determines the final stellar masses? |
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The core mass function in the Orion Nebula Cluster region what determines the final stellar masses? |
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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. Gesehen am 21.04.2021 |
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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. Gesehen am 21.04.2021 |
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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. Gesehen am 21.04.2021 |
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