TY - JOUR
T1 - The selection function of the RAVE survey
AU - Wojno, Jennifer
AU - Kordopatis, Georges
AU - Piffl, Tilmann
AU - Binney, James
AU - Steinmetz, Matthias
AU - Matijevič, Gal
AU - Bland-Hawthorn, Joss
AU - Sharma, Sanjib
AU - McMillan, Paul
AU - Watson, Fred
AU - Reid, Warren
AU - Kunder, Andrea
AU - Enke, Harry
AU - Grebel, Eva K.
AU - Seabroke, George
AU - Wyse, Rosemary F.G.
AU - Zwitter, Tomaž
AU - Bienaymé, Olivier
AU - Freeman, Kenneth C.
AU - Gibson, Brad K.
AU - Gilmore, Gerry
AU - Helmi, Amina
AU - Munari, Ulisse
AU - Navarro, Julio F.
AU - Parker, Quentin A.
AU - Siebert, Arnaud
PY - 2017/7
Y1 - 2017/7
N2 - We characterize the selection function of RAdial Velocity Experiment (RAVE) using 2 Micron All Sky Survey (2MASS) as our underlying population, which we assume represents all stars that could have potentially been observed.We evaluate the completeness fraction as a function of position, magnitude and colour in two ways: first, on a field-by-field basis, and second, in equal-size areas on the sky. Then, we consider the effect of the RAVE stellar parameter pipeline on the final resulting catalogue, which in principle limits the parameter space over which our selection function is valid. Our final selection function is the product of the completeness fraction and the selection function of the pipeline. We then test if the application of the selection function introduces biases in the derived parameters. To do this, we compare a parent mock catalogue generated using GALAXIA with a mock-RAVE catalogue where the selection function of RAVE has been applied. We conclude that for stars brighter than I = 12, between 4000 < Teff < 8000K and 0.5 < log g < 5.0, RAVE is kinematically and chemically unbiased with respect to expectations from GALAXIA.
AB - We characterize the selection function of RAdial Velocity Experiment (RAVE) using 2 Micron All Sky Survey (2MASS) as our underlying population, which we assume represents all stars that could have potentially been observed.We evaluate the completeness fraction as a function of position, magnitude and colour in two ways: first, on a field-by-field basis, and second, in equal-size areas on the sky. Then, we consider the effect of the RAVE stellar parameter pipeline on the final resulting catalogue, which in principle limits the parameter space over which our selection function is valid. Our final selection function is the product of the completeness fraction and the selection function of the pipeline. We then test if the application of the selection function introduces biases in the derived parameters. To do this, we compare a parent mock catalogue generated using GALAXIA with a mock-RAVE catalogue where the selection function of RAVE has been applied. We conclude that for stars brighter than I = 12, between 4000 < Teff < 8000K and 0.5 < log g < 5.0, RAVE is kinematically and chemically unbiased with respect to expectations from GALAXIA.
KW - Galaxy: abundances
KW - Galaxy: fundamental parameters
KW - Galaxy: kinematics and dynamics
KW - Methods: data analysis
UR - http://www.scopus.com/inward/record.url?scp=85021721311&partnerID=8YFLogxK
U2 - 10.1093/mnras/stx606
DO - 10.1093/mnras/stx606
M3 - Article
SN - 0035-8711
VL - 468
SP - 3368
EP - 3380
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -