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tokens: Megeath et al. 2012 ) and included in the Herschel Orion protostar survey (HOPS; Furlan et al. 2016 ) as source 383. The submillimeter to bolometric luminosity ratio of HOPS 383 , 1.4% ( Safron et al. 2015 ) well surpasses the (0.5%) threshold for bona fide Class 0 designation ( André et al. 1993 , 2000 ). Notably, HOPS 383 is the first Class 0 protostar known to have undergone a mass-accretion-driven eruption ( Safron et al. 2015 ), which peaked by 2008 and ended by 2017 September (Appendix B ). 2. Observations We observed HOPS 383 three times with the Chandra X-ray Observatory ( Weisskopf et al. 2002 ) from 2017 December 13 to 14 with simultaneous near-infrared imaging on 2017 December 14 using the 4.1 m Southern Astrophysical Research (SOAR) telescope ( Krabbendam et al. 2004 ) in Chile. We used Chandra ’s Advanced CCD Imaging Spectrometer (ACIS-I) in the very faint mode with a frame time of 3.141 s (Appendix C.1 ). Chandra ACIS-I has on-axis a full-width half-maximum (FWHM) angular resolution of and a FWHM spectral resolution of 261 eV at 6.4 keV. Data reduction is described in Appendix C.2 . The SOAR Spartan infrared camera ( Loh et al. 2012 ) is composed of 4 CCDs of 2048 × 2048 pixels. We selected the wide-field mode with a single-detector field-of-view of (i.e., edge-to-edge) and a pixel scale of with the K -band and H 2 narrow-band filters. We used a five-point dithering pattern where, in the first exposure, HOPS 383 was put near the center of the northeastern detector (det3), which was then moved by 30′′ from its initial position sequentially toward the south, north, west, and east in the four other exposures. This sequence was repeated until the requested exposure was achieved (Appendix D.1 ). Data reduction is described in Appendix D.2 . 3. Near-infrared results The near-infrared nebulosity that was prominent during the outburst ( Safron et al. 2015 ) is not detected in our SOAR K -band image (Fig. 1 a), indeed, it vanished by 2015 December 30 ( Fischer Hillenbrand 2017 ). The H 2 -narrow filter image shows an emission knot of shocked molecular hydrogen at ∼15′′ southeast from the mid-infrared location of HOPS 383. We identify this H 2 source with the H 2 emission knot SMZ 1-2B ( Stanke et al. 2002 ) that was observed on 1997 September 13, yielding a proper motion of southeast in 20.25 yr (Fig. 1 b). The corresponding velocity is ∼(95 ± 53)×(sin i /sin69.5°) −1 × ( d /420 pc) km s −1 , where d is the distance to HOPS 383 and i is the inclination angle (90° corresponds to an edge-on view; Table 1 of Furlan et al. 2016 ). This is typical of the velocity values observed in the outflows from Class 0 protostars ( Bontemps et al. 1996 ; Reipurth Bally 2001 ). Assuming a constant velocity, the angular distance of ∼16′′ between HOPS 383 and this emission knot corresponds to a kinematical timescale of ∼180 ± 100 yr. The proper motion direction is consistent with the orientation of the outburst nebula, the 12 CO blueshifted outflow (