Outflows in the inner kiloparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFU) kinematics
| Autor: | Slater, R., Finlez, C., Nagar, N. M., Schnorr-Müller, A., Storchi-Bergmann, T., Lena, D., Ramakrishnan, V., Mundell, C. G., Riffel, R. A., Peterson, B., Robinson, A., Orellana, G. |
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| Rok vydání: | 2018 |
| Předmět: | |
| Zdroj: | A&A 621, A83 (2019) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1051/0004-6361/201730634 |
| Popis: | We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies, to quantify the nuclear inflows and outflows. Here, we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and $\sim$2.6 km s$^{-1}$ spectral resolution, and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution, and 123 km s$^{-1}$ of intrinsic spectral resolution. The morphology and kinematics of stellar, molecular (CO) and ionized ([N II]) emission lines are compared to the expectations from rotation, outflows, and streaming inflows. While both ionized and molecular gas show rotation signatures, there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc (CO). The nucleus shows a double-peaked CO profile (Full Width at Zero Intensity of 200 km s$^{-1}$), and prominent ($\sim$80 km s$^{-1}$) blue and redshifted lobes are found along the minor axis in the inner arcseconds. Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field. We thus favour the presence of a molecular outflow in the disk with true velocities of $\sim$180 km s$^{-1}$ in the nucleus and decelerating to 0 by $\sim$72 pc. The implied molecular outflow rate is $5.6~[M_{o}yr^{-1}]$, with this gas accumulating in the nuclear 2 arcsec arms. The ionized gas kinematics support an interpretation of a similar, but more spherical, outflow in the inner 100 pc, with no signs of deceleration. There is some evidence of streaming inflows of $\sim$50 km s$^{-1}$ along specific spiral arms, and the estimated molecular mass inflow rate, $\sim0.1~[M_{o}yr^{-1}]$, is significantly larger than the SMBH accretion rate ($\dot{m}=4.8\times10^{-5}~[M_{o}yr^{-1}]$). Comment: 23 pages, 16 figures, accepted for publication in A&A |
| Databáze: | arXiv |
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