Erratum: Constraints on dark photons and axionlike particles from the SuperCDMS Soudan experiment [Phys. Rev. D 101, 052008 (2020)]

Figure 1

Corrected calculated rates from combining data from the CDMSlite runs (light red dotted line), the iZIP detectors (dark red dashed line), and all datasets (black solid line). The shaded region around each line corresponds to the uncertainty on the rate limits. The elevation in the limits near 10 keV, 1 keV, 160 eV and in iZIP data around 9 keV results from the higher measured rates due to the Ge K-, L-, and M-captures and the K-capture of ${}^{65}\mathrm{Zn}$, respectively.

Figure 2

Corrected SuperCDMS Soudan upper limit (solid black) with uncertainty band (shaded gray) on the axioelectric coupling. Also shown are limits set by other direct-detection experiments including: CDMS II [1], CoGeNT [2], EDELWEISS-III [3], LUX [4], PandaX-II [5], XENON100 [6], XENON1T [7], and XMASS [8]. The shaded regions are excluded by the observed cooling of red giant (RG) [9, 10] and white dwarf (WD) stars [10, 11].

Figure 3

Corrected SuperCDMS Soudan upper limit (solid black) with uncertainty band (shaded grey) on the dark photon’s kinetic mixing. Also shown are limits set by other direct-detection experiments including DAMIC [12], EDELWEISS-III [3], SENSEI [13], the SuperCDMS HVeV device [14], An et al.’s analysis of XENON10 and XENON100 [15], and Hochberg et al.’s analysis of XENON100 [16], XENON1T [7], and XMASS [8]. The shaded regions show limits set from anomalous energy loss mechanisms in the Sun, horizontal branch stars (HB), and red giants (RG) from Ref. [15].