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1. TESS Spots a Super-Puff: The Remarkably Low Density of TOI-1420b

Author

Yoshida, Stephanie, Vissapragada, Shreyas, Latham, David W., Bieryla, Allyson, Thorngren, Daniel P., Eastman, Jason D., López-Morales, Mercedes, Barkaoui, Khalid, Beichmam, Charles, Berlind, Perry, Buchave, Lars A., Calkins, Michael L., Ciardi, David R., Collins, Karen A., Cosentino, Rosario, Crossfield, Ian J. M., Dai, Fei, DiTomasso, Victoria, Dowling, Nicholas, Esquerdo, Gilbert A., Forés-Toribio, Raquel, Ghedina, Adriano, Goliguzova, Maria V., Golub, Eli, Gonzales, Erica J., Horta, Ferran Grau, Higuera, Jesus, Hoch, Nora, Horne, Keith, Howell, Steve B., Jenkins, Jon M., Klusmeyer, Jessica, Laloum, Didier, Lissauer, Jack J., Logsdon, Sarah E., Malavolta, Luca, Matson, Rachel A., Matthews, Elisabeth C., McLeod, Kim K., Medina, Jennifer V., Muñoz, Jose A., Osborn, Hugh P., Safonov, Boris, Schlieder, Joshua, Schmidt, Michael, Schweiker, Heidi, Seager, Sara, Sozzetti, Alessandro, Srdoc, Gregor, Stefánsson, Guđmundur, Strakhov, Ivan A., Striegel, Stephanie, Villaseñor, Joel, and Winn, Joshua N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery of TOI-1420b, an exceptionally low-density ($\rho = 0.08\pm0.02$ g cm$^{-3}$) transiting planet in a $P = 6.96$ day orbit around a late G dwarf star. Using transit observations from TESS, LCOGT, OPM, Whitin, Wendelstein, OAUV, Ca l'Ou, and KeplerCam along with radial velocity observations from HARPS-N and NEID, we find that the planet has a radius of $R_p$ = 11.9 $\pm$ 0.3 $R_\Earth$ and a mass of $M_p$ = 25.1 $\pm$ 3.8 $M_\Earth$. TOI-1420b is the largest-known planet with a mass less than $50M_\Earth$, indicating that it contains a sizeable envelope of hydrogen and helium. We determine TOI-1420b's envelope mass fraction to be $f_{env} = 82^{+7}_{-6}\%$, suggesting that runaway gas accretion occurred when its core was at most $4-5\times$ the mass of the Earth. TOI-1420b is similar to the planet WASP-107b in mass, radius, density, and orbital period, so a comparison of these two systems may help reveal the origins of close-in low-density planets. With an atmospheric scale height of 1950 km, a transmission spectroscopy metric of 580, and a predicted Rossiter-McLaughlin amplitude of about $17$ m s$^{-1}$, TOI-1420b is an excellent target for future atmospheric and dynamical characterization.

Published
2023

2. Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

Author

DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martínez, Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, and Wilson, Thomas G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to $P=24.422\pm0.014$ days, $K=3.19\pm0.27$ m/s, $M$ sin $i = 10.6 \pm 1.2 M_\oplus$, and $a = 0.142 \pm0.005$ au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries., Comment: Accepted for publication in AJ, 29 pages, 17 figures

Published
2022
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3. Signatures of Clouds in Hot Jupiter Atmospheres: Modeled High Resolution Emission Spectra from 3D General Circulation Models

Author

Harada, Caleb K., Kempton, Eliza M. -R., Rauscher, Emily, Roman, Michael, Malsky, Isaac, Brinjikji, Marah, and diTomasso, Victoria

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations of scattered light and thermal emission from hot Jupiter exoplanets have suggested the presence of inhomogeneous aerosols in their atmospheres. 3D general circulation models (GCMs) that attempt to model the effects of aerosols have been developed to understand the physical processes that underlie their dynamical structures. In this work, we investigate how different approaches to aerosol modeling in GCMs of hot Jupiters affect high-resolution thermal emission spectra throughout the duration of the planet's orbit. Using results from a GCM with temperature-dependent cloud formation, we calculate spectra of a representative hot Jupiter with different assumptions regarding the vertical extent and thickness of clouds. We then compare these spectra to models in which clouds are absent or simply post-processed (i.e., added subsequently to the completed clear model). We show that the temperature-dependent treatment of clouds in the GCM produces high-resolution emission spectra that are markedly different from the clear and post-processed cases -- both in the continuum flux levels and line profiles -- and that increasing the vertical extent and thickness of clouds leads to bigger changes in these features. We evaluate the net Doppler shifts of the spectra induced by global winds and the planet's rotation and show that they are strongly phase-dependent, especially for models with thicker and more extended clouds. This work further demonstrates the importance of radiative feedback in cloudy atmospheric models of hot Jupiters, as this can have a significant impact on interpreting spectroscopic observations of exoplanet atmospheres., Comment: 23 pages, 10 figures, 2 tables, 1 animation (Fig. 6: https://tinyurl.com/v69ljww), ApJ accepted

