to the fact that the source is slightly extended for the SL and SH apertures ($3.7^{\prime\prime}$ and $4.7^{\prime\prime}$ height respectively), while it is point-like for the LL and LH apertures ($\approx11^{\prime\prime}$). Another factor of $1.15$ was applied to the low-resolution spectra to match the continuum of the high-resolution. The final rest-frame spectrum is displayed in Figure \[fig:irs\_spec\] ([*top*]{}), with a zoom on individual spectral lines ([*bottom*]{}). With a spectral resolution $\ge$500 km s$^{-1}$, the lines are not spectrally resolved.

Line fitting and flux measurements were also done in SMART. A Gaussian and second order polynomial function were fitted to the line and continuum. For total uncertainties, we added 10% of the line flux due to calibration uncertainties. The resulting fluxes and uncertainties of the most prominent lines are listed in Table \[table:lines\]. The fluxes agree within the uncertainties to those of [@wu-2006]. The \[Ne [iii]{}\] line at 36.0 $\mu$m was not observed as it falls out of the IRS spectral range.

![image](19818f03){width="17cm"} ![image](19818f04){width="17cm"}

[*Herschel*]{} data {#sect:pacs}
-------------------

Haro11 was observed with the [PACS]{} spectrometer [@poglitsch-2010] on the 27th of June 2010, OD 409 of the [*Herschel*]{} mission [@pilbratt-2010] as part of the Guaranteed Time Key Program, the Dwarf Galaxy Survey 