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1.
We review some of the evidences that dust properties are dominated by large grains in some astronomical objects. We emphasize
the effects of large grains on the extinction and emissivity, but we also discuss some dynamical implications. We also propose
a density sequence, where objects characterized by denser environments are also associated with average larger grains.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
2.
Niranjan Thatte Reinhard Genzel Harald Kroker Alfred Krabbe Lowell E. Tacconi-Garman Roberto Maiolino Matthias Tecza 《Astrophysics and Space Science》1997,248(1-2):225-234
We present new near-infrared integral field spectroscopy and adaptive optics imaging of the nucleus of NGC 1068. Using the
stellar CO absorption features in the H and K bands, we have identified a moderately extincted stellar core centered on the
nuclear position and of intrinsic size ~50 pc. We show that this nuclear stellar core is probably 5-16 × 108 years in age
and contributes at least 7% of the total nuclear luminosity of ~1 × 1011 L⊙.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
3.
Alessandro Marconi Roberto Maiolino Romain G. Petrov 《Astrophysics and Space Science》2003,286(1-2):245-254
Interferometry in the optical and near infrared has so far played a marginal role in Extragalactic Astronomy. Active Galactic
Nuclei are the brightest and most compact extragalactic sources, nonetheless only a very limited number could be studied with
speckle interferometry and none with long baseline interferometry. The VLTI will allow the study of moderately faint extragalactic
objects with very high spatial resolution thus opening a new window on the universe. With this paper we focus on three scientific
cases to show how AMBER and MIDI can be used to tackle open issues in extragalactic astronomy.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
4.
P. Ranalli †‡ A. Comastri L. Origlia R. Maiolino § 《Monthly notices of the Royal Astronomical Society》2008,386(3):1464-1480
We report on the analysis of a deep (100-ks) observation of the starburst galaxy M82 with the EPIC and RGS instruments onboard the X-ray telescope XMM–Newton . The broad-band (0.5–10 keV) emission is due to at least three spectral components: (i) continuum emission from point sources; (ii) thermal plasma emission from hot gas; and (iii) charge-exchange emission from neutral metals (Mg and Si). The plasma emission has a double-peaked differential emission measure, with the peaks at ∼0.5 and ∼7 keV. Spatially resolved spectroscopy has shown that the chemical absolute abundances are not uniformly distributed in the outflow, but are larger in the outskirts and smaller close to the galaxy centre. The abundance ratios also show spatial variations. The X-ray-derived oxygen abundance is lower than that measured in the atmospheres of red supergiant stars, leading to the hypothesis that a significant fraction of oxygen ions have already cooled off and no longer emit at energies ≳0.5 keV. 相似文献
5.
C. Vignali F. Pozzi J. Fritz A. Comastri C. Gruppioni E. Bellocchi F. Fiore M. Brusa R. Maiolino M. Mignoli F. La Franca L. Pozzetti G. Zamorani A. Merloni 《Monthly notices of the Royal Astronomical Society》2009,395(4):2189-2195
We present multiwavelength observations (from optical to submillimetre, including Spitzer and Submillimetre Common-User Bolometer Array) of H2XMMJ 003357.2−120038 (also GD 158_19), an X-ray selected, luminous narrow-line (type 2) quasar at z = 1.957 selected from the HELLAS2XMM survey. Its broad-band properties can be reasonably well modelled assuming three components: a stellar component to account for the optical and near-infrared (IR) emission; an active galactic nucleus (AGN) component (i.e. dust heated by an accreting active nucleus), dominant in the mid-IR, with an optical depth at 9.7 along the line of sight (close to the equatorial plane of the obscuring matter) of τ(9.7) = 1 and a full covering angle of the reprocessing matter (torus) of 140° and a far-IR starburst component (i.e. dust heated by star formation) to reproduce the wide bump observed longward of 70 .
The derived star formation rate is ≈1500 M⊙ yr−1 . The overall modelling indicates that GD 158_19 is a high-redshift X-ray luminous, obscured quasar with coeval powerful AGN activity and intense star formation. It is probably caught before the process of expelling the obscuring gas has started, thus quenching the star formation. 相似文献
The derived star formation rate is ≈1500 M
6.
