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Observations have shown that the disk frequency and the fraction of accreting pre-main-sequence stars decrease with the age of the population and that some stars appear to have disks while their accretion has stopped. Still, it is unclear how disk-bearing stars stop their accretion. To provide insight into the last stages of accretion in low-mass young stars, we conducted a survey of disk-bearing stars that are thought to be non-accretors to identify stars still accreting at very low rates. Here we present the first catalog of the survey of 170 disk-bearing non-accreting stars in Chamaeleon I, Orion OB1, Upper Scorpius, γ Velorum, and Upper Centaurus–Lupus, using He i λ10830 as a sensitive probe of accretion. We classify the line profiles into six types and argue that those showing redshifted and/or blueshifted absorption are still accreting. Using these classifications, we found that, among disk-bearing stars previously classified as non-accretors, at least 20%–30% are still accreting, with a larger fraction of those at younger population ages. While the difference between the outer disk signature and accretion status is unclear, we found a difference between the inner disk excess and accretion status. There is no preference in the mass of the newly identified accretors, suggesting that the processes inhibiting accretion do not directly depend on mass in the typical mass range of T Tauri stars. Lastly, we found that at a low accretion level, the “Hα width at the 10% height” criterion mischaracterizes a larger fraction of accretors than the line’s equivalent width.

To determine if tangent visual fields gathered during assessment of superior visual field deficits caused by blepharoptosis and dermatochalasis offer good correlation to clinical exam in a time and cost efficient manner. Prospective, observational case series. Subjects included all patients referred to a single surgeon (CCN) who underwent surgical correction of blepharoptosis and/or dermatochalasis. Preoperatively and postoperatively, upper margin-to-reflex distances were assessed. Tangent visual fields were performed in a timed fashion and analyzed for degrees of intact vision in the vertical meridian and degrees squared of area under the curve. Data were compared by Student t-tests and Pearson correlation coefficients. Mean preoperative superior visual fields with the eyelid in the natural position measured 8° in the vertical meridian. Measurements in the vertical meridian and area under the curve showed excellent correlation (r = 0.87). Patients with ptosis showed strong correlation between margin-to-reflex distance and superior visual fields. Patients completed field testing faster than reported times for automated or Goldmann testing. Finally, tangent screens were the least expensive type of equipment to purchase. Tangent visual fields are a rapid and inexpensive way to test for functional loss of superior visual field in patients with upper eyelid malposition. Our data revealed potential differences between tangent screen results and published results for automated or Goldmann visual field testing which warrants further studies.

Purpose: Refractory periorbital dermatitis has a chronic course with exacerbations leading to discomfort and cosmetic issues, yet characterization of treatment options is limited. Aims: The objective was to present comprehensive demographic data and medical management of a series of patients with refractory periorbital dermatitis. Settings and Design: Retrospective review identified patients treated at a single institution from January 2010 to August 2020. Methods: Descriptive analyses were performed. Demographic data and treatment history were reviewed and data including medication, use, date of use and discontinued use, reason for discontinuation (if applicable), refractory status, formulation, concentration, and dose frequency were extracted. Statistical Analysis Used: Descriptive analyses. Results: Forty-five patients were included. The average age at first diagnosis was 60.3 years (sd 14.9). 82.2% were women and 84.4% identified as Caucasian. Triamcinolone cream was most frequently used followed by tobramycin-dexamethasone, tacrolimus, and neomycin-polymyxin-dexamethasone. Less than 30% of patients on triamcinolone were refractory. 13.3% of patients used topical hydrocortisone, with over 80% of these patients experiencing refractory episodes of persistent irritation and erythema. Most patients were refractory during initial use or the first recurrence of periorbital dermatitis flare. Conclusions: By better characterizing the diverse treatment regimens in a unique subset of refractory patients, we hope to better inform potential courses of medical management for periorbital dermatitis.

We present a spectroscopic analysis of T Tauri stars (TTSs) observed with the wide-field multifiber spectrograph LAMOST in the substellar associations Ori OB1a located in the Orion Star-forming Complex. Based on GAIA-DR3 data, we selected stars with proper motions and parallaxes expected for TTSs belonging to the young association. We perform a spectroscopic analysis to obtain the spectral types and measure the equivalent widths of Li i and Hα to confirm the youth of the stars and estimate the accretion status. We also estimate extinctions, masses, and ages for the studied sample. Out of 342 TTSs with spectroscopic and kinematic properties indicating their membership of the subassociation, 2 are reported here for the first time. Finally, we detect four stellar kinematic groups located at different distances, two in the north fields and two in the south field. These groups also show different proper motions. This suggests that the star-forming scenario in this region is more complex than the traditional spatial-temporal scenario, in which a generation of stars triggers the formation of a new spatially differentiated generation of stars.

