The Big List of SW Sextantis Stars (v5.0.0 - Jan 2014)

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!):

  • 2014arXiv1401.0635 – “On the SW Sex-Type Eclipsing Cataclysmic Variable SDSS0756+0858” by Tovmassian et al.
  • 2013AJ....145..168W – “Far-Ultraviolet Spectroscopy of the Nova-Like Variable KQ Monocerotis: A New SW Sextantis Star?” by Wolfe et al.
  • 2013MNRAS.428.3559D – “The SW Sex Enigma” by Dhillon et al.
  • 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 69 29 17 23
Old Novae 9 2 2 5
High Inclination
(deep eclipses)
31 16 9 6
Moderate Inclination
(shallow eclipses)
8 2 2 4
Low Inclination
(no eclipses)
30 10 7 13
Porb < 2 hr 2 0 0 2
Porb = 2–3 hr 9 5 2 2
Porb = 2.5–4 hr 53 23 12 18
Porb = 3–4 hr 45 19 10 16
Porb > 4 hr 13 4 6 3
D. W. Hoard's Big List of SW Sex Stars
Target Characteristics Summary Table
v5.0.0 - Jan 2014

+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Target                  |SW Sex  |Porb (h)  |Eclipse     |Single|Strong  |Line  |Strong|Phase |Transient     |Dop   |Hi Vel|Super   |~ksec |Emis   |VY Scl|Circ  |Update  |
|                        |Status  |          |            |Peaked|He II   |Eclip |S-wave|Lag   |Absorption    |Tom   |Comp  |humps   |QPO   |Flares |States|Pol   |        |
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Ha122105.52-665048.8    |Possible|>5.1?     |None?       |Y     |N       |...   |N?    |...   |Y?            |...   |...   |...     |Y [a] |Y?     |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BT Mon                  |Definite|8.0115    |Deep (V)    |Y     |S+      |Y     |Y     |Y     |0.35-0.65     |Y     |Y     |N? [c]  |Y [b] |Y [b]  |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V363 Aur                |Definite|7.7098    |Deep (V)    |Y     |S+      |N [a] |Y     |Y     |0.4-0.6       |Y?    |Y     |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|AC Cnc                  |Definite|7.2115 [c]|Deep (U)    |Y     |W       |N [a] |Y     |Y     |0.45-0.55 [b] |Y     |Y     |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BF Eri                  |Possible|6.5011    |None        |Y     |W       |...   |Y     |N     |0.5-0.6       |Y     |N?    |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|1 RXS J064434.5+334451  |Probable|6.4650    |Deep (V)    |Y     |S+      |...   |Y     |Y     |0.45-0.0      |Y? [b]|...   |N       |...   |...    |...   |N [a] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V347 Pup                |Probable|5.5665    |Deep (V)    |Y     |S       |N [bc]|Y     |Y     |0.4-0.5?      |Y?    |Y     |...     |...   |...    |N     |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|RW Tri                  |Probable|5.5652    |Deep (V)    |Y     |W       |Y  [a]|Y     |Y     |0.4-0.6? [a]  |N     |N     |...     |...   |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|CZ Aql                  |Possible|4.8       |None? [a]   |Y     |...     |...   |Y     |...   |N             |...   |Y [b] |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|UX UMa                  |Probable|4.7201    |Deep (V)    |Y [d] |W       |...   |Y [d] |Y [d] |0.4-0.7 [cd]  |N [d] |Y     |...     |N? [b]|...    |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|2MASS J01074282+4845188 |Probable|4.6464    |Deep (V)    |Y     |...     |...   |Y     |? [a] |? [a]         |...   |Y     |...     |...   |? [a]  |N     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Ha094409.36-561711.4    |Probable|4.5104    |Deep (V)    |Y     |S       |...   |...   |Y     |Y?            |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|LS Peg                  |Definite|4.1946    |None        |Y     |W       |...   |...   |...   |0.3-0.9?      |N?    |Y     |...     |Y [a] |Y      |...   |Y [b] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V1193 Ori               |Definite|3.9600    |None        |Y     |N       |...   |Y     |Y     |0.3-0.5       |...   |...   |-       |Y [a] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V1776 Cyg               |Definite|3.9537    |Deep (V)    |Y     |S/S+    |...   |Y     |Y     |0.5-0.6       |Y     |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Lanning 386             |Possible|3.9372    |Deep (V)    |Y [a] |S+ [a]  |...   |Y [a] |Y [a] |0.6-0.9 [a]   |...   |...   |...     |...   |...    |N     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|UU Aqr                  |Definite|3.9313    |Deep (V) [b]|Y     |W       |N [a] |Y     |Y     |0.4-0.95      |N?    |...   |+/N?    |...   |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|LX Ser                  |Probable|3.8024    |Deep (V)    |Y     |S       |N [a] |Y     |Y     |...           |...   |...   |...     |N? [b]|...    |Y     |N? [c]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BH Lyn                  |Definite|3.7410    |Deep (V)    |Y     |W/S     |Y? [a]|Y     |Y     |0.4-0.65      |Y     |Y     |+/-     |Y [b] |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|OY Ara                  |Probable|3.7312    |Deep (V)    |Y     |S       |...   |Y     |Y     |Y?            |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V380 Oph                |Definite|3.6986    |None?       |Y     |W       |...   |Y     |Y     |0.45-0.6      |Y     |...   |-?      |Y [a] |Y [a]  |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BB Dor                  |Probable|3.6983    |None?       |Y     |N/W     |...   |Y [c] |Y [c] |0.5?          |N [b] |Y [b] |+?/-    |Y [a] |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|WY Sge                  |Possible|3.6872    |Deep (V)    |Y     |S       |...   |Y     |...   |0.7-0.9?      |...   |...   |...     |...   |...    |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BP Lyn                  |Probable|3.6675    |Shallow [a] |Y? [c]|W       |N [b] |Y     |N? [d]|0.5-0.1? [c]  |Y? [d]|...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|AO Psc                  |Possible|3.5910    |None        |Y     |S+      |...   |...   |...   |0.65-0.25 [b] |...   |...   |...     |Y [a] |...    |...   |N? [c]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V1294 Tau               |Definite|3.588     |None        |Y     |S+      |...   |Y     |Y? [a]|0.3-0.55? [a] |Y? [a]|...   |-?      |Y [b] |...    |Y? [c]|...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|HS 0220+0603            |Definite|3.5810    |Deep (V) [b]|Y [a] |W       |...   |Y     |Y     |0.35-0.6      |...   |Y     |...     |...   |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|HS 0455+8315            |Definite|3.5694    |Deep (V)    |Y? [a]|S/S+    |Y     |Y     |Y     |0.25-0.65     |Y     |Y     |...     |...   |...    |Y? [b]|...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|HS 0506+7725            |Possible|3.545     |None        |Y     |W       |...   |Y     |...   |...           |...   |...   |...     |Y [a] |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|HS 1813+6122            |Probable|3.54      |None        |Y     |W       |...   |Y     |Y?    |...           |...   |Y     |-       |Y [a] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V533 Her                |Definite|3.53      |None        |Y     |S+      |...   |Y     |Y [b] |~0.3-0.5 [b]  |Y [d] |Y     |...     |Y [c] |Y [c]  |Y     |Y? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|PX And                  |Definite|3.5125    |Shallow (V) |Y     |W/S     |N?    |Y     |Y     |0.3-0.6       |Y     |Y     |+?/- [b]|...   |...    |Y     |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|IM Eri                  |Possible|3.4949    |None        |Y [a] |N       |...   |...   |...   |0.5-0.6?      |...   |Y     |...     |N [b] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|CH CrB                  |Possible|3.4920    |Deep (V)    |Y     |S       |...   |...   |...   |...           |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Ha075648.83-124653.5    |Possible|3.49?     |None?       |Y     |N       |...   |N?    |...   |...           |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|CP Lac                  |Possible|3.4834    |Shallow? [a]|Y     |W       |...   |Y     |...   |...           |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|RR Pic                  |Possible|3.4806    |Shallow? [a]|Y? [d]|S+      |...   |Y     |Y     |N?            |Y [e] |Y     |+       |Y [b] |...    |...   |Y [c] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|VZ Scl                  |Possible|3.4709    |Deep (V)    |N? [b]|S       |Y     |Y     |...   |...           |...   |...   |...     |N?    |...    |Y     |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|LN UMa                  |Probable|3.466     |None?       |Y [a] |N/W     |...   |Y     |+Y [b]|0.3-0.5? [b]  |N?    |...   |...     |...   |...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V751 Cyg                |Possible|3.4671    |None [a]    |Y [a] |W       |...   |Y     |...   |...           |...   |N [b] |-       |Y? [c]|...    |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|EV Lyn                  |Possible|3.4327    |Shallow     |Y     |S+? [a] |...   |...   |...   |...           |...   |...   |...     |...   |...    |...   |N? [b]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|LS Cam                  |Possible|3.420     |None? [a]   |Y     |W       |...   |...   |...   |...           |...   |...   |...     |Y [b] |Y [b]  |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|AH Pic                  |Probable|3.3828    |None        |Y     |N       |...   |Y     |Y [b] |~0.5? [b]     |Y [b] |Y     |+?      |Y [a] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|RR Cha                  |Possible|3.362     |Deep (V)    |Y     |S       |...   |...   |...   |...           |...   |...   |+/-     |Y [a] |...    |...   |Y [b] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|BO Cet                  |Definite|3.3552    |None? [a]   |Y     |S       |...   |Y     |Y [b] |~0.5? [b]     |Y [b] |Y     |...     |Y [c] |Y [c]  |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V1315 Aql               |Definite|3.3526    |Deep (V)    |Y     |S       |Y     |Y     |Y     |0.4-0.65      |Y     |Y     |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|TT Tri                  |Definite|3.3513    |Deep (V)    |Y     |N?      |...   |Y     |Y     |0.35-0.6      |...   |Y     |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|WX Ari                  |Definite|3.3444    |Shallow [a] |Y     |W       |...   |Y     |Y? [b]|0.5-0.6? [b]  |...   |...   |...     |Y [c] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|TT Ari                  |Probable|3.3012    |None        |Y [e] |W [ae]  |...   |Y     |...   |...           |...   |...   |+/- [f] |Y [bd]|...    |Y [f] |N? [c]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|SDSS J075653.11+085831.8|Definite|3.2874 [a]|Deep (V)    |Y     |S+      |Y     |Y     |Y     |~0.3-0.6      |...   |Y?    |...     |...   |Y      |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|OZ Dra                  |Definite|3.2792    |Deep (V)    |Y     |S       |Y     |Y     |Y     |~0.5          |Y     |...   |...     |...   |...    |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|DW UMa                  |Definite|3.2786    |Deep (V) [e]|Y     |S/S+ [b]|Y     |Y     |Y     |0.4-0.6 [f]   |Y     |Y     |+/- [c] |Y [d] |Y [d]  |Y     |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|HL Aqr                  |Probable|3.2537    |None        |Y [a] |W       |...   |Y     |N? [c]|N [c]         |Y     |Y? [a]|...     |N? [b]|N      |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|SW Sex                  |Definite|3.2385    |Deep (V)    |Y     |S+      |Y     |Y     |Y     |0.4-0.65 [b]  |Y [c] |...   |N       |...   |...    |Y     |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|SDSS J080908.39+381406.2|Probable|3.2169    |Shallow? [b]|Y     |W/S     |...   |Y     |...   |~0.5? [a]     |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V482 Cam                |Definite|3.2069    |Deep (V)    |Y     |W       |...   |Y     |Y     |0.45-0.65     |...   |Y     |...     |Y [a] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Ha073418.56-170626.5    |Possible|3.1854    |Deep (V)    |Y     |W       |...   |...   |...   |...           |...   |...   |...     |...   |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|KQ Mon                  |Possible|3.07?     |None [a]    |Y [b] |N [b]   |...   |Y     |...   |0.5?          |...   |Y?    |...     |...   |... [c]|N?    |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V442 Oph                |Definite|2.9839    |None        |Y     |S       |...   |Y     |Y? [c]|~0.2-0.5? [c] |Y     |Y     |+?/- [a]|Y [d] |Y      |Y     |N? [b]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|AH Men                  |Definite|2.9518 [b]|None? [a]   |Y     |S       |...   |Y     |Y? [d]|~0.35-0.55 [d]|Y [d] |Y     |+/- [b] |Y [c] |N?     |Y     |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|DM Gem                  |Possible|2.944? [a]|None?       |Y     |S+      |...   |...   |...   |...           |...   |...   |+? [a]  |Y [b] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|KIC J192410.81+445934.9 |Possible|2.7451 [a]|None?       |Y [b] |W/S     |...   |Y?    |Y? [d]|...           |...   |...   |+/-? [a]|Y [c] |...    |Y?    |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V1084 Her               |Definite|2.8934    |None        |Y     |S/S+    |...   |Y     |Y [b] |~0.3-0.6 [b]  |...   |Y     |- [a]   |Y [c] |Y [c]  |...   |Y [d] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V592 Cas                |Probable|2.7615    |None        |Y [b] |W       |...   |Y     |Y [a] |Y [d]         |...   |Y [b] |+/- [c] |Y [c] |...    |...   |...   |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V795 Her                |Definite|2.5979    |None        |Y? [b]|S       |...   |Y     |Y? [c]|~0.3-0.7? [c] |Y     |Y     |+       |Y [a] |...    |...   |Y [d] |Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V Per                   |Probable|2.5710    |Deep (V)    |Y     |S+      |...   |Y     |Y     |0.4-0.7       |...   |...   |...     |...   |...    |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|V348 Pup                |Definite|2.4441    |Deep (V)    |Y     |S+      |Y? [b]|Y     |Y     |0.35-0.55     |Y     |...   |+       |Y? [c]|...    |...   |N? [a]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|SDSS J210131.26+105251.5|Possible|1.7? [a]  |None? [a]   |Y     |S       |...   |N? [a]|...   |...           |...   |...   |...     |N? [a]|...    |Y?    |N? [b]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|EX Hya                  |Possible|1.6376    |Shallow     |Y? [c]|W [c]   |...   |Y [c] |...   |~0.1-0.6? [c] |N [c] |Y [ac]|...     |Y [bc]|Y [bc] |N? [a]|N? [d]|Jan 2014|
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+
|Target                  |SW Sex  |Porb (h)  |Eclipse     |Single|Strong  |Line  |Strong|Phase |Transient     |Dop   |Hi Vel|Super   |~ksec |Emis   |VY Scl|Circ  |Update  |
|                        |Status  |          |            |Peaked|He II   |Eclip |S-wave|Lag   |Absorption    |Tom   |Comp  |humps   |QPO   |Flares |States|Pol   |        |
+------------------------+--------+----------+------------+------+--------+------+------+------+--------------+------+------+--------+------+-------+------+------+--------+

