PoS(LCDU 2013)050 ebula http://pos.sissa.it/ ce. , aiming at (1) establishing the 81, as an example, and explore ging and spectroscopic survey of riefly demonstrate the breadth and . Ladjal (DU), K. M. Exter (KUL), M. Otsuka ), R. Sahai (JPL), P. A. M. van Hoof (KSB/ORB), M. Tielens (Leiden U.) J. H. Kastner, J. Nordhaus , and Laboratory Experiments A/Harvard), H. Izumiura (OAO/NAOJ), J. A. Lopez jlstra (U. of Manchester), M. Wittkowski (ESO), S. er (UAM), B. Balick (UW), E. Behar (Technion), E. ebulae and (2) understanding the energetics Herschel Space Observatory ive Commons Attribution-NonCommercial-ShareAlike Licen , the next-generation far-IR mission. † SPICA , Djazia Ladjal, Katrina Exter, and the Herschel Planetary N ∗ [email protected] Speaker. The founding members of the HerPlaNS team are; T. Ueta (DU), D spatially-resolved far-IR characteristics of the target n depth of the HerPlaNS data setexpectations in using the one era of of the targets, NGC67 Herschel Planetary Nebula Survey (HerPlaNS)planetary is nebulae, a performed with far-IR the ima and shaping history of the circumstellar nebulae. Below we b ∗ † Copyright owned by the author(s) under the terms of the Creat c W. Vlemmings (Chalmers), and I. Yamamura (ISAS/JAXA). (ASIAA), R. Szczerba, N. Siódmiak(RIT), (NCAC), R. I. Aleman, Montez A. (Vanderbilt),Ramstedt G. I. G. (Uppsala McDonald, U.), K. O. Hebden,G. De Blackman A. Marco (U. Zi (Macquarie of U.), Rochester,(UNAM), E. Y.-H. K. Chu Villav Murakawa (UIUC), (Leeds), J. R. L. Nordon Hora (MPE), (Cf C. Sandin (AIP Toshiya Ueta Planetary Nebula Dust Haloes Revealed by Herschel University of Denver E-mail: Survey (HerPlaNS) team 18-22 November, 2013 Taipei, Taiwan The Life Cycle of Dust in the Universe: Observations, Theory PoS(LCDU 2013)050 Her- yr. b 4 Toshiya Ueta 10 ed far-IR char- × X-Rays 3 (§3). A complete 2 H ase, whose central star SPICA K) ∗ 3 radius within a diffuse, low- ′′ pen-time program of the ra of ntities in the equatorial plane as a yr) (10 1 80 N D 3 ing the potential of the data set using with an equatorial enhancement (i.e., < a thermal continuum emission and the mission without much extinction. The ells. In this contribution, we present a olar structure along the direction of the al and present masses of the central star c systems of gas and dust. Far-IR obser- these nebulae will provide more insights ence of a point source. (d) Not a ChanPlaNS target PN. -ray detection. (c) Not a ChanPlaNS target PN. The PSF b) The HerPlaNS sample is a subset of the Chandra X-ray 143 pc away [4]. Comparison of these parame- 2 ± D R Age T (kpc) (pc) (10 [6, 7]. Morpho-kinematic observations in molecular lines yr at the adopted distance of 950 pc. Hence, the spatially- List of HerPlaNS Target PNs a at 950 4 ′′ ⊙ 10 160 × × Table 1: ′′ 01.0 Bps 1–3 0.1–0.2 0.6–2 32: Y D, P 17.3 Rsai 1.3 0.14 3 47 N D, P 09.8 Bbsh 1.0 0.11 4 48 N D 29.9 Mcspa 1.5 0.09 5 48 N D, P 34.5 Lbspa 1.5 0.09 3 87 N D, P 12.7 Ecsah 1.3 0.08 5 50 N D, P 32.0 Ecspaih 1.0 0.10 4 89 N D 00.3 Bs 1.7 0.16 02.9 Bth 1.0 0.32 26 112 Y N 13.9 Ecsh 0.7 0.13 6 148 Y N 03.9 Mpi 1.4 0.14 3 170 Y P − + + + − + + + − + + [2]. Our chief objective is to examine the spatially-resolv 331.7 089.0 , respectively, and the age of the PN since the AGB turn-off is c ⊙ d NameMz 3 PN G Morph NGC 2392 197.8 NGC 40 120.0 NGC 6543 096.4 NGC 7009 037.7 NGC 6826 083.5 NGC 3242 261.0 NGC 7026 NGC 6781 041.8 NGC 6720 063.1 NGC 6445 008.0 The optical nebula of NGC 6781 shows a signature “ring” of 50 NGC 6781 is a PN near the end of the interior nuclear burning ph The Herschel Planetary Nebula Survey (HerPlaNS; [1]) is an o ters with evolutionary tracks of [5] suggests that the initi are 1.5 and 0.6 M account of the present summary is found elsewhere [1]. 