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1. A review of planetary systems around HD99492, HD147379, and HD190007 with HARPS-N

Author

Stalport, M., primary, Cretignier, M., additional, Udry, S., additional, John, A. Anna, additional, Wilson, T. G., additional, Delisle, J.-B., additional, Bonomo, A. S., additional, Buchhave, L. A., additional, Charbonneau, D., additional, Dalal, S., additional, Damasso, M., additional, Di Fabrizio, L., additional, Dumusque, X., additional, Fiorenzano, A., additional, Harutyunyan, A., additional, Haywood, R. D., additional, Latham, D. W., additional, López-Morales, M., additional, Lorenzi, V., additional, Lovis, C., additional, Malavolta, L., additional, Molinari, E., additional, Mortier, A., additional, Pedani, M., additional, Pepe, F., additional, Pinamonti, M., additional, Poretti, E., additional, Rice, K., additional, and Sozzetti, A., additional

Published
2023
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3. Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems

Author

Bonomo, A. S., primary, Dumusque, X., additional, Massa, A., additional, Mortier, A., additional, Bongiolatti, R., additional, Malavolta, L., additional, Sozzetti, A., additional, Buchhave, L. A., additional, Damasso, M., additional, Haywood, R. D., additional, Morbidelli, A., additional, Latham, D. W., additional, Molinari, E., additional, Pepe, F., additional, Poretti, E., additional, Udry, S., additional, Affer, L., additional, Boschin, W., additional, Charbonneau, D., additional, Cosentino, R., additional, Cretignier, M., additional, Ghedina, A., additional, Lega, E., additional, López-Morales, M., additional, Margini, M., additional, Martínez Fiorenzano, A. F., additional, Mayor, M., additional, Micela, G., additional, Pedani, M., additional, Pinamonti, M., additional, Rice, K., additional, Sasselov, D., additional, Tronsgaard, R., additional, and Vanderburg, A., additional

Published
2023
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4. Confirmation and characterisation of three giant planets detected by TESS from the FIES/NOT and Tull/McDonald spectrographs

Author

Knudstrup, Emil, primary, Serrano, Luisa M., additional, Gandolfi, Davide, additional, Albrecht, Simon H., additional, Cochran, William D., additional, Endl, Michael, additional, MacQueen, Phillip, additional, Tronsgaard, René, additional, Bieryla, Allyson, additional, Buchhave, Lars A., additional, Stassun, Keivan, additional, Collins, Karen A., additional, Nowak, Grzegorz, additional, Deeg, Hans J., additional, Barkaoui, Khalid, additional, Safonov, Boris S., additional, Strakhov, Ivan A., additional, Belinski, Alexandre A., additional, Twicken, Joseph D., additional, Jenkins, Jon M., additional, Howard, Andrew W., additional, Isaacson, Howard, additional, Winn, Joshua N., additional, Collins, Kevin I., additional, Conti, Dennis M., additional, Furesz, Gabor, additional, Gan, Tianjun, additional, Kielkopf, John F., additional, Massey, Bob, additional, Murgas, Felipe, additional, Murphy, Lauren G., additional, Palle, Enric, additional, Quinn, Samuel N., additional, Reed, Phillip A., additional, Ricker, George R., additional, Seager, Sara, additional, Shiao, Bernie, additional, Schwarz, Richard P., additional, Srdoc, Gregor, additional, and Watanabe, David, additional

Published
2022
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7. Exoplanet atmospheres at high resolution through a modest-size telescope

Author

Bello-Arufe, Aaron, Buchhave, Lars A., Mendonça, João M., Tronsgaard, René, Heng, Kevin, Hoeijmakers, H. Jens, and Mayo, Andrew W.

