ABSTRACT
We analysed 68 candidate planetary systems first identified during Campaigns 5 and 6 (C5 and C6) of the NASA K2 mission. We set out to validate these systems by using a suite of follow-up ...observations, including adaptive optics, speckle imaging, and reconnaissance spectroscopy. The overlap between C5 with C16 and C18, and C6 with C17, yields light curves with long baselines that allow us to measure the transit ephemeris very precisely, revisit single transit candidates identified in earlier campaigns, and search for additional transiting planets with longer periods not detectable in previous works. Using vespa, we compute false positive probabilities of less than 1 per cent for 37 candidates orbiting 29 unique host stars and hence statistically validate them as planets. These planets have a typical size of 2.2 R⊕ and orbital periods between 1.99 and 52.71 d. We highlight interesting systems including a sub-Neptune with the longest period detected by K2, sub-Saturns around F stars, several multiplanetary systems in a variety of architectures. These results show that a wealth of planetary systems still remains in the K2 data, some of which can be validated using minimal follow-up observations and taking advantage of analyses presented in previous catalogues.
We report the discovery and characterisation of a super-Earth and a sub-Neptune transiting the bright (
K
= 8.8), quiet, and nearby (37 pc) M3V dwarf TOI-1266. We validate the planetary nature of ...TOI-1266 b and c using four sectors of TESS photometry and data from the newly-commissioned 1-m SAINT-EX telescope located in San Pedro Mártir (México). We also include additional ground-based follow-up photometry as well as high-resolution spectroscopy and high-angular imaging observations. The inner, larger planet has a radius of
R
= 2.37
−0.12
+0.16
R
⊕
and an orbital period of 10.9 days. The outer, smaller planet has a radius of
R
= 1.56
−0.13
+0.15
R
⊕
on an 18.8-day orbit. The data are found to be consistent with circular, co-planar and stable orbits that are weakly influenced by the 2:1 mean motion resonance. Our TTV analysis of the combined dataset enables model-independent constraints on the masses and eccentricities of the planets. We find planetary masses of
M
p
= 13.5
−9.0
+11.0
M
⊕
(<36.8
M
⊕
at 2-
σ
) for TOI-1266 b and 2.2
−1.5
+2.0
M
⊕
(<5.7
M
⊕
at 2-
σ
) for TOI-1266 c. We find small but non-zero orbital eccentricities of 0.09
−0.05
+0.06
(<0.21 at 2-
σ
) for TOI-1266 b and 0.04 ± 0.03 (< 0.10 at 2-
σ
) for TOI-1266 c. The equilibrium temperatures of both planets are of 413 ± 20 and 344 ± 16 K, respectively, assuming a null Bond albedo and uniform heat redistribution from the day-side to the night-side hemisphere. The host brightness and negligible activity combined with the planetary system architecture and favourable planet-to-star radii ratios makes TOI-1266 an exquisite system for a detailed characterisation.
Multiple nodules on the scrotal wall Giacalone, S.; Genovese, G.; Cusini, M.
Clinical and experimental dermatology,
December 2021, Letnik:
46, Številka:
8
Journal Article
Recenzirano
Odprti dostop
Click https://wileyhealthlearning.com/#/online-courses/524c0ff4-4240-4ed9-a57f-c7a4eb6fe0fc for the corresponding questions to this CME article.
Context.
Large sub-Neptunes are uncommon around the coolest stars in the Galaxy and are rarer still around those that are metal-poor. However, owing to the large planet-to-star radius ratio, these ...planets are highly suitable for atmospheric study via transmission spectroscopy in the infrared, such as with JWST.
Aims.
Here we report the discovery and validation of a sub-Neptune orbiting the thick-disk, mid-M dwarf star TOI-2406. The star’s low metallicity and the relatively large size and short period of the planet make TOI-2406 b an unusual outcome of planet formation, and its characterisation provides an important observational constraint for formation models.
Methods.
