TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star

Luke C. Powers; Jessica Libby-Roberts; Andrea S.J. Lin; Caleb I. Cañas; Shubham Kanodia; Suvrath Mahadevan; Joe P. Ninan; Guđmundur Stefánsson; Arvind F. Gupta; Sinclaire Jones; Henry A. Kobulnicky; Andrew Monson; Brock A. Parker; Tera N. Swaby; Chad F. Bender; William D. Cochran; Leslie Hebb; Andrew J. Metcalf; Paul Robertson; Christian Schwab; John Wisniewski; Jason T. Wright

doi:10.3847/1538-3881/acd8bf

TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star

Luke C. Powers, Jessica Libby-Roberts, Andrea S.J. Lin, Caleb I. Cañas, Shubham Kanodia, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Arvind F. Gupta, Sinclaire Jones, Henry A. Kobulnicky, Andrew Monson, Brock A. Parker, Tera N. Swaby, Chad F. Bender, William D. Cochran, Leslie Hebb, Andrew J. Metcalf, Paul Robertson, Christian SchwabJohn Wisniewski, Jason T. Wright

Research output: Contribution to journal › Article › peer-review

Abstract

Using both ground-based transit photometry and high-precision radial velocity spectroscopy, we confirm the planetary nature of TOI-3785 b. This transiting Neptune orbits an M2-Dwarf star with a period of ∼4.67 days, a planetary radius of 5.14 ± 0.16 R _⊕, a mass of 14.95 − 3.92 + 4.10 M _⊕, and a density of ρ = 0.61 − 0.17 + 0.18 g cm⁻³. TOI-3785 b belongs to a rare population of Neptunes (4 R _⊕ < R _p < 7 R _⊕) orbiting cooler, smaller M-dwarf host stars, of which only ∼10 have been confirmed. By increasing the number of confirmed planets, TOI-3785 b offers an opportunity to compare similar planets across varying planetary and stellar parameter spaces. Moreover, with a high-transmission spectroscopy metric of ∼150 combined with a relatively cool equilibrium temperature of T _eq = 582 ± 16 K and an inactive host star, TOI-3785 b is one of the more promising low-density M-dwarf Neptune targets for atmospheric follow up. Future investigation into atmospheric mass-loss rates of TOI-3785 b may yield new insights into the atmospheric evolution of these low-mass gas planets around M dwarfs.

Original language	English (US)
Article number	44
Journal	Astronomical Journal
Volume	166
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/acd8bf
State	Published - Aug 1 2023

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-3881/acd8bf

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Powers, L. C., Libby-Roberts, J., Lin, A. S. J., Cañas, C. I., Kanodia, S., Mahadevan, S., Ninan, J. P., Stefánsson, G., Gupta, A. F., Jones, S., Kobulnicky, H. A., Monson, A., Parker, B. A., Swaby, T. N., Bender, C. F., Cochran, W. D., Hebb, L., Metcalf, A. J., Robertson, P., ... Wright, J. T. (2023). TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star. Astronomical Journal, 166(2), Article 44. https://doi.org/10.3847/1538-3881/acd8bf

@article{a7ea57bf194a4cd2aaad91d9303c1810,

title = "TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star",

abstract = "Using both ground-based transit photometry and high-precision radial velocity spectroscopy, we confirm the planetary nature of TOI-3785 b. This transiting Neptune orbits an M2-Dwarf star with a period of ∼4.67 days, a planetary radius of 5.14 ± 0.16 R ⊕, a mass of 14.95 − 3.92 + 4.10 M ⊕, and a density of ρ = 0.61 − 0.17 + 0.18 g cm−3. TOI-3785 b belongs to a rare population of Neptunes (4 R ⊕ < R p < 7 R ⊕) orbiting cooler, smaller M-dwarf host stars, of which only ∼10 have been confirmed. By increasing the number of confirmed planets, TOI-3785 b offers an opportunity to compare similar planets across varying planetary and stellar parameter spaces. Moreover, with a high-transmission spectroscopy metric of ∼150 combined with a relatively cool equilibrium temperature of T eq = 582 ± 16 K and an inactive host star, TOI-3785 b is one of the more promising low-density M-dwarf Neptune targets for atmospheric follow up. Future investigation into atmospheric mass-loss rates of TOI-3785 b may yield new insights into the atmospheric evolution of these low-mass gas planets around M dwarfs.",

author = "Powers, {Luke C.} and Jessica Libby-Roberts and Lin, {Andrea S.J.} and Ca{\~n}as, {Caleb I.} and Shubham Kanodia and Suvrath Mahadevan and Ninan, {Joe P.} and Gu{\d}mundur Stef{\'a}nsson and Gupta, {Arvind F.} and Sinclaire Jones and Kobulnicky, {Henry A.} and Andrew Monson and Parker, {Brock A.} and Swaby, {Tera N.} and Bender, {Chad F.} and Cochran, {William D.} and Leslie Hebb and Metcalf, {Andrew J.} and Paul Robertson and Christian Schwab and John Wisniewski and Wright, {Jason T.}",

