3,992 research outputs found
Spectroscopic characterization and detection of Ethyl Mercaptan in Orion
New laboratory data of ethyl mercaptan, CHCHSH, in the millimeter
and submillimeter-wave domains (up to 880 GHz) provided very precise values of
the spectroscopic constants that allowed the detection of
-CHCHSH towards Orion KL. 77 unblended or slightly blended
lines plus no missing transitions in the range 80-280 GHz support this
identification. A detection of methyl mercaptan, CHSH, in the spectral
survey of Orion KL is reported as well. Our column density results indicate
that methyl mercaptan is 5 times more abundant than ethyl mercaptan in
the hot core of Orion KL.Comment: Accepted for publication in ApJL (30 January 2014)/ submitted (8
January 2014
On the algorithmic construction of classifying spaces and the isomorphism problem for biautomatic groups
We show that the isomorphism problem is solvable in the class of central
extensions of word-hyperbolic groups, and that the isomorphism problem for
biautomatic groups reduces to that for biautomatic groups with finite centre.
We describe an algorithm that, given an arbitrary finite presentation of an
automatic group , will construct explicit finite models for the skeleta
of and hence compute the integral homology and cohomology of
.Comment: 21 pages, 4 figure
A High Spatial Resolution Mid-Infrared Spectroscopic Study of the Nuclei and Star-Forming Regions in Luminous Infrared Galaxies
We present a high spatial (diffraction-limited) resolution (~0.3")
mid-infrared (MIR) spectroscopic study of the nuclei and star-forming regions
of 4 local luminous infrared galaxies (LIRGs) using T-ReCS on the Gemini South
telescope. We investigate the spatial variations of the features seen in the
N-band spectra of LIRGs on scales of ~100 pc, which allow us to separate the
AGN emission from that of the star formation (SF). We compare our Gemini T-ReCS
nuclear and integrated spectra of LIRGs with those obtained with Spitzer IRS.
The 9.7um silicate absorption feature is weaker in the nuclei of the LIRGs than
in the surrounding regions. This is probably due to the either clumpy or
compact environment of the central AGN or young, nuclear starburst. We find
that the [NeII] luminosity surface density is tightly and directly correlated
with that of Pa-alpha for the LIRG star-forming regions (slope of 1.00+-0.02).
Although the 11.3um PAH feature shows also a trend with Pa-alpha, this is not
common for all the regions. We also find that the [NeII]\Pa-alpha ratio does
not depend on the Pa-alpha equivalent width (EW), i.e., on the age of the
ionizing stellar populations, suggesting that, on the scales probed here, the
[NeII] emission line is a good tracer of the SF activity in LIRGs. On the other
hand, the 11.3um PAH\Pa-alpha ratio increases for smaller values of the
Pa-alpha EW (increasing ages), indicating that the 11.3um PAH feature can also
be excited by older stars than those responsible for the Pa-alpha emission.
Additional high spatial resolution observations are essential to investigate,
in a statistical way, the star formation in local LIRGs at the smallest scales
and to probe ultimately whether they share the same physical properties as
high-z LIRGs, ULIRGs and submillimiter galaxies.Comment: 23 pages (apjstyle), 19 figures, accepted for publicacion in Ap
The Mid-Infrared Continua of Seyfert Galaxies
An analysis of archival mid-infrared (mid-IR) spectra of Seyfert galaxies
from the Spitzer Space Telescope observations is presented. We characterize the
nature of the mid-IR active nuclear continuum by subtracting a template
starburst spectrum from the Seyfert spectra. The long wavelength part of the
spectrum contains a strong contribution from the starburst-heated cool dust;
this is used to effectively separate starburst-dominated Seyferts from those
dominated by the active nuclear continuum. Within the latter category, the
strength of the active nuclear continuum drops rapidly beyond ~ 20 micron. On
average, type 2 Seyferts have weaker short-wavelength active nuclear continua
as compared to type 1 Seyferts. Type 2 Seyferts can be divided into two types,
those with strong poly-cyclic aromatic hydrocarbon (PAH) bands and those
without. The latter type show polarized broad emission lines in their optical
spectra. The PAH-dominated type 2 Seyferts and Seyfert 1.8/1.9s show very
similar mid-IR spectra. However, after the subtraction of the starburst
component, there is a striking similarity in the active nuclear continuum of
all Seyfert optical types. PAH-dominated Seyfert 2s and Seyfert 1.8/1.9s tend
to show weak active nuclear continua in general. A few type 2 Seyferts with
weak/absent PAH bands show a bump in the spectrum between 15 and 20 micron. We
suggest that this bump is the peak of a warm (~200 K) blackbody dust emission,
which becomes clearly visible when the short-wavelength continuum is weaker.
