Carmenes搜索M矮人周围的系外行星-LP 714-47B（TOI 442.01）：填充海王星沙漠

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Carmenes搜索M矮人周围的系外行星-LP 714-47B（TOI 442.01）：填充海王星沙漠

The CARMENES search for exoplanets around M dwarfs -- LP 714-47b (TOI 442.01): Populating the Neptune desert

论文作者

Dreizler, S., I., J., Crossfield, M., Kossakowski, D., Plavchan, P., S., Jeffers, V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., J., Caballero, A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., M., Osorio, R. Zapatero, Chaturvedi, P., A., Hatzes, P., Ricker, G., Vanderspek, R., D., Latham, W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., P., Amado, J., Barkaoui, K., Barbieri, M., N., Batalha, M., F., Bauer, F., Benneke, B., Benkhaldoun, Z., C, Beichman, Berberian, J., Burt, J., R., Butler, P., D., Caldwell, A., Chintada, A., Chontos, A., J., Christiansen, L., Ciardi, D. R., Cifuentes, C., K., Collins, A., K., Collins, I., Combs, D., Cortés-Contreras, M., J., Crane, D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., E., Flowers, E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., A., Howard, W., Howell, S., Huber, D., Isaacson, H., Jehin, E., E., L., Jensen, N., Kaminski, A., S., Kane, R., Kawauchi, K., J., Kielkopf, F., Klahr, H., M., Kosiarek, R., Kreidberg, L., M., Kürster, Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., R., Matson, A., Mocnik, T., J., Morales, C., P., Muirhead, S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., V., Passegger, M., Pollacco, D., F., Pozuelos, J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., M., Rose, E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., H., Şenavcı, V., Teske, J., J., Twicken, D., Villasenor, J., Wang, S. X., L., Weiss, M., Wittrock, J., Yılmaz, M., Zohrabi, F.

论文摘要

我们报告了一个类似海王星的行星（LP 714-47 b，p = 4.05204 d，m_b = 30.8 +/- 1.5 m_earth，r_b = 4.7 +/- 0.3 +/- 0.3 r_earth），位于'Hot Neptune desert'中。使用卡门，意式浓缩咖啡，雇员，Ishell和PFS以及使用Tess，Spitzer和地面的光度计，通过使用Carmenes，浓缩咖啡，雇员，Ishell和PFS来确认感兴趣的对象（TOI 442.01），并通过radial速进行跟进，并从光度计数据中获得了光度计数据。网络，El Sauce望远镜，Tubitak国家天文台，路易斯维尔大学的望远镜和黄蜂 - 南。我们还使用双子座近红外成像仪提出了高空间分辨率自适应光学成像。质量和半径确定的低不确定性位置LP 714-47 b在物理良好的行星中，可以与行星结构模型进行有意义的比较。宿主星LP 714-47是一种缓慢旋转的早期M矮人（T_eff = 3950 +/- 51 K），质量为0.59 +/- 0.02 m_sun，半径为0.58 +/- 0.02 r_sun。根据长期的光度监测和光谱活性指标，我们确定了大约33 d的恒星旋转周期。恒星活性也表现为径向速度数据中的相关噪声。在径向速度数据的功率谱中，除了行星的四天信号外，我们还检测出第二个信号，其周期为16天。这可以证明是恒星旋转期或第二行星信号的谐波。一旦获得更多苔丝数据和径向速度数据，就可以分辨出差异。

We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, m_b = 30.8 +/- 1.5 M_earth , R_b = 4.7 +/- 0.3 R_earth ) located in the 'hot Neptune desert'. Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST- South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TUBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (T_eff = 3950 +/- 51 K) with a mass of 0.59 +/- 0.02 M_sun and a radius of 0.58 +/- 0.02 R_sun. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained.

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