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15,181 results on '"Erikson, A."'

1. Architecture of TOI-561 planetary system

Author

Piotto, G., Zingales, T., Borsato, L., Egger, J. A., Correia, A. C. M., Simon, A. E., Florén, H. G., Sousa, S. G., Maxted, P. F. L., Nardiello, D., Malavolta, L., Wilson, T. G., Alibert, Y., Adibekyan, V., Bonfanti, A., Luque, R., Santos, N. C., Hooton, M. J., Fossati, L., Smith, A. M. S., Salmon, S., Lacedelli, G., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Brandeker, A., Broeg, C., Buder, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Leonardi, P., Magrin, D., Mantovan, G., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Sicilia, D., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Winn, J. N., and Wolf, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $\rho_p = 0.778 \pm 0.097 \rho_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f., Comment: 13 pages, 10 Figures. Accepted on MNRAS. Updated the author list

Published
2024

2. The CHEOPS view on the climate of WASP-3 b

Author

Scandariato, G., Carone, L., Cubillos, P. E., Maxted, P. F. L., Zingales, T., Günther, M. N., Heitzmann, A., Lendl, M., Wilson, T. G., Bonfanti, A., Bruno, G., Krenn, A., Valdes, E. Meier, Singh, V., Swayne, M. I., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Brandeker, A., Broeg, C., Buder, M., Busch, M. -D., Cameron, A. Collier, Correia, A. C. M., Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Merín, B., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92+-21 ppm in the CHEOPS passband, 83+-27 ppm for TESS and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands we propose a set of likely emission spectra which constrain the emission contribution in the \cheops and TESS passbands to approximately a few dozens of parts per million. This allowed us to measure a geometric albedo of 0.21+-0.07 in the CHEOPS passband, while the TESS data lead to a 95\% upper limit of $\sim$0.2. WASP-3 b belongs to the group of ultra-hot Jupiters which are characterized by low Bond albedo (<0.3+-0.1), as predicted by different atmospheric models. On the other hand, it unexpectedly seems to efficiently recirculate the absorbed stellar energy, unlike similar highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms may be at play other than advection (for example, dissociation and recombination of H_2). Another possibility is that the observations in different bandpasses probe different atmospheric layers, making the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.

Published
2024

3. The K2-24 planetary system revisited by CHEOPS

Author

Nascimbeni, V., Borsato, L., Leonardi, P., Sousa, S. G., Wilson, T. G., Fortier, A., Heitzmann, A., Mantovan, G., Luque, R., Zingales, T., Piotto, G., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Biondi, F., Brandeker, A., Broeg, C., Busch, M. -D., Cameron, A. Collier, Correia, A. C. M., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Isaak, K. G., Kerschbaum, F., Kiss, L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Leleu, A., Lendl, M., Magrin, D., Maxted, P. F. L., Merín, B., Mordasini, C., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Southworth, R., Stalport, M., Sulis, S., Szabó, M. Gy., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

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

K2-24 is a planetary system composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large TTVs, i.e., an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the scenario of pure disk migration through resonant capture. With 13 new CHEOPS light curves (seven of planet -b, six of planet -c), we carried out a global photometric and dynamical re-analysis by including all the available literature data as well. We got the most accurate set of planetary parameters to date for the K2-24 system, including radii and masses at 1% and 5% precision (now essentially limited by the uncertainty on stellar parameters) and non-zero eccentricities $e_b=0.0498_{-0.0018}^{+0.0011}$, $e_c=0.0282_{-0.0007}^{+0.0003}$ detected at very high significance for both planets. Such relatively large values imply the need for an additional physical mechanism of eccentricity excitation during or after the migration stage. Also, while the accuracy of the previous TTV model had drifted by up to 0.5 days at the current time, we constrained the orbital solution firmly enough to predict the forthcoming transits for the next ~15 years, thus enabling an efficient follow-up with top-level facilities such as JWST or ESPRESSO., Comment: 19 pages, 11 figures, 8 tables. Accepted for publication in A&A on September 4, 2024. Typos corrected

Published
2024
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4. Grazing exclusion-induced changes in soil fungal communities in a highly desertified Brazilian dryland

Author

Silva, Danilo F, Mazza Rodrigues, Jorge L, Erikson, Christian, Silva, Antonio MM, Huang, Laibin, Araujo, Victor LVP, Matteoli, Filipe P, Mendes, Lucas W, Araujo, Ademir SF, Pereira, Arthur PA, Melo, Vania MM, and Cardoso, Elke JBN

Subjects
Microbiology, Biological Sciences, Ecology, Life on Land, Soil Microbiology, Brazil, Mycorrhizae, Mycobiome, Fungi, Soil, Climate Change, Desert Climate, Biodiversity, DNA, Fungal, Seasons, Ecosystem, Mycorrhizal symbiosis, Fungal communities, Soil degradation, Drylands, Medical Microbiology
Abstract

Soil desertification poses a critical ecological challenge in arid and semiarid climates worldwide, leading to decreased soil productivity due to the disruption of essential microbial community processes. Fungi, as one of the most important soil microbial communities, play a crucial role in enhancing nutrient and water uptake by plants through mycorrhizal associations. However, the impact of overgrazing-induced desertification on fungal community structure, particularly in the Caatinga biome of semiarid regions, remains unclear. In this study, we assessed the changes in both the total fungal community and the arbuscular mycorrhizal fungal community (AMF) across 1. Natural vegetation (native), 2. Grazing exclusion (20 years) (restored), and 3. affected by overgrazing-induced degradation (degraded) scenarios. Our assessment, conducted during both the dry and rainy seasons in Irauçuba, Ceará, utilized Internal Transcribed Spacer (ITS) gene sequencing via Illumina® platform. Our findings highlighted the significant roles of the AMF families Glomeraceae (∼71% of the total sequences) and Acaulosporaceae (∼14% of the total sequences) as potential key taxa in mitigating climate change within dryland areas. Moreover, we identified the orders Pleosporales (∼35% of the total sequences) and Capnodiales (∼21% of the total sequences) as the most abundant soil fungal communities in the Caatinga biome. The structure of the total fungal community differed when comparing native and restored areas to degraded areas. Total fungal communities from native and restored areas clustered together, suggesting that grazing exclusion has the potential to improve soil properties and recover fungal community structure amid global climate change challenges.

Published
2024

5. TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit

Author

Alqasim, A., Grieves, N., Rosário, N. M., Gandolfi, D., Livingston, J. H., Sousa, S., Collins, K. A., Teske, J. K., Fridlund, M., Egger, J. A., Cabrera, J., Hellier, C., Lanza, A. F., Van Eylen, V., Bouchy, F., Oelkers, R. J., Srdoc, G., Shectman, S., Günther, M., Goffo, E., Wilson, T., Serrano, L. M., Brandeker, A., Wang, S. X., Heitzmann, A., Bonfanti, A., Fossati, L., Alibert, Y., Delrez, L., Sefako, R., Barros, S., Collins, K. I., Demangeon, O. D. S., Albrecht, S. H., Alonso, R., Asquier, J., Barczy, T., Barrado, D., Baumjohann, W., Beck, T., Benz, W., Billot, N., Borsato, L., Broeg, C., Bryant, E. M., Butler, R. P., Cochran, W. D., Cameron, A. Collier, Correia, A. C. M., Crane, J. D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Daylan, T., Deleuil, M., Deline, A., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Essack, Z., Fortier, A., Gazeas, K., Gillon, M., Gudel, M., Hasiba, J., Hatzes, A. P., Helling, Ch., Hirano, T., Howell, S. B., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kanodia, S., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lund, M. B., Luque, R., Mann, A. W., Magrin, D., Maxted, P. F. L., Mordasini, C., Narita, N., Nascimbeni, V., Nowak, G., Olofsson, G., Osborn, H. P., Osborne, H. L. M., Osip, D., Ottensamer, R., Pagano, I., Palle, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Redfield, S., Ribas, I., Rice, M., Ricker, G. R., Rieder, M., Salmon, S., Santos, N. C., Scandariato, G., Seager, S., Segransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Stalport, M., Szabo, Gy. M., Thompson, I., Twicken, J. D., Udry, S., Vanderspek, R., Van Grootel, V., Venturini, J., Villaver, E., Villaseñor, J., Viotto, V., Walter, I., Walton, N. A., Winn, J. N., and Yee, S. W.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $\rho_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with $e$ = 0.39$^{+0.08}_{-0.07}$, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b's formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star-star interactions during the earlier epoch of the Galactic disk formation, given the low metallicity and older age of TOI-757., Comment: Accepted for publication in MNRAS; 26 pages, 14 figures, 6 tables

Published
2024

6. Characterisation of the Warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

Author

Borsato, L., Degen, D., Leleu, A., Hooton, M. J., Egger, J. A., Bekkelien, A., Brandeker, A., Cameron, A. Collier, Günther, M. N., Nascimbeni, V., Persson, C. M., Bonfanti, A., Wilson, T. G., Correia, A. C. M., Zingales, T., Guillot, T., Triaud, A. H. M. J., Piotto, G., Gandolfi, D., Abe, L., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Bendjoya, P., Benz, W., Billot, N., Broeg, C., Busch, M. -D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gazeas, K., Gillon, M., Güdel, M., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Marafatto, L., Maxted, P. F. L., Mecina, M., Mékarnia, D., Mordasini, C., Mura, D., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Salmon, S., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Suarez, O., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., and Wolter, D.

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

Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as "lonely" and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised. Within the contest of multi-planet system hosting gas-giant on short orbits, we characterise TOI-1130 system by measuring masses and orbital parameters. This is a 2-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data that achieve the best precision to date on the planetary radii and masses and on the timings of each transit. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively., Comment: 22 pages, 10 figures, Accepted for publication by Astronomy and Astrophysics

Published
2024
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7. Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

Author

Egger, J. A., Osborn, H. P., Kubyshkina, D., Mordasini, C., Alibert, Y., Günther, M. N., Lendl, M., Brandeker, A., Heitzmann, A., Leleu, A., Damasso, M., Bonfanti, A., Wilson, T. G., Sousa, S. G., Haldemann, J., Delrez, L., Hooton, M. J., Zingales, T., Luque, R., Alonso, R., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Broeg, C., Buder, M., Castro-González, A., Cameron, A. Collier, Correia, A. C. M., Cortes, D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Lavie, B., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Merín, B., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Rodrigues, J., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and a sub-Neptune. We observe HIP 29442 with CHEOPS for a total of 9.6 days, which we model jointly with 2 sectors of TESS data to derive planetary radii of $3.410\pm0.046$, $1.551\pm0.045$ and $1.538\pm0.049$ R$_\oplus$ for planets b, c and d, which orbit HIP 29442 with periods of 13.6, 3.5 and 6.4 days. For planet d, this value deviates by more than 3 sigma from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit S/N and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduce the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then apply hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identify planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with both a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope as well as a scenario with water-rich sub-Neptunes., Comment: 30 pages, 17 figures, accepted for publication in A&A

Published
2024
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8. PLATO's signal and noise budget

Author

Börner, Anko, Paproth, Carsten, Cabrera, Juan, Pertenais, Martin, Rauer, Heike, Mas-Hesse, J. Miguel, Pagano, Isabella, Alvarez, Jose Lorenzo, Erikson, Anders, Grießbach, Denis, Levillain, Yves, Magrin, Demetrio, Mogulsky, Valery, Niemi, Sami-Matias, Prod'homme, Thibaut, Regibo, Sara, De Ridder, Joris, Rockstein, Steve, Samadi, Reza, Serrano-Velarde, Dimitri, Smith, Alan, Verhoeve, Peter, and Walton, Dave

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

ESA's PLATO mission aims the detection and characterization of terrestrial planets around solar-type stars as well as the study of host star properties. The noise-to-signal ratio (NSR) is the main performance parameter of the PLATO instrument, which consists of 24 Normal Cameras and 2 Fast Cameras. In order to justify, verify and breakdown NSR-relevant requirements the software simulator PINE was developed. PINE models the signal pathway from a target star to the digital output of a camera based on physical models and considers the major noise contributors. In this paper, the simulator's coarse mode is introduced which allows fast performance analyses on instrument level. The added value of PINE is illustrated by exemplary applications., Comment: 17 pages, 8 figures, 3 tables

Published
2024

9. The PLATO Mission

Author

Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, Cesar, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, Acuña, Lorena, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebastià Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David, Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jorgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Degl'Innocenti, Scilla, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, Estrela, Inês, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Galli, Emanuele, Garcia, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, Grießbach, Denis, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Loïc, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kučinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, Érico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Benoît, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefano, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach160, ndreas, Reina6, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Rodríguez, María Teresa Rodrigo, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Santoli, Francesco, Santos, Ângela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, Sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, Švanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingril, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze

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

PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.

