IFP gallery: (1995 - 1999).

Here some data observed on the 6m telescope with IFP installed in the OLD focal reducer are presented. These are Seyfert galaxies, spiral galaxies and nebulaes . Click on images for enlarger.

Kinematic of the Narrow Line Regions in the Seyfert galaxies

The author of the observational program is V.L. Afanasiev. We observed the 2D kinematics of Sy galaxies with following features:

IFP observations have revealed a double-component structure of the [OIII] emission line profiles. We suggest that Z-shaped spiral filaments in NLRs have a common wave origin and generated by the hydrodynamic instability due to the velocity break between a galactic interstellar medium and a outflowing gas from the central AGN. About our observations and numerical simulations (provided by team form Volgograd State University) see preprints (astro-ph/006323) and (astro-ph/0111217).

Mkn 3: [OIII] image
Mkn 3: velocity field
Mkn 3 was observed 15 Nov. 1996 in the [OIII]5007 emission line with IPCS as detector. Texp =24x280 sec, seeing 1.5", IFP260.

Mkn 573: [OIII] image
Mkn 573: velocity field
Mkn 3 was observed 16 Nov. 1996 in the [OIII]5007 emission line with IPCS as detector. Texp=24x360 sec, seeing 1", IFP260.

NGC 5252: [OIII] image
NGC 5252: velocity field
NGC 5252 was observed 23 Feb. 1998 in the [OIII]5007 emission line with CCD TK1024 as detector. Texp=24x450 sec, seeing 1.5", IFP260.

Spiral galaxies

We observed the ionized gas velocity fields of the spiral galaxies with two purpose. Firstly, it is a a search of the non-circular gas motions connected with starforming regions and bars (the author is A.V.Zasov)). Secondly, the velocity fields were used for reconstruction of the gas motions in/around spiral arms ("Vortex" project , supervisor is A.M. Fridman). A Fourier-series expansion of velocity field was developed for this goal (see article Fridman et al., 2001, A&A, 371, 538 ).

NGC 157: Ha image

Restored velocity field of NGC 157 in the reference frame rotating with the pattern speed overlaid on the Ha image of the galaxy
NGC 157: Velocity field
NGC 157 was observed October 24, 1995 in the Ha emission line with IPCS as a detector. Texp=32x180 sec, seeing 2.5", IFP501. The velocity field of the galaxy is considered by Fridman et al., 2001, A&A, 371, 538 )

NGC 972: Ha image
NGC 3631: Ha image
NGC 4100
NGC 972: Velocity field
NGC 3631: Velocity field
NGC 4100
More examples of the galaxies observed in the Ha line for Vortex project : NGC 972 (02/21/98, Texp=24x180 sec, seeing 3", IFP260), NGC 3631 (12/10/96, Texp=24x180 sec, seeing 2", IFP501) and NGC 4100 (21/03/96, Texp=24x300 sec, seeing 2", IFP260, IPCS). The preliminary analysis of the NGC972 velocity field distorted by the nuclear minibar see in Zasov & Moiseev (astro-ph/9812121) and in Moiseev & Mustsevoi (2000, Astron. Lett., 26, 565 astro-ph/0011225). The restored velocity field of the NGC3631 is considered by Fridman et al., 2001, MNRAS, 323, 651 ).

NGC 1084: Ha image

A region around "shpur" is marked
NGC 1084 was observed 26/11/95 with IPCS and IFP501, Texp=220x32 seeing 2". The data has revealed two kinematic components in the Ha line with non-circular line-of-sight velocities -100..+150 km/s around of giant star formation regions (``spur'') in the NE part of the galaxy. The first component corresponds to normal circular rotation. The second velocity component has a signature of non-circular motions of the ionized gas in shock wave fronts. An increase of the [NII]}/Ha line ratio confirms the shock wave interpretation of these features. See Moiseev (2000, A&A, 363, 843).

Nebulae around WO-star in the galaxy IC 1613

The author of this observational program is T.A. Lozinskaya). The object was observed at the 6m telescope in August, 30 1998 in the Ha with IFP260, Texp=24x240 sec, seeing 2". IFP observations reveal a giant bipolar nebula around unique WO (oxygen WR) star in the dwarf galaxy IC 1613. This figure shows monochromatic Ha image obtained with IFP by integrating the emission over all spectral channels of the line. The image of the same region in continuum near H line is indicated by isophotes. The dashed line represents the giant bipolar shell. Sizes and expansion velocities of the shells:

The extended bipolar nebula was produced by the WO-wind breaking out of the ``wall’’ in HI cupercavity. For mor information see the articles by Afanasiev et al. (2000, Astron. Lett., 26, 153 astro-ph/0011385) and Lozinskaya et al. (2001, Astron. Reports, 45, 417 astro-ph/0103312).