Subjects
530 Physics, 520 Astronomy, 500 Science
Abstract

Ground-based, high-resolution spectrographs are providing us with an unprecedented view of the dynamics and chemistry of the atmospheres of planets outside the Solar System. While there are a large number of stable and precise high-resolution spectrographs on modest-size telescopes, it is the spectrographs at observatories with apertures larger than 3.5 m that dominate the atmospheric follow-up of exoplanets. In this work we explore the potential of characterising exoplanetary atmospheres with FIES, a high-resolution spectrograph at the 2.56 m Nordic Optical Telescope. We observed two transits of MASCARA-2 b (also known as KELT-20 b) and one transit of KELT-9 b to search for atomic iron, a species that has recently been discovered in both neutral and ionised forms in the atmospheres of these ultra-hot Jupiters using large telescopes. Using a cross-correlation method, we detect a signal of Fe II at the 4.5σ and 4.0σ level in the transits of MaSCARA-2 b. We also detect Fe II in the transit of KELT-9 b at the 8.5σ level. Although we do not find any significant Doppler shift in the signal of MASCARA-2 b, we do measure a moderate blueshift (3–6 km s−1) of the feature in KELT-9 b, which might be a manifestation of high-velocity winds transporting Fe II from the planetary dayside to the nightside. Our work demonstrates the feasibility of investigating exoplanet atmospheres with FIES, and it potentially unlocks a wealth of additional atmosphere detections with this and other high-resolution spectrographs mounted on similar-size telescopes.

Published
2022
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8. HD 207897 b: A dense sub-Neptune transiting a nearby and bright K-type star

Author

Heidari, N., primary, Boisse, I., additional, Orell-Miquel, J., additional, Hébrard, G., additional, Acuña, L., additional, Hara, N. C., additional, Lillo-Box, J., additional, Eastman, J. D., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Adibekyan, V., additional, Bieryla, A., additional, Bonfils, X., additional, Bouchy, F., additional, Barclay, T., additional, Brasseur, C. E., additional, Borgniet, S., additional, Bourrier, V., additional, Buchhave, L., additional, Behmard, A., additional, Beard, C., additional, Batalha, N. M., additional, Courcol, B., additional, Cortés-Zuleta, P., additional, Collins, K., additional, Carmona, A., additional, Crossfield, I. J. M., additional, Chontos, A., additional, Delfosse, X., additional, Dalal, S., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Díaz, R. F., additional, Dumusque, X., additional, Daylan, T., additional, Dragomir, D., additional, Delgado Mena, E., additional, Dressing, C., additional, Dai, F., additional, Dalba, P. A., additional, Ehrenreich, D., additional, Forveille, T., additional, Fulton, B., additional, Fetherolf, T., additional, Gaisné, G., additional, Giacalone, S., additional, Riazi, N., additional, Hoyer, S., additional, Hobson, M. J., additional, Howard, A. W., additional, Huber, D., additional, Hill, M. L., additional, Hirsch, L. A., additional, Isaacson, H., additional, Jenkins, J., additional, Kane, S. R., additional, Kiefer, F., additional, Luque, R., additional, Latham, D. W., additional, Lubin, J., additional, Lopez, T., additional, Mousis, O., additional, Moutou, C., additional, Montagnier, G., additional, Mignon, L., additional, Mayo, A., additional, Močnik, T., additional, Murphy, J. M. A., additional, Palle, E., additional, Pepe, F., additional, Petigura, E. A., additional, Rey, J., additional, Ricker, G., additional, Robertson, P., additional, Roy, A., additional, Rubenzahl, R. A., additional, Rosenthal, L. J., additional, Santerne, A., additional, Santos, N. C., additional, Sousa, S. G., additional, Stassun, K. G., additional, Stalport, M., additional, Scarsdale, N., additional, Strøm, P. A., additional, Seager, S., additional, Segransan, D., additional, Tenenbaum, P., additional, Tronsgaard, R., additional, Udry, S., additional, Vanderspek, R., additional, Vakili, F., additional, Winn, J., additional, and Weiss, L. M., additional

Published
2022
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9. The obliquity and atmosphere of the ultra-hot Jupiter TOI-1431b (MASCARA-5b): A misaligned orbit and no signs of atomic or molecular absorptions

