LIGHTCURVE PHOTOMETRY OPPORTUNITIES: 2015 OCTOBER-DECEMBER

Abstract

We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and have no or poorly-defined lightcurve parameters. Additional data on these objects will help with shape and spin axis modeling via lightcurve inversion. We also include lists of objects that will be the target of radar observations. Lightcurves for these objects can help constrain pole solutions and/or remove rotation period ambiguities that might not come from using radar data alone.

We present several lists of asteroids that are prime targets for photometry during the period 2015 October-December.

In the first three sets of tables, “Dec” is the declination and “U” is the quality code of the lightcurve. See the asteroid lightcurve data base (LCDB; Warner et al., 2009) documentation for an explanation of the U code:

http://www.minorplanet.info/lightcurvedatabase.html

The ephemeris generator on the CALL web site allows you to create custom lists for objects reaching V ≤ 18.5 during any month in the current year, e.g., limiting the results by magnitude and declination.

http://www.minorplanet.info/PHP/call_OppLCDBQuery.php

We refer you to past articles, e.g., Minor Planet Bulletin 36, 188, for more detailed discussions about the individual lists and points of advice regarding observations for objects in each list.

Once you’ve obtained and analyzed your data, it’s important to publish your results. Papers appearing in the Minor Planet Bulletin are indexed in the Astrophysical Data System (ADS) and so can be referenced by others in subsequent papers. It’s also important to make the data available at least on a personal website or upon request. We urge you to consider submitting your raw data to the ALCDEF page on the Minor Planet Center web site:

http://www.minorplanetcenter.net/light_curve

We believe this to be the largest publicly available database of raw lightcurve data that contains 1.9 million observations for more than 2800 objects.

Now that many backyard astronomers and small colleges have access to larger telescopes, we have expanded the photometry opportunities and spin axis lists to include asteroids reaching V = 15.5.

In both of those lists, a line in italics text indicates a near-Earth asteroid (NEA). In the spin axis list, a line in bold text indicates a particularly favorable apparition. To keep the number of objects manageable, the opportunities list includes only those objects reaching a particularly favorable apparition, meaning they could all be set in bold text.

Lightcurve/Photometry Opportunities

Objects with U = 3− or 3 are excluded from this list since they will likely appear in the list below for shape and spin axis modeling. Those asteroids rated U = 1 should be given higher priority over those rated U = 2 or 2+, but not necessarily over those with no period. On the other hand, do not overlook asteroids with U = 2/2+ on the assumption that the period is sufficiently established. Regardless, do not let the existing period influence your analysis since even high quality ratings have been proven wrong at times. Note that the lightcurve amplitude in the tables could be more or less than what’s given. Use the listing only as a guide.

