scholarly journals The XXL Survey

2018 ◽  
Vol 620 ◽  
pp. A4 ◽  
Author(s):  
E. Koulouridis ◽  
L. Faccioli ◽  
A. M. C. Le Brun ◽  
M. Plionis ◽  
I. G. McCarthy ◽  
...  
Keyword(s):  
Galactic Nuclei ◽  
Mass Function ◽  
Detection Algorithm ◽  
Ratio Distribution ◽  
X Ray ◽  
Massive Galaxies ◽  
Projected Clustering ◽  
Galaxy Groups ◽  
Bolometric Luminosity ◽  
Hydrodynamical Simulations

Modern cosmological simulations heavily rely on feedback from active galactic nuclei (AGN) in order to stave off overcooling in massive galaxies, and galaxy groups and clusters. Given that AGN are a key component of such simulations, an important independent test is whether or not the simulations capture the broad demographics of the observed AGN population. However, to date, comparisons between observed and simulated AGN populations have been relatively limited. Here, we have used the cosmo-OWLS suite of cosmological hydrodynamical simulations to produce realistic synthetic catalogs of X-ray AGN out to z = 3, with the aim of comparing the catalogs to the observed X-ray AGN population in the XXL survey and other recent surveys. We focused on the unabsorbed X-ray luminosity function (XLF), the Eddington ratio distribution, the black hole mass function, and the projected clustering of X-ray AGN. To compute the unabsorbed XLF of the simulated AGN, we used recent empirically-determined (luminosity-dependent) bolometric corrections, in order to convert the simulated bolometric luminosity into an observable X-ray luminosity. We show that, using these corrections, the simulated AGN sample accurately reproduces the observed XLF over 3 orders of magnitude in X-ray luminosity in all redshift bins from z = 0 out to z = 3. To compare to the observed Eddington ratio distribution and the clustering of AGN, we produced detailed “XMM-Newton-detected” catalogs of the simulated AGN. This requires the production of synthetic X-ray images extracted from light cones of the simulations, which self-consistently contain both the X-ray AGN and the emission from diffuse, hot gas within galaxies, galaxy groups, and clusters and that fold in the relevant instrumental effects of XMM-Newton. We apply a luminosity- and redshift-dependent obscuration function for the AGN and employ the same AGN detection algorithm as used for the real XXL survey. We demonstrate that the detected population of simulated AGN reproduces the observed Eddington ratio distribution and projected clustering from XXL quite well. Based on these comparisons, we conclude that the simulations have a broadly realistic population of AGN and that our synthetic X-ray AGN catalogs should be useful for interpreting additional trends (e.g. environmental dependencies) and as a helpful tool for quantifying AGN contamination in galaxy group and cluster X-ray surveys.

scholarly journals On the occupation of X-ray-selected galaxy groups by radio active galactic nuclei since z = 1.3★

2011 ◽  
Vol 416 (1) ◽  
pp. L31-L35 ◽  
Author(s):  
V. Smolčić ◽  
A. Finoguenov ◽  
G. Zamorani ◽  
E. Schinnerer ◽  
M. Tanaka ◽  
...  
Keyword(s):  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
X Ray ◽  
Galaxy Groups

scholarly journals The relation between the diffuse X-ray luminosity and the radio power of the central AGN in galaxy groups

2020 ◽  
Vol 497 (2) ◽  
pp. 2163-2174
Author(s):  
T Pasini ◽  
M Brüggen ◽  
F de Gasperin ◽  
L Bîrzan ◽  
E O’Sullivan ◽  
...  
Keyword(s):  
Radio Emission ◽  
Galaxy Clusters ◽  
Active Galactic Nucleus ◽  
Statistical Tests ◽  
Control Sample ◽  
Radio Galaxies ◽  
Very Large Array ◽  
X Ray ◽  
Galaxy Groups ◽  
Hydrodynamical Simulations

