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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20201015T103000
DTEND;TZID=Atlantic/Canary:20201015T113000
UID:iactalks-1420
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1420
CREATED:2020-10-15T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:The abundance gradients in the Milky Way: tracing the chemical comp
 osition of the ISM using H II regions
DESCRIPTION:The abundance gradients in the Milky Way: tracing the chemical 
 composition of the ISM using H II regions\nDr. Karla Arellano\n\nThe emiss
 ion line spectrum of H II regions provides information about the chemical 
 composition of the present-day interstellar medium. The study as a functio
 n of their galactocentric distances helps to constrain chemical evolution 
 models.  In this talk, I present a reanalysis of the abundance g
 radients of C, N, O, Ne, S, Cl, and Ar for a sample of 33 Galactic H 
 II regions covering a range in Galactocentric Distances fro
 m 6-17 kpc. New values of the Galactocentric distances were calc
 ulated using Gaia DR2 parallaxes for some objects. We study
  in detail the different ICF schemes to improve the results of t
 he total abundances in Galactic H II regions. We found that the 
 re-evaluation of the distances using Gaia DR2 parallaxes produces an O gra
 dient that discards a flattening of the gradient in the inn
 er part of the Galaxy. The radial distribution of Ne/O, S/O
 , Cl/O and Ar/O are almost flat confirming a lockstep evolution of those e
 lements respect to O. Our Galaxy also shows an almost flat N/O gradient&nb
 sp;respect to other nearby spiral galaxies. We compare our results wi
 th those from B type stars and cepheids, young planetary nebulae and 
 those slopes using optical and infrared data for H II regions.
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