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101. X-ray and strong lensing mass estimate of MS2137.3-2353

Author

Donnarumma, Annamaria, Ettori, Stefano, Meneghetti, Massimo, and Moscardini, Lauro

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present new mass estimates of the galaxy cluster MS2137.3-2353, inferred from X-ray and strong lensing analyses. This cluster exhibits an outstanding strong lensing configuration and indicates a well-relaxed dynamical state, being most suitable for a mass reconstruction which combines both techniques. Despite this, several previous studies have claimed a significant discrepancy between the X-ray and the strong lensing mass estimates. The primary aim of this paper is to address and explain this mismatch. For this purpose, we have analysed Chandra observations to recover the profiles of the intra-cluster medium properties and, assuming a functional form for the matter density, the total mass distribution. The notable strong-lensing features of MS2137.3 allow us to reconstruct its projected mass in the central regions with good accuracy, by taking advantage of the lensing inversion code Lenstool. We find a good agreement between our X-ray and strong lensing mass estimates for MS2137, leading to a mean, extrapolated value of M_200 ~ 4.4 +/- 0.3*10^14 M_sun, under the assumption of the Navarro-Frenk-White (NFW) density profile. However, the strong lensing mass estimate is affected by the details of the BCG mass modeling. In particular, we do not find evidence for a high concentration for the NFW density profile, as reported in some earlier works., Comment: 13 pages, 9 figures; resubmitted to MNRAS, including the referee's comments

Published
2009
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102. Probing the small-scale structure of the intergalactic medium with ESPRESSO: spectroscopy of the lensed QSO UM673.

Author

Cristiani, Stefano, Cupani, Guido, Trost, Andrea, D'Odorico, Valentina, Guarneri, Francesco, Lo Curto, Gaspare, Meneghetti, Massimo, Di Marcantonio, Paolo, Faria, João P, González Hernández, Jonay I, Lovis, Christophe, Martins, Carlos J A P, Milaković, Dinko, Molaro, Paolo, Murphy, Michael T, Nunes, Nelson J, Pepe, Francesco, Rebolo, Rafael, Santos, Nuno C, and Schmidt, Tobias M

Subjects
INTERSTELLAR medium, ESPRESSO, DARK matter, QUASARS, SPECTROMETRY, SIGNAL-to-noise ratio, GRAVITATIONAL lenses
Abstract

The gravitationally lensed quasar J014516.6-094517 at z  = 2.719 has been observed with the ESPRESSO instrument at the ESO VLT to obtain high-fidelity spectra of the two images A and B with a resolving power R  = 70 000. At the redshifts under investigation (2.1 ≲ z ≲ 2.7), the Lyman forests along the two sightlines are separated by sub-kiloparsec physical distances and exhibit a strong correlation. We find that the two forests are indistinguishable at the present level of signal-to-noise ratio and do not show any global velocity shift, with the cross-correlation peaking at Δ v  = 12 ± 48 |$\rm m~s^{-1}$|⁠. The distribution of the difference in velocity of individual Ly α features is compatible with a null average and a mean absolute deviation of 930 |$\rm m~s^{-1}$|⁠. Significant differences in N H  i column density are not detected, putting a limit to the RMS fluctuation in the baryon density on ≲1 proper kpc scales of Δρ/ρ ≲ 3 per cent. On the other hand, metal lines show significant differences both in velocity structure and in column density. A toy model shows that the difference in velocity of the metal features between the two sightlines is compatible with the motions of the baryonic component associated with dark matter haloes of typical mass M ≃ 2 × 1010 M⊙, also compatible with the observed incidence of the metal systems. The present observations confirm the feasibility of the Sandage test of the cosmic redshift drift with high-fidelity spectroscopy of the Lyman forest of distant, bright quasars, but also provide an element of caution about the intrinsic noise associated with the usage of metal features for the same purpose. [ABSTRACT FROM AUTHOR]

Published
2024
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103. The Three Hundred: Msub–Vcirc relation.

Author

Srivastava, Atulit, Cui, Weiguang, Meneghetti, Massimo, Dave, Romeel, Knebe, Alexander, Ragagnin, Antonio, Giocoli, Carlo, Calura, Francesco, Despali, Giulia, Moscardini, Lauro, and Yepes, Gustavo

Subjects
DARK matter, GRAVITATIONAL lenses, PHYSICAL cosmology, REDSHIFT, SUPERNOVAE, GALAXY clusters
Abstract

In this study, we investigate a recent finding based on strong lensing observations, which suggests that the sub-haloes observed in clusters exhibit greater compactness compared to those predicted by ΛCDM simulations. To address this discrepancy, we compare the cumulative sub-halo mass function and the M sub– V circ relation between observed clusters and 324 simulated clusters from |$\rm \small {The\,Three\,\,Hundred}$| project, focusing on the hydrodynamic resimulations using |$\rm \small {Gadget-X}$| and |$\rm \small {Gizmo-Simba}$| baryonic models. The cumulative sub-halo mass function of |$\rm \small {Gizmo-Simba}$| simulated clusters aligns with observations, while |$\rm \small {Gadget-X}$| simulations exhibit discrepancies in the lower sub-halo mass range, possibly due to its strong supernova feedback. Both |$\rm \small {Gadget-X}$| and |$\rm \small {Gizmo-Simba}$| simulations demonstrate a redshift evolution of the sub-halo mass function and the V circ function, with slightly fewer sub-haloes observed at lower redshifts. Neither the |$\rm \small {Gadget-X}$| nor |$\rm \small {Gizmo-Simba}$| (albeit a little closer) simulated clusters' predictions for the M sub– V circ relation align with the observational result. Further investigations on the correlation between sub-halo/halo properties and the discrepancy in the M sub– V circ relation reveal that the sub-halo's half mass radius and galaxy stellar age, the baryon fraction, and sub-halo distance from the cluster's centre, as well as the halo relaxation state, play important roles on reproducing this relation. Nonetheless, challenges persist in accurately reproducing the observed M sub– V circ relationship within our current hydrodynamic cluster simulation that adheres to the standard ΛCDM cosmology. These challenges may stem from shortcomings in our baryon modelling, numerical intricacies within the simulation, or even potential limitations of the ΛCDM framework. [ABSTRACT FROM AUTHOR]

Published
2024
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104. The GLASS-JWST Early Release Science Program. III. Strong-lensing Model of Abell 2744 and Its Infalling Regions

Author

Bergamini, Pietro, primary, Acebron, Ana, additional, Grillo, Claudio, additional, Rosati, Piero, additional, Caminha, Gabriel Bartosch, additional, Mercurio, Amata, additional, Vanzella, Eros, additional, Mason, Charlotte, additional, Treu, Tommaso, additional, Angora, Giuseppe, additional, Brammer, Gabriel B., additional, Meneghetti, Massimo, additional, Nonino, Mario, additional, Boyett, Kristan, additional, Bradač, Maruša, additional, Castellano, Marco, additional, Fontana, Adriano, additional, Morishita, Takahiro, additional, Paris, Diego, additional, Prieto-Lyon, Gonzalo, additional, Roberts-Borsani, Guido, additional, Roy, Namrata, additional, Santini, Paola, additional, Vulcani, Benedetta, additional, Wang, Xin, additional, and Yang, Lilan, additional

Published
2023
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105. Realistic simulations of gravitational lensing by galaxy clusters: extracting arc parameters from mock DUNE images

Author

Meneghetti, Massimo, Melchior, Peter, Grazian, Andrea, De Lucia, Gabriella, Dolag, Klaus, Bartelmann, Matthias, Heymans, Catherine, Moscardini, Lauro, and Radovich, Mario

Subjects
Astrophysics
Abstract

We present a newly developed code that allows simulations of optical observations of galaxy fields with a variety of instruments. The code incorporates gravitational lensing effects and is targetted at simulating lensing by galaxy clusters. Our goal is to create the tools required for comparing theoretical expectations with observations to obtain a better understanding of how observational noise affects lensing applications such as mass estimates, studies on the internal properties of galaxy clusters and arc statistics. Starting from a set of input parameters, characterizing both the instruments and the observational conditions, the simulator provides a virtual observation of a patch of the sky. It includes several sources of noise such as photon-noise, sky background, seeing, and instrumental noise. Ray-tracing through simulated mass distributions accounts for gravitational lensing. Source morphologies are realistically simulated based on shapelet decompositions of galaxy images retrieved from the GOODS-ACS archive. According to their morphological class, spectral-energy-distributions are assigned to the source galaxies in order to reproduce observations of each galaxy in arbitrary photometric bands. We illustrate our techniques showing virtual observations of a galaxy-cluster core as it would be observed with the space telescope DUNE, which was recently proposed to ESA within its "Cosmic vision" programme. (Abridged), Comment: 17 pages, 15 figures submitted to A&A

Published
2007
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106. Testing the reliability of weak lensing cluster detections

Author

Pace, Francesco, Maturi, Matteo, Meneghetti, Massimo, Bartelmann, Matthias, Moscardini, Lauro, and Dolag, Klaus

Subjects
Astrophysics
Abstract

We study the reliability of dark-matter halo detections with three different linear filters applied to weak-lensing data. We use ray-tracing in the multiple lens-plane approximation through a large cosmological simulation to construct realizations of cosmic lensing by large-scale structures between redshifts zero and two. We apply the filters mentioned above to detect peaks in the weak-lensing signal and compare them with the true population of dark matter halos present in the simulation. We confirm the stability and performance of a filter optimized for suppressing the contamination by large-scale structure. It allows the reliable detection of dark-matter halos with masses above a few times 1e13 M_sun/h with a fraction of spurious detections below ~10%. For sources at redshift two, 50% of the halos more massive than ~7e13 M_sun/h are detected, and completeness is reached at ~2e14 M_sun/h., Comment: 14 pages, 13 figures, accepted on A&A