Published
2019
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4. Radial Velocities, Space Motions, and Nearby Young Moving Group Memberships of Eleven Candidate Young Brown Dwarfs

Author

Riedel, Adric R., DiTomasso, Victoria, Rice, Emily L., Alam, Munazza K., Abrahams, Ellianna, Crook, James, Cruz, Kelle L., and Faherty, Jacqueline K.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present new radial velocity (RV) measurements for 11 candidate young very-low-mass stars and brown dwarfs, with spectral types from M7 to L7. Candidate young objects were identified by features indicative of low surface gravity in their optical and/or near-infrared spectra. RV measurements are derived from high resolution (R=$\lambda$/$\Delta\lambda$=20,000) $J$ band spectra taken with NIRSPEC at the Keck Observatory. We combine RVs with proper motions and trigonometric distances to calculate three-dimensional space positions and motions and to evaluate membership probabilities for nearby young moving groups (NYMGs). We propose 2MASS J00452143+1634446 (L2$\beta$, $J$=13.06) as an RV standard given the precision and stability of measurements from three different studies. We test the precision and accuracy of our RV measurements as a function of spectral type of the comparison object, finding that RV results are essentially indistinguishable even with differences of $\pm$5 spectral subtypes. We also investigate the strengths of gravity-sensitive K~{\sc i} lines at 1.24--1.25 $\mu$m and evaluate their consistency with other age indicators. We confirm or re-confirm four brown dwarf members of NYMGs -- 2MASS J00452143+1634446, WISE J00470038+6803543, 2MASS J01174748$-$3403258, and 2MASS J19355595$-$2846343 -- and their previous age estimates. We identify one new brown dwarf member of the Carina-Near moving group, 2MASS J21543454$-$1055308. The remaining objects do not appear to be members of any known NYMGs, despite their spectral signatures of youth. These results add to the growing number of very-low-mass objects exhibiting signatures of youth that lack likely membership in a known NYMG, thereby compounding the mystery regarding local, low-density star formation., Comment: 24 pages, 10 figures, 6 tables. Accepted by AJ

Published
2019
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5. TESS Spots a Super-puff: The Remarkably Low Density of TOI-1420b

Author

Yoshida, Stephanie, primary, Vissapragada, Shreyas, additional, Latham, David W., additional, Bieryla, Allyson, additional, Thorngren, Daniel P., additional, Eastman, Jason D., additional, López-Morales, Mercedes, additional, Barkaoui, Khalid, additional, Beichman, Charles, additional, Berlind, Perry, additional, Buchave, Lars A., additional, Calkins, Michael L., additional, Ciardi, David R., additional, Collins, Karen A., additional, Cosentino, Rosario, additional, Crossfield, Ian J. M., additional, Dai, Fei, additional, DiTomasso, Victoria, additional, Dowling, Nicholas, additional, Esquerdo, Gilbert A., additional, Forés-Toribio, Raquel, additional, Ghedina, Adriano, additional, Goliguzova, Maria V., additional, Golub, Eli, additional, Gonzales, Erica J., additional, Horta, Ferran Grau, additional, Higuera, Jesus, additional, Hoch, Nora, additional, Horne, Keith, additional, Howell, Steve B., additional, Jenkins, Jon M., additional, Klusmeyer, Jessica, additional, Laloum, Didier, additional, Lissauer, Jack J., additional, Logsdon, Sarah E., additional, Malavolta, Luca, additional, Matson, Rachel A., additional, Matthews, Elisabeth C., additional, McLeod, Kim K., additional, Medina, Jennifer V., additional, Muñoz, Jose A., additional, Osborn, Hugh P., additional, Safonov, Boris, additional, Schlieder, Joshua, additional, Schmidt, Michael, additional, Schweiker, Heidi, additional, Seager, Sara, additional, Sozzetti, Alessandro, additional, Srdoc, Gregor, additional, Stefánsson, Guđmundur, additional, Strakhov, Ivan A., additional, Striegel, Stephanie, additional, Villaseñor, Joel, additional, and Winn, Joshua N., additional

