%R 1998A&AS..130..207T
%J-214
%A Tovmassian H.M., Mazzarella J.M., Tovmassian G.H., Stoll D., Tiersch H.
%T Far-infrared emission from Shakhbazian Compact Galaxy Groups.
%M ds7280
%F 1998.05.26
%B Using the IRAS archives, we searched for far-infrared (FIR) counterparts of Shakhbazian Compact Groups of Galaxies (SCGGs). Reliable IRAS detections are identified at the positions of 24 out of 367 SCGGs; another 10 IRAS sources, located within ~2arcmin of SCGGs, are possibly associated with the corresponding galaxy groups. Some of these sources are not very reliable. Previous work has shown that the fraction of E and S0 galaxies in a representative sample of SCGGs is 77%,
while E and S0 galaxies comprise about 51% of galaxies in Hickson Compact Groups (HCGs). The higher fraction of early Hubble types, combined with their greater distances, explains the low IRAS detection rate of SCGGs (7-8%) compared to HCGs (64%). The FIR colors and morphological types of galaxies in the groups suggest that active star formation or Seyfert galaxies may be the main source of the FIR emission in the SCGGs detected by IRAS, perhaps originating as the result of
tidal interactions in the dense environments of these groups.
%K infrared: galaxies - galaxies: interactions

%R 1998A&AS..130..215S
%J-222
%A Sokolov N.A.
%T Effective temperatures of Ap stars.
%M ds1458
%F 1998.05.26
%B A new method of determination of the effective temperatures of Ap stars is proposed. The method is based on the fact that the slopes of the energy distribution in the Balmer continuum near the Balmer jump for ``normal" main sequence stars and chemically peculiar stars with the same T_eff_ are identical. The effective temperature calibration is based on a sample of main sequence stars with well known temperatures (Sokolov, 1995A&AS..110..553S). It is shown that the effective
temperatures of Ap stars are derived by this method in good agreement with those derived by the infrared flux method and by the method of Stepien & Dominiczak (1989A&A...219..197S). On the other hand, the comparison of obtained T_eff_ with T_eff_ derived from the color index (B2-G) of Geneva photometry shows a large scatter of the points, nevertheless there are no systematical differences between two sets of the data.
%K stars: chemically peculiar - stars: fundamental parameters

%R 1998A&AS..130..223N
%J-232
%A North P., Carquillat J.-M., Ginestet N., Carrier F., Udry S.
%T Multiplicity among peculiar A stars. I. The Ap stars HD 8441 and HD 137909, and the Am stars HD 43478 and HD 96391.
%M ds7203
%F 1998.05.26
%B We present the first results of a radial-velocity survey of cool Ap and Am stars. HD 8441 is not only a double system with P=106.357 days, but is a triple one, the third companion having an orbital period larger than 5000 days. Improved orbital elements are given for the classical Ap star HD 137909={beta} CrB by combining our radial velocities with published ones. We yield new orbital elements of the two Am, SB2 binaries HD 43478 and HD 96391. Good estimates of the
individual masses of the components of HD 43478 can be given thanks to the eclipses of this system, for which an approximate photometric solution is also proposed.
%K stars: spectroscopic binaries - stars: eclipsing binaries - stars: individual: HD 8441, HD 43478, HD 93961, HD 137909

%R 1998A&AS..130..233C
%J-234
%A Crosby N., Lund N., Vilmer N., Sunyaev R.
%T The WATCH solar X-ray burst catalogue.
%M ds1441
%F 1998.05.26
%B The WATCH experiment aboard the GRANAT satellite provides observations of the Sun in the deka-keV range covering the years 1990 through mid-1992. An introduction to the experiment is given followed by an explanation of how the WATCH solar burst catalogue was created. The different parameters listed for each burst is given and are furthermore explained.
%K catalogs - sun: activity; flares; X-rays, gamma rays

