<figure><img src="image_35.png" /><figcaption>**Figure 32.** Zoom in (3300–5300 Å) of the prominent AGN spectral lines in Figure 31 of the spectroscopically confirmed NL AGN, Nu-cQSO, and Nu-rQSO subdivided into low (light green, light blue, and peach, respectively) and high (dark green, dark blue, and red, respectively) luminosity bins. The composite X-Shooter spectra of luminosity–redshift matched SDSS rQSOs and cQSOs (Fawcett et al. 2022) are plotted in red and blue dotted lines, and composite spectra of SDSS Type 2 QSOs (Yuan et al. 2016) as a purple dotted line for comparison.</figcaption></figure>

≈62 Ms. Due to an increase in the fraction of GO observations over the NSS40 catalog, the areal coverage, integrated exposure, number of fields, and number of sources in the NSS80 are a factor ≈3 larger than those presented in Lansbury et al. (2017b). Furthermore, we have characterized the NuSTAR-detected AGNs in terms of their X-ray, optical, and IR properties. Below, we summarize the main results:

1. Overall, we detect 1488 sources which are significant post-deblending (i.e., after accounting for contamination of the photon counts from nearby sources). To enable easy and efficient use of the NSS80, 214 NuSTAR sources residing in highly extended optical galaxies and galaxy clusters are placed in a secondary catalog, available in Appendix B, to complement the
primary catalog, which constitutes 1274 X-ray sources (Appendix A), the majority of which are dominated by AGNs in fainter field galaxies. Of these, 412 are independently detected in the hard (8–24 keV) energy band; see Section 2.3.

2. Key improvements made in the construction of the NSS80 catalog over those adopted for the NSS40 catalog include (i) mosaicking of overlapping fields from different observational programs to increase the sensitivity, and (ii) masking of fields with large optical/IR hosts post processing to construct a secondary catalog of sources which previously were excluded altogether. Overall, we find 91% of NSS40 sources are retained in NSS80, while 36 NSS40 sources are undetected in NSS80. For the majority of these undetected sources, the deeper data have improved the false-probability estimates and, consequently, eliminate low-significance detections.

3. The full-band (3–24 keV) fluxes cover a range of $f_{3-24 \text{ keV}} \approx 10^{-14}-10^{-11} \text{ erg s}^{-1} \text{ cm}^{-2}$, with a median value of $\langle f_{3-24 \text{ keV}} \rangle = 9.82 \times 10^{-14} \text{ erg s}^{-1} \text{ cm}^{-2}$; see Section 4.1.1. The NuSTAR serendipitous survey has the largest areal coverage at all fluxes compared to the NuSTAR deep-field surveys in well-studied fields (e.g., COSMOS, ECDFS, EGS, GOODS-N, and UDS), reaching similar flux depths. Consequently, the combination of NSS80 with the deep-field surveys allows for a factor ≈2 improvement in analyses of the faint end of the hard X-ray source population compared to that from just the deep-field surveys; see Section 2.2. Furthermore, in Section 4.1.3 we show that NSS80 reaches ≈2 orders of magnitude fainter than the Swift-BAT all-sky survey.

4. A large range in the observed band ratios of the NSS80 spectroscopically confirmed AGNs is seen at 3–24 keV (Section 4.1.2). This implies a range of observed photon indices going from very soft $\Gamma_{\text{eff}} \approx 3$ to very hard $\Gamma_{\text{eff}} \approx 0$. Contrary to that previously found for lower-energy X-ray bands, our results show no evidence for an anticorrelation between band ratio and X-ray count rate.

5. To study the multiwavelength properties of the NuSTAR serendipitous sources, we required lower-energy X-ray (<10 keV) counterparts with higher positional accuracies to reliably match to optical and IR counterparts. To search for lower-energy X-ray counterparts, we utilized Chandra (CSC2), XMM-Newton (4XMM-DR10/s), and Swift-XRT (2SXPS). In total, we identified a lower-energy X-ray counterpart for 76% (964/1274) of the primary NSS80 catalog detected in surveys or archival data from the four lower-energy X-ray catalogs. The remaining 310 NSS80 sources lack lower-energy X-ray counterparts, which can be attributed to either insufficient or zero lower-energy X-ray coverage or, in the minority of cases, a false NuSTAR detection (e.g., sources with detection probabilities close to the threshold; $\log(P_{\text{false,min}}) \approx -6$). We find that the lower-energy X-ray counterpart fluxes are generally in agreement with the NuSTAR fluxes for the 3–8 keV (soft) energy band. A maximum variation of a factor of ≈5 between the lower-energy X-ray and NuSTAR flux observations is identified, which can be attributed to source variability detected in the noncontemporaneous X-ray observations and Eddington bias; see Section 4.1. This variability can have two origins: either a change in intrinsic AGN

luminosity or a change in the line-of-sight column density due to the nonuniform distribution of the obscuring material surrounding the accreting supermassive black hole.

6. In NSS40 a relatively simple closest-neighbor approach was used to identify multiwavelength counterparts for follow-up spectroscopy. In the NSS80 catalog, however, we adopted a more sophisticated probabilistic approach with NWAY to identify IR (CatWISE20) and optical (PS1-DR2) counterparts; see Section 3.2. The bulk of the NSS80 sources (95%) have at least one NWAY match with a match probability >10%, 74% of which coincide with a lower-energy X-ray counterpart, and the remaining 26% have NuSTAR-only X-ray positions (due to insufficient or no lower-energy X-ray coverage). Overall, we find 953 high-probability CatWISE20/PS1 counterpart matches to the NSS80 sources, of which ~76% are at extragalactic latitudes $|b| > 20^{\circ}$.

7. Optical spectroscopic identifications (i.e., redshift measurements and source classifications) have successfully been obtained for 547 sources; see Section 3.3.3. An additional three sources have redshift estimates, but lack source classifications. We obtained spectroscopic identifications for the majority of sources (427) via our extensive campaign of ground-based spectroscopic follow-up, using a range of observatories at multiple geographic latitudes; see Section 3.3.2. We spectroscopically confirm 58 sources as Galactic objects. Of the 492 extragalactic sources (AGNs), 284 (57.7%) are classified as broad-line AGNs (BL), 194 (39.4%) are narrow-line sources (NL), 10 are galaxies (Gxy; absorption-line spectra), one is a galaxy cluster, and three are unclassified but have redshift measurements from the literature. Among these, there are three AGN pairs, of which one pair is a dual AGN system, two are AGN-galaxy pairs, and one a galaxy pair. For a further 43 sources a faint continuum (often red) is detected, lacking spectral features and, consequently, spectroscopic identifications. One of these sources is a BL Lac candidate, and another is a pair of (extremely faint) sources of unknown type. The remaining one source is a hotspot of 4C 74.26 (radio quasar), which was targeted as the primary NuSTAR science target. While similar numbers of NLs and BLs are identified at lower redshifts ($z \lesssim 1$), there is a bias against detections of high-redshift NLs that are optically fainter, and against the detection of highly obscured AGNs; see Section 4.1.3.

8. The NSS80 AGNs have redshifts covering a wide range, from 0.012 to 3.43, with a median redshift of $\langle z \rangle = 0.56$; see Section 4.1.3. The rest-frame 10–40 keV luminosities also span a wide range of $L_{10-40 \text{ keV}} \approx 10^{42-46} \text{ erg s}^{-1}$, with a median value of $\langle L_{10-40 \text{ keV}} \rangle = 1.2 \times 10^{44} \text{ erg s}^{-1}$. Previous X-ray missions with sensitivity at >10 keV were able to sample the AGN population below the knee of the X-ray luminosity function ($L_*$) for redshifts up to $z \approx 0.05$, and NuSTAR extends this to $z \approx 1$. Using the NuSTAR band ratio, we identify 22 CT candidate sources: seven are identified in the NSS40 catalog and 15 are newly identified sources with the post-NSS40 observations; see Section 4.1.2.

9. We use the distribution of WISE W1–W2 and W2–W3 colors for the extragalactic NSS80 sources, since the
reprocessed emission from the AGNs' circumnuclear dust is distinguishable from starlight (which peaks in the FIR regime) at MIR wavelengths (predominantly for high-luminosity AGNs); see Section 4.2. We find that 95% of high-$L_X$ BL AGNs will successfully be selected using the AGN wedge, while NL AGNs have a significantly lower chance of being identified as AGNs based on their MIR colors alone. This is largely driven by the lower-luminosity objects with 10–40 keV luminosities below the X-ray quasar threshold. It is notable that a number of luminous NuSTAR-selected BL AGNs are not selected in the MIR—this appears to be driven by the intrinsic AGN properties. Furthermore, from the MIR colors, we can deduce that >90% of the MIR light in two-thirds of the objects come from an AGN, while approximately a third are host dominated.

10. Given that hard X-rays are largely unbiased against dust obscuration up to CT levels, NuSTAR facilitates the discovery of rare and extreme sources such as red quasars. We therefore explore the optical and IR properties of the NSS80 AGN sample, with particular focus on red quasars and the narrative that X-rays may be telling about this peculiar subpopulation of AGNs; see Section 4.3. Forty-two percent (106/251) of the BL AGNs with robust counterpart associations have red $g-i$ colors, half of which have luminosities exceeding the X-ray quasar threshold and therefore are potentially dust-reddened quasars. The remaining 145 BLs have $g-i$ colors consistent with the typical quasar population. Furthermore, 92% of the NLs appear red in their optical colors; however, the majority are low-luminosity objects with $L_{10-40\,\text{keV}} < 10^{44}\,\text{erg s}^{-1}$ and therefore will have host-galaxy-dominated emission. Altogether, the NSS80 AGNs are typically 0.3 dex less luminous than SDSS quasars, with a median bolometric luminosity of $\langle L_{\text{bol},X} \rangle = 5.93 \times 10^4\,\text{erg s}^{-1}$ at the median BL AGN redshift of $\langle z \rangle \approx 0.8$.

11. Finally, we present optical spectra composites to study the spectral properties of the NSS80 AGNs to investigate the driving force behind the colors of the NSS80 red quasars; see Section 4.4. Overall, for all spectral types the host-galaxy features are more prominent in the low-$L_X$ when compared to the high-$L_X$ systems: These signatures are enhanced emission at red wavelengths and host-galaxy absorption features, although these are weak in some of the composites. This is consistent with basic expectations for a decreasing AGN contribution relative to the host-galaxy emission. Hence, our spectroscopic analysis indicates that reddening from the presence of a host galaxy can have a large contribution to the optical colors in the hard-X-ray-selected population of lower-luminosity quasars.

Our future work will focus on further follow-up studies of the current NSS80 sources, aiming to complete the spectroscopic follow-up of the catalog and to obtain detailed analysis of sources with >8 keV detections, which are unique to NuSTAR.

The NSS80 is a valuable legacy of the NuSTAR observatory and provides a powerful sample for future studies of the hard X-ray emitting population. Our total sample size (1488 sources) is relatively modest compared to the samples of hundreds of thousands of sources compiled with XMM-Newton, Chandra,

or Swift (e.g., Webb et al. 2020; Evans et al. 2019, 2020)—achieved thanks to the larger fields of view, higher sensitivities, and longer lifetimes of these observatories compared to NuSTAR—or the much larger samples (at soft X-ray energies) that are now being provided by dedicated surveys with eROSITA (Merloni et al. 2012; Predehl et al. 2021; Brunner et al. 2022). In contrast to these prior studies, we have been careful to ensure our sample consists only of truly serendipitous detections and excludes any sources associated with the targets of the observations, which is vital for carrying out scientific studies that require an unbiased sampling of the population (see also Delaney et al. 2023). Our sample remains unique in accessing faint sources at hard ($\gtrsim$8 keV) X-ray energies with a high degree of spectroscopic completeness, providing important constraints on the obscured AGN population outside the local Universe.

## Acknowledgments

This paper is jointly led by L.K. and C.L.G.: the original draft was primarily produced by L.K., and formed a major component of her PhD thesis, and the modifications made to the draft following an extensive referee report were carried out by C.L.G.. We acknowledge financial support from the following: a Faculty of Science Durham Doctoral Scholarship (L.K.), a European Southern Observatory (ESO) postdoctoral research fellowship (G.B.L. and M.H.), the Science and Technology Facilities Council (STFC; D.M.A. and D.J.R. through grant code ST/P000541/1; D.M.A. and C.L.G. through grant codes ST/T000244/1 and ST/X001075/1), and an STFC Ernest Rutherford Fellowship (J.A. through grant code ST/P004172/1). The work of D.S. and T.C. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (grant No. 80NM0018D0004). F.E. B. acknowledges support from ANID-Chile BASAL AFB-170002, ACE210002, and FB210003, FONDECYT Regular 1200495 and 1190818, and Millennium Science Initiative Program - ICN12_009. P.G.B. acknowledges financial support from the Czech Science Foundation project No. 22-22643S. W. N.B. acknowledges financial support from the V.M. Willaman Endowment. V.A.F. acknowledges funding from a United Kingdom Research and Innovation grant (code: MR/ V022830/1). E.S.K. acknowledges financial support from the Centre National d'Etudes Spatiales (CNES). S.M. acknowledges funding from the the INAF "Progetti di Ricerca di Rilevante Interesse Nazionale" (PRIN), Bando 2019 (project: "Piercing through the clouds: a multiwavelength study of obscured accretion in nearby supermassive black holes"). G.N. acknowledges funding support from the Natural Sciences and Engineering Research Council (NSERC) of Canada through a Discovery Grant and Discovery Accelerator Supplement, and from the Canadian Space Agency through grant No. 18JWST-GTO1. C.R. acknowledges support from Fondecyt Regular grant No. 1230345 and ANID BASAL project FB210003. E.R. C. and P.V. acknowledges the support of the South African National Research Foundation. E.T. acknowledges support from FONDECYT Regular 1190818 and 1200495, ANID grants CATA-Basal AFB-170002, ACE210002, and FB210003, and Millennium Nucleus NCN19_058. C.M.U. would like to acknowledge support from the National Aeronautics and Space Administration via ADAP grant No. 80NSSC18K0418.
We extend gratitude to Sam Tweety Anthony, Subhash Bose, Tea Freedman-Susskind, Tyler George, Elena González Egea, Feiyang Liu, Dan MacMillan, Jeff Maggio, Adric Riedel, Michael Rivkin, Manika Sidhu, Jamie Soon, Thomas Venville, Yerong Xu, and Emily Zhang for their support during the ground-based follow-up observations. We thank Victoria Fawcett for her valuable contribution by producing the composite spectra presented in Section 4.4.

This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).

*Facilities:* CXO, VLT:Antu (FORS2), Keck:I, NuSTAR, Hale, SALT, Sloan, Swift, WISE, XMM.

Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under programs 2017-1-SCI-053, 2017-2-SCI-037, and 2018-2-MLT-006 (PI: L. Klindt). The Wide-field Infrared Survey Explorer (WISE) is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This research uses services or data provided by the Astro Data Lab, which is part of the Community Science and Data Center (CSDC) program at NSF's National Optical-Infrared Astronomy Research

Laboratory. NOIRLab is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation.

*Software:* Astropy (Astropy Collaboration et al. 2013, 2018, 2022), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), and SciPy (Virtanen et al. 2020).

