0048-071|OB -082   |Our 43GHz image shows a single-sided jet to the northwest, in the opposite direction of the kiloparsec-scale lobe (P. Kharb+ 2020, in preparation) -- http://www.physics.purdue.edu/astro/MOJAVE/sourcepages/0048-071.shtml
0106+013|4C +01.02 |Our image shows that the innermost jet structure (<1mas) is along the east-west direction (in a position angle ~-110{deg}), then it bends toward the southwest (~-140{deg}) at about 2mas from the core. This is in agreement with the low-frequency VLBI images (Lister+ 2009AJ....138.1874L).
0113-118|          |This source is very compact at 43GHz, we only detect a core and a faint extension within 1mas. However, it was not detected on space-ground baselines in the 5GHz VSOP AGN Survey (Dodson+ 2008ApJS..175..314D).
0119+041|OC +033   |The brightness temperature of the core is 1.6x10^10^K at 43GHz, the derived Doppler factor is below unity which is consistent with the slow jet motion found in the literature (Lister+ 2009AJ....138.1874L; Piner+ 2012ApJ...758...84P). Neither the Compton Gamma Ray Observatory Energetic Gamma Ray Experiment Telescope nor Fermi/LAT has detected this source. The 15GHz light curve from the Owens Valley Radio Observatory (OVRO) 40m radio telescope shows that the flux density does not have significant variation from 2008 to mid-2017 (Richards+ 2011ApJS..194...29R). The VLBI structure (the core and the eastern jet component) does not show noticeable change (Lister+ 2009AJ....138.1874L; Piner+ 2012ApJ...758...84P). The overall radio spectrum peaks at about 7GHz. All these pieces of evidence imply that this is a GPS source, rather than a blazar.
0122-003|UM 321    |Our image shows a compact core and three jet components along a straight line to the west. It is in good agreement with the 5 and 15GHz VLBA images (Fomalont+ 2000ApJS..131...95F; Lister+ 2013AJ....146..120L).
0130-171|OC -150   |The compact core is 0.08mas in size. We detected a series of jet components extending to the southwest.
0149+218|          |This source shows a compact structure at 43GHz. A relatively weak component extending to the north is detected.
0202-172|          |The jet shows a centrally symmetric S-shaped morphology within 5mas. An extended feature is located at ~2mas from the core, sitting in the gap between the inner jet and the outer 3mas jet.
0208+106|          |The jet points southeast up to 1mas from the core, then it bends toward northeast as seen in the 15GHz VLBA image obtained in the Monitoring Of Jets in Active galactic nuclei with VLBA Experiments (MOJAVE) survey (Lister+ 2009AJ....138.1874L), with a 70{deg} change in position angle. The outer (>1mas) bent jet is diffuse at 43GHz.
0221+067|4C +06.11 |The source shows a compact core-jet structure within 1mas. Our high dynamic range image detected two weaker jet components to the west.
0224+671|4C +67.05 |The core is 0.13mas in size. A jet component to the north is detected and has the similar flux density with the core at 43GHz.
0229+131|4C +13.14 |The source displays considerable emission on both sides of the core at arcsec scales (Punsly 1995AJ....109.1555P). Our image shows a bright core and an inner jet pointing to the northeast, which is consistent with the high-resolution 5GHz VSOP image (Dodson+ 2008ApJS..175..314D).
0239+108|OD +166   |The source shows a compact core-jet structure. According to the total flux density light curve from the 15GHz OVRO monitoring program (Richards+ 2011ApJS..194...29R), our 43GHz observation was made in a fading phase of the source.
0241+622|          |This is a low-redshift (z=0.045) Seyfert 1.2 galaxy (Veron-Cetty & Veron 2006A&A...455..773V). The eastern jet component is consistent with the 15GHz VLBA image (Lister+ 2009AJ....138.1874L). However, there is another component appearing on the opposite (western) side of the core with an intensity in excess of 7{sigma} image noise, indicating a reliable detection. A detailed study of this component would require future high-resolution and high-sensitivity VLBI observations.
0306+102|OE +110   |The source is very compact in lower-frequency VLBI images. A faint radio emission is detected in the northeast.
0309+411|NRAO 128  |This is a strongly core-dominated broad-line radio galaxy showing core and double lobe morphology (de Bruyn 1989A&A...226L..13D; Marcha+ 1996MNRAS.281..425M). Our 43GHz VLBA image reveals a prominent core and a straight jet extending to 1mas, aligning with the brighter and advancing kiloparsec-scale jet.
