An Investigation of Disk Thickness in M51 from H-alpha, Pa-alpha, and Mid-Infrared Power Spectra
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arXiv
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| Formato: | Preprint |
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2025
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| author | Elmegreen, Bruce G. Calzetti, Daniela Adamo, Angela Sandstrom, Karin Dale, Daniel Bajaj, Varun Boyer, Martha L. Duarte-Cabral, Ana Chown, Ryan Correnti, Matteo Dalcanton, Julianne J. Draine, Bruce T. Gaches, Brandt Gallagher III, John S. Grasha, Kathryn Gregg, Benjamin Hunt, Leslie K. Johnson, Kelsey E. Kennicutt, Jr., Robert Klessen, Ralf S. Leroy, Adam K. Linden, Sean McLeod, Anna F. Messa, Matteo Ostlin, Goran Padave, Mansi Roman-Duval, Julia Smith, J. D. Walter, Fabian Weinbeck, Tony D. |
| author_facet | Elmegreen, Bruce G. Calzetti, Daniela Adamo, Angela Sandstrom, Karin Dale, Daniel Bajaj, Varun Boyer, Martha L. Duarte-Cabral, Ana Chown, Ryan Correnti, Matteo Dalcanton, Julianne J. Draine, Bruce T. Gaches, Brandt Gallagher III, John S. Grasha, Kathryn Gregg, Benjamin Hunt, Leslie K. Johnson, Kelsey E. Kennicutt, Jr., Robert Klessen, Ralf S. Leroy, Adam K. Linden, Sean McLeod, Anna F. Messa, Matteo Ostlin, Goran Padave, Mansi Roman-Duval, Julia Smith, J. D. Walter, Fabian Weinbeck, Tony D. |
| contents | Power spectra (PS) of high-resolution images of M51 (NGC 5194) taken with the Hubble Space Telescope and the James Webb Space Telescope have been examined for evidence of disk thickness in the form of a change in slope between large scales, which map two-dimensional correlated structures, and small scales, which map three-dimensional correlated structures. Such a slope change is observed here in H-alpha, and possibly Pa-alpha, using average PS of azimuthal intensity scans that avoid bright peaks. The physical scale of the slope change occurs at ~120 pc and ~170 pc for these two transitions, respectively. A radial dependence in the shape of the H-alpha PS also suggests that the length scale drops from ~180 pc at 5 kpc, to ~90 pc at 2 kpc, to ~25 pc in the central ~kpc. We interpret these lengths as comparable to the thicknesses of the star-forming disk traced by HII regions. The corresponding emission measure is ~100 times larger than what is expected from the diffuse ionized gas. PS of JWST Mid-IR Instrument (MIRI) images in 8 passbands have more gradual changes in slope, making it difficult to determine a specific value of the thickness for this emission. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_05430 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | An Investigation of Disk Thickness in M51 from H-alpha, Pa-alpha, and Mid-Infrared Power Spectra Elmegreen, Bruce G. Calzetti, Daniela Adamo, Angela Sandstrom, Karin Dale, Daniel Bajaj, Varun Boyer, Martha L. Duarte-Cabral, Ana Chown, Ryan Correnti, Matteo Dalcanton, Julianne J. Draine, Bruce T. Gaches, Brandt Gallagher III, John S. Grasha, Kathryn Gregg, Benjamin Hunt, Leslie K. Johnson, Kelsey E. Kennicutt, Jr., Robert Klessen, Ralf S. Leroy, Adam K. Linden, Sean McLeod, Anna F. Messa, Matteo Ostlin, Goran Padave, Mansi Roman-Duval, Julia Smith, J. D. Walter, Fabian Weinbeck, Tony D. Astrophysics of Galaxies Power spectra (PS) of high-resolution images of M51 (NGC 5194) taken with the Hubble Space Telescope and the James Webb Space Telescope have been examined for evidence of disk thickness in the form of a change in slope between large scales, which map two-dimensional correlated structures, and small scales, which map three-dimensional correlated structures. Such a slope change is observed here in H-alpha, and possibly Pa-alpha, using average PS of azimuthal intensity scans that avoid bright peaks. The physical scale of the slope change occurs at ~120 pc and ~170 pc for these two transitions, respectively. A radial dependence in the shape of the H-alpha PS also suggests that the length scale drops from ~180 pc at 5 kpc, to ~90 pc at 2 kpc, to ~25 pc in the central ~kpc. We interpret these lengths as comparable to the thicknesses of the star-forming disk traced by HII regions. The corresponding emission measure is ~100 times larger than what is expected from the diffuse ionized gas. PS of JWST Mid-IR Instrument (MIRI) images in 8 passbands have more gradual changes in slope, making it difficult to determine a specific value of the thickness for this emission. |
| title | An Investigation of Disk Thickness in M51 from H-alpha, Pa-alpha, and Mid-Infrared Power Spectra |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.05430 |