Planetary nebulae: Multiwavelength probes of stellar and galactic evolution Proceedings IAU Symposium No. 323, 2016 (cid:13)c 2016InternationalAstronomicalUnion X. Liu, L. Stanghellini, & A. Karakas, eds. DOI:00.0000/X000000000000000X Herschel observations of planetary nebulae † Griet C. Van de Steene1 1 Royal Observatory of Belgium, Department Astronomy and Astrophysics Ringlaan 3, BE-1180, Brussels, Belgium email: [email protected] Abstract. This article presents an overview of the published results for planetary nebulae basedonimagesandspectroscopyfromthePACS,SPIRE,andHIFIinstrumentsonboardthe Herschel satellite. 7 Keywords. ISM: abundances, atoms, dust, globules, molecules, planetary nebulae: general, 1 infrared: ISM, stars: circumstellar matter 0 2 n a 1. Introduction J 4 Grains play an important role in many environments, including planetary nebulae 2 (PNe), because of extinction, photoelectric heating, their influence on the charge and ionization balance of the gas, as catalysts for grain-surface chemical reactions and as ] R seeds for freeze-out of molecules. Previous satellite missions such as IRAS, ISO, Spitzer, S and AKARI have allowed us to study the dust in PNe, but unfortunately the angular . resolution of these instruments was too low to get detailed information on the spatial h distribution of the dust. This has changed with the Herschel satellite, which has allowed p - us to study the spatial structures in unprecedented detail. o r t s a 2. Herschel and its instruments [ The Herschel Space Observatory (Pilbratt et al. 2010) was launched on May 14 2009 1 andoperatedfornearlyfouryears.Itcarriedthelargest,mostpowerfulinfraredtelescope v ever flown in space and three sensitive scientific instruments. Herschels observations 7 finished on April 29 2014 when the tank of liquid helium used to cool the instruments 9 finally ran dry. 7 6 Thethreeinstrumentsonboardwere:PACS(PhotoconductorArrayCameraandSpec- 0 trometer),SPIRE(SpectralandPhotometricImagingREceiver),andHIFI(Heterodyne . InstrumentfortheFarInfrared),ahigh-resolutionspectrometer.Theseinstrumentswere 1 0 designed for deep, wideband photometry with high spatial resolution and full spectral 7 coverage,makingHerschelthefirstspacefacilitytocompletelycoverthefarinfraredand 1 submillimeter range from 55 to 672µm. : v PACS (Photodetecting Array Camera and Spectrometer) (Poglitsch et al. 2010) was i an imaging camera and low-resolution spectrometer covering wavelengths from 55 to X 210µm. The spectrometer had a spectral resolution between R=1000 and R=5000. It r a operatedasanintegralfieldspectrograph,combiningspatialandspectralresolution.The imaging camera was able to image simultaneously in two bands (either 60 − 85 / 85 − 130µm and 130 − 210µm) with a detection limit of a few mJy. † Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. 1 2 G. C. Van de Steene SPIRE(SpectralandPhotometricImagingReceiver)(Griffinetal.2010)wasanimag- ing camera and low-resolution spectrometer covering 194 to 672µm wavelength. The spectrometer had a resolution between R=40 and R=1000 at a wavelength of 250µm and was able to image point sources with brightnesses around 100mJy and extended sources with brightnesses of around 500mJy. The imaging camera observed simultane- ously in three bands, centred at 250, 350 and 500µm, each with 139, 88 and 43 pixels respectively. It was able to detect point sources with brightness above 2mJy. HIFI (Heterodyne Instrument for the Far Infrared) (de Grauw et al. 2010) is a hetero- dyne detector able to electronically separate radiation of different wavelengths, giving a spectralresolutionuptoR=107 .Thespectrometerwasoperatedwithintwowavelength bands, from 157 to 212µm and from 240 to 625µm. 3. PACS and SPIRE imaging results The extended circumstellar envelopes of evolved