Nova* . | N H † . | Distance . | U.L.‡ . | N s § . | Reference for distance . |
---|---|---|---|---|---|
. | (cm−2) . | (kpc) . | ave (min–max) . | . | . |
V2672 Oph | 4.18 × 1021 | 19 ± 2 | 2.51 (0.71–4.24) | 22 | Takei et al. (2014) |
V5584 Sgr | 3.96 × 1021 | 6.3 ± 0.5 | 1.20 (0.38–3.28) | 134 | Raj et al. (2015) |
V496 Sct | 6.81 × 1021 | 2.9 ± 0.3 | 2.22 (0.74–4.75) | 45 | Raj et al. (2012) |
KT Eri | 5.52 × 1020 | 6.6 ± 0.8 | 1.71 (0.61–6.03) | 109 | Imamura and Tanabe (2012) |
V1722 Aql | 9.14 × 1021 | 5 | 1.97 (0.63–6.01) | 112 | Munari et al. (2010) |
V2673 Oph | 2.84 × 1021 | 7.4 | 1.42 (0.43–4.38) | 77 | Munari and Dallaporta (2010) |
V5585 Sgr | 2.75 × 1021 | N/A | 1.76 (0.50–4.36) | 44 | |
V2674 Oph | 4.12 × 1021 | 9 | 1.75 (0.67–3.96) | 30 | Munari, Dallaporta, and Ochner (2010) |
V407 Cyg | 8.19 × 1021 | 2.7 | 1.83 (0.56–4.46) | 52 | Munari, Margoni and Stagni (1990) |
V5586 Sgr | 9.60 × 1021 | N/A | 2.79 (1.21–5.64) | 23 | |
V1311 Sco | 4.78 × 1021 | N/A | 1.98 (0.52–4.44) | 20 | |
V1723 Aql | 1.23 × 1022 | 6 | 1.76 (0.49–4.97) | 140 | Weston et al. (2016) |
V5587 Sgr | 4.09 × 1021 | N/A | 1.56 (0.30–3.67) | 126 | |
V5588 Sgr | 5.47 × 1021 | 7.6 | 2.15 (0.65–5.67) | 122 | Munari et al. (2015) |
T Pyx | 1.88 × 1021 | 3.5 ± 1 | 1.87 (0.43–8.19) | 35 | Schaefer (2010) |
V1312 Sco | 5.14 × 1021 | N/A | 1.61 (0.47–4.64) | 118 | |
PR Lup | 4.82 × 1021 | N/A | 1.25 (0.39–3.76) | 144 | |
V1313 Sco | 4.77 × 1021 | N/A | 1.09 (0.26–3.71) | 55 | |
V965 Per | 1.20 × 1021 | N/A | 3.56 (1.37–8.18) | 17 | |
V834 Car | 4.98 × 1021 | N/A | 1.49 (0.38–5.09) | 121 | |
V1368 Cen | 4.30 × 1021 | N/A | 1.37 (0.46–3.50) | 47 | |
V2676 Oph | 3.02 × 1021 | N/A | 1.34 (0.36–3.56) | 89 | |
V5589 Sgr | 3.35 × 1021 | N/A | 2.21 (0.47–5.85) | 111 | |
V5590 Sgr | 2.64 × 1021 | N/A | 2.19 (0.70–5.50) | 107 | |
V2677 Oph | 3.38 × 1021 | N/A | 3.46 (0.79–11.27) | 44 | |
V1324 Sco | 4.35 × 1021 | 4.5 | 2.56 (0.79–6.05) | 47 | Ackermann et al. (2014) |
V5591 Sgr | 4.27 × 1021 | N/A | 2.31 (0.61–6.59) | 134 | |
V5592 Sgr | 1.49 × 1021 | N/A | 2.01 (0.72–5.96) | 93 | |
V5593 Sgr | 6.54 × 1021 | N/A | 2.31 (0.66–5.97) | 115 | |
V959 Mon | 6.29 × 1021 | 3.6 | 2.68 (0.71–9.77) | 118 | Shore et al. (2013) |
V1724 Aql | 1.47 × 1022 | N/A | 2.49 (0.61–7.11) | 133 | |
V809 Cep | 8.22 × 1021 | 6.5 | 1.98 (0.65–5.25) | 93 | Munari et al. (2014) |
V1533 Sco | 7.42 × 1021 | N/A | 2.10 (0.66–4.36) | 84 | |
V339 Del | 1.36 × 1021 | 4.2 | 2.04 (0.64–6.08) | 140 | Shore (2013) |
V1830 Aql | 1.23 × 1022 | N/A | 3.08 (0.86–8.20) | 128 | |
