CaltechAUTHORS
  A Caltech Library Service

BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc

Kawamuro, Taiki and Ricci, Claudio and Imanishi, Masatoshi and Mushotzky, Richard F. and Izumi, Takuma and Ricci, Federica and Bauer, Franz E. and Koss, Michael J. and Trakhtenbrot, Benny and Ichikawa, Kohei and Rojas, Alejandra F. and Smith, Krista Lynne and Shimizu, Taro and Oh, Kyuseok and den Brok, Jakob S. and Baba, Shunsuke and Baloković, Mislav and Chang, Chin-Shin and Kakkad, Darshan and Pfeifle, Ryan W. and Privon, George C. and Temple, Matthew J. and Ueda, Yoshihiro and Harrison, Fiona A. and Powell, Meredith C. and Stern, Daniel and Urry, Meg and Sanders, David B. (2022) BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc. Astrophysical Journal, 938 (1). Art. No. 87. ISSN 0004-637X. doi:10.3847/1538-4357/ac8794. https://resolver.caltech.edu/CaltechAUTHORS:20221025-983475200.3

Full text is not posted in this repository. Consult Related URLs below.

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20221025-983475200.3

Abstract

To understand the origin of nuclear (≲100 pc) millimeter-wave (mm-wave) continuum emission in active galactic nuclei (AGNs), we systematically analyzed subarcsecond resolution Band-6 (211–275 GHz) Atacama Large Millimeter/submillimeter Array data of 98 nearby AGNs (z < 0.05) from the 70 month Swift/BAT catalog. The sample, almost unbiased for obscured systems, provides the largest number of AGNs to date with high mm-wave spatial resolution sampling (∼1–200 pc), and spans broad ranges of 14–150 keV luminosity {40 < log[L₁₄₋₁₅₀/(erg s⁻¹)] < 45}, black hole mass [5 < log(M_(BH)M_(⊙)) < 10], and Eddington ratio (-4 < logλ_(Edd) < 2). We find a significant correlation between 1.3 mm (230 GHz) and 14–150 keV luminosities. Its scatter is ≈0.36 dex, and the mm-wave emission may serve as a good proxy of the AGN luminosity, free of dust extinction up to N_H ∼ 10²⁶ cm⁻². While the mm-wave emission could be self-absorbed synchrotron radiation around the X-ray corona according to past works, we also discuss different possible origins of the mm-wave emission: AGN-related dust emission, outflow-driven shocks, and a small-scale (<200 pc) jet. The dust emission is unlikely to be dominant, as the mm-wave slope is generally flatter than expected. Also, due to no increase in the mm-wave luminosity with the Eddington ratio, a radiation-driven outflow model is possibly not the common mechanism. Furthermore, we find independence of the mm-wave luminosity on indicators of the inclination angle from the polar axis of the nuclear structure, which is inconsistent with a jet model whose luminosity depends only on the angle.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ac8794DOIArticle
ORCID:
AuthorORCID
Kawamuro, Taiki0000-0002-6808-2052
Ricci, Claudio0000-0001-5231-2645
Imanishi, Masatoshi0000-0001-6186-8792
Mushotzky, Richard F.0000-0002-7962-5446
Izumi, Takuma0000-0001-9452-0813
Ricci, Federica0000-0001-5742-5980
Bauer, Franz E.0000-0002-8686-8737
Koss, Michael J.0000-0002-7998-9581
Trakhtenbrot, Benny0000-0002-3683-7297
Ichikawa, Kohei0000-0002-4377-903X
Rojas, Alejandra F.0000-0003-0006-8681
Smith, Krista Lynne0000-0001-5785-7038
Shimizu, Taro0000-0002-2125-4670
Oh, Kyuseok0000-0002-5037-951X
den Brok, Jakob S.0000-0002-8760-6157
Baba, Shunsuke0000-0002-9850-6290
Baloković, Mislav0000-0003-0476-6647
Chang, Chin-Shin0000-0001-9910-3234
Kakkad, Darshan0000-0002-2603-2639
Pfeifle, Ryan W.0000-0001-8640-8522
Privon, George C.0000-0003-3474-1125
Temple, Matthew J.0000-0001-8433-550X
Ueda, Yoshihiro0000-0001-7821-6715
Harrison, Fiona A.0000-0003-2992-8024
Powell, Meredith C.0000-0003-2284-8603
Stern, Daniel0000-0003-2686-9241
Urry, Meg0000-0002-0745-9792
Sanders, David B.0000-0002-1233-9998
Additional Information: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., 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, JP20K14531, and JP21K03632, respectively. F.R. acknowledges support from PRIN MIUR 2017 PH3WAT ("Black hole winds and the baryon life cycle of galaxies"). K.O. acknowledges support from 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 made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. This paper makes use of 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, #2015.1.00925.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, #2016.2.00046.S, #2016.2.00055.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, #2017.1.01158.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, #2018.1.00986.S, #2018.1.01321.S, #2019.1.00363.S, #2019.1.00763.L, #2019.1.01229.S, #2019.1.01742.S, and #2019.2.00129.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 Multiwavelength Data Analysis System operated by the Astronomy Data Center (ADC), National Astronomical Observatory of Japan.
Group:Astronomy Department, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3200470
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3210157
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3220516
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)11190831
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1200495
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1190818
Agencia Nacional de Investigación y Desarrollo (ANID)FB210003
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)ICN12 009
Japan Society for the Promotion of Science (JSPS)JP20K14529
Japan Society for the Promotion of Science (JSPS)JP20K14531
Japan Society for the Promotion of Science (JSPS)JP21K03632
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)PH3WAT
National Research Foundation of KoreaNRF-2020R1C1C1005462
Yale Center for Astronomy and AstrophysicsUNSPECIFIED
Issue or Number:1
DOI:10.3847/1538-4357/ac8794
Record Number:CaltechAUTHORS:20221025-983475200.3
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20221025-983475200.3
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:117571
Collection:CaltechAUTHORS
Deposited By: Research Services Depository
Deposited On:08 Nov 2022 19:25
Last Modified:08 Nov 2022 19:25

Repository Staff Only: item control page