low-mass AGB stars display a large variety of morphologies. Understanding the various mechanisms that give rise to these extended structures is important to trace their mass-loss history. The data presented by Cox et al. (2012) showed for the first time the variety of interaction between the circumstellar shell and the interstellar medium, which can be divided in roughly four categories: “fermata”, “eyes”, “irregular”, and “rings”. In particular the star’s peculiar spacevelocityandthedensityoftheISMappeardecisiveindetectingemissionfrombow shocks or detached rings. Tentatively, the ”eyes” class objects are associated to (visual) binaries, while the ”rings” generally do not appear to occur for M-type stars, only for C or S-type objects that have experienced a thermal pulse. The occurrence of the observed eye-shapeofAGBdetachedshellsismoststronglyinfluencedbytheinterstellarmagnetic field, the stellar space motion, and density of the interstellar medium (van Marle et al. 2014). Observability of this transient phase is favoured for lines-of-sight perpendicular to the interstellar magnetic field direction. The simulations of van Marle et al. (2014) indicatethatsuch“eye”shapesofsuchpre-PNcircumstellarshellcanstronglyaffectthe shape and size of PNe. A total of 18 well known PNe have been imaged with PACS and SPIRE instruments in the framework of MESS and HerPlans programs. Seven PNe (NGC 6720, NGC 650, NGC 7293, NGC 6853, NGC 3587, NGC 7027) were imaged by the MESS team. Mass loss of Evolved StarS (MESS) was a Guarenteed Time Key Programmes to study the circumstellar environment of evolved post main sequence stars. A detailed description of the program can be found in Groenewegen et al. (2011). An overview of the Herschel observationsofPNeintheMESSprogramwaspresentedinvanHoofetal.(2012).Eleven PNe (NGC 40, NGC 2392, NGC 3242, NGC 6445, NGC 6543, NGC 6720, NGC 6781, NGC 6826, NGC 7009, NGC 7026, Mz 3) have been observed in the Herschel Planetary Nebulae Survey (HerPlanS). A data overview and first analysis was presented in Ueta et al. (2014). HerPlaNS obtained far-infrared broadband images and spectra of eleven well- known PNe with the PACS and SPIRE instruments. The target PNe all have distances less than ∼1.5 kpc and are dominated by relatively high-excitation nebulae as they were selected from the Chandra Planetary Nebula Survey (ChanPlaNS; Kastner et al. 2012) Herschel PACS and SPIRE imaging showed that the dust emission in PNe has a very clumpy structure for all nebula. There is excellent agreement between the H images of 2 and the PACS 70µm maps. For the Ring nebula (NGC6720) it appears to be the first observational evidence that H forms on oxygen rich dust grains. van Hoof et al. (2010) 2 developedaphotoionisationmodeloftheRingnebulawithCloudytoinvestigatepossible formation scenarios for H . They concluded that the most plausible scenario is that the 2 Herschel observations of PNe 3 H resides in high density knots which were formed after the recombination of the gas 2 started, when the central star luminosity dropped steeply after the central star entered the cooling track. H formation may still be ongoing at this moment, depending on the 2 density of the knots and the properties of the grains in the knots (van Hoof et al. 2010). This is also a possible scenario for the formation of high density clumps in other evolved nebula with a central star on the cooling track such as the Helix (NGC 7293) and the Dumbell (NGC 6853). Comparison between the 70µm Herschel and corresponding optical maps showed that they are very similar indicating that there is a very steep temperature gradient from theionizedregiontothedustyphotodissociationregion.ForNGC6781thePACS70µm map, showing the distribution of thermal dust continuum is very similar to what is seen in the [Nii]λ658.4 nm image (Ueta et al. 2014). For the Helix it was also observed and shown that the radiation field decreases rapidly outwards through the barrel wall (Fig. 9, Van de Steene et al. 2015). Previous knowledge of the 3D structure of the nebula is extremely useful to correctly interpretthefarinfraredimages.Forinstance,thePACSandSPIREimagesoftheHelix nebulacouldbeunderstoodbasedonthekinematicmodelofZeigleretal.