Synchrotron superbubble in the galaxy IC 10: The ionized gas structure, kinematics, and emission spectrum

Monthly Notices of the Royal Astronomical Society

Lozinskaya

2012

We present the results of an ionized gas turbulent motions study in several nearby dwarf galaxies using a scanning Fabry–Perot interferometer with the 6‐m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS). Combining the ‘intensity–velocity dispersion’ diagrams () with two‐dimensional maps of radial velocity dispersion, we found a number of common patterns pointing to the relation between the value of chaotic ionized gas motions and processes of current star formation. In five out of the seven analysed galaxies, we identified expanding shells of ionized gas with diameters of 80–350 pc and kinematic ages of 1–4 Myr. We also demonstrate that the diagrams may be useful for the search of supernova remnants, other small expanding shells or unique stars in nearby galaxies. As an example, a candidate luminous blue variable (LBV) was found in UGC 8508. We propose some additions to the interpretation, previously used by Muñoz‐Tuñón et al. to explain the diagrams for giant star formation regions. In the case of dwarf galaxies, a major part of the regions with high velocity dispersion belongs to the diffuse low surface brightness emission, surrounding the star‐forming regions. We attribute this to the presence of perturbed low‐density gas with high values of turbulent velocities around the giant H ii regions.

Section: Introductionmentioning

confidence: 99%

Ionized gas velocity dispersion in nearby dwarf galaxies: looking at supersonic turbulent motions★

Monthly Notices of the Royal Astronomical Society

Lozinskaya

2012

“…The two cubes are then combined into one and spectra of masked regions in each cube are substituted by the corresponding "good" spectra from the other data set. One of the best examples of application of the above algorithm is the reduction of observations of the nearby dwarf galaxy IC 10 reported by Lozinskaya et al (2008). Here the image of emission shells of ionized gas occupies more than half of the entire field of view of SCORPIO instrument.…”

Section: Ghosts Subtractionmentioning

confidence: 99%

Reduction of CCD observations made with the Fabry-Perot scanning interferometer. II. Additional procedures

Egorov

2008

Astrophys. Bull.

Self Cite

Abstract. We describe a software package used at the Special Astrophysical Observatory of the Russian Academy of Sciences to reduce and analyze the data obtained with the Fabry-Perot scanning interferometer. We already described most of the algorithms employed in our earlier Paper I (Moiseev, 2002). In this paper we focus on extra procedures required in the case of the use of a high-resolution Fabry-Perot interferometer: removal of ghosts and measurement of the velocity dispersion of ionized gas in galactic and extragalactic objects.

“…We observed the ionized gas in the synchrotron superbubble region with the SAO RAS 6‐m telescope using the SCORPIO focal reducer (Afanasiev & Moiseev 2005) operating in three modes: direct [S ii ] line images, long‐slit spectroscopy, and observations with a scanning Fabry–Perot interferometer (FPI) in the Hα line. We report the detailed results of our observations in a separate paper (Lozinskaya et al 2007). In this Letter we summarize the main results of these observations and the ensuing conclusions.…”

Section: Results Of Observationsmentioning

confidence: 98%

A synchrotron superbubble in the IC 10 galaxy: a hypernova remnant?

Lozinskaya¹,

Monthly Notices of the Royal Astronomical Society: Letters

2007

Self Cite

The nature of the synchrotron superbubble in the IC 10 galaxy is discussed using the results of our investigation of its ionized gas structure, kinematics and emission spectrum from observations made with the 6‐m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences, and based on our analysis of the radio emission of the region. The hypernova explosion is shown to be a more plausible mechanism of formation of the synchrotron superbubble compared with the earlier proposed model of multiple supernova explosions. A compact remnant of this hypernova may be identified with the well‐known X‐ray binary X‐1 – an accreting black hole.