Repository logo
 

Star formation as a function of environment in the MeerKAT Galaxy Clusters Legacy Survey=Ulwazibunkanyezi Njengethuluzi Lokuhlola isiqoqzinkanyezi iMeerKAT Galaxy Clusters Legacy.

Simple item page
dc.contributor.advisorHilton, Matthew James.
dc.contributor.advisorKnowles, Kenda Leigh.
dc.contributor.authorKesebonye, Kabelo Calvin.
dc.date.accessioned2023-09-01T13:30:55Z
dc.date.available2023-09-01T13:30:55Z
dc.date.created2023
dc.date.issued2023
dc.descriptionDoctoral Degree. University of KwaZulu-Natal, Durban.en_US
dc.description.abstractProbing the star formation (SF) activity of cluster galaxies paves an important path towards the understanding of cluster evolution. This thesis presents the study of star formation rates (SFR) in clusters using dustunbiased radio luminosities from the MeerKAT Galaxy Clusters Legacy Survey (MGCLS). Our radio data is complemented by optical data from the Dark Energy Camera Legacy Survey (DECaLS), for photometric redshifts, and also Sunyaev-Zel’dovich (SZ) effect-derived cluster masses from the Atacama Cosmology Telescope (ACT). We present the first statistical study of SFR in clusters using MeerKAT-detected galaxies which takes advantage of MeerKAT’s large field of view to investigate the relation between SF activity and cluster environments out to 2R200. Using radio diffuse emission in the form of haloes and relics as a proxy for cluster merger activity, we divide our cluster sample between disturbed/merger clusters and relaxed clusters. We observe a higher fraction of star-forming galaxies (fSF) in disturbed clusters than in relaxed clusters. Disturbed clusters also have higher masses (M200) and total SFR (ΣSFR) in contrast to relaxed clusters. On analysing the redshift evolution of the massnormalised ΣSFR, we observe a ≈ 4× decline in the SF activity of clusters from the redshift of 0.35 to 0.15, corresponding to ≈ 2 Gyr in look-back time. Our result is roughly consistent with the one from cluster studies that used infrared-derived SFR (≈ 5× decline) at a similar redshift slice as our sample. We use a subsample of double relic-hosting clusters to investigate the relation between cluster SF activity and the time that has passed since the merger started (tmerger) estimated from the relic distances from cluster cores. We observe an anti-correlation between ΣSFR and merger, suggesting that younger mergers have a higher SF activity. However, we see no clear correlation in the mass-normalised ΣSFR with tmerger. We also investigate for differences in the SF activity of galaxies closer to radio relics and those away from the relics and observe no significant differences between the two populations. Iqoqa Ukuhlola kokusebenza kolwazi-bunkanyezi ( star formation -SF) kwesixhobo sezinkanyezi cluster galaxies kucabe indlela emqoka ukuqonda kokukhula kwalamaqoqo (cluster evolution). Lolu cwaningo lwethula ukuhlolwa lwe star (formation rates -SFR) kuma-clusters kusetshenziswa i dust-unbiased radio luminosities kuMeerKAT Galaxy Clusters Legacy Survey (MGCLS). Imininingo ye-radio isebenzisana ne-optical data yeDark Energy Camera Legacy Survey (DECaLS), ukuhlola iphotometric redshifts, ne Sunyaev-Zel'dovich (SZ) nomthelela odalwa yicluster masses esuka kwiAtacama Cosmology Telescope (ACT). Kube sekwethulwa ucwaningo lokuqala lwezibalo lweSFR in clusters kusetshenziswa iMeerKAT-detected galaxies. Kusetshenziswe ithuba lobukhulu bomkhakha lokubonakala kahle kweMeerKAT ukuhlola ubudlelwane phakathi kwe-SFR nemvelo yamaclusters ezinhlobonhlobo zedynamical states. Kusetshenziswe iradio diffuse emission eyizinhlobo zehaloes nerelics njengegunya lokuhlola ukuhlangana kwamacluster , amasampula ama-cluster ahlukaniswe phakathi kwamadisturbed/merger clusters namarelaxed clusters. Okutholakele ukuthi ihigher fraction of star-forming galaxies (fSF) kumaclusters aphazamisekile (disturbed clusters) kunama clusters akhululekile (relaxed clusters). Amaclusters aphazamisekile anama masi aphezulu (M200) kanti isamba sonke siwuSFR (∑SFR) uma eqhathaniswa namaclusters aphazamisekile . Sekucutshungulwa iredshift evolution yemass-normalised ∑SFR, kutholakale ukuthi aphindwe kawu ≅4 times decline ekusebenzeni kwe SF esukela kwiredshift of 0.35 to 0.15, ahlobana ne ≅2 Gyr kwi look-back time. Imiphumela ilinganiselwe ngokuhambisana nezifundo zamacluster kusetshenziswa i-infrared-derived SFR (≅5 times decline) ngokufanayo neredshift slice njengamasampula ocwaningo lolu .Kusetshenziswe elinye isampula esigabeni sesibili ukuze kwenziwe idouble relic-hosting clusters ukuhlola ubudlelwane okusebenza kwama clusters (SF activity) kanye nesikhathi esisuke sidlulile ehlanganiswe (t_merger) kulinganiselwe kusukela ebangeni lerelic distances kucluster ewumsuka (cluster cores). Kutholakale ukungadlelani phakathi kwe ∑SFR ne t_merger, okuchaza ukuthi ukuhlanganiswa kwalawo asemancane kusebenzisa izinga eliphezulu (SF activity). Yize-kunjalo , akubonakali ubudlelwane obucacile kumass-normalised ∑SFR ne t_merger. Kuphinde kwahlolwa ukusebenza okungefani kumagalaxies asondelene neradio relics nalawo aqhelile kumarelics kwase kwangatholakala mehluko otheni kule miphakathi yomibili. en_US
dc.identifier.doihttps://doi.org/10.29086/10413/22200
dc.identifier.urihttps://researchspace.ukzn.ac.za/handle/10413/22200
dc.language.isoenen_US
dc.subject.otherStars--Galaxy clusters.en_US
dc.subject.otherStars--Formation.en_US
dc.subject.otherDark energy.en_US
dc.subject.otherMeerKAT.en_US
dc.subject.otherGalaxies.en_US
dc.titleStar formation as a function of environment in the MeerKAT Galaxy Clusters Legacy Survey=Ulwazibunkanyezi Njengethuluzi Lokuhlola isiqoqzinkanyezi iMeerKAT Galaxy Clusters Legacy.en_US
dc.typeThesisen_US
local.sdgSDG9

Files

Original bundle
Now showing 1 - 1 of 1
Thumbnail Image
Name:
KabeloKesebonye_FinalThesis.pdf
Size:
10.72 MB
Format:
Adobe Portable Document Format
Description:
Kesebonye_Kabelo_Calvin_2023
Download
License bundle
Now showing 1 - 1 of 1
No Thumbnail Available
Name:
license.txt
Size:
1.64 KB
Format:
Item-specific license agreed upon to submission
Description:
Download

Collections

Doctoral Degrees (Applied Mathematics)