TESS News and Results

There is 18.8 jupiter mass planet/brown dwarf around TOI1136 ?.How inner planets avoided disruptions / perturbation and still transit the host star?
https://exoplanet.eu/catalog/toi_1136_h--8881/

tommi59 wrote:

There is  18.8 jupiter mass planet/brown dwarf around TOI1136 ?.How  inner planets avoided disruptions / perturbation and still transit the host star?
https://exoplanet.eu/catalog/toi_1136_h--8881/

Mysteries of the Universe... (awaiting to be solved).
Actually the seventh planet candidate’s parameters are loosely constrained, but the mass estimate is not in Jupiter rather Earth masses and likely less than 18.8. EPE is collecting a little too much typos lately.

Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815
https://arxiv.org/abs/2401.15709

But have we missed this piece of news from TESS? 85 candidate planets within the HZ (so mainstream media too say).

TESS Duotransit Candidates from the Southern Ecliptic Hemisphere
https://warwick.ac.uk/fac/sci/physics/research/astro/people/faithhawthorne/duotransit_candidates.pdf

815 c seems to be extralarge super earth    It  is surprising discovery I did not not expect that

I wouldn't be surprised if there are additional (non-transiting) planets in the system contributing to the RV behaviour of the star that hasn't been modelled out. Additional planets are more common than high-density sub-Neptunes.

Yes you are right but sometime we can find them .HD 88986 and
HD 207897 b for example

Edasich wrote:

A 1.55 R⊕ habitable-zone planet hosted by TOI-715, an M4 star near the ecliptic South Pole
https://arxiv.org/abs/2305.06206

Now in Monthly Notices of the Royal Astronomical Society, Volume 527, Issue 1, January 2024, Pages 35–52,

https://doi.org/10.1093/mnras/stad1439

I am really curious what is the mass of the TOI715 b as both kepler 138 c,d and l 98-59 d are water worlds K2-3 d follows this trend

TESS discovery "mega-pack"!

The TESS-Keck Survey. XII. A Dense 1.8 R⊕ Ultra-Short-Period Planet Possibly Clinging to a High-Mean-Molecular-Weight Atmosphere After the First Gyr
https://arxiv.org/abs/2402.07451

The TESS-Keck Survey. XVIII. A sub-Neptune and spurious long-period signal in the TOI-1751 system
https://arxiv.org/abs/2402.07110

The TESS-Keck Survey XXI: 13 New Planets and Homogeneous Properties for 21 Subgiant Systems
https://arxiv.org/abs/2402.07893

The PFS view of TOI-677 b: A spin-orbit aligned warm Jupiter in a dynamically hot system
https://arxiv.org/abs/2402.07346

TOI-1199b and TOI-1273b: Two new transiting hot Saturns detected and characterized with SOPHIE and TESS
https://arxiv.org/abs/2402.07861

https://exoplanetarchive.ipac.caltech.edu/overview/HD%20110067
Possible 2 more planets in that system ? Why RV did not detect it

The occurrence of small, short-period planets younger than 200 Myr with TESS

Quote :

Within the first few hundreds of millions of years, many physical processes sculpt the eventual properties of young planets. NASA's TESS mission has surveyed young stellar associations across the entire sky for transiting planets providing glimpses into the various stages of planetary evolution. Using our own detection pipeline, we search a magnitude-limited sample of 7219 young stars (≤200 Myr) observed in the first four years of TESS for small (2-8 R⊕), short period (1.6-20 days) transiting planets. The completeness of our survey is characterized by a series of injection and recovery simulations. Our analysis of TESS 2-minute cadence and Full Frame Image (FFI) light curves recover all known TOIs, as well as four new planet candidates not previously identified as TOIs. We derive an occurrence rate of 35+13−10% for mini-Neptunes and 27+10−8% for super-Neptunes from the 2-minute cadence data, and 22+8.6−6.8% for mini-Neptunes and 13+3.9−4.9% for super-Neptunes from FFI data. To independently validate our results, we compare our survey yield with the predicted planet yield assuming Kepler planet statistics. We consistently find a mild increase in the occurrence of super-Neptunes and a significant increase in the occurrence of Neptune-sized planets with orbital periods of 6.2-12 days when compared to their mature counterparts. The young planet distribution from our study is most consistent with evolution models describing the early contraction of hydrogen-dominated atmospheres undergoing atmospheric escape and inconsistent with heavier atmosphere models offering only mild radial contraction early on.

Confronting compositional confusion through the characterisation of the sub-Neptune orbiting HD 77946
https://arxiv.org/abs/2403.04464

Also known as TOI-1778.01.