bluuebunny/crossref_metadata_2025 huggingface dataset:
Optical Interferometry: Summary and Perspectives
Authors: Léna P.J.
Published: June 2019

The outstanding progress of radio astronomical interferometric imaging – a gain in angular resolution of 1010 in 50 years – demonstrates that once basic physical principles are established and technology developed, the field can develop with immense benefits for astronomy. Today, physics and technology give solid foundations for rapid growth of optical interferometry.
The Molecular Spiral Structure in M51 Derived from CO(J=2-1) Line Observations
Authors: Guélin M. , Garcia-Burillo S. , Blundell R. , Cernicharo J. , Despois D. , Steppe H.
Published: June 2019

We present preliminary results of a high angular resolution-high sensitivity survey of CO(J = 2—1) line emission in M51 made with the IRAM 30 m telescope.
Molecular Cloud Spiral Arms and Results from Tidal Interaction Modeling
Authors: Hjalmarson Åke
Published: June 2019

I wish to report on some results from mapping of molecular cloud distributions in galaxies and from tidal interaction modeling – work performed at Onsala Space Observatory and in the Astrophysics Group of Institute of Theoretical Physics, Chalmers University of Technology/University of Göteborg.
Co Observations of the Central Region of NGC4258
Authors: Sofue Yoshiaki
Published: June 2019

12CO(J = 1-0) observations of the central region of NGC4258 at a resolution of 17” revealed a high-density concentration of molecular gas toward the center. The molecular clump lies on a central depression in the HI bar. No clear interaction of the molecular gas with the continuum anomalous arms has been found.
The Correlation of CO and IR Emission from Galaxies: What Does it Tell Us?
Authors: Verter Frances
Published: June 2019

Almost all galaxy properties correlate with each other to some degree; in this bounty of agreement, how are we to extract essentials? Fortunately, there is a framework in which to interpret CO correlations. Empirical studies have indicated that the fundamental galaxy properties are scale and form (Whitmore 1984), and theoretical work has implied that this follows from the physics of galaxy formation (see Lin and Pringle 1987, and references therein). It is known that the CO luminosity of galaxies is a function of both their scale (Young and Scoville 1982) and their form (Verter 1987). But the interpretation of any individual correlation is shrouded by uncertainties in the conversion from observables to source population properties.
Recent CO(2-1) Observations of Galaxies with the CSO
Authors: Sargent A.I. , Phillips T. G. , Sanders D. B. , Scoville N. Z.
Published: June 2019

CO(2→1) observations of a number of galaxies have recently been obtained with the CSO. Examples are presented here to illustrate the capabilities of the instrument.
CO in M82 and Other Mildly Active Galaxies
Authors: Wielebinski R.
Published: June 2019

A large project of studying various transitions and isotopie species of CO in M82 has been carried out with the 30-m IRAM radio telescope. A 1.′6×1.′0 area was mapped in 12CO(2→1) with 13″ resolution (Loiseau et al., 1988a). The purpose of these observations was to obtain high signal-to-noise, high resolution data for comparison with the 12CO(1→0) observations of Nakai et al. (1987). A 13CO(2→1) observation covered the central 110×017 region (Loiseau et al., 1988b) and allowed to establish the velocity field of CO in the inner nuclear region. The position angle of the rotation axis of 13CO is aligned with the optical rotation and at some 30° relative to the 12CO velocity field. The 13CO map also shows the existence of clumped emission in the central region. All data show the rotating molecular ring. At some selected points (nucleus, major axis) 12CO/13CO ratios in both the (1→0) and (2-H) transition have been determined. The earlier suggestion that optical depth plays an important role in M82 has been confirmed. Variations of optical depth have been determined in the sources that there are several extended (>100pc) molecular complexes.
The Ratio of H2 to HI Gas in Infrared Luminous Galaxies
Authors: Mirabel I. F. , Sanders D. B.
Published: June 2019

The majority of infrared active galaxies (ffir/fb ≥ 2) have molecular to atomic mass fractions in the range of 0.5 to 2.0. Among the galaxies with the higher infrared excesses there are spectacular cases of HI deficient systems, where less than 15% of the total mass of interstellar gas is in atomic form. The optical morphology of luminous infrared galaxies suggest that the overall mass fractions of molecular to atomic gas, and the infrared luminosities per nucleon of interstellar gas are enhanced during galaxy-galaxy interactions.
Introduction and Basic References for Stellar Photometry with CCD
Authors: Rufener F.
Published: June 2019

An object of this meeting is to define and emphasize the best practices that allow stellar photometry done with array detectors to be as accurate as possible. We dream of applying simple and clearly justified principles; in reality, we find the equipment has physical and technical properties that interfere with each other. Photometry is a method, a metrology; so we first have to define the desired accuracy. Some will be happy with 0.1 magnitude; others need 0.01, or even 0.001 magnitude. The necessary precautions must be matched to these ambitions.
CCD Imagers for Astronomy: Past Problems and Future Hopes
Authors: Geary John C.
Published: June 2019

The search for high-quality, large-format CCD imagers during the 1980’s reminds me of a journey across a large and forbidding desert. One starts off full of great expectations of a quick completion, but discouragement sets in around mid-journey as the barrenness of the landscape becomes apparent and the goal on the horizon is shown to be only a mirage. Finally, mountains resolve themselves from the mirages and we take heart in knowing that we seem finally to be making some progress. I think the analogy fits the CCD situation well, starting with the view from the time period 1979–80 and working toward the present.
The CCD Mosaic Project by ESO and INSU / Toulouse Observatory
Authors: D’Odorico Sandro , Prieur Jean-Louis
Published: June 2019

