Abstract
Background
The variation of right main stem bronchus leads to the orifice of the right upper lobe bronchus may be obstructed or increase the incidence of malposition intraoperatively when ...the right sided double-lumen tube is used. Therefore, the aim of this study was to compare the accuracy of three methods measured the length of the right main stem bronchus via chest computed tomography as a guide to the use of right sided double-lumen tube.
Methods
In this study, 168 adult patients undergoing left sided thoracic surgery were included. All these patients were allocated to carina-proximal (C-P) group, carina-distal (C-D) group and carina-carina (C-C) group. The position of endobronchial cuff observed via Fiberoptic bronchoscopy after successful initial placement and after turning the patients to the lateral decubitus position, as well as the incidence of malposition of right sided double-lumen tube intraoperative were recorded to assess the accuracy of three methods in predicting the position of right sided double-lumen tube.
Results
The distance between the carina to the proximal margin of the right upper lobe orifice, carina to the distal margin of the right upper lobe orifice and carina to the first right interlobar carina of the right upper lobe orifice were 17.2 ± 2.3 mm, 25.4 ± 3.7 mm and 28.5 ± 3.1 mm (
P
< 0.05). In the C-D group, the number of endobronchial cuffs seen to be herniating out of the carina, the number of bronchoscopies during initial placement and on the lateral position, the number of total malposition intraoperative and the number of reposition manoeuvres intraoperative were significantly less than the C-P group or the C-C group (
P
< 0.05).
Conclusions
The length of the right main stem bronchus measured by the carina to distal margin of right upper lobe orifice method was more accurate than the other two methods in guiding the use of right sided double-lumen tube.
Trials registration
Clinical Trials. gov. no. NCT04127903. Registered at
https://register.clinicaltrials.gov
on 16/10/2019.
Abstract
We present Magellan/IMACS, Anglo-Australian Telescope/AAOmega+2dF, and Very Large Telescope/GIRAFFE+FLAMES spectroscopy of the Carina II (Car II) and Carina III (Car III) dwarf galaxy ...candidates, recently discovered in the Magellanic Satellites Survey (MagLiteS). We identify 18 member stars in Car II, including two binaries with variable radial velocities and two RR Lyrae stars. The other 14 members have a mean heliocentric velocity
and a velocity dispersion of
. Assuming Car II is in dynamical equilibrium, we derive a total mass within the half-light radius of
, indicating a mass-to-light ratio of
/
. From equivalent width measurements of the calcium triplet lines of nine red giant branch (RGB) stars, we derive a mean metallicity of
with dispersion
. Considering both the kinematic and chemical properties, we conclude that Car II is a dark-matter-dominated dwarf galaxy. For Car III, we identify four member stars, from which we calculate a systemic velocity of
. The brightest RGB member of Car III has a metallicity of
. Due to the small size of the Car III spectroscopic sample, we cannot conclusively determine its nature. Although these two systems have the smallest known physical separation (
) among Local Group satellites, the large difference in their systemic velocities,
, indicates that they are unlikely to be a bound pair. One or both systems are likely associated with the Large Magellanic Cloud (LMC), and may remain LMC satellites today. No statistically significant excess of
γ
-ray emission is found at the locations of Car II and Car III in eight years of
Fermi
-LAT data.
Abstract Surgical treatment of carinal tumors that extend into the lobar bronchus is a procedure that challenges thoracic surgeons. There is no consensus on the suitable technique for a safe ...anastomosis in lobar lung resection with carina. The preferred Barclay technique has a high rate of anastomosis-related complications. Although a lobe-sparing end-to-end anastomosis technique has been previously described, the double-barrel method can be applied as an alternative technique. We present a case where we performed double-barrel anastomosis and neo-carina formation after tracheal sleeve right upper lobectomy.
