========================================================================== J/AN/333/706 Bochum survey of the southern Galactic disk (Haas+, 2012) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat table2.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AN/333/706 ==========================================================================
drwxr-xr-x 7 cats archive 140 May 23 2013 [Up] drwxr-xr-x 4 cats archive 311 Sep 18 16:10 [TAR file] -rw-r--r-- 1 cats archive 476 Oct 23 2013 .message -r--r--r-- 1 cats archive 7002 Oct 23 2013 ReadMe -rw-r--r-- 1 cats archive 1027 Oct 23 2013 +footg5.gif -rw-r--r-- 1 cats archive 2592 Oct 23 2013 +footg8.gif -r--r--r-- 1 cats archive 960 May 23 2013 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 233376 May 23 2013 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/AN/333/706 Bochum survey of the southern Galactic disk (Haas+, 2012) ================================================================================ The Bochum survey of the southern Galactic disk: I. Survey design and first results on 50 square degrees monitored in 2011. Haas M., Hackstein M., Ramolla M., Drass H., Watermann R., Lemke R., Chini R. <Astron. Nachrichten, 333, 706-716 (2012)> =2012AN....333..706H ================================================================================ ADC_Keywords: Surveys ; Stars, variable ; Photometry Keywords: surveys - stars: variables: general Abstract: We are monitoring a 6deg wide stripe along the southern Galactic disk simultaneously in the r and i bands, using a robotic 15-cm twin telescope of the Universitatsternwarte Bochum near Cerro Armazones in Chile. Utilising the telescope's 2.7deg field of view, the survey aims at observing a mosaic of 268 fields once per month and to monitor dedicated fields once per night. The survey reaches a sensitivity from 10m down to 18m (AB system), with a completeness limit of r 15.5m and i 14.5m which - due to the instrumental pixel size of 2.4" - refers to stars separated by >3". This brightness range is ideally suited to examine the intermediately bright stellar population supposed to be saturated in deep variability surveys with large telescopes. To connect to deep surveys or to explore faint long term variables, coadded images of several nights reach a depth of 20m. The astrometric accuracy is better than 1", as determined from the overlap of neighbouring fields. We describe the survey design, the data properties and our procedures to derive the light curves and to extract variable stars. We present a list of 2200 variable stars identified in 50 square degrees with 50-80 observations between May and October 2011. For bright stars the variability amplitude A reaches down to A 0.05m, while at the faint end variations of A>1m are detected. About 200 stars were known to be variable, and their amplitudes and periods - as far as determinable from our six month monitoring - agree with literature values, demonstrating the performance of the Bochum Galactic Disk Survey.