A 20 kiloparsec bipolar Lyman $α$ outflow from a radio galaxy at z=2.95
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| Format: | Preprint |
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2024
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| _version_ | 1866929345492156416 |
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| author | Puga, Miguel Coloma Balmaverde, Barbara Capetti, Alessandro Almeida, Cristina Ramos Massaro, Francesco Venturi, Giacomo |
| author_facet | Puga, Miguel Coloma Balmaverde, Barbara Capetti, Alessandro Almeida, Cristina Ramos Massaro, Francesco Venturi, Giacomo |
| contents | The study of ionized gas kinematics in high-z active galaxies plays a key part in our understanding of galactic evolution, in an age where nuclear activity was widespread and star formation close to its peak. We present a study of TXS 0952-217, a radio galaxy at z=2.95, using VLT/MUSE integral field optical spectroscopy as part of a project aimed studying of the properties of ionized gas in high redshift radio galaxies (HzRGs). The Lyman $α$ line profile of this object presents various emission and absorption components. By utilizing Voronoi binning, we obtained a comprehensive map of the kinematic properties of these components. These observations revealed the presence of a redshifted, high velocity (v $\sim 500$ km s$^-1$) bipolar structure of Lyman $α$ emission, most likely corresponding to an outflow of ionized gas. The outflow extends beyond the compact radio source on both sides, with a total size of $\sim$ 21 kpc. Its kinetic power ($10^{42.1}$ erg s$^{-1}$) is about five orders of magnitude smaller than its radio power. Additional ionized lines, including HeII$λ$1640, CIV$λ$1550 and CIII]$λ$1908 were detected and their line flux ratios determined. The presence of HeII allowed for a precise redshift measurement (z=2.945$\pm$0.002). Along with the recent discovery of a similar structure in TN J1049-1258, another HzRG, it displays the feasibility of using Lyman $α$ as a tracer of outflowing gas in high redshift sources, and particularly so when supported by non-resonant ionized lines such as HeII, which allow for accurate redshift and velocity measurements. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2405_09884 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A 20 kiloparsec bipolar Lyman $α$ outflow from a radio galaxy at z=2.95 Puga, Miguel Coloma Balmaverde, Barbara Capetti, Alessandro Almeida, Cristina Ramos Massaro, Francesco Venturi, Giacomo Astrophysics of Galaxies The study of ionized gas kinematics in high-z active galaxies plays a key part in our understanding of galactic evolution, in an age where nuclear activity was widespread and star formation close to its peak. We present a study of TXS 0952-217, a radio galaxy at z=2.95, using VLT/MUSE integral field optical spectroscopy as part of a project aimed studying of the properties of ionized gas in high redshift radio galaxies (HzRGs). The Lyman $α$ line profile of this object presents various emission and absorption components. By utilizing Voronoi binning, we obtained a comprehensive map of the kinematic properties of these components. These observations revealed the presence of a redshifted, high velocity (v $\sim 500$ km s$^-1$) bipolar structure of Lyman $α$ emission, most likely corresponding to an outflow of ionized gas. The outflow extends beyond the compact radio source on both sides, with a total size of $\sim$ 21 kpc. Its kinetic power ($10^{42.1}$ erg s$^{-1}$) is about five orders of magnitude smaller than its radio power. Additional ionized lines, including HeII$λ$1640, CIV$λ$1550 and CIII]$λ$1908 were detected and their line flux ratios determined. The presence of HeII allowed for a precise redshift measurement (z=2.945$\pm$0.002). Along with the recent discovery of a similar structure in TN J1049-1258, another HzRG, it displays the feasibility of using Lyman $α$ as a tracer of outflowing gas in high redshift sources, and particularly so when supported by non-resonant ionized lines such as HeII, which allow for accurate redshift and velocity measurements. |
| title | A 20 kiloparsec bipolar Lyman $α$ outflow from a radio galaxy at z=2.95 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.09884 |