In the last few years, as the CCD cameras have been routinely used in most of the Observatories, there has been a growing concern among the scientific community about the major weakness of this very good detector: the format of the available chips is too small for many applications.
High Energy Processes in the Interstellar Medium
Authors: Cesarsky Catherine J.
Published: June 2019

The relationship between high energy phenomena and the interstellar medium is wide. I had to make a selection, and only cover a few aspects: cosmic rays, gamma rays, correlation between radio synchrotron and infra red emission and its influence on cosmic rays; and finally some new observational results.
Reference Systems and Frames as Proposed by the Working Group on Reference Systems
Authors: Kovalevsky J.
Published: June 2019

Among the nine recommendations of the Working Group on Reference Frames as finalized during the Virginia Beach meeting, four are directly addressing the reference systems. They are the result of the work of the subgroup on coordinate frames and origins and other contributors whose names are given in section 6. The resulting document (Kovalevsky, 1991) was further revised by the working group as a whole and recommendations published (1991).
Explanation of Resolution VIII proposed by the IAU/WGRS Sub-Group on Astronomical Constants
Authors: Fukushima Toshio
Published: June 2019

The IAU Working Group on Reference Systems (WGRS) Sub-Group on Astronomical Constants (SGAC) was established in June, 1989, as a consequence of resolutions adopted by Commissions 4, 7, 8 and 24 at the IAU General Assembly at Baltimore in 1988. The given missions of this sub-group were stated clearly by J. Hughes, the chairman of the WGRS.
Background of Recommendation IX
Authors: McCarthy D.
Published: June 2019

Due to weather-related travel delays Dr. McCarthy was unable to present his scheduled paper. In his absence, J.A. Hughes gave a short talk indicating that Recommendation IX had received essentially universal approval at and since the Virginia Beach Colloquium, and that it would undoubtedly be approved by the Joint Commission Meeting as presently written, and then submitted as a Commission Resolution.
Time Scales for Theory and Practice
Authors: Winkler Gernot M. R.
Published: June 2019

Very early human experience has suggested a practical definition for the measurement of time: We define a unit of time by defining a standard (cyclical) process. Whenever this process completes its cycle identically, a unit of time has elapsed. This is the origin for the various measures of time in classical astronomy. Nature suggests strongly that we use as such standard processes the year (defined as a complete revolution of the earth around the Sun), the month (the completion of a revolution of the moon around the earth), and the day which again can be measured in several different ways. While the sidereal day is measured by a rotation in respect to the vernal equinox, the mean solar day is measured in respect to the mean. Sun. More recently, we have distinguished many more different ways of defining measures of time, partly in response to perceived needs of the applications, but in part also from purely aesthetic principles.
Recent Ginga Results on Galactic X-Ray Binaries
Authors: Tanaka Y.
Published: June 2019

Based on the recent Ginga results, following topics on X-ray binaries are briefly discussed: The cyclotron resonnance features observed from several X-ray pulsars, and related problem of the magnetic field decay. Search for millisec. pulsations from LMXRBs. Very bright transients which are suspected to be new black hole candidates, and an estimation of the number of such black hole sources in our galaxy.
Sigma Observations of the Galactic Centre
Authors: Cordier B. , Ballet J. , Goldwurm A. , Paul J. , Bouchet L. , Roques J.P. , Mandrou P. , Vedrenne G. , Sunyaev R. , Churazov E. , Gilfanov M. , Diachkov A. , Khavenson N. , Chulkov I. , Kuznetzov A. , Novikov B.
Published: June 2019

After the first year of performance of SIGMA, more than 390 hours of data on the Galactic Centre region have been recorded. This survey establishes the extremely variable nature of this region. During a period of 6 months, 3 sources have dominated successively: 1E 1740.7-2942, GRS 1758-258, GX1 + 4. Concerning the two first sources, their spectral shape and their variability suggest to include them in the list of the black hole candidates.
The First EUV Survey: White Dwarfs and Cool Stars
Authors: Jordan C. , Pounds K.A.
Published: June 2019

Preliminary results from the survey carried out with the Wide Field Camera (WFC) on ROS AT are presented. 732 sources were detected, of which 230 were observable in both the S1 and S2 filters. The distribution of sources with galactic longitude, near the galactic plane, shows the greatest number in the quadrant where H I absorption is least. The identifiable sources include a high proportion of hot white dwarfs and ‘normal’ late-type stars. The optical follow-up programme has identified over 40 new white dwarfs and over 60 late-type stars including RS CVn systems and cataclysmic variables. Emission from some A stars detected appears to come from white dwarf companions. Individual sources of particular interest are discussed. The systematic analysis of a sample of late-type stars has begun.
The Cosmic Infrared Background
Authors: Hauser M. G.
Published: June 2019

