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 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 2010MNRAS.409..619K; Bates et al. 2012MNRAS.427.1052B 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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 ugauss <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)
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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).
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History:
From electronic version of the journal
References:
Keith et al., Paper I 2010MNRAS.409..619K 2010MNRAS.409..619K
Bates et al., Paper II 2011MNRAS.416.2455B 2011MNRAS.416.2455B
Burke-Spolaor et al., Paper III 2011MNRAS.416.2465B 2011MNRAS.416.2465B
Keith et al., Paper IV 2012MNRAS.419.1752K 2012MNRAS.419.1752K
Burke-Spolaor et al., Paper V 2012MNRAS.423.1351B 2012MNRAS.423.1351B, Cat. J/MNRAS/423/1351
Bates et al., Paper VI 2012MNRAS.427.1052B 2012MNRAS.427.1052B
Burgay et al., Paper VII 2013MNRAS.433..259B 2013MNRAS.433..259B
Levin et al., Paper VIII 2013MNRAS.434.1387L 2013MNRAS.434.1387L
Barr et al., Paper IX 2013MNRAS.435.2234B 2013MNRAS.435.2234B
Ng et al., Paper X 2014MNRAS.439.1865N 2014MNRAS.439.1865N
Bates et al., Paper XI 2015MNRAS.446.4019B 2015MNRAS.446.4019B
Ng et al., Paper XII 2015MNRAS.450.2922N 2015MNRAS.450.2922N, Cat. J/MNRAS/450/2922
(End) Patricia Vannier [CDS] 20-Nov-2017