IRIS: A new generation of IRAS maps

The Infrared Astronomical Satellite (IRAS) had a tremendous impact on many areas of modern astrophysics. In particular it revealed the ubiquity of infrared cirrus that are a spectacular manifestation of the interstellar medium complexity but also an important foreground for observational cosmology. With the forthcoming Planck satellite there is a need for all-sky complementary data sets with arcminute resolution that can bring informations on specific foreground emissions that contaminate the Cosmic Microwave Background radiation. With its 4 arcmin resolution matching perfectly the high-frequency bands of Planck, IRAS is a natural data set to study the variations of dust properties at all scales. But the latest version of the images delivered by the IRAS team (the ISSA plates) suffer from calibration, zero level and striping problems that can preclude its use, especially at 12 and 25 micron. In this paper we present how we proceeded to solve each of these problems and enhance significantly the general quality of the ISSA plates in the four bands (12, 25, 60 and 100 micron). This new generation of IRAS images, called IRIS, benefits from a better zodiacal light subtraction, from a calibration and zero level compatible with DIRBE, and from a better destriping. At 100 micron the IRIS product is also a significant improvement from the Schlegel et al. (1998) maps. IRIS keeps the full ISSA resolution, it includes well calibrated point sources and the diffuse emission calibration at scales smaller than 1 degree was corrected for the variation of the IRAS detector responsivity with scale and brightness. The uncertainty on the IRIS calibration and zero level are dominated by the uncertainty on the DIRBE calibration and on the accuracy of the zodiacal light model.Comment: 16 pages, 17 figures, accepted for publication in ApJ (Suppl). Higher resolution version available at http://www.cita.utoronto.ca/~mamd/IRIS/IrisTechnical.htm

Probing the origin of the microwave anomalous foreground

The galactic anomalous microwave emission detected between 10 and 90 GHz is a major foreground to CMB fluctuations. Well correlated to dust emission at 100 $\mu$m, the anomalous emission is interstellar but its origin is still debated. Some possible explanations relate it to dust: emission of spinning, small (nanometric) grains carrying a permanent electric dipole or magnetic fluctuations in larger (submicronic) grains. To probe the origin of the anomalous emission, we compare microwave data to dust IR emission and search for specific signatures predicted by models of spinning dust. For the anomalous emission, we use the 23 GHz all-sky map deduced from WMAP data by Miville-Deschenes et al. (2008). The dust emission is traced by IRAS data. Models show that spinning dust emission is little sensitive to the intensity of the radiation field (Go) for 10<nu<30 GHz while the corresponding mid-IR emission is proportional to Go. To test this behaviour in our comparison, we derive Go from the dust temperature maps of Schlegel et al. (1998). From all-sky maps, we show that the anomalous emission is better correlated to the emission of small grains (at 12 $\mu$m) than to that of big grains (at 100 $\mu$m). In addition we show that the former correlation is significantly improved when the 12 $\mu$m flux is divided by Go, as predicted by current models of spinning dust.Comment: 4 pages, 5 figures, accepted by A&

Serendipity observations of far infrared cirrus emission in the Spitzer Infrared Nearby Galaxies Survey: Analysis of far-infrared correlations

We present an analysis of far-infrared dust emission from diffuse cirrus clouds. This study is based on serendipitous observations at 160 microns at high galactic latitude with the Multiband Imaging Photometer (MIPS) onboard the Spitzer Space Telescope by the Spitzer Infrared Nearby Galaxies Survey (SINGS). These observations are complemented with IRIS data at 100 and 60 microns and constitute one of the most sensitive and unbiased samples of far infrared observations at small scale of diffuse interstellar clouds. Outside regions dominated by the cosmic infrared background fluctuations, we observe a substantial scatter in the 160/100 colors from cirrus emission. We compared the 160/100 color variations to 60/100 colors in the same fields and find a trend of decreasing 60/100 with increasing 160/100. This trend can not be accounted for by current dust models by changing solely the interstellar radiation field. It requires a significant change of dust properties such as grain size distribution or emissivity or a mixing of clouds in different physical conditions along the line of sight. These variations are important as a potential confusing foreground for extragalactic studies.Comment: 25 pages, 7 figures, 2 tables, accepted to Ap

Turbulence et instabilité thermique du milieu interstellaire atomique neutre (une approche numérique)

