The Big List of SW Sextantis Stars (v4.1.1 - Oct 2011)

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The Big List of SW Sextantis Stars (v4.1.1 - Oct 2011)

Introduction

The SW Sextantis stars are a sub-class of cataclysmic variables (CVs) that share a number of characteristic observational properties (e.g., transient absorption in their emission line cores that appears at specific orbital phases, single-peaked emission lines rather than the double-peaked lines characteristic of disk-accreting CVs, indications of very high mass transfer rate, etc. – follow this link for a more complete and detailed list of the observational characteristics of the SW Sex stars). Although studied individually for a number of years, the SW Sex stars were first identified as an observationally similar group in the early 1990s.

Establishing a complete census of membership in the SW Sex class is a difficult task, as our understanding of the range and possible origins of the SW Sex syndrome has evolved over the past two decades. For example, original defining characteristics of being a high inclination (i.e., eclipsing) CV and having He II λ4686 emission comparable in strength to that of Hβ have been relaxed as it has become apparent that these were likely selection effects that influenced the discovery of the first SW Sex stars. Meanwhile, some recent work has suggested that the SW Sex stars might be the weakest magnetic CVs with the highest mass transfer rates (follow this link for a discussion of the magnetic scenario for the SW Sex stars), while other theories utilize complex accretion disk structural models (e.g., tilted, warped, precessing disks).

Townsley & Gänsicke (2009) make the following interesting statement about the possible origin of the SW Sex syndrome: “Speculating that high [white dwarf effective temperature] and [mean mass transfer rate] are a common characteristic to all VY Scl/SW Sex stars suggests that these systems represent an exceptional phase in CV evolution. One possible explanation is that these are systems that just evolved into a semi-detached configuration, as the mass transfer goes through a short peak during turn-on (e.g., D'Antona et al. 1989), and that CVs are preferentially born within the 3-4 hr period range, which would be the case if the initial mass distribution is peaked toward equal masses in the progenitor MS binaries (de Kool 1992).”

Consequently, determining the full census of the SW Sex stars is important, as the SW Sex syndrome appears to be increasingly widespread among the CV population, and possibly has important implications related to the secular evolution of CVs. A full understanding of the SW Sex syndrome will likely depend on a complete understanding of the number and range of CVs that are afflicted with it. To this end, I have compiled The Big List of SW Sextantis Stars. It is not necessarily intended to be the definitive SW Sex star census, but it is exhaustive in the sense that it contains all CVs that have been linked to the SW Sex stars in published sources.

The Big List of SW Sextantis Stars is complete to the best of my knowledge (as of the last modified date). During each update of the Big List, I locate new SW Sex stars by running a NASA-ADS search, with a publication window starting 1 month prior to the last Big List update, for text strings “SW Sex” and “cataclysmic” in paper abstracts, cross-correlated with a full-text ADS search for just “SW Sex” anywhere in the body of the paper. If you know of a new SW Sex star that I've missed, please email its name or other identifying information to me, and I'll add it to the list. Some of the information shown here is unavoidably subjective (mainly the assessment of the “SW Sexiness” of a CV – Definite, Probable, or Possible). If you disagree with any of my assessments, you can also email me and I will consider changing the appropriate entry, based on your persuasiveness!

Citation Text

If the material presented here has aided in the completion of your research project, then I would appreciate the inclusion of the following citations in any corresponding publications:

A citation to my paper in which the Big List is first described:

Hoard, D.~W., Szkody, P., Froning, C.~S., Long, K.~S., \& Knigge, C.\ 2003, \aj, 126, 2473
A footnote giving this URL, located near the usage of Big List data in the publication text; for example,

\footnote{See D.~W.\ Hoard's Big List of SW Sextantis Stars at \url{http://www.dwhoard.com/biglist} (Hoard et al.\ 2003).}

The following papers cite the Big List of SW Sex Stars (thank you!):

2011MNRAS.410..963N – “Dark Spot, Spiral Waves, and the SW Sextantis Behaviour: It is all about UX Ursae Majoris” by Neustroev et al.
2010AJ....140.1313H – “Simultaneous X-ray and Ultraviolet Observations of the SW Sextantis Star DW Ursae Majoris” by Hoard et al.
2009ApJ...697.1717B – “On the Accretion Rates of SW Sextantis Nova-like Variables” by Ballouz & Sion
2009A&A...496..765K – “Nova-like cataclysmic variable TT Arietis. QPO behaviour coming back from positive superhumps” by Kim et al.
2007MNRAS.377.1747R – “SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 hours” by Rodríguez-Gil et al.
2004ApJ...615L.129K – “Time-resolved ultraviolet spectroscopy of the SW Sex star DW UMa: Confirmation of a hidden white dwarf and the ultraviolet counterpart to phase 0.5 absorption events” by Knigge et al.
2003PASP..115.1118W – “Investigating the Sloan Digital Sky Survey cataclysmic variable SDSS J132723.39+652854.2” by Wolfe et al.