Cosmic infrared background radiation, expected to carry the radiative record of luminous objects since they first formed, has yet to be detected. The Diffuse Infrared Background Experiment (DIRBE) on the Cosmic Background Explorer (COBE) satellite is designed to search for this primeval background over the spectral range from 1 to 300 μm. Initial examination of data from this experiment show that foreground radiations from the solar system and Galaxy dominate the diffuse infrared sky brightness, with relative minima near 3.5 μm and in the submillimeter wavelength range. DIRBE measurements do not confirm some previous data from rockets and IRAS. Preliminary upper limits on the cosmic infrared background are generally above theoretical expectations for pregalactic and protogalactic sources, and substantially above estimated lower limits based upon observations of external galaxies. Careful foreground modeling is required to reduce these limits or identify an isotropic residual.
RATAN-600 and CMB Anisotropy: New RATAN-600 Limits
Authors: Parijskij Yu. N. , Erukhimov B. L. , Mingaliev M. G. , Chernenkov V. N. , Verkhodanov O. V. , Chepurnov A. V.
Published: June 2019

We present new limits on the small scale 3 K emission anisotropy. At scales of 1°-3.3° all seven harmonics have amplitudes below 10-5 in ΔT/T at our wavelength of 7.6 cm. At the 6.1x103 to 17.5x103 (rad-1) scale, this limit is about 2.8x10-4 (at 2.7 cm wavelength) and the observations may be fully explained by contributions from discrete sources. The low baryonic content of the Universe and present limit on the ΔT/T at the horizon scale suggest that (ΔM/M)gravitating ≪ (ΔM/M)baryonic. speculate that the 3 K anisotropy measurements prove a) the existence of the dark matter, b) the nonbaryonic nature of this dark matter and c) that the space distribution of this matter is much more homogeneous than that of the visible one.
The Hipparcos Observing Programme. Performances of the Input Catalogue
Authors: Turon C. , Arenou F. , Crifo F. , Gómez A. , Morin D.
Published: June 2019

The Hipparcos observing programme is composed of 118 000 selected stars, one QSO (3C273), 48 minor planets, and 2 satellites of major planets. These objects were selected on the ground of scientific proposals submitted by the world-wide astronomical community, while taking into account die specific operating mode of the satellite and using at best its observing possibilities. The content of the stellar part of this observing programme and the way in which the star selection was performed is described in details in a paper accepted for publication in Astronomy & Astrophysics.
Accuracy Uniformity of Hipparcos Parallaxes and Proper Motions: Strategy and Current Status
Authors: Crézé M. , Chareton M.
Published: June 2019

Even before the launch difficulties, it was planned to monitor the trend of the accuracy acquisition resulting from the adopted observing process and eventually to modulate the initial values of the observing strategy parameters whenever it may help correcting distorsions in the final uniforme accuracy. Of course this monitoring of accuracy acquisition became more important when, as a result of the revised orbit, large departures from the nominal observations take place. The observing strategy and the associated modulation process behave according to expectation and may smooth out on the long range inhomogeneities. However important effects due to the complete lack of long sequences of observations in the early period in some regions will not be compensated unless the real mission extends substantially beyond the end of 92.
New Proper Motions for HIPPARCOS Stars
Authors: Jahreiß H. , Crifo F. , Réquième Y.
Published: June 2019

During the preparation of the Hipparcos Input Catalogue precise positions were measured very recently by the Bordeaux automatic meridian circle (BMC) for about 5500 stars in the northern hemisphere. On average eight observations were made for each star at a mean epoch 1987. The estimated mean error in α is 0″.12 and in δ 0″. 18. With 2555 stars almost half the BMC sample lies in the declination zone -2° < δ < +32°. In this zone the (x,y) measurements of all Astrographic Catalogue plates have been newly reduced (S. Röser, priv. comm.). So, at least two independent positions are available for practically all stars down to the limiting magnitude of the AC with epochs around 1910 and with a mean positional error of 0”. 28. A combination of these two sources should provide proper motions to an accuracy of 0″. 004 yr−1.
First Results of the Sphere Solution Based on HIPPARCOS Data
Authors: Lindegren L. , van Leeuwen F. , Petersen C. , Söderhjelm S.
Published: June 2019

Results from a test solution of the positions and parallaxes for about 10,000 stars are presented in statistical form. The solution is based on about 1300 hours of Hipparcos observations made from November 1989 to February 1991, representing about 1/5 of the scientifically useful data collected in that period. Due to the short time span of the data no attempt was made to determine proper motions. The positions, many of which are already in the 2-5 milli-arcsec accuracy range, clearly reveal systematic errors of up to 0.2 arcsec in the ground-based positions of the Input Catalogue. Perhaps the most convincing evidence of the quality of the satellite data is provided by the distribution of trigonometric parallaxes determined in this solution. By comparison with the expected distribution of true parallaxes, based on a standard model of the Galaxy, we conclude that the external errors of the best parallaxes have a standard deviation around 5 milli-arcsec. Any global offset of the parallax zero point appears to be less than 1 milli-arcsec. The accuracy obtained is consistent with pre-launch predictions, if allowance is made for the reduced data collection efficiency due to the faulty orbit, and supports the assertion that the 2 milli-arcsec goal can still be reached in the present orbit. Details of the solution are being published in Astronomy & Astrophysics.
HIPPARCOS Main Mission Photometric Processing
Authors: Mignard F. , Froeschlé M. , Falin J.L.
Published: June 2019

In addition to its astrometric capabilitie the Hipparcos main detector proves to be a good phototometer. The main features of the reduction are outlined altogether with a presentation of some conspicuous results which already provide good clues as to the quality of the final results when more than three years of data are analysed.
Long Period Variable Stars in the Hipparcos Observing Program
Authors: Barthes D. , Boughaleb H. , Figueras F. , Foster E. G. , Mattei J. A. , Mennessier M. O. , Waagen E. O.
Published: June 2019

