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A CO molecular gas wind 340 pc away from the Seyfert 2 nucleus in ESO 420-G13 probes an elusive radio jet

Identificadores del recurso

Astronomy and Astrophysics 633: A127(2020)

0004-6361

https://www.aanda.org/articles/aa/full_html/2020/01/aa36552-19/aa36552-19.html

http://hdl.handle.net/20.500.12666/265

10.1051/0004-6361/201936552

1432-0746

http://dx.doi.org/10.13039/501100003981

http://dx.doi.org/10.13039/100012818

http://dx.doi.org/10.13039/501100013209

Procedencia

(DIGITAL.INTA)

Ficha

Título:: A CO molecular gas wind 340 pc away from the Seyfert 2 nucleus in ESO 420-G13 probes an elusive radio jet
Tema:: ISM: jets and outflows; Galaxies: active; Galaxies: individual; ESO 420-G13; Submillimeter: ISM; Galaxies: evolution; Techniques: high angular resolution
Descripción:: A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of 340-600 pc from the nucleus. The wind morphology resembles the characteristic funnel shape, formed by a highly collimated filamentary emission at the base, and likely traces the jet propagation through a tenuous medium, until a bifurcation point at 440 pc. Here the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner less than or similar to 340 pc using the [NeII](12.8 mu m) line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of similar to 8 x 10(6) M-circle dot at an average wind projected speed of similar to 160 km s(-1), which implies a mass outflow rate of similar to 14 M-circle dot yr(-1). Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where a previously unknown jet is revealed through its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain an outflow at this distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy.; The authors acknowledge the referee for his/her useful comments that helped to improve the manuscript. JAFO acknowledges financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. JAFO and KMD acknowledge financial support by the Hellenic Foundation for Research and Innovation (HFRI), under the first call for the creation of research groups by postdoctoral researchers that was launched by the General Secretariat For Research and Technology (project number 1882). MPS acknowledges support from the Comunidad de Madrid, Spain, through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and STFC through grants ST/N000919/1 and ST/N002717/1. CR acknowledges support from the CONI-CYT +PAI, Convocatoria Nacional subvencion a instalacion en la academia, convocatoria ano 2017 PAI77170080. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00236.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).; Peer review
Idioma:: English
Autor/Productor:: Fernández Ontiveros, J. A.; Dasyra, K. M.; Hatziminaoglou, Evanthia; Malkan, M. A.; Pereira Santaella, M.; Papachristou, M.; Spinoglio, L.; Combes, F.; Aalto, S.; Nagar, N.; Imanishi, M.; Andreani, P.; Ricci, C.; Slater, R.
Editor:: EDP Sciences
Otros colaboradores/productores:: Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Fernández Ontiveros, J. A. [0000-0001-9490-899X]; Hatziminaoglou, E. [0000-0003-0917-9636]; Spignoglio, L. [0000-0001-8840-1551]; Combes, F. [0000-0003-2658-7893]; Nagar, N. [0000-0001-6920-662X]; Imanishi, M. [0000-0001-6186-8792]; Andreani, P. [0000-0001-9493-0169]; Agenzia Spaziale Italiana (ASI); Comunidad de Madrid; Hellenic Foundation for Research and Innovation (HFRI); Comisión Nacional de Investigación Científica y Tecnológica (CONICYT); http://dx.doi.org/10.13039/501100002848
Derechos:: Attribution-NonCommercial-NoDerivatives 4.0 International; © ESO 2020; https://creativecommons.org/licenses/by-nc-nd/4.0/; info:eu-repo/semantics/openAccess
Fecha:: 2021-04-12T11:01:08Z; 2020-01-21
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Formato:: application/pdf