Orbital Period Distribution of SW Sex Stars

Counting Statistics for the Big List

Category	Total	Definite	Probable	Possible
Number of CVs	67	30	12	25
Old Novae	9	2	2	5
High Inclination (deep eclipses)	33	16	6	11
Moderate Inclination (shallow eclipses)	6	4	0	2
Low Inclination (no eclipses)	28	10	6	12
P_orb < 2 hr	2	0	0	2
P_orb = 2–3 hr	9	5	2	2
P_orb = 2.5–4 hr	52	25	9	18
P_orb = 3–4 hr	44	21	7	16
P_orb > 4 hr	12	4	3	5

Summary Table of Target Characteristics

(hover on column headings for explanatory information)

`Target and SW Sex Status`	`P_orb (hr)`	`Eclipse and i (°)`	`Magnetic`	`Super- humps`	`QPOs (s)`	`References and Notes`
`Ha122105.52-665048.8` `Possible`	`>3.6?^a`	`None?^a` `...`	`...`	`...`	`≈920^a†`	`Oct 2011`
`BT Mon` `Definite`	`8.0115^b`	`Deep^ab` `82.2(3.2)^b`	`P?/IP?^ab†`	`...`	`∼1800^b`	`Oct 2011`
`V363 Aur` `Definite`	`7.7098^b`	`Deep^†` `70(2)^a 69.7(4)^b`	`...`	`...`	`...`	`Oct 2011`
`AC Cnc` `Definite`	`7.2115^c`	`Deep^a` `75.6(7)^b`	`...`	`...`	`...`	`Oct 2011`
`BF Eri` `Possible`	`6.5011^a`	`None` `38–70^a†`	`...`	`...`	`...`	`Oct 2011`
`1RXS J064434.5+334451` `Possible`	`6.4650^a`	`Deep^a` `>76^a`	`No^a†`	`No^a`	`...`	`Oct 2011`
`V347 Pup` `Probable`	`5.5665^f`	`Deep^a` `87(3)^a 84(2.3)^f 77–84^e`	`...`	`...`	`...`	`Oct 2011`
`RW Tri` `Probable`	`5.5652^†`	`Deep^c‡` `67–75^a 75^*`	`...`	`...`	`...`	`Oct 2011`
`CZ Aql` `Possible`	`4.812^a`	`None?^†` `...`	`Yes?^a‡`	`...`	`...`	`Oct 2011`
`UX UMa` `Probable^†`	`4.7201^b`	`Deep^b` `71.0(6)^b` `65–75^e`	`Not an IP^c`	`...`	`≈29^c‡`	`Oct 2011`
`2MASS J01074282+4845188` `Possible`	`4.6464^a`	`Deep^a` `...`	`...`	`...`	`...`	`Oct 2011`
`Ha094409.36-561711.4` `Possible`	`4.5104^a`	`Deep^ab` `84–90^b`	`...`	`...`	`...`	`Oct 2011`
`LS Peg` `Definite`	`4.1946^a`	`None^†` `≪72^ab`	`IP?^c`	`...`	`∼1140^d 1242(18)^a 1776(108)^c‡ 2010(132)^c`	`Oct 2011`
`V1193 Ori` `Possible`	`3.9600^c`	`None^†` `...`	`...`	`negative^a`	`649–1720^b ≈1200^c`	`Oct 2011`
`V1776 Cyg` `Definite`	`3.9537^b`	`Deep^b` `75(3)^b`	`...`	`...`	`...`	`Oct 2011`
`Lanning 386` `Possible`	`3.9372^a`	`Deep^a` `...`	`No?^a`	`...`	`...`	`Oct 2011`
`UU Aqr` `Definite`	`3.9313^g`	`Deep^bdg†` `71–83^a 78(2)^b`	`...`	`positive^‡`	`...`	`Oct 2011`
`LX Ser` `Probable`	`3.8024^c`	`Deep^a` `74–76^b`	`...`	`...`	`∼140^†`	`Oct 2011`
`BH Lyn` `Definite`	`3.7410^c`	`Deep^†` `81^a 79(+5/-3)^b`	`...`	`positive^‡ negative^c`	`1030?^* 2700?^c`	`Oct 2011`
`OY Ara` `Probable`	`3.7312^a`	`Deep^a` `74.3(1.2)^a`	`...`	`...`	`...`	`Oct 2011`
`V380 Oph` `Definite`	`3.6986^c`	`None?^bc` `...`	`IP?^c`	`negative?^bc`	`2802(6)^c†`	`Oct 2011`
`WY Sge` `Possible`	`3.6872^b`	`Deep^†` `≈90^a >70–75^b`	`...`	`...`	`...`	`Oct 2011`
`BP Lyn` `Definite`	`3.6675^b`	`Shallow^abc†` `50–70^c`	`...`	`...`	`25.5^‡`	`Oct 2011`
`AO Psc` `Probable`	`3.5910^†`	`None^‡` `<30^b`	`IP^a`	`...`	`≈805^a*`	`Oct 2011`
`V1294 Tau` `Definite`	`3.588^b`	`None^a` `...`	`IP?^a`	`negative?^a`	`...`	`Oct 2011`
`HS 0220+0603` `Definite`	`3.5810^b`	`Deep^ab` `...`	`...`	`...`	`...`	`Oct 2011`
`HS 0455+8315` `Definite`	`3.5694^c`	`Deep^abc` `...`	`...`	`...`	`...`	`Oct 2011`
`HS 1813+6122` `Definite`	`3.55^b`	`None^ab` `...`	`...`	`negative^b`	`∼600–1200^b`	`Oct 2011`
`HS 0506+7725` `Possible`	`3.545^a`	`None^a` `...`	`...`	`...`	`∼600–1200^a`	`Oct 2011`
`PX And` `Definite`	`3.5125^d`	`Deep^†` `73.6^a`	`Not likely^c`	`positive^‡ negative^de`	`...`	`Oct 2011`
`V533 Her` `Definite`	`3.53^b`	`None^b` `≈62^c`	`IP?^c`	`...`	`63.63^† 1399.8(94.8)?^c‡`	`Oct 2011`
`IM Eri` `Possible`	`3.4949`	`None^a` `14–30^b`	`...`	`...`	`...`	`Oct 2011`
