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1. ESPRESSO high resolution transmission spectroscopy of WASP-76b

Author

Tabernero, H. M., Osorio, M. R. Zapatero, Allart, R., Borsa, F., Casasayas-Barris, N., Demangeon, O., Ehrenreich, D., Lillo-Box, J., Lovis, C., Pallé, E., Sousa, S. G., Rebolo, R., Santos, N. C., Pepe, F., Cristiani, S., Adibekyan, V., Prieto, C. Allende, Alibert, Yann, Barros, S. C. C., Bouchy, F., Bourrier, V., D'Odorico, V., Dumusque, X., Faria, J. P., Figueira, P., Santos, R. Génova, Hernández, J. I. González, Hojjatpanah, S., Curto, G. Lo, Lavie, B., Martins, C. J. A. P., Martins, J. H. C., Mehner, A., Micela, G., Molaro, P., Nunes, N. J., Poretti, E., Seidel, J. V., Sozzetti, A., Mascareño, A. Suárez, Udry, S., Aliverti, M., Affolter, M., Alves, D., Amate, M., Avila, G., Bandy, T., Benz, W., Bianco, A., Broeg, C., Cabral, A., Conconi, P., Coelho, J., Cumani, C., Deiries, S., Dekker, H., Delabre, B., Fragoso, A., Genoni, M., Genolet, L., Hughes, I., Knudstrup, J., Kerber, F., Landoni, M., Lizon, J. L., Maire, C., Manescau, A., Di Marcantonio, P., Mégevand, D., Monteiro, M., Moschetti, M., Mueller, E., Modigliani, A., Oggioni, L., Oliveira, A., Pariani, G., Pasquini, L., Rasilla, J. L., Redaelli, E., Riva, M., Santana-Tschudi, S., Santin, P., Santos, P., Segovia, A., Sosnowska, D., Spanò, P., Tenegi, F., Iwert, O., Zanutta, A., and Zerbi, F.

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

Aims. We report on ESPRESSO high-resolution transmission spectroscopic observations of two primary transits of the highly-irradiated, ultra-hot Jupiter-size planet WASP-76b. We investigate the presence of several key atomic and molecular features of interest that may reveal the atmospheric properties of the planet. Methods. We extracted two transmission spectra of WASP-76b with R approx 140,000 using a procedure that allowed us to process the full ESPRESSO wavelength range (3800-7880 A) simultaneously. We observed that at a high signal-to-noise ratio, the continuum of ESPRESSO spectra shows wiggles that are likely caused by an interference pattern outside the spectrograph. To search for the planetary features, we visually analysed the extracted transmission spectra and cross-correlated the observations against theoretical spectra of different atomic and molecular species. Results. The following atomic features are detected: Li I, Na I, Mg I, Ca II, Mn I, K I, and Fe I. All are detected with a confidence level between 9.2 sigma (Na I) and 2.8 sigma (Mg I). We did not detect the following species: Ti I, Cr I, Ni I, TiO, VO, and ZrO. We impose the following 1 sigma upper limits on their detectability: 60, 77, 122, 6, 8, and 8 ppm, respectively. Conclusions. We report the detection of Li I on WASP-76b for the first time. In addition, we found the presence of Na I and Fe I as previously reported in the literature. We show that the procedure employed in this work can detect features down to the level of ~ 0.1 % in the transmission spectrum and ~ 10 ppm by means of a cross-correlation method. We discuss the presence of neutral and singly ionised features in the atmosphere of WASP-76b., Comment: 20 pages, 19 figures, accepted for publication in Astronomy and Astrophysics

Published
2020
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2. ESPRESSO@VLT -- On-sky performance and first results

Author

Pepe, F., Cristiani, S., Rebolo, R., Santos, N. C., Dekker, H., Cabral, A., Di Marcantonio, P., Figueira, P., Curto, G. Lo, Lovis, C., Mayor, M., Mégevand, D., Molaro, P., Riva, M., Osorio, M. R. Zapatero, Amate, M., Manescau, A., Pasquini, L., Zerbi, F. M., Adibekyan, V., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Allart, R., Prieto, C. Allende, Álvarez, D., Alves, D., Avila, G., Baldini, V., Bandy, T., Barros, S. C. C., Benz, W., Bianco, A., Borsa, F., Bourrier, V., Bouchy, F., Broeg, C., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., D'Odorico, V., Damasso, M., Deiries, S., Delabre, B., Demangeon, O. D. S., Dumusque, X., Ehrenreich, D., Faria, J. P., Fragoso, A., Genolet, L., Genoni, M., Santos, R. Génova, Hernández, J. I. González, Hughes, I., Iwert, O., Kerber, F., Knudstrup, J., Landoni, M., Lavie, B., Lillo-Box, J., Lizon, J. -L., Maire, C., Martins, C. J . A. P., Mehner, A., Micela, G., Modigliani, A., Monteiro, M. A., Monteiro, M. J. P. F. G., Moschetti, M., Murphy, M. T., Nunes, N., Oggioni, L., Oliveira, A., Oshagh, M., Pallé, E., Pariani, G., Poretti, E., Rasilla, J. L., Rebordão, J., Redaelli, E. M., Tschudi, S. Santana, Santin, P., Santos, P., Ségransan, D., Schmidt, T. M., Segovia, A., Sosnowska, D., Sozzetti, A., Sousa, S. G., Spanò, P., Mascareño, A. Suárez, Tabernero, H., Tenegi, F., Udry, S., and Zanutta, A.

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

ESPRESSO is the new high-resolution spectrograph of ESO's Very-Large Telescope (VLT). It was designed for ultra-high radial-velocity precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UT) of the VLT at a spectral resolving power of 140,000 or 190,000 over the 378.2 to 788.7 nm wavelength range, or with all UTs together, turning the VLT into a 16-m diameter equivalent telescope in terms of collecting area, while still providing a resolving power of 70,000. We provide a general description of the ESPRESSO instrument, report on the actual on-sky performance, and present our Guaranteed-Time Observation (GTO) program with its first results. ESPRESSO was installed on the Paranal Observatory in fall 2017. Commissioning (on-sky testing) was conducted between December 2017 and September 2018. The instrument saw its official start of operations on October 1st, 2018, but improvements to the instrument and re-commissioning runs were conducted until July 2019. The measured overall optical throughput of ESPRESSO at 550 nm and a seeing of 0.65 arcsec exceeds the 10% mark under nominal astro-climatic conditions. We demonstrate a radial-velocity precision of better than 25 cm/s during one night and 50 cm/s over several months. These values being limited by photon noise and stellar jitter show that the performanceis compatible with an instrumental precision of 10 cm/s. No difference has been measured across the UTs neither in throughput nor RV precision. The combination of the large collecting telescope area with the efficiency and the exquisite spectral fidelity of ESPRESSO opens a new parameter space in RV measurements, the study of planetary atmospheres, fundamental constants, stellar characterisation and many other fields., Comment: 26 pages, 28 figures

Published
2020
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3. A precise architecture characterization of the $\pi$ Men planetary system

Author

Damasso, M., Sozzetti, A., Lovis, C., Barros, S. C. C., Sousa, S. G., Demangeon, O. D. S., Faria, J. P., Lillo-Box, J., Cristiani, S., Pepe, F., Rebolo, R., Santos, N. C., Osorio, M. R. Zapatero, Hernández, J. I. González, Amate, M., Pasquini, L., Zerbi, F. M., Adibekyan, V., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Allart, R., Prieto, C. Allende, Álvarez, D., Alves, D., Avila, G., Baldini, V., Bandy, T., Benz, W., Bianco, A., Borsa, F., Bossini, D., Bourrier, V., Bouchy, F., Broeg, C., Cabral, A., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., D'Odorico, V., Deiries, S., Dekker, H., Delabre, B., Di Marcantonio, P., Dumusque, X., Ehrenreich, D., Figueira, P., Fragoso, A., Genolet, L., Genoni, M., Santos, R. Génova, Hughes, I., Iwert, O., Kerber, F., Knudstrup, J., Landoni, M., Lavie, B., Lizon, J. -L., Curto, G. Lo, Maire, C., Martins, C. J . A. P., Mégevand, D., Mehner, A., Micela, G., Modigliani, A., Molaro, P., Monteiro, M. A., Monteiro, M. J. P. F. G., Moschetti, M., Mueller, E., Murphy, M. T., Nunes, N., Oggioni, L., Oliveira, A., Oshagh, M., Pallé, E., Pariani, G., Poretti, E., Rasilla, J. L., Rebordão, J., Redaelli, E. M., Riva, M., Tschudi, S. Santana, Santin, P., Santos, P., Ségransan, D., Schmidt, T. M., Segovia, A., Sosnowska, D., Spanò, P., Mascareño, A. Suárez, Tabernero, H., Tenegi, F., Udry, S., and Zanutta, A.

