scholarly journals A Comparison of the Centimetre-to-Submillimetre Continuum Spectra of BL Lacertae Objects and Flat Spectrum Radio Quasars

1994 ◽  
Vol 159 ◽  
pp. 523-523
Author(s):  
J.A. Stevens ◽  
S.J. Litchfield ◽  
E.I. Robson ◽  
W. K. Gear ◽  
D.H. Hughes
Keyword(s):  
High Frequency ◽  
Spectral Shape ◽  
Continuum Emission ◽  
Frequency Range ◽  
Frequency Spectra ◽  
Bl Lacertae Objects ◽  
Bl Lacertae ◽  
Spectrum Radio ◽  
Bl Lacs ◽  
The Continuum

A comparison of the centimetre to submillimetre continuum spectra of 22 BL Lacertae objects and 24 flat-spectrum radio quasars (FSRQ) has been conducted in order to search for systematic differences between the two classes. The same overall spectral shape is found for all sources and it is concluded that the same basic physical model applies to the continuum emission over this frequency range in both cases. There is clear evidence, however, for the BL Lacs to have flatter high frequency spectra and this difference is reconciled with an intrinsic difference in the underlying jets of the two classes.

scholarly journals Outflow Angles and Bulk Lorentz Factors for Different Categories of AGN

1997 ◽  
Vol 163 ◽  
pp. 695-696 ◽  
Author(s):  
Erick. J. Guerra ◽  
Ruth A. Daly
Keyword(s):  
Lorentz Factor ◽  
Radio Galaxies ◽  
Line Of Sight ◽  
Radio Sources ◽  
Bl Lacertae Objects ◽  
Bl Lacertae ◽  
High Polarization ◽  
Inverse Compton ◽  
Doppler Factor ◽  
Bl Lacs

AbstractRelativistic outflows from AGN can be parameterized by θ, the angle subtended by the direction of the outflow and the line of sight to the observer, and γ, the bulk Lorentz factor of the outflow. The Doppler factor, δ, and the apparent speed in the plane of the sky, βapp, are combinations of θ and γ. The Doppler factor can be estimated using either the equipartition Doppler factor, δeq (Readhead 1994), or the inverse Compton Doppler factor, δIC. These Doppler factor estimates are combined with observed βapp to solve for θ and γ for different categories of AGN.Ghisellini et al. (1993) compute δIC for 105 compact radio sources, and Güijosa & Daly (1996) compute δeq for the same sample. Daly, Guerra, & Güijosa (1996) estimate θ and γ for the 43 sources that have βapp listed by Vermeulen & Cohen (1994) and δeq computed by Güijosa & Daly (1996).Solutions and errors for θ and γ are presented in Figures 1 and 2 using δeq and δIC respectively. Guerra & Daly (1996) discuss these estimates and errors in greater detail. These AGN fall into the following categories: BL Lacertae objects (BL Lacs), core-dominated high-polarization quasars (CDHPQ), core-dominated low-polarization quasars (CDLPQ), core-dominated quasars with no polarization information (CDQ(NPI)), lobe-dominated quasars (LDQ), and radio galaxies (RG).

scholarly journals CSS versus Large Size Sources

1996 ◽  
Vol 175 ◽  
pp. 63-66 ◽  
Author(s):  
R. Fanti ◽  
R. E. Spencer
Keyword(s):  
Flux Density ◽  
High Power ◽  
High Frequency ◽  
Large Fraction ◽  
Radio Sources ◽  
Frequency Spectra ◽  
Large Size ◽  
Spectrum Radio

A large fraction of the sources in flux density limited radio samples have angular sizes < 2 arcsec (and hence projected linear sizes ≤ 10–15 kpc for H0 = 100 Km/(sec Mpc), and steep (α > 0.5, S∝ v–α) high frequency spectra (Kapahi, 1981; Peacock and Wall 1982). The proportion of these Compact Steep–spectrum Sources (CSSs) is high (15–30% depending on the selection frequency) amongst distant (z > 0.2) radio sources of high power, both galaxies and quasars. We include in this class the GHz Peaked Spectrum Radio Sources (GPS), sub–kpc objects whose radio spectra are peaked at GHz frequencies (see, e.g., O'Dea et al, 1991).

scholarly journals BL Lacertae objects as an evolutionary population

1986 ◽  
Vol 119 ◽  
pp. 491-492
Author(s):  
A. Cavaliere ◽  
E. Giallongo ◽  
F. Vagnetti
Keyword(s):  
Luminosity Function ◽  
Bl Lacertae Objects ◽  
Bl Lac Objects ◽  
Bl Lacertae ◽  
Bl Lac ◽  
Bl Lacs

If the BL Lac Objects are active nuclei with a beamed component that is dominant when directed at us, their observed luminosity function must comprise a flat faint branch: N(L)dL ∝ L1+1/pdL with p=4.5 (Urry and Shafer 1984). If this is flatter than the LF NP(L) of the parent objects at equal observed L, then we expect the counts of BL Lacs to flatten out in turn at fluxes quite higher than the counts of the parents, even when both populations evolve strongly and uniformly with comparable timescales (Cavaliere, Giallongo and Vagnetti 1985).

