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Astron. Astrophys. 358, 812-818 (2000)

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2. NGC 5668: general properties

NGC 5668 is a nearly face-on (inclination [FORMULA]) late type spiral galaxy (Sc(s) II-III). A wide band optical image of the galaxy can be seen in Fig. 1  1. We will adopt a distance of 22.6 Mpc, consistent with [FORMULA]. Its size (the blue isophote at 25 mag/arcsec is 3.3 arcmin in diameter) makes it an ideal target for observation with TAURUS II (which has a FOV of about 5 arcmin)). The measured radial scale length for NGC 5668 is 27.3 arcsec, which means that our observations reach up to around 4.4 scale lengths. The FIR and [FORMULA] luminosities of NGC 5668 (S96) show that it has an important amount of star formation. A summary of its main properties is shown in Table 1.

[FIGURE] Fig. 1. Optical image of NGC 5668


[TABLE]

Table 1. Galaxy properties


NGC 5668 was observed in the HI line by means of the Arecibo telescope by Schulman et al. (1994). They detected high velocity wings in the line shape, which were attributed to HVC's in the galaxy. As the Arecibo observations did not contain information on the spatial distribution of gas, subsequent observations were taken with the VLA telescope by S96. These observations confirmed the existence of the HVC's. They found that the amount of mass on neutral hydrogen in HVC's is about [FORMULA]. Their observations lacked sufficient spatial resolution (the FWHM of the synthesized beam was [FORMULA]) to detect the shells or chimneys in the disk that could be the origin of this large amount of gas in high velocity components. The main purpose of this paper is to try to detect such features by means of Fabry-Perot spectroscopy.

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© European Southern Observatory (ESO) 2000

Online publication: June 20, 2000
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