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

The bright star $\pi$ Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the ESO's Very-Large Telescope (VLT). The star hosts a multi-planet system (a transiting 4 M$_\oplus$ planet at $\sim$0.07 au, and a sub-stellar companion on a $\sim$2100-day eccentric orbit) which is particularly appealing for a precise multi-technique characterization. With the new ESPRESSO observations, that cover a time span of 200 days, we aim to improve the precision and accuracy of the planet parameters and search for additional low-mass companions. We also take advantage of new photometric transits of $\pi$ Men c observed by TESS over a time span that overlaps with that of the ESPRESSO follow-up campaign. We analyse the enlarged spectroscopic and photometric datasets and compare the results to those in the literature. We further characterize the system by means of absolute astrometry with Hipparcos and Gaia. We used the spectra of ESPRESSO for an independent determination of the stellar fundamental parameters. We present a precise characterization of the planetary system around $\pi$ Men. The ESPRESSO radial velocities alone (with typical uncertainty of 10 cm/s) allow for a precise retrieval of the Doppler signal induced by $\pi$ Men c. The residuals show an RMS of 1.2 m/s, and we can exclude companions with a minimum mass less than $\sim$2 M$_\oplus$ within the orbit of $\pi$ Men c). We improve the ephemeris of $\pi$ Men c using 18 additional TESS transits, and in combination with the astrometric measurements, we determine the inclination of the orbital plane of $\pi$ Men b with high precision ($i_{b}=45.8^{+1.4}_{-1.1}$ deg). This leads to the precise measurement of its absolute mass $m_{b}=14.1^{+0.5}_{-0.4}$ M$_{Jup}$, and shows that the planetary orbital planes are highly misaligned., Comment: Accepted for publication on A&A

Published
2020
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4. Characterization of the K2-38 planetary system. Unraveling one of the densest planets known to date

Author

Toledo-Padrón, B., Lovis, C., Mascareño, A. Suárez, Barros, S. C. C., Hernández, J. I. González, Sozzetti, A., Bouchy, F., Osorio, M. R. Zapatero, Rebolo, R., Cristiani, S., Pepe, F. A., Santos, N. C., Sousa, S. G., Tabernero, H. M., Lillo-Box, J., Bossini, D., Adibekyan, V., Allart, R., Damasso, M., D'Odorico, V., Figueira, P., Lavie, B., Curto, G. Lo, Mehner, A., Micela, G., Modigliani, A., Nunes, N. J., Pallé, E., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Prieto, C. Allende, Alves, D., Amate, M., Avila, G., Baldini, V., Bandy, T., Benatti, S., Benz, W., Bianco, A., Broeg, C., Cabral, A., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., Deiries, S., Dekker, H., Delabre, B., Demangeon, O., Di Marcantonio, P., Ehrenreich, D., Fragoso, A., Genolet, L., Genoni, M., Santos, R. Génova, Hughes, I., Iwert, O., Knudstrup, J., Landoni, M., Lizon, J. L., Maire, C., Manescau, A., Martins, C. J. A. P., Mégevand, D., Molaro, P., Monteiro, M. J. P. F. G., Monteiro, M. A., Moschetti, M., Mueller, E., Oggioni, L., Oliveira, A., Oshagh, M., Pariani, G., Pasquini, L., Poretti, E., Rasilla, J. L., Redaelli, E., Riva, M., Tschudi, S. Santana, Santin, P., Santos, P., Segovia, A., Sosnowska, D., Spanò, P., Tenegi, F., Udry, S., Zanutta, A., and Zerbi, F.

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

We characterized the transiting planetary system orbiting the G2V star K2-38 using the new-generation echelle spectrograph ESPRESSO. We carried out a photometric analysis of the available K2 photometric light curve of this star to measure the radius of its two known planets. Using 43 ESPRESSO high-precision radial velocity measurements taken over the course of 8 months along with the 14 previously published HIRES RV measurements, we modeled the orbits of the two planets through a MCMC analysis, significantly improving their mass measurements. Using ESPRESSO spectra, we derived the stellar parameters, $T_{\rm eff}$=5731$\pm$66, $\log g$=4.38$\pm$0.11~dex, and $[Fe/H]$=0.26$\pm$0.05~dex, and thus the mass and radius of K2-38, $M_{\star}$=1.03 $^{+0.04}_{-0.02}$~M$_{\oplus}$ and $R_{\star}$=1.06 $^{+0.09}_{-0.06}$~R$_{\oplus}$. We determine new values for the planetary properties of both planets. We characterize K2-38b as a super-Earth with $R_{\rm P}$=1.54$\pm$0.14~R$_{\rm \oplus}$ and $M_{\rm p}$=7.3$^{+1.1}_{-1.0}$~M$_{\oplus}$, and K2-38c as a sub-Neptune with $R_{\rm P}$=2.29$\pm$0.26~R$_{\rm \oplus}$ and $M_{\rm p}$=8.3$^{+1.3}_{-1.3}$~M$_{\oplus}$. We derived a mean density of $\rho_{\rm p}$=11.0$^{+4.1}_{-2.8}$~g cm$^{-3}$ for K2-38b and $\rho_{\rm p}$=3.8$^{+1.8}_{-1.1}$~g~cm$^{-3}$ for K2-38c, confirming K2-38b as one of the densest planets known to date. The best description for the composition of K2-38b comes from an iron-rich Mercury-like model, while K2-38c is better described by a rocky model with a H2 envelope. The maximum collision stripping boundary shows how giant impacts could be the cause for the high density of K2-38b. The irradiation received by each planet places them on opposite sides of the radius valley. We find evidence of a long-period signal in the radial velocity time-series whose origin could be linked to a 0.25-3~M$_{\rm J}$ planet or stellar activity., Comment: 16 pages, 14 figures

Published
2020
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5. Revisiting Proxima with ESPRESSO

Author

Mascareño, A. Suárez, Faria, J. P., Figueira, P., Lovis, C., Damasso, M., Hernández, J. I. González, Rebolo, R., Cristiano, S., Pepe, F., Santos, N. C., Osorio, M. R. Zapatero, Adibekyan, V., Hojjatpanah, S., Sozzetti, A., Murgas, F., Abreo, M., Affolter, M., Alibert, Y., Aliverti, M., Allart, R., Prieto, C. Allende, Alves, D., Amate, M., Avila, G., Baldini, V., Bandi, T., Barros, S. C. C., Bianco, A., Benz, W., Bouchy, F., Broeng, C., Cabral, A., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., D'Odorico, V., Deiries, S., Delabre, B., Di Marcantonio, P., Dumusque, X., Ehrenreich, D., Fragoso, A., Genolet, L., Genoni, M., Santos, R. Génova, Hughes, I., Iwert, O., Ferber, K., Knusdrtrup, J., Landoni, M., Lavie, B., Lillo-Box, J., Lizon, J., Curto, G. Lo, Maire, C., Manescau, A., Martins, C. J. A. P., Mégevand, D., Mehner, A., Micela, G., Modigliani, A., Molaro, P., Monteiro, M. A., Monteiro, M. J. P. F. G., Moschetti, M., Mueller, E., Nunes, N. J., Oggioni, L., Oliveira, A., Pallé, E., Pariani, G., Pasquini, L., Poretti, E., Rasilla, J. L., Redaelli, E., Riva, M., Tschudi, S. Santana, Santin, P., Santos, P., Segovia, A., Sosnoswska, D., Sousa, S., Spanò, P., Tenegi, F., Udry, S., Zanutta, A., and Zerbi, F.

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

We aim to confirm the presence of Proxima b using independent measurements obtained with the new ESPRESSO spectrograph, and refine the planetary parameters taking advantage of its improved precision. We analysed 63 spectroscopic ESPRESSO observations of Proxima taken during 2019. We obtained radial velocity measurements with a typical radial velocity photon noise of 26 cm/s. We ran a joint MCMC analysis on the time series of the radial velocity and full-width half maximum of the cross-correlation function to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with stellar activity. We confirm the presence of Proxima b independently in the ESPRESSO data. The ESPRESSO data on its own shows Proxima b at a period of 11.218 $\pm$ 0.029 days, with a minimum mass of 1.29 $\pm$ 0.13 Me. In the combined dataset we measure a period of 11.18427 $\pm$ 0.00070 days with a minimum mass of 1.173 $\pm$ 0.086 Me. We find no evidence of stellar activity as a potential cause for the 11.2 days signal. We find some evidence for the presence of a second short-period signal, at 5.15 days with a semi-amplitude of merely 40 cm/s. If caused by a planetary companion, it would correspond to a minimum mass of 0.29 $\pm$ 0.08 Me. We find that the FWHM of the CCF can be used as a proxy for the brightness changes and that its gradient with time can be used to successfully detrend the radial velocity data from part of the influence of stellar activity. The activity-induced radial velocity signal in the ESPRESSO data shows a trend in amplitude towards redder wavelengths. Velocities measured using the red end of the spectrograph are less affected by activity, suggesting that the stellar activity is spot-dominated. The data collected excludes the presence of extra companions with masses above 0.6 Me at periods shorter than 50 days., Comment: 25 pages, 26 figures

