Table A.1
Observation details of the stellar occultation by the TNO Huya.
| Chord number | Observatory (Country) IAU code |
Latitude (N) Longitude (E) Altitude (m) |
Telescope diameter (m) Detector |
Exposure time Cycle time (seconds) |
Observer(s) | Detection σflux |
|---|---|---|---|---|---|---|
| 1 | TÜBITAK National Observatory-1 (Turkey) A84 |
36° 49’17.1” 30° 20’08.0” 2470 |
1.0 SI 1100 Cryo |
2.0 7.44 |
Y. Kilic, T. Ozisik O. Erece, S.E. Kilic |
Positive 0.021 |
| 2 | TÜBITAK National Observatory-2 (Turkey) A84 |
36° 49’29.1” 30° 20’08.2” 2455 |
0.60 FLI Proline 3041 |
15.0 20.0 |
Y. Kilic, T. Ozisik O. Erece, S.E. Kilic |
Positive 0.048 |
| 3 | Romanian Academy, Astron. Obs. Cluj, Feleacu Station (Romania) — |
46° 42’37.6” 23° 35’35.7” 783 |
0.30 SBIG STT-1603ME |
4.0 4.5 |
V. Turcu | Positive 0.038 |
| 4 | ROASTERR-1 Observatory (Romania) L04 |
46° 49’15.6” 23° 35’47.0” 390 |
0.30 ASI 120MM |
0.2 0.5 |
L. Hudin | Positive 0.093 |
| 5 | W-FAST at Wise Observatory (Israel) 097 |
30° 35’48.0” 34° 45’48.0” 900 |
0.57 Andor Zyla |
1.0 1.007 |
G. Nir | Positive 0.015 |
| 6 | C18 at Wise Observatory (Israel) 097 |
30° 35’48.0” 34° 45’48.0” 900 |
0.45 QSI 683 |
3.0 4.46 |
S. Kaspi | Positive 0.009 |
| 7 | Astronomical Inst. of Romanian Academy-1 (Romania) 073 |
44° 24’43.2” 26° 05’38.2” 83 |
0.50 FLI PL16803 |
2.0 4.2 |
A. Sonka S. Anghel |
Positive 0.047 |
| 8 | Astronomical Inst. of Romanian Academy-2 (Romania) 073 |
44° 24’48.0” 26° 05’48.0” 81 |
0.50 Andor Zyla |
1.0 1.025 |
D.A. Nedelcu | Positive 0.041 |
| 9 | ISTEK Belde Observatory (Turkey) — |
41° 01’49.3” 29° 02’33.6” 150 |
0.40 Sony IMX236LQJ CMOS |
0.8 0.8 |
M. Acar A. Atesf C. Kayhan |
Positive 0.088 |
| 10 | Amateur Observatory-1 (Romania) — |
44° 55’05.0” 25° 58’12.1” 167 |
0.15 QHY6 CCD |
4.0 6.0 |
E. Petrescu | Positive 0.030 |
| 11 | St. George Observatory (Romania) L15 |
45° 00’25.2” 25° 58’42.2” 242 |
0.18 ATIK 460EX |
3.0 4.0 |
C. Danescu | Positive 0.026 |
| 12 | Amateur Observatory-2 (Romania) — |
44° 26’36.5” 26° 31’12.5” 65 |
0.20 ASI 1600MM |
0.20 0.25 |
V. Dumitrescu | Positive 0.053 |
| 13 | Stardust Observatory (Romania) L13 |
45° 38’30.0” 25° 37’19.0” 597 |
0.20 CCD Atik 383L+mono (KAF8300) |
8.0 12.0 |
L. Curelaru | Positive 0.016 |
| 14 | Stardreams Observatory —(Romania) L16 |
45° 12’13.3” 26° 02’44.2” 379 |
0.20 ZWO ASI120MM-S |
1.0 1.01 |
R. Gherase | Positive 0.074 |
| 15 | Martin S. Kraar Obs. / Weizmann Inst. (Israel) C78 |
31° 54’29.0” 34° 48’45.0” 107 |
0.40 QHY 367C |
1.0 3.83 |
I. Manulis | Positive 0.056 |
| ★ | Amateur Observatory-3 (Romania) — |
47° 05’02.3” 24° 23’30.9” 331 |
0.40 Watec 902H2 Ultimate |
0.0333 0.0333 |
R. Truta | Positive 0.074 |
| 16 | Amateur Observatory-4 (Romania) — |
44° 45’41.5” 27° 20’25.1” 41 |
0.20 QHY 163M-CMOS |
0.20 0.25 |
D. Bertesfteanu | Positive 0.093 |
| 17 | Bacau Observatory (Romania) L57 |
46° 33’56.3” 26° 54’15.0” 170 |
0.35 SBIG STL 6303E |
2.0 9.0 |
R. Anghel | Positive 0.026 |
| 18 | Galat, i Observatory-1 (Romania) C73 |
45° 25’07.9” 28° 01’57.0” 31 |
0.40 CCD SBIG STL-6303E |
20.0 24.8 |
J.O. Tercu A.-M. Stoian |
Positive 0.011 |
| 18 | Galat, i Observatory-2 (Romania) C73 |
45° 25’07.9” 28° 01’57.0” 31 |
0.20 CCD Atik 383L+Mono |
20.0 31.3 |
J.O. Tercu A.-M. Stoian |
Positive 0.031 |
| 19 | Barlad Observatory (Romania) L22 |
46° 13’54.1” 27° 40’10.2” 70 |
0.20 ASI 1600 |
0.50 0.82 |
C. Vantdevara | Positive 0.068 |
| QOS Observatory (Ukraine) L18 |
48° 50’54.0” 26° 43’12.0” 352 |
0.30 ZWO ASI 174MM |
0.2 0.200016 |
T. O. Dementiev O. M. Kozhukhov |
Negative 0.106 |
|
| Çukurova University (Turkey) — |
37° 03’23.0” 35° 21’04.0” 130 |
0.50 Orion Parsec 8300M |
90 108 |
A. Solmaz M. Tekes |
Negative 0.027 |
|
This Table includes the sites from where the occultation was detected and the closest negatives used to constrain the instantaneous shape of the object. σflux is the flux dispersion, i.e. the standard deviation of the normalized flux (outside of the occultation in the case of positive detections). Sites are sorted by their distance to the center of the predicted shadow path, from West to East. The data from the site marked with * was not used in the final analysis of the occultation (see Section 3 for a detailed explanation).
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