A planet within the debris disk around the pre-main-sequence star AU Microscopii

Peter Plavchan; Thomas Barclay; Jonathan Gagné; Peter Gao; Bryson Cale; William Matzko; Diana Dragomir; Sam Quinn; Dax Feliz; Keivan Stassun; Ian J.M. Crossfield; David A. Berardo; David W. Latham; Ben Tieu; Guillem Anglada-Escudé; George Ricker; Roland Vanderspek; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Stephen Rinehart; Akshata Krishnamurthy; Scott Dynes; John Doty; Fred Adams; Dennis A. Afanasev; Chas Beichman; Mike Bottom; Brendan P. Bowler; Carolyn Brinkworth; Carolyn J. Brown; Andrew Cancino; David R. Ciardi; Mark Clampin; Jake T. Clark; Karen Collins; Cassy Davison; Daniel Foreman-Mackey; Elise Furlan; Eric J. Gaidos; Claire Geneser; Frank Giddens; Emily Gilbert; Ryan Hall; Coel Hellier; Todd Henry; Jonathan Horner; Andrew W. Howard; Chelsea Huang; Joseph Huber; Stephen R. Kane; Matthew Kenworthy; John Kielkopf; David Kipping; Chris Klenke; Ethan Kruse; Natasha Latouf; Patrick Lowrance; Bertrand Mennesson; Matthew Mengel; Sean M. Mills; Tim Morton; Norio Narita; Elisabeth Newton; America Nishimoto; Jack Okumura; Enric Palle; Joshua Pepper; Elisa V. Quintana; Aki Roberge; Veronica Roccatagliata; Joshua E. Schlieder; Angelle Tanner; Johanna Teske; C. G. Tinney; Andrew Vanderburg; Kaspar von Braun; Bernie Walp; Jason Wang; Sharon Xuesong Wang; Denise Weigand; Russel White; Robert A. Wittenmyer; Duncan J. Wright; Allison Youngblood; Hui Zhang; Perri Zilberman

doi:10.1038/s41586-020-2400-z

A planet within the debris disk around the pre-main-sequence star AU Microscopii

Peter Plavchan, Thomas Barclay, Jonathan Gagné, Peter Gao, Bryson Cale, William Matzko, Diana Dragomir, Sam Quinn, Dax Feliz, Keivan Stassun, Ian J.M. Crossfield, David A. Berardo, David W. Latham, Ben Tieu, Guillem Anglada-Escudé, George Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. JenkinsStephen Rinehart, Akshata Krishnamurthy, Scott Dynes, John Doty, Fred Adams, Dennis A. Afanasev, Chas Beichman, Mike Bottom, Brendan P. Bowler, Carolyn Brinkworth, Carolyn J. Brown, Andrew Cancino, David R. Ciardi, Mark Clampin, Jake T. Clark, Karen Collins, Cassy Davison, Daniel Foreman-Mackey, Elise Furlan, Eric J. Gaidos, Claire Geneser, Frank Giddens, Emily Gilbert, Ryan Hall, Coel Hellier, Todd Henry, Jonathan Horner, Andrew W. Howard, Chelsea Huang, Joseph Huber, Stephen R. Kane, Matthew Kenworthy, John Kielkopf, David Kipping, Chris Klenke, Ethan Kruse, Natasha Latouf, Patrick Lowrance, Bertrand Mennesson, Matthew Mengel, Sean M. Mills, Tim Morton, Norio Narita, Elisabeth Newton, America Nishimoto, Jack Okumura, Enric Palle, Joshua Pepper, Elisa V. Quintana, Aki Roberge, Veronica Roccatagliata, Joshua E. Schlieder, Angelle Tanner, Johanna Teske, C. G. Tinney, Andrew Vanderburg, Kaspar von Braun, Bernie Walp, Jason Wang, Sharon Xuesong Wang, Denise Weigand, Russel White, Robert A. Wittenmyer, Duncan J. Wright, Allison Youngblood, Hui Zhang, Perri Zilberman

Astrophysical Sciences

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102 Scopus citations

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 years¹. AU Mic possesses a relatively rare² and spatially resolved³ edge-on debris disk extending from about 35 to 210 astronomical units from the star⁴, and with clumps exhibiting non-Keplerian motion^5–7. 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^8,9. 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.

