SPHEREx: Aromatics, Aliphatics and PAH Size across the Iris Nebula

Abstract

Observations by the SpectroPhotometer for the History of the Universe, Epoch of Reionization, and Ices Explorer (SPHEREx) are combined with Spitzer spectral map data to study the aromatic, aliphatic, and PAH size evolution across the northwest photo-dissociation region (PDR) of the Iris Nebula (NGC7023). The 3.3-3.4 $\mu$m complex (I${}_{3.3}$) and 11.2 $\mu$m (I${}_{11.2}$) PAH band strength are determined through direct integration. In addition, the former is decomposed into a 3.3 (I'${}_{3.3}$) and 3.4 $\mu$m (I'${}_{3.4}$) sub-feature by fitting SPHEREx bandpass-integrated photometry using a modeled, highly sampled, multi-component spectrum. I${}_{3.3}$, I${}_{11.2}$, I'${}_{3.3}$, and I'${}_{3.4}$ all peak at the PDR. The NASA Ames PAH IR Spectroscopic Database is used to obtain the average number of carbon atoms ($\overline{{\mathrm{N}}_{\mathrm{C}}}$) and small PAH fraction ($f_{\mathrm{small}}$) by fitting the isolated PAH component of the Spitzer segment; $70\lesssim \overline{N_C}\lesssim 76$ and $0.24\lesssim {\text{f}}_{\mathrm{small}}\lesssim 0.36$. I'${}_{3.4}$/I'${}_{3.4}$, I${}_{11.2}$/I${}_{3.3}$, $\overline{{\mathrm{N}}_{\mathrm{C}}}$, and $f_{\mathrm{small}}$ all show a demarcation that matches the large-scale morphology of the region. For I'${}_{3.3}$ and I'${}_{3.4}$ this is reflected by two distinct trends when plotted against each other, one associated with the dense, the other with the diffuse medium; $[N_{\mathrm{H},\mathrm{ali}}/N_{\mathrm{H},\mathrm{aro}}{]}_{\mathrm{dense}}$ = 0.42$\pm$0.01 and $[N_{\mathrm{H},\mathrm{ali}}/N_{\mathrm{H},\mathrm{aro}}{]}_{\mathrm{diffuse}}$ = 0.10$\pm$0.01. $\overline{{\mathrm{N}}_{\mathrm{C}}}$ and $f_{\mathrm{small}}$ are tentatively correlated with I${}_{11.2}$/I${}_{3.3}$ (R=0.54$\pm$0.05 and -0.45$\pm$0.05, respectively). A wider variety of large(r) extended interstellar medium objects is required to tighten the correlations, turn them into quantitative calibrators for PAH size, and pin down the discrepancy of correlations with I'${}_{3.3}$ involved.

arXiv comment17 pages, 11 figures, accepted for publication in The Astrophysical Journal

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