2015ApJ...814...54A


Query : 2015ApJ...814...54A

2015ApJ...814...54A - Astrophys. J., 814, 54 (2015/November-3)

SOFIA/FORCAST observations of warm dust in S106: a fragmented environment.

ADAMS J.D., HERTER T.L., HORA J.L., SCHNEIDER N., LAU R.M., STAGUHN J.G., SIMON R., SMITH N., GEHRZ R.D., ALLEN L.E., BONTEMPS S., CAREY S.J., FAZIO G.G., GUTERMUTH R.A., GUZMAN FERNANDEZ A., HANKINS M., HILL T., KETO E., KOENIG X.P., KRAEMER K.E., MEGEATH S.T., MIZUNO D.R., MOTTE F., MYERS P.C. and SMITH H.A.

Abstract (from CDS):

We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 µm), IRTF/MIRLIN (11.3 and 12.5 µm), and Herschel/PACS (70 and 160 µm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is ≳(9.02±1.01)x104 L, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼75-90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.

Abstract Copyright:

Journal keyword(s): circumstellar matter - H ii regions - infrared: stars - radiative transfer - stars: formation

Nomenclature: Table 2: [AHH2015] CL N (Nos CL 1-Cl 7), [AHH2015] WL N (Nos WL 1-WL 3), [AHH2015] SL N (Nos SL 1-SL 3), [AHH2015] PL N (No PL 1).

Simbad objects: 29

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Number of rows : 29
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 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 634 1
2 EM* SR 3 Y*O 16 26 09.3229222944 -24 34 12.172009728   10.9 9.88   9.01 A0 116 0
3 [AHH2015] PL 1 FIR 20 27 23.84 +37 21 37.8           ~ 1 0
4 [GGC82] IRS 1 IR 20 27 25.16 +37 22 33.4           ~ 3 0
5 [AHH2015] SL 3 FIR 20 27 25.25 +37 22 21.0           ~ 1 0
6 [GGC82] IRS 2 IR 20 27 25.46 +37 22 58.0           ~ 5 0
7 [GGC82] IRS 3 PoC 20 27 25.75 +37 22 42.3           ~ 16 1
8 [AHH2015] CL 7 FIR 20 27 25.80 +37 22 51.2           ~ 1 0
9 [AHH2015] SL 1 FIR 20 27 25.96 +37 22 28.8           ~ 1 0
10 [AHH2015] SL 2 FIR 20 27 26.46 +37 22 35.8           ~ 1 0
11 NAME SH 2-106 IR Y*O 20 27 26.502 +37 22 42.03           ~ 163 1
12 SH 2-106 HII 20 27 26.8 +37 22 49           ~ 440 1
13 [GGC82] IRS 5 IR 20 27 26.87 +37 22 57.2           ~ 4 0
14 [GGC82] IRS 6 PoC 20 27 27.02 +37 22 27.1           ~ 4 0
15 [AHH2015] CL 1 FIR 20 27 27.03 +37 22 50.5           ~ 1 0
16 [AHH2015] CL 2 FIR 20 27 27.11 +37 22 41.0           ~ 1 0
17 [AHH2015] CL 3 FIR 20 27 27.39 +37 22 45.4           ~ 1 0
18 [GGC82] IRS 7 IR 20 27 27.45 +37 22 38.9           ~ 3 0
19 [GGC82] IRS 8 IR 20 27 27.54 +37 23 00.7           ~ 3 0
20 [AHH2015] WL 1 FIR 20 27 27.61 +37 22 39.4           ~ 1 0
21 [AHH2015] CL 5 FIR 20 27 27.67 +37 22 53.1           ~ 1 0
22 [AHH2015] CL 4 FIR 20 27 27.69 +37 22 31.6           ~ 1 0
23 [AHH2015] WL 2 FIR 20 27 27.82 +37 22 48.9           ~ 1 0
24 [AHH2015] CL 6 FIR 20 27 28.25 +37 22 54.1           ~ 1 0
25 [AHH2015] WL 3 FIR 20 27 28.33 +37 22 48.1           ~ 1 0
26 NAME Cyg X BL? 20 30 04.7973633 +40 51 36.002197           ~ 841 1
27 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 702 0
28 NAME Cave Nebula RNe 22 13 27 +70 15.3           ~ 55 0
29 * bet Peg LP* 23 03 46.45746 +28 04 58.0336 6.05 4.09 2.42 0.92 -0.40 M2.5II-III 593 1

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