2022A&A...663A.116W


Query : 2022A&A...663A.116W

2022A&A...663A.116W - Astronomy and Astrophysics, volume 663A, 116-116 (2022/7-1)

Pulsar scintillation studies with LOFAR. I. The census.

WU Z., VERBIEST J.P.W., MAIN R.A., GRIESSMEIER J.-M., LIU Y., OSLOWSKI S., MOOCHICKAL AMBALAPPAT K., BAK NIELSEN A.-S., KUNSEMOLLER J., DONNER J.Y., TIBURZI C., PORAYKO N., SERYLAK M., KUNKEL L., BRUGGEN M. and VOCKS C.

Abstract (from CDS):


Context. Interstellar scintillation (ISS) of pulsar emission can be used both as a probe of the ionized interstellar medium (IISM) and cause corruptions in pulsar timing experiments. Of particular interest are so-called scintillation arcs which can be used to measure time-variable interstellar scattering delays directly, potentially allowing high-precision improvements to timing precision.
Aims. The primary aim of this study is to carry out the first sizeable and self-consistent census of diffractive pulsar scintillation and scintillation-arc detectability at low frequencies, as a primer for larger-scale IISM studies and pulsar-timing related propagation studies with the LOw-Frequency ARray (LOFAR) High Band Antennae (HBA).
Methods. We use observations from five international LOFAR stations and the LOFAR core in the Netherlands. We analyze the 2D auto-covariance function of the dynamic spectra of these observations to determine the characteristic bandwidth and timescale of the ISS toward the pulsars in our sample and investigate the 2D power spectra of the dynamic spectra to determine the presence of scintillation arcs.
Results. In this initial set of 31 sources, 15 allow for the full determination of the scintillation properties; nine of these show detectable scintillation arcs at 120-180 MHz. Eight of the observed sources show unresolved scintillation; and the final eight do not display diffractive scintillation. Some correlation between scintillation detectability and pulsar brightness and a dispersion measure is apparent, although no clear cut-off values can be determined. Our measurements across a large fractional bandwidth allow a meaningful test of the frequency scaling of scintillation parameters, uncorrupted by influences from refractive scintillation variations.
Conclusions. Our results indicate the powerful advantage and great potential of ISS studies at low frequencies and the complex dependence of scintillation detectability on parameters such as pulsar brightness and interstellar dispersion. This work provides the first installment of a larger-scale census and longer-term monitoring of ISS effects at low frequencies.

Abstract Copyright: © ESO 2022

Journal keyword(s): pulsars: general - ISM: clouds

Simbad objects: 31

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Number of rows : 31
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 PSR B0031-07 Psr 00 34 08.9100 -07 21 56.000           ~ 322 0
2 PSR J0034-05 Psr 00 34 21.8281 -05 34 36.620           ~ 182 0
3 PSR B0320+39 Psr 03 23 26.6619 +39 44 52.403           ~ 129 0
4 PSR B0329+54 Psr 03 32 59.3370698592 +54 34 45.028206408           ~ 644 1
5 PSR B0809+74 Psr 08 14 59.500 +74 29 05.70           ~ 405 0
6 PSR B0823+26 Psr 08 26 51.5068 +26 37 21.297           ~ 512 1
7 PSR B0834+06 Psr 08 37 05.642 +06 10 14.56           ~ 437 0
8 PSR B0919+06 Psr 09 22 14.1600 +06 38 28.800           ~ 292 0
9 PSR B0943+10 Psr 09 46 07.31 +09 51 57.3           ~ 340 1
10 PSR B0950+08 Psr 09 53 09.2970 +07 55 36.400           ~ 755 2
11 PSR J1012+5307 Psr 10 12 33.4345449600 +53 07 02.548542576     19.5     DA 378 1
12 PSR B1133+16 Psr 11 36 03.0720 +15 51 15.500           ~ 668 0
13 PSR B1237+25 Psr 12 39 40.386 +24 53 49.87           ~ 466 0
14 PSR B1257+12 Psr 13 00 03.1075 +12 40 55.155           ~ 517 1
15 PSR B1508+55 Psr 15 09 25.7 +55 31 33           ~ 300 1
16 PSR B1534+11 Psr 15 37 09.9603 +11 55 55.554           ~ 429 1
17 PSR B1604-00 Psr 16 07 12.1 -00 32 41           ~ 215 0
18 PSR B1642-03 Psr 16 45 02.0330 -03 17 57.200           ~ 363 0
19 PSR B1737+13 Psr 17 40 07.3455 +13 11 56.690           ~ 175 0
20 PSR B1855+09 Psr 18 57 36.390620 +09 43 17.20712           DA 529 1
21 PSR B1919+21 Psr 19 21 44.815 +21 53 02.25           ~ 383 0
22 PSR B1929+10 Psr 19 32 14.0570 +10 59 33.380           ~ 753 0
23 PSR J1959+2048 Psr 19 59 36.7643141520 +20 48 14.896407996   21.08 20.16 19.53 18.79 G: 805 3
24 PSR B2016+28 Psr 20 18 03.8999255016 +28 39 54.940329468           ~ 355 0
25 PSR B2020+28 Psr 20 22 37.0671 +28 54 23.104           ~ 306 1
26 PSR B2021+51 Psr 20 22 49.8730 +51 54 50.233           ~ 265 1
27 PSR B2045-16 Psr 20 48 35.7700 -16 16 47.000           ~ 318 0
28 PSR B2110+27 Psr 21 13 04.3506 +27 54 01.160           ~ 103 0
29 PSR B2217+47 Psr 22 19 48.139 +47 54 53.93           ~ 219 0
30 PSR B2310+42 Psr 23 13 08.5976 +42 53 12.987           ~ 135 0
31 PSR B2327-20 Psr 23 30 26.9740 -20 05 29.500           ~ 123 0

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