%R 1998A&AS..130..235S
%J-244
%A Samain E., Mangin J.F., Veillet C., Torre J.M., Fridelance P., Chabaudie J.E., Feraudy D., Glentzlin M., Pham Van J., Furia M., Journet A., Vigouroux G.
%T Millimetric Lunar Laser Ranging at OCA (Observatoire de la Cote d'Azur).
%M ds1427
%F 1998.05.26
%B The Lunar Laser Ranging station at the Observatoire de la Cote d'Azur, France, permits to measure the Earth-Moon distance with millimetric precision. Applications in astronomy, lunar science, geodesy, and gravitation are summarised. Expected scientific results with millimetric Lunar Laser Ranging data are presented. A complete error budget is given, showing that the precision is mainly limited by the orientation and the size of the corner cube arrays placed on the Moon.
The measurement accuracy is degraded by the bad knowledge of the air index. The time stability, computed from the lunar echoes, permits to extract the real precision of the Earth-Moon distance and to optimise the integration time of the normal points.
%K moon - gravitation - time instrumentation: miscellaneous

%R 1998A&AS..130..245V
%J-250
%A Vaz L.P.R., Andersen J., Casey B.W., Clausen J.V., Mathieu R.D., Heyer I.
%T Four-colour photometry of eclipsing binaries. XXXIX. Light curves of the pre-main sequence triple system TY Coronae Australis.
%M ds1433
%F 1998.05.26
%B Complete uvby light curves of the detached Herbig Be eclipsing binary TY Coronae Australis are presented. A total of 1789 photometric measurements in each of the four colours were obtained in 1989 and in 1992-1994. A detailed analysis of the y light curve obtained in 1992-1993 is published separately Casey et al. (1997, AJ, in press, Paper III). The reflection nebula around the system contributes about 30% of the light in all four passbands. Here we present and discuss the non-eclipse-related
photometric variability of the system. We suggest that these variations are the result of variable obscuration, possibly linked to dust shells physically associated to the system.
%K binaries: eclipsing: - stars: individual: TY CrA - stars: pre-main sequence

%R 1998A&AS..130..251L
%J-265
%A Longhetti M., Rampazzo R., Bressan A., Chiosi C.
%T Star formation history of early-type galaxies in low density environments. I. Nuclear line-strength indices.
%M ds1429
%F 1998.05.26
%B This paper is the first of a series (Longhetti et al., 1998A&AS..130..267L, 1998b, Paper III) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or signatures of interaction. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin & Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi & Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The                
spectral range covers 3700{AA}<{lambda}<5700{AA} at 2.1{AA} FWHM resolution. We measure 16 red ({lambda}>4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}<4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985), H+K(CaII) and H{delta}/FeI defined by
Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy Leonardi & Rose (1996AJ....111..182L). The determination of these indices, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T>10000K) which may be used for extending W92 fitting functions toward high temperatures.
%K galaxies: fundamental parameters - galaxies: elliptical and lenticular - galaxies: interactions - galaxies: evolution

%R 1998A&AS..130..267L
%J-283
%A Longhetti M., Rampazzo R., Bressan A., Chiosi C.
%T Star formation history of early-type galaxies in low density environments. II. Kinematics.
%M ds1431
%F 1998.05.26
%B The present paper is a companion of two others dedicated one to the measurement of the line-strength indices (Longhetti et al.,1998A&AS..130..251L) and the second to trace back the star formation history of a sample of early-type galaxies by comparing observed indices to the predictions of new spectro-photometric models Longhetti et al. (1998b, Paper III). The sample of 51 early-type galaxies in low density environments is composed of two sub-sets of galaxies: 21 shell galaxies from the Malin & Carter
(1983) catalogue (one of which shows double nucleous and has been considered as two separate objects) and 30 members of isolated interacting pairs from the Reduzzi & Rampazzo (1995ApL....30....1R) catalogue. Most of the objects show fine structures. The paper collects nuclear kinematic data together with the velocity and velocity dispersion curves of the stellar and gaseous components as a function of the distance from the galaxies centres. The galaxies heliocentric systemic velocity
compares within -1+/-32km/s with RC3 data, while their central velocity dispersion compares within 9+/-9km/s, 10+/-27km/s and 2+/-33km/s with Gonzalez (1993, Ph
.D. thesis), Davies et al. (1987ApJS...64..581D) and Carter et al. (1988MNRAS.235..813C) respectively. The detailed comparison between our velocity and velocity dispersion curves and those from several authors is discussed. 9 out of 22 shell galaxies nuclei show emission lines, 4 of which, using data in the literature, have line ratios
characteristic of LINERs. 10 members of pairs out of 30 show emission lines. RR 331a has a Seyfert like nucleus, while for the remaining galaxies the ([O III] {lambda} 5007)/H{beta} ratio is characteristic of low ionization regions. In a small fraction of the objects the emission component is detectable outside the central value. None of the objects in the sample shows counter-rotation of the gaseous versus the stellar component. The two components appear associated,
although, in two cases there is evidence that gas and stars lie on different planes. This latter phenomenon could be associated to accretion events. Emission lines in the central part of the RR 331a show a secondary component in the emission lines profile. E 2400100 has two nuclei embedded in the main body of the galaxy. The U-shape profile of the stellar velocity profile shows the ongoing interaction of the two nuclei. V/{sigma} profile of shell galaxies is, finally,
discussed in relation to the hypothesis of the accretion/merging origin of these galaxies.
%K galaxies: elliptical and lenticular - galaxies: interactions - galaxies: kinematics and dynamics

