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 - Matijevic, 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, Tomaz
AU - Bienayme, 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
Y1 - 2017
N2 - We characterize the selection function of RAVE using 2MASS as our underlying population, which we assume represents all stars which could have potentially been observed. We evaluate the completeness fraction as a function of position, magnitude, and color 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 4000K < 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 RAVE using 2MASS as our underlying population, which we assume represents all stars which could have potentially been observed. We evaluate the completeness fraction as a function of position, magnitude, and color 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 4000K < TEFF < 8000K and 0:5 < log g < 5:0, RAVE is kinematically and chemically unbiased with respect to expectations from Galaxia.
KW - galactic dynamics
KW - galaxies
KW - kinematics
KW - surveys
UR - http://handle.westernsydney.edu.au:8081/1959.7/uws:41324
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 -