The JCMT Nearby Galaxies Legacy Survey

Sánchez-Gallego, José R.; Knapen, Johan H.; Heiner, J. S.; Wilson, C. D.; Warren, B. E.; Allen, R. J.; Azimlu, Mohaddesseh; Barmby, P.; Bendo, G. J.; Comerón, Sébastien; Israel, F. P.; Serjeant, S.; Tilanus, R. P. J.; Vlahakis, C.; Werf, P. van der

doi:10.1051/0004-6361/201014930

Cited by 8 publications

(3 citation statements)

References 44 publications

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“…For NGC 3031 studied at 0.6 kpc the weak Σ star -Σ dust SR could be explained by its dust-to-star mass ratio, a factor 2 times lower than the corresponding mean value for galaxies of the same morphological stage (T = 2, data from DustPedia database and Table 7 of C20). We recall that NGC 3031 is a kind of prototype of CO-poor galaxies (e.g., Solomon & de Zafra 1975;Combes et al 1977;Brouillet et al 1991;Sage & Westpfahl 1991;Sakamoto et al 2001;Helfer et al 2003;Knapen et al 2006;Casasola et al 2007;Sánchez-Gallego et al 2011). Since the formation of H 2 molecules takes place on the surface of dust grains (Gould & Salpeter 1963), a connection between dust and molecular gas is expected and observed.…”

Section: Appendix A: Additional Figures -Scaling Relationsmentioning

confidence: 90%

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 Relationsmentioning

confidence: 90%

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

Casasola¹,

Bianchi²,

Magrini³

et al. 2022

A&A

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“…CO observations of M82 show that the molecular gas extends far beyond the disk, with the well-known gas outflows dominating the distribution (Leroy et al 2015). The CO in M81 is much less prominent and mainly associated with the dust in the spiral arms (Sánchez-Gallego et al 2011;Brouillet et al 1991). The CO in NGC 3077 is discussed in Walter et al (2002b) and Meier et al (2001).…”

Section: The South-east Cloudsmentioning

confidence: 98%

A High-resolution Mosaic of the Neutral Hydrogen in the M81 Triplet

Blok

Walter

Ferguson

et al. 2018

ApJ

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We present a 3 • ×3 • , 105-pointing, high-resolution neutral hydrogen (H i) mosaic of the M81 galaxy triplet, (including the main galaxies M81, M82 and NGC 3077, as well as dwarf galaxy NGC 2976) obtained with the Very Large Array (VLA) C and D arrays. This H i synthesis mosaic uniformly covers the entire area and velocity range of the triplet. The observations have a resolution of ∼ 20 or ∼ 420 pc. The data reveal many small-scale anomalous velocity features highlighting the complexity of the interacting M81 triplet. We compare our data with Green Bank Telescope (GBT) observations of the same area. This comparison provides evidence for the presence of a substantial reservoir of low-column density gas in the northern part of the triplet, probably associated with M82. Such a reservoir is not found in the southern part. We report a number of newly discovered kpc-sized low-mass H i clouds with H i masses of a few times 10 6 M . A detailed analysis of their velocity widths show that their dynamical masses are much larger than their baryonic masses, which could indicate the presence of dark matter if the clouds are rotationally supported. However, due to their spatial and kinematical association with H i tidal features, it is more likely that the velocity widths indicate tidal effects or streaming motions. We do not find any clouds that are not associated with tidal features down to an H i mass limit of a few times 10 4 M . We compare the H i column densities with resolved stellar density maps and find a star formation threshold around 3 − 6 · 10 20 cm −2 . We investigate the widths of the H i velocity profiles in the triplet and find that extreme velocity dispersions can be explained by a superposition of multiple components along the line of sight near M81 as well as winds or outflows around M82. The velocity dispersions found are high enough that these processes could explain the linewidths of Damped-Lyman-α absorbers observed at high redshift.

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“…All the CO J = 3-2 observations have been completed and the continuum observations have begun. Further information about the scope and science goals of this survey can be found in Wilson et al (2009) as well as in the subsequent series of papers which make use of the CO J = 3-2 data (Bendo et al 2010;Warren et al 2010;Irwin et al 2011;Sánchez-Gallego et al 2011;Wilson et al 2011).…”

mentioning

confidence: 99%

The JCMT Nearby Galaxies Legacy Survey - VII. H imaging and massive star formation properties

Sánchez-Gallego

Knapen

Wilson

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present Hα fluxes, star formation rates (SFRs) and equivalent widths (EWs) for a sample of 156 nearby galaxies observed in the 12CO J= 3–2 line as part of the James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey. These are derived from images and values in the literature and from new Hα images for 72 galaxies which we publish here. We describe the sample, observations and procedures to extract the Hα fluxes and related quantities. We discuss the SFR properties of our sample and confirm the well‐known correlation with galaxy luminosity, albeit with high dispersion. Our SFRs range from 0.1 to 11 M⊙ yr−1 with a median SFR value for the complete sample of 0.2 M⊙ yr−1. This median value is somewhat lower than similar published measurements, which we attribute, in part, to our sample being H i selected and, thus, not biased towards high SFRs as has frequently been the case in previous studies. Additionally, we calculate internal absorptions for the Hα line, A(Hα), which are lower than many of those used in previous studies. Our derived EWs, which range from 1 to 880 Å with a median value of 27 Å, show little dependence on luminosity but rise by a factor of 5 from early‐ to late‐type galaxies. This paper is the first in a series aimed at comparing SFRs obtained from Hα imaging of galaxies with information derived from other tracers of star formation and atomic and molecular gas.

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The JCMT Nearby Galaxies Legacy Survey

Cited by 8 publications

References 44 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

A High-resolution Mosaic of the Neutral Hydrogen in the M81 Triplet

The JCMT Nearby Galaxies Legacy Survey - VII. H imaging and massive star formation properties

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