Early Enrichment Population Theory at High Redshift
An early enrichment population (EEP) has been theorized to produce the observed intracluster medium (ICM) metallicity of galaxy clusters. This population likely existed at high redshifts ( z ∼ 10), relics of which we posit exist today as dwarf galaxies. Previous work has argued that the initial mas...
Saved in:
| Main Authors: | , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad9826 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1841525322351116288 |
|---|---|
| author | Anne E. Blackwell Joel N. Bregman |
| author_facet | Anne E. Blackwell Joel N. Bregman |
| author_sort | Anne E. Blackwell |
| collection | DOAJ |
| description | An early enrichment population (EEP) has been theorized to produce the observed intracluster medium (ICM) metallicity of galaxy clusters. This population likely existed at high redshifts ( z ∼ 10), relics of which we posit exist today as dwarf galaxies. Previous work has argued that the initial mass function (IMF) of the EEP must be flatter than those found at lower redshifts, but with considerable uncertainties. In this work, we present a more quantitative model for the EEP and demonstrate how observational constraints can be applied to the IMF using supernova Type Ia (SN Ia) rates, delay time distributions (DTDs), and the luminosity functions (LFs) of galaxy clusters. We determine best-fit values for the slope and mass break of the IMF by comparing IMFs from literature with observed DTDs and the low-luminosity component ( M ( R ) > −12) of the Coma LF. We derive two best-fit IMFs, flatter than standard IMFs: (1) α _lo = −0.13 ± 0.24 for 0.07 < M / M _⊙ < 1.75 and α _hi = 0.53 ± 0.01 for 1.75 < M / M _⊙ < 150; and (2) α _lo = 1.06 ± 0.11 for 0.07 < M / M _⊙ < 6 and α _hi = 0.53 ± 0.01 for 6 < M / M _⊙ < 150. We compare these with sl-5 from M. Loewenstein (2013), with α = 0.5 for 0.07 < M / M _⊙ < 8 and α = 0.3 for 8 < M / M _⊙ < 150. This EEP model, along with stars formed at later times, can produce the observed ICM metallicity, is consistent with observations, and predicts a significant rise in the SN Ia rate at increasing redshift. |
| format | Article |
| id | doaj-art-bd75bc8786c84186b7bc736dd1f54231 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-bd75bc8786c84186b7bc736dd1f542312025-01-17T15:59:24ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197917410.3847/1538-4357/ad9826Early Enrichment Population Theory at High RedshiftAnne E. Blackwell0https://orcid.org/0000-0002-8195-0563Joel N. Bregman1https://orcid.org/0000-0001-6276-9526University of Michigan , Ann Arbor, MI 48104, USAUniversity of Michigan , Ann Arbor, MI 48104, USAAn early enrichment population (EEP) has been theorized to produce the observed intracluster medium (ICM) metallicity of galaxy clusters. This population likely existed at high redshifts ( z ∼ 10), relics of which we posit exist today as dwarf galaxies. Previous work has argued that the initial mass function (IMF) of the EEP must be flatter than those found at lower redshifts, but with considerable uncertainties. In this work, we present a more quantitative model for the EEP and demonstrate how observational constraints can be applied to the IMF using supernova Type Ia (SN Ia) rates, delay time distributions (DTDs), and the luminosity functions (LFs) of galaxy clusters. We determine best-fit values for the slope and mass break of the IMF by comparing IMFs from literature with observed DTDs and the low-luminosity component ( M ( R ) > −12) of the Coma LF. We derive two best-fit IMFs, flatter than standard IMFs: (1) α _lo = −0.13 ± 0.24 for 0.07 < M / M _⊙ < 1.75 and α _hi = 0.53 ± 0.01 for 1.75 < M / M _⊙ < 150; and (2) α _lo = 1.06 ± 0.11 for 0.07 < M / M _⊙ < 6 and α _hi = 0.53 ± 0.01 for 6 < M / M _⊙ < 150. We compare these with sl-5 from M. Loewenstein (2013), with α = 0.5 for 0.07 < M / M _⊙ < 8 and α = 0.3 for 8 < M / M _⊙ < 150. This EEP model, along with stars formed at later times, can produce the observed ICM metallicity, is consistent with observations, and predicts a significant rise in the SN Ia rate at increasing redshift.https://doi.org/10.3847/1538-4357/ad9826Galaxy clustersSupernovaeInitial mass functionLuminosity functionIntracluster mediumMetallicity |
| spellingShingle | Anne E. Blackwell Joel N. Bregman Early Enrichment Population Theory at High Redshift The Astrophysical Journal Galaxy clusters Supernovae Initial mass function Luminosity function Intracluster medium Metallicity |
| title | Early Enrichment Population Theory at High Redshift |
| title_full | Early Enrichment Population Theory at High Redshift |
| title_fullStr | Early Enrichment Population Theory at High Redshift |
| title_full_unstemmed | Early Enrichment Population Theory at High Redshift |
| title_short | Early Enrichment Population Theory at High Redshift |
| title_sort | early enrichment population theory at high redshift |
| topic | Galaxy clusters Supernovae Initial mass function Luminosity function Intracluster medium Metallicity |
| url | https://doi.org/10.3847/1538-4357/ad9826 |
| work_keys_str_mv | AT anneeblackwell earlyenrichmentpopulationtheoryathighredshift AT joelnbregman earlyenrichmentpopulationtheoryathighredshift |