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Exploring 3D data of Dwarf Galaxies

Published online by Cambridge University Press:  30 October 2019

Katarzyna Bensch Open the ORCID record for Katarzyna Bensch [Opens in a new window] ,
Christina Thöne Open the ORCID record for Christina Thöne [Opens in a new window] ,
Antonio de Ugarte Postigo Open the ORCID record for Antonio de Ugarte Postigo [Opens in a new window] ,
Luca Izzo  and
David Alexander Kann
Katarzyna Bensch
Affiliation:
Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008, Granada, Spain email: kasia@iaa.es
Christina Thöne
Affiliation:
Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008, Granada, Spain email: kasia@iaa.es
Antonio de Ugarte Postigo
Affiliation:
Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008, Granada, Spain email: kasia@iaa.es
Luca Izzo
Affiliation:
Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008, Granada, Spain email: kasia@iaa.es
David Alexander Kann
Affiliation:
Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008, Granada, Spain email: kasia@iaa.es
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Abstract

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Dwarf irregular galaxies are places of ongoing star-formation in the low-redshift Universe. Low metallicity dwarfs were originally thought to be the youngest galaxies in the local Universe, however, there is now evidence that they consist of matter which has previously undergone evolution and is enriched by star-formation. Here we present a sample of seven nearby metal-poor dwarf galaxies with a young stellar populations selected from the SDSS which we study using integral field unit (IFU) data from the VIMOS instrument, covering the spectral range between the He II 4686 line and the [SII] 6718/6733 Å doublet. We present property maps across the galaxies and compare different galaxies and different HII regions within the same galaxy. We find that the properties within one galaxy are not uniform and they also differ between different galaxies concerning star-formation, kinematics and metallicity and morphology. The observed differences across individual galaxies together with disturbed kinematics and morphologies can be interpreted as possible signs of recent interactions and/or mergers. Additionally, we present a comparison of different metallicity calibrations and search for systematic differences obtained using different methods.

Keywords

Dwarf galaxiesStar-formationEvolutionIFU
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 359 - 362
Copyright
© International Astronomical Union 2019 

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