Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics

R. Slater, C. Finlez, N. M Nagar, A. Schnorr-Muller, T. Storchi-Bergmann, V. Ramakrishnan, Carole Mundell, R. A. Riffel, B. Peterson, A. Robinson, G. Orellana

Research output: Contribution to journalArticle

Abstract

We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies, to quantify the nuclear inflows and outflows. Here, we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and ∼2.6 km s−1 spectral resolution, and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution, and 123 km s−1 of intrinsic spectral resolution. The morphology and kinematics of stellar, molecular (CO) and ionized ([N II]) emission lines are compared to the expectations from rotation, outflows, and streaming inflows. While both ionized and molecular gas show rotation signatures, there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc (CO). The nucleus shows a double-peaked CO profile (Full Width at Zero Intensity of 200 km s−1), and prominent (∼80 km s−1) blue and redshifted lobes are found along the minor axis in the inner arcseconds. Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field. We thus favour the presence of a molecular outflow in the disk with true velocities of ∼180 km s−1 in the nucleus and decelerating to 0 by ∼72 pc. The implied molecular outflow rate is 5.6 [Moyr−1], with this gas accumulating in the nuclear 2 arcsec arms. The ionized gas kinematics support an interpretation of a similar, but more spherical, outflow in the inner 100 pc, with no signs of deceleration. There is some evidence of streaming inflows of ∼50 km s−1 along specific spiral arms, and the estimated molecular mass inflow rate, ∼0.1 [Moyr−1], is significantly larger than the SMBH accretion rate (m˙=4.8×10−5 [Moyr−1]).
Original languageEnglish
Number of pages23
JournalAstronomy & Astrophysics
Publication statusAccepted/In press - 29 Mar 2018

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ionized gases
molecular gases
outflow
kinematics
inflow
gas
spectral resolution
active galaxies
nuclei
deceleration
lobes
velocity distribution
spatial resolution
signatures
perturbation
accretion
profiles
gases
rate

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Slater, R., Finlez, C., Nagar, N. M., Schnorr-Muller, A., Storchi-Bergmann, T., Ramakrishnan, V., ... Orellana, G. (Accepted/In press). Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics. Astronomy & Astrophysics.

Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics. / Slater, R.; Finlez, C.; Nagar, N. M; Schnorr-Muller, A.; Storchi-Bergmann, T.; Ramakrishnan, V.; Mundell, Carole; Riffel, R. A.; Peterson, B.; Robinson, A.; Orellana, G.

In: Astronomy & Astrophysics, 29.03.2018.

Research output: Contribution to journalArticle

Slater, R, Finlez, C, Nagar, NM, Schnorr-Muller, A, Storchi-Bergmann, T, Ramakrishnan, V, Mundell, C, Riffel, RA, Peterson, B, Robinson, A & Orellana, G 2018, 'Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics', Astronomy & Astrophysics.
Slater R, Finlez C, Nagar NM, Schnorr-Muller A, Storchi-Bergmann T, Ramakrishnan V et al. Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics. Astronomy & Astrophysics. 2018 Mar 29.
Slater, R. ; Finlez, C. ; Nagar, N. M ; Schnorr-Muller, A. ; Storchi-Bergmann, T. ; Ramakrishnan, V. ; Mundell, Carole ; Riffel, R. A. ; Peterson, B. ; Robinson, A. ; Orellana, G. / Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics. In: Astronomy & Astrophysics. 2018.
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title = "Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics",
abstract = "We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies, to quantify the nuclear inflows and outflows. Here, we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and ∼2.6 km s−1 spectral resolution, and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution, and 123 km s−1 of intrinsic spectral resolution. The morphology and kinematics of stellar, molecular (CO) and ionized ([N II]) emission lines are compared to the expectations from rotation, outflows, and streaming inflows. While both ionized and molecular gas show rotation signatures, there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc (CO). The nucleus shows a double-peaked CO profile (Full Width at Zero Intensity of 200 km s−1), and prominent (∼80 km s−1) blue and redshifted lobes are found along the minor axis in the inner arcseconds. Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field. We thus favour the presence of a molecular outflow in the disk with true velocities of ∼180 km s−1 in the nucleus and decelerating to 0 by ∼72 pc. The implied molecular outflow rate is 5.6 [Moyr−1], with this gas accumulating in the nuclear 2 arcsec arms. The ionized gas kinematics support an interpretation of a similar, but more spherical, outflow in the inner 100 pc, with no signs of deceleration. There is some evidence of streaming inflows of ∼50 km s−1 along specific spiral arms, and the estimated molecular mass inflow rate, ∼0.1 [Moyr−1], is significantly larger than the SMBH accretion rate (m˙=4.8×10−5 [Moyr−1]).",
author = "R. Slater and C. Finlez and Nagar, {N. M} and A. Schnorr-Muller and T. Storchi-Bergmann and V. Ramakrishnan and Carole Mundell and Riffel, {R. A.} and B. Peterson and A. Robinson and G. Orellana",
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T1 - Outflows in the inner kilosparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFS) kinematics

