331 research outputs found
Client-Side Cornucopia : Comparing the Built-In Application Architecture Models in the Web Browser
Peer reviewe
Fe/Co Alloys for the Catalytic Chemical Vapor Deposition Synthesis of Single- and Double-Walled Carbon Nanotubes (CNTs). 1. The CNT−Fe/Co−MgO System
Mg0.90FexCoyO (x + y ) 0.1) solid solutions were synthesized by the ureic combustion route. Upon reduction at 1000 °C in H2-CH4 of these powders, Fe/Co alloy nanoparticles are formed, which are involved in the formation of carbon nanotubes, which are mostly single and double walled, with an average diameter close to 2.5 nm. Characterizations of the materials are performed using 57Fe Mo¨ssbauer spectroscopy and electron microscopy, and a well-established macroscopic method, based on specific-surface-area measurements, was applied to quantify the carbon quality and the nanotubes quantity. A detailed investigation of the Fe/Co alloys’ formation and composition is reported. An increasing fraction of Co2+ ions hinders the dissolution of iron in the MgO lattice and favors the formation of MgFe2O4-like particles in the oxide powders. Upon reduction, these particles form R-Fe/Co particles with a size and composition (close to Fe0.50Co0.50) adequate for the increased production of carbon nanotubes. However, larger particles are also produced resulting in the formation of undesirable carbon species. The highest CNT quantity and carbon quality are eventually obtained upon reduction of the iron-free Mg0.90Co0.10O solid solution, in the absence of clusters of metal ions in the starting material. Introduction Catalyti
A Study of Heating and Cooling of the ISM in NGC 1097 with Herschel-PACS and Spitzer-IRS
NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst
ring, a strong large-scale bar and an active nucleus. We present a detailed
study of the spatial variation of the far infrared (FIR) [CII]158um and
[OI]63um lines and mid-infrared H2 emission lines as tracers of gas cooling,
and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the
photoelectric heating, using Herschel-PACS, and Spitzer-IRS infrared spectral
maps. We focus on the nucleus and the ring, and two star forming regions (Enuc
N and Enuc S). We estimated a photoelectric gas heating efficiency
([CII]158um+[OI]63um)/PAH in the ring about 50% lower than in Enuc N and S. The
average 11.3/7.7um PAH ratio is also lower in the ring, which may suggest a
larger fraction of ionized PAHs, but no clear correlation with
[CII]158{\mu}m/PAH(5.5 - 14um) is found. PAHs in the ring are responsible for a
factor of two more [CII]158um and [OI]63um emission per unit mass than PAHs in
the Enuc S. SED modeling indicates that at most 25% of the FIR power in the
ring and Enuc S can come from high intensity photodissociation regions (PDRs),
in which case G0 ~ 10^2.3 and nH ~ 10^3.5 cm^-3 in the ring. For these values
of G0 and nH PDR models cannot reproduce the observed H2 emission. Much of the
the H2 emission in the starburst ring could come from warm regions in the
diffuse ISM that are heated by turbulent dissipation or shocks.Comment: 17 pages, 14 figures, 5 tables; accepted for publication in Ap
Observations of Ultraluminous Infrared Galaxies with the Infrared Spectrograph on the Spitzer Space Telescope: Early Results on Mrk 1014, Mrk 463, and UGC 5101
We present spectra taken with the Infrared Spectrograph on Spitzer covering
the 5-38micron region of three Ultraluminous Infrared Galaxies (ULIRGs): Mrk
1014 (z=0.163), and Mrk 463 (z=0.051), and UGC 5101 (z=0.039). The continua of
UGC 5101 and Mrk 463 show strong silicate absorption suggesting significant
optical depths to the nuclei at 10microns. UGC 5101 also shows the clear
presence of water ice in absorption. PAH emission features are seen in both Mrk
1014 and UGC 5101, including the 16.4micron line in UGC 5101. The fine
structure lines are consistent with dominant AGN power sources in both Mrk 1014
and Mrk 463. In UGC 5101 we detect the [NeV] 14.3micron emission line providing
the first direct evidence for a buried AGN in the mid-infrared. The detection
of the 9.66micron and 17.03micron H emission lines in both UGC 5101 and
Mrk 463 suggest that the warm molecular gas accounts for 22% and 48% of the
total molecular gas masses in these galaxies.Comment: Accepted in ApJ Sup. Spitzer Special Issue, 4 pages, 3 figure
The Infrared Spectrograph on the Spitzer Space Telescope
The Infrared Spectrograph (IRS) is one of three science instruments on the
Spitzer Space Telescope. The IRS comprises four separate spectrograph modules
covering the wavelength range from 5.3 to 38micron with spectral resolutions, R
\~90 and 600, and it was optimized to take full advantage of the very low