Among the long period variable stars included in the Hipparcos observing program, 245 large-amplitude ones require brightness predictions during the mission in order to allocate the necessary observing time. We present the computation of the light ephemerides with numeric and symbolic methods using AAVSO’s 75-year data on maxima and minima dates and magnitudes and 20 years of individuai observations; the evaluation and revision of the ephemerides using ground-based observations compiled monthly by the AAVSO from observers world-wide and real-time monitoring of ephemerides stars from satellite observations performed at ESOC; the statistical results derived from one-and-a-half years of simultaneous ground-based and Hipparcos observations. We show the usefulness of all this work in understanding the physics of these pulsating variable stars.
A Progress Report on optical and Radio Astrometry of Hipparcos Inertial Link Objects
Authors: Vegt C. De , Zacharias N. , Hughes J.A. , Hindsley R. , Johnston K.J.
Published: June 2019

The status of our longterm joint optical- and radio observing program for the establishment of a new inertial optical- and radio reference frame is described. A special attempt is made to provide a suitable number of extragalactic sources and radiostars for an inertial HIPPARCOS reference link.
Accuracy Predictions and Final Prospects for the HIPPARCOS Mission
Authors: Lindegren L. , Kovalevsky J.
Published: June 2019

The pre-launch accuracy prediction for the Hipparcos mission is reviewed with regard to the observed performance and expected lifetime of the satellite in its present orbit. Given the excellent quality of the data it is likely that the target accuracy of 2 milli-arcsec for typical programme stars can be achieved if operations continue at least until the end of 1993. We emphasize that any extension of the operational lifetime beyond that point strongly enhances the scientific value of the results.
Linking Hipparcos to the galaxies: the Bonn and Potsdam programmes
Authors: Brosche P. , Dick W. R. , Galas R. , Geffert M. , Hirte S. , Schilbach E. , Scholz R.-D.
Published: June 2019

Besides the link of the HIPPARCOS reference frame to extragalactic objects via radio stars or by the HST, also photographic astrometry is able to calibrate the HIPPARCOS proper motions with regard to an inertial system. Numerical simulations have shown that even with a very small number of well-distributed link fields (3 to 5) the photographic method is competitive with other techniques.
Comparison of preliminary StarMapper positions with Carlsberg meridian circle observations
Authors: Morrison L.V. , van Leeuwen F. , Evans D.W.
Published: June 2019

The process of satellite attitude reconstruction carried out at RGO enables the assumed positions of the stars taken from INCA to be improved. The attitude reconstruction is determined from polynomial fits to the residuals between the observed StarMapper positions and those taken from INCA. The degree of the polynomial is such that smoothing occurs over a typical arc length of about 10°. The positions from different passes are combined, giving a typical internal accuracy for a star of 0"·02 in RA and Dec. The observations discussed here were accumulated from provisional magnetic tapes received from Darmstadt before the end of 1990.
HST Imaging of PSR1913+16
Authors: Crane Philippe
Published: June 2019

An image of the region of the binary pulsar PSR1913+16 has been obtained with the Planetary Camera on board the Hubble Space Telescope. This image confirms previous observations of a source coincident with the radio position of the pulsar to within 0,15 arcsec. The image shows a marginal extension not seen in other so urce of similar brightness in the field.
The Goddard High Resolution Spectrograph Status; Absorption lines in 3C 273
Authors: Brandt John C.
Published: June 2019

The Goddard High Resolution Spectrograph (GHRS) is an ultraviolet spectrograph developed by the Goddard Space Flight Center and constructed by the Ball Aerospace Systems Group. The basic performance characteristics are given in Table 1. The detectors are Digicons with an approximately 500-diode linear array; the faceplate/photocathode combinations are LiF/CsI for Side 1 and MgF2/CsTe for Side 2. The two science apertures are 2x2 and 0.25 x 0.25 arc seconds square. The GHRS has several undispersed-light modes for target acquisition.
FOC Observations of SN 1987A
Authors: Panagia N.
Published: June 2019

We present and discuss the first images of SN 1987A obtained on day 1278 with the FOC on board the Hubble Space Telescope. The supernova is well detected and resolved spatially in the four observed bands. The UV luminosity of SN 1987A is found to be comparable to that emitted in the visible and infrared spectrum. Narrow-band [OUI] imaging reveals that the circumstellar nebula surrounding SN 1987A has the shape of a perfectly elliptical ring, implying an inclination of 43° ±3°. A comparison of the ring angular size with its absolute size derived from an analysis of the light curves of narrow UV lines measured with IUE, gives an accurate determination of the distance to SN 1987A, i.e. d(1987A) = 51.2±3.1 kpc. Allowing for the relative position of SN 1987A within the LMC, the distance to the center of the LMC turns out to be 50.1 ± 3.1 kpc. This value agrees very well with the determinations obtained from light curve analyses of variable stars.
Atomic Data, Stellar Atmospheres, and the Hubble Space Telescope
Authors: Lambert David L.
Published: June 2019

