Ionized gas rotation curves in nearby dwarf galaxies

Моисеев, А. В.

doi:10.1134/s1990341314010015

Cited by 31 publications

(39 citation statements)

References 40 publications

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“…The final angular resolution corresponds to a seeing of 1. 8 in comparison to Moiseev (2014) and Moiseev et al (2015) with deeper data but with a worse 2. 7 resolution.…”

Section: Bta Datamentioning

confidence: 86%

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Pustilnik¹,

Макарова²,

Perepelitsyna³

et al. 2016

Mon. Not. R. Astron. Soc.

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The paper presents new results of the ongoing study of the unusual Lynx-Cancer void galaxy DDO 68 with record-low-metallicity regions (12+log(O/H)∼7.14) of the current star formation (SF). They include: a) a new spectrum and photometry with the 6-m SAO RAS telescope (BTA) for the Luminous Blue Variable (LBV = DDO68-V1). Photometric data sets are complemented with those based on the Sloan Digital Sky Survey (SDSS) and the Hubble Space Telescope (HST) archive images; b) the analysis of the DDO 68 supergiant shell (SGS) and the prominent smaller Hα arcs/shells visible at the HST image coupled with kinematics maps in Hα obtained with the Fabry-Perot interferometer (FPI) at the BTA; c) the list of identified at the HST images of about 50 most luminous stars (−9.1 < M V < −6.0 mag) related to star-forming regions with the known extremely low O/H. This is intended to pave the path for the actual science with the next generation of giant telescopes. We confirm the earlier hints on significant variations of the LBV optical light deriving its amplitude of ∆V 3.7 mag for the first time. New data suggest that in 2008-2010 the LBV reached M V = -10.5 and probably underwent a giant eruption. We argue that the structure of star-forming complexes along the SGS ('Northern Ring') perimeter provides evidence for the sequential induced SF episodes caused by the shell gas instabilities and gravitational collapse. The variability of some DDO 68 luminous extremely metal-poor stars can be monitored with medium-size telescopes at sites with superb seeing.

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“…The final angular resolution corresponds to a seeing of 1. 8 in comparison to Moiseev (2014) and Moiseev et al (2015) with deeper data but with a worse 2. 7 resolution.…”

Section: Bta Datamentioning

confidence: 86%

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Pustilnik¹,

Макарова²,

Perepelitsyna³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We constructed a rotation model of Ho II from the H i velocity field using the tilted-ring approximation adapted to dwarf galaxy kinematics (Moiseev 2014) with initial parameters for Ho II taken from Oh et al (2011) (we list them in Table 2) and then subtracted this model from the observed data cube. As a result, we have obtained the data cube that reflects the local motions caused by stellar feedback.…”

Section: Optical Fpi Observationsmentioning

confidence: 99%

Complexes of triggered star formation in supergiant shell of Holmberg II

Egorov

Lozinskaya

Моисеев

et al. 2016

Mon. Not. R. Astron. Soc.

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We report a detailed analysis of all regions of current star formation in the walls of the supergiant H i shell (SGS) in the galaxy Holmberg II based on observations with a scanning Fabry-Perot interferometer at the 6-m SAO RAS telescope. We compare the structure and kinematics of ionized gas with that of atomic hydrogen and with the stellar population of the SGS. Our deep Hα images and archival images taken by the HST demonstrate that current star formation episodes are larger and more complicated than previously thought: they represent unified star-forming complexes with sizes of several hundred pc rather than 'chains' of separate bright nebulae in the walls of the SGS. The fact that we are dealing with unified complexes is evidenced by identified faint shell-like structures of ionized and neutral gas which connect several distinct bright H ii regions. Formation of such complexes is due to the feedback of stars with very inhomogeneous ambient gas in the walls of the SGS. The arguments supporting an idea about the triggering of star formation in SGS by the H i supershells collision are presented. We also found a faint ionized supershell inside the H i SGS expanding with a velocity of no greater than 10 − 15 km s −1 . Five OB stars located inside the inner supershell are sufficient to account for its radiation, although a possibility of leakage of ionizing photons from bright H ii regions is not ruled out as well.

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“…We construct a rotation model of IC 2574 from the H i velocity field (moment 1) using the tilted-ring approximation adapted to dwarf galaxy kinematics (Moiseev 2014). The coordinates of the dynamical centre, the inclination and the initial value of the major axis position angle were adapted from Oh et al (2008), who performed a careful study of the H i kinematics of this galaxy.…”

Section: Construction Of a Circular Rotation Modelmentioning

confidence: 99%

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Egorov¹,

Lozinskaya²,

Моисеев³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We analyse the ionized gas kinematics in the star formation regions of the supergiant shell (SGS) of the IC 2574 galaxy using observations with the Fabry-Perot interferometer at the 6-m telescope of SAO RAS; the data of the THINGS survey are used to analyze the neutral gas kinematics in the area. We perform the 'derotation' of the Hα and H i data cubes and show its efficiency in kinematics analysis. We confirm the SGS expansion velocity 25 km s −1 obtained by Walter & Brinks (1999) and conclude that the SGS is located at the far side of the galactic disc plane. We determine the expansion velocities, kinematic ages, and the required mechanical energy input rates for four star formation complexes in the walls of the SGS; for the remaining ones we give the limiting values of the above parameters. A comparison with the age and energy input of the complexes' stellar population shows that sufficient energy is fed to all H ii regions except one. We discuss in detail the possible nature of this region and that of another one, which was believed to be an SNR according to radio observations. We measured the expansion velocity of the latter and confirm its identification as an old SNR. Our observations allowed us to identify a faint diffuse Hα emission inside the SGS which was never observed before.

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Ionized gas rotation curves in nearby dwarf galaxies

Cited by 31 publications

References 40 publications

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Complexes of triggered star formation in supergiant shell of Holmberg II

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

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