V556 Ser | 4.87 × 1021 | N/A | 2.54 (0.93–6.70) | 89 | |
V1369 Cen | 5.84 × 1021 | 2.4 | 2.58 (0.74–8.95) | 83 | Shore et al. (2014) |
V962 Cep | 3.30 × 1021 | N/A | 2.72 (1.11–11.86) | 125 | |
V1534 Sco | 3.88 × 1021 | 13 | 1.77 (0.79–4.24) | 22 | Joshi et al. (2015) |
V2659 Cyg | 4.92 × 1021 | N/A | 2.27 (0.73–6.13) | 124 |
Nova* . | N H † . | Distance . | U.L.‡ . | N s § . | Reference for distance . |
---|---|---|---|---|---|
. | (cm−2) . | (kpc) . | ave (min–max) . | . | . |
V2672 Oph | 4.18 × 1021 | 19 ± 2 | 2.51 (0.71–4.24) | 22 | Takei et al. (2014) |
V5584 Sgr | 3.96 × 1021 | 6.3 ± 0.5 | 1.20 (0.38–3.28) | 134 | Raj et al. (2015) |
V496 Sct | 6.81 × 1021 | 2.9 ± 0.3 | 2.22 (0.74–4.75) | 45 | Raj et al. (2012) |
KT Eri | 5.52 × 1020 | 6.6 ± 0.8 | 1.71 (0.61–6.03) | 109 | Imamura and Tanabe (2012) |
V1722 Aql | 9.14 × 1021 | 5 | 1.97 (0.63–6.01) | 112 | Munari et al. (2010) |
V2673 Oph | 2.84 × 1021 | 7.4 | 1.42 (0.43–4.38) | 77 | Munari and Dallaporta (2010) |
V5585 Sgr | 2.75 × 1021 | N/A | 1.76 (0.50–4.36) | 44 | |
V2674 Oph | 4.12 × 1021 | 9 | 1.75 (0.67–3.96) | 30 | Munari, Dallaporta, and Ochner (2010) |
V407 Cyg | 8.19 × 1021 | 2.7 | 1.83 (0.56–4.46) | 52 | Munari, Margoni and Stagni (1990) |
V5586 Sgr | 9.60 × 1021 | N/A | 2.79 (1.21–5.64) | 23 | |
V1311 Sco | 4.78 × 1021 | N/A | 1.98 (0.52–4.44) | 20 | |
V1723 Aql | 1.23 × 1022 | 6 | 1.76 (0.49–4.97) | 140 | Weston et al. (2016) |
V5587 Sgr | 4.09 × 1021 | N/A | 1.56 (0.30–3.67) | 126 | |
V5588 Sgr | 5.47 × 1021 | 7.6 | 2.15 (0.65–5.67) | 122 | Munari et al. (2015) |
T Pyx | 1.88 × 1021 | 3.5 ± 1 | 1.87 (0.43–8.19) | 35 | Schaefer (2010) |
V1312 Sco | 5.14 × 1021 | N/A | 1.61 (0.47–4.64) | 118 | |
PR Lup | 4.82 × 1021 | N/A | 1.25 (0.39–3.76) | 144 | |
V1313 Sco | 4.77 × 1021 | N/A | 1.09 (0.26–3.71) | 55 | |
V965 Per | 1.20 × 1021 | N/A | 3.56 (1.37–8.18) | 17 | |
V834 Car | 4.98 × 1021 | N/A | 1.49 (0.38–5.09) | 121 | |
V1368 Cen | 4.30 × 1021 | N/A | 1.37 (0.46–3.50) | 47 | |
V2676 Oph | 3.02 × 1021 | N/A | 1.34 (0.36–3.56) | 89 | |
V5589 Sgr | 3.35 × 1021 | N/A | 2.21 (0.47–5.85) | 111 | |
V5590 Sgr | 2.64 × 1021 | N/A | 2.19 (0.70–5.50) | 107 | |
V2677 Oph | 3.38 × 1021 | N/A | 3.46 (0.79–11.27) | 44 | |
V1324 Sco | 4.35 × 1021 | 4.5 | 2.56 (0.79–6.05) | 47 | Ackermann et al. (2014) |
V5591 Sgr | 4.27 × 1021 | N/A | 2.31 (0.61–6.59) | 134 | |
V5592 Sgr | 1.49 × 1021 | N/A | 2.01 (0.72–5.96) | 93 | |
V5593 Sgr | 6.54 × 1021 | N/A | 2.31 (0.66–5.97) | 115 | |
V959 Mon | 6.29 × 1021 | 3.6 | 2.68 (0.71–9.77) | 118 | Shore et al. (2013) |
