Detection of X-ray emission from the host clusters of 3CR quasars     

C. S. Crawford  I. Lehmann  A. C. Fabian  M. N. Bremer  G. Hasinger 《Monthly notices of the Royal Astronomical Society》1999,308(4):1159-1172

We report the detection of extended X-ray emission around several powerful 3CR quasars with redshifts out to 0.73. The ROSAT HRI images of the quasars have been corrected for spacecraft wobble and compared with an empirical point-spread function. All the quasars examined show excess emission at radii of 15 arcsec and more, the evidence being strong for the more distant objects and weak only for the two nearest ones, which are known from other wavelengths not to lie in strongly clustered environments. The spatial profile of the extended component is consistent with thermal emission from the intracluster medium of moderately rich host clusters to the quasars. The total luminosities of the clusters are in the range ∼4×10⁴⁴–3×10⁴⁵ erg s⁻¹, assuming a temperature of 4 keV. The inner regions of the intracluster medium are, in all cases, dense enough to be part of a cooling flow.  相似文献   

Tectonic Plate Parameters Estimated in the International Terrestrial Reference Frame ITRF2008 Based on SLR Stations     

Katarzyna Kraszewska  Marcin Jagoda  Miloslawa Rutkowska 《Acta Geophysica》2016,64(5):1495-1512

This paper concerns an analysis of the accuracy of estimated parameters Ω (Φ, Λ, ω) which define the tectonic plate motions. The study is based on the velocities of station positions published by ITRF2008 for Satellite Laser Ranging (SLR) technique. The Eurasian, African, North American and Australian plates were used in the analysis. Influence of the number and location of stations on the plate surface on estimation accuracy of the tectonic plate motion parameters was discussed. The results were compared with the APKIM 2005 IGN model. In general, a remarkable concurrence agreement between our solutions and the APKIM 2005 model was found.  相似文献   

DETECTING ENERGY-BALANCE MODIFICATIONS AT THE ONSET OF SPRING     

Mark D. Schwartz  Todd M. Crawford 《自然地理学》2013,34(5):394-409

The nature of energy-flux transitions during the onset of midlatitude spring has not been widely examined, despite their critical implications for global-scale biospheric measures and climate change. Further conventional assessment of these phenomena across multiple locations is restricted by satellite-derived data limitations, and the paucity of surface measurement sites. In this paper, we explore a new phenology-based strategy for evaluating the spring surface energy-balance shift that can address these concerns. Our technique can reflect native-species responses and atmospheric surface layer change at a variety of sites, using synoptic-scale first leaf and first bloom phenology models. We test the approach at three locations with diverse climates, and within a group of stations in the state of Oklahoma, which has moderate climate variations across an east-to-west gradient. The results show that the onset of spring in midlatitudes is a modally abrupt (rather than gradual) seasonal transition in terms of energy balance (sensible and latent heat levels) and carbon-flux change that can be linked directly to vegetation phenology. The consistent temporal pattern and magnitude of flux variations across diverse sites suggest that this technique has potential as a proxy for spring energy-balance change at many locations. [Key words: phenology, spring, energy balance, North America.]  相似文献   

Petrogenesis and chronology of lunar meteorite Northwest Africa 4472: A KREEPy regolith breccia from the Moon     

K.H. Joy  R. Burgess  V.A. Fernandes  I.A. Crawford  A.T. Kearsley  EIMFg 《Geochimica et cosmochimica acta》2011,75(9):2420-7225

Northwest Africa (NWA) 4472 is a polymict lunar regolith meteorite. The sample is KREEP-rich (high concentrations of potassium, rare earth elements and phosphorus) and comprises a heterogeneous array of lithic and mineral fragments. These clasts and mineral fragments were sourced from a range of lunar rock types including the lunar High Magnesian Suite, the High Alkali Suite, KREEP basalts, mare basalts and a variety of impact crater environments. The KREEP-rich nature of NWA 4472 indicates that the sample was ejected from regolith on the nearside of the Moon in the Procellarum KREEP Terrane and we have used Lunar Prospector gamma-ray remote sensing data to show that the meteorite is most similar to (and most likely sourced from) regoliths adjacent to the Imbrium impact basin.U-Pb and Pb-Pb age dates of NWA 4472 phosphate phases reveal that the breccia has sampled Pre-Nectarian (4.35 Ga) rocks related to early episodes of KREEP driven magmatism. Some younger phosphate U-Pb and Pb-Pb age dates are likely indicative of impact resetting events at 3.9-4 Ga, consistent with the suggested timing of basin formation on the Moon. Our study also shows that NWA 4472 has sampled impact melts and glass with an alkali-depleted, incompatible trace element-rich (high Sc, low Rb/Th ratios, low K) compositional signature not related to typical Apollo high-K KREEP, or that sampled by KREEPy lunar meteorite Sayh al Uhaymir (SaU) 169. This provides evidence that there are numerous sources of KREEP-rich protoliths on the Moon.  相似文献   

