Context.
Due to their scarcity, microlensing events in the Galactic disk are of great interest and high-cadence photometric observations, supplemented by spectroscopic follow-up, are necessary for ...constraining the physical parameters of the lensing system. In particular, a precise estimate of the source characteristics is required to accurately measure the lens distance and mass.
Aims.
We conducted a spectroscopic follow-up of microlensing event Gaia19bld to derive the properties of the microlensing source and, ultimately, to estimate the mass and distance of the lens.
Methods.
We obtained low- and high-resolution spectroscopy from multiple sites around the world during the course of the event. The spectral lines and template matching analysis has led to two independent, consistent characterizations of the source.
Results.
We found that the source is a red giant located at ~8.5 kpc from the Earth. Combining our results with the photometric analysis has led to a lens mass of
M
l
~ 1.1
M
⊙
at a distance of
D
l
~ 5.5 kpc. We did not find any significant blend light in the spectra (with an upper detection limit of
V
≤ 17 mag), which is in agreement with photometric observations. Therefore, we cannot exclude the possibility that the lens is a main-sequence star. Indeed, we predict in this scenario a lens brightness of
V
~ 20 mag, a value that would make it much fainter than the detection limit.
Purpose
It is important for the surgeon to determine the position of the CI electrode array during and after its placement within the cochlea. Most preferably, this should be within the scala tympani ...to obtain the best audiological outcome. Thus, misplacement into the scala vestibuli or tip fold-over should be prevented. Since there are different ways to ensure proper positioning of the electrode array within the scala tympani (e.g., intraoperative radiography, electrophysiological recordings), our study was aimed at detecting intraoperative electrophysiologic characteristics to better understand the mechanisms of those electrode tip fold-overs.
Material and methods
In a multi-centric, retrospective case–control series, patients with a postoperatively by radiography detected tip fold-over in perimodiolar electrodes were included. The point of fold-over (i.e., the electrode position) was determined and the intraoperative Auto-NRT recordings were analysed and evaluated.
Results
Four patients were found to have an electrode tip fold-over (out of 85 implantees). Significant changes of the Auto-NRT recordings were not detected. All tip fold-overs occurred in the most apical part of the electrodes.
Discussion
Cochlear implantation for hearing impaired patients plays a decisive role in modern auditory rehabilitation. Perimodiolar electrode arrays may fold over during the insertion and, hence, could have a negative impact on audiological outcome. Characteristic electrophysiologic changes to possibly predict this were not found in our series.
Abstract
We report the discovery of one super-Earth- (TOI-1749b) and two sub-Neptune-sized planets (TOI-1749c and TOI-1749d) transiting an early M dwarf at a distance of 100 pc, which were first ...identified as planetary candidates using data from the TESS photometric survey. We have followed up this system from the ground by means of multiband transit photometry, adaptive optics imaging, and low-resolution spectroscopy, from which we have validated the planetary nature of the candidates. We find that TOI-1749b, c, and d have orbital periods of 2.39, 4.49, and 9.05 days, and radii of 1.4, 2.1, and 2.5
R
⊕
, respectively. We also place 95% confidence upper limits on the masses of 57, 14, and 15
M
⊕
for TOI-1749b, c, and d, respectively, from transit timing variations. The periods, sizes, and tentative masses of these planets are in line with a scenario in which all three planets initially had a hydrogen envelope on top of a rocky core, and only the envelope of the innermost planet has been stripped away by photoevaporation and/or core-powered mass-loss mechanisms. These planets are similar to other planetary trios found around M dwarfs, such as TOI-175b,c,d and TOI-270b,c,d, in the sense that the outer pair has a period ratio within 1% of 2. Such a characteristic orbital configuration, in which an additional planet is located interior to a near 2:1 period-ratio pair, is relatively rare around FGK dwarfs.
Abstract
We report the discovery and characterization of seven transiting exoplanets from the HATNet survey. The planets, which are hot Jupiters and Saturns transiting bright Sun-like stars, include: ...HAT-P-58b (with mass
M
p
= 0.37
M
J
, radius
R
p
= 1.33
R
J
, and orbital period
P
= 4.0138 days), HAT-P-59b (
M
p
= 1.54
M
J
,
R
p
= 1.12
R
J
,
P
= 4.1420 days), HAT-P-60b (
M
p
= 0.57
M
J
,
R
p
= 1.63
R
J
,
P
= 4.7948 days), HAT-P-61b (
M
p
= 1.06
M
J
,
R
p
= 0.90
R
J
,
P
= 1.9023 days), HAT-P-62b (
M
p
= 0.76
M
J
,
R
p
= 1.07
R
J
,
P
= 2.6453 days), HAT-P-63b (
M
p
= 0.61
M
J
,
R
p
= 1.12
R
J
,
P
= 3.3777 days), and HAT-P-64b (
M
p
= 0.58
M
J
,
R
p
= 1.70
R
J
,
P
= 4.0072 days). The typical errors on these quantities are 0.06
M
J
, 0.03
R
J
, and 0.2 s, respectively. We also provide accurate stellar parameters for each of the host stars. With
V
= 9.710 ± 0.050 mag, HAT-P-60 is an especially bright transiting planet host, and an excellent target for additional follow-up observations. With
R
p
= 1.703 ± 0.070
R
J
, HAT-P-64b is a highly inflated hot Jupiter around a star nearing the end of its main-sequence lifetime, and is among the largest known planets. Five of the seven systems have long-cadence observations by TESS which are included in the analysis. Of particular note is HAT-P-59 (TOI-1826.01) which is within the northern continuous viewing zone of the TESS mission, and HAT-P-60, which is the TESS candidate TOI-1580.01.
