SPIRE Map-Making Test Report

The photometer section of SPIRE is one of the key instruments on board of Herschel. Its legacy depends very much on how well the scanmap observations that it carried out during the Herschel mission can be converted to high quality maps. In order to have a comprehensive assessment on the current status of SPIRE map-making, as well as to provide guidance for future development of the SPIRE scan-map data reduction pipeline, we carried out a test campaign on SPIRE map-making. In this report, we present results of the tests in this campaign.Comment: This document has an executive summary, 6 chapters, and 102 pages. More information can be found at: https://nhscsci.ipac.caltech.edu/sc/index.php/Spire/SPIREMap-MakingTest201

The emission by dust and stars of nearby galaxies in the Herschel KINGFISH survey

Using new far-infrared imaging from the Herschel Space Observatory with ancillary data from ultraviolet (UV) to submillimeter wavelengths, we estimate the total emission from dust and stars of 62 nearby galaxies in the KINGFISH survey in a way that is as empirical and model independent as possible. We collect and exploit these data in order to measure from the spectral energy distributions (SEDs) precisely how much stellar radiation is intercepted and re-radiated by dust, and how this quantity varies with galaxy properties. By including SPIRE data, we are more sensitive to emission from cold dust grains than previous analyses at shorter wavelengths, allowing for more accurate estimates of dust temperatures and masses. The dust/stellar flux ratio, which we measure by integrating the SEDs, has a range of nearly three decades (from 10(-2.2) to 10(0.5)). The inclusion of SPIRE data shows that estimates based on data not reaching these far-IR wavelengths are biased low by 17% on average. We find that the dust/stellar flux ratio varies with morphology and total infrared (IR) luminosity, with dwarf galaxies having faint luminosities, spirals having relatively high dust/stellar ratios and IR luminosities, and some early types having low dust/stellar ratios. We also find that dust/stellar flux ratios are related to gas-phase metallicity ((log(f(dust)/f(*)) over bar) = -0.66 +/- 0.08 and -0.22 +/- 0.12 for metal-poor and intermediate-metallicity galaxies, respectively), while the dust/stellar mass ratios are less so (differing by approximate to 0.2 dex); the more metal-rich galaxies span a much wider range of the flux ratios. In addition, the substantial scatter between dust/stellar flux and dust/stellar mass indicates that the former is a poor proxy of the latter. Comparing the dust/stellar flux ratios and dust temperatures, we also show that early types tend to have slightly warmer temperatures (by up to 5 K) than spiral galaxies, which may be due to more intense interstellar radiation fields, or possibly to different dust grain compositions. Finally, we show that early types and early-type spirals have a strong correlation between the dust/stellar flux ratio and specific star formation rate, which suggests that the relatively bright far-IR emission of some of these galaxies is due to ongoing (if limited) star formation as well as to the radiation field from older stars, which is heating the dust grains

Risk stratification in heart failure decompensation in the community: HEFESTOS score

Aims: Because evidence regarding risk stratification predicting prognosis of patients with heart failure (HF) decompensation attended in primary care is lacking, we developed and externally validated a model to forecast death/hospitalization during the first 30 days after an episode of decompensation. The predictive model is based on variables easily obtained in primary care settings. Methods and results: HEFESTOS is a multinational study consisting of a derivation cohort of HF patients recruited in 14 primary healthcare centres in Barcelona and a validation cohort from primary healthcare in 9 other European countries. The derivation and validation cohorts included 561 and 250 patients, respectively. Percentages of women in the derivation and validation cohorts were 56.3% and 47.6% (P = 0.026), respectively. Mean age was 82.2 years (SD 8.03) in the derivation cohort, and 79.3 years (SD 10.3) in the validation one (P = 0.001). HF with preserved ejection fraction represented 72.1% in the derivation cohort and 58.8% in the validation one (P = 0.004). Mortality/hospitalization during the first 30 days after a decompensation episode was 30.5% and 26% (P = 0.225) for the derivation and validation cohorts, respectively. Multivariable logistic regression models were performed to develop a score of risk. The identified predictors were worsening of dyspnoea [odds ratio (OR): 2.5; P = 0.001], orthopnoea (OR: 2.16; P = 0.01), paroxysmal nocturnal dyspnoea (OR: 2.25; P = 0.01), crackles (OR: 2.35; P = 0.01), New York Heart Association functional class III/IV (OR: 2.11; P = 0.001), oxygen saturation ≤ 90% (OR: 4.98; P 100 b.p.m. (OR: 2.72; P = 0.002), and previous hospitalization due to HF (OR: 2.45; P 20%. Outcome incidence was 2.7% for the low-risk group, 12.8% for medium risk, and 46.2% for high risk in the derivation cohort, and 9.1%, 12.9%, and 39.6% in the validation one. Conclusions: The HEFESTOS score, based on variables easily accessible in a community setting and validated in an external European cohort, properly predicted the risk of death/hospitalization during the first 30 days after an HF decompensation episode

