1. 15 Jan 2004 SINGS Tucson Meeting - DAD 1 SL and LL visualizations

2. 15 Jan 2004 SINGS Tucson Meeting - DAD 2

3. 3 SL S/N

4. 15 Jan 2004 SINGS Tucson Meeting - DAD 4 SL S/N

5. 15 Jan 2004 SINGS Tucson Meeting - DAD 5 SH lines

6. 15 Jan 2004 SINGS Tucson Meeting - DAD 6 LH lines

7. 15 Jan 2004 SINGS Tucson Meeting - DAD 7 LH lines

8. 15 Jan 2004 SINGS Tucson Meeting - DAD 8 LL cut

9. 15 Jan 2004 SINGS Tucson Meeting - DAD 9 IRS sensitivity

10. 15 Jan 2004 SINGS Tucson Meeting - DAD 10

11. LL Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 11 I've taken the ISO 7 and 15 micron maps for N6946, and used my SED models, to predict the surface brightness at IRS LL wavelengths. The first plot displays the (S/N) spectra from the 11x79 different 4.8" pixels that lie within the 1'x6.4' IRS SED strip (see example image at 27.0 microns). The largest-valued spectra come from the nucleus, whereas the weakest spectra represent the fainter disk. I am assuming the pre-flight sensitivity is applicable (1sigma sensitivity).

12. LL Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 12 The second plot displays the (S/N) spectra you would get if binning was carried out 2x2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28.0 microns). The lines represent spectra from 5x39 different 9.6" pixels that lie with the strip.

13. MIPS SED Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 13 I've taken the ISO 7 and 15 micron maps for N6946, and used my SED models, to predict the surface brightness at MIPS SED wavelengths. The first plot displays the (S/N) spectra from the 6x43 different 9.9" pixels that lie within the 1'x7' MIPS SED strip (see example image at 75.4 microns). The largest-valued spectra come from the nucleus, whereas the weakest spectra represent the fainter disk.

14. LL Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 14 The second plot displays the (S/N) spectra you would get if binning was carried out 2x2 spatially, and collapsing spectrally by combining five 1.7 micron pixels into 8.5 micron pixels (see example image at 75.4 microns). The lines represent spectra from 3x22 different 19.8" pixels that lie with the strip. I am assuming the conservative end of Chad's recent sensitivity range is applicable: 3sigma=36-45 mJy (3sigma=3.2 MJy/sr).

15. LL Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 15 The second plot displays the (S/N) spectra you would get if binning was carried out 2x2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28.0 microns). The lines represent spectra from 5x39 different 9.6" pixels that lie with the strip.

16. LL Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 16 The second plot displays the (S/N) spectra you would get if binning was carried out 2x2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28.0 microns). The lines represent spectra from 5x39 different 9.6" pixels that lie with the strip.

17. MIPS SED Simulations 15 Jan 2004 SINGS Tucson Meeting - DAD 17 The second plot displays the (S/N) spectra you would get if binning was carried out 2x2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28.0 microns). The lines represent spectra from 5x39 different 9.6" pixels that lie with the strip.