Table A.1.
Set-up of the FP observations.
| Parameter | OAN-SPM | OHP | ||
|---|---|---|---|---|
| Telescope | 2.1 m | 1.93 m | ||
| Instrument | PUMA(1) | GHASP | ||
| Seeing | 2.9 arcsec | 2.5 - 4.5 arcsec | ||
| Galaxy Hα wavelength range | 6593 - 6600 Å | |||
| velocity range | 1380 - 1672 km s−1 | |||
| Observation date | 2017-02-23 | 2021-01-14 to 18 | 2021-01-16 to 18 | |
| 2021-02-11 | ||||
| Number of cycles | 1 | 80 | 37 | |
| Total exposure time | 96 min | 427 min | 200 min | |
| Scanning FP interferometer | ICOS - ET-50(2) | |||
| Calibration (Neon line) | 6598.95 Å | |||
| Finesse (F) | 19.9 | 12.3±0.3(3) | ||
p(4) at H = 6562.8 (Hα(5) = 6596.8Å) |
330 (328) | 793 (789) | ||
| Resolution power (pF) at Hα(5) | 6533 | 9704±25 | ||
| Free spectral range at Hα(5) | 20.05 Å / 911 km s−1 | 8.35 Å / 379 km s−1 | ||
| Spectral resolution at Hα(5) | 1.01 Å / 45.8 km s−1 | 0.68 Å / 30.9 km s−1 | ||
| Spectral sampling at Hα(5) | 0.42 Å / 19.0 km s−1 | 0.26 Å / 11.9 km s−1 | ||
| Line spread function (σLSF) | 0.43 Å / 19.5 km s−1 | 0.29 Å / 13.1 km s−1 | ||
| Scanning steps | 48 | 32 | ||
| Exposure time per channel | 120 s | 10 s | ||
| Detector Name | Spectral 2 (6) | IPCS (GaAs) | ||
| Detector size | 512 × 512 pixels2 | 512 × 512 pixels2 | ||
| Field-of-view | 10 × 10 arcmin2 | 5.8 × 5.8 arcmin2 | ||
| Image scale | 1.27(7) arcsec pix−1 | 0.68(8) arcsec pix−1 | ||
Notes. (1) https://www.astrossp.unam.mx/instrumentos/interferometria/puma/docs/manualespuma/puma.html. (2)Queensgate Instruments, which is now called IC Optical Systems. (3) Mean and standard deviation of the finesse (F) measured from eight different calibration cubes. (4) p is the interference order. (5) Hα0 is the wavelength of the Hα-line at rest, and Hα the wavelength at the galaxy heliocentric LoS velocity (see Table 1). (6) https://www.astrossp.unam.mx/en/users/ccd-s. (7) After 4 ×4 electronic binning on the CCD. (8) After 2 ×2 electronic binning on the IPCS.
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