On the impact of Helium abundance on the Cepheid Period-Luminosity and Wesenheit relations and the Distance Ladder

This work analyses the effect of the Helium content on synthetic Period-Luminosity Relations (PLRs) and Period-Wesenheit Relations (PWRs) of Cepheids and the systematic uncertainties on the derived distances that a hidden population of He-enhanced Cepheids may generate. We use new stellar and pulsation models to build a homogeneous and consistent framework to derive the Cepheid features. The Cepheid populations expected in synthetic color-magnitude diagrams of young stellar systems (from 20 Myr to 250 Myr) are computed in several photometric bands for Y = 0.25 and Y = 0.35, at a fixed metallicity (Z = 0.008). The PLRs appear to be very similar in the two cases, with negligible effects (few %) on distances, while PWRs differ somewhat, with systematic uncertainties in deriving distances as high as about 7% at log P < 1.5. Statistical effects due to the number of variables used to determine the relations contribute to a distance systematic error of the order of few percent, with values decreasing from optical to near-infrared bands. The empirical PWRs derived from multi-wavelength datasets for the Large Magellanic Cloud (LMC) is in a very good agreement with our theoretical PWRs obtained with a standard He content, supporting the evidence that LMC Cepheids do not show any He effect

Multipopulation aftereffects on the color-magnitude diagram and Cepheid variables of young stellar systems

Context: The evidence of a multipopulation scenario in Galactic globular clusters raises several questions about the formation and evolution of the two (or more) generations of stars. These populations show differences in their age and chemical composition. These differences are found in old- and intermediate- age stellar clusters in the Local Group. The observations of young stellar systems are expected to present footprints of multiple stellar populations. Aims: This theoretical work intends to be a specific step in exploring the space of the observational indicators of multipopulations, without covering all the combinations of parameters that may contribute to the formation of multiple generations of stars in a cluster or in galaxy. The goal is to shed light on the possible observational features expected by core He-burning stars that belong to two stellar populations with different original He content and ages. Methods: The tool adopted was the stellar population synthesis. We used new stellar and pulsation models to construct a homogeneous and consistent framework. Synthetic color-magnitude diagrams (CMDs) of young- and intermediate-age stellar systems (from 20 Myr up to 1 Gyr) were computed in several photometric bands to derive possible indicators of double populations both in the observed CMDs and in the pulsation properties of the Cepheids. Results: We predict that the morphology of the red/blue clump in VIK bands can be used to photometrically indicate the two stellar populations in a rich assembly of stars if there is a significant difference in their original He content. Moreover, the period distribution of the Cepheids appears to be widely affected by the coeval multiple generations of stars within stellar systems. We show that the Wesenheit relations may be affected by the helium content of the Cepheids.Comment: in press on A&

Photometric and spectroscopic study of the intermediate-age open cluster NGC 2355

In this paper we analyse the evolutionary status and properties of the old open cluster NGC 2355, located in the Galactic anticentre direction, as a part of the long term programme BOCCE. NGC 2355 was observed with LBC@LBT using the Bessel $B$, $V$, and $I_c$ filters. The cluster parameters have been obtained using the synthetic colour-magnitude diagram (CMD) method, as done in other papers of this series. Additional spectroscopic observations with FIES@NOT of three giant stars were used to determine the chemical properties of the cluster. Our analysis shows that NGC 2355 has metallicity slightly less than solar, with [Fe/H]$=-0.06$ dex, age between 0.8 and 1 Gyr, reddening $E(B-V)$ in the range 0.14 and 0.19 mag, and distance modulus $(m-M)_0$ of about 11 mag. We also investigated the abundances of O, Na, Al, $\alpha$, iron-peak, and neutron capture elements, showing that NGC 2355 falls within the abundance distribution of similar clusters (same age and metallicity). The Galactocentric distance of NGC~2355 places it at the border between two regimes of metallicity distribution; this makes it an important cluster for the study of the chemical properties and evolution of the disc.Comment: 20 pages, 11 figures, Accepted on MNRA

Synthetic sustainability index (SSI) based on life cycle assessment approach of low impact development in the Mediterranean area

AbstractClimate change and the processes of urbanization alter the hydrologic and hydraulic regime of runoffs formation in urban areas. Low impact infrastructure development (LID) contributes to achieving conditions of invariance hydrological and hydraulics. The purpose of this work is to identify an index of synthetic sustainability (SSI) based on life cycle assessment (LCA). Such LCA evaluates design alternatives through the comparison of the different values of the SSI. The proposed methodology allows the evaluation of the SSI attributing to the individual layers of the LIDs different weights and taking into account both of the influence that each of them perform on invariance hydrologic and hydraulic both of the LCA normalized output. In this paper is showed a methodological implementation obtained by the analysis of a green roof and a permeable pavement. This green roof has been realized, on real scale, in the Urban Hydrology Experimental Park in University of Calabria (Italy)

