Published June 25, 2020
| Accepted Version + Supplemental Material
Journal Article
Open
A planet within the debris disk around the pre-main-sequence star AU Microscopii
- Creators
-
Plavchan, Peter
-
Barclay, Thomas
-
Gagné, Jonathan
-
Gao, Peter
-
Cale, Bryson
- Matzko, William
-
Dragomir, Diana
-
Quinn, Sam
-
Feliz, Dax
-
Stassun, Keivan
-
Crossfield, Ian J. M.
-
Berardo, David A.
-
Latham, David W.
- Tieu, Ben
-
Anglada-Escudé, Guillem
-
Ricker, George
-
Vanderspek, Roland
-
Seager, Sara
-
Winn, Joshua N.
-
Jenkins, Jon M.
- Rinehart, Stephen
-
Krishnamurthy, Akshata
-
Dynes, Scott
-
Doty, John
-
Adams, Fred
- Afanasev, Dennis A.
-
Beichman, Chas
-
Bottom, Mike
-
Bowler, Brendan P.
- Brinkworth, Carolyn
- Brown, Carolyn J.
- Cancino, Andrew
-
Ciardi, David R.
-
Clampin, Mark
-
Clark, Jake T.
-
Collins, Karen
- Davison, Cassy
-
Foreman-Mackey, Daniel
-
Furlan, Elise
-
Gaidos, Eric J.
-
Geneser, Claire
- Giddens, Frank
-
Gilbert, Emily
- Hall, Ryan
-
Hellier, Coel
-
Henry, Todd
-
Horner, Jonathan
-
Howard, Andrew W.
-
Huang, Chelsea
- Huber, Joseph
-
Kane, Stephen R.
-
Kenworthy, Matthew
-
Kielkopf, John
-
Kipping, David
- Klenke, Chris
-
Kruse, Ethan
-
Latouf, Natasha
-
Lowrance, Patrick
-
Mennesson, Bertrand
-
Mengel, Matthew
-
Mills, Sean M.
-
Morton, Tim
-
Narita, Norio
-
Newton, Elisabeth
- Nishimoto, America
-
Okumura, Jack
-
Palle, Enric
-
Pepper, Joshua
-
Quintana, Elisa V.
-
Roberge, Aki
-
Roccatagliata, Veronica
-
Schlieder, Joshua E.
-
Tanner, Angelle
- Teske, Johanna
-
Tinney, C. G.
-
Vanderburg, Andrew
-
von Braun, Kaspar
-
Walp, Bernie
-
Wang, Jason
-
Wang, Sharon Xuesong
- Weigand, Denise
-
White, Russel
-
Wittenmyer, Robert A.
-
Wright, Duncan J.
-
Youngblood, Allison
-
Zhang, Hui
-
Zilberman, Perri
Abstract
AU Microscopii (AU Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 22 million years. AU Mic possesses a relatively rare and spatially resolved edge-on debris disk extending from about 35 to 210 astronomical units from the star, and with clumps exhibiting non-Keplerian motion. Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic 'activity' on the star. Here we report observations of a planet transiting AU Mic. The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07 astronomical units, a radius of 0.4 Jupiter radii, and a mass of less than 0.18 Jupiter masses at 3σ confidence. Our observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution.
