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7.1 HST WFPC2 Image

The HST WFPC2 image on which the simulations presented in this Chapter are based is a Planetary Camera (PC, see Section 6.1) image of the central regions of the M100 spiral galaxy, obtained with a 900 s exposure with the F555W filter. This image was chosen because it contains most interesting features one would like to observe in bright galaxies: a conspicuous core, large surface brightness variations on short space scales, spiral arms and HII regions7.1. The central part of this image, namely a square of about 16 arcsec side whose flux map was reconstructed from the simulated observations, is shown in Figure 7.1.

Figure 7.1: HST WFPC2 PC image of M100. Central part of a WFPC2 PC image of the spiral galaxy M100, obtained with a 900 s exposure with the F555W filter, similar to $ V$. Encircled on the right image is the position of the eight zones used to calculate the median surface brightness in Table 7.1 (letters $ a$-$ h$) and of the five HII regions of which aperture photometry is carried out in Section 7.7 (numbers 1-5). The image side is about 16 arcsec and the circles have a diameter of about 0.7 arcsec.
\begin{figure}\begin{center}
\mbox{
\hspace{-0.02\textwidth}
\subfigure{\epsfig{...
...es/m100_hst_small_ann.eps,
width=0.435449\textwidth}}}
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The median surface brightness in $ V$ inside the eight circles marked by letters is given in Table 7.1. These values were calculated following the WFPC2 photometric calibration obtained by [Holtzman et al. 1995b], and indicate the surface brightness range spanned by the image. Note that the median surface brightness of the whole image is $ \mu_V=19.42$ mag/arcsec$ ^2$.

Table 7.1: Characteristic values of $ V$-band surface brightness of the HST image of M100. Median $ V$-band surface brightness within the zones indicated in Figure 7.1, expressed in mag/arcsec$ ^2$.
Zone $ a$ $ b$ $ c$ $ d$ $ e$ $ f$ $ g$ $ h$
Median $ \mu_V$ 19.10 20.65 20.71 18.96 17.83 18.35 17.59 16.80

M100 is classified as Sc(s)I in [Sandage and Bedke 1994] and the [de Vaucouleurs et al. 1991] report a photoelectric total magnitude $ B_T=10.05$ and an effective radius of about 104 arcsec, meaning that the sky region shown in Figure 7.1 covers its very central parts only.


next up previous contents
Next: 7.2 GAIA BBP Flux Up: 7. A Case Study: Previous: 7. A Case Study:   Contents
Mattia Vaccari 2000-12-05