Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies
We present a statistical method for measuring the average H I spin temperature in distant galaxies using the expected detection yields from future wide-field 21 cm absorption surveys. As a demonstrative case study, we consider an all-southern-sky simulated survey of 2-h per pointing with the Austral...
| Main Authors: | , , , |
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| Format: | Journal article |
| Language: | English |
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Oxford University Press
2016
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| _version_ | 1826279527758692352 |
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| author | Allison, J Zwaan, M Duchesne, S Curran, S |
| author_facet | Allison, J Zwaan, M Duchesne, S Curran, S |
| author_sort | Allison, J |
| collection | OXFORD |
| description | We present a statistical method for measuring the average H I spin temperature in distant galaxies using the expected detection yields from future wide-field 21 cm absorption surveys. As a demonstrative case study, we consider an all-southern-sky simulated survey of 2-h per pointing with the Australian Square Kilometre Array Pathfinder for intervening H I absorbers at intermediate cosmological redshifts between z = 0.4 and 1. For example, if such a survey yielded 1000 absorbers, we would infer a harmonic-mean spin temperature of T¯¯¯¯spin∼100 K for the population of damped Lyman α absorbers (DLAs) at these redshifts, indicating that more than 50 per cent of the neutral gas in these systems is in a cold neutral medium (CNM). Conversely, a lower yield of only 100 detections would imply T¯¯¯¯spin∼1000 K and a CNM fraction less than 10 per cent. We propose that this method can be used to provide independent verification of the spin temperature evolution reported in recent 21 cm surveys of known DLAs at high redshift and for measuring the spin temperature at intermediate redshifts below z ≈ 1.7, where the Lyman α line is inaccessible using ground-based observatories. Increasingly more sensitive and larger surveys with the Square Kilometre Array should provide stronger statistical constraints on the average spin temperature. However, these will ultimately be limited by the accuracy to which we can determine the H I column density frequency distribution, the covering factor and the redshift distribution of the background radio source population. |
| first_indexed | 2024-03-07T00:00:04Z |
| format | Journal article |
| id | oxford-uuid:75a0918f-bf83-45b9-910c-9886f8c04fd9 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T00:00:04Z |
| publishDate | 2016 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:75a0918f-bf83-45b9-910c-9886f8c04fd92022-03-26T20:10:33ZUsing 21 cm absorption surveys to measure the average H I spin temperature in distant galaxiesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:75a0918f-bf83-45b9-910c-9886f8c04fd9EnglishSymplectic Elements at OxfordOxford University Press2016Allison, JZwaan, MDuchesne, SCurran, SWe present a statistical method for measuring the average H I spin temperature in distant galaxies using the expected detection yields from future wide-field 21 cm absorption surveys. As a demonstrative case study, we consider an all-southern-sky simulated survey of 2-h per pointing with the Australian Square Kilometre Array Pathfinder for intervening H I absorbers at intermediate cosmological redshifts between z = 0.4 and 1. For example, if such a survey yielded 1000 absorbers, we would infer a harmonic-mean spin temperature of T¯¯¯¯spin∼100 K for the population of damped Lyman α absorbers (DLAs) at these redshifts, indicating that more than 50 per cent of the neutral gas in these systems is in a cold neutral medium (CNM). Conversely, a lower yield of only 100 detections would imply T¯¯¯¯spin∼1000 K and a CNM fraction less than 10 per cent. We propose that this method can be used to provide independent verification of the spin temperature evolution reported in recent 21 cm surveys of known DLAs at high redshift and for measuring the spin temperature at intermediate redshifts below z ≈ 1.7, where the Lyman α line is inaccessible using ground-based observatories. Increasingly more sensitive and larger surveys with the Square Kilometre Array should provide stronger statistical constraints on the average spin temperature. However, these will ultimately be limited by the accuracy to which we can determine the H I column density frequency distribution, the covering factor and the redshift distribution of the background radio source population. |
| spellingShingle | Allison, J Zwaan, M Duchesne, S Curran, S Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title | Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title_full | Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title_fullStr | Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title_full_unstemmed | Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title_short | Using 21 cm absorption surveys to measure the average H I spin temperature in distant galaxies |
| title_sort | using 21 cm absorption surveys to measure the average h i spin temperature in distant galaxies |
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