Diving beneath the sea of stellar activity: chromatic radial velocities of the young AU mic planetary system
We present updated radial-velocity (RV) analyses of the AU Mic system. AU Mic is a young (22 Myr) early-M dwarf known to host two transiting planets—P b ∼ 8.46 days, , P c ∼ 18.86 days, . With visible RVs from Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and opti...
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2021 December 7
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| In: |
The astronomical journal
Year: 2021, Jahrgang: 162, Heft: 6, Pages: 1-32 |
| ISSN: | 1538-3881 |
| DOI: | 10.3847/1538-3881/ac2c80 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.3847/1538-3881/ac2c80
|
| Verfasserangaben: | Bryson L. Cale, Michael Reefe, Peter Plavchan, Angelle Tanner, Eric Gaidos, Jonathan Gagné, Peter Gao, Stephen R. Kane, Víctor J.S. Béjar, Nicolas Lodieu, Guillem Anglada-Escudé, Ignasi Ribas, Enric Pallé, Andreas Quirrenbach, Pedro J. Amado, Ansgar Reiners, José A. Caballero, María Rosa Zapatero Osorio, Stefan Dreizler, Andrew W. Howard, Benjamin J. Fulton, Sharon Xuesong Wang, Kevin I. Collins, Mohammed El Mufti, Justin Wittrock, Emily A. Gilbert, Thomas Barclay, Baptiste Klein, Eder Martioli, Robert Wittenmyer, Duncan Wright, Brett Addison, Teruyuki Hirano, Motohide Tamura, Takayuki Kotani, Norio Narita, David Vermilion, Rena A. Lee, Claire Geneser, Johanna Teske, Samuel N. Quinn, David W. Latham, Gilbert A. Esquerdo, Michael L. Calkins, Perry Berlind, Farzaneh Zohrabi, Caitlin Stibbards, Srihan Kotnana, Jon Jenkins, Joseph D. Twicken, Christopher Henze, Richard Kidwell, Christopher Burke, Joel Villaseñor, and Patricia Boyd |
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| 245 | 1 | 0 | |a Diving beneath the sea of stellar activity |b chromatic radial velocities of the young AU mic planetary system |c Bryson L. Cale, Michael Reefe, Peter Plavchan, Angelle Tanner, Eric Gaidos, Jonathan Gagné, Peter Gao, Stephen R. Kane, Víctor J.S. Béjar, Nicolas Lodieu, Guillem Anglada-Escudé, Ignasi Ribas, Enric Pallé, Andreas Quirrenbach, Pedro J. Amado, Ansgar Reiners, José A. Caballero, María Rosa Zapatero Osorio, Stefan Dreizler, Andrew W. Howard, Benjamin J. Fulton, Sharon Xuesong Wang, Kevin I. Collins, Mohammed El Mufti, Justin Wittrock, Emily A. Gilbert, Thomas Barclay, Baptiste Klein, Eder Martioli, Robert Wittenmyer, Duncan Wright, Brett Addison, Teruyuki Hirano, Motohide Tamura, Takayuki Kotani, Norio Narita, David Vermilion, Rena A. Lee, Claire Geneser, Johanna Teske, Samuel N. Quinn, David W. Latham, Gilbert A. Esquerdo, Michael L. Calkins, Perry Berlind, Farzaneh Zohrabi, Caitlin Stibbards, Srihan Kotnana, Jon Jenkins, Joseph D. Twicken, Christopher Henze, Richard Kidwell, Christopher Burke, Joel Villaseñor, and Patricia Boyd |
| 264 | 1 | |c 2021 December 7 | |
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| 500 | |a Gesehen am 21.01.2022 | ||
| 520 | |a We present updated radial-velocity (RV) analyses of the AU Mic system. AU Mic is a young (22 Myr) early-M dwarf known to host two transiting planets—P b ∼ 8.46 days, , P c ∼ 18.86 days, . With visible RVs from Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical echelle Spectrographs (CARMENES)-VIS, CHIRON, HARPS, HIRES, Minerva-Australis, and Tillinghast Reflector Echelle Spectrograph, as well as near-infrared (NIR) RVs from CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a 5σ upper limit to the mass of AU Mic c of M c ≤ 20.13 M ⊕ and present a refined mass of AU Mic b of . Used in our analyses is a new RV modeling toolkit to exploit the wavelength dependence of stellar activity present in our RVs via wavelength-dependent Gaussian processes. By obtaining near-simultaneous visible and near-infrared RVs, we also compute the temporal evolution of RV “color” and introduce a regressional method to aid in isolating Keplerian from stellar activity signals when modeling RVs in future works. Using a multiwavelength Gaussian process model, we demonstrate the ability to recover injected planets at 5σ significance with semi-amplitudes down to ≈10 m s−1 with a known ephemeris, more than an order of magnitude below the stellar activity amplitude. However, we find that the accuracy of the recovered semi-amplitudes is ∼50% for such signals with our model. | ||
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| 700 | 1 | |a Latham, David W. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Esquerdo, Gilbert A. |e VerfasserIn |4 aut | |
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