Relevant bibliographies by topics / Globular clusters: individual(NGC 7006)

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  1. Journal articles
  2. Dissertations / Theses

Academic literature on the topic 'Globular clusters: individual(NGC 7006)'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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Journal articles on the topic "Globular clusters: individual(NGC 7006)"

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Buonanno, R., F. F. Pecci, E. Capellaro, S. Ortolani, T. Richtler, and E. H. Geyer. "CCD photometry of globular clusters. IV - NGC 7006." Astronomical Journal 102 (September 1991): 1005. http://dx.doi.org/10.1086/115928.

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Dinescu, Dana I., Steven R. Majewski, Terrence M. Girard, and Kyle M. Cudworth. "Orbits of Globular Clusters in the Outer Galaxy: NGC 7006." Astronomical Journal 122, no. 4 (2001): 1916–27. http://dx.doi.org/10.1086/323094.

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Wehlau, Amelia, and James M. Nemec. "RR Lyrae Variables in the Second-Parameter Globular Cluster NGC 7006." International Astronomical Union Colloquium 139 (1993): 420. http://dx.doi.org/10.1017/s0252921100118111.

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AbstractThe distant globular cluster NGC7006 was one of the first clusters studied for which the distribution of stars along the horizontal branch of its C-M diagram showed evidence for a “second parameter” in addition to metallicity. Studies of the more than 60 known RR Lyrae stars in this cluster should yield some statistically significant trends or correlations which might help to identify the second parameter. In the first stage of this study (Wehlau, Nemec, Han-Ian $ Rich 1992, AJ, 103, 1583) photographic data from 1984 were combined with previously published data from the 1930's and 1950
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Chun, Mun-Suk. "Inhomogeneities in Globular Clusters." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 37–40. http://dx.doi.org/10.1017/s1323358000024826.

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AbstractInhomogeneities in globular clusters are reviewed with the observational evidence for chemical abundance variations from star to star in individual clusters and the large-scale structural variation of clusters. The reality of the radial colour gradient is tested in 47 Tuc (NGC 104). The result shows that the observed radial colour gradient comes from the integration of the calculated colours of individual stars. The cause of this radial colour variation is the result of the concentration of evolved stars and the reddening of the main sequence in the central region. We propose that the
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Geisler, Doug, Taft Armandroff, Gary Da Costa, Myung Gyoon Lee, and Ata Sarajedini. "HST Color-Magnitude Diagrams of Globular Clusters in NGC 185 and NGC 205." Symposium - International Astronomical Union 192 (1999): 231–36. http://dx.doi.org/10.1017/s0074180900204166.

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We present a progress report on our ongoing HST WFPC2 study of globular clusters in NGC 185 and NGC 205. Most of the cluster candidates studied previously only from the ground are indeed globular clusters; however, several candidates turn out to be either foreground stars or background galaxies. In addition, we have discovered one new, previously unsuspected cluster. A complete knowledge of the globular cluster systems in even these nearby galaxies requires high spatial resolution data. We then derive preliminary I, (V – I) color-magnitude diagrams for some of the clusters, as well as for thei
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Held, Enrico V., Luciana Federici, Carla Cacciari, and Vincenzo Testa. "Ages and Metallicities of Globular Clusters in NGC 5128." Symposium - International Astronomical Union 207 (2002): 269–74. http://dx.doi.org/10.1017/s007418090022384x.

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We have obtained multislit spectroscopy of 40 known globular clusters in the nearby peculiar elliptical galaxy NGC 5128 at the ESO NTT telescope. Measurements of metal and hydrogen absorption line indices have been used to estimate the age and metal content of individual clusters. The results have been combined with previous data from multifibre spectroscopy of clusters in the halo of NGC 5128 to study the age and metallicity distribution of the globular cluster system.
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Harris, Gretchen L. H. "NGC 5128: The Giant Beneath." Publications of the Astronomical Society of Australia 27, no. 4 (2010): 475–81. http://dx.doi.org/10.1071/as09063.