The age of the Cuddapah and Kurnool systems,southern India     

A. R. Crawford  W. Compston 《Australian Journal of Earth Sciences》2013,60(4):453-464

In southern India the older Precambrian is overlain unconformably in the Cuddapah Basin by the Cuddapah and Kurnool Systems. The former is tilted and unmetamorphosed in the west but eastwards becomes strongly folded and metamorphosed. It contains lavas and sills, particularly in the lower two groups, is intruded by dolerites and at Chelima by diatremes of kimberlitic affinities related to those intruding the older gneisses west of the Cuddapah Basin in the Wajrakarur area. The Kurnool System lacks any igneous rocks; its basal conglomerate is diamondi‐ferous.

Rb‐Sr dating of lava samples from the lowest group of the Cuddapah System shows that the age of the base of the system may be as great as 1,700 m.y. Together with data for a granite which intrudes probable Cuddapah rocks near the disturbed eastern margin of the basin the data imply that the base is unlikely to be younger than 1,555 m.y. Metamorphism affected some lavas at about 1,360 m.y. The diatremes have two ages of intrusion, about 1,225 m.y. and 1,140 m.y., the latter being the age of the Majhgawan pipe near Panna in northern India. Pre‐Kurnool dolerites have an age of 980 ±110 m.y.

The lavas and dolerites show a range of initial ⁸⁷Sr/⁸⁶Rb ratios from about 0.704 to 0.708 and possibly 0.712.

The age data suggest that no simple correlation can be made with other Precambrian sequences in northern peninsular India. Deposition of the Cuddapah System appears to have started well before the start of the deposition of the Vindhyan System, while the Kurnool System is coeval with only part of the Upper Vindhyan. The data also suggest that present interpretations of the structural development of the Cuddapah Basin may need some revision.  相似文献   

Sediment shear properties from seafloor compliance measurements: Faroes-Shetland basin case study     

Wayne C. Crawford  Satish C. Singh 《Geophysical Prospecting》2008,56(3):313-325

Shear properties provide important information about the lithology, fluid content and stability of sediments but are difficult to measure using conventional seismics in the marine environment. Seafloor compliance measurements are sensitive to subsurface shear properties but have only been used in the Pacific Ocean and on shallow coastal shelves, where the source wave energy is known to be strong. We show here that seafloor compliance measurements can provide useful information about shear properties of marine sediments in less energetic settings and under high noise conditions caused by strong seafloor currents. We measured compliance at three sites in the Faroes‐Shetland sedimentary basin north of the Atlantic ocean. The sites have 1000 times higher noise levels than quiet seafloor sites and the source wave power is highly variable, but the data still reveal significant differences in sediment properties between two sites down to 2 kilometres beneath the seafloor. The first site, at the northern end of the basin, has an average shear velocity of 400 m/s in the upper 0.6 kilometres beneath the seafloor, increasing to approximately 2100 m/s at 2 kilometres beneath the seafloor. The second site, further south and to the west of the basin axis, has an average shear velocity of 150 m/s in the upper 0.6 kilometres beneath the seafloor, increasing to 1400 m/s at 2 kilometres beneath the seafloor. The sediments are probably unconsolidated in the upper 0.6 kilometres beneath the seafloor at both sites, with a mean grain size of 1 μm at the southern site and 20 μm at the northern site. The southern site has higher porosity at all depths and a higher risk of borehole collapse during drilling.  相似文献   

MoonLITE: A UK-led mission to the Moon     

Ian Crawford  Alan Smith 《Astronomy& Geophysics》2008,49(3):3.11-3.14

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Determination of High Field Strength Elements, Rb, Sr, Mo, Sb, Cs, Tl and Bi at ng g⁻¹ Levels in Geological Reference Materials by Magnetic Sector ICP-MS after HF/HClO₄ High Pressure Digestion     

