Mean Distribution of Stars According to Apparent Magnitude and Galactic Latitude

Seares, Frederick H.; Rhijn, P. J. van; Joyner, Mary C.; Richmond, Myrtle L.

doi:10.1086/142940

Cited by 34 publications

(12 citation statements)

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“…For our analysis, we have attempted to underdraw the individual star deflections (the entries labelled "total" in Table 2) in order to permit a comparison with predicted intensities based on star counts. In Figure 3> we show plots of the results of our analysis for integrated starlight, Ik Milky Way and near the galactic pole is now about 10, in substantial agreement with our earlier remarks An integration of intensities based on star counts is possible by reference to the classical study of van Rhijn [1925 ] who published tables of log N m to m(pg) = 18.0 for 10,296 discrete regions of the celestial sphere. * The results are necessarily highly smoothed since their basis is the 206 "Selected Areas" the study of which was initiated by Kapteyn in 1906.…”

Section: The Integrated Starlightsupporting

confidence: 85%

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Absolute photometry of the light of the night sky:

Roach¹

1964

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A study is presented of one year of systematic zenith observations made with similar photometers at two observing stations: Haleakala (latitude N 20.7°) and Fritz Peak (latitude N 39-9°). It is shown that, for an effective wavelength of 5300 A, there is a change of intensity with sidereal time (and therefore right ascension) due to three components:(l) integrated starlight, (2) zodiacal light, and (3) airglow continuum. Quantitative separation of the components is made. A critical comparison is made with some earlier investigations with particular reference to the problem of the galactic light.

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Section: The Integrated Starlightsupporting

confidence: 85%

“…According to Seares, et al [1925], the total light from all the stars is equivalent to that from 1092 stars of the first visual magnitude.…”

Section: The Observational Materialsmentioning

confidence: 99%

Absolute photometry of the light of the night sky:

Roach¹

1964

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“…Roach and Megill (see also Megill and Roach, 1961) integrated the GR43 star counts at Kapteyn's 206 S As to obtain the integrated starlight. Star counts by Seares et al (1925) in SAs 1-139 using the Mount Wilson star catalogs deviate substantially from those of GR43 as the galactic plane is approached. Integrated starlight levels derived from the former are systematically lower than those derived from the latter.…”

Section: Modern Star Counts and Photometric Surveys Of Background Lightmentioning

confidence: 87%

Optical Observations of Galactic and Extragalactic Light: Implications for Galactic Structure

Toller

1990

Symp. - Int. Astron. Union

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A historical review of integrated starlight, diffuse galactic light, and extragalactic light studies is presented. Together, these components compose the “background light.” Methods ranging from star counts to space-based photometric surveys have succeeded in quantifying the contribution of each component of the background. Integrated starlight is the dominant component. The contribution of diffuse galactic light in the general interstellar medium peaks slightly off the galactic plane and declines toward higher latitudes. The extragalactic light has been determined from both galaxy counts and photometric methods. The blue and red intensity and B–R color distribution of background light have been mapped. The relation between galactic structure and background light measurements is established. The distribution of interstellar extinction is the primary regulator of the brightness. However, spiral arm and stellar distribution effects are discerned in Carina and Sagittarius. The sun lies 13 pc north of the galactic plane as defined by brightness and dust distributions.

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“…Seares et al (1925). Neglecting overexposure and overlapping, the classification time would probably amount to several months (a few weeks) for a visual classifier, who classifies at a rate of 40 spectra h" 1 and with time allowed for checking purposes.…”

Section: Some Implications Of Automatic Spectral Classificationmentioning

confidence: 99%

Automatic Classification of Objective Prism Spectra

West

1973

Symp. - Int. Astron. Union

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Abstract. Methodological problems and hardware/software requirements of efficient automatic clas sification of objective prism stellar spectra are described on the basis of experience from 'microphotometer-computer' classification. Significant advances in hardware (two-dimensional scanners, on-line computers) as well as in software (image processing techniques) have now brought high-speed, exhaustive, automatic classification within reach. Some astronomical implications of automatic spectral surveys are discussed.

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Mean Distribution of Stars According to Apparent Magnitude and Galactic Latitude

Cited by 34 publications

References 0 publications

Absolute photometry of the light of the night sky:

Absolute photometry of the light of the night sky:

Optical Observations of Galactic and Extragalactic Light: Implications for Galactic Structure

Automatic Classification of Objective Prism Spectra

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