644 results on '"Hidalgo, D."'
Search Results
2. The CARMENES search for exoplanets around M dwarfs -- LP 714-47b (TOI 442.01): Populating the Neptune desert
- Author
-
Dreizler, S., Crossfield, M., Kossakowski, D., Plavchan, P., Jeffers, V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., Caballero, A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., Osorio, R. Zapatero, Chaturvedi, P., Hatzes, P., Ricker, G., Vanderspek, R., Latham, W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., Amado, J., Barkaoui, K., Barbieri, M., Batalha, M., Bauer, F., Benneke, B., Benkhaldoun, Z., Beichman, Berberian, J., Burt, J., Butler, P., Caldwell, A., Chintada, A., Chontos, A., Christiansen, L., Ciardi, D. R., Cifuentes, C., Collins, A., Collins, I., Combs, D., Cortés-Contreras, M., Crane, D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., Flowers, E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., Howard, W., Howell, S., Huber, D., Isaacson, H., Jehin, E., Jensen, N., Kaminski, A., Kane, R., Kawauchi, K., Kielkopf, F., Klahr, H., Kosiarek, R., Kreidberg, L., Kürster, Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., Matson, A., Mocnik, T., Morales, C., Muirhead, S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., Passegger, M., Pollacco, D., Pozuelos, J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., Rose, E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., Şenavcı, V., Teske, J., Twicken, D., Villasenor, J., Wang, S. X., Weiss, M., Wittrock, J., Yılmaz, M., and Zohrabi, F.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, m_b = 30.8 +/- 1.5 M_earth , R_b = 4.7 +/- 0.3 R_earth ) located in the 'hot Neptune desert'. Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST- South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TUBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (T_eff = 3950 +/- 51 K) with a mass of 0.59 +/- 0.02 M_sun and a radius of 0.58 +/- 0.02 R_sun. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained., Comment: Accepted for publication in A&A. 24 pages, 21 figures, 5 tables
- Published
- 2020
- Full Text
- View/download PDF
3. Obliquity measurement and atmospheric characterization of the WASP-74 planetary system
- Author
-
Luque, R., Casasayas-Barris, N., Parviainen, H., Chen, G., Pallé, E., Livingston, J., Béjar, V. J. S., Crouzet, N., Esparza-Borges, E., Fukui, A., Hidalgo, D., Kawashima, Y., Kawauchi, K., Klagyivik, P., Kurita, S., Kusakabe, N., de Leon, J. P., Madrigal-Aguado, A., Montañés-Rodríguez, P., Mori, M., Murgas, F., Narita, N., Nishiumi, T., Nowak, G., Oshagh, M., Sánchez-Benavente, M., Stangret, M., Tamura, M., Terada, Y., and Watanabe, N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We present new transit observations of the hot Jupiter WASP-74 b ($T_\mathrm{eq} \sim$ 1860 K) using the high-resolution spectrograph HARPS-N and the multi-colour simultaneous imager MuSCAT2. We refine the orbital properties of the planet and its host star, and measure its obliquity for the first time. The measured sky-projected angle between the stellar spin-axis and the planet's orbital axis is compatible with an orbit well-aligned with the equator of the host star ($\lambda = 0.77\pm0.99 \mathrm{deg}$). We are not able to detect any absorption feature of H$\alpha$, or any other atomic spectral features, in its high-resolution transmission spectra due to low S/N at the line cores. Despite previous claims regarding the presence of strong optical absorbers such TiO and VO gases in the atmosphere of WASP-74 b, the new ground-based photometry combined with a reanalysis of previously reported observations from the literature shows a slope in the low-resolution transmission spectrum steeper than expected from Rayleigh scattering alone., Comment: Accepted for publication in Astronomy & Astrophysics. 12 pages, 8 figures, 5 tables
- Published
- 2020
- Full Text
- View/download PDF
4. Precise mass and radius of a transiting super-Earth planet orbiting the M dwarf TOI-1235: a planet in the radius gap?
- Author
-
Bluhm, P., Luque, R., Espinoza, N., Palle, E., Caballero, J. A., Dreizler, S., Livingston, J. H., Mathur, S., Quirrenbach, A., Stock, S., Van Eylen, V., Nowak, G., Lopez, E., Csizmadia, Sz., Osorio, M. R. Zapatero, Schoefer, P., Lillo-Box, J., Oshagh, M., Amado, P. J., Barrado, D., Bejar, V. J. S., Cale, B., Chaturvedi, P., Cifuentes, C., Cochran, W. D., Collins, K. A., Collins, K. I., Cortes-Contreras, M., Alonso, E. Diez, Mufti, M. El, Ercolino, A., Fridlund, M., Gaidos, E., Garcia, R. A., Gonzalez-Alvarez, E., Gonzalez-Cuesta, L., Guerra, P., Hatzes, A. P., Henning, T., Herrero, E., Hidalgo, D., Isopi, G., Jeffers, S. V., Jenkins, J. M., Jensen, E. L. N., Kabath, P., Kemmer, J., Korth, J., Kossakowski, D., Kuerster, M., Lafarga, M., Mallia, F., Montes, D., Morales, J. C., Morales-Calderon, M., Murgas, F., Narita, N., Plavchan, P., Passegger, V. M., Pedraz, S., Rauer, H., Redfield, S., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rodriguez-Lopez, C., Santos, A. R. G., Seager, S., Shan, Y., Schlecker, M., Schweitzer, A., Soto, M. G., Subjak, J., Tal-Or, L., Trifonov, T., Vanaverbeke, S., Vanderspek, R., Wittrock, J., Zechmeister, M., and Zohrabi, F.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the confirmation of a transiting planet around the bright, inactive M0.5 V star TOI-1235 (TYC 4384-1735-1, V = 11.5 mag), whose transit signal was detected in the photometric time series of Sectors 14, 20, and 21 of the TESS space mission. We confirm the planetary nature of the transit signal, which has a period of 3.44 d, by using precise radial velocity measurements with CARMENES and HARPS-N spectrographs. A comparison of the properties derived for TOI-1235 b's with theoretical models reveals that the planet has a rocky composition, with a bulk density slightly higher than Earth's. In particular, we measure a mass of M_p = 5.9+/-0.6 M_Earth and a radius of R_p = 1.69+/-0.08 R_Earth, which together result in a density of rho_p = 6.7+1.3-1.1 g/cm3. When compared with other well-characterized exoplanetary systems, the particular combination of planetary radius and mass puts our discovery in the radius gap, a transition region between rocky planets and planets with significant atmospheric envelopes, with few known members. While the exact location of the radius gap for M dwarfs is still a matter of debate, our results constrain it to be located at around 1.7 R_Earth or larger at the insolation levels received by TOI-1235 b (~60 S_Earth), which makes it an extremely interesting object for further studies of planet formation and atmospheric evolution., Comment: A&A, in press
