L’accessibilité aérienne comme clé de compréhension de la dépendance économique au tourisme des espaces insulaires. Exemple des Maldives, des Seychelles, de l’île Maurice et de l’île de la Réunion

Très tôt, le tourisme est apparu comme la solution la plus pertinente pour instaurer une croissance dynamique et permettre le développement des petits espaces insulaires. Les études empiriques ont fait apparaître un lien positif significatif entre les recettes touristiques et la croissance du PIB pour les petites économies insulaires touristiques. De manière plus précise, « la stratégie touristique pourrait-elle être un facteur de développement durable pour les petites économies insulaires ?

A 1-Year Prospective French Nationwide Study of Emergency Hospital Admissions in Children and Adults with Primary Immunodeficiency.

PURPOSE: Patients with primary immunodeficiency (PID) are at risk of serious complications. However, data on the incidence and causes of emergency hospital admissions are scarce. The primary objective of the present study was to describe emergency hospital admissions among patients with PID, with a view to identifying "at-risk" patient profiles. METHODS: We performed a prospective observational 12-month multicenter study in France via the CEREDIH network of regional PID reference centers from November 2010 to October 2011. All patients with PIDs requiring emergency hospital admission were included. RESULTS: A total of 200 admissions concerned 137 patients (73 adults and 64 children, 53% of whom had antibody deficiencies). Thirty admissions were reported for 16 hematopoietic stem cell transplantation recipients. When considering the 170 admissions of non-transplant patients, 149 (85%) were related to acute infections (respiratory tract infections and gastrointestinal tract infections in 72 (36%) and 34 (17%) of cases, respectively). Seventy-seven percent of the admissions occurred during winter or spring (December to May). The in-hospital mortality rate was 8.8% (12 patients); death was related to a severe infection in 11 cases (8%) and Epstein-Barr virus-induced lymphoma in 1 case. Patients with a central venous catheter (n = 19, 13.9%) were significantly more hospitalized for an infection (94.7%) than for a non-infectious reason (5.3%) (p = 0.04). CONCLUSION: Our data showed that the annual incidence of emergency hospital admission among patients with PID is 3.4%. The leading cause of emergency hospital admission was an acute infection, and having a central venous catheter was associated with a significantly greater risk of admission for an infectious episode

The ‘Coral Bulker’ Fuel Oil Spill on the North Coast of Portugal: Spatial and Temporal Biomarker Responses in Mytilus galloprovincialis

In December 2000, the ship ‘Coral Bulker’ ran aground at the entrance of the port of Viana do Castelo (North–west coast of Portugal). A large amount of fuel oil was spilled and part of it reached the shore. To evaluate the spatial and temporal impact of this oil spill, a field study, and several laboratory toxicity tests were performed using Mytilus galloprovincialis as biological indicator of environmental contamination and the biomarkers glutathione S-transferases (GSTs) and acetylcholinesterase (AChE) as indicative criteria. Fifteen days after the oil spill, mussels collected at stations located near the ship presented higher and lower values of GSTs and AChE activity, respectively. These results, and those obtained in the laboratory toxicity tests, evidence that these biomarkers were sensitive indicators of exposure to this kind of pollution and were able to monitor a spatial impact of the oil spill of at least 10 km, confirming the higher level of contamination near the ship and a contamination gradient along the sampling stations. One year after the accident, such a contamination gradient was no longer evident. This study highlight the potential suitability of a biomarker approach for assessing spatial and temporal impacts of marine pollution accidents, such as fuel oil spills, suggesting the inclusion of these biomarkers in risk assessment studies, as cost-effective and early warning recognized tools. Major advantages and limitations of the biomarker approach used in this study are further discussed

CONCERTO: Extracting the power spectrum of the [C II ] emission line

International audienceCONCERTO is the first experiment to perform a [CII] line intensity mapping survey to target $z>5.2$. Measuring the [CII] power spectrum allows us to study the role of dusty star-forming galaxies in the star formation history during the Reionization and post-Reionization. The main obstacle to this measurement is the contamination by bright foregrounds. We evaluate our ability to retrieve the [CII] signal in mock observations using the Simulated Infrared Dusty Extragalactic Sky. We compared two methods for dealing with the dust continuum emission from galaxies: the standard PCA and the arPLS method. For line interlopers, the strategy relies on masking low-redshift galaxies using external catalogues. As we do not have observations of CO or classical CO proxies ,we relied on the COSMOS stellar mass catalogue. To measure the power spectrum of masked data, we adapted the P of K EstimatoR and discuss its use on LIM data. The arPLS method achieves a reduction of the continuum background to a sub-dominant level of the [CII] at z=7 by a factor of>70. When using PCA, this factor is only 0.7. The masking lowers the power amplitude of line contamination down to $2 \times 10^2 Jy^2/sr$ This residual level is dominated by faint undetected sources. For our [CII] model, this results in a detection at z = 5.2 with a power ratio [CII]/(residual interlopers) = $62 \pm 32$ for a 22 % area survey loss. However, at z = 7, [C II ] / (residual interlopers)$=2.0 \pm 1.4$. Thanks to the large area covered by SIDES-Uchuu, we show that the power amplitude of line residuals varies by 12-15% for z=5.2-7. We present an end-to-end simulation of the extragalactic foreground removal that we ran to detect the [CII] at high redshift via its power spectrum. We show that dust continuum emission are not a limiting foreground for [CII] LIM. Residual CO and [CI] limits our ability to measure the [CII] power spectrum at z>7

