Context. 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 that are between Earth and Neptune in size, the most abundant type of planet orbiting Sun-like stars with periods of less than a few years. Aims. Among many other K2 candidates, we discovered a multi-planetary system around EPIC 246471491, referred to henceforth as K2-285, which contains four planets, ranging in size from twice the size of Earth to nearly the size of Neptune. We aim here at confirming their planetary nature and characterizing the properties of this system. Methods. We measure the mass of the planets of the K2-285 system by means of precise radial-velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. Results. 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. Conclusions. We find that K2-285b has a mass of Mb = 9.68−1.37+1.21 $9.68 _{ - 1.37 } ^ { + 1.21 } $ 9.68−1.37+1.21 M⊕ and a radius of Rb = 2.59−0.06+0.06 R⊕ $2.59 _{ - 0.06 } ^ { + 0.06 }\,R_{\oplus}$2.59−0.06+0.06 R⊕ , yielding a mean density of ρb = 3.07−0.45+0.45 g cm−3 $\rho_{\mathrm{b}}{\,=\,}3.07_{-0.45}^{+0.45}\,\textrm{g}\,\textrm{cm}^{-3}$ρb = 3.07−0.45+0.45 g cm−3 , while K2-285c has a mass of Mc = 15.68−2.13+2.28 M⊕ $15.68 _{ - 2.13 } ^ { + 2.28 }\,M_{\oplus}$15.68−2.13+2.28 M⊕ , radius of Rc = 3.53−0.08+0.08 R⊕ $3.53 _{ - 0.08 } ^ { + 0.08 }\,R_{\oplus}$3.53−0.08+0.08 R⊕ , and a mean density of ρc = 1.95−0.28+0.32 g cm−3 $\rho_{\mathrm{c}}{\,=\,}1.95_{-0.28}^{+0.32}\,\textrm{g}\,\textrm{cm}^{-3}$ρc = 1.95−0.28+0.32 g cm−3 . For K2-285d (Rd = 2.48−0.06+0.06 R⊕ $2.48 _{ - 0.06 } ^ { + 0.06 }\,R_{\oplus}$2.48−0.06+0.06 R⊕ ) and K2-285e (Re = 1.95−0.05+0.05 R⊕ $1.95 _{ - 0.05 } ^ { + 0.05 }\,R_{\oplus}$1.95−0.05+0.05 R⊕ ), the upper limits for the masses are 6.5 M⊕ and 10.7 M⊕, respectively. The system is thus composed of an (almost) 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 would provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories.
We present the discovery and characterization of a new transiting planet from Campaign 17 of the Kepler extended mission K2. The planet K2-292 b is a warm sub-Neptune on a 17 day orbit around a ...bright (V = 9.9 mag) solar-like G3 V star with a mass and radius of M⋆ = 1.00 ± 0.03 M⊙ and R⋆ = 1.09 ± 0.03 R⊙, respectively. We modeled simultaneously the K2 photometry and CARMENES spectroscopic data and derived a radius of Rp=2.63−0.10+0.12 R⊕ $R_{\mathrm{p}} = 2.63_{-0.10}^{+0.12}\,{R_{\oplus}}$ Rp=2.63−0.10+0.12 R⊕ and mass of Mp=24.5−4.4+4.4 M⊕ $M_{\mathrm{p}} = 24.5_{-4.4}^{+4.4}\,{M_{\oplus}}$Mp=24.5−4.4+4.4 M⊕ , yielding a mean density of ρp=7.4−1.5+1.6 g cm−3 $\rho_{\mathrm{p}} = 7.4_{-1.5}^{+1.6}\,\mathrm{g\,cm^{-3}}$ρp=7.4−1.5+1.6 g cm−3 , which makes it one of the densest sub-Neptunian planets known to date. We also detected a linear trend in the radial velocities of K2-292 ( γ˙RV = −0.40−0.07+0.07 m s−1 d−1 $\dot{\gamma}_{\textrm{RV}}= -0.40^{+0.07}_{-0.07}\,\mathrm{m\,s^{-1}\,d^{-1}}$γ˙RV=−0.40−0.07+0.07 m s−1 d−1 ) that suggests a long-period companion with a minimum mass on the order of 33 M⊕. If confirmed, it would support a formation scenario of K2-292 b by migration caused by Kozai-Lidov oscillations.