Since the birth of astronomical spectroscopy in the last century astronomers have appealed for atomic and molecular data. As capabilities at astronomical observatories have grown, and now as a large orbiting telescope equipped with a high-resolution ultraviolet spectrometer is returning novel data, our appeals continue. The appeals are not rooted in exotic chemical compositions and severely extreme physical conditions to be found in stellar atmospheres. Rather the appeals arise very often because stellar atmospheres are more extensive light sources than can be attained in laboratories. The inability to replicate stellar conditions in the laboratory applies to all types of stars. The theoretical quantum chemist/physicist is not so limited as the experimental spectroscopist. Although much vital data can now be supplied through computations, experimental data is absolutely required in many areas: e.g., detailed lists of classified lines, accurate cross-sections for a variety of collisional processes needed for studies of non-LTE line formation.
The s-Process in AGB Stars
Authors: Gallino R. , Raiteri C.M. , Busso M.
Published: June 2019

The evidence of an exponential distribution of neutron exposures for reproducing the solar-system s-isotopes between Zr and Pb, the main component, comes from a phenomenological analysis of the s-path in the σN versus A plot (see Käppeler, Beer and Wisshak, 1989). The resulting mean neutron exposure is τ0 = 0.30 ± 0.01 mb−1. The study of branchings with no or weak temperature dependence (95Zr; 147Nd, 147,148Pm; 185W, 186Re) allows one to derive an effective neutron density nn =(3.4±1.0)×108cm−3. On the other hand, an effective temperature is obtained from the branchings 134’135Cs, 151Sm, 154Eu and 176Lu: T8 = 3.4 ± 0.5 (Käppeler et al., 1990). Although the phenomenological approach is very useful because it is independent of stellar models, nonetheless it can only lead to effective physical conditions, symplifying the complexity of the astrophysical sites.
White Dwarf Stars: Evolution of the Envelope Composition
Authors: Liebert James
Published: June 2019

Over the last several years, evidence has been unfolding that the surface abundances of white dwarfs may evolve as the stars cool. It is possible that some post-AGB stars enter the white dwarf sequence with far less hydrogen and helium than predicted by standard theory of the quenching of shell sources, and with atmospheres dominated by C and O. The interplay of diffusion and episodes of convective mixing may lead first to He-rich atmospheres, then H-rich, and finally He-rich again.
Coronal Holes and the Solar Wind
Authors: Leer Egil
Published: June 2019

Around the turn of the century Professor Kristian Birkeland at the University of Kristiania (Oslo) carried out laboratory studies of the emission of charged particles from the Sun and their interaction with comets and magnetized planets. He found that cathode rays emitted by a magnetized sphere are bent toward the equator along trajectories similar to the structures observed in the solar corona during the 1901 eclipse. He also concluded that comet tails are formed by charged particles from the Sun interacting with dust and gas around the comet.

Birkeland carried out extensive observing programs of the aurora, geomagnetic storms, and the zodiacal light. During a 9 months campaign from mid 1902 he observed recurrent geomagnetic storms from stations in Northern Norway, at Novaja Semlja, Iceland, and Spitsbergen, and correlated the occurence and periodicity of magnetic storms with solar activity. He found that the period of recurrent geomagnetic storms was generally larger than the period of “near equator” solar phenomena. He also found that “Very often large maxima of storminess are not accompanied by any sun-spots at all”. (Birkeland 1913, p. 524).
Asymmetric MHD Stellar Winds and Related Flows
Authors: Tsinganos K.
Published: June 2019

Some well established observational facts about most wind-type astrophysical outflows are the following: (i) they are strongly nonspherically symmetric and at least two-dimensional; fast solar wind streams from polar coronal holes and jets from stars and galaxies are two representative and characteristic examples, (ii) some kind of nonthermal heating is required, at least during the initial acceleration stage of the outflow; therefore, the flow is far from beeing adiabatic and the assumption of polytropicity with an arbitrarily specified index γ, although useful from the mathematical point of view to solve the governing equations and provide some physical insight into the problem, is nevertheless artificial. (iii) the ubiquitous magnetic field seems to play a decisive direct, or at least, indirect role in heating stellar coronae and driving stellar winds. Nevertheless – perhaps for the sake of simplicity – most studies on astrophysical outflows and winds so far have neglected to incorporate the above three basic features of nonspherical expansion, nonpolytropic equation of state and magnetohydrodynamic description of the problem. We have recently embarked in an effort to model wind-type outflows by incorporating those basic physical constraints (Low and Tsinganos, 1986; Tsinganos and Low, 1989; Tsinganos and Trussoni, 1990, 1991; Tsinganos and Sauty, 1992a,b).
Optical Redshift Surveys
Authors: Costa L. Nicolaci da
Published: June 2019

Redshift surveys of galaxies have been over the past decade the major source of information for studies of the large-scale structure of the Universe. Following the completion of the original CfA Redshift Survey, several groups have joined the endeavor, probing different regions of the sky to different depths in a remarkable long-term effort to study the nature of the galaxy distribution and its statistical properties at different scales. Here I summarize the current status of the ongoing surveys drawn from optical galaxy catalogs. The review is not intended to be complete but rather to demonstrate the vitality of the area and to point out that exciting new data should be forthcoming in the next few years.
No Backside Infall into the Great Attractor
Authors: Mathewson D.S. , Ford V.L. , Buchhorn M.
Published: June 2019