## Appendix A
### Description of the Primary NSS80 Source Catalog

The primary NuSTAR serendipitous survey source catalog, containing 1274 sources in total, is available as an electronic table on the NSS80 web page. Here we describe the columns of the catalog, which are summarized in Table 11.

*Column 1:* The unique source identification number, in order of increasing R.A.

*Column 2:* The unique NuSTAR source name, following the IAU-approved format: NuSTAR JHHMMSSDDDMM.m, where “m” is the truncated fraction of 1' for the arcseconds component of the decl.

*Column 3:* The unique NuSTAR field and source index.

*Column 4:* The unique L17 source identification number.

*Column 5:* The unique L17 NuSTAR field and source index.

*Columns 6, 7:* The NuSTAR R.A. and decl. coordinates (J2000), as described in Section 2.3. *Units:* degrees.

*Columns 8, 9:* The IAU 1958 Galactic latitude and longitude. *Units:* degrees.

*Columns 10–12:* A binary flag indicating whether the source is detected with a false probability lower than the threshold of $log(P_{\text{False}}) = -6$, for the soft (3–8 keV), hard (8–24 keV), and full (3–24 keV) bands. These three bands are abbreviated as SB, HB, and FB, respectively, throughout the source catalog.

*Columns 13–15:* The same as columns 10–12, after deblending has been performed to account for contamination of the source counts from very nearby sources (Section 2.3.2 of Mullaney et al. 2015). Deblending only affects a very small fraction of the overall sample (see, e.g., Section 2.4 in L17).

*Columns 16–18:* The logarithm of the false probabilities ($P_{\text{false}}$) of the NuSTAR-detected source, for the three standard energy bands.

*Columns 19:* The NuSTAR detection likelihood ($P_{\text{false,min}}$).

*Columns 20–22:* The same as columns 16–18, after deblending has been performed.

*Columns 23:* The same as column 19, after deblending has been performed.

*Column 24:* A binary flag indicating whether the NuSTAR-detected source remains significant after deblending, in at least one of the three standard energy bands.

*Columns 25–39:* Photometric quantities, calculated at the NuSTAR source coordinates, and using a source aperture of 30" radius (see Section 2.2). The values are non-aperture-corrected, i.e., they correspond to the 30" values, and have not been corrected to the full PSF values. We provide the total counts (i.e., all counts within the source aperture) and associated errors (84% confidence level, CL), the background counts scaled to the source aperture, and the net source counts (i.e., total minus background) and associated errors. For the net source counts, we give 90% CL upper limits for sources not detected in a given band. Throughout the table, upper limits are flagged with a –99 value in the error column.

*Columns 40–51:* The same as columns 25–39, after deblending has been performed.
<table><caption>**Table 11**

Column Descriptions for the Primary NSS80 Catalog</caption><thead><tr><th>Column Number</th><th>Column Name</th><th>Description</th></tr></thead><tbody><tr><td>1</td><td>ID</td><td>The unique source identification number, in order of increasing R.A.</td></tr><tr><td>2</td><td>NSS80_Name</td><td>The unique NuSTAR source name, following the IAU-approved format: NuSTAR JHHMMSSDDMM.m, where "m" is the truncated fraction of 1' for the arcseconds component of the decl.</td></tr><tr><td>3</td><td>Serendip</td><td>The unique NuSTAR field and source index.</td></tr><tr><td>4</td><td>IDL17</td><td>The unique L17 source identification number.</td></tr><tr><td>5</td><td>Serendip_L17</td><td>The unique L17 NuSTAR field and source index.</td></tr><tr><td>6, 7</td><td>RAJ2000,DECJ2000</td><td>The NuSTAR R.A. and decl. coordinates (J2000), as described in Section 2.3.</td></tr><tr><td>8, 9</td><td>Gal_lat, Gal_Long</td><td>IAU 1958 Galactic latitude and longitude.</td></tr><tr><td>10, 11, 12</td><td>SFlag,HFlag,HFlag</td><td>A binary flag indicating the energy bands for which the source is detected for the three standard NuSTAR energy bands.</td></tr><tr><td>13, 14, 15</td><td>SdbFlag,HdbFlag, FdbFlag</td><td>Same as columns 10–12, post-deblending.</td></tr><tr><td>16, 17, 18</td><td>logSP,logHP,logFP</td><td>The logarithm of the false probabilities for the three standard NuSTAR energy bands.</td></tr><tr><td>19</td><td>logMinP</td><td>The NuSTAR detection likelihood.</td></tr><tr><td>20, 21, 22</td><td>logSdbP,logHdbP, logFdbP</td><td>The same as columns 16–18, post-deblending.</td></tr><tr><td>23</td><td>logMindbP</td><td>The same as column 19, post-deblending.</td></tr><tr><td>24</td><td>dbFlag</td><td>A binary flag indicating whether the source is significant post-deblending, for at least one energy band.</td></tr><tr><td>25, 26</td><td>Scts_e_Scts</td><td>Total source count for the soft energy band and associated errors.</td></tr><tr><td>27</td><td>SBck</td><td>Background count for the soft energy band.</td></tr><tr><td>28, 29</td><td>SNet, e_SNet</td><td>Net source count for the soft energy band and associated errors.</td></tr><tr><td>30, 31</td><td>Hcts, e_Hcts</td><td>Total source count for the hard energy band and associated errors.</td></tr><tr><td>32</td><td>HBck</td><td>Background count for the hard energy band.</td></tr><tr><td>33, 34</td><td>HNet, e_HNet</td><td>Net source count for the hard energy band and associated errors.</td></tr><tr><td>35, 36</td><td>Fcts, e_Fcts</td><td>Total source count for the full energy band and associated errors.</td></tr><tr><td>37</td><td>FBck</td><td>Background count for the full energy band.</td></tr><tr><td>38, 39</td><td>FNet, e_FNet</td><td>Net source count for the full energy band and associated errors.</td></tr><tr><td>40</td><td>Sdbcts</td><td>Total source count for the soft energy band, post-deblending.</td></tr><tr><td>41</td><td>SdbBck</td><td>Background count for the soft energy band, post-deblending.</td></tr><tr><td>42, 43</td><td>SdbNet, e_SdbNet</td><td>Net source count for the soft energy band, post-deblending and associated errors.</td></tr><tr><td>44</td><td>Hdbcts</td><td>Total source count for the hard energy band, post-deblending.</td></tr><tr><td>45</td><td>HdbBck</td><td>Background count for the hard energy band, post-deblending.</td></tr><tr><td>46, 47</td><td>HdbNet, e_HdbNet</td><td>Net source count for the hard energy band, post-deblending and associated errors.</td></tr><tr><td>48</td><td>Fdbcts</td><td>Total source count for the full energy band, post-deblending.</td></tr><tr><td>49</td><td>FdbBck</td><td>Background count for the full energy band, post-deblending.</td></tr><tr><td>50, 51</td><td>FdbNet, e_FdbNet</td><td>Net source count for the full energy band, post-deblending and associated errors.</td></tr><tr><td>52, 53, 54</td><td>Sexp, Hexp, Fexp</td><td>Net vignetting-corrected exposure times at the source position, for the combined A + B data.</td></tr><tr><td>55, 56</td><td>SCR, eSCR</td><td>Total source count rate for the soft energy band and associated errors.</td></tr><tr><td>57</td><td>SCRBck</td><td>Background count rate for the soft energy band.</td></tr><tr><td>58, 59</td><td>SNetCR, e_SNetCR</td><td>Net source count rate for the soft energy band and associated errors.</td></tr><tr><td>60, 61</td><td>HCR, e_HCR</td><td>Total source count rate for the hard energy band and associated errors.</td></tr><tr><td>62</td><td>HCRBck</td><td>Background count rate for the hard energy band.</td></tr><tr><td>63, 64</td><td>HNetCR, e_HNetCR</td><td>Net source count rate for the hard energy band and associated errors.</td></tr><tr><td>65, 66</td><td>FCR, e_FCR</td><td>Total source count rate for the full energy band and associated errors.</td></tr><tr><td>67</td><td>FCRBck</td><td>Background count rate for the full energy band.</td></tr><tr><td>68, 69</td><td>FNetCR, e_FNetCR</td><td>Net source count rate for the full energy band and associated errors.</td></tr><tr><td>70, 71</td><td>SdbNetCR, e_SdbNetCR</td><td>Deblended net source count rate for the soft energy band and associated errors.</td></tr><tr><td>72, 73</td><td>HdbNetCR, e_HdbNetCR</td><td>Deblended net source count rate for the hard energy band and associated errors.</td></tr><tr><td>74, 75</td><td>FdbNetCR, e_FdbNetCR</td><td>Deblended net source count rate for the full energy band and associated errors.</td></tr><tr><td>76</td><td>H/S</td><td>Band ratio computed from using the NuSTAR hard and soft energy bands.</td></tr><tr><td>77</td><td>upH/S</td><td>Band ratio upper error.</td></tr><tr><td>78</td><td>lowH/S</td><td>Band ratio lower error.</td></tr><tr><td>79</td><td>gamma</td><td>Effective photon index.</td></tr><tr><td>80</td><td>upgamma</td><td>Effective photon index upper error.</td></tr><tr><td>81</td><td>lowgamma</td><td>Effective photon index lower error.</td></tr><tr><td>82, 83</td><td>SdbFlux, e_SdbFlux</td><td>Deblended fluxes in the soft energy band and associated errors.</td></tr><tr><td>84, 85</td><td>HdbFlux, e_HdbFlux</td><td>Deblended fluxes in the hard energy band and associated errors.</td></tr><tr><td>86, 87</td><td>FdbFlux, e_FdbFlux</td><td>Deblended fluxes in the full energy band and associated errors.</td></tr><tr><td>88</td><td>FLAG_softX_cov</td><td>Abbreviated code indicating the lower-energy X-ray coverage with Chandra, XMM-Newton, and/or Swift-XRT.</td></tr><tr><td>89</td><td>XOrig</td><td>Reference for the adopted lower-energy X-ray (Chandra, XMM-Newton, or Swift-XRT) counterpart.</td></tr><tr><td>90, 91</td><td>XRAdeg, XDEdeg</td><td>R.A. and decl. of the lower-energy X-ray counterpart.</td></tr><tr><td>92</td><td>e_Xdeg</td><td>Positional uncertainty of the lower-energy X-ray counterpart (where available, otherwise of the NuSTAR source) used for NWAY.</td></tr></tbody></table>
<table><caption>**Table 11**
(Continued)</caption><thead><tr><th>Column Number</th><th>Column Name</th><th>Description</th></tr></thead><tbody><tr><td>93</td><td>XOff_NuSTAR</td><td>Angular separation between the NuSTAR and lower-energy X-ray counterpart positions.</td></tr><tr><td>94</td><td>E_SoftX_KEV</td><td>Reference for the lower-energy X-ray flux used to compute the 3–8 keV fluxes (i.e., XFlux).</td></tr><tr><td>95, 96, 97</td><td>XFlux, XFlux_Lerr, XFlux_Uerr</td><td>3–8 keV (CSC2, 4XMM-DR10/s, or 2SXPS) flux of the lower-energy X-ray counterpart, with associated lower and upper errors.</td></tr><tr><td>98, 99, 100</td><td>TXFlux, TXFlux_Lerr, TXFlux_Uerr</td><td>Total 3–8 keV flux of all (CSC2, 4XMM-DR10/s, or 2SXPS) sources within 30" of the NuSTAR position, with associated lower and upper errors.</td></tr><tr><td>101</td><td>gal_ext_Av</td><td>Galactic extinction, A<sub>v</sub>.</td></tr><tr><td>102, 103, 104</td><td>gal_ext_g, gal_ext_r, gal_ext_i</td><td>Galactic line-of-sight absorption in the g, r, and i bands.</td></tr><tr><td>105, 106</td><td>Pbest_CatWISE, Pany_CatWISE</td><td>The NWAY best-match probability and probability that any of the CatWISE20 sources is the right counterpart.</td></tr><tr><td>107, 108</td><td>RA_CatWISE, DEC_CatWISE</td><td>R.A. and decl. of the “best” NWAY-identified CatWISE20 counterpart.</td></tr><tr><td>109</td><td>IROff_NuSTAR</td><td>Angular separation between the NWAY-matched WISE counterpart position and the NuSTAR position.</td></tr><tr><td>110</td><td>IROff_SoftX</td><td>Angular separation between the NWAY-matched WISE counterpart position and the adopted lower-energy X-ray counterpart.</td></tr><tr><td>111, 112</td><td>W1_CatWISE, e_W1_CatWISE</td><td>WISE W1 magnitude (3.4 µm), with associated errors.</td></tr><tr><td>113, 114</td><td>W2_CatWISE, e_W2_CatWISE</td><td>WISE W2 magnitude (4.6 µm), with associated errors.</td></tr><tr><td>115, 116</td><td>RA_AllWISE, DEC_AllWISE</td><td>R.A. and decl. of the closest AllWISE counterpart.</td></tr><tr><td>117, 118</td><td>W3_AllWISE, e_W3_AllWISE</td><td>WISE W3 magnitude (12 µm), with associated errors.</td></tr><tr><td>119, 120</td><td>W4_AllWISE, e_W4_AllWISE</td><td>WISE W4 magnitude (22 µm), with associated errors.</td></tr><tr><td>121, 122</td><td>Pbest_PS1, Pany_PS1</td><td>The NWAY best-match probability and probability that any of the PS1-DR2 sources is the right counterpart.</td></tr><tr><td>123, 124</td><td>RA_PS1, DEC_PS1</td><td>R.A. and decl. of the “best” NWAY-identified PS1-DR2 counterpart.</td></tr><tr><td>125</td><td>OOff_PS1_NuSTAR</td><td>Angular separation between the NWAY-matched PS1-DR2 counterpart position and the NuSTAR position.</td></tr><tr><td>126</td><td>OOff_PS1_SoftX</td><td>Angular separation between the NWAY-matched PS1-DR2 counterpart position and the adopted lower-energy X-ray position.</td></tr><tr><td>127</td><td>OOff_PS1_CatWISE</td><td>Angular separation between the NWAY-matched PS1-DR2 and CatWISE20 counterpart positions.</td></tr><tr><td>128, 129</td><td>gmag_PS1, e_gmag_PS1</td><td>g-band magnitude for the NWAY-identified PS1-DR2 counterpart, with associated errors.</td></tr><tr><td>130, 131</td><td>rmag_PS1, e_rmag_PS1</td><td>r-band magnitude for the NWAY-identified PS1-DR2 counterpart, with associated errors.</td></tr><tr><td>132, 133</td><td>imag_PS1, e_image_PS1</td><td>i-band magnitude for the NWAY-identified PS1-DR2 counterpart, with associated errors.</td></tr><tr><td>134</td><td>mag_type_PS1</td><td>Three letter code indicating the type of PS1 magnitude in each band: “K” (Kron), “P” (PSF), “A” (aperture), or “-” (unavailable).</td></tr><tr><td>135</td><td>NWAY_RFlag</td><td>A binary flag indicating the NWAY reliable sample following p<sub>Cat/PS,best</sub> > 0.4 and p<sub>Cat/PS,any</sub> > 0.5.</td></tr><tr><td>136</td><td>OOrig_cpart</td><td>Reference for the adopted optical counterpart, in order of preference: PS1-DR2, SDSS, NSC2, DES-DR2, or USNOB1.</td></tr><tr><td>137, 138</td><td>ORAdeg_cpart, ODEdeg_cpart</td><td>R.A. and decl. of the adopted optical counterpart.</td></tr><tr><td>139, 140</td><td>gmag_cpart, e_gmag_cpart</td><td>g-band magnitude for the adopted optical counterpart, with associated errors.</td></tr><tr><td>141, 142</td><td>rmag_cpart, e_rmag_cpart</td><td>r-band magnitude for the adopted optical counterpart, with associated errors.</td></tr><tr><td>143, 144</td><td>imag_cpart, e_image_cpart</td><td>i-band magnitude for the adopted optical counterpart, with associated errors.</td></tr><tr><td>145</td><td>mag_type_cpart</td><td>Three letter code indicating the type of PS1 magnitude in each band (if used for counterpart): “K” (Kron), “P” (PSF), “A” (aperture), or “-” (unavailable).</td></tr><tr><td>146</td><td>OOff_NuSTAR</td><td>Angular separation between the adopted optical counterpart position and the NuSTAR position.</td></tr><tr><td>147</td><td>OOff_SoftX</td><td>Angular separation between the adopted optical counterpart position and the best soft X-ray position.</td></tr><tr><td>148</td><td>OOff_CatWISE</td><td>Angular separation between the adopted optical counterpart position and the best CatWISE20 position.</td></tr><tr><td>149</td><td>MainCAT</td><td>Flag indicating sources which are included in the unique primary catalog.</td></tr><tr><td>150</td><td>SpecCAT</td><td>Flag indicating sources which are included in the spectroscopic catalog.</td></tr><tr><td>151, 152</td><td>RAdeg_spec, DEdeg_spec</td><td>R.A. and decl. of the spectroscopic target.</td></tr><tr><td>153</td><td>OOff_Spec_Cpart</td><td>Angular separation between the spectroscopic target and the adopted optical counterpart.</td></tr><tr><td>154</td><td>zspec</td><td>Spectroscopic redshift.</td></tr><tr><td>155</td><td>zQuality</td><td>Quality flag of the spectroscopic redshift measurement.</td></tr><tr><td>156, 157</td><td>Classification, Class_extra</td><td>Spectroscopic classification and additional source class information.</td></tr><tr><td>158, 159</td><td></td><td>A binary flag indicating a NWAY CatWISE20/PS1-DR2 match to the spectroscopic target.</td></tr></tbody></table>
<table><caption>**Table 11**
(Continued)</caption><thead><tr><th>Column Number</th><th>Column Name</th><th>Description</th></tr></thead><tbody><tr><td></td><td>NWAY_CatWISE,<br>NWAY_PS1</td><td></td></tr><tr><td>160</td><td>Cpart_RFlag</td><td>A flag indicating the reliability of the spectroscopic target as the correct counterpart.</td></tr><tr><td>161</td><td>SpecRef</td><td>Reference for the information used for the spectroscopic target.</td></tr><tr><td>162, 163</td><td>gmag_spec,e_gmag_spec</td><td>r-band magnitude for the spectroscopic target, with associated errors.</td></tr><tr><td>164, 165</td><td>rmag_spec,e_rmag_spec</td><td>r-band magnitude for the spectroscopic target, with associated errors.</td></tr><tr><td>166, 167</td><td>imag_spec,e_image_spec</td><td>r-band magnitude for the spectroscopic target, with associated errors.</td></tr><tr><td>168</td><td>L10_40keV</td><td>Non-absorption-corrected, rest-frame 10–40 keV luminosity.</td></tr><tr><td>169</td><td>PFlag</td><td>A binary flag indicating sources that show evidence for being associated with the primary science targets of their respective NuSTAR observations.</td></tr><tr><td>170</td><td>CTFlag</td><td>A binary flag indicating Compton-thick candidates.</td></tr></tbody></table>

