Ca II K observations of QSOs in the line-of-sight to the Magellanic Bridge

We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument (EMMI) in the CaII K line (lambda air = 3933.661 angstrom) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R =lambda/Delta lambda = 6000, five of the sightlines have a signal-to-noise ( S/N) ratio of similar to 20 or higher. Definite Ca absorption due to Bridge material is detected towards 3 objects, with probable detection towards two other sightlines. Gas-phase CaII K Bridge and Milky Way abundances or lower limits for the all sightlines are estimated by the use of Parkes 21-cm H. emission line data. These data only have a spatial resolution of 14 arcmin compared with the optical observations which have milli-arcsecond resolution. With this caveat, for the three objects with sound CaII K detections, we find that the ionic abundance of CaII K relative to HI, A = log( N( CaK)/ N( HI)) for low- velocity Galactic gas ranges from - 8.3 to - 8.8 dex, with HI column densities varying from 3- 6 x 10(20) cm(-2). For Magellanic Bridge gas, the values of A are similar to 0.5 dex higher, ranging from similar to- 7.8 to - 8.2 dex, with N( HI) = 1- 5 x 1020 cm(-2). Higher values of A correspond to lower values of N( HI), although numbers are small. For the sightline towards B 0251 - 675, the Bridge gas has two different velocities, and in only one of these is CaII tentatively detected, perhaps indicating gas of a different origin or present-day characteristics ( such as dust content), although this conclusion is uncertain and there is the possibility that one of the components could be related to the Magellanic Stream. Higher signal-to-noise CaII K data and higher resolution H. data are required to determine whether A changes with N( HI) over the Bridge and if the implied difference in the metalicity of the two Bridge components towards B 0251-675 is real.

Observations towards early-type stars in the ESO-POP Survey - II. Searches for intermediate- and high-velocity clouds

We present Ca it K and Ti it optical spectra of early-type stars taken mainly from the ultraviolet and visual echelle spectrograph (LIVES) Paranal Observatory Project, plus H 1 21-cm spectra, from the Vila-Elisa and Leiden-Dwingeloo Surveys, which are employed to obtain distances to intermediate- and high-velocity clouds (IHVCs). H I emission at a velocity of -117 km s(-1) towards the sightline HD 30677 (l, b = 190 degrees.2, -22 degrees.2) with column density -1.7 x 10(19) cm(-2) has no corresponding Ca Pi K absorption in the LIVES spectrum, which has a signal-to-noise ratio (S/N) of 610 per resolution element. The star has a spectroscopically determined distance of 2.7 kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185 with 1, b = 222 0, -10 degrees.1), H1 at a velocity of +122 km s(-1) and column density of 1.2 x 10(19) cm(-2) is seen. The corresponding Ca Pi K spectrum has a S/N of 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9 kpc towards this parcel of gas that may be an intermediate-velocity (IV) cloud. The lack of IV Ca it absorption towards HD 196426 (1, b = 45 degrees.8, -23 degrees.3) at a S/N of 500 reinforces a lower distance limit of -700 pc towards this part of complex gp, where the H I column density is 1.1 x 1019 cm(-2) and velocity is +78 km s(-1). Additionally, no IV Cart is seen in absorption in the spectrum of HD 19445, which is strong in H I with a column density of 8 x 10(19) cm(-2) at a velocity of - -42 km s(-1), placing a firm although uninteresting lower distance limit of 39 pc to this part of IV South. Finally, no high-velocity Call K absorption is seen towards HD 115363 (l, b = 306.0,-1.0) at a S/N of 410, placing a lower distance of -3.2 kpc towards the HVC gas at velocity of - +224 km s(-1) and WE column density of 5.2 x 10(19) cm(-2). This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of Ca it K absorption sets a lower distance of -3.2 kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System.

Review of: Ucko, P; Hunter, M; Clark, A; and David, A. Avebury reconsidered: from the 1660s to the 1990s. London, Unwin Hyman. 1991.

, Albion, 1993. 25(2): p. 318-9.

John Thompson: Seeing through China

In 1848, Karl Marx predicted that a flow of cheap commodities would be the heavy artillery which would batter down all Chinese walls and open up the country to the west (Marx, 1978, p. 477). The Scottish photographer John Thomson (1837-1921) was both chronicler of and participant in the early moments of this process. Thomson was a commercial photographer who first arrived in the Far East in 1862. He earned the moniker of 'China' in a decade-long stay during which he photographed what he considered to be the key aspects of its culture and landscape. In this body of work, Illustrations of China and its People (first published in 1874) is perhaps the most comprehensive. It explores, through two hundred photographs and accompanying texts, a series of phenomena from the macro-scale of landscape, infrastructure and industry to the smaller scales of streetscapes, domestic spaces, individual portraits, and other details of everyday life. Despite his own description of the volumes as encyclopedic, Illustrations is geographically quite limited. Thomson's explorations into the hinterland proceed up the country’s principal rivers from those coastal ports which had already been wrested into western hands during the Opium Wars (of the 1840s) and subsequently opened up to trade. This is perhaps one of the reasons why Illustrations has been described as an explicitly colonial text, a guide-book for the prospective settler whose content offered the strategic knowledge of land, culture and natural resources necessary if the territorial advantages of the coastal periphery were to extended to the interior (Jeffrey, 1981, p. 64). It can also be argued, however, that Thomson’s volume offered justification for a potential colonial presence. Faced with a civilization whose history was as sophisticated as the west, it depicts a culture that is static and moribund, its addiction to traditional values an impediment to progress. While this is perhaps most explicit in the texts of Illustrations of China, it can also be seen in the images whose uniform chemical rendering also serves to make an essentially diverse culture seem homogenous. Yet it is these images that distinguish Illustrations from previous attempts to collate China’s culture and landscape. Here, the mechanical precision of his camera captures a reality that often subverts the colonial narrative, confounding stereotypes as Thomson’s mass-produced images allow another China to emerge.