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1. The GAPS Programme at TNG XXXIX -- Multiple molecular species in the atmosphere of the warm giant planet WASP-80 b unveiled at high resolution with GIANO-B

Author

Carleo, Ilaria, Giacobbe, Paolo, Guilluy, Gloria, Cubillos, Patricio E., Bonomo, Aldo S., Sozzetti, Alessandro, Brogi, Matteo, Gandhi, Siddharth, Fossati, Luca, Turrini, Diego, Biazzo, Katia, Borsa, Francesco, Lanza, Antonino F., Malavolta, Luca, Maggio, Antonio, Mancini, Luigi, Micela, Giusi, Pino, Lorenzo, Poretti, Ennio, Rainer, Monica, Scandariato, Gaetano, Schisano, Eugenio, Andreuzzi, Gloria, Bignamini, Andrea, Cosentino, Rosario, Fiorenzano, Aldo, Harutyunyan, Avet, Molinari, Emilio, Pedani, Marco, Redfield, Seth, and Stoev, Hristo

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is still unknown. We observed four transits of WASP-80 b, a warm transiting giant planet orbiting a late-K dwarf star with the near-infrared GIANO-B spectrograph installed at the Telescopio Nazionale Galileo and performed high resolution transmission spectroscopy analysis. We report the detection of several molecular species in its atmosphere. Combining the four nights and comparing our transmission spectrum to planetary atmosphere models containing the signature of individual molecules within the cross-correlation framework, we find the presence of H2O, CH4, NH3 and HCN with high significance, tentative detection of CO2, and inconclusive results for C2H2 and CO. A qualitative interpretation of these results, using physically motivated models, suggests an atmosphere consistent with solar composition and the presence of disequilibrium chemistry and we therefore recommend the inclusion of the latter in future modelling of sub-1000K planets., Comment: 12 pages, 4 figures. AJ, Accepted July 11th, 2022

Published
2022
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2. A super-massive Neptune-sized planet

Author

Naponiello, Luca, Mancini, Luigi, Sozzetti, Alessandro, Bonomo, Aldo S., Morbidelli, Alessandro, Dou, Jingyao, Zeng, Li, Leinhardt, Zoe M., Biazzo, Katia, Cubillos, Patricio E., Pinamonti, Matteo, Locci, Daniele, Maggio, Antonio, Damasso, Mario, Lanza, Antonino F., Lissauer, Jack J., Collins, Karen A., Carter, Philip J., Jensen, Eric L. N., Bignamini, Andrea, Boschin, Walter, Bouma, Luke G., Ciardi, David R., Cosentino, Rosario, Crossfield, Ian, Desidera, Silvano, Dumusque, Xavier, Fiorenzano, Aldo F. M., Fukui, Akihiko, Giacobbe, Paolo, Gnilka, Crystal L., Ghedina, Adriano, Guilluy, Gloria, Harutyunyan, Avet, Howell, Steve B., Jenkins, Jon M., Lund, Michael B., Kielkopf, John F., Lester, Katie V., Malavolta, Luca, Mann, Andrew W., Matson, Rachel A., Matthews, Elisabeth C., Nardiello, Domenico, Narita, Norio, Pace, Emanuele, Pagano, Isabella, Palle, Enric, Pedani, Marco, Seager, Sara, Schlieder, Joshua E., Schwarz, Richard P., Shporer, Avi, Twicken, Joseph D., Winn, Joshua N., Ziegler, Carl, and Zingales, Tiziano

Published
2023
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3. On The Synergy Between Ariel And Ground-Based High-Resolution Spectroscopy

Author

Guilluy, Gloria, Sozzetti, Alessandro, Giacobbe, Paolo, Bonomo, Aldo S., and Micela, Giuseppina

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Since the first discovery of an extra-solar planet around a main-sequence star, in 1995, the number of detected exoplanets has increased enormously. Over the past two decades, observational instruments (both onboard and on ground-based facilities) have revealed an astonishing diversity in planetary physical features (i. e. mass and radius), and orbital parameters (e.g. period, semi-major axis, inclination). Exoplanetary atmospheres provide direct clues to understand the origin of these differences through their observable spectral imprints. In the near future, upcoming ground and space-based telescopes will shift the focus of exoplanetary science from an era of 'species discovery' to one of 'atmospheric characterization'. In this context, the Atmospheric Remote-sensing Infrared Exoplanet Large (Ariel) survey, will play a key role. As it is designed to observe and characterize a large and diverse sample of exoplanets, Ariel will provide constraints on a wide gamut of atmospheric properties allowing us to extract much more information than has been possible so far (e.g. insights into the planetary formation and evolution processes). The low resolution spectra obtained with Ariel will probe layers different from those observed by ground-based high resolution spectroscopy, therefore the synergy between these two techniques offers a unique opportunity to understanding the physics of planetary atmospheres. In this paper, we set the basis for building up a framework to effectively utilise, at near-infrared wavelengths, high-resolution datasets (analyzed via the cross-correlation technique) with spectral retrieval analyses based on Ariel low-resolution spectroscopy. We show preliminary results, using a benchmark object, namely HD 209458 b, addressing the possibility of providing improved constraints on the temperature structure and molecular/atomic abundances., Comment: 24 pages,6 figures, accepted for publication in EXPA as EXPA-D-20-00055R2 ---- for the ARIEL Phase B Special Issue

Published
2021
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4. Ariel: Enabling planetary science across light-years

Author

Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Da Peppo, Vania, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Di Giorgio, Anna, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Van Eylen, Vincent, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Van der Swaelmen, Mathieu, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Del Vecchio, Ciro, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/

Published
2021

5. Five carbon- and nitrogen-bearing species in a hot giant planet's atmosphere

Author

Giacobbe, Paolo, Brogi, Matteo, Gandhi, Siddharth, Cubillos, Patricio E., Bonomo, Aldo S., Sozzetti, Alessandro, Fossati, Luca, Guilluy, Gloria, Carleo, Ilaria, Rainer, Monica, Harutyunyan, Avet, Borsa, Francesco, Pino, Lorenzo, Nascimbeni, Valerio, Benatti, Serena, Biazzo, Katia, Bignamini, Andrea, Chubb, Katy L., Claudi, Riccardo, Cosentino, Rosario, Covino, Elvira, Damasso, Mario, Desidera, Silvano, Fiorenzano, Aldo F. M., Ghedina, Adriano, Lanza, Antonino F., Leto, Giuseppe, Maggio, Antonio, Malavolta, Luca, Maldonado, Jesus, Micela, Giuseppina, Molinari, Emilio, Pagano, Isabella, Pedani, Marco, Piotto, Giampaolo, Poretti, Ennio, Scandariato, Gaetano, Yurchenko, Sergei N., Fantinel, Daniela, Galli, Alberto, Lodi, Marcello, Sanna, Nicoletta, and Tozzi, Andrea