Published
2007
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107. Arc sensitivity to cluster ellipticity, asymmetries and substructures

Author

Meneghetti, Massimo, Argazzi, Rodolfo, Pace, Francesco, Moscardini, Lauro, Dolag, Klaus, Bartelmann, Matthias, Li, Guoliang, and Oguri, Masamune

Subjects
Astrophysics
Abstract

We investigate how ellipticity, asymmetries and substructures separately affect the ability of galaxy clusters to produce strong lensing events, i.e. gravitational arcs, and how they influence the arc morphologies and fluxes. This is important for those studies aiming, for example, at constraining cosmological parameters from statistical lensing, or at determining the inner structure of galaxy clusters through gravitational arcs. We do so by creating two-dimensional gradually smoothed, differently elliptical and asymmetric versions of some numerical models. On average, we find that the contributions of ellipticity, asymmetries and substructures amount to ~40%, ~10% and ~30% of the total strong lensing cross section, respectively. However, our analysis shows that substructures play a more important role in less elliptical and asymmetric clusters, even if located at large distances from the cluster centers (~1Mpc/h). Conversely, their effect is less important in highly asymmetric lenses. The morphology, position and flux of individual arcs are strongly affected by the presence of substructures in the clusters. Removing substructures on spatial scales <~50kpc/h, roughly corresponding to mass scales <~5 10^{10}M_\odot/h, alters the image multiplicity of ~35% of the sources used in the simulations and causes position shifts larger than 5'' for ~40% of the arcs longer than 5''. We conclude that any model for cluster lens cannot neglect the effects of ellipticity, asymmetries and substructures. On the other hand, the high sensitivity of gravitational arcs to deviations from regular, smooth and symmetric mass distributions suggests that strong gravitational lensing is potentially a powerfull tool to measure the level of substructures and asymmetries in clusters., Comment: 16 pages, 18 figures. Accepted version. Version with full resolution images can be found at http://www.ita.uni-heidelberg.de/~massimo/sub/publications.html

Published
2006
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108. Mass Distributions of HST Galaxy Clusters from Gravitational Arcs

Author

Comerford, Julia M., Meneghetti, Massimo, Bartelmann, Matthias, and Schirmer, Mischa

Subjects
Astrophysics
Abstract

Although N-body simulations of cosmic structure formation suggest that dark matter halos have density profiles shallower than isothermal at small radii and steeper at large radii, whether observed galaxy clusters follow this profile is still ambiguous. We use one such density profile, the asymmetric NFW profile, to model the mass distributions of 11 galaxy clusters with gravitational arcs observed by HST. We characterize the galaxy lenses in each cluster as NFW ellipsoids, each defined by an unknown scale convergence, scale radius, ellipticity, and position angle. For a given set of values of these parameters, we compute the arcs that would be produced by such a lens system. To define the goodness of fit to the observed arc system, we define a chi^2 function encompassing the overlap between the observed and reproduced arcs as well as the agreement between the predicted arc sources and the observational constraints on the source system. We minimize this chi^2 to find the values of the lens parameters that best reproduce the observed arc system in a given cluster. Here we report our best-fit lens parameters and corresponding mass estimates for each of the 11 lensing clusters. We find that cluster mass models based on lensing galaxies defined as NFW ellipsoids can accurately reproduce the observed arcs, and that the best-fit parameters to such a model fall within the reasonable ranges defined by simulations. These results assert NFW profiles as an effective model for the mass distributions of observed clusters., Comment: Submitted to ApJ, 14 figures included

Published
2005
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109. The Lensed Arc Production Efficiency of Galaxy Clusters: A Comparison of Matched Observed and Simulated Samples

Author

Horesh, Assaf, Ofek, Eran O., Maoz, Dan, Bartelmann, Matthias, Meneghetti, Massimo, and Rix, Hans-Walter

Subjects
Astrophysics
Abstract

We compare the statistical properties of giant gravitationally lensed arcs produced in matched simulated and observed cluster samples. The observed sample consists of 10 X-ray selected clusters at redshifts z ~ 0.2 imaged with HST by Smith et al. The simulated dataset is produced by lensing the Hubble Deep Field, which serves as a background source image, with 150 realizations (different projections and shifts) of five simulated z = 0.2 clusters from a LambdaCDM N-body simulation. The real and simulated clusters have similar masses, the real photometric redshift is used for each background source, and all the observational effects influencing arc detection in the real dataset, including light from cluster galaxies, are simulated in the artificial dataset. We develop, and apply to both datasets, an objective automatic arc-finding algorithm. We find consistent arc statistics in the real and in the simulated sample, with an average of ~ 1 detected giant (length to width ratio >= 10) arc per cluster and ~ 0.2 giant luminous (R<22.3 mag) arc per cluster. Thus, taking into account a realistic source population and observational effects, the clusters predicted by LambdaCDM have the same arc-production efficiency as the observed clusters. If, as suggested by other studies, there is a discrepancy between the predicted and the observed total number of arcs on the sky, it must be the result of differences between the redshift dependent cluster mass functions, and not due to differences in the lensing efficiency of the most massive clusters., Comment: 13 pages, Accepted by ApJ, High resolution version of the paper can be found at: ftp://wise3.tau.ac.il/pub/assafh/horesh_arcs_stat_2005.ps.gz, Arc-finding algorithm available at: http://wise-obs.tau.ac.il/~assafh/ ; A comment was added ; A missing x-axis label in Fig. 7 was added

Published
2005
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110. The impact of gas physics on strong cluster lensing

Author

Puchwein, Ewald, Bartelmann, Matthias, Dolag, Klaus, and Meneghetti, Massimo

Subjects
Astrophysics
Abstract

Previous studies of strong gravitational lensing by galaxy clusters neglected the potential impact of the intracluster gas. Here, we compare simulations of strong cluster lensing including gas physics at increasing levels of complexity, i.e. with adiabatic, cooling, star-forming, feedback-receiving, and thermally conducting gas, and with different implementations of the artificial viscosity in the SPH simulations. Each cluster was simulated starting from the same initial conditions such as to allow directly comparing the simulated clusters. We compare the clusters' shapes, dynamics and density profiles and study their strong-lensing cross sections computed by means of ray-tracing simulations. We find that the impact of adiabatic gas depends on the amount of turbulence that builds up, which means that the artificial viscosity plays an important role. With the common viscosity implementation, adiabatic gas has little effect on strong cluster lensing, while lower viscosity allows stronger turbulence, thus higher non-thermal pressure and a generally broader gas distribution which tends to lower lensing cross sections. Conversely, cooling and star formation steepen the core density profiles and can thus increase the strong-lensing efficiency considerably., Comment: 8 pages, 10 figures, revised version published in A&A, added discussion of artificial viscosity

Published
2005
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111. Constraints on Dark Energy Models from Galaxy Clusters with Multiple Arcs

Author

Meneghetti, Massimo, Jain, Bhuvnesh, Bartelmann, Matthias, and Dolag, Klaus

Subjects
Astrophysics
Abstract

We make an exploratory study of how well dark energy models can be constrained using lensed arcs at different redshifts behind cluster lenses. Arcs trace the critical curves of clusters, and the growth of critical curves with source redshift is sensitive to the dark-energy equation of state. Using analytical models and numerically simulated clusters, we explore the key factors involved in using cluster arcs as a probe of dark energy. We quantify the sensitivity to lens mass, concentration and ellipticity with analytical models that include the effects of dark energy on halo structure. We show with simple examples how degeneracies between mass models and cosmography may be broken using arcs at multiple redshifts or additional constraints on the lens density profile. However we conclude that the requirements on the data are so stringent that it is very unlikely that robust constraints can be obtained from individual clusters. We argue that surveys of clusters, analyzed in conjunction with numerical simulations, are a more promising prospect for arc-cosmography. We use such numerically simulated clusters to estimate how large a sample of clusters/arcs could provide interesting constraints on dark energy models. We focus on the scatter produced by differences in the mass distribution of individual clusters. We find from our sample of simulated clusters that at least 1000 pairs of arcs are needed to obtain constraints if the mass distribution of individual clusters is taken to be undetermined. We discuss several unsolved problems that need study to fully develop this method for precision studies with future surveys., Comment: 10 pages, 8 figures, submitted to MNRAS

Published
2004
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112. Strong lensing by cluster-sized haloes in dark-energy cosmologies

Author

Meneghetti, Massimo, Bartelmann, Matthias, Dolag, Klaus, Moscardini, Lauro, Perrotta, Francesca, Baccigalupi, Carlo, and Tormen, Giuseppe

Subjects
Astrophysics
Abstract

We study the efficiency of numerically simulated galaxy clusters for producing strong gravitational lensing events in different dark-energy cosmologies with constant and time-variable equation of state and we compare it with ``standard'' $\Lambda$CDM and OCDM models. Our main results are that: (1) the expected abundance of gravitational arcs with large length-to-width ratio depends on the equation of state of dark energy at the epoch of formation of the halo; (2) as found in previous studies, the strong lensing cross section of galaxy clusters is very sensitive to dynamical processes like mergers, whose impact however is different for different cosmologies, being stronger for models in which halos are less concentrated. As expected, the largest differences in the lensing optical depth occur at moderate and high redshift., Comment: 10 pages, 6 figures, submitted to A&A

Published
2004
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113. Do arcs require flat halo cusps?