V1724 Aql | 1.47 × 1022 | N/A | 2.49 (0.61–7.11) | 133 | |
V809 Cep | 8.22 × 1021 | 6.5 | 1.98 (0.65–5.25) | 93 | Munari et al. (2014) |
V1533 Sco | 7.42 × 1021 | N/A | 2.10 (0.66–4.36) | 84 | |
V339 Del | 1.36 × 1021 | 4.2 | 2.04 (0.64–6.08) | 140 | Shore (2013) |
V1830 Aql | 1.23 × 1022 | N/A | 3.08 (0.86–8.20) | 128 | |
V556 Ser | 4.87 × 1021 | N/A | 2.54 (0.93–6.70) | 89 | |
V1369 Cen | 5.84 × 1021 | 2.4 | 2.58 (0.74–8.95) | 83 | Shore et al. (2014) |
V962 Cep | 3.30 × 1021 | N/A | 2.72 (1.11–11.86) | 125 | |
V1534 Sco | 3.88 × 1021 | 13 | 1.77 (0.79–4.24) | 22 | Joshi et al. (2015) |
V2659 Cyg | 4.92 × 1021 | N/A | 2.27 (0.73–6.13) | 124 |
*U Sco, V1310 Sco, V5666 Sgr, and V745 Sco listed in table 1 are removed (see text).
†Total Galactic H i column density toward the source as the average of the values obtained by the Leiden/Argentine/Bonn (LAB) map (Kalberla et al. 2005) and the DL map (Dickey & Lockman 1990), calculated using the HEASARC website 〈http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/w3nh/w3nh.pl〉.
‡90% C.L. upper limit for the flux in the 2–4 keV band for each scan in units of 10−2 counts s−1 cm−2. The average (minimum and maximum) fluxes among Ns scans are shown.
§Number of GSC scans in the searched period.
Nova* . | N H † . | Distance . | U.L.‡ . | N s § . | Reference for distance . |
---|---|---|---|---|---|
. | (cm−2) . | (kpc) . | ave (min–max) . | . | . |
V2672 Oph | 4.18 × 1021 | 19 ± 2 | 2.51 (0.71–4.24) | 22 | Takei et al. (2014) |
V5584 Sgr | 3.96 × 1021 | 6.3 ± 0.5 | 1.20 (0.38–3.28) | 134 | Raj et al. (2015) |
V496 Sct | 6.81 × 1021 | 2.9 ± 0.3 | 2.22 (0.74–4.75) | 45 | Raj et al. (2012) |
KT Eri | 5.52 × 1020 | 6.6 ± 0.8 | 1.71 (0.61–6.03) | 109 | Imamura and Tanabe (2012) |
V1722 Aql | 9.14 × 1021 | 5 | 1.97 (0.63–6.01) | 112 | Munari et al. (2010) |
V2673 Oph | 2.84 × 1021 | 7.4 | 1.42 (0.43–4.38) | 77 | Munari and Dallaporta (2010) |
V5585 Sgr | 2.75 × 1021 | N/A | 1.76 (0.50–4.36) | 44 | |
V2674 Oph | 4.12 × 1021 | 9 | 1.75 (0.67–3.96) | 30 | Munari, Dallaporta, and Ochner (2010) |
V407 Cyg | 8.19 × 1021 | 2.7 | 1.83 (0.56–4.46) | 52 | Munari, Margoni and Stagni (1990) |
V5586 Sgr | 9.60 × 1021 | N/A | 2.79 (1.21–5.64) | 23 | |
V1311 Sco | 4.78 × 1021 | N/A | 1.98 (0.52–4.44) | 20 | |
V1723 Aql | 1.23 × 1022 | 6 | 1.76 (0.49–4.97) | 140 | Weston et al. (2016) |
V5587 Sgr | 4.09 × 1021 | N/A | 1.56 (0.30–3.67) | 126 | |
V5588 Sgr | 5.47 × 1021 | 7.6 | 2.15 (0.65–5.67) | 122 | Munari et al. (2015) |
T Pyx | 1.88 × 1021 | 3.5 ± 1 | 1.87 (0.43–8.19) | 35 | Schaefer (2010) |
