Keywords: Magnetars (992), Binary pulsars (153), Massive stars (732), Core-collapse supernovae (304), Runaway stars (1417)
Abstract: Core-collapse Supernovae (CCSNe) are considered the primary magnetar formation channel, with 15 magnetars associated with supernova remnants (SNRs). A large fraction of these should occur in massive stellar binaries that are disrupted by the explosion, meaning that $\sim45\%$ of magnetars should be nearby high-velocity stars. Here we conduct a multi-wavelength search for unbound stars, magnetar binaries, and SNR shells using public optical ($uvgrizy-$bands), infrared ($J-$, $H-$, $K-$, and $K_s-$bands), and radio ($888$\,MHz, $1.4$\,GHz, and $3$\,GHz) catalogs. We use Monte Carlo analyses of candidates to estimate the probability of association with a given magnetar based on their proximity, distance, proper motion, and magnitude. In addition to recovering a proposed magnetar binary, a proposed unbound binary, and 13 of 15 magnetar SNRs, we identify two new candidate unbound systems: an OB star from the \textit{Gaia} catalog we associate with SGR\,J1822.3-1606, and an X-ray pulsar we associate with 3XMM\,J185246.6+003317. Using a Markov-Chain Monte Carlo simulation that assumes all magnetars descend from CCSNe, we constrain the fraction of magnetars with unbound companions to $5\lesssim fu \lesssim 24\%$, which disagrees with neutron star population synthesis results. Alternate formation channels are unlikely to wholly account for the lack of unbound binaries as this would require $31\lesssim f{nc} \lesssim 66\%$ of magnetars to descend from such channels. Our results support a high fraction ($48\lesssim f_m \lesssim 86\%$) of pre-CCSN mergers, which can amplify fossil magnetic fields to preferentially form magnetars.
Description: Each table contains data and association p-values for the magnetars, massive OB stars and candidates, and supernova remnants (SNR) and candidates used for the search described in Sherman et al., 2024. These can be read in Python as an hdu list using astropy with the commands below:
>> from astropy.io import fits
>> hdul = fits.open("all_magnetars_properties_table.fits")
or to read as an astropy Table:
>> from astropy.table import Table
>> data_table = Table.read("all_magnetars_properties_table.fits")
For more information, see https://docs.astropy.org/en/stable/io/fits/ and https://docs.astropy.org/en/stable/io/fits/usage/table.html . Magnetar data is compiled using the McGill Magnetar Catalog (Olausen and Kaspi, 2014), SIMBAD, and the available literature (see Table 1 in Sherman et al. 2024 for references). Stellar data is compiled using PanSTARRs DR2 (Flewelling et al., 2020), SkyMapper (Onken et al., 2024) UKIDSS (Dye et al., 2006), VVV and VIRACS (Nikzat et al., 2022; Smith et al., 2018), and 2MASS (Skrutskie et al., 2006). SNR data is compiled using SIMBAD and the Green SNR Catalog (Green et al., 2019). Derived parameters are also provided; see Sherman et al., 2024 for details on their definition. Sources identified 'by-eye' are labelled 'SREB-24-survey-JRA+DEC'. For the search tables, each hdu in the provided fits files (and the data descriptions below) corresponds to a single magnetar; see the header file in the Primary HDU (index 0) for a mapping of hdu indices to magnetars. For the 'all_magnetars_unbound_search_table', a short-circuit method was used to evaluate the total p-value. Therefore, all sources will have a p_1 estimate, while only those with both p_1 and p_4 below 5% will have total p-values. Note the p-values reported here may marginally differ from those in Sherman et al., 2024 since they were completed in a separate simulation run to create these tables. In addition, some p-values are computed with insufficient samples as discussed in the text. P-values are provided in these tables for completeness, but please defer to Sherman et al., 2024 Section 3 and Table 3 to confirm the validity of p-values for any candidate.