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The atmospheres of gaseous giant exoplanets orbiting close to their parent stars (hot Jupiters) have been probed for nearly two decades. They allow us to investigate the chemical and physical properties of planetary atmospheres under extreme irradiation conditions. Previous observations of hot Jupiters as they transit in front of their host stars have revealed the frequent presence of water vapour and carbon monoxide in their atmospheres; this has been studied in terms of scaled solar composition under the usual assumption of chemical equilibrium. Both molecules as well as hydrogen cyanide were found in the atmosphere of HD 209458b, a well studied hot Jupiter (with equilibrium temperature around 1,500 kelvin), whereas ammonia was tentatively detected there and subsequently refuted. Here we report observations of HD 209458b that indicate the presence of water (H2O), carbon monoxide (CO), hydrogen cyanide (HCN), methane (CH4), ammonia (NH3) and acetylene (C2H2), with statistical significance of 5.3 to 9.9 standard deviations per molecule. Atmospheric models in radiative and chemical equilibrium that account for the detected species indicate a carbon-rich chemistry with a carbon-to-oxygen ratio close to or greater than 1, higher than the solar value (0.55). According to existing models relating the atmospheric chemistry to planet formation and migration scenarios, this would suggest that HD 209458b formed far from its present location and subsequently migrated inwards. Other hot Jupiters may also show a richer chemistry than has been previously found, which would bring into question the frequently made assumption that they have solar-like and oxygen-rich compositions., Comment: As part of the Springer Nature Content Sharing Initiative, it is possible to access a view-only version of this paper by using the following SharedIt link: https://rdcu.be/cifrz

Published
2021
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6. The GAPS Programme at TNG XXVIII -- A pair of hot-Neptunes orbiting the young star TOI-942

Author

Carleo, Ilaria, Desidera, Silvano, Nardiello, Domenico, Malavolta, Luca, Lanza, Antonino F., Livingston, John, Locci, Daniele, Marzari, Francesco, Messina, Sergio, Turrini, Diego, Baratella, Martina, Borsa, Francesco, D'Orazi, Valentina, Nascimbeni, Valerio, Pinamonti, Matteo, Rainer, Monica, Alei, Eleonora, Bignamini, Andrea, Gratton, Raffaele, Micela, Giuseppina, Montalto, Marco, Sozzetti, Alessandro, Squicciarini, Vito, Affer, Laura, Benatti, Serena, Biazzo, Katia, Bonomo, Aldo S., Claudi, Riccardo, Cosentino, Rosario, Covino, Elvira, Damasso, Mario, Esposito, Massimiliano, Fiorenzano, Aldo, Frustagli, Giuseppe, Giacobbe, Paolo, Harutyunyan, Avet, Leto, Giuseppe, Magazzú, Antonio, Maggio, Antonio, Mainella, Giovanni, Maldonado, Jesus, Mallonn, Matthias, Mancini, Luigi, Molinari, Emilio, Molinaro, Marco, Pagano, Isabella, Pedani, Marco, Piotto, Giampaolo, Poretti, Ennio, Redfield, Seth, and Scandariato, Gaetano

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Both young stars and multi-planet systems are primary objects that allow us to study, understand and constrain planetary formation and evolution theories. We validate the physical nature of two Neptune-type planets transiting TOI-942 (TYC 5909-319-1), a previously unacknowledged young star (50+30-20 Myr) observed by the TESS space mission in Sector 5. Thanks to a comprehensive stellar characterization, TESS light curve modelling and precise radial-velocity measurements, we validated the planetary nature of the TESS candidate and detect an additional transiting planet in the system on a larger orbit. From photometric and spectroscopic observations we performed an exhaustive stellar characterization and derived the main stellar parameters. TOI-942 is a relatively active K2.5V star (logR'hk = -4.17+-0.01) with rotation period Prot = 3.39+-0.01 days, a projected rotation velocity vsini=13.8+-0.5 km/s and a radius of ~0.9 Rsun. We found that the inner planet, TOI-942b, has an orbital period Pb=4.3263+-0.0011 days, a radius Rb=4.242-0.313+0.376 Rearth and a mass upper limit of 16 Mearth at 1-sigma confidence level. The outer planet, TOI-942c, has an orbital period Pc=10.1605-0.0053+0.0056 days, a radius Rc=4.793-0.351+0.410 Rearth and a mass upper limit of 37 Mearth at 1-sigma confidence level.

Published
2020
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7. TOI-1235 b: a keystone super-Earth for testing radius valley emergence models around early M dwarfs

Author

Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G., Nava, Chantanelle, Ment, Kristo, Lopez, Eric D., Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Tenenbaum, Peter, Sozzetti, Alessandro, Sha, Lizhou, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Roy, Arpita, Robertson, Paul, Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepper, Joshua, Pepe, Francesco, Molinari, Emilio, Mocnik, Teo, Micela, Giuseppina, Mayor, Michel, Fiorenzano, Aldo F. Martinez, Mallia, Franco, Lubin, Jack, Lovis, Christophe, López-Morales, Mercedes, Kosiarek, Molly R., Kielkopf, John F., Kane, Stephen R., Jensen, Eric L. N., Isopi, Giovanni, Huber, Daniel, Hill, Michelle L., Harutyunyan, Avet, Gonzales, Erica, Giacalone, Steven, Ghedina, Adriano, Ercolino, Andrea, Dumusque, Xavier, Dressing, Courtney D., Damasso, Mario, Dalba, Paul A., Cosentino, Rosario, Conti, Dennis M., Colón, Knicole D., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Christiansen, Jessie, Chontos, Ashley, Cecconi, Massimo, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Beichman, Charles, Behmard, Aida, Beard, Corey, and Murphy, Joseph M. Akana

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/non-rocky transition in period-radius space. Here we present the confirmation of TOI-1235 b ($P=3.44$ days, $r_p=1.738^{+0.087}_{-0.076}$ R$_{\oplus}$), a planet whose size and period are intermediate between the competing model predictions thus making the system an important test case for emergence models of the rocky/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$, which implies an iron core mass fraction of $20^{+15}_{-12}$% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like and we constrain a H/He envelope mass fraction to be $<0.5$% at 90% confidence. Our results are consistent with model predictions from thermally-driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remain efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically-determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin ($P=21.8^{+0.9}_{-0.8}$ days, $m_p\sin{i}=13.0^{+3.8}_{-5.3}$ M$_{\oplus}$) that cannot be firmly ruled out by our data., Comment: Accepted to The Astronomical Journal. 8 figures & 5 tables. Table 2 is provided in the arXiv source code