`SDSS J160745.02+362320.7` `Possible`	`3.4920^b`	`Deep^ab` `...`	`...`	`...`	`...`	`Oct 2011`
`Ha075648.83-124653.5` `Possible`	`3.49?^b`	`None?^a` `...`	`...`	`...`	`...`	`Oct 2011`
`CP Lac` `Possible`	`3.4834^†`	`Shallow?^a‡` `...`	`...`	`...`	`...`	`Oct 2011`
`RR Pic` `Possible`	`3.4806^†`	`Shallow?^‡` `60–80^f ∼70^d 65^c*`	`No?^††`	`positive^g`	`20–40^b‡‡ 780^g`	`Oct 2011`
`VZ Scl` `Possible`	`3.4709^a`	`Deep^a` `≥76^c`	`...`	`...`	`...`	`Oct 2011`
`LN UMa` `Definite`	`3.466^a`	`None?^a` `...`	`...`	`...`	`...`	`Oct 2011`
`V751 Cyg` `Possible`	`3.4671^d`	`None^acd` `30±20^c`	`No?^c`	`negative^d`	`None^d`	`Oct 2011`
`SDSS J075443.01+500729.2` `Possible`	`3.4327^b`	`Deep^b` `...`	`No^a†`	`...`	`...`	`Oct 2011`
`LS Cam` `Probable`	`3.420^b`	`None?^ab†` `...`	`IP?^a`	`...`	`≈3000?^a`	`Oct 2011`
`AH Pic` `Probable`	`3.3828^b`	`None^a` `25–37^b`	`...`	`...`	`∼600–1200^a`	`Oct 2011`
`RR Cha` `Possible`	`3.362^a`	`Deep^a` `...`	`IP^ab`	`positive^a negative^a`	`≈1950^a†`	`Oct 2011`
`BO Cet` `Definite`	`3.3552^a`	`None?^a†` `35–52^a`	`IP?^a`	`...`	`1194(54)^a‡`	`Oct 2011`
`V1315 Aql` `Definite`	`3.3526^e`	`Deep^a` `83^e 78^a`	`...`	`...`	`...`	`Oct 2011`
`TT Tri` `Definite`	`3.3513^bc`	`Deep^bc` `≈70-76^b†`	`No?^‡`	`...`	`...`	`Oct 2011`
`WX Ari` `Definite`	`3.3444^c`	`Shallow^c` `≈72^c`	`...`	`...`	`1180^†`	`Oct 2011`
`TT Ari` `Probable`	`3.3012^e`	`None^e†` `∼30^c 29(6)^e`	`IP?^b`	`positive^e‡ negative^bg`	`200–300^b* 918^b 1000–1700^†† 1200^d 1266^g 1740(180)^e`	`Oct 2011`
`SDSS J132723.39+652854.2` `Definite`	`3.2792^ab`	`Deep^a` `80^a`	`No^a†`	`...`	`...`	`Oct 2011`
`DW UMa` `Definite`	`3.2786^g`	`Deep^a` `82(4)^g 82^d 80(2)^e ≈80^a >71–72^cg`	`IP?^e`	`positive^fi negative^f`	`Noneⁱ 1620^e ≈1800^† 2974/2375^f`	`Oct 2011`
`HL Aqr` `Probable`	`3.2537^d`	`None^bd` `19–27^d`	`...`	`...`	`19.6^b†`	`Oct 2011`
`SW Sex` `Definite`	`3.2385^cd`	`Deep^a` `79(1)^a >75^c`	`...`	`...`	`...`	`Oct 2011`
`SDSS J080908.39+381406.2` `Definite`	`3.2169^d†`	`Shallow?^bc‡` `65(5)^c`	`...`	`...`	`...`	`Oct 2011`
`HS 0728+6738` `Definite`	`3.2067^a`	`Deep^a` `85(4)^a`	`...`	`...`	`420–600^a`	`Oct 2011`
`Ha073418.56-170626.5` `Possible`	`3.1854^a`	`Deep^a` `...`	`...`	`...`	`...`	`Oct 2011`
`KQ Mon` `Possible`	`3.07?^a`	`None^†` `...`	`...`	`...`	`...`	`Oct 2011`
`V442 Oph` `Definite`	`2.9839^bc`	`None^a` `<65^a`	`...`	`positive?^c negative^c`	`None^a ∼800–1200^c ∼1000^c`	`Oct 2011`
`DM Gem` `Possible`	`2.947?^a`	`None^a` `...`	`IP?^a`	`positive?^a`	`∼1320^a`	`Oct 2011`
`KIC J192410.81+445934.9` `Possible`	`2.94?^a`	`None/Shallow?^a` `...`	`...`	`...`	`≈650^a ≈1200^a`	`Oct 2011`
`AH Men` `Definite`	`2.95^b`	`Shallow?^a†` `∼70^a >56^d`	`IP?^d‡`	`positive^ab negative^b`	`∼600–2400^a 1040.4^b* 1293.4/1707.6^b`	`Oct 2011`
`V1084 Her` `Definite`	`2.8934^a`	`None^ab` `...`	`Yes^c†`	`negative^ab`	`1000^a ≈600–1200^c‡`	`Oct 2011`
`V592 Cas` `Probable`	`2.7615^a`	`None^b` `28(+11/-10)^b`	`No?^e`	`positive^a negative^a`	`≈1300^c†`	`Oct 2011`
`V795 Her` `Definite`	`2.5979^a`	`None^a` `≈56^b`	`IP^abcd†`	`positive^e‡`	`1150^e 4847 or 6386^a*`	`Oct 2011`
`V Per` `Probable`	`2.5710^d`	`Deep^a` `79.4/85.4^d† 74–88/≈90^b‡`	`IP?^bc`	`...`	`...`	`Oct 2011`
`V348 Pup` `Definite`	`2.4441^be`	`Deep^a` `81.1(1)^b ∼80^c`	`IP^ac†`	`positive^bc`	`∼900?^c`	`Oct 2011`
`SDSS J210131.26+105251.5` `Possible`	`1.8?^b`	`None?^ab` `...`	`Yes?^a No^b`	`...`	`...`	`Oct 2011`
`EX Hya` `Possible`	`1.6376^†`	`Deep^i‡` `78(1)^a 76.0–77.6^e`	`IP^dj`	`...`	`2007(4)^b 4021.8^al*`	`Oct 2011`