CONCERTO: Extracting the power spectrum of the [C II ] emission line

International audienceCONCERTO is the first experiment to perform a [CII] line intensity mapping survey to target $z>5.2$. Measuring the [CII] power spectrum allows us to study the role of dusty star-forming galaxies in the star formation history during the Reionization and post-Reionization. The main obstacle to this measurement is the contamination by bright foregrounds. We evaluate our ability to retrieve the [CII] signal in mock observations using the Simulated Infrared Dusty Extragalactic Sky. We compared two methods for dealing with the dust continuum emission from galaxies: the standard PCA and the arPLS method. For line interlopers, the strategy relies on masking low-redshift galaxies using external catalogues. As we do not have observations of CO or classical CO proxies ,we relied on the COSMOS stellar mass catalogue. To measure the power spectrum of masked data, we adapted the P of K EstimatoR and discuss its use on LIM data. The arPLS method achieves a reduction of the continuum background to a sub-dominant level of the [CII] at z=7 by a factor of>70. When using PCA, this factor is only 0.7. The masking lowers the power amplitude of line contamination down to $2 \times 10^2 Jy^2/sr$ This residual level is dominated by faint undetected sources. For our [CII] model, this results in a detection at z = 5.2 with a power ratio [CII]/(residual interlopers) = $62 \pm 32$ for a 22 % area survey loss. However, at z = 7, [C II ] / (residual interlopers)$=2.0 \pm 1.4$. Thanks to the large area covered by SIDES-Uchuu, we show that the power amplitude of line residuals varies by 12-15% for z=5.2-7. We present an end-to-end simulation of the extragalactic foreground removal that we ran to detect the [CII] at high redshift via its power spectrum. We show that dust continuum emission are not a limiting foreground for [CII] LIM. Residual CO and [CI] limits our ability to measure the [CII] power spectrum at z>7

CONCERTO: Extracting the power spectrum of the [C II ] emission line

International audienceCONCERTO is the first experiment to perform a [CII] line intensity mapping survey to target $z>5.2$. Measuring the [CII] power spectrum allows us to study the role of dusty star-forming galaxies in the star formation history during the Reionization and post-Reionization. The main obstacle to this measurement is the contamination by bright foregrounds. We evaluate our ability to retrieve the [CII] signal in mock observations using the Simulated Infrared Dusty Extragalactic Sky. We compared two methods for dealing with the dust continuum emission from galaxies: the standard PCA and the arPLS method. For line interlopers, the strategy relies on masking low-redshift galaxies using external catalogues. As we do not have observations of CO or classical CO proxies ,we relied on the COSMOS stellar mass catalogue. To measure the power spectrum of masked data, we adapted the P of K EstimatoR and discuss its use on LIM data. The arPLS method achieves a reduction of the continuum background to a sub-dominant level of the [CII] at z=7 by a factor of>70. When using PCA, this factor is only 0.7. The masking lowers the power amplitude of line contamination down to $2 \times 10^2 Jy^2/sr$ This residual level is dominated by faint undetected sources. For our [CII] model, this results in a detection at z = 5.2 with a power ratio [CII]/(residual interlopers) = $62 \pm 32$ for a 22 % area survey loss. However, at z = 7, [C II ] / (residual interlopers)$=2.0 \pm 1.4$. Thanks to the large area covered by SIDES-Uchuu, we show that the power amplitude of line residuals varies by 12-15% for z=5.2-7. We present an end-to-end simulation of the extragalactic foreground removal that we ran to detect the [CII] at high redshift via its power spectrum. We show that dust continuum emission are not a limiting foreground for [CII] LIM. Residual CO and [CI] limits our ability to measure the [CII] power spectrum at z>7