This warm blackbody emission is also observed in other Seyfert optical
subtypes, suggesting a common origin in these active galactic nuclei.Comment: 25 pages, 3 tables, 11 figures; Accepted for Publication in Nov. 2009
ApJ issue
The Anatomy of Star Formation in NGC 300
The Spitzer Space Telescope was used to study the mid-infrared to
far-infrared properties of NGC 300, and to compare dust emission to Halpha to
elucidate the heating of the ISM and the star formation cycle at scales < 100
pc. The new data allow us to discern clear differences in the spatial
distribution of 8 micron dust emission with respect to 24 micron dust and to
HII regions traced by the Halpha light. The 8 micron emission highlights the
rims of HII regions, and the 24 micron emission is more strongly peaked in star
forming regions than at 8 microns. We confirm the existence and approximate
amplitude of interstellar dust emission at 4.5 microns, detected statistically
in Infrared Space Observatory (ISO) data, and conclude it arises in star
forming regions. When averaging over regions larger than ~ 1 kpc, the ratio of
Halpha to Aromatic Feature emission in NGC 300 is consistent with the values
observed in disks of spiral galaxies. The mid-to-far-infrared spectral energy
distribution of dust emission is generally consistent with pre-Spitzer models.Comment: to appear in the ApJS Spitzer special issue (September 2004
Optimal performance of endoreversible quantum refrigerators
The derivation of general performance benchmarks is important in the design of highly optimized heat engines and refrigerators. To obtain them, one may model phenomenologically the leading sources of irreversibility ending up with results that are model independent, but limited in scope. Alternatively, one can take a simple physical system realizing a thermodynamic cycle and assess its optimal operation from a complete microscopic description. We follow this approach in order to derive the coefficient of performance at maximum cooling rate for any endoreversible quantum refrigerator. At striking variance with the universality of the optimal efficiency of heat engines, we find that the cooling performance at maximum power is crucially determined by the details of the specific system-bath interaction mechanism. A closed analytical benchmark is found for endoreversible refrigerators weakly coupled to unstructured bosonic heat baths: an ubiquitous case study in quantum thermodynamics
Analysis of solar direct irradiance models under clear-skies: Evaluation of the improvements for locally adapted models
Direct solar irradiance has to be determined for the design of many energy applications such as photovoltaic systems and concentration systems, and the generation of solar potential maps for energy use. Knowledge of the accurate values of radiation components in a local area will allow optimal sizing of solar energy conversion systems. The estimated values of direct solar irradiance from models are still necessary at those sites where no measurements are available. In this work, different models used for the estimation of the direct component of solar irradiance are analyzed. First, an evaluation of the performance of eight existing original models was performed from which three were selected. Second, the selected models were calibrated to adapt them to our studied geographical area, which is the important aspect of this work, and an assessment of performance improvements for locally adapted models is reported. Experimental data consisted of hourly horizontal global, direct, and diffuse solar irradiance values, provided by the National Meteorological Agency in Spain (AEMET) for Madrid. Long-term data series, corresponding to a total period of time of 32 years (1980–2011), have been used in this study. Only clear sky models were treated at present. The three selected models were adapted to the specific location of Madrid, and root mean square error (RMSE) and mean-biased error were determined. By comparing the performance in the direct horizontal irradiance estimation from existing original and the corresponding locally adapted models, it is found that the values of RMSE decreased from 9.9% to 5.7% for the Louche model, from 7.8% to 7.4% for the Robledo-Soler model, and finally from 8.8% to 6.7% for the European Solar Radiation Atlas model. Thus, significant improvements can be reached when parametric models are locally adapted. In our case, it is up to approximately 4% for the Louche model. It is expected that calibrated algorithms presented in this work will be applicable to regions of similar climatic characteristics.Spanish Government (grant ENE2011-27511) and the Department of Culture and Education of the Regional Government of Castilla y León, Spain (grant BU358A12-2
Extremely Red Objects in The Lockman Hole
We investigate Extremely Red Objects (EROs) using near- and mid-infrared
observations in five passbands (3.6 to 24 micron) obtained from the Spitzer
Space Telescope, and deep ground-based R and K imaging. The great sensitivity
of the IRAC camera allows us to detect 64 EROs in only 12 minutes of IRAC
exposure time, by means of an R-[3.6] color cut (analogous to the traditional
red R-K cut). A pure infrared K-[3.6] red cut detects a somewhat different
population and may be more effective at selecting z > 1.3 EROs. We find 17% of
all galaxies detected by IRAC at 3.6 or 4.5 micron to be EROs. These
percentages rise to about 40% at 5.8 micron, and about 60% at 8.0 micron. We
utilize the spectral bump at 1.6 micron to divide the EROs into broad redshift
slices using only near-infrared colors (2.2/3.6/4.5 micron). We conclude that
two-thirds of all EROs lie at redshift z > 1.3. Detections at 24 micron imply
that at least 11% of 0.6 1.3 EROs are
dusty star-forming galaxies.Comment: to appear in the special Spitzer issue of the ApJ
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