| Common Name: | PKS 0925-203 | VLBA 2cm Image | | VLBA 1.4 GHz: |
| B1950 Name: | 0925-203 |  |
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| J2000 Name: | J0927-2034 | ||
| R.A. and Dec. (J2000): | 9h27m51.824s -20d34'51.233" |
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| AGN Class: | LSP Quasar | ||
| Redshift: | 0.348 (Eracleous and Halpern 1994, ApJS 90, 1) | Luminosity Distance: | 1833 Mpc ; 4.89 pc/mas |
| Radio Spectrum: | Flat | ||
| Gamma-ray Association | LAT: Y, EGRET: N, TeV: N | ||
| Kpc-scale morphology: | Core | ||
| Jet Speed: | Maximum: Unknown ; Median: Unknown ; |
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| Separation Versus Time Plot: | Not available | ||
| Stacked epoch 15 GHz VLBA
images: Uniform weight: Not Available Natural weight: Not Available Circular Beam : Not Available Tapered Beam: Not Available Rotation Measure Map: | Not available | Spectral Index Map: | Not available | |
VLBA 23 GHz: |
Kpc-scale: Healey et al. 2007, ApJS 171, 61 | |
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| Fermi LAT and 15 GHz VLBA Light Curves |
VLBA 43 GHz: Cheng et al. 2020 |
Multiepoch Radio Spectrum: |
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| Comments: | new MOJAVE 1.5JyQC source | ||
If you use these data in a publication, we ask that you please contact us so we can add a link to the list of external MOJAVE publications, and ask that you cite Lister et al., 2018, ApJS, 234, 12 and include the following acknowledgment: "This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2018)"
Important Note: The MOJAVE team, working with the OVRO 40m AGN monitoring group, discovered a systematic error in the flux densities of all VLBA 15 GHz observations taking place after a date that lies between 2019 April 16 and 2019 May 16. Observations after that date have correlated flux densities that are between 10% and 20% too low. We have adjusted the flux density scaling of the MOJAVE VLBA data up to 2022 Jan 3 based on near-simultaneous OVRO 40m measurements at 15 GHz.
Asterisked entries below denote epochs that have not yet been corrected for the VLBA flux density scaling problem.
Important Note: The MOJAVE team, working with the OVRO 40m AGN monitoring group, discovered a systematic error in the flux densities of all VLBA 15 GHz observations taking place after a date that lies between 2019 April 16 and 2019 May 16. Observations after that date have correlated flux densities that are between 10% and 20% too low. We have adjusted the flux density scaling of the MOJAVE VLBA data up to 2022 Jan 3 based on near-simultaneous OVRO 40m measurements at 15 GHz.
Asterisked entries below denote epochs that have not yet been corrected for the VLBA flux density scaling problem.
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