+++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++

Possible Possibles - Targets to Watch:
=========================================
(SW Sexiness has been suggested, but too little data currently exist to assess)

AQ Men, V382 Vel (Nova Vel 1999), and SDSS J0920+0043 (V524 Hya) - Listed as 
   confirmed SW Sex stars in 2012MmSAI..83..610S, with details forthcoming in a 
   future paper (Schmidtobreick, L., Rodriguez-Gil, P., Gaensicke, B. T., 2011, 
   MNRAS, in preparation), which does not yet appear to have been published.

V842 Cen (Nova Cen 1986), V728 Sco (Nova Sco 1862), and XX Tau (Nova Tau 1927) - 
   These three post-outburst classical novae are suggested as "low mass transfer 
   rate SW Sex stars," based mainly on the coincidence of their orbital periods 
   (~3.5-3.9 hr, 3.32 hr, and 3.26 hr, respectively) being in the 3-4 hr range 
   in which the bulk of the known SW Sex stars are found, along with the 
   supposition (based on a proposed evolutionary scenario) that prior to their 
   nova outbursts, they would have had high mass transfer rates.  See 
   2013arXiv1303.2921S.

2MASS J22560844+5954299 - As yet unpublished observations (R. Groebel, 2012, 
   private communication) show a V-shaped eclipse with depth of ~0.6 mag and an 
   orbital period of 5.49 hr.  The target is an H-alpha emission source in the 
   IPHAS catalog (IPHAS J225608.45+595430.0; 2008MNRAS.384.1277W).

+++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++

Key to Column Headings:
==========================
-Except where noted below, the standard column entries are:
     ... = No relevant data available.
       N = No, characteristic is not present in relevant data.
       Y = Yes, characteristic is present.
 Entries may be modified with:
       ? = Absence or presence of feature is uncertain.
     [x] = See note x in Target References and Notes List.

-Target = Standard variable star name (if assigned); see References and 
          Notes List for alternate names commonly used in publications. 

-SW Sex Status = Definite: The CV has been intentionally and convincingly 
                           linked to the SW Sex stars based on observational 
                           data in one or more publications.  
                 Probable: The CV has been intentionally linked to the SW Sex 
                           stars in one or more publications, but the evidence 
                           is not overly compelling.  
                 Possible: Some evidence of the known characteristics of the 
                           SW Sex stars exists in published data for the CV 
                           (based on available data, there is a reasonable 
                           chance that additional observations will provide 
                           convincing evidence that the CV is an SW Sex star).

