Dynamical streams in the solar neighbourhood

The true nature of the Hyades and Sirius superclusters is still an open question. In this contribution, we confront Eggen's hypothesis that they are cluster remnants with the results of a kinematic analysis of more than 6000 K and M giants in the solar neighbourhood. This analysis includes new radial velocity data from a large survey performed with the Coravel spectrometer, complemented by Hipparcos parallaxes and Tycho-2 proper motions (Famaey et al. 2004). A maximum-likelihood method, based on a bayesian approach, has been applied to the data, in order to make full use of all the available data (including less precise parallaxes) and to derive the properties of the different kinematic subgroups. Two such subgroups can be identified with the Hyades and Sirius superclusters. Stars belonging to them span a very wide range of age, which is difficult to account for in Eggen's scenario. These groups are thus most probably "dynamical streams" related to the dynamical perturbation by spiral waves rather than to cluster remnants. In this scenario, the Hyades and Ursa Major clusters just happen to be in the Hyades and Sirius streams, which are purely dynamical features that have nothing to do with the remnants of more massive primordial clusters. This mechanism could be the key to understanding the presence of an old metal-rich population, and of many exoplanetary systems in our neighbourhood. Moreover, a strong spiral pattern seems to be needed in order to yield such prominent streams. Since spiral structure is usually baryonic, this would leave very little room for dark matter. This may be an indication that the era of the dark-matter paradigm explaining the dynamics of the Galaxy may come to an end, and is being superseded by modified gravity.Comment: 5 pages, 1 figure, to appear in The Three Dimensional Universe with GAIA, eds M. Perryman & C. Turo

Microlensing Events from Measurements of the Deflection Angle

Microlensing events are now regularly being detected by monitoring the flux of a large number of potential sources and measuring the combined magnification of the images. This phenomenon could also be detected directly from the gravitational deflection, by means of high precision astrometry using interferometry. Relative astrometry at the level of 10\muas may become possible in the near future. The gravitational deflection can be measured by astrometric monitoring of a bright star having a background star within a small angular separation. This type of monitoring program will be carried out for the independent reasons of discovering planets from the angular motion they induce on the nearby star around which they are orbiting, and for measuring parallaxes, proper motions and orbits of binary stars. We discuss three applications of the measurement of gravitational deflections by astrometric monitoring: measuring the mass of the bright stars that are monitored, measuring the mass of brown dwarfs or giant planets around the bright stars, and detecting microlensing events by unrelated objects near the line of sight to the two stars. We discuss the number of stars whose mass could be measured by this procedure. We also give expressions for the number of expected microlensing events by unrelated objects, which could be stars, brown dwarfs, or other compact objects accounting for dark matter in the halo or in the disk.Comment: submitted to ApJ Letter

Building the cosmic distance scale: from Hipparcos to Gaia

Hipparcos, the first ever experiment of global astrometry, was launched by ESA in 1989 and its results published in 1997 (Perryman et al., Astron. Astrophys. 323, L49, 1997; Perryman & ESA (eds), The Hipparcos and Tycho catalogues, ESA SP-1200, 1997). A new reduction was later performed using an improved satellite attitude reconstruction leading to an improved accuracy for stars brighter than 9th magnitude (van Leeuwen & Fantino, Astron. Astrophys. 439, 791, 2005; van Leeuwen, Astron. Astrophys. 474, 653, 2007). The Hipparcos Catalogue provided an extended dataset of very accurate astrometric data (positions, trigonometric parallaxes and proper motions), enlarging by two orders of magnitude the quantity and quality of distance determinations and luminosity calibrations. The availability of more than 20000 stars with a trigonometric parallax known to better than 10% opened the way to a drastic revision of our 3-D knowledge of the solar neighbourhood and to a renewal of the calibration of many distance indicators and age estimations. The prospects opened by Gaia, the next ESA cornerstone, planned for launch in June 2013 (Perryman et al., Astron. Astrophys. 369, 339, 2001), are still much more dramatic: a billion objects with systematic and quasi simultaneous astrometric, spectrophotometric and spectroscopic observations, about 150 million stars with expected distances to better than 10%, all over the Galaxy. All stellar distance indicators, in very large numbers, will be directly measured, providing a direct calibration of their luminosity and making possible detailed studies of the impacts of various effects linked to chemical element abundances, age or cluster membership. With the help of simulations of the data expected from Gaia, obtained from the mission simulator developed by DPAC, we will illustrate what Gaia can provide with some selected examples.Comment: 16 pages, 16 figures, Conference "The Fundamental Cosmic Distance scale: State of the Art and the Gaia perspective, 3-6 May 2011, INAF, Osservatorio Astronomico di Capodimonte, Naples. Accepted for publication in Astrophysics & Space Scienc