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AbstractThis paper reviews what has been learned about the old stellar population of NGC 5128, the only large elliptical galaxy close enough that we can currently observe individual stars as faint as the horizontal branch. Although its galaxy type is still a matter of debate, the uncertainties over distance are now largely resolved; comparison of five stellar distance indicators gives d= 3.8±0.1 Mpc. The globular cluster system, which was once perplexingly invisible, is now known to be predominantly old with a substantial metal-rich component. The globular cluster system (GCS) total population
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Anders, Peter, Uta Fritze –. v. Alvensleben, and Richard de Grijs. "Young Star Clusters: Progenitors of Globular Clusters!?" Highlights of Astronomy 13 (2005): 366–68. http://dx.doi.org/10.1017/s1539299600015987.

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AbstractStar cluster formation is a major mode of star formation in the extreme conditions of interacting galaxies and violent starbursts. Young clusters are observed to form in a variety of such galaxies, a substantial number resembling the progenitors of globular clusters in mass and size, but with significantly enhanced metallicity. From studies of the metal-poor and metal-rich star cluster populations of galaxies, we can therefore learn about the violent star formation history of these galaxies, and eventually about galaxy formation and evolution. We present a new set of evolutionary synth
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Bastian, Nate, Christopher Usher, Sebastian Kamann, et al. "Multiple populations in integrated light spectroscopy of intermediate-age clusters." Monthly Notices of the Royal Astronomical Society: Letters 489, no. 1 (2019): L80—L85. http://dx.doi.org/10.1093/mnrasl/slz130.

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ABSTRACT The presence of star-to-star light-element abundance variations (also known as multiple populations, MPs) appears to be ubiquitous within old and massive clusters in the Milky Way and all studied nearby galaxies. Most previous studies have focused on resolved images or spectroscopy of individual stars, although there has been significant effort in the past few years to look for multiple population signatures in integrated light spectroscopy. If proven feasible, integrated light studies offer a potential way to vastly open parameter space, as clusters out to 10s of Mpc can be studied.
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Smith, Graeme H., Michael M. Briley, and Daniel Harbeck. "A Comparison between Carbon and Nitrogen Abundances of Bright Giants in the Globular Clusters M13, M10, and NGC 7006." Astronomical Journal 129, no. 3 (2005): 1589–95. http://dx.doi.org/10.1086/427714.

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Dissertations / Theses on the topic "Globular clusters: individual(NGC 7006)"

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Johnson, Christian I., Nelson Caldwell, R. Michael Rich, et al. "Chemical Complexity in the Eu-enhanced Monometallic Globular NGC 5986." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624431.

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NGC 5986 is a poorly studied but relatively massive Galactic globular cluster that shares several physical and morphological characteristics with "iron-complex" clusters known to exhibit significant metallicity and heavy-element dispersions. In order to determine whether NGC 5986 joins the iron-complex cluster class, we investigated the chemical composition of 25 red giant branch and asymptotic giant branch cluster stars using high-resolution spectra obtained with the Magellan-M2FS instrument. Cluster membership was verified using a combination of radial velocity and [Fe/H] measurements, and w
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Johnson, Christian I., R. Michael Rich, Nelson Caldwell, et al. "Exploring the Chemical Composition and Double Horizontal Branch of the Bulge Globular Cluster NGC 6569." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626525.

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Photometric and spectroscopic analyses have shown that the Galactic bulge cluster Terzan 5 hosts several populations with different metallicities and ages that manifest as a double red horizontal branch (HB). A recent investigation of the massive bulge cluster NGC 6569 revealed a similar, though less extended, HB luminosity split, but little is known about the cluster's detailed chemical composition. Therefore, we have used high- resolution spectra from the Magellan-M2FS and VLT-FLAMES spectrographs to investigate the chemical compositions and radial velocity distributions of red giant branch
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Johnson, Christian I., Nelson Caldwell, R. Michael Rich, et al. "A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623231.

