HD 203030

The NASA Exoplanet Archive has HD 203030 b, which is 437 AU from a G-type star. It's mass, within the error margins listed, could be 13 Jupiter-masses. The object is from 2006, so it's not really "new."
http://exoplanetarchive.ipac.caltech.edu./cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+203030+b&type=CONFIRMED_PLANET

Only EPE refuses to list it...

Miles-Páez et al. "The Prototypical Young L/T-Transition Dwarf HD 203030B Likely Has Planetary Mass"
https://arxiv.org/abs/1710.11274

Revised age and mass range.

Lazarus wrote:

Miles-Páez et al. "The Prototypical Young L/T-Transition Dwarf HD 203030B Likely Has Planetary Mass"
https://arxiv.org/abs/1710.11274

Revised age and mass range.

I hope this will convince EPE staff to list this long-time imaged exoplanet, along with another imaged planet with ring too, i.e. G 196-3 b.

Edasich wrote:

I hope this will convince EPE staff to list this long-time imaged exoplanet

Here it is... http://exoplanet.eu/catalog/hd_203030_b/

Lazarus wrote:

Edasich wrote:

I hope this will convince EPE staff to list this long-time imaged exoplanet

Here it is... http://exoplanet.eu/catalog/hd_203030_b/

At last! Now G 196-3 b has to come next, right?

Cloud Atlas: Variability in and out of the Water Band in the Planetary-mass HD 203030B Points to Cloud Sedimentation in Low-gravity L Dwarfs
https://arxiv.org/abs/1908.09403

Quote :

We use the Wide Field Camera 3 on the {\sl Hubble Space Telescope} to spectrophotometrically monitor the young L7.5 companion HD~203030B. Our time series reveal photometric variability at 1.27\,μm and 1.39\,μm on time scales compatible with rotation. We find a rotation period of 7.5+0.6−0.5 h: comparable to those observed in other brown dwarfs and planetary-mass companions younger than 300 Myr. We measure variability amplitudes of 1.1±0.3% (1.27\,μm) and 1.7±0.4% (1.39\,μm), and a phase lag of 56∘±28∘ between the two light curves. We attribute the difference in photometric amplitudes and phases to a patchy cloud layer that is sinking below the level where water vapor becomes opaque. HD 203030B and the few other known variable young late-L dwarfs are unlike warmer (earlier-type and/or older) L dwarfs, for which variability is much less wavelength-dependent across the 1.1--1.7μm region. We further suggest that a sinking of the top-most cloud deck below the level where water or carbon monoxide gas become opaque may also explain the often enhanced variability amplitudes of even earlier-type low-gravity L dwarfs. Because these condensate and gas opacity levels are already well-differentiated in T dwarfs, we do not expect the same variability amplitude enhancement in young vs.\ old T dwarfs.