(2013)andthe Herschel images of NGC 6781 with the 3D model of Schwarz & Monteiro (2006). Both show bipolar, barrel-like structures inclined to the line of sight, a frequent morphology in PNe. Herschel PACS imaging photometry was obtained for these 17 different PNe in the MESS and HerPlanS projects (van Hoof et al. 2010, van Hoof et al. 2013, Van de Steene et al. 2015,Van de Steene et al. in preparation, Ueta et al. 2014, Ueta et al. in prepa- ration) with the PACS and SPIRE instruments at 70, 160, 250, 350, and 500µm. This photometry was complemented with photometry obtained from the literature at many otherwavelengthsfromtheUVtoradiowavelengthstoconstructfullSEDs.Themodified blackbodyfittotheseSEDsrevealedthattheemissionfactorβ isalwayscloseto1.0,in- dicating that the dust grains are mainly amorphous carbon (Menella et al. 1995, Boudet et al. 2005). The fit to the SED also showed that the flux emitted in the far infrared is significant: without far-IR data fitting constraints the dust mass gets underestimated by 40%. The dust temperature obtained from the SED fits and the temperature maps made, showed that the cool dust temperature of the PNe is around 30 to 100K. For the He- lix nebula the gas kinetic temperature T was determined to be about 20 to 40 K k (Zack & Ziurys 2013, Etxaluze et al. 2014), which is similar the Helix’ dust tempera- ture (Van de Steene et al. 2015). The gas density of the H cometary globules is on 2 the order of n(H )∼(15)105cm−3. Goldsmith (2001) found that for gas densities higher 2 than 104.5cm−3 the dust and gas temperatures will be closely coupled, also for the dust temperatures determined for the Helix nebula. The dust masses found so far for NGC6781, NGC7293, and NGC650 are all a few thousandthsofsolarmasses.Byintegratingovertheentirenebula,thedustcolumnmass density map the total mass of far emitting dust mass was determined to be 4x10−3M (cid:12) forNGC6781atadistanceof950pcand3.5x10−3M fortheHelixnebulaatdistanceof (cid:12) 216pc, while for NGC 650 the dust mass is about 1.4x10−3M at a distance of 1200pc (cid:12) based on Cloudy modeling (Ueta et al. 2014, Van de Steene et al. 2015, van Hoof et al. 2013) One of the goals of HerPlaNS is to empirically obtain spatially resolved gas-to-dust massratiodistributionmapsbyderivingboththedustandgascolumnmassdistribution maps directly from observational data. For NGC6781 direct comparison of the dust and gas column mass maps constrained data allowed to construct an empirical gas-to-dust 4 G. C. Van de Steene mass ratio map, which showed a large range of ratios with the median of 195±110 and hence,isgenerallyconsistentwiththetypicalspatially-unresolvedratiobetween100and 400 widely used in the literature for the case of PNe and AGB stars (Ueta et al. 2014). The MESS and HerPlaNS teams have collected not only photometry, but also other spectroscopicdatafromtheliteratureoverthewholespectralrangefromX-raystoradio to make the most comprehensive Cloudy models ever made of NGC650 (van Hoof et al. 2013) and NGC6781 (M. Otsuki, this volume). For NGC 650 the Cloudy model showedthatthegrainsintheionizednebulaarelarge(assumingsingle-sizedgrains,they would have a radius of 0.15 µm). Most likely these large grains were inherited from the asymptotic giant branch phase. However the PACS 70/160µm temperature map showed evidence of two radiation components heating the