A Radio Continuum Study of Dwarf Galaxies: 6 cm Imaging of LITTLE THINGS

Hindson, L.; Kitchener, Ged; Brinks, E.; Heesen, V.; Westcott, Jonathan; Hunter, Deidre A.; Zhang, Hong Xin; Rupen, M. P.; Rau, Urvashi

doi:10.3847/1538-4365/aaa42c

Cited by 29 publications

(39 citation statements)

References 79 publications

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“…It is interesting that despite the fact that these two regions appear to be good SNR candidates, they do not exhibit any bright emission in the radio continuum. Only a faint source of the non-thermal radio continuum could be identi-fied between the regions MH7 and d in the images presented by Hindson et al (2018). This fact does not contradict their identification as SNRs.…”

Section: Regions Mh7 and D (Complex 3): Snr Candidatesmentioning

confidence: 64%

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Star formation complexes in the ‘galaxy-sized’ supergiant shell of the galaxy HolmbergI

Egorov

Lozinskaya

Моисеев

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the results of observations of the galaxy Holmberg I carried out at the Russian 6-m telescope in the narrow-band imaging, long-slit spectroscopy, and scanning Fabry-Perot interferometer modes. A detailed analysis of gas kinematics, ionization conditions, and metallicity of star-forming regions in the galaxy is presented. The aim of the paper is to analyse the propagation of star formation in the galaxy and to understand the role of the ongoing star formation in the evolution of the central 'galaxy-sized' supergiant H i shell (SGS), where all regions of star formation are observed. We show that star formation in the galaxy occurs in large unified complexes rather than in individual giant H ii regions. Evidence of the triggered star formation is observed both on scales of individual complexes and of the whole galaxy. We identified two supernova-remnant candidates and one late-type WN star and analysed their spectrum and surrounding-gas kinematics. We provide arguments indicating that the SGS in Holmberg I is destructing by the influence of star formation occurring on its rims.

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Section: Regions Mh7 and D (Complex 3): Snr Candidatesmentioning

confidence: 64%

“…The most interesting fact is that the only bright (1.4 mJy) radio continuum point-like source in the galaxy according to the VLA observations presented in Hindson et al (2018) (see fig. 20 there) clearly coincides with the MH20a region.…”

Section: Mh20 and Mh20a (Complex 4)mentioning

confidence: 89%

Star formation complexes in the ‘galaxy-sized’ supergiant shell of the galaxy HolmbergI

Egorov

Lozinskaya

Моисеев

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The evolution of the radio-IR relation has been calibrated on bright detected galaxies in our field, however, it has not yet been tested for lowmass galaxies. Local studies show that dwarf galaxies are often fainter than expected in radio continuum emission (e.g., Bell 2003;Leroy et al 2005;Paladino et al 2006;Filho et al 2019), with studies such as Hindson et al (2018) suggesting that the non-thermal synchrotron emission is suppressed. Measuring the radio-SED for a range of representative galaxies will be essential to resolve these issues.…”

Section: Systematic Uncertaintiesmentioning

confidence: 99%

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Leslie

Schinnerer

Liu

et al. 2020

ApJ

111

143

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We provide a coherent, uniform measurement of the evolution of the logarithmic star formation rate (SFR) -stellar mass (M * ) relation, called the main sequence of star-forming galaxies (MS), for starforming and all galaxies out to z ∼ 5. We measure the MS using mean stacks of 3 GHz radio continuum images to derive average SFRs for ∼ 200,000 mass-selected galaxies at z > 0.3 in the COSMOS field. We describe the MS relation adopting a new model that incorporates a linear relation at low stellar mass (log(M * /M )<10) and a flattening at high stellar mass that becomes more prominent at low redshift (z < 1.5). We find that the SFR density peaks at 1.5 < z < 2 and at each epoch there is a characteristic stellar mass (M * = 1−4×10 10 M ) that contributes the most to the overall SFR density. This characteristic mass increases with redshift, at least to z ∼ 2.5. We find no significant evidence for variations in the MS relation for galaxies in different environments traced by the galaxy number density at 0.3 < z < 3, nor for galaxies in X-ray groups at z ∼ 0.75. We confirm that massive bulgedominated galaxies have lower SFRs than disk-dominated galaxies at a fixed stellar mass at z < 1.2. As a consequence, the increase in bulge-dominated galaxies in the local star-forming population leads to a flattening of the MS at high stellar masses. This indicates that "mass-quenching" is linked with changes in the morphological composition of galaxies at a fixed stellar mass.

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“…We solve equations (8) and (9) with the vacuum boundary conditions and symmetry conditions (19) for a range of the disc aspect ratios and a range of R 0 in the rotation curve (4) to obtain D c and then the |D c | Figure 2. As in Fig.…”

Section: Critical Rotation Speedmentioning

confidence: 99%

The Origin of Large-Scale Magnetic Fields in Low-Mass Galaxies

2019

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The origin of large-scale magnetic fields, detected in some low-mass (dwarf and irregular) galaxies via polarised synchrotron emission and Faraday rotation, remained unexplained for a long time. We suggest that mean-field dynamo can be active in galaxies of this class despite their slow rotation because their discs are relatively thick. Earlier assessments of the possibility of the mean-field dynamo action in low-mass galaxies relied on estimates applicable to thin discs, such as those in massive spiral galaxies. Using both order-of-magnitude estimates and numerical solutions, we show that the strength of differential rotation required to amplify magnetic field reduces as the aspect ratio of the galactic gas layer increases. Thus, the puzzle of the origin of large-scale magnetic fields appears to be solved. As a result, this class of galaxies provides a new ground for testing our understanding of galactic magnetism.

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A Radio Continuum Study of Dwarf Galaxies: 6 cm Imaging of LITTLE THINGS

Cited by 29 publications

References 79 publications

Star formation complexes in the ‘galaxy-sized’ supergiant shell of the galaxy HolmbergI

Star formation complexes in the ‘galaxy-sized’ supergiant shell of the galaxy HolmbergI

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

The Origin of Large-Scale Magnetic Fields in Low-Mass Galaxies

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