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 | |
State | Published - Aug 1 2023 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Access to Document
Other files and links
Cite this
- APA
- Author
- BIBTEX
- Harvard
- Standard
- RIS
- Vancouver
}
In: Astronomical Journal, Vol. 166, No. 2, 44, 01.08.2023.
Research output: Contribution to journal › Article › peer-review
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.
UR - http://www.scopus.com/inward/record.url?scp=85164429125&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85164429125&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/acd8bf
DO - 10.3847/1538-3881/acd8bf
M3 - Article
AN - SCOPUS:85164429125
SN - 0004-6256
VL - 166
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 44
ER -