Reduction of the Harvard-Groningen Durchmusterung to the International System of Magnitude and Color

Seares, Frederick H.; Joyner, Mary C.; Richmond, Myrtle L.

doi:10.1086/142890

Cited by 4 publications

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“…Hence, when all the Areas of the MWC were considered and averaged together in the distribution tables of the early papers, binned as they were only by Galactic latitude, not by longitude as well (cf. Seares et al 1925aSeares et al , 1925b, the large systematic differences shown in Table 12 were extremes and were missed.…”

Section: The Color Equationmentioning

confidence: 99%

“…New star counts in B are compared with the earlier counts listed by Seares et al (1925b) and discussed log N(m ) pg further by Seares & Joyner (1928). Because the area covered by the original Mount Wilson work is so small, being a circular region of diameter 23Ј (0.115 deg 2 ), Seares et al (1925b) originally augmented their data using counts of brighter stars in the much larger area of each of the fields that are listed in the Durchmusterung of Selected Areas (Pickering & Kapteyn 1918;Pickering, Kapteyn, & van Rhijn 1923, 1924, as reduced to the international scale by Seares, Joyner, & Richmond (1925a). The total data were summarized by van Rhijn (1929) in his homogenization of many individual sources.…”

Section: The Present Programmentioning

confidence: 99%

“…The work had many purposes and uses. Examples include studies of the structure of the Galaxy using star counts (Seares 1917(Seares , 1928Seares et al 1925a, 1925b, van Rhijn 1917, 1929; magnitude sequences to calibrate the early galaxy counts by Fath (1914) and Seares (1925); magnitude standards that were transferred to special regions such as NGC 6822, M33, and M31 (Hubble 1925(Hubble , 1926(Hubble , 1929 for the photometry of their Cepheid variables; the magnitude sequences of Hubble (1934Hubble ( , 1936aHubble ( , 1936b for new galaxy counts in his attempt to measure the curvature of space using them; magnitude sequences used by Baade (1938) and Baade & Zwicky (1938) for the photometry of the light curves of the supernovae SN 1937C and SN 1937D in IC 4182 and NGC 1003, respectively; magnitude sequences transferred from several Selected Areas into M31 and M33 for photometry of their supergiant blue variables (Hubble & Sandage 1953); and many more.…”

Section: Introductionmentioning

confidence: 99%

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The Mount Wilson Halo Mapping Project 1975–1985. II. Photometric Properties of the Mount Wilson Catalogue of Photographic Magnitudes in Selected Areas 1–139

Sandage

2001

PUBL ASTRON SOC PAC

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This paper is partly a review of the history of the making of the Mount Wilson Catalogue of Photographic Magnitudes in Selected Areas 1-139 (hereafter the MWC), begun in 1909 and completed in 1930, and it is partly the presentation of new photometric results concerning it. Photoelectric photometry of 435 stars in the 11 Selected Areas of SA 28, 29, 45, 55, 57, 71, 82, 94, 106, 107, and 118 of the MWC is given. The data are used to derive magnitude corrections to the MWC for these areas. Ten of the areas are in the Galactic meridional plane (Galactic longitudes of 0Њ and 180Њ). These are the same areas used by Becker in his Basel program of star counts for the study of Galactic structure.The first purpose of the paper is to extend the Basel star counts to fainter magnitudes. For this, 200 inch photographic plates were measured to the plate limits near , calibrated with the photoelectric photometry B p 22 listed here. A second purpose is to derive certain properties of the catalog. The interests are (1) to determine the internal (random) measuring errors of the MWC as a function of magnitude after correcting for the systematic scale error in each area, (2) to test for a color equation between the corrected m pg (MWC) values and the B pe system that must be present because of the difference in reflectivity between silvered and aluminized mirrors, and (3) to test for possible distance-to-center corrections of the scale-corrected MWC magnitudes.Photographic photometry is used to complete the count surveys in each of the program areas to the limit of the 200 inch plates. Color-magnitude diagrams are shown for each area, generally complete to , V p 20 BϪ . The work is preparatory to an analysis for Galactic structure when the larger database is available V p 2.0 in a program by Majewski using Kitt Peak 4 m plates, epoch circa 1975, that will be to provide both a deeper count survey in B and V and proper motions for the larger sample.

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Section: The Color Equationmentioning

confidence: 99%

Section: The Present Programmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Mount Wilson Halo Mapping Project 1975–1985. II. Photometric Properties of the Mount Wilson Catalogue of Photographic Magnitudes in Selected Areas 1–139

Sandage

2001

PUBL ASTRON SOC PAC

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Relative Farbhelligkeiten von 26 Polsternen

Lohmann

1939

Astron Nachr

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Eingegangen 1939 Juni 9Am Spiegelspektrographen der Universitats2ternwarte LTipzig wurden Spektrogramme der Bergstrandst$rne am Nordpol aufgenommen. Sie wurden zwischen 36ooA und 64mA in 14 aufeinanderfolgenden Bereichen zu zooA Breite photometriert (,)Farbhelligkeiten(() und an zwei Fundamentalsterne von Kienle angeschlossen.Neben der gewohnlichen Extinktion muDte bei einem groI3en Teile der Platten ein zeitlicher Effekt beriicksichtigt werden, der als Empfindlichkeitsanderung der Platten oder Durchsichtsverbesserung des Himmels gedeutet werden kann.Die photometrische Skala wurde durch ein Beugungsgitter erzeugt, an der P D geeicht und die Farbhelligkeiten in das internationale (photovisuelle) System gebracht.Nach Einfuhrung und Diskussion der rFarbung((, eines Analogons des Gradienten, wurde eine vorlaufige Verbindung zwischen den Leipziger Farbhelligkeiten und dem Gottinger Temperaturprogramm hergestellt und ein Vergleich mit den Edinburger Gradienten durchgefuhrt.AbschlieDend wurden von I z photometrischen Systemen (Integralhelligkeiten) nach einem Naherungsverfahren isophote Wellenlangen bestimmt.

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Verbesserte Helligkeiten von 229 Sternen im System der RHP mit Beitrag zur Prüfung der Skala der RHP

Günther¹

1952

Astron Nachr

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Reduction of the Harvard-Groningen Durchmusterung to the International System of Magnitude and Color

Cited by 4 publications

References 0 publications

The Mount Wilson Halo Mapping Project 1975–1985. II. Photometric Properties of the Mount Wilson Catalogue of Photographic Magnitudes in Selected Areas 1–139

The Mount Wilson Halo Mapping Project 1975–1985. II. Photometric Properties of the Mount Wilson Catalogue of Photographic Magnitudes in Selected Areas 1–139

Relative Farbhelligkeiten von 26 Polsternen

Verbesserte Helligkeiten von 229 Sternen im System der RHP mit Beitrag zur Prüfung der Skala der RHP

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