Table A.1.
Included hot subdwarfs with a hint of IR excess.
| Name | Class | Reference |
|---|---|---|
| TYC 7489-686-1 | sdB+dM/BD | [6, 11] |
| Feige 34 | sdO+dM | [7] |
| V*EQPsc/PB 5450 | sdBV+dM | [5] |
| PG 1619+522 | sdB+dM | [3, 4] |
| GD 1068 | sdB+dM | [10] |
| CD−23 15853 | sdO+dM | This work. |
| Feige 36 | sdB+dM | [1, 2] |
| HD 149382* | sdOB+dM | [8, 12, 13, 14] |
| TYC 5977-517-1 | sdB+dM/BD | [9] |
| UCAC4 219-125136† | sdB+? | This work. |
Notes. * The hint of IR excess in the SED more likely comes from a nearby contamination star. † A strong IR excess in this system likely comes from background contamination.
References. 1) Saffer et al. (1998), 2) Moran et al. (1999), 3) Maxted et al. (2001), 4) Morales-Rueda et al. (2003), 5) Jeffery & Ramsay (2014), 6) Kawka et al. (2015), 7) Latour et al. (2018a), 8) Schneider et al. (2018), 9) Krzesinski & Balona (2022), 10) Schaffenroth et al. (2022) 11) Schaffenroth et al. (2023), 12) Geier et al. (2009), 13) Ostensen et al. (2005), 14) Jacobs et al. (2011)
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