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441. source comment
. Comment on J0646+4451 . An extremely high redshift quasar. An estimate of the apparent angular proper motion of the secondary component gives ~0.09 mas/year, based on two previous epochs (Gurvits et al. 1992; Xu et al. 1995). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0646+4451.comment.htm -- 1.5 Кб -- 16.10.2000
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442. source comment
. Comment on J0636-2034 . No detection: an FR-II radio galaxy. The compact core at 1.4 GHz has a flux density of <10 mJy (VLA data, Baum et al. 1988). Thus, the source is below our detection limit. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0636-2034.comment.htm -- 1.5 Кб -- 16.10.2000
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443. source comment
Comment on J0627-3529 . We have detected the core of an FR-I object and early-type galaxy (Venturi et al. 1995). The core is 0.54 Jy at 2.3 GHz on the Parkes-Tidbinbilla baseline (Morganti et al. 1997) and 0.6 Jy at 5 GHz (VLA data, Ekers et al. (1989) and Morganti, Killeen & Tadhunter (1993)). The VLBA image at 2.3 GHz with the resolution of 15x9 mas shows a "core-jet" structure, with the core brightness of 494 mJy/beam (Venturi et al. ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0627-3529.comment.htm -- 1.9 Кб -- 16.10.2000
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444. source comment
. Comment on J0620-3711 . No detection: our non-detection is compatible with the results of Jones, McAdam & Reynolds (1994) with Parkes-Tidbinbilla two-element interferometer, who measured a compact core with S(2.3GHz)<30 mJy and S(8.4GHz)=15 mJy (alpha>-0.54). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0620-3711.comment.htm -- 1.5 Кб -- 16.10.2000
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445. source comment
. Comment on J0627-0553 . No detection: a steep spectrum (alpha=-0.87), symmetric double source, resolved with the VLA at 5 and 1.4 GHz (Ulvestad et al. 1981; Pearson, Readhead & Perley 1985). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0627-0553.comment.htm -- 1.5 Кб -- 16.10.2000
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446. source comment
. Comment on J0616-3456 . No detection: the position is probably okay, hence, the source is probably resolved out completely. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0616-3456.comment.htm -- 1.4 Кб -- 16.10.2000
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447. source comment
. Comment on J0607+6720 . The redshift is from R.C. Vermeulen & G.B. Taylor, private communication. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0607+6720.comment.htm -- 1.4 Кб -- 16.10.2000
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448. source comment
. Comment on J0604-3155 . No detection: the source has a relatively steep spectrum, alpha=-0.62, in the frequency range from 80 MHz to 8 GHz and the position is probably okay. Hence, the source is probably resolved. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0604-3155.comment.htm -- 1.5 Кб -- 16.10.2000
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449. source comment
. Comment on J0530-2503 . Our image agrees with those at 2.3 and 8.4 GHz, available in the VLBA Calibrators database. The source was not detected at 5 GHz in VLBI observation by Hong et al. (1999). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0530-2503.comment.htm -- 1.5 Кб -- 16.10.2000
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450. source comment
Comment on J0513-2159 . Our image shows an extension to about 5 mas SE from the brightest feature. The EVN 8 GHz image by Dallacasa et al. (1998), with about five times larger resolution, shows an extension from the brightest feature roughly opposite to our direction. As noted by Dallacasa et al. (1998), the structure detected has a highly inverted spectrum, which, together with the reported variability in the source, could explain the structural disagreement. ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0513-2159.comment.htm -- 1.8 Кб -- 16.10.2000
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451. source comment
... The source exhibits a mas-scale structure which, according to the USNO multi-epoch monitoring at 2.3 and 8.4 GHz over the period from 1994 July through 1998 April, undergoes considerable changes in the brightness distribution and positions of the major structural features. Our image is qualitatively consistent with the structural pattern of the source. ... We note a difference of ~90 in position angles of secondary components in our image and the 5 GHz VLBI image by Shen et al. 1998). ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0457-2324.comment.htm -- 2.3 Кб -- 16.10.2000
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452. source comment
. Comment on J0455-3006 . No detection: the source may be resolved out or the position could be in error by more 30". The position comes from Griffith & Wright (1993). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0455-3006.comment.htm -- 1.5 Кб -- 16.10.2000
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453. source comment
. Comment on J0437+2940 . The source has extended structure on the arcsecond scale over a very broad range of frequencies, from 25 MHz (Megn et al. 1987) to 98 GHz (Okayasu, Ishiguro & Tabara 1992). In our observation, the source is well resolved. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0437+2940.comment.htm -- 1.5 Кб -- 16.10.2000
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454. source comment
. Comment on J0437-1844 . In our observation, the source is well resolved but shows no particular structural features. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0437-1844.comment.htm -- 1.4 Кб -- 16.10.2000
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455. source comment
. Comment on J0431+2037 . A Gigahertz Peaked Spectrum (GPS) galaxy with complex radio structure on the scale of 10 to 100 mas (combined EVN+MERLIN data at 1.6 GHz, Dallacasa et al. 1995). Our image is consistent with the center-southern features of Dallacasa et al. (1995). The northern feature, ~180 mas N-NW from the field center, outside the boundary of the displayed image, can barely be seen in our data. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0431+2037.comment.htm -- 1.7 Кб -- 16.10.2000
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456. source comment
. Comment on J0424+0036 . A redshift z=0.310 is reported by Smith & Nair (1995) but is not listed in V ron-Cetty & V ron (1998). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0424+0036.comment.htm -- 1.4 Кб -- 16.10.2000
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457. source comment
. Comment on J0414+0534 . A gravitational lens with an overall size of 2.2" (e.g. Katz, Moore & Hewitt 1997). Two of the four lensed components are in our field of view, separated by ~430 mas (Figure 4). See Porcas (1998) and Trotter, Winn & Hewitt (2000) for recent 5 GHz VLBI images of this system. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0414+0534.comment.htm -- 1.6 Кб -- 16.10.2000
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458. source comment
. Comment on J0414+3418 . The source is unresolved at 8 GHz with VLA-A (Wilkinson et al. 1998); and our image agrees with the 2.3 GHz image in the VLBA Calibrators database. The correlation position was 15" from the core position, so there may be some smoothing in our image. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0414+3418.comment.htm -- 1.6 Кб -- 16.10.2000
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459. source comment
. Comment on J0405+3803 . Our image contains a feature of 25 mJy at 14 mas E-NE from the brightest component. It is not visible in the Caltech-Jodrell (CJ) survey image at 5 GHz (Xu et al. 1995) obtained about 6 years earlier. The 1.6 GHz CJ image (Polatidis et al. 1995) does show an extended feature close to the position in question, but somewhat displaced toward west. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0405-1308.comment.htm -- 1.6 Кб -- 16.10.2000
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460. source comment
. Comment on J0405-1308 . Our image is in qualitative agreement with the 2.3 and 8.4 GHz USNO images. The 5 GHz image by Shen et al. (1998) does not show an extension at the position visible in our image. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0405+3803.comment.htm -- 1.5 Кб -- 16.10.2000
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