466 research outputs found

    Parsec-scale HI absorption structure in a low-redshift galaxy seen against a Compact Symmetric Object

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    We present global VLBI observations of the 21-cm transition of atomic hydrogen seen in absorption against the radio source J0855+5751. The foreground absorber (SDSS~J085519.05+575140.7) is a dwarf galaxy at zz = 0.026. As the background source is heavily resolved by VLBI, the data allow us to map the properties of the foreground HI gas with a spatial resolution of 2pc. The absorbing gas corresponds to a single coherent structure with an extent >>35pc, but we also detect significant and coherent variations, including a change in the HI optical depth by a factor of five across a distance of ≤\leq6pc. The large size of the structure provides support for the Heiles & Troland model of the ISM, as well as its applicability to external galaxies. The large variations in HI optical depth also suggest that caution should be applied when interpreting TST_S measurements from radio-detected DLAs. In addition, the distorted appearance of the background radio source is indicative of a strong jet-cloud interaction in its host galaxy. We have measured its redshift (zz = 0.54186) using optical spectroscopy on the William Herschel Telescope and this confirms that J0855+5751 is a FRII radio source with a physical extent of <<1kpc and supports the previous identification of this source as a Compact Symmetric Object. These sources often show absorption associated with the host galaxy and we suggest that both HI and OH should be searched for in J0855+5751.Comment: 14 pages and 10 figures. Accepted for publication in MNRA

    Analysis and Modeling of the Quasi-Z-Source-Inverter

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    This paper presents a dynamic average model of the Quasi-Z-Source Inverter (QZSI), based on the short term average values over one PWM-period, and the analysis of the possible switching states that can occur in the QZSI. The model is considerably descriptive since the modeling has been performed by analyzing the physical and functional relations with only little mathematical complexity. Another advantage of the proposed model is that the load current only acts as a disturbance input, and is not directly linked with the model structure itself. This allows a separate examination of either command input or disturbance response and makes the model independent of the given load. The model has been tested successfully in conjunction with an adequate cascade control loop design and a QZSI-prototype in hardware

    Mapping the galactic gravitational potential with peculiar acceleration

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    It has been suggested recently that the change in cosmological redshift (the Sandage test of expansion) could be observed in the next generation of large telescopes and ultra-stable spectrographs. In a recent paper we estimated the change of peculiar velocity, i.e. the peculiar acceleration, in nearby galaxies and clusters and shown it to be of the same order of magnitude as the typical cosmological signal. Mapping the acceleration field allows for a reconstruction of the galactic gravitational potential without assuming virialization. In this paper we focus on the peculiar acceleration in our own Galaxy, modeled as a Kuzmin disc and a dark matter spherical halo. We estimate the peculiar acceleration for all known Galactic globular clusters and find some cases with an expected velocity shift in excess of 20 cm/sec for observations fifteen years apart, well above the typical cosmological acceleration. We then compare the predicted signal for a MOND (modified Newtonian dynamics) model in which the spherical dark matter halo is absent. We find that the signal pattern is qualitatively different, showing that the peculiar acceleration field could be employed to test competing theories of gravity. However the difference seems too small to be detectable in the near future.Comment: 11 pages, 10 figures, 3 tables, minor changes, accepted for publication by MNRA
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