Shielded open-circuited probe for in-situ measurements of soil permittivity in Very high frequency (VHF) and Ultra high frequency (UHF) bands

2021 ◽  
pp. 014233122110377
Author(s):  
Konstantin Muzalevskiy ◽  
Andrey Karavaysky
Keyword(s):  
Reflection Coefficient ◽  
Root Mean Square Error ◽  
Mean Square Error ◽  
Root Mean Square ◽  
High Frequency ◽  
Mean Square ◽  
Frequency Range ◽  
Frequency Spectra ◽  
Determination Coefficient ◽  
Error Determination

In this paper, the shielded open-circuited probe operating in the wide frequency range from 75MHz to 2GHz is proposed. The probe is made of an SubMiniature version A (SMA) flange connector. The central rod of the SMA connector emerges from a coaxial transition in the flange and shielded by four rods. The robe design allows us to calculate of the probe reflection coefficient S11 used simple analytical transmission line model (TEM wave mode), the parameters of which were calibrated on a set of substances with a known frequency spectrum of permittivity. The refractive index (RI) and normalized attenuation coefficient (NAC) retrieval technique is based on solving the inverse problem of minimizing the residual norm between measured and calculated frequency spectra of reflection coefficient S11. After calibration, the root-mean-square error (determination coefficient) between the measured and calculated module and phase of the reflection coefficient S11 for the sets of calibration media air, distilled water, butanol, pure ice, water solution with NaCl of salinity of 8.9% do not exceed 0.26dB (0.995) and 0.03 rad (0.999), respectively, in the frequency range from 75MHz to 2GHz. The root-mean-square error (determination coefficient) between the measured RI and NAC spectra for four soil cover samples (variation of the clay fraction from 10.5 g/g to 47.6 g/g) using the proposed probe and a precision coaxial cell not exceeds 0.109 (0.993) and 0.057 (0.986), respectively, in the frequency range from 75 MHz to 2 GHz. As a result, it is experimentally shown that RI и NAC can be measured by the proposed non-precision probe with an error comparable to the precision coaxial cell.

scholarly journals The De-beamed γ-Ray Emissions in Blazars

2013 ◽  
Vol 9 (S304) ◽  
pp. 159-160 ◽  
Author(s):  
J. H. Fan ◽  
Z. Y. Ji
Keyword(s):  
Flux Density ◽  
Strong Correlations ◽  
Bl Lacertae Objects ◽  
Present Sample ◽  
Bl Lacertae ◽  
Spectrum Radio ◽  
Γ Ray

AbstractBlazars (BL Lacertae objects and flat spectrum radio quasars) are strong γ-ray emitters, the γ-ray emissions are strongly beamed. In this work, we compiled a sample of Fermi blazars with available beaming factors, δR, to investigate the correlation between the γ-ray flux density, logfγ, and redshift, logz for the whole sample and the subclasses of the present sample. The analysis shows that there is no correlation between logfγ and logz for the observed γ-ray flux density, but there are strong correlations between the de-beamed flux densities, logfγdb and logz for the whole sample and the subclasses. Our results confirm that the γ-ray emissions are strongly beamed and imply that it is possible for one to use the radio beaming factor, δR for the beaming effect discussions in the γ-ray bands for Fermi blazars.

Correlation between Eddington Ratios and Broad-Line Luminosities in Flat-Spectrum Radio Quasars, BL Lacertae Objects, and Radio Galaxies

2007 ◽  
Vol 133 (5) ◽  
pp. 2187-2191 ◽  
Author(s):  
H. Dai ◽  
G. Z. Xie ◽  
S. B. Zhou ◽  
H. Z. Li ◽  
L. E. Chen ◽  
...  
Keyword(s):  
Radio Galaxies ◽  
Broad Line ◽  
Bl Lacertae Objects ◽  
Bl Lacertae ◽  
Spectrum Radio

scholarly journals Optical Variability of a Newly Discovered Blazar Sample from the BZCAT Catalog

2021 ◽  
Vol 257 (2) ◽  
pp. 41
Author(s):  
Nibedita Kalita ◽  
Alok C. Gupta ◽  
Minfeng Gu
Keyword(s):  
Monitoring Program ◽  
Optical Monitoring ◽  
Spectral Slope ◽  
Spectral Evolution ◽  
Flux Variation ◽  
Significance Level ◽  
Bl Lacertae ◽  
Spectrum Radio ◽  
Bl Lacs ◽  
Radio Quasar

Abstract In an optical monitoring program to characterize the variability properties of blazars, we observed 10 sources from the Roma-BZCAT catalog for 26 nights in V and R bands during 2014 October to 2015 June with two telescopes located in India. The sample includes mainly newly discovered BL Lacertae objects (BL Lacs) for which the redshift of some sources is not yet known. We present the results of flux and color variations of the sample on intraday and short timescales obtained by using the power-enhanced F-test and the nested-ANOVA tests, along with their spectral behavior. We find significant intraday variability in the single flat-spectrum radio quasar in our sample, having an amplitude of variation ∼12%. Although a few of the BL Lacs showed probable variation in some nights, none of them passed the variability tests at 99.9% significance level. We find that 78% of the sample showed significant negative color–magnitude correlations, i.e., a redder-when-brighter spectral evolution. Those that do not show strong or clear chromatism predominantly exhibit a redder-when-brighter trend. Unlike on hourly timescales, the high-synchrotron-peaked blazars in the sample (BZGJ0656+4237, BZGJ0152+0147, and BZBJ1728+5013) show strong flux variation on timescales of days to months, where again we detect a decreasing trend of the spectral slope with brightness. We observe a global steepening of the optical spectrum with increasing flux on the intranight timescale for the entire blazar sample. The nonvariability in the BL Lacs in our sample might be caused by the distinct contribution from the disk as well as from other components in the studied energy range.

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