2018A&A...616A.139G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:23:09

2018A&A...616A.139G - Astronomy and Astrophysics, volume 616A, 139-139 (2018/8-1)

SMA observations of polarized dust emission in solar-type Class 0 protostars: Magnetic field properties at envelope scales.

GALAMETZ M., MAURY A., GIRART J.M., RAO R., ZHANG Q., GAUDEL M., VALDIVIA V., KETO E. and LAI S.-P.

Abstract (from CDS):


Aims. Although from a theoretical point of view magnetic fields are believed to play a significant role during the early stages of star formation, especially during the main accretion phase, the magnetic field strength and topology is poorly constrained in the youngest accreting Class 0 protostars that lead to the formation of solar-type stars.
Methods. We carried out observations of the polarized dust continuum emission with the SMA interferometer at 0.87mm to probe the structure of the magnetic field in a sample of 12 low-mass Class 0 envelopes in nearby clouds, including both single protostars and multiple systems. Our SMA observations probed the envelope emission at scales ∼600-5000au with a spatial resolution ranging from 600 to 1500au depending on the source distance.
Results. We report the detection of linearly polarized dust continuum emission in all of our targets with average polarization fractions ranging from 2% to 10% in these protostellar envelopes. The polarization fraction decreases with the continuum flux density, which translates into a decrease with the H2 column density within an individual envelope. Our analysis show that the envelope-scale magnetic field is preferentially observed either aligned or perpendicular to the outflow direction. Interestingly, our results suggest for the first time a relation between the orientation of the magnetic field and the rotational energy of envelopes, with a larger occurrence of misalignment in sources in which strong rotational motions are detected at hundreds to thousands of au scales. We also show that the best agreement between the magnetic field and outflow orientation is found in sources showing no small-scale multiplicity and no large disks at ∼100au scales.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - circumstellar matter - ISM: magnetic fields - polarization - techniques: polarimetric

Simbad objects: 51

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Number of rows : 51

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 7C 0059+5808 QSO 01 02 45.76238248 +58 24 11.1366009   20.09 19.22 18.57 17.90 ~ 189 1
2 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3545 3
3 LDN 1448 DNe 03 22.5 +30 35           ~ 466 0
4 NAME LDN 1448 IRS 2 Y*O 03 25 22.32 +30 45 13.9           ~ 117 0
5 LDN 1448NW Y*? 03 25 35.66 +30 45 34.2           ~ 59 0
6 [SDA2014] West8 Y*O 03 25 36.22 +30 45 15.7           ~ 98 0
7 SSTc2d J032536.4+304522 Y*O 03 25 36.49 +30 45 22.2           ~ 186 1
8 IRAS 03225+3034 IR 03 25 36.49 +30 45 22.2           ~ 149 1
9 NAME LDN 1448-mm Y*O 03 25 38.83 +30 44 06.2           ~ 301 0
10 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 390 3
11 NAME HH 7-11 MMS 3 smm 03 29 01.964 +31 15 38.04           ~ 50 0
12 NAME HH 7-11 MMS 2 smm 03 29 03.056 +31 15 51.67           ~ 64 0
13 [SVS76] NGC 1333 13A smm 03 29 03.73 +31 16 03.8           ~ 43 0
14 V* V512 Per Or* 03 29 03.7567945196 +31 16 03.959183877           ~ 348 0
15 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 332 0
16 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 81 1
17 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 596 1
18 [JCC87] IRAS 4A1 Y*O 03 29 10.510 +31 13 31.01           ~ 74 1
19 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1219 1
20 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 553 0
21 [JCC87] IRAS 4B2 smm 03 29 12.8 +31 13 02           ~ 7 0
22 IRAS 03282+3035 cor 03 31 20.98 +30 45 30.1           ~ 160 0
23 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1061 0
24 HH 797A HH 03 43 55.51 +32 04 15.2           ~ 14 0
25 [PZR2014b] IC 348-SMM2E Y*O 03 43 57.73 +32 03 10.1           ~ 21 0
26 [CAZ2013] IC 348 MMS2 smm 03 43 57.73 +32 03 10.5           ~ 6 0
27 IC 348 OpC 03 44 34 +32 09.8           ~ 1227 1
28 LDN 1527 DNe 04 39 53 +25 45.0           ~ 495 0
29 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 480 0
30 [MCK88] NGC 2024 FIR 5 cor 05 41 44.6 -01 55 38           ~ 91 0
31 ICRF J092703.0+390220 Sy1 09 27 03.0139516273 +39 02 20.847968628   17.17 17.00 16.486   ~ 932 1
32 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5320 1
33 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2704 2
34 QSO B1514-24 BLL 15 17 41.8135246339 -24 22 19.482167214   15.13 14.00 13.95   ~ 645 3
35 QSO B1622-297 QSO 16 26 06.02083867 -29 51 26.9710860   18.41 20.5 17.6   ~ 364 0
36 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
37 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1035 1
38 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 178 0
39 NAME IRAS 16293-2422A Y*O 16 32 22.869 -24 28 36.11           ~ 107 0
40 4C 09.57 BLL 17 51 32.81857318 +09 39 00.7284829   17.46 16.78 15.57   ~ 811 1
41 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 236 2
42 NAME Aql Rift DNe 18 32 -01.0           ~ 234 1
43 ICRF J192748.4+735801 Sy1 19 27 48.4944745594 +73 58 01.571908984     15.5 15.11   ~ 491 2
44 HH 119A HH 19 36 51.57 +07 34 10.4           ~ 8 0
45 LDN 663 DNe 19 36 55 +07 34.4           ~ 555 0
46 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 484 0
47 LDN 1177 DNe 21 17 38.62 +68 17 34.0           ~ 81 1
48 [LNW2010] CB 230-IRS2 smm 21 17 39.9 +68 17 36           ~ 5 0
49 [LNW2010] CB 230-IRS1 smm 21 17 39.9 +68 17 36           ~ 6 0
50 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2506 2
51 [BC86b] LDN 1448 IRS 2A IR ~ ~           ~ 3 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-07:23:09

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