Author

Stangret, M., primary, Pallé, E., additional, Casasayas-Barris, N., additional, Oshagh, M., additional, Bello-Arufe, A., additional, Luque, R., additional, Nascimbeni, V., additional, Yan, F., additional, Orell-Miquel, J., additional, Sicilia, D., additional, Malavolta, L., additional, Addison, B. C., additional, Buchhave, L. A., additional, Bonomo, A. S., additional, Borsa, F., additional, Cabot, S. H. C., additional, Cecconi, M., additional, Fischer, D. A., additional, Harutyunyan, A., additional, Mendonça, J. M., additional, Nowak, G., additional, Parviainen, H., additional, Sozzetti, A., additional, and Tronsgaard, R., additional

Published
2021
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10. Is ozone a reliable proxy for molecular oxygen?: I. The O2–O3 relationship for Earth-like atmospheres.

Author

Kozakis, Thea, Mendonça, João M., and Buchhave, Lars A.

Subjects
HABITABLE planets, OZONE, STELLAR spectra, TEMPERATURE inversions, NATURAL satellite atmospheres, PLANETARY atmospheres, SOLAR atmosphere
Abstract

Molecular oxygen (O2) paired with a reducing gas is regarded as a promising biosignature pair for the atmospheric characterization of terrestrial exoplanets. In circumstances when O2 may not be detectable in a planetary atmosphere (e.g., at mid-IR wavelengths) it has been suggested that ozone (O3), the photochemical product of O2, could be used as a proxy to infer the presence of O2. However, O3 production has a nonlinear dependence on O2 and is strongly influenced by the UV spectrum of the host star. To evaluate the reliability of O3 as a proxy for O2, we used Atmos, a 1D coupled climate and photochemistry code, to study the O2–O3 relationship for "Earth-like" habitable zone planets around a variety of stellar hosts (G0V-M5V) and O2 abundances. Overall, we found that the O2–O3 relationship differed significantly with stellar hosts and resulted in different trends for hotter stars (G0V-K2V) versus cooler stars (K5V-M5V). Planets orbiting hotter host stars counter-intuitively experience an increase in O3 when O2 levels are initially decreased from 100% Earth's present atmospheric level (PAL), with a maximum O3 abundance occurring at 25–55% PAL O2. As O2 abundance initially decreases, larger amounts of UV photons capable of O2 photolysis reach the lower (denser) regions of the atmosphere where O3 production is more efficient, thus resulting in these increased O3 levels. This effect does not occur for cooler host stars (K5V-M5V), since the weaker incident UV flux does not allow O3 formation to occur at dense enough regions of the atmosphere where the faster O3 production can outweigh a smaller source of O2 from which to create O3. Thus, planets experiencing higher amounts of incident UV possessed larger stratospheric temperature inversions, leading to shallower O3 features in planetary emission spectra. Overall it will be extremely difficult (or impossible) to infer precise O2 levels from an O3 measurement, however, with information about the UV spectrum of the host star and context clues, O3 will provide valuable information about potential surface habitability of an exoplanet. [ABSTRACT FROM AUTHOR]

Published
2022
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12. Three years of HARPS-N high-resolution spectroscopy and precise radial velocity data for the Sun

Author

Dumusque, X., primary, Cretignier, M., additional, Sosnowska, D., additional, Buchschacher, N., additional, Lovis, C., additional, Phillips, D. F., additional, Pepe, F., additional, Alesina, F., additional, Buchhave, L. A., additional, Burnier, J., additional, Cecconi, M., additional, Cegla, H. M., additional, Cloutier, R., additional, Collier Cameron, A., additional, Cosentino, R., additional, Ghedina, A., additional, González, M., additional, Haywood, R. D., additional, Latham, D. W., additional, Lodi, M., additional, López-Morales, M., additional, Maldonado, J., additional, Malavolta, L., additional, Micela, G., additional, Molinari, E., additional, Mortier, A., additional, Pérez Ventura, H., additional, Pinamonti, M., additional, Poretti, E., additional, Rice, K., additional, Riverol, L., additional, Riverol, C., additional, San Juan, J., additional, Ségransan, D., additional, Sozzetti, A., additional, Thompson, S. J., additional, Udry, S., additional, and Wilson, T. G., additional