Ha122105.52-665048.8	2008MNRAS.385.1471P ^a
`Notes:`	`^†This QPO was detected on one night but absent on the following night (2008MNRAS.385.1471P).`

BT Mon (Monocerotis) Nova Mon 1939	1996ApJ...456..777W ^a 1998MNRAS.296..465S ^b
`Notes:`	`^†Magnetic nature of the WD is considered unlikely, but not impossible (1998MNRAS.296..465S).`

V363 Aur (Aurigae) Lanning 10	1986ApJ...307..760S ^a 2004MNRAS.353.1135T ^b
`Notes:`	`^†See 1982ApJ...252..681H.`

AC Cnc (Cancri) SVS 1280	1983PASJ...35..423Y ^a 2004MNRAS.353.1135T ^b	2007A&A...466..589Q ^c
`Notes:`	`•Possible tertiary companion based on long-term cyclic orbital period change: cool, low mass M dwarf in 16.2 yr orbit (2007A&A...466..589Q). •Transient absorption in emission lines is weak (2004MNRAS.353.1135T).`

BF Eri (Eridani) 1WGA J0439.4-0433	2008MNRAS.386.1366N ^a
`Notes:`	•Balmer line Doppler tomograms show characteristic emission in lower left quadrant; emission lines are single-peaked (2008MNRAS.386.1366N). •Massive WD (M_WD > 1.23 M_sun) with an evolved K3±0.5 secondary star (2008MNRAS.386.1366N). •“...we question the current classification...as a dwarf nova...BF Eri might be an old nova exhibiting ‘stunted’ outbursts“ – 2008MNRAS.386.1366N. •BF Eri has a large space velocity and is possibly a halo object (2007PASP..119..494S). ^†Upper limit inclination based on absence of eclipses; lower limit based on the WD mass not exceeding the Chandrasekhar mass (2008MNRAS.386.1366N).

1RXS J064434.5+334451 NSVS 7178256	2007A&A...474..951S ^a
`Notes:`	`^†Circular polarization of 0.003±0.003% (2007A&A...474..951S).`

V347 Pup (Puppis) Pup2 LB 1800	1990ApJ...355..617B ^a 1994ApJ...424..347M ^b 1996ApJ...461..377S ^c	1998MNRAS.299..545S ^d 1999ApJ...523..786D ^e 2005MNRAS.357..881T ^f
`Notes:`	`•Possible weak transient absorption around φ≈0.4 in Hβ, Hγ, He I λ4471, and (to an even lesser degree) He II λ4686 emission lines (2005MNRAS.357..881T, 1990ApJ...355..617B).`

RW Tri (Trianguli)	1983ApJ...267..239K ^a 1995MNRAS.273..849S ^b	2004A&A...417..283G ^c
`Notes:`	`•SW Sex characteristics during bright states (2004A&A...417..283G). •Eclipse mapping during low state shows inner accretion disk radial temperature profile is flatter than standard steady state model, while outer disk follows standard model (2008IBVS.5861....1H). ^†See 2006IBVS.5710....1P and 1991AJ....102.1176R. ^‡Also see 2006IBVS.5710....1P, 1995AcA....45..259S, and 1963ApJ...137..485W. ^*See 1992A&A...260..213R.`

CZ Aql (Aquilae)	2007PASP..119..494S ^a
`Notes:`	`•No transient absorption detected in the (optical) He I emission lines (2007PASP..119..494S). ^†Lack of eclipses is assumed from the fact that detection of eclipses has not yet been noted in the literature, but there appears to have been little time-series photometry obtained for this CV. ^‡“...emission lines have strong wings that move with large velocity amplitude, suggesting a magnetically channeled accretion flow.” – 2007PASP..119..494S.`

UX UMa (Ursae Majoris)	1983ApJS...53..397S ^a 1995ApJ...448..395B ^b 1998ApJ...499..429K ^c	2003ApJ...584..433F ^d 2011MNRAS.410..963N ^e
`Notes:`	•UV light curve “dip” centered around φ≈0.6 has been attributed to an asymmetric vertical extension in the outer accretion disk absorbing flux from the disk interior (1997MNRAS.290L..23M, 2003ApJ...584..433F) and is reminiscent of the SW Sex star phase-dependent absorption. ^†Displayed SW Sex characteristics during observations made in 1999, but these had almost completely disappeared in observations made in 2008 (2011MNRAS.410..963N). ^‡This QPO is classified as a dwarf nova oscillation. Also see 1972MNRAS.159..429W.

2MASS J01074282+4845188	2012NewA...17...34D ^a
`Notes:`	`•2012NewA...17...34D note that the CV was first identified as a short-period eclipsing binary in 2008AJ....135..850D, but was listed in the latter at the wrong coordinates, corresponding to a nearby, non-variable star (2MASS J01074441+4844581).`

Ha094409.36-561711.4	2008MNRAS.385.1471P ^a 2011IBVS.5971....1S ^b
`Notes:`	`...`

LS Peg (Pegasi) Peg2 S193 NSV 13903	1999PASP..111..184T ^a 1999MNRAS.305..661M ^b	2001ApJ...548L..49R ^c 2001AJ....121.2761S ^d
`Notes:`	`^†See, for example, 1992JAVSO..21...81G. ^‡This QPO is possibly the WD spin period, although 2008MNRAS.387.1157R note that a 35 ksec XMM-Newton X-ray observation shows no evidence for a WD spin period between a few hundred sec and ≈10 ksec.`

V1193 Ori (Orionis) Hamuy's Star	2005NewA...11..147A ^a 2006MNRAS.368..361P ^b	2006A&A...456..599P ^c 2009AAS...21343411S ^d
`Notes:`	`^†See summary description in support of this conclusion in 2006A&A...456..599P.`

