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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 (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). 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; 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). 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; Paper XXI); b = Optical photometry values are adopted from Subasavage et al. (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); 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; 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; 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 pm [80.1/2970.6] Proper motion µ (2) 128-130 F3.1 mas 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; 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 pm [99.6/1915.2] Relative proper motion µ (2) 116-118 F3.1 mas 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 <plx> [17/233] Adopted weighted mean trigonometric parallax (1) 20- 23 F4.2 mas e_<plx> [0.19/2.67] Error in <plx> 25 I1 --- o_<plx> [1/5] Number of <plx> values 27- 37 A11 --- r_<plx> References for <plx>; 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_<plx> 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), 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 <plx> [17.2/232.4] Weighted mean trigonometric parallax 21- 24 F4.2 mas e_<plx> [0.19/2.67] Error in <plx> 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_<plx> References for <plx>; 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: Henry et al., Paper I 1994AJ....108.1437H Kirkpatrick et al., Paper II 1995AJ....109..797K Simons et al., Paper III 1996AJ....112.2238S Henry et al., Paper IV 1997AJ....114..388H Patterson et al., Paper V 1998AJ....115.1648P Henry et al., Paper VI 2002AJ....123.2002H Jao et al., Paper VII 2003AJ....125..332J Hambly et al., Paper VIII 2004AJ....128..437H Golimowski et al., Paper IX 2004AJ....128.1733G Henry et al., Paper X 2004AJ....128.2460H Deacon et al., Paper XI 2005AJ....129..409D Subasavage et al., Paper XII 2005AJ....129..413S, Cat. J/AJ/129/413 Jao et al., Paper XIII 2005AJ....129.1954J Costa et al., Paper XIV 2005AJ....130..337C Subasavage et al., Paper XV 2005AJ....130.1658S, Cat. J/AJ/130/1658 Costa et al., Paper XVI 2006AJ....132.1234C Henry et al., Paper XVII 2006AJ....132.2360H Finch et al., Paper XVIII 2007AJ....133.2898F, Cat. J/AJ/133/2898 Subasavage et al., Paper XIX 2007AJ....134..252S, Cat. J/AJ/134/252 Subasavage et al., Paper XX 2008AJ....136..899S Subasavage et al., Paper XXI 2009AJ....137.4547S Riedel et al., Paper XXII 2010AJ....140..897R Winters et al., Paper XXIII 2011AJ....141...21W, Cat. J/AJ/141/21 Jao et al., Paper XXIV 2011AJ....141..117J Boyd et al., Paper XXV 2011AJ....142...10B, Cat. J/AJ/142/10 Riedel et al., Paper XXVI 2011AJ....142..104R Boyd et al., Paper XXVII 2011AJ....142...92B, Cat. J/AJ/142/92 Dieterich et al., Paper XXVIII 2012AJ....144...64D, Cat. J/AJ/144/64 Cantrell et al., Paper XXIX 2013AJ....146...99C Mamajek et al., Paper XXX 2013AJ....146..154M Jao et al., Paper XXXI 2014AJ....147...21J Dieterich et al., Paper XXXII 2014AJ....147...94D, Cat. J/AJ/147/94 Riedel et al., Paper XXXIII 2014AJ....147...85R, Cat. J/AJ/147/85 Lurie et al., Paper XXXIV 2014AJ....148...91L Winters et al., Paper XXXV 2015AJ....149....5W, Cat. J/AJ/149/5 Hosey et al., Paper XXXVI 2015AJ....150....6H, Cat. J/AJ/150/6 Benedict et al., Paper XXXVII 2016AJ....152..141B, Cat. J/AJ/152/141 Winters et al., Paper XXXVIII 2017AJ....153...14W, Cat. J/AJ/153/14
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 03-Oct-2017
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