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2025年度

25/10/03 進捗報告

研究ログを取らないのは悪である。

📄 RGM250918.pdf

In the previous figure, there were dependencies at each mass and even crossing behaviors.

RGM250918-2

However, in the previous study (Byrne et al. 2023), the evolution of individual halos was plotted, capturing their evolutionary tracks. To align with that approach, I decided to compute the median stellar mass and BH mass at each snapshot, plot them, and connect the points with lines. This way, the figure now represents the statistical evolution of halos.

RGM250918-3

In the new figure, the previously observed phenomena disappeared, and instead, a clear transition emerged at a certain stellar mass. This result is consistent with the previous study (Byrne et al. 2023).

Using the same method, I also created a plot of stellar surface density versus BH mass.

RGM250918-4

Here too, a transition appears at a certain stellar mass, but the transition is not as cleanly aligned. In addition, I found a phenomenon where the stellar surface density decreases at low redshift. The cause of this is unknown. Considering that 700 pc is the resolution limit of this simulation, it could be due to resolution issues. Alternatively, it might reflect some physical phenomenon.

RGM250918-5

I also examined other radii. Starting from around 3 kpc, a clean transition appeared, consistent with the earlier study (Byrne et al. 2023).

Moreover, it is not yet clear why the critical density of the transition differs.

RGM250918-6

RGM250918-7

ToDo-1

image-20251003161146964

In Figure 2;

  • [ToDo-1.1] v1を消してv2の２つのCviscにする
  • [ToDo-1.2] Baron & Menard 19を消す
  • [ToDo-1.3] Χ^2を計算する
  • [ToDo-1.4] 色も変えて見やすくする
  • [ToDo-1.5] NoAGNのランも追加する（時間かかる⏱️）

ToDo-1.4

Seabornのカラーパレットを参考にしながら作成することにする。

https://seaborn.pydata.org/

RGB HEX
(0.2980392156862745, 0.4470588235294118, 0.6901960784313725) #4c72b0
(0.8666666666666667, 0.5176470588235295, 0.3215686274509804) #dd8452
(0.3333333333333333, 0.6588235294117647, 0.40784313725490196) #55a868
(0.7686274509803922, 0.3058823529411765, 0.3215686274509804) #c44e52
(0.5058823529411764, 0.4470588235294118, 0.7019607843137254) #8172b3
(0.5764705882352941, 0.47058823529411764, 0.3764705882352941) #937860
(0.8549019607843137, 0.5450980392156862, 0.7647058823529411) #da8bc3
(0.5490196078431373, 0.5490196078431373, 0.5490196078431373) #8c8c8c
(0.8, 0.7254901960784313, 0.4549019607843137) #ccb974
(0.39215686274509803, 0.7098039215686275, 0.803921568627451) #64b5cd

image-20251003174522660

ToDo-1.5

Already has the SNonly, which corresponds to NoAGN, been completed.

[z6b481@squidhpc1 CROCODILE_v2]$ diff L50N512_fiducial/param.txt L50N512_SNonly/param.txt
143,144c143,144
< AGNFeedbackEfficiency                             0.15
< AGNFeedbackTemperature                            3.16e8
---
> #AGNFeedbackEfficiency                             0.15
> #AGNFeedbackTemperature                            3.16e8

According to Oku's paper:

SNonly について

  • 考慮されるフィードバック: 超新星 (SN) フィードバックのみを実装
    • 機械的フィードバック（SN残骸が与える運動量注入）
    • SN駆動の銀河風モデル（高温ガスの放出）
  • 考慮されないもの: AGN（活動銀河核）フィードバック
  • 目的: 銀河進化における SN フィードバック単独の効果を分離して解析するためのシミュレーション設定
  • 特徴:
    • 低質量銀河では、SNフィードバックが主に星形成抑制と金属放出を担う
    • AGNによる大規模バブル（Mpcスケールの高金属ガス分布）は見られない

Target Directory:

/sqfs2/cmc/1/work/hp240141/z6a801/OsakaCosmologyDatabase/ProductionRuns_v2/L50N512_SNonly

解析結果

 wstar_bin  BH_median     BH_p16     BH_p84     N
      8.67       5.17       5.17       5.17  1455
      9.00       5.17       5.17       5.18  1213
      9.33       5.20       5.17       5.55  1081
      9.67       5.38       5.20       9.66   656
     10.00       5.59       5.26      10.03   484
     10.33       5.86       5.31      10.37   303
     10.67       6.49       5.47      10.87   182
     11.00      10.75       5.68      11.15    90
     11.33      11.12       5.94      11.55    61
     11.67      11.38       5.51      11.75    32
     12.00      11.85       5.84      12.02    12
     12.33        nan        nan        nan     0

image-20251003180655086

CROCODILE v1のSNonlyも同じような感じなので間違ってはなさそう。

# z = 0.106, a = 0.904, h = 0.67742, BoxSize = 50.00 Mpc/h, Ngroups_Total = 162216, Nsubhalos_Total = 172024
# Mstar, BH mass(median), BH mass(16%tile), BH mass(84%tile), #(gal)
 8.66667  5.17066  5.16952  5.17498     1337
 9.00000  5.17535  5.17086  5.19832     1129
 9.33333  5.22437  5.18096  7.16639     1007
 9.66667  5.44772  5.21619  9.92055      738
10.00000  5.61970  5.27336 10.15056      499
10.33333  5.92747  5.39010 10.59065      325
10.66667  6.50930  5.48358 10.89670      189
11.00000 10.84632  5.75692 11.23917      105
11.33333 11.03284  5.25487 11.48500       48
11.66667 11.22254  5.48842 11.82567       26
12.00000  9.55665  6.18686 12.15430        7
12.33333      nan      nan      nan        0

https://github.com/YuriOku/figure_introducing-crocodile/blob/main/mstar_mbh_relation/BH_z0_SNonly.dat

完成品

image-20251003182422314