4.2 Environmental Effect on Properties of Galaxies
4.2.3 LSS by SSFF on Properties of Galaxies
Finally, we study the Small-Scale-Filament Factor (SSFF) effect on properties of galax-ies. We separate three different SSFF regions, High SSFF, Middle SSFF, and Low SSFF, shows in solid line, dash line, and dot line, respectively, that detail see§ 3.2.
Here we have no expectation, where K-S tests are compare between each others of different SSFF regions, and taking the p-value of K-S test, which to explain the level of similarity.
Figure 4.37 and 4.38, are the correlation of SSFF and color. Three different SSFF regions are solid line, dash line, and dot line, those are correspond to High SSFF, Middle SSFF, and Low SSFF.
We can see the solid line shift to right side, dot line close to left side. close to right side means trend to red color. We also calculate and present this property’s p-value which is from K-S test of High SSFF versus Low SSFF.
It means the High SSFF galaxies are redder then the low SSFF galaxies, the KS-test shows they are unlikely(p < 0.0001).
In Figure 4.39 and 4.40, shows the correlation of SSFF and Stellar mass, & correlation of SSFF and dynamical mass. We also calculate and present this property’s p-value which is from K-S test of High SSFF galaxies versus Low SSFF galaxies.
We found the red line trend to right side, green line close to left side. the K-S test of dynamical mass shows that are from different host population(p < 0.01). Its means SSFF have a significantly effect on dynamical mass, but only have a weak effect on stellar mass(0.02 < p < 0.03).
Figure 4.41 are correlation of SSFF and Dark matter, there still are no correlation.
However, we found the EW[OII] of Middle SSFF and Low SSFF which are very unlikely(p < 0.01). Moreover, on sSFR, High SSFF and Middle SSFF that both versus Low SSFF, shows all from different host population(p < 0.004).
It means sSFR and SSFF are strongly correlated, when SSFF larger than a threshold, that sSFR will be different.
0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 g
−r (Absolute magnitude)
0.0
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.37: The figure shows the cumulative distribution of g−r color of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type. We can see the High SSFF type shift to right, it means the High SSFF type galaxies are redder then the Low SSFF type galaxies, the KS-test shows them is unlikely(p < 0.01).
0 1 2 3 4 5 6 u
−r (Absolute magnitude)
0.0
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.38: The figure shows the cumulative distribution of u− r color of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this prop-erty’s p-value, which is from K-S test of between each SSFF type. We can see the High SSFF type shift to right, it means the High SSFF type galaxies are redder then the Low SSFF type galaxies, the KS-test shows them is unlikely (p < 0.01).
10
810
910
1010
1110
12Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.39: The figure shows the cumulative distribution of Stellar mass of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type. We find the stellar mass in the High SSFF type galaxies are bigger than Low SSFF type galaxies, but the KS-test shows their correlation are weak (p < 0.02).
10
1310
1410
1510
1610
1710
18Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.40: The figure shows the cumulative distribution of Dynamical mass of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type. We find the dynamical mass in the High SSFF type galaxies are bigger than Low SSFF type galaxies, the KS-test shows they are from different parent population (p < 0.01).
10
210
310
410
510
610
710
8M
dyn,r,P/M
∗0.0 0.2 0.4 0.6 0.8 1.0 1.2
Cumulative Frequency
High vs. Mid KS-test(p)=
0.1656
High vs. Low KS-test(p)=
0.0683
Mid vs. Low KS-test(p)=
0.2936
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.41: The figure shows the cumulative distribution of Dynamical mass/Stellar mass of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type.
0 10
110
2EW[OII]
3729[ ]
0.0 0.2 0.4 0.6 0.8 1.0 1.2
Cumulative Frequency
High vs. Mid KS-test(p)=
0.7447
High vs. Low KS-test(p)=
0.03 Mid vs. Low KS-test(p)=
0.0136
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.42: The figure shows the cumulative distribution of [OII] equivalent width of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type.
10
110
210
3EW[H α ] [ ]
0.0 0.2 0.4 0.6 0.8 1.0 1.2
Cumulative Frequency
High vs. Mid KS-test(p)=
0.8788
High vs. Low KS-test(p)=
0.0612
Mid vs. Low KS-test(p)=
0.0428
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.43: The figure shows the cumulative distribution of Halpha equivalent width of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type.