-Porb = Orbital period in hours from the latest online edition of the Ritter & 
        Kolb catalog (2003, A&A, 404, 301; http://www.mpa-garching.mpg.de/RKcat/) 
        if there is no better published value.

-Eclipse = Presence of (optical) photometric (i.e., continuum) eclipses.
              Deep: Eclipse of the WD with depth > ~1 mag; corresponds to high 
                    inclination (i > ~75 deg).  Eclipse profile shape (V or U) 
                    is indicated in parentheses (V-shaped eclipse profiles are 
                    typical for the SW Sex stars).  Note that the eclipse 
                    profile shape corresponds to measurements in magnitudes; 
                    a V-shaped profile in magnitudes can appear as a U-shaped 
                    profile when measured in flux density units (e.g., Jy).
           Shallow: Eclipse of the WD or accretion disk with depth < ~ 1 mag; 
                    corresponds to moderate inclination (i ~ 60-75 deg).
              None: No eclipses observed; corresponds to low inclination 
                    (i < ~60 deg).

-Single Peaked = Presence of single-peaked emission lines in the average 
                 spectrum or during a significant fraction of the orbit.

-Strong He II = Presence of He II 4686 emission.
                ... = No available data.
                  N = None or not apparent from available data.
                  W = Weak; < ~25% amplitude of the H-beta emission line.
                  S = Strong; ~25-75% amplitude of H-beta.
                 S+ = Very strong; > ~75% amplitude of H-beta.

-Line Eclip = In eclipsing systems, the Balmer and He I lines are only 
              shallowly or not at all eclipsed, while the He II 4686 line is 
              deeply eclipsed.

-Strong S-wave = Presence of strong S-wave in the Balmer and/or He I emission 
                 line radial velocity curves, with typical semi-amplitude of 
                 > ~200 km/s.

-Phase Lag = Red-to-blue zero crossing of Balmer and/or He I radial velocity 
             S-wave lags (i.e. occurs after) binary orbital phase zero (i.e., 
             inferior conjunction of the secondary star = primary eclipse) by 
             ~ +0.1-0.2 in phase.

-Transient Absorption = Presence of transient absorption feature in the Balmer 
                        and/or He I emission lines; the range of binary orbital 
                        phase (i.e., zero point at inferior conjunction of the
                        secondary star = eclipse in high inclination systems)
                        displaying the absorption is noted when available.

-Dop Tom = Doppler tomograms of Balmer and/or He I lines show emission locii 
           in 3rd (lower left) quadrant (primary characteristic) and/or 2nd
           (lower right) quadrant.

-Hi Vel Comp = Presence of faint high velocity emission (or sometimes 
               absorption) line component extending past 1000 km/s, possibly 
               related to the presence of an overflowing accretion stream.  
               The radial velocity curve of this component is typically out 
               of phase with that of the main line (peak and low velocity 
               wings), with maximum blue velocity around binary orbital phase 
               0.5.  This feature is often (much) stronger on the blue-shifted 
               side of the line center.

-Superhumps = Presence of positive [+] (apsidal) and/or negative [-] (nodal) 
              superhumps in optical light curves.

-~ksec QPO = Presence of persistent/stable quasiperiodic oscillations with 
             timescale from hundreds to thousands of seconds observed in 
             optical light curves.

-Emis Flares = Presence of quasiperiodic flaring of emission lines.

-VY Scl States = Presence of faint states in the long-term light curve, as 
                 seen in the VY Scl stars.

-Circ Pol = Detection of (intrinsic) circular polarization in any wavelength
            band, which may indicate a weak WD magnetic field.  Generally, a
            3-sigma mean value and/or variable polarization with 3-sigma 
            peak-to-peak amplitude is considered significant (i.e., non-zero).
            Non-detections (i.e., <3-sigma detections), as well as upper 
            limits, are generally listed as "N?" since the possibility of 
            variable polarization makes a single (or average) null measurement 
            unreliable.

-Update = Date of most recent literature check/update for this target.

+++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++

Target References and Notes:
===============================

Ha122105.52-665048.8   
    Alt Names: 2MASS J12210553-6650487
   References: 1 = 2008MNRAS.385.1471P
        Notes: a = ~900 sec optical photometric QPO detected on one night but 
                   absent on the following night [1].


BT Mon  (Monocerotis)
    Alt Names: Nova Mon 1939
   References: 1 = 1992ApJ...401..628S
               2 = 1996ApJ...456..777W
               3 = 1998MNRAS.296..465S
               4 = 2008A&A...478..815D
        Notes: a = Measured circular polarization values of 0.10(17)%, 
                   0.04(6)%, 0.21(12)% in the 3200-8600 A region are all less 
                   than 3-sigma significant [1].
               b = ~1900 sec QPO manifests as flaring of the optical emission 
                   lines [3].
               c = Lack of superhumps expected from disk size estimate failing 
                   to reach 3:1 resonance limit [4].


V363 Aur  (Aurigae)
    Alt Names: Lanning 10
   References: 1 = 1982ApJ...252..681H 
               2 = 1986ApJ...307..760S
               3 = 1992A&A...260..213R
               4 = 2004MNRAS.353.1135T
        Notes: a = Balmer, He I, and He II lines all display shallow (or no) 
                   eclipses [4].


AC Cnc  (Cancri)
    Alt Names: SVS 1280
   References: 1 = 1983PASJ...35..423Y
               2 = 2004MNRAS.353.1135T
               3 = 2007A&A...466..589Q
        Notes: a = Balmer, He I, and He II lines all display deep eclipses [2].
               b = Transient absorption in emission lines is weak [2].
               c = Possible tertiary companion based on long-term cyclic 
                   orbital period change: cool, low mass M dwarf in 16.2 yr 
                   orbit [3].


BF Eri  (Eridani)
    Alt Names: 1WGA J0439.4-0433
   References: 1 = 2007PASP..119..494S
               2 = 2008MNRAS.386.1366N
        Notes: ...


1RXS J064434.5+334451 
    Alt Names: 2MASS J06443435+3344566
               NSV 7178256
   References: 1 = 2007A&A...474..951S
               2 = 2012MmSAI..83..729H
        Notes: a = Measured circular polarization value of +0.003(3)% in the 
                   4200-8400 A region (from observations spanning 0.3 in 
                   orbital phase) is less than 3-sigma significant [1].
               b = Emission is localized to 2nd (lower right) quadrant of 
                   Balmer line tomograms [2].


V347 Pup  (Puppis)
    Alt Names: LB 1800
               Pup2
   References: 1 = 1990ApJ...355..617B
               2 = 1994ApJ...424..347M
               3 = 1998MNRAS.299..545S
               4 = 1999ApJ...523..786D
               5 = 2005MNRAS.357..881T
        Notes: a = Measured circular polarization upper limit of <0.5% in the 
                   wavelength region 0.34-1.6 microns [1].
               b = H-beta line displays deep eclipse, while He II line displays 
                   shallow eclipse [2].
               c = Balmer, He I, and He II lines all display deep eclipses [5].


RW Tri  (Trianguli) 
    Alt Names: ...
   References: 1 = 1983ApJ...267..239K 
               2 = 1995AcA....45..259S
               3 = 1995MNRAS.273..849S
               4 = 2004A&A...417..283G
               5 = 2008IBVS.5861....1H 
        Notes: a = SW Sex characteristics mainly during bright states [3,4].


CZ Aql  (Aquilae) 
    Alt Names: ...
   References: 1 = 2007PASP..119..494S
        Notes: a = 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 (or no) time-series photometry 
                   obtained for this CV. 
               b = "...emission lines have strong wings that move with large 
                   velocity amplitude, suggesting a magnetically channeled 
                   accretion flow." [1]


UX UMa  (Ursae Majoris) 
    Alt Names: ...
   References: 1 = 1983ApJS...53..397S
               2 = 1992ApJ...401..628S
               3 = 1994AcA....44...59S
               4 = 1995ApJ...448..395B
               5 = 1998ApJ...499..429K
               6 = 2003ApJ...584..433F
               7 = 2011MNRAS.410..963N
        Notes: a = Measured circular polarization value of -0.06(4)% in the 
                   3200-8600 A region [2] is less than 3-sigma significant.
               b = A short ~29 sec QPO, although not always present [4,6], has 
                   been consistently detected in UV observations of UX UMa [5]. 
                   There have been no reported detections of ~ksec QPOs 
                   (e.g., [4,6]).
               c = UV light curve "dip" centered around orbital phase 0.6 has 
                   been attributed to an asymmetric vertical extension in the 
                   outer accretion disk absorbing flux from the disk interior 
                   [6] and is reminiscent of the SW Sex star phase-dependent 
                   absorption. 
               d = Displayed SW Sex characteristics during observations made in 
                   1999, but these had almost completely disappeared in 
                   observations made in 2008 [7].


