Heterogeneous Sensory Innervation and Extensive Intrabulbar Connections of Olfactory Necklace Glomeruli

The mammalian nose employs several olfactory subsystems to recognize and transduce diverse chemosensory stimuli. These subsystems differ in their anatomical position within the nasal cavity, their targets in the olfactory forebrain, and the transduction mechanisms they employ. Here we report that they can also differ in the strategies they use for stimulus coding. Necklace glomeruli are the sole main olfactory bulb (MOB) targets of an olfactory sensory neuron (OSN) subpopulation distinguished by its expression of the receptor guanylyl cyclase GC-D and the phosphodiesterase PDE2, and by its chemosensitivity to the natriuretic peptides uroguanylin and guanylin and the gas CO2. In stark contrast to the homogeneous sensory innervation of canonical MOB glomeruli from OSNs expressing the same odorant receptor (OR), we find that each necklace glomerulus of the mouse receives heterogeneous innervation from at least two distinct sensory neuron populations: one expressing GC-D and PDE2, the other expressing olfactory marker protein. In the main olfactory system it is thought that odor identity is encoded by a combinatorial strategy and represented in the MOB by a pattern of glomerular activation. This combinatorial coding scheme requires functionally homogeneous sensory inputs to individual glomeruli by OSNs expressing the same OR and displaying uniform stimulus selectivity; thus, activity in each glomerulus reflects the stimulation of a single OSN type. The heterogeneous sensory innervation of individual necklace glomeruli by multiple, functionally distinct, OSN subtypes precludes a similar combinatorial coding strategy in this olfactory subsystem

Effect of Gd polarization on the large magnetocaloric effect of GdCrO4 in a broad temperature range

The ferromagnetic zircon-type phase of GdCrO4 presents high values for the magnetocaloric (MC) parameters. This compound has large isothermal entropy changes ¿ST under the magnetic field action in a wide temperature range, from 5 to 35 K, reaching a maximum |¿ST|=29.0±0.1J/kgK at 22 K, for a field increment ¿B=9 T. It orders ferromagnetically at TC=21.3K via the Cr-Cr exchange interaction and shows a second transition at 4.8 K due to the ordering of the Gd sublattice. The large MC effect is enhanced by the polarization of the Gd3+ ions by the Cr5+ ones via a weaker Gd-Cr interaction. This effect is an interesting feature to be considered in the search for new compounds with a high MC effect in the range of liquid hydrogen or natural gas, regarding the liquefaction of gases by magnetization-demagnetization cycles. This paper contains experimental measurements of magnetization, heat capacity, and direct determinations of the MC effect. The magnetic contribution to the heat capacity Cm has been obtained after subtracting the lattice component. Approximate values for the exchange constants J1 (Cr-Cr) and J3 (Gd-Cr) have been deduced from Cm

HI holes in galactic disks: Tracing the dark matter distribution

Multiple SN explosions in disk galaxies efficiently evacuate gas and form cavities with the sizes and shapes of the surrounding envelopes determined by the total amount of injected energy and by the initial gas distribution. Such cavities are seen as HI holes when observed in face-on galaxies. Gas hydrodynamics simulations are performed to obtain the quantitative characteristics of HI holes that could serve for the determination of the gas vertical scale height and the corresponding dark matter content and its distribution. Among these characteristics is the ratio of the maximum column density in the HI ring surrounding the hole to the background HI column density and the vertical expansion velocity of gas in the HI ring. We show that in some cases the extragalactic background ionizing radiation may produce HI holes in the outer regions of galaxies, and can account for the existence of HI holes in nearby face-on galaxies with the apparent lack of an underlying stellar population.Comment: 8 pages, 6 figures, accepted for publication in Astronomy & Astrophysic

Numerical simulations of expanding supershells in dwarf irregular galaxies. I. Application to Holmberg I

Numerical hydrodynamical modelling of supernova-driven shell formation is performed with a purpose to reproduce a giant HI ring (diameter 1.7 kpc) in the dwarf irregular galaxy Holmberg I (Ho I). We find that the contrast in HI surface density between the central HI depression and the ring is sensitive to the shape of the gravitational potential. This circumstance can be used to constrain the total mass (including the dark matter halo) of nearly face-on dwarf irregulars. We consider two models of Ho I, which differ by an assumed mass of the dark matter halo M_h. The contrast in HI surface density between the central HI depression and the ring, as well as the lack of gas expansion in the central hole, are better reproduced by the model with a massive halo of M_h=6.0*10^9 M_sun than by that with a small halo of M_h=4.0*10^8 M_sun, implying that Ho I is halo-dominated. Assuming the halo mass of 6.0*10^9 M_sum, we determine the mechanical energy required to form the observed ring equal to (3.0 +- 0.5)*10^53 ergs, equivalent 300+-50 Type II supernovae. The inclination of Ho I is constrained to 15-20 degrees by comparing the modelled HI spectrum and channel maps with those observed.Comment: 11 pages, 11 figures, accepted for publication in Astronomy and Astrophysic