We first infer properties of the host star by analysing the star’s near-infrared spectrum, spectral energy distribution, and
Gaia
parallax. We use multi-band photometry to confirm that the transit event is on-target and achromatic, and we statistically validate the TESS signal as a transiting exoplanet. We then determine physical properties of the planet through global transit modelling of the TESS and ground-based time-series data.
Results.
We determine the host to be a metal-poor M4 V star, located at a distance of 56 pc, with properties
T
eff
= 3100 ± 75 K,
M
*
= 0.162 ± 0.008
M
⊙
,
R
*
= 0.202 ± 0.011
R
⊙
, and Fe∕H = −0.38 ± 0.07, and a member of the thick disk. The planet is a relatively large sub-Neptune for the M-dwarf planet population, with
R
p
= 2.94 ± 0.17
R
⊕
and
P
= 3.077 d, producing transits of 2% depth. We note the orbit has a non-zero eccentricity to 3
σ
, prompting questions about the dynamical history of the system.
Conclusions.
This system is an interesting outcome of planet formation and presents a benchmark for large-planet formation around metal-poor, low-mass stars. The system warrants further study, in particular radial velocity follow-up to determine the planet mass and constrain possible bound companions. Furthermore, TOI-2406 b is a good target for future atmospheric study through transmission spectroscopy. Although the planet’s mass remains to be constrained, we estimate the S/N using amass-radius relationship, ranking the system fifth in the population of large sub-Neptunes, with TOI-2406 b having a much lower equilibrium temperature than other spectroscopically accessible members of this population.
Uterine artery embolization is an attractive option for the management of postpartum haemorrhage, however it is not available in every hospital. We compared the clinical characteristics and ...haemodynamic state of patients with postpartum haemorrhage, before and after helicopter transfer to a tertiary hospital for possible uterine artery embolization. We also analysed whether the type of treatment could modify the outcome.
Between 1999 and 2019 in Switzerland, we retrospectively found 82 consecutive patients with postpartum haemorrhage who were transferred by a physician-staffed helicopter emergency medical service to the tertiary hospital for potential uterine artery embolization. The collected data included the type of delivery, estimated blood loss, shock index and blood lactate levels before transfer and at destination, uterine artery embolization rate and hospital mortality rate. Our primary outcome was to describe the clinical characteristics, outcomes and haemodynamic state of the patients with postpartum haemorrhage before and after helicopter transfer. Our secondary outcome was to report the treatments performed at the tertiary hospital. The collected data were analysed with Stata version 14 (Stata Corporation, College Station, TX, USA). Continuous data are compared by using the Student's t-test or the Mann-Whitney U test, as appropriate.
We included 69 patients. Postpartum haemorrhage occurred after vaginal delivery in 38 cases (55%). Blood loss prior to transfer exceeded 2 L in 34% of cases. The median shock index was 1 (IQR 0.8–1.1) before transfer and 0.9 (IQR 0.8–1.1) after transfer (p = 0.41). The median lactate level was 2.9 mmol/L (IQR 2.1–6.8) before, and 2.1 mmol/L (IQR 1.55–3.5) after transfer (p = 0.90). Forty-four patients underwent uterine artery embolization (64%), with an overall success rate of 93%. One patient died (1.4%), from a haemorrhagic shock of abdominal origin.
Interhospital helicopter transfer of patients with postpartum haemorrhage to a tertiary hospital seems to be safe in our setting, despite a significant proportion of patients exhibiting signs of haemodynamic instability. Decision criteria would be helpful to better guide choices regarding the transfer of patients with postpartum haemorrhage.
