Published November 2023 | Published
Journal Article Open

BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100–200 pc

  • 1. ROR icon Diego Portales University
  • 2. ROR icon National Astronomical Observatory of Japan
  • 3. ROR icon RIKEN
  • 4. ROR icon Peking University
  • 5. ROR icon University of Maryland, College Park
  • 6. ROR icon The Graduate University for Advanced Studies, SOKENDAI
  • 7. ROR icon Pontificia Universidad Católica de Chile
  • 8. ROR icon Millennium Institute of Astrophysics
  • 9. ROR icon Space Science Institute
  • 10. ROR icon University of Bologna
  • 11. ROR icon Osservatorio astronomico di Bologna
  • 12. ROR icon Roma Tre University
  • 13. ROR icon Eureka Scientific
  • 14. ROR icon National Radio Astronomy Observatory
  • 15. ROR icon University of Florida
  • 16. ROR icon University of Virginia
  • 17. ROR icon Tel Aviv University
  • 18. ROR icon Tohoku University
  • 19. ROR icon Max Planck Institute for Extraterrestrial Physics
  • 20. ROR icon University of Antofagasta
  • 21. ROR icon Stanford University
  • 22. ROR icon Southern Methodist University
  • 23. ROR icon University College London
  • 24. ROR icon Korea Astronomy and Space Science Institute
  • 25. ROR icon ETH Zurich
  • 26. Argelander Institute for Astronomy
  • 27. ROR icon Kagoshima University
  • 28. ROR icon Yale University
  • 29. ROR icon Atacama Large Millimeter Submillimeter Array
  • 30. ROR icon European Southern Observatory
  • 31. ROR icon George Mason University
  • 32. ROR icon Kyoto University
  • 33. ROR icon California Institute of Technology
  • 34. ROR icon Jet Propulsion Lab
  • 35. ROR icon University of Hawaii at Manoa

Abstract

We present a catalog of the millimeter-wave (mm-wave) continuum properties of 98 nearby (z < 0.05) active galactic nuclei (AGNs) selected from the 70 month Swift/BAT hard-X-ray catalog that have precisely determined X-ray spectral properties and subarcsecond-resolution Atacama Large Millimeter/submillimeter Array Band 6 (211–275 GHz) observations as of 2021 April. Due to the hard-X-ray (>10 keV) selection, the sample is nearly unbiased for obscured systems at least up to Compton-thick-level obscuration, and provides the largest number of AGNs with high-physical-resolution mm-wave data (≲100–200 pc). Our catalog reports emission peak coordinates, spectral indices, and peak fluxes and luminosities at 1.3 mm (230 GHz). Additionally, high-resolution mm-wave images are provided. Using the images and creating radial surface brightness profiles of mm-wave emission, we identify emission extending from the central sources and isolated blob-like emission. Flags indicating the presence of these emission features are tabulated. Among 90 AGNs with significant detections of nuclear emission, 37 AGNs (≈41%) appear to have both or one of extended or blob-like components. We, in particular, investigate AGNs that show well-resolved mm-wave components and find that these seem to have a variety of origins (i.e., a jet, radio lobes, a secondary AGN, stellar clusters, a narrow-line region, galaxy disk, active star formation regions, or AGN-driven outflows), and some components have currently unclear origins.

Copyright and License

© 2023. The Author(s). Published by the American Astronomical Society.

Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Acknowledgement

We thank the reviewer for the useful comments, which helped us improve the quality of the manuscript. We acknowledge support from FONDECYT Postdoctral Fellowships 3200470 (T.K.), 3210157 (A.R.), and 3220516 (M.J.T.), FONDECYT Iniciacion grant 11190831 (C.R.), FONDECYT Regular 1200495 and 1190818 (F.E.B.), ANID BASAL project FB210003 (C.R. and F.E.B), and Millennium Science Initiative Program ICN12_009 (F.E.B). T.K., T.I., and M.I. are supported by JSPS KAKENHI grant Nos. JP20K14529/JP23K13153, JP20K14531, and JP21K03632, respectively. B.T. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement 950533) and from the Israel Science Foundation (grant 1849/19). K.O. acknowledges support from the Korea Astronomy and Space Science Institute under the R&D program (Project No. 2023-1-868-03) supervised by the Ministry of Science and ICT, and the National Research Foundation of Korea (NRF-2020R1C1C1005462). M.B. acknowledges support from the YCAA Prize Postdoctoral Fellowship. The scientific results reported in this article are based on data obtained from the Chandra Data Archive. This research has used software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. This paper uses the following ALMA data: ADS/JAO.ALMA #2012.1.00139.S, #2012.1.00474.S, #2013.1.00525.S, #2013.1.00623.S, #2013.1.01161.S, #2015.1.00086.S, #2015.1.00370.S, #2015.1.00597.S, #2015.1.00872.S, #2016.1.00254.S, #2016.1.00839.S, #2016.1.01140.S, #2016.1.01279.S, #2016.1.01385.S, #2016.1.01553.S, #2017.1.00236.S, #2017.1.00255.S, #2017.1.00395.S, #2017.1.00598.S, #2017.1.00886.L, #2017.1.00904.S, #2017.1.01439.S, #2018.1.00006.S, #2018.1.00037.S, #2018.1.00211.S, #2018.1.00248.S, #2018.1.00538.S, #2018.1.00576.S, #2018.1.00581.S, #2018.1.00657.S, #2018.1.00978.S, and #2019.1.01742.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. Data analysis was in part carried out on the Multi-wavelength Data Analysis System operated by the Astronomy Data Center (ADC), National Astronomical Observatory of Japan. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which 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. This research has made use of the NASA/IPAC Extragalactic Database, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr).

Funding

We acknowledge support from FONDECYT Postdoctral Fellowships 3200470 (T.K.), 3210157 (A.R.), and 3220516 (M.J.T.), FONDECYT Iniciacion grant 11190831 (C.R.), FONDECYT Regular 1200495 and 1190818 (F.E.B.), ANID BASAL project FB210003 (C.R. and F.E.B), and Millennium Science Initiative Program ICN12_009 (F.E.B). T.K., T.I., and M.I. are supported by JSPS KAKENHI grant Nos. JP20K14529/JP23K13153, JP20K14531, and JP21K03632, respectively. B.T. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement 950533) and from the Israel Science Foundation (grant 1849/19). K.O. acknowledges support from the Korea Astronomy and Space Science Institute under the R&D program (Project No. 2023-1-868-03) supervised by the Ministry of Science and ICT, and the National Research Foundation of Korea (NRF-2020R1C1C1005462). M.B. acknowledges support from the YCAA Prize Postdoctoral Fellowship. 

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Created:
December 10, 2024
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December 10, 2024