Warm Dust and Spatially Variable PAH Emission in the Dwarf Starburst Galaxy NGC 1705

We present Spitzer observations of the dwarf starburst galaxy NGC 1705 obtained as part of SINGS. The galaxy morphology is very different shortward and longward of ~5 microns: short-wavelength imaging shows an underlying red stellar population, with the central super star cluster (SSC) dominating the luminosity; longer-wavelength data reveals warm dust emission arising from two off-nuclear regions offset by ~250 pc from the SSC. These regions show little extinction at optical wavelengths. The galaxy has a relatively low global dust mass (~2E5 solar masses, implying a global dust-to-gas mass ratio ~2--4 times lower than the Milky Way average). The off-nuclear dust emission appears to be powered by photons from the same stellar population responsible for the excitation of the observed H Alpha emission; these photons are unassociated with the SSC (though a contribution from embedded sources to the IR luminosity of the off-nuclear regions cannot be ruled out). Low-resolution IRS spectroscopy shows moderate-strength PAH emission in the 11.3 micron band in the eastern peak; no PAH emission is detected in the SSC or the western dust emission complex. There is significant diffuse 8 micron emission after scaling and subtracting shorter wavelength data; the spatially variable PAH emission strengths revealed by the IRS data suggest caution in the interpretation of diffuse 8 micron emission as arising from PAH carriers alone. The metallicity of NGC 1705 falls at the transition level of 35% solar found by Engelbracht and collaborators; the fact that a system at this metallicity shows spatially variable PAH emission demonstrates the complexity of interpreting diffuse 8 micron emission. A radio continuum non-detection, NGC 1705 deviates significantly from the canonical far-IR vs. radio correlation. (Abridged)Comment: ApJ, in press; please retrieve full-resolution version from http://www.astro.wesleyan.edu/~cannon/pubs.htm

The Nature of Infrared Emission in the Local Group Dwarf Galaxy NGC 6822 As Revealed by Spitzer

We present Spitzer imaging of the metal-deficient (Z ~30% Z_sun) Local Group dwarf galaxy NGC 6822. On spatial scales of ~130 pc, we study the nature of IR, H alpha, HI, and radio continuum emission. Nebular emission strength correlates with IR surface brightness; however, roughly half of the IR emission is associated with diffuse regions not luminous at H alpha (as found in previous studies). The global ratio of dust to HI gas in the ISM, while uncertain at the factor of ~2 level, is ~25 times lower than the global values derived for spiral galaxies using similar modeling techniques; localized ratios of dust to HI gas are about a factor of five higher than the global value in NGC 6822. There are strong variations (factors of ~10) in the relative ratios of H alpha and IR flux throughout the central disk; the low dust content of NGC 6822 is likely responsible for the different H alpha/IR ratios compared to those found in more metal-rich environments. The H alpha and IR emission is associated with high-column density (> ~1E21 cm^-2) neutral gas. Increases in IR surface brightness appear to be affected by both increased radiation field strength and increased local gas density. Individual regions and the galaxy as a whole fall within the observed scatter of recent high-resolution studies of the radio-far IR correlation in nearby spiral galaxies; this is likely the result of depleted radio and far-IR emission strengths in the ISM of this dwarf galaxy.Comment: ApJ, in press; please retrieve full-resolution version from http://www.astro.wesleyan.edu/~cannon/pubs.htm

Spitzer and JCMT Observations of the Active Galactic Nucleus in the Sombrero Galaxy (NGC 4594)

We present Spitzer 3.6-160 micron images, Spitzer mid-infrared spectra, and JCMT SCUBA 850 micron images of the Sombrero Galaxy (NGC 4594), an Sa galaxy with a 10^9 M_solar low luminosity active galactic nucleus (AGN). The brightest infrared sources in the galaxy are the nucleus and the dust ring. The spectral energy distribution of the AGN demonstrates that, while the environment around the AGN is a prominent source of mid-infrared emission, it is a relatively weak source of far-infrared emission, as had been inferred for AGN in previous research. The weak nuclear 160 micron emission and the negligible polycyclic aromatic hydrocarbon emission from the nucleus also implies that the nucleus is a site of only weak star formation activity and the nucleus contains relatively little cool interstellar gas needed to fuel such activity. We propose that this galaxy may be representative of a subset of low ionization nuclear emission region galaxies that are in a quiescent AGN phase because of the lack of gas needed to fuel circumnuclear star formation and Seyfert-like AGN activity. Surprisingly, the AGN is the predominant source of 850 micron emission. We examine the possible emission mechanisms that could give rise to the 850 micron emission and find that neither thermal dust emission, CO line emission, bremsstrahlung emission, nor the synchrotron emission observed at radio wavelengths can adequately explain the measured 850 micron flux density by themselves. The remaining possibilities for the source of the 850 micron emission include a combination of known emission mechanisms, synchrotron emission that is self-absorbed at wavelengths longer than 850 microns, or unidentified spectral lines in the 850 micron band.Comment: Accepted to ApJ, 200

