Accretion and nuclear activity in Virgo early-type galaxies

Vattakunnel, S.; Trussoni, E.; Capetti, A.; Baldi, Ranieri D.

doi:10.1051/0004-6361/201014611

Cited by 6 publications

(8 citation statements)

References 31 publications

(46 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We note that Vattakunnel et al (2010) provide estimates of jet power andṀB for two additional radio-loud AGNs which do not display extended radio jets or X-ray cavities. For this reason, their jet power estimates are based on an indirect method that relies on using a correlation between core radio luminosity and jet power.…”

Section: Observationsmentioning

confidence: 96%

“…For this reason, their jet power estimates are based on an indirect method that relies on using a correlation between core radio luminosity and jet power. In our sample, we only keep sources for which Pjet was estimated directly from X-ray cavities used as jet calorimeters and hence we exclude the two AGNs studied by Vattakunnel et al (2010). ) Balmaverde et al 2008 Figure 1.…”

Section: Observationsmentioning

confidence: 99%

“…For instance, Allen et al (2006) observed that Pjet ∼ a few per centṀBc 2 (cf. also Merloni & Heinz 2007;Balmaverde, Baldi & Capetti 2008;Vattakunnel et al 2010;. McNamara, Rohanizadegan & Nulsen (2011) found that Pjet >ṀBc 2 for the most powerful radio galaxies, i.e.…”

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

On the efficiency of jet production in radio galaxies

Nemmen¹,

Tchekhovskoy²

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The mechanisms that produce and power relativistic jets are fundamental open questions in black hole (BH) astrophysics. In order to constrain these mechanisms, we analyze the energy efficiency of jet production η based on archival Chandra observations of 27 nearby, low-luminosity active galactic nuclei. We obtain η as the ratio of the jet power, inferred from the energetics of jet powered X-ray emitting cavities, to the BH mass accretion rateṀ BH . The standard assumption in estimatingṀ BH is that all the gas from the Bondi radius r B makes it down to the BH. It is now clear, however, that only a small fraction of the gas reaches the hole. To account for this effect, we use the standard disk mass-loss scaling,Ṁ (r) ∝ (r/r B ) sṀBondi . This leads to much lower values ofṀ BH and higher values of η than in previous studies. If hot accretion flows are characterized by 0.5 s 0.6 -on the lower end of recent theoretical and observational studies -then dynamically-important magnetic fields near rapidly spinning BHs are necessary to account for the high η ≈ 100 − 300 per cent in the sample. Moreover, values of s > 0.6 are essentially ruled out, or there would be insufficient energy to power the jets. We discuss the implications of our results for the distribution of massive BH spins and the possible impact of a significant extra cold gas supply on our estimates.

show abstract

Section: Observationsmentioning

confidence: 96%

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

On the efficiency of jet production in radio galaxies

Nemmen¹,

Tchekhovskoy²

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The location of an AGN within the group/cluster of galaxies might have a profound effect on the level of accretion and, consequently, on its nuclear power (see, e.g., Koulouridis et al 2018). For example, by exploring the properties of early-type galaxies in the Virgo cluster, Vattakunnel et al (2010) found a suggestive trend be-tween jet power and location within the cluster. A similar result was found by Croston et al (2019).…”

Section: Location Of the Rgs Within The Group/cluster Of Galaxiesmentioning

confidence: 99%

Large-scale environment of FR 0 radio galaxies

Capetti

Massaro

Baldi

2020

A&A

Self Cite

View full text Add to dashboard Cite

We explore the properties of the large-scale environment of the sources in the Faranoff-Riley class 0 catalog (FR0CAT). This sample includes 104 compact radio sources that are associated with nearby (z < 0.05) early-type galaxies. Using various estimators, we find that FR 0s are located in regions with higher than the average number of galaxies. The average galaxies density around FR 0s is a factor two lower with respect to FR I radio galaxies. This latter difference is driven by the large fraction (63%) of FR 0s that are located in groups formed by fewer than 15 galaxies. FR Is rarely (17%) inhabit an environment like this. In addition to the lack of substantial extended radio emission that defines the FR 0 class, this is the first significant difference between the properties of these two populations of low-power radio galaxies. We interpret the differences in environment between FR 0s and FR Is as due to an evolutionary link between local galaxies density, black hole spin, jet power, and extended radio emission.

show abstract

“…Bondi accretion is also invoked to estimate accretion rates Ṁ from X-ray observations of hot gas surrounding galaxy-centered and cluster-centered black holes (e.g. Allen et al 2006;Balmaverde et al 2008;Vattakunnel et al 2010). However, as with the cosmological computations, X-ray observations of sources having greater feedback power require mass accretion rates considerably in excess of the Bondi rate (Rafferty et al 2006;Hardcastle et al 2007;McNamara et al 2011).…”

Section: Radiating Bondi Flowsmentioning

confidence: 99%

Radiating Bondi and Cooling Site Flows

Mathews

Guo

2012

ApJ

View full text Add to dashboard Cite

Steady accretion of a radiating gas onto a central mass point is described and compared to classic Bondi accretion. Radiation losses are essential for accretion flows to be observed. Unlike Bondi flows, radiating Bondi flows pass through a sonic point at a finite radius and become supersonic near the center. The morphology of all radiating flows is described by a single dimensionless parameter proportional toṀ /M T s where T s is the gas temperature at the sonic point. In radiating Bondi flows the relationship between the mass accretion rate and central mass,Ṁ ∝ M p with p ∼ 1, differs significantly from the quadratic dependence in classical Bondi flows,Ṁ ∝ M 2 . Mass accretion rates onto galaxy or cluster-centered black holes estimated from traditional and radiating Bondi flows are significantly different. In radiating Bondi flows the gas temperature increases at large radii, as in the cores of many galaxy groups and clusters, allowing radiating Bondi flows to merge naturally with gas arriving from their cluster environments. Some radiating flows cool completely before reaching the center of the flow, and this also occurs in cooling site flows, in which there is no central gravitating mass.

show abstract

Accretion and nuclear activity in Virgo early-type galaxies

Cited by 6 publications

References 31 publications

On the efficiency of jet production in radio galaxies

On the efficiency of jet production in radio galaxies

Large-scale environment of FR 0 radio galaxies

Radiating Bondi and Cooling Site Flows

Contact Info

Product

Resources

About