Colin Southwell, Louise Emmerson, Akinori Takahashi, Akiko Kato, Christophe Barbraud, Karine Delord, Henri Weimerskirch. (2017). Recent studies overestimate colonization and extinction events for Adelie Penguin breeding coloniesEstudios recientes sobreestiman los eventos de colonización y extinción de Pygoscelis adeliae en reproducciónColonization and extinction events for Adelie Penguin colonies (Vol. 134).
Abstract: Abstract. Modeling metapopulation dynamics is potentially a useful and powerful tool for ecologists and conservation biologists. However, the key processes dri
Programme: 109
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Leclaire Sarah, Blanchard Pierrick, White Joël, Hatch Scott A, Danchin Étienne, . (2013). Symmetry of black wingtips is related to clutch size and integument coloration in Black-legged Kittiwakes ( Rissa tridactyla )
. The Auk, 130(3), 541–547.
Abstract: Fluctuating asymmetry has been suggested to be a phenotypic marker of developmental stability and is often seen as an indicator of overall quality. However, its role in sexual selection has been debated. To determine the potential role of black wingtip asymmetry in sexual selection in Black-legged Kittiwakes (Rissa tridactyla), we investigated whether symmetry was correlated with reproductive success and integument coloration, a trait probably sexually selected in this species. We found that, in males, asymmetry was associated with low clutch size and brood size but was independent of fledging success, which suggests that wingtip symmetry may reflect fertility in males. Asymmetry of black wingtip was also associated with duller integument, which emphasizes the potential importance of integument color in indicating individual quality. Further studies are needed to determine whether Black-legged Kittiwakes can discriminate between asymmetric and symmetric birds and use it as a cue in mate choice or intrasexual competition.
Programme: 1162
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Colin Southwell, Louise Emmerson, Akinori Takahashi, Akiko Kato, Christophe Barbraud, Karine Delord, Henri Weimerskirch. (2017). Recent studies overestimate colonization and extinction events for Adelie Penguin breeding colonies (Vol. 134).
Abstract: Modeling metapopulation dynamics is potentially a useful and powerful tool for ecologists and conservation biologists. However, the key processes driving metapopulation dynamics are colonization and extinction events, which are notoriously difficult to study. A recent global assessment of Adelie Penguin (Pygoscelis adeliae) breeding populations reported multiple potential colonization and extinction events from occupancy observations using recent high-resolution satellite imagery and examination of historical occupancy literature, but emphasized that the events should be confirmed with direct observations. We evaluated these conclusions by developing a comprehensive database of direct observations of Adelie Penguin breeding site occupancy across East Antarctica. The database allowed 16 of 19 proposed colonization and extinction events in this region to be evaluated using direct observations that were concurrent in space and time (same breeding season) with observations from satellite imagery. We concluded that none of the 16 proposed colonization and extinction events had occurred. One true extinction event may have been correctly identified from satellite imagery, but a conclusive evaluation was not possible because the direct and satellite observations were not concurrent in time. The evaluation identified several sources of error in observations from satellite imagery, including errors of omission through failure to detect small colonies and errors of commission through misidentification of other biological and physical features as Adelie Penguin guano. The occupancy database corrected issues of poor precision and accuracy in locations of historical occupancy data. Our results improve understanding of key parameters for Adelie Penguin metapopulation dynamics and facilitate improved interpretation of satellite imagery in the future.
Programme: 109
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E. Chapellier, D. Mékarnia, L. Abe, T. Guillot, K. Agabi, J.-P. Rivet, F.-X. Schmider, N. Crouzet, E. Aristidi. (2016). A CATALOG OF ECLIPSING BINARIES AND VARIABLE STARS OBSERVED WITH ASTEP 400 FROM DOME C, ANTARCTICA (Vol. 226).
Abstract: We used the large photometric database of the ASTEP program, whose primary goal was to detect exoplanets in the southern hemisphere from Antarctica, to search for eclipsing binaries (EcBs) and variable stars. 673 EcBs and 1166 variable stars were detected, including 31 previously known stars. The resulting online catalogs give the identification, the classification, the period, and the depth or semi-amplitude of each star. Data and light curves for each object are available at http://astep-vo.oca.eu.
