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A precessing jet from an active galactic nucleus drives gas outflow from a disk galaxy.

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Title: A precessing jet from an active galactic nucleus drives gas outflow from a disk galaxy.
Authors: Kader, Justin A. (AUTHOR), U, Vivian (AUTHOR), Barcos-Muñoz, Loreto (AUTHOR), Bianchin, Marina (AUTHOR), Song, Yiqing (AUTHOR), Linden, Sean T. (AUTHOR), Canalizo, Gabriela (AUTHOR), Aravindan, Archana (AUTHOR), Privon, George C. (AUTHOR), Díaz-Santos, Tanio (AUTHOR), Hayward, Christopher (AUTHOR), Malkan, Matthew A. (AUTHOR), Armus, Lee (AUTHOR), McGurk, Rosalie C. (AUTHOR), Rich, Jeffrey A. (AUTHOR), Medling, Anne M. (AUTHOR), Stierwalt, Sabrina (AUTHOR), Max, Claire E. (AUTHOR), Evans, Aaron S. (AUTHOR), Agostino, Christopher J. (AUTHOR)
Source: Science. 2/26/2026, Vol. 391 Issue 6788, p911-916. 6p.
Subjects: Active galactic nuclei, Astrophysical jets, Ionized gases, Astronomical observations, Galaxies, Star formation, Supermassive black holes, Galactic evolution
Abstract: To reproduce observed galaxy properties, cosmological simulations require that massive galaxies experience feedback from active galactic nuclei, which regulates star formation within those galaxies. However, the energetics and timescales of these feedback processes are poorly constrained. We combined optical, infrared, submillimeter, and radio observations of the active galaxy VV 340a, which is hosting a low-power jet launched from a supermassive black hole at its center. We found that the jet undergoes precession, with a period of (8.2 ± 5.5) × 105 years, and drives an outflow of gas at a rate of 19.4 ± 7.9 solar masses per year. The jet shocks the gas, producing highly ionized plasma that extends several kiloparsecs from the nucleus. The outflow ejects sufficient gas from the galaxy to influence its star-formation rate. Editor's summary: Star formation in galaxies is regulated by various feedback processes, including from a supermassive black hole accreting at the galaxy's center, an active galactic nucleus (AGN). Theoretical models of AGN feedback indicate that gas can be ejected by a jet launched by the AGN; however, directly observing that process is difficult. Kader et al. combined observations at multiple wavelengths to investigate different components of a nearby galaxy with a low-power AGN. They identified an outflow of ionized gas and showed that is it driven by a jet from the AGN. The jet undergoes precession, producing a biconical outflow of gas. —Keith T. Smith INTRODUCTION: Galaxies consist of stars, gas, and black holes, which interact as the galaxy evolves over time. Theoretical models indicate that feedback from stars and accreting supermassive black holes [an active galactic nucleus (AGN)] affects the physical conditions in the gas reservoir and ejects some gas from the galaxy through winds and outflows. Galactic outflows driven by active supermassive black holes reduce the galaxy's reservoir of cold gas, which is the fuel for star formation, potentially halting star formation entirely. The underlying physics of this AGN feedback process is difficult to discern without multifaceted observations. RATIONALE: The physical mechanisms for AGN feedback manifest differently at different physical scales and components of a galaxy's interstellar medium. Determining the energetics, geometry, and timescales of this feedback mode requires multiwavelength observations that probe the interstellar gas on multiple scales. AGN feedback in the form of galactic outflows is common in interacting galaxy systems, so we investigated the early-stage galaxy merger VV 340. The proximity of the merging system (157 Mpc) and the edge-on orientation of the northern component VV 340a facilitate the separation of the gas outflows from the disk of this spiral galaxy. We used observations of VV 340a with integral field spectroscopy at optical and mid-infrared wavelengths and imaging at