%R 1996A&AS..117..417H
%J-444
%A Heraudeau P., Simien F., Mamon G.A.
%T Near-infrared surface photometry of spiral galaxies. I. The data.
%F 1996.05.29
%B We present K'-band surface photometry of a sample of 31 inclined Sa-Scd galaxies, together with additional J- and H-band data for four of them. In this first paper of a series, profiles are presented, together with global and isophotal parameters. Our profiles are compared to similar B, R and I data collected from other sources. Three galaxies exhibit previously unknown small bars in their center, while in five others, such bars may also be present. Four objects present a
narrow elongated feature in their center aligned with their major axis, which could be an inward extension of the disk. A few galaxies display very thin spiral arms. Color-color diagrams indicate that the extinction inside the four galaxies for which we have JHK' images is limited to A_V_<2.
%K galaxies: spiral - galaxies: photometry - infrared: galaxies

%R 1996A&AS..117..445C
%J-447
%A Carquillat N., Ginestet J.M.
%T Contribution a l'etude des binaires des types F, G, K, M. VII. HD 147395, une geante M binaire spectroscopique. Contribution to the study of F, G, K, M binaries. VII. HD 147395, a M giant spectroscopic binary.
%F 1996.05.29
%B HD 147395, a giant M2 star, was found to be a spectroscopic binary by the Mount Wilson astronomers some time ago, but its orbit remained unknown so far. Radial velocity observations carried out at the Observatoire de Haute-Provence with the CORAVEL spectrovelocimeter permitted us to obtain the orbital elements of this binary. They are as follows: P=335.537days; T=4448335.0JD; {omega}=336.9deg ; e=0.235; K=16.87km/s; V_0_=-20.12km/s; a_1_sini=75.67Gm;
f(M)=0.154M_{sun}_. The spectral type of the primary, and the f(M) value, lead to M_2_>=1.0+/-0.2M_{sun}_ for the mass of the unseen companion. According to the color indices B-V and U-B of the system, the secondary star should be a F5V. We estimate at 1.25+/-0.1UA the mean linear separation of the components; nevertheless, both the distance of this binary (d~275pc) and the expected value of {DELTA}m seem too important for the system to be resolved by interferometry.
%K stars: individual: \object{HD 147395} - stars: spectroscopic binaries - stars: fundamental parameters

%R 1996A&AS..117..449Z
%J-465
%A Zwitter T., Munari U.
%T CCD spectrophotometry of CVs. III. 3270-9000A atlas for 38 faint systems.
%F 1996.05.29
%B A 7 A resolution, 3270-9000A spectrophotometric atlas is presented for 38 objects from the Downes & Shara (1993) catalogue of Cataclysmic Variables (CVs). The stars were selected among those listed as lacking published spectra. As for previous papers in this series, the aim is to check the CV status of the objects spectroscopically and to provide high quality absolute spectrophotometry over a wide wavelength range. For all programme stars accurate UBVRI magnitudes,
continuum fluxes at selected wavelengths and integrated fluxes of emission lines are derived. Among the 38 programme stars, only 16 clearly show a CV-like spectrum. In the three papers of this series we have so far surveyed 94 objects among the entries in the Downes and Shara catalogue which lack spectroscopic confirmation. The fraction of validated CVs is 56%. For objects from the Palomar-Green survey the rate of confirmed CVs is particularly low, amounting to only 23%.
%K stars: cataclysmic variables - white dwarfs - atlases

%R 1996A&AS..117..467G
%J-473
%A Garnier R., Paturel G., Petit C., Marthinet M.C., Rousseau J.
%T An image database. II. Catalogue between {delta}=-30deg and {delta}=70deg.
%F 1996.05.29
%B A preliminary list of 68.040 galaxies was built from extraction of 35.841 digitized images of the Palomar Sky Survey (Paper I). For each galaxy, the basic parameters are obtained: coordinates, diameter, axis ratio, total magnitude, position angle. On this preliminary list, we apply severe selection rules to get a catalog of 28.000 galaxies, well identified and well documented. For each parameter, a comparison is made with standard measurements. The accuracy of the raw
photometric parameters is quite good despite of the simplicity of the method. Without any local correction, the standard error on the total magnitude is about 0.5 magnitude up to a total magnitude of B_T_=17. Significant secondary effects are detected concerning the magnitudes: distance to plate center effect and air-mass effect.
%K galaxies: general - catalogue - galaxies: photometry

