Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo
It has long been suspected that powerful radio sources may lower the efficiency with which stars form from the molecular gas in their host galaxy, however so far, alternative mechanisms, in particular related to the stellar mass distribution in the massive bulges of their host galaxies, have not bee...
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| creator | Nesvadba, N. P. H. Wagner, A. Y. Mukherjee, D. Mandal, A. Janssen, R. M. J. Zovaro, H. Neumayer, N. Bagchi, J. Bicknell, G. |
| description | It has long been suspected that powerful radio sources may lower the efficiency with which stars form from the molecular gas in their host galaxy, however so far, alternative mechanisms, in particular related to the stellar mass distribution in the massive bulges of their host galaxies, have not been ruled out. We present new, arcsecond-resolution Atacama Large Millimeter Array (ALMA) CO(1−0) interferometry, which probes the spatially resolved, cold molecular gas in the nearby (
z
= 0.08), massive (
M
stellar
= 4 × 10
11
M
⊙
), isolated, late-type spiral galaxy 2MASSX J23453269−044925, which is outstanding for having two pairs of powerful, giant radio jets, and a bright X-ray halo of hot circumgalactic gas. The molecular gas is in a massive (
M
gas
= 2.0 × 10
10
M
⊙
), 24 kpc wide, rapidly rotating ring, which is associated with the inner stellar disk. Broad (
FWHM
= 70−180 km s
−1
) emission lines with complex profiles associated with the radio source are seen over large regions in the ring, indicating gas velocities that are high enough to keep the otherwise marginally Toomre-stable gas from fragmenting into gravitationally bound, star-forming clouds. About 1−2% of the jet kinetic energy is required to power these motions. Resolved star-formation rate surface densities derived from Galaxy Evolution Explorer and Wide-Field Infrared Survey Explorer fall by factors of 30−70 short of expectations from the standard Kennicutt–Schmidt law of star-forming galaxies, and near gas-rich early-type galaxies with signatures of star formation that are lowered by jet feedback. We argue that radio Active Galactic Nucleus (AGN) feedback is the only plausible mechanism to explain the low star-formation rates in this galaxy. Previous authors have already noted that the X-ray halo of J2345−0449 implies a baryon fraction that is close to the cosmic average, which is very high for a galaxy. We contrast this finding with other, equally massive, and equally baryon-rich spiral galaxies without prominent radio sources. Most of the baryons in these galaxies are in stars, not in the halos. We also discuss the implications of our results for our general understanding of AGN feedback in massive galaxies. |
| doi_str_mv | 10.1051/0004-6361/202140544 |
| format | Article |
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z
= 0.08), massive (
M
stellar
= 4 × 10
11
M
⊙
), isolated, late-type spiral galaxy 2MASSX J23453269−044925, which is outstanding for having two pairs of powerful, giant radio jets, and a bright X-ray halo of hot circumgalactic gas. The molecular gas is in a massive (
M
gas
= 2.0 × 10
10
M
⊙
), 24 kpc wide, rapidly rotating ring, which is associated with the inner stellar disk. Broad (
FWHM
= 70−180 km s
−1
) emission lines with complex profiles associated with the radio source are seen over large regions in the ring, indicating gas velocities that are high enough to keep the otherwise marginally Toomre-stable gas from fragmenting into gravitationally bound, star-forming clouds. About 1−2% of the jet kinetic energy is required to power these motions. Resolved star-formation rate surface densities derived from Galaxy Evolution Explorer and Wide-Field Infrared Survey Explorer fall by factors of 30−70 short of expectations from the standard Kennicutt–Schmidt law of star-forming galaxies, and near gas-rich early-type galaxies with signatures of star formation