Published
2020
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8. Author Correction: A super-massive Neptune-sized planet

Author

Naponiello, Luca, Mancini, Luigi, Sozzetti, Alessandro, Bonomo, Aldo S., Morbidelli, Alessandro, Dou, Jingyao, Zeng, Li, Leinhardt, Zoe M., Biazzo, Katia, Cubillos, Patricio E., Pinamonti, Matteo, Locci, Daniele, Maggio, Antonio, Damasso, Mario, Lanza, Antonino F., Lissauer, Jack J., Collins, Karen A., Carter, Philip J., Jensen, Eric L. N., Bignamini, Andrea, Boschin, Walter, Bouma, Luke G., Ciardi, David R., Cosentino, Rosario, Crossfield, Ian, Desidera, Silvano, Dumusque, Xavier, Fiorenzano, Aldo F. M., Fukui, Akihiko, Giacobbe, Paolo, Gnilka, Crystal L., Ghedina, Adriano, Guilluy, Gloria, Harutyunyan, Avet, Howell, Steve B., Jenkins, Jon M., Lund, Michael B., Kielkopf, John F., Lester, Katie V., Malavolta, Luca, Mann, Andrew W., Matson, Rachel A., Matthews, Elisabeth C., Nardiello, Domenico, Narita, Norio, Pace, Emanuele, Pagano, Isabella, Palle, Enric, Pedani, Marco, Seager, Sara, Schlieder, Joshua E., Schwarz, Richard P., Shporer, Avi, Twicken, Joseph D., Winn, Joshua N., Ziegler, Carl, and Zingales, Tiziano

Published
2023
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10. SIOUX project: a simultaneous multiband camera for exoplanet atmospheres studies

Author

Christille, Jean Marc, Bonomo, Aldo Stefano, Borsa, Francesco, Busonero, Deborah, Calcidese, Paolo, Claudi, Riccardo, Damasso, Mario, Giacobbe, Paolo, Molinari, Emilio, Pace, Emanuele, Riva, Alberto, Sozzetti, Alessandro, Toso, Giorgio, and Tresoldi, Daniela

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The exoplanet revolution is well underway. The last decade has seen order-of-magnitude increases in the number of known planets beyond the Solar system. Detailed characterization of exoplanetary atmospheres provide the best means for distinguishing the makeup of their outer layers, and the only hope for understanding the interplay between initial composition chemistry, temperature-pressure atmospheric profiles, dynamics and circulation. While pioneering work on the observational side has produced the first important detections of atmospheric molecules for the class of transiting exoplanets, important limitations are still present due to the lack of sys- tematic, repeated measurements with optimized instrumentation at both visible (VIS) and near-infrared (NIR) wavelengths. It is thus of fundamental importance to explore quantitatively possible avenues for improvements. In this paper we report initial results of a feasibility study for the prototype of a versatile multi-band imaging system for very high-precision differential photometry that exploits the choice of specifically selected narrow-band filters and novel ideas for the execution of simultaneous VIS and NIR measurements. Starting from the fundamental system requirements driven by the science case at hand, we describe a set of three opto-mechanical solutions for the instrument prototype: 1) a radial distribution of the optical flux using dichroic filters for the wavelength separation and narrow-band filters or liquid crystal filters for the observations; 2) a tree distribution of the optical flux (implying 2 separate foci), with the same technique used for the beam separation and filtering; 3) an exotic solution consisting of the study of a complete optical system (i.e. a brand new telescope) that exploits the chromatic errors of a reflecting surface for directing the different wavelengths at different foci.

Published
2016
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11. Ground-breaking Exoplanet Science with the ANDES spectrograph at the ELT

Author

Palle, Enric, Biazzo, Katia, Bolmont, Emeline, Molliere, Paul, Poppenhaeger, Katja, Birkby, Jayne, Brogi, Matteo, Chauvin, Gael, Chiavassa, Andrea, Hoeijmakers, Jens, Lellouch, Emmanuel, Lovis, Christophe, Maiolino, Roberto, Nortmann, Lisa, Parviainen, Hannu, Pino, Lorenzo, Turbet, Martin, Wender, Jesse, Albrecht, Simon, Antoniucci, Simone, Barros, Susana C., Beaudoin, Andre, Benneke, Bjorn, Boisse, Isabelle, Bonomo, Aldo S., Borsa, Francesco, Brandeker, Alexis, Brandner, Wolfgang, Buchhave, Lars A., Cheffot, Anne-Laure, Deborde, Robin, Debras, Florian, Doyon, Rene, Di Marcantonio, Paolo, Giacobbe, Paolo, Hernandez, Jonay I. Gonzalez, Helled, Ravit, Kreidberg, Laura, Machado, Pedro, Maldonado, Jesus, Marconi, Alessandro, Martins, B. L. Canto, Miceli, Adriano, Mordasini, Christoph, N'Diaye, Mamadou, Niedzielski, Andrezj, Nisini, Brunella, Origlia, Livia, Peroux, Celine, Pietrow, Alex G. M., Pinna, Enrico, Rauscher, Emily, Reffert, Sabine, Rousselot, Philippe, Sanna, Nicoletta, Simonnin, Adrien, Mascareno, Alejandro Suarez, Zanutta, Alessio, Zechmeister, Mathias, Palle, Enric, Biazzo, Katia, Bolmont, Emeline, Molliere, Paul, Poppenhaeger, Katja, Birkby, Jayne, Brogi, Matteo, Chauvin, Gael, Chiavassa, Andrea, Hoeijmakers, Jens, Lellouch, Emmanuel, Lovis, Christophe, Maiolino, Roberto, Nortmann, Lisa, Parviainen, Hannu, Pino, Lorenzo, Turbet, Martin, Wender, Jesse, Albrecht, Simon, Antoniucci, Simone, Barros, Susana C., Beaudoin, Andre, Benneke, Bjorn, Boisse, Isabelle, Bonomo, Aldo S., Borsa, Francesco, Brandeker, Alexis, Brandner, Wolfgang, Buchhave, Lars A., Cheffot, Anne-Laure, Deborde, Robin, Debras, Florian, Doyon, Rene, Di Marcantonio, Paolo, Giacobbe, Paolo, Hernandez, Jonay I. Gonzalez, Helled, Ravit, Kreidberg, Laura, Machado, Pedro, Maldonado, Jesus, Marconi, Alessandro, Martins, B. L. Canto, Miceli, Adriano, Mordasini, Christoph, N'Diaye, Mamadou, Niedzielski, Andrezj, Nisini, Brunella, Origlia, Livia, Peroux, Celine, Pietrow, Alex G. M., Pinna, Enrico, Rauscher, Emily, Reffert, Sabine, Rousselot, Philippe, Sanna, Nicoletta, Simonnin, Adrien, Mascareno, Alejandro Suarez, Zanutta, Alessio, and Zechmeister, Mathias

