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Table 1.

Companions detected around PDS 456.

Src RA Dec D(kpc) z tracers
(1) (2) (3) (4) (5) (6)
K1 262.0818 −14.26599 9 0.1847 (a) Continuum K-band, Emission line CO(3–2), Absorption lines NaID
K2 262.0820 −14.26629 10 0.1845 (a) Continuum K-band, Emission line CO(3–2), Absorption lines NaID
K3 262.0821 −14.26640 11 0.1837 (a) Continuum K-band, Emission line CO(3–2), Absorption lines NaID
M1 262.0826 −14.2665 11 0.1847 Rest-frame optical emission lines and continuum in MUSE
M2 262.0809 −14.2666 21 0.1829/0.1836 (b) Emission line CO(3–2), rest-frame optical emission lines and continuum in MUSE
M3 262.0802 −14.2679 38 0.1838 Rest-frame optical emission lines and continuum in MUSE
M4 262.0802 −14.2653 25 0.1843 Rest-frame optical emission lines and continuum in MUSE
M5 262.0800 −14.2647 28 0.1840 Rest-frame optical emission lines and continuum in MUSE

Notes. Column (1): source name; Cols. (2) and (3): coordinates in degrees; Cols. (4) and (5): projected distances in kpc from PDS 456 and redshift, respectively; Col. (6): tracers, such as continuous lines or bands, employed to identify the redshift of the sources. The sources were detected with ALMA observations in B19, with the Near-Infrared Camera on the W. M. Keck Telescope in Yun et al. (2004), and with the IFS MUSE-WFM data in this work.

(a)

The redshift was obtained by fitting the NaID absorption feature.

(b)

The first (second) value indicates the CO (1–0) (Hα) based redshift.

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