J/ApJ/872/42 Opt. spectroscopy of redback ms pulsar binaries (Strader+, 2019)
Optical spectroscopy and demographics of redback millisecond pulsar binaries.
Strader J., Swihart S., Chomiuk L., Bahramian A., Britt C., Cheung C.C.,
Dage K., Halpern J., Li K.-L., Mignani R.P., Orosz J.A., Peacock M.,
Salinas R., Shishkovsky L., Tremou E.
<Astrophys. J., 872, 42 (2019)>
=2019ApJ...872...42S 2019ApJ...872...42S
ADC_Keywords: Pulsars; Radial velocities; Spectra, optical; Photometry, UBVRI;
Proper motions
Keywords: binaries: spectroscopic ; gamma rays: stars ; pulsars: general ;
stars: neutron ; X-rays: binaries
Abstract:
We present the first optical spectroscopy of five confirmed (or strong
candidate) redback millisecond pulsar binaries, obtaining complete
radial velocity curves for each companion star. The properties of
these millisecond pulsar binaries with low-mass, hydrogen-rich
companions are discussed in the context of the 14 confirmed and 10
candidate field redbacks. We find that the neutron stars in redbacks
have a median mass of 1.78±0.09M☉ with a dispersion of
σ=0.21±0.09. Neutron stars with masses in excess of 2M☉
are consistent with, but not firmly demanded by, current observations.
Redback companions have median masses of 0.36±0.04M☉ with a
scatter of σ=0.15±0.04M☉, and a tail possibly extending
up to 0.7-0.9M☉. Candidate redbacks tend to have higher
companion masses than confirmed redbacks, suggesting a possible
selection bias against the detection of radio pulsations in these more
massive candidate systems. The distribution of companion masses
between redbacks and the less massive black widows continues to be
strongly bimodal, which is an important constraint on evolutionary
models for these systems. Among redbacks, the median efficiency of
converting the pulsar spin-down energy to γ-ray luminosity is ∼10%.
Description:
The spectroscopic observations of the redback systems were all made
using the Goodman Spectrograph on the SOAR telescope in Chile. Good
spectra were obtained for a minimum of 13 epochs (PSR J1048+2339) to a
maximum of 44 epochs (3FGL J2039.6-5618).
We also obtained optical BVI photometry of PSR J1431-3715 with ANDICAM
on the SMARTS 1.3m telescope at CTIO in early 2018.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 42 100 Modified Barycentric radial velocities of
5 redbacks (PSR J1048+2339, PSR J1431-4715,
PSR J1622-0315, PSR J1628-3205, and
3FGL J2039.6-5618)
table2.dat 32 309 SMARTS photometry of PSR J1431-4715
table3.dat 154 24 Observed and derived properties of confirmed and
candidate redbacks
table5.dat 90 24 Observed and derived properties of redbacks
(including orbital periods)
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See also:
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IX/57 : The Chandra Source Catalog (CSC), Release 2.0 (Evans+, 2019)
J/ApJ/769/108 : Optical photometry of 4 millisecond pulsars (Breton+, 2013)
J/ApJS/208/17 : 2nd Fermi LAT cat. of gamma-ray pulsars (2PC) (Abdo+, 2013)
J/ApJS/218/23 : Fermi LAT third source catalog (3FGL) (Acero+, 2015)
J/ApJ/820/8 : 3FGL sources statistical classifications (Saz Parkinson+, 2016)
J/ApJ/831/89 : Eclipsing LMXB at 3FGL J0427.9-6704 center (Strader+, 2016)
J/MNRAS/458/3341 : 42 ms pulsars high-precision timing (Desvignes+, 2016)
J/ApJ/851/31 : 2FGL J0846.0+2820 opt. counterpart follow-up (Swihart+, 2017)
J/ApJ/866/83 : Opt/NIR obs. of 1FGLJ1417.7-4407 (Swihart+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Name
18- 30 F13.7 d MBJD [57158.3/58223.3] Modified Barycentric
Julian Date on the TDB system
32- 37 F6.1 km/s RVel [-511/380] Radial velocity
39- 42 F4.1 km/s e_RVel [5/36] Uncertainty in RVel
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 F11.5 d MBJD [58143.3/58328] Modified Barycentric
Julian date of observation
15 A1 --- Band [BVI] Broadband filter used (B, V, or I)
19- 24 F6.3 mag omag [17.17/18.41] Apparent (Vega) magnitude in Band
28- 32 F5.3 mag e_omag [0.015/0.09] The 1-sigma error in omag
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Name
18- 50 A33 --- OName Other name(s)
52 A1 --- f_OName [b] b: This association is uncertain
54- 55 I2 h RAh Hour of right ascension (J2000) (1)
57- 58 I2 min RAm Minute of right ascension (J2000)
60- 67 F8.5 s RAs Second of right ascension (J2000)
69- 75 F7.5 s e_RAs RAs uncertainty (1)
77 A1 --- DE- Sign of declination (J2000) (1)
78- 79 I2 deg DEd Degree of declination (J2000) (1)
81- 82 I2 arcmin DEm Arcminute of declination (J2000)
84- 89 F6.3 arcsec DEs Arcsecond of declination (J2000)
91- 95 F5.3 arcsec e_DEs DEs uncertainty (1)
97-102 F6.3 mas Plx [-1.6/1.2]? Parallax ω (1)
104-108 F5.3 mas e_Plx [0.03/1.3]? Plx uncertainty
110-115 F6.2 mas pmRA [-18.8/20.2]? Proper motion along RA;
µαcosδ (1)
117-120 F4.2 mas e_pmRA [0.07/2]? pmRA uncertainty
122-127 F6.2 mas pmDE [-24/10.2]? Proper motion along DE;
µδ (1)
129-132 F4.2 mas e_pmDE [0.05/3.5]? pmDE uncertainty
134-139 F6.3 mag Gmag [14.3/20.9]? Gaia mean G-band magnitude (1)
141-145 F5.3 mag e_Gmag [0.001/0.08]? Gmag uncertainty
147-154 A8 --- State State (2)
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Note (1): The coordinates, parallax, proper motion, and mean G magnitudes are
all are from Gaia DR2 (Gaia Collaboration, 2018, I/345), excepting that
for PSR J1302-3258: preliminary position from 2CXO J130225.5-325837;
see Section 4.2.1.