We have recently completed a survey of the peculiar velocities of 1355 southern spiral galaxies. The Tully – Fisher relation was used to estimate the distances to the spirals. The photometry was done in the I-band using CCDs on the lm telescope and the Anglo-Australian Telescope at Siding Spring Observatory. The rotational velocities were measured from 1042 H-alpha rotation curves obtained with the 2.3m telescope at SSO and 609 H 1 profiles obtained with the Parkes radio telescope.
Textures and Galaxy Formation
Authors: Spergel David N.
Published: June 2019

Textures will produce positively skewed non-Gaussian primordial fluctuations. This implies that galaxies and quasars formed earlier in this model than in a Gaussian model with the same power spectrum. The model also predicts the existence of more high velocity dispersion clusters and richer superclusters. We describe the texture model and our numerical simulations of the origin of structure in the model.
Archives of Photometric Data
Authors: Mermilliod J.-C.
Published: June 2019

The process of archiving photometric data and compiling catalogues is in principle easy to solve, but, in practice, does not appear so simple. Data retrieval may become difficult and inefficient if sufficient care is not taken to solve the general problems which are encoutered: (i) the lack of definition of fundamental identificators; (ii) the lack of coordinates for thousands of faint stars; (iii) the innacuracy of the identification and description of the components observed in double stars or multiple systems: A, B, C, AB, or BC; (iv) the fact that the number of observations is often not published.
Progress in Adaptive Optics for Astronomy
Authors: Merkle Fritz
Published: June 2019

The problem of optical distortion produced by the earth’s atmosphere has been known in astronomy since Isaac Newton. In 1953 H. W. Babcock (1953) proposed in his paper “The Possibility of Compensating Astronomical Seeing” to use a deformable optical element driven by a wavefront sensor to correct the distortions induced by the atmosphere that affect astronomical imaging. It took another 20 years for this principle to be demonstrated successfully for defence related laser applications. And only in the early eighties the first astronomical adaptive optics projects had been triggered.
Testing an astronomical observing site in Antarctica
Authors: Recabarren Pablo , Puerta Juan
Published: June 2019

During the winters of 1989 and 1990, the Observatorio Astronomico de Cordoba conducted observational site testing in the Antarctic. The search was carried out amongst the Argentinian stations to take advantage of existing logistic facilities. Belgrano II was chosen because it is the most southerly one, has the most stable climatological conditions, and is ground-based. The results are not very promising for astronomical work, but we have obtained important experience for this kind of task in the Antarctic.
Antarctic observations of the cosmic microwave background
Authors: Smoot George F
Published: June 2019

In the standard cosmology of the Big Bang theory the cosmic microwave background (CMB) is the remnant radiation from the hot early universe. The sky signal is comprised of radiation from the CMB, from Galactic emission, from atmospheric emission, and from instrument sidelobes seeing the ground and man-made interference. One observes in directions of minimum galactic signal. The antarctic polar plateau provides the best site in the world for low atmospheric emission, low horizons, low man-made interference, and reasonable accessibility. The low column density of precipitable water and extreme stability for periods exceeding a week, combined with low RFI are critical. A very important secondary benefit for anisotropy experiments is the ability to observe the same part of the sky continuously at a high elevation angle.
An international research station in Antarctica
Authors: Lynch John T
Published: June 2019

Many people, including Wernher von Braun, have drawn an analogy between the manned exploration of the solar system and scientific stations in Antarctica. Some of the Space/Antarctic parallels are quite obvious, such as the necessity to select small groups of highly trained individuals who can work together in isolation for extended periods, or in the case of the Moon/Antarctic comparison, the long day/night cycle. However, the parallel can be carried considerably further to include the types of science to be done, and, in some cases, there is even a strong similarity in environmental conditions. It may be worth while to build a new Antarctic station just to learn more about how to do planetary exploration.
Molecular Clouds in Dwarf Irregular Galaxies
Authors: Henkel C.
Published: June 2019

The study of molecular clouds in dwarf galaxies was, until recently, an arduous task and provided detections in only a handful of sources (see Thronson and Bally 1986; Wiklind et al. 1986; Tacconi and Young 1987; Arnoult et al. 1988). Line strengths observed in CO were small (<100mK) and measurements were confined to one position per source, thus inhibiting any detailed work. However, dwarf galaxies appear to be much more abundant than either spirals or large ellipticals and play an important role in our understanding of star and galaxy formation (see e.g. Gerola et al. 1980; Gallagher and Hunter 1984; Silk et al. 1987). With small rotational velocities (typically 50-lOOkms-1), the absence of density waves, and low metallicities, they provide, by "local" standards, an interstellar environment with even more extreme conditions than the outer Galaxy. Detailed molecular studies are hence important.
A New Text from Asia Minor
Authors: Reynolds Joyce
Published: June 2019

By courtesy of the owner, I publish a standard weight found in Asia Minor and now in the Collection Breusch. It is a hexagonal plaque of lead, pierced at one angle for suspension by a cord, of maximum width 0·16 m. and weight 2·6 kg. Both faces are inscribed with letters in relief, within a raised border. On face (a) the letters are above and on either side of a relief showing the bust of a curly-headed man facing right and carrying a caduceus over his left shoulder—certainly Hermes Agoraios, patron of the market-place. The inscription on face (b) is upside down to that on face (a).

Face (a). Letters, c. 0·012; (See Plate I.)