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A. Kokori, A. Tsiaras, B. Edwards, A. Jones, G. Pantelidou, G. Tinetti, L. Bewersdorff, A. Iliadou, Y. Jongen, G. Lekkas, A. Nastasi, E. Poultourtzidis, C. Sidiropoulos, F. Walter, A. Wünsche, R. Abraham, V. K. Agnihotri, R. Albanesi, E. Arce-Mansego, D. Arnot, M. Audejean, C. Aumasson, M. Bachschmidt, G. Baj, P. R. Barroy, A. A. Belinski, D. Bennett, P. Benni, K. Bernacki, L. Betti, A. Biagini, P. Bosch, P. Brandebourg, L. Brát, M. Bretton, S. M. Brincat, S. Brouillard, A. Bruzas, A. Bruzzone, R. A. Buckland, M. Caló, F. Campos, A. Carreño, J. A. Carrion Rodrigo, R. Casali, G. Casalnuovo, M. Cataneo, C.-M. Chang, L. Changeat, V. Chowdhury, R. Ciantini, M. Cilluffo, J.-F. Coliac, G. Conzo, M. Correa, G. Coulon, N. Crouzet, M. V. Crow, I. A. Curtis, D. Daniel, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, G. Dransfield, R. Dymock, T. Eenmäe, N. Esseiva, P. Evans, C. Falco, R. G. Farfán, E. Fernández-Lajús, S. Ferratfiat, S. L. Ferreira, A. Ferretti, J. Fiołka, M. Fowler, S. R. Futcher, D. Gabellini, T. Gainey, J. Gaitan, P. Gajdoš, A. García-Sánchez, J. Garlitz, C. Gillier, C. Gison, J. Gonzales, D. Gorshanov, F. Grau Horta, G. Grivas, P. Guerra, T. Guillot, C. A. Haswell, T. Haymes, V.-P. Hentunen, K. Hills, K. Hose, T. Humbert, F. Hurter, T. Hynek, M. Irzyk, J. Jacobsen, A. L. Jannetta, K. Johnson, P. Jóźwik-Wabik, A. E. Kaeouach, W. Kang, H. Kiiskinen, T. Kim, Ü Kivila, B. Koch, U. Kolb, H. Kučáková, S.-P. Lai, D. Laloum, S. Lasota, L. A. Lewis, G.-I. Liakos, F. Libotte, F. Lomoz, C. Lopresti, R. Majewski, A. Malcher, M. Mallonn, M. Mannucci, A. Marchini, J.-M. Mari, A. Marino, G. Marino, J.-C. Mario, J.-B. Marquette, F. A. Martínez-Bravo, M. Mašek, P. Matassa, P. Michel, J. Michelet, M. Miller, E. Miny, D. Molina, T. Mollier, B. Monteleone, N. Montigiani, M. Morales-Aimar, F. Mortari, M. Morvan, L. V. Mugnai, G. Murawski, L. Naponiello, J.-L. Naudin, R. Naves, D. Néel, R. Neito, S. Neveu, A. Noschese, Y. Öğmen, O. Ohshima, Z. Orbanic, E. P. Pace, C. Pantacchini, N. I. Paschalis, C. Pereira, I. Peretto, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, J. Plazas, A. J. Poelarends, A. Popowicz, J. Purcell, N. Quinn, M. Raetz, D. Rees, F. Regembal, M. Rocchetto, P.-F. Rocci, M. Rockenbauer, R. Roth, L. Rousselot, X. Rubia, N. Ruocco, E. Russo, M. Salisbury, F. Salvaggio, A. Santos, J. Savage, F. Scaggiante, D. Sedita, S. Shadick, A. F. Silva, N. Sioulas, V. Školník, M. Smith, M. Smolka, A. Solmaz, N. Stanbury, D. Stouraitis, T.-G. Tan, M. Theusner, G. Thurston, F. P. Tifner, A. Tomacelli, A. Tomatis, J. Trnka, M. Tylšar, P. Valeau, J.-P. Vignes, A. Villa, A. Vives Sureda, K. Vora, M. Vrašt’ák, D. Walliang, B. Wenzel, D. E. Wright, R. Zambelli, M. Zhang, M. Zíbar. (2023). ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations (Vol. 265).
Abstract: The ExoClock project has been created to increase the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates, in order to produce a consistent catalog of reliable and precise ephemerides. This work presents a homogenous catalog of updated ephemerides for 450 planets, generated by the integration of ∼18,000 data points from multiple sources. These sources include observations from ground-based telescopes (the ExoClock network and the Exoplanet Transit Database), midtime values from the literature, and light curves from space telescopes (Kepler, K2, and TESS). With all the above, we manage to collect observations for half of the postdiscovery years (median), with data that have a median uncertainty less than 1 minute. In comparison with the literature, the ephemerides generated by the project are more precise and less biased. More than 40% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95%), and also the identification of missing data. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (transit-timing variations) for a sample of 19 planets. All the products, data, and codes used in this work are open and accessible to the wider scientific community.