Published
2021
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13. High-resolution transmission spectroscopy of MASCARA-2 b with EXPRES

Author

Hoeijmakers, H. Jens, primary, Cabot, Samuel H. C., additional, Zhao, Lily, additional, Buchhave, Lars A., additional, Tronsgaard, René, additional, Davis, Allen B., additional, Kitzmann, Daniel, additional, Grimm, Simon L., additional, Cegla, Heather M., additional, Bourrier, Vincent, additional, Ehrenreich, David, additional, Heng, Kevin, additional, Lovis, Christophe, additional, and Fischer, Debra A., additional

Published
2020
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14. So close, so different: Characterization of the K2-36 planetary system with HARPS-N

Author

Andrew Collier Cameron, A. Coffinet, Ken Rice, Pedro Figueira, Stéphane Udry, Christopher A. Watson, Ennio Poretti, Annelies Mortier, Mercedes Lopez-Morales, David F. Phillips, Andrew Vanderburg, Lars A. Buchhave, Andrew W. Mayo, Michel Mayor, Emilio Molinari, Francesco Pepe, Mario Damasso, Aldo S. Bonomo, Alessandro Sozzetti, David W. Latham, Luca Malavolta, Li Zeng, Science & Technology Facilities Council, European Commission, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Stars: individual: k2-36, FOS: Physical sciences, Library science, Astrophysics, 01 natural sciences, K2-36 (TYC 266-622-1, EPIC 201713348) [Stars- individual], 0103 physical sciences, QB Astronomy, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, QC, QB, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], 010308 nuclear & particles physics, DAS, Astronomy and Astrophysics, individual: k2-36 [Stars], Planets and satellites: detection, Planets and satellites: composition, Techniques: radial velocities, detection [Planets and satellites], QC Physics, 13. Climate action, Space and Planetary Science, astro-ph.EP, composition [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract

K2-36 is a K dwarf orbited by two small ($R_{\rm b}=1.43\pm0.08$ $R_\oplus$ and $R_{\rm c}=3.2\pm0.3$ $R_\oplus$), close-in ($a_{\rm b}$=0.022 AU and $a_{\rm c}$=0.054 AU) transiting planets discovered by Kepler/K2. They are representatives of two families of small planets ($R_{\rm p}$, Comment: Accepted for publication on Astronomy $\&$ Astrophysics

Published
2019
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15. An ultra-short period rocky super-Earth orbiting the G2-star HD 80653

Author

Frustagli, G., primary, Poretti, E., additional, Milbourne, T., additional, Malavolta, L., additional, Mortier, A., additional, Singh, V., additional, Bonomo, A. S., additional, Buchhave, L. A., additional, Zeng, L., additional, Vanderburg, A., additional, Udry, S., additional, Andreuzzi, G., additional, Collier-Cameron, A., additional, Cosentino, R., additional, Damasso, M., additional, Ghedina, A., additional, Harutyunyan, A., additional, Haywood, R. D., additional, Latham, D. W., additional, López-Morales, M., additional, Lorenzi, V., additional, Martinez Fiorenzano, A. F., additional, Mayor, M., additional, Micela, G., additional, Molinari, E., additional, Pepe, F., additional, Phillips, D., additional, Rice, K., additional, and Sozzetti, A., additional

Published
2020
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16. The Hubble PanCET program: an extensive search for metallic ions in the exosphere of GJ 436 b

Author

dos Santos, L. A., primary, Ehrenreich, D., additional, Bourrier, V., additional, Lecavelier des Etangs, A., additional, López-Morales, M., additional, Sing, D. K., additional, Ballester, G., additional, Ben-Jaffel, L., additional, Buchhave, L. A., additional, García Muñoz, A., additional, Henry, G. W., additional, Kataria, T., additional, Lavie, B., additional, Lavvas, P., additional, Lewis, N. K., additional, Mikal-Evans, T., additional, Sanz-Forcada, J., additional, and Wakeford, H., additional

