2,498 research outputs found
Thermal Fluctuations and Validity of the 1-Loop Effective Potential
We examine the validity of the 1-loop approximation to the effective
potential at finite temperatures and present a simple test for its reliability.
As an application we study the standard electroweak potential, showing that for
a Higgs mass above 70 GeV, and afirly independent of the top mass (with , the 1-loop approximation is no longer valid for temperatures in the
neighborhood of the critical temperature.Comment: 15 pages , LATEX, 2 figures (not included but available upon
request), DART-HEP-92/08 ``REVISED VERSION'
Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068
We present sub-arcsecond 7.513 m imaging- and spectro-polarimetric
observations of NGC 1068 using CanariCam on the 10.4-m Gran Telescopio
CANARIAS. At all wavelengths, we find:
(1) A 90 60 pc extended polarized feature in the northern ionization
cone, with a uniform 44 polarization angle. Its polarization
arises from dust and gas emission in the ionization cone, heated by the active
nucleus and jet, and further extinguished by aligned dust grains in the host
galaxy. The polarization spectrum of the jet-molecular cloud interaction at
24 pc from the core is highly polarized, and does not show a silicate
feature, suggesting that the dust grains are different from those in the
interstellar medium.
(2) A southern polarized feature at 9.6 pc from the core. Its
polarization arises from a dust emission component extinguished by a large
concentration of dust in the galaxy disc. We cannot distinguish between dust
emission from magnetically aligned dust grains directly heated by the jet close
to the core, and aligned dust grains in the dusty obscuring material
surrounding the central engine. Silicate-like grains reproduce the polarized
dust emission in this feature, suggesting different dust compositions in both
ionization cones.
(3) An upper limit of polarization degree of 0.3 per cent in the core. Based
on our polarization model, the expected polarization of the obscuring dusty
material is 0.1 per cent in the 813 m wavelength range. This
low polarization may be arising from the passage of radiation through aligned
dust grains in the shielded edges of the clumps.Comment: 17 pages, 10 figures, accepted for publication at MNRA
Diseño de una secuencia de enseñanza aprendizaje del sistema digestivo que fomente el desarrollo de competencias específicas en ciencias naturales, en estudiantes de 6° de una institución educativa del Distrito de Buenaventura [recurso electrónico]
Esta investigación se centró en el diseño de una secuencia de enseñanza aprendizaje sobre el sistema digestivo, que permitiera fomentar el desarrollo de competencias específicas en ciencias naturales en estudiantes de 6° de una institución educativa del distrito de Buenaventura. Lo anterior, se desarrolló gracias a una metodología cualitativa e interpretativa, con la que fue posible, en primer lugar; realizar una revisión documental sobre las competencias específicas en ciencias naturales, sus aportes para la elaboración de actividades y las características generales de las secuencias de enseñanza tomado como apoyo una rejilla de análisis. En segundo lugar, se usaron diarios de campo para reflexionar y analizar una experiencia de enseñanza que fue previamente implementada en práctica docente 1 por las autoras de este trabajo; hecho que favoreció la identificación de las fortalezas y debilidades de aquella experiencia para facilitar su reestructuración, incluyendo no solo elementos teóricos, sino también elementos contextuales que sólo pueden ser vivenciados desde la práctica educativa. Para analizar la información anterior y cumplir a cabalidad con la intención planteada, se empleó una matriz DOFA con la que fue posible comprender los hallazgos y estructurar la secuencia de enseñanza. Con ello se brindan aportes para que los docentes puedan mejorar su acto educativo, tener una mejor planificación de su práctica y así, aproximarse a la mejora del proceso de enseñanza y aprendizaj
A deep look at the nuclear region of UGC 5101 through high angular resolution mid-IR data with GTC/CanariCam
We present an analysis of the nuclear infrared (IR, 1.6–18 μm) emission of the ultraluminous IR galaxy UGC 5101 to derive the properties of its active galactic nucleus (AGN) and its obscuring material. We use new mid-IR high angular resolution (0.3–0.5 arcsec) imaging using the Si-2 filter (λ_C = 8.7 μm) and 7.5–13 μm spectroscopy taken with CanariCam (CC) on the 10.4 m Gran Telescopio CANARIAS. We also use archival Hubble Space Telescope/NICMOS and Subaru/COMICS imaging and Spitzer/IRS spectroscopy. We estimate the near- and mid-IR unresolved nuclear emission by modelling the imaging data with GALFIT. We decompose the Spitzer/IRS and CC spectra using a power-law component, which represents the emission due to dust heated by the AGN, and a starburst component, both affected by foreground extinction. We model the resulting unresolved near- and mid-IR, and the starburst subtracted CC spectrum with the CLUMPY torus models of Nenkova et al. The derived geometrical properties of the torus, including the large covering factor and the high foreground extinction needed to reproduce the deep 9.7 μm silicate feature, are consistent with the lack of strong AGN signatures in the optical. We derive an AGN bolometric luminosity L_(bo)l ∼ 1.9 × 10^(45) erg s^(−1) that is in good agreement with other estimates in the literature