0354+559|          |The source shows a complex jet in low-frequency VLBI images (Fomalont+ 2003AJ....126.2562F). In our 43GHz image, the jet points to the northwest and then bends to the southwest within 1mas. The source has rich structure even at a milliarcsecond and probably a submilliarcsecond scale, calling for a detailed study.
0400+258|CTD 026   |The core size is 0.21mas. The jet extends to the southeast up to about 2mas; this is also seen by Dodson+ (2008ApJS..175..314D). Further out, the jet becomes diffuse and bends to the northeast, as seen only at larger scales with lower-frequency VLBI imaging (e.g., Fomalont+ 2000ApJS..131...95F; Lister+ 2009AJ....138.1874L).
0403-132|OF -105   |Our 43GHz VLBA image shows a very compact core and faint jet emission extending to the southeast. Cooper+ 2007ApJS..171..376C detected an unresolved core and radio emission to the southwest. The VLBI data at 2.3 and 15GHz exhibit a bright core and jet emission extending to the southern direction (Fomalont+ 2000ApJS..131...95F; Lister+ 2009AJ....138.1874L).
0405-123|OF -109   |This source is the second Seyfert 1.2 galaxy in our sample (Veron-Cetty & Veron 2006A&A...455..773V). The VLA image shows two hot spots in the north-south direction, and only the one in the northern lobe was detected in X-rays and optical (Sambruna+ 2004ApJ...608..698S). The lower-frequency VLBI images show a core-jet structure extending ~30mas to the north. Our image shows a resolved structure within 2mas, with the south component corresponding to the core.
0507+179|          |de Vries+ (2000A&AS..143..181D) identified it as a BL Lac object. The core brightness temperature is the maximum in our sample.
0529+075|OG 050    |Our image shows the inner jet extending to the northwest within 3mas. However, the kiloparsec-scale structure is pointing to the opposite direction (Cooper+ 2007ApJS..171..376C).
0605-085|OC -010   |The most important concern for this source is the core identification, considering that our observation took place during a flare (Richards+ 2011ApJS..194...29R). Two components along the east-west direction have equal brightness. Referring to the 15GHz VLBA image (Lister+ 2009AJ....138.1874L), we assume that the most compact and upstream component, i.e., the western component, is the core, even if it is not the brightest one. Further high-frequency VLBI observations are needed to confirm this.
0648-165|          |The source shows a large jet bending from the northwest as indicated by our image to the west-southwest which can be better seen in lower-frequency VLBI images (Lister+ 2009AJ....138.1874L; Pushkarev & Kovalev 2012A&A...544A..34P)
0657+172|          |The jet direction of the source at parsec-scale in our image (west-northwest) is different from that seen in low-frequency (2.3 and 8.6GHz) VLBI images (Pushkarev & Kovalev 2012A&A...544A..34P). Based also on radio spectrum data (from NED), we suggest that this source is a GPS or high-frequency peaker (HFP) candidate.
0723-008|          |Our image shows a jet pointing to the northeast at ~35{deg} position angle, in good agreement with the 15GHz VLBA image (Lister+ 2009AJ....138.1874L).
0736+017|OI +061   |We only detect a compact core and a new weak jet component to the northeast at a distance of 0.41mas.
0738+313|OI +363   |This is a GPS quasar (Stanghellini+ 1998A&AS..131..303S). Our 43GHz VLBA image shows a core-jet structure, consistently with the 15GHz image (Stanghellini+ 2001A&A...377..377S). Although the position of the radio core in this AGN is uncertain, we assumed the most compact feature at the base of the jet to be the core. A more extended component appears at 3.5mas south of the core.
0742+103|OI +171   |This is a high-redshift (z=2.624) GPS quasar (Stanghellini+ 1998A&AS..131..303S) which shows a large jet bending. We detect a bright component and two diffuse inner jet components in the northwest within 3mas at 43GHz. Further out, the jet bends to the northeast in the 15GHz VLBA image (Lister+ 2009AJ....138.1874L). The 1.4GHz (from unpublished data observed in the project BG196 (PI: D. Gabuzda) -- http://astrogeo.org/) and 2.3GHz (Pushkarev & Kovalev 2012A&A...544A..34P) VLBA images show the jet bending from northeast to southeast. Although the position of the radio core in this GPS source is uncertain, we assumed the most compact feature at the base of the jet as the core. The coherent jet bending from northwest (inner ~2mas) to northeast (inner 4mas), to east (12mas), then to southeast (~200mas) suggests a 180{deg} curved trajectory.
0743-006|OI -072   |This is a GPS quasar (Stanghellini+ 1998A&AS..131..303S). Although the core position is uncertain, we assumed the most compact feature at the base of the jet as the core.
