Wide CPM companion to G 158-77 (Eggen & Greenstein
1965ApJ...142..925E). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G). Farihi
(2009MNRAS.398.2091F) suggests that this is a triple system containing an
unresolved double degenerate system and also identifies G 158-77 as an
M0V on the basis of photometry. However, Gracés, Catalán & Ribas
(2011A&A...531A...7G) give a spectral type of K6V, while Arazimová, Kawka &
Vennes (2010ASPC..435..147A) give K7.5V. Our mass estimate is closer to K6V.
A wide binary first noted by Greenstein (1984ApJ...276..602G) who
gives DA3+sdM. Our WD parameters are taken from Limoges & Bergeron
(2010ApJ...714.1037). Dhital et al. (2010AJ....139.2566D) in the Sloan
Low-mass Wide Pairs of Kinematically Equivalent Stars Catalog estimates type
and distance of the main sequence companion to be K7.1V. The WD is SDSS
J0043302.80-214512.8 and the K star is SDSS J004301.59-214527.9.
Unresolved DA companion to the photospherically spotted G5 giant
AY Cet. The orbital period of 56.8 days for this star are taken from Simon,
Fekel & Gibson (1985ApJ...295..153S), who also estimate a Teff=18,000K
and logg=8. From the IUE Lyman alpha profile we estimate a mass of
0.62M☉ for the WD and use the mass estimate of the G5III companion of
2.2M☉ from Tautvaišiene et al. (2011AN....332..925T). From their
analysis of the radial velocity variations Simon et al. (1985ApJ...295..153S)
estimate an orbital asini=0.041AU and give a mass function. Using the
mass estimates in Table 2 we find a=0.041AU.
(GJ 86B). The primary K0V star (GJ 86) hosts the giant
exoplanet (GJ86b). Searches for further faint companions (Els et al.
2001A&A...370....1S) detected a faint star 2'' from the primary. Mugrauer &
Neuhauser (2005MNRAS.361L..15M) obtained J, H & K band photometry and showing
it to be a WD and presented evidence of orbital motion. Recent HST photometry
and spectrometry of Farihi et al. (2013MNRAS.430..652F) clearly show the
orbital motion of the WD as well as identifying the star as a DQ making the
system remarkable similar to Procyon A and B. WD parameters, orbital positions
and WD mass are from Farihi et al. (2013MNRAS.430..652F).
Unresolved companion to the barium star HD 13611. It was
discovered as an UV excess by Böhm-Vitense, & Johnson
(1985ApJ...293..288B). The masses of the WD and primary star are poorly known
but are taken from Böhm-Vitense, & Johnson. Speckle observations of Roberts
(2011MNRAS.413.1200R) give a separation upper limit of 0.16'' while Hipparcos
astrometry gives an orbital period of P=4.496yr (Pourbaix, & Boffin
A CPM pair from Oswalt & Strunk 1994AAS...184.2809O. WD parameters are taken from Eisenstein
et al. (2006ApJS..167...40), Kleinman et al. (2013ApJS..204....5K) however,
give no mass estimate. Our distance is estimated spectroscopically from the
Identified as a magnetic DB (Reimers, et al. 1998A&A...337L..13R).
However, Schmidt et al. (2001MNRAS.328..203S) interpret the spectra as an
unresolved hot non-magnetic DA plus a K5V companion, of comparable magnitude.
This is the well studied eclipsing pre-CV system V 471 Tau. WD and
companion parameters are taken from O'Brien, Bond & Sion
(2001ApJ...563..971O). Guinan & Ribas (2001ApJ...546L..43G) have used eclipse
timings to infer a third body, possibly a brown dwarf, in a 30 year orbit.
(40 Eri B) This is a well known triple system with the DA white
dwarf and companion M star (40 Eri C) orbiting the K0.5V star
HD 25535 at distance 415AU. While the dynamical mass and
gravitational redshift for the white dwarf are known with respect to 40 Eri C
(see Holberg et al. 2012AJ....143...68H), the Sirius-Like nature of this
system pertains top 40 Eri A.
(ε Ret B) Long known as a resolved binary system,
the faint companion was not recognized as a WD until Chauvin et al.
(2006A&A...456.1165C) obtained near IR photometry demonstrating its degenerate
nature. Echelle spectra of the WD obtained by Farihi et al.
(2011MNRAS.417.1735F) revealed it to be DA3.5 WD in a P>2665 yr orbit. This
system also contains a giant planet (HD 27442b) with a mass>1.6MJ in a
The WD companion of the Hyades Cluster star HD 27483 was
discovered from an IUE UV excess by Böhm-Vitense (1993AJ....106.1113B). The
primary consists of two F6V stars in a 3.05 day orbit. In estimating the
orbital period of the WD, the primary mass in Table 2 assumes two F6V stars.
This system was resolved at 1.276" by Barstow et al. 2001MNRAS.322..891B. We estimate orbital period of
275yrs, well above the system scenarios considered by Böhm-Vitense et al.
Noted as an IUE UV excess source by Landsman et al.