Author

Bartelmann, Matthias and Meneghetti, Massimo

Subjects
Astrophysics
Abstract

It was recently claimed that several galaxy clusters containing radial and tangential gravitational arcs and having a measured velocity-dispersion profile for the brightest cluster galaxy had to have central density profiles considerably flatter than those found in CDM cluster simulations. Using a simple analytic mass model, we confirm this result_for axially symmetric_ mass distributions, but show that steep density profiles are well in agreement with the cluster requiring the flattest axially symmetric profile once even small deviations from axial symmetry are introduced., Comment: submitted to A&A

Published
2003
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114. The impact of cluster mergers on arc statistics

Author

Torri, Elena, Meneghetti, Massimo, Bartelmann, Matthias, Moscardini, Lauro, Rasia, Elena, and Tormen, Giuseppe

Subjects
Astrophysics
Abstract

We study the impact of merger events on the strong lensing properties of galaxy clusters. Previous lensing simulations were not able to resolve dynamical time scales of cluster lenses, which arise on time scales which are of order a Gyr. In this case study, we first describe qualitatively with an analytic model how some of the lensing properties of clusters are expected to change during merging events. We then analyse a numerically simulated lens model for the variation in its efficiency for producing both tangential and radial arcs while a massive substructure falls onto the main cluster body. We find that: (1) during the merger, the shape of the critical lines and caustics changes substantially; (2) the lensing cross sections for long and thin arcs can grow by one order of magnitude and reach their maxima when the extent of the critical curves is largest; (3) the cross section for radial arcs also grows, but the cluster can efficiently produce this kind of arcs only while the merging substructure crosses the main cluster centre; (4) while the arc cross sections pass through their maxima as the merger proceeds, the cluster's X-ray emission increases by a factor of $\sim5$. Thus, we conclude that accounting for these dynamical processes is very important for arc statistics studies. In particular, they may provide a possible explanation for the arc statistics problem., Comment: 16 pages, submitted to MNRAS, revised version after referee' Comments. Gzipped file including full resolution images can be downloaded at http://dipastro.pd.astro.it/~cosmo/massimo/high-res-images.tar.gz

Published
2003
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115. Numerical study of halo concentrations in dark-energy cosmologies

Author

Dolag, Klaus, Bartelmann, Matthias, Perrotta, Francesca, Baccigalupi, Carlo, Moscardini, Lauro, Meneghetti, Massimo, and Tormen, Giuseppe

Subjects
Astrophysics
Abstract

We study the concentration parameters, their mass dependence and redshift evolution, of dark-matter halos in different dark-energy cosmologies with constant and time-variable equation of state, and compare them with "standard'' Lambda-CDM and OCDM models. We find that previously proposed algorithms for predicting halo concentrations can be well adapted to dark-energy models. When centred on the analytically expected values, halo concentrations show a log-normal distribution with a uniform standard deviation of ~0.2. The dependence of averaged halo concentrations on mass and redshift permits a simple fit of the form (1+z) c=c0 (M/M0)^a, with a~-0.1 throughout. We find that the cluster concentration depends on the dark energy equation of state at the cluster formation redshift z_{coll} through the linear growth factor D_+(z_{coll}). As a simple correction accounting for dark-energy cosmologies, we propose scaling c0 from Lambda-CDM with the ratio of linear growth factors, c0 -> c0 D_+(z_{coll})/D_{+,Lambda-CDM}(z_{coll})., Comment: 11 pages, submitted to Astronomy & Astrophysics

Published
2003
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116. Arc statistics with realistic cluster models

Author

Meneghetti, Massimo, Bartelmann, Matthias, Moscardini, Lauro, Rasia, Elena, Tormen, Giuseppe, and Torri, Elena

Subjects
Astrophysics
Abstract

Arc statistics is known to be a powerful cosmological tool. Numerical lensing simulations show that orders of magnitude differences in the number of {\em giant} arcs on the whole sky are expected in different cosmological models. In this paper, we discuss the analytic and numerical methods in arc statistics and show that analytic models fail to reproduce the efficiency for strong lensing of more realistic numerical cluster models. Then, we discuss two recent extensions of the lensing simulations, i.e. the effects of cD galaxies in the lensing clusters and the impact of cluster mergers on arc statistics. We show that cD galaxies can increase the lensing cross sections for long and thin arcs by perhaps up to $\sim50%$, while major mergers can change the cluster efficiency for producing such arcs by up to one order of magnitude., Comment: 14 pages, 6 figures, to appear in "Gravitational Lensing: A Unique Tool For Cosmology", Aussois 2003, eds. D. Valls-Gabaud & J.-P. Kneib

Published
2003

117. cD galaxy contribution to the strong lensing cross sections of galaxy clusters

Author

Meneghetti, Massimo, Bartelmann, Matthias, and Moscardini, Lauro

Subjects
Astrophysics
Abstract

We perform ray-tracing simulations evaluating the effect of a cD galaxy on the strong lensing properties of five galaxy cluster halos obtained from N-body simulations. The cD galaxy is modelled using both axially symmetric and elliptical models and assuming several masses for its dark matter halo. The effect of the cD orientation with respect to the mass distribution of the host galaxy cluster is also investigated. The simulations are carried out in an open and a flat model universe with cosmological constant. We find that the enhancement of the cluster lensing cross sections for long and thin arcs due to the presence of a massive cD at the cluster centre is typically less than 100%, depending on the model used for the cD galaxy and its orientation. The impact of the cD on the cluster efficiency for producing radially magnified images is larger only for those clusters whose lensing cross section for radial arcs is very small in absence of the central galaxy. We conclude that the presence of a cD galaxy at the cluster centre can only moderately influence the cluster efficiency for strong lensing and in particular fails to explain the discrepancy between the observed number of giant arcs in galaxy clusters and their abundance predicted from lensing simulations in the currently most favoured $\Lambda$CDM model., Comment: 11 pages, MNRAS in press, minor changes to match the referee' comments

Published
2003
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118. Arc Statistics in Cosmological Models with Dark Energy

Author

Bartelmann, Matthias, Meneghetti, Massimo, Perrotta, Francesca, Baccigalupi, Carlo, and Moscardini, Lauro

Subjects
Astrophysics
Abstract

We investigate how the probability of the formation of giant arcs in galaxy clusters is expected to change in cosmological models dominated by dark energy with an equation of state p=w rho c^2 compared to cosmological-constant or open models. To do so, we use a simple analytic model for arc cross sections based on the Navarro-Frenk-White density profile which we demonstrate reproduces essential features of numerically determined arc cross sections. Since analytic lens models are known to be inadequate for accurate absolute quantifications of arc probabilities, we use them only for studying changes relative to cosmological-constant models. Our main results are (1) the order of magnitude difference between the arc probabilities in low density, spatially flat and open CDM models found numerically is reproduced by our analytic model, and (2) dark-energy cosmologies with w>-1 increase the arc optical depth by at most a factor of two and are thus unlikely to reconcile arc statistics with spatially flat cosmological models with low matter density., Comment: 8 pages, accepted by A&A

Published
2002
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119. Cluster cross sections for strong lensing: analytic and numerical lens models

Author

Meneghetti, Massimo, Bartelmann, Matthias, and Moscardini, Lauro

Subjects
Astrophysics
Abstract

The statistics of gravitationally lensed arcs was recognised earlier as a potentially powerful cosmological probe. However, while fully numerical models find orders of magnitude difference between the arc probabilities in different cosmological models, analytic models tend to find markedly different results. We introduce in this paper an analytic cluster lens model which improves upon existing analytic models in four ways. (1) We use the more realistic Navarro-Frenk-White profile instead of singular isothermal spheres, (2) we include the effect of cosmology on the compactness of the lenses, (3) we use elliptical instead of axially symmetric lenses, and (4) we take the intrinsic ellipticity of sources into account. While these improvements to the analytic model lead to a pronounced increase of the arc probability, comparisons with numerical models of the same virial mass demonstrate that the analytic models still fall short by a substantial margin of reproducing the results obtained with numerical models. Using multipole expansions of cluster mass distributions, we show that the remaining discrepancy can be attributed to substructure inside clusters and tidal fields contributed by the cluster surroundings, effects that cannot reasonably and reliably be mimicked in analytic models., Comment: 10 pages, MNRAS in press. Added a new subsection quantifying the substructure of the numerical cluster models

Published
2002
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120. Constraining cosmological models using arc statistics in future SZ cluster surveys

Author

Meneghetti, Massimo, Bartelmann, Matthias, and Moscardini, Lauro

Subjects
Astrophysics
Abstract

Upcoming wide-area surveys in the submillimetre regime will allow the construction of complete galaxy cluster samples through their thermal Sunyaev-Zel'dovich effect. We propose an analytic method to predict the number of gravitationally lensed giant arcs produced by the cluster sample expected to be detectable for the Planck satellite. The statistics of lensed arcs can be used to constrain cosmological parameters. This computation implies the choice of an analytic cluster model which has to reproduce the lensing properties of realistic galaxy clusters. Comparing the results of analytic computations and numerical ray-tracing simulations, we show that spherical models with the Navarro-Frenk-White density profile fail by far to produce as many giant arcs as realistic galaxy clusters. This confirms the great importance of asymmetries and substructures in the lensing matter distribution. By elliptically distorting the lensing potential of spherical NFW density profiles, we show that the discrepancy between analytic and numerical computations can almost completely be removed., Comment: 5 pages, Latex using mrs2001 style, to appear in "Where's the Matter? Tracing Dark and Bright Matter with the New Generation of Large Scale Surveys", Eds. Treyer & Tresse, 2001, Frontier Group

Published
2001

121. Giant cluster arcs as a constraint on the scattering cross-section of dark matter

Author

Meneghetti, Massimo, Yoshida, Naoki, Bartelmann, Matthias, Moscardini, Lauro, Springel, Volker, Tormen, Giuseppe, and White, Simon D. M.

