Correction to: Searching for magnetar binaries disrupted by core-collapse supernovae

The recent publication Sherman et al. (2024) contains minor errata in the position uncertainties used for magnetars 1E 1547.0–5408, AX J1818.8–1559 and PSR J1846–0258 which we address here. During re-analysis of these sources, an additional bug was found which truncated queries of the UKIDSS point source catalogue for the IR bound stellar companion search. We correct these in the sections below, and find they have not altered the conclusions of Sherman et al. (2024). The incorrect position errors for magnetars 1E 1547.0–5408, AX J1818.8–1559, and PSR J1846–0258 were listed in table 1 and used in the Monte Carlo simulations. For 1E 1547.0–5408, this resulted from a failure to convert the units of the RA and declination from seconds and arcseconds, respectively, to degrees when copying the values from Deller et al. (2012). The systematic uncertainties from astrometric fitting were also neglected. The correct errors, summing the fit and calibrator position errors in quadrature, are |$\sigma _{\alpha }=15{\rm cos}(\delta)\sqrt{0{_{.}^{\rm s}}00005^2 + 0{_{.}^{\rm s}}00064^2}=0{_{.}^{\prime\prime}} 0056$| (where |$\delta =-54^{\circ }18^\prime 24{_{.}^{\prime\prime}} 11$| is the declination converted to radians) and |$\sigma _{\delta }=\sqrt{0{_{.}^{\prime\prime}} 0003^2 + 0{_{.}^{\prime\prime}} 0020^2}=0{_{.}^{\prime\prime}} 0020$|⁠. For AX J1818.8–1559, a factor of |$\cos (\delta)$| (where |$\delta = -15^\circ 59^\prime 22{_{.}^{\prime\prime}} 62$| in radians) was neglected in converting the RA uncertainty from seconds to arcseconds. However, the systematic uncertainty of |$0{_{.}^{\prime\prime}}6$| on the Chandra X-ray Observatory (CXO) position was also neglected in both RA and declination. This dominates the position uncertainties, and thus we use |$0{_{.}^{\prime\prime}}6$| as the corrected position error. Similarly, for PSR J1846–0258, the factor of |$\cos (\delta)$| was neglected in converting the RA uncerainty from seconds to arcseconds. Since for this source, |$\cos (\delta)=0.998$| (where |$\delta = -02^\circ 58^\prime 30{_{.}^{\prime\prime}} 10$| in radians), the change is small and the correct RA uncertainty rounded to two decimal places is still |$15\cos (\delta)(0{_{.}^{\rm s}}01) = 0{_{.}^{\prime\prime}} 15$|⁠. We provide the corrected table, with the revised position errors boldfaced, in Table 1. Magnetars and magnetar candidates from the McGill catalogue (revised position errors are boldfaced for clarity). Note. Abbreviated magnetar names are given with full names in parentheses, which are used throughout this work. RA (⁠|$\alpha$|⁠), declination (⁠|$\delta$|⁠), and distance are taken from the McGill magnetar catalogue (Olausen & Kaspi 2014), while proper motions (⁠|$\mu _\alpha {\rm cos}(\delta)$| and |$\mu _{\delta }$|⁠) were found in the available literature. Italicized entries are unconfirmed magnetar candidates and boldfaced entries have confirmed or proposed supernova remnant associations. Proposed associations are indicated by a |$^{*}$|⁠. |$A_V$| extinction estimates are from the Bayestar19 map for magnetars with |$\delta \gtrsim -30^\circ$|⁠. Magnetars outside this range have |$A_V\!