Context.
Long-period transiting planets provide the opportunity to better understand the formation and evolution of planetary systems. Their atmospheric properties remain largely unaltered by tidal ...or radiative effects of the host star, and their orbital arrangement reflects a different and less extreme migrational history compared to close-in objects. The sample of long-period exoplanets with well-determined masses and radii is still limited, but a growing number of long-period objects reveal themselves in the Transiting Exoplanet Survey Satellite (TESS) data.
Aims.
Our goal is to vet and confirm single-transit planet candidates detected in the TESS space-based photometric data through spectroscopic and photometric follow-up observations with ground-based instruments.
Methods.
We used high-resolution spectrographs to confirm the planetary nature of the transiting candidates and measure their masses. We also used the Next Generation Transit Survey (NGTS) to photometrically monitor the candidates in order to observe additional transits. Using a joint modeling of the light curves and radial velocities, we computed the orbital parameters of the system and were able to precisely measure the mass and radius of the transiting planets.
Results.
We report the discovery of two massive, warm Jupiter-size planets, one orbiting the F8-type star TOI-5153 and the other orbiting the G1-type star NGTS-20 (=TOI-5152). From our spectroscopic analysis, both stars are metal rich with a metallicity of 0.12 and 0.15, respectively. Only TOI-5153 presents a second transit in the TESS extended mission data, but NGTS observed NGTS-20 as part of its mono-transit follow-up program and detected two additional transits. Follow-up high-resolution spectroscopic observations were carried out with CORALIE, CHIRON, FEROS, and HARPS. TOI-5153 hosts a planet with a period of 20.33 days, a planetary mass of 3.26
−0.17
+0.18
Jupiter masses (
M
J
), a radius of 1.06
−0.04
+0.04
R
J
, and an orbital eccentricity of 0.091
−0.026
+0.024
. NGTS-20 b is a 2.98
−0.15
+0.16
M
J
planet with a radius of 1.07
−0.04
+0.04
R
J
on an eccentric 0.432
−0.023
+0.023
orbit with an orbital period of 54.19 days. Both planets are metal enriched and their heavy element content is in line with the previously reported mass-metallicity relation for gas giants.
Conclusions.
Both warm Jupiters orbit moderately bright host stars, making these objects valuable targets for follow-up studies of the planetary atmosphere and measurement of the spin-orbit angle of the system.
Context.
The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete ...their picture.
Aims.
In this paper, we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star.
Methods.
We use a set of precise radial velocity observations from HARPS, PFS, and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system.
Results.
We find that TOI-969 b is a transiting close-in (
P
b
~ 1.82 days) mini-Neptune planet (
m
b
= 9.1
−1.0
+1.1
M
⊕
,
R
b
= 2.765
−0.097
+0.088
R
⊕
), placing it on the lower boundary of the hot-Neptune desert (
T
eq,b
= 941 ± 31 K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of
P
c
= 1700
−280
+290
days, a minimum mass of
m
c
sin
i
c
= 11.3
−0.9
+1.1
M
Jup
, and a highly eccentric orbit of
e
c
= 0.628
−0.036
+0.043
.
Conclusions.
The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93 and orbits a moderately bright (
G
= 11.3 mag) star, making it an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems.
ABSTRACT Background: Meat is an important source of nutrients. However, in recent years their consumption is associated with chronic-degenerative diseases giving it the perception of “unhealthy food” ...Given that meat is an affordable source of quality protein; its improvement entails a huge challenge for the industry and science. Methods: The search and structured review of the literature in the last ten years in the scientific databases of articles related to the elaboration of restructured meat products with functional ingredients derived from plants. Objective: This work presents a general overview, as well as the most representative studies on the elaboration of restructured meat with ingredients from plants considered functional. Conclusions: The present review is intended to emphasize the use of plant natural ingredients in the elaboration of functional restructured meat products as an alternative for consumers allowing the inclusion of functional compounds beneficial to human health in their daily diet.
Water-Use Efficiency (WUE) integrally determined as seed production per unit of water consumed is a trait of recent interest; however, until now little research has been performed to evaluate the ...importance of different components as reproductive habits in such trait. The aim of this study was to determine if reproductive habits are a main component of integral WUE on common bean. Pinto Saltillo cultivar of high WUE in spring-summer and autumn-winter cycles generated 39.4 and 43.9 % fewer flowers than the cultivar susceptible to limited water conditions; nevertheless, a lower rate of abortion along with more efficient reproductive habits as the capacity to produce 1.6 seeds more per pod on average permitted Pinto Saltillo to have a higher integral WUE; therefore, reproductive habits had a great impact on the trait here studied and these should be considered on the breeding programs.
Mesquite tree (
Prosopis
spp.), is an important species in arid zones, due to its nitrogen-fixing and adaptability to drought seasons, it also provides food for many species of wild animals which ...feed on its nectar, pollen, leaves and pods. This plant is an excellent source of protein, fiber, sugars and phytochemical compounds such as alkaloids, tannins, phenolics, steroids, terpenes and flavonoids. Mesquite has been used in farm animal nutrition as supplement with recommended proportions between 20 and 40%. The nutritional contributions also depend on the usage of pods or foliage, however, most of the studies highly recommend an enzymatic pretreatment to increase the biomass digestibility. Its nutritional characteristics and ability to grow under scarce water conditions turn it as a potential source to replace expensive forages for farm animal feeding especially in semiarid regions; however, the results in animal feeding are diverse. The usage of tree species in arid zones for animal feeding has been long proposed, but, for
Prosopis
spp. there are few updated studies despite of its potential usage. This work presents a general overview of the mesquite tree usage in animal feed.