that are lowered by jet feedback. We argue that radio Active Galactic Nucleus (AGN) feedback is the only plausible mechanism to explain the low star-formation rates in this galaxy. Previous authors have already noted that the X-ray halo of J2345−0449 implies a baryon fraction that is close to the cosmic average, which is very high for a galaxy. We contrast this finding with other, equally massive, and equally baryon-rich spiral galaxies without prominent radio sources. Most of the baryons in these galaxies are in stars, not in the halos. We also discuss the implications of our results for our general understanding of AGN feedback in massive galaxies.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/202140544</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Active galactic nuclei ; Astrophysics ; Baryons ; Feedback ; Galactic bulge ; Galactic evolution ; Galactic halos ; Galaxy distribution ; Infrared astronomy ; Kinetic energy ; Legal issues ; Mass distribution ; Molecular gases ; Physics ; Radio astronomy ; Radio jets (astronomy) ; Radio sources (astronomy) ; Radio telescopes ; Space telescopes ; Spiral galaxies ; Star & galaxy formation ; Star formation ; Stars & galaxies ; Stellar evolution ; Stellar mass ; X-ray astronomy</subject><ispartof>Astronomy and astrophysics (Berlin), 2021-10, Vol.654, p.A8</ispartof><rights>2021. This work is licensed under http://creativecommons.org/licenses/by/4.0 (the “License”). Notwithstanding the ProQuest Terms and conditions, you may use this content in accordance with the terms of the License.</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c356t-90afb3e53a19b07178fc3a781cfa6a901acf8973a41ab0b6a4624c0b24ec5c1f3</citedby><cites>FETCH-LOGICAL-c356t-90afb3e53a19b07178fc3a781cfa6a901acf8973a41ab0b6a4624c0b24ec5c1f3</cites><orcidid>0000-0001-5783-6544 ; 0000-0002-1852-2507</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,3713,27903,27904</link.rule.ids><backlink>$$Uhttps://hal.science/hal-03362653$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Nesvadba, N. P. H.</creatorcontrib><creatorcontrib>Wagner, A. Y.</creatorcontrib><creatorcontrib>Mukherjee, D.</creatorcontrib><creatorcontrib>Mandal, A.</creatorcontrib><creatorcontrib>Janssen, R. M. J.</creatorcontrib><creatorcontrib>Zovaro, H.</creatorcontrib><creatorcontrib>Neumayer, N.</creatorcontrib><creatorcontrib>Bagchi, J.</creatorcontrib><creatorcontrib>Bicknell, G.</creatorcontrib><title>Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo</title><title>Astronomy and astrophysics (Berlin)</title><description>It has long been suspected that powerful radio sources may lower the efficiency with which stars form from the molecular gas in their host galaxy, however so far, alternative mechanisms, in particular related to the stellar mass distribution in the massive bulges of their host galaxies, have not been ruled out. We present new, arcsecond-resolution Atacama Large Millimeter Array (ALMA) CO(1−0) interferometry, which probes the spatially resolved, cold molecular gas in the nearby (
z
= 0.08), massive (
M
stellar
= 4 × 10
11
M
⊙
), isolated, late-type spiral galaxy 2MASSX J23453269−044925, which is outstanding for having two pairs of powerful, giant radio jets, and a bright X-ray halo of hot circumgalactic gas. The molecular gas is in a massive (
M
gas
= 2.0 × 10
10
M
⊙
), 24 kpc wide, rapidly rotating ring, which is associated with the inner stellar disk. Broad (
FWHM
= 70−180 km s
−1