Version History: 2024-04-06: Initial Submission 2024-05-08: Accepted to MNRAS after referee review; Updated XTE J1810, Swift J1818, and pulsar analysis; Updated PSR B1952+32 and PSR J1124-5916 proper motion uncertainties 2024-08-24: Correction of 1E 1547-5408 position error
ReadMe 80 . this file
all_magnetars_properties_table 457 31
all_gaia_sample_table 494 156572
all_magnetars_snr_search_table 243 19
all_magnetars_unbound_search_table 513 491
all_magnetars_bound_search_table 840 68
all_pulsars_unbound_search_table 566 441
1- 32 A32 --- name Magnetar name (McGill Catalog) 34- 45 F12.8 degree ra [15.17/345.29] J2000 Right Ascension 47- 57 E11.6 degree ra_error [0.0/3.8] Error in RA 59- 71 F13.9 degree dec [-72.2/61.76] J2000 Declination 73- 83 E11.6 degree dec_error [0.0/3.8] Error in Dec 85- 90 F6.2 kpc distance [1.6/62.4] Distance 92- 96 F5.2 kpc distance_upper_error [0.07/2.5] Distance upper error 98-102 F5.2 kpc distance_lower_error [0.07/2.5] Distance lower error 104-122 F19.15 --- distance_modulus [11.02/18.98] Distance modulus 5log(d/1pc) - 5 124-128 F5.2 mas.yr-1 pmra [-6.6/4.8] Proper motion magnitude in right ascension times cosine of declination 130-134 F5.2 mas.yr-1 pmra_error [0.05/1.4] Error in RA proper motion 136-141 F6.2 mas.yr-1 pmdec [-11.72/5.89] Proper motion magnitude in declination 143-147 F5.2 mas.yr-1 pmdec_error [0.09/2.0] Error in dec proper motion 149-168 F20.18 --- f_crit [0.03/1.0] Critical search statistic for unbound companion search in V-band magnitude and init angular separation space 170-189 F20.17 --- E(B-V) [0.1/17.46] B-V Interstellar Reddening 191-222 A32 --- extinction_method Method used to get B-V Extinction; either from Bayestar19 library (Green et al., 2018,2019), mean Gaia GSP Photometry for nearby sources (Vallenari et al., 2022), or scaling linearly with column density (Predehl & Schmitt, 1995) 224-230 F7.3 10+14G B_surface [0.06/20.0] Surface dipole magnetic field strength B = (3.2e19)x(P\dot{P})^{1/2} 232-256 F25.20 10+33erg.s-1 L_x [0.0/189.0] X-ray luminosity in the 2-10 keV range 258-279 E22.17 10+22cm-2 N_H [0.0/0.01] Hydrogen column density 281-302 E22.17 10+22cm-2 N_H_upper_error [0.0/0.01] Column density upper error 304-325 E22.17 10+22cm-2 N_H_lower_error [0.0/0.01] Column density lower error 327-347 F21.15 kyr best_age [0.24/3525.05] Age estimate used for Sherman et al. 2024 analysis 349-369 F21.14 kyr best_age_upper_error [178.5/10940.97] Age upper error 371-391 F21.15 kyr best_age_lower_error [44.43/2578.89] Age lower error 393-424 A32 --- best_age_method Method used for best age estimate; either SNR if based on the association of magnetar with supernova remnant, Decay if estimated from magnetic field decay (Sherman et al., 2024 Appendix D1 and Ferrario & Wickramsinghe 2006, 2008), Spindown if from spindown rate P/2\dot{P} 426-447 F22.16 kyr decay_age [1.27/8325.11] Age estimate from magnetic field decay (Sherman et al., 2024 Appendix D1 and Ferrario & Wickramsinghe 2006, 2008) 449-457 F9.2 kyr spindown_age [0.24/36000.0] Spindown age estimate as P/2\dot{P} using McGill Catalog values
