... With the FORS1 instrument of the ESO VLT, we have performed during the 2007 apparition of 133P/Elst-Pizarro quasisimultaneous photometry and polarimetry of its nucleus at nine epochs in the phase angle range 0 - 20 . ... Geometric information about the dust tails of 133P/Elst-Pizarro. ... The most logical explanation of the almost absent coma and the narrow dust tails is low nucleus activity and the small terminal expansion velocity of the dust grains after release by the nucleus of 133P/Elst...

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... ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ ^ 2.08 ^ 0.03 2.33 ^ 0.02 2.31 ^ 0.01 2.44 ^ 0.01 2.41 ^ 0.01 2.30 ^ 0.02 2.55 ^ 0.02 2.51 ^ 0.01 1.95 ^ 0.02 2.27 ^ 0.02 2.27 ^ 0.02 2.60 ^ 0.01 2.35 ^ 0.01 2.54 ^ 0.01 2.38 ^ 0.01 2.55 ^ 0.03 2.25 ^ 0.01 2.55 ^ 0.01 2.55 ^ 0.02 2.46 ^ 0.01 2.42 ^ 0.01 2.56 ^ ... 17 in our sample with the predictions of the stellar population models. ...

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Astronomy & Astrophysics manuscript no. rcw79f2 (DOI: will be inserted by hand later) September 12, 2005 Triggered massive-star formation on the borders of Galactic H II regions II. ... All these facts strongly indicate that the massive-star formation observed at the border of the H II region RCW 79 has been triggered by its expansion, most probably by the collect and collapse process. ... Stars: formation ґ Stars: early-type ґ ISM: H II regions ґ ISM: individual: RCW 79 1. ... Fig. ... This in- Fig. ...

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... Number 5721 . ... 8 August 2006 . ... Data file: 5721-t3 . ... IBVS No. ... 2000.0 Max Min Type References h m s o ' m m 780217 V1675 Ori 05 34 23.8 -05 08 16 13.70 ( 0.08 ) Ic INB 072 USNO 780218 V1676 Ori 05 34 23.9 -05 15 40 11.19 ( 0.16 Ic) J INB 072 USNO 780219 V1677 Ori 05 34 24.3 -06 06 56 12.96 ( 0.10 ) Ic INB 072 USNO 780220 V1678 Ori 05 34 25.3 -04 54 39 13.24 ( 0.09 ) Ic INB 072 USNO 780221 V1679 Ori 05 34 26.1 -06 15 33 15.64 ( 0.14 ) Ic INB ... Sgr . ... Ori...

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R And S5/4.5e. S And SN (NGC 224). W And S7.5/1-e. X And S5/7-e. Z And The light curve is characterized by outbursts up to 4m with intervals of 10 - 20 years. In the intervals cyclic variations are observed with the mean period of 632d and variations with cycles of several days and Delta(m) ~ 0.1m - 0.5m. The spectrum is symbiotic, with features of a late M giant, narrow low-excitation emission lines (Bleq) and forbidden lines characteristic of highly excited nebulae. RR And S6/3.5e. RT And Min II 8.88; DI

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id | x | y | mag | coord2000 -----------+---------+---------+--------+--------------------------------------------- 585574124 | 4063.52 | 2539.02 | 16.66 | ( 7h 3m 17.700477s , +57d 9m 35.690306s) 585574123 | 4062.73 | 2712.82 | 17.657 | ( 7h 2m 38.320318s , +57d 8m 41.251248s) 585574122 | 4062.23 | 2202.82 | 16.845 | ( 7h 4m 33.867593s , +57d 11m 24.064723s) 585574121 | 4062.07 | 1764.03 | 18.755 | ( 7h 6m 13.525438s , +57d 13m 38.470789s) 585574120 | 4060.8 | 2925.84 | 17.665 | ( 7h 1m 50.06688s , +57d 7m

31. http://www.stecf.org/goods/spectroscopy/CDFS_Mastercat/szokoly04.ps