Abstract

In the past decade the study of exoplanet atmospheres at high-spectral resolution, via transmission/emission spectroscopy and cross-correlation techniques for atomic/molecular mapping, has become a powerful and consolidated methodology. The current limitation is the signal-to-noise ratio during a planetary transit. This limitation will be overcome by ANDES, an optical and near-infrared high-resolution spectrograph for the ELT. ANDES will be a powerful transformational instrument for exoplanet science. It will enable the study of giant planet atmospheres, allowing not only an exquisite determination of atmospheric composition, but also the study of isotopic compositions, dynamics and weather patterns, mapping the planetary atmospheres and probing atmospheric formation and evolution models. The unprecedented angular resolution of ANDES, will also allow us to explore the initial conditions in which planets form in proto-planetary disks. The main science case of ANDES, however, is the study of small, rocky exoplanet atmospheres, including the potential for biomarker detections, and the ability to reach this science case is driving its instrumental design. Here we discuss our simulations and the observing strategies to achieve this specific science goal. Since ANDES will be operational at the same time as NASA's JWST and ESA's ARIEL missions, it will provide enormous synergies in the characterization of planetary atmospheres at high and low spectral resolution. Moreover, ANDES will be able to probe for the first time the atmospheres of several giant and small planets in reflected light. In particular, we show how ANDES will be able to unlock the reflected light atmospheric signal of a golden sample of nearby non-transiting habitable zone earth-sized planets within a few tenths of nights, a scientific objective that no other currently approved astronomical facility will be able to reach., Comment: 66 pages (103 with references) 20 figures. Submitted to Experimental Astronomy

Published
2023

12. GAPS2: the origin of planetary systems diversity

Author

AFFER, Laura, BENATTI, Serena, BIAZZO, Katia, BIGNAMINI, ANDREA, BORSA, Francesco, CARLEO, Ilaria, CLAUDI, Riccardo, COSENTINO, Rosario, COVINO, Elvira, DAMASSO, Mario, DESIDERA, Silvano, GIACOBBE, Paolo, GUILLUY, GLORIA, HARUTYUNYAN, Avet, LANZA, Antonino Francesco, LETO, Giuseppe, MAGGIO, Antonio, Malavolta, L., MALDONADO PRADO, Jesus, Mancini, Luigi, MICELA, Giuseppina, MOLINARI, Emilio Carlo, NARDIELLO, Domenico, NASCIMBENI, VALERIO, PAGANO, Isabella, PINAMONTI, Matteo, PIOTTO , GIAMPAOLO, PORETTI, Ennio, RAINER, Monica, SCANDARIATO, GAETANO, SOZZETTI, Alessandro, and ITA

Abstract

This report described the work done in the GAPS2 programme so far. The goal of the project was to take advantage of the unique capabilities of the instrumentation at the TNG to study the origin of the diversity of planetary systems, shaped by variable degrees of orbital evolution, exploring uncharted territories in the realm of planet formation and evolution with emphasis on the innermost regions.

Published
2023

15. The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B ∗

Author

Carleo, Ilaria, primary, Giacobbe, Paolo, additional, Guilluy, Gloria, additional, Cubillos, Patricio E., additional, Bonomo, Aldo S., additional, Sozzetti, Alessandro, additional, Brogi, Matteo, additional, Gandhi, Siddharth, additional, Fossati, Luca, additional, Turrini, Diego, additional, Biazzo, Katia, additional, Borsa, Francesco, additional, Lanza, Antonino F., additional, Malavolta, Luca, additional, Maggio, Antonio, additional, Mancini, Luigi, additional, Micela, Giusi, additional, Pino, Lorenzo, additional, Poretti, Ennio, additional, Rainer, Monica, additional, Scandariato, Gaetano, additional, Schisano, Eugenio, additional, Andreuzzi, Gloria, additional, Bignamini, Andrea, additional, Cosentino, Rosario, additional, Fiorenzano, Aldo, additional, Harutyunyan, Avet, additional, Molinari, Emilio, additional, Pedani, Marco, additional, Redfield, Seth, additional, and Stoev, Hristo, additional

Published
2022
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16. Five carbon- and nitrogen-bearing species in a hot giant planet’s atmosphere

Author

Giacobbe, Paolo, primary, Brogi, Matteo, additional, Gandhi, Siddharth, additional, Cubillos, Patricio E., additional, Bonomo, Aldo S., additional, Sozzetti, Alessandro, additional, Fossati, Luca, additional, Guilluy, Gloria, additional, Carleo, Ilaria, additional, Rainer, Monica, additional, Harutyunyan, Avet, additional, Borsa, Francesco, additional, Pino, Lorenzo, additional, Nascimbeni, Valerio, additional, Benatti, Serena, additional, Biazzo, Katia, additional, Bignamini, Andrea, additional, Chubb, Katy L., additional, Claudi, Riccardo, additional, Cosentino, Rosario, additional, Covino, Elvira, additional, Damasso, Mario, additional, Desidera, Silvano, additional, Fiorenzano, Aldo F. M., additional, Ghedina, Adriano, additional, Lanza, Antonino F., additional, Leto, Giuseppe, additional, Maggio, Antonio, additional, Malavolta, Luca, additional, Maldonado, Jesus, additional, Micela, Giuseppina, additional, Molinari, Emilio, additional, Pagano, Isabella, additional, Pedani, Marco, additional, Piotto, Giampaolo, additional, Poretti, Ennio, additional, Scandariato, Gaetano, additional, Yurchenko, Sergei N., additional, Fantinel, Daniela, additional, Galli, Alberto, additional, Lodi, Marcello, additional, Sanna, Nicoletta, additional, and Tozzi, Andrea, additional

Published
2021
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17. Ariel: Enabling planetary science across light-years

Author

Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Peppo, Vania Da, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Giorgio, Anna Di, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Eylen, Vincent Van, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Swaelmen, Mathieu Van der, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Vecchio, Ciro Del, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, Zuppella, Paola, Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Peppo, Vania Da, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Giorgio, Anna Di, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Eylen, Vincent Van, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Swaelmen, Mathieu Van der, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Vecchio, Ciro Del, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola

Abstract

The concept of a mission devoted to atmospheric characterization of exoplanets through transit spectroscopy was first considered in Europe in 2007, shortly after the DARWIN proposal submitted to ESA for the first Cosmic Vision call for L-class missions was rejected because of the need for further scientific and technical developments. Following the decision, both ESA (EP-RAT panel report, October 2010) and the Exoplanetary Community (Blue Dot Team – Barcelona conference, September 2009) started a discussion to define a roadmap for exoplanetary research. Both groups concluded that an intermediate step was needed, both scientifically and technically, before the characterisation of Earth-like planets could be tackled, and recommended a transit spectroscopy mission as a first step to atmospheric characterisation. A short study was undertaken at ESTEC in the context of the ExoPlanet Roadmap Advisory Team mandate under the name ESM (Exoplanet Spectroscopy Mission). Following this study the Exoplanet Characterisation Observatory (EChO) was proposed and accepted for assessment phase study in the context of the ESA Cosmic Vision 2015-2025 programme M3 medium class mission opportunity. Although eventually not selected, the EChO study1 allowed further development of the technical building blocks and the science case for an eventual transit spectroscopy mission. In response to the call for the next medium class opportunity, Cosmic Vision M4, a proposal was submitted in January 2015: the Atmospheric Remote-sensing InfraRed Large-survey (ARIEL). The mission was one of the three selected in June 2015 for study in a Phase 0/A, a competitive assessment phase2. ARIEL was eventually selected as M4 in March 2018, and went into Phase B1, the definition study phase. The name of the mission has been changed to Ariel after selection. During Phase B1, the science case was studied in depth and consolidated under auspices of the Science Advisory Team, the bulk of the work be

Published
2020

18. TOI-1235 b: A Keystone Super-Earth for Testing Radius Valley Emergence Models around Early M Dwarfs

Author

Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, MIT Kavli Institute for Astrophysics and Space Research, Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G., Nava, Chantanelle, Ment, Kristo, Lopez, Eric D., Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Tenenbaum, Peter, Sozzetti, Alessandro, Sha, Lizhou, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Roy, Arpita, Robertson, Paul, Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepper, Joshua, Pepe, Francesco, Molinari, Emilio, Mocnik, Teo, Micela, Giuseppina, Mayor, Michel, Martinez Fiorenzano, Aldo F., Mallia, Franco, Lubin, Jack, Lovis, Christophe, López-Morales, Mercedes, Kosiarek, Molly R., Kielkopf, John F., Kane, Stephen R., Jensen, Eric L. N., Isopi, Giovanni, Huber, Daniel, Hill, Michelle L., Harutyunyan, Avet, Gonzales, Erica, Giacalone, Steven, Ghedina, Adriano, Ercolino, Andrea, Dumusque, Xavier, Dressing, Courtney D., Damasso, Mario, Dalba, Paul A., Cosentino, Rosario, Conti, Dennis M., Colón, Knicole D., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Christiansen, Jessie, Chontos, Ashley, Cecconi, Massimo, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Beichman, Charles, Behmard, Aida, Beard, Corey, Akana Murphy, Joseph M., Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, MIT Kavli Institute for Astrophysics and Space Research, Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G., Nava, Chantanelle, Ment, Kristo, Lopez, Eric D., Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Tenenbaum, Peter, Sozzetti, Alessandro, Sha, Lizhou, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Roy, Arpita, Robertson, Paul, Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepper, Joshua, Pepe, Francesco, Molinari, Emilio, Mocnik, Teo, Micela, Giuseppina, Mayor, Michel, Martinez Fiorenzano, Aldo F., Mallia, Franco, Lubin, Jack, Lovis, Christophe, López-Morales, Mercedes, Kosiarek, Molly R., Kielkopf, John F., Kane, Stephen R., Jensen, Eric L. N., Isopi, Giovanni, Huber, Daniel, Hill, Michelle L., Harutyunyan, Avet, Gonzales, Erica, Giacalone, Steven, Ghedina, Adriano, Ercolino, Andrea, Dumusque, Xavier, Dressing, Courtney D., Damasso, Mario, Dalba, Paul A., Cosentino, Rosario, Conti, Dennis M., Colón, Knicole D., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Christiansen, Jessie, Chontos, Ashley, Cecconi, Massimo, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Beichman, Charles, Behmard, Aida, Beard, Corey, and Akana Murphy, Joseph M.

Abstract

Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period-radius space. Here we present the confirmation of TOI-1235 b (P = 3.44 days, rp1.738-0.076+0.087 R⊕), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (R s = 0.630± 0.015 ⊕, M s = 0.640 ± 0.016 ⊙. We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of 6.91-0.85+0.75M⊕ which implies an iron core mass fraction of 20-12+15% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be <0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin ( = P 21.8+0.9-0.8days,mp sin =13.0+ 3.8-5.3M⊕) that cannot be firmly ruled out by our data.

Published
2020

19. TOI-1235 b: A Keystone Super-Earth for Testing Radius Valley Emergence Models around Early M Dwarfs

Author

Cloutier, Ryan, primary, Rodriguez, Joseph E., additional, Irwin, Jonathan, additional, Charbonneau, David, additional, Stassun, Keivan G., additional, Mortier, Annelies, additional, Latham, David W., additional, Isaacson, Howard, additional, Howard, Andrew W., additional, Udry, Stéphane, additional, Wilson, Thomas G., additional, Watson, Christopher A., additional, Pinamonti, Matteo, additional, Lienhard, Florian, additional, Giacobbe, Paolo, additional, Guerra, Pere, additional, Collins, Karen A., additional, Beiryla, Allyson, additional, Esquerdo, Gilbert A., additional, Matthews, Elisabeth, additional, Matson, Rachel A., additional, Howell, Steve B., additional, Furlan, Elise, additional, Crossfield, Ian J. M., additional, Winters, Jennifer G., additional, Nava, Chantanelle, additional, Ment, Kristo, additional, Lopez, Eric D., additional, Ricker, George, additional, Vanderspek, Roland, additional, Seager, Sara, additional, Jenkins, Jon M., additional, Ting, Eric B., additional, Tenenbaum, Peter, additional, Sozzetti, Alessandro, additional, Sha, Lizhou, additional, Ségransan, Damien, additional, Schlieder, Joshua E., additional, Sasselov, Dimitar, additional, Roy, Arpita, additional, Robertson, Paul, additional, Rice, Ken, additional, Poretti, Ennio, additional, Piotto, Giampaolo, additional, Phillips, David, additional, Pepper, Joshua, additional, Pepe, Francesco, additional, Molinari, Emilio, additional, Mocnik, Teo, additional, Micela, Giuseppina, additional, Mayor, Michel, additional, Martinez Fiorenzano, Aldo F., additional, Mallia, Franco, additional, Lubin, Jack, additional, Lovis, Christophe, additional, López-Morales, Mercedes, additional, Kosiarek, Molly R., additional, Kielkopf, John F., additional, Kane, Stephen R., additional, Jensen, Eric L. N., additional, Isopi, Giovanni, additional, Huber, Daniel, additional, Hill, Michelle L., additional, Harutyunyan, Avet, additional, Gonzales, Erica, additional, Giacalone, Steven, additional, Ghedina, Adriano, additional, Ercolino, Andrea, additional, Dumusque, Xavier, additional, Dressing, Courtney D., additional, Damasso, Mario, additional, Dalba, Paul A., additional, Cosentino, Rosario, additional, Conti, Dennis M., additional, Colón, Knicole D., additional, Collins, Kevin I., additional, Cameron, Andrew Collier, additional, Ciardi, David, additional, Christiansen, Jessie, additional, Chontos, Ashley, additional, Cecconi, Massimo, additional, Caldwell, Douglas A., additional, Burke, Christopher, additional, Buchhave, Lars, additional, Beichman, Charles, additional, Behmard, Aida, additional, Beard, Corey, additional, and Akana Murphy, Joseph M., additional