Published
2019
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17. So close, so different: characterization of the K2-36 planetary system with HARPS-N

Author

Damasso, M., primary, Zeng, L., additional, Malavolta, L., additional, Mayo, A., additional, Sozzetti, A., additional, Mortier, A., additional, Buchhave, L. A., additional, Vanderburg, A., additional, Lopez-Morales, M., additional, Bonomo, A. S., additional, Cameron, A. C., additional, Coffinet, A., additional, Figueira, P., additional, Latham, D. W., additional, Mayor, M., additional, Molinari, E., additional, Pepe, F., additional, Phillips, D. F., additional, Poretti, E., additional, Rice, K., additional, Udry, S., additional, and Watson, C. A., additional

Published
2019
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19. Hubble PanCET: an extended upper atmosphere of neutral hydrogen around the warm Neptune GJ 3470b

Author

Bourrier, V., primary, Lecavelier des Etangs, A., additional, Ehrenreich, D., additional, Sanz-Forcada, J., additional, Allart, R., additional, Ballester, G. E., additional, Buchhave, L. A., additional, Cohen, O., additional, Deming, D., additional, Evans, T. M., additional, García Muñoz, A., additional, Henry, G. W., additional, Kataria, T., additional, Lavvas, P., additional, Lewis, N., additional, López-Morales, M., additional, Marley, M., additional, Sing, D. K., additional, and Wakeford, H. R., additional

Published
2018
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20. Eyes on K2-3: A system of three likely sub-Neptunes characterized with HARPS-N and HARPS

Author

Damasso, M., primary, Bonomo, A. S., additional, Astudillo-Defru, N., additional, Bonfils, X., additional, Malavolta, L., additional, Sozzetti, A., additional, Lopez, E., additional, Zeng, L., additional, Haywood, R. D., additional, Irwin, J. M., additional, Mortier, A., additional, Vanderburg, A., additional, Maldonado, J., additional, Lanza, A. F., additional, Affer, L., additional, Almenara, J.-M., additional, Benatti, S., additional, Biazzo, K., additional, Bignamini, A., additional, Borsa, F., additional, Bouchy, F., additional, Buchhave, L. A., additional, Cameron, A. C., additional, Carleo, I., additional, Charbonneau, D., additional, Claudi, R., additional, Cosentino, R., additional, Covino, E., additional, Delfosse, X., additional, Desidera, S., additional, Di Fabrizio, L., additional, Dressing, C., additional, Esposito, M., additional, Fares, R., additional, Figueira, P., additional, Fiorenzano, A. F. M., additional, Forveille, T., additional, Giacobbe, P., additional, González-Álvarez, E., additional, Gratton, R., additional, Harutyunyan, A., additional, Johnson, J. Asher, additional, Latham, D. W., additional, Leto, G., additional, Lopez-Morales, M., additional, Lovis, C., additional, Maggio, A., additional, Mancini, L., additional, Masiero, S., additional, Mayor, M., additional, Micela, G., additional, Molinari, E., additional, Motalebi, F., additional, Murgas, F., additional, Nascimbeni, V., additional, Pagano, I., additional, Pepe, F., additional, Phillips, D. F., additional, Piotto, G., additional, Poretti, E., additional, Rainer, M., additional, Rice, K., additional, Santos, N. C., additional, Sasselov, D., additional, Scandariato, G., additional, Ségransan, D., additional, Smareglia, R., additional, Udry, S., additional, Watson, C., additional, and Wünsche, A., additional

Published
2018
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21. The HARPS-N Rocky Planet Search