- Published
- 2020
- Full Text
- View/download PDF
5. The CARMENES search for exoplanets around M dwarfs. Two planets on the opposite sides of the radius gap transiting the nearby M dwarf LTT 3780
- Author
-
Nowak, G., Luque, R., Parviainen, H., Pallé, E., Molaverdikhani, K., Béjar, V. J. S., Lillo-Box, J., Rodríguez-López, C., Caballero, J. A., Zechmeister, M., Passegger, V. M., Cifuentes, C., Schweitzer, A., Narita, N., Cale, B., Espinoza, N., Murgas, F., Hidalgo, D., Osorio, M. R. Zapatero, Pozuelos, F. J., Aceituno, F. J., Amado, P. J., Barkaoui, K., Barrado, D., Bauer, F. F., Benkhaldoun, Z., Caldwell, D. A., Barris, N. Casasayas, Chaturvedi, P., Chen, G., Collins, K. A., Collins, K. I., Cortés-Contreras, M., Crossfield, I. J. M., de León, J. P., Alonso, E. Díez, Dreizler, S., Mufti, M. El, Esparza-Borges, E., Essack, Z., Fukui, A., Gaidos, E., Gillon, M., Gonzales, E. J., Guerra, P., Hatzes, A., Henning, T., Herrero, E., Hesse, K., Hirano, T., Howell, S. B., Jeffers, S. V., Jehin, E., Jenkins, J. M., Kaminski, A., Kemmer, J., Kielkopf, J. F., Kossakowski, D., Kotani, T., Kürster, M., Lafarga, M., Latham, D. W., Law, N., Lissauer, J. J., Lodieu, N., Madrigal-Aguado, A., Mann, A. W., Massey, B., Matson, R. A., Matthews, E., Montanés-Rodríguez, P., Montes, D., Morales, J. C., Mori, M., Nagel, E., Oshagh, M., Pedraz, S., Plavchan, P., Pollacco, D., Quirrenbach, A., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rose, M. E., Schlecker, M., Schlieder, J. E., Seager, S., Stangret, M., Stock, S., Tamura, M., Tanner, A., Teske, J., Trifonov, T., Twicken, J. D., Vanderspek, R., Watanabe, D., Wittrock, J., Ziegler, C., and Zohrabi, F.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We present the discovery and characterisation of two transiting planets observed by the Transiting Exoplanet Survey Satellite (TESS) orbiting the nearby (d ~ 22 pc), bright (J ~ 9 mag) M3.5 dwarf LTT 3780 (TOI-732). We confirm both planets and their association with LTT 3780 via ground-based photometry and determine their masses using precise radial velocities measured with the CARMENES spectrograph. Precise stellar parameters determined from CARMENES high resolution spectra confirm that LTT 3780 is a mid-M dwarf with an effective temperature of T_eff = 3360 +\- 51 K, a surface gravity of log(g) = 4.81 +/- 0.04 (cgs), and an iron abundance of [Fe/H] = 0.09 +/- 0.16 dex, with an inferred mass of M_star = 0.379 +/- 0.016 M_sun and a radius of R_star = 0.382 +/- 0.012 R_sun. The ultra-short-period planet LTT 3780 b (P_b = 0.77 d) with a radius of 1.35^{+0.06}_{-0.06} R_earth, a mass of 2.34^{+0.24}_{-0.23} M_earth, and a bulk density of 5.24^{+0.94}_{-0.81} g cm^{-3} joins the population of Earth-size planets with rocky, terrestrial composition. The outer planet, LTT 3780 c, with an orbital period of 12.25 d, radius of 2.42^{+0.10}_{-0.10} R_earth, mass of 6.29^{+0.63}_{-0.61} M_earth, and mean density of 2.45^{+0.44}_{-0.37} g cm^{-3} belongs to the population of dense sub-Neptunes. With the two planets located on opposite sides of the radius gap, this planetary system is an excellent target for testing planetary formation, evolution and atmospheric models. In particular, LTT 3780 c is an ideal object for atmospheric studies with the James Webb Space Telescope., Comment: 21 pages, 15 figures, 4 tables, submitted to A&A
- Published
- 2020
- Full Text
- View/download PDF
6. Three planets transiting the evolved star EPIC 249893012: a hot 8.8-M$_\oplus$ super-Earth and two warm 14.7 and 10.2-M$_\oplus$ sub-Neptunes
- Author
-
Hidalgo, D., Pallé, E., Alonso, R., Gandolfi, D., Fridlund, M., Nowak, G., Luque, R., Hirano, T., Justesen, A. B., Cochran, W. D., Barragan, O., Spina, L., Rodler, F., Albrecht, S., Anderson, D., Amado, P., Bryant, E., Caballero, J. A., Cabrera, J., Csizmadia, Sz., Dai, F., De Leon, J., Deeg, H. J., Eigmuller, Ph., Endl, M., Erikson, A., Esposito, M., Figueira, P., Georgieva, I., Grziwa, S., Guenther, E., Hatzes, A. P., Hjorth, M., Hoeijmakers, H. J., Kabath, P., Korth, J., Kuzuhara, M., Lafarga, M., Lampon, M., Leao, I. C., Livingston, J., Mathur, S., Montanes-Rodriguez, P., Morales, J. C., Murgas, F., Nagel, E., Narita, N., Nielsen, L. D., Patzold, M., Persson, C. M., Prieto-Arranz, J., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I., Smith, A. M. S., Subjak, J., Van Eylen, V., and Wilson, P. A.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the discovery of a new planetary system with three transiting planets, one super-Earth and two sub-Neptunes, that orbit EPIC\,249893012, a G8\,IV-V evolved star ($M_\star$\,=\,1.05\,$\pm$\,0.05\,$M_\odot$, $R_\star$\,=\,1.71\,$\pm$\,0.04\,$R_\odot$, $T_\mathrm{eff}$\,=5430\,$\pm$\,85\,K). The star is just leaving the main sequence. We combined \ktwo \ photometry with IRCS adaptive-optics imaging and HARPS, HARPS-N, and CARMENES high-precision radial velocity measurements to confirm the planetary system, determine the stellar parameters, and measure radii, masses, and densities of the three planets. With an orbital period of $3.5949^{+0.0007}_{-0.0007}$ days, a mass of $8.75^{+1.09}_{-1.08}\ M_{\oplus}$ , and a radius of $1.95^{+0.09}_{-0.08}\ R_{\oplus}$, the inner planet b is compatible with nickel-iron core and a silicate mantle ($\rho_b= 6.39^{+1.19}_{-1.04}$ g cm$^{-3}$). Planets c and d with orbital periods of $15.624^{+0.001}_{-0.001}$ and $35.747^{+0.005}_{-0.005}$ days, respectively, have masses and radii of $14.67^{+1,84}_{-1.89}\ M_{\oplus}$ and $3.67^{+0.17}_{-0.14}\ R_{\oplus}$ and $10.18^{+2.46}_{-2.42}\ M_{\oplus}$ and $3.94^{+0.13}_{-0.12}\ R_{\oplus}$, respectively, yielding a mean density of $1.62^{+0.30}_{-0.29}$ and $0.91^{+0.25}_{-0.23}$ g cm$^{-3}$, respectively. The radius of planet b lies in the transition region between rocky and gaseous planets, but its density is consistent with a rocky composition. Its semimajor axis and the corresponding photoevaporation levels to which the planet has been exposed might explain its measured density today. In contrast, the densities and semimajor axes of planets c and d suggest a very thick atmosphere. The singularity of this system, which orbits a slightly evolved star that is just leaving the main sequence, makes it a good candidate for a deeper study from a dynamical point of view., Comment: Accepted for publication in A\& A
- Published
- 2020
- Full Text
- View/download PDF
7. Manure biostabilization by effective microorganisms as a way to improve its agronomic value
- Author
-
Hidalgo, D., Corona, F., and Martín-Marroquín, J.M.