note = "Funding Information: Based on observations obtained with the Samuel Oschin 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Z.T.F. is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. Funding Information: We want to thank the anonymous referee for their thoughtful suggestions and time spent on this work. Their comments regarding the specifics of planetary occurrence and Neptune detection were helpful in shaping the discussion of this planetary target. The Center for Exoplanets and Habitable Worlds is supported by Penn State and the Eberly College of Science. Computations for this research were performed on the Penn State's Institute for Computational and Data Sciences{\textquoteright} Advanced Cyber Infrastructure (ICDS-ACI). This content is solely the responsibility of the authors and does not necessarily represent the views of the Institute for Computational and Data Sciences. The Pennsylvania State University campuses are located on the original homelands of the Erie, Haudenosaunee (Seneca, Cayuga, Onondaga, Oneida, Mohawk, and Tuscarora), Lenape (Delaware Nation, Delaware Tribe, Stockbridge-Munsee), Shawnee (Absentee, Eastern, and Oklahoma), Susquehannock, and Wahzhazhe (Osage) Nations. As a land grant institution, we acknowledge and honor the traditional caretakers of these lands and strive to understand and model their responsible stewardship. We also acknowledge the longer history of these lands and our place in that history. Funding Information: Some of the observations in this paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Funding Information: Data presented were obtained by the NEID spectrograph built by Penn State University and operated at the WIYN Observatory by NSF{\textquoteright}s NOIRLab, under the NN-EXPLORE partnership of the National Aeronautics and Space Administration and the National Science Foundation. This work was performed for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the United States Government under the Prime Contract 80NM0018D0004 between Caltech and NASA. These results are based on observations obtained with NEID under proposals 2021B-0035 (PI: S. Kanodia), 2021B-0435 (PI: S. Kanodia), 2022A-452266 (PI: S. Kanodia), and 2022A-794607 (PI: J. Libby-Roberts). We thank the NEID Queue Observers and WIYN Observing Associates for their skillful execution of our NEID observations. Funding Information: Some of the data presented in this paper were obtained from MAST at STScI. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This work includes data collected by the TESS mission, which are publicly available from MAST. Funding for the TESS mission is provided by the NASA Science Mission directorate. Funding Information: W.D.C. acknowledges support from NSF grant AST 2108801. Funding Information: C.I.C. acknowledges support by NASA Headquarters through an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA and the NASA Earth and Space Science Fellowship Program through grant 80NSSC18K1114. Funding Information: These results are based on observations obtained with the Habitable-zone Planet Finder Spectrograph on the HET. We acknowledge support from NSF grants AST-1006676, AST-1126413, AST-1310885, AST-1310875, AST-1910954, AST-1907622, AST-1909506, ATI 2009889, ATI-2009982, AST-2108512, and the NASA Astrobiology Institute (NNA09DA76A) in the pursuit of precision radial velocities in the NIR. The HPF team also acknowledges support from the Heising-Simons Foundation via grant 2017-0494. The Hobby–Eberly Telescope is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universit{\"a}t M{\"u}nchen, and Georg-August Universit{\"a}t Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The HET collaboration acknowledges the support and resources from the Texas Advanced Computing Center. We thank the Resident Astronomers and Telescope Operators at the HET for the skillful execution of our observations with HPF. We would like to acknowledge that the HET is built on Indigenous land. Moreover, we would like to acknowledge and pay our respects to the Carrizo & Comecrudo, Coahuiltecan, Caddo, Tonkawa, Comanche, Lipan Apache, Alabama-Coushatta, Kickapoo, Tigua Pueblo, and all the American Indian and Indigenous Peoples and communities who have been or have become a part of these lands and territories in Texas, here on Turtle Island. Funding Information: We want to thank the anonymous referee for their thoughtful suggestions and time spent on this work. Their comments regarding the specifics of planetary occurrence and Neptune detection were helpful in shaping the discussion of this planetary target. The Center for Exoplanets and Habitable Worlds is supported by Penn State and the Eberly College of Science. Computations for this research were performed on the Penn State's Institute for Computational and Data Sciences{\textquoteright} Advanced Cyber Infrastructure (ICDS-ACI). This content is solely the responsibility of the authors and does not necessarily represent the views of the Institute for Computational and Data Sciences. The Pennsylvania State University campuses are located on the original homelands of the Erie, Haudenosaunee (Seneca, Cayuga, Onondaga, Oneida, Mohawk, and Tuscarora), Lenape (Delaware Nation, Delaware Tribe, Stockbridge-Munsee), Shawnee (Absentee, Eastern, and Oklahoma), Susquehannock, and Wahzhazhe (Osage) Nations. As a land grant institution, we acknowledge and honor the traditional caretakers of these lands and strive to understand and model their responsible stewardship. We also acknowledge the longer history of these lands and our place in that history. Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = aug,

