Notes on Sirius-like systems

Additional useful information not included in table1 or table2 (Appendix A)

WD 0022-745 Simbad
Identified by Burleigh, Barstow, & Fleming (1997MNRAS.287..381B) as a ROSAT EUV excess source associated with HD 2133. The WD mass is estimated from the Teff and logg of Burleigh et al. (1997MNRAS.287..381B). This close DA+F7V system was resolved with WFPC2 by Barstow et al. 2001MNRAS.322..891B.

WD 0023-109 Simbad
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.

WD 0030+444 Simbad
Suggested as a CPM by Greenstein (1974ApJ...189L.131G). WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 0040-220 Simbad
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.

WD 0041+092 Simbad
An EUV excess source associated with BD +08 102, first noted by Fleming et al. (1991A&A...246L..47F). The WD parameters are taken from Kawka & Vennes (2010ASPC..435..189K). The system was unresolved by WFPC2 (Barstow et al. 2001MNRAS.322..891B).

WD 0042+140 Simbad
A CPM system (OHL), listed as G6+DC. WD possibly shows Ca H & K lines, which would indicate a DZ. Little additional information is available. The V-band magnitude is estimated from the SDSS magnitude.

WD 0052+115 Simbad
A faint CPM system from Oswalt & Strunk 1994AAS...184.2809O listed as DB+late F or early G. No reliable distance estimate is available.

WD 0114+027 Simbad
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.

WD 0208-510 Simbad
(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).

WD 0210+086 Simbad
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 2003A&A...398.1163P).

WD 0221+399 Simbad
A CPM system (OHL) classification spectra gives dK+cool DC. It is also listed as DC in Reid (1996AJ....111.2000R). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 0226-615 Simbad
Discovered as an UV excess source associated with the F3IV/V star HD 15638 Landsman, Simon, & Bergeron (1993PASP..105..841L) and an ROSAT EUV excess source by Barstow et al. (1994MNRAS.270..516B). The WD parameters used here are taken from Kawka & Vennes (2010ASPC..435..189K). Vennes et al. (1998ApJ...502..763V) found no velocity variations in the primary star. The system was unresolved by WFP2 (Barstow et al. 2001MNRAS.322..891B). The estimated orbital period is less than 54 yrs.

WD 0227-005 Simbad
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 K0V companion.

WD 0250-007 Simbad
A CPM system (OHL). WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 0252-055 Simbad
The EUV excess source associated with HD 18131 discussed by Vennes et al. (1995A&A...299L..29V). The WD parameters used here are from Kawka & Vennes (2010ASPC..435..189K). Vennes et al. (1998ApJ...502..763V) noted evidence of low level radial velocity variations. The system was unresolved by WFPC2 (Barstow et al. 2001MNRAS.322..891B).

WD 0304+154 Simbad
A narrowly separated CPM system from Oswalt & Strunk 1994AAS...184.2809O, which list the system as DA+K6V. Lee (1984AJ.....89..720L) gives K3V and a spectroscopic parallax of 0.014".

WD 0315-011 Simbad
A CPM system (OHL). WD data is from Catalán et al. (2008A&A...477..213C).

WD 0338-388 Simbad
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.

WD 0347+171 Simbad
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.

WD 0353+284 Simbad
An EUV source and a barium-rich K2V star (Jeffries & Smalley 1996A&A...315L..19J).

WD 0354-368 Simbad
First detected as the X-ray source MS0354.6-3650 by Einstein (Stocke et al. 1991ApJS...76..813S) and later as the EUV source EUVE J0356-366 by Christian et al. (1996AJ....112..258C) from which the WD parameters were taken. The system was resolved by WFPC2 (Barstow et al. 2001MNRAS.322..891B).

WD 0400-346 Simbad
The WD was identified as a CPM companion separated by some 64'' from HD 25535 by Gould & Chanamé (2004ApJS..150..455G). The WD parameters are taken from Kawka, Vennes & Németh (2010ASPC..435..127K).

WD 0413-077 Simbad
(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.

WD 0415-594 Simbad
(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 428day orbit.

WD 0418+137 Simbad
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.

WD 0421+338 Simbad
First discovered by Landsman, Simon, & Bergeron (1996PASP..108..250L) as a UV excess in 56 Per. The WD parameters are taken from Landsman et al. (1996PASP..108..250L). 56 Per is quadruple system resolved by WFPC2 (Barstow et al. 2001MNRAS.322..891B), and is discussed in the text.

WD 0433+270 Simbad
A cool CPM companion to HD 283750 (OHL). It also contains a brown dwarf candidate HD 283750b system with a separation of 0.025'' (Lucas & Roach 2002MNRAS.336..637L). WD parameters are taken from Zhao et al. (2011AJ....141..107Z).