- Published
- 2022
- Full Text
- View/download PDF
8. Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star
- Author
-
Fukui, A., Suzuki, D., Koshimoto, N., Bachelet, E., Vanmunster, T., Storey, D., Maehara, H., Yanagisawa, K., Yamada, T., Yonehara, A., Hirano, T., Bennett, D. P., Bozza, V., Mawet, D., Penny, M. T., Awiphan, S., Oksanen, A., Heintz, T. M., Oberst, T. E., Bejar, V. J. S., Casasayas-Barris, N., Chen, G., Crouzet, N., Hidalgo, D., Klagyivik, P., Murgas, F., Narita, N., Palle, E., Parviainen, H., Watanabe, N., Kusakabe, N., Mori, M., Terada, Y., de Leon, J. P., Hernandez, A., Luque, R., Monelli, M., Montanes-Rodriguez, P., Prieto-Arranz, J., Murata, K. L., Shugarov, S., Kubota, Y., Otsuki, C., Shionoya, A., Nishiumi, T., Nishide, A., Fukagawa, M., Onodera, K., Villanueva Jr., S., Street, R. A., Tsapras, Y., Hundertmark, M., Kuzuhara, M., Fujita, M., Beichman, C., Beaulieu, J. -P., Alonso, R., Kawai, D. E. Reichart N., and Tamura, M.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the analysis of additional multiband photometry and spectroscopy and new adaptive optics (AO) imaging of the nearby planetary microlensing event TCP J05074264+2447555 (Kojima-1), which was discovered toward the Galactic anticenter in 2017 (Nucita et al.). We confirm the planetary nature of the light-curve anomaly around the peak while finding no additional planetary feature in this event. We also confirm the presence of apparent blending flux and the absence of significant parallax signal reported in the literature. The AO image reveals no contaminating sources, making it most likely that the blending flux comes from the lens star. The measured multiband lens flux, combined with a constraint from the microlensing model, allows us to narrow down the previously unresolved mass and distance of the lens system. We find that the primary lens is a dwarf on the K/M boundary (0.581 \pm 0.033 M_sun) located at 505 \pm 47 pc and the companion (Kojima-1Lb) is a Neptune-mass planet (20.0 \pm 2.0 M_earth) with a semi-major axis of 1.08 ^{+0.62}_{-0.18} au. This orbit is a few times smaller than those of typical microlensing planets and is comparable to the snow-line location at young ages. We calculate that the a priori detection probability of Kojima-1Lb is only \sim 35%, which may imply that Neptunes are common around the snow line, as recently suggested by the transit and radial velocity techniques. The host star is the brightest among the microlensing planetary systems (Ks = 13.7), offering a great opportunity to spectroscopically characterize this system, even with current facilities., Comment: 27 pages, 12 figures, published in Astronomical Journal
- Published
- 2019
- Full Text
- View/download PDF
9. K2-290: a warm Jupiter and a mini-Neptune in a triple-star system
- Author
-
Hjorth, M., Justesen, A. B., Hirano, T., Albrecht, S., Gandolfi, D., Dai, F., Alonso, R., Barragán, O., Esposito, M., Kuzuhara, M., Lam, K. W. F., Livingston, J. H., Montanes-Rodriguez, P., Narita, N., Nowak, G., Prieto-Arranz, J., Redfield, S., Rodler, F., Van Eylen, V., Winn, J. N., Antoniciello, G., Cabrera, J., Cochran, W. D., Csizmadia, Sz., de Leon, J., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fridlund, M., Grziwa, S., Guenther, E., Hatzes, A. P., Heeren, P., Hidalgo, D., Korth, J., Luque, R., Nespral, D., Palle, E., Pätzold, M., Persson, C. M., Rauer, H., Smith, A. M. S., and Trifonov, T.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of two transiting planets orbiting K2-290 (EPIC 249624646), a bright (V=11.11) late F-type star residing in a triple-star system. It was observed during Campaign 15 of the K2 mission, and in order to confirm and characterise the system, follow-up spectroscopy and AO imaging were carried out using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia data we identify two M-dwarf companions at a separation of $113 \pm 2$ AU and $2467_{-155}^{+177}$ AU. From radial velocities, K2 photometry, and stellar characterisation of the host star, we find the inner planet to be a mini-Neptune with a radius of $3.06 \pm 0.16 R_{\oplus}$ and an orbital period of $P = 9.2$ days. The radius of the mini-Neptune suggests that the planet is located above the radius valley, and with an incident flux of $F\sim 400 F_{\oplus}$, it lies safely outside the super-Earth desert. The outer warm Jupiter has a mass of $0.774\pm 0.047 M_{\rm J}$ and a radius of $1.006\pm 0.050R_{\rm J}$, and orbits the host star every 48.4 days on an orbit with an eccentricity $e<0.241$. Its mild eccentricity and mini-Neptune sibling suggest that the warm Jupiter originates from in situ formation or disk migration., Comment: 16 pages, 8 figures, accepted for publication in MNRAS. Updated to accepted version (including K2 name)
- Published
- 2019
- Full Text
- View/download PDF
10. Metal-based nanoadditives for increasing biomass and biohydrogen production in microalgal cultures: A review
- Author
-
Hidalgo, D., Martín-Marroquín, J.M., and Corona, F.
- Published
- 2023
- Full Text
- View/download PDF
11. Detection and characterization of an ultra-dense sub-Neptune planet orbiting the Sun-like star HD 119130
- Author
-
Luque, R., Nowak, G., Pallé, E., Dai, F., Kaminski, A., Nagel, E., Hidalgo, D., Bauer, F., Lafarga, M., Livingston, J., Barragán, O., Hirano, T., Fridlund, M., Gandolfi, D., Justesen, A. B., Hjorth, M., Van Eylen, V., Winn, J. N., Esposito, M., Morales, J. C., Albrecht, S., Alonso, R., Amado, P. J., Beck, P., Caballero, J. A., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fukui, A., Grziwa, S., Guenther, E. W., Hatzes, A. P., Knudstrup, E., Korth, J., Lam, K. W. F., Lund, M. N., Mathur, S., Montañes-Rodríguez, P., Narita, N., Nespral, D., Niraula, P., Pätzold, M., Persson, C. M., Prieto-Arranz, J., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I., and Smith, A. M. S.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery and characterization of a new transiting planet from Campaign 17 of the Kepler extended mission K2. HD 119130 b is a warm sub-Neptune on a 17-d orbit around a bright (V = 9.9 mag) solar-like G3 V star with a mass and radius of $M_\star = 1.00\pm0.03\,\mathrm{M_\odot}$ and $R_\star = 1.09\pm0.03\,\mathrm{R_\odot}$, respectively. We model simultaneously the K2 photometry and CARMENES spectroscopic data and derive a radius of $R_\mathrm{p} = 2.63_{-0.10}^{+0.12}\,\mathrm{R_\oplus}$ and mass of $M_\mathrm{p} = 24.5_{-4.4}^{+4.4}\,\mathrm{M_\oplus}$, yielding a mean density of $\rho_\mathrm{p} = 7.4_{-1.5}^{+1.6}\,\mathrm{g\,cm^{-3}}$, which makes it one of the densest sub-Neptune planets known to date. We also detect a linear trend in radial velocities of HD 119130 ($\dot{\gamma}_{\rm RV}= -0.40^{+0.07}_{-0.07}\,\mathrm{m\,s^{-1}\,d^{-1}}$) that suggests a long-period companion with a minimum mass on the order of $33\,\mathrm{M_\oplus}$. If confirmed, it would support a formation scenario of HD 119130 b by migration caused by Kozai-Lidov oscillations., Comment: Submitted to A&A; 9 pages, 8 figures, 4 tables
- Published
- 2018
- Full Text
- View/download PDF
12. HD219666b: A hot-Neptune from TESS Sector 1
- Author
-