Author

Motalebi, F., Udry, S., Gillon, M., Lovis, C., Ségransan, D., Buchhave, L. A., Demory, B. O., Malavolta, L., Dressing, C. D., Sasselov, D., Rice, K., Charbonneau, D., Collier Cameron, A., Latham, D., Molinari, E., Pepe, F., Affer, L., Bonomo, A. S., Cosentino, R., Dumusque, X., Figueira, P., Fiorenzano, A. F. M., Gettel, S., Harutyunyan, A., Haywood, R. D., Johnson, J., Lopez, E., Lopez-Morales, M., Mayor, M., Micela, G., Mortier, A., Nascimbeni, V., Philips, D., Piotto, G., Pollacco, D., Queloz, D., Sozzetti, A., Vanderburg, A., and Watson, C. A.

Subjects
520 Astronomy
Abstract

We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V = 5.5) and close-by (6.5 pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935 ± 0.0003 days, on a quasi-circular orbit with a semi-major axis of 0.0382 ± 0.0003 AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date. From the amplitude of the radial velocity variation (2.25 ± 0.22 ms-1) and observed depth of the transit (359 ± 38 ppm), the planet mass and radius are estimated to be 4.36 ± 0.44 M⊕ and 1.606 ± 0.086 R⊕, leading to a mean density of 5.76 ± 1.09 g cm-3, suggesting a rocky composition. One additional planet with minimum-mass of 2.78 ± 0.65 M⊕ moves on a close-in, quasi-circular orbit with a period of 6.767 ± 0.004 days. The third planet in the system has a period of 46.66 ± 0.08 days and a minimum-mass of 8.94 ± 1.13 M⊕, at 0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ± 0.11. The period of this planet is close to the rotational period of the star estimated from variations of activity indicators (42.3 ± 0.1 days). The planetary origin of the signal is, however, thepreferred solution as no indication of variation at the corresponding frequency is observed for activity-sensitive parameters. Finally, a fourth additional longer-period planet of mass of 71 M⊕ orbits the star in 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at a distance of 2.56 AU.

Published
2015
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23. The HARPS-N Rocky Planet Search

Author

Motalebi, F., primary, Udry, S., additional, Gillon, M., additional, Lovis, C., additional, Ségransan, D., additional, Buchhave, L. A., additional, Demory, B. O., additional, Malavolta, L., additional, Dressing, C. D., additional, Sasselov, D., additional, Rice, K., additional, Charbonneau, D., additional, Collier Cameron, A., additional, Latham, D., additional, Molinari, E., additional, Pepe, F., additional, Affer, L., additional, Bonomo, A. S., additional, Cosentino, R., additional, Dumusque, X., additional, Figueira, P., additional, Fiorenzano, A. F. M., additional, Gettel, S., additional, Harutyunyan, A., additional, Haywood, R. D., additional, Johnson, J., additional, Lopez, E., additional, Lopez-Morales, M., additional, Mayor, M., additional, Micela, G., additional, Mortier, A., additional, Nascimbeni, V., additional, Philips, D., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Sozzetti, A., additional, Vanderburg, A., additional, and Watson, C. A., additional

Published
2015
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26. Constraining planet structure from stellar chemistry: the cases of CoRoT-7, Kepler-10, and Kepler-93

Author

Pedro Figueira, Stéphane Udry, S. G. Sousa, Christoph Mordasini, Francesco Pepe, Nuno C. Santos, E. Delgado-Mena, Willy Benz, Annelies Mortier, Alexandre Santerne, Lars A. Buchhave, V. Adibekyan, Caroline Dorn, European Commission, and University of St Andrews. School of Physics and Astronomy

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Kepler, spectroscopic [Techniques], Planet, Abundance (ecology), 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Line (formation), Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, 3rd-DAS, Planetary systems, detection [Planets and satellites], Stars, QC Physics, 13. Climate action, Space and Planetary Science, abundances [Stars], Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Low Mass, Mass fraction, Astrophysics - Earth and Planetary Astrophysics
Abstract