1- 32 A32 --- Source_ID Gaia DR3 designation 34- 55 F22.18 degree ra [0.0/360.0] J2000 Right Ascension 57- 76 F20.15 arcsecond ra_error [15.15/2685.29] Error in RA 78-101 F24.20 degree dec [-89.89/82.76] J2000 Declination 103-122 F20.15 arcsecond dec_error [17.61/2577.15] Error in Dec 124-143 F20.17 mas parallax [-0.72/1.82] Parallax angle 145-156 F12.10 mas parallax_error [0.0/1.04] Error in parallax 158-177 F20.17 kpc distance [0.33/11.67] Distance from Parallax using Bailer-Jones et al., 2021,2023 179-198 F20.17 kpc distance_upper_error [0.0/11.32] Distance upper error 200-218 F19.17 kpc distance_lower_error [0.0/6.26] Distance lower error 220-237 F18.15 --- distance_modulus [7.63/15.34] Distance modulus 5log(d/1pc) - 5 239-262 E24.17 mas.yr-1 pmra [-88.76/90.28] Proper motion magnitude in right ascension times cosine of declination 264-275 F12.10 mas.yr-1 pmra_error [0.0/0.85] Error in RA proper motion 277-300 E24.17 mas.yr-1 pmdec [-116.58/58.86] Proper motion magnitude in declination 302-313 F12.10 mas.yr-1 pmdec_error [0.0/0.85] Error in dec proper motion 315-324 F10.7 magnitude Gmag_apparent [3.61/18.39] G-band apparent magnitude 326-349 E24.17 magnitude Gmag_absolute [-49.49/1.16] G-band absolute magnitude using parallax distance and extinction 351-374 E24.17 magnitude Vmag_absolute [-28.66/1.19] V-band absolute magnitude using parallax distance and extinction 376-396 F21.18 --- E(B-V) B-V Interstellar Reddening 398-418 F21.17 --- AV V-band Extinction, 3.2E(B-V) 420-438 F19.17 --- E(BP-RP) BP-RP Interstellar Reddening 440-461 F22.18 --- AG [-0.05/52.13] G-band Extinction from Gaia GSP Photometry 463-494 A32 --- extinction_method Method used to get B-V Extinction; either from Bayestar19 library (Green et al., 2018,2019) or Gaia GSP Photometry (Vallenari et al., 2022)
1- 32 A32 --- Source_ID SIMBAD Source designation (or SREB- if from this work) 34- 51 F18.15 degree ra [25.6/27.59] J2000 Right Ascension 53- 62 F10.7 arcsecond ra_error [0.5/0.51] Error in RA 64- 81 F18.15 degree dec [61.26/62.01] J2000 Declination 83- 92 F10.7 arcsecond dec_error [0.5/0.51] Error in Dec 94- 97 F4.1 kpc distance [3.6/3.6] Distance 99-102 F4.1 kpc distance_upper_error [0.4/0.4] Distance upper error 104-107 F4.1 kpc distance_lower_error [0.4/0.4] Distance lower error 109-127 F19.15 --- distance_modulus [12.78/12.79] Distance modulus 5log(d/1pc) - 5 129-132 F4.1 mas.yr-1 pmra [-4.1/-4.09] Proper motion magnitude in right ascension times cosine of declination 134-137 F4.1 mas.yr-1 pmra_error [1.0/1.0] Error in RA proper motion 139-142 F4.1 mas.yr-1 pmdec [1.9/1.9] Proper motion magnitude in declination 144-147 F4.1 mas.yr-1 pmdec_error [1.0/1.0] Error in dec proper motion 149-167 F19.15 arcsecond major_error [-4.5/51.2] Major axis of error ellipse 169-187 F19.15 arcsecond minor_error [-17.05/43.89] Minor axis of error ellipse 189-210 F22.16 degree pa_error [-38.29/5156.63] Position angle (E of N) of error ellipse 212-214 F3.0 degree major_size Major axis of best fit ellipse 216-218 F3.0 degree minor_size Minor axis of best fit ellipse 220-223 F4.1 degrees pa Position angle (E of N) of best fit ellipse 225-243 F19.16 --- p_value [0.91/1.0] Final p-value for association (0 = likely associated, 1 = unlikely associated)
