Table information for 'k2c9vst.photpoints'


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Resource Description: 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.

For a list of all services and tables belonging to this table's resource, see Information on resource 'Coordinated microlensing survey observations with Kepler K2/C9 using VST'

Citing this table

This table has an associated publication. If you use data from it, it may be appropriate to reference either in addition to or instead of the service reference.

To cite the table as such, we suggest the following BibTeX entry:

  title={Photometric Points Obtained by K2/C9 followup},
  author={Hundertmark, M. and Korhonen, H. and Jørgensen, U. and Street, R and Penny, M. and Tsapras, Y. and Dominik, M. and Kerins, E. and Cassan, A. and Snodgrass, C. and Bachelet, E. and Bramich, D. and Bozza, V.},
  howpublished={{VO} resource provided by the {GAVO} Data Center}


Sorted by DB column index. [Sort alphabetically]

NameTable Head DescriptionUnitUCD
accref Product key Access key for the data N/A meta.ref.url
owner Owner Owner of the data N/A N/A
embargo Embargo ends Date the data will become/became public a N/A
mime Type MIME type of the file served N/A meta.code.mime
accsize File size Size of the data in bytes byte VOX:Image_FileSize
did Dataset ID Local dataset identifier for the lightcurve this point belongs to. N/A;meta.main
event_id Event Associated Event N/A N/A
obs_time Time Time this photometry corresponds to. d time.epoch
phot m_r SDSS r-band instrumental magnitude (warning: zeropoint may be off several mag). mag phot.mag;em.opt.R
image Source VST image this point was taken from. The raw images are available at N/A meta.ref;meta.file
df Diff. Flux Difference flux as defined by 2008MNRAS.386L..77B adu phot.flux
e_df Err. DF Error in difference flux. adu stat.error;phot.flux
rf Ref. Flux Reference flux as defined by 2008MNRAS.386L..77B adu phot.flux
e_rf Err. RF Error in reference Flux adu stat.error;phot.flux
e_phot Err. m_r Error in SDSS r-band instrumental magnitude. mag stat.error;phot.mag
exp_time Exp. Time Exposure time. s time.duration;obs.exposure
fwhm FWHM FWHM of the point spread function averaged over all stars on the subimage used. arcsec phys.angSize;instr.det.psf
sky_background Sky Median sky background flux. adu instr.background
phot_scale_factor Phot. SF Scale factor according to 2008MNRAS.386L..77B; if small, photometry was obtained under suboptimal atmospheric transparency. N/A N/A
chi2_px χ²/pixel See 2008MNRAS.386L..77B, sect. 2.1 N/A
dx Δx Pixel offset of frame wrt. the reference frame, x direction [Note t] pixel pos.cartesian.x;arith.diff
dy Δy Pixel offset of frame wrt. the reference frame, y direction [Note t] pixel pos.cartesian.y;arith.diff
corr_coeff Corr. Coefficients of correction polynomial for frame: TBD [Note t] N/A N/A

Columns that are parts of indices are marked like this.


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Note t

These are the coefficients of the transformation polynoms of the reference frame to the transformed reference frame (for which the kernel is computed). The transformation equations are:

xct = c[0]*xc + c[1]*yc + dx
yct = c[2]*xc + c[3]*yc + dy

where c is given in corr_coeff, dx and dy are from the columns,