2013 - Minor Planet Photometry

357 Ninina
All sessions were linked internally using Canopus V10 CSS method. Red J-C photometric filter were used. No zero point adjustment were made and 0.1 magnitude dispersion could be from tumbling effect. however the slope fitted well into the light curve suggesting that dispersion was due to change in phases and shadowing.

357 Ninina
This light curve was after the individual sessions zero point were adjusted so they all line up.
The period of close to 36 and is 1.5 times commensurate to rotation period of earth.
The light curve is not unique and will require collaboration.

582 Olympia

The H and G Calculator were ploted with data taken with Red filter. The reduced magnitude ploted was based on data directly obtained through calculations based on CSS. no adjustment of the zero point is done.

806 Gyldenia

870 Manto

1110 Jaroslawa

1367 Ngonoma

1387 Kama

1717 Arlon

1830 Pogson
Observations in collaboration with PSABA group. Sessions showing events hence the incongruent light curves. however the primary period is correctly shown.

1979 Sakharov

2055 Dvorak
Data captured with 24" .
PSABA target

2077 Kiangsu

13921 Sgarbini
The object was imaged on some nights with both .35m and .61m telescopes. The  data were measured with the same  method of reduction and same comparison stars to check the reliability of the measurements. the zero point were both needed to be adjusted to obtain this shorter 7.4h period, consistent with  period obtained previously by other observers. Due to the very low amplitude of 0.10m, the 7.4h period is not unique and most likely be the case where the light curve latched on to  it.

2897 Ole_Romer

3060 Delcano
PSABA target

3951 Zichichi
PSABA light curves collaboration with some event captured

26984 Fernand-Roland

4905 Hiromi
PSABA target

6265 1985 TW3

6401 Roentgen
Nearly 12 hours rotation period or 0.5 times commmensurate with earth rotation. Need collaboration to get a unique solution

10484 Hecht

11901 PV11

13921 Sgarbini
The object was imaged on some nights with both .35m and .61m telescopes. The  data were measured with the same  method of reduction and same comparison stars to check the reliability of the measurements. the zero point were both needed to be adjusted to obtain this shorter 7.4h period, consistent with  period obtained previously by other observers. Due to the very low amplitude of 0.10m, the 7.4h period is not unique and most likely be the case where the light curve latched on to  it.

13921 Sgarbini
This light curve is obtained using the usual reduction using solar coloured comparison stars based on 2MASS catalogue. No zero point vertical adjustments were made and the period is searched up to 100h. Presuming 2nd order resulting in bimodal light curve, the 43h period is real. Private communication with Petr Pravec suggest that the period is not unique for lack of supporting data and inconclusive in 2 periodic solutions suggesting binary.

26636 2000 HX57

29818 CM 117

30769 1984 ST2
Another target of opportunity and only obtain 1 session.

34706 2001 OP83

43904 1995 WO
although all sessions were linked, if data zero point were adjusted then there is a period found to be 4.59 hours but with extremely low amplitude of 0.07magnitude. with such low amplitude, the period search tend to latch on to an incorrect period. Further observations required.

43904 1995 WO
All sessions were linked and 43904 found to be a long period asteroid with period approaching 100h.
PSABA target

49636 1999 HJ1
PSABA target

67747 2000 UF43
Opportunity target but period is very provisional. Since the data plot is quite sparse and the duration of the observation is short, this conclusion is not reliable.

99942 Apophis

12854 1998 HA13
This long period asteroid is most likely a tumbler especially due to the different value of the slope diverged from the average light curve.

214736 2006 TY38

163364 2002 OD20

285263 1998 QE2
The close approach of this asteroid provide opportunity for the astronomical community in asteroid research. Radar observations show that this asteroid is a multiple system that photometric observations will show distinctive light curve that suggest binary or multiplicity. However due to the apparent speed during close approach, the light curve changes dramatically making linkages within the nightly observation difficult

53008 1998 VY5