PoS(LCDU 2013)014 http://pos.sissa.it/ mplications for understanding to study the conditions of the axies, which reflects significant id-IR spectroscopy has shown a a much wider range of the ISM adiation through the evolution of nd mid-IR. Herschel now enables recently, spatial resolutions in the e and a size distribution. AKARI ools to trace star-forming activities ission properties of dust and PAHs s of far-IR dust and PAH emission nteractions with interstellar shocks, ange from passive elliptical galaxies ures and PAH to far-IR dust ratios to mation activity. Spectral information ocarbons (PAHs) absorb a significant l areas within a galaxy, however, their t are mixed well in the ISM, producing e intensity ratio of the aromatic to the ous grains in harsh interstellar environ- -)luminous infrared galaxies. In particu- 8602, Japan , and Laboratory Experiments e them in the infrared (IR). Hence the IR ating structural changes of carbonaceous e Commons Attribution-NonCommercial-ShareAlike Licence. ∗ [email protected] Speaker. far-IR were extremely poor compared withus those to in make the a near- a within detailed a comparison galaxy. of the spatialThis distribution paper reviews recent observational resultsexposed on to various the environments IR of em nearby galaxies, which r ments to understand the fate of dust processed by shocks and r on the dust and PAH emission would have much deeper physical i global correlations between their IRabundance luminosities. ratios In are loca expected tohard UV vary radiation substantially fields due and to diffuse i X-ray hot plasmas. Until to starburst galaxies with galactic superwinds, andlar, the (ultra paper focuses on variationsdiscuss in their the implications PAH for spectral the feat processing of carbonace galaxies. fraction of stellar ultraviolet (UV) photons and re-radiat in galaxies. However they are not merely tracers of star-for the properties of thephysical ISM. conditions External than galaxies our provide Galaxy. us with For example, Spitzer m interstellar environments. In general, PAHs and far-IR dus In star-forming regions, dust and polycyclic aromatic hydr luminosities due to dust and PAH emission are both powerful t variety of the PAH emission features for various types of gal grains in shocked regions. The relation of PAH to far-IR dust is another important probe changes in the properties of PAHs, such as analiphatic ionization hydrocarbon spectral stat feature in galaxies, indic near-IR spectroscopy has revealed spatial variations in th ∗ Copyright owned by the author(s) under the terms of the Creativ c

The Life Cycle of Dust in the Universe: Observations, Theory 18-22 November, 2013 Taipei, Taiwan Hidehiro Kaneda E-mail: Properties of dust and PAHs inenvironments various of nearby galaxies Graduate School of Science, Nagoya University, Nagoya 464- PoS(LCDU 2013)014 . m µ detector m spectra of h sensitivities µ t based on the weak 6–9 s. Faint galax- Hidehiro Kaneda structures of the 3; IRAS detected nvironments, and Herschel, such as ness of interstellar pes and the overall itions of the inter- ecently, significant higher sensitivities MC) and the Small are notably similar be more efficiently and therefore nearby m feature [14]. The e relatively nearby ( g the photometric sur- µ -IR were initiated with vely. A sub-mm wave- ies and even early-type alaxies as star-formation xies such as luminous IR m broad feature commonly ction between stars and the m and 2.5–5 galaxy; early-type galaxies r/IRS sample of 91 nearby by galaxies, which covered m feature can be explained dentedly high spatial resolu- µ µ or normal galaxies [9]. µ y galaxies m to the 11.3 µ 2 m continuously [7, 8]. In particular, spectroscopic studies of µ m was realized with Herschel/SPIRE. There are many observational µ m PAH features relative to the features at longer wavelengths (Fig.1) 10 Mpc) enables us to perform spatially-resolved studies on the ISM µ . Space IR observations of dust in nearby galaxies started with IRAS in 198 Nearby galaxies provide a wide range of the physical and chemical cond Following IRAS and ISO, Spitzer enabled us to study nearby galaxies with hig With Spitzer/IRS, detailed studies of the PAH emission features are carried ou more than 25000 galaxies,galaxies which [1, included 