Low-power jet-interstellar medium interaction in NGC 7319 revealed by JWST/MIRI MRS
Low-power jet-interstellar medium interaction in NGC 7319 revealed by JWST/MIRI MRS
We present JWST/MIRI MRS spectroscopy of NGC7319, the largest galaxy in the Stephan's Quintet, observed as part of the Early Release Observations (ERO). NGC7319 hosts a type 2 active galactic nucleus (AGN) and a low-power radio jet (L_1.4GHz = 3.3x1022 W Hz-1) with two asymmetric radio hotspots at 430 pc (N2) and 1.5 kpc (S2) projected distances from the unresolved radio core. The MRS data suggest that the molecular material in the disk of the galaxy decelerates the jet and causes this length asymmetry. We find enhanced emission from warm and hot H_2 (T_w=330+-40 K, T_h = 900+-60 K) and ionized gas at the intersection between the jet axis and dust lanes in the disk. This emission is coincident with the radio hotspot N2, the hotspot closer to the core, suggesting that the jet-interstellar medium (ISM) interaction decelerates the jet. Conversely, the mid-infrared emission at the more distant hotspot is fainter, more highly ionized, and with lower H_2 excitation, suggesting a more diffuse atomic environment where the jet can progress to farther distances. At the N2 radio hotspot, the ionizedgas mass (M_ion = (2.4-12)x105 Msun) is comparable to that of the warm H_2, but the former is more turbulent (sigma_ion~300 vs. sigma_H2~150km/s), so the mechanical energy of the ionized gas is ~1.3-10 times higher. From these estimates, we find that only 0.3-1.5 kpc) high-ionization emission ([MgV], [NeVI], and[NeV]) close to the radio hotspots. This initial analysis of NGC7319 shows the potential of MIRI/MRS to investigate the AGN feedback mechanisms due to radio jets and their radiation field in the, often heavily dust-enshrouded, central regions of galaxies. Understanding these mechanisms is an essential ingredient in the development of cosmological simulations of galaxy evolution.
Astrophysics - Astrophysics of Galaxies, Galaxies: ISM, Galaxies: jets, Infrared: galaxies
Pereira-Santaella, M.
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Álvarez-Márquez, J.
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García-Bernete, I.
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Labiano, A.
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Colina, L.
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Alonso-Herrero, A.
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Bellocchi, E.
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García-Burillo, S.
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Hönig, S. F.
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Ramos Almeida, C.
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Rosario, D.
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23 September 2022
Pereira-Santaella, M.
273d2fb4-ea55-4bd1-9031-37bf7a2cda75
Álvarez-Márquez, J.
1e7ffc0a-615a-403e-a7bb-f7ccf4e260cb
García-Bernete, I.
b9dbd878-1c37-4ba0-883d-acf9ba7dcd79
Labiano, A.
59c841a1-579a-40e1-a87b-76e643147522
Colina, L.
4419ad4b-e4a9-4ead-ba4a-c9cf7ac0bcbe
Alonso-Herrero, A.
ae11bfb3-7ba7-43a3-a071-8fac055b6f62
Bellocchi, E.
e7dfe770-16bb-48af-b6b3-d74949409512
García-Burillo, S.
56a7c385-47c0-4550-ba26-f939f36d071a
Hönig, S. F.
be0bb8bc-bdac-4442-8edc-f735834f3917
Ramos Almeida, C.
5de8e01a-be52-4502-864b-f47ea0d6473c
Rosario, D.
3e714b97-1e01-4691-813a-e0f7e510d9de
Pereira-Santaella, M., Álvarez-Márquez, J., García-Bernete, I., Labiano, A., Colina, L., Alonso-Herrero, A., Bellocchi, E., García-Burillo, S., Hönig, S. F., Ramos Almeida, C. and Rosario, D.
(2022)
Low-power jet-interstellar medium interaction in NGC 7319 revealed by JWST/MIRI MRS.
Astronomy & Astrophysics, 665 (L11), [L11].