Large Binocular Telescope observations of PSR J2043+2740

We present the results of deep optical imaging of the radio/$\gamma$-ray pulsar PSR J2043+2740, obtained with the Large Binocular Telescope (LBT). With a characteristic age of 1.2 Myr, PSR J2043+2740 is one of the oldest (non recycled) pulsars detected in $\gamma$-rays, although with still a quite high rotational energy reservoir ($\dot{E}_{\rm rot} = 5.6 \times 10^{34}$ erg s$^{-1}$). The presumably close distance (a few hundred pc), suggested by the hydrogen column density ($N_{\rm H} \lesssim 3.6 \times 10^{20}$ cm$^{-2}$), would make it a viable target for deep optical observations, never attempted until now. We observed the pulsar with the Large Binocular Camera of the LBT. The only object (V=25.44$\pm$0.05) detected within ~3" from the pulsar radio coordinates is unrelated to it. PSR J2043+2740 is, thus, undetected down to V~26.6 (3-$\sigma$), the deepest limit on its optical emission. We discuss the implications of this result on the pulsar emission properties.Comment: 4 pages, 3 figures, accepted for publication on MNRA

Results from the Blazar Monitoring Campaign at the Whipple 10m Gamma-ray Telescope

In September 2005, the observing program of the Whipple 10 m gamma-ray telescope was redefined to be dedicated almost exclusively to AGN monitoring. Since then the five Northern Hemisphere blazars that had already been detected at Whipple are monitored routinely each night that they are visible. Thanks to the efforts of a large number of multiwavelength collaborators, the first year of this program has been very successful. We report here on the analysis of Markarian 421 observations taken from November, 2005 to May, 2006 in the gamma-ray, X-ray, optical and radio bands.Comment: 4 pages; contribution to the 30th International Cosmic Ray Conference, Merida, Mexico, July 200

Ameloblastoma plexiforme del maxilar: manejo quirúrgico y protético. A propósito de un caso

El ameloblastoma es un tumor odontógeno benigno de derivación epitelial, de elevada invasión local, crecimiento intermitente y con alta probabilidad de recidiva. Puede dividirse en los siguientes tipos histológicos: folicular, plexiforme, acantomatoso, a células basales y granulares. El ameloblastoma folicular es el subtipo histológico más común. Se manifiesta prevalentemente durante la tercera, cuarta y quinta década de vida, sin predilección para el sexo, aun así se puede encontrar en cualquier grupo de edad incluyendo niños. La mayoría de los ameloblastomas se encuentra sobretodo en mandíbula (al nivel del ángulo y rama). Las características clínicas, incluso si complementadas con radiografías y muestras histológicas, no son útiles a la hora de predeterminar el comportamiento biológico y por lo tanto el pronóstico de un ameloblastoma individual. Los autores presentan un caso localizado de ameloblastoma plexiforme localizado en la parte posterior del maxilar de un hombre de 30 años; el término "plexiforme" se refiere al aspecto de anastomosis de los islotes del epitelio odontógeno, en contraste con el tipo «folicular». En este artículo se discuten importantes aspectos de la patología, del tratamiento quirúrgico y protésico. En conclusión, es necesaria una cooperación estricta a largo plazo de un grupo de clínicos, patólogos, cirujanos y prostodoncistas, para ofrecer el mejor tratamiento individualizado en cada caso. The ameloblastoma is a clinically persistent benign tumor derived from odontogenic epithelium, locally invasive, intermittent in growth and with high a probability of recurrence. The following histologic patterns may be distinguished: follicular, plexiform, spindle cell, acanthomatous, basal cell type and granular cell. The follicular ameloblastoma is the most common histologic tipe. The majority of patients are in 3th, 4th and 5th decade, but can be found in any age group including children. The majority of ameloblastomas are observed in the mandible (mostly angle or ramus). Clinical features, even if combined with radiology or histology findings, are not useful when trying to determine the biological behaviour and therefore the prognosis of an individual ameloblastoma. The authors report a case of plexiform ameloblastoma in the posterior maxilla, in male 30 year old otherwise healthy; the term "plexiform" refers to the appearance of anastomosing islands of odontogenic epithelium in contrast to a follicular pattern. Important questions on pathology, surgical and prosthetic therapy are discussed in this paper. In conclusion, a close cooperation of clinicians, pathologists, surgeons and prosthesists is necessary and very important over a long period of time for the best management of each individual case