2MASS J01074282+4845188 
    Alt Names: ...
   References: 1 = 2012NewA...17...34D
               2 = 2013A&A...551A.125K
        Notes: a = Presence of some characteristic SW Sex observational 
                   features cannot be confirmed with existing spectroscopic 
                   data [2].


Ha094409.36-561711.4 
    Alt Names: 2MASS J09440940-5617117
   References: 1 = 2008MNRAS.385.1471P
               2 = 2011IBVS.5971....1S
        Notes: ...


LS Peg  (Pegasi)
    Alt Names: NSV 13903
               S193
               Peg2
   References: 1 = 1992JAVSO..21...81G
               2 = 1992ApJ...401..628S
               3 = 1999PASP..111..184T
               4 = 1999MNRAS.305..661M
               5 = 2001ApJ...548L..49R
               6 = 2001AJ....121.2761S
               7 = 2008MNRAS.387.1157R
        Notes: a = Multiple optical photometric QPOs in the range ~1000-2000 
                   sec are detected [3,5,6].  A 1776(108) sec QPO is possibly 
                   the WD spin period [5], although a 35 ksec XMM-Newton X-ray 
                   observation shows no evidence for a WD spin period between 
                   a few hundred sec and 10 ksec, possibly because the spin and 
                   magnetic axes of the WD are closely aligned [7].
               b = Measured circular polarization varies between 0.0% and -0.3% 
                   on a period of 29.6(1.8) min in the wavelength region 
                   3720-5070 A [5].  Previous circular polarization measurement 
                   of -0.01(5)% in the wavelength region 5000-6000 A [2] is 
                   less than 3-sigma significant, but the uncertainty is 
                   possibly elevated by the variability observed by [5].


V1193 Ori  (Orionis)
    Alt Names: Hamuy's Star
   References: 1 = 1987PASP...99.1097B
               2 = 1994MNRAS.271..323R
               3 = 2005NewA...11..147A
               4 = 2006MNRAS.368..361P
               5 = 2006A&A...456..599P
               6 = 2009AAS...21343411S
               7 = 2012MmSAI..83..610S
        Notes: a = Optical photometric QPOs in the range 649-1720 sec are 
                   detected [4], including a dominant signal at ~1200 sec [5].


V1776 Cyg  (Cygni)
    Alt Names: Lanning 90
   References: 1 = 1983PASP...95..206S
               2 = 1990ApJ...365..696G
               3 = 1998PhDT........10H
        Notes: ...


Lanning 386 
    Alt Names: ...
   References: 1 = 2008PASP..120..301B
        Notes: a = This CV behaves like a dwarf nova with frequent outbursts 
                   of amplitude up to ~2 mag, but shows SW Sex star 
                   characteristics during the outburst peaks [1].


UU Aqr  (Aquarii)
    Alt Names: S196
   References: 1 = 1991AJ....102.1417D
               2 = 1994ApJ...433..332B
               3 = 1996MNRAS.282...99B
               4 = 1998MNRAS.294..689H
               5 = 1998ApJ...499..444K
               6 = 2002AN....323...75V
               7 = 2005PASP..117.1204P
               8 = 2008ApJ...676.1240B
        Notes: a = H-alpha line is deeply eclipsed [3].
               b = 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 [8].


LX Ser  (Serpentis)
    Alt Names: Stepanyan's Star
   References: 1 = 1980IBVS.1743....1L
               2 = 1980ApJ...242L.167H
               3 = 1981ApJ...244..259Y
               4 = 1984PASP...96..372E
               5 = 1992ApJ...401..628S
        Notes: a = H-gamma and He II 4686 are both deeply eclipsed [3].
               b = ~140 sec optical photometric QPO is only marginally detected 
                   [4] and is classified as a dwarf nova oscillation (DNO); no 
                   other QPOs are detected [4].
               c = Measured circular polarization value of +0.04(7)% in the 
                   3200-8600 A region [3] is less than 3-sigma significant.


BH Lyn  (Lyncis)
    Alt Names: PG 0818+513
   References: 1 = 1991AJ....102..683T
               2 = 1992MNRAS.258..225D
               3 = 1997ApJ...481..433H
               4 = 2002PASP..114.1364P
               5 = 2005PASP..117.1204P
               6 = 2006A&A...455..223S
        Notes: a = In some observations, the Balmer lines are deeply eclipsed 
                   while He I 4471 line is only shallowly eclipsed [2].
               b = Possible ~1030 sec [4] and ~2700 sec [6] optical photometric 
                   QPOs are detected.


OY Ara  (Arae)
    Alt Names: Nova Ara 1910
               HD 149990
   References: 1 = 1997ApJ...483..899Z
        Notes: ...


V380 Oph  (Ophiuchi) 
    Alt Names: ...
   References: 1 = 1985AJ.....90..643S
               2 = 2005ASPC..330..495R
               3 = 2007MNRAS.374.1359R
        Notes: a = 2802(6) sec 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 [3].


BB Dor  (Doradus)
    Alt Names: EC 05287-5857
   References: 1 = 2001MNRAS.325...89C
               2 = 2012MmSAI..83..610S
               3 = 2012MNRAS.422..731S
               4 = 2012MNRAS.422.2332R
        Notes: a = Optical photometric QPOs in the range ~900-1560 sec are 
                   detected [1].
               b = Two high velocity, out of phase, H-alpha "satellite lines" 
                   observed during photometric faint state in 2009 [3].  
                   Emission from these features in the 1st (upper right) and 
                   4th (upper left) quadrants dominates the H-alpha Doppler 
                   tomograms [3].
               c = During intermittent accretion events in the 2008-2009 faint 
                   state, the radial velocity of the H-alpha line wings has a 
                   phase lag of ~0.2 [4].


WY Sge  (Sagittae)
    Alt Names: Nova Sge 1783
   References: 1 = 1983ApJ...264..560S
               2 = 1984ApJ...282..763S
               3 = 1992ApJ...401..628S
               4 = 1996MNRAS.278..845S
               5 = 1997MNRAS.284..359S
        Notes: a = Measured circular polarization value of +0.32(46)% in the 
                   3200-8600 A region [3] is less than 3-sigma significant.


BP Lyn  (Lyncis)
    Alt Names: PG 0859+414
               Lyn1
   References: 1 = 1994AJ....108..214G
               2 = 1996ApJ...470.1052H
               3 = 1996MNRAS.282..943S
        Notes: a = Eclipse of the accretion disk bright spot only [3].
               b = H-alpha line is eclipsed but He I 5876 line is not [3].
               c = Lines are double-peaked at orbital phase 0.8-0.2 and 
                   single-peaked at other phases [2,3]; unclear if this is due 
                   to transient absorption at phases 0.8-0.2 or "filling in" of 
                   double-peaked profile at phases 0.3-0.7.  Trailed spectra 
                   imply that phase-dependent double-peaked/single-peaked 
                   profiles are produced by two out of phase emission 
                   components [3].  However, spectra at some phases around 
                   0.6-0.7 show H-beta and H-gamma absorption component below 
                   the continuum [2].
               d = Balmer emission tomograms show almost ring-like structure 
                   with possibly enhanced emission in 2nd (lower right) 
                   quadrant [2,3]; however, interpretation of the tomograms is 
                   somewhat uncertain, since the orbital phasing based on the 
                   eclipse (which is assumed to be of the disk bright spot, not 
                   the WD) is likely skewed relative to the line-of-centers 
                   between the stars (which also introduces uncertainty to the 
                   determination of the phase offset of the radial velocity 
                   curves) [2].


AO Psc  (Piscium)
    Alt Names: H 2252-035
   References: 1 = 1984A&A...131..137V
               2 = 1984AcA....34..397K 
               3 = 1986MNRAS.222..225C
               4 = 1991MNRAS.248..233H
               5 = 1992ApJ...401..628S
               6 = 2005ApJ...626.1028H
               7 = 2009A&A...496..891B
        Notes: a = The detected ~805 sec UV-optical photometric and 
                   spectroscopic QPO is possibly the WD spin period, while the 
                   related ~859 sec QPO is the beat period between the shorter 
                   QPO and the orbital period [2,6].
               b = Transient absorption observed in HST/STIS UV spectra [6].
               c = Measured circular polarization values of +0.03(3)% in the 
                   5700-9200 A region (with maximum peak-to-peak variability of 
                   1.30+/-0.50%) [3], and -0.02% through +0.3% in the UBVRI 
                   bands (simultaneous) [7], are less than 3-sigma significant. 
                   Also see additional circular polarization non-detections 
                   in [5].