$| from the X-ray column density |$N_{\rm H}$| (indicated by a |$^\ddagger$|⁠) using the Predehl & Schmitt (1995) relation: |$A_V\approx (5.59\times 10^{-22}\, {\rm cm}^{2})N_{\rm H}$|⁠. If no |$N_{\rm H}$| measurement is available, we list the median |$A_V$| from Gaia GSP photometry for massive sources within |$1^\circ$| (indicated by a |$^\dagger$|⁠; see section 3 for details). Relevant citations referenced in the rightmost column are below: (1) Haschke, Grebel & Duffau (2012); (2) Lamb et al. (2002); (3) Durant & van Kerkwijk (2006); (4) Hulleman, Van Kerkwijk & Kulkarni (2004); (5) Tendulkar, Cameron & Kulkarni (2013); (6) van der Horst et al. (2010); (7) Lin et al. (2011); (8) Göǧüş et al. (2010b); (9) Gaensler & Chatterjee (2008); (10) Kulkarni et al. (2003); (11) Klose et al. (2004); (12) Wang & Chakrabarty (2002); (13) Gaensler et al. (2005); (14) Tiengo et al. (2010); (15) Deller et al. (2012); (16) Gelfand & Gaensler (2007); (17) Levin et al. (2010); (18) Anderson et al. (2012); (19) Corbel et al. (1999); (20) Wachter et al. (2004); (21) Kothes & Dougherty (2008); (22) Muno et al. (2006); (23) Israel et al. (2003); (24) Tian & Leahy (2012); (25) Halpern & Gotthelf (2010a); (26) Halpern & Gotthelf (2010b); (27) Bower et al. (2014); (28) Mori et al. (2013); (29) Shannon & Johnston (2013); (30) Bower et al. (2015); (31) Bibby et al. (2008); (32) Israel et al. (2005); (33) Tendulkar, Cameron & Kulkarni (2012); (34) Minter et al. (2008); (35) Helfand et al. (2007); (36) Karuppusamy et al. (2020); (37) Stamatikos et al. (2020); (38) Ding et al. (2020a); (39) Scholz et al. (2012); (40) Pagani, Beardmore & Kennea (2011); (41) Göǧüş et al. (2010a); (42) Leahy & Tian (2008a); (43) Kargaltsev et al. (2012); (44) Tian & Leahy (2008); (45) Wachter et al. (2004); (46) Vasisht & Gotthelf (1997); (47) Zhou et al. (2014); (48) Davies et al. (2009); (49) Frail, Kulkarni & Bloom (1999); (50) Gaensler (2014); (51) Israel et al. (2016); (52) Zhong et al. (2020); (53) Kothes & Foster (2012); (54) Fahlman & Gregory (1981); (55) Hulleman et al. (2001); (56) Barthelmy et al. (2016); (57) Doroshenko et al. (2021); (58) Richardson et al. (2023); (59) Cline et al. (2000); (60) Lamb et al. (2003); (61) Mereghetti et al. (2012); (62) Torii et al. (1998); (63) Gaensler, Gotthelf & Vasisht (1999); (64) Tam et al. (2006); (65) Sakamoto et al. (2011); (66) Leahy & Tian (2007); (67) Gotthelf et al. (2000); (68) Helfand, Collins & Gotthelf (2003); (69) Blumer et al. (2019); (70) Lin, Webb & Barret (2012); (71) Roming et al. (2008); (72) Barthelmy et al. (2016); (73) Jing et al. (2023); (74) Ponti et al. (2015); (75) Yalinewich, Piran & Sari (2017); (76) Cline et al. (1982); (77) Park et al. (2012); (78) Park et al. (2020); (79) Sano et al. (2023); (80) Borkowski & Reynolds (2017); (81) Zhou et al. (2019); (82) Kothes et al. (2018); (83) Zhou et al. (2020); (84) Nakano et al. (2017); (85) Leahy & Tian (2008b); (86) Straal, Gelfand & Eagle (2023); and (87) Ding et al. (2020b). Magnetars and magnetar candidates from the McGill catalogue (revised position errors are boldfaced for clarity). Note. Abbreviated magnetar names are given with full names in parentheses, which are used throughout this work. RA (⁠|$\alpha$|⁠), declination (⁠|$\delta$|⁠), and distance are taken from the McGill magnetar catalogue (Olausen & Kaspi 2014), while proper motions (⁠|$\mu _\alpha {\rm cos}(\delta)$| and |$\mu _{\delta }$|⁠) were found in the available literature. Italicized entries are unconfirmed magnetar candidates and boldfaced entries have confirmed or proposed supernova remnant associations. Proposed associations are indicated by a |$^{*}$|⁠. |$A_V$| extinction estimates are from the Bayestar19 map for magnetars with |$\delta \gtrsim -30^\circ$|⁠. Magnetars outside this range have |$A_V\!