---
abstract: 'We present results of single-epoch very long baseline interferometry (VLBI) observations of gamma-ray bright active galactic nuclei (AGNs) using the Korean VLBI Network (KVN) at 22, 43, 86, and 129 GHz bands, which are part of a KVN key science program, Interferometric Monitoring of Gamma-ray Bright AGNs (iMOGABA).  We selected a total of 34 radio-loud AGNs of which 30 sources are gamma-ray bright AGNs with flux densities of $>6\times10^{-10}$ ph cm$^{-2}$ s$^{-1}$. Single-epoch multi-frequency VLBI observations of the target sources were conducted during a 24-hr session on 2013 November 19 and 20.  All observed sources were detected and imaged at all frequency bands with or without a frequency phase transfer technique which enabled the imaging of 12 faint sources at 129 GHz, except for one source.  Many of the target sources are resolved on milliarcsecond scales, yielding a core-jet structure with the VLBI core dominating the synchrotron emission on the milliarcsecond scale.  CLEAN flux densities of the target sources are 0.43-28 Jy, 0.32-21 Jy, 0.18-11 Jy, and 0.35-8.0 Jy in the 22, 43, 86, and 129 GHz bands, respectively.  Spectra of the target sources become steeper at higher frequency with the mean of the spectral indices of -0.40, -0.62, and -1.00 in the 22-43 GHz, 43-86 GHz and 86-129 GHz bands, respectively, implying that the target sources become optically thin at higher frequency (e.g., 86-129GHz).' 
author:
- 'Sang-Sung Lee, Kiyoaki Wajima, Juan-Carlos Algaba, Guang-Yao Zhao, Jeffrey A. Hodgson, Dae-Won Kim, Jongho Park, Jae-Young Kim, Atsushi Miyazaki, Do-Young Byun, Sincheol Kang, Jeong-Sook Kim, Soon-Wook Kim, Motoki Kino, and Sascha Trippe'
title: 'Interferometric Monitoring of Gamma-ray Bright AGNs I: Results of Single-epoch Multifrequency Observations'
---

Introduction
============

Active galactic nuclei (AGNs) are the most powerful and violent celestial objects in the Universe.  AGNs emit a wide range of electromagnetic radiation in the radio to gamma-ray range, producing huge luminosity ($\sim10^{42}-10^{48}$ erg s$^{-1}$) in very compact emitting regions on sub-pc scales; their emission is often highly variable and polarized [see e.g., @kro99].  The AGNs are believed to have supermassive black holes (SMBH) in the centers, accretion disks around the SMBHs, and relativistic jets launched perpendicular to the accretion disk plane into interstellar space.  Relativistic jets of the radio-loud AGNs often show variability in brightness (e.g., in radio, optical, etc.)  on timescales of hours to years, and morphological changes on milliarcsecond (mas) scale [see e.g., @boe+12 for review].  Very rapid and strong variabilities (or flares) in the gamma-ray range from radio-loud AGNs have been observed during intensive gamma-ray monitoring of AGNs by several gamma-ray space telescopes: INTEGRAL [^1], AGILE [^2], FERMI [^3], etc.  The gamma-ray flares were detected from more than 100 AGNs including 3C 273, 4C +21.35, 4C 454.3 and 1510-089, by the Fermi Gamma-ray Space Telescope (GST) [see @kan+15 for references].  To understand the gamma-ray flares in the AGNs, multiwavelength monitoring studies have been conducted to investigate the correlation between emission at gamma-ray and other wavelengths [e.g., @mar+08; @abd+10].  The gamma-ray flares are correlated with the variability in brightness, polarization, and morphology of the jets at low energy regimes (e.g., radio, optical, etc.).  The correlation of the gamma-ray flares with multiwavelength variability, in principle, implies co-spatiality of the gamma-ray flaring regions and the emission regions at other wavelengths. 

[@mar+08] suggested that the gamma-ray flares from BL Lac may be generated through inverse Compton scattering in the innermost region of the jets threaded by a helical magnetic field or in a bright very long baseline interferometry (VLBI) core region corresponding to a standing shock wave, through compression by the shock front. [ @abd+10] reported that the gamma-ray flares correlated with the change of optical polarization angle of 3C 279 provide evidence for the co-spatiality of the gamma-ray and optical emission regions with a highly ordered jet magnetic field in a curved trajectory within the jet.  The different understandings of the cause and location of the gamma-ray flares imply that either the gamma-ray flares are generated under various situations or our understanding of the gamma-ray flares may still be uncertain. 

Gamma-ray flares leading a delayed outburst at radio frequencies [e.g., @jor+01] motivated the conducting of many single-dish and VLBI observations (or monitoring programs) at centimeter (cm) and millimeter (mm) wavelengths [@sav+02; @LV03; @lis+09; @ojh+09; @mar+11; @ang+12; @nag+13].  Those VLBI monitoring programs are conducted only at a single frequency of $\le$43 GHz, except for the TANAMI [@ojh+09] at 8.4 and 22 GHz, implying that those programs are not able to determine frequency-dependent properties of the gamma-ray flaring AGNs on mas-scales, including such properties as spectral index variation, time-dependent multiwavelength light curves of mas-scale structures, etc.,  which may be very important to investigate the correlation of the gamma-ray flares with both the optically thin and thick emissions of the jets. 

The Korean VLBI Network (KVN) has enabled us to regularly obtain mas-scale images of gamma-ray bright AGNs at cm-to-mm wavelengths, leading to a key science program (KSP) of the KVN, the Interferometric Monitoring of Gamma-ray Bright AGNs (iMOGABA), which is a VLBI monitoring program for about 30 gamma-ray bright AGNs using the KVN at multifrequency bands (22-129 GHz).  The iMOGABA initially started in 2012 December by conducting monthly one 24-hr VLBI observation in the 22, 43, 86, and 129 GHz bands.  The iMOGABA has been selected as a KVN KSP since 2015 March, aiming at studying the origins of the gamma-ray flares of the AGNs.  We selected a total of 34 radio-loud AGNs, as summarized in Table \[t1\], of which 30 sources are gamma-ray bright AGNs with their flux densities of $>6\times10^{-10}$ ph cm$^{-2}$ s$^{-1}$, including 24 sources monitored by the Fermi Gamma-ray Space Telescope using the Large Area Telescope on board.  The selected sources consist of 24 quasars, 7 BL Lacs, and 3 radio galaxies. 

In this paper, the first representative paper from the iMOGABA program, we report the results of a single-epoch VLBI observations of the iMOGABA.  In Section \[obs\_analysis\], the observations and data analysis of the single-epoch VLBI session used in this paper is described.  Then, we present the results of the single-epoch observations in Section \[results\]; in Section \[dis\], we present our discussion.  Finally, in Section \[sum\], we summarize what we have found. 

Observations and data analysis\[obs\_analysis\]
===============================================

Observations\[obs\]
-------------------

We observed a total of 34 radio-loud AGNs in the 22 GHz, 43 GHz, 86 GHz, and 129 GHz bands on 2013 November 19 UT 02:00 - November 20 UT 01:53, using the KVN which consists of three identical 21-m radio telescopes [@lee+11]: KVN Yonsei (KY), KVN Ulsan (KU), and KVN Tamna (KT), with baseline lengths of 305–476 km [@lee+14], and a simultaneous multifrequency observing system [@han+08; @han+13].  All sources were observed with 1-8 scans of 5 min in length.  The observing frequencies were 21.700–21.764 GHz, 43.400–43.464 GHz, 86.800–86.864 GHz, and 129.300–129.364 GHz, and in left circular polarization (LCP).  The ratio of the starting frequencies is an integer so that the frequency phase technique can be applied to faint sources [@alg+15].  The total bandwidth is 256 MHz and is divided evenly for each frequency band.  In order to measure changes in the opacity of the atmosphere during the observations, we conducted sky tipping curve measurements every hour, i.e., we measured the system temperatures at 8 elevations: 18.21$^\circ$, 20.17$^\circ$, 22.62$^\circ$, 25.77$^\circ$, 30.00$^\circ$, 36.03$^\circ$, 45.58$^\circ$, and 65.38$^\circ$, during the observations.  Cross-scan observations for target sources were conducted every scan to correct antenna pointing offsets, which are the main source of amplitude uncertainty in KVN observations.  The received signals were digitized (i.e. 2-bit quantized) by digital samplers in the antenna cabin and transmitted through optical fibers to the observing building.  The transferred digital signals were requantized and divided into 16 sub-bands (IFs) of 16 MHz wide by a digital filter bank, and recorded by the Mark 5B system at a recording rate of 1024 Mbps.  Correlation of the data was performed with the DiFX software correlator in the Korea-Japan Correlator Center [@lee+15a]. 

Data analysis\[da\]
-------------------

The DiFX correlator produced the spectrum of the cross-correlation function with resolution of 0.125 MHz and accumulation period of 1 s. Post-correlation processing was done using the NRAO Astronomical Image Processing System (AIPS).  A standard AIPS procedure was applied.  An antenna-based fringe fitting was conducted using AIPS task FRING.  KVN Ulsan (KU) was selected as the reference antenna.  The 5 min long scans were split into solution intervals that were 30 s long.  Baseline-based fringe solutions (phase delays and delay rates) were searched for individual IF at all frequency bands.  The baseline-based fringe solutions were used to determine the antenna-based fringe solutions. 

All sources were detected at lower frequencies (e.g., 22-86 GHz) with this standard post-correlation processing.  However, about a dozen of the observed sources were not detected in the 129 GHz band.  In order to detect the non-detected sources, the FPT technique was applied, using an automatic VLBI data reduction pipeline developed for the KVN observations.  The operation of the KVN Pipeline was described in detail by [@hod+16].  Thanks to the FPT technique, i.e., by transferring phase solutions from lower frequencies to higher as described by [@rio+11] and [@rio+14], sensitivity at high frequency was improved, and all of the non-detected sources were detected in the 129 GHz band. 

Amplitude calibrations were performed based on system temperatures measured during observations at each station and on elevation dependence of the antenna gains provided.  The system temperatures were corrected for the atmospheric opacity estimated from the sky tipping curve measurements conducted every hour.  We expect that thanks to the good quality of the system temperatures, antenna gains, and atmospheric opacity for KVN stations, the uncertainty of the amplitude calibration is witin 10-30% at 22-129 GHz bands.  Re-normalization of the fringe amplitudes was made to correct for the amplitude distortion due to quantization, and the quantization and re-quantization losses were corrected [@lee+15b]. 

Imaging with calibrated data\[imaging\]
---------------------------------------

The phase- and amplitude-calibrated data were used to produce CLEAN contour maps of the sources via the Caltech DIFMAP software [@she+94].  The calibrated data were averaged in frequency, and the data at band edges were chopped to avoid flux loss due to bandpass shape.  The [*uv*]{}-data were also averaged in time over 30 seconds in the 22, 43, and 86 GHz bands, and over 10 seconds in the 129 GHz band, taking into account coherence time at each frequency bands, and expecting a decoherence loss of upto 30% at 86-129GHz bands.  Some outliers in the $uv$-data were flagged by investigating the visibility amplitude. 

The averaged and edited [*uv*]{}-data were then fitted using a single circular two-dimensional Gaussian model, and the visibility phase was self-calibrated with the model.  After removing the single Gaussian model, a combination of CLEAN point source models was applied.  The visibility phase was again self-calibrated with the CLEAN model to produce the final CLEAN contour maps of the detected sources, when available.  The visibility amplitude was not modified. 

