J/MNRAS/474/4629 Polarimetry of 600 pulsars from 1.4GHz obs. (Johnston+, 2018)
Polarimetry of 600 pulsars from observations at 1.4 GHz with the
Parkes radio telescope.
Johnston S., Kerr M.
<Mon. Not. R. Astron. Soc., 474, 4629-4636 (2018)>
=2018MNRAS.474.4629J 2018MNRAS.474.4629J (SIMBAD/NED BibCode)
ADC_Keywords: Pulsars ; Radio sources ; Polarization
Keywords: astronomical data bases: miscellaneous - pulsars: general
Abstract:
Over the past 13yr, the Parkes radio telescope has observed a large
number of pulsars using digital filter bank backends with high time
and frequency resolution and the capability for Stokes recording.
Here, we use archival data to present polarimetry data at an observing
frequency of 1.4GHz for 600 pulsars with spin-periods ranging from
0.036 to 8.5s. We comment briefly on some of the statistical
implications from the data and highlight the differences between
pulsars with high and low spin-down energy. The data set, images and
table of properties for all 600 pulsars are made available in a public
data archive maintained by the CSIRO.
Description:
The observations span a time period from 2004 November to 2017
February and data were taken from the public Data Archive Portal
(Hobbs et al. 2011; http://data.csiro.au). A total of 600 pulsars were
used for this work, many of them observed multiple times.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 142 600 Pulsar polarization properties at 1.4 GHz
fits/* . 602 Individual fits files in psrfits format
fig/* . 600 Individual figures
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See also:
http://data.csiro.au : CSIRO Home Page
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Name, JHHMM+DDMM
12- 17 F6.1 ms Per Spin period
19- 24 F6.1 pc/cm2 DM Dispersion measure
26- 32 F7.1 rad/m2 RM Rotation measure
34- 37 F4.1 10-7W dE/dt Spin down energy
39- 42 I4 --- Nbin Number of bin
44- 47 F4.2 mJy rms rms noise
49- 55 F7.2 mJy S1.4 ?=0 Flux density at 1.4GHz
57- 62 F6.1 deg W50 Width of the profile at 50 per cent of the peak
64- 69 F6.1 % L/I Percentage of linear polarization
71- 76 F6.1 % V/I Percentage of circular polarization
78- 83 F6.1 % |V|/I Percentage of the absolute value of the
circular polarization
85- 89 F5.1 % e_|V|/I rms uncertainty on |V|/I
91- 92 A2 --- Flag Flag (1)
94-119 A26 --- FileName Name of the fits file in subdirectory fits
121-142 A22 --- Fig Name of the png file in subdirectory fig (2)
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Note (1): Flag as follows:
W = pulsar has a peak flux density less than 15 times the rms; W50 and the
fractional polarization values should be treated with caution.
R = pulsar for which we could obtain no RM either because the pulsar is weak
or the fractional linear polarization is intrinsically low. The RM is
set to zero for these cases.
S = pulsar showing strong (clearly visible by eye) scatter-broadening of the
profile due to the interstellar medium. In this case, the true pulse
width will be smaller than the measured width and the measured
fractional polarization will be lower than the true value.
N = pulsars that are not flux calibrated
I = pulsars with an interpulse
NR = pulsar for which we could obtain no RM either because the pulsar is weak
or the fractional linear polarization is intrinsically low and
no flux calibrated.
SI = pulsar showing strong (clearly visible by eye) scatter-broadening of the
profile due to the interstellar medium and interpulse
SR = pulsar showing strong (clearly visible by eye) scatter-broadening of the
profile due to the interstellar medium and pulsar for which we could
obtain no RM either because the pulsar is weak or the fractional linear
polarization is intrinsically low.
WI = pulsar has a peak flux density less than 15 times the rms and interpulse
WN = pulsar has a peak flux density less than 15 times the rms and
no flux calibrated
WR = pulsar has a peak flux density less than 15 times the rms and for which
we could obtain no RM
WS = pulsar has a peak flux density less than 15 times the rms and showing
strong (clearly visible by eye) scatter-broadening of the profile due
to the interstellar medium
Note (2): Figures for pulsar in ull polarization.
In the lower panel, the black line denotes Stokes I, the red trace shows the
linear polarization and the blue trace the circular polarization.
Left-hand circular polarization is defined to be positive.
The top panel shows the position angle of the linear polarization, corrected
to infinite frequency using the RM listed in the table.
Position angles are only plotted when the linear polarization
exceeds 3σ.
The zero-point of pulse longitude is set to the peak of the total
intensity profile
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Mar-2021