A model of Mira's cometary head/tail entering the Local Bubble

We model the cometary structure around Mira as the interaction of an AGB wind from Mira A, and a streaming environment. Our simulations introduce the following new element: we assume that after 200 kyr of evolution in a dense environment Mira entered the Local Bubble (low density coronal gas). As Mira enters the bubble, the head of the comet expands quite rapidly, while the tail remains well collimated for a 100 kyr timescale. The result is a broad-head/narrow-tail structure that resembles the observed morphology of Mira's comet. The simulations were carried out with our new adaptive grid code WALICXE, which is described in detail.Comment: 12 pages, 8 figures (4 in color). Accepted for publication in The Astrophysical Journa

A latitude-dependent wind model for Mira's cometary head

We present a 3D numerical simulation of the recently discovered cometary structure produced as Mira travels through the galactic ISM. In our simulation, we consider that Mira ejects a steady, latitude-dependent wind, which interacts with a homogeneous, streaming environment. The axisymmetry of the problem is broken by the lack of alignment between the direction of the relative motion of the environment and the polar axis of the latitude-dependent wind. With this model, we are able to produce a cometary head with a ``double bow shock'' which agrees well with the structure of the head of Mira's comet. We therefore conclude that a time-dependence in the ejected wind is not required for reproducing the observed double bow shock.Comment: 4 pages, 4 figures, accepted for publication in ApJ

El Bentos: les coves

Es descriuen les comunitats bentòniques de les coves i túnels de l'Arxipèlag de Cabrera, en funció dels principals grups d'organismes que les habiten. L'estudi s'ha basat concretament en la Cova des Calamars, la Cova Blava i el Túnel de l'Estell des Coll. Les comunitats de coves de l'Arxipèlag corresponen a les típiques de les coves balears, caracteritzades per la manca o escassesa d'octocoralaris (p. e. Corallium rubrum), i per la proliferació dels briozous. La comparació de les coves de Cabrera amb les d'altres indrets de la Mediterrània Occidental (Costa Catalana, Marsella i Nàpols) mostren diferències qualitatives i quantitatives importants que semblen estar condicionades per la distància geogràfica, la profunditat i la topografia de les coves.The benthic communities of caves and tunnels of the Cabrera Archipelago are described on the basis of the groups of organisms they harbour. The Calamars Cave, Blava Cave and Estell des Coll tunnel have been used as a model for the study. The communities found correspond to those typical from the Balearic caves, characterized by the absence or paucity of Octocorallia (e. g. Corallium rubrum), and the abundance of Bryozoans. Comparisons of the Cabrera caves with those from other localities in the Western Mediterranean (Catalonia, Marseilles and Naples) show sizeable qualitative and quantitative differences. Geographical distance, cave topography and depth are likely the main factors responsible for these differences

Els Bentos: les comunitats

Es descriuen les comunitats bentòniques de l'Arxipèlag de Cabrera en funció dels principals organismes animals i vegetals que les constitueixen. També es detalla la localització d'aquestes comunitats en l'espai a partir d'una sèrie de transsectes efectuats entre el nivell zero i la fondària màxima de -115 metres. Són destacables: (a) la representació en l'Arxipèlag de la majoria de comunitats bentòniques de plataforma continental descrites a la zona de la Mediterrània Central; (b) la gran riquesa especifica i el bon estat de conservació general de les comunitats; (c) la presència de parets submergides ininterrompudes entre O i-50 (-65) metres, la qual cosa fa de Cabrera un lloc privilegiat per a l'estudi de la zonació i les causes que la determinen; (d) les baixes cotes batimètriques enregistrades com a límit de la zona infra lit oral (-40 a -45 metres) i com a límit dels poblaments algals (-110 metres); i (e) l'elevat nombre d'endemismes mediterranis i de determinades espècies de mars càlids que reafirmen l'existència d'una província biogeogràfica centromediterrània. Finalment, es localitzen les zones submergides de l'Arxipèlag amb un valor biològic més elevat, per tal de prioritzar i facilitar la seva conservació.The benthic communities of the archipelago of Cabrera are described attending to their main faunistic and floristic components. Each community is spatially located and its bathymetric range is given, starting from different transects made between O and -115 meters of maximum depth. The main results obtained are: (a) most of the littoral and the continental shelf benthic communities described from the Central Mediterranean are well represented in the area; (b) species diversity and conservation of the communities is very high for Mediterranean standards; (c) the presence of some undisturbed and continuous underwater cliffs between O and -50 (-65) meters are of major interest to carry out future studies on zonation in Mediterranean benthic communities and on environmental factors forcing it; (d) lowermost bathymetric limits for the infralittoral zone (-40 to -45 meters) and algal growth (-110 meters) have been determined by SCUBA and submersible dives; and (e) the abundance of mediterranean endemisms and warm-water species reassert the existence of a centro-mediterranean biogeographic province. Finally, the areas of highest biological interest in the submersed part of the archipelago are indicated, in order to priorize its immediate preservation

