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Moiseev, G. K.; Vatolin, N. A.

doi:10.1023/a:1010182716950

Cited by 11 publications

(24 citation statements)

References 11 publications

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“…This galaxy is known to have strong nuclear and patchy circumnuclear Hα emission (Knapen et al 2006). It possesses kinematically distinct regions; Afanasiev et al (1988) first detected non‐circular phenomena in the central region ( R < 5 arcsec) and in the periphery of the galaxy at around 40–50 arcsec to the north‐east from the centre, which was later confirmed by Moiseev (2000) who also drew attention to the ‘spur’ of H ii regions in the north‐east part of the galaxy which does not follow the spiral arms. Condon (1987) mapped the galaxy at 1.49 GHz and noted a continuum source 3.5 arcmin south of the galaxy.…”

Section: Introductionmentioning

confidence: 93%

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Study of star formation in NGC 1084

Ramya

Sahu

Prabhu

2007

Monthly Notices of the Royal Astronomical Society

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We present UBVRI broad band, H$\alpha$ narrow band photometry of the star forming complexes in the infra-red bright galaxy NGC 1084. Results of medium resolution spectroscopy of some of the brighter complexes are also discussed. Spectroscopic data is used to better estimate the internal reddening within the galaxy which is found to be highly variable and to calculate metallicity which is close to the solar value. Diagnostic diagram identifies the shocked regions within this galaxy. The narrow band H$\alpha$ flux and its equivalent width are used to determine the star formation rates of the complexes and the distribution of ages. Star formation rates for a few of the complexes are found to be as high as 0.5 $M_{\odot}$/year. The star forming complexes lie in the age range 3 Myr to 6.5 Myr. U-B vs V-I colour-colour mixed population model created using the Starburst99 model colours is used to estimate the ages of the stellar populations present within these regions. Using this technique, it is found that the star formation in NGC 1084 has taken place in a series of short bursts over the last 40 Myr or so. It is proposed that the likely trigger for enhanced star formation is merger with a gas rich dwarf galaxy.Comment: 9 figures and 6 tables, Accepted in MNRAS for publicatio

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Section: Introductionmentioning

confidence: 93%

“…The size of the image is 3 × 3 arcmin 2 . The trapezium labelled as M represents the ‘spur’ region of Moiseev (2000) (see for explanation).…”

Section: Observations and Analysismentioning

confidence: 99%

Study of star formation in NGC 1084

Ramya

Sahu

Prabhu

2007

Monthly Notices of the Royal Astronomical Society

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“…Reduction of the observational material was performed using the software package operating in the IDL environment (Moiseev, 2002;Moiseev & Egorov, 2008). The reduction result is a data cube where each pixel in the field of view contains a 36-or 40-channel spectrum.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Ionized gas rotation curves in nearby dwarf galaxies

Моисеев

2014

Astrophys. Bull.

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Abstract. We present the results of study of the ionized gas velocity fields in 28 nearby (systemic velocity below 1000 km s −1 ) dwarf galaxies. The observations were made at the 6-m BTA telescope of the SAO RAS with the scanning Fabry-Perot interferometer in the Hα emission line. We were able to measure regular circular rotation parameters in 25 galaxies. As a rule, rotation velocities measured in H II are in a good agreement with the data on the H I kinematics at the same radii. Three galaxies reveal position angles of the kinematic axis in the H II velocity fields that strongly (tens of degrees) differ from the measurements in neutral hydrogen at large distances from the center or from the orientation of the major axis of optical isophotes. The planes of the gaseous and stellar disks in these galaxies most likely do not coincide. Namely, in DDO 99 the gaseous disk is warped beyond the optical radius, and in UGC 3672 and UGC 8508 the inclination of orbits of gas clouds varies in the inner regions of galaxies. It is possible that the entire ionized gas in UGC 8508 rotates in the plane polar to the stellar disk.

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“…Also the position angle of the bar PA b must be added for an arbitrary coordinate axes orientation. The model was calculated through the iterative technique by means of the IDL-based software GIDRA (Moiseev 1998). As a first step we average the original image data in the ellipses with PA 0 and i 0 and calculate a first approximation of the m d and r d in the disk-dominated region from the brightness profile obtained.…”

Section: Embedded Disks?mentioning

confidence: 99%

Structure and kinematics of candidate double-barred galaxies

Моисеев

Valdés

Chavushyan

2004

A&A

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Abstract.Results of optical and NIR spectral and photometric observations of a sample of candidate double-barred galaxies are presented. Velocity fields and velocity dispersion maps of stars and ionized gas, continuum and emission-line images were constructed from integral-field spectroscopy observations carried out at the 6 m telescope (BTA) of SAO RAS, with the MPFS spectrograph and the scanning Fabry-Perot Interferometer. NGC 2681 was also observed with the long-slit spectrograph of the BTA. Optical and NIR images were obtained at the BTA and at the 2.1 m telescope (OAN, México). High-resolution images were retrieved from the HST data archive. Morphological and kinematic features of all 13 sample objects are described in detail. Attention is focused on the interpretation of observed non-circular motions of gas and stars in circumnuclear (one kiloparsec-scale) regions. We have shown first of all that these motions are caused by the gravitational potential of a large-scale bar. NGC 3368 and NGC 3786 have nuclear bars only, their isophotal twist at larger radii being connected with the bright spiral arms. Three cases of inner polar disks in our sample (NGC 2681, NGC 3368 and NGC 5850) are considered. We found ionized-gas counter-rotation in the central kiloparsec of the lenticular galaxy NGC 3945. Seven galaxies (NGC 470, NGC 2273, NGC 2681, NGC 3945, NGC 5566, NGC 5905, and NGC 6951) have inner mini-disks nested in large-scale bars. Minispiral structures occur often in these nuclear disks. It is interesting that the majority of the observed, morphological and kinematical, features in the sample galaxies can be explained without the secondary bar hypothesis. Thus we suggest that a dynamically independent secondary bar is a rarer phenomenon than follows from isophotal analysis of the images only.

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Cited by 11 publications

References 11 publications

Study of star formation in NGC 1084

Study of star formation in NGC 1084

Ionized gas rotation curves in nearby dwarf galaxies

Structure and kinematics of candidate double-barred galaxies

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