<figure><img src="image_20.png" /></figure>

**Figure 16.** Stellar effective temperature vs. effective incident flux on a planet. The boundaries of the habitable zone defined by Kopparapu et al. (2014) are illustrated as shaded regions. The black circles show all transiting exoplanets listed in the NASA exoplanet archive, where the filled circles show only planets that have a mass measurement to better than 30% accuracy. The orange triangle shows the properties of TOI 4633 c. There are no other transiting planets within the habitable zone that are brighter than 11th magnitude, and only four that are brighter than 13th magnitude.

instruments such as the Keck Planet Imager and Characterizer
(Delorme et al. 2020).

7.3. TOI4633 c: A Mini-Neptune in the Habitable Zone

The search for exoplanets in the habitable zones of their host
stars has been a focal point in the field of exoplanet research,
where the habitable zone is defined as the region around a star
where the surface temperature is favorable for liquid water to
exist. We estimate the location of the habitable zone around
TOI 4633 following the prescriptions defined by Kopparapu
et al. (2014). The habitable zone boundaries of “Recent
Venus,” “Maximum Greenhouse,” and “Runaway Green-
house” conditions are shown in Figure 16 (for more details
on how these boundaries are defined see Kopparapu et al.
2014). Using this definition of the habitable zone we find that
TOI 4633 c, with an insolation of 1.56<sup>+0.20</sup><sub>-0.16</sub> F<sub>⊕</sub>, lies inside the
inner edge of the potentially habitable region of the star
between the Recent Venus and Maximum Greenhouse
boundaries. Using the Stefan–Boltzman law and assuming an
albedo equivalent to that of Neptune (0.29), we show that the
effective surface temperature of planet c is ~290 K when only
the energy contribution of star A is considered. When
accounting for the energy contribution of stars A and B at
the time of periastron (stellar separation ~4.5 au), the effective
surface temperature increases to ~420 K.

According to the Catalog of Habitable Zone Exoplanets by
Hill et al. (2023), TOI 4633 is the brightest star known to host a
transiting planet in the habitable zone, with no other transiting
planets within the habitable zone that are brighter than 11th
magnitude, five that are brighter than 13th magnitude, and 29
that are brighter than 15th magnitude. Even though planet c is
at a distance from its host star where liquid water could
potentially reside, the density of the planet (>0.11 g cm<sup>-3</sup>)
suggests that it has a large and dense atmosphere that likely
makes surface level liquid water impossible. However, as
shown independently by Sucerquia et al. (2019) and Dobos
et al. (2021), the probability of a planet hosting a satellite
increases with increased orbital period. As such, the brightness
of the system and the long orbital period of planet c makes
TOI 4633 c a valuable target for further characterization in the
future and, in particular, for the search of planet satellites.

7.4. Conclusion

We present the discovery and validation of a transiting mini-
Neptune ($P_c = 271.9445_{-0.0040}^{+0.0039}$ days, $R_c = 3.2_{-0.19}^{+0.20} R_⊕$, $M_c =
47.8_{-23.8}^{+27.6} M_⊕$) that was discovered by citizen scientists taking
part in the Planet Hunters TESS citizen science project. The
planet's long orbital period places it in the optimistic habitable
zone of its host star, with an insolation of $1.56_{-0.16}^{+0.20} F_⊕$. RV
monitoring of the system with Keck/HIRES and OHP/
SOPHIE revealed an additional 34 days periodic signal that is
not seen in the photometric data. Due to a lack of strong
evidence that this periodic signal is caused by stellar activity,
we tentatively consider this signal to be a planet candidate
($M_b \text{sini} < 109 M_⊕$). Furthermore, we used high-contrast
imaging observations spanning over 117 yr (1905–2023) to
constrain the orbit of the bound stellar companion star ($a_{\text{bin}} =
48.6_{-3.5}^{+4.4} \text{ au}$, $e_{\text{bin}} = 0.91_{-0.03}^{+0.03}$).