The final is badly formed and looks more like
S.E.G. IX, 63
Authors: Reynolds Joyce
Published: June 2019

This inscription, dated in A.D. 2/3 and comprising a prose introduction and a set of verses cut in small letters (c. 1 cm.) below a relief of a man reclining on a couch, cup in hand, was found in the Sanctuary of Apollo at Cyrene in 1925 and published by G. Oliverio in 1933. Of the controversies that the monument has aroused, I am concerned only with the last line of the text=the last couplet of verses, where Oliverio's reading is difficult to translate. Various emendations have already been proposed, none of them wholly satisfying.
The Recentiores of the Ciris
Authors: Lyne R. O. A. M.
Published: June 2019

In a notice of Knecht's new edition of the Ciris to appear in due course in the Classical Review, I was able to commend the book only in one respect: that it provided copious information on largely neglected recentiores. For the first time all the manuscripts which have ever been considered possibly significant for the text of the Ciris were assembled and fully reported in one place. However, this mass of information was ill-digested: the conclusions drawn from it were vague, or inadequately argued – or simply wrong; and much was left unsaid. But I thought that the results towards which Knecht's work pointed were interesting and that it would be a pity if they remained obscured. Since to clarify them involved more space than a review allowed, I offer the following short paper. Necessarily it will have some of the appearance of a review article; but I shall try to make it as self-contained as possible. Knecht never once ventures a stemma – in my remarks I shall have in mind Goodyear's stemma on p. 99 of the OCT Appendix.
Early Hellenistic Elegy: P. Sorbonn. 2254
Authors: Page Dennys
Published: June 2019

Apart from Callimachus, I know no new piece of Hellenistic elegy more interesting than P. Sorbonn. inv. 2254, first published by M. Papathomopoulos in Recherches de Papyrologie II and most admirably edited by Professor Barns and Professor Lloyd-Jones in SIFC xxxv, 205 ff.

Lloyd-Jones proves, I believe beyond question, two points:

(a) That this elegy belongs to the world as it was before Callimachus; it is only our fourth large specimen of the literary elegy from the early part of the third century, the others being the long extracts from Hermesianax, Phanocles and Alexander Aetolus most conveniently read in Powell's Collectanea Alexandrina.

(b) That the subject-matter is of a very unusual nature; the lines are ‘spoken by an unknown person threatening an enemy with a punishment quite out of the ordinary’ – viz. with tattooing on his skin the images of punishments suffered by notorious legendary sinners. The poet's enemy is to be tattooed with a picture of the stone of Tantalus, with another of the Calydonian boar sent to punish Oeneus, and with at least one other (there is a fragmentary second column, one line beginning στίξ[ω).
Horatian Notes II: Despised Readings in the Manuscripts of the Odes, Book II
Authors: Brink C. O.
Published: June 2019

I continue on die lines set out in the last volume but one of these Proceedings. 1. C. II. 2. 19–20 numero beatorum / eximit Virtus (Prahaten). The noun beatus is well established in classical verse as well as prose, although naturally it never reached the substantival status of bonus or honestus. D. R. Shackleton Bailey's repointing of 1. 37. 9–10 contaminato cum grege turpium, / morbo uirorum, etc.,2 assumes a noun tur pis; thus Hor. S. 1. 6. 63–4 qui turpi secernis hones turn / non patre praeclaro, sed uita et pectore puro, A.P. 213 rusticus urbano confusus, tur pis honesto. These two passages suggest that it was the likeness of such terms as bonus or honestus that facilitated this usage. A search in the materials of the Latin Thesaurus (for which I am much obliged to Dr W. Ehlers) shows that this development is, as one might expect, much older than Horace. I am not thinking of Pl. Poen. 338 (where the notion is ‘plain, ugly’, promoted by the contrast with pulchra), but Cic. Att. x. 8. 2 turpissimorum honores, cf. Sen. Dial. VII. 8. ι nec minus turpes dedecus suum quam honestos egregia delectant, 24. 3 in turpes indignos que, Quint. I.O. III. 38 honestis contrasted with apud turpes.

Shackleton Bailey pays tribute to Bendey's taste when he said ‘in illa locutione, uirorum turpium morbo, non agnosco elegantiam Flacci’, while (rightly) refusing the same critic's conjecture opprobriorum for morbo uirorum. At first I found it hard to believe that turpium could be divorced from morbo uirorum, the words immediately following. But now I think that the pun morbo uirorum, ‘men only in vice’, is highly persuasive, and likely, even in a text without punctuation, to be effective in dissociating uirorum from turpium.
Meal patterns of cows offered complete diets with different ratios of concentrate to silage
Authors: Tolkamp B.J. , Friggens N.C. , Emmans G.C. , Kyriazakis I. , Oldham J.D.
Published: June 2019

It is frequently assumed that energy intakes from mixed foods with a high proportion of silage (HS) are lower than those from mixed foods with a high proportion of concentrate (HC), because of short-term constraints, i.e. gut fill, that physically limit the amount of food a cow can consume. It was the aim of the present study to analyse how different proportions of concentrate in mixed foods affect short-term feeding behaviour. We hypothesised that cows offered HS are likely to have more meals that are more spread out during the day and vary less in size than cows offered HC. Alternatively, we expected higher correlations between meal size and the length of intervals before (pre-prandial) or after (post-prandial) meals for cows offered HS than for cows offered HC. We tested the hypotheses with a data set of 21195 meals.
The effect of fodder beet inclusion on milk production and nitrogen and energy utilization of grass silage based diets by lactating dairy cattle
Authors: McIlmoyle D.G. , Patterson D.C. , Kilpatrick D.J.
Published: June 2019