		Brightest			LCDB Data
Number	Name	Date	Mag	Dec	Period	Amp	U
9165	Raup	10 03.8	14.5	−2	560.	1.05	2
12331	1992 UH6	10 04.5	15.1	−6	2.727	0.02	1
1237	Genevieve	10 04.9	13.8	−7	16.37	0.17–0.23	2−
1878	Hughes	10 04.9	15.3	+4
6827	Wombat	10 08.1	15.4	+12	40.1315	0.34	2
3489	Lottie	10 08.6	15.4	+5
2974	Holden	10 08.8	14.9	+10
4815	Anders	10 09.2	15.5	+8
5047	Zanda	10 09.3	15.5	+8
3811	Karma	10 11.3	14.4	+17	11.52	0.20	2
5840	Raybrown	10 13.9	15.3	+7
9851	Sakamoto	10 13.9	15.0	−1
10707	1981 UV23	10 15.2	14.6	−1
4272	Entsuji	10 15.9	13.8	+3
3000	Leonardo	10 19.0	15.0	+9
1016	Anitra	10 20.0	13.6	+13	5.9288	0.28–0.50	2+
3055	Annapavlova	10 21.3	15.4	+21	> 7.
25282	1998 WR	10 22.1	15.1	−3	11.5129	0.40	2
303142	2004 DU24	10 22.8	15.4	+7
705	Erminia	10 22.9	12.6	+28	53.96	0.05–0.17	2
18005	1999 JD91	10 23.1	15.5	−5
26514	2000 CH48	10 23.5	14.9	+7	4.963	0.72	2
5364	1980 RC1	10 25.9	15.1	+18
6339	Giliberti	10 25.9	15.4	+19
4273	Dunhuang	10 28.8	15.1	+7
2343	Siding Spring	10 29.0	13.9	+13
2941	Alden	10 30.3	15.0	+16
1654	Bojeva	10 30.9	14.3	+17		0.1
2959	Scholl	10 31.3	14.9	+6	>16.	0.14	1
4950	House	10 31.3	15.4	+4		0.18
6734	Benzenberg	10 31.8	15.3	+8		0.19
11268	Spassky	11 01.5	15.2	+13
9533	Aleksejleonov	11 01.6	15.5	+11
9060	Toyokawa	11 02.2	15.4	+18
5236	Yoko	11 02.7	15.1	+12	2.768	0.30	2+
14890	1991 VG3	11 03.9	15.5	+13
2787	Tovarishch	11 09.8	15.3	+21
13487	1981 VN	11 10.9	15.3	+21
24602	Mozzhorin	11 10.9	15.3	+16
1001	Gaussia	11 15.9	13.5	+25	9.17	0.04–0.16	2−
5960	Wakkanai	11 16.3	15.1	+20
25332	1999 KK6	11 16.7	15.4	+5	2.4139	0.06–0.08	2+
46620	1994 EL1	11 16.8	15.5	+10	>20.	0.2	2
838	Seraphina	11 16.9	13.4	+20	15.67	0.07–0.30	2
5226	Pollack	11 17.1	15.3	+14	2.725	0.30	2
28321	Arnabdey	11 17.1	15.2	+20
2387	Xi'an	11 19.5	15.0	+20	4.2985	0.24	2
2947	Kippenhahn	11 20.0	14.6	+24	10.5	0.42	2
12738	Satoshimiki	11 20.7	15.2	−8	8.7081	0.20–0.25	2+
4747	Jujo	11 23.2	15.4	+20
2906	Caltech	11 25.6	14.2	+1	12.99	0.16	2
3149	Okudzhava	11 27.0	15.3	+9	2.58	0.3	2
3433	Fehrenbach	11 27.2	14.3	+30	3.9178	0.26	2
1912	Anubis	11 27.7	15.1	+20	4.6256	0.47	2
11643	1997 AM22	12 01.5	15.5	+15
14625	1998 UH31	12 03.1	14.7	+26	4.4873	0.38	2
3613	Kunlun	12 06.0	15.3	+23
7302	1993 CQ	12 09.8	15.3	+11	3.2754	0.19	2
2545	Verbiest	12 11.1	14.4	+34	10.	0.06	1+
3136	Anshan	12 11.1	15.5	+23
1249	Rutherfordia	12 11.3	13.4	+23	18.2	0.69–0.81	2+
2758	Cordelia	12 15.2	15.5	+29
3115	Baily	12 17.3	13.3	+21	16.22	0.08–0.14	2+
4762	Dobrynya	12 19.4	15.1	+37
4904	Makio	12 20.2	15.0	+12	7.83	0.08	2
21609	Williamcaleb	12 23.7	15.4	+10	112.	0.5	2
2282	Andres Bello	12 27.3	15.1	+14

Low Phase Angle Opportunities

The Low Phase Angle list includes asteroids that reach very low phase angles. The “α” column is the minimum solar phase angle for the asteroid. Getting accurate, calibrated measurements (usually V band) at or very near the day of opposition can provide important information for those studying the “opposition effect.” Use the on-line query form for the LCDB

http://www.minorplanet.info/PHP/call_OppLCDBQuery.php to get more details about a specific asteroid.

You will have the best chance of success working objects with low amplitude and periods that allow covering at least half a cycle every night. Objects with large amplitudes and/or long periods are much more difficult for phase angle studies since, for proper analysis, the data must be reduced to the average magnitude of the asteroid for each night. This reduction requires that you determine the period and the amplitude of the lightcurve; for long period objects that can be tricky. Refer to Harris, et al., 1989 (“Phase Relations of High Albedo Asteroids.” Icarus 81, p365 ff) for the details of the analysis procedure.

As an aside, some use the maximum light to find the phase slope parameter (G). However, this can produce a significantly different value for both H and G versus when using average light, which is the method used for values listed by the Minor Planet Center.