We explore the possibility that the stellar relative abundances of different species can be used to constrain the bulk abundances of known transiting rocky planets. We use high resolution spectra to derive stellar parameters and chemical abundances for Fe, Si, Mg, O, and C in three stars hosting low mass, rocky planets: CoRoT-7, Kepler-10, and Kepler-93. These planets follow the same line along the mass-radius diagram, pointing toward a similar composition. The derived abundance ratios are compared with the solar values. With a simple stoichiometric model, we estimate the iron mass fraction in each planet, assuming stellar composition. We show that in all cases, the iron mass fraction inferred from the mass-radius relationship seems to be in good agreement with the iron abundance derived from the host star's photospheric composition. The results suggest that stellar abundances can be used to add constraints on the composition of orbiting rocky planets., Comment: A&A Letters, in press

Published
2015
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27. Characterization of the planetary system Kepler-101 with HARPS-N

Author

Bonomo, A. S., primary, Sozzetti, A., additional, Lovis, C., additional, Malavolta, L., additional, Rice, K., additional, Buchhave, L. A., additional, Sasselov, D., additional, Cameron, A. C., additional, Latham, D. W., additional, Molinari, E., additional, Pepe, F., additional, Udry, S., additional, Affer, L., additional, Charbonneau, D., additional, Cosentino, R., additional, Dressing, C. D., additional, Dumusque, X., additional, Figueira, P., additional, Fiorenzano, A. F. M., additional, Gettel, S., additional, Harutyunyan, A., additional, Haywood, R. D., additional, Horne, K., additional, Lopez-Morales, M., additional, Mayor, M., additional, Micela, G., additional, Motalebi, F., additional, Nascimbeni, V., additional, Phillips, D. F., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ségransan, D., additional, Szentgyorgyi, A., additional, and Watson, C., additional

Published
2014
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28. HATS-2b: A transiting extrasolar planet orbiting aK-type star showing starspot activity

Author

Mohler-Fischer, M., primary, Mancini, L., additional, Hartman, J. D., additional, Bakos, G. Á., additional, Penev, K., additional, Bayliss, D., additional, Jordán, A., additional, Csubry, Z., additional, Zhou, G., additional, Rabus, M., additional, Nikolov, N., additional, Brahm, R., additional, Espinoza, N., additional, Buchhave, L. A., additional, Béky, B., additional, Suc, V., additional, Csák, B., additional, Henning, T., additional, Wright, D. J., additional, Tinney, C. G., additional, Addison, B. C., additional, Schmidt, B., additional, Noyes, R. W., additional, Papp, I., additional, Lázár, J., additional, Sári, P., additional, and Conroy, P., additional

Published
2013
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29. HAT-P-42b and HAT-P-43b

Author

Boisse, I., primary, Hartman, J. D., additional, Bakos, G. Á., additional, Penev, K., additional, Csubry, Z., additional, Béky, B., additional, Latham, D. W., additional, Bieryla, A., additional, Torres, G., additional, Kovács, G., additional, Buchhave, L. A., additional, Hansen, T., additional, Everett, M., additional, Esquerdo, G. A., additional, Szklenár, T., additional, Falco, E., additional, Shporer, A., additional, Fulton, B. J., additional, Noyes, R. W., additional, Stefanik, R. P., additional, Lázár, J., additional, Papp, I., additional, and Sári, P., additional

Published
2013
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30. HATS-2b: A transiting extrasolar planet orbiting a K-type star showing starspot activity.

Author

Mohler-Fischer, M., Mancini, L., Hartman, J. D., Bakos, G. Á., Penev, K., Bayliss, D., Jordán, A., Csubry, Z., Zhou, G., Rabus, M., Nikolov, N., Brahm, R., Espinoza, N., Buchhave, L. A., Béky, B., Suc, V., Csák, B., Henning, T., Wright, D. J., and Tinney, C. G.