The residual noise in the final CLEAN map was investigated to evaluate the quality of the image, taking into account the assumption that the residual noise of the properly CLEAN image is random noise, and hence the amplitude of each pixel in the residual map should have a Gaussian distribution.  So, the noise in the final image can be expressed quantitatively by the ratio of image noise rms to its mathematical expectation, $\xi_{\rm r} = s_{\rm r} / s_{\rm {r,exp}}$, where $|s_{\rm r}|$ is the maximum absolute flux density in the residual image and $|s_{\rm r,exp}|$ is the expectation of $s_{\rm r}$. For Gaussian noise with a zero mean, the expectation of $s_{\rm r}$ is $|s_{\rm {r,exp}}| = \sigma_{\rm r} { \left[ \sqrt{2} \ln{\left( \frac{N_{\rm pix}} {\sqrt{2\pi}\sigma_{\rm r}} \right) }\right]}^{1/2}$, where $N_{\rm pix}$ is the total number of pixels in the image, and $\sigma_{\rm r}$ is the image noise rms.  If $ \xi_{\rm r} \rightarrow 1 $, the residual noise approaches Gaussian noise; if $ \xi_{\rm r} > 1 $, not all the structure has been adequately recovered; if $ \xi_{\rm r} < 1 $, the image model has an excessively large number of degrees of freedom [@lob+06].  The values of $\xi_{\rm r} $ of the images obtained in this paper are 0.42-0.74 at 22 GHz, 0.41-0.77 at 43 GHz, 0.43-0.75 at 86 GHz, and 0.43-0.81 at 129 GHz, as shown in Figure \[fig-hist-q\] and summarized in Table \[t2\], implying that the images adequately represent the structure detected in the visibility data. 

Model fitting and estimating parameters\[modelfit\]
---------------------------------------------------

Circular two-dimensional Gaussian models were used to fit the final CLEAN images, yielding the general fit parameters: [*$S_{\rm tot}$*]{} (total flux density), [*$S_{\rm peak}$*]{} (peak flux density), [*$\sigma_{\rm rms}$*]{} (post-fit rms), $d$ (size), $r$ (radial distance, for jet components), $\theta$ (position angle, measured for jet components, with respect to the location of the core component), as summarized in Table \[t3\].  The uncertainties of the fit parameters were estimated, based on the signal-to-noise ratio of each component detection, by adopting an analytical first order approximation given by [@fom99]: $\sigma_{\rm peak} = \sigma_{\rm rms}{\left({1+\frac{S_{\rm peak}}{\sigma_{\rm rms}}}\right)}^{1/2}$, $\sigma_{\rm tot} = \sigma_{\rm peak}{\left({1+\frac{S_{\rm tot}^2}{S_{\rm peak}^2}}\right)}^{1/2}$, $\sigma_{d} = d\frac{\sigma_{\rm peak}}{S_{\rm peak}}$, $\sigma_{r} = \frac{1}{2}\sigma_{d}$, and $\sigma_{\theta} ={\rm atan}\left(\frac{\sigma_{r}}{r}\right)$, where $\sigma_{\rm peak}$, $\sigma_{\rm tot}$, $\sigma_{\rm rms}$, $\sigma_{d}$, $\sigma_{r}$, and $\sigma_{\theta}$ are the uncertainties of peak flux density, total flux density, post-fit rms, size, radial distance, and position angle of a component, respectively.  A component was considered to be unresolved when the fitted component size $d$ is smaller than its minimum resolvable size [@lob05] as given by $d_{\rm min}=\frac{2^{1+\beta/2}}{\pi}{\left[{\pi ab\ln2\ln{\frac{\rm S/N}{{\rm S/N}-1}}}\right]}^{1/2}$, where [*a*]{} and [*b*]{} are the axes of the restoring beam, S/N is the signal-to-noise ratio, and $\beta$ is the weighting function, which is 0 for natural weighting or 2 for uniform weighting.  If $d<d_{\rm min}$, the uncertainties were estimated according to $d=d_{\rm min}$.

The total flux density and measured size of a Gaussian component leads to a simple estimation of the rest frame brightness temperature $T_{\rm b}$ of the given emission region represented by the Gaussian model as $T_{\rm b} = \frac{2\ln{2}}{{\pi}{k}}\frac{S_{\rm tot}\lambda^2}{d^2}(1+z)$, where $\lambda$ is the wavelength of observation, $z$ is the redshift, and $k$ is the Boltzmann constant.  If $d < d_{\rm min}$, then the lower limit of $T_{\rm b}$ is obtained using $d=d_{\rm min}$.

Results\[results\]
==================

Out of 34 sources, 32 sources were detected and imaged at all frequency bands with or without a frequency phase transfer technique that enabled us to detect and image 13 faint sources at 129 GHz, except for 0218+357 which was detected for only one baseline at all frequency bands.  The first 129 GHz VLBI images were made for most of the sources in this project. 

In Figure \[fig-image\], CLEAN contour maps for each source are presented for the 22, 43, 86, and 129 GHz bands, when available.  A set of plots for each source at each frequency consists of a contour map in the left panel, a plot of the corresponding visibility amplitude against [*uv*]{}-radius in the top right panel, and a plot of the corresponding [*uv*]{}-sampling distribution in the bottom right panel.  The contour map is shown with the X- and Y-axes in units of mas.  The source name and the observing frequency are given at the top of the map.  The FWHM of the restoring beam is drawn as a shaded ellipse on the map.  The peak flux density and rms noise level are identified in the lower right corner of the map.  The contours are drawn with a logarithmic spacing at -1, 1, 1.4,...,$1.4^n$ of the lowest flux density level which corresponds to three times the rms noise level.  Most contour maps are centered on their brightest emission region (which is considered to be a VLBI core with fainter emission regions being the corresponding jet component, except for 3C 84 and 4C+39.25), but for some maps with extended source structure, the map center is shifted to fit the map in the box.  The plot of the visibility amplitude, at the top right of each set, is drawn as a function of the [*uv*]{}-radius, i.e., the length of the baseline used to obtain the corresponding visibility point in units of $10^6\lambda$, where $\lambda$ is the observing wavelength.  The visibility amplitude (i.e., the correlated flux density) is shown in units of Jy.  The [*uv*]{}-sampling distribution, at the bottom right of each set, shows the distribution of the visibility in the [*uv*]{}-plane, whose range corresponds to that of the [*uv*]{}-radius.  For the 12 sources (0235+164, 0528+134, 0735+178, 0827+243, 0836+710, 1127-145, 1156+295, 1222+216, 1343+451, 1611+343, and 3C 286) the FPTed images, i.e., the images obtained by the FPT technique, are presented for the 129 GHz band.  In particular, the 43 and 86 GHz images for 3C 286 are also FPTed. 

The KVN observations for this paper were done without the phase-referencing technique, i.e., without relative (or absolute) astrometric information of core or jet components with respect to calibrators.  So, we considered a brightest emission region to be a VLBI core in each image and the others the jet, following a general strategy for identifying VLBI cores.  However, we found that for some cases, maybe rare but well-known, the brightest component may not be the core.  For example, 3C 84 (0316+413), the J3 component is brighter than the core (C) at 43 and 86 GHz.  At 43 GHz, in particular, the J3 component was centered and the core was located in the northern area in the beginning of the imaging process due to its brightness.  Considering the spectral index of the core (C) to be flat, we identified the northern component as a core, and shifted the map to south.  Another exceptional source is 4C $+$39.25 (0923+392).  The eastern component (J1) is brighter than the western component (C) and was located in the map center in the imaging process.  Since, however, the fainter component is usually identified as the core [e.g., @nii+14], we considered the fainter component as the core and shifted the map to have the core in the center. 

Parameters of the contour maps presented in Figure \[fig-image\] are summarized in Table \[t2\].  For each image, Table \[t2\] lists the source name, the observing frequency band, the parameters of the restoring beam (the size of the major axis $B_{\rm maj}$, the minor axis $B_{\rm min}$, and the position angle of the beam $B_{\rm PA}$), the total flux $S_{\rm KVN}$, the peak flux density $S_{\rm p}$, the off-source RMS $\sigma$, the dynamic range of the image $D$, and the quality $\xi_{\rm r}$ of the residual noise in the image. 

The parameters of each model-fit component are listed in Table \[t3\]: the total flux $S_{\rm tot}$, peak flux density $S_{\rm peak}$, size $d$, radius, $r$ (only for jet components), position angle $\theta$ (only for jet components), and measured brightness temperature $T_{\rm b}$. In cases of multiple components (i.e., VLBI core and jet components) fitted, the parameters of the core component are followed by those of the jet components.  The estimated uncertainties are given as in Section \[modelfit\].  The upper limits of size $d$, and the lower limits of brightness temperature $T_{\rm b}$ are in italics with flag symbols. 

Discussion\[dis\]
=================

Source morphology on mas scales
-------------------------------

Many of the target sources are resolved on mas scales, yielding a core-jet structure.  Out of 33 sources imaged, 22 sources show a core-jet structure at at least one of the observing frequency bands.  Most of the sources with core-jet structure are imaged to show a single jet component, except for 0316+413 (3C 84), 1226+023 (3C 273B), 1611+343, 1641+399 (3C 345), 2230+114 (CTA102), and 2251+158 (3C 454.3), which show more than one jet component at at least one frequency band on the scales of 1-11 mas, contributing to the CLEAN flux density of the sources by $<$50%, as summarized in Table \[t3\].  Although many of the target sources are resolved, they are highly core-dominated in flux, i.e., the VLBI core flux density ($S_{\rm c}$) dominates the synchrotron emission on the mas-scales ($S_{\rm KVN}$), as shown in Figure \[fig-hist-ratio\].  Some of the very compact sources show a ratio of $S_{\rm c}/S_{\rm KVN}$ larger than unity due to uncertainty of the CLEAN flux and of the model fitting. 

The distributions of angular size for the core components of the imaged sources were investigated.  As introduced in Section \[modelfit\], a core component was considered to be unresolved when the fitted core size was smaller than its minimum resolvable size, yielding the upper limit of the angular size.  The numbers of unresolved cores are 14 (22 GHz), 3 (43 GHz), 4 (86 GHz), and 5 (129 GHz) out of 33 imaged sources.  Excluding the upper limits, the mean (and median) values of the measured core angular sizes are 1.135 mas (0.912 mas), 0.586 mas (0.591 mas), 0.411 mas (0.438 mas), and 0.232 mas (0.179 mas) in the 22, 43, 86, and 129 GHz bands, respectively, implying that the resolved core sizes become smaller at higher frequencies. 

Brightness temperature {#tb}
----------------------

Figure \[fig-hist-tb\] shows the brightness temperatures of the VLBI cores, including the lower limits (in grey), which were obtained for the unresolved cores (see Section \[modelfit\]).  Excluding the limits, the measured brightness temperatures are in the ranges of $2.1\times10^{7}$ K - $7.5\times10^{8}$ K, $2.1\times10^{7}$ K - $3.8\times10^{10}$ K, $1.4\times10^{8}$ K - $3.2\times10^{10}$ K, and $7.7\times10^{8}$ K - $1.2\times10^{11}$ K, at 22, 43, 86, and 129 GHz, respectively.  The mean values of the measured brightness temperature are $1.7\times10^{9}$ K, $4.2\times10^{9}$ K, $6.0\times10^{9}$ K, and $1.7\times10^{10}$ K in the 22, 43, 86, and 129 GHz bands, respectively, implying that the brightness temperatures of the sources become higher at higher frequency. 

These results are different from those reported by [@lee13], [@lee14], and [@lee+16]: the brightness temperatures of the VLBI cores imaged at 86 GHz with the Global Millimeter VLBI Array (GMVA) are lower than those obtained at 2-15 GHz with the global VLBI array.  The mean values of the brightness temperatures for the VLBI cores in [@lee+16] are $8.9\times10^{11}$ K and $1.3\times10^{11}$ K at 15 and 86 GHz, respectively; these values are higher than those we obtained in this work, by factors of about 50 and 20, respectively, although the source samples and their sizes are different from each other.  This difference may be due to the spatial resolution difference between the global VLBI arrays, which have a maximum baseline of about 10000 km, and the KVN, with its maximum baseline of about 500 km.  However, the lower brightness temperatures at lower frequencies (e.g., 22 GHz) obtained with the KVN cannot be fully explained by the resolution difference.  One explanation may be that the sources resolved at 22 GHz with the KVN are largely different from those resolved with the global array, since half of the cores in our sample were unresolved.  Another explanation may be that the brightness temperature measurements at lower frequencies are affected partly by an instrumental beam blending effect: the core region may be diluted by jet emission [see e.g., @lee+16 and references therein].  The core blending effect would make larger both the observed core flux density and the size.  In this case of the 22 GHz observations with the KVN, the increasing factor of the observed core size $d$ is much larger than that of the observed core flux density $S_{\rm tot}$, and hence the brightness temperature ($\propto S_{\rm tot}/d^2$) becomes lower than its true value. 