0838+133|3C 207    |This is a powerful Fanaroff-Riley II (FR II) radio galaxy (Laing+ 1983MNRAS.204..151L). The 1.4 and 8.4GHz VLA images show a fairly symmetric triple structure (Bogers+ 1994A&AS..105...91B). Our 43GHz VLBA image shows a bright core and a one-sided extended jet toward the east. This is in good agreement with what was found previously at 1.4 and 15GHz (Lister+ 2009AJ....138.1874L).
0859-140|OJ -199   |The source shows a compact core and two lobes aligned in the north-south direction at 408MHz (Bondi+ 1996A&A...308..415B). Our image shows a faint and smoothly curved jet to the south-southeast within 2mas, which is in good agreement with the previous 15GHz VLBA image (Kellermann+ 1998AJ....115.1295K).
0906+015|4C +01.24 |The VLA image at 1.6GHz shows a compact core and a bright component 12" east of the core on a kiloparsec scale (Murphy+ 1993MNRAS.264..298M). The 2.3, 8.6, and 15GHz VLBI images show a jet toward the northeast from 5 to 30mas (Fey & Charlot 2000ApJS..128...17F; Lister+ 2009AJ....138.1874L). There are three jet components detected toward the northeast within 2mas in our 43GHz image.
0945+408|4C +40.24 |The large-scale structure of this source is resolved into a very compact core with a one-sided jet extending over 4" (~18kpc) in the northeast direction using the VLA at 5GHz and the Multi-Element Radio-Linked Interferometer Network at 408 and 1666MHz (Reid+ 1995A&AS..110..213R). The inner jet structure extends to the southeast in our image, which appears to have a 90{deg} misalignment with respect to the large-scale structure.
1036+054|          |The 1.4GHz VLA image shows a bright core and extended jet emission structure in the northeast-southwest direction until ~18" (Kharb+ 2010ApJ...710..764K). The 1.4GHz VLBA image detected a one-sided jet pointing to the northeast over ~150mas. The position of the 15GHz core (Lister+ 2009AJ....138.1874L) coincides with the southernmost component in our image. The brightening jet component might be associated with the major outburst in late 2014 seen in the OVRO 40m light curve (Richards+ 2011ApJS..194...29R). Taking into account the jet proper motion of 0.22mas/yr (Lister+ 2009AJ....138.1874L) and the time interval between the outburst and our VLBA observation (2015 October 10), the flare-generated shock should have moved about 0.4mas downstream, roughly consistently with the bright jet component seen in our 43GHz image.
1045-188|OL -176   |The 1.4GHz VLA image shows a bright core and extended jet emission structure in the northwest-southeast direction until ~14" (Kharb+ 2010ApJ...710..764K). The 1.4GHz VLBA image shows a one-sided jet pointing to the northeast over ~55mas. The typical beam size at 15GHz in the MOJAVE survey is 1.5masx0.5mas (Lister+ 2009AJ....138.1874L). In our new 43GHz image, we detected two components within the area of the 15GHz beam. We assumed the most compact and northernmost component as the core. Our J1 component corresponds to the bright 15GHz core. More high-frequency VLBI observations are needed to clarify this.
1124-186|OM -148   |Fey+ (2015AJ....150...58F) only detect a compact core at 2.3 and 8.6GHz. We detect a core and an extended faint emission feature to the south, in agreement with the 15GHz image (Lister+ 2009AJ....138.1874L).
1150+497|4C +49.22 |The 1.5GHz VLA image shows a complex triple source with a halo in the north-south direction (Ulvestad+ 1981AJ.....86.1010U). The source is not detected on space-Earth baselines at 5GHz with the VSOP (Dodson+ 2008ApJS..175..314D). In our image, we detect a bright core and a series of jet components to the southwest.
1219+044|4C +04.42 |The source shows a compact core and extended jet emission aligned in the north-south direction until ~5" (Kharb+ 2010ApJ...710..764K). The 15GHz VLBA image only detected a one-sided jet pointing to the south until 7mas (Lister+ 2009AJ....138.1874L). Our new image shows a bright core and a faint emission to the south.
1228+126|M87       |This is a well-known low-luminosity FR I radio galaxy (Laing+ 1983MNRAS.204..151L). The large-scale image of M87 observed with the VLA at 90cm wavelength suggests that the outward flow from the nucleus extends well beyond the 2kpc radio jet (Owen+ 2000ApJ...543..611O). The 15GHz VLBA image displays an unresolved core and complex jet structure with an extent of 22mas. Our 43GHz VLBA image suggests a limb-brightening morphology with two ridge lines extending to the northwest and west directions. The jet opening angle, estimated from the northern and southern bright jet knots, is about 45{deg} in projection, as is approximately consistent with the value reported in Hada+ (2016ApJ...817..131H) and Zhao+ (2019Galax...7...86Z).