ABSTRACT Our understanding of how active galactic nucleus feedback operates in galaxy clusters has improved in recent years owing to large efforts in multiwavelength observations and hydrodynamical simulations. However, it is much less clear how feedback operates in galaxy groups, which have shallower gravitational potentials. In this work, using very deep Very Large Array and new MeerKAT observations from the MIGHTEE survey, we compiled a sample of 247 X-ray selected galaxy groups detected in the COSMOS field. We have studied the relation between the X-ray emission of the intra-group medium and the 1.4 GHz radio emission of the central radio galaxy. For comparison, we have also built a control sample of 142 galaxy clusters using ROSAT and NVSS data. We find that clusters and groups follow the same correlation between X-ray and radio emission. Large radio galaxies hosted in the centres of groups and merging clusters increase the scatter of the distribution. Using statistical tests and Monte Carlo simulations, we show that the correlation is not dominated by biases or selection effects. We also find that galaxy groups are more likely than clusters to host large radio galaxies, perhaps owing to the lower ambient gas density or a more efficient accretion mode. In these groups, radiative cooling of the intra-cluster medium could be less suppressed by active galactic nucleus heating. We conclude that the feedback processes that operate in galaxy clusters are also effective in groups.

scholarly journals The role of galaxy mass on AGN emission: a view from the VANDELS survey

2020 ◽  
Vol 493 (3) ◽  
pp. 3838-3853 ◽  
Author(s):  
M Magliocchetti ◽  
L Pentericci ◽  
M Cirasuolo ◽  
G Zamorani ◽  
R Amorin ◽  
...  
Keyword(s):  
Formation Rate ◽  
Galactic Nuclei ◽  
Host Galaxy ◽  
Radio Luminosity ◽  
Ancillary Data ◽  
X Ray ◽  
Massive Galaxies ◽  
Fundamental Quantity ◽  
Stellar Masses

ABSTRACT We present a comparative analysis of the properties of active galactic nuclei (AGNs) emitting at radio and X-ray wavelengths. The study is performed on 907 X-ray AGNs and 100 radio AGNs selected on the CDFS and UDS fields and makes use of new and ancillary data available to the VANDELS collaboration. Our results indicate that the mass of the host galaxy is a fundamental quantity that determines the level of AGN activity at the various wavelengths. Indeed, large stellar masses are found to be connected with AGN radio emission, as virtually all radio-active AGNs reside within galaxies of M* > 1010 M⊙. Large stellar masses also seem to favour AGN activity in the X-ray, even though X-ray AGNs present a mass distribution that is more spread out and with a non-negligible tail at M* ≲ 109 M⊙. Stellar mass alone is also observed to play a fundamental role in simultaneous radio and X-ray emission: the percentage of AGNs active at both wavelengths increases from around 1 per cent of all X-ray AGNs residing within hosts of M* < 1011 M⊙ to ∼13 per cent in more massive galaxies. In the case of radio-selected AGNs, such a percentage moves from ∼15 per cent to ∼45 per cent (but up to ∼80 per cent in the deepest fields). Neither cosmic epoch, nor radio luminosity, X-ray luminosity, Eddington ratio or star formation rate of the hosts are found to be connected to an enhanced probability for joint radio + X-ray emission of AGN origin. Furthermore, only a loose relation is observed between X-ray and radio luminosity in those AGNs that are simultaneously active at both frequencies.

scholarly journals IGM Heating and AGN activity in Fossil Galaxy Groups

2013 ◽  
Vol 9 (S304) ◽  
pp. 349-350
Author(s):  
H. Miraghaei ◽  
H. G. Khosroshahi ◽  
H.-R. Klöckner ◽  
T. J. Ponman ◽  
N. N. Jetha ◽  
...  
Keyword(s):  
Active Galactic Nuclei ◽  
Intergalactic Medium ◽  
Galactic Nuclei ◽  
Heating Power ◽  
X Ray ◽  
Galaxy Groups ◽  
Recent Group ◽  
Emission Loss

AbstractFossil galaxy groups are energetically and morphologically ideal environments to study the intergalactic medium (IGM) heating, because their inter-galactic gas is undisturbed due to the lack of recent group scale mergers. We study the role of active galactic nuclei (AGN) in heating the IGM in a sample of five fossil galaxy groups by employing properties at 610 MHz and 1.4 GHz. We find that two of the dominant galaxies in fossil groups, ESO 3060170 and RX J1416.4+2315, are associated with the radio lobes. We evaluate the PdV work of the radio lobes and their corresponding heating power and compare to the X-ray emission loss within cooling radius. Our results show that the power due to mechanical heating is not sufficiently high to suppress the cooling.

scholarly journals Constraints on precipitation-limited hot haloes from massive galaxies to galaxy clusters

