==========================================================================
J/other/PASA/35.7 Long-term BVRI photometry of V2492 Cygni (Ibryamov+, 2018)
The following files can be converted to FITS (extension .fit or fit.gz)
table1.dat
==========================================================================
Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/other/PASA/35.7
==========================================================================
drwxr-xr-x 31 cats archive 4096 Mar 21 2023 [Up]
drwxr-xr-x 3 cats archive 248 Jan 12 2023 [TAR file]
-rw-r--r-- 1 cats archive 472 Dec 19 2022 .message
-r--r--r-- 1 cats archive 6073 Jan 3 2019 ReadMe
-r--r--r-- 1 cats archive 11401 Jan 2 2019 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :J/other/PASA/35.7 Long-term BVRI photometry of V2492 Cygni (Ibryamov+, 2018)
================================================================================
V2492 Cygni: Optical BVRI Variability During the Period 2010-2017.
Ibryamov S.I., Semkov E.H., Peneva S.P.
<Publ. Astron. Soc. Australia, 35, 7 (2018)>
=2018PASA...35....7I (SIMBAD/NED BibCode)
================================================================================
ADC_Keywords: Stars, variable ; Stars, pre-main sequence ; Photometry, UBVRI
Keywords: stars: pre-main sequence - stars: individual: V2492 Cygni
Abstract:
Results from BVRI photometric observations of the young stellar object
V2492 Cyg collected during the period from August 2010 to December
2017 are presented. The star is located in the field of the Pelican
Nebula and it was discovered in 2010 due to its remarkable increase in
the brightness by more than 5mag in R-band. According to the first
hypothesis of the variability, V2492 Cyg is an FUor candidate. During
subsequent observations, it was reported that the star shows the
characteristics inherent to EXor- and UXor-type variables. The optical
data show that during the whole time of observations the star exhibits
multiple large amplitude increases and drops in the brightness. In the
beginning of 2017, we registered a significant increase in the optical
brightness of V2492 Cyg, which seriously exceeds the maximal
magnitudes registered after 2010.
Description:
BVRI photometric data of V2492 Cyg collected during the period from
August 2010 to December 2017 are presented. The CCD observations were
carried out with the 2-m Ritchey-Chretien-Coude, the 50/70-cm Schmidt
and the 60-cm Cassegrain telescopes administered by Rozhen National
Astronomical Observatory in Bulgaria and the 1.3-m Ritchey-Chretien
telescope administered by Skinakas Observatory in Greece. The
technical parameters and specifications for the cameras used, the
observational procedure, and the data reduction process are given in
Ibryamov et al. (2015PASA...32...21I, Cat. J/other/PASA/32.21. All
frames were taken through a standard Johnson-Cousins set of filters.
All data were analysed using the same aperture, which was chosen to
have a 4-arcsec radius, while the background annulus was taken from 9
to 14-arcsec. The magnitudes of V2492 Cyg from all CCD frames are
measured with the standard stars reported in the current paper. The
average value of the errors in the reported magnitudes is 0.01-0.02mag
for the I- and R-band data, 0.01-0.03mag for the V-band data, and
0.02-0.04mag for the B-band data.
Objects:
--------------------------------------------------
RA (2000) DE Designation(s)
--------------------------------------------------
20 51 26.23 +44 05 23.9 V2492 Cyg = PTF 10nvg
--------------------------------------------------