%R 1996A&AS..117..475F
%J-486
%A Fiorucci M., Tosti G.
%T Automatic optical monitoring of 10 blazars.
%F 1996.05.29
%B We report the BVR_c_I_c_ data for 10 blazars observed in the first phase of a long-term photometric monitoring program of about 30 objects. The observations were carried out with a 0.40-m automatic imaging telescope, recently developed by our group at the Perugia University Observatory. During our period of observation 1215+303 and 1424+240 were at their highest values of magnitude, while 0754+100 and 0829+043 displayed large amplitude flares. We further report optical
data of Mrk 501 during the same period in which TeV {gamma}-rays were detected by the Whipple Observatory.
%K galaxies: active - BL Lacertae objects: general

%R 1996A&AS..117..487M
%J-496
%A Maia M.A.G., Suzuki J.A., da Costa L.N., Willmer C.N.A., Rite C.
%T New southern galaxies with active nuclei. II.
%F 1996.05.29
%B This paper contains a list of new AGN candidates identified from the examination of 3500 optical spectra contained in the database of the Southern Sky Redshift Survey Extension (SSRS2). The classification of galaxies was done using standard diagnostics and a total of (5) Seyfert 1, (12) Seyfert 2 and (10) LINERs were found. We also present a list of 60 galaxies for which we could not secure a definite classification, but which might present some level of nuclear activity.
%K galaxies: active; Seyfert: redshifts - surveys

%R 1996A&AS..117..497H
%J-518
%A Herbstmeier U., Kalberla P.M.W., Mebold U., Weiland H., Souvatzis I., Wennmacher A., Schmitz J.
%T Single-dish and aperture synthesis H I observations towards the Draco nebula. I. The data.
%F 1996.05.29
%B We describe 21-cm line observations of the Draco nebula region and present the results as channel maps. These observations have been performed with the Effelsberg 100-m telescope, the Westerbork Synthesis Radiotelescope, and the Very Large Array. The measurements reveal the full extent of the cloud as well as the detailed morphological and kinematical structure of several subareas. A list of continuum point sources found in the aperture synthesis maps is included.
%K ISM: clouds - ISM: individual objects: \object{Draco cloud} - ISM: structure - radio lines: ISM

%R 1996A&AS..117..519E
%J-555
%A Escalera E., MacGillivray H.T.
%T Detection of structures on multiple scales around the South Galactic Pole. A two-dimensional analysis of the COSMOS/UKST Southern Sky Galaxy Catalogue.
%F 1996.05.29
%B We report the results of a 2D analysis of distributions of galaxies in a search for structures on a wide range of scales, from clusters up to superclusters and beyond, including the identification of voids. The structures are identified in data from the COSMOS/UKST Southern Sky Galaxy Catalogue (CUSSGC). The subsample used in this first investigation contains some 1.4x10^6^ galaxies in an area of ~69x44degrees around the South Galactic Pole. From our analysis, we find
25 very large-scale structures (of 10 degrees or more in extent), about 60 structures of intermediate scales (superclusters and/or elongated features), and more than 220 cluster-sized objects. All these features are significant, having high confidence levels for detection. Some extended voids are also detected in this area, likewise with high significance. This work is based on the use of the wavelet transform, the method of which has already been extensively described in a
previous paper in which we demonstrated the principle of the technique. The wavelet analysis gives the position of the structures detected, together with significance levels and some parametrisation of their properties (extent, population, elongation, etc). Ultimately, our aim is the construction of a large and homogeneous database of structures on all scales in this important part of the southern sky.
%K cosmology: large-scale structure of Universe - galaxies: clusters - surveys - methods: data analysis

