1,723,172 research outputs found
Block Card 5824 Fryer Avenue
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Ranch houses | 5824 Fryer Avenue (Toledo, Ohio) | Dwelling | Inverness Suburban Acres (Toledo, Ohio) | Reynolds Corners Area (Toledo, Ohio) | 5824 Fryer Avenue (Toledo, Ohio
Existence of tidal tails for the globular cluster NGC 5824
No full textContext. Several dynamically cold streams have been associated with certain globular clusters (GCs) based on orbital energies and angular momenta. Some of these streams are surprisingly far apart from their progenitors and one such pair is Triangulum and NGC 5824. Triangulum can be considered as a piece of the leading tail of NGC 5824 since the cluster’s future orbit matches well with the stream’s track. The existence of the leading tail of NGC 5824 is the motivation behind the search for its trailing tail.
Aims. Our goal is to confirm the connection between Triangulum and NGC 5824. We also search for the trailing tail of the cluster.
Methods. The selection of member stars of Triangulum is made through various cuts in metallicity, proper motions (PMs), radial velocity and a color–magnitude diagram (CMD). The selected members are compared in phase space to a mock stream that models the disruption of NGC 5824. We then try to detect the trailing tail of the cluster based on a modified matched-filter technique. Stars are assigned weights using their color differences from the cluster’s locus in the CMD. These weights are further scaled, based on the stars’ departures from expected PMs of the model stream.
Results. A total of 26 member stars for Triangulum are obtained, 16 of which are newly identified. These members are consistent with the mock stream in the phase space, and their metalicity and position on the CMD are in good agreement with NGC 5824. By applying the matched filter, a tenuous trailing tail of the cluster is detected, spanning ∼50° long on sky. The signature matches well with the mock stream’s trajectory.
Conclusions. Our results support that the Triangulum stream acts as a part of the leading tail for NGC 5824. On the trailing side, we detected a 50° tail extending from the cluster. The existence of both leading and trailing tails for the GC NGC 5824 is verified
Block Card 5824 Everwood Road
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Ranch houses | 5824 Everwood Road (Toledo, Ohio) | Dwelling | Greenwood Park Area (Toledo, Ohio
Block Card 5824 Secor Road
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Girard Hardware (Toledo, Ohio) | post-modern | one story | commercial buildings | Trilby Place Addition (Toledo, Ohio) | Trilby Area (Toledo, Ohio)) | 5824 Secor Road (Toledo, Ohio
Block Card 5824 Sims Drive
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Ranch houses | 5824 Sims Drive (Toledo, Ohio) | Dwelling | Extension of Oak Grove Gardens (Toledo, Ohio) | Reynolds Corners Area (Toledo, Ohio
Block Card 5824 Semoff Drive
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Ranch Style | 5824 Semoff Drive (Toledo, Ohio) | Dwelling | Garnet Place Addition (Toledo, Ohio) | Trilby Area (Toledo, Ohio)
Linked collectors and determiners for: Fungario (LPS Tipos) - División Micología "Instituto Spegazzini".
No full textNatural history specimen data linked to collectors and determiners held within, "Fungario (LPS Tipos) - División Micología "Instituto Spegazzini"". Claims or attributions were made on Bionomia by volunteer Scribes, <a href="http://bionomia.net/dataset/6b84f3b4-5824-41fb-b8f8-b41a7494873a">https://bionomia.net/dataset/6b84f3b4-5824-41fb-b8f8-b41a7494873a</a> using specimen data from the dataset aggregated by the Global Biodiversity Information Facility, <a href="https://gbif.org/dataset/6b84f3b4-5824-41fb-b8f8-b41a7494873a">https://gbif.org/dataset/6b84f3b4-5824-41fb-b8f8-b41a7494873a</a>. Formatted as a Frictionless Data package
Hans Hörmann, Psychologie der Sprache. Berlin : Springer Verlag, 1967. 365 p.
No full textContains fulltext :
5824.pdf (Publisher’s version ) (Open Access
Ngc 5824: A luminous outer halo globular cluster with an intrinsic abundance spread
No full textWe present a detailed study of the strengths of the calcium triplet absorption lines in the spectra of a large sample of red giant members of the luminous outer Galactic halo globular cluster NGC 5824. The spectra were obtained with the FORS2 and GMOS-S multi-object spectrographs at the VLT and the Gemini-S telescope, respectively. By comparing the line strengths of the NGC 5824 stars with those for red giants in clusters with well-established abundances, we conclude that there is an intrinsic abundance dispersion in NGC 5824 characterized by an inter-quartile range in [Fe/H] of 0.10 dex and a total range of ∼0.3 dex. As for ω Cen and M22, the abundance distribution shows a steep rise on the metal-poor side and a shallower decline on the metal-rich side. There is also some indication that the distribution is not unimodal with perhaps three distinct abundance groupings present. NGC 5824 has a further unusual characteristic: the outer surface density profile shows no signs of a tidal cutoff. Instead, the profile has a power-law distribution with cluster stars detected to a radius exceeding 400 pc. We postulate that NGC 5824 may be the remnant nuclear star cluster of a now disrupted dwarf galaxy accreted during the formation of the Galaxy's halo. We further speculate that the presence of an intrinsic [Fe/H] spread is the characteristic that distinguishes former nuclear star clusters from other globular clusters
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