The Bayesian approach to significance testing, that makes use of prior information, has been studied in the last years, particularly
to allow the detection of deformations which are small with respect to measurement errors from repeated surveys. Some investigations
showed up to now that, under particular conditions concerning both the parameters of the prior distribution and the structure
of the control network, Bayesian tests give stronger results than tests based on the frequentist approach, with regard to
the detectability of deformations. In the present paper, after illustrating the essential developments and the most relevant
results of previous works, new analytical developments and numerical simulations are carried out, to illustrate some critical
aspects and advantages of the frequentist and Bayesian methods. It is shown, starting from simple examples involving only
Gaussian and truncated Gaussian distributions and from a simplified formulation of the prior deformation model, that the testing
procedures based on the frequentist approach, which do not introduce any a priori information, are in many cases of practical
interest insensitive to internal consistencies of the displacements (e.g., to the fact that they have a common direction).
It is also illustrated that the introduction of prior information, even in a non Bayesian context, more easily allows the
detection of little displacements. Besides it is noted that in some cases Bayesian tests detect displacements in the presence
of observed non-coherent movements, even if prior probability densities describing coherent movements are introduced. 相似文献
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9.
Vincenza Guarino Rogério Guitarrari Azzone Pietro Brotzu Celso de Barros Gomes Leone Melluso Lucio Morbidelli Excelso Ruberti Colombo Celso Gaeta Tassinari Mauro Brilli 《Mineralogy and Petrology》2012,104(1-2):43-61
The Ipanema alkaline-carbonatitic complex is part of the Meso-Cenozoic alkaline magmatism located within the southeastern part of the Brazilian Platform. Drill-core and field sampling have indicated the occurrence of glimmerites, with subordinate shonkinites (mela-syenites), clinopyroxene-bearing glimmerites, diorites and syenites. The glimmerites are cross-cut by lamprophyric dykes and calciocarbonatites. Fenitization has deeply affected the country rocks, originating dioritic and syenitic rocks. The Ipanema rocks show a distinct potassic affinity. The initial Sr-Nd- isotopic composition of the Ipanema rocks (87Sr/86Sr?=?0.70661–0.70754 and 143Nd/144Nd?=?0.51169–0.51181) is similar to that of tholeiitic and potassium-rich-alkaline rocks of the Eastern Paraguay. Stable isotope data for the Ipanema calciocarbonatite suggest interaction with fluids at temperatures typical of hydrothermal stages, as hypothesized for other carbonatite complexes from southeastern Brazil. The chemical differences between the lamprophyre, glimmerites, carbonatites, apatitites and magnetitites, and the absence of marked REE enrichment in the evolved lithologies, all indicate that fractional crystallization and accumulus of liquidus phases in a magma reservoir, likely coupled with liquid immiscibility processes, may have played an important role in the genesis of the Ipanema rocks. 相似文献
10.
M. Guainazzi G. Matt L. A. Antonelli L. Bassani A. C. Fabian R. Maiolino A. Marconi F. Fiore K. Iwasawa L. Piro 《Monthly notices of the Royal Astronomical Society》1999,310(1):10-20
We present an X-ray spectroscopic study of the bright Compton-thick Seyfert 2 galaxies NGC 1068 and the Circinus Galaxy, performed with BeppoSAX . Matt et al. interpreted the spectrum above 4 keV as the superposition of Compton reflection and warm plasma scattering of the nuclear radiation. When this continuum is extrapolated downwards to 0.1 keV, further components arise. The NGC 1068 spectrum is rich in emission lines, mainly owing to K α transitions of He-like elements from oxygen to iron, plus a K α fluorescent line from neutral iron. If the ionized lines originate in the warm scatterer, its thermal and ionization structure must be complex. From the continuum and line properties, we estimate a column density, N warm , of the warm scatterer less than a few×1021 cm−2 . In the Circinus Galaxy, the absence of highly ionized iron is consistent with a scattering medium with U X ≲5 and N warm ∼ a few×1022 cm−2 . In both cases the neutral iron line is most naturally explained as fluorescence in the medium responsible for the Compton reflection continuum. In NGC 1068 an optically thin plasma emission with kT ≃500 eV and strongly sub-solar metallicity is required, while such a component is only marginal in the Circinus Galaxy. We tentatively identify this component as emission of diffuse hot gas in the nuclear starbursts. Possible causes for the metal depletion are discussed. 相似文献