J/MNRAS/511/4669 Study of galactic PSRs mainly from ATNF (Kutukcu+, 2022)
Distances of galactic radio pulsars first quadrant -2° < l < 90°
and -2° < b < 2°.
Kutukcu P., Ankay A., Yazgan E., Bozkurt K.
<Mon. Not. R. Astron. Soc. 511, 4669-4684 (2022)>
=2022MNRAS.511.4669K 2022MNRAS.511.4669K (SIMBAD/NED BibCode)
ADC_Keywords: Pulsars ; Milky Way ; Radio sources ; Positional data ;
Rotational velocities ; Stars, ages ; Stars, distances
Keywords: methods: statistical - stars: distances - stars: neutron -
H II regions - ISM: structure - Galaxy: structure
Abstract:
Distance versus dispersion measure relations are constructed for
Galactic radio pulsars in small solid angle intervals. The
calculations are based on some basic criteria, as well as using the
independent distance measurements of well examined pulsars for the
first Galactic quadrant, including Galactic central directions. Values
of average free electron density for these regions are derived from
the fits to distance versus dispersion measure relations and checked
for consistency and smoothness. The effects of plasma in the Galactic
arms and within the central parts of the Galactic bulge region are
also compared and discussed. Our adopted distances for the radio
pulsars are compared with the ones given in some other models. Some
basic results on distributions of the radio pulsars and the plasma are
presented.
Description:
Since the first observation of a PSR in 1967, more than 2800 PSRs were
observed up to date according to the Australia Telescope National
Facility Pulsar Catalog (ATNFPC; Manchester et al.
2005AJ....129.1993M 2005AJ....129.1993M, Cat. B/psr). Most of these PSRs are observable at
radio frequencies due to their synchrotron emission. In this work, we
present an improved version of a basic and reliable method to
determine distances of all radio PSRs with known dispersion measure
(DM) values based on constructing distance-DM relations (Ankay et al.
2016SerAJ.193....1A 2016SerAJ.193....1A). It is possible to derive average-free electron
densities in the line of sight (LOS) of the radio PSRs from these
relations to constrain the distributions of the plasma, as well as the
radio PSRs in the Galaxy, (i.e see Introduction section).
Some basic criteria based on observational results are listed to
construct distance versus DM relations (Ankay et al.
2016SerAJ.193....1A 2016SerAJ.193....1A). We assume that the main contribution to the
measured DM values is mainly due to the plasma in the H II regions,
SNRs, and probably the Galactic central region. A low-density plasma
distribution between the Galactic arms and at high latitudes are also
taken into consideration. When adopting distances for PSRs in each
solid angle interval independent distance measurements for them like
trigonometric parallax and associations with SNRs or stellar clusters
are also taken into consideration, (i.e see section 2).
Using the results of such measurements and making comparisons between
PSRs in each group, data lead to improved values of both distance and
uncertainty in distance. The data used are mainly l, b, DM, RM and
τ, and some of the other data displayed in the each dedicated
solid angle interval subsections 3.1-3.21 and in tablea1-a20.dat. In
these tables we collect data from ATNFPC and the ones adopted and
calculated in this study are shown in separate columns.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 132 30 Radio PSRs measurements in solid angle interval
2° < l < 6° & -2 < b < 2°
tablea2.dat 132 26 Radio PSRs measurements in solid angle interval
6° < l < 10° & -2° < b < 2°
tablea3.dat 132 27 Radio PSRs measurements in solid angle interval
10° < l < 14° & -2° < b < 2°
