k2c9vst.photpoinivo://org.gavo.dc/k2c9vst/q/photpointsThe GAVO DC teamHundertmark, M.Korhonen, H.Jørgensen, U.Street, RPenny, M.Tsapras, Y.Dominik, M.Kerins, E.Cassan, A.Snodgrass, C.Bachelet, E.Bramich, D.Bozza, V.2026-01-16T10:35:23ZGAVO Data Centre Team

Mönchhofstrasse 12-14, D-69120 Heidelberg

gavo@ari.uni-heidelberg.de+49 6221 54 1837light-curvesexoplanetsgravitational-microlensingtime-domain-astronomy The Kepler satellite has observed the Galactic center in a campaign lasting from April until the end of June 2016 (K2/C9). The main objective of the 99 hours for the microlensing program 097.C-0261(A) using the ESO VLT Survey Telescope (VST) was to monitor the superstamp (i.e., the actually downloaded region of K2/C9) in service mode for improving the event coverage and securing some color-information. Due to weather conditions, the majority of images were taken in the red band. These are part of the present release. The exact pointing strategy was adjusted to cover the superstamp with 6 pointings and to contain as many microlensing events from earlier seasons as possible. In addition, a two-point dither was requested to reduce the impact of bad pixels and detector gaps. Consequently, some events were getting more coverage and have been observed with different CCDs. The large footprint of roughly 1 square degree and the complementary weather conditions at Cerro Paranal have lead to the coverage of 147 events (this resource's events table), but ~60 of those were already at baseline.http://archive.eso.org/wdb/wdb/eso/sched_rep_arc/query?progid=097.C-0261(A)http://dc.g-vo.org/tableinfo/k2c9vst.photpointsArchiveResearchESOVST5/7198,7216-7217,7220-7221,7226-7227,7266 6/28782-28783,28796,28798-28799,28823,28829,28854-28855,28860-28861,28863,28872-28873,28875-28877,28888-28889,28892-28893,28898,28902-28903,28920,28922-28923,29056,29058-29059,29205,29253,29255,2926156693 57663Opticaltimeseriesk2c9vst The Kepler satellite has observed the Galactic center in a campaign lasting from April until the end of June 2016 (K2/C9). The main objective of the 99 hours for the microlensing program 097.C-0261(A) using the ESO VLT Survey Telescope (VST) was to monitor the superstamp (i.e., the actually downloaded region of K2/C9) in service mode for improving the event coverage and securing some color-information. Due to weather conditions, the majority of images were taken in the red band. These are part of the present release. The exact pointing strategy was adjusted to cover the superstamp with 6 pointings and to contain as many microlensing events from earlier seasons as possible. In addition, a two-point dither was requested to reduce the impact of bad pixels and detector gaps. Consequently, some events were getting more coverage and have been observed with different CCDs. The large footprint of roughly 1 square degree and the complementary weather conditions at Cerro Paranal have lead to the coverage of 147 events (this resource's events table), but ~60 of those were already at baseline.k2c9vst.photpoints The Kepler satellite has observed the Galactic center in a campaign lasting from April until the end of June 2016 (K2/C9). The main objective of the 99 hours for the microlensing program 097.C-0261(A) using the ESO VLT Survey Telescope (VST) was to monitor the superstamp (i.e., the actually downloaded region of K2/C9) in service mode for improving the event coverage and securing some color-information. Due to weather conditions, the majority of images were taken in the red band. These are part of the present release. The exact pointing strategy was adjusted to cover the superstamp with 6 pointings and to contain as many microlensing events from earlier seasons as possible. In addition, a two-point dither was requested to reduce the impact of bad pixels and detector gaps. Consequently, some events were getting more coverage and have been observed with different CCDs. The large footprint of roughly 1 square degree and the complementary weather conditions at Cerro Paranal have lead to the coverage of 147 events (this resource's events table), but ~60 of those were already at baseline.9384accrefAccess key for the datameta.ref.urlAccess.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.Size30157792.022857.044613.0447301.0longnullabledidLocal dataset identifier for the lightcurve this point belongs to.meta.id;meta.maincharindexednullableevent_idAssociated Eventcharnullableobs_timeTime this photometry corresponds to.dtime.epoch2.45749e+062.45749e+062.45753e+062.45756e+062.45756e+061doublenullablephotSDSS r-band instrumental magnitude (warning: zeropoint may be off several mag).magphot.mag;em.opt.R15.503217.204320.206722.557128.40631doublenullableimageVST image this point was taken from. The raw images are available at http://archive.eso.org/wdb/wdb/eso/eso_archive_main/query?prog_id=097.C-0261(A)meta.ref;meta.filecharnullabledfDifference flux as defined by 2008MNRAS.386L..77Baduphot.flux-105651-43555.728.96013777.14773121doublenullablee_dfError in difference flux.adustat.error;phot.flux65.203797.5333173.61322.863535.9671floatnullablerfReference flux as defined by 2008MNRAS.386L..77Baduphot.flux421.672765.7484975.661692082986841doublenullablee_rfError in reference Fluxadustat.error;phot.flux153.848191.575509.7771185.641237.551floatnullablee_photError in SDSS r-band instrumental magnitude.magstat.error;phot.mag0.001499150.00394050.03743750.339084465.2711floatnullableexp_timeExposure time.stime.duration;obs.exposure60606060601floatnullablefwhmFWHM of the point spread function averaged over all stars on the subimage used.arcsecphys.angSize;instr.det.psf2.1142.948585.154157.022179.44961floatnullablesky_backgroundMedian sky background flux.aduinstr.background98.9249150.865236.323849.8761630.81floatnullablephot_scale_factorScale factor according to 2008MNRAS.386L..77B; if small, photometry was obtained under suboptimal atmospheric transparency.0.07110380.4321640.9721891.003931.113121floatnullablechi2_pxSee 2008MNRAS.386L..77B, sect. 2.1stat.fit.chi200.6315350.8963852.589087.913921floatnullabledxPixel offset of frame wrt. the reference frame, x directionpixelpos.cartesian.x;arith.diff-29.7382-5.58953-0.0292556.1255930.25251floatnullabledyPixel offset of frame wrt. the reference frame, y directionpixelpos.cartesian.y;arith.diff-27.6162-5.46111-0.672526.0649625.06951floatnullablecorr_coeffCoefficients of correction polynomial for frame: TBDfloatnullablek2c9vst.eventsevent_idevent_id