论文标题
揭示轨道toi-2076的年轻子纽扣的真实时期
Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076
论文作者
论文摘要
上下文：TOI-2076是一个旋转明亮（G = 8.9 mag），Young（$ 340 \ pm80 $ Myr）K-Type Star的子脉中的三个型号系统。尽管经过验证的行星系统，但两个外行星的轨道没有受限，因为在苔丝光度法中只看到了两个非连续的转移。这留下了11和7可能的时期别名。 目的：为了揭示这两个长期行星的真实轨道，需要针对最高概率时期别名的精确光度法。对多行星系统中的转运的长期监测也可以通过TTV测量来帮助限制行星质量。 方法：我们使用Monotools软件包来确定要遵循哪些别名，然后使用Cheops，Saint-EX和LCO望远镜进行TOI-2076 C和D的空间和地面光度随访。 结果：Cheops的观察结果显示，$ p = 21.01538^{+0.00084} _ { - 0.00074} $ d的TOI-2076 c清晰检测，并允许我们排除三个最有可能的TOI-2076 d的时期别名。地面光度法进一步使我们能够排除剩余的别名并确认$ p = 35.12537 \ pm0.00067 $ d别名。这些观察结果还提高了所有三个子纽扣的半径精度至$ 2.518 \ pm0.036 $，$ 3.497 \ pm0.043 $和$ 3.232 \ pm0.063 $ $ $ $ $ r_ \ oplus $。我们的观察结果还揭示了行星B和C之间的明显抗相关TTV信号可能是由于其靠近2：1共振引起的，而行星C和D行星C和D则接近5：3个周期的交配性，尽管模型退化性意味着我们无法检索强大的TTV质量。它们膨胀的半径可能是由于HE大气的扩展，结合了较低的日光度，使所有三个行星都使所有三个行星都出色，可与JWST进行比较的传播光谱。
Context: TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young ($340\pm80$ Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims: To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods: We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results: CHEOPS observations revealed a clear detection for TOI-2076 c at $P=21.01538^{+0.00084}_{-0.00074}$ d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the $P=35.12537\pm0.00067$ d alias. These observations also improved the radius precision of all three sub-Neptunes to $2.518\pm0.036$, $3.497\pm0.043$, and $3.232\pm0.063$ $R_\oplus$. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.
