The Impact of Polarized Extragalactic Radio Sources on the Detection of CMB Anisotropies in Polarization

Table 5

Expected total numbers of ERS with polarized intensity ≥𝑃_lim over the full sky at Planck frequencies. For each Planck channel, the minimum and maximum values here indicated refer to our predictions calculated by the more “optimistic” and by the more “conservative” cases previously discussed (see Table 4).

𝑃lim	𝜈 [GHz]
[mJY]	30	44	70	100	143	217	353
50	107–164	91–140	98–151	83–129	71–109	59–89	47–70
80	49–77	42–66	47–74	41–64	35–55	30–46	25–37
100	34–53	29–46	33–52	28–45	25–39	21–33	18–27
200	10–16	9–14	10–16	9–15	8–13	7–12	6–10
300	5–7	4–7	5–8	4–7	4–7	4–6	3–5
400	3-4	2–4	3–5	3-4	2–4	2–4	2-3
WMAP1	8	6	4

1Number of polarized ERS detected in the WMAP 5 yr data at |𝑏|>5^∘ by [55] at 33, 41 and 61 GHz (𝑃_lim≈300mJy).