We present near-infrared light curves of supernova (SN) 2011fe in M101, including 34 epochs in H band starting 14 days before maximum brightness in the B band. The light curve data were obtained with ...the WIYN High-Resolution Infrared Camera. When the data are calibrated using templates of other Type Ia SNe, we derive an apparent H-band magnitude at the epoch of B-band maximum of 10.85 + or - 0.04. This implies a distance modulus for M101 that ranges from 28.86 to 29.17 mag, depending on which absolute calibration for Type Ia SNe is used.
Although modern cochlear implants (CIs) are approved for magnetic resonance imaging (MRIs) adverse events still occur with unacceptable frequency. Methods: In this retrospective study, magnet ...displacement due to MRIs was analysed. Relevant factors e.g. symptoms during MRI, diagnostics, surgical intervention following the diagnosis and possible subsequent damage were assessed.
16 patients were enclosed. All patients complained about pain while the scan was conducted. Computed tomography (CT) scans of the temporal bone or X-rays of the skull were performed to confirm diagnosis. Artefacts on CT scans delayed immediate diagnosis in some cases.
Despite various studies demonstrating the range of adverse events related to CIs following MRI, little information is available on diagnosis and radiologic recognition of magnet dislocation. In patients complaining about pain following an MRI scan an X-ray of the head should be performed immediately. Most adverse events occur in radiological centres without expertise in cochlear implants.
Comprehensive training of patients, surgeons and radiologists is the most efficient tool to prevent damage to the CI and the patient. X-ray of the skull is suggested to be used as the method of choice in imaging.
After cochlear implantation (CI), long-term follow-up is obligatory. Remote-care options which provide a standard of care comparable to in-person consultations, could be an attractive addition to a ...cochlear implant centre's portfolio. The aim of this study was to evaluate the accuracy of photographs of the skin covering the implant to reliably detect skin irritations or soft tissue complications.
During routine follow-up consultations, 109 CI patients were examined in person and asked to take a photograph of the skin covering the implant using their smartphones. Photographs were digitally and remotely evaluated by two CI physicians who were blinded to the findings during the in-person examination.
In nine cases, skin abnormalities were detected by the CI physician upon in-person examination, seven of which required immediate treatment. Both digital evaluators reliably detected all treatment-requiring conditions. Overall, more skin irritations were suspected digitally compared to in-person examination. Without additional information from the patients' medical record, sensitivity was 100% and specificity was 63%; with additional information provided, sensitivity was 100%, and specificity increased to 65.3%.
Digital photographic assessment of the skin covering the implant is a highly sensitive method to detect skin irritations and could reduce the number of necessary in-person consultations.
To examine radiation-doses imparted during multislice (MSCT) and cone-beam computed-tomography (CBCT) for perioperative examination of cochlear-implant insertion.
Radiation-doses were assessed during ...standardized petrous-bone CT-protocols at different MSCT ((I) single-source CT-scanner Somatom-Definition-AS+, (II) 2nd generation of dual-source CT-scanner Somatom-Definition-Flash, (III) 3rd generation of dual-source CT-scanner Somatom-Force and at the CBCT Ziehm-Vision-RFD3D ((IV) (a) RFD-3D (Standard-modifier), (b) RFD-3D (Low-dose-modifier)). Image quality was examined by two radiologists appraising electrode-array placement, quality-control of cochlear-implant surgery and complications based on real patients' examinations (n=78).
In MSCT-setting following radiation-doses were assessed (CTDIw; DLP): (I) 21.5mGy; 216mGycm; (II) 19.7mGy; 195mGycm; (III) 12.7mGy; 127mGycm; in the CBCT setting radiation doses were distributed as follows: (IV) (a) 1.9mGy; 19.4mGycm; (b) 1.2mGy; 12.9mGycm. Overall, image quality was evaluated as good for both, MSCT- and CBCT-examinations, with a good interrater reliability (r=0.81).
CBCT bears considerable dose-saving potential for the perioperative examination of cochlear-implant insertion while maintaining adequate image quality.
We investigate the star cluster population in the outer parts of the starburst galaxy NGC 5253 using archive images taken with the Hubble Space Telescope's Advanced Camera for Surveys. Based on the ...F415W, F555W and F814W photometry ages and masses are estimated for bona fide star cluster candidates. We find three potentially massive (≥105 M⊙) star clusters at ages of the order of 1-2 Gyr, implying, if confirmed, a high global star formation rate in NGC 5253 during that epoch. This result underlines earlier findings that the current starburst is just one episode in a very active dwarf galaxy.
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