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401. source comment
. Comment on J1842+7946 . Comparing the brightnesses of the two main features seen in our 5 GHz image with higher frequency VLBI images available in the literature (at 8.4 GHz from the USNO database and at 15 GHz by Kellermann et al. (1998)), one can conclude that the NW component has a steeper spectrum since the SE one becomes relatively stronger as the observing frequency increases. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1842+7946.comment.htm -- 1.7 Кб -- 16.10.2000
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402. source comment
. Comment on J1833-2103 . A gravitational lens system; the two lensed images are given in Figure 4. See Guirado et al. (1999) for more detailed, 2.3 and 8.4 GHz VLBI observations. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1833-2103.comment.htm -- 1.5 Кб -- 16.10.2000
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403. source comment
. Comment on J1804+0101 . The southern jet position angle is consistent with the 8.4 GHz EVN image by Dallacasa et al. (1998). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1804+0101.comment.htm -- 1.4 Кб -- 16.10.2000
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404. source comment
. Comment on J1745-0753 . The derived position in Table 1 is 22" west of the correlation position. Hence, some of the apparent north-south extent of the source may be caused by instrumental smearing. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1745-0753.comment.htm -- 1.5 Кб -- 16.10.2000
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405. source comment
. Comment on J1733-1304 . There is weak extended emission at ~20-30 mas N of the core which is also seen in a 2.3 GHz USNO image, but is probably resolved out in the 5 GHz VLBI image of Shen et al. (1997). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1733-1304.comment.htm -- 1.5 Кб -- 16.10.2000
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406. source comment
. Comment on J1724-0241 . No detection: the source is probably extended. It was not detected at 2.3 GHz by Preston et al. (1985). There is a redshift in SIMBAD (z=0.033) based on a wrong optical identification with a galaxy (Stickel, K hr & Fried 1993). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1724-0241.comment.htm -- 1.5 Кб -- 16.10.2000
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407. source comment
. Comment on J1720-0058 . Resolved: this FR-II radio galaxy is not detected at 2.3 GHz by Preston et al. (1985). A VLA map at 8.4 GHz is published by Swain, Bridle & Baum (1998). However, there is correlated signal at the shortest baselines from which a position has been derived and is listed in the table. Our best guess is that the residual core has a flux density of 0.15 Jy and a size of ~15 mas. See Figure 3. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1720-0058.comment.htm -- 1.7 Кб -- 16.10.2000
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408. source comment
. Comment on J1710+0036 . No detection: This source is probably 4C+00.65 and is probably resolved, although the position may be in error by more than 30". It was also not detected at 2.3 GHz by Preston et al. (1985). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1710+0036.comment.htm -- 1.5 Кб -- 16.10.2000
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409. source comment
. Comment on J1658-0739 . The derived position was 19" W of the correlating position, so some image smoothing in the N/S direction is possible. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1658-0739.comment.htm -- 1.4 Кб -- 16.10.2000
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410. source comment
. Comment on J1651+0459 . No detection: this symmetric double-lobe radio galaxy is not detected in our VLBA survey. The jet-dominated VLA structure at 1.4 and 5 GHz is shown by Harvanek & Hardcastle (1998) and Dreher & Feigelson (1984). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1651+0459.comment.htm -- 1.5 Кб -- 16.10.2000
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411. source comment
. Comment on J1640+1220 . Augusto, Wilkinson & Browne (1998) show a 5 GHz MERLIN image and describe the source as a core-jet: their jet component is at PA=-50 . This, and our image, imply a gently curved jet from mas to 100 mas scale. The mas-scale structure is similar in the 8.4 GHz image from the VLBA Calibrators database. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1640+1220.comment.htm -- 1.6 Кб -- 16.10.2000
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412. source comment
. Comment on J1554-2704 . The image here is in good agreement with a 2.3 GHz image from the VLBA Calibrators database. Lovell (in preparation) gives a position of RA=15h 54m 02.47s, Dec=-27 04 40.2", in good agreement with that derived from these observations. The correlating position was 9" offset, but should not affect the quality of the image. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1554-2704.comment.htm -- 1.6 Кб -- 16.10.2000
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413. source comment
. Comment on J1546+0026 . The emission extending to both sides of the core in our image is in agreement with the results by Stanghellini, O'Dea & Murphy (1999). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1546+0026.comment.htm -- 1.4 Кб -- 16.10.2000
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414. source comment
. Comment on J1530-4231 . No detection: the source is probably extended. ATCA observations confirm that the source has a steep spectral index (Tasker, private communication). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1530-4231.comment.htm -- 1.5 Кб -- 16.10.2000
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415. source comment
. Comment on J1526-1351 . Our VLBI image is probably the first published. A VLA 5 GHz image (Reid, Kronberg & Perley 1999) shows elongated structure in the NE-SW direction. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1526-1351.comment.htm -- 1.5 Кб -- 16.10.2000
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416. source comment
... The derived position here agrees with the position from recent ATCA observations, RA=15h 01m 34.74s, Dec=39 18 39.2" (Tasker, private communication) which found the source unresolved. Because of the relatively large position offset, the reality of the fainter component 0.12" to the west is somewhat in doubt. However, the ATCA centroid position is offset by 0.3" to the south-east of the VLBA position, suggesting that the faint component may be part of more extended structure. ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1501-3918.comment.htm -- 1.8 Кб -- 16.10.2000
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417. source comment
. Comment on J1419-1928 . A 5 GHz VLA image is published by Antonucci (1985). There is a hint of an extension to the core in our VLBI image, at a position angle near the arcsec-scale structure. A 8.4 GHz image from the VLBA Calibrators database also shows a secondary component in this direction (SW). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1419-1928.comment.htm -- 1.6 Кб -- 16.10.2000
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418. source comment
. Comment on J1411+5212 . No detecton: extended double-lobe radio galaxy, no core is seen in a MERLIN 1.6 GHz image (Akujor et al. 1994). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1411+5212.comment.htm -- 1.4 Кб -- 16.10.2000
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419. source comment
. Comment on J1332+0200 . A 1.4 GHz VLA image by Harvanek & Hardcastle (1998) shows a double-lobe radio galaxy with a one-sided jet to the western lobe. Our first-time VLBI image shows extension in the same direction. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1332+0200.comment.htm -- 1.5 Кб -- 16.10.2000
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420. source comment
. Comment on J1325-4301 . Our image, limited by the short observing time, shows symmetrical structure elongated in the NE-SW direction which is not useful to study the details of this complex source. High dynamic range images of this source are published by Tingay et al. (1998). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1325-4301.comment.htm -- 1.6 Кб -- 16.10.2000
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