Subjects
Astrophysics
Abstract

We carry out ray tracing through five high resolution simulations of a galaxy cluster to study how its ability to produce giant gravitationally lensed arcs is influenced by the collision cross-section of its dark matter. In three cases typical dark matter particles in the cluster core undergo between 1 and 100 collisions per Hubble time; two more explore the long (``collisionless'') and short (``fluid'') mean free path limits. We study the size and shape distributions of arcs and compute the cross-section for producing ``extreme'' arcs of various sizes. Even a few collisions per particle modify the core structure enough to destroy the cluster's ability to produce long, thin arcs. For larger collision frequencies the cluster must be scaled up to unrealistically large masses before it regains the ability to produce giant arcs. None of our models with self-interacting dark matter (except the ``fluid'' limit) is able to produce radial arcs; even the case with the smallest scattering cross-section must be scaled to the upper limit of observed cluster masses before it produces radial arcs. Apparently the elastic collision cross-section of dark matter in clusters must be very small, below 0.1 cm^2 g^-1, to be compatible with the observed ability of clusters to produce both radial arcs and giant arcs., Comment: 8 pages, Latex using MN style, accepted version, to appear in MNRAS. Other figures not included in the paper can be found at http://www.mpa-garching.mpg.de/~massimo/SIDMlens.html

Published
2000
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122. Cluster galaxies: contribution to the arc statistics

Author

Meneghetti, Massimo, Bolzonella, Micol, Bartelmann, Matthias, Moscardini, Lauro, and Tormen, Giuseppe

Subjects
Astrophysics
Abstract

We present the results of a set of numerical simulations aiming at evaluating the effects of cluster galaxies on the arc statistics. At this goal we use nine different galaxy clusters obtained from N-body simulations. We mimic the presence of a population of galaxies inside each cluster, trying to reproduce the observed luminosity function and the spatial distribution. We compare the statistical distributions of the properties of the gravitational arcs produced by our clusters with and without galaxies. We find that the cluster galaxies do not introduce perturbations strong enough to significantly change the number of arcs and the distributions of the properties of long arcs., Comment: 4 pages, Latex using moriond2000.sty. To be published in Proc. of the XXXVth Rencontres de Moriond--XXth Moriond Astrophysics Meeting on "L2K Cosmological Physics with Gravitational Lensing", J.P. Kneib, Y. Mellier, M. Moniez, J. Tran Thanh Van eds., Editions Frontieres

Published
2000

123. Effects of cluster galaxies on arc statistics

Author

Meneghetti, Massimo, Bolzonella, Micol, Bartelmann, Matthias, Moscardini, Lauro, and Tormen, Giuseppe

Subjects
Astrophysics
Abstract

We present the results of a set of numerical simulations evaluating the effect of cluster galaxies on arc statistics. We perform a first set of gravitational lensing simulations using three independent projections for each of nine different galaxy clusters obtained from N-body simulations. The simulated clusters consist of dark matter only. We add a population of galaxies to each cluster, mimicking the observed luminosity function and the spatial galaxy distribution, and repeat the lensing simulations including the effects of cluster galaxies, which themselves act as individual lenses. Each galaxy is represented by a spherical Navarro, Frenk & White (1997) density profile. We consider the statistical distributions of the properties of the gravitational arcs produced by our clusters with and without galaxies. We find that the cluster galaxies do not introduce perturbations strong enough to significantly change the number of arcs and the distributions of lengths, widths, curvature radii and length-to-width ratios of long arcs. We find some changes to the distribution of short-arc properties in presence of cluster galaxies. The differences appear in the distribution of curvature radii for arc lengths smaller than 12'', while the distributions of lengths, widths and length-to-width ratios are significantly changed only for arcs shorter than 4''., Comment: 11 pages, Latex using MN style, 6 figures enclosed. Version accepted for publication in MNRAS. Gzipped file including a full resolution version of Figures 2a, 2b, 3a, 3b, 3c can be downloaded by anonymous ftp at http://gt.pd.astro.it/~bepi/PAPERS/lensing.ps.gz

Published
1999
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125. A Bayesian chemical evolution model of the DustPedia Galaxy M74

Author

Calura, Francesco, primary, Palla, Marco, additional, Morselli, Laura, additional, Spitoni, Emanuele, additional, Casasola, Viviana, additional, Verma, Kuldeep, additional, Enia, Andrea, additional, Meneghetti, Massimo, additional, Bianchi, Simone, additional, Pozzi, Francesca, additional, and Gruppioni, Carlotta, additional

Published
2023
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126. Early Results from GLASS-JWST. XIX. A High Density of Bright Galaxies at z ≈ 10 in the A2744 Region

Author

Castellano, Marco, primary, Fontana, Adriano, additional, Treu, Tommaso, additional, Merlin, Emiliano, additional, Santini, Paola, additional, Bergamini, Pietro, additional, Grillo, Claudio, additional, Rosati, Piero, additional, Acebron, Ana, additional, Leethochawalit, Nicha, additional, Paris, Diego, additional, Bonchi, Andrea, additional, Belfiori, Davide, additional, Calabrò, Antonello, additional, Correnti, Matteo, additional, Nonino, Mario, additional, Polenta, Gianluca, additional, Trenti, Michele, additional, Boyett, Kristan, additional, Brammer, G., additional, Broadhurst, Tom, additional, Caminha, Gabriel B., additional, Chen, Wenlei, additional, Filippenko, Alexei V., additional, Fortuni, Flaminia, additional, Glazebrook, Karl, additional, Mascia, Sara, additional, Mason, Charlotte A., additional, Menci, Nicola, additional, Meneghetti, Massimo, additional, Mercurio, Amata, additional, Metha, Benjamin, additional, Morishita, Takahiro, additional, Nanayakkara, Themiya, additional, Pentericci, Laura, additional, Roberts-Borsani, Guido, additional, Roy, Namrata, additional, Vanzella, Eros, additional, Vulcani, Benedetta, additional, Yang, Lilan, additional, and Wang, Xin, additional

Published
2023
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127. The Three Hundred Project: the evolution of physical baryon profiles

Author

Qingyang Li, Weiguang Cui, Xiaohu Yang, Romeel Davé, Elena Rasia, Stefano Borgani, Meneghetti Massimo, Alexander Knebe, Klaus Dolag, and Jack Sayers

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The distribution of baryons provides a significant way to understand the formation of galaxy clusters by revealing the details of its internal structure and changes over time. In this paper, we present theoretical studies on the scaled profiles of physical properties associated with the baryonic components, including gas density, temperature, metallicity, pressure and entropy as well as stellar mass, metallicity and satellite galaxy number density in galaxy clusters from $z=4$ to $z=0$ by tracking their progenitors. These mass-complete simulated galaxy clusters are coming from THE THREE HUNDRED with two runs: GIZMO-SIMBA and Gadget-X. Through comparisons between the two simulations, and with observed profiles which are generally available at low redshift, we find that (1) the agreements between the two runs and observations are mostly at outer radii $r \gtrsim 0.3r_{500}$, in line with the self-similarity assumption. While Gadget-X shows better agreements with the observed gas profiles in the central regions compared to GIZMO-SIMBA; (2) the evolution trends are generally consistent between the two simulations with slightly better consistency at outer radii. In detail, the gas density profile shows less discrepancy than the temperature and entropy profiles at high redshift. The differences in the cluster centre and gas properties imply different behaviours of the AGN models between Gadget-X and GIZMO-SIMBA, with the latter, maybe too strong for this cluster simulation. The high-redshift difference may be caused by the star formation and feedback models or hydrodynamics treatment, which requires observation constraints and understanding., 20 pages, 20 figures, accepted in MNRAS

Published
2023

128. The probability of galaxy–galaxy strong lensing events in hydrodynamical simulations of galaxy clusters

Author

Meneghetti, Massimo, primary, Ragagnin, Antonio, additional, Borgani, Stefano, additional, Calura, Francesco, additional, Despali, Giulia, additional, Giocoli, Carlo, additional, Granato, Gian Luigi, additional, Grillo, Claudio, additional, Moscardini, Lauro, additional, Rasia, Elena, additional, Rosati, Piero, additional, Angora, Giuseppe, additional, Bassini, Luigi, additional, Bergamini, Pietro, additional, Caminha, Gabriel B., additional, Granata, Giovanni, additional, Mercurio, Amata, additional, Metcalf, Robert Benton, additional, Natarajan, Priyamvada, additional, Nonino, Mario, additional, Pignataro, Giada Venusta, additional, Ragone-Figueroa, Cinthia, additional, Vanzella, Eros, additional, Acebron, Ana, additional, Dolag, Klaus, additional, Murante, Giuseppe, additional, Taffoni, Giuliano, additional, Tornatore, Luca, additional, Tortorelli, Luca, additional, and Valentini, Milena, additional

Published
2022
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129. Unveiling the Universe with emerging cosmological probes

