2010MNRAS.405.2179P


Query : 2010MNRAS.405.2179P

2010MNRAS.405.2179P - Mon. Not. R. Astron. Soc., 405, 2179-2205 (2010/July-2)

Spitzer mid-infrared observations of seven bipolar planetary nebulae.

PHILLIPS J.P. and RAMOS-LARIOS G.

Abstract (from CDS):

We have investigated the mid-infrared (MIR) and visual structures of seven bipolar planetary nebulae (BPNe), using imaging and spectroscopy acquired using the Spitzer Space Telescope (SST), and the Observatorio Astronomico Nacional in Mexico. The results show that the sources are more extended towards longer MIR wavelengths, as well as having higher levels of surface brightness in the 5.8- and 8.0-µm bands. It is also noted that the 5.8µm/4.5µm and 8.0µm/4.5µm flux ratios increase with increasing distance from the nuclei of the sources. All of these latter trends may be attributable to emission by polycyclic aromatic hydrocarbons (PAHs) and/or warm dust continua within circumnebular photodissociation regions (PDRs). A corresponding decrease in the flux ratios 8.0µm/5.8µm may, by contrast, arise due to changes in the properties of the PAH emitting grains. We note evidence for 8.0µm ring-like structures in the envelope of NGC 2346, located in a region beyond the minor axis limits of the ionized envelope. An analysis of the inner two rings shows that whilst they have higher surface brightnesses at longer MIR wavelengths, they are relatively stronger (compared to underlying emission) at 3.6 and 4.5µm. There is also evidence for point-reflection symmetry along the major axis of the outflow. Finally, the fall-off in surface brightness along the nebular minor axis suggests that progenitor mass-loss rates were more-or-less constant. NGC 6905 shows evidence for a centrally located and unresolved MIR emission excess. We show that whilst flux ratios are inconsistent with stellar and ionized gas components of emission, the emission can be explained in terms of shock-excited H2, or grain continuum and PAH emission bands. We provide the deepest image so far published of the outer visual structure of NGC 6445, and compare these results with Spitzer imaging at 8.0µm. The distributions are quite distinct, and may indicate collimation of the outer ionized emission by a cylindrical PDR. We finally note that the MIR colours of the lobes and nuclei of the sources are radically different. It is also shown that 3.6-µm emission in BPNe differs from that for the generality of planetary nebulae. We discuss various mechanisms which may contribute to these differences of colour.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): (ISM:) planetary nebulae: general - ISM: jets and outflows - photodissociation region (PDR) - infrared: ISM

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 M 76 PN 01 42 19.6557728208 +51 34 31.534970052     17.48   17.69 DOZ 368 2
2 NGC 2346 PN 07 09 22.5215800440 -00 48 23.610997332   11.76 11.58     A5V 565 0
3 PN ARO 121 PN 07 57 51.6169237320 +53 25 16.950484848   16.775 17.128 17.288 17.501 DQ 158 1
4 NGC 2818A PN 09 16 01.4901525600 -36 37 37.516376856           ~ 227 1
5 NGC 3242 PN 10 24 46.1335521792 -18 38 32.296857792   11.83 12.15     ~ 814 1
6 V* V Hya C* 10 51 37.2615873024 -21 15 00.333928044   12.23 6.80 7.42   C-N:6 355 0
7 NGC 3699 PN 11 27 57.70 -59 57 28.0   10 13.00     ~ 91 1
8 PN Mz 1 PN 15 34 16.6410983544 -59 09 08.105422716   12.8 13.10     ~ 119 0
9 NGC 6072 PN 16 12 58.3635385680 -36 13 47.395106184     12.10     ~ 169 0
10 PN M 2-9 PN 17 05 37.96152 -10 08 32.5068           ~ 516 0
11 NGC 6445 PN 17 49 15.21 -20 00 34.5   18.9       ~ 290 0
12 M 57 PN 18 53 35.0967659112 +33 01 44.883287544   15.405 15.769 15.901 16.062 DA(O?) 818 2
13 NGC 6781 PN 19 18 28.085 +06 32 19.29     11.8     ~ 258 0
14 NGC 6905 PN 20 22 22.9919225472 +20 06 16.285052088   16.3 14.5     [WC3] 340 0
15 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 859 1
16 NGC 7354 PN 22 40 19.8733664208 +61 17 08.746685772           ~ 273 1

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2023.01.28-11:59:31

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