(doi:10.1051/0004-6361/202244725).
Abstract
We present JWST/MIRI MRS spectroscopy of NGC7319, the largest galaxy in the Stephan's Quintet, observed as part of the Early Release Observations (ERO). NGC7319 hosts a type 2 active galactic nucleus (AGN) and a low-power radio jet (L_1.4GHz = 3.3x1022 W Hz-1) with two asymmetric radio hotspots at 430 pc (N2) and 1.5 kpc (S2) projected distances from the unresolved radio core. The MRS data suggest that the molecular material in the disk of the galaxy decelerates the jet and causes this length asymmetry. We find enhanced emission from warm and hot H_2 (T_w=330+-40 K, T_h = 900+-60 K) and ionized gas at the intersection between the jet axis and dust lanes in the disk. This emission is coincident with the radio hotspot N2, the hotspot closer to the core, suggesting that the jet-interstellar medium (ISM) interaction decelerates the jet. Conversely, the mid-infrared emission at the more distant hotspot is fainter, more highly ionized, and with lower H_2 excitation, suggesting a more diffuse atomic environment where the jet can progress to farther distances. At the N2 radio hotspot, the ionizedgas mass (M_ion = (2.4-12)x105 Msun) is comparable to that of the warm H_2, but the former is more turbulent (sigma_ion~300 vs. sigma_H2~150km/s), so the mechanical energy of the ionized gas is ~1.3-10 times higher. From these estimates, we find that only 0.3-1.5 kpc) high-ionization emission ([MgV], [NeVI], and[NeV]) close to the radio hotspots. This initial analysis of NGC7319 shows the potential of MIRI/MRS to investigate the AGN feedback mechanisms due to radio jets and their radiation field in the, often heavily dust-enshrouded, central regions of galaxies. Understanding these mechanisms is an essential ingredient in the development of cosmological simulations of galaxy evolution.
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Accepted/In Press date: 13 September 2022
Published date: 23 September 2022
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We thank the referee for their useful comments and suggestions. We thank P. Gandhi and E. Hicks for the careful reading of the manuscript and useful discussion. The authors acknowledge the ERO team for developing their observing program with a zero-exclusive-access period. MPS acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). JAM, AL, and LC acknowledge support by grant PIB2021-127718NB-100 by the Spanish Ministry of Science and Innovation/State Agency of Research (MCIN/AEI). IGB acknowledges support from STFC through grant ST/S000488/1. AAH acknowledges support from grant PGC2018-094671-B-I00 funded by MCIN/AEI/ 10.13039/501100011033 and by ERDF A way of making Europe. SGB acknowledges support from the research project PID2019-106027GA-C44 of the Spanish Ministerio de Ciencia e Innovación. CRA acknowledges support from grant PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033, from EUR2020-112266, funded by MICINN-AEI/10.13039/501100011033 and the European Union NextGenerationEU/PRTR, and from the Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant ProID2020010105, ACCISI/FEDER, UE. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST; and from the European JWST archive (eJWST) operated by the ESAC Science Data Centre (ESDC) of the European Space Agency. These observations are associated with program #2732, #1049, #1050. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with programs 11502 and 12301.
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Keywords:
Astrophysics - Astrophysics of Galaxies, Galaxies: ISM, Galaxies: jets, Infrared: galaxies
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Local EPrints ID: 471936
URI: http://eprints.soton.ac.uk/id/eprint/471936
ISSN: 0004-6361
PURE UUID: 34a557e5-5b12-4916-b3cf-e9d3cb0ce00d
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Date deposited: 22 Nov 2022 17:58
Last modified: 16 Mar 2024 22:55
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Author:
M. Pereira-Santaella
Author:
J. Álvarez-Márquez
Author:
I. García-Bernete
Author:
A. Labiano
Author:
L. Colina
Author:
A. Alonso-Herrero
Author:
E. Bellocchi
Author:
S. García-Burillo
Author:
C. Ramos Almeida
Author:
D. Rosario
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