Author

Moresco, Michele, primary, Amati, Lorenzo, additional, Amendola, Luca, additional, Birrer, Simon, additional, Blakeslee, John P., additional, Cantiello, Michele, additional, Cimatti, Andrea, additional, Darling, Jeremy, additional, Della Valle, Massimo, additional, Fishbach, Maya, additional, Grillo, Claudio, additional, Hamaus, Nico, additional, Holz, Daniel, additional, Izzo, Luca, additional, Jimenez, Raul, additional, Lusso, Elisabeta, additional, Meneghetti, Massimo, additional, Piedipalumbo, Ester, additional, Pisani, Alice, additional, Pourtsidou, Alkistis, additional, Pozzetti, Lucia, additional, Quartin, Miguel, additional, Risaliti, Guido, additional, Rosati, Piero, additional, and Verde, Licia, additional

Published
2022
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130. Galaxies in the central regions of simulated galaxy clusters

Author

Ragagnin, Antonio, primary, Meneghetti, Massimo, additional, Bassini, Luigi, additional, Ragone-Figueroa, Cinthia, additional, Luigi Granato, Gian, additional, Despali, Giulia, additional, Giocoli, Carlo, additional, Granata, Giovanni, additional, Moscardini, Lauro, additional, Bergamini, Pietro, additional, Rasia, Elena, additional, Valentini, Milena, additional, Borgani, Stefano, additional, Calura, Francesco, additional, Dolag, Klaus, additional, Grillo, Claudio, additional, Mercurio, Amata, additional, Murante, Giuseppe, additional, Natarajan, Priyamvada, additional, Rosati, Piero, additional, Taffoni, Giuliano, additional, Tornatore, Luca, additional, and Tortorelli, Luca, additional

Published
2022
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131. LoVoCCS. I. Survey Introduction, Data Processing Pipeline, and Early Science Results

Author

Fu, Shenming, primary, Dell’Antonio, Ian, additional, Chary, Ranga-Ram, additional, Clowe, Douglas, additional, Cooper, M. C., additional, Donahue, Megan, additional, Evrard, August, additional, Lacy, Mark, additional, Lauer, Tod, additional, Liu, Binyang, additional, McCleary, Jacqueline, additional, Meneghetti, Massimo, additional, Miyatake, Hironao, additional, Montes, Mireia, additional, Natarajan, Priyamvada, additional, Ntampaka, Michelle, additional, Pierpaoli, Elena, additional, Postman, Marc, additional, Sohn, Jubee, additional, Umetsu, Keiichi, additional, Utsumi, Yousuke, additional, and Wilson, Gillian, additional

Published
2022
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132. Pilot-WINGS: An extended MUSE view of the structure of Abell 370

Author

Lagattuta, David J, primary, Richard, Johan, additional, Bauer, Franz Erik, additional, Cerny, Catherine, additional, Claeyssens, Adélaïde, additional, Guaita, Lucia, additional, Jauzac, Mathilde, additional, Jeanneau, Alexandre, additional, Koekemoer, Anton M, additional, Mahler, Guillaume, additional, Prieto Lyon, Gonzalo, additional, Acebron, Ana, additional, Meneghetti, Massimo, additional, Niemiec, Anna, additional, Zitrin, Adi, additional, Bianconi, Matteo, additional, Connor, Thomas, additional, Cen, Renyue, additional, Edge, Alastair, additional, Faisst, Andreas L, additional, Limousin, Marceau, additional, Massey, Richard, additional, Sereno, Mauro, additional, Sharon, Keren, additional, and Weaver, John R, additional

Published
2022
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134. Euclid preparation - XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields

Author

Euclid Collaboration, Moneti, A., McCracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Chary, R., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Cuby, J., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., ANDREON, Stefano, BARDELLI, Sandro, Faisst, A. L., Camera, S., Graciá-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Sureau, F., Tenti, M., Vassallo, T., ZACCHEI, Andrea, Masters, D. C., ZUCCA, Elena, Baccigalupi, C., Balaguera-Antolínez, A., Bernardeau, F., BIVIANO, ANDREA, BOLZONELLA, MICOL, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CAPPI, Alberto, McPartland, C., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., FARINA, Maria, FINELLI, FABIO, Flose-Reimberg, P., Mobasher, B., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Sanders, D. B., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, SCARAMELLA, Roberto, Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Stern, D., Scottez, V., SEFUSATTI, Emiliano, Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Hildebrandt, H., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., AURICCHIO, NATALIA, Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillis, B., GIOCOLI, Carlo, Granett, B. R., GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Moscardini, L., Munari, Emiliano, Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Moneti, A., Mccracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Chary, R., Cuby, J., Faisst, A. L., Masters, D. C., Mcpartland, C., Mobasher, B., Sanders, D. B., Scaramella, R., Stern, D., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Granett, B. R., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., K??mmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Cresp??, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Camera, S., Graci??-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Sureau, F., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antol??nez, A., Bernardeau, F., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., Farina, M., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., S??nchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., Viel, M., Hildebrandt, H., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, UAM. Departamento de Física Teórica, Moneti A., Mccracken H.J., Shuntov M., Kauffmann O.B., Capak P., Davidzon I., Ilbert O., Scarlata C., Toft S., Weaver J., Chary R., Cuby J., Faisst A.L., Masters D.C., Mcpartland C., Mobasher B., Sanders D.B., Scaramella R., Stern D., Szapudi I., Teplitz H., Zalesky L., Amara A., Auricchio N., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Capobianco V., Carbone C., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Fosalba P., Frailis M., Franceschi E., Fumana M., Garilli B., Gillis B., Giocoli C., Granett B.R., Grazian A., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Rix H., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Andreon S., Bardelli S., Camera S., Gracia-Carpio J., Medinaceli E., Mei S., Polenta G., Romelli E., Sureau F., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Bernardeau F., Biviano A., Bolzonella M., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Di Ferdinando D., Farina M., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I., Joachimi B., Kansal V., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., Maturi M., Metcalf R.B., Morgante G., Morisset N., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tubio O., Tutusaus I., Valiviita J., Viel M., Hildebrandt H., Kummel, M., Tallada-Crespi, P., Gracia-Carpio, J., Balaguera-Antolinez, A., and Sanchez, A. G.

Subjects
SAMPLE, Large-scale structure of Universe, DATA RELEASE, Formation, Surveys, observations, Dark energy, Dark matter, Galaxy: formation, Large-scale structure of Universe, Surveys [Cosmology], kosmologia, Astrophysics, Cosmology: observation, dark matter, galaksijoukot, pimeä aine, surveys, Dark energy, Dark matter, observations [Cosmology], dark energy, Observations, LEGACY SURVEY, Astrophysics of Galaxies, Física, Astronomy and Astrophysics, 115 Astronomy, Space science, EVOLUTION, Cosmology, galaksit, GALAXIES, Cosmology: observations, Galaxy: formation, Galaxy, formation [Galaxy], Space and Planetary Science, cosmology: observations, large-scale structure of Universe, pimeä energia, Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Artículo escrito por un elevado núnmero de autores, sólo se referencian el qque aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope's Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg2 in the 3.6 and 4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and 8 μm bands. They reach at least 24 AB magnitude (measured to 5σ, in a 2″​​.5 aperture) in the 3.6 μm band and up to ∼5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16 "< "[3.6]< 19 is ≲ 0″​​.15. The photometric calibration is in excellent agreement with previous WISE measurements. We extracted source number counts from the 3.6 μm band mosaics, and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s