Published
2024

10. CHEOPS in-flight performance: A comprehensive look at the first 3.5 years of operations

Author

Fortier, A., Simon, A. E., Broeg, C., Olofsson, G., Deline, A., Wilson, T. G., Maxted, P. F. L., Brandeker, A., Cameron, A. Collier, Beck, M., Bekkelien, A., Billot, N., Bonfanti, A., Bruno, G., Cabrera, J., Delrez, L., Demory, B. -O., Futyan, D., Florén, H. -G., Günther, M. N., Heitzmann, A., Hoyer, S., Isaak, K. G., Sousa, S. G., Stalport, M., Turin, A., Verhoeve, P., Akinsanmi, B., Alibert, Y., Alonso, R., Bánhidi, D., Bárczy, T., Barrado, D., Barros, S. C., Baumjohann, W., Baycroft, T., Beck, T., Benz, W., Bíró, B. I., Bódi, A., Bonfils, X., Borsato, L., Charnoz, S., Cseh, B., Csizmadia, Sz., Csányi, I., Cubillos, P. E., Davies, M. B., Davis, Y. T., Deleuil, M., Demangeon, O. D. S., Derekas, A., Dransfield, G., Ducrot, E., Ehrenreich, D., Erikson, A., Fariña, C., Fossati, L., Fridlund, M., Gandolfi, D., Garai, Z., Garcia, L., Gillon, M., Chew, Y. Gómez Maqueo, Gómez-Muñoz, M. A., Granata, V., Güdel, M., Guterman, P., Hegedüs, T., Helling, Ch., Jehin, E., Kalup, Cs., Kilkenny, D., Kiss, L., Kriskovics, L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Pina, A. Lopez, Luntzer, A., Magrin, D., Miller, N. J., Contreras, D. Modrego, Mordasini, C., Munari, M., Murray, C. A., Nascimbeni, V., Ottacher, H., Ottensamer, R., Pagano, I., Pál, A., Pallé, E., Pasetti, A., Pedersen, P., Peter, G., Petrucci, R., Piotto, G., Pizarro-Rubio, A., Pollacco, D., Pribulla, T., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Sabin, L., Santos, N. C., Scandariato, G., Schanche, N., Schroffenegger, U., Scutt, O. J., Sebastian, D., Ségransan, D., Seli, B., Smith, A. M. S., Southworth, R., Standing, M. R., Szabó, M. Gy., Szakáts, R., Thomas, N., Timmermans, M., Triaud, A. H. M. J., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., Vinkó, J., Walton, N. A., Wells, R., and Wolter, D.

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

CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission and remains in excellent operational conditions. The mission has been extended until the end of 2026. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive analysis of the mission's performance. In this article, we present the results of this analysis with a twofold goal. First, we aim to inform the scientific community about the present status of the mission and what can be expected as the instrument ages. Secondly, we intend for this publication to serve as a legacy document for future missions, providing insights and lessons learned from the successful operation of CHEOPS. To evaluate the instrument performance in flight, we developed a comprehensive monitoring and characterisation programme. It consists of dedicated observations that allow us to characterise the instrument's response. In addition to the standard collection of nominal science and housekeeping data, these observations provide input for detecting, modelling, and correcting instrument systematics, discovering and addressing anomalies, and comparing the instrument's actual performance with expectations. The precision of the CHEOPS measurements has enabled the mission objectives to be met and exceeded. Careful modelling of the instrumental systematics allows the data quality to be significantly improved during the light curve analysis phase, resulting in more precise scientific measurements. CHEOPS is compliant with the driving scientific requirements of the mission. Although visible, the ageing of the instrument has not affected the mission's performance., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2024

11. HIP 41378 observed by CHEOPS: Where is planet d?

Author

Sulis, S., Borsato, L., Grouffal, S., Osborn, H. P., Santerne, A., Brandeker, A., Günther, M. N., Heitzmann, A., Lendl, M., Fridlund, M., Gandolfi, D., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C., Baumjohann, W., Beck, T., Benz, W., Bergomi, M., Billot, N., Bonfanti, A., Broeg, C., Cameron, A. Collier, van Damme, C. Corral, Correia, A. C. M., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Steinberger, M., Szabó, M. Gy., Tuson, A., Udry, S., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Wilson, T. G., Wolter, D., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If $P_\mathrm{d} \neq 278.36$ d, the periods that minimize the eccentricity would be $101.22$ d and $371.14$ d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2024
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12. Photo-dynamical characterisation of the TOI-178 resonant chain

Author

Leleu, A., Delisle, J. -B., Delrez, L., Bryant, E. M., Brandeker, A., Osborn, H. P., Hara, N., Wilson, T. G., Billot, N., Lendl, M., Ehrenreich, D., Chakraborty, H., Günther, M. N., Hooton, M. J., Alibert, Y., Alonso, R., Alves, D. R., Anderson, D. R., Apergis, I., Armstrong, D., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Battley, M. P., Baumjohann, W., Bayliss, D., Beck, T., Benz, W., Borsato, L., Broeg, C., Burleigh, M. R., Casewell, S. L., Cameron, A. Collier, Correia, A. C. M., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. -O., Derekas, A., Edwards, B., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gazeas, K., Gillen, E., Gillon, M., Goad, M. R., Güdel, M., Hawthorn, F., Heitzmann, A., Helling, Ch., Isaak, K. G., Jenkins, J. S., Jenkins, J. M., Kendall, A., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., McCormac, J., Mordasini, C., Moyano, M., Nascimbeni, V., Olofsson, G., Osborn, A., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Saha, S., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Vanderspek, R., Venturini, J., Villaver, E., Vinés, J. I., Walton, N. A., West, R. G., Winn, J., and Zivave, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with radii ranging from 1.2 to 2.9 earth radius and orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision event has taken place since the formation and migration of the planets in the protoplanetary disc, hence providing important anchors for planet formation models. We aim to improve the characterisation of the architecture of this key system, and in particular the masses and radii of its planets. In addition, since this system is one of the few resonant chains that can be characterised by both photometry and radial velocities, we aim to use it as a test bench for the robustness of the planetary mass determination with each technique. We perform a global analysis of all available photometry and radial velocity. We also try different sets of priors on the masses and eccentricity, as well as different stellar activity models, to study their effects on the masses estimated by each method. We show how stellar activity is preventing us from obtaining a robust mass estimation for the three outer planets using radial velocity data alone. We also show that our joint photo-dynamical and radial velocity analysis resulted in a robust mass determination for planets c to g, with precision of 12% for the mass of planet c, and better than 10% for planets d to g. The new precisions on the radii range from 2 to 3%. The understanding of this synergy between photometric and radial velocity measurements will be valuable during the PLATO mission. We also show that TOI-178 is indeed currently locked in the resonant configuration, librating around an equilibrium of the chain.

Published
2024
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13. Characterisation of the TOI-421 planetary system using CHEOPS, TESS, and archival radial velocity data

Author

Krenn, A. F., Kubyshkina, D., Fossati, L., Egger, J. A., Bonfanti, A., Deline, A., Ehrenreich, D., Beck, M., Benz, W., Cabrera, J., Wilson, T. G., Leleu, A., Sousa, S. G., Adibekyan, V., Correira, A. C. M., Alibert, Y., Delrez, L., Lendl, M., Patel, J. A., Venturini, J., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hasiba, J., Heitzmann, A., Helling, C., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Rieder, M., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Villaver, E., Viotto, V., Walton, N. A., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric data of three TESS sectors and six CHEOPS visits as well as 156 radial velocity data points to retrieve improved planetary parameters. We also searched for TTVs and modelled the interior structure of the planets. Finally, we simulated the evolution of the primordial H-He atmospheres of the planets using two different modelling frameworks. We determine the planetary radii and masses of TOI-421 b and c to be $R_{\rm b} = 2.64 \pm 0.08 \, R_{\oplus}$, $M_{\rm b} = 6.7 \pm 0.6 \, M_{\oplus}$, $R_{\rm c} = 5.09 \pm 0.07 \, R_{\oplus}$, and $M_{\rm c} = 14.1 \pm 1.4 \, M_{\oplus}$. We do not detect any statistically significant TTV signals. Assuming the presence of a hydrogen-dominated atmosphere, the interior structure modelling results in both planets having extensive envelopes. While the modelling of the atmospheric evolution predicts for TOI-421 b to have lost any primordial atmosphere that it could have accreted at its current orbital position, TOI-421 c could have started out with an initial atmospheric mass fraction somewhere between 10 and 35%. We conclude that the low observed mean density of TOI-421 b can only be explained by either a bias in the measured planetary parameters (e.g. driven by high-altitude clouds) and/or in the context of orbital migration. We also find that the results of atmospheric evolution models are strongly dependent on the employed planetary structure model., Comment: 21 pages, 12 figures, accepted for publication in A&A

Published
2024

14. Detailed cool star flare morphology with CHEOPS and TESS

Author

Bruno, G., Pagano, I., Scandariato, G., Florén, H. -G., Brandeker, A., Olofsson, G., Maxted, P. F. L., Fortier, A., Sousa, S. G., Sulis, S., Van Grootel, V., Garai, Z., Boldog, A., Kriskovics, L., Szabó, M. Gy., Gandolfi, D., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Borsato, L., Broeg, C., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Farinato, J., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Mordasini, C., Nascimbeni, V., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Sarajlic, M., Ségransan, D., Simon, A. E., Singh, V., Smith, A. M. S., Stalport, M., Thomas, N., Udry, S., Ulmer, B., Venturini, J., Villaver, E., Walton, N. A., and Wilson, T. G.

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

Context. White-light stellar flares are proxies for some of the most energetic types of flares, but their triggering mechanism is still poorly understood. As they are associated with strong X and UV emission, their study is particularly relevant to estimate the amount of high-energy irradiation onto the atmospheres of exoplanets, especially those in their stars' habitable zone. Aims. We used the high-cadence, high-photometric capabilities of the CHEOPS and TESS space telescopes to study the detailed morphology of white-light flares occurring in a sample of 130 late-K and M stars, and compared our findings with results obtained at a lower cadence. We developed dedicated software for this purpose. Results. Multi-peak flares represent a significant percentage ($\gtrsim 30$\%) of the detected outburst events. Our findings suggest that high-impulse flares are more frequent than suspected from lower-cadence data, so that the most impactful flux levels that hit close-in exoplanets might be more time-limited than expected. We found significant differences in the duration distributions of single-peak and complex flare components, but not in their peak luminosity. A statistical analysis of the flare parameter distributions provides marginal support for their description with a log-normal instead of a power-law function, leaving the door open to several flare formation scenarios. We tentatively confirmed previous results about quasi-periodic pulsations in high-cadence photometry, report the possible detection of a pre-flare dip, and did not find hints of photometric variability due to an undetected flare background. Conclusions. The high-cadence study of stellar hosts might be crucial to evaluate the impact of their flares on close-in exoplanets, as their impulsive phase emission might otherwise be incorrectly estimated. Future telescopes such as PLATO and Ariel will help in this respect., Comment: 28 pages, 25 figures, 4 tables, to be published in Astronomy & Astrophysics