1- 32 A32 --- Source_ID Gaia DR3 designation, magnetar name 34- 51 F18.15 degree ra [21.64/31.54] J2000 Right Ascension 53- 72 F20.15 arcsecond ra_error [0.5/1451.02] Error in RA 74- 91 F18.15 degree dec [56.79/66.67] J2000 Declination 93-112 F20.15 arcsecond dec_error [0.5/1468.63] Error in Dec 114-133 F20.17 mas parallax [0.24/1.55] Parallax angle 135-147 F13.10 mas parallax_error [0.0/0.59] Error in parallax 149-166 F18.16 kpc distance [0.5/5.16] Unbiased distance from Parallax using Bailer-Jones et al., 2021,2023 168-186 F19.17 kpc distance_upper_error [0.0/1.25] Distance upper error 188-206 F19.17 kpc distance_lower_error [0.0/2.07] Distance lower error 208-225 F18.15 --- distance_modulus [8.51/13.57] Distance modulus 5log(d/1pc) - 5 227-249 F23.19 mas.yr-1 pmra [-12.22/33.43] Proper motion magnitude in right ascension times cosine of declination 251-262 F12.10 mas.yr-1 pmra_error [0.0/1.0] Error in RA proper motion 264-285 F22.18 mas.yr-1 pmdec [-14.37/8.95] Proper motion magnitude in declination 287-298 F12.10 mas.yr-1 pmdec_error [0.0/1.0] Error in dec proper motion 300-310 F11.7 magnitude Gmag_apparent [6.96/14.84] G-band apparent magnitude 312-332 F21.18 magnitude Gmag_absolute [-6.13/1.15] G-band absolute magnitude using unbiased parallax distance and extinction 334-355 F22.19 magnitude Vmag_absolute [-6.1/1.19] V-band absolute magnitude using parallax distance and extinction 357-376 F20.17 --- E(B-V) [0.1/1.71] B-V Interstellar Reddening 378-397 F20.17 --- AV [0.35/5.48] V-band Extinction, 3.2E(B-V) 399-418 F20.17 --- E(BP-RP) [0.22/2.11] BP-RP Interstellar Reddening 420-438 F19.16 --- AG [0.29/5.07] G-band Extinction from Gaia GSP Photometry 440-471 A32 --- extinction_method Method used to get B-V reddening; either from Bayestar19 library (Green et al., 2018,2019) or Gaia GSP Photometry (Vallenari et al., 2022) 473-491 F19.16 --- f_statistic [1.0/1.01] Search statistic from magnitude and angular separation 493-497 F5.2 --- p_value_1 [0.99/0.99] P-value from magnitude and angular separation (0 = likely associated, 1 = unlikely associated) 499-501 F3.0 --- p_value_2 P-value from difference in 2D travel time (0 = likely associated, 1 = unlikely associated) 503-505 F3.0 --- p_value_3 P-value from 3D magnetar travel time (0 = likely associated, 1 = unlikely associated) 507-509 F3.0 --- p_value_4 P-value from magnetar and source distance (0 = likely associated, 1 = unlikely associated) 511-513 F3.0 --- p_value Final p-value for association (0 = likely associated,
1 = unlikely associated)
1- 64 A64 --- Source_ID Designation from 2MASS, VVV, UKIDSS PS1 or SkyMapper Survey (or SREB- if from this work) 66- 83 F18.15 degree ra [26.57/26.62] J2000 Right Ascension 85- 94 F10.7 arcsecond ra_error [0.5/0.51] Error in RA 96-113 F18.15 degree dec [61.74/61.76] J2000 Declination 115-124 F10.7 arcsecond dec_error [0.5/0.51] Error in Dec 126-129 F4.1 kpc distance [3.6/3.6] Distance 131-134 F4.1 kpc distance_upper_error [0.4/0.4] Distance upper error 136-139 F4.1 kpc distance_lower_error [0.4/0.4] Distance lower error 141-159 F19.15 --- distance_modulus [12.78/12.79] Distance