Published
2020
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6. 4MOST: Project overview and information for the First Call for Proposals

Author

de Jong, R. S., Agertz, O., Berbel, A. Agudo, Aird, J., Alexander, D. A., Amarsi, A., Anders, F., Andrae, R., Ansarinejad, B., Ansorge, W., Antilogus, P., Anwand-Heerwart, H., Arentsen, A., Arnadottir, A., Asplund, M., Auger, M., Azais, N., Baade, D., Baker, G., Baker, S., Balbinot, E., Baldry, I. K., Banerji, M., Barden, S., Barklem, P., Barthélémy-Mazot, E., Battistini, C., Bauer, S., Bell, C. P. M., Bellido-Tirado, O., Bellstedt, S., Belokurov, V., Bensby, T., Bergemann, M., Bestenlehner, J. M., Bielby, R., Bilicki, M., Blake, C., Bland-Hawthorn, J., Boeche, C., Boland, W., Boller, T., Bongard, S., Bongiorno, A., Bonifacio, P., Boudon, D., Brooks, D., Brown, M. J. I., Brown, R., Brüggen, M., Brynnel, J., Brzeski, J., Buchert, T., Buschkamp, P., Caffau, E., Caillier, P., Carrick, J., Casagrande, L., Case, S., Casey, A., Cesarini, I., Cescutti, G., Chapuis, D., Chiappini, C., Childress, M., Christlieb, N., Church, R., Cioni, M. -R. L., Cluver, M., Colless, M., Collett, T., Comparat, J., Cooper, A., Couch, W., Courbin, F., Croom, S., Croton, D., Daguisé, E., Dalton, G., Davies, L. J. M., Davis, T., de Laverny, P., Deason, A., Dionies, F., Disseau, K., Doel, P., Döscher, D., Driver, S. P., Dwelly, T., Eckert, D., Edge, A., Edvardsson, B., Youssoufi, D. El, Elhaddad, A., Enke, H., Erfanianfar, G., Farrell, T., Fechner, T., Feiz, C., Feltzing, S., Ferreras, I., Feuerstein, D., Feuillet, D., Finoguenov, A., Ford, D., Fotopoulou, S., Fouesneau, M., Frenk, C., Frey, S., Gaessler, W., Geier, S., Fusillo, N. Gentile, Gerhard, O., Giannantonio, T., Giannone, D., Gibson, B., Gillingham, P., González-Fernández, C., Gonzalez-Solares, E., Gottloeber, S., Gould, A., Grebel, E. K., Gueguen, A., Guiglion, G., Haehnelt, M., Hahn, T., Hansen, C. J., Hartman, H., Hauptner, K., Hawkins, K., Haynes, D., Haynes, R., Heiter, U., Helmi, A., Aguayo, C. Hernandez, Hewett, P., Hinton, S., Hobbs, D., Hoenig, S., Hofman, D., Hook, I., Hopgood, J., Hopkins, A., Hourihane, A., Howes, L., Howlett, C., Huet, T., Irwin, M., Iwert, O., Jablonka, P., Jahn, T., Jahnke, K., Jarno, A., Jin, S., Jofre, P., Johl, D., Jones, D., Jönsson, H., Jordan, C., Karovicova, I., Khalatyan, A., Kelz, A., Kennicutt, R., King, D., Kitaura, F., Klar, J., Klauser, U., Kneib, J., Koch, A., Koposov, S., Kordopatis, G., Korn, A., Kosmalski, J., Kotak, R., Kovalev, M., Kreckel, K., Kripak, Y., Krumpe, M., Kuijken, K., Kunder, A., Kushniruk, I., Lam, M. I, Lamer, G., Laurent, F., Lawrence, J., Lehmitz, M., Lemasle, B., Lewis, J., Li, B., Lidman, C., Lind, K., Liske, J., Lizon, J. -L., Loveday, J., Ludwig, H. -G., McDermid, R. M., Maguire, K., Mainieri, V., Mali, S., Mandel, H., Mandel, K., Mannering, L., Martell, S., Delgado, D. Martinez, Matijevic, G., McGregor, H., McMahon, R., McMillan, P., Mena, O., Merloni, A., Meyer, M. J., Michel, C., Micheva, G., Migniau, J. -E., Minchev, I., Monari, G., Muller, R., Murphy, D., Muthukrishna, D., Nandra, K., Navarro, R., Ness, M., Nichani, V., Nichol, R., Nicklas, H., Niederhofer, F., Norberg, P., Obreschkow, D., Oliver, S., Owers, M., Pai, N., Pankratow, S., Parkinson, D., Parry, I., Paschke, J., Paterson, R., Pecontal, A., Phillips, D., Pillepich, A., Pinard, L., Pirard, J., Piskunov, N., Plank, V., Plüschke, D., Pons, E., Popesso, P., Power, C., Pragt, J., Pramskiy, A., Pryer, D., Quattri, M., Queiroz, A. B. de Andrade, Quirrenbach, A., Rahurkar, S., Raichoor, A., Ramstedt, S., Rau, A., Recio-Blanco, A., Reiss, R., Renaud, F., Revaz, Y., Rhode, P., Richard, J., Richter, A. D., Rix, H. -W., Robotham, A. S. G., Roelfsema, R., Romaniello, M., Rosario, D., Rothmaier, F., Roukema, B., Ruchti, G., Rupprecht, G., Rybizki, J., Ryde, N., Saar, A., Sadler, E., Sahlén, M., Salvato, M., Sassolas, B., Saunders, W., Saviauk, A., Sbordone, L., Schmidt, T., Schnurr, O., Scholz, R. -D., Schwope, A., Seifert, W., Shanks, T., Sheinis, A., Sivov, T., Skúladóttir, Á., Smartt, S., Smedley, S., Smith, G., Smith, R., Sorce, J., Spitler, L., Starkenburg, E., Steinmetz, M., Stilz, I., Storm, J., Sullivan, M., Sutherland, W., Swann, E., Tamone, A., Taylor, E. N., Teillon, J., Tempel, E., ter Horst, R., Thi, W. -F., Tolstoy, E., Trager, S., Traven, G., Tremblay, P. -E., Tresse, L., Valentini, M., van de Weygaert, R., Ancker, M. van den, Veljanoski, J., Venkatesan, S., Wagner, L., Wagner, K., Walcher, C. J., Waller, L., Walton, N., Wang, L., Winkler, R., Wisotzki, L., Worley, C. C., Worseck, G., Xiang, M., Xu, W., Yong, D., Zhao, C., Zheng, J., Zscheyge, F., and Zucker, D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs ($R = \lambda/\Delta\lambda \sim 6500$), and 812 fibres transferring light to the high-resolution spectrograph ($R \sim 20\,000$). After a description of the instrument and its expected performance, a short overview is given of its operational scheme and planned 4MOST Consortium science; these aspects are covered in more detail in other articles in this edition of The Messenger. Finally, the processes, schedules, and policies concerning the selection of ESO Community Surveys are presented, commencing with a singular opportunity to submit Letters of Intent for Public Surveys during the first five years of 4MOST operations., Comment: Part of the 4MOST issue of The Messenger, published in preparation of 4MOST Community Workshop, see http://www.eso.org/sci/meetings/2019/4MOST.html

Published
2019
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7. ESPRESSO: The next European exoplanet hunter

Author

Pepe, F., Molaro, P., Cristiani, S., Rebolo, R., Santos, N. C., Dekker, H., Mégevand, D., Zerbi, F. M., Cabral, A., Di Marcantonio, P., Abreu, M., Affolter, M., Aliverti, M., Prieto, C. Allende, Amate, M., Avila, G., Baldini, V., Bristow, P., Broeg, C., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cupani, G., D'Odorico, V., De Caprio, V., Delabre, B., Dorn, R., Figueira, P., Fragoso, A., Galeotta, S., Genolet, L., Gomes, R., Hernández, J. I. González, Hughes, I., Iwert, O., Kerber, F., Landoni, M., Lizon, J. -L., Lovis, C., Maire, C., Mannetta, M., Martins, C., Monteiro, M., Oliveira, A., Poretti, E., Rasilla, J. L., Riva, M., Tschudi, S. Santana, Santos, P., Sosnowska, D., Sousa, S., Spanó, P., Tenegi, F., Toso, G., Vanzella, E., Viel, M., and Osorio, M. R. Zapatero