grains. The first component is direct emission from the central star, while the second component is diffuse emission from the ionized gas (mainly Lyα). Unlike what was thought before, the neutral material resides in dense clumps inside the ionized region. These may also harbour stochastically heated verysmallgrainsinadditiontothelargegrains.Thisisunusualforsuchahighlyevolved PN. In the past, far-IR SED fitting with broadband fluxes were performed under the as- sumption of negligible line contamination. With the Herschel data and Cloudy modeling weverifiedthatthedegreeoflinecontaminationisapproximately820%(Uetaetal.2014, van Hoof et al. 2013) and does not significantly affect the fitting results. 4. PACS and SPIRE spectroscopic results 4.1. NGC 6781 The Herschel spectra obtained at various locations within NGC6781 revealed both the physical and chemical nature of the nebula. The spectra showed a number of ionic and atomic lines such as [Oiii]52, 88µm, [Niii]57µm, [Nii]122, 205µm, [Cii]158µm, and [Oi]63, 146µm, as well as various molecular lines, in particular, high-J CO rotational transitions, OH, and OH+ emission lines. Thermal dust continuum emission was also detected in most bands in these deep exposure spectra. On average, the relative distri- butions of emission lines of various nature suggested that the barrel cavity in NGC6781 is uniformly highly ionized, with a region of lower ionization delineating the inner sur- face of the barrel wall. The least ionic and atomic gas, molecular, and dust species are concentrated in the cylindrical barrel structure. Based on the PACS IFU spectral cube data, Ueta et al. (2014) derived line maps in the detected ionic and atomic fine-structure lines. Next diagnostics of the electron temperatureanddensityusinglineratiossuchas[Oiii]52/88µmand[Nii]122/205µm, resulted in (T , n ) and ionic/elemental/relative abundance profiles for the first time in e e the far-IR for any PN. The derived T profile substantiated the typical assumption of e uniform T = 104K in the main ionized region, while showing an interesting increase in e the barrel (up to 10% higher), followed by a sudden tapering off toward the halo region. Then profileofhigh-excitationspeciesisnearlyflatacrosstheinnercavityofthenebula, e whereas the n profile of low excitation species exhibits a radially increasing tendency e with a somewhat complex variation around the barrel wall. In fact, this n [Nii] profile e is reflected in the physical stratification of the nebula revealed by the ionic/elemental abundanceanalysis.Thedetectedstratificationisconsistentwiththepreviousinferences madefromthepastopticalimagingobservationsinvariousemissionlinesofvaryinglevels of excitation. The derived relative elemental abundance profiles showed uniformly low N and C abundances, confirming the low initial mass (< 2 M ) and marginally carbon- (cid:12) Herschel observations of PNe 5 rich nature of the central star. However, the profiles did not appear to reveal variations reflectingtheevolutionarychangeofthecentralstar,suchasaradiallyincreasingcarbon abundance. 4.2. SPIRE spectroscopy: OH+ and CO (b) SPIRE 250µm image and spectrum of molecules in the Helix nebula NGC7293. (a) SPIRE and PACS spectra of molecules in the Ring nebula NGC6720. Figure 1: Herschel spectra of molecules in the Ring and Helix nebula Etxaluzeetal.(2014)andAlemanetal.