High resolution cosmid and P1 maps spanning the 14 Mb genome of the fission yeast S. pombe.

Gridded on high density filters, a P1 genomic library of 17-fold coverage and a cosmid library of 8 genome equivalents, both made from S. pombe strain 972h-, were ordered by hybridizing genetic markers and individual clones from the two libraries. Yeast artificial chromosome (YAC) clones covering the entire genome were used to subdivide the libraries, and hybridization of short oligonucleotides and DNA pools made from randomly selected cosmids provided further mapping information. Restriction digests were generated as an independent confirmation of the clone order. The high resolution clone map was aligned to the genetic map and the physical Notl and YAC maps. The usefulness of the various mapping techniques and cloning procedures could be assessed upon the different data sets.

Theoretical predictions and experimental observations of genomic mapping by anchoring random clones.

Genome mapping by anchoring random clones has recently been the subject of intensive theoretical study. In this paper, differences between published predictions of properties of anchored groups of clones ("contigs") are analyzed and simplifications of the mathematical formulae describing these properties are presented. The theoretical predictions are compared with the experimental results from the physical mapping of the genome of Schizosaccharomyces pombe. Information about the number of genome sections with no anchored clone on them ("oceans") and the number of undetected overlaps between the contigs at a given stage of the experiment is required for the decision to change from the random strategy to that of a directed closure of gaps. We demonstrate that the expected number of oceans can be approximated by the number of groups of clones anchored by a single probe ("singletons"), as can the expected number of undetected overlaps between contigs by the number of contigs containing more than one anchor.

Complete coverage of the Schizosaccharomyces pombe genome in yeast artificial chromosomes.

The genome of the fission yeast, Schizosaccharomyces pombe, consists of some 14 million base pairs of DNA contained in three chromosomes. On account of its excellent genetics we used it as a test system for a strategy designed to map mammalian chromosomes and genomes. Data obtained from hybridization fingerprinting established an ordered library of 1,248 yeast artificial chromosome clones with an average size of 535 kilobases. The clones fall into three contigs completely representing the three chromosomes of the organism. This work provides a high resolution physical and clone map of the genome, which has been related to available genetic and physical map information.

The 2.5-12 micrometers spectrum of comet Halley from the IKS-VEGA experiment.

The infrared instrument IKS flown on board the VEGA space probes was designed for the detection of emission bands of parent molecules, and for a measurement of the size and temperature of the thermal emitting nuclear region. The instrument had three channels with cooled detectors: an "imaging channel" designed to modulate the signal of the nucleus and two spectroscopic channels operating at 2.5-5 and 6-12 micrometers, respectively, equipped with circular variable filters of resolving power approximately 50. This paper presents and discusses the results from the spectral channels. On VEGA 1, usable spectra were obtained at distances D from the comet nucleus ranging from 250,000 to 40,000 km corresponding to fields of view 4000 and 700 km in diameter, respectively. The important internal background signal caused by the instrument itself, which could not be cooled, had to be eliminated. Since no sky chopping was performed, we obtain difference spectra between the current spectrum and a reference spectrum with little or no cometary signal taken at the beginning of the observing sequence (D approximately 200,000 km). Final discrimination between cometary signal and instrumental background is achieved using their different time evolution, since the instrumental background is proportional to the slow temperature drift of the instrument, and the cometary signal due to parent molecules or dust grains is expected to vary in first order as D-1. The 2.5-5 micrometers IKS spectra definitely show strong narrow signals at 2.7 and 4.25 micrometers, attributed to the nu 3 vibrational bands of H2O and CO2, respectively, and a broader signal in the region 3.2-3.5 micrometers, which may be attributed to CH-bearing molecules. All these signals present the expected D-1 intensity variation. Weaker emission features at 3.6 and 4.7 micrometers could correspond to the nu 1 and nu 5 bands of H2CO and the (1 - 0) band of CO, respectively. Molecular production rates are derived from the observed emissions, assuming that they are due to resonance fluorescence excited by the Sun's infrared radiation. For the strong bands of H2O and CO2, the rovibrational lines are optically thick, and radiative transfer is taken into account. We derive production rates, at the moment of the VEGA 1 flyby, of approximately 10(30) sec-1 for H2O, approximately 2.7 x 10(28) sec-1 for CO2, approximately 5 x 10(28) sec-1 for CO, and 4 x 10(28) sec-1 for H2CO, if attributions to CO and H2CO are correct. The production rate of carbon atoms in CH-bearing molecules is approximately 9 x 10(29) sec-1 assuming fluorescence of molecules in the gas phase, but could be much less if the 3.2-3.5 micrometers emission is attributed to C-H stretch in polycyclic aromatic hydrocarbons or small organic grains. In addition, marginal features are present at 4.85 and 4.45 micrometers, tentatively attributed to OCS and molecules with the CN group, respectively. Broad absorption at 2.8-3.0 micrometers, as well as a narrow emission at 3.15 micrometers, which follow well the D-1 intensity variation, might be due to water ice. Emission at 2.8 micrometers is also possibly present, and might be due to OH created in vibrationally excited states after water photodissociation. The 6-12 micrometers spectrum does not show any molecular emission, nor emission in the 7.5-micrometers region. The spectrum is dominated by silicate emission showing a double structure with maxima at 9.0 and 11.2 micrometers, which suggests the presence of olivine.