day = "1",

doi = "10.3847/1538-3881/acd8bf",

language = "English (US)",

volume = "166",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "2",

}

Powers, LC, Libby-Roberts, J, Lin, ASJ, Cañas, CI, Kanodia, S, Mahadevan, S, Ninan, JP, Stefánsson, G, Gupta, AF, Jones, S, Kobulnicky, HA, Monson, A, Parker, BA, Swaby, TN, Bender, CF, Cochran, WD, Hebb, L, Metcalf, AJ, Robertson, P, Schwab, C, Wisniewski, J & Wright, JT 2023, 'TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star', Astronomical Journal, vol. 166, no. 2, 44. https://doi.org/10.3847/1538-3881/acd8bf

TY - JOUR

T1 - TOI-3785 b

T2 - A Low-density Neptune Orbiting an M2-dwarf Star

AU - Powers, Luke C.

AU - Libby-Roberts, Jessica

AU - Lin, Andrea S.J.

AU - Cañas, Caleb I.

AU - Kanodia, Shubham

AU - Mahadevan, Suvrath

AU - Ninan, Joe P.

AU - Stefánsson, Guđmundur

AU - Gupta, Arvind F.

AU - Jones, Sinclaire

AU - Kobulnicky, Henry A.

AU - Monson, Andrew

AU - Parker, Brock A.

AU - Swaby, Tera N.

AU - Bender, Chad F.

AU - Cochran, William D.

AU - Hebb, Leslie

AU - Metcalf, Andrew J.

AU - Robertson, Paul

AU - Schwab, Christian

AU - Wisniewski, John

AU - Wright, Jason T.

N1 - Funding Information: Based on observations obtained with the Samuel Oschin 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Z.T.F. is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. Funding Information: We want to thank the anonymous referee for their thoughtful suggestions and time spent on this work. Their comments regarding the specifics of planetary occurrence and Neptune detection were helpful in shaping the discussion of this planetary target. The Center for Exoplanets and Habitable Worlds is supported by Penn State and the Eberly College of Science. Computations for this research were performed on the Penn State's Institute for Computational and Data Sciences’ Advanced Cyber Infrastructure (ICDS-ACI). This content is solely the responsibility of the authors and does not necessarily represent the views of the Institute for Computational and Data Sciences. The Pennsylvania State University campuses are located on the original homelands of the Erie, Haudenosaunee (Seneca, Cayuga, Onondaga, Oneida, Mohawk, and Tuscarora), Lenape (Delaware Nation, Delaware Tribe, Stockbridge-Munsee), Shawnee (Absentee, Eastern, and Oklahoma), Susquehannock, and Wahzhazhe (Osage) Nations. As a land grant institution, we acknowledge and honor the traditional caretakers of these lands and strive to understand and model their responsible stewardship. We also acknowledge the longer history of these lands and our place in that history. Funding Information: Some of the observations in this paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Funding Information: Data presented were obtained by the NEID spectrograph built by Penn State University and operated at the WIYN Observatory by NSF’s NOIRLab, under the NN-EXPLORE partnership of the National Aeronautics and Space Administration and the National Science Foundation. This work was performed for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the United States Government under the Prime Contract 80NM0018D0004 between Caltech and NASA. These results are based on observations obtained with NEID under proposals 2021B-0035 (PI: S. Kanodia), 2021B-0435 (PI: S. Kanodia), 2022A-452266 (PI: S. Kanodia), and 2022A-794607 (PI: J. Libby-Roberts). We thank the NEID Queue Observers and WIYN Observing Associates for their skillful execution of our NEID observations. Funding Information: Some of the data presented in this paper were obtained from MAST at STScI. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This work includes data collected by the TESS mission, which are publicly available from MAST. Funding for the TESS mission is provided by the NASA Science Mission directorate. Funding Information: W.D.C. acknowledges support from NSF grant AST 2108801. Funding Information: C.I.C. acknowledges support by NASA Headquarters through an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA and the NASA Earth and Space Science Fellowship Program through grant 80NSSC18K1114. Funding Information: These results are based on observations obtained with the Habitable-zone Planet Finder Spectrograph on the HET. We acknowledge support from NSF grants AST-1006676, AST-1126413, AST-1310885, AST-1310875, AST-1910954, AST-1907622, AST-1909506, ATI 2009889, ATI-2009982, AST-2108512, and the NASA Astrobiology Institute (NNA09DA76A) in the pursuit of precision radial velocities in the NIR. The HPF team also acknowledges support from the Heising-Simons Foundation via grant 2017-0494. The Hobby–Eberly Telescope is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August Universität Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The HET collaboration acknowledges the support and resources from the Texas Advanced Computing Center. We thank the Resident Astronomers and Telescope Operators at the HET for the skillful execution of our observations with HPF. We would like to acknowledge that the HET is built on Indigenous land. Moreover, we would like to acknowledge and pay our respects to the Carrizo & Comecrudo, Coahuiltecan, Caddo, Tonkawa, Comanche, Lipan Apache, Alabama-Coushatta, Kickapoo, Tigua Pueblo, and all the American Indian and Indigenous Peoples and communities who have been or have become a part of these lands and territories in Texas, here on Turtle Island. Funding Information: We want to thank the anonymous referee for their thoughtful suggestions and time spent on this work. Their comments regarding the specifics of planetary occurrence and Neptune detection were helpful in shaping the discussion of this planetary target. The Center for Exoplanets and Habitable Worlds is supported by Penn State and the Eberly College of Science. Computations for this research were performed on the Penn State's Institute for Computational and Data Sciences’ Advanced Cyber Infrastructure (ICDS-ACI). This content is solely the responsibility of the authors and does not necessarily represent the views of the Institute for Computational and Data Sciences. The Pennsylvania State University campuses are located on the original homelands of the Erie, Haudenosaunee (Seneca, Cayuga, Onondaga, Oneida, Mohawk, and Tuscarora), Lenape (Delaware Nation, Delaware Tribe, Stockbridge-Munsee), Shawnee (Absentee, Eastern, and Oklahoma), Susquehannock, and Wahzhazhe (Osage) Nations. As a land grant institution, we acknowledge and honor the traditional caretakers of these lands and strive to understand and model their responsible stewardship. We also acknowledge the longer history of these lands and our place in that history. Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

