Stellar subsystems of the galaxy NGC 1313

Тихонов, Н. А.; Galazutdinova, O. A.

doi:10.1134/s1063773716070082

Cited by 6 publications

(2 citation statements)

References 48 publications

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“…This southwestern region where the localized starburst is observed is just outside of the observation footprint of this study. A difference in stellar metallicity tracing a separate population was found throughout the disk by Tikhonov & Galazutdinova (2016), which they attribute to a past merger with a low-mass dwarf satellite that did not gravitationally distort the arms or central region of NGC 1313.…”

Section: Ngc 1313mentioning

confidence: 97%

ALMA-LEGUS. I. The Influence of Galaxy Morphology on Molecular Cloud Properties

Finn,

Johnson,

Indebetouw

et al. 2024

ApJ

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We present a comparative study of the molecular gas in two galaxies from the Legacy ExtraGalactic UV Survey (LEGUS) sample: barred spiral NGC 1313 and flocculent spiral NGC 7793. These two galaxies have similar masses, metallicities, and star formation rates, but NGC 1313 is forming significantly more massive star clusters than NGC 7793, especially young massive clusters (<10 Myr, >104 M ⊙). Using Atacama Large Millimeter/submillimeter Array (ALMA) CO(2–1) observations of the two galaxies with the same sensitivity and resolution (13 pc), we directly compare the molecular gas in these two similar galaxies to determine the physical conditions responsible for their large disparity in cluster formation. By fitting size–line width relations for the clouds in each galaxy, we find that NGC 1313 has a higher intercept than NGC 7793, implying that its clouds have higher kinetic energies at a given size scale. NGC 1313 also has more clouds near virial equilibrium than NGC 7793, which may be connected to its higher rate of massive cluster formation. However, these virially bound clouds do not show a stronger correlation with young clusters than with the general cloud population. We find surprisingly small differences between the distributions of molecular cloud populations in the two galaxies, though the largest of those differences is that NGC 1313 has higher surface densities and lower freefall times.

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Section: Ngc 1313mentioning

confidence: 97%

ALMA-LEGUS. I. The Influence of Galaxy Morphology on Molecular Cloud Properties

Finn,

Johnson,

Indebetouw

et al. 2024

ApJ

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“…A small number of red giants in a galaxy on the constructed CM diagram or an insufficient photometric limit of its images lead to great uncertainties in measuring the position of the TRGB jump and, hence, to a low accuracy in measuring the distance to the galaxy. Furthermore, the fact that a charge transfer inefficiency appeared in the ACS/WFC in the time of their work under cosmic radiation (Anderson and Bedin, 2010;Massey et al, 2010;Tikhonov and Galazutdinova, 2016), which becomes progressively larger from year to year, should be taken into account. The central part of the ACS/WFC became virtually unsuitable for accurate photometric measurements due to this effect.…”

Section: Distance Measurementsmentioning

confidence: 99%

Distances to 18 Dwarf Galaxies from the Arecibo Survey

Тихонов

Galazutdinova

2019

Astron. Lett.

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Based on the archival Hubble Space Telescope images, we have performed stellar photometry for 18 dwarf galaxies. Branches of young and old stars are seen on the constructed Hertzsprung-Russell diagrams. Using the photometry of red giants and applying the TRGB method, we have determined accurate distances for all 18 galaxies for the first time. The galaxies AGC 238890 and AGC 747826 have minimum (D = 5.1 Mpc) and maximum (D = 12.0 Mpc) distances, respectively. The distances to the remaining galaxies lie within this range. Low-metallicity galaxies have been identified by measuring the color indices of the red giant branch:

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Ultraluminous X-ray sources with flat-topped noise and QPO

Атапин

Fabrika

Caballero‐García

2019

Monthly Notices of the Royal Astronomical Society

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We analyzed the X-ray power density spectra of five ultraluminous X-ray sources (ULXs) NGC 5408 X-1, NGC 6946 X-1, M 82 X-1, NGC 1313 X-1 and IC 342 X-1 that are the only ULXs which display both flat-topped noise (FTN) and quasi-periodic oscillations (QPO). We studied the QPO frequencies, fractional root-mean-square (rms) variability, X-ray luminosity and spectral hardness. We found that the level of FTN is anti-correlated with the QPO frequency. As the frequency of the QPO and brightness of the sources increase, their fractional variability decreases. We propose a simple interpretation using the spherizarion radius, viscosity time and α-parameter as basic properties of these systems. The main physical driver of the observed variability is the mass accretion rate which varies 3 between different observations of the same source. As the accretion rate decreases the spherization radius reduces and the FTN plus the QPO move toward higher frequencies resulting in a decrease of the fractional rms variability. We also propose that in all ULXs when the accretion rate is low enough (but still super-Eddington) the QPO and FTN disappear. Assuming that the maximum X-ray luminosity depends only on the black hole (BH) mass and not on the accretion rate (not considering the effects of either the inclination of the super-Eddington disc nor geometrical beaming of radiation) we estimate that all the ULXs have about similar BH masses, with the exception of M 82 X-1, which might be 10 times more massive.

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Stellar subsystems of the galaxy NGC 1313

Cited by 6 publications

References 48 publications

ALMA-LEGUS. I. The Influence of Galaxy Morphology on Molecular Cloud Properties

ALMA-LEGUS. I. The Influence of Galaxy Morphology on Molecular Cloud Properties

Distances to 18 Dwarf Galaxies from the Arecibo Survey

Ultraluminous X-ray sources with flat-topped noise and QPO

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