Table 1
Optical and IR photometry, and fluxes of the main IR emission lines and spectral features measured for the nucleus of IC 3639.
| Instrument/filter | λ (μm ) | Δλ (μm) | Flux (mJy) | Aperture |
|---|---|---|---|---|
| FOC/F210M | 0.22 | 0.04 | (17 ± 2) × 10−3 | 0.′′14 |
| WFPC2/F606W | 0.60 | 0.15 | 0.22 ± 0.02 | 0.′′14 |
| ISAAC/L band | 3.78 | 0.58 | 18.9 ± 0.2 | 0.′′50 |
| ISAAC/M band | 4.66 | 0.10 | 32 ± 1 | 0.′′50 |
| T-ReCS/N band | 10.36 | 2.64 | 305 ± 9a | 0.′′40 |
| VISIR/PAH2 | 11.25 | 0.59 | 326 ± 17b | 0.′′40 |
| VISIR/NEII | 12.81 | 0.10 | 532 ± 30 | 0.′′50 |
| VISIR/NEII_2 | 13.04 | 0.22 | 543 ± 29b | 0.′′40 |
| MIDI/N band (UT2–UT3) | 10.5 | 2.5 | 84 ± 17c | 0.′′52 |
| MIDI/N band (UT1–UT2) | 10.5 | 2.5 | 95 ± 21c | 0.′′52 |
| MIDI/N band (UT3–UT4) | 10.5 | 2.5 | 90 ± 17c | 0.′′52 |
| Instrument | Line | Flux ( × 10−17 W m−2) | Slit width | |
|---|---|---|---|---|
| ESO-MPG2.2 m/EFOSC2 | [O III] |
20.3 ± 0.2d | ~1″ | |
| ESO-MPG2.2 m/EFOSC2 | [O III] |
185.7 ± 1.8d | ~1″ | |
| Spitzer/IRS | PAH11.3 μm | 111e | 4.′′7 × 11.′′3 | |
| Spitzer/IRS | [Ne II]12.8 μm | 45.2 ± 0.5e | 4.′′7 × 11.′′3 | |
| Spitzer/IRS | [Ne V]14.3 μm | 11.2 ± 0.6e | 4.′′7 × 11.′′3 | |
| Spitzer/IRS | [Ne III]15.6 μm | 27.0 ± 0.4e | 4.′′7 × 11.′′3 | |
| Spitzer/IRS | [O Iv]25.9 μm | 21.2 ± 0.6e | 11.′′1 × 22.′′3 | |
| Herschel/PACS | [O III]88 μm | 41.9 ± 1.7f | 28.′′2 × 28.′′2 | |
| VISIR | [S Iv]10.5 μm | 7.1 ± 1.6 | 0.′′52 | |
| VISIR | PAH11.3 μm | 41.4 ± 0.4 | 0.′′52 | |
| VISIR | [Ne II]12.8 μm | 33.4 ± 1.0 | 0.′′52 |
Notes. Optical photometric fluxes have been corrected for Galactic extinction (E(B − V ) = 0.06 mag; Schlafly & Finkbeiner 2011; Cardelli et al. 1989). In the subsequent analysis, data were also corrected for redshift. (a) PSF photometry from Asmus et al. (2014). (b) Photometry from Gandhi et al. (2009). (c) Correlated flux in the UT2–UT3 (46 m), UT1–UT2 (56.5 m), and UT3–UT4 (57.8 m) baselines. (d) Line fluxes from Temporin et al. (2003), including both observed and corrected fluxes from the measured Balmer decrement of 6.1, assuming an intrinsic decrement of 3.0 (Bassani et al. 1999). (e) Line fluxes from Tommasin et al. (2008). (f) Line flux from Fernández-Ontiveros et al. (2016).
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