Zongshou Yu  Philip Robinson  Ashley T. Townsend  Carsten Mnker  Anthony J. Crawford 《Geostandards and Geoanalytical Research》2000,24(1):39-50

Six low abundance rock reference materials (basalt BIR-1, dunite DTS-1, dolerite DNC-1, peridotite PCC-1, serpentine UB-N and basalt TAFAHI) have been analysed for high field strength elements (Zr, Nb, Hf, Ta, Th and U), Rb, Sr, Mo, Sb, Cs, Tl and Bi at ng g⁻¹ levels (in rock) by magnetic sector inductively coupled plasma-mass spectrometry after HF/HClO₄ high pressure decomposition. The adopted method uses only indium as an internal standard. Detection limits were found to be in the range of 0.08 to 16.2 pg ml⁻¹ in solution (equivalent to 0.08 to 16.2 ng g⁻¹ in rock). Our data for high field strength elements, Rb, Sr, Mo, Sb, Cs, Tl and Bi for the six selected low abundance geological reference materials show general agreement with previously published data. Our Ta values in DTS-1 and PCC-1 (1.3 and 0.5 ng g⁻¹) are lower than in previously published studies, providing smooth primitive mantle distribution patterns. Lower values were also found for Tl in BIR-1, DTS-1 and PCC-1 (2, 0.4 and 0.8 ng g⁻¹). Compared with quadrupole ICP-MS studies, the proposed magnetic sector ICP-MS method can generally provide better detection limits, so that the measurement of high field strength elements, Rb, Sr, Mo, Sb, Cs, Tl and Bi at ng g⁻¹ levels can be achieved without pre-concentration, ion exchange separation or other specialised techniques.  相似文献   

Detection of a variable interstellar absorption component towards δ Orionis A     

R. J. Price  I. A. Crawford  M. J. Barlow 《Monthly notices of the Royal Astronomical Society》2000,312(3):L43-L48

Observations of δ Ori A made with the UHRF in its highest resolution mode ( R ≈900 000) have revealed the presence of a cool ( T _k350 K) variable absorption component at a heliocentric velocity of +21.3 km s⁻¹. The component is detected in Na  i D₁, where clear hyperfine splitting is seen, and Ca  ii K. Comparison of our data with existing spectra suggests that the component has consistently increased in strength from 1966 to 1994, and subsequently reduced in intensity by 1999. Following a discussion of the possible origins of this component it is concluded that an interstellar, rather than circumstellar, origin is most likely. This is one of very few detections of variable interstellar absorption reported in the literature, and we suggest an origin within filamentary material associated with the expanding H  i shell surrounding the Orion–Eridanus superbubble.  相似文献   

Extended line emission around seven radio-loud quasars at redshift z ∼ 2     

R. J. Wilman  R. M. Johnstone  C. S. Crawford 《Monthly notices of the Royal Astronomical Society》2000,317(1):9-22

We present near-infrared spectra of seven radio-loud quasars with a median redshift of 2.1, five of which were previously known to have Ly α nebulae. Extended [O  iii ] λ 5007 and H α emission are evident around six objects, at the level of a few times 10⁻¹⁶ erg cm⁻² arcsec⁻² s⁻¹ within ≃2 arcsec of the nucleus (≡16 kpc in the adopted cosmology). Nuclear [O  ii ] λ 3727 is detected in three of the five quasars studied at this wavelength and clearly extended in one of them.
The extended [O  iii ] tends to be brighter on the side of the nucleus with the stronger, jet-like radio emission, indicating at least that the extranuclear gas is distributed anisotropically. It is also typically redshifted by several hundred km s⁻¹ from the nuclear [O  iii ], perhaps because of the latter being blueshifted from the host galaxy's systemic velocity. Alternatively, the velocity shifts could be due to infall (which is suggested by linewidths ∼1000 km s⁻¹ FWHM) in combination with a suitable dust geometry. Ly α /H α ratios well below the case B value suggest that some dust is present.
Photoionization modelling of the [O  iii ]/[O  ii ] ratios in the extended gas suggests that its pressure is around or less than a few times 10⁷ cm⁻³ K; any confining intracluster medium is thus likely to host a strong cooling flow. A comparison with lower redshift work suggests that there has been little evolution in the nuclear emission-line properties of radio-loud quasars between redshifts 1 and 2.  相似文献