Published
2024

15. Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution

Author

Rosário, N. M., Demangeon, O. D. S., Barros, S. C. C., Gandolfi, D., Egger, J. A., Serrano, L. M., Osborn, H. P., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Wilson, T. G., Alibert, Y., Fossati, L., Hooton, M. J., Delrez, L., Santos, N. C., Sousa, S. G., Bonfanti, A., Salmon, S., Adibekyan, V., Nigioni, A., Venturini, J., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barragán, O., Baumjohann, W., Beck, T., Billot, N., Biondi, F., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Cessa, V., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demory, B. -O., Ehrenreich, D., Erikson, A., Esposito, M., Fortier, A., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Osborne, H. L. M., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Eylen, V., Van Grootel, V., Villaver, E., Walter, I., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to improve the accuracy of the mass and radius estimates for both planets. We reanalyse light curves from TESS sectors 3 and 4 and analyse new data from sector 30, correcting for long-term stellar activity. Subsequently, we perform a joint fit of the TESS and CHEOPS light curves, and all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fits the planetary signals, the stellar activity signal and the instrumental decorrelation model for the CHEOPS data simultaneously. The stellar activity was modelled using a Gaussian-process regression on both the RV and activity indicators. We finally employ a Bayesian retrieval code to determine the internal composition and structure of the planets. We derive updated and highly precise parameters for the HD 15337 system. Our improved precision on the planetary parameters makes HD 15337 b one of the most precisely characterised rocky exoplanets, with radius and mass measurements achieving a precision better than 2\% and 7\%, respectively. We are able to improve the precision of the radius measurement of HD 15337 c to 3\%. Our results imply that the composition of HD 15337 b is predominantly rocky, while HD 15337 c exhibits a gas envelope with a mass of at least $0.01\ M_\oplus$.Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and give new insights into their composition and formation history and the causes behind the radius gap., Comment: 17 pages, including appendix

Published
2024
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16. The tidal deformation and atmosphere of WASP-12b from its phase curve

Author

Akinsanmi, B., Barros, S. C. C., Lendl, M., Carone, L., Cubillos, P. E., Bekkelien, A., Fortier, A., Florén, H. -G., Cameron, A. Collier, Boué, G., Bruno, G., Demory, B. -O., Brandeker, A., Sousa, S. G., Wilson, T. G., Deline, A., Bonfanti, A., Scandariato, G., Hooton, M. J., Correia, A. C. M., Demangeon, O. D. S., Smith, A. M. S., Singh, V., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Navascues, D. Barrado, Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, Ch., Buder, M., Charnoz, S., Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Ehrenreich, D., Erikson, A., Farinato, J., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mecina, M., Mordasini, Ch., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Ségransan, D., Simon, A. E., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Ultra-hot Jupiters present a unique opportunity to understand the physics and chemistry of planets at extreme conditions. WASP-12b stands out as an archetype of this class of exoplanets. We performed comprehensive analyses of the transits, occultations, and phase curves of WASP-12b by combining new CHEOPS observations with previous TESS and Spitzer data to measure the planet's tidal deformation, atmospheric properties, and orbital decay rate. The planet was modeled as a triaxial ellipsoid parameterized by the second-order fluid Love number, $h_2$, which quantifies its radial deformation and provides insight into the interior structure. We measured the tidal deformation of WASP-12b and estimated a Love number of $h_2=1.55_{-0.49}^{+0.45}$ (at 3.2$\sigma$) from its phase curve. We measured occultation depths of $333\pm24$ppm and $493\pm29$ppm in the CHEOPS and TESS bands, respectively, while the dayside emission spectrum indicates that CHEOPS and TESS probe similar pressure levels in the atmosphere at a temperature of 2900K. We also estimated low geometric albedos of $0.086\pm0.017$ and $0.01\pm0.023$ in the CHEOPS and TESS passbands, respectively, suggesting the absence of reflective clouds in the dayside of the WASP-12b. The CHEOPS occultations do not show strong evidence for variability in the dayside atmosphere of the planet. Finally, we refine the orbital decay rate by 12% to a value of -30.23$\pm$0.82 ms/yr. WASP-12b becomes the second exoplanet, after WASP-103b, for which the Love number has been measured (at 3$sigma$) from the effect of tidal deformation in the light curve. However, constraining the core mass fraction of the planet requires measuring $h_2$ with a higher precision. This can be achieved with high signal-to-noise observations with JWST since the phase curve amplitude, and consequently the induced tidal deformation effect, is higher in the infrared., Comment: accepted for publication in A&A

Published
2024

17. A National Portrait of Unlisted Home-Based Child Care Providers: The Communities Where Providers Live. HBCCSQ NSECE Analysis Brief. OPRE Brief 2023-146

Author

Administration for Children and Families (DHHS), Office of Planning, Research and Evaluation (OPRE), Mathematica, Erikson Institute, Schochet, Owen, Li, Ann, Del Grosso, Patricia, Atkins-Burnett, Sally, Porter, Toni, Reid, Natalie, and Bromer, Juliet

Abstract

In 2019, more than 5 million providers cared for one or more children either in their own home or in a child's home. Home-based child care (HBCC) providers are a varied group that includes listed providers and unlisted providers who do and do not receive payment. HBCC is especially prevalent in communities of color, communities with high concentrations of people from immigrant backgrounds, areas of concentrated poverty, and rural communities. Yet, research on HBCC lags behind research on center-based child care and early education (CCEE), and the least is known about unlisted providers who do not appear on state or national provider lists and work outside the formal systems supporting CCEE programs. This brief focuses on describing the characteristics of the communities in which unlisted HBCC providers live and, for many, where they typically care for children. It uses the 2019 National Survey of Early Care and Education (NSECE), the American Community Survey (ACS), and the Child Opportunity Index (COI) 2.0.

Published
2023

19. Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815

Author

Psaridi, Angelica, Osborn, Hugh, Bouchy, François, Lendl, Monika, Parc, Léna, Billot, Nicolas, Broeg, Christopher, Sousa, Sérgio G., Adibekyan, Vardan, Attia, Omar, Bonfanti, Andrea, Chakraborty, Hritam, Collins, Karen A., Davoult, Jeanne, Delgado-Mena, Elisa, Grieves, Nolan, Guillot, Tristan, Heitzmann, Alexis, Helled, Ravit, Hellier, Coel, Jenkins, Jon M., Knierim, Henrik, Krenn, Andreas, Lissauer, JackJ., Luque, Rafael, Rapetti, David, Santos, Nuno C., Suárez, Olga, Venturini, Julia, Wilkin, Francis P., Wilson, Thomas G., Winn, Joshua N., Ziegler, Carl, Zingales, Tiziano, Alibert, Yann, Brandeker, Alexis, Egger, Jo Ann, Gandolfi, Davide, Hooton, Matthew J., Tuson, Amy, Ulmer-Moll, Solène, Abe, Lyu, Allart, Romain, Alonso, Roi, Anderson, David R., Anglada, Guillem, Bárczy, Tamas, Barrado, David, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Mathias, Beck, Thomas, Benz, Willy, Bonfils, Xavier, Borsato, Luca, Bourrier, Vincent, Ciardi, David R., Cameron, Andrew Collier, Charnoz, Sébastien, Cointepas, Marion, Csizmadia, Szilárd, Cubillos, Patricio, Curto, Gaspare Lo, Davies, Melvyn B., Daylan, Tansu, Deleuil, Magali, Deline, Adrien, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dorn, Caroline, Dumusque, Xavier, Ehrenreich, David, Erikson, Anders, Etangs, Alain Lecavelier des, Ferreras, Elena Diana de Miguel, Fortier, Andrea, Fossati, Luca, Frensch, Yolanda G. C., Fridlund, Malcolm, Gillon, Michaël, Güdel, Manuel, Günther, Maximilian N., Hagelberg, Janis, Helling, Christiane, Hoyer, Sergio, Isaak, Kate G., Kiss, Laszlo L., Lam, Kristine, Laskar, Jacques, Lavie, Baptiste, Lovis, Christophe, Magrin, Demetrio, Marafatto, Luca, Maxted, Pierre, McDermott, Scott, Mékarnia, Djamel, Mordasini, Christoph, Murgas, Felipe, Nascimbeni, Valerio, Nielsen, Louise D., Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Ramos, Devin, Rando, Nicola, Rauer, Heike, Reimers, Christian, Ribas, Ignasi, Seager, Sara, Ségransan, Damien, Scandariato, Gaetano, Simon, Attila, Smith, Alexis M. S., Stalport, Manu, Steller, Manfred, Szabó, Gyula, Thomas, Nicolas, Pritchard, Tyler A., Udry, Stéphane, Van Damme, Carlos Corral, Van Grootel, Valérie, Villaver, Eva, Walter, Ingo, Walton, Nicholas, Watkins, Cristilyn N., and West, Richard G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery and characterization of two warm mini-Neptunes transiting the K3V star TOI-815 in a K-M binary system. Analysis of the spectra and rotation period reveal it to be a young star with an age of $200^{+400}_{-200}$Myr. TOI-815b has a 11.2-day period and a radius of 2.94$\pm$0.05$\it{R_{\rm\mathrm{\oplus}}}$ with transits observed by TESS, CHEOPS, ASTEP, and LCOGT. The outer planet, TOI-815c, has a radius of 2.62$\pm$0.10$\it{R_{\rm\mathrm{\oplus}}}$, based on observations of three non-consecutive transits with TESS, while targeted CHEOPS photometry and radial velocity follow-up with ESPRESSO were required to confirm the 35-day period. ESPRESSO confirmed the planetary nature of both planets and measured masses of 7.6$\pm$1.5 $\it{M_{\rm \mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=1.64$^{+0.33}_{-0.31}$gcm$^{-3}$) and 23.5$\pm$2.4$\it{M_{\rm\mathrm{\oplus}}}$ ($\rho_\mathrm{P}$=7.2$^{+1.1}_{-1.0}$gcm$^{-3}$) respectively. Thus, the planets have very different masses, unlike the usual similarity of masses in compact multi-planet systems. Moreover, our statistical analysis of mini-Neptunes orbiting FGK stars suggests that weakly irradiated planets tend to have higher bulk densities compared to those suffering strong irradiation. This could be ascribed to their cooler atmospheres, which are more compressed and denser. Internal structure modeling of TOI-815b suggests it likely has a H-He atmosphere constituting a few percent of the total planet mass, or higher if the planet is assumed to have no water. In contrast, the measured mass and radius of TOI-815c can be explained without invoking any atmosphere, challenging planetary formation theories. Finally, we infer from our measurements that the star is viewed close to pole-on, which implies a spin-orbit misalignment at the 3$\sigma$ level., Comment: 24 pages, 27 figures, 6 tables

Published
2024

20. Functional genes related to N and P cycling in degraded and restored areas from Brazilian drylands

Author

Silva, Danilo F, Cardoso, Elke JBN, Huang, Laibin, Erikson, Christian, Silva, Antonio MM, Araujo, Victor LVP, Silva, Davila EO, Melo, Vania MM, Araujo, Ademir SF, Pereira, Arthur PA, and Rodrigues, Jorge L Mazza

Subjects
Agricultural, Veterinary and Food Sciences, Biological Sciences, Ecology, Forestry Sciences, Life on Land, Soil functions, Microbial ecology, N and P cycles, Drylands, Environmental Sciences, Agricultural and Veterinary Sciences, Agronomy & Agriculture, Agricultural, veterinary and food sciences, Biological sciences, Environmental sciences
Published
2024

21. The value of marsh restoration for flood risk reduction in an urban estuary.

Author

Lowrie, Christopher, Tehranirad, Babak, Lowe, Jeremy, Erikson, Li, Barnard, Patrick, Reguero, Borja, Beck, Michael, and Taylor-Burns, Rae

Abstract

The use of nature-based solutions (NBS) for coastal climate adaptation has broad and growing interest, but NBS are rarely assessed with the same rigor as traditional engineering solutions or with respect to future climate change scenarios. These gaps pose challenges for the use of NBS for climate adaptation. Here, we value the flood protection benefits of stakeholder-identified marsh restoration under current and future climate change within San Francisco Bay, a densely urbanized estuary, and specifically on the shores of San Mateo County, the county most vulnerable to future flooding in California. Marsh restoration provides a present value of $21 million which increases to over $100 million with 0.5 m of sea level rise (SLR), and to about $500 million with 1 m of SLR. There are hotspots within the county where marsh restoration delivers very high benefits for adaptation, which reach $9 million/hectare with likely future sea level and storm conditions. Todays investments in nature and community resilience can result in increasing payoffs as climate change progresses and risk increases.

