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Start Over Author "Anglada-Escudé, G." Publisher oxford university press (oup)
16 results on '"Anglada-Escudé, G."'

1. DMPP-4: candidate sub-Neptune mass planets orbiting a naked-eye star

Author

Barnes, J R, primary, Standing, M R, additional, Haswell, C A, additional, Staab, D, additional, Doherty, J P J, additional, Waller-Bridge, M, additional, Fossati, L, additional, Soto, M, additional, Anglada-Escudé, G, additional, Llama, J, additional, McCune, C, additional, and Lewis, F W, additional

Published
2023
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2. Analysis of Early Science observations with the CHaracterising ExOPlanets Satellite (CHEOPS) using pycheops

Author

Maxted, P F L, primary, Ehrenreich, D, additional, Wilson, T G, additional, Alibert, Y, additional, Cameron, A Collier, additional, Hoyer, S, additional, Sousa, S G, additional, Olofsson, G, additional, Bekkelien, A, additional, Deline, A, additional, Delrez, L, additional, Bonfanti, A, additional, Borsato, L, additional, Alonso, R, additional, Anglada Escudé, G, additional, Barrado, D, additional, Barros, S C C, additional, Baumjohann, W, additional, Beck, M, additional, Beck, T, additional, Benz, W, additional, Billot, N, additional, Biondi, F, additional, Bonfils, X, additional, Brandeker, A, additional, Broeg, C, additional, Bárczy, T, additional, Cabrera, J, additional, Charnoz, S, additional, Corral Van Damme, C, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Demangeon, O D S, additional, Demory, B-O, additional, Erikson, A, additional, Florén, H G, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Futyan, D, additional, Gandolfi, D, additional, Gillon, M, additional, Guedel, M, additional, Guterman, P, additional, Heng, K, additional, Isaak, K G, additional, Kiss, L, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Nascimbeni, V, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Pozuelos, F J, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Reimers, C, additional, Ribas, I, additional, Salmon, S, additional, Santos, N C, additional, Scandariato, G, additional, Simon, A E, additional, Smith, A M S, additional, Steller, M, additional, Swayne, M I, additional, Szabó, Gy M, additional, Ségransan, D, additional, Thomas, N, additional, Udry, S, additional, Van Grootel, V, additional, and Walton, N A, additional

Published
2021
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3. The EBLM project-VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves

Author

Swayne, MI, Maxted, PFL, Triaud, AHMJ, Sousa, SG, Broeg, C, Florén, HG, Guterman, P, Simon, AE, Boisse, I, Bonfanti, A, Martin, D, Santerne, A, Salmon, S, Standing, MR, Van Grootel, V, Wilson, TG, Alibert, Y, Alonso, R, Anglada Escudé, G, Asquier, J, Bárczy, T, Barrado, D, Barros, SCC, Battley, M, Baumjohann, W, Beck, M, Beck, T, Bekkelien, A, Benz, W, Billot, N, Bonfils, X, Brandeker, A, Busch, MD, Cabrera, J, Charnoz, S, Collier Cameron, A, Csizmadia, S, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, BO, Dransfield, G, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Futyan, D, Gandolfi, D, Gillon, M, Guedel, M, Hébrard, G, Heidari, N, Hellier, C, Heng, K, Hobson, M, Hoyer, S, Isaak, KG, Kiss, L, Kunovac Hodžić, V, Lalitha, S, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, McCormac, J, Miller, N, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Smith, AMS, Steinberger, M, Steller, M, Szabó, GM, Thomas, N, Udry, S, Walter, I, Walton, NA, Willett, E, Swayne, MI [0000-0002-2609-3159], Triaud, AHMJ [0000-0002-5510-8751], Sousa, SG [0000-0001-9047-2965], Santerne, A [0000-0002-3586-1316], Wilson, TG [0000-0001-8749-1962], Battley, M [0000-0002-1357-9774], Baumjohann, W [0000-0001-6271-0110], Collier Cameron, A [0000-0002-8863-7828], Csizmadia, S [0000-0001-6803-9698], Delrez, L [0000-0001-6108-4808], Fridlund, M [0000-0002-0855-8426], Gandolfi, D [0000-0001-8627-9628], Hoyer, S [0000-0003-3477-2466], Lendl, M [0000-0001-9699-1459], Miller, N [0000-0001-9550-1198], and Apollo - University of Cambridge Repository

Subjects
techniques: photometric, stars: low-mass, Astrophysics::Solar and Stellar Astrophysics, binaries: eclipsing, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, Astrophysics::Galaxy Astrophysics, techniques: spectroscopic
Abstract

The accuracy of theoretical mass, radius and effective temperature values for M-dwarf stars is an active topic of debate. Differences between observed and theoretical values have raised the possibility that current theoretical stellar structure and evolution models are inaccurate towards the low-mass end of the main sequence. To explore this issue we use the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions. We use these light curves combined with the spectroscopic orbit for the solar-type companion to measure the mass, radius and effective temperature of the M-dwarf star. Here we present the analysis of three eclipsing binaries. We use the pycheops data analysis software to fit the observed transit and eclipse events of each system. Two of our systems were also observed by the TESS satellite -- we similarly analyse these light curves for comparison. We find consistent results between CHEOPS and TESS, presenting three stellar radii and two stellar effective temperature values of low-mass stellar objects. These initial results from our on-going observing programme with CHEOPS show that we can expect to have ~24 new mass, radius and effective temperature measurements for very low mass stars within the next few years.

