SL and LL visualizations 1 15 Jan 2004

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

2 15 Jan 2004 SINGS Tucson Meeting - DAD

SL S/N 3 15 Jan 2004 SINGS Tucson Meeting - DAD

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

SH lines 5 15 Jan 2004 SINGS Tucson Meeting - DAD

LH lines 6 15 Jan 2004 SINGS Tucson Meeting - DAD

LH lines 7 15 Jan 2004 SINGS Tucson Meeting - DAD

LL cut 8 15 Jan 2004 SINGS Tucson Meeting - DAD

IRS sensitivity 9 15 Jan 2004 SINGS Tucson Meeting - DAD

10 15 Jan 2004 SINGS Tucson Meeting - DAD

LL Simulations I've taken the ISO 7 and 15 micron maps for N 6946, and used my SED models, to predict the surface brightness at IRS LL wavelengths. The first plot displays the (S/N) spectra from the 11 x 79 different 4. 8" pixels that lie within the 1'x 6. 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 (1 sigma sensitivity). 11 15 Jan 2004 SINGS Tucson Meeting - DAD

LL Simulations The second plot displays the (S/N) spectra you would get if binning was carried out 2 x 2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28. 0 microns). The lines represent spectra from 5 x 39 different 9. 6" pixels that lie with the strip. 12 15 Jan 2004 SINGS Tucson Meeting - DAD

MIPS SED Simulations I've taken the ISO 7 and 15 micron maps for N 6946, and used my SED models, to predict the surface brightness at MIPS SED wavelengths. The first plot displays the (S/N) spectra from the 6 x 43 different 9. 9" pixels that lie within the 1'x 7' 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. 13 15 Jan 2004 SINGS Tucson Meeting - DAD

LL Simulations The second plot displays the (S/N) spectra you would get if binning was carried out 2 x 2 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 3 x 22 different 19. 8" pixels that lie with the strip. I am assuming the conservative end of Chad's recent sensitivity range is applicable: 3 sigma=36 -45 m. Jy (3 sigma=3. 2 MJy/sr). 14 15 Jan 2004 SINGS Tucson Meeting - DAD

LL Simulations The second plot displays the (S/N) spectra you would get if binning was carried out 2 x 2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28. 0 microns). The lines represent spectra from 5 x 39 different 9. 6" pixels that lie with the strip. 15 15 Jan 2004 SINGS Tucson Meeting - DAD

LL Simulations The second plot displays the (S/N) spectra you would get if binning was carried out 2 x 2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28. 0 microns). The lines represent spectra from 5 x 39 different 9. 6" pixels that lie with the strip. 16 15 Jan 2004 SINGS Tucson Meeting - DAD

MIPS SED Simulations The second plot displays the (S/N) spectra you would get if binning was carried out 2 x 2 spatially, and collapsing spectrally by combining five spectral elements into one (see example image at 28. 0 microns). The lines represent spectra from 5 x 39 different 9. 6" pixels that lie with the strip. 17 15 Jan 2004 SINGS Tucson Meeting - DAD