1. From: The evolution of star formation activity in galaxy groups
Figure 2. The left-hand panels show SFR_IR versus SFR_SED colour-coded by stellar mass before re-calibration for EGS, COSMOS and GOODS-S from top to bottom, respectively. The middle panels show corresponding SFR_IR versus re-calibrated SFR_SED. The dashed line shows the one-to-one relation. The right-hand panels show the histogram of corresponding SFR_IR–SFR_SED. The black and red histograms show before (black) and after (red) re-calibration.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

2. From: The evolution of star formation activity in galaxy groups
Figure 1. L_X–σ relation for X-ray groups. The dashed blue line shows our expectation for the L_X–σ relation from scaling relations (Leauthaud et al. 2010) and the solid red line is our bisector fit to data.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

3. From: The evolution of star formation activity in galaxy groups
Figure 3. Left-hand panel: spectroscopic completeness per stellar mass bin in the low-redshift sample (black histogram) and in the simulated ‘incomplete’ mock catalogue (red line) in the same redshift range. Right-hand panel: spectroscopic completeness per SFR bin for the low-redshift sample (black histogram) and in the simulated ‘incomplete’ mock catalogue (red line).
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

4. From: The evolution of star formation activity in galaxy groups
Figure 4. M₂₀₀ versus redshift for the final sample of galaxy groups in our analysis. The vertical dashed line separates low-z and high-z sample.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

5. From: The evolution of star formation activity in galaxy groups
Figure 8. Velocity dispersion from gapper estimator versus true velocity dispersion for mock groups. The orange points show the choice of constant initial velocity dispersion and the green one is based on the initial velocity dispersion computed from M₂₀₀.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

6. From: The evolution of star formation activity in galaxy groups
Figure 5. Spectroscopic completeness for different fields in R-band magnitude. We use v-band magnitude for GOODS-N.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

7. From: The evolution of star formation activity in galaxy groups
Figure 6. Completeness and contamination level of the member galaxies using the gapper estimator method with initial condition from M₂₀₀ (grey points) and M₂₀₀ with error (orange points) in the mock catalogue. The right-hand panels show corresponding histograms. The solid lines in the histograms show galaxies with M_* > 10¹⁰ M_⊙ and the dashed histograms are related to the whole sample.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

8. From: The evolution of star formation activity in galaxy groups
Figure 7. Distribution of the residuals of the logarithm of the ‘true’ and ‘observed’ velocity dispersion. The blue histogram shows the distribution of the residuals obtained from the original mock catalogues. The red histogram shows the distribution obtained if we take into account the error on M₂₀₀ derived from L_X as done in the real data set. The green histogram shows the same diagram but with the ‘observed’ velocity dispersion estimated on the basis of the ‘incomplete’ mock catalogue.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

9. From: The evolution of star formation activity in galaxy groups
Figure 9. From left to right, ‘true’ values of total SFR, total stellar masses and halo occupation number of the groups versus our estimates in the ‘incomplete catalogues’ with the same level of spectroscopic incompleteness of the surveys used in this work.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

10. From: The evolution of star formation activity in galaxy groups
Figure 16. Fraction of star-forming galaxies versus velocity dispersion for groups in the high-z sample with more than 10 spectroscopic members. The magenta line is the upper envelope of Poggianti et al. (2006) for the EDisCS clusters and groups at z = 0.4–0.8. The horizontal blue line and the shaded blue area show the median fraction of star-forming galaxies and its corresponding 1σ error in low-z groups.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

11. From: The evolution of star formation activity in galaxy groups
Figure 10. ΣSFR– (upper panel), HOD– (middle panel) and ΣM_*– (bottom panel) M₂₀₀ relations for member galaxies with M_* > 10¹⁰ M_⊙ in the low-z sample (0.15 < z < 0.5, in blue) and the high-z groups (0.5 < z < 1.1, in red). The blue and red lines show the best-fitting relations using the ordinary least-squares regression method presented by Akritas & Bershady (1996). The total SF activity in high-z groups is higher with respect to the low-z sample at any mass by 0.8 ± 0.12 dex. The HOD– and ΣM_*–M₂₀₀ are consistent with a linear relation in both redshift bins with no evolution since z ∼ 1.1.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

12. From: The evolution of star formation activity in galaxy groups
Figure 13. Normalized distribution of differences between MS SFR and observed SFR of member galaxies (ΔSFR). The red vertical lines show our limit for separation of MS member galaxies.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

13. From: The evolution of star formation activity in galaxy groups
Figure 14. Fraction of star-forming galaxies as a function of halo mass for the low-z sample with more than 10 members (blue points) and less than 10 members (in grey). The Spearman test confirms no correlation for this sample.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

14. From: The evolution of star formation activity in galaxy groups
Figure 15. Fraction of star-forming galaxies as a function of halo mass for the high-z sample with more than 10 members (red points) and less than 10 members (in grey). The Spearman test confirms a significant anticorrelation for the this sample.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

15. From: The evolution of star formation activity in galaxy groups
Figure 11. ΣSFR– (left-hand panel), HOD– (middle panel) and ΣM_*- (right-hand panel) M₂₀₀ relations for a subsample of Yang et al. (2007) optically selected catalogue at z < 0.085 (grey points). The magenta points connected by the solid line show the median per bin of M₂₀₀ in the Yang et al. (2007) subsample. The blue solid lines show the best-fitting relation of our low-z sample and the red solid lines show the best-fitting relation of our high-z group sample. The ΣSFR and total mass of the nearby groups are strongly correlated. We do not see, however, a simple linear correlation in the log–log space but a double slope, flatter ($\Sigma {{\rm SFR}} \propto M_{200}^{0.56\pm 0.01}$) at M₂₀₀ < 10¹³ M_⊙ and steeper ($\Sigma {{\rm SFR}} \propto M_{200}^{0.89\pm 0.03}$) at M₂₀₀ > 10¹³ M_⊙.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

16. From: The evolution of star formation activity in galaxy groups
Figure 12. Mean SFR as a function of redshift. Black points show the mean of SFR for galaxies in the whole galaxy population and the red points and the error bars indicate the mean SFR in bins of redshift and respective errors in the mean.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

17. From: The evolution of star formation activity in galaxy groups
Figure 17. ΣSFR– (upper panel), HOD– (middle panel) and ΣM_*– (bottom panel) M₂₀₀ relations for the groups with 0 < z < 0.5 (in red) and 0.5 < z < 1 (in blue) and with 1 < z < 2 (in grey) for the mock catalogue. The dashed lines show the results based on the observations.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

18. From: The evolution of star formation activity in galaxy groups
Figure 18. SFR as a function of stellar mass for the member galaxies in the mock catalogue. The red points show the position of the MS for the lowest redshift (z = 0, 0.5 and 1 from left to right, respectively) in each bin.
From: The evolution of star formation activity in galaxy groups
Mon Not R Astron Soc. 2014;445(3): doi: /mnras/stu1883
Mon Not R Astron Soc | © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society