Source spectra
--------------

The 129 GHz images presented in this paper are the first results for most of the radio loud AGNs in our sample.  Moreover, the simultaneous multifrequency images obtained at four frequency bands (22-129 GHz) are also the first results for the radio-loud AGNs, enabling us to investigate mas-scale spectral information for the radio loud AGNs free from any variability of source.  Here we discuss the spectral properties of the target sources, taking into account the CLEAN flux densities obtained on mas-scales. 

The CLEAN flux densities $S_{\rm KVN}$ of the target sources obtained with the KVN are in the ranges of 0.43-28 Jy, 0.32-21 Jy, 0.18-11 Jy, and 0.35-8.0 Jy in the 22, 43, 86, and 129 GHz bands, respectively, as shown in Figure \[fig-hist-CLEAN\].  The distributions of the CLEAN flux density peak at around 2 Jy (22 and 43 GHz bands) and 1 Jy (86 and 129 GHz bands); these values show that most of the sources are brighter than 0.1 Jy at all frequencies.  The mean values of the CLEAN flux density are 4.7 Jy (21.7 GHz), 3.8 Jy (43.4 GHz), 2.5 Jy (86.8 GHz), and 1.6 Jy (129.3 GHz), implying that the sources become fainter at higher frequency on mas-scales. 

To investigate the spectral properties of the target sources, three models were used to fit it to the CLEAN flux density data: the power law, the broken power law, and the curved power law, as given by $$\label{eqn:plaw}
S=a \nu^{\alpha},$$ where $S$ is the CLEAN flux density in Jansky, $\nu$ is the observing frequency in GHz, $a$ is constant in Jansky, and $\alpha$ is the spectral index for the power law, $$\label{eqn:blaw}
S=b \left\{\left(\frac{\nu}{\nu_{\rm c}}\right)^{-\alpha_{\rm L}n}+\left(\frac{\nu}{\nu_{\rm c}}\right)^{-\alpha_{\rm H}n}\right\}^{-1/n},$$ where $b$ is constant in Jansky, $\nu_{\rm c}$ is a break frequency of the broken power law, $\alpha_{\rm L}$ and $\alpha_{\rm H}$ are the spectral indices at lower and higher frequencies than the break frequency, and $n$ is a numerical factor governing the sharpness of the break, here fixed to be 100 in order to make the break very sharp; and, $$\label{eqn:claw}
S=c_1 \left(\frac{\nu}{\nu_{\rm r}}\right)^{\alpha +c_2 {\rm ln}(\nu/\nu_{\rm r})},$$ where $c_1$ (in Jansky) and $c_2$ are constant, $\nu_{\rm r}$ is a reference frequency, and $\alpha$ is the spectral index at $\nu_{\rm r}$. As a first step, we attempt to fit the power law to the data.  When the power law does not fit to the data, we use the curved power law.  For 7 sources, the power law and curved power law do not fit well to the data and, hence, a broken power law is used to fit to the data for those sources.  The CLEAN flux spectra of the 32 sources (except for 3C 286) are shown in Figure \[fig-spind\] with their best fitting model and the best fitting parameters: the spectral index $\alpha$ for the power law, the cut-off (turnover) frequency $\nu_{\rm c}$, the spectral indices at lower ($\alpha_{\rm L}$) and higher ($\alpha_{\rm H}$) frequencies than the break frequency, obtained from the broken power law, the cut-off (turnover) frequency $\nu_{\rm c}$, the peak flux density $S_{\rm m}$, and the spectral indices between 22-43 GHz (KQ), 43-86 GHz (QW), and 86-129 GHz (WD), obtained from the curved power law.  Out of 32 sources, only 5 sources show the spectra well fitted with the power law; 27 sources have spectra with either a break or a curvature.  For the 32 spectra shown in Figure \[fig-spind\], we used the best fitting model to obtain spectral indices in the KQ-band, QW-band, and WD-band.  Figure \[fig-hist-spind\] shows the distributions of the spectral indices, with mean (median) values of -0.40 (-0.42), -0.62 (-0.66), and -1.00 (-0.99) in the KQ, QW, and WD bands, respectively, indicating that many sources become optically thin at higher frequency (e.g., in the 86 and 129 GHz bands). 

VLBI core size and jet geometry
-------------------------------

In the VLBI observations, the location of the $\tau=1$ surface of the AGN thick core depends on the frequency according to the relation $r\propto\nu^{-1/k_r}$, leading to the well-known ‘core-shift’ effect [see, e.g. @lob98; @hir05; @OG09; @alg+12].  This implies that, at various observing frequencies, the VLBI core actually probes different distances from the SMBH.  At the same time, if we consider the VLBI core as the innermost upstream regions of the unresolved jet, this suggests that measuring the core size at different frequencies can help us to investigate the innermost jet size at different locations, via the core-shift and, hence, the jet’s geometry.  This approach has already been successfully applied in, for example, [@had+11] and [@alg+16].  However, the former considered only one source, and the latter considered observations spanning over several years.  The iMOGABA does not have any of these drawbacks and can consider a whole sample of simultaneous multi-frequency observations. 

In Figure \[fig-geometry\] we show a representative subset of sources to which this method has been applied.  Here we plot the core radius (1/2 of the size) against the inverse of the frequency, which is proportional to the distance from the SMBH.  We performed an exponential fit following $(size)\propto(distance^{\epsilon})$ to find the inferred jet geometry ($\epsilon=1$ conical; $\epsilon=1/2$ parabolic; c.f. [ @ghi+85]).  In general, we can distinguish three different trends: i) all points seem to be reasonably well aligned and fit to a jet size increasing with distance (left column), ii) a certain convex trend is found for the data (middle column) or iii) other peculiar patterns are found (right column).  In the following we briefly discuss these cases. 

There are several cases in which the data are well fitted by an exponential function, in agreement with the discussion above.  The largest group, however, shows an increase of the core size, which does not follow the expected exponential trend, but rather seems to show a size saturation threshold at lower frequencies.  One possibility is that, due to the large scatter and limited data in the [*uv*]{}-plane, a small offset in the amplitude in one scan may cause the fitted Gaussian size to be slightly different, especially in the case of compact sources, which are common in the iMOGABA sample. 

In some cases, the fit indicates a jet with a size that roughly constant or decreasing with size; the jet may even show a possibly oscillatory pattern.  Whilst this phenomenology could be true for a reduced number of sources in very specific conditions for a given time, we believe that this is not the case here.  Instead, we suggest that this behavior is rather due to other effects such as jet blending, the existence of various unresolved components, or extremely large viewing angles.  As for the case mentioned above, the lack of a significant amount of data in the [*uv*]{}-plane may also contribute to a certain extent to the misidentification of some core sizes; thus, care should be taken.  Averaging of the data through various epochs may partially solve this issue.  This will be discussed in a forthcoming paper.  Further discussion can also be found in [@alg+16]. 

Summary\[sum\]
==============

An interferometric monitoring program for gamma-ray bright AGNs was launched and, by conducting monthly multifrequency VLBI observations of a total of 34 radio loud AGNs, continues to aim at revealing the origins of gamma-ray flares often detected in AGNs.  One of the observing sessions in the program was conducted in 2013 on November 19 and 20, yielding 32 sources detected and imaged at all frequency bands with or without use of frequency phase transfer technique.  The first 129 GHz VLBI images were made from most of the sources, establishing a 129 GHz VLBI image database with a size of 32 sources.  In addition to the CLEAN images, we used two-dimensional circular Gaussian models to fit the CLEAN images and obtained the VLBI core sizes and brightness temperatures. 

We find that the 22 sources show the core-jet structure at at least one of the observing frequency bands.  Most of the sources with the core-jet structure are imaged to show a single jet component, except for six sources with multiple jet components on the scales of 1-11 mas, contributing to the CLEAN flux density of the sources by $<$50%.  Although many of the target sources are resolved, they are highly core-dominated in flux.  We also find that the resolved core sizes become smaller at higher frequencies, with the mean values of the measured core angular sizes of 1.135 mas, 0.586 mas, 0.411 mas, and 0.232 mas in the 22, 43, 86, and 129 GHz bands, respectively. 

The mean values of the measured brightness temperature are $1.7\times10^{9}$ K, $4.2\times10^{9}$ K, $6.0\times10^{9}$ K, and $1.7\times10^{10}$ K in the 22, 43, 86, and 129 GHz bands, respectively, implying that the brightness temperatures of the sources become higher at higher frequency.  We find that these brightness temperatures are lower than those obtained with global VLBI arrays, indicating that the brightness temperature measurements are affected by the low spatial resolution of the KVN observations and by the instrumental beam blending effect, especially in the 22 GHz band. 

Thanks to the simultaneous multifrequency VLBI observations, we are able to investigate the spectral properties free from any source variability.  We find that the sources become fainter at higher frequency, yielding optically thin spectra at mm wavelengths.  More sophisticated modelling studies for spectral energy distribution with data in broader wavelength bands will be presented in forthcoming papers on individual sources in the iMOGABA program. 

We would like to thank the anonymous referee for important comments and suggestions which have enormously improved the manuscript.  We are grateful to all staff members at KVN who helped to operate the array and to correlate the data.  The KVN is a facility operated by the Korea Astronomy and Space Science Institute.  The KVN operations are supported by KREONET (Korea Research Environment Open NETwork) which is managed and operated by KISTI (Korea Institute of Science and Technology Information).  This work was supported by the National Research Foundation of Korea(NRF) grant funded by the Korea government(MSIP) (No.  NRF-2016R1C1B2006697).  Dae-Won Kim and Sascha Trippe acknowledge support from the National Research Foundation of Korea (NRF) via grant NRF-2015-R1D1A1A-01056807.  Jongho Park acknowledges support via NRF PhD fellowship grant 2014H1A2A1018695.  Guang-Yao Zhao acknowledges the support from Korea Research Fellowship Program through the National Research Foundation of Korea(NRF) funded by the Ministry of Science, ICT and Future Planning (NRF-2015H1D3A1066561). 

[*Facilities:*]{}

Abdo, A. A., Ackermann, M., Ajello, M., et al.  2010, , 463, 919

Algaba, J.-C., Gabuzda, D. C., & Smith, P. S. 2012, , 420, 542

Algaba, J.-C., Zhao, G.-Y., Lee, S.-S., et al.  2015, JKAS, 48, 237

Algaba, J.-C., Nakamura, M., Asada, K., & Lee, S.-S. 2016, in prep. 

