We present the results of a study investigating the galaxy stellar-mass function (GSMF), size-mass relations, and morphological properties of star-forming and quiescent galaxies over the redshift range 0.25

The HAWC Observatory collected 6 yr of extensive data, providing an ideal platform for long-term monitoring of blazars in the very high energy (VHE) band, without bias toward specific flux states. HAWC continuously monitors blazar activity at TeV energies, focusing on sources with a redshift of z ≤ 0.3, based on the Third Fermi-LAT Catalog of High-Energy sources. We specifically focused our analysis on Mrk 421 and Mrk 501, as they are the brightest blazars observed by the HAWC Observatory. With a data set of 2143 days, this work significantly extends the monitoring previously published, which was based on 511 days of observation. By utilizing HAWC data for the VHE γ -ray emission in the 300 GeV–100 TeV energy range, in conjunction with Swift-XRT data for the 0.3–10 keV X-ray emission, we aim to explore potential correlations between these two bands. For Mrk 501, we found evidence of a long-term correlation. Additionally, we identified a period in the light curve where the flux was very low for more than 2 yr. On the other hand, our analysis of Mrk 421 measured a strong linear correlation for quasi-simultaneous observations collected by HAWC and Swift-XRT. This result is consistent with a linear dependence and a multiple-zone synchrotron self-Compton model to explain the X-ray and γ -ray emission. Finally, as suggested by previous findings, we confirm a harder-when-brighter behavior in the spectral evolution of the flux properties for Mrk 421. These findings contribute to the understanding of blazar emissions and their underlying mechanisms.

Universal cytomegalovirus (CMV) prophylaxis is recommended for at-risk lung transplant recipients. Valganciclovir (VGCV) is currently the preferred first-line agent. VGCV-related myelosuppression, however, can lead to drug discontinuation or reduction in antimetabolite immunosuppression. Variable VGCV pharmacokinetics in the setting of renal injury are also associated with development of resistant CMV. Letermovir, a newer anti-CMV agent, is an attractive alternative for first-line prophylaxis in many lung transplant recipients. Initially investigated in bone marrow transplant, there are now multiple retrospective studies of lung transplant recipients who were switched from VGCV to letermovir because of tolerability, dosing, or resistance. These studies have reaffirmed the safety and efficacy of letermovir in the lung transplant population. Despite this, letermovir continues to be recommended as second-line prophylaxis with use limited to those who fail VGCV. We argue that there are now sufficient data to support letermovir use in lung transplant recipients at high risk of VGCV toxicity. This includes patients with renal insufficiency, of advanced age, and with cytolytic immunosuppression, high risk of rejection, and telomere biology disorders, among other conditions. First-line letermovir would reduce the risk of VGCV-related myelosuppression and attendant reduction in immunosuppression, as well as development of CMV resistance due to variable renal function and VGCV pharmacokinetics.

The High-Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory, located on the side of the Sierra Negra volcano in Mexico, has been fully operational since 2015. The HAWC collaboration has recently significantly improved their extensive air shower reconstruction algorithms, which has notably advanced the observatory performance. The energy resolution for primary gamma rays with energies below 1 TeV was improved by including a noise-suppression algorithm. Corrections have also been made to systematic errors in direction fitting related to the detector and shower plane inclinations, O(0.degrees 1) biases in highly inclined showers, and enhancements to the core reconstruction. The angular resolution for gamma rays approaching the HAWC array from large zenith angles (>37 degrees) has improved by a factor of 4 at the highest energies (>70 TeV) as compared to previous reconstructions. The inclusion of a lateral distribution function fit to the extensive air shower footprint on the array to separate gamma-ray primaries from cosmic-ray ones based on the resulting chi(2) values improved the background rejection performance at all inclinations. At large zenith angles, the improvement in significance is a factor of 4 compared to previous HAWC publications. These enhancements have been verified by observing the Crab Nebula, which is an overhead source for the HAWC Observatory. We show that the sensitivity to Crab-like point sources (E-2.63) with locations overhead to 30 degrees zenith is comparable to or less than 10% of the Crab Nebula's flux between 2 and 50 TeV. Thanks to these improvements, HAWC can now detect more sources, including the Galactic center.