2, spiral galaxies, 3,galaxies Seyfert 4]. (LIRGs) galax and ultraluminous IRAS IR discoveredveys galaxies new (ULIRGs) by [5, classes IRAS, 6]. ISO of Followin performeda IR-bright IR wavelength gala range spectroscopic from observations 2 of to near 200 stellar medium (ISM), compared to ourMagellanic Galaxy, the Cloud Large (SMC). Magellanic These Cloud ISM (L radiation conditions include field, the metallicity, intensity stellar andso hard population, on. large-scale shocks, Their proximity hot ( plasma e nearby galaxies were obtained withlength Spitzer/IRS coverage and beyond AKARI/IRC, 200 respecti [15, 16, 17, 18].early-type According galaxies to show recent the results, PAH emission, about and half 80–90 of % the ofby Spitze them predominance show of similarly either large PAHs or neutral PAHs. The low ratios can polycyclic aromatic hydrocarbons (PAHs) for galaxiesISO, in which the were near- carried and out mid not only for IR-bright galaxies but alsoand f high imaging capabilities especiallytechnologies. in the AKARI mid-IR, performed thanks to all-skyand the surveys spatial improvement in resolutions in than the the IRAS. mid- Recentlytions Herschel and realized in far-IR unprece the with far-IR thankscold to ISM a in 3.5-m-diameter nearby galaxies. telescope, Spectroscopically, which high-sensitivity detected 5–35 detailed detected in galaxies, which shows a very tight correlation with the 11.3 ISM. The latter study cangalaxies be are carried out complementary for to our Galacticies, Galaxy and and such Magellanic the as targets LMC/SMC, dwarf for and the10 elliptical ISM Mpc). galaxies, studie Accurate can calibration only of beindicators infrared is studied (IR) also when dust important they for emission ar study in of nearby distant g galaxies. structures of galaxies, although they are not close enough to study intera Properties of dust and PAHs in various environments of nearb 1. Infrared observations of dust in nearby galaxies mid-IR spectra of the SINGSamong star-forming sample galaxies. [14]. Spitzer/IRS improves the It determinationstrengths is of of the the found PAH sha profiles. that One the of the PAH Spitzer/IRS features findings is the 17 PAH features [19, 20]. The low ratios of the 7.7 programs which systematically study nearbySINGS galaxies [10], with ISMGN Spitzer, [11], AKARI, KINGFISH [12], or and DGS [13]. feature is likely due to relativelyvariations large of PAHs the in PAH a spectral C-C-C features bending wereshow discovered mode. unusually from weak More galaxy r 6–9 to PoS(LCDU 2013)014 . T n of FISH and β [22] clearly arby galaxies. Hidehiro Kaneda m spectral energy old dust in nearby KINGFISH galax- which is thought to µ t in low-metallicity tions of dust temper- e metallicity effects on d that a threshold for the h is more reasonable for trend that low-metallicity ust temperature increases m). They interpreted that µ S: (left) star-forming galaxies [14] and m in the left panel are faint in the right µ y galaxies 10 K) dust, which calls for unrealistically ∼ res at 6–9 between the samples. They also found excess β 3 m band intensity ratios are low in HII regions, while in galaxies to find an anti-correlation between µ β m / MIPS 24 µ m) are well correlated with cold dust (MIPS 160 m on top of the modified blackbody dust continuum from a substantial fractio µ µ Mid-IR spectra of nearby galaxies obtained with Spitzer/IR and emissivity power-law index T Herschel/PACS and SPIRE enable us to map the properties of cold dust in ne The correlations between the spatial distributions of PAHs, hot dust and c Using the KINGFISH sample, Galametz etature al. [25] derived the spatial distribu galaxies were studied usingshowed Spitzer/IRAC that and the MIPS IRAC 8 imaging data. Bendo et al. their sample galaxies. This mayhigh be dust-to-gas due mass to ratios. very Another cold possibilitybe ( is PAHs. spinning This dust, scenario the is, origin of however, inconsistent with the observational PAHs (IRAC 8 emission at 500 (right) elliptial galaxies [18]. Note that strong PAH featu PAHs are selectively destroyed due tothe intense PAH emission radiation and in IR colors HII werepresence regions. also of revealed Th PAHs by exists Spitzer. It around was 12+log(O/H)=8with foun decreasing [23] metallicity