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Table 2

Derived distances for the 16 CVs and related objects shown in Table 1.

Source Pre-Gaia distance Gaia distance AAVSO Vis M V X-ray luminosity
(pc) (pc) (mag) (mag) (erg s-1)

Classical novae
V603 Aql 249 HST parallax (1) 328.3 ± 77.9 –0.5 11.7 –8.1 4.1 2.9 × 1032 (Swift)
RR Pic 521 HST (1), 600 ± 60 expansion (2) 388.3 ± 87.8 1.0 12.2 –6.9 4.3 0.4 × 1031 (0.3–5 keV, XMM)
HR Del 970 ± 70 expansion (3) 560.7 ± 170.5 3.6 12.1 –5.1 3.4 1.5 × 1031 (Swift)

Nova-like
TT Ari 335 ± 50 white dwarf/secondary (4) 228.8 ± 29.6 10.1 15.9 3.3 9.1 6.4–131 × 1030 (Swift)
IX Vel 96 Hipp parallax (5) 88.8 ± 3.2 9.0 10.5 4.3 5.8 7.9 × 1030 (ASCA)
UX UMa 345 ± 34 colours/models (6) 263.5 ± 30.4 12.2 14.9 5.1 6.7 0.7 × 1031 (0.2–10 keV, XMM)
V3885 Sgr 110 Hipp parallax (5) 135.9 ± 8.3 9.8 10.8 4.1 5.1 7.7 × 1030 (Swift)

Dwarf novae
RX And ~200 spectra/models (7) 185.5 ± 23.7 10.1 15.6 3.8 9.3 3.6–53 × 1030 (Swift)
HL CMa None 309.8 ± 42.7 10.6 14.9 3.1 7.4 2.5–4.0 × 1032 (Swift)
AH Her 660 parallax (8) 325.0 ± 47.2 10.9 14.8 3.3 7.2
SS Cyg 114 ± 2 VLA (9) 117.1 ± 6.2 8.0 12.7 2.6 7.4 4.7–63 × 1031 (Swift)
121 ± 6, 166 ± 12 HST (10,11)
Z Cam 163 parallax (8) 219.3 ± 19.5 10.1 14.0 3.4 7.3 8.1–18.4 × 1030 (Swift)
BV Cen ~435 UV models (12) 344.3 ± 64.8 10.7 13.5 3.0 5.8 1.9 × 1032 (2–10 keV, Suzaku)

Magnetic
AE Aqr 102 parallax (8) 91.4 ± 3.3 10.6 12.2 5.8 7.4 7.5 × 1030 (XMM Suzaku)

Others
QU Car >500 (13) 410.2 ± 86.1 10.8 12.4 2.7 4.3 1.9 × 1032 (0.2–12 keV XMM)
V Sge 320 parallax (14) 761.5 ± 213.4 9.6 13.3 0.2 2.3

Notes. The distances were taken from the catalogue of Astraatmadja & Bailer-Jones (2016) and we used the values for a scale length, L = 0.11 kpc. We also give the distance estimates prior to Gaia where available, the observed optical brightness range in the V-band determined from AAVSO data spanning the period 1995–2015 (apart from the three old novae), and the range in absolute magnitude MV implied by the TGAS distances. We determine X-ray luminosities using the TGAS distance and X-ray flux compiled from the literature or from an analysis of Swift data.

Reference. (1) Harrison et al. (2013); (2) Gill & O’Brien (1998); (3) Harman & O’Brien (2003); (4) Gänsicke et al. (1999); (5) Duerbeck (1999); (6) Baptista et al. (1995); (7) Sion et al. (2001); (8) Thorstensen (2003); (9) Miller-Jones et al. (2013); (10) Nelan & Bond (2013); (11) Harrison et al. (1999); (12) Sion et al. (2007); (13) Gilliland & Philips (1982); (14) van Altena et al. (1995).

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