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http://hdl.handle.net/20.500.12386/23933
Title: | Chemical Abundances and Properties of the Ionized Gas in NGC 1705 | Authors: | ANNIBALI, FRANCESCA TOSI, Monica Pasquali, A. Aloisi, A. MIGNOLI, Marco ROMANO, Donatella |
Issue Date: | 2015 | Journal: | THE ASTRONOMICAL JOURNAL | Number: | 150 | Issue: | 5 | First Page: | 143 | Abstract: | We obtained [O iii] narrow-band imaging and multi-slit MXU spectroscopy of the blue compact dwarf (BCD) galaxy NGC 1705 with FORS2@VLT to derive chemical abundances of planetary nebulae and H ii regions and, more in general, to characterize the properties of the ionized gas. The auroral [O iii]λ 4363 line was detected in all but 1 of the 11 analyzed regions, allowing for a direct estimate of their electron temperature. The only object for which the [O iii]λ 4363 line was not detected is a possible low-ionization PN, the only one detected in our data. For all the other regions, we derived the abundances of nitrogen, oxygen, neon, sulfur, and argon out to ̃1 kpc from the galaxy center. We detect for the first time in NGC 1705 a negative radial gradient in the oxygen metallicity of -0.24+/- 0.08 dex kpc<SUP>-1</SUP>. The element abundances are all consistent with values reported in the literature for other samples of dwarf irregular and BCD galaxies. However, the average (central) oxygen abundance, 12+{log}({{O}}/{{H}})=7.96+/- 0.04, is ̃0.26 dex lower than previous literature estimates for NGC 1705 based on the [O iii]λ 4363 line. From classical emission line diagnostic diagrams, we exclude a major contribution from shock excitation. On the other hand, the radial behavior of the emission line ratios is consistent with the progressive dilution of radiation with increasing distance from the center of NGC 1705. This suggests that the strongest starburst located within the central ̃150 pc is responsible for the ionization of the gas out to at least ̃1 kpc. The gradual dilution of the radiation with increasing distance from the center reflects the gradual and continuous transition from the highly ionized H ii regions in the proximity of the major starburst into the diffuse ionized gas. | Acknowledgments: | F.A. and this work have been supported by PRIN MIUR through grant 2010LY5N2T_006. D.R. and M.T. have also been supported by the same grant. We acknowledge support from the ESO telescope operator I. Condor. Based on observations made with the ESO Telescopes at the La Silla Paranal Observatory under programme ID 084.D-0248 and 086.D-0761. We thank the anonymous referee for useful comments, which helped to improve our paper. | URI: | http://hdl.handle.net/20.500.12386/23933 | URL: | https://iopscience.iop.org/article/10.1088/0004-6256/150/5/143 https://arxiv.org/pdf/1505.05545 |
ISSN: | 0004-6256 | DOI: | 10.1088/0004-6256/150/5/143 | Bibcode ADS: | 2015AJ....150..143A | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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Annibali_2015_AJ_150_143.pdf | pdf editoriale | 2.18 MB | Adobe PDF | View/Open |
1505.05545.pdf | preprint | 986.18 kB | Adobe PDF | View/Open |
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