Table 1.
Physical properties of our four new targets and the three targets that were already observed by GRAVITY.
| Object | RA | Dec | z | log λLλ (5100 Å) | Ref. | σ* | Ref. | DA |
|---|---|---|---|---|---|---|---|---|
| (J2000) | (J2000) | (erg s−1) | (km s−1) | (Mpc) | ||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| Mrk 509 | 20:44:09.738 | −10:43:24.54 | 0.0344 | 44.19 | 1 | 182 | 8 | 144 |
| PDS 456 | 17:28:19.796 | −14:15:55.87 | 0.185 | 46.30 | 2 | 182(1) | This work | 657 |
| Mrk 1239 | 09:52:19.102 | −01:36:43.46 | 0.020 | 44.40(2) | 3 | ∼250(3) | 9 | 86 |
| IC 4329A | 13:49:19.266 | −30:18:33.97 | 0.016 | 43.51 | 4 | ∼225 | 9 | 69 |
| 3C 273 | 12:29:06.700 | +02:03:08.60 | 0.158 | 45.90 | 1 | 210 | 10 | 582 |
| NGC 3783 | 11:39:01.762 | −37:44:19.21 | 0.0097 | 43.02 | 6 | 95 | 11 | 42 |
| IRAS 09149-6206 | 09:16:09.39 | −62:19:29.90 | 0.0573 | 44.92d | 5,7 | 250(4) | 7 | 236 |
Notes. Column (1): Object name. Column (2): Right ascension. Column (3): Declination. Column (4): Redshift from NASA/IPAC Extragalactic Database (NED). Column (5): AGN optical luminosity at 5100 Å. Column (6): References for λLλ (5100 Å). Column (7): Stellar velocity dispersion. Column (8): References for σ*. Column (9): Angular diameter distance.
References. (1) Du & Wang (2019), (2) Nardini et al. (2015), (3) Pan et al. (2021), (4) Bentz et al. (2023), (5) Koss et al. (2017), (6) Bentz et al. (2021a), (7) GRAVITY Collaboration (2020a), (8) Grier et al. (2013), (9) Oliva et al. (1999), (10) Husemann et al. (2019), (11) Onken et al. (2004). (1)The stellar velocity dispersion of PDS 456 is estimated in this work by using the measured dynamical mass of PDS 456 by Bischetti et al. (2019) and virial theorem. (2)Although Pan et al. (2021) measures the extinction-corrected optical luminosity of Mrk 1239, caution is still needed as Mrk 1239 is widely known to show high polarisation and high extinction. (3)The stellar velocity dispersion of Mrk 1239 is highly uncertain due to the shallowness of its stellar features (Onken et al. 2004). (4)The dispersion of IRAS 09149-6206 is based on the [OIII] line and is very uncertain (GRAVITY Collaboration 2020a).
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