The IACOB project: A new Era in the Study of Galactic OB Stars

Start year
2014
End year
2017
Organizational Unit

Grants related:

    General
    Description

    IACOB is an ambitious long-term project whose main scientific goal is to provide an unprecedented empirical overview of the main physical properties of Galactic massive O- and B-type stars which can be used as definitive anchor point for our theories of stellar atmospheres, winds, interiors and evolution of massive stars

    Principal investigator
    Collaborators
    Dr.
    KLAUS SIMON RUBKE ZUÑIGA
    Dr.
    INÉS CAMACHO IÑESTA
    Dr.
    Jesús Maíz Apellaniz
    Dr.
    Ignacio Negueruela
    Dr.
    Norberto Castro
    Dr.
    Carolina Sabín-Sanjulian
    Dr.
    Javier Lorenzo
    Dr.
    Ricardo Dorda e
    Dr.
    María Fernanda Nieva
    Dr.
    Jorge García-Rojas
    Dr.
    Nevy Markova
    Dr.
    Miguel A. Urbaneja

    Related publications

    • The massive multiple system HD 64315
      Context. The O6 Vn star HD 64315 is believed to belong to the star-forming region known as NGC 2467, but previous distance estimates do not support this association. Moreover, it has been identified as a spectroscopic binary, but existing data support contradictory values for its orbital period. Aims: We explore the multiple nature of this star
      Lorenzo, J. et al.

      Advertised on:

      10
      2017
      Citations
      14
    • The VLT-FLAMES Tarantula Survey. XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula
      A spectroscopic analysis has been undertaken for the B-type multiple systems (excluding those with supergiant primaries) in the VLT-FLAMES Tarantula Survey (VFTS). Projected rotational velocities, vesini, for the primaries have been estimated using a Fourier Transform technique and confirmed by fitting rotationally broadened profiles. A subset of
      Garland, R. et al.

      Advertised on:

      7
      2017
      Citations
      17
    • The VLT-FLAMES Tarantula Survey. XXVI. Properties of the O-dwarf population in 30 Doradus
      Context. The VLT-FLAMES Tarantula Survey has observed hundreds of O-type stars in the 30 Doradus region of the Large Magellanic Cloud (LMC). Aims: We study the properties of a statistically significant sample of O-type dwarfs in the same star-forming region and test the latest atmospheric and evolutionary models of the early main-sequence phase of
      Sabín-Sanjulián, C. et al.

      Advertised on:

      5
      2017
      Citations
      46
    • Kepler sheds new and unprecedented light on the variability of a blue supergiant: Gravity waves in the O9.5Iab star HD 188209
      Stellar evolution models are most uncertain for evolved massive stars. Asteroseismology based on high-precision uninterrupted space photometry has become a new way to test the outcome of stellar evolution theory and was recently applied to a multitude of stars, but not yet to massive evolved supergiants.Our aim is to detect, analyse and interpret
      Aerts, C. et al.

      Advertised on:

      6
      2017
      Citations
      39
    • The VLT-FLAMES Tarantula Survey . XXIV. Stellar properties of the O-type giants and supergiants in 30 Doradus
      Context. The Tarantula region in the Large Magellanic Cloud (LMC) contains the richest population of spatially resolved massive O-type stars known so far. This unmatched sample offers an opportunity to test models describing their main-sequence evolution and mass-loss properties. Aims: Using ground-based optical spectroscopy obtained in the
      Ramírez-Agudelo, O. H. et al.

      Advertised on:

      4
      2017
      Citations
      73
    • A study of the effect of rotational mixing on massive stars evolution: surface abundances of Galactic O7-8 giant stars
      Context. Massive star evolution remains only partly constrained. In particular, the exact role of rotation has been questioned by puzzling properties of OB stars in the Magellanic Clouds. Aims: Our goal is to study the relation between surface chemical composition and rotational velocity, and to test predictions of evolutionary models including
      Martins, F. et al.

      Advertised on:

      2
      2017
      Citations
      20
    • The Gaia-ESO Survey: Calibration strategy
      The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and
      Pancino, E. et al.

      Advertised on:

      1
      2017
      Citations
      60
    • The deep OB star population in Carina from the VST Photometric Hα Survey (VPHAS+)
      Massive OB stars are critical to the ecology of galaxies and yet our knowledge of OB stars in the Milky Way, fainter than V ˜ 12, remains patchy. Data from the VST Photometric Hα Survey (VPHAS+) permit the construction of the first deep catalogues of blue excess-selected OB stars, without neglecting the stellar field. A total of 14 900 candidates
      Mohr-Smith, M. et al.

      Advertised on:

      2
      2017
      Citations
      31
    • The IACOB project . III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars
      Context. The term macroturbulent broadening is commonly used to refer to a certain type of non-rotational broadening affecting the spectral line profiles of O- and B-type stars. It has been proposed to be a spectroscopic signature of the presence of stellar oscillations; however, we still lack a definitive confirmation of this hypothesis. Aims: We
      Simón-Díaz, S. et al.