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

The acronym ESPRESSO stems for Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations; this instrument will be the next VLT high resolution spectrograph. The spectrograph will be installed at the Combined-Coud\'e Laboratory of the VLT and linked to the four 8.2 m Unit Telescopes (UT) through four optical Coud\'e trains. ESPRESSO will combine efficiency and extreme spectroscopic precision. ESPRESSO is foreseen to achieve a gain of two magnitudes with respect to its predecessor HARPS, and to improve the instrumental radial-velocity precision to reach the 10 cm/s level. It can be operated either with a single UT or with up to four UTs, enabling an additional gain in the latter mode. The incoherent combination of four telescopes and the extreme precision requirements called for many innovative design solutions while ensuring the technical heritage of the successful HARPS experience. ESPRESSO will allow to explore new frontiers in most domains of astrophysics that require precision and sensitivity. The main scientific drivers are the search and characterization of rocky exoplanets in the habitable zone of quiet, nearby G to M-dwarfs and the analysis of the variability of fundamental physical constants. The project passed the final design review in May 2013 and entered the manufacturing phase. ESPRESSO will be installed at the Paranal Observatory in 2016 and its operation is planned to start by the end of the same year., Comment: 12 pages, figures included, accepted for publication in Astron. Nachr

Published
2014

8. ESPRESSO high-resolution transmission spectroscopy of WASP-76 b

Author

Tabernero, H. M., Zapatero Osorio, M. R., Allart, R., Borsa, F., Casasayas Barris, N., Demangeon, O. D. S., Ehrenreich, D., Lillo Box, J., Lovis, C., Pallé, E., Sousa, S. G., Rebolo, R., Santos, N. C., Pepe, F., Cristiani, S., Adibekyan, V., Allende Prieto, C., Alibert, Y., Barros, S. C. C., Bouchy, F., Bourrier, V., D´Odorico, V., Dumusque, X., Faria, J. P., Figueira, P., Genova Santos, R., González Hernández, J. I., Hojjatpanah, S., Lo Curto, G., Lavie, B., Martins, C. J. A. P., Martins, J. H. C., Mehner, A., Micela, G., Molaro, P., Nunes, N. J., Poretti, E., Seidel, J. V., Sozzetti, A., Suárez Mascareño, A., Udry, S., Aliverti, M., Affolter, M., Alves, D., Amate, M., Ávila, G., Bandy, T., Benz, W., Bianco, A., Broeg, C., Cabral, A., Conconi, P., Coelho, J., Cumani, C., Deiries, S., Dekker, H., Delabre, B., Fragoso, A., Genoni, M., Genolet, L., Hughes, I., Knudstrup, J., Kerber, F., Landoni, M., Lizon, J. L., Maire, C., Manescau, A., Di Marcoantonio, P., Mégevand, D., Monteiro, M., Moschetti, M., Mueller, E., Modigliani, A., Oggioni, L., Oliveira, A., Pariani, G., Pasquini, L., Rasilla, J. L., Redaelli, E., Riva, M., Santana Tschudi, S., Santin, P., Santos, P., Segovia, A., Sosnowska, D., Spanò, P., Tenegi, F., Iwert, O., Zanutta, A., Zerbi, Filippo M., Cabral, A. [0000-0002-9433-871X], Monteiro, M. J. [0000-0003-0513-8116], Coelho, F. M. [0000-0002-4339-0550], Faria, J. [0000-0002-6728-244X], Santos, N. [0000-0003-4422-2919], European Research Council (ERC), Fundacao para a Ciencia e a Tecnologia (FCT), Agencia Estatal de Investigación (AEI), and Istituto Nazionale di Astrofisica (INAF)

Subjects
individual: WASP-76b [Planets and satellites], atmospheres [Planets and satellites]
Abstract

Based on guaranteed time observations collected at the European Southern Observatory under ESO programme 1102.C-0744 by the ESPRESSO Consortium. Aims. We report on ESPRESSO high-resolution transmission spectroscopic observations of two primary transits of the highly irradiated, ultra-hot Jupiter-sized planet, WASP-76b. We investigated the presence of several key atomic and molecular features of interest that may reveal the atmospheric properties of the planet. Methods. We extracted two transmission spectra of WASP-76b with R ≈ 140 000 using a procedure that allowed us to process the full ESPRESSO wavelength range (3800–7880 Å) simultaneously. We observed that at a high signal-to-noise ratio, the continuum of ESPRESSO spectra shows ‘wiggles’, which are likely caused by an interference pattern outside the spectrograph. To search for the planetary features, we visually analysed the extracted transmission spectra and cross-correlated the observations against theoretical spectra of different atomic and molecular species. Results. The following atomic features are detected: Li I, Na I, Mg I, Ca II, Mn I, K I, and Fe I. All are detected with a confidence level between 9.2 σ (Na I) and 2.8 σ (Mg I). We did not detect the following species: Ti I, Cr I, Ni I, TiO, VO, and ZrO. We impose the following 1 σ upper limits on their detectability: 60, 77, 122, 6, 8, and 8 ppm, respectively. Conclusions. We report the detection of Li I on WASP-76b for the first time. In addition, we confirm the presence of Na I and Fe I as previously reported in the literature. We show that the procedure employed in this work can detect features down to the level of ~0.1% in the transmission spectrum and ~10 ppm by means of a cross-correlation method. We discuss the presence of neutral and singly ionised features in the atmosphere of WASP-76b. This work was supported by FCT - FundacAo para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e InternacionalizacAo by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/ 32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01- 0145-FEDER-028987. V.A., S.G.S., S.C.C.B. acknowledge support from FCT through Investigador FCT contracts ns degrees IF/00650/2015/CP1273/CT0001; IF/00028/2014/CP1215/CT0002; IF/01312/2014/CP1215/CT0004. S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). J.P.F., O.D., and J.H.C.M. acknowledge support from FCT through national funds in the form of a work contract with the references DL 57/2016/CP1364/CT0005; DL 57/2016/CP1364/CT0004; DL 57/2016/CP1364/CT0007. H.M.T. and M.R.Z.O. acknowledge financial support from the Spanish Ministerio de Ciencia, Innovacion y Universidades (MICIU) through project AYA2016-79425-C3-2. A.S.M., R.R., J.I.G.H., C.A.P. acknowledge financial support from the Spanish MICIU project AYA2017-86389-P. J.I.G.H. acknowledges financial support from the Spanish MICIU under the 2013 Ramon y Cajal program RYC-2013-14875. This work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. The INAF authors acknowledge financial support of the Italian Ministry of Education, University, and Research with PRIN 201278X4FL and the Progetti Premiali funding scheme. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (projectFOUR ACES; grant agreement No 724427). N.J.N. acknowledges support from FCT through Investigador FCT contract and exploratory project IF/00852/2015, and project PTDC/FIS-OUT/29048/2017. J.V.S. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). Peerreview

Published
2021

9. ESPRESSO high-resolution transmission spectroscopy of WASP-76 b

Author

Tabernero, H. M., primary, Zapatero Osorio, M. R., additional, Allart, R., additional, Borsa, F., additional, Casasayas-Barris, N., additional, Demangeon, O., additional, Ehrenreich, D., additional, Lillo-Box, J., additional, Lovis, C., additional, Pallé, E., additional, Sousa, S. G., additional, Rebolo, R., additional, Santos, N. C., additional, Pepe, F., additional, Cristiani, S., additional, Adibekyan, V., additional, Allende Prieto, C., additional, Alibert, Y., additional, Barros, S. C. C., additional, Bouchy, F., additional, Bourrier, V., additional, D’Odorico, V., additional, Dumusque, X., additional, Faria, J. P., additional, Figueira, P., additional, Génova Santos, R., additional, González Hernández, J. I., additional, Hojjatpanah, S., additional, Lo Curto, G., additional, Lavie, B., additional, Martins, C. J. A. P., additional, Martins, J. H. C., additional, Mehner, A., additional, Micela, G., additional, Molaro, P., additional, Nunes, N. J., additional, Poretti, E., additional, Seidel, J. V., additional, Sozzetti, A., additional, Suárez Mascareño, A., additional, Udry, S., additional, Aliverti, M., additional, Affolter, M., additional, Alves, D., additional, Amate, M., additional, Avila, G., additional, Bandy, T., additional, Benz, W., additional, Bianco, A., additional, Broeg, C., additional, Cabral, A., additional, Conconi, P., additional, Coelho, J., additional, Cumani, C., additional, Deiries, S., additional, Dekker, H., additional, Delabre, B., additional, Fragoso, A., additional, Genoni, M., additional, Genolet, L., additional, Hughes, I., additional, Knudstrup, J., additional, Kerber, F., additional, Landoni, M., additional, Lizon, J. L., additional, Maire, C., additional, Manescau, A., additional, Di Marcantonio, P., additional, Mégevand, D., additional, Monteiro, M., additional, Moschetti, M., additional, Mueller, E., additional, Modigliani, A., additional, Oggioni, L., additional, Oliveira, A., additional, Pariani, G., additional, Pasquini, L., additional, Rasilla, J. L., additional, Redaelli, E., additional, Riva, M., additional, Santana-Tschudi, S., additional, Santin, P., additional, Santos, P., additional, Segovia, A., additional, Sosnowska, D., additional, Spanò, P., additional, Tenegi, F., additional, Iwert, O., additional, Zanutta, A., additional, and Zerbi, F., additional