0 10
110
2EW[H β ] [ ]
0.0 0.2 0.4 0.6 0.8 1.0 1.2
Cumulative Frequency
High vs. Mid KS-test(p)=
0.8826
High vs. Low KS-test(p)=
0.0824
Mid vs. Low KS-test(p)=
0.0069
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.44: The figure shows the cumulative distribution of Hbeta equivalent width of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type.
13 12 11 10 9 8
Quantitative definition of SSS by "SSFF"
High SSFF Mid SSFF Low SSFF
Figure 4.45: The figure shows the cumulative distribution of sSFR of galaxies for each SSFF type. Solid line, dash line, and dot line, are correspond to High SSFF, Middle SSFF, and Low SSFF type galaxies, respectively. We also calculate and present this property’s p-value, which is from K-S test of between each SSFF type. In sSFR, Low SSFF type galaxies have stronger sSFR than High, and Middle SSFF type, that KS-test are smaller than (P < 0.004).
Summary & Discussion
We have developed quantitative methods to objectively characterize the large-scale structure of the universe surrounding galaxies, to qualitatively investigate the relation be-tween the properties of galaxies and their large-scale environments.
The environments are characterized by:
(1) The conventional Spherical Density which we measure it using the aperture equiv-alent to the distance of the 5th closest neighbor (typically 2-5 Mpc), and
(2) MAD (Multi-Axis Density) that utilize ”square” aperture in 13 axes of the scale close to 10 Mpc. On the basis of MAD, we further develop ”Large-Scale-Filament Factor (LSFF)” that are designed to be more sensitive to the larger and elongated structure of the universe, such as large-scale filament.
Additionally, by combining LSFF and the conventional Spherical Density, we further develop the measure called ”Small-Scale-Filament Factor (SSFF)” that is seemingly sen-sitive the filamentary structure of a scale smaller than what we can characterize by MAD and comparable to the scale associated with the Spherical Density.
Our results are:
(1) We find a significant correlation between colour of galaxies and MAD, as well as the Spherical Density in such way that red galaxies exist more in the crowded region.
(2) We find a significant correlation between the stellar mass of galaxies and MAD, as well as the Spherical Density.
(3) We find a significant correlation between the dynamical mass and MAD; however, no correlation with the Spherical Density.
(4) We find a significant correlation between the equivalent with of Halpha, Hbeta, and OII of galaxies and MAD, as well as the Spherical Density.
(5) We find a significant correlation between colour of galaxies and Small-Scale-Filament Factor.
(6) We find a weak correlation between the stellar mass of galaxies and Small-Scale-Filament Factor.
(7) We find a significant correlation between dynamical mass of galaxies and Small-Scale-Filament Factor.
(8) We find a significant correlation between the specific star formation rate (sSFR) of galaxies and Small-Scale-Filament Factor.
Our conclusions are as follows:
(1) The red galaxies exist preferably inside the high Spherical Density region, that is a manifestation of the well known ”morphology versus density” relation. (consistent with Dressler, Thompson & Shectman 1985; Couch & Sharples 1987; Balogh et al. 1997, 1998, 1999, 2002; Hashimoto et al. 1998; Poggianti et al. 1999; Couch et al. 2001; Solanes et al. 2001; Lewis at al. 2002a; Gomez et al. 2002)
(2) The red galaxies also exist preferably inside the large-scale filament (typically larger than 10 Mpc), consistent with Grogin & Geller (1999), and Rojas et al. (2004) claiming that their red galaxy fraction is high inside their subjectively defined ”filament”.
(3) In the low Spherical Density region, meanwhile, the red galaxies tend to be defi-cient, only when there is no ”small scale filament” of the 2 Mpc scale.
In general, galaxies apparently get influenced by both large and small-scale
environ-even smaller scale local environments will be needed.
It should be also noted that our sample only uses the box of the scale with 40 Mpc, so, the interpretation of our result has to be in the cautious manner, because our result may well be a consequence of the cosmic variance. Further studies with much bigger sample of galaxies should be conducted in the future. About the SSFF, although that remove the Spherical Density effect but that still seems contain the LSFF effect. We will solve this problem by some way, like try to use smaller aperture of MAD then fit the correlation of its result and SSFF, further to find the truly SSFF.
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