Biodiversitet implementert i landskapsarkitektur : et prosjekteksempel fra Asker sentrum

Norsk: Mer enn halvparten av jordens befolkning bor i urbane områder og tallet øker kraftig. Samtidig er vi vitner til den største utryddelsen av arter siden dinosaurene døde ut for 65 millioner år siden. Det er i hovedsak menneskelig aktivitet som truer det biologiske mangfoldet gjennom tap, forringelse og fragmentering av habitat. Urbanisering og fortetting reduserer fragmentering av habitat, men dette går ofte på bekostning av grøntområdene. Denne oppgaven utforsker muligheter for å ivareta biologisk mangfold i et presset urbant område. Tematikken er høyst akuell, men får for lite oppmerksomhet innen fagfeltet landskapsarkitektur til tross for landskapsarkitekters posisjon til direkte påvirkning av omgivelsene. Oppgaven presenterer først anvendt kunnskap om biodiversitet i urbane områder, og deretter omsettes kunnskapen til en verktøykasse bestående av fem deler: landskapsøkologiske prinsipper, menneskers preferanser i forhold til urban natur, tiltak for biodiversitet, artsvalg og vegetasjonsmodeller. Her legges det frem konkrete funn som ulike planters betydning for andre arter og hvordan man kan tilrettelegge for biodiversitet i grøntanlegg. Videre følger en analyse av Asker kommune før verktøykassen anvendes konseptuelt på prosjekteksempelet Asker sentrum. Avslutningsvis følger en diskusjon av oppgaven med hensyn på problemstillingen der det påpekes en brist i kunnskapsformidling samt nødvendigheten av større grad av tverrfaglig samarbeid. English: More than half of the world’s population is now living in urban areas and the number is constantly increasing. At the same time we are witnessing the greatest extinction of species since the dinosaurs died 65million years ago. It is mainly human activity that is causing this threat to loss of biodiversity through loss, degrading and fragmentation of habitat. Urbanization and densification reduces fragmentation of habitat, but this is often at the expence of the green areas. This thesis is exploring how to maintain biodiversity in urban areas under pressure. The topic is highly relevant, but rarely receive attention within the field of landscape architecture, despite the landscape architects position to directly shape the environments. The thesis first presents utilized knowledge on biodiversity in urban areas and then the knowledge is put into a toolbox divided into five parts: landscape ecological principles, human preferences in urban nature, measures to enhance biodiversity, selection of species and models of vegetation. Here it is presented specific findings like plants different significance for other species and how to enhance biodiversity in a green area. Afterwards comes an analysis of Asker municipality before the toolbox is applied conceptually in the case study in Asker center. At the end follows a discussion of the whole thesis focused on the research question, where a shortcoming is addressed in the flow of knowledge, in addition to the necessity of greater interdisciplinary collaboration

Emission en infrarouge moyen des poussières dans les galaxies spirales : liens avec la formation d'étoiles et avec la dynamique des galaxies barrées

The dust emission of a sample of 69 nearby spiral galaxies was studied through observations with the ISOCAM camera between 5 and 18 microns, comprising maps in two broadband filters allowing a morphological study and five low-resolution spectra, used to identify and separate the different emission components. The usefulness of two dust species as indicators of the star formation rate was established over five orders of magnitude in star formation rate density, together with the appropriate validity limits. The properties of strongly barred galaxies were also compared to those of weakly or non-barred galaxies and interpreted in the frame of hydrodynamical models. Physical parameters regulating mid-infrared color variations were extracted and discussed.Un échantillon de 69 galaxies spirales proches a été étudié à travers l'émission de la poussière, observée par la caméra ISOCAM entre 5 et 18 microns. Les cartes complètes dans deux filtres larges, permettant une étude morphologique, ainsi que cinq spectres à basse résolution, utiles pour identifier et séparer les différentes composantes d'émission, ont été analysés. Des régions circumnucléaires de 1 à 4 kpc de diamètre, où le régime de chauffage de la poussière est distinct de celui des disques, ont été isolées.La validité de l'émission en infrarouge moyen en tant que traceur de la formation d'étoiles a d'abord été examinée dans les disques, où une seule phase de poussière domine (les porteurs des bandes aromatiques), puis cette étude a été étendue aux régionscircumnucléaires, plus denses et actives, ainsi qu'à des galaxies à flambée de formation d'étoiles, où un continuum thermique se superpose aux bandes aromatiques. La réponse de la poussière à la formation d'étoiles a été explorée sur cinq ordres de grandeur.Par ailleurs, les propriétés des galaxies fortement barrées ont été comparées à celles des galaxies faiblement ou non barrées, et interprétées dans le cadre des modèles hydrodynamiques, qui prévoient qu'un potentiel gravitationnel barré peut induire des écoulements de gaz massifs vers les régions centrales, avec des conséquences indirectes sur l'activité stellaire et l'évolution morphologique des galaxies isolées. Au cours de cette étude, quelques paramètres régulant les variations des couleurs en infrarouge moyen ont été mis en relief