Angelakis, E., Fuhrmann, L., Nestoras, I., et al.  2012, J. Phys.  Conf.  Ser.,  372, 012007

Boettcher, M., Harris, D. E., & Krawczynski, H. 2012, Relativistic Jets from Active Galactic Nuclei (Berlin: Wiley)

Fomalont, E. B. 1999, Synthesis Imaging in Radio Astronomy II, 180, 301

Ghisellini, G., Maraschi, L., & Treves, A. 1985, , 146, 204

Hada, K., Doi, A., Kino, M., Nagai, H., Hagiwara, Y. & Kawaguchi, N. 2011, , 477, 185

Han, S.-T., Lee, J.-W., Kang, J., et al.  2008, Int.  J. Infrared Milli.  Waves, 29, 69

Han, S.-T., Lee, J.-W., Kang, J. et al.  2013, , 125, 539

Hirotani, K. 2005, , 619, 73

Hodgson, J., Lee, S.-S., Zhao, G.-Y., et al.  2016, JKAS, in press

Jorstad, S. G., Marscher, A. P., Mattox, J. R., et al.  2001, , 556, 738

Kang, S., Lee, S.-S., and Byun, D.-Y. 2015, JKAS, 48, 257

Krolik, J. H. 1999, Active galactic nuclei : from the central black hole to the galactic environment (Princeton: Princeton University Press)

L[ä]{}hteenm[ä]{}ki, A. & Valtaoja, E. 2003, , 590, 95

Lee, S.-S., Byun, D. Y., Kim, J., et al.  2011, , 123, 1398

Lee, S. S. 2013, JKAS, 46, 243

Lee, S. S. 2014, JKAS, 47, 303

Lee, S.-S., Petrov, L., Byun, D. Y., et al.  2014, , 147, 77

Lee, S.-S., Oh, C. S., Roh, D. G., et al.  2015a, JKAS, 48, 125

Lee, S.-S., Byun, D.-Y., Oh, C. S., et al.  2015b, JKAS, 48, 229

Lee, S.-S., Lobanov, A., Krichbaum, T. P., et al.  2016, , 826, 135

Lister, M. L., Homan, D. C., Kadler, M., et al.  2009, , 696, 22

Lobanov, A. P. 1998, , 330, 79

Lobanov, A. P. 2005, arXiv astro-ph/0503225

Lobanov, A. P., Krichbaum, T. P., Witzel, A., & Zensus, J. A. 2006, , 58, 253

Marscher, A. P., Jorstad, S. G., D’Arcangelo, F. D., et al.  2008, , 452, 966

Marscher, A. P., Jorstad, S. G., Larionov, V. M., et al.  2011, JApA, 32, 233

Nagai, H., Kino, M., Niinuma, K., et al.  2013, , 65, 24

Niinuma, K., Lee, S.-S., Kino, M., et al.  2014, , 66, 103

Ojha, R., Kadler, M., B[ö]{}ck, M., et al.  2010, , 519, 45

O’Sullivan, S. P. & Gabuzda, D. C. 2009, , 400, 26

Savolainen, T., Wiik, K., Valtaoja, E., et la.  2002, , 394, 851

Rioja, M., & Dodson, R. 2011, , 141, 114

Rioja, M. J., Dodson, R., Jung, T., et al.  2014, , 148, 84

Shepherd, M. C., Pearson, T. J., & Taylor, G. B. 1994, , 26, 987

V[é]{}ron-Cetty, M.-P., & V[é]{}ron, P. 2006, , 455, 773

[lcccccc]{} 0218$+$357 & & Q & 0.944 & 02 21 05.468 & $+$35 56 13.73456 & 4.6e-09\
0234$+$285 & 4C +28.07& Q & 1.206 & 02 37 52.405 & $+$28 48 08.98998 & 9.7e-09\
0235$+$164 & & B & 0.940 & 02 38 38.930 & $+$16 36 59.27450 & 1.0e-08\
0316$+$413 & 3C 84& G & 0.018 & 03 19 48.160 & $+$41 30 42.10558 & 2.1e-08\
0415$+$379 & 3C 111& G & 0.049 & 04 18 21.277 & $+$38 01 35.80018 & ...\
0420$-$014 & & Q & 0.916 & 04 23 15.800 & $-$01 20 33.06558 & 5.6e-09\
0528$+$134 & & Q & 2.070 & 05 30 56.416 & $+$13 31 55.14944 & 3.7e-09\
0716$+$714 & & B & 0.127 & 07 21 53.448 & $+$71 20 36.36340 & 2.2e-08\
0727$-$115 & & Q & 1.591 & 07 30 19.112 & $-$11 41 12.60064 & 1.8e-08\
0735$+$178 & & B & 0.450 & 07 38 07.393 & $+$17 42 18.99811 & ...\
0827$+$243 & & Q & 0.942 & 08 30 52.086 & $+$24 10 59.82027 & 1.1e-09\
0836$+$710 & & Q & 2.218 & 08 41 24.365 & $+$70 53 42.17302 & 1.3e-09\
0851$+$202 & OJ 287& B & 0.306 & 08 54 48.874 & $+$20 06 30.64077 & 5.9e-09\
0923$+$392 & 4C +39.25& Q & 0.695 & 09 27 03.013 & $+$39 02 20.85177 & ...\
1055$+$018 & & Q & 0.888 & 10 58 29.605 & $+$01 33 58.82359 & 6.5e-09\
1101$+$384 & Mrk 421& B & 0.031 & 11 04 27.313 & $+$38 12 31.79895 & 3.0e-08\
1127$-$145 & & Q & 1.184 & 11 30 07.052 & $-$14 49 27.38835 & 9.0e-10\
1156$+$295 & & Q & 0.725 & 11 59 31.833 & $+$29 14 43.82678 & 8.4e-09\
1222$+$216 & & Q & 0.434 & 12 24 54.458 & $+$21 22 46.38856 & 2.6e-08\
1226$+$023 & 3C 273B& Q & 0.158 & 12 29 06.699 & $+$02 03 08.59796 & 9.4e-09\
1228$+$126 & M87& G & 0.004 & 12 30 49.423 & $+$12 23 28.04365 & 1.3e-09\
1253$-$055 & 3C 279& Q & 0.536 & 12 56 11.166 & $-$05 47 21.52490 & 2.1e-08\
1308$+$326 & & Q & 0.997 & 13 10 28.663 & $+$32 20 43.78277 & 3.7e-09\
1328$+$307 & 3C 286& Q & 0.846 & 13 31 08.288 & $+$30 30 32.95924 & ...\
1343$+$451 & & Q & 2.534 & 13 45 33.172 & $+$44 52 59.57257 & 6.5e-09\
1611$+$343 & & Q & 1.400 & 16 13 41.064 & $+$34 12 47.90878 & 6.5e-10\
1633$+$382 & 4C +38.41& Q & 1.813 & 16 35 15.492 & $+$38 08 04.50043 & 1.1e-08\
1641$+$399 & 3C 345& Q & 0.593 & 16 42 58.809 & $+$39 48 36.99385 & 2.5e-09\
1749$+$096 & & B & 0.322 & 17 51 32.818 & $+$09 39 00.72829 & 4.3e-09\
1921$-$293 & & Q & 0.353 & 19 24 51.055 & $-$29 14 30.12115 & 2.2e-09\
2200$+$420 & & B & 0.069 & 22 02 43.291 & $+$42 16 39.97986 & 1.6e-08\
2223$-$052 & 3C 446& Q & 1.404 & 22 25 47.259 & $-$04 57 01.39090 & 1.9e-09\
2230$+$114 & CTA 102& Q & 1.037 & 22 32 36.408 & $+$11 43 50.90394 & 5.0e-09\
2251$+$158 & 3C 454.3& Q & 0.859 & 22 53 57.747 & $+$16 08 53.56073 & 1.1e-07\

