J/AJ/154/32 Solar neighborhood. XXXIX. Nearby white dwarfs (Subasavage+, 2017)
The solar neighborhood. XXXIX. Parallax results from the CTIOPI and NOFS
programs: 50 new members of the 25 parsec white dwarf sample.
Subasavage J.P., Jao W.-C., Henry T.J., Harris H.C., Dahn C.C.,
Bergeron P., Dufour P., Dunlap B.H., Barlow B.N., Ianna P.A., Lepine S.,
Margheim S.J.
<Astron. J., 154, 32-32 (2017)>
=2017AJ....154...32S 2017AJ....154...32S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, white dwarf ; Stars, nearby ; Parallaxes, trigonometric ;
Photometry, UBVRI ; Photometry, infrared ; Positional data ;
Spectral types ; Proper motions ; Stars, masses ;
Effective temperatures
Keywords: astrometry - Galaxy: evolution - solar neighborhood -
stars: distances - white dwarfs
Abstract:
We present 114 trigonometric parallaxes for 107 nearby white dwarf
(WD) systems from both the Cerro Tololo Inter-American Observatory
Parallax Investigation (CTIOPI) and the U. S. Naval Observatory
Flagstaff Station (NOFS) parallax programs. Of these, 76 parallaxes
for 69 systems were measured by the CTIOPI program and 38 parallaxes
for as many systems were measured by the NOFS program. A total of 50
systems are confirmed to be within the 25-pc horizon of interest.
Coupled with a spectroscopic confirmation of a common proper-motion
companion to a Hipparcos star within 25pc as well as confirmation
parallax determinations for two WD systems included in the recently
released Tycho Gaia Astrometric Solution catalog, we add 53 new
systems to the 25-pc WD sample-a 42% increase. Our sample presented
here includes four strong candidate halo systems, a new metal-rich DAZ
WD, a confirmation of a recently discovered nearby short-period
(P=2.85hr) double degenerate, a WD with a new astrometric perturbation
(long period, unconstrained with our data), and a new triple system
where the WD companion main-sequence star has an astrometric
perturbation (P∼1.6year).
Description:
Standardized photometric observations were carried out at three
separate telescopes.
The Small & Moderate Aperture Research Telescope System (SMARTS) 0.9m
telescope at Cerro Tololo Inter-American Observatory (CTIO) was used
during Cerro Tololo Inter-American Observatory Parallax Investigation
(CTIOPI) observing runs when conditions were photometric. A Tektronics
2K*2K detector was used in region-of-interest mode centered on the
central quarter of the full CCD producing a Field Of View (FOV) of
6.8'*6.8'. The SMARTS 1.0m telescope at CTIO was used with the Y4KCam
4K*4K imager, producing a 19.7'*19.7' FOV. Finally, the Ritchey 40-in
telescope at USNO Flagstaff Station (NOFS) was used with a Tektronics
2K*2K detector with a 20.0'*20.0' FOV.
Near-infrared JHKs photometry was collected for WD0851-246, at the
CTIO 4.0 m Blanco telescope using the NEWFIRM during an engineering
night on 2011.27 UT. National Optical Astronomy Observatory (NOAO)
Extremely Wide-field Infrared Image (NEWFIRM) is a 4K*4K InSb mosaic
that provides a 28'*28' FOV on the Blanco telescope.
Additional photometry values were extracted from the Sloan Digital Sky
Survey (SDSS) DR12 (Alam et al. 2015, Cat. V/147), 2MASS, and the
United Kingdom Infra-Red Telescope (UKIRT) Infrared Sky Survey
(UKIDSS) DR9 Large Area Survey (LAS; see Lawrence et al. 2012, Cat.
II/319), when available.
Two White Dwarfs (WDs) presented here (WD1743-545 and WD2057-493) are
newly discovered nearby WDs identified during a spectroscopic survey
of WD candidates in the southern hemisphere (J. Subasavage et al.