Published
2023
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6. LHS 1903 provides evidence for gas-depleted formation of planets around M-dwarfs

Author

Wilson, Thomas, primary, Simpson, Anna, additional, Cameron, Andrew Collier, additional, Cloutier, Ryan, additional, Adibekyan, Vardan, additional, John, Ancy Anna, additional, Alibert, Y, additional, Stalport, Manu, additional, Egger, J, additional, Bonfanti, Andrea, additional, Billot, Nicolas, additional, Guterman, Pascal, additional, Maxted, Pierre, additional, Simon, Attila, additional, Sousa, Sergio, additional, Fridlund, Malcolm, additional, Beck, M, additional, Bekkelien, Anja, additional, Salmon, S, additional, Grootel, Valerie Van, additional, Fossati, Luca, additional, Mustill, Alexander, additional, Osborn, Hugh, additional, Zingales, Tiziano, additional, Hooton, M, additional, Affer, Laura, additional, Aigrain, Suzanne, additional, Alonso, Roi, additional, Anglada-Escude, G, additional, Antoniadis-Karnavas, Alexandros, additional, Barczy, T, additional, Barrado, David, additional, Barros, Susana, additional, Baumjohann, Wolfgang, additional, Beck, T, additional, Benz, W, additional, Biondi, Federico, additional, Bonfils, Xavier, additional, Borsato, Luca, additional, Brandeker, Alexis, additional, Broeg, Christopher, additional, Buchhave, Lars, additional, Buder, Maximilian, additional, Cabrera, Juan, additional, Gaxiola, S Carrazco, additional, Charnoz, Sébastien, additional, Ciardi, David, additional, Collins, Karen, additional, Collins, Kevin, additional, Cosentino, Rosario, additional, Csizmadia, Szilard, additional, Cubillos, P, additional, Dalal, Shweta, additional, Damasso, Mario, additional, Davenport, James, additional, Davies, Melvyn, additional, Deleuil, Magali, additional, Delrez, L, additional, Demangeon, Olivier, additional, Demory, Brice-Olivier, additional, DiTomasso, Victoria, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Dumusque, Xavier, additional, Ehrenreich, David, additional, Erikson, Anders, additional, Esparza-Borges, Emma, additional, Fortier, Andrea, additional, Fukuda, Izuru, additional, Fukui, Akihiko, additional, Gandolfi, Davide, additional, Ghedina, Adriano, additional, Giacalone, Steven, additional, Gill, Holden, additional, Gillon, Michaël, additional, Chew, Y Gomez Maqueo, additional, Güdel, Manuel, additional, Guerra, Pere, additional, Günther, Maximilian, additional, Hara, Nathan, additional, Harutyunyan, Avet, additional, Hayashi, Yuya, additional, Haywood, Raphaëlle, additional, Holcomb, Rae, additional, Horne, Keith, additional, Hoyer, S, additional, Huang, Chelsea, additional, Ikoma, Masahiro, additional, Isaak, K, additional, Jackman, James, additional, Jenkins, Jon, additional, Jensen, Eric, additional, Jontof-Hutter, Daniel, additional, Kawai, Yugo, additional, Kiss, Laszlo, additional, Lakeland, Ben, additional, Laskar, J, additional, Latham, David, additional, des Etangs, Alain Lecavelier, additional, Leleu, Adrien, additional, Lendl, Monika, additional, de Leon, J, additional, Lienhard, Florian, additional, López-Morales, Mercedes, additional, Lovis, Christophe, additional, Lund, Michael, additional, Luque, Rafael, additional, Magrin, D, additional, Malavolta, Luca, additional, Fiorenzano, Aldo, additional, Mayo, Andrew, additional, Mayor, Michel, additional, Mordasini, C, additional, Mortier, Annelies, additional, Murgas, Felipe, additional, Narita, Norio, additional, Nascimbeni, Valerio, additional, Nicholson, Belinda, additional, Olofsson, Göran, additional, Ottensamer, Roland, additional, Pagano, Isabella, additional, Palethorpe, Larissa, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Pedani, Marco, additional, Pepe, Francesco, additional, Peter, Gisbert, additional, Pinamonti, Matteo, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Poretti, Ennio, additional, Queloz, Didier, additional, Quinn, Sam, additional, Ragazzoni, R, additional, Rando, N, additional, Rapetti, David, additional, Ratti, F, additional, Rauer, Heike, additional, Rescigno, Federica, additional, Ribas, Ignasi, additional, Rice, William, additional, Ricker, George, additional, Robertson, Paul, additional, de Roche, Thierry, additional, Sabin, L, additional, Santos, Nuno, additional, Sasselov, Dimitar, additional, Savel, Arjun, additional, Scandariato, Gaetano, additional, Schanche, Nicole, additional, Schroffenegger, Urs, additional, Schwarz, Richard, additional, Seager, Sara, additional, Sefako, Ramotholo, additional, Ségransan, Damien, additional, Shporer, Avi, additional, Silva, André, additional, Smith, Alexis, additional, Sozzetti, Alessandro, additional, Steller, Manfred, additional, Szabo, Gyula, additional, Tamura, Motohide, additional, Thomas, Nicolas, additional, Tuson, Amy, additional, Udry, Stéphane, additional, Vanderburg, Andrew, additional, Vanderspek, Roland, additional, Venturini, J, additional, Verrecchia, Francesco, additional, Walton, Nicholas, additional, Watson, Christopher, additional, Wells, Robert, additional, Winn, Joshua, additional, Zambelli, Roberto, additional, and Ziegler, Carl, additional