and [24]. also that the d distributions (SEDs) with metallicity; dustsample, in but the there DGS is sample no is systematic warmer difference than in in the KING reproduced by predominance of neutral PAHs [21], the situation of whic panel. soft radiation field due to old stars in elliptical galaxies [17, 18]. Figure 1: Properties of dust and PAHs in various environments of nearb Rémy-Ruyer et al. [26]dwarf systematically galaxies, investigated combining the 48 properties DGS galaxies ofies with cold with 12+log(O/H)=7.0–8.5 12+log(O/H)=7.8–8.7. dus and They 61 found a systematic change in the 70–500 PoS(LCDU 2013)014 , , min PAH U q al im- , PAH q [38]. With -metallicity llar radiation ing the DL07 neighborhood, wer (70–90 %) associated with atially-resolved Hidehiro Kaneda servational data total dust, ls for studies of sistently through for example, the ared to the far-UV observed extinction posed for the origin [40]. As a result, the stic heating mode in PAH component has omponents similarly, k et al. [29] reported iffuse ISM component e Spitzer SEDs for the related to the nature of ged, such as [31], while the DustEM oulanger, and Puget [30], very small grains (VSGs) g almost a half of the total ] for carbonaceous dust. The y galaxies . By applying the dust model to the SEDs of is assumed to follow a power-law distribution and photodissociation region (PDR) component max U U 4 min to U , used in the PDR model. For galaxies, the mass of min 0 U G m for the KINGFISH sample, which may be related to metallicity µ 20 % larger when Herschel data are included in the analysis [39]. [35]. Before the Spitzer era, Galliano et al. [36] created a sophisticated ∼ dU α − illuminated by the radiation field U ) m excess [28]. Although the excess emission has potentially important physic µ ∝ U ( ) U dust ( . except that the fraction of dust heating attributed to intense radiation fields M The high spatial resolution of Herschel imaging data enables to perform sp Proper modeling of dust SEDs is indispensable to physically interpret IR ob In the Spitzer and Herschel eras, one of the most popular dust SED mode dust dust , which is defined in a photon energy range of 0–13.6 eV [34]. This is comp M shows a significant variationthe from model, galaxy it to was galaxy clearlyrather shown than with that dust a dust in median in PDRs.KINGFISH value the sample, Even diffuse of the when model ISM 3.5 Herschel parameters dominates are data % found the points to be IR are relatively po unchan added to th dM the Spitzer/SINGS sample, it was found that the fractional mass of PAHs to the which has a power-law distribution from dust SED fitting to amodel, combination dust-to-gas mass of ratio the maps were Spitzer created for mid-IR NGC and 628 and Herschel NGC 6946 far-IR data. Us (6–13.6 eV) interstellar radiation field, of nearby galaxies. In thethree classical dust dust components model are establishedamd incorporated, by big Désert, namely B grains PAHs, (BGs). carbonaceous (and The emission). dust size Since then, distributionbut is every dust there chosen model, is to in reproduce a principle, the Draine significant assumed & difference Li these in model c (DL07) the [21]model grain adopted [32] opacity the used optical from those properties of model of hydrogenatedradiation graphite to amorphous field carbon model; intensity (HAC) is [33 usually given in units of the starlight intensity in the solar PDRs is found to be nearby galaxies has been the DL07been model improved [21], much, in which compared the tofield, treatment to the of the which previous dust models. isrepresented by exposed, In a consists the single radiation of model, field two strength the components: interste the general d effects. 