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---- /!\ '''Edit conflict - your version:''' ---- || SSS || ||MPE || || || Novae || FWH, WNP ||MPE? || || || pre-CVs || || ADS (AIP) || all known non-resolved WD/dM pairs || || AM CVns, UCBs || || AR |||| || Symbiotics || || ADS(AIP)|| || ---- /!\ '''End of edit conflict''' ---- |
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---- /!\ '''Edit conflict - your version:''' ---- || White Dwarfs || KW, VB, ADS ||IAAT - TR || || || NSs - Pulsars || ||VD ||version by VD: [[attachment:atnf.fits]] based on ATNF catalogue. Includes also PWN pulsars and isolated NSs (most). X-ray fluxes are only estimates (based spin/dot as done in Vink et al, 2011). NS classes are quoted according to HEASARC (limited), so difficult to select subsets of NSs || || NSs - PWN || || WB|| || || NSs - isolated || WB, FWH, MS, GP, ASa, VD, AP, ADS, TP, TT || AP,VD,DK || XDINs, AXPs, SGRs, CCOs, RRATs || || ULX || ||VD ||version by VD: [[attachment:ulxcat.fits]] based on Swartz et al 2011 || ---- /!\ '''End of edit conflict''' ---- |
Catalogs as input for the eROSITA catalog tool
OBJECT CLASS |
Science |
Catalogs |
comment |
CVs |
ADS, IT, VB, RSC, AR |
ADS(AIP) |
known CVs and candidates with and without orbital periods |
![/!\](/moin_static1911/modernized/img/alert.png "/!\"){kind=small}
Edit conflict - other version:
SSS |
|
MPE |
|
Novae |
FWH, WNP |
MPE? |
|
pre-CVs |
|
ADS (AIP) |
all known non-resolved WD/dM pairs |
AM CVns, UCBs |
|
AR |
|
Symbiotics |
|
ADS(AIP) |
|
Edit conflict - your version:
SSS |
|
MPE |
|
Novae |
FWH, WNP |
MPE? |
|
pre-CVs |
|
ADS (AIP) |
all known non-resolved WD/dM pairs |
AM CVns, UCBs |
|
AR |
|
Symbiotics |
|
ADS(AIP) |
|
End of edit conflict
LMXBs |
ASa, SP, LD, TT |
AR,VD |
version by VD: lmxbcat.fits based on Liu et al 2007, and Ritter&Kolb v 7.17 |
HMXBs |
DK, IK, LD, ASa, FWH |
VD |
version by VD: hmxbcat.fits based on Liu et al, 2006 |
BHCs |
JW, WNP, FWH, AR |
AR |
Edit conflict - other version:
White Dwarfs |
KW, VB, ADS |
IAAT - TR |
|
NSs - Pulsars |
|
VD |
version by VD: atnf.fits based on ATNF catalogue. Includes also PWN pulsars and isolated NSs (most). X-ray fluxes are only estimates (based spin/dot as done in Vink et al, 2011). NS classes are quoted according to HEASARC (limited), so difficult to select subsets of NSs |
NSs - PWN |
|
WB |
|
NSs - isolated |
WB, FWH, MS, GP, ASa, VD, AP, ADS, TP, TT |
AP,VD,DK |
XDINs, AXPs, SGRs, CCOs, RRATs |
ULX |
|
VD |
version by VD: ulxcat.fits based on Swartz et al 2011 |
Edit conflict - your version:
White Dwarfs |
KW, VB, ADS |
IAAT - TR |
|
NSs - Pulsars |
|
VD |
version by VD: atnf.fits based on ATNF catalogue. Includes also PWN pulsars and isolated NSs (most). X-ray fluxes are only estimates (based spin/dot as done in Vink et al, 2011). NS classes are quoted according to HEASARC (limited), so difficult to select subsets of NSs |
NSs - PWN |
|
WB |
|
NSs - isolated |
WB, FWH, MS, GP, ASa, VD, AP, ADS, TP, TT |
AP,VD,DK |
XDINs, AXPs, SGRs, CCOs, RRATs |
ULX |
|
VD |
version by VD: ulxcat.fits based on Swartz et al 2011 |
End of edit conflict