Integral field spectroscopy of the planetary nebula NGC 3242 and the puzzling nature of its low ionization structures
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| Main Authors: | , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Konstantinou, L. Akras, S. Garcia-Rojas, J. Bouvis, K. Gonçalves, D. R. Monteiro, H. Boumis, P. Mari, M. B. Aleman, I. Monreal-Ibero, A. |
| author_facet | Konstantinou, L. Akras, S. Garcia-Rojas, J. Bouvis, K. Gonçalves, D. R. Monteiro, H. Boumis, P. Mari, M. B. Aleman, I. Monreal-Ibero, A. |
| contents | The physico-chemical properties of the planetary nebula (PN) NGC 3242 are investigated in both 1D and 2D, using Integral Field Unit (IFU) data. This PN has a complex morphology with multiple shells and contains a pair of structures with a lower degree of ionization compared to the main nebular components. These structures are known as low ionization structures (LISs), and their origin is still a mystery. With the capabilities provided by IFU spectroscopy, we aim to gain a better understanding of the behavior of nebular properties in the LISs. Data from the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT) were used in order to perform a spatially resolved physico-chemical analysis of NGC 3242 both in 2D, through the analysis of emission line maps, and in 1D, simulating long-slit spectroscopy, with pseudo-slits. Through the deeper investigation of MUSE data, we detect new structures perpendicular to the pair of LISs of NGC 3242, which are mainly seen in the light of [S III] and [N II]. In addition, two arc-like structures are revealed. Moreover, an inner jet-like structure is found through its [Fe III] emission. The interaction of the jet with the rim may be related to the formation of knots and blobs. The higher value of Te, is estimated from the [S III] diagnostic lines, followed by Te ([N II]), Te(H I) and finally Te (He I). In all cases, Te is higher at the inner nebular structures. Regarding electron density, ne, is lower at the LISs, while an increase is observed at the nebular rim. Diagnostic diagrams confirm that NGC 3242 is a highly ionized nebula. Moreover, the MUSE data unveiled for the first time in this PN, the atomic line [C I] λ8727, primarily emitted from the LISs. This finding suggests that these structures may consist of a molecular core surrounded by neutral and ionized gas |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_16662 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Integral field spectroscopy of the planetary nebula NGC 3242 and the puzzling nature of its low ionization structures Konstantinou, L. Akras, S. Garcia-Rojas, J. Bouvis, K. Gonçalves, D. R. Monteiro, H. Boumis, P. Mari, M. B. Aleman, I. Monreal-Ibero, A. Solar and Stellar Astrophysics Astrophysics of Galaxies The physico-chemical properties of the planetary nebula (PN) NGC 3242 are investigated in both 1D and 2D, using Integral Field Unit (IFU) data. This PN has a complex morphology with multiple shells and contains a pair of structures with a lower degree of ionization compared to the main nebular components. These structures are known as low ionization structures (LISs), and their origin is still a mystery. With the capabilities provided by IFU spectroscopy, we aim to gain a better understanding of the behavior of nebular properties in the LISs. Data from the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT) were used in order to perform a spatially resolved physico-chemical analysis of NGC 3242 both in 2D, through the analysis of emission line maps, and in 1D, simulating long-slit spectroscopy, with pseudo-slits. Through the deeper investigation of MUSE data, we detect new structures perpendicular to the pair of LISs of NGC 3242, which are mainly seen in the light of [S III] and [N II]. In addition, two arc-like structures are revealed. Moreover, an inner jet-like structure is found through its [Fe III] emission. The interaction of the jet with the rim may be related to the formation of knots and blobs. The higher value of Te, is estimated from the [S III] diagnostic lines, followed by Te ([N II]), Te(H I) and finally Te (He I). In all cases, Te is higher at the inner nebular structures. Regarding electron density, ne, is lower at the LISs, while an increase is observed at the nebular rim. Diagnostic diagrams confirm that NGC 3242 is a highly ionized nebula. Moreover, the MUSE data unveiled for the first time in this PN, the atomic line [C I] λ8727, primarily emitted from the LISs. This finding suggests that these structures may consist of a molecular core surrounded by neutral and ionized gas |
| title | Integral field spectroscopy of the planetary nebula NGC 3242 and the puzzling nature of its low ionization structures |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.16662 |