Hot Jupiters are generally observed to lack close planetary companions, a trend that has been interpreted as evidence for high-eccentricity migration. We present the discovery and validation of WASP-132 c (TOI-822.02), a 1.85 ± 0.10 R ⊕ planet on a 1.01 day orbit interior to the hot Jupiter WASP-132 b. Transiting Exoplanet Survey Satellite and ground-based follow-up observations, in conjunction with vetting and validation analysis, enable us to rule out common astrophysical false positives and validate the observed transit signal produced by WASP-132 c as a planet. Running the validation tools vespa and TRICERATOPS on this signal yields false-positive probabilities of 9.02 × 10−5 and 0.0107, respectively. Analysis of archival CORALIE radial velocity data leads to a 3σ upper limit of 28.23 ms−1 on the amplitude of any 1.01 day signal, corresponding to a 3σ upper mass limit of 37.35 M ⊕. Dynamical simulations reveal that the system is stable within the 3σ uncertainties on the planetary and orbital parameters for timescales of ∼100 Myr. The existence of a planetary companion near the hot Jupiter WASP-132 b makes the giant planet’s formation and evolution via high-eccentricity migration highly unlikely. Being one of just a handful of nearby planetary companions to hot Jupiters, WASP-132 c carries with it significant implications for the formation of the system and hot Jupiters as a population.

Abstract Introduction: Maxillary ameloblastoma is a rare, slow-growing odontogenic tumor that can recur after surgical excision, be locally aggressive, and rarely develop systemic metastases. We describe the course and management of a patient with recurrent maxillary ameloblastoma with orbital invasion and systemic metastases, the fourth case of its kind to be described in the literature. Case Presentation: A 50-year-old female presented with left hyperglobus. A diagnosis of maxillary ameloblastoma was made based on biopsy and neuroimaging with MRI and CT. Surgical management included partial maxillectomy with orbital floor reconstruction, given the orbital invasion. Three years later, left hyperglobus recurred, and the patient was found to have orbital recurrence and lung metastases on PET imaging. The lung and orbital lesions have responded well to chemoradiation therapy without surgical intervention. Conclusion: Maxillary ameloblastoma is a rare tumor that typically arises from odontogenic tissues. Though considered benign, they can recur and in the case of our patient, metastasize. Complete surgical excision with wide surgical margins is associated with a shorter average time to recurrence and a lower incidence of metastasis. Cases of metastasis are managed with chemotherapy with or without adjuvant radiotherapy. Precision medicine may play a role in managing this entity in the future, given the discovery of differing profiles of maxillary ameloblastoma compared to mandibular. Ophthalmologists should be aware of this tumor as it can invade the orbit, resulting in significant ocular morbidity and mortality.

Non-Hodgkin lymphoma of the orbit and ocular adnexa is the most common primary orbital malignancy. Treatments for low- (extra-nodal marginal zone and follicular lymphomas) and high-grade (diffuse large B-cell lymphoma) are associated with local and vision-threatening toxicities. High-grade lymphomas relapse frequently and exhibit poor survival rates. Despite advances in genomic profiling and precision medicine, orbital and ocular adnexal lymphomas remain poorly characterized molecularly. We performed targeted next-generation sequencing (NGS) profiling of 38 formalin-fixed, paraffin-embedded orbital and ocular adnexal lymphomas obtained from a single-center using a panel targeting near-term, clinically relevant genes. Potentially actionable mutations and copy number alterations were prioritized based on gain- and loss-of-function analyses, and catalogued, approved, and investigational therapies. Of 36 informative samples, including marginal zone lymphomas ( n =20), follicular lymphomas ( n =9), and diffuse large B-cell lymphomas ( n =7), 53% harbored a prioritized alteration (median=1, range 0–5/sample). MYD88 was the most frequently altered gene in our cohort, with potentially clinically relevant hotspot gain-of-function mutations identified in 71% of diffuse large B-cell lymphomas and 25% of marginal zone lymphomas. Prioritized alterations in epigenetic modulators were common and included gain-of-function EZH2 and loss-of-function ARID1A mutations (14% of diffuse large B-cell lymphomas and 22% of follicular lymphomas contained alterations in each of these two genes). Single prioritized alterations were also identified in the histone methyltransferases KMT2B (follicular lymphoma) and KMT3B (diffuse large B-cell lymphoma). Loss-of-function mutations and copy number alterations in the tumor suppressors TP53 (diffuse large B-cell and follicular lymphoma), CDKN2A (diffuse large B-cell and marginal zone lymphoma), PTEN (diffuse large B-cell lymphoma), ATM (diffuse large B-cell lymphoma), and NF1 (diffuse large B-cell lymphoma), and gain-of-function mutations in the oncogenes HRAS (follicular lymphoma) and NRAS (diffuse large B-cell lymphoma) were also observed. Together, our study demonstrates that NGS can be used to profile routine formalin-fixed, paraffin-embedded orbital and ocular adnexal lymphomas for identification of somatic-driving alterations and nomination of potential therapeutic strategies.

