CCD observations in the Vilnius photometric system.

Boyle, R. P.; Vrba, F. J.; Smriglio, F.; Dasgupta, A. K.; Straižys, V.

doi:10.1515/astro-1996-0208

Cited by 9 publications

(10 citation statements)

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“…primary intention of our group was to study the interstellar reddening in the direction of the globular clusters M 56 and M 71 using photoelectric and CCD photometry of the field stars in the Vilnius system (Smriglio et al 1991, Boyle et al 1992. This system gives a photometric classification of stars of any spectral type and luminosity class in presence of interstellar reddening.…”

Section: Resultsmentioning

confidence: 99%

“…The spectral type, absolute magnitude, distance and color excess have been determined for each star. The reddening, as a function of the distance, for the three areas and their relative errors have been determined by Smriglio et al (1991) and Boyle et al (1992). The dispersion of the reddening values in each area is significantly larger than the photometric errors.…”

Section: Observationsmentioning

confidence: 94%

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A study of dust cloud parameters by Vilnius photometry

Smriglio¹,

Dasgupta²,

Boyle³

1996

Open Astronomy

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Abstract. Three-dimensional classification of stars based on their seven-color CCD photometry in the Vilnius system has been succesfully applied to study the small scale structure of interstellar dust clouds. In the present paper the statistical equations of Münch are modified and applied to stars located beyond the galactic absorbing layer. This particular use of Miinch's statistics and the properties of CCD photometry in the Vilnius system offer a better possibility of probing the small scale structure of interstellar medium outside of the solar vicinity. This new technique and the first results are discussed.

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Section: Resultsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 94%

A study of dust cloud parameters by Vilnius photometry

Smriglio¹,

Dasgupta²,

Boyle³

1996

Open Astronomy

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“…This bias is pushed further towards luminous stars by the large total extinction A V suffered by radiation (see below). On the other hand, the patchiness of interstellar extinction (Boyle et al 1992, the effects of which have been found on scales down to 30 square arcmin by) makes it likely that many stars within our 730 square arcmin fields will be observed through transparent "windows" in the dust column (or conversely through dust screens). These effects, coupled with uncertainties in absolute magnitude M V calibration (at least ±0.3 mag, or 15% distance uncertainty) mean that a wide range of stars could be considered as possible candidates for association with the SWB.…”

Section: Stellar Residents Within the Swbmentioning

confidence: 98%

The Galactic Plane region near $\mathsf{\ell = 93\degr}$

Foster

Routledge

Kothes

2004

A&A

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Abstract. New Canadian Galactic Plane Survey λ21 cm H  line observations towards supernova remnant (SNR) 3C 434.1 (G94.0+1.0) are presented. We find a fragmented and thin-walled atomic hydrogen shell inside which the SNR is seen to be contained at v −80 km s −1 , which we report to be a highly evolved stellar wind bubble (SWB) associated with the remnant. A dark area in the midst of otherwise bright line emission is also seen near −71 km s −1 . An absorption profile to the extragalactic continuum source 4C 51.45 (superimposed on the shell's north face) allows us to probe the shell's optical depth, kinetic temperature and expansion velocity. The material in the dark area has the same properties as material in the fragmented shell, suggesting that the dark area is actually the far-side "cap" of the shell seen absorbing emission from warm background gas, the first instance of H  Self Absorption (HISA) seen in such a structure. We show that the kinematic distance of 10 kpc derived from a flat Galactic rotation model is highly improbable, and that this bubble/SNR system is most likely resident in the Perseus Spiral Arm, lying 5.2 kpc distant. We model the SWB shell in three dimensions as a homologously expanding ellipsoid. Physical and dynamical characteristics of the bubble are determined, showing its advanced evolutionary state. Finally, from a photometric search for one or more stars associated with the SWB, we determine that three B0V stars and one O4V star currently inhabit this bubble, and that the progenitor of 3C 434.1 was at latest also an O4 type star.

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“…Boyle et al (1996), applying CCD Vilnius photometry to several fields in open clusters and dark clouds, have shown that the precision required by the Vilnius system is readily attainable down to V=17 with a 1 meter telescope. If applied to the MEGA fields, the CCD photometry would allow to reach three magnitudes below those achieved in our photoelectric survey (Bartasiute 1994(Bartasiute , 1996 using a telescope of the same aperture.…”

Section: Summary and Future Workmentioning

confidence: 99%

UBVR and UPXYZVS sequences of standard stars for the MEGA program fields along the main meridian of the Galaxy

Andruk¹,

Bartasiute²,

Kharchenko³

1996

Open Astronomy

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Abstract. Within the framework of the MEGA program devoted to the study of the main meridional section of the Galaxy, photoelectric observations have been made in the Johnson UBVR and Vilnius UPXYZVS systems to obtain photometric sequences of standard stars in a number of proper motion fields, each of 1.4 square degree size, located approximately along the main galactic meridian.The catalog of our UBVR observations includes a total of 1141 stars which provide sequences for 47 MEGA fields and for a few of other fields. Each of the sequences contains 15 to 28 stars almost uniformly distributed in the V magnitude range from 4.5 to 15.5 mag. The external rms errors of the observations are dh 0.014 for the magnitude V and ± 0.026, ± 0.012 and ± 0.016 for the color indices U-B, B-V and V-R, respectively. These standards will be used for the reduction of photographic magnitudes.In the medium-band Vilnius system, the photoelectric sequences have been established for six MEGA fields near the galactic poles, each of which consists of about 50 standards in the magnitude range 8.5 < V< 13.5 mag. The errors of the UPXYZVS magnitudes and color indices range from ± 0.008 to ± 0.020 mag, depending on the brightness of a star.The possibility of making use of these standard sequences for CCD observations is discussed.

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CCD observations in the Vilnius photometric system.

Cited by 9 publications

References 0 publications

A study of dust cloud parameters by Vilnius photometry

A study of dust cloud parameters by Vilnius photometry

The Galactic Plane region near $\mathsf{\ell = 93\degr}$

UBVR and UPXYZVS sequences of standard stars for the MEGA program fields along the main meridian of the Galaxy

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