2015A&A...578A..82C


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.22CET02:46:45

2015A&A...578A..82C - Astronomy and Astrophysics, volume 578A, 82-82 (2015/6-1)

VLT near- to mid-IR imaging and spectroscopy of the M17 UC1-IRS5 region.

CHEN Z., NUERNBERGER D.E.A., CHINI R., JIANG Z. and FANG M.

Abstract (from CDS):

We investigate the surroundings of the hypercompact HII region M17 UC1 to probe the physical properties of the associated young stellar objects and the environment of massive star formation. We use diffraction-limited near-IR (VLT/NACO) and mid-IR (VLT/VISIR) images to reveal the different morphologies at various wavelengths. Likewise, we investigate the stellar and nebular content of the region with VLT/SINFONI integral field spectroscopy with a resolution R∼1500 at H+K bands. Five of the seven point sources in this region show L-band excess emission. A geometric match is found between the H2 emission and near-IR polarized light in the vicinity of IRS5A, and between the diffuse mid-IR emission and near-IR polarization north of UC1. The H2 emission is typical for dense photodissociation regions (PDRs), which are initially far-ultraviolet pumped and repopulated by collisional de-excitation. The spectral types of IRS5A and B273A are B3-B7 V/III and G4-G5 III, respectively. The observed infrared luminosity LIR in the range 1-20µm is derived for three objects; we obtain 2.0x103L for IRS5A, 13L for IRS5C, and 10L for B273A. IRS5 might be a young quadruple system. Its primary star IRS5A is confirmed to be a high-mass protostellar object (∼9M, ∼1x105yrs); it might have terminated accretion due to the feedback from stellar activities (radiation pressure, outflow) and the expanding HII region of M17. The object UC1 might also have terminated accretion because of the expanding hypercompact HII region, which it ionizes. The disk clearing process of the low-mass young stellar objects in this region might be accelerated by the expanding HII region. The outflows driven by UC1 are running south-north with its northeastern side suppressed by the expanding ionization front of M17; the blue-shifted outflow lobe of IRS5A is seen in two types of tracers along the same line of sight in the form of H2 emission filament and mid-emission. The H2 line ratios probe the properties of M17 SW PDR, which is confirmed to have a clumpy structure with two temperature distributions: warm, dense molecular clumps with nH>105cm–3 and T≃575K and cooler atomic gas with nH∼3.7x103-1.5x104cm–3 and T∼50-200K.

Abstract Copyright:

Journal keyword(s): stars: early-type - stars: individual: M17 UC1 - ISM: individual objects: M17 SW - photon-dominated region (PDR) - stars: formation

Nomenclature: Fig. 1, Table 2: [CNC2015] B273A (Nos B273A-B273B), [CNC2015] IRS5A (Nos IRS5A-IRS5E).

Simbad objects: 36

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Number of rows : 36

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * 53 Ari bC* 03 07 25.6726547580 +17 52 47.971172068 5.18 5.997 6.117     B1.5V 133 1
2 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1727 1
3 HD 36166 V* 05 29 54.7755487007 +01 47 21.323228963 4.74 5.562 5.745     B2V 112 0
4 NAME Orion S reg 05 35 12.9 -05 24 10           ~ 123 0
5 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 737 0
6 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 576 1
7 HD 94481 * 10 54 17.7767264404 -13 45 28.935298555   6.487 5.651     G4III-IIIb 55 0
8 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 466 0
9 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 666 1
10 * 61 UMa PM* 11 41 03.0159358291 +34 12 05.882438337 6.31 6.08 5.34 4.73 4.38 G8V 572 0
11 HD 110621 PM* 12 43 43.2212558894 -44 40 31.556081512   10.34 9.92     Fpw 68 0
12 * d Sco PM* 16 18 17.9001656 -28 36 50.476788   4.804 4.782     A1Va 149 0
13 HD 161743 * 17 48 57.9259632149 -38 07 07.504425479   7.67 7.20     B9IV 17 0
14 Cl* NGC 6618 B 358 * 18 20 21.3567619124 -16 09 59.556740122           O8V 11 0
15 NAME M 17 SW SFR 18 20 23.1 -16 11 43           ~ 251 0
16 [CNC2015] IRS5C IR 18 20 24.54 -16 11 41.2           ~ 1 0
17 [CNC2015] IRS5B IR 18 20 24.54 -16 11 39.0           ~ 1 0
18 [CW98] IRS 5 IR 18 20 24.6 -16 11 40           ~ 15 1
19 [CNC2015] IRS5A IR 18 20 24.60 -16 11 39.4           ~ 3 0
20 [CNC2015] IRS5D IR 18 20 24.63 -16 11 40.7           ~ 1 0
21 [CNC2015] IRS5E IR 18 20 24.69 -16 11 40.5           ~ 1 0
22 NAME M 17 UC1 HII 18 20 24.82 -16 11 34.9           ~ 48 1
23 [CNC2015] B273A IR 18 20 25.08 -16 11 34.4           ~ 1 0
24 2MASS J18202508-1611339 Y*O 18 20 25.083 -16 11 33.99           ~ 8 0
25 [CNC2015] B273B IR 18 20 25.14 -16 11 34.6           ~ 1 0
26 Cl* NGC 6618 CEN 64 * 18 20 25.71 -16 11 41.7           A7V 1 0
27 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1500 0
28 HD 169990 V* 18 27 56.4798185292 -17 48 01.272766319   6.176 6.182     B8III/IV 42 0
29 HD 171207 PM* 18 35 16.5954100686 -41 12 14.305911681   10.02 9.35     G2V 6 0
30 HD 173994 * 18 50 41.3750131446 -47 46 47.082996760 6.21 6.910 7.059     B2IV 33 0
31 2MASS J19014805-3657219 Y*O 19 01 48.056 -36 57 21.95           ~ 97 0
32 CHLT 3 * 19 01 48.10 -36 57 22.7           K6V 30 0
33 HD 179029 * 19 12 34.5412903219 -37 31 26.533195308   7.22 7.15     B5V 16 0
34 HD 188112 HS* 19 54 31.4192112333 -28 20 20.679022097   10.01 10.22     sdB 81 0
35 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2348 1
36 * 18 Peg * 22 00 07.9274510425 +06 43 02.812464798 5.31 5.88 6.00     B3III 103 0

    Equat.    Gal    SGal    Ecl

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2021.01.22-02:46:45

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