Published
2021
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10. ESPRESSO at VLT

Author

Pepe, F., primary, Cristiani, S., additional, Rebolo, R., additional, Santos, N. C., additional, Dekker, H., additional, Cabral, A., additional, Di Marcantonio, P., additional, Figueira, P., additional, Lo Curto, G., additional, Lovis, C., additional, Mayor, M., additional, Mégevand, D., additional, Molaro, P., additional, Riva, M., additional, Zapatero Osorio, M. R., additional, Amate, M., additional, Manescau, A., additional, Pasquini, L., additional, Zerbi, F. M., additional, Adibekyan, V., additional, Abreu, M., additional, Affolter, M., additional, Alibert, Y., additional, Aliverti, M., additional, Allart, R., additional, Allende Prieto, C., additional, Álvarez, D., additional, Alves, D., additional, Avila, G., additional, Baldini, V., additional, Bandy, T., additional, Barros, S. C. C., additional, Benz, W., additional, Bianco, A., additional, Borsa, F., additional, Bourrier, V., additional, Bouchy, F., additional, Broeg, C., additional, Calderone, G., additional, Cirami, R., additional, Coelho, J., additional, Conconi, P., additional, Coretti, I., additional, Cumani, C., additional, Cupani, G., additional, D’Odorico, V., additional, Damasso, M., additional, Deiries, S., additional, Delabre, B., additional, Demangeon, O. D. S., additional, Dumusque, X., additional, Ehrenreich, D., additional, Faria, J. P., additional, Fragoso, A., additional, Genolet, L., additional, Genoni, M., additional, Génova Santos, R., additional, González Hernández, J. I., additional, Hughes, I., additional, Iwert, O., additional, Kerber, F., additional, Knudstrup, J., additional, Landoni, M., additional, Lavie, B., additional, Lillo-Box, J., additional, Lizon, J.-L., additional, Maire, C., additional, Martins, C. J. A. P., additional, Mehner, A., additional, Micela, G., additional, Modigliani, A., additional, Monteiro, M. A., additional, Monteiro, M. J. P. F. G., additional, Moschetti, M., additional, Murphy, M. T., additional, Nunes, N., additional, Oggioni, L., additional, Oliveira, A., additional, Oshagh, M., additional, Pallé, E., additional, Pariani, G., additional, Poretti, E., additional, Rasilla, J. L., additional, Rebordão, J., additional, Redaelli, E. M., additional, Santana Tschudi, S., additional, Santin, P., additional, Santos, P., additional, Ségransan, D., additional, Schmidt, T. M., additional, Segovia, A., additional, Sosnowska, D., additional, Sozzetti, A., additional, Sousa, S. G., additional, Spanò, P., additional, Suárez Mascareño, A., additional, Tabernero, H., additional, Tenegi, F., additional, Udry, S., additional, and Zanutta, A., additional

Published
2021
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11. A precise architecture characterization of theπMensae planetary system

Author

Damasso, M., primary, Sozzetti, A., additional, Lovis, C., additional, Barros, S. C. C., additional, Sousa, S. G., additional, Demangeon, O. D. S., additional, Faria, J. P., additional, Lillo-Box, J., additional, Cristiani, S., additional, Pepe, F., additional, Rebolo, R., additional, Santos, N. C., additional, Zapatero Osorio, M. R., additional, González Hernández, J. I., additional, Amate, M., additional, Pasquini, L., additional, Zerbi, F. M., additional, Adibekyan, V., additional, Abreu, M., additional, Affolter, M., additional, Alibert, Y., additional, Aliverti, M., additional, Allart, R., additional, Allende Prieto, C., additional, Álvarez, D., additional, Alves, D., additional, Avila, G., additional, Baldini, V., additional, Bandy, T., additional, Benz, W., additional, Bianco, A., additional, Borsa, F., additional, Bossini, D., additional, Bourrier, V., additional, Bouchy, F., additional, Broeg, C., additional, Cabral, A., additional, Calderone, G., additional, Cirami, R., additional, Coelho, J., additional, Conconi, P., additional, Coretti, I., additional, Cumani, C., additional, Cupani, G., additional, D’Odorico, V., additional, Deiries, S., additional, Dekker, H., additional, Delabre, B., additional, Di Marcantonio, P., additional, Dumusque, X., additional, Ehrenreich, D., additional, Figueira, P., additional, Fragoso, A., additional, Genolet, L., additional, Genoni, M., additional, Génova Santos, R., additional, Hughes, I., additional, Iwert, O., additional, Kerber, F., additional, Knudstrup, J., additional, Landoni, M., additional, Lavie, B., additional, Lizon, J.-L., additional, Lo Curto, G., additional, Maire, C., additional, Martins, C. J. A. P., additional, Mégevand, D., additional, Mehner, A., additional, Micela, G., additional, Modigliani, A., additional, Molaro, P., additional, Monteiro, M. A., additional, Monteiro, M. J. P. F. G., additional, Moschetti, M., additional, Mueller, E., additional, Murphy, M. T., additional, Nunes, N., additional, Oggioni, L., additional, Oliveira, A., additional, Oshagh, M., additional, Pallé, E., additional, Pariani, G., additional, Poretti, E., additional, Rasilla, J. L., additional, Rebordão, J., additional, Redaelli, E. M., additional, Riva, M., additional, Santana Tschudi, S., additional, Santin, P., additional, Santos, P., additional, Ségransan, D., additional, Schmidt, T. M., additional, Segovia, A., additional, Sosnowska, D., additional, Spanò, P., additional, Suárez Mascareño, A., additional, Tabernero, H., additional, Tenegi, F., additional, Udry, S., additional, and Zanutta, A., additional

Published
2020
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12. Characterization of the K2-38 planetary system

Author

Toledo-Padrón, B., primary, Lovis, C., additional, Suárez Mascareño, A., additional, Barros, S. C. C., additional, González Hernández, J. I., additional, Sozzetti, A., additional, Bouchy, F., additional, Zapatero Osorio, M. R., additional, Rebolo, R., additional, Cristiani, S., additional, Pepe, F. A., additional, Santos, N. C., additional, Sousa, S. G., additional, Tabernero, H. M., additional, Lillo-Box, J., additional, Bossini, D., additional, Adibekyan, V., additional, Allart, R., additional, Damasso, M., additional, D’Odorico, V., additional, Figueira, P., additional, Lavie, B., additional, Lo Curto, G., additional, Mehner, A., additional, Micela, G., additional, Modigliani, A., additional, Nunes, N. J., additional, Pallé, E., additional, Abreu, M., additional, Affolter, M., additional, Alibert, Y., additional, Aliverti, M., additional, Allende Prieto, C., additional, Alves, D., additional, Amate, M., additional, Avila, G., additional, Baldini, V., additional, Bandy, T., additional, Benatti, S., additional, Benz, W., additional, Bianco, A., additional, Broeg, C., additional, Cabral, A., additional, Calderone, G., additional, Cirami, R., additional, Coelho, J., additional, Conconi, P., additional, Coretti, I., additional, Cumani, C., additional, Cupani, G., additional, Deiries, S., additional, Dekker, H., additional, Delabre, B., additional, Demangeon, O., additional, Di Marcantonio, P., additional, Ehrenreich, D., additional, Fragoso, A., additional, Genolet, L., additional, Genoni, M., additional, Génova Santos, R., additional, Hughes, I., additional, Iwert, O., additional, Knudstrup, J., additional, Landoni, M., additional, Lizon, J. L., additional, Maire, C., additional, Manescau, A., additional, Martins, C. J. A. P., additional, Mégevand, D., additional, Molaro, P., additional, Monteiro, M. J. P. F. G., additional, Monteiro, M. A., additional, Moschetti, M., additional, Mueller, E., additional, Oggioni, L., additional, Oliveira, A., additional, Oshagh, M., additional, Pariani, G., additional, Pasquini, L., additional, Poretti, E., additional, Rasilla, J. L., additional, Redaelli, E., additional, Riva, M., additional, Santana Tschudi, S., additional, Santin, P., additional, Santos, P., additional, Segovia, A., additional, Sosnowska, D., additional, Spanò, P., additional, Tenegi, F., additional, Udry, S., additional, Zanutta, A., additional, and Zerbi, F., additional

Published
2020
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13. Revisiting Proxima with ESPRESSO