) emission lines with complex profiles associated with the radio source are seen over large regions in the ring, indicating gas velocities that are high enough to keep the otherwise marginally Toomre-stable gas from fragmenting into gravitationally bound, star-forming clouds. About 1−2% of the jet kinetic energy is required to power these motions. Resolved star-formation rate surface densities derived from Galaxy Evolution Explorer and Wide-Field Infrared Survey Explorer fall by factors of 30−70 short of expectations from the standard Kennicutt–Schmidt law of star-forming galaxies, and near gas-rich early-type galaxies with signatures of star formation that are lowered by jet feedback. We argue that radio Active Galactic Nucleus (AGN) feedback is the only plausible mechanism to explain the low star-formation rates in this galaxy. Previous authors have already noted that the X-ray halo of J2345−0449 implies a baryon fraction that is close to the cosmic average, which is very high for a galaxy. We contrast this finding with other, equally massive, and equally baryon-rich spiral galaxies without prominent radio sources. Most of the baryons in these galaxies are in stars, not in the halos. We also discuss the implications of our results for our general understanding of AGN feedback in massive galaxies.</description><subject>Active galactic nuclei</subject><subject>Astrophysics</subject><subject>Baryons</subject><subject>Feedback</subject><subject>Galactic bulge</subject><subject>Galactic evolution</subject><subject>Galactic halos</subject><subject>Galaxy distribution</subject><subject>Infrared astronomy</subject><subject>Kinetic energy</subject><subject>Legal issues</subject><subject>Mass distribution</subject><subject>Molecular gases</subject><subject>Physics</subject><subject>Radio astronomy</subject><subject>Radio jets (astronomy)</subject><subject>Radio sources (astronomy)</subject><subject>Radio telescopes</subject><subject>Space telescopes</subject><subject>Spiral galaxies</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars & galaxies</subject><subject>Stellar evolution</subject><subject>Stellar mass</subject><subject>X-ray astronomy</subject><issn>0004-6361</issn><issn>1432-0746</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNo9kUFLAzEQhYMoWKu_wEvAk4fVySab7R6LaKsUvSh4C7Np0ka3m5psq737w81S6WmY4eO94T1CLhncMCjYLQCITHLJbnPImYBCiCMyYILnGZRCHpPBgTglZzF-pDVnIz4gv0-my-bBbU1Lx5Nnao2Z16g_qW_pyjdGbxoMdIGRYjunjf-mscOQWR9W2LkEGWuddqbVO-painSFMSa1hGpsaFy7kMYCG_zZ0W_XLRNSB7dYdvQ9C7ijS2z8OTmx2ERz8T-H5O3h_vVums1eJo9341mmeSG7rAK0NTcFR1bVULJyZDXHcsS0RYkVMNR2VJUcBcMaaolC5kJDnQujC80sH5LrvW4yVevgVhh2yqNT0_FM9TfgXOay4FuW2Ks9uw7-a2Nipz78JrTpPZUXyQugKnii-J7SwccYjD3IMlB9NaoPXvXBq0M1_A98k4C2</recordid><startdate>202110</startdate><enddate>202110</enddate><creator>Nesvadba, N. P. H.</creator><creator>Wagner, A. Y.</creator><creator>Mukherjee, D.</creator><creator>Mandal, A.</creator><creator>Janssen, R. M. J.</creator><creator>Zovaro, H.</creator><creator>Neumayer, N.</creator><creator>Bagchi, J.</creator><creator>Bicknell, G.</creator><general>EDP Sciences</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0001-5783-6544</orcidid><orcidid>https://orcid.org/0000-0002-1852-2507</orcidid></search><sort><creationdate>202110</creationdate><title>Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo</title><author>Nesvadba, N. P. H. ; Wagner, A. Y. ; Mukherjee, D. ; Mandal, A. ; Janssen, R. M. J. ; Zovaro, H. ; Neumayer, N. ; Bagchi, J. ; Bicknell, G.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c356t-90afb3e53a19b07178fc3a781cfa6a901acf8973a41ab0b6a4624c0b24ec5c1f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Active galactic nuclei</topic><topic>Astrophysics</topic><topic>Baryons</topic><topic>Feedback</topic><topic>Galactic bulge</topic><topic>Galactic evolution</topic><topic>Galactic halos</topic><topic>Galaxy distribution</topic><topic>Infrared astronomy</topic><topic>Kinetic energy</topic><topic>Legal issues</topic><topic>Mass distribution</topic><topic>Molecular gases</topic><topic>Physics</topic><topic>Radio astronomy</topic><topic>Radio jets (astronomy)</topic><topic>Radio sources (astronomy)</topic><topic>Radio telescopes</topic><topic>Space telescopes</topic><topic>Spiral galaxies</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars & galaxies</topic><topic>Stellar evolution</topic><topic>Stellar mass</topic><topic>X-ray astronomy</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Nesvadba, N. P. H.