scholarly journals Another Photographic Survey of the Heavens

Nature ◽  
1889 ◽  
Vol 40 (1035) ◽  
pp. 417-418
Keyword(s):  
1999 ◽  
Vol 118 (1) ◽  
pp. 421-431 ◽  
Author(s):  
A. Fresneau ◽  
R. Monier

2006 ◽  
Vol 63 (1) ◽  
pp. 95-104 ◽  
Author(s):  
Tore Haug ◽  
Garry B. Stenson ◽  
Peter J. Corkeron ◽  
Kjell T. Nilssen

Abstract From 14 March to 6 April 2002 aerial surveys were carried out in the Greenland Sea pack ice (referred to as the “West Ice”), to assess the pup production of the Greenland Sea population of harp seals, Pagophilus groenlandicus. One fixed-wing twin-engined aircraft was used for reconnaissance flights and photographic strip transect surveys of the whelping patches once they had been located and identified. A helicopter assisted in the reconnaissance flights, and was used subsequently to fly visual strip transect surveys over the whelping patches. The helicopter was also used to collect data for estimating the distribution of births over time. Three harp seal breeding patches (A, B, and C) were located and surveyed either visually or photographically. Results from the staging flights suggest that the majority of harp seal females in the Greenland Sea whelped between 16 and 21 March. The calculated temporal distribution of births were used to correct the estimates obtained for Patch B. No correction was considered necessary for Patch A. No staging was performed in Patch C; the estimate obtained for this patch may, therefore, be slightly negatively biased. The total estimate of pup production, including the visual survey of Patch A, both visual and photographic surveys of Patch B, and photographic survey of Patch C, was 98 500 (s.e. = 16 800), giving a coefficient of variation of 17.9% for the survey. Adding the obtained Greenland Sea pup production estimate to recent estimates obtained using similar methods in the Northwest Atlantic (in 1999) and in the Barents Sea/White Sea (in 2002), it appears that the entire North Atlantic harp seal pup production, as determined at the turn of the century, is at least 1.4 million animals per year.


Author(s):  
Salvatore Antonio Biancardo ◽  
Cristina Oreto ◽  
Nunzio Viscione ◽  
Francesca Russo ◽  
Gigliola Ausiello ◽  
...  

The growing need to recover and digitally represent heritage infrastructure has led to the challenge of choosing different Building Information Modeling (BIM) platforms that will be used to manage the implementation of the semi-automatic design and reconstruction processes of reverse engineering modeling. The approach to the integrated management of information derived through Heritage-BIM (H-BIM) has been applied to Via del Duomo, one of the main roads in the old town of Naples, Italy. During preliminary inspections of the construction site it was possible to acquire geometric features and pavement/subgrade information, as well as to conduct a photographic survey, with 1,618 photographs collected. Subsequently, the acquired data were processed, using different BIM-based tools, to obtain the 3D mesh; objects were then converted from pure graphic solids into parametric entities by proposing a specific algorithm. Then a library, with the inclusion of all the possible stone paving package alternatives, including all the structural and stress-deforming characteristics such as Young Modulus (E), Poisson coefficient (n), and Safety factor (SF), was created. In this way, it is possible to associate to the generic element the optimal pavement package solution, depending on different construction contexts. As preliminary result, a dynamic model that updates its information package and modifies the output of the analysis every time the data worksheet is integrated with new collected results is proposed for further pavement management operations evaluation.


1989 ◽  
Vol 131 ◽  
pp. 61-61
Author(s):  
E. Capellaro ◽  
M. Turatto ◽  
F. Sabbadin

The object (α1950 = 18h04m.3; δ1950 = −8o56!4) was discovered in a 103a-E+RG 1 objective prism plate taken with the 92/67-cm Schmidt telescope of the Astrophysical Observatory of Asiago (Italy). It presents only the Hα emission and no stellar continuum; following Kohoutek (1965, 1969, 1972) it is a bona fide planetary nebula. This classification is confirmed by the appearance of the object in the red and infrared plates of the Near Infrared Photographic Survey of the galactic plane (Sabbadin, 1986): it is quite bright in the red plate and almost invisible in the infrared one.


1984 ◽  
Vol 78 ◽  
pp. 489-498
Author(s):  
J.A. Tyson

AbstractCounts of faint galaxies should reveal any evidence of galaxy luminosity or color evolution, as well as new information on the faint end of the galaxy luminosity function. The FOCAS automated detection and classification software is reviewed, and results of the deep 4m PF photographic survey to 24th magnitude in 23 fields covering 9 sq. degrees are presented. Color-magnitude plots for stars and galaxies are shown, and galaxy color evolution is discussed. Evidence is found for a faint galaxy blue trend at 22-24 J mag. However, the k-correction becomes so severe at redshift ~1 that the intrinsically fainter galaxies are emphasized in any magnitude-limited survey. No unambiguous evidence is found for evolution. New 4m limit CCD multi-color data are shown and discussed. The limiting magnitude for detection is 27th J magnitude in 2 hours integration. The data exclude evolution starting at any one epoch for z<10.


1977 ◽  
Vol 42 ◽  
pp. 66-71
Author(s):  
H. Mauder

During a photographic survey of the Chamaeleon T association in 1971/1972, evidence was found for quasiperiodic light changes of three variable stars, see Mauder and Sosna (1975). The period of 6.2 days for SY Cha is well seen, the periods of 7 days for VZ Cha and of 8 days for TW Cha are less pronounced. Intrinsic variations are present in addition to the cyclic variations. The three stars were classified by Hoffmeister (1963) as T Tauri type stars from their light variations. Objective prism spectra obtained by Henize and Mendoza (1973) confirm this classification, they found conspicuous emission lines. For SY Cha and TW Cha they got slit spectra, too, which show the typical veiling. The stars SY Cha, TW Cha and VZ Cha have been observed in the UBV system from 1974 March 12 until 1974 March 22, using the ESO standard photometer. In Figures 1 - 3 the light and colour curves are given for SY Cha, TH Cha and VZ Cha. Each point is a mean of generally 8 to 12 integrations, each integration lasting 5 seconds.


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