AGN and starburst radio activity in the A3558 cluster complex

Giacintucci, S.; Venturi, T.; Bardelli, S.; Dallacasa, D.; Zucca, E.

doi:10.1051/0004-6361:20040071

Cited by 21 publications

(42 citation statements)

References 50 publications

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“…By plotting the adaptively smoothed isodensity contours of all galaxies in this bin, we found that the overdensity coincides with two galaxy clumps close to each other (∼4 Mpc). This fact is consistent with the claim of Owen et al (1999) that cluster merging triggers radio emission (see also Giacintucci et al 2004). Unfortunately, no velocity dispersion estimate is possible because the two clumps are located just outside the region covered by the spectroscopic survey.…”

Section: The Redshift Distributionssupporting

confidence: 93%

The VVDS-VLA deep field

Bardelli

Zucca

Bolzonella

et al. 2008

A&A

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Aims. The availability of wide angle and deep surveys, both in the optical and the radio band, allows us to explore the evolution of radio sources with optical counterparts up to redshift z ∼ 1.1 in an unbiased way using large numbers of radio sources and well defined control samples of radio-quiet objects. Methods. We use the 1.4 GHz VIMOS-VLA Deep Survey, the optical VIMOS-VLT Deep Survey and the CFHT Legacy Survey to compare the properties of radio-loud galaxies with respect to the whole population of optical galaxies. The availability of multiband photometry and high quality photometric redshifts allows us to derive rest-frame colors and radio luminosity functions to a limit of a B rest-frame magnitude of M B = −20. We derive spectrophotometric types, following the classification of Zucca et al. (2006, A&A, 455, 879), in order to have a priori knowledge of the optical evolution of different galaxy classes. Results. Galaxy properties and luminosity functions are estimated up to z ∼ 1 for radio-loud and radio-quiet early and late type galaxies. Radioloud late type galaxies show significantly redder colors than radio-quiet objects of the same class and this is related to the presence of more dust in stronger star forming galaxies. We estimate the optical luminosity functions, stellar masses and star formation rate distributions for radio sources and compare them with those derived for a well defined control sample, finding that the probability of a galaxy to be a radio emitter significantly increases at high values of these parameters. Radio-loud early type galaxies exhibit luminosity evolution in their bivariate radio-optical luminosity function, due to evolution in the radio-optical ratio. The lack of evolution of the mass function of radio-loud early type galaxies means that no new AGN are formed at redshift z < 1. In contrast, radio-loud late type objects exhibit a strong evolution, both in luminosity and density, of the radio luminosity function for z > 0.7. This evolution is a direct effect of the strong optical evolution of this class and no significant change with redshift in the radio-optical ratio is required. With the knowledge of the radio-optical ratio and the optical and radio luminosity functions for late type galaxies, we show that it is possible to estimate the star formation history of the Universe up to redshift z ∼ 1.5, using optical galaxies as tracers of the global radio emission.

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Section: The Redshift Distributionssupporting

confidence: 93%

The VVDS-VLA deep field

Bardelli

Zucca

Bolzonella

et al. 2008

A&A

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“…But alongside there also are contradictory findings according to which mergers may as well strip away gas from galaxies and result in inhibition of both the processes (e.g. see Giacintucci et al 2004). Thirdly, a configuration containing a NCC cluster with zero mass deposition rate and a central radio source may be obtained through a merger between a NCC cluster and a CC cluster, latter harboring a central AGN, in such a way that it results in disruption of the cool core and leaves behind only traces of the past cooling activity.…”