[lcccrrrrrr]{} 0234$+$285 &K & 5.533 & 3.076 & 83.8 & 2.957 & 2.824 & 11 & 260 & 0.68\
&Q & 2.906 & 1.463 & 81.8 & 2.262 & 2.076 & 11 & 195 & 0.65\
&W & 1.459 & 0.723 & 82.9 & 1.384 & 1.234 & 35 & 35 & 0.70\
&D & 0.959 & 0.535 & $-$86.1 & 0.808 & 0.784 & 38 & 21 & 0.63\
0235$+$164 &K & 7.635 & 3.025 & $-$57.2 & 0.862 & 0.857 & 12 & 72 & 0.54\
&Q & 3.833 & 1.458 & $-$60.0 & 0.775 & 0.755 & 17 & 44 & 0.62\
&W & 1.887 & 0.701 & $-$60.4 & 0.432 & 0.420 & 54 & 8 & 0.49\
&D & 1.495 & 0.509 & $-$53.4 & 0.290 & 0.275 & 46 & 6 & 0.50\
0316$+$413 &K & 5.866 & 2.790 & 88.3 & 27.795 & 23.617 & 162 & 146 & 0.62\
&Q & 3.075 & 1.420 & $-$82.3 & 17.830 & 11.196 & 56 & 201 & 0.77\
&W & 1.446 & 0.688 & 80.9 & 10.350 & 4.951 & 67 & 73 & 0.71\
&D & 0.939 & 0.517 & $-$83.5 & 6.720 & 3.250 & 19 & 174 & 0.72\
0415$+$379 &K & 6.363 & 3.020 & 72.0 & 4.204 & 3.953 & 24 & 163 & 0.61\
&Q & 3.379 & 1.435 & 69.7 & 3.714 & 3.708 & 24 & 152 & 0.69\
&W & 1.710 & 0.712 & 69.7 & 3.830 & 3.724 & 30 & 124 & 0.59\
&D & 1.096 & 0.498 & 76.8 & 2.706 & 2.688 & 36 & 75 & 0.52\
0420$-$014 &K & 6.414 & 3.265 & $-$63.3 & 4.984 & 5.058 & 81 & 62 & 0.52\
&Q & 3.297 & 1.604 & $-$65.1 & 3.814 & 3.777 & 50 & 76 & 0.46\
&W & 1.664 & 0.800 & $-$66.3 & 2.452 & 2.453 & 17 & 144 & 0.46\
&D & 1.085 & 0.553 & $-$52.2 & 1.610 & 1.616 & 56 & 29 & 0.44\
0528$+$134 &K & 5.360 & 3.323 & 86.2 & 1.259 & 1.159 & 6 & 199 & 0.53\
&Q & 2.767 & 1.566 & 82.3 & 0.887 & 0.878 & 11 & 82 & 0.55\
&W & 1.344 & 0.776 & 86.7 & 0.532 & 0.519 & 19 & 27 & 0.56\
&D & 0.888 & 0.566 & $-$81.5 & 0.337 & 0.335 & 18 & 19 & 0.55\
0716$+$714 &K & 5.826 & 4.243 & $-$61.5 & 2.507 & 2.511 & 17 & 145 & 0.58\
&Q & 2.897 & 1.992 & $-$69.9 & 2.658 & 2.654 & 21 & 127 & 0.61\
&W & 1.462 & 0.975 & $-$70.8 & 2.064 & 2.045 & 31 & 66 & 0.58\
&D & 0.970 & 0.681 & $-$60.8 & 1.431 & 1.424 & 20 & 73 & 0.61\
0727$-$115 &K & 6.929 & 3.570 & $-$54.7 & 3.821 & 3.754 & 23 & 166 & 0.48\
&Q & 3.589 & 1.749 & $-$58.2 & 2.298 & 2.291 & 13 & 176 & 0.44\
&W & 1.757 & 0.888 & $-$57.4 & 1.155 & 1.155 & 12 & 95 & 0.43\
&D & 1.206 & 0.588 & $-$45.9 & 0.770 & 0.766 & 5 & 158 & 0.48\
0735$+$178 &K & 7.012 & 3.033 & $-$59.8 & 1.088 & 1.013 & 4 & 250 & 0.62\
&Q & 3.521 & 1.456 & $-$62.7 & 0.891 & 0.836 & 7 & 127 & 0.60\
&W & 1.867 & 0.708 & $-$61.1 & 0.687 & 0.569 & 18 & 31 & 0.59\
&D & 1.050 & 0.501 & $-$57.3 & 0.392 & 0.366 & 14 & 27 & 0.48\
0827$+$243 &K & 9.665 & 3.073 & 60.9 & 0.872 & 0.868 & 19 & 46 & 0.46\
&Q & 5.178 & 1.436 & 60.8 & 0.606 & 0.592 & 20 & 29 & 0.48\
&W & 2.603 & 0.713 & 61.2 & 0.305 & 0.273 & 7 & 38 & 0.47\
&D & 1.614 & 0.521 & 64.0 & 0.278 & 0.275 & 18 & 15 & 0.47\
0836$+$710 &K & 5.680 & 4.162 & $-$53.6 & 1.762 & 1.648 & 11 & 148 & 0.55\
&Q & 2.924 & 1.998 & $-$52.8 & 1.187 & 1.048 & 4 & 264 & 0.64\
&W & 1.466 & 0.991 & $-$53.7 & 0.688 & 0.601 & 16 & 38 & 0.55\
&D & 0.926 & 0.700 & $-$50.8 & 0.403 & 0.336 & 10 & 33 & 0.58\
0851$+$202 &K & 6.126 & 3.080 & $-$65.4 & 4.974 & 4.746 & 15 & 317 & 0.74\
&Q & 3.223 & 1.480 & $-$66.3 & 3.716 & 3.683 & 25 & 149 & 0.64\
&W & 1.585 & 0.734 & $-$64.7 & 2.425 & 2.453 & 48 & 51 & 0.70\
&D & 1.067 & 0.512 & $-$58.5 & 1.692 & 1.651 & 47 & 35 & 0.59\
0923$+$392 &K & 6.429 & 3.181 & $-$61.0 & 8.338 & 8.039 & 50 & 162 & 0.65\
&Q & 3.314 & 1.515 & $-$60.1 & 5.475 & 4.830 & 33 & 147 & 0.62\
&W & 1.697 & 0.730 & $-$63.0 & 3.173 & 2.376 & 49 & 48 & 0.59\
&D & 1.023 & 0.569 & $-$58.8 & 1.588 & 1.193 & 41 & 29 & 0.67\
1055$+$018 &K & 5.620 & 3.449 & $-$68.7 & 2.879 & 2.862 & 23 & 123 & 0.53\
&Q & 3.807 & 1.617 & $-$58.0 & 2.314 & 2.348 & 40 & 58 & 0.48\
&W & 1.754 & 0.781 & $-$60.4 & 1.607 & 1.484 & 28 & 53 & 0.57\
&D & 1.546 & 0.510 & $-$50.7 & 1.053 & 1.047 & 33 & 32 & 0.47\
1101$+$384 &K & 5.229 & 3.170 & $-$80.4 & 0.433 & 0.435 & 3 & 143 & 0.51\
&Q & 2.663 & 1.508 & $-$83.3 & 0.316 & 0.311 & 7 & 43 & 0.56\
&W & 1.329 & 0.741 & $-$82.8 & 0.222 & 0.191 & 9 & 20 & 0.54\
&D & 0.992 & 0.509 & 89.8 & 0.354 & 0.348 & 17 & 21 & 0.45\
1127$-$145 &K & 9.106 & 3.832 & 44.7 & 2.040 & 2.068 & 60 & 34 & 0.42\
&Q & 4.378 & 1.913 & 49.2 & 1.798 & 1.795 & 123 & 15 & 0.49\
&W & 2.228 & 0.933 & 51.9 & 1.496 & 1.404 & 76 & 19 & 0.52\
&D & 1.359 & 0.683 & 52.7 & 0.754 & 0.748 & 93 & 8 & 0.49\
1156$+$295 &K & 6.153 & 2.993 & 77.5 & 0.858 & 0.853 & 20 & 44 & 0.43\
&Q & 3.218 & 1.437 & 75.3 & 0.800 & 0.809 & 20 & 40 & 0.41\
&W & 1.656 & 0.702 & 75.3 & 0.672 & 0.635 & 24 & 26 & 0.48\
&D & 1.089 & 0.480 & 80.5 & 0.478 & 0.481 & 23 & 21 & 0.46\
1222$+$216 &K & 5.343 & 3.317 & $-$75.0 & 2.298 & 2.286 & 21 & 107 & 0.57\
&Q & 2.728 & 1.553 & $-$75.3 & 1.744 & 1.503 & 26 & 59 & 0.59\
&W & 1.399 & 0.760 & $-$73.3 & 1.086 & 0.778 & 11 & 68 & 0.61\
&D & 1.336 & 0.506 & $-$53.7 & 0.569 & 0.432 & 12 & 36 & 0.43\
1226$+$023 &K & 5.816 & 3.493 & $-$72.7 & 8.297 & 6.496 & 87 & 74 & 0.68\
&Q & 3.130 & 1.708 & $-$73.2 & 6.802 & 4.606 & 25 & 187 & 0.72\
&W & 1.604 & 0.801 & $-$66.0 & 3.688 & 2.219 & 47 & 47 & 0.69\
&D & 0.963 & 0.596 & $-$67.6 & 2.354 & 1.564 & 26 & 61 & 0.71\
1228$+$126 &K & 5.186 & 3.445 & $-$83.9 & 2.052 & 1.854 & 14 & 129 & 0.60\
&Q & 2.661 & 1.642 & $-$80.9 & 1.383 & 1.293 & 8 & 158 & 0.57\
&W & 1.353 & 0.793 & $-$78.8 & 0.956 & 0.947 & 14 & 70 & 0.66\
&D & 0.962 & 0.561 & $-$65.4 & 0.663 & 0.659 & 16 & 40 & 0.54\
1253$-$055 &K & 5.499 & 4.506 & 66.6 & 27.655 & 26.394 & 130 & 202 & 0.53\
&Q & 2.659 & 2.116 & $-$74.7 & 20.980 & 18.749 & 95 & 197 & 0.54\
&W & 1.885 & 0.777 & $-$66.9 & 12.517 & 7.642 & 26 & 298 & 0.64\
&D & 1.141 & 0.551 & $-$54.4 & 7.983 & 4.399 & 29 & 154 & 0.81\
1308$+$326 &K & 6.875 & 3.004 & 70.0 & 1.464 & 1.464 & 10 & 140 & 0.45\
&Q & 3.685 & 1.411 & 69.1 & 1.062 & 1.054 & 13 & 84 & 0.43\
&W & 1.793 & 0.721 & 69.7 & 0.726 & 0.631 & 19 & 34 & 0.44\
1328$+$307 &K & 5.438 & 3.117 & 83.2 & 0.819 & 0.401 & 24 & 17 & 0.63\
&Q & 2.682 & 1.494 & 86.0 & 0.067 & 0.061 & 7 & 9 & 0.67\
&W & 1.473 & 0.705 & $-$70.7 & 0.084 & 0.081 & 6 & 14 & 0.47\
&D & 0.966 & 0.507 & $-$60.5 & 0.189 & 0.190 & 14 & 13 & 0.45\
1343$+$451 &K & 5.258 & 3.243 & 86.2 & 0.820 & 0.819 & 8 & 100 & 0.68\
&Q & 2.626 & 1.559 & 89.7 & 0.585 & 0.551 & 12 & 46 & 0.57\
&W & 1.313 & 0.766 & $-$83.6 & 0.333 & 0.262 & 21 & 12 & 0.48\
&D & 0.853 & 0.544 & $-$76.3 & 0.274 & 0.267 & 16 & 17 & 0.60\
1611$+$343 &K & 6.967 & 3.088 & 66.1 & 4.018 & 3.331 & 19 & 172 & 0.67\
&Q & 3.524 & 1.486 & 67.0 & 2.244 & 2.106 & 34 & 61 & 0.63\
&W & 1.792 & 0.727 & 68.2 & 1.315 & 1.191 & 38 & 32 & 0.55\
&D & 1.684 & 0.515 & 65.6 & 0.309 & 0.324 & 70 & 5 & 0.47\
1633$+$382 &K & 6.263 & 3.389 & 65.5 & 5.233 & 5.170 & 34 & 151 & 0.70\
&Q & 3.303 & 1.644 & 63.6 & 5.500 & 5.502 & 61 & 91 & 0.72\
&W & 1.705 & 0.818 & 62.5 & 4.837 & 4.476 & 35 & 127 & 0.62\
&D & 1.023 & 0.538 & 73.8 & 3.056 & 3.002 & 54 & 55 & 0.62\
1641$+$399 &K & 5.053 & 3.521 & $-$81.7 & 4.866 & 4.200 & 40 & 104 & 0.63\
&Q & 2.524 & 1.697 & $-$85.5 & 3.695 & 3.231 & 31 & 106 & 0.62\
&W & 1.251 & 0.832 & $-$81.2 & 2.390 & 1.875 & 22 & 85 & 0.66\
&D & 0.974 & 0.568 & 80.3 & 1.257 & 1.253 & 44 & 29 & 0.59\
1749$+$096 &K & 5.135 & 3.567 & $-$83.9 & 2.933 & 2.829 & 12 & 230 & 0.62\
&Q & 2.621 & 1.717 & $-$86.6 & 2.560 & 2.390 & 13 & 181 & 0.67\
&W & 1.350 & 0.821 & $-$80.5 & 1.891 & 1.502 & 26 & 58 & 0.77\
&D & 0.885 & 0.568 & $-$78.0 & 1.174 & 1.124 & 41 & 28 & 0.65\
1921$-$293 &K & 6.856 & 5.243 & $-$22.3 & 7.553 & 7.452 & 77 & 97 & 0.57\
&Q & 3.466 & 2.604 & $-$17.4 & 5.092 & 4.822 & 27 & 178 & 0.62\
&W & 1.841 & 1.252 & $-$18.8 & 3.012 & 2.246 & 87 & 26 & 0.61\
&D & 1.320 & 0.798 & $-$23.4 & 1.549 & 1.542 & 81 & 19 & 0.49\
2200$+$420 &K & 5.575 & 3.196 & 87.6 & 5.239 & 4.573 & 20 & 223 & 0.70\
&Q & 2.799 & 1.588 & 81.0 & 4.674 & 4.271 & 28 & 152 & 0.64\
&W & 1.423 & 0.776 & 77.9 & 3.458 & 3.497 & 94 & 37 & 0.70\
&D & 0.900 & 0.546 & $-$84.4 & 2.253 & 2.190 & 101 & 22 & 0.61\
2223$-$052 &K & 5.495 & 3.886 & 78.0 & 2.312 & 2.242 & 10 & 222 & 0.56\
&Q & 2.827 & 1.878 & 81.0 & 1.452 & 1.361 & 6 & 213 & 0.56\
&W & 1.446 & 0.921 & 82.0 & 0.629 & 0.604 & 16 & 39 & 0.65\
&D & 0.909 & 0.650 & $-$70.3 & 0.267 & 0.253 & 22 & 11 & 0.52\
2230$+$114 &K & 5.268 & 3.409 & $-$88.0 & 2.313 & 2.088 & 10 & 208 & 0.59\
&Q & 2.689 & 1.642 & 87.6 & 2.138 & 2.023 & 15 & 138 & 0.70\
&W & 1.354 & 0.792 & 82.1 & 1.506 & 1.519 & 30 & 51 & 0.61\
&D & 0.876 & 0.564 & $-$72.3 & 1.568 & 1.089 & 18 & 59 & 0.59\
2251$+$158 &K & 5.205 & 3.419 & $-$81.5 & 7.036 & 6.044 & 25 & 239 & 0.54\
&Q & 2.722 & 1.582 & $-$84.1 & 9.040 & 8.790 & 42 & 209 & 0.61\
&W & 1.348 & 0.781 & $-$86.3 & 8.404 & 8.067 & 64 & 126 & 0.75\
&D & 0.901 & 0.553 & $-$82.8 & 6.520 & 5.975 & 67 & 89 & 0.62\

