The circumnuclear environment of the peculiar galaxy NGC3310
Gas and star velocity dispersions have been derived for eight circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC3310 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca triplet in the near-IR, using...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2010 |
| País: | México |
| Institución: | Instituto Nacional de Astrofísica, Óptica y Electrónica |
| Repositorio: | Repositorio Institucional del INAOE |
| Idioma: | inglés |
| OAI Identifier: | oai:inaoe.repositorioinstitucional.mx:1009/1382 |
| Acceso en línea: | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1382 |
| Access Level: | acceso abierto |
| Palabra clave: | info:eu-repo/classification/Inspec/H regions info:eu-repo/classification/Inspec/Galaxies: individual: NGC3310 info:eu-repo/classification/Inspec/Galaxies: kinematics and dynamics info:eu-repo/classification/Inspec/Galaxies: starburst info:eu-repo/classification/Inspec/Galaxies: star clusters info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 |
| Sumario: | Gas and star velocity dispersions have been derived for eight circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC3310 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca triplet in the near-IR, using cross-correlation techniques, while gas velocity dispersions have been measured by Gaussian fits to the Hβ λ4861Å and [O ] λ5007Å emission lines. The CNSFR stellar velocity dispersions range from 31 to 73 km s⁻¹. These values, together with the sizes measured on archival Hubble Space Telescope images, yield upper limits to the dynamical masses for the individual star clusters between 1.8 and 7.1 × 10⁶M⊙, for the whole CNSFR between 2 × 10⁷ and 1.4 × 10⁸M⊙, and 5.3 × 10⁷M⊙, for the nucleus inside the inner 14.2 pc. The masses of the ionizing stellar population responsible for the H región gaseous emission have been derived from their published Hα luminosities and are found to be between 8.7 × 10⁵ and 2.1 × 10⁶M⊙ for the star-forming regions and 2.1 × 10⁵M⊙ for the galaxy nucleus; they therefore constitute between 1 and 7 per cent of the total dynamical mass. The ionized gas kinematics is complex; two different kinematical components seem to be present as evidenced by different linewidths and Doppler shifts. |
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