modulus 5log(d/1pc) - 5 161-164 F4.1 mas.yr-1 pmra [-4.1/-4.09] Proper motion magnitude in right ascension times cosine of declination 166-169 F4.1 mas.yr-1 pmra_error [1.0/1.0] Error in RA proper motion 171-174 F4.1 mas.yr-1 pmdec [1.9/1.9] Proper motion magnitude in declination 176-179 F4.1 mas.yr-1 pmdec_error [1.0/1.0] Error in dec proper motion 181-203 F23.20 arcsecond major_error [-0.76/0.91] Major axis of error ellipse 205-227 F23.20 arcsecond minor_error [-0.21/1.64] Minor axis of error ellipse 229-249 F21.16 degree pa_error [-1.74/135.0] Position angle (E of N) of error ellipse 251-269 F19.16 --- p_value [0.75/1.0] Final p-value for association (0 = likely associated, 1 = unlikely associated) 271-289 F19.15 --- Jmag [13.18/16.44] J-band apparent PSF magnitude 291-311 F21.18 --- e_Jmag [0.02/0.15] Error in J-band apparent PSF magnitude 313-331 F19.15 --- Hmag [12.65/15.73] H-band apparent PSF magnitude 333-352 F20.17 --- e_Hmag [0.03/0.15] Error in H-band apparent PSF magnitude 354-372 F19.15 --- gmag [16.82/22.29] g-band apparent PSF magnitude 374-394 F21.18 --- e_gmag [0.0/0.23] Error in g-band apparent PSF magnitude 396-414 F19.15 --- rmag [15.68/21.65] r-band apparent PSF magnitude 416-437 F22.19 --- e_rmag [0.0/0.19] Error in r-band apparent PSF magnitude 439-457 F19.15 --- imag [15.01/21.43] i-band apparent PSF magnitude 459-480 F22.19 --- e_imag [0.0/0.36] Error in i-band apparent PSF magnitude 482-500 F19.15 --- zmag [14.61/21.31] z-band apparent PSF magnitude 502-522 F21.18 --- e_zmag [0.0/0.44] Error in z-band apparent PSF magnitude 524-542 F19.15 --- ymag [14.35/20.37] y-band apparent PSF magnitude 544-565 F22.19 --- e_ymag [0.0/0.32] Error in y-band apparent PSF magnitude 567-585 F19.15 --- Krongmag [16.86/21.56] g-band apparent Kron magnitude (variance-weighted mean for SkyMapper) 587-608 F22.19 --- e_Krongmag [0.0/0.31] Error in g-band apparent Kron magnitude 610-628 F19.15 --- Kronrmag [15.74/21.28] r-band apparent Kron magnitude (variance-weighted mean for SkyMapper) 630-651 F22.19 --- e_Kronrmag [0.0/0.32] Error in r-band apparent Kron magnitude 653-671 F19.15 --- Kronimag [15.05/21.38] i-band apparent Kron magnitude (variance-weighted mean for SkyMapper) 673-694 F22.19 --- e_Kronimag [0.0/0.29] Error in i-band apparent Kron magnitude 696-714 F19.15 --- Kronzmag [14.66/21.14] z-band apparent Kron magnitude (variance-weighted mean for SkyMapper) 716-737 F22.19 --- e_Kronzmag [0.0/0.3] Error in z-band apparent Kron magnitude 739-757 F19.15 --- Kronymag [14.36/20.28] y-band apparent Kron magnitude (variance-weighted mean for SkyMapper) 759-780 F22.19 --- e_Kronymag [0.0/0.13] Error in y-band apparent Kron magnitude 782-800 F19.15 --- Vmag [11.45/16.76] V-band apparent PSF magnitude 802-820 F19.15 --- e_upper_Vmag [7.25/10.01] Upper error in V-band apparent PSF magnitude 822-840 F19.15 --- e_lower_Vmag [7.26/10.03] Lower error in V-band apparent PSF magnitude