[lccccrrrr]{} 0234+285 & K & C & 2.951$\pm$0.111 & 2.816$\pm$0.077 & 0.876$\pm$0.024 & ... & ... & 1.394$\pm$ 0.076\
& & J2 & 0.084$\pm$0.018 & 0.085$\pm$0.013 & $<$[*0.602*]{} & 3.741$\pm$0.046 & 1.4$\pm$0.7 & $>$[*0.084*]{}\
& Q & C & 2.290$\pm$0.322 & 2.050$\pm$0.215 & 0.629$\pm$0.066 & ... & ... & 2.098$\pm$ 0.440\
& & J1 & 0.111$\pm$0.095 & 0.123$\pm$0.070 & $<$[*1.171*]{} & 1.820$\pm$0.334 & -26.1$\pm$10.4 & $>$[*0.029*]{}\
& W & C & 1.522$\pm$0.125 & 1.218$\pm$0.078 & 0.468$\pm$0.030 & ... & ... & 2.519$\pm$ 0.323\
& D & C & 0.839$\pm$0.060 & 0.785$\pm$0.041 & 0.183$\pm$0.010 & ... & ... & 9.080$\pm$ 0.949\
0235+164 & K & C & 0.884$\pm$0.027 & 0.857$\pm$0.019 & 0.744$\pm$0.016 & ... & ... & 0.509$\pm$ 0.022\
& Q & C & 0.846$\pm$0.028 & 0.756$\pm$0.018 & 0.698$\pm$0.017 & ... & ... & 0.553$\pm$ 0.027\
& W & C & 0.496$\pm$0.069 & 0.420$\pm$0.045 & 0.408$\pm$0.043 & ... & ... & 0.950$\pm$ 0.202\
& D & C & 0.314$\pm$0.149 & 0.275$\pm$0.098 & 0.361$\pm$0.128 & ... & ... & 0.768$\pm$ 0.551\
0316+413 & K & C & 28.231$\pm$1.670 & 22.837$\pm$1.050 & 1.770$\pm$0.081 & ... & ... & 1.507$\pm$ 0.139\
& & J1 & 1.481$\pm$0.175 & 1.435$\pm$0.122 & 0.713$\pm$0.061 & 2.991$\pm$0.030 & 1.7$\pm$0.6 & 0.487$\pm$ 0.083\
& & J2 & 0.408$\pm$0.300 & 0.458$\pm$0.224 & $<$[*2.004*]{} & 6.403$\pm$0.490 & -129.2$\pm$4.4 & $>$[*0.017*]{}\
& Q & C & 7.317$\pm$1.670 & 5.894$\pm$1.047 & 0.855$\pm$0.152 & ... & ... & 1.673$\pm$ 0.596\
& & J3 & 11.060$\pm$2.242 & 11.175$\pm$1.593 & $<$[*0.281*]{} & 1.985$\pm$0.020 & -178.9$\pm$0.6 & $>$[*23.345*]{}\
& W & C & 6.029$\pm$1.303 & 4.497$\pm$0.779 & 0.517$\pm$0.090 & ... & ... & 3.771$\pm$ 1.308\
& & J3 & 8.149$\pm$1.490 & 3.340$\pm$0.565 & 0.928$\pm$0.157 & 2.413$\pm$0.079 & 179.1$\pm$1.9 & 1.582$\pm$ 0.535\
& D & C & 3.795$\pm$0.329 & 3.246$\pm$0.214 & 0.276$\pm$0.018 & ... & ... & 8.329$\pm$ 1.097\
& & J3 & 2.977$\pm$0.313 & 1.830$\pm$0.164 & 0.487$\pm$0.044 & 2.444$\pm$0.022 & 177.3$\pm$0.5 & 2.099$\pm$ 0.376\
& & J4 & 0.469$\pm$0.186 & 0.338$\pm$0.109 & 0.441$\pm$0.142 & 1.559$\pm$0.071 & 177.9$\pm$2.6 & 0.403$\pm$ 0.260\
& & J5 & 0.689$\pm$0.374 & 0.288$\pm$0.144 & 0.700$\pm$0.351 & 0.812$\pm$0.175 & 150.6$\pm$12.2 & 0.235$\pm$ 0.236\
0415+379 & K & C & 3.934$\pm$0.344 & 3.940$\pm$0.243 & $<$[*0.255*]{} & ... & ... & $>$[*10.466*]{}\
& & J1 & 0.237$\pm$0.119 & 0.250$\pm$0.086 & $<$[*1.460*]{} & 6.446$\pm$0.252 & 64.5$\pm$2.2 & $>$[*0.019*]{}\
& Q & C & 3.696$\pm$0.394 & 3.708$\pm$0.279 & $<$[*0.156*]{} & ... & ... & $>$[*26.125*]{}\
& W & C & 3.894$\pm$0.090 & 3.712$\pm$0.062 & 0.219$\pm$0.004 & ... & ... & 13.994$\pm$ 0.471\
& D & C & 2.749$\pm$0.047 & 2.688$\pm$0.033 & 0.102$\pm$0.001 & ... & ... & 45.541$\pm$ 1.124\
0420-014 & K & C & 5.113$\pm$0.064 & 5.058$\pm$0.045 & 0.463$\pm$0.004 & ... & ... & 7.508$\pm$ 0.134\
& Q & C & 4.046$\pm$0.132 & 3.777$\pm$0.090 & 0.574$\pm$0.014 & ... & ... & 3.866$\pm$ 0.184\
& W & C & 2.402$\pm$0.711 & 2.453$\pm$0.508 & $<$[*0.227*]{} & ... & ... & $>$[*14.685*]{}\
& D & C & 1.643$\pm$0.164 & 1.616$\pm$0.115 & 0.110$\pm$0.008 & ... & ... & 42.745$\pm$ 6.083\
0528+134 & K & C & 1.147$\pm$0.083 & 1.149$\pm$0.059 & $<$[*0.203*]{} & ... & ... & $>$[*14.053*]{}\
& & J1 & 0.179$\pm$0.096 & 0.066$\pm$0.033 & 4.406$\pm$2.224 & 4.543$\pm$1.112 & 37.6$\pm$13.8 & 0.005$\pm$ 0.005\
& Q & C & 0.935$\pm$0.045 & 0.878$\pm$0.031 & 0.520$\pm$0.018 & ... & ... & 1.744$\pm$ 0.122\
& W & C & 0.614$\pm$0.054 & 0.519$\pm$0.035 & 0.420$\pm$0.028 & ... & ... & 1.756$\pm$ 0.238\
& D & C & 0.333$\pm$0.069 & 0.336$\pm$0.049 & $<$[*0.097*]{} & ... & ... & $>$[*17.823*]{}\
0716+714 & K & C & 2.490$\pm$0.465 & 2.511$\pm$0.330 & $<$[*0.616*]{} & ... & ... & $>$[*1.213*]{}\
& Q & C & 2.733$\pm$0.047 & 2.654$\pm$0.033 & 0.427$\pm$0.005 & ... & ... & 2.775$\pm$ 0.069\
& W & C & 2.061$\pm$0.041 & 2.045$\pm$0.029 & 0.109$\pm$0.002 & ... & ... & 32.119$\pm$ 0.902\
& D & C & 1.436$\pm$0.034 & 1.425$\pm$0.024 & 0.073$\pm$0.001 & ... & ... & 49.894$\pm$ 1.679\
0727-115 & K & C & 3.848$\pm$0.126 & 3.724$\pm$0.088 & 0.866$\pm$0.020 & ... & ... & 2.184$\pm$ 0.103\
& & J1 & 0.101$\pm$0.048 & 0.108$\pm$0.035 & $<$[*1.587*]{} & 3.822$\pm$0.258 & -82.9$\pm$3.9 & $>$[*0.017*]{}\
& Q & C & 2.367$\pm$0.044 & 2.292$\pm$0.031 & 0.428$\pm$0.006 & ... & ... & 5.500$\pm$ 0.148\
& W & C & 1.146$\pm$0.198 & 1.155$\pm$0.141 & $<$[*0.143*]{} & ... & ... & $>$[*23.705*]{}\
& D & C & 0.786$\pm$0.025 & 0.766$\pm$0.018 & 0.129$\pm$0.003 & ... & ... & 20.106$\pm$ 0.931\
0735+178 & K & C & 1.000$\pm$0.090 & 1.002$\pm$0.063 & $<$[*0.274*]{} & ... & ... & $>$[*3.167*]{}\
& & J1 & 0.104$\pm$0.033 & 0.052$\pm$0.015 & 3.588$\pm$1.005 & 4.290$\pm$0.502 & 71.7$\pm$6.7 & 0.002$\pm$ 0.001\
& Q & C & 0.908$\pm$0.045 & 0.819$\pm$0.030 & 0.659$\pm$0.024 & ... & ... & 0.498$\pm$ 0.037\
& W & C & 0.738$\pm$0.079 & 0.551$\pm$0.047 & 0.550$\pm$0.047 & ... & ... & 0.581$\pm$ 0.099\
& D & C & 0.426$\pm$0.031 & 0.380$\pm$0.021 & 0.229$\pm$0.012 & ... & ... & 1.935$\pm$ 0.211\
& & J1 & 0.068$\pm$0.017 & 0.068$\pm$0.012 & $<$[*0.118*]{} & 0.645$\pm$0.010 & 29.7$\pm$0.9 & $>$[*1.169*]{}\
0827+243 & K & C & 0.905$\pm$0.027 & 0.868$\pm$0.019 & 0.912$\pm$0.020 & ... & ... & 0.347$\pm$ 0.015\
& Q & C & 0.667$\pm$0.039 & 0.592$\pm$0.026 & 0.727$\pm$0.032 & ... & ... & 0.403$\pm$ 0.035\
& W & C & 0.324$\pm$0.028 & 0.267$\pm$0.018 & 0.467$\pm$0.032 & ... & ... & 0.474$\pm$ 0.064\
& D & C & 0.287$\pm$0.015 & 0.275$\pm$0.011 & 0.158$\pm$0.006 & ... & ... & 3.668$\pm$ 0.286\
0836+710 & K & C & 1.994$\pm$0.141 & 1.633$\pm$0.089 & 2.265$\pm$0.124 & ... & ... & 0.205$\pm$ 0.023\
& & J1 & 0.061$\pm$0.027 & 0.065$\pm$0.020 & $<$[*1.470*]{} & 4.698$\pm$0.227 & -136.9$\pm$2.8 & $>$[*0.015*]{}\
& Q & C & 1.065$\pm$0.029 & 1.048$\pm$0.021 & 0.317$\pm$0.006 & ... & ... & 5.603$\pm$ 0.221\
& & J2 & 0.137$\pm$0.017 & 0.137$\pm$0.012 & 0.213$\pm$0.018 & 2.458$\pm$0.009 & -140.1$\pm$0.2 & 1.596$\pm$ 0.274\
& W & C & 0.656$\pm$0.160 & 0.590$\pm$0.107 & 0.460$\pm$0.083 & ... & ... & 1.639$\pm$ 0.596\
& D & C & 0.519$\pm$0.060 & 0.335$\pm$0.032 & 0.566$\pm$0.055 & ... & ... & 0.857$\pm$ 0.165\
& & J3 & 0.053$\pm$0.007 & 0.044$\pm$0.005 & 0.359$\pm$0.038 & 0.954$\pm$0.019 & -153.8$\pm$1.1 & 0.217$\pm$ 0.046\
0851+202 & K & C & 4.707$\pm$0.435 & 4.714$\pm$0.307 & $<$[*0.266*]{} & ... & ... & $>$[*14.244*]{}\
& & J1 & 0.252$\pm$0.134 & 0.123$\pm$0.059 & 3.476$\pm$1.659 & 4.026$\pm$0.829 & -107.2$\pm$11.6 & 0.004$\pm$ 0.004\
& Q & C & 3.838$\pm$0.089 & 3.683$\pm$0.062 & 0.414$\pm$0.007 & ... & ... & 4.805$\pm$ 0.162\