Author

Suárez Mascareño, A., primary, Faria, J. P., additional, Figueira, P., additional, Lovis, C., additional, Damasso, M., additional, González Hernández, J. I., additional, Rebolo, R., additional, Cristiani, S., additional, Pepe, F., additional, Santos, N. C., additional, Zapatero Osorio, M. R., additional, Adibekyan, V., additional, Hojjatpanah, S., additional, Sozzetti, A., additional, Murgas, F., additional, Abreu, M., additional, Affolter, M., additional, Alibert, Y., additional, Aliverti, M., additional, Allart, R., additional, Allende Prieto, C., additional, Alves, D., additional, Amate, M., additional, Avila, G., additional, Baldini, V., additional, Bandi, T., additional, Barros, S. C. C., additional, Bianco, A., additional, Benz, W., additional, Bouchy, F., additional, Broeng, C., additional, Cabral, A., additional, Calderone, G., additional, Cirami, R., additional, Coelho, J., additional, Conconi, P., additional, Coretti, I., additional, Cumani, C., additional, Cupani, G., additional, D’Odorico, V., additional, Deiries, S., additional, Delabre, B., additional, Di Marcantonio, P., additional, Dumusque, X., additional, Ehrenreich, D., additional, Fragoso, A., additional, Genolet, L., additional, Genoni, M., additional, Génova Santos, R., additional, Hughes, I., additional, Iwert, O., additional, Kerber, F., additional, Knusdstrup, J., additional, Landoni, M., additional, Lavie, B., additional, Lillo-Box, J., additional, Lizon, J., additional, Lo Curto, G., additional, Maire, C., additional, Manescau, A., additional, Martins, C. J. A. P., additional, Mégevand, D., additional, Mehner, A., additional, Micela, G., additional, Modigliani, A., additional, Molaro, P., additional, Monteiro, M. A., additional, Monteiro, M. J. P. F. G., additional, Moschetti, M., additional, Mueller, E., additional, Nunes, N. J., additional, Oggioni, L., additional, Oliveira, A., additional, Pallé, E., additional, Pariani, G., additional, Pasquini, L., additional, Poretti, E., additional, Rasilla, J. L., additional, Redaelli, E., additional, Riva, M., additional, Santana Tschudi, S., additional, Santin, P., additional, Santos, P., additional, Segovia, A., additional, Sosnowska, D., additional, Sousa, S., additional, Spanò, P., additional, Tenegi, F., additional, Udry, S., additional, Zanutta, A., additional, and Zerbi, F., additional

Published
2020
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15. ESPRESSO: The next European exoplanet hunter

Author

Pepe, F., primary, Molaro, P., additional, Cristiani, S., additional, Rebolo, R., additional, Santos, N.C., additional, Dekker, H., additional, Mégevand, D., additional, Zerbi, F.M., additional, Cabral, A., additional, Di Marcantonio, P., additional, Abreu, M., additional, Affolter, M., additional, Aliverti, M., additional, Allende Prieto, C., additional, Amate, M., additional, Avila, G., additional, Baldini, V., additional, Bristow, P., additional, Broeg, C., additional, Cirami, R., additional, Coelho, J., additional, Conconi, P., additional, Coretti, I., additional, Cupani, G., additional, D'Odorico, V., additional, De Caprio, V., additional, Delabre, B., additional, Dorn, R., additional, Figueira, P., additional, Fragoso, A., additional, Galeotta, S., additional, Genolet, L., additional, Gomes, R., additional, González Hernández, J.I., additional, Hughes, I., additional, Iwert, O., additional, Kerber, F., additional, Landoni, M., additional, Lizon, J.‐L., additional, Lovis, C., additional, Maire, C., additional, Mannetta, M., additional, Martins, C., additional, Monteiro, M., additional, Oliveira, A., additional, Poretti, E., additional, Rasilla, J.L., additional, Riva, M., additional, Santana Tschudi, S., additional, Santos, P., additional, Sosnowska, D., additional, Sousa, S., additional, Spanó, P., additional, Tenegi, F., additional, Toso, G., additional, Vanzella, E., additional, Viel, M., additional, and Zapatero Osorio, M.R., additional

Published
2014
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16. OmegaCAM at the VLT Survey Telescope

Author

Cappellaro, E., Andrea Baruffolo, Cascone, E., Greggio, L., Kuijken, K., Bender, R., Muschielok, B., Iwert, O., Mitsch, W., Nicklas, H., Valentijn, E. A., and Astronomy

Subjects
Instrumentation: detectors, Surveys
Abstract

We present the status of the VLT Survey Telescope (VST) and OmegaCAM projects. VST is a 2.6m telescope which will be integrated in the ESO-VLT environment at Paranal and will be equipped with a 16k × 16k CCD camera (OmegaCAM) covering 1 square degree with a resolution of 0.21 arcsec/pix. The main scope of this observing facility is the selection of targets for VLT science. It is expected that VST+OmegaCAM will become operational in spring 2004.

Published
2003

17. 4MOST - 4-metre multi-object spectroscopic telescope

Author

De Jong, R. S., Bellido-Tirado, O., Chiappini, C., Depagne, É., Haynes, R., Johl, D., Schnurr, O., Schwope, A., Walcher, J., Dionies, F., Haynes, D., Kelz, A., Kitaura, F. S., Lamer, G., Minchev, I., Müller, V., Nuza, S. E., Olaya, J. -C, Piffl, T., Popow, E., Steinmetz, M., Ural, U., Williams, M., Winkler, R., Wisotzki, L., Ansorge, W. R., Banerji, M., Solares, E. G., Irwin, M., Kennicutt Jr., R. C., King, D., McMahon, R., Koposov, S., Parry, I. R., Sun, D., Walton, N. A., Finger, G., Iwert, O., Krumpe, M., Lizon, J. -L, Vincenzo, M., Amans, J. -P, Bonifacio, P., Cohen, M., Francois, P., Jagourel, P., Mignot, S. B., Royer, F., Sartoretti, P., Bender, R., Grupp, F., Hess, H. -J, Lang-Bardl, F., Muschielok, B., Böhringer, H., Boller, T., Bongiorno, A., Brusa, M., Dwelly, T., Merloni, A., Nandra, K., Salvato, M., Pragt, J. H., Navarro, R., Gerlofsma, G., Roelfsema, R., Dalton, G. B., Middleton, K. F., Tosh, I. A., Boeche, C., Caffau, E., Christlieb, N., Grebel, E. K., Hansen, C., Koch, A., Ludwig, H. -G, Quirrenbach, A., Sbordone, L., Seifert, W., Thimm, G., Trifonov, T., Helmi, A., Trager, S. C., Feltzing, S., Korn, Andreas, Boland, W., De Jong, R. S., Bellido-Tirado, O., Chiappini, C., Depagne, É., Haynes, R., Johl, D., Schnurr, O., Schwope, A., Walcher, J., Dionies, F., Haynes, D., Kelz, A., Kitaura, F. S., Lamer, G., Minchev, I., Müller, V., Nuza, S. E., Olaya, J. -C, Piffl, T., Popow, E., Steinmetz, M., Ural, U., Williams, M., Winkler, R., Wisotzki, L., Ansorge, W. R., Banerji, M., Solares, E. G., Irwin, M., Kennicutt Jr., R. C., King, D., McMahon, R., Koposov, S., Parry, I. R., Sun, D., Walton, N. A., Finger, G., Iwert, O., Krumpe, M., Lizon, J. -L, Vincenzo, M., Amans, J. -P, Bonifacio, P., Cohen, M., Francois, P., Jagourel, P., Mignot, S. B., Royer, F., Sartoretti, P., Bender, R., Grupp, F., Hess, H. -J, Lang-Bardl, F., Muschielok, B., Böhringer, H., Boller, T., Bongiorno, A., Brusa, M., Dwelly, T., Merloni, A., Nandra, K., Salvato, M., Pragt, J. H., Navarro, R., Gerlofsma, G., Roelfsema, R., Dalton, G. B., Middleton, K. F., Tosh, I. A., Boeche, C., Caffau, E., Christlieb, N., Grebel, E. K., Hansen, C., Koch, A., Ludwig, H. -G, Quirrenbach, A., Sbordone, L., Seifert, W., Thimm, G., Trifonov, T., Helmi, A., Trager, S. C., Feltzing, S., Korn, Andreas, and Boland, W.

Abstract

The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field (>3 square degree, goal >5 square degree), high-multiplex (>1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at resolution R∼5000 (λ=390-1000 nm) and more than 2 million spectra at R∼20,000 (395-456.5 nm & 587-673 nm). The 4MOST design is especially intended to complement three key all-sky, space-based observatories of prime European interest: Gaia, eROSITA and Euclid. Initial design and performance estimates for the wide-field corrector concepts are presented. Two fibre positioner concepts are being considered for 4MOST. The first one is a Phi-Theta system similar to ones used on existing and planned facilities. The second one is a new R-Theta concept with large patrol area. Both positioner concepts effectively address the issues of fibre focus and pupil pointing. The 4MOST spectrographs are fixed configuration two-arm spectrographs, with dedicated spectrographs for the high- and low-resolution fibres. A full facility simulator is being developed to guide trade-off decisions regarding the optimal field-of-view, number of fibres needed, and the relative fraction of high-to-low resolution fibres. The simulator takes mock catalogues with template spectra from Design Reference Surveys as starting point, calculates the output spectra based on a throughput simulator, assigns targets to fibres based on the capabilities of the fibre positioner designs, and calculates the required survey time by tiling the fields on the sky. The 4MOST consortium aims to deliver the full 4MOST facility by the end of 2018 and start delivering high-level data products for both consortium and ESO community targets a year later with yearly increments., Sponsors: The Society of Photo-Optical Instrumentation Engineers (SPIE)

Published
2012
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19. A Tenth Birthday Present for UVES: A CCD Upgrade of the Red Arm

Author

Smoker, J., Haddad, N., Iwert, O., Deiries, S., Modigliani, A., Randall, S., D Odorico, S., James, G., Lo Curto, G., Robert, P., Pasquini, L., Downing, M., Ledoux, C., Martayan, C., Dall, T., Vinther, J., Claudio Melo, Fox, A., Pritchard, J., Baade, D., and Dekker, H.