2020 ◽  
Vol 501 (2) ◽  
pp. 2467-2477
Author(s):  
Priyanka Singh ◽  
G M Voit ◽  
Biman B Nath
Keyword(s):  
Time Scale ◽  
Free Fall ◽  
Mass Range ◽  
Model Parameters ◽  
Data Sets ◽  
X Ray ◽  
Massive Galaxies ◽  
Galaxy Groups ◽  
Diffuse Halo ◽  
Halo Gas

ABSTRACT We present constraints on a simple analytical model for hot diffuse halo gas, derived from a fit spanning two orders of magnitude in halo mass ($M_{500} \sim 10^{12.5}\!-\!10^{14.5} \, \mathrm{M}_{\odot }$). The model is motivated by the observed prevalence of a precipitation limit, and its main free parameter is the central ratio of gas cooling time-scale to free-fall time-scale (tcool/tff). We use integrated X-ray and thermal Sunyaev–Zel’dovich observations of the environments around massive galaxies, galaxy groups, and clusters, averaged in halo mass bins, and obtain the best-fitting model parameters. We find tcool/tff ∼ 50–110, depending on the model extrapolation beyond the halo virial radius and possibly on biases present in the data sets used in the fitting analysis. The model adequately describes the entire mass range, except for intermediate mass haloes ($M_{500} \sim 10^{13.5} \, \mathrm{M}_{\odot }$) that systematically fall below the model predictions. However, the best fits for tcool/tff substantially exceed the values typically derived from X-ray observations of individual systems (tcool/tff ∼ 10–30). We consider several explanations for those discrepancies, including X-ray selection biases and a potential anticorrelation between X-ray luminosity and the central galaxy’s stellar mass.

scholarly journals X-RAY SPECTRAL CONSTRAINTS FORz≈ 2 MASSIVE GALAXIES: THE IDENTIFICATION OF REFLECTION-DOMINATED ACTIVE GALACTIC NUCLEI

2011 ◽  
Vol 738 (1) ◽  
pp. 44 ◽  
Author(s):  
D. M. Alexander ◽  
F. E. Bauer ◽  
W. N. Brandt ◽  
E. Daddi ◽  
R. C. Hickox ◽  
...  
Keyword(s):  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
X Ray ◽  
Massive Galaxies

scholarly journals The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

2019 ◽  
Vol 489 (2) ◽  
pp. 2439-2470 ◽  
Author(s):  
Nicholas A Henden ◽  
Ewald Puchwein ◽  
Debora Sijacki
Keyword(s):  
High Redshift ◽  
Scaling Relations ◽  
Observational Constraints ◽  
Lower Mass ◽  
X Ray ◽  
Galaxy Groups ◽  
Mass Scaling ◽  
Low Mass ◽  
Hydrodynamical Simulations ◽  
Intrinsic Scatter

Abstract We study the redshift evolution of the X-ray and Sunyaev–Zel’dovich (SZ) scaling relations for galaxy groups and clusters in the fable suite of cosmological hydrodynamical simulations. Using an expanded sample of 27 high-resolution zoom-in simulations, together with a uniformly sampled cosmological volume to sample low-mass systems, we find very good agreement with the majority of observational constraints up to z ∼ 1. We predict significant deviations of all examined scaling relations from the simple self-similar expectations. While the slopes are approximately independent of redshift, the normalizations evolve positively with respect to self-similarity, even for commonly used mass proxies such as the YX parameter. These deviations are due to a combination of factors, including more effective active galactic nuclei feedback in lower mass haloes, larger binding energy of gas at a given halo mass at higher redshifts, and larger non-thermal pressure support from kinetic motions at higher redshifts. Our results have important implications for cluster cosmology from upcoming SZ surveys such as SPT-3G, ACTpol, and CMB-S4, as relatively small changes in the observable–mass scaling relations (within theoretical uncertainties) have a large impact on the predicted number of high-redshift clusters and hence on our ability to constrain cosmology using cluster abundances. In addition, we find that the intrinsic scatter of the relations, which agrees well with most observational constraints, increases at lower redshifts and for lower mass systems. This calls for a more complex parametrization than adopted in current observational studies to be able to accurately account for selection biases.

scholarly journals A new RASS galaxy cluster catalogue with low contamination extending to z ∼ 1 in the DES overlap region