1324+224|          |The deep VLA image at 1.4GHz only detected a compact core (Cooper+ 2007ApJS..171..376C). The 1.4GHz VLBA image shows the jet pointing to the northwest up to 10mas, then bending toward the northeast until 90mas from the core. In the 15GHz VLBA image, the source shows a very compact core and a weak emission feature approximately 3mas to the southwest (Lister+ 2009AJ....138.1874L). However, our new 43GHz image indicates an inner jet toward the northwest on an angular scale of 2mas, at a position angle consistent with the 1.4GHz VLBA image.
1435+638|VIPS 0792 |The 1.4GHz VLA image presents a faint lobe separated from the core by 15.4" in the southwest. It was not detected at 5GHz (Reid+ 1995A&AS..110..213R). Previous studies presumed the radio core to lie at the northernmost end of the jet, based on the 5 and 15GHz VLBA maps (Helmboldt+ 2007ApJ...658..203H; Lister+ 2016AJ....152...12L). We also associated the northeastern component with the radio core in our image.
1504-166|OR -107   |The 1.4GHz VLA map exhibits only radio core emission (Kharb+ 2010ApJ...710..764K). The 1.4GHz VLBA image shows the jet pointing to the west up to ~150mas. The 8 and 15GHz VLBI images show a compact core and extended structure to the south and southeast (Lister+ 2009AJ....138.1874L; Pushkarev & Kovalev 2012A&A...544A..34P). Our new 43GHz image shows the inner jet pointing to the south, which suggests a jet bending.
1514+004|4C +00.56 |The source is a nearby radio galaxy (z=0.052). The 1.4GHz NRAO VLA Sky Survey (NVSS) image shows a symmetric triple source extending in the northwest-southeast direction (Condon+ 1998AJ....115.1693C). In our image, we detect a core and bright jet component pointing to the northwest, in good agreement with the 15GHz VLBA image (Lister+ 2009AJ....138.1874L).
1548+056|4C +05.64 |Kharb+ (2010ApJ...710..764K) detected a bright core and a relatively faint extended radio emission to the north with the VLA at 1.5GHz. On milliarcsecond scales, the source is dominated by a compact core with a jet extending to the north, as was seen previously at 1.4GHz. In our image, we see a complex and curved jet extending to the north and then bending to the northeast at 2mas from the core.
1637+826|NGC 6251  |This is a well-studied FR I radio galaxy that shows both a bright core and large extended asymmetric jet emission (Perley+ 1984ApJS...54..291P). Lower-frequency VLBI observations only detected the jet extending to the southwest direction (Fey+ 2004AJ....127.3587F; Lister+ 2009AJ....138.1874L). Our 43GHz image shows the jet aligned well with the kiloparsec-scale jet.
1716+686|          |The 4.5GHz VLA observation shows a diffuse halo of 10" extension surrounding the core (Taylor+ 1996ApJS..107...37T). Lister+ (2009AJ....138.1874L) presented a jet extending to the northwest up to ~10mas, in a position angle in agreement with our image within 2mas.
1926+611|          |The 1.5GHz VLA image only detected a core (Condon+ 1998AJ....115.1693C), but the 1.7GHz VLBI image shows a bright core and a jet structure extended to the south (Polatidis+ 1995ApJS...98....1P). However, our image exhibits two jet components to the southeast, in agreement with the 15GHz VLBA image (Lister+ 2009AJ....138.1874L). This indicates a jet bending from the south to the southeast, with nearly 70{deg} change in the position angle.
2007+777|          |The image made with the VLA at 1.5GHz shows two-sided radio emission in the east-west direction (Antonucci+ 1986AJ.....92....1A). The eastern component is a prominent hot spot (Murphy+ 1993MNRAS.264..298M). Our image shows the jet extending to the west, corresponding to the western side of the jet in the VLA image.
2021+317|4C +31.56 |The 1.4 and 15GHz VLBA images display the jet extending toward the south (Lister+ 2009AJ....138.1874L), consistently with our new 43GHz VLBA image. However, we also detect a new component off-axis from the persistent jet, on the northwestern side. We believe this northwestern component is the core, and therefore the jet undergoes a sudden bending within 1mas. Future observations can confirm the properties of this intriguing object.