2017, in preparation) taken from the SUPERBLINK catalog (Lepine &
Shara 2015ASPC..493..455S 2015ASPC..493..455S). A third WD included here (WD2307-691) was
previously unclassified, yet is a common proper-motion companion to a
Hipparcos star within 25pc (HIP114416). A fourth WD (WD2028-171) was
suspected to be a WD by the authors based on a trawl of the New Luyten
Two Tenths (NLTT) catalog (Luyten 1979, Cat. I/98). Finally, a fifth
WD (WD1241-798) was first spectroscopically identified as a WD by
Subasavage et al. (2008AJ....136..899S 2008AJ....136..899S; Paper XX) but with an
ambiguous spectral type of DC/DQ. The SOuthern Astrophysical Research
(SOAR) 4m telescope with the Goodman spectrograph was used for
spectroscopic follow up as part of a larger spectroscopic campaign to
identify nearby WDs to be released in a future publication.
Observations were taken with a 600 lines-per-mm VPH grating with a
1.0'' slit width to provide 2.1Å resolution in wavelength range of
3600Å-6200Å.
Trigonometric parallax data acquisition and reduction techniques for
the CTIOPI program are discussed fully in Jao et al.
(2005AJ....129.1954J 2005AJ....129.1954J). In brief, the instrument setup and basic data
calibrations are identical to those used for photometric observations
(i.e., the SMARTS 0.9m telescope coupled with the central quarter of a
Tektronics 2K*2K detector). A parallax target's reference field is
determined upon first observation. We use one of the
Johnson-Kron-Cousins VRI filters, selected to optimize the signal on
the PI star and reference stars (the parallax filter), as well as to
keep exposure times greater than ∼30s and less than ∼600s, when
possible.
Because of a damaged Tek 2 V filter (referred to as oV) that occurred
in early 2005, the CTIOPI program used a comparable V filter (referred
to as nV) from 2005 to mid-2009. The astrometry is affected by this
change because the passbands were slightly different. It was
determined empirically that trigonometric parallax determinations are
sound if at least ∼1-2 years of data are available both before and
after the filter switch. However, subtle signals from a perturbing
companion would not be reliable. In 2009, it was determined that the
crack near the corner of the filter did not impact the FOV of the
CTIOPI data, as only the central quarter of the CCD is used. Thus, a
switch back to the original V (oV) was completed in mid-2009.
U. S. Naval Observatory Flagstaff Station (NOFS) astrometric data have
been collected with the Kaj Strand 61-in Astrometric Reflector using
three separate CCDs over the multiple decades that NOFS has measured
stellar parallaxes. Initially, a Texas Instruments (TI) 800*800
(TI800) CCD, followed by a Tektronics 2048*2048 (Tek2K) CCD, and most
recently an EEV (English Electric Valve, now e2v) 2048*4096 (EEV24)
CCD were used. The latter two cameras are still in operation at NOFS
for astrometric work and were used for all but two of the NOFS
parallaxes presented here. The TI800 CCD was used to measure the
parallaxes for WD0213+396 and WD1313-198. A total of four filters were
used for astrometric work. ST-R (also known as STWIDER) is centered
near 700nm with a FWHM of 250nm. A2-1 is an optically flat
interference filter centered near 698nm with a FWHM of 172nm. I-2 is
an optically flat interference filter centered near 810nm with a FWHM
of 191nm. Z-2 is an optically flat 3mm thick piece of Schott RG830
glass that produces a relatively sharp blue-edge cutoff near 830nm and
for which the red edge is defined by the CCD sensitivity. More details
on the filters can be found in C. Dahn et al. (2017, in preparation).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 121 108 Photometric results