2. Interpretations based on dust SED models plications, the presence of theno excess substantial itself excess is at 500 still controversial; Kirkpatric dust SED model, in which theyUV-optical determined and the IR-mm interstellar radiation observations field withgalaxies, self-con IR they ionic found lines. the presencedust Applying of mass the very [37]. model cold They to dust pointedthe low (5–7 out low-metallicity that K) environments [37]. most occupyin grains are likely to be in a stocha Properties of dust and PAHs in various environments of nearb dwarf galaxies show relatively lowamorphous PAH abundances. solid opacity The [27]. excess mayof Very recently, be the metallic 500 particles were also pro U PoS(LCDU 2013)014 ed in the DL07 [41]; the result Hidehiro Kaneda tate physics can s that interstellar ment in the SMC grains, C-rich and contribution to the -mm emissivity for egions due to higher ich AGBs are rather t to the difference in ed regions are in the 100 km/s shocks for the dust mass derived 0.004–0.04) within the ∼ us silicate, causing car- ∼ e abundance of C atoms r studying the dependence Figure 2 shows the spatial rmation of PAHs, but rather e assumption of amorphous totic giant branch (AGB) stars, AGB stars along the Galactic plane y galaxies m band fluxes in the AKARI all-sky point- µ KARI all-sky survey data. s, as defined by the equation in the panel, along the 5 band fluxes [47]. As can be seen in the figure, the K , and H , J (Top) Spatial distribution of oxygen-rich and carbon-rich A dominant dust population may be different between far-IR and sub-mm r The DustEM model adopts amorphous carbon instead of graphite which is us As to the behavior of the sub-mm opacity of amorphous grains, pure solid-s absorption efficiency of amorphous carbonbonaceous dust in to the have near-IR higher temperaturesdistributions than of than carbon-rich amorpho silicate (C-rich) and dust oxygen-rich [32, (O-rich) asymp 21]. derived using the color-color diagrams of the 9 and 18 amorphous carbon, but only 15carbon % for for carbonaceous graphite [45, grains 46].observed might in be Therefore shocked th better regions. to explain the gas-phas model. The change of amorphousby carbon the from model graphite results fitting inamorphous by lowering carbon a [43]. factor Observationally of 80–100gas 2–3, % phase of because [44], the of while C the 30–100 atoms higher % in shock far-IR of to dust sub is expected to be destroyed by galaxies [40]. The high spatial resolutionof of Herschel the data PAH also allows abundance fo suggested on that the the dependence metallicity is not for causedby by individual metallicity-dependent their fo HII destruction; a regions similar in result[42]. galaxies was reported for the low-metallicity environ Galactic plane. Both distributions are obtained using the A [47]. (Bottom) Distribution of PAH/far-IR intensity ratio dust-to-gas mass ratio is found to vary by almost one order of magnitude ( O-rich AGBs are more concentrated towarduniformly the distributed Galactic throughout center, while the thePAHs Galactic C-r and plane. far-IR dust grains Thethe are lower similar distribution panel in between indicate the the spatialO-rich dominant distribution, AGBs. suppliers in contras of This may carbonaceous suggestfar-IR and emission that silicate in silicate the grains diffuse ISM, do but not to make the a sub-mm significant regions. source catalog, with the 2MASS Figure 2: Properties of dust and PAHs in various environments of nearb PoS(LCDU 2013)014 α ratio istance ). It is IR with the ⊙ L / 1 L 3 − . m emission , which is a 12 3 3 µ L − 10 m) luminosity, idely extended Hidehiro Kaneda 15 %) polarized µ 10 e consistent with 3.3 > the s important infor- 0kms up to 4 with wave- − ≃ or future dust SED IR ∼ e 34 near-IR spectra or example, Spitzer, β aliphatic to aromatic Hs even in the harsh L IR ut of the disk through cessed are likely to be to understand the pro- n by tunneling effects m excess indicated by L charge distribution with µ ), luminous IR galaxies ust observed for particu- / etween the PAH and H at the PAHs are produced ⊙ 3 se of . halo. L 3 d that the dust flow velocity re quite different from those cially the degree of process- L 11 down to mer galaxies, nearby edge-on 0.01–0.1, a global relation is 1 10 ∼ − < IR is significantly (5 L α with temperature [49]. Thus the sub-mm with physical parameters [27]. One com- y galaxies 200 km s , and the total IR (8–1000 m features are unusually strong in the halo, ∼ β β 3 . µ 3 L 6 25 % of all the dust has been expelled from the disk ∼ m luminosity, µ line decreases from α photons from the galactic disk are scattered by dust grains in the ) and ultra-luminous IR galaxies (ULIRGs: ⊙ α L 12 10 − 11 m features are clearly detected in the halo regions, which are located at a d 10 µ ∼ IR L