J/AJ/155/215 Speckle interferometry of red dwarf stars (Mason+, 2018)
Speckle interferometry of red dwarf stars.
Mason B.D., Hartkopf W.I., Miles K.N., Subasavage J.P., Raghavan D.,
Henry T.J.
<Astron. J., 155, 215-215 (2018)>
=2018AJ....155..215M 2018AJ....155..215M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Stars, M-type ; Stars, double and multiple ;
Interferometry ; Ephemerides
Keywords: binaries: general - binaries: visual - stars: individual: G 161-7 -
techniques: interferometric
Abstract:
We report high-resolution optical speckle observations of 336 M dwarfs,
which results in 113 measurements of the relative position of 80 systems
and 256 other stars with no indications of duplicity. These are the first
measurements for two of the systems. We also present the earliest
measurements of relative position for 17 others. We include orbits for
six of the systems, two revised and four reported for the first time.
For one of the systems with a new orbit, G 161-7, we determine masses
of 0.156±0.011 and 0.1175±0.0079 M☉ for the A and B components,
respectively. All six of these new calculated orbits have short periods
(between five and 38 years) and hold the promise of deriving accurate
masses in the near future. For many other pairs we can establish their
nature as physical or chance alignment, depending on their relative
motion. Of the 80 systems, 32 have calculated orbits, 25 others are
physical pairs, four are optical pairs, and 19 are currently unknown.
Description:
The observing runs included many different projects, as speckle
interferometry is a fast observing technique with up to 20 objects per
hour observed and nightly totals of 120-220 stars, depending on hours of
dark time. Most of the data that were not specific to this M dwarf program
were massive stars (Mason et al. 2009, J/AJ/137/3358) or exoplanet hosts
(Mason et al. 2011, J/AJ/142/176). Other data are presented in Appendix A.
The instrument used for these observations was the USNO speckle
interferometer, which is described in detail in Mason et al. (2009,
J/AJ/137/3358; 2011, J/AJ/142/176). Briefly, the camera consists of two
different microscope objectives giving different scales, interference
filters of varying FWHM to allow fainter objects to be observed, Risley
prisms that correct for atmospheric dispersion, and finally a Gen IIIc
intensified charge coupled device (ICCD) capable of very short exposures
necessary to take advantage of the "speckling" generated by atmospheric
turbulence. Each observation represents the directed vector autocorrelation
(Bagnuolo et al. 1992AJ....103.1399B 1992AJ....103.1399B) of 2000+ individual exposures, each
1-15 ms long, depending on an object's brightness and the filter in use.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 139 118 Speckle interferometric measurements of red
dwarf pairs
table3.dat 163 6 New orbital elements
table4.dat 86 6 New linear elements
table5.dat 96 12 Ephemerides
table7.dat 139 110 Speckle interferometric measurements of other
pairs
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See also:
B/wds : The Washington Visual Double Star Catalog (Mason+ 2001-2014)
J/AJ/137/3358 : Speckle interferometry of massive stars (Mason+, 2009)
J/AJ/142/176 : Exoplanet host stars. II. Speckle interferometry (Mason+, 2011)
Byte-by-byte Description of file: table2.dat table7.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- WDS WDS designation (HHMMm+DDMM, J2000)
12- 19 A8 --- Disc Discoverer designation
21- 25 A5 --- Comp Component designation
27- 33 F7.4 yr Epoch [5.8614/10.5916] Epoch of observation
(expressed as a fractional Julian year, -2000)
35- 39 F5.1 deg theta [0.1/355.4]? Position angle θ (1)
40 A1 --- u_theta [:] Uncertainty flag on theta (:=measure with
reduced accuracy due to observing conditions)
42- 46 F5.3 arcsec rho [0.047/8.106]? Separation ρ
47 A1 --- u_rho [:] Uncertainty flag on rho (:=measure with
reduced accuracy due to observing conditions)
49 I1 --- N [1/5] Number of observation(s) contained in
the mean position
51- 55 F5.1 deg (O-C)t [-17.6/43.1]? The O-C position angle residual
to the orbit or rectilinear fit referenced in
column Ref (not in Table 7)
57- 62 F6.3 arcsec (O-C)r [-0.247/0.058]? The O-C separation residual
to the orbit or rectilinear fit referenced in
column Ref (not in Table 7)
64- 86 A23 --- Ref Reference for the orbit or rectilinear fit
(not in Table 7)
88-106 A19 --- Bibcode Bibcode of the reference (not in Table 7)
108-128 A21 --- Com Comment on the reference (not in Table 7)
130-139 A10 --- n_WDS Note(s) on the WDS system (2)
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Note (1): The position angle has not been corrected for precession, and thus is
based on the equinox for the epoch of observation.
Note (2): Note as follows:
* = System used in characterizing errors or investigating detection space;
1 = Based on the very similar proper motions of the components and the lack of
significant change in the relative position, this pair is deemed physical;
2 = Based on the high proper motion of the primary and the lack of significant
change in the relative position, this pair is deemed physical;
3 = New linear solution. Unless indicated otherwise, counted as optical. See
Table 4;
4 = Preliminary elements were published in Miles & Mason (2016, IAU DS
Circular 190 1);
5 = Measures indicate non-linearity, i.e., physical. However, current data
insufficient for orbit determination. Continued observation justified;
6 = First observation of this pair;
7 = New orbit. See Table 3;
8 = Pair unresolved on date of observation. The secondary could have moved to
closer than 0.03" or the Δm>2.0 due to variability of one or both
components, or this may indicate the companion was optical due and no
longer visible due to the high proper motion of the primary;
A = First observation of this pair;
B = We crudely estimate the Δm in V as 3.0;
C = We crudely estimate the Δm in V as 0.5;
D = This pair was originally associated with LP 876-10. LP 876-10 was examined
multiple times (Mamajek et al. 2013AJ....146..154M 2013AJ....146..154M), none of which showed
any hint of elongation. Tokovinin et al. (2015, J/AJ/150/50) also did not
detect it. Mamajek et al. effectively ruled this out an optical
coincidence between the high proper motion LP 876-10 and a background
star. The tentative conclusion is that a different pair was observed and
that the 2010 measure (see Table B1) was not of LP 876-10, but instead of
some other unidentified pair which may or may not be a physical pair.