Published
2020
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20. Neutral Iron Emission Lines from the Dayside of KELT-9b: The GAPS Program with HARPS-N at TNG XX

Author

Pino, Lorenzo, primary, Désert, Jean-Michel, additional, Brogi, Matteo, additional, Malavolta, Luca, additional, Wyttenbach, Aurélien, additional, Line, Michael, additional, Hoeijmakers, Jens, additional, Fossati, Luca, additional, Bonomo, Aldo Stefano, additional, Nascimbeni, Valerio, additional, Panwar, Vatsal, additional, Affer, Laura, additional, Benatti, Serena, additional, Biazzo, Katia, additional, Bignamini, Andrea, additional, Borsa, Franscesco, additional, Carleo, Ilaria, additional, Claudi, Riccardo, additional, Cosentino, Rosario, additional, Covino, Elvira, additional, Damasso, Mario, additional, Desidera, Silvano, additional, Giacobbe, Paolo, additional, Harutyunyan, Avet, additional, Lanza, Antonino Francesco, additional, Leto, Giuseppe, additional, Maggio, Antonio, additional, Maldonado, Jesus, additional, Mancini, Luigi, additional, Micela, Giuseppina, additional, Molinari, Emilio, additional, Pagano, Isabella, additional, Piotto, Giampaolo, additional, Poretti, Ennio, additional, Rainer, Monica, additional, Scandariato, Gaetano, additional, Sozzetti, Alessandro, additional, Allart, Romain, additional, Borsato, Luca, additional, Bruno, Giovanni, additional, Fabrizio, Luca Di, additional, Ehrenreich, David, additional, Fiorenzano, Aldo, additional, Frustagli, Giuseppe, additional, Lavie, Baptiste, additional, Lovis, Christophe, additional, Magazzù, Antonio, additional, Nardiello, Domenico, additional, Pedani, Marco, additional, and Smareglia, Riccardo, additional

Published
2020
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21. A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU

Author

Damasso, Mario, primary, Del Sordo, Fabio, additional, Anglada-Escudé, Guillem, additional, Giacobbe, Paolo, additional, Sozzetti, Alessandro, additional, Morbidelli, Alessandro, additional, Pojmanski, Grzegorz, additional, Barbato, Domenico, additional, Butler, R. Paul, additional, Jones, Hugh R. A., additional, Hambsch, Franz-Josef, additional, Jenkins, James S., additional, López-González, María José, additional, Morales, Nicolás, additional, Peña Rojas, Pablo A., additional, Rodríguez-López, Cristina, additional, Rodríguez, Eloy, additional, Amado, Pedro J., additional, Anglada, Guillem, additional, Feng, Fabo, additional, and Gómez, Jose F., additional

Published
2020
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22. GAPS2: the origin of planetary systems diversity

Author

AFFER, Laura, BENATTI, Serena, BIAZZO, Katia, BIGNAMINI, ANDREA, BONOMO, ALDO STEFANO, BORSA, Francesco, CARLEO, Ilaria, CLAUDI, Riccardo, COSENTINO, Rosario, COVINO, Elvira, DAMASSO, Mario, DESIDERA, Silvano, GIACOBBE, Paolo, HARUTYUNYAN, Avet, LANZA, Antonino Francesco, LETO, Giuseppe, MAGGIO, Antonio, Malavolta, L., MALDONADO PRADO, Jesus, Mancini, Luigi, MICELA, Giuseppina, MOLINARI, Emilio Carlo, NASCIMBENI, VALERIO, PAGANO, Isabella, PIOTTO , GIAMPAOLO, PORETTI, Ennio, RAINER, Monica, SCANDARIATO, GAETANO, SOZZETTI, Alessandro, and ITA

Abstract

This report described the work done in the GAPS2 programme so far. The goal of the project is to take advantage of the unique capabilities of GIARPS to study the origin of the diversity of planetary systems, shaped by variable degrees of orbital evolution, exploring uncharted territories in the realm of planet formation and evolution with emphasis on the innermost regions.

Published
2019

23. GAPS2: the origin of planetary systems diversity

Author

AFFER, Laura, BENATTI, Serena, BIAZZO, Katia, BIGNAMINI, ANDREA, BONOMO, ALDO STEFANO, BORSA, Francesco, CARLEO, Ilaria, CLAUDI, Riccardo, COSENTINO, Rosario, COVINO, Elvira, DAMASSO, Mario, DESIDERA, Silvano, Esposito, M, GIACOBBE, Paolo, Gonzalez, Esther, GRATTON, Raffaele, HARUTYUNYAN, Avet, LANZA, Antonino Francesco, LETO, Giuseppe, MAGGIO, Antonio, Malavolta, L., MALDONADO PRADO, Jesus, Mancini, Luigi, MASIERO, SABRINA, MICELA, Giuseppina, MOLINARI, Emilio Carlo, NASCIMBENI, VALERIO, PAGANO, Isabella, PIOTTO , GIAMPAOLO, PORETTI, Ennio, RAINER, Monica, SCANDARIATO, GAETANO, SMAREGLIA, Riccardo, SOZZETTI, Alessandro, and ITA

Abstract

This report detailed the work done in the GAPS2 programme up to now. The goal of the project is to take advantage of the unique capabilities of GIARPS to study the origin of planetary systems diversity shaped by variable degrees of orbital evolution, exploring uncharted territory in the realm of planet formation and evolution with emphasis on the innermost regions.

