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На этой странице приведены все страницы сервера www.vsop.isas.ac.jp ,которые мы индексируем. Показаны документы 421 - 440 из 477.

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421. source comment

. Comment on J1242-0446 . No detection: an extended double-lobe radio galaxy, not detected at 2.3 GHz by Preston et al. (1985). Mantovani et al. (1997) did not detect a core even with the VLA at 8.4 and 15 GHz. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1242-0446.comment.htm -- 1.5 Кб -- 16.10.2000
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422. source comment

. Comment on J1239-1023 . No image is shown by Dallacasa et al. (1998) as they did not find the VLBI structure at 2.3 and 8.4 GHz prominent, just dominated by a compact region barely resolved in position angle about -45 . In our case the source is well resolved, with a jet pointing to the W-NW direction, in agreement with what is seen in the images at 2.3 and 8.4 GHz from the VLBA Calibrators database. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1239-1023.comment.htm -- 1.7 Кб -- 16.10.2000
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423. source comment

. Comment on J1232-0224 . Hooimeyer et al (1992a) detected the source on the Green Bank-Owens Valley baseline at 5 GHz (correlated flux density 180 mJy) and found that the nuclear emission was probably diffuse. The jet position angle in a 1.4 GHz VLA image (Hintzen, Ulvestad & Owen 1983) is similar to that in our VLBA image. Our image is consistent with the images at 2.3 and 8.4 GHz from the VLBA Calibrators database. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1232-0224.comment.htm -- 1.7 Кб -- 16.10.2000
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424. source comment

. Comment on J1225+1253 . Early 2.3 GHz VLBI observations (Jones, Terzian & Sramek 1981) indicate an elongated source structure in the N-S direction, in agreement with our image. Giovannini, Feretti & Comoretto (1990) measured a 180 mJy correlated flux density at 1.6 GHz on the shortest VLBI baselines. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1225+1253.comment.htm -- 1.6 Кб -- 16.10.2000
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425. source comment

. Comment on J1158+2450 . The complicated structure seen in our image is in agreement with other VLBI images found in the literature (USNO image database; Kellermann et al. 1998). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1158+2450.comment.htm -- 1.5 Кб -- 16.10.2000
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426. source comment

. Comment on J1146-3328 . The derived position here is about 20" from that of the PMN survey position (Griffith & Wright 1993). The source is only detected on the shorter baselines and is probably resolved, although some smearing may be caused by the large position offset. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1146-3328.comment.htm -- 1.6 Кб -- 16.10.2000
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427. source comment

. Comment on J1139-1350 . The 15 GHz VLA image of Bogers et al. (1994) shows an asymmetric triple source ~1 in size, oriented SE-NW. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1139-1350.comment.htm -- 1.4 Кб -- 16.10.2000
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428. source comment

. Comment on J1130-1449 . There are two dominant components in our image. Comparison with the 15 GHz image of Kellermann et al. (1998) reveals that the western component is brighter at the higher frequency, indicating that the brighter (eastern) component in our image may have a steep spectrum. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1130-1449.comment.htm -- 1.6 Кб -- 16.10.2000
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429. source comment

. Comment on J1058+1951 . The source structure is elongated in the N-S direction. The 15 GHz image by Kellermann et al. (1998) shows a 4 mas jet to the N. The 5 GHz image by Hooimeyer et al. (1992b) has extensions to both N and S. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1058+1951.comment.htm -- 1.5 Кб -- 16.10.2000
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430. source comment

. Comment on J1041+0242 . No detection: the source is probably extended, and it was not detected at 2.3 GHz by Preston et al. (1985). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1041+0242.comment.htm -- 1.4 Кб -- 16.10.2000
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431. source comment

. Comment on J1037-2934 . The extension to the E-NE is not seen in the 5 GHz VLBI image of Hong et al. (1999). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1037-2934.comment.htm -- 1.4 Кб -- 16.10.2000
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432. source comment

. Comment on J1035+5628 . 8.4 and 15 GHz VLBA images of this CSO are published by Taylor, Readhead & Pearson (1996). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1035+5628.comment.htm -- 1.4 Кб -- 16.10.2000
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433. source comment

. Comment on J1018-3144 . Resolved: There is 0.5 Jy of correlated flux density at the shortest baselines. The position is accurate, so the source is resolved. It was also not detected at 2.3 GHz by Preston et al. (1985). See Figure 3. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1018-3144.comment.htm -- 1.5 Кб -- 16.10.2000
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434. source comment

. Comment on J1006+3454 . Our image shows a jet extending up to 10 mas to the W-NW. See Conway (1999) for a detailed VLBI image taken at 1.29 GHz. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J1006+3454.comment.htm -- 1.4 Кб -- 16.10.2000
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435. source comment

. Comment on J0957+5522 . A 5 GHz MERLIN image (Xu et al. 1995) shows a 200 mas jet pointing to the W, and indicates that the core is elongated to the SW. Our map of the core region indicates a bending jet from mas to arcsecond angular scales. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0957+5522.comment.htm -- 1.5 Кб -- 16.10.2000
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436. source comment

. Comment on J0949+6614 . No detection: the source was also not detected with VLBI at 1.6 GHz (Polatidis et al. 1995). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0949+6614.comment.htm -- 1.4 Кб -- 16.10.2000
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437. source comment

. Comment on J0834+5534 . A compact symmetric object (CSO) with ~160 mas separation between components, as shown by 1.6 GHz VLBI observations (Polatidis et al. 1995). The weaker component is not detected in our survey (see also Pearson & Readhead 1988). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0834+5534.comment.htm -- 1.5 Кб -- 16.10.2000
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438. source comment

. Comment on J0824+3916 . Widely separated (~0.3") components. Gravitational lensing was rejected by King et al. (1999). See Figure 4. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0824+3916.comment.htm -- 1.4 Кб -- 16.10.2000
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439. source comment

. Comment on J0758+3747 . Our image is in agreement with that of Polatidis et al. (1995) and Xu et al. (1995) at 1.6 and 5 GHz. A VLA image shows a source extended by 2 in position angle 120 , with a strong arcsecond jet aligned in the same direction as the mas jet. VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0758+3747.comment.htm -- 1.6 Кб -- 16.10.2000
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440. source comment

. Comment on J0648-3957 . No detection: a steep spectrum, alpha=-0.82, between 80 MHz and 8.4 GHz. Tasker, private communication, found the source to be heavily resolved on ATCA baselines ( reference ). VLBApls home page . Last modified: 16 Oct 2000

[ Сохраненная копия ] Ссылки http://www.vsop.isas.ac.jp/VLBApls/J0648-3957.comment.htm -- 1.5 Кб -- 16.10.2000
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