V1294 Tau  (Tauri) 
    Alt Names: KUV 03580+0614
               HS 0357+0614
               Tau2
   References: 1 = 2001MNRAS.326.1235T
               2 = 2001PASP..113.1215S
               3 = 2005ASPC..330..335R
               4 = 2012MmSAI..83..610S
        Notes: a = Balmer line red-to-blue zero crossing in arbitrary 
                   spectroscopic orbital phasing is assumed to have a +0.2 
                   phase lag from the binary orbital phase zero (inferior 
                   conjunction of the secondary star), as is typical for the 
                   SW Sex stars [1].  In [2], the phase of the red-to-blue 
                   crossing of the He II 4686 line radial velocity curve was 
                   assumed to reflect the motion of the WD, resulting in a 
                   similar relative phase lag of the Balmer line velocities.
               b = ~1200 sec optical photometric QPO is detected [2].
               c = VY Scl status is not noted in the literature, but long-term 
                   AAVSO light curve shows probable faint states in 2009 and 
                   late-2013 through 2014 (ongoing).


HS 0220+0603 
    Alt Names: 2MASS J02230165+0616496
   References: 1 = 2005ASPC..330..335R
               2 = 2007MNRAS.377.1747R
               3 = 2012MmSAI..83..602R
        Notes: a = Shows unusual N II and Si II emission lines suggesting that 
                   the donor star may have experienced nuclear evolution via 
                   the CNO cycle [2].
               b = Eclipse is narrow and flat-bottomed during the faint 
                   state [3].


HS 0455+8315 
    Alt Names: 2MASS J05064821+8319235
   References: 1 = 2002pcvr.conf..623G
               2 = 2005ASPC..330..335R
               3 = 2007MNRAS.377.1747R
        Notes: a = Balmer and He I lines in average [1] and trailed [3] 
                   spectrum are slightly double-peaked, while the He II 4686 
                   line is single-peaked.
               b = VY Scl status is not noted in the literature, but long-term 
                   AAVSO light curve shows possible faint state in 2013.
               

HS 0506+7725
    Alt Names: ...
   References: 1 = 2005A&A...443..995A
        Notes: a = Optical photometric QPOs in the range ~600-1200 sec are 
                   detected [1].


HS 1813+6122 
    Alt Names: 2MASS J18142983+6123344
   References: 1 = 2005ASPC..330..335R
               2 = 2007MNRAS.377.1747R
        Notes: a = Optical photometric QPOs in the range ~600-1200 sec are 
                   detected [2].


V533 Her  (Herculis)
    Alt Names: Nova Her 1963
   References: 1 = 1979ApJ...233L..13P
               2 = 1983ApJ...273..255R
               3 = 1992ApJ...401..628S
               4 = 2000MNRAS.312..629T
               5 = 2002MNRAS.337..209R
               6 = 2004PASP..116..115W
               7 = 2004AJ....128.1279H
        Notes: a = Measured circular polarization values of -0.38(11)% and 
                   0.00(7)% in the 3200-8600 A region [3] are more and less 
                   than 3-sigma significant, respectively.
               b = Balmer line red-to-blue zero crossing in arbitrary 
                   spectroscopic orbital phasing is assumed to have a +0.2 
                   phase lag from the binary orbital phase zero (inferior 
                   conjunction of the secondary star), as is typical for the 
                   SW Sex stars [4].  
               c = 1400(95) sec QPO manifests as optical emission line flaring, 
                   and is possibly the (magnetic) WD spin period [5].  The 
                   origin of a shorter ~63 sec QPO has been suggested as the 
                   spin [1] or pulsation [2] of the WD or a dwarf nova 
                   oscillation (DNO) [6], but it has not been consistently 
                   re-detected in later observations [2,4].  
               d = Note that [5] claim that the faint emission spot in the 1st 
                   (upper right) quadrant of the He I doppler tomograms of 
                   V533 Her is a real feature, and dispute the conclusion by 
                   2000ApJ...537..936H that a similar feature in the He I 4471 
                   tomogram of V442 Oph is an artifact.  Unfortunately, [5] 
                   have mistakenly claimed that 2000ApJ...537..936H conclude 
                   that the artifact is caused by the phase 0.5 transient 
                   absorption; hence, when it still appears in the tomograms 
                   constructed by 2000ApJ...537..936H from just the spectra 
                   unaffected by the absorption, it must be real.  However, 
                   2000ApJ...537..936H made no such claim; instead they note
                   that inspection of the forward-projections of the tomograms 
                   of V442 Oph shows that the feature is a reflection artifact 
                   of the emission locus in the 3rd (lower left) quadrant of 
                   the tomogram - it is *not* present in the original trailed 
                   spectrum.  The implication is that the origin of the 
                   emission locus in the 3rd quadrant defies the fundamental 
                   assumption of tomography; namely, that all emission regions 
                   are visible at all orbital phases.  Hence, the corresponding 
                   emission region must not be visible at orbital phases 
                   corresponding to its location in the 1st quadrant of the 
                   tomogram (i.e., orbital phases ~0.1-0.2, assuming it is 
                   associated with the accretion disk).  This is consistent 
                   with the "ridgeline" model proposed and described in 
                   2000ApJ...537..936H.


PX And  (Andromedae)
    Alt Names: PG 0027+260
               And1
   References: 1 = 1991AJ....102..272T
               2 = 1992ApJ...401..628S
               3 = 1994ApJ...431L.107H
               4 = 1995MNRAS.273..863S
               5 = 1999dicb.conf...61P
               6 = 2002A&A...394..625S
               7 = 2005PASP..117.1204P
               8 = 2010A&A...514A..30T
        Notes: a = Measured circular polarization values of -0.02(9)% and 
                   +0.06(4)% in the 3200-8600 A region [2] are less than 
                   3-sigma significant.
               b = No evidence for positive superhumps [8] found in earlier 
                   observations [5,7].


IM Eri  (Eridani)
    Alt Names: EC 04224-2014
   References: 1 = 2001MNRAS.325...89C
               2 = 2009AAS...21343411S
        Notes: a = Balmer lines are broad absorption troughs with emission 
                   cores when the CV is bright, and broad emission lines when 
                   it is faint [1].
               b = No detected optical photometric QPOs with periods 
                   >20 sec [1].


CH CrB  (Coronae Borealis)
    Alt Names: SDSS J160745.02+362320.7
   References: 1 = 2006AJ....131..973S
               2 = 2010NewA...15..476Z
        Notes: ...


Ha075648.83-124653.5 
    Alt Names: 2MASS J07564886-1246538
   References: 1 = 2008MNRAS.385.1471P
               2 = 2010MNRAS.403..398P
        Notes: ...


CP Lac  (Lacertae)
    Alt Names: Nova Lac 1936
   References: 1 = 1996MNRAS.281..192R
               2 = 2005A&A...431..289R
               3 = 2006PASP..118..687P
        Notes: a = Presence of shallow eclipses is tentatively suggested, 
                   although based on only one such observed event [2].


RR Pic  (Pictoris)
    Alt Names: Nova Pic 1925
               Hen 3-15
   References: 1 = 1975A&A....41...15V
               2 = 1981MNRAS.195..101W
               3 = 1982A&A...109..171H
               4 = 1984AcA....34..331K
               5 = 1985A&A...150..325H
               6 = 1986MNRAS.219..751W
               7 = 2003MNRAS.342..145S
               8 = 2006PASP..118...84R
               9 = 2008MNRAS.389.1345S
        Notes: a = Shallow eclipses of the accretion disk/bright spot are noted 
                   [1].  The strong orbital modulation seen in the 1970s was 
                   replaced in the 1980s by an irregular, shallow eclipse 
                   superimposed on a flickering background [6], but was 
                   subsequently not reliably detected [9]. 
               b = In addition to a 780 sec optical photometric QPO [9], RR Pic 
                   displays a 20-40 sec QPO that is a possible dwarf nova 
                   oscillation with most stable period near 32 sec [2].  A 
                   possible IP classification was suggested based on a claimed 
                   900 sec photometric periodicity [4], but this was refuted by 
                   non-detections of the periodicity in several subsequent 
                   observing programs [5,6].  The somewhat shorter (780 sec) 
                   QPO reported by [9] in recent observations is perhaps a 
                   recurrence of the 900 sec periodicity from [4] (which had 
                   reported aliases at 780 and 1020 sec).
               c = Measured circular polarization is +0.17(1)% in unfiltered 
                   (blue) optical light [3].
               d = Balmer emission line profiles show slight double-peaking 
                   that is present for most of the orbit [7,8].
               e = Main H-alpha emission sites in doppler tomograms located in 
                   2nd (lower right) and 4th (upper left) quadrants [7]; 
                   tomograms in [8] show emission in 3rd (lower left) quadrant.