radio, submillimeter, and x-ray wavelengths to assess the influence of AGN feedback on the evolution of this galaxy. RESULTS: Mid-infrared integral-field spectroscopy of the high-ionization [Ne v] emission line shows an extended (3 kpc) and highly collimated outflow of gas away from the central AGN. The outflow extends into the galactic halo (at least 15 kpc from the galactic center), where it appears in the optical integral field spectroscopy of the lower-ionization [O iii] emission line. This lower-ionization gas exhibits a similar morphology and velocity structure to those of the higher-ionization gas. An S-shaped jet is visible in the radio continuum images, which aligns with the collimated ionized gas outflow. We interpret these features as being due to a precessing jet driving the gas outflow. Modeling of this scenario indicates a mass outflow rate of 19.4 ± 7.9 solar masses per year and a precession period of (8.2 ± 5.5) × 105 years. CONCLUSION: The collimated morphology and optical emission line ratios observed in the extraplanar nebulae indicate that the radio jet is the dominant mechanism driving the outflow. Our calculation of the mass outflow rate indicates that it is not sufficient to outpace star formation in the galaxy but is enough to substantially reduce the gas depletion timescale. Therefore, the AGN feedback from the radio jet affects the star formation history of VV 340a. Multiwavelength image of the edge-on galaxy VV 340a.: A background optical image is overlain with [O iii] gas emission (semitransparent blue layer), which extends for 15 kpc. White contours indicate the radio continuum emission, showing the S-shaped jet extending from the central AGN and the disc of the galaxy. [ABSTRACT FROM AUTHOR]
Copyright of Science is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: A precessing jet from an active galactic nucleus drives gas outflow from a disk galaxy.
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  Data: <searchLink fieldCode="AR" term="%22Kader%2C+Justin+A%2E%22">Kader, Justin A.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22U%2C+Vivian%22">U, Vivian</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Barcos-Muñoz%2C+Loreto%22">Barcos-Muñoz, Loreto</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Bianchin%2C+Marina%22">Bianchin, Marina</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Song%2C+Yiqing%22">Song, Yiqing</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Linden%2C+Sean+T%2E%22">Linden, Sean T.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Canalizo%2C+Gabriela%22">Canalizo, Gabriela</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Aravindan%2C+Archana%22">Aravindan, Archana</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Privon%2C+George+C%2E%22">Privon, George C.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Díaz-Santos%2C+Tanio%22">Díaz-Santos, Tanio</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Hayward%2C+Christopher%22">Hayward, Christopher</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Malkan%2C+Matthew+A%2E%22">Malkan, Matthew A.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Armus%2C+Lee%22">Armus, Lee</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22McGurk%2C+Rosalie+C%2E%22">McGurk, Rosalie C.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Rich%2C+Jeffrey+A%2E%22">Rich, Jeffrey A.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Medling%2C+Anne+M%2E%22">Medling, Anne M.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Stierwalt%2C+Sabrina%22">Stierwalt, Sabrina</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Max%2C+Claire+E%2E%22">Max, Claire E.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Evans%2C+Aaron+S%2E%22">Evans, Aaron S.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Agostino%2C+Christopher+J%2E%22">Agostino, Christopher J.</searchLink> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Science%22">Science</searchLink>. 2/26/2026, Vol. 391 Issue 6788, p911-916. 6p.