1- 32 A32 --- Source_ID Gaia DR3 designation, magnetar name 34- 51 F18.15 degree ra [26.56/36.34] J2000 Right Ascension 53- 73 F21.16 arcsecond ra_error [0.53/1515.79] Error in RA 75- 92 F18.15 degree dec [59.85/69.63] J2000 Declination 94-113 F20.15 arcsecond dec_error [3.6/1852.36] Error in Dec 115-134 F20.17 mas parallax [0.29/1.55] Error in parallax 136-148 F13.10 mas parallax_error [0.0/0.68] Error in parallax 150-167 F18.16 kpc distance [0.5/3.2] Unbiased distance from Parallax using Bailer-Jones et al., 2021,2023 169-188 F20.17 kpc distance_upper_error [0.0/0.52]Distance upper error 190-209 F20.17 kpc distance_lower_error [0.0/0.68]Distance lower error 211-228 F18.15 --- distance_modulus [8.51/12.53] Distance modulus 5log(d/1pc) - 5 230-252 F23.19 mas.yr-1 pmra [-11.47/23.26] Proper motion magnitude in right ascension times cosine of declination 254-265 F12.10 mas.yr-1 pmra_error [0.0/0.5] Error in RA proper motion 267-288 F22.18 mas.yr-1 pmdec [-10.31/6.11] Proper motion magnitude in declination 290-301 F12.10 mas.yr-1 pmdec_error [0.0/0.65] Error in dec proper motion 303-313 F11.7 magnitude Gmag_apparent [8.2/15.91] G-band apparent magnitude 315-335 F21.18 magnitude Gmag_absolute [-6.7/1.15] G-band absolute magnitude using parallax distance and extinction 337-358 F22.19 magnitude Vmag_absolute [-6.64/1.19] V-band absolute magnitude using parallax distance and extinction 360-379 F20.17 --- E(B-V) [0.28/2.46] B-V Interstellar Reddening 381-399 F19.16 --- AV [0.89/7.85] V-band Extinction, 3.2E(B-V) 401-420 F20.17 --- E(BP-RP) [0.45/2.98] BP-RP Interstellar Reddening 422-440 F19.16 --- AG [0.82/8.04] G-band Extinction from Gaia GSP Photometry 442-473 A32 --- extinction_method Method used to get B-V reddening; either from Bayestar19 library (Green et al., 2018,2019) or Gaia GSP Photometry (Vallenari et al., 2022) 475-494 F20.17 --- f_statistic [0.02/1.01] Search statistic from magnitude and angular separation 496-500 F5.2 --- p_value_1 [0.01/0.99] P-value from magnitude and angular separation (0 = likely associated, 1 = unlikely associated) 502-520 F19.16 --- p_value_2 [0.01/1.0] P-value from difference in 2D travel time (0 = likely associated, 1 = unlikely associated) 522-540 F19.16 --- p_value_3 [0.72/1.0] P-value from 3D magnetar travel time (0 = likely associated, 1 = unlikely associated) 542-546 F5.2 --- p_value_4 [0.01/0.01] P-value from magnetar and source distance (0 = likely associated, 1 = unlikely associated) 548-566 F7.4 --- p_value [0.82/1.0] Final p-value for association (0 = likely associated, 1 = unlikely associated)
Acknowledgements:
For additional data, please contact Myles Sherman at msherman@caltech.edu. The authors would like to thank the members of the Deep Synoptic Array (DSA-110) team for their support and insight with regards to this search effort. The authors thank staff members of the Owens Valley Radio Observatory and the Caltech radio group, including Kristen Bernasconi, Stephanie Cha-Ramos, Sarah Harnach, Tom Klinefelter, Lori McGraw, Corey Posner, Andres Rizo, Michael Virgin, Scott White, and Thomas Zentmyer. Their tireless efforts were instrumental to the success of the DSA-110. The DSA-110 is supported by the National Science Foundation Mid-Scale Innovations Program in Astronomical Sciences (MSIP) under grant AST-1836018. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE‐1745301.