As also shown in Fig. 3, using the AKARI near-IR spectroscopy, the PAH This section and the next describe several results on the properties of d For about 200 star-forming galaxies in the redshift range of [57]. The sample is classified into IR galaxies (IRGs; IR confirmed that many of the IRGs and LIRGs follow the relationship ratio typical of starburst galaxies [58]. At the same time, it is also found that (LIRGs: toward the halo regions. It is found that there is an excellent correlation b [52, 53]. Figure 3 shows the distribution of the PAH emission in M 82, which is w lar targets of active and passive galaxies,starburst respectively. galaxies Among with the prominent for galactic superwindscessing are of important dust targets through materialAKARI, circulation and on Herschel a detect galactic copiousgalactic scale. amounts superwinds of [50, For BGs 51, M and 52]. 82, PAHs flowing f In o total, height from the disk (0–1.4 kpc),falling which back implies toward that the the disk dust [54]. grains thus pro investigated between the PAH 3.3 L the correlation length for charge neutrality [48], which predicts an increa halo toward us. The excellent spatialby correlation can shattering be of explained the such dust th estimated grains by from shocks a [55]. shift of Moreover it the was H foun and the 3.4–3.6 suggesting the dominance of aliphatic structurestaken over from aromatic the ones. center, From diskratios th and systematically increase halo with regions the of distancethe M82, from above the it picture center, of is which shattering seems revealed of to that carbonaceous b grains the by shocks in the ponent to be considered for the sub-mm opacity is related to the disordered opacity depends on the physical properties of amorphous grains, espe length. Another is expresseddue as to two defects level in systems lattice, causing which charge predicts transitio a decrease of ing, but not chemical compositionthe much. Herschel Although data the is origin stillmation of quite the on uncertain, 500 the the sub-mm nature opacity ofmodels. potentially grains, deliver and its proper treatment should be required f 3. Properties of dust in active galaxies [54], which suggests that H distributions [51]. The spectro-polarimetry showed that H Properties of dust and PAHs in various environments of nearb explain the change of the emissivity power-law index of 2 kpc away fromenvironment of the the galactic M82 center, halo thus [56].commonly confirming The seen the observed in spectral presence other properties of spiral a galaxies; PA the 3.4–3.6 PoS(LCDU 2013)014 -band B m feature is µ e galaxies may Hidehiro Kaneda images [51]. The ators for studies of α d of the lifecycle of osities and laxies with unusual r) origin is yet to be H processing through ocal ULIRGs may in- onclusion on whether fficient destruction by ny early-type galaxies, f debate (e.g. [4]). Some int C-C vibration features once by shocks which oc- central reservoir may play ones, become dominant in sistent with the observational wn together, which are taken from y galaxies m emission does not represent any star-forming µ m (PAH) band overlaid on the H 7 µ m feature is notably weak, whereas the 11.3 µ m map. µ Contour map of M 82 in the AKARI 7 m spectra obtained by the AKARI near-IR spectroscopy are sho m. It should be noted that the PAH 11.3 µ µ Elliptical galaxies provide us with another extreme case, representing the en dust. In such passive galaxies, theelliptical origin galaxies of contain dust itself surprisingly has largesputtering been dust in a the masses, matter hot o considering plasma the environments [60,but e 61, did 62]. not Spitzer observed clearly ma show a significant correlation between their far-IR lumin luminosities [63]. This result suggestsnot that be the related amount to of thea the stellar BGs majority mass remaining loss of in of dust th evolvedreached. is cool stars. of As internal Hence described a (stellar) above,band clear origin Spitzer ratios; c or detected the usually external PAH emission strongest (gas-rich 7.7 in merge elliptical ga galaxies. It is suggested that the AGN-assisted feedback outflow from a activity in this case, although PAH emission is often used as star-formation indic relatively strong. It is concludedvery that soft neutral radiation PAHs, fields, rather typical than of ionized ellipticalat galaxies, 6–8 giving rise to the fa the positions indicated in the 7 considerably decreases toward the luminous end intrinsically the possess ULIRG smaller population. amounts of L PAHs relativerecent to galaxy BGs, mergers. as Some a fraction result of ofcurred PAHs PA may during have a been merging destroyed process, whereasindication BGs that survive, local which ULIRGs is are con merging galaxies (e.g. [59]). 