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  Data: <searchLink fieldCode="DE" term="%22Active+galactic+nuclei%22">Active galactic nuclei</searchLink><br /><searchLink fieldCode="DE" term="%22Astrophysical+jets%22">Astrophysical jets</searchLink><br /><searchLink fieldCode="DE" term="%22Ionized+gases%22">Ionized gases</searchLink><br /><searchLink fieldCode="DE" term="%22Astronomical+observations%22">Astronomical observations</searchLink><br /><searchLink fieldCode="DE" term="%22Galaxies%22">Galaxies</searchLink><br /><searchLink fieldCode="DE" term="%22Star+formation%22">Star formation</searchLink><br /><searchLink fieldCode="DE" term="%22Supermassive+black+holes%22">Supermassive black holes</searchLink><br /><searchLink fieldCode="DE" term="%22Galactic+evolution%22">Galactic evolution</searchLink>
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  Data: To reproduce observed galaxy properties, cosmological simulations require that massive galaxies experience feedback from active galactic nuclei, which regulates star formation within those galaxies. However, the energetics and timescales of these feedback processes are poorly constrained. We combined optical, infrared, submillimeter, and radio observations of the active galaxy VV 340a, which is hosting a low-power jet launched from a supermassive black hole at its center. We found that the jet undergoes precession, with a period of (8.2 ± 5.5) × 105 years, and drives an outflow of gas at a rate of 19.4 ± 7.9 solar masses per year. The jet shocks the gas, producing highly ionized plasma that extends several kiloparsecs from the nucleus. The outflow ejects sufficient gas from the galaxy to influence its star-formation rate. Editor's summary: Star formation in galaxies is regulated by various feedback processes, including from a supermassive black hole accreting at the galaxy's center, an active galactic nucleus (AGN). Theoretical models of AGN feedback indicate that gas can be ejected by a jet launched by the AGN; however, directly observing that process is difficult. Kader et al. combined observations at multiple wavelengths to investigate different components of a nearby galaxy with a low-power AGN. They identified an outflow of ionized gas and showed that is it driven by a jet from the AGN. The jet undergoes precession, producing a biconical outflow of gas. —Keith T. Smith INTRODUCTION: Galaxies consist of stars, gas, and black holes, which interact as the galaxy evolves over time. Theoretical models indicate that feedback from stars and accreting supermassive black holes [an active galactic nucleus (AGN)] affects the physical conditions in the gas reservoir and ejects some gas from the galaxy through winds and outflows. Galactic outflows driven by active supermassive black holes reduce the galaxy's reservoir of cold gas, which is the fuel for star formation, potentially halting star formation entirely. The underlying physics of this AGN feedback process is difficult to discern without multifaceted observations. RATIONALE: The physical mechanisms for AGN feedback manifest differently at different physical scales and components of a galaxy's interstellar medium. Determining the energetics, geometry, and timescales of this feedback mode requires multiwavelength observations that probe the interstellar gas on multiple scales. AGN feedback in the form of galactic outflows is common in interacting galaxy systems, so we investigated the early-stage galaxy merger VV 340. The proximity of the merging system (157 Mpc) and the edge-on orientation of the northern component VV 340a facilitate the separation of the gas outflows from the disk of this spiral galaxy. We used observations of VV 340a with integral field spectroscopy at optical and mid-infrared wavelengths and imaging at radio, submillimeter, and x-ray wavelengths to assess the influence of AGN feedback on the evolution of this galaxy. RESULTS: Mid-infrared integral-field spectroscopy of the high-ionization [Ne v] emission line shows an extended (3 kpc) and highly collimated outflow of gas away from the central AGN. The outflow extends into the galactic halo (at least 15 kpc from the galactic center), where it appears in the optical integral field spectroscopy of the lower-ionization [O iii] emission line. This lower-ionization gas exhibits a similar morphology and velocity structure to those of the higher-ionization gas. An S-shaped jet is visible in the radio continuum images, which aligns with the collimated ionized gas outflow. We interpret these features as being due to a precessing jet driving the gas outflow. Modeling of this scenario indicates a mass outflow rate of 19.4 ± 7.9 solar masses per year and a precession period of (8.2 ± 5.5) × 105 years. CONCLUSION: The collimated morphology and optical emission line ratios observed in the extraplanar nebulae indicate that the radio jet is the dominant mechanism driving the outflow. Our calculation of the mass outflow rate indicates that it is not sufficient to outpace star formation in the galaxy but is enough to substantially reduce the gas depletion timescale. Therefore, the AGN feedback from the radio jet affects the star formation history of VV 340a. Multiwavelength image of the edge-on galaxy VV 340a.: A background optical image is overlain with [O iii] gas emission (semitransparent blue layer), which extends for 15 kpc. White contours indicate the radio continuum emission, showing the S-shaped jet extending from the central AGN and the disc of the galaxy. [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
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  Data: <i>Copyright of Science is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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      – SubjectFull: Ionized gases
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