$| from the X-ray column density |$N_{\rm H}$| (indicated by a |$^\ddagger$|⁠) using the Predehl & Schmitt (1995) relation: |$A_V\approx (5.59\times 10^{-22}\, {\rm cm}^{2})N_{\rm H}$|⁠. If no |$N_{\rm H}$| measurement is available, we list the median |$A_V$| from Gaia GSP photometry for massive sources within |$1^\circ$| (indicated by a |$^\dagger$|⁠; see section 3 for details). Relevant citations referenced in the rightmost column are below: (1) Haschke, Grebel & Duffau (2012); (2) Lamb et al. (2002); (3) Durant & van Kerkwijk (2006); (4) Hulleman, Van Kerkwijk & Kulkarni (2004); (5) Tendulkar, Cameron & Kulkarni (2013); (6) van der Horst et al. (2010); (7) Lin et al. (2011); (8) Göǧüş et al. (2010b); (9) Gaensler & Chatterjee (2008); (10) Kulkarni et al. (2003); (11) Klose et al. (2004); (12) Wang & Chakrabarty (2002); (13) Gaensler et al. (2005); (14) Tiengo et al. (2010); (15) Deller et al. (2012); (16) Gelfand & Gaensler (2007); (17) Levin et al. (2010); (18) Anderson et al. (2012); (19) Corbel et al. (1999); (20) Wachter et al. (2004); (21) Kothes & Dougherty (2008); (22) Muno et al. (2006); (23) Israel et al. (2003); (24) Tian & Leahy (2012); (25) Halpern & Gotthelf (2010a); (26) Halpern & Gotthelf (2010b); (27) Bower et al. (2014); (28) Mori et al. (2013); (29) Shannon & Johnston (2013); (30) Bower et al. (2015); (31) Bibby et al. (2008); (32) Israel et al. (2005); (33) Tendulkar, Cameron & Kulkarni (2012); (34) Minter et al. (2008); (35) Helfand et al. (2007); (36) Karuppusamy et al. (2020); (37) Stamatikos et al. (2020); (38) Ding et al. (2020a); (39) Scholz et al. (2012); (40) Pagani, Beardmore & Kennea (2011); (41) Göǧüş et al. (2010a); (42) Leahy & Tian (2008a); (43) Kargaltsev et al. (2012); (44) Tian & Leahy (2008); (45) Wachter et al. (2004); (46) Vasisht & Gotthelf (1997); (47) Zhou et al. (2014); (48) Davies et al. (2009); (49) Frail, Kulkarni & Bloom (1999); (50) Gaensler (2014); (51) Israel et al. (2016); (52) Zhong et al. (2020); (53) Kothes & Foster (2012); (54) Fahlman & Gregory (1981); (55) Hulleman et al. (2001); (56) Barthelmy et al. (2016); (57) Doroshenko et al. (2021); (58) Richardson et al. (2023); (59) Cline et al. (2000); (60) Lamb et al. (2003); (61) Mereghetti et al. (2012); (62) Torii et al. (1998); (63) Gaensler, Gotthelf & Vasisht (1999); (64) Tam et al. (2006); (65) Sakamoto et al. (2011); (66) Leahy & Tian (2007); (67) Gotthelf et al. (2000); (68) Helfand, Collins & Gotthelf (2003); (69) Blumer et al. (2019); (70) Lin, Webb & Barret (2012); (71) Roming et al. (2008); (72) Barthelmy et al. (2016); (73) Jing et al. (2023); (74) Ponti et al. (2015); (75) Yalinewich, Piran & Sari (2017); (76) Cline et al. (1982); (77) Park et al. (2012); (78) Park et al. (2020); (79) Sano et al. (2023); (80) Borkowski & Reynolds (2017); (81) Zhou et al. (2019); (82) Kothes et al. (2018); (83) Zhou et al. (2020); (84) Nakano et al. (2017); (85) Leahy & Tian (2008b); (86) Straal, Gelfand & Eagle (2023); and (87) Ding et al. (2020b). We have repeated the Gaia search for unbound companion stars, the radio search for supernova remnant (SNR) associations, and the optical and infrared (IR) searches for bound companion stars with the updated position errors. The revised Gaia search critical thresholds for each magnetar (table B1 in Sherman et al. 2024) are given in Table 3. We find the results are unchanged. No candidate bound or unbound companions are identified with 95 per cent confidence for 1E 1547.0–5408 nor PSR J1846–0258, while their respective associated SNRs, G327.2–00.1 and Kes 75 are still recovered through the radio search with revised p-values |$p=1.5$| per cent and |$p=1.0$| per cent, respectively (Gotthelf et al. 2000; Gelfand & Gaensler 