WD 0457-103 Simbad
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 & Vennes (2010ASPC..435..189K).

WD 0458-364 Simbad
This corresponds to the EUV and UV excess in the uncataloged V=13.7 K6V star discussed by Burleigh, Barstow & Holberg (1998MNRAS.300..511B).

WD 0512+326 Simbad
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).

WD 0551+123 Simbad
A narrowly separated CPM system from Oswalt & Strunk 1994AAS...184.2809O, who give spectral types of DA+G9V.

WD 0551+560 Simbad
A narrowly separated CPM system from Oswalt & Strunk 1994AAS...184.2809O. Very little is known concerning either component.

WD 0615-591 Simbad
A CPM system from OHL. The WD parameters are from Bergeron et al. (2011ApJ...737...28B).

WD 0642-166 Simbad
Well known resolved companion to Sirius with a well established orbit and within 20pc.

WD 0642-285 Simbad
A CPM system from Oswalt & Strunk 1994AAS...184.2809O. WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G)and the WD V magnitude from T. Oswalt & J.A. Smith, private communication.

WD 0658+712 Simbad
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 communication.

WD 0659+130 Simbad
Noted as an unresolved EUV source by Vennes et al. (1997A&A...318L...9V). The Distance of 115pc is from Barstow et al. (2010ApJ...723.1762B), while WD parameters are taken from Kawka & Vennes (2010ASPC..435..189K).

WD 0727-387 Simbad
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.

WD 0736+053 Simbad
The well studied resolved companion to Procyon with a well established orbit. The WD and K5IV/V companion parameters are taken from Liebert et al. (2013ApJ...769....7L).

WD 0743-336 Simbad
VB 03 is the CPM companion of HR 3018 (Van Biesbroeck 1961AJ.....66..528V) and one of coolest WD stars and widest binary among the Sirius-Like systems (Kunkel, Liebert & Boronson 1984PASP...96..891K).

WD 0834+576 Simbad
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.

WD 0842+490 Simbad
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.

WD 0845-188 Simbad
Noted as a CPM system by Greenstein (1984ApJ...276..602G). The WD parameters are from Bergeron et al. (2011ApJ...737...28B). The WD is a flux standard.

WD 0905-724 Simbad
First detected as a UV excess source associated HR 3643 by Landsman et al. (1996PASP..108..250L), where the WD parameters used here are taken. The system was not resolved with WFPC2 by Barstow et al. 2001MNRAS.322..891B.

WD 0911+023 Simbad
Is the unresolved hot DA companion to the B9.5V star θHyd discovered by Burleigh & Barstow (1999A&A...341..795B).

WD 0930+815 Simbad
Discovered as a UV excess in the K3 giant HD 81817 by Reimers (1984A&A...136L...5R).

WD 1004+665 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. Distance of 63pc estimated from Reimers (1984A&A...136L...5R).

WD 1009-184 Simbad
The CPM companion to BD-17 3088 noted by Holberg et al. (2008AJ....135.1239H) and within 20pc.

WD 1021+266 Simbad
Associated with the EUV excess in HD 90052 (Vennes et al. 1998ApJ...502..763V). The system was not resolved by Barstow et al. 2001MNRAS.322..891B.

WD 1024+326 Simbad
Identified as an EUVE excess source by Génova et al. (1995AJ....110..788G). The WD parameters are taken from Kawka & Vennes (2010ASPC..435..189K).

WD 1027-039 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. Distance estimate from Zhao et al. (2011AJ....141..107Z).

WD 1107-257 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O and also from Gould & Chanamé (2004ApJS..150..455G).

WD 1109-225 Simbad
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.).

WD 1130+189 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O, which list the system DA+G2V.

WD 1132-325 Simbad
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 the primary.

WD 1133+619 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O and also from Gould & Chanamé (2004ApJS..150..455G). Oswalt & Strunk 1994AAS...184.2809O lists the system as DZ+K5V.

WD 1209-060 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O, which lists the system as DC+K5V. WD parameters from Garcés et al. (2011A&A...531A...7G)

WD 1227+292 Simbad
A wide pair from OHL, little else is known about this system.

WD 1250-226 Simbad
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. (1998MNRAS.301L..33G).

WD 1304+227 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1306+083 Simbad
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.

WD 1354+340 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O. The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1425+540 Simbad
Noted as a CPM by Greenstein (1984ApJ...276..602G). The WD parameters are from Bergeron et al. (2011ApJ...737...28B).