The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. The UKIDSS project is defined in \citet{2007MNRAS.379.1599L}. The national facility capability for SkyMapper has been funded through ARC LIEF grant LE130100104 from the Australian Research Council, awarded to the University of Sydney, the Australian National University, Swinburne University of Technology, the University of Queensland, the University of Western Australia, the University of Melbourne, Curtin University of Technology, Monash University and the Australian Astronomical Observatory. SkyMapper is owned and operated by The Australian National University's Research School of Astronomy and Astrophysics. The survey data were processed and provided by the SkyMapper Team at ANU. The SkyMapper node of the All-Sky Virtual Observatory (ASVO) is hosted at the National Computational Infrastructure (NCI). Development and support of the SkyMapper node of the ASVO has been funded in part by Astronomy Australia Limited (AAL) and the Australian Government through the Commonwealth's Education Investment Fund (EIF) and National Collaborative Research Infrastructure Strategy (NCRIS), particularly the National eResearch Collaboration Tools and Resources (NeCTAR) and the Australian National Data Service Projects (ANDS).
UKIDSS uses the UKIRT Wide Field Camera (WFCAM; \citet{2007A&A...467..777C}). The photometric system is described in \citet{2006MNRAS.367..454H}, and the calibration is described in \citet{2009MNRAS.394..675H}. The pipeline processing and science archive are described in \citet{irwin2004vista} and \citet{2008MNRAS.384..637H}. The VISTA Data Flow System pipeline processing and science archive are described in \citet{irwin2004vista}, \citet{2008MNRAS.384..637H} and \citet{cross2012vista}. We have used data from the 5th data release of the Vista Variables in the Via Lactea (VVV) Survey, which is described in detail in \citet{nikzat2022vvv}, and the VVV Infrared Astrometric Catalogue, described in detail in \citet{smith2018virac}. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
This work also uses data obtained from Inyarrimanha Ilgari Bundara / the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamaji People as the Traditional Owners and native title holders of the Observatory site. CSIRO’s ASKAP radio telescope is part of the Australia Telescope National Facility (https://ror.org/05qajvd42). Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. ASKAP uses the resources of the Pawsey Supercomputing Research Centre. Establishment of ASKAP, Inyarrimanha Ilgari Bundara, the CSIRO Murchison Radio-astronomy Observatory and the Pawsey Supercomputing Research Centre are initiatives of the Australian Government, with support from the Government of Western Australia and the Science and Industry Endowment Fund. This paper includes archived data obtained through the CSIRO ASKAP Science Data Archive, CASDA (https://data.csiro.au). This work has utilized data from the LoTSS survey and image archive, which is described in detail in \citet{shimwell2022lofar}. This work has made use of data from the European Space Agency (ESA) mission {\it Gaia} (\url{https://www.cosmos.esa.int/gaia}), processed by the {\it Gaia} Data Processing and Analysis Consortium (DPAC, \url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the {\it Gaia} Multilateral Agreement. This research has made use of the CIRADA cutout service at \url{cutouts.cirada.ca}, operated by the Canadian Initiative for Radio Astronomy Data Analysis (CIRADA). CIRADA is funded by a grant from the Canada Foundation for Innovation 2017 Innovation Fund (Project 35999), as well as by the Provinces of Ontario, British Columbia, Alberta, Manitoba and Quebec, in collaboration with the National Research Council of Canada, the US National Radio Astronomy Observatory and Australia’s Commonwealth Scientific and Industrial Research Organisation.