Measuring the baryonic Tully-Fisher relation below the detection threshold
We present a novel 2D flux density model for observed H i emission lines combined with a Bayesian stacking technique to measure the baryonic Tully-Fisher relation below the nominal detection threshold. We simulate a galaxy catalogue, which includes H i lines described with either Gaussian or busy fu...
| Main Authors: | , , , , , , |
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| 格式: | Journal article |
| 语言: | English |
| 出版: |
Oxford University Press
2021
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| _version_ | 1826308111022948352 |
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| author | Pan, H Jarvis, MJ Ponomareva, AA Santos, MG Allison, JR Maddox, N Frank, BS |
| author_facet | Pan, H Jarvis, MJ Ponomareva, AA Santos, MG Allison, JR Maddox, N Frank, BS |
| author_sort | Pan, H |
| collection | OXFORD |
| description | We present a novel 2D flux density model for observed H i emission lines combined with a Bayesian stacking technique to measure the baryonic Tully-Fisher relation below the nominal detection threshold. We simulate a galaxy catalogue, which includes H i lines described with either Gaussian or busy function profiles, and H i data cubes with a range of noise and survey areas similar to the MeerKAT International Giga-Hertz Tiered Extragalactic Exploration (MIGHTEE) survey. With prior knowledge of redshifts, stellar masses, and inclinations of spiral galaxies, we find that our model can reconstruct the input baryonic Tully-Fisher parameters (slope and zero-point) most accurately in a relatively broad redshift range from the local Universe to z = 0.3 for all the considered levels of noise and survey areas and up to z = 0.55 for a nominal noise of 90 μJy/channel over 5 deg2. Our model can also determine the MHI - M∗ relation for spiral galaxies beyond the local Universe and account for the detailed shape of the H I emission line, which is crucial for understanding the dynamics of spiral galaxies. Thus, we have developed a Bayesian stacking technique for measuring the baryonic Tully-Fisher relation for galaxies at low stellar and/or H I masses and/or those at high redshift, where the direct detection of H I requires prohibitive exposure times. |
| first_indexed | 2024-03-07T07:13:07Z |
| format | Journal article |
| id | oxford-uuid:f91772f7-594f-4832-a912-1f34f00f836a |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T07:13:07Z |
| publishDate | 2021 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:f91772f7-594f-4832-a912-1f34f00f836a2022-07-12T12:23:44ZMeasuring the baryonic Tully-Fisher relation below the detection thresholdJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:f91772f7-594f-4832-a912-1f34f00f836aEnglishSymplectic ElementsOxford University Press2021Pan, HJarvis, MJPonomareva, AASantos, MGAllison, JRMaddox, NFrank, BSWe present a novel 2D flux density model for observed H i emission lines combined with a Bayesian stacking technique to measure the baryonic Tully-Fisher relation below the nominal detection threshold. We simulate a galaxy catalogue, which includes H i lines described with either Gaussian or busy function profiles, and H i data cubes with a range of noise and survey areas similar to the MeerKAT International Giga-Hertz Tiered Extragalactic Exploration (MIGHTEE) survey. With prior knowledge of redshifts, stellar masses, and inclinations of spiral galaxies, we find that our model can reconstruct the input baryonic Tully-Fisher parameters (slope and zero-point) most accurately in a relatively broad redshift range from the local Universe to z = 0.3 for all the considered levels of noise and survey areas and up to z = 0.55 for a nominal noise of 90 μJy/channel over 5 deg2. Our model can also determine the MHI - M∗ relation for spiral galaxies beyond the local Universe and account for the detailed shape of the H I emission line, which is crucial for understanding the dynamics of spiral galaxies. Thus, we have developed a Bayesian stacking technique for measuring the baryonic Tully-Fisher relation for galaxies at low stellar and/or H I masses and/or those at high redshift, where the direct detection of H I requires prohibitive exposure times. |
| spellingShingle | Pan, H Jarvis, MJ Ponomareva, AA Santos, MG Allison, JR Maddox, N Frank, BS Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title | Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title_full | Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title_fullStr | Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title_full_unstemmed | Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title_short | Measuring the baryonic Tully-Fisher relation below the detection threshold |
| title_sort | measuring the baryonic tully fisher relation below the detection threshold |
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