Num	Name	Date	α	V	Dec	Period	Amp	U
74	Galatea	10 01.7	0.60	10.6	+04	17.268	0.08–0.16	3
2159	Kukkamaki	10 01.8	0.64	15.1	+05	4.06	0.32	3
2899	Runrun Shaw	10 02.7	0.62	14.9	+02
5674	Wolff	10 02.7	0.90	14.8	+02
215	Oenone	10 02.8	0.29	12.7	+03	27.937	0.18–0.20	3
32774	1986 VZ	10 02.9	0.53	15.5	+03
1023	Thomana	10 03.0	0.49	13.5	+05	17.56	0.27–0.36	3−
158	Koronis	10 03.9	0.57	12.8	+05	14.218	0.28–0.43	3
13762	1998 SG130	10 04.4	0.54	14.5	+03
1878	Hughes	10 04.9	0.07	15.3	+04
82	Alkmene	10 05.1	0.35	12.4	+04	12.999	0.18–0.54	3
3039	Yangel	10 07.2	0.49	15.5	+04
1938	Lausanna	10 07.4	0.85	15.5	+04
1735	ITA	10 08.6	0.75	14.1	+08	12.599	0.27	3−
3489	Lottie	10 08.6	0.34	15.3	+05
2591	Dworetsky	10 09.0	0.25	15.3	+07	12.77	0.45	2
5047	Zanda	10 09.2	0.72	15.5	+08
586	Thekla	10 10.0	0.42	13.3	+08	13.670	0.22–0.30	3
561	Ingwelde	10 11.1	0.43	15.5	+06	12.012	0.38	3
2323	Zverev	10 11.9	0.50	15.1	+08	3.921	0.36–0.39	3
3791	Marci	10 12.2	0.55	15.5	+09
5840	Raybrown	10 13.9	0.23	15.3	+07
340	Eduarda	10 14.0	0.37	12.9	+07	8.0062	0.17–0.32	3
162	Laurentia	10 14.4	0.69	13.4	+06	11.8686	0.28–0.35	3
1894	Haffner	10 14.7	0.46	15.4	+09
80019	1999 HL2	10 14.7	0.26	15.4	+08
855	Newcombia	10 14.8	0.46	14.9	+09	3.003	0.35	3
3454	Lieske	10 15.8	0.75	15.0	+07
187	Lamberta	10 16.1	0.07	12.7	+09	10.670	0.23–0.32	3
229	Adelinda	10 16.4	0.16	13.2	+09	6.60	0.04–0.30	3
30988	2000 WT141	10 18.2	0.54	15.5	+08
3000	Leonardo	10 19.0	0.21	14.9	+09
761	Brendelia	10 19.1	0.05	14.3	+10	57.96	0.25	2+
4017	Disneya	10 19.7	0.29	15.5	+09
2042	Sitarski	10 20.0	0.57	15.5	+11
417	Suevia	10 21.5	0.44	13.6	+09	7.034	0.06–0.22	3
362	Havnia	10 24.7	0.34	11.9	+12	16.92	0.09–0.11	3
3415	Danby	10 26.3	0.46	14.7	+14	5.666	0.09–0.18	3
147	Protogeneia	10 29.3	0.51	12.7	+15	7.8528	0.25–0.28	3
8579	Hieizan	10 29.7	0.80	15.7	+12
2369	Chekhov	10 29.8	0.31	15.5	+13
3403	Tammy	10 31.4	0.76	15.5	+12	11.85	0.10	1
797	Montana	11 01.1	0.92	13.8	+17	4.5463	0.32–0.50	3
5508	Gomyou	11 01.2	0.20	15.4	+15
11268	Spassky	11 01.4	0.95	15.2	+13
257	Silesia	11 02.3	0.22	13.0	+15	15.7095	0.29–0.30	3
1704	Wachmann	11 04.2	0.45	15.4	+16	3.314	0.40	3
1257	Mora	11 04.9	0.32	15.4	+15	5.2948	0.23–0.43	3
3987	Wujek	11 07.7	0.26	15.0	+16
1128	Astrid	11 09.1	0.14	14.4	+16	10.228	0.29	2+
24602	Mozzhorin	11 11.0	0.74	15.2	+16
936	Kunigunde	11 12.1	0.26	14.4	+17	8.80	0.25	2
5401	Minamioda	11 13.2	0.44	14.7	+19
919	Ilsebill	11 13.3	0.15	14.4	+18	5.0325	0.25	3
1421	Esperanto	11 13.5	0.59	14.9	+20	21.982	0.15–0.42	3−