Esposito, M., Armstrong, D. J., Gandolfi, D., Adibekyan, V., Fridlund, M., Santos, N. C., Livingston, J. H., Mena, E. Delgado, Fossati, L., Lillo-Box, J., Barragán, O., Barrado, D., Cubillos, P. E., Cooke, B., Justesen, A. B., Meru, F., Díaz, R. F., Dai, F., Nielsen, L. D., Persson, C. M., Wheatley, P. J., Hatzes, A. P., Van Eylen, V., Musso, M. M., Alonso, R., Beck, P., Barros, S. C. C., Bayliss, D., Bonomo, A. S., Bouchy, F., Brown, D. J. A., Bryant, E., Cabrera, J., Cochran, W. D., Csizmadia, S., Deeg, H., Demangeon, O., Deleuil, M., Dumusque, X., Eigmüller, P., Endl, M., Erikson, A., Faedi, F., Figueira, P., Fukui, A., Grziwa, S., Guenther, E. W., Hidalgo, D., Hjorth, M., Hirano, T., Hojjatpanah, S., Knudstrup, E., Korth, J., Lam, K. W. F., de Leon, J., Lund, M. N., Luque, R., Mathur, S., Rodríguez, P. Montañés, Narita, N., Nespral, D., Niraula, P., Nowak, G., Osborn, H. P., Pallé, E., Pätzold, M., Pollacco, D., Prieto-Arranz, J., Rauer, H., Redfield, S., Ribas, I., Sousa, S. G., Smith, A. M. S., Tala-Pinto, M., Udry, S., and Winn, J. N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD219666 (Mstar = 0.92 +/- 0.03 MSun, Rstar = 1.03 +/- 0.03 RSun, tau_star = 10 +/- 2 Gyr). With a mass of Mb = 16.6 +/- 1.3 MEarth, a radius of Rb = 4.71 +/- 0.17 REarth, and an orbital period of P ~ 6 days, HD219666b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with HARPS@ESO3.6m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (Teff = 5527 +/- 65 K, log g = 4.40 +/- 0.11 (cgs), [Fe/H]= 0.04 +/- 0.04 dex, log R'HK = -5.07 +/- 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmospheric metal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects., Comment: Accepted for publication in A&A
- Published
- 2018
- Full Text
- View/download PDF
13. The CARMENES search for exoplanets around M dwarfs: The warm super-Earths in twin orbits around the mid-type M dwarfs Ross 1020 (GJ 3779) and LP 819-052 (GJ 1265)
- Author
-
Luque, R., Nowak, G., Pallé, E., Kossakowski, D., Trifonov, T., Zechmeister, M., Béjar, V. J. S., Guillén, C. Cardona, Tal-Or, L., Hidalgo, D., Ribas, I., Reiners, A., Caballero, J. A., Amado, P. J., Quirrenbach, A., Aceituno, J., Cortés-Contreras, M., Díez-Alonso, E., Dreizler, S., Guenther, E. W., Henning, T., Jeffers, S. V., Kaminski, A., Kürster, M., Lafarga, M., Montes, D., Morales, J. C., Passegger, V. M., Schmitt, J. H. M. M., and Schweitzer, A.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We announce the discovery of two planetary companions orbiting around the low mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity observations in the visual channel as part of its survey for exoplanets around M dwarfs. In the case of GJ 1265, CARMENES observations were complemented with publicly available Doppler measurements from HARPS. The datasets reveal one planetary companion for each star that share very similar properties: minimum masses of $8.0\pm0.5$ M$_{\oplus}$ and $7.4\pm0.5$ M$_{\oplus}$ in low-eccentricity orbits with periods of $3.023\pm0.001$ d and $3.651\pm0.001$ d for GJ 3779 b and GJ 1265 b, respectively. The periodic signals around three days found in the radial velocity data have no counterpart in any spectral activity indicator. Besides, we collected available photometric data for the two host stars, which confirm that the additional Doppler variations found at periods around 95 d can be attributed to the rotation of the stars. The addition of these planets in a mass-period diagram of known planets around M dwarfs suggests a bimodal distribution with a lack of short-period low-mass planets in the range of 2-5 M$_{\oplus}$. It also indicates that super-Earths (> 5 M$_{\oplus}$) currently detected by radial velocity and transit techniques around M stars are usually found in systems dominated by a single planet., Comment: Accepted for publication in A&A. 15 pages, 12 figures, 4 tables
- Published
- 2018
- Full Text
- View/download PDF
14. K2-140b and K2-180b - Characterization of a hot Jupiter and a mini-Neptune from the K2 mission
- Author
-
Korth, J., Csizmadia, Sz., Gandolfi, D., Fridlund, M., Pätzold, M., Hirano, T., Livingston, J., Persson, C. M., Deeg, H. J., Justesen, A. B., Barragán, O., Grziwa, S., Endl, M., Tronsgaard, R., Dai, F., Cochran, W. D., Albrecht, S., Alonso, R., Cabrera, J., Cauley, P. W., Cusano, F., Eigmüller, Ph., Erikson, A., Esposito, M., Guenther, E. W., Hatzes, A. P., Hidalgo, D., Kuzuhara, M., Montañes, P., Napolitano, N. R., Narita, N., Niraula, P., Nespral, D., Nowak, G., Palle, E., Petrillo, C. E., Redfield, S., Prieto-Arranz, J., Rauer, H., Smith, A. M. S., Tortora, C., Van Eylen, V., and Winn, J. N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the independent discovery and characterization of two K2 planets: K2-180b, a mini-Neptune-size planet in an 8.9-day orbit transiting a V = 12.6 mag, metal-poor ([Fe/H] =$-0.65\pm0.10$) K2V star in K2 campaign 5; K2-140b, a transiting hot Jupiter in a 6.6-day orbit around a V = 12.6 mag G6V ([Fe/H] = $+0.10\pm0.10$) star in K2 campaign 10. Our results are based on K2 time-series photometry combined with high-spatial resolution imaging and high-precision radial velocity measurements. We present the first mass measurement of K2-180b. K2-180b has a mass of $M_\mathrm{p}=11.3\pm1.9$ ${M_{\oplus}}$ and a radius of $R_\mathrm{p}=2.2\pm0.1$ ${R_{\oplus}}$ , yielding a mean density of $\rho_\mathrm{p}=5.6\pm1.9\,g\,cm^{-3}$, suggesting a rock composition. Given its radius, K2-180b is above the region of the so-called `planetary radius gap'. K2-180b is in addition not only one of the densest mini-Neptune-size planets, but also one of the few mini-Neptune-size planets known to transit a metal-poor star. We also constrain the planetary and orbital parameters of K2-140b and show that, given the currently available Doppler measurements, the eccentricity is consistent with zero, contrary to the results of a previous study., Comment: accepted in MNRAS
- Published
- 2018
- Full Text
- View/download PDF
15. CARMENES input catalogue of M dwarfs IV. New rotation periods from photometric time series
- Author
-
Alonso, E. Diez, Caballero, J. A., Montes, D., Juez, F. J. de Cos, Dreizler, S., Dubois, F., Jeffers, S. V., Lalitha, S., Naves, R., Reiners, A., Ribas, I., Vanaverbeke, S., Amado, P. J., Bejar, V. J. S., Cortes-Contreras, M., Herrero, E., Hidalgo, D., Kurster, M., Logie, L., Quirrenbach, A., Rau, S., Seifert, W., Schofer, P., and Tal-Or, L.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
Aims. The main goal of this work is to measure rotation periods of the M-type dwarf stars being observed by the CARMENES exoplanet survey to help distinguish radial-velocity signals produced by magnetic activity from those produced by exoplanets. Rotation periods are also fundamental for a detailed study of the relation between activity and rotation in late-type stars. Methods. We look for significant periodic signals in 622 photometric time series of 337 bright, nearby M dwarfs obtained by long-time baseline, automated surveys (MEarth, ASAS, SuperWASP, NSVS, Catalina, ASAS-SN, K2, and HATNet) and for 20 stars which we obtained with four 0.2-0.8 m telescopes at high geographical latitudes. Results. We present 142 rotation periods (73 new) from 0.12 d to 133 d and ten long-term activity cycles (six new) from 3.0 a to 11.5 a. We compare our determinations with those in the existing literature; we investigate the distribution of P rot in the CARMENES input catalogue,the amplitude of photometric variability, and their relation to vsin i and pEW(Halfa); and we identify three very active stars with new rotation periods between 0.34 d and 23.6 d., Comment: 34 pages, 43 figures, 2 appendix tables
- Published
- 2018
- Full Text
- View/download PDF
16. Torrefaction at low temperature as a promising pretreatment of lignocellulosic biomass in anaerobic digestion
- Author
-
Hidalgo, D., Castro, J., Díez, D., Martín-Marroquín, J.M., Gómez, M., and Pérez, E.