AU - Slater, R.

AU - Finlez, C.

AU - Nagar, N. M

AU - Schnorr-Muller, A.

AU - Storchi-Bergmann, T.

AU - Ramakrishnan, V.

AU - Mundell, Carole

AU - Riffel, R. A.

AU - Peterson, B.

AU - Robinson, A.

AU - Orellana, G.

PY - 2018/3/29

Y1 - 2018/3/29

N2 - We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies, to quantify the nuclear inflows and outflows. Here, we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and ∼2.6 km s−1 spectral resolution, and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution, and 123 km s−1 of intrinsic spectral resolution. The morphology and kinematics of stellar, molecular (CO) and ionized ([N II]) emission lines are compared to the expectations from rotation, outflows, and streaming inflows. While both ionized and molecular gas show rotation signatures, there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc (CO). The nucleus shows a double-peaked CO profile (Full Width at Zero Intensity of 200 km s−1), and prominent (∼80 km s−1) blue and redshifted lobes are found along the minor axis in the inner arcseconds. Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field. We thus favour the presence of a molecular outflow in the disk with true velocities of ∼180 km s−1 in the nucleus and decelerating to 0 by ∼72 pc. The implied molecular outflow rate is 5.6 [Moyr−1], with this gas accumulating in the nuclear 2 arcsec arms. The ionized gas kinematics support an interpretation of a similar, but more spherical, outflow in the inner 100 pc, with no signs of deceleration. There is some evidence of streaming inflows of ∼50 km s−1 along specific spiral arms, and the estimated molecular mass inflow rate, ∼0.1 [Moyr−1], is significantly larger than the SMBH accretion rate (m˙=4.8×10−5 [Moyr−1]).

AB - We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies, to quantify the nuclear inflows and outflows. Here, we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and ∼2.6 km s−1 spectral resolution, and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution, and 123 km s−1 of intrinsic spectral resolution. The morphology and kinematics of stellar, molecular (CO) and ionized ([N II]) emission lines are compared to the expectations from rotation, outflows, and streaming inflows. While both ionized and molecular gas show rotation signatures, there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc (CO). The nucleus shows a double-peaked CO profile (Full Width at Zero Intensity of 200 km s−1), and prominent (∼80 km s−1) blue and redshifted lobes are found along the minor axis in the inner arcseconds. Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field. We thus favour the presence of a molecular outflow in the disk with true velocities of ∼180 km s−1 in the nucleus and decelerating to 0 by ∼72 pc. The implied molecular outflow rate is 5.6 [Moyr−1], with this gas accumulating in the nuclear 2 arcsec arms. The ionized gas kinematics support an interpretation of a similar, but more spherical, outflow in the inner 100 pc, with no signs of deceleration. There is some evidence of streaming inflows of ∼50 km s−1 along specific spiral arms, and the estimated molecular mass inflow rate, ∼0.1 [Moyr−1], is significantly larger than the SMBH accretion rate (m˙=4.8×10−5 [Moyr−1]).

M3 - Article

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

ER -