Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

G. Speranza; C. Ramos Almeida; J. A. Acosta-Pulido; R. A. Riffel; C. Tadhunter; J. C.S. Pierce; A. Rodríguez-Ardila; M. Coloma Puga; M. Brusa; B. Musiimenta; D. M. Alexander; A. Lapi; F. Shankar; C. Villforth

doi:10.1051/0004-6361/202243585

Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

G. Speranza, C. Ramos Almeida, J. A. Acosta-Pulido, R. A. Riffel, C. Tadhunter, J. C.S. Pierce, A. Rodríguez-Ardila, M. Coloma Puga, M. Brusa, B. Musiimenta, D. M. Alexander, A. Lapi, F. Shankar, C. Villforth

Research output: Contribution to journal › Article › peer-review

21 Citations (SciVal)

Abstract

We analyse Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 1045.7 erg s-1 and a redshift of z=0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 μm where low ionization (Paα and BRΔ), high ionization ([S XI]λ1.920 μm and [Si VI]λ1.963 μm), and warm molecular lines (from H21-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low and high ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.33; (686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM) = 350-400 km s-1, while Paα, BRΔ, and [Si VI] are best fitted with two blue-shifted Gaussian components of FWHM 800 and 1700 km s-1, in addition to a narrow component of ã300 km s-1. We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to -840 km s-1, in the south-east direction (PA ã 125), extending up to a distance of ã3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of á1; ? out,max = 42-51 Myr-1, and its kinetic power represents 0.1% of the quasar bolometric luminosity. Very Large Array (VLA) data of J0945 show extended radio emission (PA ã 100) that is aligned with the clumpy emission traced by the narrow component of the ionized lines up to scales of several kiloparsecs, and with the innermost part of the outflow (central ã0.43; = 915 pc). Beyond that radius, at the edge of the radio jet, the high velocity gas shows a different PA of ã125. This might be an indication that the line-emitting gas is being compressed and accelerated by the shocks generated by the radio jet.

Original language	English
Article number	A55
Journal	Astronomy and Astrophysics
Volume	665
DOIs	https://doi.org/10.1051/0004-6361/202243585
Publication status	Published - 1 Sept 2022

Bibliographical note

Funding Information:
Based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This action has received funding from the European Union’s Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement No 860744 (BID4BEST). G.S. and C.R.A. acknowledge the project “Feeding and feedback in active galaxies”, with reference PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033. C.R.A. also acknowledges support from the projects “Quantifying the impact of quasar feedback on galaxy evolution”, with reference 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 “Quasar feedback and molecular gas reservoirs”, with reference ProID2020010105, ACCISI/FEDER, UE. R.A.R. acknowledges the support from Conselho Nacional de Desenvolvimento Científico e Tecnológico and Fundação de Amparo à pesquisa do Estado do Rio Grande do Sul. G.S. and C.R.A. thank Santiago García Burillo for useful advice on determining the near and far side of the galaxy and Anelise Audibert for alternative calculations of the SFR. J.P. acknowledges support from the Science and Technology Facilities Council (STFC) via grant ST/V000624/1.

Funding

Based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This action has received funding from the European Union’s Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement No 860744 (BID4BEST). G.S. and C.R.A. acknowledge the project “Feeding and feedback in active galaxies”, with reference PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033. C.R.A. also acknowledges support from the projects “Quantifying the impact of quasar feedback on galaxy evolution”, with reference 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 “Quasar feedback and molecular gas reservoirs”, with reference ProID2020010105, ACCISI/FEDER, UE. R.A.R. acknowledges the support from Conselho Nacional de Desenvolvimento Científico e Tecnológico and Fundação de Amparo à pesquisa do Estado do Rio Grande do Sul. G.S. and C.R.A. thank Santiago García Burillo for useful advice on determining the near and far side of the galaxy and Anelise Audibert for alternative calculations of the SFR. J.P. acknowledges support from the Science and Technology Facilities Council (STFC) via grant ST/V000624/1. Based on observations obtained at the international Gemini Observatory, a program of NSF s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigaci n y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog a e Innovaci n (Argentina), Minist rio da Ci ncia, Tecnologia, Inova es e Comunica es (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This action has received funding from the European Union s Horizon 2020 research and innovation programme under Marie Sk?odowska-Curie grant agreement No 860744 (BID4BEST). G.S. and C.R.A. acknowledge the project "Feeding and feedback in active galaxies", with reference PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033. C.R.A. also acknowledges support from the projects "Quantifying the impact of quasar feedback on galaxy evolution", with reference EUR2020-112266, funded by MICINN-AEI/10.13039/501100011033 and the European Union NextGenerationEU/PRTR, and from the Consejer a de Econom a, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant "Quasar feedback and molecular gas reservoirs", with reference ProID2020010105, ACCISI/FEDER, UE. R.A.R. acknowledges the support from Conselho Nacional de Desenvolvimento Cient fico e Tecnol gico and Funda o de Amparo pesquisa do Estado do Rio Grande do Sul. G.S. and C.R.A. thank Santiago Garc a Burillo for useful advice on determining the near and far side of the galaxy and Anelise Audibert for alternative calculations of the SFR. J.P. acknowledges support from the Science and Technology Facilities Council (STFC) via grant ST/V000624/1.

Keywords

Galaxies: kinematics and dynamics
Galaxies: nuclei
Galaxy: evolution
Quasars: emission lines
Quasars: supermassive black holes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1051/0004-6361/202243585Licence: CC BY

Cite this

Speranza, G., Ramos Almeida, C., Acosta-Pulido, J. A., Riffel, R. A., Tadhunter, C., Pierce, J. C. S., Rodríguez-Ardila, A., Coloma Puga, M., Brusa, M., Musiimenta, B., Alexander, D. M., Lapi, A., Shankar, F., & Villforth, C. (2022). Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737. Astronomy and Astrophysics, 665, Article A55. https://doi.org/10.1051/0004-6361/202243585

Speranza, G, Ramos Almeida, C, Acosta-Pulido, JA, Riffel, RA, Tadhunter, C, Pierce, JCS, Rodríguez-Ardila, A, Coloma Puga, M, Brusa, M, Musiimenta, B, Alexander, DM, Lapi, A, Shankar, F & Villforth, C 2022, 'Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737', Astronomy and Astrophysics, vol. 665, A55. https://doi.org/10.1051/0004-6361/202243585

@article{42babdf07060475da99e4871ce2d1307,

title = "Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737",

abstract = "We analyse Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 1045.7 erg s-1 and a redshift of z=0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 μm where low ionization (Paα and BRΔ), high ionization ([S XI]λ1.920 μm and [Si VI]λ1.963 μm), and warm molecular lines (from H21-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low and high ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.33; (686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM) = 350-400 km s-1, while Paα, BRΔ, and [Si VI] are best fitted with two blue-shifted Gaussian components of FWHM 800 and 1700 km s-1, in addition to a narrow component of {\~a}300 km s-1. We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to -840 km s-1, in the south-east direction (PA {\~a} 125), extending up to a distance of {\~a}3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of {\'a}1; ? out,max = 42-51 Myr-1, and its kinetic power represents 0.1% of the quasar bolometric luminosity. Very Large Array (VLA) data of J0945 show extended radio emission (PA {\~a} 100) that is aligned with the clumpy emission traced by the narrow component of the ionized lines up to scales of several kiloparsecs, and with the innermost part of the outflow (central {\~a}0.43; = 915 pc). Beyond that radius, at the edge of the radio jet, the high velocity gas shows a different PA of {\~a}125. This might be an indication that the line-emitting gas is being compressed and accelerated by the shocks generated by the radio jet.",

keywords = "Galaxies: kinematics and dynamics, Galaxies: nuclei, Galaxy: evolution, Quasars: emission lines, Quasars: supermassive black holes",

author = "G. Speranza and {Ramos Almeida}, C. and Acosta-Pulido, {J. A.} and Riffel, {R. A.} and C. Tadhunter and Pierce, {J. C.S.} and A. Rodr{\'i}guez-Ardila and {Coloma Puga}, M. and M. Brusa and B. Musiimenta and Alexander, {D. M.} and A. Lapi and F. Shankar and C. Villforth",

note = "Funding Information: Based on observations obtained at the international Gemini Observatory, a program of NSF{\textquoteright}s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigaci{\'o}n y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog{\'i}a e Innovaci{\'o}n (Argentina), Minist{\'e}rio da Ci{\^e}ncia, Tecnologia, Inova{\c c}{\~o}es e Comunica{\c c}{\~o}es (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This action has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation programme under Marie Sk{\l}odowska-Curie grant agreement No 860744 (BID4BEST). G.S. and C.R.A. acknowledge the project “Feeding and feedback in active galaxies”, with reference PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033. C.R.A. also acknowledges support from the projects “Quantifying the impact of quasar feedback on galaxy evolution”, with reference EUR2020-112266, funded by MICINN-AEI/10.13039/501100011033 and the European Union NextGenerationEU/PRTR, and from the Consejer{\'i}a de Econom{\'i}a, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant “Quasar feedback and molecular gas reservoirs”, with reference ProID2020010105, ACCISI/FEDER, UE. R.A.R. acknowledges the support from Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gico and Funda{\c c}{\~a}o de Amparo {\`a} pesquisa do Estado do Rio Grande do Sul. G.S. and C.R.A. thank Santiago Garc{\'i}a Burillo for useful advice on determining the near and far side of the galaxy and Anelise Audibert for alternative calculations of the SFR. J.P. acknowledges support from the Science and Technology Facilities Council (STFC) via grant ST/V000624/1. ",

year = "2022",

month = sep,

day = "1",

doi = "10.1051/0004-6361/202243585",

language = "English",

volume = "665",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

AU - Speranza, G.