V1776 Cyg (Cygni) Lanning 90	1983PASP...95..206S ^a 1990ApJ...365..696G ^b	1998PhDT........10H ^c
`Notes:`	`...`

Lanning 386	2008PASP..120..301B ^a
`Notes:`	`•This CV behaves like a dwarf nova with frequent outbursts of amplitude up to ∼2 mag, but shows some SW Sex star characteristics during the outburst peaks (2008PASP..120..301B).`

UU Aqr (Aquarii) S196	1991AJ....102.1417D ^a 1994ApJ...433..332B ^b 1996MNRAS.282...99B ^c 1998MNRAS.294..689H ^d	1998ApJ...499..444K ^e 2000MNRAS.314..713B ^f 2008ApJ...676.1240B ^g
`Notes:`	`•Eclipse mapping shows that the low- and high-brightness states of UU Aqr can be accounted for by changes in the mass transfer rate of 20%-50%. The otherwise roughly steady state accretion disk contains long-lasting asymmetric arcs produced by tidally induced spiral shocks. The spiral arms account for 25% of the steady-light flux and are the dominant source of flickering at both low and high frequencies (2008ApJ...676.1240B). ^†Also see 1989IBVS.3361....1G. ^‡See 2005PASP..117.1204P.`

LX Ser (Serpentis) Stepanyan's Star	1980ApJ...242L.167H ^a 1981ApJ...244..259Y ^b	1984PASP...96..372E ^c
`Notes:`	`^†This QPO is only marginally detected (1984PASP...96..372E) and is classified as a DNO (see 2004PASP..116..115W).`

BH Lyn (Lyncis) PG 0818+513	1992MNRAS.258..225D ^a 1997ApJ...481..433H ^b	2006A&A...455..223S ^c
`Notes:`	`^†For example, see 1989IBVS.3388....1A. ^‡See 2005PASP..117.1204P. ^*See 2002PASP..114.1364P.`

OY Ara (Arae) Nova Ara 1910 HD 149990	1997ApJ...483..899Z ^a
`Notes:`	`...`

V380 Oph (Ophiuchi)	1985AJ.....90..643S ^a 2005ASPC..330..495SR ^b	2007MNRAS.374.1359R ^c 2009PASP..121..942Z ^d
`Notes:`	`•“...another example of an SW Sex star with a reddish UV-optical spectral energy distribution that cannot be fit successfully with standard disk models.” – 2009PASP..121..942Z. ^†This QPO manifests as (optical) emission line flaring and could be related to the spin of a magnetic WD; however, its long-term coherence has not yet been established (2007MNRAS.374.1359R).`

WY Sge (Sagittae) Nova Sge 1783	1984ApJ...282..763S ^a 1996MNRAS.278..845S ^b	1997MNRAS.284..359S ^c
`Notes:`	`^†See 1983ApJ...264..560S.`

BP Lyn (Lyncis) Lyn1 PG 0859+414	1994AJ....108..214G ^a 1996MNRAS.282..943S ^b	1996ApJ...470.1052H ^c
`Notes:`	`^†Eclipse of the bright spot only (e.g., 1996MNRAS.282..943S). ^‡This QPO is classified as a DNO (see 2004PASP..116..115W).`

AO Psc (Piscium) H 2252-035	2005ApJ...626.1028H ^a 2007ApJ...656..444H ^b
`Notes:`	`•Maximum peak-to-peak circular polarization of 1.30±0.50% (2009A&A...496..891B). ^†See 2001PASP..113..736P. ^‡For example, see 1984AcA....34..397K and 1984A&A...131..137V. ^*This QPO is probably the WD spin period (2005ApJ...626.1028H).`

V1294 Tau (Tauri) KUV 03580+0614 Tau2 HS 0357+0614	2001PASP..113.1215S ^a 2001MNRAS.326.1235T ^b	2005ASPC..330..335R ^c
`Notes:`	`...`

HS 0220+0603	2005ASPC..330..335R ^a 2007MNRAS.377.1747R ^b
`Notes:`	`•Shows unusual N II and Si II emission lines suggesting that the donor star may have experienced nuclear evolution via the CNO cycle (2007MNRAS.377.1747R).`

HS 0455+8315	2002pcvr.conf..623G ^a 2005ASPC..330..335R ^b	2007MNRAS.377.1747R ^c
`Notes:`	`•He II λ4686 and C III/N III Bowen blend are especially strong (2007MNRAS.377.1747R).`

HS 1813+6122	2005ASPC..330..335R ^a 2007MNRAS.377.1747R ^b
`Notes:`	`...`

HS 0506+7725	2005A&A...443..995A ^a
`Notes:`	`...`

PX And (Andromedae) And1 PG 0027+260	1991AJ....102..272T ^a 1994ApJ...431L.107H ^b 1995MNRAS.273..863S ^c	2002A&A...394..625S ^d 2010A&A...514A..30T ^e
`Notes:`	`•Founding member. ^†See, for example, 1990IBVS.3434....1L. ^‡See 2005PASP..117.1204P. 2010A&A...514A..30T found a negative superhump, but no evidence of positive superhumps.`

V533 Her (Herculis) Nova Her 1963	1979ApJ...233L..13P ^a 2000MNRAS.312..629T ^b	2002MNRAS.337..209R ^c
`Notes:`	`^†This QPO is classified as a DNO (1979ApJ...233L..13P), but has not been consistently re-detected (2000MNRAS.312..629T). ^‡This QPO manifests as (optical) emission line flaring, and is possibly the (magnetic) WD spin period (2002MNRAS.337..209R).`

IM Eri (Eridani) EC 04224-2014	2001MNRAS.325...89C ^a 2009AAS...21343411S ^b
`Notes:`	`...`

