A Statistical Study of XBLs, RBLs and FSRQs at 1.5 GHz

Zhou, Junyong; Jiang, Fan; Li, Juan; Liu, Yi

doi:10.1088/1009-9271/7/5/03

Cited by 8 publications

(7 citation statements)

References 32 publications

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“…It is therefore expected that beaming model is more pronounced in BLs and FSRQs than in RGs. Thus, these results are quite consistent with a number of previous results on orientation and beaming effects in AGNs (see, e.g., Fan et al 2011;2005;Zhou et al, 2007;Resconi et al 2017;Iyida et al 2021). The fact that RGs, BLs and FSRQs populate distinct and practically like regions in the log Rγ − logLγ,un and Rγ − logLγ,b plots implies that they have distinctive evolutionary histories (e.g.…”

Section: Discussionsupporting

confidence: 93%

Orientation and Beaming Effects in active galactic nuclei: Implication for radio galaxy - Blazar Evolution

Iyida

Onah²,

Eya

et al. 2023

Preprint

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The orientation and evolution based on unified scheme for jetted extragalactic radio sources posits that BL Lacertae objects (BLs), flat-spectrum radio quasars (FSRQs) and normal radio galaxies (RGs) represent increasingly misaligned populations of active galactic nuclei (AGNs). Using compiled radio, X-ray and γ-ray data of 397 blazars and 110 RGs from the Fermi Large Area Telescope (Fermi-LAT) catalogue, we computed the viewing angles, γ-ray core-dominance parameter and γ-ray emission components in order to study the consequences of orientation and relativistic beaming effects on γ-ray properties of RGs, BLs and FSRQs. Our results show continuous distributions of core-dominance parameters (X-ray, RX and γ-ray, Rγ) from RGs at low values, largest viewing angles to FSRQs at high values and BLs subsets with the least values. The difference on the plane is significantly larger for FSRQs and BLs than for RGs, indicating an evolutionary link between them. A two-sample Wilcoxon rank-sum and Kolmogorov-Smirnov tests carried out on our data suggest that the probabilities of the distribution of RX and Rγ of RGs and blazar types to come from the same parent distribution are pWRS ∼ 0 and pK−S < 10-5, suggestive of stronger beaming effects in blazars than in RGs. There is a significant correlation (r > 0.60) between log Rr - log RX for the combined sample types. Furthermore, a significant anti-correlation (r ∼ -0.80) exists in the log Rγ - log Lγ,un plot which is indicative of evolutionary sequence via relativistic beaming model. These results imply that the evolutionary track of jetted AGNs is RGs - BLs FSRQs

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Section: Discussionsupporting

confidence: 93%

Orientation and Beaming Effects in active galactic nuclei: Implication for radio galaxy - Blazar Evolution

Iyida

Onah²,

Eya

et al. 2023

Preprint

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“…Sources of Data Kollgaard et al (1996) compiled x-ray-selected BL Lacs objects (XBLs) detected by First High-Energy Astrophysics Observatory Large Area Sky Survey (HEAO-1 LASS ) and compared their core and extended luminosity with radio-selected BL Lacertae objects (RBLs) from Einstein Medium Sensitivity Survey (EMSS) (Rector et al, 2000) in the range of 10 23 to 10 25 WHz −1 . Zhou et al (2007) later used these same data to do a statistical study of XBLs, RBLs and FSRQs at 1.5GHz. In our work however, we did a careful selection of the data from Zhou et al (2007) and Rector et al (2000) with specific reference to the core luminosity (LC), extended luminosity (LE), core dominance parameter (R), and Redshift (z) for the RBL and XBL samples.…”

Section: 1mentioning

confidence: 99%

“…Zhou et al (2007) later used these same data to do a statistical study of XBLs, RBLs and FSRQs at 1.5GHz. In our work however, we did a careful selection of the data from Zhou et al (2007) and Rector et al (2000) with specific reference to the core luminosity (LC), extended luminosity (LE), core dominance parameter (R), and Redshift (z) for the RBL and XBL samples. Furthermore, we employed Fanaroff-Riley Type I (FRI) radio samples from Wang et al (2006) to complete our sample selection.…”

Section: 1mentioning

confidence: 99%

“…The core dominance parameter also known as the core-to-lobe ratio of an AGN is the ratio of the core luminosity to the extended or lobe luminosity of any active galactic nuclei. This parameter is a measure of the relative orientation of the source (Zhou et al, 2007). Mathematically, considering the relativistic property of the source for two opposite jets, the core dominance parameter was given by Fan…”

mentioning

confidence: 99%

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On the Unification of Low Luminosity Active Galactic Nuclei

