The detections of four apparently young radio pulsars in the Milky Way globular clusters are difficult to reconcile with standard neutron star formation scenarios associated with massive star evolution. Here, we discuss formation of these young pulsars through white dwarf mergers in dynamically old clusters that have undergone core collapse. Based on observed properties of magnetic white dwarfs, we argue neutron stars formed via white dwarf merger are born with spin periods of roughly 10-100 ms and magnetic fields of roughly 10(11) -10(13) G. As these neutron stars spin down via magnetic dipole radiation, they naturally reproduce the four observed young pulsars in the Milky Way clusters. Rates inferred from N-body cluster simulations as well as the binarity, host cluster properties, and cluster offsets observed for these young pulsars hint further at a white dwarf merger origin. These young pulsars may be descendants of neutron stars capable of powering fast radio bursts analogous to the bursts observed recently in a globular cluster in M81.

The Takab-Delijan (T-D) magmatic belt in NW Iran is a part of the Zagros orogenic belt which has imminence with epithermal, porphyry and carlin types of mineralization. This magmatic belt has been classified into 3 different phases by radiometric dating, including early (16-24 Ma), middle-late (10-12 Ma), and late Miocene (8 > Ma), among which the gold/basemetal mineralization is related to the first two phases in this area. The lower Miocene phase formed during the formation of a metamorphic core complex and upwelling basement in the form of synextentional magmatism. This magmatic event is shaped in an extensional regime within shallow marine basins which are correlated with the limestone formation of Qom Formation (QF) in a pre- to syncollisional environment. This volcanism (edifice) acceded to the surface rapidly via NW extensional faults and made stratovolcanic structures in the Takab and Delijan areas. These complexes have been formed by sequences of pyroclastic and lava flows with a composition of dacite to andesite and trachyandesite that are crosscut by microdiorite porphyritic subvolcanic. These epithermal-porphyr systems are related to the Cu +/- Au +/- Ag deposits. The main phase of gold mineralization is related to the magmatic phase with middle-late Miocene and the age of similar to 10.7-12 Ma. The geological environment for forming this magmatic phase is related to the extensionalcompressional regime by the right-lateral strike-slip shear zone during shortening, folding, and thickening in synto post-collisional events. The magmatism is in the form of dacitic to rhyolitic domes on the surface. The gold/ silver mineralization is associated with the hydrothermal metal suite of As, Sb, Te, Pb, and Zn, and it is characterized by very low Cu contents of subvolcanic. The final stage of tectonic evolution events is the thrusting of prior normal faults and exhumation in the late Miocene-Pliocene age which is together with post-collision magmatism.

We present CI(2-1) and multi-transition (CO)-C-12 observations of a dusty star-forming galaxy, ACT J2029+0120, which we spectroscopically confirm to lie at z = 2.64. We detect CO(3-2), CO(5-4), CO(7-6), CO(8-7), and CI (2-1) at high significance, tentatively detect HCO+(4-3), and place strong upper limits on the integrated strength of dense gas tracers (HCN(4-3) and CS(7-6)). Multi-transition CO observations and dense gas tracers can provide valuable constraints on the molecular gas content and excitation conditions in high-redshift galaxies. We therefore use this unique data set to construct a CO spectral line energy distribution (SLED) of the source, which is most consistent with that of a ULIRG/Seyfert or QSO host object in the taxonomy of the Herschel Comprehensive ULIRG Emission Survey. We employ RADEX models to fit the peak of the CO SLED, inferring a temperature of T similar to 117 K and n(H2) similar to 10(5) cm(-3), most consistent with a ULIRG/QSO object and the presence of high-density tracers. We also find that the velocity width of the C I line is potentially larger than seen in all CO transitions for this object, and that the L'(Ci(2-1))/L'(CO(3-2)) ratio is also larger than seen in other lensed and unlensed submillimeter galaxies and QSO hosts; if confirmed, this anomaly could be an effect of differential lensing of a shocked molecular outflow.

The origin, evolution, and cycling of volatiles on the Moon are established by processes such as the giant moon forming impact, degassing of the lunar magma ocean, degassing during surface eruptions, and lunar surface gardening events. These processes typically induce mass-dependent stable isotope fractionations. Mass-independent fractionation of stable isotopes has yet to be demonstrated during events that release large volumes of gas on the moon and establish transient lunar atmospheres. We present quadruple sulfur isotope compositions of orange and black glass beads from drive tube 74002/1. The sulfur isotope and concentration data collected on the orange and black glasses confirm a role for magmatic sulfur loss during eruption. The Delta S-33 value of the orange glasses is homogenous (Delta S-33 = -0.029 parts per thousand +/- 0.004 parts per thousand, 2SE) and different from the isotopic composition of lunar basalts (Delta S-33 = 0.002 parts per thousand +/- 0.004 parts per thousand, 2SE). We link the negative Delta S-33 composition of the orange glasses to an anomalous sulfur source in the lunar mantle. The nature of this anomalous sulfur source remains unknown and is either linked to (a) an impactor that delivered anomalous sulfur after late accretion, (b) sulfur that was photochemically processed early during lunar evolution and was transported to the lunar mantle, or (c) a primitive sulfur component that survived mantle mixing. The examined black glass preserves a mass-dependent Delta S-33 composition (-0.008 parts per thousand +/- 0.006 parts per thousand, 2SE). The orange and black glasses are considered genetically related, but the discrepancy in Delta S-33 composition among the two samples calls their relationship into question.

Lactobacilli and Acetobacter sp. are commercially important bacteria that often form communities in natural fermentations, including food preparations, spoilage, and in the digestive tract of the fruit fly Drosophila melanogaster. Communities of these bacteria are widespread and prolific, despite numerous strain-specific auxotrophies, suggesting they have evolved nutrient interdependencies that regulate their growth. The use of a chemically-defined medium (CDM) supporting the growth of both groups of bacteria would facilitate the identification of the molecular mechanisms for the metabolic interactions between them. While numerous CDMs have been developed that support specific strains of lactobacilli or Acetobacter, there has not been a medium formulated to support both genera. We developed such a medium, based on a previous CDM designed for growth of lactobacilli, by modifying the nutrient abundances to improve growth yield. We further simplified the medium by substituting casamino acids in place of individual amino acids and the standard Wolfe's vitamins and mineral stocks in place of individual vitamins and minerals, resulting in a reduction from 40 to 8 stock solutions. These stock solutions can be used to prepare several CDM formulations that support robust growth of numerous lactobacilli and Acetobacters. Here, we provide the composition and several examples of its use, which is important for tractability in dissecting the genetic and metabolic basis of natural bacterial species interactions.