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J/MNRAS/436/3557   HTRU survey: long-period pulsars polarimetry (Tiburzi+, 2013)

The High Time Resolution Universe survey. IX. Polarimetry of long-period pulsars. Tiburzi C., Johnston S., Bailes M., Bates S.D., Bhat N.D.R., Burgay M., Burke-Spolaor S., Champion D., Coster P., D'Amico N., Keith M.J., Kramer M., Levin L., Milia S., Ng C., Possenti A., Stappers B.W., Thornton D., van Straten W. <Mon. Not. R. Astron. Soc., 436, 3557-3572 (2013)> =2013MNRAS.436.3557T (SIMBAD/NED BibCode)
ADC_Keywords: Pulsars ; Polarization Keywords: magnetic fields - polarization - methods: observational - pulsars: general Abstract: We present a polarimetric analysis of 49 long-period pulsars discovered as part of the High Time Resolution Universe (HTRU) southern survey. The sources exhibit the typical characteristics of 'old' pulsars, with low fractional linear and circular polarization and narrow, multi-component profiles. Although the position angle swings are generally complex, for two of the analysed pulsars (J1622-3751 and J1710-2616) we obtained an indication of the geometry via the rotating vector model. We were able to determine a value of the rotation measure (RM) for 34 of the sources which, when combined with their dispersion measures (DM), yields an integrated magnetic field strength along the line of sight. With the data presented here, the total number of values of RM associated with pulsars discovered during the HTRU southern survey sums to 51. The RMs are not consistent with the hypothesis of a counter-clockwise direction of the Galactic magnetic field within an annulus included between 4 and 6kpc from the Galactic Centre. A partial agreement with a counter-clockwise sense of the Galactic magnetic field within the spiral arms is, however, found in the area of the Carina-Sagittarius arm. Description: We present the polarization analysis of a sample of 49 long-period pulsars, whose spin periods range from a few hundred milliseconds to about two and a half seconds. They were all discovered during the mid-latitude part of the HTRU survey (Keith et al. 2010MNRAS.409..619K; Bates et al. 2012MNRAS.427.1052B) apart from PSR J1846-4249 (that has been discovered in the high latitude survey and it will be presented in one of the next papers of the HTRU series). After discovery and confirmation, the pulsars were followed-up with the third Parkes Digital Filterbank, observing them for at least one year to allow the determination of a complete timing solution. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 102 34 Pulsars for which RM can be determined table2.dat 102 15 Pulsars for which no RM can be determined
See also: J/MNRAS/423/1351 : Energy distribution in pulsars (Burke-Spolaor+, 2012) J/MNRAS/450/2922 : HTRU survey new pulsars (Ng+, 2015) Byte-by-byte Description of file: table1.dat table2.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name Name (JHHMM+DDMM) 12- 16 F5.3 s P Spin period 18- 20 I3 ms W10 Profile width at 10 per cent 22- 24 I3 ms W50 Profile width at 50 per cent 26- 29 F4.1 [-] LogdE/dt Logarithm of the spin-down luminosity 31- 34 F4.2 mJy S0 Total intensity flux 36- 38 F3.2 mJy e_S0 rms uncertainty on S0 (3sigma) 40- 43 F4.1 % L Percentage of the linear polarisation 45- 47 F3.1 % e_L rms uncertainty on L (1sigma) 49- 52 F4.1 % V Percentage of the circular polarisation 54- 56 F3.1 % e_V rms uncertainty on V (1sigma) 58- 61 F4.1 % |V| Absolute value of percentage of the circular polarisation 63- 65 F3.1 % e_|V| rms uncertainty on |V| (1sigma) 67- 70 I4 rad/m2 RM ?=- Rotation measure 72- 73 I2 rad/m2 e_RM ?=- rms uncertainty on RM (1sigma) 75- 80 F6.2 pc/cm3 DM Dispersion measure (decimal values for corrected values from erratum) (2) 81- 84 F4.2 pc/cm3 e_DM ? rms uncertainty on DM for corrected values from erratum (2) 86- 89 F4.2 kpc Dist ? DM derived distance (1) 91- 96 F6.3 uG <B||> ?=- Average value of the magnetic field along the line of sight 98-100 F3.1 [-] logtauC logarithm of the characteristic age 102 A1 --- Corr [*] * for corrected values (2)
Note (1): DM derived distance from the Sun (via the NE2001 electron density model from Cordes & Lazio (2002, preprint (astro-ph/020715), that gives uncertainties up to about 30 per cent). Note (2): DM, RM, and <B||> updated from erratum (2014, MNRAS, 445, 3009).
History: From electronic version of the journal References: Keith et al., Paper I 2010MNRAS.409..619K Bates et al., Paper II 2011MNRAS.416.2455B Burke-Spolaor et al., Paper III 2011MNRAS.416.2465B Keith et al., Paper IV 2012MNRAS.419.1752K Burke-Spolaor et al., Paper V 2012MNRAS.423.1351B, Cat. J/MNRAS/423/1351 Bates et al., Paper VI 2012MNRAS.427.1052B Burgay et al., Paper VII 2013MNRAS.433..259B Levin et al., Paper VIII 2013MNRAS.434.1387L Barr et al., Paper IX 2013MNRAS.435.2234B Ng et al., Paper X 2014MNRAS.439.1865N Bates et al., Paper XI 2015MNRAS.446.4019B Ng et al., Paper XII 2015MNRAS.450.2922N, Cat. J/MNRAS/450/2922
(End) Patricia Vannier [CDS] 20-Nov-2017
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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