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11 results on '"Mallorquín, Manuel"'

1. TOI-837b is a Young Saturn-sized Exoplanet with a Massive 70 $M_{\oplus}$ Core

Author

Barragán, Oscar, Yu, Haochuan, Freckelton, Alix Violet, Meech, Annabella, Cretignier, Michael, Mortier, Annelies, Aigrain, Suzanne, Klein, Baptiste, O'Sullivan, Niamh K., Gillen, Edward, Nielsen, Louise Dyregaard, Mallorquín, Manuel, and Zicher, Norbert

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

We present an exhaustive photometric and spectroscopic analysis of TOI-837, a F9/G0 35 Myr young star, hosting a transiting exoplanet, TOI-837b, with an orbital period of 8.32d. Utilising data from TESS and ground-based observations, we determine a planetary radius of 0.82 R_J for TOI-837b. Through detailed HARPS spectroscopic time series analysis, we derive a Doppler semi-amplitude of 35 m/s, corresponding to a planetary mass of 0.39 M_J. The derived planetary properties suggest a substantial core of approximately 70 M_E, constituting about 60% of the planet's total mass. This finding poses a significant challenge to existing theoretical models of core formation. We propose that future atmospheric observations with JWST could provide insights into resolving ambiguities of TOI-837b, offering new perspectives on its composition, formation, and evolution., Comment: MNRAS published version, MNRAS, 531, 4275

Published
2024
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2. SG-WAS: a new Wireless Autonomous Night Sky Brightness Sensor

Author

Alarcon, Miguel R., Puig-Subirà, Marta, Serra-Ricart, Miquel, Lemes-Perera, Samuel, Mallorquín, Manuel, and López, César

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The main features of SG-WAS (SkyGlow Wireless Autonomous Sensor), a low-cost device for measuring Night Sky Brightness (NSB), are presented. SG-WAS is based on the TSL237 sensor --like the Unihedron Sky Quality Meter (SQM) or the STARS4ALL Telescope Encoder and Sky Sensor (TESS)--, with wireless communication (LoRa, WiFi, or LTE-M) and solar-powered rechargeable batteries. Field tests have been performed on its autonomy, proving that it can go up to 20 days without direct solar irradiance and remain hibernating after that for at least \mbox{4 months}, returning to operation once re-illuminated. A new approach to the acquisition of average NSB measurements and their instrumental uncertainty (of the order of thousandths of a magnitude) is presented. In addition, the results of a new Sky Integrating Sphere (SIS) method have shown the possibility of performing mass device calibration with uncertainties below 0.02 mag/arcsec$^2$. SG-WAS is the first fully autonomous and wireless low-cost NSB sensor to be used as an independent or networked device in remote locations without any additional infrastructure., Comment: 15 pages, 9 figures

Published
2021
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3. TOI-837 b is a young Saturn-sized exoplanet with a massive 70 M⊕ core

Author

Barragán, Oscar, primary, Yu, Haochuan, additional, Freckelton, Alix Violet, additional, Meech, Annabella, additional, Cretignier, Michael, additional, Mortier, Annelies, additional, Aigrain, Suzanne, additional, Klein, Baptiste, additional, O’Sullivan, Niamh K, additional, Gillen, Edward, additional, Nielsen, Louise Dyregaard, additional, Mallorquín, Manuel, additional, and Zicher, Norbert, additional

Published
2024
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4. TOI-837 b is a young Saturn-sized exoplanet with a massive 70 M⊕ core.

Author

Barragán, Oscar, Yu, Haochuan, Freckelton, Alix Violet, Meech, Annabella, Cretignier, Michael, Mortier, Annelies, Aigrain, Suzanne, Klein, Baptiste, O'Sullivan, Niamh K, Gillen, Edward, Nielsen, Louise Dyregaard, Mallorquín, Manuel, and Zicher, Norbert

Subjects
TIME series analysis, PLANETARY mass, NATURAL satellites, EXTRASOLAR planets
Abstract

We present an exhaustive photometric and spectroscopic analysis of TOI-837, a F9/G0 35 Myr young star, hosting a transiting exoplanet, TOI-837 b, with an orbital period of ∼8.32 d. Utilizing data from the Transiting Exoplanet Survey Satellite and ground-based observations, we determine a planetary radius of |$0.818_{-0.024}^{+0.034}$| R J for TOI-837 b. Through detailed High Accuracy Radial Velocity Planet Searcher spectroscopic time series analysis, we derive a Doppler semi-amplitude of |$34.7_{-5.6}^{+5.3}$| |${\rm m\, s^{-1}}$|⁠ , corresponding to a planetary mass of |$0.379_{-0.061}^{+0.058}$| M J. The derived planetary properties suggest a substantial core of approximately 70 M⊕, constituting about 60 per cent of the planet's total mass. This finding poses a significant challenge to existing theoretical models of core formation. We propose that future atmospheric observations with JWST could provide insights into resolving ambiguities of TOI-837 b, offering new perspectives on its composition, formation, and evolution. [ABSTRACT FROM AUTHOR]

