J/ApJ/914/122 Stellar polarimetry with Gaia DR2 data (Doi+, 2021)
Two-component magnetic field along the line of sight to the Perseus molecular
cloud: contribution of the foreground Taurus molecular cloud.
Doi Y., Hasegawa T., Bastien P., Tahani M., Arzoumanian D., Coude S.,
Matsumura M., Sadavoy S., Hull C.L.H., Shimajiri Y., Furuya R.S.,
Johnstone D., Plume R., Inutsuka S.-I., Kwon J., Tamura M.
<Astrophys. J., 914, 122 (2021)>
=2021ApJ...914..122D 2021ApJ...914..122D
ADC_Keywords: Polarization; Cross identifications; Stars, distances; Reddening;
Magnetic fields; Optical; Infrared
Keywords: Interstellar clouds ; Starlight polarization ;
Interstellar magnetic fields ; Polarimetry
Abstract:
Optical stellar polarimetry in the Perseus molecular cloud direction
is known to show a fully mixed bimodal distribution of position angles
across the cloud. We study the Gaia trigonometric distances to each of
these stars and reveal that the two components in position angles
trace two different dust clouds along the line of sight. One
component, which shows a polarization angle of -37.6±35.2 and a
higher polarization fraction of 2.0±1.7%, primarily traces the
Perseus molecular cloud at a distance of 300pc. The other component,
which shows a polarization angle of +66.8±19.1 and a lower
polarization fraction of 0.8±0.6%, traces a foreground cloud at a
distance of 150pc. The foreground cloud is faint, with a maximum
visual extinction of ≤1mag. We identify that foreground cloud as the
outer edge of the Taurus molecular cloud. Between the Perseus and
Taurus molecular clouds, we identify a lower-density ellipsoidal dust
cavity with a size of 100-160pc. This dust cavity is located at
l=170°, b=-20°, and d=240pc, which corresponds to an HI shell
generally associated with the Per OB2 association. The two-component
polarization signature observed toward the Perseus molecular cloud can
therefore be explained by a combination of the plane-of-sky
orientations of the magnetic field both at the front and at the back
of this dust cavity.
Description:
We use optical polarimetry of 88 sources in the direction of the
Perseus molecular cloud observed by Goodman+ (1990ApJ...359..363G 1990ApJ...359..363G).
The passband of the observations were centered at 762.5nm with a
bandwidth of 245nm.
We also use NIR polarimetry data taken toward NGC 1333 in the Perseus
molecular cloud, as shown in the inset of Figure 1. We use K-band
polarimetry by Tamura+ (1988MNRAS.231..445T 1988MNRAS.231..445T), (14 sources) and R- and
J-band polarimetry by Alves+ (2011AJ....142...33A 2011AJ....142...33A) (33 sources).
We estimate the B-field orientation measured in submillimeter dust
emission by using Planck data at 353GHz (Planck Col. 2020A&A...641A..12P 2020A&A...641A..12P).
See Section 2.2.
We estimate the stellar distances by using Gaia astrometry data
(DR2, I/345) and use SIMBAD positions to cross-match the stars in the
Gaia catalog. See Section 2.3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 118 143 Cross-matching results between stellar polarimetry
data and the Gaia catalog
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
J/ApJ/646/1009 : Structures of dust in Perseus molecular cloud (Kirk+, 2006)
J/ApJS/182/143 : SCUPOL Legacy polarimetry of SCUBA (Matthews+, 2009)
J/ApJ/723/1019 : Galactic SFR and gas surface densities (Heiderman+, 2010)
J/A+A/584/A91 : Dense cores in Aquila from Herschel (Konyves+, 2015)
J/MNRAS/459/342 : Dense cores in Taurus L1495 cloud (Marsh+, 2016)
J/A+A/587/A106 : Perseus dust opt. depth and column density maps (Zari+, 2016)
J/ApJ/865/73 : GOBELINS. V. Kinematics of Perseus (Ortiz-Leon+, 2018)
J/A+A/614/A100 : Molecular clouds los magnetic field structure (Tahani+, 2018)
J/A+A/625/A135 : Gal. interstellar dust Gaia-2MASS 3D maps (Lallement+, 2019)
J/A+A/621/A48 : Gaia extended kinematical maps. I. (Lopez-Corredoira+, 2019)
J/A+A/624/L8 : Starlight polarization (Panopoulou+, 2019)
J/ApJ/872/56 : R-band linear polarization of Gaia stars (Panopoulou+, 2019)
J/ApJ/904/172 : Properties of dense cores in Cepheus (Di Francesco+, 2020)
J/A+A/638/A85 : 3D view of Taurus with Gaia & Herschel (Roccatagliata+, 2020)
J/A+A/645/A55 : Catalogue of cold cores in Perseus (Pezzuto+, 2021)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 1 I1 --- Ref [1/4] Reference number (1)
3- 4 I2 --- No [1/88] Source number in each reference
6- 13 F8.5 deg RAdeg [50.89/57.3] Right Ascension (ICRS)
at Epoch=2015.5
15- 22 F8.5 deg DEdeg [29.9/33] Declination (ICRS) at Epoch=2015.5
24- 28 F5.2 % Pol [0.02/18.5] Stellar polarization, percentage
30- 33 F4.2 % e_Pol [0.02/3.51] Uncertainty in Pol
35- 39 F5.1 deg PA [-87/87] Position angle of B-field orientation
41- 42 I2 deg e_PA [0/52] Uncertainty in PA
44- 61 I18 --- GaiaDR2 Gaia DR2 source identification
63- 69 F7.1 pc Dist [-7713/9365]? Distance, 1000/parallax
71- 79 F9.1 pc E_Dist [-301576/18642]? Upper uncertainty on Dist
81- 87 F7.1 pc e_Dist [-6529/11237]? Lower uncertainty on Dist
89- 94 F6.4 mag AG [0.008/3]? Reddening in Gaia G band
(from Gaia DR2)
96-102 F7.4 mag E_AG [0.05/1.2]? Upper uncertainty in AG
104-110 F7.4 mag e_AG [-0.5/-0.004]? Lower uncertainty in AG
112-116 F5.2 --- RUWE [0.7/44.1] Renormalised Unit Weight Error;
(∼1.0=good fit for single-star model;
See section 2.3)
118-118 I1 --- Flag [0/1] Bad flag (1=bad) (2)
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Note (1): References as follows:
1 = Optical (Goodman et al. 1990ApJ...359..363G 1990ApJ...359..363G, Table 3;
<[GBM90] Per NN> in Simbad);
2 = R-band (Alves et al. 2011AJ....142...33A 2011AJ....142...33A, Table 5;
<[AAG2011] NN> in Simbad);
3 = J-band (Alves et al. 2011AJ....142...33A 2011AJ....142...33A, Table 5;
<[AAG2011] NN> in Simbad);
4 = K-band (Tamura et al. 1988MNRAS.231..445T 1988MNRAS.231..445T, Table 2;
<[SVS76] NGC 1333 NN> in Simbad).
Note (2): Bad flag of 1 indicates that the data entry is discarded from the
analysis in this paper because of its large RUWE (>1.4), non-reliable
Gaia parallax (NA or negative values), or erroneous identification
(Gmag>15mag for data by Goodman et al. 1990ApJ...359..363G 1990ApJ...359..363G).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Dec-2022