CONCERTO: Extracting the power spectrum of the [C II ] emission line

International audienceCONCERTO is the first experiment to perform a [CII] line intensity mapping survey to target $z>5.2$. Measuring the [CII] power spectrum allows us to study the role of dusty star-forming galaxies in the star formation history during the Reionization and post-Reionization. The main obstacle to this measurement is the contamination by bright foregrounds. We evaluate our ability to retrieve the [CII] signal in mock observations using the Simulated Infrared Dusty Extragalactic Sky. We compared two methods for dealing with the dust continuum emission from galaxies: the standard PCA and the arPLS method. For line interlopers, the strategy relies on masking low-redshift galaxies using external catalogues. As we do not have observations of CO or classical CO proxies ,we relied on the COSMOS stellar mass catalogue. To measure the power spectrum of masked data, we adapted the P of K EstimatoR and discuss its use on LIM data. The arPLS method achieves a reduction of the continuum background to a sub-dominant level of the [CII] at z=7 by a factor of>70. When using PCA, this factor is only 0.7. The masking lowers the power amplitude of line contamination down to $2 \times 10^2 Jy^2/sr$ This residual level is dominated by faint undetected sources. For our [CII] model, this results in a detection at z = 5.2 with a power ratio [CII]/(residual interlopers) = $62 \pm 32$ for a 22 % area survey loss. However, at z = 7, [C II ] / (residual interlopers)$=2.0 \pm 1.4$. Thanks to the large area covered by SIDES-Uchuu, we show that the power amplitude of line residuals varies by 12-15% for z=5.2-7. We present an end-to-end simulation of the extragalactic foreground removal that we ran to detect the [CII] at high redshift via its power spectrum. We show that dust continuum emission are not a limiting foreground for [CII] LIM. Residual CO and [CI] limits our ability to measure the [CII] power spectrum at z>7

KISS: a spectrometric imager for millimetre cosmology

International audienceClusters of galaxies are used to map the large-scale structures in the universe and as probe of universe evolution. They can be observed through the Sunyaev-Zel’dovich (SZ) effect. In this respect the spectro-imaging at low resolution frequency is an important tool, today, for the study of cluster of galaxies. We have developed KISS (KIDs Interferometer Spectrum Survey), a spectrometric imager dedicated to the secondary anisotropies of the Cosmic Microwave Background (CMB). The multi-frequency approach permits to improve the component separation with respect to predecessor experiments. In this paper, firstly, we provide a description of the scientific context and the state of the art of SZ observations. Secondly, we describe the KISS instrument. Finally, we show preliminary results of the ongoing commissioning campaign

KISS: a spectrometric imager for millimetre cosmology

Clusters of galaxies are used to map the large-scale structures in the universe and as probe of universe evolution. They can be observed through the Sunyaev-Zel’dovich (SZ) effect. In this respect the spectro-imaging at low resolution frequency is an important tool, today, for the study of cluster of galaxies. We have developed KISS (KIDs Interferometer Spectrum Survey), a spectrometric imager dedicated to the secondary anisotropies of the Cosmic Microwave Background (CMB). The multi-frequency approach permits to improve the component separation with respect to predecessor experiments. In this paper, firstly, we provide a description of the scientific context and the state of the art of SZ observations. Secondly, we describe the KISS instrument. Finally, we show preliminary results of the ongoing commissioning campaign

CONCERTO: Simulating the CO, [CII], and [CI] line emission of galaxies in a 117 deg2\rm deg^2 field and the impact of field-to-field variance

In the submm regime, spectral line scans and line intensity mapping (LIM) are new promising probes for the cold gas content and star formation rate of galaxies across cosmic time. However, both of these two measurements suffer from field-to-field variance. We study the effect of field-to-field variance on the predicted CO and [CII] power spectra from future LIM experiments such as CONCERTO, as well as on the line luminosity functions (LFs) and the cosmic molecular gas mass density that are currently derived from spectral line scans. We combined a 117 $\rm deg^2$ dark matter lightcone from the Uchuu cosmological simulation with the simulated infrared dusty extragalactic sky (SIDES) approach. We find that in order to constrain the CO LF with an uncertainty below 20%, we need survey sizes of at least 0.1 $\rm deg^2$. Furthermore, accounting for the field-to-field variance using only the Poisson variance can underestimate the total variance by up to 80%. The lower the luminosity is and the larger the survey size is, the higher the level of underestimate. At $z$3$the variance decreases more slowly with survey size and for example drops below 10$^2$fields. Finally, we find that the CO and [CII] LIM power spectra can vary by up to 50$\rm 1 deg^2$fields. This limits the accuracy of the constraints provided by the first 1 deg$^2$ surveys. The level of the shot noise power is always dominated by the sources that are just below the detection thresholds. We provide an analytical formula to estimate the field-to-field variance of current or future LIM experiments. The code and the full SIDES-Uchuu products (catalogs, cubes, and maps) are publicly available