(2014)reportedthefirstdetectionofextended OH+linesinemissionin5PNeobservedaspartoftheHerPlansinNGC6445,NGC6720 (Fig.1a),andNGC6781andMESSinNGC7293(Fig.1b).AlsoNGC6853showsOH+ in emission (Van de Steene et al., in preparation). All five PNe are molecule rich, with dense clumpy structures and hot central stars (Teff > 100000K). The OH+ emission is most likely due to excitation in a photodissociation region. Although other factors such as high density and low C/O ratio may also play a role in the enhancement of the OH+ emission. The fact that OH+ is not detected in objects with T < 100000 K suggests eff thatthehardnessoftheionisingcentralstarspectracouldbeanimportantfactorinthe production of OH+ emission in PNe. The Herschel spectra towards the Helix nebula also show, besides OH+, CO emission lines (from J = 4 to 8), [Nii] at 1461 GHz from ionized gas, and [Ci] (3P −3P ). The 2 1 SPIRE spectral maps suggest that CO arises from dense and shielded clumps in the western rims of the Helix nebula, whereas OH+ and [Ci] lines trace the diffuse gas and the UV and X-ray illuminated clump surfaces where molecules reform after CO photodissociation. The [Nii] line traces a more diffuse ionized gas component in the interclump medium (Etxaluze et al. 2014). 6 G. C. Van de Steene For NGC 6781 the CO observations and analysis with higher-J transitions sampled much warmer CO gas component in the cylindrical barrel structure, probably located closer to the equatorial region along the line of sight, compared with the previous CO measurements and diagnostics by Bachiller et al. (1993). However, the amount of this warm component was determined to be an order of magnitude smaller than the cold component (Ueta et al. 2014). 4.3. Crystalline olivine Blommaert at al. (2014) (GT1 ”Forsterite dust in the circumstellar environment of evolved stars”) presented 48 PACS spectra of evolved stars in the wavelength range of 67−72µm,coveringthe69µmbandofcrystallineolivine(Mg Fe( SiO ).For27ob- 22x 2x) 4 jectsinthesample,theydetectedthe69µmbandofcrystallineolivine(Mg Fe SiO ). (22x) (2x) 4 The 69µm band showed that all the sources produce pure forsterite grains containing no iron in their lattice structure. They fit the 69µm band and used its width and wave- length position to probe the composition and temperature of the crystalline olivine. The fits showed that on average the temperature of the crystalline olivine is highest in the groupofOH/IRstarsandthepost-AGBstarswithconfirmedKepleriandisks.Thetem- perature is lower for the other post-AGB stars and lowest for the PNe. A couple of the detected 69µm bands are broader than those of pure magnesium-rich crystalline olivine, which can be due to a temperature gradient in the circumstellar environment of these stars. 5. HIFI 5.1. HIFISTARS TheHerschelguaranteedtimekeyprogrammeHIFISTARS(Bujarrabaletal.2012)aimed to study the physical conditions, particularly the excitation state, of the intermediate- temperature gas in proto-PNe and young PNe. The information that the observations of the different components deliver is of particular importance for the wind-shock inter- action and hence the understanding the evolution and shaping of PNe. They performed Herschel/HIFI observations of intermediate-excitation molecular lines in the far-infrared range of a sample of ten nebulae. The high spectral resolution provided by HIFI al- lows the accurate measurement of the line profiles. The dynamics and evolution of these nebulae are known to result from the presence of several gas components, notably fast bipolaroutflowsandslowshells(thatoftenarethefossilAGBshells),andtheinteraction between them. Because of the diverse kinematic properties of the different components, their emission can be identified in the line profiles. The observation of these high-energy transitionsallowsanaccuratestudyoftheexcitationconditions,particularlyinthewarm gas, which cannot be properly studied from the low-energy lines. They detected far in- frared lines of several molecules, in particular of 12CO, 13CO, and H O. Emission from 2 other species, like NH , OH, H 18O, HCN, SiO, etc., has been also detected. Wide pro- 3 2 files showing sometimes spectacular line wings have been found. In the case of CRL618 the 