Pre- and Post-Adaptation Effects of Buffers in High-Concentrate Lamb Diets

A gradual increase in grain cover a period of 2 to 4 weeks is commonly required before ruminant animals become adapted to high-concentrate diets. Various dietary materials including sodium bicarbonate, sodium betonite, limestone and forage have been indicated as potential adis in the prevention of acidosis during adaptation. Benefits from feeding of these materials following adaptation have been less pronounced or lacking. Objectives of studies reported herein were (1) to investigate the effects of buffers and limited quantitites of alfalfa hay on physiological and rumen fermentation changs occuring in lambs during the early phase of adaptation to high-concentrate diets and (2) to study ruminal and systemic parameters and nutrient utilization as influenced by buffers in the diets of lambs previously adapted to the high-concentrate diet

Characterizing the Circumgalactic Medium of the Lowest-mass Galaxies: A Case Study of IC 1613

Using 10 sight lines observed with the Hubble Space Telescope/Cosmic Origins Spectrograph, we study the circumgalactic medium (CGM) and outflows of IC 1613, which is a low-mass (M_* ~ 10⁸ M_⊙), dwarf irregular galaxy on the outskirts of the Local Group. Among the sight lines, four are pointed toward UV-bright stars in IC 1613, and the other six sight lines are background QSOs at impact parameters from 6 kpc (<0.1R_(200)) to 61 kpc (0.6R_(200)). We detect a number of Si ii, Si iii, Si iv, C ii, and C iv absorbers, most of which have velocities less than the escape velocity of IC 1613 and thus are gravitationally bound. The line strengths of these ion absorbers are consistent with the CGM absorbers detected in dwarf galaxies at low redshifts. Assuming that Si ii, Si iii, and Si iv comprise nearly 100% of the total silicon, we find 3% (~8 × 10³ M_⊙), 2% (~7 × 10³ M_⊙), and 32%–42% [~(1.0–1.3) × 10⁵ M_⊙] of the silicon mass in the stars, interstellar medium, and within 0.6R_(200) of the CGM of IC 1613. We also estimate the metal outflow rate to be Ṁ_(out,Z) ⩾ 1.1 x 10⁻⁵ M_⊙ yr⁻¹ and the instantaneous metal mass loading factor to be η_Z ≥ 0.004, which are in broad agreement with available observation and simulation values. This work is the first time a dwarf galaxy of such low mass is probed by a number of both QSO and stellar sight lines, and it shows that the CGM of low-mass, gas-rich galaxies can be a large reservoir enriched with metals from past and ongoing outflows

Predicting length of stay in head and neck patients who undergo free flap reconstruction

ObjectiveUnderstanding factors that affect postoperative length of stay (LOS) may improve patient recovery, hasten postoperative discharge, and minimize institutional costs. This study sought to (a) describe LOS among head and neck patients undergoing free flap reconstruction and (b) identify factors that predict increased LOS.MethodsA retrospective cohort was performed of 282 head and neck patients with free flap reconstruction for oncologic resection between 2011 and 2013 at a tertiary academic medical center. Patient demographics, tumor characteristics, and surgical and infectious complications were characterized. Multivariable regression identified predictors of increased LOS.ResultsA total of 282 patients were included. Mean age was 64.7 years (SD = 12.2) and 40% were female. Most tumors were located in the oral cavity (53.9% of patients), and most patients underwent radial forearm free flap (RFFF) reconstruction (RFFF—73.8%, anterolateral thigh flap—11.3%, and fibula free flap—14.9%). Intraoperative complications were rare. The most common postoperative complications included nonwound infection (pneumonia [PNA] or urinary tract infection [UTI]) (15.6%) and wound breakdown/fistula (15.2%). Mean and median LOS were 13 days (SD = 7.7) and 10 days (interquartile range = 7), respectively. Statistically significant predictors of increased LOS included flap take back (Beta coefficient [C] = +4.26, P < .0001), in‐hospital PNA or UTI (C = +2.52, P = .037), wound breakdown or fistula (C = +5.0, P < .0001), surgical site infection (C = +3.54, P = .017), and prior radiation therapy (C = +2.59, P = .004).ConclusionSeveral perioperative factors are associated with increased LOS. These findings may help with perioperative planning, including the need for vigilant wound care, optimization of antibiotics prophylaxis, and institution‐level protocols for postoperative care and disposition of free flap patients.Level of Evidence2b; retrospective cohort.Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/155916/1/lio2410.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/155916/2/lio2410_am.pd

Tentative detection of the circumgalactic medium of the isolated low-mass dwarf galaxy WLM

We report a tentative detection of the circumgalactic medium (CGM) of Wolf–Lundmark–Melotte (WLM), an isolated, low-mass (logM*/M⊙ ≈ 7.6), dwarf irregular galaxy in the Local Group (LG). We analyse an HST/COS archival spectrum of a quasar sightline (PHL2525), which is 45 kpc (0.5 virial radius) from WLM and close to the Magellanic Stream (MS). Along this sightline, two ion absorbers are detected in Si II, Si III, Si IV, C II, and C IV at velocities of ∼−220 km s⁻¹ (Component v-220) and ∼−150 km s⁻¹ (Component v-150). To identify their origins, we study the position–velocity alignment of the components with WLM and the nearby MS. Near the magellanic longitude of PHL2525, the MS-related neutral and ionized gas moves at ≲−190 km s⁻¹, suggesting an MS origin for Component v-220, but not for Component v-150. Because PHL2525 passes near WLM and Component v-150 is close to WLM’s systemic velocity (∼−132 km s⁻¹), it is likely that Component v-150 arises from the galaxy’s CGM. This results in a total Si mass in WLM’s CGM of M^(CGM)_(Si)∼(0.2−1.0)×10⁵ M⊙ using assumption from other COS dwarf studies. Comparing M^(CGM)_(Si) to the total Si mass synthesized in WLM over its lifetime (∼1.3 × 10⁵ M⊙), we find ∼3 per cent is locked in stars, ∼6 per cent in the ISM, ∼15–77 per cent in the CGM, and the rest (∼14–76 per cent) is likely lost beyond the virial radius. Our finding resonates with other COS dwarf galaxy studies and theoretical predictions that low-mass galaxies can easily lose metals into their CGM due to stellar feedback and shallow gravitational potential