(This table is available in its entirety in machine-readable form in the online article.)

**Columns 52–54:** The average net, vignetting-corrected exposure time at the source coordinates (columns 3 and 4), for each energy band. These correspond to the A + B data, so should be divided by 2 to obtain the average exposure per FPM. **Units:** seconds.

**Columns 55–69:** The non-aperture-corrected total, background, and net count rates (and associated errors; 84% CL) determined from the photometric values in columns 25–39, and the exposure times in columns 52–54. **Units:** s⁻¹.

**Columns 70–75:** The debленed net count rates and associated errors, determined from the photometric values in columns 40–51, and the exposure times in columns 52–54. **Units:** s⁻¹.

**Columns 76–78:** The NuSTAR band ratio (BR<sub>Nu</sub>) and associated errors. Upper limits, lower limits, and sources with no constraints are flagged with −99, −88, and −77 values, respectively, in the error columns.

**Columns 79–81:** The effective photon index (Γ<sub>eff</sub>) and associated errors, estimated from the band ratio values in columns 76–78.

**Columns 82–87:** The observed-frame fluxes and associated errors (84% CL) for the three standard energy bands, after deb blending has been performed. These are aperture-corrected values (i.e., they correspond to the full NuSTAR PSF), and are calculated from the count rates in columns 70–75 using the conversion factors listed in L17. **Units:** erg s⁻¹ cm⁻².

**Column 88:** An abbreviated code indicating the lower-energy (< 10 keV) X-ray coverage. “C,” “X,” and “S” indicate sources which have Chandra, XMM-Newton, and Swift-XRT coverage, respectively.

**Column 89:** An abbreviated code indicating the origin of the adopted lower-energy X-ray counterpart: CSC2 indicates counterparts from the Chandra Source Catalog Release 2.0 (Evans et al. 2019), 4XMM-DR10 and 4XMM-DR10s indicate the Fourth XMM-Newton Serendipitous Source Catalog, Tenth Data Release (Webb et al. 2020) and its stacked version (Traulsen et al. 2020), and 2SXPS indicates the Swift-XRT Point Source Catalog (Evans et al. 2020), respectively. CXO_MAN, XMM_MAN, and XRT_MAN indicate sources manually identified using archival Chandra, XMM-Newton, and Swift-XRT data, respectively. Sources that lack a soft X-ray counterpart are indicated with the code “NULL”; Section 3.1 details the counterpart matching.

**Columns 90, 91:** The R.A. and decl. coordinates (J2000) of the adopted lower-energy X-ray counterpart. Sources that lack

a lower-energy X-ray counterpart have R.A. and decl. values of (−999, −999). **Units:** degrees.

**Column 92:** Positional uncertainty for lower-energy (where available) or NuSTAR coordinates used for NWAY matching. **Units:** degrees.

**Column 93:** The angular offset between the NuSTAR position (columns 6 and 7) and the lower-energy X-ray counterpart position (columns 90 and 91). Sources lacking a soft X-ray counterpart are flagged with a value of −77. **Units:** arcseconds.

**Column 94:** Reference for the lower-energy X-ray flux used to compute the 3–8 keV fluxes in columns 95–97: 2–7 keV, 0.5–7 keV, or 0.1–10 keV for CSC2 fluxes, 4.5–12 keV for 4XMM-DR10/s fluxes, and 2–10 keV for 2SXPS fluxes.

**Columns 95–97:** The observed-frame 3–8 keV flux of the lower-energy X-ray counterpart (with associated lower and upper errors) for sources with counterparts in the CSC2, 4XMM-DR10/s, and 2SXPS catalogs. For CSC2 sources, we convert to the 3–8 keV flux from the 2–7 keV flux using a conversion factor of 0.83, for the 4XMM-DR10/s sources we convert from the 4.5–12 keV flux using a conversion factor of 0.92, and for the 2SXPS sources we convert from the 2–10 keV flux using a conversion factor of 0.62. Sources lacking a soft X-ray counterpart have values of 0. **Units:** erg s⁻¹ cm⁻².

**Columns 98–100:** The total combined 3–8 keV flux of all (CSC2, 4XMM-DR10/s, or 2SXPS) sources within 30'' of the NuSTAR position, with associated lower and upper errors. Sources lacking soft X-ray counterparts have values of 0. **Units:** erg s⁻¹ cm⁻².

**Column 101:** Galactic extinction, A<sub>v</sub>, i.e., the total absorption in magnitudes at V.

**Columns 102–104:** Galactic line-of-sight absorption in g, r, and i magnitudes.

**Columns 105, 106:** The NWAY-calculated probability that each CatWISE20 (Marocco et al. 2021) source is the correct counterpart to the (adopted lower-energy or NuSTAR) X-ray source (p<sub>Cat,best</sub> for CatWISE20), and the probability that any of the CatWISE20 sources is the right counterpart (p<sub>Cat,any</sub> for CatWISE20; a higher probability indicates a lower false-association likelihood.) Sources lacking a CatWISE20 counterpart are flagged with a value of −77.

**Columns 107, 108:** The CatWISE20 R.A. and decl. coordinates (J2000) for the most probable NWAY-matched
WISE counterpart. Sources that lack a CatWISE20 counterpart have R.A. and decl. values of (−999, −999). *Units*: degrees.

**Column 109:** The angular offset between the best NWAY-matched CatWISE20 position and the NuSTAR position. Sources lacking a CatWISE20 match are flagged with a −77 value. *Units*: arcseconds.

**Column 110:** The angular offset between the best NWAY-matched CatWISE20 position and the adopted lower-energy X-ray counterpart position. Sources that lack a CatWISE20 counterpart are flagged with values of −77. *Units*: arcseconds.

**Columns 111–114:** The CatWISE20 WISE profile-fit magnitudes and associated errors, for the two standard WISE bands available in CatWISE20: W1 (λ ≈ 3.4 μm) and W2 (λ ≈ 4.6 μm). Sources with no constraints are flagged with a −77 value, and upper limits are flagged with a −99 value in the error column. *Units*: Vega magnitudes.

**Columns 115, 116:** The AllWISE R.A. and decl. coordinates (J2000) for crossmatches with CatWISE20 coordinates. Sources that lack an AllWISE counterpart have R.A. and decl. values of (−999, −999). *Units*: degrees.

**Columns 117–120:** The AllWISE WISE profile-fit magnitudes and associated errors, for the two remaining standard WISE bands: W3 (λ ≈ 12 μm) and W4 (λ ≈ 22 μm). Sources with no constraints are flagged with a −77 value, and upper limits are flagged with a −99 value in the error column. *Units*: Vega magnitudes.

**Columns 121, 122:** The NWAY-calculated probability that each PS1-DR2 (Flewelling 2018) source is the correct counterpart to the (adopted lower-energy or NuSTAR) X-ray source ($\rho_{PS1,best}$), and the probability that any of the PS1-DR2 sources is the right counterpart ($\rho_{PS1,any}$). A higher probability indicates a lower false-association likelihood. Sources lacking a PS1-DR2 counterpart are flagged with a value of −77.

**Columns 123, 124:** The PS1-DR2 R.A. and decl. coordinates (J2000) for the best NWAY-matched Pan-STARRS counterpart. Sources that lack a PS1-DR2 NWAY match have R.A. and decl. values of (−999, −999). *Units*: degrees.

**Column 125:** The angular offset between the best NWAY-matched PS1-DR2 position and the NuSTAR position. Sources lacking a PS1-DR2 match are flagged with a −77 value. *Units*: arcseconds.

**Column 126:** The angular offset between the best NWAY-matched PS1-DR2 position and the adopted lower-energy X-ray position. Sources lacking a PS1-DR2 match are flagged with a −77 value. *Units*: arcseconds.

**Column 127:** The angular offset between the best NWAY-matched PS1-DR2 and CatWISE20 positions. Sources lacking a PS1-DR2/CatWISE20 match are flagged with a −77 value. *Units*: arcseconds.

**Columns 128–134:** The g-, r- and i-band magnitudes (with associated errors) of the best NWAY-matched PS1-DR2 counterpart. Magnitudes are not corrected for Galactic extinction. All Pan-STARRS magnitudes quoted in the NSS80 catalog are, in order of preference, Kron, PSF, or the default aperture magnitudes, with the selected type for each band indicated in column 132. Sources with unconstrained magnitudes are denoted with −77, and limits with −99 values in the error columns. *Units*: AB magnitudes.

**Column 135:** A binary flag indicating the subsample of higher-probability CatWISE20 or PS1-DR2 matches (i.e., NWAY reliable sample) with thresholds of $p_{Cat/PS1,best} > 0.4$ and $p_{Cat/PS1,any} > 0.5$. Section 3.2 details the IR/optical counterpart matching using NWAY.

**Column 136:** Reference indicating the origin of the adopted principal optical counterpart to the NuSTAR source. The code "PS1-NWAY" indicates sources with lower-energy X-ray counterparts and successful NWAY matches in the PS1-DR2 catalog (Flewelling 2018). The codes "PS1-MAN," "SDSS," "NSC2," "DES2" and "USNOB1" indicate sources with lower-energy X-ray counterparts and successful matches in the PS1-DR2 catalog (where OOff_PS1_CatWISE > 2.7 and therefore rematched to search for nominally closer PS1 matches), the SDSS photometric catalog DR12 (Alam et al. 2015), the second data release of the NOIRLab Source Catalog (Nidever et al. 2021), the Dark Energy Survey DR2 (Abbott et al. 2016), and the USNOB1 catalog (Monet et al. 2003), respectively. "PS1-CatWISE," "SDSS-CatWISE," "NSC2-CatWISE," "DES2-CatWISE," and "USNOB1-CatWISE20" indicate the cases where there is no lower-energy X-ray counterpart to the NuSTAR position, but a CatWISE20 AGN candidate is identified within the NuSTAR error circle and successfully matched to the PS1-DR2, SDSS-DR12, NSC2, DES-DR2, or USNOB1 catalog. "PS1-softX," "SDSS-softX," "NSC2-softX," "DES2-softX," and "USNO1-softX" indicate the cases where there is a lower-energy X-ray counterpart to the NuSTAR position, but no CatWISE20 candidate is identified within the NuSTAR error circle. "NULL" indicates sources that lack an optical identification. We give a detailed description of the procedure used to identify optical counterparts in Section 3.2.

**Columns 137, 138:** The R.A. and decl. coordinates (J2000) of the adopted optical counterpart, for sources with PS1-DR2, SDSS-DR12, NSC2, DES-DR2, and USNOB1 matches. Sources that lack an identified optical counterpart have R.A. and decl. values of (−999, −999). *Units*: degrees.

**Columns 139–145:** The g-, r- and i-band magnitudes (and associated errors) of the adopted optical counterpart. If the counterpart is sourced from PS1-DR2, the selected magnitude type for each band is indicated in column 143. Sources with no constraints are flagged with a −77 value, and limits are flagged with −99, respectively, in the error column. *Units*: AB magnitudes.

**Column 146:** The angular offset between the adopted optical position and the NuSTAR position. Sources lacking an optical identification are flagged with a −77 value. *Units*: arcseconds.

**Column 147:** The angular offset between the adopted optical position and the adopted lower-energy X-ray position. Sources lacking a PS1-DR2 match are flagged with a −77 value. *Units*: arcseconds.