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30. <dc:subject>Galaxies: active</dc:subject>
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45. <dim:field element="description" lang="es" mdschema="dc" qualifier="sponsorship">The authors acknowledge the referee for his/her useful comments that helped to improve the manuscript. JAFO acknowledges financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. JAFO and KMD acknowledge financial support by the Hellenic Foundation for Research and Innovation (HFRI), under the first call for the creation of research groups by postdoctoral researchers that was launched by the General Secretariat For Research and Technology (project number 1882). MPS acknowledges support from the Comunidad de Madrid, Spain, through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and STFC through grants ST/N000919/1 and ST/N002717/1. CR acknowledges support from the CONI-CYT +PAI, Convocatoria Nacional subvencion a instalacion en la academia, convocatoria ano 2017 PAI77170080. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00236.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).</dim:field>
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2. <creator>Fernández Ontiveros, J. A.</creator>
3. <creator>Dasyra, K. M.</creator>
4. <creator>Hatziminaoglou, Evanthia</creator>
5. <creator>Malkan, M. A.</creator>
6. <creator>Pereira Santaella, M.</creator>
7. <creator>Papachristou, M.</creator>
8. <creator>Spinoglio, L.</creator>
9. <creator>Combes, F.</creator>
10. <creator>Aalto, S.</creator>
11. <creator>Nagar, N.</creator>
12. <creator>Imanishi, M.</creator>
13. <creator>Andreani, P.</creator>
14. <creator>Ricci, C.</creator>
15. <creator>Slater, R.</creator>
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17. <contributor>Fernández Ontiveros, J. A. [0000-0001-9490-899X]</contributor>
18. <contributor>Hatziminaoglou, E. [0000-0003-0917-9636]</contributor>
19. <contributor>Spignoglio, L. [0000-0001-8840-1551]</contributor>
20. <contributor>Combes, F. [0000-0003-2658-7893]</contributor>
21. <contributor>Nagar, N. [0000-0001-6920-662X]</contributor>
22. <contributor>Imanishi, M. [0000-0001-6186-8792]</contributor>
23. <contributor>Andreani, P. [0000-0001-9493-0169]</contributor>
24. <contributor>Agenzia Spaziale Italiana (ASI)</contributor>
25. <contributor>Comunidad de Madrid</contributor>
26. <contributor>Hellenic Foundation for Research and Innovation (HFRI)</contributor>
27. <contributor>Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)</contributor>
28. <contributor>http://dx.doi.org/10.13039/501100002848</contributor>
29. <subject>ISM: jets and outflows</subject>
30. <subject>Galaxies: active</subject>
31. <subject>Galaxies: individual</subject>
32. <subject>ESO 420-G13</subject>
33. <subject>Submillimeter: ISM</subject>
34. <subject>Galaxies: evolution</subject>
35. <subject>Techniques: high angular resolution</subject>
36. <description>A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of 340-600 pc from the nucleus. The wind morphology resembles the characteristic funnel shape, formed by a highly collimated filamentary emission at the base, and likely traces the jet propagation through a tenuous medium, until a bifurcation point at 440 pc. Here the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner less than or similar to 340 pc using the [NeII](12.8 mu m) line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of similar to 8 x 10(6) M-circle dot at an average wind projected speed of similar to 160 km s(-1), which implies a mass outflow rate of similar to 14 M-circle dot yr(-1). Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where a previously unknown jet is revealed through its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain an outflow at this distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy.</description>
37. <date>2021-04-12</date>
38. <date>2021-04-12</date>
39. <date>2020-01-21</date>
40. <type>info:eu-repo/semantics/article</type>
41. <identifier>Astronomy and Astrophysics 633: A127(2020)</identifier>
42. <identifier>0004-6361</identifier>
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50. <language>eng</language>
51. <rights>© ESO 2020</rights>
52. <rights>https://creativecommons.org/licenses/by-nc-nd/4.0/</rights>
53. <rights>info:eu-repo/semantics/openAccess</rights>
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1. <dc:title>A CO molecular gas wind 340 pc away from the Seyfert 2 nucleus in ESO 420-G13 probes an elusive radio jet</dc:title>
2. <dc:creator>Fernández Ontiveros, J. A.</dc:creator>
3. <dc:creator>Dasyra, K. M.</dc:creator>
4. <dc:creator>Hatziminaoglou, Evanthia</dc:creator>
5. <dc:creator>Malkan, M. A.</dc:creator>
6. <dc:creator>Pereira Santaella, M.</dc:creator>
7. <dc:creator>Papachristou, M.</dc:creator>
8. <dc:creator>Spinoglio, L.</dc:creator>
9. <dc:creator>Combes, F.</dc:creator>
10. <dc:creator>Aalto, S.</dc:creator>
11. <dc:creator>Nagar, N.</dc:creator>
12. <dc:creator>Imanishi, M.</dc:creator>
13. <dc:creator>Andreani, P.</dc:creator>
14. <dc:creator>Ricci, C.</dc:creator>
15. <dc:creator>Slater, R.</dc:creator>
16. <dc:contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</dc:contributor>
