0000000000040598

AUTHOR

Sofia Feltzing

showing 3 related works from this author

The Gaia-ESO Survey: The origin and evolution of s-process elements

2018

Context. Several works have found an increase of the abundances of the s-process neutron-capture elements in the youngest Galactic stellar populations. These trends provide important constraints on stellar and Galactic evolution and they need to be confirmed with large and statistically significant samples of stars spanning wide age and distance intervals. Aims. We aim to trace the abundance patterns and the time evolution of five s-process elements - two belonging to the first peak, Y and Zr, and three belonging to the second peak, Ba, La, and Ce - using the Gaia-ESO IDR5 results for open clusters and disc stars. Methods. From the UVES spectra of cluster member stars, we determined the ave…

astro-ph.GAMetallicityFOS: Physical sciencesContext (language use)AstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysics01 natural sciencesGalaxy: diskAstronomi astrofysik och kosmologiAbundance (ecology)QB4600103 physical sciencesAstronomy Astrophysics and CosmologyAstrophysics::Solar and Stellar AstrophysicsDisc010303 astronomy & astrophysicsComputingMilieux_MISCELLANEOUSAstrophysics::Galaxy AstrophysicsPhysicsgeneral [Open clusters and associations][SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]010308 nuclear & particles physicsStar formationAstronomy and AstrophysicsOpen clusters and associations: generalAstrophysics - Astrophysics of GalaxiesStarsAbundances [Galaxy][SDU]Sciences of the Universe [physics]13. Climate actionSpace and Planetary ScienceAstrophysics of Galaxies (astro-ph.GA)Galaxy: abundancesAstrophysics::Earth and Planetary AstrophysicsDisk [Galaxy]s-processOpen cluster
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Gaia -ESO Survey: Analysis of pre-main sequence stellar spectra

2015

This paper describes the analysis of UVES and GIRAFFE spectra acquired by the Gaia-ESO Public Spectroscopic Survey in the fields of young clusters whose population includes pre-main sequence (PMS) stars. Both methods that have been extensively used in the past and new ones developed in the contest of the Gaia-ESO survey enterprise are available and used. The internal precision of these quantities is estimated by inter-comparing the results obtained by such different methods, while the accuracy is estimated by comparison with independent external data, like effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. Specific strategi…

Accuracy and precisionPopulationFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysicsstars: pre-main sequenceSurveysfundamental parameters [Stars]Astronomical spectroscopysurveysAngular diameterpre-main sequence [Stars]Astrophysics::Solar and Stellar AstrophysicsSurveydata analysis [Methods]educationSolar and Stellar Astrophysics (astro-ph.SR)Astrophysics::Galaxy AstrophysicsAstronomía y AstrofísicaPhysicseducation.field_of_studygeneral [Open clusters and associations][SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]Astronomy and AstrophysicsStars: fundamental parameterAstronomy and AstrophysicEffective temperatureopen clusters and associations: generalSurface gravitymethods: data analysisAccretion (astrophysics)StarsAstrophysics - Solar and Stellar AstrophysicsMethods: data analysis; Open clusters and associations: general; Stars: fundamental parameters; Stars: pre-main sequence; Surveys; Astronomy and Astrophysics; Space and Planetary ScienceSpace and Planetary Science[SDU]Sciences of the Universe [physics]open clusters and associations: general; surveys ; methods: data analysisAstrophysics::Earth and Planetary Astrophysicsstars: fundamental parametersMethods: data analysi
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GRB 030227: The first multiwavelength afterglow of an INTEGRAL GRB

2003

We present multiwavelength observations of a gamma-ray burst detected by INTEGRAL (GRB 030227) between 5.3 hours and ~1.7 days after the event. Here we report the discovery of a dim optical afterglow (OA) that would not have been detected by many previous searches due to its faintess (R~23). This OA was seen to decline following a power law decay with index Alpha_R= -0.95 +/- 0.16. The spectral index Beta_opt/NIR yielded -1.25 +/- 0.14. These values may be explained by a relativistic expansion of a fireball (with p = 2.0) in the cooling regime. We also find evidence for inverse Compton scattering in X-rays.

PhysicsSpectral indexBurstsAstrophysics (astro-ph)Gamma raysCompton scatteringbursts [gamma rays]FOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsGamma rays ; Bursts ; Photometric ; Cosmology observationsPhotometricUNESCO::ASTRONOMÍA Y ASTROFÍSICAAstrophysicsCosmology observationsPower law:ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO]observations [cosmology]Afterglowphotometric [techniques]Space and Planetary ScienceAstronomy Astrophysics and CosmologyUNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogoniaGamma-ray burst:ASTRONOMÍA Y ASTROFÍSICA [UNESCO]
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