SDSS J160745.02+362320.7	2006AJ....131..973S ^a 2010NewA...15..476Z ^b
`Notes:`	`...`

Ha075648.83-124653.5	2008MNRAS.385.1471P ^a 2010MNRAS.403..398P ^b
`Notes:`	`...`

CP Lac (Lacertae) Nova Lac 1936	2005A&A...431..289R ^a
`Notes:`	`^†See 2006PASP..118..687P. ^‡Presence of shallow eclipses is tentatively suggested, although based on only one such observed event (2005A&A...431..289R).`

RR Pic (Pictoris) Nova Pic 1925 Hen 3-15	1975A&A....41...15V ^a 1981MNRAS.195..101W ^b 1982A&A...109..171H ^c 1986MNRAS.219..751W ^d	2003MNRAS.342..145S ^e 2006PASP..118...84R ^f 2008MNRAS.389.1345S ^g
`Notes:`	^†See 1991IBVS.3665....1H. ^‡Shallow eclipses of the accretion disk/bright spot are noted (1975A&A....41...15V). The strong orbital modulation seen in the 1970s was replaced in the 1980s by an irregular, shallow eclipse superimposed on a flickering background (1986MNRAS.219..751W), but was subsequently not reliably detected (2008MNRAS.389.1345S). ^*This inclination assumes that only the bright spot in the disk is eclipsed (1982A&A...109..171H). ^††A possible IP classification is suggested in 1984AcA....34..331K based on a claimed 15 min photometric periodicity, but this was refuted by 1985A&A...150..325H and others (1986MNRAS.219..751W). ^‡‡This QPO is a possible dwarf nova oscillation, with most stable period near 32 sec (1981MNRAS.195..101W).

VZ Scl (Sculptoris)	1975MNRAS.172..433W ^a 1984MNRAS.206..859S ^b	1987MNRAS.225...43O ^c 1999AAS...195.3612M ^d
`Notes:`	`...`

LN UMa (Ursae Majoris) UMa7 PG 1000+667	1998AJ....115.2044H ^a 2007MNRAS.374.1359R ^b
`Notes:`	`...`

V751 Cyg (Cygni)	1974PASP...86..401R ^a 1998A&A...336..626G ^b 1999A&A...343..183G ^c	2001PASP..113...72P ^d 2009PASP..121..942Z ^e
`Notes:`	`•2001PASP..113...72P note departures from “normal” SW Sex star spectroscopic observational characteristics, but these could be due to viewing at low inclination. •“...V751 Cygni look[s] too red for a standard accretion disk SED in terms of UV-optical color.” – 2009PASP..121..942Z.`

SDSS J075443.01+500729.2	2006AJ....131..973S ^a 2007MNRAS.382.1145S ^b
`Notes:`	`^†Circular polarization <0.1% (3-sigma upper limit; 2007MNRAS.382.1145S).`

LS Cam (Camelopardalis) HS 0551+7241	1998AJ....115.1634D ^a 2005ASPC..330..335R ^b
`Notes:`	`^†A possible shallow eclipse was reported by 1998AJ....115.1634D but not subsequently re-observed by 2005ASPC..330..335R.`

AH Pic (Pictoris) EC 05565-5935	2001MNRAS.325...89C ^a 2007MNRAS.374.1359R ^b
`Notes:`	`...`

RR Cha (Charmaeleontis) Nova Cha 1953 S5346	2002MNRAS.335...44W ^a 2003MNRAS.342L...1R ^b
`Notes:`	`^†This QPO is believed to be related to the (magnetic) WD spin period, either directly or via reprocessing (2002MNRAS.335...44W).`

BO Cet (Ceti) Cet4 1H 0204-023	2007MNRAS.374.1359R ^a
`Notes:`	`^†Lack of eclipses assumed based on inclination estimates derived from spectroscopic observations (2007MNRAS.374.1359R). ^‡This QPO manifests as (optical) emission line flaring, and is possibly related to the (magnetic) WD spin period (2007MNRAS.374.1359R).`

V1315 Aql (Aquilae) KPD 1911+1212	1986ApJ...301..240D ^a 1991AJ....102..272T ^b 1993MNRAS.264..619S ^c	1995MNRAS.277..777D ^d 1996ApJ...471..949H ^e
`Notes:`	`•Founding member.`

TT Tri (Trianguli) HS 0129+2933 GR 286	2005ASPC..330..335R ^a 2006PASP..118.1373W ^b	2007MNRAS.377.1747R ^c
`Notes:`	`^†The inclination estimates of 76.1, 72.6, and 70.4 degrees are dependent on assumed mass ratio, and correspond to q=0.3, 0.6, and 0.9, respectively (2006PASP..118.1373W). ^‡“...there is no compelling evidence for a truncated inner disk in TT Tri based on our eclipse studies.” – 2006PASP..118.1373W.`

WX Ari (Arietis) PG 0244+104	1992A&A...256..442B ^a 1994A&A...289..148H ^b	2000A&A...355..181R ^c
`Notes:`	`^†See 2002PASP..114.1364P.`

TT Ari (Arietis) BD +14 341 RX J0206.8+1517	1985ApJ...290..707S ^a 1992A&A...265...77H ^b 1999A&A...347..178G ^c 2002PASP..114.1364P ^d	2002ApJ...569..418W ^e 2007AJ....133.1204H ^f 2009A&A...496..765K ^g
`Notes:`	^†Also see 1996A&A...312..121T and 1979IBVS.1710....1S. ^‡Positive superhump present during bright states in 1997-2005, replacing the negative superhump seen in faint states during 1988-1997 (2007AJ....133.1204H). Since 2005, negative superhumps have returned (2009A&A...496..765K). ^*This QPO is possibly the WD spin period (1992A&A...265...77H). ^††Displayed a trend of decreasing QPO timescale from 1962 (∼1700 sec) to 1985 (∼1000 sec), which continued to more recent observations (e.g., ∼900 sec in 1988) – see 1992A&A...265...77H.

