The X-ray statistical properties of dust-obscured galaxies detected by eROSITA

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Volume 702 (October 2025)

A&A, 702 (2025) A34

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Table C.2.

Upper limits of L_6 μm.

	Condition	Criteria		Upper Limit Flag	# eFEDS-DOGs
(1)	3 band detected			No	44
(2)	Only W2 band undetected	& (1 + z)×λ_6μm < λ_W3	& $f_{W 2}^{Estimated} < f_{W 2}^{limit}$ $f^{\mathrm{Estimated}}_{W2} < f^{\mathrm{limit}}_{W2}$	No	1
(3)	Only W3 band undetected	& $f_{W 3}^{Estimated} < f_{W 3}^{limit}$ $f^{\mathrm{Estimated}}_{W3} < f^{\mathrm{limit}}_{W3}$		No	3
(4)	Only W3 band undetected	& $f_{W 3}^{limit} < f_{W 3}^{Estimated}$ $f^{\mathrm{limit}}_{W3} < f^{\mathrm{Estimated}}_{W3}$		Yes	15
(5)	W2 & W3 bands undetected			Yes	2

Total					65

Condition: Statuses of three MIR bands, Criteria: Definitions and explanations for the terms used in the table, Upper Limit flag: We attached/did not attach upper limit flags if objects have these Condition, # eFEDS-DOGs: Number of eFEDS-DOGs classified under these Condition. λ_W3, λ_6 μm, $f_{W 2}^{Estimated}$ $f^{\mathrm{Estimated}}_{W2}$ , $f_{W 2}^{limit}$ $f^{\mathrm{limit}}_{W2}$ , $f_{W 3}^{Estimated}$ $f^{\mathrm{Estimated}}_{W3}$ , and $f_{W 3}^{limit}$ $f^{\mathrm{limit}}_{W3}$ denote W3 band wavelength, 6 μm, estimated flux at W2 band, W2 band limiting flux, estimated flux at W3 band, and W3 band limiting flux, respectively. Each estimated flux is calculated as follows:

(1): Best-fit function from MIR 3 band fitting (see Section 2.2).

(2): Interpolated function from W3 and W4 bands data.

(3): Interpolated or extrapolated function from W2 and W4 bands data.

(4): Interpolated function from W2, W3, and W4 bands data.

(5): Interpolated function from W2, W3, and W4 bands data.

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