2021+614|OW +637   |The source was classified as a CSO (Tschager+ 2000A&A...360..887T). No radio emission was detected on scales larger than 0.2" with the VLA at 1.4GHz (Kharb+ 2010ApJ...710..764K). Lister+ (2009AJ....138.1874L) identified the core feature located in the end of the southwestern component. We also use the same component as the core for our image, even though the J3 component at ~2.5mas is more compact than the core.
2029+121|OW +149   |The image made with the VLA in A-array at 1.4GHz shows a one-sided, edge-brightened morphology pointing to the northwest (Rector & Stocke 2001AJ....122..565R). The jet in our image extends to the southwest in -130{deg} position angle, in agreement with the 2.3 and 8.6GHz VLBA images (Fey+ 2015AJ....150...58F).
2126-158|OX -146   |This is the highest-redshift AGN in our sample (z=3.268), a GPS quasar (Stanghellini+ 1997A&A...325..943S). The peak emission component in our image has a flat spectrum between 5 and 15GHz and is also identified as the core by Stanghellini+ (2001A&A...377..377S). Our image shows a bright core and a faint jet extending to the southwest.
2134+004|OX +057   |Torniainen+ (2005A&A...435..839T) identified this source as a GPS quasar. Orienti+ (2006A&A...450..959O) found that the core of the source is located in the easternmost component. The core is also the brightest component in the 43GHz radio structure.
2141+175|OX +169   |Large-scale VLA observations only detected a core at 1.4GHz Condon+ (1998AJ....115.1693C). In the 2.3 and 8.6GHz VLBI images, the jet extends to the north, out to a distance of 25mas (~85pc; Petrov+ 2005AJ....129.1163P). We detect the jet initially pointing to the west and then changing its position angle to the northwest, indicating that it has a large (~90{deg}) bending that starts at ~0.2mas.
2155-152|OX -192   |The image made with the VLA at 1.4GHz shows a triple structure with a size of 6" surrounding a central compact component in the north-south direction (Cooper+ 2007ApJS..171..376C). Our image shows a jet toward the southwest up to 2mas, in good agreement with the 5 and 15GHz VLBA images (Fomalont+ 2000ApJS..131...95F; Lister+ 2009AJ....138.1874L).
2209+236|          |Dallacasa+ (2000A&A...363..887D) identified the source as an HFP. The 5GHz VLBA image (Fomalont+ 2000ApJS..131...95F) shows no indication of extended emission. Lister+ (2016AJ....152...12L) found a jet component to the northeast and determined a maximum apparent proper motion 1.35c. Our image shows the inner jet bending to the northeast.
2223+210|DA 580    |The jet structure extends to the southwest in the 2.3, 8.6, and 15GHz VLBI images (Beasley+ 2002ApJS..141...13B ; Lister+ 2009AJ....138.1874L). We detect two compact components inside the low-frequency VLBI core region. Although the eastern one is not the brightest component, it appears in the upstream direction. Therefore we identify this as the radio core.
2227-088|          |The source shows an integrated flux density of 2.7Jy in the core at 43GHz, and only 21mJy in the extended emission. Tingay+ (2003PASJ...55..351T) found this source highly variable at 4.8GHz with Australia Telescope Compact Array (ATCA). The many VLBI images made at lower frequencies13 indicate a faint, wiggling jet toward the north.
2234+282|CTD 135   |Lister+ (2016AJ....152...12L) identified the core in this BL Lac object with the northernmost jet feature in their 15GHz VLBA images. Earlier An+ (2016AN....337...65A) claimed this source to be a rare {gamma}-ray emitting CSO candidate with a two-sided jet, based on a comparison of VLBA maps at 8.4 and 15GHz. In our new 43GHz image, the southwestern component is the brightest and most compact, suggesting that this is the true core, instead of the northeastern feature (Lister+ 2016AJ....152...12L). Also, our new observations are at odds with the CSO interpretation (An+ 2016AN....337...65A).
2243-123|          |The jet points to the northeast in the previous 5 and 15GHz VLBA images (Fomalont+ 2000ApJS..131...95F; Lister+ 2009AJ....138.1874L). In our image, the innermost section of the jet points closer to the north, within 4mas from the core.
2318+049|OZ +031   |VLA images show a barely resolved structure along the -40{deg} position angle (Hutchings+ 1998PASP..110..111H). In our VLBA image, the source shows a compact core-jet structure extending to the northwest in about the same direction. This is consistent with lower-frequency VLBI images (e.g., Fomalont+ 2000ApJS..131...95F; Lister+ 2009AJ....138.1874L). Note that the 5GHz VSOP Survey image also shows emission within 2mas extended in the same direction, albeit with no clear indication of the core (Scott+ 2004ApJS..155...33S).