2. HerPlaNS Data Demonstration with NGC6781 (CSPN) is of 110 kK [3] and 385 L emission nebula extending 190 [8, 9] indicated that thebarrel) nebula with is a a dynamical nearly age of pole-on 4 cylinder resolved data of NGC 6781function will of radius, reveal taking variations into nebular accountline qua the of height sight. of the bip schel Space Observatory acteristics of planetary nebulae (PNs; Tablevations 1) allow as simultaneous energeti probing of the dustgas component component vi via far-IR fine-structure andspatially-resolved molecular energetics line e as a function of location in about the evolution of the central star and circumstellar sh brief overview of the survey andNGC 6781 its data as products, an summariz example (§2), and hint at expectations for the e of XMM-Newton does not allow clear determination of the pres (a) According to the morphologicalPlanetary classification Nebula by Survey [10]. [11]: D ( - diffuse, P - point-source X Planetary Nebula Dust Haloes Revealed by Herschel 1. Herschel Planetary Nebula Survey (HerPlaNS) PoS(LCDU 2013)050 are 2 − resolution 5007 map resolution. The emis- ′′ λ ′′ 4 Toshiya Ueta . 3 . 02 28 28 60 25 . . . . . field at 70 and 1 3 3 4 2 eak, and the black ′′ ν ± ± ± ± ± F 41 42 88 04 56 , respectively, from top 600 . . . . . m. Far-IR images of 1 µ − × ′′ ) (Jy) ) map at the 36 2 ) the NOT [OIII] sky noise in mJy arcsec NII] image taken at the Nordic resolution. β − ′′ σ 4 . threshold (Table 2). The surface sky σ [N II] emission of a deep exposure t points of the inclined barrel. The r pole-on cylindrical barrel. The to- sky Top Right σ ) mapof NGC6781at the 11 with contours at a 2K interval from 40 to ness and 1- dust T ) (mJyarcsec 2 − ) map at the 11 1 ly. At the top-right corner, the beam is shown: 5.61, − 3 field at 250, 350, and 500 peak pix I ) The power-law index ( ′′ ⊙ 480 × ′′ λ m) (mJyarcsec Bottom Left ∆ µ ) The dust temperature ( ; [6]). σ m is co-spatial with low-ionization optical line emission. m) ( µ λ µ ( Far-IR Image Characteristics and Photometry of NGC6781 Top Left , respectively. Contours are 90, 70, 50, 30, 10, and 5% of the p ′′ threshold. The pixel scales are 1, 1, 2, 6, 9, and 14arcsecpix radius at 5- σ ′′ Table 2: contours are always overlaid in other frames. ( dust ) The dust column mass density (M T SPIREPLW 500 200 0.327 0.046 6 Band PACSBlue 70 25 11.623 0.022 65 PACSRed 160 85 6.68 0.06 64 SPIREPSW 250 76 2.41 0.06 30 SPIREPMW 350 103 0.982 0.042 14 [Left] HerPlaNS broadband far-IR images of NGC6781 with an [ m and SPIRE imaging of a 240 HerPlaNS broadband imaging consists of PACS imaging of a 600 µ Bottom Right Optical Telescope (NOT) [7]. The far-IR peak surface bright Figure 1: Planetary Nebula Dust Haloes Revealed by Herschel 160 NGC 6781 (Figure 1, left) revealtal the fluxes signature are ring measured of the by nea aperture photometry with thesion 3- peaks at the easternextent and of the western far-IR rims emission representimage is the (about about 100 pivo the same as the diffuse showing the high-ionization regions. ( 11.39, 18.2, 24.9, and 36.3 indicated at the bottom-left and right corners, respective derived by a power-law dust26K. emissivity fit. These The peak is 41.3K, ( contour indicates 3- 2.1 Broadband Imaging: Diagnostics via Dust Continuum brightness distribution at 70 left to bottom right. [Right] ( PoS(LCDU 2013)050 , e e ′′ T T dust 120 T 40 K) the , , where ∼ & β ) CS range dust arrel cavity. l barrel. Toshiya Ueta T ( on the “ring”), ν region ( 6 B − β − n 35 spectra in the dust T λ m coverage at the “cen- to 10 ∝ µ 5 ν ) and on the eastern “rim” − m, resulting in 25 spectra Spectra of NGC6781 over S ). in the PACS range and less µ m) over a field of a 2 10 2 − µ − ) of the nebula. The flux units = ative line strengths of the two vity ( drical radius (Figure 3). The ure of dust [12], consistent with m –220 sed on these spectra. Moreover, h along the line of sight, corrob- µ black line ) maps using far-IR line ratio maps m) by solving the equation of statis- 160 ight). The high e τ an be rendered into spectral line maps µ IR emitting dust is determined to be gure 3). In the case of NGC 6781, we n gray line e at both pointings in the SPIRE range. ter” ( ( are set to(mJy arcsec show the surface brightness Figure 2: the entire 51–672 al highly-ionized cavity. red and modeled with optical data. By onized. While rich in lines, we determine 10 mJy arcsec m at two spatial pointings (at the center and . µ ) maps can be translated into ionic/elemental m) augmented with other optical-to-far-IR line e 6583/122 µ n λ , 4 e T m/205 µ is the temperature), we successively derive the dust ) and electron density ( T m and [N II] e T µ 9,000 K) in the highly-ionized barrel cavity, surrounded by 5007 line emission, delineating the highly-ionized inner b ∼ ( λ e 5007/88 T m and [N II] 122 in the SPIRE range. Thermal dust continuum emission in the PA λ and roughly 50 % of which appears contained in the cylindrica µ m) and 19 spectra in the SLW band (303–672 2 ⊙ − µ M field and SPIRE Fourier-transform spectroscopy resulting i 3 m/88 − ′′ µ 10 47 × × 8 ′′ . 3 map is almost entirely unity, suggesting a carbon-based nat = By fitting these emission maps with the power-law dust emissi Because far-IR thermal dust continuum is optically thin ( HerPlaNS spectroscopy includes PACS integral-field over 51 Besides continuum, a plethora of lines are detected. The rel β is the dust emissivity index and dust radius. Figure 2 shows spectra for the whole 51–672 β Planetary Nebula Dust Haloes Revealed by Herschel SSW band (194–313 optical depth, and dust column mass density maps (Figure 1, r ratio maps (e.g., [O III] tical equilibrium [13 – 15]. Moreover, these ( The the previous assessments [7, 15]. over a 47 eastern rim), at which continuum is detected at about the dust column mass densityorating map the probes the pole-on whole barrel nebula structure dept previously only infer M integrating over the entire nebula, the total amount of far- 2.2 Spatio-Spectroscopy: Diagnostics via Gas Emission than a few mJy arcsec abundance maps [16]. Here we show 1-D profiles along the cylin is co-spatial with the [O III] PACS/SPIRE spectra taken by arrays of spaxels/bolometersby c integrating the data cubederived over the specific electron emission temperature lines (Fi ( that line contamination in broadband images is at most 20 % ba is generally stronger at the easternThis rim, indicates but that is a about cold the dust sam envelope surrounds the centr pointings suggest that the central cavity is more strongly i profiles reveals constant (e.g., [O III] 52 PoS(LCDU 2013)050 ). ∼ ′′ 50 ). The 12, and & )+ 12. H middle Toshiya Ueta / )+ C ( H initial mass. / O ⊙ ( , log profiles ( + ) line emission in indi- e T : C and log ). The legend is given in each bottom + e can empirically determine 2 ). The relative elemental abun- m( ). The log :O C 6781, the derived dust-to-gas µ tratification: the highly ionized top Triangles bottom sider the presently