J/MNRAS/521/2504 NS in binary systems kick velocities study (O'Doherty+, 2023)
An observationally derived kick distribution for neutron stars in binary
systems.
O'Doherty T.N., Bahramian A., Miller-Jones J.C.A., Goodwin A.J., Mandel I.,
Willcox R., Atri P., Strader J.
<Mon. Not. R. Astron. Soc. 521, 2504-2524 (2023)>
=2023MNRAS.521.2504O 2023MNRAS.521.2504O (SIMBAD/NED BibCode)
ADC_Keywords: Stars, neutron ; Binaries, X-ray ; Pulsars ;
Stars, double and multiple ; Photometry ; Optical ;
Stars, distances ; Velocity dispersion ; Rotational velocities ;
Radial velocities ; Proper motions ; References ; Combined data
Keywords: proper motions - stars: neutron - pulsars: general -
supernovae: general
Abstract:
Understanding the natal kicks received by neutron stars (NSs) during
formation is a critical component of modelling the evolution of
massive binaries. Natal kicks are an integral input parameter for
population synthesis codes, and have implications for the formation of
double NS systems and their subsequent merger rates. However, many of
the standard observational kick distributions that are used are
obtained from samples created only from isolated NSs. Kick
distributions derived in this way overestimate the intrinsic NS kick
distribution. For NSs in binaries, we can only directly estimate the
effect of the natal kick on the binary system, instead of the natal
kick received by the NS itself. Here, for the first time, we present a
binary kick distribution for NSs with low-mass companions. We compile
a catalogue of 145 NSs in low-mass binaries with the best available
constraints on proper motion, distance, and systemic radial velocity.
For each binary, we use a three-dimensional approach to estimate its
binary kick. We discuss the implications of these kicks on system
formation, and provide a parametric model for the overall binary kick
distribution, for use in future theoretical modelling work. We compare
our results with other work on isolated NSs and NSs in binaries,
finding that the NS kick distributions fit using only isolated pulsars
underestimate the fraction of NSs that receive low kicks. We discuss
the implications of our results on modelling double NS systems, and
provide suggestions on how to use our results in future theoretical
works.
Description:
Neutron stars (NSs) are ultra-dense remnants left behind after massive
stars end their lives in a supernova explosion, and are most often
observed as pulsars and in X-ray binaries (XRBs). Pulsars are highly
magnetic, rapidly rotating NSs that produce beamed radio emission.
Typical pulsars are young (<108 yr) and have spin periods ∼1 s.
However, millisecond pulsars (MSPs) are much older (>109 yr) with
spin periods < 30 ms and weaker magnetic fields. The NS XRBs are
binary systems with an NS accreting material from a stellar companion.
Systems with low-mass companions (Mc ≤ 1 M☉) are called
low-mass XRBs (LMXBs) and are long lived (>109 yr) with stable mass
transfer occurring during the long lifetime of the companion.
Recently, Atri et al. (2019MNRAS.489.3116A 2019MNRAS.489.3116A) developed a novel method
for estimating the binary kicks of old binary systems. The technique
uses the system's distance, proper motion, and systemic radial
velocity to robustly estimate the potential binary kick distribution
for each system. While Atri et al. (2019MNRAS.489.3116A 2019MNRAS.489.3116A) focused on
black hole LMXBs, this technique is equally applicable to estimating
the binary kicks of old NSs like MSPs and NS LMXBs. In this paper, we
compile a sample of 145 old NSs and estimate the potential binary kick
distribution they could have received at birth, comparing them first
to different classes of old NSs, and then to other NSs and black
holes.
Estimates distance methods, kick distribution and fits models are
fully discussed in section 2. As presented in section 3, with
searching for Gaia EDR3/DR3 counterparts, we firstly compiled 14
confirmed redback pulsars mostly originated from Strader et al.
(2019ApJ...872...42S 2019ApJ...872...42S; Cat. J/ApJ/872/42). Secondly in a way, we
compiled 19 NS LMXB systems in the field from Arnason et al.