V1312 Sco | 5.14 × 1021 | N/A | 1.61 (0.47–4.64) | 118 | |
PR Lup | 4.82 × 1021 | N/A | 1.25 (0.39–3.76) | 144 | |
V1313 Sco | 4.77 × 1021 | N/A | 1.09 (0.26–3.71) | 55 | |
V965 Per | 1.20 × 1021 | N/A | 3.56 (1.37–8.18) | 17 | |
V834 Car | 4.98 × 1021 | N/A | 1.49 (0.38–5.09) | 121 | |
V1368 Cen | 4.30 × 1021 | N/A | 1.37 (0.46–3.50) | 47 | |
V2676 Oph | 3.02 × 1021 | N/A | 1.34 (0.36–3.56) | 89 | |
V5589 Sgr | 3.35 × 1021 | N/A | 2.21 (0.47–5.85) | 111 | |
V5590 Sgr | 2.64 × 1021 | N/A | 2.19 (0.70–5.50) | 107 | |
V2677 Oph | 3.38 × 1021 | N/A | 3.46 (0.79–11.27) | 44 | |
V1324 Sco | 4.35 × 1021 | 4.5 | 2.56 (0.79–6.05) | 47 | Ackermann et al. (2014) |
V5591 Sgr | 4.27 × 1021 | N/A | 2.31 (0.61–6.59) | 134 | |
V5592 Sgr | 1.49 × 1021 | N/A | 2.01 (0.72–5.96) | 93 | |
V5593 Sgr | 6.54 × 1021 | N/A | 2.31 (0.66–5.97) | 115 | |
V959 Mon | 6.29 × 1021 | 3.6 | 2.68 (0.71–9.77) | 118 | Shore et al. (2013) |
V1724 Aql | 1.47 × 1022 | N/A | 2.49 (0.61–7.11) | 133 | |
V809 Cep | 8.22 × 1021 | 6.5 | 1.98 (0.65–5.25) | 93 | Munari et al. (2014) |
V1533 Sco | 7.42 × 1021 | N/A | 2.10 (0.66–4.36) | 84 | |
V339 Del | 1.36 × 1021 | 4.2 | 2.04 (0.64–6.08) | 140 | Shore (2013) |
V1830 Aql | 1.23 × 1022 | N/A | 3.08 (0.86–8.20) | 128 | |
V556 Ser | 4.87 × 1021 | N/A | 2.54 (0.93–6.70) | 89 | |
V1369 Cen | 5.84 × 1021 | 2.4 | 2.58 (0.74–8.95) | 83 | Shore et al. (2014) |
V962 Cep | 3.30 × 1021 | N/A | 2.72 (1.11–11.86) | 125 | |
V1534 Sco | 3.88 × 1021 | 13 | 1.77 (0.79–4.24) | 22 | Joshi et al. (2015) |
V2659 Cyg | 4.92 × 1021 | N/A | 2.27 (0.73–6.13) | 124 |
Nova* . | N H † . | Distance . | U.L.‡ . | N s § . | Reference for distance . |
---|---|---|---|---|---|
. | (cm−2) . | (kpc) . | ave (min–max) . | . | . |
V2672 Oph | 4.18 × 1021 | 19 ± 2 | 2.51 (0.71–4.24) | 22 | Takei et al. (2014) |
V5584 Sgr | 3.96 × 1021 | 6.3 ± 0.5 | 1.20 (0.38–3.28) | 134 | Raj et al. (2015) |
V496 Sct | 6.81 × 1021 | 2.9 ± 0.3 | 2.22 (0.74–4.75) | 45 | Raj et al. (2012) |
KT Eri | 5.52 × 1020 | 6.6 ± 0.8 | 1.71 (0.61–6.03) | 109 | Imamura and Tanabe (2012) |
V1722 Aql | 9.14 × 1021 | 5 | 1.97 (0.63–6.01) | 112 | Munari et al. (2010) |
V2673 Oph | 2.84 × 1021 | 7.4 | 1.42 (0.43–4.38) | 77 | Munari and Dallaporta (2010) |
V5585 Sgr | 2.75 × 1021 | N/A | 1.76 (0.50–4.36) | 44 | |
V2674 Oph | 4.12 × 1021 | 9 | 1.75 (0.67–3.96) | 30 | Munari, Dallaporta, and Ochner (2010) |
V407 Cyg | 8.19 × 1021 | 2.7 | 1.83 (0.56–4.46) | 52 | Munari, Margoni and Stagni (1990) |
V5586 Sgr | 9.60 × 1021 | N/A | 2.79 (1.21–5.64) | 23 | |