Abstract
WISE J080822.18–644357.3 (WISE J0808–6443) was recently identified as a new M dwarf debris disc system and a candidate member of the 45 Myr-old Carina association. Given that the strength of ...its infrared excess (LIR/L⋆ ≃ 0.1) appears to be more consistent with a young protoplanetary disc, we present the first optical spectra of the star and reassess its evolutionary and membership status. We find WISE J0808−6443 to be a Li-rich M5 star with strong H α emission (−125 < EW < −65 Å over 4 epochs) whose strength and broad width are consistent with accretion at a low level (∼10−10 M⊙ yr−1) from its disc. The spectral energy distribution of the star is consistent with a primordial disc and is well-fitted using a two-temperature blackbody model with Tinner ≃ 1100 K and Touter ≃ 240 K. AllWISE multi-epoch photometry shows the system exhibits significant variability in the 3.4 and 4.6 $\mu$m bands. We calculate an improved proper motion based on archival astrometry, and combined with a new radial velocity, the kinematics of the star are consistent with membership in Carina at a kinematic distance of 90 ± 9 pc. The spectroscopic and photometric data are consistent with WISE J0808−6443 being a ∼0.1 M⊙ Classical T-Tauri star and one of the oldest known accreting M-type stars. These results provide further evidence that the upper limit on the lifetimes of gas-rich discs – and hence the time-scales to form and evolve protoplanetary systems – around the lowest mass stars may be longer than previously recognized, or some mechanism may be responsible for regenerating short-lived discs at later stages of pre-main sequence evolution.
We present Magellan/IMACS, Anglo-Australian Telescope/AAOmega+2dF, and Very Large Telescope/GIRAFFE+FLAMES spectroscopy of the Carina II (Car II) and Carina III (Car III) dwarf galaxy candidates, ...recently discovered in the Magellanic Satellites Survey (MagLiteS). We identify 18 member stars in Car II, including two binaries with variable radial velocities and two RR Lyrae stars. The other 14 members have a mean heliocentric velocity and a velocity dispersion of . Assuming Car II is in dynamical equilibrium, we derive a total mass within the half-light radius of , indicating a mass-to-light ratio of / . From equivalent width measurements of the calcium triplet lines of nine red giant branch (RGB) stars, we derive a mean metallicity of with dispersion . Considering both the kinematic and chemical properties, we conclude that Car II is a dark-matter-dominated dwarf galaxy. For Car III, we identify four member stars, from which we calculate a systemic velocity of . The brightest RGB member of Car III has a metallicity of . Due to the small size of the Car III spectroscopic sample, we cannot conclusively determine its nature. Although these two systems have the smallest known physical separation ( ) among Local Group satellites, the large difference in their systemic velocities, , indicates that they are unlikely to be a bound pair. One or both systems are likely associated with the Large Magellanic Cloud (LMC), and may remain LMC satellites today. No statistically significant excess of γ-ray emission is found at the locations of Car II and Car III in eight years of Fermi-LAT data.
ABSTRACT
The key empirical property of the X-ray emission from O stars is a strong
correlation between the bolometric and X-ray luminosities. In the framework of
the
Chandra
Carina Complex Project, ...129 O and B stars have been
detected as X-ray sources; 78 of those, all with spectral type earlier than B3,
have enough counts for at least a rough X-ray spectral characterization. This
leads to an estimate of the
L
X
–
L
BOL
ratio for an
exceptional number of 60 O stars belonging to the same region and triples the
number of Carina massive stars studied spectroscopically in X-rays. The derived
log(
L
X
/
L
BOL
) is
−7.26 for single objects, with a dispersion of only 0.21 dex. Using the
properties of hot massive stars listed in the literature, we compare the X-ray
luminosities of different types of objects. In the case of O stars, the
L
X
–
L
BOL
ratios are
similar for bright and faint objects, as well as for stars of different
luminosity classes or spectral types. Binaries appear only slightly harder and
slightly more luminous in X-rays than single objects; the differences are not
formally significant (at the 1% level), except for the
L
X
–
L
BOL
ratio in the
medium (1.0–2.5 keV) energy band. Weak-wind objects have similar X-ray
luminosities but they display slightly softer spectra compared with “normal” O
stars with the same bolometric luminosity. Discarding three overluminous
objects, we find a very shallow trend of harder emission in brighter objects.