**Column 148:** The angular offset between the adopted optical position and the best NWAY-identified CatWISE20 position. Sources lacking a PS1-DR2/CatWISE20 match are flagged with a −77 value. *Units*: arcseconds.

**Column 149:** A flag indicating whether the source is in the unique primary catalog, i.e., a single entry for each NuSTAR source with its principal optical counterpart. A value of 1 indicates principal counterpart entries; those that are secondary counterpart candidates are flagged with a value of 0.

**Column 150:** A flag indicating whether the source is in the main spectroscopic catalog presented in Table 14: a value of 1 indicates the unique source entries for the spectroscopic catalog; a value of −1 flags sources with photometric redshifts;
and sources which have not been targeted during our spectroscopic campaign are flagged with a value of 0.

*Columns 151, 152:* The R.A. and decl. coordinates (J2000) of the spectroscopic target observed during the ground-based follow-up program; see Section 3.3. Untargeted sources have R.A. and decl. values of (–999, –999). *Units:* degrees.

*Column 153:* The angular offset between the spectroscopic target position and the adopted optical position. Sources lacking spectroscopic follow-up or an optical identification are flagged with a –77 value. *Units:* arcseconds.

*Column 154:* The spectroscopic redshift of the NuSTAR source. The large majority of the redshifts were obtained through our own campaign of ground-based spectroscopic follow-up of NuSTAR serendipitous survey sources (see Section 3.3). Sources which have been followed up but lack redshift measurements due to low-S/N spectra are flagged with –99 values, while unobserved sources have entries of –77.

*Column 155:* Quality flag of the spectroscopic redshift measurement. Single-line measurements are flagged as “quality B” redshift measurements, photometric redshifts obtained from literature are flagged as “quality C”, and sources with a faint continuum detected (but lack a redshift measurement) are flagged as “quality F.”

*Column 156:* Spectroscopic classification of the NuSTAR source: BL ≡ broad-line object (i.e., quasar); NL ≡ narrow-line object (AGN or galaxy); Gxy ≡ galaxy (absorption lines); Galactic ≡ Galactic sources at z = 0. See Section 3.3.3.

*Column 157:* Additional classification information for the duplicate source entries, e.g., AGN pairs (“BL_pair” and “NL_pair”), dual AGN (“Dual_AGN”), galaxy pairs (“Gxy_pair”), and more than one counterpart candidate (“2cpart_candidates”).

*Columns 158, 159:* Binary flags indicating whether the spectroscopic target position matches to the best NWAY-identified counterpart for CatWISE20 and PS1-DR2.

*Column 160:* A flag indicating the reliability of the spectroscopic target as the correct counterpart: 1 ≡ correct counterpart; 0 ≡ counterpart uncertainty; –1 ≡ unobserved.

*Column 161:* Reference indicating the catalog origin of the spectroscopic counterpart.

*Columns 162–167:* The g-, r- and i-band magnitudes (with associated errors) of the spectroscopic target. Magnitudes are not corrected for Galactic extinction. Sources with unconstrained magnitudes are denoted with –77, and limits with –99 values in the error column. *Units:* AB magnitudes.

*Column 168:* The rest-frame 10–40 keV luminosity, estimated from the fluxes in columns 82–87. The luminosities are observed values, uncorrected for any absorption along the line of sight. The intrinsic luminosities may therefore be higher, for highly absorbed AGNs. Sources with no constraints are flagged with a –77 value. *Units:* erg s⁻¹.

*Column 169:* A binary flag indicating the few sources that show evidence for being associated with the primary science target of their respective NuSTAR observations, according to the definition in Section 3.3.3 (Δ(cz) < 0.05 cz). 1 ≡ associated with primary target; 0 ≡ not associated; –1 ≡ no spectroscopy.

*Column 170:* A binary flag indicating the NuSTAR sources which are CT candidates (N_H ≳ 1.5 × 10²⁴ cm⁻²). These sources can be (crudely) identified from their extreme band ratios, as demonstrated in Section 4.1.2.

## Appendix B

### Description of the Secondary NSS80 Source Catalog

The secondary NuSTAR serendipitous survey source catalog contains 214 sources in total, and is available as an electronic table on the NSS80 web page. Here we describe the columns of the catalog, which are summarized in Table 12.

<table><caption>**Table 12**

Column Descriptions for the Secondary NSS80 Catalog</caption><thead><tr><th>Column Number</th><th>Description</th></tr></thead><tbody><tr><td>1</td><td>Unique source identification number (ID).</td></tr><tr><td>2</td><td>Unique NuSTAR source name.</td></tr><tr><td>3</td><td>Unique NuSTAR field and source ID.</td></tr><tr><td>4, 5</td><td>Unique L17 NuSTAR source ID and field; the secondary L17 catalog is appended with an “S.”</td></tr><tr><td>6, 7</td><td>R.A. and decl.</td></tr><tr><td>8–10</td><td>Flags indicating the energy bands for which the source is detected.</td></tr><tr><td>11–13</td><td>Same as columns 10–12, post-deblending.</td></tr><tr><td>14–16</td><td>The logarithm of the false probabilities for the three standard NuSTAR energy bands.</td></tr><tr><td>17</td><td>The NuSTAR detection likelihood.</td></tr><tr><td>18–20</td><td>Same as columns 16–18, post-deblending.</td></tr><tr><td>21</td><td>The same as column 19, post-deblending.</td></tr><tr><td>22</td><td>Flag indicating whether the source is significant post-deblending, for at least one energy band.</td></tr><tr><td>23–37</td><td>Total, background, and net source counts for the three standard energy bands and associated errors.</td></tr><tr><td>38–49</td><td>Same as columns 25–39, post-deblending.</td></tr><tr><td>50–52</td><td>Net vignetting-corrected exposure times at the source position, for the combined A + B data.</td></tr><tr><td>53–67</td><td>Total, background, and net source count rates for the three standard energy bands and associated errors.</td></tr><tr><td>68–73</td><td>Deblended net source count rates for the three standard energy bands and associated errors.</td></tr><tr><td>74–76</td><td>Band ratio and upper and lower errors.</td></tr><tr><td>77–79</td><td>Effective photon index and upper and lower errors.</td></tr><tr><td>80–85</td><td>Deblended fluxes in the three standard bands and associated errors.</td></tr><tr><td>86, 87</td><td>Flags indicating optical mask and optical source name.</td></tr></tbody></table>

(This table is available in its entirety in machine-readable form in the online article.)
## Appendix C
### Comparison to the NSS40 Catalog

Overall, we find a 91% match between the primary NSS80 catalog and NSS40 for a search radius of 25" (which is the positional accuracy of NuSTAR for faint sources), with 36 primary NSS40 sources reported in L17 undetected in the NSS80. For the majority of these sources the deeper data has

improved the false-probability estimates and, consequently, eliminates false detections. This is particularly noticeable for L17 sources with detections in a single energy band only. We summarize potential reasons to explain the undetected L17 sources in Table 13: 32 sources have improved false probabilities, one source lies in an excess background region, and three sources are on the peripheries of coadded fields.

<table><caption>**Table 13**
A List of the NSS40 Serendipitous Sources Reported in L17 that Are Undetected in the NSS80 Catalog</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Science Target Name<br>(3)</th><th>R.A.<br>(deg)<br>(4)</th><th>Decl.<br>(deg)<br>(5)</th><th>Type<br>(6)</th><th>z<sub>spec</sub><br>(7)</th><th>Explanation<br>(8)</th></tr></thead><tbody><tr><td>2</td><td>NuSTARJ001130+0057.8</td><td>SDSSJ001111d97p005626d3</td><td>2.88</td><td>0.96</td><td>BL</td><td>1.492</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>5</td><td>NuSTARJ001717+8127.3</td><td>S50014p81</td><td>4.32</td><td>81.46</td><td>...</td><td>...</td><td>Undetected in HB+FB; logSdbP ≈ −6.</td></tr><tr><td>9</td><td>NuSTARJ001953+5911.8</td><td>IC10_X1</td><td>4.97</td><td>59.2</td><td>...</td><td>...</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>78</td><td>NuSTARJ040730+0344.2</td><td>3C105</td><td>61.88</td><td>3.74</td><td>...</td><td>...</td><td>Undetected in SB+FB; logHdbP ≈ −6.</td></tr><tr><td>79</td><td>NuSTARJ042349+0410.9</td><td>2MASXJ04234080p0408017</td><td>65.96</td><td>4.18</td><td>...</td><td>...</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>81</td><td>NuSTARJ042509−5709.5</td><td>1H_0419m577</td><td>66.29</td><td>−57.16</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>89</td><td>NuSTARJ043724−4722.2</td><td>PSRJ0437m4715</td><td>69.35</td><td>−47.37</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>99</td><td>NuSTARJ052100−2528.8</td><td>IRAS05189m2524</td><td>80.25</td><td>−25.48</td><td>BL</td><td>1.666</td><td>Possible false detection on the edge of an exposure.</td></tr><tr><td>121</td><td>NuSTARJ065922−5558.6</td><td>Bullet_Bullet_shock</td><td>104.84</td><td>−55.98</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>179</td><td>NuSTARJ095440+6942.6</td><td>SN2014J</td><td>148.67</td><td>69.71</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>192</td><td>NuSTARJ095801+6859.4</td><td>M81_X9</td><td>149.51</td><td>68.99</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>193</td><td>NuSTARJ095806+6910.3</td><td>M81_X9</td><td>149.53</td><td>69.17</td><td>...</td><td>...</td><td>Undetected in HB+FB; logSdbP ≈ −6.</td></tr><tr><td>196</td><td>NuSTARJ095853+6901.3</td><td>M81_X9</td><td>149.72</td><td>69.02</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>211</td><td>NuSTARJ102318+0036.5</td><td>PSRJ1023p0038</td><td>155.83</td><td>0.61</td><td>Gal</td><td>0.0</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>212</td><td>NuSTARJ102328+0043.9</td><td>PSRJ1023p0038</td><td>155.87</td><td>0.73</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>219</td><td>NuSTARJ102802−4351.0</td><td>NGC3256</td><td>157.01</td><td>−43.85</td><td>BL</td><td>1.784</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>227</td><td>NuSTARJ105931+2429.8</td><td>IRAS_10565p2448</td><td>164.88</td><td>24.5</td><td>BL</td><td>0.908</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>233</td><td>NuSTARJ110632+7225.9</td><td>NGC3516</td><td>166.64</td><td>72.43</td><td>...</td><td>...</td><td>Undetected in SB+FB; logHdbP ≈ −6.</td></tr><tr><td>236</td><td>NuSTARJ110752+7230.7</td><td>NGC3516</td><td>166.97</td><td>72.51</td><td>BL</td><td>0.901</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>256</td><td>NuSTARJ120242+4437.2</td><td>NGC4051</td><td>180.68</td><td>44.62</td><td>NL?</td><td>0.296</td><td>Possible false detection on the edge of an exposure.</td></tr><tr><td>261</td><td>NuSTARJ120613+4957.2</td><td>2MASXJ12055599p4959561</td><td>181.56</td><td>49.95</td><td>BL</td><td>0.784</td><td>Undetected in SB; logFdbP ≈ −6.</td></tr><tr><td>302</td><td>NuSTARJ125657+5644.6</td><td>Mrk231</td><td>194.24</td><td>56.74</td><td>NL</td><td>2.073</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>303</td><td>NuSTARJ130108−6356.2</td><td>2RXPJ130159d6m635806</td><td>195.28</td><td>−63.94</td><td>...</td><td>...</td><td>Undetected in SB+FB; logHdbP ≈ −6.</td></tr><tr><td>313</td><td>NuSTARJ133311−3406.8</td><td>ESO383_18</td><td>203.3</td><td>−34.11</td><td>NL?</td><td>0.091</td><td>Possible false detection on the edge of an exposure.</td></tr><tr><td>330</td><td>NuSTARJ141215−6519.6</td><td>Circinus_XMM2</td><td>213.07</td><td>−65.33</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>375</td><td>NuSTARJ165346+3953.7</td><td>Mkn501</td><td>253.44</td><td>39.9</td><td>NL</td><td>0.354</td><td>Undetected in SB+FB; logHdbP ≈ −6.</td></tr><tr><td>376</td><td>NuSTARJ165351+3938.5</td><td>Mkn501</td><td>253.46</td><td>39.64</td><td>Gal</td><td>0.0</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>384</td><td>NuSTARJ171718−6239.1</td><td>NGC6300</td><td>259.33</td><td>−62.65</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr><tr><td>389</td><td>NuSTARJ172755−1417.4</td><td>PDS_456</td><td>261.98</td><td>−14.29</td><td>...</td><td>...</td><td>Undetected in HB+FB; logSdbP ≈ −6.</td></tr><tr><td>390</td><td>NuSTARJ172803−1423.0</td><td>PDS_456</td><td>262.02</td><td>−14.38</td><td>BL</td><td>1.555</td><td>Contaminated by stray light.</td></tr><tr><td>395</td><td>NuSTARJ172843−1419.0</td><td>PDS_456</td><td>262.18</td><td>−14.32</td><td>...</td><td>...</td><td>Undetected in HB+FB; logSdbP ≈ −6.</td></tr><tr><td>407</td><td>NuSTARJ182447−2444.5</td><td>PSR_B1821m24</td><td>276.2</td><td>−24.74</td><td>...</td><td>...</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>414</td><td>NuSTARJ183422−0840.6</td><td>HESSJ1834m087_TeV</td><td>278.59</td><td>−8.68</td><td>...</td><td>...</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>413</td><td>NuSTARJ183422−0841.4</td><td>HESSJ1834m087_TeV</td><td>278.59</td><td>−8.69</td><td>...</td><td>...</td><td>P<sub>false</sub> condition not met in NSS80 reductions.</td></tr><tr><td>485</td><td>NuSTARJ224302+2942.1</td><td>Ark_564</td><td>340.76</td><td>29.7</td><td>...</td><td>...</td><td>Undetected in SB+FB; logHdbP ≈ −6.</td></tr><tr><td>491</td><td>NuSTARJ231811−4228.8</td><td>NGC7582</td><td>349.55</td><td>−42.48</td><td>...</td><td>...</td><td>Undetected in SB+HB; logFdbP ≈ −6.</td></tr></tbody></table>

**Notes.** Columns: (1): unique source identification number in L17. (2): unique NuSTAR source name in L17. (3): object name for the primary science target of the NuSTAR observation in L17. (4): R.A. as recorded in L17. (5): decl. as recorded in L17. (6): spectroscopic classification of the optical counterpart. (7): spectroscopic redshift. (8): explanation for nondetection of the NSS40 serendipitous source in the NSS80 catalog.
## Appendix D

### Comparison of CatWISE20 Counterparts to Spectroscopic Targets

Our assessment of the reliability of the followed-up spectroscopic sources takes into account the positional offset between the best CatWISE20 counterpart and the spectroscopic counterpart in combination with the CatWISE20 probability. In Figure D1, we plot the offset between the best CatWISE20 counterpart and the followed-up spectroscopic target as a function of the NWAY best-match probability, color coded by the different spectral classifications. Each spectroscopic class is further divided into NSS80 sources with lower-energy X-ray (solid symbols) and without lower-energy X-ray (white filled, color-edged symbols) counterparts. Overall, there is a good match to NWAY for the majority of the spectroscopically classified sources, indicating that the correct spectroscopic counterpart has been identified: the positional offset for the majority of the sources is < 5”; we consider 5” as a reasonable threshold since it broadly corresponds to the CatWISE20 positional uncertainty. The reliability of the targets with larger positional offsets is less certain. The NWAY probability for the best CatWISE20 counterpart is strongly dependent on the availability of a lower-energy X-ray counterpart. For example, the dual AGN system in the NSS80 catalog (NuSTARJ054231+6054.4; open, purple-edged star) is the correct counterpart based on its AGN-like WISE colors, but it has a low NWAY probability due to the lack of lower-energy X-ray information (Swift-XRT coverage, but undetected). Most of the large-offset NSS80 sources without lower-energy X-ray counterparts have low-to-intermediate

<figure><img src="image_36.png" /></figure>

**Figure D1.** Separation in arcseconds between the NWAY-identified CatWISE20 counterpart and the spectroscopic target vs. the best CatWISE20 match probability, color coded by spectral classifications: BL (blue circle), NL (green circle), galaxy (Gxy; peach “×”), Galactic sources (gray circle), AGN-Gxy pairs (peach star), dual AGN (purple star), and a BL Lac candidate (white, black-edged “×”). Solid symbols indicate NSS80 sources with lower-energy (i.e., soft) X-ray counterparts and white filled symbols mark NSS80 sources which lack lower-energy X-ray counterparts and, therefore, have a lower match probability given the large uncertainty in the NuSTAR position (i.e., ~25"). The vertical black dashed-dotted line indicates the probability cut we applied in Section 3.2 to obtain reliable counterpart associations to the X-ray source.

