Optical Spectropolarimetric Variability Properties in Blazars PKS 0637-75 and PKS 1510-089
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| Format: | Preprint |
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2024
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| _version_ | 1866911932419670016 |
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| author | Podjed, Stephanie A. Hickox, Ryan C. Isler, Jedidah C. Böttcher, Markus Schutte, Hester M. |
| author_facet | Podjed, Stephanie A. Hickox, Ryan C. Isler, Jedidah C. Böttcher, Markus Schutte, Hester M. |
| contents | Spectropolarimetry is a powerful tool to investigate the central regions of active galactic nuclei (AGNs) as polarization signatures are key to probing magnetic field structure, evolution, and the physics of particle acceleration in jets. Optical linear polarization of blazars is typically greater than a few percent, indicating the emission is dominated by nonthermal synchrotron radiation, while polarization less than a few percent is common for other type 1 AGNs. We present a spectropolarimetric study of PKS 0637-75 and PKS 1510-089 to determine how the head-on orientation of a jet and dominant emission processes influence polarimetric variations in the broad lines and continuum. Observations were obtained biweekly from the Robert Stobie Spectrograph on the Southern African Large Telescope. Variability in the continuum polarization is detected for both PKS 0637-75 and PKS 1510-089, with a total average level of 2.5% +/- 0.1% and 7.5% +/- 0.1%, respectively. There is no clear polarization in the broad Balmer emission lines and weak polarization in Mg II as the average level across all observations is 0.2% +/- 0.1% for Hbeta, 0.2% +/- 0.3% for Hgamma, and 0.6% +/- 0.2% for Mg II. We find that polarization measurements confirm the conclusions drawn from spectral energy distribution modeling of the disk-jet contributions to the emission as optical polarization and time variability for PKS 0637-75 are shown to be dominated by accretion disk emission while those of PKS 1510-089 are due to both disk and jet emission, with greater jet contribution during flaring states. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2406_17687 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Optical Spectropolarimetric Variability Properties in Blazars PKS 0637-75 and PKS 1510-089 Podjed, Stephanie A. Hickox, Ryan C. Isler, Jedidah C. Böttcher, Markus Schutte, Hester M. Astrophysics of Galaxies High Energy Astrophysical Phenomena Spectropolarimetry is a powerful tool to investigate the central regions of active galactic nuclei (AGNs) as polarization signatures are key to probing magnetic field structure, evolution, and the physics of particle acceleration in jets. Optical linear polarization of blazars is typically greater than a few percent, indicating the emission is dominated by nonthermal synchrotron radiation, while polarization less than a few percent is common for other type 1 AGNs. We present a spectropolarimetric study of PKS 0637-75 and PKS 1510-089 to determine how the head-on orientation of a jet and dominant emission processes influence polarimetric variations in the broad lines and continuum. Observations were obtained biweekly from the Robert Stobie Spectrograph on the Southern African Large Telescope. Variability in the continuum polarization is detected for both PKS 0637-75 and PKS 1510-089, with a total average level of 2.5% +/- 0.1% and 7.5% +/- 0.1%, respectively. There is no clear polarization in the broad Balmer emission lines and weak polarization in Mg II as the average level across all observations is 0.2% +/- 0.1% for Hbeta, 0.2% +/- 0.3% for Hgamma, and 0.6% +/- 0.2% for Mg II. We find that polarization measurements confirm the conclusions drawn from spectral energy distribution modeling of the disk-jet contributions to the emission as optical polarization and time variability for PKS 0637-75 are shown to be dominated by accretion disk emission while those of PKS 1510-089 are due to both disk and jet emission, with greater jet contribution during flaring states. |
| title | Optical Spectropolarimetric Variability Properties in Blazars PKS 0637-75 and PKS 1510-089 |
| topic | Astrophysics of Galaxies High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2406.17687 |