bgds2.matchedivo://org.gavo.dc/bgds/l2/matcheddoi:10.21938/dChYyzuCGA00rsfzfQ8v:QThe GAVO DC teamBlex, J.Hackstein, M.Westhues, C.Ramolla, M.Demleitner, M.Fein, C.Chini, R.2026-04-07T10:09:44ZGAVO Data Centre Team

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gavo@ari.uni-heidelberg.de+49 6221 54 1837surveysgalaxy-planesmilky-way-galaxyvariable-starsbroad-band-photometrytime-domain-astronomy Median photometry in U, B, V, z, r, and i broadbands as well as the narrow bands OIII, NB, Halpha and SII for particular objects; all measurements have been matched to the nearest Gaia DR3 object. For the raw measurements, see the bgds2.phot_all table and the medphot service. 2026AN....34770087Bhttps://dc.g-vo.org/tableinfo/bgds2.matchedSurveyResearchIsNewVersionOfBGDS light curves DR1Universitätssternwarte Bochum near Cerro ArmazonesRobotic Bochum Twin Telescope (RoBoTT)3/336,338,450-451,461,472,591-592,613,615,621,651-652,659,662-663 4/1301,1303,1358,1376-1377,1379-1380,1382,1794,1816,1818-1819,1822-1823,1829,1840-1841,1892,1894,1897,2327,2333,2335,2357-2359,2376,2378,2400,2402,2408,2492-2493,2495,2528,2530,2536,2538,2591,2599,2601-2603,2612-2614,2616,2634-2635,2643,2646-2647,2656-2657,2688-269055439 58751.41.777e-19 6.621e-19Opticaltimeseriesbgds2 From the Bochum Galactic Disk Survey, time series have been obtained in the r and i bands on an (up to) nightly basis. Depending on the field, the time series contain up to more than 300 nights over 9 years. Each measurement in r and i represents the averaged flux over 10 minutes of observation (from 9 averaged 10s images). Additionally, intermittent measurements in Johnson UVB, Sloan z and the narrowbands OIII, NB, Halpha and SII have been recorded as well. The Bochum Galactic Disk Survey is a project to monitor the stellar content of the Galactic disk in a 6 degree wide stripe centered on the Galactic plane. The data has been recorded from September 2010 to September 2019 in Sloan r and i simultaneously with the Robotic Bochum Twin Telescope (RoBoTT) at the Universitaetssternwarte Bochum near Cerro Armazones in the Chilean Atacama desert. It contains measurements of about 2x10^7 stars over nine years. The source images are available from ivo://org.gavo.dc/bgds/q/sia.bgds2.matched Median photometry in U, B, V, z, r, and i broadbands as well as the narrow bands OIII, NB, Halpha and SII for particular objects; all measurements have been matched to the nearest Gaia DR3 object. For the raw measurements, see the bgds2.phot_all table and the medphot service. 22000000raICRS RA of the object, obtained as the median of all RA measurements of all r and i measurements. If there are no r and i positions, this is the median of the positions from all filters.degpos.eq.ra;meta.maindoubleindexednullabledecICRS Declination of the object, obtained as the median of all declination measurements of all r and i measurements. If there are no r and i positions, this is the median of the positions from all filters.degpos.eq.dec;meta.maindoubleindexednullablegdr3_idGaia DR3 source_id of this object.meta.id;meta.main29296384285929734403.0276701637698514e+185.334893060128903e+186.053414365808342e+1860709987389031877120.99951667longindexednullablei_med_magMedian magnitude in SDSS i'magphot.mag;em.opt.Ifloatnullableerr_i_med_magUncertainty in i_med_magmagstat.error;phot.mag;em.opt.Ifloatnullablei_fluxMedian