13165	1995 WS1	11 14.2	0.54	15.3	+19
1151	Ithaka	11 15.5	0.83	14.7	+17	4.9312	0.12–0.15	3
5960	Wakkanai	11 16.4	0.82	15.0	+20
838	Seraphina	11 17.0	0.67	13.4	+20	15.67	0.07–0.30	2
28321	Arnabdey	11 17.2	0.51	15.2	+20
1343	Nicole	11 17.7	0.79	14.5	+21	70.	0.29	1
2387	Xi’an	11 19.5	0.38	14.9	+20
6476	1987 VT	11 20.3	0.59	15.3	+21
156	Xanthippe	11 21.1	0.27	13.1	+21	22.37	0.10–0.12	3
4012	Geballe	11 22.0	0.49	14.7	+21
26	Proserpina	11 22.7	0.46	11.2	+21	13.110	0.08–0.21	3
1540	Kevola	11 23.1	0.86	14.6	+23	20.082	0.23	3−
4747	Jujo	11 23.2	0.27	15.4	+20
2197	Shanghai	11 24.2	0.14	15.3	+21	5.99	0.16	2
1857	Parchomenko	11 24.3	0.45	13.8	+20	3.1177	0.22–0.27	3
243	Ida	11 24.7	0.63	13.5	+22	4.634	0.40–0.86	3
640	Brambilla	11 24.8	0.70	13.8	+18	7.768	0.25	3
8610	Goldhaber	11 25.0	0.04	15.3	+21
1545	Thernoe	11 25.9	0.38	14.7	+22	17.20	0.76	3
4801	Ohre	11 27.4	0.20	15.4	+21	32.000	0.50–0.60	3
1912	Anubis	11 27.7	0.38	15.1	+20
3249	Musashino	11 29.4	0.66	14.6	+20	4.5527	0.55	3
1363	Herberta	11 30.0	0.30	15.1	+21
1480	Aunus	11 30.1	0.30	14.9	+22
523	Ada	12 01.6	0.61	12.8	+23	10.03	0.52–0.70	3
3606	Pohjola	12 01.7	0.28	14.6	+22
4323	Hortulus	12 01.8	0.83	15.0	+23	4.7354	0.23	3−
403	Cyane	12 02.1	0.46	12.3	+21	12.283	0.21–0.45	3
220	Stephania	12 02.2	0.92	13.4	+24	18.198	0.21–0.45	3
13388	1999 AE6	12 03.7	0.90	15.0	+20
3613	Kunlun	12 06.0	0.08	15.3	+23
2847	Parvati	12 07.5	0.29	15.3	+22
268	Adorea	12 07.8	0.77	12.7	+20	7.80	0.15–0.20	3
579	Sidonia	12 09.0	0.58	12.1	+21	16.286	0.02–0.28	3−
6384	Kervin	12 09.1	0.26	15.0	+22	3.6203	0.06–0.10	3
395	Delia	12 09.2	0.13	14.4	+23	19.71	0.25	2
1576	Fabiola	12 09.3	0.56	14.4	+21	6.7	0.2	2
2534	Houzeau	12 09.9	0.42	15.1	+22
15305	1992 WT1	12 10.5	0.62	15.5	+22
3136	Anshan	12 11.1	0.12	15.5	+23
2972	Niilo	12 11.9	0.77	15.5	+21
580	Selene	12 13.7	0.57	14.1	+21	9.47	0.27	3−
2555	Thomas	12 14.3	0.23	15.3	+24
2476	Andersen	12 14.7	0.14	15.1	+23
1498	Lahti	12 14.9	0.37	15.4	+24	58.	0.8	1+
951	Gaspra	12 16.4	0.77	13.1	+22	7.042	0.2 1.0	3
1667	Pels	12 16.4	0.23	14.8	+24	3.268	0.20–0.42	3
3115	Baily	12 17.3	0.88	13.3	+21	16.22	0.08–0.14	2+
20762	2000 EE36	12 21.0	0.06	14.9	+24	8.891	0.46	3−
1078	Mentha	12 21.5	0.61	13.6	+22	85.	0.87	3
27	Euterpe	12 25.1	0.14	8.4	+23	10.4082	0.13–0.21	3
1306	Scythia	12 25.8	0.17	13.5	+24	7.525	0.15–0.25	3
1725	CrAO	12 26.7	0.67	15.3	+21	21.45	0.08–0.28	3
2563	Boyarchuk	12 27.7	0.35	15.4	+22	11.04	0.11	2
1209	Pumma	12 31.3	0.43	15.5	+25	8.5001

