ISOGAL Survey of Baade’s Windows in the Mid-infrared

The ISOGAL mid-infrared survey of areas close to the Galactic Plane aims to determine their stellar content and its possible bearing on the history of the Galaxy. The NGC6522 and Sgr I Baade’s Windows of low obscuration towards the inner parts of the Bulge represent ideal places in which to calibrate and understand the ISOGAL colour-magnitude diagrams, which are more difficult to interpret in heavily reddened fields. The survey observations were made with the ISOCAM instrument of the ISO satellite. The filter bands chosen were LW2 (∼7μm) and LW3 (∼15μm). The results presented here show that most of the detected objects are late M-type giants on the AGB, with a cut-off for those earlier than M3–M4. The most luminous members of these two Bulge fields at 7μm are the Mira variables. However, it is evident that they represent the end of a sequence of increasing 15μm dust emission which commences with M giants of earlier sub-type. In observations of late-type giants the ISOCAM 15μm band is mainly sensitive to the cool silicate or aluminate dust shells which overwhelm the photospheric emission. However, in ordinary M-giant stars, the 7μm band is not strongly affected by dust emission and may be influenced instead by absorption. The ν2 band of water at 6.25μm and the SiO fundamental at 7.9μm are likely contributors to this effect. Miras are more luminous at 7μm and have redder K0–[7] colours than other M giants. Their [7]–[15] colours are consequently bluer than might be expected by extrapolating from warmer M-giants. A group of late M stars has been found which vary little or not at all but have infrared colours typical of well-developed dust shells. Their luminosities are similar to those of 200–300 day Miras but they have slightly redder [7]–[15] colours which form an extension of the ordinary M giant sequence. They may belong to the class of red semi-regular variables. The Mira dust shells show a mid-infrared [7]–[15] colour-period relation. In these two fields there is no component of high-luminosity late-type variables obscured at K and shorter wavelengths such as is seen in the Magellanic Clouds. The upper limit of LPV periods in these fields remains at ca 700 days.