(2021MNRAS.502.5455A 2021MNRAS.502.5455A), 17 black widow systems extracted from Hui & Li
(2019Galax...7...93H 2019Galax...7...93H) using their table of Galactic field black
widows. Finally, we focus on 95 MSPs using ATNF catalog from
Manchester et al. (2005AJ....129.1993M 2005AJ....129.1993M, Cat. B/psr). Results from PKVs
probability distributions analysis as well as astrometrics and
distances used are provided in tables msps.dat, blwidows.dat,
nslmxbs.dat, redbacks.dat respectively for samples of 145 NS binary
systems.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
nslmxbs.dat 281 19 Parameters used in the creation of the PKV
distributions for each redback system
redbacks.dat 281 14 Parameters used in the creation of the PKV
distributions for each NS LMXB system
blwidows.dat 235 17 Parameters used in the creation of the PKV
distributions for each black widow system
msps.dat 235 95 Parameters used in the creation of the PKV
distributions for each MSP system
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See also:
J/MNRAS/484/3691 : UTMOST pulsar timing programme. I. (Jankowski+, 2019)
J/MNRAS/458/3341 : 42 millisecond pulsars high-precision timing
(Desvignes+, 2016)
J/MNRAS/437/1791 : RMS survey: molecular observations (Urquhart+, 2014)
J/MNRAS/360/974 : Proper motions of pulsars (Hobbs+, 2005)
J/A+A/665/A31 : Neutron-star kicks in HMXBs with Gaia EDR3 (Fortin+, 2022)
J/A+A/624/A66 : Massive runaway and walkaway stars models (Renzo+, 2019)
J/A+A/469/807 : Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)
J/A+A/455/1165 : Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)
J/ApJ/910/160 : Fermi LAT sources observed with the GMRT
(Bhattacharyya+, 2021)
J/ApJ/876/8 : BVI LCs and radial velocities of PSR J1306-40
(Swihart+, 2019)
J/ApJ/872/42 : Opt. spectroscopy of redback ms pulsar binaries
(Strader+, 2019)
J/ApJ/872/43 : IR spectroscopy of symbiotic stars. XII. V934 Her
(Hinkle+, 2019)
J/ApJ/810/85 : Observation of first Fermi-LAT sources at Parkes
(Camilo+, 2015)
J/ApJ/702/1472 : Column densities for HI, AlIII, SiIV, CIV, OVI
(Savage+, 2009)
J/ApJS/208/17 : 2nd Fermi LAT cat. of gamma-ray pulsars (2PC) (Abdo+, 2013)
J/ApJS/179/360 : Thermonuclear X-ray bursts observed by RXTE (Galloway+,2008)
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: nslmxbs.dat redbacks.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Source Source pulsar name (Source)
21- 40 F20.16 mas/yr pmRA Proper motion in right ascension pmRA*cosDE of
the source in ICRS at Ep=2016.0 (pmra)
42- 59 F18.16 mas/yr e_pmRA Standard error of proper motion in right
ascension direction (pmra_error)
61- 80 F20.16 mas/yr pmDE Proper motion in declination direction (pmdec)
82- 99 F18.16 mas/yr e_pmDE Standard error of proper motion in declination
direction (pmdec_error)
101-121 F21.16 d Pb ? Pulsation period (PB)
123-144 E22.17 d e_Pb ? Uncertainty of Pb (PB_error)
146-153 F8.3 km/s RV ? Radial velocity (RV)
155-160 F6.3 km/s e_RV ? Uncertainty of RV (RV_error)
162-180 F19.16 mas Plx Parallax (parallax)
182-199 F18.16 mas e_Plx Uncertainty of Plx (parallax_error)
201-205 F5.2 kpc D ? Distance from parallax (d)
207-210 F4.2 kpc e_D ? Uncertainty of D (d_error)
212-230 F19.15 km/s PKV Potential kick velocity quantity estimated
with PKV distributions best fit (PKV) (G1)
232-250 F19.15 km/s E_PKV Upper uncertainty of PKV as 84.1 percentiles
of the PKV distribution (PKVuppererror)
252-270 F19.15 km/s e_PKV Lower uncertainty of PKV as 15.9 percentiles
of the PKV distribution (PKVlowererror)
272-281 A10 --- r_Source Literature references (References) (1)