(1993PASP..105..841L) and an EUV excess source by Wonnacott, Kellett &
Strickland (1993MNRAS.262..277W). The primary is the K0IV star <&smb.query "HR
1608">. Vennes et al. determine a radial velocity period of 903d. The
system was not resolved by Barstow et al. 2001MNRAS.322..891B. The WD parameters are taken from Kawka &
Hodgkin et al. (1993MNRAS.263..229H) first noted the EUV excess in
the C component of the 14 Aur system. Barstow et al. 2001MNRAS.322..891Bhave shown this system to consist
of at least five physical components: an unresolved spectroscopic binary 14
Aur A (KW Aur) of spectral type A9V; an unresolved spectroscopic
binary 14 Aur Ca of spectral type F2V; and 14 Aur Cb which is the
DA WD responsible for the EUV excess. The nature of short period (days) for
the orbital companions of 14 Aur A and 14 Aur C is unknown.
In Table 1 the separation and position angle of the WD are with respect to Ca,
Component A is more distant at 15''. Vennes et al. (1998ApJ...502..763V) find
an orbital period of 0.00819 yrs, however as noted by Barstow et al. 2001MNRAS.322..891Bthis cannot be due
to the WD. We estimate an orbital period in Table 2 of 2430 yrs. The WD
parameters used here are those of Vennes et al. (1998ApJ...502..763V).
A widely separated CPM pair noted by Greenstein
(1980ApJ...242..738G) who designated the WD a DC. Little is known of the faint
DC WD. Our V magnitude comes from T. Oswalt & J.A. Smith, private
The unresolved hot DA companion to the B3V star HD 59635
(y Pup) detected as an EUV excess source by Burleigh & Barstow
(1998MNRAS.295L..15B). Parthasarathy et al. (2007NewAR..51..524P) estimate the
mass of the white dwarf to be 1M☉based on the assumption that it is the
remnant of a star more massive than HD 59635. Vennes
(2000A&A...354..995V) has shown that HD 59635 is actually a close binary
with a B6V companion in a 15 day orbit.
Little is known of this system beyond its listing in Stepanian
(2005RMxAA..41..155S) as `DA+G'. SDSS photometry shows composite colors. In
the GALEX survey this system also appears as a UV excess object.
This DA1.3 WD was discovered as a suspected CPM companion to the
A2V star HD 74389 by Sanduleak & Pesh (1990PASP..102..440S). Its
separation is (20.1'') and its 84.3°position angle places it inconveniently
near the diffraction spikes from the primary star in many telescopes (Liebert,
Bergeron & Saffer 1990PASP..102.1126L). In support of the interpretation of a
common distance for the WD and the A2 star Holberg, Bergeron, & Gianninas
(2008AJ....135.1239H) find a spectroscopic distance of 119 ±2.25pc vs
111.5±7pc for HD 74389 from the Hipparcos parallax. Also evident
in 2MASS and SDSS finder images is a second bluish star with a separation and
position angle of 10'' and 345°. Recent Hαspectra of this star show a
weak narrow Hαabsorption profile embedded in a featureless continuum,
reminiscent of sdB stars. This star appears to share the proper motion of
HD 74389. Not previously reported, is a third star buried within the glare of
the primary at an estimated separation and position angle of 5'' and 270°.
Recent spectra of this star show it to be an M-star; no proper motion
information is available.
The EUV excess in βCrt was discussed in
Fleming et al. (1991A&A...246L..47F). Burleigh et al. (2001MNRAS.327.1158B)
analyzed the FUSE and EUVE spectra of βCrt, finding a very low mass
(0.43M☉) indicating a history of interacting binary evolution resulting in
a He-core WD. The system was not resolved by Barstow et al. 2001MNRAS.322..891B, indicating a semi-major
axis of less than 9.3AU and an orbital period of less than a decade. There is
ample evidence of radial velocity variations but no agreement on an orbital
period. Recently a spectroscopic orbit for the primary shows a 6yr orbital
period, (D. Willmarth, private com.).
VB 04 is the CPM of HD 100623 (Van Biesbroeck
1961AJ.....66..528V). Although separated by 16'' from its 6th mag. primary
star there is no definitive determination of temperature or mass. A spectrum
showing its DC nature is shown in Giammichele, Bergeron & Dufour
(2012ApJS..199...29G). Dieterich et al. (2012AJ....144...64D) gives K0.0V for
A barely resolved hot WD around the central star of the planetary
nebula PK 303+40.1 (A35). The WD parameters are from Heald & Bianchi
(2002ApJ...580..434H) who studied this system with, FUSE, STIS and IUE. The
separation is the mean of the values given in Gatti et al.
This source corresponds to the EUV source RE J1309+081
and it is thought to be hot DA WD companion to a V=11.5 F9V star. The SDSS
field shows no blue objects other than the F9V star. Barstow et al. 2001MNRAS.322..891Bfailed to resolve
this source with WFPC2 imaging.
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. SDSS spectrum shows a featureless DC
continuum. Assuming a logg of 8 the SDSS photometry indicates a Teff
of 7000K a distance of 79pc and a mass of 0.79M☉.