17. <dc:contributor>Fernández Ontiveros, J. A. [0000-0001-9490-899X]</dc:contributor>
18. <dc:contributor>Hatziminaoglou, E. [0000-0003-0917-9636]</dc:contributor>
19. <dc:contributor>Spignoglio, L. [0000-0001-8840-1551]</dc:contributor>
20. <dc:contributor>Combes, F. [0000-0003-2658-7893]</dc:contributor>
21. <dc:contributor>Nagar, N. [0000-0001-6920-662X]</dc:contributor>
22. <dc:contributor>Imanishi, M. [0000-0001-6186-8792]</dc:contributor>
23. <dc:contributor>Andreani, P. [0000-0001-9493-0169]</dc:contributor>
24. <dc:contributor>Agenzia Spaziale Italiana (ASI)</dc:contributor>
25. <dc:contributor>Comunidad de Madrid</dc:contributor>
26. <dc:contributor>Hellenic Foundation for Research and Innovation (HFRI)</dc:contributor>
27. <dc:contributor>Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)</dc:contributor>
28. <dc:contributor>http://dx.doi.org/10.13039/501100002848</dc:contributor>
29. <dc:subject>ISM: jets and outflows</dc:subject>
30. <dc:subject>Galaxies: active</dc:subject>
31. <dc:subject>Galaxies: individual</dc:subject>
32. <dc:subject>ESO 420-G13</dc:subject>
33. <dc:subject>Submillimeter: ISM</dc:subject>
34. <dc:subject>Galaxies: evolution</dc:subject>
35. <dc:subject>Techniques: high angular resolution</dc:subject>
36. <dcterms:abstract>A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of 340-600 pc from the nucleus. The wind morphology resembles the characteristic funnel shape, formed by a highly collimated filamentary emission at the base, and likely traces the jet propagation through a tenuous medium, until a bifurcation point at 440 pc. Here the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner less than or similar to 340 pc using the [NeII](12.8 mu m) line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of similar to 8 x 10(6) M-circle dot at an average wind projected speed of similar to 160 km s(-1), which implies a mass outflow rate of similar to 14 M-circle dot yr(-1). Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where a previously unknown jet is revealed through its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain an outflow at this distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy.</dcterms:abstract>
37. <dcterms:dateAccepted>2021-04-12T11:01:08Z</dcterms:dateAccepted>
38. <dcterms:available>2021-04-12T11:01:08Z</dcterms:available>
39. <dcterms:created>2021-04-12T11:01:08Z</dcterms:created>
40. <dcterms:issued>2020-01-21</dcterms:issued>
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42. <dc:identifier>Astronomy and Astrophysics 633: A127(2020)</dc:identifier>
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51. <dc:language>eng</dc:language>
52. <dc:rights>© ESO 2020</dc:rights>
53. <dc:rights>https://creativecommons.org/licenses/by-nc-nd/4.0/</dc:rights>
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  4. <dc:creator>Hatziminaoglou, Evanthia</dc:creator>
  5. <dc:creator>Malkan, M. A.</dc:creator>
  6. <dc:creator>Pereira Santaella, M.</dc:creator>
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  11. <dc:creator>Nagar, N.</dc:creator>
  12. <dc:creator>Imanishi, M.</dc:creator>
  13. <dc:creator>Andreani, P.</dc:creator>
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  18. <dc:contributor>Hatziminaoglou, E. [0000-0003-0917-9636]</dc:contributor>
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  29. <dc:subject>ISM: jets and outflows</dc:subject>
  30. <dc:subject>Galaxies: active</dc:subject>
  31. <dc:subject>Galaxies: individual</dc:subject>
  32. <dc:subject>ESO 420-G13</dc:subject>
  33. <dc:subject>Submillimeter: ISM</dc:subject>
  34. <dc:subject>Galaxies: evolution</dc:subject>
  35. <dc:subject>Techniques: high angular resolution</dc:subject>
  36. <dc:description>A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of 340-600 pc from the nucleus. The wind morphology resembles the characteristic funnel shape, formed by a highly collimated filamentary emission at the base, and likely traces the jet propagation through a tenuous medium, until a bifurcation point at 440 pc. Here the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner less than or similar to 340 pc using the [NeII](12.8 mu m) line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of similar to 8 x 10(6) M-circle dot at an average wind projected speed of similar to 160 km s(-1), which implies a mass outflow rate of similar to 14 M-circle dot yr(-1). Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where a previously unknown jet is revealed through its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain an outflow at this distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy.</dc:description>
  37. <dc:date>2021-04-12T11:01:08Z</dc:date>
  38. <dc:date>2021-04-12T11:01:08Z</dc:date>
  39. <dc:date>2020-01-21</dc:date>
  40. <dc:type>info:eu-repo/semantics/article</dc:type>
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  50. <dc:language>eng</dc:language>
  51. <dc:rights>© ESO 2020</dc:rights>
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  53. <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
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