Note (2): The accretion state of the binary as follows:
PSR = rotation-powered (14 occurrences);
disk = accretion powered;
PSR/disk = transitional systems;
PSR(?) = systems that appear to be in the rotation-powered state, but
for which no pulsar has yet been detected.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Name
18- 29 F12.10 d Per [0.15/8.14] Orbital period
31- 42 F12.10 d e_Per [2e-10/0.0005]? Per uncertainty
44- 45 I2 --- r_Per [2/33] Period references (3)
47- 51 F5.1 km/s K2 [39.3/423]? Semi-amplitude K2 of
the companion star
53- 56 F4.2 km/s e_K2 [0/1.5]? K2 uncertainty
58- 61 I4 km/s gamma [-135/144]? Systemic velocity γ of the
binary
63- 64 I2 km/s e_gamma [1/15]? gamma uncertainty
66- 67 I2 --- Ref [10/43]? K2 and gamma references (3)
69- 72 I4 km/s U [-360/142]? U component of the
galactocentric velocity (4)
74- 75 I2 km/s e_U [1/10]? U uncertainty
77- 80 I4 km/s V [-187/78]? V component of the
galactocentric velocity (4)
82- 83 I2 km/s e_V [1/14]? V uncertainty
85- 88 I4 km/s W [-263/106]? W component of the
galactocentric velocity (4)
90 I1 km/s e_W [1/8]? W uncertainty
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Note (3): References as follows:
2 = Deneva et al. (2016ApJ...823..105D 2016ApJ...823..105D)
3 = Bates et al. (2015MNRAS.446.4019B 2015MNRAS.446.4019B)
4 = Sanpa-Arsa S. (2016, PhD thesis Univ. of Virginia)
6 = Kong et al. (2012ApJ...747L...3K 2012ApJ...747L...3K)
7 = Crawford et al. (2013ApJ...776...20C 2013ApJ...776...20C)
8 = Stovall et al. (2014ApJ...791...67S 2014ApJ...791...67S)
9 = Stovall et al. (2016ApJ...833..192S 2016ApJ...833..192S)
10 = Bellm et al. (2016ApJ...816...74B 2016ApJ...816...74B)
12 = Abdo et al. (2013, J/ApJS/208/17)
15 = Pletsch & Clark (2015ApJ...807...18P 2015ApJ...807...18P)
16 = Cromartie et al. (2016ApJ...819...34C 2016ApJ...819...34C)
17 = D. Lorimer (http://astro.phys.wvu.edu/GalacticMSPs/GalacticMSPs.txt)
20 = Archibald et al. (2013arXiv1311.5161A 2013arXiv1311.5161A)
21 = Roy et al. (2015ApJ...800L..12R 2015ApJ...800L..12R)
23 = Linares et al. (2017MNRAS.465.4602L 2017MNRAS.465.4602L)
24 = Camilo et al. (2016ApJ...820....6C 2016ApJ...820....6C)
26 = Li et al. (2016ApJ...833..143L 2016ApJ...833..143L)
27 = Strader et al. (2014ApJ...788L..27S 2014ApJ...788L..27S)
28 = Halpern et al. (2017ApJ...844..150H 2017ApJ...844..150H)
29 = this work
30 = Swihart et al. (2017, J/ApJ/851/31)
31 = Li et al. (2018ApJ...863..194L 2018ApJ...863..194L)
32 = Strader et al. (2016, J/ApJ/831/89)
33 = Britt et al. (2017ApJ...849...21B 2017ApJ...849...21B)
34 = Swihart et al., in preparation
36 = Strader et al. (2015ApJ...804L..12S 2015ApJ...804L..12S)
37 = Kaplan et al. (2013ApJ...765..158K 2013ApJ...765..158K)
38 = Romani & Shaw (2011ApJ...743L..26R 2011ApJ...743L..26R)
39 = de Martino et al. (2014MNRAS.444.3004D 2014MNRAS.444.3004D)
40 = Antoniadis et al., in preparation
41 = McConnell et al. (2015MNRAS.451.3468M 2015MNRAS.451.3468M)
42 = Linares et al. (2017MNRAS.465.4602L 2017MNRAS.465.4602L)
43 = Linares (2018MNRAS.473L..50L 2018MNRAS.473L..50L)
Note (4): We use the proper motions, distances, and radial velocities to
determine the UVW components of the galactocentric velocity for 21 of
the 24 systems; assuming the left-handed (U positive toward the
Galactic anticenter) convention.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Jul-2020