SDSS J132723.39+652854.2 SDSS 0496-083	2003PASP..115.1118W ^a 2010NewA...15..476Z ^b
`Notes:`	`^†Circular polarization of <0.24% (2003PASP..115.1118W).`

DW UMa (Ursae Majoris) PG 1030+590	1988ApJ...327..248S ^a 1991AJ....102..272T ^b 1994MNRAS.266..859D ^c 2000ApJ...539L..49K ^d 2000A&A...364..573B ^e 2002PASP..114.1364P ^f	2003ApJ...583..437A ^g 2003AJ....126.2473H ^h 2004A&A...416.1057S ⁱ 2004ApJ...615L.129K ^j 2010AJ....140.1313H ^k
`Notes:`	`•Founding member. •Very soft X-ray spectrum and likely partial X-ray eclipse, implying X-ray reprocessing in a vertically extended region (2010AJ....140.1313H). ^†This QPO manifests as (optical) emission line flaring; it is reported only as a private communication in 2007MNRAS.377.1747R.`

HL Aqr (Aquarii) PHL 227	1985A&A...149L...4H ^a 1987MNRAS.224..231H ^b	1995AJ....110.1824D ^c 2007MNRAS.374.1359R ^d
`Notes:`	`•“HL Aqr is definitely not a ‘typical’ SW Sex star.” – 2007MNRAS.374.1359R. ^†This QPO is classified as a DNO (1987MNRAS.224..231H).`

SW Sex (Sextantis) PG 1012-029	1984ApJ...276..233P ^a 1991AJ....102..272T ^b	1997MNRAS.291..694D ^c 2001A&A...368..183G ^d
`Notes:`	`•Founding member.`

SDSS J080908.39+381406.2 HS 0805+3822	2002AAS...201.1608F ^a 2003AJ....126.1499S ^b	2007ApJ...654.1036L ^c 2007MNRAS.377.1747R ^d
`Notes:`	`^†Also see 2009MNRAS.397.2170G. ^‡Possible grazing eclipses, similar to WX Ari (2007MNRAS.377.1747R).`

HS 0728+6738	2004A&A...424..647R ^a 2005ASPC..330..335R ^b
`Notes:`	`...`

Ha073418.56-170626.5	2008MNRAS.385.1471P ^a
`Notes:`	`...`

KQ Mon (Monocerotis) EC 04224-2014	2005IBVS.5627....1S ^a 2009AAS...21343411S ^b
`Notes:`	`•This CV is a close visual triple, resolved in 2MASS images (2002ApJ...565..511H). ^†See 1982NASCP2338..460S.`

V442 Oph (Ophiuchi) SVS 337	1983PASP...95..509S ^a 2000ApJ...537..936H ^b	2002PASP..114.1364P ^c
`Notes:`	`...`

DM Gem (Geminorum) Nova Gem 1903 HD 48328	2005A&A...431..289R ^a
`Notes:`	`...`

KIC J192410.81+445934.9 Kepler 8751494	2010AJ....139.2587W ^a 2010MNRAS.409.1470O ^b
`Notes:`	`•Located in the Kepler Mission field.`

AH Men (Mensae) Men1 1H 0551-819	1993MNRAS.265..926B ^a 1995PASP..107..657P ^b	1999A&A...346..151G ^c 2007MNRAS.374.1359R ^d
`Notes:`	`^†Dips at maximum light are possibly shallow eclipses, but this has not been confirmed (1993MNRAS.265..926B). ^‡Also see 1991MNRAS.248..370W and 1991MNRAS.252..386W. ^*WD spin period is possibly twice this QPO period (1995PASP..107..657P).`

V1084 Her (Herculis) RX J1643.7+3402	2002PASP..114.1364P ^a 2002A&A...381..894M ^b	2009MNRAS.395..973R ^c
`Notes:`	`^†Variable circular polarization is present with amplitude ranging from 0%-0.5% on a period of 19.38±0.39 min (2009MNRAS.395..973R). ^‡This QPO manifests as (optical) emission line flaring (2009MNRAS.395..973R).`

V592 Cas (Cassiopeiae) KPD 0018+5525 LS I +55 8	1998PASP..110.1148T ^a 1998PASP..110..784H ^b 2002IBVS.5358....1K ^c 2003MNRAS.346..861W ^d	2004MNRAS.355..137P ^e 2009AJ....137..197K ^f 2009ApJ...693..236H
`Notes:`	•Evidence for disk wind absorption in emission lines (e.g., P Cygni profiles) varies over the orbital period and is possibly phase-dependent, indicating an asymmetric outflow (2009AJ....137..197K, 2004MNRAS.355..137P, 2003MNRAS.346..861W). •Spitzer Space Telescope observations show evidence for excess IR (dust) emission at wavelengths longer than 8 microns (2009ApJ...693..236H). •Both 2004MNRAS.355..137P and 1998PASP..110.1148T discuss V592 Cas's departures from the observational characteristics of the SW Sex stars. ^†No superhumps were detected during the observations in which this QPO was detected (2002IBVS.5358....1K).

