The ALMaQUEST Survey. VIII. What Causes the Discrepancy in the Velocity between the CO and Hα Rotation Curves in Galaxies?

Su, Yung-Chau; Lin, Lihwai; Pan, Hsi-An; Cobá, Carlos López; Hsieh, Bau-Ching; Sanchez, Sebastian Francisco Sanchez; Thorp, Mallory; Bureau, Martin; Ellison, Sara L.

doi:10.3847/1538-4357/ac77fd

Cited by 9 publications

(7 citation statements)

References 43 publications

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“…We note that only 7/41 galaxies from the Genzel et al (2020) sample are observed in molecular gas, with the remainder being ionized gas, and Übler et al (2021) also model this gas phase. However, several published studies find very little measurable difference in rotation curves derived from ionized versus molecular gas (Genzel et al 2013;Übler et al 2018;Su et al 2022). 12/14 of the galaxies in our sample have higher asymmetry than the average galaxy in the Genzel et al (2020) sample, and 7/14 have higher asymmetry than the average galaxy in the Übler et al (2021) sample.…”

Section: Discussioncontrasting

confidence: 49%

“…Furthermore, inspection of the CO-Hα velocity curves for each galaxy in the ALMaQUEST subsample does not show significant asymmetric differences as a function of distance from the galaxy center. While it is unknown how much the difference in CO-Hα velocity curves may vary over cosmic time or with environment, a difference like that from the Su et al (2022) sample is insignificant compared to the other sources of uncertainty we already take into account. Furthermore, certain environmental effects that are particularly strong in dense environments, like ram pressure, are expected to have an even greater impact on the kinematics of the less dense ionized phase than the denser molecular gas, as has been observed, for example, in Boselli et al (1994).…”

Section: Girard Et Al 2021mentioning

confidence: 97%

“…This two-step fitting process with 3DBarolo helps ensure a more realistic rotation curve measurement than if the geometric and kinematic parameters were fit at the same time, which tends to lead to more unphysical discontinuities in the rotation field due to oscillations in the inclination and the P.A. (Teodoro & Fraternali 2015;Su et al 2022). In the second run we also utilize 3DBarolo's built-in method for estimating the uncertainty in the measurement of the rotation velocity and velocity dispersion.…”

Section: Kinematic Modelingmentioning

confidence: 99%

“…Genzel et al (2013) and Übler et al (2018) found excellent agreement in the rotation curve derived from Hα and CO in two star-forming galaxies at z ∼ 1.5. Also, in a larger sample of 17 nearby galaxies from the ALMaQUEST survey, the authors compared the rotation curve derived with 3DBarolo from separate ionized and molecular gas observations of each galaxy (Su et al 2022). They found that about half the galaxies had a measurable difference in the circular velocity of the two gas phases, with a median total velocity difference of 6.5 km s −1 .…”

Section: Girard Et Al 2021mentioning

confidence: 99%

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A Large-scale Kinematic Study of Molecular Gas in High-z Cluster Galaxies: Evidence for High Levels of Kinematic Asymmetry

Cramer

Noble

Cairns

et al. 2023

ApJ

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We investigate the resolved kinematics of the molecular gas, as traced by the Atacama Large Millimeter/submillimeter Array in CO (2−1), of 25 cluster member galaxies across three different clusters at a redshift of z ∼ 1.6. This is the first large-scale analysis of the molecular gas kinematics of cluster galaxies at this redshift. By separately estimating the rotation curve of the approaching and receding sides of each galaxy via kinematic modeling, we quantify the difference in total circular velocity to characterize the overall kinematic asymmetry of each galaxy. 3/14 of the galaxies in our sample that we are able to model have similar degrees of asymmetry as that observed in galaxies in the field at similar redshift based on observations of mainly ionized gas. However, this leaves 11/14 galaxies in our sample with significantly higher asymmetry, and some of these galaxies have degrees of asymmetry of up to ∼50 times higher than field galaxies observed at similar redshift. Some of these extreme cases also have one-sided tail-like morphology seen in the molecular gas, supporting a scenario of tidal and/or ram pressure interaction. Such stark differences in the kinematic asymmetry in clusters versus the field suggest the evolutionary influence of dense environments, established as being a major driver of galaxy evolution at low redshift, is also active in the high-redshift universe.