VZ Scl  (Sculptoris) 
    Alt Names: ...
   References: 1 = 1975MNRAS.172..433W
               2 = 1984MNRAS.206..859S
               3 = 1986MNRAS.222..225C
               4 = 1987MNRAS.225...43O
               5 = 1999AAS...195.3612M
        Notes: a = Measured circular polarization value of +0.18(8)% in the 
                   3500-9200 A region [3] is (barely) less than 3-sigma 
                   significant.
               b = Balmer emission line profiles show slight double-peaking [4].


LN UMa  (Ursae Majoris)
    Alt Names: PG 1000+667
               UMa7
   References: 1 = 1998AJ....115.2044H
               2 = 2004AJ....128.1279H
               3 = 2007MNRAS.374.1359R
               4 = 2009JAD....15....1P
        Notes: a = H-beta and higher order Balmer lines manifest as broad 
                   absorption troughs with strong emission cores [1,3].
               b = Spectroscopic phase offset from the binary orbital phasing 
                   is defined by assuming that a "flux deficit" in the emission 
                   lines corresponds to transient absorption at orbital phase 
                   0.5, under the assumption that the CV is an SW Sex star [3].


V751 Cyg  (Cygni)
    Alt Names: ...
   References: 1 = 1974PASP...86..401R
               2 = 1998A&A...336..626G
               3 = 1999A&A...343..183G
               4 = 2001PASP..113...72P
        Notes: a = [4] note departures from "normal" SW Sex star spectroscopic 
                   observational characteristics, but suggest these could be 
                   due to viewing at low inclination. 
               b = Emission lines are situated in broad absorption troughs; 
                   orbital behavior of the absorption troughs is similar to 
                   that seen for the high velocity emission wings in some 
                   SW Sex stars [4].
               c = Inspection of optical light curves by eye suggests ~1000 sec 
                   photometric QPO is present, but this is not strongly 
                   confirmed by power spectrum analysis [4].


EV Lyn  (Lyncis)
    Alt Names: SDSS J075443.01+500729.2
   References: 1 = 2006AJ....131..973S
               2 = 2007MNRAS.382.1145S
        Notes: a = He II 4686 emission line is comparable in strength to 
                   H-beta, but the Balmer lines are quite weak [1].
               b = Measured circular polarization upper limit of <0.1-0.4% in 
                   the optical [1].


LS Cam  (Camelopardalis) 
    Alt Names: HS 0551+7241
   References: 1 = 1998AJ....115.1634D
               2 = 2005ASPC..330..335R
        Notes: a = The possible start of an eclipse was observed [1] but has 
                   not been subsequently confirmed.
               b = ~3000 sec QPO manifests as optical emission line flaring [1].


AH Pic  (Pictoris)
    Alt Names: EC 05565-5935
   References: 1 = 2001MNRAS.325...89C
               2 = 2007MNRAS.374.1359R
        Notes: a = Optical photometric QPOs in the range ~600-1200 sec are 
                   detected [1].
               b = Spectroscopic phasing transformed to binary orbital phasing 
                   by assuming that lowest velocity narrow emission line 
                   component originates on the secondary star [2].


RR Cha  (Chamaeleontis)
    Alt Names: Nova Cha 1953
               S5346
   References: 1 = 1996A&AS..117..449Z
               2 = 2002MNRAS.335...44W
               3 = 2003MNRAS.342L...1R
        Notes: a = ~1950 sec optical photometric QPO is believed to be related 
                   to the (magnetic) WD spin period, either directly or via 
                   reprocessing [2].
               b = Measured circular polarization is highly variable between 
                   negative and positive values with peak-to-peak amplitude 
                   of ~10% [3].


BO Cet  (Ceti)
    Alt Names: 1H 0204-023
               Cet4
   References: 1 = 1995A&AS..114..575Z
               2 = 2007MNRAS.374.1359R
        Notes: a = Lack of eclipses assumed based on inclination estimates 
                   derived from spectroscopic observations [2]. 
               b = Spectroscopic phasing transformed to binary orbital phasing 
                   by assuming that lowest velocity narrow emission line 
                   component originates on the secondary star [2].
               c = 1194(54) sec QPO manifests as optical emission line flaring, 
                   and is possibly related to the (magnetic) WD spin period [2].


V1315 Aql  (Aquilae)
    Alt Names: KPD 1911+1212
   References: 1 = 1986ApJ...301..240D
               2 = 1991MNRAS.252..342D
               3 = 1993MNRAS.264..619S
               4 = 1995MNRAS.277..777D
               5 = 1996ApJ...471..949H
        Notes: ...


TT Tri  (Trianguli)
    Alt Names: HS 0129+2933
               GB 286
   References: 1 = 2005ASPC..330..335R
               2 = 2006PASP..118.1373W
               3 = 2007MNRAS.377.1747R
        Notes: ...


WX Ari  (Arietis)
    Alt Names: PG 0244+104
   References: 1 = 1983IBVS.2295....1W
               2 = 1992A&A...256..442B
               3 = 1994A&A...289..148H
               4 = 1998PhDT........10H
               5 = 2000A&A...355..181R
               6 = 2002PASP..114.1364P
        Notes: a = Early time-series observations of WX Ari did not reveal 
                   eclipses [1,2,3], but shallow eclipses were found in later 
                   long-term photometric observations [5].
               b = If spectroscopic phase offset relative to binary phasing is 
                   +0.2 as found in other SW Sex stars, then transient 
                   absorption occurs at phases 0.5-0.6 [2,4].
               c = ~1180 sec optical photometric QPO is detected [6].


TT Ari  (Arietis)
    Alt Names: RX J0206.8+1517
               BD +14 341
   References: 1 = 1985ApJ...290..707S
               2 = 1992A&A...265...77H
               3 = 1992ApJ...401..628S
               4 = 1999A&A...347..178G
               5 = 2002ApJ...569..418W
               6 = 2002PASP..114.1364P
               7 = 2009A&A...496..765K
        Notes: a = Weak or no He II 4686 emission observed during the faint 
                   state [1,4].
               b = Optical photometric QPOs in the range ~200-300 sec possibly 
                   result from the WD spin period; this is inferred under the 
                   assumption that the observed longer timescale (~1000-2000 
                   sec) QPOs result from the beat period between the WD spin 
                   and the orbital period of the inner edge of a truncated 
                   accretion disk [2,4]. 
               c = Measured circular polarization values of -0.01(2)% and 
                   -0.02(2)% in the 3200-8600 A region [3] are less than 
                   3-sigma significant.
               d = Possibly displayed a trend of decreasing dominant QPO 
                   timescale from 1962 (∼1700 sec) to 1985 (∼1000 sec), which 
                   continued to more recent observations (e.g., ∼900 sec in 
                   1988) [2]; this is disputed by [7], who observed a longer 
                   QPO (~1300 s) starting in late 2005 through early 2006, 
                   following the transition from displaying positive superhumps 
                   (during 1997-2005) back to negative superhumps.
               e = During the bright state, the Balmer lines are broad 
                   absorption troughs with strong narrow emission cores; 
                   He II 4686 emission is also present, but is not comparable 
                   in strength to the emission core of the H-beta line [5].
               f = The long-term AAVSO light curve of TT Ari shows the 
                   following behavior: deep (~5 mag) faint states occurred 
                   during 1979-1986 (with an extended return to almost the 
                   bright state level during 1981) and during late-2009 through 
                   early 2011.  An intermediate (~0.5-1 mag) faint state 
                   occurred during 2005.  An extended shallow (~0.3 mag) faint 
                   state occurred during 1997 through 2004.  Published 
                   time-series observations show the following behavior: a 
                   positive superhump was present during 1997-2005 (shallow and 
                   intermediate faint states), replacing the negative 
                   superhump seen during 1988-1997 (bright state) [6].  A 
                   negative superhump returned in late 2005 (bright state 
                   following the intermediate faint state) [7].


SDSS J075653.11+085831.8
    Alt Names: SDSS 0756+0858
   References: 1 = 2011AJ....142..181S
               2 = 2014arXiv1401.0635.pdf 
        Notes: a = Orbital period determined from multiple nights of 
                   photometric and spectroscopic time-series observations [2].


OZ Dra  (Draconis)
    Alt Names: SDSS J132723.39+652854.2
               SDSS 496-083
   References: 1 = 2003PASP..115.1118W
               2 = 2010NewA...15..476Z
        Notes: a = Measured circular polarization upper limit of <0.24(17)% in 
                   the wavelength range 4000-8000 A [1].