%R 1996A&AS..117..557C
%J-559
%A Chandra S., Maheshwari V.U., Sharma A.K.
%T Einstein A-coefficients for vib-rotational transitions in CO.
%F 1996.05.29
%B Einstein A-coefficients for vib-rotational transitions in CO isotopomers, for vibrational quantum number v up to 20, rotational quantum number J up to 140, and {DELTA}v up to 4, are calculated. The change in J is governed by the selection rules {DELTA}J=+/-1. These coefficients play an important role in astronomy, as CO is the most abundant molecule after H_2_, and has been observed in almost all the astronomical objects.
%K ISM: molecules - molecular data

%R 1996A&AS..117..561H
%J-568
%A Hure J.M., Roueff E.
%T Analytic representations of rovibrational dipole matrix elements for the CO molecule and its isotopomers.
%F 1996.05.29
%B We report new calculations of transition matrix elements for more than thirty thousand infrared lines of the CO molecule and its isotopomers inside the X^1^{SIGMA}^+^ ground electronic state. These lines belong to the {DELTA}v=1, 2, 3 bands involving very high excited states such as v'<=41 and J'<=133. The transition matrix elements have been calculated from an accurate solution of the Schroedinger equation by using two different theoretical electric dipole moment
functions (Werner 1981; Langhoff & Bauschlicher 1995). For low lying levels, our data compare satisfactorily with experimental ones and related works (Goorvitch & Chackerian 1994a, b; Chackerian et al. 1994, Goorvitch 1994). Moreover, we make predictions for oscillator strengths and Einstein coefficients involving high excited transitions. In addition, we report simple analytic formulae that fit our results for ^12^C^16^O with an accuracy better than 10^-2^ as a function of
m=[J'(J'+1)-J"(J"+1)]/2 for each vibrational sequence and band. They offer an easy way to compute the various intensities of these rovibrational transitions whose transition energies may be introduced via the available Dunham coefficients.
%K molecular data - ISM: molecules

%R 1996A&AS..117..569M
%J-582
%A Muciaccia P.F., Bersanelli M., De Bernardis P., Vittorio N., Masi S., Mandolesi N.
%T Sub-degree CMB anisotropy from space. I. Sky coverage and sensitivity.
%F 1996.05.29
%B Decisive progress in cosmology is expected from a space mission dedicated to an extensive mapping of the Cosmic Microwave Background (CMB) with high angular and temperature sensitivity. Based on the European Space Agency COBRAS/SAMBA mission concept, we have studied the attainable sensitivity and sky coverage taking into account the effect of solar-system sources for the two far-Earth candidate orbits (Lagrangian points Moon-Earth L5 and Sun-Earth L2). We also take into
account the microwave emission of the Galaxy in limiting the useful sky coverage. Our results provide a quantitative assessment of the relative observational merits of the two orbit options, and show that the Sun-Earth L2 orbit allows significantly better observational conditions.
%K cosmic microwave background - space vehicles - cosmology: observations

%R 1996A&AS..117..583M
%J-591
%A Michard R.
%T Artefacts in the deconvolution of images of E-S0 galaxies.
%F 1996.05.29
%B Unexpected circumnuclear isophotal structures were observed during tests of Lucy's deconvolution technique, performed upon high resolution CFHT frames. They contain an enhanced nuclear disk surrounded by a "boxy" ring; an upward hump in ellipticity corresponds with this ring. Such structures are produced in the deconvolution of synthetic images having large enough surface brightness gradients and ellipticities, as is the case for two of our test galaxies. Similar
stuctures occur in convolving and deconvolving model galaxies with a model of the HST's PSF prior to the telescope renovation, but they are limited in radial extent up to less than 1 arcsec of isophotal major axis. If the deconvolution is performed with a PSF differing somewhat from the one used in the convolution, large and far extending artefacts can occur.
%K galaxies: elliptical and lenticulars, cD - galaxies: photometry - techniques: image processing