& W & C & 2.755$\pm$0.112 & 2.453$\pm$0.074 & 0.345$\pm$0.010 & ... & ... & 4.966$\pm$ 0.301\
& D & C & 1.764$\pm$0.106 & 1.653$\pm$0.073 & 0.179$\pm$0.008 & ... & ... & 11.813$\pm$ 1.041\
0923+392 & K & C & 0.552$\pm$0.123 & 6.518$\pm$0.123 & 3.812$\pm$0.072 & ... & ... & 0.011$\pm$ 0.001\
& & J1 & 7.994$\pm$18.767 & 0.262$\pm$0.615 & $<$[*0.326*]{} & 5.683$\pm$0.383 & 100.3$\pm$3.9 & $>$[*20.917*]{}\
& Q & C & 0.743$\pm$0.127 & 0.237$\pm$0.039 & 1.147$\pm$0.187 & ... & ... & 0.157$\pm$ 0.051\
& & J1 & 5.222$\pm$2.652 & 0.555$\pm$0.280 & 0.607$\pm$0.307 & 3.174$\pm$0.153 & 100.6$\pm$2.8 & 3.947$\pm$ 3.986\
& W & C & 0.509$\pm$0.056 & 0.501$\pm$0.039 & 0.755$\pm$0.059 & ... & ... & 0.249$\pm$ 0.039\
& & J1 & 3.309$\pm$2.701 & 0.301$\pm$0.245 & 0.629$\pm$0.511 & 2.779$\pm$0.256 & 98.3$\pm$5.3 & 2.329$\pm$ 3.787\
& D & C & 1.899$\pm$0.306 & 1.141$\pm$0.158 & 0.555$\pm$0.077 & ... & ... & 1.717$\pm$ 0.475\
1055+018 & K & C & 2.849$\pm$0.262 & 2.856$\pm$0.185 & $<$[*0.269*]{} & ... & ... & $>$[*12.239*]{}\
& Q & C & 2.438$\pm$0.071 & 2.348$\pm$0.049 & 0.438$\pm$0.009 & ... & ... & 3.942$\pm$ 0.166\
& W & C & 1.717$\pm$0.064 & 1.475$\pm$0.041 & 0.426$\pm$0.012 & ... & ... & 2.935$\pm$ 0.165\
& D & C & 1.068$\pm$0.030 & 1.047$\pm$0.021 & 0.103$\pm$0.002 & ... & ... & 31.226$\pm$ 1.233\
1101+384 & K & C & 0.442$\pm$0.019 & 0.435$\pm$0.013 & 0.530$\pm$0.016 & ... & ... & 0.266$\pm$ 0.016\
& Q & C & 0.347$\pm$0.018 & 0.311$\pm$0.012 & 0.661$\pm$0.025 & ... & ... & 0.134$\pm$ 0.010\
& W & C & 0.222$\pm$0.052 & 0.187$\pm$0.034 & 0.438$\pm$0.079 & ... & ... & 0.196$\pm$ 0.071\
& D & C & 0.365$\pm$0.018 & 0.348$\pm$0.012 & 0.151$\pm$0.005 & ... & ... & 2.711$\pm$ 0.188\
1127-145 & K & C & 2.074$\pm$0.144 & 2.068$\pm$0.102 & $<$[*0.273*]{} & ... & ... & $>$[*10.012*]{}\
& Q & C & 1.837$\pm$0.213 & 1.794$\pm$0.149 & 0.464$\pm$0.039 & ... & ... & 3.062$\pm$ 0.509\
& W & C & 1.391$\pm$0.285 & 1.406$\pm$0.203 & $<$[*0.197*]{} & ... & ... & $>$[*12.913*]{}\
& D & C & 0.747$\pm$0.087 & 0.749$\pm$0.061 & $<$[*0.074*]{} & ... & ... & $>$[*48.720*]{}\
1156+295 & K & C & 0.866$\pm$0.027 & 0.853$\pm$0.019 & 0.496$\pm$0.011 & ... & ... & 0.998$\pm$ 0.044\
& Q & C & 0.892$\pm$0.044 & 0.809$\pm$0.030 & 0.624$\pm$0.023 & ... & ... & 0.649$\pm$ 0.048\
& W & C & 0.790$\pm$0.064 & 0.635$\pm$0.040 & 0.462$\pm$0.029 & ... & ... & 1.049$\pm$ 0.132\
& D & C & 0.490$\pm$0.032 & 0.481$\pm$0.022 & 0.095$\pm$0.004 & ... & ... & 15.387$\pm$ 1.418\
1222+216 & K & C & 2.351$\pm$0.044 & 2.287$\pm$0.031 & 0.713$\pm$0.010 & ... & ... & 1.090$\pm$ 0.029\
& Q & C & 1.734$\pm$0.090 & 1.495$\pm$0.059 & 0.792$\pm$0.031 & ... & ... & 0.651$\pm$ 0.051\
& & J1 & 0.175$\pm$0.019 & 0.171$\pm$0.013 & 0.356$\pm$0.028 & 1.603$\pm$0.014 & 13.6$\pm$0.5 & 0.325$\pm$ 0.051\
& W & C & 0.872$\pm$0.109 & 0.776$\pm$0.073 & 0.336$\pm$0.031 & ... & ... & 1.820$\pm$ 0.341\
& & J1 & 0.253$\pm$0.072 & 0.258$\pm$0.051 & $<$[*0.195*]{} & 0.981$\pm$0.019 & 4.2$\pm$1.1 & $>$[*1.575*]{}\
& D & C & 0.403$\pm$0.136 & 0.426$\pm$0.099 & $<$[*0.187*]{} & ... & ... & $>$[*2.708*]{}\
& & J1 & 0.123$\pm$0.057 & 0.123$\pm$0.040 & $<$[*0.247*]{} & 0.925$\pm$0.040 & -14.1$\pm$2.5 & $>$[*0.473*]{}\
1226+023 & K & C & 6.945$\pm$0.810 & 6.391$\pm$0.548 & 1.307$\pm$0.112 & ... & ... & 0.774$\pm$ 0.133\
& & J3 & 1.511$\pm$0.375 & 1.538$\pm$0.268 & $<$[*0.745*]{} & 4.120$\pm$0.065 & -136.2$\pm$0.9 & $>$[*0.519*]{}\
& Q & C & 4.749$\pm$0.062 & 4.688$\pm$0.044 & 0.259$\pm$0.002 & ... & ... & 13.472$\pm$ 0.251\
& & J2 & 0.823$\pm$0.041 & 0.800$\pm$0.029 & 0.377$\pm$0.014 & 1.962$\pm$0.007 & -140.2$\pm$0.2 & 1.102$\pm$ 0.079\
& & J3 & 0.958$\pm$0.054 & 0.675$\pm$0.031 & 1.386$\pm$0.064 & 4.344$\pm$0.032 & -143.5$\pm$0.4 & 0.095$\pm$ 0.009\
& & J4 & 1.373$\pm$0.212 & 0.350$\pm$0.052 & 3.064$\pm$0.459 & 7.402$\pm$0.230 & -141.9$\pm$1.8 & 0.028$\pm$ 0.008\
& & J5 & 0.720$\pm$0.161 & 0.291$\pm$0.060 & 2.353$\pm$0.487 & 10.642$\pm$0.243 & -141.6$\pm$1.3 & 0.025$\pm$ 0.010\
& W & C & 2.987$\pm$0.248 & 2.144$\pm$0.145 & 0.641$\pm$0.043 & ... & ... & 1.383$\pm$ 0.187\
& & J1 & 1.293$\pm$0.246 & 0.852$\pm$0.135 & 0.709$\pm$0.113 & 1.043$\pm$0.056 & -138.2$\pm$3.1 & 0.489$\pm$ 0.156\
& & J2 & 0.184$\pm$0.096 & 0.198$\pm$0.071 & $<$[*0.398*]{} & 1.931$\pm$0.071 & -143.1$\pm$2.1 & $>$[*0.221*]{}\
& D & C & 1.829$\pm$0.225 & 1.605$\pm$0.149 & 0.279$\pm$0.026 & ... & ... & 4.471$\pm$ 0.829\
& & J1 & 0.936$\pm$0.403 & 0.427$\pm$0.167 & 0.704$\pm$0.276 & 0.903$\pm$0.138 & -143.1$\pm$8.7 & 0.359$\pm$ 0.282\
1228+126 & K & C & 1.837$\pm$0.210 & 1.844$\pm$0.149 & $<$[*0.321*]{} & ... & ... & $>$[*2.933*]{}\
& & J1 & 0.199$\pm$0.013 & 0.198$\pm$0.009 & 0.408$\pm$0.018 & 5.115$\pm$0.009 & -69.7$\pm$0.1 & 0.197$\pm$ 0.018\
& Q & C & 1.286$\pm$0.197 & 1.295$\pm$0.140 & $<$[*0.213*]{} & ... & ... & $>$[*4.690*]{}\
& & J1 & 0.098$\pm$0.034 & 0.090$\pm$0.023 & $<$[*0.449*]{} & 3.023$\pm$0.057 & -70.0$\pm$1.1 & $>$[*0.080*]{}\
& W & C & 1.068$\pm$0.049 & 0.947$\pm$0.033 & 0.362$\pm$0.012 & ... & ... & 1.345$\pm$ 0.093\
& D & C & 0.657$\pm$0.073 & 0.659$\pm$0.051 & $<$[*0.054*]{} & ... & ... & $>$[*37.271*]{}\
1253-055 & K & C & 30.173$\pm$1.175 & 26.605$\pm$0.777 & 1.882$\pm$0.055 & ... & ... & 2.150$\pm$ 0.126\
& Q & C & 20.803$\pm$0.811 & 18.545$\pm$0.540 & 0.857$\pm$0.025 & ... & ... & 7.148$\pm$ 0.416\
& & J1 & 1.888$\pm$0.356 & 1.720$\pm$0.240 & 0.843$\pm$0.118 & 2.106$\pm$0.059 & -137.2$\pm$1.6 & 0.670$\pm$ 0.187\
& W & C & 7.396$\pm$1.100 & 6.780$\pm$0.743 & 0.300$\pm$0.033 & 0.287$\pm$0.016 & 28.3$\pm$3.3 & 20.738$\pm$ 4.553\
& & J1 & 5.256$\pm$1.195 & 5.320$\pm$0.850 & $<$[*0.183*]{} & 0.454$\pm$0.015 & -152.8$\pm$1.8 & $>$[*39.733*]{}\
& D & C & 7.699$\pm$1.481 & 4.123$\pm$0.699 & 0.591$\pm$0.100 & ... & ... & 5.562$\pm$ 1.887\
& & J1 & 2.372$\pm$0.688 & 2.426$\pm$0.492 & $<$[*0.153*]{} & 0.726$\pm$0.016 & -153.7$\pm$1.2 & $>$[*25.569*]{}\
1308+326 & K & C & 1.436$\pm$0.405 & 1.464$\pm$0.289 & $<$[*0.851*]{} & ... & ... & $>$[*0.650*]{}\
& Q & C & 1.105$\pm$0.030 & 1.055$\pm$0.021 & 0.434$\pm$0.009 & ... & ... & 1.925$\pm$ 0.077\
& W & C & 0.740$\pm$0.113 & 0.615$\pm$0.072 & 0.442$\pm$0.052 & ... & ... & 1.243$\pm$ 0.292\
1328+307 & K & C & 0.602$\pm$0.194 & 0.375$\pm$0.103 & 2.917$\pm$0.798 & ... & ... & 0.021$\pm$ 0.012\
& & J1 & 0.453$\pm$0.070 & 0.283$\pm$0.037 & 2.875$\pm$0.376 & 5.248$\pm$0.188 & 43.2$\pm$2.1 & 0.017$\pm$ 0.004\
& Q & C & 0.083$\pm$0.015 & 0.061$\pm$0.009 & 1.106$\pm$0.166 & ... & ... & 0.021$\pm$ 0.006\
& W & C & 0.102$\pm$0.010 & 0.081$\pm$0.006 & 0.472$\pm$0.037 & ... & ... & 0.139$\pm$ 0.022\
