Predicting the Number of Radio Sources Seen by Both VLASS and LSST
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| Format: | Preprint |
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2024
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| _version_ | 1866917781443706880 |
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| author | Tellez, Alex Gordon, Yjan Bechtol, Keith |
| author_facet | Tellez, Alex Gordon, Yjan Bechtol, Keith |
| contents | Radio surveys typically sample extragalactic sources in higher redshift regimes than is typical for optical surveys, resulting in many radio sources not having a detected optical counterpart. Over the next decade the Legacy Survey of Space and Time (LSST) will be performing the deepest ($i < 26.4\,$mag) wide-area optical survey to date increasing the fraction of radio sources for which we have optical data. In this Research Note we use the Hyper Suprime-Cam survey to analyse how the fraction of radio sources in the Very Large Array Sky Survey (VLASS) with optical detections varies as a function of $i$-band magnitude and extrapolate to predict the number of optical counterparts we expect LSST to detect. Assuming a final VLASS point source depth of $S_{3\,\text{GHz}}\lesssim350\,μ$Jy, we expect LSST to identify optical counterparts to $\sim 10^6$ radio sources in VLASS. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_13850 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Predicting the Number of Radio Sources Seen by Both VLASS and LSST Tellez, Alex Gordon, Yjan Bechtol, Keith Astrophysics of Galaxies Instrumentation and Methods for Astrophysics Radio surveys typically sample extragalactic sources in higher redshift regimes than is typical for optical surveys, resulting in many radio sources not having a detected optical counterpart. Over the next decade the Legacy Survey of Space and Time (LSST) will be performing the deepest ($i < 26.4\,$mag) wide-area optical survey to date increasing the fraction of radio sources for which we have optical data. In this Research Note we use the Hyper Suprime-Cam survey to analyse how the fraction of radio sources in the Very Large Array Sky Survey (VLASS) with optical detections varies as a function of $i$-band magnitude and extrapolate to predict the number of optical counterparts we expect LSST to detect. Assuming a final VLASS point source depth of $S_{3\,\text{GHz}}\lesssim350\,μ$Jy, we expect LSST to identify optical counterparts to $\sim 10^6$ radio sources in VLASS. |
| title | Predicting the Number of Radio Sources Seen by Both VLASS and LSST |
| topic | Astrophysics of Galaxies Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2409.13850 |