flux in SDSS i'mJyphot.flux;em.opt.Ifloatnullableerr_i_fluxUncertainty in i_fluxmJystat.error;phot.flux;em.opt.Ifloatnullabler_med_magMedian magnitude in SDSS r'magphot.mag;em.opt.rfloatnullableerr_r_med_magUncertainty in r_med_magmagstat.error;phot.mag;em.opt.rfloatnullabler_fluxMedian flux in SDSS r'mJyphot.flux;em.opt.rfloatnullableerr_r_fluxUncertainty in r_fluxmJystat.error;phot.flux;em.opt.rfloatnullableha_med_magMedian magnitude in Astrodon Halphamagphot.mag;em.line.halphafloatnullableerr_ha_med_magUncertainty in ha_med_magmagstat.error;phot.mag;em.line.halphafloatnullableha_fluxMedian flux in Astrodon HalphamJyphot.flux;em.line.halphafloatnullableerr_ha_fluxUncertainty in ha_fluxmJystat.error;phot.flux;em.line.halphafloatnullablenb_med_magMedian magnitude in Astrodon NBmagphot.mag;em.linefloatnullableerr_nb_med_magUncertainty in nb_med_magmagstat.error;phot.mag;em.linefloatnullablenb_fluxMedian flux in Astrodon NBmJyphot.flux;em.linefloatnullableerr_nb_fluxUncertainty in nb_fluxmJystat.error;phot.flux;em.linefloatnullableoiii_med_magMedian magnitude in Astrodon OIIImagphot.mag;em.line.oiiifloatnullableerr_oiii_med_magUncertainty in oiii_med_magmagstat.error;phot.mag;em.line.oiiifloatnullableoiii_fluxMedian flux in Astrodon OIIImJyphot.flux;em.line.oiiifloatnullableerr_oiii_fluxUncertainty in oiii_fluxmJystat.error;phot.flux;em.line.oiiifloatnullablesii_med_magMedian magnitude in Astrodon SIImagphot.mag;em.linefloatnullableerr_sii_med_magUncertainty in sii_med_magmagstat.error;phot.mag;em.linefloatnullablesii_fluxMedian flux in Astrodon SIImJyphot.flux;em.linefloatnullableerr_sii_fluxUncertainty in sii_fluxmJystat.error;phot.flux;em.linefloatnullableb_med_magMedian magnitude in Johnson Bmagphot.mag;em.opt.bfloatnullableerr_b_med_magUncertainty in b_med_magmagstat.error;phot.mag;em.opt.bfloatnullableb_fluxMedian flux in Johnson BmJyphot.flux;em.opt.bfloatnullableerr_b_fluxUncertainty in b_fluxmJystat.error;phot.flux;em.opt.bfloatnullableu_med_magMedian magnitude in Johnson Umagphot.mag;em.opt.Ufloatnullableerr_u_med_magUncertainty in u_med_magmagstat.error;phot.mag;em.opt.Ufloatnullableu_fluxMedian flux in Johnson UmJyphot.flux;em.opt.Ufloatnullableerr_u_fluxUncertainty in u_fluxmJystat.error;phot.flux;em.opt.Ufloatnullablev_med_magMedian magnitude in Johnson Vmagphot.mag;em.opt.Vfloatnullableerr_v_med_magUncertainty in v_med_magmagstat.error;phot.mag;em.opt.Vfloatnullablev_fluxMedian flux in Johnson VmJyphot.flux;em.opt.Vfloatnullableerr_v_fluxUncertainty in v_fluxmJystat.error;phot.flux;em.opt.Vfloatnullablez_med_magMedian magnitude in SDSS z'magphot.mag;em.opt.Ifloatnullableerr_z_med_magUncertainty in z_med_magmagstat.error;phot.mag;em.opt.Ifloatnullablez_fluxMedian flux in SDSS z'mJyphot.flux;em.opt.Ifloatnullableerr_z_fluxUncertainty in z_fluxmJystat.error;phot.flux;em.opt.Ifloatnullablevar1 if at least one of the r or i light curves was classified as variable. 0 otherwise. The variability analysis is done only for r and i.meta.code;src.var00.00.00.011.0shortnullablesptSpectral type estimated via UBV photometry, the reddening path (from 1956ApJ...124..367H), and the fiducial colours per spectral type (from Tab. 1-2 in 1970A&A.....4..234F). This is only given where UBV photometry is available and the reddening path as a unique intersection with the spectral type.src.sptypecharnullable