table2.dat 153 76 Cerro Tololo Inter-American Observatory Parallax
Investigation (CTIOPI) astrometric results
table3.dat 145 38 U. S. Naval Observatory Flagstaff Station (NOFS)
astrometric results
table4.dat 127 103 Physical parameters
figure1.dat 27 9174 Southern Astrophysical Research Telescope
(SOAR)+Goodman confirmation spectra for newly
discovered nearby white dwarfs
figure3.dat 60 103 Data of the Hertzsprung-Russell diagram for the
objects with parallaxes presented here
figure7.dat 36 40 Component radial velocity curves for WD 1242-105
as a function of time
refs.dat 137 41 References
--------------------------------------------------------------------------------
See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
I/238 : Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)
I/98 : NLTT Catalogue (Luyten, 1979)
J/MNRAS/449/3966 : Ultracool white dwarfs (Gianninas+, 2015)
J/ApJS/219/19 : Census of SUPERBLINK nearby white dwarfs (Limoges+, 2015)
J/AJ/143/103 : New white dwarfs (Sayres+, 2012)
J/ApJ/743/138 : Spectroscopic survey of bright WDs (Gianninas+, 2011)
J/ApJ/663/1291 : DZ stars in SDSS DR4 (Dufour+, 2007)
J/AJ/134/252 : New nearby WD systems (Subasavage+, 2007; Pap. XIX)
J/ApJ/643/402 : Cool WDs in the solar neighborhood (Kawka+, 2006)
J/AJ/125/1598 : New northern high proper motion stars (Lepine+, 2003)
J/other/Sci/292.698 : Candidate halo dark matter (Oppenheimer+, 2001)
J/AJ/103/638 : USNO Photographic Parallaxes. I. (Monet+, 1992)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd) (1)
11 A1 --- m_WD [AB] White dwarf component (A or B)
13- 29 A17 --- OName Other name (1)
31- 35 F5.2 mag Bmag [12.34/51.45]? Johnson B band magnitude (BJ)
37 I1 --- o_Bmag [1/6]? Number of observations in Bmag (NB)
39- 43 F5.2 mag Vmag [11/18.1]? Johnson V band magnitude (VJ)
45 A1 --- u_Vmag [:] Uncertain flag in Vmag
47 I1 --- o_Vmag [1/6]? Number of observations in Vmag (NV)
49- 53 F5.2 mag Rmag [11.15/18]? Kron-Cousins R band magnitude (RKC)
55 A1 --- u_Rmag [:] Uncertain flag in Rmag
57 I1 --- o_Rmag [1/5]? Number of observations in Rmag (NR)
59- 63 F5.2 mag Imag [10.5/18.4]? Kron-Cousins I band magnitude (IKC)
65 A1 --- u_Imag [:] Uncertain flag in Imag
67 I1 --- o_Imag [1/6]? Number of observations in Imag (NI)
69 A1 --- Flt [VRI] Parallax filter π (V, R, or I) (2)
71- 77 F7.4 mag sigma [0/0.018]? The PI star (parallax target)
photometric standard deviation (σ) in
parallax filter (3)
79- 80 I2 --- Nn [9/38]? Number of nights (4)
82- 84 I3 --- Nf [44/235]? Number of frames (4)
86- 90 F5.2 mag Jmag [9.12/17.1]? 2MASS J band magnitude (J2M)
92- 95 F4.2 mag e_Jmag [0.02/0.1]? Error in Jmag
97-101 F5.2 mag Hmag [8.48/16.55]? 2MASS H band magnitude (H2M)
103-106 F4.2 mag e_Hmag [0.02/0.2]? Error in Hmag
108-112 F5.2 mag Kmag [8.19/16.2]? 2MASS Ks band magnitude (Ks2M)
114-117 F4.2 mag e_Kmag [0.02/0.21]? Error in Kmag
119-121 A3 --- Note Notes (5)
--------------------------------------------------------------------------------
Note (1): For the Cerro Tololo Inter-American Observatory Parallax Investigation
(CTIOPI) program, relative brightnesses were also recorded for the parallax
target (hereafter referred to as the "PI" star) compared to the astrometric
reference field stars in the filter used for the astrometry as part of the
CTIOPI reduction pipeline. From these data, we gauge whether the PI star
shows any variability. If any of the reference stars show variability above
∼2%, they are removed from the variability analysis. This analysis was not
performed for the U. S. Naval Observatory Flagstaff Station (NOFS) targets
as it was not part of the reduction pipeline. Photometry values are given
in this table.
