Access to Astronomical Catalogues

← Click to display the menu
J/MNRAS/457/1320    OGLE-III planet detection efficiency        (Tsapras+, 2016)

The OGLE-III planet detection efficiency from six years of microlensing observations (2003-2008). Tsapras Y., Hundertmark M., Wyrzykowski L., Horne K., Udalski A., Snodgrass C., Street R., Bramich D.M., Dominik M., Bozza V., Figuera Jaimes R., Kains N., Skowron J., Szymanski M.K., Pietrzynski G., Soszynski I., Ulaczyk K., Kozlowski P.Pietrukowicz S., Poleski R. <Mon. Not. R. Astron. Soc. 457, 1320 (2016)> =2016MNRAS.457.1320T (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets Keywords: gravitational lensing: micro - planetary systems Abstract: We use six years (2003-2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M{earth} The survey sensitivity to small planets is highest in the range 1-4au, shifting to slightly larger separations for more massive ones. Description: The FITS file represents the surface plotted in Figure 10, which is the main result of the paper. Each pixel value in the FITS file represents the expected number of planet detections at a specific planetary mass and orbital radius, assuming that each star surveyed has a single such planet (see figure caption for more details). The FITS file contains a world coordinate system in the header which gives coordinates to each pixel. The x coordinate is the log10(orbital radius in AU), and the y coordinate is the log 10(planet mass in Earth masses). The data product is essential for any further analysis of planet abundances using the original OGLE light curve data. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 90 1 Informations on fits file planet_matrix.fits 2880 300 Fits file
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Nx Number of pixels along X-axis 5- 7 I3 --- Ny Number of pixels along Y-axis 9- 13 F5.2 [AU] blog10(a) Lower value of orbital radius interval 15- 18 F4.2 [AU] Blog10(a) Upper value of orbital radius interval 20- 23 F4.2 [AU] dlog10(a) Resolution in orbital radius 25- 29 F5.2 --- blog10(M) Lower value of planetary mass interval in M unit 31- 33 F3.1 --- Blog10(M) Upper value of planetary mass interval in M unit 35- 38 F4.2 --- dlog10(M) Resolution in planetary mass 40- 42 I3 Kibyte size Size of FITS file 44- 61 A18 --- FileName Name of FITS file 63- 90 A28 --- Text Title of the FITS file (1)
Note (1): The FITS file represents the surface plotted in Figure 10, which is the main result of the paper. Each pixel value in the FITS file represents the expected number of planet detections at a specific planetary mass and orbital radius, assuming that each star surveyed has a single such planet (see figure caption for more details). The FITS file contains a world coordinate system in the header which gives coordinates to each pixel. The x coordinate is the log10(orbital radius in AU), and the y coordinate is the log 10(planet mass in Earth masses).
Acknowledgements: Dan Bramich,
(End) Patricia Vannier [CDS] 08-Feb-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact