V455 And
V515 And
AE Aqr
FO Aqr
V349 Aqr
XY Ari
V405 Aur
V647 Aur
HT Cam
MU Cam
DW Cnc
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
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
PBC J0927.8
PBC J1841.1
RX J1804
RX J2015
RX J2113
RX J2133
RX J2306
Swift J0717
Swift J1839
Swift J2006
Swift J2138

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Pretorius & Mukai 2014

Bibinfo (this paper at ADS)
Pretorius, M.L., Mukai, K., 2014, MNRAS, 442, 2580-2585.
Observational: Space density.
FO Aqr, XY Ari, V405 Aur, TV Col, PQ Gem, NY Lup, V2400 Oph, V2731 Oph, GK Per, AO Psc, V1223 Sgr, V1062 Tau, EI UMa, IGR J15094-6649, and IGR J16500-3307. as well as other BAT-detected IPs.
There are 19 CVs that are detected by BAT above a flux threshold of 2.5 x 10-11 and located at Galactic latitude greatre than 5 degrees (|b|>5), and 15 of them are IPs (the other 4 are SS Cyg, AM Her, BY Cam and V1432 Aql). Distance estimates for these 15 long-period IPs are evaluated, leading to an estimate of their space density of 1 (+1, -0.5) x 10-7pc-3. Although these IPs are at LX ~ 1033 erg/s, there is evidence of a fainter population (including BAT-detected IPs V1025 Cen, DO Dra, and EX Hya) dominated by short-period IPs, whose space density may be considerably higher.

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