We report the detection of a transiting Earth-size planet around GJ 357, a nearby M2.5 V star, using data from the Transiting Exoplanet Survey Satellite (TESS). GJ 357 b (TOI-562.01) is a transiting, ...hot, Earth-sized planet (Teq = 525 ± 11 K) with a radius of Rb = 1.217 ± 0.084 R⊕ and an orbital period of Pb = 3.93 d. Precise stellar radial velocities from CARMENES and PFS, as well as archival data from HIRES, UVES, and HARPS also display a 3.93-day periodicity, confirming the planetary nature and leading to a planetary mass of Mb = 1.84 ± 0.31 M⊕. In addition to the radial velocity signal for GJ 357 b, more periodicities are present in the data indicating the presence of two further planets in the system: GJ 357 c, with a minimum mass of Mc = 3.40 ± 0.46 M⊕ in a 9.12 d orbit, and GJ 357 d, with a minimum mass of Md = 6.1 ± 1.0 M⊕ in a 55.7 d orbit inside the habitable zone. The host is relatively inactive and exhibits a photometric rotation period of Prot = 78 ± 2 d. GJ 357 b isto date the second closest transiting planet to the Sun, making it a prime target for further investigations such as transmission spectroscopy. Therefore, GJ 357 b represents one of the best terrestrial planets suitable for atmospheric characterization with the upcoming JWST and ground-based ELTs.
Los trabajos sobre la Prehistoria de la comarca de La Janda (provincia de Cádiz) fueron realizados a principios de siglo desde el Historicismo Cultural. En la presente década nuestro grupo ha llevado ...a cabo prospecciones arqueológicas sistemáticas y excavaciones de urgencia, con el fin de conformar el proceso histórico de las sociedades cazadoras-recolectoras, tribales y clasistas iniciales, que habitaron la Banda Atlántica de Cádiz. La aplicación de técnicas geoarqueológicas al estudio de los productos arqueológicos y el análisis mineralógico y petrológico, tanto de las materias primas utilizadas como de los materiales geológicos, permiten vislumbrar interesantes aspectos sobre el proceso histórico y económico de dichas formaciones sociales.
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⋆ = 1.05 ± 0.05 M☉, R⋆ = ...1.71 ± 0.04 R☉, Teff = 5430 ± 85 K). The star is just leaving the main sequence. We combined K2 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+0.0007days, a mass of 8.75-1.08+1.09 M⊕, and a radius of 1.95-0.08+0.09 R⊕, the inner planet b is compatible with nickel-iron core and a silicate mantle (ρb = 6.39-1.04+1.19 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 14.67-1.89+1,84 M⊕ and 3.67-0.14+0.17 R⊕ and 10.18-2.42+2.46 M⊕ and 3.94-0.12+0.13 R⊕, respectively, yielding a mean density of 1.62-0.29+0.30 and 0.91-0.23+0.25 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.
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⋆ = 0.379 ± 0.016M⊙ and a radius of R⋆ = 0.382 ± 0.012R⊙. The ultra-short-period planet LTT 3780 b (P(b) = 0.77 d) with a radius of 1.35(−0.06,+0.06) R⊕, a mass of 2.34(−0.23,+0.24) M⊕, and a bulk density of 5.24(−0.81,+0.94) g/cu.cm 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⊕, mass of 6.29(−0.61,+0.63) M⊕, and mean density of 2.45(−0.37,+0.44) g/cu.cm 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 (JWST).
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
⋆
= 1.05 ± 0.05
M
⊙
,
R
⋆
...= 1.71 ± 0.04
R
⊙
,
T
eff
= 5430 ± 85 K). The star is just leaving the main sequence. We combined K2 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
−1.08
+1.09
M
⊕
, and a radius of 1.95
−0.08
+0.09
R
⊕
, the inner planet b is compatible with nickel-iron core and a silicate mantle (
ρ
b
= 6.39
−1.04
+1.19
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
−1.89
+1,84
M
⊕
and 3.67
−0.14
+0.17
R
⊕
and 10.18
−2.42
+2.46
M
⊕
and 3.94
−0.12
+0.13
R
⊕
, respectively, yielding a mean density of 1.62
−0.29
+0.30
and 0.91
−0.23
+0.25
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.
Intellectual disability (ID) affects approximately 1% of the worldwide population and individuals with ID have a higher comorbidity with mental illness, and specifically psychotic disorders. ...Unfortunately, among individuals with ID, limited research has been conducted since ID individuals are usually excluded from mental illness epidemiological studies and clinical trials. Here we perform a clinical trial to investigate the effectiveness of clozapine in the treatment of resistant psychosis in individuals with ID. The article highlights the complexity of diagnosing and treating psychopathological alterations associated with ID and advocates for more rigorous research in this field.