12CO and 13CO high excitation line profiles present a composite structure showing spectacular wings in some cases, which become dominant as the energy level increases (Soria-Ruiz et al. 2013). Bujarrabal et al. (2012) mainly studied the excitation proper- ties of the high-velocity emission, which is known to come from fast bipolar outflows. From comparison with general theoretical predictions, they find that CRL618 showed a particularly warm fast wind ∼300K, hotter than previously estimated (Soria-Ruiz et al. 2013). In contrast, the fast winds in OH231.8+4.2 and NGC6302 are cold, T ∼30K. k Herschel observations of PNe 7 Other nebulae, like CRL2688, show intermediate temperatures, with characteristic val- uesaround100K.Theyarguethatthedifferencesintemperatureinthedifferentnebulae can be caused by cooling after the gas acceleration (that is probably caused by shocks). Forinstance,CRL618isacaseofveryrecentaccelerationofthegasbyshocks,lessthan ∼100yrago,whilethefastgasinOH231.8+4.2wasaccelerated∼1000yrago.Theyalso find indications that the densest gas tends to be cooler, which may be explained by the expected increase of the radiative cooling efficiency with density. The dense central core of CRL618 is characterised by a very low expansion velocity, ∼5kms−1, and a strong velocity gradient. This component is very likely to be the unaltered circumstellar layers that are lost in the last AGB phase, where the ejection velocity is particularly low. The physical properties of the diffuse halo and the double empty shell, contribute to its line profiles mainly in the low-J CO transitions (Soria-Ruiz et al. 2013). 5.2. Shapemol Herschel/HIFI has opened a new window for probing molecular warm gas. On the other hand, the software SHAPE (Steffen & Lopez 2006, Steffen et al. 2011) has emerged in the past few years as a standard tool for determining the morphology and velocity field of different kinds of gaseous emission nebulae via spatio-kinematical modelling. SHAPE implements radiative transfer solving, but it is only available for atomic species and not formolecules.Shapemol(Santander-Garcaetal.2015)isacomplementtoSHAPEwhich enables user-friendly, spatio-kinematic modelling with accurate non-LTE calculations of excitationandradiativetransferinCOlines.Shapemolisaplug-incompletelyintegrated within SHAPE v5 . It allows radiative transfer solving in the 12CO and 13COJ=10 to J=1716 lines, but its implementation permits easily extending the code to different transitions and other molecular species, either by the code developers or by the user. Used along Shape, Shapemol allows easily generating synthetic maps and synthetic line profiles to match against observations. As an example of the power and versatility of Shapemol, a model of the molecu- lar envelope of the planetary nebula NGC6302 was made and compared with 12CO and 13COJ=21 interferometric maps from SMA and high-J transitions from HIFI. Santander-Garca et al. (2015) found that its molecular envelope has a complex, bro- ken ring-like structure with an inner, hotter region and several fingers and high-velocity blobs,emergingoutwardsfromtheplaneofthering.TheHerschelspectraareextremely rich, especially in terms of molecular line transitions. HIFI data have also allowed a very detailed description of the young PN NGC 7027. Santander-Garcia et al. (2012) also used Shapemol doing radiative transfer, spatio- kinematic modeling of the molecular envelope of the young planetary nebula NGC 7027 in several high- and low-J 12CO and 13CO transitions observed by HIFI and the IRAM 30mradiotelescope,anddiscussedthestructureanddynamicsofthemolecularenvelope. They used this code to build a Russian doll model to account for the physical and exci- tationconditionsofthemolecularenvelopeofNGC7027.Themodelnebulaconsistedof four