Conflit(s) et public(s) : orientations bibliographiques

Veilleux, Christian

doi:10.7202/1064529ar

Cited by 5 publications

(10 citation statements)

References 5 publications

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“…Then, we select those galaxies with an increase in the optical line ratios [N ii]/Hα, [O iii]/Hβ, [S ii]/Hα and [O i]/Hα along the semiminor axis and the disk vertical direction. These increments are characteristic of shocks produced by galactic outflows (Veilleux & Rupke 2002;Veilleux et al 2005), although they are not exclusive of these processes. Here increase means that the ionization is not compatible with the typical line-ratios observed in SF regions.…”

Section: Candidates Selectionmentioning

confidence: 97%

“…However, this morphological structure does not exist in all outflows. In many cases they present a variety of complex morphologies (e.g., Cecil et al 2001;Veilleux et al 2001;Martin et al 2002;Veilleux & Rupke 2002). Depending on the shock velocities, ionization by shocks can cover a wide range of line ratios making them rather difficult to identify in the classical diagnostic diagrams (e.g., Baldwin et al 1981;Veilleux & Osterbrock 1987), at difference with other ionizing sources which are confined to specific regions of these diagrams.…”

Section: Candidates Selectionmentioning

confidence: 99%

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Systematic study of outflows in the Local Universe using CALIFA: I. Sample selection and main properties

López-Cobá

Sánchez

Bland-Hawthorn

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a sample of 17 objects from the CALIFA survey where we find initial evidence of galactic winds based on their off-axis ionization properties. We identify the presence of outflows using various optical diagnostic diagrams (e.g., EW(Hα), [N ii]/Hα, [S ii]/Hα, [O i]/Hα line-ratio maps). We find that all 17 candidate outflow galaxies lie along the sequence of active star formation in the M vs. star-formation rate diagram, without a clear excess in the integrated SFR. The location of galaxies along the star-formation main sequence (SFMS) does not influence strongly the presence or not of outflows. The analysis of the star-formation rate density (Σ SFR ) reveals that the CALIFA sources present higher values when compared with normal star-forming galaxies. The strength of this relation depends on the calibrator used to estimate the SFR. This excess in Σ SFR is significant within the first effective radius supporting the idea that most outflows are driven by processes in the inner regions of a galaxy. We find that the molecular gas mass density (Σ gas ) is a key parameter that plays an important role in the generation of outflows through its association with the local SFR. The canonical threshold reported for the generation of outflows -Σ SFR > 0.1 M yr −1 kpc −2 -is only marginally exceeded in our sample. Within the Kennicutt-Schmidt diagram we propose a domain for galaxies hosting starburst-driven outflows defined by Σ SFR > 10 −2 M yr −1 kpc −2 and Σ gas > 10 1.2 M pc −2 within a central kiloparcec region.

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Section: Candidates Selectionmentioning

confidence: 97%

Section: Candidates Selectionmentioning

confidence: 99%

Systematic study of outflows in the Local Universe using CALIFA: I. Sample selection and main properties

López-Cobá

Sánchez

Bland-Hawthorn

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…However, a more likely explanation for the low shock fraction is that we are simply probing material close to the galaxy disks where the large scale stellar radiation field is strong. Low shock fractions are observed close to the disks of several prototypical starburst driven superwind galaxies including M82, NGC 1482 and NGC 253 (Shopbell & Bland-Hawthorn 1998;Veilleux & Rupke 2002;Westmoquette et al 2011).…”

Section: Ionization Mechanismsmentioning

confidence: 99%

Kiloparsec Scale Properties of Star Formation Driven Outflows at z ∼ 2.3 in the SINS/zC-SINF AO Survey*

Davies

Schreiber

Übler

et al. 2019

ApJ

100

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We investigate the relationship between star formation activity and outflow properties on kiloparsec scales in a sample of 28 star forming galaxies at z ∼ 2 -2.6, using adaptive optics assisted integral field observations from SINFONI on the VLT. The narrow and broad components of the Hα emission are used to simultaneously determine the local star formation rate surface density (Σ SFR ), and the outflow velocity v out and mass outflow rateṀ out , respectively. We find clear evidence for faster outflows with larger mass loading factors at higher Σ SFR . The outflow velocities scale as v out ∝ Σ SFR 0.34±0.10 , which suggests that the outflows may be driven by a combination of mechanical energy released by supernova explosions and stellar winds, as well as radiation pressure acting on dust grains. The majority of the outflowing material does not have sufficient velocity to escape from the galaxy halos, but will likely be re-accreted and contribute to the chemical enrichment of the galaxies. In the highest Σ SFR regions the outflow component contains an average of ∼45% of the Hα flux, while in the lower Σ SFR regions only ∼10% of the Hα flux is associated with outflows. The mass loading factor, η =Ṁ out /SFR, is positively correlated with Σ SFR but is relatively low even at the highest Σ SFR : η 0.5 × (380 cm −3 /n e ). This may be in tension with the η 1 required by cosmological simulations, unless a significant fraction of the outflowing mass is in other gas phases and has sufficient velocity to escape the galaxy halos.

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“…1) is not aligned with our posited outflow axis. Further, apart from the Seyfert 1 clas- sification there are no data (e.g., maser disks) to constrain the orientation of the central engine; (b) outflows are also often seen perpendicular to the plane of the disk, especially in the case of starburst driven winds (eg., Veilleux & Rupke 2002;Veilleux et al 2005;Leroy et al 2015). However, for such a polar outflow the blueshifted (redshifted) emission would be seen towards the far (near) side of the galaxy disk, the opposite of that seen in NGC 1566; (c) a large (e.g.…”

Section: Modeling Observed Velocities: Molecular Outflows?mentioning

confidence: 99%

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

Slater

Nagar

Schnorr-Müller

et al. 2019

A&A

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Context. Tracing nuclear inflows and outflows in AGNs, determining the mass of gas involved in these, and their impact on the host galaxy and nuclear black hole, requires 3-D imaging studies of both the ionized and molecular gas. Aims. 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. Methods. 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. Results. 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 [M yr −1 ], with this gas accumulating in the nuclear 2 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 [M yr −1 ], is significantly larger than the SMBH accretion rate (ṁ = 4.8 × 10 −5 [M yr −1 ]).

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Conflit(s) et public(s) : orientations bibliographiques

Cited by 5 publications

References 5 publications

Systematic study of outflows in the Local Universe using CALIFA: I. Sample selection and main properties

Systematic study of outflows in the Local Universe using CALIFA: I. Sample selection and main properties

Kiloparsec Scale Properties of Star Formation Driven Outflows at z ∼ 2.3 in the SINS/zC-SINF AO Survey*

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

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