Published
2021

4. The EBLM project – VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves

Author

Swayne, M I, primary, Maxted, P F L, additional, Triaud, A H M J, additional, Sousa, S G, additional, Broeg, C, additional, Florén, H-G, additional, Guterman, P, additional, Simon, A E, additional, Boisse, I, additional, Bonfanti, A, additional, Martin, D, additional, Santerne, A, additional, Salmon, S, additional, Standing, M R, additional, Van Grootel, V, additional, Wilson, T G, additional, Alibert, Y, additional, Alonso, R, additional, Anglada Escudé, G, additional, Asquier, J, additional, Bárczy, T, additional, Barrado, D, additional, Barros, S C C, additional, Battley, M, additional, Baumjohann, W, additional, Beck, M, additional, Beck, T, additional, Bekkelien, A, additional, Benz, W, additional, Billot, N, additional, Bonfils, X, additional, Brandeker, A, additional, Busch, M-D, additional, Cabrera, J, additional, Charnoz, S, additional, Collier Cameron, A, additional, Csizmadia, Sz, additional, Davies, M B, additional, Deleuil, M, additional, Deline, A, additional, Delrez, L, additional, Demangeon, O D S, additional, Demory, B-O, additional, Dransfield, G, additional, Ehrenreich, D, additional, Erikson, A, additional, Fortier, A, additional, Fossati, L, additional, Fridlund, M, additional, Futyan, D, additional, Gandolfi, D, additional, Gillon, M, additional, Guedel, M, additional, Hébrard, G, additional, Heidari, N, additional, Hellier, C, additional, Heng, K, additional, Hobson, M, additional, Hoyer, S, additional, Isaak, K G, additional, Kiss, L, additional, Kunovac Hodžić, V, additional, Lalitha, S, additional, Laskar, J, additional, Lecavelier des Etangs, A, additional, Lendl, M, additional, Lovis, C, additional, Magrin, D, additional, Marafatto, L, additional, McCormac, J, additional, Miller, N, additional, Nascimbeni, V, additional, Olofsson, G, additional, Ottensamer, R, additional, Pagano, I, additional, Pallé, E, additional, Peter, G, additional, Piotto, G, additional, Pollacco, D, additional, Queloz, D, additional, Ragazzoni, R, additional, Rando, N, additional, Rauer, H, additional, Ribas, I, additional, Santos, N C, additional, Scandariato, G, additional, Ségransan, D, additional, Smith, A M S, additional, Steinberger, M, additional, Steller, M, additional, Szabó, Gy M, additional, Thomas, N, additional, Udry, S, additional, Walter, I, additional, Walton, N A, additional, and Willett, E, additional

Published
2021
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5. RedDots: a temperate 1.5 Earth-mass planet candidate in a compact multiterrestrial planet system around GJ 1061

Author

Dreizler, S, primary, Jeffers, S V, primary, Rodríguez, E, primary, Zechmeister, M, primary, Barnes, J R, primary, Haswell, C A, primary, Coleman, G A L, primary, Lalitha, S, primary, Hidalgo Soto, D, primary, Strachan, J B P, primary, Hambsch, F-J, primary, López-González, M J, primary, Morales, N, primary, Rodríguez López, C, primary, Berdiñas, Z M, primary, Ribas, I, primary, Pallé, E, primary, Reiners, A, primary, and Anglada-Escudé, G, primary

Published
2020
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6. Stellar activity analysis of Barnard’s Star: Very slow rotation and evidence for long-term activity cycle