2007). No candidate bound companions, unbound companions, or SNRs are identified for AX J1818.8–1559. Thus there are no significant changes to the conclusions. We provide the corrected results table (table 3 in Sherman et al. 2024) in Table 2; the revised p-values for 1E 1547.0–4508 and PSR J1846–0258 are boldfaced for clarity. Search results and completeness ratios (revised candidates and p-values are boldfaced for clarity). Notes. For each magnetar (written with its abbreviated name), the SNR candidates, bound companion candidates, and unbound companion candidates with |$p\lt 5\%$| are given, with p-values in brackets. Candidates suspected to be false positives are given in italics. Sources identified ‘by-eye’ which are not confidently associated with any known object are labelled using the format, ‘S24-survey-Jhhmmss|$\pm$|ddmmss’, where survey is the survey used and the italicized portion is the J2000 RA and declination of the centroid. For each search, the completeness along each magnetar’s sightline is indicated by a |$\checkmark$|⁠, meaning the search is either partially or fully sensitive to stars or remnants, or by an ✗, meaning that even the brightest expected stars or remnants would not be detectable. The radio search completeness is labelled with ‘R’, ‘V’, or ‘N’ to indicate whether the RACS, VLASS, or NVSS survey is used. The optical/IR bound search is considered partially or fully complete if either the optical or IR search are complete. These are labelled with ‘P’ or ‘S’, to indicate whether the PS1 or SkyMapper survey is used, and ‘T’, ‘U’, or ‘V’ to indicate whether the 2MASS, PS1, or VVV survey is used. The Gaia search is considered partially or fully complete if both the V-band magnitude and expected relative proper motion are detectable. Four magnetars or candidates have no distance measures and the completeness cannot be determined; these are marked with ‘–’.Candidates for SNR, bound, or unbound companions from previous analyses are provided in the last column with references matched to the following: (1) Gaensler & Chatterjee (2008); (2) Klose et al. (2004); (3) Gelfand & Gaensler (2007); (4) Anderson et al. (2012); (5) Corbel et al. (1999); (6) Clark et al. (2014); (7) Halpern & Gotthelf (2010a); (8) Chrimes et al. (2022); (9) Corbel & Eikenberry (2004); (10) Kargaltsev et al. (2012); (11) Vasisht & Gotthelf (1997); (12) Vrba et al. (2000); (13) Gaensler (2014); (14) Fahlman & Gregory (1981); (15) Gaensler et al. (1999); (16) Gotthelf et al. (2000); (17) Zhou et al. (2014); (18) Ponti et al. (2015); (19) Yalinewich et al. (2017); (20) Cline et al. (2000); (21) H. E. S. S. Collaboration et al. (2018); and (22) Ding et al. (2020b). |$^\dagger$|For the Gaia search for unbound companions, we consider the proper motion sensitivity in four magnitude bins as described in Gaia Collaboration et al. (2023): |$m_G \gt 15$| (⁠|$\mu _{\rm min} = 0.025$| mas yr|$^{-1}$|⁠), |$m_G = 17$| (⁠|$\mu _{\rm min} = 0.07$| mas yr|$^{-1}$|⁠), |$m_G = 20$| (⁠|$\mu _{\rm min} = 0.5$| mas yr|$^{-1}$|⁠), and |$m_G = 21$| (⁠|$\mu _{\rm min} = 1.4$| mas yr|$^{-1}$|⁠). |$^\ddagger$|For conciseness, we omit the names of the 17 and 28 false positives found for SGR 1801–23 and SGR 1808–20, resectively. For the former, the false positives are rejected in favour of W28 identified by Cline et al. (2000). Detailed discussion for the latter is provided in section 5.3. |$^{*}$|CXOU J185238.6 + 004020 is an X-ray pulsar associated with Kes 79. We explore the scenario that the progenitors of 3XMM J1852 and this pulsar were bound in section 5.3. Search