- Published
- 2023
- Full Text
- View/download PDF
17. Overexpression of EC-SOD Attenuates Hypoxia-induced Platelet Activation
- Author
-
Colon Hidalgo, D., primary, Posey, J., additional, Jordan, M., additional, Burciaga, S.D., additional, Delaney, C., additional, and Nozik, E., additional
- Published
- 2024
- Full Text
- View/download PDF
18. TESS's first planet: a super-Earth transiting the naked-eye star $\pi$ Mensae
- Author
-
Gandolfi, D., Barragan, O., Livingston, J., Fridlund, M., Justesen, A. B., Redfield, S., Fossati, L., Mathur, S., Grziwa, S., Cabrera, J., Garcia, R. A., Persson, C. M., Van Eylen, V., Hatzes, A. P., Hidalgo, D., Albrecht, S., Bugnet, L., Cochran, W. D., Csizmadia, Sz., Deeg., H., Eigmuller, Ph., Endl, M., Erikson, A., Esposito, M., Guenther, E., Korth, J., Luque, R., Rodriguez, P. Montanes, Nespral, D., Nowak, G., Patzold, M., and Prieto-Arranz, J.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report on the confirmation and mass determination of Pi Men c, the first transiting planet discovered by NASA's TESS space mission. Pi Men is a naked-eye (V=5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (Pi Men b) on a long-period (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES@AAT Doppler measurements, and archival HARPS@ESO-3.6m radial velocities, we found that Pi Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 +/- 0.81 MEarth, and a radius of Rc = 2.06 +/- 0.03 REarth. Based on the planet's orbital period and size, Pi Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars., Comment: Accepted for publication in A&A. Eleven pages, 5 figures, 5 tables
- Published
- 2018
- Full Text
- View/download PDF
19. Detection and Doppler monitoring of EPIC 246471491, a system of four transiting planets smaller than Neptune
- Author
-
Palle, E., Nowak, G., Luque, R., Hidalgo, D., Barragan, O., Prieto-Arranz, J., Hirano, T., Fridlund, M., Gandolfi, D., Livingston, J., Dai, F., Morales, J. C., Lafarga, M., Albrecht, S., Alonso, R., Amado, P. J., Caballero, J. A., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fukui, A., Guenther, E. W., Grziwa, S., Hatzes, A. P., Korth, J., Kürster, M., Kuzuhara, M., Rodriguez, P. Montañes, Murgas, F., Narita, N., Nespral, D., Pätzold, M., Persson, C. M., Quirrenbach, A., Rauer, H., Redfield, S., Reiners, A., Ribas, I., Smith, A. M. S., Van Eylen, V., Winn, J. N., and Zechmeister, M.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
The Kepler extended mission, also known as K2, has provided the community with a wealth of planetary candidates that orbit stars typically much brighter than the targets of the original mission. These planet candidates are suitable for further spectroscopic follow-up and precise mass determinations, leading ultimately to the construction of empirical mass-radius diagrams. Particularly interesting is to constrain the properties of planets between the Earth and Neptune in size, the most abundant type of planets orbiting Sun-like stars with periods less than a few years. Among many other K2 candidates, we discovered a multi-planetary system around EPIC246471491, with four planets ranging in size from twice the size of Earth, to nearly the size of Neptune. We measure the mass of the planets of the EPIC246471491 system by means of precise radial velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. With our data we are able to determine the mass of the two inner planets of the system with a precision better than 15%, and place upper limits on the masses of the two outer planets. We find that EPIC246471491b has a mass of 9.68 Me, and a radius of 2.59 Re, yielding a mean density of 3.07 g/cm3, while EPIC246471491c has a mass of 15.68 Me, radius of 3.53 Re, and a mean density of 19.5 g/cm3. For EPIC246471491d (R=2.48Re) and EPIC246471491e (R=1.95Re) the upper limits for the masses are 6.5 and 10.7 Me, respectively. The system is thus composed of a nearly Neptune-twin planet (in mass and radius), two sub-Neptunes with very different densities and presumably bulk composition, and a fourth planet in the outermost orbit that resides right in the middle of the super-Earth/sub-Neptune radius gap. Future comparative planetology studies of this system can provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories., Comment: Submitted to A&A
- Published
- 2018
- Full Text
- View/download PDF
20. K2-295 b and K2-237 b: two transiting hot Jupiters
- Author
-
Smith, A. M. S., Csizmadia, Sz., Gandolfi, D., Albrecht, S., Alonso, R., Barragán, O., Cabrera, J., Cochran, W. D., Dai, F., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fridlund, M., Fukui, A., Grziwa, S., Guenther, E. W., Hatzes, A. P., Hidalgo, D., Hirano, T., Korth, J., Kuzuhara, M., Livingston, J., Narita, N., Nespral, D., Niraula, P., Nowak, G., Palle, E., Pätzold, M., Persson, C. M., Prieto-Arranz, J., Rauer, H., Redfield, S., Ribas, I., and Van Eylen, V.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery from K2 of two transiting hot Jupiter systems. K2-295 (observed in Campaign 8) is a K5 dwarf which hosts a planet slightly smaller than Jupiter, orbiting with a period of 4.0 d. We have made an independent discovery of K2-237 b (Campaign 11), which orbits an F6 dwarf every 2.2 d and has an inflated radius 50 - 60 per cent larger than that of Jupiter. We use high-precision radial velocity measurements, obtained using the HARPS and FIES spectrographs, to measure the planetary masses. We find that K2-295 b has a similar mass to Saturn, while K2-237 b is a little more massive than Jupiter., Comment: 26 pages, 12 figures, accepted for publication in Acta Astronomica
- Published
- 2018
- Full Text
- View/download PDF
21. K2-260 b: a hot Jupiter transiting an F star, and K2-261 b: a warm Saturn around a bright G star
- Author
-
Johnson, M. C., Dai, F., Justesen, A. B., Gandolfi, D., Hatzes, A. P., Nowak, G., Endl, M., Cochran, W. D., Hidalgo, D., Watanabe, N., Parviainen, H., Hirano, T., Villanueva Jr., S., Prieto-Arranz, J., Narita, N., Palle, E., Guenther, E. W., Barragán, O., Trifonov, T., Niraula, P., MacQueen, P. J., Cabrera, J., Csizmadia, Sz., Eigmüller, Ph., Grziwa, S., Korth, J., Pätzold, M., Smith, A. M. S., Albrecht, S., Alonso, R., Deeg, H., Erikson, A., Esposito, M., Fridlund, M., Fukui, A., Kusakabe, N., Kuzuhara, M., Livingston, J., Rodriguez, P. Montañes, Nespral, D., Persson, C. M., Purismo, T., Raimundo, S., Rauer, H., Ribas, I., Tamura, M., Van Eylen, V., and Winn, J. N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery and confirmation of two new transiting giant planets from the Kepler extended mission K2. K2-260 b is a hot Jupiter transiting a $V=12.7$ F6V star in K2 Field 13, with a mass and radius of $M_{\star}=1.39_{-0.06}^{+0.05} M_{\odot}$ and $R_{\star}=1.69 \pm 0.03 R_{\odot}$. The planet has an orbital period of $P=2.627$ days, and a mass and radius of $M_P=1.42^{+0.31}_{-0.32} M_J$ and $R_P=1.552^{+0.048}_{-0.057} R_J$. This is the first K2 hot Jupiter with a detected secondary eclipse in the Kepler bandpass, with a depth of $71 \pm 15$ ppm, which we use to estimate a geometric albedo of $A_g\sim0.2$. We also detected a candidate stellar companion at 0.6" from K2-260; we find that it is very likely physically associated with the system, in which case it would be an M5-6V star at a projected separation of $\sim400$ AU. K2-261 b is a warm Saturn transiting a bright ($V=10.5$) G7IV/V star in K2 Field 14. The host star is a metal-rich ([Fe/H]$=0.36 \pm 0.06$), mildly evolved $1.10_{-0.02}^{+0.01} M_{\odot}$ star with $R_{\star}=1.65 \pm 0.04 R_{\odot}$. Thanks to its location near the main sequence turn-off, we can measure a relatively precise age of $8.8_{-0.3}^{+0.4}$ Gyr. The planet has $P=11.633$ days, $M_P=0.223 \pm 0.031 M_J$, and $R_P=0.850^{+0.026}_{-0.022} R_J$, and its orbit is eccentric ($e=0.39 \pm 0.15$). Its brightness and relatively large transit depth make this one of the best known warm Saturns for follow-up observations to further characterize the planetary system., Comment: Published in MNRAS. 18 pages, 10 figures
- Published
- 2018
- Full Text
- View/download PDF
22. Super-Earth of 8 Mearth in a 2.2-day orbit around the K5V star K2-216
- Author
-
Persson, C. M., Fridlund, M., Barragán, O., Dai, F., Gandolfi, D., Hatzes, A. P., Hirano, T., Grziwa, S., Korth, J., Prieto-Arranz, J., Fossati, L., Van Eylen, V., Justesen, A. Bo, Livingston, J., Kubyshkina, D., Deeg, H. J., Guenther, E. W., Nowak, G., Eigmüller, J. Cabrera Ph., Csizmadia, Sz, Smith, A. M. S., Erikson, A., Sobrino, S. Albrecht R. Alonso, Cochran, W. D., Endl, M., Esposito, M., Fukui, A., Heeren, P., Hidalgo, D., Hjorth, M., Kuzuhara, M., Narita, N., Nespral, D., Palle, E., Pätzold, M., Rauer, H., Rodler, F., and Winn, J. N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