DW UMa  (Ursae Majoris) 
    Alt Names: PG 1030+590
   References:  1 = 1988ApJ...327..248S
                2 = 1992ApJ...401..628S
                3 = 1994MNRAS.266..859D
                4 = 1998PhDT........10H
                5 = 2000ApJ...539L..49K
                6 = 2000A&A...364..573B
                7 = 2002PASP..114.1364P
                8 = 2003ApJ...583..437A
                9 = 2003AJ....126.2473H
               10 = 2004A&A...416.1057S
               11 = 2004AJ....128.1279H
               12 = 2004ApJ...615L.129K
               13 = 2007MNRAS.377.1747R
               14 = 2010AJ....140.1313H
               15 = 2013MNRAS.428.3559D
        Notes:  a = Measured circular polarization value of +0.06(14)% in the 
                   3200-8600 A region [2] is less than 3-sigma significant.
                b = Faint state observation shows no He II 4686 emission [3].
                c = Superhump changed from negative to positive between 1996 
                   and 2002 [7].
                d = A reported ~1800 sec QPO manifests as optical emission line 
                   flaring; however it is attributed only as a private 
                   communication in [13].  [9] found no evidence for emission 
                   line flaring or periods other than the orbital period in 
                   far-UV observations; however, optical emission line flaring 
                   has been observed [13,15].  Additional QPOs in the range 
                   ~1600-3000 sec have been observed [6,7].
                e = Very soft X-ray spectrum and likely partial X-ray eclipse, 
                   implying X-ray reprocessing in a vertically extended 
                   region [14]. 
                f = In addition to the usual orbital phase 0.5 transient 
                   absorption, stationary "tramline" absorption features in the 
                   H-beta trailed spectrum are attributed to blobs of material 
                   ejected from the inner binary (possibly via a magnetic 
                   propeller) and passing across the line of sight [15].


HL Aqr  (Aquarii) 
    Alt Names: PHL 227
   References: 1 = 1985A&A...149L...4H
               2 = 1987MNRAS.224..231H
               3 = 1995AJ....110.1824D
               4 = 2004PASP..116..115W
               5 = 2007MNRAS.374.1359R
        Notes: a = Balmer lines of H-beta and higher are broad absorption 
                   troughs with narrow single-peaked emission cores [1]; 
                   H-alpha manifests as a narrow single-peaked emission line 
                   [2].  The orbital behavior of the absorption troughs is 
                   similar to that seen for the high velocity emission wings in 
                   some SW Sex stars [5].
               b = A short 19.6 sec optical photometric QPO found by [2] is 
                   classified as a dwarf nova oscillation (DNO) by [4].
               c = "HL Aqr is definitely not a 'typical' SW Sex star."  For 
                   example, the phase offset of the Balmer line radial 
                   velocities is ~ -0.1 (instead of +0.1-0.2) and there is no 
                   apparent transient absorption [5].


SW Sex  (Sextantis) 
    Alt Names: PG 1012-029
   References: 1 = 1984ApJ...276..233P
               2 = 1992ApJ...401..628S
               3 = 1997MNRAS.291..694D
               4 = 2001A&A...368..183G
               5 = 2012NewA...17..533R
               6 = 2013MNRAS.428.3559D
        Notes: a = Measured circular polarization upper limit of <0.15% in 
                   unfiltered broad-band (optical) light [1], as well as 
                   measured circular polarization values of +0.05(14)% and 
                   -0.03(5)% in the 3200-8600 A region [2], are less than 
                   3-sigma significant.
               b = When SW Sex was observed during an apparently rare faint 
                   state, the transient absorption seen in the emission lines 
                   at orbital phase 0.5 during the normal bright state was not 
                   detected [4,6].
               c = Balmer line Doppler tomograms during the faint state show 
                   emission localized along the accretion stream trajectory and 
                   a faint emission ring [6].


SDSS J080908.39+381406.2 
    Alt Names: HS 0805+3822
   References: 1 = 2003AJ....126.1499S
               2 = 2007ApJ...654.1036L
               3 = 2007MNRAS.377.1747R
        Notes: a = Zero point of phasing uncertain, but appears to have been 
                   assigned to the red-to-blue crossing of the Balmer emission 
                   line radial velocity curves [1,2], so is likely offset by 
                   ~ +0.1-0.2 from the binary orbital phasing (with inferior 
                   conjunction of the secondary star at phase zero).
               b = Possible grazing eclipses, similar to WX Ari [3].


V482 Cam  (Camelopardalis)
    Alt Names: HS 0728+6738
   References: 1 = 2004A&A...424..647R
        Notes: a = Optical photometric QPOs in the range ~420-600 sec (with 
                   dominant signal at 426 sec) are detected [1].


Ha073418.56-170626.5	
    Alt Names: 2MASS J07341858-1706265
   References: 1 = 2008MNRAS.385.1471P
        Notes: ...


KQ Mon  (Monocerotis) 
    Alt Names: EC 04224-2014
   References: 1 = 2002ApJ...565..511H
               2 = 2005IBVS.5627....1S
               3 = 2009AAS...21343411S
               4 = 2012MmSAI..83..610S
               5 = 2013AJ....145..168W
        Notes: a = This CV is a close visual triple, resolved in 2MASS near-IR 
                   images [1].
               b = Only the H-alpha emission line is apparent; the shorter 
                   wavelength region of the optical spectrum is almost 
                   featureless blue continuum with weak Balmer absorption [2,5].
               c = [5] attribute detection of high velocity emission wings in 
                   KQ Mon to 2005ASPC..330..335R and cite the Big List (where 
                   they state that KQ Mon is classified as a "probable" SW Sex 
                   star) as the source of this information.  This is incorrect 
                   on all fronts.  KQ Mon is not included at all in 
                   2005ASPC..330..335R (which also does not discuss high 
                   velocity emission wings in any SW Sex star candidate), nor 
                   is that reference cited for KQ Mon in the Big List; the 
                   classification of KQ Mon in the Big List has always been 
                   "possible".  The conclusion in [5] that KQ Mon is a likely 
                   SW Sex star based primarily on the similarity of its UV 
                   spectrum to the UV spectra of BP Lyn, V795 Her, and LS Peg 
                   is not convincing.


V442 Oph  (Ophiuchi) 
    Alt Names: SVS 337
   References: 1 = 1983PASP...95..509S
               2 = 1988PASP..100.1522G
               3 = 1992ApJ...401..628S
               4 = 2000ApJ...537..936H
               5 = 2001ApJ...553L.177D
               6 = 2002PASP..114.1364P
        Notes: a = Fourier analysis of time-series optical photometric data by 
                   [1] showed no stable oscillation period down to 20 s, but 
                   the UV continuum varied on a period of 3.37 hr that is 
                   significant at the 95% level [1] and is possibly a positive 
                   superhump, consistent with a possible 3.22 hr signal 
                   inferred by [6].  [6] additionally found a persistent 
                   negative superhump at a period of 2.9016 hr.
               b = Measured circular polarization values of +0.01(5)% and 
                   -0.03(8)% in the 3200-8600 A region [3] are less than 
                   3-sigma significant.
               c = Spectroscopic phase of the red-to-blue crossing of the 
                   He II 4686 line radial velocity curve was assumed to reflect 
                   the motion of the WD, corresponding to a phase lag of +0.08 
                   for the Balmer line velocities [4].
               d = Optical photometric QPOs in the range ~800-1200 sec (with 
                   most stable component at ~1000 sec) were detected [6].


AH Men  (Mensae) 
    Alt Names: 1H 0551-819
               Men1
   References: 1 = 1993MNRAS.265..926B
               2 = 1995PASP..107..657P
               3 = 1995A&AS..114..575Z
               4 = 1999A&A...346..151G
               5 = 2007MNRAS.374.1359R
        Notes: a = Dips at maximum light are possibly shallow eclipses, but 
                   this has not been confirmed [1].
               b = Although the orbital period of AH Men is still somewhat 
                   uncertain, it is believed that the stable period found by 
                   [2] (2.95 hr) is the best candidate, with the longer 
                   (3.34 hr, 3.05 hr) and shorter (2.88 hr) periods found by 
                   [1,2] and [2], respectively, originating from positive and 
                   negative superhumps, respectively [5].
               c = (Magnetic) WD spin period is possibly twice the observed 
                   1040 sec QPO period [2].  Other photometric QPO signals in 
                   the ~600-2400 sec range are observed [1,2].
               d = Spectroscopic radial velocity phase offset estimated under 
                   the assumption that the radial velocities behave as those of 
                   a "standard" SW Sex star [5].


DM Gem  (Geminorum) 
    Alt Names: Nova Gem 1903
               HD 48328
   References: 1 = 2000IAUC.7433....3L.pdf
               2 = 2005A&A...431..289R
        Notes: a = Photometric periods of 0.12266 d (2.944 hr) and 0.12287 d 
                   (2.949 hr) found by [1] (and supported by the identification 
                   of a single period of 0.123 d by [2]) are interpreted here 
                   as the orbital period and a positive superhump period, 
                   respectively.
               b = 1355(5) sec optical photometric QPO is detected [2].


