Another X-ray UFO without a momentum-boosted molecular outflow

Author(s): Francesca Bonanomi, Claudia Cicone, Paola Severgnini, Valentina Braito, Cristian Vignali, James N. Reeves, Mattia Sirressi, Isabel Montoya Arroyave, Roberto Della Ceca, Lucia Ballo, Massimo Dotti
Abstract: We present Atacama Large Millimetre/submillimetre Array (ALMA) CO(1–0) observations of the nearby infrared luminous (LIRG) galaxy pair IRAS 05054+1718 (also known as CGCG 468-002), as well as a new analysis of X-ray data of this source collected between 2012 and 2021 using the Nuclear Spectroscopic Telescope Array (NuSTAR), Swift, and the XMM-Newton satellites. The western component of the pair, NED01, hosts a Seyfert 1.9 nucleus that is responsible for launching a powerful X-ray ultra-fast outflow (UFO). Our X-ray spectral analysis suggests that the UFO could be variable or multi-component in velocity, ranging from v/c ∼ −0.12 (as seen in Swift) to v/c ∼ −0.23 (as seen in NuSTAR), and constrains its momentum flux to be p_out^X−ray ∼ (4 ± 2) × 10³⁴ g cm s⁻². The ALMA CO(1–0) observations, obtained with an angular resolution of 2.2⁰⁰, although targeting mainly NED01, also include the eastern component of the pair, NED02, a less-studied LIRG with no clear evidence of an active galactic nucleus (AGN). We study the CO(1–0) kinematics in the two galaxies using the 3D-BAROLO code. In both sources we can model the bulk of the CO(1–0) emission with rotating disks and, after subtracting the best-fit models, we detect compact residual emission at S/N = 15 within ∼3 kpc of the centre. A molecular outflow in NED01, if present, cannot be brighter than such residuals, implying an upper limit on its outflow rate of M _out^mol . 19 ± 14 M yr⁻¹ and on its momentum rate of p^mol_out . (2.7 ± 2.4) × 10³⁴ g cm s⁻¹. Combined with the revised energetics of the X-ray wind, we derive an upper limit on the momentum rate ratio of p^mol_out / p^X_out^−ray < 0.67. We discuss these results in the context of the expectations of AGN feedback models, and we propose that the X-ray disk wind in NED01 has not significantly impacted the molecular gas reservoir (yet), and we can constrain its effect to be much smaller than expectations of AGN ‘energy-driven’ feedback models. We also consider and discuss the hypothesis of asymmetries of the molecular disk not properly captured by the 3D-BAROLO code. Our results highlight the challenges in testing the predictions of popular AGN disk-wind feedback theories, even in the presence of good-quality multi-wavelength observations.
Organisation(s): Department of Astrophysics
External organisation(s): Instituto Nazionale die Astrofisica (INAF), Università degli Studi di Milano-Bicocca, University of Oslo, INAF Osservatorio Astronomico di Brera, Catholic University of America, University of Bologna, Oskar Klein Centre, European Space Astronomy Centre (ESA)
Journal: Astronomy and Astrophysics
Volume: 673
No. of pages: 24
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/202245630
Publication date: 05-2023
Peer reviewed: Yes
Austrian Fields of Science 2012: 103003 Astronomy, 103004 Astrophysics
Keywords
ASJC Scopus subject areas: Astronomy and Astrophysics, Space and Planetary Science
Portal url: https://ucrisportal.univie.ac.at/en/publications/effcb218-5c05-4f53-9ec0-c6647b662819

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