While no nearby known pairs in the WDS matches the approximate morphology
of the pair, in this magnitude range an unknown double star would not be a
surprise. As we are unsure what star was examined the WDS does not provide
a precise position, the magnitudes of the components are degraded, and it
has been disassociated with Fomalhaut.
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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- 10 A10 --- WDS WDS designation (HHMMm+DDMM, J2000)
12- 18 A7 --- Disc Discovery designation
20- 28 A9 --- OName Other designation
30- 35 F6.3 yr Per [5.075/34.582] Period
37- 41 F5.3 yr e_Per [0.016/2.6] Uncertainty in Per
43- 48 F6.4 arcsec a [0.1981/0.87] Semimajor axis
50- 55 F6.4 arcsec e_a [0.0021/0.033] Uncertainty in a
57- 62 F6.2 deg i [20/143] Inclination
64- 68 F5.2 deg e_i [0.66/15] Uncertainty in i
70- 75 F6.2 deg Omega [117/303] Longitude of node Ω (J2000)
77- 81 F5.2 deg e_Omega [0.48/22] Uncertainty in Omega
83- 90 F8.3 yr T0 [1988.39/2023.21] Epoch of periastron passage
(expressed as a fractional Julian year)
92- 96 F5.3 yr e_T0 [0.036/1.1] Uncertainty in T0
98-103 F6.4 --- e [0.183/0.839] Eccentricity
105-110 F6.4 --- e_e [0.008/0.056] Uncertainty in e
112-117 F6.2 deg omega [19.5/359] Longitude of periastron ω
119-123 F5.2 deg e_omega [0.75/25] Uncertainty in omega
125 I1 --- Grade [3/5] Orbit grade (see Hartkopf et al.
2001AJ....122.3472H 2001AJ....122.3472H) (1)
127-143 A17 --- Ref Reference for a previous orbit determination,
if one exists
145-163 A19 --- Bibcode Bibcode of the reference
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Note (1): Orbit grades are on a 1-5 scale. In the case of the orbits presented
here, a grade of 3 indicates the orbit is "reliable", 4 is "preliminary" and
5 is "indeterminate". In all of the cases here, the numbers are indicative
of the small number of observations and incomplete phase coverage.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- WDS WDS designation (HHMMm+DDMM, J2000)
12- 18 A7 --- Disc Discoverer designation
20- 24 A5 --- Comp Component designation
26- 34 F9.6 arcsec x0 [-1.120781/1.935622] Zero point in x (x0) (1)
36- 44 F9.6 arcsec/yr ax [-0.028649/0.04407] Slope in x (ax) (1)
46- 54 F9.6 arcsec y0 [-0.435759/1.922322] Zero point in y (y0) (1)
56- 64 F9.6 arcsec/yr ay [-0.056288/0.025295] Slope in y (ay) (1)
66- 73 F8.3 yr T0 [1973.89/2023.42] Time of closest apparent
separation T0 (1)
75- 79 F5.3 arcsec p0 [0.409/2.665] Closest apparent separation
ρ0 (1)
81- 86 F6.2 deg theta0 [29.85/234.52] Position angle at T0,
θ0 (1)
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Note (1): See Hartkopf & Mason (2015, Catalog of Rectilinear Elements
(Washington, D.C.: U.S. Naval Observatory)) for a description of all terms.
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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- 10 A10 --- WDS WDS designation (HHMMm+DDMM, J2000)
12- 18 A7 --- Disc Discoverer designation
20- 24 A5 --- Comp Component designation
26- 30 F5.1 deg theta18 [2.6/335] Predicted value of θ for
the year 2018.0
32- 36 F5.3 arcsec rho18 [0.147/2.736] Predicted value of ρ for
the year 2018.0
38- 42 F5.1 deg theta19 [22.9/331.3] Predicted value of θ for
the year 2019.0
44- 48 F5.3 arcsec rho19 [0.062/2.742] Predicted value of ρ for
the year 2019.0
50- 54 F5.1 deg theta20 [17.2/325.9] Predicted value of θ for
the year 2020.0
56- 60 F5.3 arcsec rho20 [0.148/2.748] Predicted value of ρ for
the year 2020.0
62- 66 F5.1 deg theta21 [11.2/334.9] Predicted value of θ for
the year 2021.0
68- 72 F5.3 arcsec rho21 [0.095/2.756] Predicted value of ρ for
the year 2021.0
74- 78 F5.1 deg theta22 [2.6/349] Predicted value of θ for
the year 2022.0
80- 84 F5.3 arcsec rho22 [0.124/2.766] Predicted value of ρ for
the year 2022.0
86- 90 F5.1 deg theta23 [3.6/357.3] Predicted value of θ for
the year 2023.0
92- 96 F5.3 arcsec rho23 [0.085/2.776] Predicted value of ρ for
the year 2023.0
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 11-Dec-2018