En Astrophysique, la compréhension du processus de formation d'étoiles reste l'une des principales questions. Elle est directement reliée à l'évolution du gaz interstellaire dans les galaxies, et en particulier aux processus de refroidissement et de condensation pour lesquels la turbulence et l'instabilité thermique jouent un rôle dominant. Ce travail se concentre sur l'évolution du gaz atomique et diffus qui fournit les conditions initiales à la formation des nuages moléculaires et se base sur une comparaison étroite entre observations à 21 cm et simulations numériques hydrodynamiques. Pour comprendre les rôles de l'instabilité thermique et de la turbulence dans la transition du gaz chaud (WNM, T ~ 8000 K, n = 0.5 cm- ) vers le gaz froid (CNM, T ~ 80 K, n = 50 cm- ), j'ai produit 90 simulations à basse résolution qui ont permis d'étudier l'influence de la densité initiale du WNM et de la compressibilité du forçage de la turbulence sur l'efficacité de la production de CNM. Un résultat important permet de conclure que le gaz chaud, dans les conditions de turbulence caractéristiques de ce qui est observé, ne transite pas vers le gaz froid quelque soit l'amplitude de la turbulence. Ces simulations à basse résolution ont aussi permis de déterminer quelles conditions initiales permettent de reproduire les propriétés déduites des observations telles que le nombre de Mach, la quantité de CNM en masse ou la dispersion de vitesse turbulente. Un processus de compression, que l'on peut reproduire soit en augmentant la densité initiale du WNM (n >= 1.5 cm- ) soit en appliquant un champ de forçage compressif, est nécessaire. Ces conditions initiales ont ensuite été utilisées pour produire deux simulations à haute résolution (1024 ) pour lesquelles j'ai montré que les propriétés de la turbulence et de l'instabilité du milieu atomique neutre sont bien reproduites. Les histogrammes de température portent en effet la trace d'un milieu biphasique et les distributions de pression sont semblables aux observations. D'autre part, les spectres de puissance de la densité sont caractéristiques d'un milieu fortement contrasté alors que ceux de la vitesse restent caractéristiques d'une turbulence subsonique. Finalement, les structures froides de ces deux simulations reproduisent les relations masse-échelle et dispersion de vitesse-échelle observées dans les nuages moléculaires, suggérant que la structure des nuages moléculaires pourrait être héritée de celle des nuages de HI à partir desquels ils se sont formés. Le dernier aspect de mon travail est relié à la difficulté rencontrée lors de l'interprétation des données qui n'est possible qu'à partir de grandeurs projetées en deux dimensions. J'ai donc comparé en détails les deux simulations à haute résolution à des observations de cirrus en créant des observations artificielles à 21 cm. Les spectres d'émission et les cartes de densité de colonne ainsi produits sont semblables aux observations. De plus, les simulations donnant accès à l'information en trois dimensions, j'ai étudié les effets de l'auto-absorption dans la création de cartes de densité de colonne à partir de spectres de température de brillance. J'ai conclu de cette étude que l'auto-absorption ne peut être négligée mais qu'elle ne concerne que les lignes de visée les plus brillantes et les plus denses et que la correction habituellement appliquée sur les observations est efficace. Finalement, j'ai appliqué une méthode de décomposition en gaussiennes sur les spectres synthétiques. Cette méthode a pour objectif d'étudier les propriétés de chacune des deux phases thermiques du HI. Les résultats montrent qu'elle est prometteuse pour l'analyse des données de spectro-imagerie à 21 cm, bien que nécessitant des améliorations. Elle permet en effet de bien séparer les phases chaude et froide du milieu atomique et d'en déduire la distribution massique de chacune d'elles.One of the main current questions in Astrophysics is the understanding of the star formation process, directly related to the processes involved in the cooling and the condensation of the gas yielding to intricate filamentary structures of molecular clouds. Thermal instability and turbulence are playing dominant roles in this complex dynamics. The work presented here is focused on the evolution of the atomic and diffuse interstellar medium that provides the initial conditions to the formation of molecular clouds and is based on the comparison of hydrodynamical numerical simulations and observations. To understand the roles of thermal instability and turbulence in the WNM (warm neutral medium, T ~ 8000 K, n = 0.5 cm- ) to CNM (cold neutral medium, T ~ 80 K, n = 50 cm- ) transition, I produced 90 hydrodynamical numerical simulations of thermally bistable HI and used them to study the impact of the WNM initial density and the compressibility of the turbulent stirring on the efficiency of the CNM production. The main result here is that the warm gas in the observed turbulent conditions do not transit naturally to cold gas whatever the amplitude of turbulent motions. These small resolution simulations also allowed me to determine which initial conditions lead to the reproduction of the observed properties, as the Mach number, the amount of CNM or the amplitude of the turbulent motions. A compression is needed to trigger this transition either by increasing the initial density (n >= 1.5 cm- ) or by stirring with a compressive field. These initial conditions have been used to produce two high resolution simulations (1024 ). I showed that these two simulations reproduce well the properties of the turbulence and the thermal instability. The temperature histograms present the evidences of a bistable gas and the pressure distributions are in agreement with the observations. On the other hand, the power spectra of the density are characteristic of a high contrasted medium while the power spectra of the velocity remain characteristic of subsonic turbulence. Finally the cold structures of these two simulations reproduce well the mass-size and velocity dispersion-size relations observed in molecular clouds. This suggests that the molecular cloud structure could be inherited from the clouds of atomic gas from which they are born. One of the main limitations in the analysis of observations comes from the fact that it can only be done on integrated quantities in two dimensions. In the last part of my work I compared the two high resolution simulations to observations by creating synthetic 21 cm observations. The emission spectra and column density maps produced in that way are similar to the ones observed. Besides, with the three dimensional informations, I was able to study the effect of the self-absorption in the creation of the column density maps from the brightness temperature spectra. I concluded from this study that the self-absorption cannot be neglected but that it only concerns the brightest and densest lines of sight and that the correction usually applied on observations is efficient. Finally I applied a method of gaussian decomposition on the synthetic spectra. This method has been build to study the properties of each thermal phase in the HI. The results show that it is a highly promising method for the analysis of 21 cm spectro-imaging data even if some improvements are needed. Indeed, it allows a good separation of the cold and warm phases of the atomic medium and a reasonable deduction of the massive distribution of each one.PARIS11-SCD-Bib. électronique (914719901) / SudocSudocFranceF