The properties of the few B stars bright enough to yield some spectral
information appear to be different overall (constant X-ray luminosities, harder
spectra), hinting that another mechanism for producing X-rays, besides wind
shocks, might be at work. However, it must be stressed that the earliest and
X-ray brightest among these few detected objects are similar to the latest O
stars, suggesting a possibly smooth transition between the two processes.
VACTERL is a complicated syndrome with an unknown etiology where many studies have failed to identify the cause. In esophageal atresia (EA) roughly 10%–23% also have concurrent anomalies that align ...with VACTERL disorder. The aim of this study is to investigate if there is a difference regarding localization of the tracheoesophageal fistula between patients with VACTERL and non-VACTERL patients.
Retrospective chart review of newborn operated for esophageal atresia between 2006 and 2016 at our Institution was performed. Children with a C-type fistula according to Gross and reliable preoperative tracheoesophageal fistula to carina distance measurement at rigid tracheoscopy were included in the study.
A total of 90 patients were included in the study. Fifteen of those were diagnosed with VACTERL. Before and after adjusting for weight and gestational week patients with VACTERL had significantly shorter carina to fistula distance at perioperative rigid tracheoscopy (p = <0.001 nonadjusted, p = 0.016 adjusted).
Patients with VACTERL born with EA type C had shorter carina to fistula distance as shown at perioperative rigid tracheoscopy. The significantly shorter distance may not only present surgical difficulties but may also suggest a structural or molecular difference in the development of the esophageal atresia between the two groups.
III.
An Introduction to the Chandra Carina Complex Project Townsley, Leisa K; Broos, Patrick S; Corcoran, Michael F ...
The Astrophysical journal. Supplement series,
05/2011, Volume:
194, Issue:
1
Journal Article, Web Resource
Peer reviewed
Open access
The Great Nebula in Carina provides an exceptional view into the violent massive star formation and feedback that typifies giant H II regions and starburst galaxies. We have mapped the Carina ...star-forming complex in X-rays, using archival Chandra data and a mosaic of 20 new 60 ks pointings using the Chandra X-ray Observatory's Advanced CCD Imaging Spectrometer, as a testbed for understanding recent and ongoing star formation and to probe Carina's regions of bright diffuse X-ray emission. This study has yielded a catalog of properties of >14,000 X-ray point sources; >9800 of them have multiwavelength counterparts. Using Chandra's unsurpassed X-ray spatial resolution, we have separated these point sources from the extensive, spatially-complex diffuse emission that pervades the region; X-ray properties of this diffuse emission suggest that it traces feedback from Carina's massive stars. In this introductory paper, we motivate the survey design, describe the Chandra observations, and present some simple results, providing a foundation for the 15 papers that follow in this special issue and that present detailed catalogs, methods, and science results.
We present spectroscopic data for individual stars observed from 2004 March through 2008 August as part of our Michigan/MIKE Fiber System (MMFS) survey of four dwarf spheroidal (dSph) galaxies: ...Carina, Fornax, Sculptor, and Sextans. Using MMFS at the Magellan/Clay Telescope at Las Campanas Observatory, we have acquired 8855 spectra from 7103 red-giant candidates in these Galactic satellites. We list measurements of each star's line-of-sight velocity (median error ±2.1 km s -1) and spectral line indices for iron and magnesium absorption features. We use globular cluster spectra to calibrate the indices onto standard Fe/H metallicity scales, but comparison of the resulting metallicities with published values suggests that the MMFS indices are best used as indicators of relative, not absolute, metallicity. The empirical distributions of velocity and spectral indices also allow us to quantify the amount of contamination by foreground stars. In a companion paper, we develop an algorithm that evaluates the membership probability for each star, showing that the present MMFS sample contains more than 5000 dSph members, including 774 Carina members, 2483 Fornax members, 1365 Sculptor members, and 441 Sextans members.
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