A Phase IIB, open-label, randomized, multicenter clinical trial (NCT04529226) is currently ongoing to assess the efficacy of oral clozapine in individuals diagnosed with ID and suffering from treatment-resistant psychosis. We aim to recruit one-hundred and fourteen individuals (N=114) with ID and resistant psychosis, who will be randomized to TAU (
) and treatment-with-clozapine conditions. As secondary outcomes, changes in other clinical scales (PANSS and SANS) and the improvement in functionality, assessed through changes in the Euro-QoL-5D-5L were assessed. The main outcome variables will be analyzed using generalized linear mixed models (GLMM), assessing the effects of status variable (TAU vs. Clozapine), time, and the interaction between them.
The treatment of resistant psychosis among ID individuals must be directed by empirically supported research. CLOZAID clinical trial may provide relevant information about clinical guidelines to optimally treat adults with ID and treatment-resistant psychosis and the benefits and risks of an early use of clozapine in this underrepresented population in clinical trials.
Clinicaltrials.gov: NCT04529226. EudraCT: 2020-000091-37.
The goal of the study was to evaluate the use of parenteral nutrition formulas with standardized g. of nitrogen, carbohydrates and lipids, and to analyze whether the nutritional requirements of the ...patients treated in our hospital were covered by said formulas or whether it was necessary to change and/or standardize a new formula. To do so, a review was made of 5.646 parental nutrition mixtures prepared in the Pharmacy Service and patterned by the Nutrition Service from April, 1991, to May, 1992, for 308 adult patients. The distribution of the mixtures by services, diagnoses and the frequency of the different standard formulas were studied, comparing standard formula frequency with that of non-standard formulas. Findings showed that 41.9% of nutrition mixtures were patterned in surgery, and the most common diagnosis, cancer, appeared in 24%. Of the mixtures, 67.6% were preestablished formulas, and 32.4% were non-standard formulas. The order of frequency among standard formulas was: basic standard formulas, stress formulas, initial formulas, peripheral formulas, hemodialysis formulas and low-volume formulas. All covered the nutritional needs of a large share of the patients for the different pathologies in which they were indicated. Nevertheless the question of designing a new formula to cover a greater number of situations was raised. Protocolization should take place rationally, to meet the hospital's most frequent pathologies, and effectiveness should be evaluated after tracking and checking each patient.
BackgroundClinical practice guidelines recommend the use of the new oral anticoagulants (NOACs) in patients with non-valvular atrial fibrillation (AF) as a strategy before and after cardioversion, ...which is very common in the Emergency Department. A dispensing procedure from the pharmacy service was established in such cases.PurposeTo analyse compliance of the established procedure in the prescription and dispensation of NACOs, as well as to follow-up on safety.Material and methodsRetrospective study conducted from July to September 2015. We evaluated all of the prescriptions and dispensations of NACOs within the procedure. In all cases an appointment with cardiology had to be programmed to value the continuity of treatment and/or cardioversion. We collected the cause and appropriateness of prescription, NOAC prescribed, dispensation and citation with cardiology, and continuity of the treatment by the cardiologist. Mistakes and improvement areas were identified.ResultsThe procedure was applied in 15 patients (80% women, average age 72.6 ± 9.8 years). Patients distribution was: 26.7% AF of <48 h and high thrombosis risk (cardioversion in emergency department and dispensation for 4 weeks), 53.3% AF of >48 h and low risk (cardioversion programmed in cardiology and dispensation pre and post-cardioversión) and 20% AF >48 h and high risk (dispensing for 4 weeks until review by the cardiologist).The most prescribed NOAC was rivaroxaban (73.3%) followed by apixaban (20%) and dabigatran (6.7%). In all cases the prescription was well indicated according to the procedure. However, dispensation adequacy was 73.3%. In four cases (26%) the cardiology consultation was programmed exceeding the time covered by the dispensation. A prescription error due to underdosing was identified. Only in one case was scheduled cardioversion performed according to the procedure provided for (the rest reverted to sinus rhythm spontaneously). NOAC prescription was maintained by the cardiologist in 5 cases andmodified to acenocumarol in 3 cases.ConclusionAlthough the procedure was followed by the emergency physician, this study reveals the need to improve the coordination between emergency and cardiology services to avoid delays, with the resultingrisk of under treatment, as well as to ensure the correct cardioversion programming.The availability of medication by pharmacy must also be improved. As the most prescribed anticoagulant was rivaroxaban, it seems advisable to restrict the procedure to this NACO to facilitate its knowledge and management, avoiding errors of prescription.No conflict of interest.
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