%R 1998A&AS..130..285C
%J-298
%A Contini T., Considere S., Davoust E.
%T Starbursts in barred spiral galaxies. III. Definition of a homogeneous sample of starburst nucleus galaxies.
%M ds1465
%F 1998.05.26
%B This paper presents optical long-slit spectroscopic observations of 105 barred Markarian IRAS galaxies. These observations are used to determine the spectral type (starburst or Seyfert) of emission-line regions in the nucleus and along the bar of the galaxies, in order to define a homogeneous sample of Starburst Nucleus Galaxies (SBNGs). Our selection criteria (ultraviolet excess, far infrared emission and barred morphology) have been very efficient for selecting
star-forming galaxies, since our sample of 221 emission-line regions includes 82% nuclear or extranuclear starbursts. The contamination by Seyferts is low (9%). The remaining galaxies (9%) are objects with ambiguous classification (Hii or LINER). The dust content and H{alpha} luminosity increase towards the nuclei of the galaxies. No significant variation of the electron density is found between nuclear and bar Hii regions. However, the mean H{alpha} luminosity and electron
density in the bar are higher than in typical disk Hii regions. We investigate different mechanisms for explaining the excess of nitrogen emission observed in our starburst nuclei. There is no evidence for the presence of a weak hidden active galactic nucleus in our starburst galaxies. The cause of this excess is probably a selective enrichment of nitrogen in the nuclei of the galaxies, following a succession of short and intense bursts of star formation. Our sample of SBNGs,
located at a mean redshift of ~0.015, has moderate H{alpha} (~10^41^erg/s) and far infrared (~10^10^L_{sun}_) luminosities. The types are distributed equally among early- and late-type giant spirals with a slight preference for Sbc/Sc types because of their barred morphology. The majority (62%) of SBNGs are isolated with no sign of gravitational interaction. In terms of distance, luminosity and level of interaction, SBNGs are intermediate between Hii galaxies and
luminous infrared galaxies.
%K galaxies: starburst - galaxies: active - galaxies: statistics - galaxies: ISM - infrared: galaxies

%R 1998A&AS..130..299S
%J-304
%A Sinachopoulos D., van Dessel E.
%T CCD astrometry and UBV photometry of visual binaries. II. Visual double stars with mainly G - type primaries and relatively small angular separation.
%M ds1470
%F 1998.05.26
%B Differences {DELTA}V of magnitude and {DELTA}(B-V) and {DELTA}(U-B) colours, as well as separations and position angles of 42 relatively close double stars are presented. The selection criteria of our sample are: the relatively small separation (between 2.5 and 5 arcseconds), magnitude difference under 1.25mag, and mainly G-type primaries. The CCD observations, performed at the 90 cm Dutch telescope at ESO, were made using the Bessel U, B and V filters; the astrometry was
done in the V filter only. From the analysis of the photometric data we conclude that 16 binaries in our sample have components with practically the same T_eff_, since they have almost the same colours; one binary has components with identical characteristics. We also note the good internal accuracy of the astrometric CCD measurements.
%K stars: binaries: visual - astrometry

