meeting 2023 09 21 n57 - JacobPilawa/TriaxSchwarzschild_wiki_5 GitHub Wiki

Environments of Massive Ellipticals

List

  • I ended up taking the Saglia+2016 dataset, and filtered for all black holes with M>3e9 Msun:

    • A1836
    • NGC3842
    • NGC4486
    • NGC4649
    • NGC4889
    • NGC6086
    • NGC1407
    • NGC1550
    • NGC3091
    • NGC5328
    • NGC5419
    • NGC5516
    • NGC0057 (added at the end)

  • I queried 2MASS HDC for number of group members (some of the galaxies above didn't appear in the catalog, so I had to supplement with additional constrained cone searches (unless there is a different best practice?))

  • And here's a plot showing the results from the NED Constrained Cone Search but for the galaxies above -- NGC 57 is certainly the most isolated when considering only the small constrained cone searches, but remains in the top 3 lowest numbers of neighbors when expanding beyond the lower sets of bins.

Plot
Galaxy Constrained Cone Search Number of Group Members Listed in HDC
A1836 images/230921/Screenshot 2023-09-21 at 10.59.56 AM.png Not listed as part of a group but this is a cluster BCG...
NGC3842 images/230921/Screenshot 2023-09-21 at 10.59.58 AM.png N=42
NGC4486 images/230921/Screenshot 2023-09-21 at 11.00.50 AM.png N=205
NGC4649 images/230921/Screenshot 2023-09-21 at 11.00.52 AM.png N=205
NGC4889 images/230921/Screenshot 2023-09-21 at 11.00.55 AM.png N=49
NGC6086 images/230921/Screenshot 2023-09-21 at 11.00.57 AM.png Not listed in HDC...but is BCG of A2162
NGC1407 images/230921/Screenshot 2023-09-21 at 11.01.08 AM.png N=42
NGC1550 images/230921/Screenshot 2023-09-21 at 11.01.09 AM.png N=15
NGC3091 images/230921/Screenshot 2023-09-21 at 11.01.10 AM.png N=7
NGC5328 images/230921/Screenshot 2023-09-21 at 11.01.12 AM.png N=6
NGC5419 images/230921/Screenshot 2023-09-21 at 11.01.13 AM.png N=32
NGC5516 images/230921/Screenshot 2023-09-21 at 11.01.16 AM.png N=6
NGC0057 images/230921/Screenshot 2023-09-21 at 11.01.18 AM.png Only listed in LDC...has N=4 for LDC

N57 Diagnostic Plots

Plot of bin centers for the current binning scheme we are using. Note that we have already removed any of the Mitchell bins which overlap with the GMOS data.
Plot
  • I've also tried to narrow down the difference between mine and Irina's sigma profiles, but I think the discrepency we saw last time is largely an artefact of the plotting. I've gone ahead and plotted a few iterations of the sigma profile below, and Irina's data does seem to have the same discrepency at the GMOS-->Mitchell boundary as I seem to have, but mine is exaggerated largely because of how I am plotting the data, I believe.
First, here are the kinematics before and after point symmetrizations
Plot GMOS Only Mitchell Only
And here are some comparsions to Irina's data -- I can't plot them in the same 1-to-1 style because we're using different binning schemes, but I think largely these data look consistent except for maybe the region near the very center?
All Kinematics Mitchell Only Irina's Input
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