Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Wu, Yu-Ting; Trejo, Alfonso; Espada, Daniel; Miyamoto, Yusuke

doi:10.1093/mnras/stab1087

Cited by 6 publications

(4 citation statements)

References 49 publications

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“…We note in passing that observations of external barred spirals oftentimes show evidence for an alignment of the molecular bar (if present) with a stellar bar. Examples are M 83 (Lundgren et al 2004;Hirota et al 2018), M 100 (Sempere & Garcia-Burillo 1997), NGC 4569 (Boone et al 2007), and even doubled-barred spirals such as NGC 3504 (Kuno et al 2000;Wu et al 2021). For the Milky Way, determinations of the bar inclination angle indicate values between 20 • (Queiroz et al 2021) and 45 • (Anders et al 2019), but neither of these angles agrees with the vanishing inclination angle of the feature described above.…”

Section: Resultsmentioning

confidence: 90%

Bayesian inference of three-dimensional gas maps

Mertsch

Vittino

2021

A&A

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Carbon monoxide (CO) is the best tracer of Galactic molecular hydrogen (H2). Its lowest rotational emission lines are in the radio regime, and thanks to Galactic rotation, emission at different distances is Doppler shifted. For a given gas flow model, the observed spectra can thus be deprojected along the line of sight to infer the gas distribution. We used the CO-line survey of Dame et al. (2001, ApJ, 547, 792) to reconstruct the three-dimensional density of H2. We considered the deprojection as a Bayesian variational inference problem. The posterior distribution of the gas densities allowed us to estimate the mean and uncertainty of the reconstructed density. Unlike most of the previous attempts, we took the correlations of gas on a variety of scales into account, which allowed us to correct for some of the well-known pathologies, such as finger-of-god effects. The two gas flow models that we adopted incorporate a Galactic bar that induces radial motions in the inner few kiloparsecs and thus offers spectral resolution towards the Galactic centre. We compared our gas maps with those of earlier studies and characterise their statistical properties, for instance the radial profile of the average surface mass density.

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Section: Resultsmentioning

confidence: 90%

Bayesian inference of three-dimensional gas maps

Mertsch

Vittino

2021

A&A

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“…This model assumes the gas is flowing along f bar . This expression is similar to Hirota et al (2009) and Wu et al (2021), assuming that the gas flows parallel to the bar major axis.…”

Section: Kinematic Interpretation Of the Oval Distortionmentioning

confidence: 81%

“…We showed that this is achieved just by fixing the orientation of the stream flow to the bar major axis in the models, and the radial profiles of the noncircular velocities are consistent with the residuals from circular rotation, with possible differences in amplitudes due to assymmetric drift and other random motions not considered in the model as we showed in Figure 7. Apart from the elliptical motions considered in the bisymmetric models, radial inflows are expected in bars, and these are observed to occur along the bardust lanes (Wu et al 2021;Sormani et al 2023). Our implementation of an inflow model is therefore physically motivated.…”

Section: Discussionmentioning

confidence: 99%

Unveiling a Hidden Bar-like Structure in NGC 1087: Kinematic and Photometric Evidence Using MUSE/VLT, ALMA, and JWST

López-Cobá,

Lin,

Sánchez

2024

ApJ

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We report a faint nonaxisymmetric structure in NGC 1087 through the use of James Webb Space Telescope Near Infrared Camera, with an associated kinematic counterpart observed as an oval distortion in the stellar velocity map, Hα, and CO J = 2 → 1 velocity fields. This structure is not evident in the MUSE optical continuum images but only revealed in the near-IR with the F200W and F300M band filters at 2 μm and 3 μm, respectively. Due to its elongation, this structure resembles a stellar bar although with remarkable differences with respect to conventional stellar bars. Most of the near-IR emission is concentrated within 6″∼500 pc with a maximum extension up to 1.2 kpc. The spatial extension of the large-scale noncircular motions is coincident with the bar, which undoubtedly confirms the presence of a nonaxisymmetric perturbation in the potential of NGC 1087. The oval distortion is enhanced in CO due to its dynamically cold nature rather than in Hα. We found that the kinematics in all phases, including stellar, ionized, and molecular, can be described simultaneously by a model containing a bisymmetric perturbation; however, we find that an inflow model of gas along the bar major axis is also likely. Furthermore, the molecular mass inflow rate associated can explain the observed star-formation rate in the bar. This reinforces the idea that bars are mechanisms for transporting gas and triggering star formation. This work contributes to our understanding of nonaxisymmetry in galaxies using the most sophisticated data so far.

