MOJAVE Sample: 0027+056

Common Name:	PKS 0027+056	MOJAVE 15 GHz [Total intensity movie] \| [Polariz. movie]	VLBA 1.4 GHz:
B1950 Name:	0027+056
J2000 Name:	J0029+0554
R.A. and Dec. (J2000):	0h29m45.896s +5d54'40.712"
AGN Class:	LSP Quasar
Redshift:	1.317 (Schneider et al. 1999, AJ 117, 40)
Luminosity Distance:	9360 Mpc ; 8.45 pc/mas
Radio Spectrum:	Flat
Gamma-ray Association	LAT: N, EGRET: N, TeV: N
Kpc-scale morphology:	One-sided
Jet Speed:	Maximum: 23 ± 6 μas/y ; 1.45 ± 0.38 c Median: N/A ; based on 3 moving features Lister et al. 2019, ApJ,874,43
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] Pushkarev et al. 2017 : FITS Rotation Measure Map: \| Not available \| Spectral Index Map: \| Not available \|		VLBA 23 GHz:	Kpc-scale: Browne et al., 1998, MNRAS 293, 257

Fermi LAT and 15 GHz VLBA Light Curves		VLBA 43 GHz:	Multiepoch Radio Spectrum:
Fermi LAT and 15 GHz VLBA Light Curves
Comments:	Was a possible revised EGRET catalog (2008) association (YYK); LAMOST DR4 z = 0.58 likely incorrect

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.

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
2020-07-02	BL229BG	498	16	3.2	60	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2019-08-27	BL229BB	454	10	2.3	58	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2011-07-24	BL149DN	506	12	2.3	141	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2010-10-25	BL149CT	488	9.0	1.8	127	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2010-06-19	BL149CK	538	13	2.4	138	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2009-08-19	BL149BR	634	9.2	1.5	125	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS
2009-05-28	BL149BL	650	19	2.9	124	FITS PNG PS	FITS PNG PS	PNG PS	uvf	PNG PS	PNG PS