Section: Cooling and Agn Activitymentioning

confidence: 99%

AGN heating and ICM cooling in the $\textit{HIFLUGCS}$ sample of galaxy clusters

Mittal

Hudson²,

Reiprich³

et al. 2009

A&A

184

248

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Active galactic nuclei (AGN) at the center of galaxy clusters with gas cooling times that are much shorter than the Hubble time have emerged as heating agents powerful enough to prevent further cooling of the intracluster medium (ICM). We carried out an intensive study of the AGN heating−ICM cooling network by comparing various cluster parameters to the integrated radio luminosity of the central AGN, L R , defined as the total synchrotron power between 10 MHz and 15 GHz. This study is based on the HIFLUGCS sample comprising the 64 X-ray brightest galaxy clusters. We adopted the central cooling time, t cool , as the diagnostic to ascertain cooling properties of the HIFLUGCS sample and classify clusters with t cool < 1 Gyr as strong cool-core (SCC) clusters, with 1 Gyr < t cool < 7.7 Gyr as weak cool-core (WCC) clusters and with t cool > 7.7 Gyr as non-cool-core (NCC) clusters. We find 48 out of 64 clusters (75%) contain cluster center radio sources (CCRS) cospatial with or within 50 h −1 71 kpc of the X-ray peak emission. Furthermore, we find that the probability of finding a CCRS increases from 45% to 67% to 100% for NCC, WCC, and SCC clusters, respectively.We use a total of ∼140 independent radio flux-density measurements, with data at more than two frequencies for more than 54% of the sources extending below 500 MHz, enabling the determination of accurate estimates of L R . We find that L R in SCC clusters depends strongly on the cluster scale such that more massive clusters harbor more powerful radio AGN. The same trend is observed between L R and the classical mass deposition rate,Ṁ classical in SCC and partly also in WCC clusters, and can be quantified as L R ∝Ṁ 1.69±0.25 classical . We also perform correlations of the luminosity for the brightest cluster galaxy, L BCG , close to the X-ray peak in all 64 clusters with L R and cluster parameters, such as the virial mass, M 500 , and the bolometric X-ray luminosity, L X . To this end, we use the 2MASS K-band magnitudes and invoke the near-infrared bulge luminosity-black hole mass relation to convert L BCG to supermassive black hole mass, M BH . We find a weak correlation between M BH and L R for SCC clusters, L R ∼ M 4.10±0.42 BH , although with a few outliers. We find an excellent correlation of L BCG with M 500 and L X for the entire sample, the SCC clusters showing a tighter trend in both the cases. We discuss the plausible reasons behind these scaling relations in the context of cooling flows and AGN feedback.Our results strongly suggest an AGN-feedback machinery in SCC clusters, which regulates the cooling in the central regions. Since the dispersion in these correlations, such as that between L R andṀ classical or L R and M BH , increases in going from SCC to WCC clusters, we conclude there must be secondary processes that work either in conjunction with the AGN heating or independently to counteract the radiative losses in WCC clusters.

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“…However, Best et al (2005) claim that the phenomena generating the emission lines and the radio emission are statistically independent, even if recent results indicate that radio-loud emission-line AGN favour higher densities than radio-quiet ones (Kauffmann et al 2008) (see also Caputi et al 2009, for a study in the IR). Secondly, only specific environments have been considered, mainly clusters or groups (Miller et al 2002;Hill & Lilly 1991;Giacintucci et al 2004), and therefore we are lacked coverage of a large dynamical range of densities.…”

Section: Introductionmentioning

confidence: 99%

Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

Bardelli¹,

Schinnerer

Smolčić

et al. 2010

A&A

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Aims. We investigate the properties and the environment of radio sources with optical counterparts from the combined VLA-COSMOS and zCOSMOS samples. The advantage of this sample is the availability of optical spectroscopic informations, high quality redshifts, and accurate density determination. Methods. By comparing the star formation rates estimated from the optical spectral energy distribution with those based on the radio luminosity, we divide the radio sources in to three families passive AGN, non-passive AGN, and star-forming galaxies. These families occupy specific regions of the 8.0−4.5 μm infrared color-specific star-formation plane, from which we extract the corresponding control samples. Results. Only the passive AGN have a significantly different environmental distribution from their control sample. The fraction of radio-loud passive AGN increases from ∼2% in underdense regions to ∼15% for overdensities (1 + δ) greater than 10. This trend is also present as a function of richness of the groups hosting the radio sources. Passive AGN in overdensities tend to have higher radio luminosities than those in lower density environments. Since the black hole mass distribution is similar in both environments, we speculate that, for low radio luminosities, the radio emission is controlled (by fuel availability or confinement of the radio jet by local gas pressure) by the interstellar medium of the host galaxy, while in other cases it is determined by the structure (group or cluster) in which the galaxy resides.

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AGN and starburst radio activity in the A3558 cluster complex

Cited by 21 publications

References 50 publications

The VVDS-VLA deep field

The VVDS-VLA deep field

AGN heating and ICM cooling in the $\textit{HIFLUGCS}$ sample of galaxy clusters

Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

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