Star formation and the kinematics of gas in the disk of NGC 628

Сахибов, Ф. Х.; Смирнов, М. А.

doi:10.1134/1.1836023

Cited by 17 publications

(35 citation statements)

References 16 publications

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“…Comparison of the pattern speed with the pure circular motion of the gas provided the velocity of gas inflow into the spiral arm at different radial distances. Corresponding corotation radius locates at R cor ≈ 7 kpc (Sakhibov & Smirnov 2004).…”

Section: Ngc 628 Previous Studiesmentioning

confidence: 99%

“…The rotation speed of the arms (pattern speed) is determined along with other parameters of the spiral-density wave (Sakhibov & Smirnov 2004) via a Fourier analysis of the azimuthal distribution of the observed radial velocities (Shostak & van der Kruit 1984) in annular zones of the disc of NGC 628. Comparison of the pattern speed with the pure circular motion of the gas provided the velocity of gas inflow into the spiral arm at different radial distances.…”

Section: Ngc 628 Previous Studiesmentioning

confidence: 99%

“…This study is based on our own observations of the galaxy in Hα line, obtained on the Maidanak Observatory with the 1.5 m telescope, Galaxy Evolution Explorer (GALEX) far-ultraviolet (FUV) data (Gusev & Efremov 2013;Gusev et al 2014), as well as a Fourier analysis of the spatial distribution of the radial velocities of the neutral gas in the disc (Sakhibov & Smirnov 2004).…”

Section: Introductionmentioning

confidence: 99%

“…Previously we compared a variation of the velocity of gas inflow, v ⊥ , into the spirals and the surface density of star formation rate, Σ SFR , in the disc with the galactocentric distance r in the spiral galaxy NGC 628 (Sakhibov & Smirnov 2004). We believe that the radial distribution of the SFR surface density, Σ SFR , over the disc has a ring form with the maximum at the galactocentric distance r ∼ 3 kpc, whereas the maximum of the velocity of gas inflow v ⊥ is situated at r ∼ 5 kpc.…”

Section: Introductionmentioning

confidence: 99%

“…We believe that the radial distribution of the SFR surface density, Σ SFR , over the disc has a ring form with the maximum at the galactocentric distance r ∼ 3 kpc, whereas the maximum of the velocity of gas inflow v ⊥ is situated at r ∼ 5 kpc. We derived the velocities of gas inflow v ⊥ into the spirals at different galactocentric distances via a Fourier analysis of the azimuthal distribution of the observed radial velocities in annular (ring form) zones of the disc of the NGC 628 and the radial profile of the surface density of SFR, using the empirical 'SFR vs. linear size' relation for star formation complexes (Sakhibov & Smirnov 2004) and coordinates, Hα fluxes, and the sizes of H II regions presented by Belley & Roy (1992).…”

Section: Introductionmentioning

confidence: 99%

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Star formation rates and the kinematics of gas in the spiral arms of NGC 628

2015

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Relations between star formation rates along the spiral arms and the velocities of gas inflow into the arms in grand-design galaxy NGC 628 were studied. We found that the radial distribution of average star formation rate in individual star formation regions in regular spiral arms correlates with the velocity of gas inflow into the spiral arms. Both distributions have maxima at a galactocentric distance of 4.5-5 kpc. There are no correlations between the radial distributions of average star formation rate in star formation regions in spiral arms and outside spiral arms in the main disc. We also did not find a correlation between the radial distribution of average star formation rate in star formation regions in spiral arms and H I column density.

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Section: Ngc 628 Previous Studiesmentioning

confidence: 99%

Section: Ngc 628 Previous Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Star formation rates and the kinematics of gas in the spiral arms of NGC 628

2015

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The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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Abstract. This paper examines relations between the radio surface brightness Σ and the diameter D (also known as Σ − D relations) for a sample of extragalactic supernova remnants (SNRs) as constructed from a combination of published data and data from our own surveys. Our sample of extragalactic SNRs is the largest ever devised for the purpose of analyzing Σ − D relations. The main results of this paper may be summarized as follows: (i) the empirical relations for SNRs in 10 of the 11 nearby galaxies studied have the approximately trivial Σ ∝ D −2 form, therefore limiting their interpretation as physically meaningful relations. In addition, these relations are subject to selection effects rendering them even less useful. Further Monte Carlo simulations suggest that the effect of survey sensitivity has the opposite effect of volume selection (e.g. Malmquist bias, a volume selection effect that shapes the Galactic sample) by tending to flatten the slopes toward a trivial relation. In this case, the true slopes may be steeper than the observed slopes; (ii) compact M 82 SNRs appear to follow a uniquely different Σ− D relation in comparison to the larger, older SNRs in the other 10 galaxies. Monte Carlo simulations suggest that the probability of this difference arising by chance is ≈1% to 10%, depending on what is assumed regarding the underlying SNR population; (iii) three candidate hypernova remnants were identified in our sample of 11 nearby galaxies.

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Direct Measurement of Neutron Star Recoil in the Oxygen‐rich Supernova Remnant Puppis A

Winkler

Petre

2007

ApJ

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A sequence of three Chandra X-ray Observatory High Resolution Camera images taken over a span of five years reveals arc-second-scale displacement of RX J0822-4300, the stellar remnant (presumably a neutron star) near the center of the Puppis A supernova remnant. We measure its proper motion to be 0.165 ± 0.025 arcsec yr −1 toward the west-southwest. At a distance of 2 kpc, this corresponds to a transverse space velocity of ∼1600 km s −1 . The space velocity is consistent with the explosion center inferred from proper motions of the oxygen-rich optical filaments, and confirms the idea that Puppis A resulted from an asymmetric explosion accompanied by a kick that imparted roughly 3×10 49 ergs of kinetic energy (some 3 percent of the kinetic energy for a typical supernova) to the stellar remnant. We discuss constraints on core-collapse supernova models that have been proposed to explain neutron star kick velocities.

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Star formation and the kinematics of gas in the disk of NGC 628

Cited by 17 publications

References 16 publications

Star formation rates and the kinematics of gas in the spiral arms of NGC 628

Star formation rates and the kinematics of gas in the spiral arms of NGC 628

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Direct Measurement of Neutron Star Recoil in the Oxygen‐rich Supernova Remnant Puppis A

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