Note (2): The filter of parallax observation.
Note (3): As a gauge for variability.
Note (4): Number of nights and frames used for the variability analysis.
Note (5): The codes for the notes are defined as follows:
a = Optical photometry values are adopted from Subasavage et al.
(2009AJ....137.4547S 2009AJ....137.4547S; Paper XXI);
b = Optical photometry values are adopted from Subasavage et al.
(2008AJ....136..899S 2008AJ....136..899S; Paper XX);
c = JHKS photometry has been transformed from the United Kingdom
Infra-Red Telescope (UKIRT) Infrared Sky Survey (UKIDSS) system using
the transformations of Hodgkin et al. (2009MNRAS.394..675H 2009MNRAS.394..675H);
d = Optical photometry values are adopted from Subasavage et al. 2007
(Cat. J/AJ/134/252; Paper XIX);
e = Optical photometry values include additional measures than those
presented in Subasavage et al. (2009AJ....137.4547S 2009AJ....137.4547S; Paper XXI) and,
thus, supercede the values presented in that publication;
f = Optical photometry values include additional measures than those
presented in Subasavage et al. 2007 (Cat. J/AJ/134/252; Paper XIX)
and, thus, supercede the values presented in that publication;
g = Likely variable at the ∼1-2% level;
h = Optical photometry values include additional measures than those
presented in Subasavage et al. (2008AJ....136..899S 2008AJ....136..899S; Paper XX) and,
thus, supercede the values presented in that publication;
i = Variability analysis is contaminated by a nearby source, hence the
brackets in the sigma column indicating erroneous variability;
j = Optical magnitudes for this close binary (ρ≃6.3'' at
PA=226.5°, epoch=2014.91832) are uncertain because of the marginal
calibrators for PSF photometry in the 6.8'2 Field of View (FOV);
k = JHKS magnitudes are from National Optical Astronomy Observatory
(NOAO) Extremely Wide-field Infrared Image (NEWFIRM) and are on the
MKO system;
N = The error in the Kmag value is NULL.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd)
11 A1 --- m_WD [AB] White dwarf component (A or B)
13- 25 A13 --- OName Other name
27- 28 I2 h RAh Hour of Right Ascension (J2000)
30- 31 I2 min RAm Minute of Right Ascension (J2000)
33- 37 F5.2 s RAs Second of Right Ascension (J2000)
39 A1 --- DE- Sign of the Declination (J2000)
41- 42 I2 deg DEd Degree of Declination (J2000)
44- 45 I2 arcmin DEm Arcminute of Declination (J2000)
47- 50 F4.1 arcsec DEs Arcsecond of Declination (J2000)
52 A1 --- Flt [VRI] Filter used for parallax observation (V, R,
or I)
54- 55 I2 --- Ns [3/17] Number of seasons the PI star was observed
(Nsea)
56 A1 --- f_Ns [cgs] Flag on Ns (c, g, or s) (1)
58- 60 I3 --- Nfr [44/235] Total number of frames used in the
parallax reduction (Nfrm)
62- 68 F7.2 yr Year0 [1999.64/2010.52] Starting time of coverage of
the parallax data
69 A1 --- --- [-]
70- 76 F7.2 yr Year1 [2007.6/2016.06] Ending time of coverage of the
parallax data
78- 82 F5.2 --- Nyr [2.18/16.19] Number of years during the coverage
84- 85 I2 --- Nref [5/22] Number of reference stars used (Nref)
87- 92 F6.2 mas Rplx [16.4/230.9] Relative trigonometric parallax
π(rel)
94- 97 F4.2 mas e_Rplx [0.54/2.67] Error in Rplx
99-102 F4.2 mas pcorr [0.28/2.37] Correction to absolute parallax
π(corr)
104-107 F4.2 mas e_pcorr [0.02/0.39] Error in pcorr
109-114 F6.2 mas Aplx [17.22/232.12] Absolute trigonometric parallax
π(abs)
116-119 F4.2 mas e_Aplx [0.54/2.67] Error in Aplx
121-126 F6.1 mas/yr pm [80.1/2970.6] Proper motion µ (2)
128-130 F3.1 mas/yr e_pm [0.1/1.7] Error in pm
132-136 F5.1 deg PA [17.9/345] Position Angle of proper motion (2)
138-141 F4.2 deg e_PA [0.01/0.89] Error in PA
143-147 F5.1 km/s Vtan [4.9/255] Tangential velocity (Vtan) (3)
149-153 A5 --- Note Notes (a, b, c, and/or d) (4)
--------------------------------------------------------------------------------
Note (1): The flags on the seasons number are defined as follows:
c = The observation was continuous throughout every season within the time
coverage;
g = In some cases, mostly because of the cracked V filter problem
discussed in Section 2.3.1, the "g" signifies a significant gap
(multiple years) in the observation;
s = The observation was scattered such that there is at least one season
with only one night's data (or no data for an entire season).
