National Aeronautics and Space Administration

IPs

V455 And
V515 And
AE Aqr
FO Aqr
V349 Aqr
XY Ari
V405 Aur
V647 Aur
HT Cam
MU Cam
DW Cnc
BG CMi
V709 Cas
V1025 Cen
V1033 Cas
TV Col
TX Col
UU Col
V2069 Cyg
V2306 Cyg
DO Dra
PQ Gem
V418 Gem
DQ Her
V1323 Her
V1460 Her
V1674 Her
EX Hya
NY Lup
V2400 Oph
V2731 Oph
V3037 Oph
V598 Peg
GK Per
AO Psc
HZ Pup
V667 Pup
WX Pyx
V1223 Sgr
V4743 Sgr
CC Scl
V1062 Tau
EI UMa
AX J1740.1
AX J1832.3
AX J1853.3
CTCV J2056
CXO J174954
IGR J04571
IGR J08390
IGR J15094
IGR J16500
IGR J16547
IGR J17014
IGR J17195
IGR J18151
IGR J18173
IGR J18308
IGR J19267
LAMOST 0240
PBC J0927.8
PBC J1841.1
RX J1804
RX J2015
RX J2113
RX J2133
RX J2306
Swift J0717
Swift J1839
Swift J2006
Swift J2138

Full Catalog

Related Systems

Potential IP Candidates

There are some objects for which I have not put on the list of IPs and IP candidates, most often because of insufficient information. I would like to see further observational results before placing them on my scale from "doubtful" to "ironclad." These are:

• Parisi et al. 2012 proposed that PBC J0826.3-7033 (= Swift J0826.2-7033 = 1RXS J082623.5-703142 = 1ES 0826-703) is a non-magnetic CV, based in part on their distance estimate of 90 pc. However, it is now known to be more distant (~350 pc), and hence more luminous.
• Tomsick et al. (2012) published Chandra position of INTEGRAL sources including IGR J12489-6243, which they considered a possible CV, and IGR J15293-5609, which they thought was a symbiotic star. Fortin et al. (2018) considered both to be CVs based on IR observations. Little else is known for these sources.
• Shears et al. 2015 considered the possibility that HW Boo is an IP.
• Shears 2015 considered the possibility that 1RXS J140429.5+172352 is an IP.
• Greiner & Richter 2015 speculated that their Sagitta Field source 120a (likely also the XMM Slew Survey source XMMSL1J201359.1+154419) with a variable (16.5-18.0 mag) blue counterpart may be an IP.
• Lutovinov et al. 2015 proposed AX J173548-3207 (originally detected in the ASCA Galactic Plane survey, Sugizaki et al. 2001) to be a quiescent LMXB. They may well be right, but it's not easy to distinguish between qLMXBs and CVs with the sparse data available for this object.
• Fornasini et al. 2014 considers AX J1637.8-4656 (another source from the ASCA Galactic Plane survey, Sugizaki et al. 2001) to be an IP candidate, even though the possible 7100 s period of this source would be extremely long to be the spin period of an IP.
• Four sources from Tomsick et al. 2017 are of potential interest in this connection:
  • P49: NuSTAR J233426-2343.9 = 1RXS J233427.8-234419
  • P144: NuSTAR J073959-3147.8 = 3XMM J074000.5-314759
  • S27: NuSTAR J105008-5958.8 = 3XMM J105008.1-595902
  • P408: NuSTAR 182604-0707.9 = CXO J182604.6-070806
• So are eight source from Fornasini et al. 2017
  • NNR4: CXOU J163750.8-465545
  • NNR6: CXOU J163355.1-473804
  • NNR9: CXOU J163912.9-462357
  • NNR12: CXOU J164027.8-462513
  • NNR13: CXOU J163957.8-46254
  • NNR18: CXOU J163329.5-473332 (see also Bodaghee et al. 2014)
  • NNR19: NuSTAR J164116-4632.2
  • NNR25: NuSTAR J163600-4748.4
• Peng & Shen 2021 claimed that OGLE-UCXB-01 to be an IP.