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DTSTART;TZID=Atlantic/Canary:20230905T103000
DTEND;TZID=Atlantic/Canary:20230905T113000
UID:iactalks-1710
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1710
CREATED:2023-09-05T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Tracing the Chemical Evolution of Metals in local Star-Forming Gala
 xies: aperture effects and abundance patterns
DESCRIPTION:Tracing the Chemical Evolution of Metals in local Star-Forming 
 Galaxies: aperture effects and abundance patterns\nDr. Karla Z. Arellano-C
 ordova\n\nNebular  emission lines are a powerful diagnostic tool for traci
 ng the chemical  evolution in star-forming galaxies (SFGs) across cosmic t
 ime. Due  to their proximity, SGFs are ideal for studying the physical  pr
 operties, stellar population, and nebular gas in much more detail. The  CO
 S Legacy Spectroscopy SurveY (CLASSY) is a treasury survey that  comprises
  UV+optical spectra of 45 local SFGs covering a  broad range of physical p
 roperties. In this talk, I present the results  of the physical conditions
  and metallicities for the CLASSY sample  focused on the impact of the ape
 rture effects of the inferred  metallicities and the abundance patterns of
  several elements.  We found that the results for the inferred electron de
 nsity,  temperature, and metallicity derived using different aperture size
 s,  1″-3″, are consistent, indicating a uniform mapping of the
  nebular gas.  We also showed that the physical properties derived from  t
 he optical are appropriate for observations in the far-UV, allowing a  bet
 ter interpretation of the interplay between the stellar and gas  component
 s. I will also discuss the results of the Ne/O, Cl/O, S/O, and  Ar/O vs. O
 /H relations and their behaviour with  different galaxy properties (e.g., 
 stellar mass and star formation  rate). We found that such abundance ratio
 s follow a constant trend with  O/H as expected, except for Ne/O and Ar/O,
  which show a significant  trend at high metallicities. We discuss the sca
 tter  involved in the N/O versus O/H relation and its connection with the 
  different UV+optical observables. Finally, we compare these results with 
  the chemical abundances derived at z > 6 galaxies observed with the  J
 WST.
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