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Table 3

List of debris-disk candidates with the AKARI 18 μm excess emission (the 2MASS based sample).

Star name IRC name Spectral Distance Age F18,obs$ F18, ∗ $ Excess References
type (pc) (Gyr) (Jy) (Jy) ratio$
(1) (2) (3) (4) (5) (6) (7) (8) (9)

HD 9186 0132297+675740 (B9) 300 ± 80 0.341 0.00775 43 g
HD 9672 0134378-154034 A1V 61 ± 3 0.197 0.0873 1.26 a, g, h
HD 16485 0240209+493337 B9V 500 ± 200 0.191 0.0481 2.97 g
HD 26912 0415320+085332 B3V (B3IV) 130 ± 20 0.351 0.205 0.708 a, g
HD 28375 0428321+012250 (B3V) 120 ± 20 0.570 0.0586 8.73 a, g
HD 32509 0504500+264315 (A2e) 150 ± 30 0.256 0.0223 10.5 a, g
HD 34890 0520289-054843 (A0) 180 ± 50 0.166 0.00638 25 g
HD 36546 0533307+243743 (B8) 100 ± 10 0.684 0.0252 26.1 g
HD 39415 0554415+443007 F5V 0.271 0.0197 12.7 a, h
HD 44892 0623427-162801 (A9/F0IV) 160 ± 20 0.580 0.0742 6.82 a, g, h
HD 64145 0753297+264556 A3V 78 ± 6 0.300 0.183 0.641 h
HD 65372 0758303+025609 (A3) 240 ± 50 0.743 0.0452 15.4 a, g
HD 75416 0841193-785747 B8V 97 ± 4 0.165 0.0604 1.73 f, g
HD 93942 1049236-584703 A1V 34.4 0.00279 12300 b
HD 102323 1146229-562242 (A2IV) 400 ± 200 0.378 0.00646 57.6 a, g
HD 105209 1206526-593529 A1V 0.234 0.0212 10.1 a, b, h
HD 118978 1342010-584712 (B9III) 200 ± 30 0.339 0.0898 2.78 a, g
HD 120780 1352354-505518 K3V (K0V) 16.4 ± 0.3 0.199 0.123 0.61
HD 121617 1357411-470035 A1V 0.321 0.0185 16.4 h
HD 145263 1610551-253122 F0V 120 ± 20 0.481 0.0106 44.6 g, h
HD 146055 1615080-243518 B9V 0.172 0.0196 7.78
HD 155401 1712251-274544 B9V(N) 170 ± 20 0.412 0.0429 8.61 a, g
HD 165014 1804432-205643 F2V 0.948 0.0269 34.3 b, h
HD 166191 1810303-233401 F3/5V (F4V) 140 ± 30 2.44 0.0236 102 a, b, h
HD 167905 1818182-232819 F3V 1.75 0.0317 54.2 a, b, h
HD 169666 1819080+713104 (F5) 51 ± 1 2.0 ± 0.7(1), 2.0(3) 0.128 0.0801 0.604 g
HD 187748 1948154+592523 (G0) 28.4 ± 0.4 3.2(3) 0.197 0.115 0.718
HD 215592 2245380+415258 (A0) 600 ± 300 0.332 0.00953 33.9 g
HD 222173 2338082+431604 B8V 150 ± 20 0.256 0.159 0.611 g
HD 225132 0003444-172009 (B9IVn) 70 ± 4 0.303 0.182 0.662 g
HD 279128 0352162+332422 (B8) 300 ± 100 0.362 0.0232 14.6 g

Notes. Column (1): HD name. Col. (2): Source ID in the AKARI mid-IR PSC. Col. (3): Spectral type quoted from the Tycho-2 spectral type catalog (Wright et al. 2003). The definition in the SIMBAD database is written in parenthesis if it is different from that in the Tycho-2 spectral type catalog. Col. (4): Distance (pc) converted from the parallax in the Hipparcos catalog (Perryman et al. 1997). Col. (5): Stellar age quoted from the literature. References are: (1) Chen et al. (2001) is based on the lithium abundances, (2) Feltzing et al. (2001), and (3) Holmberg et al. (2009). Col. (6): AKARI 18 μm flux. Col. (7): Predicted flux of photosphere at 18 μm. Col. (8): Excess ratio calculated as (F18,obsF18, ∗) /F18, ∗. Col. (9): References for the excess detection are: (a) Oudmaijer et al. (1992), (b) Clarke et al. (2005), (c) Rieke et al. (2005), (d) Bryden et al. (2006), (e) Trilling et al. (2008), (f) Su et al. (2006), (g) McDonald et al. (2012), (h) Fujiwara et al. (2013).

(∗)

Excess ratio shows notably large excess as for debris disks.

(†)

Teff of the central star as a result of photosphere fitting is significantly different from that expected from the spectral type.

(‡)

Diffuse emission component is recognized in the AKARI 18 μm image.

($)

The typical error for the flux, estimated photospheric flux, excess ratio are ~6%, ~2%, and ~6%, respectively.

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