NWAY probabilities, and sensitive lower-energy X-ray observations are required to improve the counterpart identification. By comparison, most of the large-offset NSS80 sources with lower-energy X-ray counterparts have high NWAY probabilities, but NWAY has selected a different source as the best match, typically a brighter lower-energy X-ray counterpart to that spectroscopically followed up (see, e.g., Figure 20). To better determine the reliability between the best CatWISE20 counterpart and the followed-up counterpart of these more uncertain sources requires further investigation including, for example, spectroscopic follow-up of the best CatWISE20 counterpart.

## Appendix E

### Optical Spectroscopic Properties of Individual post-NSS40 Objects

#### E.1. Optical Spectroscopic Properties of Individual post-NSS40 Objects

Here we provide details of the optical spectroscopic properties of individual sources from the NuSTAR serendipitous survey. As described in Section 3.3.1, these largely result from our dedicated follow-up campaign using the Keck, Palomar, VLT, and SALT facilities, and also from existing publicly available spectroscopy (primarily SDSS spectroscopy).

Details for individual sources are tabulated in Table 14, the columns of which are as follows:

(1) Unique NuSTAR source identification number, in order of increasing R.A.

(2) Unique NuSTAR source name as listed in source catalog.

(3) The unique observing run identification number, as defined in Table 6 (“S” and “Lit” mark spectra obtained from the SDSS and from elsewhere in the literature, respectively).

(4) Source redshift (mainly in spectroscopic data).

(5) Source classification as described in Section 3.3.3 (sources with photometric redshift measurements are appended with a “C” symbol and sources with a level of ambiguity in the optical classification are appended with a “?” symbol).

(6) Quality flag of spectroscopic redshift. Single-line measurements are annotated with “B” and photometric redshift measurements with “C”; “F” annotates sources which lack a reliable redshift measurement (usually faint, red continuum spectra).

(7) NWAY association flag: 0 = mismatch between spectroscopic target and NWAY source; 1 = match between spectroscopic target and NWAY source; -99 = secondary post-NSS40 objects.

(8) A binary flag indicating sources that show evidence for being associated with the primary science target of their respective NuSTAR observations, according to the definition $\Delta(cz) < 0.05 \text{ cz}$.

(9) An abbreviated flag indicating a NWAY CatWISE20 (“C”) and/or PS1-DR2 (“P”) counterpart match to the spectroscopic target.

(10) Notes based on our visual assessment of the spectra.