Published
2022

135. Euclid preparation XV. Forecasting cosmological constraints for the Euclid and CMB joint analysis

Author

Euclid Collaboration, Ilić, S., Aghanim, N., Baccigalupi, C., BERMEJO CLIMENT, JOSE RAMON, Fabbian, G., Legrand, L., PAOLETTI, DANIELA, Ballardini, M., Archidiacono, M., Douspis, M., Kubik, B., Kümmel, M., Kurki-Suonio, H., Laureijs, R., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MANSUTTI, Oriana, Marggraf, O., Marulli, F., FINELLI, FABIO, Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, Emiliano, Niemi, S. M., Ganga, K., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Hernández-Monteagudo, C., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., SCARAMELLA, Roberto, Schneider, P., Secroun, A., Seidel, G., Serrano, S., LATTANZI, Mario Gilberto, Sirignano, C., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., VALENZIANO, LUCA, Verdoes Kleijn, G. A., Marinucci, D., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Medinaceli, E., Mei, S., Rosset, C., Sureau, F., Vassallo, T., Migliaccio, M., ZACCHEI, Andrea, ANDREON, Stefano, Balaguera-Antolínez, A., Baldi, M., BARDELLI, Sandro, BIVIANO, ANDREA, BORGANI, STEFANO, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CARBONE, Carmelita, CAPPI, Alberto, Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Di Ferdinando, D., Dole, H., Casas, S., FARINA, Maria, Ferreira, P. G., Flose-Reimberg, P., GALEOTTA, Samuele, Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Martinelli, M., Maino, D., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, Neissner, C., Nightingale, J., Nucita, A. A., Potter, D., RICCIO, GIUSEPPE, Tutusaus, I., Romelli, Erik, Schirmer, M., Schultheis, M., Scottez, V., Teyssier, R., Tramacere, A., Valiviita, J., VIEL, MATTEO, Whittaker, L., ZUCCA, Elena, Natoli, P., Ntelis, P., Pagano, L., Wenzl, L., GRUPPUSO, ALESSANDRO, Kitching, T., Langer, M., Mauri, N., Patrizii, L., Renzi, A., Sirri, G., Stanco, L., Tenti, M., Vielzeuf, P., Lacasa, F., Polenta, G., Yankelevich, V., Blanchard, A., Sakr, Z., Pourtsidou, A., Camera, S., CARDONE, Vincenzo Fabrizio, Kilbinger, M., Kunz, M., Markovic, K., Pettorino, V., Sánchez, A. G., Sapone, D., Amara, A., AURICCHIO, NATALIA, Bender, R., Bodendorf, C., BONINO, Donata, Branchini, Enzo, BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FRANZETTI, PAOLO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B., GIOCOLI, Carlo, GRAZIAN, Andrea, Grupp, F., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Universidad de La Laguna [Tenerife - SP] (ULL), Instituto de Astrofisica de Canarias (IAC), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, Dipartimento di Matematica [Roma II] (DIPMAT), Università degli Studi di Roma Tor Vergata [Roma], Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Paris-Saclay, Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Astronomy, Intelligent Systems, Ilic S., Aghanim N., Baccigalupi C., Bermejo-Climent J.R., Fabbian G., Legrand L., Paoletti D., Ballardini M., Archidiacono M., Douspis M., Finelli F., Ganga K., Hernandez-Monteagudo C., Lattanzi M., Marinucci D., Migliaccio M., Carbone C., Casas S., Martinelli M., Tutusaus I., Natoli P., Ntelis P., Pagano L., Wenzl L., Gruppuso A., Kitching T., Langer M., Mauri N., Patrizii L., Renzi A., Sirri G., Stanco L., Tenti M., Vielzeuf P., Lacasa F., Polenta G., Yankelevich V., Blanchard A., Sakr Z., Pourtsidou A., Camera S., Cardone V.F., Kilbinger M., Kunz M., Markovic K., Pettorino V., Sanchez A.G., Sapone D., Amara A., Auricchio N., Bender R., Bodendorf C., Bonino D., Branchini E., Brescia M., Brinchmann J., Capobianco V., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Ealet A., Farrens S., Fosalba P., Frailis M., Franceschi E., Franzetti P., Fumana M., Garilli B., Gillard W., Gillis B., Giocoli C., Grazian A., Grupp F., Guzzo L., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kohley R., Kubik B., Kummel M., Kurki-Suonio H., Laureijs R., Ligori S., Lilje P.B., Lloro I., Mansutti O., Marggraf O., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Percival W., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Roncarelli M., Rossetti E., Saglia R., Scaramella R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Starck J.L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Valentijn E.A., Valenziano L., Verdoes Kleijn G.A., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Medinaceli E., Mei S., Rosset C., Sureau F., Vassallo T., Zacchei A., Andreon S., Balaguera-Antolinez A., Baldi M., Bardelli S., Biviano A., Borgani S., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Cuby J., De La Torre S., Di Ferdinando D., Dole H., Farina M., Ferreira P.G., Flose-Reimberg P., Galeotta S., Gozaliasl G., Gracia-Carpio J., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Martinet N., Maturi M., Metcalf R.B., Morgante G., Neissner C., Nightingale J., Nucita A.A., Potter D., Riccio G., Romelli E., Schirmer M., Schultheis M., Scottez V., Teyssier R., Tramacere A., Valiviita J., Viel M., Whittaker L., Zucca E., Euclid, Collaboration, Ilić, S., Aghanim, N., Baccigalupi, C., Bermejo-Climent, J. R., Fabbian, G., Legrand, L., Paoletti, D., Ballardini, M., Archidiacono, M., Douspis, M., Finelli, F., Ganga, K., Hernández-Monteagudo, C., Lattanzi, M., Marinucci, D., Migliaccio, M., Carbone, C., Casas, S., Martinelli, M., Tutusaus, I., Natoli, P., Ntelis, P., Pagano, L., Wenzl, L., Gruppuso, A., Kitching, T., Langer, M., Mauri, N., Patrizii, L., Renzi, A., Sirri, G., Stanco, L., Tenti, M., Vielzeuf, P., Lacasa, F., Polenta, G., Yankelevich, V., Blanchard, A., Sakr, Z., Pourtsidou, A., Camera, S., Cardone, V. F., Kilbinger, M., Kunz, M., Markovic, K., Pettorino, V., Sánchez, A. G., Sapone, D., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Capobianco, V., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Kubik, B., Kümmel, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Verdoes Kleijn, G. A., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Medinaceli, E., Mei, S., Rosset, C., Sureau, F., Vassallo, T., Zacchei, A., Andreon, S., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Di Ferdinando, D., Dole, H., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Galeotta, S., Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Neissner, C., Nightingale, J., Nucita, A. A., Potter, D., Riccio, G., Romelli, E., Schirmer, M., Schultheis, M., Scottez, V., Teyssier, R., Tramacere, A., Valiviita, J., Viel, M., Whittaker, L., Zucca, E., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Ilic, S., Hernandez-Monteagudo, C., Sanchez, A. G., Kummel, M., Tallada-Crespi, P., Balaguera-Antolinez, A., De La Torre, S., Gracia-Carpio, J., Ili??, S., Hern??ndez-Monteagudo, C., S??nchez, A. G., K??mmel, M., Tallada-Cresp??, P., Balaguera-Antol??nez, A., and Graci??-Carpio, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, statistical [methods], FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, Joint analysis, kosmologia, 01 natural sciences, methods, NO, pimeä aine, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], mikroaallot, Settore FIS/05 - Astronomia e Astrofisica, surveys, 0103 physical sciences, tsz, survey, 010303 astronomy & astrophysics, Physics, methods: statistical, 010308 nuclear & particles physics, Computer Science::Information Retrieval, maailmankaikkeus, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, cross-correlation, 115 Astronomy, Space science, Cosmic background radiation, Large-scale structure of Universe, Methods: statistical, Surveys, kosminen taustasäteily, Space and Planetary Science, method, large-scale structure of Universe, pimeä energia, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The combination and cross-correlation of the upcoming $Euclid$ data with cosmic microwave background (CMB) measurements is a source of great expectation since it will provide the largest lever arm of epochs, ranging from recombination to structure formation across the entire past light cone. In this work, we present forecasts for the joint analysis of $Euclid$ and CMB data on the cosmological parameters of the standard cosmological model and some of its extensions. This work expands and complements the recently published forecasts based on $Euclid$-specific probes, namely galaxy clustering, weak lensing, and their cross-correlation. With some assumptions on the specifications of current and future CMB experiments, the predicted constraints are obtained from both a standard Fisher formalism and a posterior-fitting approach based on actual CMB data. Compared to a $Euclid$-only analysis, the addition of CMB data leads to a substantial impact on constraints for all cosmological parameters of the standard $\Lambda$-cold-dark-matter model, with improvements reaching up to a factor of ten. For the parameters of extended models, which include a redshift-dependent dark energy equation of state, non-zero curvature, and a phenomenological modification of gravity, improvements can be of the order of two to three, reaching higher than ten in some cases. The results highlight the crucial importance for cosmological constraints of the combination and cross-correlation of $Euclid$ probes with CMB data., Comment: 20 pages, 8 figures, 5 tables, 1 appendix; updated to match version accepted by journal

Published
2022

137. The KLEVER survey: nitrogen abundances at z ∼ 2 and probing the existence of a fundamental nitrogen relation

Author

Hayden-Pawson, Connor, primary, Curti, Mirko, additional, Maiolino, Roberto, additional, Cirasuolo, Michele, additional, Belfiore, Francesco, additional, Cappellari, Michele, additional, Concas, Alice, additional, Cresci, Giovanni, additional, Cullen, Fergus, additional, Kobayashi, Chiaki, additional, Mannucci, Filippo, additional, Marconi, Alessandro, additional, Meneghetti, Massimo, additional, Mercurio, Amata, additional, Peng, Yingjie, additional, Swinbank, Mark, additional, and Vincenzo, Fiorenzo, additional

Published
2022
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138. VLT/MUSE Observations of SDSS J1029+2623: Toward a High-precision Strong Lensing Model*

Author

Acebron, Ana, primary, Grillo, Claudio, additional, Bergamini, Pietro, additional, Mercurio, Amata, additional, Rosati, Piero, additional, Caminha, Gabriel Bartosch, additional, Tozzi, Paolo, additional, Brammer, Gabriel B., additional, Meneghetti, Massimo, additional, Morelli, Andrea, additional, Nonino, Mario, additional, and Vanzella, Eros, additional

Published
2022
Full Text
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139. Euclid preparation: XIII. Forecasts for galaxy morphology with the Euclid Survey using Deep Generative Models