%R 1998A&AS..130..305V
%J-310
%A Villata M., Raiteri C.M., Lanteri L., Sobrito G., Cavallone M.
%T BVR photometry of comparison stars in selected blazar fields. I. Photometric sequences for 10 BL Lacertae objects.
%M ds1482
%F 1998.05.26
%B We present photometric sequences in the Johnson's BV and Cousins' R bands in the fields of 10 BL Lacertae objects (BL Lacs) monitored at the Torino Astronomical Observatory. Data were taken during 14 photometric nights from February 1995 to May 1997. The 56 calibrated stars are brighter than V=16 and can be used as comparison objects in order to derive the BL Lac magnitudes. Finding charts are included for the stars identification.
%K galaxies: active - BL Lacertae objects: general

%R 1998A&AS..130..311M
%J-315
%A Mayer P., Niarchos P.G., Lorenz R., Wolf M., Christie G.
%T New times of minima and ephemeris for several OB eclipsing binaries.
%M ds1452
%F 1998.05.26
%B New times of minimum light were measured for several early-type eclipsing binaries: V337 Aql, V1182 Aql, V1331 Aql, IU Aur, QZ Car and V382 Cyg. The O-C diagram for these systems is discussed and new ephemeris is given for AH Cep; observation of AQ Cir is added. It is shown that the scatter of times of minima is several times larger than the measuring errors for most of the binaries studied.
%K stars: binaries: eclipsing - stars: early type

%R 1998A&AS..130..317J
%J-321
%A Jilinski E.G., Puliaev S.P., Penna J.L., Andrei A.H., Sinceac V., Chollet F., Delmas C.
%T Solar diameter observations with the Astrolabe at Observatorio Nacional - Rio de Janeiro.
%M ds7143
%F 1998.05.26
%B Observations of the solar diameter are reported from the astrolabe station at Observatorio Nacional. All the observations presented here were taken with the 1986-CERGA prototype of Variable Prism, which enables many diameter measurements per day and to observe all year round. The 1996 DANOF software for digital CCD image acquisition and data processing has been used. We adopted the recording of 46 CCD frames with direct and reflected images of the limbs along the Sun's
transit through the almucantar. The independent observable is the accurate UT datation of each frame. Here the first campaign results, from January to July/1997, are presented. An asymmetry between the east and west transit is noticeable. The west transit leads to a larger value for the mean semi-diameter and exhibits a larger standard deviation. No clear dependence is found upon the daily results, either on time or on observational parameters. The main outcome of this
campaign remains the average solar semi-diameter, from 1149 transits (863 East and 286 West), obtained as 959.21"+/-0.03".
%K sun: general, fundamental parameters - CCD observations

%R 1998A&AS..130..323V
%J-332
%A Vettolani G., Zucca E., Merighi R., Mignoli M., Proust D., Zamorani G., Cappi A., Guzzo L., Maccagni D., Ramella M., Stirpe G.M., Blanchard A., Cayatte V., Collins C., MacGillivray H., Maurogordato S., Scaramella R., Balkowski C., Chincarini G., Felenbok P.
%T The ESO Slice Project (ESP) galaxy redshift survey. III. The sample.
%M ds1479
%F 1998.05.26
%B 1.3cm The ESO Slice Project (ESP) is a galaxy redshift survey extending over about 23 square degrees, in a region near the South Galactic Pole. The survey is ~85% complete to the limiting magnitude b_J_=19.4 and consists of 3342 galaxies with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one-dimensional pencil beams; the spanned volume is ~5x10^4^h^-3^Mpc^3^ at the sensitivity peak (z~0.1). In this paper we
present the description of the observations and of the data reduction, the ESP redshift catalogue and the analysis of the quality of the velocity determinations. 
%K galaxies: distances and redshifts - cosmology: observations; large-scale structure of the Universe

