2017ApJ...840...72L


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST12:00:40

2017ApJ...840...72L - Astrophys. J., 840, 72-72 (2017/May-2)

Systematic analysis of spectral energy distributions and the dust opacity indices for Class 0 young stellar objects.

LI J.I.-H., LIU H.B., HASEGAWA Y. and HIRANO N.

Abstract (from CDS):

We are motivated by the recent measurements of dust opacity indices (β) around young stellar objects (YSOs), which suggest that efficient grain growth may have occurred earlier than the Class I stage. The present work makes use of abundant archival interferometric observations at submillimeter, millimeter, and centimeter wavelength bands to examine grain growth signatures in the dense inner regions (<1000 au) of nine Class 0 YSOs. A systematic data analysis is performed to derive dust temperatures, optical depths, and dust opacity indices based on single-component modified blackbody fittings to the spectral energy distributions (SEDs). The fitted dust opacity indices (β) are in a wide range of 0.3-2.0 when single-component SED fitting is adopted. Four out of the nine observed sources show β lower than 1.7, the typical value of the interstellar dust. Low dust opacity index (or spectral index) values may be explained by the effect of dust grain growth, which makes β1.7. Alternatively, the very small observed values of β may be interpreted by the presence of deeply embedded and hot inner disks, which only significantly contribute to the observed fluxes at long wavelength bands. This possibility can be tested by the higher angular resolution imaging observations of ALMA or more detailed sampling of SEDs in the millimeter and centimeter bands. The β values of the remaining five sources are close to or consistent with 1.7, indicating that grain growth would start to significantly reduce the values of β no earlier than the late Class 0 stage for these YSOs.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): evolution - radio continuum: stars - stars: formation - submillimeter: stars - submillimeter: stars

Simbad objects: 23

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Number of rows : 23

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 IRAS 03222+3034 Y*O 03 25 22.32 +30 45 13.9           ~ 128 0
2 JCMTSE J032536.1+304514 Y*O 03 25 36.22 +30 45 15.7           ~ 107 0
3 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 244 1
4 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 314 0
5 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 408 3
6 BD+30 547 Y*O 03 28 57.2107612240 +31 14 19.076624755   10.73 9.98 9.1   G4V 96 1
7 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 94 1
8 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 626 1
9 [JCC87] IRAS 4A1 Y*O 03 29 10.510 +31 13 31.01           ~ 84 1
10 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 470 0
11 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 276 0
12 [HRF2005] 3 PoC 03 33 21.3 +31 07 27           ~ 66 0
13 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 87 0
14 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1131 0
15 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1251 0
16 LDN 1527 DNe 04 39 53 +25 45.0           ~ 526 0
17 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 121 0
18 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3156 1
19 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
20 DCld 001.6+03.8 DNe 17 35 47.50 -25 32 59.0           ~ 56 0
21 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 241 2
22 HH 375 Y*O 20 39 06.2 +68 02 15           ~ 166 0
23 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 505 0

    Equat.    Gal    SGal    Ecl

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2021.04.18-12:00:40

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