| Common Name: | GB6 J2024+1718 | MOJAVE 15 GHz [Total intensity movie] | [Polariz. movie] | VLBA 1.4 GHz: |
| B1950 Name: | 2022+171 |  |
 |
| J2000 Name: | J2024+1718 | ||
| R.A. and Dec. (J2000): | 20h24m56.563s +17d18'13.198" |
||
| AGN Class: | LSP Quasar | ||
| Redshift: | 1.05 (1996ESOSR..17....1V) | Luminosity Distance: | 7052 Mpc ; 8.14 pc/mas |
| Radio Spectrum: | Flat | ||
| Gamma-ray Association | LAT: N, EGRET: N, TeV: N | ||
| Kpc-scale morphology: | Core | ||
| Jet Speed: | Maximum: 32 ± 31 μas/y ; 1.8 ± 1.7 c Median: N/A ; based on 1 moving feature Lister et al. 2021, ApJ,923,30 |
||
| Separation Versus Time Plot: | PNG PS | ||
| Stacked epoch 15 GHz VLBA
images: Uniform weight: [PDF] [GIF] Natural weight: [PDF] [GIF] Circular Beam : [PDF] [GIF] Tapered Beam: [PDF] [GIF] Rotation Measure Map: | Not available | Spectral Index Map: | Not available | |
VLBA 23 GHz: |
Kpc-scale: Healey et al. 2007, ApJS 171, 61 | |
|
|
||
| Fermi LAT and 15 GHz VLBA Light Curves |
VLBA 43 GHz: |
Multiepoch Radio Spectrum: |
|
|---|---|---|---|
|
 |
||
| Comments: | Non-GPS due to variability, robopol control sample | ||
![[GIF]](../stackedimages/2022+171.u.stacked.icu.gif){kind=link}
![[GIF]](../stackedimages/2022+171.u.stacked.icd.gif){kind=link}
![[GIF]](../stackedimages/2022+171.u.stacked.icc.gif){kind=link}
![[GIF]](../stackedimages/2022+171.u.stacked.ict.gif){kind=link}
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.
| Epoch (Y-M-D) | VLBA Code | VLBA I (mJy) |
VLBA P (mJy) |
VLBA P (%) |
VLBA EVPA (deg.) |
I Image (Nat. Weight) | Tapered I Image | Tapered I Image (Widefield) | Visibility Data |
Stokes I Radplot | Pol. Image |
2020-05-25 | BL229BE | 894 | 5.6 | 0.6 | 28 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS | 2019-01-19 | BL229AU | 806 | 11 | 1.4 | 107 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS | 2018-05-31 | BL229AO | 901 | 8.3 | 0.9 | 98 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS | 2017-07-30 | BL229AJ | 823 | 2.7 | 0.3 | 101 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS | 2017-03-11 | BL229AF | 740 | 9.8 | 1.3 | 77 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS | 2017-01-03 | BL229AD | 760 | 8.5 | 1.1 | 79 | FITS PNG PS | FITS PNG PS | PNG PS | uvf | PNG PS | PNG PS |
| Home | Science | AGN Samples | Data Archive | Status | Publications | Movies | RM Maps | α Maps | People | Outreach |