Lifetime of the embedded phase of low-mass star formation and the envelope depletion rates

Motivated by a considerable scatter in the observationally inferred lifetimes of the embedded phase of star formation, we study the duration of the Class 0 and Class I phases in upper-mass brown dwarfs and low-mass stars using numerical hydrodynamics simulations of the gravitational collapse of a large sample of cloud cores. We resolve the formation of a star/disk/envelope system and extend our numerical simulations to the late accretion phase when the envelope is nearly totally depleted of matter. We adopted a classification scheme of Andre et al. and calculate the lifetimes of the Class 0 and Class I phases (\tau_C0 and \tau_CI, respectively) based on the mass remaining in the envelope. When cloud cores with various rotation rates, masses, and sizes (but identical otherwise) are considered, our modeling reveals a sub-linear correlation between the Class 0 lifetimes and stellar masses in the Class 0 phase with the least-squares fit exponent m=0.8 \pm 0.05. The corresponding correlation between the Class I lifetimes and stellar masses in the Class I is super-linear with m=1.2 \pm 0.05. If a wider sample of cloud cores is considered, which includes possible variations in the initial gas temperature, cloud core truncation radii, density enhancement amplitudes, initial gas density and angular velocity profiles, and magnetic fields, then the corresponding exponents may decrease by as much as 0.3. The duration of the Class I phase is found to be longer than that of the Class~0 phase in most models, with a mean ratio \tau_CI / \tau_C0 \approx 1.5--2. A notable exception are YSOs that form from cloud cores with large initial density enhancements, in which case \tau_C0 may be greater than \tau_CI. Moreover, the upper-mass (>= 1.0 Msun) cloud cores with frozen-in magnetic fields and high cloud core rotation rates may have the \tau_CI / \tau_C0 ratios as large as 3.0--4.0. (Abdridged).Comment: Accepted for publication by The Astrophysical Journa

Properties of the Youngest Protostars in Perseus, Serpens, and Ophiuchus

We present an unbiased census of deeply embedded protostars in Perseus, Serpens, and Ophiuchus, assembled by combining large-scale 1.1 mm Bolocam continuum and Spitzer Legacy surveys. We identify protostellar candidates based on their mid-infrared properties, correlate their positions with 1.1 mm core positions, and construct well-sampled SEDs using our extensive wavelength coverage (lam=1.25-1100 micron). Source classification based on the bolometric temperature yields a total of 39 Class 0 and 89 Class I sources in the three cloud sample. We compare to protostellar evolutionary models using the bolometric temperature-luminosity diagram, finding a population of low luminosity Class I sources that are inconsistent with constant or monotonically decreasing mass accretion rates. This result argues strongly for episodic accretion during the Class I phase, with more than 50% of sources in a ``sub-Shu'' (dM/dt < 1e-6 Msun/yr) accretion state. Average spectra are compared to protostellar radiative transfer models, which match the observed spectra fairly well in Stage 0, but predict too much near-IR and too little mid-IR flux in Stage I. Finally, the relative number of Class 0 and Class I sources are used to estimate the lifetime of the Class 0 phase; the three cloud average yields a Class 0 lifetime of 1.7e5 yr, ruling out an extremely rapid early accretion phase. Correcting photometry for extinction results in a somewhat shorter lifetime (1.1e5 yr). In Ophiuchus, however, we find very few Class 0 sources (N(Class0)/N(ClassI)=0.1-0.2), similar to previous studies of that cloud. The observations suggest a consistent picture of nearly constant average accretion rate through the entire embedded phase, with accretion becoming episodic by at least the Class I stage, and possibly earlier.Comment: 31 pages, 19 figures, 8 tables; accepted for publication in Ap

El 'Proyecto educativo de centro' en el ámbito universitario. Reflexiones y propuestas a partir de la experiencia de la Facultad de Derecho de la Universidad de Barcelona (2005-2016)