Author

Euclid Collaboration, Bretonnière, H., Huertas-Company, M., Boucaud, A., Lanusse, F., Jullo, E., MERLIN, Emiliano, Tuccillo, D., CASTELLANO, MARCO, Brinchmann, J., Conselice, C. J., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Dole, H., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Cabanac, R., Torradeflot, F., Valentijn, E. A., VALENZIANO, LUCA, Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Baldi, M., BARDELLI, Sandro, Courtois, H. M., Camera, S., FARINELLI, Ruben, Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Tenti, M., Vassallo, T., ZACCHEI, Andrea, ZUCCA, Elena, Castander, F. J., Baccigalupi, C., Balaguera-Antolínez, A., BIVIANO, ANDREA, BORGANI, STEFANO, Bozzo, E., BURIGANA, CARLO, CAPPI, Alberto, Carvalho, C. S., Casas, S., Castignani, G., Duc, P. A., Colodro-Conde, C., Coupon, J., de la Torre, S., Fabricius, M., FARINA, Maria, Ferreira, P. G., Flose-Reimberg, P., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Guinet, D., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., McCracken, H. J., Metcalf, R. B., MORGANTE, GIANLUCA, Morisset, N., Nightingale, J., Kruk, S., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Kuchner, U., SEFUSATTI, Emiliano, Teyssier, R., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Whittaker, L., Knapen, J. H., Serrano, S., Soubrie, E., Tramacere, A., Wang, L., Amara, A., AURICCHIO, NATALIA, Bender, R., Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Capobianco, Vito, CARBONE, Carmelita, Carretero, J., CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B., GIOCOLI, Carlo, GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., MENEGHETTI, MASSIMO, Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, Emiliano, Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Cosmologie et Statistiques (LCS - COSMOSTAT), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Lanusse, Francois, UAM. Departamento de Física Teórica, Bretonniere, H., Huertas-Company, M., Boucaud, A., Lanusse, F., Jullo, E., Merlin, E., Tuccillo, D., Castellano, M., Brinchmann, J., Conselice, C. J., Dole, H., Cabanac, R., Courtois, H. M., Castander, F. J., Duc, P. A., Fosalba, P., Guinet, D., Kruk, S., Kuchner, U., Serrano, S., Soubrie, E., Tramacere, A., Wang, L., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Capobianco, V., Carbone, C., Carretero, J., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kummel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., Meneghetti, M., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespi, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Baldi, M., Bardelli, S., Camera, S., Farinelli, R., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolinez, A., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., De La Torre, S., Fabricius, M., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Mccracken, H. J., Metcalf, R. B., Morgante, G., Morisset, N., Nightingale, J., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tutusaus, I., Valiviita, J., Viel, M., Whittaker, L., Knapen, J. H., Bretonniere H., Huertas-Company M., Boucaud A., Lanusse F., Jullo E., Merlin E., Tuccillo D., Castellano M., Brinchmann J., Conselice C.J., Dole H., Cabanac R., Courtois H.M., Castander F.J., Duc P.A., Fosalba P., Guinet D., Kruk S., Kuchner U., Serrano S., Soubrie E., Tramacere A., Wang L., Amara A., Auricchio N., Bender R., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Capobianco V., Carbone C., Carretero J., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Frailis M., Franceschi E., Fumana M., Garilli B., Gillard W., Gillis B., Giocoli C., Grazian A., Grupp F., Haugan S.V.H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Melchior M., Meneghetti M., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pettorino V., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Sirignano C., Sirri G., Stanco L., Starck J.-L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Valentijn E.A., Valenziano L., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Baldi M., Bardelli S., Camera S., Farinelli R., Medinaceli E., Mei S., Polenta G., Romelli E., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Biviano A., Borgani S., Bozzo E., Burigana C., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., De La Torre S., Fabricius M., Farina M., Ferreira P.G., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I.M., Joachimi B., Kansal V., Kashlinsky A., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., McCracken H.J., Metcalf R.B., Morgante G., Morisset N., Nightingale J., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tutusaus I., Valiviita J., Viel M., Whittaker L., Knapen J.H., Astronomy, Bretonniere, H, Huertas-Company, M, Boucaud, A, Lanusse, F, Jullo, E, Merlin, E, Tuccillo, D, Castellano, M, Brinchmann, J, Conselice, Cj, Dole, H, Cabanac, R, Courtois, Hm, Castander, Fj, Duc, Pa, Fosalba, P, Guinet, D, Kruk, S, Kuchner, U, Serrano, S, Soubrie, E, Tramacere, A, Wang, L, Amara, A, Auricchio, N, Bender, R, Bodendorf, C, Bonino, D, Branchini, E, Brau-Nogue, S, Brescia, M, Capobianco, V, Carbone, C, Carretero, J, Cavuoti, S, Cimatti, A, Cledassou, R, Congedo, G, Conversi, L, Copin, Y, Corcione, L, Costille, A, Cropper, M, Da Silva, A, Degaudenzi, H, Douspis, M, Dubath, F, Duncan, Caj, Dupac, X, Dusini, S, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Fumana, M, Garilli, B, Gillard, W, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Haugan, Svh, Holmes, W, Hormuth, F, Hudelot, P, Jahnke, K, Kermiche, S, Kiessling, A, Kilbinger, M, Kitching, T, Kohley, R, Kummel, M, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, Pb, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Marulli, F, Massey, R, Maurogordato, S, Melchior, M, Meneghetti, M, Meylan, G, Moresco, M, Morin, B, Moscardini, L, Munari, E, Nakajima, R, Niemi, Sm, Padilla, C, Paltani, S, Pasian, F, Pedersen, K, Pettorino, V, Pires, S, Poncet, M, Popa, L, Pozzetti, L, Raison, F, Rebolo, R, Rhodes, J, Roncarelli, M, Rossetti, E, Saglia, R, Schneider, P, Secroun, A, Seidel, G, Sirignano, C, Sirri, G, Stanco, L, Starck, Jl, Tallada-Crespi, P, Taylor, An, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Valentijn, Ea, Valenziano, L, Wang, Y, Welikala, N, Weller, J, Zamorani, G, Zoubian, J, Baldi, M, Bardelli, S, Camera, S, Farinelli, R, Medinaceli, E, Mei, S, Polenta, G, Romelli, E, Tenti, M, Vassallo, T, Zacchei, A, Zucca, E, Baccigalupi, C, Balaguera-Antolinez, A, Biviano, A, Borgani, S, Bozzo, E, Burigana, C, Cappi, A, Carvalho, C, Casas, S, Castignani, G, Colodro-Conde, C, Coupon, J, de la Torre, S, Fabricius, M, Farina, M, Ferreira, Pg, Flose-Reimberg, P, Fotopoulou, S, Galeotta, S, Ganga, K, Garcia-Bellido, J, Gaztanaga, E, Gozaliasl, G, Hook, Im, Joachimi, B, Kansal, V, Kashlinsky, A, Keihanen, E, Kirkpatrick, Cc, Lindholm, V, Mainetti, G, Maino, D, Maoli, R, Martinelli, M, Martinet, N, Mccracken, Hj, Metcalf, Rb, Morgante, G, Morisset, N, Nightingale, J, Nucita, A, Patrizii, L, Potter, D, Renzi, A, Riccio, G, Sanchez, Ag, Sapone, D, Schirmer, M, Schultheis, M, Scottez, V, Sefusatti, E, Teyssier, R, Tutusaus, I, Valiviita, J, Viel, M, Whittaker, L, Knapen, Jh, Department of Physics, Research Program in Systems Oncology, and Helsinki Institute of Physics

Subjects
INFORMATION, structure [Galaxies], FOS: Physical sciences, Techniques: image processing, Morphology (biology), observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Cosmology: observation, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, DEPENDENCE, Galaxies: structure, galaxies, evolution, 0103 physical sciences, image processing [Techniques], structure, Survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, COSMOS, Physics, 010308 nuclear & particles physics, galaxie, Cosmology: observations, [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxies: evolution, Física, Astronomy and Astrophysics, technique, 115 Astronomy, Space science, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, techniques, image processing, surveys, cosmology, observations, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SIMULATION, Generative grammar
Abstract

Artículo escrito por un elevado número de autores, sólo se referencian el que aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere., We present a machine learning framework to simulate realistic galaxies for the Euclid Survey, producing more complex and realistic galaxies than the analytical simulations currently used in Euclid. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of 0.4 deg2 as it will be seen by the Euclid visible imager VIS, and we show that galaxy structural parameters are recovered to an accuracy similar to that for pure analytic Sérsic profiles. Based on these simulations, we estimate that the Euclid Wide Survey (EWS) will be able to resolve the internal morphological structure of galaxies down to a surface brightness of 22.5 mag arcsec-2, and the Euclid Deep Survey (EDS) down to 24.9 mag arcsec-2. This corresponds to approximately 250 million galaxies at the end of the mission and a 50% complete sample for stellar masses above 1010.6 M (resp. 109.6 M) at a redshift z ∼ 0.5 for the EWS (resp. EDS). The approach presented in this work can contribute to improving the preparation of future high-precision cosmological imaging surveys by allowing simulations to incorporate more realistic galaxies

Published
2021

141. Systematic search for lensed X-ray sources in the CLASH fields

Author

Liu, Ang, primary, Tozzi, Paolo, additional, Rosati, Piero, additional, Bergamini, Pietro, additional, Caminha, Gabriel Bartosch, additional, Gilli, Roberto, additional, Grillo, Claudio, additional, Meneghetti, Massimo, additional, Mercurio, Amata, additional, Nonino, Mario, additional, and Vanzella, Eros, additional

Published
2021
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142. KLEVER survey: nitrogen abundances at z ∼ 2 and probing the existence of a fundamental nitrogen relation.