WD 1440+068 Simbad
A wide pair from Oswalt & Strunk 1994AAS...184.2809O.

WD 1455+300 Simbad
Identified by Gould & Chanamé (2004ApJS..150..455G) as a CPM companion to BD +30 2592 with a separation of 23''.

WD 1501+301 Simbad
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☉.

WD 1514+411 Simbad
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 photometry.

WD 1516+207 Simbad
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.

WD 1542+729 Simbad
A CPM pair from Oswalt & Strunk 1994AAS...184.2809O, where the WD is listed as a DC. This system is also noted in Gould & Chanamé (2004ApJS..150..455G), with no WD spectral type given.

WD 1544-377 Simbad
Noted as a CPM companion by Wegner (1973MNRAS.163..381W). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1619+123 Simbad
Noted as a CPM by Farihi, Becklin, & Zuckerman (2005ApJS..161..394F). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1620-391 Simbad
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).

WD 1623+022 Simbad
(Also LPSM J1626+0210N, from Lépine & Shara 2005, Cat. I/298) Identified by Gould & Chanamé (2004ApJS..150..455G) as a CPM companion to LSH 3194. Reid & Gizis (2005PASP..117..676R) give DC spectral type.

WD 1634-573 Simbad
The DOZ1 companion to HD 149499. It is both a UV and EUV source and the WD parameters are taken from Jordan et al. (1997A&A...318..461J). The separation and position angle are taken from Holden (1977PASP...89..588H).

WD 1635+530 Simbad
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.

WD 1659-531 Simbad
A wide pair from OHL. The WD parameters from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1706+332 Simbad
Noted as a CPM by Greenstein (1984ApJ...276..602G). The WD parameters are from Holberg et al. (2012AJ....143...68H).

WD 1710+683 Simbad
Noted as a CPM by Greenstein (1984ApJ...276..602G). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1730-370 Simbad
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).

WD 1734+742 Simbad
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.

WD 1736+133 Simbad
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.

WD 1750+098 Simbad
Noted as a CPM in Eggen & Greenstein (1965ApJ...142..925E). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 1803-482 Simbad
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 0.277AU.

WD 1848+688 Simbad
(LDS 2471B) the CPM companion to BD +68 1027 (Lépine & Shara 2005, Cat. I/298, and Gould & Chanamé 2004ApJS..150..455G))

WD 1921-566 Simbad
Noted as a EUV excess in Barstow et al. (1994MNRAS.270..516B). The WD parameters are taken from Kawka & Vennes (2010ASPC..435..189K). The system was resolved with WFPC2 in Barstow et al. 2001MNRAS.322..891B.

WD 2048+809 Simbad
Noted as a CPM by Greenstein (1984ApJ...276..602G). The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 2110+300 Simbad
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 1.6AU.

WD 2123-226 Simbad
Noted as a UV excess in the barium star <&smb.query "* zet Cap"|"ζ Cap"> by Böhm-Vitense (1980ApJ...239L..79B), who estimate a Teff  23000 K for the WD.

WD 2124+191 Simbad
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.

WD 2129+000 Simbad
A wide CPM first noted as containing a WD by Kuiper (1943ApJ....97..275K). The WD parameters are taken from the analysis of DB stars by Bergeron et al. (2011ApJ...737...28B).

WD 2217+221 Simbad
Identified as a CPM in Hintzen (1986AJ.....92..431H), also noted as a CPM pair in Gould & Chanamé (2004ApJS..150..455G). Relatively little is known of either star.

WD 2253-081 Simbad
A wide CPM from Oswalt & Strunk 1994AAS...184.2809O. The WD parameters are from Gianninas, Bergeron & Ruiz (2011ApJ...743..138G).

WD 2257-073 Simbad
Noted as an EUV excess system by Barstow et al. (1994MNRAS.270..516B). The WD parameters are taken from Barstow et al. (2010ApJ...723.1762B) and Kawka & Vennes (2010ASPC..435..189K).

WD 2258+406 Simbad
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.

WD 2301+762 Simbad
A CPM system from OHL. Spectral is type from Greenstein (1984ApJ...276..602G).

WD 2304+251 Simbad
(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.

WD 2350-083 Simbad
Noted as a CPM by Greenstein (1980ApJ...242..738G). WD parameters from Zhao et al. (2012ApJ...746..144Z)

WD 2350-706 Simbad
Noted as an EUV excess source by Barstow et al. (1994MNRAS.270..516B). The system was resolved with WFPC2 (Barstow et al. 2001MNRAS.322..891B). The WD parameters are taken from Kawka & Vennes (2010ASPC..435..189K).

Last revised: 2014-11-23


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