Identification of Protein Palmitoylation Inhibitors from a Scaffold Ranking Library

The addition of palmitoyl moieties to proteins regulates their membrane targeting, subcellular localization, and stability. Dysregulation of the enzymes which catalyzed the palmitoyl addition and/or the substrates of these enzymes have been linked to cancer, cardiovascular, and neurological disorders, implying these enzymes and substrates are valid targets for pharmaceutical intervention. However, current chemical modulators of zDHHC PAT enzymes lack specificity and affinity, underscoring the need for screening campaigns to identify new specific, high affinity modulators. This report describes a mixture based screening approach to identify inhibitors of Erf2 activity. Erf2 is the Saccharomyces cerevisiae PAT responsible for catalyzing the palmitoylation of Ras2, an ortholog of the human Ras oncogene proteins. A chemical library developed by the Torrey Pines Institute for Molecular Studies consists of more than 30 million compounds designed around 68 molecular scaffolds that are systematically arranged into positional scanning and scaffold ranking formats. We have used this approach to identify and characterize several scaffold backbones and R-groups that reduce or eliminate the activity of Erf2 in vitro. Here, we present the analysis of one of the scaffold backbones, bis-cyclic piperazine. We identified compounds that inhibited Erf2 auto-palmitoylation activity using a fluorescence-based, coupled assay in a high throughput screening (HTS) format and validated the hits utilizing an orthogonal gel-based assay. Finally, we examined the effects of the compounds on cell growth in a yeast cell-based assay. Based on our results, we have identified specific, high affinity palmitoyl transferase inhibitors that will serve as a foundation for future compound design

Galactic and Magellanic Evolution with the SKA

As we strive to understand how galaxies evolve it is crucial that we resolve physical processes and test emerging theories in nearby systems that we can observe in great detail. Our own Galaxy, the Milky Way, and the nearby Magellanic Clouds provide unique windows into the evolution of galaxies, each with its own metallicity and star formation rate. These laboratories allow us to study with more detail than anywhere else in the Universe how galaxies acquire fresh gas to fuel their continuing star formation, how they exchange gas with the surrounding intergalactic medium, and turn warm, diffuse gas into molecular clouds and ultimately stars. The $\lambda$21-cm line of atomic hydrogen (HI) is an excellent tracer of these physical processes. With the SKA we will finally have the combination of surface brightness sensitivity, point source sensitivity and angular resolution to transform our understanding of the evolution of gas in the Milky Way, all the way from the halo down to the formation of individual molecular clouds.Comment: 25 pages, from "Advancing Astrophysics with the Square Kilometre Array", to appear in Proceedings of Scienc

