Publications

This section contains the publications database that collects IAC articles published in scientific journals. Please, click on the arrow to see full search filter and sort options: author, journal, year, etc..

It also provides access to IAC Preprints Repository here: https://research.iac.es/preprints/

  • Characterization of the atmospheric extinction in the near infrared at the Teide Observatory

    Atmospheric extinction data covering a long period are analysed. We present infrared atmospheric extinction in the J, H and K bands obtained at the Teide Observatory from 1989 to 1997. We find high-quality statistical values, similar to those of other good sites, such as Mauna Kea. We devote special attention to the study of the dependence of the

    Fuensalida, J. J. et al.

    Advertised on:

    11
    1998
    Citations
    3
  • Chemical abundance analysis of the open clusters Berkeley 32, NGC 752, Hyades, and Praesepe

    Context. Open clusters are ideal test particles for studying the chemical evolution of the Galactic disc. However, the number and accuracy of existing high-resolution abundance determinations, not only of [Fe/H], but also of other key elements, remains largely insufficient. Aims: We attempt to increase the number of Galactic open clusters that have

    Carrera, R. et al.

    Advertised on:

    11
    2011
    Citations
    113
  • Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1. Abundances in different galactic populations

    Aims.We used the UVES spectrograph (VLT-UT2 telescope) to obtain high-resolution spectra of 6 stars hosting transiting planets, namely for OGLE-TR-10, 56, 111, 113, 132, and TrES-1. These spectra are now used to derive and discuss the chemical abundances for C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn. Methods: .Abundances

    Santos, N. C. et al.

    Advertised on:

    11
    2006
    Citations
    27
  • Chemical abundances of late-type pre-main sequence stars in the σ Orionis cluster

    Context: The young σ Orionis cluster is an important location for studying the formation and evolution of stars, brown dwarfs, and planetary-mass objects. Its metallicity, although it is a fundamental parameter, has not been well determined yet. Aims: We present the first determination of the metallicity of nine young late-type stars in σ Orionis

    González Hernández, J. I. et al.

    Advertised on:

    11
    2008
    Citations
    34
  • Chemical abundances of Planetary Nebulae in M 33

    Using spectroscopic data presented in Magrini et al. (cite{m03}), we have analyzed with the photoionization code CLOUDY 94.00 (Ferland et al. cite{ferland}) 11 Planetary Nebulae belonging to the spiral galaxy M 33. Central star temperatures and nebular parameters have been determined. In particular the chemical abundances of He/H, O/H, N/H, Ar/H

    Magrini, L. et al.

    Advertised on:

    11
    2004
    Citations
    31
  • Chemical analysis of 8 recently discovered extra-solar planet host stars

    We present the chemical analysis of a new set of stars known to harbor low mass companions, namely HD 1237, HD 52265, HD 82943, HD 83443, HD 169830, and HD 202206. In addition, we have also analyzed HD 13445 and HD 75289, already studied elsewhere. The abundances of C and alpha -elements O, S, Si, Ca and Ti are presented and discussed in the

    Santos, N. C. et al.

    Advertised on:

    11
    2000
    Citations
    149