J/A+A/686/A169 Position angle for the FinAGN sample (Zheng+ 2024)
Alignments in the orientation of radio jets from AGN and their host galaxies.
Zheng X., Zhang Y., Rottgering H.
<Astron. Astrophys. 686, A169 (2024)>
=2024A&A...686A.169Z 2024A&A...686A.169Z (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Positional data ; Cross identifications ;
Morphology ; Radio sources
Keywords: galaxies: active - galaxies: jets - galaxies: nuclei -
galaxies: supermassive black hole - radio continuum: galaxies
Abstract:
It is well established that AGNs play an important role in the
evolution of galaxies. These AGNs can be linked to the accretion
processes onto massive black holes and past merger events in their
host galaxies, which may lead to different alignments of the jets with
respect to the host galaxies. This paper presents a study of the PA
differences between radio and optical images of radio AGNs based on
the LoTSS DR2, the FIRST, the DESI Legacy Imaging Surveys and the
SDSS. We assessed PA measurement biases in the data and classified the
radio AGNs based on the radio luminosity and infrared colour from the
WISE. This resulted in the largest yet published sample of 3682 radio
AGNs with reliable radio and optical PA measurements. The PA
difference (dPA) distributions for the radio AGN sample show a
prominent minor-axis alignment tendency. Based on some simple
assumptions, we simulated the projection effect to estimate the
intrinsic jet-galaxy alignment. The observed dPA distribution can be
well described by a two-component jet-alignment model in which one
component is more aligned with the minor axis of the host galaxy than
the other. The fitting results indicate that the jet alignment is
dependent on radio luminosity and the shape of the host galaxies, with
the jets being more likely to be aligned with the minor axis of the
galaxy for lower radio luminosity and for optically more elongated
radio AGNs. The minor-axis alignment of the entire sample may suggest
a coherent accretion model present in most AGN host galaxies, while a
considerable number of luminous radio-AGN with massive host galaxies
might have undergone an accretion according to the chaotic model or
past merger events.
Description:
Basic parameters and cross-IDs for the 3682 sources in the FinAGN
sample defined in Zheng+2024. For each source, the radio and optical
positional angle and their differences, the redshift, stellar mass,
radio luminosity, size and the identifications in the DESI Legacy
Surveys and SDSS (if exists) are given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 142 3682 Basic information for the FinAGN
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See also:
VII/292 : DESI Legacy Imaging Surveys DR8 photometric redshifts
(Duncan, 2022)
J/A+A/659/A1 : LOFAR Two-metre Sky Survey (LoTSS) DR2 (Shimwell+, 2022)
J/A+A/678/A151 : LoTSS DR2 optical IDs (Hardcastle+, 2023)
J/A+A/672/A163 : Properties of the 2060 giant radio galaxies (Oei+, 2023)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 24 A24 --- Source Unique ID for radio sources from the LoTSS
DR2, ILT JHHMMSS.ss+DDMMSS.s or
SDSS JHHMMSS.ss+DDMMSS.s. Sources without a
LoTSS DR2 ID are named based on the
sky coordinates in the SDSS.
26- 41 I16 --- LS ? Unique ID in the Legacy Surveys (1)
43- 47 I5 --- Plate ?=-1 SDSS plate ID if a SDSS counterpart
is present
49- 53 I5 --- MJD ?=-1 SDSS MJD ID. if a SDSS counterpart
is present
55- 57 I3 --- Fiber ?=-1 SDSS Fiber ID if a SDSS counterpart
is present
59- 66 F8.4 deg RAdeg Right ascension (J2000) of the optical
counterpart
68- 75 F8.4 deg DEdeg Declination (J2000) of the optical
counterpart
77- 80 F4.2 --- z Best redshift measurement
82- 87 A6 --- r_z Source of the redshift (2)
89- 93 F5.1 deg PAradio Position angle of the radio source,
defined from north to east
95- 99 F5.1 deg PAopt Position angle of the optical source,
defined from north to east
101-104 F4.1 deg dPA Radio-optical misalignment angle
106-110 F5.2 [Msun] logM Stellar mass of the galaxy (3)
112-116 F5.2 [W/Hz] logL150 150MHz luminosity estimated in this work
118-121 F4.2 --- b/a Opitical axis ratio (4)
123-128 F6.1 arcsec AngSize Projected largest angular size of the radio
source
130-136 F7.2 kpc Size Projected linear size of the radio source.
138-142 A5 --- CatSource Source catalogue of which the radio source
is from (5)
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Note (1): The LS id is different from the 'Legacy_ID' in the LoTSS DR2
VAC (Hardcastle et al., 2023A&A...678A.151H 2023A&A...678A.151H, Cat. J/A+A/678/A151),
but the same as in the Legacy Surveys.
Note (2): Source of the redshift as follows:
SDSS = taken from the SDSS
DESI = taken from the DESI spectroscopic survey
HETDEX = from the HETDEX
Phot = it is a photo-z from Duncan (2022MNRAS.512.3662D 2022MNRAS.512.3662D, Cat. VII/292)
Note (3): If the source is in the FIRSTAGN sample, the stellar mass is based on
the MPA- JHU results, else estimated from infrared luminosity as in
Wen et al. (2013MNRAS.433.2946W 2013MNRAS.433.2946W).
Note (4): If the source is in the FIRSTAGN sample, it is 'deVAB_r' in the SDSS,
else estimated from the Legacy Surveys.
Note (5): Source catalogue of which the radio source is from as follows:
LoTSS = from the LoTSS DR2 VAC,
FIRST = from FIRST
GRG = from Oei et al. (2023A&A...672A.163O 2023A&A...672A.163O, Cat. J/A+A/672/A163)
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Acknowledgements:
Xuechen Zheng, zhengxc2022(at)outlook.com
References:
Condon et al., 1998AJ....115.1693C 1998AJ....115.1693C, Cat. VIII/65
Dey et al., 2019AJ....157..168D 2019AJ....157..168D
Duncan, 2022MNRAS.512.3662D 2022MNRAS.512.3662D, Cat. VII/292
Hardcastle et al., 2023A&A...678A.151H 2023A&A...678A.151H, Cat. J/A+A/678/A151
Helfand et al., 2015ApJ...801...26H 2015ApJ...801...26H, Cat. VIII/92
Oei et al., 2023A&A...672A.163O 2023A&A...672A.163O, Cat. J/A+A/672/A163
Shimwell et al., 2022A&A...659A...1S 2022A&A...659A...1S, Cat. J/A+A/659/A1
Wen et al., 2013MNRAS.433.2946W 2013MNRAS.433.2946W,
York et al., 2000AJ....120.1579Y 2000AJ....120.1579Y
(End) Xuechen Zheng [SHAO], Patricia Vannier [CDS] 07-Mar-2024