2013A&A...553A...2O


Query : 2013A&A...553A...2O

2013A&A...553A...2O - Astronomy and Astrophysics, volume 553A, 2-2 (2013/5-1)

Probing the role of polycyclic aromatic hydrocarbons in the photoelectric heating within photodissociation regions.

OKADA Y., PILLERI P., BERNE O., OSSENKOPF V., FUENTE A., GOICOECHEA J.R., JOBLIN C., KRAMER C., ROELLIG M., TEYSSIER D. and VAN DER TAK F.F.S.

Abstract (from CDS):

We observationally investigate the relation between the photoelectric heating efficiency in photodissociation regions (PDRs) and the charge of polycyclic aromatic hydrocarbons (PAHs), which are considered to play a key role in photoelectric heating. Using PACS onboard Herschel, we observed six PDRs spanning a wide range of far-ultraviolet radiation fields (G0=100-105). To measure the photoelectric heating efficiency, we obtained the intensities of the main cooling lines in these PDRs, i.e., the [Oi] 63µm, 145µm, and [Cii] 158µm, as well as the far-infrared (FIR) continuum intensity. We used Spitzer/IRS spectroscopic mapping observations to investigate the mid-infrared (MIR; 5.5-14µm) PAH features in the same regions. We decomposed the MIR PAH emission into that of neutral (PAH0) and positively ionized (PAH+) species to derive the fraction of the positively charged PAHs in each region, and compare it to the photoelectric heating efficiency. The heating efficiency traced by ([Oi] 63µm + [Oi] 145µm + [Cii] 158µm)/TIR, where TIR is the total infrared flux, ranges between 0.1% and 0.9% in different sources, and the fraction of PAH+ relative to (PAH0+ PAH+) spans from 0 (+11)% to 87 (±10)%. All positions with a high PAH+ fraction show a low heating efficiency, and all positions with a high heating efficiency have a low PAH+ fraction, supporting the scenario in which a positive grain charge results in a decreased heating efficiency. Theoretical estimates of the photoelectric heating efficiency show a stronger dependence on the charging parameter γ=G0 T1/2/ne than the observed efficiency reported in this study, and the discrepancy is significant at low γ. The photoelectric heating efficiency on PAHs, traced by ([Oi] 63µm + [Oi] 145µm + [Cii] 158µm)/(PAH-band emission + [Oi] 63µm + [Oi] 145µm + [Cii] 158µm), shows a much better match between the observations and the theoretical estimates. The good agreement of the photoelectric heating efficiency on PAHs with a theoretical model indicates the dominant contribution of PAHs to the photoelectric heating. This study demonstrates the fundamental role that PAHs have in photoelectric heating. More studies of their charging behavior are crucial to understand the thermal balance of the interstellar medium.

Abstract Copyright:

Journal keyword(s): HII regions - ISM: lines and bands - photon-dominated region (PDR)

CDS comments: Fig.1 PDR 1 not in Simbad

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 5838 1
2 * sig Ori Y*O 05 38 44.7653828520 -02 36 00.283179888 2.54 3.58 3.79 3.87 4.11 O9.5V+B0.2V(n) 801 0
3 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 511 0
4 LDN 1630 DNe 05 45.5 -00 59           ~ 381 0
5 NAME Mon R2 IRS 4 * 06 07 45.25 -06 23 19.9           ~ 18 0
6 NAME Mon R2 IRS 2 * 06 07 45.83 -06 22 53.5           B0 111 0
7 NAME Mon R2 IRS 1 cor 06 07 46.20 -06 23 09.5           B0 64 0
8 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 742 2
9 NAME Mon R2 IRS 3 Y*O 06 07 47.8 -06 22 55           ~ 142 0
10 Cl Trumpler 14 OpC 10 43 56.6 -59 33 11   5.70 5.5     ~ 509 0
11 Cl Trumpler 16 OpC 10 45 00.7 -59 42 00           ~ 484 0
12 NGC 3372 HII 10 45 02.23 -59 41 59.8           ~ 1014 2
13 LDN 1721 DNe 16 14 28.1 -18 54 44           ~ 25 0
14 W 49n HII 19 10 13.2 +09 06 12           ~ 469 3
15 W 49 SFR 19 10 20 +09 07.7           ~ 575 1
16 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 702 0
17 HD 200775 Ae* 21 01 36.9205762896 +68 09 47.789578836 7.34 7.754 7.427 8.13   B2Ve 557 0
18 BD+69 1231 Y*O 22 13 24.5285030448 +70 15 05.081570064   9.41 9.29     B9.5V 47 2
19 NAME Cave Nebula RNe 22 13 27 +70 15.3           ~ 55 0

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