Dynamical simulations were used to constrain the mutual
inclination between the binary orbit and that of TOI 4633 c.
The *N*-body simulations showed that if the 34 days planet
candidate is inclined such that it only narrowly avoids
transiting, then the mutual inclination between planet *c* and
the binary orbit has to be less than ~45° to ensure that the
system is stable for longer than $10^6$ yr.

Overall, TOI 4633 stands out due to its brightness, the long
orbital period of the transiting planet TOI 4633 c that places it
in the optimistic habitable zone, and the presence of the bound,
near equal mass, stellar companion. TOI 4633 c is currently
only the fourth habitable zone planet identified in the TESS
data, and the only one transiting a G dwarf star. The system is
valuable for studying planet formation and evolution in
binaries, as well as for being an excellent target for detailed
investigation of planets in habitable zones, particularly in
multiple star systems. While the two stars in the system cannot
currently be resolved from the ground (due to their proximity),
the binary orbit modeling showed that in around 30 yr time the
stars will be separated by more than 150 mas on the sky, a
distance large enough to be able to resolve with modern
spectrographs such as the Keck Planet Imager and Character-
izer. This will enable further characterization of the two stars
and the planets in the system.

8. Software and Data Availability

The TESS data used within this article are hosted and made
publicly available by the Mikulski Archive for Space
Telescopes (MAST, http://archive.stsci.edu/tess/). All the
TESS data used in this paper can be found in
MAST:10.17909/pepe-f853. This work also used data from
the NASA Exoplanet Archive (NASA Exoplanet
Archive 2019), and ExoFOP (ExoFOP 2019).

This work made use of Astropy, a community-developed
core Python package for Astronomy (Astropy Collaboration
et al. 2013), matplotlib (Hunter 2007), pandas (McKinney et al.
2010), NumPy (Walt 2011), astroquery (Ginsburg et al. 2019),
sklearn (Pedregosa et al. 2011), emcee (Foreman-Mackey et al.
2013), PTEMCEE (Vousden et al. 2016), TRICERATOPS
(Giacalone et al. 2021), LATTE (Eisner et al. 2020a), lightkurve
(Lightkurve Collaboration et al. 2018), pyaneti (Barragán et al.
2022a), ORBITIZE! (Blunt et al. 2020), Mercury (Chambers
1999), corner (Foreman-Mackey 2016).
## Acknowledgments

We would like to thank all of the planet hunters who have taken part in the Planet Hunters TESS citizen science project over the past six years. Without all of their dedicated work, many of whom have been part of the project ab initio, this exciting system would not have been found.

We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.

We thank the Observatoire de Haute-Provence (CNRS) staff for its support. This work was supported by the “Programme National de Planétologie” (PNP) of CNRS/INSU.” Some of the observations in this paper made use of the high-resolution imaging instrument ‘Alopeke and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).

N.E. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant number 1829740, the Brinson Foundation, and the Moore Foundation. C.A.C. acknowledges that this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). N.S. acknowledges support from the National Science Foundation through the Graduate Research Fellowship Program under grant 1842402. J.V.Z. acknowledges support from the Future Investigators in NASA Earth and Space Science and Technology (FINESST) grant 80NSSC22K1606. J.M.A.M. acknowledges support from the National Science Foundation Graduate Research Fellowship Program under grant number DGE-1842400 and from NASA’s Interdisciplinary Consortia for Astrobiology Research (NNH19ZDA001N-ICAR) under award number 19-ICAR19_2-0041. Xavier Delfosse acknowledges support by the French National Research Agency in the framework of the Investissements d’Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life” project of the Grenoble-Alpes University. F.K. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (COBREX; grant agreement number 885593), and from the Initiative de Recherches Interdisciplinaires et Stratégiques (IRIS) of Université PSL “Origines et Conditions d’Apparition de la Vie (OCAV)”. E.M. acknowledges funding from FAPEMIG under project number APQ-02493-22 and a research productivity grant number 309829/2022-4 awarded

by the CNPq, Brazil. CJ gratefully acknowledges support from the Netherlands Research School of Astronomy (NOVA) and from the Research Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM).

Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected with the TESS mission, obtained from the MAST data archive at STScI. Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Finally, N.E. and S.G. wish to thank the Harry Potter franchise for providing us with the in-house nickname for this system of *Percival*, inspired by Albus Percival Wulfric Brian Dumbledore’s wisdom.