--------------------------------------------------------------------------------
Note (1): Literature references firstly for redback pulsars and secondly for
NS LMXBs are as follows:
1 = Deller et al. (2012ApJ...756L..25D 2012ApJ...756L..25D),
for NS LMXBs Gaia Collaboration (2021A&A...649A...1G 2021A&A...649A...1G,
Cat. I/350)
2 = Archibald et al. (2009Sci...324.1411A 2009Sci...324.1411A),
for NS LMXBs Kuulkers et al. (2010A&A...514A..65K 2010A&A...514A..65K)
3 = McConnell et al. (2015MNRAS.451.3468M 2015MNRAS.451.3468M),
for NS LMXBs Ashcraft et al. (2012MNRAS.424..620A 2012MNRAS.424..620A)
4 = Gaia Collaboration (2021A&A...649A...1G 2021A&A...649A...1G, Cat. I/350),
for NS LMXBs Jonker et al. (2012MNRAS.424..620A 2012MNRAS.424..620A)
5 = Deneva et al. (2021ApJ...909....6D 2021ApJ...909....6D),
for NS LMXBs In't Zand et al. (2008A&A...485..183I 2008A&A...485..183I)
6 = Strader et al. (2019ApJ...872...42S 2019ApJ...872...42S, Cat. J/ApJ/872/42),
for NS LMXBs Gonzalez Hernandez et al. (2005A&A...435.1185G 2005A&A...435.1185G)
7 = Roy et al. (2015ApJ...800L..12R 2015ApJ...800L..12R),
for NS LMXBs Casares et al. (2007A&A...470.1033C 2007A&A...470.1033C)
8 = De Martino et al. (2014MNRAS.444.3004D 2014MNRAS.444.3004D),
for NS LMXBs Wang et al. (2018MNRAS.478.5174W 2018MNRAS.478.5174W)
9 = Swihart et al. (2019ApJ...876....8S 2019ApJ...876....8S, Cat. J/ApJ/876/8),
for NS LMXBs Casares et al. (2006MNRAS.373.1235C 2006MNRAS.373.1235C)
10 = Camilo et al. (2016ApJ...820....6C 2016ApJ...820....6C),
for NS LMXBs Galloway et al. (2006ApJ...639.1033G 2006ApJ...639.1033G)
11 = Strader et al. (2015ApJ...804L..12S 2015ApJ...804L..12S),
for NS LMXBs Staubert et al. (2009A&A...500..883S 2009A&A...500..883S)
12 = Bates et al. (2015MNRAS.446.4019B 2015MNRAS.446.4019B),
for NS LMXBs Reynolds et al. (1997MNRAS.288...43R 1997MNRAS.288...43R)
13 = Sanpa-Arsa (2016PhDT.......539S 2016PhDT.......539S),
for NS LMXBs Iaria et al. (2018MNRAS.473.3490I 2018MNRAS.473.3490I)
14 = Ray et al. (2012arXiv1205.3089R 2012arXiv1205.3089R),
for NS LMXBs Ponti et al. (2018MNRAS.481L..94P 2018MNRAS.481L..94P)
15 = Crawford et al. (2013ApJ...776...20C 2013ApJ...776...20C),
for NS LMXBs Galloway et al. (2008ApJS..179..360G 2008ApJS..179..360G,
Cat. J/ApJS/179/360)
16 = Antoniadis et al. (2013ApJ...776...20C 2013ApJ...776...20C, Cat. J/A+A/686/A88),
for NS LMXBs Wachter (1998PhDT.........1W 1998PhDT.........1W)
17 = Stovall et al. (2014ApJ...791...67S 2014ApJ...791...67S),
for NS LMXBs Strohmayer et al. (2018ApJ...858L..13S 2018ApJ...858L..13S)
18 = Kaplan et al. (2013ApJ...765..158K 2013ApJ...765..158K),
for NS LMXBs Keek et al. (2017ApJ...836..111K 2017ApJ...836..111K)
19 = Stovall et al. (2016ApJ...833..192S 2016ApJ...833..192S),
for NS LMXBs Hinkle et al. (2019ApJ...872...43H 2019ApJ...872...43H,
Cat. J/ApJ/872/43)
20 = Bellm et al. (2016ApJ...816...74B 2016ApJ...816...74B),
for NS LMXBs Hinkle et al. (2006ApJ...641..479H 2006ApJ...641..479H)
21 = Abdo et al. (2013ApJS..208...17A 2013ApJS..208...17A, Cat. J/ApJS/208/17),
for NS LMXBs Casares et al. (2006MNRAS.373.1235C 2006MNRAS.373.1235C)
22 = Linares, Shahbaz & Casares (2018ApJ...859...54L 2018ApJ...859...54L),
for NS LMXBs Augusteijn et al. (1998A&A...332..561A 1998A&A...332..561A)
23 = Pletsch & Clark (2015ApJ...807...18P 2015ApJ...807...18P),
for NS LMXBs Falanga et al. (2008A&A...484...43F 2008A&A...484...43F)
24 = Romani & Shaw (2011ApJ...743L..26R 2011ApJ...743L..26R),
for NS LMXBs Mata Sanchez et al. (2017MNRAS.464L..41M 2017MNRAS.464L..41M)