Subjects
EXTRASOLAR planets, K stars, WAVELENGTHS, LIGHT curves, PARAMETER estimation
Abstract

We report the discovery of HATS-2b, the second transiting extrasolar planet detected by the HATSouth survey. HATS-2b is moving on a circular orbit around a V = 13:6 mag, K-type dwarf star (GSC 6665-00236), at a separation of 0:0230 ± 0:0003 AU and with a period of 1:3541 days. The planetary parameters have been robustly determined using a simultaneous fit of the HATSouth, MPG/ESO 2.2m/GROND, Faulkes Telescope South/Spectral transit photometry, and MPG/ESO 2.2m/FEROS, Euler 1.2m/CORALIE, AAT 3.9m/CYCLOPS radial-velocity measurements. HATS-2b has a mass of 1:37 ± 0:16 MJ, a radius of 1:14 ± 0:03 RJ, and an equilibrium temperature of 1567 ± 30 K. The host star has a mass of 0:88 ± 0:04 M☉ and a radius of 0:89 ± 0:02 R☉, and it shows starspot activity. We characterized the stellar activity by analyzing two photometric follow-up transit light curves taken with the GROND instrument, both obtained simultaneously in four optical bands (covering the wavelength range of 3860-9520 Å). The two light curves contain anomalies compatible with starspots on the photosphere of the host star along the same transit chord. [ABSTRACT FROM AUTHOR]

Published
2013
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31. High-resolution transmission spectroscopy of MASCARA-2 b with EXPRES

Author

Hoeijmakers, Jens H., Cabot, Samuel H. C., Zhao, Lily, Buchhave, Lars A., Tronsgaard, René, Davis, Allen B., Kitzmann, Daniel, Grimm, Simon L., Cegla, Heather M., Bourrier, Vincent, Ehrenreich, David, Heng, Kevin, Lovis, Christophe, and Fischer, Debra A.

Subjects
530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics, 500 Science, 3. Good health
Abstract

We report detections of atomic species in the atmosphere of MASCARA-2 b, using the first transit observations obtained with the newly commissioned EXPRES spectrograph. EXPRES is a highly stabilized optical echelle spectrograph, designed to detect stellar reflex motions with amplitudes down to 30 cm s−1, and has recently been deployed at the Lowell Discovery Telescope. By analyzing the transmission spectrum of the ultra-hot Jupiter MASCARA-2 b using the cross-correlation method, we confirm previous detections of Fe I, Fe II, and Na I, which likely originate in the upper regions of the inflated atmosphere. In addition, we report significant detections of Mg I and Cr II. The absorption strengths change slightly with time, possibly indicating different temperatures and chemistry in the day- and nightside terminators. Using the effective stellar line-shape variation induced by the transiting planet, we constrain the projected spin-orbit misalignment of the system to 1.6 ± 3.1 degrees, consistent with an aligned orbit. We demonstrate that EXPRES joins a suite of instruments capable of phase-resolved spectroscopy of exoplanet atmospheres.

32. Constraining planet structure from stellar chemistry: the cases of CoRoT-7, Kepler-10, and Kepler-93

Author

Adibekyan, V., Dorn, Caroline, Santos, N. C., Mortier, A., Benz, Willy, Sousa, S. G., Delgado-Mena, E., Buchhave, L., Pepe, F., Udry, S., Santerne, A., Figueira, P., and Mordasini, Christoph

Subjects
13. Climate action, 530 Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. We explore the possibility that the stellar relative abundances of different species can be used to constrain the bulk abundances of known transiting rocky planets. Methods. We use high resolution spectra to derive stellar parameters and chemical abundances for Fe, Si, Mg, O, and C in three stars hosting low mass, rocky planets: CoRoT-7, Kepler-10, and Kepler-93. These planets follow the same line along the mass-radius diagram, pointing toward a similar composition. The derived abundance ratios are compared with the solar values. With a simple stoichiometric model, we estimate the iron mass fraction in each planet, assuming stellar composition. Results. We show that in all cases, the iron mass fraction inferred from the mass-radius relationship seems to be in good agreement with the iron abundance derived from the host star's photospheric composition. Conclusions. The results suggest that stellar abundances can be used to add constraints on the composition of orbiting rocky planets.

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