Este estudio valora la oportunidad y la viabilidad del Proyecto Educativo de "centro", o de Facultad, en un contexto universitario. Para ello se define qué es un proyecto educativo de centro y se identifica el origen del concepto en la literatura y en nuestro sistema educativo así como su aceptación en la universidad española. En segundo lugar se enumeran los elementos que, eventualmente, pueden configurar un proyecto educativo de centro universitario, y se hace a partir de la experiencia académico-docente de la Facultad de Derecho de la Universidad de Barcelona; a partir de este caso, se relacionan los elementos que han integrado el núcleo del proyecto educativo de centro y los elementos complementarios; además se proponen algunas líneas por donde podría discurrir la evolución de este proyecto educativo de centro. La presente aportación, en definitiva, aspira a fomentar un debate, sobre todo entre las facultades de Derecho, y por extensión también entre el resto de Facultades de las universidades públicas españolas, acerca de la conveniencia de disponer y de publicar un Proyecto Educativo de Facultad explícito que marque y oriente nuestra acción docente, que sea un eficaz instrumento de planificación educativa, que fije el marco educativo de los estudiantes, y que se convierta en elemento de identidad institucional

El programa institucional de mejora de la calidad docente de la Facultat de Derecho de la Universidad de Barcelona (2004-2012)

Esta comunicación muestra las líneas básicas del programa institucional de mejora de la calidad docente de la Facultad de Derecho de la Universidad de Barcelona. Si en CIDUI 2011 analizábamos los factores causales y determinantes del rendimiento académico en la universidad española actual y se proponían, con cierto carácter general, acciones de mejora vinculadas a cada categoría causal, en esta ocasión se describe una experiencia concreta y real: se presentan las 15 principales acciones o engranajes que actúan de forma simultánea y en ámbitos o direcciones diferentes para conseguir el doble objetivo de mejorar la calidad docente e incrementar el rendimiento académico en un marco de exigencia y rigor

Bolocam Survey for 1.1 mm Dust Continuum Emission in the c2d Legacy Clouds. II. Ophiuchus

We present a large-scale millimeter continuum map of the Ophiuchus molecular cloud. Nearly 11 square degrees, including all of the area in the cloud with visual extinction more than 3 magnitudes, was mapped at 1.1 mm with Bolocam on the Caltech Submillimeter Observatory (CSO). By design, the map also covers the region mapped in the infrared with the Spitzer Space Telescope. We detect 44 definite sources, and a few likely sources are also seen along a filament in the eastern streamer. The map indicates that dense cores in Ophiuchus are very clustered and often found in filaments within the cloud. Most sources are round, as measured at the half power point, but elongated when measured at lower contour levels, suggesting spherical sources lying within filaments. The masses, for an assumed dust temperature of 10 K, range from 0.24 to 3.9 solar masses, with a mean value of 0.96 solar masses. The total mass in distinct cores is 42 solar masses, 0.5 to 2% of the total cloud mass, and the total mass above 4 sigma is about 80 solar masses. The mean densities in the cores are quite high, with an average of 1.6 x 10^6 per cc, suggesting short free-fall times. The core mass distribution can be fitted with a power law with slope of 2.1 plus or minus 0.3 for M>0.5 solar masses, similar to that found in other regions, but slightly shallower than that of some determinations of the local IMF. In agreement with previous studies, our survey shows that dense cores account for a very small fraction of the cloud volume and total mass. They are nearly all confined to regions with visual extinction at least 9 mag, a lower threshold than found previously.Comment: 47 pages, 16 figures, accepted for Ap

Proximate, minerals and antinutrient assessment of the leaves and tenderstem of Leptadenia hastate (pers.) decne

The study evaluated the proximate, minerals and antinutrient contents of the plant Leptadenia hastata (Pers.) decne (Asclepiadaceae). Nutrient and antinutritional factors were determined using standard analytical methods and parameters subjected to statistical analysis. Manganese (Mn), Calcium (Ca) and Cobalt (Co) were found to be significantly (p&lt;0.001) higher in the leaves when compared to the tender stem while Iron (Fe), Zinc (Zn) and Magnesium (Mg) were found to be significantly (p&lt;0.001) higher in the tender stems when compared to the leaves. The percentages of Moisture content, Crude proteins and Total ash were found to be significantly (p&lt;0.05) higher in the leaves when compared to the tender stem while crude fiber and Nitrogen Free Extract (NFE) was significantly (p&lt;0.05) higher in the stem when compared to the leaves. Oxalate and phytic acid were anti nutrient found to be significantly (p&lt;0.001) higher in the leaves when compared to the tender stem. However, Copper (Cu), Lead (Pb), Potassium (K) and Crude fat were not significantly (p&gt;0.05) different when compared in the leaves and tender stem. Correlation analysis indicated that antinutrient contents in the tender stems will not affect the mineral absorption in the leaves while negative correlation between Fe and Cu in the stems could affect the absorption of iron. Therefore, Leptadenia hastata leave and tender stem consumed in soup and local salad in northern Nigeria proved to be rich in minerals and nutrients to support its dietary role as a consumed vegetable.Keywords: Leptadenia hastata, Minerals, Proximate, Antinutrients, Tender stems, Leave