Additional Information
© 2020 Springer Nature Limited. Received 16 February 2019; Accepted 17 March 2020; Published 24 June 2020. This work was supported by grants to P.P. from NASA (award 16-APROBES16-0020 and support from the Exoplanet Exploration Program) and the National Science Foundation (Astronomy and Astrophysics grant 1716202), the Mount Cuba Astronomical Foundation and George Mason University start-up funds.The NASA Infrared Telescope Facility is operated by the University of Hawaii under contract NNH14CK55B with NASA. Funding for the TESS mission is provided by NASA's Science Mission directorate. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with NASA under the Exoplanet Exploration Program. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This research has made use of the services of the ESO Science Archive Facility, based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere with the HARPS spectrometer. This work has made use of data from the European Space Agency (ESA) mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grant DP180100972, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida and University of Texas at Austin. This work was partly supported by JSPS KAKENHI grant numbers JP18H01265 and 18H05439, JST PRESTO grant number JPMJPR1775, NSFC grant number 11673011 and MINECO grant ESP2016-80435-C2-2-R. D.D. acknowledges support for this work provided by NASA through Hubble Fellowship grant HST-HF2-51372.001-A awarded by the Space Telescope Science Institute. B.P.B. acknowledges support from National Science Foundation grant AST-1909209. J.W. and P.G. acknowledge support from the Heising-Simons Foundation 51 Pegasi b fellowship. Data availability: In addition to the figure data available, all raw spectroscopic data are available either in the associated observatory archive or upon request from the corresponding author. The TESS light curve is available at the MAST archive, and the SuperWASP light curve is available at the NASA Exoplanet Archive. Source data are provided with this paper. Code availability: All code that is not readily available on GitHub is available upon request. Author Contributions: P.P.: lead author, principal investigator for CSHELL/iSHELL gas cell and observations, analysis and interpretation. J.G., P.G., B.C., A.T., S.X.W., R.W.: CSHELL/iSHELL data reduction and forward model codes. W.M.: RADVEL analysis. T.B., D.D., S.Q., D.F.-M., E. Gilbert, C. Huang, D.K., E.K., E.V.Q., A.V.: analysis of TESS light curve. K.S., K.C., N.N., E.P., J.P.: follow-up ground-based observations. I.J.M.C., D.A.B., P.L., E.N.: Spitzer light curve. D.F., B.T., C. Hellier: inspection of ground-based light curves. D.W.L.: TRES. G.A.-E.: HARPS. G.R., R.V., S.S., J.N.W., J.M.J.: TESS mission architects. S.R., A.K., S.D., J.T.: TESS mission. F.A., M.C., M.K., A.R., V.R., J.W.: disk physics. D.A.A., J.E.S., A.Y.: flare analysis. C. Beichman, M.B., C. Brinkworth, D.R.C., S.R.K., B.M., S.M.M., K.v.B.: CSHELL/iSHELL instrumentation. B.P.B., C.J.B., J.T.C., J. Horner, J.K., J.O., C.G.T., R.A.W., D.J.W., H.Z.: MINERVA-Australis. A.C., C.D., E.F., C.G., F.G., R.H., T.H., J.H., C.K., N.L., M.M., T.M., A.N., J.T., B.W., D.W., P.Z.: CSHELL/iSHELL observers. E.J.G.: stellar parameters. A.W.H.: Keck HIRES. The authors declare no competing interests.Errata
In Fig. 3 of this Article, the subscript 'Sun' symbols on both axis labels (R☉ and M☉) should have been subscript 'Earth' symbols (R⊕ and M⊕), as appears correctly in the legend. This error has been corrected online.Attached Files
Accepted Version - 2006.13248.pdf
Accepted Version - nihms-1577725.pdf
Supplemental Material - 41586_2020_2400_Fig10_ESM.webp
Supplemental Material - 41586_2020_2400_Fig11_ESM.webp
Supplemental Material - 41586_2020_2400_Fig12_ESM.webp
Supplemental Material - 41586_2020_2400_Fig4_ESM.webp
Supplemental Material - 41586_2020_2400_Fig5_ESM.webp
