Table 1.
Results from the fitting of the spectrum extracted from a circular aperture of radius 0.15″ centered on the spatial peak of the emission.
| Measurement | [km s−1] |
|---|---|
| FWHM Hαhost galaxy | 519 ± 58 |
| FWHM Hαoutflow | 1491 ± 206 |
| FWHM HαBLR | 9008 ± 407 |
| FWHM [O III] λ5007 Å | 553 ± 105 |
| Δv Hαhost galaxy, outflow | −441 ± 129 |
| Δv Hαhost galaxy, BLR | 427 ± 201 |
| Measurement | [erg s−1 cm−2]×10−20 |
| F Hαhost galaxy | 174 ± 34 |
| F Hαoutflow | 123 ± 91 |
| F HαBLR | 2804 ± 198 |
| F [N II] λ6584 Åhost galaxy | 252 ± 44 |
| F [N II] λ6584 Åoutflow | 460 ± 150 |
| F [N II] λ6548 Åhost galaxy | 83 ± 14 |
| F [N II] λ6548 Åoutflow | 151 ± 49 |
| F [O III] λ5007 Å | 291 ± 73 |
| F Hβ | < 83 |
Notes. On top: FWHM of the detected lines and velocity shift between the systemic velocity identified by the narrow component of the Hα relative to the host and the centroid of the outflow (broader component) and BLR Δv Hαhost galaxy, outflow = v Hαhost galaxy − v Hαoutflow. On the bottom: fluxes of the detected lines.
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