Context : Sh2-104 is a Galactic H ii region with a bubble morphology , detected at optical and radio wavelengths .
It is considered the first observational confirmation of the collect-and-collapse model of triggered star-formation .

Aims : We aim to analyze the dust and gas properties of the Sh2-104 region to better constrain its effect on local future generations of stars .
In addition , we investigate the relationship between the dust emissivity index \beta and the dust temperature , T _ { dust } .

Methods : Using Herschel PACS and SPIRE images at 100 , 160 , 250 , 350 and 500 \mu m we determine T _ { dust } and \beta throughout Sh2-104 , fitting the spectral energy distributions ( SEDs ) obtained from aperture photometry .
With the SPIRE Fourier transform spectrometer ( FTS ) we obtained spectra at different positions in the Sh2-104 region .
We detect J -ladders of ^ { 12 } CO and ^ { 13 } CO , with which we derive the gas temperature and column density .
We also detect proxies of ionizing flux as the [ N ii ] ^ { 3 } P _ { 1 } - ^ { 3 } P _ { 0 } and [ C i ] ^ { 3 } P _ { 2 } - ^ { 3 } P _ { 1 } transitions .

Results : We find an average value of \beta \sim 1.5 throughout Sh2-104 , as well as a T _ { dust } difference between the photodissociation region ( PDR , \sim 25 K ) and the interior ( \sim 40 K ) of the bubble .
We recover the anti-correlation between \beta and dust temperature reported numerous times in the literature .
The relative isotopologue abundances of CO appear to be enhanced above the standard ISM values , but the obtained value is very preliminary and is still affected by large uncertainties .

Conclusions :