A Mid-Infrared Imaging Survey of Embedded Young Stellar Objects in the Rho Ophiuchi Cloud Core

Results of a comprehensive, new, ground-based mid-infrared imaging survey of the young stellar population of the Rho Ophiuchi cloud are presented. Data were acquired at the Palomar 5-m and at the Keck 10-m telescopes with the MIRLIN and LWS instruments, at 0.25 arcsec and 0.25 arcsec resolutions, respectively. Of 172 survey objects, 85 were detected. Among the 22 multiple systems observed, 15 were resolved and their individual component fluxes determined. A plot of the frequency distribution of the detected objects with SED spectral slope shows that YSOs spend ~400,000 yr in the Flat Spectrum phase, clearing out their remnant infall envelopes. Mid-infrared variability is found among a significant fraction of the surveyed objects, and is found to occur for all SED classes with optically thick disks. Large-amplitude near-infrared variability, also found for all SED classes with optically thick disks, seems to occur with somewhat higher frequency at the earlier evolutionary stages. Although a general trend of mid-infrared excess and NIR veiling exists proceeding through SED classes, with Class I objects generally exhibiting K-veilings > 1, Flat Spectrum objects with K-veilings > 0.58, and Class III objects with K-veilings =0, Class II objects exhibit the widest range of K-band veiling values, 0-4.5. However, the highly variable value of veiling that a single source can exhibit in any of the SED classes in which active disk accretion can take place is striking, and is direct observational evidence for highly time-variable accretion activity in disks. Finally, by comparing mid-infrared vs. near-infrared excesses in a subsample with well-determined effective temperatures and extinction values, disk clearing mechanisms are explored. The results are consistent with disk clearing proceeding from the inside-out.Comment: 18 pages + 5 tables + 7 figure

Excitonic effects in two-dimensional vibrational spectra of liquid formamide

The linear and two-dimensional infrared (2DIR) responses of the amide I vibrational mode in liquid formamide are investigated experimentally and theoretically using molecular dynamics simulations. The recent method based on the numerical integration of the Schrödinger equation is employed to calculate the 2DIR spectra. Special attention is devoted to the interplay of the structural dynamics and the excitonic nature of the amide I modes in determining the optical response of the studied system. In particular, combining experimental data, simulated spectra and analysis of the simulated atomic trajectory in terms of a transition dipole coupling model, we provide a convincing explanation of the peculiar features of the 2DIR spectra, which show a substantial increase of the antidiagonal bandwidth with increasing frequency. We point out that, at variance with liquid water, the 2DIR spectral profile of formamide is determined more by the excitonic nature of the vibrational states than by the fast structural dynamics responsible for the frequency fluctuations

Impacts of hydrological changes in the Mediterranean zone: environmental modifications and rural development in the Merguellil catchment, central Tunisia / Un exemple d'évolution hydrologique en Méditerranée: impacts des modifications environnementales et du développement agricole dans le bassin-versant du Merguellil (Tunisie centrale)

The Merguellil catchment (central Tunisia), which is typical of the Mediterranean situation, has undergone rapid hydrological changes over the last decades. The most visible signs are a marked decrease in surface runoff in the upstream catchment and a complete change in the recharge processes of the Kairouan aquifer downstream. Fluctuations in rainfall have had a limited hydrological impact. Much more important have been the consequences of human activities, such as soil and water conservation works, small and large dams, and pumping for irrigation. Several independent investigations of the catchment were implemented, based on hydrodynamics, thermal surveys, and geochemistry including isotopes. These helped to identify the different terms of the regional water balance and to characterize their changes over time. However, major uncertainties remain and our results may contradict previous interpretations or calculations. Conservation works, now covering more than a quarter of the upstream catchment, drastically reduce the runoff production from rain events of less than 40 mm. Wadi Merguellil now ends in the big El Haouareb Reservoir, which loses more than half of its water by infiltration through karstic fissures and 30% by evaporation, the rest being pumped or released. El Haouareb Dam was built in 1989 and the reservoir has often dried up in the last decade. The major modifications in groundwater flow resulting from construction of the dam are observed in the geochemical tracers in the first seven kilometres downstream from it. Temperature measurements confirmed the recent invasion of new water. The rest of the Kairouan plain aquifer retains the signature of older recharge, but the whole aquifer is affected by the decrease in the water table (about 1 m per year), the consequence of the ever increasing pumping for irrigation

Mesure statistique de la résistance de contact d’une grille sérigraphiée pour cellules solaires au silicium multicristallin

La métallisation par sérigraphie est une des étapes les plus importantes dans la technologie d’élaboration des cellules solaires pour une production à grande échelle. Néanmoins, elle demeure dépendante de plusieurs paramètres variables. Pour le silicium multi cristallin, tout changement dans le procédé de réalisation des cellules solaires influence directement l’optimisation du profil de recuit de la métallisation par sérigraphie. Les plaquettes de silicium multi cristallin subissent toutes les étapes classiques de réalisation des cellules solaires comme le nettoyage chimique et la décontamination, une diffusion au phosphore et le dépôt du nitrure de silicium SiNx par PECVD (Plasma Enhanced Chemical Vapor Deposition). Il y a juste le dépôt du contact Argent Ag sur la face avant de la plaquette. Nous avons utilisé la pâte de sérigraphie Ag Ferro 3349. La grille métallique comporte six (06) motifs TLM (Transfer Length Method) pour les mesures de la résistance de contact. Le principal but de ce travail est le contrôle de la qualité du contact Ag/SiNx/n+-Si dans les cellules solaires au silicium multicristallin. Les mesures TLM révèlent une cartographie des valeurs de la résistance de contact pour chaque température. Le profil optimal de température de recuit est autour de 750 °C

