S. Simón‐Díaz

Instituto de Astrofísica de Canarias

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i-10 index

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Document Type

Co-Authors

A. Herrero

Universidad de La Laguna

164

J. Maíz Apellániz

Centro de Astrobiología

118

C. J. Evans

Space Telescope Science Institute

H. Sana

KU Leuven

N. Castro

Leibniz Institute for Astrophysics Potsdam

D. J. Lennon

Instituto de Astrofísica de Canarias

N. Langer

University of Bonn

J. S. Vink

Armagh Observatory & Planetarium

A. de Koter

University of Amsterdam

W. D. Taylor

UK Astronomy Technology Centre

Cooperative Institutions

Centre National de la Recherche Scientifique

180

Max Planck Society

144

Instituto de Astrofísica de Canarias

129

European Southern Observatory

103

Universidad de La Laguna

Université Paris Cité

Max Planck Institute for Astronomy

Osservatorio Astronomico di Padova

Consejo Superior de Investigaciones Científicas

National Institute for Astrophysics

Author Statistics

Papers

Citation

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Quantitative spectroscopic analyses in the IACOB+OWN project: Massive O-type stars in the Galaxy with the current Gaia information

Proceedings of the International Astronomical Union (2016)

G. Holgado S. Simón‐Díaz R. H. Barbá

We present the results from the quantitative spectroscopic analysis of ~280 likely single O stars targeted by the IACOB and OWN surveys. This implies the largest sample of Galactic O-type stars analyzed homogeneously to date. We used the iacob-broad and iacob-gbat tools (see Simón-Díaz et al. 2011,2015) to obtain the complete set of spectroscopic parameters which can be determined from the optical spectrum of O-type stars: projected rotational velocity ( v sin i ), macroturbulence velocity ( v mac ), effective temperature ( T eff ), gravity (log g ), wind-strength (log Q ), helium abundance ( Y He ), microturbulence (ξ t ), and the exponent of the wind-law (β).

Microturbulence

Effective temperature

Exponent

Star (game theory)

10.1017/s1743921317001120

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Citations (1)

OB and Oe/Be v sin i distributions in the SMC

AAS (2019)

Kevin Paggeot N. Castro M. Oey S. Simón‐Díaz J. Dorigo Jones

Source

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Citations (0)

MONOS: Multiplicity Of Northern O-type Spectroscopic systems

Astronomy and Astrophysics (2019)

J. Maíz Apellániz E. Páez I. Negueruela R. H. Barbá S. Simón‐Díaz

[ABRIDGED] AIMS. MONOS is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 1st paper we describe the sample and provide spectral classifications and additional information for objects with previous SB or EB orbits. In the future we will test the validity of previous solutions and calculate new SB orbits. METHODS.The spectra in this paper have 2 sources: GOSSS, which is obtaining blue-violet R~2500 spectroscopy of thousands of massive stars, and LiLiMaRlin, a library of libraries of high-resolution spectroscopy of massive stars obtained from 4 different surveys and additional data from our own observing programs and public archives. We also use lucky images from AstraLux. RESULTS. We present homogeneous spectral classifications for 92 O-type spectroscopic multiple systems and 10 optical companions. We discuss the visual multiplicity of each system with the support of AstraLux images and additional sources. For 11 O-type objects and for 6 B-type objects we present their first GOSSS spectral classifications. For 2 known EBs we detect SB2/SB1 lines for the first time, to which we add a third system already reported by us recently. For 2 previous SB1 systems we detect their SB2 nature for the first time and give their first separate spectral classifications, something we also do for a 3rd object just recently identified as a SB2. We also detect 9 new astrometric companions and provide updated information on several others. For sigma Ori AaAbB we provide spectral classifications for the 3 components with a single observation for the first time thanks to a lucky spectroscopy observation obtained close to the Aa,Ab periastron and for theta^1 Ori CaCb we add it to the class of Galactic Of?p stars, raising the number of its members to 6. Our sample of O-type spectroscopic binaries contains more triple/higher-order systems than double systems.

Multiplicity (mathematics)

10.1051/0004-6361/201935359

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Citations (49)

VizieR Online Data Catalog: VFTS. OVz stars in 30 Dor (Sabin-Sanjulian+, 2014)

yCat (2014)

C. Sabín-Sanjulián S. Simón‐Díaz A. Herrero N. R. Walborn J. Puls

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Citations (0)

Near-infrared study of the stellar population of Sh2-152

Astronomy and Astrophysics (2011)