Since 2018, the ESPRESSO spectrograph at the VLT has been hunting for planets in the southern skies via the radial velocity (RV) method. One of its goals is to follow up on candidate planets from ...transit surveys such as the TESS mission, with a particular focus on small planets for which ESPRESSO's RV precision is vital. We aim to confirm and characterise, in detail, three super-Earth candidate transiting planets from TESS using precise RVs from ESPRESSO. We analysed photometry from TESS and ground-based facilities, high-resolution imaging, and RVs from ESPRESSO, HARPS, and HIRES, to confirm and characterise three new planets: TOI-260 b, transiting a late K dwarf, and TOI-286 b and c, orbiting an early K dwarf. We also updated the parameters for the known super-Earth TOI-134 b (L 168-9 b), which is hosted by an M dwarf. TOI-260 b has a d period, $4.23 M_ oplus $ mass, and $1.71 R_ oplus $ radius. For TOI-286 b we find a d period, $4.53 M_ oplus $ mass, and $1.42 R_ oplus $ radius; for TOI-286 c, we find a d period, $3.72 M_ oplus $ mass, and $1.88 R_ oplus $ radius. For TOI-134 b we obtain a d period, $4.07 M_ oplus $ mass, and $1.63 R_ oplus $ radius. Circular models are preferred for all the planets, although for TOI-260 b the eccentricity is not well constrained. We computed bulk densities and placed the planets in the context of composition models. TOI-260 b lies within the radius valley, and is most likely a rocky planet. However, the uncertainty on the eccentricity and thus on the mass renders its composition hard to determine. TOI-286 b and c span the radius valley, with TOI-286 b lying below it and having a likely rocky composition, while TOI-286 c is within the valley, close to the upper border, and probably has a significant water fraction. With our updated parameters for TOI-134 b, we obtain a lower density than previous findings, giving a rocky or Earth-like composition.
The GAPS programme at TNG Carleo, I.; Malavolta, L.; Desidera, S. ...
Astronomy and astrophysics (Berlin),
2/2024, Letnik:
682
Journal Article
Recenzirano
Context . Different theories have been developed to explain the origins and properties of close-in giant planets, but none of them alone can explain all of the properties of the warm Jupiters (WJs, P ...orb = 10–200 days). One of the most intriguing characteristics of WJs is that they have a wide range of orbital eccentricities, challenging our understanding of their formation and evolution. Aims . The investigation of these systems is crucial in order to put constraints on formation and evolution theories. TESS is providing a significant sample of transiting WJs around stars bright enough to allow spectroscopic follow-up studies. Methods . We carried out a radial velocity (RV) follow-up study of the TESS candidate TOI-4515 b with the high-resolution spectrograph HARPS-N in the context of the GAPS project, the aim of which is to characterize young giant planets, and the TRES and FEROS spectrographs. We then performed a joint analysis of the HARPS-N, TRES, FEROS, and TESS data in order to fully characterize this planetary system. Results . We find that TOI-4515 b orbits a 1.2 Gyr-old G-star, has an orbital period of P b = 15.266446 ± 0.000013 days, a mass of M b = 2.01 ± 0.05 M J , and a radius of R b = 1.09 ± 0.04 R J . We also find an eccentricity of e = 0.46 ± 0.01, placing this planet among the WJs with highly eccentric orbits. As no additional companion has been detected, this high eccentricity might be the consequence of past violent scattering events.
The detection and characterization of exoplanets and brown dwarfs (BDs) around massive AF-type stars is essential to investigate and constrain the impact of stellar mass on planet properties. ...However, such targets are still poorly explored in radial velocity (RV) surveys because they only feature a small number of stellar lines and those are usually broadened and blended by stellar rotation as well as stellar jitter. As a result, the available information about the formation and evolution of planets and BDs around hot stars is limited. We aim to increase the sample and precisely measure the masses and eccentricities of giant planets and BDs transiting AF-type stars detected by the Transiting Exoplanet Survey Satellite (TESS). We followed bright (V < 12 mag) stars with \(T_{\mathrm{eff}}\) > 6200 K that host giant companions (R > 7 \(\mathrm{R_{\rm \oplus}}\)) using ground-based photometric observations as well as high precision RV measurements from the CORALIE, CHIRON, TRES, FEROS, and MINERVA-Australis spectrographs. In the context, we present the discovery of three BD companions, TOI-629b, TOI-1982b, and TOI-2543b, and one massive planet, TOI-1107b. From the joint analysis we find the BDs have masses between 66 and 68 \(\mathrm{M_{\rm Jup}}\), periods between 7.54 and 17.17 days, and radii between 0.95 and 1.11 \(\mathrm{R_{\rm Jup}}\). The hot Jupiter TOI-1107b has an orbital period of 4.08 days, a radius of 1.30 \(\mathrm{R_{\rm Jup}}\), and a mass of 3.35 \(\mathrm{M_{\rm Jup}}\). As a by-product of this program, we identified four low-mass eclipsing components (TOI-288b, TOI-446b, TOI-478b, and TOI-764b). Both TOI-1107b and TOI-1982b present an anomalously inflated radius with respect to the age of these systems. TOI-629 is among the hottest stars with a known transiting brown dwarf. TOI-629b and TOI-1982b are among the most eccentric brown dwarfs.
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