Hepatic steatosis progresses faster in HIV mono-infected than HIV/HCV co-infected patients and is associated with liver fibrosis

Background & Aims Hepatic steatosis (HS) seems common in patients infected with human immunodeficiency virus (HIV). However, the relative effect of HIV, as well as hepatitis C virus (HCV) in those co-infected, and the influence of HS on liver fibrosis progression are unclear. Methods The LIVEr disease in HIV (LIVEHIV) is a Canadian prospective Cohort using transient elastography and associated controlled attenuation parameter (CAP) to screen for HS and liver fibrosis in unselected HIV-infected adults. HS progression was defined as development of any grade HS (CAP ≥248 dB/m), or transition to severe HS (CAP ≥292 dB/m) for those with any grade HS at baseline. Fibrosis progression was defined as development of significant liver fibrosis (liver stiffness measurement [LSM] ≥7.1kPa), or transition to cirrhosis (LSM ≥12.5kPa) for those with significant liver fibrosis at baseline. Cox regression analysis was used to assess predictors of HS and fibrosis progression. Results A prospective cohort study was conducted, which included 726 HIV-infected patients (22.7% HCV co-infected). Prevalence of any grade HS did not differ between HIV mono-infected and HIV/HCV co-infected patients (36.1% vs 38.6%, respectively). 313 patients were followed for a median of 15.4 (interquartile range 8.5-23.0) months. The rate of HS progression was 37.8 (95% confidence interval [CI] 29.2-49.0) and 21.9 (95% CI 15.6-30.7) per 100 person-years in HIV mono-infection and HIV/HCV co-infection, respectively. HCV co-infection was an independent negative predictor of HS progression (adjusted hazard ratio [aHR] 0.50, 95% CI 0.28-0.89). HS predicted liver fibrosis progression in HIV mono-infection (aHR 4.18, 95% CI 1.21-14.5), but not in HIV/HCV co-infection. Conclusion HS progresses faster and is associated with liver fibrosis progression in HIV mono-infection but not in HIV/HCV co-infection

Two-Tier Care Pathways for Liver Fibrosis Associated to Non-Alcoholic Fatty Liver Disease in HIV Mono-Infected Patients

(1) Background: Developing strategies to identify significant liver fibrosis in people with HIV (PWH) is crucial to prevent complications of non-alcoholic fatty liver disease (NAFLD). We aim to investigate if five simple serum biomarkers applied to PWH can optimize a care pathway to identify significant liver fibrosis defined by transient elastography (TE). (2) Methods: A two-tier fibrosis pathway was applied to three prospective cohorts of PWH undergoing TE with CAP. NAFLD was diagnosed as a controlled attenuation parameter ≥ 248 dB/m. Five simple fibrosis biomarkers (FIB-4 < 1.3, BARD score 0–1, NAFLD fibrosis score < −1.455, AST:ALT ratio < 0.8 and APRI < 0.5) were applied as first-tiers to exclude significant liver fibrosis. We determined the decrease in referral for TE that would have occurred based on biomarker assessment and the discordance between low simple fibrosis biomarkers and high TE (≥7.1 kPa), indicating significant liver fibrosis. (3) Results: Of the 1749 consecutive PWH, 15.1% had significant liver fibrosis by TE and 39.1% had NAFLD. The application of the fibrosis biomarkers as first tiers would have resulted in a decrease in TE referrals between 24.9% (BARD score) and 86.3% (APRI). The lowest discordance rate was with NAFLD fibrosis score (8.5%). After adjustments, BMI (odds ratio (OR) 1.12, 95% CI: 1.08–1.17) and triglycerides (OR 1.26, 95% CI: 1.11–1.44) were independent predictors of discordance for APRI < 0.5 and TE ≥ 7.1. The performance of the two-tier pathways was similar in PWH with and without NAFLD. (4) Conclusions: Implementing a two-tier pathway could save a substantial proportion up of TE examinations, reducing costs and helping resource optimization in HIV care. Patients with metabolic risk factors for NAFLD and low fibrosis biomarker may still be considered for TE referral