1998ApJ...509..299L


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.25CEST01:34:22

1998ApJ...509..299L - Astrophys. J., 509, 299-308 (1998/December-2)

350 micron continuum imaging of the Orion A molecular cloud with the submillimeter high angular resolution camera.

LIS D.C., SERABYN E., KEENE J., DOWELL C.D., BENFORD D.J., PHILLIPS T.G., HUNTER T.R. and WANG N.

Abstract (from CDS):

We have used the Submillimeter High Angular Resolution Camera (SHARC) bolometer camera at the Caltech Submillimeter Observatory to map the distribution of the broadband 350 µm continuum emission toward the Orion A molecular cloud. A comparison of the 350 µm flux densities in OMC-1 with previous 1100 µm measurements indicates a strong spatial variation of the grain emissivity exponent, β. The lowest value of the exponent (β ≃ 1.75) is found toward the Orion Bar photon-dominated region (PDR), while the highest value (β ≃ 2.5) is found toward the Orion Ridge north of IRc2. This variation is consistent with the destruction of grain mantles by the UV photons from the Trapezium cluster. The observed spatial variation of β in OMC-1 suggests that the long-wavelength grain emissivity may also vary significantly in GMC cores on small linear scales (≲0.5 pc), affecting H2 column density and mass estimates. The 350 µm continuum emission in the Orion Bar region correlates well with the CO (6-5) peak brightness temperature and is shifted by ∼10" from the molecular component traced by the 13CO (6-5) emission. This indicates that the 350 µm dust emission in this region originates predominantly in the outer high-temperature PDR layers. Several filamentary structures previously detected in molecular tracers are also seen in our map at flux levels comparable to those seen in the Bar. Over 30 compact dust sources are detected in the OMC-2 and OMC-3 clouds, including a dozen sources not previously known. The average 350/1300 µm flux ratio based on our data and previous observations of this region (63 ±19) indicates low dust temperatures (17±4 K, assuming β = 2) for most of the sources. The brightest 350 µm source in OMC-3 has a low 350/1300 µm ratio (∼23), indicating a very low dust temperature (∼10 K), or a significant opacity at 350 µm (∼2.5). This source appears to be a deeply embedded and cold young protostar. A comparison of the mass estimate for the OMC-2/3 filament based on the 350 µm continuum emission with previous C18O mass estimates indicates a relatively high grain emissivity, Q(350) = 4x10–4, in this region.

Abstract Copyright:

Journal keyword(s): ISM: Dust, Extinction - Infrared: ISM: Continuum - ISM: Clouds - ISM: individual (OMC-1, OMC-2) - ISM: Individual: Alphanumeric: OMC-3 - Stars: Formation

Nomenclature: Table 1: [LSK98] NN (Nos 1-33).

Status at CDS:  

CDS comments: T.1: MMS = [CRW97] OMC-3 MMS, FIR = [MWZ90] OMC-2 FIR

Simbad objects: 45

goto Full paper

goto View the reference in ADS

Number of rows : 45

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1007 2
2 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 569 1
3 NGC 1977 SFR 05 35 16.0 -04 49 15           ~ 184 0
4 V* V2282 Ori Or* 05 35 16.15536 -05 00 02.5848           ~ 18 0
5 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1269 1
6 IRAS 05328-0501 IR 05 35 16.6 -04 59 24           ~ 4 0
7 [TSO2008] 8 Rad 05 35 17.1 -05 00 03           ~ 3 0
8 [TSO2008] 9 mm 05 35 18.030 -05 00 17.77           ~ 17 0
9 [TUK93] 3 Y*O 05 35 18.32712 -05 00 32.9400           ~ 54 2
10 HOPS 91 Y*O 05 35 18.98 -05 00 51.6           ~ 29 0
11 V* V2358 Ori Or* 05 35 19.82376 -05 15 35.3304           ~ 19 0
12 2MASS J05351997-0501024 Y*O 05 35 19.97 -05 01 02.5           ~ 28 0
13 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 217 1
14 V* V2364 Ori Or* 05 35 20.1521915741 -05 13 15.688010752   20.263 18.348   12.859 K5-M0e 46 0
15 JCMTSF J053521.2-051450 Y*? 05 35 21.3 -05 14 54           ~ 7 0
16 HOY J053521.34-051319.5 cor 05 35 21.4 -05 13 14           ~ 24 0
17 COUP 1177 * 05 35 21.9324343914 -05 14 27.604633212 18.870 17.039 15.800   12.960 M2-3 33 0
18 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 710 0
19 [TSO2008] 13 Y*O 05 35 22.4451 -05 01 14.123           ~ 39 1
20 [TSO2008] 21 Rad 05 35 22.9 -05 06 41           ~ 2 0
21 2MASS J05352332-0507096 Y*O 05 35 23.326 -05 07 09.66           ~ 14 0
22 [TSO2008] 34 IR 05 35 23.4 -05 12 36           ~ 11 0
23 [TSO2008] 23 IR 05 35 23.4 -05 07 32           ~ 14 0
24 2MASS J05352341-0512023 Y*O 05 35 23.417 -05 12 02.34           ~ 21 0
25 [TSO2008] 14 mm 05 35 23.420 -05 01 30.35           ~ 57 0
26 [SMD2014] 083.8513-05.1419 Y*O 05 35 24.2999 -05 08 30.686           ~ 43 0
27 [TSO2008] 24 Y*? 05 35 24.6 -05 07 53           ~ 23 0
28 [TSO2008] 33 Rad 05 35 24.7 -05 12 33           ~ 2 0
29 [TSO2008] 25 Rad 05 35 25.0 -05 08 19           ~ 2 0
30 NAME OMC 2 IRS 3 HII 05 35 26.00 -05 10 16.6           ~ 61 0
31 [TSO2008] 18 mm 05 35 26.0 -05 05 42           ~ 37 1
32 [TSO2008] 32 Rad 05 35 26.3 -05 12 23           ~ 2 0
33 [TSO2008] 27 Rad 05 35 26.4 -05 08 25           ~ 2 0
34 JCMTSF J053526.4-050521 mm 05 35 26.5 -05 05 17           ~ 22 1
35 IRAS 05329-0505 Y*O 05 35 26.746 -05 03 55.08           ~ 70 0
36 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 110 0
37 OMC 2 MoC 05 35 27 -05 10.1           ~ 380 1
38 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 70 0
39 V* V419 Ori Or* 05 35 28.1422985224 -05 10 13.849253883     15.46   12.95 M2e 50 0
40 TKK 870 Y*O 05 35 28.19 -05 03 41.2           ~ 34 0
41 [SKN2015] AzTEC-Ori 337 cor 05 35 29.4 -04 58 31           ~ 13 0
42 [TSO2008] 6 Rad 05 36 13.9 -04 59 29           ~ 3 0
43 NAME Ori A MoC 05 38 -07.1           ~ 2661 0
44 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1481 0
45 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 693 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 1998ApJ...509..299L and select 'bookmark this link' or equivalent in the popup menu


2020.05.25-01:34:22

© Université de Strasbourg/CNRS

    • Contact