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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 90 1 Informations on fits file
planet_matrix.fits 2880 300 Fits file
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Byte-by-byte Description of file: list.dat
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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)
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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).
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Acknowledgements:
Dan Bramich,
(End) Patricia Vannier [CDS] 08-Feb-2016