Published
2024

22. The EBLM Project XI. Mass, radius and effective temperature measurements for 23 M-dwarf companions to solar-type stars observed with CHEOPS

Author

Swayne, M. I., Maxted, P. F. L., Triaud, A. H. M. J., Sousa, S. G., Deline, A., Ehrenreich, D., Hoyer, S., Olofsson, G., Boisse, I., Duck, A., Gill, S., Martin, D., McCormac, J., Persson, C. M., Santerne, A., Sebastian, D., Standing, M. R., Acuña, L., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Baycroft, T. A., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Bourrier, V., Brandeker, A., Broeg, C., Carmona, A., Charnoz, S., Cameron, A. Collier, Cortés-Zuleta, P., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dransfield, G., Erikson, A., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hara, N., Hébrard, G., Heidari, N., Hellier, C., Helling, Ch., Isaak, K. G., Kerschbaum, F., Kiefer, F., Kiss, L. L., Kunovac, V., Lalitha, S., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Marafatto, L., Martioli, E., Miller, N. J., Mordasini, C., Moutou, C., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Southworth, R., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A., Willett, E., and Wilson, T. G.

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

Observations of low-mass stars have frequently shown a disagreement between observed stellar radii and radii predicted by theoretical stellar structure models. This ``radius inflation'' problem could have an impact on both stellar and exoplanetary science. We present the final results of our observation programme with the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions (EBLMs). Combined with the spectroscopic orbits of the solar-type companion, we can derive the masses, radii and effective temperatures of 23 M-dwarf stars. We use the PYCHEOPS data analysis software to analyse their primary and secondary occultations. For all but one target, we also perform analyses with TESS light curves for comparison. We have assessed the impact of starspot-induced variation on our derived parameters and account for this in our radius and effective temperature uncertainties using simulated light curves. We observe trends for inflation with both metallicity and orbital separation. We also observe a strong trend in the difference between theoretical and observational effective temperatures with metallicity. There is no such trend with orbital separation. These results are not consistent with the idea that observed inflation in stellar radius combines with lower effective temperature to preserve the luminosity predicted by low-mass stellar models. Our EBLM systems are high-quality and homogeneous measurements that can be used in further studies into radius inflation., Comment: 21 pages, 10 figures, accepted for publication in MNRAS, Supplementary material provided as ancillary files

Published
2023

23. Characterising TOI-732 b and c: new insights on the M-dwarf radius and density valley

Author

Bonfanti, A., Brady, M., Wilson, T. G., Venturini, J., Egger, J. A., Brandeker, A., Sousa, S. G., Lendl, M., Simon, A. E., Queloz, D., Olofsson, G., Adibekyan, V., Alibert, Y., Fossati, L., Hooton, M. J., Kubyshkina, D., Luque, R., Murgas, F., Mustill, A. J., Santos, N. C., Van Grootel, V., Alonso, R., Asquier, J., Bandy, T., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Bean, J., Beck, M., Beck, T., Benz, W., Bergomi, M., Billot, N., Borsato, L., Broeg, C., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kasper, D., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Seifahrt, A., Smith, A. M. S., Stalport, M., Stefánsson, G., Steinberger, M., Stürmer, J., Szabó, Gy. M., Thomas, N., Udry, S., Villaver, E., Walton, N. A., Westerdorff, K., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

TOI-732 is an M dwarf hosting two transiting planets, which are located on the two opposite sides of the radius valley. By doubling the number of available space-based observations and increasing the number of radial velocity (RV) measurements, we aim at refining the parameters of TOI-732 b and c. We also aim at using the results to study the slope of both the radius valley and the density valley for a well characterised sample of M dwarf exoplanets. We performed a global MCMC analysis by jointly modelling ground-based light curves, CHEOPS and TESS observations, along with RV time series both taken from the literature and obtained with the MAROON-X spectrograph. The slopes of the M dwarf valleys were quantified via a Support Vector Machine (SVM) procedure. TOI-732 b is an ultra short period planet ($P\sim0.77$ d) with a radius $R_b=1.325_{-0.058}^{+0.057}$ $R_{\oplus}$ and a mass $M_b=2.46\pm0.19$ $M_{\oplus}$ (mean density $\rho_b=5.8_{-0.8}^{+1.0}$ g cm$^{-3}$), while the outer planet at $P\sim12.25$ d has $R_c=2.39_{-0.11}^{+0.10}$ $R_{\oplus}$, $M_c=8.04_{-0.48}^{+0.50}$ $M_{\oplus}$, and thus $\rho_c=3.24_{-0.43}^{+0.55}$ g cm$^{-3}$. Also considering our interior structure calculations TOI-732 b is a super-Earth and TOI-732 c is a mini-Neptune. Following the SVM approach, we quantified $\mathrm{d}\log{R_{p,{\mathrm{valley}}}}/\mathrm{d}\log{P}=-0.065_{-0.013}^{+0.024}$, which is flatter than for Sun-like stars. In line with former analyses, we noted a more filled radius valley for M-planets and we further quantified the density valley slope as $\mathrm{d}\log{\hat{\rho}_{\mathrm{valley}}}/\mathrm{d}\log{P}=-0.02_{-0.04}^{+0.12}$. Compared to FGK stars, the weaker dependence of the position of the radius valley with orbital period might indicate a heavier influence of formation relative to evolution mechanisms in shaping the radius valley around M-dwarfs., Comment: 28 pages (17 in the main text), 18 figures (9 in the main text), 11 tables (7 in the main text). Accepted for publication in A&A

Published
2023

24. CHEOPS observations of KELT-20 b/MASCARA-2 b: an aligned orbit and signs of variability from a reflective dayside

Author

Singh, V., Scandariato, G., Smith, A. M. S., Cubillos, P. E., Lendl, M., Billot, N., Fortier, A., Queloz, D., Sousa, S. G., Csizmadia, Sz., Brandeker, A., Carone, L., Wilson, T. G., Akinsanmi, B., Patel, J. A., Krenn, A., Demangeon, O. D. S., Bruno, G., Pagano, I., Hooton, M. J., Cabrera, J., Santos, N. C., Alibert, Y., Alonso, R., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Bergomi, M., Bonfanti, A., Bonfils, X., Borsato, L., Broeg, C., Charnoz, S., Cameron, A. Collier, Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Harre, J. -V., Heitzmann, A., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mischler, H., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Salmon, S., Ségransan, D., Simon, A. E., Stalport, M., Steinberger, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., and Zingales, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Occultations are windows of opportunity to indirectly peek into the dayside atmosphere of exoplanets. High-precision transit events provide information on the spin-orbit alignment of exoplanets around fast-rotating hosts. We aim to precisely measure the planetary radius and geometric albedo of the ultra-hot Jupiter (UHJ) KELT-20 b as well as the system's spin-orbit alignment. We obtained optical high-precision transits and occultations of KELT-20 b using CHEOPS observations in conjunction with the simultaneous TESS observations. We interpret the occultation measurements together with archival infrared observations to measure the planetary geometric albedo and dayside temperatures. We further use the host star's gravity-darkened nature to measure the system's obliquity. We present time-averaged precise occultation depth of 82(6) ppm measured with seven CHEOPS visits and 131(+8/-7) ppm from the analysis of all available TESS photometry. Using these measurements, we precisely constrain the geometric albedo of KELT-20 b to 0.26(0.04) and the brightness temperature of the dayside hemisphere to 2566(+77/-80) K. Assuming Lambertian scattering law, we constrain the Bond albedo to 0.36(+0.04/-0.05) along with a minimal heat transfer to the nightside. Furthermore, using five transit observations we provide stricter constraints of 3.9(1.1) degrees on the sky-projected obliquity of the system. The aligned orbit of KELT-20 b is in contrast to previous CHEOPS studies that have found strongly inclined orbits for planets orbiting other A-type stars. KELT-20 b's comparably high planetary geometric albedo corroborates a known trend of strongly irradiated planets being more reflective. Finally, we tentatively detect signs of temporal variability in the occultation depths, which might indicate variable cloud cover advecting onto the planetary dayside., Comment: 27 pages, 15 figures, Accepted for publication in Astronomy & Astrophysics

Published
2023

25. A National Portrait of Unlisted Home-Based Child Care Providers: Caregiving Histories, Motivations, and Professional Engagement. HBCCSQ NSECE Analysis Brief. OPRE Brief 2022-281

Author

Administration for Children and Families (DHHS), Office of Planning, Research and Evaluation (OPRE), Mathematica, Erikson Institute, Schochet, Owen, Li, Ann, Del Grosso, Patricia, Aikens, Nikki, Atkins-Burnett, Sally, Porter, Toni, and Bromer, Juliet

Abstract

In 2019, more than 5 million providers cared for one or more children either in their own home or in a child's home. Home-based child care (HBCC) providers are a varied group that includes both listed providers and unlisted providers who do and do not receive payment. HBCC is especially prevalent in communities of color, communities with high concentrations of people from immigrant backgrounds, areas of concentrated poverty, and rural communities. Yet, research on HBCC lags behind research on center-based child care and early education (CCEE), and the least is known about unlisted providers who do not appear on state or national provider lists and work outside the formal systems supporting CCEE programs. Using the 2019 National Survey of Early Care and Education (NSECE), this brief focuses on unlisted providers' caregiving histories, motivations, and recent experiences with professional supports.

Published
2022

26. A National Portrait of Unlisted Home-Based Child Care Providers: Provider Demographics, Economic Wellbeing, and Health. HBCCSQ NSECE Analysis Brief. OPRE Brief 2022-280

Author

Administration for Children and Families (DHHS), Office of Planning, Research and Evaluation (OPRE), Mathematica, Erikson Institute, Schochet, Owen, Li, Ann, Del Grosso, Patricia, Aikens, Nikki, Atkins-Burnett, Sally, Porter, Toni, and Bromer, Juliet

Abstract

In 2019, more than 5 million providers cared for one or more children either in their own home or in a child's home. Home-based child care (HBCC) providers are a varied group that includes both listed providers and unlisted providers who do and do not receive payment. HBCC is especially prevalent in communities of color, communities with high concentrations of people from immigrant backgrounds, areas of concentrated poverty, and rural communities. Yet, research on HBCC lags behind research on center-based child care and early education (CCEE), and the least is known about unlisted providers who do not appear on state or national provider lists and work outside the formal systems supporting CCEE programs. Using the 2019 National Survey of Early Care and Education (NSECE), this brief focuses on the demographic, educational, economic, and health and wellbeing characteristics of unlisted HBCC providers.

Published
2022

27. A National Portrait of Unlisted Home-Based Child Care Providers: Learning Activities, Caregiving Services, and Children Served. HBCCSQ NSECE Analysis Brief. OPRE Brief 2022-292

Author

Administration for Children and Families (DHHS), Office of Planning, Research and Evaluation (OPRE), Mathematica, Erikson Institute, Schochet, Owen, Li, Ann, Del Grosso, Patricia, Aikens, Nikki, Atkins-Burnett, Sally, Toni, Porter, and Bromer, Juliet

Abstract

In 2019, more than 5 million providers cared for one or more children either in their own home or in a child's home. Home-based child care (HBCC) providers are a varied group that includes both listed providers and unlisted providers who do and do not receive payment. HBCC is especially prevalent in communities of color, communities with high concentrations of people from immigrant backgrounds, areas of concentrated poverty, and rural communities. Yet, research on HBCC lags behind research on center-based child care and early education (CCEE), and the least is known about unlisted providers who do not appear on state or national provider lists and work outside the formal systems supporting CCEE programs. Using the 2019 National Survey of Early Care and Education (NSECE), this brief focuses on how unlisted HBCC providers spend their caregiving time, what kinds of caregiving services they provide, and the characteristics of the children they serve.

Published
2022

33. No random transits in CHEOPS observations of HD 139139

Author

Alonso, R., Hoyer, S., Deleuil, M., Simon, A. E., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Borsato, L., Brandeker, A., Gandolfi, D., Wilson, T. G., Zingales, T., Alibert, Y., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, Ch., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Sz., Csizmadia, Cubillos, P. E., Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D, Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Maxted, P. F. L., Mordasini, Ch., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Smith, A. M. S., Sousa, S. G., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van grootel, V., Venturini, J., Verrecchia, F., and Walton, N. A.