Individual source spectra are available online and example spectra of the first four sources for the different spectral classes are shown in Figures E1–E5: BL AGNs, NL AGNs, galaxies, Galactic sources, and unclassified objects with a faint continuum detected, respectively. The spectra for each class are given in
<table><caption>**Table 14**
Summary of the Optical Spectroscopy for the post-NSS40 Serendipitous Survey Sources</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>2</td><td>NuSTARJ000303+7017.7</td><td>24</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Possibly incorrect counterpart due to high source density.</td></tr><tr><td>3</td><td>NuSTARJ000333+7013.7</td><td>20</td><td>0.391</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>4</td><td>NuSTARJ000423+7017.2</td><td>20</td><td>0.775</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>5</td><td>NuSTARJ000549+2013.0</td><td>S</td><td>1.974</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Mg II BALQSO.</td></tr><tr><td>6</td><td>NuSTARJ000613+2018.3</td><td>23</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected.</td></tr><tr><td>10</td><td>NuSTARJ001443+8131.9</td><td>24</td><td>0.365</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>15</td><td>NuSTARJ001952-7057.0</td><td>25</td><td>0.813</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>17</td><td>NuSTARJ002046-7057.6</td><td>30</td><td>0.271</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>19</td><td>NuSTARJ002112+5542.5</td><td>7</td><td>0.409</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>20</td><td>NuSTARJ002113-7053.5</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; two potential candidates within XMM error circle.</td></tr><tr><td>27</td><td>NuSTARJ004220-1254.0</td><td>7</td><td>0.803</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>28</td><td>NuSTARJ004230-1255.3</td><td>1</td><td>0.521</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>31</td><td>NuSTARJ005219+1725.3</td><td>22</td><td>0.102</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>[O III] affected by chip gap.</td></tr><tr><td>40</td><td>NuSTARJ005538+4613.1</td><td>23</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>41</td><td>NuSTARJ005543+4605.6</td><td>23</td><td>0.452</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>42</td><td>NuSTARJ005730-2220.5</td><td>28</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Low S/N spectrum; potentially Hα at z = 0.195.</td></tr><tr><td>43</td><td>NuSTARJ005748-2218.8</td><td>27</td><td>1.260</td><td>BL</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>45</td><td>NuSTARJ010710-1732.4</td><td>32</td><td>0.369</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>46</td><td>NuSTARJ010718-1130.9</td><td>13</td><td>1.146</td><td>BL?</td><td>B</td><td>0</td><td>C</td><td>1</td><td>Extremely faint; potential Mg II detected.</td></tr><tr><td>48</td><td>NuSTARJ010736-1732.3</td><td>L</td><td>0.0217</td><td>NL</td><td>...</td><td>1</td><td>C+P</td><td>1</td><td>Emission-line galaxy (da Costa et al. 1998) associated with the NuSTAR science target (Strauss et al. 1992; Arp 1966 IC 1623).</td></tr><tr><td>49</td><td>NuSTARJ010739-1139.1</td><td>5</td><td>0.048</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>UKST/6dF spectrum also available (Jones et al. 2009); reported in Swift-BAT BASS DR2 (Koss et al. 2022).</td></tr><tr><td>56</td><td>NuSTARJ011429-3241.9</td><td>27</td><td>0.693</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>60</td><td>NuSTARJ012227+0056.2</td><td>S</td><td>1.698</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>62</td><td>NuSTARJ012618+2559.2</td><td>16</td><td>0.410</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>63</td><td>NuSTARJ012633+2556.2</td><td>S</td><td>0.427</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>64</td><td>NuSTARJ012642+2554.9</td><td>18</td><td>0.208</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>68</td><td>NuSTARJ012947-6036.9</td><td>28</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; continuum detected.</td></tr><tr><td>69</td><td>NuSTARJ013003-4600.4</td><td>29</td><td>0.159</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Hα lost to A-band telluric feature.</td></tr><tr><td>72</td><td>NuSTARJ013859+2920.0</td><td>7</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; target is bright in W3.</td></tr><tr><td>73</td><td>NuSTARJ014316+1337.7</td><td>1</td><td>0.844</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>74</td><td>NuSTARJ014333+1342.2</td><td>13</td><td>0.343</td><td>Gxy</td><td>...</td><td>0</td><td>P</td><td>1</td><td>Possibly an obscured AGN in an early-type galaxy; weak Hα detection.</td></tr><tr><td>75</td><td>NuSTARJ014904+2143.5</td><td>5</td><td>0.614</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>78</td><td>NuSTARJ015548+0227.2</td><td>22</td><td>0.481</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>79</td><td>NuSTARJ020344+1137.3</td><td>5</td><td>0.167</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; Hα affected by A-band telluric feature.</td></tr><tr><td>82</td><td>NuSTARJ020601-0011.7</td><td>S</td><td>1.337</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Strong [O II] emission line.</td></tr><tr><td>83</td><td>NuSTARJ020614+6449.3</td><td>24</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>2</td><td>Possibly two sources contributing to NuSTAR detection; continuum detected for both targets.</td></tr><tr><td>84</td><td>NuSTARJ020622-0023.5</td><td>23</td><td>2.793</td><td>NL</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>Tentative Lyα and C III] emission lines detected.</td></tr><tr><td>87</td><td>NuSTARJ021435-0042.7</td><td>S</td><td>0.437</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>88</td><td>NuSTARJ021449-0045.2</td><td>7</td><td>0.940</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Oxygen lines offset from a continuum source.</td></tr><tr><td>89</td><td>NuSTARJ021454-6425.9</td><td>30</td><td>0.068</td><td>Gxy/pair</td><td>...</td><td>1</td><td>...</td><td>2</td><td>Galaxy companion at z = 0.075 which is associated with the NuSTAR science target (RBS 0295; Schwope et al. 2000); Hα affected by chip gap.</td></tr><tr><td>90</td><td>NuSTARJ021810+4236.0</td><td>12</td><td>0.967</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>91</td><td>NuSTARJ021902+7348.5</td><td>20</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Unusual WISE (bright in W3) optical colors for Galactic source.</td></tr><tr><td>92</td><td>NuSTARJ021934-0508.8</td><td>S</td><td>1.324</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Counterpart uncertainty; the nominally closer (but fainter) CXO source is a SDSS BL at z = 2.305.</td></tr><tr><td>93</td><td>NuSTARJ022023-0403.2</td><td>20</td><td>3.190</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>C IV affected by telluric feature.</td></tr><tr><td>94</td><td>NuSTARJ022032-0403.3</td><td>S</td><td>0.822</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>95</td><td>NuSTARJ022222+2505.9</td><td>20</td><td>0.342</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>97</td><td>NuSTARJ022742+3331.5</td><td>20</td><td>0.090</td><td>NL/pair</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Borderline AGN from BPT diagnostics; NL companion (star-forming from BPT) north of NuSTAR position at the same redshift.</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>99</td><td>NuSTARJ022746+3334.6</td><td>23</td><td>0.387</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>101</td><td>NuSTARJ022943-0857.8</td><td>24</td><td>1.182</td><td>BL</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>102</td><td>NuSTARJ022951-0856.4</td><td>24</td><td>0.300</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>104</td><td>NuSTARJ023013-0853.2</td><td>24</td><td>0.180</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty based on XMM position and WISE AGN candidate; target is an emission-line galaxy.</td></tr><tr><td>105</td><td>NuSTARJ023023-0857.7</td><td>22</td><td>0.449</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>106</td><td>NuSTARJ023030-0856.9</td><td>24</td><td>0.631</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>110</td><td>NuSTARJ024111+0711.1</td><td>28</td><td>2.983</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>C III] affected by A-band telluric feature.</td></tr><tr><td>111</td><td>NuSTARJ024143+0708.4</td><td>30</td><td>0.403</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>[O III] affected by chip gap.</td></tr><tr><td>112</td><td>NuSTARJ024144+0512.3</td><td>22</td><td>0.070</td><td>NL</td><td>...</td><td>1</td><td>C+P</td><td>1</td><td>2MASX J02414414+0512203 (Bilicki et al. 1996); associated with the NuSTAR science target (2MASX J02420381+0510061; Gu et al. 1997).</td></tr><tr><td>113</td><td>NuSTARJ024213+0516.1</td><td>23</td><td>0.441</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Narrow Mg II.</td></tr><tr><td>114</td><td>NuSTARJ024213-0001.5</td><td>S</td><td>0.687</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>116</td><td>NuSTARJ024243-0006.4</td><td>23</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>117</td><td>NuSTARJ024254-0004.6</td><td>S</td><td>1.850</td><td>BL</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>119</td><td>NuSTARJ024304+0000.1</td><td>S</td><td>1.995</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>C IV BALQSO; C III] affected by telluric feature.</td></tr><tr><td>125</td><td>NuSTARJ025932+3642.3</td><td>13</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected.</td></tr><tr><td>126</td><td>NuSTARJ030008+4415.0</td><td>8</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Counterpart uncertainty; difficult to assess due to deficient soft X-ray information. (Figure 1 of Fiore et al. 2000).</td></tr><tr><td>131</td><td>NuSTARJ031015-7651.5</td><td>L</td><td>1.187</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>NWAY disagreement; faint red continuum source next to bright star.</td></tr><tr><td>147</td><td>NuSTARJ032419+3413.8</td><td>24</td><td>...</td><td>...</td><td>F</td><td>0</td><td>...</td><td>2</td><td>...</td></tr><tr><td>149</td><td>NuSTARJ032439+3415.1</td><td>24</td><td>1.412</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>156</td><td>NuSTARJ033331-0506.9</td><td>31</td><td>0.458</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hβ affected by chip gap.</td></tr><tr><td>160</td><td>NuSTARJ033835+0110.4</td><td>19</td><td>0.171</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>170</td><td>NuSTARJ035542-6252.8</td><td>26</td><td>0.408</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>175</td><td>NuSTARJ035902-3011.7</td><td>25</td><td>0.093</td><td>NL</td><td>...</td><td>1</td><td>C</td><td>1</td><td>Associated with the NuSTAR science target (SARS 059.33488-30.34397; Katgert et al. 1998).</td></tr><tr><td>177</td><td>NuSTARJ035918-3009.6</td><td>26</td><td>0.549</td><td>NL?</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Low S/N spectrum; Hβ + [O III] affected by A-band telluric feature.</td></tr><tr><td>178</td><td>NuSTARJ035951-3009.9</td><td>28</td><td>0.685</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; [O III] affected by telluric feature.</td></tr><tr><td>179</td><td>NuSTARJ040702+0346.8</td><td>24</td><td>0.088</td><td>NL</td><td>B</td><td>1</td><td>C</td><td>1</td><td>Associated with the NuSTAR science target (3C 105 Nilsson 1998).</td></tr><tr><td>183</td><td>NuSTARJ041426+2805.9</td><td>24</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Known T-Tauri star (Luhman et al. 2010); the brighter companion is also a known T-Tauri star; counterpart uncertainty.</td></tr><tr><td>184</td><td>NuSTARJ041656+0058.0</td><td>7</td><td>0.438</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>194</td><td>NuSTARJ042914-2110.2</td><td>27</td><td>0.818</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>206</td><td>NuSTARJ044901+1123.2</td><td>2</td><td>0.872</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Type-2 quasar.</td></tr><tr><td>212</td><td>NuSTARJ045348+0408.6</td><td>2</td><td>1.357</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Likely Type-2 quasar.</td></tr><tr><td>213</td><td>NuSTARJ050449-1016.6</td><td>19</td><td>0.342</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>214</td><td>NuSTARJ050501-1010.4</td><td>19</td><td>0</td><td>Galactic</td><td>B</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>218</td><td>NuSTARJ050559-2349.9</td><td>2</td><td>0.137</td><td>NL</td><td>...</td><td>1</td><td>...</td><td>2</td><td>Counterpart uncertainty; NL at z = 0.036 is associated with the NuSTAR science target (LEDA178130; Jones et al. 2004, 2009; Lansbury et al. 2017b).</td></tr><tr><td>222</td><td>NuSTARJ050919+0544.1</td><td>20</td><td>1.492</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>227</td><td>NuSTARJ050941+0541.7</td><td>20</td><td>0.796</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>232</td><td>NuSTARJ051926-4546.0</td><td>26</td><td>0</td><td>Galactic</td><td>B</td><td>0</td><td>C</td><td>1</td><td>Continuum detected.</td></tr><tr><td>233</td><td>NuSTARJ051926-3242.8</td><td>25</td><td>0.915</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>234</td><td>NuSTARJ051935-3235.9</td><td>26</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty.</td></tr><tr><td>235</td><td>NuSTARJ051937-3233.3</td><td>25</td><td>0.640</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>236</td><td>NuSTARJ051945-3235.2</td><td>25</td><td>1.174</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>237</td><td>NuSTARJ052056-2524.1</td><td>25</td><td>0.111</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>241</td><td>NuSTARJ052116-2514.1</td><td>30</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected with red configuration.</td></tr><tr><td>243</td><td>NuSTARJ052438-2341.7</td><td>27</td><td>0.322</td><td>Gxy</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; require deeper optical/IR imaging.</td></tr><tr><td>245</td><td>NuSTARJ052613-2118.7</td><td>31</td><td>0.214</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hβ and Hα affected by chip gaps.</td></tr><tr><td>249</td><td>NuSTARJ053120+2132.9</td><td>24</td><td>0.379</td><td>NL?</td><td>...</td><td>0</td><td>...</td><td>2</td><td>...</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>261</td><td>NuSTARJ053823+2225.7</td><td>24</td><td>0.153</td><td>NL?</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Faint, red Type-2 AGN (no blue extraction); Counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>264</td><td>NuSTARJ054231+6054.4</td><td>20</td><td>0.257</td><td>NL/Dual</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Targeted W3-detected WISE source; deficient soft X-ray information; Hα affected by A-band telluric feature.</td></tr><tr><td>267</td><td>NuSTARJ054349-5536.7</td><td>29</td><td>0.272</td><td>BL</td><td>...</td><td>1</td><td>C</td><td>1</td><td>Dual AGN; pair of merging, obscured AGNs.</td></tr><tr><td>281</td><td>NuSTARJ061820+2234.2</td><td>24</td><td>0.776</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Associated with the NuSTAR science target (2FGL J0543.9-5532; Chang et al. 2019).</td></tr><tr><td>295</td><td>NuSTARJ063325+0549.3</td><td>20</td><td>0.347</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>304</td><td>NuSTARJ064331+5530.4</td><td>24</td><td>0.167</td><td>NL?</td><td>...</td><td>0</td><td>P</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>335</td><td>NuSTARJ073530-6936.7</td><td>31</td><td>1.055</td><td>BL?</td><td>B</td><td>0</td><td>C</td><td>1</td><td>Low S/N spectrum; C II) + Mg II affected by chip gaps.</td></tr><tr><td>337</td><td>NuSTARJ073651-6935.9</td><td>30</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>343</td><td>NuSTARJ074113-5442.6</td><td>26</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>345</td><td>NuSTARJ074317+6509.5</td><td>24</td><td>0.760</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>360</td><td>NuSTARJ081003-7527.2</td><td>30</td><td>...</td><td>BL Lac?</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected; bright X-ray source with featureless power-law spectrum.</td></tr><tr><td>363</td><td>NuSTARJ081323+2541.1</td><td>9</td><td>0.899</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Also observed in SDSS-DR16 but with lower S/N; WISEA J081322.80+254119.0.</td></tr><tr><td>382</td><td>NuSTARJ084149+0101.0</td><td>20</td><td>0.560</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hβ affected by A-band telluric line.</td></tr><tr><td>384</td><td>NuSTARJ084337+3555.1</td><td>3</td><td>0.699</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>385</td><td>NuSTARJ084407+3552.8</td><td>S</td><td>0.467</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>387</td><td>NuSTARJ084725-2337.5</td><td>26</td><td>0.216</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>390</td><td>NuSTARJ085429+6424.3</td><td>9</td><td>0.806</td><td>Gxy</td><td>...</td><td>0</td><td>P</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; likely spurious NuSTAR detection.</td></tr><tr><td>395</td><td>NuSTARJ090529+6930.1</td><td>20</td><td>0.418</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>396</td><td>NuSTARJ090602+6933.1</td><td>20</td><td>0.777</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>404</td><td>NuSTARJ091519+2931.9</td><td>S</td><td>1.099</td><td>BL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; the fainter WISE-XMM source is a SDSS BL at z = 1.099 Richards et al. (2009).</td></tr><tr><td>405</td><td>NuSTARJ091534+4054.6</td><td>S</td><td>1.298</td><td>BL/pair</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>BL AGN pair; SDSS quasar companion at same redshift matches to NWAY.</td></tr><tr><td>408</td><td>NuSTARJ091912+5527.8</td><td>S</td><td>0.049</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Possibly Sy2 (Véron-Cetty & Véron 2006; Ahn et al. 2012).</td></tr><tr><td>418</td><td>NuSTARJ094133+3441.5</td><td>S</td><td>1.779</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>422</td><td>NuSTARJ094847+0023.6</td><td>9</td><td>0.262</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>423</td><td>NuSTARJ094907+0026.2</td><td>S</td><td>2.461</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>424</td><td>NuSTARJ094910+0022.9</td><td>14</td><td>0.093</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Nearby extended source is an emission-line galaxy at z = 0.11; possibly both sources contributing to NuSTAR detection.</td></tr><tr><td>441</td><td>NuSTARJ095709+2511.6</td><td>S</td><td>0.902</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>457</td><td>NuSTARJ100620-3350.1</td><td>27</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>458</td><td>NuSTARJ100642-3355.1</td><td>27</td><td>0.069</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty; WISE AGN candidate on edge of CXO error circle.</td></tr><tr><td>459</td><td>NuSTARJ100648+6535.4</td><td>3</td><td>0.983</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Mg II affected by chip gap.</td></tr><tr><td>460</td><td>NuSTARJ100700+6530.1</td><td>3</td><td>0.117</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Emission-line galaxy; counterpart uncertainty.</td></tr><tr><td>474</td><td>NuSTARJ102313+1956.7</td><td>S</td><td>1.087</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>489</td><td>NuSTARJ103135-4206.0</td><td>L</td><td>0.0615</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Paturel et al. (2005).</td></tr><tr><td>492</td><td>NuSTARJ103456+3939.6</td><td>S</td><td>0.151</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Ahn et al. (2012).</td></tr><tr><td>493</td><td>NuSTARJ103514+3939.0</td><td>S</td><td>0.107</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Abazajian et al. (2009).</td></tr><tr><td>501</td><td>NuSTARJ104950+2301.6</td><td>S</td><td>0.143</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>503</td><td>NuSTARJ110021+6458.4</td><td>S</td><td>0.882</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>505</td><td>NuSTARJ110333-2333.8</td><td>26</td><td>1.372</td><td>BL</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>506</td><td>NuSTARJ110349-2326.2</td><td>26</td><td>0.173</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>507</td><td>NuSTARJ110354-2324.8</td><td>28</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected.</td></tr><tr><td>510</td><td>NuSTARJ110415-2328.6</td><td>26</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>513</td><td>NuSTARJ110526+7238.1</td><td>L</td><td>1.399</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Chu et al. (1998)</td></tr><tr><td>528</td><td>NuSTARJ111518+7935.7</td><td>9</td><td>0.693</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>529</td><td>NuSTARJ111822-6127.0</td><td>25</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; two potential soft X-ray counterparts associated with non-AGN WISE sources.</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>537</td><td>NuSTARJ112026+1340.4</td><td>S</td><td>0.984</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>540</td><td>NuSTARJ112745-2911.0</td><td>29</td><td>0.190</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>H&beta; + [O III] affected by chip gap.</td></tr><tr><td>547</td><td>NuSTARJ113253+5303.6</td><td>S</td><td>0.509</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>563</td><td>NuSTARJ114934-0413.6</td><td>30</td><td>0.341</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>564</td><td>NuSTARJ114948+5323.1</td><td>3</td><td>0.499</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>566</td><td>NuSTARJ114957+5320.1</td><td>3</td><td>0.233</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>568</td><td>NuSTARJ115658+5508.2</td><td>S</td><td>0.080</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Albareti et al. (2017).</td></tr><tr><td>570</td><td>NuSTARJ115809+5532.4</td><td>S</td><td>1.607</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>C IV BALQSO.</td></tr><tr><td>586</td><td>NuSTARJ120530+1649.9</td><td>3</td><td>0.216</td><td>BL/pair</td><td>...</td><td>1</td><td>C+P</td><td>1</td><td>AGN pair; WISEA J120530.63+164941.4 (Ahn et al. 2012; Toba et al. 2014); NL companion is on the edge of BPT composite region; associated with the NuSTAR science target (2MASX J12054771 +1651085; Darling & Giovanelli 2006).</td></tr><tr><td>587</td><td>NuSTARJ120539+1657.0</td><td>3</td><td>0.548</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>H&beta; + [O III] affected by A-band telluric feature.</td></tr><tr><td>588</td><td>NuSTARJ120551+1657.9</td><td>3</td><td>0.416</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Emission-line galaxy.</td></tr><tr><td>593</td><td>NuSTARJ121249+0659.7</td><td>S</td><td>0.210</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>612</td><td>NuSTARJ121932+4717.8</td><td>3</td><td>1.233</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>613</td><td>NuSTARJ122119+3015.8</td><td>S</td><td>0.646</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty; the closer CXO source to the NuSTAR detection is a SDSS BL at z = 0.531.</td></tr><tr><td>615</td><td>NuSTARJ122222+0416.4</td><td>S</td><td>1.190</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>624</td><td>NuSTARJ123755+1147.0</td><td>10</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected.</td></tr><tr><td>625</td><td>NuSTARJ123849-1614.4</td><td>30</td><td>...</td><td>...</td><td>F</td><td>0</td><td>P</td><td>2</td><td>Possibly incorrect counterpart based on WISE colors deficient soft X-ray information; continuum detected.</td></tr><tr><td>633</td><td>NuSTARJ125442-2657.1</td><td>L</td><td>0.0586</td><td>Gxy</td><td>...</td><td>1</td><td>C+P</td><td>1</td><td>Paturel et al. (2005); associated with the NuSTAR science target (2MASX J12545637-2657021 Parisi et al. 2014).</td></tr><tr><td>634</td><td>NuSTARJ125524+5656.2</td><td>S</td><td>1.189</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>641</td><td>NuSTARJ125631+5649.5</td><td>S</td><td>1.188</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Albareti et al. (2017).</td></tr><tr><td>651</td><td>NuSTARJ130432-1024.5</td><td>9</td><td>1.059</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>653</td><td>NuSTARJ130519-4934.2</td><td>31</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Flux calibration failure.</td></tr><tr><td>654</td><td>NuSTARJ130617-4021.5</td><td>26</td><td>1.052</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>672</td><td>NuSTARJ132139+0023.9</td><td>S</td><td>1.621</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>673</td><td>NuSTARJ132231-1647.4</td><td>25</td><td>0.349</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>674</td><td>NuSTARJ132240-1642.7</td><td>3</td><td>2.386</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>675</td><td>NuSTARJ132250-1645.1</td><td>3</td><td>0.656</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Possibly spurious feature at 4800 Å due to cosmic ray.