Table A.1
Catalogue of the objects in our final sample that have a low-resolution, optical spectrum and an SED indicative of a disc.
| Object | Right ascension | Declination | LBB | LSED | Teff, SED | E(B − V)SED | Spectral typea | Variabilityb | Remarksc |
| (h:m:s) | (d:m:s) | (L⊙) | (L⊙) | (K) | |||||
|
|
|||||||||
| J044458.39-703522.6 | 04:44:58.39 | -70:35:22.6 | 2000 | 2000 ± 50 | 7000 ± 250 | 0.04 ± 0.01 | F2IIpe! | Ceph. (47.60004) | |
| J045243.16-704737.3 | 04:52:43.17 | -70:47:37.4 | 2000 | 2170 ± 37 | 5500 ± 250 | 0.17 ± 0.01 | F7IIp(e) | SV | |
| J045623.21-692749.0 | 04:56:23.21 | -69:27:49.0 | 6000 | 5780 ± 90 | 4250 ± 250 | 0.07 ± 0.01 | K3Ibp(e) | SV, Fr-99 | |
| J050143.46-694048.4 | 05:01:43.47 | -69:40:48.5 | 2000 | 2900 ± 60 | 5000 ± 250 | 0.23 ± 0.01 | G0Ibp | SV | |
| J050304.95-684024.7 | 05:03:04.96 | -68:40:24.8 | 3000 | 2700 ± 40 | 5750 ± 250 | 0.05 ± 0.01 | F7-9Ibpe | Ceph. (63.51), RVT | AG |
| J051159.40-692532.9 | 05:11:59.40 | -69:25:33.0 | 11000 | 12200 ± 200 | 6250 ± 250 | 0.12 ± 0.01 | F5Ibp | Ceph. (47.92) | |
| J051333.74-663418.9d | 05:13:33.74 | -66:34:19.0 | 20000 | 32500 ± 270 | 6250 ± 250 | 0.00 ± 0.00 | F8-G0Ipe | NV | |
| J051418.09-691234.9 | 05:14:18.10 | -69:12:35.0 | 7000 | 8300 ± 800 | 6250 ± 250 | 0.25 ± 0.04 | F7-9Ibpe | Ceph. (96.745), RVT | AG |
| J051845.47-690321.8 | 05:18:45.47 | -69:03:21.8 | 4000 | 6300 ± 190 | 6750 ± 250 | 0.29 ± 0.01 | F2-4Ibpe | Ceph. (71.505), RVT | AG |
| J052221.13-655551.6 | 05:22:21.14 | -65:55:51.6 | 4000 | 5200 ± 80 | 4250 ± 250 | 0.26 ± 0.01 | K2-3IIp | SV | |
| J052519.48-705410.0 | 05:25:19.49 | -70:54:10.0 | 3000 | 2140 ± 27 | 5500 ± 250 | 0.00 ± 0.00 | G0Ib | Ceph. (67.600), RVT | AG |
| J052627.23-664258.7 | 05:26:27.23 | -66:42:58.7 | 4000 | 4590 ± 100 | 6250 ± 250 | 0.14 ± 0.01 | F6Ibp | Ceph. (71.537) | G |
| J053253.51-695915.1 | 05:32:53.51 | -69:59:15.1 | 1200 | 1440 ± 38 | 4750 ± 250 | 0.11 ± 0.01 | G5 | Ceph. (91.04) | |
| J053336.35-692312.6 | 05:33:36.35 | -69:23:12.7 | 19000 | 11640 ± 180 | 4750 ± 250 | 0.02 ± 0.01 | G8pe | SRV, Fr-99 | G |
| J053453.75-690802.0 | 05:34:53.76 | -69:08:02.1 | 30000 | 32400 ± 1400 | 4250 ± 250 | 0.26 ± 0.03 | K2:Ib(e) | SRV | |
| J053605.89-695802.6 | 05:36:05.90 | -69:58:02.7 | 6000 | 9210 ± 180 | 6750 ± 250 | 0.23 ± 0.01 | F2III: | SV | G |
| J054312.86-683357.1 | 05:43:12.86 | -68:33:57.2 | 3000 | 3900 ± 210 | 6250 ± 250 | 0.33 ± 0.02 | F7Ibp | Ceph. (61.933), RVT | A |
| J054333.39-662202.8 | 05:43:33.39 | -66:22:02.9 | 5000 | 5330 ± 80 | 4500 ± 250 | 0.08 ± 0.01 | G8II | NV, Fr9 | |
| J055326.02-665851.5 | 05:53:26.03 | -66:58:51.6 | 3000 | 2560 ± 50 | 5500 ± 250 | 0.01 ± 0.01 | G0Ibpe | Ceph. (62.444) | |
Notes. We list for each object the name, the position, the calculated values of the luminosity (both based on the BB fit and the SED), the effective temperature, the interstellar reddening, the spectral type, some variability remarks and the catalogues of other types of objects in the LMC in which it is listed.
All spectral types indicated with a superscript a were found in the catalogue of massive stars of Bonanos et al. (2009), the others were determined based on our low-resolution, optical spectra.
The variability remarks are based on both the luminosity curves as discussed in Sect. 5.2 and cross-correlation with the catalogue of Fraser et al. (2008). The latter is indicated with “Fr” with the correct sequence in subscript. Sequences 9, 0 and –99 indicate subsequently that the star is identified with the One-Year Artifact which is caused by the annual observing schedule of the MACHO project, that the star is outside the boundaries of any period-luminosity classification, or that Fraser et al. (2008) were unable to classify this object. The other abbreviations used to characterise the variability of the different objects are Population II Cepheids (Ceph.) which include the subclass of RV Tauri stars (RVT), semi-regular variables (SRV) with the subclass of sequence-D variables (Seq. D) that were recognized by us, objects with lightcurves in Fig. 18 that show long-term, slow variations (SV), R CrB stars (R CrB), objects in regions of very strong nebular emission (em), Ae and Be stars (AB) and objects that do not show strong evidence of variability (NV). For all Population II Cepheids, the periods we computed between deep minima or two cycles of the light curve if the minima are of equal depth, are listed in days.
The final column contains the empirically confirmed cross-matches of the object in the catalogues of Sect. 5.1.3 with “A” standing for the RV T stars listed in the recent OGLE-III Catalogue of Variable Stars (Soszyński et al. 2008), “B” for the R CrB stars in Soszyński et al. (2009b), “C” for the MSX post-AGB stars of Wood & Cohen (2001), “D” are the YSOs from Seale et al. (2009), “E” the AGB stars from Trams et al. (1999), “F” the PNe in Reid & Parker (2006) and “G” the galaxies in the line of sight of the LMC from NED.
This star is unique in our sample in combining a solar type, with unusually strong broad Ca II absorption, and emission of He i (Table 2).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.