</creatorcontrib><creatorcontrib>Wagner, A. Y.</creatorcontrib><creatorcontrib>Mukherjee, D.</creatorcontrib><creatorcontrib>Mandal, A.</creatorcontrib><creatorcontrib>Janssen, R. M. J.</creatorcontrib><creatorcontrib>Zovaro, H.</creatorcontrib><creatorcontrib>Neumayer, N.</creatorcontrib><creatorcontrib>Bagchi, J.</creatorcontrib><creatorcontrib>Bicknell, G.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Nesvadba, N. P. H.</au><au>Wagner, A. Y.</au><au>Mukherjee, D.</au><au>Mandal, A.</au><au>Janssen, R. M. J.</au><au>Zovaro, H.</au><au>Neumayer, N.</au><au>Bagchi, J.</au><au>Bicknell, G.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2021-10</date><risdate>2021</risdate><volume>654</volume><spage>A8</spage><pages>A8-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><eissn>1432-0756</eissn><abstract>It has long been suspected that powerful radio sources may lower the efficiency with which stars form from the molecular gas in their host galaxy, however so far, alternative mechanisms, in particular related to the stellar mass distribution in the massive bulges of their host galaxies, have not been ruled out. We present new, arcsecond-resolution Atacama Large Millimeter Array (ALMA) CO(1−0) interferometry, which probes the spatially resolved, cold molecular gas in the nearby (
z
= 0.08), massive (
M
stellar
= 4 × 10
11
M
⊙
), isolated, late-type spiral galaxy 2MASSX J23453269−044925, which is outstanding for having two pairs of powerful, giant radio jets, and a bright X-ray halo of hot circumgalactic gas. The molecular gas is in a massive (
M
gas
= 2.0 × 10
10
M
⊙
), 24 kpc wide, rapidly rotating ring, which is associated with the inner stellar disk. Broad (
FWHM
= 70−180 km s
−1
) emission lines with complex profiles associated with the radio source are seen over large regions in the ring, indicating gas velocities that are high enough to keep the otherwise marginally Toomre-stable gas from fragmenting into gravitationally bound, star-forming clouds. About 1−2% of the jet kinetic energy is required to power these motions. Resolved star-formation rate surface densities derived from Galaxy Evolution Explorer and Wide-Field Infrared Survey Explorer fall by factors of 30−70 short of expectations from the standard Kennicutt–Schmidt law of star-forming galaxies, and near gas-rich early-type galaxies with signatures of star formation that are lowered by jet feedback. We argue that radio Active Galactic Nucleus (AGN) feedback is the only plausible mechanism to explain the low star-formation rates in this galaxy. Previous authors have already noted that the X-ray halo of J2345−0449 implies a baryon fraction that is close to the cosmic average, which is very high for a galaxy. We contrast this finding with other, equally massive, and equally baryon-rich spiral galaxies without prominent radio sources. Most of the baryons in these galaxies are in stars, not in the halos. We also discuss the implications of our results for our general understanding of AGN feedback in massive galaxies.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202140544</doi><orcidid>https://orcid.org/0000-0001-5783-6544</orcidid><orcidid>https://orcid.org/0000-0002-1852-2507</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | Astronomy and astrophysics (Berlin), 2021-10, Vol.654, p.A8 |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; EDP Sciences |
| subjects | Active galactic nuclei Astrophysics Baryons Feedback Galactic bulge Galactic evolution Galactic halos Galaxy distribution Infrared astronomy Kinetic energy Legal issues Mass distribution Molecular gases Physics Radio astronomy Radio jets (astronomy) Radio sources (astronomy) Radio telescopes Space telescopes Spiral galaxies Star & galaxy formation Star formation Stars & galaxies Stellar evolution Stellar mass X-ray astronomy |
| title | Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo |
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