%R 1998A&AS..130..333T
%J-339
%A Theureau G., Bottinelli L., Coudreau-Durand N., Gouguenheim L., Hallet N., Loulergue M., Paturel G., Teerikorpi P.
%T Kinematics of the local universe. VII. New 21-cm line measurements of 2112 galaxies.
%M ds1487
%F 1998.05.26
%B This paper presents 2112 new 21-cm neutral hydrogen line measurements carried out with the meridian transit Nancay radiotelescope. Among these data we give also 213 new radial velocities which complement those listed in three previous papers of this series. These new measurements, together with the HI data collected in LEDA, put to 6 700 the number of galaxies with 21-cm line width, radial velocity, and apparent diameter in the so-called KLUN sample.
%K catalogs - galaxies: distances and redshifts; ISM - radio lines: galaxies

%R 1998A&AS..130..341T
%J-358
%A Trasarti-Battistoni R.
%T Loose groups of galaxies in the Perseus-Pisces survey.
%M ds5593
%F 1998.05.26
%B We present a large catalog of loose groups of galaxies in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. All our catalogs contain about 200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. Groups
are identified with the adaptive Friends-Of-Friends (FOF) algorithm of Huchra & Geller (1982ApJ...257..423H), with suitable normalizations D_0_=0.231h^-1^Mpc and V_0_=350km/s at cz_0_=1000km/s. The luminosity function (LF) normalization {phi}_*_=0.02h^3^Mpc^-3^ appropriate for PPS yields a number density threshold {delta}n/n=~180 for the adopted D_0_, instead of {delta}n/n=~80 used in previous studies of other samples. However, the customary choice of D_0_ obtained
(through the LF) from a fixed mass overdensity {delta}{rho}/{rho}=80, well motivated in theory, suffers from important observational uncertainties and sample-to-sample variations of the LF normalization, and from major uncertainties in the relation between galaxy density n and mass density {rho}. We discuss how to self-consistently match FOF parameters among different galaxy samples. We then separately vary several FOF and sample parameters, and discuss their effect on group
properties. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. The group properties vary little with different redshift corrections, redshift cut-off, and galaxy LF, but are rather sensitive to the adopted links D_0_ and V_0_. More precisely, the typical group size (velocity dispersion) is linearly related to the adopted distance (velocity) link, while it is rather insensitive to the adopted velocity (distance) link. Physical
properties of groups in PPS and in directly comparable samples show good agreement. There is a complex interplay among LSS features, sample depth, FOF grouping procedure, and group properties.
%K catalogs - galaxies: clusters of luminosity function - cosmology: large scale structure of the Universe

%R 1998A&AS..130..359S
%J-367
%A Spagna A., Lattanzi M.G., McLean B.J., Massone G., Lasker B.M.
%T Faint photometric BVR_c_ CCD sequences. The North galactic pole (b=~85{deg}) and the anticenter (l=133.2deg, b=-1.6deg).
%M ds1234
%F 1998.05.26
%B Lists of CCD photometric standard stars in the BVR_c_ system of Johnson and Cousins are presented for two regions of importance in studies of galactic structure and kinematics: one at the North galactic pole (NGP) (b_II_=85{deg}), and a second on the galactic equator toward the anti-center (l_II_=133.2deg, b_II_=-1.6deg). Precision of both magnitudes and colors is better than 0.05mag down to V=18.5 for the NGP sample, and to V=18.0 for the set on the galactic plane.
Accuracy is also better than 0.05 mag, as shown by comparison to standard (intrinsic) color-color diagrams. These sequences should fulfil the needs for faint reference stars in the photometric calibration of old and new large-area surveys using wide-angle photographic plates. This is the case, for example, of the new multicolor surveys of the Palomar Observatory, which uses the Oschin Schmidt telescope, and the Second Generation Southern Sky Survey, which utilizes UK Schmidt
of the Anglo Australian Observatory in Siding Spring.
%K catalogs - Galaxy: structure - techniques: photometric