We present the discovery and characterization of a transiting sub-Neptune that orbits the nearby (28 pc) and bright (
V
= 8.37) K0V star HD 207897 (TOI-1611) with a 16.20-day period. This discovery ...is based on photometric measurements from the Transiting Exoplanet Survey Satellite mission and radial velocity (RV) observations from the SOPHIE, Automated Planet Finder, and HIRES high-precision spectrographs. We used EXOFASTv2 to model the parameters of the planet and its host star simultaneously, combining photometric and RV data to determine the planetary system parameters. We show that the planet has a radius of 2.50 ± 0.08
R
E
and a mass of either 14.4 ± 1.6
M
E
or 15.9 ± 1.6
M
E
with nearly equal probability. The two solutions correspond to two possibilities for the stellar activity period. The density accordingly is either 5.1 ± 0.7 g cm
−3
or 5.5
−0.7
+0.8
g cm
−3
, making it one of the relatively rare dense sub-Neptunes. The existence of this dense planet at only 0.12 AU from its host star is unusual in the currently observed sub-Neptune (2 <
R
E
< 4) population. The most likely scenario is that this planet has migrated to its current position.
La tamponnade cardiaque est une urgence vitale. Elle se définit comme une accumulation de liquide dans l’espace intrapéricardique, favorisant une augmentation de la pression intrapéricardique et une ...altération du remplissage cardiaque. Il s’agit d’une des causes du choc obstructif, et la rapidité d’installation détermine le degré d’instabilité hémodynamique. La morbidité et la mortalité dépendent de la rapidité du diagnostic et de sa prise en charge. Peu fréquemment, l’étiologie est tumorale. Ce type d’étiologie se traduit le plus souvent par des tableaux cliniques d’installation lente et progressive. C’est le cas du sujet qui est présenté dans cet article : un homme de 50 ans sans suivi médical et consommateur d’alcool et de tabac, vivant dans un contexte social difficile. L’issue fatale du cas clinique témoigne de la gravité du tableau de présentation initiale. L’électrocardiogramme peut révéler des signes caractéristiques comme le microvoltage du QRS et l’alternance électrique. La méthode standard pour détecter un épanchement péricardique est l’échocardiographie : le diagnostic de tamponnade cardiaque requiert la présence de collapsus complet du coeur droit et dans les cas plus graves des cavités gauches. Les compétences de l’urgentiste en termes d’échographie permettent un diagnostic plus rapide et précis. Le traitement de la tamponnade cardiaque repose principalement sur le soutien hémodynamique (administration volumique et traitement des éventuels troubles du rythme secondaires) en urgence. Cependant, le traitement définitif reste le drainage du liquide accumulé par péricardiocentèse ou par approche chirurgicale.
Cardiac tamponade is a life-threatening emergency. It is defined as an accumulation of fluid in the pericardial space, causing an increase in intra-pericardial pressure and impairing cardiac filling. This is one of the causes of obstructive shock, and the rapidity of onset determines the degree of hemodynamic instability. Morbidity and mortality depend on the quickness of the diagnosis and its management. The etiology is rarely neoplastic; if this is the case, the clinical presentation translates in a slow and progressive installation. A 50-year old man without any medical followup and an alcohol and tobacco addiction, from a difficult social background, has inspired our case report. The fatal outcome reflects hence the severity of the initial presentation. Electrocardiogram can reveal characteristic signs such as QRS microvoltage and electrical alternation. The standard method for detecting pericardial effusion is echocardiography, where the diagnosis of tamponade requires the presence of complete collapses of the right heart and, in more severe cases, of the left cavities. The skills of the emergency doctor in terms of ultrasound allow a faster and more accurate diagnosis. The emergency treatment of cardiac tamponade relies on hemodynamic support (volume administration and treatment of possible secondary rhythm disorders). However, the definitive treatment remains drainage of the extra-pericardial fluid by pericardiocentesis or a surgical approach.
Our argument is that in the XXI century resistance and cooperation formed the central axis of relations among Latin American regional agreements and helped promote an interactive game among them. ...Though threats posed by the international system exerted influence on the game, this article looks at how peripheral nations in Latin America reacted to actions of other peripheral nations in the same region rather than to actions of central powers. We identify the main factors behind neighboring nations' resistance to different regional agreements, place them in an interactive study of Latin American regionalism (2000-2018), and discuss how decisions taken in a regional agreement influence other regional actors' future decisions, combining game theory and discourse analysis. The article contributes supporting arguments to the literature that stresses actorness (agency) by developing nations.
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