Molecular cloud matching in CO and dust in M33 II. Physical properties of giant molecular clouds
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| Main Authors: | , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Keilmann, Eduard Kabanovic, Slawa Schneider, Nicola Ossenkopf-Okada, Volker Stutzki, Jürgen Kobayashi, Masato I. N. Simon, Robert Buchbender, Christof Riechers, Dominik Bigiel, Frank Tabatabaei, Fatemeh |
| author_facet | Keilmann, Eduard Kabanovic, Slawa Schneider, Nicola Ossenkopf-Okada, Volker Stutzki, Jürgen Kobayashi, Masato I. N. Simon, Robert Buchbender, Christof Riechers, Dominik Bigiel, Frank Tabatabaei, Fatemeh |
| contents | Understanding mass, size, and surface mass density of giant molecular clouds (GMCs) in galaxies is key to insights into star formation processes. We analyze these in M33 using Herschel dust and archival IRAM 30m telescope data, compared to Milky Way CO data. A Dendrogram algorithm on a 2D dust map and a Xco factor map are used for M33 instead of a constant value. Dust and CO-derived values are similar, with mean radii of $\sim\,$$58\,$pc for the dust and $\sim\,$$68\,$pc for CO.
Largest GMAs are about $150\,$pc in radius, similar to the Milky Way, suggesting a size-limiting process. M33 contains less massive, lower-density GMCs compared to the Milky Way. The highest mass GMCs observed in the Milky Way are mostly absent in M33. M33's mean surface mass density is much lower, due to the Milky Way's higher column densities despite similar GMC areas.
No systematic gradients in M33's physical properties were found with galactocentric radius, but higher densities and masses near the center suggest increased star formation. In both galaxies, 30% of molecular mass is central. The GMC mass power-law spectrum index is $α=2.3\pm0.1$ and $α=1.9\pm0.1$ for dust and CO in M33, respectively.
We conclude that M33 and Milky Way GMCs are mostly similar, though M33 lacks high-mass GMCs, with no clear explanation. GMC properties weakly depend on galactic environment, with stellar feedback as a factor needing further study. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2411_10806 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Molecular cloud matching in CO and dust in M33 II. Physical properties of giant molecular clouds Keilmann, Eduard Kabanovic, Slawa Schneider, Nicola Ossenkopf-Okada, Volker Stutzki, Jürgen Kobayashi, Masato I. N. Simon, Robert Buchbender, Christof Riechers, Dominik Bigiel, Frank Tabatabaei, Fatemeh Astrophysics of Galaxies Understanding mass, size, and surface mass density of giant molecular clouds (GMCs) in galaxies is key to insights into star formation processes. We analyze these in M33 using Herschel dust and archival IRAM 30m telescope data, compared to Milky Way CO data. A Dendrogram algorithm on a 2D dust map and a Xco factor map are used for M33 instead of a constant value. Dust and CO-derived values are similar, with mean radii of $\sim\,$$58\,$pc for the dust and $\sim\,$$68\,$pc for CO. Largest GMAs are about $150\,$pc in radius, similar to the Milky Way, suggesting a size-limiting process. M33 contains less massive, lower-density GMCs compared to the Milky Way. The highest mass GMCs observed in the Milky Way are mostly absent in M33. M33's mean surface mass density is much lower, due to the Milky Way's higher column densities despite similar GMC areas. No systematic gradients in M33's physical properties were found with galactocentric radius, but higher densities and masses near the center suggest increased star formation. In both galaxies, 30% of molecular mass is central. The GMC mass power-law spectrum index is $α=2.3\pm0.1$ and $α=1.9\pm0.1$ for dust and CO in M33, respectively. We conclude that M33 and Milky Way GMCs are mostly similar, though M33 lacks high-mass GMCs, with no clear explanation. GMC properties weakly depend on galactic environment, with stellar feedback as a factor needing further study. |
| title | Molecular cloud matching in CO and dust in M33 II. Physical properties of giant molecular clouds |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2411.10806 |