Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

Pan, Hsi-An; Kuno, Nario

doi:10.3847/1538-4357/aa60c2

Cited by 21 publications

(20 citation statements)

References 71 publications

(124 reference statements)

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“…Measurements of GMC properties may be affected by the missing flux (e.g., Rosolowsky & Leroy 2006;Pan & Kuno 2017). Our ALMA observations did not recover the total CO(1 − 0) flux due to the lack of Atacama Compact Array (ACA) measurements.…”

Section: Impact Of the Missing Fluxmentioning

confidence: 79%

Properties of giant molecular clouds in the strongly barred galaxy NGC 1300

Maeda

Ohta

Fujimoto

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Star formation activity depends on galactic-scale environments. To understand the variations in star formation activity, comparing the properties of giant molecular clouds (GMCs) among environments with different star formation efficiency (SFE) is necessary. We thus focus on a strongly barred galaxy to investigate the impact of the galactic environment on the GMCs properties, because the SFE is clearly lower in bar regions than in arm regions. In this paper, we present the 12 CO(1 − 0) observations toward the western bar, arm and bar-end regions of the strongly barred galaxy NGC 1300 with ALMA 12-m array at a high angular resolution of ∼40 pc. We detected GMCs associated with the dark lanes not only in the arm and bar-end regions but also in the bar region, where massive star formation is not seen. Using the CPROPS algorithm, we identified and characterized 233 GMCs across the observed regions. Based on the Kolmogorov-Smirnov test, we find that there is virtually no significant variations in GMC properties (e.g., radius, velocity dispersion, molecular gas mass, and virial parameter) among the bar, arm and bar-end region. These results suggest that systematic differences in the physical properties of the GMCs are not the cause for SFE differences with environments, and that there should be other mechanisms which control the SFE of the GMCs such as fast cloud-cloud collisions in NGC 1300.

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Section: Impact Of the Missing Fluxmentioning

confidence: 79%

Properties of giant molecular clouds in the strongly barred galaxy NGC 1300

Maeda

Ohta

Fujimoto

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…From these, we can see that although our SEDIGISM clouds do show some correlation on both plots, neither of these follow the scaling relations proposed by previous works. The right-hand side panels show a compilation of literature catalogues of molecular clouds in green colour scale, including both Galactic studies (Oka et al 2001;Heyer et al 2009;Roman-Duval et al 2010;Rice et al 2016;Barnes et al 2016;Miville-Deschênes et al 2017;Colombo et al 2019;Rigby et al 2019) and extragalactic studies (Rosolowsky & Blitz 2005;Bolatto et al 2008;Wong et al 2011;Gratier et al 2012;Wei et al 2012;Donovan Meyer et al 2013;Colombo et al 2014;Leroy et al 2015;Utomo et al 2015;Faesi et al 2016;Tosaki et al 2017;Freeman et al 2017;Pan & Kuno 2017;Schruba et al 2017). On those, we overplot the loci of the distribution of our science sample as the black ellipse, produced from a principal component analysis 15 , where the dashed-line represents the Larson relation.…”

Section: Science Samplementioning

confidence: 99%

The SEDIGISM survey: molecular clouds in the inner Galaxy

Duarte-Cabral

Colombo

Urquhart

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use the 13CO (2-1) emission from the SEDIGISM (Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium) high-resolution spectral-line survey of the inner Galaxy, to extract the molecular cloud population with a large dynamic range in spatial scales, using the Spectral Clustering for Interstellar Molecular Emission Segmentation (scimes) algorithm. This work compiles a cloud catalogue with a total of 10663 molecular clouds, 10300 of which we were able to assign distances and compute physical properties. We study some of the global properties of clouds using a science sample, consisting of 6664 well resolved sources and for which the distance estimates are reliable. In particular, we compare the scaling relations retrieved from SEDIGISM to those of other surveys, and we explore the properties of clouds with and without high-mass star formation. Our results suggest that there is no single global property of a cloud that determines its ability to form massive stars, although we find combined trends of increasing mass, size, surface density and velocity dispersion for the sub-sample of clouds with ongoing high-mass star formation. We then isolate the most extreme clouds in the SEDIGISM sample (i.e. clouds in the tails of the distributions) to look at their overall Galactic distribution, in search for hints of environmental effects. We find that, for most properties, the Galactic distribution of the most extreme clouds is only marginally different to that of the global cloud population. The Galactic distribution of the largest clouds, the turbulent clouds and the high-mass star-forming clouds are those that deviate most significantly from the global cloud population. We also find that the least dynamically active clouds (with low velocity dispersion or low virial parameter) are situated further afield, mostly in the least populated areas. However, we suspect that part of these trends may be affected by some observational biases (such as completeness and survey limitations), and thus require further follow up work in order to be confirmed.

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“…The emergence of modern facilities such as the Atacama Large Millimeter Array has brought with it studies of GMCs across a much greater variety of galaxies. Observations of barred spiral galaxies shows clouds in the barred/nuclear regions have higher surface densities compared to their arm/inter-arm brethren (Freeman et al 2017;Pan & Kuno 2017;Egusa et al 2018;Hirota et al 2018), with the galaxy as a whole containing a diverse cloud population (see also Tosaki et al 2017;Wu et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The changing GMC population in galaxy interactions

Pettitt

Egusa

Dobbs

et al. 2018

Monthly Notices of the Royal Astronomical Society

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With the advent of modern observational efforts providing extensive giant molecular cloud catalogues, understanding the evolution of such clouds in a galactic context is of prime importance. While numerous previous numerical and theoretical works have focused on the cloud properties in isolated discs, few have looked into the cloud population in an interacting disc system. We present results of the first study investigating the evolution of the cloud population in galaxy experiencing an M51-like tidal fly-by using numerical simulations including star formation, interstellar medium cooling and stellar feedback. We see the cloud population shift to large unbound clouds in the wake of the companion passage, with the largest clouds appearing as fleeting short-lived agglomerations of smaller clouds within the tidal spiral arms, brought together by large scale streaming motions. These are then sheared apart as they leave the protection of the spiral arms. Clouds appear to lead diverse lives, even within similar environments, with some being born from gas shocked by filaments streaming into the spiral arms, and others from effectively isolated smaller colliding pairs. Overall this cloud population produces a shallower mass function than the disc in isolation, especially in the arms compared to the inter-arm regions. Direct comparisons to M51 observations show similarities between cloud populations, though models tailored to the mass and orbital models of M51 appear necessary to precisely reproduce the cloud population.

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Variation in GMC Association Properties across the Bars, Spiral Arms, Inter-arms, and Circumnuclear Region of M100 (NGC 4321) Extracted from ALMA Observations

Cited by 21 publications

References 71 publications

Properties of giant molecular clouds in the strongly barred galaxy NGC 1300

Properties of giant molecular clouds in the strongly barred galaxy NGC 1300

The SEDIGISM survey: molecular clouds in the inner Galaxy

The changing GMC population in galaxy interactions

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