25 = for NS LMXBs Jonker & Nelemans (2004MNRAS.354..355J 2004MNRAS.354..355J)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: blwidows.dat msps.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 21 A21 --- Source Source pulsar name (Source)
23- 35 F13.9 mas/yr pmRA Proper motion in right ascension pmRA*cosDE
of the source in ICRS at Ep=2016.0 (pmra)
37- 46 F10.8 mas/yr e_pmRA Standard error of proper motion in right
ascension direction (pmra_error)
48- 60 F13.9 mas/yr pmDE Proper motion in declination direction
(pmdec)
62- 71 F10.8 mas/yr e_pmDE Standard error of proper motion in
declination direction (pmdec_error)
73- 89 F17.13 d Pb ? Pulsation period (PB)
91- 97 E7.3 d e_Pb ? Uncertainty of Pb (PB_error)
99-104 F6.4 kpc dNE2001 Distance estimate with NE2001 model
(d_NE2001) (1)
106-110 F5.3 kpc dYMW16 Distance estimate with YMW16 model (d_YMW16)
(1)
112-130 F19.15 km/s PKVNE2001 Potential kick velocity quantity estimated
with NE2001 model (PKV_NE2001) (G1)
132-150 F19.15 km/s E_PKVNE2001 Upper uncertainty of PKVNE2001 as 84.1
percentiles of the PKV distribution
(PKVNE2001upper_error)
152-169 F18.15 km/s e_PKVNE2001 Lower uncertainty of PKVNE2001 as 15.9
percentiles of the PKV distribution
(PKVNE2001lower_error)
171-189 F19.15 km/s PKVYMW16 Potential kick velocity quantity estimated
with YMW16 model (PKV_YMW16) (G1)
191-209 F19.15 km/s E_PKVYMW16 Upper uncertainty of PKVYMW16 as 84.1
percentiles of the PKV distribution
(PKVYMW16upper_error)
211-229 F19.15 km/s e_PKVYMW16 Lower uncertainty of PKVYMW16 as 15.9
percentiles of the PKV distribution
(PKVYMW16lower_error)
231-235 A5 --- r_Source Literature references (References) (2)
--------------------------------------------------------------------------------
Note (1): As fully discussed in sect. 2.1 Distances, if a reliable parallax is
not available for a source, we turn to optical light-curve fitting.
This technique involves estimating the stellar companion's intrinsic
luminosity, correcting for extinction, and then comparing the
predicted absolute magnitude to the observed apparent magnitude.
Where this is not feasible, we turn to the Cordes & Lazio
(2002astro.ph..7156C 2002astro.ph..7156C) as NE2001 and Yao et al. (2017ApJ...835...29Y 2017ApJ...835...29Y)
as YMW16 dispersion measure (DM) models to estimate distances.
Note (2): Literature references firstly for msps and secondly for black widows
are as follows:
1 = Manchester et al. (2005AJ....129.1993M 2005AJ....129.1993M, Cat. B/psr)
2 = Desvignes et al. (2016MNRAS.458.3341D 2016MNRAS.458.3341D, Cat. J/MNRAS/458/3341),
for black widows Arzoumanian et al. (2018ApJS..235...37A 2018ApJS..235...37A)
3 = Kerr et al. (2012ApJ...748L...2K 2012ApJ...748L...2K),
for black widows Guillemot et al. (2016A&A...587A.109G 2016A&A...587A.109G)
4 = Martinez et al. (2019ApJ...881..166M 2019ApJ...881..166M),
for black widows Desvignes et al. (2016MNRAS.458.3341D 2016MNRAS.458.3341D,
Cat. J/MNRAS/458/3341)
5 = Du et al. (2019ApJ...881..166M 2019ApJ...881..166M),
for black widows Pletsch et al. (2012Sci...338.1314P 2012Sci...338.1314P)
6 = Jennings et al. (2018ApJ...864...26J 2018ApJ...864...26J),
for black widows Ng et al. (2014MNRAS.439.1865N 2014MNRAS.439.1865N)
7 = Ransom et al. (2014Natur.505..520R 2014Natur.505..520R),
for black widows Lynch et al. (2018ApJ...859...93L 2018ApJ...859...93L)
8 = Reardon et al. (2016MNRAS.455.1751R 2016MNRAS.455.1751R),
for black widows Barr et al. (2013MNRAS.429.1633B 2013MNRAS.429.1633B)
9 = Arzoumanian et al. (2018ApJS..235...37A 2018ApJS..235...37A),
for black widows Deneva et al. (2021ApJ...909....6D 2021ApJ...909....6D)
10 = Guillemot et al. (2016A&A...587A.109G 2016A&A...587A.109G),