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Section: Discussioncontrasting

confidence: 49%

Section: Girard Et Al 2021mentioning

confidence: 97%

Section: Kinematic Modelingmentioning

confidence: 99%

Section: Girard Et Al 2021mentioning

confidence: 99%

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A Large-scale Kinematic Study of Molecular Gas in High-z Cluster Galaxies: Evidence for High Levels of Kinematic Asymmetry

Cramer

Noble

Cairns

et al. 2023

ApJ

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“…Therefore, we have an almost perfect agreement between the kinematic of the stars and that of the interstellar medium. This is not always the case, because in several galaxies, these two components have different rotational patterns (see, e.g., Williams et al 2021;Su et al 2022).…”

Section: Kinematics Of Stars and Gasmentioning

confidence: 99%

A Molecular Gas Ring Hidden in the Sombrero Galaxy

Sutter

Fadda

2022

ApJ

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We present Herschel, ALMA, and MUSE observations of the molecular ring of Messier 104, also known as the Sombrero galaxy. These previously unpublished archival data shed new light on the content of the interstellar medium of M104. In particular, molecular hydrogen measured by CO emission and dust measured by far-infrared light are uniformly distributed along the ring. The ionized gas revealed by Hα and [C ii] emission is distributed in knots along the ring. Despite being classified as an SAa galaxy, M104 displays features typical of early-type galaxies. We therefore compared its [C ii] and dust emission to a sample of early-type galaxies observed with Herschel and SOFIA. The [C ii]/FIR ratio of M104 is much lower than that of typical star-forming galaxies and is instead much more similar to that of early-type galaxies. By classifying regions using optical emission line diagnostics, we also find that regions classified as H ii lie closer to star-forming galaxies in the [C ii]/FIR diagram than those classified as low-ionization emission regions. The good match between [C ii] and Hα emission, in conjunction with the lack of correlation between CO emission and star formation, suggests that there is very limited active star formation along the ring and that most of the [C ii] emission is from ionized and neutral atomic gas rather than molecular gas. From the total intensity of the CO line, we estimate a molecular hydrogen mass of 0.9 × 109 M ⊙, a value intermediate between those of early-type galaxies and the content of the molecular ring of our galaxy.

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AGN feedback in the Local Universe: Multiphase outflow of the Seyfert galaxy NGC 5506

Esposito,

Alonso-Herrero,

García-Burillo

et al. 2024

A&A

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We present new optical GTC/MEGARA seeing-limited ($0.9 integral-field observations of NGC 5506, together with ALMA observations of the CO($3-2$) transition at a $0.2 pc) resolution. NGC 5506 is a luminous (bolometric luminosity of $ $ erg s$^ $) nearby (26 Mpc) Seyfert galaxy, part of the Galaxy Activity, Torus, and Outflow Survey (GATOS). We modelled the CO($3-2$) kinematics with 3D Barolo revealing a rotating and outflowing cold gas ring within the central 1.2 kpc. We derived an integrated cold molecular gas mass outflow rate for the ring of $ odot $ yr$^ $. We fitted the optical emission lines with a maximum of two Gaussian components to separate rotation from non-circular motions. We detected high OIII 5007$ projected velocities (up to $ 1000$ km $) at the active galactic nucleus (AGN) position, decreasing with radius to an average $ 330$ km $ around $ pc. We also modelled the OIII gas kinematics with a non-parametric method, estimating the ionisation parameter and electron density in every spaxel, from which we derived an ionised mass outflow rate of $0.076$ M$_ odot $ yr$^ $ within the central 1.2 kpc. Regions of high CO($3-2$) velocity dispersion, extending to projected distances of $ 350$ pc from the AGN, appear to be the result from the interaction of the AGN wind with molecular gas in the galaxy's disc. Additionally, we find the ionised outflow to spatially correlate with radio and soft X-ray emission in the central kiloparsec. We conclude that the effects of AGN feedback in NGC 5506 manifest as a large-scale ionised wind interacting with the molecular disc, resulting in outflows extending to radial distances of 610 pc.

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The ALMaQUEST Survey. VIII. What Causes the Discrepancy in the Velocity between the CO and Hα Rotation Curves in Galaxies?

Cited by 9 publications

References 43 publications

A Large-scale Kinematic Study of Molecular Gas in High-z Cluster Galaxies: Evidence for High Levels of Kinematic Asymmetry

A Large-scale Kinematic Study of Molecular Gas in High-z Cluster Galaxies: Evidence for High Levels of Kinematic Asymmetry

A Molecular Gas Ring Hidden in the Sombrero Galaxy

AGN feedback in the Local Universe: Multiphase outflow of the Seyfert galaxy NGC 5506

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