The fast radio burst dispersion measure distribution
We compare the dispersion measure (DM) statistics of FRBs detected by the ASKAP and Parkes radio telescopes. We jointly model their DM distributions, exploiting the fact that the telescopes have different survey fluence limits but likely sample the same underlying population. After accounting for th...
| Main Authors: | , , , , |
|---|---|
| Format: | Journal Article |
| Language: | English |
| Published: |
OXFORD UNIV PRESS
2021
|
| Subjects: | |
| Online Access: | http://purl.org/au-research/grants/arc/DP180100857 http://hdl.handle.net/20.500.11937/91557 |
| _version_ | 1848765546989879296 |
|---|---|
| author | Arcus, W.R. Macquart, Jean-Pierre Sammons, M.W. James, Clancy Ekers, Ronald |
| author_facet | Arcus, W.R. Macquart, Jean-Pierre Sammons, M.W. James, Clancy Ekers, Ronald |
| author_sort | Arcus, W.R. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We compare the dispersion measure (DM) statistics of FRBs detected by the ASKAP and Parkes radio telescopes. We jointly model their DM distributions, exploiting the fact that the telescopes have different survey fluence limits but likely sample the same underlying population. After accounting for the effects of instrumental temporal and spectral resolution of each sample, we find that a fit between the modelled and observed DM distribution, using identical population parameters, provides a good fit to both distributions. Assuming a one-to-one mapping between DM and redshift for an homogeneous intergalactic medium (IGM), we determine the best-fitting parameters of the population spectral index, $\hat{\alpha }$, and the power-law index of the burst energy distribution, $\hat{\gamma }$, for different redshift evolutionary models. Whilst the overall best-fitting model yields $\hat{\alpha }=2.2_{-1.0}^{+0.7}$ and $\hat{\gamma }=2.0_{-0.1}^{+0.3}$, for a strong redshift evolutionary model, when we admit the further constraint of α = 1.5 we favour the best fit $\hat{\gamma }=1.5 \pm 0.2$ and the case of no redshift evolution. Moreover, we find no evidence that the FRB population evolves faster than linearly with respect to the star formation rate over the DM (redshift) range for the sampled population. |
| first_indexed | 2025-11-14T11:36:59Z |
| format | Journal Article |
| id | curtin-20.500.11937-91557 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| language | English |
| last_indexed | 2025-11-14T11:36:59Z |
| publishDate | 2021 |
| publisher | OXFORD UNIV PRESS |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-915572023-05-11T03:52:50Z The fast radio burst dispersion measure distribution Arcus, W.R. Macquart, Jean-Pierre Sammons, M.W. James, Clancy Ekers, Ronald Science & Technology Physical Sciences Astronomy & Astrophysics methods: data analysis surveys cosmology: miscellaneous astro-ph.CO astro-ph.CO astro-ph.HE We compare the dispersion measure (DM) statistics of FRBs detected by the ASKAP and Parkes radio telescopes. We jointly model their DM distributions, exploiting the fact that the telescopes have different survey fluence limits but likely sample the same underlying population. After accounting for the effects of instrumental temporal and spectral resolution of each sample, we find that a fit between the modelled and observed DM distribution, using identical population parameters, provides a good fit to both distributions. Assuming a one-to-one mapping between DM and redshift for an homogeneous intergalactic medium (IGM), we determine the best-fitting parameters of the population spectral index, $\hat{\alpha }$, and the power-law index of the burst energy distribution, $\hat{\gamma }$, for different redshift evolutionary models. Whilst the overall best-fitting model yields $\hat{\alpha }=2.2_{-1.0}^{+0.7}$ and $\hat{\gamma }=2.0_{-0.1}^{+0.3}$, for a strong redshift evolutionary model, when we admit the further constraint of α = 1.5 we favour the best fit $\hat{\gamma }=1.5 \pm 0.2$ and the case of no redshift evolution. Moreover, we find no evidence that the FRB population evolves faster than linearly with respect to the star formation rate over the DM (redshift) range for the sampled population. 2021 Journal Article http://hdl.handle.net/20.500.11937/91557 10.1093/mnras/staa3948 English http://purl.org/au-research/grants/arc/DP180100857 OXFORD UNIV PRESS fulltext |
| spellingShingle | Science & Technology Physical Sciences Astronomy & Astrophysics methods: data analysis surveys cosmology: miscellaneous astro-ph.CO astro-ph.CO astro-ph.HE Arcus, W.R. Macquart, Jean-Pierre Sammons, M.W. James, Clancy Ekers, Ronald The fast radio burst dispersion measure distribution |
| title | The fast radio burst dispersion measure distribution |
| title_full | The fast radio burst dispersion measure distribution |
| title_fullStr | The fast radio burst dispersion measure distribution |
| title_full_unstemmed | The fast radio burst dispersion measure distribution |
| title_short | The fast radio burst dispersion measure distribution |
| title_sort | fast radio burst dispersion measure distribution |
| topic | Science & Technology Physical Sciences Astronomy & Astrophysics methods: data analysis surveys cosmology: miscellaneous astro-ph.CO astro-ph.CO astro-ph.HE |
| url | http://purl.org/au-research/grants/arc/DP180100857 http://hdl.handle.net/20.500.11937/91557 |