4. Properties of dust in passive galaxies Figure 3: Properties of dust and PAHs in various environments of nearb 2.5–4.5 PoS(LCDU 2013)014 bserva- in prep.). 9, together m continuum m maps of the mediate-mass µ µ Hidehiro Kaneda 4589 at 70, 100 s [64, 65]; PAHs lution of the ISM -axis dust lane in 9. ite similar to PAHs. w-mass O-rich stars rge grains. ed stars (if they are both -mass O-rich stars make trong absorption features ins. Hence the Herschel ob- m feature and 5.5–6.5 µ el/PACS 70, 100 and 160 y galaxies 8 m from much wider areas of the galaxy than the PAH and dust µ m) continuum emission [66]. The distributions of both the PAH µ m, obtained by deep imaging observations with Herschel/PACS (Kaneda et al. Spitzer/IRS spectral mapping images of the PAH 11.3 µ m and the continuum emission were obtained with Spitzer/IRS spectral mapping o µ Figure 4 shows the spatial distribution of PAHs in an elliptical galaxy, NGC 458 emission [67]. These absorption features[68], are which most are likely currently supplying toservation silicate originate suggests but from that not lo the carbonaceous silicate gra grainsonly being a currently minor produced contribution by to low the total far-IR dust emission observed in NGC 458 11.3 tions. The figure reveals thatthe the galactic PAHs center. are compactly Figure distributedand 4 along 160 also a shows minor theThe spatial far-IR distribution dust of emission dust is in spatiallySince well NGC PAHs resolved, are exhibiting likely distributions qu tostars, while be silicate old grains are remnants currently being originatingof produced internal from origin), by this mass low-mass evolv similarity losses may havein from deep old inter physical galaxies. implications The for the AKARI evo due near-IR to spectroscopy SiO of and NGC CO 4589 around shows 4.2–4.7 s an important role in supplying dust into the interstellar space of elliptical galaxie emission for the elliptical galaxysame galaxies. NGC 4589 [66]. The Hersch might come from residual dust fragments originating from the sputtering of la with that of the stellar (5.5–6.5 Figure 4: Properties of dust and PAHs in various environments of nearb PoS(LCDU 2013)014 mation on the r environments Hidehiro Kaneda t HII regions in uctures of nearby mission in galaxies nabled us to discuss s been obtained with erstand the fate of dust cial to understand their havior of the dust opacity ture mid- to far-IR spectral e chemical compositions of cially on the degree of dust complement the Spitzer and e, the mass fraction of PAHs nravel the whole story of the life cycle Quasars measured by the Infrared y galaxies rvational facilities. m excess and the aliphatic to aromatic ratios in µ 9 815. 308 ApJ , 1986, Illustration to show that nearby galaxies are important to u Astronomical Satellite Thanks to the development of IR observational technologies in space, str [1] G. Neugebauer, G. K. Miley, B. T. Soifer and P. E. Clegg, galaxies are now spatially resolved in PAH, VSGtheir and relationships BG in emission, some which has detail. e Inhas particular, improved the understanding very of much thedistributions PAH with of e BGs the within advent galaxies and ofHerschel. their Spitzer, The spatially-resolved properties AKARI while ha all-sky many surveysHerschel and pieces studies near-IR of of spectroscopy nearby will galaxies. infor Amongto the results BGs presented and abov the PAH bandin ratios galaxies: are found for to example, varyspiral with substantially galaxies, with the and the the intense interstella soft radiation radiationin field field the in in far-IR early-type to dwarf galaxies. sub-mm galaxies, region The gian including be the 500 of dust in the universe with the current and future major obse 5. 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