The KESPRINT consortium identified K2-216 as a planetary candidate host star in the K2 space mission Campaign 8 field with a transiting super-Earth. The planet has recently been validated as well. Our aim was to confirm the detection and derive the main physical characteristics of K2-216b, including the mass. We performed a series of follow-up observations: high resolution imaging with the FastCam camera at the TCS, the Infrared Camera and Spectrograph at Subaru, and high resolution spectroscopy with HARPS (ESO, La Silla), HARPS-N (TNG), and FIES (NOT). The stellar spectra were analyzed with the SpecMatch-Emp and SME codes to derive the stellar fundamental properties. We analyzed the K2 light curve with the Pyaneti software. The radial-velocity measurements were modelled with both a Gaussian process (GP) regression and the floating chunk offset (FCO) technique to simultaneously model the planetary signal and correlated noise associated with stellar activity. Imaging confirms that K2-216 is a single star. Our analysis discloses that the star is a moderately active K5V star of mass 0.70+/-0.03 Msun and radius 0.72+/-0.03 Rsun. Planet b is found to have a radius of 1.75+0.17-0.10 Rearth and a 2.17-day orbit in agreement with previous results. We find consistent results for the planet mass from both models: 7.4+/-2.2 Mearth from the GP regression, and 8.0+/-1.6 Mearth from the FCO technique, which implies that this planet is a super-Earth. The planet parameters put planet b in the middle of, or just below, the gap of the radius distribution of small planets. The density is consistent with a rocky composition of primarily iron and magnesium silicate. In agreement with theoretical predictions, we find that the planet is a remnant core, stripped of its atmosphere, and is one of the largest planets found that has lost its atmosphere., Comment: 17 pages, 10 figures, accepted by Astronomy & Astrophysics 28 June 2018
- Published
- 2018
- Full Text
- View/download PDF
23. HD 89345: a bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2
- Author
-
Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., García, R. A., Guenther, E., Hjorth, M., Justesen, A. B., Livingston, J., Lund, M. N., Hernández, F. Pérez, Prieto-Arranz, J., Regulo, C., Bugnet, L., Everett, M. E., Hirano, T., Nespral, D., Nowak, G., Palle, E., Aguirre, V. Silva, Trifonov, T., Winn, J. N., Barragán, O., Beck, P. G., Chaplin, W. J., Cochran, W. D., Csizmadia, S., Deeg, H., Endl, M., Heeren, P., Grziwa, S., Hatzes, A. P., Hidalgo, D., Korth, J., Mathis, S., Rodriguez, P. Montañes, Narita, N., Patzold, M., Persson, C. M., Rodler, F., and Smith, A. M. S.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star ($V = 9.3$ mag) observed by the K2 mission with one-minute time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be $1.12^{+0.04}_{-0.01}~M_\odot$ and $1.657^{+0.020}_{-0.004}~R_\odot$, respectively. The star appears to have recently left the main sequence, based on the inferred age, $9.4^{+0.4}_{-1.3}~\mathrm{Gyr}$, and the non-detection of mixed modes. The star hosts a "warm Saturn" ($P = 11.8$~days, $R_p = 6.86 \pm 0.14~R_\oplus$). Radial-velocity follow-up observations performed with the FIES, HARPS, and HARPS-N spectrographs show that the planet has a mass of $35.7 \pm 3.3~M_\oplus$. The data also show that the planet's orbit is eccentric ($e\approx 0.2$). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter-McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to conform to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity., Comment: Submitted to MNRAS on 23 February 2018, accepted for publication, 4 May 2018
- Published
- 2018
- Full Text
- View/download PDF
24. Mass determination of the 1:3:5 near-resonant planets transiting GJ 9827 (K2-135)
- Author
-
Prieto-Arranz, J., Palle, E., Gandolfi, D., Barragán, O., Guenther, E. W., Dai, F., Fridlund, M., Hirano, T., Livingston, J., Niraula, P., Persson, C. M., Redfield, S., Albrecht, S., Alonso, R., Antoniciello, G., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Everett, M. E., Fukui, A., Grziwa, S., Hatzes, A. P., Hidalgo, D., Hjorth, M., Korth, J., Lorenzo-Oliveira, D., Murgas, F., Narita, N., Nespral, D., Nowak, G., Pätzold, M., Rodríguez, P. Montañés, Rauer, H., Ribas, I., Smith, A. M. S., Van Eylen, V., and Winn, J. N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
Aims. GJ 9827 (K2-135) has recently been found to host a tightly packed system consisting of three transiting small planets whose orbital periods of 1.2, 3.6, and 6.2 days are near the 1:3:5 ratio. GJ 9827 hosts the nearest planetary system (d = $30.32\pm1.62$ pc) detected by Kepler and K2 . Its brightness (V = 10.35 mag) makes the star an ideal target for detailed studies of the properties of its planets. Results. We find that GJ 9827 b has a mass of $M_\mathrm{b}=3.74^{+0.50}_{-0.48}$ $M_\oplus$ and a radius of $R_\mathrm{b}=1.62^{+0.17}_{-0.16}$ $R_\oplus$, yielding a mean density of $\rho_\mathrm{b} = 4.81^{+1.97}_{-1.33}$ g cm$^{-3}$. GJ 9827 c has a mass of $M_\mathrm{c}=1.47^{+0.59}_{-0.58}$ $M_\oplus$, radius of $R_\mathrm{c}=1.27^{+0.13}_{-0.13}$ $R_\oplus$, and a mean density of $\rho_\mathrm{c}= 3.87^{+2.38}_{-1.71}$ g cm$^{-3}$. For GJ 9827 d we derive $M_\mathrm{d}=2.38^{+0.71}_{-0.69}$ $M_\oplus$, $R_\mathrm{d}=2.09^{+0.22}_{-0.21}$ $R_\oplus$, and $\rho_\mathrm{d}= 1.42^{+0.75}_{-0.52}$ g cm$^{-3}$. Conclusions. GJ 9827 is one of the few known transiting planetary systems for which the masses of all planets have been determined with a precision better than 30%. This system is particularly interesting because all three planets are close to the limit between super-Earths and mini-Neptunes. We also find that the planetary bulk compositions are compatible with a scenario where all three planets formed with similar core/atmosphere compositions, and we speculate that while GJ 9827 b and GJ 9827 c lost their atmospheric envelopes, GJ 9827 d maintained its atmosphere, owing to the much lower stellar irradiation. This makes GJ 9827 one of the very few systems where the dynamical evolution and the atmospheric escape can be studied in detail for all planets, helping us to understand how compact systems form and evolve., Comment: 15 pages, 10 Figures, 8 tables
- Published
- 2018
- Full Text
- View/download PDF
25. Analytic topologically non-trivial solutions of the (3+1)-dimensional $U(1)$ gauged Skyrme model and extended duality
- Author
-
Avilés, L., Canfora, F., Dimakis, N., and Hidalgo, D.
- Subjects
High Energy Physics - Theory - Abstract
We construct the first analytic examples of topologically non-trivial solutions of the (3+1)-dimensional $U(1)$ gauged Skyrme model within a finite box in (3+1)-dimensional flat space-time. There are two types of gauged solitons. The first type corresponds to gauged Skyrmions living within a finite volume. The second corresponds to gauged time-crystals (smooth solutions of the $U(1)$ gauged Skyrme model whose periodic time-dependence is protected by a winding number). The notion of electromagnetic duality can be extended for these two types of configurations in the sense that the electric and one of the magnetic components can be interchanged. These analytic solutions show very explicitly the Callan-Witten mechanism (according to which magnetic monopoles may "swallow" part of the topological charge of the Skyrmion) since the electromagnetic field contribute directly to the conserved topological charge of the gauged Skyrmions. As it happens in superconductors, the magnetic field is suppressed in the core of the gauged Skyrmions. On the other hand, the electric field is strongly suppresed in the core of gauged time crystals., Comment: 19 pages, 2 figures, version accepted for publication in Physical Review D
- Published
- 2017
- Full Text
- View/download PDF
26. K2-141 b: A 5-M$_\oplus$ super-Earth transiting a K7 V star every 6.7 hours
- Author
-
Barragán, O., Gandolfi, D., Dai, F., Livingston, J., Persson, C. M., Hirano, T., Narita, N., Csizmadia, Sz., Winn, J. N., Nespral, D., Prieto-Arranz, J., Smith, A. M. S., Nowak, G., Albrecht, S., Antoniciello, G., Justesen, A. Bo, Cabrera, J., Cochran, W. D., Deeg., H., Eigmuller, Ph., Endl, M., Erikson, A., Fridlund, M., Fukui, A., Grziwa, S., Guenther, E., Hatzes, A. P., Hidalgo, D., Johnson, M. C., Korth, J., Palle, E., Patzold, M., Rauer, H., Tanaka, Y., and Van Eylen, V.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report on the discovery of K2-141 b (EPIC 246393474 b), an ultra-short-period super-Earth on a 6.7-hour orbit transiting an active K7 V star based on data from K2 campaign 12. We confirmed the planet's existence and measured its mass with a series of follow-up observations: seeing-limited MuSCAT imaging, NESSI high-resolution speckle observations, and FIES and HARPS high-precision radial-velocity monitoring. K2-141 b has a mass of $5.31 \pm 0.46 $ $M_{\oplus}$ and radius of $1.54^{+0.10}_{-0.09}$ $R_{\oplus}$, yielding a mean density of $8.00_{ - 1.45 } ^ { + 1.83 }$ $\mathrm{g\,cm^{-3}}$ and suggesting a rocky-iron composition. Models indicate that iron cannot exceed $\sim$70 % of the total mass. With an orbital period of only 6.7 hours, K2-141 b is the shortest-period planet known to date with a precisely determined mass., Comment: 11 pages, 4 Tables, 10 Figures, accepted for publication by A&A
- Published
- 2017
- Full Text
- View/download PDF
27. A novel framework for relationship of manufacturing tolerance and component-level performance of journal bearings
- Author
-
Hidalgo, D., Ruiz, R.O., and Delgado, A.