Note (2): Measured with respect to the reference field (i.e., relative, not
corrected for reflex motion due to the Sun's movement in the Galaxy).
Note (3): Not corrected for solar motion.
Note (4): The codes for the notes are defined as follows:
a = Astrometric determinations presented here supersede those of
Subasavage et al. (2009AJ....137.4547S 2009AJ....137.4547S; Paper XXI) because they
include additional data over ∼6 years;
b = New member of the 25-pc WD sample;
c = Object is discussed in Section 4.2;
d = Both oV and nV data were used to determine the astrometric solution as
described in Section 2.3.1.1 (in brief, because of a damaged Tek2 V
filter (referred to as oV) that occurred in early 2005, the CTIOPI
program used a comparable V filter (referred to as nV) from 2005 to
mid-2009).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd)
12- 13 I2 h RAh Hour of Right Ascension (J2000)
15- 16 I2 min RAm Minute of Right Ascension (J2000)
18- 22 F5.2 s RAs Second of Right Ascension (J2000)
24 A1 --- DE- Sign of the Declination (J2000)
26- 27 I2 deg DEd Degree of Declination (J2000)
29- 30 I2 arcmin DEm Arcminute of Declination (J2000)
32- 35 F4.1 arcsec DEs Arcsecond of Declination (J2000)
37- 40 A4 --- Flt Filter used for parallax observation (A2-1, I-2,
ST-R, or Z-2) (1)
42- 44 I3 --- Nn [22/173] Number of nights the PI star was
observed (Nngt)
46- 48 I3 --- Nfr [24/285] Total number of frames in the
astrometric reduction (Nfrm)
50- 56 F7.2 yr Year0 [1990.78/2013.2] Starting time of coverage of
the parallax data
57 A1 --- --- [-]
58- 64 F7.2 yr Year1 [1995.41/2016.43] Ending time of coverage of the
parallax data
66- 70 F5.2 --- Nyr [3.01/10.21] Number of years during the coverage
72- 73 I2 --- Nref [4/47] Number of reference stars (Nref)
75- 80 F6.2 mas Rplx [39.43/108.76] Relative trigonometric parallax
π(rel)
82- 85 F4.2 mas e_Rplx [0.22/1.34] Error in Rplx
87- 90 F4.2 mas pcorr [0.45/1.77] Correction to absolute parallax
π(corr)
92- 95 F4.2 mas e_pcorr [0.03/0.58] Error in pcorr
97-102 F6.2 mas Aplx [40.15/110.27] Absolute trigonometric parallax
π(abs)
104-107 F4.2 mas e_Aplx [0.23/1.34] Error in Aplx
109-114 F6.1 mas/yr pm [99.6/1915.2] Relative proper motion µ (2)
116-118 F3.1 mas/yr e_pm [0.1/0.7] Error in pm
120-124 F5.1 deg PA [47.4/348.4] Relative Position Angle of proper
motion (2)
126-129 F4.2 deg e_PA [0.01/0.14] Error in PA
131-135 F5.1 km/s Vtan [10.5/159.2] Tangential velocity (Vtan) (2)
137-141 A5 --- CCD CCD camera used for parallax observation (EEV24,
TI800, or Tek2K) (3)
143-145 A3 --- Note Notes (a or b) (4)
--------------------------------------------------------------------------------
Note (1): The four filters used for astrometric work are defined as follows:
A2-1 = Optically flat interference filter centered near 698nm with a FWHM
of 172nm;
ST-R = Described in detail by Monet et al. 1992 (Cat. J/AJ/103/638) and is
centered near 700nm with a FWHM of 250nm. Also known as STWIDER;
I-2 = Optically flat interference filter centered near 810nm with a FWHM
of 191nm;
Z-2 = Optically flat 3mm thick piece of Schott RG830 glass that produces a
relatively sharp blue-edge cutoff near 830nm and for which the red
edge is defined by the CCD sensitivity.