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

HD 139139 (a.k.a. 'The Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events ($\sim$200 ppm -- equivalent to transiting objects with radii of $\sim$1.5 R$_\oplus$ in front of a Sun-like star), and their non-periodicity, constitutes a challenge for the photometric follow-up of this star. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. We performed observations with CHEOPS, for a total accumulated time of 12.75 d, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We use the duration and times of the events seen in the K2 curve to estimate how many should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8 %. We suggest three different scenarios to explain our results: 1) Our observing window was not long enough, and the events were missed with the estimated 4.8 % probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment., Comment: 7 pages, 3 figures, accepted for publication in A&A. Language-corrected version

Published
2023
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34. Constraining the reflective properties of WASP-178b using Cheops photometry

Author

Pagano, I., Scandariato, G., Singh, V., Lendl, M., Queloz, D., Simon, A. E., Sousa, S. G., Brandeker, A., Cameron, A. Collier, Sulis, S., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bruno, G., Carone, L., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Reimers, C., Ribas, I., Rieder, M., Santos, N. C., Ségransan, D., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. This leads to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency $\epsilon$, which quantifies the energy transport within the atmosphere. In this work we aim to measure $A_g$ and $\epsilon$ for the planet WASP-178 b, a highly irradiated giant planet with an estimated equilibrium temperature of 2450 K.} We analyzed archival spectra and the light curves collected by Cheops and Tess to characterize the host WASP-178, refine the ephemeris of the system and measure the eclipse depth in the passbands of the two respective telescopes. We measured a marginally significant eclipse depth of 70$\pm$40 ppm in the Tess passband and statistically significant depth of 70$\pm$20 ppm in the Cheops passband. Combining the eclipse depth measurement in the Cheops (lambda_eff=6300 AA) and Tess (lambda_eff=8000 AA) passbands we constrained the dayside brightness temperature of WASP-178 b in the 2250-2800 K interval. The geometric albedo 0.1<$\rm A_g$<0.35 is in general agreement with the picture of poorly reflective giant planets, while the recirculation efficiency $\epsilon>$0.7 makes WASP-178 b an interesting laboratory to test the current heat recirculation models., Comment: Accepted by Astronomy and Astrophysics on 31/08/2023

Published
2023

35. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author

Delrez, L., Leleu, A., Brandeker, A., Gillon, M., Hooton, M. J., Cameron, A. Collier, Deline, A., Fortier, A., Queloz, D., Bonfanti, A., Van Grootel, V., Wilson, T. G., Egger, J. A., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Güdel, M., Hasiba, J., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Luque, R., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Vanderspek, R., Venturini, J., Viotto, V., Walton, N. A., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital distance to the star, contrary to what one would expect based on simple formation and evolution models. To improve the characterisation of this key system and prepare for future studies (in particular with JWST), we perform a detailed photometric study based on 40 new CHEOPS visits, one new TESS sector, as well as previously published CHEOPS, TESS, and NGTS data. First we perform a global analysis of the 100 transits contained in our data to refine the transit parameters of the six planets and study their transit timing variations (TTVs). We then use our extensive dataset to place constraints on the radii and orbital periods of potential additional transiting planets in the system. Our analysis significantly refines the transit parameters of the six planets, most notably their radii, for which we now obtain relative precisions $\lesssim$3%, with the exception of the smallest planet $b$ for which the precision is 5.1%. Combined with the RV mass estimates, the measured TTVs allow us to constrain the eccentricities of planets $c$ to $g$, which are found to be all below 0.02, as expected from stability requirements. Taken alone, the TTVs also suggest a higher mass for planet $d$ than the one estimated from the RVs, which had been found to yield a surprisingly low density for this planet. However, the masses derived from the current TTV dataset are very prior-dependent and further observations, over a longer temporal baseline, are needed to deepen our understanding of this iconic planetary system., Comment: 20 pages, 5 figures, 9 tables. Accepted for publication in A&A

Published
2023
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36. CHEOPS and TESS view of the ultra-short period super-Earth TOI-561 b

Author

Patel, J. A., Egger, J. A., Wilson, T. G., Bourrier, V., Carone, L., Beck, M., Ehrenreich, D., Sousa, S. G., Benz, W., Brandeker, A., Deline, A., Alibert, Y., Lam, K. W. F., Lendl, M., Alonso, R., Anglada, G., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, C., Busch, M. -D., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Viotto, V., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Ultra-short period planets (USPs) are a unique class of super-Earths with an orbital period of less than a day and hence subject to intense radiation from their host star. While most of them are consistent with bare rocks, some show evidence of a heavyweight envelope, which could be a water layer or a secondary metal-rich atmosphere sustained by an outgassing surface. Much remains to be learned about the nature of USPs. The prime goal of the present work is to study the bulk planetary properties and atmosphere of TOI-561b, through the study of its transits and occultations. We obtained ultra-precise transit photometry of TOI-561b with CHEOPS and performed a joint analysis of this data with four TESS sectors. Our analysis of TOI-561b transit photometry put strong constraints on its properties, especially on its radius, Rp=1.42 +/- 0.02 R_Earth (at ~2% error). The internal structure modelling of the planet shows that the observations are consistent with negligible H/He atmosphere, however requiring other lighter materials, in addition to pure iron core and silicate mantle to explain the observed density. We find that this can be explained by the inclusion of a water layer in our model. We searched for variability in the measured Rp/R* over time to trace changes in the structure of the planetary envelope but none found within the data precision. In addition to the transit event, we tentatively detect occultation signal in the TESS data with an eclipse depth of ~27 +/- 11 ppm. Using the models of outgassed atmospheres from the literature we find that the thermal emission from the planet can mostly explain the observation. Based on this, we predict that NIR/MIR observations with JWST should be able to detect silicate species in the atmosphere of the planet. This could also reveal important clues about the planetary interior and help disentangle planet formation and evolution models., Comment: 17 pages, 10 + 3 figures, 4 tables, accepted for publication in A&A (abstract abbreviated)

Published
2023
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37. Women’s Empowerment in Local and Global Fiction: From Toba Beyond

Author

Karisma erikson tarigan and Rosa Maria Simamora

Subjects
women's empowerment, literature, gender roles, Language. Linguistic theory. Comparative grammar, P101-410
Abstract

This study explores women's empowerment in literature, focusing on the interplay between tradition and modernity across different cultural contexts. Employing comparative literary analysis, this research examines Lucy by Jamaica Kincaid and Mangalua by Idris Pasaribu. The methodology involves thematic and narrative analysis, where thematic analysis identifies key motifs related to empowerment, resistance, and gender roles, while narrative analysis examines how each character's story arc reflects broader societal norms. Through these analyses, the study highlights how each protagonist navigates societal expectations and challenges gender norms within traditional and modern frameworks. Findings indicate that both novels use women’s empowerment as a lens to critique and reshape cultural expectations, offering insights into gender roles across varied societies. The study concludes with recommendations for further research on cross-cultural gender narratives, acknowledges the limitations of focusing on only two novels, and suggests broader literary comparisons for future studies.

Published
2024
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38. Investigating the visible phase-curve variability of 55 Cnc e

Author

Valdés, E. A. Meier, Morris, B. M., Demory, B. -O., Brandeker, A., Kitzmann, D., Benz, W., Deline, A., Florén, H. -G., Sousa, S. G., Bourrier, V., Singh, V., Heng, K., Strugarek, A., Bower, D. J., Jäggi, N., Carone, L., Lendl, M., Jones, K., Oza, A. V., Demangeon, O. D. S., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Sarajlic, M., Scandariato, G., Ségransan, D., Sicilia, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A., Wilson, T. G., and Wolter, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

55 Cnc e is an ultra-short period super-Earth transiting a Sun-like star. Previous observations in the optical range detected a time-variable flux modulation that is phased with the planetary orbital period, whose amplitude is too large to be explained by reflected light and thermal emission alone. The goal of the study is to investigate the origin of the variability and timescale of the phase-curve modulation in 55 Cnc e. To this end, we used the CHaracterising ExOPlanet Satellite (CHEOPS), whose exquisite photometric precision provides an opportunity to characterise minute changes in the phase curve from one orbit to the next. CHEOPS observed 29 individual visits of 55 Cnc e between March 2020 and February 2022. Based on these observations, we investigated the different processes that could be at the origin of the observed modulation. In particular, we built a toy model to assess whether a circumstellar torus of dust driven by radiation pressure and gravity might match the observed flux variability timescale. We find that the phase-curve amplitude and peak offset of 55 Cnc e do vary between visits. The sublimation timescales of selected dust species reveal that silicates expected in an Earth-like mantle would not survive long enough to explain the observed phase-curve modulation. We find that silicon carbide, quartz, and graphite are plausible candidates for the circumstellar torus composition because their sublimation timescales are long. The extensive CHEOPS observations confirm that the phase-curve amplitude and offset vary in time.We find that dust could provide the grey opacity source required to match the observations. However, the data at hand do not provide evidence that circumstellar material with a variable grain mass per unit area causes the observed variability. Future observations with the James Webb Space Telescope promise exciting insights into this iconic super-Earth., Comment: 27 pages, 22 figures. Accepted for publication on A&A

Published
2023
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39. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906

Author

Tuson, Amy, Queloz, Didier, Osborn, Hugh P., Wilson, Thomas G., Hooton, Matthew J., Beck, Mathias, Lendl, Monika, Olofsson, Göran, Fortier, Andrea, Bonfanti, Andrea, Brandeker, Alexis, Buchhave, Lars A., Cameron, Andrew Collier, Ciardi, David R., Collins, Karen A., Gandolfi, Davide, Garai, Zoltan, Giacalone, Steven, da Silva, João Gomes, Howell, Steve B., Patel, Jayshil A., Persson, Carina M., Serrano, Luisa M., Sousa, Sérgio G., Ulmer-Moll, Solène, Vanderburg, Andrew, Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Borsato, Luca, Broeg, Christopher, Cabrera, Juan, Charnoz, Sébastien, Conti, Dennis M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dragomir, Diana, Dressing, Courtney D., Ehrenreich, David, Erikson, Anders, Essack, Zahra, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Furlan, Elise, Gill, Holden, Gillon, Michaël, Gnilka, Crystal L., Gonzales, Erica, Güdel, Manuel, Günther, Maximilian N., Hoyer, Sergio, Isaak, Kate G., Jenkins, Jon M., Kiss, Laszlo L., Laskar, Jacques, Latham, David W., Law, Nicholas, Etangs, Alain Lecavelier des, Curto, Gaspare Lo, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Mann, Andrew W., Maxted, Pierre F. L., Mayor, Michel, McDermott, Scott, Mecina, Marko, Mordasini, Christoph, Mortier, Annelies, Nascimbeni, Valerio, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Pritchard, Tyler, Ragazzoni, Roberto, Rando, Nicola, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Savel, Arjun B., Scandariato, Gaetano, Schwarz, Richard P., Seager, Sara, Ségransan, Damien, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula M., Thomas, Nicolas, Torres, Guillermo, Tronsgaard, René, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valérie, Vanderspek, Roland, Venturini, Julia, Walton, Nicholas A., Winn, Joshua N., and Wohler, Bill

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., Comment: 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS

Published
2023
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40. Refined parameters of the HD 22946 planetary system and the true orbital period of planet d

Author

Garai, Z., Osborn, H. P., Gandolfi, D., Brandeker, A., Sousa, S. G., Lendl, M., Bekkelien, A., Broeg, C., Cameron, A. Collier, Egger, J. A., Hooton, M. J., Alibert, Y., Delrez, L., Fossati, L., Salmon, S., Wilson, T. G., Bonfanti, A., Tuson, A., Ulmer-Moll, S., Serrano, L. M., Borsato, L., Alonso, R., Anglada, G., Asquier, J., Navascues, D. Barrado y, Barros, S. C. C., Bárczy, T., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfils, X., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Van Eylen, V., Fortier, A., Fridlund, M., Gillon, M., Van Grootel, V., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Kristiansen, M. H., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. HD 22946 is a bright star around which 3 transiting planets were identified via TESS photometry, but the true orbital period of the outermost planet d was unknown until now. We aim to use CHEOPS to uncover the true orbital period of HD 22946d and to refine the orbital and planetary properties of the system, especially the radii of the planets. We used the available TESS photometry of HD 22946 and observed several transits of the planets b, c, and d using CHEOPS. We identified 2 transits of planet d in the TESS photometry, calculated the most probable period aliases based on these data, and then scheduled CHEOPS observations. The photometric data were supplemented with ESPRESSO radial velocity data. Finally, a combined model was fitted to the entire dataset. We successfully determined the true orbital period of the planet d to be 47.42489 $\pm$ 0.00011 d, and derived precise radii of the planets in the system, namely 1.362 $\pm$ 0.040 R$_\oplus$, 2.328 $\pm$ 0.039 R$_\oplus$, and 2.607 $\pm$ 0.060 R$_\oplus$ for planets b, c, and d, respectively. Due to the low number of radial velocities, we were only able to determine 3$\sigma$ upper limits for these respective planet masses, which are 13.71 M$_\oplus$, 9.72 M$_\oplus$, and 26.57 M$_\oplus$. We estimated that another 48 ESPRESSO radial velocities are needed to measure the predicted masses of all planets in HD 22946. Planet c appears to be a promising target for future atmospheric characterisation. We can also conclude that planet d, as a warm sub-Neptune, is very interesting because there are only a few similar confirmed exoplanets to date. Such objects are worth investigating in the near future, for example in terms of their composition and internal structure.

