scholarly journals Internal R-process Abundance Spread of M15 and a Single Stellar Population Model

2021 ◽  
Vol 921 (1) ◽  
pp. L11
Author(s):  
Yuta Tarumi ◽  
Naoki Yoshida ◽  
Shigeki Inoue
Keyword(s):  
Population Model ◽  
Stellar Population ◽  
R Process

scholarly journals Visual–IR Color Gradients in Elliptical Galaxies

1987 ◽  
Vol 127 ◽  
pp. 443-444
Author(s):  
R. F. Peletier ◽  
E. A. Valentijn ◽  
R. F. Jameson
Keyword(s):  
Population Model ◽  
Stellar Population ◽  
Main Sequence ◽  
Elliptical Galaxies ◽  
Strong Constraint ◽  
Average Temperature ◽  
Simultaneous Measurements ◽  
Continuity Of Solutions ◽  
Different Populations ◽  
Color Gradients

Dissipational formation theories (e.g. Larson 1974) predict a metallicity change with distance from the center in elliptical galaxies. Several authors have reported small color gradients in visual colors like B–V and B–R. The interpretation of these data is not easy, due to uncertainties caused by the short wavelength–baseline, and by the presence of a hot stellar population suggested by IUE–data (e.g. Burstein et al. 1986). Simultaneous measurements of visual and visual-infrared colors provide the means to determine both the average temperature of the giant branch and the turnoff–temperature of the main sequence. This allows to model fractional contributions of different populations, including age– and metallicity–effects. The required continuity of solutions at different radii provides a strong constraint in selecting a more unique overall population model, and relieves the ambiguous interpretation of single measurements.

scholarly journals Magellan/M2FS Spectroscopy of Galaxy Clusters: Stellar Population Model and Application to Abell 267

2017 ◽  
Vol 154 (3) ◽  
pp. 113 ◽  
Author(s):  
Evan Tucker ◽  
Matthew G. Walker ◽  
Mario Mateo ◽  
Edward W. Olszewski ◽  
John I. Bailey ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Population Model ◽  
Stellar Population

scholarly journals Did brightest cluster galaxies experience more than one star formation epoch?

2012 ◽  
Vol 8 (S295) ◽  
pp. 320-320
Author(s):  
D. N. Viljoen ◽  
S. I. Loubser
Keyword(s):  
Star Formation ◽  
Population Model ◽  
Stellar Population ◽  
Star Formation History ◽  
Full Spectrum ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Formation History ◽  
Spectrum Fitting ◽  
Fitting Ability

AbstractWe use the full spectrum fitting ability of ULySS, with the Pegase.HR stellar population model to fit the observed spectra of 40 brightest cluster galaxies in order to determine whether a single or a composite stellar population provided the most probable representation of the star formation history (SFH). We find that some galaxies in the sample have more complex SFHs.

scholarly journals Comparison of stellar population model predictions using optical and infrared spectroscopy

2017 ◽  
Vol 473 (4) ◽  
pp. 4698-4721 ◽  
Author(s):  
C. Baldwin ◽  
R. M. McDermid ◽  
H. Kuntschner ◽  
C. Maraston ◽  
C. Conroy
Keyword(s):  
Infrared Spectroscopy ◽  
Population Model ◽  
Stellar Population ◽  
Model Predictions

scholarly journals The Chemical Properties of Milky Way and M31 Globular Clusters. II. Stellar Population Model Predictions

2005 ◽  
Vol 129 (3) ◽  
pp. 1412-1427 ◽  
Author(s):  
Michael A. Beasley ◽  
Jean P. Brodie ◽  
Jay Strader ◽  
Duncan A. Forbes ◽  
Robert N. Proctor ◽  
...  
Keyword(s):  
Population Model ◽  
Globular Clusters ◽  
Stellar Population ◽  
Milky Way ◽  
Chemical Properties ◽  
Model Predictions

Distribution of R- and S-Process Elements in the Galactic Halo

1988 ◽  
Vol 132 ◽  
pp. 501-506
Author(s):  
C. Sneden ◽  
C. A. Pilachowski ◽  
K. K. Gilroy ◽  
J. J. Cowan
Keyword(s):  
Heavy Element ◽  
Galactic Halo ◽  
Low Noise ◽  
Heavy Elements ◽  
Process Synthesis ◽  
Element Abundances ◽  
Halo Stars ◽  
Abundance Patterns ◽  
R Process ◽  
Process Elements

Current observational results for the abundances of the very heavy elements (Z>30) in Population II halo stars are reviewed. New high resolution, low noise spectra of many of these extremely metal-poor stars reveal general consistency in their overall abundance patterns. Below Galactic metallicities of [Fe/H] Ã −2, all of the very heavy elements were manufactured almost exclusively in r-process synthesis events. However, there is considerable star-to-star scatter in the overall level of very heavy element abundances, indicating the influence of local supernovas on element production in the very early, unmixed Galactic halo. The s-process appears to contribute substantially to stellar abundances only in stars more metal-rich than [Fe/H] Ã −2.

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