Supplemental Material - 41586_2020_2400_Fig6_ESM.webp
Supplemental Material - 41586_2020_2400_Fig7_ESM.webp
Supplemental Material - 41586_2020_2400_Fig8_ESM.webp
Supplemental Material - 41586_2020_2400_Fig9_ESM.webp
Supplemental Material - 41586_2020_2400_MOESM10_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM11_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM12_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM1_ESM.csv
Supplemental Material - 41586_2020_2400_MOESM2_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM3_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM4_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM5_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM6_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM7_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM8_ESM.xlsx
Supplemental Material - 41586_2020_2400_MOESM9_ESM.xlsx
Supplemental Material - 41586_2020_2400_Tab1_ESM.jpg
Files
41586_2020_2400_Tab1_ESM.jpg
Files
(36.7 MB)
| Name | Size | Download all |
|---|---|---|
|
md5:d4a17028a6f30a25371f92b443f6adb8
|
19.9 kB | Download |
|
md5:83431da506124af5aa8a93f4cc6ab79b
|
38.4 kB | Preview Download |
|
md5:593ac5a17de66b6f10945e90c0be183d
|
26.5 kB | Download |
|
md5:8cd81b25a0b95f219fe32bca1af05c97
|
108.5 kB | Download |
|
md5:57c6eada13b55170b6dd2b2add627f8d
|
95.6 kB | Download |
|
md5:34d9cf4a269ee4d009d1ce1016d473f9
|
108.7 kB | Download |
|
md5:78ab92e14237333e46cb06f85205fe21
|
116.8 kB | Download |
|
md5:cc2bc71c76c50a52f74d4b77033dcd2f
|
42.1 kB | Download |
|
md5:76b8393eff58c816a864a1c3e24b1bf3
|
12.1 kB | Download |
|
md5:a41f8086971ff26e4a16cf262d5aa185
|
232.8 kB | Download |
|
md5:ec166341576dd5daa93ecd379b241e15
|
441.2 kB | Preview Download |
|
md5:2e6abfdae66a7fc6eb2d7ac361f6e57b
|
639.2 kB | Download |
|
md5:a67d99103f43e9755dfe681437987477
|
7.0 MB | Download |
|
md5:6229159a45b31008c8c12adc2a3594c3
|
227.8 kB | Download |
|
md5:9771607dee018216286a879e77d7349e
|
2.7 MB | Preview Download |
|
md5:48259baffbfb69a751659938996f1269
|
4.4 MB | Download |
|
md5:32c1f61154ad05dcc68ec6ad96289983
|
495.3 kB | Download |
|
md5:2750007d098cf76b772f91169f60611e
|
3.2 MB | Download |
|
md5:f2e8ca9d0eea5a1f11256cb6900a9de2
|
108.8 kB | Download |
|
md5:d5d4d71223c27937ca316be0ed3ed439
|
59.7 kB | Download |
|
md5:f842a44a34a553b3295ecba370500a74
|
192.8 kB | Download |
|
md5:e4bc3d3b158544535b18abd09571c440
|
6.9 MB | Download |
|
md5:694f420083b64da88867dcb58bd50a5b
|
9.6 MB | Preview Download |
|
md5:b9bf49864de1029ea4c3428191c8cc0c
|
16.2 kB | Download |
Additional details
- Alternative title
- A planet within the debris disk around the pre-main-sequence star AU Mic
- PMCID
- PMC7323865
- Eprint ID
- 104097
- Resolver ID
- CaltechAUTHORS:20200626-144356489
- 16-APROBES16-0020
- NASA
- AST-1716202
- NSF
- Mt. Cuba Astronomical Foundation
- George Mason University
- NNH14CK55B
- NASA
- W. M. Keck Foundation
- NAS5-26555
- NASA
- Gaia Multilateral Agreement
- LE160100001
- Australian Research Council
- DP180100972
- Australian Research Council
- University of Southern Queensland
- Massachusetts Institute of Technology (MIT)
- Nanjing University
- University of Louisville
- University of California, Riverside
- University of Florida
- University of Texas at Austin
- JP18H01265
- Japan Society for the Promotion of Science (JSPS)
- 18H05439
- Japan Society for the Promotion of Science (JSPS)
- JPMJPR1775
- Japan Science and Technology Agency
- 11673011
- National Natural Science Foundation of China
- ESP2016-80435-C2-2-R
- Ministerio de Economía, Industria y Competitividad (MINECO)
- HST-HF2-51372.001-A
- NASA Hubble Fellowship
- AST-1909209
- NSF
- 51 Pegasi b Fellowship
- Heising-Simons Foundation
- Created
-
2020-06-26Created from EPrint's datestamp field
- Updated
-
2023-06-01Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, Infrared Processing and Analysis Center (IPAC)