The origin of high-energy galactic cosmic rays is yet to be understood, but some galactic cosmic-ray accelerators can accelerate cosmic rays up to PeV energies. The high-energy cosmic rays are expected to interact with the surrounding material or radiation, resulting in the production of gamma-rays and neutrinos. To optimize for the detection of such associated production of gamma-rays and neutrinos for a given source morphology and spectrum, a multimessenger analysis that combines gamma-rays and neutrinos is required. In this study, we use the Multi-Mission Maximum Likelihood framework with IceCube Maximum Likelihood Analysis software and HAWC Accelerated Likelihood to search for a correlation between 22 known gamma-ray sources from the third HAWC gamma-ray catalog and 14 yr of IceCube track-like data. No significant neutrino emission from the direction of the HAWC sources was found. We report the best-fit gamma-ray model and 90% CL neutrino flux limit from the 22 sources. From the neutrino flux limit, we conclude that, for five of the sources, the gamma-ray emission observed by HAWC cannot be produced purely from hadronic interactions. We report the limit for the fraction of gamma-rays produced by hadronic interactions for these five sources.

Purpose: Valganciclovir (VGV) is the standard of care for cytomegalovirus (CMV) prophylaxis after solid organ transplant; however, VGV-associated myelosuppression limits its tolerability. Letermovir (LET), a viral terminase inhibitor, is approved by the FDA for use as CMV prophylaxis in stem cell transplant. Data are limited regarding its use in lung transplant recipients (LTRs).

The gas in the interstellar medium (ISM) of galaxies is supersonically turbulent. Measurements of turbulence typically rely on cold gas emission lines for low-z galaxies and warm ionized gas observations for z > 0 galaxies. Studies of warm gas kinematics at z > 0 conclude that the turbulence strongly evolves as a function of redshift, due to the increasing impact of gas accretion and mergers in the early Universe. However, recent findings suggest potential biases in turbulence measurements derived from ionized gas at high-z, impacting our understanding of turbulence origin, ISM physics and disk formation. We investigate the evolution of turbulence using velocity dispersion (sigma) measurements from cold gas tracers (i.e., CO, [CI], [CII]). The initial dataset comprises 17 galaxy disks with high data quality from the ALPAKA sample, supplemented with galaxies from the literature, resulting in a sample of 57 galaxy disks spanning the redshift range z = 0 - 5. This extended sample consists of main-sequence and starburst galaxies with stellar masses greater than or similar to 10(10) M-circle dot. The comparison with current H alpha kinematic observations and existing models demonstrates that the velocity dispersion inferred from cold gas tracers differ by a factor of approximate to 3 from those obtained using emission lines tracing the warm, ionized gas. We show that stellar feedback is the main driver of turbulence measured from cold gas tracers and the physics of turbulence driving does not appear to evolve with time. This is fundamentally different from the conclusions of studies based on warm gas, which had to consider additional turbulence drivers to explain the high values of sigma. We present a model predicting the redshift evolution of turbulence in galaxy disks, attributing the increase of sigma with redshift to the higher energy injected by supernovae due to the elevated star-formation rate in high-z galaxies. This supernova-driven model suggests that turbulence is lower in galaxies with lower stellar mass compared to those with higher stellar mass. Additionally, it forecasts the evolution of sigma in Milky-Way like progenitors.

Extended very-high-energy (VHE; 0.1–100 TeV) γ-ray emission has been observed around several middle-aged pulsars and referred to as “TeV halos.” Their formation mechanism remains under debate. It is also unknown whether they are ubiquitous or related to a certain subgroup of pulsars. With 2321 days of observation, the High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory detected VHE γ-ray emission at the location of the radio-quiet pulsar PSR J0359+5414 with >6σ significance. By performing likelihood tests with different spectral and spatial models and comparing the TeV spectrum with multiwavelength observations of nearby sources, we show that this excess is consistent with a TeV halo associated with PSR J0359+5414, though future observation of HAWC and multiwavelength follow-ups are needed to confirm this nature. This new halo candidate is located in a noncrowded region in the outer galaxy. It shares similar properties to the other halos but its pulsar is younger and radio-quiet. Our observation implies that TeV halos could commonly exist around pulsars and their formation does not depend on the configuration of the pulsar magnetosphere.

