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Luminous and dark matter density profiles in the inner regions of a group-scale lens at z = 0.6

Published online by Cambridge University Press:  04 June 2020

Mônica Tergolina Open the ORCID record for Mônica Tergolina [Opens in a new window] ,
Cristina Furlanetto  and
Marina Trevisan
Mônica Tergolina
Affiliation:
Universidade Federal do Rio Grande do Sul, Instituto de Física Av. Bento Gonçalves, 9500, 91501-970, Porto Alegre, Brazil email: [email protected]
Cristina Furlanetto
Affiliation:
Universidade Federal do Rio Grande do Sul, Instituto de Física Av. Bento Gonçalves, 9500, 91501-970, Porto Alegre, Brazil email: [email protected]
Marina Trevisan
Affiliation:
Universidade Federal do Rio Grande do Sul, Instituto de Física Av. Bento Gonçalves, 9500, 91501-970, Porto Alegre, Brazil email: [email protected]
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Abstract

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Density profiles of galaxy groups can provide an insight on how large-scale structure in the Universe formed and evolved, since galaxy groups bridge the gap between individual galaxies and galaxy clusters. Studying the galaxy group that is gravitational lensing HELMS18, a submillimeter galaxy at z = 2.39 from the Herschel’s HerMES Large Mode Survey (HELMS), we aim to probe the total density profile by combining strong gravitational lensing with kinematics of the centrally-located galaxies and kinematics of the group members. We have high-resolution data of HELMS18 obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) and multi-object spectroscopic data of the group members from Gemini-GMOS. Our main goal is to match these observations to probe the DM and stellar density profiles and to establish a complete description of this galaxy group.

Keywords

gravitational lensing: stronggalaxies: groupsgalaxies: generalgalaxies: high-redshift
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 295 - 296
Copyright
© International Astronomical Union 2020

References

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