V1311 Sco | 4.78 × 1021 | N/A | 1.98 (0.52–4.44) | 20 | |
V1723 Aql | 1.23 × 1022 | 6 | 1.76 (0.49–4.97) | 140 | Weston et al. (2016) |
V5587 Sgr | 4.09 × 1021 | N/A | 1.56 (0.30–3.67) | 126 | |
V5588 Sgr | 5.47 × 1021 | 7.6 | 2.15 (0.65–5.67) | 122 | Munari et al. (2015) |
T Pyx | 1.88 × 1021 | 3.5 ± 1 | 1.87 (0.43–8.19) | 35 | Schaefer (2010) |
V1312 Sco | 5.14 × 1021 | N/A | 1.61 (0.47–4.64) | 118 | |
PR Lup | 4.82 × 1021 | N/A | 1.25 (0.39–3.76) | 144 | |
V1313 Sco | 4.77 × 1021 | N/A | 1.09 (0.26–3.71) | 55 | |
V965 Per | 1.20 × 1021 | N/A | 3.56 (1.37–8.18) | 17 | |
V834 Car | 4.98 × 1021 | N/A | 1.49 (0.38–5.09) | 121 | |
V1368 Cen | 4.30 × 1021 | N/A | 1.37 (0.46–3.50) | 47 | |
V2676 Oph | 3.02 × 1021 | N/A | 1.34 (0.36–3.56) | 89 | |
V5589 Sgr | 3.35 × 1021 | N/A | 2.21 (0.47–5.85) | 111 | |
V5590 Sgr | 2.64 × 1021 | N/A | 2.19 (0.70–5.50) | 107 | |
V2677 Oph | 3.38 × 1021 | N/A | 3.46 (0.79–11.27) | 44 | |
V1324 Sco | 4.35 × 1021 | 4.5 | 2.56 (0.79–6.05) | 47 | Ackermann et al. (2014) |
V5591 Sgr | 4.27 × 1021 | N/A | 2.31 (0.61–6.59) | 134 | |
V5592 Sgr | 1.49 × 1021 | N/A | 2.01 (0.72–5.96) | 93 | |
V5593 Sgr | 6.54 × 1021 | N/A | 2.31 (0.66–5.97) | 115 | |
V959 Mon | 6.29 × 1021 | 3.6 | 2.68 (0.71–9.77) | 118 | Shore et al. (2013) |
V1724 Aql | 1.47 × 1022 | N/A | 2.49 (0.61–7.11) | 133 | |
V809 Cep | 8.22 × 1021 | 6.5 | 1.98 (0.65–5.25) | 93 | Munari et al. (2014) |
V1533 Sco | 7.42 × 1021 | N/A | 2.10 (0.66–4.36) | 84 | |
V339 Del | 1.36 × 1021 | 4.2 | 2.04 (0.64–6.08) | 140 | Shore (2013) |
V1830 Aql | 1.23 × 1022 | N/A | 3.08 (0.86–8.20) | 128 | |
V556 Ser | 4.87 × 1021 | N/A | 2.54 (0.93–6.70) | 89 | |
V1369 Cen | 5.84 × 1021 | 2.4 | 2.58 (0.74–8.95) | 83 | Shore et al. (2014) |
V962 Cep | 3.30 × 1021 | N/A | 2.72 (1.11–11.86) | 125 | |
V1534 Sco | 3.88 × 1021 | 13 | 1.77 (0.79–4.24) | 22 | Joshi et al. (2015) |
V2659 Cyg | 4.92 × 1021 | N/A | 2.27 (0.73–6.13) | 124 |
*U Sco, V1310 Sco, V5666 Sgr, and V745 Sco listed in table 1 are removed (see text).
†Total Galactic H i column density toward the source as the average of the values obtained by the Leiden/Argentine/Bonn (LAB) map (Kalberla et al. 2005) and the DL map (Dickey & Lockman 1990), calculated using the HEASARC website 〈http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/w3nh/w3nh.pl〉.
‡90% C.L. upper limit for the flux in the 2–4 keV band for each scan in units of 10−2 counts s−1 cm−2. The average (minimum and maximum) fluxes among Ns scans are shown.
§Number of GSC scans in the searched period.
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