Original language	English (US)
Pages (from-to)	497-500
Number of pages	4
Journal	Nature
Volume	582
Issue number	7813
DOIs	https://doi.org/10.1038/s41586-020-2400-z
State	Published - Jun 25 2020

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Plavchan, P., Barclay, T., Gagné, J., Gao, P., Cale, B., Matzko, W., Dragomir, D., Quinn, S., Feliz, D., Stassun, K., Crossfield, I. J. M., Berardo, D. A., Latham, D. W., Tieu, B., Anglada-Escudé, G., Ricker, G., Vanderspek, R., Seager, S., Winn, J. N., ... Zilberman, P. (2020). A planet within the debris disk around the pre-main-sequence star AU Microscopii. Nature, 582(7813), 497-500. https://doi.org/10.1038/s41586-020-2400-z

@article{0ed1595688d5486db9bbf3ac5f1c035a,

title = "A planet within the debris disk around the pre-main-sequence star AU Microscopii",

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 years1. AU Mic possesses a relatively rare2 and spatially resolved3 edge-on debris disk extending from about 35 to 210 astronomical units from the star4, and with clumps exhibiting non-Keplerian motion5–7. Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic {\textquoteleft}activity{\textquoteright} on the star8,9. 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.",

author = "Peter Plavchan and Thomas Barclay and Jonathan Gagn{\'e} and Peter Gao and Bryson Cale and William Matzko and Diana Dragomir and Sam Quinn and Dax Feliz and Keivan Stassun and Crossfield, {Ian J.M.} and Berardo, {David A.} and Latham, {David W.} and Ben Tieu and Guillem Anglada-Escud{\'e} and George Ricker and Roland Vanderspek and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Stephen Rinehart and Akshata Krishnamurthy and Scott Dynes and John Doty and Fred Adams and Afanasev, {Dennis A.} and Chas Beichman and Mike Bottom and Bowler, {Brendan P.} and Carolyn Brinkworth and Brown, {Carolyn J.} and Andrew Cancino and Ciardi, {David R.} and Mark Clampin and Clark, {Jake T.} and Karen Collins and Cassy Davison and Daniel Foreman-Mackey and Elise Furlan and Gaidos, {Eric J.} and Claire Geneser and Frank Giddens and Emily Gilbert and Ryan Hall and Coel Hellier and Todd Henry and Jonathan Horner and Howard, {Andrew W.} and Chelsea Huang and Joseph Huber and Kane, {Stephen R.} and Matthew Kenworthy and John Kielkopf and David Kipping and Chris Klenke and Ethan Kruse and Natasha Latouf and Patrick Lowrance and Bertrand Mennesson and Matthew Mengel and Mills, {Sean M.} and Tim Morton and Norio Narita and Elisabeth Newton and America Nishimoto and Jack Okumura and Enric Palle and Joshua Pepper and Quintana, {Elisa V.} and Aki Roberge and Veronica Roccatagliata and Schlieder, {Joshua E.} and Angelle Tanner and Johanna Teske and Tinney, {C. G.} and Andrew Vanderburg and {von Braun}, Kaspar and Bernie Walp and Jason Wang and Wang, {Sharon Xuesong} and Denise Weigand and Russel White and Wittenmyer, {Robert A.} and Wright, {Duncan J.} and Allison Youngblood and Hui Zhang and Perri Zilberman",

note = "Funding Information: Acknowledgements 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{\textquoteright}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. Publisher Copyright: {\textcopyright} 2020, The Author(s), under exclusive licence to Springer Nature Limited.",

year = "2020",

month = jun,

day = "25",

doi = "10.1038/s41586-020-2400-z",

language = "English (US)",

volume = "582",

pages = "497--500",

journal = "Nature",

issn = "0028-0836",

publisher = "Nature Publishing Group",

number = "7813",

}

Plavchan, P, Barclay, T, Gagné, J, Gao, P, Cale, B, Matzko, W, Dragomir, D, Quinn, S, Feliz, D, Stassun, K, Crossfield, IJM, Berardo, DA, Latham, DW, Tieu, B, Anglada-Escudé, G, Ricker, G, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Rinehart, S, Krishnamurthy, A, Dynes, S, Doty, J, Adams, F, Afanasev, DA, Beichman, C, Bottom, M, Bowler, BP, Brinkworth, C, Brown, CJ, Cancino, A, Ciardi, DR, Clampin, M, Clark, JT, Collins, K, Davison, C, Foreman-Mackey, D, Furlan, E, Gaidos, EJ, Geneser, C, Giddens, F, Gilbert, E, Hall, R, Hellier, C, Henry, T, Horner, J, Howard, AW, Huang, C, Huber, J, Kane, SR, Kenworthy, M, Kielkopf, J, Kipping, D, Klenke, C, Kruse, E, Latouf, N, Lowrance, P, Mennesson, B, Mengel, M, Mills, SM, Morton, T, Narita, N, Newton, E, Nishimoto, A, Okumura, J, Palle, E, Pepper, J, Quintana, EV, Roberge, A, Roccatagliata, V, Schlieder, JE, Tanner, A, Teske, J, Tinney, CG, Vanderburg, A, von Braun, K, Walp, B, Wang, J, Wang, SX, Weigand, D, White, R, Wittenmyer, RA, Wright, DJ, Youngblood, A, Zhang, H & Zilberman, P 2020, 'A planet within the debris disk around the pre-main-sequence star AU Microscopii', Nature, vol. 582, no. 7813, pp. 497-500. https://doi.org/10.1038/s41586-020-2400-z