Published
2023
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41. Two Warm Neptunes transiting HIP 9618 revealed by TESS & Cheops

Author

Osborn, Hugh P., Nowak, Grzegorz, Hébrard, Guillaume, Masseron, Thomas, Lillo-Box, J., Pallé, Enric, Bekkelien, Anja, Florén, Hans-Gustav, Guterman, Pascal, Simon, Attila E., Adibekyan, V., Bieryla, Allyson, Borsato, Luca, Brandeker, Alexis, Ciardi, David R., Cameron, Andrew Collier, Collins, Karen A., Egger, Jo A., Gandolfi, Davide, Hooton, Matthew J., Latham, David W., Lendl, Monika, Matthews, Elisabeth C., Tuson, Amy, Ulmer-Moll, Solène, Vanderburg, Andrew, Wilson, Thomas G., Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Arnold, Luc, Asquier, Joel, Navascues, David Barrado y, Baumjohann, Wolfgang, Beck, Thomas, Belinski, Alexandr A., Benz, Willy, Biondi, Federico, Boisse, Isabelle, Bonfils, Xavier, Broeg, Christopher, Buchhave, Lars A., Bárczy, Tamas, Barros, S. C. C., Cabrera, Juan, Guillen, Carlos Cardona, Carleo, Ilaria, Castro-González, Amadeo, Charnoz, Sébastien, Christiansen, Jessie, Cortes-Zuleta, Pia, Csizmadia, Szilard, Dalal, Shweta, Davies, Melvyn B., Deleuil, Magali, Delfosse, Xavier, Delrez, Laetitia, Demory, Brice-Olivier, Dunlavey, Ava B., Ehrenreich, David, Erikson, Anders, Fernandes, Rachel B., Fortier, Andrea, Forveille, Thierry, Fossati, Luca, Fridlund, Malcolm, Gillon, Michaël, Goeke, Robert F., Goliguzova, Maria V., Gonzales, Erica J., Günther, M. N., Güdel, Manuel, Heidari, Neda, Henze, Christopher E., Howell, Steve, Hoyer, Sergio, Frey, Jonas Immanuel, Isaak, Kate G., Jenkins, Jon M., Kiefer, Flavien, Kiss, Laszlo, Korth, Judith, Maxted, Pierre F. L., Laskar, Jacques, Etangs, Alain Lecavelier des, Lovis, Christophe, Lund, Michael B., Luque, Rafa, Magrin, Demetrio, Almenara, Jose Manuel, Martioli, Eder, Mecina, Marko, Medina, Jennifer V., Moldovan, Daniel, Morales-Calderón, María, Morello, Giuseppe, Moutou, Claire, Murgas, Felipe, Jensen, Eric L. N., Nascimbeni, Valerio, Olofsson, Göran, Ottensamer, Roland, Pagano, Isabella, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rando, Nicola, Rauer, Heike, Ribas, Ignasi, Ricker, George, Demangeon, Olivier D. S., Smith, Alexis M. S., Santos, Nuno, Scandariato, Gaetano, Seager, Sara, Sousa, Sergio G., Steller, Manfred, Szabó, Gyula M., Ségransan, Damien, Thomas, Nicolas, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valerie, Vanderspek, Roland, Walton, Nicholas, and Winn, Joshua N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright ($G=9.0$ mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of $3.9 \pm 0.044$ $R_\oplus$ (HIP 9618 b) and $3.343 \pm 0.039$ $R_\oplus$ (HIP 9618 c). While the 20.77291 day period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-day gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE and CAFE revealed a mass of $10.0 \pm 3.1 M_\oplus$ for HIP 9618 b, which, according to our interior structure models, corresponds to a $6.8\pm1.4\%$ gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of $< 18M_\oplus$. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion ($0.08^{+0.12}_{-0.05} M_\odot$) orbiting at $26^{+19}_{-11}$ au. This detection makes HIP 9618 one of only five bright ($K<8$ mag) transiting multi-planet systems known to host a planet with $P>50$ d, opening the door for the atmospheric characterisation of warm ($T_{\rm eq}<750$ K) sub-Neptunes., Comment: 19 pages, 16 figures, 9 tables. Accepted at MNRAS. CHEOPS, RV and ground-based photometric data is available on CDS at https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/523/3069

Published
2023
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42. TOI-5678 b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS

Author

Ulmer-Moll, S., Osborn, H. P., Tuson, A., Egger, J. A., Lendl, M., Maxted, P., Bekkelien, A., Simon, A. E., Olofsson, G., Adibekyan, V., Alibert, Y., Bonfanti, A., Bouchy, F., Brandeker, A., Fridlund, M., Gandolfi, D., Mordasini, C., Persson, C. M., Salmon, S., Serrano, L. M., Sousa, S. G., Wilson, T. G., Rieder, M., Hasiba, J., Asquier, J., Sicilia, D., Walter, I., Alonso, R., Anglada, G., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bárczy, T., Cabrera, J., Charnoz, S., Cointepas, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Eisner, N. L., Erikson, A., Fortier, A., Fossati, L., Gillon, M., Grieves, N., Güdel, M., Hagelberg, J., Helled, R., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Nascimbeni, V., Otegi, J., Ottensammer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Psaridi, A., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Smith, A. M. S., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., and Walton, N. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and for shedding light on the formation and evolution of planetary systems. Indeed, compared to hot Jupiters, the atmospheric properties and orbital parameters of cooler gas giants are unaltered by intense stellar irradiation and tidal effects. We identify long-period planets in the Transiting Exoplanet Survey Satellite (TESS) data as duo-transit events. To solve the orbital periods of TESS duo-transit candidates, we use the CHaracterising ExOPlanet Satellite (CHEOPS) to observe the highest-probability period aliases in order to discard or confirm a transit event at a given period. We also collect spectroscopic observations with CORALIE and HARPS in order to confirm the planetary nature and measure the mass of the candidates. We report the discovery of a warm transiting Neptune-mass planet orbiting TOI-5678. After four non-detections corresponding to possible periods, CHEOPS detected a transit event matching a unique period alias. Joint modeling reveals that TOI-5678 hosts a 47.73 day period planet. TOI-5678 b has a mass of 20 (+-4) Me and a radius of 4.91 (+-0.08 Re) . Using interior structure modeling, we find that TOI-5678 b is composed of a low-mass core surrounded by a large H/He layer with a mass of 3.2 (+1.7, -1.3) Me. TOI-5678 b is part of a growing sample of well-characterized transiting gas giants receiving moderate amounts of stellar insolation (11 Se). Precise density measurement gives us insight into their interior composition, and the objects orbiting bright stars are suitable targets to study the atmospheric composition of cooler gas giants., Comment: 17 pages, 10 figures, accepted to A&A

Published
2023
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43. Coronal Heating as Determined by the Solar Flare Frequency Distribution Obtained by Aggregating Case Studies