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E. Bachelet, I.-G. Shin, C. Han, P. Fouqué, A. Gould, J. W. Menzies, J.-P. Beaulieu, D. P. Bennett, I. A. Bond, Subo Dong, D. Heyrovský, J.-B. Marquette, J. Marshall, J. Skowron, R. A. Street, T. Sumi, A. Udalski, L. Abe, K. Agabi, M. D. Albrow, W. Allen, E. Bertin, M. Bos, D. M. Bramich, J. Chavez, G. W. Christie, A. A. Cole, N. Crouzet, S. Dieters, M. Dominik, J. Drummond, J. Greenhill, T. Guillot, C. B. Henderson, F. V. Hessman, K. Horne, M. Hundertmark, J. A. Johnson, U. G. Jørgensen, R. Kandori, C. Liebig, D. Mékarnia, J. McCormick, D. Moorhouse, T. Nagayama, D. Nataf, T. Natusch, S. Nishiyama, J.-P. Rivet, K. C. Sahu, Y. Shvartzvald, G. Thornley, A. R. Tomczak, Y. Tsapras, J. C. Yee, V. Batista, C. S. Bennett, S. Brillant, J. A. R. Caldwell, A. Cassan, E. Corrales, C. Coutures, D. Dominis Prester, J. Donatowicz, D. Kubas, R. Martin, A. Williams, M. Zub, L. Andrade de Almeida, D. L. DePoy, B. S. Gaudi, L.-W. Hung, F. Jablonski, S. Kaspi, N. Klein, C.-U. Lee, Y. Lee, J.-R. Koo, D. Maoz, J. A. Muñoz, R. W. Pogge, D. Polishook, A. Shporer, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, P. Harris, Y. Itow, S. Kobara, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, K. Ohmori, K. Ohnishi, N. J. Rattenbury, To Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, I. Soszyński, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzyński, \L Wyrzykowski, N. Kains, C. Snodgrass, I. A. Steele, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, S. Dreizler, F. Finet, T. Gerner, S. Hardis, K. Harpsøe, T. C. Hinse, E. Kerins, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Southworth, J. Surdej, J. Wambsganss, and (The MiNDSTEp Consortium). (2012). MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT (Vol. 754).
Abstract: Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet–star mass ratio is q = (2.181 ± 0.004) × 10−3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the “microlens parallax” and the lens flux, we can only limit the host mass to the range 0.13 < M/M☉ < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M* = 0.67+0.33− 0.13 M☉ and mp = 1.5+0.8− 0.3 MJUP at a distance of D = 2.3 ± 0.6 kpc, and with a semi-major axis of a = 2+3− 1 AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.
Programme: 1066
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M Chadid and J Vernin and G Preston and C Zalian and C Pouzenc and L Abe and A Agabi and E Aristidi and LY Liu and D, . (2014). First Detection of Multi-shocks in RR Lyrae Stars from Antarctica: A Possible Explanation of the
. Astron. J. (N. Y.), 148(5), 88–.
Abstract: We present the first detection of multi-shocks propagating through the atmosphere of the Blazhko star S Arae using uninterrupted, accurate optical photometric data collected during one polar night, 150 days from Antarctica at Dome C, with the Photometer AntarctIca eXtinction (PAIX). We acquired 89,736 CCD frames during 323 pulsation cycles and 3 Blazhko cycles. We detected two new light curve properties in the PAIX light curve, ${jump}$ and ${rump}$, which we associated with two new post-maximum shock waves ShPM1 and ShPM2. ${jump}$, lump, ${rump}$, bump, and hump are induced by five shock waves, with different amplitudes and origins, ShPM1, ShPM, ShPM2, ShPM3, and the main shock ShH + He. Correlations between the length of rise time and light amplitude and ShPM3 are monotonous during three Blazhko cycles, but the pulsation curve is double peaked. We discuss the physical mechanisms driving the modulation of these quantities. Finally, we hypothesize that the origin of the Blazhko effect is a dynamical interaction between a multi-shock structure and an outflowing wind in a coronal structure.
Programme: 1096
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L. G. Bouma, J. D. Hartman, R. Brahm, P. Evans, K. A. Collins, G. Zhou, P. Sarkis, S. N. Quinn, J. de Leon, J. Livingston, C. Bergmann, K. G. Stassun, W. Bhatti, J. N. Winn, G. Á Bakos, L. Abe, N. Crouzet, G. Dransfield, T. Guillot, W. Marie-Sainte, D. Mékarnia, A. H. M. J. Triaud, C. G. Tinney, T. Henning, N. Espinoza, A. Jordán, M. Barbieri, S. Nandakumar, T. Trifonov, J. I. Vines, M. Vuckovic, C. Ziegler, N. Law, A. W. Mann, G. R. Ricker, R. Vanderspek, S. Seager, J. M. Jenkins, C. J. Burke, D. Dragomir, A. M. Levine, E. V. Quintana, J. E. Rodriguez, J. C. Smith, B. Wohler. (2020). Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602 (Vol. 160). Bachelor's thesis, , .