KIC J192410.81+445934.9 
    Alt Names: KIC 8751494
   References: 1 = 2010AJ....139.2587W
               2 = 2010MNRAS.409.1470O
               3 = 2013PASJ...65...76K
        Notes: a = The orbital period was confirmed by [3] with the previous 
                   candidate (2.94 hr; [1]) now identified as a positive 
                   superhump period.  [3] also detected a possible negative 
                   superhump with period of ~2.57-2.59 hr.
               b = Balmer lines are broad absorption troughs with strong, 
                   narrow emission cores [1,2].
               c = Optical photometric QPOs with periods of ~650 sec and 
                   ~1200 sec are detected [1].
               d = If it is assumed that the optical maximum in the 
                   phase-folded light curve is due to the reflection effect on 
                   the secondary star (and, therefore, corresponds to binary 
                   orbital phase 0.0), then the time of spectroscopic phase 
                   zero (red-to-blue crossing) of [1] corresponds to a phase 
                   lag of +0.20(4) relative to the binary orbital phasing [3].  
                   Note that [3] mistakenly state in the text of their Section 
                   2.4 that they assign orbital phase 0.5 to the optical 
                   maximum, but the folded light curve shown in their Figure 5 
                   has correctly labelled the optical *minimum* as phase 0.5.


V1084 Her  (Herculis) 
    Alt Names: RX J1643.7+3402
   References: 1 = 2002A&A...381..894M
               2 = 2002PASP..114.1364P
               3 = 2009MNRAS.395..973R
        Notes: a = [2] found a negative superhump period of 2.807 in data from 
                   Apr-Jun 2002, but did not recover the likely negative 
                   superhump period of 2.595 hr found with large amplitude 
                   (~0.1 mag) by [1] in data from Sep 2000.
               b = Light curve constructed from the phase-folded optical 
                   photometry exhibits double-humped profile that is possibly 
                   ellipsoidal variation; blue-to-red crossing radial velocity 
                   phase offset of +0.2 is estimated under the assumption that 
                   the shallower of the two minima in the folded light curve 
                   corresponds to inferior conjunction of the secondary star 
                   (i.e., binary orbital phase 0.0) [1,2].
               c = Optical photometric QPOs in the range ~600-1200 sec are 
                   detected, including an apparently stable component at 
                   1043 sec [1,2,3].  An additional 2330(23) sec QPO manifests 
                   as optical emission line flaring at twice the polarimetric 
                   period [3].
               d = Measured circular polarization is variable with amplitude 
                   ranging from -0.5% to +0.5% on a period of 19.38(39) min 
                   = 1163(23) sec [3].


V592 Cas  (Cassiopeiae) 
    Alt Names: KPD 0018+5525
               LS I +55 8
   References: 1 = 1998PASP..110..784H
               2 = 1998PASP..110.1148T
               3 = 2002IBVS.5358....1K
               4 = 2003MNRAS.346..861W
               5 = 2004MNRAS.355..137P
               6 = 2009AJ....137..197K
        Notes: a = Balmer line radial velocity curve phase offset is measured 
                   relative to the He II 4686 radial velocity curve [1].
               b = H-beta and H-gamma lines are broad absorption troughs with 
                   strong, narrow emission cores; the absorption trough for 
                   H-beta is quite shallow, while for H-gamma (and higher order 
                   Balmer lines) it is substantially deeper [1,2,4].  The 
                   velocity and depth behavior of the blue side of the 
                   absorption trough is reminiscent of the faint high velocity 
                   emission component seen in some SW Sex stars [4]; this 
                   behavior is also present in the UV lines [5].
               c = Despite detection of both positive and negative superhumps 
                   by [2], no superhumps were detected during the observations 
                   by [3] in which a ~1300 sec photometric QPO was detected.
               d = Evidence for disk wind absorption in UV and optical emission 
                   lines (e.g., P Cygni profiles) varies over the orbital 
                   period and is possibly phase-dependent, indicating an 
                   asymmetric outflow [4,5,6]. 


V795 Her  (Herculis) 
    Alt Names: PG 1711+336
   References: 1 = 1990ApJ...354..708S
               2 = 1996MNRAS.278..219C
               3 = 1997MNRAS.286..447D
               4 = 2002ASPC..261..533R
               5 = 2002PASP..114.1364P
               6 = 2010A&A...514A..30T
        Notes: a = Detected optical photometric QPOs of ~4860 sec and ~6370 sec 
                   were suggested as possibly the WD spin period in the case of 
                   single beam or dipole beam IP models, respectively [1]; 
                   however, the polarization variability results suggest a 
                   shorter WD spin period [4], similar to the 1150 sec optical 
                   photometric QPO noted by [5].
               b = Peaks of the Balmer emission lines are slightly 
                   double-peaked throughout most of the orbit [1,2,3].
               c = The He II 4686 radial velocity curve was assumed to track 
                   the motion of the WD in order to estimate the phase offset 
                   of the Balmer and He I radial velocity curves and transform 
                   the spectroscopic phasing (zero point at the red-to-blue 
                   zero crossing) to the binary orbital phase (zero point at 
                   inferior conjunction of the secondary star) [2].
               d = Measured circular polarization increases from mean levels of 
                   0.16(4)% in U-band to 0.41(13)% in I-band, and is variable 
                   with a peak-to-peak amplitude of 0.12% in U-band on a period 
                   of 1170 sec (or twice that) [4].


V Per  (Persei) 
    Alt Names: Nova Per 1887
               BD +56 406a
               HD 12244
   References: 1 = 1989ApJ...339L..75S
               2 = 1992ApJ...393..729W
               3 = 1992ApJ...401..628S
               4 = 1996MNRAS.281..192R
               5 = 2006ApJ...644.1104S
               6 = 2007IBVS.5751....1H
        Notes: a = Measured circular polarization value of -0.81(82)% in the 
                   3200-8600 A region [3] is less than 3-sigma significant.


V348 Pup  (Puppis) 
    Alt Names: 1H 0709-360
               Pup1
   References: 1 = 1990ApJ...359..204T
               2 = 2000MNRAS.317..759R
               3 = 2001MNRAS.328..903R
               4 = 2003AJ....126..964F
               5 = 2010MNRAS.409.1195D
        Notes: a = Measured circular polarization values of -0.09(11)% in the 
                   3400-5300 A region and +0.14(13)% in the 5500-8400 A region 
                   [1] are less than 3-sigma significant.
               b = Both the Balmer and He II 4686 emission lines display 
                   relatively shallow eclipses [3]; the former is expected in 
                   SW Sex stars, but the latter is not.
               c = ~900 sec photometric QPO possibly present in short R-band 
                   light curve [3]; however, [4] find no evidence for periodic 
                   variability in UV observations that would signal the 
                   presence of a magnetic WD.


SDSS J210131.26+105251.5 
    Alt Names: 2XMM J210131.2+105251
   References: 1 = 2003AJ....126.1499S
               2 = 2006AJ....132.2743H
        Notes: a = The photometric and spectroscopic time-series behavior is 
                   complex, but has no dominant signal that obviously 
                   represents the orbital period; the best candidate for the 
                   orbital period is ~100 min based on a weak modulation in the 
                   X-ray and optical light curves [1,2].
               b = Measured circular polarization upper limit of <0.4% in 
                   optical spectropolarimetry [2].


EX Hya  (Hydrae) 
    Alt Names: EUVE J1252-29.2 
               1E 1249-2858 
   References: 1 = 1986MNRAS.222..225C
               2 = 1987MNRAS.228..463H
               3 = 1987ApJ...317..765K
               4 = 1989MNRAS.238.1107H
               5 = 1990A&A...240..360R
               6 = 1992ApJ...401..628S
               7 = 2000MNRAS.313..703H
               8 = 2007MNRAS.380..353M
               9 = 2009IBVS.5876....1M
        Notes: a = EX Hya is a known IP, with 15 photometric (dwarf nova) 
                   outbursts of ~3 mag in amplitude lasting ~2-4 days observed 
                   during the 44 years leading up to 2000.  It is likely that 
                   the number of observed outbursts is ~50% of the total number 
                   of outbursts during this time, leading to an average 
                   recurrence time scale of ~1.5 yr (however, the outbursts 
                   occur irregularly).  EX Hya displays some SW Sex star 
                   characteristics (linked to a disk-overflowing accretion 
                   stream) during outbursts [7].
               b = The spin of the magnetic WD produces a ~4020 sec photometric 
                   and spectroscopic modulation [2,3,7] that is best-phased 
                   with a cubic ephemeris [9] and is detected in both quiescent 
                   [2,3,7] and outburst [5] states.
               c = Observations obtained during outburst [4,5,8].
               d = Measured circular polarization values of -0.02(4)% in the 
                   5700-9200 A region [1] and +0.01(2)% in the 5900-8600 A 
                   region [6] are less than 3-sigma significant.



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