FRIICAT: A FIRST catalog of FR II radio galaxies
Aims. We built a catalog of 122 FR II radio galaxies, called FRIICAT, selected from a published sample obtained by combining observations from the NVSS, FIRST, and SDSS surveys. The catalog includes sources with redshift ≤ 0.15, an edge-brightened radio morphology, and those with at least one of the...
Saved in:
Published in | Astronomy and astrophysics (Berlin) Vol. 601 |
---|---|
Main Authors | , , |
Format | Journal Article |
Language | English |
Published |
Heidelberg
EDP Sciences
01.05.2017
|
Subjects | |
Online Access | Get full text |
Cover
Loading…
Summary: | Aims. We built a catalog of 122 FR II radio galaxies, called FRIICAT, selected from a published sample obtained by combining observations from the NVSS, FIRST, and SDSS surveys. The catalog includes sources with redshift ≤ 0.15, an edge-brightened radio morphology, and those with at least one of the emission peaks located at radius r larger than 30 kpc from the center of the host. Methods. The radio luminosity at 1.4 GHz of the FRIICAT sources covers the range L1.4 ~ 1039.5−1042.5erg s-1. The FRIICAT catalog has 90% of low and 10% of high excitation galaxies (LEGs and HEGs), respectively. The properties of these two classes are significantly different. The FRIICAT LEGs are mostly luminous (−20 ≳ Mr ≳ −24), red early-type galaxies with black hole masses in the range 108 ≲ MBH ≲ 109M⊙; they are essentially indistinguishable from the FR Is belonging to the FRICAT. The HEG FR IIs are associated with optically bluer and mid-IR redder hosts than the LEG FR IIs and to galaxies and black holes that are smaller, on average, by a factor ~2. Results. FR IIs have a factor ~3 higher average radio luminosity than FR Is. Nonetheless, most (~ 90%) of the selected FR IIs have a radio power that is lower, by as much as a factor of ~100, than the transition value between FR Is and FR IIs found in the 3C sample. The correspondence between the morphological classification of FR I and FR II and the separation in radio power disappears when including sources selected at low radio flux thresholds, which is in line with previous results. In conclusion, a radio source produced by a low power jet can be edge brightened or edge darkened, and the outcome is not related to differences in the optical properties of the host galaxy. |
---|---|
Bibliography: | dkey:10.1051/0004-6361/201630247 istex:124AC209B736E1938F9EFA345D53A7E1C5C30A03 Table 1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A81 bibcode:2017A%26A...601A..81C publisher-ID:aa30247-16 e-mail: capetti@oato.inaf.it ark:/67375/80W-CVRKJ5B2-2 |
ISSN: | 0004-6361 1432-0746 |
DOI: | 10.1051/0004-6361/201630247 |