background in the space environment. The IRS is performing at or better than
the pre-launch predictions. An autonomous target acquisition capability enables
the IRS to locate the mid-infrared centroid of a source, providing the
information so that the spacecraft can accurately offset that centroid to a
selected slit. This feature is particularly useful when taking spectra of
sources with poorly known coordinates. An automated data reduction pipeline has
been developed at the Spitzer Science Center.Comment: Accepted in ApJ Sup. Spitzer Special Issue, 6 pages, 4 figure
TRAPPIST-1: Global results of the Spitzer Exploration Science Program Red Worlds
With more than 1000 hours of observation from Feb 2016 to Oct 2019, the
Spitzer Exploration Program Red Worlds (ID: 13067, 13175 and 14223) exclusively
targeted TRAPPIST-1, a nearby (12pc) ultracool dwarf star orbited by seven
transiting Earth-sized planets, all well-suited for a detailed atmospheric
characterization with the upcoming JWST. In this paper, we present the global
results of the project. We analyzed 88 new transits and combined them with 100
previously analyzed transits, for a total of 188 transits observed at 3.6 or
4.5 m. We also analyzed 29 occultations (secondary eclipses) of planet b
and eight occultations of planet c observed at 4.5 m to constrain the
brightness temperatures of their daysides. We identify several orphan
transit-like structures in our Spitzer photometry, but all of them are of low
significance. We do not confirm any new transiting planets. We estimate for
TRAPPIST-1 transit depth measurements mean noise floors of 35 and 25 ppm
in channels 1 and 2 of Spitzer/IRAC, respectively. most of this noise floor is
of instrumental origins and due to the large inter-pixel inhomogeneity of IRAC
InSb arrays, and that the much better interpixel homogeneity of JWST
instruments should result in noise floors as low as 10ppm, which is low enough
to enable the atmospheric characterization of the planets by transit
transmission spectroscopy. We construct updated broadband transmission spectra
for all seven planets which show consistent transit depths between the two
Spitzer channels. We identify and model five distinct high energy flares in the
whole dataset, and discuss our results in the context of habitability. Finally,
we fail to detect occultation signals of planets b and c at 4.5 m, and can
only set 3 upper limits on their dayside brightness temperatures (611K
for b 586K for c)
Exoplanet Atmosphere Measurements from Transmission Spectroscopy and other Planet-Star Combined Light Observations
It is possible to learn a great deal about exoplanet atmospheres even when we
cannot spatially resolve the planets from their host stars. In this chapter, we
overview the basic techniques used to characterize transiting exoplanets -
transmission spectroscopy, emission and reflection spectroscopy, and full-orbit
phase curve observations. We discuss practical considerations, including
current and future observing facilities and best practices for measuring
precise spectra. We also highlight major observational results on the
chemistry, climate, and cloud properties of exoplanets.Comment: Accepted review chapter; Handbook of Exoplanets, eds. Hans J. Deeg
and Juan Antonio Belmonte (Springer-Verlag). 22 pages, 6 figure
Differential Effect of TLR2 and TLR4 on the Immune Response after Immunization with a Vaccine against Neisseria meningitidis or Bordetella pertussis
Neisseria meningitidis and Bordetella pertussis are Gram-negative bacterial pathogens that can cause serious diseases in humans. N. meningitidis outer membrane vesicle (OMV) vaccines and whole cell pertussis vaccines have been successfully used in humans to control infections with these pathogens. The mechanisms behind their effectiveness are poorly defined. Here we investigated the role of Toll-like receptor (TLR) 2 and TLR4 in the induction of immune responses in mice after immunization with these vaccines. Innate and adaptive immune responses were compared between wild type mice and mice deficient in TLR2, TLR4, or TRIF. TRIF-deficient and TLR4-deficient mice showed impaired immunity after immunization. In contrast, immune responses were not lower in TLR2−/− mice but tended even to be higher after immunization. Together our data demonstrate that TLR4 activation contributes to the immunogenicity of the N. meningitidis OMV vaccine and the whole cell pertussis vaccine, but that TLR2 activation is not required
Molecular excitation in the Interstellar Medium: recent advances in collisional, radiative and chemical processes
We review the different excitation processes in the interstellar mediumComment: Accepted in Chem. Re
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