A nuclear ionized gas outflow in the Seyfert 2 galaxy UGC 2024
| العنوان: | A nuclear ionized gas outflow in the Seyfert 2 galaxy UGC 2024 |
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| المؤلفون: | D. Lena, Neil M. Nagar, Travis Fischer, Allan Schnorr-Müller, C. Finlez, D. Michael Crenshaw, Pamela Soto-Pinto, Venkatessh Ramakrishnan, V. Firpo, Rogemar A. Riffel, Martin Elvis, Thaisa Storchi-Bergmann, Dania Muñoz-Vergara, Henrique R. Schmitt, R. Slater, Pedro K. Humire, Andrew Robinson, Steven B. Kraemer |
| المصدر: | Monthly Notices of the Royal Astronomical Society, 487, 3679-3692 Monthly Notices of the Royal Astronomical Society, 487, 3, pp. 3679-3692 |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Plasma, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Outflow, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics |
| الوصف: | As part of a high-resolution observational study of feeding and feedback processes occurring in the vicinity of the active galactic nucleus in 40 galaxies, we observed the inner 3${^{\prime\prime}_{.}}$5 × 5 arcsec of the nearby spiral and Seyfert 2 galaxy UGC 2024 with the integral field unit of the Gemini-South Telescope. The observations enabled a study of the stellar and gas kinematics in this region at a spatial resolution of 0${^{\prime\prime}_{.}}$5 (218 pc), and a spectral resolution of 36 km s−1 over the wavelength range 4100–7300 Å. For the strongest emission-lines (H β, [$\rm{O\,{\small III}}$] λ5007 Å, H α, [$\rm{N\,{\small II}}$] λ6584 Å, and [$\rm{S\,{\small II}}$] λλ6717,6731 Å) we derived maps of the flux, radial velocity, and velocity dispersion. The flux distribution and kinematics of the [$\rm{O\,{\small III}}$] emission line are roughly symmetric around the nucleus: the radial velocity is close to systemic over the full field of view. The kinematics of the other strong emission lines trace both this systemic velocity component, and ordered rotation (with kinematic centre 0${^{\prime\prime}_{.}}$2 north-west of the nucleus). The stellar continuum morphology and kinematics are, however, asymmetrical around the nucleus. We interpret these unusual kinematics as the superposition of a component of gas rotating in the galaxy disc plus a ‘halo’ component of highly ionized gas. This halo either traces a quasi-spherical fountain with average radial velocity 200 km s−1, in which case the total nuclear outflow mass and momentum are 2 × 105 M⊙ and 4 × 107 M⊙ km s−1, respectively, or a dispersion supported halo created by a past nuclear starburst. |
| وصف الملف: | application/pdf |
| تدمد: | 0035-8711 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::27b51cab68f2b574a8f92a8857c5cebb https://doi.org/10.1093/mnras/stz1572 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....27b51cab68f2b574a8f92a8857c5cebb |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 00358711 |
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