for black widows Hessels et al. (2011AIPC.1357...40H 2011AIPC.1357...40H)
11 = Ransom et al. (2011ApJ...727L..16R 2011ApJ...727L..16R),
for black widows Arzoumanian et al. (1994ApJ...426L..85A 1994ApJ...426L..85A)
12 = Deller et al. (2009Sci...323.1327D 2009Sci...323.1327D),
for black widows Shaifullah et al. (2016MNRAS.462.1029S 2016MNRAS.462.1029S)
13 = Kramer et al. (2006Sci...314...97K 2006Sci...314...97K),
for black widows Guillemot et al. (2019A&A...629A..92G 2019A&A...629A..92G)
14 = Cromartie et al. (2020NatAs...4...72C 2020NatAs...4...72C),
for black widows Jankowski et al. (2019MNRAS.484.3691J 2019MNRAS.484.3691J,
Cat. J/MNRAS/484/3691)
15 = Ng et al. (2014MNRAS.439.1865N 2014MNRAS.439.1865N),
for black widows Keith et al. (2011MNRAS.414.1292K 2011MNRAS.414.1292K)
16 = Deller et al. (2019ApJ...875..100D 2019ApJ...875..100D),
for black widows Crowter et al. (2020MNRAS.495.3052C 2020MNRAS.495.3052C)
17 = Bhattacharyya et al. (2021ApJ...910..160B 2021ApJ...910..160B, Cat. J/ApJ/910/160)
18 = Konacki & Wolszczan (2003ApJ...591L.147K 2003ApJ...591L.147K)
19 = Sanpa-Arsa (2016PhDT.......539S 2016PhDT.......539S)
20 = Swiggum et al. (2017ApJ...847...25S 2017ApJ...847...25S)
21 = Spiewak et al. (2020MNRAS.496.4836S 2020MNRAS.496.4836S)
22 = Camilo et al. (2015ApJ...810...85C 2015ApJ...810...85C, Cat. J/ApJ/810/85)
23 = Lewandowski et al. (2004ApJ...600..905L 2004ApJ...600..905L)
24 = Lynch et al. (2018ApJ...859...93L 2018ApJ...859...93L)
25 = Zhu et al. (2015ApJ...809...41Z 2015ApJ...809...41Z)
26 = Freire et al. (2012MNRAS.423.3328F 2012MNRAS.423.3328F)
27 = Ferdman et al. (2010ApJ...711..764F 2010ApJ...711..764F)
28 = Ng et al. (2020MNRAS.493.1261N 2020MNRAS.493.1261N)
29 = Freire et al. (2011MNRAS.412.2763F 2011MNRAS.412.2763F)
30 = Gonzalez et al. (2011ApJ...743..102G 2011ApJ...743..102G)
31 = Liu et al. (2020MNRAS.499.2276L 2020MNRAS.499.2276L)
32 = Parent et al. (2019ApJ...886..148P 2019ApJ...886..148P)
33 = Graikou et al. (2017MNRAS.471.4579G 2017MNRAS.471.4579G)
34 = Barr et al. (2017MNRAS.465.1711B 2017MNRAS.465.1711B)
35 = Zhu et al. (2019ApJ...881..165Z 2019ApJ...881..165Z)
36 = Nice et al. (2001ApJ...549..516N 2001ApJ...549..516N)
37 = Clark et al. (2021MNRAS.502..915C 2021MNRAS.502..915C)
38 = Berezina et al. (2017MNRAS.470.4421B 2017MNRAS.470.4421B)
39 = Stovall et al. (2019ApJ...870...74S 2019ApJ...870...74S)
40 = Fonseca et al. (2016ApJ...832..167F 2016ApJ...832..167F)
41 = Spiewak et al. (2018MNRAS.475..469S 2018MNRAS.475..469S)
--------------------------------------------------------------------------------
Global notes:
Note (G1): As fully discussed in sect. 2.2 Kicks, as in Atri et al.
(2019MNRAS.489.3116A 2019MNRAS.489.3116A), we estimate the potential binary kick of a
system using its measured parallax, proper motion, and systemic
radial velocity as distribution functions. We obtained estimated
peculiar velocities form the 'potential kick velocity' (PKV)
distribution. This distribution of velocities is used as a proxy
for the kick the system could have received at birth as a result of
formation of the compact object. It is important to note one of the
main underlying assumptions is that the system was formed in the
Galactic plane. As all systems in this work were selected such that
they are in the Galactic field, we implicitly assume they formed in
the plane. Then as explained in section 4, best fits results are
presented in results of the PKV profiles as defined by equation 8
of the section 2.4 Model fitting.
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License: CC-BY-4.0
(End) Luc Trabelsi [CDS] 01-Jun-2026