Episodic accretion at early stages of evolution of low mass stars and brown dwarfs: a solution for the observed luminosity spread in HR diagrams?

We present evolutionary models for young low mass stars and brown dwarfs taking into account episodic phases of accretion at early stages of the evolution, a scenario supported by recent large surveys of embedded protostars. An evolution including short episodes of vigorous accretion (\mdot \ge 10^{-4} \msolyr) followed by longer quiescent phases (\mdot < 10^{-6} \msolyr) can explain the observed luminosity spread in HR diagrams of star forming regions at ages of a few Myr, for objects ranging from a few Jupiter masses to a few tenths of a solar mass. The gravitational contraction of these accreting objects strongly departs from the standard Hayashi track at constant \te. The best agreement with the observed luminosity scatter is obtained if most of the accretion shock energy is radiated away. The obtained luminosity spread at 1 Myr in the HR diagram is equivalent to what can be misinterpreted as a $\sim$ 10 Myr age spread for non-accreting objects. We also predict a significant spread in radius at a given \te, as suggested by recent observations. These calculations bear important consequences on our understanding of star formation and early stages of evolution and on the determination of the IMF for young ($\le$ a few Myr) clusters. Our results also show that the concept of a stellar birthline for low-mass objects has no valid support.Comment: 8 pages, 5 figures, accepted for publication in APJ Lette

Comparing Star Formation on Large Scales in the c2d Legacy Clouds: Bolocam 1.1 mm Dust Continuum Surveys of Serpens, Perseus, and Ophiuchus

We have undertaken an unprecedentedly large 1.1 millimeter continuum survey of three nearby star forming clouds using Bolocam at the Caltech Submillimeter Observatory. We mapped the largest areas in each cloud at millimeter or submillimeter wavelengths to date: 7.5 sq. deg in Perseus (Paper I), 10.8 sq. deg in Ophiuchus (Paper II), and 1.5 sq. deg in Serpens with a resolution of 31", detecting 122, 44, and 35 cores, respectively. Here we report on results of the Serpens survey and compare the three clouds. Average measured angular core sizes and their dependence on resolution suggest that many of the observed sources are consistent with power-law density profiles. Tests of the effects of cloud distance reveal that linear resolution strongly affects measured source sizes and densities, but not the shape of the mass distribution. Core mass distribution slopes in Perseus and Ophiuchus (alpha=2.1+/-0.1 and alpha=2.1+/-0.3) are consistent with recent measurements of the stellar IMF, whereas the Serpens distribution is flatter (alpha=1.6+/-0.2). We also compare the relative mass distribution shapes to predictions from turbulent fragmentation simulations. Dense cores constitute less than 10% of the total cloud mass in all three clouds, consistent with other measurements of low star-formation efficiencies. Furthermore, most cores are found at high column densities; more than 75% of 1.1 mm cores are associated with Av>8 mag in Perseus, 15 mag in Serpens, and 20-23 mag in Ophiuchus.Comment: 32 pages, including 18 figures, accepted for publication in Ap

A complete 1.1mm survey of Perseus with Bolocam

We have completed a 7.5 square degree λ=1.1mm map of Perseus using Bolocam. Our map is the largest unbiased survey of Perseus at millimeter wavelengths to date, and covers the same area as the c2d Spitzer IRAC and MIPS maps of Perseus. We find that that the mass function shape is similar to that seen in other clouds and to the local IMF. Despite the large area surveyed, few new sources are found outside the known cluster regions