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381. J0057+3021
... 5-GHz total flux density . ... 0.017 * = the position has been determined to an accuracy of 10 mas from the VLBApls data . VLBApls image at 5 GHz . color gif | contour gif | ... Correlated flux density (Jy) vs. projected baseline length plot . gif | ... flux density (Jy) . EW position (mas) . ... major axis (mas) . minor axis (mas) . position angle ( ) . ... 2.0 0.3 . ... 5 GHz: see Gurvits et al. ... VLBApls reference: Fomalont et al. ... VLBApls home page . ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0057+3021.htm -- 3.7 Кб -- 08.05.2001
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382. http://www.vsop.isas.ac.jp/vsopsymp/papers/vsopsymp.errata
... The caption to Color Figure 3 refers to the source 1928+734, which should be 1928+738. In the summary section on page 49 (Murphy et al.), the sentence "In that time, we have observed a variety of structural changes in the inner jet region near the region." should read "In that time, we have observed a variety of structural changes in the inner jet region near the core." In the references on page 175 (Fomalont et al.) and page 182 (Moellenbrock et al.) ...
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Ссылки http://www.vsop.isas.ac.jp/vsopsymp/papers/vsopsymp.errata -- 2.3 Кб -- 09.01.2001
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383. http://www.vsop.isas.ac.jp/VLBApls/img/1833-210MAPSW.ps
J1833ґ2103 SW
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/img/1833-210MAPSW.ps -- 41.3 Кб -- 17.10.2000
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384. http://www.vsop.isas.ac.jp/VLBApls/img/1833-210MAPNE.ps
J1833ґ2103 NE
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/img/1833-210MAPNE.ps -- 42.0 Кб -- 17.10.2000
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385. http://www.vsop.isas.ac.jp/VLBApls/img/1501-391MAPW.ps
J1501ґ3918 W
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/img/1501-391MAPW.ps -- 48.5 Кб -- 17.10.2000
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386. http://www.vsop.isas.ac.jp/VLBApls/img/1501-391MAPE.ps
J1501ґ3918 E
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/img/1501-391MAPE.ps -- 38.6 Кб -- 17.10.2000
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387. VLBApls acknowledgements
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. ... LIG acknowledges partial support from the European Commission's TRM Programme, "Access to Large-Scale Facilities", under contract ERBFMGECT950012 and the European Commission's TRM programme, Research Network Contract ERBFMRXCT 96-0034 "CERES". ... the US Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID), . ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/acknowledgements.htm -- 2.9 Кб -- 17.10.2000
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388. VLBApls source sample
... The VSOP Survey Continuum Source List . The radio sample for the VSOP continuum survey was defined to include all extragalactic radio sources with: . a total flux density at 5 GHz, S>=1.0 Jy . ... The sample also included all sources in the sky with a 5 GHz flux density S>5 Jy, regardless of spectral index and galactic latitude. ... The source would then be included in the VSOP sample (three of the sources were found with a flux density above 1 Jy and added to the sample). ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/sample.htm -- 4.1 Кб -- 17.10.2000
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389. source comment
. Comment on J2346+0930 . See Figure 4 for an image of each component. The source was detected at 2.3 GHz by Preston et al. (1985) (correlated flux density 40 mJy) with much higher resolution. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2346+0930.comment.htm -- 1.5 Кб -- 16.10.2000
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390. source comment
. Comment on J2250+1419 . Resolved: the source is extended, with about 0.15 Jy correlated flux density observed with the shortest VLBA baselines. It was not detected at 2.3 GHz by Preston et al. (1985). Augusto, Wilkinson & Browne (1998) find it partially resolved with MERLIN at 5 GHz. See Figure 3. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2250+1419.comment.htm -- 1.6 Кб -- 16.10.2000
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391. source comment
. Comment on J2249+1136 . Resolved: this "head-tail" radio galaxy is extended, although 0.15 Jy correlated flux density is observed with the shortest VLBA baselines. See Figure 3. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2249+1136.comment.htm -- 1.5 Кб -- 16.10.2000
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392. source comment
Comment on J2246-1206 . In contrast to the jet pointing to the NE in our image, the 5 GHz VLBI image of Shen et al. (1998) shows no indication of extended emission above the 20 mJy/beam level. Hong et al. (1999) find a jet component to the SE and identify that with a "superluminal" component possibly ejected in 1992. A 15 GHz image from the USNO database, taken nearly at the same epoch as the image of Hong et al. (1999) does not show any component at this position angle. ...
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2246-1206.comment.htm -- 1.9 Кб -- 16.10.2000
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393. source comment
. Comment on J2243-2544 . The jet extends in the opposite direction to that shown by Shen et al. (1998) at 5 GHz with about 2 times higher resolution than our image. The structure we see is confirmed by the 2.3 and the 8.4 GHz images 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/J2243-2544.comment.htm -- 1.5 Кб -- 16.10.2000
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394. source comment
. Comment on J2225+2118 . 2.3 and 8.4 GHz EVN data show a single dominant component; images are not published by Dallacasa et al. (1998). Our 5 GHz image shows a clear core-jet structure extending to the SW. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2225+2118.comment.htm -- 1.5 Кб -- 16.10.2000
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395. source comment
. Comment on J2209-2331 . Not detected: the source is probably extended, and 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/J2209-2331.comment.htm -- 1.4 Кб -- 16.10.2000
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396. source comment
. Comment on J2206-1835 . Resolved: the source is extended, and has been detected only on the short Australian baselines at 2.3 GHz by Preston et al. (1989). Moellenbrock et al. (1996) did not detect the source in the 22 GHz VLBI survey. The correlated flux density is 1.2 Jy on the shortest VLBA baseline (see Figure 3). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2206-1835.comment.htm -- 1.6 Кб -- 16.10.2000
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397. source comment
. Comment on J2158-1501 . There is a striking difference between our and the 5 GHz image of Shen et al. (1998): the jet position angle differs by ~180 . All other VLBI images found in the literature (USNO image database; Kellermann et al. 1998) are consistent with our image. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2158-1501.comment.htm -- 1.6 Кб -- 16.10.2000
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398. source comment
. Comment on J2136+0041 . The eastern of the two major components is stronger at 15 GHz (Kellermann et al. 1998) than the western one, indicating that the brightest component in our image may have a steep spectrum. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J2136+0041.comment.htm -- 1.5 Кб -- 16.10.2000
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399. source comment
. Comment on J1957-3845 . The extension we see to the S-SE is not present in the 5 GHz VLBI image by Shen et al. (1998). VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1957-3845.comment.htm -- 1.4 Кб -- 16.10.2000
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400. source comment
. Comment on J1924-2914 . The extended feature to the NE of the core in not seen in the 5 GHz image by Shen et al. (1997), probably because their higher resolution resolved out this component. VLBApls home page . Last modified: 16 Oct 2000
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Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1924-2914.comment.htm -- 1.5 Кб -- 16.10.2000
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