Note (2): Not corrected for solar motion.
Note (3): The cameras identifications are defined as follows:
EEV24 = English Electric Valve 2048*4096 (EEV24) CCD;
TI800 = Texas Instruments 800*800 (TI800) CCD;
Tek2K = Tektronics 2048*2048 (Tek2K) CCD.
Note (4): The codes for the notes are defined as follows:
a = New member of the 25-pc WD sample;
b = Object is discussed in Section 4.2.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd)
11 A1 --- m_WD [AB] White dwarf component (A or B)
13- 18 F6.2 mas [17/233] Adopted weighted mean trigonometric
parallax (1)
20- 23 F4.2 mas e_ [0.19/2.67] Error in
25 I1 --- o_ [1/5] Number of values
27- 37 A11 --- r_ References for ; in refs.dat file
39- 43 I5 K Teff [3490/23360]? Effective temperature (Teff)
45- 48 I4 K e_Teff [20/7640]? Error in Teff
50- 53 F4.2 [cm/s] logg [7.02/8.81]? Surface gravity
55- 58 F4.2 [cm/s] e_logg [0.01/0.14]? Error in logg
60- 65 A6 --- SpT Spectral type
67- 71 A5 --- r_SpT Reference for SpT; in refs.dat file
73- 81 A9 --- Model Atmospheric model used (He, He(+C), He(+Ca),
He(+H), or He(+H,Ca), or H)
83- 86 F4.2 Msun Mass [0.21/1.1]? Mass (M/M☉)
88- 91 F4.2 Msun e_Mass [0.01/0.11]? Error in Mass
93- 97 F5.2 mag VMag [10.5/16.66] Absolute V band magnitude (MV)
99-102 F4.2 mag e_VMag [0.02/0.21] Error in VMag
104-108 F5.2 Lsun Lum [-4.63/-1.34]? Luminosity (logL/L☉)
110-113 F4.2 Lsun e_Lum [0.01/0.49]? Error in Lum
115-118 F4.2 Gyr Age [0.03/8.6]? WD age (3)
120-123 F4.2 Gyr e_Age [0.01/0.84]? Error in age
125-127 A3 --- Note Notes (4)
--------------------------------------------------------------------------------
Note (1): The adopted parallaxes are weighted means in cases of multiple
parallax determinations for a system. Model parameters were determined
using these values. The r_ column identifies the source(s) of each
parallax.
Note (3): WD cooling age only, not including main-sequence lifetime.