*Facilities:* TESS, OHP/SOPHIE, Gemini North/‘Alopeke, Keck/HIRES, Palomar/PHARO, WIYN/NESSI, Keck II/NIRC2.

## ORCID iDs

Nora L. Eisner https://orcid.org/0000-0002-9138-9028

Samuel K. Grunblatt https://orcid.org/0000-0003-4976-9980

Oscar Barragán https://orcid.org/0000-0003-0563-0493

Thea H. Faridani https://orcid.org/0000-0003-3799-3635

Chris Lintott https://orcid.org/0000-0001-5578-359X

Suzanne Aigrain https://orcid.org/0000-0003-1453-0574

Cole Johnston https://orcid.org/0000-0002-3054-4135

Keivan G. Stassun https://orcid.org/0000-0002-3481-9052

Megan Bedell https://orcid.org/0000-0001-9907-7742

Andrew W. Boyle https://orcid.org/0000-0001-6037-2971

David R. Ciardi https://orcid.org/0000-0002-5741-3047

Catherine A. Clark https://orcid.org/0000-0002-2361-5812

David W. Hogg https://orcid.org/0000-0003-2866-9403

Steve B. Howell https://orcid.org/0000-0002-2532-2853

Joe Llama https://orcid.org/0000-0003-4450-0368

Joshua N. Winn https://orcid.org/0000-0002-4265-047X

Lily L. Zhao https://orcid.org/0000-0002-3852-3590

Joseph M. Akana Murphy https://orcid.org/0000-0001-8898-8284

Corey Beard https://orcid.org/0000-0001-7708-2364

Casey L. Brinkman https://orcid.org/0000-0002-4480-310X

Ashley Chontos https://orcid.org/0000-0003-1125-2564

Pia Cortes-Zuleta https://orcid.org/0000-0002-6174-4666

Steven Giacalone https://orcid.org/0000-0002-8965-3969

Emily A. Gilbert https://orcid.org/0000-0002-0388-8004

Rae Holcomb https://orcid.org/0000-0002-5034-9476

Jon M. Jenkins https://orcid.org/0000-0002-4715-9460

Flavien Kiefer https://orcid.org/0000-0001-9129-4929

Jack Lubin https://orcid.org/0000-0001-8342-7736

Eder Martioli https://orcid.org/0000-0002-5084-168X

Alex S. Polanski https://orcid.org/0000-0001-7047-8681

Nicholas Saunders https://orcid.org/0000-0003-2657-3889

Sara Seager https://orcid.org/0000-0002-6892-6948

Avi Shporer https://orcid.org/0000-0002-1836-3120

Dakotah Tyler https://orcid.org/0000-0003-0298-4667
## Acknowledgments

We would like to thank all of the planet hunters who have taken part in the Planet Hunters TESS citizen science project over the past six years. Without all of their dedicated work, many of whom have been part of the project ab initio, this exciting system would not have been found.

We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.

We thank the Observatoire de Haute-Provence (CNRS) staff for its support. This work was supported by the “Programme National de Planétologie” (PNP) of CNRS/INSU.” Some of the observations in this paper made use of the high-resolution imaging instrument ‘Alopeke and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).

N.E. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant number 1829740, the Brinson Foundation, and the Moore Foundation. C.A.C. acknowledges that this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). N.S. acknowledges support from the National Science Foundation through the Graduate Research Fellowship Program under grant 1842402. J.V.Z. acknowledges support from the Future Investigators in NASA Earth and Space Science and Technology (FINESST) grant 80NSSC22K1606. J.M.A.M. acknowledges support from the National Science Foundation Graduate Research Fellowship Program under grant number DGE-1842400 and from NASA’s Interdisciplinary Consortia for Astrobiology Research (NNH19ZDA001N-ICAR) under award number 19-ICAR19_2-0041. Xavier Delfosse acknowledges support by the French National Research Agency in the framework of the Investissements d’Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life” project of the Grenoble-Alpes University. F.K. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (COBREX; grant agreement number 885593), and from the Initiative de Recherches Interdisciplinaires et Stratégiques (IRIS) of Université PSL “Origines et Conditions d’Apparition de la Vie (OCAV)”. E.M. acknowledges funding from FAPEMIG under project number APQ-02493-22 and a research productivity grant number 309829/2022-4 awarded

by the CNPq, Brazil. CJ gratefully acknowledges support from the Netherlands Research School of Astronomy (NOVA) and from the Research Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM).

Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected with the TESS mission, obtained from the MAST data archive at STScI. Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Finally, N.E. and S.G. wish to thank the Harry Potter franchise for providing us with the in-house nickname for this system of *Percival*, inspired by Albus Percival Wulfric Brian Dumbledore’s wisdom.

*Facilities:* TESS, OHP/SOPHIE, Gemini North/‘Alopeke, Keck/HIRES, Palomar/PHARO, WIYN/NESSI, Keck II/NIRC2.

## ORCID iDs

Nora L. Eisner https://orcid.org/0000-0002-9138-9028

Samuel K. Grunblatt https://orcid.org/0000-0003-4976-9980

Oscar Barragán https://orcid.org/0000-0003-0563-0493

Thea H. Faridani https://orcid.org/0000-0003-3799-3635

Chris Lintott https://orcid.org/0000-0001-5578-359X

Suzanne Aigrain https://orcid.org/0000-0003-1453-0574

Cole Johnston https://orcid.org/0000-0002-3054-4135

Keivan G. Stassun https://orcid.org/0000-0002-3481-9052

Megan Bedell https://orcid.org/0000-0001-9907-7742

Andrew W. Boyle https://orcid.org/0000-0001-6037-2971

David R. Ciardi https://orcid.org/0000-0002-5741-3047

Catherine A. Clark https://orcid.org/0000-0002-2361-5812

David W. Hogg https://orcid.org/0000-0003-2866-9403

Steve B. Howell https://orcid.org/0000-0002-2532-2853

Joe Llama https://orcid.org/0000-0003-4450-0368

Joshua N. Winn https://orcid.org/0000-0002-4265-047X

Lily L. Zhao https://orcid.org/0000-0002-3852-3590

Joseph M. Akana Murphy https://orcid.org/0000-0001-8898-8284

Corey Beard https://orcid.org/0000-0001-7708-2364

Casey L. Brinkman https://orcid.org/0000-0002-4480-310X

Ashley Chontos https://orcid.org/0000-0003-1125-2564

Pia Cortes-Zuleta https://orcid.org/0000-0002-6174-4666

Steven Giacalone https://orcid.org/0000-0002-8965-3969

Emily A. Gilbert https://orcid.org/0000-0002-0388-8004

Rae Holcomb https://orcid.org/0000-0002-5034-9476

Jon M. Jenkins https://orcid.org/0000-0002-4715-9460

Flavien Kiefer https://orcid.org/0000-0001-9129-4929

Jack Lubin https://orcid.org/0000-0001-8342-7736

Eder Martioli https://orcid.org/0000-0002-5084-168X

Alex S. Polanski https://orcid.org/0000-0001-7047-8681

Nicholas Saunders https://orcid.org/0000-0003-2657-3889

Sara Seager https://orcid.org/0000-0002-6892-6948

Avi Shporer https://orcid.org/0000-0002-1836-3120

Dakotah Tyler https://orcid.org/0000-0003-0298-4667
Judah Van Zandt https://orcid.org/0000-0002-4290-6826

Daval J. Amratlal https://orcid.org/0009-0004-3918-7244

Milton K. D Bosch https://orcid.org/0000-0002-9766-2400

Lisa Stiller https://orcid.org/0000-0002-1825-7133

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Shappee, B. J., Prieto, J. L., Grupe, D., et al. 2014, ApJ, 788, 48
Judah Van Zandt https://orcid.org/0000-0002-4290-6826

Daval J. Amratlal https://orcid.org/0009-0004-3918-7244

Milton K. D Bosch https://orcid.org/0000-0002-9766-2400

Lisa Stiller https://orcid.org/0000-0002-1825-7133

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