Figure 2 - uploaded by Eleazar Rodrigo Carrasco
Content may be subject to copyright.
Adaptively smoothed X-ray image of MS 0440.5+0204 galaxy cluster in the 0.2-6.0 KeV energy range. The X-ray peak position coincides with galaxy 896(B). The image shows a slightly elongation, with a position angle in agreement with that obtained from strong lensing (see section 5).
Source publication
We present a parametric strong-lensing modeling of the galaxy cluster MS 0440.5+0204 (located at z = 0.19). We have performed a strong-lensing mass reconstruction of the cluster using three different models. The first model uses the image positions of four multiply imaged systems (providing 26 constraints). The second one combines strong-lensing co...
Contexts in source publication
Context 1
... final image has been smoothed with kernels with minimum scale of 0.5 arcsec and maximum scale of 5 arcsec, with a minimum signal to noise of 3 arcsec per kernel. The smoothed Chandra image of the cluster in the 0.2-6 keV energy band is shown in Figure 2. ...
Context 2
... values, and in the left panel of Fig. 10 the critical lines and the predicted positions of the images. Comparing this figure with Fig. 5, we conclude that both models recover the image positions equally well, which is consistent with their similar χ 2 / DOF (see also section §5). The 2D contours and the PDFs for the free parameters are shown in Fig. 12. We note that the model M lens-σ s produces similar critical lines and predicted positions to those for the model M lens . We obtain χ 2 / DOF = 2.5 for this second model, with the best value for the redshift of system M5 equal to z = 1.3 +0.2 −0.1 . Model M lens-σ s -mass -Finally, we include the WL mass in our last model. From our ...
Context 3
... degeneracies depicted in Figures 11, 12, and 13 are expected; and similar results have been presented previously by different authors (e.g., Jullo et al. 2007;Elíasdóttir et al. 2007). We can appreciate that the 2D contours and the best values for σ * 0 and r * cut change significantly in each model, reflecting a degeneracy in mass between the smooth cluster component and the galaxies. ...
Similar publications
Three galaxy clusters selected from the XXL X-ray survey at high redshift and low mass ( z ~ 1 and M 500 ~ 1 – 2 × 10 ¹⁴ M ⊙ ) were observed with NIKA2 to image their Sunyaev-Zel'dovich effect (SZ) signal. They all present an SZ morphology, together with the comparison with X-ray and optical data, that indicates dynamical activity related to mergin...
Radio relics are extended radio emission features which trace shock waves in the periphery of galaxy clusters originating from cluster mergers. Some radio relics show a highly polarised emission, which make relics an excellent probe for the magnetisation of the intra-cluster medium. The origin of the relic polarisation is still debated. It could be...
We present MeerKAT Fornax Survey atomic hydrogen (HI) observations of the dwarf galaxies located in the central ~2.5 x 4 deg$^2$ of the Fornax galaxy cluster. The HI images presented in this work have a $3\sigma$ column density sensitivity between 2.7 and 50 x 10$^{18}$ cm$^{-2}$ over 25 km s$^{-1}$ for spatial resolution between 4 and 1 kpc. We ar...
We study the galaxy mass-size relation in 15 spectroscopically confirmed clusters at 1.4 < z < 2.8 from the CARLA survey. Our clusters span a total stellar mass in the range 11.3 < log( M * c / M ⊙ ) < 12.6 (with an approximate halo mass in the range 13.5 ≲ log( M h c / M ⊙ ) ≲ 14.5). Our main finding is that cluster passive early-type galaxies (ET...
![Figure 3. Comparison of the DM density profile obtained by [16,17] and...](publication/360693098/figure/fig2/AS:11431281079080117@1660531970751/Comparison-of-the-DM-density-profile-obtained-by-16-17-and-the-density-profile_Q320.jpg)
In this paper, we extend the work of Freundlich et al. 2020 who showed how to obtain a Dekel–Zhao density profile with mass dependent shape parameters in the case of galaxies. In the case of Freundlich et al. 2020, the baryonic dependence was obtained using the NIHAO set of simulations. In our case, we used simulations based on a model of ours. Fol...
Citations
We present an optical study of the strong-lensing galaxy cluster MS 0440.5+0204 at z=0.19593, based on CFHT/MegaCam g′, r′ photometry and GMOS/Gemini and CFHT/MOS/SIS spectroscopy in a broader area than previous works. We have determined new spectroscopic redshifts for the most prominent gravitational arcs surrounding the central galaxy in the cluster. The new redshifts and the information provided by the photometric
catalog allow us to perform a detailed weak- and strong-lensing mass reconstruction of the cluster. The large number of member galaxies and the area covered by our observations allow us to estimate more accurately the velocity dispersion and mass of the cluster and to examine in detail the nature of the cluster and surrounding structures. The dynamical mass is in good agreement with the mass inferred from the lensing analysis and X-ray estimates. About 68% of the galaxies are located in the inner <~0.86 h^-1_70 Mpc region of the cluster. The galaxy redshift distribution in the inner region of the cluster shows a complex structure with at least three substructures along the line of sight. Other substructures are also identified in the galaxy density map and in the weak-lensing mass map. The member galaxies in the northeast overdensity are distributed in a filament between the clusters MS 0440.5+0204 and ZwCL 0441.1+0211, suggesting that these two structures might be connected. MS 0440.5 +0204 appears to be dynamically active, with a cluster core that is likely experiencing a merging process, and with other nearby groups at projected distances of <~1 h^ -1_70 Mpc that could be being accreted by the cluster.
We present an optical study of the strong-lensing galaxy cluster MS 0440.5+0204 at z=0.19593, based on CFHT/MegaCam g′, r′ photometry and GMOS/Gemini and CFHT/MOS/SIS spectroscopy in a broader area than previous works. We have determined new spectroscopic redshifts for the most prominent gravitational arcs surrounding the central galaxy in the cluster. The new redshifts and the information provided by the photometric catalog allow us to perform a detailed weak- and strong-lensing mass reconstruction of the cluster. The large number of member galaxies and the area covered by our observations allow us to estimate more accurately the velocity dispersion and mass of the cluster and to examine in detail the nature of the cluster and surrounding structures. The dynamical mass is in good agreement with the mass inferred from the lensing analysis and X-ray estimates. About 68% of the galaxies are located in the inner <~0.86 h^-1_70 Mpc region of the cluster. The galaxy redshift distribution in the inner region of the cluster shows a complex structure with at least three substructures along the line of sight. Other substructures are also identified in the galaxy density map and in the weak-lensing mass map. The member galaxies in the northeast overdensity are distributed in a filament between the clusters MS 0440.5+0204 and ZwCL 0441.1+0211, suggesting that these two structures might be connected. MS 0440.5 +0204 appears to be dynamically active, with a cluster core that is likely experiencing a merging process, and with other nearby groups at projected distances of <~1 h^ -1_70 Mpc that could be being accreted by the cluster.