V795 Her (Herculis) PG 1711+336	1990ApJ...354..708S ^a 1996MNRAS.278..219C ^b 1997MNRAS.286..447D ^c	2002ASPC..261..533R ^d 2002PASP..114.1364P ^e 2010A&A...514A..30T ^e
`Notes:`	`^†Variable circular polarization with a periodicity of 1170 sec (or twice that; 2002ASPC..261..533R). ^‡Also see 2005PASP..117.1204P and 2006A&A...456..599P. ^*This QPO is reported as possibly the WD spin period, but the polarization variability results suggest a shorter WD spin period (1990ApJ...354..708S).`

V Per (Persei) Nova Per 1887 HD 12244 BD +56 406a	1989ApJ...339L..75S ^a 1992ApJ...393..729W ^b 2001A&A...368..183G ^c	2006ApJ...644.1104S ^d 2007IBVS.5751....1H ^e
`Notes:`	`^†Both of these inclination estimates are from eclipse profile model fitting; the lower estimate assumes a mass ratio of q=0.4, while the higher assumes a mass ratio of q=0.20 (2006ApJ...644.1104S). ^‡The lower of these inclination estimates is from eclipse mapping, while the higher assumes a model involving a flared outer accretion disk rim (1992ApJ...393..729W).`

V348 Pup (Puppis) Pup1 1H 0709-360	1990ApJ...359..204T ^a 2000MNRAS.317..759R ^b 2001MNRAS.328..903R ^c	2003AJ....126..964F ^d 2010MNRAS.409.1195D ^e
`Notes:`	`•Orbital period increasing at a rate of 5.8(±1.9)×10^-12 s s^-1, possibly as part of a longer period modulation (2010MNRAS.409.1195D). ^†However, 1994MNRAS.269..913R note that a follow-up ROSAT observation showed an X-ray flux more than 70 times fainter than the HEAO-1 X-ray flux taken by 1990ApJ...359..204T as evidence of the IP nature of this CV.`

SDSS J210131.26+105251.5	2003AJ....126.1499S ^a 2006AJ....132.2743H ^b
`Notes:`	`...`

EX Hya (Hydrae) EUVE J1252-29.2 1E 1249-2858	1987MNRAS.228..463H ^a 1987ApJ...317..765K ^b 2000MNRAS.313..703H ^c 2002A&A...382..984E ^d 2003A&A...412..821B ^e 2003ApJ...587..373B ^f 2004AJ....128..448B ^g	2005ApJ...628..946H ^h 2005AJ....129.1985B ⁱ 2007ApJ...656..444H ^j 2008A&A...480..199B ^k 2009IBVS.5876....1M ^l 2011MNRAS.411.1317R ^m
`Notes:`	`•SW Sex characteristics during outbursts (2000MNRAS.313..703H). •No evidence for circumbinary material (e.g., dust; 2004AJ....128..448B). •X-ray observations show evidence for reflection from the disk, most likely from a large bulge at the accretion impact zone (2011MNRAS.411.1177P). ^†See 1983A&A...118..325S. ^‡Also see, for example, 1967ApJS...15....1M. ^*This QPO is the WD spin period (1987MNRAS.228..463H, 2009IBVS.5876....1M).`

General and/or Important Papers about the SW Sex Stars

SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 hours by P. Rodriguez-Gil et al. 2007MNRAS.377.1747R
Spectroscopic search for new SW Sextantis stars in the 3-4 h orbital period range - I by P. Rodriguez-Gil 2007MNRAS.374.1359R
HS 0139+0559, HS 0229+8016, HS 0506+7725, and HS 0642+5049: four new long-period cataclysmic variables by A. Aungwerojwit et al. 2005A&A...443..995A
The role of the SW Sextantis stars in the picture of CV evolution by P. Rodriguez-Gil 2005ASPC..330..335R
Some updates on the role of magnetic fields in cataclysmic variables by C. Hellier 2004RMxAC..20..148H
Time-resolved ultraviolet spectroscopy of the SW Sex star DW UMa: confirmation of a hidden white dwarf and the ultraviolet counterpart to phase 0.5 absorption events by C. Knigge et al. 2004ApJ...615L.129K
FS Aurigae: a new class of cataclysmic variables or the missing link between intermediate polars and SW Sextantis objects? by G. Tovmassian et al. 2003PASP..115..725T
Observations of the SW Sextantis star DW Ursae Majoris with the Far Ultraviolet Spectroscopic Explorer by D. W. Hoard et al. 2003AJ....126.2473H
VY Sculptoris stars as magnetic cataclysmic variables by J.-M. Hameury & J.-P. Lasota 2002A&A...394..231H
Superhumps in cataclysmic binaries. XXIII. V442 Ophiuchi and RX J1643.7+3402 by J. Patterson et al. 2002PASP..114.1364P
V533 Herculis: the second SW Sex old nova displaying emission-line flaring by P. Rodríguez-Gil & I. G. Martínez-Pais 2002MNRAS.337..209R
Evidence of magnetic accretion in an SW Sextantis star: discovery of variable circular polarization in LS Pegasi by P. Rodríguez-Gil et al. 2001ApJ...548L..49R
The SW Sextantis stars by C. Hellier 2000NewAR..44..131H
Orbital period of the low-inclination SW Sextantis star V442 Ophiuchi by D. W. Hoard et al. 2000ApJ...537..936H
A self-occulting accretion disk in the SW Sextantis star DW Ursae Majoris by C. Knigge et al. 2000ApJ...539L..49K
Disk-anchored magnetic propellers - a cure for the SW Sex syndrome by K. Horne 1999mcv..work..349H
The phase 0.5 absorption in SW Sextantis-type cataclysmic variables by C. Hellier 1998PASP..110..420H
Accretion and structure in the SW Sextantis stars by D. W. Hoard 1998PhDT........10H
V1315 Aquilae and the nature of SW Sextantis stars by C. Hellier 1996ApJ...471..949H
PX Andromedae and the SW Sextantis phenomenon by C. Hellier & E. L. Robinson 1994ApJ...431L.107H
PG0027+260 - an example of a class of cataclysmic binaries with mysterious, but consistent, behavior by J. R. Thorstensen et al. 1991AJ....102..272T
The phase 0.5 absorption in V1315 Aquilae, SW Sextantis, and DW Ursae Majoris by P. Szkody & F. Piché 1990ApJ...361..235S

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