%R 1998A&AS..130..369L
%J-379
%A Legg T.H.
%T A proposed new design for a large radio telescope.
%M ds6260
%F 1998.05.26
%B A new type of radio telescope is proposed which may make very large telescopes more affordable. The telescope is considered to be one of several identical elements that form a synthesis array. It is composed of an almost flat primary reflector that is slightly adjustable in shape and made up of identical square flat panels supported by the ground. A very long focal length imposes the unusual condition that the receiver be carried by an airborne vehicle such as a powered,
helium-filled balloon. The position of the balloon is measured and controlled as accurately as possible and residual errors in the balloon's position are dealt with in two ways. Errors of a few metres are corrected by moving the receiver feed point electronically. Larger errors are corrected by adjusting the primary reflector so as to move its focal point to follow the balloon. These features maintain telescope efficiency and correct pointing so long as the balloon lies
anywhere within a large volume surrounding its ideal position. The problem of controlling the balloon position is thereby substantially eased. The telescope has the wide sky coverage needed for synthesis observations and an estimated optimum diameter in the range 100 to 300 m. It will operate from decimetre to short centimetre wavelengths, or, with smaller panels, millimetre wavelengths.
%K telescopes - instrumentation: interferometers

%R 1998A&AS..130..381P
%J-393
%A Pfeiffer M.J., Frank C., Baumueller D., Fuhrmann K., Gehren T.
%T FOCES - a fibre optics Cassegrain Echelle spectrograph.
%M h0572
%F 1998.05.26
%B We have designed and built the echelle spectrograph FOCES fed by 100{mu}m optical fibres to be mounted at the Cassegrain focus of either the 2.2m or the 3.5m telescope at the Calar Alto Observatory. The spectrograph itself follows a white-pupil design collimated with two off-axis parabolic mirrors. The 15cm beam leaving the 31.6lines/mm R2 echelle is refocussed in the vicinity of a small folding mirror which allows efficient removal of scattered light. The
cross-dispersion is achieved with a tandem prism mounting, and the beam imaged with an f/3 transmission camera onto a field centered on a 1024^2^ thinned Tektronix CCD with 24{mu}m pixel diameter. The echelle image covers the visible spectral region from 380 to 750nm displayed in 70 spectral orders with full spectral coverage. Spectral orders are separated by 20 pixels in the blue and by 10 pixels in the red. The maximum spectral resolution is 
R={lambda}/{DELTA}{lambda}=40600 with a 2 pixel resolution element; unvignetted resolution as defined by the fibre alone would be obtained at R=18000. Replacing the CCD by a 2048^2^ chip with 15 {mu}m pixel diameter and taking into account light losses from a reduced entrance slit width a full 2 pixel resolution of R=65000 is obtained. The above concept has made FOCES an extremely well-defined instrument. A number of successful test installations at the Cassegrain foci of the Wendelstein 80cm
telescope, the Calar Alto 2.2m and 3.5m telescopes has produced spectra of high quality for up to 60min exposures. The limiting magnitude for a 1hr exposure with an S/N ratio of 100 scales to V=12 for a 3.5m telescope which is only slightly less than expected from laboratory tests. In an alternative mode FOCES offers a second fibre carrying the sky background signal to correct extremely faint object spectra. This mode obtains the required higher cross-dispersion from
an additional grism resulting in a correspondingly reduced spectral coverage.
%K instrumentation: spectrographs - methods: observational - methods: data analysis - techniques: spectroscopic

%R 1998A&AS..130..395M
%J-401
%A Morel S., Koechlin L.
%T The DELTA photon counting camera concept.
%M ds1423
%F 1998.05.26
%B In this paper we present new ideas for a high sensitivity array detector, which yields the space and time coordinates of photo-events at sustained count rates superior to one million per second. The DELTA camera (Detector Enhancement by Linear-projections on Three Axes) has been initially designed for astronomy. However, it has advantages for a wide range of high-resolution problems in the visible and near I.R. It is noticeable for its optical design, its smooth flat field
and its very high temporal resolution and throughput in photon counting mode. The resolution of the prototype described is 512 x 591 pixels in space and 2.6{mu}s in time. The principle of this detector is based on a projection - back-projection scheme (the {DELTA}-process) and on the use of three one-dimensional CCDs. We describe the technical solutions which could lead to an operational prototype. From numerical simulations of the {DELTA}-process, we give some expected
characteristics of this camera.
%K instrumentation: detectors - techniques: interferometric