20. ESPRESSO: The next European exoplanet hunter

Author

Pepe, F., Molaro, P., Cristiani, S., Rebolo, R., Santos, N. C., Dekker, H., Mégevand, D., Filippo Maria Zerbi, Cabral, A., Di Marcantonio, P., Abreu, M., Affolter, M., Aliverti, M., Allende Prieto, C., Amate, M., Avila, G., Baldini, V., Bristow, P., Broeg, C., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cupani, G., D Odorico, V., Caprio, V., Delabre, B., Dorn, R., Figueira, P., Fragoso, A., Galeotta, S., Genolet, L., Gomes, R., González Hernández, J. I., Hughes, I., Iwert, O., Kerber, F., Landoni, M., Lizon, J. -L, Lovis, C., Maire, C., Mannetta, M., Martins, C., Monteiro, M., Oliveira, A., Poretti, E., Rasilla, J. L., Riva, M., Santana Tschudi, S., Santos, P., Sosnowska, D., Sousa, S., Spanó, P., Tenegi, F., Toso, G., Vanzella, E., Viel, M., and Zapatero Osorio, M. R.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

The acronym ESPRESSO stems for Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations; this instrument will be the next VLT high resolution spectrograph. The spectrograph will be installed at the Combined-Coud\'e Laboratory of the VLT and linked to the four 8.2 m Unit Telescopes (UT) through four optical Coud\'e trains. ESPRESSO will combine efficiency and extreme spectroscopic precision. ESPRESSO is foreseen to achieve a gain of two magnitudes with respect to its predecessor HARPS, and to improve the instrumental radial-velocity precision to reach the 10 cm/s level. It can be operated either with a single UT or with up to four UTs, enabling an additional gain in the latter mode. The incoherent combination of four telescopes and the extreme precision requirements called for many innovative design solutions while ensuring the technical heritage of the successful HARPS experience. ESPRESSO will allow to explore new frontiers in most domains of astrophysics that require precision and sensitivity. The main scientific drivers are the search and characterization of rocky exoplanets in the habitable zone of quiet, nearby G to M-dwarfs and the analysis of the variability of fundamental physical constants. The project passed the final design review in May 2013 and entered the manufacturing phase. ESPRESSO will be installed at the Paranal Observatory in 2016 and its operation is planned to start by the end of the same year., Comment: 12 pages, figures included, accepted for publication in Astron. Nachr

21. OmegaCAM: the 16k×16k CCD camera for the VLT survey telescope

Author

Kuijken, K., Bender, R., Cappellaro, E., Muschielok, B., Andrea Baruffolo, Cascone, E., Iwert, O., Mitsch, W., Nicklas, H., Valentijn, E. A., Baade, D., Begeman, K. G., Bortolussi, A., Boxhoorn, D., Christen, F., Deul, E. R., Geimer, C., Greggio, L., Harke, R., Häfner, R., Hess, G., Hess, H. -J, Hopp, U., Ilijevski, I., Klink, G., Kravcar, H., Lizon, J. L., Magagna, C. E., Müller, Ph, Niemeczek, R., Pizzol, L., Poschmann, H., Reif, K., Rengelink, R., Reyes, J., Silber, A., Wellem, W., and Astronomy

Subjects
VLT, CCD Cameras
Abstract

In 2004, OmegaCAM will start operations on Paranal as the sole instrument on the 2.6-m VLT Survey Telescope. OmegaCAM is a huge optical CCD imaging camera: its 16k × 16k CCD pixels cover the square degree field of view of the VST almost entirely. The primary function of the VST and its instrument is to provide surveys in support of VLT science, be it in the form of large homogeneous multi-colour imaging surveys which form the basis for largescale spectroscopic follow-up work, or in its ability to find rare or extreme astronomical objects for further study.

22. A precise architecture characterization of the π Mensae planetary system

Author

Damasso, M., Sozzetti, A., Lovis, C., Barros, S. C. C., Sousa, S. G., Demangeon, O. D. S., Faria, J. P., Lillo-Box, J., Cristiani, S., Pepe, F., Rebolo, R., Santos, N. C., Zapatero Osorio, M. R., González Hernández, J. I., Amate, M., Pasquini, L., Zerbi, F. M., Adibekyan, V., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Allart, R., Allende Prieto, C., Álvarez, D., Alves, D., Avila, G., Baldini, V., Bandy, T., Benz, Willy, Bianco, A., Borsa, F., Bossini, D., Bourrier, V., Bouchy, F., Broeg, C., Cabral, A., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., D’Odorico, V., Deiries, S., Dekker, H., Delabre, B., Di Marcantonio, P., Dumusque, X., Ehrenreich, D., Figueira, P., Fragoso, A., Genolet, L., Genoni, M., Génova Santos, R., Hughes, I., Iwert, O., Kerber, F., Knudstrup, J., Landoni, M., Lavie, B., Lizon, J.-L., Lo Curto, G., Maire, C., Martins, C. J. A. P., Mégevand, D., Mehner, A., Micela, G., Modigliani, A., Molaro, P., Monteiro, M. A., Monteiro, M. J. P. F. G., Moschetti, M., Mueller, E., Murphy, M. T., Nunes, N., Oggioni, L., Oliveira, A., Oshagh, M., Pallé, E., Pariani, G., Poretti, E., Rasilla, J. L., Rebordão, J., Redaelli, E. M., Riva, M., Santana Tschudi, S., Santin, P., Santos, P., Ségransan, D., Schmidt, T. M., Segovia, A., Sosnowska, D., Spanò, P., Suárez Mascareño, A., Tabernero, H., Tenegi, F., Udry, S., and Zanutta, A.

Subjects
13. Climate action, 520 Astronomy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 500 Science, 620 Engineering, Astrophysics::Galaxy Astrophysics
Abstract

The bright star π Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the ESO's Very-Large Telescope (VLT). The star hosts a multi-planet system (a transiting 4 M⊕ planet at ∼0.07 au, and a sub-stellar companion on a ∼2100-day eccentric orbit) which is particularly appealing for a precise multi-technique characterization. With the new ESPRESSO observations, that cover a time span of 200 days, we aim to improve the precision and accuracy of the planet parameters and search for additional low-mass companions. We also take advantage of new photometric transits of π Men c observed by TESS over a time span that overlaps with that of the ESPRESSO follow-up campaign. We analyse the enlarged spectroscopic and photometric datasets and compare the results to those in the literature. We further characterize the system by means of absolute astrometry with Hipparcos and Gaia. We used the spectra of ESPRESSO for an independent determination of the stellar fundamental parameters. We present a precise characterization of the planetary system around π Men. The ESPRESSO radial velocities alone (with typical uncertainty of 10 cm/s) allow for a precise retrieval of the Doppler signal induced by π Men c. The residuals show an RMS of 1.2 m/s, and we can exclude companions with a minimum mass less than ∼2 M⊕ within the orbit of π Men c). We improve the ephemeris of π Men c using 18 additional TESS transits, and in combination with the astrometric measurements, we determine the inclination of the orbital plane of π Men b with high precision (ib=45.8+1.4−1.1 deg). This leads to the precise measurement of its absolute mass mb=14.1+0.5−0.4 MJup, and shows that the planetary orbital planes are highly misaligned.

23. ESPRESSO — An Echelle SPectrograph for Rocky Exoplanets Search and Stable Spectroscopic Observations

Author

Pepe, F., Cristiani, S., Rebolo, R., Santos, N. C., Dekker, H., Mégevand, D., Zerbi, F. M., Cabral, A., Molaro, P., Di Marcantonio, P., Abreu, M., Affolter, M., Aliverti, M., Allende Prieto, C., Amate, M., Avila, G., Baldini, V., Bristow, P., Broeg, C., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cupani, G., Valentina D'Odorico, Caprio, V., Delabre, B., Dorn, R., Figueira, P., Fragoso, A., Galeotta, S., Genolet, L., Gomes, R., González Hernández, J. I., Hughes, I., Iwert, O., Kerber, F., Landoni, M., Lizon, J. -L, Lovis, C., Maire, C., Mannetta, M., Martins, C., Monteiro, M. A., Oliveira, A., Poretti, E., Rasilla, J. L., Riva, M., Santana Tschudi, S., Santos, P., Sosnowska, D., Sousa, S., Spanò, P., Tenegi, F., Toso, G., Vanzella, E., Viel, M., and Zapatero Osorio, M. R.

