Difference between revisions of "Jan 13, 2020"
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[[File:Galfield compare 1632to1832Mpc rmlambda7to200 ndmap h vectors 25a.png | 600px]] | [[File:Galfield compare 1632to1832Mpc rmlambda7to200 ndmap h vectors 25a.png | 600px]] | ||
| − | The inclusion of Redmagic galaxies may not seem to make a major difference based on the above comparison, but when comparing the stacks, it's clear that they are needed. Remaking the combined stack shown as the first plot in this post with only CMASS galaxies for orientation yields the following image. | + | The inclusion of Redmagic galaxies may not seem to make a major difference based on the above comparison, but when comparing the stacks, it's clear that they are needed. Remaking the combined stack shown as the first plot in this post with only CMASS galaxies for orientation yields the following image. |
[[File:1032 to 2032 Mpc stacked cmass 17pt8Mpc smth hess 5965cls.png | 400px]] | [[File:1032 to 2032 Mpc stacked cmass 17pt8Mpc smth hess 5965cls.png | 400px]] | ||
| + | This is clearly worse than the first plot, so including Redmagic is necessary. | ||
Revision as of 09:13, 13 January 2020
Combining stacks of different redshifts
I've written a program to take the stacks of clusters in different 200Mpc slices, resize them all to the same physical size, and stack them. Below are plots showing the stack from one slice, then adding the stacks from each successively more distant slice. This combination helps to bring out the signal. These were all done using the combined CMASS and Redmagic galaxy maps for orientation, at an ~18 Mpc smoothing scale, with the ellipticity 0 < e < 2 (more written on the ellipticity later). In order, left to right and up to down, the images below start at the 1000-1200 Mpc slice, then add and average the successive 200 Mpc stacks until the final image is the average of 5 stacks in the 1000-2000 Mpc range.
Radial profiles and looking at changes with redshift
For all the stacks which went into the above combined stack, we can decompose them into multipoles. The variation of the m=2 component with the radial coordinate, when phi=0, is shown below.
It would be interesting to make some measure of how the filamentary structure changes with redshift, e.g. in the distance range shown above. I don't know if this is possible given the SNR of the stacks, and I'm not sure about the best way to do this. We would want to compare stacks of the same number of clusters in each redshift slice. Currently, there are ~600 clusters in the 1000-1200 Mpc slice, and that number goes up with each slice to about 1200 in the 1800-2000 Mpc slice. So, say we were interested in the evolution from 2000 Mpc away until 1000 Mpc away (z~.52 to ~.24) we'd need to limit all slices to only 600 clusters per slice. Would probably want to do some random re-sampling of the clusters in each slice to get bootstrap errors.
Importance of including Redmagic galaxies
Given Bhuvnesh's warning about how the Redmagic galaxy sample is difficult to mock, we had been wondering if it is possible to do this project with orientations given by the CMASS galaxy field alone. I tested this by making stacks of the same clusters oriented using a number-density field of just the CMASS galaxies, and comparing those with the same stacks when oriented using the CMASS+Redmagic field. An example for the 1600-1800Mpc slice is shown below. White headless vectors show the orientation directions, centered on cluster positions (I haven't plotted the cluster positions themselves, to be able to see the arrows better).
The inclusion of Redmagic galaxies may not seem to make a major difference based on the above comparison, but when comparing the stacks, it's clear that they are needed. Remaking the combined stack shown as the first plot in this post with only CMASS galaxies for orientation yields the following image.
This is clearly worse than the first plot, so including Redmagic is necessary.