Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness
JWST/MIRI images have been used to study the Fourier transform power spectra (PS) of two spiral galaxies, NGC 628 and NGC 5236, and two dwarfs, NGC 4449 and NGC 5068, at distances ranging from 4 to 10 Mpc. The PS slopes on scales larger than 200 pc range from $-0.6$ at $21\mu$m to $-1.2$ at $5.6\mu$...
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Maynooth Academic Publishing
2025-02-01
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| Series: | The Open Journal of Astrophysics |
| Online Access: | https://doi.org/10.33232/001c.130810 |
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| author | Bruce Elmegreen Angela Adamo Varun Bajaj Ana Duarte-Cabral Daniela Calzetti Michele Cignoni Matteo Correnti John S. Gallagher Kathryn Grasha Benjamin Gregg Kelsey E. Johnson Sean T. Linden Matteo Messa Goran Ostlin Alex Pedrini Jenna Ryon |
| author_facet | Bruce Elmegreen Angela Adamo Varun Bajaj Ana Duarte-Cabral Daniela Calzetti Michele Cignoni Matteo Correnti John S. Gallagher Kathryn Grasha Benjamin Gregg Kelsey E. Johnson Sean T. Linden Matteo Messa Goran Ostlin Alex Pedrini Jenna Ryon |
| author_sort | Bruce Elmegreen |
| collection | DOAJ |
| description | JWST/MIRI images have been used to study the Fourier transform power spectra (PS) of two spiral galaxies, NGC 628 and NGC 5236, and two dwarfs, NGC 4449 and NGC 5068, at distances ranging from 4 to 10 Mpc. The PS slopes on scales larger than 200 pc range from $-0.6$ at $21\mu$m to $-1.2$ at $5.6\mu$m. These slopes for one-dimensional PS are consistent with the PS slopes observed elsewhere using HI and dust emission. They are likely related to turbulence, but they may also be viewed as a hierarchical distribution of objects having a size-luminosity relation and size distribution function. There is no evidence for a kink or steepening of the PS at some transition from two-dimensional to three-dimensional turbulence on the scale of the disk thickness. This lack of a kink could be from large positional variations in the PS depending on two opposite effects: local bright sources that make the slope shallower and exponential galaxy profiles that make the slope steeper. The sources could also be confined to a layer of molecular clouds that is thinner than the HI or cool dust layers where PS kinks have been observed before. If the star formation layers observed in the mid-infrared here are too thin, then the PS kink could also be hidden in the broad tail of the JWST point spread function. |
| format | Article |
| id | doaj-art-99b528ed382948b09c6947341d9fa4a4 |
| institution | Kabale University |
| issn | 2565-6120 |
| language | English |
| publishDate | 2025-02-01 |
| publisher | Maynooth Academic Publishing |
| record_format | Article |
| series | The Open Journal of Astrophysics |
| spelling | doaj-art-99b528ed382948b09c6947341d9fa4a42025-08-20T03:33:17ZengMaynooth Academic PublishingThe Open Journal of Astrophysics2565-61202025-02-01810.33232/001c.130810Power Spectra of JWST images of Local Galaxies: Searching for Disk ThicknessBruce ElmegreenAngela AdamoVarun BajajAna Duarte-CabralDaniela CalzettiMichele CignoniMatteo CorrentiJohn S. GallagherKathryn GrashaBenjamin GreggKelsey E. JohnsonSean T. LindenMatteo MessaGoran OstlinAlex PedriniJenna RyonJWST/MIRI images have been used to study the Fourier transform power spectra (PS) of two spiral galaxies, NGC 628 and NGC 5236, and two dwarfs, NGC 4449 and NGC 5068, at distances ranging from 4 to 10 Mpc. The PS slopes on scales larger than 200 pc range from $-0.6$ at $21\mu$m to $-1.2$ at $5.6\mu$m. These slopes for one-dimensional PS are consistent with the PS slopes observed elsewhere using HI and dust emission. They are likely related to turbulence, but they may also be viewed as a hierarchical distribution of objects having a size-luminosity relation and size distribution function. There is no evidence for a kink or steepening of the PS at some transition from two-dimensional to three-dimensional turbulence on the scale of the disk thickness. This lack of a kink could be from large positional variations in the PS depending on two opposite effects: local bright sources that make the slope shallower and exponential galaxy profiles that make the slope steeper. The sources could also be confined to a layer of molecular clouds that is thinner than the HI or cool dust layers where PS kinks have been observed before. If the star formation layers observed in the mid-infrared here are too thin, then the PS kink could also be hidden in the broad tail of the JWST point spread function.https://doi.org/10.33232/001c.130810 |
| spellingShingle | Bruce Elmegreen Angela Adamo Varun Bajaj Ana Duarte-Cabral Daniela Calzetti Michele Cignoni Matteo Correnti John S. Gallagher Kathryn Grasha Benjamin Gregg Kelsey E. Johnson Sean T. Linden Matteo Messa Goran Ostlin Alex Pedrini Jenna Ryon Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness The Open Journal of Astrophysics |
| title | Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness |
| title_full | Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness |
| title_fullStr | Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness |
| title_full_unstemmed | Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness |
| title_short | Power Spectra of JWST images of Local Galaxies: Searching for Disk Thickness |
| title_sort | power spectra of jwst images of local galaxies searching for disk thickness |
| url | https://doi.org/10.33232/001c.130810 |
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