24. Unraveling one of the densest planets known to date

Author

Toledo-Padrón, B., Lovis, C., Suárez Mascareño, A., Barros, S. C. C., González Hernández, J. I., Sozzetti, A., Bouchy, F., Zapatero Osorio, M. R., Rebolo, R., Cristiani, S., Pepe, F. A., Santos, N. C., Sousa, S. G., Tabernero, H. M., Lillo-Box, J., Bossini, D., Adibekyan, V., Allart, R., Damasso, M., D’Odorico, V., Figueira, P., Lavie, B., Lo Curto, G., Mehner, A., Micela, G., Modigliani, A., Nunes, N. J., Pallé, E., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Allende Prieto, C., Alves, D., Amate, M., Avila, G., Baldini, V., Bandy, T., Benatti, S., Benz, W., Bianco, A., Broeg, C., Cabral, A., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., Deiries, S., Dekker, H., Delabre, B., Demangeon, O., Di Marcantonio, P., Ehrenreich, D., Fragoso, A., Genolet, L., Genoni, M., Génova Santos, R., Hughes, I., Iwert, O., Knudstrup, J., Landoni, M., Lizon, J. L., Maire, C., Manescau, A., Martins, C. J. A. P., Mégevand, D., Molaro, P., Monteiro, M. J. P. F. G., Monteiro, M. A., Moschetti, M., Mueller, E., Oggioni, L., Oliveira, A., Oshagh, M., Pariani, G., Pasquini, L., Poretti, E., Rasilla, J. L., Redaelli, E., Riva, M., Santana Tschudi, S., Santin, P., Santos, P., Segovia, A., Sosnowska, D., Spanò, P., Tenegi, F., Udry, S., Zanutta, A., and Zerbi, F.

Subjects
530 Physics, 520 Astronomy, 500 Science, 620 Engineering
Abstract

We characterized the transiting planetary system orbiting the G2V star K2-38 using the new-generation echelle spectrograph ESPRESSO. We carried out a photometric analysis of the available K2 photometric light curve of this star to measure the radius of its two known planets. Using 43 ESPRESSO high-precision radial velocity measurements taken over the course of 8 months along with the 14 previously published HIRES RV measurements, we modeled the orbits of the two planets through a MCMC analysis, significantly improving their mass measurements. Using ESPRESSO spectra, we derived the stellar parameters, Teff=5731±66, logg=4.38±0.11~dex, and [Fe/H]=0.26±0.05~dex, and thus the mass and radius of K2-38, M⋆=1.03 +0.04−0.02~M⊕ and R⋆=1.06 +0.09−0.06~R⊕. We determine new values for the planetary properties of both planets. We characterize K2-38b as a super-Earth with RP=1.54±0.14~R⊕ and Mp=7.3+1.1−1.0~M⊕, and K2-38c as a sub-Neptune with RP=2.29±0.26~R⊕ and Mp=8.3+1.3−1.3~M⊕. We derived a mean density of ρp=11.0+4.1−2.8~g cm−3 for K2-38b and ρp=3.8+1.8−1.1~g~cm−3 for K2-38c, confirming K2-38b as one of the densest planets known to date. The best description for the composition of K2-38b comes from an iron-rich Mercury-like model, while K2-38c is better described by a rocky model with a H2 envelope. The maximum collision stripping boundary shows how giant impacts could be the cause for the high density of K2-38b. The irradiation received by each planet places them on opposite sides of the radius valley. We find evidence of a long-period signal in the radial velocity time-series whose origin could be linked to a 0.25-3~MJ planet or stellar activity.

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25. ESPRESSO at VLT

Author

Pepe, F., Cristiani, S., Rebolo, R., Santos, N. C., Dekker, H., Cabral, A., Di Marcantonio, P., Figueira, P., Lo Curto, G., Lovis, C., Mayor, M., Mégevand, D., Molaro, P., Riva, M., Zapatero Osorio, M. R., Amate, M., Manescau, A., Pasquini, L., Zerbi, F. M., Adibekyan, V., Abreu, M., Affolter, M., Alibert, Y., Aliverti, M., Allart, R., Allende Prieto, C., Álvarez, D., Alves, D., Avila, G., Baldini, V., Bandy, T., Barros, S. C. C., Benz, W., Bianco, A., Borsa, F., Bourrier, V., Bouchy, F., Broeg, C., Calderone, G., Cirami, R., Coelho, J., Conconi, P., Coretti, I., Cumani, C., Cupani, G., D’Odorico, V., Damasso, M., Deiries, S., Delabre, B., Demangeon, O. D. S., Dumusque, X., Ehrenreich, D., Faria, J. P., Fragoso, A., Genolet, L., Genoni, M., Génova Santos, R., González Hernández, J. I., Hughes, I., Iwert, O., Kerber, F., Knudstrup, J., Landoni, M., Lavie, B., Lillo-Box, J., Lizon, J.-L., Maire, C., Martins, C. J. A. P., Mehner, A., Micela, G., Modigliani, A., Monteiro, M. A., Monteiro, M. J. P. F. G., Moschetti, M., Murphy, M. T., Nunes, N., Oggioni, L., Oliveira, A., Oshagh, M., Pallé, E., Pariani, G., Poretti, E., Rasilla, J. L., Rebordão, J., Redaelli, E. M., Santana Tschudi, S., Santin, P., Santos, P., Ségransan, D., Schmidt, T. M., Segovia, A., Sosnowska, D., Sozzetti, A., Sousa, S. G., Spanò, P., Suárez Mascareño, A., Tabernero, H., Tenegi, F., Udry, S., and Zanutta, A.

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26. Nightside condensation of iron in an ultrahot giant exoplanet.

Author

Ehrenreich D, Lovis C, Allart R, Zapatero Osorio MR, Pepe F, Cristiani S, Rebolo R, Santos NC, Borsa F, Demangeon O, Dumusque X, González Hernández JI, Casasayas-Barris N, Ségransan D, Sousa S, Abreu M, Adibekyan V, Affolter M, Allende Prieto C, Alibert Y, Aliverti M, Alves D, Amate M, Avila G, Baldini V, Bandy T, Benz W, Bianco A, Bolmont É, Bouchy F, Bourrier V, Broeg C, Cabral A, Calderone G, Pallé E, Cegla HM, Cirami R, Coelho JMP, Conconi P, Coretti I, Cumani C, Cupani G, Dekker H, Delabre B, Deiries S, D'Odorico V, Di Marcantonio P, Figueira P, Fragoso A, Genolet L, Genoni M, Génova Santos R, Hara N, Hughes I, Iwert O, Kerber F, Knudstrup J, Landoni M, Lavie B, Lizon JL, Lendl M, Lo Curto G, Maire C, Manescau A, Martins CJAP, Mégevand D, Mehner A, Micela G, Modigliani A, Molaro P, Monteiro M, Monteiro M, Moschetti M, Müller E, Nunes N, Oggioni L, Oliveira A, Pariani G, Pasquini L, Poretti E, Rasilla JL, Redaelli E, Riva M, Santana Tschudi S, Santin P, Santos P, Segovia Milla A, Seidel JV, Sosnowska D, Sozzetti A, Spanò P, Suárez Mascareño A, Tabernero H, Tenegi F, Udry S, Zanutta A, and Zerbi F

Abstract

Ultrahot giant exoplanets receive thousands of times Earth's insolation 1,2 . Their high-temperature atmospheres (greater than 2,000 kelvin) are ideal laboratories for studying extreme planetary climates and chemistry 3-5 . Daysides are predicted to be cloud-free, dominated by atomic species 6 and much hotter than nightsides 5,7,8 . Atoms are expected to recombine into molecules over the nightside 9 , resulting in different day and night chemistries. Although metallic elements and a large temperature contrast have been observed 10-14 , no chemical gradient has been measured across the surface of such an exoplanet. Different atmospheric chemistry between the day-to-night ('evening') and night-to-day ('morning') terminators could, however, be revealed as an asymmetric absorption signature during transit 4,7,15 . Here we report the detection of an asymmetric atmospheric signature in the ultrahot exoplanet WASP-76b. We spectrally and temporally resolve this signature using a combination of high-dispersion spectroscopy with a large photon-collecting area. The absorption signal, attributed to neutral iron, is blueshifted by -11 ± 0.7 kilometres per second on the trailing limb, which can be explained by a combination of planetary rotation and wind blowing from the hot dayside 16 . In contrast, no signal arises from the nightside close to the morning terminator, showing that atomic iron is not absorbing starlight there. We conclude that iron must therefore condense during its journey across the nightside.

Published
2020
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