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J/ApJ/743/54      Polarization around star-forming regions    (Targon+, 2011)

Correlating the interstellar magnetic field with protostellar jets and its sources. Targon C.G., Rodrigues C.V., Cerqueira A.H., Hickel G.R. <Astrophys. J., 743, 54 (2011)> =2011ApJ...743...54T
ADC_Keywords: YSOs ; Magnetic fields ; Polarization Keywords: Herbig-Haro objects - ISM: jets and outflows - ISM: magnetic fields - stars: formation - techniques: polarimetric Abstract: This paper combines new CCD polarimetric data with previous information about protostellar objects in a search for correlations involving the interstellar magnetic field (ISMF). Specifically, we carried out an optical polarimetric study of a sample of 28 fields of 10'x10' located in the neighborhood of protostellar jets and randomly spread over the Galaxy. The polarimetry of a large number of field stars is used to estimate both the average and dispersion of the ISMF direction in each region. The results of the applied statistical tests are as follows. Concerning the alignment between the jet direction and the ISMF, the whole sample does not show alignment. There is, however, a statistically significant alignment for objects of Classes 0 and I. Regarding the ISMF dispersion, our sample presents values slightly larger for regions containing T Tauri objects than for those harboring younger protostars. Moreover, the ISMF dispersion in regions containing high-mass objects tends to be larger than in those including only low-mass protostars. In our sample, the mean interstellar polarization as a function of the average interstellar extinction in a region reaches a maximum value around 3% for A(V)=5, after which it decreases. Our data also show a clear correlation of the mean value of the interstellar polarization with the dispersion of the ISMF: the larger the dispersion, the smaller the polarization. Based on a comparison of our and previous results, we suggest that the dispersion in regions forming stars is larger than in quiescent regions. Description: This catalog presents the polarimetry of field stars in 28 regions in the direction of Herbig-Haro objects. The table includes the position and R band polarization of many objects in each field. The field number is presented in the first column. The identification number of a given object in each field is presented in the second column. The observations were carried out in 1998 December 18, between 2005 February 11 and 17, and on 2007 May 7, with the 0.60m Boller & Chivens telescope at the Observatorio do Pico dos Dias, Brazil, operated by the Laboratorio Nacional de Astrofisica, Brazil. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 76 28 Star-forming region or cloud in the direction of each field table4.dat 49 4872 Polarimetry of field stars in each field
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Field Field number 4- 76 A73 --- Region Region designation
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Field Field number 3 A1 --- m_Field [AB] Multiplicity index on Field 5- 7 I3 --- ID Identification of the object in the field 9- 10 I2 h RAh Hour of Right Ascension (B1950) 12- 13 I2 min RAd Minute of Right Ascension (B1950) 15- 19 F5.2 s RAs Second of Right Ascension (B1950) 21 A1 --- DE- Sign of the Declination (B1950) 22- 23 I2 deg DEd Degree of Declination (B1950) 25- 26 I2 arcmin DEm Arcminute of Declination (B1950) 28- 32 F5.2 arcsec DEs Arcsecond of Declination (B1950) 34- 38 F5.2 % P Linear polarization 40- 43 F4.2 % e_P Error in P 45- 49 F5.1 deg PA Position angle of the polarization
Acknowledgements: Claudia V. Rodrigues, claudiavilega(at)
(End) Claudia V. Rodrigues [INPE], Patricia Vannier [CDS] 24-Feb-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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