A Deep Look at the Nuclear Region of UGC 5101 Through High Angular Resolution Mid-IR Data with GTC/CanariCam
We present an analysis of the nuclear infrared (IR, 1.6–18 μm) emission of the ultraluminous IR galaxy UGC 5101 to derive the properties of its active galactic nucleus (AGN) and its obscuring material. We use new mid-IR high angular resolution (0.3–0.5 arcsec) imaging using the Si-2 filter (λC = 8.7 μm) and 7.5–13 μm spectroscopy taken with CanariCam (CC) on the 10.4 m Gran Telescopio CANARIAS. We also use archival Hubble Space Telescope/NICMOS and Subaru/COMICS imaging and Spitzer/IRS spectroscopy. We estimate the near- and mid-IR unresolved nuclear emission by modelling the imaging data with GALFIT. We decompose the Spitzer/IRS and CC spectra using a power-law component, which represents the emission due to dust heated by the AGN, and a starburst component, both affected by foreground extinction. We model the resulting unresolved near- and mid-IR, and the starburst subtracted CC spectrum with the CLUMPY torus models of Nenkova et al. The derived geometrical properties of the torus, including the large covering factor and the high foreground extinction needed to reproduce the deep 9.7 μm silicate feature, are consistent with the lack of strong AGN signatures in the optical. We derive an AGN bolometric luminosity Lbol ~ 1.9 × 1045 erg s−1 that is in good agreement with other estimates in the literature
A mid-infrared view of the inner parsecs of the Seyfert galaxy Mrk 1066 using CanariCam/GTC
We present mid-infrared (MIR) imaging and spectroscopic data of the Seyfert 2 galaxy Mrk 1066 obtained with CanariCam (CC) on the 10.4-m Gran Telescopio CANARIAS (GTC). The galaxy was observed in imaging mode with an angular resolution of 0.24 arcsec (54 pc) in the Si-2 filter (8.7 μm). The image reveals a series of star-forming knots within the central ∼400 pc, after subtracting the dominant active galactic nucleus (AGN) component. We also subtracted this AGN unresolved component from the 8–13 μm spectra of the knots and the nucleus, and measured equivalent widths (EWs) of the 11.3 μm polycyclic aromatic hydrocarbon (PAH) feature which are typical of pure starburst galaxies. This EW is larger in the nucleus than in the knots, confirming that, at least in the case of Mrk 1066, the AGN dilutes, rather than destroys, the molecules responsible for the 11.3 μm PAH emission. By comparing the nuclear GTC/CC spectrum with the Spitzer/Infrared Spectrograph (IRS) spectrum of the galaxy, we find that the AGN component that dominates the continuum emission at λ < 15 μm on scales of ∼60 pc (90–100 per cent) decreases to 35–50 per cent when the emission of the central ∼830 pc is considered. On the other hand, the AGN contribution dominates the 15–25 μm emission (75 per cent) on the scales probed by Spitzer/IRS. We reproduced the nuclear infrared emission of the galaxy with clumpy torus models, and derived a torus gas mass of 2 × 10^5 M_⊙, contained in a clumpy structure of ∼2 pc radius and with a column density compatible with Mrk 1066 being a Compton-thick candidate, in agreement with X-ray observations. We find a good match between the MIR morphology of Mrk 1066 and the extended Paβ, Brγ and [O iii] λ5007 emission. This coincidence implies that the 8.7 μm emission is probing star formation, dust in the narrow-line region and the oval structure previously detected in the near-infrared. On the other hand, the Chandra soft X-ray morphology does not match any of the previous, contrary to what it is generally assumed for Seyfert galaxies. A thermal origin for the soft X-ray emission, rather than AGN photoionization, is suggested by the different data analysed here
Microphysical Approach to Nonequilibrium Dynamics of Quantum Fields
We examine the nonequilibrium dynamics of a self-interacting
scalar field theory. Using a real time formulation of finite temperature field
theory we derive, up to two loops and , the effective equation of
motion describing the approach to equilibrium. We present a detailed analysis
of the approximations used in order to obtain a Langevin-like equation of
motion, in which the noise and dissipation terms associated with quantum
fluctuations obey a fluctuation-dissipation relation. We show that, in general,
the noise is colored (time-dependent) and multiplicative (couples nonlinearly
to the field), even though it is still Gaussian distributed. The noise becomes
white in the infinite temperature limit. We also address the effect of
couplings to other fields, which we assume play the r\^ole of the thermal bath,
in the effective equation of motion for . In particular, we obtain the
fluctuation and noise terms due to a quadratic coupling to another scalar
field.Comment: 30 pages, LaTex (uses RevTex 3.0), DART-HEP-93/0
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