Addendum: Dark matter in elliptical galaxies – II. Estimating the mass within the virial radius     

《Monthly notices of the Royal Astronomical Society》2006,370(3):1582-1582

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Statistical characteristics of the observed Lyα forest and the shape of the initial power spectrum     

M. Demia&#;ski  A. G. Doroshkevich  V. I. Turchaninov 《Monthly notices of the Royal Astronomical Society》2006,371(2):915-934

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Testing models of the individual and cosmological evolutions of powerful radio galaxies     

Paramita Barai  Paul J. Wiita 《Monthly notices of the Royal Astronomical Society》2006,372(1):381-400

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The fundamental properties of galaxies and a new galaxy classification system     

Christopher J. Conselice 《Monthly notices of the Royal Astronomical Society》2006,373(4):1389-1408

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Constraints on the velocity profiles of galaxies from strong lensing statistics and semi-analytical modelling of galaxy formation     

Kyu-Hyun Chae  Shude Mao  Xi Kang 《Monthly notices of the Royal Astronomical Society》2006,373(4):1369-1378

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Molecular line mapping of the giant molecular cloud associated with RCW 106 – I. ¹³CO     

I. Bains  T. Wong  M. Cunningham  P. Sparks  D. Brisbin  P. Calisse  J. T. Dempsey  G. Deragopian  S. Ellingsen  B. Fulton  F. Herpin  P. Jones  Y. Kouba  C. Kramer  E. F. Ladd  S. N. Longmore  J. McEvoy  M. Maller  V. Minier  B. Mookerjea  C. Phillips  C. R. Purcell  A. Walsh  M. A. Voronkov  M. G. Burton 《Monthly notices of the Royal Astronomical Society》2006,367(4):1609-1628

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On the origin of warps and the role of the intergalactic medium     

F. J. Sánchez-Salcedo 《Monthly notices of the Royal Astronomical Society》2006,365(2):555-571

There is still no consensus as to what causes galactic discs to become warped. Successful models should account for the frequent occurrence of warps in quite isolated galaxies, their amplitude as well as the observed azimuthal and vertical distributions of the H  i layer. Intergalactic accretion flows and intergalactic magnetic fields may bend the outer parts of spiral galaxies. In this paper we consider the viability of these non-gravitational torques to take the gas off the plane. We show that magnetically generated warps are clearly flawed because they would wrap up into a spiral in less than two or three galactic rotations. The inclusion of any magnetic diffusivity to dilute the wrapping effect causes the amplitude of the warp to damp. We also consider the observational consequences of the accretion of an intergalactic plane-parallel flow at infinity. We have computed the amplitude and warp asymmetry in the accretion model, for a disc embedded in a flattened dark matter halo, including self-consistently the contribution of the modes with azimuthal wavenumbers   m = 0  and   m = 1  . Since the m = 0 component, giving a U-shaped profile, is not negligible compared to the m = 1 component, this model predicts quite asymmetric warps, maximum gas displacements on the two sides in the ratio 3 : 2 for the preferred Galactic parameters, and the presence of a fraction ∼3.5 per cent of U-shaped warps, at least. The azimuthal dependence of the moment transfer by the ram pressure would produce a strong asymmetry in the thickness of the H  i layer and asymmetric density distributions in z , in conflict with observational data for the warp in our Galaxy and in external galaxies. The amount of accretion that is required to explain the Galactic warp would give gas scaleheights in the far outer disc that are too small. We conclude that accretion of a flow with no net angular momentum cannot be the main and only cause of warps.  相似文献   

Erratum: Near-infrared and optical luminosity functions from the 6dF Galaxy Survey     

《Monthly notices of the Royal Astronomical Society》2006,370(3):1583-1584

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Cassini CIRS retrievals of ammonia in Jupiter's upper troposphere     

Richard K. Achterberg  Barney J. Conrath 《Icarus》2006,182(1):169-180

The zonal mean ammonia abundance on Jupiter between the 400- and 500-mbar pressure levels is inferred as a function of latitude from Cassini Composite Infrared Spectrometer data. Near the Great Red Spot, the ammonia abundance is mapped as a function of latitude and longitude. The Equatorial Zone is rich in ammonia, with a relative humidity near unity. The North and South Equatorial Belts are depleted relative to the Equatorial Zone by an order of magnitude. The Great Red Spot shows a local maximum in the ammonia abundance. Ammonia abundance is highly correlated with temperature perturbations at the same altitude. Under the assumption that anomalies in ammonia and temperature are both perturbed from equilibrium by vertical motion, we find that the adjustment time constant for ammonia equilibration is about one third of the radiative time constant.  相似文献   

The 2-Micron All-Sky Survey galaxy angular power spectrum: probing the galaxy distribution to gigaparsec scales     

W. J. Frith  P. J. Outram  T. Shanks 《Monthly notices of the Royal Astronomical Society》2005,364(2):593-600

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