Shape/Spin Modeling Opportunities

Those doing work for modeling should contact Josef Ďurech at the email address above. If looking to add lightcurves for objects with existing models, visit the Database of Asteroid Models from Inversion Techniques (DAMIT) web site

http://astro.troja.mff.cuni.cz/projects/asteroids3D

An additional dense lightcurve, along with sparse data, could lead to the asteroid being added to or improving one in DAMIT, thus increasing the total number of asteroids with spin axis and shape models.

Included in the list below are objects that:

1. Are rated U = 3− or 3 in the LCDB

2. Do not have reported pole in the LCDB Summary table

3. Have at least three entries in the Details table of the LCDB where the lightcurve is rated U > 2.

The caveat for condition #3 is that no check was made to see if the lightcurves are from the same apparition or if the phase angle bisector longitudes differ significantly from the upcoming apparition. The last check is often not possible because the LCDB does not list the approximate date of observations for all details records. Including that information is an on-going project.

		Brightest			LCDB Data
Num	Name	Date	Mag	Dec	Period	Amp	U
1459	Magnya	10 01.6	13.5	−13	4.678	0.57–0.85	3
74	Galatea	10 01.8	10.6	+4	17.268	0.08–0.16	3
3870	Mayre	10 02.7	15.2	+8	3.9915	0.44–0.45	3
215	Oenone	10 02.8	12.7	+3	27.937	0.18–0.20	3
1023	Thomana	10 03.0	13.5	+5	17.56	0.27–0.36	3−
2074	Shoemaker	10 05.9	15.2	+24	2.5328	0.06–0.12	3
514	Armida	10 06.6	13.0	+10	21.851	0.16–0.42	3
729	Watsonia	10 07.3	13.9	−17	25.23	0.17–0.30	3
890	Waltraut	10 08.5	15.2	−2	12.581	0.32–0.36	3
266	Aline	10 09.6	11.9	+20	13.018	0.07–0.10	3
586	Thekla	10 10.0	13.3	+8	13.67	0.22–0.30	3
929	Algunde	10 10.3	14.3	+10	3.3102	0.13–0.19	3
2323	Zverev	10 11.9	15.1	+8	3.921	0.36–0.39	3
1967	Menzel	10 12.3	13.7	+2	2.835	0.24–0.39	3
3915	Fukushima	10 13.0	15.2	−2	9.418	0.50–0.79	3
759	Vinifera	10 13.3	13.9	+39	14.229	0.36–0.40	3
66146	1998 TU3	10 14.2	15.5	+9	2.375	0.07–0.15	3
855	Newcombia	10 14.7	14.9	+9	3.003	0.33–0.41	3
782	Montefiore	10 16.0	13.9	+1	4.0728	0.42–0.45	3
908	Buda	10 19.2	14.0	−10	14.572	0.09–0.41	3
212	Medea	10 20.1	12.1	+16	10.283	0.04–0.16	3
754	Malabar	10 20.1	13.6	−6	11.74	0.19–0.38	3
947	Monterosa	10 20.9	11.8	+6	5.164	0.15–0.23	3−
362	Havnia	10 24.7	11.9	+12	16.92	0.09–0.17	3
4159	Freeman	10 25.0	14.4	−10	4.4021	0.23–0.40	3
3285	Ruth Wolfe	10 25.3	14.6	+33	3.919	0.20	3
3415	Danby	10 26.2	14.8	+14	5.666	0.09–0.18	3
143	Adria	10 26.9	13.4	+27	22.005	0.05–0.10	3
530	Turandot	10 27.0	13.2	+1	19.96	0.10–0.16	3−
1093	Freda	10 27.2	12.9	−1	19.67	0.04–0.21	3
380	Fiducia	10 29.1	12.6	+5	13.69	0.04–0.32	3
3873	Roddy	10 30.3	15.3	+37	2.4782	0.05–0.11	3
797	Montana	11 01.0	13.8	+17	4.5463	0.32–0.50	3
785	Zwetana	11 03.3	13.8	+5	8.8882	0.13–0.18	3
1425	Tuorla	11 04.7	15.1	+4	7.75	0.17–0.40	3
1257	Mora	11 04.9	15.4	+15	5.2948	0.23–0.43	3
975	Perseverantia	11 05.2	13.9	+16	7.267	0.14–0.23	3
275	Sapientia	11 05.9	13.1	+9	14.931	0.05–0.12	3−
1274	Delportia	11 07.5	14.9	+23	5.615	0.05–0.09	3
1730	Marceline	11 08.1	14.5	+3	3.837	0.94–1.00	3
235	Carolina	11 08.9	12.9	+12	17.61	0.30–0.38	3
3640	Gostin	11 10.5	14.6	+24	3.2641	0.40–0.47	3
2448	Sholokhov	11 12.4	15.4	−7	10.061	0.21–0.63	3−
1115	Sabauda	11 14.4	13.7	+10	6.75	0.16–0.27	3−
1151	Ithaka	11 15.3	14.7	+17	4.9311	0.12–0.15	3
517	Edith	11 16.2	12.6	+22	9.2747	0.08–0.18	3
1999	Hirayama	11 17.3	15.4	+1	15.63	0.45–0.57	3−
6823	1988 ED1	11 19.7	14.9	+4	2.546	0.10–0.30	3−
156	Xanthippe	11 21.1	13.1	+21	22.37	0.10–0.12	3
11424	1999 LZ24	11 22.7	14.1	+17	2.925	0.08	3
240	Vanadis	11 24.4	11.1	+17	10.64	0.30–0.34	3
3682	Welther	11 24.7	13.7	+27	3.5973	0.21–0.35	3
118	Peitho	11 25.1	11.1	+24	7.8055	0.08–0.33	3
698	Ernestina	11 25.1	14.6	+27	5.0363	0.30–0.69	3
504	Cora	11 25.9	13.2	+7	7.588	0.20–0.27	3−
1077	Campanula	11 27.1	14.5	+31	3.8508	0.24–0.40	3
4801	Ohre	11 27.4	15.4	+21	32.	0.50–0.60	3
3028	Zhangguoxi	11 28.1	15.1	+10	4.826	0.12–0.25	3
1225	Ariane	11 30.2	14.1	+26	5.5068	0.30–0.36	3
689	Zita	11 30.9	14.3	+11	6.425	0.30–0.62	3
1376	Michelle	12 01.9	15.1	+16	5.9748	0.03–0.20	3
2294	Andronikov	12 02.1	14.9	+29	3.1529	0.35–0.42	3
5806	Archieroy	12 04.8	15.2	+54	12.163	0.34–0.47	3
762	Pulcova	12 06.3	12.6	+38	5.839	0.18–0.30	3
6384	Kervin	12 09.0	15.1	+22	3.6203	0.06–0.10	3
348	May	12 09.8	13.1	+19	7.3812	0.14–0.16	3
33342	1998 WT24#	12 10.6	11.3	+2	3.697	0.25–0.56	3
1864	Daedalus	12 10.9	15.4	+52	8.572	0.85–1.04	3
204	Kallisto	12 11.3	13.4	+13	19.489	0.09–0.26	3
756	Lilliana	12 12.3	15.1	+1	7.834	0.18–0.99	3
1667	Pels	12 16.3	14.8	+24	3.268	0.20–0.42	3
2105	Gudy	12 17.7	13.3	+33	15.795	0.18–0.52	3−
888	Parysatis	12 18.7	12.2	+8	5.9314	0.22–0.26	3
1520	Imatra	12 20.1	14.5	+18	18.635	0.27–0.35	3−
4254	Kamel	12 22.1	14.9	+2	2.739	0.17–0.19	3
1830	Pogson	12 22.9	14.6	+17	2.57	0.10–0.17	3
1017	Jacqueline	12 24.2	14.4	+18	7.87	0.6–0.72	3
131	Vala	12 25.1	13.2	+27	5.1812	0.09–0.32	3
2004	Lexell	12 25.1	14.6	+28	5.4429	0.42–0.51	3
289	Nenetta	12 25.5	13.2	+13	6.902	0.11–0.19	3
5080	Oja	12 26.3	14.5	+34	7.222	0.31–0.39	3
1505	Koranna	12 26.6	15.3	+14	4.451	0.55–0.70	3
373	Melusina	12 27.4	13.9	+45	12.97	0.20–0.25	3
635	Vundtia	12 27.8	13.3	+7	11.79	0.15–0.27	3
309	Fraternitas	12 28.0	14.6	+29	22.398	0.10–0.13	3
1523	Pieksamaki	12 30.3	14.5	+31	5.3202	0.28–0.47	3

