English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/211166
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:


NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

AuthorsCazzoli, S.; Gil de Paz, A.; Márquez, Isabel ; Masegosa, Josefa ; Iglesias-Páramo, J. ; Gallego, J.; Carrasco, E.; Cedazo, R.;; García-Vargas, M. L.; Castillo-Morales, Á.; Pascual, S.; Cardiel, N.; Pérez-Calpena, A.; Gómez-Alvarez, P.; Martínez-Delgado, I.; Hermosa Muñoz, L.
KeywordsTechniques: spectroscopic
Galaxies: active
Galaxies: ISM
Galaxies: kinematics and dynamics
Issue Date2020
PublisherOxford University Press
CitationMonthly Notices of the Royal Astronomical Society 493: 3656–3675 (2020)
AbstractWe present our analysis of high-resolution (R similar to 20 000) GTC/MEGARA integral-field unit spectroscopic observations, obtained during the commissioning run, in the inner region (12.5 arcsec x 11.3 arcsec) of the active galaxy NGC7469, at spatial scales of 0.62 arcsec. We explore the kinematics, dynamics, ionization mechanisms, and oxygen abundances of the ionized gas, by modelling the H alpha-[N II] emission lines at high signal-to-noise (> 15) with multiple Gaussian components. MEGARA observations reveal, for the first time for NGC 7469, the presence of a very thin (20 pc) ionized gas disc supported by rotation (V/sigma = 4.3), embedded in a thicker (222 pc), dynamically hotter (V/sigma = 1.3) one. These discs nearly corotate with similar peak-to-peak velocities (163 versus 137 km s(-1)), but with different average velocity dispersion (38 +/- 1 versus 108 +/- 4 km s(-1)). The kinematics of both discs could be possibly perturbed by star-forming regions. We interpret the morphology and the kinematics of a third (broader) component (sigma > 250 km s(-1)) as suggestive of the presence of non-rotational turbulent motions possibly associated either to an outflow or to the lense. For the narrow component, the [N II]/H alpha ratios point to the star-formation as the dominant mechanism of ionization, being consistent with ionization from shocks in the case of the intermediate component. All components have roughly solar metallicity. In the nuclear region of NGC7469, at r <= 1.85 arcsec, a very broad (FWHM = 2590 km s(-1)) H alpha component is contributing (41 per cent) to the global H alpha-[N II] profile, being originated in the (unresolved) broad line region of the Seyfert 1.5 nucleus of NGC7469.© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Publisher version (URL)http://dx.doi.org/10.1093/mnras/staa409
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2020staa409.pdf2,75 MBAdobe PDFThumbnail
Show full item record
Review this work

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.