The central region of spiral galaxies as seen by Herschel. M 81, M 99, and M 100

Sauvage, M., Sacchi, N., Bendo, G. J., Boselli, A., Pohlen, M., Wilson, C. D., Auld, R., Baes, M., Barlow, M. J., Bock, J. J., Bradford, M., Buat, V., Castro-Rodriguez, N., Chanial, P., Charlot, S., Ciesla, L., Clements, D. L., Cooray, A., Cormier, D., Cortese, L., Davies, J. I., Dwek, E., Eales, S. A., Elbaz, D., Galametz, M., Galliano, F., Gear, W. K., Glenn, J., Gomez, H. L., Griffin, M., Hony, S., Isaak, K. G., Levenson, L. R., Lu, N., Madden, S. C., O'Halloran, B., Okumura, K., Oliver, S., Page, M. J., Panuzzo, P., Papageorgiou, A., Parkin, T. J., Perez-Fournon, I., Rangwala, N., Rigby, E. E., Roussel, H., Rykala, A., Schulz, B., Schirm, M. R. P., Smith, M. W. L., Spinoglio, L., Stevens, Jason, Srinivasan, S., Symeonidis, M., Trichas, M., Vaccari, M., Vigroux, L., Wozniak, H., Wright, G. S. and Zeilinger, W.W. (2010) The central region of spiral galaxies as seen by Herschel. M 81, M 99, and M 100. Astronomy & Astrophysics, 518: L64. ISSN 0004-6361

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With appropriate spatial resolution, images of spiral galaxies in thermal infrared (~10 micron and beyond) often reveal a bright central component, distinct from the stellar bulge, superimposed on a disk with prominent spiral arms. ISO and Spitzer studies have shown that much of the scatter in the mid-infrared colors of spiral galaxies is related to changes in the relative importance of these two components, rather than to other modifications, such as the morphological type or star formation rate, that affect the properties of the galaxy as a whole. With the Herschel imaging capability from 70 to 500 micron, we revisit this two-component approach at longer wavelengths, to see if it still provides a working description of the brightness distribution of galaxies, and to determine its implications on the interpretation of global far-infrared properties of galaxies.

Item Type	Article
Keywords	infrared: galaxies, submillimeter: galaxies, galaxies:, spiral, galaxies: nuclei, galaxies: fundamental parameters
Date Deposited	15 May 2025 12:19
Last Modified	30 May 2025 23:48