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. The DA WD was observed by Eisenstein et
al. (2006ApJS..167...40) who obtained Teff = 12,960 ±140 K and log
g=7.86 ±0.03. The distance of 139±3pc is calculated from the SDSS
This unresolved Sirius-Like system involving a G8II-III barium
star was noted as a spectroscopic binary (de Medeiros & Mayor
1999A&AS..139..433D). This was followed by (Frankowski et al.
2007A&A...464..377F) who subsequently noted it to be a proper motion binary
from Hipparcos data. Stefanik, et al. (2011AJ....141..144S) have analyzed all
available radial velocity and astrometric data, including an unpublished IUE
spectrum which clearly establishes the DA nature of the companion. They have
determined an orbital period of 1.71 yrs and estimated the temperature and
mass of the WD companion and re-estimated the Hipparcos parallax. In Tables 1
and 2 we have used the Stefanik results to estimate a spectroscopic mass of
0.80M☉ for the WD.
Discovered as a nearby wide CPM system by Stephenson, Sanduleak,
& Hoffliet (1968PASP...80...92S). A bright well studied DA WD within 20pc,
whose companion HR 6094 (HD 147513) also has an exoplanet (HD147513b)
with a period of 528.4 days at a distance of 1.32AU. The WD is widely
separated (4895pc) from HR 6094 and its exoplanet. The WD parameters
are taken from Holberg et al. (2012AJ....143...68H).
Is an unresolved companion to the B9.5V star 16 Dra discovered by
Burleigh & Barstow (1998MNRAS.295L..15B). 16 Dra is in turn associated with
17 DraA/B, respectively a B9V and A1V pair. The Teff and logg of the
WD are poorly defined by the EUVE spectrum.
The unresolved companion to λSco which
Burghoeffer, Vennes & Dupuis (2000ApJ...538..854B) identify as source of the
soft X-ray and EUV excess as a massive hot DA WD. The primary has an orbital
velocity period of 5.959 days but the companion is uneclipsed. Burghoeffer et
al. use EUV and orbit constraints to estimate the companion must be very
massive (>1.25M☉ and hot (>64000K).
The WD is a companion to the BaII star (HD 160538). Fekel
et al. (1993AJ....106.2370F) find an IUE UV continuum corresponding DA with a
Teff = 30000 K and log = 8 (which corresponds to a mass of 0.65M☉) and
a radial velocity orbit having a period of 14.24 yrs and an estimated
separation of 1.84AU.
Discovered by accidently by Böhm-Vitense (1992AJ....104.1539B)
with IUE while observing HD 160365. Böhm-Vitense determines that
the WD is a visual binary located approximately 8" south of the F6III star.
Noted as CPM by Eggen & Greenstein (1965ApJ...142..925E). The WD
is a companion to the Ba II star (HD 165141). Fekel et al.
(1993AJ....106.2370F) find an IUE UV continuum corresponding DA with a
Teff=35000K, logg=8 (which corresponds to a mass of 0.66M☉) and a
radial velocity orbit having a period of 2.47yr an estimated separation of
Noted as a possible UV excess in the mild barium star ζCyg by
Böhm-Vitense (1980ApJ...239L..79B) and confirmed by Dominy & Lambert
(1983ApJ...270..180D), who estimate a Teff 12000 K for the WD. Griffin
& Keenan (1992Obs...112..168G) give a radial velocity period of 17.8 yrs. WD
was resolved with WFPC2 (Barstow et al. 2001MNRAS.322..891B) at 0.032'' giving projected separation of
First noted as an EUV excess in the A8V star IK Peg (Wonnacott,
Kellett & Strickland 1993MNRAS.262..277W), and confirmed as a UV excess by
Landsman, Simon, & Bergeron (1993PASP..105..841L). Vennes et al.
(1998ApJ...502..763V) determine an orbital period of 0.05947 yrs. The WD is
massive (1.20M☉) Vennes & Kawka (2008MNRAS.389.1367V). The physical
separation computed from the orbital period and the assumed masses. The system
was not resolved with WFPC2 in Barstow et al. 2001MNRAS.322..891B.
First noted as a CPM pair by Greenstein (1969ApJ...158..281G), who
designated the companion as `sdK8'. The pair has been included in several
gravitational redshift and IFMR studies but no further spectral type is given
for the companion. Using the distance modulus for the WD (2.95) the absolute V
magnitude of the companion is +8.62, making it a border line K9 or M0 star and
the least luminous companion among the Sirius-Likes in this paper. The WD is a
ZZ Ceti variable analyzed in Gianninas et al. (2005ApJ...631.1100G), where the
WD parameters used here are from, including the distance of 38.9pc.
(56 Peg B) The unresolved companion of the mild BaII star
HD 218356 discovered by Schlndier et al. (1982ApJ...263..269S) as a
UV spectral excess. Griffin (2006Obs...126....1G) finds a low amplitude
radial velocity curve with a period of 111.140 days and gives a mass function
and an asini constraint.