nested, mildly bipolar shells plus a pair of high-velocity blobs. The innermost shell is the thinnest and showed a significant increase in physical conditions (temperature, density, abundance, and velocity) compared to the adjacent shell. This is a clear indica- tion of a shock front in the system, which may have played a role in shaping the nebula. Each of the high-velocity blobs is divided into two sections with considerably different physicalconditions.ThestrikingpresenceofH OinNGC7027,aC-richnebula,islikely 2 due to photo-induced chemistry from the hot central star, although formation of water by shocks cannot be ruled out. 8 G. C. Van de Steene 6. Outlook Soon,theTHROESatlas(Garcia-Larioetal.2016,thisvolume)willbepubliclyavail- able through the Herschel science archive. THROES is a catalogue of fully reprocessed, homogenouslyreducedPACSspectraofallevolvedstarsfromtheAGBtothePNstage, including some massive red supergiants and LBVs, complemented with ancillary data taken by other facilities. SPIRE spectra will be added later. The catalog will contain more than 200 sources, originally part of more than 40 different research programs. This will hopefully trigger additional research by the community. AlotofHerschelobservationsofPNeareavailabletobeexploitedandmoreinteresting, scientific results await discovery. References Aleman, I., Ueta, T., Ladjal, D., 2014, A&A, 566, A79 achiller, R., Huggins, P. J., Cox, P., Forveille, T., 1993, A&A, 267, 177 Bujarrabal, V., Alcolea, J., Soria-Ruiz, R., et al., 2012, A&A, 537, A8 Blommaert, J. A. D. L., de Vries, B. L.,Waters, L. B. F. M., et al., 2014, A&A, 565, A109 Boudet, N., Mutschke, H., Nayral, C., et al., 2005, ApJ., 633, 272 Cox N. L. J., Kerschbaum F., van Marle A.-J. et al., 2012, A&A, 537, 35 de Graauw, T., Helmich, F.P., Phillips, T.G. et al., 2010, A&A, 518, L4 Etxaluze, M., Cernicharo, J., Goicoechea, J. R., et al., 2014, A&A, 566, A78 Goldsmith, P. F., 2001, ApJ, 557, 736 Griffin, M. J., Abergel, A., Abreu, A., et al., 2010, A&A, 518, L3 Groenewegen, M. A. T., Waelkens, C., Barlow, M. J., et al., 2011, A&A, 526, A162 Kastner, J. H., Montez, R., Jr., Balick, B., et al., 2012, AJ, 144, 58 Mennella, V., Colangeli, L., Bussoletti, E., 1995, A&A, 295, 165 Santander-Garca M., Bujarrabal V., Alcolea J., 2012, A&A, 545, 114 Santander-Garca M., Bujarrabal V., Koning N., Steffen W., 2015, A&A, 573, 56 Schwarz, H. E., Monteiro, H., 2006, ApJ, 648, 430 Soria-Ruiz R., Bujarrabal V., Alcolea J., 2013, A&A, 559, 45 Steffen W. & Lopez J. A., 2006 Rev. Mexicana AyA 26 30 Steffen W., Koning N., Wenger S., Morisset C. and Magnor M., 2011, IEEE Transactions on visualisation and computer graphics, 17, 454 Pilbratt, G. L., Riedinger, J. R., Passvogel, T., et al., 2010, A&A, 518, L1 Poglitsch, A., Waelkens, C., Geis, N., et al., 2010, A&A, 518, L2 Ueta, T., Ladjal, D., Exter, K. M., et al., 2014, A&A, 565, A36 Van de Steene G. C., van Hoof P. A. M., Exter K. M., et al., 2015, A&A, 574, 134 van Hoof, P. A. M., Van de Steene, G. C., Barlow, M. J., et al., 2010, A&A, 518, L137 van Hoof, P. A. M., Barlow, M. J., Van de Steene, G. C., et al., 2012, IAU Symp., 283, 41 van Hoof, P. A. M., Van de Steene, G. C., Exter, K. M., et al., 2013, A&A, 560, A7 van Marle A. J., Cox N. L. J., Decin L., 2014, A&A, 570, 131 Zack, L. N., Ziurys, L. M., 2013, ApJ, 765, 112 Zeigler, N. R., Zack, L. N., Woolf, N. J., Ziurys, L. M., 2013, ApJ, 778, 16 Acknowledgements IthanktheSOCforinvitingmetodothisreviewtalk.Iamindebtedtomycolleaguesof theMESSandHerPlanSconsortiawhohavecloselycollaboratedwithherontheHerschel data. G. Van de Steene wishes to acknowledge support from FWO through travel grant K1C8716N. G. Van de Steene and the MESS consortium wish to acknowledge support from the Belgian Science Policy office through the ESA PRODEX programme.