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“…Our proposed scenarios in association with the models by Sormani et al (2019Sormani et al ( , 2020 and (Tress et al 2020) can be supported by observations of galactic centres in other galaxies. Equivalents of the near and far side dust lanes, attributed to the Milky Way's CMZ, have been observed in, for example the centres of M 83 (Harada et al 2019;Callanan et al 2021), NGC 3504 (Wu et al 2021), and, recently, in a couple of more nearby galaxies thanks to the high angular resolution of the PHANGS survey (Physics at High Angular resolution in Nearby GalaxieS, e.g. Lee et al 2022).…”

Section: Implications For the Cmzmentioning

confidence: 99%

Living on the edge of the Milky Way's central molecular zone

Busch

Riquelme

Güsten

et al. 2022

A&A

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Context. The 1 • .3 (G1.3) and 1 • .6 (G1.6) cloud complexes in the central molecular zone (CMZ) of our Galaxy have been proposed to possibly reside at the intersection region of the X1 and X2 orbits for several reasons. This includes the detection of co-spatial low-and high-velocity clouds, high velocity dispersion, high fractional molecular abundances of shock-tracing molecules, and kinetic temperatures that are higher than for usual CMZ clouds. Aims. By investigating the morphology and deriving physical properties as well as chemical composition, we want to find the origin of the turbulent gas and, in particular, whether evidence of an interaction between clouds can be identified. Methods. We mapped both cloud complexes in molecular lines in the frequency range from 85 to 117 GHz with the IRAM 30 m telescope. The APEX 12 m telescope was used to observe higher frequency transitions between 210 and 475 GHz from selected molecules that are emitted from higher energy levels. We performed non-local thermodynamic equilibrium (non-LTE) modelling of the emission of an ensemble of CH 3 CN lines to derive kinetic temperatures and H 2 volume densities. These were used as starting points for non-LTE modelling of other molecules, for which column densities and abundances were determined and compared with values found for other sources in the CMZ.Results. The kinematic structure of G1.3 reveals an 'emission bridge' at intermediate velocities (∼150 km s −1 ) connecting lowvelocity (∼100 km s −1 ) and high-velocity (∼180 km s −1 ) gas and an overall fluffy shell-like structure. These may represent observational evidence of cloud-cloud interactions. Low-and high-velocity gas components in G1.6 do not show this type of evidence of an interaction, suggesting that they are spatially separated. We selected three positions in each cloud complex for further analysis. Each position reveals several gas components at various peak velocities and of various line widths. We derived kinetic temperatures of 60-100 K and H 2 volume densities of 10 4 -10 5 cm −3 in both complexes. Molecular abundances relative to H 2 suggest a similar chemistry of the two clouds, which is moreover similar to that of other GC clouds and, especially, agrees well with that of G+0.693 and G−0.11. Conclusions. We conclude that G1.3 may indeed exhibit signs of cloud-cloud interactions. In particular, we propose an interaction of gas that is accreted from the near-side dust lane to the CMZ, with gas pre-existing at this location. Low-and high-velocity components in G1.6 are rather coincidentally observed along the same line of sight. They may be associated with either overshot decelerated gas from the far-side dust line or actual CMZ gas and high-velocity gas moving on a dust lane. These scenarios would be in agreement with numerical simulations.

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Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Cited by 6 publications

References 49 publications

Bayesian inference of three-dimensional gas maps

Bayesian inference of three-dimensional gas maps

Unveiling a Hidden Bar-like Structure in NGC 1087: Kinematic and Photometric Evidence Using MUSE/VLT, ALMA, and JWST

Living on the edge of the Milky Way's central molecular zone

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