Author

Mason, James Paul, Werth, Alexandra, West, Colin G., Youngblood, Allison A., Woodraska, Donald L., Peck, Courtney, Lacjak, Kevin, Frick, Florian G., Gabir, Moutamen, Alsinan, Reema A., Jacobsen, Thomas, Alrubaie, Mohammad, Chizmar, Kayla M., Lau, Benjamin P., Dominguez, Lizbeth Montoya, Price, David, Butler, Dylan R., Biron, Connor J., Feoktistov, Nikita, Dewey, Kai, Loomis, N. E., Bodzianowski, Michal, Kuybus, Connor, Dietrick, Henry, Wolfe, Aubrey M., Guerrero, Matt, Vinson, Jessica, Starbuck, Peter, Litton, Shelby D, Beck, M. G., Fisch, Jean-Paul, West, Ayana, Muniz, Alexis A., Chavez, Luis, Upthegrove, Zachary T., Runyon, Brenton M., Salazar, J., Kritzberg, Jake E., Murrel, Tyler, Ho, Ella, LaFemina, Quintin Y., Elbashir, Sara I., Chang, Ethan C., Hudson, Zachary A., Nussbaum, Rosemary O., Kennedy, Kellen, Kim, Kevin, Arango, Camila Villamil, Albakr, Mohammed A., Rotter, Michael, Garscadden, A. J., Salcido-Alcontar JR, Antonio, Pearl, Harrison M., Stepaniak, Tyler, Marquez, Josie A., Marsh, Lauren, Andringa, Jesse C, Osogwin, Austin, Shields, Amanda M., Brookins, Sarah, Hach, Grace K., Clausi, Alexis R., Millican, Emily B., Jaimes, Alan A, Graham, Alaina S., Burritt, John J., Perez, J. S., Ramirez, Nathaniel, Suri, Rohan, Myer, Michael S., Kresek, Zoe M., Goldsberry, C. A., Payne, Genevieve K., Jourabchi, Tara, Hu, J., Lucca, Jeffrey, Feng, Zitian, Gilpatrick, Connor B., Khan, Ibraheem A., Warble, Keenan, Sweeney, Joshua D., Dorricott, Philip, Meyer, Ethan, Kothamdi, Yash S., Sohail, Arman S., Grell, Kristyn, Floyd, Aidan, Bard, Titus, Mathieson, Randi M., Reed, Joseph, Cisneros, Alexis, Payne, Matthew P., Jarriel, J. R., Mora, Jacqueline Rodriguez, Sundell, M. E., Patel, Kajal, Alesmail, Mohammad, Alnasrallah, Yousef A, Abdullah, Jumana T., Molina-Saenz, Luis, Tayman, K. E., Brown, Gabriel T., Kerr-Layton, Liana, Berriman-Rozen, Zachary D., Hiatt, Quinn, Kalra, Etash, Ong, Jason, Vadayar, Shreenija, Shannahan, Callie D., Benke, Evan, zhang, Jinhua, Geisman, Jane, Martyr, Cara, Ameijenda, Federico, Akruwala, Ushmi H., Nehring, Molly, Kissner, Natalie, Rule, Ian C., Learned, Tyler, Smith, Alexandra N., Mazzotta, Liam, Rounsefell, Tyndall, Eyeson, Elizabeth A., Shelby, Arlee K., Moll, Tyler S, Menke, Riley, Shahba, Hannan, House Jr., Tony A., Clark, David B., Burns, Annemarie C., de La Beaujardiere, Tristan, Trautwein, Emily D., Plantz, Will, Reeves, Justin, Faber, Ian, Buxton, B. W., Highhouse, Nigel, Landrey, Kalin, Hansen, Connor M, Chen, Kevin, Hales, Ryder Buchanan, Borgerding, Luke R., Guo, Mutian, Crow, Christian J., Whittall, Lloyd C., Simmons, Conor, Folarin, Adeduni, Parkinson, Evan J., Rahn, Anna L., Blevins, Olivia, Morelock, Annalise M., Kelly, Nicholas, Parker, Nathan L., Smith, Kelly, Plzak, Audrey E., Saeb, David, Hares, Cameron T., Parker, Sasha R., McCoy, Andrew, Pham, Alexander V., Lauzon, Megan, Kennedy, Cayla J., Reyna, Andrea B., Acosta, Daniela M. Meza, Cool, Destiny J., Steinbarth, Sheen L., Mendoza-Anselmi, Patricia, Plutt, Kaitlyn E., Kipp, Isabel M, Rakhmonova, M., Brown, Cameron L., Van Anne, Gabreece, Moss, Alexander P., Golden, Olivia, Kirkpatrick, Hunter B., Colleran, Jake R., Sullivan, Brandon J, Tran, Kevin, Carpender, Michael Andrew, Mundy, Aria T., Koenig, Greta, Oudakker, Jessica, Engelhardt, Rasce, Ales, Nolan, Wexler, Ethan Benjamin, Beato, Quinn I, Chen, Lily, Cochran, Brooke, Hill, Paula, Hamilton, Sean R., Hashiro, Kyle, Khan, Usman, Martinez, Alexa M., Brockman, Jennifer L., Mallory, Macguire, Reed, Charlie, Terrile, Richard, Singh, Savi, Watson, James Adam, Creany, Joshua B., Price, Nicholas K., Miften, Aya M., Tran, Bryn, Kamenetskiy, Margaret, Martinez, Jose R., Opp, Elena N., Huang, Jianyang, Fails, Avery M., Belei, Brennan J., Slocum, Ryan, Astalos, Justin, East, Andrew, Nguyen, Lena P., Pherigo, Callie C, East, Andrew N., Li, David Y., Nelson, Maya LI, Taylor, Nicole, Odbayar, Anand, Rives, Anna Linnea, Mathur, Kabir P., Billingsley, Jacob, Polikoff, Hyden, Driscoll, Michael, Wilson, Orion K., Lahmers, Kyle, Toon, Nathaniel J., Lippincott, Sam, Musgrave, Andrew J., Gregory, Alannah H., Pitsuean-Meier, Sedique, Jesse, Trevor, Smith, Corey, Miles, Ethan J., Kainz, Sabrina J. H. T., Ji, Soo Yeun, Nguyen, Lena, Aryan, Maryam, Dinser, Alexis M., Shortman, Jadon, Bastias, Catalina S, Umbricht, Thomas D, Cage, Breonna, Randolph, Parker, Pollard, Matthew, Simone, Dylan M., Aramians, Andrew, Brecl, Ariana E., Robert, Amanda M., Zenner, Thomas, Saldi, Maxwell, Morales, Gavin, Mendez, Citlali, Syed, Konner, Vogel, Connor Maklain, Cone, Rebecca A., Berhanu, Naomi, Carpenter, Emily, Leoni, Cecilia, Bryan, Samuel, Ramachandra, Nidhi, Shaw, Timothy, Lee, E. C., Monyek, Eli, Wegner, Aidan B., Sharma, Shajesh, Lister, Barrett, White, Jamison R., Willard, John S., Sulaiman, S. A, Blandon, Guillermo, Narayan, Anoothi, Ruger, Ryan, Kelley, Morgan A., Moreno, Angel J., Balcer, Leo M, Ward-Chene, N. R. D., Shelby, Emma, Reagan, Brian D., Marsh, Toni, Sarkar, Sucheta, Kelley, Michael P., Fell, Kevin, Balaji, Sahana, Hildebrand, Annalise K., Shoha, Dominick, Nandu, Kshmya, Tucker, Julia, Cancio, Alejandro R., Wang, Jiawei, Rapaport, Sarah Grace, Maravi, Aimee S., Mayer, Victoria A., Miller, Andrew, Bence, Caden, Koke, Emily, Fauntleroy, John T, Doermer, Timothy, Al-Ghazwi, Adel, Morgan, Remy, Alahmed, Mohammed S., Mathavan, Adam Izz Khan Mohd Reduan, Silvester, H. K., Weiner, Amanda M., Liu, Nianzi, Iovan, Taro, Jensen, Alexander V., AlHarbi, Yazeed A., Jiang, Yufan, Zhang, Jiaqi, Jones, Olivia M., Huang, Chenqi, Reh, Eileen N., Alhamli, Dania, Pettine, Joshua, Zhou, Chongrui, Kriegman, Dylan, Yang, Jianing, Ash, Kevin, Savage, Carl, Kaiser, Emily, Augenstein, Dakota N., Padilla, Jacqueline, Stark, Ethan K., Hansen, Joshua A., Kokes, Thomas, Huynh, Leslie, Sanchez-Sanchez, Gustavo, Jeseritz, Luke A., Carillion, Emma L., Vepa, Aditya V., Khanal, Sapriya, Behr, Braden, Martin, Logan S., McMullan, Jesse J., Zhao, Tianwei, Williams, Abigail K., Alqabani, Emeen, Prinster, Gale H., Horne, Linda, Ruggles-Delgado, Kendall, Otto, Grant, Gomez, Angel R., Nguyen, Leonardo, Brumley, Preston J., Venegas, Nancy Ortiz, Varela, Ilian, Brownlow, Jordi, Cruz, Avril, Leiker, Linzhi, Batra, Jasleen, Hutabarat, Abigail P., Nunes-Valdes, Dario, Jameson, Connor, Naqi, Abdulaziz, Adams, Dante Q., Biediger, Blaine B., Borelli, William T, Cisne, Nicholas A., Collins, Nathaniel A., Curnow, Tyler L., Gopalakrishnan, Sean, Griffin, Nicholas F., Herrera, Emanuel, McGarvey, Meaghan V., Mellett, Sarah, Overchuk, Igor, Shaver, Nathan, Stratmeyer, Cooper N., Vess, Marcus T., Juels, Parker, Alyami, Saleh A., Gale, Skylar, Wallace, Steven P., Hunter, Samuel C, Lonergan, Mia C., Stewart, Trey, Maksimuk, Tiffany E., Lam, Antonia, Tressler, Judah, Napoletano, Elena R., Miller, Joshua B., Roy, Marc G., Chanders, Jasey, Fischer, Emmalee, Croteau, A. J., Kuiper, Nicolas A., Hoffman, Alex, DeBarros, Elyse, Curry, Riley T., Brzostowicz, A., Courtney, Jonas, Zhao, Tiannie, Szabo, Emi, Ghaith, Bandar Abu, Slyne, Colin, Beck, Lily, Quinonez, Oliver, Collins, Sarah, Madonna, Claire A., Morency, Cora, Palizzi, Mallory, Herwig, Tim, Beauprez, Jacob N., Ghiassi, Dorsa, Doran, Caroline R., Yang, Zhanchao, Padgette, Hannah M., Dicken, Cyrus A., Austin, Bryce W., Phalen, Ethan J., Xiao, Catherine, Palos, Adler, Gerhardstein, Phillip, Altenbern, Ava L., Orbidan, Dan, Dorr, Jackson A., Rivas, Guillermo A., Ewing, Calvin A, Giebner, B. C., McEntee, Kelleen, Kite, Emily R., Crocker, K. A., Haley, Mark S., Lezak, Adrienne R., McQuaid, Ella, Jeong, Jacob, Albaum, Jonathan, Hrudka, E. M., Mulcahy, Owen T., Tanguma, Nolan C., Oishi-Holder, Sean, White, Zachary, Coe, Ryan W., Boyer, Christine, Chapman, Mitchell G., Fortino, Elise, Salgado, Jose A., Hellweg, Tim, Martinez, Hazelia K., Mitchell, Alexander J., Schubert, Stephanie H., Schumacher, Grace K, Tesdahl, Corey D, Uphoff, C. H., Vassilyev, Alexandr, Witkoff, Briahn, Wolle, Jackson R., Dice, Kenzie A., Behrer, Timothy A., Bowen, Troy, Campbell, Andrew J, Clarkson, Peter C, Duong, Tien Q., Hawat, Elijah, Lopez, Christian, Olson, Nathaniel P., Osborn, Matthew, Peou, Munisettha E., Vaver, Nicholas J., Husted, Troy, Kallemeyn, Nicolas Ian, Spangler, Ava A, Mccurry, Kyle, Schultze, Courtney, Troisi, Thomas, Thomas, Daniel, Ort, Althea E., Singh, Maya A., Soon, Caitlin, Patton, Catherine, Billman, Jayce A., Jarvis, Sam, Hitt, Travis, Masri, Mirna, Albalushi, Yusef J., Schofer, Matthew J, Linnane, Katherine B., Knott, Philip Whiting, Valencia, Whitney, Arias-Robles, Brian A., Ryder, Diana, Simone, Anna, Abrams, Jonathan M., Belknap, Annelene L., Rouse, Charlotte, Reynolds, Alexander, Petric, Romeo S. L., Gomez, Angel A., Meiselman-Ashen, Jonah B., Carey, Luke, Dias, John S., Fischer-White, Jules, Forbes, Aidan E., Galarraga, Gabriela, Kennedy, Forrest, Lawlor, Rian, Murphy, Maxwell J., Norris, Cooper, Quarderer, Josh, Waller, Caroline, Weber, Robert J., Gunderson, Nicole, Boyne, Tom, Gregory, Joshua A., Propper, Henry Austin, von Peccoz, Charles B. Beck, Branch, Donovan, Clarke, Evelyn, Cutler, Libby, Dabberdt, Frederick M., Das, Swagatam, Figueirinhas, John Alfred D., Fougere, Benjamin L., Roy, Zoe A., Zhao, Noah Y., Cox, Corben L., Barnhart, Logan D. W., Craig, Wilmsen B., Moll, Hayden, Pohle, Kyle, Mueller, Alexander, Smith, Elena K., Spicer, Benjamin C., Aycock, Matthew C., Bat-Ulzii, Batchimeg, Murphy, Madalyn C., Altokhais, Abdullah, Thornally, Noah R., Kleinhaus, Olivia R., Sarfaraz, Darian, Barnes, Grant M., Beard, Sara, Banda, David J, Davis, Emma A. B., Huebsch, Tyler J., Wagoner, Michaela, Griego, Justus, Hale, Jack J. Mc, Porter, Trevor J., Abrashoff, Riley, Phan, Denise M., Smith, Samantha M., Srivastava, Ashish, Schlenker, Jared A. W., Madsen, Kasey O., Hirschmann, Anna E., Rankin, Frederick C, Akbar, Zainab A., Blouin, Ethan, Coleman-Plante, Aislinn, Hintsa, Evan, Lookhoff, Emily, Amer, Hamzi, Deng, Tianyue, Dvorak, Peter, Minimo, Josh, Plummer, William C., Ton, Kelly, Solt, Lincoln, AlAbbas, Batool H., AlAwadhi, Areej A., Cooper, Nicholas M., Corbitt, Jessica S, Dunlap, Christian, Johnson, Owen, Malone, Ryan A., Tellez, Yesica, Wallace, Logan, Ta, Michael-Tan D., Wheeler, Nicola H., Ramirez, Ariana C., Huang, Shancheng, Mehidic, Amar, Christiansen, Katherine E, Desai, Om, Domke, Emerson N., Howell, Noah H., Allsbrook, Martin, Alnaji, Teeb, England, Colin, Siles, Nathan, Burton, Nicholas David, Cruse, Zoe, Gilmartin, Dalton, Kim, Brian T., Hattendorf, Elsie, Buhamad, Maryam, Gayou, Lily, Seglem, Kasper, Alkhezzi, Tameem, Hicks, Imari R., Fife, Ryann, Pelster, Lily M., Fix, Alexander, Sur, Sohan N., Truong, Joshua K., Kubiak, Bartlomiej, Bondar, Matthew, Shi, Kyle Z., Johnston, Julia, Acevedo, Andres B., Lee, Junwon, Solorio, William J., Johnston, Braedon Y., McCormick, Tyler, Olguin, Nicholas, Pastor, Paige J., Wilson, Evan M., Trunko, Benjamin L., Sjoroos, Chris, Adams, Kalvyn N, Bell, Aislyn, Brumage-Heller, Grant, Canales, Braden P., Chiles, Bradyn, Driscoll, Kailer H., Hill, Hallie, Isert, Samuel A., Ketterer, Marilyn, Kim, Matthew M., Mewhirter, William J., Phillips, Lance, Phommatha, Krista, Quinn, Megan S., Reddy, Brooklyn J., Rippel, Matthew, Russell, Bowman, Williams, Sajan, Pixley, Andrew M., Gapin, Keala C., Peterson, B., Ruprecht, Collin, Hardie, Isabelle, Li, Isaac, Erickson, Abbey, Gersabeck, Clint, Gopalani, Mariam, Allanqawi, Nasser, Burton, Taylor, Cahn, Jackson R., Conti, Reese, White, Oliver S., Rojec, Stewart, Hogen, Blake A., Swartz, Jason R., Dick, R., Battist, Lexi, Dunn, Gabrielle M., Gasser, Rachel, Logan, Timothy W., Sinkovic, Madeline, Schaller, Marcus T., Heintz, Danielle A., Enrich, Andrew, Sanchez, Ethan S., Perez, Freddy, Flores, Fernando, Kapla, Shaun D., Shockley, Michael C., Phillips, Justin, Rumley, Madigan, Daboub, Johnston, Karsh, Brennan J., Linders, Bridget, Chen, Sam, Do, Helen C., Avula, Abhinav, French, James M., Bertuccio, Chrisanna, Hand, Tyler, Lee, Adrianna J., Neeland, Brenna K, Salazar, Violeta, Andrew, Carter, Barmore, Abby, Beatty, Thomas, Alonzi, Nicholas, Brown, Ryan, Chandler, Olivia M., Collier, Curran, Current, Hayden, Delasantos, Megan E., Bonilla, Alberto Espinosa de los Monteros, Fowler, Alexandra A., Geneser, Julianne R., Gentry, Eleanor, Gustavsson, E. R., Hansson, Jonathan, Hao, Tony Yunfei, Herrington, Robert N., Kelly, James, Kelly, Teagan, Kennedy, Abigail, Marquez, Mathew J., Meillon, Stella, Palmgren, Madeleine L., Pesce, Anneliese, Ranjan, Anurag, Robertson, Samuel M., Smith, Percy, Smith, Trevor J, Soby, Daniel A., Stratton, Grant L., Thielmann, Quinn N., Toups, Malena C., Veta, Jenna S., Young, Trenton J., Maly, Blake, Manzanares, Xander R., Beijer, Joshua, George, Jacob D., Mills, Dylan P., Ziebold, Josh J, Chambers, Paige, Montoya, Michael, Cheang, Nathan M., Anderson, Hunter J., Duncan, Sheridan J., Ehrlich, Lauren, Hudson, Nathan C., Kiechlin, Jack L., Koch, Will, Lee, Justin, Menassa, Dominic, Oakes, S. H., Petersen, Audrey J., Bunsow, J. R. Ramirez, Bay, Joshua, Ramirez, Sacha, Fenwick, Logan D., Boyle, Aidan P., Hibbard, Lea Pearl, Haubrich, Calder, Sherry, Daniel P., Jenkins, Josh, Furney, Sebastian, Velamala, Anjali A., Krueger, Davis J., Thompson, William N., Chhetri, Jenisha, Lee, Alexis Ying-Shan, Ray, Mia G. V., Recchia, John C., Lengerich, Dylan, Taulman, Kyle, Romero, Andres C., Steward, Ellie N., Russell, Sloan, Hardwick, Dillon F., Wootten, Katelynn, Nguyen, Valerie A., Quispe, Devon, Ragsdale, Cameron, Young, Isabel, Atchley-Rivers, N. S., Stribling, Jordin L., Gentile, Julia G, Boeyink, Taylor A., Kwiatkowski, Daniel, Dupeyron, Tomi Oshima, Crews, Anastasia, Shuttleworth, Mitchell, Dresdner, Danielle C., Flackett, Lydia, Haratsaris, Nicholas, Linger, Morgan I, Misener, Jay H., Patti, Samuel, Pine, Tawanchai P., Marikar, Nasreen, Matessi, Giorgio, Routledge, Allie C., Alkaabi, Suhail, Bartman, Jessica L., Bisacca, Gabrielle E., Busch, Celeste, Edwards, Bree, Staudenmier, Caitlyn, Starling, Travis, McVey, Caden, Montano, Maximus, Contizano, Charles J., Taylor, Eleanor, McIntyre, James K., Victory, Andrew, McCammon, Glen S., Kimlicko, Aspen, Sheldrake, Tucker, Shelchuk, Grace, Von Reich, Ferin J., Hicks, Andrew J., O'neill, Ian, Rossman, Beth, Taylor, Liam C., MacDonald, William, Becker, Simone E., Han, Soonhee, O'Sullivan, Cian, Wilcove, Isaac, Brennan, David J., Hanley, Luke C., Hull, Owen, Wilson, Timothy R., Kalmus, Madison H., Berv, Owen A., Harris, Logan Swous, Doan, Chris H, Londres, Nathan, Parulekar, Anish, Adam, Megan M., Angwin, Abigail, Cabbage, Carter C., Colleran, Zachary, Pietras, Alex, Seux, Octave, Oros, Ryan, Wilkinson, Blake C., Nguyen, Khoa D, Trank-Greene, Maedee, Barone, Kevin M., Snyder, G. L., Biehle, Samuel J, Billig, Brennen, Almquist, Justin Thomas, Dixon, Alyssa M., Erickson, Benjamin, Evans, Nathan, Genne, SL, Kelly, Christopher M, Marcus, Serafima M., Ogle, Caleb, Patel, Akhil, Vendetti, Evan, Courtney, Olivia, Deel, Sean, Del Foco, Leonardo, Gjini, Michael, Haines, Jessica, Hoff, Isabelle J., Jones, M. R., Killian, Dominic, Kuehl, Kirsten, Kuester, Chrisanne, Lantz, Maxwell B., Lee, Christian J, Mauer, Graham, McKemey, Finbar K., Millican, Sarah J., Rosasco, Ryan, Stewart, T. C., VanEtten, Eleanor, Derwin, Zachary, Serio, Lauren, Sickler, Molly G., Blake, Cassidy A., Patel, Neil S., Fox, Margaret, Gray, Michael J, Ziegler, Lucas J., Kumar, Aman Priyadarshi, Polly, Madelyn, Mesgina, Sarah, McMorris, Zane, Griffin, Kyle J., Haile, L. N., Bassel, Claire, Dixon, Thomas J., Beattie, Ryan, Houck, Timothy J, Rodgers, Maeve, Trofino, Tyson R., Lukianow, Dax, Smart, Korben, Hall, Jacqueline L., Bone, Lauren, Baldwin, James O., Doane, Connor, Almohsen, Yousef A., Stamos, Emily, Acha, Iker, Kim, Jake, Samour II, Antonio E., Chavali, S., Kanokthippayakun, Jeerakit, Gotlib, Nicholas, Murphy, Ryan C., Archibald, Jack. W., Brimhall, Alexander J, Boyer, Aidan, Chapman, Logan T., Chadda, Shivank, Sibrell, Lisa, Vallery, Mia M., Conroy, Thomas C., Pan, Luke J., Balajonda, Brian, Fuhrman, Bethany E. S., Alkubaisi, Mohamed, Engelstad, Jacob, Dodrill, Joshua, Fuchs, Calvin R., Bullard-Connor, Gigi, Alhuseini, Isehaq, Zygmunt, James C., Sipowicz, Leo, Hayrynen, Griffin A., McGill, Riley M., Keating, Caden J., Hart, Omer, Cyr, Aidan St., Steinsberger, Christopher H., Thoman, Gerig, Wood, Travis M., Ingram, Julia A., Dominguez, J., Georgiades, Nathaniel James, Johnson, Matthew, Johnson, Sawyer, Pedersen, Alexander J., Ralapanawe, Anoush K, Thomas, Jeffrey J., Sato, Ginn A., Reynolds, Hope, Nasser, Liebe, Mizzi, Alexander Z., Damgaard, Olivia, Baflah, Abdulrahman A., Liu, Steven Y., Salindeho, Adam D., Norden, Kelso, Gearhart, Emily E., Krajnak, Zack, Szeremeta, Philip, Amos, Meggan, Shin, Kyungeun, Muckenthaler, Brandon A., Medialdea, Melissa, Beach, Simone, Wilson, Connor B., Adams, Elena R, Aldhamen, Ahmed, Harris, Coyle M., Hesse, Troy M., Golding, Nathan T., Larter, Zachary, Hernandez, Angel, Morales, Genaro, Traxler, Robert B., Alosaimi, Meshal, Fitton, Aidan F., Aaron, James Holland, Lee, Nathaniel F., Liao, Ryan Z., Chen, Judy, French, Katherine V., Loring, Justin, Colter, Aurora, McConvey, Rowan, Colozzi, Michael, Vann, John D., Scheck, Benjamin T., Weigand, Anthony A, Alhabeeb, Abdulelah, Idoine, Yolande, Woodard, Aiden L., Medellin, Mateo M., Ratajczyk, Nicholas O, Tobin, Darien P., Collins, Jack C., Horning, Thomas M., Pellatz, Nick, Pitten, John, Lordi, Noah, Patterson, Alyx, Hoang, Thi D, Zimmermann, Ingrid H, Wang, Hongda, Steckhahn, Daniel, Aradhya, Arvind J., Oliver, Kristin A., Cai, Yijian, Wang, Chaoran, Yegovtsev, Nikolay, Wu, Mengyu, Ganesan, Koushik, Osborne, Andrew, Wickenden, Evan, Meyer, Josephine C., Chaparro, David, Visal, Aseem, Liu, Haixin, Menon, Thanmay S., Jin, Yan, Wilson, John, Erikson, James W., Luo, Zheng, Shitara, Nanako, Nelson, Emma E, Geerdts, T. R., Ortiz, Jorge L Ramirez, and Lewandowski, H. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Flare frequency distributions represent a key approach to addressing one of the largest problems in solar and stellar physics: determining the mechanism that counter-intuitively heats coronae to temperatures that are orders of magnitude hotter than the corresponding photospheres. It is widely accepted that the magnetic field is responsible for the heating, but there are two competing mechanisms that could explain it: nanoflares or Alfv\'en waves. To date, neither can be directly observed. Nanoflares are, by definition, extremely small, but their aggregate energy release could represent a substantial heating mechanism, presuming they are sufficiently abundant. One way to test this presumption is via the flare frequency distribution, which describes how often flares of various energies occur. If the slope of the power law fitting the flare frequency distribution is above a critical threshold, $\alpha=2$ as established in prior literature, then there should be a sufficient abundance of nanoflares to explain coronal heating. We performed $>$600 case studies of solar flares, made possible by an unprecedented number of data analysts via three semesters of an undergraduate physics laboratory course. This allowed us to include two crucial, but nontrivial, analysis methods: pre-flare baseline subtraction and computation of the flare energy, which requires determining flare start and stop times. We aggregated the results of these analyses into a statistical study to determine that $\alpha = 1.63 \pm 0.03$. This is below the critical threshold, suggesting that Alfv\'en waves are an important driver of coronal heating., Comment: 1,002 authors, 14 pages, 4 figures, 3 tables, published by The Astrophysical Journal on 2023-05-09, volume 948, page 71