Radar-Optical Opportunities

There are several resources to help plan observations in support of radar.

Future radar targets:

http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods.html

Past radar targets:

http://echo.jpl.nasa.gov/~lance/radar.nea.periods.html

Arecibo targets:

http://www.naic.edu/~pradar/sched.shtml

http://www.naic.edu/~pradar

Goldstone targets:

http://echo.jpl.nasa.gov/asteroids/goldstone_asteroid_schedule.html

However, these are based on known targets at the time the list was prepared. It is very common for newly discovered objects to move up the list and become radar targets on short notice. We recommend that you keep up with the latest discoveries using the RSS feeds from the Minor Planet Center

http://www.minorplanetcenter.net/iau/rss/mpc_feeds.html

In particular, monitor the NEA feed and be flexible with your observing program. In some cases, you may have only 1-3 days when the asteroid is within reach of your equipment. Be sure to keep in touch with the radar team (through Dr. Benner’s email listed above) if you get data. The team may not always be observing the target but, in some cases, your initial results may change their plans. In all cases, your efforts are greatly appreciated.

Use the ephemerides below as a guide to your best chances for observing, but remember that photometry may be possible before and/or after the ephemerides given below. Note that geocentric positions are given. Use these web sites to generate updated and topocentric positions:

MPC: http://www.minorplanetcenter.net/iau/MPEph/MPEph.html

JPL: http://ssd.jpl.nasa.gov/?horizons

In the ephemerides below, ED and SD are, respectively, the Earth and Sun distances (AU), V is the estimated Johnson V magnitude, and α is the phase angle. SE and ME are the great circles distances (in degrees) of the Sun and Moon from the asteroid. MP is the lunar phase and GB is the galactic latitude. “PHA” in the header indicates that the object is a “potentially hazardous asteroid”, meaning that at some (long distant) time, its orbit might take it very close to Earth.

Some of the targets listed here may be carry-overs from the previous quarter’s photometry opportunities article since they are still reachable targets for at least part of the covered quarter-year.

(436724) 2011 UW158 (Oct, H = 19.4, PHA)

This asteroid continues to be an accessible target in early October. It made its closest approach on 2015 July 19 (0.0164 AU) and, at the time this was written in early July, was predicted to be one of the strongest radar target in years. Extensive work by Bruce Gary in 2015 June and July (http://www.brucegary.net/UW158/) found, among other things, a period of 0.610843 ± 0.00005 h (or about 36.651 minutes) with an amplitude of 0.52 mag at a phase angle of 80.5°. The amplitude at low phase angles may be considerably less. Don’t let the existing results dissuade you from obtaining additional data. Observations in October will be at much lower phase angles and so be helpful for modeling the asteroid when combined with existing data.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
10/01	23 54.8	+23 18	0.27	1.25	18.0	17.3	158	48	−0.87	−38
10/02	23 54.5	+22 56	0.27	1.26	18.1	16.9	159	61	−0.78	−38
10/03	23 54.3	+22 33	0.28	1.26	18.1	16.7	159	74	−0.68	−38
10/04	23 54.1	+22 11	0.28	1.27	18.2	16.4	159	86	−0.57	−39
10/05	23 53.9	+21 49	0.29	1.27	18.2	16.2	159	99	−0.47	−39
10/06	23 53.7	+21 28	0.29	1.28	18.2	16.1	159	111	−0.37	−39
10/07	23 53.6	+21 07	0.30	1.28	18.3	16.0	159	122	−0.28	−40
10/08	23 53.5	+20 46	0.31	1.29	18.3	16.0	159	133	−0.19	−40