Note (4): The codes for the notes are defined as follows:
c = Absolute V magnitude is determined from the best atmospheric model fit
given that no apparent magnitude was measured in the V-band;
d = No optical BVRI photometry was obtained, thus, the Spectral Energy
Distribution (SED) was derived from standardized SDSS gri taken at the
U. S. Naval Observatory Flagstaff Station (NOFS) 1.3-m telescope on a
photometric night. Photometric values are 15.42, 15.27, and 15.24 for
gri, respectively;
e = The best fit atmospheric model included [log He/H=-1.21];
f = The best fit atmospheric model included [log H/He=-3.5],
[log Ca/He=-10.21];
g = No optical BVRI photometry was obtained, thus, the Spectral Energy
Distribution (SED) was derived from SDSS ugriz photometry extracted
from DR12 (Alam et al. 2015, Cat. V/147);
h = Physical parameters are based on a single WD; however, there is
evidence that this object is an unresolved binary and thus, a single
star model does not accurately characterize the system;
i = The best fit atmospheric model included [log C/He=-6.49];
j = The best fit atmospheric model included [log C/He=-6.6];
k = While no Balmer lines are present in the spectra, as pointed out by
Giammichele et al. (2012ApJS..199...29G 2012ApJS..199...29G), the Ca H&K lines are too
sharp for a He-dominated atmosphere and thus, a pure-H model was
adopted;
l = The best fit atmospheric model included [log H/He=-3.5],
[log Ca/He=-10.99];
m = The best fit atmospheric model included [log H/He=-5.0],
[log Ca/He=-9.26];
n = The best fit atmospheric model included [log H/He=-3.7],
[log Ca/He=-10.57];
o = No satisfactory model fit was obtained, thus, derived parameters
are likely unreliable;
p = The best fit atmospheric model included [log C/He=-5.18];
q = The best fit atmospheric model included [log C/He=-7.15];
r = The best fit atmospheric model included [log H/He=-5.0],
[log Ca/He=-11.25];
s = The best fit atmospheric model included [log H/He=-5.0],
[log Ca/He=-9.38];
t = The best fit atmospheric model included [log C/He=-3.91];
u = The best fit atmospheric model included [log H/He=-5.0],
[log Ca/He=-8.63];
v = Effective temperature is the limit of the model grid and for which
additional pressure effects in this regime are not accounted;
w = The best fit atmospheric model included [log C/He=-5.14].
--------------------------------------------------------------------------------
Byte-by-byte Description of file: figure1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd)
12- 18 F7.2 0.1nm lambda [3700.02/6099.92] Wavelength λ (in Å)
20- 27 F8.6 --- Flux [0.24/2.08] Normalized flux (Fλ)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: figure3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [WD]
3- 10 A8 --- WD White Dwarf (WD) name (HHMM+DDd)
11 A1 --- m_WD [AB] White dwarf component (A or B)
13- 18 F6.2 mas [17.2/232.4] Weighted mean trigonometric parallax
21- 24 F4.2 mas e_ [0.19/2.67] Error in
26- 30 F5.2 mag VMag [10.5/16.63] Absolute V band magnitude
33- 36 F4.2 mag e_VMag [0.03/0.21] Error in VMag
38- 42 F5.2 mag V-I [-0.29/1.92] V-I color index
45- 48 F4.2 mag e_V-I [0.04/0.07] Error in V-I
50- 60 A11 --- r_ References for ; in refs.dat file
--------------------------------------------------------------------------------
Byte-by-byte Description of file: figure7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 s Time [0/13227] Relative time of observation (1)
10- 16 F7.2 km/s V1RV [-157.71/208.69] V1 Radial Velocity
18- 22 F5.2 km/s e_V1RV [4.28/12.5] Error in V1RV
24- 30 F7.2 km/s V2RV [-81.16/180.42] V2 Radial Velocity
32- 36 F5.2 km/s e_V2RV [2.63/10.26] Error in V2RV
--------------------------------------------------------------------------------
Note (1): The Julian Date corresponding to time=0 is 2456040.59137 and the
Heliocentric Julian Date corresponding to time=0 is 2456040.59684.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference code
4- 22 A19 --- BibCode Bibliographic Code
24- 44 A21 --- Aut Author's name
46-137 A92 --- Com Comment
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
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Kar et al., Paper LI 2024AJ....167..196K 2024AJ....167..196K, Cat. J/AJ/167/196
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 03-Oct-2017