Author

Toledo-Padrón, B, primary, Hernández, J I González, additional, Rodríguez-López, C, additional, Mascareño, A Suárez, additional, Rebolo, R, additional, Butler, R P, additional, Ribas, I, additional, Anglada-Escudé, G, additional, Johnson, E N, additional, Reiners, A, additional, Caballero, J A, additional, Quirrenbach, A, additional, Amado, P J, additional, Béjar, V J S, additional, Morales, J C, additional, Perger, M, additional, Jeffers, S V, additional, Vogt, S, additional, Teske, J, additional, Shectman, S, additional, Crane, J, additional, Díaz, M, additional, Arriagada, P, additional, Holden, B, additional, Burt, J, additional, Rodríguez, E, additional, Herrero, E, additional, Murgas, F, additional, Pallé, E, additional, Morales, N, additional, López-González, M J, additional, Alonso, E Díez, additional, Tuomi, M, additional, Kiraga, M, additional, Engle, S G, additional, Guinan, E F, additional, Strachan, J B P, additional, Aceituno, F J, additional, Aceituno, J, additional, Casanova, V M, additional, Martín-Ruiz, S, additional, Montes, D, additional, Ortiz, J L, additional, Sota, A, additional, Briol, J, additional, Barbieri, L, additional, Cervini, I, additional, Deldem, M, additional, Dubois, F, additional, Hambsch, F-J, additional, Harris, B, additional, Kotnik, C, additional, Logie, L, additional, Lopez, J, additional, McNeely, M, additional, Ogmen, Y, additional, Pérez, L, additional, Rau, S, additional, Rodríguez, D, additional, Urquijo, F S, additional, and Vanaverbeke, S, additional

Published
2019
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12. Two planets around Kapteyn's star: a cold and a temperate super-Earth orbiting the nearest halo red dwarf

Author

Anglada-Escudé, G., primary, Arriagada, P., additional, Tuomi, M., additional, Zechmeister, M., additional, Jenkins, J. S., additional, Ofir, A., additional, Dreizler, S., additional, Gerlach, E., additional, Marvin, C. J., additional, Reiners, A., additional, Jeffers, S. V., additional, Butler, R. P., additional, Vogt, S. S., additional, Amado, P. J., additional, Rodríguez-López, C., additional, Berdiñas, Z. M., additional, Morin, J., additional, Crane, J. D., additional, Shectman, S. A., additional, Thompson, I. B., additional, Díaz, M., additional, Rivera, E., additional, Sarmiento, L. F., additional, and Jones, H. R. A., additional

Published
2014
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13. Precision radial velocities of 15 M5–M9 dwarfs

Author

Barnes, J. R., primary, Jenkins, J. S., additional, Jones, H. R. A., additional, Jeffers, S. V., additional, Rojo, P., additional, Arriagada, P., additional, Jordán, A., additional, Minniti, D., additional, Tuomi, M., additional, Pinfield, D., additional, and Anglada-Escudé, G., additional

Published
2014
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14. Red Dots: A temperate 1.5 Earth-mass planet candidate in a compact multi-terrestrial planet system around GJ 1061

Author

Dreizler, S., Jeffers, S. V., Rodríguez, E., Zechmeister, M., Barnes, J. R., Haswell, C. A., Coleman, G. A. L., Lalitha, S., Soto, D. Hidalgo, Strachan, J. B. P., Hambsch, F.-J., López-González, M. J., Morales, N., López, C. Rodríguez, Berdiñas, Z. M., Ribas, I., Pallé, E., Reiners, A., Anglada-Escudé, G., Dreizler, S., Jeffers, S. V., Rodríguez, E., Zechmeister, M., Barnes, J. R., Haswell, C. A., Coleman, G. A. L., Lalitha, S., Soto, D. Hidalgo, Strachan, J. B. P., Hambsch, F.-J., López-González, M. J., Morales, N., López, C. Rodríguez, Berdiñas, Z. M., Ribas, I., Pallé, E., Reiners, A., and Anglada-Escudé, G.

Abstract

Small low-mass stars are favourable targets for the detection of rocky habitable planets. In particular, planetary systems in the solar neighbourhood are interesting and suitable for precise characterisation. The Red Dots campaigns seek to discover rocky planets orbiting nearby low-mass stars. The 2018 campaign targeted GJ 1061, which is the 20th nearest star to the Sun. For three consecutive months we obtained nightly, high-precision radial velocity measurements with the HARPS spectrograph. We analysed these data together with archival HARPS data. We report the detection of three planet candidates with periods of 3.204 ± 0.001, 6.689 ± 0.005 and 13.03 ± 0.03 days, which are close to 1:2:4 period commensurability. After several considerations related to the properties of the noise and sampling, we conclude that a 4th signal is most likely explained by stellar rotation, although it may be due to a planet. The proposed three-planet system (and the potential four-planet solution) is long-term dynamically stable. Planet-planet gravitational interactions are below our current detection threshold. The minimum masses of the three planets range from 1.4±0.2 to 1.8±0.3 M⊕. Planet d, with msin i = 1.64 ± 0.24M⊕, receives a similar amount of energy as Earth receives from the Sun. Consequently it lies within the liquid-water habitable zone of the star and has a similar equilibrium temperature to Earth. GJ 1061 has very similar properties to Proxima Centauri but activity indices point to lower levels of stellar activity.