3200 Phaethon (Oct-Dec, H = 14.6, PHA)

The period for this NEA is well-known at ~3.604 h. Additional observations will help model the asteroid, including a check on whether YORP (a thermal effect) is causing the spin rotation to speed up or down.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
10/01	04 00.6	+42 16	1.66	2.31	18.6	22.4	118	31	−0.88	−8
10/11	03 43.9	+42 44	1.57	2.34	18.4	19.2	130	111	−0.03	−10
10/21	03 21.7	+42 34	1.50	2.36	18.2	15.4	141	115	+0.52	−12
10/31	02 55.8	+41 33	1.46	2.38	18.0	11.6	151	42	−0.84	−16
11/10	02 29.2	+39 37	1.45	2.39	17.9	9.5	156	148	−0.03	−19
11/20	02 05.2	+36 57	1.48	2.40	18.0	10.8	153	67	+0.58	−24
11/30	01 46.1	+33 56	1.54	2.40	18.2	14.1	144	85	−0.81	−28
12/10	01 32.6	+30 58	1.62	2.40	18.5	17.6	132	143	−0.02	−31

(163899) 2003 SD220 (Oct-Dec, H = 16.8, PHA)

The rotation period for this NEA is not known. The estimated diameter is 1.2 km, so it is unlikely that the rotation period is < 2h. The very large phase angles could make for some unusually shaped lightcurves due to deep shadowing effects.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
10/01	08 58.9	+49 57	0.26	0.94	17.3	96.2	69	79	−0.88	+41
10/11	09 12.0	+49 03	0.25	0.96	17.0	90.6	75	58	−0.03	+43
10/21	09 29.8	+47 32	0.23	0.98	16.7	86.4	80	143	+0.52	+46
10/31	09 50.8	+45 23	0.21	1.00	16.4	83.3	84	58	−0.84	+50
11/10	10 14.7	+42 23	0.19	1.00	16.1	81.3	88	70	−0.03	+55
11/20	10 42.1	+38 04	0.16	1.00	15.7	80.7	90	149	+0.58	+61
11/30	11 14.9	+31 15	0.13	1.00	15.3	82.4	90	46	−0.81	+69
12/10	11 58.3	+19 22	0.10	0.98	14.9	88.5	86	69	−0.02	+76
12/20	13 00.3	−01 48	0.08	0.96	15.0	102.7	73	177	+0.66	+61
12/30	14 30.6	−28 54	0.08	0.94	16.2	121.9	54	72	−0.79	+29

(206378) 2003 RB (Oct-Dec, H = 18.7, PHA)

Pravec et al. (2003) reported a period of P > 16 h and amplitude A > 0.2 mag. The low galactic latitudes may make this a difficult target. The long period makes it a good project for a collaboration of observers at significantly different longitudes.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
10/01	06 55.7	+56 58	0.18	1.01	17.9	81.2	89	61	−0.88	+23
10/11	07 14.8	+54 51	0.21	1.04	18.0	74.2	94	76	−0.03	+25
10/21	07 22.8	+53 15	0.24	1.07	18.1	66.2	101	142	+0.52	+26
10/31	07 21.1	+51 58	0.26	1.11	18.1	57.3	110	39	−0.84	+25
11/10	07 09.7	+50 47	0.28	1.16	18.1	47.6	120	103	−0.03	+23
11/20	06 49.2	+49 16	0.31	1.21	18.1	37.2	132	118	+0.58	+20
11/30	06 23.3	+47 03	0.33	1.27	18.0	26.7	145	37	−0.81	+15
12/10	05 57.5	+44 04	0.37	1.33	18.1	17.3	156	142	−0.02	+10

(413577) 2005 UL5 (Nov, H = 20.0, PHA)

Thomas et al. (2014; Icarus 228, 217-246) report this is a type Sq asteroid. Given this, the estimated size for the NEA is about 270 meters. The low galactic latitudes will make this a challenge.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
11/10	05 51.3	+03 15	0.11	1.07	17.2	40.3	135	119	−0.03	−12
11/11	05 54.9	+03 04	0.10	1.07	17.0	40.7	135	130	−0.01	−11
11/12	05 59.2	+02 49	0.09	1.06	16.7	41.3	135	140	+0.00	−10
11/13	06 04.6	+02 32	0.08	1.05	16.5	42.2	135	149	+0.02	−9
11/14	06 11.6	+02 10	0.07	1.04	16.2	43.4	134	158	+0.05	−8
11/15	06 21.0	+01 40	0.06	1.03	15.8	45.2	132	162	+0.11	−6
11/16	06 34.5	+00 57	0.05	1.02	15.5	48.1	130	162	+0.18	−3
11/17	06 55.1	−00 08	0.04	1.01	15.1	52.7	126	159	+0.26	+1
11/18	07 30.4	−01 59	0.03	1.00	14.6	60.9	118	156	+0.36	+8
11/19	08 38.2	−05 21	0.02	0.99	14.4	77.2	102	158	+0.47	+21
11/20	10 50.1	−10 15	0.02	0.98	15.2	109.0	70	162	+0.58	+42
11/21	13 23.9	−11 45	0.02	0.97	18.9	144.9	35	147	+0.69	+50