Recent JWST/NIRcam imaging taken for the ultra-deep UNCOVER program reveal a very red, triply imaged, compact dropout object at z phot (cid:39) 7 . 66 which is prominently lensed by the galaxy cluster Abell 2744 ( z d = 0 . 308). All three images are very compact, i.e. unresolved, with an inferred de-lensed size upper limit of r e (cid:46) 35 pc. The observed F444W magnitude of the three images is m ∼ 25 − 26 AB and the source’s absolute UV magnitude is M UV , 1450 = − 16 . 81 ± 0 . 09, after correcting for magnification. From the sum of observed fluxes and from a spectral energy distribution (SED) fit we

We present a 1.1 mm stacking analysis of moderately massive (log(M*/M⊙) = 10.7 ± 0.2) quiescent galaxies (QGs) at ⟨z⟩∼1.5, searching for cold dust continuum emission, which serves as an excellent tracer of dust and gas mass. Using both the recent GOODS-ALMA survey, as well as the full suite of ALMA Band-6 ancillary data in the GOODS-S field, we report the tentative detection of a dust continuum equivalent of the dust mass log(Mdust/M⊙) = 7.47 ± 0.13 and gas mass log(Mgas/M⊙) = 9.42 ± 0.14. The emerging gas fraction is fgas = 5.3 ± 1.8%, consistent with the results of previous stacking analyses based on lower resolution sub(mm) observations. Our results support the scenario where high-z QGs exhibit a larger fgas value by one order of magnitude compared to their local counterparts and have experienced quenching with a non-negligible gas reservoir in their interstellar medium, namely, with gas retention. Our subsequent analysis yields an anti-correlation between the fgas and the stellar mass of QGs, especially in the high-mass end where galaxies reside in the most massive halos. The fgas − M* anti-correlation promotes the selection bias as a possible solution to the tension between the stacking results pointing towards gas retention in high-z QGs of moderate M* and studies of individual targets that favour a fully depleted ISM in massive (log(M*/M⊙) > 11.2) high-z QGs.

We present individual star-formation histories of $\sim3000$ massive galaxies (log($\mathrm{M_*/M_{\odot}}$)>10.5) from the Large Early Galaxy Astrophysics Census (LEGA-C) spectroscopic survey at a lookback time of $\sim$7 billion years and quantify the population trends leveraging 20hr-deep integrated spectra of these $\sim$ 1800 star-forming and $\sim$ 1200 quiescent galaxies at 0.6<$z$<1.0. Essentially all galaxies at this epoch contain stars of age<3 Gyr, in contrast with older massive galaxies today, facilitating better recovery of previous generations of star formation at cosmic noon and earlier. We conduct spectro-photometric analysis using parametric and non-parametric Bayesian SPS modeling tools - Bagpipes and Prospector to constrain the median star-formation histories of this mass-complete sample and characterize population trends. A consistent picture arises for the late-time stellar mass growth when quantified as $t_{50}$ and $t_{90}$, corresponding to the age of the universe when galaxies formed 50\% and 90\% of their total stellar mass, although the two sets of models disagree at the earliest formation times (e.g. $t_{10}$). Our results reveal trends in both stellar mass and stellar velocity dispersion as in the local universe - low-mass galaxies with shallower potential wells grow their stellar masses later in cosmic history compared to high-mass galaxies. Unlike local quiescent galaxies, the median duration of late-time star-formation ($\tau_{SF,late}$ = $t_{90}$ - $t_{50}$) does not consistently depend on the stellar mass. This census sets a benchmark for future deep spectro-photometric studies of the more distant universe.

In the quest for high-energy neutrino sources, the Astrophysical Multimessenger Observatory Network has implemented a new search by combining data from the High Altitude Water Cherenkov (HAWC) Observatory and the Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) neutrino telescope. Using the same analysis strategy as in a previous detector combination of HAWC and IceCube data, we perform a search for coincidences in HAWC and ANTARES events that are below the threshold for sending public alerts in each individual detector. Data were collected between 2015 July and 2020 February with a live time of 4.39 yr. Over this time period, three coincident events with an estimated false-alarm rate of <1 coincidence per year were found. This number is consistent with background expectations.

