Gas-dust correlations in nearby galaxies: a case study of NGC 3184 and NGC 7793

Saikia, Gautam; Patra, Narendra Nath; Roy, Nirupam; Jog, Chanda J.

doi:10.1093/mnras/stz3635

Cited by 6 publications

(6 citation statements)

References 45 publications

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“…This could indicate a peculiar overabundance of Hi, with respect to dust, that correlates well with the dust itself, within r 25 . The pixel-by-pixel SR between dust and Hi in NGC 7793 has been recently studied by Saikia et al (2020) finding a weaker correlation than ours. This discrepancy could be due to a mixture of different factors.…”

Section: Appendix A: Additional Figures -Scaling Relationscontrasting

confidence: 77%

“…This resolution is that of the Herschel-SPIRE 500 µm maps used in the spectral energy distribution (SED) fitting procedures in C17. All maps are resampled to a pixel size equal to the adopted dust resolution, 36 , that is one pixel per beam (see, e.g., Viaene et al 2014;Vutisalchavakul et al 2014;Casasola et al 2015;Saikia et al 2020, for a similar treatment of images). This choice differs from that adopted in C17 where the maps have been resampled to a pixel size equal to 12 (1/3 × FWHM).…”

Section: Image Convolution and Resizingmentioning

confidence: 99%

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The resolved scaling relations in DustPedia: Zooming in on the local Universe

Casasola¹,

Bianchi²,

Magrini³

et al. 2022

A&A

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Aims. We perform a homogeneous analysis of an unprecedented set of spatially resolved scaling relations (SRs) between interstellar medium (ISM) components, that is to say dust, gas, and gas-phase metallicity, and other galaxy properties, such as stellar mass (M star ), total baryonic content, and star-formation rate (SFR), in a range of physical scales between 0.3 and 3.4 kpc. We also study some ratios between galaxy components: dust-to-stellar, dust-to-gas, and dust-to-metal ratios. Methods. We use a sample of 18 large, spiral, face-on DustPedia galaxies. The sample consists of galaxies with spatially resolved dust maps corresponding to 15 Herschel-SPIRE 500 µm resolution elements across the optical radius, with the morphological stage spanning from T = 2 to 8, M star from 2 × 10 9 to 1 × 10 11 M , SFR from 0.2 to 13 M yr −1 , and oxygen abundance from 12 + log(O/H) = 8.3 to 8.8. Results. All the SRs are moderate or strong correlations except the dust-Hi SR that does not exist or is weak for most galaxies. The SRs do not have a universal form but each galaxy is characterized by distinct correlations, affected by local processes and galaxy peculiarities. The SRs hold, on average, starting from the scale of 0.3 kpc, and if a breaking down scale exists it is below 0.3 kpc. By evaluating all galaxies together at the common scale of 3.4 kpc, differences due to peculiarities of individual galaxies are cancelled out and the corresponding SRs are consistent with those of whole galaxies. By comparing subgalactic and global scales, the most striking result emerges from the SRs involving ISM components: the dust-total gas SR is a good correlation at all scales, while the dust-H 2 and dust-Hi SRs are good correlations at subkiloparsec/kiloparsec and total scales, respectively. For the other explored SRs, there is a good agreement between small and global scales and this may support the picture where the main physical processes regulating the properties and evolution of galaxies occur locally. In this scenario, our results are consistent with the hypothesis of self-regulation of the star-formation process. The analysis of subgalactic ratios between galaxy components shows that they are consistent with those derived for whole galaxies, from low to high redshift, supporting the idea that also these ratios could be set by local processes. Conclusions. Our results highlight the heterogeneity of galaxy properties and the importance of resolved studies on local galaxies in the context of galaxy evolution. They also provide fundamental observational constraints to theoretical models and updated references for high-redshift studies.

