36,308 research outputs found
Many homes for tourism:re-considering spatializations of home and away in tourism mobilities
Tourism mobilities have long been spatialized as circular structures emanating from a primary home that is opposed to a space of ‘away’. Increasingly complex personal mobilities and experiences with multiple homes, however, challenge the assumptions on which this spatialization of tourism rests. This article utilizes an analysis of travel memoir narratives of return home and second home mobilities to deconstruct the oppositions within traditional spatializations of tourism, revealing in the process the way in which the everyday and tourism are entangled and interactive. Memoir authors construct complex relationships between spaces and places, wherein second homes can inspire new tourism practices at both unfamiliar locations and primary homes, and returning to previous homes can involve tourism of and at home. A consideration of these relationships reveals the difficulty of labeling mobilities as essentially touristic and suggests possibilities for new spatializations, ontology and methodologies that leave room for many homes for tourism
Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr
We carried out a photometric and structural analysis in the rest-frame
band of a mass-selected () sample of red-sequence
galaxies in 14 galaxy clusters, 6 of which are at . To this end, we
reduced/analyzed about 300 orbits of multicolor images taken with the Advanced
Camera for Survey and the Wide Field Camera 3 on the Hubble Space Telescope. We
uniformly morphologically classified galaxies from to , and
we homogeneously derived sizes (effective radii) for the entire sample.
Furthermore, our size derivation allows, and therefore is not biased by, the
presence of the usual variety of morphological structures seen in early-type
galaxies, such as bulges, bars, disks, isophote twists, and ellipiticy
gradients. By using such a mass-selected sample, composed of 244 red-sequence
early-type galaxies, we find that the of the galaxy size at a fixed
stellar mass, has increased with time at a rate of
dex per Gyr over the last 10 Gyr, in marked contrast with the
threefold increase found in the literature for galaxies in the general field
over the same period. This suggests, at face value, that secular processes
should be excluded as the primary drivers of size evolution because we observed
an environmental environmental dependent size growth. Using spectroscopic ages
of Coma early-type galaxies we also find that recently quenched early-type
galaxies are a numerically minor population not different enough in size to
alter the mean size at a given mass, which implies that the progenitor bias is
minor, i.e., that the size evolution measured by selecting galaxies at the
redshift of observation is indistinguishable from the one that compares
ancestors and descendents.Comment: A&A 593, A2 (2016) after revision of the z=1.63 cluster name,
mis-typed in previous version. No result of our paper is affected by having
mis-typed the cluster nam
Probing the halo of Centaurus A: a merger dynamical model for the PN population
Photometry and kinematics of the giant elliptical galaxy NGC~5128
(Centaurus~A) based on planetary nebulae observations (Hui~\etal 1995) are used
to build dynamical models which allow us to infer the presence of a dark matter
halo. To this end, we apply a Quadratic Programming method. Constant
mass-to-light ratio models fail to reproduce the major axis velocity dispersion
measurements at large radii: the profile of this kind of models falls off too
steeply when compared to the observations, clearly suggesting the necessity of
including a dark component in the halo. By assuming a mass-to-light ratio which
is increasing with radius, the model satisfactorily matches the observations.
The total mass for the best fit model is of which
about 50\% is dark matter. However, models with different total masses and dark
halos are also consistent with the data; we estimate that the total mass of
Cen~A within 50~kpc may vary between and
. The best fit model consists of 75\% of stars rotating
around the short axis and 25\% of stars rotating around the long axis .
Finally, the morphology of the projected velocity field is analyzed using
Statler's classification criteria (Statler 1991). We find that the appearance
of our velocity field is compatible with a type 'Nn' or 'Nd'.Comment: 13 pages, uuencoded compressed postscript, without figures. The full
postscript version, including all 14 figures, is available via anonymous ftp
at ftp://naos.rug.ac.be/pub/cena.ps.
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