A comparison of optical and near infrared colours of Magellanic Cloud star clusters with predictions of simple stellar population models

No obstante, como esta enfermedad afecta a cada persona de manera diferente, no todas las opciones de cuidado y tratamiento pueden ser apropiadas para cada individuo.. La forma

We find that the mass and radius values for GJ 357 b based on a given method to derive the stellar parameters of the host star exhibit considerable uncertainties. However,

to simultaneously fit the photometry and spectroscopy, and thereby derive the formation lookback time, by which point half of the observed stellar mass has been formed, and the

That is, local MS stars located at a dis- tance shorter than ∼2.5 kpc are not affected by the presence of the star-forming region G61.48 +0.09, but more distant MS stars have

• Stellar kinematic signatures of intermediate mass black holes in nuclear stellar clusters (with T.. Compare star formation history deduced from fit to absorption line spectra

We explored the entire input parameter space in 24 differ- ent tests to choose the best combination of parameters for the STECKMAP run (see Sect. All these tests can be inter- preted

Using a combination of optical photometry and spectroscopy we esti- mate stellar masses, ages, and foreground extinction values of the brightest part of the population

In summary, from the cluster analysis of individual bright knots and from the integrated photometry of the whole complex, there are clear indications that there is a complex