(33342) 1998 WT24 (Nov-Jan, H = 18.0, PHA)

The period for 1998 WT24 is known to be about 3.698 h. This makes it a potential binary candidate, so higher-precision data are encouraged.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
11/01	09 06.6	−05 59	0.19	0.97	17.4	91.1	78	44	−0.75	+26
11/11	08 58.9	−06 07	0.15	1.00	16.6	82.4	89	83	−0.01	+25
11/21	08 43.5	−06 12	0.10	1.01	15.6	72.3	102	139	+0.69	+21
12/01	07 56.9	−05 26	0.06	1.02	13.8	55.5	122	24	−0.72	+12
12/11	04 17.3	+02 24	0.03	1.01	11.3	23.5	156	163	+0.00	−32
12/21	00 01.4	+09 23	0.05	0.99	14.4	81.4	96	28	+0.76	−52
12/31	23 01.3	+09 41	0.10	0.96	16.5	102.2	72	165	−0.70	−45
01/10	22 35.0	+09 06	0.14	0.91	18.0	116.0	57	56	+0.00	−41

3122 Florence (Dec-Feb, H = 14.2, PHA)

Here is another potential binary candidate: the rotation period is known to be 2.358 h. Observations throughout the ephemeris period can help establish the H and G parameters. The estimated size is 4.5 km.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
12/01	11 16.4	+15 09	1.80	1.97	18.1	29.9	84	34	−0.72	+65
12/11	11 23.3	+13 52	1.72	2.01	18.1	29.2	92	87	+0.00	+66
12/21	11 27.3	+12 48	1.63	2.06	18.0	28.0	101	137	+0.76	+66
12/31	11 28.0	+11 59	1.54	2.10	17.8	26.0	111	9	−0.70	+65
01/10	11 24.9	+11 25	1.46	2.14	17.7	23.1	121	120	+0.00	+64
01/20	11 17.7	+11 06	1.39	2.18	17.5	19.3	133	98	+0.82	+63
01/30	11 06.4	+11 00	1.33	2.22	17.3	14.6	146	33	−0.70	+61
02/09	10 51.7	+11 02	1.30	2.25	17.0	9.0	159	164	+0.00	+58

(294739) 2008 CM (Dec-Jan, H = 17.1, PHA)

Warner (2014, MPB 41, 157-168) found a period of 3.054 h. The amplitude was 0.48 mag at a phase angle α = 70°, about the same as during the first few days of the ephemeris below.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
12/20	14 35.0	+55 09	0.12	0.99	15.7	84.0	89	117	+0.66	+56
12/25	12 11.8	+50 15	0.08	1.01	14.1	68.1	108	80	+1.00	+66
12/30	09 06.6	+15 09	0.06	1.03	12.7	34.9	143	18	−0.79	+37
01/04	07 32.4	−16 45	0.09	1.06	13.8	37.3	139	95	−0.34	+1
01/09	06 50.8	−28 03	0.15	1.08	15.0	44.7	129	133	−0.01	−12
01/14	06 29.6	−32 30	0.20	1.11	15.9	47.7	124	106	+0.19	−18
01/19	06 17.6	−34 29	0.26	1.14	16.5	48.7	120	63	+0.72	−21
01/24	06 10.8	−35 20	0.32	1.17	17.0	48.8	117	59	+1.00	−23

1994 AW1 (Dec-Jan, H = 17.0, PHA)

This is a known binary (Pravec and Hahn, 1997; Icarus 127, 431-440). The primary rotation period is 2.519 h. The orbital period the satellite is 22.3 h, making it difficult for a single station to cover mutual events (occultations and/or eclipses), if viewing geometry allows, thoroughly. This would be a good project for a group of observers who are widely separated in longitude.

DATE	RA	Dec	ED	SD	V	α	SE	ME	MP	GB
12/01	20 49.8	+62 58	0.36	1.10	17.8	62.0	99	103	−0.72	+12
12/06	21 30.4	+62 30	0.35	1.11	17.7	60.6	101	111	−0.26	+8
12/11	22 14.4	+61 22	0.34	1.12	17.6	59.1	104	101	+0.00	+4
12/16	22 59.6	+59 21	0.33	1.12	17.5	57.5	106	74	+0.22	+0
12/21	23 43.5	+56 25	0.33	1.13	17.5	56.1	108	54	+0.76	−5
12/26	00 24.0	+52 37	0.32	1.13	17.4	54.8	110	79	−0.99	−10
12/31	01 00.1	+48 08	0.32	1.14	17.4	53.9	111	121	−0.70	−15
01/05	01 31.8	+43 14	0.33	1.14	17.5	53.4	111	145	−0.25	−19