Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Molecular observations of four planetary nebulae (PNe), M4-17, Hu 1-1, M1-59, and Na 2, were conducted at 1–3 mm using the Arizona Radio Observatory’s 12 m antenna and Submillimeter Telescope, and the Institut de Radioastronomie Millimétrique 30 m Telescope. Toward M4-17, HNC ( J = 3 → 2), CCH ( N =...
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| author | K. R. Gold D. R. Schmidt L. M. Ziurys |
| author_facet | K. R. Gold D. R. Schmidt L. M. Ziurys |
| author_sort | K. R. Gold |
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| description | Molecular observations of four planetary nebulae (PNe), M4-17, Hu 1-1, M1-59, and Na 2, were conducted at 1–3 mm using the Arizona Radio Observatory’s 12 m antenna and Submillimeter Telescope, and the Institut de Radioastronomie Millimétrique 30 m Telescope. Toward M4-17, HNC ( J = 3 → 2), CCH ( N = 2 → 1, N = 3 → 2), CN ( N = 1 → 0, N = 2 → 1), H _2 CO ( J _Ka,Kc = 2 _1,2 → 1 _1,1 , J _Ka,Kc = 2 _0,2 → 1 _0,1 , J _Ka,Kc = 2 _1,1 → 1 _1,0 ), CS ( J = 3 → 2, J = 5 → 4), and H ^13 CN ( J = 2 → 1) were detected. An almost identical set of transitions was identified toward Hu 1-1. Moreover, c–C _3 H _2 was detected in Hu 1-1 via three 2 mm lines: J _Ka,Kc = 3 _1,2 → 2 _2,1 , J _Ka,Kc = 4 _1,4 → 3 _0,3 , and J _Ka,Kc = 3 _2, 2 → 2 _1,1 . HNC, CCH, CN, CS, and H ^13 CN were found in M1-59, as well as H _2 S via its J _Ka,Kc = 1 _1,0 → 1 _0,1 line—the first detection of this key sulfur species in PNe. In addition, CCH and CN were identified in the 27,000 yr old Na 2. Among these four sources, CN and CCH were the most prevalent molecules (after CO and H _2 ) with fractional abundances, relative to H _2 , of f ∼ 0.9–7.5 × 10 ^−7 and 0.8–7.5 × 10 ^−7 , respectively. CS and HNC have abundances in the range f ∼ 0.5–5 × 10 ^−8 , the latter resulting in HCN/HNC ∼ 3 across all three PNe. The unusual species H _2 CO, c–C _3 H _2 , and H _2 S had f ∼ 3–4 × 10 ^−7 , 10 ^−8 , and 6 × 10 ^−8 . This study suggests that elliptical PNe such as Hu 1-1 can have a diverse molecular composition. The presence of CN, CCH, and HCO ^+ in Na 2, with comparable abundances to younger PNe, demonstrates that molecular content is maintained into the late PN stage. |
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| spelling | doaj-art-c0debb2e1ae440cea99ceb4cb5d005552024-11-22T08:23:17ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01976219610.3847/1538-4357/ad83beExpanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2K. R. Gold0https://orcid.org/0000-0002-6830-6239D. R. Schmidt1https://orcid.org/0000-0001-7519-6819L. M. Ziurys2https://orcid.org/0000-0002-1805-3886Department of Chemistry and Biochemistry, University of Arizona , PO Box 210041, Tucson, AZ 85721-0041, USA ; lziurys@arizona.eduDepartment of Physics and Astronomy, Franklin & Marshall College , PO Box 3003, Lancaster, PA 17604-3003, USADepartment of Chemistry and Biochemistry, University of Arizona , PO Box 210041, Tucson, AZ 85721-0041, USA ; lziurys@arizona.edu; Department of Astronomy, Arizona Radio Observatory, and Steward Observatory, University of Arizona , 933 N. Cherry Avenue, Tucson, AZ 85721-0065, USAMolecular observations of four planetary nebulae (PNe), M4-17, Hu 1-1, M1-59, and Na 2, were conducted at 1–3 mm using the Arizona Radio Observatory’s 12 m antenna and Submillimeter Telescope, and the Institut de Radioastronomie Millimétrique 30 m Telescope. Toward M4-17, HNC ( J = 3 → 2), CCH ( N = 2 → 1, N = 3 → 2), CN ( N = 1 → 0, N = 2 → 1), H _2 CO ( J _Ka,Kc = 2 _1,2 → 1 _1,1 , J _Ka,Kc = 2 _0,2 → 1 _0,1 , J _Ka,Kc = 2 _1,1 → 1 _1,0 ), CS ( J = 3 → 2, J = 5 → 4), and H ^13 CN ( J = 2 → 1) were detected. An almost identical set of transitions was identified toward Hu 1-1. Moreover, c–C _3 H _2 was detected in Hu 1-1 via three 2 mm lines: J _Ka,Kc = 3 _1,2 → 2 _2,1 , J _Ka,Kc = 4 _1,4 → 3 _0,3 , and J _Ka,Kc = 3 _2, 2 → 2 _1,1 . HNC, CCH, CN, CS, and H ^13 CN were found in M1-59, as well as H _2 S via its J _Ka,Kc = 1 _1,0 → 1 _0,1 line—the first detection of this key sulfur species in PNe. In addition, CCH and CN were identified in the 27,000 yr old Na 2. Among these four sources, CN and CCH were the most prevalent molecules (after CO and H _2 ) with fractional abundances, relative to H _2 , of f ∼ 0.9–7.5 × 10 ^−7 and 0.8–7.5 × 10 ^−7 , respectively. CS and HNC have abundances in the range f ∼ 0.5–5 × 10 ^−8 , the latter resulting in HCN/HNC ∼ 3 across all three PNe. The unusual species H _2 CO, c–C _3 H _2 , and H _2 S had f ∼ 3–4 × 10 ^−7 , 10 ^−8 , and 6 × 10 ^−8 . This study suggests that elliptical PNe such as Hu 1-1 can have a diverse molecular composition. The presence of CN, CCH, and HCO ^+ in Na 2, with comparable abundances to younger PNe, demonstrates that molecular content is maintained into the late PN stage.https://doi.org/10.3847/1538-4357/ad83beAstrochemistryInterstellar moleculesPlanetary nebulaeRadio astronomyMolecular spectroscopy |
| spellingShingle | K. R. Gold D. R. Schmidt L. M. Ziurys Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 The Astrophysical Journal Astrochemistry Interstellar molecules Planetary nebulae Radio astronomy Molecular spectroscopy |
| title | Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 |
| title_full | Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 |
| title_fullStr | Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 |
| title_full_unstemmed | Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 |
| title_short | Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2 |
| title_sort | expanding the inventory of molecule rich planetary nebulae new observations of m4 17 hu 1 1 m1 59 and na 2 |
| topic | Astrochemistry Interstellar molecules Planetary nebulae Radio astronomy Molecular spectroscopy |
| url | https://doi.org/10.3847/1538-4357/ad83be |
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