Abstract: We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA TESS mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a $T=9.9$ mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore $35^{+11}{-5}$ million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of $8.3\,{\rm d}$ and is slightly smaller than Jupiter ($R{\rm p} = 0.77^{+0.09}{-0.07} \,R{\rm Jup}$). From radial velocity monitoring, we limit $M{\rm p}\sin i$ to less than 1.20 $M{\rm Jup}$ (3-$\sigma$). The transits either graze or nearly graze the stellar limb. Grazing transits are a cause for concern, as they are often indicative of astrophysical false positive scenarios. Our follow-up data show that such scenarios are unlikely. Our combined multi-color photometry, high-resolution imaging, and radial velocities rule out hierarchical eclipsing binary scenarios. Background eclipsing binary scenarios, though limited by speckle imaging, remain a 0.2% possibility. TOI 837b is therefore a validated adolescent exoplanet. The planetary nature of the system can be confirmed or refuted through observations of the stellar obliquity and the planetary mass. Such observations may also improve our understanding of how the physical and orbital properties of exoplanets change in time.
Keywords: Astrophysics – Earth and Planetary Astrophysics Astrophysics – Solar and Stellar Astrophysics
Programme: 1066
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Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, Bill Wohler. (2022). TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux (Vol. 163).
Abstract: Mature super-Earths and sub-Neptunes are predicted to be ≃ Jovian radius when younger than 10 Myr. Thus, we expect to find 5–15 R ⊕ planets around young stars even if their older counterparts harbor none. We report the discovery and validation of TOI 1227b, a 0.85 ± 0.05 R J (9.5 R ⊕) planet transiting a very-low-mass star (0.170 ± 0.015 M ⊙) every 27.4 days. TOI 1227's kinematics and strong lithium absorption confirm that it is a member of a previously discovered subgroup in the Lower Centaurus Crux OB association, which we designate the Musca group. We derive an age of 11 ± 2 Myr for Musca, based on lithium, rotation, and the color–magnitude diagram of Musca members. The TESS data and ground-based follow-up show a deep (2.5%) transit. We use multiwavelength transit observations and radial velocities from the IGRINS spectrograph to validate the signal as planetary in nature, and we obtain an upper limit on the planet mass of ≃0.5 M J. Because such large planets are exceptionally rare around mature low-mass stars, we suggest that TOI 1227b is still contracting and will eventually turn into one of the more common <5 R ⊕ planets.
Programme: 1066
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Rebekah I. Dawson, Chelsea X. Huang, Rafael Brahm, Karen A. Collins, Melissa J. Hobson, Andrés Jordán, Jiayin Dong, Judith Korth, Trifon Trifonov, Lyu Abe, Abdelkrim Agabi, Ivan Bruni, R. Paul Butler, Mauro Barbieri, Kevin I. Collins, Dennis M. Conti, Jeffrey D. Crane, Nicolas Crouzet, Georgina Dransfield, Phil Evans, Néstor Espinoza, Tianjun Gan, Tristan Guillot, Thomas Henning, Jack J. Lissauer, Eric L. N. Jensen, Wenceslas Marie Sainte, Djamel Mékarnia, Gordon Myers, Sangeetha Nandakumar, Howard M. Relles, Paula Sarkis, Pascal Torres, Stephen Shectman, François-Xavier Schmider, Avi Shporer, Chris Stockdale, Johanna Teske, Amaury H. M. J. Triaud, Sharon Xuesong Wang, Carl Ziegler, G. Ricker, R. Vanderspek, David W. Latham, S. Seager, J. Winn, Jon M. Jenkins, L. G. Bouma, Jennifer A. Burt, David Charbonneau, Alan M. Levine, Scott McDermott, Brian McLean, Mark E. Rose, Andrew Vanderburg, Bill Wohler. (2021). Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b (Vol. 161).
Abstract: TOI-216 hosts a pair of warm, large exoplanets discovered by the TESS mission. These planets were found to be in or near the 2:1 resonance, and both of them exhibit transit timing variations (TTVs). Precise characterization of the planets’ masses and radii, orbital properties, and resonant behavior can test theories for the origins of planets orbiting close to their stars. Previous characterization of the system using the first six sectors of TESS data suffered from a degeneracy between planet mass and orbital eccentricity. Radial-velocity measurements using HARPS, FEROS, and the Planet Finder Spectrograph break that degeneracy, and an expanded TTV baseline from TESS and an ongoing ground-based transit observing campaign increase the precision of the mass and eccentricity measurements. We determine that TOI-216c is a warm Jupiter, TOI-216b is an eccentric warm Neptune, and that they librate in 2:1 resonance with a moderate libration amplitude of deg, a small but significant free eccentricity of for TOI-216b, and a small but significant mutual inclination of 1.°2–3.°9 (95% confidence interval). The libration amplitude, free eccentricity, and mutual inclination imply a disturbance of TOI-216b before or after resonance capture, perhaps by an undetected third planet.
Programme: 1066
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