In a previous experiment with dairy cows at this Institute, in which fodder beet was included as a third component of the diet along with grass silage and concentrate, fodder beet considerably increased metabolisable energy intake (MEI), but there was little effect on milk yield (unpublished data). The main objectives of the present study were to examine the effects of including fodder beet versus concentrate in a grass silage diet, on milk production, digestibility of nutrients and the utilization of nitrogen (N) and energy at equal ME intake in lactating dairy cattle.
Changes in GIT digesta VFA as a result of fermentable carbohydrates in piglet diets
Authors: Williams B.A. , Bosch M.W. , Noteborn R. , Verstegen M.W.A.
Published: June 2019

The gastro-intestinal tract (GIT) microflora is thought to remain essentially stable in terms of the range of species present, but it is hypothesized that its activity can be influenced by the diet of the host. The addition of fermentable carbohydrates to an animal diet, may therefore affect the activity of the GIT microflora.
Genetic evaluations and parameter estimates for dairy cow fertility in the United Kingdom
Authors: Kadarmideen H. N. , Coffey M.P. , Kossaibati M.A. , Esslemont R.J.
Published: June 2019

Selection for milk production alone would lead to a genetic decline in cow fertility (e.g. Kadarmideen et al., 2000) thus incorporation of fertility in selection seems desirable. The Dairy Information System (DAISY) is a comprehensive recording scheme for insemination and health events and hence the data quality is more reliable for genetic analysis of cow fertility. The objective of this study was to analyse DAISY data to estimate sire breeding values and genetic parameters for various fertility measures based on insemination and calving events on daughters.
Genetic Evaluation of Dairy Bulls For Energy Balance Traits Using Random Regression
Authors: Coffey M.P. , Emmans G.C. , Brotherstone S.
Published: June 2019

The term ‘negative energy balance’ (NEB) is used to describe the condition in early lactation when the energy available from food intake is lower than that of the energy used by the cow for milk output, maintenance and activity. Current selection objectives may be favouring cows that are genetically predisposed to mobilise body tissue. This may have consequences for fertility since cows appear to resume reproductive activity only after the nadir of NEB has passed (Veerkamp et al., 2000). Extreme NEB may be considered generally undesirable, as it is a precursor to health and fertility problems. The aims of this study were: 1) to predict genetic merit for sires for traits contributing to energy balance; 2) to combine those breeding values into an overall energy balance evaluation for bulls using either daily energy flux or body state changes.
Analysis of PrP genotype in relation to performance traits in Suffolk sheep
Authors: Roden J. A. , Haresign W. , Anderson J. M. L.
Published: June 2019

At a time of high public awareness of food safety issues, particularly with respect to transmissable encephalopathies, and a government policy to eradicate scrapie, there is increasing pressure for breeders to select for scrapie resistance in sheep. Genetic variation has been identified at the PrP locus that confers differing degrees of susceptibility to scrapie. In the Suffolk breed this variation is confined to amino acid variations at codon 171, resulting in two alleles R and Q. Animals with the genotype RR and RQ show a greater degree of resistance to scrapie than animals with genotype QQ (Hunter, Moore, Hosie, Dingwall and Greig, 1997).

Genotyping of pedigree animals has now become routine for many breeders and RR animals are favoured. It is, however, unknown whether there is a relationship between PrP genotype and performance traits. The objective of this study was to analyse the relationship between PrP genotype at codon 171 and the performance traits included in the Lean Index (Simm and Dingwall, 1989), which is used for selection in the Suffolk breed.
On the diet selection of sheep: effects of adding urea to foods with different protein contents
Authors: James S. M. , Kyriazakis I. , Emmans G.C.
Published: June 2019

The basis of diet selection for protein in ruminants remains unclear. Tolkamp et al., (1998) proposed a hypothesis to account for the conflicting findings. They proposed that ruminants select their diet on the basis of effective rumen degradable protein (eRDP) rather than for MP yield. As the protein supply of ruminants comes largely from microbial protein, the idea that ruminants select a diet that meets the requirement for eRDP, which is captured and utilised by the microbes to produce microbial protein, is not an unreasonable one. The objective of this experiment was to test the hypothesis that both inadequate and abundant eRDP levels would be avoided by growing sheep when given choices of foods.
Effect of resource density on the use of spatial memory by foraging sheep
Authors: Rodway-Dyer S. J. , Cook J. E. , Rook A. J.
Published: June 2019

Sheep can use spatial memory to locate preferred food items in a background of less preferred items and forage more efficiently if the preferred patches are aggregated (Edwards et al. 1994). However, if a constant proportion of available patches contain food, foraging efficiency is not affected by the total number of patches (Edwards et al. 1996). The objective of this study was to test the hypothesis that spatial memory will be used to a lesser extent as the proportion of patches containing food increases. Not only is the animal faced with a potentially more complex task as the proportion of food patches increases but the cost:benefit ratio of using spatial memory is less. If 10 of 100 potential foraging sites contain food, an animal with perfect spatial memory could locate 5 of these patches in only 5 visits, whereas random searching requires 50 visits. If 50 patches contain food, 5 visits are required with perfect spatial memory but only 10 visits using random searching. Thus the benefit of using spatial memory over random search is reduced from 5:1 to 2:1.