This is the 60µm IRAS image.
You may also see images at other wavelengths by clicking on the colorbar at a point above any of the dashed arrows (which point to other regions of the spectrum at which images are available). The solid arrow shows the spectral region you are seeing now. This is not intended to be a linear scale in wavelength, but only a rough guide to the wavelength of the observation.
This heavily embedded aggregate in the L1641 Center region is the location of a powerful molecular outflow (Fukui et al. 1986). This group was studied photometrically by Chen et al. (1993) and is extremely young as shown by the luminosity function (Strom, Strom & Merrill (1993). Many of the stars in this cluster suffer enormous extinctions (>30 magnitude). Few are seen in the visible.
This mid-infrared pseudocolor image was made using a color map having white is the brightest, then blue, green, yellow, red and black at the faint end, to display the intensity of each pixel. Note that the star seen on the edge of the near infrared image is no longer visible. The strongest source in the field at 60µm corresponds to a group of stars just becoming visible at 2µm and seen as very red faint stars in the near infrared image. The strong molecular outflow in this field is centered in this group.
If you wish more information about these images, a page is available for your perusal. You may also return to the overview page.
Chen, H., Tokunaga, A.T., Strom, K.M. & Hodapp, K.-W. 1993, ApJ, 407, 639
Fukui,Y. et al. 1986, ApJ Letters, 311, L85
Strom, K.M., Strom, S.E. & Merrill, K.M. 1993, ApJ, 412, 233