MIGHTEE-H I: the H I size–mass relation over the last billion years
We present the observed H I size–mass relation of 204 galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in H I mass, ranging from dwarf galaxies to massive spirals, and including all morphologica...
| Main Authors: | , , , , , , , , , , , , , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
Oxford University Press
2022
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| _version_ | 1797107318411755520 |
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| author | Rajohnson, SHA Frank, BS Ponomareva, AA Maddox, N Kraan-Korteweg, RC Jarvis, MJ Adams, EAK Oosterloo, T Baes, M Spekkens, K Adams, NJ Glowacki, M Kurapati, S Prandoni, I Heywood, I Collier, JD Sekhar, S Taylor, R |
| author_facet | Rajohnson, SHA Frank, BS Ponomareva, AA Maddox, N Kraan-Korteweg, RC Jarvis, MJ Adams, EAK Oosterloo, T Baes, M Spekkens, K Adams, NJ Glowacki, M Kurapati, S Prandoni, I Heywood, I Collier, JD Sekhar, S Taylor, R |
| author_sort | Rajohnson, SHA |
| collection | OXFORD |
| description | We present the observed H I size–mass relation of 204 galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in H I mass, ranging from dwarf galaxies to massive spirals, and including all morphological types. This is the first time the relation has been explored on a blind homogeneous data set that extends over a previously unexplored redshift range of 0 < z < 0.084, i.e. a period of around one billion years in cosmic time. The sample follows the same tight logarithmic relation derived from previous work, between the diameter (DHI) and the mass (MHI) of H I discs. We measure a slope of 0.501 ± 0.008, an intercept of −3.252+0.073−0.074, and an observed scatter of 0.057 dex. For the first time, we quantify the intrinsic scatter of 0.054 ± 0.003 dex (∼10 per cent), which provides a constraint for cosmological simulations of galaxy formation and evolution. We derive the relation as a function of galaxy type and find that their intrinsic scatters and slopes are consistent within the errors. We also calculate the DHI−MHI relation for two redshift bins and do not find any evidence for evolution with redshift. These results suggest that over a period of one billion years in look-back time, galaxy discs have not undergone significant evolution in their gas distribution and mean surface mass density, indicating a lack of dependence on both morphological type and redshift. |
| first_indexed | 2024-03-07T07:12:53Z |
| format | Journal article |
| id | oxford-uuid:cbd3430b-58b2-4666-9f18-877bde4dc9c3 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T07:12:53Z |
| publishDate | 2022 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:cbd3430b-58b2-4666-9f18-877bde4dc9c32022-07-11T16:31:53ZMIGHTEE-H I: the H I size–mass relation over the last billion yearsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:cbd3430b-58b2-4666-9f18-877bde4dc9c3EnglishSymplectic ElementsOxford University Press2022Rajohnson, SHAFrank, BSPonomareva, AAMaddox, NKraan-Korteweg, RCJarvis, MJAdams, EAKOosterloo, TBaes, MSpekkens, KAdams, NJGlowacki, MKurapati, SPrandoni, IHeywood, ICollier, JDSekhar, STaylor, RWe present the observed H I size–mass relation of 204 galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in H I mass, ranging from dwarf galaxies to massive spirals, and including all morphological types. This is the first time the relation has been explored on a blind homogeneous data set that extends over a previously unexplored redshift range of 0 < z < 0.084, i.e. a period of around one billion years in cosmic time. The sample follows the same tight logarithmic relation derived from previous work, between the diameter (DHI) and the mass (MHI) of H I discs. We measure a slope of 0.501 ± 0.008, an intercept of −3.252+0.073−0.074, and an observed scatter of 0.057 dex. For the first time, we quantify the intrinsic scatter of 0.054 ± 0.003 dex (∼10 per cent), which provides a constraint for cosmological simulations of galaxy formation and evolution. We derive the relation as a function of galaxy type and find that their intrinsic scatters and slopes are consistent within the errors. We also calculate the DHI−MHI relation for two redshift bins and do not find any evidence for evolution with redshift. These results suggest that over a period of one billion years in look-back time, galaxy discs have not undergone significant evolution in their gas distribution and mean surface mass density, indicating a lack of dependence on both morphological type and redshift. |
| spellingShingle | Rajohnson, SHA Frank, BS Ponomareva, AA Maddox, N Kraan-Korteweg, RC Jarvis, MJ Adams, EAK Oosterloo, T Baes, M Spekkens, K Adams, NJ Glowacki, M Kurapati, S Prandoni, I Heywood, I Collier, JD Sekhar, S Taylor, R MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title | MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title_full | MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title_fullStr | MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title_full_unstemmed | MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title_short | MIGHTEE-H I: the H I size–mass relation over the last billion years |
| title_sort | mightee h i the h i size mass relation over the last billion years |
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