rampant “one- th a single gas-to-dust mass ratio. aries radially from over 550 to 100 . The marginal N abundance (not e understanding of not only the PN profiles show a uniform distribution ly-resolved physical stratifications in e nt of gas or dust component by scaling cal ballpark figure of roughly 400 for Squares n top in hue used for systems that are not necessarily which many excellent reports can be found ) and a radially increasing distribution of a 3 − 29.6 eV) are ionized, the inner barrel wall ( ). ) and [NII]122 based on [NII], 3 > e − ( n top 5 , + 12, and N/O, e T m( 400 cm : µ )+ ∼ tapers off. The H ; 14.5 eV) are ionized, and beyond the barrel wall ( / e T > N Pluses ). The C/O and N/O profiles ( ( ( m line intensity map ( 0 µ ; 100–600 cm pluses ), log middle 35.1 eV) and N > ) The relative ionic abundance profiles ( filled 12; ( crosses ( [OIII] ( = + e + 2 n H Right N based on [OIII], ), N e [N II] ( 24.4 eV) and N ) The [NII]122 ).( e n 5; [17]) suggests that the CSPN is most likely less than 2 M > . n , ( e 0 open T ( + : . ) Spatial variation of [NIII]57 Middle + bottom 10,500 K) beyond which ) in which O O ′′ / ∼ : N Left ( 30 Crosses . profiles ( Circles By combining the above analyses of broadband and line maps, w Moreover, the ionic abundance profiles reveal the physical s e ) in which C n ′′ log Figure 3: Planetary Nebula Dust Haloes Revealed by Herschel vidual spectra. ( dance profiles (where log of a high-ionization gas maximum ( low-ionization gas C/O, Similarly, the CNO elementalType abundance I, as profiles N are derived frame — 3. Future Prospects the gas and dust columnmass maps ratio independently distribution (Figure is 4).carbon-rich in For AGB general winds NG [18]. consistent However, with weover a note the that typi the cylindrical ratio barrel v wall.value-fits-all” approach Hence, of extrapolating we the may unknownthe amou need empirically to determined recon amount ofWith the the rich other HerPlaNS component data wi set,these we dusty will gaseous decipher systems. the spatial physics These itself insights but also will the enhancespatially general th resolved far-IR (e.g., line luminous diagnostics infrared galaxies;in for the present proceedings issue). cavity ( 50 PoS(LCDU 2013)050 radius in ′′ Toshiya Ueta with contours at 90, 70, 50, ard issued by JPL/Caltech, ⊙ , 280 (2001) , 513 (2011) 374 Y2013 long-term invitation fellow- , e via the ESA PRODEX Programme. , 177 (1993) 415 [Top] Total gas (left) and dust (right) col- , 1251 (2004) , 1231 (2004) , A&A , edited by D. R. Flower, 233 (1983) 267 353 353 , , , MNRAS A&A the color scale of logM 30, 10, and 5%mass ratio of distribution the map in peak.tours the log at scale [Bottom] the with Gas-to-dust linear con- and ratio 50 (left) of and 500, with thetours 400, dust (right), column 300, to mass indicate 200, map typical con- 100, gas-to-dustvalues mass in ratio the dust barrel structures. Figure 4: umn mass maps of NGC6781 within a 60 6 , 134 (2011) MNRAS MNRAS 141 , AJ , 430 (2006) Planetary Nebulae , 125 (1994) , A20 (2013) 648 92 , , 557 , , L1 (2010) ApJ , 343 (2001) , 435 (1988) ApJS A&A , 58 (2012) 518 323 331 , , , , Macquarie University (2008) 144 , 273 (1985) , , 181 (2005) ApJ A&A AJ , in press 293 , 187 MNRAS , A&A ApJ Ph.D. Thesis A&A Major support for this work was provided by NASA through an aw [2] G. L. Pilbratt, et al., [1] T. Ueta, et al., [8] R. Bachiller, P. J. Huggins, P. Cox, & T. Forveille, [7] J. P. Phillips, G. Ramos-Larios, & M. A. Guerrero, [3] D. J. Frew, [9] D. 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