</td></tr><tr><td>676</td><td>NuSTARJ132253-1636.7</td><td>25</td><td>1.631</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>678</td><td>NuSTARJ132455-3822.4</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>1</td><td>Bright in WISE W3-band.</td></tr><tr><td>680</td><td>NuSTARJ132525-3821.0</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>681</td><td>NuSTARJ132533-3828.7</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; WISE-XMM candidate identified with NWAY matches to a faint optical source.</td></tr><tr><td>682</td><td>NuSTARJ132535-3830.7</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>683</td><td>NuSTARJ132535-3825.6</td><td>L</td><td>0.445</td><td>GClstr</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty; Cluster of Galaxies; Burke et al. (2003).</td></tr><tr><td>689</td><td>NuSTARJ132939+4719.2</td><td>S</td><td>1.028</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>690</td><td>NuSTARJ133213-0511.7</td><td>10</td><td>0.481</td><td>BL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; XRT-WISE AGN candidate identified with NWAY; [O III]/H&beta; agrees with Type-2 AGN relation, but broad Mg II evident.</td></tr><tr><td>692</td><td>NuSTARJ133343-3400.1</td><td>27</td><td>2.715</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>BALQSO; C IV absorption.</td></tr><tr><td>694</td><td>NuSTARJ133401-3403.6</td><td>27</td><td>0.145</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>H&alpha; affected by A-band telluric feature.</td></tr><tr><td>699</td><td>NuSTARJ133843+4818.1</td><td>S</td><td>1.732</td><td>BL</td><td>...</td><td>0</td><td>P</td><td>1</td><td>Albareti et al. (2017).</td></tr><tr><td>700</td><td>NuSTARJ134547+7317.0</td><td>9</td><td>0.579</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty; H&beta; affected by A-band telluric feature.</td></tr><tr><td>710</td><td>NuSTARJ135345-0209.2</td><td>10</td><td>0.627</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>711</td><td>NuSTARJ135351-0204.2</td><td>28</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected; counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>713</td><td>NuSTARJ140459+2552.2</td><td>10</td><td>1.363</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>NALQSO; C IV and Mg II doublet absorption lines.</td></tr><tr><td>717</td><td>NuSTARJ140536+2551.7</td><td>S</td><td>0.943</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>729</td><td>NuSTARJ141842+2100.1</td><td>S</td><td>1.122</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>730</td><td>NuSTARJ141857+2105.1</td><td>4</td><td>0.895</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>731</td><td>NuSTARJ141914+2104.2</td><td>S</td><td>0.109</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Emission-line galaxy.</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>736</td><td>NuSTARJ142510+3320.4</td><td>S</td><td>0.258</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Galaxy spectrum with narrow Hα Emission-line; Albareti et al. (2017).</td></tr><tr><td>738</td><td>NuSTARJ142904+0120.4</td><td>S</td><td>0.101</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Ahn et al. (2012).</td></tr><tr><td>745</td><td>NuSTARJ143442-0144.6</td><td>3</td><td>0.285</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Star-forming galaxy (Driver et al. 2011).</td></tr><tr><td>746</td><td>NuSTARJ143517-0146.5</td><td>4</td><td>0.690</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Counterpart uncertainty due to deficient soft X-ray information WISE AGN candidates.</td></tr><tr><td>750</td><td>NuSTARJ143707+3639.5</td><td>S</td><td>0.861</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Early-type galaxy with strong oxygen lines.</td></tr><tr><td>759</td><td>NuSTARJ144932-4012.3</td><td>L</td><td>0.057</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Jones et al. (2009).</td></tr><tr><td>762</td><td>NuSTARJ145034+0508.3</td><td>S</td><td>1.635</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>769</td><td>NuSTARJ145452+0331.2</td><td>21</td><td>2.606</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>C IV affected by chip gap; potentially C IV BALQSO from SALT spectrum.</td></tr><tr><td>772</td><td>NuSTARJ145513+0322.7</td><td>S</td><td>0.423</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>774</td><td>NuSTARJ145528+0324.4</td><td>21</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected.</td></tr><tr><td>775</td><td>NuSTARJ145812-3133.4</td><td>31</td><td>...</td><td>...</td><td>F</td><td>0</td><td>...</td><td>1</td><td>Continuum detected.</td></tr><tr><td>785</td><td>NuSTARJ150225-4208.3</td><td>L</td><td>0.054</td><td>Gxy</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Jones et al. (2009).</td></tr><tr><td>787</td><td>NuSTARJ150334-4152.5</td><td>L</td><td>0.335</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Winkler & Long (1997).</td></tr><tr><td>788</td><td>NuSTARJ150516+0324.0</td><td>11</td><td>0.533</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>[O III] affected by A-band telluric feature.</td></tr><tr><td>789</td><td>NuSTARJ150529+0322.6</td><td>S</td><td>2.358</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>792</td><td>NuSTARJ150915+5702.2</td><td>15</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Counterpart uncertainty; require deeper optical/IR imaging.</td></tr><tr><td>794</td><td>NuSTARJ150937+5703.6</td><td>S</td><td>0.308</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>796</td><td>NuSTARJ151008+5705.8</td><td>S</td><td>0.548</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>The nominally closer W3-detected X-ray source is a galaxy at z = 0.272; Eckart et al. (2006).</td></tr><tr><td>798</td><td>NuSTARJ151148-1050.3</td><td>3</td><td>0.947</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>803</td><td>NuSTARJ151519+5615.6</td><td>9</td><td>0.490</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Counterpart uncertainty; XMM source is undetected with Keck; spectrum is a z = 0.490 emission-line galaxy at 3′′4 offset.</td></tr><tr><td>807</td><td>NuSTARJ151626+5620.7</td><td>S</td><td>1.349</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>813</td><td>NuSTARJ152548+4139.3</td><td>S</td><td>0.679</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>815</td><td>NuSTARJ152722+3600.2</td><td>S</td><td>0.269</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>819</td><td>NuSTARJ153601+5435.1</td><td>3</td><td>1.150</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>820</td><td>NuSTARJ153602-5749.0</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>821</td><td>NuSTARJ153632-5751.2</td><td>25</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information and high source density at low Galactic latitude.</td></tr><tr><td>824</td><td>NuSTARJ153640+5435.1</td><td>S</td><td>0.447</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>825</td><td>NuSTARJ153700+5434.2</td><td>4</td><td>1.315</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>829</td><td>NuSTARJ154407+2827.1</td><td>S</td><td>0.303</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>830</td><td>NuSTARJ154430+2828.1</td><td>S</td><td>0.231</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>849</td><td>NuSTARJ160817+1221.4</td><td>10</td><td>0.181</td><td>NL</td><td>...</td><td>0</td><td>P</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; W3-detected target seems correct.</td></tr><tr><td>850</td><td>NuSTARJ160832+1222.4</td><td>10</td><td>0.944</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Mg II affected by chip gap; WISEA J160833.89 +122216.7.</td></tr><tr><td>852</td><td>NuSTARJ161404+4702.8</td><td>S</td><td>0.551</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Albareti et al. (2017).</td></tr><tr><td>853</td><td>NuSTARJ161417+4701.8</td><td>23</td><td>0.151</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>854</td><td>NuSTARJ161424+4709.3</td><td>S</td><td>1.502</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>C IV BALQSO.</td></tr><tr><td>855</td><td>NuSTARJ161445+4659.3</td><td>23</td><td>0.153</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>857</td><td>NuSTARJ161548+2210.9</td><td>S</td><td>1.698</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>860</td><td>NuSTARJ161723+3225.2</td><td>4</td><td>1.028</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; NWAY disagreement; a post-starburst galaxy.</td></tr><tr><td>867</td><td>NuSTARJ162035+8530.3</td><td>10</td><td>0.258</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>881</td><td>NuSTARJ163108+2350.1</td><td>11</td><td>0.038</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; associated with a known local starburst; difficult to assess due to deficient soft X-ray information.</td></tr><tr><td>882</td><td>NuSTARJ163114+2358.1</td><td>S</td><td>0.038</td><td>Gxy</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Albareti et al. (2017).</td></tr><tr><td>883</td><td>NuSTARJ163126+2357.0</td><td>10</td><td>0.751</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>886</td><td>NuSTARJ164323+3948.4</td><td>S</td><td>0.0306</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Galaxy spectrum with narrow Hα emission line.</td></tr><tr><td>890</td><td>NuSTARJ164503+2624.9</td><td>S</td><td>0.127</td><td>NL</td><td>...</td><td>0</td><td>P</td><td>1</td><td>Broad + narrow Hα emission line; galaxy shining through.</td></tr><tr><td>892</td><td>NuSTARJ164511+2620.4</td><td>S</td><td>1.168</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>894</td><td>NuSTARJ164718+2103.5</td><td>4</td><td>0.882</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>NALQSO; Mg II λλ2796,2803 absorption doublets.</td></tr><tr><td>895</td><td>NuSTARJ164724+2105.5</td><td>4</td><td>0.788</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>897</td><td>NuSTARJ165059+0440.5</td><td>10</td><td>0.299</td><td>BL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; two AGN-like WISE candidates within XRT error circle.</td></tr><tr><td>913</td><td>NuSTARJ165315-0158.3</td><td>9</td><td>0.189</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>915</td><td>NuSTARJ165349-0154.8</td><td>11</td><td>0.627</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>916</td><td>NuSTARJ165414+3949.9</td><td>S</td><td>1.636</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>917</td><td>NuSTARJ165417+3946.8</td><td>S</td><td>0.354</td><td>NL?</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Adelman-McCarthy et al. (2008).</td></tr><tr><td>924</td><td>NuSTARJ165825+5855.8</td><td>23</td><td>0.105</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; CXO source (NWAY) is the more probable counterpart.</td></tr><tr><td>929</td><td>NuSTARJ170632-6138.4</td><td>26</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty based on WISE colors and multiple candidates within XRT error circle.</td></tr><tr><td>947</td><td>NuSTARJ172405+5058.4</td><td>23</td><td>0.298</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>968</td><td>NuSTARJ175307-0123.7</td><td>28</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>974</td><td>NuSTARJ180958-4552.6</td><td>L</td><td>0.070</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Flat-Spectrum Radio Source; blazar (Healey et al. 2007; Jones et al. 2009); reported in Swift-BAT BASS DR2 (Koss et al. 2022).</td></tr><tr><td>978</td><td>NuSTARJ181313-1240.0</td><td>17</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C+P</td><td>1</td><td>Continuum detected; heavily reddened source.</td></tr><tr><td>997</td><td>NuSTARJ182622-1446.6</td><td>15</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Counterpart uncertainty; all three bright objects are Galactic sources.</td></tr><tr><td>1001</td><td>NuSTARJ183042+0931.1</td><td>6</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1002</td><td>NuSTARJ183052+0925.3</td><td>6</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1005</td><td>NuSTARJ183250-0913.9</td><td>13</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to high source density at low Galactic latitude problematic WISE imaging.</td></tr><tr><td>1009</td><td>NuSTARJ183428+3239.4</td><td>4</td><td>0.292</td><td>Gxy</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Possibly two sources contributing to NuSTAR detection; early-type galaxy with hints of [NII] emission.</td></tr><tr><td>1018</td><td>NuSTARJ183511+4357.9</td><td>23</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Unusual WISE (bright in W3) optical colors for Galactic source.</td></tr><tr><td>1043</td><td>NuSTARJ184449+7212.1</td><td>23</td><td>1.298</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1045</td><td>NuSTARJ184552+8428.2</td><td>23</td><td>0.233</td><td>NL/pair</td><td>...</td><td>1</td><td>...</td><td>1</td><td>NL AGN with an early-type galaxy companion at the same redshift (NWAY position); associated with the NuSTAR science target (1RXS J184642.2+842506; Bauer et al. 2000; Koss et al. 2022).</td></tr><tr><td>1047</td><td>NuSTARJ184628+7214.2</td><td>23</td><td>0.750</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1048</td><td>NuSTARJ185528+0123.7</td><td>21</td><td>...</td><td>...</td><td>F</td><td>0</td><td>P</td><td>1</td><td>Red continuum</td></tr><tr><td>1049</td><td>NuSTARJ185544+0124.7</td><td>32</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty and NWAY disagreement; require deeper optical/IR data.</td></tr><tr><td>1055</td><td>NuSTARJ190642+0917.5</td><td>15</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to high source density at low Galactic latitude.</td></tr><tr><td>1057</td><td>NuSTARJ190813-3925.7</td><td>31</td><td>0.075</td><td>Gxy</td><td>...</td><td>1</td><td>C</td><td>1</td><td>Hα lost to chip gap; associated with the NuSTAR science target (2MASX J19075035-3923315 Jones et al. 2009; Malizia et al. 2012).</td></tr><tr><td>1061</td><td>NuSTARJ192215-5844.9</td><td>30</td><td>0.231</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1069</td><td>NuSTARJ192607+4134.1</td><td>23</td><td>0.777</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1092</td><td>NuSTARJ194226-1016.0</td><td>5</td><td>0.449</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1093</td><td>NuSTARJ194234-1011.9</td><td>13</td><td>0.849</td><td>NL?</td><td>B</td><td>0</td><td>C+P</td><td>1</td><td>Emission-line galaxy; possible obscured AGN; tentative C III, [Ne V] and [O III] detections at z = 0.849.</td></tr><tr><td>1098</td><td>NuSTARJ195204+0234.6</td><td>23</td><td>1.168</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1100</td><td>NuSTARJ195221+2930.2</td><td>7</td><td>...</td><td>...</td><td>F</td><td>0</td><td>P</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; red continuum.</td></tr><tr><td>1108</td><td>NuSTARJ200727-4431.6</td><td>26</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected.</td></tr><tr><td>1109</td><td>NuSTARJ200735-4436.6</td><td>31</td><td>0.405</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; [O III] affected by chip gap.</td></tr><tr><td>1110</td><td>NuSTARJ200755-4439.7</td><td>25</td><td>0.456</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1111</td><td>NuSTARJ200821-4437.9</td><td>25</td><td>0.524</td><td>NL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1113</td><td>NuSTARJ201501+3710.8</td><td>4</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to high source density; possibly incorrect based on XRT-WISE NWAY candidate.</td></tr><tr><td>1115</td><td>NuSTARJ201536+3704.9</td><td>4</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty given the high source density at low Galactic latitude.</td></tr><tr><td>1116</td><td>NuSTARJ201545+3714.3</td><td>4</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>1</td><td>Ultra-red source; heavily embedded.</td></tr><tr><td>1118</td><td>NuSTARJ201645+5810.7</td><td>24</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>P</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information.</td></tr><tr><td>1119</td><td>NuSTARJ201727+5815.5</td><td>24</td><td>0.278</td><td>NL?</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>1124</td><td>NuSTARJ202029+4356.8</td><td>24</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>2</td><td>Red continuum detected for the second source in the WISE error circle.</td></tr><tr><td>1128</td><td>NuSTARJ202108+6136.5</td><td>23</td><td>1.553</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Counterpart uncertainty; two stars, possibly not the X-ray emitter.</td></tr><tr><td>1129</td><td>NuSTARJ202226+6141.3</td><td>23</td><td>0.259</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1140</td><td>NuSTARJ203353+6010.9</td><td>7</td><td>1.863</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1147</td><td>NuSTARJ204256+7503.1</td><td>13</td><td>...</td><td>Hotspot</td><td>F</td><td>0</td><td>...</td><td>2</td><td>Hotspot of 4C 74.26 (science target), a radio quasar at z = 0.104 (Erlund et al. 2010).</td></tr><tr><td>1154</td><td>NuSTARJ210737-0512.1</td><td>21</td><td>0.841</td><td>BL?</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Strong [O III] lines, but broad Mg II detected; Akiyama et al. (2003).</td></tr><tr><td>1156</td><td>NuSTARJ211152+8210.4</td><td>11</td><td>0.421</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hα affected by telluric feature.</td></tr><tr><td>1157</td><td>NuSTARJ211421+0605.5</td><td>24</td><td>0.216</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1168</td><td>NuSTARJ212807+5649.5</td><td>12</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1171</td><td>NuSTARJ212931-0431.4</td><td>4</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1172</td><td>NuSTARJ212954-0425.4</td><td>4</td><td>2.065</td><td>BL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to multiple XMM/WISE AGN candidates; NALQSO; C III] affected by telluric feature.</td></tr><tr><td>1173</td><td>NuSTARJ212956-0435.5</td><td>31</td><td>0</td><td>Galactic</td><td>B</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; potentially spurious NuSTAR detection.</td></tr><tr><td>1174</td><td>NuSTARJ213005-0427.4</td><td>4</td><td>0.277</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Quasar with host galaxy showing through.</td></tr><tr><td>1175</td><td>NuSTARJ213309+5106.5</td><td>22</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1176</td><td>NuSTARJ213347+5112.1</td><td>23</td><td>0.168</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hα affected by A-band telluric feature.</td></tr><tr><td>1178</td><td>NuSTARJ213900-2640.4</td><td>28</td><td>0.551</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hβ affected by telluric feature.</td></tr><tr><td>1180</td><td>NuSTARJ214239+4330.9</td><td>5</td><td>0.0174</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>NED counterpart with same spec-z but quality B estimated; WISEA J214238.71+433057.9.</td></tr><tr><td>1181</td><td>NuSTARJ214320+4334.8</td><td>5</td><td>0.0131</td><td>NL</td><td>...</td><td>0</td><td>P</td><td>1</td><td>NED counterpart; UGC11797 (Seeberger et al. 1994).</td></tr><tr><td>1185</td><td>NuSTARJ214755+0651.8</td><td>24</td><td>0.182</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1186</td><td>NuSTARJ214758-3502.4</td><td>29</td><td>0.439</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; Hβ affected by chip gap.</td></tr><tr><td>1194</td><td>NuSTARJ220039+1039.7</td><td>24</td><td>1.389</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1204</td><td>NuSTARJ221133+1841.5</td><td>S</td><td>0.578</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1205</td><td>NuSTARJ221457-3842.5</td><td>28</td><td>0.800</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1206</td><td>NuSTARJ221716+0051.1</td><td>19</td><td>1.934</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Also observed in SDSS-DR16 but with lower S/N; C III] affected by chip gap.</td></tr><tr><td>1207</td><td>NuSTARJ221735-0820.7</td><td>S</td><td>0.085</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Galaxy shining through Adelman-McCarthy et al. (2008).</td></tr><tr><td>1208</td><td>NuSTARJ222348-0201.4</td><td>4</td><td>0.274</td><td>NL</td><td>...</td><td>0</td><td>P</td><td>2</td><td>Counterpart uncertainty; NWAY disagreement; lack soft X-ray detection; emission-line galaxy.</td></tr><tr><td>1212</td><td>NuSTARJ223536+3359.0</td><td>21</td><td>0.485</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1213</td><td>NuSTARJ223538-2554.9</td><td>27</td><td>0.429</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; require spectrum of NWAY candidate for further assessment.</td></tr><tr><td>1214</td><td>NuSTARJ223547-2558.7</td><td>L</td><td>0.304</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>SyI galaxy (Caccianiga et al. 2008; Lin et al. 2012).</td></tr><tr><td>1215</td><td>NuSTARJ223630+3425.9</td><td>24</td><td>1.767</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>Mg II affected by A-band telluric feature.</td></tr><tr><td>1216</td><td>NuSTARJ223653+3423.6</td><td>24</td><td>0.149</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Hβ affected by chip gap.</td></tr><tr><td>1220</td><td>NuSTARJ223728+3425.6</td><td>24</td><td>1.571</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1224</td><td>NuSTARJ224200-4539.3</td><td>28</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>2</td><td>Counterpart uncertainty; difficult to assess due to deficient soft X-ray information. Hβ + [O III] lost to chip gap.</td></tr><tr><td>1228</td><td>NuSTARJ224230+2939.4</td><td>23</td><td>0.120</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1230</td><td>NuSTARJ224239-3707.9</td><td>28</td><td>0.222</td><td>BL</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1232</td><td>NuSTARJ224252+2941.5</td><td>24</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1233</td><td>NuSTARJ224252+2937.0</td><td>S</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected.</td></tr><tr><td>1236</td><td>NuSTARJ224306+2941.4</td><td>23</td><td>0.158</td><td>Gxy</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; Hβ lost to chip gap; Hα lost to A-band telluric feature.</td></tr><tr><td>1237</td><td>NuSTARJ224536+3947.1</td><td>8</td><td>0.081</td><td>NL</td><td>...</td><td>1</td><td>C+P</td><td>1</td><td>2MASX J22453396+3946591 (Bilicki et al. 1996); associated with the NuSTAR science target (3C 452 Véron-Cetty & Véron 2006).</td></tr><tr><td>1238</td><td>NuSTARJ224618+3941.6</td><td>7</td><td>0.341</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1240</td><td>NuSTARJ224925-1917.5</td><td>1</td><td>0.444</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1242</td><td>NuSTARJ225513-0302.4</td><td>19</td><td>0.797</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1245</td><td>NuSTARJ230147-5920.8</td><td>32</td><td>0.366</td><td>BL?</td><td>...</td><td>0</td><td>C</td><td>1</td><td>...</td></tr><tr><td>1246</td><td>NuSTARJ230443+1216.4</td><td>4</td><td>1.410</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Véron-Cetty & Véron (2010).</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>ID<br>(1)</th><th>NuSTAR Name<br>(2)</th><th>Run<br>(3)</th><th>z<br>(4)</th><th>Type<br>(5)</th><th>Quality<br>(6)</th><th>PFlag<br>(7)</th><th>NWAY<br>(8)</th><th>F<sub>Cpart</sub><br>(9)</th><th>Notes</th></tr></thead><tbody><tr><td>1255</td><td>NuSTARJ232728-0047.1</td><td>19</td><td>0.217</td><td>NL?</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>...</td></tr><tr><td>1257</td><td>NuSTARJ233200+0016.0</td><td>S</td><td>0.352</td><td>BL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Ahn et al. (2012).</td></tr><tr><td>1258</td><td>NuSTARJ233221+0020.8</td><td>19</td><td>1.853</td><td>NL</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>High-redshift Type-2 quasar.</td></tr><tr><td>1261</td><td>NuSTARJ233917-0537.2</td><td>7</td><td>...</td><td>...</td><td>F</td><td>0</td><td>C</td><td>1</td><td>Continuum detected.</td></tr><tr><td>1262</td><td>NuSTARJ233948-0536.6</td><td>5</td><td>0</td><td>Galactic</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty; other non-AGN WISE source in field is a galaxy at z = 0.413.</td></tr><tr><td>1263</td><td>NuSTARJ235538+3008.2</td><td>23</td><td>0.556</td><td>NL</td><td>...</td><td>0</td><td>...</td><td>2</td><td>Counterpart uncertainty due to deficient soft X-ray information; Hβ affected by A-band telluric feature.</td></tr><tr><td>1264</td><td>NuSTARJ235553+3015.0</td><td>24</td><td>0.874</td><td>BL?</td><td>...</td><td>0</td><td>C+P</td><td>1</td><td>Faint continuum detected with tentatively broad Mg II and weak oxygen lines.</td></tr><tr><td>1272</td><td>NuSTARJ235806-3237.9</td><td>25</td><td>0.795</td><td>BL</td><td>B</td><td>0</td><td>C</td><td>1</td><td>...</td></tr></tbody></table>

