KMS of Xinjiang Astronomical Observatory, CAS
| Components of star formation in NGC 253: Non-negative matrix factorization analysis with the ALCHEMI integrated intensity images | |
Kishikawa, Ryo1; Harada, Nanase2,3; Saito, Toshiki4,5; Aalto, Susanne; Colzi, Laura6; Gorski, Mark7,8; Henkel, Christian9,10 ; Mangum, Jeffrey G.11; Martin, Sergio12,13; Muller, Sebastian5; Nishimura, Yuri14; Rivilla, Victor M.6; Sakamoto, Kazushi15; van der Werf, Paul16; Viti, Serena16,17
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| 2024-11-29 | |
| Source Publication | PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
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| ISSN | 0004-6264 |
| Pages | 20 |
| Contribution Rank | 10 |
| Abstract | It is essential to examine the physical or chemical properties of molecular gas in starburst galaxies to reveal the underlying mechanisms characterizing starbursts. We used non-negative matrix factorization (NMF) to extract individual molecular or physical components involved in the star formation process in NGC 253. We used images of 148 transitions from 44 different species of the ALMA large program ALCHEMI. Additionally, we included the continuum images at ALMA Bands 3 and 7 from the same dataset. For the five NMF components (NF1-NF5), we obtained that their distributions correspond to various basic phenomena related to star formation: (i) low-density gas extended through the galactic central molecular zone (NF2), (ii) shocks (NF3), (iii) starburst regions (NF4), and (iv) young star-forming regions (NF5). The other component (NF1) is related to excitation; three components obtained by NMF (NF3, NF1, and NF5) show a strong dependence upon the upper state energies of transitions, and represent low, intermediate, and high excitation, respectively. We also compared our results using principal component analysis (PCA) previously applied to the same dataset. Molecular components extracted from NMF are similar to the ones obtained from PCA. However, NMF is better at extracting components associated with a single physical component, while a single component in PCA usually contains information on multiple physical components. This is especially true for features with weak intensities like emission from outflows. Our results suggest that NMF can be one of the promising methods for interpreting molecular line survey data, especially in the upcoming era of wide-band receivers. |
| Keyword | galaxies: starburst galaxies: star formation galaxies: individual (NGC 253) ISM: molecules methods: data analysis |
| DOI | 10.1093/pasj/psae095 |
| Indexed By | SCI |
| Language | 英语 |
| WOS Keyword | CENTRAL MOLECULAR ZONE ; STARBURST ; OUTFLOW ; GAS ; EMISSION ; GALAXIES ; METHANOL ; DIAGNOSTICS ; CLUSTERS ; FEEDBACK |
| Funding Project | National Astronomical Observatory of Japan[2018.1.00162] ; ALMA ; National Astronomical Observatory of Japan[JP23K13140] ; National Astronomical Observatory of Japan[JP23K20035] ; JSPS KAKENHI |
| WOS Research Area | Astronomy & Astrophysics |
| WOS Subject | Astronomy & Astrophysics |
| WOS ID | WOS:001367251300001 |
| Publisher | OXFORD UNIV PRESS |
| Funding Organization | National Astronomical Observatory of Japan ; ALMA ; National Astronomical Observatory of Japan ; JSPS KAKENHI |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/7246 |
| Collection | 中国科学院新疆天文台 射电天文研究室_恒星形成与演化研究团组 |
| Corresponding Author | Kishikawa, Ryo |
| Affiliation | 1.Tokyo Metropolitan Univ, Dept Phys, 1-1 Minami Osawa, Hachioji, Tokyo 1920397, Japan 2.Natl Astron Observ Japan, Mitaka, 1818588, Japan 3.SOKENDAI, Grad Inst Adv Studies, Astron Sci Program, 2-21-1 Osawa, Mitaka, Tokyo 1811855, Japan 4.Shizuoka Univ, Fac Global Interdisciplinary Sci & Innovat, 836 Ohya, Suruga Ku, Shizuoka 4228529, Japan 5.Chalmers Univ Technol, Dept Space Earth & Environm, Onsala Space Observ, Onsala, Sweden 6.CSIC INTA, Ctr Astrobiol CAB, Ctra Ajalvir Km 4, Madrid 28850, Spain 7.Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys CIE, Evanston, IL 60208 USA 8.Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA 9.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany 10.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China 11.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA 12.European Southern Observ, Alonso de Cordova 3107, Santiago, Chile 13.Joint ALMA Observ, Alonsode Cordova 3107, Santiago, Chile 14.Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, 1810015, Japan 15.Acad Sinica, Inst Astron & Astrophys, 11F NTU Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 106216, Taiwan 16.Leiden Univ Observ, POB 9513, Leiden, Netherlands 17.UCL, Dept Phys & Astron, London WC1E 6BT, England |
| Recommended Citation GB/T 7714 | Kishikawa, Ryo,Harada, Nanase,Saito, Toshiki,et al. Components of star formation in NGC 253: Non-negative matrix factorization analysis with the ALCHEMI integrated intensity images[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,2024:20. |
| APA | Kishikawa, Ryo.,Harada, Nanase.,Saito, Toshiki.,Aalto, Susanne.,Colzi, Laura.,...&Viti, Serena.(2024).Components of star formation in NGC 253: Non-negative matrix factorization analysis with the ALCHEMI integrated intensity images.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,20. |
| MLA | Kishikawa, Ryo,et al."Components of star formation in NGC 253: Non-negative matrix factorization analysis with the ALCHEMI integrated intensity images".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN (2024):20. |
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| Kishikawa-2024-Compo（2768KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-SA | View Application Full Text | |
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