Published
2024
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5. Dynamical masses of two young transiting Neptune-size planets in the young 400 Myr star HD63433

Author

Mallorquín, Manuel, Lodieu, Nicolas, S. Béjar, Víctor J., Zapatero-Osorio, María Rosa, Suárez Mascareño, Alejandro, Zechmeister, Mathias, Tabernero, Hugo M., Pallé, Enric, Luque, Rafa, and Montes, David

Subjects
Exoplanets
Abstract

Despite the discovery of thousands of exoplanets, the mechanisms of planet formation and evolution have not been well tested with observations, mainly because the lack of a complete photometric and spectroscopic characterization of young planets, which presents a big challenge due to the high stellar activity of young stars. By determining the masses of young exoplanets, we can establish their composition, and investigate their evolution with age. For these observations, we can deduce if they were formed without gas (rocky planets) from their origin, or if they are born as small gaseous planets that lose their atmosphere rapidly (~tens of Myr) by photoevaporation (Murray-Clay et al. 2019) or slowly (~1 Gyr) by core-powered mass loss (Ginzburg et al. 2018). HD63433 is a very bright and fast rotating (6.46 days) solar-type star of the young (~400Myr) Ursa Major moving group hosting two transiting mini-Neptune-size exoplanets (Mann et al. 2020) with orbital periods of 7.11 (HD63433 b) and 20.55 (HD63433 c) days. We have collected 150 Radial Velocity (RV) measurements of HD63433 with CARMENES spectrograph over 1.4 years to determine the mass of the planets (Mallorquín et al. 2022, in prep). We have jointly modeled the transits, the keplerian planetary signal, and stellar activity with Gaussian Processes combining the TESS photometry and the CARMENES RV dataset. Our results reveal that the outer planet is detected in the CARMENES time series with an amplitude of 4.1+-1.0 m/s at the level of 4-sigma, which correspond to an absolute mass of Mp=17.4+-4.3 mass of the Earth for HD63433 c, making it the smallest planet with a robust mass determination at young ages. We report an upper limit of Mp

Published
2022
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8. Column Integrated Water Vapor and Aerosol Load Characterization with the New ZEN-R52 Radiometer

Author

Almansa, Antonio Fernando, primary, Cuevas, Emilio, additional, Barreto, África, additional, Torres, Benjamín, additional, García, Omaira Elena, additional, Delia García, Rosa, additional, Velasco-Merino, Cristian, additional, Cachorro, Victoria Eugenia, additional, Berjón, Alberto, additional, Mallorquín, Manuel, additional, López, César, additional, Ramos, Ramón, additional, Guirado-Fuentes, Carmen, additional, Negrillo, Ramón, additional, and de Frutos, Ángel Máximo, additional

Published
2020
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10. Light conditions and heterogeneity in illumination affect growth and survival of Octopus vulgaris paralarvae reared in the hatchery

Author

Tur, Ricardo, Roura, Á., Márquez, L., López-Galindo, Cristina, Lago, M. J., Mallorquín, Manuel, Almansa, Eduardo, Tur, Ricardo, Roura, Á., Márquez, L., López-Galindo, Cristina, Lago, M. J., Mallorquín, Manuel, and Almansa, Eduardo

Abstract

In order to succeed in common octopus (Octopus vulgaris) aquaculture, it is necessary to overcome the massive paralarval mortalities, which are likely related to zootechnical and/or nutritional aspects. Among the zootechnical aspects, the effect of light could be vital for the development of paralarvae given their sophisticated visual system. O. vulgaris paralarvae display vertical behavior in the wild, being in deeper waters during the day and close to the surface at night. For this reason, the present study traces a collection of light assays in captivity, to test ecologically-driven hypotheses on the growth and survival of octopus paralarvae. The first assay tested a factorial combination of light colors (blue vs white) and intensity (low ~13 lx (36 W/ m2 ), medium ~87 lx (151 W/m2 ) and high ~265 lx (422 W/m2 )). The results pointed to a significant negative impact of low light intensities (13 and 87 lx) on paralarval growth. The second assay was designed to contrast light colors (blue vs white), different levels of intensities (300 lx (478 W/m2 ) vs 600 lx (1077 W/m2 )) and partial coverage of the tanks using a shade mesh, named as “shadow zone” (half-covered vs non-covered tanks). In halfcovered tanks, survival was significantly improved, with the best results coming from half-covered tanks with blue light and 600 lx, but no differences in dry weight were observed. The third experiment tested a factor called “light source position” with two levels: “Control” when the light incidence angle was 0° with respect to the normal direction (i.e. perpendicular to the water surface), and “Oblique” when the light incidence angle was 60° with respect to the normal direction. In this experiment, survival significantly improved under oblique light but no differences in dry weight were detected. The last experiment was an unifactorial design combining “light source position” and “tank partial coverage” with three treatments: i) control light with uncovered tanks, ii) oblique

Published
2018

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