Published
2018

24. Transiti planetari, Astrometria, Fotometria, Nane rosse, Missione spaziale GAIA

Author

Giacobbe, Paolo, Lattanzi, Mario Gilberto, Matteucci, Maria Francesca, and Sozzetti, Alessandro

Subjects
Astrofisica, Astrometria, Esopianeti, Transiti planetari, Fotometria, FIS/05 ASTRONOMIA E ASTROFISICA, Missione spaziale GAIA, SCUOLA DI DOTTORATO DI RICERCA IN FISICA, Nane rosse
Abstract

2012/2013 Small-size ground-based telescopes can effectively be used to look for transiting rocky planets around nearby low-mass M stars using the photometric transit method. Since 2008, a consortium of the Astrophysical Observatory of Torino (OATo-INAF) and the Astronomical Observatory of the Autonomous Region of Aosta Valley (OAVdA) have been preparing for the long-term photometric survey APACHE (A PAthway toward the Characterization of Habitable Earths), aimed at finding transiting small-size planets around thousands of nearby early and mid-M dwarfs. APACHE uses an array of five dedicated and identical 40-cm Ritchey-Chretien telescopes and its routine science operations started at the beginning of summer 2012. Here I present the results of the `pilot study', a year-long photometric monitoring campaign of a sample of 23 nearby dM stars, and of the APACHE survey first year data. In these studies, I set out to (i) demonstrate the sensitivity to > 2 Rearth transiting planets with periods of up to a few days around our programme stars, through a two-fold approach that combines a characterization of the statistical noise properties of our photometry with the determination of transit detection probabilities via simulations; and (ii), where possible, improves our knowledge of some astrophysical properties (e.g. activity, rotation) of our targets by combining our differential photometric measurements with spectroscopic information from the long-term programme GAPS with the HARPS-N spectrograph on the Telescopio Nazionale Galileo. Furthermore, cool M dwarfs within a few tens of parsecs from the Sun are becoming the focus of dedicated observational programs in the realm of exoplanet astrophysics that will make use of astrometric measurements. I present numerical simulations to gauge the Gaia potential for precision astrometry of exoplanets orbiting a sample of known dM stars within ~ 30 pc from the Sun. I then investigate some aspects of the synergy between the astrometric data expected from the Gaia mission on nearby M dwarfs and the APACHE program. XXV Ciclo 1985

Published
2014

25. SIOUX project: a simultaneous multiband camera for exoplanet atmospheres studies

Author

Christille, Jean Marc, additional, Bonomo, Aldo Stefano, additional, Borsa, Francesco, additional, Busonero, Deborah, additional, Calcidese, Paolo, additional, Claudi, Riccardo, additional, Damasso, Mario, additional, Giacobbe, Paolo, additional, Molinari, Emilio, additional, Pace, Emanuele, additional, Riva, Alberto, additional, Sozzetti, Alesandro, additional, Toso, Giorgio, additional, and Tresoldi, Daniela, additional

Published
2016
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28. Theia: Faint objects in motion or the new astrometry frontier

Author

Boehm, Céline, Krone-Martins, Alberto, Amorim, António, Anglada-Escudé, Guillem, Brandeker, Alexis, Courbin, Frederic, Enßlin, Torsten, Falcão, António, Freese, Katherine, Holl, Berry, Labadie, Lucas, Leger, Alain, Malbet, Fabien, Mamon, Gary, Mcarthur, Barbara, Mora, Alcione, Shao, Michael, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Albertus, Conrado, Bertone, Stefano, Bouy, Hervé, Boylan-Kolchin, Michael, Brown, Anthony, Brown, Warren, Cardoso, Vitor, Chemin, Laurent, Claudi, Riccardo, Correia, Alexandre C. M., Crosta, Mariateresa, Crouzier, Antoine, Cyr-Racine, Francis-Yan, Damasso, Mario, Da Silva, António, Davies, Melvyn, Das, Payel, Dayal, Pratika, Val-Borro, Miguel, Diaferio, Antonaldo, Erickcek, Adrienne, Fairbairn, Malcolm, Fortin, Morgane, Fridlund, Malcolm, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hambly, Nigel, Hara, Nathan, Hobbs, David, Hog, Erik, Holland, Andrew, Ibata, Rodrigo, Jordi, Carme, Klioner, Sergei, Kopeikin, Sergei, Lacroix, Thomas, Laskar, Jacques, Le Poncin-Lafitte, Christophe, Luri, Xavier, Majumdar, Subhabrata, Makarov, Valeri, Massey, Richard, Mennesson, Bertrand, Michalik, Daniel, Almeida, André Moitinho, Mourão, Ana, Moustakas, Leonidas, Murray, Neil, Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Perez-Garcia, Angeles, Platais, Imants, I Portell I Mora, Jord, Quirrenbach, Andreas, Randall, Lisa, Read, Justin, Regos, Eniko, Rory, Barnes, Rybicki, Krzysztof, Scott, Pat, Schneider, Jean, Jakub Scholtz, Siebert, Arnaud, Tereno, Ismael, Tomsick, John, Traub, Wesley, Valluri, Monica, Walker, Matt, Walton, Nicholas, Watkins, Laura, White, Glenn, Evans, Dafydd Wyn, Wyrzykowski, Lukasz, Wyse, Rosemary, Abbas, Ummi, Alimi, Jean-Michel, Altmann, Martin, Alves, João, Anderson, Richard, Arenou, Frédéric, Bailer-Jones, Coryn, Carlton, Baugh, Biermann, Michael, Blanco-Cuaresma, Sergi, Bonomo, Aldo Stefano, Broderick, Avery, Busso, Giorgia, Cabrera, Juan, Carrasco, Josep Manel, Carvalho, Carla Sofia, Castellani, Marco, Cermeño-Gavilán, Marina, Chadwick, Paula, Darling, Jeremy, Davidson, Michael, Angeli, Francesca, Carvalho, Reinaldo, Desidera, Silvano, Done, Chris, Ducourant, Christine, Erkal, Denis, Eyer, Laurent, Famey, Benoit, Feltzing, Sofia, Garcia, Emilio Fraile, Gomez, Facundo Ariel, Frenk, Carlos, Gai, Mario, Galli, Phillip, Galluccio, Laurent, Gavras, Panagiotis, Giacobbe, Paolo, Gratton, Raffaele, Guglielmetti, Fabrizia, Gunther, Eike, Hall, David, Harrison, Diana, Hatzes, Artie, Hestroffer, Daniel, Ishida, Emille, Jablonka, Pascale, Jacobs, Christopher, Janson, Markus, Jasche, Jens, Jauzac, Mathilde, Jones, Hugh, Jonker, Peter, Julbe, Francesc, Kneib, Jean-Paul, Kordopatis, Georges, Lancon, Arianne, Lattanzi, Mario Gilberto, Leguidou, Jean-Michel, Lehnert, Matt, Lehto, Harry, Lopes, Ilidio, Maldonado, Jesus, Marconi, Marcella, Martin, Nicolas, Marie-Elisabeth, Maury, Mazumdar, Anupam, Michtchenko, Tatiana, Minardi, Stefano, Munoz, Carlos, Murante, Giuseppe, Musella, Ilaria, Gerhard, Ortwin, Pagano, Isabella, Pani, Paolo, Paetzold, Martin, Daniel, Pfenniger, Piotto, Giampaolo, Preis, Olivier, Produit, Nicolas, Prost, Jean-Pierre, Rauer, Heike, Raymond, Sean, Reinaldo, Rosa, Revaz, Yves, Rita, Ribeiro, Rimoldini, Lorenzo, Huguet, Arnau Rios, Ripepi, Vincenzo, Rocci, Pier-Francesco, Rodriguez Frias, Maria D., Rosa, Reinaldo R., Sahlmann, Johannes, Saltas, Ippocratis, E E Lemos, José Pizarro Sand, Sarro, Luis M., Schaefer, Bjoern Malte, Schewtschenko, Jascha, Segransan, Damien, Selsis, Franck, Silk, Joe, Silva, Manuel, Solitro, Filomena, Spagna, Alessandro, Springel, Volker, Süveges, Maria, Teixeira, Ramachrisna, Shindou, Tetsuo, Thebault, Philippe, Tian, Feng, Turon, Catherine, Valle, José W. F., Vasiliev, Eugene, Vladilo, Juan, Martin, Vollmann, Ward, Martin, Weller, Jochen, Wilkinson, Mark, Wolf, Sebastian, Xiaoting, Fu, Yamada, Yoshiyuki, Zschocke, Sven, Zucker, Shay, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Blaise Pascal - Clermont-Ferrand 2 (UBP), Centre National d’Études Spatiales [Paris] (CNES), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Theia, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
[PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