Morphology of the 12-micron Seyfert Galaxies: II. Optical and Near-Infrared Image Atlas

We present 263 optical and near-infrared (NIR) images for 42 Seyfert 1s and 48 Seyfert 2s, selected from the Extended 12-micron Galaxy Sample. Elliptically-averaged profiles are derived from the images, and isophotal radii and magnitudes are calculated from these. We also report virtual aperture photometry, that judging from comparison with previous work, is accurate to roughly 0.05mag in the optical, and 0.07mag in the NIR. Our B-band isophotal magnitude and radii, obtained from ellipse fitting, are in good agreement with those of RC3. When compared with the B band, V, I, J, and K isophotal diameters show that the colors in the outer regions of Seyferts are consistent with the colors of normal spirals. Differences in the integrated isophotal colors and comparison with a simple model show that the active nucleus+bulge is stronger and redder in the NIR than in the optical. Finally, roughly estimated Seyfert disk surface brightnesses are significantly brighter in B and K than those in normal spirals of similar morphological type.Comment: 17 pgs including figures; Table 2 is a separate file. Complete Figure 1 is available by contacting the authors. Accepted for publication in ApJ

A Subarcsecond Companion to the T Tauri Star AS 353B

Adaptive optics imaging of the bright visual T Tauri binary AS 353 with the Subaru Telescope shows that it is a hierarchical triple system. The secondary component, located 5.6" south of AS 353A, is resolved into a subarcsecond binary, AS 353Ba and Bb, separated by 0.24". Resolved spectroscopy of the two close components shows that both have nearly identical spectral types of about M1.5. Whereas AS 353A and Ba show clear evidence for an infrared excess, AS 353Bb does not. We discuss the possible role of multiplicity in launching the large Herbig-Haro flow associated with AS 353A.Comment: AASTeXv5.0, 21 pages, 5 figures, Astronomical Journal, in pres

The Stellar Population of the Chamaeleon I Star-Forming Region

I present a new census of the stellar population in the Chamaeleon I star-forming region. Using optical and near-IR photometry and followup spectroscopy, I have discovered 50 new members of Chamaeleon I, expanding the census of known members to 226 objects. Fourteen of these new members have spectral types later than M6, which doubles the number of known members that are likely to be substellar. I have estimated extinctions, luminosities, and effective temperatures for the known members, used these data to construct an H-R diagram for the cluster, and inferred individual masses and ages with the theoretical evolutionary models of Baraffe and Chabrier. The distribution of isochronal ages indicates that star formation began 3-4 and 5-6 Myr ago in the southern and northern subclusters, respectively, and has continued to the present time at a declining rate. The IMF in Chamaeleon I reaches a maximum at a mass of 0.1-0.15 M_sun, and thus closely resembles the IMFs in IC 348 and the Orion Nebula Cluster. In logarithmic units where the Salpeter slope is 1.35, the IMF is roughly flat in the substellar regime and shows no indication of reaching a minimum down to a completeness limit of 0.01 M_sun. The low-mass stars are more widely distributed than members at other masses in the northern subcluster, but this is not the case in the southern subcluster. Meanwhile, the brown dwarfs have the same spatial distribution as the stars out to a radius of 3 deg (8.5 pc) from the center of Chamaeleon I

Misaligned spin and orbital axes cause the anomalous precession of DI Herculis

The orbits of binary stars precess as a result of general relativistic effects, forces arising from the asphericity of the stars, and forces from additional stars or planets in the system. For most binaries, the theoretical and observed precession rates are in agreement. One system, however -- DI Herculis -- has resisted explanation for 30 years. The observed precession rate is a factor of four slower than the theoretical rate, a disagreement that once was interpreted as evidence for a failure of general relativity. Among the contemporary explanations are the existence of a circumbinary planet and a large tilt of the stellar spin axes with respect to the orbit. Here we report that both stars of DI Herculis rotate with their spin axes nearly perpendicular to the orbital axis (contrary to the usual assumption for close binary stars). The rotationally induced stellar oblateness causes precession in the direction opposite to that of relativistic precession, thereby reconciling the theoretical and observed rates.Comment: Nature, in press [11 pg

Context-dependent plant traits drive fine-scale species persistence in old-growth forests

Questions: we studied old growth beech forest vegetation in Permanent Monitoring Plots (PMPs) located in Italy, with the following questions: is species turnover the main component of the observed changes or the present species assemblages is an impoverished sub-sets of the former ones?; 2) how compositional changes are reflected by specific plant functional traits? Location: we selected 4 PMPs (50 x 50 m) of the CONECOFOR network, placed along a latitudinal and climatic gradient in Italy, from south to north: CALABRIA03, CAMPANIA04, ABRUZZO01 and VENETO20. Methods: presence/absence of herb layer species were recorded in 100 permanent micro-plots of 50 x 50 cm over 12 years (1999-2011). For all sampled species we chose a set of 8 easy-to-measure functional traits. We compared the persistence, nestedness and turnover components of compositional changes. The role of plant traits explaining species persistence were analyzed by classification and regression tree. Results: Analysis in species diversity reveal antithetical ecological phenomena due to the diversity and complexity of the 4 different forest stands. ABRUZZO01 and CALABRIA03 show a clear nestedness trends over time with persistent species in ABR01 having higher seed mass and persistent species in CALABRIA03 having scleromorphic leaves and mesoporphic leaves, with large below-ground budbank. On the other hand, VENETO20 and CAMPANIA04 exibit a significant turnover trends over the 12 years characterized by persistent species in VENETO20 having helomorphic leaves, while in CAMPANIA04 large below-ground budbank and smaller SLA were the most important traits for species survival. Conclusion: Fine-scale approach highlight different mechanisms for the maintenance of species diversity in different complex forest systems driven significantly by specific traits, influenced by context-dependent factors