Author

Hayden-Pawson, Connor, Curti, Mirko, Maiolino, Roberto, Cirasuolo, Michele, Belfiore, Francesco, Cappellari, Michele, Concas, Alice, Cresci, Giovanni, Cullen, Fergus, Kobayashi, Chiaki, Mannucci, Filippo, Marconi, Alessandro, Meneghetti, Massimo, Mercurio, Amata, Peng, Yingjie, Swinbank, Mark, and Vincenzo, Fiorenzo

Subjects
GALACTIC redshift, ASTRONOMICAL surveys, AGE of stars, STAR formation, GALACTIC evolution, STELLAR mass
Abstract

We present a comparison of the nitrogen-to-oxygen ratio (N/O) in 37 high-redshift galaxies at z ∼ 2 taken from the KMOS Lensed Emission Lines and VElocity Review (KLEVER) Survey with a comparison sample of local galaxies, taken from the Sloan Digital Sky Survey (SDSS). The KLEVER sample shows only a mild enrichment in N/O of +0.1 dex when compared to local galaxies at a given gas-phase metallicity (O/H), but shows a depletion in N/O of −0.35 dex when compared at a fixed stellar mass (M *). We find a strong anticorrelation in local galaxies between N/O and SFR in the M *–N/O plane, similar to the anticorrelation between O/H and SFR found in the mass–metallicity relation (MZR). We use this anticorrelation to construct a fundamental nitrogen relation (FNR), analogous to the fundamental metallicity relation (FMR). We find that KLEVER galaxies are consistent with both the FMR and the FNR. This suggests that the depletion of N/O in high- z galaxies when considered at a fixed M * is driven by the redshift evolution of the mass–metallicity relation in combination with a near redshift-invariant N/O–O/H relation. Furthermore, the existence of an fundamental nitrogen relation suggests that the mechanisms governing the fundamental metallicity relation must be probed by not only O/H, but also N/O, suggesting pure-pristine gas inflows are not the primary driver of the FMR, and other properties such as variations in galaxy age and star formation efficiency must be important. [ABSTRACT FROM AUTHOR]

Published
2022
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143. Three Hundred project: dissecting the Fundamental Plane of galaxy clusters up to z = 1.

Author

Díaz-García, Luis A, Umetsu, Keiichi, Rasia, Elena, Cui, Weiguang, and Meneghetti, Massimo

Subjects
GALAXY clusters, PLANCK (Artificial satellite), DARK matter
Abstract

We perform a systematic study of the recently discovered Fundamental Plane of galaxy clusters (CFP) using ∼250 simulated clusters from The Three Hundred project, focusing on the stability of the plane against different temperature definitions and its dependence on the dynamical relaxation state of clusters. The CFP is characterized by |$T\propto M_\mathrm{s}^\alpha \, r_\mathrm{s}^\beta$|⁠ , defined with the gas temperature (T) and the characteristic halo scale radius and mass (r s and M s) assuming a Navarro–Frenk–White halo description. We explore two definitions of weighted temperatures, namely mass-weighted and spectroscopic-like temperatures, in three radial ranges. The Three Hundred project clusters at z  = 0 lie on a thin plane whose parameters (α, β) and dispersion (0.015–0.030 dex) depend on the gas temperature definition. The CFP for mass-weighted temperatures is closer to the virial equilibrium expectation (α = 1, β = −1) with a smaller dispersion. For gas temperatures measured within |$500\ h^{-1}$|  kpc, the resulting CFP deviates the most from the virial expectation and shifts towards the similarity solution for a secondary infall model (α = 1.5, β = −2). Independently of the temperature definition, we find that clusters at z  = 1 and relaxed clusters form a CFP similar to the virial expectation, unlike disturbed clusters exhibiting stronger evolution. Only systems formed over the last 4 Gyr present a CFP that is closer to the similarity solution. All these findings are compatible with the CFP obtained for a Cluster Lensing And Supernova survey with Hubble subsample excluding the hottest clusters with T X > 12 keV. [ABSTRACT FROM AUTHOR]

Published
2022
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145. Euclid preparation

Author

Euclid Collaboration, Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., CARDONE, Vincenzo Fabrizio, Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, Erik, Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Conti, I. F., Sánchez, A. G., Sapone, D., SCARAMELLA, Roberto, Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., AURICCHIO, NATALIA, Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Baldi, M., VALENZIANO, LUCA, Vannier, M., Vassallo, T., Zoubian, J., ZUCCA, Elena, BARDELLI, Sandro, Biviano, A., BONINO, Donata, Borsato, E., Bozzo, E., Branchini, Enzo Franco, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., BURIGANA, CARLO, Camera, S., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Casas, S., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., FRAILIS, Marco, Fumana, M., GALEOTTA, Samuele, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B. R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., Maciaszek, T., MAIORANO, Elisabetta, Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., MEDINACELI VILLEGAS, EDUARDO, Mei, S., Mellier, Y., MENEGHETTI, MASSIMO, Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., PASIAN, Fabio, Pettorino, V., Pires, S., Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Queen Mary University of London (QMUL), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), and Euclid Collaboration

Subjects
Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, gravitational lensing: weak, Shear (geology), Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, addenda, errata
Abstract

International audience; Authors Lacasa, Martinelli, Pourtsidou, Tutusaus, were inadvertently missed from the original authorship list. This is now corrected.

Published
2020

146. Three Gravitationally Lensed Supernovae Behind Clash Galaxy Clusters

Author

Patel, Brandon, McCully, Curtis, Jha, Saurbh W, Rodney, Steven A, Jones, David O, Graur, Or, Merten, Julian, Zitrin, Adi, Riess, Adam G, Matheson, Thomas, Sako, Masao, Holoien, Thomas W. -S, Postman, Marc, Coe, Dan, Bartelmann, Matthias, Balestra, Italo, Benitez, Narciso, Bouwens, Rychard, Bradley, Larry, Broadhurst, Tom, Cenko, Stephen Bradley, Donahue, Megan, Filippenko, Alexei V, Ford, Holland, Garnavich, Peter, Grillo, Claudio, Infante, Leopoldo, Jouvel, Stephanie, Kelson, Daniel, Koekemoer, Anton, Lahav, Ofer, Lemze, Doron, Maoz, Dan, Medezinski, Elinor, Melchior, Peter, Meneghetti, Massimo, Molino, Alberto, Moustakas, John, Moustakas, Leonidas A, Nonino, Mario, Rosati, Piero, Seitz, Stella, Strolger, Louis G, Umetsu, Keiichi, and Zheng, Wei

Subjects
Astronomy, Astrophysics
Abstract

We report observations of three gravitationally lensed supernovae (SNe) in the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program. These objects, SN CLO12Car (z = 1.28), SN CLN12Did (z = 0.85), and SN CLA11Tib (z = 1.14), are located behind three different clusters, MACSJ1720.2+3536 (z = 0.391), RXJ1532.9+3021 (z = 0.345), and A383 (z = 0.187), respectively. Each SN was detected in Hubble Space Telescope optical and infrared images. Based on photometric classification, we find that SNe CLO12Car and CLN12Did are likely to be Type Ia supernovae (SNe Ia), while the classification of SN CLA11Tib is inconclusive. Using multi-color light-curve fits to determine a standardized SN Ia luminosity distance, we infer that SN CLO12Car was approx. 1.0 +/- 0.2 mag brighter than field SNe Ia at a similar redshift and ascribe this to gravitational lens magnification. Similarly, SN CLN12Did is approx. 0.2 +/- 0.2 mag brighter than field SNe Ia. We derive independent estimates of the predicted magnification from CLASH strong+weak-lensing maps of the clusters (in magnitude units, 2.5 log10 μ): 0.83 +/- 0.16 mag for SN CLO12Car, 0.28 +/- 0.08 mag for SN CLN12Did, and 0.43 +/- 0.11 mag for SN CLA11Tib. The two SNe Ia provide a new test of the cluster lens model predictions: we find that the magnifications based on the SN Ia brightness and those predicted by the lens maps are consistent. Our results herald the promise of future observations of samples of cluster-lensed SNe Ia (from the ground or space) to help illuminate the dark-matter distribution in clusters of galaxies, through the direct determination of absolute magnifications.

Published
2014
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147. Constraints on the [C ii] luminosity of a proto-globular cluster at z ∼ 6 obtained with ALMA

Author

Calura, Francesco, primary, Vanzella, Eros, additional, Carniani, Stefano, additional, Gilli, Roberto, additional, Rosati, Piero, additional, Meneghetti, Massimo, additional, Paladino, Rosita, additional, Decarli, Roberto, additional, Brusa, Marcella, additional, Lupi, Alessandro, additional, D’Amato, Quirino, additional, Bergamini, Pietro, additional, and Caminha, Gabriel B, additional

Published
2020
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148. A magnified young galaxy from about 500 million years after the Big Bang

Author

Zheng, Wei, Postman, Marc, Zitrin, Adi, Moustakas, John, Shu, Xinwen, Jouvel, Stephanie, Høst, Ole, Molino, Alberto, Bradley, Larry, Coe, Dan, Moustakas, Leonidas A., Carrasco, Mauricio, Ford, Holland, Benítez, Narciso, Lauer, Tod R., Seitz, Stella, Bouwens, Rychard, Koekemoer, Anton, Medezinski, Elinor, Bartelmann, Matthias, Broadhurst, Tom, Donahue, Megan, Grillo, Claudio, Infante, Leopoldo, Jha, Saurabh W., Kelson, Daniel D., Lahav, Ofer, Lemze, Doron, Melchior, Peter, Meneghetti, Massimo, Merten, Julian, Nonino, Mario, Ogaz, Sara, Rosati, Piero, Umetsu, Keiichi, and van der Wel, Arjen

Published
2012
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149. An excess of small-scale gravitational lenses observed in galaxy clusters

Author

Meneghetti, Massimo, primary, Davoli, Guido, additional, Bergamini, Pietro, additional, Rosati, Piero, additional, Natarajan, Priyamvada, additional, Giocoli, Carlo, additional, Caminha, Gabriel B., additional, Metcalf, R. Benton, additional, Rasia, Elena, additional, Borgani, Stefano, additional, Calura, Francesco, additional, Grillo, Claudio, additional, Mercurio, Amata, additional, and Vanzella, Eros, additional

Published
2020
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