In the context of the ESA M5 (medium mission) call we proposed a new satellite mission, Theia, based on relative astrometry and extreme precision to study the motion of very faint objects in the Universe. Theia is primarily designed to study the local dark matter properties, the existence of Earth-like exoplanets in our nearest star systems and the physics of compact objects. Furthermore, about 15 $\%$ of the mission time was dedicated to an open observatory for the wider community to propose complementary science cases. With its unique metrology system and "point and stare" strategy, Theia's precision would have reached the sub micro-arcsecond level. This is about 1000 times better than ESA/Gaia's accuracy for the brightest objects and represents a factor 10-30 improvement for the faintest stars (depending on the exact observational program). In the version submitted to ESA, we proposed an optical (350-1000nm) on-axis TMA telescope. Due to ESA Technology readiness level, the camera's focal plane would have been made of CCD detectors but we anticipated an upgrade with CMOS detectors. Photometric measurements would have been performed during slew time and stabilisation phases needed for reaching the required astrometric precision., Comment: http://theia.phyip3.dur.ac.uk

30. Radial-velocity fitting challenge. II. First results of the analysis of the data set

Author

X. Dumusque, F. Borsa, M. Damasso, R. F. Díaz, P. C. Gregory, N. C. Hara, A. Hatzes, V. Rajpaul, M. Tuomi, S. Aigrain, G. Anglada-Escudé, A. S. Bonomo, G. Boué, F. Dauvergne, G. Frustagli, P. Giacobbe, R. D. Haywood, H. R. A. Jones, J. Laskar, M. Pinamonti, E. Poretti, M. Rainer, D. Ségransan, A. Sozzetti, S. Udry, Dumusque, X., Borsa, F., Damasso, M., Dã­az, R. F., Gregory, P. C., Hara, N. C., Hatzes, A., Rajpaul, V., Tuomi, M., Aigrain, S., Anglada Escudé, G., Bonomo, A. S., Bouã©, G., Dauvergne, F., Frustagli, G., Giacobbe, Paolo, Haywood, R. D., Jones, H. R. A., Laskar, J., Pinamonti, Matteo, Poretti, E., Rainer, M., Sã©gransan, D., Sozzetti, A., Udry, S., ITA, USA, GBR, CHE, Observatoire de Genève, INAF-Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807, Merate (LC), Italy, INAF-Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025, Pino Torinese, Italy, Department of Physics and Astronomy, University of British Columbia, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Astronomie et systèmes dynamiques (ASD), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Türinger Landessternwarte Tautenburg, Department of Physics, Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Harvard-Smithsonian Center for Astrophysics, and Dipartimento di Fisica, Università di Genova e Sezione INFN

Subjects
Stars: activity, oscillations [stars], Planetary system, Ciencias Físicas, FOS: Physical sciences, Star (graph theory), 01 natural sciences, Signal, purl.org/becyt/ford/1 [https], Methods: data analysis, Planet, Planetary systems, Stars: oscillations, Techniques: radial velocities, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, data analysis [methods], Limit (mathematics), 010306 general physics, 010303 astronomy & astrophysics, planetary systems, Earth and Planetary Astrophysics (astro-ph.EP), Physics, activity [stars], radial velocitie [Techniques], oscillation [Stars], radial velocities [techniques], purl.org/becyt/ford/1.3 [https], Astronomy and Astrophysic, Computational physics, Radial velocity, Data set, data analysi [Methods], Astronomía, Orbit, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Order of magnitude, CIENCIAS NATURALES Y EXACTAS, Astrophysics - Earth and Planetary Astrophysics
Abstract

Radial-velocity (RV) signals induce RV variations an order of magnitude larger than the signal created by the orbit of Earth-twins, thus preventing their detection. The goal of this paper is to compare the efficiency of the different methods used to deal with stellar signals to recover extremely low-mass planets despite. However, because observed RV variations at the m/s precision level or below is a combination of signals induced by unresolved orbiting planets, by the star, and by the instrument, performing such a comparison using real data is extremely challenging. To circumvent this problem, we generated simulated RV measurements including realistic stellar and planetary signals. Different teams analyzed blindly those simulated RV measurements, using their own method to recover planetary signals despite stellar RV signals. By comparing the results obtained by the different teams with the planetary and stellar parameters used to generate the simulated RVs, it is therefore possible to compare the efficiency of these different methods. The most efficient methods to recover planetary signals {take into account the different activity indicators,} use red-noise models to account for stellar RV signals and a Bayesian framework to provide model comparison in a robust statistical approach. Using the most efficient methodology, planets can be found down to K/N= K_pl/RV_rms*sqrt{N_obs}=5 with a threshold of K/N=7.5 at the level of 80-90% recovery rate found for a number of methods. These recovery rates drop dramatically for K/N smaller than this threshold. In addition, for the best teams, no false positives with K/N > 7.5 were detected, while a non-negligible fraction of them appear for smaller K/N. A limit of K/N = 7.5 seems therefore a safe threshold to attest the veracity of planetary signals for RV measurements with similar properties to those of the different RV fitting challenge systems., 36 pages (including 10 pages of appendix), 23 figures, Accepted in A&A

Published
2017

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