- Published
- 2022
- Full Text
- View/download PDF
28. Quality assessment of Clinical Practice Guidelines (CPG) for the diagnosis and treatment of inflammatory bowel disease using the AGREE II instrument: a systematic review
- Author
-
Zambrano-Sánchez, R., Alvarez-Mena, P., Hidalgo, D., Liquitay, C. M. Escobar, Franco, J. V. A., Vernooij, R. W. M., Simancas-Racines, D., Viteri-García, A., and Montesinos-Guevara, C.
- Published
- 2022
- Full Text
- View/download PDF
29. Influence of cavitation, pelleting, extrusion and torrefaction petreatments on anaerobic biodegradability of barley straw and vine shoots
- Author
-
Hidalgo, D., Martín-Marroquín, J.M., Castro, J., Gómez, M., and Garrote, L.
- Published
- 2022
- Full Text
- View/download PDF
30. Disproval of the validated planets K2-78b, K2-82b, and K2-92b
- Author
-
Cabrera, J., Barros, S. C. C., Armstrong, D., Hidalgo, D., Santos, N. C., Almenara, J. M., Alonso, R., Deleuil, M., Demangeon, O., Diaz, R. F., Lendl, M., Pfaff, J., Rauer, H., Santerne, A., Serrano, L. M., and Zucker, S.
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Transiting super-Earths orbiting bright stars in short orbital periods are interesting targets for the study of planetary atmospheres. While selecting super-Earths suitable for further characterization from the ground among a list of confirmed and validated exoplanets detected by K2, we found some suspicious cases that led to us re-assessing the nature of the detected transiting signal. We did a photometric analysis of the K2 light curves and centroid motions of the photometric barycenters. Our study shows that the validated planets K2-78b, K2-82b, and K2-92b are actually not planets but background eclipsing binaries. The eclipsing binaries are inside the Kepler photometric aperture, but outside the ground-based high resolution images used for validation. We advise extreme care on the validation of candidate planets discovered by space missions. It is important that all the assumptions in the validation process are carefully checked. An independent confirmation is mandatory in order to avoid wasting valuable resources on further characterization of non-existent targets., Comment: accepted for publication in A&A
- Published
- 2017
- Full Text
- View/download PDF
31. K2-137 b: an Earth-sized planet in a 4.3-hour orbit around an M-dwarf
- Author
-
Smith, A. M. S., Cabrera, J., Csizmadia, Sz., Dai, F., Gandolfi, D., Hirano, T., Winn, J. N., Albrecht, S., Alonso, R., Antoniciello, G., Barragán, O., Deeg, H., Eigmüller, Ph., Endl, M., Erikson, A., Fridlund, M., Fukui, A., Grziwa, S., Guenther, E. W., Hatzes, A. P., Hidalgo, D., Howard, A. W., Isaacson, H., Korth, J., Kuzuhara, M., Livingston, J., Narita, N., Nespral, D., Nowak, G., Palle, E., Pätzold, M., Persson, C. M., Petigura, E., Prieto-Arranz, J., Rauer, H., Ribas, I., and Van Eylen, V.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery from K2 of a transiting terrestrial planet in an ultra-short-period orbit around an M3-dwarf. K2-137 b completes an orbit in only 4.3 hours, the second-shortest orbital period of any known planet, just 4 minutes longer than that of KOI 1843.03, which also orbits an M-dwarf. Using a combination of archival images, AO imaging, RV measurements, and light curve modelling, we show that no plausible eclipsing binary scenario can explain the K2 light curve, and thus confirm the planetary nature of the system. The planet, whose radius we determine to be 0.89 +/- 0.09 Earth radii, and which must have a iron mass fraction greater than 0.45, orbits a star of mass 0.463 +/- 0.052 Msol and radius 0.442 +/- 0.044 Rsol., Comment: 12 pages, 9 figures, accepted for publication in MNRAS
- Published
- 2017
- Full Text
- View/download PDF
32. K2-137 b: an Earth-sized planet in a 4.3-h orbit around an M-dwarf
- Author
-
Smith, AMS, Cabrera, J, Csizmadia, Sz, Dai, F, Gandolfi, D, Hirano, T, Winn, JN, Albrecht, S, Alonso, R, Antoniciello, G, Barragán, O, Deeg, H, Eigmüller, Ph, Endl, M, Erikson, A, Fridlund, M, Fukui, A, Grziwa, S, Guenther, EW, Hatzes, AP, Hidalgo, D, Howard, AW, Isaacson, H, Korth, J, Kuzuhara, M, Livingston, J, Narita, N, Nespral, D, Nowak, G, Palle, E, Pätzold, M, Persson, CM, Petigura, E, Prieto-Arranz, J, Rauer, H, Ribas, I, and Van Eylen, V
- Subjects
planets and satellites: detection ,planets and satellites: individual: K2-137 b ,astro-ph.EP ,Astronomical and Space Sciences ,Astronomy & Astrophysics - Abstract
We report the discovery in K2's Campaign 10 of a transiting terrestrial planet in an ultrashort- period orbit around an M3-dwarf. K2-137 b completes an orbit in only 4.3 h, the second shortest orbital period of any known planet, just 4 min longer than that of KOI 1843.03, which also orbits an M-dwarf. Using a combination of archival images, adaptive optics imaging, radial velocity measurements, and light-curve modelling, we show that no plausible eclipsing binary scenario can explain the K2 light curve, and thus confirm the planetary nature of the system. The planet, whose radius we determine to be 0.89 ± 0.09 R⊕, and which must have an iron mass fraction greater than 0.45, orbits a star of mass 0.463 ± 0.052 M⊙ and radius 0.442 ± 0.044 R⊙.
- Published
- 2018
33. Prostatic artery embolization treatment for patients with benign prostatic hyperplasia who are permanent urinary catheter users ineligible for de-obstructive surgery
- Author
-
Salvador Hidalgo, D., Bernardello Ureta, M., Sbriglio, M., García Gámez, A., Sampere Moragas, J., Areal Calama, J., and Ágreda Castañeda, F.
- Published
- 2021
- Full Text
- View/download PDF
34. K2-99: a subgiant hosting a transiting warm Jupiter in an eccentric orbit and a long-period companion
- Author
-
Smith, A. M. S., Gandolfi, D., Barragán, O., Bowler, B., Csizmadia, Sz., Endl, M., Fridlund, M. C. V., Grziwa, S., Guenther, E., Hatzes, A. P., Nowak, G., Albrecht, S., Alonso, R., Cabrera, J., Cochran, W. D., Cusano, F., Deeg, H. J., Eigmüller, Ph., Erikson, A., Hidalgo, D., Hirano, T., Johnson, M. C., Korth, J., Mann, A., Narita, N., Nespral, D., Palle, E., Pätzold, M., Prieto-Arranz, J., Rauer, H., Ribas, I., Tingley, B., and Wolthoff, V.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery from K2 of a transiting planet in an 18.25-d, eccentric (0.19$\pm$ 0.04) orbit around K2-99, an 11th magnitude subgiant in Virgo. We confirm the planetary nature of the companion with radial velocities, and determine that the star is a metal-rich ([Fe/H] = 0.20$\pm$0.05) subgiant, with mass $1.60^{+0.14}_{-0.10}~M_\odot$ and radius $3.1\pm 0.1~R_\odot$. The planet has a mass of $0.97\pm0.09~M_{\rm Jup}$ and a radius $1.29\pm0.05~R_{\rm Jup}$. A measured systemic radial acceleration of $-2.12\pm0.04~{\rm m s^{-1} d^{-1}}$ offers compelling evidence for the existence of a third body in the system, perhaps a brown dwarf orbiting with a period of several hundred days., Comment: 10 pages, 6 figures, 4 tables, accepted for publication in MNRAS
- Published
- 2016
- Full Text
- View/download PDF
35. Nutrient recycling: from waste to crop
- Author
-
Hidalgo, D., Corona, F., and Martín-Marroquín, J. M.