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Section: Appendix A: Additional Figures -Scaling Relationscontrasting

confidence: 77%

Section: Image Convolution and Resizingmentioning

confidence: 99%

The resolved scaling relations in DustPedia: Zooming in on the local Universe

Casasola¹,

Bianchi²,

Magrini³

et al. 2022

A&A

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“…has found that in smaller LMC-like galaxies GMC properties tend to be similarly shifted to lower values. Thus the it is not unexpected that NGC 7793, which has approximately a tenth of the gas mass of our simulated galaxies (Saikia et al 2020) has distributions centred at lower values.…”

Section: Gmc Propertiesmentioning

confidence: 57%

Physical properties and scaling relations of molecular clouds: the impact of star formation

Grisdale

2020

Monthly Notices of the Royal Astronomical Society

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Using hydrodynamical simulations of a Milky Way-like galaxy, reaching 4.6 pc resolution, we study how the choice of star formation criteria impacts both galactic and Giant Molecular Clouds (GMC) scales. We find that using a turbulent, self-gravitating star formation criteria leads to an increase in the fraction of gas with densities between 10 and $10^{4}{\, \rm {cm^{-3}}}$ when compared with a simulation using a molecular star formation method, despite both having nearly identical gaseous and stellar morphologies. Furthermore, we find that the site of star formation is effected with the the former tending to only produce stars in regions of very high density ($>10^{4}{\, \rm {cm^{-3}}}$) gas while the latter forms stars along the entire length of its spiral arms. The properties of GMCs are impacted by the choice of star formation criteria with the former method producing larger clouds. Despite the differences we find that the relationships between clouds properties, such as the Larson relations, remain unaffected. Finally, the scatter in the measured star formation efficiency per free-fall time of GMCs remains present with both methods and is thus set by other factors.

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“…Theoretically, in the absence of turbulence in the ISM, the HI spectral width is expected to be ∼ few km/s solely due to kinetic temperature. However, the turbulence significantly increases this width, such as the signature of a two-phase medium can be observed at much higher spectral widths (Saikia et al 2020). Saikia et al (2020) used the HI spectral cubes of two galaxies, NGC 3184 and NGC 7793, and decomposed them into multiple Gaussian components (using the same technique we use here).…”

Section: The Efficiency Of the Fittingmentioning

confidence: 99%

“…However, the turbulence significantly increases this width, such as the signature of a two-phase medium can be observed at much higher spectral widths (Saikia et al 2020). Saikia et al (2020) used the HI spectral cubes of two galaxies, NGC 3184 and NGC 7793, and decomposed them into multiple Gaussian components (using the same technique we use here). They found a clear bimodal distribution in the widths of the Gaussian components (see Fig.…”

Section: The Efficiency Of the Fittingmentioning

confidence: 99%

The GMRT archive atomic gas survey -- I. Survey definition, methodology, and initial results from the pilot sample

Biswas,

Patra,

Roy

et al. 2022

Preprint

Self Cite

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Interferometric observations of HI in galaxies played a pivotal role in studies of nearby galaxies. Compared to singledish observation, it provides resolved distribution of gas in galaxies with unprecedented resolution. Several extensive HI surveys of nearby galaxies have been performed in the past; however, most of them consist of less than 100 galaxies due to individual efforts. On the other hand, present-day archives of the radio telescopes include data for at least several hundred galaxies. To utilize these data sets to their full potential, we construct a sample including all galaxies observed by the Giant Meter wave Radio Telescope (GMRT) in HI. This results in a total of 515 galaxies, the largest sample to date. We intend to analyze all the data uniformly and carry out different exciting science. As a pilot project, we analyze data from 11 galaxies and present the data products in this paper. We further investigate the neutral ISM in these galaxies and extract cold and warm phases using a multi-Gaussian decomposition method. This pilot project assures the quality of the data, which will enable us to perform critical science investigations using the full sample.

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Gas-dust correlations in nearby galaxies: a case study of NGC 3184 and NGC 7793

Cited by 6 publications

References 45 publications

The resolved scaling relations in DustPedia: Zooming in on the local Universe

The resolved scaling relations in DustPedia: Zooming in on the local Universe

Physical properties and scaling relations of molecular clouds: the impact of star formation

The GMRT archive atomic gas survey -- I. Survey definition, methodology, and initial results from the pilot sample

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