15. DMPP-4: candidate sub-Neptune mass planets orbiting a naked-eye star

Author

Barnes, J. R., Standing, M. R., Haswell, C. A., Staab, D., Doherty, J. P. J., Waller-Bridge, M., Fossati, L., Soto, M., Anglada-Escudé, G., Llama, J., McCune, C., Lewis, F. W., Barnes, J. R., Standing, M. R., Haswell, C. A., Staab, D., Doherty, J. P. J., Waller-Bridge, M., Fossati, L., Soto, M., Anglada-Escudé, G., Llama, J., McCune, C., and Lewis, F. W.

Abstract

We present radial velocity measurements of the very bright (V ∼ 5.7) nearby F star, DMPP-4 (HD 184960). The anomalously low Ca ii H&K emission suggests mass loss from planets orbiting a low activity host star. Periodic radial velocity variability with ∼10 m s−1 amplitude is found to persist over a > 4 year timescale. Although the non-simultaneous photometric variability in four TESS sectors supports the view of an inactive star, we identify periodic photometric signals and also find spectroscopic evidence for stellar activity. We used a posterior sampling algorithm that includes the number of Keplerian signals, Np, as a free parameter to test and compare (1) purely Keplerian models (2) a Keplerian model with linear activity correlation and (3) Keplerian models with Gaussian processes. A preferred model, with one Keplerian and quasi-periodic Gaussian process indicates a planet with a period of $P_\textrm {b} = 3.4982^{+0.0015}_{-0.0027}$ d and corresponding minimum mass of $m_\textrm {b}\, \textrm {sin}\, i = 12.2^{+1.8}_{-1.9}$ M⊕. Without further high time resolution observations over a longer timescale, we cannot definitively rule out the purely Keplerian model with 2 candidates planets with $P_\textrm {b} = 2.4570^{+0.0026}_{-0.0462}$ d, minimum mass $m_\textrm {b}\, \textrm {sin}\, i = 8.0^{+1.1}_{-1.5}$ M⊕ and $P_\textrm {c} = 5.4196^{+0.6766}_{-0.0030}$ d and corresponding minimum mass of $m_\textrm {b}\, \textrm {sin}\, i = 12.2^{+1.4}_{-1.6}$ M⊕. The candidate planets lie in the region below the lower-envelope of the Neptune Desert. Continued mass loss may originate from the highly irradiated planets or from an as yet undetected body in the system.

16. Red Dots: A temperate 1.5 Earth-mass planet candidate in a compact multi-terrestrial planet system around GJ 1061

Author

Dreizler, S., Jeffers, S. V., Rodríguez, E., Zechmeister, M., Barnes, J. R., Haswell, C. A., Coleman, G. A. L., Lalitha, S., Soto, D. Hidalgo, Strachan, J. B. P., Hambsch, F.-J., López-González, M. J., Morales, N., López, C. Rodríguez, Berdiñas, Z. M., Ribas, I., Pallé, E., Reiners, A., Anglada-Escudé, G., Dreizler, S., Jeffers, S. V., Rodríguez, E., Zechmeister, M., Barnes, J. R., Haswell, C. A., Coleman, G. A. L., Lalitha, S., Soto, D. Hidalgo, Strachan, J. B. P., Hambsch, F.-J., López-González, M. J., Morales, N., López, C. Rodríguez, Berdiñas, Z. M., Ribas, I., Pallé, E., Reiners, A., and Anglada-Escudé, G.

Abstract

Small low-mass stars are favourable targets for the detection of rocky habitable planets. In particular, planetary systems in the solar neighbourhood are interesting and suitable for precise characterisation. The Red Dots campaigns seek to discover rocky planets orbiting nearby low-mass stars. The 2018 campaign targeted GJ 1061, which is the 20th nearest star to the Sun. For three consecutive months we obtained nightly, high-precision radial velocity measurements with the HARPS spectrograph. We analysed these data together with archival HARPS data. We report the detection of three planet candidates with periods of 3.204 ± 0.001, 6.689 ± 0.005 and 13.03 ± 0.03 days, which are close to 1:2:4 period commensurability. After several considerations related to the properties of the noise and sampling, we conclude that a 4th signal is most likely explained by stellar rotation, although it may be due to a planet. The proposed three-planet system (and the potential four-planet solution) is long-term dynamically stable. Planet-planet gravitational interactions are below our current detection threshold. The minimum masses of the three planets range from 1.4±0.2 to 1.8±0.3 M⊕. Planet d, with msin i = 1.64 ± 0.24M⊕, receives a similar amount of energy as Earth receives from the Sun. Consequently it lies within the liquid-water habitable zone of the star and has a similar equilibrium temperature to Earth. GJ 1061 has very similar properties to Proxima Centauri but activity indices point to lower levels of stellar activity.

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