Published
2023
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7. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author

DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Collier Cameron, Andrew, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Martínez Fiorenzano, A. F., Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, Wilson, Thomas G., DiTomasso, Victoria, Nava, Chantanelle, López-Morales, Mercedes, Bieryla, Allyson, Cloutier, Ryan, Malavolta, Luca, Mortier, Annelies, Buchhave, Lars A., Stassun, Keivan G., Sozzetti, Alessandro, Bonomo, Aldo Stefano, Charbonneau, David, Collier Cameron, Andrew, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Martínez Fiorenzano, A. F., Ghedina, Adriano, Harutyunyan, Avet, Haywood, R. D., Latham, David, Molinari, Emilio, Pepe, Francesco A., Pinamonti, Matteo, Poretti, Ennio, Rice, Ken, Sasselov, Dimitar, Stalport, Manu, Udry, Stéphane, Watson, Christopher, and Wilson, Thomas G.

Abstract

We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD 79210 and HD 79211, two M0V members of a gravitationally bound binary system. We detect a planet candidate with a period of days around HD 79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES, and RVs spanning a total of 25 yr, we further refine the planet candidate parameters to P = 24.422 ± 0.014 days, K = 3.19 ± 0.27 m s−1, M sin i = 10.6 ± 1.2M⊕, and a = 0.142 ± 0.005 au. We do not find any additional planet candidate signals in the data of HD 79211, nor do we find any planet candidate signals in HD 79210. This system adds to the number of exoplanets detected in binaries with M-dwarf members and serves as a case study for planet formation in stellar binaries.

Published
2023

8. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author

DiTomasso, Victoria, primary, Nava, Chantanelle, additional, López-Morales, Mercedes, additional, Bieryla, Allyson, additional, Cloutier, Ryan, additional, Malavolta, Luca, additional, Mortier, Annelies, additional, Buchhave, Lars A., additional, Stassun, Keivan G., additional, Sozzetti, Alessandro, additional, Bonomo, Aldo Stefano, additional, Charbonneau, David, additional, Collier Cameron, Andrew, additional, Cosentino, Rosario, additional, Damasso, Mario, additional, Dumusque, Xavier, additional, Martínez Fiorenzano, A. F., additional, Ghedina, Adriano, additional, Harutyunyan, Avet, additional, Haywood, R. D., additional, Latham, David, additional, Molinari, Emilio, additional, Pepe, Francesco A., additional, Pinamonti, Matteo, additional, Poretti, Ennio, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Stalport, Manu, additional, Udry, Stéphane, additional, Watson, Christopher, additional, and Wilson, Thomas G., additional

Published
2023
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9. The Search for the 24.4 Day Planet Candidate Around HD79211 with HARPS-N

Author

DiTomasso, Victoria

Subjects
HARPS-N, exoplanets, stellar binary, radial velocities, rotation period
Abstract

M dwarfs are the focus of many exoplanet studies and as many as 46% of M dwarfs are members of binaries, but as few as 30 exoplanets (less than 7% of the total found around M-dwarfs) have been detected in M dwarf binaries so far. HD79210 and HD79211 are two M0V members of a gravitationally-bound binary system located 6.3 pc from Earth. Using new photometric observations from KeplerCam on the 1.2 m telescope at the Fred Lawrence Whipple Observatory (FLWO) we collected from Feb-Jun 2021, we constrain the rotation period of HD79211 to approximately 17.5 days. Using high-precision radial velocities from the HARPS-N spectrograph on the 3.6 m Telescopio Nazionale Galileo (TNG) in La Palma, Spain, we detect a signal with a period of 24.423days, which was originally identified in CARMENES radial velocity data alone. Using HARPS-N, CARMENES and HIRES radial velocities spanning a total of 23 years (June 1997-Feb 2020), we further refine the planet candidate parameters to P=24.418days, K=3.21 m/s, Msin i = 10.6 MEarth, and a = 0.1419 AU. We do not find any additional planet candidate signals in the data of HD79211.