ABSTRACT We present the JWST cycle 1 53.8 h medium program FRESCO, short for ‘First Reionization Epoch Spectroscopically Complete Observations’. FRESCO covers 62 arcmin2 in each of the two GOODS/CANDELS fields for a total area of 124 arcmin2 exploiting JWST’s powerful new grism spectroscopic capabilities at near-infrared wavelengths. By obtaining ∼2 h deep NIRCam/grism observations with the F444W filter, FRESCO yields unprecedented spectra at R ∼ 1600 covering 3.8–5.0 µm for most galaxies in the NIRCam field of view. This setup enables emission line measurements over most of cosmic history, from strong PAH lines at z ∼ 0.2–0.5, to Pa α and Pa β at z ∼ 1–3, He i and [S iii] at z ∼ 2.5–4.5, H α and [N ii] at z ∼ 5–6.5, up to [O iii] and H β for z ∼ 7–9 galaxies. FRESCO’s grism observations provide total line fluxes for accurately estimating galaxy stellar masses and calibrating slit-loss corrections of NIRSpec/MSA spectra in the same field. Additionally, FRESCO results in a mosaic of F182M, F210M, and F444W imaging in the same fields to a depth of ∼28.2 mag (5σ in 0${_{.}^{\prime\prime}}$32 diameter apertures). Here, we describe the overall survey design and the key science goals that can be addressed with FRESCO. We also highlight several, early science results, including: spectroscopic redshifts of Lyman break galaxies that were identified almost 20 yr ago, the discovery of broad-line active galactic nuclei at z > 4, and resolved Pa α maps of galaxies at z ∼ 1.4. These results demonstrate the enormous power for serendipitous discovery of NIRCam/grism observations.

Recent JWST/NIRcam imaging taken for the ultra-deep UNCOVER program reveal a very red, triply imaged, compact dropout object at z phot (cid:39) 7 . 66 which is prominently lensed by the galaxy cluster Abell 2744 ( z d = 0 . 308). All three images are very compact, i.e

PurposeInvasive fungal infections (IFIs) remain a frequent complication in the lung transplant (LTx) population even in the current era of antifungal prophylaxis. The organ donor and peri-transplant period risk factors for IFI remain ill-defined. Our study goal is to identify novel risk factors for IFI, focusing on the organ donor and the recipient's transplant hospitalization.MethodsWe performed a single-center, case-control study. The source cohort included all adults who underwent LTx between 1/1/12-3/31/17. The primary outcome was a Probable or Proven IFI within 6 months of transplantation, as defined by EORTC/MSG criteria. Multivariable logistic regression and Cox proportional hazard regression analyses were used to identify independent risk factors for IFI.ResultsOf 329 LTx recipients, 45 (14%) developed IFI. The median time to IFI was 50 days (IQR: 25-110) after transplantation. Independent risk factors for IFI included: donor steroid pre-conditioning (aOR 2.24, 95%CI: 1.05-4.77, p=0.04); cardiopulmonary bypass (aOR 3.07, 95%CI: 1.06-8.87, p=0.04); ICU length of stay >30 days (aOR 3.34, 95%CI: 1.48-75, p<0.01); and bronchial anastomotic dehiscence (aOR 14.06, 95%CI: 1.99-99.34, p=0.01). Mold isolated on donor respiratory culture increased the hazard of IFI in LTx recipients (Table 1). Peri-transplant hospitalization complications that increased the hazard of IFI included: multiple positive fungal cultures, airway ischemia, and prolonged ICU stay (Table 1). Fungal treatment for ≥90 days after transplant was protective against development of IFI (Table 1).ConclusionIFI was common in our LTx cohort. Certain donor characteristics and peri-transplant complications increased the likelihood of IFI. Interventional studies, targeting the modifiable risk factors identified in this study, are needed to reduce IFI risk in LTx recipients.

We determine the intrinsic, 3-dimensional shape distribution of star-forming galaxies at 0 1e10 Msol) disks are the most common geometric shape at all z < 2. Lower-mass galaxies at z>1 possess a broad range of geometric shapes: the fraction of elongated (prolate) galaxies increases toward higher redshifts and lower masses. Galaxies with stellar mass 1e9 Msol (1e10 Msol) are a mix of roughly equal numbers of elongated and disk galaxies at z~1 (z~2). This suggests that galaxies in this mass range do not yet have disks that are sustained over many orbital periods, implying that galaxies with present-day stellar mass comparable to that of the Milky Way typically first formed such sustained stellar disks at redshift z~1.5-2. Combined with constraints on the evolution of the star formation rate density and the distribution of star formation over galaxies with different masses, our findings imply that, averaged over cosmic time, the majority of stars formed in disks.