results and completeness ratios (revised candidates and p-values are boldfaced for clarity). Notes. For each magnetar (written with its abbreviated name), the SNR candidates, bound companion candidates, and unbound companion candidates with |$p\lt 5\%$| are given, with p-values in brackets. Candidates suspected to be false positives are given in italics. Sources identified ‘by-eye’ which are not confidently associated with any known object are labelled using the format, ‘S24-survey-Jhhmmss|$\pm$|ddmmss’, where survey is the survey used and the italicized portion is the J2000 RA and declination of the centroid. For each search, the completeness along each magnetar’s sightline is indicated by a |$\checkmark$|⁠, meaning the search is either partially or fully sensitive to stars or remnants, or by an ✗, meaning that even the brightest expected stars or remnants would not be detectable. The radio search completeness is labelled with ‘R’, ‘V’, or ‘N’ to indicate whether the RACS, VLASS, or NVSS survey is used. The optical/IR bound search is considered partially or fully complete if either the optical or IR search are complete. These are labelled with ‘P’ or ‘S’, to indicate whether the PS1 or SkyMapper survey is used, and ‘T’, ‘U’, or ‘V’ to indicate whether the 2MASS, PS1, or VVV survey is used. The Gaia search is considered partially or fully complete if both the V-band magnitude and expected relative proper motion are detectable. Four magnetars or candidates have no distance measures and the completeness cannot be determined; these are marked with ‘–’.Candidates for SNR, bound, or unbound companions from previous analyses are provided in the last column with references matched to the following: (1) Gaensler & Chatterjee (2008); (2) Klose et al. (2004); (3) Gelfand & Gaensler (2007); (4) Anderson et al. (2012); (5) Corbel et al. (1999); (6) Clark et al. (2014); (7) Halpern & Gotthelf (2010a); (8) Chrimes et al. (2022); (9) Corbel & Eikenberry (2004); (10) Kargaltsev et al. (2012); (11) Vasisht & Gotthelf (1997); (12) Vrba et al. (2000); (13) Gaensler (2014); (14) Fahlman & Gregory (1981); (15) Gaensler et al. (1999); (16) Gotthelf et al. (2000); (17) Zhou et al. (2014); (18) Ponti et al. (2015); (19) Yalinewich et al. (2017); (20) Cline et al. (2000); (21) H. E. S. S. Collaboration et al. (2018); and (22) Ding et al. (2020b). |$^\dagger$|For the Gaia search for unbound companions, we consider the proper motion sensitivity in four magnitude bins as described in Gaia Collaboration et al. (2023): |$m_G \gt 15$| (⁠|$\mu _{\rm min} = 0.025$| mas yr|$^{-1}$|⁠), |$m_G = 17$| (⁠|$\mu _{\rm min} = 0.07$| mas yr|$^{-1}$|⁠), |$m_G = 20$| (⁠|$\mu _{\rm min} = 0.5$| mas yr|$^{-1}$|⁠), and |$m_G = 21$| (⁠|$\mu _{\rm min} = 1.4$| mas yr|$^{-1}$|⁠). |$^\ddagger$|For conciseness, we omit the names of the 17 and 28 false positives found for SGR 1801–23 and SGR 1808–20, resectively. For the former, the false positives are rejected in favour of W28 identified by Cline et al. (2000). Detailed discussion for the latter is provided in section 5.3. |$^{*}$|CXOU J185238.6 + 004020 is an X-ray pulsar associated with Kes 79. We explore the scenario that the progenitors of 3XMM J1852 and this pulsar were bound in section 5.3. Critical Thresholds for Magnetar Association Tests (revised thresholds are boldfaced for clarity). Critical Thresholds for Magnetar Association Tests (revised thresholds are boldfaced for clarity). For the IR search for bound companions, the 2MASS, UKIDSS, and VVV point source catalogues were queried for candidate stars within 1|$^\prime$| of