We present the discovery and characterization of TOI-4364b, a young mini-Neptune in the tidal tails of the Hyades cluster, identified through TESS transit observations and ground-based follow-up photometry. The planet orbits a bright M dwarf (K = 9.1 mag) at a distance of 44 pc, with an orbital period of 5.42 days and an equilibrium temperature of 488−7+9 K. The host star's well-constrained age of 710 Myr makes TOI-4364b an exceptional target for studying early planetary evolution around low-mass stars. We determined a planetary radius of 2.01−0.08+0.10R⊕ , indicating that this planet is situated near the upper edge of the radius valley. This suggests that the planet retains a modest H/He envelope. As a result, TOI-4364b provides a unique opportunity to explore the transition between rocky super-Earths and gas-rich mini-Neptunes at the early stages of evolution. Its radius, which may still evolve as a result of ongoing atmospheric cooling, contraction, and photoevaporation, further enhances its significance for understanding planetary development. Furthermore, TOI-4364b’s moderately high transmission spectroscopy metric of 44.2 positions it as a viable candidate for atmospheric characterization with instruments such as JWST. This target has the potential to offer crucial insights into atmospheric retention and loss in young planetary systems.

Few studies have examined outcomes for Mohs micrographic surgery (MMS) for cutaneous squamous cell carcinoma (cSCC) in Black versus White patients. We compared time to surgery and defect sizes after MMS between Black versus White patients with cSCC. Patients with biopsy-proven cSCC treated with MMS at the Hospital of the University of Pennsylvania were identified from a prospectively maintained database (2006–2023). Our primary outcomes included time to surgery (days from the diagnostic biopsy to the first MMS) and defect size (final MMS defect surface area). Univariate and multivariate linear regression models were performed to compare outcomes between Black and White patients with adjustments for age, gender, and tumor location. We identified 8445 cSCC, including 8329 (98.2%) in White patients and 116 (1.4%) in Black patients. Mean time to surgery was 31% longer for Black (76 ± 3.9 days) versus White patients (58 ± 0.5 days) [ p  < 0.001]. Mean post-MMS cSCC defect size was nearly four times larger for Black (18.6 ± 1.2 cm 2 ) versus White patients (4.8 ± 0.1 cm 2 ) [ p  < 0.0001]. These differences remained significant when adjusted for age, gender, and tumor location [ p  < 0.0001]. In conclusion, Black patients with cSCC have significantly longer treatment delays and larger MMS defects than White patients. This study highlights the need for earlier diagnosis and more timely access to MMS for Black patients with cSCC.

Young eclipsing binaries (EBs) are powerful probes of early stellar evolution. Current models are unable to simultaneously reproduce the measured and derived properties that are accessible for EB systems (e.g., mass, radius, temperature, and luminosity). In this study we add a benchmark EB to the pre-main-sequence population with our characterization of TOI 450 (TIC 77951245). Using Gaia astrometry to identify its comoving, coeval companions, we confirm TOI 450 is a member of the ∼40 Myr Columba association. This eccentric (e = 0.2969), equal-mass (q = 1.000) system provides only one grazing eclipse. Despite this, our analysis achieves the precision of a double-eclipsing system by leveraging information in our high-resolution spectra to place priors on the surface-brightness and radius ratios. We also introduce a framework to include the effect of star spots on the observed eclipse depths. Multicolor eclipse light curves play a critical role in breaking degeneracies between the effects of star spots and limb-darkening. Including star spots reduces the derived radii by ∼2% from a unspotted model (>2σ) and inflates the formal uncertainty in accordance with our lack of knowledge regarding the starspot orientation. We derive masses of 0.1768( ± 0.0004) and 0.1767( ± 0.0003) M ⊙, and radii of 0.345(±0.006) and 0.346(±0.006) R ⊙ for the primary and secondary, respectively. We compare these measurements to multiple stellar evolution isochones, finding good agreement with the association age. The MESA MIST and SPOTS (f s = 0.17) isochrones perform the best across our comparisons, but detailed agreement depends heavily on the quantities being compared.