2019 ◽  
Vol 488 (1) ◽  
pp. 739-769 ◽  
Author(s):  
M Klein ◽  
S Grandis ◽  
J J Mohr ◽  
M Paulus ◽  
T M C Abbott ◽  
...  
Keyword(s):  
Matched Filter ◽  
Galaxy Cluster ◽  
Galactic Nuclei ◽  
Mass Function ◽  
Optical Data ◽  
X Ray ◽  
Sky Survey ◽  
Infrared Sources ◽  
Step Selection

ABSTRACT We present the MARD-Y3 catalogue of between 1086 and 2171 galaxy clusters (52 per cent and 65 per cent new) produced using multicomponent matched filter (MCMF) follow-up in 5000 deg2 of DES-Y3 optical data of the ∼20 000 overlapping ROSAT All-Sky Survey source catalogue (2RXS) X-ray sources. Optical counterparts are identified as peaks in galaxy richness as a function of redshift along the line of sight towards each 2RXS source within a search region informed by an X-ray prior. All peaks are assigned a probability fcont of being a random superposition. The clusters lie at 0.02 < z < 1.1 with more than 100 clusters at z > 0.5. Residual contamination is 2.6 per cent and 9.6 per cent for the cuts adopted here. For each cluster we present the optical centre, redshift, rest frame X-ray luminosity, M500 mass, coincidence with NWAY infrared sources, and estimators of dynamical state. About 2 per cent of MARD-Y3 clusters have multiple possible counterparts, the photo-z’s are high quality with σΔz/(1 + z) = 0.0046, and ∼1 per cent of clusters exhibit evidence of X-ray luminosity boosting from emission by cluster active galactic nuclei. Comparison with other catalogues (MCXC, RM, SPT-SZ, Planck) is performed to test consistency of richness, luminosity, and mass estimates. We measure the MARD-Y3 X-ray luminosity function and compare it to the expectation from a fiducial cosmology and externally calibrated luminosity- and richness–mass relations. Agreement is good, providing evidence that MARD-Y3 has low contamination and can be understood as a simple two step selection – X-ray and then optical – of an underlying cluster population described by the halo mass function.

scholarly journals GOODS-ALMA: 1.1 mm galaxy survey

2018 ◽  
Vol 620 ◽  
pp. A152 ◽  
Author(s):  
M. Franco ◽  
D. Elbaz ◽  
M. Béthermin ◽  
B. Magnelli ◽  
C. Schreiber ◽  
...  
Keyword(s):  
Near Infrared ◽  
Detection Algorithm ◽  
Point Sources ◽  
Blind Detection ◽  
Expected Number ◽  
Photometric Redshifts ◽  
Mid Infrared ◽  
X Ray ◽  
Massive Galaxies ◽  
Number Counts

Aims. We present a 69 arcmin2 ALMA survey at 1.1 mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band part of the GOODS-South field. Methods. We tapered the 0″24 original image with a homogeneous and circular synthesized beam of 0″60 to reduce the number of independent beams – thus reducing the number of purely statistical spurious detections – and optimize the sensitivity to point sources. We extracted a catalog of galaxies purely selected by ALMA and identified sources with and without HST counterparts down to a 5σ limiting depth of H = 28.2 AB (HST/WFC3 F160W). Results. ALMA detects 20 sources brighter than 0.7 mJy at 1.1 mm in the 0″60 tapered mosaic (rms sensitivity σ ≃ 0.18 mJy beam−1) with a purity greater than 80%. Among these detections, we identify three sources with no HST nor Spitzer-IRAC counterpart, consistent with the expected number of spurious galaxies from the analysis of the inverted image; their definitive status will require additional investigation. We detect additional three sources with HST counterparts either at high significance in the higher resolution map, or with different detection-algorithm parameters ensuring a purity greater than 80%. Hence we identify in total 20 robust detections. Conclusions. Our wide contiguous survey allows us to push further in redshift the blind detection of massive galaxies with ALMA with a median redshift of z = 2.92 and a median stellar mass of M⋆ = 1.1 × 1011 M⊙. Our sample includes 20% HST-dark galaxies (4 out of 20), all detected in the mid-infrared with Spitzer-IRAC. The near-infrared based photometric redshifts of two of them (z ∼ 4.3 and 4.8) suggest that these sources have redshifts z >  4. At least 40% of the ALMA sources host an X-ray AGN, compared to ∼14% for other galaxies of similar mass and redshift. The wide area of our ALMA survey provides lower values at the bright end of number counts than single-dish telescopes affected by confusion.

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