VizieR Online Data Catalog: Study of relativistic jets in blazar objets (Keenan+, 2021)

In this paper, our aim is to re-examine blazar phenomenology and in particular the evidence for a dichotomy in the jet population and its link to accretion. The general approach we have taken in this study is similar to M11, in that our aim is to collect the largest possible sample of well-characterized jet SEDs, in order to get the most complete picture of the phenomenology of the population.

The initial sample of jetted AGN was compiled from the catalogues of jetted sources listed in table1.dat where we give the catalogue informations such as the total number of sources in that sample and the total from that sample included in our 'well-sampled' (TEX/UEX) catalogue. The total sample comprises 6856 sources after accounting for duplicates. Many sources in this list have very poorly sampled SEDs, often with little to no data beyond the radio. We have attempted to gather as much archival photometric and/or imaging data as possible at all wavelengths for this initial sample, and have also conducted observing campaigns in the radio and sub-mm in order to maximize the subset of the sample with well-sampled SEDs.

These observing campaigns (VLA and ALMA observations respectively table3.dat and table4.dat) complete published data source from NED and other surveys (i.e table 2 section 2.2.1). We have reduced and analysed (throught gaussian fits via CASA photometry package) 434 archival observations from the pre-upgrade Very Large Array (VLA) and 26 observations from the upgraded Karl G. Jansky Very Large Array (JVLA). We analysed 116 archival observations from the Atacama Large Millimetre/submillimetre array (ALMA) for this project. We also analysed 16, 25, and 12 new ALMA observations from our projects (also reduced with CASA photometry package).

Hereafter, we analysed SEDs with fitting functions of our sample to study the jet power of blazars by calculating frequencies and luminoties of lobes, cores and synchrotrons peaks. (i.e more details in sections 2.3 Jet power and 2.4 SED fitting). Consequently, from the initial sample of nearly 7000 sources, we have selected those where the full SED had sufficient spectral coverage to reliably fit the synchrotron peak and return a value for the peak frequency and luminosity. All SEDs were assessed visually for goodness of fit, without any a priori knowledge about their identity or type, simply based on being well-fit with an appropriate amount of spectral coverage, following the same procedure as in Meyer et al. (2011ApJ...740...98M, Cat. J/ApJ/740/98).

Generally, those that were eliminated lacked coverage over significant portions of the spectrum (e.g. no optical and/or X-ray) or could be reasonably fit by two or more very different SED shapes (often in these cases the X-ray spectral index is unknown - see Appendix section).

Remained after assessing the reliability of the broad-band SED fit. Of these, 1045 sources have estimates of the extended radio luminosity, and we call this sample the 'Trusted Extended' (TEX) sample. Additionally, another 1079 sources with good broad-band SEDs only have upper limits on Lexti (lobes luminosity). We call this the 'Unknown Extended' (UEX) sample as in Meyer et al. (2011ApJ...740...98M, Cat. J/ApJ/740/98). We regroup radio and broad-band properties of TEX in table6.dat and table7.dat and synthesize those for UEX in tableb1.dat, (More details on tables contains in section 2.5, 2.7 and 2.8).

(6 data files).