AU - Ramos Almeida, C.

AU - Acosta-Pulido, J. A.

AU - Riffel, R. A.

AU - Tadhunter, C.

AU - Pierce, J. C.S.

AU - Rodríguez-Ardila, A.

AU - Coloma Puga, M.

AU - Brusa, M.

AU - Musiimenta, B.

AU - Alexander, D. M.

AU - Lapi, A.

AU - Shankar, F.

AU - Villforth, C.

N1 - Funding Information: Based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This action has received funding from the European Union’s Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement No 860744 (BID4BEST). G.S. and C.R.A. acknowledge the project “Feeding and feedback in active galaxies”, with reference PID2019-106027GB-C42, funded by MICINN-AEI/10.13039/501100011033. C.R.A. also acknowledges support from the projects “Quantifying the impact of quasar feedback on galaxy evolution”, with reference 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 “Quasar feedback and molecular gas reservoirs”, with reference ProID2020010105, ACCISI/FEDER, UE. R.A.R. acknowledges the support from Conselho Nacional de Desenvolvimento Científico e Tecnológico and Fundação de Amparo à pesquisa do Estado do Rio Grande do Sul. G.S. and C.R.A. thank Santiago García Burillo for useful advice on determining the near and far side of the galaxy and Anelise Audibert for alternative calculations of the SFR. J.P. acknowledges support from the Science and Technology Facilities Council (STFC) via grant ST/V000624/1.

PY - 2022/9/1

Y1 - 2022/9/1

N2 - We analyse Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 1045.7 erg s-1 and a redshift of z=0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 μm where low ionization (Paα and BRΔ), high ionization ([S XI]λ1.920 μm and [Si VI]λ1.963 μm), and warm molecular lines (from H21-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low and high ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.33; (686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM) = 350-400 km s-1, while Paα, BRΔ, and [Si VI] are best fitted with two blue-shifted Gaussian components of FWHM 800 and 1700 km s-1, in addition to a narrow component of ã300 km s-1. We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to -840 km s-1, in the south-east direction (PA ã 125), extending up to a distance of ã3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of á1; ? out,max = 42-51 Myr-1, and its kinetic power represents 0.1% of the quasar bolometric luminosity. Very Large Array (VLA) data of J0945 show extended radio emission (PA ã 100) that is aligned with the clumpy emission traced by the narrow component of the ionized lines up to scales of several kiloparsecs, and with the innermost part of the outflow (central ã0.43; = 915 pc). Beyond that radius, at the edge of the radio jet, the high velocity gas shows a different PA of ã125. This might be an indication that the line-emitting gas is being compressed and accelerated by the shocks generated by the radio jet.

AB - We analyse Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 1045.7 erg s-1 and a redshift of z=0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 μm where low ionization (Paα and BRΔ), high ionization ([S XI]λ1.920 μm and [Si VI]λ1.963 μm), and warm molecular lines (from H21-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low and high ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.33; (686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM) = 350-400 km s-1, while Paα, BRΔ, and [Si VI] are best fitted with two blue-shifted Gaussian components of FWHM 800 and 1700 km s-1, in addition to a narrow component of ã300 km s-1. We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to -840 km s-1, in the south-east direction (PA ã 125), extending up to a distance of ã3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of á1; ? out,max = 42-51 Myr-1, and its kinetic power represents 0.1% of the quasar bolometric luminosity. Very Large Array (VLA) data of J0945 show extended radio emission (PA ã 100) that is aligned with the clumpy emission traced by the narrow component of the ionized lines up to scales of several kiloparsecs, and with the innermost part of the outflow (central ã0.43; = 915 pc). Beyond that radius, at the edge of the radio jet, the high velocity gas shows a different PA of ã125. This might be an indication that the line-emitting gas is being compressed and accelerated by the shocks generated by the radio jet.

KW - Galaxies: kinematics and dynamics

KW - Galaxies: nuclei

KW - Galaxy: evolution

KW - Quasars: emission lines

KW - Quasars: supermassive black holes

UR - http://www.scopus.com/inward/record.url?scp=85140138025&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202243585

DO - 10.1051/0004-6361/202243585

M3 - Article

AN - SCOPUS:85140138025

SN - 0004-6361

VL - 665

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A55

ER -

Warm molecular and ionized gas kinematics in the type-2 quasar J0945+1737

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