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Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this "iron-complex" cluster class, and we provide here a chemical and kinematic analysis of > 300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the Magellan-M2FS and VLT-FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that
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Dupree, A. K., A. Dotter, C. I. Johnson, et al. "NGC 1866: First Spectroscopic Detection of Fast-rotating Stars in a Young LMC Cluster." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625815.

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High-resolution spectroscopic observations were taken of 29 extended main-sequence turnoff (eMSTO) stars in the young (similar to 200 Myr) Large Magellanic Cloud (LMC) cluster, NGC 1866, using the Michigan/Magellan Fiber System and MSpec spectrograph on the Magellan-Clay 6.5 m telescope. These spectra reveal the first direct detection of rapidly rotating stars whose presence has only been inferred from photometric studies. The eMSTO stars exhibit Ha emission (indicative of Be-star decretion disks), others have shallow broad H alpha absorption (consistent with rotation. greater than or similar
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Bellini, Andrea, Mattia Libralato, Luigi R. Bedin та ін. "The HST Large Programme on ω Centauri. II. Internal Kinematics". IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627043.

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In this second installment of the series, we look at the internal kinematics of the multiple stellar populations of the globular cluster omega Centauri in one of the parallel Hubble Space Telescope (HST) fields, located at about 3.5 hal-flight radii from the center of the cluster. Thanks to the over 15 yr long baseline and the exquisite astrometric precision of the HST cameras, well-measured stars in our proper-motion catalog have errors as low as similar to 10 mu as yr(-1), and the catalog itself extends to near the hydrogen-burning limit of the cluster. We show that second-generation (2G) st
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Gruyters, Pieter. "Exploring the Chemical Evolution of Globular Clusters and their Stars : Observational Constraints on Atomic Diffusion and Cluster Pollution in NGC 6752 and M4." Doctoral thesis, Uppsala universitet, Observationell astrofysik, 2014. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-230182.

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Through the cosmic matter cycle, the chemical evolution of the Milky Way is imprinted in the elemental abundance patterns of late-type stars (spectral types F to K). Due to their long lifetimes ( 1 Hubble time), these stars are of particular importance when it comes to studying the build-up of elements during the early times of our Galaxy. The chemical composition of the atmospheric layers of such stars is believed to resemble the gas from which they were formed. However, recent observations in globular clusters seem to contradict this assumption. The observations indicate that processes are a
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Libralato, Mattia, Andrea Bellini, Luigi R. Bedin та ін. "The HST Large Programme on ω Centauri. III. Absolute Proper Motion". IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627099.

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In this paper, we report a new estimate of the absolute proper motion (PM) of the globular cluster NGC 5139 (omega Cen) as part of the HST large program GO-14118+ 14662. We analyzed a field 17 arcmin southwest of the center of omega Cen and computed PMs with epoch spans of similar to 15.1 years. We employed 45 background galaxies to link our relative PMs to an absolute reference-frame system. The absolute PM of the cluster in our field is (mu(alpha) cos delta, mu(delta))=(-3.341. 0.028, -6.557 +/- 0.043) mas yr(-1). Upon correction for the effects of viewing perspective and the known cluster r
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Sakari, Charli. "Chemical Abundances of Local Group Globular Clusters." Thesis, 2014. http://hdl.handle.net/1828/5621.

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Detailed chemical abundances of globular clusters in the Milky Way and M31 (the Andromeda Galaxy) are presented based on analyses of high resolution spectra. The unusual Milky Way cluster Palomar 1 (Pal 1) is studied through spectra of individual red giant branch stars; these abundances show that Pal 1 is not a classical globular cluster, and may have been accreted from a dwarf satellite of the Milky Way. The Milky Way globular clusters 47 Tuc, M3, M13, NGC 7006, and M15 are studied through their integrated light (i.e. a single spectrum is obtained for each cluster) in order to test high
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Simon, Amélie. "Étude de l'influence de la composition du cœur des naines blanches sur le calcul des âges." Thèse, 2017. http://hdl.handle.net/1866/20608.

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