Coordinates, spectral types, distances, radial velocities (RV), and SED groupa of the program stars.
|Star||α (J2000.0)||δ (J2000.0)||Sp. Type||d [pc]||RV [km s-1]||Groupa|
|HD 95881||11:01:57.62||–71:30:48.3||A1/A2III/IVef||118f||+36 ± 2g||II|
|HD 97048||11:08:03.32||–77:39:17.5||A0Vpshed||180d||+18 ± 3h||I|
|HD 100546||11:33:25.44||–70:11:41.2||B9Vned||103d||+16 ± 2h||I|
|HD 101412||11:39:44.46||–60:10:27.7||B9.5Vee||160g||−3 ± 2g||I/II|
|HD 135344B||15:15:48.43||–37:09:16.0||F4Vef||140f||+ 2.5 ± 1.5i||II, TD|
|HD 141569||15:49:57.75||–03:55:16.4||A0Ved||99d||−2 ± 2g||II, TD|
|HD 144432||16:06:57.96||–27:43:09.8||A9IVef||145f||+2 ± 2g||II|
|HD 150193||16:40:17.92||–23:53:45.2||A1Ved||150d||− 6 ± 2g||II|
|51 Oph||17:31:24.95||–23:57:45.5||B9.5Ved||130d||−11 ± 3j||II|
|HD 169142||18:24:29.78||–29:46:49.4||A5Vef||145f||− 3 ± 2g||I|
|R CrA||19:01:53.65||–36:57:07.6||A1-F7ef||130f||0 ± 2g||II|
|HD 179218||19:11:11.25||+15:47:15.6||A0IVed||240d||− 9 ± 2g||I|
|HD 190073||20:03:02.51||+05:44:16.7||A2IVpee||>290g||+3 ± 2g||II|
SED classification by Meeus et al. (2001). Group I sources are with “flared” disks and Group II sources are “self-shadowed” disks. TD means transition disk. These stars lack or have a weak near-infrared excess. This is interpreted as evidence of a hole or gap in the inner disk. Because the star shows evidence of accretion the gap refers only to the lack of small dust particles in the inner disk.
Manoj et al. (2002) argue that HD 58647 may not be a Herbig Ae/Be star but a classical B[e] star. Baines et al. (2006) suggest that HD 58647 is a binary star based on spectropolarimetry of the Hα line.
The status of HD 87643 as a Herbig Ae/Be star is controversial. Oudmaijer et al. (1998) argue that HD 87643 is an evolved B[e] star (see also Kraus 2009). Millour et al. (2009) based on AMBER-VLTI observations reported a close companion at 34 mas. References for the spectral type, distance, and heliocentric radial velocity:
van den Ancker et al. (1998);
Acke et al. (2004) and references therein;
Acke et al. (2005) and references therein;
Kharchenko et al. (2007).
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