tablea4.dat 132 28 Radio PSRs measurements in solid angle interval
14° < l < 18° & -2° < b < 2°
tablea5.dat 132 32 Radio PSRs measurements in solid angle interval
18° < l < 22° & -2° < b < 2°
tablea6.dat 132 41 Radio PSRs measurements in solid angle interval
22° < l < 26° & -2° < b < 2°
tablea7.dat 130 50 Radio PSRs measurements in solid angle interval
26° < l < 30° & -2° < b < 2°
tablea8.dat 132 31 Radio PSRs measurements in solid angle interval
30° < l < 34° & -2° < b < 2°
tablea9.dat 132 47 Radio PSRs measurements in solid angle interval
34° < l < 38° & -2° < b < 2°
tablea10.dat 130 55 Radio PSRs measurements in solid angle interval
38° < l < 42° & -2° < b < 2°
tablea11.dat 132 40 Radio PSRs measurements in solid angle interval
42° < l < 46° & -2° < b < 2°
tablea12.dat 130 21 Radio PSRs measurements in solid angle interval
46° < l < 50° & -2° < b < 2°
tablea13.dat 132 27 Radio PSRs measurements in solid angle interval
50° < l < 54° & -2° < b < 2°
tablea14.dat 132 19 Radio PSRs measurements in solid angle interval
54° < l < 58° & -2° < b < 2°
tablea15.dat 132 14 Radio PSRs measurements in solid angle interval
58° < l < 62° & -2° < b < 2°
tablea16.dat 132 9 Radio PSRs measurements in solid angle interval
62° < l < 66° & -2° < b < 2°
tablea17.dat 132 11 Radio PSRs measurements in solid angle interval
66° < l < 70° & -2° < b < 2°
tablea18.dat 132 5 Radio PSRs measurements in solid angle interval
70° < l < 74° & -2° < b < 2°
tablea19.dat 132 4 Radio PSRs measurements in solid angle interval
74° < l < 78° & -2° < b < 2°
tablea20.dat 132 3 *Radio PSRs measurements in solid angle interval
78° < l < 90° & -2° < b < 2°
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Note on tablea20.dat: The last distance in kpc with value D = 2.2 &
errD [+0.36,-0.32] are from parallax in Deller et al. 2019ApJ...875..100D 2019ApJ...875..100D.
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See also:
J/ApJ/783/130 : Parallaxes of high mass star forming regions (Reid+, 2014)
J/A+A/569/A125 : Spiral structure of the Milky Way (Hou+, 2014)
J/ApJS/212/2 : Giant molecular clouds in the 4th Galactic quadrant
(Garcia+, 2014)
VII/284 : A Catalogue of Galactic Supernova Remnants (Green, 2019)
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
Byte-by-byte Description of file: tablea?.dat tablea??.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PSR Pulsar name designation (PSR JHHMM±DDMMA)
13- 18 F6.3 deg GLON Galactic longitude of the pulsar (b)
20- 25 F6.3 deg GLAT Galactic latitude of the pulsar (l)
27- 36 F10.5 pc/cm3 DM Radio PSRs dispersion measure expressed as
in the equation 2 of the section
Introduction (DM)
38- 45 F8.5 pc/cm3 e_DM Mean error of DM (errorDM)
47- 55 F9.3 rad/m2 RM ? The pulsar rotation measure RM expressed
as in the equation 3 of the section
Introduction (RM)
57- 63 F7.1 rad/m2 e_RM ? Mean error of RM (errorRM)
65- 75 F11.5 Myr tau ? Characteristic ages τ of the PSRs
expressed as in the equation 7 of the
section 2 in this work (τ)
77- 84 F8.4 --- RM/DM ? The ratio of RM/DM (RM/DM)
86- 93 F8.4 kpc D ? Adopted and computed pulsar distance in
this study (d)
95- 99 F5.2 kpc E_D ? Upper mean error of D
101- 105 F5.2 kpc e_D ? Lower mean error of D
107- 111 F5.2 kpc s_D ? Mean ±error of D (errorD)
113- 117 F5.2 kpc Dcrab400 ? Crab upper limit for the distance using
the measured fluxes at 400 MHz (dcrab400)
119- 124 F6.1 kpc Dcrab1400 ? Crab upper limit for the distance using
the measured fluxes at 1400 MHz with are
lower than Dcrab400 limits (dcrab1400)
126- 132 F7.2 pc zD Pulsar distance to the Galactic plane z
calculated from the adopted distance (z)
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 30-Jan-2025