S. Ramírez Alegría A. Herrero A. Marín-Franch E. Puga F. Najarro

Context: The discovery of new massive star clusters and massive stellar populations in previously known clusters in our Galaxy by means of infrared studies has changed our view of the Milky Way from an inactive to an active star-forming machine. Within this scenario, we present a near-infrared spectrophotometric study of the stellar content of the compact H II region Sh2-152. Aims: We aim to determine the distance, extinction, age, and mass of Sh2-152, using for the first time near-infrared stellar classification for several sources in the region. Methods: Using our near-infrared (J, H, and Ks) photometry and the colour-magnitude diagram for the cluster field, we selected 13 bright stars, candidate members of the reddened cluster's main sequence, for H- and K- spectroscopy and spectral classification. This near-infrared information was complemented with an optical spectrum of the ionizing central star to confirm its spectral nature. Results: From the 13 spectroscopically observed stars, 5 were classified as B-type, 3 as G-type, 2 were young stellar objects (YSOs), and 3 remained unclassified (because of the poor data quality). The cluster's extinction varies from A_{Ks}=0.5 to 2.6 magnitudes (A_V=4.5 to 24 magnitudes) and the distance is estimated to be 3.21\pm0.21 kpc. The age of the cluster is younger than 9.4 Myr and the lower limit to the total mass of the cluster is (2.45\pm0.79)\cdot10^3 M_{Sun}. We compare the number of ionizing photons emitted from the OB-type stars with the Lyman continuum photons derived from the radio observations and conclude that both quantities are consistent for the central region of Sh2-152. In contrast, the main ionizing source of the lower region remains unidentified.

Stellar population

Star (game theory)

10.1051/0004-6361/201016427

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Citations (11)

Multiwavelength study of the fast rotating supergiant high-mass X-ray binary IGR J16465-4507

HAL (Le Centre pour la Communication Scientifique Directe) (2016)

S. Chaty A. Lereun I. Neguerela A. Coleiro N. Castro

Source

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Citations (1)

Characterization of massive blue stars in NGC 55

N. Castro A. Herrero M. A. Urbaneja M. García S. Simón‐Díaz

Characterization

Source

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Citations (0)

Astrophysical parameters and orbital solution of the peculiar X-ray transient IGR J00370+6122

Astronomy and Astrophysics (2014)

A. Gónzalez-Galán I. Negueruela N. Castro S. Simón‐Díaz J. Lorenzo

BD+6073 is the optical counterpart of the X-ray source IGR J00370+6122, a probable accretion-powered X-ray pulsar. The X-ray light curve of this binary system shows clear periodicity at 15.7 d, which has been interpreted as repeated outbursts around the periastron of an eccentric orbit. We obtained high-resolution spectra of BD+6073 at different epochs. We used the FASTWind code to generate a stellar atmosphere model to fit the observed spectrum and obtain physical magnitudes. The synthetic spectrum was used as a template for cross-correlation with the observed spectra to measure radial velocities. The radial velocity curve provided an orbital solution for the system. We have also analysed the RXTE/ASM and Swift/BAT light curves to confirm the stability of the periodicity. BD +6073 is a BN0.7 Ib low-luminosity supergiant located at an approximate distance of 3.1 kpc, in the CasOB4 association. We derive Teff=24000 K and log gc=3.0, and chemical abundances consistent with a moderately high level of evolution. The spectroscopic and evolutionary masses are consistent at the 1 sigma level with a mass of 15 solar masses. The recurrence time of the X-ray flares is the orbital period of the system. The NS is in a high eccentricity (e=0.56) orbit, and the X-ray emission is strongly peaked around orbital phase 0.2, though the observations are consistent with some level of X-ray activity happening at all orbital phases. The X-ray behaviour of IGR J00370+6122 is reminiscent of intermediate SFXTs, though its peak luminosity is rather low. The orbit is somewhat wider than those of classical persistent supergiant X-ray binaries, which, combined with the low luminosity of the mass donor, explains the low X-ray luminosity. IGR J00370+6122 will likely evolve towards a persistent supergiant system, highlighting the evolutionary connection between different classes of wind-accreting X-ray sources.

Orbit (dynamics)

Orbital elements

Transient (computer programming)

Orbital period

X-ray pulsar

10.1051/0004-6361/201423554

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Citations (15)

A Definitive Test of Rotational Mixing in Massive Stars

HST Proposal (2016)

Charles Proffitt I. Brott Kátia Cunha P. L. Dufton N. Langer

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A spectroscopic analysis of the Trapezium Cluster stars

Symposium - International Astronomical Union (2003)

S. Simón‐Díaz A. Herrero C. Esteban

We consider the Orion Nebula (M 42) within a project aimed at studying the interaction between massive stars and their surrounding ISM. This is an H ii region ionized by θ 1 Ori C, one of the four massive stars in the Trapezium Cluster. θ 1 Ori C has the earliest spectral type (O7Vp) among them, emitting an ionizing flux several orders of magnitude larger than those of the other stars. We present a spectral analysis of the Trapezium Cluster stars to determine their stellar parameters. We use spectra between 4250 – 4750 Å and compare them with synthetic spectra obtained by means of an updated version of fastwind that includes an approximated treatment of metal-line blanketing.

Blanketing

Orion Nebula

10.1017/s007418090021334x

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Citations (1)