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

Full Catalog

Related Systems

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X-ray Fluxes

In this version of the catalog, X-ray fluxes are taken from major catalogs whenever available.

Hard X-ray Fluxes

I took the hard X-ray (14-195 keV) fluxes listed in the Swift BAT 157 month survey catalog. This is the latest update by the BAT team, continuing from the 22 month survey (Tueller et al. ), the 70 month survey (Baumgartner et al.), and the 105 month survey (Oh et al.).

X-ray Fluxes from the XMM-Newton Serendipitous Survey

For the traditional (<10 keV) X-ray band, I first search for the object in the Fourth XMM-Newton Serendipitous Source Catalog (4XMM-DR11; see Webb et al. 2020) and list the band 8 (0.2-12 keV) flux from combined EPIC data. In a few cases, I used the stacked version of the catalog (Traulsen et al.).

As a back-up option (after 4XMM-DR11 and 2SXPS) is the XMM Slew Survey catalog (Saxton et al. 2008). In this case, the flux is also for the total band (0.2-12 keV) of EPIC instruments.

X-ray Fluxes from the Swift X-ray Telescope Point Source Catalog

When an object is not listed in the XMM-Newton Serendipitous Survey catalog, I then consulted the Swift XRT point source catalog (2SXPS; see Evans et al.). This catalog reports 0.3-10 keV fluxes based on power-law and thermal plasma model fits; for most IPs, the former usually provides a better phenomenological fit (presumably because of the complex absorber usually present in the X-ray spectra of IPs), so that value is adopted for the purpose of the IP catalog.

However, if I know that the Swift observations were taken mostly during nova eruptions or dwarf nova outbursts, then I do not use the 2SXPS fluxes, since the intent is to list a typical X-ray flux during normal accretion-powered phase of each IP or candidate.

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Please send your comments, suggestions etc. to Koji.Mukai@nasa.gov and/or Koji.Mukai@umbc.edu
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