%0 Generic %1 Muldrew2011 %A Muldrew, Stuart I. %A Croton, Darren J. %A Skibba, Ramin A. %A Pearce, Frazer R. %A Ann, Hong Bae %A Baldry, Ivan K. %A Brough, Sarah %A Choi, Yun-Young %A Conselice, Christopher J. %A Cowan, Nicolas B. %A Gallazzi, Anna %A Gray, Meghan E. %A Grützbauch, Ruth %A Li, I-Hui %A Park, Changbom %A Pilipenko, Sergey V. %A Podgorzec, Bret J. %A Robotham, Aaron S. G. %A Wilman, David J. %A Yang, Xiaohu %A Zhang, Youcai %A Zibetti, Stefano %D 2011 %K environment %T Measures of Galaxy Environment I - What is "Environment"? %U http://arxiv.org/abs/1109.6328 %X The influence of a galaxy's environment on its evolution has been studied and compared extensively in the literature, although differing techniques are often used to define environment. Most methods fall into two broad groups: those that use nearest neighbours to probe the underlying density field and those that use fixed apertures. The differences between the two inhibit a clean comparison between analyses and leave open the possibility that, even with the same data, different properties are actually being measured. In this work we apply twenty published environment definitions to a common mock galaxy catalogue constrained to look like the local Universe. We find that nearest neighbour-based measures best probe the internal densities of high-mass haloes, while at low masses the inter-halo separation dominates and acts to smooth out local density variations. The resulting correlation also shows that nearest neighbour galaxy environment is largely independent of dark matter halo mass. Conversely, aperture-based methods that probe super-halo scales accurately identify high-density regions corresponding to high mass haloes. Both methods show how galaxies in dense environments tend to be redder, with the exception of the largest apertures, but these are the strongest at recovering the background dark matter environment. We also warn against using photometric redshifts to define environment in all but the densest regions. When considering environment there are two regimes: the 'local environment' internal to a halo best measured with nearest neighbour and 'large-scale environment' external to a halo best measured with apertures. This leads to the conclusion that there is no universal environment measure and the most suitable method depends on the scale being probed.

@misc{Muldrew2011, abstract = { The influence of a galaxy's environment on its evolution has been studied and compared extensively in the literature, although differing techniques are often used to define environment. Most methods fall into two broad groups: those that use nearest neighbours to probe the underlying density field and those that use fixed apertures. The differences between the two inhibit a clean comparison between analyses and leave open the possibility that, even with the same data, different properties are actually being measured. In this work we apply twenty published environment definitions to a common mock galaxy catalogue constrained to look like the local Universe. We find that nearest neighbour-based measures best probe the internal densities of high-mass haloes, while at low masses the inter-halo separation dominates and acts to smooth out local density variations. The resulting correlation also shows that nearest neighbour galaxy environment is largely independent of dark matter halo mass. Conversely, aperture-based methods that probe super-halo scales accurately identify high-density regions corresponding to high mass haloes. Both methods show how galaxies in dense environments tend to be redder, with the exception of the largest apertures, but these are the strongest at recovering the background dark matter environment. We also warn against using photometric redshifts to define environment in all but the densest regions. When considering environment there are two regimes: the 'local environment' internal to a halo best measured with nearest neighbour and 'large-scale environment' external to a halo best measured with apertures. This leads to the conclusion that there is no universal environment measure and the most suitable method depends on the scale being probed. }, added-at = {2011-09-30T18:34:38.000+0200}, author = {Muldrew, Stuart I. and Croton, Darren J. and Skibba, Ramin A. and Pearce, Frazer R. and Ann, Hong Bae and Baldry, Ivan K. and Brough, Sarah and Choi, Yun-Young and Conselice, Christopher J. and Cowan, Nicolas B. and Gallazzi, Anna and Gray, Meghan E. and Grützbauch, Ruth and Li, I-Hui and Park, Changbom and Pilipenko, Sergey V. and Podgorzec, Bret J. and Robotham, Aaron S. G. and Wilman, David J. and Yang, Xiaohu and Zhang, Youcai and Zibetti, Stefano}, biburl = {https://www.bibsonomy.org/bibtex/2ef81a26fddb52b30243fcbf9933d05b5/miki}, description = {[1109.6328] Measures of Galaxy Environment I - What is "Environment"?}, interhash = {48d1f2edd4f1b05a42ad89a0cf5a9644}, intrahash = {ef81a26fddb52b30243fcbf9933d05b5}, keywords = {environment}, note = {cite arxiv:1109.6328 Comment: 14 pages, 9 figures, 1 table, accepted to MNRAS}, timestamp = {2011-09-30T18:34:38.000+0200}, title = {Measures of Galaxy Environment I - What is "Environment"?}, url = {http://arxiv.org/abs/1109.6328}, year = 2011 }