Hydrological processes affecting the subtropical NE Atlantic (34-38° N) over the last 30 ka: Evidence from phyto- and zooplankton assemblages

International audienceNew dinocyst analyses were conducted on core MD99-2339 retrieved from the central Gulf of Cadiz. Dinocyst and foraminiferal assemblages from this core are combined with existing data off SW Portugal and NW Morocco to investigate past hydrological and primary productivity regimes in the subtropical NE Atlantic Ocean over the last 30 ka. Our results have revealed highest upwelling intensity during Heinrich Stadial 1 (HS 1) and the Younger Dryas and weaker upwelling cells during the Last Glacial Maximum and HS 2, off the SW Iberian and NW Moroccan margins. Similar assemblages between Cadiz and Morocco and distinct species off Portugal were observed during the cold climatic extremes that punctuated the last 30 ka. This pattern has been linked to the occurrence of a hydrological structure between SW Iberia and Cadiz during the last glacial period, probably similar to the modern Azores Front. This front was probably responsible locally for heterotrophic dinocysts found in the Gulf of Cadiz during the last glacial period, even if this sector is not conductive to upwelling phenomena by Ekman transport. Regional reconstructions of paleo-sea-surface temperatures using dinocyst and foraminiferal transfer functions, as well as alkenones, are also discussed and depict coherent scenarios over the last 30 ka. However, some mismatches are observed between the different quantitative reconstructions such as during HS 1 in the Gulf of Cadiz and during the LGM at the three core locations. © 2011 Author(s)

Detection of an inner gaseous component in a Herbig Be star accretion disk: Near- and mid-infrared spectro-interferometry and radiative transfer modeling of MWC 147

We study the geometry and the physical conditions in the inner (AU-scale) circumstellar region around the young Herbig Be star MWC 147 using long-baseline spectro-interferometry in the near-infrared (NIR K-band, VLTI/AMBER observations and PTI archive data) as well as the mid-infrared (MIR N-band, VLTI/MIDIobservations). The emission from MWC 147 is clearly resolved and has a characteristic physical size of approx. 1.3 AU and 9 AU at 2.2 micron and 11 micron respectively (Gaussian diameter). The spectrally dispersed AMBER and MIDI interferograms both show a strong increase in the characteristic size towards longer wavelengths, much steeper than predicted by analytic disk models assuming power-law radial temperature distributions. We model the interferometric data and the spectral energy distribution of MWC 147 with 2-D, frequency-dependent radiation transfer simulations. This analysis shows that models of spherical envelopes or passive irradiated Keplerian disks (with vertical or curved puffed-up inner rim) can easily fit the SED, but predict much lower visibilities than observed; the angular size predicted by such models is 2 to 4 times larger than the size derived from the interferometric data, so these models can clearly be ruled out. Models of a Keplerian disk with optically thick gas emission from an active gaseous disk (inside the dust sublimation zone), however, yield a good fit of the SED and simultaneously reproduce the absolute level and the spectral dependence of the NIR and MIR visibilities. We conclude that the NIR continuum emission from MWC 147 is dominated by accretion luminosity emerging from an optically thick inner gaseous disk, while the MIR emission also contains contributions from the outer, irradiated dust disk.Comment: 44 pages, 15 figures, accepted for publication in The Astrophysical Journal. The quality of the figures was slightly reduced in order to comply with the astro-ph file-size restrictions. You can find a high-quality version of the paper at http://www.mpifr-bonn.mpg.de/staff/skraus/papers/mwc147.pd