each magnetar. We have identified a bug in our code which truncated the results of the UKIDSS query to the first 50 sources along each sightline. Our code made use of the astropy.Vizier.1 module for the UKIDSS search, for which the Vizier.ROW_LIMIT variable must be set to −1 to include all sources.2 We have resolved this and re-run the UKIDSS search; while additional sources are now included for 24 magnetars, the resulting candidates are unchanged for all but SGR J1822.3–1607. In addition to the two false-positive 2MASS sources discussed in appendix C3.2, we now recover their corresponding UKIDSS counterparts (UKIDSS J182218.39–160424.0, UKIDSS J182218.39–160424.1, UKIDSS J182217.94–160426.0, and UKIDSS J182217.94–160425.9) with |$p\lt 0.1$| per cent. Furthermore, two new IR sources are identified with |$p\lt 5$| per cent for SGR J1822.3–1606: UKIDSS J182217.97–160436.0 (⁠|$p=2.0$| per cent) and UKIDSS J182217.97–160435.9 (⁠|$p=1.0$| per cent), both of which are associated with the marginal candidate 2MASS 18221797–1604360 (⁠|$p\approx 5$| per cent). We revise the first paragraph of appendix C3.2, describing the new candidate as a false positive, as follows: ‘Three distinct IR sources nearby SGR J1822.3–1606 are found to have |$p\lt 5~\%$|⁠: 2MASS 18221839–1604241 (⁠|$p\lt 0.1~\%$|⁠; UKIDSS J182218.39–160424.0, UKIDSS J182218.39–160424.1), 2MASS 18221794–1604259 (⁠|$p\lt 0.1~\%$|⁠; UKIDSS J182217.94–160425.9, UKIDSS J182217.94–160426.0), and 2MASS 18221797–1604360 (⁠|$p\approx 5~\%$|⁠; UKIDSS J182217.97–160436.0, UKIDSS J182217.97–160435.9). The first is unlikely based on its angular separation |$\sim 6.7^{\prime \prime }\pm 0.7^{\prime \prime }$|⁠; at the magnetar’s distance |$1.6\pm 0.3$| kpc, this corresponds to |$\sim 0.05$| pc which is too large for a bound orbit. While this could be an unbound companion, it was not recovered in the Gaia search, and the absolute |$J-H$| color is inconsistent with OB stars at the |$5\sigma$| level when placed at the magnetar distance, with |$J-H\approx 0.85\pm 0.10$| (Chrimes et al. 2022). The latter source was identified with |$p\lt 5~\%$| only for the UKIDSS counterparts (⁠|$p=1~\%,2~\%$|⁠), while the 2MASS source had a marginal |$p\approx 5~\%$|⁠. Again, we find it unlikely this is associated with SGR J1822 based on its angular separation |$\sim 9.2^{\prime \prime }\pm 0.7^{\prime \prime }$| and color |$J-H\approx 1.69\pm 0.14$|⁠. We conclude that both 2MASS 18221839–1604241 and 2MASS 18221797–1604360 are false positives for bound companions’. The revised results table entry for SGR J1822.3–1606 is given in Table 2, and the revised IR image (fig. 3, middle right in Sherman et al. 2024) is shown in Fig. 1. Note there was also a plotting error in the original SGR J1822.3–1606 image which led to the incorrect candidates being highlighted; this has been corrected in Fig. 1 and did not affect any of the other figures in Sherman et al. (2024). Revised Infrared |$1^\prime \times 1^\prime$| image cutout for SGR J1822. The authors would like to thank the anonymous referee and for comments that helped identify additional errata and improve the final work. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The CaltechDATA repository for the original article (https://doi.org/10.22002/fbdqe-hez98) has been updated with the corrected position uncertainties for 1E 1547.0–5408, AX J1818.8–1559, and PSR J1846–0258, the additional UKIDSS sources from the updated query, and new p-values for each optical, IR, and radio source analyzed in the revised search.

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