2011A&A...532A.109G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:49:13

2011A&A...532A.109G - Astronomy and Astrophysics, volume 532A, 109-109 (2011/8-1)

Mid-infrared interferometry of the massive young stellar object NGC 2264 IRS 1.

GRELLMANN R., RATZKA T., KRAUS S., LINZ H., PREIBISCH T. and WEIGELT G.

Abstract (from CDS):

The optically invisible infrared-source NGC 2264 IRS 1 lying north of the Cone Nebula is thought to be a massive young stellar object (∼10M). Although strong infrared excess clearly shows that the central object is surrounded by large amounts of circumstellar material, no information about the spatial distribution of this circumstellar material has been available until now. We used the ESO Very Large Telescope Interferometer to perform long-baseline interferometric observations of NGC 2264 IRS 1 in the mid-infrared regime. Our observations resolve the circumstellar material around NGC 2264 IRS 1, provide the first direct measurement of the angular size of the mid-infrared emission, and yield direct constraints on the spatial distribution of the dust. We analyze the spectrally dispersed interferometric data taken with MIDI at two different position angles and baseline lengths. We use different approaches (a geometrical model, a temperature-gradient model, and radiative transfer models) to jointly model the observed interferometric visibilities and the spectral energy distribution. The derived visibility values between ∼0.02 and ∼0.3 show that the mid-infrared emission is clearly resolved. The characteristic size of the MIR-emission region is ∼30-60AU; this value is typical for other YSOs with similar or somewhat lower luminosities. A comparison of the sizes for the two position angles shows a significant elongation of the dust distribution. Simple spherical envelope models are therefore inconsistent with the data. The radiative transfer modeling of our data suggests that we observe a geometrically thin and optically thick circumstellar disk with a mass of about 0.1M. Our modeling indicates that NGC 2264 IRS 1 is surrounded by a flat circumstellar disk that has properties similar to disks typically found around lower-mass young stellar objects. This result supports the assumption that massive young stellar objects form via accretion from circumstellar disks.

Abstract Copyright:

Journal keyword(s): techniques: interferometric - stars: individual: NGC 2264 IRS 1 - stars: formation - circumstellar matter

Simbad objects: 30

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Number of rows : 30

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 * bet Col PM* 05 50 57.5921991 -35 46 05.915211 5.49 4.28 3.12 2.27 1.69 K1III_CN+1 133 0
5 HD 259431 Ae* 06 33 05.1905483916 +10 19 19.987469692 8.39 8.95 8.72     B6ep 261 1
6 NAME Mon I MoC 06 35 +10.1           ~ 214 0
7 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
8 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1587 1
9 NAME Cone Nebula DNe 06 41.1 +09 53           ~ 74 1
10 RAFGL 989 Y*O 06 41 10.1592954288 +09 29 33.635497596   17.4 16.8 18.26 17.28 B2 241 0
11 HD 48217 PM* 06 41 56.3857394576 -09 10 03.123066225   6.717 5.194     K5III 38 0
12 * 17 Mon * 06 47 19.8294628711 +08 02 14.123889454 7.82 6.17 4.77 3.74 3.04 K4III 110 0
13 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 532 3
14 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1757 0
15 [FPA77] NGC 3603 IRS 9A IR 11 15 11.34 -61 16 45.2           ~ 18 0
16 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 940 1
17 IRAS 13481-6124 Y*O 13 51 37.85568 -61 39 07.5168           ~ 39 0
18 NAME M 8E IR Y*O 18 04 53.9 -24 26 41           ~ 81 0
19 W 33a Y*O 18 14 39.0 -17 52 03           ~ 584 0
20 NAME M 17 SW SFR 18 20 23.1 -16 11 43           ~ 249 0
21 RAFGL 2136 SFR 18 22 26.8740 -13 30 17.177           ~ 244 0
22 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 266 0
23 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 396 0
24 BD+40 4124 Ae* 20 20 28.2415737117 +41 21 51.527810947 11.11 11.36 10.62 10.510   B2Ve 275 1
25 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 570 0
26 HD 200775 Ae* 21 01 36.9184805541 +68 09 47.770037306 7.34 7.754 7.427 8.13   B2Ve 508 0
27 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
28 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 634 2
29 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 589 0
30 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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2020.07.04-21:49:13

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