Published
2022
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11. Mapping M Dwarf Metallicities

Author

DiTomasso, Victoria and Schmidt, Sarah J.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We use distances derived from Gaia parallaxes cross-matched with SDSS, WISE and 2MASS photometry to assemble a sample of approximately 2 million M dwarfs, defined as stars with SDSS colors redder than r-i = 0.3 and i-z = 0.2. Previous work has found relations between SDSS r-z and WISE W1-W2 colors and the effective temperature and metallicities of cool stars (3550-4200 K). Using our sample and these previously derived relationships, we measure these stars' metallicities and effective temperatures. We calculate the metallicity distribution gradient as a function of galactic height for M dwarfs within 1000 pc of the Sun, which ultimately lends insight to the kinematic and chemical evolution of the Galaxy., {"references":["Cheng, J. Y., et al. Metallicity Gradients in the Milky Way Disk as Observed by the SEGUE Survey","Davenport, J. R. A. & Dorn-Wallenstein, T. Z., Photometric Metallicities for Low-mass Stars with Gaia and WISE","Garcia Perez, A. E., et al. (2015) ASPCAP: The APOGEE Stellar Parameter and Chemical Abundances Pipeline","Green, G. M., et al. (2018) Galactic reddening in 3D from stellar photometry - an improved map","Hartkopf, W.I. & Yoss, K.M. (1982) A Kinematic and Abundance Survey at the Galactic Poles","Schlesinger, K.J., et al. (2014) The Vertical Metallicity Gradient of the Milky Way Disk: Transitions in [α/Fe] Populations","Schmidt, S. J., et al. (2016) Examining the relationships between colour, Teff, and [M/H] for APOGEE K and M dwarfs","Woolf, V. M. & West, A. A. (2012) The M dwarf problem in the Galaxy"]}

Published
2019
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14. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author

Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson, DiTomasso, Victoria [0000-0003-0741-7661], Nava, Chantanelle [0000-0001-8838-3883], López-Morales, Mercedes [0000-0003-3204-8183], Bieryla, Allyson [0000-0001-6637-5401], Cloutier, Ryan [0000-0001-5383-9393], Malavolta, Luca [0000-0002-6492-2085], Mortier, Annelies [0000-0001-7254-4363], Buchhave, Lars A [0000-0003-1605-5666], Stassun, Keivan G [0000-0002-3481-9052], Sozzetti, Alessandro [0000-0002-7504-365X], Bonomo, Aldo Stefano [0000-0002-6177-198X], Charbonneau, David [0000-0002-9003-484X], Collier Cameron, Andrew [0000-0002-8863-7828], Cosentino, Rosario [0000-0003-1784-1431], Damasso, Mario [0000-0001-9984-4278], Dumusque, Xavier [0000-0002-9332-2011], Martínez Fiorenzano, AF [0000-0002-4272-4272], Ghedina, Adriano [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Latham, David [0000-0001-9911-7388], Molinari, Emilio [0000-0002-1742-7735], Pinamonti, Matteo [0000-0002-4445-1845], Poretti, Ennio [0000-0003-1200-0473], Rice, Ken [0000-0002-6379-9185], Sasselov, Dimitar [0000-0001-7014-1771], Stalport, Manu [0000-0003-0996-6402], Udry, Stéphane [0000-0001-7576-6236], Watson, Christopher [0000-0002-9718-3266], Wilson, Thomas G [0000-0001-8749-1962], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, The Solar System, Exoplanets, and Astrobiology, Exoplanets, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, Astrobiology, M dwarf stars, Binary stars, QC Physics, Rare Diseases, Space and Planetary Science, astro-ph.EP, QB Astronomy, Exoplanet detection methods, Solar System, 51 Physical Sciences, QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to $P=24.422\pm0.014$ days, $K=3.19\pm0.27$ m/s, $M$ sin $i = 10.6 \pm 1.2 M_\oplus$, and $a = 0.142 \pm0.005$ au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries., Comment: Accepted for publication in AJ, 29 pages, 17 figures

Published
2023

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