TY - JOUR

T1 - A planet within the debris disk around the pre-main-sequence star AU Microscopii

AU - Plavchan, Peter

AU - Barclay, Thomas

AU - Gagné, Jonathan

AU - Gao, Peter

AU - Cale, Bryson

AU - Matzko, William

AU - Dragomir, Diana

AU - Quinn, Sam

AU - Feliz, Dax

AU - Stassun, Keivan

AU - Crossfield, Ian J.M.

AU - Berardo, David A.

AU - Latham, David W.

AU - Tieu, Ben

AU - Anglada-Escudé, Guillem

AU - Ricker, George

AU - Vanderspek, Roland

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Rinehart, Stephen

AU - Krishnamurthy, Akshata

AU - Dynes, Scott

AU - Doty, John

AU - Adams, Fred

AU - Afanasev, Dennis A.

AU - Beichman, Chas

AU - Bottom, Mike

AU - Bowler, Brendan P.

AU - Brinkworth, Carolyn

AU - Brown, Carolyn J.

AU - Cancino, Andrew

AU - Ciardi, David R.

AU - Clampin, Mark

AU - Clark, Jake T.

AU - Collins, Karen

AU - Davison, Cassy

AU - Foreman-Mackey, Daniel

AU - Furlan, Elise

AU - Gaidos, Eric J.

AU - Geneser, Claire

AU - Giddens, Frank

AU - Gilbert, Emily

AU - Hall, Ryan

AU - Hellier, Coel

AU - Henry, Todd

AU - Horner, Jonathan

AU - Howard, Andrew W.

AU - Huang, Chelsea

AU - Huber, Joseph

AU - Kane, Stephen R.

AU - Kenworthy, Matthew

AU - Kielkopf, John

AU - Kipping, David

AU - Klenke, Chris

AU - Kruse, Ethan

AU - Latouf, Natasha

AU - Lowrance, Patrick

AU - Mennesson, Bertrand

AU - Mengel, Matthew

AU - Mills, Sean M.

AU - Morton, Tim

AU - Narita, Norio

AU - Newton, Elisabeth

AU - Nishimoto, America

AU - Okumura, Jack

AU - Palle, Enric

AU - Pepper, Joshua

AU - Quintana, Elisa V.

AU - Roberge, Aki

AU - Roccatagliata, Veronica

AU - Schlieder, Joshua E.

AU - Tanner, Angelle

AU - Teske, Johanna

AU - Tinney, C. G.

AU - Vanderburg, Andrew

AU - von Braun, Kaspar

AU - Walp, Bernie

AU - Wang, Jason

AU - Wang, Sharon Xuesong

AU - Weigand, Denise

AU - White, Russel

AU - Wittenmyer, Robert A.

AU - Wright, Duncan J.

AU - Youngblood, Allison

AU - Zhang, Hui

AU - Zilberman, Perri

N1 - Funding Information: Acknowledgements 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. Publisher Copyright: © 2020, The Author(s), under exclusive licence to Springer Nature Limited.

PY - 2020/6/25

Y1 - 2020/6/25

N2 - 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 years1. AU Mic possesses a relatively rare2 and spatially resolved3 edge-on debris disk extending from about 35 to 210 astronomical units from the star4, and with clumps exhibiting non-Keplerian motion5–7. 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 star8,9. 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.

AB - 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 years1. AU Mic possesses a relatively rare2 and spatially resolved3 edge-on debris disk extending from about 35 to 210 astronomical units from the star4, and with clumps exhibiting non-Keplerian motion5–7. 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 star8,9. 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.

UR - http://www.scopus.com/inward/record.url?scp=85086804890&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85086804890&partnerID=8YFLogxK

U2 - 10.1038/s41586-020-2400-z

DO - 10.1038/s41586-020-2400-z

M3 - Article

C2 - 32581383

AN - SCOPUS:85086804890

SN - 0028-0836

VL - 582

SP - 497

EP - 500

JO - Nature

JF - Nature

IS - 7813

ER -

A planet within the debris disk around the pre-main-sequence star AU Microscopii

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