      Advertised on:

      1
      2017
      Citations
      112
    • The IACOB project. IV. New predictions for high-degree non-radial mode instability domains in massive stars and their connection with macroturbulent broadening
      Context. Asteroseismology is a powerful tool to access the internal structure of stars. Apart from the important impact of theoretical developments, progress in this field has been commonly associated with the analysis of time-resolved observations. Recently, the so-called macroturbulent broadening has been proposed as a complementary and less
      Godart, M. et al.

      Advertised on:

      1
      2017
      Citations
      22
    • B field in OB stars (BOB): The outstandingly strong magnetic field in the evolved He-strong star CPD -62° 2124
      The origin and evolution of magnetism in OB stars is far from being well understood. With approximately 70 magnetic OB stars known, any new object with unusual characteristics may turn out to be a key piece of the puzzle. We report the detection of an exceptionally strong magnetic field in the He-strong B2IV star CPD -62° 2124. Spectropolarimetric
      Castro, N. et al.

      Advertised on:

      1
      2017
      Citations
      25
    • Open cluster Dolidze 25: Stellar parameters and the metallicity in the Galactic anticentre
      Context. The young open cluster Dolidze 25, in the direction of the Galactic anticentre, has been attributed a very low metallicity, with typical abundances between -0.5 and -0.7 dex below solar. Aims: We intend to derive accurate cluster parameters and accurate stellar abundances for some of its members. Methods: We have obtained a large sample of
      Negueruela, I. et al.

      Advertised on:

      12
      2015
      Citations
      11
    • The little-studied cluster Berkeley 90. II. The foreground ISM
      Context. Nearly one century after their discovery, the carrier or carriers of diffuse interstellar bands (DIBs) is/are still unknown and there are few sightlines studied in detail for a large number of DIBs. Aims: We want to study the ISM sightlines toward LS III +46 11 and LS III +46 12, two early-O-type stellar systems, and LS III +46 11 B, a mid
      Maíz Apellániz, J. et al.

      Advertised on:

      11
      2015
      Citations
      15
    • B fields in OB stars (BOB). Detection of a strong magnetic field in the O9.7 V star HD 54879
      The number of magnetic stars detected among massive stars is small; nevertheless, the role played by the magnetic field in stellar evolution cannot be disregarded. Links between line profile variability, enhancements/depletions of surface chemical abundances, and magnetic fields have been identified for low-mass B-stars, but for the O-type domain
      Castro, N. et al.

      Advertised on:

      9
      2015
      Citations
      39
    • Observational Consequences of Turbulent Pressure in the Envelopes of Massive Stars
      The major mass fraction of the envelope of hot luminous stars is radiatively stable. However, the partial ionization of hydrogen, helium, and iron gives rise to extended sub-surface convection zones in all of them. In this work, we investigate the effect of the pressure induced by the turbulent motion in these zones based on the mixing-length
      Grassitelli, L. et al.

      Advertised on:

      7
      2015
      Citations
      48
    • The little-studied cluster Berkeley 90. I. LS III +46 11: a very massive O3.5 If* + O3.5 If* binary
      Context. It appears that most (if not all) massive stars are born in multiple systems. At the same time, the most massive binaries are hard to find owing to their low numbers throughout the Galaxy and the implied large distances and extinctions. Aims: We want to study LS III +46 11, identified in this paper as a very massive binary; another nearby
      Lorenzo, J. et al.

      Advertised on:

      7
      2015
      Citations
      21
    • Surface abundances of ON stars
      Context. Massive stars burn hydrogen through the CNO cycle during most of their evolution. When mixing is efficient or when mass transfer in binary systems occurs, chemically processed material is observed at the surface of O and B stars. Aims: ON stars show stronger lines of nitrogen than morphologically normal counterparts. Whether this
      Martins, F. et al.

      Advertised on:

      6
      2015
      Citations
      29
    • Orbital and Physical Properties of the σ Ori Aa, Ab, B Triple System
      We provide a complete characterization of the astrophysical properties of the σ Ori Aa, Ab, B hierarchical triple system and an improved set of orbital parameters for the highly eccentric σ Ori Aa, Ab spectroscopic binary. We compiled a spectroscopic data set comprising 90 high-resolution spectra covering a total time span of 1963 days. We applied
      Simón-Díaz, S. et al.

      Advertised on:

      2
      2015
      Citations
      44
    • B fields in OB stars (BOB): on the detection of weak magnetic fields in the two early B-type stars β CMa and ɛ CMa. Possible lack of a "magnetic desert" in massive stars
      Only a small fraction of massive stars seem to host a measurable structured magnetic field, whose origin is still unknown and whose implications for stellar evolution still need to be assessed. Within the context of the "B fields in OB stars (BOB)" collaboration, we used the HARPSpol spectropolarimeter to observe the early B-type stars β CMa (HD
      Fossati, L. et al.

      Advertised on:

      2
      2015
      Citations
      67
    • MY Camelopardalis, a very massive merger progenitor
      Context. The early-type binary MY Cam belongs to the young open cluster Alicante 1, embedded in Cam OB3. Aims: MY Cam consists of two early-O type main-sequence stars and shows a photometric modulation suggesting an orbital period slightly above one day. We intend to confirm this orbital period and derive orbital and stellar parameters. Methods
      Lorenzo, J. et al.

      Advertised on:

      12
      2014
      Citations
      15

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