et al. 2023

IJFMR

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We have used the distributions of observed radio properties of a subset of AGNs called low luminosity AGNs (LLAGNs) to investigate the relationship between radio-selected BL Lacs (RBLs and XBLs) and Fanaroff-Riley Type I radio galaxies (FRI) in accordance with the unified scheme. Analysis of the core and extended luminosity show that RBLs are more core dominated than XBLs which are also more core dominated than FRI radio galaxies. Distributions of core dominance parameter (R) give Rm ≈ 42.41 ± 10.77, 5.08 ± 1.57, and 0.34 ± 0.0024 for RBLs, XBLs, and FRI, corresponding to mean viewing angles (ϕm) in the range ϕ ≈ 70 − 170, 130 − 240 and 200 − 280 respectively. Regression analysis of the three samples shows that the core to extended luminosity plot (LC − LE) yields a strong correlation of r ≈ 0.67±0.52, 0.85±0.46, and 0.79±0.61 for FRI, RBLs and XBLs at 95% confidence level. Similarly, regression analysis of R and ϕ for FRI, RBLs, and XBLs all yield a strong anti-correlation of r ≈ −0.98±0.02, −0.64±40.52, and 0.75±4.45. These results are consistent with BL Lac/FRI unification and suggest that relativistic beaming of the core and extended emissions is significant in low luminosity AGNs and thus a strong support for the unified scheme.

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“…Based on the Hubble diagram, Xie et al [7] claimed that FRIs and FRIIs with optical morphology as a galaxy (FRII-G) are the parent population of BL Lac objects while FRIIs with optical morphology as a quasar (FRII-Q) are the parent population of FSRQs, which was confirmed later by some authors: Fan et al [8] by Hubble diagram using the infrared data, Bai & Lee [9] discussed the unification spectrum index α rx , while Wang et al [10] used the unbeamed radio luminosity to do it. Zhou et al [11] discussed the sequence scheme for a large sample of blazers.…”

mentioning

confidence: 99%

An X-ray luminosity analysis for FRIs and FRIIs

Zhang

Fan

2009

Sci. China Ser. G-Phys. Mech. Astron.

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Radio galaxies are divided into two groups according to their luminosities at 178 MHz, namely Fanaroff-Riley type Is (FRIs) and Fanaroff-Riley type IIs (FRIIs) with FRIs showing lower radio luminosities than FRIIs. In this paper, the X-ray data are compiled for 183 radio galaxies (61 FRIs and 122 FRIIs), from the available literature, for the analysis of the X-ray properties. The 1 keV X-ray luminosities are calculated and discussed for the two groups, and an averaged X-ray luminosity of logL X 1 keV = 41.30±2.51 erg·s −1 ·keV −1 is found for FRIs, which is lower than that for FRIIs, logL X 1 KeV = 43.39±3.06 erg·s −1 ·keV −1 .A Kolmogorov-Smirnov (K-S) test indicates that the probability for the X-ray luminosity distributions of the two groups to be from the same parent distribution is 1.44×10 −10 . We also discuss the origin and the mechanism of the X-ray emission for FRIs and FRIIs.active galactic nuclei, radio galaxies, relativistic beaming Radio galaxies are divided into two groups according to their luminosities at 178 MHz, namely Fanaroff-Riley type Is (FRIs) and Fanaroff-Riley type IIs (FRIIs) [1] . FRIs with L 178 MHz ≤2×10 25 W·Hz −1 ·Sr −1 are low luminosity sources associated with their emission centred on the core and decreased gradually along the jets. They are "edge-darkened". FRIIs with L 178 MHz ≥ 2×10 25W·Hz −1 ·Sr −1 are high luminosity sources, and their morphologies are opposite to FRIs', so they are called "edge-brightened" galaxies. That means that their highest brightness comes from the hotspots at the ends of their brightened jets [1] . Depending on the optical properties, FRIIs can be divided into different sub-classes: radio-loud quasars (Qs), narrow line radio galaxies (NLRGs), broad line radio galaxies (BLRGs), and low excitation radio galaxies (LERGs). Recently, there are many fierce debates on the Fanaroff-Riley (FR) galaxies. Zirbel & Baum [2] found that the median value of radio core powers for FRIIs is 4 times greater than that for FRIs, while the median value of total radio core powers for FRIIs is 40 times greater than that for FRIs. The mass of the molecular gas is lower in FRIs than that in FRIIs and there are more FRII galaxies at higher z compared to the FRI galaxies [3] .Active galactic nuclei (AGNs) are the most interesting class in the Universe showing active features. Blazar is a subclass of AGNs showing even extreme observation properties. They have high polarization, strong and rapid variability, weak emission lines or no emission line at all or very strong emission lines, superluminal motions and gamma-ray emissions etc. These particular characters are generally interpreted as a consequence of nonthermal emission from a relativistic jet oriented close to the line of sight [4] . From the unified scheme of AGNs [5,6] , different orientations of the source axis to the observer's line of sight will result in different subclasses of AGNs. It is generally believed that FRIs and FRIIs are the unbeamed parent populations of BL Lac objects and flat spectrum radio quasars (F...

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A Statistical Study of XBLs, RBLs and FSRQs at 1.5 GHz

Cited by 8 publications

References 32 publications

Orientation and Beaming Effects in active galactic nuclei: Implication for radio galaxy - Blazar Evolution

Orientation and Beaming Effects in active galactic nuclei: Implication for radio galaxy - Blazar Evolution

On the Unification of Low Luminosity Active Galactic Nuclei

An X-ray luminosity analysis for FRIs and FRIIs

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