- Published
- 2021
- Full Text
- View/download PDF
36. Power-to-methane, coupling CO2 capture with fuel production: An overview
- Author
-
Hidalgo, D. and Martín-Marroquín, J.M.
- Published
- 2020
- Full Text
- View/download PDF
37. Selective separation of CH4 and CO2 using membrane contactors
- Author
-
Hidalgo, D., Sanz-Bedate, S., Martín-Marroquín, J.M., Castro, J., and Antolín, G.
- Published
- 2020
- Full Text
- View/download PDF
38. Correction to: Nutrient recycling: from waste to crop
- Author
-
Hidalgo, D., Corona, F., and Martín-Marroquín, J. M.
- Published
- 2022
- Full Text
- View/download PDF
39. A multi-waste management concept as a basis towards a circular economy model
- Author
-
Hidalgo, D., Martín-Marroquín, J.M., and Corona, F.
- Published
- 2019
- Full Text
- View/download PDF
40. Marketing para comunicar servicios profesionales farmacéuticos: experiencia en una farmacia comunitaria de l’Alfàs del Pi
- Author
-
García Zaragozá ME, Arocas Ruiz N, Puerta Rodríguez MD, Mira Padilla JA, Arnaudas Hidalgo D, and Avío Schmidt M
- Subjects
servicios comunitarios de farmacia ,comercialización de los servicios de salud ,cardiovascular ,Pharmacy and materia medica ,RS1-441 - Abstract
Objetivos: Iniciar un nuevo servicio remunerado para el control y cribado de factores de riesgo cardiovascular, promocionándolo mediante una novedosa campaña de marketing. Conocer el nivel de riesgo cardiovascular de nuestros usuarios, así como de algunos de sus principales factores modificables asociados. Material y métodos: Estudio observacional transversal en usuarios adultos que solicitaron participar en la campaña. Esta se denominó “First Date: una cita con tu corazón” (haciendo alusión todos sus materiales al conocido programa televisivo) y se ofreció a los pacientes un Menú Especial a 12€ compuesto por un Entrante (Perímetro abdominal, IMC, PA y Toma de pulso), Plato Principal (Colesterol total y Edad Vascular) y Postre (nivel RCV). Resultados: Realizamos 34 menús: edad media 57,8 años y 53% de mujeres. Encontramos valores por encima de los límites normales, en (% de la población total): perímetro abdominal (50%), IMC (18% sobrepeso y 5% obesidad), colesterol total (70,6%), VOP (23,5%) y PAS (14,7% PAS). Respecto a la PAD se encontraron diferencias significativas entre ambos sexos: 70.0 ± 2.0 mmHg en mujeres y 83.1 ± 3.2 mmHg en hombres (**p=0.0012 t test). También se encontraron diferencias entre sexos en el hábito tabáquico (el 75% de los fumadores eran hombres) y de consumo de alcohol (el 72,7% de consumidores habituales eran hombres). El 29,4% de la población tenían RCV medio y el 20,6% elevado. Encontramos pulso irregular sin diagnóstico previo en el 11,8% de pacientes (2 hombres y 2 mujeres). Se realizaron 4 derivaciones al médico, 7 derivaciones para control de PA en la farmacia, 26 recomendaciones sobre dieta y ejercicio, 6 recomendaciones sobre tabaco y 3 intervenciones en adherencia. Conclusiones: Ayudados por la campaña de marketing, se consiguió comunicar e iniciar adecuadamente nuestro servicio profesional (remunerado) de cribado y control de los factores de riesgo cardiovascular. Los valores encontrados en nuestra población tienen un margen de mejora elevado, sobre todo en cuanto a los niveles de PAD, colesterol total, perímetro abdominal y nivel de RCV.
- Published
- 2018
- Full Text
- View/download PDF
41. The effect of feed composition on anaerobic co-digestion of animal-processing by-products
- Author
-
Hidalgo, D., Martín-Marroquín, J.M., and Corona, F.
- Published
- 2018
- Full Text
- View/download PDF
42. Optimization of Pulsed Electrochemical Micromachining in Stainless Steel
- Author
-
Rodriguez, P., Hidalgo, D., and Labarga, J.E.
- Published
- 2018
- Full Text
- View/download PDF
43. Pulmonary Alveolar Proteinosis Secondary to Sarcoidosis
- Author
-
King, S.I., primary, Colon Hidalgo, D., additional, and Graney, B.A., additional
- Published
- 2023
- Full Text
- View/download PDF
44. Pulmonary Hypertension in a Patient With Left-Sided Partial Anomalous Pulmonary Venous Return
- Author
-
Pope, K., primary, Rhoads, S., additional, Colon Hidalgo, D., additional, and Hountras, P., additional
- Published
- 2023
- Full Text
- View/download PDF
45. Loss of Vascular EC-SOD Is Protective Against PH in the Sugen Hypoxia Model of Pulmonary Hypertension Through Changes in Mitochondrial Respiration Mediated by p-AMPK
- Author
-
Colon Hidalgo, D., primary, Burciaga, S., additional, Dee, N., additional, Elajaili, H.B., additional, Jordan, M., additional, Posey, J., additional, Jonscher, R., additional, Sparagna, G., additional, Sucharov, C., additional, Delaney, C., additional, and Nozik, E., additional
- Published
- 2023
- Full Text
- View/download PDF
46. Evaluation of Intergovernmental Panel on Climate Change (IPCC) equations to predict enteric methane emission from lactating cows fed Mediterranean diets
- Author
-
Colombini, S., primary, Graziosi, A. Rota, additional, Galassi, G., additional, Gislon, G., additional, Crovetto, G.M., additional, Enriquez-Hidalgo, D., additional, and Rapetti, L., additional
- Published
- 2023
- Full Text
- View/download PDF
47. Cattle urine metabolomics from permanent pastures and high sugar grass/white clover swards
- Author
-
Enriquez-Hidalgo, D., primary, Mead, A., additional, McAuliffe, G.A., additional, Blackwell, M.S.A., additional, Darch, T., additional, Griffith, B., additional, Fleming, H., additional, Horricks, C., additional, Hood, J., additional, Le Cocq, K., additional, Takahashi, T., additional, Lee, M.R.F., additional, and Cardenas, L., additional
- Published
- 2023
- Full Text
- View/download PDF
48. Synthesis of 2H-benzotriazole based donor-acceptor polymers bearing carbazole derivative as pendant groups: Optical, electronical and photovoltaic properties
- Author
-
Jessop, I.A., Bustos, M., Hidalgo, D., Terraza, C.A., Tundidor-Camba, A., Pardo, M.A., Fuentealba, D., Hssein, M., and Bernede, J.C.
- Published
- 2016
- Full Text
- View/download PDF
49. Long term testing of Microbial Fuel Cells: Comparison of different anode materials
- Author
-
Hidalgo, D., Tommasi, T., Velayutham, K., and Ruggeri, B.
- Published
- 2016
- Full Text
- View/download PDF
50. The study of electrochemically active planktonic microbes in microbial fuel cells in relation to different carbon-based anode materials
- Author
-
Schilirò, T., Tommasi, T., Armato, C., Hidalgo, D., Traversi, D., Bocchini, S., Gilli, G., and Pirri, C.F.
- Published
- 2016
- Full Text
- View/download PDF
Catalog
Discovery Service for Jio Institute Digital Library
For full access to our library's resources, please sign in.