Recent Star Formation in Sextans A

We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. This galaxy is currently experiencing a burst of localized star formation, the trigger of which is unknown. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter \sim 5.'3. We have compared our photometry with theoretical isochrones appropriate for Sextans A, in order to determine the ages of these populations. We have mapped out the history of star formation, most accurately for times \lesssim 100 Myr. We find that star formation in Sextans A is correlated both in time and space, especially for the most recent (\lesssim 12 Myr) times. The youngest stars in the galaxy are forming primarily along the inner edge of the large H I shell. Somewhat older populations, \lesssim 50 Myr, are found inward of the youngest stars. Progressively older star formation, from \sim 50--100 Myr, appears to have some spatially coherent structure and is more centrally concentrated. The oldest stars we can accurately sample appear to have approximately a uniform spatial distribution, which extends beyond a surface brightness of \mu_B \simeq 25.9 mag arcsec^{-2} (or, a radius r \simeq 2.'3$). Although other processes are also possible, our data provides support for a mechanism of supernova-driven expansion of the neutral gas, resulting in cold gas pileup and compression along the H I shell and sequential star formation in recent times.Comment: 64 pages, 22 figures, to appear in A

“Estudio del efecto relajante e la fibra lisa en útero asilado de rata inducido por derivados terapéuticos con y sin oxígeno”

A study on the relaxing effect'of sorne terpenic derivates, with oxygen (linalool) and without oxygen (alfa-pinene, sabinene and limonene), major components from essential oil of J. sabina L., over smooth muscle has been performed. Contraction rat isolated uterus was induced by increasing doses of oxytocin (10-10 - 10-9M). The results obtaines showed that ter penes (2,5 . 10-4M) have relaxing activity of uterus "in vitro" (non competitive antogonism with oxytocin dose depent). The use of emulsifier (sodium cholate) for help to solubility of terpenes in the water don't modifity the results obtaines when the ter penes have been homogeneity in the water for agitation.Se ha estudiado el efecto de dos series de terpenos, oxigenados (linalol) y no oxigenados (alfa-pineno, sabineno y limoneno) componentes mayoritarios estos últimos del aceite esencial del J. sabina L., tras comprobación cromatográfica, sobre la contracción del útero aislado de rata inducida por oxitocina (10-10 - 1O-9M). Los resultados obtenidos indican la presencia de un antagonismo no competitivo entre dichos fármacos y la oxitocina a partir de concentraciones de 2,5. 1O-4M. El empleo de un emulgente como fue la sal sódica del ácido cólico con la intención de mejorar la dispersión en agua de los terpenos no mejoró los resultados obtenidos tras homogeneización de los mismos cuando estaban en disolución acuosa

Sobre el origen del Mapa Geológico de España. El Mapa Geognóstico de los alrededores de Burgos de Felipe Naranjo y Garza (1841)

En el año 1841 se publicó en la revista Anales de Minas, acompañando a una memoria explicativa sobre la geología y minería de la provincia de Burgos, una cartografía geológica a escala próxima a 1:350.000. En el mapa se definen ya los tres principales rasgos litoestructurales que forman la geología de la provincia de Burgos. La memoria, por su parte, además de la geología, incide en la minería de la zona estudiada, en la que destaca la descripción de las salinas de Poza de la Sal. El autor, Felipe Naranjo y Garza (1809-1877), fue uno de los primeros ingenieros de minas españoles que, desde los múltiples puestos que desempeñó en la administración, destacó por su contribución al desarrollo de la geología en España y en sus intentos de modernizar la industria minera. En el presente trabajo pretendemos dar a conocer esta precoz cartografía geológica y analizar dicha obra científica situándola en el contexto en que se encontraba la geología española en la primera mitad del siglo XLX

Inhomogeneous electronic structure probed by spin-echo experiments in the electron doped high-Tc superconductor Pr_{1.85}Ce_{0.15}CuO_{4-y}

63Cu nuclear magnetic resonance (NMR) spin-echo decay rate (T_2^{-1}) measurements are reported for the normal and superconducting states of a single crystal of Pr_{1.85}Ce_{0.15}CuO_{4-y} (PCCO) in a magnetic field B_0=9T over the temperature range 2K<T<200K. The spin-echo decay rate is temperature-dependent for T<55K, and has a substantial dependence on the radio frequency (rf) pulse parameters below T~25K. This dependence indicates that T_2^{-1} is strongly effected by a local magnetic field distribution that can be modified by the rf pulses, including ones that are not at the nuclear Larmor frequency. The low-temperature results are consistent with the formation of a static inhomogeneous electronic structure that couples to the rf fields of the pulses.Comment: 4 pages, 4 figure