TY - JOUR
T1 - 3D Spectroscopy with GTC-MEGARA of the Triple AGN Candidate in SDSS J102700.40+174900.8
AU - Benítez, Erika
AU - Ibarra-Medel, Héctor
AU - Negrete, Castalia Alenka
AU - Cruz-González, Irene
AU - Rodríguez-Espinosa, José Miguel
AU - Liu, Xin
AU - Shen, Yue
N1 - We thank the anonymous referee for their valuable comments and suggestions. E.B., I.C.G., and J.M.R.E. acknowledge support from DGAPA-UNAM grant IN113320. I.C.G., E.B., H.I.B., C.A.N., and J.M.R.E. acknowledge support from DGAPA-UNAM grant IN119123. C.A.N. is grateful for support from DGAPA-UNAM grant IN111422 and CONACyT project Paradigmas y Controversias de la Ciencia 2022-320020. H.I.M. acknowledges support from the Instituto Politécnico Nacional (México). J.M.R.E. acknowledges the Spanish State Research Agency under grant number AYA2017-84061-P. J.M.R.E. also acknowledges the Canarian Government under the project PROID2021010077, and is indebted to the Severo Ochoa Programme at the IAC. X.L. acknowledges support from NSF grant AST-2108162. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work is based on data obtained with the MEGARA instrument, funded by European Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER 2014–2020. We acknowledge the support given by the GTC-MEGARA staff, in particular Antonio Cabrera. This work is partly based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. S.D.S.S. acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. Support for Chandra program number 14700279 was provided by NASA through Chandra Award Number GO3-14104X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS 8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. E.B. and I.C.G. acknowledge support from Conacyt Grant CF-2023-G-100.
We thank the anonymous referee for their valuable comments and suggestions. E.B., I.C.G., and J.M.R.E. acknowledge support from DGAPA-UNAM grant IN113320. I.C.G., E.B., H.I.B., C.A.N., and J.M.R.E. acknowledge support from DGAPA-UNAM grant IN119123. C.A.N. is grateful for support from DGAPA-UNAM grant IN111422 and CONACyT project Paradigmas y Controversias de la Ciencia 2022-320020. H.I.M. acknowledges support from the Instituto Politécnico Nacional (México). J.M.R.E. acknowledges the Spanish State Research Agency under grant number AYA2017-84061-P. J.M.R.E. also acknowledges the Canarian Government under the project PROID2021010077, and is indebted to the Severo Ochoa Programme at the IAC. X.L. acknowledges support from NSF grant AST-2108162. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work is based on data obtained with the MEGARA instrument, funded by European Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER 2014-2020. We acknowledge the support given by the GTC-MEGARA staff, in particular Antonio Cabrera. This work is partly based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. S.D.S.S. acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. Support for Chandra program number 14700279 was provided by NASA through Chandra Award Number GO3-14104X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS 8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. E.B. and I.C.G. acknowledge support from Conacyt Grant CF-2023-G-100.
PY - 2023/7/1
Y1 - 2023/7/1
N2 - Triple-active galactic nucleus (AGN) systems are expected to be the result of the hierarchical model of galaxy formation. Since there are very few of them confirmed as such, we present the results of a new study of the triple AGN candidate SDSS J102700.40+174900.8 (center nucleus) through observations with the GTC-MEGARA Integral Field Unit. 1D and 2D analysis of the line ratios of the three nuclei allow us to locate them in the EW(Hα) versus [N ii]/Hα diagram. The central nucleus is found to be a retired galaxy (or fake AGN). The neighbors are found to be a strong AGN (southeastern nucleus, J102700.55+174900.2), compatible with a Seyfert 2 (Sy2) galaxy, and a weak AGN (northern nucleus, J102700.38+174902.6), compatible with a LINER2. We find evidence that the neighbors constitute a dual AGN system (Sy2-LINER2) with a projected separation of 3.98 kpc in the optical bands. The Hα velocity map shows that the northern nucleus has an Hα emission with a velocity offset of ∼−500 km s−1, whereas the southeastern nucleus has a rotating disk and Hα extended emission at kiloparsec scales. Chandra archival data confirm that the neighbors have X-ray (0.5-2) keV and (2-7) keV emission, whereas the center nucleus shows no X-ray emission. A collisional ring with knots is observed in Hubble Space Telescope images of the southeastern nucleus. These knots coincide with star formation regions that, along with the ring, are predicted in a head-on collision. In this case, the morphology changes are probably due to a minor merger that was produced by the passing of the northern through the southeastern nucleus.
AB - Triple-active galactic nucleus (AGN) systems are expected to be the result of the hierarchical model of galaxy formation. Since there are very few of them confirmed as such, we present the results of a new study of the triple AGN candidate SDSS J102700.40+174900.8 (center nucleus) through observations with the GTC-MEGARA Integral Field Unit. 1D and 2D analysis of the line ratios of the three nuclei allow us to locate them in the EW(Hα) versus [N ii]/Hα diagram. The central nucleus is found to be a retired galaxy (or fake AGN). The neighbors are found to be a strong AGN (southeastern nucleus, J102700.55+174900.2), compatible with a Seyfert 2 (Sy2) galaxy, and a weak AGN (northern nucleus, J102700.38+174902.6), compatible with a LINER2. We find evidence that the neighbors constitute a dual AGN system (Sy2-LINER2) with a projected separation of 3.98 kpc in the optical bands. The Hα velocity map shows that the northern nucleus has an Hα emission with a velocity offset of ∼−500 km s−1, whereas the southeastern nucleus has a rotating disk and Hα extended emission at kiloparsec scales. Chandra archival data confirm that the neighbors have X-ray (0.5-2) keV and (2-7) keV emission, whereas the center nucleus shows no X-ray emission. A collisional ring with knots is observed in Hubble Space Telescope images of the southeastern nucleus. These knots coincide with star formation regions that, along with the ring, are predicted in a head-on collision. In this case, the morphology changes are probably due to a minor merger that was produced by the passing of the northern through the southeastern nucleus.
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U2 - 10.3847/1538-4357/acce3e
DO - 10.3847/1538-4357/acce3e
M3 - Article
AN - SCOPUS:85165720965
SN - 0004-637X
VL - 952
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 45
ER -