Published
2023
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44. Molecular and Dual-Isotopic Profiling of the Microbial Controls on Nitrogen Leaching in Agricultural Soils under Managed Aquifer Recharge

Author

Huang, Laibin, Levintal, Elad, Erikson, Christian Bernard, Coyotl, Adolfo, Horwath, William R, Dahlke, Helen E, and Rodrigues, Jorge L Mazza

Subjects
Nitrogen, Soil, Agriculture, Isotopes, Nitrates, Groundwater, NO3 (-) leaching, dual isotopes, metagenome, nitrification, denitrification, NO3− leaching, Environmental Sciences
Abstract

Nitrate (NO3-) leaching is a serious health and ecological concern in global agroecosystems, particularly those under the application of agricultural-managed aquifer recharge (Ag-MAR); however, there is an absence of information on microbial controls affecting NO3- leaching outcomes. We combine natural dual isotopes of NO3- (15N/14N and 18O/16O) with metagenomics, quantitative polymerase chain reaction (PCR), and a threshold indicator taxa analysis (TITAN) to investigate the activities, taxon profiles, and environmental controls of soil microbiome associated with NO3- leaching at different depths from Californian vineyards under Ag-MAR application. The isotopic signatures demonstrated a significant priming effect (P < 0.01) of Ag-MAR on denitrification activities in the topsoil (0-10 cm), with a 12-25-fold increase of 15N-NO3- and 18O-NO3- after the first 24 h of flooding, followed by a sharp decrease in the enrichment of both isotopes with ∼80% decline in denitrification activities thereafter. In contrast, deeper soils (60-100 cm) showed minimal or no denitrification activities over the course of Ag-MAR application, thus resulting in 10-20-fold of residual NO3- being leached. Metagenomic profiling and laboratory microcosm demonstrated that both nitrifying and denitrifying groups, responsible for controlling NO3- leaching, decreased in abundance and potential activity rates with soil depth. TITAN suggested that Nitrosocosmicus and Bradyrhizobium, as the major nitrifier and denitrifier, had the highest and lowest tipping points with regard to the NO3- changes (P < 0.05), respectively. Overall, our study provides new insight into specific depth limitations of microbial controls on soil NO3- leaching in agroecosystems.

Published
2023

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