J/A+A/618/A186 Dynamic spectra of 10 pulsars (Wang+, 2018)
Jiamusi pulsar observations: II. Scintillations of ten pulsars.
Wang P.F., Han J.L., Han L., Zhang J.H., Li J.Q., Wang C., Han J.,
Wang T., Gao X.Y.
<Astron. Astrophys. 618, A186 (2018)>
=2018A&A...618A.186W 2018A&A...618A.186W (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Pulsars
Keywords: pulsars: general - ISM: general
Abstract:
Pulsars scintillate. Dynamic spectra show brightness variation of
pulsars in the time and frequency domain. Secondary spectra
demonstrate the distribution of fluctuation power in the dynamic
spectra.
Dynamic spectra strongly depend on observational frequencies, but were
often observed at frequencies lower than 1.5GHz. Scintillation
observations at higher frequencies help to constrain the turbulence
feature of the interstellar medium over a wide frequency range and can
detect the scintillations of more distant pulsars.
Ten pulsars were observed at 2250MHz (S-band) with the Jiamusi 66m
telescope to study their scintillations. Their dynamic spectra were
first obtained, from which the decorrelation bandwidths and time
scales of diffractive scintillation were then derived by
autocorrelation. Secondary spectra were calculated by forming the
Fourier power spectra of the dynamic spectra.
Most of the newly obtained dynamic spectra are at the highest
frequency or have the longest time span of any published data for
these pulsars. For PSRs B0540+23, B2324+60 and B2351+61, these were
the first dynamic spectra ever reported. The frequency-dependence of
scintillation parameters indicates that the intervening medium can
rarely be ideally turbulent with a Kolmogorov spectrum. The thin
screen model worked well at S-band for the scintillation of PSR
B1933+16. Parabolic arcs were detected in the secondary spectra of
three pulsars, PSRs B0355+54, B0540+23 and B2154+40, all of which were
asymmetrically distributed. The inverted arclets of PSR B0355+54 were
seen to evolve along the main parabola within a continuous observing
session of 12 hours, from which the angular velocity of the pulsar was
estimated that was consistent with the measurement by very long
baseline interferometry (VLBI).
Description:
10 pulsars (PSRs B0329+54, B0355+54, B0540+23, B0740-28, B1508+55,
B1933+16, B2154+40, B2310+42, B2324+60 and B2351+61) were observed at
2250MHz (S-band) with a bandwidth of about 140MHz by the Jiamusi 66
m telescope from 2015 to 2017. The obtained dynamic spectra have
frequency resolutions of 0.58MHz or 1.17MHz, and time resolutions of
30s, 60s or 90s.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 197 10 Parameters of 10 pulsars are listed together
with frequencies for previous dynamic
spectrum observations
sp/* . 33 Individual spectra
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See also:
http://www.atnf.csiro.au/research/pulsar/psrcat : PSR cat Home page
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- PSR Pulsar name (BHHMM+DD)
10- 14 F5.3 s Per Period
16- 21 F6.2 pc/cm3 DM Dispersion measure
23- 28 F6.2 deg GLON Galactic longitude
30- 35 F6.2 deg GLAT Galactic latitude
37- 41 F5.2 kpc Z Height above the plane
43- 46 F4.2 kpc Dist Distance
48- 51 F4.2 kpc e_Dist rms uncertainty on Dist
52 A1 --- n_Dist [+] Note on Dist (2)
53 A1 --- r_Dist [de] Reference for Dist (1)
55- 57 I3 km/s Vp Transverse velocity
59- 61 I3 km/s e_Vp rms uncertainty on Vp
62 A1 --- n_Vp [+] Note on Vp (2)
63 A1 --- r_Vp [abcdf] Reference for Vp (1)
65- 99 A35 --- Freqs1 Frequencies of previous observations,
nu<2.3GHz
101-108 A8 --- Freqs2 Frequencies of previous observations,
nu≥2.3GHz
110-120 A11 --- FileName1 Name of spectrum file, in subdirectory sp
122-132 A11 --- FileName2 Name of spectrum file, in subdirectory sp
133-142 A10 --- FileName3 Name of spectrum file, in subdirectory sp
144-153 A10 --- FileName4 Name of spectrum file, in subdirectory sp
155-164 A10 --- FileName5 Name of spectrum file, in subdirectory sp
166-175 A10 --- FileName6 Name of spectrum file, in subdirectory sp
177-186 A10 --- FileName7 Name of spectrum file, in subdirectory sp
188-197 A10 --- FileName8 Name of spectrum file, in subdirectory sp
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Note (1): References as follows:
a = Brisken et al. (2002ApJ...571..906B 2002ApJ...571..906B)
b = Chatterjee et al. (2004ApJ...604..339C 2004ApJ...604..339C)
c = Chatterjee et al. (2009ApJ...698..250C 2009ApJ...698..250C)
d = Verbiest et al. (2012ApJ...755...39V 2012ApJ...755...39V)
e = Yao et al. (2017ApJ...835...29Y 2017ApJ...835...29Y)
f = Manchester et al. (2005AJ....129.1993M 2005AJ....129.1993M, Cat. B/psr)
Note (2): Uncertainties are estimated to be 15% of the values from
http://www.atnf.csiro.au/research/pulsar/psrcat/
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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1- 13 F13.8 MHz Freq Channel Frequency
15- 40 F26.20 d MJD Time (1)
42- 51 F10.6 --- Int Normalized intensity
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Note (1): Mean date of observation for each spectrum:
B0329+54 : fig1_1.dat MJD57439; fig1_2.dat MJD57442; fig1_3.dat MJD58065
B0355+54 : fig2_1.dat MJD57254; fig2_2.dat MJD57416; fig2_3.dat MJD57416;
fig2_4.dat MJD58062; fig2_5.dat MJD58066
B0540+23 : fig3_1.dat MJD57198; fig3_2.dat MJD57608; fig3_3.dat MJD58058
B0740-28 : fig4_1.dat MJD57368; fig4_2.dat MJD57413; fig4_3.dat MJD58058
B1508+55 : fig5_1.dat MJD57369; fig5_2.dat MJD58057
B1933+16 : fig6_1.dat MJD57188; fig6_2.dat MJD57436; fig6_3.dat MJD57443;
fig6_4.dat MJD57528; fig6_5.dat MJD57529; fig6_6.dat MJD57530;
fig6_7.dat MJD57531; fig6_8.dat MJD57533;
B2154+40 : fig8_1.dat MJD57412; fig8_2.dat MJD58057; fig8_3.dat MJD58067
B2310+42 : fig9_1.dat MJD57223; fig9_2.dat MJD58051
B2324+60 : fig10_1.dat MJD57841; fig10_2.dat MJD58061
B2351+61 : fig11_1.dat MJD57191; fig11_2.dat MJD57610
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Acknowledgements:
PengFei Wang & JinLin Han, pfwang(at)nao.cas.cn, hjl(at)nao.cas.cn
References:
Han et al., Paper I 2016MNRAS.456.3413H 2016MNRAS.456.3413H
(End) PengFei Wang [NAOC, China], Patricia Vannier [CDS] 23-Aug-2018