& D & C & 0.195$\pm$0.020 & 0.190$\pm$0.014 & 0.122$\pm$0.009 & ... & ... & 3.973$\pm$ 0.586\
1343+451 & K & C & 0.826$\pm$0.026 & 0.819$\pm$0.018 & 0.382$\pm$0.008 & ... & ... & 3.287$\pm$ 0.146\
& Q & C & 0.607$\pm$0.037 & 0.549$\pm$0.025 & 0.649$\pm$0.029 & ... & ... & 0.837$\pm$ 0.075\
& W & C & 0.326$\pm$0.060 & 0.250$\pm$0.036 & 0.499$\pm$0.073 & ... & ... & 0.760$\pm$ 0.221\
& D & C & 0.279$\pm$0.024 & 0.267$\pm$0.017 & 0.148$\pm$0.009 & ... & ... & 7.395$\pm$ 0.927\
1611+343 & K & C & 3.229$\pm$0.386 & 3.242$\pm$0.273 & $<$[*0.368*]{} & ... & ... & $>$[*9.380*]{}\
& & J1 & 0.723$\pm$0.129 & 0.582$\pm$0.081 & 1.940$\pm$0.271 & 4.360$\pm$0.135 & 163.9$\pm$1.8 & 0.076$\pm$ 0.021\
& & J2 & 0.258$\pm$0.102 & 0.173$\pm$0.057 & 3.041$\pm$1.001 & 3.443$\pm$0.500 & -132.2$\pm$8.3 & 0.011$\pm$ 0.007\
& Q & C & 2.317$\pm$0.144 & 2.085$\pm$0.096 & 0.678$\pm$0.031 & ... & ... & 1.987$\pm$ 0.184\
& W & C & 1.508$\pm$0.126 & 1.186$\pm$0.078 & 0.509$\pm$0.033 & ... & ... & 2.295$\pm$ 0.301\
& D & C & 0.327$\pm$0.036 & 0.324$\pm$0.026 & 0.097$\pm$0.008 & ... & ... & 13.703$\pm$ 2.171\
1633+382 & K & C & 5.266$\pm$0.104 & 5.172$\pm$0.073 & 0.608$\pm$0.009 & ... & ... & 6.584$\pm$ 0.185\
& Q & C & 5.856$\pm$0.112 & 5.503$\pm$0.077 & 0.559$\pm$0.008 & ... & ... & 8.661$\pm$ 0.241\
& W & C & 5.104$\pm$0.188 & 4.457$\pm$0.124 & 0.416$\pm$0.012 & ... & ... & 13.630$\pm$ 0.757\
& D & C & 3.247$\pm$0.145 & 3.004$\pm$0.099 & 0.202$\pm$0.007 & ... & ... & 36.776$\pm$ 2.418\
1641+399 & K & C & 4.406$\pm$0.236 & 4.184$\pm$0.163 & 0.998$\pm$0.039 & ... & ... & 1.158$\pm$ 0.090\
& & J4 & 0.960$\pm$0.333 & 0.526$\pm$0.160 & 3.537$\pm$1.077 & 5.955$\pm$0.538 & -84.5$\pm$5.2 & 0.020$\pm$ 0.012\
& Q & C & 3.432$\pm$0.210 & 3.225$\pm$0.144 & 0.534$\pm$0.024 & ... & ... & 3.150$\pm$ 0.281\
& & J3 & 0.372$\pm$0.102 & 0.308$\pm$0.065 & 0.940$\pm$0.198 & 2.667$\pm$0.099 & -90.7$\pm$2.1 & 0.110$\pm$ 0.047\
& W & C & 1.930$\pm$0.141 & 1.879$\pm$0.098 & 0.162$\pm$0.008 & ... & ... & 19.247$\pm$ 2.016\
& & J1 & 0.118$\pm$0.038 & 0.123$\pm$0.027 & $<$[*0.219*]{} & 0.787$\pm$0.024 & -128.9$\pm$1.8 & $>$[*0.644*]{}\
& & J2 & 0.363$\pm$0.102 & 0.370$\pm$0.073 & $<$[*0.190*]{} & 1.340$\pm$0.019 & -92.2$\pm$0.8 & $>$[*2.630*]{}\
& & J3 & 0.159$\pm$0.032 & 0.148$\pm$0.022 & 0.316$\pm$0.047 & 2.169$\pm$0.024 & -76.7$\pm$0.6 & 0.417$\pm$ 0.124\
& D & C & 1.215$\pm$0.392 & 1.254$\pm$0.281 & $<$[*0.160*]{} & ... & ... & $>$[*12.434*]{}\
1749+096 & K & C & 2.799$\pm$0.352 & 2.808$\pm$0.249 & $<$[*0.357*]{} & ... & ... & $>$[*4.766*]{}\
& & J1 & 0.145$\pm$0.082 & 0.091$\pm$0.043 & 3.503$\pm$1.671 & 3.845$\pm$0.835 & 48.9$\pm$12.3 & 0.003$\pm$ 0.002\
& Q & C & 2.718$\pm$0.158 & 2.382$\pm$0.104 & 0.795$\pm$0.035 & ... & ... & 0.934$\pm$ 0.082\
& W & C & 1.700$\pm$0.523 & 1.465$\pm$0.341 & 0.470$\pm$0.110 & ... & ... & 1.671$\pm$ 0.782\
& D & C & 1.273$\pm$0.318 & 1.125$\pm$0.211 & 0.284$\pm$0.053 & ... & ... & 3.428$\pm$ 1.288\
1921-293 & K & C & 8.091$\pm$0.297 & 7.456$\pm$0.201 & 1.808$\pm$0.049 & ... & ... & 0.550$\pm$ 0.030\
& Q & C & 5.223$\pm$0.354 & 4.816$\pm$0.240 & 0.888$\pm$0.044 & ... & ... & 1.472$\pm$ 0.147\
& & J2 & 0.271$\pm$0.103 & 0.281$\pm$0.074 & $<$[*0.761*]{} & 3.089$\pm$0.101 & 24.2$\pm$1.9 & $>$[*0.104*]{}\
& W & C & 2.004$\pm$0.553 & 2.043$\pm$0.395 & $<$[*0.279*]{} & ... & ... & $>$[*5.739*]{}\
& & J1 & 1.170$\pm$0.351 & 0.609$\pm$0.162 & 1.280$\pm$0.340 & 1.428$\pm$0.170 & 4.2$\pm$6.8 & 0.159$\pm$ 0.084\
& D & C & 1.697$\pm$0.087 & 1.543$\pm$0.058 & 0.320$\pm$0.012 & ... & ... & 3.683$\pm$ 0.278\
2200+420 & K & C & 4.838$\pm$0.322 & 4.544$\pm$0.220 & 1.055$\pm$0.051 & ... & ... & 0.763$\pm$ 0.074\
& & J2 & 0.605$\pm$0.087 & 0.499$\pm$0.055 & 1.859$\pm$0.206 & 4.017$\pm$0.103 & -163.8$\pm$1.5 & 0.031$\pm$ 0.007\
& Q & C & 4.351$\pm$0.164 & 4.231$\pm$0.114 & 0.350$\pm$0.009 & ... & ... & 6.236$\pm$ 0.337\
& & J1 & 0.499$\pm$0.112 & 0.283$\pm$0.055 & 1.623$\pm$0.316 & 2.038$\pm$0.158 & -161.0$\pm$4.4 & 0.033$\pm$ 0.013\
& W & C & 3.925$\pm$0.094 & 3.498$\pm$0.063 & 0.352$\pm$0.006 & ... & ... & 5.561$\pm$ 0.199\
& D & C & 2.326$\pm$0.122 & 2.191$\pm$0.084 & 0.174$\pm$0.007 & ... & ... & 13.488$\pm$ 1.029\
2223-052 & K & C & 2.240$\pm$0.164 & 2.244$\pm$0.116 & $<$[*0.225*]{} & ... & ... & $>$[*17.503*]{}\
& & J2 & 0.084$\pm$0.029 & 0.087$\pm$0.021 & $<$[*1.075*]{} & 6.026$\pm$0.130 & 94.0$\pm$1.2 & $>$[*0.029*]{}\
& Q & C & 1.427$\pm$0.134 & 1.360$\pm$0.093 & 0.503$\pm$0.034 & ... & ... & 2.228$\pm$ 0.304\
& & J1 & 0.136$\pm$0.042 & 0.094$\pm$0.024 & 1.521$\pm$0.383 & 2.632$\pm$0.191 & 107.0$\pm$4.2 & 0.023$\pm$ 0.012\
& W & C & 0.691$\pm$0.057 & 0.600$\pm$0.037 & 0.443$\pm$0.027 & ... & ... & 1.391$\pm$ 0.173\
& D & C & 0.298$\pm$0.046 & 0.253$\pm$0.030 & 0.326$\pm$0.039 & ... & ... & 1.107$\pm$ 0.263\
2230+114 & K & C & 2.227$\pm$0.097 & 2.119$\pm$0.067 & 0.968$\pm$0.031 & ... & ... & 0.795$\pm$ 0.050\
& & J1 & 0.299$\pm$0.056 & 0.189$\pm$0.030 & 3.013$\pm$0.480 & 5.372$\pm$0.240 & 167.2$\pm$2.6 & 0.011$\pm$ 0.004\
& Q & C & 2.235$\pm$0.213 & 1.995$\pm$0.142 & 0.719$\pm$0.051 & ... & ... & 1.447$\pm$ 0.206\
& W & C & 1.618$\pm$0.083 & 1.519$\pm$0.057 & 0.260$\pm$0.010 & ... & ... & 8.010$\pm$ 0.600\
& D & C & 1.308$\pm$0.171 & 1.078$\pm$0.109 & 0.325$\pm$0.033 & ... & ... & 4.144$\pm$ 0.838\
& & J1 & 0.199$\pm$0.020 & 0.190$\pm$0.014 & 0.144$\pm$0.011 & 0.761$\pm$0.005 & 73.8$\pm$0.4 & 3.212$\pm$ 0.478\
& & J2 & 0.165$\pm$0.064 & 0.170$\pm$0.046 & $<$[*0.181*]{} & 1.046$\pm$0.025 & 115.8$\pm$1.3 & $>$[*1.677*]{}\
2251+158 & K & C & 5.924$\pm$0.499 & 5.936$\pm$0.353 & $<$[*0.236*]{} & ... & ... & $>$[*32.440*]{}\
& & J2 & 0.582$\pm$0.100 & 0.485$\pm$0.064 & 1.842$\pm$0.244 & 3.856$\pm$0.122 & -92.3$\pm$1.8 & 0.052$\pm$ 0.014\
& & J3 & 0.368$\pm$0.161 & 0.388$\pm$0.117 & $<$[*1.234*]{} & 7.690$\pm$0.186 & -69.3$\pm$1.4 & $>$[*0.074*]{}\
& & J4 & 0.249$\pm$0.053 & 0.224$\pm$0.036 & 1.458$\pm$0.232 & 11.371$\pm$0.116 & -58.6$\pm$0.6 & 0.036$\pm$ 0.011\
& Q & C & 8.868$\pm$0.190 & 8.721$\pm$0.133 & 0.268$\pm$0.004 & ... & ... & 37.709$\pm$ 1.152\
& & J1 & 0.555$\pm$0.184 & 0.217$\pm$0.067 & 2.128$\pm$0.658 & 2.062$\pm$0.329 & -120.1$\pm$9.1 & 0.037$\pm$ 0.023\
& W & C & 8.954$\pm$0.424 & 8.073$\pm$0.284 & 0.331$\pm$0.012 & ... & ... & 24.961$\pm$ 1.756\
& D & C & 6.124$\pm$0.390 & 5.933$\pm$0.271 & 0.127$\pm$0.006 & ... & ... & 115.964$\pm$10.610\

[^1]: http://sci.esa.int/integral/

[^2]: http://agile.rm.iasf.cnr.it/

[^3]: http://fermi.gsfc.nasa.gov/
