2013A&A...558A..24B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:28:32

2013A&A...558A..24B - Astronomy and Astrophysics, volume 558A, 24-24 (2013/10-1)

The VLTI/MIDI survey of massive young stellar objects. Sounding the inner regions around intermediate- and high-mass young stars using mid-infrared interferometry.

BOLEY P.A., LINZ H., VAN BOEKEL R., HENNING T., FELDT M., KAPER L., LEINERT C., MUELLER A., PASCUCCI I., ROBBERTO M., STECKLUM B., WATERS L.B.F.M. and ZINNECKER H.

Abstract (from CDS):

Because of inherent difficulties involved in observations and numerical simulations of the formation of massive stars, an understanding of the early evolutionary phases of these objects remains elusive. In particular, observationally probing circumstellar material at distances ≲100AU from the central star is exceedingly difficult, as such objects are rare (and thus, on average, far away) and typically deeply embedded. Long-baseline mid-infrared interferometry provides one way of obtaining the necessary spatial resolution at appropriate wavelengths for studying this class of objects; however, interpreting such observations is often difficult due to sparse spatial-frequency coverage. We aim to characterize the distribution and composition of circumstellar material around young massive stars and to investigate exactly which physical structures in these objects are probed by long-baseline mid-infrared interferometric observations.We used the two-telescope interferometric instrument MIDI of the Very Large Telescope Interferometer of the European Southern Observatory to observe a sample of 24 intermediate- and high-mass young stellar objects in the N band (8-13µm). We had successful fringe detections for 20 objects and present spectrally-resolved correlated fluxes and visibility levels for projected baselines of up to 128m. We fit the visibilities with geometric models to derive the sizes of the emitting regions, as well as the orientation and elongation of the circumstellar material. Fourteen objects in the sample show the 10µm silicate feature in absorption in the total and correlated flux spectra. For 13 of these objects, we were able to fit the correlated flux spectra with a simple absorption model, allowing us to constrain the composition and absorptive properties of the circumstellar material.Nearly all of the massive young stellar objects observed show significant deviations from spherical symmetry at mid-infrared wavelengths. In general, the mid-infrared emission can trace both disks and outflows, and in many cases it may be difficult to disentangle these components on the basis of interferometric data alone, because of the sparse spatial frequency coverage normally provided by current long-baseline interferometers. For the majority of the objects in this sample, the absorption occurs on spatial scales larger than those probed by MIDI. Finally, the physical extent of the mid-infrared emission around these sources is correlated with the total luminosity, albeit with significant scatter.Circumstellar material is ubiquitous at distances ≲100AU around young massive stars. Long-baseline mid-infrared interferometry provides the resolving power necessary for observing this material directly. However, in particular for deeply-embedded sources, caution must be used when attempting to attribute mid-infrared emission to specific physical structures, such as a circumstellar disk or an outflow.

Abstract Copyright:

Journal keyword(s): surveys - stars: massive - techniques: interferometric

VizieR on-line data: <Available at CDS (J/A+A/558/A24): list.dat fits/*>

Simbad objects: 54

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Number of rows : 54

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 V* V376 Cas Ae* 00 11 26.5610557523 +58 50 03.750169804           A3/F2e 95 1
2 RAFGL 490 Y*O 03 27 38.7928323987 +58 47 00.017662871           ~ 339 0
3 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 297 1
4 V* V2254 Ori Or* 05 35 14.11296 -05 22 22.7316           B 286 2
5 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
6 TCC 65 Y*O 05 35 16.32060 -05 23 22.5317           ~ 37 2
7 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1272 1
8 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1466 1
9 NAME Ney-Allen Nebula ISM 05 35 17.1 -05 23 18           ~ 26 0
10 NAME Mon R2 IRS 2 * 06 07 45.83 -06 22 53.5           B0 101 0
11 NAME Mon R2 HII 06 07 46.6 -06 22 59           ~ 650 2
12 NAME Mon R2 IRS 3 Y*O 06 07 47.8 -06 22 55           ~ 134 0
13 NAME Mon R2 IRS 3S IR 06 07 47.836 -06 22 56.29           ~ 9 0
14 NAME Mon R2 IRS 3N IR 06 07 47.855 -06 22 55.49           ~ 8 0
15 NAME SH 2-255 IRS 3 Y*O 06 12 55.03 +17 59 29.9           ~ 15 0
16 V* VY Mon Ae* 06 31 06.9180562526 +10 26 04.982093681 16.65 15.45 13.70 12.49 11.00 A5:Vep 86 0
17 HD 259431 Ae* 06 33 05.1905483916 +10 19 19.987469692 8.39 8.95 8.72     B6ep 261 1
18 V* R Mon Ae* 06 39 09.9538710861 +08 44 09.559404231 10.76 12.46 11.85 10.96 10.25 B8IIIe 501 0
19 RAFGL 989 Y*O 06 41 10.1592954288 +09 29 33.635497596   17.4 16.8 18.26 17.28 B2 241 0
20 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 532 3
21 [FPA77] NGC 3603 IRS 9A IR 11 15 11.34 -61 16 45.2           ~ 18 0
22 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 940 1
23 CD-48 7859 Be* 13 01 17.8016150677 -48 53 18.781347603   10.65 10.58     B5e 42 0
24 OH 305.20 +0.21 Mas 13 11 10.4904 -62 34 38.856           ~ 42 0
25 GAL 305.20+00.21 HII 13 11 11.7 -62 34 44           ~ 25 0
26 RAFGL 4176 IR 13 43 01.704 -62 08 51.23           ~ 87 0
27 [GGB2012] G308.9176+00.1231 HII 13 43 02.1 -62 08 52           ~ 59 0
28 IRAS 13481-6124 Y*O 13 51 37.85568 -61 39 07.5168           ~ 39 0
29 [MHL2007] G332.8256-00.5498 1 HII 16 20 11.184 -50 53 17.52           ~ 10 0
30 IRAS 16164-5046 HII 16 20 14.1 -50 53 20           ~ 26 0
31 CD-42 11721 Be* 16 59 06.7622892572 -42 42 08.404916931 12.16 12.28 11.00     B0IVe 155 1
32 GM 1-24 HII 17 17 04.0 -36 21 14           ~ 45 0
33 IRAS 17216-3801 IR 17 25 06.517 -38 04 00.44           ~ 24 0
34 M 8 HII 18 03 37 -24 23.2           ~ 552 1
35 NAME M 8E IR Y*O 18 04 53.9 -24 26 41           ~ 81 0
36 W 33a Y*O 18 14 39.0 -17 52 03           ~ 584 0
37 NAME HH 80-81 HH 18 19 06 -20 51.4           ~ 194 0
38 NAME HH 80-81 IRS HII 18 19 11.8 -20 47 35           ~ 134 0
39 NAME GGD 27-ILL SFR 18 19 12.00 -20 47 31.1           ~ 16 1
40 2MASS J18191220-2047297 Y*O 18 19 12.21 -20 47 29.7           B1 123 0
41 MSX5C G014.9957-00.6735 IR 18 20 19.7 -16 13 31           ~ 37 2
42 2MASS J18202460-1611394 Y*? 18 20 24.601 -16 11 39.46           ~ 9 0
43 NAME M 17 UC1 HII 18 20 24.82 -16 11 34.9           ~ 47 1
44 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1484 0
45 [MV2004] RS 4 Rad 18 22 26.37 -13 30 11.9           ~ 4 0
46 RAFGL 2136 SFR 18 22 26.8740 -13 30 17.177           ~ 244 0
47 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 266 0
48 EM* MWC 300 Ae* 18 29 25.6915000349 -06 04 37.289920628 12.55 12.67 13.795     B1Ia+[e] 127 0
49 V* R CrA Ae* 19 01 53.6850227874 -36 57 08.145519972 12.781 12.651 11.917 11.242 10.412 B5IIIpe 449 1
50 BD+40 4124 Ae* 20 20 28.2415737117 +41 21 51.527810947 11.11 11.36 10.62 10.510   B2Ve 275 1
51 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 570 0
52 HD 200775 Ae* 21 01 36.9184805541 +68 09 47.770037306 7.34 7.754 7.427 8.13   B2Ve 508 0
53 EM* LkHA 234 Ae* 21 43 06.8214472757 +66 06 54.199354231 13.65 13.61 12.73 11.98 11.20 B5Ve 276 0
54 NAME SH 2-140 IRS 1 Y*O 22 19 18.277 +63 18 45.82           ~ 192 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:28:32

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