**Notes.** Columns: (1): unique NuSTAR source ID. (2): unique NuSTAR source name. (3): spectroscopic follow-up observing code; see Table 6. (4): spectroscopic redshift. (5): spectroscopic classification: BL ≡ broad-line object (i.e., quasar); NL ≡ narrow-line object (AGN or galaxy); Gxy ≡ galaxy (absorption lines); Galactic ≡ Galactic sources at z = 0; see Section 3.3.3. (6): spectroscopic redshift quality: F ≡ faint continuum detected; B ≡ single-line redshift measurement; C ≡ photometric redshift. (7): binary flag to indicate association to the NuSTAR science target, i.e., sources with a velocity offset from the science target smaller than 5% of the total science target velocity. (8): flag indicating whether the spectroscopic target matches to the CatWISE20 and/or PS1 NWAY-identified counterparts: C+P ≡ CatWISE20 + PS1; C ≡ CatWISE20 only; P ≡ PS1 only. (9): flag indicating the reliability of the identified spectroscopic counterpart: 0 ≡ unreliable; 1 ≡ reliable; 2 ≡ counterpart uncertainty.

The columns are described in Section E.1. Details for NSS40 sources are tabulated in Table 6 in L17.

order of increasing R.A. Shown on the top are the unique NuSTAR ID and source name, in the upper-left corner the observing telescope and run identification number (corresponding to Table 6), and in the upper-right corner the source classification and redshift. All CatWISE detections are shown with “×” marks, colored green. The NuSTAR 25" and 30" error circles are plotted in a dashed-dotted and solid black line, respectively. All PS1-DR2 detections are shown with “plus” marks, colored pink. The X-ray position is marked with the respective error circle, the CatWISE20 position is indicated with a green 2" error circle, the PS1-DR2 position is shown with a purple 2" error circle, and the spectroscopic target is marked with a red “crosshair” corresponding to the black spectrum in the left panel. Where a second spectrum is available, the spectrum, observation details, and target position are shown in peach.

## E.2. Optical Finding Charts for the Spectroscopic NSS40 Sources

Figure E6 shows optical finding charts for the first 12 NSS80 sources with measurements from literature. Figure E7 shows charts for the first 12 spectroscopically followed-up NSS40 sources reported in L17; the finding charts for the full sample are available online. Following the color scheme of Section E.1, all WISE detections are shown with “×” marks, and PS1-DR2 detections with “plus” marks. The NuSTAR 25" and 30" error circles are plotted in a dashed-dotted and solid black line, respectively. The X-ray position is marked with the respective error circle, the CatWISE20 position is indicated with a green 2" error circle, the PS1-DR2 position is shown with a purple 2" error circle, and the spectroscopic target is marked with a red “crosshair.”
<figure><img src="image_37.png" /></figure>

$\log(P_{\text{false, min}}) = -10.48$

<figure><img src="image_38.png" /></figure>

(RA, Decl.) = (1.099°, 70.284°)

<figure><img src="image_39.png" /></figure>

$\log(P_{\text{false, min}}) = -6.05$

<figure><img src="image_40.png" /></figure>

(RA, Decl.) = (1.456°, 20.219°)

<figure><img src="image_41.png" /></figure>

$\log(P_{\text{false, min}}) = -28.88$

<figure><img src="image_42.png" /></figure>

(RA, Decl.) = (3.680°, 81.537°)

<figure><img src="image_43.png" /></figure>

$\log(P_{\text{false, min}}) = -13.52$

<figure><img src="image_44.png" /></figure>

(RA, Decl.) = (4.966°, -70.950°)

<caption>**Figure E1.** Optical spectra for the first four extragalactic post-NSS40 sources classified as BL AGNs in order of NuSTAR ID. The symbol key is described in Appendix E.1.</caption>
<figure><img src="image_45.png" /><figcaption>**Figure E2.** Optical spectra for the first four extragalactic post-NSS40 sources classified as NL AGNs. The symbol key is described in Appendix E.1.</figcaption></figure>
<figure><img src="image_46.png" /><figcaption>**Figure E3.** Optical spectra for the first four extragalactic post-NSS40 sources classified as galaxies (i.e., absorption spectral features). The symbol key is described in Appendix E.1.</figcaption></figure>
<figure><img src="image_47.png" /><figcaption>**Figure E4.** Optical spectra for the first four Galactic post-NSS40 sources ($z=0$). The symbol key is described in Appendix E.1.</figcaption></figure>
<figure><img src="image_48.png" /><figcaption>**Figure E5.** Optical spectra for the first four unclassified post-NSS40 sources which lacks a redshift measurement; in some cases a red faint continuum is detected. The symbol key is described in Appendix E.1.</figcaption></figure>
131 | NuSTARJ031015-7651.5

<figure><img src="image_49.png" /></figure>

489 | NuSTARJ103135-4206.0

<figure><img src="image_50.png" /></figure>

683 | NuSTARJ132535-3825.6

<figure><img src="image_51.png" /></figure>

848 | NuSTARJ160605-7252.6

<figure><img src="image_52.png" /></figure>

290 | NuSTARJ062728-3527.9

<figure><img src="image_53.png" /></figure>

513 | NuSTARJ110526+7238.1

<figure><img src="image_54.png" /></figure>

739 | NuSTARJ143012+3318.9

<figure><img src="image_55.png" /></figure>

858 | NuSTARJ161603+2211.9

<figure><img src="image_56.png" /></figure>

485 | NuSTARJ102651+2545.0

<figure><img src="image_57.png" /></figure>

633 | NuSTARJ125442-2657.1

<figure><img src="image_58.png" /></figure>

787 | NuSTARJ150334-4152.5

<figure><img src="image_59.png" /></figure>

889 | NuSTARJ164444+2625.8

<figure><img src="image_60.png" /></figure>

**Figure E6.** 30" × 30" finding charts for the first 12 NSS80 sources with redshift measurements from the literature. For sources with decl. > −30° Pan-STARRS i-band imaging is used, and for sources with decl. < −30° Astro Data Lab (Fitzpatrick et al. 2014; Nikutta et al. 2020) i-band imaging is retrieved. The symbol key is described in Appendix E.1. Optical classifications for sources with photometric redshifts are appended with a “C” (i.e., GxyC = galaxy candidate; BLC = BL candidate). Also identified is a galaxy cluster (GClstr) at z = 0.445.
1 | NuSTARJ000011-7652.5

<figure><img src="image_61.png" /></figure>

13 | NuSTARJ001858-1022.7

<figure><img src="image_62.png" /></figure>

32 | NuSTARJ005332+7304.0

<figure><img src="image_63.png" /></figure>

54 | NuSTARJ011103-4602.7

<figure><img src="image_64.png" /></figure>

11 | NuSTARJ001542+8134.4

<figure><img src="image_65.png" /></figure>

23 | NuSTARJ002227-1854.7

<figure><img src="image_66.png" /></figure>

35 | NuSTARJ005408+7303.2

<figure><img src="image_67.png" /></figure>

59 | NuSTARJ012215+5002.2

<figure><img src="image_68.png" /></figure>

12 | NuSTARJ001852-1026.1

<figure><img src="image_69.png" /></figure>

24 | NuSTARJ002544+6818.8

<figure><img src="image_70.png" /></figure>

52 | NuSTARJ011042-4604.3

<figure><img src="image_71.png" /></figure>

66 | NuSTARJ012809-1851.6

<figure><img src="image_72.png" /></figure>

**Figure E7.** 30" × 30" finding charts for the first 12 optically followed-up NSS40 sources reported in L17. For sources with decl. > −30° Pan-STARRS i-band imaging is used, and for sources with decl. < −30° Astro Data Lab i-band imaging is retrieved. The symbol key is described in Appendix E.1.
ORCID iDs

Claire L. Greenwell https://orcid.org/0000-0002-7719-5809

Lizelke Klindt https://orcid.org/0000-0001-9307-9026

George B. Lansbury https://orcid.org/0000-0002-5328-9827

David J. Rosario https://orcid.org/0000-0002-0001-3587

David M. Alexander https://orcid.org/0000-0002-5896-6313

James Aird https://orcid.org/0000-0003-1908-8463

Daniel Stern https://orcid.org/0000-0003-2686-9241

Michael J. Koss https://orcid.org/0000-0002-7998-9581

Franz E. Bauer https://orcid.org/0000-0002-8686-8737

John Tomsick https://orcid.org/0000-0001-5506-9855

William N. Brandt https://orcid.org/0000-0002-0167-2453

Thomas Connor https://orcid.org/0000-0002-7898-7664

Peter G. Boorman https://orcid.org/0000-0001-9379-4716

David R. Ballantyne https://orcid.org/0000-0001-8128-6976

Chien-Ting Chen https://orcid.org/0000-0002-4945-5079

Francesca Civano https://orcid.org/0000-0002-2115-1137

Andrea Comastri https://orcid.org/0000-0003-3451-9970

Victoria A. Fawcett https://orcid.org/0000-0003-1251-532X

Francesca M. Formasini https://orcid.org/0000-0002-9286-9963

Poshak Gandhi https://orcid.org/0000-0003-3105-2615

Marianne Heida https://orcid.org/0000-0002-1082-7496

Ryan Hickox https://orcid.org/0000-0003-1468-9526

Elias S. Kammoun https://orcid.org/0000-0002-0273-218X

Lauranne Lanz https://orcid.org/0000-0002-3249-8224

Stefano Marchesi https://orcid.org/0000-0001-5544-0749

Encarni Romero-Colmenero https://orcid.org/0000-0003-0607-1136

Ezequiel Treister https://orcid.org/0000-0001-7568-6412

C. Megan Urry https://orcid.org/0000-0002-0745-9792

Petri Väisänen https://orcid.org/0000-0001-7673-4850

Brian van Soelen https://orcid.org/0000-0003-1873-7855

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