PY - 2023/8/1

Y1 - 2023/8/1

N2 - Using both ground-based transit photometry and high-precision radial velocity spectroscopy, we confirm the planetary nature of TOI-3785 b. This transiting Neptune orbits an M2-Dwarf star with a period of ∼4.67 days, a planetary radius of 5.14 ± 0.16 R ⊕, a mass of 14.95 − 3.92 + 4.10 M ⊕, and a density of ρ = 0.61 − 0.17 + 0.18 g cm−3. TOI-3785 b belongs to a rare population of Neptunes (4 R ⊕ < R p < 7 R ⊕) orbiting cooler, smaller M-dwarf host stars, of which only ∼10 have been confirmed. By increasing the number of confirmed planets, TOI-3785 b offers an opportunity to compare similar planets across varying planetary and stellar parameter spaces. Moreover, with a high-transmission spectroscopy metric of ∼150 combined with a relatively cool equilibrium temperature of T eq = 582 ± 16 K and an inactive host star, TOI-3785 b is one of the more promising low-density M-dwarf Neptune targets for atmospheric follow up. Future investigation into atmospheric mass-loss rates of TOI-3785 b may yield new insights into the atmospheric evolution of these low-mass gas planets around M dwarfs.

AB - Using both ground-based transit photometry and high-precision radial velocity spectroscopy, we confirm the planetary nature of TOI-3785 b. This transiting Neptune orbits an M2-Dwarf star with a period of ∼4.67 days, a planetary radius of 5.14 ± 0.16 R ⊕, a mass of 14.95 − 3.92 + 4.10 M ⊕, and a density of ρ = 0.61 − 0.17 + 0.18 g cm−3. TOI-3785 b belongs to a rare population of Neptunes (4 R ⊕ < R p < 7 R ⊕) orbiting cooler, smaller M-dwarf host stars, of which only ∼10 have been confirmed. By increasing the number of confirmed planets, TOI-3785 b offers an opportunity to compare similar planets across varying planetary and stellar parameter spaces. Moreover, with a high-transmission spectroscopy metric of ∼150 combined with a relatively cool equilibrium temperature of T eq = 582 ± 16 K and an inactive host star, TOI-3785 b is one of the more promising low-density M-dwarf Neptune targets for atmospheric follow up. Future investigation into atmospheric mass-loss rates of TOI-3785 b may yield new insights into the atmospheric evolution of these low-mass gas planets around M dwarfs.

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U2 - 10.3847/1538-3881/acd8bf

DO - 10.3847/1538-3881/acd8bf

M3 - Article

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SN - 0004-6256

VL - 166

JO - Astronomical Journal

JF - Astronomical Journal

IS - 2

M1 - 44

ER -

TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star

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